Ultraviolet to near-infrared spectroscopy of the potentially hazardous, low delta-V asteroid (175706) 1996 FG3

Perna, D.; Dotto, E.; Barucci, Maria Antonietta; Fornasier, S.; Álvarez-Candal, A.; Gourgeot, F.; Brucato, J. R.; Rossi, Alessandro

doi:10.1051/0004-6361/201321677

Cited by 11 publications

(11 citation statements)

References 33 publications

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“…A coarse-grained surface for 2001 SN263 could possibly explain the above mismatch and would also support the hypothesis by Delbo et al (2011): these authors suggested a regolithdepletion mechanism during binary asteroid formation and noted that a unique system (i.e., very spaced triple components) such as 2001 SN263 could potentially be dramatically affected by this effect. Noteworthy, surface variations possibly related with binary nature have already been suggested for the NEA (175706) 1996 FG3 (Perna et al 2013a;de León et al 2013).…”

Section: Spectramentioning

confidence: 75%

The triple near-Earth asteroid (153591) 2001 SN263: an ultra-blue, primitive target for the Aster space mission

Perna

Álvarez-Candal

Fornasier

et al. 2014

A&A

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Context. The Brazilian Aster project plans a space mission to rendezvous and characterize (153591) 2001 SN263, one of the only two known triple near-Earth asteroids (NEAs). Improving the knowledge of its physical properties is necessary to optimize the mission planning and science return. Aims. We study the surface composition and physical nature of 2001 SN263 by analyzing and comparing its reflectance spectra with laboratory spectra of minerals and meteorites. Methods. We performed spectroscopic observations of 2001 SN263 using the UV-to-NIR X-Shooter spectrograph at the ESO Very Large Telescope (VLT). Complementary photometric observations of the target were acquired with the FORS2 instrument. Results. We find B-type, featureless convex spectra (Themis-or Polana-like). 2001 SN263 presents the bluest visible spectrum ever observed for small bodies in the solar system, even bluer than NEAs Phaethon and Bennu. The spectra suggest that the surface composition is organic-and magnetite-rich, similar to that of heated CI carbonaceous chondrites. Phyllosilicates may be abundant as well. We find hints of a coarse-grained surface and composition variety within the triple system. Conclusions. Both the large grain size and surface variability might be connected to the formation of the triple system. The Aster mission will have the intriguing possibility of checking current models of asteroid binary formation.

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Section: Spectramentioning

confidence: 75%

The triple near-Earth asteroid (153591) 2001 SN263: an ultra-blue, primitive target for the Aster space mission

Perna

Álvarez-Candal

Fornasier

et al. 2014

A&A

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“…Consequently, rather than analyzing each taxon separately, in the following we define four major groupings to increase the significance of our analysis (also in terms of impact risk mitigation purposes): the "silicaceous" asteroids (184 PHAs in total), including the whole S-complex together with objects classified as Q-, A-, or O-type; the "basaltic" V-type asteroids (12 PHAs); the "carbonaceous" asteroids (40 PHAs in total), consisting of PHAs belonging to the B, C, D, P, T, and Xc classes (we stress that the only Xc-type in our sample is (175706) 1996 FG3), which clearly is of primitive nature (see Perna et al 2013b and references therein); the remaining "miscellaneous" asteroids (25 PHAs in total), i.e., those classified in the X, Xe, Xk, K, and L taxa. As stated above, such a grouping will include objects of either silicaceous, carbonaceous, enstatitic, or metallic nature (see Fornasier et al 2011 for a review on X-type asteroids).…”

Section: The Pha Population: a Statistical Analysismentioning

confidence: 88%

Grasping the Nature of Potentially Hazardous Asteroids

Perna

Dotto

Ieva

et al. 2015

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Through their delivery of water and organics, near-Earth objects (NEOs) played an important role in the emergence of life on our planet. However, they also pose a hazard to the Earth, as asteroid impacts could significantly affect our civilization. Potentially hazardous asteroids (PHAs) are those that, in principle, could possibly impact the Earth within the next century, producing major damage. About 1600 PHAs are currently known, from an estimated population of 4700±1450. However, a comprehensive characterization of the PHA physical properties is still missing. Here we present spectroscopic observations of 14 PHAs, which we have used to derive their taxonomy, meteorite analogs, and mineralogy. Combining our results with the literature, we investigated how PHAs are distributed as a function of their dynamical and physical properties. In general, the "carbonaceous" PHAs seem to be particularly threatening, because of their high porosity (limiting the effectiveness of the main deflection techniques that could be used in space) and low inclination and minimum orbit intersection distance (MOID) with the Earth (favoring more frequent close approaches). V-type PHAs also present low MOID values, which can produce frequent close approaches (as confirmed by the recent discovery of a limited space weathering on their surfaces). We also identified those specific objects that deserve particular attention because of their extreme rotational properties, internal strength, or possible cometary nature. For PHAs and NEOs in general, we identified a possible anti-correlation between the elongation and the rotational period, in the range of P rot ≈5-80 hr. This would be compatible with the behavior of gravity-dominated aggregates in rotational equilibrium. For periods 80-90 hr, such a trend stops, possibly under the influence of the YORP effect and collisions. However, the statistics is very low, and further observational and theoretical work is required to characterize such slow rotators.

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“…We found 17 C-complex and five D-type objects, all bodies pertaining to taxonomic classes linked with a primitive composition and known to be extremely rare among the low ∆V population (Kuroda et al 2014). Incidentally, two of them have already been chosen as a sample-return candidate: (101955) Bennu, target of the OSIRIS-REx mission (Lauretta et al 2017), and (175706) 1996 FG3, backup target of the ESA candidate mission MarcoPolo-R (Perna et al 2013b). In addition, we also considered three A-type PHAs in this subgroup: a type of olivine-dominated asteroid extremely rare in both the NEO population and the asteroid belt (see also Popescu et al 2018).…”

Section: Selection Of Potential Targets Of Space Missionsmentioning

confidence: 98%

Extended photometric survey of near-Earth objects

Ieva

Dotto

Epifani

et al. 2020

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Context. The near-Earth objects (NEOs), whose proximity makes them the most accessible bodies in the Solar System, allow us to sample asteroids from tens of kilometers down to objects of a few meters in size. However, while the physical properties for the largest bodies are mostly known, we have very little physical information regarding the small NEOs. These objects today represent the overall majority among the ~2500 new discoveries each year, but they are usually only bright enough to be observable during their close approaches. Aims. Our aim was to extend our survey that started in 2015 on the NEO population, using ground-based observations to characterize the fainter (and typically smaller) NEOs observable each night. Methods. We performed BVRIz photometry of NEOs, making use of the DOLORES instrument at the Telescopio Nazionale Galileo (TNG, La Palma, Spain) and the Asiago Schmidt telescope (Italy), in order to derive visible color indexes and the taxonomic classification for each target in our sample. Results. We taxonomically classified 51 new NEOs for the first time. Together with data obtained in our previous work and collected by other surveys available online, we analyzed an extended sample of 1081 individual NEOs. While the overall majority of them belong to the S-complex, our analysis of the taxonomic distribution found a larger contribution for dark bodies going toward larger H, suggesting that they could be more abundant among the fainter NEOs. Moreover, we find an interesting correlation between semi-major axis and diameter, which could be in part related to the Yarkovsky effect. Rapid characterization of the fainter NEO population shortly after their discovery will be crucial in the future, before those bodies become too faint to be observed, or lost forever.

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Ultraviolet to near-infrared spectroscopy of the potentially hazardous, low delta-V asteroid (175706) 1996 FG3

Cited by 11 publications

References 33 publications

The triple near-Earth asteroid (153591) 2001 SN263: an ultra-blue, primitive target for the Aster space mission

The triple near-Earth asteroid (153591) 2001 SN263: an ultra-blue, primitive target for the Aster space mission

Grasping the Nature of Potentially Hazardous Asteroids

Extended photometric survey of near-Earth objects

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