J/A+A/692/A140 Broadband multi-wavelength properties of M87 (Algaba+, 2024)
Broadband multi-wavelength properties of M87 during the 2018 EHT campaign
including a very high energy flaring episode.
Algaba J.C., Balokovic A., Chandra S., Cheong W.-Y., Cui Y.-Z.,
D'Ammando F., Falcone A.D., Ford N.M., Giroletti M., Goddi C., Gurwell M.A.,
Hada K., Haggard D., Jorstad S., Kaur A., Kawashima T., Kerby S., Kim J.-Y.,
Kino M., Kravchenko E.V., Lee S.-S., Lu R.-S., Markoff S., Michail J.,
Neilsen J., Nowak M.A., Principe G., Ramakrishnan V., Ripperda B.,
Sasada M., Savchenko S., Sheridan C.,
(The Event Horizon Telescope - Multi-wavelength science working group),
Akiyama K., Alberdi A., Alef W., Algaba J.C., Anantua R., Asada K.,
Azulay R., Bach U., Baczko A.-K., Ball D., Bandyopadhyay B., Barrett J.,
Bauboeck M., Benson B.A., Bintley D., Blackburn L., Blundell R.,
Bouman K.L., Bower G.C., Boyce H., Bremer M., Brissenden R., Britzen S.,
Broderick A.E., Broguiere D., Bronzwaer T., Bustamante S., Carlstrom J.E.,
Chael A., Chan C.-K., Chang D.O., Chatterjee K., Chatterjee S., Chen M.-T.,
Chen Y., Cheng X., Cho I., Christian P., Conroy N.S., Conway J.E.,
Crawford T.M., Crew G.B., Cruz-Osorio A., Cui Y., Dahale R., Davelaar J.,
De Laurentis M., Deane R., Dempsey J., Desvignes G., Dexter J., Dhruv V.,
Dihingia I.K., Doeleman S., Dzib S.A., Eatough R.P., Emami R., Falcke H.,
Farah J., Fish V.L., Fomalont E., Ford H.A., Foschi M., Fraga-Encinas R.,
Freeman W.T., Friberg P., Fromm C.M., Fuentes A., Galison P., Gammie C.F.,
Garcia R., Gentaz O., Georgiev B., Goddi C., Gold R., Gomez-Ruiz A.I.,
Gomez J.L., Gu M., Gurwell M., Hada K., Haggard D., Hesper R., Heumann D.,
Ho L.C., Ho P., Honma M., Huang L.C.-W., Huang L., Hughes D.H., Ikeda S.,
Impellizzeri C.M.V., Inoue M., Issaoun S., James D.J., Jannuzi B.T.,
Janssen M., Jeter B., Jiang W., Jimenez-Rosales A., Johnson M.D.,
Jorstad S., Jones A.C., Joshi A.V., Jung T., Karuppusamy R., Kawashima T.,
Keating G.K., Kettenis M., Kim D.-J., Kim J.-Y., Kim J., Kim J., Kino M.,
Koay J.Y., Kocherlakota P., Kofuji Y., Koch P.M., Koyama S., Kramer C.,
Kramer J.A., Kramer M., Krichbaum T.P., Kuo C.-Y., La Bella N., Lee S.-S.,
Levis A., Li Z., Lico R., Lindahl G., Lindqvist M., Lisakov M., Liu J.,
Liu K., Liuzzo E., Lo W.-P., Lobanov A.P., Loinard L., Lonsdale C.J.,
Lowitz A.E., Lu R.-S., MacDonald N.R., Mao J., Marchili N., Markoff S.,
Marrone D.P., Marscher A.P., Marti-Vidal I., Matsushita S., Matthews L.D.,
Medeiros L., Menten K.M., Mizuno I., Mizuno Y., Montgomery J., Moran J.M.,
Moriyama K., Moscibrodzka M., Mulaudzi W., Mueller C., Mueller H., Mus A.,
Musoke G., Myserlis I., Nagai H., Nagar N.M., Nair D.G., Nakamura M.,
Narayanan G., Natarajan I., Nathanail A., Navarro Fuentes S., Neilsen J.,
Ni C., Nowak M.A., Oh J., Okino H., Olivares H., Oyama T., Oezel F.,
Palumbo D.C.M., Filippos Paraschos G., Park J., Parsons H., Patel N.,
Pen U.-L., Pesce D.W., Pietu V., PopStefanija A., Porth O., Prather B.,
Psaltis D., Pu H.-Y., Ramakrishnan V., Rao R., Rawlings M.G., Raymond A.W.,
Rezzolla L., Ricarte A., Ripperda B., Roelofs F., Romero-Canizales C.,
Ros E., Roshanineshat A., Rottmann H., Roy A.L., Ruiz I., Ruszczyk C.,
Rygl K.L.J., Sanchez S., Sanchez-Argueelles D., Sanchez-Portal M.,
Sasada M., Satapathy K., Savolainen T., Schloerb F.P., Schonfeld J.,
Schuster K.-F., Shao L., Shen Z., Small D., Sohn B.W., SooHoo J.,
Sosapanta Salas L.D., Souccar K., Stanway J.S., Sun H., Tazaki F.,
Tetarenko A.J., Tiede P., Tilanus R.P.J., Titus M., Toma K., Torne P.,
Toscano T., Traianou E., Trent T., Trippe S., Turk M., van Bemmel I.,
van Langevelde H.J., van Rossum D.R., Vos J., Wagner J., Ward-Thompson D.,
Wardle J., Washington J.E., Weintroub J., Wharton R., Wielgus M., Wiik K.,
Witzel G., Wondrak M.F., Wong G.N., Wu Q., Yadlapalli N., Yamaguchi P.,
Yfantis A., Yoon D., Young A., Younsi Z., Yu W., Yuan F., Yuan Y.-F.,
Zensus J.A., Zhang S., Zhao G.-Y., Zhao S.-S.,
(The Event Horizon Telescope Collaboration),
Bellazzini R., Berenji B., Bissaldi E., Blandford R.D., Bonino R., Bruel P.,
Cameron R.A., Caraveo P.A., Cavazzuti E., Cheung C., Ciprini S.,
Cristarella Orestano P., Cutini S., Di Lalla N., Dinesh A., Di Venere L.,
Dominguez A., Fegan S.J., Franckowiak A., Fukazawa Y., Fusco P., Gargano F.,
Gasbarra C., Germani S., Giliberti M., Green D., Grenier I.A., Hays E.,
Horan D., Kuss M., Larsson S., Liodakis I., Longo F., Loparco F.,
Lovellette M.N., Maldera S., Mazziotta M.N., I.Mereu, Michelson P.F.,
Mirabal N., Mizuno T., Monzani M.E., Morselli A., Negro M., Omodei N.,
Orlando E., Persic M., Raino S., Rani B., Reimer A., Reimer O.,
Sanchez-Conde M., Saz Parkinson P.M., Sgro C., Siskind E.J., Spinelli P.,
Suson D.J., Tajima H., Torres D.F., Zaharijas G.,
(The Fermi Large Area Telescope Collaboration),
Aharonian F., Ait Benkhali F., Aschersleben J., Ashkar H., Backes M.,
Barbosa Martins V., Batzofin R., Becherini Y., Berge D., Bottcher M.,
Boisson C., Bolmont J., de Bony de Lavergne M., Borowska J., Bouyahiaoui M.,
Bradascio F., Brose R., Brown A., Bruno B., Bulik T., Burger-Scheidlin C.,
Casanova S., Cecil R., Celic J., Cerruti M., Chand T., Chen A., Chibueze J.,
Chibueze O., Cotter G., Damascene Mbarubucyeye J., Devin J., Djuvsland J.,
Dmytriiev A., Einecke S., Ernenwein J.-P., Feijen K., Fontaine G., Funk S.,
Gabici S., Glawion D., Glicenstein J.F., Goswami P., Grolleron G.,
Haerer L., He B., Holch T.L., Holler M., Horns D., Huang Z., Jamrozy M.,
Jankowsky F., Jung-Richardt I., Kasai E., Katarzynski K., Khatoon R.,
Khelifizniak B., Komin Nu., Kosack K., Kundu A., Lang R.G., Le Stum S.,
Leitl F., Lemiere A., Lemoine-Goumard M., Lenain J.-P., Leuschner F.,
Luashvili A., Mackey J., Malyshev D., Marti-Devesa G., Marx R., Meyer M.,
Mitchell A., Moderski R., Moghadam M.O., Mohrmann L., Montanari A.,
Moulin E., Niemiec J., O'Brien P., Ohm S., de Ona Wilhelmi E., Ostrowski M.,
Panny S., Panter M., Pensec U., Pita S., Quirrenbach A., Ravikularaman S.,
Reimer A., Reimer O., Reville B., Reis I., Ren H., Rieger F.,
Roellinghoff G., Rudak B., Ruiz-Velasco E., Sabri K., Sahakian V.,
Salzmann H., Santangelo A., Sasaki M., Schafer J., Schussler F.,
Schutte H.M., Shapopi J.N.S., Sharma A., Sol H., Spencer S., Stawarz L.,
Steppa C., Streil K., Suzuki H., Takahashi T., Tanaka T., Taylor A.M.,
Terrier R., Tluczykont M., Tsirou M., van Eldik C., Vecchi M., Wach T.,
Wagner S.J., Wierzcholska A., Zacharias M., Zdziarski A.A., Zech A.,
Zywucka N., (H.E.S.S. Collaboration),
Abe S., Abhir J., Abhishek A., Acciari V.A., Aguasca-Cabot A., Agudo I.,
Aniello T., Ansoldi S., Antonelli L.A., Arbet Engels A., Arcaro C.,
Artero M., Asano K., Babic A., Barres de Almeida U., Barrio J.A.,
Batkovic I., Bautista A., Baxter J., Becerra Gonzalez J., Bednarek W.,
Bernardini E., Bernete J., Berti A., Besenrieder J., Bigongiari C.,
Biland A., Blanch O., Bonnoli G., Bosnjak Z., Bronzini E., Burelli I.,
Busetto G., Campoy-Ordaz A., Carosi A., Carosi R., Carretero-Castrillo M.,
Castro-Tirado A.J., Cerasole D., 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., Delfino M.,
Delgado J., Delgado Mendez C., Di Pierro F., Di Tria R., Di Venere L.,
Dominis Prester D., Donini A., Dorner D., Doro M., Elsaesser D.,
Escudero J., Farina L., Fattorini A., Foffano L., Font L., Frose S.,
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., Gradetzke T., Grau R., Green J.G., Gunther P., Hadasch D.,
Hahn A., Hassan T., Heckmann L., Herrera Llorente J., Hrupec D., Imazawa R.,
Ishio K., Jimenez Martinez I., Jormanainen J., Kayanoki T., Kerszberg D.,
Kluge G.W., Kobayashi Y., Kouch P.M., Kubo H., Kushida J., Lainez M.,
Lamastra A., Leone F., Lindfors E., Lombardi S., 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.,
Martinez-Chicharro M., Mas-Aguilar A., 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., Nickel L., Nievas Rosillo M., Nigro C., Nikolic L.,
Nilsson K., Nishijima K., Njoh Ekoume T., Noda K., Nozaki S., Ohtani Y.,
Okumura A., Otero-Santos J., Paiano S., Paneque D., Paoletti R.,
Paredes J.M., Peresano M., Persic M., Pihet M., Pirola G., Podobnik F.,
Prada Moroni P.G., Prandini E., Priyadarshi C., Ribo M., Rico J., Righi C.,
Sahakyan N., Saito T., Saturni F.G., Schmidt K., Schmuckermaier F.,
Schubert J.L., Schweizer T., Sciaccaluga A., Silvestri G., Sitarek J.,
Sliusar V., Sobczynska D., Spolon A., Stamerra A., Striskovic J., Strom D.,
Strzys M., Suda Y., Suutarinen S., Tajima H., Takahashi M., Takeishi R.,
Tavecchio F., Temnikov P., Terauchi K., Terzic T., Teshima M., Truzzi S.,
Tutone A., Ubach S., van Scherpenberg J., Vazquez Acosta M., Ventura S.,
Verna G., Viale I., Vigorito C.F., Vitale V., Vovk I., Walter R., Will M.,
Wunderlich C., Yamamoto T., (MAGIC Collaboration),
Acharyya A., Adams C.B., Bangale P., Bartkoske J.T., Benbow W.,
Christiansen J.L., Duerr A., Errando M., Feng Q., Foote G.M., Fortson L.,
Furniss A., Hanlon W., Hervet O., Hinrichs C.E., Holder J., Humensky T.B.,
Jin W., Johnson M.N., Kaaret P., Kertzman M., Kieda D., Kleiner T.K.,
Korzoun N., Krennrich F., Kumar S., Lang M.J., Lundy M., Maier G.,
McGrath C.E., Millard M.J., Mooney C.L., Moriarty P., Mukherjee R., Ning W.,
O'Brien S., Ong R.A., Pohl M., Pueschel E., Quinn J., Ragan K.,
Reynolds P.T., Ribeiro D., Roache E., Ryan J.L., Sadeh I., Saha L.,
Sembroski G.H., Shang R., Splettstoesser M., Talluri A.K., Tucci J.V.,
Valverde J., Vassiliev V., Williams D.A., Wong S.L.,
(VERITAS Collaboration),
Chen Z., Cui L., Hirota T., Li B., Li G., Liu Q., Liu X., Liu Z., Ma J.,
Niinuma K., Ro H., Sakai N., Sawada-Satoh S., Wajima K., Wang J., Wang N.,
Xia B., Yan H., Yonekura Y., Zhang H., Zhao R., Zhong W.,
(EAVN Collaboration)
<Astron. Astrophys. 692, A140 (2024)>
=2024A&A...692A.140A 2024A&A...692A.140A (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Radio sources ; Photometry ; Optical
Keywords: galaxies: active - galaxies: individual: M87 - galaxies: jets -
galaxies: nuclei
Abstract:
The nearby elliptical galaxy M87 contains one of the only two
supermassive black holes whose emission surrounding the event horizon
has been imaged by the Event Horizon Telescope (EHT). In 2018, more
than two dozen multi-wavelength (MWL) facilities (from radio to
gamma-ray energies) took part in the second M87 EHT campaign.
The goal of this extensive MWL campaign was to better understand the
physics of the accreting black hole M87*, the relationship between
the inflow and inner jets, and the high-energy particle acceleration.
Understanding the complex astrophysics is also a necessary first step
towards performing further tests of general relativity.
The MWL campaign took place in April 2018, overlapping with the EHT
M87* observations. We present a new, contemporaneous spectral energy
distribution (SED) ranging from radio to very high energy (VHE)
gamma-rays, as well as details of the individual observations and
light curves. We also conduct phenomenological modelling to
investigate the basic source properties.
We present the first VHE gamma-ray flare from M87 detected since 2010.
The flux above 350GeV has more than doubled within a period
of ∼36 hours. We find that the X-ray flux is enhanced by about a
factor of two compared to 2017, while the radio and millimetre core
fluxes are consistent between 2017 and 2018.We detect evidence for a
monotonically increasing jet position angle that corresponds to
variations in the bright spot of the EHT image.
Our results show the value of continued MWL monitoring together with
precision imaging for addressing the origins of high-energy
particle acceleration. While we cannot currently pinpoint the precise
location where such acceleration takes place, the new VHE gamma-ray
flare already presents a challenge to simple one-zone leptonic
emission model approaches, and emphasises the need for combined image
and spectral modelling.
Description:
The 2018 EHT observations of M87 were made in April 2018
using a total of 8 stations (in 6 geographical locations) across the
globe. While observations were performed over 4 nights (April 21, 22,
25 and 28), the second and last sessions suffered from various issues
(bad weather conditions across the array, poor baseline coverage,
etc.). Therefore, reliable EHT images of M87* could only be obtained
from the data taken on April 21 and 25.
Flux results for each individual facility involved in the
observational campaign.
Further material:
- SEDMWLtable1.dat : Broadband MWL SED (see Fig. 18 in the paper)
- SEDmodelAPL_EHT.dat : Model A - for the EHT region considering a
Power Law emission for Chandra+NuSTAR (see Fig. 19 in the paper)
- SEDmodelAPL_HE.dat : Model A - for the High-Energy region considering a
Power Law emission for Chandra+NuSTAR (see Fig. 19 in the paper)
- SEDmodelABPL_EHT.dat : Model A - for the EHT region considering a
Broken Power Law emission for Chandra+NuSTAR (see Fig. 21 in the paper)
- SEDmodelABPL_HE.dat : Model A - for the High-Energy region considering
a Broken Power Law emission for Chandra+NuSTAR (see Fig. 21 in the paper)
- SED_modelB.dat : Model B (see Fig. 20 in the paper)
- Broadband spectrum table with frequency, flux density, its
uncertainty, and instrument index (format: DAT)
- Sampled posterior distributions of the SED broadband spectral
model (A-PL) described in Section 4.2 (format: DAT).
- Sampled posterior distributions of the SED broadband spectral
model (A-BPL) described in Section 4.3 (format: DAT).
- Sampled posterior distributions of the SED broadband spectral
model (B) described in Section 4.3 (format: DAT).
Objects:
-----------------------------------------
RA (2000) DE Designation(s)
-----------------------------------------
12 30 49.42 +12 23 28.0 M87 = NGC 4486
-----------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablec1.dat 70 76 Summary of radio cm-mm observations
tablec2.dat 70 38 *Summary of ALMA 2018 and SMA 2017/2018
mm observations
tablec3.dat 31 5 Kanata optical flux values for the wavelength
of 634.9nm (or 4.7 x 1014Hz)
tablec4.dat 31 7 Kanata NIR flux values for the wavelength
of 1250nm (or 2.4 x 1014Hz)
tablec5.dat 68 9 Optical and UV flux densities.
tablec6.dat 68 1 Optical and UV flux densities of the host galaxy
tablec7.dat 100 1 HST results of M87 observation in 2018 July
tablec8.dat 90 1 *The UVIT results of observations from
observations in April 2018
tablec9.dat 69 2 *The spectral results from -SXT observations
(0.3-8 keV) in April 2018
tablec10.dat 58 9 Observations and Fluxes
tablec11.dat 26 5 Chandra core fluxes for the observations
performed in 2017 and 2018
tablec12.dat 21 20 Chandra+NuSTAR spectral values for stacked
observation, normalised on 2018 emission
tablec14.dat 56 17 VHE gamma-ray Observation Summary
fmat/* . 5 Further material
--------------------------------------------------------------------------------
Note on tablec2.dat: a full description of the data processing, imaging, and
analysis see Goddi2019,Goddi2021.
Note on tablec8.dat: A region of 5" is used to make these estimations.
Note on tablec9.dat: A region of 15' centred on 87 coordinates is used as
the source region.
--------------------------------------------------------------------------------
Description of file: fmat/SEDmodelABPL_EHT.dat (Fig. 21 in the paper)
fmat/SEDmodelAPL_EHT.dat (Fig. 19 in the paper)
fmat/SEDmodelAPL_HE.dat (Fig. 19 in the paper)
--------------------------------------------------------------------------------
Byte-by-byte Description of file (#): fmat/*ABPLEHT.datfmat/*APL*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 E8.3 Hz Freq Frequency
17- 31 E15.9 mW/m2 Flux1 SYN-EHT flux
33- 41 E9.3 mW/m2 Flux2 SSC-EHT flux
49- 56 E8.3 mW/m2 Flux3 Sum-EHT flux
--------------------------------------------------------------------------------
Description of file: fmat/SED_modelB.dat (Fig. 20 in the paper)
--------------------------------------------------------------------------------
Byte-by-byte Description of file (#): fmat/SED_modelB.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
4- 19 E16.11 Hz Freq Frequency
22- 37 E16.11 mW/m2 Flux1 EHT oriented flux
40- 55 E16.11 mW/m2 Flux2 SYN-EHT flux
58- 73 E16.11 mW/m2 Flux3 SSC-EHT flux
76- 91 E16.11 mW/m2 Flux4 HE oriented flux
94-109 E16.11 mW/m2 Flux5 SYN-HE flux
112-127 E16.11 mW/m2 Flux6 SSC-HE flux
130-145 E16.11 mW/m2 Flux7 VHE-flare oriented flux
148-163 E16.11 mW/m2 Flux8 SYN-EHT flux
166-181 E16.11 mW/m2 Flux9 SSC-EHT flux
184-199 E16.11 mW/m2 Flux10 EHT+HE flux
202-217 E16.11 mW/m2 Flux11 EHT+HE+VHE flare flux
--------------------------------------------------------------------------------
--------------------------------------------------------------------------------
Table C13: Fermi-LAT fluxes for the customised-bin light curve analysis on
April 2018.
--------------------------------------------------------------------------------
MJD Significance Flux in the 0.1-1000GeV band
(σ) (10-8ph/cm2/s)
58216-58227 2.9 < 7.1
58227-58231 4.5 10.8±3.8
58231-58244 1.1 < 5.9
--------------------------------------------------------------------------------
--------------------------------------------------------------------------------
Table C15:
Results of PL fit of the spectra measured with HESS, MAGIC and VERITAS.
--------------------------------------------------------------------------------
IACT f0 E0 Γ_VHE energy range
±fstat±fsyst ±Γstat
±Γsyst
(10-12/TeV/cm2/s) [TeV] [TeV]
--------------------------------------------------------------------------------
HESS 0.74±0.06±0.15 1.27 2.05±0.11±0.10 0.31-6.90
MAGIC 17.4 ±3.3 ±1.91 0.27 2.57±0.34±0.15 0.05-1.00
VERITAS 0.83±0.16±0.21 1 2.41±0.30±0.20 0.31-3.00
--------------------------------------------------------------------------------
The notes "stat" and "syst" means statistical error and systematic error,
respectively.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec1.dat tablec2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- Sample Sample (1)
3- 16 A14 --- ObsCode Observatopn code
20 A1 --- n_ObsCode [a] Note (2)
22- 31 A10 "date" ObsDate Observation date
33- 37 I5 d MJD Modified Julin date of observation
42- 46 F5.1 GHz Freq Observed frequency
49- 53 F5.3 Jy/beam BPeak Peak Brightness at Freq
55- 59 F5.3 Jy/beam e_BPeak Peak Brightness at Freq error
62- 65 F4.2 Jy STot ? Total Flux Density at Freq
67- 70 F4.2 Jy e_STot ? Total Flux Density at Freq error
--------------------------------------------------------------------------------
Note (1): Sample as follows:
A = VERA (beam: 1.0 mas circ.)
B = EAVN/KaVA (beam: 1.0/0.5 mas circ. at 24/43GHz
C = VLBA (beam: 1.0/0.5 mas circ. at 24/43GHz)
D = KVN (beam: 1.0 mas circ. at 22/43/86/129GHz)
E = Global 43GHz VLBI (beam: 0.25mas circ.)
F = DGMVA+ALMA (beam: 0.20mas circ.)
G = ALMA (beam: ∼2.5" at 93 GHz and ∼1-1.5" at 221 GHz)
H = SMA (proj. baselines > 30 kλ; Θ < 6.8")
Note (2): Note as follows:
a = Corrected for the 22GHz receiver phase instability issue
(see text for details)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec3.dat tablec4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 "date" Obs.date Observation date
12- 19 F8.2 d Time Modified Julian date of observation
21- 25 F5.3 mJy Flux Flux
27- 31 F5.3 mJy FluxCorr Corrected flux (1)
--------------------------------------------------------------------------------
Note (1): Flux that corrects interstellar-extinction in our galaxy
(AR = 0.049, AJ = 0.016).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec5.dat tablec6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.1 d ObsDate ? Observation modified Julian date
9- 13 F5.2 mJy FV ? Flux in V band
15- 18 F4.2 mJy e_FV ? Flux in V band error
20- 23 F4.2 mJy FB Flux in B band
25- 28 F4.2 mJy e_FB Flux in B band error
30- 33 F4.2 mJy FU Flux in U band
35- 38 F4.2 mJy e_FU Flux in U band error
40- 43 F4.2 mJy FUVW1 Flux in UVW1 band
45- 48 F4.2 mJy e_FUVW1 Flux in UVW1 band error
50- 53 F4.2 mJy FUVM2 ? Flux in UVW1 band
55- 58 F4.2 mJy e_FUVM2 ? Flux in UVW1 band error
60- 63 F4.2 mJy FUVW2 Flux in UVW2 band
65- 68 F4.2 mJy e_FUVW2 Flux in UVW2 band error
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 "date" Obs.date Observation date
12- 14 I3 s TExp Exposure time
16- 21 A6 --- Filter Filter name
23- 28 F6.1 0.1nm lambda Effective wavelength (1)
30- 37 E8.3 mW/m2 Fluxcore Core flux (1)
39- 46 E8.3 mW/m2 e_Fluxcore Core flux error (1)
48- 55 E8.3 mW/m2 FluxHST HST flux (1)
57- 64 E8.3 mW/m2 e_FluxHST HST flux error (1)
66- 73 E8.3 mW/m2 NetFluxcore Core net flux (2)
75- 82 E8.3 mW/m2 e_NetFluxcore Core net flux error (2)
84- 91 E8.3 mW/m2 NetFluxHST HST net flux (2)
93-100 E8.3 mW/m2 e_NetFluxHST HST net flux error (2)
--------------------------------------------------------------------------------
Note (1): Flux is uncorrected for contribution of the host galaxy.
Note (2): Flux is corrected for contribution of the host galaxy.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 "date" ObsDate Observation date
12- 15 F4.1 ks TExp Exposure time
17- 20 A4 --- Filter Filter
22- 25 I4 0.1nm lambda Effective wavelength
27- 29 I3 0.1nm Dlambda Δλ
31- 36 F6.3 --- ZPT Zero-point used
38- 41 F4.2 --- e_ZPT Zero-point used error
43- 47 F5.2 mag mag1 Magnitude Code+HST1+Jet+Host
49- 52 F4.2 mag e_mag1 Magnitude Code+HST1+Jet+Host error
54- 59 F6.3 mag mag2 Magnitude Jet+Hostmod
61- 66 F6.3 mag mag3 Magnitude Code+Hostobs
68- 72 F5.3 mag e_mag3 Magnitude Code+Hostobs error
74- 81 E8.4 0.1mW/m2/nm FBaF2 BaF2 flux
83- 90 E8.4 0.1mW/m2/nm e_FBaF2 BaF2 flux error
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Byte-by-byte Description of file: tablec9.dat
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Bytes Format Units Label Explanations
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1- 10 A10 "date" ObsDate Observation date
12- 15 F4.1 ks TExp Exposure time
17- 23 F7.1 d MJD Observation modified Julian date
25- 28 F4.2 --- alphaC Powerlaw index for Core
29 A1 --- n_alphaC [f] Note on alphaC (1)
31- 34 F4.2 10-3ph/cm2/s/keV NC Normalisation for Core
36- 39 F4.2 10-3ph/cm2/s/keV e_NC Normalisation for Core error
40- 43 F4.2 --- alphaH Powerlaw index for HST1
44 A1 --- n_alphaH [f] Note on alphaH (1)
46- 49 F4.2 10-3ph/cm2/s/keV NH Normalisation for HST1
51- 54 F4.2 10-3ph/cm2/s/keV e_NH Normalisation for HST1 error
56- 59 F4.2 --- alphaJ Powerlaw index for Jet
60 A1 --- n_alphaJ [f] Note on alphaJ (1)
62- 65 F4.2 10-3ph/cm2/s/keV NJ Normalisation for Jet
67- 69 F3.1 10-3ph/cm2/s/keV e_NJ Normalisation for Jet error
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Note (1): f = fixed to the chandra+nustar values.
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Byte-by-byte Description of file: tablec10.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 I11 --- Obs Observation ID
13- 22 F10.4 d MJD Observation modified Julian date
24- 27 F4.2 ks Tesp Exposure time
29- 33 F5.2 10-15W/m2 Ftot Total Flux in 2-10keV band (1)
35- 38 F4.2 10-15W/m2 e_Ftot Total Flux in 2-10keV band lower error (1)
40- 43 F4.2 10-15W/m2 E_Ftot Total Flux in 2-10keV band upper error (1)
45- 48 F4.2 10-15W/m2 FBet Net Flux in 2-10keV band (2)
50- 53 F4.2 10-15W/m2 e_FBet Net Flux in 2-10keV band lower error (2)
55- 58 F4.2 10-15W/m2 E_FBet Net Flux in 2-10keV band upper error (2)
--------------------------------------------------------------------------------
Note (1): flux represents the flux derived from the spectral fits including all
large-scale emission from the surrounding galaxy and cluster.
Note (2): Net flux corresponds to the flux from the core,
the HST-1 knot, and jet, excluding larger-scale emission.
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Byte-by-byte Description of file: tablec11.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- ObsID Observation ID
9- 16 F8.2 d MJD Modified Julian date of observation
18- 21 F4.2 10-15W/m2 Flux Core flux estimated in the 2-10keV band
23- 26 F4.2 10-15W/m2 e_Flux Core flux estimated in the 2-10keV band error
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Byte-by-byte Description of file: tablec12.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 keV Energy Energy band
13- 16 F4.2 10-15W/m2 Flux Core flux estimate
18- 21 F4.2 10-15W/m2 e_Flux Core flux estimate error
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Byte-by-byte Description of file: tablec14.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- IACT Instrument
9- 16 F8.2 d Start Time (MJD)
18- 25 F8.2 d Stop Time (MJD)
27- 30 F4.2 h ObsTime Effective observation time
32- 36 A5 deg ZA Zenith angle
38- 41 F4.2 --- Signi Significance (in sigma unit)
43- 46 F4.2 10-12ph/cm2/s Flux Flux at E>350GeV
48- 51 F4.2 10-12ph/cm2/s E_Flux Error on Flux (upper value) (1)
53- 56 F4.2 10-12ph/cm2/s e_Flux Error on Flux (lower value) (1)
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Note (1): Only statistical 1σ errors on the fluxes are given.
95% confidence level upper limits are given for flux measurements
with less than 2σ significance.
--------------------------------------------------------------------------------
Acknowledgements:
Giacomo Principe, giacomo.principe(at)inaf.it
(End) Patricia Vannier [CDS] 04-Sep-2024