2020ApJ...888..115A

Query : 2020ApJ...888..115A

2020ApJ...888..115A - Astrophys. J., 888, 115-115 (2020/January-2)

Probing the properties of the pulsar wind in the gamma-ray binary HESS J0632+057 with NuSTAR and VERITAS observations.

ARCHER A., BENBOW W., BIRD R., BRILL A., BROSE R., BUCHOVECKY M., CHRISTIANSEN J.L., CHROMEY A.J., CUI W., FALCONE A., FENG Q., FINLEY J.P., FORTSON L., FURNISS A., GENT A., GILLANDERS G.H., GIURI C., GUETA O., HANNA D., HASSAN T., HERVET O., HOLDER J., HUGHES G., HUMENSKY T.B., KAARET P., KELLEY-HOSKINS N., KERTZMAN M., KIEDA D., KRAUSE M., LANG M.J., MAIER G., MORIARTY P., MUKHERJEE R., NIETO D., NIEVAS-ROSILLO M., O'BRIEN S., ONG R.A., OTTE A.N., PARK N., PETRASHYK A., PFRANG K., POHL M., PRADO R.R., PUESCHEL E., QUINN J., RAGAN K., REYNOLDS P.T., RIBEIRO D., RICHARDS G.T., ROACHE E., SADEH I., SANTANDER M., SCHLENSTEDT S., SEMBROSKI G.H., SUSHCH I., WEINSTEIN A., WILCOX P., WILHELM A., WILLIAMS D.A., WILLIAMSON T.J. (The VERITAS Collaboration), HAILEY C.J., MANDEL S., MORI K. (The NuSTAR Collaboration)

Abstract (from CDS):

HESS J0632+057 is a gamma-ray binary composed of a compact object orbiting a Be star with a period of about 315 days. Extensive X-ray and TeV gamma-ray observations have revealed a peculiar light curve containing two peaks, separated by a dip. We present the results of simultaneous observations in hard X-rays with NuSTAR and in TeV gamma-rays with VERITAS, performed in 2017 November and December. These observations correspond to the orbital phases ph ≃ 0.22 and 0.3, where the fluxes are rising toward the first light-curve peak. A significant variation of the spectral index from 1.77 ± 0.05 to 1.56 ± 0.05 is observed in the X-ray data. The multiwavelength spectral energy distributions (SED) derived from the observations are interpreted in terms of a leptonic model, in which the compact object is assumed to be a pulsar and nonthermal radiation is emitted by high-energy electrons accelerated at the shock formed by the collision between the stellar and pulsar wind. The results of the SED fitting show that our data can be consistently described within this scenario, and allow us to estimate the magnetization of the pulsar wind at the location of the shock formation. The constraints on the pulsar wind magnetization provided by our results are shown to be consistent with those obtained from other systems.

Abstract Copyright: © 2020. The American Astronomical Society. All rights reserved.

Journal keyword(s): Gamma-ray sources - High mass X-ray binary stars - Gamma-ray astronomy - Particle astrophysics - Pulsars

Simbad objects: 10

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Number of rows : 10
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 LS I +61 303 HXB 02 40 31.6644419688 +61 13 45.593918580 11.27 11.61 10.75 10.19 9.55 B0Ve 903 2
2 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
3 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5476 0
4 4FGL J0535.2-6736 HXB 05 36 00.01 -67 35 07.5           ~ 49 0
5 HD 259440 HXB 06 32 59.2566076656 +05 48 01.160755848 9.17 9.63 9.15     B0pe 256 0
6 1FGL J1018.6-5856 HXB 10 18 55.5875706288 -58 56 45.975246900   13.638 12.683     O6V((f)) 156 0
7 CPD-63 2495 HXB 13 02 47.6544015048 -63 50 08.626970292 10.34 10.72 9.98 10.03   O9.5Ve 852 0
8 2MASS J14051441-6118282 HXB 14 05 14.41560 -61 18 28.2168           O6.5III 53 0
9 V* V479 Sct HXB 18 26 15.0561548880 -14 50 54.247274304 12.02 12.23 11.27 11.04   ON6V((f))z 613 2
10 [MT91] 213 Psr 20 32 13.1247390384 +41 27 24.346666440 13.12 13.08 11.266     B0Vp 334 0

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