MAGIC sensitivity to millisecond-duration optical pulses

Hassan, Tarek; Hoang, J.; Moya, Marcos López; Barrio, J. A.; Cortina, J.; Fidalgo, D.; Fink, David J.; Tejedor, Luis; Will, Martin

doi:10.22323/1.301.0807

Cited by 4 publications

(6 citation statements)

References 14 publications

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“…These background contributors significantly reduce the confidence of a potential FRB detection, unless it is quasi-simultaneous with the radio event. MAGIC used this capability to investigate the U-band light collected by its modified unit II camera central pixel [210], which covers a 0 .…”

Section: Optical Observationsmentioning

confidence: 99%

Multiwavelength Observations of Fast Radio Bursts

Guidorzi

Palazzi²,

Zampieri

et al. 2021

Universe

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The origin and phenomenology of the Fast Radio Burst (FRB) remains unknown despite more than a decade of efforts. Though several models have been proposed to explain the observed data, none is able to explain alone the variety of events so far recorded. The leading models consider magnetars as potential FRB sources. The recent detection of FRBs from the galactic magnetar SGR J1935+2154 seems to support them. Still, emission duration and energetic budget challenge all these models. Like for other classes of objects initially detected in a single band, it appeared clear that any solution to the FRB enigma could only come from a coordinated observational and theoretical effort in an as wide as possible energy band. In particular, the detection and localisation of optical/NIR or/and high-energy counterparts seemed an unavoidable starting point that could shed light on the FRB physics. Multiwavelength (MWL) search campaigns were conducted for several FRBs, in particular for repeaters. Here we summarize the observational and theoretical results and the perspectives in view of the several new sources accurately localised that will likely be identified by various radio facilities worldwide. We conclude that more dedicated MWL campaigns sensitive to the millisecond–minute timescale transients are needed to address the various aspects involved in the identification of FRB counterparts. Dedicated instrumentation could be one of the key points in this respect. In the optical/NIR band, fast photometry looks to be the only viable strategy. Additionally, small/medium size radiotelescopes co-pointing higher energies telescopes look a very interesting and cheap complementary observational strategy.

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Section: Optical Observationsmentioning

confidence: 99%

Multiwavelength Observations of Fast Radio Bursts

Guidorzi

Palazzi²,

Zampieri

et al. 2021

Universe

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“…Additionally, the Central Pixel of the MAGIC-II telescope was modified to allow simultaneous observations in both VHE and optical. This instrument is able to detect isolated 1-ms optical flashes as faint as ∼ 13.4 mag in the blue wavelength [11]. VERITAS consists of four 12-m diameter telescopes with a 3.5 • FoV in Southern Arizona, USA (32 • N, 111 • W, 1270 m above the sea level), and is sensitive to 1% of the Crab Nebula flux within 25 hours [12].…”

Section: Vhe Instruments and Observationsmentioning

confidence: 99%

“…MAGIC installed an alternative readout system in the central PMT of the MAGIC II camera, the Central Pixel, to perform simultaneous optical observations [11]. With this upgrade, MAGIC can observe short (1 ms-1 s) optical pulses.…”

Section: Opticalmentioning

confidence: 99%

“…With this upgrade, MAGIC can observe short (1 ms-1 s) optical pulses. We searched for non-periodic optical pulses from MAXI J1820+070 that are brighter than 13 mag and last for less than 100 ms. To convert the Central Pixel output voltage to the corresponding optical absolute magnitude, we used the empirical expression mentioned in [11]. In order to improve sensitivity, an averaging filter of integration length of 1 ms was applied to de-noise the signal from the central pixel data (taken at the standard sampling rate of 10 kHz).…”

Section: Opticalmentioning

confidence: 99%

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Multiwavelength observation of MAXI J1820+070 with MAGIC, VERITAS and H.E.S.S.

Hoang¹,

Molina²,

López³

et al. 2019

Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019)

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is a new low-mass microquasar hosting a black hole recently discovered in X-rays by the MAXI instrument. It is the counterpart of ASASSN-18ey, discovered in optical a few days before by ASAS-SN. This source underwent a major outburst in 2018, during which it completed the typical "q-shaped" path in the hardness-intensity diagram. MAGIC, VERITAS and H.E.S.S. gamma-ray telescopes observed the sky position of MAXI J1820+070 for a total of more than 90 hours in 2018. In addition, some observations were carried out using MAGIC Central Pixel-a dedicated central pixel capable of detecting fast optical signals (10 kHz sampling rate, peak sensitivity in the U-band). This contribution presents the methods used to search for transient optical and very high energy gamma-ray emission from MAXI J1820+070, as well as the latest results in these energy ranges.

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“…With this upgrade, MAGIC can observe short (1 ms-1 s) optical pulses. We searched for non-periodic optical pulses from MAXI J1820+070 that are brighter than 13 mag and last for less than 100 ms. To convert the Central Pixel output voltage to the corresponding optical absolute magnitude, we used the empirical expression in [11]. In order to improve sensitivity, an averaging filter of integration length of 1 ms was applied to de-noise the signal from the Central Pixel data (taken at the standard sampling rate of 10 kHz).…”

Section: Opticalmentioning

confidence: 99%

Multi-wavelength observation of MAXI J1820+070 with MAGIC, VERITAS and H.E.S.S

Hoang,

Molina,

López

et al. 2019

Preprint

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MAXI J1820+070 is a new low-mass microquasar hosting a black hole recently discovered in X-rays by the MAXI instrument. It is the counterpart of ASASSN-18ey, discovered in optical a few days before by ASAS-SN. This source underwent a major outburst in 2018, during which it completed the typical "q-shaped" path in the hardness-intensity diagram. MAGIC, VERITAS and H.E.S.S. gamma-ray telescopes observed the sky position of MAXI J1820+070 for a total of more than 90 hours in 2018. In addition, some observations were carried out using MAGIC Central Pixel -a dedicated central pixel capable of detecting fast optical signals (10 kHz sampling rate, peak sensitivity in the U-band). This contribution presents the methods used to search for transient optical and very high energy gamma-ray emission from MAXI J1820+070, as well as the latest results in these energy ranges.

show abstract

MAGIC sensitivity to millisecond-duration optical pulses

Cited by 4 publications

References 14 publications

Multiwavelength Observations of Fast Radio Bursts

Multiwavelength Observations of Fast Radio Bursts

Multiwavelength observation of MAXI J1820+070 with MAGIC, VERITAS and H.E.S.S.

Multi-wavelength observation of MAXI J1820+070 with MAGIC, VERITAS and H.E.S.S

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