2016A&A...591A..10A

Query : 2016A&A...591A..10A

2016A&A...591A..10A - Astronomy and Astrophysics, volume 591A10-10 (2016/7-1)

Insights into the emission of the blazar 1ES 1011+496 through unprecedented broadband observations during 2011 and 2012.

ALEKSIC J., ANSOLDI S., ANTONELLI L.A., ANTORANZ P., ARCARO C., BABIC A., BANGALE P., BARRES DE ALMEIDA U., BARRIO J.A., BECERRA GONZALEZ J., BEDNAREK W., BERNARDINI E., BIASUZZI B., BILAND A., BLANCH O., BONNEFOY S., BONNOLI G., BORRACCI F., BRETZ T., CARMONA E., CAROSI A., COLIN P., COLOMBO E., CONTRERAS J.L., CORTINA J., COVINO S., DA VELA P., DAZZI F., DE ANGELIS A., DE CANEVA G., DE LOTTO B., DE ONA WILHELMI E., DELGADO MENDEZ C., DI PIERRO F., DOMINIS PRESTER D., DORNER D., DORO M., EINECKE S., EISENACHER D., ELSAESSER D., FERNANDEZ-BARRAL A., FIDALGO D., FONSECA M.V., FONT L., FRANTZEN K., FRUCK C., GALINDO D., GARCIA LOPEZ R.J., GARCZARCZYK M., GARRIDO TERRATS D., GAUG M., GODINOVIC N., GONZALEZ MUNOZ A., GOZZINI S.R., HADASCH D., HANABATA Y., HAYASHIDA M., HERRERA J., HOSE J., HRUPEC D., IDEC W., KADENIUS V., KELLERMANN H., KNOETIG M.L., KODANI K., KONNO Y., KRAUSE J., KUBO H., KUSHIDA J., LA BARBERA A., LELAS D., LEWANDOWSKA N., LINDFORS E., LOMBARDI S., LONGO F., LOPEZ M., LOPEZ-COTO R., LOPEZ-ORAMAS A., LORENZ E., LOZANO I., MAKARIEV M., MALLOT K., MANEVA G., MANNHEIM K., MARASCHI L., MARCOTE B., MARIOTTI M., MARTINEZ M., MAZIN D., MENZEL U., MIRANDA J.M., MIRZOYAN R., MORALEJO A., MUNAR-ADROVER P., NAKAJIMA D., NEUSTROEV V., NIEDZWIECKI A., NIEVAS ROSILLO M., NILSSON K., NISHIJIMA K., NODA K., ORITO R., OVERKEMPING A., PAIANO S., PALATIELLO M., PANEQUE D., PAOLETTI R., PAREDES J.M., PAREDES-FORTUNY X., PERSIC M., POUTANEN J., PRADA MORONI P.G., PRANDINI E., PULJAK I., REINTHAL R., RHODE W., RIBO M., RICO J., RODRIGUEZ GARCIA J., SAITO T., SAITO K., SATALECKA K., SCALZOTTO V., SCAPIN V., SCHWEIZER T., SHORE S.N., SILLANPAA A., SITAREK J., SNIDARIC I., SOBCZYNSKA D., STAMERRA A., STEINBRING T., STRZYS M., TAKALO L., TAKAMI H., TAVECCHIO F., TEMNIKOV P., TERZIC T., TESCARO D., TESHIMA M., THAELE J., TORRES D.F., TOYAMA T., TREVES A., VOGLER P., WILL M., ZANIN R., BUSON S., D'AMMANDO F., LAHTEENMAKI A., HOVATTA T., KOVALEV Y.Y., LISTER M.L., MAX-MOERBECK W., MUNDELL C., PUSHKAREV A.B., RASTORGUEVA-FOI E., READHEAD A.C.S., RICHARDS J.L., TAMMI J., SANCHEZ D.A., TORNIKOSKI M., SAVOLAINEN T. and STEELE I.

Abstract (from CDS):

Context. 1ES 1011+496 (z=0.212) was discovered in very high-energy (VHE, E>100GeV) γ rays with MAGIC in 2007. The absence of simultaneous data at lower energies led to an incomplete characterization of the broadband spectral energy distribution (SED).
Aims. We study the source properties and the emission mechanisms, probing whether a simple one-zone synchrotron self-Compton (SSC) scenario is able to explain the observed broadband spectrum.
Methods. We analyzed data in the range from VHE to radio data from 2011 and 2012 collected by MAGIC, Fermi-LAT, Swift, KVA, OVRO, and Metsahovi in addition to optical polarimetry data and radio maps from the Liverpool Telescope and MOJAVE.
Results. The VHE spectrum was fit with a simple power law with a photon index of 3.69±0.22 and a flux above 150GeV of (1.46±0.16)x10–11ph/cm2/s. The source 1ES 1011+496 was found to be in a generally quiescent state at all observed wavelengths, showing only moderate variability from radio to X-rays. A low degree of polarization of less than 10% was measured in optical, while some bright features polarized up to 60% were observed in the radio jet. A similar trend in the rotation of the electric vector position angle was found in optical and radio. The radio maps indicated a superluminal motion of 1.8±0.4c, which is the highest speed statistically significant measured so far in a high-frequency-peaked BL Lac.
Conclusions. For the first time, the high-energy bump in the broadband SED of 1ES 1011+496 could be fully characterized from 0.1GeV to 1TeV, which permitted a more reliable interpretation within the one-zone SSC scenario. The polarimetry data suggest that at least part of the optical emission has its origin in some of the bright radio features, while the low polarization in optical might be due to the contribution of parts of the radio jet with different orientations of the magnetic field with respect to the optical emission.

Abstract Copyright: © ESO, 2016

Journal keyword(s): BL Lacertae objects: individual 1ES 1011+496 - galaxies: active - galaxies: jets - radiation mechanisms: non-thermal - gamma rays: galaxies

Simbad objects: 9

goto Full paper

goto View the references in ADS

Number of rows : 9
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NGC 1275 Bla 03 19 48.1599902040 +41 30 42.108850836   13.10 12.48 11.09   ~ 4243 3
2 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
3 RX J1015.0+4926 BLL 10 15 04.1396533776 +49 26 00.706055496   16.56 16.15 14.58   ~ 400 3
4 M 87 AGN 12 30 49.42338414 +12 23 28.0436859 10.16 9.59 8.63   7.49 ~ 7815 3
5 3C 286 Sy1 13 31 08.2883506368 +30 30 32.960091564   17.51 17.25     ~ 4558 2
6 RX J1428.5+4240 BLL 14 28 32.6090008440 +42 40 21.048123396   16.95 16.45 14.4   ~ 549 1
7 DR 21 SFR 20 39 01.6 +42 19 38           O4.5 1121 0
8 NGC 7027 PN 21 07 01.571952 +42 14 10.47120   10.358 8.831 10.157   ~ 2541 1
9 NAME BL Lac BLL 22 02 43.2913536816 +42 16 39.979416792   15.66 14.72     ~ 2397 1

To bookmark this query, right click on this link: simbad:objects in 2016A&A...591A..10A and select 'bookmark this link' or equivalent in the popup menu