2021NatAs...5...94M

Query : 2021NatAs...5...94M

2021NatAs...5...94M - Nature Astronomy, 5, 94-102 (2021/January-0)

Discovery of oscillations above 200 keV in a black hole X-ray binary with Insight-HXMT.

MA X., TAO L., ZHANG S.-N., ZHANG L., BU Q.-C., GE M.-Y., CHEN Y.-P., QU J.-L., ZHANG S., LU F.-J., SONG L.-M., YANG Y.-J., YUAN F., CAI C., CAO X.-L., CHANG Z., CHEN G., CHEN L., CHEN T.-X., CHEN Y.-B., CHEN Y., CUI W., CUI W.-W., DENG J.-K., DONG Y.-W., DU Y.-Y., FU M.-X., GAO G.-H., GAO H., GAO M., GU Y.-D., GUAN J., GUO C.-C., HAN D.-W., HUANG Y., HUO J., JI L., JIA S.-M., JIANG L.-H., JIANG W.-C., JIN J., JIN Y.-J., KONG L.-D., LI B., LI C.-K., LI G., LI M.-S., LI T.-P., LI W., LI X., LI X.-B., LI X.-F., LI Y.-G., LI Z.-W., LIANG X.-H., LIAO J.-Y., LIU B.-S., LIU C.-Z., LIU G.-Q., LIU H.-W., LIU X.-J., LIU Y.-N., LU B., LU X.-F., LUO Q., LUO T., MENG B., NANG Y., NIE J.-Y., OU G., SAI N., SHANG R.-C., SONG X.-Y., SUN L., TAN Y., TUO Y.-L., WANG C., WANG G.-F., WANG J., WANG L.-J., WANG W.-S., WANG Y.-S., WEN X.-Y., WU B.-Y., WU B.-B., WU M., XIAO G.-C., XIAO S., XIE F.-G., XIONG S.-L., XU H., XU Y.-P., YANG J.-W., YANG S., YANG Y.-J., YI Q.-B., YIN Q.-Q., YOU Y., ZHANG A.-M., ZHANG C.-M., ZHANG F., ZHANG H.-M., ZHANG J., ZHANG T., ZHANG W.-C., ZHANG W., ZHANG W.-Z., ZHANG Y., ZHANG Y.-F., ZHANG Y.-J., ZHANG Y., ZHANG Z., ZHANG Z., ZHANG Z.-L., ZHAO H.-S., ZHAO X.-F., ZHENG S.-J., ZHOU D.-K., ZHOU J.-F., ZHU Y.-X., ZHU Y. and ZHUANG R.-L.

Abstract (from CDS):

Low-frequency quasiperiodic oscillations (LFQPOs) are commonly found in black hole X-ray binaries, and their origin is still under debate. The properties of LFQPOs at high energies (above 30 keV) are closely related to the nature of the accretion flow in the innermost regions, and thus play a crucial role in critically testing various theoretical models. The Hard X-ray Modulation Telescope is capable of detecting emissions above 30 keV, and is therefore an ideal instrument to do so. Here we report the discovery of LFQPOs above 200 keV in the new black hole MAXI J1820+070 in the X-ray hard state, which allows us to understand the behaviours of LFQPOs at hundreds of kiloelectronvolts. The phase lag of the LFQPO is constant around zero below 30 keV, and becomes a soft lag (that is, the high-energy photons arrive first) above 30 keV. The soft lag gradually increases with energy and reaches ∼0.9 s in the 150-200 keV band. The detection at energies above 200 keV, the large soft lag and the energy-related behaviours of the LFQPO pose a great challenge for most existing models, but suggest that the LFQPO probably originates from the precession of a small-scale jet.

Abstract Copyright: ©

Journal keyword(s): Astrophysics - High Energy Astrophysical Phenomena

Simbad objects: 8

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Number of rows : 8
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 MAXI J1535-571 XB* 15 35 19.73 -57 13 48.1           ~ 214 0
2 V* V381 Nor HXB 15 50 58.6637920704 -56 28 35.258385000           K3III 1254 0
3 V* V1033 Sco HXB 16 54 00.1423963019 -39 50 44.761701340       16.14   F3-6IV 1980 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 2MAXI J1753-013 LXB 17 53 28.2898766424 -01 27 06.256555272 15.30 16.73 16.46 16.15 15.64 ~ 384 0
7 MAXI J1820+070 LXB 18 20 21.9423816480 +07 11 07.284859440           ~ 511 0
8 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2810 0

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