J/AJ/136/2413 Galactic midplane Spitzer red sources (Robitaille+, 2008)
Intrinsically red sources observed by Spitzer in the Galactic midplane.
Robitaille T.P., Meade M.R., Babler B.L., Whitney B.A., Johnston K.G.,
Indebetouw R., Cohen M., Povich M.S., Sewilo M., Benjamin R.A.,
Churchwell E.
<Astron. J., 136, 2413-2440 (2008)>
=2008AJ....136.2413R 2008AJ....136.2413R
ADC_Keywords: Galactic plane ; Infrared sources ; Photometry, infrared
Mission_Name: Spitzer
Keywords: catalogs - infrared: stars - Galaxy: stellar content -
planetary nebulae: general - stars: AGB and post-AGB -
stars: formation
Abstract:
We present a highly reliable flux-limited census of 18949 point
sources in the Galactic midplane that have intrinsically red
mid-infrared colors. These sources were selected from the Spitzer
Space Telescope Galactic Legacy Infrared Midplane Survey
Extraordinaire (GLIMPSE) I and II surveys of 274°2 of the
Galactic midplane, and consist mostly of high- and intermediate-mass
young stellar objects (YSOs) and asymptotic giant branch (AGB) stars.
The selection criteria were carefully chosen to minimize the effects
of position-dependent sensitivity, saturation, and confusion. The
distribution of sources on the sky and their location in the Infrared
Array Camera and the Multiband Image Photometer for Spitzer 24um
color-magnitude and color-color space are presented. Using this large
sample, we find that YSOs and AGB stars can be mostly separated by
simple color-magnitude selection criteria into approximately 50%-70%
of YSOs and 30%-50% of AGB stars. Planetary nebulae and background
galaxies together represent at most 2%-3% of all the red sources. 1004
red sources in the GLIMPSE II region, mostly AGB stars with high
mass-loss rates, show significant (≥0.3mag) variability at 4.5
and/or 8.0um. With over 11,000 likely YSOs and over 7000 likely AGB
stars, this is to date the largest uniform census of AGB stars and
high- and intermediate-mass YSOs in the Milky Way Galaxy.
Description:
In this paper, we make use of observations taken with the Spitzer IRAC
to select intrinsically red sources. The IRAC data used are from the
GLIMPSE I survey (PI: Churchwell; PIDs 146, 186, 187, 188, 189, 190,
191, 192, and 195), the GLIMPSE II survey of the inner region of the
Galactic plane (PI: Churchwell; PID 20201), and observations of the
Galactic center (PI: Stolovy; PID 3677).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 126 18949 Final red source catalog
table3.dat 84 4455 Red sources from the GLIMPSE II region with
photometry at two epochs
--------------------------------------------------------------------------------
See also:
II/293 : GLIMPSE Source Catalog (I + II + 3D) (IPAC 2008)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- --- [SSTGLMC]
9- 25 A17 --- SSTGLMC GLIMPSE source name (GLLL.llll+BB.bbbb)
27- 34 F8.4 deg GLon Galactic longitude (G1)
36- 42 F7.4 deg GLat Galactic latitude (G1)
44- 51 F8.4 deg RAdeg Right Ascension in decimal degrees (J2000) (G1)
53- 60 F8.4 deg DEdeg Declination in decimal degrees (J2000) (G1)
62- 66 F5.2 mag Jmag ? 2MASS J band magnitude (2)
68- 72 F5.2 mag Hmag ? 2MASS H band magnitude (2)
74- 78 F5.2 mag Ksmag ? 2MASS Ks band magnitude (2)
80- 84 F5.2 mag [3.6]G ? GLIMPSE catalog 3.6um band magnitude (2)
86- 90 F5.2 mag [4.5]G GLIMPSE catalog 4.5um band magnitude (2)
92- 96 F5.2 mag [5.8]G ? GLIMPSE catalog 5.8um band magnitude (2)
98-101 F4.2 mag [8.0]G GLIMPSE catalog 8.0um band magnitude (2)
103-107 F5.2 mag [4.5] This paper's 4.5um band magnitude (2)
109-112 F4.2 mag [8.0] This paper's 8.0um band magnitude (2)
114-118 F5.2 mag Emag ? This paper's MSX E band (21um) magnitude (2)
120-123 F4.2 mag [24] ? This paper's 24um band magnitude (2)
125 A1 --- f_[4.5] [A/I] best [4.5] magnitude (3)
126 A1 --- f_[8.0] [A/I] best [8.0] magnitude (3)
--------------------------------------------------------------------------------
Note (2): The zero-magnitude fluxes assumed throughout this paper are:
Fν(J)=1594Jy, Fν(H)=1024Jy, Fν(Ks)=666.7Jy,
Fν(3.6um)=280.9Jy, Fν(4.5um)=179.7Jy,
Fν(5.8um)=115.0Jy, Fν(8.0um)=64.13Jy,
Fν(MSXE)=8.75Jy, Fν(24.0um)=7.14Jy.
Note (3): Flags as follows:
A = GLIMPSE Catalog magnitudes are in agreement with the independent
magnitudes calculated in this paper
I = the independent magnitudes calculated in this paper should be
trusted over the GLIMPSE catalog magnitudes
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- --- [SSTGLMC]
9- 25 A17 --- SSTGLMC GLIMPSE source name (GLLL.llll+BB.bbbb)
27- 34 F8.4 deg GLon Galatic longitude (G1)
36- 42 F7.4 deg GLat Galatic latitude (G1)
44- 51 F8.4 deg RAdeg Right Ascension in decimal degrees (J2000) (G1)
53- 60 F8.4 deg DEdeg Declination in decimal degrees (J2000) (G1)
62- 66 F5.2 mag [4.5]1 First epoch 4.5um band magnitude
68- 71 F4.2 mag [8.0]1 First epoch 8.0um band magnitude
73- 77 F5.2 mag [4.5]2 ? Second epoch 4.5um band magnitude
79- 82 F4.2 mag [8.0]2 ? Second epoch 8.0um band magnitude
84 A1 --- V? [Y/N] Variablity flag (2)
--------------------------------------------------------------------------------
Note (2): Variablity flag as follows:
Y = The magnitudes for the two epochs differ by at least 0.3mag at
either (or both) 4.5um or 8.0um
N = Not variable
--------------------------------------------------------------------------------
Global Notes:
Note (G1): These coordinates are set to the average position of the source
at 4.5 and at 8.0um. This position may differ slightly from the
'official' GLIMPSE position in cases where PSF fitting was used to
determine the flux of the source if the position of the source was
adjusted to obtain a better residual.
History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 03-Jun-2011