CDS

2020A&A...640A.132M

Query : 2020A&A...640A.132M

2020A&A...640A.132M - Astronomy and Astrophysics, volume 640A, 132-132 (2020/8-1)

Testing two-component models on very high-energy gamma-ray-emitting BL Lac objects.

MAGIC COLLABORATION, ACCIARI V.A., ANSOLDI S., ANTONELLI L.A., ARBET ENGELS A., BAACK D., BABIC A., BANERJEE B., BARRES DE ALMEIDA U., BARRIO J.A., BECERRA GONZALEZ J., BEDNAREK W., BELLIZZI L., BERNARDINI E., BERTI A., BESENRIEDER J., BHATTACHARYYA W., BIGONGIARI C., BILAND A., BLANCH O., BONNOLI G., BOSNJAK Z., BUSETTO G., CAROSI R., CERIBELLA G., CERRUTI M., CHAI Y., CHILINGARIAN A., CIKOTA S., COLAK S.M., COLIN U., COLOMBO E., CONTRERAS J.L., CORTINA J., COVINO S., D'AMICO G., D'ELIA V., DA VELA P., DAZZI F., DE ANGELIS A., DE LOTTO B., DELFINO M., DELGADO J., DEPAOLI D., DI PIERRO F., DI VENERE L., DO SOUTO ESPINEIRA E., DOMINIS PRESTER D., DONINI A., DORNER D., DORO M., ELSAESSER D., FALLAH RAMAZANI V., FATTORINI A., FERRARA G., FOFFANO L., FONSECA M.V., FONT L., FRUCK C., FUKAMI S., GARCIA LOPEZ R.J., GARCZARCZYK M., GASPARYAN S., GAUG M., GIGLIETTO N., GIORDANO F., GLIWNY P., GODINOVIC N., GREEN D., HADASCH D., HAHN A., HERRERA J., HOANG J., HRUPEC D., HUTTEN M., INADA T., INOUE S., ISHIO K., IWAMURA Y., JOUVIN L., KAJIWARA Y., KARJALAINEN M., KERSZBERG D., KOBAYASHI Y., KUBO H., KUSHIDA J., LAMASTRA A., LELAS D., LEONE F., LINDFORS E., LOMBARDI S., LONGO F., LOPEZ M., LOPEZ-COTO R., LOPEZ-ORAMAS A., LOPORCHIO S., MACHADO DE OLIVEIRA FRAGA B., MAGGIO C., MAJUMDAR P., MAKARIEV M., MALLAMACI M., MANEVA G., MANGANARO M., MANNHEIM K., MARASCHI L., MARIOTTI M., MARTINEZ M., MAZIN D., MENDER S., MICANOVIC S., MICELI D., MIENER T., MINEV M., MIRANDA J.M., MIRZOYAN R., MOLINA E., MORALEJO A., MORCUENDE D., MORENO V., MORETTI E., MUNAR-ADROVER P., NEUSTROEV V., NIGRO C., NILSSON K., NINCI D., NISHIJIMA K., NODA K., NOGUES L., NOZAKI S., OHTANI Y., OKA T., OTERO-SANTOS J., PALATIELLO M., PANEQUE D., PAOLETTI R., PAREDES J.M., PAVLETIC L., PENIL P., PERESANO M., PERSIC M., PRADA MORONI P.G., PRANDINI E., PULJAK I., RHODE W., RIBO M., RICO J., RIGHI C., RUGLIANCICH A., SAHA L., SAHAKYAN N., SAITO T., SAKURAI S., SATALECKA K., SCHLEICHER B., SCHMIDT K., SCHWEIZER T., SITAREK J., SNIDARIC I., SOBCZYNSKA D., SPOLON A., STAMERRA A., STROM D., STRZYS M., SUDA Y., SURIC T., TAKAHASHI M., TAVECCHIO F., TEMNIKOV P., TERZIC T., TESHIMA M., TORRES-ALBA N., TOSTI L., VAN SCHERPENBERG J., VANZO G., VAZQUEZ ACOSTA M., VENTURA S., VERGUILOV V., VIGORITO C.F., VITALE V., VOVK I., WILL M., ZARIC D., NIEVAS-ROSILLO M., ARCARO C., D'AMMANDO F., DE PALMA F., HODGES M., HOVATTA T., KIEHLMANN S., MAX-MOERBECK W., READHEAD A.C.S., REEVES R., TAKALO L., REINTHAL R., JORMANAINEN J., WIERDA F., WAGNER S.M., BERDYUGIN A., NABIZADEH A., TALEBPOUR SHESHVAN N., OKSANEN A., BACHEV R., STRIGACHEV A. and KEHUSMAA P.

Abstract (from CDS):


Context. It has become evident that one-zone synchrotron self-Compton models are not always adequate for very high-energy (VHE) gamma-ray-emitting blazars. While two-component models perform better, they are difficult to constrain due to the large number of free parameters.
Aims. In this work, we make a first attempt at taking into account the observational constraints from very long baseline interferometry (VLBI) data, long-term light curves (radio, optical, and X-rays), and optical polarisation to limit the parameter space for a two-component model and test whether or not it can still reproduce the observed spectral energy distribution (SED) of the blazars.
Methods. We selected five TeV BL Lac objects based on the availability of VHE gamma-ray and optical polarisation data. We collected constraints for the jet parameters from VLBI observations. We evaluated the contributions of the two components to the optical flux by means of decomposition of long-term radio and optical light curves as well as modelling of the optical polarisation variability of the objects. We selected eight epochs for these five objects based on the variability observed at VHE gamma rays, for which we constructed the SEDs that we then modelled with a two-component model.
Results. We found parameter sets which can reproduce the broadband SED of the sources in the framework of two-component models considering all available observational constraints from VLBI observations. Moreover, the constraints obtained from the long-term behaviour of the sources in the lower energy bands could be used to determine the region where the emission in each band originates. Finally, we attempt to use optical polarisation data to shed new light on the behaviour of the two components in the optical band. Our observationally constrained two-component model allows explanation of the entire SED from radio to VHE with two co-located emission regions.

Abstract Copyright: © ESO 2020

Journal keyword(s): galaxies: active - galaxies: jets - BL Lacertae objects: general - astronomical databases: miscellaneous - radiation mechanisms: non-thermal - gamma rays: galaxies

VizieR on-line data: <Available at CDS (J/A+A/640/A132): table1.dat tablea1.dat tablea2.dat>

Simbad objects: 11

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Number of rows : 11
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022 		#notes
1 ICRF J052145.9+211251 BLL 05 21 45.9657388992 +21 12 51.452786736           ~ 109 1
2 8C 0716+714 BLL 07 21 53.4482942664 +71 20 36.363846516   15.5 14.17 14.27   ~ 1219 1
3 QSO J0854+2006 BLL 08 54 48.8749846272 +20 06 30.639583620   15.91 15.43 15.56   ~ 2182 1
4 Mrk 421 BLL 11 04 27.3140835504 +38 12 31.798495872   13.50 12.90 8.31   ~ 2534 1
5 7C 1424+2401 BLL 14 27 00.3917926224 +23 48 00.037510776 14.52 14.34 14.95 14.5   ~ 319 1
6 4C 39.49 BLL 16 53 52.2160772976 +39 45 36.613228860 14.09 14.15 13.29 8.26   ~ 2034 2
7 6C 172704+501607 BLL 17 28 18.6242294352 +50 13 10.469553996   16.55 15.97 12.95   ~ 344 1
8 4C 09.57 BLL 17 51 32.8186120872 +09 39 00.728629416   17.46 16.78 15.57   ~ 884 1
9 QSO B1959+650 BLL 19 59 59.8520303688 +65 08 54.652536492     12.8 11.21   ~ 556 2
10 NAME BL Lac BLL 22 02 43.2913536816 +42 16 39.979416792   15.66 14.72     ~ 2137 1
11 QSO B2344+514 BLL 23 47 04.8372110928 +51 42 17.877513168     15.50 10.7   ~ 414 0

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2022.08.15-15:35:49

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