J/A+A/694/A123 Herschel DEBRIS survey of M-dwarfs (Lestrade+, 2025)
Debris disks around M-dwarfs : the HERSCHEL DEBRIS survey.
Lestrade J.-F., Matthews B.C., Kennedy G.M., Sibthorpe B., Wyatt M.C.,
Booth M., Greaves J.S., Duchene G., Moro-Martin A., Jobic C.
<Astron. Astrophys. 694, A123 (2025)>
=2025A&A...694A.123L 2025A&A...694A.123L (SIMBAD/NED BibCode)
ADC_Keywords: Stars, M-type ; Exoplanets ; Photometry, infrared
Keywords: circumstellar matter - stars: low-mass - planetary systems
Abstract:
The Herschel open-time key program Disc Emission via a Bias-free
Reconnaissance in the Infrared and Sub-millimeter (DEBRIS) is an
unbiased survey of the nearest 100 stars for each stellar type A-M
observed with a uniform photometric sensitivity to search for cold
debris disks around them. The analysis of the Photoconductor Array
Camera and Spectrometer (PACS) photometric observations of the 94
DEBRIS M dwarfs of this program is presented in this paper, following
upon two companion papers on the DEBRIS A-star and FGK-star
subsamples.
In the M-dwarf subsample, two debris disks have been detected, around
the M3V dwarf GJ 581 and the M4V dwarf Fomalhaut C (LP 876-10). This
result gives a disk detection rate of 2.1+2.7-0.7% at the 68%
confidence level, significantly less than measured for earlier stellar
types in the DEBRIS program. However, we show that the survey of the
DEBRIS M-dwarf subsample is about ten times shallower than the surveys
of the DEBRIS FGK subsamples when studied in the physical parameter
space of the disk's fractional dust luminosity versus blackbody
radius. Furthermore, had the DEBRIS K-star subsample been observed at
the same shallower depth in this parameter space, its measured disk
detection rate would have been statistically consistent with the one
found for the M-dwarf subsample. Hence, the incidence of debris disks
does not appear to drop from the K subsample to the M subsample of the
DEBRIS program, when considering disks in the same region of physical
parameter space. An alternative explanation is that the only two
bright disks discovered in the M-dwarf subsample would not, in fact,
be statistically representative of the whole population.
Description:
Herschel photometry of the DEBRIS subsample of the nearest 94
M-dwarfs. For each star, DEBRIS name, other name, spectral stellar
type, effective temperature, distance, PACS flux density at 100
microns, 1-sigma uncertainty at 100 microns, photosphere flux density
at 100 microns, 1-sigma uncertainty at 100 microns, significance of
excess above photosphere level at 100 microns, PACS flux density at
160 microns, 1-sigma uncertainty at 160 microns, photosphere flux
density at 160 microns, 1-sigma uncertainty at 160 microns,
Significance of excess above photosphere level at 160 microns, SPIRE
flux density upper limit are given.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 148 94 Herschel photometry of the 94 M-dwarfs of the
DEBRIS survey
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 6 A6 ---- Name DEBRIS name, MNNNAA
13- 21 A9 ---- GJName GJ name
27- 35 A9 ---- HName HIP or HD name
42- 45 A4 ---- SpType Stellar spectral type
52- 55 I4 K Teff Effective stellar temperature
62- 65 F4.2 pc Dist Star distance
70- 74 F5.1 mJy F100 PACS flux density at 100 microns
77- 79 F3.1 mJy e_F100 Uncertainty of PACS flux density at 100 microns
84- 88 F5.2 mJy P100 Photosphere flux density at 100 microns
91- 94 F4.2 mJy e_P100 Uncertainty of photosphere flux at 100 microns
99-103 F5.2 ---- chi100 Significance of excess above photosphere level
at 100 microns
108-112 F5.1 mJy F160 PACS flux density at 160 microns
115-117 F3.1 mJy e_F160 Uncertainty of PACS flux density at 160 microns
122-126 F5.2 mJy P160 Photosphere flux density at 160 microns
129-132 F4.2 mJy e_P160 Uncertainty of photosphere flux at 160 microns
137-141 F5.2 ---- chi160 Significance of excess above photosphere level
at 160 microns
146 A1 --- l_SPIRE Upper limit flag on SPIRE
147-148 I2 mJy SPIRE ? Upper limit on flux densities at SPIRE lambdas
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Acknowledgements:
Jean-Francois Lestrade, jean-francois.lestrade(at)obspm.fr
(End) Patricia Vannier [CDS] 14-Jan-2025