Other
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21349125l&link_type=abstract
American Astronomical Society, AAS Meeting #213, #491.25; Bulletin of the American Astronomical Society, Vol. 41, p.471
Other
2
Scientific paper
We present a nineteen-spectrum time series that documents the visible and infrared (0.8 - 5.0 microns) evolution of novae V2467 Cygni. Observations were made using SpeX on the IRTF, and VNIRIS at Lick and spanned the period from 30 Apr 2007 to 12 Aug 2008 UT. Peak brightness (discovery) was mag 7.4 on 15 Mar 2007 UT. The decline rates t2 and t3 were 7.3 and 15.1 days, respectively. Except for some early, low amplitude periodic oscillations, the light curve declined monotonically and showed no evidence of dust formation as of this writing (Oct 1, 2008). The spectrum quickly moved from low excitation on 7 May 2007 UT to showing coronal lines of [Si VI], [Si VII], [Ca VIII], [S VIII] and [S IX] by May 31 2007. At least 5 Rydberg emission lines were present in the latter spectrum and all of the coronal lines had complex profiles. An interstellar reddening of E(B-V) = 1.5. was derived from the Lyman beta-fluoresced OI lines. By 14 Dec 2007 the object displayed many high-excitation emission lines. Coronal lines of [SI VII], [Ca VIII], [Si X], and [S XI] showed notched, doubled line profiles and lines of H I, He I, He II, weak OI, and Rydberg lines were still present. On June 15, 2008 the spectrum was dominated by coronal lines. [Mg VIII] at 3.03 microns was the brightest emission line in the infrared spectrum, and lines from four separate ionization states of silicon were present: [Si VI], [Si VII], [Si IX], [Si X]. Other species displaying coronal emission lines included [P VIII], [S VIII], [S IX], [Ca VII], [Ca VIII] and possibly [Ni X]. The 12 Aug 2008 spectrum was virtually identical to the 15 June 2008 spectrum only fainter.
Lynch David K.
Rudy Richard J.
Russell Ray W.
Woodward Charles E.
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