- ID:
- ivo://CDS.VizieR/VI/132B
- Title:
- Lunar Occultation Archive
- Short Name:
- VI/132B
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Lunar occultation timings from 1623 to the present time are brought together in a consistent format. The observations have been processed and reviewed to correct a range of data errors. Provisional reductions of the observations are provided. The reductions are based on the JPL-DE422 and -DE423 ephemerides, with limb corrections derived from satellite altimetry from the Kaguya mission.
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- ID:
- ivo://CDS.VizieR/J/A+AS/110/107
- Title:
- Lunar occultations
- Short Name:
- J/A+AS/110/107
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The results of 114 photoelectric observations are analysed. They were obtained at the two Stations of O.C.A.: Calern and Nice Observatories. We first give a short description of the two photometers used and then we present the interactive reduction method. The astrometric and photometric parameters are derived from each light-curve. Finally we summarize the results and discuss about the non point-like occulted stars: we present 38 double star measurements, for 16 objects, and 11 determinations of angular diameters, for 4 objects.
- ID:
- ivo://CDS.VizieR/J/AJ/112/2786
- Title:
- 1985-1995 lunar occultations at TIRGO
- Short Name:
- J/AJ/112/2786
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A program of observations of lunar occultations in the near-infrared was started at the TIRGO observatory in late 1985. After ten years of operation, we provide a list of all the events recorded up to the end of 1995 using the facility IR photometer. A total of 157 light curves were obtained, mostly aiming at measurements of angular diameters and binaries, with a total of 54 results in these fields. In Table 1 is reported a summary of the occultation events and the parameters of their observations. In Table 2 is reported a list of cross-identifications, coordinates, and characteristics.
- ID:
- ivo://CDS.VizieR/J/A+A/532/A101
- Title:
- Lunar occultations of 184 stellar sources
- Short Name:
- J/A+A/532/A101
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Lunar occultations (LO) provide a unique combination of high angular resolution and sensitivity at near-infrared wavelengths. At the ESO Very Large Telescope, it is possible to achieve about 1 milliarcsecond (mas) resolution and detect sources as faint as K~12mag. We have taken advantage of a passage of the Moon over two crowded and reddened regions in the direction of the inner part of the Galactic bulge to obtain a high number of occultation light curves over two half nights. Our goal was to detect and characterize new binary systems, and to investigate highly extincted and relatively unknown infrared sources in search of circumstellar shells and similar peculiarities. Our target list included a significant number of very late-type stars, but the majority of the sources was without spectral classification.
- ID:
- ivo://CDS.VizieR/J/A+A/493/1171
- Title:
- Mutual phenomena of Galilean satellites PHEMU03
- Short Name:
- J/A+A/493/1171
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In 2003, the Sun and the Earth passed through both the equatorial plane of Jupiter and therefore the orbital planes of its main satellites. During this period, mutual eclipses and occultations were observed and we present the data collected. Light curves of mutual eclipses and occultations were recorded by the observers of the international campaign PHEMU03 organized by the Institut de Mecanique Celeste, Paris, France We completed 377 observations of 118 mutual events from 42 sites and the corresponding data are presented in this paper. For each observation, information about the telescope, receptor, site, and observational conditions are provided. This paper gathers all data and indicates a first estimate of its precision. This catalogue of these rare events should constitute an improved basis for accurate astrometric data useful in the development of dynamical models.
- ID:
- ivo://CDS.VizieR/J/A+AS/125/399
- Title:
- Mutual phenomena of the Galilean satellites
- Short Name:
- J/A+AS/125/399
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this paper, all the light-curves obtained during the PHEMU91 campaign of observations of the mutual phenomena of the Galilean satellites are presented. These observations give accurate astrometric positions of major interest for dynamical studies of the motion of the Galilean satellites. The aim of this work is to give observational data directly usable for theoretical studies. We made 374 observations of 111 mutual events from 56 sites. The accuracy of each observation has been deduced from a comparison with the theoretical predictions. For each observation, information is given about the telescope, the receptor, the site and the observational conditions. Other data as well as the data of the lightcurves themselves are available on the server: ftp://ftp.bdl.fr/pub/NSDC/jupiter/pheno_mut/1991
- ID:
- ivo://CDS.VizieR/J/A+A/437/705
- Title:
- Observations of PHEMU97 and PHEMU03 at Ukkel
- Short Name:
- J/A+A/437/705
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this paper we describe the observations of the mutual phenomena of the Galilean Satellites of Jupiter performed at the Royal Observatory of Belgium, as part of the PHEMU97 and PHEMU03 campaigns. The paper describes the observational technique, the data reduction and summarises the results obtained.
- ID:
- ivo://CDS.VizieR/J/PASP/107/299
- Title:
- Occultation Binaries Catalog
- Short Name:
- J/PASP/107/299
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The observation of lunar occultation phenomena allows for the determination of binary star data which can not always be obtained using classical techniques. No complete catalog has been compiled since that of Evans (1981a) in spite of a 99% increase in the available data. This catalog presents a catalog of photoelectric and occultation measures of binary and multiple systems complete through 1994.
- ID:
- ivo://CDS.VizieR/I/110
- Title:
- Occultation Double-Star Observations
- Short Name:
- I/110
- Date:
- 28 Jan 2022 08:30:21
- Publisher:
- CDS
- Description:
- (no description available)
- ID:
- ivo://CDS.VizieR/B/occ
- Title:
- Occultation lights curves
- Short Name:
- B/occ
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Lunar occultation light curves have been recorded since the mid-20th century using high-speed photomultipliers. Running at high cadence for high angular resolution, such recordings were usually made on large telescopes and limited to the brighter stars - and were not large in number. While a small number of video recordings of lunar and asteroidal occultations were made from about 1980, they became common from about the year 2000, when inexpensive low-light security cameras became available. As of 2016, almost all lunar and asteroidal occultation observations are recorded using video, with the video recording being measured using software packages such as Limovie [http://astro-limovie.info/limovie/limovie_en.html], and Tangra [http://www.hristopavlov.net/Tangra3/]. As a result, light curves are now routinely generated for almost all lunar and asteroidal occultation observations, especially those coordinated through the International Occultation Timing Association and related organisations around the world. This is resulting in large numbers of occultation light curves being obtained each year - albeit with some limitations on time resolution and signal-to-noise ratios. As of 2016, video recordings are mainly made using one or other of the two international video standards - NTSC, or PAL. Both NTSC and PAL use an interlaced video scan, whereby each frame of the video is comprised of two interlaced, time-sequential, fields. The frame rate of an NTSC system is 29.97 frames/sec (59.94 fields/sec), while that for PAL is 25 frames/sec ( 50 fields/sec). Consistent with broadcast television standards, the majority of video cameras used for recording occultations use 8-bit CCD's. However some video recordings are made using progressive scan, 12 to 16-bit digital video systems. For lunar occultations, the temporal resolution is governed by a combination of the frame (or field) rate of the video recording, and the rate of motion of the moon. The typical topocentric motion of the moon is between about 0.3"/sec and 0.4"/sec. The motion of the lunar limb in a direction normal to the star is reduced by the cosine of the difference between the direction of motion of the moon and the position angle of the star. As a result, the typical rate of motion of the lunar limb normal to the star is in the range 0.2 to 0.4 "/sec. At video frame rates this provides a spatial resolution of about 0.01" to 0.02" at frame rate, or 0.005" to 0.01" at field rate. In recent years it has been possible to accurately determine the orientation of the lunar limb at the point of an occultation, using data from the Japanese Kaguya satellite, and more recently the US Lunar Reconnaissance Orbiter - Lunar Orbiter Laser Altimeter (LRO-LOLA). The LRO-LOLA data allows the slope of the lunar limb to be reliably determined over circumferential distances of less than 0.2" in the sky plane. As a result, all data elements required to analyse a lunar occultation light curve are well determined - and are included in this archive. The motion of most asteroids is much less than the moon. As a result, the angular resolution attainable at video frame rate is much smaller than for a lunar occultation, and is commonly in the range 0.0001" to 0.001". However asteroidal occultations frequently involve fainter objects than for lunar occultations, and many observers use integrating video cameras to detect these fainter occultations; the resolution attainable with an integrating camera is reduced in proportion to the number of frames integrated. Unlike lunar occultations, the orientation of the occulting limb of an asteroid relative to the star is generally not well established. Furthermore it can generally be assumed that the limb of an asteroid is likely to have significant irregularities at scales greater than the potential angular resolution attainable, but smaller than the angular distance between adjacent observed occultation chords. There is also the issue of the rotational orientation of the asteroid differing for observers located at different points along the occultation path, placing a limit on the accuracy of the limb slope that can be derived from adjacent occultation chords. Accordingly, at this time the record does not attempt to specify the orientation of the limb of the asteroid at the occultation event.
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