2018ApJ...866..122H

Query : 2018ApJ...866..122H

2018ApJ...866..122H - Astrophys. J., 866, 122-122 (2018/October-3)

INSIGHT-HXMT observations of the new black hole candidate MAXI J1535-571 timing analysis.

HUANG Y., QU J.L., ZHANG S.N., BU Q.C., CHEN Y.P., TAO L., ZHANG S., LU F.J., LI T.P., SONG L.M., XU Y.P., CAO X.L., CHEN Y., LIU C.Z., CHANG H.-K., YU W.F., WENG S.S., HOU X., KONG A.K.H., XIE F.G., ZHANG G.B., ZHOU J.F., CHANG Z., CHEN G., CHEN L., CHEN T.X., CHEN Y.B., CUI W., CUI W.W., DENG J.K., DONG Y.W., DU Y.Y., FU M.X., GAO G.H., GAO H., GAO M., GE M.Y., GU Y.D., GUAN J., GUNGOR C., GUO C.C., HAN D.W., HU W., HUO J., JI J.F., JIA S.M., JIANG L.H., JIANG W.C., JIN J., JIN Y.J., LI B., LI C.K., LI G., LI M.S., LI W., LI X., LI X.B., LI X.F., LI Y.G., LI Z.J., LI Z.W., LIANG X.H., LIAO J.Y., LIU G.Q., LIU H.W., LIU S.Z., LIU X.J., LIU Y., LIU Y.N., LU B., LU X.F., LUO T., MA X., MENG B., NANG Y., NIE J.Y., OU G., SAI N., SHANG R.C., SUN L., TAN Y., TAO W., TUO Y.L., WANG G.F., WANG H.Y., WANG J., WANG W.S., WANG Y.S., WEN X.Y., WU B.B., WU M., XIAO G.C., XIONG S.L., XU H., YAN L.L., YANG J.W., YANG S., YANG Y.J., ZHANG A.M., ZHANG C.L., ZHANG C.M., ZHANG F., ZHANG H.M., ZHANG J., ZHANG Q., ZHANG T., ZHANG W., ZHANG W.C., ZHANG W.Z., ZHANG Y., ZHANG Y., ZHANG Y.F., ZHANG Y.J., ZHANG Z., ZHANG Z., ZHANG Z.L., ZHAO H.S., ZHAO J.L., ZHAO X.F., ZHENG S.J., ZHU Y., ZHU Y.X., ZOU C.L. (The Insight-HXMT Collaboration)

Abstract (from CDS):

We present X-ray timing results of the new black hole candidate MAXI J1535-571 during its 2017 outburst from Hard X-ray Modulation Telescope (Insight-HXMT) observations taken from 2017 September 6 to 23. Following the definitions given by Belloni, we find that the source exhibits transitions from the low/hard state to the hard intermediate state, and eventually to the soft intermediate state. Quasi-periodic oscillations (QPOs) are found in the intermediate states, which suggest different types of QPOs. With the large effective area of Insight-HXMT at high energies, we are able to present the energy dependence of the QPO amplitude and centroid frequency up to 100 keV, which has rarely been explored by previous satellites. We also find that the phase lag at the type-C QPOs centroid frequency is negative (soft lag) and strongly correlated with the centroid frequency. Assuming a geometrical origin of type-C QPOs, the source is consistent with being a high-inclination system.

Abstract Copyright: © 2018. The American Astronomical Society. All rights reserved.

Journal keyword(s): black hole physics - stars: individual: MAXI J1535-571 - X-rays: binaries

Simbad objects: 7

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Number of rows : 7
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 V* GU Mus HXB 11 26 26.5961559600 -68 40 32.877752952           K3V-K7V 734 1
2 MAXI J1535-571 XB* 15 35 19.73 -57 13 48.1           ~ 214 0
3 V* V381 Nor HXB 15 50 58.6637920704 -56 28 35.258385000           K3III 1254 0
4 V* V821 Ara LXB 17 02 49.3876391280 -48 47 23.087954544         15.322 ~ 2237 0
5 NAME XTE J17464-3213 LXB 17 46 15.59637 -32 14 00.8600           ~ 805 0
6 V* V406 Vul HXB 18 58 41.49127200 +22 39 29.7746640           G5V-K0V 409 0
7 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2810 0

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