SIMBAD references

2006ApJ...642L.119A - Astrophys. J., 642, L119-L122 (2006/May-2)

Discovery of very high energy gamma rays from 1ES 1218+30.4.

ALBERT J., ALIU E., ANDERHUB H., ANTORANZ P., ARMADA A., ASENSIO M., BAIXERAS C., BARRIO J.A., BARTELT M., BARTKO H., BASTIERI D., BAVIKADI S.R., BEDNAREK W., BERGER K., BIGONGIARI C., BILAND A., BISESI E., BOCK R.K., BRETZ T., BRITVITCH I., CAMARA M., CHILINGARIAN A., CIPRINI S., COARASA J.A., COMMICHAU S., CONTRERAS J.L., CORTINA J., CURTEF V., DANIELYAN V., DAZZI F., DE ANGELIS A., DE LOS REYES R., DE LOTTO B., DOMINGO-SANTAMARIA E., DORNER D., DORO M., ERRANDO M., FAGIOLINI M., FERENC D., FERNANDEZ E., FIRPO R., FLIX J., FONSECA M.V., FONT L., GALANTE N., GARCZARCZYK M., GAUG M., GILLER M., GOEBEL F., HAKOBYAN D., HAYASHIDA M., HENGSTEBECK T., HOHNE D., HOSE J., JACON P., KALEKIN O., KRANICH D., LAILLE A., LENISA T., LIEBING P., LINDFORS E., LONGO F., LOPEZ J., LOPEZ M., LORENZ E., LUCARELLI F., MAJUMDAR P., MANEVA G., MANNHEIM K., MARIOTTI M., MARTINEZ M., MASE K., MAZIN D., MEUCCI M., MEYER M., MIRANDA J.M., MIRZOYAN R., MIZOBUCHI S., MORALEJO A., NILSSON K., ONA-WILHELMI E., ORDUNA R., OTTE N., OYA I., PANEQUE D., PAOLETTI R., PASANEN M., PASCOLI D., PAUSS F., PAVEL N., PEGNA R., PERSIC M., PERUZZO L., PICCIOLI A., POLLER M., PRANDINI E., RHODE W., RICO J., RIEGEL B., RISSI M., ROBERT A., RUGAMER S., SAGGION A., SANCHEZ A., SARTORI P., SCALZOTTO V., SCHMITT R., SCHWEIZER T., SHAYDUK M., SHINOZAKI K., SHORE S.N., SIDRO N., SILLANPAA A., SOBCZYNSKA D., STAMERRA A., STARK L.S., TAKALO L., TEMNIKOV P., TESCARO D., TESHIMA M., TONELLO N., TORRES A., TORRES D.F., TURINI N., VANKOV H., VARDANYAN A., VITALE V., WAGNER R.M., WIBIG T., WITTEK W. and ZAPATERO J.

Abstract (from CDS):

The MAGIC collaboration has studied the high-frequency-peaked BL Lac object 1ES 1218+30.4, at a redshift z=0.182, using the MAGIC imaging air Cerenkov telescope located on the Canary Island of La Palma. A gamma-ray signal was observed with 6.4 σ significance. The differential energy spectrum for an energy threshold of 120 GeV can be fitted by a simple power law, yielding FE(E)=(8.1±2.1)x10–7[E/(250 GeV)]–3.0±0.4 TeV–1/m2/s. During the 6 days of observation in 2005 January, no time variability on timescales of days was found within the statistical errors. The observed integral flux above 350 GeV is nearly a factor of 2 below the upper limit reported by the Whipple collaboration in 2003.

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Journal keyword(s): BL Lacertae objects: individual (1ES 1218+30.4) - Gamma Rays: Observations

Simbad objects: 7

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