J/A+A/685/A117 Mrk 501 multiwavelength light curves (MAGIC Coll.+, 2024)
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., Froese 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.,
Guenther P., Hadasch D., Hahn A., Hassan T., Heckmann L., Herrera J.,
Hrupec D., Huetten 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., 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.,
Laehteenmaeki 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.,
Syrjaerinne I., Tornikoski M., Uemura M., Verrecchia F., Vervelaki A.
<Astron. Astrophys. 685, A117 (2024)>
=2024A&A...685A.117M 2024A&A...685A.117M (SIMBAD/NED BibCode)
ADC_Keywords: BL Lac objects ; Radio sources ; X-ray sources ; Gamma rays
Keywords: radiation mechanisms: non-thermal - galaxies: active -
BL Lacertae objects: individual: Markarian 501 - gamma rays: general -
X-rays: galaxies
Abstract:
We present the first multi-wavelength study of Mrk 501 including
very-high- energy (VHE) γ-ray observations simultaneous to X-ray
polarization measurements from the Imaging X-ray Polarimetry Explorer
(IXPE).
We use radio-to-VHE data from a multi-wavelength campaign organized
between 2022-03-01 and 2022-07-19 (MJD 59639 to MJD 59779). The
observations were performed by MAGIC, Fermi-LAT, NuSTAR, Swift (XRT
and UVOT), and several instruments covering the optical and radio
bands to complement the IXPE pointings. We characterize the dynamics
of the broad-band emission around the X-ray polarization measurements
through its multi-band fractional variability and correlations, and
compare changes observed in the polarization degree to changes seen in
the broad-band emission using a multi-zone leptonic scenario.
During the IXPE pointings, the VHE state is close to the average
behavior with a 0.2-1TeV flux of 20%-50% the emission of the Crab
Nebula. Additionally, it shows low variability and a hint of
correlation between VHE and X-rays. Despite the average VHE activity,
an extreme X-ray behavior is measured for the first two IXPE pointings
in March 2022 (MJD 59646 to 59648 and MJD 59665 to 59667) with a
synchrotron peak frequency >1keV. For the third IXPE pointing in July
2022 (MJD 59769 to 59772), the synchrotron peak shifts towards 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 angle 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 strengthen the hypothesis of an energy-stratified jet.
We model the broad-band spectra simultaneous to the IXPE pointings
assuming a compact zone dominating in the X-rays and VHE, and an
extended zone stretching further downstream the jet dominating 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 of magnetization
and/or emission region size, which directly connects the shift of the
synchrotron peak to lower energies with the drop in polarization
degree.
Description:
In this work, we present for the first time radio-to-TeV data of a
blazar together with simultaneous X-ray polarization measurements.
This work focuses on the BL Lac object Mrk501. We investigate the
multiwavelength variability and correlation patterns, and compare it
with the radio-to-X-ray polarization evolution. This Readme describes
the data files published together with the paper. The data from the
figures 1, 2 are made available.
Requests for the OVRO 15GHz data should be directed to the OVRO 40m
Telescope collaboration.
Objects:
----------------------------------------------------------
RA (2000) DE Designation(s)
----------------------------------------------------------
16 53 52.21 +39 45 36.6 Mrk 501 = SWIFT J1653.9+3945
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
fig1.dat 86 763 Multiwavelength light curves of Fig.1
fig2.dat 131 90 Multiwavelength SED of Fig.2
--------------------------------------------------------------------------------
Byte-by-byte Description of file: fig1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 F10.4 --- MJD Modified Julian date center
12- 18 F7.3 --- Flux/pol Flux or polarization degree/angle
20- 25 F6.3 --- E_Flux/pol ?=- Upper uncertainty on Flux/pol
27- 32 F6.3 --- e_Flux/pol ?=- Lower uncertainty on Flux/pol
34 I1 --- l_Flux/pol [0/1] If 1, Flux/pol is a upper limit at 95%
confidence level
36- 45 A10 --- Energy Energy/Frequency range or Filter
47- 58 A12 --- Inst Instrument
60- 86 A27 --- Unit Units
--------------------------------------------------------------------------------
Byte-by-byte Description of file: fig2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 22 E22.17 Hz Freq Frequency, bin center
24- 45 E22.17 mW/m2 nuFnu Energy flux
47- 68 E22.17 mW/m2 E_nuFnu ?=- Energy flux upper uncertainty
70- 91 E22.17 mW/m2 e_nuFnu ?=- Energy flux upper uncertainty
93 I1 --- l_nuFnu [0/1] If 1, nuFnu is a upper limit at 95%
confidence level
95-100 A6 --- Epoch Corresponding epoch of the SED
(see paper for details)
102-119 A18 --- Inst Instrument
121-131 A11 --- Unit Units
--------------------------------------------------------------------------------
Acknowledgements:
Lea Heckmann, heckmann(at)mpp.mpg.de
(End) Patricia Vannier [CDS] 21-Mar-2024