This catalog summarizes 117 high-confidence > 0.1 GeV gamma-ray pulsar detections using three years of data acquired by the Large Area Telescope (LAT) on the Fermi satellite. Half are neutron stars discovered using LAT data, through periodicity searches in gamma-ray and radio data around LAT unassociated source positions. The 117 pulsars are evenly divided into three groups: millisecond pulsars, young radio-loud pulsars, and young radio-quiet pulsars. We characterize the pulse profiles and energy spectra and derive luminosities when distance information exists. Spectral analysis of the off-peak phase intervals indicates probable pulsar wind nebula emission for four pulsars, and off-peak magnetospheric emission for several young and millisecond pulsars. We compare the gamma-ray properties with those in the radio, optical, and X-ray bands. We provide flux limits for pulsars with no observed gamma-ray emission, highlighting a small number of gamma-faint, radio-loud pulsars. The large, varied gamma-ray pulsar sample constrains emission models. Fermi's selection biases complement those of radio surveys, enhancing comparisons with predicted population distributions.

/pdf/the-second-fermi-large-area-telescope-catalog-of-gamma-ray-4q11dsexhc.pdf

The second fermi large area telescope catalog of gamma-ray pulsars

We investigate the birth and evolution of Galactic isolated radio pulsars. We begin by estimating their birth space velocity distribution from proper-motion measurements of Brisken and coworkers. We find no evidence for multimodality of the distribution and favor one in which the absolute one-dimensional velocity components are exponentially distributed and with a three-dimensional mean velocity of 380 km s-1. We then proceed with a Monte Carlo-based population synthesis, modeling the birth properties of the pulsars, their time evolution, and their detection in the Parkes and Swinburne Multibeam surveys. We present a population model that appears generally consistent with the observations. Our results suggest that pulsars are born in the spiral arms, with a galactocentric radial distribution that is well described by the functional form proposed by Yusifov & Kucuk, in which the pulsar surface density peaks at radius ~3 kpc. The birth spin period distribution extends to several hundred milliseconds, with no evidence of multimodality. Models that assume the radio luminosities of pulsars to be independent of the spin periods and period derivatives are inadequate, as they lead to the detection of too many old simulated pulsars in our simulations. Dithered radio luminosities proportional to the square root of the spin-down luminosity accommodate the observations well and provide a natural mechanism for the pulsars to dim uniformly as they approach the death line, avoiding an observed pileup on the latter. There is no evidence for significant torque decay (due to magnetic field decay or otherwise) over the lifetime of the pulsars as radio sources (~100 Myr). Finally, we estimate the pulsar birthrate and total number of pulsars in the Galaxy.

https://iopscience.iop.org/article/10.1086/501516/pdf

Birth and Evolution of Isolated Radio Pulsars

We review the main properties, demographics and applications of binary and millisecond radio pulsars. Our knowledge of these exciting objects has greatly increased in recent years, mainly due to successful surveys which have brought the known pulsar population to over 1800. There are now 83 binary and millisecond pulsars associated with the disk of our Galaxy, and a further 140 pulsars in 26 of the Galactic globular clusters. Recent highlights include the discovery of the young relativistic binary system PSR J1906+0746, a rejuvination in globular cluster pulsar research including growing numbers of pulsars with masses in excess of 1.5M , a precise measurement of relativistic spin precession in the double pulsar system and a Galactic millisecond pulsar in an eccentric (e = 0.44) orbit around an unevolved companion.

/pdf/binary-and-millisecond-pulsars-25dp443qnv.pdf

Binary and Millisecond Pulsars

Anomalous X-ray pulsars (AXPs) are slowly rotating neutron stars with very bright and highly variable X-ray emission that are believed to be powered by ultra-strong magnetic fields of >10(14) G, according to the 'magnetar' model. The radio pulsations that have been observed from more than 1,700 neutron stars with weaker magnetic fields have never been detected from any of the dozen known magnetars. The X-ray pulsar XTE J1810-197 was revealed (in 2003) as the first AXP with transient emission when its luminosity increased 100-fold from the quiescent level; a coincident radio source of unknown origin was detected one year later. Here we show that XTE J1810-197 emits bright, narrow, highly linearly polarized radio pulses, observed at every rotation, thereby establishing that magnetars can be radio pulsars. There is no evidence of radio emission before the 2003 X-ray outburst (unlike ordinary pulsars, which emit radio pulses all the time), and the flux varies from day to day. The flux at all radio frequencies is approximately equal--and at >20 GHz XTE J1810-197 is currently the brightest neutron star known. These observations link magnetars to ordinary radio pulsars, rule out alternative accretion models for AXPs, and provide a new window into the coronae of magnetars.

https://arxiv.org/pdf/astro-ph/0605429.pdf

Transient pulsed radio emission from a magnetar

We present pulsar timing solutions for 374 pulsars. Each ephemeris was obtained by analysing archival data stored at Jodrell Bank Observatory. This data archive contains over 5600 yr of pulsar rotational history with individual data-spans of up to 34 yr. A new method has been developed to mitigate the effects of timing noise by whitening the pulsar timing residuals. This whitening is applied before standard fitting procedures are followed to measure the astrometric and dispersion measure (DM) parameters of a pulsar. We show that the values obtained using this new technique are consistent with other methods, and that the new timing solutions are, in general, significantly more precise than those in earlier publications. We consider the second derivative of the frequency of pulsars, ‹ , and the DM gradient, d(DM)/ dt ,i ndetail. The ‹ values are obtained by fitting to timing residuals that have not been whitened and are found to be orders of magnitude larger than those expected from magnetic dipole radiation; the measured values are dominated by the effects of timing noise, and therefore lead to braking indices that are not consistent with magnetic dipole radiation. We find a dependence between |d(DM)/ dt| and DM of |d(DM)/ dt | 0 .0002 DM cm a3 pc yr a1 , which allows DM variations to be estimated for any radio pulsar. Ke yw ords: methods: data analysis — astrometry — pulsars: general.

Long‐term timing observations of 374 pulsars

Multifrequency flux density measurements of 280 pulsars

Polarimetric observations of 300 pulsars have been conducted with the 76-m Lovell telescope at Jodrell Bank at radio frequencies centred around 230, 400, 600, 920, 1400 and 1600 MHz. More than half of the pulsars have no previously published polarization profiles and this compilation represents about three times the sum of all previously published pulsar polarization data. A selection of integrated polarization profiles is provided. Tables of pulse widths and the degree of both linear and circular polarization are given for all pulsars, and these act as an index for all the data, which are available by anonymous ftp in numerical and graphical form.

/pdf/multifrequency-polarimetry-of-300-radio-pulsars-wz797a8jv7.pdf

D. M. Gould

Papers

Multifrequency flux density measurements of 280 pulsars

Multifrequency polarimetry of 300 radio pulsars

Polarization and Faraday rotation measurements of southern pulsars