CoolWiki - User contributions [en]

File:SED PLOT EXAMPLE.XLSX

2011-07-08T22:21:00Z

Legassie:

Working with the BRCs

2011-07-08T22:20:23Z

Legassie: /* Making SEDs */

''This page is an updated version of the [[Working with L1688]] and [[Working with CG4+SA101]] pages, and was developed and updated specifically for the 2011 BRC team visit. Please note: NONE of these pages are meant to be used without applying your brain! They are NOT cookbooks!''

FOR REFERENCE: [[BRC Bigger Picture and Goals]]

=Downloading the data =

[[How do I download data from Spitzer?]] has a wide variety of flavors of tutorials. The [http://irsa.ipac.caltech.edu/data/SPITZER/docs/dataanalysistools/cookbook/6/#_Toc288477466 second formal chapter] of the professional astronomer's Data Reduction Cookbook ultimately comes from last year's NITARP project. I haven't developed one customized to your project, because this year it's easier.

'''Big picture goal''': Get you comfortable enough to search for your own favorite target, understand what to do with the search results, and download data.

'''More specific shorter term goals''': Search on our targets. Understand the difference between the observations. Understand why I chose to use the observations that I did.

'''Relevant links''': [[How do I download data from Spitzer?]] and [http://sha.ipac.caltech.edu/applications/Spitzer/SHA SHA]

'''Questions for you''':
#Compare the various AORs you get as your search results when you search by position. How are they the same/different? Which do we want to download?

=Making the mosaics =

In the generic case for most targets, you can probably use the online mosaics that come as PBCD (Level 2) mosaics (or delivered products, if they exist for the region you want -- see "inventory search" in the SHA). In this case, we can use the online mosaics.

'''Big picture goal''': Recognize at a glance what is an instrumental artifact and what is real.

'''More specific shorter term goals''': Look at the online mosaics. Understand what is part of the sky and what is not. Understand which I reprocessed and why.

'''Relevant links''': [[What is a mosaic and why should I care?]] and [[Resolution]]. Why does it matter to know what is an artifact and what is not? [http://www.universetoday.com/86497/proof-bio-station-alpha-is-just-an-image-artifact/ So you don't get fooled by stuff like this.]

'''Questions for you''':
#Compare the mosaics across the bands. What changes? What stays the same? Why?
#What is saturated? What are some other instrumental effects you can see?
#Notice the pixel scale. What is the real pixel scale of IRAC (and MIPS)? What are the pixel scales of the images? Does that actually change the resolution? (for advanced folks - why did we do this?)

=Getting data from other wavelengths =

You have already made some progress on this in your literature search this Spring, but there are a TON more data we can mine.

'''Big picture goal''': Understand how to use the various archives to find non-Spitzer data.

'''More specific shorter term goals''': Go get data for both BRCs for comparison to our Spitzer data, both images and catalogs. Specifically investigate the WISE archive.

'''Relevant links''': [[How can I get data from other wavelengths to compare with infrared data from Spitzer?]] and [[Resolution]] Also: [http://irsa.ipac.caltech.edu/applications/wise/ Access the WISE archive directly here], and [http://wise.ssl.berkeley.edu/wise_image_service.html see a step-by-step WISE archive tutorial from Berkeley here].

'''Questions for you''':
#Figure out how to get data from Akari, WISE, 2MASS, MSX, IRAS, IPHAS, POSS, SDSS (NB: both clouds may not have hits, and some surveys might not cover both -- or either -- clouds), and anyplace else you want. Which will give you images, and which will give you catalogs (not all will give you both)? Go do it. For images, if you are using Skyview from Goddard, make sure to worry about pixel scale. Best to try to go direct to the source for these archives, rather than relying on Goddard. Get images covering about the same area as the Spitzer images so that they are easy to compare, but larger scale images might be useful to give a sense of context too.
#For each catalog: What wavelength is this? How is it relevant to YSOs? How is the resolution different? (You may need to do the next section before you can answer this.)

[[Luisa's BRC task notes]] (e.g., some notes on the answers I am expecting you to get! don't peek until you've tried; you might find different information than I did!)

=Investigating the mosaics=

It is "real astronomy" to spend a lot of time staring at the mosaics and understanding what you are looking at. Don't dismiss this step as not "real astronomy" just because you are not making quantitative measurements. This is time well-spent.

'''Big picture goal''': Understand what is seen at each Spitzer band and all the other archival bands.

'''More specific shorter term goals''': Recognize how the images differ between the two BRCs, and among the various bands.

'''Relevant links''': [[How can I make a color composite image using Spitzer and/or other data?]] and the questions on that page.

'''Questions for you, among just the Spitzer images''':
#How does the number of stars differ across the bands? Which band has the most stars? The fewest? (Bonus question: why?) The most nebulosity? The least? (Bonus question: why?) Are there more stars in the regions of nebulosity, or less? Why?
#What other features are the same across the bands?
#Do the star counts differ between the two BRCs? Why?
#Which objects are saturated, in which bands?
#How big are any of the features in the image (nebulosity, galaxy, space between objects)? (What do I mean by big?) in pixels, arcseconds, parsecs, and/or light years? (Hint: you need to know how far away the thing is. If it helps, there are 3.26 light years in a parsec.)
#Make a three-color image. What happens when you include a MIPS-24 mosaic in as one of the three colors with IRAC as the other two? Do the stars match up? Does the resolution matter? Can you tell from just a glance at the three-color mosaic which stars are bright at MIPS wavelengths?

'''Questions for you, among all bands you can find''':
#Figure out how to get imaging data from WISE, 2MASS, MSX, IRAS, POSS, and anyplace else you want. (See prior task too.) Line them up with the Spitzer images of comparable wavelengths (e.g., 8 um with 12 um, 25 um with 24 um). How much more detail do you see with Spitzer that was missed by IRAS or the other missions? Do you see more texture in the nebulosity? More point sources? How does the resolution and sensitivity vary?
#Which features are found across multiple wavelengths? Why?

=Previously identified sources=

You've already started to do this as part of our proposal and spring work.

'''Big picture goal''': Understand what has already been studied and what hasn't in the image.

'''More specific shorter term goals''': Determine if the previously-known objects are saturated or not. Get some numbers so that you are ready to do photometry on them (in the next step).

'''Relevant links''': [[How can I find out what scientists already know about a particular astronomy topic or object?]] and [[I'm ready to go on to the "Advanced" Literature Searching section]] and [[BRC Spring work]] (bottom of that page), specifically [[file:luisa-mergedbrc27.txt]]. luisa's region file of these objects (for use with ds9 -- NOTE THAT windoze computers will misinterpret the .reg file extension, so i've changed it to reg.txt!): [[file:luisa-mergedbrc27.reg.txt]]

BRC 27 known objects with X and Y position coordinates ... [[file:xyLuisa-mergedbrc27.xls]] --[[User:CJohnson|CJohnson]] 22:54, 6 July 2011 (PDT)

'''NEW (4/2011) resource''': [http://www.youtube.com/watch?v=fR58i8zvMwQ YouTube video] on how to take antiquated coordinates from one of our literature papers and use 2MASS to get updated current, correct coordinates for each object.

'''Questions for you''':
#For each of the known objects, you have the RA/Dec - find the objects in the image. What are the pixel coordinates in the image? Does it change among the IRAC bands? In the MIPS band?
#For each of the known objects, you have the RA/Dec - find the objects in the catalog. Which Spitzer catalog objects are the matches?

[[Luisa's BRC task notes]] (e.g., some notes on the answers I am expecting you to get! don't peek until you've tried; you might find different information than I did!)

<font color="red">'''BIG PENDING ISSUE FOR HOMEWORK(?)'''</font>: are the duplicates you found REALLY duplicates on the sky? The computer said some were duplicates, and some ended up at the same position (apparently) but with different data. What is it really, on the sky? How are you going to tell if there are really sources there? (Hint: go get 2mass images of these regions and make REALLY sure there is really only one source there, or there are really two.)

=Doing photometry =

OK, this step is doing to take the longest, be the most complex, involve the most steps and the most math.

Never just trust that the computer has done it right. It probably did what you asked it to do correctly, but you asked it to do the wrong thing. '''Always''' make some plots to test and see if the photometry seems correct.

'''Big picture goal''': Understand what photometry is, and what the steps are to accomplish it. Understand the units of Spitzer images. Understand how to assess if your photometry makes sense.

'''More specific shorter term goals''': Do photometry on a set of mosaics for the same (small) set of sources. Assess whether your photometry seems right. We should decide as a group which set of sources to measure, and have everyone measure the same sources. We will then compare all of our measurements among the whole group.

'''Relevant links''': [[Units]] and [[Photometry]] and [[I'm ready to go on to a more advanced discussion of photometry]] and [[Aperture photometry using APT]], specifically [[Aperture_photometry_using_APT#Looking_for_a_cookbook.3F|this]], which is the closest thing to a cookbook I will give you.

'''NEW (5/2011) resource:''' [http://www.youtube.com/watch?v=_w_5DgB0vKw YouTube video on using APT], including calculating the number APT needs. (15 min because it starts from software installation and goes through doing photometry.)

<font color="red">'''NEW 7/7/11'''</font> -- region files for just i1, just i2, just i3, just i4, and 'final best catalog of everything with a valid detection somewhere':
*[[file:justirac1sources.reg.txt]]
*[[file:justirac2sources.reg.txt]]
*[[file:justirac3sources.reg.txt]]
*[[file:justirac4sources.reg.txt]]
*[[file:allbandmergedsources.reg.txt]]
AND, [[file:fred.xls]], the file in which we were collecting everyone's measurements.

'''Questions for you''':
#Use APT to explore the various parameters. What is a curve of growth?
#What are the best parameters to use? (RTFM to find what the instrument teams recommend.) What are the implications of those choices? What happens if you use other choices?
#Compare the MOPEX source identifications I did from just one band with their corresponding image. Is it getting fooled by detector artifacts? ''you have the tbl files, as opposed to region files, from me for this. you can use SHA to load tbl files over images, or another standalone software package called skyview. Let me know if you want the reg files and I'll make you some.''
#Compare the MOPEX source identifications from, say, IRAC band 3 with the image from IRAC band 1, or the source extractions from MIPS-24 with image from IRAC band 1. Are there a lot of stars (or other objects) in common? How does the nebulosity affect it? ''you have the tbl files, as opposed to region files, from me for this. you can use SHA to load tbl files over images, or another standalone software package called skyview. Let me know if you want the reg files and I'll make you some.''
#Why did either of these things happen when I ran automatic source detection in MOPEX? (see below)

[[image:cg424.png]]

[[image:brc34i3.png]]

=Bandmerging the photometry =

I use my own code to do this; there is no pre-existing package to do this. If you do it by hand (or semi-by-hand) using APT, you can manually merge the photometry. My merged photometry includes J through M24.

'''Big picture goal''': Understand what this process is.

'''More specific shorter term goals''': Do this by hand.

'''Relevant links''': [[Resolution]]

'''Questions for you''':
#Make sure that I've merged the right sources across several bands by spotchecking a few of them. (Find an object that the catalog says is detected in at least 3 bands and then overlay the images in a 3-color image or Spot to see if there is really a source there, at exactly that spot, in all bands, or if it's a cluster of objects, or different objects getting bright at different bands.
#Have I 'lost' the instrumental artifacts you noticed in the previous section? Or are there instrumental artifacts or otherwise false sources sill in the list?
#Does resolution matter? (Can you find a place where more than one IRAC source can be matched to the same MIPS source?)
#Can you start merging in information from other bands (see tasks above)? Be very careful about resolution!!

=Working with the data tables =

OK, fair warning, math involved here too. And programming spreadsheets!

'''Big picture goal''': Understand how to work with the tables. Understand how to convert magnitudes back and forth to flux densities.

'''More specific shorter term goals''': Import the table into excel. Program a spreadsheet to convert between mags and flux densities.

'''Relevant links''': [[Units]] and [http://www.ipac.caltech.edu/Skyview/ Skyview] but lots of important words actually on the [http://coolwiki.ipac.caltech.edu/index.php/Working_with_L1688#Working_with_the_data_tables L1688 page itself], sorry. See also [[Central wavelengths and zero points]].

'''NEW (5/2011)''' resource for understanding how to do this: [http://www.youtube.com/watch?v=nCJ3ctOGvNk YouTube video] on what tbl files are, how to access them, and specifically how to import tbl files into xls. (10min)

Make sure you understand how I got the magnitudes from the fluxes (or the fluxes from the magnitudes). You will need magnitudes for the next step, and fluxes for the step after that.

'''Questions for you''':
#How many stars are detected in each band? Is this about what you expected based on your answer to the questions in the mosaic section above? HINT: you can do this using Excel, you don't need to count these manually!! Ask if you need a further hint on exactly how to do this.
#Which stars ''in the catalog'' are the stars identified in the literature?

=Making color-color and color-magnitude plots=

'''Big picture goal''': Understand what plots to make. Understand the basic idea of using them to pick out certain objects.

'''More specific shorter term goals''': Make some plots. Understand the basic approach of Gutermuth et al. (see [[media:gutermuth-appa.pdf| Gutermuth et al. 2009, Appendix A]])

'''Relevant links''': [[Color-Magnitude and Color-Color plots]] and [[Finding cluster members]] and [[Color-color plot ideas]] and [[Gutermuth color selection]]

'''Questions for you''':
#Pick a diagnostic color-color or color-magnitude plot to make. Does my photometry seem ok?
#Pick at least one color-color or color-magnitude plot to make. Figure out a way to ignore the -9 (no data) flags. Where are the plain stars? Where are the IR excess objects?
#Where are the famous objects in the plot? Where are the new YSO candidates I used the Gutermuth method to find?
#Make a new column in your Excel spreadsheet with some colors. Is there a way you can get Excel to tell you automatically which objects have an IR excess? Can you implement the Gutermuth selection? (You may not be able to do so.)
#Make the plots that go into the Gutermuth selection, including the relevant lines on the plot.
#Of the objects I have that fit the Gutermuth criteria, are any of them false or otherwise bad sources? How can you tell?
#Bonus but very important question: How do you know that some of these sources aren't galaxies? Can you find something that is obviously a galaxy on the images? Can you think of a way using public data that already exist to check on the "galaxy-ness" of some of these objects?

'''NEW 7/8/11''': [[file:fridayafternoon.pdf]] -- pdf of ppt from friday afternoon 7/8/11

=Investigating the images of the objects=

'''Big picture goal''': Understand why we need to look at the images of each of our short list of candidates.

'''More specific shorter term goals''': Figure out how to get thumbnails and/or find these things in our images. Calibrate your eyeball for the various images/resolutions/telescopes to figure out what is extended and what isn't. Drop the bad objects off our candidate YSO list.

'''Relevant links''': [[How can I get data from other wavelengths to compare with infrared data from Spitzer?]] and [[Resolution]] (specifically some of the concrete examples there) and [http://irsa.ipac.caltech.edu/applications/FinderChart/ IRSA finder chart]

'''NEW (5/2011)''' resource for understanding how to do use finder chart to examine the images of various candidates in bands other than Spitzer: [http://www.youtube.com/watch?v=4RHS497XeHQ YouTube video on using Finder Chart]. To use these images to also examine the original Spitzer images, load them (and the Spitzer images) into ds9, pick one of the small finder chart images, and then pick 'Frame/Match/Frame/WCS'. All will snap to alignment with North up, on the same scale, with the object in the center.

'''Questions for you''':
#Which objects are still point sources at all available bands?
#Which are instrumental artifacts? Or MOPEX hiccups?
#Which might have corrupted photometry?
#Which are correctly matched to literature values (or correctly identified as duplicates)? You'll need to go back to the literature above to check this.

=Making SEDs =

WARNING: lots of math and programming spreadsheets here too.. you WILL do this more than once to get the units right!

'''Big picture goal''': Understand what an SED is and why it matters.

'''More specific shorter term goals''': Make at least one SED yourself. Examine the SEDs for all of our candidate objects. Use them to reassess our photometry if necessary, and to drop the bad objects off the YSO candidate list.

'''Relevant links''': [[Units]] and [[SED plots]] and [[Studying Young Stars]] and for that matter the detailed object-by-object discussion in the appendix of the [http://lanl.arxiv.org/abs/1105.1180 cg4 paper]. See also [[Central wavelengths and zero points]]

Pick some objects to plot up, maybe some of the previously-identified ones from above would be a good place to start, or the ones you flagged above as having an IR excess. Start with just one. It will take time to get the units right, but once you do it right the first time, all the rest come along for free (if you're working in a spreadsheet). Spend some time looking at the SEDs. Look at their similarities and differences. Identify the bad ones, and discuss with the others why/whether to drop them off the list of YSO candidates. See also stuff above about data at other wavelengths, and include literature/archival data from other sources where appropriate and possible.

'''Questions for you''':
#What do the IR excesses look like in your plots? Do they look like you expected? Like objects in CG4 or elsewhere?
#Make some SEDs of things you know are ''not'' young stars. What do they look like?
#Which objects look like they have 1 or 2 bad photometry points? Go back and check the photometry for them.
#Which objects look like clear YSO SEDs? Which objects do not?
#Any photometry look bad? Go back and check it!
#Any objects within the maps but undetected? Go back and get limits and add those too!
--[[User:Legassie|Legassie]] 15:20, 8 July 2011 (PDT)
TIPS ON CREATING SED PLOTS USING EXCEL:
[[FILE:SED_PLOT_EXAMPLE.XLSX]]

=Literature again=

This step is important for this particular project, because of the nature of the existing literature for the objects we are studying.

'''Big picture goal''': Understand at least the basics of how what we did is different than what Chauhan et al. did with the IRAC data.

'''More specific shorter term goals''': Knowing what you do now, go back and reread Chauhan et al. Do a detailed comparison of our method for finding young stars and that from Chauhan et al.

'''Relevant links''': [[How can I find out what scientists already know about a particular astronomy topic or object?]] and [[I'm ready to go on to the "Advanced" Literature Searching section]] and [[BRC Spring work]].

'''Questions for you''':
#What are the steps (cookbook-style) that Chauhan et al. used to find YSOs?
#What were our steps?
#How are they different?
#Does our IRAC photometry agree ''within errors''? (That "within errors" is very important...)
#Did we find the same specific sources as they did? Did we find more or fewer? or exactly the same? Did we recover all of theirs? Why or why not?
#Which method do you think works better?
#'''NON-CHAUHAN:''' Did we recover all of the young stars identified by Ogura or Gregorio-Hetem or any of the other papers? Why or why not?
#'''NON-CHAUHAN:''' Are any of our surviving YSO candidates listed in SIMBAD for any reason? Are they still likely YSOs, or have they shown up as galaxies there?

=Analyzing SEDs=

'''This is advanced, and we may not get here.'''

Add a new column in Excel to calculate the slope between 2 and 8 microns in the log (lambda*F(lambda)) vs log (lambda) parameter space. This task only makes sense for those objects with both K band and IRAC-4 detections. (For very advanced folks: ''fit'' the slope to all available points between K and IRAC-4 or MIPS-24. How does this change the classifications?)
*if the slope > 0.3 then the class = I
*if the slope < 0.3 and the slope > -0.3 then the class = 'flat'
*if the slope < -0.3 and the slope > -1.6 then class = II
*if the slope < -1.6 then class = III
These classifications come from Wilking et al. (2001, ApJ, 551, 357); yes, they are the real definitions ([[Studying Young Stars|read more about the classes here]])!
#How many class I, flat, II and III objects do we have?
#Where are the objects with infrared excesses located on the images? Are all the Class Is in similar sorts of locations, but different from the Class IIIs?

For very advanced folks: [http://cfa-www.harvard.edu/youngstars/dalessio/ suite of online models from D'Alessio et al.] and [http://caravan.astro.wisc.edu/protostars/ suite of online models from Robitaille et al.]. Compare these to the SEDs we have observed.

=Writing it up!=

We need to write an AAS abstract and then the poster, and if we're lucky, a paper!

We need to include:
#How the data were taken.
#How the data were reduced.
#What the Spitzer properties are of the famous objects, including how the Spitzer observations confirm/refute/resolve/fit in context with other observations from the literature.
#What the Spitzer properties are of other sources here, including objects you think are new YSOs (or objects you think are not), and why you think that.
#How this region compares to other regions observed with Spitzer.

Take inspiration for other things to include from other Spitzer papers on star-forming regions in the literature.

Windows hints, tips, and tricks

2011-07-07T18:00:48Z

Legassie:

= Unzipping files =

You need to unzip the files that the SHA puts on your disk. You should be able to simply double-click on the zip file to make it work. You might need to install a program such as [http://www.winzip.com/ Winzip].

On a Windows XP it turns out not to be so easy. There is an embedded/native unzip program built into Windows XP. To use from Windows explorer you click and highlight a single zip file that you would like to unzip. Then from the File menu click on Extract All and the Extraction Wizard will lead you through the steps and extract your file. You will need to select the folder to extract to (same as the folder name is what I picked).

But this method does not seem to work with unzipping many files at one time.

To unzip a large group of zipped files I believe the only way is to download a program like winzip pro

I used download.com to get the trial version of Winzip 11.1. After downloading and installing the program then you can unzip many files at one time.

1. In Windows explorer click on the folder that has all of the zip folders. In the right hand window should be a list of all of the zip folders. Click on the first folder in the list holding down Shift click on the last folder. This will highlight all of the files.

2. Go the file menu and then to Winzip and to Extract to here.

After some time you will find all of the unzipped files in folders just like when you unzip the files on any other platform.

=MOPEX=

We are assuming most MOPEX users are on a unix-based (unix, linux, mac) machine, which is recommended not just for the tricks and things listed in the other pages (such as [[Make a simple mosaic]]), but also for speed and reliability. Several of the items below will help with running MOPEX on windows.

'''IF YOU RUN INTO PROBLEMS''' running MOPEX on windows that are not listed here, please check the [http://ssc.spitzer.caltech.edu/postbcd/bug-mopex.html bugs list for MOPEX] and try the solutions listed there. If you have a more ... interesting bug, please mail detailed information (windows version, amount of memory, speed of processor, version of MOPEX, AORKEY you were working on, and detailed error message information) to the SSC helpdesk at help@spitzer.caltech.edu. You want to give them enough information to reproduce your error exactly. If they can't reproduce it, they can't solve it.

=cygwin dll collision=

as of June 14, 2008, we had an error where mopex was complaining about a cygwin dll collision, telling us we needed a more recent version than we have, except that we had JUST downloaded and installed it.

Here are some steps you can try:
#Locate the following directory: C:\Program Files\mopex\platform\windows\bin
#Copy the "cygwin1.dll" into the directory above (C:\Program Files\mopex\platform\windows\bin)

The method will work on a Win XP PC if MOPEX was requesting a newer
cynwin1.dll. However, I cannot reproduce the same "cygwin dll
collision" problem on a Vista machine.

This bug may be fixed in a future version of MOPEX.

= Getting file lists =

MOPEX in particular needs as input lists of files. I have lots of tricks I use to get file lists, but most of my tricks use tools available for unix-based systems, such as redirects, grep, sed, and awk. To make those tools work on windows systems, you should download and install the Cygwin package (http://www.cygwin.com). This would give you a UNIX-like terminal window, from which to execute unix commands like
% ls -1c > list.txt
Installation is fairly straightforward.

Alternatively, to get a file list, you could just
$ dir *fits
and then copy and paste into WordPad. Of course, this isn't as powerful.

=APT=

Again, APT runs much more easily on a Mac, but it does run on Windows too. We have found two different ways to install APT. Option one is to download and install the Cygwin package (http://www.cygwin.com) and then follow the directions on the APT page.

Option two follows:

Go to a command prompt in Windows XP. To do this click on Start > All Programs > Accessories > Command Prompt

This should bring up a text window with the following or similar prompt:

C:\Documents and Settings\Username>

Then type:

C:\Documents and Settings\Username>java -version

You should see a response like

java version "1.6.xxxx"
Java(TM) SE Runtime Environment (build 1.6.xxxx)
Java HotSpot(TM) Client VM (build 1.6.xxxxx, mixed mode)

If your java version is less than 1.6, you must first download
and install the JDK from www.sun.com.

Now pick a directory and install the APT program. You will need to
"untar" it since it comes in "tar" format which is a way to combine
multiple directories (it comes from the days of data tapes and stands
for "tape archive.")

If your machine does not recognize that format, go to the following
site and install this free tar program: http://www.7-zip.org/

Click on the first download .exe file and then install it.

Once installed, you should run it on the APT tar file and get a
directory named APT_windows_vXXX with a subdirectory of APT_vXXX (whatever the current version is).

Then you need to ensure that the environment contains JAVA in the path. In the Control Panel, select System->Advanced System Settings->Environment Variables...
Under System Variables, select Path and click on Edit. In the Variable field, if path doesn't include java than append at the end the location of Java (usually in Program Files/Java/bin)..

Now you need to go back to the command prompt. In it go to the
directory APT_vXXXX (whatever the current version is), OR double-click APT.bat from File Manager

So if you have installed it in the "Program Files" directory type
the following:

C:\Documents and Settings\Username> cd \Program Files\APT_windows_vXXX\APT_vXXX

Then you should see this prompt:

C:\Program Files\APT_windows_vXXX\APT_vXXX>

Then type:

C:\Program Files\APT_windows_v0.98\APT_vXXX> java APT

This should start the program.

=[[Unix cheatsheet]]=
A list of common commands that can be used via Cygwin (see above).

BRC Proposal

2011-05-18T22:04:54Z

Legassie: /* Background on Star Formation */

=Instructions=

[[2011 proposal instructions]]

=Proposal Versions=

FINAL VERSION (some tweaks from Luisa with respect to first version below): [[file: BRC_prop3_final.doc]] --[[User:Rebull|Rebull]] 09:29, 21 March 2011 (PDT)

Third version (includes Luisa's comments, telecon tidbits, abstract): [[File: BRC_prop3.doc]]
--[[User:CJohnson|CJohnson]] 14:42, 18 March 2011 (PDT)

Luisa's hack up of version 2 (i missed version 2a, sorry): [[File: BRC_prop2_lmr.doc]] --[[User:Rebull|Rebull]] 13:46, 16 March 2011 (PDT)

Second attempt (slightly altered with Diane's changes) [[File: BRC_prop2a.doc]]
--[[User:CJohnson|CJohnson]] 11:51, 16 March 2011 (PDT)

Second attempt [[File:BRC_prop2.doc]]
--[[User:CJohnson|CJohnson]] 12:21, 15 March 2011 (PDT)

First attempt [[File:BRC_prop1.doc]]
--[[User:CJohnson|CJohnson]] 13:05, 9 March 2011 (PST)

=Background on Star Formation=

STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.

[http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]

Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]

A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]
--[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)

Powerpoint presentation giving at GISS 2011 summarizing the NITARP 2010 paper "New Young Star Candidates in CG4 and Sa101", Rebull et all, 2011 [[File:GISS_2011_Legassie_gum_nebula.pptx]] --[[User:Legassie|Legassie]] 15:04, 18 May 2011 (PDT)

=Target Selection=

STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.

The list of sources that Lori suggests we consider are here:
*[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE
*[[target selection for brc36]] 21h35m32.6s +57d31m50s
*[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula
*[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]

*[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE

Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about <s>30'</s> 10' of these positions.

Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]

CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like "we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated."

papers from discussion on the phone 16:35, 23 February 2011 (PST)
*[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with "sfo 38" http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M
*[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M

----

=STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=

''Can I delete all this ... now that our proposal has been submitted??''
--[[User:CJohnson|CJohnson]] 09:42, 23 March 2011 (PDT)

=Introduction/Background=

the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)

http://journals.cambridge.org/action/displayAbstract?fromPage=online&aid=1655856
Proceedings of the International Astronomical Union (2007), 3: 164-165
DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008
Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda
--[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)

A&A 388, 172-178 (2002)
DOI: 10.1051/0004-6361:20020451
The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1
J. B. Soares and E. Bica
Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)

A&A 426, 535-545 (2004)
DOI: 10.1051/0004-6361:20040226
A radio and mid-infrared survey of northern bright-rimmed clouds
L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao

Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK
--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)

DOES ANYBODY HAVE ACCESS TO Ogura's 2010 "Triggered Star Formation associated with HII Regions" ADS says the full paper is not available.
--[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)

'''Science Background and Context: Star Formation'''

Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of vigorous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds, or more). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages theoretical models predict that these protostars must be very luminous and look like cool red stars, however we have no method of observing them in visible wavelengths. The dust cocoon absorbs most of the visible radiation surrounding the protostar and the nebula itself obscures the protostar from our view. The energy from the protostar warms the dust, which then re-radiates the energy from the protostar as infrared radiation. Thus, protostars are detectable within their nebula at infrared wavelengths. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.

Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenesa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d < 1.2 kpc, finding young stellar objects in 75% of the clouds they studied.

Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead, or in addition to, the targets discussed here if the analysis goes faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths.

--[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)

BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)

BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui & Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura & Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)

BRC 34: Marcella
(This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).

Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).

Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).

Identifier Dist(asec) RA DEC

IRAS 21319+5755 268.14 21 33 25.0 +58 08 26

IRAS 21316+5751 283.31 21 33 10.2 +58 04 43

IRAS 21320+5752 373.69 21 33 33.4 +58 05 56

IRAS 21314+5802 429.35 21 32 55.5 +58 15 51

IRAS 21320+5752 436.65 21 32.5 +58 02

IRAS 21323+5800 578.04 21 33 52.0 +58 14 04

Previously identified stars within 10 arcminutes are listed below (SIMBAD).

Identifier Class Dist (asec) RA DEC

TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42

HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234

GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6

BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840

Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7

Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8

Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.

Identifier Dist (asec) RA DEC

1 2MASS
J21332921+5802508 463.43 21 33 29.21 +58 02 50.9

2 21 33 55.8 +58 01 18

Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.
Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation.
Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution.
Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.

... drop what you have here ...

=Analysis Plan=
--[[User:Legassie|Legassie]] 20:12, 8 March 2011 (PST)

Spitzer archival data from IRAC and MIPS will be the main focus of our research, augmented with data from 2MASS and MSX. Data for BRC27 will originate from Spitzer program 30050 (reqkeys 17512192 and 17512448) while BRC34 data will originate from program 202 (reqkeys 6031616 and 6031872). See Figure 1 for visualization of BRC27 data using the Spitzer Planning and Observation Tool (Spot). Reference Figure 2 for visualization of BRC34 data.

''Figure 1: Spot visualization of BRC27 IRAC and MIPS data on a 25-micron view of the area. IRAC data is displayed in the blue and purple regions, while MIPS is shown in tan.''

[[File:brc27_final.jpg]]

''Figure 2: Spot visualization of BRC34 IRAC and MIPS data on a 25-micron view of the area. IRAC data is displayed in the blue and purple regions, while MIPS is shown in tan.''

[[File:brc34_final.jpg]]

Our plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010), as well as look for new YSOs. To accomplish this, a well-known property of YSOs will be exploited -- namely, large near- and mid-infrared emissions from material surrounding young stars. Looking for excess emissions will be the main focus of the research, and Spitzer is excellent at detecting these emissions as well as any bipolar outflows. Using the combined data, we will generate and analyze various plots, including spectral energy distributions (SEDs) , color-magnitude diagrams, and color-color diagrams to search for stars with infrared excesses.

We will generate mosaics of the BRC objects using MOPEX-Mosaics from Photometry data (Makovoz & Marleau 2005). For data reduction, the Aperture Photometry Tool (APT) will assist us in obtaining photometry values. These tools will allow our team to conduct flux analyses as well as spatial analyses and detailed visual observations. The resultant data will be analyzed further using a spreadsheet program (MS Excel). Excel will allow students to generate color diagrams and SEDs with the data to test infrared wavelenght theories of identifying and classifying young stellar objects.

=Education and Outreach=
Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.

A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.

Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing.

''Team Spitzer at Breck School''
Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly "brown-bag discussions." Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.

Marcella:
Students at Carmel Catholic High School will participate in the Spitzer research program as an extracurricular activity. Students will meet once a week for two to four hours or as needed. Students will read a variety of resources and participate in activities to learn about the history of astronomy and stellar evolution. Students will become proficient in a variety of image processing software programs. Students will share their research findings at local outreach events at the middle school, high school, and community levels.

John:
Glencoe Astronomy at Glencoe High School. Glencoe High School students ranging from sophomores to seniors will work together on this BRC project. There are currently seven students starting this project and additional students are anticipated. Students will be given weekly readings that will be discussed during our meetings each Thursday morning. We will begin with the basic principles of stellar evolution with an emphasis on star formation. Resources will include tutorials posted on the CoolWiki website and scientific articles relevant to the BRC project. Students will work together in teams during the data analysis and continue to meet to discuss their work.

Diane:
The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. Fortuitously, as one project winds down, another comes along to replace it. Even when we do not have an organized campaign, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and other local events. Currently, students are exploring web sites and reading articles in preparation for their Spitzer work and are anxious to get started!

--updated [[User:CJohnson|CJohnson]] 11:20, 15 March 2011 (PDT)

2011-03-09T05:54:07Z

Legassie:

BRC Proposal

2011-03-09T05:53:37Z

Legassie: /* Analysis Plan */

=Instructions=

[[2011 proposal instructions]]

=Background on Star Formation=

STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.

[http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]

Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]

A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]
--[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)

=Target Selection=

STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.

The list of sources that Lori suggests we consider are here:
*[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE
*[[target selection for brc36]] 21h35m32.6s +57d31m50s
*[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula
*[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]

*[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE

Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about <s>30'</s> 10' of these positions.

Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]

CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like "we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated."

papers from discussion on the phone 16:35, 23 February 2011 (PST)
*[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with "sfo 38" http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M
*[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M

----

=STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=

=Introduction/Background=

the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)

http://journals.cambridge.org/action/displayAbstract?fromPage=online&aid=1655856
Proceedings of the International Astronomical Union (2007), 3: 164-165
DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008
Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda
--[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)

A&A 388, 172-178 (2002)
DOI: 10.1051/0004-6361:20020451
The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1
J. B. Soares and E. Bica
Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)

A&A 426, 535-545 (2004)
DOI: 10.1051/0004-6361:20040226
A radio and mid-infrared survey of northern bright-rimmed clouds
L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao

Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK
--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)

DOES ANYBODY HAVE ACCESS TO Ogura's 2010 "Triggered Star Formation associated with HII Regions" ADS says the full paper is not available.
--[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)

'''Science Background and Context: Star Formation'''

Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of vigorous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds, or more). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages theoretical models predict that these protostars must be very luminous and look like cool red stars, however we have no method of observing them in visible wavelengths. The dust cocoon absorbs most of the visible radiation surrounding the protostar and the nebula itself obscures the protostar from our view. The energy from the protostar warms the dust, which then re-radiates the energy from the protostar as infrared radiation. Thus, protostars are detectable within their nebula at infrared wavelengths. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.

Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenesa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d < 1.2 kpc, finding young stellar objects in 75% of the clouds they studied.

Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead, or in addition to, the targets discussed here if the analysis goes faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths.

--[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)

BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)

BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui & Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura & Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)

BRC 34: Marcella
(This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).

Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).

Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).

Identifier Dist(asec) RA DEC

IRAS 21319+5755 268.14 21 33 25.0 +58 08 26

IRAS 21316+5751 283.31 21 33 10.2 +58 04 43

IRAS 21320+5752 373.69 21 33 33.4 +58 05 56

IRAS 21314+5802 429.35 21 32 55.5 +58 15 51

IRAS 21320+5752 436.65 21 32.5 +58 02

IRAS 21323+5800 578.04 21 33 52.0 +58 14 04

Previously identified stars within 10 arcminutes are listed below (SIMBAD).

Identifier Class Dist (asec) RA DEC

TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42

HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234

GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6

BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840

Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7

Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8

Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.

Identifier Dist (asec) RA DEC

1 2MASS
J21332921+5802508 463.43 21 33 29.21 +58 02 50.9

2 21 33 55.8 +58 01 18

Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.
Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation.
Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution.
Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.

... drop what you have here ...

=Analysis Plan=

--[[User:Legassie|Legassie]] 20:12, 8 March 2011 (PST)

Spitzer archival data from IRAC and MIPS will be the main focus of our research, augmented with data from 2MASS and MSX. BRC27 Spitzer data will originate from Program 30050 (Reqkeys 17512192 and 17512448) while BRC34 data will originate from Program 202 (Reqkeys 6031616 and 6031872).

[[File:brc27_final.jpg]]

[[File:brc34_final.jpg]]

'''Data Reduction'''

* Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)
* Mosaics will be created using MOPEX

'''Analysis Plan'''

* Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs
* Looking for infrared excess emission from material surrounding new stars will be the main focus of the research
* Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses
** Color-Color diagrams
** Color-Magnitude diagrams
** Spectral Energcy Distribution (SED) plots
* Analysis will also involve looking at actual optical and infrared images

'''Tools'''

* MOPEX - to create mosaics (Makovoz & Marleau 2005)
* Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010)
* MS Excel – to generate data diagrams (color-color, SEDs)

=Education and Outreach=
Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.

A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.

Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)

''Team Spitzer at Breck School''
Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly "brown-bag discussions." Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.

Marcella:

John:

Diane:

The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. Fortuitously, as one project winds down, another comes along to replace it. Even when we do not have an organized campaign, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and other local events. Currently, students are exploring web sites and reading articles in preparation for their Spitzer work and are anxious to get started!

--[[User:Sartore|Sartore]] 14:06, 6 March 2011 (PST)

... drop one paragraph per teacher here ...

--[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)

File:Brc34 final red.jpg

2011-03-09T05:51:23Z

Legassie:

2011-03-09T04:22:54Z

Legassie: /* Analysis Plan */

=Instructions=

[[2011 proposal instructions]]

=Background on Star Formation=

STUFF HERE IS GENERAL OVERVIEW OF STAR FORMATION IN GENERAL. textbooks, overview articles, good things for general knowledge.

[http://coolcosmos.ipac.caltech.edu/resources/star_formation/ Luisa's tutorial on star formation from cool cosmos]

Notes from a U of Oregon lecture on star formation ... not as good as Luisa's lecture notes but a good launching point ... [http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html http://abyss.uoregon.edu/~js/ast122/lectures/lec13.html]

A more detailed explanation of Star Formation from a textbook. There's more math here than we'll need. [[File:SF.pdf]]
--[[User:CJohnson|CJohnson]] 11:05, 1 February 2011 (PST)

=Target Selection=

STUFF HERE PERTAINS TO SPECIFIC TARGET SELECTION. why we should do one region versus another, why some regions should be dropped. high-level stuff right here; links below go to stuff specific to each target.

The list of sources that Lori suggests we consider are here:
*[[target selection for brc34]] 21h32m51.2s +58d08m43s DECIDED ON THIS ONE
*[[target selection for brc36]] 21h35m32.6s +57d31m50s
*[[target selection for brc31]] 20h50m43.4s +44d21m53s SPITZER DONE ALREADY DONE in the north american nebula
*[[target selection for brc27]] 07h04m07.8s -11d16m43s DECIDED ON THIS ONE; HAS SOME IRAC ANALYSIS IN http://adsabs.harvard.edu/abs/2009MNRAS.396..964C [[media:chauhanarticle.pdf]]

*[[target selection for brc38]] 21h40m02.2s +58d20m31s RULE THIS OUT BECAUSE SPITZER DATA IS DONE

Let's collect information on literature references for each of these. Look in both ADS and SIMBAD for papers and previously known sources within about <s>30'</s> 10' of these positions.

Help on: [[Basic Literature Searching]] -- [[Advanced Literature Searching]] -- [[How_can_I_get_data_from_other_wavelengths_to_compare_with_infrared_data_from_Spitzer%3F | Getting data from other wavelengths]] -- [[Guide to NITARP participants for use of the wiki]]

CONCLUSION OF VOTES: we should do BRC 27 AND BRC 34! but we can mention in the proposal something like "we have a few other targets that we can study instead or in addition to the targets discussed here, should the analysis go faster than anticipated."

papers from discussion on the phone 16:35, 23 February 2011 (PST)
*[[media:morganpaper.pdf|Morgan 2009 paper]] -- has a figure with "sfo 38" http://adsabs.harvard.edu/abs/2009MNRAS.400.1726M
*[[media:morganpaper2008.pdf|Morgan 2008 paper]] -- defines some terms used in 2009 paper http://adsabs.harvard.edu/abs/2008A%26A...477..557M

----

=STUFF BELOW THIS LINE IS MEAT/DRAFT TEXT FOR PROPOSAL ITSELF.=

=Introduction/Background=

the formal reference to lori's poster is here: http://adsabs.harvard.edu/abs/2011AAS...21725815A --[[User:Rebull|Rebull]] 16:22, 23 February 2011 (PST)

http://journals.cambridge.org/action/displayAbstract?fromPage=online&aid=1655856
Proceedings of the International Astronomical Union (2007), 3: 164-165
DOI: 10.1017/S1743921307012823 (About DOI) Published online: 25 Jan 2008
Low-mass star formation in bright rimmed clouds V. Migenesa, M. A. Trinidada, R. Valdettaroa, F. Pallaa and J. Branda
--[[User:Sartore|Sartore]] 16:02, 23 February 2011 (PST)

A&A 388, 172-178 (2002)
DOI: 10.1051/0004-6361:20020451
The embedded star clusters in the nebulae NGC 2327 and BRC 27 in Canis Majoris R1
J. B. Soares and E. Bica
Universidade Federal do Rio Grande do Sul, IF, CP 15051, Porto Alegre 91501-970, RS, Brazil (Received 11 February 2002 / Accepted 21 March 2002 )--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)

A&A 426, 535-545 (2004)
DOI: 10.1051/0004-6361:20040226
A radio and mid-infrared survey of northern bright-rimmed clouds
L. K. Morgan, M. A. Thompson, J. S. Urquhart, G. J. White and J. Miao

Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NR, UK
--[[User:Sartore|Sartore]] 16:03, 23 February 2011 (PST)

DOES ANYBODY HAVE ACCESS TO Ogura's 2010 "Triggered Star Formation associated with HII Regions" ADS says the full paper is not available.
--[[User:Sartore|Sartore]] 12:37, 6 March 2011 (PST)

'''Science Background and Context: Star Formation'''

Few issues in astronomy are more fundamental than understanding stellar processes. Learning how stars form has been, and will continue to be, the topic of vigorous investigations. Stars are born in nebulae, giant molecular clouds of gas and dust found in abundance within disk components of spiral galaxies. Star formation may be triggered in a molecular cloud that is already contracting by shock waves from a variety of sources; supernova explosion, ignition of a very hot star nearby, collision with another molecular cloud, or spiral arm density waves. A very large cloud typically contracts to form a number of individual stars (perhaps hundreds, or more). During the processes of accretion, self-gravitation, and differentiation, protostars are shielded within their nebula, leading to the characterization of nebulae as “stellar nurseries”. During these stages theoretical models predict that these protostars must be very luminous and look like cool red stars, however we have no method of observing them in visible wavelengths. The dust cocoon absorbs most of the visible radiation surrounding the protostar and the nebula itself obscures the protostar from our view. The energy from the protostar warms the dust, which then re-radiates the energy from the protostar as infrared radiation. Thus, protostars are detectable within their nebula at infrared wavelengths. Excess infrared signatures may indicate the existence of an accompanying accretion disk. Jets from hidden protostars may also announce the presence of the still hidden protostar.

Bright Rimmed Clouds (BRC’s) are clouds that have experienced compression due to an external ionization shock, which served to focus the neutral gas into compact globules (Migenesa et.al.(2008)). These clouds generally have a radius of less than 0.5 pc, with an average mass near (or exceeding) 100 solar masses. Attention has turned to BRC’s as potential loci for star formation; their “speck globules” and “cometary globules” presenting interesting sites for possible star formation. Whether external ionization shocks compress the neutral gas into compact globules or bright rims, the boundary between neutral gas and gas ionized by incident photons is thought to be rich in potential sites for star formation. Drawn from the lists of Sugitani, Fukui, and Ogura (1991), and Sugitani and Ogura (1994), Allen et.al.(2011) imaged 32 of the closest bright-rimmed clouds located at estimated distances d < 1.2 kpc, finding young stellar objects in 75% of the clouds they studied.

Using Spitzer Space Telescope Archival Data we propose to conduct further examinations of BRC 27 and BRC 34 to search for additional Young Stellar Objects. BRC 27 is located in the molecular cloud Canis Majoris R1. BRC 34 has a variety of features worthy of deeper examination; dark nebulae, molecular and IC clouds, emission stars, and IR sources. Allen et.al.(2011) found one Class I protostar in BRC 27 and 34. Far more Class II T-Tauri stars were found in those same BRC's. Beyond that, these two BRC’s have not been well studied. We have a few other targets that we can study instead, or in addition to, the targets discussed here if the analysis goes faster than anticipated. We would like to search for undiscovered Young Stellar Objects. We believe there are more YSO’s to find in these BRC’s using Spitzer Space Telescope archival data in a variety of wavelengths.

--[[User:Sartore|Sartore]] 13:58, 26 February 2011 (PST)

BRC 27: John (Likewise, this is what I have so far for the background on BRC27. Please let me know if this is the correct approach and if there is anything else I should be including. Thanks.)

BRC27 is a star forming region located in the molecular cloud CMa R1 and is considered a type “A” bright rimmed cloud because of the moderate curvature of its morphology. The source of the shock front that triggered star formation in this region is still uncertain (Gregorio-Hetem et al, 2009). In a survey of the Canis Major star forming region, 179 H-alpha-emission stars were identified by WIRAMIHARDJA et al. (1986) using UBV photographic photometry. Sugitani, Fukui & Ogura (1991) identified a star cluster associated with BRC27 in their catalog of bright-rimmed clouds with IRAS point sources and subsequent research by Sugitani, Tamura & Ogura (1995) showed elongation of the cluster members indicating that the star formation in BRC27 was a triggered event. Using J, H, KS photometry Soares and Bica (2002, 2003) determined the distance and age of the stars in BRC27 to be 1.2 kpc and 1.5 Myr. Their distance measurement was consistent with the findings of Shevchenko, et al. (1999) who placed the distance at 1.05±0.15 kpc. Recently Gregorio-Hetem et al (2009) did a wide-field X-ray study of the CMa OB1/R1 star forming regions in an attempt to find low mass young stars that may not have been detected using previous methods. In their analysis they identified 40 members near Z CMa and 60 members near GU CMa which are both in the vicinity of BRC27. As part of a survey of 44 bright rimmed clouds, Morgan et al (2008) used submillimeter SCUBA observations and archival data from near-IR and mid- to far-IR to identify a dense core in BRC27. Using BVIC photometry Chauhan et al (2009) compared the ages of stars inside and outside the rims of BRC. As a result, they identified four BRC including BRC27 that showed evidence of a radiation driven implosion (RDI). --[[User:Gibbs|Gibbs]] 21:26, 26 February 2011 (PST)

BRC 34: Marcella
(This is my initial research. There is more to be done but I just wanted to make sure that I was on the right track. Sorry I don't know how to do a table yet and my image is missing. Can you put images on?).

Triggered star formation can often be found in areas called Bright-rimmed clouds (BRC). BRC exist at the edge of HII regions and are often produced by radiative-driven implosion (RDI). According to Morgan et al (2004) nearby massive stars shock the surrounding area to trigger star formation. The UV flux of nearby OB stars causes the BRC to collapse (Morgan 2004). Additionally, Morgan (2004) reports that recombination with the ionized boundary layer (IBL) allows the BRC to be seen at optical wavelengths. Sugitani et al 1991 (SFO91) classifies BRC based on their rim morphology: type A, B, and C with moderately curved, tightly curved, and cometary curved rims, respectively. W SFO91 classified BRC 34 as type A. e propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91).

Previously identified IRAS Point Sources within 10 arcminutes are listed below (SIMBAD).

Identifier Dist(asec) RA DEC

IRAS 21319+5755 268.14 21 33 25.0 +58 08 26

IRAS 21316+5751 283.31 21 33 10.2 +58 04 43

IRAS 21320+5752 373.69 21 33 33.4 +58 05 56

IRAS 21314+5802 429.35 21 32 55.5 +58 15 51

IRAS 21320+5752 436.65 21 32.5 +58 02

IRAS 21323+5800 578.04 21 33 52.0 +58 14 04

Previously identified stars within 10 arcminutes are listed below (SIMBAD).

Identifier Class Dist (asec) RA DEC

TYC 3975-82-1 G8 380.45 21 33 38.069 +58 07 19.42

HD 205510 A3 439.13 21 33 41.7048 +58 11 45.234

GSC 03975-00282 K 508.26 21 33 36.91 +58 02 46.6

BD+57 2346 K2 566.01 21 32 29.6670 +58 17 42.840

Cl*Trumpler 37 KUN 170 567.55 21 33 17.02 +57 59 53.7

Cl*Trumpler 37 KUN 307 590.18 21 34 05.29 +58 07 38.8

Ogura et al (2002) using Hα grism spectroscopy and narrowband imaging found two Hα emission stars in BRC 34. These are identified in the table and image below. Number 1 has been confirmed in SIMBAD.

Identifier Dist (asec) RA DEC

1 2MASS
J21332921+5802508 463.43 21 33 29.21 +58 02 50.9

2 21 33 55.8 +58 01 18

Morgan (2004) used archival data from IRA, NRAO/VLA Sky Survey (NVSS), Digitized Sky Survey (DSS) and the mid-course Space experiment (MSX) to characterize the IBL of BRC. No 20 cm emission was associated with the rim of BRC 34.
Water maser emissions, indicative of YSOs, were not detected by Valdettaro et al (2005) at 22.2 GHz in BRC 34. They surmised that the negative results were due to the emission from the heated dust near the head of the BRC. This might also be indicative of low-mass star formation.
Morgan et al (2007) studied BRC 34 by using Submillimeter Common User Array (SCUBA) data and supplemented their findings with NASA/IPAC Infrared Science Archive (IRAS at 12, 25, 60 and 100 μm) and 2 mm all sky survey (2MASS) archival data. A search of the 2 MASS catalog by Morgan (2007) found that BRC 34 did not have any T Tauri stars nor any class 1 protostellar candidates. They proposed that the lack of YSO might be due to the protostellar core being at the early stages of evolution.
Morgan et al (2009) observed CO spectra of BRC 34. As a result of this and previous work (Morgan 2007 and Morgan 2004), Morgan eliminated BRC 34 as a good candidate for RDI suggesting that its evolution would not be affected by nearby OB stars.

... drop what you have here ...

=Analysis Plan=

--[[User:Legassie|Legassie]] 20:12, 8 March 2011 (PST)

Spitzer archival data from IRAC and MIPS will be the main focus of our research, augmented with data from 2MASS and MSX. Information on the Spitzer programs we will use is provided in Table X below:

'''Table X'''
* BRC27: Program 30050
** IRAC Reqkey 17512192 (IRAC 4 bands)
** MIPS Reqkey 17512448 (MIPS 24 & 70 um)
* BRC34: Program 202
** Reqkey 6031616 (IRAC 4 bands)
** Reqkey 6031872 (MIPS 24 um)

used as our primary source of data, along with as well as 2MASS, MSX, and four bands of IRAC and 2 bands of MIPS

* Archival Spitzer IRAC 4 bands & MIPS (Programs TBD)
* 2MASS
* MSX
* Optical?

[[File:Brc34_spot_visualization.jpg]]

[[File:Brc27_spot_visualization.jpg]]

'''Data Reduction'''

* Photometry will be obtained using data reduction tools such as Aperture Photometry Tool (APT)
* Mosaics will be created using MOPEX

'''Analysis Plan'''

* Plan is to combine all available data and examine properties of previously known YSOs (Allen et al 2010) as well as look for new YSOs
* Looking for infrared excess emission from material surrounding new stars will be the main focus of the research
* Using photometry measurements, team will generate and examine several diagrams, looking for infrared excesses
** Color-Color diagrams
** Color-Magnitude diagrams
** Spectral Energcy Distribution (SED) plots
* Analysis will also involve looking at actual optical and infrared images

'''Tools'''

* MOPEX - to create mosaics (Makovoz & Marleau 2005)
* Aperture Photometry Tool (APT) - to obtain photometry (Laher et al. 2010)
* MS Excel – to generate data diagrams (color-color, SEDs)

=Education and Outreach=
Starting with a general introduction to the physical properties of light, students and teachers will collaborate to synthesize observations across the spectrum. They will compare images obtained by IRAC, MIPS and IRAS to learn about spatial resolution. Evidence will be presented to help students understand how the universe is changing, how stars and planets are forming, and how stars evolve from birth to eventual death. Combining images at different wavelengths, students will be able to produce false-color images that enhance the features of young stellar objects and the ISM composition and structures.

A key initiative in science education is authentic research. Using archival Spitzer data in this project allows our students the experience to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. They will learn about the instrumentation used in infrared astronomy and the necessity of space-based telescopes. Students and teachers will use spreadsheet and graphing programs to generate color-color plots and color-magnitude diagrams to determine stellar properties. These activities will be age-appropriate and will be shared with other teachers through educational presentations at state, regional and national conferences.

Communication is an important tool in science education. Modeling the collaboration of scientists across the world, students will use the CoolWiki to post their queries and hold on-line discussions about their analysis methods and subsequent results. The CoolWiki is designed to provide a place for teachers, students, and scientists to interact and share the materials they've developed, work on new materials, and collaborate on current projects. The wiki also provides a resource for other teachers to learn how to use the materials we've developed. The wiki is a dynamic place, constantly changing and growing. (need to develop this thought further...)

''Team Spitzer at Breck School''
Similar to previous NITARP/Spitzer projects, a small cadre of Breck School juniors and seniors will work together on this BRC project. Beginning with short tutorials on the general principles of star formation, scientific articles will be read and discussed in weekly "brown-bag discussions." Once the students feel comfortable with the material, the team will be divided into pairs to work cooperatively on the data analysis.

Marcella:

John:

Diane:

The Pine Ridge Astronomy Team has a history of participation in big projects; our first project was with the Lunar Propector in 1998. Fortuitously, as one project winds down, another comes along to replace it. Even when we do not have an organized campaign, the sky always presents something different for us to examine. The team meets during Wednesday lunchtime meetings. Team members organize Night Labs and Morning Labs to take advantage of good viewing opportunities as they arise during the school year. They also participate in community outreach activities; science night at local elementary schools, Relay for Life, and other local events. Currently, students are exploring web sites and reading articles in preparation for their Spitzer work and are anxious to get started!

--[[User:Sartore|Sartore]] 14:06, 6 March 2011 (PST)

... drop one paragraph per teacher here ...

--[[User:CJohnson|CJohnson]] 19:40, 22 February 2011 (PST)