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. Horan; M. 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

doi:10.1086/343102

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. Horan

M. 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 journal › Article › peer-review

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 language	English
Pages (from-to)	104-109
Number of pages	6
Journal	Astrophysical Journal
Volume	580
Issue number	1 I
DOIs	https://doi.org/10.1086/343102
Publication status	Published - 20 Nov 2002
Externally published	Yes

Keywords

Gamma rays: observations

Access to Document

10.1086/343102

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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., ... Weekes, T. C. (2002). The TeV spectrum of H1426+428. Astrophysical Journal, 580(1 I), 104-109. https://doi.org/10.1086/343102

@article{36a00546e6914e8aabafce13302ceb45,

title = "The TeV spectrum of H1426+428",

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.",

keywords = "Gamma rays: observations",

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

year = "2002",

month = nov,

day = "20",

doi = "10.1086/343102",

language = "English",

volume = "580",

pages = "104--109",

journal = "Astrophysical Journal",

issn = "0004-637X",

number = "1 I",

}

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

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.

KW - Gamma rays: observations

U2 - 10.1086/343102

DO - 10.1086/343102

M3 - Article

AN - SCOPUS:0038082170

SN - 0004-637X

VL - 580

SP - 104

EP - 109

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 I

ER -

The TeV spectrum of H1426+428

Abstract

Keywords

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