Characterization and Analysis of Near-Earth Objects via Lunar Impact Observations

Rembold, J. Jedediah; Ryan, E. V.

doi:10.1016/j.pss.2015.05.014

Cited by 8 publications

(12 citation statements)

References 19 publications

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“…Taking into account the total number of impacts (31), the total exposure time during which these events were collected (54 hours of Moon observations), as well as the average surface observed per night, we estimate a detection rate of 1.96×10 −7 events km −2 h −1 . This is about a factor of two higher than what has been reported before [1.03×10 −7 events km −2 h −1 (Suggs et al 2014) and 1.09×10 −7 events km −2 h −1 (Rembold & Ryan 2015)]. This is a direct result of the use of a larger aperture telescope (compared to previous campaigns) allowing for the detection of fainter events (see Fig.…”

Section: The Neliota Observationsmentioning

confidence: 58%

“…Several groups have therefore undertaken lunar monitoring surveys for NEO flashes (e.g. Madiedo et al 2014;Ortiz et al 2015;Rembold & Ryan 2015;Ait Moulay Larbi et al 2015). Ground-based surveys routinely use two or more telescopes often located at different sites in order to distinguish noise, seeing variations, cosmic rays and satellite glints from real impact events.…”

Section: Introductionmentioning

confidence: 99%

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NELIOTA: The wide-field, high-cadence, lunar monitoring system at the prime focus of the Kryoneri telescope

Xilouris

Bonanos

Bellas‐Velidis

et al. 2018

A&A

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We present the technical specifications and first results of the ESA-funded, lunar monitoring project "NELIOTA" (NEO Lunar Impacts and Optical TrAnsients) at the National Observatory of Athens, which aims to determine the size-frequency distribution of small Near-Earth Objects (NEOs) via detection of impact flashes on the surface of the Moon. For the purposes of this project a twin camera instrument was specially designed and installed at the 1.2 m Kryoneri telescope utilizing the fast-frame capabilities of scientific Complementary Metal-Oxide Semiconductor detectors (sCMOS). The system provides a wide field-of-view (17.0 ×14.4 ) and simultaneous observations in two photometric bands (R and I), reaching limiting magnitudes of 18.7 mag in 10 sec in both bands at a 2.5 signal-to-noise level. This makes it a unique instrument that can be used for the detection of NEO impacts on the Moon, as well as for any astronomy projects that demand high-cadence multicolor observations. The wide field-of-view ensures that a large portion of the Moon is observed, while the simultaneous, high-cadence, monitoring in two photometric bands makes possible, for the first time, the determination of the temperatures of the impacts on the Moon's surface and the validation of the impact flashes from a single site. Considering the varying background level on the Moon's surface we demonstrate that the NELIOTA system can detect NEO impact flashes at a 2.5 signal-to-noise level of ∼ 12.4 mag in the I-band and R-band for observations made at low lunar phases (∼ 0.1). We report 31 NEO impact flashes detected during the first year of the NELIOTA campaign. The faintest flash was at 11.24 mag in the R-band (about two magnitudes fainter than ever observed before) at lunar phase 0.32. Our observations suggest a detection rate of 1.96×10 −7 events km −2 h −1 .

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Section: The Neliota Observationsmentioning

confidence: 58%

Section: Introductionmentioning

confidence: 99%

NELIOTA: The wide-field, high-cadence, lunar monitoring system at the prime focus of the Kryoneri telescope

Xilouris

Bonanos

Bellas‐Velidis

et al. 2018

A&A

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“…A detection rate of 2.3 × 10 −7 meteoroids hr −1 km −2 based on the validated flash detections (from sporadic and stream meteoroids), which can be extended to 3.14 × 10 −7 meteoroids hr −1 km −2 if we take into account the suspected flashes too, has been derived for the NELIOTA campaign so far. If we compare this rate with the respective ones of Suggs et al (2014) (1.03×10 −7 meteoroids hr −1 km −2 ) and Rembold & Ryan (2015) (1.09 × 10 −7 meteoroids hr −1 km −2 ), it can be clearly seen that NELIOTA has over doubled the detection rate of lunar impact flashes, and obviously this reflects the use of a telescope with large diameter. Using the detection rate of NELIOTA campaign and assuming an isotropic distribution of the meteoroids in space, the frequency distributions of meteoroids near Earth and Moon were calculated.…”

Section: Summary and Discussionmentioning

confidence: 92%

“…18 see also e.g. Suggs et al 2014;Rembold & Ryan 2015;Madiedo et al 2015a,b). Therefore, using the magnitudes of a flash and assuming that its observed energy flux can be approximated by the method of Bessell et al (1998a,b), and that ∆λ R = 0.158 µm ∆λ I = 0.154 µm for R and I bands, respectively, we can calculate the luminosity and the energy for each band.…”

Section: Luminous Energy Calculation Based On the Emitted Energies Frmentioning

confidence: 93%

“…So far, there have been several regular campaigns on lunar impact flashes (Ortiz et al 2006;Bouley et al 2012;Suggs et al 2014;Madiedo et al 2014Madiedo et al , 2015bOrtiz et al 2015;Rembold & Ryan 2015;Ait Moulay Larbi et al 2015a,b). Moreover, after 2014, many lunar flashes, produced mostly during meteoroid streams, have been also reported (Madiedo et al 2017(Madiedo et al , 2019a.…”

Section: Introductionmentioning

confidence: 99%

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NELIOTA: Methods, statistics, and results for meteoroids impacting the Moon

Liakos

Bonanos

Xilouris

et al. 2020

A&A

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Context. This paper contains the results from the first 30 months of the NELIOTA project for impacts of Near-Earth Objects/meteoroids on the lunar surface. Our analysis on the statistics concerning the efficiency of the campaign and the parameters of the projectiles and the impacts is presented. Aims. The parameters of the lunar impact flashes based on simultaneous observations in two wavelength bands are used to estimate the distributions of the masses, sizes and frequency of the impactors. These statistics can be used both in space engineering and science. Methods. The photometric fluxes of the flashes are measured using aperture photometry and their apparent magnitudes are calculated using standard stars. Assuming that the flashes follow a black body law of irradiation, the temperatures can be derived analytically, while the parameters of the projectiles are estimated using fair assumptions on their velocity and luminous efficiency of the impacts. Results. 79 lunar impact flashes have been observed with the 1.2 m Kryoneri telescope in Greece. The masses of the meteoroids range between 0.7 g and 8 kg and their respective sizes between 1-20 cm depending on their assumed density, impact velocity, and luminous efficiency. We find a strong correlation between the observed magnitudes of the flashes and the masses of the meteoroids. Moreover, an empirical relation between the emitted energies of each band has been derived allowing the estimation of the physical parameters of the meteoroids that produce low energy impact flashes. Conclusions. The NELIOTA project has so far the highest detection rate and the faintest limiting magnitude for lunar impacts compared to other ongoing programs. Based on the impact frequency distribution on Moon, we estimate that sporadic meteoroids with typical masses less than 100 g and sizes less than 5 cm enter the mesosphere of the Earth with a rate ∼ 108 meteoroids hr −1 and also impact Moon with a rate of ∼ 8 meteoroids hr −1 .

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