CoolWiki - User contributions [en]

C-WAYS Summer visit logistics

2012-06-11T19:23:16Z

French: /* Flight & student & housing details */

I sent out a "big travel document" in March. It has all the information you need re: flights, etc. I will send it again in April or the beginning of May as a reminder.

It will reference [http://coolcosmos.ipac.caltech.edu/cosmic_classroom/teacher_research/visit/ this page] on the CoolCosmos website. This is where you find the legal things, like the student forms.

=High-level schedule=

The work days we've agreed upon are Jul 9-12, where there will be minimal help from me on Jul 12 as sort of a "training run" for when you go home.

I propose you come in relatively early on Jul 8, and plan on doing dinner at my house that night.

*Sunday morning/early afternoon - arrive in LA
*Sunday night - pizza party at Luisa's ... pizza arrives at 6. come by 5 or 5:30 if you want to play with Andrew!
*Monday morning 8:30-12? - lectures
*Monday afternoon 1-5 - software setup. WISE archive workthrough. Start to work with mosaics.
*Tuesday all day - hands-on work with computers -
*Tuesday lunch - career lunch at KS410
*Wednesday morning - JPL tour
*Wednesday afternoon - wrapup, plan for when you go home, learn about LCOGT
*Thursday morning - first thing, 8am, observe from FTS. Then, work on your own or small groups. Try to do some of the tasks we did as a group. Compare notes. Can you work on your own at home without me?
*Thursday afternoon - Reconvene for questions and help.
*Friday - return home

=Software to install=

Make sure you (and all your students who are coming) '''each''' have a '''functional laptop''' that you know how to use with as much of the relevant software installed as possible well before you get on the plane. Trust me. Makes it '''much''' easier if you do all this ahead of time, including starting it up to make sure it works.
*[http://hea-www.harvard.edu/RD/ds9/ ds9]
*[http://spider.ipac.caltech.edu/staff/laher/apt/ APT]
*a web browser (Firefox, Safari, or Google Chrome -- NOT MICROSOFT INTERNET EXPLORER)
*Excel or other spreadsheet program (Google Docs is ok if your school lets you access it; most of the rest of us will be working with various versions of Excel)

Please list your version of Microsoft Office in this table
{| border="1"
|'''Name'''
|'''Microsoft Office version'''
|'''or Microsoft Excell if you don't have the whole suite'''
|'''version of Windows on your laptop(s)'''
|-
|Peggy
|2003, 2007, 2010 (windows)
|
|
|-
|Jackie
|my mac 2008 12.1.7; school's pc 2007; Many students have their own computers so there may be more versions later
|
|
|-
|Lauren
| 2010 (windows on laptop) (2011 at home on mac)
|
|
|-
|Debbie
|2003, 2010 (preferred version)
|
|
|-
|Bob
|2007 at work. 2010 at home.
|
|
|-
|J.D.
|
|
|
|-
|Mark
|
|
|
|-
|Russ
|
|
|
|-
|Babar
|
|
|
|-
|Luisa
| 2008 on the desktop, 2011 on the laptop (which is what you'll see when i hook it up to the projector). NB: they are both Macs!
|
|
|}

'''Also''' make sure you have all the passwords you need for installing new software, getting on a wireless network, or getting back into your machine if it reboots.

Besides the computer, you will need something to write on and something to write with to take notes! Experience has shown that this should be more than post-it notes. I will give you handouts, so the hyperorganized among you may want, e.g., a 3-ring binder.

=Flight & student & housing details=

Debbie - probably 2 (no driving in LA please)

Jackie - 4 students

Lauren - bringing two (adult) students, one male (bringing spouse), one female

Bob - one or 2 (adult) students

Peggy - don't know because switching schools. Probably 3, including one college (will drive in LA but more than happy not to)

JD - (no students)

-> I count ~17 bodies that need to go back and forth from the hotel to campus every day. That probably means 3 vans total. We can certainly pay for 3 vans, but we need 3 drivers of the vans to volunteer...
 
Lets start collecting specifics, keeping to first names should satisfy school rules. 
When you know the names of the people you will have staying in your rooms, call Saga (info below) ask for Lori or Melodee, block of rooms being held for Peggy Piper, and secure your room with your credit card. All rooms $69/night, no charge until departure, 24 hour cancellation fee, rooms must be secured by June 15. There are rooms with two double beds for students who will be sharing rooms. There are rooms with King size beds set aside for the two married couples. The rest of the rooms for individuals will be either King size or double beds. 

Add arrival and departure times when you know them to help us coordinate rides. Arriving late morning morning/early afternoon will allow us to get settled in and then go play with Andrew:) Departing later on Friday will allow us to squeeze in any late additions or just chill by the pool. I was hoping we could all fly in to BUR, but $$ from Chicago are crazy high right now, so Jackie and I may end up needing to go to LAX 

{| border="1"
|'''Teacher'''
|'''Student first names, current grade level, male/female'''
|'''rooms reserved (King, Single, Double)'''
|'''arrival time LAX or BUR'''
|'''departure time LAX or BUR'''
|-
|Peggy driving Van #3
|Emily, 10, female Ashley, 11, female Matt, 13, male
|1 Single, 1 Double, shared Triple Matt rooming with Brandon and Sean
|10:45 a.m. LAX
|4:35 p.m. LAX
|-
|Jackie driving Van #2
|Claire, 11, female Nia, 11, female Viktor, 11, male Gabe, 11, male
|1 Single, 2 Double
|10:45 a.m. LAX
|4:35 p.m. LAX
|-
|Lauren riding in Van #3
|Trista, 14, female Alex, 13, male
|2 doubles, 1 king
|train to Pasadena
|
|-
|Debbie riding in Van #1
|Casey, 10, female Brandon, 12, male
|shared triple Brandon rooming with Matt and Sean
|3:30 p.m. LAX
|11:30 p.m. LAX
|-
|Bob driving Van #1
|Sean, 14, male
|shared triple Sean rooming with Matt and Brandon
|11 a.m. LAX
|
|-
|JD riding in Van #1
|
|
|
|
|}
 Saga Motor Hotel
1633 East Colorado Blvd.
Pasadena, California 91106

Phone:
626-795-0431

Fax:
626-792-0559

Toll Free:
800-793-7242

Email: pasadena@thesagamotorhotel.com

C-WAYS Summer visit logistics

2012-05-30T12:15:50Z

French:

I sent out a "big travel document" in March. It has all the information you need re: flights, etc. I will send it again in April or the beginning of May as a reminder.

It will reference [http://coolcosmos.ipac.caltech.edu/cosmic_classroom/teacher_research/visit/ this page] on the CoolCosmos website. This is where you find the legal things, like the student forms.

=High-level schedule=

The work days we've agreed upon are Jul 9-12, where there will be minimal help from me on Jul 12 as sort of a "training run" for when you go home.

I propose you come in relatively early on Jul 8, and plan on doing dinner at my house that night.

*Sunday morning/early afternoon - arrive in LA
*Sunday night - pizza party at Luisa's ... pizza arrives at 6. come by 5 or 5:30 if you want to play with Andrew!
*Monday morning 8:30-12? - lectures
*Monday afternoon 1-5 - software setup. WISE archive workthrough. Start to work with mosaics.
*Tuesday all day - hands-on work with computers
*Wednesday morning?? - JPL tour
*Wednesday afternoon - wrapup, plan for when you go home
*Thursday morning - Work on your own or small groups. Try to do some of the tasks we did as a group. Compare notes. Can you work on your own at home without me?
*Thursday afternoon - Reconvene for questions and help.
*Friday - return home

TO BE SCHEDULED - WHEN TO LEARN ABOUT THE LCOGT TELESCOPES.

=Software to install=

Make sure you (and all your students who are coming) '''each''' have a '''functional laptop''' that you know how to use with as much of the relevant software installed as possible well before you get on the plane. Trust me. Makes it '''much''' easier if you do all this ahead of time, including starting it up to make sure it works.
*[http://hea-www.harvard.edu/RD/ds9/ ds9]
*[http://spider.ipac.caltech.edu/staff/laher/apt/ APT]
*a web browser (Firefox, Safari, or Google Chrome -- NOT MICROSOFT INTERNET EXPLORER)
*Excel or other spreadsheet program (Google Docs is ok if your school lets you access it; most of the rest of us will be working with various versions of Excel)

Please list your version of Microsoft Office in this table
{| border="1"
|'''Name'''
|'''Microsoft Office version'''
|'''or Microsoft Excell if you don't have the whole suite'''
|'''version of Windows on your laptop(s)'''
|-
|Peggy
|2003, 2007, 2010 (windows)
|
|
|-
|Jackie
|my mac 2008 12.1.7; school's pc 2007; Many students have their own computers so there may be more versions later
|
|
|-
|Lauren
| 2010 (windows on laptop) (2011 at home on mac)
|
|
|-
|Debbie
|2003, 2010 (preferred version)
|
|
|-
|Bob
|2007 at work. 2010 at home.
|
|
|-
|J.D.
|
|
|
|-
|Mark
|
|
|
|-
|Russ
|
|
|
|-
|Babar
|
|
|
|-
|Luisa
| 2008 on the desktop, 2011 on the laptop (which is what you'll see when i hook it up to the projector). NB: they are both Macs!
|
|
|}

'''Also''' make sure you have all the passwords you need for installing new software, getting on a wireless network, or getting back into your machine if it reboots.

Besides the computer, you will need something to write on and something to write with to take notes! Experience has shown that this should be more than post-it notes. I will give you handouts, so the hyperorganized among you may want, e.g., a 3-ring binder.

=Flight & student & housing details=

Debbie - probably 2 (no driving in LA please)

Jackie - certainly 2, maybe 4 people

Lauren - bringing two (adult) students, one male (bringing spouse), one female

Bob - one or 2 (adult) students

Peggy - don't know because switching schools. Probably 3, including one college (will drive in LA but more than happy not to)

JD - (no students)

-> I count ~17 bodies that need to go back and forth from the hotel to campus every day. That probably means 3 vans total. We can certainly pay for 3 vans, but we need 3 drivers of the vans to volunteer...
 
Lets start collecting specifics, keeping to first names should satisfy school rules. 
When you know the names of the people you will have staying in your rooms, call Saga (info below) ask for Lori or Melodee, block of rooms being held for Peggy Piper, and secure your room with your credit card. All rooms $69/night, no charge until departure, 24 hour cancellation fee, rooms must be secured by June 15. There are rooms with two double beds for students who will be sharing rooms. There are rooms with King size beds set aside for the two married couples. The rest of the rooms for individuals will be either King size or double beds. 

Add arrival and departure times when you know them to help us coordinate rides. Arriving late morning morning/early afternoon will allow us to get settled in and then go play with Andrew:) Departing later on Friday will allow us to squeeze in any late additions or just chill by the pool. I was hoping we could all fly in to BUR, but $$ from Chicago are crazy high right now, so Jackie and I may end up needing to go to LAX 

{| border="1"
|'''Teacher'''
|'''Student first names, current grade level, male/female'''
|'''rooms reserved (King, Single, Double)'''
|'''arrival time LAX or BUR'''
|'''departure time LAX or BUR'''
|-
|Peggy
|Emily, 10, female Ashley, 11, female Matt, College Fr, male
|1 Single, 2 Doubles room for 1 male roommate
|
|
|-
|Jackie
|
|
|
|
|-
|Lauren
|Trista, 14, female Alex, 13, male
|2 doubles, 1 king (for married student)
|
|
|-
|Debbie
|Casey, 10, female Brandon, 12, male
|
|
|
|-
|Bob
|
|
|
|
|}
 Saga Motor Hotel
1633 East Colorado Blvd.
Pasadena, California 91106

Phone:
626-795-0431

Fax:
626-792-0559

Toll Free:
800-793-7242

Email: pasadena@thesagamotorhotel.com

Summaries and questions on discussed papers

2012-05-08T16:08:24Z

French: /* "Triggered Star Formation and Evolution of T-Tauri Stars in and Around Bright-Rimmed Clouds" by Chauhan, et al. and "Triggered Star Formation and Young Stellar Population in Bright-Rimmed Cloud SFO 38" by Choudhury, et al. */

----

== Getman 2006 X-Ray Study of Triggered Star Formation and Protostars in IC 1396N ==

An observation of IC 1396N with Chandra, so X-ray light. How long (total time) was the observation? 30 ks = 30 kilo seconds = 30,000 seconds = 500 min = 8.33 hours - '''Is this a long observation? I got the impression from the reading that it was short.'''

''Intro - What will be useful in this section for us?''

'''The cometary globule this study looks at is BRC 38?'''

Nice list of indicators of star formation in IC 1396N. Things we should know about

-IRAS source 21391 +5802

-H2O masers

-molecular outflows

-HH flows

-clusters of IR embedded sources

-radio mm portostars

Explanation of RDI - easy to understand.
Explanation of why an x-ray study - I was surprised. Didn't think about magnetic fields being active in YSO.

----
"2.1 - 2.3 Chandra Observation & Source List - The meat for us!"

The most important things here are the tables and figures. Locations given for the found sources and correlations to 2MASS. '''Will we eventually understand what each of these columns mean?'''

2.1 - Interesting that 8 corrections were made to the data. EIGHT pg 317-8
Data reduced to 117 point sources (listed in table 1); 66 of those correlated with 2MASS; 5 newly identified

----
''Sections 3, 4 & 5 - Interesting things about IC 1396N''

3.1-3.4 Data reduced to sources coming from star formation. 25 sources are probable members of the globule. Sources classified as class 0, I, II, III.

4.1- 4.3 It was interesting that there was flaring going on. '''Are YSO variable in the their light output, like a variable star?''' 4.3 was hard to understand. I have to sort out wavelengths and energies associated with each em light band.

5.1-5.3 Figure 10 a - This is a great picture of results of using different types of observations and even of resolution. Why correlation with other studies is needed.
Figure 10 c - Source 66 and 68 are so much brighter than the others. Interesting. It was also interesting that #66 is the brightest x-ray object in IC 1396N. '''What does it mean that it is 'one of the most heavily absorbed sources'?'''

Questions

1. Does this symbol mean of the Sun? M⊙ = mass in relation to the Sun?

2. What is IMF - initial mass function? pg 328, last full paragraph

3. What is MedE? pg 331 5.2

4. What is intervening column density? pg 332 5.3 2nd paragraph

5. What is extinction? pg 332 5.3 3rd paragraph

----
"Section 6 & 7 - Science questions and summary"

Section 6 pulls the info from the study into the larger science questions - What do these results say about triggered star formation and the two initiation methods mentioned? It seems that RDI (radiation driven implosion) is supported.

I like section 7's summary. Easy to understand and I like the list of classifications of the 25 YSO.

----

== Beltran 2009 The stellar population and complex structure of the bright-rimmed cloud IC 1396N ==

This article discusses the structure of this cloud and gives positions of everything it talks about. 18 pages worth of tables! Their conclusions are also different than the previous paper about star formation.

I found it interesting that individual sources we read about in the previous article have been resolved into several sources by the time this one was written.

Questions

1. They mention that bluer YSO mean older and redder are younger -- this is opposite of main sequence stars

2. '''What is on source images and off sources images? Why do you do this?''' this is to try and adjust for background light

The images went through 5 set of corrections or adjustments before photometry

3.2 The authors conclude not all star formation is triggered star formation in this cloud. Then what else is there?

3.3.1 All this info about H2 knots. Dense material. '''Does the red and blue shift indicate spinning?''' No, it is looking at a jet face on but not perpendicular

3.3.2 H2 flows are complicated. A lot of assumptions are made.

4. 736 sources found in all three bands - J, H K' 128 sources found only in HK' 67 sources found only in K' 79 sources found only in JH

Different conclusions from Getman. An age gradient is not found in the south-north direction of the globule; not all star formation in globule is by triggered star formation. NO alternative method given.

----

----

==Original SFO - Sugitani et al 1991==
Survey of BRCs to describe the BRCs themselves and look for YSOs. 
Palomar Sky Survey (PSS) and IRAS point sources. 

44 BRCs found in Palomar Sky survey prints that had associated IRAS point sources where all found to have IRAS point sources that were good candidates for being YSOs. Tables/images exist for; HII region locations, PPS finding charts, BRC location charts, IRAS point source properties (12, 25, 60, 100 micron), BRC and point source descriptions and plots. 

Questions to ask yourself as you read 

Abstract, Intro and Summary 
-what is the flow of all the types of nebulosity that they describe and the cause/effect relationship to star formation? 
-how will the understanding of this cause/effect help us in our closer study of just three BRCs? 

The Sample, Results 
-how did the authors take advantage of Palomar Sky Survey Prints? 
-how will this help future astronomers with their work? 
-table 3 lists exactly one IRAS source for each BRC, where are the rest of the YSOs we expect to see? 
Discussion 
Although 15 of the IRAS point sources were catagoized as type I and “really are” YSOs, why are all 44 of the sources considered good candidates for YSOs? 
==Most recent paper - Ogura et al 2002==
Looking for H-alpha emissions using grism spectroscopy to find previously undetected YSOs that do not have strong IR excess in order to collect more information on star formation in BRCs and contained HH objects, and further investigate small-scale sequential star formation (SSSSF). 
Optical (H-alpha using grism spectroscopy), 2 MASS 

Questions to ask yourself as you read 

Introduction, Observations and Data Reduction 
-why do the authors recommend higher resolution studies? 
-what is SSSSF and what is the evidence for supporting this hypothesis? 
-what is grism spectroscopy and how does it help “fill in some holes” in terms of YSOs? 
-how did the authors categorize H-alpha equivalent widths in “difficult cases”? Think about the usefulness of this data. 

Images and Data 
-what qualitative and quantitative information will be helpful to us in our study? List tables and images, highlighting information specific to our study. 
H-alpha stars, HH objects and Discussion 
-what did the authors find of interest in our particular BRCs? 
-what evidence is given to support further multi-wavelength studies searching for YSOs?

----

== Info to help you answer questions and things I just don't get ==

Data provided in 2002 paper - observation survey regions, dates, and exposure times; IRAS associated BRCs; H-alpha stars by BRC (BRC 27 (32 stars), 34 (2 stars), 38 (16 stars)), location, H-alpha EW, comments; H-alpha EW distribution; Finding charts (BRC 27 (chart k), 24 (chart o), 38 (chart q)); HH objects location and emission line intensities(BRC 38 only, 9 HH objects, data for 2); HH finding charts (BRC 38 only, chart d)

OB stars are hot, massive, short lived stars that emit enormous amounts of UV which ionizes surrounding interstellar gas forming HII regions and providing ionization/shock fronts to trigger star formation.
HII (H-two) regions are large, low-density clouds with large amounts of ionized atomic hydrogen and other gases. HII regions can be the birthplace of thousands of stars over millions of years until supernova explosions and stellar winds from massive stars disperse the remaining gas and leave behind a cluster (i.e. Pleiades).
Bok globules are dark dense clouds within HII regions, the result of formation of multiple star systems (can contain many young stars) that contain molecular hydrogen, carbon oxides, helium and silicate dust. Cometary globules are Bok globules that have comet like tail (can contain many young stars
BRCs (Bright Rimmed Clouds) are dense clumps of matter (can contain many young stars) in older HII regions which have been further compressed and illuminated and from which surrounding interstellar medium has been dispersed by UV radiation from nearby OB stars.
The hypothesis of small-scale sequential star formation (SSSSF) has redder stars in a BRC closer to the head of the BRC, furthest from the OB exciting star – stars are born as the shock wave moves away from the OB star, the youngest stars are the furthest from the OB star.
HH (Herbig-Haro) are short lived areas of emission nebulae from young stars (there are young stars nearby, possible still hidden in their cocoon), formed when material ejected from the poles of young stars collides with interstellar medium to produce visible light.
Hot Cirrus sources are filamentary (like cirrus clouds) structure that can be seen in the IR, but when “hot cirrus sources” are detected in an HII region, they may be YSOs that have been contaminated at the long wavelengths by emissions from the HII region.
Grism spectroscopy makes use of a prism/diffraction grating to allow light at a central wavelength to pass through. In this study a “wide H-alpha” of 6300-6750 angstroms was used.
???Author talks about JHK observations and two color diagrams, but I do not see data for this???

----

== Spitzer Observations of IC 2118: “Witch Head Nebula” ==

Summary:

The Witch Head Nebula (WHN) is thought to be a site of triggered star formation. Observations in 7 IR bands using SST and 4 bands in optical yields IR excesses in 4 of 6 previously known T Tauri stars and discovery of 6 new candidate YSOs.

This article has a nice introduction that covers a bit of stellar formation overview due to 2 mechanisms: gravitational collapse and “triggered” from nearby events like supernova. The Initial Mass Function (IMF) and the star formation efficiency are supported by the inventory of YSOs formed in a cloud, which then supports closer study of the initial conditions of star formation.

A detailed comparison of the two formation mechanisms with respect to the IMF and stellar formation efficiency will assist with understanding the mechanics of star formation itself.

The data analysis section was highly detailed and technical. This section gave me the greatest comprehension challenge and also the greatest number of questions that require a bit more clarification.

The selection of YSO candidates focused on finding sources having an infrared excess characteristic of YSOs surrounded by a dust disk. A high source contamination rate was expected. Filtering mechanisms form the literature based on Spitzer colors were used to distinguish likely galaxies from likely members. Optical information was used to further winnow the candidate list.

Both color-color and color-magnitude diagrams from IRAC were used to select sources. 459 sources were identified having colors consistent with galaxies dominated by Polycyclic Aromatic Hydrocarbons (PAHs). 765 more sources having colors consistent with active galactic nuclei (AGN), only 27 sources are not flagged as background contaminants and have colors compatible with YSOs and with IRAC excess. The list of 27 sources not flagged as contaminants bears further scrutiny. 18 of the YSO candidates have magnitudes fainter than 12. As the brightness decreases, the probability of the object being background contamination increases.

The wealth of data allowed these data to additionally constrain the YSO selection. 18 faint sources all fall in the region occupied by main-sequence stars or background galaxies. The 9 remaining YSOs with magnitudes less than 12 all appear redder, near or above a 30 Myr isochrones. These are strongly suspected to be contaminants. The 9 brighter objects are included in the list of their (the authors) IRAC selected YSO candidates. There are restrictions imposed with the consequence that leads to a distance assumption that may be problematic. The details of this challenge appear in the bottom half of page 13 for further detailed description, should curiosity require investigation.

All 9 of the IRAC selected YSO candidates are seen at MIPS-24. There is a bit more technical justification about why seeing these candidates in MIPS-24 at one of the two distances proposed (~210 pc and ~440pc).

Most of the sources seen in the observations at 24 or 70 μm are foreground stars or background galaxies.

POSS and 2MASS and optical images for each candidate were used to verify that they did not appear extended in any of these bands. All YSO candidates passed the checks and appear to be point sources in all available bands.

The MIPS selection was technically detailed and the objects seemed to fall into either Class II or Class III with weak excesses. There appears to be three distinct groups of object: 1) objects of zero color (likely foreground or background stars), 2) objects that are faint and red (likely galaxies) and 3) objects that are bright and red (likely YSOs). There doesn’t appear to be any sources between the photospehric Class III and Class II objects. The chosen selection process may have gathered the YSO candidates into the group of brightest or reddest object, lending further support that the assertion of faint object being most likely background galaxies (bottom of page 14). Why is this so??

There is a good amount of detailed description of how the candidates were sorted out from the other sources. From the list of 10 YSO candidates, six are new discoveries. One of the Class II T Tauri stars is a flat disk. The fit for the edge-on-disk candidate was not the same as for the non-disk candidates, since the slope changes significantly depending on whether the MIPS points are included in the fit for the edge-on disk. I think I’d like to understand the slope correlation a bit better…

All of the YSO candidates are located in the head of the nebula, the most massive molecular cloud of the WHN. The distributions lend further support o the assertion that the IRAC and MIPS selected bright object are likely YSOs. The expected YSO candidates for the regions further south were not found. Apparently the conditions in this region do not support substantial star formation. The head of the nebula is about 3 times more massive than any of the other clouds.

There is a nice explanation of at least two intertwined mysteries that enshroud the WHN. The distance to it, and the external source that is responsible for the surface sculpture, illumination and possible trigger mechanism. There is a nice explanation of how the possible two sources (the Trapezium and Rigel) at different distances could solve the mysteries. There are arguments for both explanations, and the conclusion is that there is no clear answer. GAIA (galactic mapping mission proposed to launch in 2013) highlighted text abovecould provide a definitive answer by deriving accurate parallaxes to some objects.

The conclusion for the work states that the inventory of YSOs and candidates has doubles as a result of using Spitzer data to search for objects with IR excess in the region. SEDs are used extensively to identify YSO candidates. If the region is a triggered star formation mechanism, then trends of age or mass as they relate to location may be established. Since there are so few objects, since the distance is uncertain and since the spectral types for most of these objects is unknown, this correlation cannot be done rigorously.

Additional follow-up spectroscopic data are needed to confirm or refute the YSO status for the six new objects.

The new edge –on disk candidate in particular warrants further study, since such objects are relatively rare.

GAIA will be needed to resolve the mystery of the distance to the WHN.

Questions:

What:
1. I want to verify that I understand correctly that bands UVRcIc stand for: Ultraviolet, Visible, Red and Infrared, respectively.
2. Fat fielding issues
3. 100 MJy/ sr
4. Median boxcar filter
5. NaNs
6. UV RcIc
7. “real matches “
8. false source associations
9. centroiding
10. ELAIS
11. U and 70 micro meters
12. Optical Mv
13. VLBA and VLBI
14. mas/yr

How and HUH? : - see text above as well…

1. APEXZ portion of MOPEX
2. Zero point used to convert flux densities to magnitudes
3. …as a final check on our measurements.
4. …through observation of Landolt standards… Does this mean that the additional epoc was just for verification of data integrity?
5. …deviate significantly from zero
Why?
1. The data were further processed…
2. …we wished to add reddened stellar models to the plots…

----

== New Young Star Candidates in the Taurus-Auriga Region as Selected from WISE ==
New Young Star Candidates in the Taurus-Auriga Region as Selected from WISE

Summary: WISE data is used to search for YSO candidates in Taurus from a 260 square degree patch of sky to encompass previously identified Taurus members. Near and mid IR colors are used to select objects with apparent IR excesses and incorporate other catalogs of ancillary data. There is likely to be contamination lingering in this candidate list, and follow up spectra are warranted.

Even though Spitzer is good at finding new young stars, some are located surprisingly far from the traditional location based on CO gas or IRAS dust maps. A 44 square degree survey of Taurus was done with Spitzer. It was found that any solely near and mid IR color selection was filled with contamination from galaxies and asymptotic giant brand (AGB) stars. The use of ancillary data was crucial to establishing a list of high quality new members of Taurus. WISE surveyed the entire sky; the depth of coverage in the Taurus region is somewhat degraded relative to regions of comparable ecliptic latitude due to Moon avoidance maneuvers. Since the cloud is only 140 pc away, both surveys (Spitzer and WISE) should easily detect legitimate Taurus members.

New Taurus candidates were selected with IR excesses using WISE colors with the Koenig et al method. There are three lists: 1) recovered young stars, 2) rejected objects, and 3) candidate new Taurus members.

A substantial multi-wavelength database was assembled for point sources throughout the Taurus region. Not every source has photometry at all bands due to variations in depth and spatial coverage among the surveys involved.

The WISE data acquisition and reduction are discussed in Wright et al, Jarrett et al and in the Explanatory Supplement to the WISE preliminary Data Release Products. Any sources with contamination and confusion flags were rejected, as were “DHOP” (what’s this?) characters.

There were about 2.38 MILLION sources. Signal to Noise Ratio (SNR) measurements were used to drastically shrink the catalog to about 7,000 sources. The SNR cut was used in W4 to limit the contamination. Since the contamination rate for any color selection is expected to be relatively large, ancillary data are crucial for culling the list to high - quality candidates. A rough total of about 2,000 contaminants per square degree were determined. Approximately 1,760 YSO candidates were obtained before imposing additional requirements (which were???) to the SNR be imposed on all four WISE channels reduced the number to 1,014.

Ancillary data were used to weed out contaminants from the list of potential YSO candidates. Only 27 sources on the list of potential YSOs found matches with SDSS spectra.

Of the 1,014 potential YSOs, 196 of them have matches to previously identified stars. 18 of these are listed as unconfirmed candidates in Rebull et al (2010).

Manual Inspection was used to sort objects into “likely contaminant” or “perhaps YSO” bins. The four criteria used to categorize were: 1) matching objects in SIMBAD, 2) matches to objects identified as contaminants in Rebull at al (2010), 3) matches to the 2MASS Extended Source Catalog, and 4) identification as extended in the SDSS pipeline. SEDs were then generated using all the photometric date in the database, and the SEDs were inspected. Based on experience, the SEDs were then categorized as still possible YSO candidates, or likely extragalactic objects. This process may have dropped viable YSO candidates similar to MHO-1 (huh?) or Haro 6-39 (huh?). This process left about 130 candidates. The sources were identified as either being likely subjected to source contamination (HOW?) resolved as a likely galaxy (HOW?) or still apparently clean, point sources (HOW?) This brought the number of candidates down to about 94 objects. All SEDs for the 94 appear in the Appendix.

Projected location of the previously identified YSOs is generally highly clustered along the filamentary distribution of gas and dust, and the new objects are less clustered. The goal was to look for new YSOs outside the canonical groupings of previously known Taurus members. This could also be an indication of persistent contamination in the surviving list of YSOs candidates. There is more discussion about the location of previously identified YSOs and contaminants.

Previous YSOs are generally found in regions of high Av, and background galaxies are found in regions of low Av. The new objects are not particularly clustered, but not evenly distributed either. Most of the previously identified YSOs are bright and most of the contaminants are faint. The new YSO candidates span the range of bright and faint.

The list of objects by type: recovery of 196 previously identified young stars with IR excess, 686 likely to be galaxies, 13 foreground stars, 1 planetary nebula, 24 objects that are likely to be confusing and 94 new YSO candidates that are widely distributed in space.

Questions:

1. What s the “J” in 2MASS J04360131
2. What is color near zero?
3. What is the reddening factor?
4. What is the meaning of “...in the right regime for JHKs diagram”
5. What is “z measurement”?
6. What are large inner disk holes?

----

== New Young Star Candidates in CG4 and Sa101 ==

The introduction to this paper also has some very good background about the Gum Nebula and the stellar formation mechanisms thought to apply within it. Previous studies by Reipurth and Pettersson are summarized, with a conclusion that stars associated with the Cometary Globule 4 (CG4) and Sa 101 are associated with the Gum Nebula. The distances to all considered objects are uncertain; the distances vary from 300 to 500 pc. The extrema of the distance estimates were tested, though the results are not strongly dependent on distance. The region contains previously identified young stars, so it is likely that there are more young stars of lower mass or more embedded than those previously discovered.

The data sections, like the other two papers summarized, are highly technical and summarizing all the details doesn’t seem fruitful beyond this very minimal overview. More detailed reading should be the way to get more detail about the data analysis.

For the IRAC data, two exposures were taken with three dithers per position. The two observational locations were reduced independently even though they overlap on the sky. Some of the very bright stars in the filed of view had instrumental effects that rendered the data very difficult to work with. There is quite a bit of detailed description of calibration technique, correlation and photometry and error reduction methods.

The MIPS 24 and 70 micron data were combined. The 24-micron data were affected by the bright objects and required additional processing. The background levels between the two observations were problematic, and a description of how this was addressed was discussed. Optimized data reduction to obtain brighter source measurements led to many sources fainter than the bright sources in the image being excluded from the catalog because the scientific goals are aimed at brighter objects. There is a good, technical justification of the filtering choices made to process the data.

The optical data used the observed Landolt (1992) standard stars of two or three fields several times per night for photometric calibration. For each target, aperture photometry was performed using multiple size apertures. There is a discussion of the correction used for a noticeable variation of the point-spread function (PSF) that is location dependent on the CCD.

The bandmerging of the photometric data was first merged from all four IRAC channels with the near IR 2MASS data for each observation. This was then merged together with the source lists from each observation. The MIPS data was then included, and then the optical data was merged. A very detailed discussion of how this was done follows.

YSO candidate properties are discussed in the subset of optical, near IR, B-band and SEDs. Optical data can greatly aid in the confirmation or refutation of YSO candidacy because they provide constraints on the Wien side of the SED. Objects with optical data that have already been ruled out as SOs based on the IRAC properties are all well below the 30 Myr isochrones scaled to 500 pc. Deeper optical data are desirable to obtain magnitude estimates for the remaining YSO candidates. The degree of reddening is difficult to estimate because the spectral types for most of the sources are not available. The candidates have infrared excess with a moderate degree of reddening. Young stars that are actively accreting from their circumstellar disks can have excess UV emission in the U or B bands or longer. These bands are also the most sensitive to reddening. Figure 13 is discussed with respect to mass accretion. The coordinates of the YSOs are listed in Table 1. The SEDs of the 22 YSO candidates are displayed in figures 14 - 16. A spectral type of MO was assumed for the remaining objects. A redden model of each object is shown and normalized to the Ks band where possible. These are presented as a guide to the eye rather than a robust fit to the object to allow the immediate IR excesses to be immediately apparent. There is quite a bit of more technically detailed description of the properties in the SEDs section than is summarized here.

There is a galaxy, ESO 257 – G 019 that is mentioned because it appears in the observation field. It has not been studied, and some basic astrometric data about it is listed.

In conclusion, 6 previously identified young stars were rediscovered. There are 16 new YSOs that were discovered and evaluated with ground-based data in the near IR from 2MASS to constrain the SEDs of the candidates. The new young star candidates were graded into confidence groups. Additional data will be needed, such as optical photometry where it is missing and optical spectroscopy to obtain spectral types.

I didn’t have any questions about this article.

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=="Triggered Star Formation and Evolution of T-Tauri Stars in and Around Bright-Rimmed Clouds" by Chauhan, et al. and "Triggered Star Formation and Young Stellar Population in Bright-Rimmed Cloud SFO 38" by Choudhury, et al.==

[[File:Chauhan et al Reading Guide.pdf]]

[[File:Choudhury Guided Reading.pdf]]
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File:Choudhury Guided Reading.pdf

2012-05-08T16:07:20Z

French:

Summaries and questions on discussed papers

2012-05-08T16:06:29Z

File:Chauhan et al Reading Guide.pdf

2012-05-08T16:05:37Z

French: uploaded a new version of "File:Chauhan et al Reading Guide.pdf"

Summaries and questions on discussed papers

2012-05-08T16:04:57Z

French:

Summaries and questions on discussed papers

2012-05-08T16:04:07Z

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== Getman 2006 X-Ray Study of Triggered Star Formation and Protostars in IC 1396N ==

An observation of IC 1396N with Chandra, so X-ray light. How long (total time) was the observation? 30 ks = 30 kilo seconds = 30,000 seconds = 500 min = 8.33 hours - '''Is this a long observation? I got the impression from the reading that it was short.'''

''Intro - What will be useful in this section for us?''

'''The cometary globule this study looks at is BRC 38?'''

Nice list of indicators of star formation in IC 1396N. Things we should know about

-IRAS source 21391 +5802

-H2O masers

-molecular outflows

-HH flows

-clusters of IR embedded sources

-radio mm portostars

Explanation of RDI - easy to understand.
Explanation of why an x-ray study - I was surprised. Didn't think about magnetic fields being active in YSO.

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"2.1 - 2.3 Chandra Observation & Source List - The meat for us!"

The most important things here are the tables and figures. Locations given for the found sources and correlations to 2MASS. '''Will we eventually understand what each of these columns mean?'''

2.1 - Interesting that 8 corrections were made to the data. EIGHT pg 317-8
Data reduced to 117 point sources (listed in table 1); 66 of those correlated with 2MASS; 5 newly identified

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''Sections 3, 4 & 5 - Interesting things about IC 1396N''

3.1-3.4 Data reduced to sources coming from star formation. 25 sources are probable members of the globule. Sources classified as class 0, I, II, III.

4.1- 4.3 It was interesting that there was flaring going on. '''Are YSO variable in the their light output, like a variable star?''' 4.3 was hard to understand. I have to sort out wavelengths and energies associated with each em light band.

5.1-5.3 Figure 10 a - This is a great picture of results of using different types of observations and even of resolution. Why correlation with other studies is needed.
Figure 10 c - Source 66 and 68 are so much brighter than the others. Interesting. It was also interesting that #66 is the brightest x-ray object in IC 1396N. '''What does it mean that it is 'one of the most heavily absorbed sources'?'''

Questions

1. Does this symbol mean of the Sun? M⊙ = mass in relation to the Sun?

2. What is IMF - initial mass function? pg 328, last full paragraph

3. What is MedE? pg 331 5.2

4. What is intervening column density? pg 332 5.3 2nd paragraph

5. What is extinction? pg 332 5.3 3rd paragraph

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"Section 6 & 7 - Science questions and summary"

Section 6 pulls the info from the study into the larger science questions - What do these results say about triggered star formation and the two initiation methods mentioned? It seems that RDI (radiation driven implosion) is supported.

I like section 7's summary. Easy to understand and I like the list of classifications of the 25 YSO.

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== Beltran 2009 The stellar population and complex structure of the bright-rimmed cloud IC 1396N ==

This article discusses the structure of this cloud and gives positions of everything it talks about. 18 pages worth of tables! Their conclusions are also different than the previous paper about star formation.

I found it interesting that individual sources we read about in the previous article have been resolved into several sources by the time this one was written.

Questions

1. They mention that bluer YSO mean older and redder are younger -- this is opposite of main sequence stars

2. '''What is on source images and off sources images? Why do you do this?''' this is to try and adjust for background light

The images went through 5 set of corrections or adjustments before photometry

3.2 The authors conclude not all star formation is triggered star formation in this cloud. Then what else is there?

3.3.1 All this info about H2 knots. Dense material. '''Does the red and blue shift indicate spinning?''' No, it is looking at a jet face on but not perpendicular

3.3.2 H2 flows are complicated. A lot of assumptions are made.

4. 736 sources found in all three bands - J, H K' 128 sources found only in HK' 67 sources found only in K' 79 sources found only in JH

Different conclusions from Getman. An age gradient is not found in the south-north direction of the globule; not all star formation in globule is by triggered star formation. NO alternative method given.

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==Original SFO - Sugitani et al 1991==
Survey of BRCs to describe the BRCs themselves and look for YSOs. 
Palomar Sky Survey (PSS) and IRAS point sources. 

44 BRCs found in Palomar Sky survey prints that had associated IRAS point sources where all found to have IRAS point sources that were good candidates for being YSOs. Tables/images exist for; HII region locations, PPS finding charts, BRC location charts, IRAS point source properties (12, 25, 60, 100 micron), BRC and point source descriptions and plots. 

Questions to ask yourself as you read 

Abstract, Intro and Summary 
-what is the flow of all the types of nebulosity that they describe and the cause/effect relationship to star formation? 
-how will the understanding of this cause/effect help us in our closer study of just three BRCs? 

The Sample, Results 
-how did the authors take advantage of Palomar Sky Survey Prints? 
-how will this help future astronomers with their work? 
-table 3 lists exactly one IRAS source for each BRC, where are the rest of the YSOs we expect to see? 
Discussion 
Although 15 of the IRAS point sources were catagoized as type I and “really are” YSOs, why are all 44 of the sources considered good candidates for YSOs? 
==Most recent paper - Ogura et al 2002==
Looking for H-alpha emissions using grism spectroscopy to find previously undetected YSOs that do not have strong IR excess in order to collect more information on star formation in BRCs and contained HH objects, and further investigate small-scale sequential star formation (SSSSF). 
Optical (H-alpha using grism spectroscopy), 2 MASS 

Questions to ask yourself as you read 

Introduction, Observations and Data Reduction 
-why do the authors recommend higher resolution studies? 
-what is SSSSF and what is the evidence for supporting this hypothesis? 
-what is grism spectroscopy and how does it help “fill in some holes” in terms of YSOs? 
-how did the authors categorize H-alpha equivalent widths in “difficult cases”? Think about the usefulness of this data. 

Images and Data 
-what qualitative and quantitative information will be helpful to us in our study? List tables and images, highlighting information specific to our study. 
H-alpha stars, HH objects and Discussion 
-what did the authors find of interest in our particular BRCs? 
-what evidence is given to support further multi-wavelength studies searching for YSOs?

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== Info to help you answer questions and things I just don't get ==

Data provided in 2002 paper - observation survey regions, dates, and exposure times; IRAS associated BRCs; H-alpha stars by BRC (BRC 27 (32 stars), 34 (2 stars), 38 (16 stars)), location, H-alpha EW, comments; H-alpha EW distribution; Finding charts (BRC 27 (chart k), 24 (chart o), 38 (chart q)); HH objects location and emission line intensities(BRC 38 only, 9 HH objects, data for 2); HH finding charts (BRC 38 only, chart d)

OB stars are hot, massive, short lived stars that emit enormous amounts of UV which ionizes surrounding interstellar gas forming HII regions and providing ionization/shock fronts to trigger star formation.
HII (H-two) regions are large, low-density clouds with large amounts of ionized atomic hydrogen and other gases. HII regions can be the birthplace of thousands of stars over millions of years until supernova explosions and stellar winds from massive stars disperse the remaining gas and leave behind a cluster (i.e. Pleiades).
Bok globules are dark dense clouds within HII regions, the result of formation of multiple star systems (can contain many young stars) that contain molecular hydrogen, carbon oxides, helium and silicate dust. Cometary globules are Bok globules that have comet like tail (can contain many young stars
BRCs (Bright Rimmed Clouds) are dense clumps of matter (can contain many young stars) in older HII regions which have been further compressed and illuminated and from which surrounding interstellar medium has been dispersed by UV radiation from nearby OB stars.
The hypothesis of small-scale sequential star formation (SSSSF) has redder stars in a BRC closer to the head of the BRC, furthest from the OB exciting star – stars are born as the shock wave moves away from the OB star, the youngest stars are the furthest from the OB star.
HH (Herbig-Haro) are short lived areas of emission nebulae from young stars (there are young stars nearby, possible still hidden in their cocoon), formed when material ejected from the poles of young stars collides with interstellar medium to produce visible light.
Hot Cirrus sources are filamentary (like cirrus clouds) structure that can be seen in the IR, but when “hot cirrus sources” are detected in an HII region, they may be YSOs that have been contaminated at the long wavelengths by emissions from the HII region.
Grism spectroscopy makes use of a prism/diffraction grating to allow light at a central wavelength to pass through. In this study a “wide H-alpha” of 6300-6750 angstroms was used.
???Author talks about JHK observations and two color diagrams, but I do not see data for this???

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== Spitzer Observations of IC 2118: “Witch Head Nebula” ==

Summary:

The Witch Head Nebula (WHN) is thought to be a site of triggered star formation. Observations in 7 IR bands using SST and 4 bands in optical yields IR excesses in 4 of 6 previously known T Tauri stars and discovery of 6 new candidate YSOs.

This article has a nice introduction that covers a bit of stellar formation overview due to 2 mechanisms: gravitational collapse and “triggered” from nearby events like supernova. The Initial Mass Function (IMF) and the star formation efficiency are supported by the inventory of YSOs formed in a cloud, which then supports closer study of the initial conditions of star formation.

A detailed comparison of the two formation mechanisms with respect to the IMF and stellar formation efficiency will assist with understanding the mechanics of star formation itself.

The data analysis section was highly detailed and technical. This section gave me the greatest comprehension challenge and also the greatest number of questions that require a bit more clarification.

The selection of YSO candidates focused on finding sources having an infrared excess characteristic of YSOs surrounded by a dust disk. A high source contamination rate was expected. Filtering mechanisms form the literature based on Spitzer colors were used to distinguish likely galaxies from likely members. Optical information was used to further winnow the candidate list.

Both color-color and color-magnitude diagrams from IRAC were used to select sources. 459 sources were identified having colors consistent with galaxies dominated by Polycyclic Aromatic Hydrocarbons (PAHs). 765 more sources having colors consistent with active galactic nuclei (AGN), only 27 sources are not flagged as background contaminants and have colors compatible with YSOs and with IRAC excess. The list of 27 sources not flagged as contaminants bears further scrutiny. 18 of the YSO candidates have magnitudes fainter than 12. As the brightness decreases, the probability of the object being background contamination increases.

The wealth of data allowed these data to additionally constrain the YSO selection. 18 faint sources all fall in the region occupied by main-sequence stars or background galaxies. The 9 remaining YSOs with magnitudes less than 12 all appear redder, near or above a 30 Myr isochrones. These are strongly suspected to be contaminants. The 9 brighter objects are included in the list of their (the authors) IRAC selected YSO candidates. There are restrictions imposed with the consequence that leads to a distance assumption that may be problematic. The details of this challenge appear in the bottom half of page 13 for further detailed description, should curiosity require investigation.

All 9 of the IRAC selected YSO candidates are seen at MIPS-24. There is a bit more technical justification about why seeing these candidates in MIPS-24 at one of the two distances proposed (~210 pc and ~440pc).

Most of the sources seen in the observations at 24 or 70 μm are foreground stars or background galaxies.

POSS and 2MASS and optical images for each candidate were used to verify that they did not appear extended in any of these bands. All YSO candidates passed the checks and appear to be point sources in all available bands.

The MIPS selection was technically detailed and the objects seemed to fall into either Class II or Class III with weak excesses. There appears to be three distinct groups of object: 1) objects of zero color (likely foreground or background stars), 2) objects that are faint and red (likely galaxies) and 3) objects that are bright and red (likely YSOs). There doesn’t appear to be any sources between the photospehric Class III and Class II objects. The chosen selection process may have gathered the YSO candidates into the group of brightest or reddest object, lending further support that the assertion of faint object being most likely background galaxies (bottom of page 14). Why is this so??

There is a good amount of detailed description of how the candidates were sorted out from the other sources. From the list of 10 YSO candidates, six are new discoveries. One of the Class II T Tauri stars is a flat disk. The fit for the edge-on-disk candidate was not the same as for the non-disk candidates, since the slope changes significantly depending on whether the MIPS points are included in the fit for the edge-on disk. I think I’d like to understand the slope correlation a bit better…

All of the YSO candidates are located in the head of the nebula, the most massive molecular cloud of the WHN. The distributions lend further support o the assertion that the IRAC and MIPS selected bright object are likely YSOs. The expected YSO candidates for the regions further south were not found. Apparently the conditions in this region do not support substantial star formation. The head of the nebula is about 3 times more massive than any of the other clouds.

There is a nice explanation of at least two intertwined mysteries that enshroud the WHN. The distance to it, and the external source that is responsible for the surface sculpture, illumination and possible trigger mechanism. There is a nice explanation of how the possible two sources (the Trapezium and Rigel) at different distances could solve the mysteries. There are arguments for both explanations, and the conclusion is that there is no clear answer. GAIA (galactic mapping mission proposed to launch in 2013) highlighted text abovecould provide a definitive answer by deriving accurate parallaxes to some objects.

The conclusion for the work states that the inventory of YSOs and candidates has doubles as a result of using Spitzer data to search for objects with IR excess in the region. SEDs are used extensively to identify YSO candidates. If the region is a triggered star formation mechanism, then trends of age or mass as they relate to location may be established. Since there are so few objects, since the distance is uncertain and since the spectral types for most of these objects is unknown, this correlation cannot be done rigorously.

Additional follow-up spectroscopic data are needed to confirm or refute the YSO status for the six new objects.

The new edge –on disk candidate in particular warrants further study, since such objects are relatively rare.

GAIA will be needed to resolve the mystery of the distance to the WHN.

Questions:

What:
1. I want to verify that I understand correctly that bands UVRcIc stand for: Ultraviolet, Visible, Red and Infrared, respectively.
2. Fat fielding issues
3. 100 MJy/ sr
4. Median boxcar filter
5. NaNs
6. UV RcIc
7. “real matches “
8. false source associations
9. centroiding
10. ELAIS
11. U and 70 micro meters
12. Optical Mv
13. VLBA and VLBI
14. mas/yr

How and HUH? : - see text above as well…

1. APEXZ portion of MOPEX
2. Zero point used to convert flux densities to magnitudes
3. …as a final check on our measurements.
4. …through observation of Landolt standards… Does this mean that the additional epoc was just for verification of data integrity?
5. …deviate significantly from zero
Why?
1. The data were further processed…
2. …we wished to add reddened stellar models to the plots…

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== New Young Star Candidates in the Taurus-Auriga Region as Selected from WISE ==
New Young Star Candidates in the Taurus-Auriga Region as Selected from WISE

Summary: WISE data is used to search for YSO candidates in Taurus from a 260 square degree patch of sky to encompass previously identified Taurus members. Near and mid IR colors are used to select objects with apparent IR excesses and incorporate other catalogs of ancillary data. There is likely to be contamination lingering in this candidate list, and follow up spectra are warranted.

Even though Spitzer is good at finding new young stars, some are located surprisingly far from the traditional location based on CO gas or IRAS dust maps. A 44 square degree survey of Taurus was done with Spitzer. It was found that any solely near and mid IR color selection was filled with contamination from galaxies and asymptotic giant brand (AGB) stars. The use of ancillary data was crucial to establishing a list of high quality new members of Taurus. WISE surveyed the entire sky; the depth of coverage in the Taurus region is somewhat degraded relative to regions of comparable ecliptic latitude due to Moon avoidance maneuvers. Since the cloud is only 140 pc away, both surveys (Spitzer and WISE) should easily detect legitimate Taurus members.

New Taurus candidates were selected with IR excesses using WISE colors with the Koenig et al method. There are three lists: 1) recovered young stars, 2) rejected objects, and 3) candidate new Taurus members.

A substantial multi-wavelength database was assembled for point sources throughout the Taurus region. Not every source has photometry at all bands due to variations in depth and spatial coverage among the surveys involved.

The WISE data acquisition and reduction are discussed in Wright et al, Jarrett et al and in the Explanatory Supplement to the WISE preliminary Data Release Products. Any sources with contamination and confusion flags were rejected, as were “DHOP” (what’s this?) characters.

There were about 2.38 MILLION sources. Signal to Noise Ratio (SNR) measurements were used to drastically shrink the catalog to about 7,000 sources. The SNR cut was used in W4 to limit the contamination. Since the contamination rate for any color selection is expected to be relatively large, ancillary data are crucial for culling the list to high - quality candidates. A rough total of about 2,000 contaminants per square degree were determined. Approximately 1,760 YSO candidates were obtained before imposing additional requirements (which were???) to the SNR be imposed on all four WISE channels reduced the number to 1,014.

Ancillary data were used to weed out contaminants from the list of potential YSO candidates. Only 27 sources on the list of potential YSOs found matches with SDSS spectra.

Of the 1,014 potential YSOs, 196 of them have matches to previously identified stars. 18 of these are listed as unconfirmed candidates in Rebull et al (2010).

Manual Inspection was used to sort objects into “likely contaminant” or “perhaps YSO” bins. The four criteria used to categorize were: 1) matching objects in SIMBAD, 2) matches to objects identified as contaminants in Rebull at al (2010), 3) matches to the 2MASS Extended Source Catalog, and 4) identification as extended in the SDSS pipeline. SEDs were then generated using all the photometric date in the database, and the SEDs were inspected. Based on experience, the SEDs were then categorized as still possible YSO candidates, or likely extragalactic objects. This process may have dropped viable YSO candidates similar to MHO-1 (huh?) or Haro 6-39 (huh?). This process left about 130 candidates. The sources were identified as either being likely subjected to source contamination (HOW?) resolved as a likely galaxy (HOW?) or still apparently clean, point sources (HOW?) This brought the number of candidates down to about 94 objects. All SEDs for the 94 appear in the Appendix.

Projected location of the previously identified YSOs is generally highly clustered along the filamentary distribution of gas and dust, and the new objects are less clustered. The goal was to look for new YSOs outside the canonical groupings of previously known Taurus members. This could also be an indication of persistent contamination in the surviving list of YSOs candidates. There is more discussion about the location of previously identified YSOs and contaminants.

Previous YSOs are generally found in regions of high Av, and background galaxies are found in regions of low Av. The new objects are not particularly clustered, but not evenly distributed either. Most of the previously identified YSOs are bright and most of the contaminants are faint. The new YSO candidates span the range of bright and faint.

The list of objects by type: recovery of 196 previously identified young stars with IR excess, 686 likely to be galaxies, 13 foreground stars, 1 planetary nebula, 24 objects that are likely to be confusing and 94 new YSO candidates that are widely distributed in space.

Questions:

1. What s the “J” in 2MASS J04360131
2. What is color near zero?
3. What is the reddening factor?
4. What is the meaning of “...in the right regime for JHKs diagram”
5. What is “z measurement”?
6. What are large inner disk holes?

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== New Young Star Candidates in CG4 and Sa101 ==

The introduction to this paper also has some very good background about the Gum Nebula and the stellar formation mechanisms thought to apply within it. Previous studies by Reipurth and Pettersson are summarized, with a conclusion that stars associated with the Cometary Globule 4 (CG4) and Sa 101 are associated with the Gum Nebula. The distances to all considered objects are uncertain; the distances vary from 300 to 500 pc. The extrema of the distance estimates were tested, though the results are not strongly dependent on distance. The region contains previously identified young stars, so it is likely that there are more young stars of lower mass or more embedded than those previously discovered.

The data sections, like the other two papers summarized, are highly technical and summarizing all the details doesn’t seem fruitful beyond this very minimal overview. More detailed reading should be the way to get more detail about the data analysis.

For the IRAC data, two exposures were taken with three dithers per position. The two observational locations were reduced independently even though they overlap on the sky. Some of the very bright stars in the filed of view had instrumental effects that rendered the data very difficult to work with. There is quite a bit of detailed description of calibration technique, correlation and photometry and error reduction methods.

The MIPS 24 and 70 micron data were combined. The 24-micron data were affected by the bright objects and required additional processing. The background levels between the two observations were problematic, and a description of how this was addressed was discussed. Optimized data reduction to obtain brighter source measurements led to many sources fainter than the bright sources in the image being excluded from the catalog because the scientific goals are aimed at brighter objects. There is a good, technical justification of the filtering choices made to process the data.

The optical data used the observed Landolt (1992) standard stars of two or three fields several times per night for photometric calibration. For each target, aperture photometry was performed using multiple size apertures. There is a discussion of the correction used for a noticeable variation of the point-spread function (PSF) that is location dependent on the CCD.

The bandmerging of the photometric data was first merged from all four IRAC channels with the near IR 2MASS data for each observation. This was then merged together with the source lists from each observation. The MIPS data was then included, and then the optical data was merged. A very detailed discussion of how this was done follows.

YSO candidate properties are discussed in the subset of optical, near IR, B-band and SEDs. Optical data can greatly aid in the confirmation or refutation of YSO candidacy because they provide constraints on the Wien side of the SED. Objects with optical data that have already been ruled out as SOs based on the IRAC properties are all well below the 30 Myr isochrones scaled to 500 pc. Deeper optical data are desirable to obtain magnitude estimates for the remaining YSO candidates. The degree of reddening is difficult to estimate because the spectral types for most of the sources are not available. The candidates have infrared excess with a moderate degree of reddening. Young stars that are actively accreting from their circumstellar disks can have excess UV emission in the U or B bands or longer. These bands are also the most sensitive to reddening. Figure 13 is discussed with respect to mass accretion. The coordinates of the YSOs are listed in Table 1. The SEDs of the 22 YSO candidates are displayed in figures 14 - 16. A spectral type of MO was assumed for the remaining objects. A redden model of each object is shown and normalized to the Ks band where possible. These are presented as a guide to the eye rather than a robust fit to the object to allow the immediate IR excesses to be immediately apparent. There is quite a bit of more technically detailed description of the properties in the SEDs section than is summarized here.

There is a galaxy, ESO 257 – G 019 that is mentioned because it appears in the observation field. It has not been studied, and some basic astrometric data about it is listed.

In conclusion, 6 previously identified young stars were rediscovered. There are 16 new YSOs that were discovered and evaluated with ground-based data in the near IR from 2MASS to constrain the SEDs of the candidates. The new young star candidates were graded into confidence groups. Additional data will be needed, such as optical photometry where it is missing and optical spectroscopy to obtain spectral types.

I didn’t have any questions about this article.

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==="Triggered Star Formation and Evolution of T-Tauri Stars in and Around Bright-Rimmed Clouds" by Chauhan, et al. and "Triggered Star Formation and Young Stellar Population in Bright-Rimmed Cloud SFO 38" by Choudhury, et al.===

Summaries and questions on discussed papers

2012-05-08T16:03:10Z

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== Getman 2006 X-Ray Study of Triggered Star Formation and Protostars in IC 1396N ==

An observation of IC 1396N with Chandra, so X-ray light. How long (total time) was the observation? 30 ks = 30 kilo seconds = 30,000 seconds = 500 min = 8.33 hours - '''Is this a long observation? I got the impression from the reading that it was short.'''

''Intro - What will be useful in this section for us?''

'''The cometary globule this study looks at is BRC 38?'''

Nice list of indicators of star formation in IC 1396N. Things we should know about

-IRAS source 21391 +5802

-H2O masers

-molecular outflows

-HH flows

-clusters of IR embedded sources

-radio mm portostars

Explanation of RDI - easy to understand.
Explanation of why an x-ray study - I was surprised. Didn't think about magnetic fields being active in YSO.

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"2.1 - 2.3 Chandra Observation & Source List - The meat for us!"

The most important things here are the tables and figures. Locations given for the found sources and correlations to 2MASS. '''Will we eventually understand what each of these columns mean?'''

2.1 - Interesting that 8 corrections were made to the data. EIGHT pg 317-8
Data reduced to 117 point sources (listed in table 1); 66 of those correlated with 2MASS; 5 newly identified

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''Sections 3, 4 & 5 - Interesting things about IC 1396N''

3.1-3.4 Data reduced to sources coming from star formation. 25 sources are probable members of the globule. Sources classified as class 0, I, II, III.

4.1- 4.3 It was interesting that there was flaring going on. '''Are YSO variable in the their light output, like a variable star?''' 4.3 was hard to understand. I have to sort out wavelengths and energies associated with each em light band.

5.1-5.3 Figure 10 a - This is a great picture of results of using different types of observations and even of resolution. Why correlation with other studies is needed.
Figure 10 c - Source 66 and 68 are so much brighter than the others. Interesting. It was also interesting that #66 is the brightest x-ray object in IC 1396N. '''What does it mean that it is 'one of the most heavily absorbed sources'?'''

Questions

1. Does this symbol mean of the Sun? M⊙ = mass in relation to the Sun?

2. What is IMF - initial mass function? pg 328, last full paragraph

3. What is MedE? pg 331 5.2

4. What is intervening column density? pg 332 5.3 2nd paragraph

5. What is extinction? pg 332 5.3 3rd paragraph

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"Section 6 & 7 - Science questions and summary"

Section 6 pulls the info from the study into the larger science questions - What do these results say about triggered star formation and the two initiation methods mentioned? It seems that RDI (radiation driven implosion) is supported.

I like section 7's summary. Easy to understand and I like the list of classifications of the 25 YSO.

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== Beltran 2009 The stellar population and complex structure of the bright-rimmed cloud IC 1396N ==

This article discusses the structure of this cloud and gives positions of everything it talks about. 18 pages worth of tables! Their conclusions are also different than the previous paper about star formation.

I found it interesting that individual sources we read about in the previous article have been resolved into several sources by the time this one was written.

Questions

1. They mention that bluer YSO mean older and redder are younger -- this is opposite of main sequence stars

2. '''What is on source images and off sources images? Why do you do this?''' this is to try and adjust for background light

The images went through 5 set of corrections or adjustments before photometry

3.2 The authors conclude not all star formation is triggered star formation in this cloud. Then what else is there?

3.3.1 All this info about H2 knots. Dense material. '''Does the red and blue shift indicate spinning?''' No, it is looking at a jet face on but not perpendicular

3.3.2 H2 flows are complicated. A lot of assumptions are made.

4. 736 sources found in all three bands - J, H K' 128 sources found only in HK' 67 sources found only in K' 79 sources found only in JH

Different conclusions from Getman. An age gradient is not found in the south-north direction of the globule; not all star formation in globule is by triggered star formation. NO alternative method given.

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==Original SFO - Sugitani et al 1991==
Survey of BRCs to describe the BRCs themselves and look for YSOs. 
Palomar Sky Survey (PSS) and IRAS point sources. 

44 BRCs found in Palomar Sky survey prints that had associated IRAS point sources where all found to have IRAS point sources that were good candidates for being YSOs. Tables/images exist for; HII region locations, PPS finding charts, BRC location charts, IRAS point source properties (12, 25, 60, 100 micron), BRC and point source descriptions and plots. 

Questions to ask yourself as you read 

Abstract, Intro and Summary 
-what is the flow of all the types of nebulosity that they describe and the cause/effect relationship to star formation? 
-how will the understanding of this cause/effect help us in our closer study of just three BRCs? 

The Sample, Results 
-how did the authors take advantage of Palomar Sky Survey Prints? 
-how will this help future astronomers with their work? 
-table 3 lists exactly one IRAS source for each BRC, where are the rest of the YSOs we expect to see? 
Discussion 
Although 15 of the IRAS point sources were catagoized as type I and “really are” YSOs, why are all 44 of the sources considered good candidates for YSOs? 
==Most recent paper - Ogura et al 2002==
Looking for H-alpha emissions using grism spectroscopy to find previously undetected YSOs that do not have strong IR excess in order to collect more information on star formation in BRCs and contained HH objects, and further investigate small-scale sequential star formation (SSSSF). 
Optical (H-alpha using grism spectroscopy), 2 MASS 

Questions to ask yourself as you read 

Introduction, Observations and Data Reduction 
-why do the authors recommend higher resolution studies? 
-what is SSSSF and what is the evidence for supporting this hypothesis? 
-what is grism spectroscopy and how does it help “fill in some holes” in terms of YSOs? 
-how did the authors categorize H-alpha equivalent widths in “difficult cases”? Think about the usefulness of this data. 

Images and Data 
-what qualitative and quantitative information will be helpful to us in our study? List tables and images, highlighting information specific to our study. 
H-alpha stars, HH objects and Discussion 
-what did the authors find of interest in our particular BRCs? 
-what evidence is given to support further multi-wavelength studies searching for YSOs?

----

== Info to help you answer questions and things I just don't get ==

Data provided in 2002 paper - observation survey regions, dates, and exposure times; IRAS associated BRCs; H-alpha stars by BRC (BRC 27 (32 stars), 34 (2 stars), 38 (16 stars)), location, H-alpha EW, comments; H-alpha EW distribution; Finding charts (BRC 27 (chart k), 24 (chart o), 38 (chart q)); HH objects location and emission line intensities(BRC 38 only, 9 HH objects, data for 2); HH finding charts (BRC 38 only, chart d)

OB stars are hot, massive, short lived stars that emit enormous amounts of UV which ionizes surrounding interstellar gas forming HII regions and providing ionization/shock fronts to trigger star formation.
HII (H-two) regions are large, low-density clouds with large amounts of ionized atomic hydrogen and other gases. HII regions can be the birthplace of thousands of stars over millions of years until supernova explosions and stellar winds from massive stars disperse the remaining gas and leave behind a cluster (i.e. Pleiades).
Bok globules are dark dense clouds within HII regions, the result of formation of multiple star systems (can contain many young stars) that contain molecular hydrogen, carbon oxides, helium and silicate dust. Cometary globules are Bok globules that have comet like tail (can contain many young stars
BRCs (Bright Rimmed Clouds) are dense clumps of matter (can contain many young stars) in older HII regions which have been further compressed and illuminated and from which surrounding interstellar medium has been dispersed by UV radiation from nearby OB stars.
The hypothesis of small-scale sequential star formation (SSSSF) has redder stars in a BRC closer to the head of the BRC, furthest from the OB exciting star – stars are born as the shock wave moves away from the OB star, the youngest stars are the furthest from the OB star.
HH (Herbig-Haro) are short lived areas of emission nebulae from young stars (there are young stars nearby, possible still hidden in their cocoon), formed when material ejected from the poles of young stars collides with interstellar medium to produce visible light.
Hot Cirrus sources are filamentary (like cirrus clouds) structure that can be seen in the IR, but when “hot cirrus sources” are detected in an HII region, they may be YSOs that have been contaminated at the long wavelengths by emissions from the HII region.
Grism spectroscopy makes use of a prism/diffraction grating to allow light at a central wavelength to pass through. In this study a “wide H-alpha” of 6300-6750 angstroms was used.
???Author talks about JHK observations and two color diagrams, but I do not see data for this???

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== Spitzer Observations of IC 2118: “Witch Head Nebula” ==

Summary:

The Witch Head Nebula (WHN) is thought to be a site of triggered star formation. Observations in 7 IR bands using SST and 4 bands in optical yields IR excesses in 4 of 6 previously known T Tauri stars and discovery of 6 new candidate YSOs.

This article has a nice introduction that covers a bit of stellar formation overview due to 2 mechanisms: gravitational collapse and “triggered” from nearby events like supernova. The Initial Mass Function (IMF) and the star formation efficiency are supported by the inventory of YSOs formed in a cloud, which then supports closer study of the initial conditions of star formation.

A detailed comparison of the two formation mechanisms with respect to the IMF and stellar formation efficiency will assist with understanding the mechanics of star formation itself.

The data analysis section was highly detailed and technical. This section gave me the greatest comprehension challenge and also the greatest number of questions that require a bit more clarification.

The selection of YSO candidates focused on finding sources having an infrared excess characteristic of YSOs surrounded by a dust disk. A high source contamination rate was expected. Filtering mechanisms form the literature based on Spitzer colors were used to distinguish likely galaxies from likely members. Optical information was used to further winnow the candidate list.

Both color-color and color-magnitude diagrams from IRAC were used to select sources. 459 sources were identified having colors consistent with galaxies dominated by Polycyclic Aromatic Hydrocarbons (PAHs). 765 more sources having colors consistent with active galactic nuclei (AGN), only 27 sources are not flagged as background contaminants and have colors compatible with YSOs and with IRAC excess. The list of 27 sources not flagged as contaminants bears further scrutiny. 18 of the YSO candidates have magnitudes fainter than 12. As the brightness decreases, the probability of the object being background contamination increases.

The wealth of data allowed these data to additionally constrain the YSO selection. 18 faint sources all fall in the region occupied by main-sequence stars or background galaxies. The 9 remaining YSOs with magnitudes less than 12 all appear redder, near or above a 30 Myr isochrones. These are strongly suspected to be contaminants. The 9 brighter objects are included in the list of their (the authors) IRAC selected YSO candidates. There are restrictions imposed with the consequence that leads to a distance assumption that may be problematic. The details of this challenge appear in the bottom half of page 13 for further detailed description, should curiosity require investigation.

All 9 of the IRAC selected YSO candidates are seen at MIPS-24. There is a bit more technical justification about why seeing these candidates in MIPS-24 at one of the two distances proposed (~210 pc and ~440pc).

Most of the sources seen in the observations at 24 or 70 μm are foreground stars or background galaxies.

POSS and 2MASS and optical images for each candidate were used to verify that they did not appear extended in any of these bands. All YSO candidates passed the checks and appear to be point sources in all available bands.

The MIPS selection was technically detailed and the objects seemed to fall into either Class II or Class III with weak excesses. There appears to be three distinct groups of object: 1) objects of zero color (likely foreground or background stars), 2) objects that are faint and red (likely galaxies) and 3) objects that are bright and red (likely YSOs). There doesn’t appear to be any sources between the photospehric Class III and Class II objects. The chosen selection process may have gathered the YSO candidates into the group of brightest or reddest object, lending further support that the assertion of faint object being most likely background galaxies (bottom of page 14). Why is this so??

There is a good amount of detailed description of how the candidates were sorted out from the other sources. From the list of 10 YSO candidates, six are new discoveries. One of the Class II T Tauri stars is a flat disk. The fit for the edge-on-disk candidate was not the same as for the non-disk candidates, since the slope changes significantly depending on whether the MIPS points are included in the fit for the edge-on disk. I think I’d like to understand the slope correlation a bit better…

All of the YSO candidates are located in the head of the nebula, the most massive molecular cloud of the WHN. The distributions lend further support o the assertion that the IRAC and MIPS selected bright object are likely YSOs. The expected YSO candidates for the regions further south were not found. Apparently the conditions in this region do not support substantial star formation. The head of the nebula is about 3 times more massive than any of the other clouds.

There is a nice explanation of at least two intertwined mysteries that enshroud the WHN. The distance to it, and the external source that is responsible for the surface sculpture, illumination and possible trigger mechanism. There is a nice explanation of how the possible two sources (the Trapezium and Rigel) at different distances could solve the mysteries. There are arguments for both explanations, and the conclusion is that there is no clear answer. GAIA (galactic mapping mission proposed to launch in 2013) highlighted text abovecould provide a definitive answer by deriving accurate parallaxes to some objects.

The conclusion for the work states that the inventory of YSOs and candidates has doubles as a result of using Spitzer data to search for objects with IR excess in the region. SEDs are used extensively to identify YSO candidates. If the region is a triggered star formation mechanism, then trends of age or mass as they relate to location may be established. Since there are so few objects, since the distance is uncertain and since the spectral types for most of these objects is unknown, this correlation cannot be done rigorously.

Additional follow-up spectroscopic data are needed to confirm or refute the YSO status for the six new objects.

The new edge –on disk candidate in particular warrants further study, since such objects are relatively rare.

GAIA will be needed to resolve the mystery of the distance to the WHN.

Questions:

What:
1. I want to verify that I understand correctly that bands UVRcIc stand for: Ultraviolet, Visible, Red and Infrared, respectively.
2. Fat fielding issues
3. 100 MJy/ sr
4. Median boxcar filter
5. NaNs
6. UV RcIc
7. “real matches “
8. false source associations
9. centroiding
10. ELAIS
11. U and 70 micro meters
12. Optical Mv
13. VLBA and VLBI
14. mas/yr

How and HUH? : - see text above as well…

1. APEXZ portion of MOPEX
2. Zero point used to convert flux densities to magnitudes
3. …as a final check on our measurements.
4. …through observation of Landolt standards… Does this mean that the additional epoc was just for verification of data integrity?
5. …deviate significantly from zero
Why?
1. The data were further processed…
2. …we wished to add reddened stellar models to the plots…

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== New Young Star Candidates in the Taurus-Auriga Region as Selected from WISE ==
New Young Star Candidates in the Taurus-Auriga Region as Selected from WISE

Summary: WISE data is used to search for YSO candidates in Taurus from a 260 square degree patch of sky to encompass previously identified Taurus members. Near and mid IR colors are used to select objects with apparent IR excesses and incorporate other catalogs of ancillary data. There is likely to be contamination lingering in this candidate list, and follow up spectra are warranted.

Even though Spitzer is good at finding new young stars, some are located surprisingly far from the traditional location based on CO gas or IRAS dust maps. A 44 square degree survey of Taurus was done with Spitzer. It was found that any solely near and mid IR color selection was filled with contamination from galaxies and asymptotic giant brand (AGB) stars. The use of ancillary data was crucial to establishing a list of high quality new members of Taurus. WISE surveyed the entire sky; the depth of coverage in the Taurus region is somewhat degraded relative to regions of comparable ecliptic latitude due to Moon avoidance maneuvers. Since the cloud is only 140 pc away, both surveys (Spitzer and WISE) should easily detect legitimate Taurus members.

New Taurus candidates were selected with IR excesses using WISE colors with the Koenig et al method. There are three lists: 1) recovered young stars, 2) rejected objects, and 3) candidate new Taurus members.

A substantial multi-wavelength database was assembled for point sources throughout the Taurus region. Not every source has photometry at all bands due to variations in depth and spatial coverage among the surveys involved.

The WISE data acquisition and reduction are discussed in Wright et al, Jarrett et al and in the Explanatory Supplement to the WISE preliminary Data Release Products. Any sources with contamination and confusion flags were rejected, as were “DHOP” (what’s this?) characters.

There were about 2.38 MILLION sources. Signal to Noise Ratio (SNR) measurements were used to drastically shrink the catalog to about 7,000 sources. The SNR cut was used in W4 to limit the contamination. Since the contamination rate for any color selection is expected to be relatively large, ancillary data are crucial for culling the list to high - quality candidates. A rough total of about 2,000 contaminants per square degree were determined. Approximately 1,760 YSO candidates were obtained before imposing additional requirements (which were???) to the SNR be imposed on all four WISE channels reduced the number to 1,014.

Ancillary data were used to weed out contaminants from the list of potential YSO candidates. Only 27 sources on the list of potential YSOs found matches with SDSS spectra.

Of the 1,014 potential YSOs, 196 of them have matches to previously identified stars. 18 of these are listed as unconfirmed candidates in Rebull et al (2010).

Manual Inspection was used to sort objects into “likely contaminant” or “perhaps YSO” bins. The four criteria used to categorize were: 1) matching objects in SIMBAD, 2) matches to objects identified as contaminants in Rebull at al (2010), 3) matches to the 2MASS Extended Source Catalog, and 4) identification as extended in the SDSS pipeline. SEDs were then generated using all the photometric date in the database, and the SEDs were inspected. Based on experience, the SEDs were then categorized as still possible YSO candidates, or likely extragalactic objects. This process may have dropped viable YSO candidates similar to MHO-1 (huh?) or Haro 6-39 (huh?). This process left about 130 candidates. The sources were identified as either being likely subjected to source contamination (HOW?) resolved as a likely galaxy (HOW?) or still apparently clean, point sources (HOW?) This brought the number of candidates down to about 94 objects. All SEDs for the 94 appear in the Appendix.

Projected location of the previously identified YSOs is generally highly clustered along the filamentary distribution of gas and dust, and the new objects are less clustered. The goal was to look for new YSOs outside the canonical groupings of previously known Taurus members. This could also be an indication of persistent contamination in the surviving list of YSOs candidates. There is more discussion about the location of previously identified YSOs and contaminants.

Previous YSOs are generally found in regions of high Av, and background galaxies are found in regions of low Av. The new objects are not particularly clustered, but not evenly distributed either. Most of the previously identified YSOs are bright and most of the contaminants are faint. The new YSO candidates span the range of bright and faint.

The list of objects by type: recovery of 196 previously identified young stars with IR excess, 686 likely to be galaxies, 13 foreground stars, 1 planetary nebula, 24 objects that are likely to be confusing and 94 new YSO candidates that are widely distributed in space.

Questions:

1. What s the “J” in 2MASS J04360131
2. What is color near zero?
3. What is the reddening factor?
4. What is the meaning of “...in the right regime for JHKs diagram”
5. What is “z measurement”?
6. What are large inner disk holes?

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== New Young Star Candidates in CG4 and Sa101 ==

The introduction to this paper also has some very good background about the Gum Nebula and the stellar formation mechanisms thought to apply within it. Previous studies by Reipurth and Pettersson are summarized, with a conclusion that stars associated with the Cometary Globule 4 (CG4) and Sa 101 are associated with the Gum Nebula. The distances to all considered objects are uncertain; the distances vary from 300 to 500 pc. The extrema of the distance estimates were tested, though the results are not strongly dependent on distance. The region contains previously identified young stars, so it is likely that there are more young stars of lower mass or more embedded than those previously discovered.

The data sections, like the other two papers summarized, are highly technical and summarizing all the details doesn’t seem fruitful beyond this very minimal overview. More detailed reading should be the way to get more detail about the data analysis.

For the IRAC data, two exposures were taken with three dithers per position. The two observational locations were reduced independently even though they overlap on the sky. Some of the very bright stars in the filed of view had instrumental effects that rendered the data very difficult to work with. There is quite a bit of detailed description of calibration technique, correlation and photometry and error reduction methods.

The MIPS 24 and 70 micron data were combined. The 24-micron data were affected by the bright objects and required additional processing. The background levels between the two observations were problematic, and a description of how this was addressed was discussed. Optimized data reduction to obtain brighter source measurements led to many sources fainter than the bright sources in the image being excluded from the catalog because the scientific goals are aimed at brighter objects. There is a good, technical justification of the filtering choices made to process the data.

The optical data used the observed Landolt (1992) standard stars of two or three fields several times per night for photometric calibration. For each target, aperture photometry was performed using multiple size apertures. There is a discussion of the correction used for a noticeable variation of the point-spread function (PSF) that is location dependent on the CCD.

The bandmerging of the photometric data was first merged from all four IRAC channels with the near IR 2MASS data for each observation. This was then merged together with the source lists from each observation. The MIPS data was then included, and then the optical data was merged. A very detailed discussion of how this was done follows.

YSO candidate properties are discussed in the subset of optical, near IR, B-band and SEDs. Optical data can greatly aid in the confirmation or refutation of YSO candidacy because they provide constraints on the Wien side of the SED. Objects with optical data that have already been ruled out as SOs based on the IRAC properties are all well below the 30 Myr isochrones scaled to 500 pc. Deeper optical data are desirable to obtain magnitude estimates for the remaining YSO candidates. The degree of reddening is difficult to estimate because the spectral types for most of the sources are not available. The candidates have infrared excess with a moderate degree of reddening. Young stars that are actively accreting from their circumstellar disks can have excess UV emission in the U or B bands or longer. These bands are also the most sensitive to reddening. Figure 13 is discussed with respect to mass accretion. The coordinates of the YSOs are listed in Table 1. The SEDs of the 22 YSO candidates are displayed in figures 14 - 16. A spectral type of MO was assumed for the remaining objects. A redden model of each object is shown and normalized to the Ks band where possible. These are presented as a guide to the eye rather than a robust fit to the object to allow the immediate IR excesses to be immediately apparent. There is quite a bit of more technically detailed description of the properties in the SEDs section than is summarized here.

There is a galaxy, ESO 257 – G 019 that is mentioned because it appears in the observation field. It has not been studied, and some basic astrometric data about it is listed.

In conclusion, 6 previously identified young stars were rediscovered. There are 16 new YSOs that were discovered and evaluated with ground-based data in the near IR from 2MASS to constrain the SEDs of the candidates. The new young star candidates were graded into confidence groups. Additional data will be needed, such as optical photometry where it is missing and optical spectroscopy to obtain spectral types.

I didn’t have any questions about this article.

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==="Triggered Star Formation and Evolution of T-Tauri Stars in and Around Bright-Rimmed Clouds" by Chauhan, et al. and "Triggered Star Formation and Young Stellar Population in Bright-Rimmed Cloud SFO 38" by Choudhury, et al.===
----

Summaries and questions on discussed papers

2012-05-08T16:02:37Z

French:

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== Getman 2006 X-Ray Study of Triggered Star Formation and Protostars in IC 1396N ==

An observation of IC 1396N with Chandra, so X-ray light. How long (total time) was the observation? 30 ks = 30 kilo seconds = 30,000 seconds = 500 min = 8.33 hours - '''Is this a long observation? I got the impression from the reading that it was short.'''

''Intro - What will be useful in this section for us?''

'''The cometary globule this study looks at is BRC 38?'''

Nice list of indicators of star formation in IC 1396N. Things we should know about

-IRAS source 21391 +5802

-H2O masers

-molecular outflows

-HH flows

-clusters of IR embedded sources

-radio mm portostars

Explanation of RDI - easy to understand.
Explanation of why an x-ray study - I was surprised. Didn't think about magnetic fields being active in YSO.

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"2.1 - 2.3 Chandra Observation & Source List - The meat for us!"

The most important things here are the tables and figures. Locations given for the found sources and correlations to 2MASS. '''Will we eventually understand what each of these columns mean?'''

2.1 - Interesting that 8 corrections were made to the data. EIGHT pg 317-8
Data reduced to 117 point sources (listed in table 1); 66 of those correlated with 2MASS; 5 newly identified

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''Sections 3, 4 & 5 - Interesting things about IC 1396N''

3.1-3.4 Data reduced to sources coming from star formation. 25 sources are probable members of the globule. Sources classified as class 0, I, II, III.

4.1- 4.3 It was interesting that there was flaring going on. '''Are YSO variable in the their light output, like a variable star?''' 4.3 was hard to understand. I have to sort out wavelengths and energies associated with each em light band.

5.1-5.3 Figure 10 a - This is a great picture of results of using different types of observations and even of resolution. Why correlation with other studies is needed.
Figure 10 c - Source 66 and 68 are so much brighter than the others. Interesting. It was also interesting that #66 is the brightest x-ray object in IC 1396N. '''What does it mean that it is 'one of the most heavily absorbed sources'?'''

Questions

1. Does this symbol mean of the Sun? M⊙ = mass in relation to the Sun?

2. What is IMF - initial mass function? pg 328, last full paragraph

3. What is MedE? pg 331 5.2

4. What is intervening column density? pg 332 5.3 2nd paragraph

5. What is extinction? pg 332 5.3 3rd paragraph

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"Section 6 & 7 - Science questions and summary"

Section 6 pulls the info from the study into the larger science questions - What do these results say about triggered star formation and the two initiation methods mentioned? It seems that RDI (radiation driven implosion) is supported.

I like section 7's summary. Easy to understand and I like the list of classifications of the 25 YSO.

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== Beltran 2009 The stellar population and complex structure of the bright-rimmed cloud IC 1396N ==

This article discusses the structure of this cloud and gives positions of everything it talks about. 18 pages worth of tables! Their conclusions are also different than the previous paper about star formation.

I found it interesting that individual sources we read about in the previous article have been resolved into several sources by the time this one was written.

Questions

1. They mention that bluer YSO mean older and redder are younger -- this is opposite of main sequence stars

2. '''What is on source images and off sources images? Why do you do this?''' this is to try and adjust for background light

The images went through 5 set of corrections or adjustments before photometry

3.2 The authors conclude not all star formation is triggered star formation in this cloud. Then what else is there?

3.3.1 All this info about H2 knots. Dense material. '''Does the red and blue shift indicate spinning?''' No, it is looking at a jet face on but not perpendicular

3.3.2 H2 flows are complicated. A lot of assumptions are made.

4. 736 sources found in all three bands - J, H K' 128 sources found only in HK' 67 sources found only in K' 79 sources found only in JH

Different conclusions from Getman. An age gradient is not found in the south-north direction of the globule; not all star formation in globule is by triggered star formation. NO alternative method given.

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----

==Original SFO - Sugitani et al 1991==
Survey of BRCs to describe the BRCs themselves and look for YSOs. 
Palomar Sky Survey (PSS) and IRAS point sources. 

44 BRCs found in Palomar Sky survey prints that had associated IRAS point sources where all found to have IRAS point sources that were good candidates for being YSOs. Tables/images exist for; HII region locations, PPS finding charts, BRC location charts, IRAS point source properties (12, 25, 60, 100 micron), BRC and point source descriptions and plots. 

Questions to ask yourself as you read 

Abstract, Intro and Summary 
-what is the flow of all the types of nebulosity that they describe and the cause/effect relationship to star formation? 
-how will the understanding of this cause/effect help us in our closer study of just three BRCs? 

The Sample, Results 
-how did the authors take advantage of Palomar Sky Survey Prints? 
-how will this help future astronomers with their work? 
-table 3 lists exactly one IRAS source for each BRC, where are the rest of the YSOs we expect to see? 
Discussion 
Although 15 of the IRAS point sources were catagoized as type I and “really are” YSOs, why are all 44 of the sources considered good candidates for YSOs? 
==Most recent paper - Ogura et al 2002==
Looking for H-alpha emissions using grism spectroscopy to find previously undetected YSOs that do not have strong IR excess in order to collect more information on star formation in BRCs and contained HH objects, and further investigate small-scale sequential star formation (SSSSF). 
Optical (H-alpha using grism spectroscopy), 2 MASS 

Questions to ask yourself as you read 

Introduction, Observations and Data Reduction 
-why do the authors recommend higher resolution studies? 
-what is SSSSF and what is the evidence for supporting this hypothesis? 
-what is grism spectroscopy and how does it help “fill in some holes” in terms of YSOs? 
-how did the authors categorize H-alpha equivalent widths in “difficult cases”? Think about the usefulness of this data. 

Images and Data 
-what qualitative and quantitative information will be helpful to us in our study? List tables and images, highlighting information specific to our study. 
H-alpha stars, HH objects and Discussion 
-what did the authors find of interest in our particular BRCs? 
-what evidence is given to support further multi-wavelength studies searching for YSOs?

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== Info to help you answer questions and things I just don't get ==

Data provided in 2002 paper - observation survey regions, dates, and exposure times; IRAS associated BRCs; H-alpha stars by BRC (BRC 27 (32 stars), 34 (2 stars), 38 (16 stars)), location, H-alpha EW, comments; H-alpha EW distribution; Finding charts (BRC 27 (chart k), 24 (chart o), 38 (chart q)); HH objects location and emission line intensities(BRC 38 only, 9 HH objects, data for 2); HH finding charts (BRC 38 only, chart d)

OB stars are hot, massive, short lived stars that emit enormous amounts of UV which ionizes surrounding interstellar gas forming HII regions and providing ionization/shock fronts to trigger star formation.
HII (H-two) regions are large, low-density clouds with large amounts of ionized atomic hydrogen and other gases. HII regions can be the birthplace of thousands of stars over millions of years until supernova explosions and stellar winds from massive stars disperse the remaining gas and leave behind a cluster (i.e. Pleiades).
Bok globules are dark dense clouds within HII regions, the result of formation of multiple star systems (can contain many young stars) that contain molecular hydrogen, carbon oxides, helium and silicate dust. Cometary globules are Bok globules that have comet like tail (can contain many young stars
BRCs (Bright Rimmed Clouds) are dense clumps of matter (can contain many young stars) in older HII regions which have been further compressed and illuminated and from which surrounding interstellar medium has been dispersed by UV radiation from nearby OB stars.
The hypothesis of small-scale sequential star formation (SSSSF) has redder stars in a BRC closer to the head of the BRC, furthest from the OB exciting star – stars are born as the shock wave moves away from the OB star, the youngest stars are the furthest from the OB star.
HH (Herbig-Haro) are short lived areas of emission nebulae from young stars (there are young stars nearby, possible still hidden in their cocoon), formed when material ejected from the poles of young stars collides with interstellar medium to produce visible light.
Hot Cirrus sources are filamentary (like cirrus clouds) structure that can be seen in the IR, but when “hot cirrus sources” are detected in an HII region, they may be YSOs that have been contaminated at the long wavelengths by emissions from the HII region.
Grism spectroscopy makes use of a prism/diffraction grating to allow light at a central wavelength to pass through. In this study a “wide H-alpha” of 6300-6750 angstroms was used.
???Author talks about JHK observations and two color diagrams, but I do not see data for this???

----

== Spitzer Observations of IC 2118: “Witch Head Nebula” ==

Summary:

The Witch Head Nebula (WHN) is thought to be a site of triggered star formation. Observations in 7 IR bands using SST and 4 bands in optical yields IR excesses in 4 of 6 previously known T Tauri stars and discovery of 6 new candidate YSOs.

This article has a nice introduction that covers a bit of stellar formation overview due to 2 mechanisms: gravitational collapse and “triggered” from nearby events like supernova. The Initial Mass Function (IMF) and the star formation efficiency are supported by the inventory of YSOs formed in a cloud, which then supports closer study of the initial conditions of star formation.

A detailed comparison of the two formation mechanisms with respect to the IMF and stellar formation efficiency will assist with understanding the mechanics of star formation itself.

The data analysis section was highly detailed and technical. This section gave me the greatest comprehension challenge and also the greatest number of questions that require a bit more clarification.

The selection of YSO candidates focused on finding sources having an infrared excess characteristic of YSOs surrounded by a dust disk. A high source contamination rate was expected. Filtering mechanisms form the literature based on Spitzer colors were used to distinguish likely galaxies from likely members. Optical information was used to further winnow the candidate list.

Both color-color and color-magnitude diagrams from IRAC were used to select sources. 459 sources were identified having colors consistent with galaxies dominated by Polycyclic Aromatic Hydrocarbons (PAHs). 765 more sources having colors consistent with active galactic nuclei (AGN), only 27 sources are not flagged as background contaminants and have colors compatible with YSOs and with IRAC excess. The list of 27 sources not flagged as contaminants bears further scrutiny. 18 of the YSO candidates have magnitudes fainter than 12. As the brightness decreases, the probability of the object being background contamination increases.

The wealth of data allowed these data to additionally constrain the YSO selection. 18 faint sources all fall in the region occupied by main-sequence stars or background galaxies. The 9 remaining YSOs with magnitudes less than 12 all appear redder, near or above a 30 Myr isochrones. These are strongly suspected to be contaminants. The 9 brighter objects are included in the list of their (the authors) IRAC selected YSO candidates. There are restrictions imposed with the consequence that leads to a distance assumption that may be problematic. The details of this challenge appear in the bottom half of page 13 for further detailed description, should curiosity require investigation.

All 9 of the IRAC selected YSO candidates are seen at MIPS-24. There is a bit more technical justification about why seeing these candidates in MIPS-24 at one of the two distances proposed (~210 pc and ~440pc).

Most of the sources seen in the observations at 24 or 70 μm are foreground stars or background galaxies.

POSS and 2MASS and optical images for each candidate were used to verify that they did not appear extended in any of these bands. All YSO candidates passed the checks and appear to be point sources in all available bands.

The MIPS selection was technically detailed and the objects seemed to fall into either Class II or Class III with weak excesses. There appears to be three distinct groups of object: 1) objects of zero color (likely foreground or background stars), 2) objects that are faint and red (likely galaxies) and 3) objects that are bright and red (likely YSOs). There doesn’t appear to be any sources between the photospehric Class III and Class II objects. The chosen selection process may have gathered the YSO candidates into the group of brightest or reddest object, lending further support that the assertion of faint object being most likely background galaxies (bottom of page 14). Why is this so??

There is a good amount of detailed description of how the candidates were sorted out from the other sources. From the list of 10 YSO candidates, six are new discoveries. One of the Class II T Tauri stars is a flat disk. The fit for the edge-on-disk candidate was not the same as for the non-disk candidates, since the slope changes significantly depending on whether the MIPS points are included in the fit for the edge-on disk. I think I’d like to understand the slope correlation a bit better…

All of the YSO candidates are located in the head of the nebula, the most massive molecular cloud of the WHN. The distributions lend further support o the assertion that the IRAC and MIPS selected bright object are likely YSOs. The expected YSO candidates for the regions further south were not found. Apparently the conditions in this region do not support substantial star formation. The head of the nebula is about 3 times more massive than any of the other clouds.

There is a nice explanation of at least two intertwined mysteries that enshroud the WHN. The distance to it, and the external source that is responsible for the surface sculpture, illumination and possible trigger mechanism. There is a nice explanation of how the possible two sources (the Trapezium and Rigel) at different distances could solve the mysteries. There are arguments for both explanations, and the conclusion is that there is no clear answer. GAIA (galactic mapping mission proposed to launch in 2013) highlighted text abovecould provide a definitive answer by deriving accurate parallaxes to some objects.

The conclusion for the work states that the inventory of YSOs and candidates has doubles as a result of using Spitzer data to search for objects with IR excess in the region. SEDs are used extensively to identify YSO candidates. If the region is a triggered star formation mechanism, then trends of age or mass as they relate to location may be established. Since there are so few objects, since the distance is uncertain and since the spectral types for most of these objects is unknown, this correlation cannot be done rigorously.

Additional follow-up spectroscopic data are needed to confirm or refute the YSO status for the six new objects.

The new edge –on disk candidate in particular warrants further study, since such objects are relatively rare.

GAIA will be needed to resolve the mystery of the distance to the WHN.

Questions:

What:
1. I want to verify that I understand correctly that bands UVRcIc stand for: Ultraviolet, Visible, Red and Infrared, respectively.
2. Fat fielding issues
3. 100 MJy/ sr
4. Median boxcar filter
5. NaNs
6. UV RcIc
7. “real matches “
8. false source associations
9. centroiding
10. ELAIS
11. U and 70 micro meters
12. Optical Mv
13. VLBA and VLBI
14. mas/yr

How and HUH? : - see text above as well…

1. APEXZ portion of MOPEX
2. Zero point used to convert flux densities to magnitudes
3. …as a final check on our measurements.
4. …through observation of Landolt standards… Does this mean that the additional epoc was just for verification of data integrity?
5. …deviate significantly from zero
Why?
1. The data were further processed…
2. …we wished to add reddened stellar models to the plots…

----

== New Young Star Candidates in the Taurus-Auriga Region as Selected from WISE ==
New Young Star Candidates in the Taurus-Auriga Region as Selected from WISE

Summary: WISE data is used to search for YSO candidates in Taurus from a 260 square degree patch of sky to encompass previously identified Taurus members. Near and mid IR colors are used to select objects with apparent IR excesses and incorporate other catalogs of ancillary data. There is likely to be contamination lingering in this candidate list, and follow up spectra are warranted.

Even though Spitzer is good at finding new young stars, some are located surprisingly far from the traditional location based on CO gas or IRAS dust maps. A 44 square degree survey of Taurus was done with Spitzer. It was found that any solely near and mid IR color selection was filled with contamination from galaxies and asymptotic giant brand (AGB) stars. The use of ancillary data was crucial to establishing a list of high quality new members of Taurus. WISE surveyed the entire sky; the depth of coverage in the Taurus region is somewhat degraded relative to regions of comparable ecliptic latitude due to Moon avoidance maneuvers. Since the cloud is only 140 pc away, both surveys (Spitzer and WISE) should easily detect legitimate Taurus members.

New Taurus candidates were selected with IR excesses using WISE colors with the Koenig et al method. There are three lists: 1) recovered young stars, 2) rejected objects, and 3) candidate new Taurus members.

A substantial multi-wavelength database was assembled for point sources throughout the Taurus region. Not every source has photometry at all bands due to variations in depth and spatial coverage among the surveys involved.

The WISE data acquisition and reduction are discussed in Wright et al, Jarrett et al and in the Explanatory Supplement to the WISE preliminary Data Release Products. Any sources with contamination and confusion flags were rejected, as were “DHOP” (what’s this?) characters.

There were about 2.38 MILLION sources. Signal to Noise Ratio (SNR) measurements were used to drastically shrink the catalog to about 7,000 sources. The SNR cut was used in W4 to limit the contamination. Since the contamination rate for any color selection is expected to be relatively large, ancillary data are crucial for culling the list to high - quality candidates. A rough total of about 2,000 contaminants per square degree were determined. Approximately 1,760 YSO candidates were obtained before imposing additional requirements (which were???) to the SNR be imposed on all four WISE channels reduced the number to 1,014.

Ancillary data were used to weed out contaminants from the list of potential YSO candidates. Only 27 sources on the list of potential YSOs found matches with SDSS spectra.

Of the 1,014 potential YSOs, 196 of them have matches to previously identified stars. 18 of these are listed as unconfirmed candidates in Rebull et al (2010).

Manual Inspection was used to sort objects into “likely contaminant” or “perhaps YSO” bins. The four criteria used to categorize were: 1) matching objects in SIMBAD, 2) matches to objects identified as contaminants in Rebull at al (2010), 3) matches to the 2MASS Extended Source Catalog, and 4) identification as extended in the SDSS pipeline. SEDs were then generated using all the photometric date in the database, and the SEDs were inspected. Based on experience, the SEDs were then categorized as still possible YSO candidates, or likely extragalactic objects. This process may have dropped viable YSO candidates similar to MHO-1 (huh?) or Haro 6-39 (huh?). This process left about 130 candidates. The sources were identified as either being likely subjected to source contamination (HOW?) resolved as a likely galaxy (HOW?) or still apparently clean, point sources (HOW?) This brought the number of candidates down to about 94 objects. All SEDs for the 94 appear in the Appendix.

Projected location of the previously identified YSOs is generally highly clustered along the filamentary distribution of gas and dust, and the new objects are less clustered. The goal was to look for new YSOs outside the canonical groupings of previously known Taurus members. This could also be an indication of persistent contamination in the surviving list of YSOs candidates. There is more discussion about the location of previously identified YSOs and contaminants.

Previous YSOs are generally found in regions of high Av, and background galaxies are found in regions of low Av. The new objects are not particularly clustered, but not evenly distributed either. Most of the previously identified YSOs are bright and most of the contaminants are faint. The new YSO candidates span the range of bright and faint.

The list of objects by type: recovery of 196 previously identified young stars with IR excess, 686 likely to be galaxies, 13 foreground stars, 1 planetary nebula, 24 objects that are likely to be confusing and 94 new YSO candidates that are widely distributed in space.

Questions:

1. What s the “J” in 2MASS J04360131
2. What is color near zero?
3. What is the reddening factor?
4. What is the meaning of “...in the right regime for JHKs diagram”
5. What is “z measurement”?
6. What are large inner disk holes?

----

== New Young Star Candidates in CG4 and Sa101 ==

The introduction to this paper also has some very good background about the Gum Nebula and the stellar formation mechanisms thought to apply within it. Previous studies by Reipurth and Pettersson are summarized, with a conclusion that stars associated with the Cometary Globule 4 (CG4) and Sa 101 are associated with the Gum Nebula. The distances to all considered objects are uncertain; the distances vary from 300 to 500 pc. The extrema of the distance estimates were tested, though the results are not strongly dependent on distance. The region contains previously identified young stars, so it is likely that there are more young stars of lower mass or more embedded than those previously discovered.

The data sections, like the other two papers summarized, are highly technical and summarizing all the details doesn’t seem fruitful beyond this very minimal overview. More detailed reading should be the way to get more detail about the data analysis.

For the IRAC data, two exposures were taken with three dithers per position. The two observational locations were reduced independently even though they overlap on the sky. Some of the very bright stars in the filed of view had instrumental effects that rendered the data very difficult to work with. There is quite a bit of detailed description of calibration technique, correlation and photometry and error reduction methods.

The MIPS 24 and 70 micron data were combined. The 24-micron data were affected by the bright objects and required additional processing. The background levels between the two observations were problematic, and a description of how this was addressed was discussed. Optimized data reduction to obtain brighter source measurements led to many sources fainter than the bright sources in the image being excluded from the catalog because the scientific goals are aimed at brighter objects. There is a good, technical justification of the filtering choices made to process the data.

The optical data used the observed Landolt (1992) standard stars of two or three fields several times per night for photometric calibration. For each target, aperture photometry was performed using multiple size apertures. There is a discussion of the correction used for a noticeable variation of the point-spread function (PSF) that is location dependent on the CCD.

The bandmerging of the photometric data was first merged from all four IRAC channels with the near IR 2MASS data for each observation. This was then merged together with the source lists from each observation. The MIPS data was then included, and then the optical data was merged. A very detailed discussion of how this was done follows.

YSO candidate properties are discussed in the subset of optical, near IR, B-band and SEDs. Optical data can greatly aid in the confirmation or refutation of YSO candidacy because they provide constraints on the Wien side of the SED. Objects with optical data that have already been ruled out as SOs based on the IRAC properties are all well below the 30 Myr isochrones scaled to 500 pc. Deeper optical data are desirable to obtain magnitude estimates for the remaining YSO candidates. The degree of reddening is difficult to estimate because the spectral types for most of the sources are not available. The candidates have infrared excess with a moderate degree of reddening. Young stars that are actively accreting from their circumstellar disks can have excess UV emission in the U or B bands or longer. These bands are also the most sensitive to reddening. Figure 13 is discussed with respect to mass accretion. The coordinates of the YSOs are listed in Table 1. The SEDs of the 22 YSO candidates are displayed in figures 14 - 16. A spectral type of MO was assumed for the remaining objects. A redden model of each object is shown and normalized to the Ks band where possible. These are presented as a guide to the eye rather than a robust fit to the object to allow the immediate IR excesses to be immediately apparent. There is quite a bit of more technically detailed description of the properties in the SEDs section than is summarized here.

There is a galaxy, ESO 257 – G 019 that is mentioned because it appears in the observation field. It has not been studied, and some basic astrometric data about it is listed.

In conclusion, 6 previously identified young stars were rediscovered. There are 16 new YSOs that were discovered and evaluated with ground-based data in the near IR from 2MASS to constrain the SEDs of the candidates. The new young star candidates were graded into confidence groups. Additional data will be needed, such as optical photometry where it is missing and optical spectroscopy to obtain spectral types.

I didn’t have any questions about this article.

----
==="Triggered Star Formation and Evolution of T-Tauri Stars in and Around Bright-Rimmed Clouds" by Chauhan, et al. and "Triggered Star Formation and Young Stellar Population in Bright-Rimmed Cloud SFO 38" by Choudhury, et al.===

File:Chauhan et al Reading Guide.pdf

2012-05-08T15:58:14Z

French:

C-WAYS Summer visit logistics

2012-04-30T15:20:50Z

French:

C-WAYS Proposal

2012-03-13T12:17:23Z

French:

=Instructions=

[[2012 proposal instructions]]

=Potentially Useful Coordinates=
'''BRC 27:''' 07h04m07.8s -11d16m43s
'''BRC 34:''' 21h32m51.2s +58d08m43s
'''BRC 38:''' 21h40m02.2s +58d20m43s

=Proposal versions=
''Peggy will collect and assemble pieces of the proposal and maintain reference list in an evolving word document. If you have changes that should be made to the document, please copy, cross-out, edit, then email or post the text to the wiki so Peggy can incorporate into document.''
 
Proposal after friday telecon Mar 2, 2012. Added Intro, BRC 27 info, Bob's images, all references sited are present, have not removed "excess" references. Minor continuity/flow edits made by Peggy. [[File:CWAYS Proposal 030312.docx]]--Peggy Piper 08:54, 3 March 2012 (PST)
 
Proposal Revision prior to friday telecon Mar 2, 2012. Includes author info, Analysis section, Education/Outreach general plus Debbie, Lauren, Peggy individual plans, references from 2011 team [[File:CWAYS Proposal 030212.docx]]--Peggy Piper 17:50, 1 March 2012 (PST)
 
Initial Skeleton for Proposal [[File:CWAYS Proposal Format.docx]]--Peggy Piper 12:52, 24 February 2012 (PST)

=Abstract hacking grounds=

Please take a look at this initial try at the abstract.

[[CWAYS Abstract]]

=Proposal nitty gritty - first round, 1/27/12=

Everyone should read last year's BRC proposal if you haven't already.

As per the instructions for this year's proposal, we need to have:

*Abstract - write that last!
*Science introduction and context - general overview - Debbie
*including summary of literature on each of the BRCs:
**BRC 38 - Jackie
**BRC 27 - Lauren
**BRC 34 - Robert
*Analysis plan - Peggy
*Edu plan - everyone

For most of this, you will now need to get into literature searching.
Tips for literature searching on the wiki [[How_can_I_find_out_what_scientists_already_know_about_a_particular_astronomy_topic_or_object%3F |are here]], with a link at the bottom of that page with more words.
In summary:
*use ADS.
*use SIMBAD.
they are interlinked, but searching in both doesn't always give you
the same results.
in SIMBAD, you can search by position, and you should use a
~10 arcmin radius to look for objects. what other named objects are
nearby? there may be other useful papers calling those other objects
by those other names.
To get articles, remember that you don't HAVE to go to the journal.
For 'old enough' papers, they will be free.
For newer papers, look for an arXiv link on the ADS abstract page.
If you still can't get it, or want the final typeset journal version,
send me an email with the ADS link, and I'll send back the PDF.
ADS will cough up abstracts to proposals, abstracts from conferences
without conference proceedings, conference proceedings, and refereed
journal articles. that list is from least useful to most useful.

somewaht confusingly, sorry, links to some of the papers i list below are collected on [[C-WAYS_Spring_work |this page]], sorry. in the interest of getting this out to you, i didn't want to spend the time going to retrieve and link all of the abstract links again. we will ultimately be adding some of the papers you find to this spring work page, so this makes sense in the long run, but sorry for any additional confusion.

So that everyone understands the big picture, read the intro to
Sugitani K., Fukui Y., Ogura K., 1991, ApJS, 77, 59. = SFO, because it
is the discovery paper for the BRC catalog.

'''Intro - Debbie''' -
look closely at last year's prop intro. go find the papers they
reference. look at the SFO paper, and others they reference. look at
the YSO background information on the wiki.

[[Media:NITARP Proposal Introduction.docx]]

'''BRC 38 - Jackie''' -
You have the biggest literature search problem, because we've done the
least collective work here.
You have leads for five papers from the wiki discussion about bouncing
target selection:
*Chauhan et al below.
*Garmire & Gordon - chandra proposal - look for a paper by these guys reporting these results, but it might not exist
*Valdettaro etal - also turns up in one of the other BRC searches.
*choudhury et al.
*Morgan et al.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before. if you find a paper, the first thing you should do is look at this list to see if we grabbed and kept it or grabbed and discarded it before. assess (and keep track of) any new ones! it is likely there more you can find. yell if you need help. don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12:''' [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.
'''UPDATE 2/2/12:''' Can you tell I'm going through some backlogged papers? I just found [http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran et al. (2009)], which does deep JHK imaging in BRC38=IC1396N. This is another really good paper, with lots of good observations.
*I have listed the articles [[Jackie_BRC_38]] that I have found and some info about BRC 38 that I have gleamed. Please look it over, edit, correct, answer questions, ask questions - Jackie

'''BRC 27 - Lauren''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before.
if you find a paper, the first thing you should do is look at this
list to see if we grabbed and kept it or grabbed and discarded it
before. assess (and keep track of) any new ones!
don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
papers i know you will want to scan:

*Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. - does JHK + spitzer search for brc 27, 38 but we know they didn't do that great a job in 27, so they probably didn't do a great job in 38! but we need to mention in the proposal that this work exists and that we will compare our results to theirs.
*Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&A, 2009, 506, 711.
*Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210.
*Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395.

*My first draft of the science background and education plan is now on [[Lauren_BRC 27]]

'''BRC 34- Robert''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]] lists all the literature we decided to care about before.
you will note that very few mention BRC 34!
The only one that was terribly useful was Ogura et al. 2002, AJ, 123,
2597, and even that, not very much.
don't forget to try a SIMBAD search by position.
if you exhaust the available literature without finding more, go help
jackie with BRC 38. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.

[[Bob BRC 34]]

'''analysis - Peggy''' -
[[Analysis Work Space]]

look at the proposal from last time.
look at Rebull et al., 2011, ApJS, 196, 4 (the taurus/WISE paper) i
gave you for that methodology.
scan the appendix of Koenig et al., 2012, ApJ, 744, 130 -- we will get
into this in more detail later, but this is the color selection
mechanism using WISE colors.
mention that we will re-reduce the Spitzer data for brc 38 if need be,
and redo photometry on the serendipitously obtained spitzer off-source
fields in the area if we need to -- the gang last year wasn't too
concerned about those objects. (you can use similar words from last
time involving MOPEX and APT). don't worry about reading the makovoz
and marleau paper - way thick reading and not all that relevant. can
cite Laher et al 2012 in prep for APT (dunno if we did that last year
or not).
we will merge with 2MASS, AKARI, anything else we can find.
don't forget that we will have ground based optical data from JD to
contribute as well. will need to get words from him on that.
other important words - BRC 27 data already in the WISE public
release; rest will be available in March 2012. i can give you a figure
with that comparison when we get there.
'''UPDATE 2/1:''' FWIW, that Barentsen et al 2011 paper is IPHAS data, so you can add in to your analysis section that we will include IPHAS data for at least brc 34 and 38. their website says a new delivery is expected in 2012, so we'll do a new search if we can, else we'll just use the more limited stuff from the published paper.

'''Edu section''' - you're all on your own :)

FOR NEXT WEEK - read the proposal and (intro to the) SFO paper, get into your proposal section and see how much progress you can make on your proposal section. if you run out of stuff to do, ask if others need help.

=Education Section=

''Here's what I have for Education and Outreach section. Please put any edits in bold. Debbie, Lauren and I each have a short description of what our groups will do. Please add your school's brief plan and I will add it to the Proposal document. Don't stress on this, it is your proposed plan and we all know proposed plans that involve students change based on students many faceted characteristics!''--Peggy Piper 18:08, 1 March 2012 (PST)

'''Education and Outreach'''

Team C-WAYS is made up of a wide variety of adult and school age learners. Our adult learners include middle school, high school, community college and informal educators. Our school age learners, therefore, will also represent a wide range of ages and abilities. Each sub team of educator and school age learners will spend time immersing themselves in general astronomy concepts and skills necessary to the success of C-WAYS research as appropriate for their age and ability. Some of these concepts and skills are;

• general properties of light and the Electromagnetic Spectrum with special emphasis on infrared 
• multiwavelength astronomy with emphasis on wavelengths and image sources that we will utilize; IRAC, MIPS, 2MASS, MSX, AKARI , IPHAS and LCOGT 
• life cycle of stars with emphasis on Young Stellar Objects (YSOs) 
• infrared excess and its relation to YSOs 
• spatial resolution with emphasis on the relative spatial resolutions of WISE vs. Spitzer images 
• similarities and differences of WISE and Spitzer missions and why they were designed as they were 
• photometry methods and terms, particularly the use of MOPEX and APT 
• data manipulation and generation of graphics using EXCEL 

With appropriate background schema in place, both adult and school age learners will experience authentic scientific research in a true collegial manner. Based on thorough literature searches, journal articles relevant to our area of study will be read analyzed and discussed. Data acquisition and analysis will take place before, during and after CWAYS’ visit to CalTech in July. Communications between sub teams will take place via regular teleconferences, video conferences, extensive use of the wiki, and email. A Scientific and an Education poster will be created and presented by the CWAYS team at the 2013 AAS based on results obtained through this process.

Participation NITARP will enrich every CWAYS’ learner with the experience of having done authentic research as part of a cross continental team. This experience will not only increase each learner’s knowledge of astronomy and the research process, but will increase their interest and excitement level towards research opportunities. This knowledge, interest and excitement will be payed forward through formal outreach to education and community groups by all learners, as well as informally to adult and school age peers of all those involved.

Team Lincoln Way High School (P. Piper). Teachers and students from several of the districts four schools (including the districts ROTC program) will be involved in this process through the district’s new “distance learning” equipment. Student interest and commitment will be assessed through weekly sessions in which students will learn basic concepts and computer skills. A school page on the wiki will be created and used to share knowledge within this sub group and to reach out to other groups. Outreach will be coordinated with Educational Outreach colleagues at Yerkes Observatory and will include sessions at local, national and international workshops. Past presentations have included local school groups, Yerkes workshops, Illinois Science Teachers Association, and Global Hands on Universe.

Team New Philadelphia High School (D. French). New Philadelphia High School Students will be participating in the NITARP research project as an extra-curricular activity and may apply for the Ohio Flex Credit option. Students will be selected via an application process in March or April 2012. Students will participate in weekly research meetings to discuss background information, journal articles, and to work on data reduction and analysis. They will be responsible for keeping a science notebook for recording notes, comments, and for keeping applicable journal articles. Students will use the NITARP CoolWiki page to obtain additional background information and communicate with other team members. After the January 2012 AAS meeting, they will present their research to the New Philadelphia Board of Education as well as other possible venues and outreach activities.

Team Reedley College (L. Novatne). A small group of college freshman and sophomores will meet weekly. For the first few weeks, the students will be instructed on the basics of star formation and stellar evolution. Once the students understand the basics, they will begin reading the appropriate journals and conduct web research for discussion. Once the data processing instruction has been completed, the students will work together and separately on the data analysis portion of the project. The weekly meetings will introduce the students to; star formation mechanism and stellar life cycle, spectral analysis, black body curves, and photometry. In the fall of 2012, the weekly meetings will include the processing of data.

Below is a rough draft for my education section. Comments/suggestions are appreciated!

"New Philadelphia High School (D. French). New Philadelphia High School Students will be participating in the NITARP research project as an extra-curricular activity and may apply for the Ohio Flex Credit option. Students will be selected via an application process in March or April 2012.

''I'm wondering what your application criteria will be. I have gone for kids with high interest level vs great academic records in the past. Do we want to find a common ground here, or are we ok with having different types of kids on different teams?''--Peggy Piper 12:41, 17 February 2012 (PST)

"Students will participate in weekly research meetings to discuss background information, journal articles, and to work on data reduction and analysis. They will be responsible for keeping a science notebook for recording notes, comments, and for keeping applicable journal articles. Students will use the NITARP CoolWiki page to obtain additional background information and communicate with other team members. After the January 2012 AAS meeting, they will present their research to the New Philadelphia Board of Education as well as other possible venues and outreach activities."
--[[User:French|French]] 08:38, 16 February 2012 (PST)

C-WAYS Proposal

2012-03-02T15:55:32Z

French:

=Instructions=

[[2012 proposal instructions]]

=Proposal versions=
''Peggy will collect and assemble pieces of the proposal and maintain reference list in an evolving word document. If you have changes that should be made to the document, please copy, cross-out, edit, then email or post the text to the wiki so Peggy can incorporate into document.''

 
Proposal Revision prior to friday telecon Mar 2, 2012. Includes author info, Analysis section, Education/Outreach general plus Debbie, Lauren, Peggy individual plans, references from 2011 team [[File:CWAYS Proposal 030212.docx]]--Peggy Piper 17:50, 1 March 2012 (PST)
 
Initial Skeleton for Proposal [[File:CWAYS Proposal Format.docx]]--Peggy Piper 12:52, 24 February 2012 (PST)

=Proposal nitty gritty - first round, 1/27/12=

Everyone should read last year's BRC proposal if you haven't already.

As per the instructions for this year's proposal, we need to have:

*Abstract - write that last!
*Science introduction and context - general overview - Debbie
*including summary of literature on each of the BRCs:
**BRC 38 - Jackie
**BRC 27 - Lauren
**BRC 34 - Robert
*Analysis plan - Peggy
*Edu plan - everyone

For most of this, you will now need to get into literature searching.
Tips for literature searching on the wiki [[How_can_I_find_out_what_scientists_already_know_about_a_particular_astronomy_topic_or_object%3F |are here]], with a link at the bottom of that page with more words.
In summary:
*use ADS.
*use SIMBAD.
they are interlinked, but searching in both doesn't always give you
the same results.
in SIMBAD, you can search by position, and you should use a
~10 arcmin radius to look for objects. what other named objects are
nearby? there may be other useful papers calling those other objects
by those other names.
To get articles, remember that you don't HAVE to go to the journal.
For 'old enough' papers, they will be free.
For newer papers, look for an arXiv link on the ADS abstract page.
If you still can't get it, or want the final typeset journal version,
send me an email with the ADS link, and I'll send back the PDF.
ADS will cough up abstracts to proposals, abstracts from conferences
without conference proceedings, conference proceedings, and refereed
journal articles. that list is from least useful to most useful.

somewaht confusingly, sorry, links to some of the papers i list below are collected on [[C-WAYS_Spring_work |this page]], sorry. in the interest of getting this out to you, i didn't want to spend the time going to retrieve and link all of the abstract links again. we will ultimately be adding some of the papers you find to this spring work page, so this makes sense in the long run, but sorry for any additional confusion.

So that everyone understands the big picture, read the intro to
Sugitani K., Fukui Y., Ogura K., 1991, ApJS, 77, 59. = SFO, because it
is the discovery paper for the BRC catalog.

'''Intro - Debbie''' -
look closely at last year's prop intro. go find the papers they
reference. look at the SFO paper, and others they reference. look at
the YSO background information on the wiki.

[[Media:NITARP Proposal Introduction.docx]]

'''BRC 38 - Jackie''' -
You have the biggest literature search problem, because we've done the
least collective work here.
You have leads for five papers from the wiki discussion about bouncing
target selection:
*Chauhan et al below.
*Garmire & Gordon - chandra proposal - look for a paper by these guys reporting these results, but it might not exist
*Valdettaro etal - also turns up in one of the other BRC searches.
*choudhury et al.
*Morgan et al.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before. if you find a paper, the first thing you should do is look at this list to see if we grabbed and kept it or grabbed and discarded it before. assess (and keep track of) any new ones! it is likely there more you can find. yell if you need help. don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12:''' [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.
'''UPDATE 2/2/12:''' Can you tell I'm going through some backlogged papers? I just found [http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran et al. (2009)], which does deep JHK imaging in BRC38=IC1396N. This is another really good paper, with lots of good observations.
*I have listed the articles [[Jackie_BRC_38]] that I have found and some info about BRC 38 that I have gleamed. Please look it over, edit, correct, answer questions, ask questions - Jackie

'''BRC 27 - Lauren''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before.
if you find a paper, the first thing you should do is look at this
list to see if we grabbed and kept it or grabbed and discarded it
before. assess (and keep track of) any new ones!
don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
papers i know you will want to scan:

*Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. - does JHK + spitzer search for brc 27, 38 but we know they didn't do that great a job in 27, so they probably didn't do a great job in 38! but we need to mention in the proposal that this work exists and that we will compare our results to theirs.
*Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&A, 2009, 506, 711.
*Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210.
*Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395.

*My first draft of the science background and education plan is now on [[Lauren_BRC 27]]

'''BRC 34- Robert''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]] lists all the literature we decided to care about before.
you will note that very few mention BRC 34!
The only one that was terribly useful was Ogura et al. 2002, AJ, 123,
2597, and even that, not very much.
don't forget to try a SIMBAD search by position.
if you exhaust the available literature without finding more, go help
jackie with BRC 38. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.

'''analysis - Peggy''' -
[[Analysis Work Space]]

look at the proposal from last time.
look at Rebull et al., 2011, ApJS, 196, 4 (the taurus/WISE paper) i
gave you for that methodology.
scan the appendix of Koenig et al., 2012, ApJ, 744, 130 -- we will get
into this in more detail later, but this is the color selection
mechanism using WISE colors.
mention that we will re-reduce the Spitzer data for brc 38 if need be,
and redo photometry on the serendipitously obtained spitzer off-source
fields in the area if we need to -- the gang last year wasn't too
concerned about those objects. (you can use similar words from last
time involving MOPEX and APT). don't worry about reading the makovoz
and marleau paper - way thick reading and not all that relevant. can
cite Laher et al 2012 in prep for APT (dunno if we did that last year
or not).
we will merge with 2MASS, AKARI, anything else we can find.
don't forget that we will have ground based optical data from JD to
contribute as well. will need to get words from him on that.
other important words - BRC 27 data already in the WISE public
release; rest will be available in March 2012. i can give you a figure
with that comparison when we get there.
'''UPDATE 2/1:''' FWIW, that Barentsen et al 2011 paper is IPHAS data, so you can add in to your analysis section that we will include IPHAS data for at least brc 34 and 38. their website says a new delivery is expected in 2012, so we'll do a new search if we can, else we'll just use the more limited stuff from the published paper.

'''Edu section''' - you're all on your own :)

FOR NEXT WEEK - read the proposal and (intro to the) SFO paper, get into your proposal section and see how much progress you can make on your proposal section. if you run out of stuff to do, ask if others need help.

=Education Section=

''Here's what I have for Education and Outreach section. Please put any edits in bold. Debbie, Lauren and I each have a short description of what our groups will do. Please add your school's brief plan and I will add it to the Proposal document. Don't stress on this, it is your proposed plan and we all know proposed plans that involve students change based on students many faceted characteristics!''--Peggy Piper 18:08, 1 March 2012 (PST)

'''Education and Outreach'''

Team C-WAYS is made up of a wide variety of adult and school age learners. Our adult learners include middle school, high school, community college and informal educators. Our school age learners, therefore, will also represent a wide range of ages and abilities. Each sub team of educator and school age learners will spend time immersing themselves in general astronomy concepts and skills necessary to the success of C-WAYS research as appropriate for their age and ability. Some of these concepts and skills are;

• general properties of light and the Electromagnetic Spectrum with special emphasis on infrared 
• multiwavelength astronomy with emphasis on wavelengths and image sources that we will utilize; IRAC, MIPS, 2MASS, MSX, AKARI , IPHAS and LCOGT 
• life cycle of stars with emphasis on Young Stellar Objects (YSOs) 
• infrared excess and its relation to YSOs 
• spatial resolution with emphasis on the relative spatial resolutions of WISE vs. Spitzer images 
• similarities and differences of WISE and Spitzer missions and why they were designed as they were 
• photometry methods and terms, particularly the use of MOPEX and APT 
• data manipulation and generation of graphics using EXCEL 

With appropriate background schema in place, both adult and school age learners will experience authentic scientific research in a true collegial manner. Based on thorough literature searches, journal articles relevant to our area of study will be read analyzed and discussed. Data acquisition and analysis will take place before, during and after CWAYS’ visit to CalTech in July. Communications between sub teams will take place via regular teleconferences, video conferences, extensive use of the wiki, and email. A Scientific and an Education poster will be created and presented by the CWAYS team at the 2013 AAS based on results obtained through this process.

Participation NITARP will enrich every CWAYS’ learner with the experience of having done authentic research as part of a cross continental team. This experience will not only increase each learner’s knowledge of astronomy and the research process, but will increase their interest and excitement level towards research opportunities. This knowledge, interest and excitement will be payed forward through formal outreach to education and community groups by all learners, as well as informally to adult and school age peers of all those involved.

Team Lincoln Way High School (P. Piper). Teachers and students from several of the districts four schools (including the districts ROTC program) will be involved in this process through the district’s new “distance learning” equipment. Student interest and commitment will be assessed through weekly sessions in which students will learn basic concepts and computer skills. A school page on the wiki will be created and used to share knowledge within this sub group and to reach out to other groups. Outreach will be coordinated with Educational Outreach colleagues at Yerkes Observatory and will include sessions at local, national and international workshops. Past presentations have included local school groups, Yerkes workshops, Illinois Science Teachers Association, and Global Hands on Universe.

Team New Philadelphia High School (D. French). New Philadelphia High School Students will be participating in the NITARP research project as an extra-curricular activity and may apply for the Ohio Flex Credit option. Students will be selected via an application process in March or April 2012. Students will participate in weekly research meetings to discuss background information, journal articles, and to work on data reduction and analysis. They will be responsible for keeping a science notebook for recording notes, comments, and for keeping applicable journal articles. Students will use the NITARP CoolWiki page to obtain additional background information and communicate with other team members. After the January 2012 AAS meeting, they will present their research to the New Philadelphia Board of Education as well as other possible venues and outreach activities.

Team Reedley College (L. Novatne). A small group of college freshman and sophomores will meet weekly. For the first few weeks, the students will be instructed on the basics of star formation and stellar evolution. Once the students understand the basics, they will begin reading the appropriate journals and conduct web research for discussion. Once the data processing instruction has been completed, the students will work together and separately on the data analysis portion of the project. The weekly meetings will introduce the students to; star formation mechanism and stellar life cycle, spectral analysis, black body curves, and photometry. In the fall of 2012, the weekly meetings will include the processing of data.

Below is a rough draft for my education section. Comments/suggestions are appreciated!

"New Philadelphia High School (D. French). New Philadelphia High School Students will be participating in the NITARP research project as an extra-curricular activity and may apply for the Ohio Flex Credit option. Students will be selected via an application process in March or April 2012.

''I'm wondering what your application criteria will be. I have gone for kids with high interest level vs great academic records in the past. Do we want to find a common ground here, or are we ok with having different types of kids on different teams?''--Peggy Piper 12:41, 17 February 2012 (PST)

"Students will participate in weekly research meetings to discuss background information, journal articles, and to work on data reduction and analysis. They will be responsible for keeping a science notebook for recording notes, comments, and for keeping applicable journal articles. Students will use the NITARP CoolWiki page to obtain additional background information and communicate with other team members. After the January 2012 AAS meeting, they will present their research to the New Philadelphia Board of Education as well as other possible venues and outreach activities."
--[[User:French|French]] 08:38, 16 February 2012 (PST)

File:NITARP Proposal Introduction.docx

2012-03-02T14:31:08Z

French:

C-WAYS Proposal

2012-03-02T14:28:05Z

French:

=Instructions=

[[2012 proposal instructions]]

=Proposal versions=
''Peggy will collect and assemble pieces of the proposal and maintain reference list in an evolving word document. If you have changes that should be made to the document, please copy, cross-out, edit, then email or post the text to the wiki so Peggy can incorporate into document.''

 
Proposal Revision prior to friday telecon Mar 2, 2012. Includes author info, Analysis section, Education/Outreach general plus Debbie, Lauren, Peggy individual plans, references from 2011 team [[File:CWAYS Proposal 030212.docx]]--Peggy Piper 17:50, 1 March 2012 (PST)
 
Initial Skeleton for Proposal [[File:CWAYS Proposal Format.docx]]--Peggy Piper 12:52, 24 February 2012 (PST)

=Proposal nitty gritty - first round, 1/27/12=

Everyone should read last year's BRC proposal if you haven't already.

As per the instructions for this year's proposal, we need to have:

*Abstract - write that last!
*Science introduction and context - general overview - Debbie
*including summary of literature on each of the BRCs:
**BRC 38 - Jackie
**BRC 27 - Lauren
**BRC 34 - Robert
*Analysis plan - Peggy
*Edu plan - everyone

For most of this, you will now need to get into literature searching.
Tips for literature searching on the wiki [[How_can_I_find_out_what_scientists_already_know_about_a_particular_astronomy_topic_or_object%3F |are here]], with a link at the bottom of that page with more words.
In summary:
*use ADS.
*use SIMBAD.
they are interlinked, but searching in both doesn't always give you
the same results.
in SIMBAD, you can search by position, and you should use a
~10 arcmin radius to look for objects. what other named objects are
nearby? there may be other useful papers calling those other objects
by those other names.
To get articles, remember that you don't HAVE to go to the journal.
For 'old enough' papers, they will be free.
For newer papers, look for an arXiv link on the ADS abstract page.
If you still can't get it, or want the final typeset journal version,
send me an email with the ADS link, and I'll send back the PDF.
ADS will cough up abstracts to proposals, abstracts from conferences
without conference proceedings, conference proceedings, and refereed
journal articles. that list is from least useful to most useful.

somewaht confusingly, sorry, links to some of the papers i list below are collected on [[C-WAYS_Spring_work |this page]], sorry. in the interest of getting this out to you, i didn't want to spend the time going to retrieve and link all of the abstract links again. we will ultimately be adding some of the papers you find to this spring work page, so this makes sense in the long run, but sorry for any additional confusion.

So that everyone understands the big picture, read the intro to
Sugitani K., Fukui Y., Ogura K., 1991, ApJS, 77, 59. = SFO, because it
is the discovery paper for the BRC catalog.

'''Intro - Debbie''' -
look closely at last year's prop intro. go find the papers they
reference. look at the SFO paper, and others they reference. look at
the YSO background information on the wiki.

[[Media:NITARP Proposal Introduction.docx]]

'''BRC 38 - Jackie''' -
You have the biggest literature search problem, because we've done the
least collective work here.
You have leads for five papers from the wiki discussion about bouncing
target selection:
*Chauhan et al below.
*Garmire & Gordon - chandra proposal - look for a paper by these guys reporting these results, but it might not exist
*Valdettaro etal - also turns up in one of the other BRC searches.
*choudhury et al.
*Morgan et al.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before. if you find a paper, the first thing you should do is look at this list to see if we grabbed and kept it or grabbed and discarded it before. assess (and keep track of) any new ones! it is likely there more you can find. yell if you need help. don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12:''' [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.
'''UPDATE 2/2/12:''' Can you tell I'm going through some backlogged papers? I just found [http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran et al. (2009)], which does deep JHK imaging in BRC38=IC1396N. This is another really good paper, with lots of good observations.
*I have listed the articles [[Jackie_BRC_38]] that I have found and some info about BRC 38 that I have gleamed. Please look it over, edit, correct, answer questions, ask questions - Jackie

'''BRC 27 - Lauren''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before.
if you find a paper, the first thing you should do is look at this
list to see if we grabbed and kept it or grabbed and discarded it
before. assess (and keep track of) any new ones!
don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
papers i know you will want to scan:

*Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. - does JHK + spitzer search for brc 27, 38 but we know they didn't do that great a job in 27, so they probably didn't do a great job in 38! but we need to mention in the proposal that this work exists and that we will compare our results to theirs.
*Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&A, 2009, 506, 711.
*Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210.
*Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395.

*My first draft of the science background and education plan is now on [[Lauren_BRC 27]]

'''BRC 34- Robert''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]] lists all the literature we decided to care about before.
you will note that very few mention BRC 34!
The only one that was terribly useful was Ogura et al. 2002, AJ, 123,
2597, and even that, not very much.
don't forget to try a SIMBAD search by position.
if you exhaust the available literature without finding more, go help
jackie with BRC 38. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.

Below is a link to what archival data is available from Spitzer for BRC 34.
[http://archive.spitzer.caltech.edu/searchByPosition.do]--[[User:French|French]] 13:17, 22 February 2012 (PST)

'''analysis - Peggy''' -
[[Analysis Work Space]]

look at the proposal from last time.
look at Rebull et al., 2011, ApJS, 196, 4 (the taurus/WISE paper) i
gave you for that methodology.
scan the appendix of Koenig et al., 2012, ApJ, 744, 130 -- we will get
into this in more detail later, but this is the color selection
mechanism using WISE colors.
mention that we will re-reduce the Spitzer data for brc 38 if need be,
and redo photometry on the serendipitously obtained spitzer off-source
fields in the area if we need to -- the gang last year wasn't too
concerned about those objects. (you can use similar words from last
time involving MOPEX and APT). don't worry about reading the makovoz
and marleau paper - way thick reading and not all that relevant. can
cite Laher et al 2012 in prep for APT (dunno if we did that last year
or not).
we will merge with 2MASS, AKARI, anything else we can find.
don't forget that we will have ground based optical data from JD to
contribute as well. will need to get words from him on that.
other important words - BRC 27 data already in the WISE public
release; rest will be available in March 2012. i can give you a figure
with that comparison when we get there.
'''UPDATE 2/1:''' FWIW, that Barentsen et al 2011 paper is IPHAS data, so you can add in to your analysis section that we will include IPHAS data for at least brc 34 and 38. their website says a new delivery is expected in 2012, so we'll do a new search if we can, else we'll just use the more limited stuff from the published paper.

'''Edu section''' - you're all on your own :)

FOR NEXT WEEK - read the proposal and (intro to the) SFO paper, get into your proposal section and see how much progress you can make on your proposal section. if you run out of stuff to do, ask if others need help.

=Education Section=

''Here's what I have for Education and Outreach section. Please put any edits in bold. Debbie, Lauren and I each have a short description of what our groups will do. Please add your school's brief plan and I will add it to the Proposal document. Don't stress on this, it is your proposed plan and we all know proposed plans that involve students change based on students many faceted characteristics!''--Peggy Piper 18:08, 1 March 2012 (PST)

'''Education and Outreach'''

Team C-WAYS is made up of a wide variety of adult and school age learners. Our adult learners include middle school, high school, community college and informal educators. Our school age learners, therefore, will also represent a wide range of ages and abilities. Each sub team of educator and school age learners will spend time immersing themselves in general astronomy concepts and skills necessary to the success of C-WAYS research as appropriate for their age and ability. Some of these concepts and skills are;

• general properties of light and the Electromagnetic Spectrum with special emphasis on infrared 
• multiwavelength astronomy with emphasis on wavelengths and image sources that we will utilize; IRAC, MIPS, 2MASS, MSX, AKARI , IPHAS and LCOGT 
• life cycle of stars with emphasis on Young Stellar Objects (YSOs) 
• infrared excess and its relation to YSOs 
• spatial resolution with emphasis on the relative spatial resolutions of WISE vs. Spitzer images 
• similarities and differences of WISE and Spitzer missions and why they were designed as they were 
• photometry methods and terms, particularly the use of MOPEX and APT 
• data manipulation and generation of graphics using EXCEL 

With appropriate background schema in place, both adult and school age learners will experience authentic scientific research in a true collegial manner. Based on thorough literature searches, journal articles relevant to our area of study will be read analyzed and discussed. Data acquisition and analysis will take place before, during and after CWAYS’ visit to CalTech in July. Communications between sub teams will take place via regular teleconferences, video conferences, extensive use of the wiki, and email. A Scientific and an Education poster will be created and presented by the CWAYS team at the 2013 AAS based on results obtained through this process.

Participation NITARP will enrich every CWAYS’ learner with the experience of having done authentic research as part of a cross continental team. This experience will not only increase each learner’s knowledge of astronomy and the research process, but will increase their interest and excitement level towards research opportunities. This knowledge, interest and excitement will be payed forward through formal outreach to education and community groups by all learners, as well as informally to adult and school age peers of all those involved.

Team Lincoln Way High School (P. Piper). Teachers and students from several of the districts four schools (including the districts ROTC program) will be involved in this process through the district’s new “distance learning” equipment. Student interest and commitment will be assessed through weekly sessions in which students will learn basic concepts and computer skills. A school page on the wiki will be created and used to share knowledge within this sub group and to reach out to other groups. Outreach will be coordinated with Educational Outreach colleagues at Yerkes Observatory and will include sessions at local, national and international workshops. Past presentations have included local school groups, Yerkes workshops, Illinois Science Teachers Association, and Global Hands on Universe.

Team New Philadelphia High School (D. French). New Philadelphia High School Students will be participating in the NITARP research project as an extra-curricular activity and may apply for the Ohio Flex Credit option. Students will be selected via an application process in March or April 2012. Students will participate in weekly research meetings to discuss background information, journal articles, and to work on data reduction and analysis. They will be responsible for keeping a science notebook for recording notes, comments, and for keeping applicable journal articles. Students will use the NITARP CoolWiki page to obtain additional background information and communicate with other team members. After the January 2012 AAS meeting, they will present their research to the New Philadelphia Board of Education as well as other possible venues and outreach activities.

Team Reedley College (L. Novatne). A small group of college freshman and sophomores will meet weekly. For the first few weeks, the students will be instructed on the basics of star formation and stellar evolution. Once the students understand the basics, they will begin reading the appropriate journals and conduct web research for discussion. Once the data processing instruction has been completed, the students will work together and separately on the data analysis portion of the project. The weekly meetings will introduce the students to; star formation mechanism and stellar life cycle, spectral analysis, black body curves, and photometry. In the fall of 2012, the weekly meetings will include the processing of data.

Below is a rough draft for my education section. Comments/suggestions are appreciated!

"New Philadelphia High School (D. French). New Philadelphia High School Students will be participating in the NITARP research project as an extra-curricular activity and may apply for the Ohio Flex Credit option. Students will be selected via an application process in March or April 2012.

''I'm wondering what your application criteria will be. I have gone for kids with high interest level vs great academic records in the past. Do we want to find a common ground here, or are we ok with having different types of kids on different teams?''--Peggy Piper 12:41, 17 February 2012 (PST)

"Students will participate in weekly research meetings to discuss background information, journal articles, and to work on data reduction and analysis. They will be responsible for keeping a science notebook for recording notes, comments, and for keeping applicable journal articles. Students will use the NITARP CoolWiki page to obtain additional background information and communicate with other team members. After the January 2012 AAS meeting, they will present their research to the New Philadelphia Board of Education as well as other possible venues and outreach activities."
--[[User:French|French]] 08:38, 16 February 2012 (PST)

C-WAYS Proposal

2012-02-22T21:17:38Z

French:

=Instructions=

[[2012 proposal instructions]]

=Proposal nitty gritty - first round, 1/27/12=

Everyone should read last year's BRC proposal if you haven't already.

As per the instructions for this year's proposal, we need to have:

*Abstract - write that last!
*Science introduction and context - general overview - Debbie
*including summary of literature on each of the BRCs:
**BRC 38 - Jackie
**BRC 27 - Lauren
**BRC 34 - Robert
*Analysis plan - Peggy
*Edu plan - everyone

For most of this, you will now need to get into literature searching.
Tips for literature searching on the wiki [[How_can_I_find_out_what_scientists_already_know_about_a_particular_astronomy_topic_or_object%3F |are here]], with a link at the bottom of that page with more words.
In summary:
*use ADS.
*use SIMBAD.
they are interlinked, but searching in both doesn't always give you
the same results.
in SIMBAD, you can search by position, and you should use a
~10 arcmin radius to look for objects. what other named objects are
nearby? there may be other useful papers calling those other objects
by those other names.
To get articles, remember that you don't HAVE to go to the journal.
For 'old enough' papers, they will be free.
For newer papers, look for an arXiv link on the ADS abstract page.
If you still can't get it, or want the final typeset journal version,
send me an email with the ADS link, and I'll send back the PDF.
ADS will cough up abstracts to proposals, abstracts from conferences
without conference proceedings, conference proceedings, and refereed
journal articles. that list is from least useful to most useful.

somewaht confusingly, sorry, links to some of the papers i list below are collected on [[C-WAYS_Spring_work |this page]], sorry. in the interest of getting this out to you, i didn't want to spend the time going to retrieve and link all of the abstract links again. we will ultimately be adding some of the papers you find to this spring work page, so this makes sense in the long run, but sorry for any additional confusion.

So that everyone understands the big picture, read the intro to
Sugitani K., Fukui Y., Ogura K., 1991, ApJS, 77, 59. = SFO, because it
is the discovery paper for the BRC catalog.

'''Intro - Debbie''' -
look closely at last year's prop intro. go find the papers they
reference. look at the SFO paper, and others they reference. look at
the YSO background inforamtion on the wiki.

'''BRC 38 - Jackie''' -
You have the biggest literature search problem, because we've done the
least collective work here.
You have leads for five papers from the wiki discussion about bouncing
target selection:
*Chauhan et al below.
*Garmire & Gordon - chandra proposal - look for a paper by these guys reporting these results, but it might not exist
*Valdettaro etal - also turns up in one of the other BRC searches.
*choudhury et al.
*Morgan et al.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before. if you find a paper, the first thing you should do is look at this list to see if we grabbed and kept it or grabbed and discarded it before. assess (and keep track of) any new ones! it is likely there more you can find. yell if you need help. don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12:''' [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.
'''UPDATE 2/2/12:''' Can you tell I'm going through some backlogged papers? I just found [http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran et al. (2009)], which does deep JHK imaging in BRC38=IC1396N. This is another really good paper, with lots of good observations.
*I have listed the articles [[Jackie_BRC_38]] that I have found and some info about BRC 38 that I have gleamed. Please look it over, edit, correct, answer questions, ask questions - Jackie

'''BRC 27 - Lauren''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before.
if you find a paper, the first thing you should do is look at this
list to see if we grabbed and kept it or grabbed and discarded it
before. assess (and keep track of) any new ones!
don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
papers i know you will want to scan:

*Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. - does JHK + spitzer search for brc 27, 38 but we know they didn't do that great a job in 27, so they probably didn't do a great job in 38! but we need to mention in the proposal that this work exists and that we will compare our results to theirs.
*Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&A, 2009, 506, 711.
*Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210.
*Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395.

*My first draft of the science background and education plan is now on [[Lauren_BRC 27]]

'''BRC 34- Robert''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]] lists all the literature we decided to care about before.
you will note that very few mention BRC 34!
The only one that was terribly useful was Ogura et al. 2002, AJ, 123,
2597, and even that, not very much.
don't forget to try a SIMBAD search by position.
if you exhaust the available literature without finding more, go help
jackie with BRC 38. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.

Below is a link to what archival data is available from Spitzer for BRC 34.
[http://archive.spitzer.caltech.edu/searchByPosition.do]--[[User:French|French]] 13:17, 22 February 2012 (PST)

'''analysis - Peggy''' -
[[Analysis Work Space]]

look at the proposal from last time.
look at Rebull et al., 2011, ApJS, 196, 4 (the taurus/WISE paper) i
gave you for that methodology.
scan the appendix of Koenig et al., 2012, ApJ, 744, 130 -- we will get
into this in more detail later, but this is the color selection
mechanism using WISE colors.
mention that we will re-reduce the Spitzer data for brc 38 if need be,
and redo photometry on the serendipitously obtained spitzer off-source
fields in the area if we need to -- the gang last year wasn't too
concerned about those objects. (you can use similar words from last
time involving MOPEX and APT). don't worry about reading the makovoz
and marleau paper - way thick reading and not all that relevant. can
cite Laher et al 2012 in prep for APT (dunno if we did that last year
or not).
we will merge with 2MASS, AKARI, anything else we can find.
don't forget that we will have ground based optical data from JD to
contribute as well. will need to get words from him on that.
other important words - BRC 27 data already in the WISE public
release; rest will be available in March 2012. i can give you a figure
with that comparison when we get there.
'''UPDATE 2/1:''' FWIW, that Barentsen et al 2011 paper is IPHAS data, so you can add in to your analysis section that we will include IPHAS data for at least brc 34 and 38. their website says a new delivery is expected in 2012, so we'll do a new search if we can, else we'll just use the more limited stuff from the published paper.

'''Edu section''' - you're all on your own :)

FOR NEXT WEEK - read the proposal and (intro to the) SFO paper, get into your proposal section and see how much progress you can make on your proposal section. if you run out of stuff to do, ask if others need help.

=Education Section=
Below is a rough draft for my education section. Comments/suggestions are appreciated!

"New Philadelphia High School (D. French). New Philadelphia High School Students will be participating in the NITARP research project as an extra-curricular activity and may apply for the Ohio Flex Credit option. Students will be selected via an application process in March or April 2012.

''I'm wondering what your application criteria will be. I have gone for kids with high interest level vs great academic records in the past. Do we want to find a common ground here, or are we ok with having different types of kids on different teams?''--Peggy Piper 12:41, 17 February 2012 (PST)

"Students will participate in weekly research meetings to discuss background information, journal articles, and to work on data reduction and analysis. They will be responsible for keeping a science notebook for recording notes, comments, and for keeping applicable journal articles. Students will use the NITARP CoolWiki page to obtain additional background information and communicate with other team members. After the January 2012 AAS meeting, they will present their research to the New Philadelphia Board of Education as well as other possible venues and outreach activities."
--[[User:French|French]] 08:38, 16 February 2012 (PST)

C-WAYS Proposal

2012-02-16T16:39:40Z

French: /* Education Section */

=Instructions=

[[2012 proposal instructions]]

=Proposal nitty gritty - first round, 1/27/12=

Everyone should read last year's BRC proposal if you haven't already.

As per the instructions for this year's proposal, we need to have:

*Abstract - write that last!
*Science introduction and context - general overview - Debbie
*including summary of literature on each of the BRCs:
**BRC 38 - Jackie
**BRC 27 - Lauren
**BRC 34 - Robert
*Analysis plan - Peggy
*Edu plan - everyone

For most of this, you will now need to get into literature searching.
Tips for literature searching on the wiki [[How_can_I_find_out_what_scientists_already_know_about_a_particular_astronomy_topic_or_object%3F |are here]], with a link at the bottom of that page with more words.
In summary:
*use ADS.
*use SIMBAD.
they are interlinked, but searching in both doesn't always give you
the same results.
in SIMBAD, you can search by position, and you should use a
~10 arcmin radius to look for objects. what other named objects are
nearby? there may be other useful papers calling those other objects
by those other names.
To get articles, remember that you don't HAVE to go to the journal.
For 'old enough' papers, they will be free.
For newer papers, look for an arXiv link on the ADS abstract page.
If you still can't get it, or want the final typeset journal version,
send me an email with the ADS link, and I'll send back the PDF.
ADS will cough up abstracts to proposals, abstracts from conferences
without conference proceedings, conference proceedings, and refereed
journal articles. that list is from least useful to most useful.

somewaht confusingly, sorry, links to some of the papers i list below are collected on [[C-WAYS_Spring_work |this page]], sorry. in the interest of getting this out to you, i didn't want to spend the time going to retrieve and link all of the abstract links again. we will ultimately be adding some of the papers you find to this spring work page, so this makes sense in the long run, but sorry for any additional confusion.

So that everyone understands the big picture, read the intro to
Sugitani K., Fukui Y., Ogura K., 1991, ApJS, 77, 59. = SFO, because it
is the discovery paper for the BRC catalog.

'''Intro - Debbie''' -
look closely at last year's prop intro. go find the papers they
reference. look at the SFO paper, and others they reference. look at
the YSO background inforamtion on the wiki.

'''BRC 38 - Jackie''' -
You have the biggest literature search problem, because we've done the
least collective work here.
You have leads for five papers from the wiki discussion about bouncing
target selection:
*Chauhan et al below.
*Garmire & Gordon - chandra proposal - look for a paper by these guys reporting these results, but it might not exist
*Valdettaro etal - also turns up in one of the other BRC searches.
*choudhury et al.
*Morgan et al.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before. if you find a paper, the first thing you should do is look at this list to see if we grabbed and kept it or grabbed and discarded it before. assess (and keep track of) any new ones! it is likely there more you can find. yell if you need help. don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12:''' [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.
'''UPDATE 2/2/12:''' Can you tell I'm going through some backlogged papers? I just found [http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran et al. (2009)], which does deep JHK imaging in BRC38=IC1396N. This is another really good paper, with lots of good observations.
*I have listed the articles [[Jackie_BRC_38]] that I have found and some info about BRC 38 that I have gleamed. Please look it over, edit, correct, answer questions, ask questions - Jackie

'''BRC 27 - Lauren''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before.
if you find a paper, the first thing you should do is look at this
list to see if we grabbed and kept it or grabbed and discarded it
before. assess (and keep track of) any new ones!
don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
papers i know you will want to scan:

*Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. - does JHK + spitzer search for brc 27, 38 but we know they didn't do that great a job in 27, so they probably didn't do a great job in 38! but we need to mention in the proposal that this work exists and that we will compare our results to theirs.
*Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&A, 2009, 506, 711.
*Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210.
*Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395.

'''BRC 34- Robert''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]] lists all the literature we decided to care about before.
you will note that very few mention BRC 34!
The only one that was terribly useful was Ogura et al. 2002, AJ, 123,
2597, and even that, not very much.
don't forget to try a SIMBAD search by position.
if you exhaust the available literature without finding more, go help
jackie with BRC 38. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.

'''analysis - Peggy''' -
[[Analysis Work Space]]

look at the proposal from last time.
look at Rebull et al., 2011, ApJS, 196, 4 (the taurus/WISE paper) i
gave you for that methodology.
scan the appendix of Koenig et al., 2012, ApJ, 744, 130 -- we will get
into this in more detail later, but this is the color selection
mechanism using WISE colors.
mention that we will re-reduce the Spitzer data for brc 38 if need be,
and redo photometry on the serendipitously obtained spitzer off-source
fields in the area if we need to -- the gang last year wasn't too
concerned about those objects. (you can use similar words from last
time involving MOPEX and APT). don't worry about reading the makovoz
and marleau paper - way thick reading and not all that relevant. can
cite Laher et al 2012 in prep for APT (dunno if we did that last year
or not).
we will merge with 2MASS, AKARI, anything else we can find.
don't forget that we will have ground based optical data from JD to
contribute as well. will need to get words from him on that.
other important words - BRC 27 data already in the WISE public
release; rest will be available in March 2012. i can give you a figure
with that comparison when we get there.
'''UPDATE 2/1:''' FWIW, that Barentsen et al 2011 paper is IPHAS data, so you can add in to your analysis section that we will include IPHAS data for at least brc 34 and 38. their website says a new delivery is expected in 2012, so we'll do a new search if we can, else we'll just use the more limited stuff from the published paper.

'''Edu section''' - you're all on your own :)

FOR NEXT WEEK - read the proposal and (intro to the) SFO paper, get into your proposal section and see how much progress you can make on your proposal section. if you run out of stuff to do, ask if others need help.

=Education Section=
Below is a rough draft for my education section. Comments/suggestions are appreciated!

"New Philadelphia High School (D. French). New Philadelphia High School Students will be participating in the NITARP research project as an extra-curricular activity and may apply for the Ohio Flex Credit option. Students will be selected via an application process in March or April 2012.

"Students will participate in weekly research meetings to discuss background information, journal articles, and to work on data reduction and analysis. They will be responsible for keeping a science notebook for recording notes, comments, and for keeping applicable journal articles. Students will use the NITARP CoolWiki page to obtain additional background information and communicate with other team members. After the January 2012 AAS meeting, they will present their research to the New Philadelphia Board of Education as well as other possible venues and outreach activities."
--[[User:French|French]] 08:38, 16 February 2012 (PST)

C-WAYS Proposal

2012-02-16T16:39:26Z

French: /* Education Section */

=Instructions=

[[2012 proposal instructions]]

=Proposal nitty gritty - first round, 1/27/12=

Everyone should read last year's BRC proposal if you haven't already.

As per the instructions for this year's proposal, we need to have:

*Abstract - write that last!
*Science introduction and context - general overview - Debbie
*including summary of literature on each of the BRCs:
**BRC 38 - Jackie
**BRC 27 - Lauren
**BRC 34 - Robert
*Analysis plan - Peggy
*Edu plan - everyone

For most of this, you will now need to get into literature searching.
Tips for literature searching on the wiki [[How_can_I_find_out_what_scientists_already_know_about_a_particular_astronomy_topic_or_object%3F |are here]], with a link at the bottom of that page with more words.
In summary:
*use ADS.
*use SIMBAD.
they are interlinked, but searching in both doesn't always give you
the same results.
in SIMBAD, you can search by position, and you should use a
~10 arcmin radius to look for objects. what other named objects are
nearby? there may be other useful papers calling those other objects
by those other names.
To get articles, remember that you don't HAVE to go to the journal.
For 'old enough' papers, they will be free.
For newer papers, look for an arXiv link on the ADS abstract page.
If you still can't get it, or want the final typeset journal version,
send me an email with the ADS link, and I'll send back the PDF.
ADS will cough up abstracts to proposals, abstracts from conferences
without conference proceedings, conference proceedings, and refereed
journal articles. that list is from least useful to most useful.

somewaht confusingly, sorry, links to some of the papers i list below are collected on [[C-WAYS_Spring_work |this page]], sorry. in the interest of getting this out to you, i didn't want to spend the time going to retrieve and link all of the abstract links again. we will ultimately be adding some of the papers you find to this spring work page, so this makes sense in the long run, but sorry for any additional confusion.

So that everyone understands the big picture, read the intro to
Sugitani K., Fukui Y., Ogura K., 1991, ApJS, 77, 59. = SFO, because it
is the discovery paper for the BRC catalog.

'''Intro - Debbie''' -
look closely at last year's prop intro. go find the papers they
reference. look at the SFO paper, and others they reference. look at
the YSO background inforamtion on the wiki.

'''BRC 38 - Jackie''' -
You have the biggest literature search problem, because we've done the
least collective work here.
You have leads for five papers from the wiki discussion about bouncing
target selection:
*Chauhan et al below.
*Garmire & Gordon - chandra proposal - look for a paper by these guys reporting these results, but it might not exist
*Valdettaro etal - also turns up in one of the other BRC searches.
*choudhury et al.
*Morgan et al.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before. if you find a paper, the first thing you should do is look at this list to see if we grabbed and kept it or grabbed and discarded it before. assess (and keep track of) any new ones! it is likely there more you can find. yell if you need help. don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12:''' [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.
'''UPDATE 2/2/12:''' Can you tell I'm going through some backlogged papers? I just found [http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran et al. (2009)], which does deep JHK imaging in BRC38=IC1396N. This is another really good paper, with lots of good observations.
*I have listed the articles [[Jackie_BRC_38]] that I have found and some info about BRC 38 that I have gleamed. Please look it over, edit, correct, answer questions, ask questions - Jackie

'''BRC 27 - Lauren''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before.
if you find a paper, the first thing you should do is look at this
list to see if we grabbed and kept it or grabbed and discarded it
before. assess (and keep track of) any new ones!
don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
papers i know you will want to scan:

*Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. - does JHK + spitzer search for brc 27, 38 but we know they didn't do that great a job in 27, so they probably didn't do a great job in 38! but we need to mention in the proposal that this work exists and that we will compare our results to theirs.
*Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&A, 2009, 506, 711.
*Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210.
*Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395.

'''BRC 34- Robert''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]] lists all the literature we decided to care about before.
you will note that very few mention BRC 34!
The only one that was terribly useful was Ogura et al. 2002, AJ, 123,
2597, and even that, not very much.
don't forget to try a SIMBAD search by position.
if you exhaust the available literature without finding more, go help
jackie with BRC 38. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.

'''analysis - Peggy''' -
[[Analysis Work Space]]

look at the proposal from last time.
look at Rebull et al., 2011, ApJS, 196, 4 (the taurus/WISE paper) i
gave you for that methodology.
scan the appendix of Koenig et al., 2012, ApJ, 744, 130 -- we will get
into this in more detail later, but this is the color selection
mechanism using WISE colors.
mention that we will re-reduce the Spitzer data for brc 38 if need be,
and redo photometry on the serendipitously obtained spitzer off-source
fields in the area if we need to -- the gang last year wasn't too
concerned about those objects. (you can use similar words from last
time involving MOPEX and APT). don't worry about reading the makovoz
and marleau paper - way thick reading and not all that relevant. can
cite Laher et al 2012 in prep for APT (dunno if we did that last year
or not).
we will merge with 2MASS, AKARI, anything else we can find.
don't forget that we will have ground based optical data from JD to
contribute as well. will need to get words from him on that.
other important words - BRC 27 data already in the WISE public
release; rest will be available in March 2012. i can give you a figure
with that comparison when we get there.
'''UPDATE 2/1:''' FWIW, that Barentsen et al 2011 paper is IPHAS data, so you can add in to your analysis section that we will include IPHAS data for at least brc 34 and 38. their website says a new delivery is expected in 2012, so we'll do a new search if we can, else we'll just use the more limited stuff from the published paper.

'''Edu section''' - you're all on your own :)

FOR NEXT WEEK - read the proposal and (intro to the) SFO paper, get into your proposal section and see how much progress you can make on your proposal section. if you run out of stuff to do, ask if others need help.

=Education Section=
Below is a rough draft for my education section. Comments/suggestions are appreciated!

"New Philadelphia High School (D. French). New Philadelphia High School Students will be participating in the NITARP research project as an extra-curricular activity and may apply for the Ohio Flex Credit option. Students will be selected via an application process in March or April 2012.

"Students will participate in weekly research meetings to discuss background information, journal articles, and to work on data reduction and analysis. They will be responsible for keeping a science notebook for recording notes, comments, and for keeping applicable journal articles. Students will use the NITARP CoolWiki page to obtain additional background information and communicate with other team members. After the January 2012 AAS meeting, they will present their research to the New Philadelphia Board of Education as well as other possible venues and outreach activites."
--[[User:French|French]] 08:38, 16 February 2012 (PST)

C-WAYS Proposal

2012-02-16T16:38:56Z

French: /* Education Section */

=Instructions=

[[2012 proposal instructions]]

=Proposal nitty gritty - first round, 1/27/12=

Everyone should read last year's BRC proposal if you haven't already.

As per the instructions for this year's proposal, we need to have:

*Abstract - write that last!
*Science introduction and context - general overview - Debbie
*including summary of literature on each of the BRCs:
**BRC 38 - Jackie
**BRC 27 - Lauren
**BRC 34 - Robert
*Analysis plan - Peggy
*Edu plan - everyone

For most of this, you will now need to get into literature searching.
Tips for literature searching on the wiki [[How_can_I_find_out_what_scientists_already_know_about_a_particular_astronomy_topic_or_object%3F |are here]], with a link at the bottom of that page with more words.
In summary:
*use ADS.
*use SIMBAD.
they are interlinked, but searching in both doesn't always give you
the same results.
in SIMBAD, you can search by position, and you should use a
~10 arcmin radius to look for objects. what other named objects are
nearby? there may be other useful papers calling those other objects
by those other names.
To get articles, remember that you don't HAVE to go to the journal.
For 'old enough' papers, they will be free.
For newer papers, look for an arXiv link on the ADS abstract page.
If you still can't get it, or want the final typeset journal version,
send me an email with the ADS link, and I'll send back the PDF.
ADS will cough up abstracts to proposals, abstracts from conferences
without conference proceedings, conference proceedings, and refereed
journal articles. that list is from least useful to most useful.

somewaht confusingly, sorry, links to some of the papers i list below are collected on [[C-WAYS_Spring_work |this page]], sorry. in the interest of getting this out to you, i didn't want to spend the time going to retrieve and link all of the abstract links again. we will ultimately be adding some of the papers you find to this spring work page, so this makes sense in the long run, but sorry for any additional confusion.

So that everyone understands the big picture, read the intro to
Sugitani K., Fukui Y., Ogura K., 1991, ApJS, 77, 59. = SFO, because it
is the discovery paper for the BRC catalog.

'''Intro - Debbie''' -
look closely at last year's prop intro. go find the papers they
reference. look at the SFO paper, and others they reference. look at
the YSO background inforamtion on the wiki.

'''BRC 38 - Jackie''' -
You have the biggest literature search problem, because we've done the
least collective work here.
You have leads for five papers from the wiki discussion about bouncing
target selection:
*Chauhan et al below.
*Garmire & Gordon - chandra proposal - look for a paper by these guys reporting these results, but it might not exist
*Valdettaro etal - also turns up in one of the other BRC searches.
*choudhury et al.
*Morgan et al.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before. if you find a paper, the first thing you should do is look at this list to see if we grabbed and kept it or grabbed and discarded it before. assess (and keep track of) any new ones! it is likely there more you can find. yell if you need help. don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12:''' [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.
'''UPDATE 2/2/12:''' Can you tell I'm going through some backlogged papers? I just found [http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran et al. (2009)], which does deep JHK imaging in BRC38=IC1396N. This is another really good paper, with lots of good observations.
*I have listed the articles [[Jackie_BRC_38]] that I have found and some info about BRC 38 that I have gleamed. Please look it over, edit, correct, answer questions, ask questions - Jackie

'''BRC 27 - Lauren''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before.
if you find a paper, the first thing you should do is look at this
list to see if we grabbed and kept it or grabbed and discarded it
before. assess (and keep track of) any new ones!
don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
papers i know you will want to scan:

*Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. - does JHK + spitzer search for brc 27, 38 but we know they didn't do that great a job in 27, so they probably didn't do a great job in 38! but we need to mention in the proposal that this work exists and that we will compare our results to theirs.
*Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&A, 2009, 506, 711.
*Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210.
*Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395.

'''BRC 34- Robert''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]] lists all the literature we decided to care about before.
you will note that very few mention BRC 34!
The only one that was terribly useful was Ogura et al. 2002, AJ, 123,
2597, and even that, not very much.
don't forget to try a SIMBAD search by position.
if you exhaust the available literature without finding more, go help
jackie with BRC 38. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.

'''analysis - Peggy''' -
[[Analysis Work Space]]

look at the proposal from last time.
look at Rebull et al., 2011, ApJS, 196, 4 (the taurus/WISE paper) i
gave you for that methodology.
scan the appendix of Koenig et al., 2012, ApJ, 744, 130 -- we will get
into this in more detail later, but this is the color selection
mechanism using WISE colors.
mention that we will re-reduce the Spitzer data for brc 38 if need be,
and redo photometry on the serendipitously obtained spitzer off-source
fields in the area if we need to -- the gang last year wasn't too
concerned about those objects. (you can use similar words from last
time involving MOPEX and APT). don't worry about reading the makovoz
and marleau paper - way thick reading and not all that relevant. can
cite Laher et al 2012 in prep for APT (dunno if we did that last year
or not).
we will merge with 2MASS, AKARI, anything else we can find.
don't forget that we will have ground based optical data from JD to
contribute as well. will need to get words from him on that.
other important words - BRC 27 data already in the WISE public
release; rest will be available in March 2012. i can give you a figure
with that comparison when we get there.
'''UPDATE 2/1:''' FWIW, that Barentsen et al 2011 paper is IPHAS data, so you can add in to your analysis section that we will include IPHAS data for at least brc 34 and 38. their website says a new delivery is expected in 2012, so we'll do a new search if we can, else we'll just use the more limited stuff from the published paper.

'''Edu section''' - you're all on your own :)

FOR NEXT WEEK - read the proposal and (intro to the) SFO paper, get into your proposal section and see how much progress you can make on your proposal section. if you run out of stuff to do, ask if others need help.

=Education Section=
Below is a rough draft for my education section. Comments/suggestions are appreciated!

"New Philadelphia High School (D. French). New Philadelphia High School Students will be participating in the NITARP research project as an extra-curricular activity and may apply for the Ohio Flex Credit option. Students will be selected via an application process in March or April 2012.

"Students will participate in weekly research meetings to discuss background information, journal articles, and to work on data reduction and analysis. They will be responsible for keeping a science notebook for recording notes, comments, and for keeping applicable journal articles. Students will use the NITARP CoolWiki page to obtain additional background information and communicate with other team members. After the January 2012 AAS meeting, they will present their research to the New Philadelphia Board of Education as well as other possible venues."
--[[User:French|French]] 08:38, 16 February 2012 (PST)

C-WAYS Proposal

2012-02-16T16:38:48Z

French: /* Education Section */

=Instructions=

[[2012 proposal instructions]]

=Proposal nitty gritty - first round, 1/27/12=

Everyone should read last year's BRC proposal if you haven't already.

As per the instructions for this year's proposal, we need to have:

*Abstract - write that last!
*Science introduction and context - general overview - Debbie
*including summary of literature on each of the BRCs:
**BRC 38 - Jackie
**BRC 27 - Lauren
**BRC 34 - Robert
*Analysis plan - Peggy
*Edu plan - everyone

For most of this, you will now need to get into literature searching.
Tips for literature searching on the wiki [[How_can_I_find_out_what_scientists_already_know_about_a_particular_astronomy_topic_or_object%3F |are here]], with a link at the bottom of that page with more words.
In summary:
*use ADS.
*use SIMBAD.
they are interlinked, but searching in both doesn't always give you
the same results.
in SIMBAD, you can search by position, and you should use a
~10 arcmin radius to look for objects. what other named objects are
nearby? there may be other useful papers calling those other objects
by those other names.
To get articles, remember that you don't HAVE to go to the journal.
For 'old enough' papers, they will be free.
For newer papers, look for an arXiv link on the ADS abstract page.
If you still can't get it, or want the final typeset journal version,
send me an email with the ADS link, and I'll send back the PDF.
ADS will cough up abstracts to proposals, abstracts from conferences
without conference proceedings, conference proceedings, and refereed
journal articles. that list is from least useful to most useful.

somewaht confusingly, sorry, links to some of the papers i list below are collected on [[C-WAYS_Spring_work |this page]], sorry. in the interest of getting this out to you, i didn't want to spend the time going to retrieve and link all of the abstract links again. we will ultimately be adding some of the papers you find to this spring work page, so this makes sense in the long run, but sorry for any additional confusion.

So that everyone understands the big picture, read the intro to
Sugitani K., Fukui Y., Ogura K., 1991, ApJS, 77, 59. = SFO, because it
is the discovery paper for the BRC catalog.

'''Intro - Debbie''' -
look closely at last year's prop intro. go find the papers they
reference. look at the SFO paper, and others they reference. look at
the YSO background inforamtion on the wiki.

'''BRC 38 - Jackie''' -
You have the biggest literature search problem, because we've done the
least collective work here.
You have leads for five papers from the wiki discussion about bouncing
target selection:
*Chauhan et al below.
*Garmire & Gordon - chandra proposal - look for a paper by these guys reporting these results, but it might not exist
*Valdettaro etal - also turns up in one of the other BRC searches.
*choudhury et al.
*Morgan et al.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before. if you find a paper, the first thing you should do is look at this list to see if we grabbed and kept it or grabbed and discarded it before. assess (and keep track of) any new ones! it is likely there more you can find. yell if you need help. don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12:''' [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.
'''UPDATE 2/2/12:''' Can you tell I'm going through some backlogged papers? I just found [http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran et al. (2009)], which does deep JHK imaging in BRC38=IC1396N. This is another really good paper, with lots of good observations.
*I have listed the articles [[Jackie_BRC_38]] that I have found and some info about BRC 38 that I have gleamed. Please look it over, edit, correct, answer questions, ask questions - Jackie

'''BRC 27 - Lauren''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before.
if you find a paper, the first thing you should do is look at this
list to see if we grabbed and kept it or grabbed and discarded it
before. assess (and keep track of) any new ones!
don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
papers i know you will want to scan:

*Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. - does JHK + spitzer search for brc 27, 38 but we know they didn't do that great a job in 27, so they probably didn't do a great job in 38! but we need to mention in the proposal that this work exists and that we will compare our results to theirs.
*Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&A, 2009, 506, 711.
*Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210.
*Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395.

'''BRC 34- Robert''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]] lists all the literature we decided to care about before.
you will note that very few mention BRC 34!
The only one that was terribly useful was Ogura et al. 2002, AJ, 123,
2597, and even that, not very much.
don't forget to try a SIMBAD search by position.
if you exhaust the available literature without finding more, go help
jackie with BRC 38. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.

'''analysis - Peggy''' -
[[Analysis Work Space]]

look at the proposal from last time.
look at Rebull et al., 2011, ApJS, 196, 4 (the taurus/WISE paper) i
gave you for that methodology.
scan the appendix of Koenig et al., 2012, ApJ, 744, 130 -- we will get
into this in more detail later, but this is the color selection
mechanism using WISE colors.
mention that we will re-reduce the Spitzer data for brc 38 if need be,
and redo photometry on the serendipitously obtained spitzer off-source
fields in the area if we need to -- the gang last year wasn't too
concerned about those objects. (you can use similar words from last
time involving MOPEX and APT). don't worry about reading the makovoz
and marleau paper - way thick reading and not all that relevant. can
cite Laher et al 2012 in prep for APT (dunno if we did that last year
or not).
we will merge with 2MASS, AKARI, anything else we can find.
don't forget that we will have ground based optical data from JD to
contribute as well. will need to get words from him on that.
other important words - BRC 27 data already in the WISE public
release; rest will be available in March 2012. i can give you a figure
with that comparison when we get there.
'''UPDATE 2/1:''' FWIW, that Barentsen et al 2011 paper is IPHAS data, so you can add in to your analysis section that we will include IPHAS data for at least brc 34 and 38. their website says a new delivery is expected in 2012, so we'll do a new search if we can, else we'll just use the more limited stuff from the published paper.

'''Edu section''' - you're all on your own :)

FOR NEXT WEEK - read the proposal and (intro to the) SFO paper, get into your proposal section and see how much progress you can make on your proposal section. if you run out of stuff to do, ask if others need help.

=Education Section=
Below is a rough draft for my education section. Comments/suggestions are appreciated!

"New Philadelphia High School (D. French). New Philadelphia High School Students will be participating in the NITARP research project as an extra-curricular activity and may apply for the Ohio Flex Credit option. Students will be selected via an application process in March or April 2012.

"Students will participate in weekly research meetings to discuss background information, journal articles, and to work on data reduction and analysis. They will be responsible for keeping a science notebook for recording notes, comments, and for keeping applicable journal articles. Students will use the NITARP CoolWiki page to obtain additional background information and communicate with other team members. After the January 2012 AAS meeting, they will present their research to the New Philadelphia Board of Education as well as other possible venues."

File:NPHS NITARP Ed Section.docx

2012-02-16T16:37:12Z

French: uploaded a new version of "File:NPHS NITARP Ed Section.docx"

C-WAYS Proposal

2012-02-16T16:36:40Z

French: /* Education Section */

=Instructions=

[[2012 proposal instructions]]

=Proposal nitty gritty - first round, 1/27/12=

Everyone should read last year's BRC proposal if you haven't already.

As per the instructions for this year's proposal, we need to have:

*Abstract - write that last!
*Science introduction and context - general overview - Debbie
*including summary of literature on each of the BRCs:
**BRC 38 - Jackie
**BRC 27 - Lauren
**BRC 34 - Robert
*Analysis plan - Peggy
*Edu plan - everyone

For most of this, you will now need to get into literature searching.
Tips for literature searching on the wiki [[How_can_I_find_out_what_scientists_already_know_about_a_particular_astronomy_topic_or_object%3F |are here]], with a link at the bottom of that page with more words.
In summary:
*use ADS.
*use SIMBAD.
they are interlinked, but searching in both doesn't always give you
the same results.
in SIMBAD, you can search by position, and you should use a
~10 arcmin radius to look for objects. what other named objects are
nearby? there may be other useful papers calling those other objects
by those other names.
To get articles, remember that you don't HAVE to go to the journal.
For 'old enough' papers, they will be free.
For newer papers, look for an arXiv link on the ADS abstract page.
If you still can't get it, or want the final typeset journal version,
send me an email with the ADS link, and I'll send back the PDF.
ADS will cough up abstracts to proposals, abstracts from conferences
without conference proceedings, conference proceedings, and refereed
journal articles. that list is from least useful to most useful.

somewaht confusingly, sorry, links to some of the papers i list below are collected on [[C-WAYS_Spring_work |this page]], sorry. in the interest of getting this out to you, i didn't want to spend the time going to retrieve and link all of the abstract links again. we will ultimately be adding some of the papers you find to this spring work page, so this makes sense in the long run, but sorry for any additional confusion.

So that everyone understands the big picture, read the intro to
Sugitani K., Fukui Y., Ogura K., 1991, ApJS, 77, 59. = SFO, because it
is the discovery paper for the BRC catalog.

'''Intro - Debbie''' -
look closely at last year's prop intro. go find the papers they
reference. look at the SFO paper, and others they reference. look at
the YSO background inforamtion on the wiki.

'''BRC 38 - Jackie''' -
You have the biggest literature search problem, because we've done the
least collective work here.
You have leads for five papers from the wiki discussion about bouncing
target selection:
*Chauhan et al below.
*Garmire & Gordon - chandra proposal - look for a paper by these guys reporting these results, but it might not exist
*Valdettaro etal - also turns up in one of the other BRC searches.
*choudhury et al.
*Morgan et al.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before. if you find a paper, the first thing you should do is look at this list to see if we grabbed and kept it or grabbed and discarded it before. assess (and keep track of) any new ones! it is likely there more you can find. yell if you need help. don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12:''' [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.
'''UPDATE 2/2/12:''' Can you tell I'm going through some backlogged papers? I just found [http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran et al. (2009)], which does deep JHK imaging in BRC38=IC1396N. This is another really good paper, with lots of good observations.
*I have listed the articles [[Jackie_BRC_38]] that I have found and some info about BRC 38 that I have gleamed. Please look it over, edit, correct, answer questions, ask questions - Jackie

'''BRC 27 - Lauren''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before.
if you find a paper, the first thing you should do is look at this
list to see if we grabbed and kept it or grabbed and discarded it
before. assess (and keep track of) any new ones!
don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
papers i know you will want to scan:

*Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. - does JHK + spitzer search for brc 27, 38 but we know they didn't do that great a job in 27, so they probably didn't do a great job in 38! but we need to mention in the proposal that this work exists and that we will compare our results to theirs.
*Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&A, 2009, 506, 711.
*Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210.
*Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395.

'''BRC 34- Robert''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]] lists all the literature we decided to care about before.
you will note that very few mention BRC 34!
The only one that was terribly useful was Ogura et al. 2002, AJ, 123,
2597, and even that, not very much.
don't forget to try a SIMBAD search by position.
if you exhaust the available literature without finding more, go help
jackie with BRC 38. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.

'''analysis - Peggy''' -
[[Analysis Work Space]]

look at the proposal from last time.
look at Rebull et al., 2011, ApJS, 196, 4 (the taurus/WISE paper) i
gave you for that methodology.
scan the appendix of Koenig et al., 2012, ApJ, 744, 130 -- we will get
into this in more detail later, but this is the color selection
mechanism using WISE colors.
mention that we will re-reduce the Spitzer data for brc 38 if need be,
and redo photometry on the serendipitously obtained spitzer off-source
fields in the area if we need to -- the gang last year wasn't too
concerned about those objects. (you can use similar words from last
time involving MOPEX and APT). don't worry about reading the makovoz
and marleau paper - way thick reading and not all that relevant. can
cite Laher et al 2012 in prep for APT (dunno if we did that last year
or not).
we will merge with 2MASS, AKARI, anything else we can find.
don't forget that we will have ground based optical data from JD to
contribute as well. will need to get words from him on that.
other important words - BRC 27 data already in the WISE public
release; rest will be available in March 2012. i can give you a figure
with that comparison when we get there.
'''UPDATE 2/1:''' FWIW, that Barentsen et al 2011 paper is IPHAS data, so you can add in to your analysis section that we will include IPHAS data for at least brc 34 and 38. their website says a new delivery is expected in 2012, so we'll do a new search if we can, else we'll just use the more limited stuff from the published paper.

'''Edu section''' - you're all on your own :)

FOR NEXT WEEK - read the proposal and (intro to the) SFO paper, get into your proposal section and see how much progress you can make on your proposal section. if you run out of stuff to do, ask if others need help.

=Education Section=
Attached is a rough draft for my education section. Comments/suggestions are appreciated!
[[Media:NPHS NITARP Ed Section]]

File:NPHS NITARP Ed Section.docx

2012-02-16T16:34:04Z

French: uploaded a new version of "File:NPHS NITARP Ed Section.docx": Reverted to version as of 16:10, 16 February 2012

C-WAYS Proposal

2012-02-16T16:26:53Z

French:

=Instructions=

[[2012 proposal instructions]]

=Proposal nitty gritty - first round, 1/27/12=

Everyone should read last year's BRC proposal if you haven't already.

As per the instructions for this year's proposal, we need to have:

*Abstract - write that last!
*Science introduction and context - general overview - Debbie
*including summary of literature on each of the BRCs:
**BRC 38 - Jackie
**BRC 27 - Lauren
**BRC 34 - Robert
*Analysis plan - Peggy
*Edu plan - everyone

For most of this, you will now need to get into literature searching.
Tips for literature searching on the wiki [[How_can_I_find_out_what_scientists_already_know_about_a_particular_astronomy_topic_or_object%3F |are here]], with a link at the bottom of that page with more words.
In summary:
*use ADS.
*use SIMBAD.
they are interlinked, but searching in both doesn't always give you
the same results.
in SIMBAD, you can search by position, and you should use a
~10 arcmin radius to look for objects. what other named objects are
nearby? there may be other useful papers calling those other objects
by those other names.
To get articles, remember that you don't HAVE to go to the journal.
For 'old enough' papers, they will be free.
For newer papers, look for an arXiv link on the ADS abstract page.
If you still can't get it, or want the final typeset journal version,
send me an email with the ADS link, and I'll send back the PDF.
ADS will cough up abstracts to proposals, abstracts from conferences
without conference proceedings, conference proceedings, and refereed
journal articles. that list is from least useful to most useful.

somewaht confusingly, sorry, links to some of the papers i list below are collected on [[C-WAYS_Spring_work |this page]], sorry. in the interest of getting this out to you, i didn't want to spend the time going to retrieve and link all of the abstract links again. we will ultimately be adding some of the papers you find to this spring work page, so this makes sense in the long run, but sorry for any additional confusion.

So that everyone understands the big picture, read the intro to
Sugitani K., Fukui Y., Ogura K., 1991, ApJS, 77, 59. = SFO, because it
is the discovery paper for the BRC catalog.

'''Intro - Debbie''' -
look closely at last year's prop intro. go find the papers they
reference. look at the SFO paper, and others they reference. look at
the YSO background inforamtion on the wiki.

'''BRC 38 - Jackie''' -
You have the biggest literature search problem, because we've done the
least collective work here.
You have leads for five papers from the wiki discussion about bouncing
target selection:
*Chauhan et al below.
*Garmire & Gordon - chandra proposal - look for a paper by these guys reporting these results, but it might not exist
*Valdettaro etal - also turns up in one of the other BRC searches.
*choudhury et al.
*Morgan et al.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before. if you find a paper, the first thing you should do is look at this list to see if we grabbed and kept it or grabbed and discarded it before. assess (and keep track of) any new ones! it is likely there more you can find. yell if you need help. don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12:''' [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.
'''UPDATE 2/2/12:''' Can you tell I'm going through some backlogged papers? I just found [http://adsabs.harvard.edu/abs/2009A%26A...504...97B Beltran et al. (2009)], which does deep JHK imaging in BRC38=IC1396N. This is another really good paper, with lots of good observations.
*I have listed the articles [[Jackie_BRC_38]] that I have found and some info about BRC 38 that I have gleamed. Please look it over, edit, correct, answer questions, ask questions - Jackie

'''BRC 27 - Lauren''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]]
lists all the literature we decided to care about before.
if you find a paper, the first thing you should do is look at this
list to see if we grabbed and kept it or grabbed and discarded it
before. assess (and keep track of) any new ones!
don't forget to try a SIMBAD search by position. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
papers i know you will want to scan:

*Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. - does JHK + spitzer search for brc 27, 38 but we know they didn't do that great a job in 27, so they probably didn't do a great job in 38! but we need to mention in the proposal that this work exists and that we will compare our results to theirs.
*Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&A, 2009, 506, 711.
*Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210.
*Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395.

'''BRC 34- Robert''' -
you are looking for any literature we missed last time, or new stuff
that has appeared in the last 13 months.
[[BRC_Spring_work |this page]] which i grabbed and updated to be the meat of
[[C-WAYS_Spring_work |this page]] lists all the literature we decided to care about before.
you will note that very few mention BRC 34!
The only one that was terribly useful was Ogura et al. 2002, AJ, 123,
2597, and even that, not very much.
don't forget to try a SIMBAD search by position.
if you exhaust the available literature without finding more, go help
jackie with BRC 38. ('''UPDATE 1/30/12''': [http://www.youtube.com/watch?v=Negz3lERk6I Screencapture tutorial] on literature searching, with particular emphasis on SIMBAD-based searching. Nearly 10 minutes long, sorry.)
'''UPDATE 1/31/12:''' see email re: [http://adsabs.harvard.edu/abs/2011MNRAS.415..103B Barentsen et al. 2011, MNRAS, 415, 103], [http://adsabs.harvard.edu/abs/1996A%26A...309..581W Weikard et al 1996, A&A, 309, 581] and [http://adsabs.harvard.edu/abs/1956BAN....13...77P Pottasch 1956, BAN, 13, 77]. Based on what i can see, brc 34 = "D" in their nomenclature and brc 38 = "E", but you should definitely check me on this. Barentsen et al are looking for YSOs using Halpha in the whole entire region, and we can check on their selection using the WISE data in the environs of the two clouds we care about.

'''analysis - Peggy''' -
[[Analysis Work Space]]

look at the proposal from last time.
look at Rebull et al., 2011, ApJS, 196, 4 (the taurus/WISE paper) i
gave you for that methodology.
scan the appendix of Koenig et al., 2012, ApJ, 744, 130 -- we will get
into this in more detail later, but this is the color selection
mechanism using WISE colors.
mention that we will re-reduce the Spitzer data for brc 38 if need be,
and redo photometry on the serendipitously obtained spitzer off-source
fields in the area if we need to -- the gang last year wasn't too
concerned about those objects. (you can use similar words from last
time involving MOPEX and APT). don't worry about reading the makovoz
and marleau paper - way thick reading and not all that relevant. can
cite Laher et al 2012 in prep for APT (dunno if we did that last year
or not).
we will merge with 2MASS, AKARI, anything else we can find.
don't forget that we will have ground based optical data from JD to
contribute as well. will need to get words from him on that.
other important words - BRC 27 data already in the WISE public
release; rest will be available in March 2012. i can give you a figure
with that comparison when we get there.
'''UPDATE 2/1:''' FWIW, that Barentsen et al 2011 paper is IPHAS data, so you can add in to your analysis section that we will include IPHAS data for at least brc 34 and 38. their website says a new delivery is expected in 2012, so we'll do a new search if we can, else we'll just use the more limited stuff from the published paper.

'''Edu section''' - you're all on your own :)

FOR NEXT WEEK - read the proposal and (intro to the) SFO paper, get into your proposal section and see how much progress you can make on your proposal section. if you run out of stuff to do, ask if others need help.

=Education Section=
Attached is a rough draft for my education section. Comments/suggestions are appreciated!
[[Media:Example.ogg]]

File:NPHS NITARP Ed Section.docx

2012-02-16T16:23:41Z

French: uploaded a new version of "File:NPHS NITARP Ed Section.docx"

File:NPHS NITARP Ed Section.docx

2012-02-16T16:11:13Z

French:

C-WAYS: follow the bouncing target selection

2012-01-23T15:43:12Z

French: /* Stuff in prep for 1/27/12 telecon */

=Stuff in prep for 1/20/12 telecon=

OK, so at the AAS we talked about LDN 1548 as a viable option. It had, we thought, good potential for yielding new young stars, it was (in projected distance) near Taurus, it has the potential for being actually related to the Taurus Molecular Cloud (and thus of scientific interest). It also has SDSS data in the archive, so that's a strong plus -- more data will help us weed out the contaminants.

BUT.

I just went and got the whole WISE tile. It's REALLY diffuse star formation, MUCH worse than I remembered. I mean, bad enough that I went and checked the coordinates. More than once. This is what I see. There is not a lot here, and there is going to be a TON of contamination: [[image:ldn1548.png]]

I've gone back to my Taurus collaborators to figure out why we thought there was something interesting there.

But that probably drops us back at the beginning in terms of target selection, sigh. Sorry. But, this is real science, and I (honest-to-God) do NOT know the answer before we get into this. This is the real thing, folks.

The ''approach'' we talked about will be the same; we just need to find a better target.

So.

I decided to go resurrect some of the other regions that were under consideration. They were:
* LDN 1548- really diffuse and un-dramatic in WISE. sigh.
* "north of LDN 1509" -- Wilson had that in his poster, and that too is really diffuse star formation, so contamination is going to be high. But at least likely to yield more YSO candidates than LDN 1548 as far as I can tell. ON the other hand, Wilson wants to do that region! :)
* NGC 1579 -- still near (in projected distance) to Taurus - see fig 2 in the Taurus paper. It has high nebulosity in parts. There are famous objects here. Spitzer data too. A friend has an AAS abstract from 2007 claiming results with Spitzer, but there is no paper from it. I don't want to scoop him. Also potentially complicated data reduction. Probably not a good target.
* Continuing the BRC27/34 work begun by the 2011 team. BRC 34 is not in the data that are public right now, but BRC 27 is, and it is also part of a region of star formation in CMa that another friend was thinking about working on, but was willing to let it go. I don't think that you guys could handle the huge multi-degree span (read: millions of sources) that this thing really covers, but maybe working just around BRC 27, and BRC 34 since it will be available in March, is tractable? It is nice to have Spitzer for comparison (for a lesson in spatial resolution). BRC 27 is right on the border between two WISE tiles, so I can't make a pretty 3-color image for you. You kind of have to trust me ('cause you know, I've been so good at that so far) that this is an interesting region. In this eyeball-wrenching image, I did red as one WISE tile, green as the other WISE tile, and blue as the Spitzer data. You can see that the cloud clearly extends beyond the Spitzer boundaries. We'd have to decide how far out to search.
[[image:brc27wisecoverage.png]]

* Other BRC options - we had considered BRC 31, 36, 38. BRC 31 is already thoroughly done (Rebull et al. 2011). BRC 34 (which the 2011 group did), BRC 36 and BRC 38 are all close to IC1396, another region I'm studying with another project. BRC 36 is in the region likely to be done to death. Our notes from a year ago say that the Spitzer data for BRC 38 are done, but I can't find the paper. We could start again from the entire BRC list and sort again? See figure below for context. The big square is someone else's (published) thesis data. The big blobby thing next to BRC 36 is [http://www.spitzer.caltech.edu/images/1058-ssc2003-06b-Dark-Globule-in-IC-1396 this], also done to death. We are also monitoring this region for changes in the stars. But BRC 38 may be a good one, or the larger context around BRC 34 or 38 (with WISE) would also work.
[[image:tr37where.png]]
* Other LDN options:
**Babar, who you have not yet met, has also suggested the following. He has Spitzer data on a few Lynds dark clouds. LDN 65 is in the WISE public release but is likely a sterile (no YSOs) cloud. The other two LDN 877 and LDN 885 do not have WISE data released yet but they are likely more promising. I've seen some of his Spitzer data, and they do look promising.
**I had a NITARP team a previous year that had to find a Lynds cloud that was likely to harbor YSOs, not well-studied, and not yet observed with Spitzer. Not an easy proposition. [[Lynds Target Selection]] is from early that year when we were trying to settle on a target. That year, in the end, we picked LDN 425 and 981. I don't think we found any reasonable YSOs -- just AGN. The targets we rejected that year were LDN 951, LDN 1143, LDN 1598, and LDN 1685. See the [[Lynds Target Selection]] page, near the bottom, for summary and images.
**Summary of several LDN choices, then:
***LDN 65 - Babar has Spitzer data, now available in WISE, unlikely to harbor YSOs.
***LDN 425 - 1 IRAS source, 1 known YSO here, picked for NITARP team before, spitzer data exist, now available in WISE, most likely no YSOs.
***LDN 877 - Babar has Spitzer data, not yet available in WISE, possible YSOs.
***LDN 881 - Babar has Spitzer data, not yet available in WISE, possible YSOs.
***LDN 951 - two submm starless cores here (rejected as prior target), no Spitzer data, not yet available in WISE, linear intriguing shape in POSS.
***LDN 981 - V1331 Cyg (famous object) at end of one of filaments; picked for NITARP team before, spitzer data exist, not yet available in WISE, probably no YSOs. But with WISE, can cover larger region than we did before, FWIW.
***LDN 1143 - 1 IRAS source, 1 known YSO here, 1 "very red object" (YSO?), sort of a checkmark shape in POSS (rejected as prior target), no Spitzer data, not yet available in WISE.
***LDN 1340 - considered as target before, dropped so as not to scoop someone who has since retired from astronomy without completing this project. Spitzer data here, WISE data available now and they look interesting, we could do both Spitzer+WISE data here. Would have to scrape literature to be sure we understand what has been done before -- simbad has 17 refs, so not ridiculous. image(s) on Lynds target selection page from that year, midway through the page.
***LDN 1598 - 19 refs in SIMBAD, part of Lambda Ori complex; also IRAS 05496+0812, also WB89 718, also HH 117 VLA 1 (so clearly several people have looked here before). no Spitzer data here (I don't think), WISE data available but tile clobbered by insanely bright star nearby. Nebulous. Unclear from image if this is a good plan or not.
***LDN 1685 - 10 references in SIMBAD, IRAS source, diaphanous in POSS, now available in WISE - fuzzy with some bright sources. Hm. possibly interesting, but also dispersed SF here.
***OR... start with the whole LDN list and sort again ....?

So, from where I sit, at the moment anyway, I think '''maybe''' following up the BRCs (WISE mostly, leveraging off Spitzer from last year's team), or LDN 1340 (we'd do Spitzer+WISE).

Additional contributions from the peanut gallery -
*berkeley 59 interesting cluster, also has footprint from same GTO program "BRC 3"
*NGC 281 interesting cluster, also has Jeff Hester, Scott Wolk warm data, plus a single GTO pointing.

=Stuff resulting from 1/20/12 telecon=

So, we are trying to decide between LDN 1340 and following up on the work from last year's NITARP team, BRC 27+34, with an option to include another BRC if we blow through them fast.

Table of properties.

{| border="1"
|'''property'''
|'''BRC 27/34 (+other?)'''
|'''LDN 1340'''
|-
|which kind of data would we use?
| WISE data around the Spitzer footprint covered by the other team. The WISE data will be newly released. If we choose to do an additional BRC, we'd get into the Spitzer data there too. We'd combine with 2MASS and AKARI and anything else we can find.
| Spitzer data, probably - it already exists (taken in 2009, more recent than I recalled), and hasn't been published yet. We'd combine with 2MASS and AKARI and anything else we can find.
|-
|Who 'owns' the existing data?
|BRC small footprints are originally Lori Allen's and Rob Gutermuth's, but they are looking at the ensemble of BRCs for their statistical properties, not particularly caring about individual objects. Data are old enough that they are now public. No one 'owns' the WISE data.
|LDN 1340's IRAC data were originally JoAnn O'Linger's. Have sent email inquiry. Data are now public; have been for some time, so technically no one 'owns' it now.
|-
|What are we looking for, and how?
|We are using infrared excess to look for new young stars, and describing the properties of the already-identified young stars, in these regions. I know they're there, because last year's group found them (both kinds).
|We are using infrared excess to look for new young stars, and describing the properties of the already-identified young stars, in this region. We are pretty sure that previously known ones are here. It is likely new ones are too, but I am less absolutely certain we will find them.
|-
|Implications for publishing?
|We could either combine with the results from the gang that just finished, or make our own paper. I don't know which would be better. This is an extension of their work, though, so it would make sense to combine it. There are also reasons (as Mark mentioned) for publishing sooner, to say nothing of my own instincts to "do it to completion" before publishing (which has tripped me up before).
|We will probably have a publishable paper.
|-
|how big is the region?
|The original BRC footprints are ~5 arcmin on a side. We'd go probably ~10 more arcminutes out, radially.
|The LDN IRAC map is ~0.7 deg on a side.
|-
|Difficulty of data reduction/manipulation? images
|images are small, and should easily load into your windows machines. not a lot of very bright stars.
|image is BIG and might give you trouble if you don't have enough RAM. some very bright stars, could make reduction tricky.
|-
|Difficulty of data reduction? photometry
|We'd use the WISE catalogs, but do lots of sanity checks to be sure that these automatically-produced things are telling us sensible things. If we picked a new BRC to continue, I'd make you do a bunch of Spitzer photometry, but I'd still do the lion's share because I can automate it.
|I'd make you do a WHOLE TON of Spitzer photometry, but I'd still do the lion's share because I can automate it.
|-
|Possibility of ground-based followup?
|BRC 27 is at -11 deg declination, BRC 34 is at +58. Both already have Haleakala data 'in the can'; we could get more to go out further. Other BRCs we could pick from would also be accessible from LCOGT since they have N and S telescopes.
|LDN 1340 is at +72. We'd have to go get the Haleakala data, and it's kind of a big region.
|-
|Timing of ground-based followup?
|''babar to fill in''
|''babar to fill in''
|-
|Original discovery papers?
|BRCs: Sugitani K., Fukui Y., Ogura K., [http://adsabs.harvard.edu/abs/1991ApJS...77...59S 1991, ApJS, 77, 59.] Nice approach of combining two large surveys -- POSS and IRAS; nice clear discussion of weed-down process. Second half of paper (detailed analysis of IRAS colors, etc.) obsolete but has same essence as what we do now. (paper should be free from journal)
|LDN: Lynds, B., [http://adsabs.harvard.edu/abs/1962ApJS....7....1L 1962, ApJS, 7, 1] In the 1960s, Beverly Lynds studied the Palomar Observatory Sky Survey (POSS) plates and made a list of things she thought were bright or dark nebulae. These of course were subjective judgements, but they are often pretty, and often forming stars. (paper should be free from journal)
|-
|Lit search?
|BRC team last year did BRC 27, 34. final list of papers is [[BRC Spring work |here]] -- note that that was in the order we discussed them, not chronological order of publishing. Punchline: 1 previous study in BRC 34, several in BRC 27; BRC team did most of coordinate sorting in BRC 27, and you will still have to do some, because they quit outside of the IRAC footprint.
|LDN 1340 - i have not worked here before. Simbad has 17 references. need to comb through them, find out what is known.
|-
|'teachable moment' potential?
|we will spend a LOT of time staring at WISE images. in this case, we have a little Spitzer data over part of the region. We will be able to instantly and vividly compare the relative spatial resolutions of these images, and be able to talk about why these missions were designed this way, and their strengths and weaknesses
|we would have to deliberately go find the WISE images for this one for the same effect. it's there, but you won't be as enmeshed in the process, because you won't be relying on the WISE data for anything.
|-
|images
|see [http://coolcosmos.ipac.caltech.edu/cosmic_classroom/teacher_research/r5-brc/poster_johnson.pdf our poster] or [[http://coolwiki.ipac.caltech.edu/images/a/a6/Brc27wise.png |this wise close-up of brc27]] and [[http://coolwiki.ipac.caltech.edu/images/2/21/Brc27wiselarge.png |this large field view]]. (small blue box is BRC 27 in both cases -- large field view is more than we would do.)
|to come.
|-
|what, physically, is going on?
|OBA stars nearby, pushing gas and dust around, likely prompting star formation in the comet-shaped dark globules
|not sure, i gotta read the literature! JD, Babar, if you get there first....
|}

ACTION ITEMS for next week: start a lit search for both these regions. see if you can add to the pros/cons list above. look at the objects as they appear in other bands (e.g., POSS from [http://skyview.gsfc.nasa.gov/cgi-bin/skvadvanced.pl Skyview]). Post a summary of what you find below ("Stuff in prep for 1/27 telecon"). Add your signature if the context seems appropriate, so we know who said what and when!

=Stuff in prep for 1/27/12 telecon=

Below is an attachment for a paper on BRC SFO 38. Page 25 has spectral energy distributions in MIR11, 29, 31, 34, 36, 38, 45, 48, 50, 54, 55, 59, 82, 86. (I'm guessing this stands for Mid-infrared and the number stands for microns--please edit mercilessly here!)

[[File:BRC SFO 38.PDF]]

The coordinates for BRC 38 are 24h39m10.3s +58:02:29. The SkyView image doesn't look very exciting, but the images in the above paper are pretty snazzy.

--[[User:French|French]] 07:43, 23 January 2012 (PST)

File:BRC SFO 38.PDF

2012-01-23T15:41:15Z

French: