Journal
ASTROPHYSICAL JOURNAL
Volume 728, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/728/1/32
Keywords
brown dwarfs; stars: low-mass; techniques: radial velocities
Categories
Funding
- W.M. Keck Foundation
- NSF [AST-0705139, AST-0349075, 0645416, AST 08-02230]
- SDSS-III consortium
- NASA [NNX07AP14G]
- University of Florida
- Alfred P. Sloan Foundation
- Participating Institutions
- National Science Foundation
- US Department of Energy
- National Aeronautics and Space Administration
- Center for Exoplanets and Habitable Worlds
- Pennsylvania State University
- Eberly College of Science
- Pennsylvania Space Grant Consortium
- Vanderbilt Initiative in Data-Intensive Astrophysics (VIDA)
- Vanderbilt University
- CNPq [476909/2006-6]
- FAPERJ [APQ1/26/170.687/2004]
- University of Arizona
- Brazilian Participation Group
- University of Cambridge
- French Participation Group
- German Participation Group
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- New Mexico State University
- New York University
- Ohio State University
- University of Portsmouth
- Princeton University
- University of Tokyo
- University of Utah
- University of Virginia
- University of Washington
- Yale University
- Vanderbilt Initiative in Data-Intensive Astrophysics (VIDA) from Vanderbilt University
Ask authors/readers for more resources
We present a new short-period brown dwarf (BD) candidate around the star TYC 1240-00945-1. This candidate was discovered in the first year of the Multi-object APO Radial Velocity Exoplanets Large-area Survey (MARVELS), which is part of the Sloan Digital Sky Survey (SDSS) III, and we designate the BD as MARVELS-1b. MARVELS uses the technique of dispersed fixed-delay interferometery to simultaneously obtain radial velocity (RV) measurements for 60 objects per field using a single, custom-built instrument that is fiber fed from the SDSS 2.5 m telescope. From our 20 RV measurements spread over a similar to 370 day time baseline, we derive a Keplerian orbital fit with semi-amplitude K = 2.533 +/- 0.025 km s(-1), period P = 5.8953 +/- 0.0004 days, and eccentricity consistent with circular. Independent follow-up RV data confirm the orbit. Adopting a mass of 1.37 +/- 0.11 M-circle dot for the slightly evolved F9 host star, we infer that the companion has a minimum mass of 28.0 +/- 1.5 M-Jup, a semimajor axis 0.071 +/- 0.002 AU assuming an edge-on orbit, and is probably tidally synchronized. We find no evidence for coherent intrinsic variability of the host star at the period of the companion at levels greater than a few millimagnitudes. The companion has an a priori transit probability of similar to 14%. Although we find no evidence for transits, we cannot definitively rule them out for companion radii less than or similar to 1 R-Jup.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available