MASTER OT 082752.77+704606.0 discovery and 6 meter telescope follow-up spectroscopic observations
ATel #3255; A. V. Moiseev (SAO RAS), E. Gorbovskoy, P. Balanutsa, V. Lipunov, V. Kornilov, A. Belinski, N. Shatskiy, N. Tyurina, D. Kuvshinov, V. Chazov, A. Kuznetsov, D. Zimnukhov, M. Kornilov (SAI, Moscow), A. Tlatov, A. V. Parhomenko, D. Dormidontov (Kislovodsk solar station of the Pulkovo observatory RAS), V. Yurkov, I. Kudelina ,Yu. Sergienko, D. Varda (Blagoveshchensk Educational University), V. Krushinski, I. Zalozhnih, A. Popov (Ural State University), K. Ivanov, S. Yazev, N. Budnev, E. Konstantinov, O. Chuvalaev, V. Poleschuk, O. Gres,(Irkutsk State University) , V. Shumkov, S. Shurpakov (MASTER team member)
on 3 Apr 2011; 12:26 UT
Credential Certification: Vladimir Lipunov (lipunov2007@gmail.com)
Subjects: Optical, AGN, Transient
The MASTER auto-detection system at Tunka (Baykal Lake, Siberia)
during a regular sky survey detect a new transient source at the
position 08h 27m 52.77s , +70d 46m 06s.0 (J2000) with a typical
uncertainty of 0.5". We see it on two images at 2011-03-26
14:09:51UT and 40 minutes later. The unfiltered magnitude of OT is
19.1 +- 0.25. Our unfiltered magnitude is well described by a
parity 0.8R + 0.2B (USNO B1). We have a number images this field
without OT.
There is no minor planet brighter then 21 mag found at this
place, but OT could be identified with very faint (j=21.7) object of
the unknown nature in GSC2.3 (N7U1004894)
The discovery image is available at http://observ.pereplet.ru/images/OT082752+704606/OT082752+704606.png
We have performed follow-up spectroscopic observations of the OT with
the SCORPIO spectrograph at the 6-m telescope (Special Astrophysical
Observatory, Russia) on 2011-03-29. The exposures were started at
19:34:23 UT. The total exposure time was 40 min under seeing value
about 2.7 arcsec. The spectral resolution (with 1 arcsec slit width)
was about 6-7 A. In the range 4000-8500 A we have found only blue
continuum with one noticeable spectral feature, that is a broad
emission line at 5320 A.
The most probable explanation is a Mg II 2789 emission line observed
in AGN (QSO or Sy2) at the redshift z=0.91. The reduced spectrum is
available at:
http://observ.pereplet.ru/images/OT082752+704606/sao-spectrum.png
High energy observations are needed.
MASTER Robotic Net
