First results of the glitching pulsar monitoring programme at the Argentine Institute of Radioastronomy

Ezequiel, Zubieta,; Missel, Ryan; Fiscella, Valentina Sosa; Lousto, Carlos O.; Palacio, Santiago; Armengol, Federico G. Lopez; García, Federico; Combi, J. A.; Wang, Linwei; Combi, Luciano; Gancio, G.; Negrelli, Carolina Soledad; Gutiérrez, Eduardo Mario

doi:10.1093/mnras/stad723

Cited by 4 publications

(2 citation statements)

References 39 publications

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“…For example, the Argentine Institute of Radio Astronomy has two single-dish telescopes capable of performing daily pulsar monitoring, which could contribute to improving the IPTA sensitivity to single sources of GWs . However, their observations use instantaneous bandwidths of 112 MHz and 56 MHz (Zubieta et al 2023). Therefore, using this type of analysis to account for DM misestimates might prove of foremost importance in achieving the timing precision required for them to be contributing to future IPTA data sets.…”

Section: Discussionmentioning

confidence: 99%

The NANOGrav 12.5-Year Data Set: Dispersion Measure Misestimations with Varying Bandwidths

Sosa Fiscella,

Lam,

Arzoumanian

et al. 2024

ApJ

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Noise characterization for pulsar-timing applications accounts for interstellar dispersion by assuming a known frequency dependence of the delay it introduces in the times of arrival (TOAs). However, calculations of this delay suffer from misestimations due to other chromatic effects in the observations. The precision in modeling dispersion is dependent on the observed bandwidth. In this work, we calculate the offsets in infinite-frequency TOAs due to misestimations in the modeling of dispersion when using varying bandwidths at the Green Bank Telescope. We use a set of broadband observations of PSR J1643−1224, a pulsar with unusual chromatic timing behavior. We artificially restricted these observations to a narrowband frequency range, then used both the broad- and narrowband data sets to calculate residuals with a timing model that does not account for time variations in the dispersion. By fitting the resulting residuals to a dispersion model and comparing the fits, we quantify the error introduced in the timing parameters due to using a reduced frequency range. Moreover, by calculating the autocovariance function of the parameters, we obtained a characteristic timescale over which the dispersion misestimates are correlated. For PSR J1643−1224, which has one of the highest dispersion measures (DM) in the NANOGrav pulsar timing array, we find that the infinite-frequency TOAs suffer from a systematic offset of ∼22 μs due to incomplete frequency sampling, with correlations over about one month. For lower-DM pulsars, the offset is ∼7 μs. This error quantification can be used to provide more robust noise modeling in the NANOGrav data, thereby increasing the sensitivity and improving the parameter estimation in gravitational wave searches.

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Section: Discussionmentioning

confidence: 99%

The NANOGrav 12.5-Year Data Set: Dispersion Measure Misestimations with Varying Bandwidths

Sosa Fiscella,

Lam,

Arzoumanian

et al. 2024

ApJ

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“…While the process that causes pulsars to glitch has still not yet been definitively identified, their impacts on timing have been addressed in many studies (e.g., Lower et al 2021;Dunn et al 2022;Zubieta et al 2023). In a simple case, the glitch appears in timing residuals as an instantaneous change in the slope.…”

Section: Introductionmentioning

confidence: 99%

The Green Bank North Celestial Cap Survey. IX. Timing Follow-up for 128 Pulsars

McEwen,

Swiggum,

Kaplan

et al. 2024

ApJ

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The Green Bank North Celestial Cap survey is one of the largest and most sensitive searches for pulsars and transient radio objects. Observations for the survey have finished; priorities have shifted toward long-term monitoring of its discoveries. In this study, we have developed a pipeline to handle large data sets of archival observations and connect them to recent, high-cadence observations taken using the Canadian Hydrogen Intensity Mapping Experiment telescope. This pipeline handles data for 128 pulsars and has produced measurements of spin, positional, and orbital parameters that connect data over observation gaps as large as 2000 days. We have also measured glitches in the timing residuals for five of the pulsars included and proper motion for 19 sources (13 new). We include updates to orbital parameters for 19 pulsars, including nine previously unpublished binaries. For two of these binaries, we provide updated measurements of post-Keplerian binary parameters, which result in much more precise estimates of the total masses of both systems. For PSR J0509+3801, the much improved measurement of the Einstein delay yields much improved mass measurements for the pulsar and its companion, 1.399(6) M ⊙ and 1.412(6) M ⊙, respectively. For this system, we have also obtained a measurement of the orbital decay due to the emission of gravitational waves, P ̇ B = − 1.37 ( 7 ) × 10 − 12 , which is in agreement with the rate predicted by general relativity for these masses.

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Timing irregularities and glitches from the pulsar monitoring campaign at IAR

Zubieta,

García,

del Palacio

et al. 2024

A&A

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Pulsars have a very stable rotation overall. However, sudden increases in their rotation frequency, known as glitches, perturb their evolution. While many observatories commonly detect large glitches, small glitches are harder to detect because of the lack of daily cadence observations over long periods of time (years). We aim to explore and characterise the timing behaviour of young pulsars on daily timescales, looking for small glitches and other irregularities, in order to further our comprehension of the real distribution of glitch sizes. Our findings have consequences for the theoretical modelling of the glitch mechanism. We observed six pulsars with up to daily cadence between December 2019 and January 2024 with the two antennas of the Argentine Institute of Radio Astronomy (IAR). We used standard pulsar timing tools to obtain the times of arrival of the pulses and to characterise the pulsar's rotation. We developed an algorithm to look for small timing events in the data and calculate the changes in the frequency (nu ) and its derivative ($ at those epochs. We find that the rotation of all pulsars in this dataset is affected by small step changes in nu and $ Among them, we find three new glitches that have not been reported before: two glitches in PSR J1048$-$5832 with relative sizes of $ $ and $ $, and one glitch in the Vela pulsar with a size of $ $. We also report new decay terms on the 2021 Vela giant glitch, and on the 2022 giant glitches in PSR J0742$-$2822 and PSR J1740$-$3015, respectively. In addition, we find that the red noise contribution significantly diminished in PSR J0742$-$2822 after its giant glitch in 2022. Our results highlight the importance of high-cadence monitoring with an exhaustive analysis of the residuals to better characterise the distribution of glitch sizes and to deepen our understanding of the mechanisms behind glitches, red noise, and timing irregularities.

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First results of the glitching pulsar monitoring programme at the Argentine Institute of Radioastronomy

Cited by 4 publications

References 39 publications

The NANOGrav 12.5-Year Data Set: Dispersion Measure Misestimations with Varying Bandwidths

The NANOGrav 12.5-Year Data Set: Dispersion Measure Misestimations with Varying Bandwidths

The Green Bank North Celestial Cap Survey. IX. Timing Follow-up for 128 Pulsars

Timing irregularities and glitches from the pulsar monitoring campaign at IAR

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