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361. Precise CCD positions of Phoebe in 2011-2014
ID:
ivo://CDS.VizieR/J/MNRAS/449/2638
Title:
Precise CCD positions of Phoebe in 2011-2014
Short Name:
J/MNRAS/449/2638
Date:
21 Oct 2021
Publisher:
CDS
Description:
346 new CCD observations during the years 2011-2014 have been reduced to derive the precise positions of Phoebe, the ninth satellite of Saturn. The observations were made by the 2.4 m telescope at Yunnan Observatory over nine nights. Due to the use of a focal-reducer on the telescope, its significant geometric distortion is solved for and removed for each CCD field of view. The positions of Phoebe are measured with respect to the stars in UCAC2 catalogue (Cat. I/289). The theoretical position of Phoebe was retrieved from the Institute de Mechanique Celeste et de Calcul des Ephemerides (IMCCE) ephemeris which includes the latest theory PH12 by Desmars et al. (2013, J/A+A/553/A36), while the position of Saturn was obtained from the Jet Propulsion Laboratory ephemeris DE431. Our results show that the mean O-Cs (observed minus computed) are -0.02 and -0.07 arcsec in right ascension and declination, respectively. The dispersions of our observations are estimated at about 0.04 arcsec in each direction.
362. Precise positions of RR Lyrae Stars with Vmax>12.5
ID:
ivo://CDS.VizieR/J/A+A/442/381
Title:
Precise positions of RR Lyrae Stars with Vmax>12.5
Short Name:
J/A+A/442/381
Date:
21 Oct 2021
Publisher:
CDS
Description:
RR Lyrae stars are of great importance for investigations of Galactic structure. However, a complete compendium of all RR-Lyraes in the solar neighbourhood with accurate classifications and coordinates does not exist to this day. Here we present a catalogue of 561 local RR-Lyrae stars (V_max_>=12.5mag) according to the magnitudes given in the Combined General Catalogue of Variable Stars (GCVS) and 16 fainter ones. The Tycho2 catalogue contains ~100 RR Lyr stars. However, many objects have inaccurate coordinates in the GCVS, the primary source of variable star information, so that a reliable cross-identification is difficult. We identified RR Lyrae from both catalogues based on an intensive literature search. In dubious cases we carried out photometry of fields to identify the variable. Mennessier & Colome (2002, Cat. <J/A+A/390/173>) have published a paper with Tyc2-GCVS identifications, but we found that many of their identifications are wrong.
363. Precise Radio Source Positions from Mark III VLBI
ID:
ivo://CDS.VizieR/I/151
Title:
Precise Radio Source Positions from Mark III VLBI
Short Name:
I/151
Date:
21 Oct 2021
Publisher:
CDS
Description:
This catalog contains observations from 600 Mark III VLBI experiments from conducted between 1979 to 1988. These experiments resulted in 237681 acceptable pairs of group delay and phase delay rate observations. These have been used to derive positions of 182 extra-galactic radio sources with typical formal standard errors less than 1 mas. The right ascension zero point of this reference frame has been aligned with the FK5 by using the optical positions of 28 extragalactic radio sources whose positions are on the FK5 system. Also included are the Mark III VLBI stations and a summary of the analysis configuration.
364. Precision meteor orbits
ID:
ivo://CDS.VizieR/J/A+AS/128/179
Title:
Precision meteor orbits
Short Name:
J/A+AS/128/179
Date:
21 Oct 2021
Publisher:
CDS
Description:
Orbital elements, encounter data and other relevant information of 359 photographic meteors (Table 2 of the paper).
365. Predicted Microlensing Events by nearby VLM objects
ID:
ivo://CDS.VizieR/J/AcA/68/351
Title:
Predicted Microlensing Events by nearby VLM objects
Short Name:
J/AcA/68/351
Date:
21 Oct 2021
Publisher:
CDS
Description:
Microlensing events can be used to directly measure the masses of single field stars to a precision of ~1-10%. The majority of direct mass measurements for stellar and sub-stellar objects typically only come from observations of binary systems. Hence microlensing provides an important channel for direct mass measurements of single stars. The Gaia satellite has observed ~1.7 billion objects, and analysis of the second data release has recently yielded numerous event predictions for the next few decades. However, the Gaia catalog is incomplete for nearby very-low-mass objects such as brown dwarfs for which mass measurements are most crucial. We employ a catalog of very-low-mass objects from Pan-STARRS data release 1 (PDR1) as potential lens stars, and we use the objects from Gaia data release 2 (GDR2) as potential source stars. We then search for future microlensing events up to the year 2070. The Pan-STARRS1 objects are first cross-matched with GDR2 to remove any that are present in both catalogs. This leaves a sample of 1718 possible lenses. We fit MIST isochrones to the Pan-STARRS1, AllWISE and 2MASS photometry to estimate their masses. We then compute their paths on the sky, along with the paths of the GDR2 source objects, until the year 2070, and search for potential microlensing events. Source-lens pairs that will produce a microlensing signal with an astrometric amplitude of greater than 0.131mas, or a photometric amplitude of greater than 0.4mmag, are retained.
366. Predicted Microlensing Events for the 21st Century
ID:
ivo://CDS.VizieR/J/AcA/68/183
Title:
Predicted Microlensing Events for the 21st Century
Short Name:
J/AcA/68/183
Date:
21 Oct 2021
Publisher:
CDS
Description:
Using Gaia data release 2 (GDR2, Cat. I/345), we present an almanac of 2509 predicted microlensing events, caused by 2130 unique lens stars, that will peak between July 25, 2026 and the end of the century. This work extends and completes a thorough search for future microlensing events initiated by Bramich and Nielsen using GDR2. The almanac includes 161 lenses that will cause at least two microlensing events each. All of the predicted microlensing events in the almanac will exhibit astrometric signals that are detectable by observing facilities with an angular resolution and astrometric precision similar to, or better than, that of the Hubble Space Telescope (e.g., NIRCam on the James Webb Space Telescope), although the events with the most extreme source-to-lens contrast ratios may be challenging. Ground-based telescopes of at least 1 m in diameter can be used to observe many of the events that are also expected to exhibit a photometric signal.
367. Predicted microlensing events from Gaia DR2
ID:
ivo://CDS.VizieR/J/A+A/618/A44
Title:
Predicted microlensing events from Gaia DR2
Short Name:
J/A+A/618/A44
Date:
21 Oct 2021
Publisher:
CDS
Description:
I search for source-lens pairs in Gaia Data Release 2 (GDR2, Cat. I/345) that could potentially lead to microlensing events between 25th July 2014 and 25th July 2026. I estimate the lens masses using GDR2 photometry and parallaxes, and appropriate model stellar isochrones. Combined with the source and lens parallax measurements from GDR2, this allows the Einstein ring radius to be computed for each source-lens pair. By considering the source and lens paths on the sky, I calculate the microlensing signals that are to be expected.
368. Preliminary Cat. of Fund. Faint Stars
ID:
ivo://CDS.VizieR/I/42
Title:
Preliminary Cat. of Fund. Faint Stars
Short Name:
I/42
Date:
21 Oct 2021
Publisher:
CDS
Description:
The PFKSZ is based on 14 catalogues, observed at 10 observatories (Bucharest, Wroslaw, Kiev, Goloseevo-GAO, Kazan, GAISH, Odessa, Pulkovo, Tashkent, Kharkov). The catalogue PFKSZ contain 587 stars from 7.3 to 8.4 vis.mag. Most of the catalogues have been obtained from differential meridian observations in the FK3 system. The proper motions were found in the FK3 system mainly from GC, AGK2 (or AGK2A), Yale and PFKSZ catalogues. The precision of PFKSZ catalogue is Mean Error(in Alfa x cos Decl.) = +/- 0.0068 timesec Mean Error(in Decl.) = +/- 0.127 arcsec for the mean epoch 1949.0.
369. Preliminary list from Tycho observations (TIC data)
ID:
ivo://CDS.VizieR/I/207
Title:
Preliminary list from Tycho observations (TIC data)
Short Name:
I/207
Date:
21 Oct 2021
Publisher:
CDS
Description:
The selection of the stars of the Tycho program is mainly based on the Tycho input catalogue (TIC), prepared by Egret et al. (1992) from existing ground-based catalogues. The TIC is far to be the definitive list of the stars that will appear in the final Tycho catalogue however. The number of stars included within (3 million) is several times larger than the number eventually expected. The selection of the TIC stars that will remain in the final catalogue is planned in two steps : The former is the "Recognition" that is based on the first year of the scientific mission. The latter step of selection is the final reduction of the Tycho data, which will require a few more years. The recognition was completed in 1992, and, among the 3,154,204 stars of the TIC, about two third were not found in the observations. This catalogue presents the 1,049,971 stars that are still in the programme. The selection is nor definitive, nor complete; but it should contain only a small percentage of stars that will still be discarded. On another side, some stars missing in the TIC have been added to the Tycho program, but the expected number of additional stars to appear in the final catalogue should be about 5 % or less. The list was announced in Halbwachs et al (1994). It is completed with data (coordinates and magnitudes) from the main file of the Tycho Input Catalogue. The cross-identifications with the Hipparcos Input Catalogue or with the INCA database included in catalogue I/197/ are not repeated here.
370. Proper motion data of M10
ID:
ivo://CDS.VizieR/J/A+AS/145/223
Title:
Proper motion data of M10
Short Name:
J/A+AS/145/223
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the first proper motion study of M10 (NGC 6254). Absolute proper motions of about 532 stars in the field of the globular cluster M10 were determined with respect to Hipparcos and ACT reference stars. In addition to photographic plates of Bonn and Shanghai also wide field CCD observations as second epoch plates were used. The wide field CCD observations show an accuracy comparable to that of the photographic plates. A good coincidence of the solutions based on reference stars from Hipparcos and from ACT was found. Our final proper motions allow a sufficient separation of cluster and field stars. Two population II Cepheids were confirmed to be members of M10. The absolute proper motion of M10 was determined and combined with its distance from the Sun and its radial velocity. The space motion and metallicity of M10 indicates the characteristics of a halo object with an orbit reaching to a maximal z-distance of less than 3kpc.

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