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

¹ Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, Hertfordshire AL10 9AB, UK
e-mail: email2yp@gmail.com
² Main Astronomical Observatory, Academy of Sciences of the Ukraine, Golosiiv Woods, 03680 Kyiv-127, Ukraine
³ Instituto de Astrofísika de Canarias, 38205, La Laguna, Tenerife, Spain
⁴ Universidad de La Laguna, Dept. Astrofísica, 38206, La Laguna, Tenerife, Spain
⁵ Centro de Astrobiología (CSIC-INTA), Ctra. Ajalvir km 4, 28850 Torrejón de Ardoz, Madrid, Spain
⁶ Taras Shevchenko National University of Kyiv, 60 Volodymyrska Str., 01033 Kyiv, Ukraine

Received: 23 June 2015
Accepted: 28 July 2015

Abstract

Context. 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.

Aims. We perform the analysis of optical and infrared spectra of both components to determine their parameters.

Methods. 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.

Results. We determine T_eff = 4625 ± 100 K, log  g = 4.5 ± 0.5 for the A component and T_eff = 3200 ± 100 K, log  g = 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.

Conclusions. 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 ∼0.4 dex 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.