Continuing optical spectroscopic observations by the ARAS Group of the symbiotic-like recurrent nova V3890 Sgr
ATel #13108; Forrest Sims, Terry Bohlsen, Paolo Cazzato, Pavol A. Dubovski, Joao Guarro Flo, Olivier Garde, Paul Luckas, Umberto Sollecchia, G. Arlic, M. Leveque, J. Souchu, JP. Nougayrede *ARAS Group)
on 14 Sep 2019; 04:30 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 and medium resolution spectroscopic monitoring of the symbiotic-like recurrent nova V3890 Sgr (see ATel #13062 for first report, #13099 for most recent optical description). The spectra cover the period from 2019 Aug. 28.7 UT to Sep. 12.2 UT with resolutions from 500 to 11000 in th spectral window 3700-7300A, exposure times of 1100 to 14000 sec, and S/N ranging from a low of about 20 to about 100 (peak line fluxes). The period before Sep. 9 UT has been described in earlier ATels by several groups, here we report the most recent changes. The Fe II and related ions (e.g., Ti II) are distributed throughout the optical spectrum, with several prominent Fe II multiplets (e.g., 27, 28, 41, 42, 46, 48, 49, 74), the lines are not resolved (a gaussian fit yields sigma ~ 150 km/s, for R=1000). This was also found for He I (4023, 4471, 4922, 5015, 5876, 6678, 7065), He II (4200, 4686, 5411). The Balmer lines, especially H-alpha and H-beta, have low broad wings (HWZI = 4000 km/s) with shoulders (there is a distinct pedestal to the broad profile) and a narrower component (sigma ~ 270 km/s) giving all Balmer lines a "prussian helmet" form typical of the pre-breakout spectra of this type of nova. The [Fe XIV] 5303 line appeared after Sep. 9.1UT and before Sep. 10.3UT; the first spectrum showed only Fe II 5315, thereafter the 5303A line increased to about twice the flux of the Fe II line. This is the only major change in the spectrum in the last week detected in our data. The N III 4636 feature has remained the same relative to He II since Sep. 5.8UT (about half the flux). There is no indication of any [O I], [N II], [O III], or [Ar III], nor is there any obvious [Fe VI] or [Fe VII] emission (5276A is at best a blend with Fe II). The spectrum now resembles a strongly photoionized wind, in many ways similar to the spectra of V407 Cyg from about two to three weeks after outburst, with the exception of the [Fe XIV] line in V3890 Sgr. Observations are continuing. Below, for convenience, we include a list of the lines measured in the last spectra, most of which have not strongly varied since Sep., 9.0.
4023.4 He I
4100.1 H delta
4175.8 Fe II (28)
4198.0 He II
4232.1 Fe II (27)
4340.6 H gamma
4350.7 Fe II (27)
4385.7 Fe II (27)
4413.6 [Fe II]
4472.1 He I
4413.2 Fe II (27)
4472.6 He I
4516.9 Fe II (27)
4551.4 Fe II (28), Fe II (37)
4584.2 Fe II (38)
4637.4 Fe II (37)
4685.2 He II
4712.7 He I
4731.3 Fe II
4861.5 H beta
4922.6 He I, Fe II (42)
4993.4 Fe II
5016.4 He I, Fe II (42)
5168.8 Fe II (42)
5183.8 Ti II
5197.2 Fe II (49)
5234.4 Fe II (49)
5276.0 Fe II (49), [Fe VII]?
5283.1 Fe II (41)
5301.6 [Fe XIV]
5315.8 Fe II (48.49)
5361.9 Fe II (48)
5411.6 He II
5532.5 ?
5678.5 N II
5875.1 He I
5890.0 Na I (ISM)
5989.9 Fe II (46)
6029.2 ?
6040.0 ?
6084.5 Fe II (46)
6105.8 ?
6126.0 ?
6147.3 Fe II (74)
6155.8 Fe II
6181.3 [Fe II]
6238.7 Fe II
6247.2 Fe II (74)
6317.3 Fe II
6346.0 Fe II (74)
6372.5 [Fe X]?
6403.4 [Fe II]
6432.0 Fe II
6492.6 Fe II
6516.0 Fe II
6562.0 H alpha
6608.0 Ti II
6636.8 Ti II
6677.1 He I
6828.2 Fe II
6915.4 ?
6979.2 Ti II
7064.1 He I
7220.7 Fe II
7281.6 He I
ARAS Nova Database
