Constraining the presence of giant planets in two-belt debris disc systems with VLT/SPHERE direct imaging and dynamical arguments

Matthews, Elisabeth C.; Hinkley, Sasha; Vigan, A.; Kennedy, Grant M.; Sutlieff, Ben J.; Wickenden, Dawn; Treves, Sam; Meshkat, Tiffany; Mawet, Dimitri; Morales, Farisa Y.; Shannon, Andrew; Stapelfeldt, K.

doi:10.1093/mnras/sty1778

Cited by 17 publications

(19 citation statements)

References 82 publications

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“…Both companion candidates around HIP 117452 were earlier identified by De Rosa et al (2011) in the course of the Volume-limited A-Star (VAST) survey as a candidate binary companion. They were later confirmed by Matthews et al (2018) as physically bound, confirming that this system was actually a quadruple system with an A0 primary (HIP 117452 A), orbited by a close binary pair Ba and Bb also resolved in this survey, and additionally by a K-type star at about 75 . Follow-up observations of the candidates were automatically scheduled and obtained using the DBI mode with J 2 J 3 filters of IRDIS, which is well adapted to distinguish background stars from physically young, early-T, or warm mid-L dwarf planets, and offers an additional epoch for a proper motion test.…”

Section: Companion Candidate Detection and Characterizationsupporting

confidence: 57%

“…We assumed that planets are a valid explanation for the formation of debris structure, as shown in the case of the Solar System where planets are known to reside between two belts of debris, and in the case of HR 8799 and HD 95086 where planets are known to reside in two-temperature debris disks. The analysis of our survey follows the work by Matthews et al (2018). The temperature values of debris belts are found in Chen et al (2014), where these temperatures were estimated using a two-temperature black-body model and a Bayesian parameter estimation to select the best model to fit the SED.…”

Section: Discussionmentioning

confidence: 99%

“…The status of the candidate around HIP 8832 still requires further follow-up. HIP 117452 BaBb is resolved and confirmed as a binary companion (De Rosa et al 2011;Matthews et al 2018). For 12 targets of our survey, where we determined the radii of the debris belt, we derived upper and lower mass limits.…”

Section: Discussionmentioning

confidence: 99%

“…For HIP 117452 Ba and Bb, the colors and magnitudes in K 1 and K 2 compared to the predictions of the evolutionary models of Siess et al (2000) suggest that Ba and Bb are a pair of M1 and M2 low-mass stars, considering an age of 40 Myr at a distance of 42 pc. Combining our relative astrometry with the one reported by Matthews et al (2018) and shown in Table 3, we performed a first orbit fitting of the pair. Following the method developed by Chauvin et al (2012), we used a Markov chain Monte Carlo (MCMC) Bayesian analysis technique (Ford & Gregory 2007), which is well suited for observations covering a small part of the whole orbit (for large orbital periods).…”

Section: Companion Candidate Detection and Characterizationmentioning

confidence: 99%

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VLT/SPHERE survey for exoplanets around young early-type stars, including systems with multi-belt architectures

Lombart

Chauvin

Rojo

et al. 2020

A&A

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Context. Dusty debris disks around pre- and main-sequence stars are potential signposts for the existence of planetesimals and exoplanets. Giant planet formation is therefore expected to play a key role in the evolution of the disk. This is indirectly confirmed by extant submillimeter near-infrared images of young protoplanetary and cool dusty debris disks around main-sequence stars that usually show substantial spatial structures. With two decades of direct imaging of exoplanets already studied, it is striking to note that a majority of recent discoveries of imaged giant planets have been obtained around young early-type stars hosting a circumstellar disk. Aims. Our aim was to create a direct imaging program designed to maximize our chances of giant planet discovery and target 22 young early-type stars. About half of them show indications of multi-belt architectures. Methods. Using the IRDIS dual-band imager and the IFS integral field spectrograph of SPHERE to acquire high-constrast coronagraphic differential near-infrared images, we conducted a systematic search in the close environment of these young, dusty, and early-type stars. We used a combination of angular and spectral differential imaging to reach the best detection performances down to the planetary mass regime. Results. We confirm that companions detected around HIP 34276, HIP 101800, and HIP 117452 are stationary background sources and binary companions. The companion candidates around HIP 8832, HIP 16095, and HIP 95619 are determined as background contaminations. Regarding the stars for which we infer the presence of debris belts, a theoretical minimum mass for planets required to clear the debris gaps can be calculated. The dynamical mass limit is at least 0.1 MJ and can exceed 1 MJ. Direct imaging data is typically sensitive to planets down to ~3.6 MJ at 1′′, and 1.7 MJ in the best case. These two limits tightly constrain the possible planetary systems present around each target. These systems will be probably detectable with the next generation of planet imagers.

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Section: Companion Candidate Detection and Characterizationsupporting

confidence: 57%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Companion Candidate Detection and Characterizationmentioning

confidence: 99%

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VLT/SPHERE survey for exoplanets around young early-type stars, including systems with multi-belt architectures

Lombart

Chauvin

Rojo

et al. 2020

A&A

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“…Our Solar System is a good example, with the Kuiper belt's inner edge shaped by Neptune, and the gap between the asteroid and Kuiper belt filled with planets. Backman et al 2009;Morales et al 2009;Chen et al 2009;Ballering et al 2014;Kennedy & Wyatt 2014), which have been used as an argument for the presence of planets in between these two components (Shannon et al 2016;Lazzoni et al 2018;Matthews et al 2018). Additionally, a few debris discs show evidence of single or multiple gaps in between broad outer belts which suggests the presence of planets formed within these icy planetesimals belts.…”

Section: Introductionmentioning

confidence: 99%

A gap in HD 92945’s broad planetesimal disc revealed by ALMA

Marino

Yelverton

Booth

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In the last few years multiwavelength observations have revealed the ubiquity of gaps/rings in circumstellar discs. Here we report the first ALMA observations of HD 92945 at 0.86 mm, that reveal a gap at about 73 ± 3 au within a broad disc of planetesimals that extends from 50 to 140 au. We find that the gap is 20 +10 −8 au wide. If cleared by a planet in situ, this planet must be less massive than 0.6 M Jup , or even lower if the gap was cleared by a planet that formed early in the protoplanetary disc and prevented planetesimal formation at that radius. By comparing opposite sides of the disc we also find that the disc could be asymmetric. Motivated by the asymmetry and the fact that planets might be more frequent closer to the star in exoplanetary systems, we show that the gap and asymmetry could be produced by two planets interior to the disc through secular resonances. These planets excite the eccentricity of bodies at specific disc locations, opening radial gaps in the planetesimal distribution. New observations are necessary to confirm if the disc is truly asymmetric, thus favouring the secular resonance model, or if the apparent asymmetry is due to a background galaxy, favouring the in-situ planet scenario. Finally, we also report the non-detection of CO and HCN gas confirming that no primordial gas is present. The CO and HCN non-detections are consistent with the destruction of volatile-rich Solar System-like comets.

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HARPS radial velocity search for planets in the Scorpius-Centaurus association

Grandjean¹,

Lagrange²,

Meunier³

et al. 2022

A&A

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Context. The Scorpius-Centaurus (Sco-Cen) young and nearby massive star-forming region is particularly well suited for extrasolar planet searches with both direct imaging and radial velocity (RV) techniques. The RV search, however, is challenging, as the stars are faster rotators on average than their older stellar counterparts of similar spectral types. Moreover, the RV time series show strong signatures of stellar variability (spots and faculae) and/or stellar pulsations. Aims. Our aim is to search for giant planets (GPs) and brown dwarfs at short orbital distances around star members of the Sco-Cen association. We also aim at using these data together with others available on young stars to estimate the GP occurrence rate for young stars for periods of up to 1000 days. Methods. We used the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph on the 3.6 m telescope at the La Silla Observatory to monitor 88 A − F Sco-Cen stars. To improve our statistics and analysis, we combined this survey with two previous surveys that focused on young nearby stars (YNS) to compute companion occurrence rates from a sample of 176 young A − M stars. Results. We report the discovery of a massive hot-Jupiter candidate around HD 145467, together with the discovery of one probable short-period (P < 10 days) brown dwarf around HD 149790. In addition, we confirm the binary nature of eight single-line binaries:

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Constraining the presence of giant planets in two-belt debris disc systems with VLT/SPHERE direct imaging and dynamical arguments

Cited by 17 publications

References 82 publications

VLT/SPHERE survey for exoplanets around young early-type stars, including systems with multi-belt architectures

VLT/SPHERE survey for exoplanets around young early-type stars, including systems with multi-belt architectures

A gap in HD 92945’s broad planetesimal disc revealed by ALMA

HARPS radial velocity search for planets in the Scorpius-Centaurus association

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