The Gemini Deep Planet Survey

By D. Lafrèniere, R. Doyon, C. Marois, D. Nadeau, B. Oppenheimer, P. Roche, F. Rigaut, J. Graham, R. Jayawardhana, D. Johnstone and 3 more. 2007

256 citations recorded by the source corpus.

We present the results of the Gemini Deep Planet Survey, a near-infrared adaptive optics search for giant planets and brown dwarfs around 85 nearby young stars. The observations were obtained with the Altair adaptive optics system at the Gemini North telescope, and angular differential imaging was used to suppress the speckle noise of the central star. Typically, the observations are sensitive to angular separations beyond 0.5'' with 5 σ contrast sensitivities in magnitude difference at 1.6 μm of 9.5 at 0.5'', 12.9 at 1'', 15.0 at 2'', and 16.5 at 5''. These sensitivities are sufficient to detect planets more massive than 2 MJ with a projected separation in the range 40-200 AU around a typical target. Second-epoch observations of 48 stars with candidates (out of 54) have confirmed that all candidates are unrelated background stars. A detailed statistical analysis of the survey results is presented. Assuming a planet mass distribution dn/dm ∝ m-1.2 and a semimajor-axis distribution dn/da ∝ a-1, the 95% credible upper limits on the fraction of stars with at least one planet of mass 0.5-13 MJ are 0.28 for the range 10-25 AU, 0.13 for 25-50 AU, and 0.093 for 50-250 AU; this result is weakly dependent on the semimajor-axis distribution power-law index. The 95% credible interval for the fraction of stars with at least one brown dwarf companion having a semimajor axis in the range 25-250 AU is 0.019, irrespective of any assumption on the mass and semimajor-axis distributions. The observations made as part of this survey have resolved the stars HD 14802, HD 166181, and HD 213845 into binaries for the first time.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/c243ef42c2cf8052ff014ff6d9285d419e084542

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In Astronomy and Astrophysics

1. B. Bowler
2. Michael C. Liu
3. Jon Fortney
4. M. Marley
5. T. Dupuy
6. N. Madhusudhan
7. Adam Burrows
8. A. Kraus

Citations in the corpus

• Direct Imaging and Spectroscopy of a Planetary-Mass Candidate Companion to a Young Solar Analog (2008, background): “However, due to the small angular separation and the high brightness contrast between a planet and its star, direct imaging has not succeeded thus far (e.g. Lafrenière et al. 2007, and referenc s therein).”
• Dynamical Outcomes of Planet-Planet Scattering (2007, background): “This trend can be verified in future observations using adaptive optics to detect and image giant planets further out (40–100 AU) from the central star (Lafrenière et al. 2007).”
• Nearby stars of the Galactic disc and halo – IV (2008, unknown): “Recent direct imaging observations of 84 Cet by Lafrenière et al. (2007), on the other hand, give no hint for a low-mass ‘Ab’ companion at separations beyond ρ = 0.72 arcsec, although the latter number is of course not unexpected for dynamical stability reasons with the more distant 84 Cet B.”
• PLANETS AROUND LOW-MASS STARS (PALMS). IV. THE OUTER ARCHITECTURE OF M DWARF PLANETARY SYSTEMS (2014, methodology): “The analysis of 100 FGK stars by Nielsen & Close (2010), which combined the surveys of Masciadri et al. (2005), Biller et al. (2007), and Lafrenière et al. (2007a), is the largest study of wideperiod planets around 0.6–1.2 M⊙ host stars to date.”
• Synthetic Spectra and Colors of Young Giant Planet Atmospheres: Effects of Initial Conditions and Atmospheric Metallicity (2008, background): “INTRODUCTION Astronomers around the world are making significant efforts to image planets in orbit around other stars (Beuzit et al. 2007; Nielsen et al. 2007; Lafrenière et al. 2007; Apai et al. 2008).”
• Forming the cores of giant planets from the radial pebble flux in protoplanetary discs (2014, background): “Although likely a rare system (Lafrenière et al. 2007), such planets in wide orbits can be formed in the pebble accretion scenario.”
• THE GEMINI/NICI PLANET-FINDING CAMPAIGN: THE FREQUENCY OF PLANETS AROUND YOUNG MOVING GROUP STARS (2013, methodology): “Based on a sample of 118 stars compiled from the surveys of Masciadri et al. (2005), Biller et al. (2007), and Lafrenière et al. (2007a), Nielsen & Close (2010) found that planets more massive than 4 MJup are found around <20% of FGKM stars in orbits between 22 and 507 AU, at 95% confidence.”
• The properties of brown dwarfs and low-mass hydrogen-burning stars formed by disc fragmentation (2008, result): “This is consistent with the results of the Gemini Deep Planet Survey that found a very low probability of BDs (with m < 40 MJ in the region 25-250 AU (∼ 1.9%; Lafrenière et al. 2007).”
• The Volume-limited A-Star (VAST) survey – I. Companions and the unexpected X-ray detection of B6–A7 stars (2011, methodology): “Alignment of short-exposure images was achieved through Gaussian centroiding, while the saturated exposures were aligned by cross-correlating the diffraction spikes (e.g. Lafrenière et al. 2007).”
• NEAR-INFRARED SPECTROSCOPY OF THE EXTRASOLAR PLANET HR 8799 b (2010, methodology): “High contrast adaptive optics (AO) observations on large telescopes are beginning to explore the outer architecture ( 10 AU) of planetary systems for the first time (e.g., Biller et al. 2007; Lafrenière et al. 2007b; Liu et al. 2009; Chauvin et al. 2010).”
• Mapping the Shores of the Brown Dwarf Desert. I. Upper Scorpius (2007, methodology): “To turn the measured detection limits and detections into estimates of the companion frequency distributions, we have employed a statistical framework similar to that of Carson et al. (2006), Lafrenière et al. (2007) and Evans et al. (2012).”
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• TWO WIDE PLANETARY-MASS COMPANIONS TO SOLAR-TYPE STARS IN UPPER SCORPIUS (2010, background): “…have included lunar occultation (e.g. Simon et al. 1995), speckle interferometry (e.g. Ghez et al. 1993), Adaptive Optics (AO) imaging (e.g. Lafrenière et al. 2007; Masciadri et al. 2005; Chauvin et al. 2010), and most recently non-redundant masking (NRM) inteferometry (Kraus et al. 2008).”
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