Pulsars identified from the NRAO VLA Sky Survey

Abstract

We identified 97 strong pulsars from the NRAO VLA Sky Survey (NVSS) at 1.4 GHz north of Dec(J2000) $>-40\degr$. The total flux density, linear polarization intensity and polarization angle (PA) of all pulsars are extracted from the NVSS catalog. The well-calibrated PA measurement of 5 pulsars can be used for absolute PA calibrations in other observations. Comparing the source positions with those in the pulsar catalog, we got the first measurement of the proper motion upper limit of PSR B0031-07, which is $\mu_{\alpha}\cos\delta = -102 \pm 74 mas/yr$ and $\mu_{\delta} = -105 \pm 78 mas/yr$.Comment: 7 pages; 3 figures; one big table; To appear in A&A Supplement

Pulsars in the Westerbork Northern Sky Survey

“…One therefore expects the differences between the pulsar flux densities in the NVSS and the flux densities reported by LYLG to be larger than the differences reported in this study. This is indeed observed: the modulation index of the WENSS sources in Table 2, excluding PSRs J0218+4232, B0329+54 and B2021+51 is 0.40, the modulation index of the NVSS sources in Table 1 of Han & Tian (1999) is 0.60. De Breuck et al (2000) show that the total spectral index distribution of WENSS sources that are correlated with a NVSS source (S 325 > 50 mJy and |b| > 15…”

“…I compare my results with those from Kaplan et al (1998) and Han & Tian (1999), who did similar analyses with data from the 1400 MHz NRAO VLA Sky Survey (NVSS). Section 2 describes the WENSS and Sect.…”

“…Extrapolation of the pulsar spectrum results in an estimated flux density at 325 MHz of 16 ± 3 mJy, much less than that of the WENSS source. Kaplan et al (1998) and Han & Tian (1999) searched the NVSS for pulsar counterparts and also noted that the pulsar is confused by a strong NVSS source 12 away.…”

“…Seventeen of the twenty-five pulsars with a WENSS counterpart are also detected in the NVSS (see Kaplan et al 1998, who did not include PSR B0138+59, and Han & Tian 1999). Two pulsars (PSR B0353+52 and PSR J1518+4904) with a marginal WENSS counterpart coincide with a NVSS source.…”

The INPOP10a planetary ephemeris and its applications in fundamental physics

“…However, by having a long timespan of observations it becomes possible to model the frequencies induced by the companion or to average the DM effect and then reduce significantly the error. Multi wavelength observations of millisecond pulsars are also performed in order to study the physics and the dynamics of these objects as the VLA polarization survey done by Taylor et al (1993) and Han and Tian (1999) or the several year program using VLBA and VLBI techniques begun by Chatterjee et al (2001) to estimate proper motions and parallaxes of about 100 pulsars. The mas level astrometry of pulsars are then an interesting tool for testing planetary ephemerides.…”