J/MNRAS/495/1943 Planet-hosting stars and debris disc (Yelverton+, 2020)
No significant correlation between radial velocity planet presence and debris
disc properties.
Yelverton B., Kennedy G.M., Su K.Y.L.
<Mon. Not. R. Astron. Soc., 495, 1943-1957 (2020)>
=2020MNRAS.495.1943Y 2020MNRAS.495.1943Y (SIMBAD/NED BibCode)
ADC_Keywords: Exoplanets ; Stars, double and multiple ; Stars, distances ;
Effective temperatures ; Optical ; Infrared
Keywords: planet-disc interactions - circumstellar matter
Abstract:
We investigate whether the tentative correlation between planets and
debris discs which has been previously identified can be confirmed at
high significance. We compile a sample of 201 stars with known planets
and existing far-infrared observations. The sample is larger than
those studied previously since we include targets from an unpublished
Herschel survey of planet hosts. We use spectral energy distribution
modelling to characterize Kuiper belt analogue debris discs within the
sample, then compare the properties of the discs against a control
sample of 294 stars without known planets. Survival analysis suggests
that there is a significant (p∼0.002) difference between the disc
fractional luminosity distributions of the two samples. However, this
is largely a result of the fact that the control sample contains a
higher proportion of close binaries and of later-type stars; both of
these factors are known to reduce disc detection rates. Considering
only Sun-like stars without close binary companions in each sample
greatly reduces the significance of the difference (p∼0.3). We also
find no evidence for a difference in the disc fractional luminosities
of stars hosting planets more or less massive than Saturn (p∼0.9).
Finally, we find that the planet hosts have cooler discs than the
control stars, but this is likely a detection bias, since the warmest
discs in the control sample are also the faintest, and would thus be
undetectable around the more distant planet hosts. Considering only
discs in each sample that could have been detected around a typical
planet host, we find p∼0.07 for the temperatures.
Description:
In this paper we study two samples of stars, distinguished by the
presence or absence of known planets.
Our sample of planet-hosting stars is a subset of the NASA Exoplanet
Archive (NEA; Akeson et al. 2013PASP..125..989A 2013PASP..125..989A), resulting from the
application of the cuts listed in Section 2.1 of the article. There
are 201 stars in the sample, and their properties are summarized in
Table 1. Note that in this table, the stellar effective temperatures
Teff and luminosities are derived from our SED modelling (outlined
in Section 3).
Our control sample is drawn from the DEBRIS sample, which is a
volume-limited sample of nearby AFGKM main-sequence stars whose
selection is detailed in Phillips et al. (2010MNRAS.403.1089P 2010MNRAS.403.1089P, Cat.
J/MNRAS/403/1089). The stars we select are all within ∼25pc. All
systems in the sample have been observed with PACS at 70 and/or
100µm, mostly through the DEBRIS survey (Matthews et al.
2010A&A...518L.135M 2010A&A...518L.135M) and some through the DUNES survey (Eiroa et al.
2010A&A...518L.131E 2010A&A...518L.131E). The control sample results from applying the
cuts listed below, and contains 294 stars, whose properties are
summarized in Table 2.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 52 201 List of stars in our planet host sample
table2.dat 36 294 List of stars in our control sample
table3.dat 95 495 Photometry in the MIPS 70µm, PACS 70µm,
and PACS 100µm bands for all systems studied
in this paper
table4.dat 34 51 List of all systems we find to have a
significant infrared excess
table5.dat 20 444 Upper limits on the fractional luminosities of
discs in systems without a significant infrared
excess
table7.dat 27 152 Systems with a significant proper motion
anomaly
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See also:
J/MNRAS/403/1089 : SUNS and DEBRIS surveys target selection (Phillips+, 2010)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Star name
12- 15 F4.1 pc Dist Distance from the NASA Exoplanet Archive (G1)
17- 20 I4 K Teff Effective temperature from SED modelling (G2)
22- 28 E7.2 Lsun Lum Luminosity from SED modelling (G3)
30- 36 E7.2 AU abin ? Closest relevant binary separation (1)
38- 44 E7.2 Mjup Msini Projected mass from the NASA Exoplanet Archive
46- 52 E7.2 AU apl ? Semimajor axis of the most massive planet in
the system from the NASA Exoplanet Archive
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Note (1): Values from the Washington Double Star Catalog
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Star name
12- 15 F4.1 pc Dist Distance from Phillips et al.
(2010MNRAS.403.1089P 2010MNRAS.403.1089P, Cat. J/MNRAS/403/1089) (G1)
17- 20 I4 K Teff Effective temperature from SED modelling (G2)
22- 28 E7.2 Lsun Lum Luminosity from SED modelling (G3)
30- 36 E7.2 AU abin ? Closest relevant binary separation from
Rodriguez et al. (2015MNRAS.449.3160R 2015MNRAS.449.3160R,
Cat. J/MNRAS/449/3160)
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Star name
12 A1 --- Sample [CP] Sample
(C: control sample ; P: planet host)
14- 20 F7.2 mJy FM70obs ? Observed flux density in the MIPS 70µm
band
22- 27 F6.2 mJy e_FM70obs ? Error on FM70obs
29- 35 F7.2 mJy FM70pre Predicted photospheric flux density in the
MIPS 70µm band
37- 41 F5.2 --- chiM70 ? Significance on the MIPS 70µm band (1)
43- 49 F7.2 mJy FP70obs ? Observed flux density in the PACS 70µm
band
51- 55 F5.2 mJy e_FP70obs ? Error on FP70obs
57- 63 F7.2 mJy FP70pre Predicted photospheric flux density in the
PACS 70µm band
65- 69 F5.2 --- chiP70 ? Significance on the PACS 70µm band (1)
71- 76 F6.2 mJy FP100obs ? Observed flux density in the PACS 100µm
band
78- 82 F5.2 mJy e_FP100obs ? Error on FP100obs
84- 89 F6.2 mJy FP100pre Predicted photospheric flux density in the
PACS 100µm band
91- 95 F5.2 --- chiP100 ? Significance on the PACS 100µm band (1)
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Note (1): We define a criterion for an excess to be considered significant as:
χ=(Fobs-Fpre)/sqrt(eFobs2+eFpre2)
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Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- Name Star name
11 A1 --- Sample [CP] Sample (C: control sample ; P: planet host)
13- 15 I3 K T Best-fitting blackbody temperature derived from
the SED modelling
17- 18 I2 K e_T Error on T
20- 26 E7.2 --- f Best-fitting fractional luminosity of the disc
derived from the SED modelling
28- 34 E7.2 --- e_f Error on f
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Star name
12 A1 --- Sample [CP] Sample (C: control sample ; P: planet host)
14- 20 E7.2 --- flim Upper limit on the fractional luminosity of the
disc
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Byte-by-byte Description of file: table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Star name
12 A1 --- Sample [CP] Sample (C: control sample ; P: planet host)
14- 19 F6.1 m/s Vt Tangential velocity anomaly
21- 25 F5.1 Mjup Manom Minimum companion mass required to explain the
proper motion anomaly (1)
27 A1 --- known [YN] Indicates if the star has a known binary
which could therefore be responsible for the
anomaly
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Note (1): We calculated Manom using equation (15) of Kervella et al.
(2019A&A...623A..72K 2019A&A...623A..72K, Cat. J/A+A/623/A72)
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Global Notes :
Note (G1): The typical uncertainty on Dist is ∼0.1pc
Note (G2): The typical uncertainty on Teff is ∼100K
Note (G3): The typical uncertainty on Lum is ∼5 per cent
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 13-Jun-2023