View source for Matching to Spitzer and Weeding the SEDs

This page follows the same conceptual structure as [[Working with the BRCs]] (specifically steps 6 through at least 11) but reflects the most recent work in Fall 2011.

=Matching known to Spitzer=

In [[Identification of Previously Known Objects on Candidate List]] (and several earlier pages), we established the complete list of previously-known YSOs.

Now, we have, independently, done the Spitzer data reduction. We need to compare this catalog of known sources with the catalog from the Spitzer data reduction (which also includes 2MASS).

When I do this, sources off the edge of the Spitzer maps will not have a match, because they have no Spitzer data.  Some sources will have only I1/I3 data, and some will have only I2/I4 data. (Do you remember why?)  Some sources in BRC 27 we have already identified as likely very interesting sources, but because they are embedded in bright, extended nebulosity, we are going to have a hard time finding an automatic match to those sources.

Here is what I get for all of the matches to the set of previously known sources in BRC 27: [[file:litsrcs+spitzer-brc27-0916-lmr.txt]] CAUTION: this is JUST the KNOWN sources. See next step.  (also, NB: this file has optical through M24 data.)

We need to do this for BRC34 too, but this is easier because there are only two previously known sources in the literature, with no optical photometry. <font color="red">PENDING</font>

=Finding IR Excess sources=

In [[Working with the BRCs]], we talked about selecting sources that appeared to have colors like young stars, e.g., objects that survive the Gutermuth selection process. I gave you a catalog of these objects on the DVD in July, for both BRC 27 and BRC 34.

=All the sources in which we are interested (for now)=

Recall that:
*There will be objects with IR excesses we discover as YSO candidates,
*there will be objects with IR excesses we REdiscover as YSO candidates that someone else identified first, and
*there will be objects someone else identified as YSO candidates that we find to not have IR excesses.

So, we need to create one file that has all of these items in one place for both BRC 27 and BRC 34.

==BRC27==

For BRC27, this is that file, as of right now: [[file:new+known-brc27-0916-lmr.txt]] '''IMPORTANT NOTES AND CAUTIONS ABOUT THIS FILE''':
*NB: this file has mags and fluxes for all available bands, optical through M24. Did I do the flux/mag conversion correctly?
*NB: this file has all previously identified names listed
*NB: this file has a column, "whyhere", which indicates why this object is included in this file. If it says "IRx", it survived the Gutermuth test. If it says "PrevKn", it is a previously known source. If it says "IRx+PrevKn", it is BOTH a survivor and a known object.
*CAUTION: See the caveats about the objects embedded in bright nebulosity above.  Those objects indeed do not have counterparts here, and we will have to pursue those separately, manually.

==BRC34==

What about for BRC 34? <font color="red">PENDING</font>

=Making and weeding the SEDs=

The next step is to make the SEDs and look critically at each one, going back to images and checking photometry (again) where it needs help, for both BRC 27 and BRC 34. Based on this, we WILL drop sources off the 'interesting' list to create a 'final' list. We will have to do this again when we get optical data for these sources from Haleakala. <font color="red">PENDING</font>

[[Notes on SEDs from BRC27]]

[[Notes on SEDs from BRC34]]