Spectroscopy of nova ASASSN-17hx
ATel #10613; M. Pavana, G. C. Anupama, G. Selvakumar, B. S. Kiran (Indian Institute of Astrophysics, Bengaluru, India)
on 2 Aug 2017; 14:54 UT
Credential Certification: G.C. Anupama (firstname.lastname@example.org)
We report the optical spectroscopic observations of ASASSN-17hx (ATel #10523, #10524, #10527, #10542, #10552, #10572) on July 03.82 UT, 26.61 UT and 27.58 UT. The spectra were obtained using the HFOSC instrument mounted on the 2m Himalayan Chandra Telescope (HCT) of the Indian Astronomical Observatory, Hanle in the 380-900nm wavelength range (July 03.82), and the OMR spectrograph mounted on the 2.3m Vainu Bappu Telescope (VBT) of the Vainu Bappu Observatory, Kavalur, India in the 380-890nm wavelength range (July 26.61 and 27.58).
On July 03.82 UT, we observed prominent and narrow emission lines with weak P- Cygni absorption features (as reported in ATel #10558). The emission component in the HeI (5876,6678) lines was absent or extremely weak. The strongest emission lines were H-alpha and H-beta followed by other Balmer lines, CaII (H & K), FeII multiplets, Paschen series, OI (7774,8446) and CaII triplet (8498, 8542, 8662). The spectrum of July 26.61 UT was dominated by absorption features, with strength of the emission component of all the lines having weakened considerably, with the exception of the H-alpha feature that did not show any prominent absorption component. In the spectrum of July 27.58, the P-Cygni absorption features developed in all the Balmer, FeII, OI and CaII lines, and the emission component strengthened in Hydrogen and FeII lines, but was still weaker in the other lines. The line velocities of H-alpha and H-beta was found to be 400 km/s and 310 km/s.