An Orbital Radial Velocity Study of PG 1701+359, a Hot Subdwarf B Star with a Cool Main Sequence Companion

Details An Orbital Radial Velocity Study of PG 1701+359, a Hot Subdwarf B Star with a Cool Main Sequence Companion An Orbital Radial Velocity Study of PG 1701+359, a Hot Subdwarf B Star with a Cool Main Sequence Companion

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21915325l&link_type=abstract

American Astronomical Society, AAS Meeting #219, #153.25

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Many hot subdwarf B (sdB) stars show composite spectra in which the companion is typically a G or K star. Binary population synthesis (BPS) models show that these systems can be formed by Roche lobe overflow but disagree on the resulting orbital parameters; some predict long periods (years) while others predict much shorter periods (days). Little evidence currently exists to support either theory, but the few observations made to date suggest the periods are not short. At Pennsylvania State University, we conducted observations to measure the orbital parameters of such systems using the Medium Resolution Spectrograph at the Hobby-Eberly Telescope with 700 m/s precision. Here we present radial velocity (RV) measurements of PG 1701+359, the most well-studied target in our sample. We observed 14 epochs from April 2005 to July 2008 and measured the velocity of the cool companion using cross-correlation techniques. Preliminary RV variations have been detected and indicate the binary has neither a short period nor a large velocity amplitude. This material is based upon work supported by the National Science Foundation under Grant No. AST-0908642.

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