J/A+A/694/A123ivo://CDS.VizieR/J/A+A/694/A123doi:10.26093/cds/vizier.36940123CDSLestrade 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.2025-05-21T20:01:20Z2025-02-06T09:50:25ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frm-starsexoplanetsinfrared-photometryThe 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.2025A&A...694A.123Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/694/A123CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/694/A123https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/694/A123http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/694/A123https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/694/A123https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/694/A123http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/694/A123GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/694/A123/table1 (Herschel photometry of the 94 M-dwarfs of the DEBRIS survey)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/694/A123/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/694/A123/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/694/A123/table1?GETtext/xml+votable180.050000true164.12050367.01472310.0055555555555555566/22 527 546 2737 4158 4444 4693 4867 5000 5420 5534 5590 6552 6672 6726 7103 8023 9471 9629 9696 10027 10149 11636 12679 13688 14515 14993 15311 15346 16041 16391 16502 16758 16827 17348 18440 18450 18496 18761 19466 20071 20100 20459 20896 22014 22289 22309 22325 22645 23910 26279 26327 26538 26560 26583 26699 26972 27201 27392 27459 27462 27731 27762 28343 32229 32335 33425 33964 34181 34448 34479 36526 36614 39499 40505 42054 42652 43580 43723 44226 44921 44937 46566 46632 46718 47061 47347 48906 48985https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/694/A123?format=asciiInfrareddefaultJ/A+A/694/A123/table1Herschel photometry of the 94 M-dwarfs of the DEBRIS surveySpTypeStellar spectral typesrc.spTypecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGJNameGJ namemeta.idcharHNameHIP or HD namemeta.idcharTeffEffective stellar temperatureKphys.temperature.effectiveintDistStar distancepcpos.distancefloatF100PACS flux density at 100 micronsmJyphot.flux.density;em.IR.60-100umfloate_F100Uncertainty of PACS flux density at 100 micronsmJystat.errorfloatP100Photosphere flux density at 100 micronsmJyphot.flux.density;em.IR.60-100umfloate_P100Uncertainty of photosphere flux at 100 micronsmJystat.errorfloatchi100Significance of excess above photosphere level at 100 micronsstat.fit.goodnessfloatF160PACS flux density at 160 micronsmJyphot.flux.density;em.mm.1500-3000GHzfloate_F160Uncertainty of PACS flux density at 160 micronsmJystat.errorfloatP160Photosphere flux density at 160 micronsmJyphot.flux.density;em.mm.1500-3000GHzfloate_P160Uncertainty of photosphere flux at 160 micronsmJystat.errorfloatchi160Significance of excess above photosphere level at 160 micronsstat.fit.goodnessfloatl_SPIREUpper limit flag on SPIREmeta.code.errorcharSPIRE? Upper limit on flux densities at SPIRE lambdasmJyphot.flux.density;em.IRintnullable_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainNameDEBRIS name, MNNNAAmeta.id;meta.maincharSimbadNameSimbad column added by the CDSmeta.idcharnullable