Flux density measurements for 32 pulsars in the 20 cm observing band

Xie, Yan-Wei; Wang, Jingbo; Hobbs, G.; Kaczmarek, Jane; Li, Di; Zhang, Jie; Dai, Shi; Cameron, Andrew D.; Zhang, Lei; Miao, Chenchen; Yuan, Mao; Wang, Shen; Zhang, Song-Bo; Xu, Heng; Xu, R. X.

doi:10.1088/1674-4527/19/7/103

Cited by 9 publications

(6 citation statements)

References 20 publications

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“…We estimate the stability of the noise-diode to be better than 3% over the decade of this observing program, which agrees with the estimate by Kerr et al (2020). A detailed study of flux calibration with the Parkes telescope has also been published by Xie et al (2019). The routine was used to measure the flux density, 𝑆 and its error, 𝑒, as follows:…”

Section: Observations and Data Reductionsupporting

confidence: 73%

Flux density variability of 286 radio pulsars from a decade of monitoring

Kumamoto,

Dai,

Johnston

et al. 2020

Preprint

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The Parkes telescope has been monitoring 286 radio pulsars approximately monthly since 2007 at an observing frequency of 1.4 GHz. The wide dispersion measure (DM) range of the pulsar sample and the uniformity of the observing procedure make the data-set extremely valuable for studies of flux density variability and the interstellar medium. Here, we present flux density measurements and modulation indices of these pulsars over this period. We derive the structure function from the light curves and discuss the contributions to it from measurement noise, intrinsic variability and interstellar scintillation. Despite a large scatter, we show that the modulation index is inversely correlated with DM, and can be generally described by a power-law with an index of ∼ −0.7 covering DMs from ∼ 10 to 1000 cm −3 pc. We present refractive timescales and/or lower limits for a group of 42 pulsars. These often have values significantly different from theoretical expectations, indicating the complex nature of the interstellar medium along individual lines of sight. In particular, local structures and non-Kolmogorov density fluctuations are likely playing important roles in the observed flux density variation of many of these pulsars.

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Section: Observations and Data Reductionsupporting

confidence: 73%

Flux density variability of 286 radio pulsars from a decade of monitoring

Kumamoto,

Dai,

Johnston

et al. 2020

Preprint

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“…A switched calibration signal was recorded before or after the observation. The data were calibrated with associated calibration files using the psrchive program pac which flattens the bandpass, flux calibrates and transforms the polarzation products to Stokes parameters (see e.g., Xie et al 2019). Topocentric times of arrival (ToAs) were obtained by cross correlating the mean pulse profile with a noisefree template using psrchive.…”

Section: Observations and Data Processingmentioning

confidence: 99%

Radio Observations of Two Intermittent Pulsars: PSRs J1832+0029 and J1841−0500

Wang

Hobbs

et al. 2020

ApJ

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We present long-term observations of two intermittent pulsars, PSRsJ1832+0029 and J1841−0500, using the Parkes 64 m radio telescope. The radio emission for these pulsars switches off for year-long durations. Our new observations have enabled us to improve the determination of the on-off timescales and the spin-down rates during those emission states. In general our results agree with previous studies of these pulsars, but we now have significantly longer data spans. We have identified two unexpected signatures in the data. Weak emission was detected in a single observation of PSRJ1832+0029 during an off emission state. For PSRJ1841−0500, we identified a quasi-periodic fluctuation in the intensities of the detectable single pulses, with a modulation period between 21 and 36 pulse periods.

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“…The PDFB and CASPSR backend systems can be calibrated (both flux density and polarisation calibration) if (as is usually the case) a switched calibration signal was recorded either prior to or after the observation. The final flux calibration is carried out by relating the calibration signal to the known flux density of Hydra A using the psrchive pulsar signal processing system (Hotan et al 2004, Manchester et al 2013and Xie et al 2019. We formed analytic templates for the bright and weak emission modes separately from our observations using paas and then obtained the flux density estimate using psrflux, which matches the template with the observation and determines the area under the template.…”

Section: Observationsmentioning

confidence: 99%

Probing the Emission States of PSR J1107−5907

Wang

Hobbs

Kerr

et al. 2020

ApJ

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The emission from PSR J1107−5907 is erratic. Sometimes the radio pulse is undetectable, at other times the pulsed emission is weak, and for short durations the emission can be very bright. In order to improve our understanding of these state changes, we have identified archival data sets from the Parkes radio telescope in which the bright emission is present, and find that the emission never switches from the bright state to the weak state, but instead always transitions to the "off" state. Previous work had suggested the identification of the "off" state as an extreme manifestation of the weak state. However, the connection between the "off" and bright emission reported here suggests that the emission can be interpreted as undergoing only two emission states: a "bursting" state consisting of both bright pulses and nulls as well as the weak-emission state.

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Flux density measurements for 32 pulsars in the 20 cm observing band

Cited by 9 publications

References 20 publications

Flux density variability of 286 radio pulsars from a decade of monitoring

Flux density variability of 286 radio pulsars from a decade of monitoring

Radio Observations of Two Intermittent Pulsars: PSRs J1832+0029 and J1841−0500

Probing the Emission States of PSR J1107−5907

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