Mutual inclinations between giant planets and their debris discs in HD 113337 and HD 38529

Xuan, Jerry W.; Kennedy, Grant M.; Wyatt, M. C.; Yelverton, Ben

doi:10.1093/mnras/staa3155

Cited by 12 publications

(10 citation statements)

References 75 publications

(125 reference statements)

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“…• HD 38529 (HIP 27253) is a G star hosting two companions with masses of 18±3 and 0.17 M Jup (Fischer et al 2003;Wittenmyer et al 2009;Barbato et al 2018;Benedict et al 2010;Xuan et al 2020). Our combined analyses estimate a mass of 10.38 +1.03 −0.88 M Jup and an inclination of 104.56 +6.39 −8.72 deg for HD 38529 c, consistent with the the solution given by Xuan et al ( 2020) but with higher precision.…”

Section: Companionsupporting

confidence: 86%

“…A good approach is to combine the RV and the astrometric difference between Hipparcos (Perryman et al 1997;van Leeuwen 2007) and Gaia (Gaia Collaboration et al 2016, 2018 for nearby stars. Various groups have used this approach to estimate the dynamical mass of directly imaged brown dwarfs (Snellen & Brown 2018;Brandt et al 2019;Kervella et al 2019;Xuan et al 2020;Kiefer et al 2021;Kervella et al 2022).…”

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confidence: 99%

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3D Selection of 167 Substellar Companions to Nearby Stars

Feng

Butler

Vogt

et al. 2022

ApJS

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We analyze 5108 AFGKM stars with at least five high-precision radial velocity points, as well as Gaia and Hipparcos astrometric data, utilizing a novel pipeline developed in previous work. We find 914 radial velocity signals with periods longer than 1000 days. Around these signals, 167 cold giants and 68 other types of companions are identified, through combined analyses of radial velocity, astrometry, and imaging data. Without correcting for detection bias, we estimate the minimum occurrence rate of the wide-orbit brown dwarfs to be 1.3%, and find a significant brown-dwarf valley around 40 M Jup. We also find a power-law distribution in the host binary fraction beyond 3 au, similar to that found for single stars, indicating no preference of multiplicity for brown dwarfs. Our work also reveals nine substellar systems (GJ 234 B, GJ 494 B, HD 13724 b, HD 182488 b, HD 39060 b and c, HD 4113 C, HD 42581 d, HD 7449 B, and HD 984 b) that have previously been directly imaged, and many others that are observable at existing facilities. Depending on their ages, we estimate that an additional 10–57 substellar objects within our sample can be detected with current imaging facilities, extending the imaged cold (or old) giants by an order of magnitude.

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Section: Companionsupporting

confidence: 86%

mentioning

confidence: 99%

3D Selection of 167 Substellar Companions to Nearby Stars

Feng

Butler

Vogt

et al. 2022

ApJS

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“…15 shows this planet could be stirring the disc, and is massive enough to have sculpted it (but not in situ). There is a probable misalignment between the planet(s) and the disc (Xuan et al 2020), and an M-star companion is also present at 4000 au (Reid et al 2007); the misalignment could be driven by the planet(s) and stellar companion (Xuan et al 2020). B.32.…”

Section: B31 Hd 113337mentioning

confidence: 99%

Planet populations inferred from debris discs: insights from 178 debris systems in the ISPY, LEECH and LIStEN planet-hunting surveys

Pearce,

Launhardt,

Ostermann

et al. 2022

Preprint

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We know little about the prevalence and properties of the outermost exoplanets in planetary systems, because current detection methods are insensitive to moderate-mass planets on wide orbits. However, debris discs provide indirect probes of the outer-planet population, because dynamical modelling of observed discs can reveal properties of undetected perturbing planets. In this paper we use four sculpting and stirring arguments to infer planet properties in 178 debris-disc systems from the ISPY, LEECH and LIStEN planet-hunting surveys. Similar analyses are often conducted for individual discs, but we consider a large number of systems in a consistent manner. We aim to predict the population of wide-separation planets, gain insight into the formation and evolution histories of planetary systems, and determine the feasibility of detecting perturbing planets in the near future. We show that a 'typical' cold debris disc likely requires a Neptune-to Saturn-mass planet at 10 − 100 au, with some needing Jupiter-mass perturbers. Our predicted planets lie below current detection limits, but modest detection-limit improvements (expected from JWST) should finally reveal many such perturbers. We find that planets thought to be perturbing debris discs at late times are very similar to those inferred to be forming in protoplanetary discs, so these could be the same population if newly formed planets do not migrate as far as currently thought. Alternatively, young planets could rapidly sculpt debris before migrating inwards, in which case the responsible planets are much more massive (and located much further inwards) than debris-disc studies assume. We also combine self-stirring and size-distribution modelling, showing that many debris discs cannot be self-stirred without having unreasonably high masses; planetor companion-stirring may therefore be the dominant stirring mechanism in many (potentially all) debris discs instead. Finally, we provide catalogues of planet predictions for our 178 systems, and identify promising targets for future planet searches.

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“…Brandt et al 2019;Brandt et al 2021), and observe an overabundance of alignments between planet and wide binary orbits for binaries with semi-major axis < 700 AU (Christian et al 2022). Orbital obliquity alignment studies such as Bryan et al 2020 andXuan et al 2020 are important probes of the angular momentum evolution of planetary systems and the influence of scattering and/or Kozai-Lidov mechanisms (Mustill et al 2021), especially in the presence of a wide stellar companion (Hjorth et al 2021). Future Gaia data releases will contain improved astrometry and acceleration information for hundreds of millions of sources 1 , making new companion identification through astrometry common place, and promising to deliver numerous planets and brown dwarf companions in wide binaries Multiple star systems should be prioritized as prime direct imaging targets for probing planetary system formation and evolution, population statistics, and planet characterization studies.…”

Section: Motivation: Substellar Companions In Wide Binariesmentioning

confidence: 99%

Companion mass limits for 17 binary systems obtained with binary differential imaging and MagAO/Clio

Pearce

Males

Weinberger

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Improving direct detection capability close to the star through improved star-subtraction and post-processing techniques is vital for discovering new low-mass companions and characterizing known ones at longer wavelengths. We present results of 17 binary star systems observed with the Magellan Adaptive Optics system (MagAO) and the Clio infrared camera on the Magellan Clay Telescope using Binary Differential Imaging (BDI). BDI is an application of Reference Differential Imaging (RDI) and Angular Differential Imaging (ADI) applied to wide binary star systems (2″ <Δρ < 10″) within the isoplanatic patch in the infrared. Each star serves as the point-spread-function (PSF) reference for the other, and we performed PSF estimation and subtraction using Principal Component Analysis. We report contrast and mass limits for the 35 stars in our initial survey using BDI with MagAO/Clio in L′ and 3.95μm bands. Our achieved contrasts varied between systems, and spanned a range of contrasts from 3.0-7.5 magnitudes and a range of separations from 0.2″to ∼2″. Stars in our survey span a range of masses, and our achieved contrasts correspond to late-type M dwarf masses down to ∼10 MJup. We also report detection of a candidate companion signal at 0.2″(18 AU) around HIP 67506 A (SpT G5V, mass ∼1.2 M⊙), which we estimate to be $\sim 60-90~\mbox{M$_{\rm Jup}$}$. We found that the effectiveness of BDI is highest for approximately equal brightness binaries in high-Strehl conditions.

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Mutual inclinations between giant planets and their debris discs in HD 113337 and HD 38529

Cited by 12 publications

References 75 publications

3D Selection of 167 Substellar Companions to Nearby Stars

3D Selection of 167 Substellar Companions to Nearby Stars

Planet populations inferred from debris discs: insights from 178 debris systems in the ISPY, LEECH and LIStEN planet-hunting surveys

Companion mass limits for 17 binary systems obtained with binary differential imaging and MagAO/Clio

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