The Most Metal-Poor Stars. I. Discovery, Data, and Atmospheric Parameters
Name
Frebel_The most 1.pdf
Size
1.1 MB
Format
Adobe PDF
Checksum (MD5)
8a95c6dbf5197eb8e5e64c14ddfb5406
Author(s)
Frebel, Anna L.
Norris, John E.
Bessell, M. S.
Yong, David
Christlieb, N.
Barklem, P. S.
Asplund, M.
Murphy, Simon J.
Beers, Timothy C.
Ryan, S. G.
Date Issued
December 2012
Journal
Astrophysical Journal
Publisher
IOP Publishing
Citation
Norris, John E. et al. “The Most Metal-Poor Stars. I. Discovery, Data, and Atmospheric Parameters.” The Astrophysical Journal 762.1 (2013): 25.
Version
Author's final manuscript
Abstract
We report the discovery of 34 stars in the Hamburg/ESO Survey for metal-poor stars and the Sloan Digital Sky Survey that have [Fe/H] [< over ~]–3.0. Their median and minimum abundances are [Fe/H] = –3.1 and –4.1, respectively, while 10 stars have [Fe/H] < –3.5. High-resolution, high signal-to-noise spectroscopic data—equivalent widths and radial velocities—are presented for these stars, together with an additional four objects previously reported or currently being investigated elsewhere. We have determined the atmospheric parameters, effective temperature (T [subscript eff]), and surface gravity (log g), which are critical in the determination of the chemical abundances and the evolutionary status of these stars. Three techniques were used to derive these parameters. Spectrophotometric fits to model atmosphere fluxes were used to derive T [subscript eff], log g, and an estimate of E(B – V); Hα, Hβ, and Hγ profile fitting to model atmosphere results provided the second determination of T [subscript eff] and log g; and finally, we used an empirical T eff-calibrated Hδ index, for the third, independent T [subscript eff] determination. The three values of T [subscript eff] are in good agreement, although the profile fitting may yield systematically cooler T [subscript eff] values, by ~100 K. This collective data set will be analyzed in future papers in the present series to utilize the most metal-poor stars as probes of conditions in the early universe.
MIT Department
Massachusetts Institute of Technology. Department of Physics
Terms of Use
Creative Commons Attribution-Noncommercial-Share Alike 3.0
Persistent DSpace Link
DOI of Published Version
https://doi.org/10.1088/0004-637X/762/1/25
