Measurement of the EBL spectral energy distribution using the VHE $\gamma$-ray spectra of H.E.S.S. blazars
- ABDALLA, H.
- ABRAMOWSKI, A.
- AHARONIAN, F.
- AIT BENKHALI, F.
- ANGÜNER, E.O.
- ARRIETA, M.
- AUBERT, P.
- BACKES, M.
- BALZER, A.
- BARNARD, M.
- BECHERINI, Y.
- BECKER TJUS, J.
- BERGE, D.
- BERNHARD, S.
- BERNLÖHR, K.
- BLACKWELL, R.
- BÖTTCHER, M.
- BOISSON, C.
- BOLMONT, J.
- BORDAS, P.
- BREGEON, J.
- BRUN, F.
- BRUN, P.
- BRYAN, M.
- BULIK, T.
- CAPASSO, M.
- CARR, J.
- CASANOVA, S.
- CERRUTI, M.
- CHAKRABORTY, N.
- CHALME-CALVET, R.
- CHAVES, R.C.G.
- CHEN, A.
- CHEVALIER, J.
- CHRÉTIEN, M.
- COLAFRANCESCO, S.
- COLOGNA, G.
- CONDON, B.
- CONRAD, J.
- CUI, Y.
- DAVIDS, I.D.
- DECOCK, J.
- DEGRANGE, B.
- DEIL, C.
- DEVIN, J.
- DEWILT, P.
- DIRSON, L.
- DJANNATI-ATAI, A.
- DOMAINKO, W.
- DONATH, A.
- DRURY, L.O'C.
- DUBUS, G.
- DUTSON, K.
- DYKS, J.
- EDWARDS, T.
- EGBERTS, K.
- EGER, P.
- ERNENWEIN, J.-P.
- ESCHBACH, S.
- FARNIER, C.
- FEGAN, S.
- FERNANDES, M.V.
- FIASSON, A.
- FONTAINE, G.
- FÖRSTER, A.
- FUNK, S.
- FÜSSLING, M.
- GABICI, S.
- GAJDUS, M.
- GALLANT, Y.A.
- GARRIGOUX, T.
- GIAVITTO, G.
- GIEBELS, B.
- GLICENSTEIN, J.F.
- GOTTSCHALL, D.
- GOYAL, A.
- GRONDIN, M.-H.
- HADASCH, D.
- HAHN, J.
- HAUPT, M.
- HAWKES, J.
- HEINZELMANN, G.
- HENRI, G.
- HERMANN, G.
- HERVET, O.
- HINTON, J.A.
- HOFMANN, W.
- HOISCHEN, C.
- HOLLER, M.
- HORNS, D.
- IVASCENKO, A.
- JACHOLKOWSKA, A.
- JAMROZY, M.
- JANIAK, M.
- JANKOWSKY, D.
- JANKOWSKY, F.
- JINGO, M.
- JOGLER, T.
- JOUVIN, L.
- JUNG-RICHARDT, I.
- KASTENDIECK, M.A.
- KATARZYŃSKI, K.
- KATZ, U.
- KERSZBERG, D.
- KHÉLIFI, B.
- KIEFFER, M.
- KING, J.
- KLEPSER, S.
- KLOCHKOV, D.
- KLUŹNIAK, W.
- KOLITZUS, D.
- KOMIN, Nu.
- KOSACK, K.
- KRAKAU, S.
- KRAUS, M.
- KRAYZEL, F.
- KRÜGER, P.P.
- LAFFON, H.
- LAMANNA, G.
- LAU, J.
- LEES, J.-P.
- LEFAUCHEUR, J.
- LEFRANC, V.
- LEMIÈRE, A.
- LEMOINE-GOUMARD, M.
- LENAIN, J.-P.
- LESER, E.
- LOHSE, T.
- LORENTZ, M.
- LIU, R.
- LÓPEZ-COTO, R.
- LYPOVA, I.
- MARANDON, V.
- MARCOWITH, Alexandre
- MARIAUD, C.
- MARX, R.
- MAURIN, G.
- MAXTED, N.
- MAYER, M.
- MEINTJES, P.J.
- MEYER, M.
- MITCHELL, A.M.W.
- MODERSKI, R.
- MOHAMED, M.
- MOHRMANN, L.
- MOULIN, E.
- MURACH, T.
- DE NAUROIS, M.
- NIEDERWANGER, F.
- NIEMIEC, J.
- OAKES, L.
- O'BRIEN, P.
- ODAKA, H.
- ÖTTL, S.
- OHM, S.
- OSTROWSKI, M.
- OYA, I.
- PADOVANI, M.
- PANTER, M.
- PARSONS, R.D.
- PEKEUR, N.W.
- PELLETIER, G.
- PERENNES, C.
- PETRUCCI, P.-O.
- PEYAUD, B.
- PIEL, Q.
- PITA, S.
- POON, H.
- PROKHOROV, D.
- PROKOPH, H.
- PÜHLHOFER, G.
- PUNCH, M.
- QUIRRENBACH, A.
- RAAB, S.
- REIMER, A.
- REIMER, O.
- RENAUD, Matthieu
- DE LOS REYES, R.
- RIEGER, F.
- ROMOLI, C.
- ROSIER-LEES, S.
- ROWELL, G.
- RUDAK, B.
- RULTEN, C.B.
- SAHAKIAN, V.
- SALEK, D.
- SANCHEZ, D.A.
- SANTANGELO, A.
- SASAKI, M.
- SCHLICKEISER, R.
- SCHÜSSLER, F.
- SCHULZ, A.
- SCHWANKE, U.
- SCHWEMMER, S.
- SETTIMO, M.
- SEYFFERT, A.S.
- SHAFI, N.
- SHILON, I.
- SIMONI, R.
- SOL, H.
- SPANIER, F.
- SPENGLER, G.
- SPIES, F.
- STEENKAMP, R.
- STEGMANN, C.
- SUSHCH, I.
- TAVERNET, J.-P.
- TAVERNIER, T.
- TAYLOR, A.M.
- TERRIER, R.
- TIBALDO, L.
- TIZIANI, D.
- TLUCZYKONT, M.
- TRICHARD, C.
- TUFFS, R.
- UCHIYAMA, Y.
- VAN DER WALT, D.J.
- VAN ELDIK, C.
- VAN RENSBURG, C.
- VAN SOELEN, B.
- VASILEIADIS, George
- VEH, J.
- VENTER, C.
- VIANA, A.
- VINCENT, P.
- VINK, J.
- VOISIN, F.
- VÖLK, H.J.
- VUILLAUME, T.
- WADIASINGH, Z.
- WAGNER, S.J.
- WAGNER, P.
- WAGNER, R.M.
- WHITE, R.
- WIERZCHOLSKA, A.
- WILLMANN, P.
- WÖRNLEIN, A.
- WOUTERS, D.
- YANG, R.
- ZABALZA, V.
- ZABOROV, D.
- ZACHARIAS, M.
- ZDZIARSKI, A.A.
- ZECH, A.
- ZEFI, F.
- ZIEGLER, A.
- ZYWUCKA, N.
- JANKOWSKI, F.
- KEANE, E.F.
- PETROFF, E.
DOIAbstract
Very high-energy γ rays (VHE, E ≳ 100 GeV) propagating over cosmological distances can interact with the low-energy photons of the extragalactic background light (EBL) and produce electron-positron pairs. The transparency of the Universe to VHE γ rays is then directly related to the spectral energy distribution (SED) of the EBL. The observation of features in the VHE energy spectra of extragalactic sources allows the EBL to be measured, which otherwise is very difficult. An EBL model-independent measurement of the EBL SED with the H.E.S.S. array of Cherenkov telescopes is presented. It was obtained by extracting the EBL absorption signal from the reanalysis of high-quality spectra of blazars. From H.E.S.S. data alone the EBL signature is de...
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