RT Journal Article
T1 Very-high-energy gamma-ray observations of the Type Ia Supernova SN 2014J with the MAGIC telescopes
A1 Antoranz Canales, Pedro
A1 Barrio Uña, Juan Abel
A1 Bonnefoy, Simon Francois Albert
A1 Contreras González, José Luis
A1 Domínguez, A.
A1 Fidalgo, D.
A1 Fonseca González, Mª Victoria
A1 López Moya, Marcos
A1 Miranda Pantoja, José Miguel
A1 Nievas Rosillo, Mireia
AB Context. In this work we present data from observations with the MAGIC telescopes of SN 2014J detected in January 21 2014, the closest Type Ia supernova since Imaging Air Cherenkov Telescopes started to operate.Aims. We probe the possibility of very-high-energy (VHE; E ≥ 100 GeV) gamma rays produced in the early stages of Type Ia supernova explosions.Methods. We performed follow-up observations after this supernova explosion for 5 days, between January 27 and February 2 in 2014. We search for gamma-ray signal in the energy range between 100 GeV and several TeV from the location of SN 2014J using data from a total of ∼ 5.5 hours of observations. Prospects for observing gamma-rays of hadronic origin from SN 2014J in the near future are also being addressed.Results. No significant excess was detected from the direction of SN 2014J. Upper limits at 95% confidence level on the integral flux, assuming a power-law spectrum, dF/dE ∝ E −Γ , with a spectral index of Γ = 2.6, for energies higher than 300 GeV and 700 GeV, are established at 1.3 × 10−12 and 4.1 × 10−13 photons cm−2 s −1 , respectively. Conclusions. For the first time, upper limits on the VHE emission of a Type Ia supernova are established. The energy fraction isotropically emitted into TeV gamma rays during the first ∼ 10 days after the supernova explosion for energies greater than 300 GeV is limited to 10−6 of the total available energy budget (∼ 1051 erg). Within the assumed theoretical scenario, the MAGIC upper limits on the VHE emission suggest that SN 2014J will not be detectable in the future by any current or planned generation of Imaging Atmospheric Cherenkov Telescopes.
PB EDP Sciencies
SN 1432-0746
YR 2017
FD 2017-06
LK https://hdl.handle.net/20.500.14352/18340
UL https://hdl.handle.net/20.500.14352/18340
LA eng
NO © ESO 2017. Artículo firmado por 153 autores. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015- 68278-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210- C6-6-R, AYA2013-47447-C3-1-P, AYA2015-71042-P, ESP2015-71662-C2-2-P, CSD2009-00064), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia “Severo Ochoa” SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia “María de Maeztu” MDM-2014-0369, by grant 268740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzW grant 745/NHESS-MAGIC/2010/0.
NO Ministerio de Economía y Competitividad (MINECO)
NO German BMBF
NO German MPG
NO Italian INFN
NO Italian INAF
NO Swiss National Fund SNF
NO Japanese JSPS
NO Japanese MEXT
NO Spanish Centro de Excelencia “Severo Ochoa”
NO Unidad de Excelencia “María de Maeztu”
NO Academy of Finland
NO Croatian Science Foundation (HrZZ)
NO University of Rijeka
NO DFG Collaborative Research Centers
NO Polish MNiSzW
DS Docta Complutense
RD 17 ago 2024