SIMBAD references

2009CBET.1898....1M - Central Bureau Electronic Telegrams, 1898, 1 (2009/August-0)

V582 Aurigae.

MUNARI U., SIVIERO A., OCHNER P., FIORUCCI M. and DALLAPORTA S.

Abstract (from CDS):

U. Munari, A. Siviero, P. Ochner, and M. Fiorucci, Istituto Nazionale di Astrofisica, Padova Astronomical Observatory; and S. Dallaporta, "Asiago Novae and Symbiotic Stars" (ANS) collaboration, report that CCD photometry of V582 Aur (cf. CBET 1896) was obtained on Aug. 5.09 and 6.08 UT, yielding magnitudes B = 17.0 and 16.9, V = 14.78 and 14.83, R_c = 13.49 and 13.50, and I_c = 12.23 and 12.22, respectively. The calibration was carried out with respect to local Tycho-2 and 2MASS catalogue stars, using the transformations of Bessell (2000, PASP 112, 961) and Caldwell et al. (1993, SAAO Circ. 15, 1). A few photographic plates imaging the sky position of V582 Aur have been located in the archives of the Asiago Schmidt telescopes; V582 Aur appeared below the plate limits, which were mag B = 16.0 on 1975 May 2, and V = 14.8 and B = 16.0 on 1980 Feb. 14. A low-resolution CCD spectrum (0.24 nm/pixel; range 380-700 nm) was obtained on Aug. 6.12 with the 1.22-m telescope of the Asiago Astrophysical Observatory, attaining S/N = 50 around H_alpha. The spectrum is dominated by absorption lines of the Balmer series (the equivalent width of H_alpha was 0.52 nm), Na I D (EW = 0.43 nm) and Ba II 649.6-nm (EW = 0.20 nm). No emission line is evident on the spectrum, whose overall appearance is that of a super giant of temperature about 5500 K, and pretty close to that of V733 Cep (an object of the FU Ori type) as presented by Reipurth et al. (2007, A.J. 133, 1000). A significant difference is the Li 670.7-nm line, which is strong in V733 Cep and weak in the spectrum of V582 Aur, not emerging above the noise.

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2021.03.03-10:37:20

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