The second Molonglo pulsar survey - discovery of 155 pulsars

Manchester, R. N.; Lyne, A. G.; Taylor, J. H.; Durdin, J. M.; Large, M. I.; Little, A. G.

doi:10.1093/mnras/185.2.409

Cited by 157 publications

(95 citation statements)

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“…However, these observations were not long enough to carry out detailed investigations of nulling and its interaction with the drifting phenomenon. Here, we report results for these pulsars from relatively longer observations, whose basic parameters are listed in Table 1. PSR J1741−0840 (PSR B1738−08) was discovered during the earlier searches (Manchester et al 1978) from the Molonglo telescope in Australia. It is a known drifting pulsar with a few studies (Weltevrede et al 2006(Weltevrede et al , 2007Basu et al 2016) reporting its abnormal drifting behavior.…”

Section: Introductionmentioning

confidence: 99%

On Nulling, Drifting, and Their Interactions in PSRs J1741–0840 and J1840–0840

Gajjar

Yuan

Yuen

et al. 2017

ApJ

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We report detailed investigation of nulling and drifting behavior of two pulsars PSRs J1741−0840 and J1840−0840 observed from the Giant Meterwave Radio Telescope at 625 MHz. PSR J1741−0840 was found to show nulling fraction (NF) of around 30±5% while PSR J1840−0840 was shown to have NF of around 50±6%. We measured drifting behavior from different profile components in PSR J1840−0840 for the first time with the leading component showing drifting with 13.5±0.7 periods while the weak trailing component showed drifting of around 18±1 periods. Large nulling do hamper accuracy of these quantities derived using standard Fourier techniques. A more accurate comparison was drawn from driftband slopes, measured after sub-pulse modeling. These measurements revealed interesting sporadic and irregular drifting behavior in both pulsars. We conclude that the previously reported different drifting periodicities in the trailing component of PSR J1741−0840 is likely due to the spread in these driftband slopes. We also find that both components of PSR J1840−0840 show similar driftband slopes within the uncertainties. Unique nulling-drifting interaction is identified in PSR J1840−0840 where, in most occasions, the pulsar tends to start nulling after what appears to be an end of a driftband. Similarly, when the pulsar switches back to an emission phase, in most occasions it starts at the beginning of a new driftband in both components. Such behaviors have not been detected in any other pulsars to our knowledge. We also found that PSR J1741−0840 seems to have no memory of its previous burst phase while PSR J1840−0840 clearly exhibits memory of its previous state even after longer nulls for both components. We discuss possible explanations for these intriguing nulling-drifting interactions seen in both pulsars based on various pulsar nulling models.

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Section: Introductionmentioning

confidence: 99%

On Nulling, Drifting, and Their Interactions in PSRs J1741–0840 and J1840–0840

Gajjar

Yuan

Yuen

et al. 2017

ApJ

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“…Send offprint requests to: T. Mineo, e-mail: mineo@pa.iasf.cnr.it PSR B0656+14 (P = 0.384 s, τ = P/2Ṗ = 1.1 × 10 5 yr) was discovered by Manchester et al (1978) and its pulsed optical emission was detected by Shearer et al (1997) and Pavlov et al (1997). In the X-ray band a pulsed signal at the radio period was observed by Cordova et al (1989) and γ-ray detection in the EGRET band has been reported by Ramanamurthy et al (1996).…”

Section: Introductionmentioning

confidence: 99%

BeppoSAX observations of the three Gamma-ray pulsars PSR B0656+14, PSR B1055-52 and PSR B1706-44

Mineo

Massaro

Cusumano

et al. 2002

A&A

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Abstract.We report the results of the observations of the three γ-ray pulsars PSR B0656+14, PSR B1055−52 and PSR B1706−44 performed with BeppoSAX. We detected a pulsed emission only for PSR B1055−52: in the range 0.1-6.5 keV the pulse profile is sinusoidal and the statistical significance is 4.5σ. The pulsed fraction was estimated 0.64 ± 0.17. This pulsation was detected also at energies greater than 2.5 keV suggesting either a non-thermal origin or a quite high temperature region on the neutron star surface. Spectral analysis showed that only the X-ray spectrum of PSR B1706−44 can be fitted by a single power-law component, while that of PSR B1055−52 requires also a blackbody component (kT = 0.075 keV) and that of PSR B0656+14 two blackbody components (kT 1 = 0.059, kT 2 = 0.12 keV).

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“…• (Manchester et al 1978), and is in one of the "Fermi bubbles" (Su et al 2010), so that the diffuse background level is higher than might otherwise be expected. Its nearness helps make it detectable.…”

Section: Six Faint Gamma-ray Pulsarsmentioning

confidence: 97%

Six faint gamma-ray pulsars seen with theFermiLarge Area Telescope

Hou

Smith

Guillemot

et al. 2014

A&A

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Context. GeV gamma-ray pulsations from over 140 pulsars have been characterized using the Fermi Large Area Telescope, enabling improved understanding of the emission regions within the neutron star magnetospheres, and the contributions of pulsars to high energy electrons and diffuse gamma rays in the Milky Way. The first gamma-ray pulsars to be detected were the most intense and/or those with narrow pulses. Aims. As the Fermi mission progresses, progressively fainter objects can be studied. In addition to more distant pulsars (thus probing a larger volume of the Galaxy), or ones in high background regions (thus improving the sampling uniformity across the Galactic plane), we detect pulsars with broader pulses or lower luminosity. Adding pulsars to our catalog with inclination angles that are rare in the observed sample, and/or with lower spindown power, will reduce the bias in the currently known gamma-ray pulsar population. Methods. We use rotation ephemerides derived from radio observations to phase-fold gamma rays recorded by the Fermi Large Area Telescope, to then determine the pulse profile properties. Spectral analysis provides the luminosities and, when the signal-to-noise ratio allows, the cutoff energies. We constrain the pulsar distances by different means in order to minimize the luminosity uncertainties.Results. We present six new gamma-ray pulsars with an eclectic mix of properties. Three are young, and three are recycled. They include the farthest, the lowest power, two of the highest duty-cycle pulsars seen, and only the fourth young gamma-ray pulsar with a radio interpulse. We discuss the biases existing in the current gamma-ray pulsar catalog, and steps to be taken to mitigate the bias.

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The second Molonglo pulsar survey - discovery of 155 pulsars

Cited by 157 publications

References 0 publications

On Nulling, Drifting, and Their Interactions in PSRs J1741–0840 and J1840–0840

On Nulling, Drifting, and Their Interactions in PSRs J1741–0840 and J1840–0840

BeppoSAX observations of the three Gamma-ray pulsars PSR B0656+14, PSR B1055-52 and PSR B1706-44

Six faint gamma-ray pulsars seen with theFermiLarge Area Telescope

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