Visible and infrared spectroscopy of the nova V6595 Sagittarii
ATel #14553; A. J. Bayless (Aerospace Corp.), R. J. Rudy (Kookoosint Scientific), and J. P. Subasavage (Aerospace Corp.)
on 15 Apr 2021; 21:42 UT
Credential Certification: Amanda Bayless (amanda.bayless@aero.org)
Subjects: Infra-Red, Optical, Nova
Referred to by ATel #: 14625
We report results derived from 0.47-2.5 microns spectroscopy of the rapidly developing nova V6595 Sagittarii. The data were obtained 2021 April 8.503 (UT) with the Aerospace Corporation's 1.0 m telescope using its Visible and Near-Infrared Imaging Spectrograph (VNIRIS). V6595 Sgr was discovered on images from 2021 April 4.825 UT by Pearce and identified as a classical nova by Taguchi et al. (CBET #4952, ATel #14513). Optical spectroscopic measurements from 2021 April 6 by Aydi et al. (ATel #14533) were used by them to classify V6595 Sgr as an Fe II type nova. They also noted P-Cygni profiles and emission lines of low contrast relative to the continuum but with exceptional breadth. Our observation from two days later indicate considerable changes: emission lines were strong and P-Cygni absorptions had mostly disappeared. The emission lines remained exceptionally broad for an Fe II novae with FWHM of 3500 km/sec or greater. Fe II features were still present along with C I, N I, and O I, but He I emission was also present, indicative of the rapid spectral evolution of this nova. The N I lines were unusually strong relative to the C I features. Although there was no indication of dust emission, V6595 Sgr was bright at near infrared wavelengths: IR magnitudes derived from the spectroscopy are J = 5.5, H = 5.0, Kshort = 4.6
