J/A+A/604/A48ivo://CDS.VizieR/J/A+A/604/A48doi:10.26093/cds/vizier.36040048CDSSkopal A.Shugarov S.Yu.Sekeras M.Wolf M.Tarasova T.N.,Teyssier F.Fujii M.Guarro J.Garde O.Graham K.Lester T.,Bouttard V.Lemoult T.Sollecchia U.Montier J.Boyd D.2017-09-04T07:59:31Z2017-08-01T06:56:03ZCDS support team

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

cds-question@unistra.frcataclysmic-variable-starsinfrared-photometryvisible-astronomybroad-band-photometryspectral-energy-distributionspectroscopyAG Peg is known as the slowest symbiotic nova, which experienced its nova-like outburst around 1850. After 165 years, during June of 2015, it erupted again showing characteristics of the Z And-type outburst. The primary objective is to determine basic characteristics, the nature and type of the 2015 outburst of AG Peg. We achieved this aim by modelling the spectral energy distribution using low-resolution spectroscopy (330-750nm), medium-resolution spectroscopy (420-720nm; R=11000), and UBVR_C_I_C_ photometry covering the 2015 outburst with a high cadence. Optical observations were complemented with the archival HST and FUSE spectra from the preceding quiescence. During the outburst, the luminosity of the hot component was in the range of 2-11x10^37^(d/0.8kpc})^2^erg/s. To generate the maximum luminosity the white dwarf (WD) had to accrete at ~3x10^-7^M_{sun}/yr, which exceeds the stable-burning limit and thus led to blowing optically thick wind from the WD. We determined its mass-loss rate to a few x10^-6^M_{sun}/yr. At the high temperature of the ionising source, 1.5-2.3x10^5^K, the wind converted a fraction of the WD's photospheric radiation into the nebular emission that dominated the optical. A one order of magnitude increase of the emission measure, from a few x10^59^(d/0.8kpc)^2^/cm^3^ during quiescence, to a few x10^60^(d/0.8kpc)^2^/cm^3^ during the outburst, caused a 2mag brightening in the LC, which is classified as the Z And-type of the outburst. The very high nebular emission and the presence of a disk-like HI region encompassing the WD, as indicated by a significant broadening and high flux of the Raman-scattered OVI 6825{AA} line during the outburst, is consistent with the ionisation structure of hot components in symbiotic stars during active phases.2017A&A...604A..48Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/604/A48CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/317/712 : UV fluxes and electron density of AG Peg (Altamore+ 1997)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/604/A48https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/604/A48http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/604/A48https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/604/A48https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/604/A48http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/604/A48GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tap2.367228618189496e-19 6.118840631666147e-19InfraredOpticaldefaultJ/A+A/604/A48/table1Observed UBVRcIc magnitudes of AG PegrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintJDJulian date (JD-2400000) (UT)time.epochdoubleUmag? U magnitude (1)magphot.mag;em.opt.UdoublenullableBmag? B magnitude (1)magphot.mag;em.opt.BdoublenullableVmag? V magnitude (1)magphot.mag;em.opt.VdoublenullableRcmag? Rc magnitude (1)magphot.mag;em.opt.RdoublenullableIcmag? Ic magnitude (1)magphot.mag;em.opt.IdoublenullablePhotType of photometry (2)meta.id;photcharJ/A+A/604/A48/table6Dereddened fluxes for HeII 4686{AA}, H-beta, H-alpha and OVI Raman line 6825{AA}recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintDateDate in the form: YYYY/MM/DD.ddd (UT)time.epochcharJDJulian date (JD-2400000) (UT)time.epochdoubleHeII? HeII 4686{AA} line flux (1)1e-14W.m**-2phot.flux;spect.linefloatnullableHbm? H-beta flux measured (1)1e-14W.m**-2phot.flux;em.line.HbetafloatnullableHbt? H-beta flux corrected for absorption (1)1e-14W.m**-2phot.flux;em.line.HbetafloatnullableHam? H-alpha flux measured (1)1e-14W.m**-2phot.flux;em.line.HalphafloatnullableHat? H-alpha flux corrected for absorption (1)1e-14W.m**-2phot.flux;em.line.HalphafloatnullableRam? Raman scattered OVI 6825{AA} flux (1)1e-14W.m**-2phot.fluxfloatnullable