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Abstract: We report the discovery of eight gamma-ray pulsars in blind frequencysearches using the LAT, onboard the Fermi Gamma-ray Space Telescope. Five ofthe eight pulsars are young tau c<100 kyr, energetic Edot>10^36 erg-s, andlocated within the Galactic plane |b|<3 deg. The remaining three are older,less energetic, and located off the plane. Five pulsars are associated withsources included in the LAT bright gamma-ray source list, but only one, PSRJ1413-6205, is clearly associated with an EGRET source. PSR J1023-5746 has thesmallest characteristic age tau c=4.6 kyr and is the most energeticEdot=1.1E37 erg-s of all gamma-ray pulsars discovered so far in blindsearches. PSRs J1957+5033 and J2055+25 have the largest characteristic agestau c~1 Myr and are the least energetic Edot~5E33 erg-s of thenewly-discovered pulsars. We present the timing models, light curves, anddetailed spectral parameters of the new pulsars. We used recent XMMobservations to identify the counterpart of PSR J2055+25 as XMMUJ205549.4+253959. In addition, publicly available archival Chandra X-ray dataallowed us to identify the likely counterpart of PSR J1023-5746 as a faint,highly absorbed source, CXOU J102302.8-574606. The large X-ray absorptionindicates that this could be among the most distant gamma-ray pulsars detectedso far. PSR J1023-5746 is positionally coincident with the TeV source HESSJ1023-575, located near the young stellar cluster Westerlund 2, while PSRJ1954+2836 is coincident with a 4.3 sigma excess reported by Milagro at amedian energy of 35 TeV. Deep radio follow-up observations of the eight pulsarsresulted in no detections of pulsations and upper limits comparable to thefaintest known radio pulsars, indicating that these can be included among thegrowing population of radio-quiet pulsars in our Galaxy being uncovered by theLAT, and currently numbering more than 20.



Autor: P.M. Saz Parkinson, M. Dormody, M. Ziegler, P.S. Ray, A.A. Abdo, J. Ballet, M.G. Baring, A. Belfiore, T.H. Burnett, G.A. Caliandr

Fuente: https://arxiv.org/







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