A Likely X-ray and Radio Counterpart of the High-Energy Gamma-ray Source 3EG J2227+6122

Details A Likely X-ray and Radio Counterpart of the High-Energy Gamma-ray Source 3EG J2227+6122 A Likely X-ray and Radio Counterpart of the High-Energy Gamma-ray Source 3EG J2227+6122

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...197.6302h&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #63.02; Bulletin of the American Astronomical Society, Vol. 32, p.1507

Astronomy and Astrophysics

Astronomy

Scientific paper

The identity of the persistent EGRET sources in the Galactic plane is largely a mystery. For one of these, \source, our complete census of X-ray and radio sources in its error circle reveals a remarkable superposition of an incomplete radio shell with a flat radio spectrum, and a compact, power-law X-ray source with photon index Γ = 1.5 and with no obvious optical counterpart. The radio shell is polarized at a level of ~= 25%. The anomalous properties of the radio source prevent us from deriving a completely satisfactory theory as to its nature. Nevertheless, using data from \ro, \asca, the VLA, and optical imaging and spectroscopy, we argue that the X-ray source may be a young pulsar with an associated wind-blown bubble or bow shock nebula, and an example of the class of radio-quiet pulsars which are hypothesized to comprise the majority of EGRET sources in the Galaxy. The distance to this source can be estimated from its X-ray absorption as 3 kpc. At this distance, the X-ray and γ -ray luminosities would be ≈ 1.7 x 1033 and ≈ 3.7 x 1035 erg s-1, respectively, which would require an energetic pulsar to power them. If, on the contrary, this X-ray source is not the counterpart of \source, then by process of elimination the X-ray luminosity of the latter must be less than 10-4 of its γ -ray luminosity, a condition not satisfied by any established class of γ -ray source counterpart. This would require the existence of at least a quantitatively new type of EGRET source.

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