Searches for Fast Radio Transients

By Jim Cordes, M. Mclaughlin. 2003

252 citations recorded by the source corpus.

We discuss optimal detection of fast radio transients from astrophysical objects while taking into account the effects of propagation through intervening ionized media, including dispersion, scattering, and scintillation. Our analysis applies to the giant-pulse phenomenon exhibited by some pulsars, for which we show examples, and to radio pulses from other astrophysical sources, such as prompt radio emission from gamma-ray burst sources and modulated signals from extraterrestrial civilizations. We estimate scintillation parameters for extragalactic sources that take into account scattering both in the host galaxy and in foreground Galactic plasma.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/63730565b4a2017a497c841cb9ef555725dc9e3e

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In Astronomy and Astrophysics

Citations in the corpus

The Brightest Pulses in the Universe: Multifrequency Observations of the Crab Pulsar’s Giant Pulses (2003, background): “Detection of giant pulses is discussed in general in Cordes & Mclaughlin (2003) and in particular from nearby galaxies in McLaughlin & Cordes (2003).”
The Repeating Fast Radio Burst FRB 121102 as Seen on Milliarcsecond Angular Scales (2017, methodology): “We have characterized the bursts using the detection statistic ξ = F/ √ w (fluence divided by the square-root of the burst width; e.g., Cordes & McLaughlin 2003; Trott et al. 2013).”
THE REPEATING FAST RADIO BURST FRB 121102: MULTI-WAVELENGTH OBSERVATIONS AND ADDITIONAL BURSTS (2016, methodology): “To convert this S/N to a flux density, we use the expression given by Cordes & McLaughlin (2003): Si = (S/N)bSsys Wi √ Wb npB , (5) where Si is the intrinsic flux density of the pulse, (S/N)b is the measured S/N of the broadened pulse, Ssys is the system-equivalent flux density, Wi and Wb are the…”
Science with ASKAP (2008, methodology): “A comprehensive review of fast radio transients and search techniques is given in Cordes and McLaughlin [64].”
Arecibo Pulsar Survey Using ALFA. I. Survey Strategy and First Discoveries (2005, methodology): “In parallel with the periodicity analysis, we also search for isolated pulses in the 96 dedispersed time series based on code developed by Cordes & McLaughlin (2003).”
FRBCAT: The Fast Radio Burst Catalogue (2016, methodology): “The observed peak flux density of the burst in Jy calculated using quantities above via the single pulse radiometre equation (Cordes & McLaughlin 2003).”
Probing the cosmic reionization history and local environment of gamma‐ray bursts through radio dispersion (2003, methodology): “The bright peak flux and fast decaying light curve should allow the dispersion signal to be readily distinguished, in the usual manner employed for pulsars (e.g. Cordes & McLaughlin 2003).”
Science with the Murchison Widefield Array (2012, background): “This delay is beneficial since it allows time to prepare for the event at low frequencies (e.g., Cordes & McLaughlin 2003; Macquart 2007).”
Fast radio bursts: search sensitivities and completeness (2014, unknown): “This process is repeated a number of times in order to search for a range of pulse widths (Cordes & McLaughlin 2003).”
Further searches for Rotating Radio Transients in the Parkes Multi-beam Pulsar Survey (2009, background): “As we detect pulses only occasionally from RRATs they are generally not detected in Fourier domain searches (although see discussion in section 3) but rather by searching for individual bright pulses (McLaughlin & Cordes 2003; Cordes & McLaughlin 2003).”