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3 results on '"Molkov SV"'

1. A multiwavelength analysis of a collection of short-duration GRBs observed between 2012 and 2015

Author

Pandey, SB, Hu, Y, Castro-Tirado, Ao J, Pozanenko, AS, Sánchez-Ramírez, R, Gorosabel, J, Guziy, S, Jelinek, M, Tello, JC, Jeong, S, Oates, SR, Zhang, B-B, Mazaeva, ED, Volnova, AA, Minaev, P Yu, van Eerten, HJ, Caballero-García, MD, Pérez-Ramírez, D, Bremer, M, Winters, J-M, Park, IH, Guelbenzu, A Nicuesa, Klose, S, Moskvitin, A, Sokolov, VV, Sonbas, E, Ayala, A, Cepa, J, Butler, N, Troja, E, Chernenko, AM, Molkov, SV, Volvach, AE, Inasaridze, R Ya, Egamberdiyev, Sh A, Burkhonov, O, Reva, IV, Polyakov, KA, Matkin, AA, Ivanov, AL, Molotov, I, Guver, T, Watson, AM, Kutyrev, A, Lee, WH, Fox, O, Littlejohns, O, Cucchiara, A, Gonzalez, J, Richer, MG, Román-Zúñiga, CG, Tanvir, NR, Bloom, JS, Prochaska, JX, Gehrels, N, Moseley, H, de Diego, JA, Ramírez-Ruiz, E, Klunko, EV, Fan, Y, Zhao, X, Bai, J, Wang, Ch, Xin, Y, Cui, Ch, Tungalag, N, Peng, Z-K, Kumar, Amit, Gupta, Rahul, Aryan, Amar, Kumar, Brajesh, Volvach, LN, Lamb, GP, and Valeev, AF

Subjects
Astronomical Sciences, Physical Sciences, gamma-rays: general, X-ray: bursts, techniques: photometric, radiation mechanims : non-thermalonova, astro-ph.HE, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

We investigate the prompt emission and the afterglow properties of short-duration gamma-ray burst (sGRB) 130603B and another eight sGRB events during 2012-2015, observed by several multiwavelength facilities including the Gran Canarias Telescope 10.4 m telescope. Prompt emission high energy data of the events were obtained by INTEGRAL-SPI-ACS, Swift-BAT, and Fermi-GBM satellites. The prompt emission data by INTEGRAL in the energy range of 0.1-10 MeV for sGRB 130603B, sGRB 140606A, sGRB 140930B, sGRB 141212A, and sGRB 151228A do not show any signature of the extended emission or precursor activity and their spectral and temporal properties are similar to those seen in case of other short bursts. For sGRB 130603B, our new afterglow photometric data constrain the pre-jet-break temporal decay due to denser temporal coverage. For sGRB 130603B, the afterglow light curve, containing both our new and previously published photometric data is broadly consistent with the ISM afterglow model. Modeling of the host galaxies of sGRB 130603B and sGRB 141212A using the LePHARE software supports a scenario in which the environment of the burst is undergoing moderate star formation activity. From the inclusion of our late-time data for eight other sGRBs we are able to: place tight constraints on the non-detection of the afterglow, host galaxy, or any underlying 'kilonova' emission. Our late-time afterglow observations of the sGRB 170817A/GW170817 are also discussed and compared with the sub-set of sGRBs.

Published
2019

2. Coordinated integral and optical observations of SS433

Author

Cherepashchuk, Am, Sunyaev, Ra, Fabrika, Sn, Molkov, Sv, Barsukova, Ea, Antokhina, Ea, Irsmambetova, Tr, Panchenko, Ie, Konstantin Postnov, Seifina, Ev, Shakura, Ni, Timokhin, An, Bikmaev, If, Sakhibullin, Na, Gnedin, Yn, Arkharov, Aa, and Larionov, Vm

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Results of simultaneous {\it INTEGRAL} and optical observations of galactic microquasar SS433 in May 2003 are presented. The analysis of the X-ray and optical eclipse duration and hard X-ray spectra obtained by {\it INTEGRAL} together with optical spectroscopy obtained on the 6-m telescope allows us to construct a model of SS433 as a massive X-ray binary. X-ray eclipse in hard X-rays has a depth of $\sim 80%$ and extended wings. The optical spectroscopy allows us to identify the optical companion as a A5-A7 supergiant and to measure its radial velocity semi-amplitude $K_v=132$ km/s. A strong heating effect in the optical star atmosphere is discovered spectroscopically. The observed broadband X-ray spectrum 2-100 keV can be described by emission from optically thin thermal plasma with $kT\sim 15-20 keV$, Comment: 8 pages, 11 figures, Proceedings of the V INTEGRAL Workshop, Munich 16-20 February 2004. ESA SP-552

3. Polarized x-rays constrain the disk-jet geometry in the black hole x-ray binary Cygnus X-1.

Author

Krawczynski H, Muleri F, Dovčiak M, Veledina A, Rodriguez Cavero N, Svoboda J, Ingram A, Matt G, Garcia JA, Loktev V, Negro M, Poutanen J, Kitaguchi T, Podgorný J, Rankin J, Zhang W, Berdyugin A, Berdyugina SV, Bianchi S, Blinov D, Capitanio F, Di Lalla N, Draghis P, Fabiani S, Kagitani M, Kravtsov V, Kiehlmann S, Latronico L, Lutovinov AA, Mandarakas N, Marin F, Marinucci A, Miller JM, Mizuno T, Molkov SV, Omodei N, Petrucci PO, Ratheesh A, Sakanoi T, Semena AN, Skalidis R, Soffitta P, Tennant AF, Thalhammer P, Tombesi F, Weisskopf MC, Wilms J, Zhang S, Agudo I, Antonelli LA, Bachetti M, Baldini L, Baumgartner WH, Bellazzini R, Bongiorno SD, Bonino R, Brez A, Bucciantini N, Castellano S, Cavazzuti E, Ciprini S, Costa E, De Rosa A, Del Monte E, Di Gesu L, Di Marco A, Donnarumma I, Doroshenko V, Ehlert SR, Enoto T, Evangelista Y, Ferrazzoli R, Gunji S, Hayashida K, Heyl J, Iwakiri W, Jorstad SG, Karas V, Kolodziejczak JJ, La Monaca F, Liodakis I, Maldera S, Manfreda A, Marscher AP, Marshall HL, Mitsuishi I, Ng CY, O'Dell SL, Oppedisano C, Papitto A, Pavlov GG, Peirson AL, Perri M, Pesce-Rollins M, Pilia M, Possenti A, Puccetti S, Ramsey BD, Romani RW, Sgrò C, Slane P, Spandre G, Tamagawa T, Tavecchio F, Taverna R, Tawara Y, Thomas NE, Trois A, Tsygankov S, Turolla R, Vink J, Wu K, Xie F, and Zane S

Abstract

A black hole x-ray binary (XRB) system forms when gas is stripped from a normal star and accretes onto a black hole, which heats the gas sufficiently to emit x-rays. We report a polarimetric observation of the XRB Cygnus X-1 using the Imaging X-ray Polarimetry Explorer. The electric field position angle aligns with the outflowing jet, indicating that the jet is launched from the inner x-ray-emitting region. The polarization degree is 4.01 ± 0.20% at 2 to 8 kiloelectronvolts, implying that the accretion disk is viewed closer to edge-on than the binary orbit. These observations reveal that hot x-ray-emitting plasma is spatially extended in a plane perpendicular to, not parallel to, the jet axis.

Published
2022
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