Development of a real-time data processing system for a prototype of the Tomo-e Gozen wide field CMOS camera

Ohsawa, Ryou; Sako, Shigeyuki; Takahashi, H.; Kikuchi, Yasuko; Doi, Mamoru; Kobayashi, Naoto; Aoki, Tsutomu; Arimatsu, Ko; Ichiki, Masaaki; Ikeda, Shiro; Ita, Yoshifusa; Kasuga, Toshihiro; Kawakita, Hideo; Kokubo, Mitsuru; Maehara, Hiroyuki; Matsunaga, Noriyuki; Mito, Hiroyuki; Mitsuda, K.; Miyata, Takashi; Mori, Kiyoshi; Mori, Yuki; Morokuma, Tomoki; Motohara, Kentaro; Nakada, Y.; Okumura, S.; Onozato, Hiroki; Osawa, Kazutoshi; Sarugaku, Yuki; Sato, Mikiya; Shigeyama, Toshikazu; Soyano, Takao; Tanaka, Masaomi; Taniguchi, Yuki; Tanikawa, Ataru; Tarusawa, K.; Tominaga, Nozomu; Totani, Tomonori; Urakawa, Seitaro; Usui, Fumihiko; Watanabe, J.; Yamaguchi, Jumpei; Yoshikawa, Makoto

doi:10.1117/12.2231615

Cited by 5 publications

(3 citation statements)

References 3 publications

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“…Streak-like signals were extracted from the movie data cube with the slant-and-compress algorithm developed by Ohsawa et al [34]. First, background emission was subtracted and stellar signals were masked.…”

Section: Data Reductionmentioning

confidence: 99%

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Luminosity function of faint sporadic meteors measured with a wide-field CMOS mosaic camera Tomo-e PM

Ohsawa

Sako

Sarugaku

et al. 2019

Planetary and Space Science

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Section: Data Reductionmentioning

confidence: 99%

“…The signal-to-noise ratio of faint meteors in the original image was enhanced by about √ n, where n was the number of pixels along the streak, by integrating signals along with the streak. Refer to Ohsawa et al [34] for details of the detection algorithm. A number of meteor candidates were detected by the algorithm.…”

Section: Data Reductionmentioning

confidence: 99%

Luminosity function of faint sporadic meteors measured with a wide-field CMOS mosaic camera Tomo-e PM

Ohsawa

Sako

Sarugaku

et al. 2019

Planetary and Space Science

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“…The optical data were reduced in a standard astronomical data reduction procedure for imaging observations: a dark frame was subtracted and a flat frame correction was applied. Meteors in the optical video data were extracted with an algorithm based on the Hough transformation (Ohsawa et al, 2016(Ohsawa et al, , 2019. The detected events are summarized in Figure 1.…”

Section: Observations With the Mu Radar And Tomo-e Gozenmentioning

confidence: 99%

Relationship between Radar Cross Section and Optical Magnitude based on Radar and Optical Simultaneous Observations of Faint Meteors

Ohsawa,

Hirota,

Morita

et al. 2020

Preprint

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Linear feature detection algorithm for astronomical surveys – II. Defocusing effects on meteor tracks

Bektesevic¹,

Vinković²,

Rasmussen

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Given the current limited knowledge of meteor plasma micro-physics and its interaction with the surrounding atmosphere and ionosphere, meteors are a highly interesting observational target for high-resolution wide-field astronomical surveys. Such surveys are capable of resolving the physical size of meteor plasma heads, but they produce large volumes of images that need to be automatically inspected for possible existence of long linear features produced by meteors. Here we show how big aperture sky survey telescopes detect meteors as defocused tracks with a central brightness depression. We derive an analytic expression for a defocused point source meteor track and use it to calculate brightness profiles of meteors modeled as uniform brightness disks. We apply our modeling to meteor images as seen by the SDSS and LSST telescopes. The expression is validated by Monte Carlo ray-tracing simulations of photons traveling through the atmosphere and the LSST telescope optics. We show that estimates of the meteor distance and size can be extracted from the measured FWHM and the strength of the central dip in the observed brightness profile. However, this extraction becomes difficult when the defocused meteor track is distorted by the atmospheric seeing or contaminated by a long lasting glowing meteor trail. The FWHM of satellites tracks is distinctly narrower than meteor values, which enables removal of a possible confusion between satellites and meteors.

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Development of a real-time data processing system for a prototype of the Tomo-e Gozen wide field CMOS camera

Cited by 5 publications

References 3 publications

Luminosity function of faint sporadic meteors measured with a wide-field CMOS mosaic camera Tomo-e PM

Luminosity function of faint sporadic meteors measured with a wide-field CMOS mosaic camera Tomo-e PM

Relationship between Radar Cross Section and Optical Magnitude based on Radar and Optical Simultaneous Observations of Faint Meteors

Linear feature detection algorithm for astronomical surveys – II. Defocusing effects on meteor tracks

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