2024A&A...685A.117M

Query : 2024A&A...685A.117M

2024A&A...685A.117M - Astronomy and Astrophysics, volume 685A117 (2024/5-1)

Insights into the broadband emission of the TeV blazar Mrk 501 during the first X-ray polarization measurements.

MAGIC COLLABORATION, ABE S., ABHIR J., ACCIARI V.A., AGUASCA-CABOT A., AGUDO I., ANIELLO T., ANSOLDI S., ANTONELLI L.A., ARBET ENGELS A., ARCARO C., ASANO K., BABIC A., BAQUERO A., BARRES DE ALMEIDA U., BARRIO J.A., BATKOVIC I., BAUTISTA A., BAXTER J., BECERRA GONZALEZ J., BEDNAREK W., BERNARDINI E., BERNARDOS M., 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., CERIBELLA G., CHAI Y., CIFUENTES A., 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., DE MENEZES R., DEL POPOLO A., DELFINO M., DELGADO J., DELGADO MENDEZ C., 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., FROSE 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., GRADETZKE T., GRAU R., GREEN D., GREEN J.G., GUNTHER P., HADASCH D., HAHN A., HASSAN T., HECKMANN L., HERRERA J., HRUPEC D., HUTTEN M., IMAZAWA R., ISHIO K., JIMENEZ MARTINEZ I., KAYANOKI T., KERSZBERG D., KLUGE G.W., KOBAYASHI Y., KOUCH P.M., KUBO H., KUSHIDA J., LAINEZ LEZAUN M., LAMASTRA A., 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., MANG N., MANGANARO M., MANGANO S., 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., PERESANO M., 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., SILVESTRI G., SITAREK J., SOBCZYNSKA D., SPOLON A., STAMERRA A., STRISKOVIC J., STROM D., SUDA Y., SUUTARINEN S., TAJIMA H., TAKAHASHI M., 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., VIALE I., VIGORITO C.F., VITALE V., VOVK I., WALTER R., WILL M., WUNDERLICH C., YAMAMOTO T. (The Multi-wavelength collaborators), LIODAKIS I., ACEITUNO F.J., AGIS-GONZALEZ B., AKITAYA H., BERNARDOS M.I., BLINOV D., BOURBAH I.G., CASADIO C., CASANOVA V., D'AMMANDO F., FALLAH RAMAZANI V., FERNANDEZ-GARCIA E., FUKAZAWA Y., GARCIA-COMAS M., GAU E., GOKUS A., GURWELL M., HAKALA P., HOVATTA T., HU Y.-D., HUSILLOS C., JORMANAINEN J., JORSTAD S.G., KAWABATA K.S., KEATING G.K., KIEHLMANN S., KONTOPODIS E., KRAWCZYNSKI H., LAHTEENMAKI A., LETO C., LISALDA L., MANDARAKAS N., MARCHINI A., MARSCHER A.P., MAX-MOERBECK W., MIDDEI R., MIZUNO T., MYSERLIS I., NAKAOKA T., PERRI M., PUCCETTI S., RAO R., READHEAD A.C.S., REEVES R., RODRIGUEZ CAVERO N., SALOME Q., SASADA M., SKALIDIS R., SOTA A., SYRJARINNE I., TORNIKOSKI M., UEMURA M., VERRECCHIA F. and VERVELAKI A.

Abstract (from CDS):

Aims. We present the first multiwavelength study of Mrk 501 that contains simultaneous very-high-energy (VHE) γ-ray observations and X-ray polarization measurements from the Imaging X-ray Polarimetry Explorer (IXPE).
Methods. We used radio-to-VHE data from a multiwavelength campaign carried out between March 1, 2022, and July 19, 2022 (MJD 59639 to MJD 59779). The observations were performed by MAGIC, Fermi-LAT, NuSTAR, Swift (XRT and UVOT), and several other instruments that cover the optical and radio bands to complement the IXPE pointings. We characterized the dynamics of the broadband emission around the X-ray polarization measurements through its multiband fractional variability and correlations, and compared changes observed in the polarization degree to changes seen in the broadband emission using a multi-zone leptonic scenario.
Results. During the IXPE pointings, the VHE state is close to the average behavior, with a 0.2-1 TeV flux of 20%-50% of the emission of the Crab Nebula. Additionally, it shows low variability and a hint of correlation between VHE γ-rays and X-rays. Despite the average VHE activity, an extreme X-ray behavior is measured for the first two IXPE pointings, taken in March 2022 (MJD 59646 to 59648 and MJD 59665 to 59667), with a synchrotron peak frequency > 1 keV. For the third IXPE pointing, in July 2022 (MJD 59769 to 59772), the synchrotron peak shifts toward lower energies and the optical/X-ray polarization degrees drop. All three IXPE epochs show an atypically low Compton dominance in the γ-rays. The X-ray polarization is systematically higher than at lower energies, suggesting an energy stratification of the jet. While during the IXPE epochs the polarization angles in the X-ray, optical, and radio bands align well, we find a clear discrepancy in the optical and radio polarization angles in the middle of the campaign. Such results further support the hypothesis of an energy-stratified jet. We modeled broadband spectra taken simultaneous to the IXPE pointings, assuming a compact zone that dominates in the X-rays and the VHE band, and an extended zone stretching farther downstream in the jet that dominates the emission at lower energies. NuSTAR data allow us to precisely constrain the synchrotron peak and therefore the underlying electron distribution. The change between the different states observed in the three IXPE pointings can be explained by a change in the magnetization and/or the emission region size, which directly connects the shift in the synchrotron peak to lower energies with the drop in the polarization degree.

Abstract Copyright: © The Authors 2024

Journal keyword(s): radiation mechanisms: non-thermal - galaxies: active - BL Lacertae objects: individual: Markarian 501 - gamma rays: general - X-rays: galaxies

VizieR on-line data: <Available at CDS (J/A+A/685/A117): fig1.dat fig2.dat>

Simbad objects: 9

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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 Z 184-50 BLL 11 04 27.3140835504 +38 12 31.798495872   13.50 12.90 8.31   ~ 2841 1
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 Z 225-7 BLL 16 53 52.21668403 +39 45 36.6088754 14.09 14.15 13.29 8.26   ~ 2304 2
7 EM* MWC 349A Or* 20 32 45.5291969760 +40 39 36.651807828           ~ 180 0
8 NGC 7027 PN 21 07 01.571952 +42 14 10.47120   10.358 8.831 10.157   ~ 2541 1
9 QSO B2344+514 BLL 23 47 04.8372110928 +51 42 17.877513168     15.50 10.7   ~ 500 1

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