|
ИСТИНА |
Войти в систему Регистрация |
ФНКЦ РР |
||
Spectroscopic confirmation of nova 2010-06d in M31статья
- Авторы: Barsukova E.A., Valeev A.F., Sholukhova O., Fabrika S., Hornoch K., Pietsch W., Goranskij V.P.
- Журнал: The Astronomer’s Telegram
- Номер: 2789
- Год издания: 2010
- Первая страница: 1
- Последняя страница: 1
- Аннотация: We have taken a spectrum of the optical nova candidate N2010-06d in M31 (RA = 00 42 55.56, Dec = +41 19 25.5, J2000). The star has been discovered by Pietsch et al. with UVOT on June 24.02 UT with the UVW1 filter having a magnitude of 19.5, and independently by K. Hornoch and M. Wolf with the 0.65-m telescope at Ondrejov Observatory on June 30.003 UT in the R filter with a magnitude of 18.6 (CBET#2347). During the BTA observations we measured the star brightness: Aug. 8.846 UT, B=19.3 +/- 0.15; 8.869, R=18.7 +/- 0.15. The spectrum of N2010-06d in M31 was obtained on 2010 August 8.86 UT with the Russian 6-m telescope (BTA) equipped with the SCORPIO spectral camera. The spectral range is 385-789 nm, the resolution is 1.3 nm. M31N 2010-06d shows a typical spectrum of the FeII group novae with a full sample of FeII emission lines. The Balmer emission lines are the strongest features in the spectrum. Equivalent widths of the H-alpha and H-beta lines are equal to 38 nm and 6 nm correspondingly. The H-alpha line width corrected for spectral resolution is FWHM = 1420 km/s, H-beta line width is 1300 km/s. The heliocentric radial velocities of Balmer lines are of about -400 km/s. The full width at zero intensity (FWZI) of H-alpha line is 3140 km/s. The line has a double peak profile with the peak maxima at -830 and -110 km/s. The next intense emissions are CaII H, K and NaI D2, D1 lines. The NaI doublet is not resolved, the total line profile has the same profile structure as that in H-alpha line. EW of NaI D2, D1 equals to 10 nm. Additionally we identified OI 777.3 nm and [OI] 557.7, 630.0 and 636.4 nm emission lines. The OI 777.3 nm close doublet shows the same double peak profile as those in H-alpha and NaI. HeI emissions are not visible.
- Добавил в систему: Горанский Виталий Петрович