V1309 Sco Nova Scorpii 2008

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

description

V1309 Sco Nova Scorpii 2008. Elena Mason, Robert Williams, Marcus Diaz ESO-Chile STCI IAG University of Sao Paulo. The FEROS nova survey. Jun 2003-Feb 2006 (ESO periods 71-76): 14 CNe; 2-12 epochs per object; La Silla 2.2+FEROS: λ -range ~400-900nm; R~48000. - PowerPoint PPT Presentation

Transcript of V1309 Sco Nova Scorpii 2008

Page 1: V1309 Sco Nova Scorpii 2008

V1309 ScoNova Scorpii 2008

Elena Mason, Robert Williams, Marcus Diaz

ESO-ChileSTCI

IAG University of Sao Paulo

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The FEROS nova survey

Jun 2003-Feb 2006 (ESO periods 71-76): 14 CNe; 2-12 epochs per object;

La Silla 2.2+FEROS: λ-range ~400-900nm; R~48000

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

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The THEA (Transient Heavy Elements Absorption) system

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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

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

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Discovery of V1309 Sco

• narrow H emission lines (FWHM~670 & 300 km/s)

• absorption lines• no P-Cyg absorption

SOAR spectrum at Cerro Pochon:• red continuum and colors: B=9.2 V=7.8

R=7.3 mag• pre-outburst mag ~14.8

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ESO DDT at UT2+UVESdic1 436+580 & dic2 437+860 3000 – 10400 A

slit 0.7” & 1.0” R~70000 – 500005 epochs (Sep 13 to Oct 20)

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__V1309 Sco __ Nova LMC 2005

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

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V1309 Sco: __ epoch 1 __ epoch 5

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

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

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Balmer emission lines evolution

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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

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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 star

Emission line phase spectra (epochs 4 & 5):

• FeII, FeI, TiII etc. absorption lines now in emission

• He 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

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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)

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but …?

V1309 Sco:

• H + low & high ionization element emission lines

• A~7 mag• how is it evolving?

red novae:

• Just Balmer emission lines emission which soon “turned off”

• A ≥ 9-10 mag

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failed nova

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

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[OI](1) & [CaII](1):

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CaI & NaI evolution