Hyppää sisältöön
    • Suomeksi
    • In English
  • Suomeksi
  • In English
  • Kirjaudu
Näytä aineisto 
  •   Etusivu
  • 3. UTUCris-artikkelit
  • Rinnakkaistallenteet
  • Näytä aineisto
  •   Etusivu
  • 3. UTUCris-artikkelit
  • Rinnakkaistallenteet
  • Näytä aineisto
JavaScript is disabled for your browser. Some features of this site may not work without it.

Monitoring of the radio galaxy M 87 during a low -emission state from m 2012 to 2015 with MAGIC

Acciari VA; Ansoldi S; Antonelli LA; Engels AA; Arcaro C; Baack D; Babic A; Banerjee B; Bangale P; de Almeida UB; Barrio JA; Gonzalez JB; Bednarek W; Bellizzi L; Bernardini E; Berti A; Besenrieder J; Bhattacharyya W; Bigongiari C; Biland A; Blanch O; Bonnoli G; Bosnjak Z; Busetto G; Carosi R; Ceribella G; Chai Y; Chilingaryan A; Cikota S; Colak SM; Colin U; Colombo E; Contreras JL; Cortina J; Covino S; D'Elia V; Da Vela P; Dazzi F; De Angelis A; De Lotto B; Delfino M; Delgado J; Depaoli D; Di Pierro F; Di Venere L; Espineira ED; Prester DD; Donini A; Dorner D; Doro M; Elsaesser D; Ramazani VF; Fattorini A; Fernandez-Barral A; Ferrara G; Fidalgo D; Foffano L; Fonseca MV; Font L; Fruck C; Fukami S; Lopez RJG; Garczarczyk M; Gasparyan S; Gaug M; Giglietto N; Giordano F; Godinovic N; Green D; Guberman D; Hadasch D; Hahn A; Herrera J; Hoang J; Hrupec D; Hutten M; Inada T; Inoue S; Ishio K; Iwamura Y; Jouvin L; Kerszberg D; Kubo H; Kushida J; Lamastra A; Lelas D; Leone F; Lindfors E; Lombardi S; Longo F; Lopez M; Lopez-Coto R; Lopez-Oramas A; Loporchio S; Fraga BMD; Maggio C; Majumdar P; Makariev M; Mallamaci M; Maneva G; Manganaro M; Mannheim K; Maraschi L; Mariotti M; Martinez M; Masuda S; Mazin D; Micanovic S; Miceli D; Minev M; Miranda JM; Mirzoyan R; Molina E; Moralejo A; Morcuende D; Moreno V; Moretti E; Munar-Adrover P; Neustroev V; Nigro C; Nilsson K; Ninci D; Nishijima K; Noda K; Nogues L; Nothe M; Nozaki S; Paiano S; Palacio J; Palatiello M; Paneque D; Paoletti R; Paredes JM; Penil P; Peresano M; Persic M; Moroni PGP; Prandini E; Puljak I; Rhode W; Ribo M; Rico J; Righi C; Rugliancich A; Saha L; Sahakyan N; Saito T; Sakurai S; Satalecka K; Schmidt K; Schweizer T; Sitarek J; Snidaric I; Sobczynska D; Somero A; Stamerra A; Strom D; Strzys M; Suda Y; Suric T; Takahashi M; Tavecchio F; Temnikov P; Terzic T; Teshima M; Torres-Alba N; Tosti L; Tsujimoto S; Vagelli V; van Scherpenberg J; Vanzo G; Acosta MV; Vigorito CF; Vitale V; Vovk I; Will M; Zaric D; Asano K; Hada K; Harris DE; Giroletti M; Jermak HE; Madrid JP; Massaro F; Richter S; Spanier F; Steele IA; Walker RC; Spanier F; Steele IA; Massaro F; Richter S; Walker RC; Jermak HE; Madrid JP

Monitoring of the radio galaxy M 87 during a low -emission state from m 2012 to 2015 with MAGIC

Acciari VA
Ansoldi S
Antonelli LA
Engels AA
Arcaro C
Baack D
Babic A
Banerjee B
Bangale P
de Almeida UB
Barrio JA
Gonzalez JB
Bednarek W
Bellizzi L
Bernardini E
Berti A
Besenrieder J
Bhattacharyya W
Bigongiari C
Biland A
Blanch O
Bonnoli G
Bosnjak Z
Busetto G
Carosi R
Ceribella G
Chai Y
Chilingaryan A
Cikota S
Colak SM
Colin U
Colombo E
Contreras JL
Cortina J
Covino S
D'Elia V
Da Vela P
Dazzi F
De Angelis A
De Lotto B
Delfino M
Delgado J
Depaoli D
Di Pierro F
Di Venere L
Espineira ED
Prester DD
Donini A
Dorner D
Doro M
Elsaesser D
Ramazani VF
Fattorini A
Fernandez-Barral A
Ferrara G
Fidalgo D
Foffano L
Fonseca MV
Font L
Fruck C
Fukami S
Lopez RJG
Garczarczyk M
Gasparyan S
Gaug M
Giglietto N
Giordano F
Godinovic N
Green D
Guberman D
Hadasch D
Hahn A
Herrera J
Hoang J
Hrupec D
Hutten M
Inada T
Inoue S
Ishio K
Iwamura Y
Jouvin L
Kerszberg D
Kubo H
Kushida J
Lamastra A
Lelas D
Leone F
Lindfors E
Lombardi S
Longo F
Lopez M
Lopez-Coto R
Lopez-Oramas A
Loporchio S
Fraga BMD
Maggio C
Majumdar P
Makariev M
Mallamaci M
Maneva G
Manganaro M
Mannheim K
Maraschi L
Mariotti M
Martinez M
Masuda S
Mazin D
Micanovic S
Miceli D
Minev M
Miranda JM
Mirzoyan R
Molina E
Moralejo A
Morcuende D
Moreno V
Moretti E
Munar-Adrover P
Neustroev V
Nigro C
Nilsson K
Ninci D
Nishijima K
Noda K
Nogues L
Nothe M
Nozaki S
Paiano S
Palacio J
Palatiello M
Paneque D
Paoletti R
Paredes JM
Penil P
Peresano M
Persic M
Moroni PGP
Prandini E
Puljak I
Rhode W
Ribo M
Rico J
Righi C
Rugliancich A
Saha L
Sahakyan N
Saito T
Sakurai S
Satalecka K
Schmidt K
Schweizer T
Sitarek J
Snidaric I
Sobczynska D
Somero A
Stamerra A
Strom D
Strzys M
Suda Y
Suric T
Takahashi M
Tavecchio F
Temnikov P
Terzic T
Teshima M
Torres-Alba N
Tosti L
Tsujimoto S
Vagelli V
van Scherpenberg J
Vanzo G
Acosta MV
Vigorito CF
Vitale V
Vovk I
Will M
Zaric D
Asano K
Hada K
Harris DE
Giroletti M
Jermak HE
Madrid JP
Massaro F
Richter S
Spanier F
Steele IA
Walker RC
Spanier F
Steele IA
Massaro F
Richter S
Walker RC
Jermak HE
Madrid JP
Katso/Avaa
Publisher's PDF (729.5Kb)
Lataukset: 

OXFORD UNIV PRESS
doi:10.1093/mnras/staa014
Näytä kaikki kuvailutiedot
Julkaisun pysyvä osoite on:
https://urn.fi/URN:NBN:fi-fe2021042822485
Tiivistelmä
M 87 is one of the closest (z = 0.004 36) extragalactic sources emitting at very high energies (VHF, E > 100 GeV). The aim of this work is to locale the region of the VHF gamma-ray emission and to describe the observed broad-band spectral energy distribution (SED) during the low VHF gamma-ray state. The data from M 87 collected between 2012 and 2015 as part of a MAGIC monitoring programme are analysed and combined with multiwavelength data from Fermi-LAT, Chandra, HST, FVN, VLBA, and the Liverpool Telescope. The averaged VHE gamma-ray spectrum can be fitted from 100 GeV to 10 TeV with a simple power law with a photon index of (-2.41 0.07), while the integral flux above 300 GeV is (1.44 0.13) x 10-12 cm 2 s I. During the campaign between 2012 and 2015, M87 is generally found in a low-emission state at all observed wavelengths. The VIIE gamma-ray flux from the present 2012-2015M 87 campaign is consistent with a constant flux with some hint of variability ( 3 a) on a daily time-scale in 2013. The low-state gamma-ray emission likely originates from the same region as the flare-state emission. Given the broad-band SED, both a leptonic synchrotron self-Compton and a hybrid photohadronic model reproduce the available data well, even if the latter is preferred. We note, however, that the energy stored in the magnetic field in the leptonic scenario is very low, suggesting a matter-dominated emission region.
Kokoelmat
  • Rinnakkaistallenteet [27094]

Turun yliopiston kirjasto | Turun yliopisto
julkaisut@utu.fi | Tietosuoja | Saavutettavuusseloste
 

 

Tämä kokoelma

JulkaisuajatTekijätNimekkeetAsiasanatTiedekuntaLaitosOppiaineYhteisöt ja kokoelmat

Omat tiedot

Kirjaudu sisäänRekisteröidy

Turun yliopiston kirjasto | Turun yliopisto
julkaisut@utu.fi | Tietosuoja | Saavutettavuusseloste