J/ApJS/259/41 Photometry of M31 AGB sample (Goldman+, 2022) ================================================================================ A census of thermally-pulsing AGB stars in the Andromeda galaxy and a first estimate of their contribution to the global dust budget. Goldman S.R., Boyer M.L., Dalcanton J., McDonald I., Girardi L., Williams B.F., Srinivasan S., Gordon K. =2022ApJS..259...41G (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Galaxies, nearby ; Stars, variable ; Photometry ; Stars, late-type Keywords: galaxies: dwarf - galaxies: stellar content - infrared: stars - Local Group - stars: AGB and post-AGB - stars: carbon Abstract: We present a near-complete catalog of the metal-rich population of thermally pulsing asymptotic giant branch (AGB) stars in the northwest quadrant of M31. This metal-rich sample complements the equally complete metal-poor Magellanic Cloud AGB catalogs produced by the SAGE program. Our catalog includes Hubble Space Telescope (HST) wide-band photometry from the Panchromatic Hubble Andromeda Treasury survey, HST medium-band photometry used to chemically classify a subset of the sample, and Spitzer mid- and far-IR photometry that we have used to isolate dust-producing AGB stars. We have detected 346623 AGB stars; these include 4802 AGB candidates producing considerable dust, and 1356 AGB candidates that lie within clusters with measured ages, and in some cases metallicities. Using the Spitzer data and chemical classifications made with the medium-band data, we have identified both carbon- and oxygen-rich AGB candidates producing significant dust. We have applied color-mass-loss relations based on dusty-AGB stars from the LMC to estimate the dust injection by AGB stars in the PHAT footprint. Applying our color relations to a subset of the chemically classified stars producing the bulk of the dust, we find that ~97.8% of the dust is oxygen-rich. Using several scenarios for the dust lifetime, we have estimated the contribution of AGB stars to the global dust budget of M31 to be 0.9%-35.5%, which is in line with previous estimates in the Magellanic Clouds. Follow-up observations of the M31 AGB candidates with the JWST will allow us to further constrain stellar and chemical evolutionary models, and the feedback and dust production of metal-rich evolved stars. Description: UV to IR photometry for AGB candidates in the PHAT footprint of M31. Additional classifications for carbon and oxygen-rich AGB stars, heavily dust enshrouded AGB stars, Red Helium Burning and Red Supergiant candidates, and associated cluster properties, where available. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table2.dat 463 346623 Photometry of the M31 AGB sample; from erratum published in 2023ApJS..268...71G (updated on 16-Jul-2026) -------------------------------------------------------------------------------- See also: J/AJ/141/61 : Star clusters in M31. II. (Caldwell+, 2011) J/ApJS/215/9 : PHAT X. UV-IR photometry of M31 stars (Williams+, 2014) J/ApJ/802/127 : PHAT stellar cluster survey. II. AP catalog (Johnson+, 2015) J/ApJS/216/10 : DUSTiNGS. I. The Good Source Catalog (Boyer+, 2015) J/ApJS/228/5 : Spitzer photometry of ~1million stars in M31 + 15 gal. (Khan, 2017) Byte-by-byte Description of file: table2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 6 I6 --- ID [1/346623] This catalog's internal identifier 8- 25 F18.15 deg RAdeg Right Ascension (J2000) 27- 44 F18.15 deg DEdeg Declination (J2000) 46- 48 I3 --- Brick [-99/23] PHAT brick identifier (1) 50- 55 F6.3 kpc R [0/20] Deprojected radius from galaxy center 57- 62 F6.3 [-] [M/H] [-0.3/0.11] Estimated [M/H] based on R (Z-Rad) (2) 64- 68 I5 --- Cl-ID [0/15121]?=-99.999 Cluster catalog identifier (Clst-ID) (3) 70- 73 F4.1 [-] Cl-[Fe/H] [-2.4/0.4]?=-99.999 Cluster [Fe/H] (Clst-Z) (3) (4) 75- 79 F5.2 [yr] logCl-Age [0/10.3]?=-99.999 log cluster age (Clst-Age) (3) 81- 83 F3.1 [Msun] logCl-Mass [0/7]?=-99.999 log cluster mass (Clst-M) (3) 85- 89 F5.2 arcsec Cl-Rad [0/6.4]?=-99.999 Cluster visible radius (Clst-R) (3) 91- 95 F5.2 arcsec Cl-Dist [0/4.8]?=-99.999 Source distance to cluster center (Clst-D) (3) 97-103 F7.3 mag F275W [15.6/41]?=0 HST/WFC3/UVIS F275W band magnitude (5) 105-111 F7.3 mag e_F275W [0.002/10]?=0 Uncertainty in F275W (5) 113-119 F7.3 mag F336W [17.7/41]?=0 HST/WFC3/UVIS F336W band magnitude (5) 121-127 F7.3 mag e_F336W [0.001/10]?=0 Uncertainty in F336W (5) 129-135 F7.3 mag F475W [14.7/38]?=0 HST/ACS/WFC F475W band magnitude (5) 137-143 F7.3 mag e_F475W [0.001/10]?=0 Uncertainty in F475W (5) 145-151 F7.3 mag F814W [13.5/35.2]?=0 HST/ACS/WFC F814W band magnitude (5) 153-159 F7.3 mag e_F814W [0.001/9]?=0 Uncertainty in F814W (5) 161-167 F7.3 mag F110W [12/26.1]?=0 HST/WFC3/IR F110W band magnitude (5) 169-175 F7.3 mag e_F110W [0.001/0.3]?=0 Uncertainty in F110W (5) 177-183 F7.3 mag F127M [15/24]?=0 HST/WFC3/IR F127M band magnitude (6) 185-191 F7.3 mag e_F127M [0.001/0.2]?=0 Uncertainty in F127M (6) 193-199 F7.3 mag F139M [14.8/24]?=0 HST/WFC3/IR F139M band magnitude (6) 201-207 F7.3 mag e_F139M [0.001/0.3]?=0 Uncertainty in F139M (6) 209-215 F7.3 mag F153M [14.4/23]?=0 HST/WFC3/IR F153M band magnitude (6) 217-223 F7.3 mag e_F153M [0.001/0.2]?=0 Uncertainty in F153M (6) 225-231 F7.3 mag F160W [12.6/25.4]?=0 HST/WFC3/IR F160W band magnitude (5) 233-239 F7.3 mag e_F160W [0.001/0.4]?=0 Uncertainty in F160W (5) 241-247 F7.3 --- S-F110W [-9.999/0.4]?=-99.999 HST/WFC3/IR F110W band sharpness 249-255 F7.3 --- S-F160W [-9.999/3]?=-99.999 HST/WFC3/IR F160W band sharpness 257-263 F7.3 --- S-F275W [-9.999/9.999]?=-99.999 HST/WFC3/UVIS F275W band sharpness 265-271 F7.3 --- S-F336W [-9.999/9.999]?=-99.999 HST/WFC3/UVIS F336W band sharpness 273-279 F7.3 --- S-F475W [-9.999/9.999]?=-99.999 HST/ACS/WFC F475W band sharpness 281-287 F7.3 --- S-F814W [-9.999/9.999]?=-99.999 HST/ACS/WFC F814W band sharpness 289-295 F7.3 --- R-F110w [-9.999/9.999]?=-99.999 HST/WFC3/IR F110W band roundness 297-303 F7.3 --- R-F160W [-9.999/9.999]?=-99.999 HST/WFC3/IR F160W band roundness 305-311 F7.3 --- R-F275W [-9.999/9.999]?=-99.999 HST/WFC3/UVIS F275W band roundness 313-319 F7.3 --- R-F336W [-9.999/9.999]?=-99.999 HST/WFC3/UVIS F336W band roundness 321-327 F7.3 --- R-F475W [-9.999/9.999]?=-99.999 HST/ACS/WFC F475W band roundness 329-335 F7.3 --- R-F814W [-9.999/9.999]?=-99.999 HST/ACS/WFC F814W band roundness 337-343 F7.3 --- C-F110W [0/9.999]?=-99.999 HST/WFC3/IR F110W band crowdedness 345-351 F7.3 --- C-F160W [0/9.999]?=-99.999 HST/WFC3/IR F160W band crowdedness 353-359 F7.3 --- C-F275W [0/9.999]?=-99.999 HST/WFC3/UVIS F275W band crowdedness 361-367 F7.3 --- C-F336W [0/9.999]?=-99.999 HST/WFC3/UVIS F336W band crowdedness 369-375 F7.3 --- C-F475W [0/9.999]?=-99.999 HST/ACS/WFC F475W band crowdedness 377-383 F7.3 --- C-F814W [0/9.999]?=-99.999 HST/ACS/WFC F814W band crowdedness 385-391 F7.3 mag IRAC1 [9.5/18]?=0 Spitzer/IRAC 3.6um band magnitude (6) 393-399 F7.3 mag e_IRAC1 [0.02/0.3]?=0 Uncertainty in IRAC1 (6) 401-407 F7.3 mag IRAC2 [9.3/18.3]?=0 Spitzer/IRAC 4.5um band magnitude (6) 409-415 F7.3 mag e_IRAC2 [0.01/0.3]?=0 Uncertainty in IRAC2 (6) 417-423 F7.3 mag IRAC3 [10.4/18.2]?=0 Spitzer/IRAC 5.8um band magnitude (7) 425-431 F7.3 mag e_IRAC3 [0.01/0.3]?=0 Uncertainty in IRAC3 (7) 433-439 F7.3 mag IRAC4 [8.7/17.4]?=0 Spitzer/IRAC 8um band magnitude (7) 441-447 F7.3 mag e_IRAC4 [0.01/0.3]?=0 Uncertainty in IRAC4 (7) 449 I1 --- HST-AGB [0/1] Classified here as AGB candidate from HST criteria 451 I1 --- X-AGB [0/1] Classified here as AGB candidate from Spitzer criteria 453 I1 --- RHeB [0/1] Classified here as RHeB candidate 455 I1 --- RSG [0/1] Classified here as Red supergiant candidate in Ren+ 2021ApJ...907...18R 457 A1 --- Chem [cm] AGB photometric chemical type from HST small regions (8) 459 A1 --- SPLASH [cm] AGB photometric chemical type from SPLASH subset (8) 461 I1 --- Gaia [0/1]? Gaia foreground candidate 463 I1 --- Flag [0/1] Flag indicating sources with chemical classifications recovered in the analysis (recovered_chem_type) -------------------------------------------------------------------------------- Note (1): From Williams et al., 2014ApJS..215....9W, Cat. J/ApJS/215/9 Note (2): Relation from Gregersen et al., 2015AJ....150..189G Note (3): From Johnson et al., 2015ApJ...802..127J, Cat. J/ApJ/802/127 (<[JSD2015] AP NNNNN> in Simbad). Note (4): Measured spectroscopically by Caldwell et al., 2011AJ....141...61C, Cat. J/AJ/141/61 Note (5): From Dalcanton et al., 2012ApJS..200...18D Note (6): Performed here following Boyer et al., 2015ApJS..216...10B, Cat. J/ApJS/216/10 Note (7): From Khan, 2017ApJS..228....5K, Cat. J/ApJS/228/5 Note (8): Chemical types were determined by Boyer et al. (2019ApJ...879..109B) in 21 fields using the medium-band HST photometry (C, M) included in this catalog, or from the additional DEIMOS/Keck II optical spectra (C, M) from the SPLASH survey (Hamren et al., 2015ApJ...810...60H). -------------------------------------------------------------------------------- Acknowledgements: Steven R. Goldman, sgoldman(at)usra.edu History: 18-Jul-2022: on-line version 02-Nov-2023: Table updated from erratum published in 2023ApJS..268...71G 16-Jul-2026: Table updated from author ================================================================================ (End) Patricia Vannier [CDS] 12-Apr-2022