J/A+A/632/A24ivo://CDS.VizieR/J/A+A/632/A24doi:10.26093/cds/vizier.36320024CDSFuhrmeister B.Czesla S.Hildebrandt L.Nagel E.Schmitt J.H.M.M.,Hintz D.Johnson E.N.Sanz-Forcada J.Schoefer P.Jeffers S.V.,Caballero J.A.Zechmeister M.Reiners A.Ribas I.Amado P.J.,Quirrenbach A.Bauer F.F.Bejar V.J.S.Cortes-Contreras M.,Diez-Alonso E.Dreizler S.Galadi-Enriquez D.Guenther E.W.,Kaminski A.Kuerster M.Lafarga M.Montes D.2021-02-05T08:04:55Z2019-11-25T08:31:33ZCDS support team

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

cds-question@unistra.frm-starsinfrared-astronomyspectroscopyThe HeI infrared (IR) triplet at 10830{AA} is an important activity indicator for the Sun and in solar-type stars, however, it has rarely been studied in relation to M dwarfs to date. In this study, we use the time-averaged spectra of 319 single stars with spectral types ranging from M0.0V to M9.0V obtained with the CARMENES high resolution optical and near-infrared spectrograph at Calar Alto to study the properties of the HeI IR triplet lines. In quiescence, we find the triplet in absorption with a decrease of the measured pseudo equivalent width (pEW) towards later sub-types. For stars later than M5.0V, the HeI triplet becomes undetectable in our study. This dependence on effective temperature may be related to a change in chromospheric conditions along theMdwarf sequence. When an emission in the triplet is observed, we attribute it to flaring. The absence of emission during quiescence is consistent with line formation by photo-ionisation and recombination, while flare emission may be caused by collisions within dense material. The HeI triplet tends to increase in depth according to increasing activity levels, ultimately becoming filled in; however, we do not find a correlation between the pEW(He IR) and X-ray properties. This behaviour may be attributed to the absence of very inactive stars (LX/Lbol<-5.5) in our sample or to the complex behaviour with regard to increasing depth and filling in.2019A&A...632A..24Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/632/A24CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/632/A24https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/632/A24http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/632/A24https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/632/A24https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/632/A24http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/632/A24GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/632/A24/table2 (HeI infrared triplet pseudo equivalent width (pEW) measurements)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/632/A24/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/632/A24/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/632/A24/table2?GETtext/xml+votable180.050000true1.295371745.78656670.0055555555555555566/497 624 725 778 811 1033 1672 1822 1875 1938 2515 2545 2681 2737 2747 2922 3031 3266 3658 3682 3715 3791 4033 4518 5041 5207 5420 5488 5534 6384 6672 6676 6980 7003 7264 7775 7837 7921 7940 7980 8123 8208 8240 8394 8733 8843 8915 9188 9529 9578 9597 10004 10149 10225 10278 10448 10464-10465 10694 10999 11177 11255 11403 11671 12191 12621 12732 13427 14277 14515 14709 14850 14993-14994 15052 15078 15602 15635 15763 15960 17020 17271 17412 17606 17870 18195 18496 18553 18789 18942 19064 19131 19306 19352 20023 20100 20109 20311 20472 20896 21051 21151 21171 21747 21953 21969 22222 22277 22309 22626 22807 23363 23453 23564 23731 23743 23867 24213 24227 24239 24995 25363 25388 25512 25528 25849 25989 26560 26563 26583 27730 27787 27912 28223 28341 28548 28646 28955 29146 29170 29684 30345 30429 30490 30505 30771 30893 31014 31191 31229 32335 32458 32491 36732 40359 40513 44967 48958 49101https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/632/A24?format=asciiInfrareddefaultJ/A+A/632/A24/table2HeI infrared triplet pseudo equivalent width (pEW) measurementsSimbadNameSimbad column added by the CDSmeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintKarmnCARMENES identificationmeta.id;meta.maincharNameCommon name of the starmeta.idcharSpTypeSpectral type of the starsrc.spTypecharTeffEffective temperatureKphys.temperature.effectiveintpEW(HeIR)He IR pseudo equivalent width0.1nmspect.line.eqWidthfloate_pEW(HeIR)Error of pEW(HeIR)0.1nmstat.errorfloatchi2chi^2^ of the Voigt fit to He IR linestat.fit.chi2floatpEW(Halpha)H{alpha} pseudo equivalent width0.1nmspect.line.eqWidthfloatpEW(CaIRT)Bluest component of CaII IRT pseudo equivalent width0.1nmspect.line.eqWidthfloatpEW(HeD3)He D_3_ pseudo equivalent width0.1nmspect.line.eqWidthfloatLX/Lbol? X-ray to bolometric luminosity ratio taken mostly from RASSphys.luminosity;arith.ratiofloatnullable_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.main