Abstract:We describe PSR J1926−0652, a pulsar recently discovered with the Five-hundred-meter Aperture Spherical radio Telescope (FAST). Using sensitive single-pulse detections from FAST and long-term timing observations from the Parkes 64-m radio telescope, we probed phenomena on both long and short time scales. The FAST observations covered a wide frequency range from 270 to 800 MHz, enabling individual pulses to be studied in detail. The pulsar exhibits at least four profile components, short-term nulling lasting fr… Show more
“…Of the remaining pulsars, PSR J1517-4356 has no particularly distinguishing characteristics (Edwards et al 2001), but we note unique phenomenology for the remaining candidates. PSR J0048+3412 (Herfindal & Rankin 2009), PSR J1926-0652 (Zhang et al 2019), and PSR J2048-1616 (Ritchings 1976) are nulling pulsars while PSR J1705-04 is a Rotating RAdio Transient (RRAT) (Karako-Argaman et al 2015). PSR J1405-4656 is a binary millisecond pulsar (Bates et al 2015).…”
We report on a likelihood stacking search for gamma-ray pulsars at 525 high latitude locations that coincide with known radio pulsar positions. We report 8 newly detected or associated pulsar candidates and 36 sub-threshold pulsar candidates. Stacking their likelihood profiles in spectral parameter space implies a pulsar-like spectral index and a flux one order of magnitude below the Fermi sensitivity. The same procedures performed on empty control fields imply a high false detection rate (20-50%) although the stacked spectra are distinctly softer than the pulsars. This study also probes a unique region of parameter space populated by older, transitional, and recycled (millisecond) pulsars. Many of these sources have lower rotational energy loss rates implying that the empirical γ-ray "death line" could be predominantly a sensitivity limit. Their luminosities, however, are consistent with the heuristic relation between spin-down power and γ-ray luminosity. If their pulsar nature can be confirmed, these results will expand the number of γ-ray pulsars by 16%. Furthermore, the improved millisecond pulsar luminosity function with these new sources can help characterize their possible contribution to the Galactic center GeV excess.
“…Of the remaining pulsars, PSR J1517-4356 has no particularly distinguishing characteristics (Edwards et al 2001), but we note unique phenomenology for the remaining candidates. PSR J0048+3412 (Herfindal & Rankin 2009), PSR J1926-0652 (Zhang et al 2019), and PSR J2048-1616 (Ritchings 1976) are nulling pulsars while PSR J1705-04 is a Rotating RAdio Transient (RRAT) (Karako-Argaman et al 2015). PSR J1405-4656 is a binary millisecond pulsar (Bates et al 2015).…”
We report on a likelihood stacking search for gamma-ray pulsars at 525 high latitude locations that coincide with known radio pulsar positions. We report 8 newly detected or associated pulsar candidates and 36 sub-threshold pulsar candidates. Stacking their likelihood profiles in spectral parameter space implies a pulsar-like spectral index and a flux one order of magnitude below the Fermi sensitivity. The same procedures performed on empty control fields imply a high false detection rate (20-50%) although the stacked spectra are distinctly softer than the pulsars. This study also probes a unique region of parameter space populated by older, transitional, and recycled (millisecond) pulsars. Many of these sources have lower rotational energy loss rates implying that the empirical γ-ray "death line" could be predominantly a sensitivity limit. Their luminosities, however, are consistent with the heuristic relation between spin-down power and γ-ray luminosity. If their pulsar nature can be confirmed, these results will expand the number of γ-ray pulsars by 16%. Furthermore, the improved millisecond pulsar luminosity function with these new sources can help characterize their possible contribution to the Galactic center GeV excess.
“…The radiation mechanism of pulsars has been studied by analyzing the structure of single pulses. 9 , 10 The scintillation of interstellar plasma has also been studied using pulsar observations, 11 and characteristic scintillation arcs have been detected ( Figure 3 ). Figure 2 The Sketch and the Timing Results of M92A and M13E (A) A cartoon to show the binary system M92A.…”
FAST has found more than 240 pulsars, including pulsars in binary systems-FAST has made great progress in the study of fast radio bursts-The FAST team will call for proposals from the whole world in 2021
“…Data taken subsequently are still being processed. While we report on FRB searches here, we note that the CRAFTS survey has already discovered over 100 new pulsars 14 (Qian et al 2019;Zhang et al 2019a).…”
Section: Fast Drift Scan Surveymentioning
confidence: 99%
“…These candidates were subsequently plotted and inspected by eye. This GPU single pulse search system (enabled by PICS) helped in the discovery of over 20 new pulsars in the FAST drift scan survey, including those reported in Qian et al (2019) and Zhang et al (2019a). This PICS-aided search system uses non-standard ranking criteria.…”
We report the discovery of a highly dispersed fast radio burst (FRB), FRB181123, from an analysis of ∼1500 hr of drift scan survey data taken using the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The pulse has three distinct emission components, which vary with frequency across our 1.0-1.5 GHz observing band. We measure the peak flux density to be >0.065 Jy and the corresponding fluence >0.2 Jy ms. Based on the observed dispersion measure of 1812 cm −3 pc, we infer a redshift of ∼1.9. From this, we estimate the peak luminosity and isotropic energy to be 2×10 43 erg s −1 and 2×10 40 erg, respectively. With only one FRB from the survey detected so far, our constraints on the event rate are limited. We derive a 95% confidence lower limit for the event rate of 900 FRBs per day for FRBs with fluences >0.025 Jy ms. We performed follow-up observations of the source with FAST for four hours and have not found a repeated burst. We discuss the implications of this discovery for our understanding of the physical mechanisms of FRBs.
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