TY - GEN
T1 - MAGIC and multi-wavelength observations of the radio galaxy NGC 1275
AU - FOR THE MAGIC COLLABORATION
AU - Colin, Pierre
AU - Eisenacher, Dorit
AU - Hildebrand, Dorothée
AU - Lindfors, Elina
AU - Lombardi, Saverio
AU - Nilsson, Kari
AU - Partini, Serena
AU - Tavecchio, Fabrizio
AU - Zandanel, Fabio
AU - Balmaverde, Barabara
AU - Kataoka, Jun
AU - Rekola, Rami
AU - Takahashi, Yosuke
N1 - Funding Information:
The Fermi-LAT Collaboration acknowledges ongoing support from a number of agencies and institutes including the NASA and the Department of Energy in the United States, the CEA and CNRS/IN2P3 in France, the ASI and INFN in Italy, the MEXT, KEK and JAXA in Japan, and the K. A. Wallenberg Foundation, the SRC and the SNSB in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the INA in Italy and the CNES in France.
Funding Information:
The MAGIC collaboration thanks the IAC for the excellent working conditions at the Observatorio del Roque de los Muchachos. The support of the German BMBF and MPG, the Italian INFN, the Swiss SNF, and the Spanish MICINN is acknowledged. This work was also supported by the CPAN and MultiDark projects of the Spanish Consolider-Ingenio, by grants of the Bulgarian NSF, the Academy of Finland, the DFG Cluster of Excellence, the D-FG Collaborative Research Centers and the Polish MNiSzW.
Publisher Copyright:
© 2013 Sociedade Brasileira de Fisica. All Rights Reserved.
PY - 2013
Y1 - 2013
N2 - The massive radio galaxy NGC 1275 at the center of the Perseus cluster is regularly observed with the MAGIC telescopes since 2009. The observation campaign (in stereoscopic mode) between August 2010 and February 2011 leads to the first detection of the source in very high energy (VHE, >100 GeV) γ rays. NGC 1275 is one of the few non-Blazar AGNs detected in this domain which is highly dominated by BL Lac objects. The proximity and the relatively large angle between the jet axis and the line of sight allow to resolve inner-jet structures with radio interferometry and to test non-thermal emission model for larger viewing angles. NGC 1275 is then a good laboratory to locate the γ -ray emission region and understand acceleration process at work in AGNs. Here we present the long term monitoring of NGC 1275 with MAGIC as well as with Fermi-LAT (in GeV band), KVA (optical) and VLBA (15 GHz). The multiwavelength lightcurves show a correlation between γ - ray, optical and a radio component of the inner-jet. We reconstructed the broad band spectral energy distributions (SED) of the source during two separated MAGIC campaigns which both lead to the detection of NGC 1275 in VHE. We applied a one-zone Synchrotron Self Compton model with a small Doppler factor (2) which can fit the SEDs and reproduces the optical/gamma correlation. Finally, we will discuss the validity of this simple model and the implication of our results for the AGN physics.
AB - The massive radio galaxy NGC 1275 at the center of the Perseus cluster is regularly observed with the MAGIC telescopes since 2009. The observation campaign (in stereoscopic mode) between August 2010 and February 2011 leads to the first detection of the source in very high energy (VHE, >100 GeV) γ rays. NGC 1275 is one of the few non-Blazar AGNs detected in this domain which is highly dominated by BL Lac objects. The proximity and the relatively large angle between the jet axis and the line of sight allow to resolve inner-jet structures with radio interferometry and to test non-thermal emission model for larger viewing angles. NGC 1275 is then a good laboratory to locate the γ -ray emission region and understand acceleration process at work in AGNs. Here we present the long term monitoring of NGC 1275 with MAGIC as well as with Fermi-LAT (in GeV band), KVA (optical) and VLBA (15 GHz). The multiwavelength lightcurves show a correlation between γ - ray, optical and a radio component of the inner-jet. We reconstructed the broad band spectral energy distributions (SED) of the source during two separated MAGIC campaigns which both lead to the detection of NGC 1275 in VHE. We applied a one-zone Synchrotron Self Compton model with a small Doppler factor (2) which can fit the SEDs and reproduces the optical/gamma correlation. Finally, we will discuss the validity of this simple model and the implication of our results for the AGN physics.
KW - AGN
KW - Fermi-LAT
KW - KVA
KW - MAGIC
KW - NGC 1275
KW - Radio galaxy
KW - Γ ray astronomy
UR - http://www.scopus.com/inward/record.url?scp=85052378265&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85052378265&partnerID=8YFLogxK
M3 - Conference contribution
AN - SCOPUS:85052378265
T3 - Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013
BT - Proceedings of the 33rd International Cosmic Rays Conference, ICRC 2013
PB - Sociedade Brasileira de Fisica
T2 - 33rd International Cosmic Rays Conference, ICRC 2013
Y2 - 2 July 2013 through 9 July 2013
ER -