CoolWiki - User contributions [en]

File:Education poster.pptx

2011-12-21T19:53:47Z

Linahan:

Please, just put all the BRC data tables in one place

2011-12-21T19:21:16Z

Linahan: /* December work ... dare I say, final? */

Here is where I will put all the final, best copies of things.

=Literature sources=

[[Identification of Previously Known Objects on Candidate List]] and as part of that discussion, [[BRC Spring work]], have the history of what is going on. Importantly, '''special objects to consider''' are on the bottom of [[Identification of Previously Known Objects on Candidate List]].

==BRC27==

The data files from the original papers with the 2mass matches and updated coordinates where relevant (final, best copies, or at least "best as of 15 Sep") are, for BRC 27:
*Ogura K., Sugitani K., Pickles A., 2002, AJ, 123, 2597. -- from Luisa, 15 sep -- [[file:ogura-luisa.txt]]
*Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964. -- (from Luisa, 23 June): [[file:Chauhan-table3.txt]] and [[file:Chauhan-table6.txt]]
*Gregorio-Hetem J., Montmerle T., Rodrigues C. V., Marciotto E., Preibisch T., Zinnecker H., 2009, A&A, 2009, 506, 711. -- (from Luisa, 23 June): [[file:gregoriohetem-tablea1.txt]]
*Shevchenko V. S., Ezhkova O. V., Ibrahimov M. A., van den Ancker M. E., Tjin A, Djie H. R. E., 1999, MNRAS, 310, 210. -- (from Luisa, 15 Sep) [[file:shev-luisa.txt]] (NB: full original table available back in [[BRC Spring work]])
*Wiramihardja S.D., Kogure T., Nakano M., Yoshida S., 1986, PASJ, 38, 395. -- [[file:wiram-luisa.txt]]

Luisa's merging for BRC 27 -- as of 15 sep, the best catalog I have is [[file:litsrcs-brc27-0915-lmr.txt]] -- This is a merging of '''all''' the literature information above, with the best possible matches to counterparts as of today, noonish.

==BRC 34==

Luisa's "merging" for BRC 34 -- [[file:litsrcs-brc34-0915-lmr.txt]] (this is just a light reformatting of the two sources in the ogura file above.)

=Spitzer (+2MASS) sources=

For the bandmerged Spitzer plus 2mass catalogs, go back to the original DVD. [[file:brcdvdreadme.txt]] from the DVD lists the files, whose names I copy here, rather than the full files (for now anyway).

==BRC 27==

brc27/working/brc27.fullcat.tbl = full bandmerged catalog, all sources, many columns, of the BRC 27 field, 2mass through M24.

==BRC 34==

brc34/working/brc34.fullcat.tbl = full bandmerged catalog, all sources, many columns, of the BRC 27 field, 2mass through M24.

=Merging Spitzer and the literature=

For the catalog of objects I assembled above from the literature, I can compare these objects to the Spitzer+2MASS catalog and make a list of just those objects. Note that these are just the previously identified YSOs, and not the infrared-selected YSOs.

see [[Matching to Spitzer and Weeding the SEDs]] for more discussion and caveats.

==BRC 27==

[[file:litsrcs+spitzer-brc27-0916-lmr.txt]] - JUST THE KNOWN SOURCES

==BRC 34==

[[file:litsrcs+spitzer-brc34-1109-lmr.txt]] - JUST THE ONE KNOWN SOURCE WITH A MATCH

=Selecting sources from Spitzer via Gutermuth method=

The Gutermuth method doesn't need optical data, so we were able to implement the Gutermuth method with just the Spitzer data. Back in July, we already had bandmerged Spitzer plus 2mass catalogs, so we were able to run this then. On the original DVD, I gave you the results of this filtering. [[file:brcdvdreadme.txt]] from the DVD lists the files, whose names I copy here, rather than the full files (for now anyway).

==BRC 27==

brc27/working/brc27ysocand.cat.tbl = full bandmerged catalog, all sources, many columns, for JUST THE YSO CANDIDATES that survive all the Gutermuth tests in BRC27.

==BRC 34==

brc34/working/brc34ysocand.cat.tbl = full bandmerged catalog, all sources, many columns, for JUST THE YSO CANDIDATES that survive all the Gutermuth tests in BRC34.

='Final' list of sources we care about (September) =

e.g., IR-selected, plus previously known sources that don't have IR excesses. see [[Matching to Spitzer and Weeding the SEDs]] for important notes and caveats, and [[Identification of Previously Known Objects on Candidate List]] for list of problem children.

==BRC 27==

[[file:new+known-brc27-0916-lmr.txt]]

BRC 27 ... need to check photometry. [[file:BRC27_photomCheck.xlsx]] Please save your version as BRC27_photomCheck_''state''.xls (insert your state where indicated).
Thanks.
--[[User:CJohnson|CJohnson]] 15:54, 21 October 2011 (PDT)

BRC 27 ... spreadsheet compiled with Florida, Illinois, Oregon and Minnesota data. Photometry checked.
[[file:BRC27_photomCheckCOMP.xlsx]]
--[[User:CJohnson|CJohnson]] 14:18, 9 November 2011 (PST)

CAUTION WITH THOSE FILES - PRIOR IDS NOT UNIFORMLY CORRECT, AND PRIOR FLUX DENSITIES ALSO NOT UNIFORMLY CORRECT. however, coordinates do seem to be right, and the redone photometry generally matches (with each other and with my redone photometry), so the photometry is ok, just the crossids are wrong.

REDONE CATALOG, with best possible photometry and source guessing: [[file:new+known+opt-brc27-1111-lmr.txt]]. see [[Matching to Spitzer and Weeding the SEDs]] for full discussion and caveats.

==BRC 34==

[[file:new+known-brc34-0916-lmr.txt]] same caveats as for the BRC 27 file!

BRC 34 ... need to check photometry. [[file:BRC34_photomCheck.xlsx]] Please save your version as BRC34_photomCheck_state.xls (insert your state where indicated). Thanks.

Sorry I didn't get this posted until now. --[[User:CJohnson|CJohnson]] 14:20, 16 November 2011 (PST)

='Final' lists of sources we've decided to keep as YSO candidates (October) =

e.g., those that survive our examination of images and SEDs.

see [[Matching to Spitzer and Weeding the SEDs]] for discussion.

==BRC 27==

[[Notes on SEDs from BRC27]]

==BRC 34==

[[Notes on SEDs from BRC34]]

=Really final: Fixing the photometry, getting the new optical data incorporated, and dropping some sources for good (November) =

BRC 34 ... here's the composite file [[file:BRC34_photomRecheckFinal.xlsx]] of our re-checked photometry for BRC 34. Besides the data listed on sheet 1, there's a separate sheet for each object with comments, SEDs, and tasty tidbits.
--[[User:CJohnson|CJohnson]] 18:52, 29 November 2011 (PST)

=December work ... dare I say, final?=

BRC 27 ... huge file [[file:BRC27huge_14Dec.xlsx]]

BRC 34 ... huge file [[file:BRC34huge_14Dec.xlsx]]

--[[User:CJohnson|CJohnson]] 18:26, 14 December 2011 (PST)
[[File:education poster.pptx]]
--[[User:Linahan|Linahan]] 11:21, 21 December 2011 (PST)

Working with the BRCs

2011-09-21T21:28:01Z

Linahan: /* Writing it up! */

''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]]

FOR REFERENCE: [[file:brcdvdreadme.txt]] from the DVD, in case yours is formatted so badly you can't read it. Includes instructions on how to force your computer to read any files with an extension you don't recognize (.tbl, .reg).

=Downloading the data =

''9/15/11: done for both BRC 27 and BRC 34''

[[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 =

''9/15/11: done for both BRC 27 and BRC 34''

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 =

''9/15/11: NOT COMPLETELY done for both BRC 27 and BRC 34, but also may be skipable. The Haleakala data also count as '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=

''9/15/11: basically done for both BRC 27 and BRC 34. we will revisit for specific sources.''

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=

''9/15/11: mostly done for both BRC 27 and BRC 34. we are on the home stretch as of 15 sep''

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!)

'''July: BIG PENDING ISSUE FOR HOMEWORK(?)''': 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.)

'''UPDATE SEP 2011''' [[Identification of Previously Known Objects on Candidate List]] tracks a lot of conversation about which objects are which.

=Doing photometry =

''9/15/11: basically done for both BRC 27 and BRC 34. we will revisit this step for specific sources''

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.)

'''NEW 7/7/11''' -- 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.

'''UPDATE SEP 2011''' [[Identification of Previously Known Objects on Candidate List]] tracks a lot of conversation about which objects are which, which then feeds into [[Matching to Spitzer and Weeding the SEDs]] which talks about photometry for a smaller set of objects.

'''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 =

''9/15/11: done for both BRC 27 and BRC 34, though we may need to revisit for certain objects, particularly those from earlier observations that should be tied to more than one object.''

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!!

'''UPDATE SEP 2011''' [[Identification of Previously Known Objects on Candidate List]] tracks a lot of conversation about which objects are which, which then feeds into [[Matching to Spitzer and Weeding the SEDs]] which talks about photometry for a smaller set of objects.

=Working with the data tables =

''9/15/11: somewhat done for at least BRC 27. Will need to redo as repercussions of recent changes above propagate forward.''

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 SED steps 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?

'''UPDATE SEP 2011''' [[Identification of Previously Known Objects on Candidate List]] tracks a lot of conversation about which objects are which, which then feeds into [[Matching to Spitzer and Weeding the SEDs]] which talks about photometry for a smaller set of objects.

=Making color-color and color-magnitude plots=

''9/15/11: somewhat done for at least BRC 27. Will need to redo as repercussions of recent changes above propagate forward.''

'''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. Includes Venn diagram of what we've been doing the last few days.

=Investigating the images of the objects=

''9/15/11: somewhat done for BRC 27. we will revisit for specific sources as the recent updates above propagate forward.''

'''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.

'''UPDATE SEP 2011''' see [[Matching to Spitzer and Weeding the SEDs]] which talks (will talk) about examining images for a smaller set of objects.

=Making SEDs =

''9/15/11: somewhat done for at least BRC 27. Will need to redo as repercussions of recent changes above propagate forward.''

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]]

'''UPDATE SEP 2011''' see [[Matching to Spitzer and Weeding the SEDs]] which talks (will talk) about examining a smaller set of objects in great detail.

=Literature again=

''9/15/11: not really done yet.''

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=

''9/15/11: not done yet, and may be skippable.''

'''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!=

''9/15/11: not done yet.''

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.

'''''Education Poster Abstract.'''''
'''version 1.0''' As part of the NASA/IPAC Teacher Archive Research Project program (NITARP), four high school teachers have participated with two to four students in a science research project using archival Spitzer data to search for young stellar objects in two bright-rimmed clouds: BRC 27 and BRC 34. Our research findings are presented in another poster, Rebull et al. These teachers are from Breck School, Carmel Catholic High School, Glencoe High School, and Pine Ridge High School. A key initiative in science education is integrating authentic scientific research into the curriculum. Since the NITARP program can only fund a limited number of teachers and students, our group has investigated the role of team leaders (both teachers and students) in educating and inspiring other teachers and students. This project allows our students to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. This poster presents our research on how the students who are chosen as the team leaders disseminate the information to other students within the school as well as to other schools and interest groups. Since three of the four teachers are women, we have also looked at how these teachers inspire young women to participate in this program and to pursue a STEM (Science, Technology, Engineering, and Math) careers. This program was made possible through the NASA/IPAC Teacher Archive Research Project program (NITARP) and was funded by NASA Astrophysics Data Program and Archive Outreach funds. --Linahan

'''version 1.1''' As part of the NASA/IPAC Teacher Archive Research Project program (NITARP), four high school teachers have participated with selected students in a research project using archival Spitzer data to search for young stellar objects in two bright-rimmed clouds: BRC 27 and BRC 34. Our research findings are presented in another poster, Johnson et al. A key initiative in science education is integrating authentic scientific research into the curriculum. Since the NITARP program funds a limited number of teachers and students, our group has investigated the role of team leaders (both teachers and students) in educating and inspiring other teachers and students. This project allows our students to assume an active role in the process of project development, teamwork, data collection and analysis, interpretation of results, and formal scientific presentations. This poster presents our research on how the student team leaders disseminate the information to other students within the school, as well as to other schools and interest groups. Since three of the four teachers are female, we have also looked at how these teachers inspire young women to participate in this program and to pursue STEM (Science, Technology, Engineering, and Math) careers. This program was made possible through the NASA/IPAC Teacher Archive Research Project program (NITARP) and was funded by NASA Astrophysics Data Program and Archive Outreach funds.

If it would be easier, we can work with a Word document. Please let me know your preference. --[[User:CJohnson|CJohnson]] 10:53, 21 September 2011 (PDT)

LOVE. IT. :) --[[User:Rebull|Rebull]] 12:51, 21 September 2011 (PDT)

'''''Science Poster Abstract.'''''
'''version 1.0'''
Found near the edges of HII regions, bright-rimmed clouds (BRCs) are thought to be home to triggered star formation. Using Spitzer Space Telescope archival data, we investigated BRC 27 and BRC 34 to search for previously known and new additional young stellar objects (YSOs). BRC 27 is located in the molecular cloud Canis Majoris R1, a known site of star formation. BRC 34 has a variety of features worthy of deeper examination: dark nebulae, molecular clouds, emission stars, and IR sources. Our team used archival Spitzer InfraRed Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS), combined with 2-Micron All-Sky Survey (2MASS) data as well as optical data from XXX. We used infrared excess to investigate the properties of previously known YSOs and to identify additional new candidate YSOs in these regions. This research was made possible through the NASA/IPAC Teacher Archive Research Project (NITARP) and was funded by NASA Astrophysics Data Program and Archive Outreach funds. --[[User:CJohnson|CJohnson]] 11:19, 21 September 2011 (PDT)

'''''Author List.'''''
from Breck School (Minneapolis, MN):
Chelen H. Johnson, Nina G. Killingstad, Taylor S. McCanna, Alayna M. O'Bryan, Stephanie D. Carlson, Melissa L. Clark, Sarah M. Koop, Tiffany A. Ravelomanantsoa

From Carmel Catholic High School (Mundelein, IL): Marcella Linahan, Holly Sprow, Abhisek Ramswaram, Amanda Pullinger, James Fagan, and Nicolas Ezyk. (need to update with student's initials and then I will delete this line. --[[User:Linahan|Linahan]] 14:28, 21 September 2011 (PDT)

--[[User:CJohnson|CJohnson]] 11:24, 21 September 2011 (PDT)

'''''Science Poster Abstract.'''''
'''version 1.1 - just tiny changes.'''
Found near the edges of HII regions, bright-rimmed clouds (BRCs) are thought to be home to triggered star formation. Using Spitzer Space Telescope archival data, we investigated two BRCs, BRC 27 and BRC 34, to search for previously known and new candidate additional young stellar objects (YSOs). BRC 27 is located in the molecular cloud Canis Majoris R1, a known site of star formation. BRC 34 has a variety of features worthy of deeper examination: dark nebulae, molecular clouds, emission stars, and IR sources. Our team used archival Spitzer InfraRed Array Camera (IRAC) and Multiband Imaging Photometer for Spitzer (MIPS), combined with 2-Micron All-Sky Survey (2MASS) data. We investigated the infrared properties of previously known YSOs and used infrared colors to identify additional new candidate YSOs in these regions. This research was made possible through the NASA/IPAC Teacher Archive Research Project (NITARP) and was funded by NASA Astrophysics Data Program and Archive Outreach funds. --[[User:Rebull|Rebull]] 12:51, 21 September 2011 (PDT)

BRC Current Research Activities

2011-07-09T21:20:15Z

Linahan: /* BRC Fall work */

=[[BRC Proposal]]=

This page will be used to assemble the pieces for the proposal we are writing.

=[[BRC Useful Links]]=

A consolidation of all sorts of useful links.

=Previous Teams' pages=
[[IC 2118 Current Research Activities]] (2004-2008), [[Lynds Clouds Current Research Activities]] (2008), and [[CG4 Current Research Activities]] (2010)

Also see [[Working with L1688]] (A sample analysis thread using Lynds 1688, developed in the context of the Lynds Cloud team) and [[Working with CG4+SA101]], an adaptation of "Working with L1688", with specific application to that project.

=[[BRC Spring work]]=
This page will be used to collect information during our work in Spring.

Here's a brief outline [[file: NITARPpreview.docx]] of things to look at before going to SSC … but we will go through all of this in more detail. Links to corresponding wiki pages are embedded within the document.
--[[User:CJohnson|CJohnson]] 20:18, 1 June 2011 (PDT)

=[[BRC Summer visit logistics]]=
This page will be used to collect logistics information about our IPAC visit.

We talked about traveling 05-July, work 06-09 July and travel home on 10-July. --[[User:CJohnson|CJohnson]] 12:40, 2 February 2011 (PST)

=[[BRC Bigger Picture and Goals]]=
In past years, I've found that "why are we doing this, again?" is a pretty frequent question ...

=[[Working with the BRCs]] -- Summer Visit Work!=
More of a step-by-step thing, but please don't make the mistake of thinking this is a cookbook.

=[[BRC Fall work]]=
Notes and results from our work in the Fall, where "Fall" means "any time after our visit in July". :)
Bright-rimmed Clouds

Things to do

1. Read Chauhan (Chauhan N, Pandey A.K., Ogura K., Ojha D.K., Bhatt B.C., Ghosh S.K., Rawat P.S., 2009, MNRAS, 396, 964.)[http://adsabs.harvard.edu/abs/2009MNRAS.396..964C]

2. Read CG4 [http://lanl.arxiv.org/PS_cache/arxiv/pdf/1105/1105.1180v1.pdf]

3. Feedback form by Sunday 7/17 to your teacher

4. Make sure that we have all the data available for both clouds.

*a. All the known objects
*b. All the “unknown objects”

5. Finish BRC 27 then work on BRC 34.

6. Answer all the questions in the Working with the BRCs. Type them up if necessary.

7. Post the URL’s for the different bands on the Wiki in the relevant links section.

8. Watch the YouTube videos for each section.

9. Where is the BRC? What is a point source? What is the BRC? What is a foreground star?

10. Under Previously identified sources, checking the duplicates.

11. What is photometry? What is it measured in? What do we convert it into?

12. What does APT really do for you?

13. Why does the MOPEX source pick up wrong objects and miss others?

14. Working with the data tables: Save files in a standard format
*a. BRC number
*b. Cand or known
*c. Underscore
*d. Initials
*e. underscore
*f. Two-number date
*g. Three letter month code
*h. Example: 27cand_chj_09jul.xls

15. Data tables:

*a. Make SEDS with the all 38 candidate objects.

16. Color-color diagram

17. Color-magnitude diagram

Long-term goals:

1. “Pretty pictures” for poster. Three-color images of BRC-27 and BRC-34.

2. Science poster

3. Education poster

4. paper?
--[[User:Linahan|Linahan]] 14:20, 9 July 2011 (PDT)

Extra notes:

Powerpoint 1:

NASA has some great observatories.

Why do we need to use different telescopes?

1. “To see different things”
*a. X-rays vs. gamma rays
*b. Atmosphere absorbs certain wavelengths
*c. Atmosphere is opaque to certain wavelengths
*d. Dusty regions are not seen in optical, can’t see through it

2. Why are we using archival data?

*a. Data does need to be sorted but by the computers but
*b. Cryogen is gone.
*c. Surpassed its lifetime.
*d. 3 & 4 and MIPS is gone but lots of data just haven’t been looked at
*e. Hotter objects shorter waves

Powerpoint 2:

1. What is SSC?

*a. Spitzer Science Center

2. Wavelengths and bands
*a. Bands are x number across but numbers correspond to center

3. Using heritage data

4. Hopefully use WISE data

5. Good to look through the rest of packet

6. P. 34 jail bars and instrument artifacts. Washed out some of the things around it. Messy.

*a. If we found this, we could smooth it out not scientific information

7. Chemistry and elements used

Powerpoint 3:

1. Star formation. Major topic on top of page 3.
*a. Small stars and stars with dusty disk
*b. Phase 0 yee hah yakky yak
*c. Probably won’t be able to pin down the age of the object but will not be able to pin down the distance.
*d. Links and files to movies

2. Extrasolar planets are hot topic
*a. Iphone app to let you know when new planets are found

PowerPoint 4:

1. Most important. Goals:
*a. Science poster
**i. Paper written
*b. Education poster:
**i. How can we bring this to other students?
**ii. How has it opened new doors for you?
**iii. STEM careers
**iv. Writing
*c. Other teams will have at least 2 posters

2. Classes on pg. 7 and how it relates to SEDs
*a. How is the energy distributed over different wavelengths

3. Blackbodies
*a. Perfect radiators
*b. Give off all the energy that they produce

4. SEDs
*a. Slopes: left and right

5. Color-color diagrams p. 15
*a. Magnitudes
*b. Reddening of the object

6. Photometry
*a. Not using the MOPEX program

--[[User:Linahan|Linahan]] 14:20, 9 July 2011 (PDT)

BRC Current Research Activities

2011-07-09T21:14:12Z

Linahan: /* BRC Fall work */

BRC Current Research Activities

2011-07-09T21:08:34Z

Linahan: /* BRC Fall work */

BRC Proposal

2011-02-27T01:25:31Z

Linahan: /* Introduction/Background */

=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
*[[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)

'''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 numerous 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). 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 protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then reradiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. 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 (Migenssa 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, should the analysis go 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

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=

mark, please also dip into the SHA (ops not i&t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)

--[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)

'''Available Data'''

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

'''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:

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

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

BRC Proposal

2011-02-27T01:23:38Z

Linahan: /* Introduction/Background */

=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
*[[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)

'''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 numerous 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). 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 protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then reradiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. 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 (Migenssa 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, should the analysis go 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

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. We propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91). SFO91 classified BRC 34 as type A.

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=

mark, please also dip into the SHA (ops not i&t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)

--[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)

'''Available Data'''

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

'''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:

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

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

BRC Proposal

2011-02-27T01:22:51Z

Linahan: /* Introduction/Background */

=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
*[[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)

'''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 numerous 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). 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 protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then reradiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. 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 (Migenssa 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, should the analysis go 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

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. We propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91). SFO91 classified BRC 34 as type A.

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=

mark, please also dip into the SHA (ops not i&t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)

--[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)

'''Available Data'''

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

'''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:

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

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

BRC Proposal

2011-02-27T01:21:34Z

Linahan: /* Introduction/Background */

=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
*[[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)

'''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 numerous 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). 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 protostars are thought to be very luminous and look like cool red stars, however this stage is not visible to us. The dust cocoon absorbs most of the visible radiation surrounding the protostar; the nebula itself obscures all visual components from our view. However, the energy from the protostar warms the dust, which then reradiates the energy from the protostar as infrared radiation. Thus, protostars are visible within their nebula at infrared wavelengths, but are not visible through optical telescopes. 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 (Migenssa 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, should the analysis go 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

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. We propose to examine young stellar objects (YSO) in BRC 34 with coordinates of 21 h 32 m 51.2s +38d08m43s and 0.75kpc (SFO91). SFO91 classified BRC 34 as type A.

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=

mark, please also dip into the SHA (ops not i&t! :) ) to see what data are available, specific AORKEYs, etc. we'll need to put that in the proposal too. --[[User:Rebull|Rebull]] 16:12, 23 February 2011 (PST)

--[[User:Legassie|Legassie]] 15:53, 23 February 2011 (PST)

'''Available Data'''

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

'''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:

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

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

Target selection for brc36

2011-02-11T22:16:00Z

Linahan: /* brc36 21h35m32.6s +57d31m50s */

== brc36 21h35m32.6s +57d31m50s ==

* BRC 36 3 articles on ADS two are on star formation but none on SIMBAD

* 3 results from ADS: 1 abstract, 2 Chandra proposals; 0 results from Simbad, however, Aladin applet Simbad identifies (and IRAS-IRIS reveals) 6 YSOs, 10 IR sources, 2 Mol Cld, Rf Neb, Br Neb, Dk Neb, stars in nebulae, and stars in clouds.

* This looks like an interesting field. Lots going on (too much?) ADS: Garmire and Getman are both proposing to use Chandra to study this area. (x-rays)

--[[User:CJohnson|CJohnson]] 16:33, 9 February 2011 (PST)

Using SIMBAD, and searching under coordinates yields 83 objects mostly stars: 17 *iC, 13 TT*, 4 *, 1 **, 8 Y*O, 4 Em*, 1 Or*, 1 *i* (star in double system), 1 *IN (star in nebula), 16 IR sources, 3 smm, 5 Molecular cloud, 2 part of cloud, 1 cloud, 1 dark nebula, 1 bright nebula, 1 reflection nebula, and 1 radio source. One of the molecular clouds is the elephant trunk nebula.--[[User:Linahan|Linahan]] 13:20, 11 February 2011 (PST)

The elephant trunk nebula has 23 references. Here is a sampling of them.
#66 NAME ELEPHANT TRUNK NEBULA 519.38 MoC 21 36 +57.4
2009AJ....137.3685B  Astron. J., 137, 3685-3699 (2009)  An infrared census of star formation in the Horsehead nebula.  BOWLER B.P., WALLER W.H., MEGEATH S.T., PATTEN B.M. and TAMURA M.
2009AJ....138.1116S  Astron. J., 138, 1116-1136 (2009)  A Spitzer view of the young open cluster NGC 2264.  SUNG H., STAUFFER J.R. and BESSELL M.S.
2009ApJ...690..683R  Astrophys. J., 690, 683-705 (2009)  Properties of protostars in the Elephant Trunk in the globule IC 1396A.  REACH W.T., FAIED D., RHO J., BOOGERT A., TAPPE A., JARRETT T.H., MORRIS P., CAMBRESY L., PALLA F. and VALDETTARO R.
2009ApJ...694L..26G  Astrophys. J., 694, L26-L30 (2009)  Driving turbulence and triggering star formation by ionizing radiation.  GRITSCHNEDER M., NAAB T., WALCH S., BURKERT A. and HEITSCH F.
2009ApJ...702.1507M  Astrophys. J., 702, 1507-1529 (2009)  Mid-infrared variability of protostars in IC 1396A.  MORALES-CALDERON M., STAUFFER J.R., REBULL L., WHITNEY B.A., BARRADO Y NAVASCUES D., ARDILA D.R., SONG I., BROOKE T.Y., HARTMANN L. and CALVET N.
2008A&A...485..753H  Astron. Astrophys., 485, 753-763 (2008)  An infrared-submillimeter study of starforming regions selected by the ISOSS 170 {mu}m survey.  HENNEMANN M., BIRKMANN S.M., KRAUSE O. and LEMKE D.
2008ApJ...675.1352V  Astrophys. J., 675, 1352-1360 (2008)  High-resolution H_2_ O maser observations toward IRAS sources in bright-rimmed clouds.  VALDETTARO R., MIGENES V., TRINIDAD M.A., BRAND J. and PALLA F.
flags: (abstract)
2007PASJ...59S.443I  Publ. Astron. Soc. Jap., 59, 443-454 (2007)  AKARI infrared imaging of reflection nebulae IC4954 and IC4955.  ISHIHARA D., ONAKA T., KANEDA H., SUZUKI T., KATAZA H., SAKON I., OKADA Y., DOI Y., FUJISHIRO N., FUJIWARA H., ITA Y., KII T., KIM W., MAKIUTI S., MATSUMOTO T., MATSUHARA H., MURAKAMI H., NAKAGAWA T., OHYAMA Y., OYABU S., SERJEANT S., SHIBAI H., TAKAGI T., TANABE T., UEMIZU K., UENO M., USUI F., WADA T., WATARAI H. and YAMAMURA I.
--[[User:Linahan|Linahan]] 13:33, 11 February 2011 (PST)

#12 and #75 The two larges sources are both stars with 28 and 24 sources. respectively. Looks like it might be a star in the elephant trunk nebula because they have overlapping sources. HD 205794 243.93 *iC 21 35 43.8294 +57 28 03.484 B0.5V 28 and 75 HD 239710 560.65 *iN 21 36 41.0395 +57 30 08.260 B3V 24

Both reference: 2004ApJS..154..385R  Astrophys. J., Suppl. Ser., 154, 385-390 (2004)  Protostars in the Elephant Trunk nebula.  REACH W.T., RHO J., YOUNG E., MUZEROLLE J., FAJARDO-ACOSTA S., HARTMANN L., SICILIA-AGUILAR A., ALLEN L., CAREY S., CUILLANDRE J.-C., JARRETT T.H., LOWRANCE P., MARSTON A., NORIEGA-CRESPO A. and HURT R.L.--[[User:Linahan|Linahan]] 13:46, 11 February 2011 (PST)

Here is the summary of information on the clouds:
#28 [IS94] 1 354.07 MoC 21 35 43 +57 26.1
1994JApA...15..157I  J. Astrophys. Astron., 15, 157-163 (1994)  Observations of the bright-rimmed molecular clouds near the Cepheus OB 2 association.  INDRANI C. and SRIDHARAN T.K.

#29 [PGS95] 14 365.70 PoC 21 36 03.6 +57 27 23
1995ApJ...447..721P  Astrophys. J., 447, 721-741 (1995)  The large-scale structure, kinematics, and evolution of IC 1396.  PATEL N.A., GOLDSMITH P.F., SNELL R.L., HEZEL T. and XIE T.

#39 IRAS 21346+5714 410.43 Cld 21 36 12.4 +57 27 34 There are 11 sources but a lot of the same sources as elephant trunk.
1995Ap&SS.224..571S  Astrophys. Space Sci., 224, 571-572 (1995)  Searches for bright-rimmed clouds with IRAS point sources.  SUGITANI K. and OGURA K.
1991ApJS...77...59S  Astrophys. J., Suppl. Ser., 77, 59-66 (1991)  A catalog of bright-rimmed clouds with IRAS Point Sources: candidates for star formation by radiation-driven implosion. I. The Northern hemisphere.  SUGITANI K., FUKUI Y. and OGURA K.

#40 [IS94] 15 410.44 MoC 21 36 12 +57 27.5
1991ApJS...77...59S  Astrophys. J., Suppl. Ser., 77, 59-66 (1991)  A catalog of bright-rimmed clouds with IRAS Point Sources: candidates for star formation by radiation-driven implosion. I. The Northern hemisphere.  SUGITANI K., FUKUI Y. and OGURA K.

#61 [DBY94] 099.1+04.0511.24 MoC 21 36 35.4 +57 30 36
1994ApJS...95..419D  Astrophys. J., Suppl. Ser., 95, 419-456 (1994)  Molecular clouds in Cygnus. I. A large-scale survey.  DOBASHI K., BERNARD J.-P., YONEKURA Y. and FUKUI Y.

#70 LBN 098.83+04.12 538.58 MoC 21 35 +57.4
2006MNRAS.369.1822M  Mon. Not. R. Astron. Soc., 369, 1822-1836 (2006)  Photometric distances to nine dark globules.  MAHESWAR G. and BHATT H.C.
1997A&A...325.1001S  Astron. Astrophys., 325, 1001-1012 (1997)  The X-ray view of the central part of IC 1396.  SCHULZ N.S., BERGHOEFER T.W. and ZINNECKER H.
1990ApJ...359..319L  Astrophys. J., 359, 319-343 (1990)  A CO survey of regions around 34 open clusters. II. Physical properties of cataloged molecular clouds.  LEISAWITZ D.
1989ApJS...70..731L  Astrophys. J., Suppl. Ser., 70, 731-812 (1989)  A CO survey of regions around 34 open clusters.  LEISAWITZ D., BASH F.N. and THADDEUS P.

#83 [PGS95] 15598.87 PoC 21 36 03.9 +57 22 47
1995ApJ...447..721P  Astrophys. J., 447, 721-741 (1995)  The large-scale structure, kinematics, and evolution of IC 1396.  PATEL N.A., GOLDSMITH P.F., SNELL R.L., HEZEL T. and XIE T.--[[User:Linahan|Linahan]] 14:16, 11 February 2011 (PST)

Target selection for brc36

2011-02-11T22:14:57Z

Linahan: /* brc36 21h35m32.6s +57d31m50s */

Target selection for brc36

2011-02-11T22:13:46Z

Linahan: /* brc36 21h35m32.6s +57d31m50s */

Target selection for brc36

2011-02-11T22:12:47Z

Linahan: /* brc36 21h35m32.6s +57d31m50s */

Target selection for brc36

2011-02-11T22:11:28Z

Linahan: /* brc36 21h35m32.6s +57d31m50s */

== brc36 21h35m32.6s +57d31m50s ==

* BRC 36 3 articles on ADS two are on star formation but none on SIMBAD

* 3 results from ADS: 1 abstract, 2 Chandra proposals; 0 results from Simbad, however, Aladin applet Simbad identifies (and IRAS-IRIS reveals) 6 YSOs, 10 IR sources, 2 Mol Cld, Rf Neb, Br Neb, Dk Neb, stars in nebulae, and stars in clouds.

* This looks like an interesting field. Lots going on (too much?) ADS: Garmire and Getman are both proposing to use Chandra to study this area. (x-rays)

--[[User:CJohnson|CJohnson]] 16:33, 9 February 2011 (PST)

Using SIMBAD, and searching under coordinates yields 83 objects mostly stars: 17 *iC, 13 TT*, 4 *, 1 **, 8 Y*O, 4 Em*, 1 Or*, 1 *i* (star in double system), 1 *IN (star in nebula), 16 IR sources, 3 smm, 5 Molecular cloud, 2 part of cloud, 1 cloud, 1 dark nebula, 1 bright nebula, 1 reflection nebula, and 1 radio source. One of the molecular clouds is the elephant trunk nebula.--[[User:Linahan|Linahan]] 13:20, 11 February 2011 (PST)

The elephant trunk nebula has 23 references. Here is a sampling of them.
#66 NAME ELEPHANT TRUNK NEBULA 519.38 MoC 21 36 +57.4
2009AJ....137.3685B  Astron. J., 137, 3685-3699 (2009)  An infrared census of star formation in the Horsehead nebula.  BOWLER B.P., WALLER W.H., MEGEATH S.T., PATTEN B.M. and TAMURA M.
2009AJ....138.1116S  Astron. J., 138, 1116-1136 (2009)  A Spitzer view of the young open cluster NGC 2264.  SUNG H., STAUFFER J.R. and BESSELL M.S.
2009ApJ...690..683R  Astrophys. J., 690, 683-705 (2009)  Properties of protostars in the Elephant Trunk in the globule IC 1396A.  REACH W.T., FAIED D., RHO J., BOOGERT A., TAPPE A., JARRETT T.H., MORRIS P., CAMBRESY L., PALLA F. and VALDETTARO R.
2009ApJ...694L..26G  Astrophys. J., 694, L26-L30 (2009)  Driving turbulence and triggering star formation by ionizing radiation.  GRITSCHNEDER M., NAAB T., WALCH S., BURKERT A. and HEITSCH F.
2009ApJ...702.1507M  Astrophys. J., 702, 1507-1529 (2009)  Mid-infrared variability of protostars in IC 1396A.  MORALES-CALDERON M., STAUFFER J.R., REBULL L., WHITNEY B.A., BARRADO Y NAVASCUES D., ARDILA D.R., SONG I., BROOKE T.Y., HARTMANN L. and CALVET N.
2008A&A...485..753H  Astron. Astrophys., 485, 753-763 (2008)  An infrared-submillimeter study of starforming regions selected by the ISOSS 170 {mu}m survey.  HENNEMANN M., BIRKMANN S.M., KRAUSE O. and LEMKE D.
2008ApJ...675.1352V  Astrophys. J., 675, 1352-1360 (2008)  High-resolution H_2_ O maser observations toward IRAS sources in bright-rimmed clouds.  VALDETTARO R., MIGENES V., TRINIDAD M.A., BRAND J. and PALLA F.
flags: (abstract)
2007PASJ...59S.443I  Publ. Astron. Soc. Jap., 59, 443-454 (2007)  AKARI infrared imaging of reflection nebulae IC4954 and IC4955.  ISHIHARA D., ONAKA T., KANEDA H., SUZUKI T., KATAZA H., SAKON I., OKADA Y., DOI Y., FUJISHIRO N., FUJIWARA H., ITA Y., KII T., KIM W., MAKIUTI S., MATSUMOTO T., MATSUHARA H., MURAKAMI H., NAKAGAWA T., OHYAMA Y., OYABU S., SERJEANT S., SHIBAI H., TAKAGI T., TANABE T., UEMIZU K., UENO M., USUI F., WADA T., WATARAI H. and YAMAMURA I.
--[[User:Linahan|Linahan]] 13:33, 11 February 2011 (PST)

#12 and #75 The two larges sources are both stars with 28 and 24 sources. respectively. Looks like it might be a star in the elephant trunk nebula because they have overlapping sources. HD 205794 243.93 *iC 21 35 43.8294 +57 28 03.484 B0.5V 28 and 75 HD 239710 560.65 *iN 21 36 41.0395 +57 30 08.260 B3V 24

Both reference: 2004ApJS..154..385R  Astrophys. J., Suppl. Ser., 154, 385-390 (2004)  Protostars in the Elephant Trunk nebula.  REACH W.T., RHO J., YOUNG E., MUZEROLLE J., FAJARDO-ACOSTA S., HARTMANN L., SICILIA-AGUILAR A., ALLEN L., CAREY S., CUILLANDRE J.-C., JARRETT T.H., LOWRANCE P., MARSTON A., NORIEGA-CRESPO A. and HURT R.L.--[[User:Linahan|Linahan]] 13:46, 11 February 2011 (PST)

Here is the summary of information on the clouds:
#28 [IS94] 1 354.07 MoC 21 35 43 +57 26.1
1994JApA...15..157I  J. Astrophys. Astron., 15, 157-163 (1994)  Observations of the bright-rimmed molecular clouds near the Cepheus OB 2 association.  INDRANI C. and SRIDHARAN T.K.
#29 [PGS95] 14 365.70 PoC 21 36 03.6 +57 27 23
1995ApJ...447..721P  Astrophys. J., 447, 721-741 (1995)  The large-scale structure, kinematics, and evolution of IC 1396.  PATEL N.A., GOLDSMITH P.F., SNELL R.L., HEZEL T. and XIE T.
#39 IRAS 21346+5714 410.43 Cld 21 36 12.4 +57 27 34 There are 11 sources but a lot of the same sources as elephant trunk.
1995Ap&SS.224..571S  Astrophys. Space Sci., 224, 571-572 (1995)  Searches for bright-rimmed clouds with IRAS point sources.  SUGITANI K. and OGURA K.
1991ApJS...77...59S  Astrophys. J., Suppl. Ser., 77, 59-66 (1991)  A catalog of bright-rimmed clouds with IRAS Point Sources: candidates for star formation by radiation-driven implosion. I. The Northern hemisphere.  SUGITANI K., FUKUI Y. and OGURA K.
#40 [IS94] 15 410.44 MoC 21 36 12 +57 27.5
1991ApJS...77...59S  Astrophys. J., Suppl. Ser., 77, 59-66 (1991)  A catalog of bright-rimmed clouds with IRAS Point Sources: candidates for star formation by radiation-driven implosion. I. The Northern hemisphere.  SUGITANI K., FUKUI Y. and OGURA K.

Target selection for brc36

2011-02-11T22:04:49Z

Linahan: /* brc36 21h35m32.6s +57d31m50s */

Target selection for brc36

2011-02-11T21:46:18Z

Linahan: /* brc36 21h35m32.6s +57d31m50s */

Target selection for brc36

2011-02-11T21:33:49Z

Linahan: /* brc36 21h35m32.6s +57d31m50s */

Target selection for brc36

2011-02-11T21:20:03Z

Linahan: /* brc36 21h35m32.6s +57d31m50s */

Target selection for brc34

2011-02-11T19:20:33Z

Linahan: /* brc34 21h32m51.2s +58d08m43s */

== brc34 21h32m51.2s +58d08m43s ==

* BRC 34 1 proposal to study by Garmire, nothing on SIMBAD

* 0 ADS abstracts; 0 Simbad citations.

* No object listed at (or near) these precise coordinates, however, AllSky Optical images reveal the clouds that were of interest to Lori. Parts of the cloud are labeled. The DSS2.POSSII image reveals 2 star clusters, a Cloud Dark Nebula, and 2 IR sources (one above & slightly to the right of the center of the image) Many hits on 2MASS

--[[User:CJohnson|CJohnson]] 16:28, 9 February 2011 (PST)

Using SIMBAD with the coordinates yields 23 targets: Dark nebula 2, Cloud 2, IR source 6, PoC (part of cloud) 3, UV source 1, MoC (molecular cloud) 1, Em* 1, *iC (star in cluster) 6 and smm (submillimetric source)1.
Starting with the most references:
# 14 HD 205510 439.13 *iC 21 33 41.7048 +58 11 45.234 has 12 references. I don't know if any are worth looking into but the last one might be a good archival source.
2006AstL...32..759G  Astron. Lett., 32, 759-771 (2006)  Pulkovo compilation of radial velocities for 35495 stars in a common system.  GONTCHAROV G.A.
1999A&A...343..446D  Astron. Astrophys., 343, 446-454 (1999)  Late A-type stars: new Stroemgren photometric calibrations of absolute magnitudes from Hipparcos.  DOMINGO A. and FIGUERAS F.
1999A&AS..137..451G  Astron. Astrophys., Suppl. Ser., 137, 451-456 (1999)  Radial velocities. IX. Measurements of 2800 B2-F5 stars for Hipparcos.  GRENIER S., BAYLAC M.-O., ROLLAND L., BURNAGE R., ARENOU F., BRIOT D., DELMAS F., DUFLOT M., GENTY V., GOMEZ A.E., HALBWACHS J.-L., MAROUARD M., OBLAK E. and SELLIER A.
1983A&AS...51..245N  Astron. Astrophys., Suppl. Ser., 51, 245-256 (1983)  Lists of photometric Am candidates.  NICOLET B.
1974RMxAA...1..175M  Rev. Mex. Astron. Astrofis., 1, 175-201 (1974)  Multicolor photometry of metallic-line stars. III. A photometric catalogue.  MENDOZA E.E.
1973A&AS...10..385H  Astron. Astrophys., Suppl. Ser., 10, 385-403 (1973)  Catalogue of Am stars with known spectral types.  HAUCK B.
1968ApJ...154..923S  Astrophys. J., 154, 923-931 (1968)  A spectroscopic and photometric investigation of the association Cepheus OB2.  SIMONSON S.C.
1967JO.....50..425B  J. Obs., 50, 425 (1967)  Observations spectrographiques d'etoiles A a spectre particulier et a raies metalliques.  BERTAUD C. and FLOQUET M.
1965JO.....48..211B  J. Obs., 48, 211 (1965)  Catalogue et bibliographie des etoiles A a spectre particulier.  BERTAUD C.
1960JO.....43..129B  J. Obs., 43, 129 (1960)  Catalogue et bibliographie des etoiles A a spectre particulier.  BERTAUD C.
1959JO.....42...45B  J. Obs., 42, 45 (1959)  Catalogue et bibliographie des etoiles a spectre particulier.  BERTAUD C.
1958TrRig...7...33A  Trudy Astrofiz. Lab. Riga, 7, 33-97 (1958)  Determination of magnitudes, color indices, and spectral classes of stars in an area centered on R.A.=21h24m, Dec=+58.5deg.  ALKSNIS A.

#16 has 11 sources and seems to be talking about the BRC. Some of the papers are refereced in BRC 27 so if I can figure out how to copy the link...JCMTSF J213332.0+580332 453.73 Cld 21 33 32.4 +58 03 28

2009MNRAS.400.1726M  Mon. Not. R. Astron. Soc., 400, 1726-1733 (2009)  CO observations towards bright-rimmed clouds.  MORGAN L.K., URQUHART J.S. and THOMPSON M.A.
2008A&A...477..557M  Astron. Astrophys., 477, 557-571 (2008)  A SCUBA survey of bright-rimmed clouds.  MORGAN L.K., THOMPSON M.A., URQUHART J.S. and WHITE G.J.
2008ApJS..175..277D  Astrophys. J., Suppl. Ser., 175, 277-295 (2008)  The SCUBA legacy catalogues: submillimeter-continuum objects detected by SCUBA.  DI FRANCESCO J., JOHNSTONE D., KIRK H., MacKENZIE T. and LEDWOSINSKA E.
2005A&A...443..535V  Astron. Astrophys., 443, 535-540 (2005)  H_2_O maser emission from bright rimmed clouds in the northern hemisphere.  VALDETTARO R., PALLA F., BRAND J. and CESARONI R.
2004A&A...426..535M  Astron. Astrophys., 426, 535-545 (2004)  A radio and mid-infrared survey of northern bright-rimmed clouds.  MORGAN L.K., THOMPSON M.A., URQUHART J.S., WHITE G.J. and MIAO J.
2002AJ....123.2597O  Astron. J., 123, 2597-2626 (2002)  H{alpha} emission stars and Herbig-Haro objects in the vicinity of bright-rimmed clouds.  OGURA K., SUGITANI K. and PICKLES A.
1997A&A...324..249L  Astron. Astrophys., 324, 249-262 (1997)  Cometary globules. III. Triggered star formation in IC 1848.  LEFLOCH B., LAZAREFF B. and CASTETS A.
1996A&A...309..581W  Astron. Astrophys., 309, 581-611 (1996)  The structure of the IC1396 region.  WEIKARD H., WOUTERLOOT J.G.A., CASTETS A., WINNEWISSER G. and SUGITANI K.
1995Ap&SS.224..571S  Astrophys. Space Sci., 224, 571-572 (1995)  Searches for bright-rimmed clouds with IRAS point sources.  SUGITANI K. and OGURA K.
1995MNRAS.276...57C  Mon. Not. R. Astron. Soc., 276, 57-73 (1995)  IRAS-selected Galactic star-forming regions. II. Water maser detections in the extended sample.  CODELLA C., PALUMBO G.G.C., PARESCHI G., SCAPPINI F., CASELLI P. and ATTOLINI M.R.
1991ApJS...77...59S  Astrophys. J., Suppl. Ser., 77, 59-66 (1991)  A catalog of bright-rimmed clouds with IRAS Point Sources: candidates for star formation by radiation-driven implosion. I. The Northern hemisphere.  SUGITANI K., FUKUI Y. and OGURA K.

#10 The next one has 5 sources LDN 1102 381.96 DNe 21 32.5 +58 03
2005A&A...432..575F  Astron. Astrophys., 432, 575-584 (2005)  Star formation in globules in IC 1396.  FROEBRICH D., SCHOLZ A., EISLOEFFEL J. and MURPHY G.C.
2005PASJ...57S...1D  Publ. Astron. Soc. Jap., 57, 1-368 (2005)  Atlas and catalog of dark clouds based on Digitized Sky Survey I.  DOBASHI K., UEHARA H., KANDORI R., SAKURAI T., KAIDEN M., UMEMOTO T. and SATO F.
2004A&A...418..131K  Astron. Astrophys., 418, 131-141 (2004)  Far-infrared loops in the 2nd Galactic Quadrant.  KISS C., MOOR A. and TOTH L.V.
2002A&A...383..631D  Astron. Astrophys., 383, 631-635 (2002)  A catalogue of dust clouds in the Galaxy.  DUTRA C.M. and BICA E.
1962ApJS....7....1L  Astrophys. J., Suppl. Ser., 7, 1-52 (1962)  Catalogue of dark nebulae.  LYNDS B.T.

#5 has 3 sources [G85] 3 330.83 PoC 21 32 59 +58 03.3
1993Afz....36..527G  Astrofizika, 36, 527-534 (1993)  Relationship between neutral hydrogen and radial systems of dark globules.  GYULBUDAGHIAN A.L.
1986Afz....24..201G  Astrofizika, 24, 201-203 (1986)  Radial systems of dark globules in the Association Cep OB2.  GYULBUDAGHIAN A.L., RODRIGUEZ L.F. and CANTO J.
1985Afz....23..295G  Astrofizika, 23, 295-306 (1985)  On the radial systems of dark globules.  GYULBUDAGHIAN A.L.

#6 has 2 Lan 435 336.39 UV 21 33 29.0 +58 11 17
2006PASP..118.1639L  Publ. Astron. Soc. Pac., 118, 1639-1647 (2006)  Proper motions of faint ultraviolet-bright sources in the Sandage two-color survey of the galactic plane.  LANNING H.H. and LEPINE S.
2000PASP..112..251L  Publ. Astron. Soc. Pac., 112, 251-263 (2000)  A finding list of faint UV-bright stars in the galactic plane. V.  LANNING H.H. and MEAKES M.

The rest have 1 or no source and many are pointing back to the same catalog or paper:
#1 TGU H590 164.50 DNe 21 32.9 +58 06 ~ 1 0 2005PASJ...57S...1D - Publ. Astron. Soc. Jap., 57, 1-368 (2005) - 17.03.05 01.02.10 February 2005
Atlas and catalog of dark clouds based on Digitized Sky Survey I.
DOBASHI K.; UEHARA H.; KANDORI R.; SAKURAI T.; KAIDEN M.; UMEMOTO T.; SATO F.

#2 [FSE2005] 16
177.28 Cld 21 33 +58.1 ~ 1 1
2005A&A...432..575F - Astron. Astrophys., 432, 575-584 (2005) - 15.03.05 02.12.05 March(III) 2005
Star formation in globules in IC 1396.
FROEBRICH D.; SCHOLZ A.; EISLOEFFEL J.; MURPHY G.C.

#11 JCMTSF J213332.7+580432 413.70 smm 21 33 32.7 +58 04 32
2008ApJS..175..277D  Astrophys. J., Suppl. Ser., 175, 277-295 (2008)  The SCUBA legacy catalogues: submillimeter-continuum objects detected by SCUBA.  DI FRANCESCO J., JOHNSTONE D., KIRK H., MacKENZIE T. and LEDWOSINSKA E.

#13 IRAS C21310+5749 436.65 IR 21 32.5 +58 02
1991ApJ...370..263S  Astrophys. J., 370, 263-271 (1991)  A search for embedded young stellar objects in and near the IC 1396 complex.  SCHWARTZ R.D., GYULBUDAGHIAN A.L. and WILKING B.A.

#17 2MASS J21332921+5802508 463.43 Em* 21 33 29.21 +58 02 50.9
2002AJ....123.2597O  Astron. J., 123, 2597-2626 (2002)  H{alpha} emission stars and Herbig-Haro objects in the vicinity of bright-rimmed clouds.  OGURA K., SUGITANI K. and PICKLES A.

#18 GSC 03975-00282 508.26 *iC 21 33 36.91 +58 02 46.6 K:...
1958TrRig...7...33A  Trudy Astrofiz. Lab. Riga, 7, 33-97 (1958)  Determination of magnitudes, color indices, and spectral classes of stars in an area centered on R.A.=21h24m, Dec=+58.5deg.  ALKSNIS A

#19 [PGS95] 9 520.32 PoC 21 33 07.5 +58 00 19 ~ 1 0 1995ApJ...447..721P  Astrophys. J., 447, 721-741 (1995)  The large-scale structure, kinematics, and evolution of IC 1396.  PATEL N.A., GOLDSMITH P.F., SNELL R.L., HEZEL T. and XIE T.

#20 BD+57 2346 566.01 *iC 21 32 29.6670 +58 17 42.840 K2
1958TrRig...7...33A  Trudy Astrofiz. Lab. Riga, 7, 33-97 (1958)  Determination of magnitudes, color indices, and spectral classes of stars in an area centered on R.A.=21h24m, Dec=+58.5deg.  ALKSNIS A.

#21 Cl* Trumpler 37 KUN 170
567.55 *iC 21 33 17.02 +57 59 53.7
1990Ap&SS.174...13K  Astrophys. Space Sci., 174, 13 (1990)  Solar-type stars in Cepheus OB 2: H-alpha emission stars and IRAS point sources.  KUN M. and PASZTOR L

# 23 Cl* Trumpler 37 KUN 307 590.18 *iC 21 34 05.29 +58 07 38.8
1990Ap&SS.174...13K  Astrophys. Space Sci., 174, 13 (1990)  Solar-type stars in Cepheus OB 2: H-alpha emission stars and IRAS point sources.  KUN M. and PASZTOR L

The rest have no sources:
#3 IRAS 21319+5755
268.14 IR 21 33 25.0 +58 08 26
#4 IRAS 21316+5751
283.31 IR 21 33 10.2 +58 04 43
#8 IRAS 21320+5752
373.69 IR 21 33 33.4 +58 05 56
#12 IRAS 21314+5802
429.35 IR 21 32 55.5 +58 15 51
--[[User:Linahan|Linahan]] 11:20, 11 February 2011 (PST)

Target selection for brc34

2011-02-11T19:17:51Z

Linahan: /* brc34 21h32m51.2s +58d08m43s */

== brc34 21h32m51.2s +58d08m43s ==

* BRC 34 1 proposal to study by Garmire, nothing on SIMBAD

* 0 ADS abstracts; 0 Simbad citations.

* No object listed at (or near) these precise coordinates, however, AllSky Optical images reveal the clouds that were of interest to Lori. Parts of the cloud are labeled. The DSS2.POSSII image reveals 2 star clusters, a Cloud Dark Nebula, and 2 IR sources (one above & slightly to the right of the center of the image) Many hits on 2MASS

--[[User:CJohnson|CJohnson]] 16:28, 9 February 2011 (PST)

Using SIMBAD with the coordinates yields 23 targets: Dark nebula 2, Cloud 2, IR source 6, PoC (part of cloud) 3, UV source 1, MoC (molecular cloud) 1, Em* 1, *iC (star in cluster) 6 and smm (submillimetric source)1.
Starting with the most references:
# 14 HD 205510 439.13 *iC 21 33 41.7048 +58 11 45.234 has 12 references. I don't know if any are worth looking into but the last one might be a good archival source.
2006AstL...32..759G  Astron. Lett., 32, 759-771 (2006)  Pulkovo compilation of radial velocities for 35495 stars in a common system.  GONTCHAROV G.A.
1999A&A...343..446D  Astron. Astrophys., 343, 446-454 (1999)  Late A-type stars: new Stroemgren photometric calibrations of absolute magnitudes from Hipparcos.  DOMINGO A. and FIGUERAS F.
1999A&AS..137..451G  Astron. Astrophys., Suppl. Ser., 137, 451-456 (1999)  Radial velocities. IX. Measurements of 2800 B2-F5 stars for Hipparcos.  GRENIER S., BAYLAC M.-O., ROLLAND L., BURNAGE R., ARENOU F., BRIOT D., DELMAS F., DUFLOT M., GENTY V., GOMEZ A.E., HALBWACHS J.-L., MAROUARD M., OBLAK E. and SELLIER A.
1983A&AS...51..245N  Astron. Astrophys., Suppl. Ser., 51, 245-256 (1983)  Lists of photometric Am candidates.  NICOLET B.
1974RMxAA...1..175M  Rev. Mex. Astron. Astrofis., 1, 175-201 (1974)  Multicolor photometry of metallic-line stars. III. A photometric catalogue.  MENDOZA E.E.
1973A&AS...10..385H  Astron. Astrophys., Suppl. Ser., 10, 385-403 (1973)  Catalogue of Am stars with known spectral types.  HAUCK B.
1968ApJ...154..923S  Astrophys. J., 154, 923-931 (1968)  A spectroscopic and photometric investigation of the association Cepheus OB2.  SIMONSON S.C.
1967JO.....50..425B  J. Obs., 50, 425 (1967)  Observations spectrographiques d'etoiles A a spectre particulier et a raies metalliques.  BERTAUD C. and FLOQUET M.
1965JO.....48..211B  J. Obs., 48, 211 (1965)  Catalogue et bibliographie des etoiles A a spectre particulier.  BERTAUD C.
1960JO.....43..129B  J. Obs., 43, 129 (1960)  Catalogue et bibliographie des etoiles A a spectre particulier.  BERTAUD C.
1959JO.....42...45B  J. Obs., 42, 45 (1959)  Catalogue et bibliographie des etoiles a spectre particulier.  BERTAUD C.
1958TrRig...7...33A  Trudy Astrofiz. Lab. Riga, 7, 33-97 (1958)  Determination of magnitudes, color indices, and spectral classes of stars in an area centered on R.A.=21h24m, Dec=+58.5deg.  ALKSNIS A.

#16 has 11 sources and seems to be talking about the BRC. JCMTSF J213332.0+580332 453.73 Cld 21 33 32.4 +58 03 28

2009MNRAS.400.1726M  Mon. Not. R. Astron. Soc., 400, 1726-1733 (2009)  CO observations towards bright-rimmed clouds.  MORGAN L.K., URQUHART J.S. and THOMPSON M.A.
2008A&A...477..557M  Astron. Astrophys., 477, 557-571 (2008)  A SCUBA survey of bright-rimmed clouds.  MORGAN L.K., THOMPSON M.A., URQUHART J.S. and WHITE G.J.
2008ApJS..175..277D  Astrophys. J., Suppl. Ser., 175, 277-295 (2008)  The SCUBA legacy catalogues: submillimeter-continuum objects detected by SCUBA.  DI FRANCESCO J., JOHNSTONE D., KIRK H., MacKENZIE T. and LEDWOSINSKA E.
2005A&A...443..535V  Astron. Astrophys., 443, 535-540 (2005)  H_2_O maser emission from bright rimmed clouds in the northern hemisphere.  VALDETTARO R., PALLA F., BRAND J. and CESARONI R.
2004A&A...426..535M  Astron. Astrophys., 426, 535-545 (2004)  A radio and mid-infrared survey of northern bright-rimmed clouds.  MORGAN L.K., THOMPSON M.A., URQUHART J.S., WHITE G.J. and MIAO J.
2002AJ....123.2597O  Astron. J., 123, 2597-2626 (2002)  H{alpha} emission stars and Herbig-Haro objects in the vicinity of bright-rimmed clouds.  OGURA K., SUGITANI K. and PICKLES A.
1997A&A...324..249L  Astron. Astrophys., 324, 249-262 (1997)  Cometary globules. III. Triggered star formation in IC 1848.  LEFLOCH B., LAZAREFF B. and CASTETS A.
1996A&A...309..581W  Astron. Astrophys., 309, 581-611 (1996)  The structure of the IC1396 region.  WEIKARD H., WOUTERLOOT J.G.A., CASTETS A., WINNEWISSER G. and SUGITANI K.
1995Ap&SS.224..571S  Astrophys. Space Sci., 224, 571-572 (1995)  Searches for bright-rimmed clouds with IRAS point sources.  SUGITANI K. and OGURA K.
1995MNRAS.276...57C  Mon. Not. R. Astron. Soc., 276, 57-73 (1995)  IRAS-selected Galactic star-forming regions. II. Water maser detections in the extended sample.  CODELLA C., PALUMBO G.G.C., PARESCHI G., SCAPPINI F., CASELLI P. and ATTOLINI M.R.
1991ApJS...77...59S  Astrophys. J., Suppl. Ser., 77, 59-66 (1991)  A catalog of bright-rimmed clouds with IRAS Point Sources: candidates for star formation by radiation-driven implosion. I. The Northern hemisphere.  SUGITANI K., FUKUI Y. and OGURA K.

#10 The next one has 5 sources0 LDN 1102 381.96 DNe 21 32.5 +58 03
2005A&A...432..575F  Astron. Astrophys., 432, 575-584 (2005)  Star formation in globules in IC 1396.  FROEBRICH D., SCHOLZ A., EISLOEFFEL J. and MURPHY G.C.
2005PASJ...57S...1D  Publ. Astron. Soc. Jap., 57, 1-368 (2005)  Atlas and catalog of dark clouds based on Digitized Sky Survey I.  DOBASHI K., UEHARA H., KANDORI R., SAKURAI T., KAIDEN M., UMEMOTO T. and SATO F.
2004A&A...418..131K  Astron. Astrophys., 418, 131-141 (2004)  Far-infrared loops in the 2nd Galactic Quadrant.  KISS C., MOOR A. and TOTH L.V.
2002A&A...383..631D  Astron. Astrophys., 383, 631-635 (2002)  A catalogue of dust clouds in the Galaxy.  DUTRA C.M. and BICA E.
1962ApJS....7....1L  Astrophys. J., Suppl. Ser., 7, 1-52 (1962)  Catalogue of dark nebulae.  LYNDS B.T.

--[[User:Linahan|Linahan]] 10:52, 11 February 2011 (PST)

#5 has 3 sources [G85] 3 330.83 PoC 21 32 59 +58 03.3
1993Afz....36..527G  Astrofizika, 36, 527-534 (1993)  Relationship between neutral hydrogen and radial systems of dark globules.  GYULBUDAGHIAN A.L.
1986Afz....24..201G  Astrofizika, 24, 201-203 (1986)  Radial systems of dark globules in the Association Cep OB2.  GYULBUDAGHIAN A.L., RODRIGUEZ L.F. and CANTO J.
1985Afz....23..295G  Astrofizika, 23, 295-306 (1985)  On the radial systems of dark globules.  GYULBUDAGHIAN A.L.

#6 has 2 Lan 435 336.39 UV 21 33 29.0 +58 11 17
2006PASP..118.1639L  Publ. Astron. Soc. Pac., 118, 1639-1647 (2006)  Proper motions of faint ultraviolet-bright sources in the Sandage two-color survey of the galactic plane.  LANNING H.H. and LEPINE S.
2000PASP..112..251L  Publ. Astron. Soc. Pac., 112, 251-263 (2000)  A finding list of faint UV-bright stars in the galactic plane. V.  LANNING H.H. and MEAKES M.

The rest have 1 or no source and many are pointing back to the same catalog or paper:
#1 TGU H590 164.50 DNe 21 32.9 +58 06 ~ 1 0 2005PASJ...57S...1D - Publ. Astron. Soc. Jap., 57, 1-368 (2005) - 17.03.05 01.02.10 February 2005
Atlas and catalog of dark clouds based on Digitized Sky Survey I.
DOBASHI K.; UEHARA H.; KANDORI R.; SAKURAI T.; KAIDEN M.; UMEMOTO T.; SATO F.

#2 [FSE2005] 16
177.28 Cld 21 33 +58.1 ~ 1 1
2005A&A...432..575F - Astron. Astrophys., 432, 575-584 (2005) - 15.03.05 02.12.05 March(III) 2005
Star formation in globules in IC 1396.
FROEBRICH D.; SCHOLZ A.; EISLOEFFEL J.; MURPHY G.C.

#11 JCMTSF J213332.7+580432 413.70 smm 21 33 32.7 +58 04 32
2008ApJS..175..277D  Astrophys. J., Suppl. Ser., 175, 277-295 (2008)  The SCUBA legacy catalogues: submillimeter-continuum objects detected by SCUBA.  DI FRANCESCO J., JOHNSTONE D., KIRK H., MacKENZIE T. and LEDWOSINSKA E.

#13 IRAS C21310+5749 436.65 IR 21 32.5 +58 02
1991ApJ...370..263S  Astrophys. J., 370, 263-271 (1991)  A search for embedded young stellar objects in and near the IC 1396 complex.  SCHWARTZ R.D., GYULBUDAGHIAN A.L. and WILKING B.A.

#17 2MASS J21332921+5802508 463.43 Em* 21 33 29.21 +58 02 50.9
2002AJ....123.2597O  Astron. J., 123, 2597-2626 (2002)  H{alpha} emission stars and Herbig-Haro objects in the vicinity of bright-rimmed clouds.  OGURA K., SUGITANI K. and PICKLES A.

#18 GSC 03975-00282 508.26 *iC 21 33 36.91 +58 02 46.6 K:...
1958TrRig...7...33A  Trudy Astrofiz. Lab. Riga, 7, 33-97 (1958)  Determination of magnitudes, color indices, and spectral classes of stars in an area centered on R.A.=21h24m, Dec=+58.5deg.  ALKSNIS A

#19 [PGS95] 9 520.32 PoC 21 33 07.5 +58 00 19 ~ 1 0 1995ApJ...447..721P  Astrophys. J., 447, 721-741 (1995)  The large-scale structure, kinematics, and evolution of IC 1396.  PATEL N.A., GOLDSMITH P.F., SNELL R.L., HEZEL T. and XIE T.

#20 BD+57 2346 566.01 *iC 21 32 29.6670 +58 17 42.840 K2
1958TrRig...7...33A  Trudy Astrofiz. Lab. Riga, 7, 33-97 (1958)  Determination of magnitudes, color indices, and spectral classes of stars in an area centered on R.A.=21h24m, Dec=+58.5deg.  ALKSNIS A.

#21 Cl* Trumpler 37 KUN 170
567.55 *iC 21 33 17.02 +57 59 53.7
1990Ap&SS.174...13K  Astrophys. Space Sci., 174, 13 (1990)  Solar-type stars in Cepheus OB 2: H-alpha emission stars and IRAS point sources.  KUN M. and PASZTOR L

# 23 Cl* Trumpler 37 KUN 307 590.18 *iC 21 34 05.29 +58 07 38.8
1990Ap&SS.174...13K  Astrophys. Space Sci., 174, 13 (1990)  Solar-type stars in Cepheus OB 2: H-alpha emission stars and IRAS point sources.  KUN M. and PASZTOR L

The rest have no sources:
#3 IRAS 21319+5755
268.14 IR 21 33 25.0 +58 08 26
#4 IRAS 21316+5751
283.31 IR 21 33 10.2 +58 04 43
#8 IRAS 21320+5752
373.69 IR 21 33 33.4 +58 05 56

Target selection for brc34

2011-02-11T19:16:26Z

Linahan: /* brc34 21h32m51.2s +58d08m43s */

== brc34 21h32m51.2s +58d08m43s ==

* BRC 34 1 proposal to study by Garmire, nothing on SIMBAD

* 0 ADS abstracts; 0 Simbad citations.

* No object listed at (or near) these precise coordinates, however, AllSky Optical images reveal the clouds that were of interest to Lori. Parts of the cloud are labeled. The DSS2.POSSII image reveals 2 star clusters, a Cloud Dark Nebula, and 2 IR sources (one above & slightly to the right of the center of the image) Many hits on 2MASS

--[[User:CJohnson|CJohnson]] 16:28, 9 February 2011 (PST)

Using SIMBAD with the coordinates yields 23 targets: Dark nebula 2, Cloud 2, IR source 6, PoC (part of cloud) 3, UV source 1, MoC (molecular cloud) 1, Em* 1, *iC (star in cluster) 6 and smm (submillimetric source)1.
Starting with the most references:
# 14 HD 205510 439.13 *iC 21 33 41.7048 +58 11 45.234 has 12 references. I don't know if any are worth looking into but the last one might be a good archival source.
2006AstL...32..759G  Astron. Lett., 32, 759-771 (2006)  Pulkovo compilation of radial velocities for 35495 stars in a common system.  GONTCHAROV G.A.
1999A&A...343..446D  Astron. Astrophys., 343, 446-454 (1999)  Late A-type stars: new Stroemgren photometric calibrations of absolute magnitudes from Hipparcos.  DOMINGO A. and FIGUERAS F.
1999A&AS..137..451G  Astron. Astrophys., Suppl. Ser., 137, 451-456 (1999)  Radial velocities. IX. Measurements of 2800 B2-F5 stars for Hipparcos.  GRENIER S., BAYLAC M.-O., ROLLAND L., BURNAGE R., ARENOU F., BRIOT D., DELMAS F., DUFLOT M., GENTY V., GOMEZ A.E., HALBWACHS J.-L., MAROUARD M., OBLAK E. and SELLIER A.
1983A&AS...51..245N  Astron. Astrophys., Suppl. Ser., 51, 245-256 (1983)  Lists of photometric Am candidates.  NICOLET B.
1974RMxAA...1..175M  Rev. Mex. Astron. Astrofis., 1, 175-201 (1974)  Multicolor photometry of metallic-line stars. III. A photometric catalogue.  MENDOZA E.E.
1973A&AS...10..385H  Astron. Astrophys., Suppl. Ser., 10, 385-403 (1973)  Catalogue of Am stars with known spectral types.  HAUCK B.
1968ApJ...154..923S  Astrophys. J., 154, 923-931 (1968)  A spectroscopic and photometric investigation of the association Cepheus OB2.  SIMONSON S.C.
1967JO.....50..425B  J. Obs., 50, 425 (1967)  Observations spectrographiques d'etoiles A a spectre particulier et a raies metalliques.  BERTAUD C. and FLOQUET M.
1965JO.....48..211B  J. Obs., 48, 211 (1965)  Catalogue et bibliographie des etoiles A a spectre particulier.  BERTAUD C.
1960JO.....43..129B  J. Obs., 43, 129 (1960)  Catalogue et bibliographie des etoiles A a spectre particulier.  BERTAUD C.
1959JO.....42...45B  J. Obs., 42, 45 (1959)  Catalogue et bibliographie des etoiles a spectre particulier.  BERTAUD C.
1958TrRig...7...33A  Trudy Astrofiz. Lab. Riga, 7, 33-97 (1958)  Determination of magnitudes, color indices, and spectral classes of stars in an area centered on R.A.=21h24m, Dec=+58.5deg.  ALKSNIS A.

#16 has 11 sources and seems to be talking about the BRC. JCMTSF J213332.0+580332 453.73 Cld 21 33 32.4 +58 03 28

2009MNRAS.400.1726M  Mon. Not. R. Astron. Soc., 400, 1726-1733 (2009)  CO observations towards bright-rimmed clouds.  MORGAN L.K., URQUHART J.S. and THOMPSON M.A.
2008A&A...477..557M  Astron. Astrophys., 477, 557-571 (2008)  A SCUBA survey of bright-rimmed clouds.  MORGAN L.K., THOMPSON M.A., URQUHART J.S. and WHITE G.J.
2008ApJS..175..277D  Astrophys. J., Suppl. Ser., 175, 277-295 (2008)  The SCUBA legacy catalogues: submillimeter-continuum objects detected by SCUBA.  DI FRANCESCO J., JOHNSTONE D., KIRK H., MacKENZIE T. and LEDWOSINSKA E.
2005A&A...443..535V  Astron. Astrophys., 443, 535-540 (2005)  H_2_O maser emission from bright rimmed clouds in the northern hemisphere.  VALDETTARO R., PALLA F., BRAND J. and CESARONI R.
2004A&A...426..535M  Astron. Astrophys., 426, 535-545 (2004)  A radio and mid-infrared survey of northern bright-rimmed clouds.  MORGAN L.K., THOMPSON M.A., URQUHART J.S., WHITE G.J. and MIAO J.
2002AJ....123.2597O  Astron. J., 123, 2597-2626 (2002)  H{alpha} emission stars and Herbig-Haro objects in the vicinity of bright-rimmed clouds.  OGURA K., SUGITANI K. and PICKLES A.
1997A&A...324..249L  Astron. Astrophys., 324, 249-262 (1997)  Cometary globules. III. Triggered star formation in IC 1848.  LEFLOCH B., LAZAREFF B. and CASTETS A.
1996A&A...309..581W  Astron. Astrophys., 309, 581-611 (1996)  The structure of the IC1396 region.  WEIKARD H., WOUTERLOOT J.G.A., CASTETS A., WINNEWISSER G. and SUGITANI K.
1995Ap&SS.224..571S  Astrophys. Space Sci., 224, 571-572 (1995)  Searches for bright-rimmed clouds with IRAS point sources.  SUGITANI K. and OGURA K.
1995MNRAS.276...57C  Mon. Not. R. Astron. Soc., 276, 57-73 (1995)  IRAS-selected Galactic star-forming regions. II. Water maser detections in the extended sample.  CODELLA C., PALUMBO G.G.C., PARESCHI G., SCAPPINI F., CASELLI P. and ATTOLINI M.R.
1991ApJS...77...59S  Astrophys. J., Suppl. Ser., 77, 59-66 (1991)  A catalog of bright-rimmed clouds with IRAS Point Sources: candidates for star formation by radiation-driven implosion. I. The Northern hemisphere.  SUGITANI K., FUKUI Y. and OGURA K.

#10 The next one has 5 sources0 LDN 1102 381.96 DNe 21 32.5 +58 03
2005A&A...432..575F  Astron. Astrophys., 432, 575-584 (2005)  Star formation in globules in IC 1396.  FROEBRICH D., SCHOLZ A., EISLOEFFEL J. and MURPHY G.C.
2005PASJ...57S...1D  Publ. Astron. Soc. Jap., 57, 1-368 (2005)  Atlas and catalog of dark clouds based on Digitized Sky Survey I.  DOBASHI K., UEHARA H., KANDORI R., SAKURAI T., KAIDEN M., UMEMOTO T. and SATO F.
2004A&A...418..131K  Astron. Astrophys., 418, 131-141 (2004)  Far-infrared loops in the 2nd Galactic Quadrant.  KISS C., MOOR A. and TOTH L.V.
2002A&A...383..631D  Astron. Astrophys., 383, 631-635 (2002)  A catalogue of dust clouds in the Galaxy.  DUTRA C.M. and BICA E.
1962ApJS....7....1L  Astrophys. J., Suppl. Ser., 7, 1-52 (1962)  Catalogue of dark nebulae.  LYNDS B.T.

--[[User:Linahan|Linahan]] 10:52, 11 February 2011 (PST)

#5 has 3 sources [G85] 3 330.83 PoC 21 32 59 +58 03.3
1993Afz....36..527G  Astrofizika, 36, 527-534 (1993)  Relationship between neutral hydrogen and radial systems of dark globules.  GYULBUDAGHIAN A.L.
1986Afz....24..201G  Astrofizika, 24, 201-203 (1986)  Radial systems of dark globules in the Association Cep OB2.  GYULBUDAGHIAN A.L., RODRIGUEZ L.F. and CANTO J.
1985Afz....23..295G  Astrofizika, 23, 295-306 (1985)  On the radial systems of dark globules.  GYULBUDAGHIAN A.L.

#6 has 2 Lan 435 336.39 UV 21 33 29.0 +58 11 17
2006PASP..118.1639L  Publ. Astron. Soc. Pac., 118, 1639-1647 (2006)  Proper motions of faint ultraviolet-bright sources in the Sandage two-color survey of the galactic plane.  LANNING H.H. and LEPINE S.
2000PASP..112..251L  Publ. Astron. Soc. Pac., 112, 251-263 (2000)  A finding list of faint UV-bright stars in the galactic plane. V.  LANNING H.H. and MEAKES M.

The rest have 1 or no source and many are pointing back to the same catalog or paper:
#1 TGU H590 164.50 DNe 21 32.9 +58 06 ~ 1 0 2005PASJ...57S...1D - Publ. Astron. Soc. Jap., 57, 1-368 (2005) - 17.03.05 01.02.10 February 2005
Atlas and catalog of dark clouds based on Digitized Sky Survey I.
DOBASHI K.; UEHARA H.; KANDORI R.; SAKURAI T.; KAIDEN M.; UMEMOTO T.; SATO F.

#2 [FSE2005] 16
177.28 Cld 21 33 +58.1 ~ 1 1
2005A&A...432..575F - Astron. Astrophys., 432, 575-584 (2005) - 15.03.05 02.12.05 March(III) 2005
Star formation in globules in IC 1396.
FROEBRICH D.; SCHOLZ A.; EISLOEFFEL J.; MURPHY G.C.

#11 JCMTSF J213332.7+580432 413.70 smm 21 33 32.7 +58 04 32
2008ApJS..175..277D  Astrophys. J., Suppl. Ser., 175, 277-295 (2008)  The SCUBA legacy catalogues: submillimeter-continuum objects detected by SCUBA.  DI FRANCESCO J., JOHNSTONE D., KIRK H., MacKENZIE T. and LEDWOSINSKA E.

#13 IRAS C21310+5749 436.65 IR 21 32.5 +58 02
1991ApJ...370..263S  Astrophys. J., 370, 263-271 (1991)  A search for embedded young stellar objects in and near the IC 1396 complex.  SCHWARTZ R.D., GYULBUDAGHIAN A.L. and WILKING B.A.

#17 2MASS J21332921+5802508 463.43 Em* 21 33 29.21 +58 02 50.9
2002AJ....123.2597O  Astron. J., 123, 2597-2626 (2002)  H{alpha} emission stars and Herbig-Haro objects in the vicinity of bright-rimmed clouds.  OGURA K., SUGITANI K. and PICKLES A.

#18 GSC 03975-00282 508.26 *iC 21 33 36.91 +58 02 46.6 K:...
1958TrRig...7...33A  Trudy Astrofiz. Lab. Riga, 7, 33-97 (1958)  Determination of magnitudes, color indices, and spectral classes of stars in an area centered on R.A.=21h24m, Dec=+58.5deg.  ALKSNIS A

#19 [PGS95] 9 520.32 PoC 21 33 07.5 +58 00 19 ~ 1 0 1995ApJ...447..721P  Astrophys. J., 447, 721-741 (1995)  The large-scale structure, kinematics, and evolution of IC 1396.  PATEL N.A., GOLDSMITH P.F., SNELL R.L., HEZEL T. and XIE T.

#20 BD+57 2346 566.01 *iC 21 32 29.6670 +58 17 42.840 K2
1958TrRig...7...33A  Trudy Astrofiz. Lab. Riga, 7, 33-97 (1958)  Determination of magnitudes, color indices, and spectral classes of stars in an area centered on R.A.=21h24m, Dec=+58.5deg.  ALKSNIS A.

#21 Cl* Trumpler 37 KUN 170
567.55 *iC 21 33 17.02 +57 59 53.7
1990Ap&SS.174...13K  Astrophys. Space Sci., 174, 13 (1990)  Solar-type stars in Cepheus OB 2: H-alpha emission stars and IRAS point sources.  KUN M. and PASZTOR L

# 23 Cl* Trumpler 37 KUN 307 590.18 *iC 21 34 05.29 +58 07 38.8
1990Ap&SS.174...13K  Astrophys. Space Sci., 174, 13 (1990)  Solar-type stars in Cepheus OB 2: H-alpha emission stars and IRAS point sources.  KUN M. and PASZTOR L

The rest have no sources:

Target selection for brc34

2011-02-11T19:15:36Z

Linahan: /* brc34 21h32m51.2s +58d08m43s */

== brc34 21h32m51.2s +58d08m43s ==

* BRC 34 1 proposal to study by Garmire, nothing on SIMBAD

* 0 ADS abstracts; 0 Simbad citations.

* No object listed at (or near) these precise coordinates, however, AllSky Optical images reveal the clouds that were of interest to Lori. Parts of the cloud are labeled. The DSS2.POSSII image reveals 2 star clusters, a Cloud Dark Nebula, and 2 IR sources (one above & slightly to the right of the center of the image) Many hits on 2MASS

--[[User:CJohnson|CJohnson]] 16:28, 9 February 2011 (PST)

Using SIMBAD with the coordinates yields 23 targets: Dark nebula 2, Cloud 2, IR source 6, PoC (part of cloud) 3, UV source 1, MoC (molecular cloud) 1, Em* 1, *iC (star in cluster) 6 and smm (submillimetric source)1.
Starting with the most references:
# 14 HD 205510 439.13 *iC 21 33 41.7048 +58 11 45.234 has 12 references. I don't know if any are worth looking into but the last one might be a good archival source.
2006AstL...32..759G  Astron. Lett., 32, 759-771 (2006)  Pulkovo compilation of radial velocities for 35495 stars in a common system.  GONTCHAROV G.A.
1999A&A...343..446D  Astron. Astrophys., 343, 446-454 (1999)  Late A-type stars: new Stroemgren photometric calibrations of absolute magnitudes from Hipparcos.  DOMINGO A. and FIGUERAS F.
1999A&AS..137..451G  Astron. Astrophys., Suppl. Ser., 137, 451-456 (1999)  Radial velocities. IX. Measurements of 2800 B2-F5 stars for Hipparcos.  GRENIER S., BAYLAC M.-O., ROLLAND L., BURNAGE R., ARENOU F., BRIOT D., DELMAS F., DUFLOT M., GENTY V., GOMEZ A.E., HALBWACHS J.-L., MAROUARD M., OBLAK E. and SELLIER A.
1983A&AS...51..245N  Astron. Astrophys., Suppl. Ser., 51, 245-256 (1983)  Lists of photometric Am candidates.  NICOLET B.
1974RMxAA...1..175M  Rev. Mex. Astron. Astrofis., 1, 175-201 (1974)  Multicolor photometry of metallic-line stars. III. A photometric catalogue.  MENDOZA E.E.
1973A&AS...10..385H  Astron. Astrophys., Suppl. Ser., 10, 385-403 (1973)  Catalogue of Am stars with known spectral types.  HAUCK B.
1968ApJ...154..923S  Astrophys. J., 154, 923-931 (1968)  A spectroscopic and photometric investigation of the association Cepheus OB2.  SIMONSON S.C.
1967JO.....50..425B  J. Obs., 50, 425 (1967)  Observations spectrographiques d'etoiles A a spectre particulier et a raies metalliques.  BERTAUD C. and FLOQUET M.
1965JO.....48..211B  J. Obs., 48, 211 (1965)  Catalogue et bibliographie des etoiles A a spectre particulier.  BERTAUD C.
1960JO.....43..129B  J. Obs., 43, 129 (1960)  Catalogue et bibliographie des etoiles A a spectre particulier.  BERTAUD C.
1959JO.....42...45B  J. Obs., 42, 45 (1959)  Catalogue et bibliographie des etoiles a spectre particulier.  BERTAUD C.
1958TrRig...7...33A  Trudy Astrofiz. Lab. Riga, 7, 33-97 (1958)  Determination of magnitudes, color indices, and spectral classes of stars in an area centered on R.A.=21h24m, Dec=+58.5deg.  ALKSNIS A.

#16 has 11 sources and seems to be talking about the BRC. JCMTSF J213332.0+580332 453.73 Cld 21 33 32.4 +58 03 28

2009MNRAS.400.1726M  Mon. Not. R. Astron. Soc., 400, 1726-1733 (2009)  CO observations towards bright-rimmed clouds.  MORGAN L.K., URQUHART J.S. and THOMPSON M.A.
2008A&A...477..557M  Astron. Astrophys., 477, 557-571 (2008)  A SCUBA survey of bright-rimmed clouds.  MORGAN L.K., THOMPSON M.A., URQUHART J.S. and WHITE G.J.
2008ApJS..175..277D  Astrophys. J., Suppl. Ser., 175, 277-295 (2008)  The SCUBA legacy catalogues: submillimeter-continuum objects detected by SCUBA.  DI FRANCESCO J., JOHNSTONE D., KIRK H., MacKENZIE T. and LEDWOSINSKA E.
2005A&A...443..535V  Astron. Astrophys., 443, 535-540 (2005)  H_2_O maser emission from bright rimmed clouds in the northern hemisphere.  VALDETTARO R., PALLA F., BRAND J. and CESARONI R.
2004A&A...426..535M  Astron. Astrophys., 426, 535-545 (2004)  A radio and mid-infrared survey of northern bright-rimmed clouds.  MORGAN L.K., THOMPSON M.A., URQUHART J.S., WHITE G.J. and MIAO J.
2002AJ....123.2597O  Astron. J., 123, 2597-2626 (2002)  H{alpha} emission stars and Herbig-Haro objects in the vicinity of bright-rimmed clouds.  OGURA K., SUGITANI K. and PICKLES A.
1997A&A...324..249L  Astron. Astrophys., 324, 249-262 (1997)  Cometary globules. III. Triggered star formation in IC 1848.  LEFLOCH B., LAZAREFF B. and CASTETS A.
1996A&A...309..581W  Astron. Astrophys., 309, 581-611 (1996)  The structure of the IC1396 region.  WEIKARD H., WOUTERLOOT J.G.A., CASTETS A., WINNEWISSER G. and SUGITANI K.
1995Ap&SS.224..571S  Astrophys. Space Sci., 224, 571-572 (1995)  Searches for bright-rimmed clouds with IRAS point sources.  SUGITANI K. and OGURA K.
1995MNRAS.276...57C  Mon. Not. R. Astron. Soc., 276, 57-73 (1995)  IRAS-selected Galactic star-forming regions. II. Water maser detections in the extended sample.  CODELLA C., PALUMBO G.G.C., PARESCHI G., SCAPPINI F., CASELLI P. and ATTOLINI M.R.
1991ApJS...77...59S  Astrophys. J., Suppl. Ser., 77, 59-66 (1991)  A catalog of bright-rimmed clouds with IRAS Point Sources: candidates for star formation by radiation-driven implosion. I. The Northern hemisphere.  SUGITANI K., FUKUI Y. and OGURA K.

#10 The next one has 5 sources0 LDN 1102 381.96 DNe 21 32.5 +58 03
2005A&A...432..575F  Astron. Astrophys., 432, 575-584 (2005)  Star formation in globules in IC 1396.  FROEBRICH D., SCHOLZ A., EISLOEFFEL J. and MURPHY G.C.
2005PASJ...57S...1D  Publ. Astron. Soc. Jap., 57, 1-368 (2005)  Atlas and catalog of dark clouds based on Digitized Sky Survey I.  DOBASHI K., UEHARA H., KANDORI R., SAKURAI T., KAIDEN M., UMEMOTO T. and SATO F.
2004A&A...418..131K  Astron. Astrophys., 418, 131-141 (2004)  Far-infrared loops in the 2nd Galactic Quadrant.  KISS C., MOOR A. and TOTH L.V.
2002A&A...383..631D  Astron. Astrophys., 383, 631-635 (2002)  A catalogue of dust clouds in the Galaxy.  DUTRA C.M. and BICA E.
1962ApJS....7....1L  Astrophys. J., Suppl. Ser., 7, 1-52 (1962)  Catalogue of dark nebulae.  LYNDS B.T.

--[[User:Linahan|Linahan]] 10:52, 11 February 2011 (PST)

#5 has 3 sources [G85] 3 330.83 PoC 21 32 59 +58 03.3
1993Afz....36..527G  Astrofizika, 36, 527-534 (1993)  Relationship between neutral hydrogen and radial systems of dark globules.  GYULBUDAGHIAN A.L.
1986Afz....24..201G  Astrofizika, 24, 201-203 (1986)  Radial systems of dark globules in the Association Cep OB2.  GYULBUDAGHIAN A.L., RODRIGUEZ L.F. and CANTO J.
1985Afz....23..295G  Astrofizika, 23, 295-306 (1985)  On the radial systems of dark globules.  GYULBUDAGHIAN A.L.

#6 has 2 Lan 435 336.39 UV 21 33 29.0 +58 11 17
2006PASP..118.1639L  Publ. Astron. Soc. Pac., 118, 1639-1647 (2006)  Proper motions of faint ultraviolet-bright sources in the Sandage two-color survey of the galactic plane.  LANNING H.H. and LEPINE S.
2000PASP..112..251L  Publ. Astron. Soc. Pac., 112, 251-263 (2000)  A finding list of faint UV-bright stars in the galactic plane. V.  LANNING H.H. and MEAKES M.

The rest have 1 or no source and many are pointing back to the same catalog or paper:
#1 TGU H590 164.50 DNe 21 32.9 +58 06 ~ 1 0 2005PASJ...57S...1D - Publ. Astron. Soc. Jap., 57, 1-368 (2005) - 17.03.05 01.02.10 February 2005
Atlas and catalog of dark clouds based on Digitized Sky Survey I.
DOBASHI K.; UEHARA H.; KANDORI R.; SAKURAI T.; KAIDEN M.; UMEMOTO T.; SATO F.

#2 [FSE2005] 16
177.28 Cld 21 33 +58.1 ~ 1 1
2005A&A...432..575F - Astron. Astrophys., 432, 575-584 (2005) - 15.03.05 02.12.05 March(III) 2005
Star formation in globules in IC 1396.
FROEBRICH D.; SCHOLZ A.; EISLOEFFEL J.; MURPHY G.C.

#11 JCMTSF J213332.7+580432 413.70 smm 21 33 32.7 +58 04 32
2008ApJS..175..277D  Astrophys. J., Suppl. Ser., 175, 277-295 (2008)  The SCUBA legacy catalogues: submillimeter-continuum objects detected by SCUBA.  DI FRANCESCO J., JOHNSTONE D., KIRK H., MacKENZIE T. and LEDWOSINSKA E.

#13 IRAS C21310+5749 436.65 IR 21 32.5 +58 02
1991ApJ...370..263S  Astrophys. J., 370, 263-271 (1991)  A search for embedded young stellar objects in and near the IC 1396 complex.  SCHWARTZ R.D., GYULBUDAGHIAN A.L. and WILKING B.A.

#17 2MASS J21332921+5802508 463.43 Em* 21 33 29.21 +58 02 50.9
2002AJ....123.2597O  Astron. J., 123, 2597-2626 (2002)  H{alpha} emission stars and Herbig-Haro objects in the vicinity of bright-rimmed clouds.  OGURA K., SUGITANI K. and PICKLES A.

#18 GSC 03975-00282 508.26 *iC 21 33 36.91 +58 02 46.6 K:...
1958TrRig...7...33A  Trudy Astrofiz. Lab. Riga, 7, 33-97 (1958)  Determination of magnitudes, color indices, and spectral classes of stars in an area centered on R.A.=21h24m, Dec=+58.5deg.  ALKSNIS A

#19 [PGS95] 9 520.32 PoC 21 33 07.5 +58 00 19 ~ 1 0 1995ApJ...447..721P  Astrophys. J., 447, 721-741 (1995)  The large-scale structure, kinematics, and evolution of IC 1396.  PATEL N.A., GOLDSMITH P.F., SNELL R.L., HEZEL T. and XIE T.

#20 BD+57 2346 566.01 *iC 21 32 29.6670 +58 17 42.840 K2
1958TrRig...7...33A  Trudy Astrofiz. Lab. Riga, 7, 33-97 (1958)  Determination of magnitudes, color indices, and spectral classes of stars in an area centered on R.A.=21h24m, Dec=+58.5deg.  ALKSNIS A.

#21 Cl* Trumpler 37 KUN 170
567.55 *iC 21 33 17.02 +57 59 53.7
1990Ap&SS.174...13K  Astrophys. Space Sci., 174, 13 (1990)  Solar-type stars in Cepheus OB 2: H-alpha emission stars and IRAS point sources.  KUN M. and PASZTOR L

Target selection for brc34

2011-02-11T19:09:57Z

Linahan: /* brc34 21h32m51.2s +58d08m43s */

== brc34 21h32m51.2s +58d08m43s ==

* BRC 34 1 proposal to study by Garmire, nothing on SIMBAD

* 0 ADS abstracts; 0 Simbad citations.

* No object listed at (or near) these precise coordinates, however, AllSky Optical images reveal the clouds that were of interest to Lori. Parts of the cloud are labeled. The DSS2.POSSII image reveals 2 star clusters, a Cloud Dark Nebula, and 2 IR sources (one above & slightly to the right of the center of the image) Many hits on 2MASS

--[[User:CJohnson|CJohnson]] 16:28, 9 February 2011 (PST)

Using SIMBAD with the coordinates yields 23 targets: Dark nebula 2, Cloud 2, IR source 6, PoC (part of cloud) 3, UV source 1, MoC (molecular cloud) 1, Em* 1, *iC (star in cluster) 6 and smm (submillimetric source)1.
Starting with the most references:
# 14 HD 205510 439.13 *iC 21 33 41.7048 +58 11 45.234 has 12 references. I don't know if any are worth looking into but the last one might be a good archival source.
2006AstL...32..759G  Astron. Lett., 32, 759-771 (2006)  Pulkovo compilation of radial velocities for 35495 stars in a common system.  GONTCHAROV G.A.
1999A&A...343..446D  Astron. Astrophys., 343, 446-454 (1999)  Late A-type stars: new Stroemgren photometric calibrations of absolute magnitudes from Hipparcos.  DOMINGO A. and FIGUERAS F.
1999A&AS..137..451G  Astron. Astrophys., Suppl. Ser., 137, 451-456 (1999)  Radial velocities. IX. Measurements of 2800 B2-F5 stars for Hipparcos.  GRENIER S., BAYLAC M.-O., ROLLAND L., BURNAGE R., ARENOU F., BRIOT D., DELMAS F., DUFLOT M., GENTY V., GOMEZ A.E., HALBWACHS J.-L., MAROUARD M., OBLAK E. and SELLIER A.
1983A&AS...51..245N  Astron. Astrophys., Suppl. Ser., 51, 245-256 (1983)  Lists of photometric Am candidates.  NICOLET B.
1974RMxAA...1..175M  Rev. Mex. Astron. Astrofis., 1, 175-201 (1974)  Multicolor photometry of metallic-line stars. III. A photometric catalogue.  MENDOZA E.E.
1973A&AS...10..385H  Astron. Astrophys., Suppl. Ser., 10, 385-403 (1973)  Catalogue of Am stars with known spectral types.  HAUCK B.
1968ApJ...154..923S  Astrophys. J., 154, 923-931 (1968)  A spectroscopic and photometric investigation of the association Cepheus OB2.  SIMONSON S.C.
1967JO.....50..425B  J. Obs., 50, 425 (1967)  Observations spectrographiques d'etoiles A a spectre particulier et a raies metalliques.  BERTAUD C. and FLOQUET M.
1965JO.....48..211B  J. Obs., 48, 211 (1965)  Catalogue et bibliographie des etoiles A a spectre particulier.  BERTAUD C.
1960JO.....43..129B  J. Obs., 43, 129 (1960)  Catalogue et bibliographie des etoiles A a spectre particulier.  BERTAUD C.
1959JO.....42...45B  J. Obs., 42, 45 (1959)  Catalogue et bibliographie des etoiles a spectre particulier.  BERTAUD C.
1958TrRig...7...33A  Trudy Astrofiz. Lab. Riga, 7, 33-97 (1958)  Determination of magnitudes, color indices, and spectral classes of stars in an area centered on R.A.=21h24m, Dec=+58.5deg.  ALKSNIS A.

#16 has 11 sources and seems to be talking about the BRC. JCMTSF J213332.0+580332 453.73 Cld 21 33 32.4 +58 03 28

2009MNRAS.400.1726M  Mon. Not. R. Astron. Soc., 400, 1726-1733 (2009)  CO observations towards bright-rimmed clouds.  MORGAN L.K., URQUHART J.S. and THOMPSON M.A.
2008A&A...477..557M  Astron. Astrophys., 477, 557-571 (2008)  A SCUBA survey of bright-rimmed clouds.  MORGAN L.K., THOMPSON M.A., URQUHART J.S. and WHITE G.J.
2008ApJS..175..277D  Astrophys. J., Suppl. Ser., 175, 277-295 (2008)  The SCUBA legacy catalogues: submillimeter-continuum objects detected by SCUBA.  DI FRANCESCO J., JOHNSTONE D., KIRK H., MacKENZIE T. and LEDWOSINSKA E.
2005A&A...443..535V  Astron. Astrophys., 443, 535-540 (2005)  H_2_O maser emission from bright rimmed clouds in the northern hemisphere.  VALDETTARO R., PALLA F., BRAND J. and CESARONI R.
2004A&A...426..535M  Astron. Astrophys., 426, 535-545 (2004)  A radio and mid-infrared survey of northern bright-rimmed clouds.  MORGAN L.K., THOMPSON M.A., URQUHART J.S., WHITE G.J. and MIAO J.
2002AJ....123.2597O  Astron. J., 123, 2597-2626 (2002)  H{alpha} emission stars and Herbig-Haro objects in the vicinity of bright-rimmed clouds.  OGURA K., SUGITANI K. and PICKLES A.
1997A&A...324..249L  Astron. Astrophys., 324, 249-262 (1997)  Cometary globules. III. Triggered star formation in IC 1848.  LEFLOCH B., LAZAREFF B. and CASTETS A.
1996A&A...309..581W  Astron. Astrophys., 309, 581-611 (1996)  The structure of the IC1396 region.  WEIKARD H., WOUTERLOOT J.G.A., CASTETS A., WINNEWISSER G. and SUGITANI K.
1995Ap&SS.224..571S  Astrophys. Space Sci., 224, 571-572 (1995)  Searches for bright-rimmed clouds with IRAS point sources.  SUGITANI K. and OGURA K.
1995MNRAS.276...57C  Mon. Not. R. Astron. Soc., 276, 57-73 (1995)  IRAS-selected Galactic star-forming regions. II. Water maser detections in the extended sample.  CODELLA C., PALUMBO G.G.C., PARESCHI G., SCAPPINI F., CASELLI P. and ATTOLINI M.R.
1991ApJS...77...59S  Astrophys. J., Suppl. Ser., 77, 59-66 (1991)  A catalog of bright-rimmed clouds with IRAS Point Sources: candidates for star formation by radiation-driven implosion. I. The Northern hemisphere.  SUGITANI K., FUKUI Y. and OGURA K.

#10 The next one has 5 sources0 LDN 1102 381.96 DNe 21 32.5 +58 03
2005A&A...432..575F  Astron. Astrophys., 432, 575-584 (2005)  Star formation in globules in IC 1396.  FROEBRICH D., SCHOLZ A., EISLOEFFEL J. and MURPHY G.C.
2005PASJ...57S...1D  Publ. Astron. Soc. Jap., 57, 1-368 (2005)  Atlas and catalog of dark clouds based on Digitized Sky Survey I.  DOBASHI K., UEHARA H., KANDORI R., SAKURAI T., KAIDEN M., UMEMOTO T. and SATO F.
2004A&A...418..131K  Astron. Astrophys., 418, 131-141 (2004)  Far-infrared loops in the 2nd Galactic Quadrant.  KISS C., MOOR A. and TOTH L.V.
2002A&A...383..631D  Astron. Astrophys., 383, 631-635 (2002)  A catalogue of dust clouds in the Galaxy.  DUTRA C.M. and BICA E.
1962ApJS....7....1L  Astrophys. J., Suppl. Ser., 7, 1-52 (1962)  Catalogue of dark nebulae.  LYNDS B.T.

--[[User:Linahan|Linahan]] 10:52, 11 February 2011 (PST)

#5 has 3 sources [G85] 3 330.83 PoC 21 32 59 +58 03.3
1993Afz....36..527G  Astrofizika, 36, 527-534 (1993)  Relationship between neutral hydrogen and radial systems of dark globules.  GYULBUDAGHIAN A.L.
1986Afz....24..201G  Astrofizika, 24, 201-203 (1986)  Radial systems of dark globules in the Association Cep OB2.  GYULBUDAGHIAN A.L., RODRIGUEZ L.F. and CANTO J.
1985Afz....23..295G  Astrofizika, 23, 295-306 (1985)  On the radial systems of dark globules.  GYULBUDAGHIAN A.L.

#6 has 2 Lan 435 336.39 UV 21 33 29.0 +58 11 17
2006PASP..118.1639L  Publ. Astron. Soc. Pac., 118, 1639-1647 (2006)  Proper motions of faint ultraviolet-bright sources in the Sandage two-color survey of the galactic plane.  LANNING H.H. and LEPINE S.
2000PASP..112..251L  Publ. Astron. Soc. Pac., 112, 251-263 (2000)  A finding list of faint UV-bright stars in the galactic plane. V.  LANNING H.H. and MEAKES M.

The rest have 1 or no source and many are pointing back to the same catalog or paper:
#1 TGU H590 164.50 DNe 21 32.9 +58 06 ~ 1 0 2005PASJ...57S...1D - Publ. Astron. Soc. Jap., 57, 1-368 (2005) - 17.03.05 01.02.10 February 2005
Atlas and catalog of dark clouds based on Digitized Sky Survey I.
DOBASHI K.; UEHARA H.; KANDORI R.; SAKURAI T.; KAIDEN M.; UMEMOTO T.; SATO F.

#2 [FSE2005] 16
177.28 Cld 21 33 +58.1 ~ 1 1
2005A&A...432..575F - Astron. Astrophys., 432, 575-584 (2005) - 15.03.05 02.12.05 March(III) 2005
Star formation in globules in IC 1396.
FROEBRICH D.; SCHOLZ A.; EISLOEFFEL J.; MURPHY G.C.

Target selection for brc34

2011-02-11T18:52:09Z

Linahan: /* brc34 21h32m51.2s +58d08m43s */

Target selection for brc34

2011-02-11T18:49:21Z

Linahan: /* brc34 21h32m51.2s +58d08m43s */

Target selection for brc34

2011-02-11T18:45:51Z

Linahan: /* brc34 21h32m51.2s +58d08m43s */

Target selection for brc34

2011-02-11T18:38:25Z

Linahan: /* brc34 21h32m51.2s +58d08m43s */