2010MNRAS.407.1203D


C.D.S. - SIMBAD4 rel 1.7 - 2020.03.31CEST15:19:54

2010MNRAS.407.1203D - Mon. Not. R. Astron. Soc., 407, 1203-1211 (2010/September-2)

The potential of red supergiants as extragalactic abundance probes at low spectral resolution.

DAVIES B., KUDRITZKI R.-P. and FIGER D.F.

Abstract (from CDS):

Red supergiants (RSGs) are among the brightest stars in the local Universe, making them ideal candidates with which to probe the properties of their host galaxies. However, current quantitative spectroscopic techniques require spectral resolutions of R ≳ 17000, making observations of RSGs at distances greater than 1 Mpc unfeasible. Here we explore the potential of quantitative spectroscopic techniques at much lower resolutions, R ~ 2-3000. We take archival J-band spectra of a sample of RSGs in the solar neighbourhood. In this spectral region the metallic lines of Fei, Mgi, Sii and Tii are prominent, while the molecular absorption features of OH, H2O, CN and CO are weak. We compare these data with synthetic spectra produced from the existing grid of model atmospheres from the MARCS project, with the aim of deriving chemical abundances. We find that all stars studied can be unambiguously fitted by the models, and model parameters of logg, effective temperatures Teff, microturbulence and global metal content may be derived. We find that the abundances derived for the stars are all very close to solar and have low dispersion, with an average of logZ = 0.13±0.14. The values of Teff fitted by the models are ∼ 150K cooler than the stars' literature values for earlier spectral types when using the Levesque et al. temperature scale, though we find that this discrepancy may be reduced at spectral resolutions of R = 3000 or higher. In any case, the temperature discrepancy has very little systematic effect on the derived abundances as the equivalent widths (EWs) of the metallic lines are roughly constant across the full temperature range of RSGs. Instead, elemental abundances are the dominating factor in the EWs of the diagnostic lines. Our results suggest that chemical abundance measurements of RSGs are possible at low to medium resolution, meaning that this technique is a viable infrared-based alternative to measuring abundance trends in external galaxies.

Abstract Copyright: © 2010 The Authors. Journal compilation © 2010 RAS

Journal keyword(s): stars: abundances - stars: late-type - stars: massive - supergiants - galaxies: abundances - galaxies: stellar content

Status at CDS:  

Simbad objects: 20

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Number of rows : 20

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME Eridanus ClG GrG 00 30 00 -21 30.0           ~ 143 0
2 BD+60 265 s*r 01 33 33.1682719604 +61 33 29.671604685   10.73 8.43     M0.5Iab 20 0
3 V* V366 And LP* 01 43 11.1052384676 +48 31 00.365981543   8.64 6.79     M2Ib 44 0
4 V* PR Per s*r 02 21 42.4096612239 +57 51 46.148946906 12.84 10.31 8.00 6.13 4.60 M1-Iab-Ib 101 0
5 V* SU Per s*r 02 22 06.8945607706 +56 36 14.896842798 13.86 11.57 9.40     M3-M4Iab 131 0
6 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5543 1
7 ACO S 373 ClG 03 38 30 -35 27.3           ~ 1513 0
8 V* V362 Aur LP* 05 27 10.2178548171 +29 55 15.796759307   9.58 7.32     M1.5Ib 76 0
9 * alf Ori s*r 05 55 10.30536 +07 24 25.4304 4.38 2.27 0.42 -1.17 -2.45 M1-M2Ia-Iab 1456 0
10 V* V384 Pup s*r 07 41 02.6294401083 -31 40 59.093363040   10.81 8.77     M3Iab-Ib 43 0
11 V* QY Pup s*r 07 47 38.5263889310 -15 59 26.480009421   8.095 6.309     K1Ia-Iab 77 0
12 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5747 0
13 * alf Her ** 17 14 38.85818 +14 23 25.2262   4.51 3.06     M5Ib-II+G5III+F2V: 188 0
14 V* V340 Sge LP? 19 39 25.3354745662 +16 34 16.036192017   8.330 6.344     K4Ib 76 0
15 HD 187238 * 19 48 11.8385353558 +22 45 46.343064783 11.27 9.23 7.19 5.60 4.59 K2Iab-Ib 45 0
16 V* NR Vul s*r 19 50 11.9279772343 +24 55 24.177460007   12.41 9.36 6.60 4.49 M1Ia: 70 0
17 V* RW Cyg s*r 20 28 50.5902663365 +39 58 54.418023246 13.00 10.60 8.00 5.32 3.25 M3-M4Ia-Iab 109 0
18 V* RW Cep s*r 22 23 07.0152079533 +55 57 47.616196874 11.25 8.87 6.65 4.94 3.78 K2_0-Ia 148 0
19 V* V424 Lac LP* 22 56 25.9984806807 +49 44 00.751810487 8.66 6.71 4.94 3.59 2.54 K5Ib 141 0
20 NAME Pup Cluster ClG ~ ~           ~ 20 0

    Equat.    Gal    SGal    Ecl

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2020.03.31-15:19:55

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