Low-energy gamma-ray emission close to CG 135 + 1

Perotti, F.; Ventura, Andrea; Villa, G.; Cocco, G. Di; Butler, R. C.; Dean, Anthony J.; Hayles, R. I.

doi:10.1086/183289

Cited by 19 publications

(5 citation statements)

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“…(Note that COMPTEL cannot resolve LSI +61 • 303 from QSO 0241+622). Although we have not displayed the MISO result (Perotti et al 1980), it clearly exhibits a higher flux than either the OSSE or COMPTEL observations. However, due to the low detection significance of all these data, it is difficult to conclude that the MISO result is inconsistent at more than a 3σ confidence level.…”

Section: The Osse Resultscontrasting

confidence: 64%

“…Since its discovery by the COS-B satellite (Hermsen et al 1977, Swanenburg et al 1981, no satisfactory explanation has been found for the nature of 2CG 135+1 and its γ-ray emission mechanism. The COS-B error box of 2CG 135+1 contains two interesting sources, the radio flaring Be star LSI +61 • 303, and the QSO 0241+622 (e.g, Perotti et al 1980). EGRET observations of 2CG 135+1 during CGRO Phase 1 and 2 (von Montigny et al 1993, Thompson et al 1995, Kniffen et al 1997 resulted in a ∼ 20 ′ wide error box location.…”

Section: Introductionmentioning

confidence: 99%

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A Multiwavelength Investigation of the Relationship between 2CG 135+1 and LSI +61o303

Strickman

Tavani

Coe

et al. 1998

ApJ

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We present the results of a multiwavelength monitoring campaign targeting the γray source 2CG 135+1 in an attempt to confirm the association of this object with the radio/Be/X-ray binary system LSI +61 • 303. The campaign included simultaneous radio, optical, infrared, and hard x-ray/γ-ray observations carried out with a variety of instruments, covering (not continously) almost three binary cycles of LSI +61 • 303 during the period April-July 1994. Three separate OSSE observations of the γ-ray source were carried out, covering different phases of the radio lightcurve. Hard X-ray/γray emission was detected from the direction of 2CG 135+1 during the first of these OSSE observations. The signal to noise ratio of the OSSE observations was insufficient to establish a spectral or intensity correlation of the high-energy emission with simultaneous radio, optical and infrared emission of LSI +61 • 303. We briefly discuss the theoretical implications of our observations.

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Section: The Osse Resultscontrasting

confidence: 64%

Section: Introductionmentioning

confidence: 99%

A Multiwavelength Investigation of the Relationship between 2CG 135+1 and LSI +61o303

Strickman

Tavani

Coe

et al. 1998

ApJ

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“…From the flux values derived for power laws with different spectral indices, we find that the COMPTEL flux points are consistent with a power-law spectrum with spectral index ,-~ 1.7. This spectrum is thus softer than the spectrum measured at energies < 1 MeV (a ~ 1.0, Perotti et al 1980), but not as soft as the spectrum measured at higher energies (a = 2 n+~176 Swanenburg et .v-0.25, al. 1981).…”

Section: Resultsmentioning

confidence: 62%

“…Downloaded to IP: 132.177.229.79 On: Mon, 24 Nov 2014 17:53:37 The COMPTEL data points and 2a upper limit for the time-averaged spectrum of observations 15.0, 31.0 and 34.0. Also plotted are the MISO flux points (Perotti et al 1980) and the COS-B > 100 MeV flux represented by two power laws with spectral indices 1.75 and 2.4 (Swanenburg et al 1981).…”

Section: Resultsmentioning

confidence: 99%

COMPTEL detection of the variable radio source GT 0236+610

Dijk¹,

Bloemen²,

Hermsen³

et al. 1994

AIP Conference Proceedings

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The highly variable and non-thermal radio source GT 0236+610 exhibits outbursts with a period of 26.496 days, modulated by a four-year period. Recent EGRET observations confirmed that this source is the counterpart of the COS-B source 2CG 135+01. COMPTEL observed this source during three observations in Phase I. We report here on the detections in each of the observations, the time-averaged spectrum, and address the question of time variability with respect to the radio phase.

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“…Among the unidentified gamma-ray sources near the Galactic plane [20] 2CG 135+1 is one of the most enigmatic. Since its discovery by the COS-B satellite [14], 2CG 135+1 was observed in the gamma-ray range by several instruments including MISO [10], OSSE [15,13], COMPTEL [23], and EGRET [5]. No radio-loud AGN [1] or strong radio pulsar [9] is known within its refined gammaray error box [5] which includes the cyclic radio flaring Be star LSI 61° 303 [2].…”

Section: The Variable Gamma-ray Source 2cg 1 3 5 +mentioning

confidence: 99%

Non-Blazar Gamma-Ray Variables in the Galactic Plane: A New Class of Gamma-Ray Sources

Tavani

1998

Highlights astron.

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We discuss recent detections of time-variable gamma-ray sources near the Galactic plane. A new bright gamma-ray transient was detected by EGRET in June 1995 near the Galactic center (GRO J1838-04). Also one of the most interesting unidentified gamma-ray sources in the plane, 2CG 135+1, was recently shown to be variable. Both GRO J1838-04 and 2CG 135+1 share many characteristics: variability of the gamma-ray flux within days/weeks, occasional peak gamma-ray emission of comparable flux (˜ 4 x 10-6ph cm-2s-1), absence of radio-loud spectrally-flat AGNs or prominent radio pulsars within their error boxes, lack of strong X-ray and/or hard X-ray counterparts. These characteristics do not match those of either gamma-ray blazars or isolated pulsars. Therefore, GRO J1838-04 and 2CG 135+1 provide strong evidence for the existence of a new class of variable gamma-ray sources.

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Low-energy gamma-ray emission close to CG 135 + 1

Cited by 19 publications

References 0 publications

A Multiwavelength Investigation of the Relationship between 2CG 135+1 and LSI +61o303

A Multiwavelength Investigation of the Relationship between 2CG 135+1 and LSI +61o303

COMPTEL detection of the variable radio source GT 0236+610

Non-Blazar Gamma-Ray Variables in the Galactic Plane: A New Class of Gamma-Ray Sources

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