Astronomy and Astrophysics – Astrophysics – Solar and Stellar Astrophysics
Scientific paper
2012-04-19
Astronomy and Astrophysics
Astrophysics
Solar and Stellar Astrophysics
Accepted by A&A, 18 pages, 11 figures, 2 figures in Appendix, 7 tables. Paper not yet corrected by A&A language editor
Scientific paper
The aim of the project is to improve our knowledge on the low-mass and low-metallicity population to investigate the influence of metallicity of the stellar (and substellar) mass function. We present the results of a photometric and proper motion search aimed at unearthing ultracool subdwarfs in large-scale surveys. We employed and combined the UKIDSS LAS DR5 and the SDSS DR7 complemented with ancillary data from 2MASS, DENIS and SuperCOSMOS. The SDSS DR7 vs UKIDSS LAS DR5 search returned a total of 32 ultracool subdwarf candidates, only two being recognised as a subdwarf in the literature. Twenty-seven candidates were followed-up spectroscopically in the optical between 600 and 1000 nm. We confirmed 20 candidates as subdwarfs, extreme subdwarfs or ultra-subdwarfs with spectral types later than M5; this represents a success rate of ~60%. Among those 20 new subdwarfs, we identified 2 early-L subdwarfs very likely located within 100 pc that we propose as templates for future searches because they are the first examples of their subclass. Another 7 sources are solar-metallicity M dwarfs with spectral types between M4 and M7 without Halpha emission, suggesting that they are old M dwarfs. The remaining 5 candidates do not have spectroscopic follow-up yet; only 1 remains as a bona-fide ultracool subdwarf after revision of their proper motions. We assigned spectral types based on the current classification schemes and, when possible, we measured their radial velocities. Using the limited number of subdwarfs with trigonometric parallaxes, we estimated distances between 90 and 600 for the new subdwarfs. We provide mid-infrared photometry from WISE for two subdwarfs and discuss their colours. Finally, we estimate a lower limit of the surface density of ultracool subdwarfs of the order of 5000-5700 times lower than that of solar-metallicity late-M dwarfs (Shortened).
Aberasturi M.
Contreras Espinoza M.
Lodieu Nicolas
Martin Eduardo L.
Solano Enrique
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