2024MNRAS.529.3894M

Query : 2024MNRAS.529.3894M

2024MNRAS.529.3894M - Mon. Not. R. Astron. Soc., 529, 3894-3911 (2024/April-3)

The variability patterns of the TeV blazar PG 1553 + 113 from a decade of MAGIC and multiband observations.

MAGIC COLLABORATION, ABE H., ABE S., ABHIR J., ACCIARI V.A., AGUDO I., ANIELLO T., ANSOLDI S., ANTONELLI L.A., ARBET ENGELS A., ARCARO C., ARTERO M., ASANO K., BAACK D., BABIC A., BAQUERO A., BARRES DE ALMEIDA U., BATKOVIC I., BAXTER J., BECERRA GONZALEZ J., BERNARDINI E., BERNETE J., BERTI A., BESENRIEDER J., BIGONGIARI C., BILAND A., BLANCH O., BONNOLI G., BOSNJAK Z., BURELLI I., BUSETTO G., CAMPOY-ORDAZ A., CAROSI A., CAROSI R., CARRETERO-CASTRILLO M., CASTRO-TIRADO A.J., CHAI Y., CIFUENTES A., CIKOTA S., 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., DEL POPOLO A., DELFINO M., DELGADO J., DELGADO MENDEZ C., DEPAOLI D., DI PIERRO F., DI VENERE L., DOMINIS PRESTER D., DONINI A., DORNER D., DORO M., ELSAESSER D., EMERY G., ESCUDERO J., FARINA L., FATTORINI A., FOFFANO L., FONT L., FUKAMI S., FUKAZAWA Y., GARCIA LOPEZ R.J., GASPARYAN S., GAUG M., GIESBRECHT PAIVA J.G., GIGLIETTO N., GIORDANO F., GLIWNY P., GRAU R., GREEN J.G., HADASCH D., HAHN A., HECKMANN L., HERRERA J., HOVATTA T., HRUPEC D., HUTTEN M., IMAZAWA R., INADA T., IOTOV R., ISHIO K., JIMENEZ MARTINEZ I., JORMANAINEN J., KERSZBERG D., KLUGE G.W., KOBAYASHI Y., KOUCH P.M., KUBO H., KUSHIDA J., LAINEZ LEZAUN M., LAMASTRA A., LEONE F., LINDFORS E., LIODAKIS I., LOMBARDI S., LONGO F., LOPEZ-MOYA M., LOPEZ-ORAMAS A., LOPORCHIO S., LORINI A., MACHADO DE OLIVEIRA FRAGA B., MAJUMDAR P., MAKARIEV M., MANEVA G., MANG N., MANGANARO M., MANNHEIM K., MARIOTTI M., MARTINEZ M., MARTINEZ-CHICHARRO M., MAS-AGUILAR A., MAZIN D., MENCHIARI S., MENDER S., MICELI D., MIENER T., MIRANDA J.M., MIRZOYAN R., MOLERO GONZALEZ M., MOLINA E., MONDAL H.A., MORALEJO A., MORCUENDE D., NAKAMORI T., NANCI C., NEUSTROEV V., NIGRO C., NIKOLIC L., NILSSON K., NISHIJIMA K., NJOH EKOUME T., NODA K., NOZAKI S., OHTANI Y., OKUMURA A., OTERO-SANTOS J., PAIANO S., PALATIELLO M., PANEQUE D., PAOLETTI R., PAREDES J.M., PAVLOVIC D., PERSIC M., PIHET M., PIROLA G., PODOBNIK F., PRADA MORONI P.G., PRANDINI E., PRINCIPE G., PRIYADARSHI C., RHODE W., RIBO M., RICO J., RIGHI C., SAHAKYAN N., SAITO T., SATALECKA K., SATURNI F.G., SCHLEICHER B., SCHMIDT K., SCHMUCKERMAIER F., SCHUBERT J.L., SCHWEIZER T., SCIACCALUGA A., SITAREK J., SPOLON A., STAMERRA A., STRISKOVIC J., STROM D., SUDA Y., SUUTARINEN S., TAJIMA H., TAKEISHI R., TAVECCHIO F., TEMNIKOV P., TERAUCHI K., TERZIC T., TESHIMA M., TOSTI L., TRUZZI S., TUTONE A., UBACH S., VAN SCHERPENBERG J., VENTURA S., VERGUILOV V., VIALE I., VIGORITO C.F., VITALE V., WALTER R., WUNDERLICH C., YAMAMOTO T. (The MWL Collaborators), JERMAK H., STEELE I.A., SMITH P.S., BLINOV D., RAITERI C.M., VILLATA M., MIRZAQULOV D.O., KURTANIDZE S.O., CAROSATI D., SAVCHENKO S.S., ACOSTA-PULIDO J.A., BORMAN G.A., BOZHILOV V., CARNERERO M.I., CHIGLADZE R.A., DAMLJANOVIC G., EHGAMBERDIEV S.A., FEIGE M., GRISHINA T.S., GUPTA A.C., HAGEN-THORN V.A., IBRYAMOV S., IVANIDZE R.Z., JORSTAD S.G., KANIA J., KIMERIDZE G.N., KOPATSKAYA E.N., KOPP M., KUNKEL L., KURTANIDZE O.M., LARIONOV V.M., LARIONOVA E.G., LARIONOVA L.V., LOREY C., MARCHINI A., MARSCHER A.P., MINEV M., MOROZOVA D.A., NIKOLASHVILI M.G., OVCHAROV E., REINHART D., SADUN A.C., SCHERBANTIN A., SCHNEIDER L., SEMKOV E., SIGUA L.A., STEINEKE R., TROITSKAYA Y.V., TROITSKIY I.S., VALCHEVA A., VASILYEV A.A., VINCE O., ZAHARIEVA E., ZOTTMANN N., KIEHLMANN S., READHEAD A., MAX-MOERBECK W., REEVES R.A., SANDRINELLI A., FALLAH RAMAZANI V., GIROLETTI M., RIGHINI S., MARCHILI N., PATRICELLI B., GHIRLANDA G. and LICO R.

Abstract (from CDS):

PG 1553 + 113 is one of the few blazars with a convincing quasi-periodic emission in the gamma-ray band. The source is also a very high energy (VHE; >100 GeV) gamma-ray emitter. To better understand its properties and identify the underlying physical processes driving its variability, the MAGIC Collaboration initiated a multiyear, multiwavelength monitoring campaign in 2015 involving the OVRO 40-m and Medicina radio telescopes, REM, KVA, and the MAGIC telescopes, Swift and Fermi satellites, and the WEBT network. The analysis presented in this paper uses data until 2017 and focuses on the characterization of the variability. The gamma-ray data show a (hint of a) periodic signal compatible with literature, but the X-ray and VHE gamma-ray data do not show statistical evidence for a periodic signal. In other bands, the data are compatible with the gamma-ray period, but with a relatively high p-value. The complex connection between the low- and high-energy emission and the non-monochromatic modulation and changes in flux suggests that a simple one-zone model is unable to explain all the variability. Instead, a model including a periodic component along with multiple emission zones is required.

Journal keyword(s): radiation mechanisms: non-thermal - galaxies: active - BL Lacertae objects: individual: (PG 1553 + 113) - gamma-rays: galaxies

Errata: erratum vol. 532, p. 3134 (2024)

Simbad objects: 8

Full paper

View the references in ADS

Number of rows : 8

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag U	Mag B	Mag V	Mag R	Sp type	#ref 1850 - 2026	#notes
1	3C 48	QSO	01 37 41.2996631208	+33 09 35.080388820		16.62	16.20		~	2924	2
2	NAME Per B	SyG	04 37 04.37535450	+29 40 13.8179631		21.7			~	533	2
3	M 1	SNR	05 34 31.8	+22 01 03					~	6516	1
4	PG 0851+202	BLL	08 54 48.8749846272	+20 06 30.639583620		15.649	15.146	15.446	~	2513	1
5	7C 122223.5+213929	Bla	12 24 54.4583146056	+21 22 46.385507388		17.56	17.50	18.2	~	770	2
6	3C 286	Sy1	13 31 08.2883506368	+30 30 32.960091564		17.51	17.25		~	4558	2
7	PG 1553+113	BLL	15 55 43.0440048528	+11 11 24.365649948	14.91	14.72	14.57	13.99	~	672	1
8	NGC 7027	PN	21 07 01.571952	+42 14 10.47120		10.358	8.831	10.157	~	2541	1

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