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

Ohsawa, Ryou; Sako, Shigeyuki; Sarugaku, Yuki; Usui, Fumihiko; Ootsubo, Takafumi; Fujiwara, Yasunori; Sato, Mikiya; Kasuga, Toshihiro; Arimatsu, Ko; Watanabe, Jun; Doi, Mamoru; Kobayashi, Naoto; Takahashi, H.; Motohara, Kentaro; Morokuma, Tomoki; Konishi, Masahiro; Aoki, Tsutomu; Soyano, Takao; Tarusawa, K.; Mori, Yuki; Nakada, Y.; Ichiki, Masaaki; Arima, Noriaki; Kojima, Yuto; Morita, Masahiro; Shigeyama, Toshikazu; Ita, Yoshifusa; Kokubo, Mitsuru; Mitsuda, K.; Maehara, Hiroyuki; Tominaga, Nozomu; Yamashita, Takuya; Ikeda, Shiro; Urakawa, Seitaro; Okumura, S.; Yoshikawa, Makoto

doi:10.1016/j.pss.2018.09.006

Cited by 6 publications

(9 citation statements)

References 35 publications

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“…22 Both these developments are being made possible by the availability of inexpensive but high performance CMOS (Complementary Metal-Oxide Semiconductor) detectors. Tomo-e-Gozen is a massivelymosaicked CMOS camera with a field-of-view of 20 deg 2 and is mounted on the Kiso 1.05-m Schmidt telescope (Sako et al 2018); see Ohsawa et al (2019) and Richmond et al (2020) for a taste of the future.…”

Section: An Exciting and Endless Frontiermentioning

confidence: 99%

Towards An Integrated Optical Transient Utility

Kulkarni¹

2020

Preprint

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The ongoing optical time-domain astronomy surveys are routinely reporting fifty transient candidates per night. Here, I investigate the demographics of astronomical transients and supernova classifications reported to the Transient Name Server in the year 2019. I find that only a tenth of the transients were spectrally classified. This severe "bottleneck" problem should concern astronomers and also funding agencies. The bottleneck will get worse by a factor of 20 (or more) once LSST comes on line. We need to fundamentally rethink the purpose of surveys for transients. Here, after undertaking a detailed investigation of this issue I offer some solutions. Going forward, astronomers will employ two different methodologies: (1) multi-band photometric method which is well suited to the study of very large, many tens of thousands, samples of faint transients; (2) spectral classifications of thousands of bright transients found in shallow and nightly cadenced wide-field photometry surveys and transients associated with galaxies in the local Universe. The latter program, in addition to unearthing new types of transients and offering astronomers opportunities to undertake extensive follow up of interesting transients, is needed to set the stage for the former. Specifically, I suggest a globally coordinated effort to spectrally classify a complete sample of bright supernovae ( 19.5 mag) and transients within the local Universe (< 200 Mpc). The proposed program is within reach -thanks to the on-going widefield surveys, the development of novel spectrographs tuned for classification, great improvements in throughput of spectrographs and the increasing availability of robotic telescopes.

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Section: An Exciting and Endless Frontiermentioning

confidence: 99%

Towards An Integrated Optical Transient Utility

Kulkarni¹

2020

Preprint

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“…The readout of the image sensor is synchronized with the GPS time and the time stamp of Tomo-e Gozen is as accurate as 0.2 ms (Sako et al, 2018). Observations are carried out in a clear filter and a nominal limiting magnitude for stars is about 18 mag, which is corresponding to about 12 mag for meteors (Ohsawa et al, 2019). At the time of the observations, only one quadrant of the camera was available and one sensor was not operating.…”

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

confidence: 99%

“…The cumulative number flux peaks out around −25 dBsm simply due to the detection limit. In a range from −20 to 20 dBsm, the cumulative number flux seems well approximated by Kresáková (1966) 3.5 2.35 −4-6 mag, 21996 visual meteors Hughes and Stephenson (1972) -2.04±0.04 30000 HF radar echoes Clifton (1973) ∼3.17 ∼2.252 7-11 mag, TV observation Hughes (1974) 3.73±0.07 2.43±0.02 −6-0 mag, 10287 visual meteors Hawkes and Jones (1975b) -2.02±0.04 3-7 mag, TV observation Štohl (1976) 3.70 -12867 visual meteors Cook et al (1980) 3.41 2.335 7-12 mag, phototubes Rendtel (2004) 2.95±0.06 2.17±0.03 301499 visual meteors, IMO VMDB Ohsawa et al (2019) 3.1±0.4 -3-9 mag, video-rate magnitude The present result 3.52±0.12 2.46±0.09 0-9 mag, MURMHED a linear function. The cumulative number flux against the RCS is converted into the luminosity function by applying Equation (1).…”

Section: Meteor Luminosity Function Of the Mu Radar Meteor Head Echo ...mentioning

confidence: 99%

“…A combination of a large aperture, high-speed and continuous imaging, and a large field-of-view is required to detect faint meteors optically. Recently, Ohsawa et al (2019) carried out observations of meteors as faint as ∼10 mag with a mosaic CMOS camera, Tomo-e PM, mounted on the 1.05-m Kiso Schmidt telescope. A combination of a large and wide-field telescope and a mosaic CMOS camera is preferable to detect faint meteors.…”

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confidence: 99%

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

Ohsawa,

Hirota,

Morita

et al. 2020

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“…The short duration of meteors and their high angular velocity leads to rapid motion and trailing losses across an image plane. As it is desirable to collect as many photons as possible, comparatively large optical apertures have previously been used for this purpose (Cook et al, 1980;Pawlowski et al, 2001;Kaiser et al, 2005;Iye et al, 2007;Ohsawa et al, 2019Ohsawa et al, , 2020.…”

Section: Introductionmentioning

confidence: 99%

Development of a Very Faint Meteor Detection System based on an EMCCD Sensor and Matched Filter Processing

Gural,

Mills,

Mazur

et al. 2021

Preprint

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The mass ranges of meteors, imaged by electro-optical (EO) cameras and backscatter radar receivers, for the most part do not overlap. Typical EO systems detect meteoroid masses down to 10 −5 kg or roughly magnitude +2 meteors when using moderate field of view optics, unintensified optical components, and meteor entry velocities around 45 km/sec. This is near the high end of the mass range of typical meteor radar observations. Having the same mass meteor measured by different sensor wavelength bands would be a benefit in terms of calibrating mass estimations for both EO and radar. To that end, the University of Western Ontario (UWO) has acquired and deployed a very low light imaging system based on an electron-multiplying CCD camera technology. This embeds a very low noise, per pixel intensifier chip in a cooled camera setup with various options for frame rate, region of interest and binning. The EO system of optics and sensor was optimally configured to collect 32 frames per second in a square field of view 14.7 degrees on a side, achieving a single-frame stellar limiting magnitude of m G = +10.5. The system typically observes meteors of +6.5. Given this hardware configuration, we successfully met the challenges associated with the

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

Cited by 6 publications

References 35 publications

Towards An Integrated Optical Transient Utility

Towards An Integrated Optical Transient Utility

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

Development of a Very Faint Meteor Detection System based on an EMCCD Sensor and Matched Filter Processing

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