2023A&A...670A..49M

Query : 2023A&A...670A..49M

2023A&A...670A..49M - Astronomy and Astrophysics, volume 670A49 (2023/2-1)

Long-term multi-wavelength study of 1ES 0647+250.

MAGIC COLLABORATION, ACCIARI V.A., 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., BARRIO J.A., BATKOVIC I., BECERRA GONZALEZ J., BEDNAREK W., BERNARDINI E., BERNARDOS M., BERTI A., BESENRIEDER J., BHATTACHARYYA W., BIGONGIARI C., BILAND A., BLANCH O., BOKENKAMP H., BONNOLI G., BOSNJAK Z., BURELLI I., BUSETTO G., CAROSI R., CARRETERO-CASTRILLO M., CERIBELLA G., CHAI Y., CHILINGARIAN 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., DO SOUTO ESPINEIRA E., DOMINIS PRESTER D., DONINI A., DORNER D., DORO M., ELSAESSER D., EMERY G., FALLAH RAMAZANI V., FARINA L., FATTORINI A., FONT L., FRUCK C., FUKAMI S., FUKAZAWA Y., GARCIA LOPEZ R.J., GARCZARCZYK M., GASPARYAN S., GAUG M., GIESBRECHT PAIVA J.G., GIGLIETTO N., GIORDANO F., GLIWNY P., GODINOVIC N., GREEN J.G., GREEN D., HADASCH D., HAHN A., HASSAN T., HECKMANN L., HERRERA J., HRUPEC D., HUTTEN M., INADA T., IOTOV R., ISHIO K., IWAMURA Y., JIMENEZ MARTINEZ I., JORMANAINEN J., KERSZBERG D., KOBAYASHI Y., KUBO H., KUSHIDA J., LAMASTRA A., LELAS D., LEONE F., LINDFORS E., LINHOFF L., LOMBARDI S., LONGO F., LOPEZ-COTO R., LOPEZ-MOYA M., LOPEZ-ORAMAS A., LOPORCHIO S., LORINI A., LYARD E., MACHADO DE OLIVEIRA FRAGA B., MAJUMDAR P., MAKARIEV M., MANEVA G., MANGANARO M., MANGANO S., MANNHEIM K., MARIOTTI M., MARTINEZ M., MAS AGUILAR A., MAZIN D., MENCHIARI S., MENDER S., MICANOVIC S., MICELI D., MIENER T., MIRANDA J.M., MIRZOYAN R., MOLINA E., MONDAL H.A., MORALEJO A., MORCUENDE D., MORENO V., NAKAMORI T., NANCI C., NAVA L., NEUSTROEV V., NIEVAS ROSILLO M., NIGRO C., NILSSON K., NISHIJIMA K., NJOH EKOUME T., NODA K., NOZAKI S., OHTANI Y., OKA T., OTERO-SANTOS J., PAIANO S., PALATIELLO M., PANEQUE D., PAOLETTI R., PAREDES J.M., PAVLETIC L., PERSIC M., PIHET M., PODOBNIK F., PRADA MORONI P.G., PRANDINI E., PRINCIPE G., PRIYADARSHI C., PULJAK I., RHODE W., RIBO M., RICO J., RIGHI C., RUGLIANCICH A., SAHAKYAN N., SAITO T., SAKURAI S., SATALECKA K., SATURNI F.G., SCHLEICHER B., SCHMIDT K., SCHMUCKERMAIER F., SCHUBERT J.L., SCHWEIZER T., SITAREK J., SLIUSAR V., SOBCZYNSKA D., SPOLON A., STAMERRA A., STRISKOVIC J., STROM D., STRZYS M., SUDA Y., SURIC T., TAKAHASHI M., TAKEISHI R., TAVECCHIO F., TEMNIKOV P., TERZIC T., TESHIMA M., TOSTI L., TRUZZI S., TUTONE A., UBACH S., VAN SCHERPENBERG J., VANZO G., VAZQUEZ ACOSTA M., VENTURA S., VERGUILOV V., VIALE I., VIGORITO C.F., VITALE V., VOVK I., WALTER R., WILL M., WUNDERLICH C., YAMAMOTO T., ZARIC D., ACOSTA-PULIDO J.A., D'AMMANDO F., HOVATTA T., KIEHLMANN S., LIODAKIS I., LETO C., MAX-MOERBECK W., PACCIANI L., PERRI M., READHEAD A.C.S., REEVES R.A. and VERRECCHIA F.

Abstract (from CDS):


Context. The BL Lac object 1ES 0647+250 is one of the few distant γ-ray emitting blazars detected at very high energies (VHEs; ≳100 GeV) during a non-flaring state. It was detected with the MAGIC telescopes during a period of low activity in the years 2009-2011 as well as during three flaring activities in the years 2014, 2019, and 2020, with the highest VHE flux in the last epoch. An extensive multi-instrument data set was collected as part of several coordinated observing campaigns over these years.
Aims. We aim to characterise the long-term multi-band flux variability of 1ES 0647+250, as well as its broadband spectral energy distribution (SED) during four distinct activity states selected in four different epochs, in order to constrain the physical parameters of the blazar emission region under certain assumptions.
Methods. We evaluated the variability and correlation of the emission in the different energy bands with the fractional variability and the Z-transformed discrete correlation function, as well as its spectral evolution in X-rays and γ rays. Owing to the controversy in the redshift measurements of 1ES 0647+250 reported in the literature, we also estimated its distance in an indirect manner through a comparison of the GeV and TeV spectra from simultaneous observations with Fermi-LAT and MAGIC during the strongest flaring activity detected to date. Moreover, we interpret the SEDs from the four distinct activity states within the framework of one-component and two-component leptonic models, proposing specific scenarios that are able to reproduce the available multi-instrument data.
Results. We find significant long-term variability, especially in X-rays and VHE γ rays. Furthermore, significant (3-4σ) correlations were found between the radio, optical, and high-energy (HE) γ-ray fluxes, with the radio emission delayed by about ∼400 days with respect to the optical and γ-ray bands. The spectral analysis reveals a harder-when-brighter trend during the non-flaring state in the X-ray domain. However, no clear patterns were observed for either the enhanced states or the HE (30 MeV < E < 100 GeV) and VHE γ-ray emission of the source. The indirect estimation of the redshift yielded a value of z = 0.45 ± 0.05, which is compatible with some of the values reported in the literature. The SEDs related to the low-activity state and the three flaring states of 1ES 0647+250 can be described reasonably well with the both one-component and two-component leptonic scenarios. However, the long-term correlations indicate the need for an additional radio-producing region located about 3.6 pc downstream from the gamma-ray producing region.

Abstract Copyright: © The Authors 2023

Journal keyword(s): galaxies: active - galaxies: jets - gamma rays: galaxies - BL Lacertae objects: individual: 1ES 0647+250

Simbad objects: 16

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Number of rows : 16
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 RX J0232.8+2017 BLL 02 32 48.6148874688 +20 17 17.486717388     18.00 13.96   ~ 387 1
2 PKS J0449-4350 BLL 04 49 24.6981911928 -43 50 08.960970948 14.95 17.52 15.24 16.27   ~ 190 1
3 PMN J0509+0541 BLL 05 09 25.9644373872 +05 41 35.333820420 15.32 14.95 14.78 15.12   ~ 589 2
4 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
5 1RXS J065033.9+205603 BLL 06 50 35.3520080787 +20 55 57.363171447           ~ 23 0
6 RX J0650.7+2502 BLL 06 50 46.4900658984 +25 02 59.625654828 16.17 15.97 15.79 16.3   ~ 175 2
7 3FHL J0653.7+2817 BLL 06 53 44.2777799088 +28 15 47.297414880           ~ 34 1
8 RX J0708.9+2241 BLL 07 08 58.2894477720 +22 41 35.498077728           ~ 52 1
9 8C 0716+714 BLL 07 21 53.4482942664 +71 20 36.363846516   15.5 15.50 14.27   ~ 1388 1
10 Z 184-50 BLL 11 04 27.3140835504 +38 12 31.798495872   13.50 12.90 8.31   ~ 2841 1
11 RX J1217.8+3007 BLL 12 17 52.0819904040 +30 07 00.634936872   16.07 15.62 13.47   G7 516 1
12 PMN J1518-2731 BLL 15 18 03.6003266832 -27 31 31.191934728           ~ 72 1
13 Z 225-7 BLL 16 53 52.21668403 +39 45 36.6088754 14.09 14.15 13.29 8.26   ~ 2304 2
14 QSO B1959+650 BLL 19 59 59.8520303688 +65 08 54.652536492     12.8 11.21   ~ 699 2
15 MAGIC J2001+435 BLL 20 01 12.8737326408 +43 52 52.840241616   15.6   15   ~ 108 1
16 QSO B2344+514 BLL 23 47 04.8372110928 +51 42 17.877513168     15.50 10.7   ~ 500 1

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