Spectroscopy and Near-Infrared Photometry of the Helium Nova V445 Puppis

Details Spectroscopy and Near-Infrared Photometry of the Helium Nova V445 Puppis Spectroscopy and Near-Infrared Photometry of the Helium Nova V445 Puppis

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..797..647w&link_type=abstract

INTERACTING BINARIES: Accretion, Evolution, and Outcomes. AIP Conference Proceedings, Volume 797, pp. 647-650 (2005).

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Novae, Spectroscopy, Stellar Photometry, Novae, Dwarf Novae, Recurrent Novae, And Other Cataclysmic Variables, Cataclysmic Binaries, Symbiotic Stars, Spectroscopy And Spectrophotometry, Photography And Photometry

Scientific paper

V445 Pup (Nova Puppis 2000) is the first observed example of a helium nova (Kato & Hachisu 2003). Here we present Magellan spectroscopy of V445 Pup, obtained three years after outburst (V = 19.91 mag). The optical spectrum consists of He I, [O I], [O II], [O III] emission lines; no hydrogen is present. The emission lines show multiple velocity components (around +/- 850 km s-1 and +/- 1600 km s-1), associated with an expanding and clearly asymmetric nova shell. Images of V445 Pup obtained under good seeing conditions show this object to be elongated and extended. The expanding nova shell should allow an accurate distance determination of V445 Pup through high-resolution imaging and integral field unit spectroscopy. We have continuously monitored the near-infrared (J, H, Ks) secular evolution since 2002 March with the Infrared Survey Facility (IRSF) from the Sutherland site of the South African Astronomical Observatory (SAAO). Nearly four years of the outburst, V445 Pup is still covered by an optically thick dust shell (2004 September 29: E(J - Ks) ~ 4.6 +/- 0.1 mag).

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