GQLup and its common proper motion companion

Mugrauer, M.; Neuhaeuser, R.

doi:10.1002/asna.200510410

Cited by 25 publications

(27 citation statements)

References 30 publications

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“…At a known distance, d, the constraint on the stellar mass can be recast as * =  * M d 1.03 0.05 156 pc ( ) ( ) , where the formal uncertainty on M * is ∼5% including systematic uncertainties estimated from more complex models (e.g., vertical structure, see Rosenfeld et al 2013). Previous estimates of the stellar mass of GQ Lup A from the literature are mostly lower than our determination, ranging between 0.7 and 1.05 M e (see discussion in Section 2, Mugrauer & Neuhäuser 2005;Seperuelo Duarte et al 2008;Donati et al 2012). The discrepancy in mass estimates results largely from differences in stellar evolutionary models and uncertainty in the effective temperature.…”

Section: ( )contrasting

confidence: 78%

“…Although they adopt a much higher effective temperature of 4300±50 K, Donati et al (2012) obtain a comparable stellar radius of 1.7±0.2 R e . Previous estimates of the mass of GQ Lup A vary between 0.7 and 1.05 M e , largely depending on the evolutionary models and effective temperatures used (Mugrauer & Neuhäuser 2005;Seperuelo Duarte et al 2008;Donati et al 2012). Adopting the higher effective temperature of 4300 K yields a mass of 1.05± 0.07 M e , the upper value in this range (Donati et al 2012).…”

Section: The Gq Lup Systemmentioning

confidence: 99%

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Alma Measurements of Circumstellar Material in the Gq Lup System

MacGregor

Wilner

Czekala

et al. 2017

ApJ

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We present Atacama Large Millimeter/submillimeter Array observations of the GQ Lup system, a young Sun-like star with a substellar-mass companion in a wide-separation orbit. These observations of 870 μm continuum and CO J=3-2 line emission with beam size ∼0 3 (∼45 au) resolve the disk of dust and gas surrounding the primary star, GQ Lup A, and provide deep limits on any circumplanetary disk surrounding the companion, GQ Lup b. The circumprimary dust disk is compact with an FWHM of 59±12 au, while the gas has a larger extent with a characteristic radius of 46.5±1.8 au. By forward-modeling the velocity field of the circumprimary disk based on the CO emission, we constrain the mass of GQ LupA to be M * =(1.03±0.05) * (d/156 pc) M e , where d is a known distance, and determine that we view the disk at an inclination angle of 60°.5±0°.5 and a position angle of 346°±1°. The 3σ upper limit on the 870 μm flux density of any circumplanetary disk associated with GQ Lup b of <0.15 mJy implies an upper limit on the dust disk mass of <0.04 M ⊕ for standard assumptions about optically thin emission. We discuss proposed mechanisms for the formation of wide-separation substellar companions given the non-detection of circumplanetary disks around GQ Lup b and other similar systems.

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Section: ( )contrasting

confidence: 78%

Section: The Gq Lup Systemmentioning

confidence: 99%

Alma Measurements of Circumstellar Material in the Gq Lup System

MacGregor

Wilner

Czekala

et al. 2017

ApJ

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“…At a projected distance of ∼440 AU, the system is probably still below the long-term stability limit of ∼700 AU for a K 7 primary star of 0.7 M , following the argumentation of Weinberg et al (1987) and Close et al (2003) (see also Mugrauer & Neuhäuser 2005, for a discussion).…”

Section: Mass Estimation and Discussionmentioning

confidence: 89%

Direct evidence of a sub-stellar companion around CT Chamaeleontis

Schmidt¹,

Neuhäuser²,

Seifahrt

et al. 2008

A&A

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Aims. In our ongoing search for close and faint companions around T Tauri stars in the Chamaeleon star-forming region, we here present observations of a new common proper motion companion to the young T-Tauri star and Chamaeleon member CT Cha and discuss its properties in comparison to other young, low-mass objects and to synthetic model spectra from different origins. Methods. Common proper motion of the companion and CT Cha was confirmed by direct Ks-band imaging data taken with the VLT Adaptive Optics (AO) instrument NACO in February 2006 and March 2007, together with a Hipparcos binary for astrometric calibration. An additional J-band image was taken in March 2007 to obtain color information for a first classification of the companion. Moreover, AO integral field spectroscopy with SINFONI in J, and H + K bands was obtained to deduce physical parameters of the companion, such as temperature and extinction. Relative flux calibration of the bands was achieved using photometry from the NACO imaging data. Results. We found a very faint (Ks = 14.9 mag, Ks 0 = 14.4 mag) object, just ∼2.67 northwest of CT Cha corresponding to a projected separation of ∼440 AU at 165 ± 30 pc. We show that CT Cha A and this faint object form a common proper motion pair and that the companion is by ≥4σ significance not a stationary background object. The near-infrared spectroscopy yields a temperature of 2600 ± 250 K for the companion and an optical extinction of A V = 5.2 ± 0.8 mag, when compared to spectra calculated from Drift-Phoenix model atmospheres. We demonstrate the validity of the model fits by comparison to several other well-known young sub-stellar objects. Conclusions. We conclude that the CT Cha companion is a very low-mass member of Chamaeleon and very likely a physical companion to CT Cha, as the probability for a by chance alignment is ≤0.01. Due to a prominent Pa-β emission in the J-band, accretion is probably still ongoing onto the CT Cha companion. From temperature and luminosity (log(L bol /L ) = -2.68 ± 0.21), we derive a radius of R = 2.20 +0.81 −0.60 R Jup . We find a consistent mass of M = 17 ± 6 M Jup for the CT Cha companion from both its luminosity and temperature when placed on evolutionary tracks. Hence, the CT Cha companion is most likely a wide brown dwarf companion or possibly even a planetary mass object.

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“…However, as shown in Mugrauer & Neuhäuser (2005), 2M1207 and its companion (Chauvin et al 2005a) are also exceeding this long-term stability limit at about three times the age of CVSO 30.…”

Section: Aanda-cvso Online Materials P 13mentioning

confidence: 84%

Direct Imaging discovery of a second planet candidate around the possibly transiting planet host CVSO 30

Schmidt

Neuhäuser

Vogt

et al. 2016

A&A

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Context. Direct imaging has developed into a very successful technique for the detection of exoplanets in wide orbits, especially around young stars. Directly imaged planets can be both followed astrometrically on their orbits and observed spectroscopically and thus provide an essential tool for our understanding of the early solar system. Aims. We surveyed the 25 Ori association for direct-imaging companions. This association has an age of only few million years. Among other targets, we observed CVSO 30, which has recently been identified as the first T Tauri star found to host a transiting planet candidate. Methods. We report on photometric and spectroscopic high-contrast observations with the Very Large Telescope, the Keck telescopes, and the Calar Alto observatory. They reveal a directly imaged planet candidate close to the young M3 star CVSO 30. Results. The JHK-band photometry of the newly identified candidate is at better than 1 σ consistent with late-type giants, early-T and early-M dwarfs, and free-floating planets. Other hypotheses such as galaxies can be excluded at more than 3.5 σ. A lucky imaging z ′ photometric detection limit z ′ = 20.5 mag excludes early-M dwarfs and results in less than 10 M Jup for CVSO 30 c if bound. We present spectroscopic observations of the wide companion that imply that the only remaining explanation for the object is that it is the first very young (< 10 Myr) L -T-type planet bound to a star, meaning that it appears bluer than expected as a result of a decreasing cloud opacity at low effective temperatures. Only a planetary spectral model is consistent with the spectroscopy, and we deduce a best-fit mass of 4 -5 Jupiter masses (total range 0.6 -10.2 Jupiter masses). Conclusions. This means that CVSO 30 is the first system in which both a close-in and a wide planet candidate are found to have a common host star. The orbits of the two possible planets could not be more different: they have orbital periods of 10.76 hours and about 27000 years. The two orbits may have formed during a mutual catastrophic event of planet-planet scattering.

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GQLup and its common proper motion companion

Cited by 25 publications

References 30 publications

Alma Measurements of Circumstellar Material in the Gq Lup System

Alma Measurements of Circumstellar Material in the Gq Lup System

Direct evidence of a sub-stellar companion around CT Chamaeleontis

Direct Imaging discovery of a second planet candidate around the possibly transiting planet host CVSO 30

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