No Title

J.-E. Arlot¹ - W. Thuillot¹ - C. Ruatti¹ - A. Ahmad² - A. Amossé⁴⁷ - P. Anbazhagan⁵⁰ - M. Andreyev⁵ - A. Antov¹² - M. Appakutty⁵⁰ - D. Asher² - S. Aubry¹ - N. Baron¹ - N. Bassiere¹ - M. Berthe³ - R. Bogdanovski¹² - F. Bosq²⁵ - E. Bredner⁶ - D. Buettner⁷ - M. Buromsky⁴⁰ - S. Cammarata²⁷ - R. Casas⁸ - G. D. Chis⁹ - A. A. Christou² - J.-P. Coquerel⁴⁴ - R. Corlan¹⁰ - C. Cremaschini¹¹ - D. Crussaire²⁶ - J. Cuypers³² - M. Dennefeld⁴⁶ - P. Descamps¹ - A. Devyatkin²² - D. Dimitrov¹² - T. N. Dorokhova¹³ - N. I. Dorokhov¹³ - G. Dourneau²⁵ - M. Dueñas^14,51 - A. Dumitrescu¹⁰ - N. Emelianov⁴³ - D. Ferrara²⁷ - D. Fiel¹⁵ - A. Fienga¹ - T. Flatres³⁹ - S. Foglia¹¹ - J. Garlitz¹⁶ - J. Gerbos¹⁷ - R. Gilbert¹ - R. M. D. Goncalves¹⁸ - D. Gonzãles^14,51 - S. Yu. Gorda¹⁹ - D. L. Gorshanov²² - M. W. Hansen⁴¹ - M. Harrington² - T. R. Irsmambetova²⁰ - Y. Ito²¹ - V. Ivanova¹² - I. S. Izmailov²² - M. Yu. Khovritchev²² - E. V. Khrutskaya²² - J. Kieken²⁵ - T. P. Kiseleva²² - K. Kuppuswamy⁵⁰ - V. Lainey¹ - M. Lavayssiére²³ - P. Lazzarotti²⁴ - J.-F. Le Campion²⁵ - E. Lellouch²⁶ - Z. L. Li⁴² - E. Lo Savio²⁷ - M. Lou^14,51 - E. Magny⁴⁴ - J. Manek²⁸ - W. Marinello¹¹ - G. Marino²⁷ - J. P. McAuliffe² - M. Michelli¹¹ - D. Moldovan⁹ - S. Montagnac⁴⁴ - V. Moorthy⁵⁰ - O. Nickel²⁹ - J. M. Nier⁴⁴ - T. Noel³⁰ - B. Noyelles^1,3 - A. Oksanen³¹ - D. Parrat⁴⁴ - T. Pauwels³² - Q. Y. Peng³³ - G. Pizzetti¹¹ - V. Priban³⁸ B. Ramachandran² - N. Rambaux^1,25 - M. Rapaport²⁵ - P. Rapavy¹⁷ - G. Rau⁴⁴ - J.-J. Sacré³⁹ - P. V. Sada³⁴ - F. Salvaggio²⁷ - P. Sarlin⁴⁴ - C. Sciuto²⁷ - G. Selvakumar⁵⁰ - A. Sergeyev⁵ - M. Sidorov²² - S. Sorescu¹⁰ - S. A. Spampinato¹¹ - I. Stellmacher¹ - E. Trunkovsky⁴³ - V. Tejfel³⁵ - V. Tudose¹⁰ - V. Turcu⁹ - I. Ugarte² - P. Vantyghem⁴⁵ - R. Vasundhara⁴ - J. Vaubaillon¹ - C. Velu⁵⁰ - A. K. Venkataramana⁵⁰ - J. Vidal-Sãinz^14,51 - A. Vienne^1,3 - J. Vilar³⁶ - P. Vingerhoets⁴⁹ - W. Vollman³⁷

1 - Institut de mécanique céleste et de calcul des éphémérides - Observatoire de Paris, UMR 8028 CNRS, UPMC, USTL, 77 avenue Denfert-Rochereau, 75014 Paris, France
2 - Armagh Observatory, Armagh, Northern Ireland, UK
3 - Observatoire de l'université de Lille, Lille, France
4 - IIA (Indian Institute of Astrophysics), Bangalore, India
5 - Terskol Observatory, Kabardino-Balkaria, Russia
6 - Dolberg, Germany
7 - Chemnitz, Germany
8 - IAC, Tenerife, Spain
9 - Cluj-Napoca, Romania
10 - Institutul Astronomic, Bucuresti, Romania
11 - Observatorio S. Zani, Lumezzane, Italy
12 - Rozhen Observatory, Bulgaria
13 - Astr. Obs. of the Odessa National University, Odessa, Ukraine
14 - Grupo Astronomico Silos, Zaragoza, Spain
15 - Lanester, France
16 - Elgin, Oregon, USA
17 - Rimavska Sobota, Slovakia
18 - Instituto Politecnico Tomar, Tomar, Portugal
19 - Ural State University, Ekaterinbourg, Russia
20 - Crimean Laboratory of the Sternberg Astronomical Institute, Moscow, Russia
21 - Sendai, Japan
22 - Pulkovo Observatory, Saint-Petersburg, Russia
23 - Observatoire de Dax, Dax, France
24 - Massa, Italy
25 - Observatoire de Bordeaux, Floirac, France
26 - Observatoire de Paris, Meudon, France
27 - GAC, Catania, Italy
28 - Czech Astronomical Society, Praha, Czech Rep.
29 - Mainz, Germany
30 - Gieres, France
31 - Nyrola Observatory, Jyvaskylan, Finland
32 - Royal Observatory of Belgium, Brussels, Belgium
33 - Jinan University, Guangzhou, PR China
34 - Universidad de Monterrey, Monterrey, Mexico
35 - Fessenkov Astrophysical Institute, Alma-Ata, Kazakhstan
36 - Mundolsheim, France
37 - Vienna, Austria
38 - Observatory and Planetarium Praha, Czech Rep.
39 - Thorigné, France
40 - Kiev National University, Kiev, Ukraine
41 - Institutt for Teorerisk Astrofysikk, Oslo, Norway
42 - Yunnan Observatory, Kunming, PR China
43 - Sternberg Astronomical Institute, Lomonosov Moscow State University, Russia
44 - C2AHP, Saint-Michel l'observatoire, France
45 - Pierrevert, France
46 - IAP, Paris, France
47 - Forum des sciences, Villeneuve d'Ascq, Lille, France
48 - Bucuresti, Romania
49 - Flemish association of amateur astronomers, Groenstraat 12, Mortsel, Belgium
50 - IIA (Indian Institute of Astrophysics), VBO, Kavalur, India
51 - Grup d'Estudis Astronòmics, Barcelona, Spain

Abstract
Context. In 2003, the Sun and the Earth passed through both the equatorial plane of Jupiter and therefore the orbital planes of its main satellites.
Aims. During this period, mutual eclipses and occultations were observed and we present the data collected.
Methods. Light curves of mutual eclipses and occultations were recorded by the observers of the international campaign PHEMU03 organized by the Institut de mécanique céleste, Paris, France.
Results. 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.
Conclusions. 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.

Key words: astrometry - eclipses - occultations - planets and satellites: individual: Jupiter

1 Introduction

Observations of natural satellite mutual events have been performed intensively since 1973 and have proved to be a very accurate way to get astrometric measurements of the natural satellites. In 2003, we encouraged observers to complete as many observations as possible by organizing and coordinating an international campaign to monitor these rare events. This campaign named PHEMU03 allowed us to collect 377 light curves of 118 mutual events studied by the observers of our international network consisting of 42 sites.

In this paper, we provide all data collected by our network. We note that 19 more observations were completed (at Meudon, Pulkovo, Armagh, Nauchny, Novara, Sendai, Terskol, and Sobota), but due to adverse meteorological conditions or hardware problems, no reliable information could be derived from the light curves, which are not included in this paper. Another paper (Emelianov 2008) will provide the astrometric data extracted from the light curves by a sophisticated photometric model of the light curves. In this paper, we aim to provide the photometric data and observational parameters useful to future work on the improvement of dynamical models and models of satellite surfaces. These data are available through the data center NSDC dedicated to the natural satellites.

2 The mutual events

The Earth and the Sun traverse the equatorial plane of Jupiter every six years. The Jovian declinations of the Earth and the Sun then become zero and, since the orbital plane of the Galilean satellites is close to the equatorial plane of Jupiter, the satellites occult and eclipse each other.

The 2003 period was particularly favorable because the equatorial plane crossing occurred during the opposition of Jupiter and the Sun.

Arlot (2002) compiled predictions of all 2003 events using the G5 ephemerides based upon Lieske's theory (Lieske 1977) and the newer L1 ephemerides from Lainey et al. (2004a,b) for the motion of the Galilean satellites. 581 mutual events were computed. Before 2003, several observational campaigns were completed during previous occurrences (Arlot et al. 1997, 2006). Table 1 presents the results derived for each campaign until the present one. Our goal was to observe as many events as possible. Two observations of each event were at least desirable to eliminate any biases in the present observations.

Since no thick atmosphere surrounds any of the Galilean satellites, the photometric observations of these phenomena are extremely accurate for astrometric purposes. The results previously obtained after similar observations of the Galilean satellites, demonstrated that high astrometric accuracy could be achieved: an accuracy of higher than 30 mas was expected (Lainey et al. 2004).

This fact allows us to provide data necessary to improve the theoretical models of the orbital motions and determine the tidal effects in the dynamics of the Galilean satellites.

3 The PHEMU03 campaign

We coordinated an international PHEMU03 campaign to acquire a significant amount of events. These events occur in a short period of time, so numerous observers located in several sites were necessary to both help avoid meteorological problems and observe different events from different longitudes. This is why observers previously involved in PHEMU observational campaigns of mutual events of the Galilean satellites were invited to join the new campaign.

3.1 Receptors

When observing mutual events, only relative photometry can generally be completed. Since the elevation of Jupiter above the horizon may be small, the air mass is often too high and absolute photometry is then impossible. Telescopes were equipped with the receptors listed in Table 2. Three kinds of receptors were used, the photoelectric photometric single channel receptors, the video cameras, and the two-dimensional CCD receptors. Visual observations are reported only for comparison. The code for the receptors are those provided in the tables for each observation.

3.2 Sites of observation

Coordinated by the IMCCE, this campaign involved the different locations given in Table 3. This table gives the names, longitudes, latitudes, and elevations of the observational sites and the telescopes used (L means refractor and T means reflector, followed by the aperture in cm).

4 Lightcurves reduction procedure

Light curves were deduced from photometric measurements either with relative photometry performed with photoelectric photometers or with CCD cameras.

For observations completed with CCD cameras in video mode, the signal was digitized with digitizing boards. The light curves were also obtained for most of them by aperture photometry. For video observations completed in Meudon or OHP, images were analyzed by completing Gaussian photometry with the AVIA software package (Arlot et al. 1989). Two dimensional measurements generally allow us to calibrate the signal from a particular satellite to that from a nearby satellite and eventually to acquire data under difficult conditions (see for example Arlot & Stavinschi 2007).

The determination of both the time of minimum light and the extent of the magnitude drop were based on a fit to the light curve of a sample polynomial. The errors in these determinations are also given. The error in the timing of the minimum is determinated as follows: we calculate the noise in magnitudes and transform it into an error time through the highest value of the speed of decreasing in magnitude during the event. The largest errors occur during the faint noisy events and the smallest for the most rapid. The errors remains comparable only if the integration times are the same.

$\begin{figure} \par\includegraphics*[scale=0.5,clip=]{zfich10.ps} \end{figure}$	Figure 1: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich11.ps} \end{figure}$	Figure 2: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich12.ps} \end{figure}$	Figure 3: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.49,clip=]{zfich13.ps} \end{figure}$	Figure 4: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.49,clip=]{zfich14.ps}\par \end{figure}$	Figure 5: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich15.ps}\par \end{figure}$	Figure 6: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich16.ps}\par \end{figure}$	Figure 7: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich17.ps}\par \end{figure}$	Figure 8: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich18.ps}\par \end{figure}$	Figure 9: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich19.ps}\par \end{figure}$	Figure 10: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich20.ps}\par \end{figure}$	Figure 11: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich21.ps}\par \end{figure}$	Figure 12: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich22.ps}\par \end{figure}$	Figure 13: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich23.ps}\par \end{figure}$	Figure 14: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich24.ps}\par \end{figure}$	Figure 15: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich25.ps} \end{figure}$	Figure 16: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich26.ps}\par \end{figure}$	Figure 17: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich27.ps}\par \end{figure}$	Figure 18: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich28.ps}\par \end{figure}$	Figure 19: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich29.ps}\par \end{figure}$	Figure 20: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich30.ps}\par \end{figure}$	Figure 21: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich31.ps}\par \end{figure}$	Figure 22: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich32.ps}\par \end{figure}$	Figure 23: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich33.ps}\par \end{figure}$	Figure 24: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich34.ps} \end{figure}$	Figure 25: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich35.ps}\par \end{figure}$	Figure 26: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich36.ps}\par \end{figure}$	Figure 27: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich37.ps}\par \end{figure}$	Figure 28: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich38.ps}\par \end{figure}$	Figure 29: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich39.ps}\par \par\end{figure}$	Figure 30: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich40.ps}\par \par\end{figure}$	Figure 31: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich41.ps}\par \par\end{figure}$	Figure 32: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich42.ps}\par \par\end{figure}$	Figure 33: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich43.ps}\par \par\end{figure}$	Figure 34: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich44.ps}\par \par\end{figure}$	Figure 35: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich45.ps}\par \par\end{figure}$	Figure 36: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich46.ps}\par \par\end{figure}$	Figure 37: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich47.ps}\par \par\end{figure}$	Figure 38: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich48.ps}\par \par\end{figure}$	Figure 39: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure}\par\includegraphics*[scale=0.5,clip=]{zfich49.ps}\par \par\end{figure}$	Figure 40: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure} \par\includegraphics*[scale=0.5,clip=]{zfich50.ps}\par \par\end{figure}$	Figure 41: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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$\begin{figure} \par\includegraphics*[scale=0.5,clip=]{zfich51.ps}\par \par\end{figure}$	Figure 42: Light curves for the observations of the mutual events of the Galilean satellites in 2002-2003.
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5 The catalogue

5.1 The data

In Table 4, we present the following data for each observed event, where all dates are in UTC:

These data and light-curves are available for anyone interested from the electronic database of the Natural Satellite Data Center (NSDC) server on the WEB server.

5.2 Discussion

This catalogue intends to provide observational information and reduced data from the PHEMU03 campaign. Another paper (Emelianov 2008) will provide the astrometric data extracted from the light curves.

The quality of each light curve may be assessed either by the errors in the determined parameters (times of both the minimum of light and magnitude drop) or by the appearance of the light curve itself.

As in the previous catalogues of such events, we computed the errors in the determined parameters as follows. The error in the light flux drop was determined from the standard deviation of the fit to the model light curve. The error in the date of the minimum is deduced from the error in the magnitude drop combined with the speed of the decrease in the light flux during the event. This explains why this error depends on the number of points, the integrating time, and the depth of the light curve. Because of this, error bars can only be compared for events observed with the same time constants and, preferably, with the same equipment to be able to derive a reliable an observational error and measurement of the quality of the observation.

6 Conclusion

We have presented the results of the PHEMU03 campaign. This catalogue presents the results obtained by all participants of the campaign who obtained significant results. To be able to observe the maximum possible number of events, it was necessary to organize an international campaign. These phenomena occur every 6 years and can enable accurate astrometric measurements to be completed which are difficult to achieve with other ground-based techniques. Furthermore, they may allow us to determine surface parameters by comparison between light curves and synthetic models. Our experience has demonstrated that past campaigns provided catalogues of data invaluable for astrometric purposes. Accurate astrometric data were deduced from the published observations and used for dynamical purposes. Compared with other types of observations, it is clear that mutual event data have the smallest residuals in the astrometric measurements derived (Lainey et al. 2004).

The PHEMU03 catalogue of observations of the mutual phenomena of the Galilean satellites of Jupiter