Search

Start Over Subject asteroids
141. Occultations of stars by asteroids 1995-96
ID:
ivo://CDS.VizieR/J/AJ/109/1363
Title:
Occultations of stars by asteroids 1995-96
Short Name:
J/AJ/109/1363
Date:
21 Oct 2021
Publisher:
CDS
Description:
Predictions, based on a computerized comparison of asteroid ephemerides with the catalog positions of 567,500 stars, are given for 155 occultations of stars by asteroids in 1995 and 1996. On average, the predictions are expected to be more accurate than in earlier searches because of the use of more modern star catalogs. A number of very favorable occultations, visible in North Armerica and elsewhere, are discussed.
142. Occultations of stars by large TNO 2004-2014
ID:
ivo://CDS.VizieR/J/PAZh/30/692
Title:
Occultations of stars by large TNO 2004-2014
Short Name:
J/PAZh/30/692
Date:
21 Oct 2021
Publisher:
CDS
Description:
Occultations of stars brighter than 15m by largest trans-Neptunian objects (TNOs) are predicted. Search was performed using the following catalogues: Hipparcos (Cat. <I/239>; Tycho2 (Cat. <I/259>) with coordinates of 2838666 stars taken from UCAC2 (Herald, 2003); UCAC2 (Zacharias et al., 2003, Cat. <I/289>) with 16356096 stars between 12.00 and 14.99mag to the north from -45{deg} declination. Predictions were made for 17 largest numbered transneptunian asteroids and 4 known binary Kuiper Belt objects. 67 events occuring at solar elongation of 30{deg} and more are selected. Observations of these occultations by all available means are extremely important since they can give unique information about the size of TNOs and improve their orbits dramatically. Finder charts and preliminary path plots are available separately at http://hea.iki.rssi.ru/~denis/TNOocc.html of by E-mail to denis@hea.iki.rssi.ru
143. 280 one-opposition near Earth asteroids
ID:
ivo://CDS.VizieR/J/A+A/609/A105
Title:
280 one-opposition near Earth asteroids
Short Name:
J/A+A/609/A105
Date:
21 Oct 2021
Publisher:
CDS
Description:
One-opposition near-Earth asteroids (NEAs) are growing in number, and they must be recovered to prevent loss and mismatch risk, and to improve their orbits, as they are likely to be too faint for detection in shallow surveys at future apparitions. We aimed to recover more than half of the one-opposition NEAs recommended for observations by the Minor Planet Center (MPC) using the Isaac Newton Telescope (INT) in soft-override mode and some fractions of available D-nights. During about 130 hours in total between 2013 and 2016, we targeted 368 NEAs, among which 56 potentially Hazardous asteroids (PHAs), observing 437 INT Wide Field Camera (WFC) fields and recovering 280 NEAs (76% of all targets). Engaging a core team of about ten students and amateurs, we used the THELI, Astrometrica, and the Find_Orb software to identify all moving objects using the blink and track-and-stack method for the faintest targets and plotting the positional uncertainty ellipse from NEODyS. Results. Most targets and recovered objects had apparent magnitudes centered around V~22.8mag, with some becoming as faint as V~24mag. One hundred and three objects (representing 28% of all targets) were recovered by EURONEAR alone by Aug 2017. Orbital arcs were prolonged typically from a few weeks to a few years; our oldest recoveries reach 16 years. The O-C residuals for our 1,854 NEA astrometric positions show that most measurements cluster closely around the origin. In addition to the recovered NEAs, 22,000 positions of about 3,500 known minor planets and another 10,000 observations of about 1,500 unknown objects (mostly main-belt objects) were promptly reported to the MPC by our team. Four new NEAs were discovered serendipitously in the analyzed fields and were promptly secured with the INT and other telescopes, while two more NEAs were lost due to extremely fast motion and lack of rapid follow-up time. They increase the counting to nine NEAs discovered by the EURONEAR in 2014 and 2015. Targeted projects to recover one-opposition NEAs are efficient in override access, especially using at least two-meter class and preferably larger field telescopes located in good sites, which appear even more efficient than the existing surveys.
144. Orbital Elements of Minor Planets 1998
ID:
ivo://CDS.VizieR/I/245
Title:
Orbital Elements of Minor Planets 1998
Short Name:
I/245
Date:
21 Oct 2021
Publisher:
CDS
Description:
The catalogue contains osculating elements of all permanently numbered minor planets as of November 25, 1996. The elements are given with respect to the ecliptic plane and equinox J2000 for the standard epoch JD2451000.5 = 1998 July 6.0 ET. The elements of (719) Albert which is considered to be lost are given for the epoch when the planet was discovered. The catalogue data, in general, correspond to those in "Ephemerides of Minor Planets for 1998", St.Petersburg, 1997 (in print). Along with these data the catalogue incorporates some connected information. (C) Copyright 1997 ITA RAS
145. Orbital Elements of Minor Planets 1997
ID:
ivo://CDS.VizieR/I/233
Title:
Orbital Elements of Minor Planets 1997
Short Name:
I/233
Date:
21 Oct 2021
Publisher:
CDS
Description:
The catalogue contains osculating elements of all permanently numbered minor planets as of November 7, 1995. The elements are given with respect to the ecliptic plane and equinox J2000 for the standard epoch JD2450800.5 = 1997 December 18.0 ET. The elements of (719) Albert which is considered to be lost are given for the epoch when the planet was discovered. The catalogue data, in general, correspond to those published in "Ephemerides of Minor Planets for 1997", St.Petersburg, 1996. Along with these data the catalogue incorporates some connected information. (C) Copyright 1996 ITA RAS
146. Orbital elements of TNOs from the Dark Energy Survey
ID:
ivo://CDS.VizieR/J/AJ/159/133
Title:
Orbital elements of TNOs from the Dark Energy Survey
Short Name:
J/AJ/159/133
Date:
21 Oct 2021
Publisher:
CDS
Description:
The outer solar system contains a large number of small bodies (known as trans-Neptunian objects or TNOs) that exhibit diverse types of dynamical behavior. The classification of bodies in this distant region into dynamical classes-subpopulations that experience similar orbital evolution-aids in our understanding of the structure and formation of the solar system. In this work, we propose an updated dynamical classification scheme for the outer solar system. This approach includes the construction of a new (automated) method for identifying mean motion resonances. We apply this algorithm to the current data set of TNOs observed by the Dark Energy Survey (DES) and present a working classification for all of the DES TNOs detected to date. Our classification scheme yields 1 inner centaur, 19 outer centaurs, 21 scattering disk objects, 47 detached TNOs, 48 securely resonant objects, 7 resonant candidates, and 97 classical belt objects. Among the scattering and detached objects, we detect 8 TNOs with semimajor axes greater than 150au.
147. Orbital parameters of Kuiper Belt objects
ID:
ivo://CDS.VizieR/J/AJ/154/62
Title:
Orbital parameters of Kuiper Belt objects
Short Name:
J/AJ/154/62
Date:
21 Oct 2021
Publisher:
CDS
Description:
We measured the mean plane of the Kuiper Belt as a function of semimajor axis. For the classical Kuiper Belt as a whole (the nonresonant objects in the semimajor axis range 42-48au), we find a mean plane of inclination i_m_=1.8{deg}_-0.4{deg}_^+0.7{deg}^ and longitude of ascending node {Omega}_m_=77{deg}_-14{deg}_^+18{deg}^ (in the J2000 ecliptic-equinox coordinate system), in accord with theoretical expectations of the secular effects of the known planets. With finer semimajor axis bins, we detect a statistically significant warp in the mean plane near semimajor axes 40-42au. Linear secular theory predicts a warp near this location due to the {nu}_18_ nodal secular resonance; however, the measured mean plane for the 40.3-42au semimajor axis bin (just outside the {nu}_18_) is inclined ~13{deg} to the predicted plane, a nearly 3{sigma} discrepancy. For the more distant Kuiper Belt objects of semimajor axes in the range 50-80au, the expected mean plane is close to the invariable plane of the solar system, but the measured mean plane deviates greatly from this: it has inclination i_m_=9.1{deg}_-3.8{deg}_^+6.6{deg}^ and longitude of ascending node {Omega}_m_=227{deg}_-44{deg}_^+18{deg}^. We estimate this deviation from the expected mean plane to be statistically significant at the ~97%-99% confidence level. We discuss several possible explanations for this deviation, including the possibility that a relatively close-in (a<~100au), unseen, small planetary-mass object in the outer solar system is responsible for the warping.
148. Orbits of Minor Planets
ID:
ivo://CDS.VizieR/B/astorb
Title:
Orbits of Minor Planets
Short Name:
B/astorb
Date:
07 Feb 2022 15:12:49
Publisher:
CDS
Description:
astorb is a database of osculating orbital elements and ephemeris uncertainties near the current epoch for all known asteroids in the Solar System. It has been hosted at Lowell Observatory since the 1990's and is actively curated to be automatically updated as new objects are discovered. Access to the database, additional documentation, additional data, and associated tools are available at asteroid.lowell.edu.
149. OSSOS. VII. TNOs complete data release
ID:
ivo://CDS.VizieR/J/ApJS/236/18
Title:
OSSOS. VII. TNOs complete data release
Short Name:
J/ApJS/236/18
Date:
21 Oct 2021
Publisher:
CDS
Description:
The Outer Solar System Origins Survey (OSSOS), a wide-field imaging program in 2013-2017 with the Canada-France-Hawaii Telescope, surveyed 155deg^2^ of sky to depths of m_r_=24.1-25.2. We present 838 outer solar system discoveries that are entirely free of ephemeris bias. This increases the inventory of trans-Neptunian objects (TNOs) with accurately known orbits by nearly 50%. Each minor planet has 20-60 Gaia/Pan-STARRS-calibrated astrometric measurements made over 2-5 oppositions, which allows accurate classification of their orbits within the trans-Neptunian dynamical populations. The populations orbiting in mean-motion resonance with Neptune are key to understanding Neptune's early migration. Our 313 resonant TNOs, including 132 plutinos, triple the available characterized sample and include new occupancy of distant resonances out to semimajor axis a ~130au. OSSOS doubles the known population of the nonresonant Kuiper Belt, providing 436 TNOs in this region, all with exceptionally high-quality orbits of a uncertainty {sigma}_a_<=0.1%; they show that the belt exists from a>~37au, with a lower perihelion bound of 35au. We confirm the presence of a concentrated low-inclination a~44 au "kernel" population and a dynamically cold population extending beyond the 2:1 resonance. We finely quantify the survey's observational biases. Our survey simulator provides a straightforward way to impose these biases on models of the trans-Neptunian orbit distributions, allowing statistical comparison to the discoveries. The OSSOS TNOs, unprecedented in their orbital precision for the size of the sample, are ideal for testing concepts of the history of giant planet migration in the solar system.
150. OSSOS. XII. Subaru/HSC obs. of 65 TNOs
ID:
ivo://CDS.VizieR/J/ApJS/244/19
Title:
OSSOS. XII. Subaru/HSC obs. of 65 TNOs
Short Name:
J/ApJS/244/19
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present variability measurements and partial light curves of trans-Neptunian objects (TNOs) from a two-night pilot study using Hyper Suprime-Cam (HSC) on the Subaru Telescope (Maunakea, Hawaii, USA). Subaru's large aperture (8m) and HSC's large field of view (1.77deg^2^) allow us to obtain measurements of multiple objects with a range of magnitudes in each telescope pointing. We observed 65 objects with m_r_=22.6-25.5mag in just six pointings, allowing 20-24 visits of each pointing over the two nights. Our sample, all discovered in the recent Outer Solar System Origins Survey (OSSOS), spans absolute magnitudes of H_r_=6.2-10.8mag and thus investigates smaller objects than previous light curve projects have typically studied. Our data supports the existence of a correlation between the light curve amplitude and absolute magnitude seen in other works but does not support a correlation between the amplitude and orbital inclination. Our sample includes a number of objects from different dynamical populations within the trans-Neptunian region, but we do not find any relationship between variability and the dynamical class. We were only able to estimate periods for 12 objects in the sample and found that a longer baseline of observations is required for a reliable period analysis. We find that 31 objects (just under half of our sample) have variability of {Delta}_mag_ greater than 0.4mag during all of the observations; in smaller 1.25hr, 1.85hr, and 2.45hr windows, the median {Delta}_mag_ is 0.13, 0.16, and 0.19mag, respectively. The fact that variability on this scale is common for small TNOs has important implications for discovery surveys (such as OSSOS or the Large Synoptic Survey Telescope) and color measurements.