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Nova LMC 2009

ATEL # 1930; Marina Orio (INAF-Padova & U Wisconsin), Elena Mason (ESO), Jay Gallagher (U Wisconsin) and Tim Abbott (CTIO)
on 11 Feb 2009; 23:18 UT
Password Certification: Marina Orio (orio@astro.wisc.edu)

Subjects: Optical, Nova

We obtained an optical spectrum of Nova LMC 2009 on 2009/2/6.9 with the CTIO Blanco 4-m telescope using the R-C Cassegrain spectrograph and the KPGL1-1 grating in the 3365-6435 Angstrom wavelength range. All spectral features shortwards of H(delta) are blue shifted and primarily in absorption, probably arising in an optically thick shell, while the other features at longer wavelengths are in emission with P-Cyg profiles. Most of the H-Balmer emission lines appear double peaked, with the highest peak sometimes in the blue and sometimes in the red portion of the line. We detect a strong H(beta) line with flux in emission 4E-12 erg/cm^2/s (about 600 Lsun), a prominent H(gamma) line with flux in emission of 1E12 erg/cm^2/s, Other emission lines are broader and single peaked, including He I at 4471 Angstroms and at 5016 Angstrom, (most likely blended with Fe II), as well as the strong 5876 line with a P-Cygni profile (9E-13 erg/cm^2/s). A pronounced emission blend of NII and NIII is at 4650 Angstrom, and a blend of N II lines around 5690 Angstrom. The full width at half maximum of the emission lines is slightly above 4200 km/s and the center of the P-Cyg absorption profiles is blue shifted by 2700 to 2900 km/s, with a second component blue shifted out to approximately 4800 km/s in H(gamma). The large expansion velocity is typical of a recurrent nova and we find that the most similar published spectrum of a nova at this stage is the one of U Sco (Iijima, T. 2002, A&A, 387, 1013).


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