The Brown Dwarf Desert at 75-1200 AU

By C. McCarthy, B. Zuckerman. 2004

125 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

Low-Luminosity Companions to White Dwarfs (2005, background): “This value is consistent with similar searches around solar type main sequence stars for comparable sensitivities in mass and separation (Oppenheimer et al. 2001; McCarthy & Zuckerman 2004).”
How Dry is the Brown Dwarf Desert? Quantifying the Relative Number of Planets, Brown Dwarfs, and Stellar Companions around Nearby Sun-like Stars (2004, background): “However, there seems to be a brown dwarf desert – a deficit in the frequency of brown dwarf companions either relative to the frequency of less massive planetary companions (Marcy & Butler 2000) or relative to the frequency of more massive stellar companions to Sun-like hosts ( McCarthy & Zuckerman ”
Stellar, brown dwarf and multiple star properties from hydrodynamical simulations of star cluster formation (2008, background): “McCarthy & Zuckerman (2004) found that the frequency of wide brown dwarfs to G, K, and M stars between 75-300 AU was 1%±1%.”
Stellar Multiplicity and the Initial Mass Function: Most Stars Are Single (2006, background): “I note here that even if one considers substellar companions this estimate for the SSF will not likely alter significantly since as mentioned earlier, surveys have revealed a dearth of substellar companions to G, K and M stars (Marcy & Butler 2000; McCarthy and Zuckerman 2004).”
THE RUNTS OF THE LITTER: WHY PLANETS FORMED THROUGH GRAVITATIONAL INSTABILITY CAN ONLY BE FAILED BINARY STARS (2009, background): “This range of separations falls beyond the well-established inner brown dwarf “desert” (McCarthy & Zuckerman 2004), and has not been well probed due to observational difficulties at these low mass ratios.”
Stellar Multiplicity (2013, background): “Among visual companions, the stringent limits on the presence of substellar companions obtained a decade ago (≤1% ; e.g., Hinz et al. 2002, McCarthy & Zuckerman 2004, Oppenheimer et al. 2001) applied to samples largely dominated by low-mass stars.”
Discovery of Two T Dwarf Companions with the Spitzer Space Telescope (2006, methodology): “…have been performed toward young stars and brown dwarfs within 100 pc of the Sun (τ ∼ 10-400 Myr, Chauvin et al. 2003; Neuhäuser et al. 2000a; McCarthy & Zuckerman 2004; Lowrance et al. 2005), resulting in the discovery of several substellar companions that include G196-3 B (Rebolo et…”
Imaging Extrasolar Giant Planets (2016, background): “…2005), speckle cameras (Neuhäuser et al. 2003), or newly-commissioned adaptive optics systems from the ground with facility instruments (Oppenheimer et al. 2001; Macintosh et al. 2001; Chauvin et al. 2003; McCarthy & Zuckerman 2004; Carson et al. 2005; Nakajima et al. 2005; Tanner et al. 2007).”
Exploring the Frequency of Close-in Jovian Planets around M Dwarfs (2006, methodology): “We follow the procedure outlined in the Appendix of Burgasser et al. (2003) and McCarthy & Zuckerman (2004), and estimate the companion frequency f by using the binominal distribution Pd( f ) ¼ f d(1 f )N d N !”
THE PALOMAR/KECK ADAPTIVE OPTICS SURVEY OF YOUNG SOLAR ANALOGS: EVIDENCE FOR A UNIVERSAL COMPANION MASS FUNCTION (2008, background): “…with examples where the authors have resorted to by-eye identification of candidate companions (e.g., Tokovinin et al. 1999; Brandner et al. 2000; Schroeder et al. 2000; Luhman & Jayawardhana 2002; McCarthy & Zuckerman 2004; Masciadri et al. 2005; Luhman et al. 2005; Lafrenière et al. 2007).”
The Gemini Deep Planet Survey (2007, background): “…the last five years, see for example Biller et al. (2007); Chauvin et al. (2006); Metchev (2006); Lowrance et al. (2005); Masciadri et al. (2005); McCarthy & Zuckerman (2004); and Luhman & Jayawardhana (2002) for searches carried out inJ, H, or K, or Kasper et al. (2007) and Heinze et al. (2006)…”
PLANETS AROUND LOW-MASS STARS (PALMS). IV. THE OUTER ARCHITECTURE OF M DWARF PLANETARY SYSTEMS (2014, background): “…young M dwarfs with ground-based adaptive optics or the Hubble Space Telescope have primarily been sensitive to brown dwarfs at wide separations, rarely reaching 1–5 MJup limits at small separations of ∼10 AU (McCarthy & Zuckerman 2004; Lowrance et al. 2005; Daemgen et al. 2007; Allen & Reid 2008).”
LOW-MASS TERTIARY COMPANIONS TO SPECTROSCOPIC BINARIES. I. COMMON PROPER MOTION SURVEY FOR WIDE COMPANIONS USING 2MASS (2009, methodology): “We required our sample to differentiate statistically between the 1− 2% observed wide companion rate of ‘single’ stars (McCarthy & Zuckerman 2004) and the > 10% results predicted by Sterzik & Durisen (2003), Delgado-Donate et al. (2004), and Umbreit et al. (2005).”