Spitzer Space Telescope and Visible/IR Spectrophotometry of V574 Pupis (Nova Pupis 2004)

Details Spitzer Space Telescope and Visible/IR Spectrophotometry of V574 Pupis (Nova Pupis 2004) Spitzer Space Telescope and Visible/IR Spectrophotometry of V574 Pupis (Nova Pupis 2004)

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...209.0906r&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #09.06; Bulletin of the American Astronomical Society, V

Astronomy and Astrophysics

Astronomy

1

Scientific paper

V574 Pup was a nova whose observational properties were intermediate between those typical of explosions on a carbon/oxygen (CO) or a oxygen/magnesium/neon (OMgNe) white dwarf. A strong Fe II emitter shortly after outburst, V574 Pup’s light curve had a slow decline rate (t2 20 days) and emission lines of moderate width ( 1800 km/sec) characteristic of a high mass ejection from a CO white dwarf. However, V574 Pup did not form dust and its spectrum developed the strong nitrogen and helium lines and the fairly high excitation coronal lines (e.g., [S IX], [Si X]) more representative of the energetic outburst from an OMgNe white dwarf.
Data will be presented from two epochs_0.43-2.5 micron spectroscopy from two months after outburst, and Spitzer observations from 5-20 microns together with simultaneous visible and near-infrared measurements one year past outburst. Spitzer makes possible the study of nova spectra to unprecedented faintness levels and in V574 Pup reveals the strong coronal lines of Mg and Ne ions (but no [Ne II] at 12.8 microns), behavior that is again suggestive of an explosion on the surface of a OMgNe white dwarf.
Support for this work was provided by NASA and by the The Aerospace Corporation’s Independent Research and Development progam.

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