Further spectroscopic observations of Nova Del 2013 = PNV J20233073+2046041 with the Ondrejov Observatory

ATel #5282; S. N. Shore (University of Pisa and INFN-Pisa, Italy); P. Skoda and P. Rutsch (Astronomical Institute, Academy of Sciences of the Czech Republic- Ond?ejov, Czech Republic)
on 15 Aug 2013; 04:43 UT
Credential Certification: S. N. Shore (shore@df.unipi.it)

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We report high resolution results (0.23A at 6563A) results for the newly announced nova Del 2013 = PNV J20233073+2046041. These extend the report by Darnley et al. (ATEL #5279) based on low resolution spectra. Our grating spectra, obtained on 2013 Aug. 14.87 with the coude spectrograph at the 2 meter Zeiss telescope of the Ondrejov Observatory, shows strong H-alpha emission with a P Cyg profile extending to a maximum radial velocities of -2300 km/s (absorption, EW approx 8.1A) and +2400 km/s (emission, EW \approx 52.9A) with no terminal edge at high negative velocity. The emission is broad, asymmetric (stronger blueward) and now structureless. The He I 6678 appears to show a detached absorption feature at -870 km/s without strong emission. In contrast, He I 5875 shows a strong P Cyg line with velocities similar to H\alpha. Both components of Si II 6347, 6371 (RMT 2, see Williams, R. E. 2012, AJ, 144, 98) are present in absorption with vrad \approx -1100 km/s; Fe II 6456, and N I 6486 also appear to be present with vrad \approx -1100 and -960 km/s, respectively. The spectrum is typical of a classical nova -- possibly CO type -- in the early (optically thick) fireball stage but with indications of the onset of the recombination event (e.g. Shore et al. 2012, A&A, 537, C2) , based on weak displaced broad absorption from the Na I D lines. The interstellar components of Na I D are not saturated, suggesting the extinction is relatively low. The LAB H I 21 cm profile (Kalberla, P.M.W. et al. 2005, A&A, 440, 775) has a total HI column density of 1.15E21/ccm^2 at a peak v(LSR)=14.1 km/s, this is likely an upper limit since the 21 cm profile is broad. Observations are continuing and we strongly encourage continuing spectroscopic monitoring, especially in the infrared.