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Optical Spectroscopy Confirms PNV J17355050-2934240 is a Fe II-type Classical Nova

ATel #8817; S. Frank (Ohio State), R. M. Wagner (LBTO and Ohio State), S. Starrfield (Arizona State), C. E. Woodward (Minnesota), and M. Neric (Arizona State)
on 15 Mar 2016; 06:04 UT
Credential Certification: R. Mark Wagner (rmw@as.arizona.edu)

Subjects: Optical, Nova

Referred to by ATel #: 8841, 8853

Following the discovery of a nova candidate by M. Yamamoto and reported on the CBAT Transient Object Confirmation Page (PNV J17355050-2934240), subsequent near-infrared spectroscopy by Srivastaa et al. (ATEL #8809), and pre-discovery observations by Mroz et al.(ATEL #8811), we obtained an optical spectrum (range: 398-686 nm; resolution 0.38 nm) of PNV J17355050-2934240 on 2016 March 14.51 UT with the Hiltner 2.4 m telescope (+OSMOS) of the MDM Observatory on Kitt Peak. The spectrum exhibits broad emission lines with P Cygni-type line profiles of the Balmer series of hydrogen (Hα, Hβ, and Hγ), Fe II (multiplets 37, 38, 42, 48, 49, and 74), and Na I D superposed on a reddened continuum. In addition, the interstellar features of Na I D (superposed on the broader profile), 578.0, and 628.4 nm are strong and prominent. The equivalent width of the 578 nm feature (0.19 nm) correlates with A_V ~ 5-6 mag using an older calibration (Herbig, 1975, ApJ, 196, 129) and is comparable with that reported by Mroz et al. (ATEL #8811). The Hα profile exhibits at least two emission line components in addition to the blue-shifted absorption component. A simple Gaussian de-convolution of the line profile gives a displacement of -850 km/s for the center of the absorption line and displacements of +91 and +1087 km/s with respect to line center for the two emission line components respectively. A comparison of our spectrum with those presented in the atlas by Williams, Phillips, and Hamuy (1994, ApJS, 90. 297) confirms the earlier suggestion by Srivastava et al. (ATEL #8809) that PNV J17355050-2934240 is a Fe II-type classical nova discovered early in the outburst. Further optical and infrared photometry and spectroscopy are encouraged.