CCD observations of Phoebe, 9th satellite of Saturn

Fienga, A.; Arlot, J. E.; Baron, Nicole; Bec-Borsenberger, A.; Crochot, A.; Emelyanov, N. V.; Thuillot, W.

doi:10.1051/0004-6361:20020803

Cited by 12 publications

(13 citation statements)

References 8 publications

(8 reference statements)

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“…Also, indirect measurement is partly responsible for the poor quality since the measuring error of S 1 is incorporated into the position of Phoebe. When compared to recently published CCD observations in Veiga et al (2000) and Fienga et al (2002) as shown in Table 5, the new calibration method allows us to obtain a "clean" and more precise position of Phoebe since our observation is obtained directly from the ACT catalogue. SAT136 in our reduction is the latest ephemeris that has been developed for "CASSINI" and it is thought to be Veiga et al 2000, F+02: Fienga et al 2002 when measured with respect to the theory of Jacobson (1998).…”

Section: Positions Of Phoebe With Respect To Act1 and Comparison Withmentioning

confidence: 99%

“…Veiga et al (2000) and Fienga et al (2002) have published astrometric CCD observations of the 9th satellite of Saturn, Phoebe. It is well known that the astrometric calibration of a CCD image with a small field of view (for example, 5 × 5 ) is difficult.…”

Section: Introductionmentioning

confidence: 99%

“…Veiga et al (2000) and Fienga et al (2002) determined the position of Phoebe by a two-step routine. First, they calibrated the field of view with the USNO A2.0 stars and obtained Phoebe's position with respect to these stars.…”

Section: Introductionmentioning

confidence: 99%

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Precise calibration of CCD images with a small field of view

Peng

Vienne

Han

et al. 2004

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Abstract. A precise astrometric calibration method is presented for a CCD image with a small field of view. Its detailed computational formulae are given, and its feasibility and accuracy are tested by the observations of both the star and Phoebe, the 9th satellite of Saturn. This new method can also be applicable to other planetary satellites, asteroids and optical counterparts of extragalactic radio sources.

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Section: Positions Of Phoebe With Respect To Act1 and Comparison Withmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Precise calibration of CCD images with a small field of view

Peng

Vienne

Han

et al. 2004

A&A

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“…This is due to its extremely faint visual magnitude (about 16.5) and to its great distance from the primary. Recently, Fienga et al (2002) pointed out that the quality of the ephemerides will decrease if no new observations are provided in the near future. The situation gives impetus to scientists to acquire new, high quality astrometric observations of this satellite.…”

Section: Introductionmentioning

confidence: 99%

“…The situation gives impetus to scientists to acquire new, high quality astrometric observations of this satellite. In recent years, several new series of accurate CCD observations of Phoebe have been published by Veiga et al (2000), Fienga et al (2002), andPeng et al (2004). Veiga et al (2000) and Fienga et al (2002) used the very high density USNO A2 star catalogue (Monet et al 1998), while Peng et al (2004 used the high accuracy ACT catalogue (Urban et al 1998) with an overlap reduction.…”

Section: Introductionmentioning

confidence: 99%

CCD astrometric observations of Phoebe in 2003–2004

Qiao

Tang

Shen³

et al. 2006

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In 2003-2004, we obtained 115 new observations of Phoebe, the 9th Saturnian faint satellite (visual magnitude of about 16.5). We used a large CCD detector (2048 × 2048 pixels) mounted on the 1.56 m astrometric reflector at the Sheshan Station, near Shanghai. In our reduction, an up-to-date catalogue of stars, UCAC2 (Zacharias et al. 2004), was chosen to ensure a proper astrometric calibration. A comparison of our observations to three recently available, high quality ephemerides, including the JPL SAT185 by Jacobson (2004b), has shown that most of our observed positions of Phoebe present an accuracy of some tens of mas, which appears to be a very high level for such a faint satellite.

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Phoebe’s orbit from ground-based and space-based observations

Desmars

Tajeddine

et al. 2013

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Context. The ephemeris of Phoebe, the ninth satellite of Saturn, is not very accurate. Previous dynamical models were usually too simplified, the astrometry is heterogeneous and, the Saturn's ephemeris itself is an additionnal source of error. Aims. The aim is to improve Phoebe's ephemeris by using a large set of observations, correcting some systematic errors and updating the dynamical model. Methods. The dynamical model makes use of the most recent ephemeris of planets and Saturnian satellites. The astrometry of Phoebe is improved by using a compilation of ground-based and space-based observations and by correcting the bias in stellar catalogues used for the reduction.Results. We present an accurate ephemeris of Phoebe with residuals of 0.45 arcsec and with an estimated accuracy of Phoebe's position of less that 100 km on 1990-2020 period.

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CCD observations of Phoebe, 9th satellite of Saturn

Cited by 12 publications

References 8 publications

Precise calibration of CCD images with a small field of view

Precise calibration of CCD images with a small field of view

CCD astrometric observations of Phoebe in 2003–2004

Phoebe’s orbit from ground-based and space-based observations

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