The EGRET detection of quasar 1633 + 382

J. R. Mattox; D. L. Bertsch; J. Chiang; B. L. Dingus; C. E. Fichtel; R. C. Hartman; S. D. Hunter; G. Kanbach; D. A. Kniffen; P. W. Kwok; Y. C. Lin; H. A. Mayer-Hasselwander; P. F. Michelson; C. Von Montigny; P. L. Nolan; K. Pinkau; E. Schneid; P. Sreekumar; D. J. Thompson

doi:10.1086/172778

The EGRET detection of quasar 1633 + 382

J. R. Mattox^*
, D. L. Bertsch
, J. Chiang
, B. L. Dingus
, C. E. Fichtel
, R. C. Hartman
, S. D. Hunter
, G. Kanbach
, D. A. Kniffen
, P. W. Kwok
, Y. C. Lin
, H. A. Mayer-Hasselwander
, P. F. Michelson
, C. Von Montigny
, P. L. Nolan
, K. Pinkau
, E. Schneid
, P. Sreekumar
, D. J. Thompson

^*Corresponding author for this work

Manipal Centre for Natural Sciences, Manipal

Research output: Contribution to journal › Article › peer-review

153 Citations (Scopus)

Abstract

In the course of a full-sky survey, the EGRET instrument aboard the Compton Observatory detected an intense, high Galactic latitude source (GRO J1635 + 38), which is identified as OVV (optically violent variable) quasar 1633 + 382. The spectrum is represented by a power law with an energy spectral index of 0.9 between 30 MeV and 30 GeV. The γ-ray power per decade is ∼100 times larger than typical values at any longer wavelength. Significant variation of the γ-ray flux density on a time scale as short as 2 days was observed, limiting the size of the region in which the γ-rays are produced. Assuming the X-rays detected by the Einstein Observatory from this quasar are produced in the same region as the γ-rays, and a similar X-ray flux density was extant at the time of the EGRET observation, the emission must be beamed to avoid a pair-production optical depth of ∼10⁴ which would exist otherwise. If beaming arises from bulk relativistic motion, the minimum Doppler factor required is 7.6.

Original language	English
Pages (from-to)	609-614
Number of pages	6
Journal	Astrophysical Journal
Volume	410
Issue number	2
DOIs	https://doi.org/10.1086/172778
Publication status	Published - 20-06-1993

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.1086/172778

Cite this

Mattox, J. R., Bertsch, D. L., Chiang, J., Dingus, B. L., Fichtel, C. E., Hartman, R. C., Hunter, S. D., Kanbach, G., Kniffen, D. A., Kwok, P. W., Lin, Y. C., Mayer-Hasselwander, H. A., Michelson, P. F., Von Montigny, C., Nolan, P. L., Pinkau, K., Schneid, E., Sreekumar, P., & Thompson, D. J. (1993). The EGRET detection of quasar 1633 + 382. Astrophysical Journal, 410(2), 609-614. https://doi.org/10.1086/172778

@article{396cbc1fb9ba45899c5b391be1e7dc9f,

title = "The EGRET detection of quasar 1633 + 382",

abstract = "In the course of a full-sky survey, the EGRET instrument aboard the Compton Observatory detected an intense, high Galactic latitude source (GRO J1635 + 38), which is identified as OVV (optically violent variable) quasar 1633 + 382. The spectrum is represented by a power law with an energy spectral index of 0.9 between 30 MeV and 30 GeV. The γ-ray power per decade is ∼100 times larger than typical values at any longer wavelength. Significant variation of the γ-ray flux density on a time scale as short as 2 days was observed, limiting the size of the region in which the γ-rays are produced. Assuming the X-rays detected by the Einstein Observatory from this quasar are produced in the same region as the γ-rays, and a similar X-ray flux density was extant at the time of the EGRET observation, the emission must be beamed to avoid a pair-production optical depth of ∼104 which would exist otherwise. If beaming arises from bulk relativistic motion, the minimum Doppler factor required is 7.6.",

author = "Mattox, \{J. R.\} and Bertsch, \{D. L.\} and J. Chiang and Dingus, \{B. L.\} and Fichtel, \{C. E.\} and Hartman, \{R. C.\} and Hunter, \{S. D.\} and G. Kanbach and Kniffen, \{D. A.\} and Kwok, \{P. W.\} and Lin, \{Y. C.\} and Mayer-Hasselwander, \{H. A.\} and Michelson, \{P. F.\} and \{Von Montigny\}, C. and Nolan, \{P. L.\} and K. Pinkau and E. Schneid and P. Sreekumar and Thompson, \{D. J.\}",

year = "1993",

month = jun,

day = "20",

doi = "10.1086/172778",

language = "English",

volume = "410",

pages = "609--614",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

number = "2",

}

Mattox, JR, Bertsch, DL, Chiang, J, Dingus, BL, Fichtel, CE, Hartman, RC, Hunter, SD, Kanbach, G, Kniffen, DA, Kwok, PW, Lin, YC, Mayer-Hasselwander, HA, Michelson, PF, Von Montigny, C, Nolan, PL, Pinkau, K, Schneid, E, Sreekumar, P & Thompson, DJ 1993, 'The EGRET detection of quasar 1633 + 382', Astrophysical Journal, vol. 410, no. 2, pp. 609-614. https://doi.org/10.1086/172778

TY - JOUR

T1 - The EGRET detection of quasar 1633 + 382

AU - Mattox, J. R.

AU - Bertsch, D. L.

AU - Chiang, J.

AU - Dingus, B. L.

AU - Fichtel, C. E.

AU - Hartman, R. C.

AU - Hunter, S. D.

AU - Kanbach, G.

AU - Kniffen, D. A.

AU - Kwok, P. W.

AU - Lin, Y. C.

AU - Mayer-Hasselwander, H. A.

AU - Michelson, P. F.

AU - Von Montigny, C.

AU - Nolan, P. L.

AU - Pinkau, K.

AU - Schneid, E.

AU - Sreekumar, P.

AU - Thompson, D. J.

PY - 1993/6/20

Y1 - 1993/6/20

N2 - In the course of a full-sky survey, the EGRET instrument aboard the Compton Observatory detected an intense, high Galactic latitude source (GRO J1635 + 38), which is identified as OVV (optically violent variable) quasar 1633 + 382. The spectrum is represented by a power law with an energy spectral index of 0.9 between 30 MeV and 30 GeV. The γ-ray power per decade is ∼100 times larger than typical values at any longer wavelength. Significant variation of the γ-ray flux density on a time scale as short as 2 days was observed, limiting the size of the region in which the γ-rays are produced. Assuming the X-rays detected by the Einstein Observatory from this quasar are produced in the same region as the γ-rays, and a similar X-ray flux density was extant at the time of the EGRET observation, the emission must be beamed to avoid a pair-production optical depth of ∼104 which would exist otherwise. If beaming arises from bulk relativistic motion, the minimum Doppler factor required is 7.6.

AB - In the course of a full-sky survey, the EGRET instrument aboard the Compton Observatory detected an intense, high Galactic latitude source (GRO J1635 + 38), which is identified as OVV (optically violent variable) quasar 1633 + 382. The spectrum is represented by a power law with an energy spectral index of 0.9 between 30 MeV and 30 GeV. The γ-ray power per decade is ∼100 times larger than typical values at any longer wavelength. Significant variation of the γ-ray flux density on a time scale as short as 2 days was observed, limiting the size of the region in which the γ-rays are produced. Assuming the X-rays detected by the Einstein Observatory from this quasar are produced in the same region as the γ-rays, and a similar X-ray flux density was extant at the time of the EGRET observation, the emission must be beamed to avoid a pair-production optical depth of ∼104 which would exist otherwise. If beaming arises from bulk relativistic motion, the minimum Doppler factor required is 7.6.

UR - https://www.scopus.com/pages/publications/0001362986

UR - https://www.scopus.com/pages/publications/0001362986#tab=citedBy

U2 - 10.1086/172778

DO - 10.1086/172778

M3 - Article

AN - SCOPUS:0001362986

SN - 0004-637X

VL - 410

SP - 609

EP - 614

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

ER -

The EGRET detection of quasar 1633 + 382

Abstract

All Science Journal Classification (ASJC) codes

Access to Document

Other files and links

Fingerprint

Cite this