Very high-energy observations of PSR B1951 + 32

R. Srinivasan; P. J. Boyle; J. H. Buckley; D. A. Carter-Lewis; M. Catanese; M. F. Cawley; E. Colombo; D. J. Fegan; J. P. Finley; J. A. Gaidos; J. Bussons Gordo; A. M. Hillas; F. Krennrich; R. C. Lamb; R. W. Lessard; J. M. Mcenery; P. Moriarty; J. Quinn; H. J. Rose; F. W. Samuelson; G. Sembroski; T. C. Weekes; C. Wilson; J. Zweerink

doi:10.1086/304781

Very high-energy observations of PSR B1951 + 32

R. Srinivasan, P. J. Boyle, J. H. Buckley, D. A. Carter-Lewis, M. Catanese, M. F. Cawley, E. Colombo, D. J. Fegan, J. P. Finley, J. A. Gaidos, J. Bussons Gordo, A. M. Hillas, F. Krennrich, R. C. Lamb, R. W. Lessard, J. M. Mcenery, P. Moriarty, J. Quinn, H. J. Rose, F. W. SamuelsonG. Sembroski, T. C. Weekes, C. Wilson, J. Zweerink

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Abstract

PSR B1951+32 is a γ-ray pulsar detected by the Energetic Gamma Ray Experiment Telescope (EGRET) and identified with the 39.5 ms radio pulsar in the supernova remnant CTB 80. The pulsar energy spectrum is consistent with an unbroken power law with differential photon index of -1.8 ± 0.1 between 50 MeV and 10 GeV. The EGRET data shows no evidence for a spectral turnover. Here we report on the first observations of PSR B1951+32 beyond 30 GeV. The observations were carried out with the 10 m γ-ray telescope at the Whipple Observatory on Mount Hopkins, Arizona. In 8.1 hours of observation we find no evidence for steady or periodic emission from PSR B1951 +32 above ∼260 GeV. Flux upper limits are derived and compared with model extrapolations from lower energies and the predictions of emission models.

Original language	English
Pages (from-to)	170-174
Number of pages	5
Journal	Astrophysical Journal
Volume	489
Issue number	1 PART I
DOIs	https://doi.org/10.1086/304781
Publication status	Published - 1997
Externally published	Yes

Keywords

Gamma rays: observations
Supernova remnants

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10.1086/304781

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Srinivasan, R., Boyle, P. J., Buckley, J. H., Carter-Lewis, D. A., Catanese, M., Cawley, M. F., Colombo, E., Fegan, D. J., Finley, J. P., Gaidos, J. A., Bussons Gordo, J., Hillas, A. M., Krennrich, F., Lamb, R. C., Lessard, R. W., Mcenery, J. M., Moriarty, P., Quinn, J., Rose, H. J., ... Zweerink, J. (1997). Very high-energy observations of PSR B1951 + 32. Astrophysical Journal, 489(1 PART I), 170-174. https://doi.org/10.1086/304781

@article{3f796b7490a84f87ac980dce4522fdf9,

title = "Very high-energy observations of PSR B1951 + 32",

abstract = "PSR B1951+32 is a γ-ray pulsar detected by the Energetic Gamma Ray Experiment Telescope (EGRET) and identified with the 39.5 ms radio pulsar in the supernova remnant CTB 80. The pulsar energy spectrum is consistent with an unbroken power law with differential photon index of -1.8 ± 0.1 between 50 MeV and 10 GeV. The EGRET data shows no evidence for a spectral turnover. Here we report on the first observations of PSR B1951+32 beyond 30 GeV. The observations were carried out with the 10 m γ-ray telescope at the Whipple Observatory on Mount Hopkins, Arizona. In 8.1 hours of observation we find no evidence for steady or periodic emission from PSR B1951 +32 above ∼260 GeV. Flux upper limits are derived and compared with model extrapolations from lower energies and the predictions of emission models.",

keywords = "Gamma rays: observations, Supernova remnants",

author = "R. Srinivasan and Boyle, \{P. J.\} and Buckley, \{J. H.\} and Carter-Lewis, \{D. A.\} and M. Catanese and Cawley, \{M. F.\} and E. Colombo and Fegan, \{D. J.\} and Finley, \{J. P.\} and Gaidos, \{J. A.\} and \{Bussons Gordo\}, J. and Hillas, \{A. M.\} and F. Krennrich and Lamb, \{R. C.\} and Lessard, \{R. W.\} and Mcenery, \{J. M.\} and P. Moriarty and J. Quinn and Rose, \{H. J.\} and Samuelson, \{F. W.\} and G. Sembroski and Weekes, \{T. C.\} and C. Wilson and J. Zweerink",

year = "1997",

doi = "10.1086/304781",

language = "English",

volume = "489",

pages = "170--174",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "1 PART I",

}

Srinivasan, R, Boyle, PJ, Buckley, JH, Carter-Lewis, DA, Catanese, M, Cawley, MF, Colombo, E, Fegan, DJ, Finley, JP, Gaidos, JA, Bussons Gordo, J, Hillas, AM, Krennrich, F, Lamb, RC, Lessard, RW, Mcenery, JM, Moriarty, P, Quinn, J, Rose, HJ, Samuelson, FW, Sembroski, G, Weekes, TC, Wilson, C & Zweerink, J 1997, 'Very high-energy observations of PSR B1951 + 32', Astrophysical Journal, vol. 489, no. 1 PART I, pp. 170-174. https://doi.org/10.1086/304781

TY - JOUR

T1 - Very high-energy observations of PSR B1951 + 32

AU - Srinivasan, R.

AU - Boyle, P. J.

AU - Buckley, J. H.

AU - Carter-Lewis, D. A.

AU - Catanese, M.

AU - Cawley, M. F.

AU - Colombo, E.

AU - Fegan, D. J.

AU - Finley, J. P.

AU - Gaidos, J. A.

AU - Bussons Gordo, J.

AU - Hillas, A. M.

AU - Krennrich, F.

AU - Lamb, R. C.

AU - Lessard, R. W.

AU - Mcenery, J. M.

AU - Moriarty, P.

AU - Quinn, J.

AU - Rose, H. J.

AU - Samuelson, F. W.

AU - Sembroski, G.

AU - Weekes, T. C.

AU - Wilson, C.

AU - Zweerink, J.

PY - 1997

Y1 - 1997

N2 - PSR B1951+32 is a γ-ray pulsar detected by the Energetic Gamma Ray Experiment Telescope (EGRET) and identified with the 39.5 ms radio pulsar in the supernova remnant CTB 80. The pulsar energy spectrum is consistent with an unbroken power law with differential photon index of -1.8 ± 0.1 between 50 MeV and 10 GeV. The EGRET data shows no evidence for a spectral turnover. Here we report on the first observations of PSR B1951+32 beyond 30 GeV. The observations were carried out with the 10 m γ-ray telescope at the Whipple Observatory on Mount Hopkins, Arizona. In 8.1 hours of observation we find no evidence for steady or periodic emission from PSR B1951 +32 above ∼260 GeV. Flux upper limits are derived and compared with model extrapolations from lower energies and the predictions of emission models.

AB - PSR B1951+32 is a γ-ray pulsar detected by the Energetic Gamma Ray Experiment Telescope (EGRET) and identified with the 39.5 ms radio pulsar in the supernova remnant CTB 80. The pulsar energy spectrum is consistent with an unbroken power law with differential photon index of -1.8 ± 0.1 between 50 MeV and 10 GeV. The EGRET data shows no evidence for a spectral turnover. Here we report on the first observations of PSR B1951+32 beyond 30 GeV. The observations were carried out with the 10 m γ-ray telescope at the Whipple Observatory on Mount Hopkins, Arizona. In 8.1 hours of observation we find no evidence for steady or periodic emission from PSR B1951 +32 above ∼260 GeV. Flux upper limits are derived and compared with model extrapolations from lower energies and the predictions of emission models.

KW - Gamma rays: observations

KW - Supernova remnants

UR - https://www.scopus.com/pages/publications/0040631025

U2 - 10.1086/304781

DO - 10.1086/304781

M3 - Article

SN - 0004-637X

VL - 489

SP - 170

EP - 174

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 PART I

ER -

Very high-energy observations of PSR B1951 + 32

Abstract

Keywords

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