J/ApJ/753/71 Mass-loss return from LMC evolved stars. VI. (Riebel+, 2012)
The mass-loss return from evolved stars to the Large Magellanic Cloud.
VI. Luminosities and mass-loss rates on population scales.
Riebel D., Srinivasan S., Sargent B., Meixner M.
<Astrophys. J., 753, 71 (2012)>
=2012ApJ...753...71R 2012ApJ...753...71R
ADC_Keywords: Magellanic Clouds ; Mass loss ; Photometry, infrared ;
Stars, giant ; Photometry, UBV ; Effective temperatures
Keywords: evolution; infrared: stars; Magellanic Clouds; radiative transfer
stars: AGB and post-AGB; stars: mass-loss
Abstract:
We present results from the first application of the Grid of Red
Supergiant and Asymptotic Giant Branch ModelS (GRAMS) model grid to
the entire evolved stellar population of the Large Magellanic Cloud
(LMC). GRAMS is a pre-computed grid of 80843 radiative transfer models
of evolved stars and circumstellar dust shells composed of either
silicate or carbonaceous dust. We fit GRAMS models to ∼30000
asymptotic giant branch (AGB) and red supergiant (RSG) stars in the
LMC, using 12 bands of photometry from the optical to the
mid-infrared. Our published data set consists of thousands of evolved
stars with individually determined evolutionary parameters such as
luminosity and mass-loss rate. The GRAMS grid has a greater than 80%
accuracy rate discriminating between oxygen- and carbon-rich
chemistry.
Description:
Our data set consists of 33718 sources extracted from the SAGE Mosaic
Photometry Archive. These sources have been matched to optical data
from MCPS (Zaritsky et al. 2004, Cat. J/AJ/128/1606), near-infrared
photometry from the 2MASS survey (Skrutskie et al. 2006,
Cat. II/246), and the variability information of the MACHO survey
(Alcock et al. 1999PASP..111.1539A 1999PASP..111.1539A), allowing us to construct 12 band
SEDs from the U band to 24um for most of our sources.
Looking for young stellar objects, Gruendl et al. published a list
of 13 "extremely red objects" (2008ApJ...688L...9G 2008ApJ...688L...9G) that they
spectroscopically identified as carbon stars, based on the presence of
SiC absorption. Twelve of these sources lie outside our defined CMD
cuts and are therefore not included in our initial data set, but we
have manually added them to our list, using the photometry published
in that work. All of these sources are classified as extreme AGB
candidates.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 405 33503 List of AGB candidates used in the study
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See also:
II/305 : SAGE LMC and SMC IRAC Source Catalog (IPAC 2009)
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
J/A+A/537/A105 : Modelisation of AGB stars in the LMC (Gullieuszik+, 2012)
J/A+A/530/A90 : Optically bright LMC post-AGB population (van Aarle+, 2011)
J/A+A/532/A54 : GRAMS carbon-star model grid (Srinivasan+, 2011)
J/ApJ/723/1195 : SAGE AGB candidates (Riebel+, 2010)
J/AJ/137/3139 : LMC SAGE. New variable evolved stars and YSOs (Vijh+, 2009)
J/AJ/137/4810 : LMC-SAGE AGB star candidates (Srinivasan+, 2009)
J/AJ/138/1003 : IR photometry of massive LMC stars (Bonanos+, 2009)
J/A+A/506/1277 : Magellanic Cloud C/O stars modelisation (Groenewegen+, 2009)
J/MNRAS/376/313 : Carbon star in Magellanic Cloud (Groenewegen+, 2007)
J/A+A/425/595 : OGLE+2MASS+DENIS LPV in Magellanic Clouds (Groenewegen, 2004)
J/AJ/128/1606 : Magellanic Clouds Phot. Survey: the LMC (Zaritsky+, 2004)
J/A+A/369/932 : RI photometry of LMC carbon stars (Kontizas+, 2001)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1 - 30 A30 --- Name Star Designation (1)
32 A1 --- Cl [coxs] Photometric classification: c=C-rich,
o=O-rich, x=eXtreme AGB, o=other Stars) (2)
34 A1 --- GCl [co] C-rich or O-rich GRAMS classification (3)
36- 41 F6.2 --- chi2 Best-fit model χ2/data point
43- 50 E8.2 Msun/yr dM/dt Dust mass-loss rate of best-fit model
52- 59 E8.2 Msun/yr e_dM/dt Uncertainty in dM/dt
61- 67 I7 Lsun Lbol [1000/] Bolometric luminosity of best-fit model
69- 74 I6 Lsun e_Lbol ?=-99 Uncertainty in Lbol
76- 79 I4 K Teff [2100/4700] Effective temperature of best-fit
model
81- 84 I4 K e_Teff ?=-99 Uncertainty in Teff
86- 92 F7.5 --- tau Optical depth of best-fit model (4)
94-102 F9.5 --- e_tau ?=-99 Uncertainty in tau
104-108 F5.3 mag Amp [0/9] MACHO lightcurve variability amplitude
110-117 F8.3 d Per MACHO lightcurve derived variability period
119-129 E11.4 Jy FU Flux in MCPS U band (J/AJ/128/1606)
131-141 E11.4 Jy e_FU ?=-99 Uncertainty in FU
143-153 E11.4 Jy FB Flux in MCPS B band (J/AJ/128/1606)
155-165 E11.4 Jy e_FB ?=-99 Uncertainty in FB
167-177 E11.4 Jy FV Flux in MCPS V band (J/AJ/128/1606)
179-189 E11.4 Jy e_FV ?=-99 Uncertainty in FV
191-201 E11.4 Jy FI Flux in MCPS I band (J/AJ/128/1606)
203-213 E11.4 Jy e_FI ?=-99 Uncertainty in FI
215-225 E11.4 Jy FJ Flux in 2MASS J band (II/246)
227-237 E11.4 Jy e_FJ ?=-99 Uncertainty in FJ
239-249 E11.4 Jy FH Flux in 2MASS H band (II/246)
251-261 E11.4 Jy e_FH ?=-99 Uncertainty in FH
263-273 E11.4 Jy FK Flux in 2MASS Ks band (II/246)
275-285 E11.4 Jy e_FK ?=-99 Uncertainty in FK
287-297 E11.4 Jy F3.6 ?=-99 Flux in SAGE 3.6um band (II/305)
299-309 E11.4 Jy e_F3.6 ?=-99 Uncertainty in F3.6
311-321 E11.4 Jy F4.5 ?=-99 Flux in SAGE 4.5um band (II/305)
323-333 E11.4 Jy e_F4.5 ?=-99 Uncertainty in F4.5
335-345 E11.4 Jy F5.8 ?=-99 Flux in SAGE 5.8um band (II/305)
347-357 E11.4 Jy e_F5.8 ?=-99 Uncertainty in F5.8
359-369 E11.4 Jy F8.0 ?=-99 Flux in SAGE 8.0um band (II/305)
371-381 E11.4 Jy e_F8.0 ?=-99 Uncertainty in F8.0
383-393 E11.4 Jy F24 ?=-99 Flux in SAGE 24um band (II/305)
395-405 E11.4 Jy e_F24 ?=-99 Uncertainty in F24
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Note (1): "SSTISAGEMA JHHMMSS.ss+DDMMSS.s" for sources from SAGE (II/305),
or "[GCS2008] JHHMMSS.ss+DDMMSS.s" for the carbon stars from Gruendl
et al. (2008ApJ...688L...9G 2008ApJ...688L...9G) (see Sec. 4).
Note (2): CMD Classifications are described in Cioni et al.
(2006A&A...448...77C 2006A&A...448...77C) and Riebel et al. (2010, Cat. J/ApJ/723/1195).
Note (3): O-rich or C-rich classification based on best fitting GRAMS model
(Grid of RSG and AGB ModelS, SRINIVASAN et al. 2011, Cat. J/A+A/532/A54)
Note (4): Determined at 10.0 microns for O-rich sources and at 11.3 microns
for C-rich sources
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History:
From electronic version of the journal
References:
Srinivasan et al. Paper I 2009AJ....137.4810S 2009AJ....137.4810S
Sargent et al. Paper II. 2010ApJ...716..878S 2010ApJ...716..878S
Srinivasan et al. Paper III. 2010A&A...524A..49S 2010A&A...524A..49S
Sargent et al. Paper IV. 2011ApJ...728...93S 2011ApJ...728...93S
Srinivasan et al. Paper V. 2011A&A...532A..54S 2011A&A...532A..54S Cat. J/A+A/532/54
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 13-Feb-2014