Jovian satellite positions from Hubble Space Telescope images

Mallama, Anthony; Aelion, H. M.; Mallama, Celeste A.

doi:10.1016/j.icarus.2003.10.011

Cited by 15 publications

(16 citation statements)

References 28 publications

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“…This technique allowed us to measure the position of Jupiter as precisely as 0.03 arcsec (internal precision). Mallama, Aelion & Mallama (2004) confirmed the accuracy of this edge‐detection (or limb‐fitting) technique using observations with the Hubble Space Telescope . Here, we should distinguish between internal precision and external accuracy.…”

Section: Introductionsupporting

confidence: 56%

“…They chose 12 points around the edge of the rings of Saturn. The space observations were derived from the CCD imaging obtained in 1995–1996 by PC/WF chips of the Hubble Space Telescope (see also Mallama et al 2004). One sees that the present method from a CCD ground‐based telescope might be comparable to the HST , WF chip method.…”

Section: Calibration Of Ccd Images and Resultsmentioning

confidence: 99%

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New confirmation of image-processing techniques for astrometry of Saturn and its satellites

Peng

2005

Monthly Notices of the Royal Astronomical Society

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The image‐processing techniques used by Peng et al. are further improved to measure precisely the positions of Saturn and its satellites. 495 CCD images taken with the 1‐m telescope at the Yunnan Observatory during the years 2002–2004 are processed with these techniques. These measured pixel positions are compared to their theoretical positions computed with the ephemerides of TASS1.7 for the satellites and JPL DE405 for Saturn itself. Analysis of the data for the intersatellite positions among four bright Saturnian satellites (S3–S6) and for Saturn–satellite (i.e. Saturn–Titan) positions shows that these measured positions have the same dispersions, i.e. about 0.05 and 0.06 arcsec in right ascension and declination, respectively. However, for the fainter satellites, Enceladus and Mimas, poorer residuals up to 0.1 and 0.2 arcsec, respectively, in both directions are found mainly due to their small separations from the primary planet and short exposure time in order to obtain useful images of Saturn.

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Section: Introductionsupporting

confidence: 56%

Section: Calibration Of Ccd Images and Resultsmentioning

confidence: 99%

New confirmation of image-processing techniques for astrometry of Saturn and its satellites

Peng

2005

Monthly Notices of the Royal Astronomical Society

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“…2 we introduce our new astrometric reduction model, based on an approach more generally used for ground-based observations, and compare it to the Cassini ISS model proposed by Owen (2003). In the same section, we describe our satellite limb-measuring technique, inspired by Mallama et al (2004), and our method for fitting an elliptical model of the satellite's shape to the measured limb. We also evaluate the importance of image distortion in limb-fitting.…”

Section: Introductionmentioning

confidence: 99%

Astrometric reduction ofCassiniISS images of the Saturnian satellites Mimas and Enceladus

Tajeddine¹,

Cooper²,

Lainey³

et al. 2013

A&A

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Aims. We provide astrometric observations of two of Saturn's main satellites, Mimas and Enceladus, using high resolution Cassini ISS Narrow Angle Camera images. Methods. We developed a simplified astrometric reduction model for Cassini ISS images as an alternative to the one proposed by the Jet Propulsion Labratory (JPL). The particular advantage of the new model is that it is easily invertible, with only marginal loss in accuracy. We also describe our new limb detection and fitting technique. Results. We provide a total of 1790 Cassini-centred astrometric observations of Mimas and Enceladus, in right ascension (α) and declination (δ) in the International Celestial Reference Frame (ICRF). Mean residuals compared to JPL ephemerides SAT317 and SAT351 of about one kilometre for Mimas and few hundreds of metres for Enceladus were obtained, in α cos δ and δ, with a standard deviation of a few kilometres for both satellites. A frequency analysis of the residuals revealed some periodic variability in the right ascension for Mimas. An additional analysis of Mimas' mean longitude suggests that some short-period terms are missing in the TASS orbital model.

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“…The CALSPEC stars are being used by the DES as a portion of their calibration process and help form the basis of the Pan-STARRS1 photometry system (Tonry et al 2012). They continue to find use in comparing observations to models and simulations such as the work by Mallama (2015) to investigate the Sloan Digital Sky Survey (SDSS) magnitude system.…”

Section: Nist To the Sky (Ja Smith)mentioning

confidence: 99%

Division B Commission 25: Astronomical Photometry and Polarimetry

Walker¹,

Adelman²,

Milone³

et al. 2015

Proc. IAU

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Commission 25 (C25) deals with the techniques and issues involved with the measurement of optical and infrared radiation intensities and polarization from astronomical sources. As such, in recent years attention has focused on photometric standard stars, atmospheric extinction, photometric passbands, transformation between systems, nomenclature, and observing and reduction techniques. At the start of the trimester C25 changed its name from Stellar Photometry and Polarization to Astronomical Photometry and Polarization so as to explicitly include in its mandate particular issues arising from the measurement of resolved sources, given the importance of photometric redshifts of distant galaxies for many of the large photometric surveys now underway. We begin by summarizing commission activities over the 2012-2014 period, follow with a report on Polarimetry, continue with Photometry topics that have been of interest to C25 members, and conclude with a Vision for the Future.

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Jovian satellite positions from Hubble Space Telescope images

Cited by 15 publications

References 28 publications

New confirmation of image-processing techniques for astrometry of Saturn and its satellites

New confirmation of image-processing techniques for astrometry of Saturn and its satellites

Astrometric reduction ofCassiniISS images of the Saturnian satellites Mimas and Enceladus

Division B Commission 25: Astronomical Photometry and Polarimetry

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