Planets of<i>β</i> Pictoris revisited

Freistetter, Florian; Krivov, A. V.; Löhne, T.

doi:10.1051/0004-6361:20066746

Cited by 37 publications

(49 citation statements)

References 23 publications

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“…The other two were around the A-type stars Fomalhaut (Kalas et al 2008), which is the first planet candidate discovered in the optical regime using the Hubble Space Telescope (HST), and β Pic (Lagrange et al 2009(Lagrange et al , 2010, a planet within the large edge-on disk at only about twice the separation of Jupiter from the Sun. This had previously been predicted by Freistetter et al (2007), for instance, from the structural gaps in the disk.…”

Section: Introductionsupporting

confidence: 57%

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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Section: Introductionsupporting

confidence: 57%

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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“…The existence of a giant planet orbiting β Pic has been proposed by various studies during the past few decades (e.g. Freistetter et al 2007). The main indirect indicators are (i) the inner warped component of the β Pic circumstellar disk, together with additional asymmetries observed in the outer part (Mouillet et al 1997;Kalas & Jewitt 1995); (ii) the photometric transit-like event observed in 1981 (Lecavelier des Etangs et al 1997); and (iii) the cometary activity observed in the absorption spectrum of β Pic (Ferlet et al 1987;Lagrange et al 1996;VidalMadjar et al 1998;Petterson & Tobin 1999).…”

Section: Discussionmentioning

confidence: 99%

Orbital characterization of theβPictoris b giant planet

Chauvin¹,

Lagrange²,

Beust³

et al. 2012

A&A

156

221

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Context. In June 2010, we confirmed the existence of a giant planet in the disk of the young star β Pictoris located between 8 AU and 15 AU from the star. This young planet offers the rare opportunity to monitor a large fraction of the orbit using the imaging technique over a reasonably short timescale. It also offers the opportunity to study its atmospheric properties using spectroscopy and multi-band photometry, and possibly derive its dynamical mass by combining imaging with radial velocity data to set tight constraints on giant planet formation theories. Aims. We aim to measure the evolution of the planet's position relative to the star β Pictoris to determine the planetary orbital properties. Our ultimate goal is to relate both the planetary orbital configuration and physical properties to either the disk structure or the cometary activity observed for decades in the β Pictoris system. Methods. Using the NAOS-CONICA adaptive-optics instrument (NACO) at the Very Large Telescope (VLT), we obtained repeated follow-up images of the β Pictoris system in the K s and L filters at four new epochs in 2010 and 2011. Complementing these data with previous measurements, we conduct a homogeneous analysis, which covers more than eight yrs, to accurately monitor the β Pictoris b position relative to the star. We then carefully consider the various sources of uncertainties that may affect the orbital parameter determination. Results. On the basis of the evolution of the planet's relative position with time, we derive the best-fit orbital solutions for our measurements using two fitting methods, a least squares Levenberg-Marquardt algorithm and a Markov-chain Monte Carlo approach. More reliable results are found with the second approach as our measurements do not cover the complete planetary orbit, and are biased toward the most recent epochs since the planet recovery. The solutions favor a low-eccentricity orbit e < ∼ 0.17, with semi-major axis in the range 8-9 AU corresponding to orbital periods of 17-21 yrs. Our solutions favor a highly inclined solution with a peak around i = 88.5 ± 1.7 • , and a longitude of ascending node tightly constrained at Ω = −147.5 ± 1.5 • . These results indicate that the orbital plane of the planet is likely to be above the midplane of the main disk, and compatible with the warp component of the disk being tilted between 3.5 deg and 4.0 deg. This suggests that the planet plays a key role in the origin of the inner warped-disk morphology of the β Pic disk. Finally, these orbital parameters are consistent with the hypothesis that the planet is responsible for the transit-like event observed in November 1981, and also linked to the cometary activity observed in the β Pic system.

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“…The star hosts an ∼1000-AU-wide gas-rich debris disk (Smith & Terrile 1984) presented nearly edge-on. Asymmetries in the disk and variability in high-resolution spectra indicative of dynamic comets (Kiefer et al 2014) suggested the presence of one or more planets long before the discovery of β Pic b itself (Lagrange-Henri et al 1988;Beust et al 1990;Roques et al 1993;Levison et al 1994;Mouillet et al 1997;Freistetter et al 2007;Beust & Valiron 2007). Finally, the giant exoplanet β Pic b was imaged (Lagrange et al 2009) and confirmed (Lagrange et al 2010) using adaptive optics (AO) at VLT/NaCo.…”

Section: Introductionmentioning

confidence: 97%

MAGELLAN ADAPTIVE OPTICS FIRST-LIGHT OBSERVATIONS OF THE EXOPLANETβPIC b. II. 3–5μm DIRECT IMAGING WITH MagAO+Clio, AND THE EMPIRICAL BOLOMETRIC LUMINOSITY OF A SELF-LUMINOUS GIANT PLANET

Morzinski

Males

Skemer

et al. 2015

ApJ

124

123

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Young giant exoplanets are a unique laboratory for understanding cool, low-gravity atmospheres. A quintessential example is the massive extrasolar planet β Pic b, which is 9 AU from and embedded in the debris disk of the young nearby A6V star β Pictoris. We observed the system with first light of the Magellan Adaptive Optics (MagAO) system. In Paper I (Males et al. 2014) we presented the first CCD detection of this planet with MagAO+VisAO. Here we present four MagAO+Clio images of β Pic b at 3.1 µm, 3.3 µm, L ′ , and M ′ , including the first observation in the fundamental CH 4 band. To remove systematic errors from the spectral energy distribution (SED), we re-calibrate the literature photometry and combine it with our own data, for a total of 22 independent measurements at 16 passbands from 0.99-4.8 µm. Atmosphere models demonstrate the planet is cloudy but are degenerate in effective temperature and radius. The measured SED now covers >80% of the planet's energy, so we approach the bolometric luminosity empirically. We calculate the luminosity by extending the measured SED with a blackbody and integrating to find log(L bol /L ⊙ ) = −3.78 ± 0.03. From our bolometric luminosity and an age of 23±3 Myr, hot-start evolutionary tracks give a mass of 12.7±0.3 M Jup , radius of 1.45±0.02 R Jup , and T eff of 1708±23 K (model-dependent errors not included). Our empirically-determined luminosity is in agreement with values from atmospheric models (typically −3.8 dex), but brighter than values from the field-dwarf bolometric correction (typically −3.9 dex), illustrating the limitations in comparing young exoplanets to old brown dwarfs.

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Planets ofβ Pictoris revisited

Cited by 37 publications

References 23 publications

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

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

Orbital characterization of theβPictoris b giant planet

MAGELLAN ADAPTIVE OPTICS FIRST-LIGHT OBSERVATIONS OF THE EXOPLANETβPIC b. II. 3–5μm DIRECT IMAGING WITH MagAO+Clio, AND THE EMPIRICAL BOLOMETRIC LUMINOSITY OF A SELF-LUMINOUS GIANT PLANET

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