J/A+AS/146/103ivo://CDS.VizieR/J/A+AS/146/103CDSMontes D.Fernandez-Figueroa M.J.De Castro E.Cornide M.Latorre A.,Sanz-Forcada J.2000-11-11T20:31:58Z2000-11-11T21:30:57ZCDS support team

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

cds-question@unistra.frspectroscopic-binary-starsspectroscopyThis is the third paper of a series aimed at studying the chromosphere of active binary systems using the information provided for several optical spectroscopic features. High resolution echelle spectra including all the optical chromospheric activity indicators from the CaII H&K to CaII IRT lines are analysed here for 16 systems. The chromospheric contribution in these lines has been determined using the spectral subtraction technique. Very broad wings have been found in the subtracted H{alpha} profile of the very active star HU Vir. These profiles are well matched using a two-component Gaussian fit (narrow and broad) and the broad component can be interpreted as arising from microflaring. Red-shifted absorption features in the H{alpha} line have been detected in several systems and excess emission in the blue wing of FG UMa was also detected. These features indicate that several dynamical processes, or a combination of them, may be involved. Using the E_H{alpha}_/E_H{beta}_ ratio as a diagnostic we have detected prominence-like extended material viewed off the limb in many stars of the sample, and prominences viewed against the disk at some orbital phases in the dwarfs OU Gem and BF Lyn. The He I D_3_ line has been detected as an absorption feature in mainly all the giants of the sample. Total filling-in of the He I D_3_, probably due to microflaring activity, is observed in HU Vir. Self-absorption with red asymmetry is detected in the CaII H&K lines of the giants 12 Cam, FG UMa and BM CVn. All the stars analysed show clear filled-in CaII IRT lines or even notable emission reversal. The small values of the E_8542_/E_8498_ ratio we have found indicate CaII IRT emission arises from plage-like regions. Orbital phase modulation of the chromospheric emission has been detected in some systems, in the case of HU Vir evidence of an active longitude area has been found.2000A&AS..146..103Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+AS/146/103CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toV/76 : Chromospherically Active Binaries (Strassmeier+ 1993)J/A+A/312/221 : Excess CaII H+K emission in active binaries (Montes+, 1996)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+AS/146/103https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+AS/146/103http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+AS/146/103https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+AS/146/103https://vizier.iucaa.in/viz-bin/votable?-source=J/A+AS/146/103http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+AS/146/103GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+AS/146/103/stars (Star positions (from Simbad))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+AS/146/103/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/A+AS/146/103/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+AS/146/103/stars?GETtext/xml+votable180.050000true76.55041759.0213890.0055555555555555566/845 2017 5772 6241 7451 8669 10464 10490 11048 12009 22909 23960 25452 26133 26679 40321https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+AS/146/103?format=asciiOpticaldefaultJ/A+AS/146/103/starsStar positions (from Simbad)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar namemeta.id;meta.maincharprimaryRAJ2000Right ascension (J2000.0)pos.eq.ra;meta.mainDEJ2000Declination (J2000.0)pos.eq.dec;meta.mainJ/A+AS/146/103/table3H{alpha} line measures in the observed and subtracted spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameNamemeta.id;meta.maincharprimaryObsTelescope and observation run (G1)meta.code;obscharphi[0/1[? Orbital phasetime.phasefloatnullableE[HCTP] Type of emission (G2)src.classcharSH? Relative contribution of the hot component to the total continuumstat.paramfloatnullableSC? Relative contribution of the cool component to the total continuumstat.paramfloatnullableHalpha[AEF] Observed H{alpha} profile: A: absorption, E: emission, F: totally filled-in by emissionspect.index;em.line.HalphacharWobs? Full width at half maximum in the observed spectrum0.1nmspect.line.widthfloatnullableRcResidual intensity in the observed spectrum (Rc=Fc/Fcont)phot.count;em.optfloatEWobs? Equivalent width in the observed spectrum0.1nmspect.line.eqWidthfloatnullableWsub? Full width at half maximum in the subtracted spectrum0.1nmspect.line.widthfloatnullableInt? Peak emission intensity in the subtracted spectrumspect.line.intensityfloatnullableEWSubExcess H{alpha} emission equivalent width in the subtracted spectrum (1)0.1nmspect.line.eqWidthfloatlogFS(Ha)Absolute flux at the stellar surfacelog(10mW.m**-2.nm**-1)phot.fluxfloatJ/A+AS/146/103/table5H{beta} line measurements in the observed and subtracted spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameNamemeta.id;meta.maincharprimaryObsTelescope and observation run (G1)meta.code;obscharphi[0/1[? Orbital phasetime.phasefloatnullableE[HCTP] Type of emission (G2)src.classcharWobs? Full width at half maximum in the observed spectrum0.1nmspect.line.widthfloatnullableRcResidual intensity in the observed spectrumphot.count;em.optfloatEWobs? Equivalent width in the observed spectrum0.1nmspect.line.eqWidthfloatnullableWsub? Full width at half maximum in the subtracted spectrum0.1nmspect.line.widthfloatnullableInt? Peak emission intensity in the subtracted spectrumspect.line.intensityfloatnullableEWSubExcess H{alpha} emission equivalent width in the subtracted spectrum (1)0.1nmspect.line.eqWidthfloatEW(Ha)/EW(Hb)? Ratio of excess emission EW in the H{alpha} and H{beta} linesphot.flux;arith.ratiofloatnullableE(Ha)/E(Hb)? Corrected ratio of excess emission (2)phot.flux;arith.ratiofloatnullableJ/A+AS/146/103/table6CaII H&K and H{epsilon} lines measures in the observed and subtracted spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameNamemeta.id;meta.maincharprimaryObsTelescope and observation run (G1)meta.code;obscharphi[0/1[? Orbital phasetime.phasefloatnullableE[CHTPS] Type of emission (G2)src.classcharEW(K)rCaII K equivalent width obtained by reconstruction of the absorption line profile0.1nmspect.line.eqWidthfloatEW(H)rCaII H equivalent width obtained by reconstruction of the absorption line profile0.1nmspect.line.eqWidthfloatEW(He)r? H{epsilon} equivalent width obtained by reconstruction of the absorption line profile0.1nmspect.line.eqWidthfloatnullableEW(K)sCaII K equivalent width using spectral subtraction technique (1)0.1nmspect.line.eqWidthfloatEW(H)sCaII H equivalent width using spectral subtraction technique (1)0.1nmspect.line.eqWidthfloatEW(He)s? H{epsilon} equivalent width using spectral subtraction technique (1)0.1nmspect.line.eqWidthfloatnullablelogF(K)CaII K surface flux (2)log(10mW.m**-2.nm**-1)phot.fluxfloatlogF(H)CaII H surface flux (2)log(10mW.m**-2.nm**-1)phot.fluxfloatlogF(He)? H{epsilon} surface flux (2)log(10mW.m**-2.nm**-1)phot.fluxfloatnullableJ/A+AS/146/103/table7CaII IRT lines measures in the observed and subtracted spectrarecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameNamemeta.id;meta.maincharprimaryObsTelescope and observation run (G1)meta.code;obscharphi[0/1[? Orbital phasetime.phasefloatnullableE[CHTPS] Type of emission (G2)src.classcharEW(8498)r? {lambda}8498 equivalent width obtained by absorption line profile reconstruction0.1nmspect.line.eqWidthfloatnullableEW(8542)r? {lambda}8542 equivalent width obtained by absorption line profile reconstruction0.1nmspect.line.eqWidthfloatnullableEW(8662)r? {lambda}8662 equivalent width obtained by absorption line profile reconstruction0.1nmspect.line.eqWidthfloatnullableEW(8498)s? {lambda}8498 equivalent width using spectral subtraction technique (1)0.1nmspect.line.eqWidthfloatnullableEW(8542)s? {lambda}8542 equivalent width using spectral subtraction technique (1)0.1nmspect.line.eqWidthfloatnullableEW(8662)s? {lambda}8662 equivalent width using spectral subtraction technique (1)0.1nmspect.line.eqWidthfloatnullableEW(8582)/EW(8498)? Ratio of excess emission EW (2)phot.flux;arith.ratiofloatnullablelogF(8498)? {lambda}8498 surface flux (3)log(10mW.m**-2.nm**-1)phot.fluxfloatnullablelogF(8542)? {lambda}8542 surface flux (3)log(10mW.m**-2.nm**-1)phot.fluxfloatnullablelogF(8662)? {lambda}8662 surface flux (3)log(10mW.m**-2.nm**-1)phot.fluxfloatnullable