========================================================================== J/A+A/492/923 Pulsar Timing for Fermi Gamma-ray Space Telescope (Smith+, 2008) The following files can be converted to FITS (extension .fit .fgz or .fiZ) table1.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/A+A/492/923 ==========================================================================
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Beginning of ReadMe : J/A+A/492/923 Pulsar Timing for Fermi Gamma-ray Space Telescope (Smith+, 2008) ================================================================================ Pulsar Timing for the Fermi Gamma-ray Space Telescope. Smith D.A., Guillemot L., Camilo F., Cognard I., Dumora D., Espinoza C., Freire P.C.C., Gotthelf E.V., Harding A.K., Hobbs G.B., Johnston S., Kaspi V.M., Kramer M., Livingstone M.A., Lyne A.G., Manchester R.N., Marshall F.E., McLaughlin M.A., Noutsos A., Ransom S.M., Roberts M.S.E., Romani R.W., Stappers B.W., Theureau G., Thompson D.J., Thorsett S.E., Wang N., Weltevrede P. <Astron. Astrophys. 492, 923 (2008)> =2008A&A...492..923S ================================================================================ ADC_Keywords: Pulsars ; Radio sources ; Gamma rays Keywords: space vehicles: instruments - stars: pulsars: general - gamma-rays: observations - ephemerides Abstract: We describe a comprehensive pulsar monitoring campaign for the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope (formerly GLAST). The detection and study of pulsars in gamma rays give insights into the populations of neutron stars and supernova rates in the Galaxy, into particle acceleration mechanisms in neutron star magnetospheres, and into the "engines" driving pulsar wind nebulae. LAT's unprecedented sensitivity between 20MeV and 300GeV together with its 2.4sr field-of-view makes detection of many gamma-ray pulsars likely, justifying the monitoring of over two hundred pulsars with large spin-down powers. To search for gamma-ray pulsations from most of these pulsars requires a set of phase-connected timing solutions spanning a year or more to properly align the sparse photon arrival times. We describe the choice of pulsars and the instruments involved in the campaign. Description: Pulsars being timed for the Fermi Large Area Telescope (all known pulsars with dE/dt>10^34^ergs/s), ordered by sqrt(dE/dt)/d^2^, where dE/dt is the spin-down energy loss rate and d is the distance. sqrt(dE/dt)/d^2^ as an indicator of expected gamma flux suffers many large uncertainties (see text).
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