Continuing spectroscopic observations of the SMC classical nova ASASSN-19qv
ATel #12990; Terry C. Bohlsen (ARAS group; Mirranook, Armidale, NSW Australia)
on 5 Aug 2019; 21:03 UT
Distributed as an Instant Email Notice Novae
Credential Certification: S. N. Shore (shore@df.unipi.it)
We report the results of our continuing optical low resolution spectroscopic monitoring of the SMC nova ASASSN-19qv (see ATel #12917, #12938). All spectra were flux calibrated with exposure times of 3100 to 3670 sec and S/N ranging from a low of about 10 to 30 (peak line fluxes). Spectra were obtained from 2019 Jul 13.5 - Aug. 3.5 UT. Integrated fluxes (1E-11 erg/s/cm^2; no reddening correction; 4000-7000A) were Jul 13.5, 9.8; 14,5, 8.4; 17.5, 6.8; 19.5, 5.0; 25.5, 3.5;28.5, 2.4, Aug 3.5, 3.6 (uncertainties approx. 0.2). It appears that the last observation caught a brightening of the nova, consistent with our simultaneous photometric monitoring. Absorption was present on all Balmer lines until Jul 28, when it disappeared; the emission wings extended to 2000 km/s (HWZI), while during the transition to optically thin the absorption radial velocity varied slightly, from -2400 km/s to -2000 km/s. Fe II was dominant in the emission lines (although always far weaker than the Balmer lines), with e.g., Fe II 4921, 5018, and 5169, 4549, 4629 A being detectable; Fe II 4630 A -- that first appeared on Jul 19, -- was about half the integrated flux of Hbeta in the last spectrum. He I 5876A may have been present (based on coincidence of high velocity absorption with Hbeta, -2200 km/s) on Jul. 14 and Jul 19 but the S/N is too low to say much about its persistence; He I 6678 was not detected at all, and the spectra ae generally too noisy to reveal other transitions such as Si II 6347. No [O I] 6300A was detected. The nova, despite its high expansion velocities, seems to still be very opaque. Its brightness is now below the limit of our monitoring.
ARAS Nova Database