Abstract:Context. Less than one percent of the discovered small Solar System objects have highly inclined orbits (i > 60°), and revolve around the Sun on near-polar or retrograde orbits. The origin and evolutionary history of these objects are not yet clear.
Aims. In this work we study the surface properties and orbital dynamics of selected high-inclination objects.
Methods. BVRI photometric observations were performed in 2019–2020 using the 2.0 m telescope at the Terskol Observatory and the 2.6 m telescope at the C… Show more
“…Both observing runs were conducted under clear (sky 90% cloudless at elevation >30°, transmission variation <10%) or photometric (sky cloudless, transmission variation <2%) conditions as defined by ESO; as a result, we expect the continuum colors of our spectra to be minimally affected by clouds, and therefore accurate. As in previously reported observational epochs (Kiss et al 2013;Szabó et al 2018;Hromakina et al 2021), 2012 DR 30 was found to be inactive both times we observed it.…”
Section: Observationssupporting
confidence: 90%
“…In Figure 2 we present our optical reflectance spectra of 2012 DR 30 in comparison to all published optical photometric and spectroscopic reflectance data where such data cover 0.6 μm, enabling consistent scaling between data sets (literature data sets include those reported by Kiss et al 2013;Szabó et al 2018;Hromakina et al 2021). Optical photometric colors were converted to coarse reflectance spectra using methods described by Hainaut & Delsanti (2002) and were scaled relative to the reflectance value at 0.6 μm on a line drawn between the two data points on either side of that wavelength.…”
Section: Discussionmentioning
confidence: 86%
“…As a collection, the optical colors reported for 2012 DR 30 so far suggest that its color varies significantly between observational epochs (Kiss et al 2013;Szabó et al 2018;Hromakina et al 2021).…”
Section: Introductionmentioning
confidence: 99%
“…To date, multiband photometry has been the main technique used for characterization of the surfaces of HiHq Centaurs, and half of those currently known have published optical colors. 127546 (2002 XU 93 ), 528219 (2008 KV 42 ), 2010 WG 9 , and 2012 DR 30 have all been reported to have gray to moderately red optical colors similar to those of cometary nuclei, the Damocloids, the Trojan asteroids of Jupiter and Neptune, the less-red trans-Neptunian objects (TNOs), and the primitive Xand D-type asteroids (Sheppard 2010;Hainaut et al 2012;Kiss et al 2013;Rabinowitz et al 2013;Jewitt 2015;Szabó et al 2018;Hromakina et al 2021). The similarity between the colors of these minor planet populations and those of HiHq Centaurs suggests that the HiHq Centaurs are likely to have dark and carbonaceous surfaces that may have experienced significant irradiation and thermal evolution (e.g., Sheppard 2010).…”
Centaurs with high orbital inclinations and perihelia (i > 60°; q ≳ 5 au) are a small group of poorly understood minor planets that are predicted to enter the giant planet region of the solar system from the inner Oort Cloud. As such, they are one of the few samples of relatively unaltered Oort Cloud material that can currently be directly observed. Here we present two new reflectance spectra of one of the largest of these objects, 2012 DR30, in order to constrain its color and surface composition. Contrary to reports that 2012 DR30 has variable optical color, we find that consistent measurements of its spectral gradient from most new and published data sets at 0.55–0.8 μm agree with a spectral gradient of
S
′
≃
10
%
±
1
%
/
0.1
μ
m
within their uncertainties. The spectral variability of 2012 DR30 at near-UV/blue and near-IR wavelengths, however, is still relatively unconstrained; self-consistent rotationally resolved follow-up observations are needed to characterize any spectral variation in those regions. We tentatively confirm previous detections of water ice on the surface of 2012 DR30, and we also consistently observe a steady steepening of the gradient of its spectrum from λ ∼ 0.6 μm toward near-UV wavelengths. Plausible surface materials responsible for the observed reddening may include ferric oxides contained within phyllosilicates and aromatic refractory organics.
“…Both observing runs were conducted under clear (sky 90% cloudless at elevation >30°, transmission variation <10%) or photometric (sky cloudless, transmission variation <2%) conditions as defined by ESO; as a result, we expect the continuum colors of our spectra to be minimally affected by clouds, and therefore accurate. As in previously reported observational epochs (Kiss et al 2013;Szabó et al 2018;Hromakina et al 2021), 2012 DR 30 was found to be inactive both times we observed it.…”
Section: Observationssupporting
confidence: 90%
“…In Figure 2 we present our optical reflectance spectra of 2012 DR 30 in comparison to all published optical photometric and spectroscopic reflectance data where such data cover 0.6 μm, enabling consistent scaling between data sets (literature data sets include those reported by Kiss et al 2013;Szabó et al 2018;Hromakina et al 2021). Optical photometric colors were converted to coarse reflectance spectra using methods described by Hainaut & Delsanti (2002) and were scaled relative to the reflectance value at 0.6 μm on a line drawn between the two data points on either side of that wavelength.…”
Section: Discussionmentioning
confidence: 86%
“…As a collection, the optical colors reported for 2012 DR 30 so far suggest that its color varies significantly between observational epochs (Kiss et al 2013;Szabó et al 2018;Hromakina et al 2021).…”
Section: Introductionmentioning
confidence: 99%
“…To date, multiband photometry has been the main technique used for characterization of the surfaces of HiHq Centaurs, and half of those currently known have published optical colors. 127546 (2002 XU 93 ), 528219 (2008 KV 42 ), 2010 WG 9 , and 2012 DR 30 have all been reported to have gray to moderately red optical colors similar to those of cometary nuclei, the Damocloids, the Trojan asteroids of Jupiter and Neptune, the less-red trans-Neptunian objects (TNOs), and the primitive Xand D-type asteroids (Sheppard 2010;Hainaut et al 2012;Kiss et al 2013;Rabinowitz et al 2013;Jewitt 2015;Szabó et al 2018;Hromakina et al 2021). The similarity between the colors of these minor planet populations and those of HiHq Centaurs suggests that the HiHq Centaurs are likely to have dark and carbonaceous surfaces that may have experienced significant irradiation and thermal evolution (e.g., Sheppard 2010).…”
Centaurs with high orbital inclinations and perihelia (i > 60°; q ≳ 5 au) are a small group of poorly understood minor planets that are predicted to enter the giant planet region of the solar system from the inner Oort Cloud. As such, they are one of the few samples of relatively unaltered Oort Cloud material that can currently be directly observed. Here we present two new reflectance spectra of one of the largest of these objects, 2012 DR30, in order to constrain its color and surface composition. Contrary to reports that 2012 DR30 has variable optical color, we find that consistent measurements of its spectral gradient from most new and published data sets at 0.55–0.8 μm agree with a spectral gradient of
S
′
≃
10
%
±
1
%
/
0.1
μ
m
within their uncertainties. The spectral variability of 2012 DR30 at near-UV/blue and near-IR wavelengths, however, is still relatively unconstrained; self-consistent rotationally resolved follow-up observations are needed to characterize any spectral variation in those regions. We tentatively confirm previous detections of water ice on the surface of 2012 DR30, and we also consistently observe a steady steepening of the gradient of its spectrum from λ ∼ 0.6 μm toward near-UV wavelengths. Plausible surface materials responsible for the observed reddening may include ferric oxides contained within phyllosilicates and aromatic refractory organics.
“…The data obtained with reprocessed observations of asteroids for this long-term period are highly useful for a more detailed study of the dynamics and modern orbital parameters of asteroids (see, for example, Savanevych et al 2015;Savanevych et al 2018;Hromakina et al 2021;Vavilova et al 2022) as well as the obtained photometric parameters are very complementary with present-day data for studying changes in brightness and light curves (see, for example, Marzari, 2020).…”
For more than 50 years, the continuous photographic observations of asteroids have been carried outwith telescopes of the Astronomical Observatory of the Taras Shevchenko National University of Kyiv and the Main Astronomical Observatory of the National Academy of Sciences of Ukraine. About 3,000 photographic plates were obtained, some of which were exposed in 1908. We collected the data on more than 5,500 positions and magnitudes of asteroids on these astroplates taking into account all results of the processing of observations available in various publications and in the Minor Planet Center database. All positional data were compared with JPL ephemeris and analyzed. From different series of asteroid observations the values of positional accuracy were obtained, depending on the methods of measuring and processing the plates and reference catalogs of stars. In order to systematically improve the obtained asteroid positions, we evaluated the possibilities of reprocessing some of the earliest asteroid observations applying the modern star high accuracy catalogs. Using the Tycho-2, Gaia DR2, and Gaia EDR3 as the reference catalogs, the 590 astroplates exposed on the MAO NASU Double Long-Focus Astrograph (DLA) in 1952-1986 were reprocessed based on old plate measurements. All newly determined and previous original asteroid positions were compared with the JPL ephemeris. The comparison results show an improvement in the systematic and random components of the accuracy of coordinates for new positions of asteroids. When comparing the new positions of the asteroids determined in the Tycho-2 and Gaia catalog systems, no significant changes in accuracy were found.
Small Solar system bodies serve as pristine records that have been minimally altered since their formation. Their observations provide valuable information regarding the formation and evolution of our Solar system. Interstellar objects can also provide insight on the formation of exoplanetary systems and planetary system evolution as a whole. In this work, we present the application of our framework to search for small Solar system bodies in exoplanet transit survey data collected by the Antarctic Search for Transiting ExoPlanets (ASTEP) project. We analysed data collected during the Austral winter of 2021 by the ASTEP 400 telescope located at the Concordia Station, at Dome C, Antarctica. We identified 20 known objects from dynamical classes ranging from Inner Main-belt asteroids to one comet. Our search recovered known objects down to a magnitude of V = 20.4 mag, with a retrieval rate of ∼80 per cent for objects with V ≤ 20 mag. Future work will apply the pipeline to archival ASTEP data that observed fields for periods of longer than a few hours to treat them as deep-drilling data sets and reach fainter limiting magnitudes for slow-moving objects, on the order of V ≈ 23–24 mag.
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