- ID:
- ivo://CDS.VizieR/J/A+A/569/A3
- Title:
- Rotational properties of TNOs
- Short Name:
- J/A+A/569/A3
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present results for the short-term variability of Binary Trans-Neptunian Objects (BTNOs). We performed CCD photometric observations using the 3.58m Telescopio Nazionale Galileo (TNG), the 1.5m Sierra Nevada Observatory (OSN) telescope, and the 1.23m Centro Astronomico Hispano Aleman (CAHA) telescope at Calar Alto Observatory. We present results based on five years of observations and report the short-term variability of six BTNOs. Our sample contains three classical objects: (174567) 2003 MW_12_, or Varda, (120347) 2004 SB_60_, or Salacia, and 2002 VT_130_; one detached disk object: (229762) 2007 UK_126_; and two resonant objects: (341520) 2007 TY_430_ and (38628) 2000 EB_173_, or Huya. For each target, possible rotational periods and/or photometric amplitudes are reported. We also derived some physical properties from their lightcurves, such as density, primary and secondary sizes, and albedo. We compiled and analyzed a vast lightcurve database for Trans-Neptunian Objects (TNOs) including centaurs to determine the lightcurve amplitude and spin frequency distributions for the binary and non-binary populations. The mean rotational periods, from the Maxwellian fits to the frequency distributions, are 8.63+/-0.52h for the entire sample, 8.37+/-0.58h for the sample without the binary population, and 10.11+/-1.19h for the binary population alone. Because the centaurs are collisionally more evolved, their rotational periods might not be so primordial. We computed a mean rotational period, from the Maxwellian fit, of 8.86+/-0.58h for the sample without the centaur population, and of 8.64+/-0.67h considering a sample without the binary and the centaur populations. According to this analysis, regular TNOs spin faster than binaries, which is compatible with the tidal interaction of the binaries. Finally, we examined possible formation models for several systems studied in this work and by our team in previous papers.
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Search Results
- ID:
- ivo://CDS.VizieR/J/ApJS/255/4
- Title:
- Rotation periods from the K2 Campaign 9
- Short Name:
- J/ApJS/255/4
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Kepler mission is a powerful tool for the study of different types of astrophysical objects or events in the distant universe. However, the spacecraft also provides an opportunity to study solar system objects passing in the telescope's field of view. The aim of this paper is to determine, for the first time, the rotation periods of a number of asteroids observed by the K2 satellite during the K2 Campaign 9. Using publicly available data from the Kepler mission, we have used the Modified Causal Pixel Model code to perform the aperture-like and point-response function-like photometry of 1026 asteroids. The results allowed us to determine the rotation periods for 188 asteroids. For asteroids with rotation periods that were previously measured, we compared the results and found very good agreement. There are an additional 20 asteroids for which we obtained lower limits on rotation periods and in all cases these limits are at least 100hr.
- ID:
- ivo://CDS.VizieR/J/ApJS/227/20
- Title:
- Rotation periods of asteroids using iPTF
- Short Name:
- J/ApJS/227/20
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In order to look for large super-fast rotators, in late 2014 and early 2015, five dedicated surveys covering ~188deg^2^ in the ecliptic plane have been carried out in the R-band, with ~10min cadence using the intermediate Palomar Transient Factory. Among 1029 reliable rotation periods obtained from the surveys, we discovered 1 new large super-fast rotator, (40511) 1999 RE88, and 18 other candidates. (40511) 1999 RE88 is an S-type inner main-belt asteroid with a diameter of D=1.9+/-0.3km, a rotation period of P=1.96+/-0.01hr, and a light curve amplitude of {Delta}m~1.0mag. To maintain such fast rotation, an internal cohesive strength of ~780Pa is required. Combining all known large super-fast rotators, their cohesive strengths all fall in the range of 100-1000Pa of lunar regolith. However, the number of large super-fast rotators seems to be far less than the whole asteroid population. This might indicate a peculiar asteroid group for them. Although the detection efficiency for a long rotation period is greatly reduced due to our two-day observation time span, the spin-rate distributions of this work show consistent results with Chang+ (2015, J/ApJS/219/27), after considering the possible observational bias in our surveys. It shows a number decrease with an increase of spin rate for asteroids with a diameter of 3<=D<=15km, and a number drop at a spin rate of f=5rev/day for asteroids with D<=3km.
- ID:
- ivo://CDS.VizieR/J/A+A/407/1139
- Title:
- RVB photometry of Kuiper-Belt object 1999 TD10
- Short Name:
- J/A+A/407/1139
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present photometric observations of the Kuiper-Belt object 1999 TD_10_ at different phase angles and for three different broad band filters (B, V and R). This object was observed with the Danish 1.54-m telescope of ESO in Chile during six different observing nights corresponding to a phase angle of 0.30, 0.37, 0.92, 3.43, 3.48 and 3.66{deg}. Extra observations were obtained in September 2002 with the VLT UT1/FORS1 combination to confirm that 1999 TD_10_ does not exhibit any cometary activity, and in October 2001 with the Sierra Nevada Observatory 1.50-m telescope in order to add relative magnitudes to improve the determination of the rotation period.
- ID:
- ivo://CDS.VizieR/J/A+A/572/A43
- Title:
- Saturnian satellites Cassini ISS astrometry
- Short Name:
- J/A+A/572/A43
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We provide astrometric observations of the Saturnian satellites Mimas, Enceladus, Tethys, Dione and Rhea from Cassini Imaging Science Subsystem (ISS) narrow-angle camera (NAC) images. Image sequences were designed to observe mutual occultations between these satellites.
- ID:
- ivo://CDS.VizieR/J/A+A/635/A54
- Title:
- SBNAF Infrared Database
- Short Name:
- J/A+A/635/A54
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this paper, we present the Small Bodies: Near and Far (SBNAF) Infrared Database, an easy-to-use tool intended to facilitate the modelling of thermal emission of small bodies of the Solar System. Our database collects measurements of thermal emissions for small Solar System targets that are otherwise available in scattered sources and provides a complete description of the data, including all information necessary to perform direct scientific analyses and without the need to access additional external resources. This public database contains representative data of asteroid observations of large surveys (e.g. AKARI, IRAS, and WISE) as well as a collection of small body observations of infrared space telescopes (e.g. the Herschel Space Observatory) and provides a web interface to access this data (https://ird.konkoly.hu).We also provide an example for the direct application of the database and show how it can be used to estimate the thermal inertia of specific populations, e.g. asteroids within a given size range. We show how different scalings of thermal inertia with heliocentric distance (i.e. temperature) may affect our interpretation of the data and discuss why the widely-used radiative conductivity exponent (alpha=-3/4) might not be adequate in general, as suggested in previous studies.
- ID:
- ivo://CDS.VizieR/J/ApJ/749/10
- Title:
- SDSS observations of Kuiper belt objects
- Short Name:
- J/ApJ/749/10
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Colors of trans-Neptunian objects (TNOs) are used to study the evolutionary processes of bodies in the outskirts of the solar system and to test theories regarding their origin. Here I describe a search for serendipitous Sloan Digital Sky Survey (SDSS) observations of known TNOs and Centaurs. I present a catalog of SDSS photometry, colors, and astrometry of 388 measurements of 42 outer solar system objects. I find weak evidence, at the {approx} 2{sigma} level (per trial), for a correlation between the g - r color and inclination of scattered disk objects and hot classical Kuiper Belt objects. I find a correlation between the g - r color and the angular momentum in the z direction of all the objects in this sample. These findings should be verified using larger samples of TNOs. Light curves as a function of phase angle are constructed for 13 objects. The steepness of the slopes of these light curves suggests that the coherent backscatter mechanism plays a major role in the reflectivity of outer solar system small objects at small phase angles. I find weak evidence for an anticorrelation, significant at the 2{sigma} confidence level (per trial), between the g-band phase-angle slope parameter and the semimajor axis, as well as the aphelion distance, of these objects (i.e., they show a more prominent "opposition effect" at smaller distances from the Sun). However, this plausible correlation should be verified using a larger sample. I discuss the origin of this possible correlation and argue that if this correlation is real it probably indicates that "Sedna"-like objects have a different origin than other classes of TNOs. Finally, I identify several objects with large variability amplitudes.
- ID:
- ivo://CDS.VizieR/J/A+A/652/A59
- Title:
- SDSS Solar System Objects
- Short Name:
- J/A+A/652/A59
- Date:
- 22 Feb 2022
- Publisher:
- CDS
- Description:
- The populations of small bodies of the Solar System (asteroids, comets, Kuiper-Belt objects) are used to constrain the origin and evolution of the Solar System. Both their orbital distribution and composition distribution are required to track the dynamical pathway from their regions of formation to their current locations. We aim at increasing the sample of Solar System objects that have multi-filter photometry and compositional taxonomy. We search for moving objects in the archive of the Sloan Digital Sky Survey. We attempt at maximizing the number of detections by using loose constraints on the extraction. We then apply a suite of filters to remove false-positive detections (stars or galaxies) and mark out spurious photometry and astrometry. We release a catalog of 1542522 entries, consisting of 1036322 observations of 379714 known and unique SSOs together with 506200 observations of moving sources not linked with any known SSOs. The catalog completeness is estimated to be about 95% and the purity to be above 95% for known SSOs.
- ID:
- ivo://CDS.VizieR/J/ApJS/241/6
- Title:
- Searching for super-fast rotators using PS1
- Short Name:
- J/ApJS/241/6
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A class of asteroids, called large super-fast rotators (large SFRs), have rotation periods shorter than 2hr and diameters larger than ~0.3km. They pose challenges to the usual interior rubble-pile structure unless a relatively high bulk density is assumed. So far, only six large SFRs have been found. Therefore, we present a survey of asteroid rotation periods using the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) 1 telescope during 2016 October 26-31 to search for more large SFRs and to study their properties. A total of 876 reliable rotation periods are measured, among which seven are large SFRs, thereby increasing the inventory of known large SFRs. These seven newly discovered large SFRs have diverse colors and locations in the main asteroid belt, suggesting that the taxonomic tendency and the location preference in the inner main belt of the six previously known large SFRs could be a bias due to various observational limits. Interestingly, five out of the seven newly discovered large SFRs are mid main-belt asteroids (MBAs). Considering the rare discovery rates of large SFR in the previously similar surveys and the survey condition in this work, the chance of detecting a large SFR in the inner main belt seems to be relatively low. This probably suggests that the inner main belt harbors fewer large SFRs than the mid main belt. From our survey, we also found a drop in the number appearing at f>5rev/day on the spin-rate distribution for the outer MBAs of D<3km, which was reported for the inner and mid main belt by Chang et al. (2015, J/ApJS/219/27 ; 2016ApJ...816...71C).
- ID:
- ivo://CDS.VizieR/J/A+A/522/A93
- Title:
- Short-term variability of 29 minor planets
- Short Name:
- J/A+A/522/A93
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present results of 6 years of observations, reduced and analyzed with the same tools in a systematic way. We present completely new data on 15 objects (1998SG35, 2002GB10, 2003EL61, 2003FY128, 2003MW12, 2003OP32, 2003WL7, 2004SB60, 2004UX10, 2005CB79, 2005RM43, 2005RN43, 2005RR43, 2005UJ438, 2007UL126 (or 2002KY14)), for 5 objects we present a new analysis of previously published results plus additional data (2000WR106, 2002CR46, 2002TX300, 2002VE95, 2005FY9) and for 9 objects we present a new analysis of data already published (1996TL66, 1999TZ1, 2001YH140, 2002AW197, 2002LM60, 2003AZ84, 2003CO1, 2003VS2, 2004DW). Lightcurves, possible rotation periods and photometric amplitudes are reported for all of them. The photometric variability is smaller than previously thought: the mean amplitude of our sample is 0.1mag and only around 15% of our sample has a larger variability than 0.15mag. The smaller variability than previously thought seems to be a bias of previous observations. We find a very weak trend of faster spinning objects towards smaller sizes, which appears to be consistent with the fact that the smaller objects are more collisionally evolved, but could also be a specific feature of the Centaurs, the smallest objects in our sample.We also find that the smaller the objects, the larger their amplitude, which is also consistent with the idea that small objects are more collisionally evolved and thus more deformed. Average rotation rates from our work are 7.5h for the whole sample, 7.6h for the TNOs alone and 7.3h for the Centaurs. All of them appear to be somewhat faster than what one can derive from a compilation of the scientific literature and our own results. Maxwellian fits to the rotation rate distribution give mean values of 7.5h (for the whole sample) and 7.3h (for the TNOs only). Assuming hydrostatic equilibrium we can determine densities from our sample under the additional assumption that the lightcurves are dominated by shape effects, which is likely no realistic. The resulting average density is 0.92g/cm^3^ which is not far from the density constraint that one can derive from the apparent spin barrier that we observe.
