High-Precision Near-Infrared Photometry of a Large Sample of Bright Stars Visible from the Northern Hemisphere

Kidger, M.; Martín-Luis, F.

doi:10.1086/374996

Cited by 37 publications

(48 citation statements)

References 18 publications

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“…d GJ 504b's effective temperature, surface gravity, bolometric luminosity, and mass are estimated by comparing its age (160 +350 −60 Myr) and J H K s L -band magnitude with the most commonly used cooling model (Baraffe et al 2003). For quantifying best estimates and lower/upper limits for all of these quantities, we apply the same calculation as described in Section 4.2. e The provided errors of the stellar J H K photometry are less than 0.01 mag (Kidger & Martín-Luis 2003), while L photometry was obtained in this work with an error of 0.09 mag (see Section 3.5). f The H-band photometric magnitude is based on the weighted mean of the March and May values.…”

Section: Age Of Gj 504mentioning

confidence: 65%

Direct Imaging of a Cold Jovian Exoplanet in Orbit Around the Sun-Like Star Gj 504

Kuzuhara

Tamura

Kudo

et al. 2013

ApJ

224

170

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Direct Imaging of a Cold Jovian Exoplanet in Orbit around the Sun-like Star GJ 504Kuzuhara, M.; et al., [Unknown]; Thalmann, C.D. General rightsIt is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulationsIf you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: http://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. Download date: 13 May 2018The Astrophysical Journal, 774:11 (18pp) ABSTRACT Several exoplanets have recently been imaged at wide separations of >10 AU from their parent stars. These span a limited range of ages (<50 Myr) and atmospheric properties, with temperatures of 800-1800 K and very red colors (J − H > 0.5 mag), implying thick cloud covers. Furthermore, substantial model uncertainties exist at these young ages due to the unknown initial conditions at formation, which can lead to an order of magnitude of uncertainty in the modeled planet mass. Here, we report the direct-imaging discovery of a Jovian exoplanet around the Sun-like star GJ 504, detected as part of the SEEDS survey. The system is older than all other known directly imaged planets; as a result, its estimated mass remains in the planetary regime independent of uncertainties related to choices of initial conditions in the exoplanet modeling. Using the most common exoplanet cooling model, and given the system age of 160 +350 −60 Myr, GJ 504b has an estimated mass of 4 +4.5 −1.0 Jupiter masses, among the lowest of directly imaged planets. Its projected separation of 43.5 AU exceeds the typical outer boundary of ∼30 AU predicted for the core accretion mechanism. GJ 504b is also significantly cooler (510 +30 −20 K) and has a bluer color (J − H = −0.23 mag) than previously imaged exoplanets, suggesting a largely cloud-free atmosphere accessible to spectroscopic characterization. Thus, it has the potential of providing novel insights into the origins of giant planets as well as their atmospheric properties.

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Section: Age Of Gj 504mentioning

confidence: 65%

Direct Imaging of a Cold Jovian Exoplanet in Orbit Around the Sun-Like Star Gj 504

Kuzuhara

Tamura

Kudo

et al. 2013

ApJ

224

170

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“…(c) Morel et al (1978); Bessell et al (1998);Ducati et al (2002). (d) Glass (1974); Glass (1975); Mould & Hyland (1976); Morel et al (1978); Leggett (1992); Ducati et al (2002); Kidger & Martín-Luis (2003); the 2MASS catalogue (Cutri et al 2003). (e) We refered to Colina et al (1996) for the apparent magnitudes of the Sun.…”

Section: Resultsmentioning

confidence: 99%

The angular sizes of dwarf stars and subgiants

Kervella

Thévenin

Folco

et al. 2004

A&A

495

546

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Abstract. The availability of a number of new interferometric measurements of Main Sequence and subgiant stars makes it possible to calibrate the surface brightness relations of these stars using exclusively direct angular diameter measurements. These empirical laws make it possible to predict the limb darkened angular diameters θ LD of dwarfs and subgiants using their dereddened Johnson magnitudes, or their effective temperature. The smallest intrinsic dispersions of σ ≤ 1% in θ LD are obtained for the relations based on the K and L magnitudes, for instance logOur calibrations are valid between the spectral types A0 and M2 for dwarf stars (with a possible extension to later types when using the effective temperature), and between A0 and K0 for subgiants. Such relations are particularly useful for estimating the angular sizes of calibrators for long-baseline interferometry from readily available broadband photometry.

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“…Whereas the result of the Hipparcos photometric observation estimated that the star remains in an MS stage with a spectral type of K1 V, recent reports showed a spectral type of M2 III (Kidger et al 2003;Tsvetkov et al 2008). The color index of HD 220074 was estimated to be approximately 1.7 by Hipparcos data, which was reduced afresh by Leeuwen (2007) and shows the same result.…”

Section: Fundamental Parametersmentioning

confidence: 86%

“…The V − K color of 4.39 is similar to an M2 giant (V − K = 4.30) in Bessel & Brett (1988), which also indicates that the star is likely to be a giant. As a result, HD 220074 should be an M2 giant star (Kidger et al 2003;Tsvetkov et al 2008). …”

Section: Fundamental Parametersmentioning

confidence: 99%

Planetary companions orbiting M giants HD 208527 and HD 220074

Lee

Han

Park

2012

A&A

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Aims. The purpose of the present study is to research the origin of planetary companions by using a precise radial velocity (RV) survey. Methods. The high-resolution spectroscopy of the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) at Bohyunsan Optical Astronomy Observatory (BOAO) was used from September 2008 to June 2012. Results. We report the detection of two exoplanets in orbit around HD 208527 and HD 220074 exhibiting periodic variations in RV of 875.5 ± 5.8 and 672.1 ± 3.7 days. The RV variations are not apparently related to the surface inhomogeneities, and a Keplerian motion of the planetary companion is the most likely explanation. Assuming possible stellar masses of 1.6 ± 0.4 and 1.2 ± 0.3 M , we obtain the minimum masses for the exoplanets at 9.9 ± 1.7 and 11.1 ± 1.8 M Jup around HD 208527 and HD 220074 with orbital semi-major axes of 2.1 ± 0.2 and 1.6 ± 0.1 AU and eccentricities of 0.08 and 0.14, respectively. We also find that the previously known spectral classification of HD 208527 and HD 220074 was in error. Our new estimation of stellar parameters suggests that both HD 208527 and HD 220074 are M giants. Therefore, HD 208527 and HD 220074 are so far the first candidate M giants found to harbor a planetary companion.

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High-Precision Near-Infrared Photometry of a Large Sample of Bright Stars Visible from the Northern Hemisphere

Cited by 37 publications

References 18 publications

Direct Imaging of a Cold Jovian Exoplanet in Orbit Around the Sun-Like Star Gj 504

Direct Imaging of a Cold Jovian Exoplanet in Orbit Around the Sun-Like Star Gj 504

The angular sizes of dwarf stars and subgiants

Planetary companions orbiting M giants HD 208527 and HD 220074

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