Zapata Vélez, Alnaldo J.

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    Possible radius-to-intensity mapping in pulsar magnetospheres from observations with the Arecibo radio telescope
    (2022-12-13) Zapata Vélez, Alnaldo J.; Radovan, Henri A.; College of Arts and Sciences - Sciences; Méndez Mella, Héctor; Santana-Colón, Samuel; Department of Physics; Quiñones Otal, Emilia
    We used the Arecibo Observatory and the Mock spectrometers to conduct pulsar radio observations at frequencies of 433, 1169 and 1620 MHz for two targets: PSR B0525+21 and PSR B0611+22. Radius-to-Frequency Mapping (RFM) states that there is a mathematical relationship between the emission height of pulses within the first open field lines at the magnetic poles and the observing frequency. In analogy to RFM, we hypothesize that the peak flux density of pulses might be related to their emission heights as a Radius-to-Intensity Mapping (RIM). The recorded data was flux calibrated with the radiometer equation to convert arbitrary units into janskys (Jy). We sorted single pulses by their peak flux density using a MATLAB algorithm and divided them into five increasing intensity bins for each observing frequency, where an average profile was generated for each bin. For each frequency, we measured the widths and emission heights of the average profiles at 3% intensity level. We plotted single pulse equivalent widths, energies, and intensities to further investigate RIM. Our results show that the intensity of pulses is weakly related to their emission height; emission at a particular frequency originates from a small range of emission heights. We also found that for all frequencies and both pulsars, the emission height radius of pulses decreases with increasing frequency, validating RFM.