Eruption of recurrent nova V3890 Sgr

Alerts and Monitoring of Novae

Re: Eruption of recurrent nova V3890 Sgr

Postby umberto sollecchia » Fri Aug 30, 2019 8:09 am

Merci beaucoup François, je dois féliciter Joan pour son fabuleux spectroscope fait maison.
La nuit dernière, j’ai encore regardé la nova, le ciel n’était pas dégagé, voici le profil, le graphique du V.R. et une comparaison avec 28-08-2019.
Umberto

v3890sgr_20190829_835_U.Sollecchia.png
v3890sgr_20190829_835_U.Sollecchia.png (41.78 KiB) Viewed 4798 times


v3890sgr_20190829_835_V.R. _U. Sollecchia.png
v3890sgr_20190829_835_V.R. _U. Sollecchia.png (21.79 KiB) Viewed 4798 times


v3890sgr_20190829_835_ Comparazione - U. Sollecchia.png
v3890sgr_20190829_835_ Comparazione - U. Sollecchia.png (55.97 KiB) Viewed 4798 times
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Re: Eruption of recurrent nova V3890 Sgr

Postby Francois Teyssier » Fri Aug 30, 2019 8:35 am

X-Ray emission detecyed by Swift:



ATEL #13050 ATEL #13050

Title: Swift X-ray detection during the optical peak of the recurrent
nova V3890 Sgr
Author: K. V. Sokolovsky (MSU), M. Orio (INAF Padova and University
of Wisconsin-Madison), K. L. Page, A. Beardmore, J. P. Osborne (U.
Leicester), P. Kuin (MSSL/UCL), J. Leahy-McGregor, E. Aydi, L. Chomiuk,
A. Kawash, J. Strader (MSU), J. D. Linford (NRAO), M. Rupen (NRC HAA)
Queries: kirx@kirx.net
Posted: 29 Aug 2019; 18:12 UT
Subjects:Optical, Ultra-Violet, X-ray, Nova

The 2019 eruption of the symbiotic recurrent nova V3890 Sgr was
discovered by A. Pereira on 2019-08-27.87 UT and confirmed by many
observers (ATel #13047; previous eruptions: 1962-06-02 and
1990-04-27, Schaefer 2010, ApJS, 187, 275). The latest pre-outburst
observation was performed by R. Stubbings on 2019-08-27.521, who
visually estimated the object brightness as 15.2mag
(vsnet-alert 23507, AAVSO Alert Notice 677).

Swift observed V3890 Sgr for 2 ks on 2019-08-28.438. Swift/XRT
detected an X-ray source with the net count rate of
1.85 ±0.03 cts/s (grade 0 events) at the position of the nova.
The XRT was operating in Windowed Timing mode to avoid optical
loading. The nova spectrum can be fitted with a heavily absorbed
thermal plasma with kT = 7.9 +2.3/-1.6 keV and
n_HI = (3.4 ±0.3) x10^22 cm^-2. The Fe emission feature with
EW ~ 1 keV is clearly visible at 6.67 +0.07/-0.06 keV.
The feature can be reproduced by the APEC plasma emission model if
the Fe abundance (by number) is increased by a factor of 3 with
respect to the solar value. The unabsorbed 0.3-10 keV flux is
1.8x10^-10 ergs/cm^2/s. The ultraviolet count rate is too high
for Swift/UVOT allowing us to place only a lower limit on the nova
brightness: UVW1 < 8.6.

Optical photometry of the nova was performed with
the 0.6m telescope of the MSU Campus Observatory (MPC code 766).

JD(UT) Band mag err
2458723.5492 V 7.36 0.01
2458723.5514 B 7.99 0.01
2458723.5528 I 6.68 0.02
2458723.5536 R 6.76 0.01
2458723.6188 V 7.17 0.01
2458723.6204 B 7.78 0.01
2458723.6216 R 6.58 0.01
2458723.6222 I 6.44 0.01
2458723.6516 V 7.28 0.01
2458723.6529 B 7.91 0.01
2458723.6540 R 6.65 0.02
2458723.6546 I 6.51 0.02
2458723.6734 V 7.41 0.01
2458723.6746 B 8.01 0.01
2458723.6758 R 6.76 0.03
2458723.6764 I 6.60 0.02

The lightcurve suggests that the nova had peaked at V=7.17
on 2019-08-28.1188. We adopted the following magnitudes for
the comparison star HD 170434 B=8.566, V=8.255, R=8.070, I=8.312
(taken or color-transformed from APASS).

V3890 Sgr is one of 4 known symbiotic (red giant donor) recurrent
novae, along with T CrB, RS Oph, and V745 Sco. The 2014 eruption
of V745 Sco (Page et al. 2015, MNRAS, 454, 3108) and the 2006
eruption of RS Oph (Bode et al. 2006, ApJ, 652, 629) were followed
with Swift providing a direct comparison. In both novae, the hard
thermal X-ray emission was detected in the first days of
the outburst. The emission was attributed to the shock-heated
plasma produced by the nova blast wave propagating in
the red giant wind.

We encourage a continued high cadence monitoring of V3890 Sgr
at all wavelengths.
Francois Teyssier
 
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Re: Eruption of recurrent nova V3890 Sgr

Postby Olivier GARDE » Fri Aug 30, 2019 9:49 am

Here's my contribution with my eShel spectrograph. From my home, the target is very low, so difficult to take a good spectrum.

The full spectrum (croped at 4500 Å because of the noise below this wavelength)

Image

And H Alpha line with a resolution better than 12000
Image
LHIRES III #5, LISA, e-Shel, C14, RC400 Astrosib, AP1600
http://o.garde.free.fr/astro/Spectro1/Bienvenue.html
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Re: Eruption of recurrent nova V3890 Sgr

Postby Joan Guarro Flo » Fri Aug 30, 2019 10:34 am

Hello al,

Good result Olivier !

Unfortunately yesterday Piera was cloudy and I didn't can used the NOU_T, but the weather was fine in Sta. Maria, so I was observed V3890 Sgr with the LINX echelle. There are the results. Both cases have a long time exposure.

Robin, I have this star about 20 degrees above the horizon, that means an important atmospheric estinction with a remarkable humidity sometimes in Piera, in Sta. Maria it's another thing..By the way, I think I've had a little of lucky..

Regards, Joan.
Attachments
_2V3890 SGR_A.png
_2V3890 SGR_A.png (15.95 KiB) Viewed 4780 times
_2V3890 SGR_B.png
_2V3890 SGR_B.png (20.83 KiB) Viewed 4780 times
_2V3890 SGR_C.png
_2V3890 SGR_C.png (26.1 KiB) Viewed 4780 times
Joan Guarro Flo
 
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Re: Eruption of recurrent nova V3890 Sgr

Postby Robin Leadbeater » Fri Aug 30, 2019 3:25 pm

Joan Guarro Flo wrote:Robin, I have this star about 20 degrees above the horizon, that means an important atmospheric estinction with a remarkable humidity sometimes in Piera, in Sta. Maria it's another thing..By the way, I think I've had a little of lucky..


Ah yes of course they are mostly just Telluric lines :oops:

Thanks
Robin
LHIRES III #29 ATIK314 ALPY 600/200 ATIK428 Star Analyser 100/200 C11 EQ6
http://www.threehillsobservatory.co.uk
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Re: Eruption of recurrent nova V3890 Sgr

Postby Francois Teyssier » Sat Aug 31, 2019 7:45 am

Title: 0.38-2.5 micron spectroscopy of the recurrent nova V3890 Sagittarii
Author: Richard Rudy, John Subasavage, Kirk Crawford, David Gutierrez,
Ray Russell, Sloane Wiktorowicz (The Aerospace Corporation)
Queries: CorrespondingAuthor&#39;sEmailAddress
Posted: 31 Aug 2019; 01:45 UT
Subjects:Infra-Red, Optical, Nova

Optical and IR spectra from 0.38-2.5 microns (resolution: 6-30 angstroms)
of the recurrent nova V3890 Sagittarii were obtained 2019 August 30.18
(UT) with the Aerospace Corporation's 1.0 m telescope using its Visible
and Near-Infrared Imaging Spectrograph (VNIRIS). Our observations show
changes from the spectrum of Strader et. al. (#ATel 13047) from 2 days
previous. The broad absorption on the wing of H-alpha is no longer apparent
and the spectrum displays weak Fe II emission and strong O I lines. The
lines remain very broad with full width zero intensities reaching 10,000
km/sec. The reddening derived from the O I lines at 0.8446, 1.1287, and
1.3165 microns is E(B-V) = 0.5 +- 0.2. The nova is very bright. We derive
infrared magnitudes from our spectroscopy for J, H, and K of 6.6, 6.4,
and 6.0, respectively, and a V magnitude of 8.9.

------------------------------------------------------------------------------
Password Certification: Richard Rudy (richard.j.rudy@aero.org)
http://www.astronomerstelegram.org/?read=13059
==============================================================================
ATEL #13060 ATEL #13060

Title: Optical spectroscopy of the recurrent nova V3890 Sagittarii

Author: M. Pavana, G. C. Anupama, S. Pramod Kumar (Indian Institute
of Astrophysics, Bengaluru, India)
Queries: gca@iiap.res.in
Posted: 31 Aug 2019; 06:56 UT
Subjects:Optical, Nova

We report optical spectroscopic observations of the recurrent nova V3890
Sagittarii (ATels #13047, #13050, #13059) on 2019 Aug 30.71 UT. The spectrum
was obtained using the HFOSC instrument mounted on the 2m Himalayan Chandra
Telescope (HCT) of the Indian Astronomical Observatory, Hanle, in the 380-900
nm wavelength range. The spectrum consists of strong, broad hydrogen Balmer
lines, with an average FWZI of ~9500 km/s. The narrower core has an average
FWHM of ~2000 km/s. The dominant non-Balmer lines are O I (7774 and 8446),
He I (5876, 6678, 7065) and Fe II, with an average FWHM of ~2000 km/s.

We thank the HCT observers for sparing time to carry out the ToO observations.
Francois Teyssier
 
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Re: Eruption of recurrent nova V3890 Sgr

Postby Joan Guarro Flo » Sat Aug 31, 2019 10:16 am

Hello all,

V3980 Sgr results again.

Joan.
Attachments
_3V3890SGR.png
_3V3890SGR.png (26.34 KiB) Viewed 4724 times
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Re: Eruption of recurrent nova V3890 Sgr

Postby Paolo Berardi » Sat Aug 31, 2019 10:58 am

Congratulations to all! Joan, your spectra are *incredible*!

Too low on the horizon from my observatory... sadly, I cannot observe this very peculiar nova.

Paolo
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Re: Eruption of recurrent nova V3890 Sgr

Postby Francois Teyssier » Sun Sep 01, 2019 5:28 pm

The nova is declining quickly, as expected.
But the slope seems to weaken a little bit.
V3890Sgr_V.PNG
V3890Sgr_V.PNG (4.43 KiB) Viewed 4654 times


Evolution with low resolution Spectra
Pavol A. Dubovski
Arlic G., Leveque M., Souchu J., Nougayrede JP.'
Paul Luckas

v3890sgr_LR.png
v3890sgr_LR.png (32.94 KiB) Viewed 4654 times


H alpha Line
Joan Guarro
Umberto Sollecchia
Olivier Garde

v3890sgr_Ha.png
v3890sgr_Ha.png (45.87 KiB) Viewed 4654 times



A spectrum obtained 18 days after 1990 outburst
showing very high ionization lines [Fe X] and [Fe XIV], resp. 262 and 392 eV!

1990.PNG
1990.PNG (42.27 KiB) Viewed 4654 times


Of course further observations are very welcome until nebular stage

Bonne continuation,
François
Francois Teyssier
 
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Re: Eruption of recurrent nova V3890 Sgr

Postby Francois Teyssier » Mon Sep 02, 2019 4:52 pm

ATEL #13062 ATEL #13062

Title: Optical spectroscopy of V3890 Sagittarii
Author: Hiroyuki Maehara (National Astronomical Observatory of Japan),
Keisuke Isogai (Kyoto University)
Queries: hiroyuki.maehara@nao.ac.jp
Posted: 1 Sep 2019; 19:04 UT
Subjects:Optical, Nova

We report optical spectroscopic observations of the recurrent nova V3890
Sagittarii (ATel #13047, #13050, #13059, #13060). We obtained low-resolution
spectra of this object on 2019-08-30.509 and 2019-08-31.469 with the fiber-fed
integral field spectrograph (KOOLS-IFU; <a href="https://ui.adsabs.harvard.edu/abs/2019arXiv190505430M/abstract"
target="_blank">Matsubayashi et al. 2019</a>) mounted on the 3.8-m Seimei
telescope at Okayama Observatory, Kyoto University. Both spectra show
broad Balmer, He I, He II/N III, N II, and O I lines in emission. Fe II
(multiplet 27, 37/38, 42, 48, 49, 55, 74) and Si II (6347/6371) lines
are also seen in emission. The FWZI of H-alpha line is ~9000 km/s. The
spectra can be seen at the following URL: <a href="http://www.kwasan.kyoto-u.ac.jp/~maehara/seimei/V3890_Sgr/V3890_Sgr-20190830.pdf"
target="_blank">http://www.kwasan.kyoto-u.ac.jp/~maehara/seimei/V3890_Sgr/V3890_Sgr-20190830.pdf</a>.
Francois Teyssier
 
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