Details

Autor(en) / Beteiligte

• Nielsen, Eric L
• Liu, Michael C
• WAHHAJ, ZAHED
• Biller, Beth A
• Hayward, Thomas L
• Close, Laird M
• Males, Jared R
• Skemer, Andrew J
• Chun, Mark
• Ftaclas, Christ

Titel

THE GEMINI NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF GIANT PLANETS AROUND YOUNG B AND A STARS

Ist Teil von

• The Astrophysical journal, 2013-10, Vol.776 (1), p.1-35

Ort / Verlag

United States

Erscheinungsjahr

2013

Quelle

Electronic Journals Library

Beschreibungen/Notizen

• We have carried out high contrast imaging of 70 young, nearby B and A stars to search for brown dwarf and planetary companions as part of the Gemini NICI Planet-Finding Campaign. Our survey represents the largest, deepest survey for planets around high-mass stars ([approx =]1.5-2.5 M sub([middot in circle])) conducted to date and includes the planet hosts [beta] Pic and Fomalhaut. We obtained follow-up astrometry of all candidate companions within 400 AU projected separation for stars in uncrowded fields and identified new low-mass companions to HD 1160 and HIP 79797. We have found that the previously known young brown dwarf companion to HIP 79797 is itself a tight (3 AU) binary, composed of brown dwarfs with masses 58 super(+21) sub(-20) M sub(Jup) and 55 super(+20) sub(-19) M sub(Jup), making this system one of the rare substellar binaries in orbit around a star. Considering the contrast limits of our NICI data and the fact that we did not detect any planets, we use high-fidelity Monte Carlo simulations to show that fewer than 20% of 2 M sub([middot in circle]) stars can have giant planets greater than 4 M sub(Jup) between 59 and 460 AU at 95% confidence, and fewer than 10% of these stars can have a planet more massive than 10 M sub(Jup) between 38 and 650 AU. Overall, we find that large-separation giant planets are not common around B and A stars: fewer than 10% of B and A stars can have an analog to the HR 8799 b (7 M sub(Jup), 68 AU) planet at 95% confidence. We also describe a new Bayesian technique for determining the ages of field B and A stars from photometry and theoretical isochrones. Our method produces more plausible ages for high-mass stars than previous age-dating techniques, which tend to underestimate stellar ages and their uncertainties.