Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S.

The γ-ray pulsar PSR B1706-44 and the adjacent supernova remnant (SNR) candidate G343.1-2.3 were observed by H.E.S.S. during a dedicated observation campaign in 2007. As a result of this observation campaign, a new source of very-high-energy (VHE; E > 100 GeV) γ-ray emission, H.E.S.S.J1708-44...

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Detalles Bibliográficos
Autor principal: Abramowski, A.
Formato: JOUR
Materias:
gamma rays: general
ISM: individual objects: G343.1-2.3
pulsars: individual: PSRB1706-44
Germanium compounds
Optical transfer function
Pulsars
Spectrum analysis
Tellurium compounds
Gamma rays: generals
Gamma-ray emission
Pulsar wind nebula
Pulsars: individuals
Statistical significance
Supernova remnants
Very high energies
Gamma rays
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_00046361_v528_n_p_Abramowski
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id todo:paper_00046361_v528_n_p_Abramowski
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spelling todo:paper_00046361_v528_n_p_Abramowski2023-10-03T14:00:34Z Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S. Abramowski, A. gamma rays: general ISM: individual objects: G343.1-2.3 pulsars: individual: PSRB1706-44 Germanium compounds Optical transfer function Pulsars Spectrum analysis Tellurium compounds Gamma rays: generals Gamma-ray emission ISM: individual objects: G343.1-2.3 Pulsar wind nebula Pulsars: individuals Statistical significance Supernova remnants Very high energies Gamma rays The γ-ray pulsar PSR B1706-44 and the adjacent supernova remnant (SNR) candidate G343.1-2.3 were observed by H.E.S.S. during a dedicated observation campaign in 2007. As a result of this observation campaign, a new source of very-high-energy (VHE; E > 100 GeV) γ-ray emission, H.E.S.S.J1708-443, was detected with a statistical significance of 7σ, although no significant point-like emission was detected at the position of the energetic pulsar itself. In this paper, the morphological and spectral analyses of the newly-discovered TeV source are presented. The centroid of H.E.S.S.J1708-443 is considerably offset from the pulsar and located near the apparent center of the SNR, at αJ2000 = 17h08 m11s ± 17s and δJ2000 = -44°20′ ± 4′. The source is found to be significantly more extended than the H.E.S.S. point spread function (∼0.1°), with an intrinsic Gaussian width of 0.29° ± 0.04°. Its integral flux between 1 and 10 TeV is ~ 3.8 × 10-12 ph cm-2 s -1, equivalent to 17% of the Crab Nebula flux in the same energy range. The measured energy spectrum is well-fit by a power law with a relatively hard photon index Γ = 2.0 ± 0.1stat ± 0.2 sys. Additional multi-wavelength data, including 330 MHz VLA observations, were used to investigate the VHE γ-ray source's possible associations with the pulsar wind nebula of PSR B1706-44 and/or with the complex radio structure of the partial shell-type SNR G 343.1-2.3. © 2011 ESO. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00046361_v528_n_p_Abramowski
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic gamma rays: general
ISM: individual objects: G343.1-2.3
pulsars: individual: PSRB1706-44
Germanium compounds
Optical transfer function
Pulsars
Spectrum analysis
Tellurium compounds
Gamma rays: generals
Gamma-ray emission
ISM: individual objects: G343.1-2.3
Pulsar wind nebula
Pulsars: individuals
Statistical significance
Supernova remnants
Very high energies
Gamma rays
spellingShingle gamma rays: general
ISM: individual objects: G343.1-2.3
pulsars: individual: PSRB1706-44
Germanium compounds
Optical transfer function
Pulsars
Spectrum analysis
Tellurium compounds
Gamma rays: generals
Gamma-ray emission
ISM: individual objects: G343.1-2.3
Pulsar wind nebula
Pulsars: individuals
Statistical significance
Supernova remnants
Very high energies
Gamma rays
Abramowski, A.
Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S.
topic_facet gamma rays: general
ISM: individual objects: G343.1-2.3
pulsars: individual: PSRB1706-44
Germanium compounds
Optical transfer function
Pulsars
Spectrum analysis
Tellurium compounds
Gamma rays: generals
Gamma-ray emission
ISM: individual objects: G343.1-2.3
Pulsar wind nebula
Pulsars: individuals
Statistical significance
Supernova remnants
Very high energies
Gamma rays
description The γ-ray pulsar PSR B1706-44 and the adjacent supernova remnant (SNR) candidate G343.1-2.3 were observed by H.E.S.S. during a dedicated observation campaign in 2007. As a result of this observation campaign, a new source of very-high-energy (VHE; E > 100 GeV) γ-ray emission, H.E.S.S.J1708-443, was detected with a statistical significance of 7σ, although no significant point-like emission was detected at the position of the energetic pulsar itself. In this paper, the morphological and spectral analyses of the newly-discovered TeV source are presented. The centroid of H.E.S.S.J1708-443 is considerably offset from the pulsar and located near the apparent center of the SNR, at αJ2000 = 17h08 m11s ± 17s and δJ2000 = -44°20′ ± 4′. The source is found to be significantly more extended than the H.E.S.S. point spread function (∼0.1°), with an intrinsic Gaussian width of 0.29° ± 0.04°. Its integral flux between 1 and 10 TeV is ~ 3.8 × 10-12 ph cm-2 s -1, equivalent to 17% of the Crab Nebula flux in the same energy range. The measured energy spectrum is well-fit by a power law with a relatively hard photon index Γ = 2.0 ± 0.1stat ± 0.2 sys. Additional multi-wavelength data, including 330 MHz VLA observations, were used to investigate the VHE γ-ray source's possible associations with the pulsar wind nebula of PSR B1706-44 and/or with the complex radio structure of the partial shell-type SNR G 343.1-2.3. © 2011 ESO.
format JOUR
author Abramowski, A.
author_facet Abramowski, A.
author_sort Abramowski, A.
title Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S.
title_short Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S.
title_full Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S.
title_fullStr Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S.
title_full_unstemmed Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S.
title_sort detection of very-high-energy γ-ray emission from the vicinity of psrb1706-44 and g343.1-2.3 with h.e.s.s.
url http://hdl.handle.net/20.500.12110/paper_00046361_v528_n_p_Abramowski
work_keys_str_mv AT abramowskia detectionofveryhighenergygrayemissionfromthevicinityofpsrb170644andg343123withhess
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