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161. Saturn's G and D68 rings ISS observations
ID:
ivo://CDS.VizieR/J/ApJ/811/67
Title:
Saturn's G and D68 rings ISS observations
Short Name:
J/ApJ/811/67
Date:
21 Oct 2021
Publisher:
CDS
Description:
The appearance of debris disks around distant stars depends upon the scattering/phase function (SPF) of the material in the disk. However, characterizing the SPFs of these extrasolar debris disks is challenging because only a limited range of scattering angles are visible to Earth-based observers. By contrast, Saturn's tenuous rings can be observed over a much broader range of geometries, so their SPFs can be much better constrained. Since these rings are composed of small particles released from the surfaces of larger bodies, they are reasonable analogs to debris disks and so their SPFs can provide insights into the plausible scattering properties of debris disks. This work examines two of Saturn's dusty rings: the G ring (at 167500km from Saturn's center) and the D68 ringlet (at 67600km). Using data from the cameras on board the Cassini spacecraft, we are able to estimate the rings' brightnesses at scattering angles ranging from 170{deg} to 0.5{deg}. We find that both of the rings exhibit extremely strong forward-scattering peaks, but for scattering angles above 60{deg} their brightnesses are nearly constant. These SPFs can be well approximated by a linear combination of three Henyey-Greenstein functions, and are roughly consistent with the SPFs of irregular particles from laboratory measurements. Comparing these data to Fraunhofer and Mie models highlights several challenges involved in extracting information about particle compositions and size distributions from SPFs alone. The SPFs of these rings also indicate that the degree of forward scattering in debris disks may be greatly underestimated.
162. SBNAF Infrared Database
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.
163. SDSS Solar System Objects
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.
164. Search for extraterrestrial intelligence with ATA
ID:
ivo://CDS.VizieR/J/ApJ/869/66
Title:
Search for extraterrestrial intelligence with ATA
Short Name:
J/ApJ/869/66
Date:
21 Oct 2021
Publisher:
CDS
Description:
We report a novel radio autocorrelation search for extraterrestrial intelligence. For selected frequencies across the terrestrial microwave window (1-10GHz), observations were conducted at the Allen Telescope Array to identify artificial non-sinusoidal periodic signals with radio bandwidths greater than 4Hz, which are capable of carrying substantial messages with symbol rates from 4 to 10^6^Hz. Out of 243 observations, about half (101) were directed toward sources with known continuum flux >~1Jy over the sampled bandwidth (quasars, pulsars, supernova remnants, and masers), based on the hypothesis that they might harbor heretofore undiscovered natural or artificial repetitive, phase or frequency modulation. The rest of the observations were directed mostly toward exoplanet stars with no previously discovered continuum flux. No signals attributable to extraterrestrial technology were found in this study. We conclude that the maximum probability that future observations like the ones described here will reveal repetitively modulated emissions is less than 5% for continuum sources and exoplanets alike. The paper concludes by describing a new approach to expanding this survey to many more targets and much greater sensitivity using archived data from interferometers all over the world.
165. Sky Body Tracker
ID:
ivo://vopdc.obspm/imcce/skybot
Title:
Sky Body Tracker
Short Name:
SkyBoT
Date:
10 Jan 2017
Publisher:
Paris Astronomical Data Centre - IMCCE
Description:
SkyBoT is a VO service which allows to seek and identify solar system objects (planet, satellites, asteroids, comets) in any field of view at a given epoch (cone-search method). It provides also a solar system object name resolver which convert the name or the designation of solar system objects into their celestial coordinates at a given epoch (resolver method). The SkyBoT service are available through a Web interface and a Web service (SOAP+WSDL+HTTP) which implements the IVOA Simple Cone-Search protocol.
166. Sky Body Tracker - Remote application
ID:
ivo://vopdc.obspm/imcce/skybot/cea
Title:
Sky Body Tracker - Remote application
Short Name:
SkyBoT
Date:
10 Jan 2017
Publisher:
Paris Astronomical Data Centre - IMCCE
Description:
SkyBoT is a VO service which allows to seek and identify solar system objects (planet, satellites, asteroids, comets) in any field of view at a given epoch (cone-search method). It provides also a solar system object name resolver which convert the name or the designation of solar system objects into their celestial coordinates at a given epoch (resolver method). The SkyBoT service are available through a Web interface and a Web service (SOAP+WSDL+HTTP) which implements the IVOA Simple Cone-Search protocol.
167. Slowly diffusing planetary solutions freq. analysis
ID:
ivo://CDS.VizieR/J/A+A/628/A84
Title:
Slowly diffusing planetary solutions freq. analysis
Short Name:
J/A+A/628/A84
Date:
21 Oct 2021
Publisher:
CDS
Description:
Over short time-intervals, planetary ephemerides have traditionally been represented in analytical form as finite sums of periodic terms or sums of Poisson terms that are periodic terms with polynomial amplitudes. This representation is not well adapted for the evolution of planetary orbits in the solar system over million of years which present drifts in their main frequencies as a result of the chaotic nature of their dynamics. We aim to develop a numerical algorithm for slowly diffusing solutions of a perturbed integrable Hamiltonian system that will apply for the representation of chaotic planetary motions with varying frequencies. By simple analytical considerations, we first argue that it is possible to exactly recover a single varying frequency. Then, a function basis involving time-dependent fundamental frequencies is formulated in a semi-analytical way. Finally, starting from a numerical solution, a recursive algorithm is used to numerically decompose the solution into the significant elements of the function basis. Simple examples show that this algorithm can be used to give compact representations of different types of slowly diffusing solutions. As a test example, we show that this algorithm can be successfully applied to obtain a very compact approximation of the La2004 solution of the orbital motion of the Earth over 40Myr ([-35Myr,5Myr]). This example was chosen because this solution is widely used in the reconstruction of the past climates.
168. Solar and Lunar Eclipses: 1996-2020
ID:
ivo://CDS.VizieR/VI/97
Title:
Solar and Lunar Eclipses: 1996-2020
Short Name:
VI/97
Date:
21 Oct 2021
Publisher:
CDS
Description:
Solar Eclipses - During the twenty-five year period 1996-2020, some portion of the Moon's shadow will sweep across the Earth a total of fifty-six times. Twenty-one of these events result in partial solar eclipses, seventeen of them are annular eclipses, sixteen more are total eclipses and the remaining two are both annular and total along sections of their narrow paths. Local circumstances at the instant of greatest eclipse1 for every event during this quarter century period are presented in solar.dat. The date and Universal Time of the instant of greatest eclipse are found in the first two columns. The eclipse type is given (T=Total, A=Annular, AT=Annular/Total or P=Partial) along with the Saros series, as defined by van den Bergh (1955). The magnitude of the eclipse is defined as the fraction of the Sun's diameter obscured at greatest eclipse. The latitude and longitude of the umbra are given for the instant of greatest eclipse, along with the Sun's altitude, the width of the path (kilometers) and the duration of totality or annularity. For partial eclipses, the latitude and longitude of the point closest to the umbra's axis at the instant of greatest eclipse are listed. The altitude of the Sun at this location is 0 degrees. Note: Greatest eclipse is defined as the instant when the axis of the Moon's shadow passes closest to the Earth's center. For total eclipses, the instant of greatest eclipse is virtually identical to the instants of greatest magnitude and greatest duration. However, for annular eclipses, the instant of greatest duration may occur at either the time of greatest eclipse or near the sunrise and sunset points of the eclipse path. Lunar Eclipses - During the twenty-five year period 1996-2020, the Moon will swing through some portion of Earth's shadow a total of fifty-eight times. Twenty-three of these events result in penumbral lunar eclipses, twelve of them are partial (umbral) eclipses, twenty-three more are total lunar eclipses. Local circumstances at the instant of greatest eclipse1 for every event during this quarter century period are presented in Table 1. The date and Universal Time of the instant of greatest eclipse are found in the first two columns. The eclipse type is given (T=Total, P=Partial [Umbral], or P=Penumbral) along with the Saros series, as defined by van den Bergh (1955). The penumbral and umbral magnitudes of the eclipse are defined as the fraction of the Moon's diameter obscured by either shadow at greatest eclipse. The partial and total semi-durations of the eclipse along with the Greenwich Siderial Time at midnight, and the Moon's Right Ascension and Declination are listed. The start and end times of the partial eclipse can be calculated by respectively subtacting and adding the partial semi-duration (i.e. - Par. SDur) to the instant of greatest eclipse. Likewise, the start and end times of the total eclipse can be calculated by respectively subtacting and adding the total semi-duration (i.e. - Total SDur) to the instant of greatest eclipse. Note: Greatest eclipse is defined as the instant when the Moon passes closest to the axis of Earth's shadow(s). This marks the instant when the Moon is deepest in Earth's shadow(s).
169. Solar s-process contributions with GCE model
ID:
ivo://CDS.VizieR/J/ApJ/787/10
Title:
Solar s-process contributions with GCE model
Short Name:
J/ApJ/787/10
Date:
21 Oct 2021
Publisher:
CDS
Description:
We study the s-process abundances (A>~90) at the epoch of the solar system formation. Asymptotic giant branch yields are computed with an updated neutron capture network and updated initial solar abundances. We confirm our previous results obtained with a Galactic chemical evolution (GCE) model: (1) as suggested by the s-process spread observed in disk stars and in presolar meteoritic SiC grains, a weighted average of s-process strengths is needed to reproduce the solar s distribution of isotopes with A>130; and (2) an additional contribution (of about 25%) is required in order to represent the solar s-process abundances of isotopes from A=90 to 130. Furthermore, we investigate the effect of different internal structures of the ^13^C pocket, which may affect the efficiency of the ^13^C({alpha},n)^16^O reaction, the major neutron source of the s process. First, keeping the same ^13^C profile adopted so far, we modify by a factor of two the mass involved in the pocket; second, we assume a flat ^13^C profile in the pocket, and we test again the effects of the variation of the mass of the pocket. We find that GCE s predictions at the epoch of the solar system formation marginally depend on the size and shape of the ^13^C pocket once a different weighted range of ^13^C-pocket strengths is assumed. We obtain that, independently of the internal structure of the ^13^C pocket, the missing solar system s-process contribution in the range from A=90 to 130 remains essentially the same.
170. Solar system survey with Spacewatch
ID:
ivo://CDS.VizieR/J/AJ/133/1247
Title:
Solar system survey with Spacewatch
Short Name:
J/AJ/133/1247
Date:
21 Oct 2021
Publisher:
CDS
Description:
We have completed a low-inclination ecliptic survey for distant and slow-moving bright objects in the outer solar system. This survey used data taken over 34 months by the University of Arizona's Spacewatch Project based at Steward Observatory, Kitt Peak. Spacewatch revisits the same sky area every three to seven nights in order to track cohorts of main-belt asteroids. This survey used a multiple-night detection scheme to extend our rate sensitivity to as low as 0.012"/hr. When combined with our plate scale and flux sensitivity (V~21), this survey was sensitive to Mars-sized objects out to 300AU and Jupiter-sized planets out to 1200AU. The survey covered approximately 8000deg^2^ of raw sky, mostly within 10{deg} of the ecliptic but away from the Galactic center. An automated motion detection program was modified for this multinight search and processed approximately 2 terabytes of imagery into motion candidates. This survey discovered 2003 MW12, currently the tenth largest classical Kuiper Belt object. In addition, several known large Kuiper Belt objects and Centaurs were detected, and the detections were used with a model of our observational biases to make population estimates as a check on our survey efficiency. We found no large objects at low inclinations despite having sufficient sensitivity in both flux and rate to see them out as far as 1200AU. For low inclinations, we can rule out more than one to two Pluto-sized objects out to 100AU and one to two Mars-sized objects to 200AU.