<scp>psrchive</scp> and <scp>psrfits</scp>: An Open Approach to Radio Pulsar Data Storage and Analysis

Hotan, A. W.; Straten, W. van; Manchester, R. N.

doi:10.1071/as04022

Cited by 859 publications

(812 citation statements)

References 8 publications

(10 reference statements)

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“…The 1.4 GHz NRT values are reproduced from Figure 1(b). These are fundamentally consistent with Parkes measurements at the same frequency, which were obtained from six full-Stokes observations using pulsar digital filterbanks (DFBs) analyzed with PSRCHIVE (Hotan et al 2004) and 12 analog filterbank (AFB) observations.…”

Section: Radio Spectrumsupporting

confidence: 75%

Radio Disappearance of the Magnetar Xte J1810–197 and Continued X-Ray Timing

Camilo

Ransom

Halpern

et al. 2016

ApJ

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135

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We report on timing, flux density, and polarimetric observations of the transient magnetar and 5.54 s radio pulsar XTEJ1810−197 using the Green Bank, Nançay, and Parkes radio telescopes beginning in early 2006, until its sudden disappearance as a radio source in late 2008. Repeated observations through 2016 have not detected radio pulsations again. The torque on the neutron star, as inferred from its rotation frequency derivativeṅ, decreased in an unsteady manner by a factor of three in the first year of radio monitoring, until approximately mid-2007. By contrast, during its final year as a detectable radio source, the torque decreased steadily by only 9%. The periodaveraged flux density, after decreasing by a factor of 20 during the first 10 months of radio monitoring, remained relatively steady in the next 22 months, at an average of 0.7±0.3 mJy at 1.4 GHz, while still showing day-to-day fluctuations by factors of a few. There is evidence that during this last phase of radio activity the magnetar had a steep radio spectrum, in contrast to earlier flat-spectrum behavior. No secular decrease presaged its radio demise. During this time, the pulse profile continued to display large variations; polarimetry, including of a new profile component, indicates that the magnetic geometry remained consistent with that of earlier times. We supplement these results with X-ray timing of the pulsar from its outburst in 2003 up to 2014. For the first 4 years, XTEJ1810 −197 experienced non-monotonic excursions in frequency derivative by at least a factor of eight. But since 2007, itsṅ has remained relatively stable near its minimum observed value. The only apparent event in the X-ray record that is possibly contemporaneous with the radio shutdown is a decrease of ≈20% in the hot-spot flux in 2008-2009, to a stable, minimum value. However, the permanence of the high-amplitude, thermal X-ray pulse, even after the (unexplained) radio demise, implies continuing magnetar activity.

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Section: Radio Spectrumsupporting

confidence: 75%

Radio Disappearance of the Magnetar Xte J1810–197 and Continued X-Ray Timing

Camilo

Ransom

Halpern

et al. 2016

ApJ

Self Cite

135

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“…Software:PRESTO (https://github.com/scottransom/presto), PSRCHIVE (Hotan et al 2004), TEMPO (http://tempo. sourceforge.net/), PINT (https://github.com/nanograv/PINT), IRAF (Tody 1986(Tody , 1993, SCAMP (Bertin & Arnouts 1996 …”

Section: Resultsmentioning

confidence: 99%

“…Subbanded timing data were dedispersed and folded modulo the pulsar's spin period, resulting in files containing subintegrations equivalent in length to the pulsar's spin period and 64 frequency channels across the band. The RFI was removed interactively with pazi, part of the PSRCHIVE pulsar-processing software package 32 (Hotan et al 2004). After downsampling all cleaned detections in time and frequency, the resulting folded profile was used to determine ON/OFF pulse windows of equal size.…”

Section: Nulling and Intermittent Pulsarsmentioning

confidence: 99%

The Green Bank North Celestial Cap Pulsar Survey. III. 45 New Pulsar Timing Solutions

Lynch

Swiggum

Kondratiev

et al. 2018

ApJ

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We provide timing solutions for 45 radio pulsars discovered by the Robert C. Byrd Green Bank Telescope. These pulsars were found in the Green Bank North Celestial Cap pulsar survey, an all-GBT-sky survey being carried out at a frequency of 350 MHz. We include pulsar timing data from the Green Bank Telescope and Low Frequency Array. Our sample includes five fully recycled millisecond pulsars (MSPs, three of which are in a binary system), a new relativistic double neutron star system, an intermediate-mass binary pulsar, a mode-changing pulsar, a 138 ms pulsar with a very low magnetic field, and several nulling pulsars. We have measured two post-Keplerian parameters and thus the masses of both objects in the double neutron star system. We also report a tentative companion mass measurement via Shapiro delay in a binary MSP. Two of the MSPs can be timed with high precision and have been included in pulsar timing arrays being used to search for low-frequency gravitational waves, while a third MSP is a member of the black widow class of binaries. Proper motion is measurable in five pulsars, and we provide an estimate of their space velocity. We report on an optical counterpart to a new black widow system and provide constraints on the optical counterparts to other binary MSPs. We also present a preliminary analysis of nulling pulsars in our sample. These results demonstrate the scientific return of long timing campaigns on pulsars of all types.

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“…Data calibration was conducted using standard data reduction tools (Hotan, van Straten & Manchester 2004). To excise radio-frequency interference, we median-filtered each sub-integration in the frequency domain.…”

Section: Fold-mode Observationsmentioning

confidence: 99%

Limitations in timing precision due to single-pulse shape variability in millisecond pulsars

Shannon

Osłowski

Dai

et al. 2014

Monthly Notices of the Royal Astronomical Society

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114

113

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High-sensitivity radio-frequency observations of millisecond pulsars usually show stochastic, broadband, pulse-shape variations intrinsic to the pulsar emission process. These variations induce jitter noise in pulsar timing observations; understanding the properties of this noise is of particular importance for the effort to detect gravitational waves with pulsar timing arrays. We assess the short-term profile and timing stability of 22 millisecond pulsars that are part of the Parkes Pulsar Timing Array sample by examining intra-observation arrival time variability and single-pulse phenomenology. In 7 of the 22 pulsars, in the band centred at approximately 1400 MHz, we find that the brightest observations are limited by intrinsic jitter. We find consistent results, either detections or upper limits, for jitter noise in other frequency bands. PSR J1909−3744 shows the lowest levels of jitter noise, which we estimate to contribute ∼ 10 ns root mean square error to the arrival times for hour-duration observations. Larger levels of jitter noise are found in pulsars with wider pulses and distributions of pulse intensities. The jitter noise in PSR J0437−4715 decorrelates over a bandwidth of ∼ 2 GHz. We show that the uncertainties associated with timing pulsar models can be improved by including physically motivated jitter uncertainties. Pulse-shape variations will limit the timing precision at future, more sensitive, telescopes; it is imperative to account for this noise when designing instrumentation and timing campaigns for these facilities.

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psrchive and psrfits: An Open Approach to Radio Pulsar Data Storage and Analysis

Cited by 859 publications

References 8 publications

Radio Disappearance of the Magnetar Xte J1810–197 and Continued X-Ray Timing

Radio Disappearance of the Magnetar Xte J1810–197 and Continued X-Ray Timing

The Green Bank North Celestial Cap Pulsar Survey. III. 45 New Pulsar Timing Solutions

Limitations in timing precision due to single-pulse shape variability in millisecond pulsars

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