Enhanced Optical Emission During Crab Giant Radio Pulses

Shearer, A.; Stappers, B. W.; O’Connor, P.; Golden, Aaron; Strom, R. G.; Redfern, M.; Ryan, Oliver

doi:10.1126/science.1084919

Cited by 118 publications

(130 citation statements)

References 16 publications

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“…The phase of the main-and interpulses has counter parts at γ-ray wavelengths. Shearer et al (2003) report enhanced emission at optical wavelengths coincident with the radio giant pulses. However, this is not seen at γ-ray wavelengths at either 800 MHz (Lundgren et al 1995) or at 8.9 GHz (Bilous et al 2011).…”

Section: Discussionmentioning

confidence: 99%

Crab giant pulses at low frequencies

Karuppusamy

Stappers

Lee

2012

A&A

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We report observations of the Crab pulsar at frequencies in the range of 110-180 MHz. The combination of coherent dedispersion and the narrow synthesised beam of the Westerbork Synthesis Radio Telescope resulted in a sensitive observation. Our improved sensitivity and resolution allow us to confirm the presence of a precursor to the interpulse at these frequencies. We also detected more than 1000 giant pulses and find that the interpulse precursor component shows no giant pulse emission. Therefore, we attribute it to a similar emission source as the precursor to the mainpulse. Together these precursors might be the normal emission seen from the majority of radio pulsars. From the dispersion-free giant pulses, we find that the emission rate is ∼10-20 × 10 −3 s −1 and the scatter timescale in the range of ∼1.5-5.6 ms. We further find that the radio flux of the pulsar is 6-11 Jy in this frequency range.

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Section: Discussionmentioning

confidence: 99%

Crab giant pulses at low frequencies

Karuppusamy

Stappers

Lee

2012

A&A

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“…As bursts are not expected to be more frequent in some directions than others, SGARFACE data are taken toward whichever target the Whipple 10m telescope is tracking and data is taken in the galactic plane as much as away from the galactic plane. Data taken in the direction of the Crab Nebula will be used in a dedicated analysis to search for counterparts to pulsar giant radio pulses (19).…”

Section: Discussionmentioning

confidence: 99%

SGARFACE: a novel detector for microsecond gamma ray bursts

LeBohec

Krennrich

Sleege

2005

Astroparticle Physics

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The Short GAmma Ray Front Air Cherenkov Experiment (SGARFACE) is operated at the Whipple Observatory utilizing the Whipple 10 m γ-ray telescope. SGARFACE is sensitive to γ-ray bursts of more than 100 MeV with durations from 100 ns to 35 µs and provides a fluence sensitivity as low as 0.8 γ rays per m 2 above 200 MeV (0.05 γ rays per m 2 above 2 GeV) and allows to record the burst time structure.

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“…Giant radio pulses (GRPs) are normally coincident with main pulse and inter-pulse [11] but can apparently also occur in other phase regions [23]. While an analogous phenomenon has not so far been seen in the optical, an average 3% enhancement in flux of the optical pulse, in coincidence with GRPs, has been reported [11].…”

Section: Search For Giant Pulsesmentioning

confidence: 99%

“…The optical emission also provides a bridge between the well studied radio and X-ray bands. The recent claim of enhanced optical emission associated with giant radio pulses (GRPs) of the Crab pulsar [11], acts as an additional motivation for further studies.…”

Section: Introductionmentioning

confidence: 99%