Analysis of single pulse radio flux measurements of PSR B1133+16 at 4.85 and 8.35 GHz

Krzeszowski, K.; Maron, O.; Słowikowska, A.; Dyks, J.; Jessner, A.

doi:10.1093/mnras/stu293

Cited by 4 publications

(6 citation statements)

References 21 publications

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“…PSR B1133+16 is one of the strongest and most frequently observed pulsars. Since 2000 there were many observations which allowed us to extend the original data (19 measurements) from Maron et al (2000) with additional 41 measurements that were gathered in Krzeszowski et al (2014). Fig.…”

Section: Psr B1133+16mentioning

confidence: 99%

“…1 shows the results of fitting the flicker noise spectrum to PSR B1133+16 flux measurements. These data were divided into two sets: original set of points from Maron et al (2000) marked with black filled circles and all measurements from Krzeszowski et al (2014) marked with black filled circles and black opened circles altogether. The fits are plotted with solid line and dashed line for Maron's data and Krzeszowski's data, respectively, however both fits are indistinguishable.…”

Section: Psr B1133+16mentioning

confidence: 99%

“…In Krzeszowski et al (2014) we fitted Löhmer model to 60 flux measurements using the least squares method and got the following results: S 0 = 3.39 ± 0.77 Jy, τ = 0.40 ± 0.05 ns, n = 0.118 ± 0.022 and χ 2 red = 4.7. The model is non-linear and the obtained χ 2 red is much greater than 1 and the error distribution is not normal, hence least squares method is not appropriate here (see Sec.…”

Section: Psr B1133+16mentioning

confidence: 99%

“…Flux [mJy] q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q q 0.01 (2000), while black open circles denote 41 additional points gathered in Krzeszowski et al (2014). The fits are plotted with solid line and dashed line for Maron's data and Krzeszowski's datasets, respectively.…”

Section: Psr B1133+16mentioning

confidence: 99%

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Flicker noise pulsar radio spectra

Krzeszowski¹,

Maron²,

Słowikowska³

et al. 2014

Preprint

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We present new results of fitting 108 spectra of radio pulsars with the flicker noise model proposed by Löhmer et al. (2008) and compare them with the spectral indices of power-law fits published by Maron et al. (2000). The fits to the model were carried out using the Markov chain Monte Carlo (MCMC) method appropriate for the non-linear fits. Our main conclusion is that pulsar radio spectra can be statistically very well described by the flicker noise model over wide frequency range from a few tens of MHz up to tens of GHz. Moreover, our dataset allows us to conduct statistical analysis of the model parameters. As our results show, there is a strong negative correlation between the flicker noise spectrum model parameters log S 0 and n and a strong positive relationship between n and the power-law spectral index α. The latter implies that their physical meaning is similar, however the flicker noise model has an advantage over broken power-law model. Not only it describes the spectra in higher frequency range with only two parameters, not counting scaling factor S 0 , but also it shows smooth transition from flat to steep behaviour at lower and higher frequencies, respectively. On the other hand, there are no correlations of the flicker noise model parameters S 0 , τ and n with any of pulsar physical properties.

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Section: Psr B1133+16mentioning

confidence: 99%

Section: Psr B1133+16mentioning

confidence: 99%

Section: Psr B1133+16mentioning

confidence: 99%

Section: Psr B1133+16mentioning

confidence: 99%

See 2 more Smart Citations

Flicker noise pulsar radio spectra

Krzeszowski¹,

Maron²,

Słowikowska³

et al. 2014

Preprint

Self Cite

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show abstract

“…One of the best-studied slow pulsars, PSR B1133+16 shows, at high frequencies (ν > 4 GHz) individual pulses with power-law statistics, of ∼ 2 ms width (Kramer et al 2003;Krzeszowski et al 2014). The bright pulses orig-3 E-mail: ryan.shannon@csiro.au inate predominantly from the trailing edge of the first component of the double-cone profile.…”

Section: Introductionmentioning

confidence: 99%

Two Radio-Emission Mechanisms in PSR J0901–4624

Raithel

Shannon

Johnston

et al. 2015

ApJ

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We have detected sporadic, bright, short-duration radio pulses from PSR J0901−4624. These pulses are emitted simultaneously with persistent, periodic emission that dominates the flux density when averaging over many periods of the pulsar. The bright pulses have energies that are consistent with a power-law distribution. The integrated profile of PSR J0901−4624 is highly polarized and shows four distinct components. The bright pulses appear to originate near the magnetic pole of the pulsar and have polarization properties unlike that of the underlying emission at the same pulse phase. We conclude that the bright pulses represent a secondary giant-micropulse emission process, possibly from a different region in the pulsar magnetosphere.

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A LOFAR census of non-recycled pulsars: average profiles, dispersion measures, flux densities, and spectra

Bilous

Kondratiev

Krämer

et al. 2016

A&A

129

165

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We present first results from a LOFAR census of non-recycled pulsars. The census includes almost all such pulsars known (194 sources) at declinations Dec > 8• and Galactic latitudes |Gb| > 3• , regardless of their expected flux densities and scattering times. Each pulsar was observed for ≥20 min in the contiguous frequency range of 110-188 MHz. Full-Stokes data were recorded. We present the dispersion measures, flux densities, and calibrated total intensity profiles for the 158 pulsars detected in the sample. The median uncertainty in census dispersion measures (1.5 × 10 −3 pc cm −3 ) is ten times smaller, on average, than in the ATNF pulsar catalogue. We combined census flux densities with those in the literature and fitted the resulting broadband spectra with single or broken power-law functions. For 48 census pulsars such fits are being published for the first time. Typically, the choice between single and broken power-laws, as well as the location of the spectral break, were highly influenced by the spectral coverage of the available flux density measurements. In particular, the inclusion of measurements below 100 MHz appears essential for investigating the lowfrequency turnover in the spectra for most of the census pulsars. For several pulsars, we compared the spectral indices from different works and found the typical spread of values to be within 0.5-1.5, suggesting a prevailing underestimation of spectral index errors in the literature. The census observations yielded some unexpected individual source results, as we describe in the paper. Lastly, we will provide this unique sample of wide-band, low-frequency pulse profiles via the European Pulsar Network Database.

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Analysis of single pulse radio flux measurements of PSR B1133+16 at 4.85 and 8.35 GHz

Cited by 4 publications

References 21 publications

Flicker noise pulsar radio spectra

Flicker noise pulsar radio spectra

Two Radio-Emission Mechanisms in PSR J0901–4624

A LOFAR census of non-recycled pulsars: average profiles, dispersion measures, flux densities, and spectra

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