========================================================================== J/A+A/492/145 UBV(RI)C light curves of Nova Cygni 2006 (Munari+, 2008) The following files can be converted to FITS (extension .fit or fit.gz) table1.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/A+A/492/145 ==========================================================================
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Beginning of ReadMe : J/A+A/492/145 UBV(RI)c light curves of Nova Cygni 2006 (Munari+, 2008) ================================================================================ The nature and evolution of Nova Cygni 2006. Munari U., Siviero A., Henden A., Cardarelli G., Cherini G., Dallaporta S., Dalla Via G., Frigo A., Jurdana-Sepic R., Moretti S., Ochner P., Tomaselli S., Tomasoni S., Valisa P., Navasardyan H., Valentini M. <Astron. Astrophys., 492, 145-162 (2008)> =2008A&A...492..145M ================================================================================ ADC_Keywords: Novae ; Photometry, UBVRI ; Photometry, Cousins Keywords: stars: dwarf novae - stars: individual: V2362 Cyg Abstract: Nova Cyg 2006 has been intensively observed throughout its full outburst. We investigate the energetics and evolution of the central source and of the expanding ejecta, their chemical abundances and ionization structure, and the formation of dust. We recorded low, medium, and/or high-resolution spectra (calibrated into accurate absolute fluxes) on 39 nights, along with 2353 photometric UBVRcIc measures on 313 nights, and complemented them with IR data from the literature. The nova displayed initially the normal photometric and spectroscopic evolution of a fast nova of the FeII-type. Pre-maximum, principal, diffuse-enhanced, and Orion absorption systems developed in a normal way. After the initial outburst, the nova progressively slowed its fading pace until the decline reversed and a second maximum was reached (eight months later), accompanied by large spectroscopic changes. Following the rapid decline from second maximum, the nova finally entered the nebular phase and formed optically thin dust. We performed a photo-ionization analysis of the emission-line spectrum during the nebular phase, which showed a strong enrichment of the ejecta in nitrogen and oxygen, and none in neon, in agreement with theoretical predictions for the estimated 1.0M_sun_ white dwarf in Nova Cyg 2006. The similarities with the poorly investigated V1493 Nova Aql 1999a are discussed. Description: UBVRcIc photometry of Nova Cyg 2006 = V2362 Cyg mapping its photometric evolution until advanced phases is given. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 21 11 32.3 +44 48 04 V2362 Cyg = NOVA Cyg 2006 ----------------------------------------------------------
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