A Direct Imaging Survey of Spitzer-detected Debris Disks: Occurrence of Giant Planets in Dusty Systems<sup>*</sup>

Meshkat, Tiffany; Mawet, Dimitri; Bryan, M.; Hinkley, Sasha; Bowler, Brendan P.; Stapelfeldt, K.; Batygin, Konstantin; Padgett, Deborah; Morales, Farisa Y.; Serabyn, Eugene; Christiaens, Valentin; Brandt, Timothy D.; Wahhaj, Z.

doi:10.3847/1538-3881/aa8e9a

Cited by 109 publications

(85 citation statements)

References 133 publications

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“…Recent determinations of the occurrence rates of massive planets (M > 2M Jup ) beyond 10-20 au are in the range of a few up to 5% (Bowler & Nielsen 2018). More specifically, the 68% confidence interval is estimated to be [1.6 − 5.1]% for 2 − 14M Jup planets between 8 and 400 au by Lannier et al (2016), [4−10]% for 5−20M Jup planets between 10 and 1000 au by Meshkat et al (2017) and [0.75−5.7]% for 0.5 − 75M Jup between 20 and 300 au by Vigan et al (2017). Note, however, that such estimates suffer from very large uncertainties, depending on whether one uses a hot or a cold start model for the planet.…”

Section: Resultsmentioning

confidence: 99%

The newborn planet population emerging from ring-like structures in discs

Lodato

Dipierro

Ragusa

et al. 2019

Monthly Notices of the Royal Astronomical Society

145

126

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ALMA has observed a plethora of ring-like structures in planet forming discs at distances of 10-100 au from their host star. Although several mechanisms have been invoked to explain the origin of such rings, a common explanation is that they trace new-born planets. Under the planetary hypothesis, a natural question is how to reconcile the apparently high frequency of gap-carving planets at 10-100 au with the paucity of Jupiter mass planets observed around main sequence stars at those separations. Here, we provide an analysis of the new-born planet population emerging from observations of gaps in discs, under the assumption that the observed gaps are due to planets. We use a simple estimate of the planet mass based on the gap morphology, and apply it to a sample of gaps recently obtained by us in a survey of Taurus with ALMA. We also include additional data from recent published surveys, thus analysing the largest gap sample to date, for a total of 48 gaps. The properties of the purported planets occupy a distinctively different region of parameter space with respect to the known exo-planet population, currently not accessible through planet finding methods. Thus, no discrepancy in the mass and radius distribution of the two populations can be claimed at this stage. We show that the mass of the inferred planets conforms to the theoretically expected trend for the minimum planet mass needed to carve a dust gap. Finally, we estimate the separation and mass of the putative planets after accounting for migration and accretion, for a range of evolutionary times, finding a good match with the distribution of cold Jupiters.

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Section: Resultsmentioning

confidence: 99%

The newborn planet population emerging from ring-like structures in discs

Lodato

Dipierro

Ragusa

et al. 2019

Monthly Notices of the Royal Astronomical Society

145

126

View full text Add to dashboard Cite

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“…This means that the requirement of measuring a complete planetary orbital phase is fulfilled for direct Jupiter analogs. Beyond this orbital regime, the RV data cover a fraction of the total orbital phase, and the sensitivity of experiments skane@ucr.edu to Uranus/Neptune analogs (Kane 2011) and the occurrence rate of long-period giant planets is more adequately covered by exoplanet surveys using the microlensing (Cassan et al 2012;Mróz et al 2017;Penny et al 2019) and imaging (Meshkat et al 2017;Kopparapu et al 2018;Stone et al 2018) techniques. Longperiod planets also present a compelling advantage due to thw synergy between RV and astrometric observations, wherein such planets impart a significant reciprocal astrometric motion on their host star (Eisner & Kulkarni 2002).…”

Section: Introductionmentioning

confidence: 99%

Detection of Planetary and Stellar Companions to Neighboring Stars via a Combination of Radial Velocity and Direct Imaging Techniques

Kane

Dalba

et al. 2019

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The sensitivities of radial velocity (RV) surveys for exoplanet detection are extending to increasingly long orbital periods, where companions with periods of several years are now being regularly discovered. Companions with orbital periods that exceed the duration of the survey manifest in the data as an incomplete orbit or linear trend, a feature that can either present as the sole detectable companion to the host star, or as an additional signal overlain on the signatures of previously discovered companion(s). A diagnostic that can confirm or constrain scenarios in which the trend is caused by an unseen stellar, rather than planetary, companion is the use of high-contrast imaging observations. Here, we present RV data from the Anglo-Australian Planet Search (AAPS) for twenty stars that show evidence of orbiting companions. Of these, six companions have resolved orbits, with three that lie in the planetary regime. Two of these (HD 92987b and HD 221420b) are new discoveries. Follow-up observations using the Differential Speckle Survey Instrument (DSSI) on the Gemini South telescope revealed that five of the twenty monitored companions are likely stellar in nature. We use the sensitivity of the AAPS and DSSI data to place constraints on the mass of the companions for the remaining systems. Our analysis shows that a planetary-mass companion provides the most likely self-consistent explanation of the data for many of the remaining systems.

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“…In fact, statistical analyses of directly imaged planets find massive gas giants (5-13 M Jup ) to occur only around ∼0.6% of stars at distances of 30-300au (Bowler 2016; see also Meshkat et al 2017 who quote an occurrence rate of ∼0.7% at distances of 10-1000au). Combining radial velocity trends with imaging, Bryan et al (2016) report that the occurrence rate of gas giant companions to RV-detected systems tends to fall off at distances beyond ∼10au.…”

Section: Warm Jupiters and The Lack Of Wide-orbit Gas Giantsmentioning

confidence: 99%

Inner Super-Earths, Outer Gas Giants: How Pebble Isolation and Migration Feedback Keep Jupiters Cold

Fung

Lee

2018

ApJ

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The majority of gas giants (planets of masses 10 2 M ⊕ ) are found to reside at distances beyond ∼1 au from their host stars. Within 1 au, the planetary population is dominated by super-Earths of 2-20M ⊕ . We show that this dichotomy between inner super-Earths and outer gas giants can be naturally explained should they form in nearly inviscid disks. In laminar disks, a planet can more easily repel disk gas away from its orbit. The feedback torque from the pile-up of gas inside the planet's orbit slows down and eventually halts migration. A pressure bump outside the planet's orbit traps pebbles and solids, starving the core. Gas giants are born cold and stay cold: more massive cores are preferentially formed at larger distances, and they barely migrate under disk feedback. We demonstrate this using two-dimensional hydrodynamical simulations of disk-planet interaction lasting up to 10 5 years: we track planet migration and pebble accretion until both come to an end by disk feedback. Whether cores undergo runaway gas accretion to become gas giants or not is determined by computing one-dimensional gas accretion models. Our simulations show that in an inviscid minimum mass solar nebula, gas giants do not form inside ∼0.5au, nor can they migrate there while the disk is present. We also explore the dependence on disk mass and find that gas giants form further out in less massive disks.

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A Direct Imaging Survey of Spitzer-detected Debris Disks: Occurrence of Giant Planets in Dusty Systems^*

Cited by 109 publications

References 133 publications

The newborn planet population emerging from ring-like structures in discs

The newborn planet population emerging from ring-like structures in discs

Detection of Planetary and Stellar Companions to Neighboring Stars via a Combination of Radial Velocity and Direct Imaging Techniques

Inner Super-Earths, Outer Gas Giants: How Pebble Isolation and Migration Feedback Keep Jupiters Cold

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A Direct Imaging Survey of Spitzer-detected Debris Disks: Occurrence of Giant Planets in Dusty Systems*

Cited by 109 publications

References 133 publications

The newborn planet population emerging from ring-like structures in discs

The newborn planet population emerging from ring-like structures in discs

Detection of Planetary and Stellar Companions to Neighboring Stars via a Combination of Radial Velocity and Direct Imaging Techniques

Inner Super-Earths, Outer Gas Giants: How Pebble Isolation and Migration Feedback Keep Jupiters Cold

Contact Info

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A Direct Imaging Survey of Spitzer-detected Debris Disks: Occurrence of Giant Planets in Dusty Systems^*