The TeV spectrum of H1426+428

D. Petry, I. H. Bond, S. M. Bradbury, J. H. Buckley, D. A. Carter-Lewis, W. Cui, C. Duke, I. De La Calle Perez, A. Falcone, D. J. Fegan, S. J. Fegan, J. P. Finley, J. A. Gaidos, K. Gibbs, S. Gammell, J. Hall, T. A. Hall, A. M. Hillas, J. Holder, D. HoranM. Jordan, M. Kertzman, D. Kieda, J. Kildea, J. Knapp, K. Kosack, F. Krennrich, S. LeBohec, P. Moriarty, D. Müller, T. N. Nagai, R. Ong, M. Page, R. Pallassini, B. Power-Mooney, J. Quinn, N. W. Reay, P. T. Reynolds, H. J. Rose, M. Schroedter, G. H. Sembroski, R. Sidwell, N. Stanton, S. P. Swordy, V. V. Vassiliev, S. P. Wakely, G. Walker, T. C. Weekes

Research output: Contribution to journalArticle

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Abstract

The BL Lac object H1426+428 was recently detected as a high-energy γ-ray source by the VERITAS collaboration (Horan et al.). We have reanalyzed the 2001 portion of the data used in the detection in order to examine the spectrum of H1426+428 above 250 GeV. We find that the time-averaged spectrum agrees with a power law of the shape (dF/dE) (E) = 10 -7.31±0.15stat±0.16syst E -3.50±0.35stat±0.05syst m-2 s-1 TeV-1. The statistical evidence from our data for emission above 2.5 TeV is 2.6 σ. At the 95% confidence level, the integral flux of H1426+428 above 2.5 TeV is larger than 3% of the corresponding flux from the Crab Nebula. The spectrum is consistent with the (noncontemporaneous) measurement by Aharonian et al. both in shape and in normalization. Below 800 GeV, the data clearly favor a spectrum steeper than that of any other TeV blazar observed so far, indicating a difference in the processes involved either at the source or in the intervening space.

Original languageEnglish (US)
Pages (from-to)104-109
Number of pages6
JournalAstrophysical Journal
Volume580
Issue number1 I
DOIs
StatePublished - Nov 20 2002

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Crab nebula
crab
confidence
rays
power law
energy
detection
normalisation

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Petry, D., Bond, I. H., Bradbury, S. M., Buckley, J. H., Carter-Lewis, D. A., Cui, W., ... Weekes, T. C. (2002). The TeV spectrum of H1426+428. Astrophysical Journal, 580(1 I), 104-109. https://doi.org/10.1086/343102
Petry, D. ; Bond, I. H. ; Bradbury, S. M. ; Buckley, J. H. ; Carter-Lewis, D. A. ; Cui, W. ; Duke, C. ; De La Calle Perez, I. ; Falcone, A. ; Fegan, D. J. ; Fegan, S. J. ; Finley, J. P. ; Gaidos, J. A. ; Gibbs, K. ; Gammell, S. ; Hall, J. ; Hall, T. A. ; Hillas, A. M. ; Holder, J. ; Horan, D. ; Jordan, M. ; Kertzman, M. ; Kieda, D. ; Kildea, J. ; Knapp, J. ; Kosack, K. ; Krennrich, F. ; LeBohec, S. ; Moriarty, P. ; Müller, D. ; Nagai, T. N. ; Ong, R. ; Page, M. ; Pallassini, R. ; Power-Mooney, B. ; Quinn, J. ; Reay, N. W. ; Reynolds, P. T. ; Rose, H. J. ; Schroedter, M. ; Sembroski, G. H. ; Sidwell, R. ; Stanton, N. ; Swordy, S. P. ; Vassiliev, V. V. ; Wakely, S. P. ; Walker, G. ; Weekes, T. C. / The TeV spectrum of H1426+428. In: Astrophysical Journal. 2002 ; Vol. 580, No. 1 I. pp. 104-109.
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abstract = "The BL Lac object H1426+428 was recently detected as a high-energy γ-ray source by the VERITAS collaboration (Horan et al.). We have reanalyzed the 2001 portion of the data used in the detection in order to examine the spectrum of H1426+428 above 250 GeV. We find that the time-averaged spectrum agrees with a power law of the shape (dF/dE) (E) = 10 -7.31±0.15stat±0.16syst E -3.50±0.35stat±0.05syst m-2 s-1 TeV-1. The statistical evidence from our data for emission above 2.5 TeV is 2.6 σ. At the 95{\%} confidence level, the integral flux of H1426+428 above 2.5 TeV is larger than 3{\%} of the corresponding flux from the Crab Nebula. The spectrum is consistent with the (noncontemporaneous) measurement by Aharonian et al. both in shape and in normalization. Below 800 GeV, the data clearly favor a spectrum steeper than that of any other TeV blazar observed so far, indicating a difference in the processes involved either at the source or in the intervening space.",
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Petry, D, Bond, IH, Bradbury, SM, Buckley, JH, Carter-Lewis, DA, Cui, W, Duke, C, De La Calle Perez, I, Falcone, A, Fegan, DJ, Fegan, SJ, Finley, JP, Gaidos, JA, Gibbs, K, Gammell, S, Hall, J, Hall, TA, Hillas, AM, Holder, J, Horan, D, Jordan, M, Kertzman, M, Kieda, D, Kildea, J, Knapp, J, Kosack, K, Krennrich, F, LeBohec, S, Moriarty, P, Müller, D, Nagai, TN, Ong, R, Page, M, Pallassini, R, Power-Mooney, B, Quinn, J, Reay, NW, Reynolds, PT, Rose, HJ, Schroedter, M, Sembroski, GH, Sidwell, R, Stanton, N, Swordy, SP, Vassiliev, VV, Wakely, SP, Walker, G & Weekes, TC 2002, 'The TeV spectrum of H1426+428', Astrophysical Journal, vol. 580, no. 1 I, pp. 104-109. https://doi.org/10.1086/343102

The TeV spectrum of H1426+428. / Petry, D.; Bond, I. H.; Bradbury, S. M.; Buckley, J. H.; Carter-Lewis, D. A.; Cui, W.; Duke, C.; De La Calle Perez, I.; Falcone, A.; Fegan, D. J.; Fegan, S. J.; Finley, J. P.; Gaidos, J. A.; Gibbs, K.; Gammell, S.; Hall, J.; Hall, T. A.; Hillas, A. M.; Holder, J.; Horan, D.; Jordan, M.; Kertzman, M.; Kieda, D.; Kildea, J.; Knapp, J.; Kosack, K.; Krennrich, F.; LeBohec, S.; Moriarty, P.; Müller, D.; Nagai, T. N.; Ong, R.; Page, M.; Pallassini, R.; Power-Mooney, B.; Quinn, J.; Reay, N. W.; Reynolds, P. T.; Rose, H. J.; Schroedter, M.; Sembroski, G. H.; Sidwell, R.; Stanton, N.; Swordy, S. P.; Vassiliev, V. V.; Wakely, S. P.; Walker, G.; Weekes, T. C.

In: Astrophysical Journal, Vol. 580, No. 1 I, 20.11.2002, p. 104-109.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The TeV spectrum of H1426+428

AU - Petry, D.

AU - Bond, I. H.

AU - Bradbury, S. M.

AU - Buckley, J. H.

AU - Carter-Lewis, D. A.

AU - Cui, W.

AU - Duke, C.

AU - De La Calle Perez, I.

AU - Falcone, A.

AU - Fegan, D. J.

AU - Fegan, S. J.

AU - Finley, J. P.

AU - Gaidos, J. A.

AU - Gibbs, K.

AU - Gammell, S.

AU - Hall, J.

AU - Hall, T. A.

AU - Hillas, A. M.

AU - Holder, J.

AU - Horan, D.

AU - Jordan, M.

AU - Kertzman, M.

AU - Kieda, D.

AU - Kildea, J.

AU - Knapp, J.

AU - Kosack, K.

AU - Krennrich, F.

AU - LeBohec, S.

AU - Moriarty, P.

AU - Müller, D.

AU - Nagai, T. N.

AU - Ong, R.

AU - Page, M.

AU - Pallassini, R.

AU - Power-Mooney, B.

AU - Quinn, J.

AU - Reay, N. W.

AU - Reynolds, P. T.

AU - Rose, H. J.

AU - Schroedter, M.

AU - Sembroski, G. H.

AU - Sidwell, R.

AU - Stanton, N.

AU - Swordy, S. P.

AU - Vassiliev, V. V.

AU - Wakely, S. P.

AU - Walker, G.

AU - Weekes, T. C.

PY - 2002/11/20

Y1 - 2002/11/20

N2 - The BL Lac object H1426+428 was recently detected as a high-energy γ-ray source by the VERITAS collaboration (Horan et al.). We have reanalyzed the 2001 portion of the data used in the detection in order to examine the spectrum of H1426+428 above 250 GeV. We find that the time-averaged spectrum agrees with a power law of the shape (dF/dE) (E) = 10 -7.31±0.15stat±0.16syst E -3.50±0.35stat±0.05syst m-2 s-1 TeV-1. The statistical evidence from our data for emission above 2.5 TeV is 2.6 σ. At the 95% confidence level, the integral flux of H1426+428 above 2.5 TeV is larger than 3% of the corresponding flux from the Crab Nebula. The spectrum is consistent with the (noncontemporaneous) measurement by Aharonian et al. both in shape and in normalization. Below 800 GeV, the data clearly favor a spectrum steeper than that of any other TeV blazar observed so far, indicating a difference in the processes involved either at the source or in the intervening space.

AB - The BL Lac object H1426+428 was recently detected as a high-energy γ-ray source by the VERITAS collaboration (Horan et al.). We have reanalyzed the 2001 portion of the data used in the detection in order to examine the spectrum of H1426+428 above 250 GeV. We find that the time-averaged spectrum agrees with a power law of the shape (dF/dE) (E) = 10 -7.31±0.15stat±0.16syst E -3.50±0.35stat±0.05syst m-2 s-1 TeV-1. The statistical evidence from our data for emission above 2.5 TeV is 2.6 σ. At the 95% confidence level, the integral flux of H1426+428 above 2.5 TeV is larger than 3% of the corresponding flux from the Crab Nebula. The spectrum is consistent with the (noncontemporaneous) measurement by Aharonian et al. both in shape and in normalization. Below 800 GeV, the data clearly favor a spectrum steeper than that of any other TeV blazar observed so far, indicating a difference in the processes involved either at the source or in the intervening space.

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DO - 10.1086/343102

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Petry D, Bond IH, Bradbury SM, Buckley JH, Carter-Lewis DA, Cui W et al. The TeV spectrum of H1426+428. Astrophysical Journal. 2002 Nov 20;580(1 I):104-109. https://doi.org/10.1086/343102