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Abstract:

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.

Registro:

Documento: Artículo
Título:Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S.
Autor:Abramowski, A. et al.
Este artículo contiene 199 autores, consultelos en el artículo en formato pdf.
Filiación: Este artículo contiene 199 autores con sus filiaciones, consultelas en el artículo en formato pdf.
Palabras clave: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
Año:2011
Volumen:528
DOI: http://dx.doi.org/10.1051/0004-6361/201015381
Título revista:Astronomy and Astrophysics
Título revista abreviado:Astron. Astrophys.
ISSN:00046361
CODEN:AAEJA
Registro:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_00046361_v528_n_p_Abramowski

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Citas:

---------- APA ----------
(2011) . Detection of very-high-energy γ-ray emission from the vicinity of PSRB1706-44 and G343.1-2.3 with H.E.S.S. Astronomy and Astrophysics, 528.
http://dx.doi.org/10.1051/0004-6361/201015381
---------- CHICAGO ----------
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." Astronomy and Astrophysics 528 (2011).
http://dx.doi.org/10.1051/0004-6361/201015381
---------- MLA ----------
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." Astronomy and Astrophysics, vol. 528, 2011.
http://dx.doi.org/10.1051/0004-6361/201015381
---------- VANCOUVER ----------
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. Astron. Astrophys. 2011;528.
http://dx.doi.org/10.1051/0004-6361/201015381