2015A&A...582A..92P


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.17CEST21:16:34

2015A&A...582A..92P - Astronomy and Astrophysics, volume 582A, 92-92 (2015/10-1)

Probing M subdwarf metallicity with an esdK5+esdM5.5 binary.

PAVLENKO Ya.V., ZHANG Z.H., GALVEZ-ORTIZ M.C., KUSHNIRUK I.O. and JONES H.R.A.

Abstract (from CDS):

We present a spectral analysis of the binary G 224-58 AB, which consists of the coolest M extreme subdwarf (esdM5.5) and a brighter primary (esdK5). This binary may serve as a benchmark for metallicity measurement calibrations and as a test bed for atmospheric and evolutionary models for esdM objects. We perform the analysis of optical and infrared spectra of both components to determine their parameters. We determine abundances primarily using high-resolution optical spectra of the primary. Other parameters were determined from the fits of synthetic spectra computed with these abundances to the observed spectra from 0.4 to 2.5-microns for both components. We determine Teff=4625±100K, logg=4.5±0.5 for the A component and Teff=3200±100K, logg=5.0±0.5, for the B component. We obtained abundances of [Mg/H]=-1.51±0.08, [Ca/H]=-1.39±0.03, [Ti/H]=-1.37±0.03 for alpha group elements and [CrH]=-1.88±0.07, [Mn/H]=-1.96±0.06, [Fe/H]=-1.92±0.02, [Ni/H]=-1.81±0.05 and [Ba/H]=-1.87±0.11 for iron group elements from fits to the spectral lines observed in the optical and infrared spectral regions of the primary. We find consistent abundances with fits to the secondary albeit at lower signal to noise. Abundances of different elements in G 224-58 A and G 224-58 B atmospheres cannot be described by one metallicity parameter. The offset of ∼0.4dex between the abundances derived from alpha element and iron group elements corresponds with our expectation for metal-deficient stars. We thus clarify that some indices used to date to measure metallicities for establishing esdM stars, based on CaH, MgH, and TiO band system strength ratios in the optical and H2O in the infrared, relate to abundances of alpha-element group rather than to iron peak elements. For metal deficient M dwarfs with [Fe/H]←1.0, this provides a ready explanation for apparently inconsistent metallicities derived with different methods.

Abstract Copyright:

Journal keyword(s): stars: abundances - stars: low-mass - stars: Population II - stars: late-type - stars: individual: G 224-58 A - binaries: spectroscopic

Simbad objects: 5

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Number of rows : 5

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 SCG2 0018-4854 CGG 00 21 23.0 -48 38 20   13.91       ~ 16 0
2 Cl Melotte 25 OpC 04 26 54.00 +15 52 00.0           ~ 2581 0
3 LP 251-35 PM* 05 22 05.3054965945 +38 14 14.636995453   16.6 16.25 14.6   esdM3.0 17 0
4 G 224-58 PM* 15 16 49.877 +60 54 36.08   14.33   13.18   ~ 7 0
5 G 224-58B LM* 15 16 50.3388641635 +60 53 05.326514677   21.0   18.9   M4V 6 0

    Equat.    Gal    SGal    Ecl

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2019.10.17-21:16:34

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