Modeling the IR De-Absorbed g-Ray Spectra of TeV BL Lacs

Details Modeling the IR De-Absorbed g-Ray Spectra of TeV BL Lacs Modeling the IR De-Absorbed g-Ray Spectra of TeV BL Lacs

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....5.2611k&link_type=abstract

Proceedings of the 28th International Cosmic Ray Conference. July 31-August 7, 2003. Trukuba, Japan. Under the auspices of the I

Physics

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Scientific paper

A sample of the BL Lac objects detected so far in TeV γ -rays consists of four well established sources, in particular Mkn 501, Mkn 421, 1ES 1426+428, and 1ES 1959+650. The energy spectra of these objects at TeV energies show the steep ening in the spectral slope, which can be attributed to the γ -ray absorption onto extra-galactic infra-red (IR) background light. Based on the empirically based model of the IR spectral energy distribution (SED) we have unfolded the intrinsic spectra of two BL Lac objects: Mkn 501 and Mkn 421 and modeled the TeV γ -ray emission in the synchrotron-self Compton (SSC) scenario. 2. Introduction It was suggested long ago that TeV γ -rays could be absorb ed by interacting with diffuse interstellar or intergalactic IR radiation [1]. Owing to the lack of direct measurements of the IR background radiation in the wavelength range 1-50 µm [2], a computation of the opacity of the intergalactic medium to TeV γ -rays must be based on a model of the diffuse radiation field. Here, we use the distributions of the extra-galactic background light (EBL) given by [3] to estimate both the magnitude and the uncertainty in the IR absorption and construct intrinsic spectra of TeV BL Lac objects. Having constructed the intrinsic spectrum we use the SSC model described by [4] to obtain a fit. The SSC model provides a reasonable fit for recent data on TeV γ -ray spectra measured from two BL Lacs Mkn 501 and Mkn 421 (i.e. for Mkn 421 in low and high state of activity). 3. IR opacities There have been a number of attempts in past to measure the SED of EBL in the mid-IR range, which is most relevant for interaction of the γ -rays of

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