X-ray, Radio, and Optical Observations of the Putative Pulsar in the Supernova Remnant CTA 1Reportar como inadecuado



 X-ray, Radio, and Optical Observations of the Putative Pulsar in the Supernova Remnant CTA 1


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A Chandra image of the central X-ray source RX J0007.0+7303 in the supernova remnant CTA 1 reveals a point source, a compact nebula, and a bent jet, all of which are characteristic of energetic, rotation-powered pulsars. Using the MDM 2.4m telescope we obtain upper limits in the optical at the position of the point source, J2000 00h07m01.56s, +73o0308.1-, determined to an accuracy of 0.1-, of B25.4, V24.8, R25.1, and I23.7; these correspond to an X-ray-to-optical flux ratio 100. Neither a VLA image at 1425 MHz, nor a deep pulsar search at 820 MHz using the NRAO Green Bank Telescope, reveal a radio pulsar counterpart to an equivalent luminosity limit at 1400 MHz of 0.02 mJy kpc^2, which is equal to the lowest luminosity known for any radio pulsar. The Chandra point source accounts for about 30% of the flux of RX J0007.0+7303, while its compact nebula plus jet comprise about 70%. The X-ray spectrum of the point source is fitted with a power-law plus blackbody model with Gamma = 1.6+-0.6, kT {infty} = 0.13+-0.05 keV, and R infty = 0.37 km, values typical of a young pulsar. An upper limit of T^{infty} e 6.6x10^5 K to the effective temperature of the entire neutron star surface is derived, which is one of the most constraining data points on cooling models. The 0.5-10 keV luminosity of RX J0007.0+7303 is 4x10^{31}d-1.4 kpc^2 ergs s^{-1}, but the larger ~18 diameter synchrotron nebula in which it is embedded is two orders of magnitude more luminous. These properties allow us to estimate, albeit crudely, that the spin-down luminosity of the underlying pulsar is in the range 10^{36}-10^{37} ergs s^{-1}, and support the identification of the high-energy gamma-ray source 3EG J0010+7309 as a pulsar even though its spin parameters have not yet been determined.



Autor: J. P. Halpern; E. V. Gotthelf; F. Camilo; D. J. Helfand; S. M. Ransom

Fuente: https://archive.org/







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