The astrometric<i>Gaia</i>-FUN-SSO observation campaign of 99942 Apophis

Thuillot, W.; Bancelin, David; Ivantsov, Anatoliy; Desmars, J.; Assafin, M.; Eggl, Siegfried; Hestroffer, Daniel; Rocher, Patrick; Carry, B.; David, Pedro; Abe, Lyu; Андреев, М. В.; Arlot, J. E.; Asami, A.; Ayvasian, Vova; Baransky, Alexander; Belcheva, M.; Bendjoya, P.; Bikmaev, I.; Бурхонов, О.; Camcı, Uğur; Carbognani, A.; Colas, F.; Devyatkin, A. V.; Ehgamberdiev, S. A.; Enikova, P.; Eyer, L.; Galeev, A.; Gerlach, E.; Godunova, V.; Golubaev, A. V.; Gorshanov, D. L.; Gumerov, R.; Hashimoto, N.; Helvacı, M.; Ibryamov, S.; Inasaridze, R.; Khamitov, I.; Kostov, A.; Kozhukhov, A. M.; Kozyryev, Y.; Krugly, Yu. N.; Kryuchkovskiy, V. F.; Kulichenko, N.; Maigurova, N. V.; Manilla-Robles, A.; Martyusheva, A. A.; Молотов, И. Е.; Nikolov, Geno; Nikolov, Plamen; Nishiyama, K.; Okumura, S.; Palaversa, L.; Parmonov, O. U.; Peng, Q. Y.; Петрова, С.Н.; Pinigin, G. I.; Pomazan, A.; Rivet, Jean‐Pierre; Sakamoto, T.; Sakhibullin, N.; Sergeev, O. A.; Sergeyev, A.; Shulga, O. V.; Suárez, Olga; Sybiryakova, Y.; Takahashi, N.; Tarady, V. K.; Todd, Michael; Urakawa, Seitaro; Uysal, O.; Văduvescu, O.; Vovk, Vasyl; Zhang, X. L.

doi:10.1051/0004-6361/201425603

Cited by 13 publications

(7 citation statements)

References 24 publications

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“…Apophis has a diameter of around 400 m (Müller et al 2014;Licandro et al 2015) and will have a close fly-by in 2029 (Figure 13). While it had been thought there was potentially a high probability of impact during this fly-by, or one in 2036, this has now been significantly downgraded (Chesley et al 2010;Krolikowska & Sitarski 2010;Thuillot et al 2015). Nevertheless, passing around 31,000 km from the Earth's surface, Apophis will come within the orbits of geosynchronous satellites (see Figure 13).…”

Section: Availability Of Solar System Bodiesmentioning

confidence: 99%

Terminus: A Versatile Simulator for Space-based Telescopes

Edwards

Stotesbury²

2021

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Space-based telescopes offer unparalleled opportunities for characterizing exoplanets, solar system bodies, and stellar objects. However, observatories in low-Earth orbits (e.g., Hubble, CHaracterising ExOPlanets Satellite, Twinkle, and an ever-increasing number of cubesats) cannot always be continuously pointed at a target due to Earth obscuration. For exoplanet observations consisting of transit, or eclipse, spectroscopy, this causes gaps in the light curve, which reduces the information content and can diminish the science return of the observation. Terminus, a time-domain simulator, has been developed to model the occurrence of these gaps to predict the potential impact on future observations. The simulator is capable of radiometrically modeling exoplanet observations as well as producing light curves and spectra. Here, Terminus is baselined on the Twinkle mission, but the model can be adapted for any space-based telescope and is especially applicable to those in a low-Earth orbit. Terminus also has the capability to model observations of other targets such as asteroids or brown dwarfs.Unified Astronomy Thesaurus concepts: Exoplanet atmospheres (487); Space telescopes (1547); Asteroids (72); Astronomical instrumentation (799); Infrared telescopes (794)

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Section: Availability Of Solar System Bodiesmentioning

confidence: 99%

Terminus: A Versatile Simulator for Space-based Telescopes

Edwards

Stotesbury²

2021

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“…Apophis is usually fainter than 20 mag (apparent magnitude) while it can be detected using the stacking method or observing with a large-diameter telescope (Guo et al 2022). Nevertheless, Wang et al (2015) and Thuillot et al (2015) obtained precise astrometric positions when it is much brighter (<17 mag), in the year 2013.…”

Section: Observations Of Apophismentioning

confidence: 99%

Precise Distance Measurement for a Near-Earth Asteroid by the Refined Rotational Reflex Velocity Method

Guo

Peng

Lin

et al. 2023

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The rotational reflex velocity (RRV) method was proposed by Heinze and Metchev in 2015 and was used to measure the distances of main-belt asteroids (MBAs). Later, Lin et al. generalized this method using spherical astronomy in 2016. The method measures the distances of MBAs using the observations from a single ground-based telescope over two nights. We refined this method and extend it further to the distance measurement of near-Earth asteroids (NEAs). In practice, we measure the distance of the potentially hazardous asteroid (99942) Apophis from the acquired CCD frames using the newly refined method. According to the requirement of the newly refined method, we also simulate the distance measurements of the four typical NEAs, (1221) Amor, (1862) Apollo, (2062) Aten, and (163693) Atira, on their discovery dates and follow-up dates. The measurement results of Apophis based on the newly refined RRV method show that the mean relative errors for the independent exposure frames on the successive two nights is ∼0.08% (about a factor of 2 improvement in comparison with the research of Lin et al.) compared with the distance from JPL ephemeris. Our simulation results also show that this refined method can accurately and precisely measure the distances of newly discovered NEAs in an astrometric way without performing orbital determination. The accurate and precise distances of newly discovered asteroids help us to conveniently evaluate their impact risks within a shorter time, leaving us more time to take defense precautions.

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“…PRAIA was conceived to determine photometry and accurate positions from large numbers of CCD images as unsupervised as possible. Its use and performance have been reported by various works (see, for instance, Assafin et al 2013;Thuillot et al 2015;Gomes-Júnior et al 2016) from reference frame to solar system studies. The reference catalog used here for astrometry is the Gaia Data Release 2 (Lindegren et al 2018).…”

Section: Astrometrymentioning

confidence: 99%

Astrometry and Occultation Predictions to Trans-Neptunian and Centaur Objects Observed within the Dark Energy Survey

Banda-Huarca¹,

Camargo²,

Desmars³

et al. 2019

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Trans-Neptunian objects (TNOs) are a source of invaluable information to access the history and evolution of the outer solar system. However, observing these faint objects is a difficult task. As a consequence, important properties such as size and albedo are known for only a small fraction of them. Now, with the results from deep sky surveys and the Gaia space mission, a new exciting era is within reach as accurate predictions of stellar occultations by numerous distant small solar system bodies become available. From them, diameters with kilometer accuracies can be determined. Albedos, in turn, can be obtained from diameters and absolute magnitudes. We use observations from the Dark Energy Survey (DES) from 2012 November until 2016 February, amounting to 4,292,847 charge-coupled device (CCD) frames. We searched them for all known small solar system bodies and recovered a total of 202 TNOs and Centaurs, 63 of which have been discovered by the DES collaboration as of the date of submission. Their positions were determined using the Gaia Data Release 2 as

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The astrometricGaia-FUN-SSO observation campaign of 99942 Apophis

Cited by 13 publications

References 24 publications

Terminus: A Versatile Simulator for Space-based Telescopes

Terminus: A Versatile Simulator for Space-based Telescopes

Precise Distance Measurement for a Near-Earth Asteroid by the Refined Rotational Reflex Velocity Method

Astrometry and Occultation Predictions to Trans-Neptunian and Centaur Objects Observed within the Dark Energy Survey

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