J/ApJS/266/37 Time evolution of Mrk501 emission during 2017-2020 (Abe+, 2023)
Multimessenger characterization of Markarian 501 during historically low X-ray
and γ-ray activity.
Abe H., Abe S., 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., Barrio J.A., Batkovic I.,
Baxter J., Becerra Gonzalez J., Bednarek W., Bernardini E., Bernardos M.,
Berti A., Besenrieder J., Bhattacharyya W., Bigongiari C., Biland A.,
Blanch O., Bonnoli G., Bosnjak Z., Burelli I., Busetto G., Carosi R.,
Carretero-Castrillo M., Castro-Tirado A.J., 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.,
Escudero J., Fallah Ramazani V., Farina L., Fattorini A., Foffano L.,
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., Grau R., Green D.,
Green J.G., Hadasch D., Hahn A., Hassan T., Heckmann L., Herrera J.,
Hrupec D., Hutten M., Imazawa R., Inada T., Iotov R., Ishio K.,
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., Mang N., 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., Okumura A., Otero-Santos J., Paiano S., Palatiello M., Paneque D.,
Paoletti R., Paredes J.M., Pavletic L., 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., 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., 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.,
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.,
The MAGIC Collaboration,
Cerruti M., Acosta-Pulido J.A., Apolonio G., Bachev R.,
Balokovic M., Benitez E., Bjorklund I., Bozhilov V., Brown L.F., Bugg A.,
Carbonell W., Carnerero M.I., Carosati D., Casadio C., Chamani W.,
Chen W.P., Chigladze R.A., Damljanovic G., Epps K., Erkenov A., Feige M.,
Finke J., Fuentes A., Gazeas K., Giroletti M., Grishina T.S., Gupta A.C.,
Gurwell M.A., Heidemann E., Hiriart D., Hou W.J., Hovatta T., Ibryamov S.,
Joner M.D., Jorstad S.G., Kania J., Kiehlmann S., Kimeridze G.N.,
Kopatskaya E.N., Kopp M., Korte M., Kotas B., Koyama S., Kramer J.A.,
Kunkel L., Kurtanidze S.O., Kurtanidze O.M., Lahteenmaki A., Lopez J.M.,
Larionov V.M., Larionova E.G., Larionova L.V., Leto C., Lorey C.,
Mujica R., Madejski G.M., Marchili N., Marscher A.P., Minev M.,
Modaressi A., Morozova D.A., Mufakharov T., Myserlis I., Nikiforova A.A.,
Nikolashvili M.G., Ovcharov E., Perri M., Raiteri C.M., Readhead A.C.S.,
Reimer A., Reinhart D., Righini S., Rosenlehner K., Sadun A.C.,
Savchenko S.S., Scherbantin A., Schneider L., Schoch K., Seifert D.,
Semkov E., Sigua L.A., Singh C., Sola P., Sotnikova Y., Spencer M.,
Steineke R., Stojanovic M., Strigachev A., Tornikoski M., Traianou E.,
Tramacere A., Troitskaya Y.V., Troitskiy I.S., Trump J.B., Tsai A.,
Valcheva A., Vasilyev A.A., Verrecchia F., Villata M., Vince O.,
Vrontaki K., Weaver Z.R., Zaharieva E., Zottmann N.,
<Astrophys. J. Suppl. Ser., 266, 37 (2023)>
=2023ApJS..266...37A 2023ApJS..266...37A
ADC_Keywords: BL Lac objects; Active gal. nuclei; Gamma rays; X-ray sources;
Radio sources; Photometry; Optical; Polarization;
Energy distributions; Ultraviolet
Keywords: Active galaxies ; BL Lacertae objects ; Markarian galaxies ;
Active galactic nuclei ; Blazars
Abstract:
We study the broadband emission of Mrk 501 using multiwavelength
observations from 2017 to 2020 performed with a multitude of
instruments, involving, among others, MAGIC, Fermi's Large Area
Telescope (LAT), NuSTAR, Swift, GASP-WEBT, and the Owens Valley Radio
Observatory. Mrk 501 showed an extremely low broadband activity, which
may help to unravel its baseline emission. Nonetheless, significant
flux variations are detected at all wave bands, with the highest
occurring at X-rays and very-high-energy (VHE) γ-rays. A
significant correlation (>3σ) between X-rays and VHE
γ-rays is measured, supporting leptonic scenarios to explain the
variable parts of the emission, also during low activity. This is
further supported when we extend our data from 2008 to 2020, and
identify, for the first time, significant correlations between the
Swift X-Ray Telescope and Fermi-LAT. We additionally find correlations
between high-energy γ-rays and radio, with the radio lagging by
more than 100 days, placing the γ-ray emission zone upstream of
the radio-bright regions in the jet. Furthermore, Mrk 501 showed a
historically low activity in X-rays and VHE γ-rays from mid-2017
to mid-2019 with a stable VHE flux (>0.2TeV) of 5% the emission of the
Crab Nebula. The broadband spectral energy distribution (SED) of this
2yr long low state, the potential baseline emission of Mrk 501, can be
characterized with one-zone leptonic models, and with (lepto)-hadronic
models fulfilling neutrino flux constraints from IceCube. We explore
the time evolution of the SED toward the low state, revealing that the
stable baseline emission may be ascribed to a standing shock, and the
variable emission to an additional expanding or traveling shock.
Description:
This study focuses on the multiwavelength (MWL) data collected from
Mrk 501 during the 4yr period spanning from the beginning of the
observational period in the year 2017 until the end of the
observational period in the year 2020 (MJD 57754 to MJD 59214).
The coordinated observations involve a large number of instruments,
including FACT, MAGIC, Fermi-LAT, Swift, GLAST-AGILE Support Program
(GASP)-Whole Earth Blazar Telescope (WEBT), and OVRO. Additionally,
three 10hr long observations with NuSTAR yielded a precise measurement
of the falling segment of the low-energy bump, which is expected to be
dominated by the highest-energy electrons at the source.
Objects:
----------------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------------
16 53 52.21 +39 45 36.6 Mrk 501 = MCG+07-35-002
----------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
vhe.dat 121 630 All published very-high-energy (VHE; E>0.1TeV) data
(Data behind Figure 1)
xrt.dat 68 1156 Swift-XRT data (Data behind Figure 1)
lat.dat 59 312 Fermi-LAT data in 14 day bins (data behind Figure 1)
ovro.dat 41 635 Owens Valley Radio Observatory (OVRO) data
(Data behind Figure 1)
magic.dat 107 178 MAGIC data (Data behind Figure 2)
lat2.dat 59 95 Fermi-LAT data in 14 day bins (data behind Figure 2)
xray.dat 68 444 X-ray data in daily bins including Swift-XRT and
three NuSTAR observations (data behind Figure 2)
uvot.dat 49 759 Swift-UVOT data (data behind Figure 2)
rband.dat 61 901 Optical R-band data from GASP-WEBT and Tuorla
(Data behind Figure 2)
radio.dat 49 475 Radio data including OVRO, Metsahovi, Medicina,
IRAM, RATAN-600 and SMA (Data behind Figure 2)
pol.dat 62 336 Polarization data (Data behind Figure 2)
fig9a.dat 97 43 *Broadband SED of the identified low-state period
spanning from 2017-06-17 to 2019-07-23
(MJD57921 to MJD58687)
fig9b.dat 97 35 *Broadband SED around the first NuSTAR observation
(NuSTAR-1) on 2017-04-28 (MJD57871)
fig9c.dat 97 35 *Broadband SED around the the second NuSTAR
observation (NuSTAR-2) on 2017-05-25 (MJD57898)
--------------------------------------------------------------------------------
Note on fig9a.dat: Broadband SED of the identified low-state period spanning
from 2017-06-17 to 2019-07-23 (MJD 57921 to MJD 58687), which includes
the NuSTAR observation on 2018-04-20 (MJD 58228). Archival WISE data
points from 2010 are also depicted.
Note on fig9b.dat: Broadband SED around the first NuSTAR observation (NuSTAR-1)
on 2017-04-28 (MJD 57871). For MAGIC and Fermi-LAT, the γ-ray spectra
is derived using data from a 2-week interval centered at NuSTAR-1.
Note on fig9c.dat: Broadband SED around the second NuSTAR observation (NuSTAR-2)
on 2017-05-25 (MJD 57898). For Fermi-LAT, the γ-ray spectrum is
derived using data from a 2-week interval centered at NuSTAR-2.
Archival WISE data from 2010 are also shown.
--------------------------------------------------------------------------------
Description of file:
The three tar.gz files containing the original FITS files for the
three Figures 1, 2 and 9 are also available on the FTP.
See also:
II/328 : AllWISE Data Release (Cutri+ 2013)
VIII/76 : Leiden/Argentine/Bonn (LAB) Survey of Galactic HI (Kalberla+ 2005)
J/A+AS/132/305 : Extragal. radio sources at 22, 37 and 87GHz (Terasranta+ 1998)
J/AJ/134/799 : Multiwaveband polarimetry of 15 AGN (Jorstad+, 2007)
J/ApJ/716/30 : SED of Fermi bright blazars (Abdo+, 2010)
J/ApJ/741/30 : Radio/γ-ray correlation in AGN (Ackermann+, 2011)
J/ApJ/740/98 : Synchroton peak for blazars and radio galaxies (Meyer+, 2011)
J/ApJS/194/29 : Observations of blazars at 15GHz (Richards+, 2011)
J/ApJ/792/30 : NEOWISE magnitudes for near-Earth objects (Mainzer+, 2014)
J/A+A/573/A50 : Multiwavelength obs. of Mrk 501 in 2008 (Aleksic+, 2015)
J/A+A/576/A126 : The 2009 multiwavelength campaign on Mrk421 (Aleksic+, 2015)
J/A+A/596/A78 : R-band polarization curves of 48 BL Lacs (Hovatta+, 2016)
J/ApJ/846/98 : Jet kinematics of blazars at 43GHz with VLBA (Jorstad+, 2017)
J/AN/338/700 : Flux densities for 290 blazars (Mingaliev+, 2017)
J/ApJ/864/84 : Swift follow-up obs. of TXS 0506+056 blazar (Keivani+, 2018)
J/ApJS/247/33 : The Fermi LAT fourth source catalog (4FGL) (Abdollahi+, 2020)
J/ApJS/247/16 : Extreme high-frequency-peaked BL Lac objects (Acciari+, 2020)
J/A+A/655/A93 : Mrk 501 long-term multi-band photometry (Arbet-Engels+, 2021)
J/ApJ/923/30 : MOJAVE. XVIII. Bright radio-loud active AGNs (Lister+, 2021)
J/ApJS/260/12 : Jet kinematics of blazars at 43GHz (Weaver+, 2022)
http://www.oato.inaf.it/blazars/webt/ : Whole Earth Blazar Telescope home page
Byte-by-byte Description of file: vhe.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.7 d MJD [53518.9/59082.91] Modified Julian Date
15- 24 F10.7 --- Flux [-0.11/6.51] Flux in Crab units
26- 34 F9.7 --- e_Flux [0/0.6] Flux uncertainty (Crab units)
36- 42 A7 --- Inst Instrument (1)
44 A1 --- l_Energy Upper limit flag on Energy
46- 49 F4.2 TeV Energy Energy threshold of each analysis (2)
51- 76 A26 --- Ref Reference to the publication the data is
taken from (3)
78-121 A44 --- DOI DOI of the reference
--------------------------------------------------------------------------------
Note (1): Instrument as follows:
FACT = the First G-APD Cherenkov Telescope (288 occurrences)
MAGIC = the Major Atmospheric Gamma-ray Imaging Cherenkov telescopes located
at the Roque de los Muchachos Observatory, on the Canary Island of
La Palma (232 occurrences)
Veritas = the VERITAS array located at the Fred Lawrence Whipple Observatory
in southern Arizona (80 occurrences)
Whipple = (26 occurrences)
HESS = the High Energy Stereoscopic System (6 occurrences)
Note (2): Due to different energy thresholds used in the various publications,
the Crab flux from Aleksic+ 2015 (J/A+A/573/A50) was used to scale the
fluxes to units of Crab units and make them comparable.
Systematics accounting for the different energy thresholds are NOT applied.
Note (3): Reference as follows:
Acciari et al. (2020a) = 2020A&A...637A..86M 2020A&A...637A..86M
Ahnen et al. (2017a) = 2017A&A...603A..31A 2017A&A...603A..31A
Ahnen et al. (2018) = 2018A&A...620A.181A 2018A&A...620A.181A
Albert et al. (2007) = 2007ApJ...669..862A 2007ApJ...669..862A
Aleksi et al. (2015a) = 2015, Cat. J/A+A/573/A50
Anderhub et al. (2009) = 2009ApJ...705.1624A 2009ApJ...705.1624A
Arbet-Engels et al. (2021) = 2021, Cat. J/A+A/655/A93
Cologna et al. (2017) = 2017AIPC.1792e0019C 2017AIPC.1792e0019C
Furniss et al. (2015) = 2015ApJ...812...65F 2015ApJ...812...65F
this work = Abe+ 2023ApJS..266...37A 2023ApJS..266...37A (90 occurrences)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: xrt.dat xray.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.7 d MJD [53481/59112.9] Modified Julian Date
15- 26 E12.7 mW/m2 Flux [4.7e-12/4.9e-10] Flux in erg/cm2/s
28- 39 E12.7 mW/m2 e_Flux [1e-13/2e-11] Lower uncertainty in Flux
41- 52 E12.7 mW/m2 E_Flux [1e-13/3e-11] Upper uncertainty in Flux
54- 62 A9 --- Inst The instrument ("Swift-XRT" or "NuSTAR")
64- 68 A5 keV Band X-ray range (0.3-2, 2-10, 3-7 or 7-30)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: lat*.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.7 d MJD [54695/59119.01] Modified Julian Date
15 I1 --- Bin [7] MJD bin (always "7")
17- 28 E12.7 ph.cm-2.s-1 Flux [4.4e-09/6.3e-08] Flux in ph/cm2/s
30- 41 E12.7 ph.cm-2.s-1 e_Flux [2.7e-09/8.7e-09] Uncertainty in Flux
43- 51 A9 --- Inst [Fermi-LAT] Instrument (always "Fermi-LAT")
53- 59 A7 GeV Band Band (always "0.3-500")
--------------------------------------------------------------------------------
Byte-by-byte Description of file: ovro.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.7 d MJD [54853.5/59200] Modified Julian Date
15- 23 F9.7 Jy Flux [0.96/1.31] Flux
25- 33 F9.7 Jy e_Flux [0.006/0.3] Uncertainty in Flux
35- 38 A4 --- Inst [OVRO] Instrument (always "OVRO")
40- 41 I2 GHz Band [15] Band (always 15)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: magic.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.7 d MJD [57834.2/59082.91] Modified Julian Date
15- 23 F9.7 --- Bin [0.006/3.5] The MJD bin size
25- 37 E13.7 ph.cm-2.s-1 Flux [-1.6e-12/6e-11] Flux in ph/cm2/s
39- 50 E12.7 ph.cm-2.s-1 e_Flux [1e-12/8.2e-12] Flux uncertainty
52- 63 E12.7 --- Limit [6.8e-12/4.2e-11]? Upper limit in flux (1)
65- 86 A22 --- Inst Instrument (either nightly binned
or weekly binned)
88- 107 A20 --- Band Band (always >0.2 TeV)
--------------------------------------------------------------------------------
Note (1): The upper limit in Flux, provided for data points where the
significance of the flux measurement is less than 2 sigma.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: uvot.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.7 --- MJD [57777/59112.9] Modified Julian Date
15- 18 F4.2 mJy Flux [1.3/3] Flux
20- 23 F4.2 mJy e_Flux [0.05/0.15] Uncertainty in Flux
25- 34 A10 --- Inst [Swift-UVOT] Instrument (always "Swift-UVOT")
36- 37 A2 --- Filt Swift UV filter (W1, M2, W2)
39- 49 A11 eV Band Band range (3.76-6.5, 4.52-7.09 or 4.8-9.75)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: rband.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.7 d MJD [57800.5/59190.5] Modified Julian Date
15- 23 F9.7 mJy Flux [3.7/6] Flux
25- 33 F9.7 mJy e_Flux [0.06/0.6] Uncertainty in Flux
35- 54 A20 --- Inst Instrument (always "GASP-WEBT and Tuorla")
56- 61 A6 --- Band Band (always "R-band")
--------------------------------------------------------------------------------
Byte-by-byte Description of file: radio.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.7 d MJD [57762/59205.4] Modified Julian Date
15- 23 F9.7 Jy Flux [0.2/1.6] Flux
25- 33 F9.7 Jy e_Flux [0.01/0.2] Uncertainty in Flux
35- 43 A9 --- Inst Instrument ("RATAN", "Metsahovi", "OVRO",
"SMA", "IRAM" or "Medicina")
45- 49 F5.1 GHz Band [4.7/345] Band (4.7, 8, 15, 24, 37, 100, 230
or 345)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: pol.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.7 d MJD [57767/59138.2] Modified Julian Date
15- 20 F6.3 % Pol [0.4/12.8] Polarization degree
22- 26 F5.3 % e_Pol [0.1/4] Uncertainty in the polarization degree
28- 33 F6.2 deg PA [13/242.6] Polarization angle
35- 39 F5.2 deg e_PA [0.6/26] Uncertainty in the polarization angle
41- 47 A7 --- Inst Instrument ("Steward", "Crimean", "Perkins",
"NOT", & "VLBA")
49- 55 A7 --- lam "Optical" or "Radio"
57- 62 A6 --- Band Band ("R-band" or "43GHz" for the VLBA data)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: fig9*.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 12 E12.7 eV Energy [6.2e-05/1.7e+12] Center energy
14- 25 E12.7 eV b_Energy Minimum energy
27- 38 E12.7 eV B_Energy Maximum energy
40- 51 E12.7 mW/m2 E2dNdE [1.5e-13/4.3e-11] Center flux density
in erg/cm2/s units
53- 64 E12.7 mW/m2 b_E2dNdE Minimum flux density
66- 77 E12.7 mW/m2 B_E2dNdE Maximum flux density
79- 97 A19 --- Label Legend label (including instrument name)
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 11-Aug-2023