Wendi's table of all data sources - Revision history

Rebull at 23:24, 29 May 2013

2013-05-29T23:24:33Z

2013-05-22T23:27:33Z

2013-05-22T23:13:39Z

2013-05-22T21:44:35Z

The table

2013-05-15T23:19:30Z

2013-05-08T23:30:55Z

2013-05-08T23:29:30Z

2013-04-17T23:22:24Z

2013-04-03T23:50:24Z

The table

2013-04-03T23:32:19Z

@@ Line 57: / Line 57: @@
 |-
 |WISE
+|3.4, 4.6, 12, 22 microns
+|primary way of finding our YSOs!
+|over whole sky, has done photometry for us but BE CAREFUL about things in catalog claiming to be real sources at 12 and 22 um!
 |-
 |AKARI
+|shortest two bands are 9 and 18 um.
+|can be used to flesh out SEDs but only for the brightest sources!
+|no image provided, only catalogs, so use with caution!
 |-
 |Spitzer
+| IRAC: 3.6, 4.5, 5.8, 8 um; MIPS: 24, 70, 160 um.
+|really useful for images and SED help, but don't have over a large area
+| we will have to do photometry ourselves in this region!
 |-
 |}

@@ Line 32: / Line 32: @@
 |-
 |Barentsen et al. 2011
+|r', i', Halpha (IPHAS)
+|optical data will help us flesh out the SED, optical CMDs can help us weed out contamination
+|they tabulate candidates and rejects (useful to know things they have weeded out as members)
 |-
 | IPHAS
 |r', i', Halpha
-|optical data will help us flesh out the SED
+|optical data will help us flesh out the SED, optical CMDs can help us weed out contamination
-|i have the whole catalog from Barentsen himself, not just the ttauris or rejected candidates.
+|i have the whole catalog from Barentsen himself, not just the TTauris or rejected candidates.
 |-
 |Nakano et al. 2012
+|Halpha, IPHAS, Akari, crossmatching to prior literature.
+|similar issues as to Barentsen, IPHAS.
+|only one object with Akari data tabulated for BRC 38 (our region specifically)
 |-
 |2MASS

@@ Line 37: / Line 37: @@
 |-
 | IPHAS
+|r', i', Halpha
+|optical data will help us flesh out the SED
+|i have the whole catalog from Barentsen himself, not just the ttauris or rejected candidates.
 |-
 |Nakano et al. 2012

@@ Line 14: / Line 14: @@
 |X-ray
 |X-rays trace stellar magnetic activity, can reduce number of foreground/background objects by requiring X-ray detections. Young stars are bright in X-rays because they are rotating quickly and therefore flaring a lot.
-|25 Gloubule sources identified as YSOs in the center. 117 sources tabulated in Table 1. Also, entire Nisini catalog included in Table 3. (Nisini is deeper JHK than 2MASS.) SEDs in Figure 5 good for comparison to ours.
+|25 Globule sources identified as YSOs in the center. 117 sources tabulated in Table 1. Also, entire Nisini catalog included in Table 3. (Nisini is deeper JHK than 2MASS.) SEDs in Figure 5 good for comparison to ours.
 |-
 |Choudhury et al. 2010

@@ Line 17: / Line 17: @@
 |-
 |Choudhury et al. 2010
+|optical (including Halpha, IRAC, MIPS, 2MASS), some spectra (from which they got spectral types)
+|very similar data sets, and analysis (at least to aspire to), though over a smaller area, and certainly seems to be reliable in terms of data reduction and coordinate accuracy. Identified 118 sources, 40 YSOs+13 candidates.
+|published whole table.
 |-
 |Chauhan et al. 2009
+|BVI, IRAC
+|identified only 18 sources, but still useful, also over small region. Experience in BRC 27 with this paper suggests we need to be cautious with their data tables. Check to make sure sources really match.
+|published just the YSOs.
 |-
 |Ogura et al. 2002

@@ Line 47: / Line 47: @@
 |-
 |2MASS
+|JHKs over whole region, not just a subset
+|point sources can be matched across bands
+|over whole region!
 |-
 |Beltran et al. 2009
-|NIR (JHK') and H2 (1.2-2.2 um)
+|NIR (JHK') and H2 (1.2-2.2 um) (deeper than 2MASS!)
 |link the point sources across all available bands; look for complex H2 structures, unclear if we will find them.
 |Further data on BIMA 1,2,3 and Source C

@@ Line 29: / Line 29: @@
 |Halpha = 6563 A
 |because young accreting stars are bright in Halpha
-|we have updated the coordinates for the BRC 38 sources listed. also note that they have finding charts of their sources, and the HH sources they have identified here. objects tabulated in this paper with small Ha EQWs are probably just chromosphere and not accretion.
+|We have updated the coordinates for the BRC 38 sources listed. Also note that they have finding charts of their sources, and of the HH sources they have identified here. Objects tabulated in this paper with small Ha EQWs are probably just chromospheric activity and not accretion.
 |-
 |Barentsen et al. 2011