V1309 Sco Nova Scorpii 2008 Elena Mason, Robert Williams, Marcus Diaz ESO-Chile STCI IAG University...

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  • V1309 ScoNova Scorpii 2008Elena Mason, Robert Williams, Marcus DiazESO-ChileSTCIIAG University of Sao Paulo

  • The FEROS nova surveyJun 2003-Feb 2006 (ESO periods 71-76): 14 CNe; 2-12 epochs per object; La Silla 2.2+FEROS: -range ~400-900nm; R~48000 [Williams et al. 2008, ApJ, 685, 451]

  • The THEA (Transient Heavy Elements Absorption) system

  • The THEA (Transient Heavy Elements Absorption) system s-elements (Fe, Ti, Sc, V, Cr, Y, Sr, Zr) low velocities (~500 km/s) low dispersion velocities (35-300 km/s) disappear ~1 month after the nova outburst are external to the CN expanding ejecta

  • [Williams et al. 2008, ApJ, 685, 451]

  • Discovery of V1309 Sco narrow H emission lines (FWHM~670 & 300 km/s) absorption lines no P-Cyg absorptionSOAR spectrum at Cerro Pochon: red continuum and colors: B=9.2 V=7.8 R=7.3 mag pre-outburst mag ~14.8

  • ESO DDT at UT2+UVESdic1 436+580 & dic2 437+860 3000 10400 Aslit 0.7 & 1.0 R~70000 500005 epochs (Sep 13 to Oct 20)

  • __V1309 Sco __ Nova LMC 2005

  • singly ionized s-elements + FeI, CrI, low velocity (~-50 km/s with respect to systemic) low dispersion velocities (FWHM~30 km/s)

  • V1309 Sco: __ epoch 1 __ epoch 5

  • __ epoch 1, __ epoch 5__ FeII (49) 5477.7 & FeI (15)5497.5

  • FeII (41) 5384.1 (46) 5991.4 (40) 6432.7 & (74) 6456.4

  • Balmer emission lines evolution

  • The Balmer lines: double peaked profile absorption + emission narrow: emission ~140 km/s absorption ~ 70 km/s small relative velocity with respect to systemic (~50 km/s) burst at late epochs

  • Spectroscopic characteristics - summary:Absorption phase spectra (epochs 1-3):

    Enormous amount of abs. lines from FeI, FeII, TiII, VII, ScII, SrII, YII, CrI, CrII, CaI, MnI and MgI strong & narrow H Balmer in emission with complex profiles continuum possibly consistent with a K type starEmission line phase spectra (epochs 4 & 5):

    FeII, FeI, TiII etc. absorption lines now in emissionHe I, OI, NI, [OI]stronger H Balmer lines (by a factor up to a few 100s)fainter but redder continuum + [CaII] emission at 7291 & 7323 A

  • What is it?not a classical CN (spc. evolution & line velocities)not an AGB or post-AGB (outburst amplitude)not a symbiotic (giant at 13kpc toward the GC?)not a born again AGB (spc evolution ) cooler continuum s-element absorption red nova (V838 Mon, V4332 Sgr type) narrow H emission ? planet/stellar merging (Retter & Marom 03, Tylenda & Soker 06) 50000 K Wolf Rayet outburst (Munari et al. 05) CN on a low mass WD (Iben & Tutukov 92)

  • but ?V1309 Sco:H + low & high ionization element emission linesA~7 mag how is it evolving? red novae:Just Balmer emission lines emission which soon turned off A 9-10 mag

  • failed nova

  • HeI profiles (multiplets 48, 4, 11, 46 & 10):

  • [OI](1) & [CaII](1):

  • CaI & NaI evolution

    *R(P0SS)=19 mag ?

    ******F/XYZ=0.047 Ne~10E11 cm3. Ferland in AGN: observed CaII spectrum can be reproduced only assuming high column densities (~1e23 cm2), regardless of density or photoionization parameters***HeI (11) 5876 is a factor 5 stronger (rescaled in the picture) and was visible already at epoch 1**Colored spectra have been scaled by a factor 5 (constant 1 added).

    *