Very high energy gamma rays from the vela pulsar direction

T. Yoshikoshi; T. Kifune; S. A. Dazeley; P. G. Edwards; T. Hara; Y. Hayami; F. Kakimoto; T. Konishi; A. Masaike; Y. Matsubara; T. Matsuoka; Y. Mizumoto; M. Mori; H. Muraishi; Y. Muraki; T. Naito; K. Nishijima; S. Oda; S. Ogio; T. Ohsaki; J. R. Patterson; M. D. Roberts; G. P. Rowell; T. Sako; K. Sakurazawa; R. Susukita; A. Suzuki; T. Tamura; T. Tanimori; G. J. Thornton; S. Yanagita; T. Yoshida

doi:10.1086/310874

Very high energy gamma rays from the vela pulsar direction

T. Yoshikoshi, T. Kifune, S. A. Dazeley, P. G. Edwards, T. Hara, Y. Hayami, F. Kakimoto, T. Konishi, A. Masaike, Y. Matsubara, T. Matsuoka, Y. Mizumoto, M. Mori, H. Muraishi, Y. Muraki, T. Naito, K. Nishijima, S. Oda, S. Ogio, T. OhsakiJ. R. Patterson, M. D. Roberts, G. P. Rowell, T. Sako, K. Sakurazawa, R. Susukita, A. Suzuki, T. Tamura, T. Tanimori, G. J. Thornton, S. Yanagita, T. Yoshida

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Abstract

We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging Čerenkov telescope near Woomera, South Australia between 1993 January and 1995 March. Evidence of an unpulsed gamma-ray signal has been detected at the 5.8 σ level. The detected gamma-ray flux is (2.9 ± 0.5 ± 0.4) × 10^-12 photons cm^-2 s^-1 above 2.5 ± 1.0 TeV, and the signal is consistent with steady emission over the 2 years. The gamma-ray emission region is offset from the Vela pulsar position to the southeast by about 0°.13. No pulsed emission modulated with the pulsar period has been detected, and the 95% confidence flux upper limit to the pulsed emission from the pulsar is (3.7 ± 0.7) × 10^-13 photons cm^-2 s^-1 above 2.5 ± 1.0 TeV.

Original language	English
Pages (from-to)	L65-L68
Journal	Astrophysical Journal
Volume	487
Issue number	1 PART II
DOIs	https://doi.org/10.1086/310874
Publication status	Published - 1997
Externally published	Yes

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/310874

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Yoshikoshi, T., Kifune, T., Dazeley, S. A., Edwards, P. G., Hara, T., Hayami, Y., Kakimoto, F., Konishi, T., Masaike, A., Matsubara, Y., Matsuoka, T., Mizumoto, Y., Mori, M., Muraishi, H., Muraki, Y., Naito, T., Nishijima, K., Oda, S., Ogio, S., ... Yoshida, T. (1997). Very high energy gamma rays from the vela pulsar direction. Astrophysical Journal, 487(1 PART II), L65-L68. https://doi.org/10.1086/310874

Yoshikoshi, T, Kifune, T, Dazeley, SA, Edwards, PG, Hara, T, Hayami, Y, Kakimoto, F, Konishi, T, Masaike, A, Matsubara, Y, Matsuoka, T, Mizumoto, Y, Mori, M, Muraishi, H, Muraki, Y, Naito, T, Nishijima, K, Oda, S, Ogio, S, Ohsaki, T, Patterson, JR, Roberts, MD, Rowell, GP, Sako, T, Sakurazawa, K, Susukita, R, Suzuki, A, Tamura, T, Tanimori, T, Thornton, GJ, Yanagita, S & Yoshida, T 1997, 'Very high energy gamma rays from the vela pulsar direction', Astrophysical Journal, vol. 487, no. 1 PART II, pp. L65-L68. https://doi.org/10.1086/310874

@article{7e6b25532a9a42fa811d0194996e4a9a,

title = "Very high energy gamma rays from the vela pulsar direction",

abstract = "We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging {\v C}erenkov telescope near Woomera, South Australia between 1993 January and 1995 March. Evidence of an unpulsed gamma-ray signal has been detected at the 5.8 σ level. The detected gamma-ray flux is (2.9 ± 0.5 ± 0.4) × 10-12 photons cm-2 s-1 above 2.5 ± 1.0 TeV, and the signal is consistent with steady emission over the 2 years. The gamma-ray emission region is offset from the Vela pulsar position to the southeast by about 0°.13. No pulsed emission modulated with the pulsar period has been detected, and the 95% confidence flux upper limit to the pulsed emission from the pulsar is (3.7 ± 0.7) × 10-13 photons cm-2 s-1 above 2.5 ± 1.0 TeV.",

author = "T. Yoshikoshi and T. Kifune and Dazeley, {S. A.} and Edwards, {P. G.} and T. Hara and Y. Hayami and F. Kakimoto and T. Konishi and A. Masaike and Y. Matsubara and T. Matsuoka and Y. Mizumoto and M. Mori and H. Muraishi and Y. Muraki and T. Naito and K. Nishijima and S. Oda and S. Ogio and T. Ohsaki and Patterson, {J. R.} and Roberts, {M. D.} and Rowell, {G. P.} and T. Sako and K. Sakurazawa and R. Susukita and A. Suzuki and T. Tamura and T. Tanimori and Thornton, {G. J.} and S. Yanagita and T. Yoshida",

note = "Funding Information: This work is supported by International Scientific Research Program of a Grant-in-Aid in Scientific Research of the Ministry of Education, Science, Sports, and Culture, Japan, and by the Australian Research Council. T. Kifune and T. Tanimori acknowledge the support of the Sumitomo Foundation. The receipt of JSPS Research Fellowships (P. G. E., T. N., M. D. R., K. S., G. J. T., and T. Yoshikoshi) is also acknowledged.",

year = "1997",

doi = "10.1086/310874",

language = "English",

volume = "487",

pages = "L65--L68",

journal = "Astrophysical Journal",

issn = "0004-637X",

number = "1 PART II",

}

TY - JOUR

T1 - Very high energy gamma rays from the vela pulsar direction

AU - Yoshikoshi, T.

AU - Kifune, T.

AU - Dazeley, S. A.

AU - Edwards, P. G.

AU - Hara, T.

AU - Hayami, Y.

AU - Kakimoto, F.

AU - Konishi, T.

AU - Masaike, A.

AU - Matsubara, Y.

AU - Matsuoka, T.

AU - Mizumoto, Y.

AU - Mori, M.

AU - Muraishi, H.

AU - Muraki, Y.

AU - Naito, T.

AU - Nishijima, K.

AU - Oda, S.

AU - Ogio, S.

AU - Ohsaki, T.

AU - Patterson, J. R.

AU - Roberts, M. D.

AU - Rowell, G. P.

AU - Sako, T.

AU - Sakurazawa, K.

AU - Susukita, R.

AU - Suzuki, A.

AU - Tamura, T.

AU - Tanimori, T.

AU - Thornton, G. J.

AU - Yanagita, S.

AU - Yoshida, T.

N1 - Funding Information: This work is supported by International Scientific Research Program of a Grant-in-Aid in Scientific Research of the Ministry of Education, Science, Sports, and Culture, Japan, and by the Australian Research Council. T. Kifune and T. Tanimori acknowledge the support of the Sumitomo Foundation. The receipt of JSPS Research Fellowships (P. G. E., T. N., M. D. R., K. S., G. J. T., and T. Yoshikoshi) is also acknowledged.

PY - 1997

Y1 - 1997

N2 - We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging Čerenkov telescope near Woomera, South Australia between 1993 January and 1995 March. Evidence of an unpulsed gamma-ray signal has been detected at the 5.8 σ level. The detected gamma-ray flux is (2.9 ± 0.5 ± 0.4) × 10-12 photons cm-2 s-1 above 2.5 ± 1.0 TeV, and the signal is consistent with steady emission over the 2 years. The gamma-ray emission region is offset from the Vela pulsar position to the southeast by about 0°.13. No pulsed emission modulated with the pulsar period has been detected, and the 95% confidence flux upper limit to the pulsed emission from the pulsar is (3.7 ± 0.7) × 10-13 photons cm-2 s-1 above 2.5 ± 1.0 TeV.

AB - We have observed the Vela pulsar region at TeV energies using the 3.8 m imaging Čerenkov telescope near Woomera, South Australia between 1993 January and 1995 March. Evidence of an unpulsed gamma-ray signal has been detected at the 5.8 σ level. The detected gamma-ray flux is (2.9 ± 0.5 ± 0.4) × 10-12 photons cm-2 s-1 above 2.5 ± 1.0 TeV, and the signal is consistent with steady emission over the 2 years. The gamma-ray emission region is offset from the Vela pulsar position to the southeast by about 0°.13. No pulsed emission modulated with the pulsar period has been detected, and the 95% confidence flux upper limit to the pulsed emission from the pulsar is (3.7 ± 0.7) × 10-13 photons cm-2 s-1 above 2.5 ± 1.0 TeV.

UR - http://www.scopus.com/inward/record.url?scp=21944433405&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=21944433405&partnerID=8YFLogxK

U2 - 10.1086/310874

DO - 10.1086/310874

M3 - Article

AN - SCOPUS:21944433405

SN - 0004-637X

VL - 487

SP - L65-L68

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1 PART II

ER -

Very high energy gamma rays from the vela pulsar direction

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