J/A+A/618/A143ivo://CDS.VizieR/J/A+A/618/A143doi:10.26093/cds/vizier.36180143CDSNicolaes D.Groenewegen M.A.T.Royer P.Lombaert R.Danilovich T.,Decin L.2018-11-05T11:36:59Z2018-10-26T08:51:04ZCDS support team

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

cds-question@unistra.frstellar-mass-lossinfrared-sourcesinfrared-astronomyspectroscopyAt the end of their lives AGB stars are prolific producers of dust and gas. The details of this mass-loss process are still not understood very well. Herschel PACS and SPIRE spectra which cover the wavelength range from ~55 to 670um almost continuously, offer a unique way of investigating properties of AGB stars in general and the mass-loss process in particular as this is the wavelength region where dust emission is prominent and molecules have many emission lines. We present the community with a catalogue of AGB stars and red supergiants (RSGs) with PACS and/or SPIRE spectra reduced according to the current state of the art. The Herschel Interactive Processing Environment (HIPE) software with the latest calibration is used to process the available PACS and SPIRE spectra of 40 evolved stars. The SPIRE spectra of some objects close to the Galactic plane require special treatment because of the weaker fluxes in combination with the strong and complex background emission at those wavelengths. The spectra are convolved with the response curves of the PACS and SPIRE bolometers and compared to the fluxes measured in imaging data of these sources. Custom software is used to identify lines in the spectra, and to determine the central wavelengths and line intensities. Standard molecular line databases are used to associate the observed lines. Because of the limited spectral resolution of the PACS and SPIRE spectrometers (~1500), several known lines are typically potential counterparts to any observed line. To help identifications in follow-up studies the relative contributions in line intensity of the potential counterpart lines are listed for three characteristic temperatures based on local thermodynamic equilibrium (LTE) calculations and assuming optically thin emission. The following data products are released: the reduced spectra, the lines that are measured in the spectra with wavelength, intensity, potential identifications, and the continuum spectra, i.e. the full spectra with all identified lines removed. As simple examples of how this data can be used in future studies we have fitted the continuum spectra with three power laws (two wavelength regimes covering PACS, and one covering SPIRE) and find that the few OH/IR stars seem to have significantly steeper slopes than the other oxygen- and carbon-rich objects in the sample, possibly related to a recent increase in mass-loss rate. As another example we constructed rotational diagrams for CO (and HCN for the carbon stars) and fitted a two-component model to derive rotational temperatures.2018A&A...618A.143Nhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/618/A143CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/618/A143https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/618/A143http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/618/A143https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/618/A143https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/618/A143http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/618/A143GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/618/A143/table2 (Basic properties of the stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/618/A143/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/618/A143/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/618/A143/table2?GETtext/xml+votable180.050000true16.608287512.59802530.0055555555555555566/1986 3640 4365 5273 9939 13677 13813 14457 14600 14674 15401 16132 17716 18364 18998 20022 23471 23611 25228 28807 29528 29817 29877 29963 30087 30244 30260 30306 30313 30605-30606 33233 35641 37352 39905 41849 43890 46318 48301 48650https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/618/A143?format=asciiInfrareddefaultJ/A+A/618/A143/table2Basic properties of the starsSimbadNameSimbad column added by the CDSmeta.idcharONameIdentifier(s)meta.idcharr_vLSRvLRS reference (1)meta.ref;phys.veloc;pos.frameintDistDistancekpcpos.distance;pos.heliocentricfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTypeType (AGB-stars or Red-SG for Red Super Giants)src.classcharIRASIRAS namemeta.id;meta.maincharCType[MSC] Chemical typemeta.notecharVTypeVariability typemeta.notecharr_DistDistance reference (1)meta.ref;pos.frameintvLSRLSR velocitykm/sphys.veloc;pos.lsrfloatdM/dtMass loss ratesolMass/yrphys.mass.lossdoubler_dM/dtdM/dt reference (1)meta.ref;pos.frameintNameSource name, as in lines.dat filemeta.idcharlinesDisplay the integrated line strengthsmeta.ref.urlcharsplistDisplay the list of spectrameta.ref.urlchar_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.mainJ/A+A/618/A143/splistList of all spectrum filesInstInstrument (1)meta.id;instrcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSource name, as in lines.dat filemeta.idcharsp1Show the spectrummeta.ref.urlcharsp2Show the spectrummeta.ref.urlcharsp3Show the spectrummeta.ref.urlcharsp4Show the spectrummeta.ref.urlcharsp5Show the spectrummeta.ref.urlcharFileName1Spectrum file name, in subdirectory spmeta.id;meta.filecharFileName2Spectrum file name, in subdirectory spmeta.id;meta.filecharFileName3Spectrum file name, in subdirectory spmeta.id;meta.filecharFileName4Spectrum file name, in subdirectory spmeta.id;meta.filecharFileName5Spectrum file name, in subdirectory spmeta.id;meta.filecharJ/A+A/618/A143/linesIntegrated line strengths and possible identifications for the selected spectral linesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSource namemeta.idcharprimaryBandSpectral band (1)instr.bandpasscharlambdaObsObserved wavelengthumem.wlfloatnuObsObserved frequencyGHzem.freqdoubleFintIntegrated line fluxW.m**-2phot.flux;spect.linedoublee_Fintrms uncertainty on FintW.m**-2stat.errordoubleRelFWHMRelative FWHM of the line (2)spect.line.width;spect.linefloatSpeciesMolecular speciesmeta.id;phys.molTransTransitionmeta.id;phys.atmol.transitionlambda0? Laboratory wavelengthumem.wlfloatnullablenu0? Laboratory frequencyGHzem.freqdoublenullablel_Con75KLimit flag on Con75Kmeta.code.errorcharCon75K? Contribution of the laboratory line to the observed line for temperature of 75K assuming LTE and optically thin line emission%stat.fit.paramfloatnullablel_Con300KLimit flag on Con300Kmeta.code.errorcharCon300K? Contribution of the laboratory line to the observed line for temperature of 300K assuming LTE and optically thin line emission%stat.fit.paramfloatnullablel_Con500KLimit flag on Con500Kmeta.code.errorcharCon500K? Contribution of the laboratory line to the observed line for temperature of 500K assuming LTE and optically thin line emission%stat.fit.paramfloatnullable