Spectra of luminous nova M31N 2013-10h (= Swift J004304.9+411630) in brighteningстатья

Дата последнего поиска статьи во внешних источниках: 28 мая 2015 г.

Работа с статьей

[1] Spectra of luminous nova m31n 2013-10h (= swift j004304.9+411630) in brightening / S. Fabrika, E. A. Barsukova, A. F. Valeev et al. // The Astronomer’s Telegram. — 2013. — no. 5554. — P. 1–1. We report optical spectroscopy and photometry of the recent M31 nova candidate M31N 2013-10h (= Swift J004304.9+411630 = TCP J00430483+4116306) discovered as Swift UVOT transient (ATel #5528). Koichi Nishiyama, Kurume and Fujio Kabashima, Miyaki (CBAT, 2013 10 31.4963) have confirmed the transient in the optical as 17.9 mag source in unfiltered CCD frames (on Oct. 29.571 UT they have reported only an upper limit). The confirmation was 1.2 - 1.4 days after the Swift discovery (the uncertainty is determined by Swift pointings). Using the Russian BTA telescope equipped with the SCORPIO spectrograph we have obtained spectra and photometry of the nova M31N 2013-10h on three occasions: on 2013 Nov. 1.67 UT (blue_1), Nov. 1.97 UT (red_1) and Nov. 2.66 UT (blue_2). The blue spectra have a resolution of 5 Å and spectral range 4050 - 5850 Å, the red spectrum has the same resolution and spectral range 5750 - 7500 Å. The nova appeared to be in a brightening phase during our observations. We classify the nova as of Fe II class. Its spectrum has many blue-shifted absorption lines of hydrogen, Fe II, Si II, Mg II, Na I with weak emission components having P Cyg type profiles. The two blue spectra taken with the same configuration and separated by one day have not shown a strong evolution, however the second spectrum became redder. The expansion velocity measured as the separation between the center of the absorption and the emission peak in the blue_1 spectrum is 700 km/s in Hβ, 600-700 km/s in the brightest Fe II lines, and it is 700 km/s in Hα in the red_1 spectrum. One day later in the blue_2 spectrum the velocity decreased by 100 km/s (mostly because of the blue wing of the blue-shifted absorptions). All equivalent widths decreased respectively: from 2.1 Å to 0.6 Å in Hβ emission, from 4.6 Å to 3.6 Å in Hβ absorption. In the red_1 spectrum the Hα line has an EW = 8 Å in emission and 6 Å in absorption. In our three epochs of observation the photometry of the nova gives (errors are 0.02 - 0.03 mag): B = 16.66, V = 16.45, Rc = 16.30 (blue_1), B = 16.63, V = 16.39, Rc = 16.19 (red_1), B = 16.08, V = 15.81, Rc = 15.62 (blue_2). The nova continuously brightened and reddened during our observations. We conclude that M31N 2013-10h is too luminous to represent the V723 Cas case, while it's emission line width and expansion velocity appear too low to match the luminous nova M31N 2007-11d. Further spectral and photometric monitoring of M31N 2013-10h are strongly encouraged.

Публикация в формате сохранить в файл сохранить в файл сохранить в файл сохранить в файл сохранить в файл сохранить в файл скрыть