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

Elisabeth Matthews, Sasha Hinkley, Arthur Vigan, Grant Kennedy, Ben Sutlieff, Dawn Wickenden, Sam Treves, Trevor David, Tiffany Meshkat, Dimitri Mawet, Farisa Morales, Andrew Brian Shannon, Karl Stapelfeldt

Research output: Contribution to journalArticle

1 Citation (Scopus)

Abstract

Giant, wide-separation planets often lie in the gap between multiple, distinct rings of circumstellar debris: this is the case for the HR 8799 and HD95086 systems, and even the Solar system where the Asteroid and Kuiper belts enclose the four gas and ice giants. In the case that a debris disc, inferred from an infrared excess in the SED, is best modelled as two distinct temperatures, we infer the presence of two spatially separated rings of debris. Giant planets may well exist between these two belts of debris, and indeed could be responsible for the formation of the gap between these belts. We observe 24 such two-belt systems using the VLT/SPHERE high-contrast imager, and interpret our results under the assumption that the gap is indeed formed by one or more giant planets. A theoretical minimum mass for each planet can then be calculated, based on the predicted dynamical time-scales to clear debris. The typical dynamical lower limit is ~0.2MJ in this work, and in some cases exceeds 1MJ. Direct imaging data, meanwhile, are typically sensitive to planets down to ~3.6MJ at 1 arcsec, and 1.7MJ in the best case. Together, these two limits tightly constrain the possible planetary systems present around each target, many of which will be detectable with the next generation of high-contrast imagers.

Original languageEnglish (US)
Pages (from-to)2757-2783
Number of pages27
JournalMonthly Notices of the Royal Astronomical Society
Volume480
Issue number2
DOIs
StatePublished - Oct 1 2018

Fingerprint

debris
planets
planet
Kuiper belt
asteroid belts
planetary systems
rings
solar system
asteroid
ice
timescale
gases
gas
temperature

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Matthews, Elisabeth ; Hinkley, Sasha ; Vigan, Arthur ; Kennedy, Grant ; Sutlieff, Ben ; Wickenden, Dawn ; Treves, Sam ; David, Trevor ; Meshkat, Tiffany ; Mawet, Dimitri ; Morales, Farisa ; Shannon, Andrew Brian ; Stapelfeldt, Karl. / Constraining the presence of giant planets in two-belt debris disc systems with VLT/SPHERE direct imaging and dynamical arguments. In: Monthly Notices of the Royal Astronomical Society. 2018 ; Vol. 480, No. 2. pp. 2757-2783.
@article{c2b9f21737be45b6be0a3de0c4156d2f,
title = "Constraining the presence of giant planets in two-belt debris disc systems with VLT/SPHERE direct imaging and dynamical arguments",
abstract = "Giant, wide-separation planets often lie in the gap between multiple, distinct rings of circumstellar debris: this is the case for the HR 8799 and HD95086 systems, and even the Solar system where the Asteroid and Kuiper belts enclose the four gas and ice giants. In the case that a debris disc, inferred from an infrared excess in the SED, is best modelled as two distinct temperatures, we infer the presence of two spatially separated rings of debris. Giant planets may well exist between these two belts of debris, and indeed could be responsible for the formation of the gap between these belts. We observe 24 such two-belt systems using the VLT/SPHERE high-contrast imager, and interpret our results under the assumption that the gap is indeed formed by one or more giant planets. A theoretical minimum mass for each planet can then be calculated, based on the predicted dynamical time-scales to clear debris. The typical dynamical lower limit is ~0.2MJ in this work, and in some cases exceeds 1MJ. Direct imaging data, meanwhile, are typically sensitive to planets down to ~3.6MJ at 1 arcsec, and 1.7MJ in the best case. Together, these two limits tightly constrain the possible planetary systems present around each target, many of which will be detectable with the next generation of high-contrast imagers.",
author = "Elisabeth Matthews and Sasha Hinkley and Arthur Vigan and Grant Kennedy and Ben Sutlieff and Dawn Wickenden and Sam Treves and Trevor David and Tiffany Meshkat and Dimitri Mawet and Farisa Morales and Shannon, {Andrew Brian} and Karl Stapelfeldt",
year = "2018",
month = "10",
day = "1",
doi = "10.1093/MNRAS/STY1778",
language = "English (US)",
volume = "480",
pages = "2757--2783",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "2",

}

Matthews, E, Hinkley, S, Vigan, A, Kennedy, G, Sutlieff, B, Wickenden, D, Treves, S, David, T, Meshkat, T, Mawet, D, Morales, F, Shannon, AB & Stapelfeldt, K 2018, 'Constraining the presence of giant planets in two-belt debris disc systems with VLT/SPHERE direct imaging and dynamical arguments', Monthly Notices of the Royal Astronomical Society, vol. 480, no. 2, pp. 2757-2783. https://doi.org/10.1093/MNRAS/STY1778

Constraining the presence of giant planets in two-belt debris disc systems with VLT/SPHERE direct imaging and dynamical arguments. / Matthews, Elisabeth; Hinkley, Sasha; Vigan, Arthur; Kennedy, Grant; Sutlieff, Ben; Wickenden, Dawn; Treves, Sam; David, Trevor; Meshkat, Tiffany; Mawet, Dimitri; Morales, Farisa; Shannon, Andrew Brian; Stapelfeldt, Karl.

In: Monthly Notices of the Royal Astronomical Society, Vol. 480, No. 2, 01.10.2018, p. 2757-2783.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Constraining the presence of giant planets in two-belt debris disc systems with VLT/SPHERE direct imaging and dynamical arguments

AU - Matthews, Elisabeth

AU - Hinkley, Sasha

AU - Vigan, Arthur

AU - Kennedy, Grant

AU - Sutlieff, Ben

AU - Wickenden, Dawn

AU - Treves, Sam

AU - David, Trevor

AU - Meshkat, Tiffany

AU - Mawet, Dimitri

AU - Morales, Farisa

AU - Shannon, Andrew Brian

AU - Stapelfeldt, Karl

PY - 2018/10/1

Y1 - 2018/10/1

N2 - Giant, wide-separation planets often lie in the gap between multiple, distinct rings of circumstellar debris: this is the case for the HR 8799 and HD95086 systems, and even the Solar system where the Asteroid and Kuiper belts enclose the four gas and ice giants. In the case that a debris disc, inferred from an infrared excess in the SED, is best modelled as two distinct temperatures, we infer the presence of two spatially separated rings of debris. Giant planets may well exist between these two belts of debris, and indeed could be responsible for the formation of the gap between these belts. We observe 24 such two-belt systems using the VLT/SPHERE high-contrast imager, and interpret our results under the assumption that the gap is indeed formed by one or more giant planets. A theoretical minimum mass for each planet can then be calculated, based on the predicted dynamical time-scales to clear debris. The typical dynamical lower limit is ~0.2MJ in this work, and in some cases exceeds 1MJ. Direct imaging data, meanwhile, are typically sensitive to planets down to ~3.6MJ at 1 arcsec, and 1.7MJ in the best case. Together, these two limits tightly constrain the possible planetary systems present around each target, many of which will be detectable with the next generation of high-contrast imagers.

AB - Giant, wide-separation planets often lie in the gap between multiple, distinct rings of circumstellar debris: this is the case for the HR 8799 and HD95086 systems, and even the Solar system where the Asteroid and Kuiper belts enclose the four gas and ice giants. In the case that a debris disc, inferred from an infrared excess in the SED, is best modelled as two distinct temperatures, we infer the presence of two spatially separated rings of debris. Giant planets may well exist between these two belts of debris, and indeed could be responsible for the formation of the gap between these belts. We observe 24 such two-belt systems using the VLT/SPHERE high-contrast imager, and interpret our results under the assumption that the gap is indeed formed by one or more giant planets. A theoretical minimum mass for each planet can then be calculated, based on the predicted dynamical time-scales to clear debris. The typical dynamical lower limit is ~0.2MJ in this work, and in some cases exceeds 1MJ. Direct imaging data, meanwhile, are typically sensitive to planets down to ~3.6MJ at 1 arcsec, and 1.7MJ in the best case. Together, these two limits tightly constrain the possible planetary systems present around each target, many of which will be detectable with the next generation of high-contrast imagers.

UR - http://www.scopus.com/inward/record.url?scp=85055160666&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85055160666&partnerID=8YFLogxK

U2 - 10.1093/MNRAS/STY1778

DO - 10.1093/MNRAS/STY1778

M3 - Article

VL - 480

SP - 2757

EP - 2783

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 2

ER -