J/A+A/578/A122ivo://CDS.VizieR/J/A+A/578/A122doi:10.26093/cds/vizier.35780122CDSMehner A.Davidson K.Humphreys R.M.Walter F.M.Baade D.de Wit W.J.,Martin J.Ishibashi K.Rivinius T.Martayan C.Ruiz M.T.Weis K.2017-06-13T11:08:16Z2015-11-03T14:13:43ZCDS support team

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

cds-question@unistra.frvariable-starsline-intensitiesEvery 5.5-years, {eta} Car's light curve and spectrum change remarkably across all observed wavelength bands. These so-called spectroscopic events are most likely caused by the close approach of a companion. We compare the recent spectroscopic event in mid-2014 to the events in 2003 and 2009 and investigate long-term trends. Eta Car was observed with HST STIS, VLT UVES, and CTIO 1.5m CHIRON for a period of more than two years in 2012-2015. Archival observations with these instruments cover three orbital cycles and the events of 2003.5, 2009.1, and 2014.6. The STIS spectra provide high spatial resolution and include epochs during the 2014 event when observations from most ground-based observatories were not feasible. The strategy for UVES observations allows for a multidimensional analysis, because each location in the reflection nebula is correlated with a different stellar latitude. Important spectroscopic diagnostics during {eta} Car's events show significant changes in 2014 compared to previous events. While the timing of the first HeII {lambda}4686 flash was remarkably similar to previous events, the HeII equivalent widths were slightly larger, and the line flux increased by a factor of ~7 compared to 2003. The second HeII peak occurred at about the same phase as in 2009, but was stronger. The HeI line flux grew by a factor of ~8 in 2009-2014 compared to 1998-2003. The NII emission lines also increased in strength. On the other hand, H{alpha} and FeII lines show the smallest emission strengths ever observed in {eta} Car. The optical continuum brightened by a factor of ~4 in the past 10-15 years. The polar spectrum shows fewer changes in the broad wind emission lines: the FeII emission strength decreased by a factor of ~2 (compared to a factor of ~4 in our direct line of sight). The HeII equivalent widths at FOS4 were larger in 2009 and 2014 than during the 2003 event.2015A&A...578A.122Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/578/A122CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJS/71/983 : UV spectrum of eta Car (Viotti+ 1989)J/A+A/304/415 : uvby-Hbeta photometry of eta Car 1992-94 (van Genderen+, 1995)J/A+A/343/847 : Geneva Photometry of eta Car (van Genderen+ 1999)J/AJ/129/2018 : RXTE scaled fluxes of eta Car (Corcoran+, 2005)J/ApJS/157/138 : UV spectrum of eta Car (Nielsen+, 2005)J/ApJS/163/173 : UV spectrum of eta Car in 2003.5 (Gull+, 2006)J/ApJS/168/289 : NUV spectrum of eta Car in 2003.5 (Nielsen+, 2007)J/ApJS/181/473 : Analysis of the spectrum of eta Car (Nielsen+, 2009)J/A+A/493/1093 : BVRI light curves of eta Car (Fernandez-Lajus+, 2009)J/other/NewA/15.108 : UBVRIH{alpha} of eta Car in 2009 (Fernandez-Lajus+ 2010)J/A+A/540/A133 : eta Car emission spectrum (1700-10400{AA}) (Zethson+, 2012)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/578/A122https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/578/A122http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/578/A122https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/578/A122https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/578/A122http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/578/A122GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/578/A122/table3HeII equivalent width and velocity at FOS4recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPosPosition (Star or FOS4)meta.idcharInstInstrumentmeta.id;instrcharDateObservation datetime.epoch;obsnullableMJDModified Julian date of observationdtime.epochfloatPhasePhasetime.phasefloatmEWOpposit of HeII equivalent width (-EW)0.1nmspect.line.eqWidthfloate_mEWrms uncertainty on EW0.1nmstat.errorfloatVel? Peak velocity (1)km/sspect.dopplerVelocintnullablee_Vel? rms uncertainty on Velkm/sstat.errorintnullableJ/A+A/578/A122/table2HeII equivalent width and velocity in direct view of the starrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintPosPosition (Star or FOS4)meta.idcharInstInstrumentmeta.id;instrcharDateObservation datetime.epoch;obsnullableMJDModified Julian date of observationdtime.epochfloatPhasePhasetime.phasefloatmEWOpposit of HeII equivalent width (-EW)0.1nmspect.line.eqWidthfloate_mEWrms uncertainty on EW0.1nmstat.errorfloatVel? Peak velocity (1)km/sspect.dopplerVelocintnullablee_Vel? rms uncertainty on Velkm/sstat.errorintnullableJ/A+A/578/A122/table1Journal of observationsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintInstInstrumentmeta.id;instrcharPosPosition (Star or FOS4)meta.idcharDateObservation datetime.epoch;obsnullableMJDModified Julian date of observationdtime.epochfloatPhasePhasetime.phasefloatWaveWavelength interval or code for wavelength interval (in {AA}) (1)em.wlcharExpTimeExposure time(s) (in s) (2)time.duration;obs.exposurechar