2011ApJ...733...96A

Query : 2011ApJ...733...96A

2011ApJ...733...96A - Astrophys. J., 733, 96 (2011/June-1)

Gamma-ray observations of the Be/Pulsar binary 1A 0535+262 during a giant X-ray outburst.

ACCIARI V.A., ALIU E., ARAYA M., ARLEN T., AUNE T., BEILICKE M., BENBOW W., BRADBURY S.M., BUCKLEY J.H., BUGAEV V., BYRUM K., CANNON A., CESARINI A., CIUPIK L., COLLINS-HUGHES E., CUI W., DICKHERBER R., DUKE C., FALCONE A., FINLEY J.P., FORTSON L., FURNISS A., GALANTE N., GALL D., GODAMBE S., GRIFFIN S., GUENETTE R., GYUK G., HANNA D., HOLDER J., HUGHES G., HUI C.M., HUMENSKY T.B., IMRAN A., KAARET P., KERTZMAN M., KRAWCZYNSKI H., KRENNRICH F., MADHAVAN A.S., MAIER G., MAJUMDAR P., McARTHUR S., MORIARTY P., ONG R.A., OTTE A.N., PANDEL D., PARK N., PERKINS J.S., POHL M., PROKOPH H., QUINN J., RAGAN K., REYES L.C., REYNOLDS P.T., ROACHE E., ROSE H.J., SAXON D.B., SEMBROSKI G.H., SENTURK G.D., SMITH A.W., TESIC G., THEILING M., THIBADEAU S., VARLOTTA A., VINCENT S., VIVIER M., WAKELY S.P., WARD J.E., WEEKES T.C., WEINSTEIN A., WEISGARBER T., WENG S., WILLIAMS D.A., WOOD M. and ZITZER B.

Abstract (from CDS):

Giant X-ray outbursts, with luminosities of about 10³⁷ erg/s, are observed roughly every five years from the nearby Be/pulsar binary 1A 0535+262. In this article, we present observations of the source with VERITAS at very high energies (VHEs; E >100 GeV) triggered by the X-ray outburst in 2009 December. The observations started shortly after the onset of the outburst and provided comprehensive coverage of the episode, as well as the 111 day binary orbit. No VHE emission is evident at any time. We also examined data from the contemporaneous observations of 1A 0535+262 with the Fermi/Large Area Telescope at high-energy photons (E > 0.1 GeV) and failed to detect the source at GeV energies. The X-ray continua measured with the Swift/X-Ray Telescope and the RXTE/PCA can be well described by the combination of blackbody and Comptonized emission from thermal electrons. Therefore, the gamma-ray and X-ray observations suggest the absence of a significant population of non-thermal particles in the system. This distinguishes 1A 0535+262 from those Be X-ray binaries (such as PSR B1259-63 and LS I +61°303) that have been detected at GeV-TeV energies. We discuss the implications of the results on theoretical models.

Abstract Copyright: ∼

Journal keyword(s): acceleration of particles - binaries: general - gamma rays: general - stars: individual: 1A 0535+262

Simbad objects: 9

Full paper

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Number of rows : 9

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	HD 245770	HXB	05 38 54.5748918624	+26 18 56.836952784	9.30	9.84	9.39	8.77	8.30	O9/B0III/Ve	1045	0
3	SNR G180.0-01.7	SNR	05 39 00.000	+27 50 00.00						~	294	2
4	GRO J0542+26	gam	05 42	+26.0						~	21	1
5	IC 443	SNR	06 17 00.0000000	+22 34 11.998901						~	1314	1
6	6C 061934+332747	BLL	06 22 52.22196634	+33 26 10.4109110						~	78	1
7	HD 259440	HXB	06 32 59.2566076656	+05 48 01.160755848	9.17	9.63	9.15			B0pe	256	0
8	PSR J0633+1746	Psr	06 33 54.153	+17 46 12.91						~	1308	0
9	CPD-63 2495	HXB	13 02 47.6544015048	-63 50 08.626970292	10.34	10.72	9.98	10.03		O9.5Ve	852	0

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