Constraining the Orbit and Mass of epsilon Eridani b with Radial Velocities, Hipparcos IAD-Gaia DR2 Astrometry, and Multiepoch Vortex Coronagraphy Upper Limits

Llop-Sayson, Jorge; Wang, Jason; Ruffio, Jean-Baptiste; Mawet, Dimitri; Blunt, Sarah; Absil, Olivier; Bond, C.; Brinkman, Casey; Bowler, Brendan P.; Bottom, Michael; Chontos, Ashley; Dalba, Paul A.; Fulton, B. J.; Giacalone, Steven; Hill, Michelle L.; Hirsch, Lea A.; Howard, Andrew W.; Isaacson, Howard; Karlsson, Mikael; Polanski, Alex S.; Madurowicz, Alex; Matthews, K.; Morris, Evan; Perrin, Marshall D.; Ren, Bin; Rice, Malena; Rosenthal, Lee J.; Ruane, Garreth; Rubenzahl, Ryan A.; Sun, He; Wallack, Nicole L.; Xuan, Jerry W.; Ygouf, Marie

doi:10.3847/1538-3881/ac134a

Cited by 29 publications

(22 citation statements)

References 70 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The disc is probably axisymmetric in SMA and Spitzer images (MacGregor et al 2015;Backman et al 2009), although there may be low-significance clumps. A 0.66 +0.12 −0.09 M Jup planet lies much closer in at 3.52 ± 0.04 au, which may be significantly inclined relative to the disc (Llop-Sayson et al 2021). Figure 15 shows this planet could be stirring the disc, and is massive enough to have sculpted it (but not in situ).…”

Section: Appendix A: System Datamentioning

confidence: 98%

Planet populations inferred from debris discs

Pearce

Launhardt

Ostermann

et al. 2022

A&A

View full text Add to dashboard Cite

We know little about the outermost exoplanets in planetary systems because our detection methods are insensitive to moderate-mass planets on wide orbits. However, debris discs can probe the outer-planet population because dynamical modelling of observed discs can reveal properties of perturbing planets. 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 sample 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 these 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 are currently undetectable, but modest detection-limit improvements (e.g. from JWST) should reveal many such perturbers. We find that planets thought to be perturbing debris discs at late times are 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, meaning that the responsible planets are more massive (and located farther inwards) than debris-disc studies assume. We combine self-stirring and size-distribution modelling to show that many debris discs cannot be self-stirred without having unreasonably high masses; planet- or companion-stirring may therefore be the dominant mechanism in many (perhaps all) debris discs. Finally, we provide catalogues of planet predictions and identify promising targets for future planet searches.

show abstract

Section: Appendix A: System Datamentioning

confidence: 98%

Planet populations inferred from debris discs

Pearce

Launhardt

Ostermann

et al. 2022

A&A

View full text Add to dashboard Cite

show abstract

“…The star hosts a prominent debris disk that includes warm emission from a proposed asteroid belt 49,50 . Most noteworthy, the star is orbited by a 0.66 M J planet at 3.5 au 51,52 which has not been imaged previously, but will be easily detectable by our observations in about one night of observations. ϵ Eri also hosts a massive zodiacal cloud 11 that is expected to contain structures from the gravitational interaction with any planet present, likely allowing for the indirect detection of lower-mass planets than we could image directly, and for the better characterization of detected planets through the structures they create in the dust.…”

Section: Targets and Required Observing Timementioning

confidence: 60%

Imaging nearby, habitable-zone planets with the Large Binocular Telescope Interferometer

Wagner¹,

Leisenring²,

Apai³

et al. 2022

Optical and Infrared Interferometry and Imaging VIII

View full text Add to dashboard Cite

One of the main design considerations of the Large Binocular Telescope (LBT) was the goal to resolve the habitable zones (HZs) of the nearest stars at mid-infrared wavelengths around 10 µm. The LBT Interferometer (LBTI) makes use of the telescope's two 8.4 m mirrors on a common mount and their 22.7 m edge-to-edge separation for sensitive, high-angular resolution observations at thermal-infrared wavelengths. In addition to adaptive optics imaging using the two mirrors separately, the instrument enables nulling and Fizeau imaging interferometry exploiting the full resolving power of the LBT. The LBTI team has successfully completed the Hunt for Observable Signatures of Terrestrial planetary Systems (HOSTS), for which we used nulling-interferometry to search for exozodiacal dust, and we are continuing the characterization of the detected systems. Here, we describe a new program to exploit the LBTI's Fizeau imaging interferometric capabilities for a deep imaging search for low-mass, HZ planets around a small sample of particularly suitable, nearby stars. We also review the LBTI's current status relevant to the proposed project to demonstrate the instrument is ready for such a large project.

show abstract

“…2, this region is where radial velocity measurements can provide detection limits of multi-Jupiter or better in Hurt et al (2021). Future works following Mawet et al (2019) and Llop-Sayson et al (2021) in combining measurements including direct imaging here and radial velocity in Hurt et al (2021), as well as upcoming imaging observations with JWST GTO-1193, in ad-dition to the VFN and PLN concepts to detect planets towards ∼0 . 1, can enable us to obtain the most holistic understanding for the planetary system of this historical photometric standard star -Vega.…”

Section: Discussionmentioning

confidence: 93%

Planet Search with the Keck/NIRC2 Vortex Coronagraph in Ms-band for Vega

Ren¹,

Wallack²,

Hurt³

et al. 2023

Preprint

View full text Add to dashboard Cite

Context. Gaps in circumstellar disks can signal the existence of planetary perturbers, making such systems preferred targets for direct imaging observations of exoplanets. Aims. Being one of the brightest and closest stars to the Sun, the photometric standard star Vega hosts a two-belt debris disk structure. Together with the fact that its planetary system is being viewed nearly face-on, Vega has been one of the prime targets for planet imaging efforts. Methods. Using the vector vortex coronagraph on Keck/NIRC2 in M s -band at 4.67 µm, we report the planet detection limits from 1 au to 22 au for Vega with an on-target time of 1.8 h. Results. We reach a 3 M Jupiter limit exterior to 12 au, which is nearly an order of magnitude deeper than existing studies. Combining with existing radial velocity studies, we can confidently rule out the existence of companions more than ∼8 M Jupiter from 22 au down to 0.1 au for Vega. Interior and exterior to ∼4 au, this combined approach reaches planet detection limits down to ∼2-3 M Jupiter using radial velocity and direct imaging, respectively. Conclusions. By reaching multi-Jupiter mass detection limits, our results are expected to be complemented by the planet imaging of Vega in the upcoming observations using the James Webb Space Telescope to obtain a more holistic understanding of the planetary system configuration around Vega.

show abstract

Constraining the Orbit and Mass of epsilon Eridani b with Radial Velocities, Hipparcos IAD-Gaia DR2 Astrometry, and Multiepoch Vortex Coronagraphy Upper Limits

Cited by 29 publications

References 70 publications

Planet populations inferred from debris discs

Planet populations inferred from debris discs

Imaging nearby, habitable-zone planets with the Large Binocular Telescope Interferometer

Planet Search with the Keck/NIRC2 Vortex Coronagraph in Ms-band for Vega

Contact Info

Product

Resources

About