Pulse Morphology of the Galactic Center Magnetar PSR J1745–2900

Pearlman, Aaron B.; Majid, Walid A.; Prince, Thomas A.; Kocz, J.; Horiuchi, S.

doi:10.3847/1538-4357/aade4d

Cited by 42 publications

(74 citation statements)

References 88 publications

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“…Shortly after the discovery of radio pulsations from J1745−2900, several measurements of the dispersion and scattering were made. Eatough et al (2013) Our measurement of a 10 GHz pulse broadening time of τ sc,10 = 0.09±0.03 ms is consistent with the τ sc,10 = 0.1−0.3 ms expected at 10 GHz from the Spitler et al (2014) scattering relation, but is much less than the τ sc,10 ≈ 3 ms expected from the Pearlman et al (2018) result. Our DM measurement of DM = 1760.0 +2.4 −1.3 pc cm −3 is consistent with the DM = 1762 ± 11 pc cm −3 value seen by Desvignes et al (2018) over a four year span.…”

Section: Comparison With Previous Resultssupporting

confidence: 86%

VLA Observations of Single Pulses from the Galactic Center Magnetar

Wharton

Chatterjee

Cordes

et al. 2019

ApJ

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We present the results of a 7-12 GHz phased-array study of the Galactic center magnetar J1745−2900 with the Karl G. Jansky Very Large Array (VLA). Using data from two 6.5 hour observations from September 2014, we find that the average profile is comprised of several distinct components at these epochs and is stable over ∼day timescales and ∼GHz frequencies. Comparison with additional phased VLA data at 8.7 GHz shows significant profile changes on longer timescales. The average profile at 7-12 GHz is dominated by the jitter of relatively narrow pulses. The pulses in each of the four main profile components seen in September 2014 are uncorrelated in phase and amplitude, though there is a small but significant correlation in the occurrence of pulses in two of the profile components. Using the brightest pulses, we measure the dispersion and scattering parameters of J1745−2900. A joint fit of 38 pulses gives a 10 GHz pulse broadening time of τ sc,10 = 0.09 ± 0.03 ms and a dispersion measure of DM = 1760 +2.4 −1.3 pc cm −3 . Both of these results are consistent with previous measurements, which suggests that the scattering and dispersion measure of J1745−2900 may be stable on timescales of several years.

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Section: Comparison With Previous Resultssupporting

confidence: 86%

VLA Observations of Single Pulses from the Galactic Center Magnetar

Wharton

Chatterjee

Cordes

et al. 2019

ApJ

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“…These bands are not caused by interstellar scintillation, and rather likely to be either intrinsic to the emission process or caused by exotic propagation effects like plasma lensing. Similar frequency bands, albeit without the drifting in some cases, have also been observed from a number of Galactic neutron stars (the Crab pulsar PSR B0531+21, Hankins et al 2016; the Galactic Center Magnetar PSR J1745−2900, Pearlman et al 2018;Magnetar XTE J1810−197, Maan et al 2019). However, any links between these galactic neutron stars and FRBs are as yet unclear, and require further study.…”

Section: Introductionsupporting

confidence: 65%

Repeating fast radio bursts with WSRT/Apertif

Oostrum

Maan

Leeuwen

et al. 2020

A&A

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Context. Repeating fast radio bursts (FRBs) present excellent opportunities to identify FRB progenitors and host environments, as well as decipher the underlying emission mechanism. Detailed studies of repeating FRBs might also hold clues to the origin of FRBs as a population. Aims. We aim to detect bursts from the first two repeating FRBs: FRB 121102 (R1) and FRB 180814.J0422+73 (R2), and characterise their repeat statistics. We also want to significantly improve the sky localisation of R2 and identify its host galaxy. Methods. We use the Westerbork Synthesis Radio Telescope to conduct extensive follow-up of these two repeating FRBs. The new phased-array feed system, Apertif, allows covering the entire sky position uncertainty of R2 with fine spatial resolution in a single pointing. The data were searched for bursts around the known dispersion measures of the two sources. We characterise the energy distribution and the clustering of detected R1 bursts. Results. We detected 30 bursts from R1. The non-Poissonian nature is clearly evident from the burst arrival times, consistent with earlier claims. Our measurements indicate a dispersion measure of 563.5(2) pc cm −3 , suggesting a significant increase in DM over the past few years. Assuming a constant position angle across the burst, we place an upper limit of 8% on the linear polarisation fraction for the brightest burst in our sample. We did not detect any bursts from R2. Conclusions. A single power-law might not fit the R1 burst energy distribution across the full energy range or widely separated detections. Our observations provide improved constraints on the clustering of R1 bursts. Our stringent upper limits on the linear polarisation fraction imply a significant depolarisation, either intrinsic to the emission mechanism or caused by the intervening medium, at 1400 MHz that is not observed at higher frequencies. The non-detection of any bursts from R2, despite nearly 300 hrs of observations, implies either a highly clustered nature of the bursts, a steep spectral index, or a combination of both assuming the source is still active. Another possibility is that R2 has turned off completely, either permanently or for an extended period of time.

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“…Similar structures have been seen in the second repeating FRB as well (CHIME/FRB Collaboration et al 2019). Except for the high-frequency interpulse giantpulses from the Crab pulsar (Hankins et al 2016) and in some faint emission components of PSR 1745−2900 (Pearlman et al 2018), such frequency structures have not been seen from any known pulsar or magnetar. In Figure 4, we show that the spiky emission from J1810−197 also exhibits frequency structures which cannot be caused by the ISM scintillation.…”

Section: Any Links With Frbs?mentioning

confidence: 96%

Distinct Properties of the Radio Burst Emission from the Magnetar XTE J1810–197

Maan

Joshi

Surnis

et al. 2019

ApJL

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XTE J1810−197 (PSR J1809−1943 was the first ever magnetar which was found to emit transient radio emission. It has recently undergone another radio and high-energy outburst. This is only the second radio outburst that has been observed from this source. We observed J1810−197 soon after its recent radio outburst at low radio frequencies using the Giant Metrewave Radio Telescope. We present the 650 MHz flux density evolution of the source in the early phases of the outburst, and its radio spectrum down to frequencies as low as 300 MHz. The magnetar also exhibits radio emission in the form of strong, narrow bursts. We show that the bursts have a characteristic intrinsic width of the order of 0.5−0.7 ms, and discuss their properties in the context of giant pulses and giant micropulses from other pulsars. We also show that the bursts exhibit spectral structures which cannot be explained by interstellar propagation effects. These structures might indicate a phenomenological link with the repeating fast radio bursts which also show interesting, more detailed frequency structures. While the spectral structures are particularly noticeable in the early phases of the outburst, these seem to be less prominent as well as less frequent in the later phases, suggesting an evolution of the underlying cause of these spectral structures.

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Pulse Morphology of the Galactic Center Magnetar PSR J1745–2900

Cited by 42 publications

References 88 publications

VLA Observations of Single Pulses from the Galactic Center Magnetar

VLA Observations of Single Pulses from the Galactic Center Magnetar

Repeating fast radio bursts with WSRT/Apertif

Distinct Properties of the Radio Burst Emission from the Magnetar XTE J1810–197

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