J/MNRAS/480/2757 Giant planets in two-belt debris disc systems (Matthews+, 2018)
Constraining the presence of giant planets in two-belt debris disc systems with
VLT/SPHERE direct imaging and dynamical arguments.
Matthews E., Hinkley S., Vigan A., Kennedy G., Sutlieff B., Wickenden D.,
Treves S., David T., Meshkat T., Mawet D., Morales F., Shannon A.,
Stapelfeldt K.
<Mon. Not. R. Astron. Soc., 480, 2757-2783 (2018)>
=2018MNRAS.480.2757M 2018MNRAS.480.2757M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Photometry
Keywords: planet-disc interactions - circumstellar matter - planetary systems
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 HD 95086 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.
Description:
Each of the targets was observed with the SPHERE planet-finding
instrument on the VLT. Data were collected in the dual imaging IRDIFS
mode, which splits the light into two subsystems: a differential
imager and spectrograph (IRDIS), and an integral field spectrometer
(IFS).
We use several methods to distinguish between genuine companions and
background objects: we refer to previous literature, use common proper
motion testing where there are multiple epochs of SPHERE data, and
study the H2-H3 colours for candidates with an absolute magnitude
fainter than 15 in the H2 filter.
The final designation of each candidate is given in Table 4.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 36 20 List of survey stars
table4.dat 69 317 Candidate companion astrometry and magnitudes
for the survey
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Star HD name
11- 12 I2 h RAh Simbad right ascension (J2000)
14- 15 I2 min RAm Simbad right ascension (J2000)
17- 21 F5.2 s RAs Simbad right ascension (J2000)
23 A1 --- DE- Declination sign (J2000)
24- 25 I2 deg DEd Declination (J2000)
27- 28 I2 arcmin DEm Declination (J2000)
30- 33 F4.1 arcsec DEs Declination (J2000)
35- 36 I2 --- N Number of measurements in table4
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Star HD name
11- 20 A10 "date" Date Observation date
22- 23 I2 --- Seq ? Candidate number with the star
25- 28 F4.1 mag DH2 ? Contrast ({DELTA}H2)
30- 35 F6.1 mas Sep ? Separation
37- 40 F4.1 mas e_Sep ? Separation error
42- 47 F6.2 deg PA ? Position angle
49- 52 F4.2 deg e_PA ? Position angle error
54- 65 A12 --- Ref References (1)
67- 69 A3 --- Status Status (2)
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Note (1): References as follows:
B17 = Bonnefoy et al. (2017A&A...597L...7B 2017A&A...597L...7B)
J13 = Janson et al. (2013ApJ...773...73J 2013ApJ...773...73J)
N13 = Nielsen et al. (2013ApJ...776....4N 2013ApJ...776....4N)
dR11 = De Rosa et al. (2011MNRAS.415..854D 2011MNRAS.415..854D)
R13 = Rameau et al. (2013ApJ...779L..26R 2013ApJ...779L..26R)
G16 = Galicher et al. (2016A&A...594A..63G 2016A&A...594A..63G, Cat. J/A+A/594/A63)
Note (2): Status as follows:
BG = background object
?BG = likely background object
C = object with detected companions
S? = likely speckle object
TF = candidate too faint to be redetected
OS = candidate off-screen in this epoch
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 13-May-2022