References of "Bouchet, P"
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See detailInfrared aperture photometry at ESO (1983-1994) and its future use.
van der Bliek, N. S.; Manfroid, Jean ULg; Bouchet, P.

in Astronomy and Astrophysics. Supplement Series (1996), 119

We describe the infrared (IR) photometric system for the single channel photometers at ESO, which have been used from 1983 until 1994. In addition to the broadband near infrared (NIR, 1-5μm) photometric ... [more ▼]

We describe the infrared (IR) photometric system for the single channel photometers at ESO, which have been used from 1983 until 1994. In addition to the broadband near infrared (NIR, 1-5μm) photometric system presented in 1991 by Bouchet et al. and Bersanelli et al., we describe a narrow-band NIR photometric system and a mid infrared (MIR, 7-20μm) photometric system. We also extend the set of NIR standard stars by Bouchet et al. towards fainter objects (K=~9). The photometric data of the standard stars in these systems were extracted from the complete IR photometric data archive of ESO, covering 10 years. The zeropoints of the NIR photometry are set by assuming that HR 3314 has a V-magnitude of 3.89, and that V-K=-0.05, J-K=-0.01, H-K=-0.01, K-L'=0.00, K-M=0.00. The zeropoints of the MIR photometry are set by assuming that the colours ofβ Hyi (HR 0098) and α CenA (HR 5459) are equal to the colours of the Sun. We adopt the absolute calibration of Megessier (1995A&A...296..771M) for the NIR and we argue that this calibration can be extrapolated to 20μm, using the MIR calibrations by Rieke et al. (1985AJ.....90..900R) and Cohen et al. (1992AJ....104.1650C). The definition of the zeropoints is consistent with the absolute calibration. We obtained accurate (Ï =~0.02mag.) NIR photometry of about 240 standard stars and MIR photometry of about 40 standard stars (Ï =~0.04mag). Comparison of our NIR photometric system with other well established systems shows that there are some small colour dependencies and zeropoint offsets which are always smaller than about 0.02mag. except for the L' band. [less ▲]

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See detailIR photometry of ESO calibration stars (van der Bliek+ 1996)
van der Bliek, N. S.; Manfroid, Jean ULg; Bouchet, P.

Report (1996)

We describe the infrared (IR) photometric system for the single channel photometers at ESO, which have been used from 1983 until 1994. In addition to the broadband near infrared (NIR, 1-5μm) photometric ... [more ▼]

We describe the infrared (IR) photometric system for the single channel photometers at ESO, which have been used from 1983 until 1994. In addition to the broadband near infrared (NIR, 1-5μm) photometric system presented in 1991 by Bouchet et al. and Bersanelli et al., we describe a narrow-band NIR photometric system and a mid infrared (MIR, 7-20μm) photometric system. We also extend the set of NIR standard stars by Bouchet et al. towards fainter objects (K=~9). The photometric data of the standard stars in these systems were extracted from the complete IR photometric data archive of ESO, covering 10 years. The zeropoints of the NIR photometry are set by assuming that HR 3314 has a V-magnitude of 3.89, and that V-K=-0.05, J-K=-0.01, H-K=-0.01, K-L'=0.00, K-M=0.00. The zeropoints of the MIR photometry are set by assuming that the colours ofβ Hyi (HR 0098) and α CenA (HR 5459) are equal to the colours of the Sun. We adopt the absolute calibration of Megessier (1995A&A...296..771M) for the NIR and we argue that this calibration can be extrapolated to 20μm, using the MIR calibrations by Rieke et al. (1985AJ.....90..900R) and Cohen et al. (1992AJ....104.1650C). The definition of the zeropoints is consistent with the absolute calibration. We obtained accurate (Ï =~0.02mag.) NIR photometry of about 240 standard stars and MIR photometry of about 40 standard stars (Ï =~0.04mag). Comparison of our NIR photometric system with other well established systems shows that there are some small colour dependencies and zeropoint offsets which are always smaller than about 0.02mag. except for the L' band. (3 data files). [less ▲]

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See detailStandard stars for the Infrared Space Observatory, ISO.
van der Bliek, N. S.; Bouchet, P.; Habing, H. J. et al

in The Messenger (1992), 70

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See detailJHKLM standard stars in the ESO system
Bouchet, P.; Schmider, F. X.; Manfroid, Jean ULg

in Astronomy and Astrophysics. Supplement Series (1991), 91

A list of 199 standard stars suitable for the ESO standard photometric system at JHKLM is given. Faint stars (although brighter than K = 7.7) to be used on larger telescopes are included. This list is ... [more ▼]

A list of 199 standard stars suitable for the ESO standard photometric system at JHKLM is given. Faint stars (although brighter than K = 7.7) to be used on larger telescopes are included. This list is based on an analysis of all infrared photometric observations carried out at La Silla from 1979 until 1989 inclusive. The accuracy of the data (about 0.02 mag. at J, H, K, L, and M) is similar to the one achieved at SAAO and CTIO. Comparisons with these systems, as well as with the AAO and MSSO systems, are made: it is shown that the ESO system is very close to the other ones, with the exception of CTIOs. [less ▲]

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See detailPhotometry of comet Austin.
Manfroid, Jean ULg; Bouchet, P.; Gouiffes, C.

in The Messenger (1990), 59

Strömgren photometry of Gomet Austin (1989 c 1) has been obtained at La Silla with the ESO-SAT 50-cm telescope, between February 12 and February 25, 1990. Two diaphragms were selected, 35 arcsec and 240 ... [more ▼]

Strömgren photometry of Gomet Austin (1989 c 1) has been obtained at La Silla with the ESO-SAT 50-cm telescope, between February 12 and February 25, 1990. Two diaphragms were selected, 35 arcsec and 240 arcsec, in an attempt to distinguish between the nucleus and the coma. [less ▲]

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See detailComet Austin (1989c1)
Manfroid, Jean ULg; Gouiffes, C.; Bouchet, P.

Diverse speeche and writing (1990)

IAUC 4971 available at Central Bureau for Astronomical Telegrams.

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See detailComet Austin (1989c1)
Bouchet, P.; West, R. M.; Lebertre, T. et al

in International Astronomical Union Circulars [=IAUCs] (1990), 4962

IAUC 4962 available at Central Bureau for Astronomical Telegrams.

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See detailInfrared photometry and spectrophotometry of SN 1987A. I - March to October 1987 observations
Bouchet, P.; Slezak, E.; Le Bertre, T. et al

in Astronomy and Astrophysics. Supplement Series (1989), 80

IR (1-20 micron) observations, photometry, and narrow band spectrophotometry of SN 1987A obtained between March 16 and October 12, 1987, are presented. Variations of the bolometric luminosity are ... [more ▼]

IR (1-20 micron) observations, photometry, and narrow band spectrophotometry of SN 1987A obtained between March 16 and October 12, 1987, are presented. Variations of the bolometric luminosity are determined from IR and optical photometry. The spectral energy distribution, effective radius, and effective temperature of the hotter component are derived. Also, observations of hydrogen lines and CO emission are discussed. [less ▲]

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See detailHot carbon stars - More about V348 SGR
Houziaux, Léo ULg; Bouchet, P.; Heck, A. et al

in Quarterly Journal of the Royal Astronomical Society (1987), 28

New observational techniques (sensitive receivers, access to ultraviolet and infrared spectroscopy), as well as recent theoretical investigations on advanced stages of stellar evolution focus attention ... [more ▼]

New observational techniques (sensitive receivers, access to ultraviolet and infrared spectroscopy), as well as recent theoretical investigations on advanced stages of stellar evolution focus attention again on hydrogen-poor and helium-rich objects known as "carbon stars". The case of the hot peculiar variable V348 Sgr is discussed. New visible and infrared observations are presented, but the exact nature of the star remains much of an enigma. [less ▲]

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See detailInfrared photometry of SN 1987A - The first four months
Bouchet, P.; Le Bertre, Th; Manfroid, Jean ULg et al

in European Southern Observatory Astrophysics Symposia (1987)

The results of the first 4 mo of the ESO La Silla IR photometric monitoring program of SN 1987A. IR light curves are presented, and the IR data are combined with optical photometry to determine the ... [more ▼]

The results of the first 4 mo of the ESO La Silla IR photometric monitoring program of SN 1987A. IR light curves are presented, and the IR data are combined with optical photometry to determine the luminosity, the effective radius, and the effective temperature, and how they evolved. Particular attention is given to the IR excess which become apparent beginning less than 1 mo after the explosion. Three possible interpretations of the excess IR emission are presented: an IR echo from preexisting dust, thermal emission from dust that has just condensed from the ejecta, and free-free emission from the expanding ejecta. None of the models are entirely satisfactory. [less ▲]

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See detailLow and intermediate resolution IR spectroscopy
Bouchet, P.; Le Bertre, Th; Manfroid, Jean ULg et al

in European Southern Observatory Astrophysics Symposia (1987)

The authors present the results of the first four months of the ESO-La Silla program of IR spectrophotometric monitoring of SN 1987A. The spectra show mainly hydrogen lines with their intensities ... [more ▼]

The authors present the results of the first four months of the ESO-La Silla program of IR spectrophotometric monitoring of SN 1987A. The spectra show mainly hydrogen lines with their intensities increasing with time. The He I 1.083 μm line is also observed with a weak emission component and a strong absorption component. There are also several features whose nature is unclear. [less ▲]

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See detailNew evidence for a ring around Neptune
Manfroid, Jean ULg; Haefner, R.; Bouchet, P.

in Astronomy and Astrophysics (1986), 157

This paper presents an account of observations of the 1984 July 22 appulse of Neptune to SAO 186001. An occultation of 0.8 s duration (FWHM) was detected from La Silla at 05:40:08.6 UTC by two telescopes ... [more ▼]

This paper presents an account of observations of the 1984 July 22 appulse of Neptune to SAO 186001. An occultation of 0.8 s duration (FWHM) was detected from La Silla at 05:40:08.6 UTC by two telescopes operating in I and K bands. This, combined with earlier observations led to the recognition of the existence of an irregular ring around Neptune. [less ▲]

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See detailQu'y a-t-il autour de Neptune?
Manfroid, Jean ULg; Haefner, R.; Bouchet, P.

Article for general public (1986)

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See detailDiscovery of Neptune's ring at La Silla
Haefner, R.; Manfroid, Jean ULg; Bouchet, P.

in The Messenger (1985), 42

The unexpected rediscovery of the Uranian rings in 1977 and the discovery of the faint Jovian rings in 1979 led to an intensified search for rings around Neptune. A description is given of observing ... [more ▼]

The unexpected rediscovery of the Uranian rings in 1977 and the discovery of the faint Jovian rings in 1979 led to an intensified search for rings around Neptune. A description is given of observing programs at the European Southern Observatory (ESO) in Chile, which led to a discovery of such a ring, taking into account the utilization of the ESO 0.5 m and 1 m telescopes. The discovery is based on observations made on the night of July 22, 1984, in connection with a stellar occultation by the planet. Explanations for the observed differences in shape and timing of the occultation event, as recorded by both telescopes, are discussed. The obtained conclusions could be confirmed by a study of the results of a group of American astronomers working at the Cerro Tololo observatory. The observations strongly favor the existence of, at least, a part of a ring which has a width of roughly 10-15 km over a length of at least 100 km. [less ▲]

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See detailOccultation detection of a Neptune ring segment
Hubbard, W. B.; Brahic, A.; Bouchet, P. et al

in Journal of Geophysical Research. Supplement (1985, November 01), 90

A stellar occulation event of Neptune revealed a ring segment that was previously undetected. It appears that the object is not a complete ring, but rather a localized swarm of particles which follows a ... [more ▼]

A stellar occulation event of Neptune revealed a ring segment that was previously undetected. It appears that the object is not a complete ring, but rather a localized swarm of particles which follows a ring orbit over a limited range of longitudes. To avoid confusion with the standard use of the word ring it is suggested that the feature be called an arc. The distance of the arc zone is not precisely known because so far there has been no confirmed occultation by both an arc and the planet. [less ▲]

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See detailOccultation Detection of a Neptune Ring Segment
Hubbard, W. B.; Brahic, A.; Bouchet, P. et al

in Lunar and Planetary Institute Science Conference Abstracts (1985, March 01)

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See detailOccultation detection of a Neptune ring segment
Hubbard, W. B.; Brahic, A.; Bouchet, P. et al

in LPI Contributions (1985), 559

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See detailPossible detection of a 10-kilometer sized object around Neptune.
Roques, F.; Sicardy, B.; Bouchet, P. et al

in Bulletin of the American Astronomical Society (1984, September 01)

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See detailOn the Period of the W UMa System epsilon CrA
Manfroid, Jean ULg; Lunel, M.; Bergeat, J. et al

in Information Bulletin on Variable Stars (1984), 2479

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See detailComet Bradfield (1978c)
Surdej, Jean ULg; Surdej, Anna ULg; Herald, D. et al

in International Astronomical Union Circulars [=IAUCs] (1978), (3185), 1

IAUC 3185 available at Central Bureau for Astronomical Telegrams.

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