RT Journal Article
T1 Simultaneous multiwavelength observations of the blazar 1ES 1959+650 at a low TeV flux
A1 Antoranz Canales, Pedro
A1 Barrio Uña, Juan Abel
A1 Contreras González, José Luis
A1 Fonseca González, María Victoria
A1 López Moya, Marcos
A1 Miranda Pantoja, José Miguel
A1 Nieto Castaño, Daniel
AB We present the results from a multiwavelength campaign on the TeV blazar 1ES 1959+650, performed in 2006 May. Data from the optical, UV, soft- and hard-X-ray, and very high energy (VHE) gamma-ray ( E > 100 GeV) bands were obtained with the Suzaku and Swift satellites, the MAGIC telescope, and other ground-based facilities. The source spectral energy distribution (SED), derived from Suzaku and MAGIC observations at the end of 2006 May, shows the usual double hump shape, with the synchrotron peak at a higher flux level than the Compton peak. With respect to historical values, during our campaign the source exhibited a relatively high state in X-rays and optical, while in the VHE band it was at one of the lowest level so far recorded. We also monitored the source for flux spectral variability on a time window of 10 days in the optical-UVand X-ray bands and 7 days in the VHE band. The source varies more in the X-ray than in the optical band, with the 2-10 keV X-ray flux varying by a factor of similar to 2. The synchrotron peak is located in the X-ray band and moves to higher energies as the source gets brighter, with the X-ray fluxes above it varying more rapidly than the X-ray fluxes at lower energies. The variability behavior observed in the X-ray band cannot be produced by emitting regions varying independently and suggests instead some sort of "standing shock'' scenario. The overall SED is well represented by a homogeneous one-zone synchrotron inverse Compton emission model, from which we derive physical parameters that are typical of high-energy peaked blazars.
PB IOP Publishing
SN 0004-637X
YR 2008
FD 2008-06-01
LK https://hdl.handle.net/20.500.14352/50833
UL https://hdl.handle.net/20.500.14352/50833
LA eng
NO © The American Astronomical Society. We thank Neil Gehrels and the whole Swift team for the ToO observations and the Suzaku team for their assistance in the analysis of our Suzaku data.We thank the IAC for the excellent workingconditions at the ORM. We acknowledge financial supportfrom the ASI-INAF contract I /088/06/0. TheMAGIC project issupported by the German BMBF and MPG, the Italian INFN, the Spanish CICYT, the Swiss ETH Research Grant TH34/04, and the Polish MNiI Grant 1P03D01028.
NO ASI-INAF
NO German BMBF
NO German MPG
NO Italian INFN
NO Spanish CICYT
NO Swiss ETH
NO Polish MNiI
DS Docta Complutense
RD 7 jun 2025