Access to Astronomical Catalogues

← Click to display the menu
J/MNRAS/457/2814    SAGE SMC evolved stars candidates        (Srinivasan+, 2016)

The evolved-star dust budget of the Small Magellanic Cloud: the critical role of a few key players. Srinivasan S., Boyer M.L., Kemper F., Meixner M., Sargent B.A., Riebel D. <Mon. Not. R. Astron. Soc., 457, 2814-2838 (2016)> =2016MNRAS.457.2814S (SIMBAD/NED BibCode)
ADC_Keywords: Magellanic Clouds ; Stars, supergiant ; Photometry Keywords: stars: AGB and post-AGB - stars: carbon - stars: mass-loss - supergiants - Magellanic Clouds Abstract: The life cycle of dust in the interstellar medium is heavily influenced by outflows from asymptotic giant branch (AGB) and red supergiant (RSG) stars, a large fraction of which is contributed by a few very dusty sources. We compute the dust input to the Small Magellanic Cloud (SMC) by fitting the multi-epoch mid-infrared spectral energy distributions of AGB/RSG candidates with models from the Grid of RSG and AGB ModelS grid, allowing us to estimate the luminosities and dust-production rates (DPRs) of the entire population. By removing contaminants, we guarantee a high-quality data set with reliable DPRs and a complete inventory of the dustiest sources. We find a global AGB/RSG dust-injection rate of (1.3±0.1)x10-6M/yr, in agreement with estimates derived from mid-infrared colours and excess fluxes. As in the Large Magellanic Cloud, a majority (66 per cent) of the dust arises from the extreme AGB stars, which comprise only ∼7 per cent of our sample. A handful of far-infrared sources, whose 24µm fluxes exceed their 8µm fluxes, dominate the dust input. Their inclusion boosts the global DPR by ∼1.5x, making it necessary to determine whether they are AGB stars. Model assumptions, rather than missing data, are the major sources of uncertainty; depending on the choice of dust shell expansion speed and dust optical constants, the global DPR can be up to ∼10 times higher. Our results suggest a non-stellar origin for the SMC dust, barring as yet undiscovered evolved stars with very high DPRs. Description: Using a very careful selection procedure, we produce the most complete data set of mass-losing evolved stars in the SMC to date. We fit dust radiative transfer models to these sources to resolve their chemical types and estimate their luminosities and DPRs. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table5.dat 872 9621 Photometry and SED fit results for our candidate list of evolved stars
See also: II/305 : SAGE LMC and SMC IRAC Source Catalog (IPAC 2009) 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/ApJ/723/1195 : SAGE AGB candidates (Riebel+, 2010) J/MNRAS/451/3504 : Classification of IRS sources in the SMC (Ruffle+, 2015) Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 30 A30 --- SAGE SAGE Designation of IRAC source (Mosaic Archive by default; if missing, Epoch 1 Archive) (IRAC_DESIGNATION) 32- 36 A5 --- Class Colour classification (COLOUR_CLASS) 38- 55 A18 --- OGLE3 OGLE-III identifier (OGLE3_ID) 57- 61 A5 --- AKARI AKARI identifier (AKARI_ID) 63- 81 A19 --- WISE WISE identifier (WISE_ID) 83- 90 E8.4 Jy FU ?=-99 Broadband flux in U (FLUXU) 92- 99 E8.4 Jy e_FU ?=-99 Broadband flux uncertainty in U (DFLUXU) 101-108 E8.4 Jy FB ?=-99 Broadband flux in B (FLUXB) 110-117 E8.4 Jy e_FB ?=-99 Broadband flux uncertainty in B (DFLUXB) 119-126 E8.4 Jy FV ?=-99 Broadband flux in V (FLUXV) 128-135 E8.4 Jy e_FV ?=-99 Broadband flux uncertainty in V (DFLUXV) 137-144 E8.4 Jy FI ?=-99 Broadband flux in I (FLUXI) 146-153 E8.4 Jy e_FI ?=-99 Broadband flux uncertainty in I (DFLUXI) 155-162 E8.4 Jy FJ ?=-99 Broadband flux in J (FLUXJ) 164-171 E8.4 Jy e_FJ ?=-99 Broadband flux uncertainty in J (DFLUXJ) 173-181 F9.5 Jy FH ?=-99 Broadband flux in H (FLUXH) 183-190 E8.4 Jy e_FH ?=-99 Broadband flux uncertainty in H (DFLUXH) 192-200 F9.5 Jy FKs ?=-99 Broadband flux in Ks (FLUXK_S) 202-209 E8.4 Jy e_FKs ?=-99 Broadband flux uncertainty in Ks (DFLUXK_S) 211-219 F9.5 Jy F3.6 ?=-99 Broadband flux in Spitzer/IRAC 3.6um (FLUX3_6) 221-228 E8.4 Jy e_F3.6 ?=-99 Broadband flux uncertainty in Spitzer/IRAC 3.6um (DFLUX3_6) 230-237 E8.4 Jy F4.5 ?=-99 Broadband flux in Spitzer/IRAC 4.5um (FLUX4_5) 239-246 E8.4 Jy e_F4.5 ?=-99 Broadband flux uncertainty in Spitzer/IRAC 4.5um (DFLUX4_5) 248-256 F9.5 Jy F5.8 ?=-99 Broadband flux in Spitzer/IRAC 5.8um (FLUX5_8) 258-265 E8.4 Jy e_F5.8 ?=-99 Broadband flux uncertainty in Spitzer/IRAC 5.8um (DFLUX5_8) 267-275 F9.5 Jy F8.0 ?=-99 Broadband flux in Spitzer/IRAC 8.0um (FLUX8_0) 277-284 E8.4 Jy e_F8.0 ?=-99 Broadband flux uncertainty in Spitzer/IRAC 8.0um (DFLUX8_0) 286-294 F9.5 Jy F24 ?=-99 Broadband flux in Spitzer/MIPS 24um (FLUX24) 296-303 E8.4 Jy e_F24 ?=-99 Broadband flux uncertainty in Spitzer/MIPS 24um (DFLUX24) 305-313 F9.5 Jy F11 ?=-99 Broadband flux in AKARI S11 (11um) (FLUXN11) 315-323 F9.5 Jy e_F11 ?=-99 Broadband flux uncertainty in AKARI S11 (11um) (DFLUXN11) 325-333 F9.5 Jy F15 ?=-99 Broadband flux in AKARI L15 (15um) (FLUXL15) 335-342 E8.4 Jy e_F15 ?=-99 Broadband flux uncertainty in AKARI L15 (15um) (DFLUXL15) 344-352 F9.5 Jy FW3 ?=-99 Broadband flux in WISE W3 (11.6 um) (FLUXW3) 354-361 E8.4 Jy e_FW3 ?=-99 Broadband flux uncertainty in WISE W3 (11.6um) (DFLUXW3) 363-370 F8.4 mag Umag ?=-99 Broadband magnitude in U (MAGU) 372-380 F9.5 mag e_Umag ?=-99 Broadband magnitude uncertainty in U (DMAGU) 382-389 F8.4 mag Bmag ?=-99 Broadband magnitude in B (MAGB) 391-399 F9.5 mag e_Bmag ?=-99 Broadband magnitude uncertainty in B (DMAGB) 401-408 F8.4 mag Vmag ?=-99 Broadband magnitude in V (MAGV) 410-418 F9.5 mag e_Vmag ?=-99 Broadband magnitude uncertainty in V (DMAGV) 420-428 F9.5 mag Imag ?=-99 Broadband magnitude in I (MAGI) 430-438 F9.5 mag e_Imag ?=-99 Broadband magnitude uncertainty in I (DMAGI) 440-448 F9.5 mag Jmag ?=-99 Broadband magnitude in J (MAGJ) 450-458 F9.5 mag e_Jmag ?=-99 Broadband magnitude uncertainty in J (DMAGJ) 460-468 F9.5 mag Hmag ?=-99 Broadband magnitude in H (MAGH) 470-478 F9.5 mag e_Hmag ?=-99 Broadband magnitude uncertainty in H (DMAGH) 480-488 F9.5 mag Ksmag ?=-99 Broadband magnitude in Ks (MAGK_S) 490-498 F9.5 mag e_Ksmag ?=-99 Broadband magnitude uncertainty in Ks (DMAGK_S) 500-508 F9.5 mag [3.6] ?=-99 Broadband magnitude in Spitzer/IRAC 3.6um (MAG3_6) 510-518 F9.5 mag e_[3.6] ?=-99 Broadband magnitude uncertainty in Spitzer/IRAC 3.6um (DMAG3_6) 520-528 F9.5 mag [4.5] ?=-99 Broadband magnitude in Spitzer/IRAC 4.5um (MAG4_5) 530-538 F9.5 mag e_[4.5] ?=-99 Broadband magnitude uncertainty in Spitzer/IRAC 4.5um (DMAG4_5) 540-548 F9.5 mag [5.8] ?=-99 Broadband magnitude in Spitzer/IRAC 5.8um (MAG5_8) 550-558 F9.5 mag e_[5.8] ?=-99 Broadband magnitude uncertainty in Spitzer/IRAC 5.8um (DMAG5_8) 560-568 F9.5 mag [8.0] ?=-99 Broadband magnitude in Spitzer/IRAC 8.0um (MAG8_0) 570-578 F9.5 mag e_[8.0] ?=-99 Broadband magnitude uncertainty in Spitzer/IRAC 8.0um (DMAG8_0) 580-588 F9.5 mag [24] ?=-99 Broadband magnitude in Spitzer/MIPS 24um (MAG24) 590-598 F9.5 mag e_[24] ?=-99 Broadband magnitude uncertainty in Spitzer/MIPS 24um (DMAG24) 600-608 F9.5 mag S11mag ?=-99 Broadband magnitude in AKARI S11 (11um) (MAGN11) 610-618 F9.5 mag e_S11mag ?=-99 Broadband magnitude uncertainty in AKARI S11 (11um) (DMAGN11) 620-628 F9.5 mag L15mag ?=-99 Broadband magnitude in AKARI L15 (15um) (MAGL15) 630-638 F9.5 mag e_L15mag ?=-99 Broadband magnitude uncertainty in AKARI L15 (15um) (DMAGL15) 640-648 F9.5 mag W3mag ?=-99 Broadband magnitude in WISE W3 (11.6um) (MAGW3) 650-658 F9.5 mag e_W3mag ?=-99 Broadband magnitude uncertainty in WISE W3 (11.6um) (DMAGW3) 660-666 A7 --- FIRGroup FIR group number (FIR_GROUP) 668-670 A3 --- SMCIRS SMC IRS identifier from Ruffle et al. (2015, Cat. J/MNRAS/451/3504) (SMC_IRS) 672-684 A13 --- SpClassS Spectroscopic classification from Ruffle et al. (2015, Cat. J/MNRAS/451/3504) (SAGESPECCLASS) 686 A1 --- GClass GRAMS chemical classification (GRAMS_CLASS) 688-693 A6 --- ClassConf Confidence of chemical classification (CLASS_CONFIDENCE) 695-705 F11.6 --- chi2Best Lowest chi-square for best-fit chemical type (CHISQ_BEST) 707-719 F13.7 --- chi2Alt Lowest chi-square for alternate chemical type (CHISQ_ALT) 721-727 E7.4 Lsun Lum ?=-99 Luminosity (LUM) 729-742 F14.8 Lsun e_Lum ?=-99 Luminosity uncertainty (DLUM) 744-751 F8.6 Msun/yr DPR ?=-99 Dust-production rate (DPR) 753-761 E9.4 Msun/yr e_DPR ?=-99 Dust-production rate uncertainty (DDPR) 763-769 E7.4 --- tau ?=-99 Optical depth at 10um (11.3um) for O-rich (C-rich) model (TAU) 771-778 E8.4 --- e_tau ?=-99 Optical depth uncertainty at 10um (11.3um) for O-rich (C-rich) model (DTAU) 780-783 F4.1 --- Rin ?=-99 Dust shell inner radius in stellar radii (RIN) 785-790 F6.2 --- e_Rin ?=-99 Dust shell inner radius uncertainty in stellar radii (DRIN) 792-800 F9.4 K Tin Temperature at dust shell inner radius (TIN) 802-810 F9.5 K e_Tin Temperature uncertainty at dust shell inner radius (DTIN) 812-815 I4 K Teff ?=-99 Effective temperature of model photosphere (TEFF) 817-819 I3 K e_Teff ?=-99 Effective temperature uncertainty of model photosphere (DTEFF) 821-826 F6.3 [cm/s2] logg ?=-99 Surface gravity of model photosphere (LOGG) 828-836 F9.5 [cm/s2] e_logg ?=-99 Surface gravity uncertainty of model photosphere (DLOGG) 838-872 A35 --- Com Fit comment (FITCOMMENT)
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 18-Nov-2016
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© Unistra/CNRS