The unseen companion of HD114762: a probable brown dwarf

“…We note that massive planets around normal dwarf stars may already be detected by the Digital Speedometer, such as the case of HAT-P-2b (see later Fig. 4) or the early result of Latham et al (1989).…”

Section: Reconaissance Spectroscopymentioning

confidence: 99%

Search for Transiting Exoplanets with HATNet

et al. 2008

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Abstract.HATNet is a network of six identical, fully automated wide field telescopes, four of which are located in Arizona, and two at Hawaii. The purpose of the network is to search for transiting extrasolar planets around relatively bright stars (8 < I < 12). The longitudinal coverage of 3.5 hours greatly enhances transit detection efficiency. HATNet has been operational since 2004, and has taken more than 1/2 million science frames at 5-min integrations, covering about 7% of the sky. Photometric precision reaches 3 mmag rms at 5.5 min cadence at I ≈ 8, and is 1% at I ≈ 11.3. Hundreds of transit candidates have been detected in the data, and have been subject to vigorous follow-up by various 1m-class facilities, both spectroscopy and follow-up photometry. A fraction of the candidates that have survived these steps as not being false alarms have been observed by high resolution and precision spectrographs (primarily Keck/HIRES), to confirm their planetary nature and characterize their properties. So far nine transiting planets have been reported, making HATNet a very successful survey.

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“…Defined as objects found using the high-precision radial-velocity technique around stars with little or no intrinsic variability and previously thought to be without companions, the rv60 extrasolar giant planets (EGPs; Burrows et al 1995) that have been discovered to date span more than two orders of magnitude in mpsin(i), semi-major axis, and period Cochran et al 1997;Delfosse et al 1998;Fischer et al 1999;Henry et al 2000;Korzennik et al 2000;Latham et al 1989;Marcy and Butler 1996;Marcy et al 1999;Marcy, Butler, and Vogt 2000;Marcy, Cochran, and Major 2000;Mayor and Queloz 1995;Mazeh et al 2000;Noyes et al 1997;Queloz et al 2000;Santos et al 2000;Ddry et al 2000;Vogt et al 2000;and references therein). Collectively, EGPs show the wide range of eccentricities typical of stellar companions, while those within rvO.07 A.D. have the small eccentricities expected for objects that have experienced significant tidal dissipation.…”

Section: New Worldsmentioning

confidence: 99%