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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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2021.06.23-04:38:29

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