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

C.D.S. - SIMBAD4 rel 1.7 - 2020.11.30CET22:25:22

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

Full paper

View the reference in ADS

Number of rows : 11

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag U	Mag B	Mag V	Mag R	Sp type	#ref 1850 - 2021	#notes
1	ICRF J052145.9+211251	BLL	05 21 45.9656490719	+21 12 51.454716382					~	84	1
2	8C 0716+714	BLL	07 21 53.4484901266	+71 20 36.362058601		15.5	14.17	14.27	~	1141	1
3	QSO J0854+2006	BLL	08 54 48.8749311881	+20 06 30.642936668		15.91	15.43	15.56	~	2030	1
4	Mrk 421	BLL	11 04 27.3139210166	+38 12 31.798324828		13.50	12.90	8.31	~	2410	1
5	7C 1424+2401	BLL	14 27 00.3918388878	+23 48 00.035406946	14.52	14.34	14.95	14.5	~	293	1
6	4C 39.49	BLL	16 53 52.21668494	+39 45 36.6089458	14.09	14.15	13.29	8.26	~	1938	2
7	6C 172704+501607	BLL	17 28 18.6239898055	+50 13 10.472390025		16.55	15.97	12.95	~	324	1
8	4C 09.57	BLL	17 51 32.81857318	+09 39 00.7284829		17.46	16.78	15.57	~	820	1
9	QSO B1959+650	BLL	19 59 59.8525497024	+65 08 54.651170114			12.8	11.21	~	510	2
10	NAME BL Lac	BLL	22 02 43.2913773726	+42 16 39.978417860		15.66	14.72		~	2026	1
11	QSO B2344+514	BLL	23 47 04.8376303689	+51 42 17.875387216			15.50	10.7	~	394	0

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