A NEW MODEL FOR GAMMA-RAY CASCADES IN EXTRAGALACTIC MAGNETIC FIELDS

被引：29

作者：

Huan, H. ^{[1
]}

Weisgarber, T. ^{[1
]}

Arlen, T. ^{[2
]}

Wakely, S. P. ^{[1
]}

机构：

[1] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA

[2] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2011年 / 735卷 / 02期

关键词：

astroparticle physics; BL Lacertae objects: individual (RGB J0710+591); cosmic background radiation; gamma rays: general; intergalactic medium; magnetic fields; ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; ACCELERATION; EMISSION; CONSTRAINTS; RADIATION; BLAZARS; HALOS;

D O I：

10.1088/2041-8205/735/2/L28

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Very high energy (VHE, E greater than or similar to 100 GeV) gamma rays emitted by extragalactic sources, such as blazars, initiate electromagnetic cascades in the intergalactic medium. The cascade photons arrive at the Earth with angular and temporal distributions correlated with the extragalactic magnetic field (EGMF). We have developed a new semi-analytical model of the cascade properties which is more accurate than previous analytic approaches and faster than full Monte Carlo simulations. Within its range of applicability, our model can quickly generate cascade spectra for a variety of source emission models, EGMF strengths, and assumptions about the source livetime. In this Letter, we describe the properties of the model and demonstrate its utility by exploring the gamma-ray emission from the blazar RGB J0710+591. In particular, we predict, under various scenarios, the VHE and high-energy (100 MeV less than or similar to E less than or similar to 300 GeV) fluxes detectable with the VERITAS and Fermi Large Area Telescope observatories. We then develop a systematic framework for comparing the predictions to published results, obtaining constraints on the EGMF strength. At a confidence level of 95%, we find the lower limit on the EGMF strength to be similar to 2 x 10(-16) G if no limit is placed on the livetime of the source or similar to 3 x 10(-18) G if the source livetime is limited to the past similar to 3 years during which Fermi observations have taken place.

引用

页数：5

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