Rotational properties of near-earth objects obtained by the IMPACTON project

Monteiro, F.; Silva, J.S.; Lazzaro, D.; Arcoverde, Plícida; Medeiros, Hissa; Rodrigues, Teresinha; Souza, Roberto

doi:10.1016/j.pss.2018.06.016

Cited by 7 publications

(5 citation statements)

References 12 publications

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“…Photometric observations of the asteroid were performed during its apparition in February 2006. Monteiro et al (2017) reported that 2001 FC7 has a rotational period of 4.230 hr. The rotational period, however, could not be determined in this study because there were insufficient data for rotational analysis.…”

Section: 2001 Fc7mentioning

confidence: 99%

Physical properties of near-Earth asteroids with a low delta-v: Survey of target candidates for the Hayabusa2 mission

Hasegawa

Kuroda

Kitazato

et al. 2018

Publications of the Astronomical Society of Japan

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Sample return from the near-Earth asteroid known as 25143 Itokawa was conducted as part of the Hayabusa mission, with a large number of scientific findings being derived from the returned samples. Following the Hayabusa mission, Hayabusa2 was planned, targeting sample return from a primitive asteroid. The primary target body of Hayabusa2 was asteroid 162173 Ryugu; however, it was also necessary to gather physical information for backup target selection. Therefore, we examined five asteroids spectroscopically, 43 asteroids spectrophotometrically, and 41 asteroids through periodic analysis. Hence, the physical properties of 74 near-Earth asteroids were obtained, which helped the Hayabusa2 backup target search and, also, furthered understanding of the physical properties of individual asteroids and their origins.

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Section: 2001 Fc7mentioning

confidence: 99%

Physical properties of near-Earth asteroids with a low delta-v: Survey of target candidates for the Hayabusa2 mission

Hasegawa

Kuroda

Kitazato

et al. 2018

Publications of the Astronomical Society of Japan

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“…As previously mentioned, the main goal of the IMPACTON project is the physical characterization of NEOs, and these objects correspond to nearly 60% of all the observations made in the period 2011-2018 (Figure 7, top). We have observed different percentages of the several sub-population of NEOs (Figure 7, bottom), from Atiras to Atens, Apollos and Amors (Monteiro et al 2017(Monteiro et al , 2018a(Monteiro et al , 2018bPerna et al 2017;Rondón et al 2019). We have also observed a large number of MBA, ∼25% (Figure 7, top), because these objects are assumed to be the source of NEOs (Silva & Lazzaro 2015;Marciniak et al 2019;Martino et al 2019).…”

Section: Some Results From the Oasi Neo Samplementioning

confidence: 72%

“…The observations of NEOs performed at the OASI allowed to derive reliable rotational period for a total of 68 objects, of the Aten, Apollo and Amor groups, with quality code greater than 2, according to the lightcurve database LCDB 9 (Warner et al 2009). For 23 of these objects this was the first period determination (Silva & Lazzaro 2015;Silva et al 2016;Monteiro et al 2017Monteiro et al , 2018aMonteiro et al , 2018b. Compared to the 302 periods available in the literature for these populations, our contribution corresponds to 22.5% of the total.…”

Section: Some Results From the Oasi Neo Samplementioning

confidence: 99%

“…The scientific aims of the observations performed at OASI include determination of rotation period, pole and shape through differential photometry, determination of solar phase curves and colors though flux-calibrated photometry, search for dust comae from measurements of radial profiles, and orbit determination/improvement from astrometric observations for selected targets (Monteiro et al 2017(Monteiro et al , 2018a(Monteiro et al , 2018bPerna et al 2017;Rondón et al 2019). More recently, the main focus of the observations has been to obtain a complete photometric characterization of the NEOs, observing the rotational light curve simultaneously to the phase curve and to the photometric spectrum, in order to get reliable physical parameters (Rondón et al 2019).…”

Section: Some Results From the Oasi Neo Samplementioning

confidence: 99%

“…Compared to the 302 periods available in the literature for these populations, our contribution corresponds to 22.5% of the total. Spin direction and shape were also determined for the first time for 9 of these objects (Silva & Lazzaro 2015;Silva et al 2016;Monteiro et al 2018b). Considering that presently 22 NEOs have these parameters included in the DAMIT database (Durech et al 2010), obtained using the same method of lightcurve inversion, the OASI contributed with 40.9% of all the known pole direction of NEOs.…”

Section: Some Results From the Oasi Neo Samplementioning

confidence: 99%

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OASI: A Brazilian Observatory Dedicated to the Study of Small Solar System Bodies—Some Results on NEO’s Physical Properties

Rondón

Lazzaro

Rodrigues

et al. 2020

PASP

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The distribution of professional observatories around the world is quite biased toward the Northern Hemisphere, and this tendency is even more pronounced when considering those dedicated only to the study of small solar system bodies. In the Southern Hemisphere, the IMPACTON project deployed the Observatório Astronômico do Sertão de Itaparica (OASI), dedicated to the observation of minor bodies of the solar system with emphasis on Near-Earth Objects (NEOs). The observatory is located at the county of Itacuruba, in the Pernambuco State of Brazil, and operate a 1 m Cassegrain telescope. Here, we present a complete characterization of the OASI instruments and the sky conditions during the first eight years of operations. The limiting magnitudes are determined in the different available filters. The median seeing results to be 1 22, with a higher number of photometric nights from April to October. We also give an overview of the results obtained from the OASI observations and discuss them in the light of similar data from the literature. In particular, the rotational periods of 23 NEOs, and the spin directions and shapes of 9 NEOs, have been determined for the very first time using our observations. Analyzing rotational periods, sizes and taxonomic classification from the literature and OASI, we conclude that the fast rotating NEOs are predominantly S-type objects. However, rotational periods obtained at the OASI and with similar value from LCDB database allowed to identify the first fast rotator C-type NEO: asteroid 436724. With an estimated tensile strength as low as 0.5 KPa, this asteroid allows us to suggest that it defines the border between the C-and S-type fast rotators in the size versus period diagram. Although this hypothesis is based on a very small sample it is compatible with all presently available data. Only new observations, however, can prove if this hypothesis is correct.

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The EURONEAR Lightcurve Survey of Near Earth Asteroids—Teide Observatory, Tenerife, 2015

Văduvescu

Cornea

Macias³

et al. 2021

Earth Moon Planets

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Rotational properties of near-earth objects obtained by the IMPACTON project

Cited by 7 publications

References 12 publications

Physical properties of near-Earth asteroids with a low delta-v: Survey of target candidates for the Hayabusa2 mission

Physical properties of near-Earth asteroids with a low delta-v: Survey of target candidates for the Hayabusa2 mission

OASI: A Brazilian Observatory Dedicated to the Study of Small Solar System Bodies—Some Results on NEO’s Physical Properties

The EURONEAR Lightcurve Survey of Near Earth Asteroids—Teide Observatory, Tenerife, 2015

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