A Radial Velocity Study of Hot Subdwarf B Stars with Cool Main Sequence Companions

Details A Radial Velocity Study of Hot Subdwarf B Stars with Cool Main Sequence Companions A Radial Velocity Study of Hot Subdwarf B Stars with Cool Main Sequence Companions

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21940803b&link_type=abstract

American Astronomical Society, AAS Meeting #219, #408.03

Astronomy and Astrophysics

Astronomy

Scientific paper

Many hot subdwarf B (sdB) stars show composite spectra and energy distributions indicative of G- or K-type main sequence companions. Binary population synthesis (BPS) models demonstrate such systems can be formed by Roche lobe overflow but disagree on whether the resulting orbital periods will be long (years) or short (days). Few studies have been carried out to assess the orbital parameters of these composite binaries; what little observations there are suggest the periods are long. To help address this problem, we selected fifteen moderately-bright (V 13) sdB stars with composite spectra for synoptic radial velocity (RV) monitoring. From January 2005 to July 2008, we acquired between 4 and 14 observations of each target using the bench-mounted Medium Resolution Spectrograph on the Hobby-Eberly Telescope. Cross-correlation techniques were used to measure RVs from the cool companion lines with 700 m/s precision. Here we present RV measurements and orbital parameter estimates (when appropriate) for all systems in our sample and discuss the constraints they place on BPS models. Preliminary measurements of PG 1701+359, the most well-studied object in our sample, indicate the orbit has neither a short period nor a high velocity amplitude. This material is based upon work supported by the National Science Foundation under Grant No. AST-0908642.

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