MASTER Optical Flare Detection from the Fastes Accretor in Our Galaxy - IGR J00291+5934.

ATel #7835; V. Lipunov (Lomonosov Moscow State University, SAI), R. Rebolo, M. Serra-Ricart , N. Lodieu, G. Israelian (The Instituto de Astrofisica de Canarias),V. Lipunov, E. Gorbovskoy, V. Kornilov, P. Balanutsa, N. Tiurina, A. Kuznetsov, V. Chazov, D. Vlasenko, I. Gorbunov (Lomonosov Moscow State University, Sternberg Astronomical Institute), D. Buckley, S. Potter, M. Kotze (South African Astronomical Observatory), O. Gress, N. M. Budnev, K. Ivanov (Applied Physics Institute, Irkutsk State University), A. Tlatov, D. Dormidontov, V. Senik, A. V. Parhomenko (Kislovodsk Solar Station of the Pulkovo Observatory), V. Krushinski, I. Zalozhnykh (Ural Federal University), Yu. Sergienko, A. Gabovich, V. Yurkov (Blagoveschensk Educational State University)
on 24 Jul 2015; 19:12 UT
Credential Certification: Nataly Tyurina (tiurina@sai.msu.ru)

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MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru, Lipunov et al., Advances in Astronomy, MASTER Global Robotic Net, 2010) located in IAC was pointed to the Swift IGR J00291+5934 (Cummings et al., GCN 18051) 24 sec after notice time and 1103 sec after trigger time at 2015-07-24 05:42:03 UT. On our first (180s exposure) set we haven`t found optical transient within SWIFT error-box.

The 5-sigma upper limit has been about 17.2 mag

MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru ) located in Tunka was pointed to the Swift IGR J00291+5934 Swift Trigger 35223 sec after notice time and 36279 sec after trigger time at 2015-07-24 15:28:16 UT. On our first (180s exposure) set we found optical transient within Swift error-box ~ 17.5 unfileterd mag (CCD is red, m=0.2B+0.8R with respect to USNO B ) very close to coordinates
00 29 03.06 +59 34 19.0.

The 5-sigma upper limit has been about 19.4 mag .

This OT brightness very close to flare discovered ~11 years ago by P60 ( Derek B. Fox and S. R. Kulkarni, Atel #354). The IGR J00291+5934 is the close binary system with low magnetized Neutron Stars on Accreot stage (Lipunov, V.M., Astrophysics of the Neutron Stars, Spriner Verlag, 1992 ). By the way its peiod very close to other fastes millisecond pulsars (Ejector or Accretor) (~640 Hz). This means that neutron stars equation of state is hard (Lipunov and Postnov, 1984;; Friedman, J.L., Ipser, J.R. and Parker, L., 1985, ApJ., v.292, p.111-117 )

MASTER Global Robotic Net