Vela pulsar: single pulses analysis with machine learning techniques

LOUSTO, CARLOS O.; MISSEL, RYAN; PRAJAPATI, HARSHKUMAR; FISCELLA, VALENTINA SOSA; LÓPEZ ARMENGOL, FEDERICO G.; GYAWALI, PRASHNNA KUMAR; WANG, LINWEI; CAHILL, NATHAN D.; COMBI, LUCIANO; DEL PALACIO, SANTIAGO; COMBI, JORGE A.; GANCIO, GUILLERMO; GARCÍA, FEDERICO; GUTIÉRREZ, EDUARDO M.; HAUSCARRIAGA, FERNANDO

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

WILEY-BLACKWELL PUBLISHING, INC

Año: 2022 vol. 509 p. 5790 - 5808

0035-8711

We study individual pulses of Vela (PSR B0833−45/J0835−4510) from daily observations of over 3 h (around 120 000 pulses per observation), performed simultaneously with the two radio telescopes at the Argentine Institute of Radioastronomy. We select four days of observations in 2021 January to March and study their statistical properties with machine learning techniques. We first use Density-Based Spatial Clustering of Applications with Noise clustering techniques, associating pulses mainly by amplitudes, and find a correlation between higher amplitudes and earlier arrival times. We also find a weaker (polarization dependent) correlation with the mean width of the pulses. We identify clusters of the so-called mini-giant pulses, with ∼10 times the average pulse amplitude. We then perform an independent study, with Self-Organizing Maps (SOM) clustering techniques. We use Variational AutoEncoder (VAE) reconstruction of the pulses to separate them clearly from the noise and select one of the days of observation to train VAE and apply it to the rest of the observations. We use SOM to determine four clusters of pulses per day per radio telescope and conclude that our main results are robust and self-consistent. These results support models for emitting regions at different heights (separated each by roughly a hundred km) in the pulsar magnetosphere. We also model the pulses amplitude distribution with interstellar scintillation patterns at the inter-pulses time-scale finding a characterizing exponent nISS ∼ 7–10. In the appendices, we discuss independent checks of hardware systematics with the simultaneous use of the two radio telescopes in different one-polarization/two-polarizations configurations. We also provide a detailed analysis of the processes of radio-interferences cleaning and individual pulse folding.