. Alain Badiou, Court traité d’ontologie transitoire , Paris, Seuil, (coll. « L’ordre philosophique »), 1998, 199 p., Petit manuel d’inesthétique , Paris, Seuil, ( coll. « L’ordre philosophique »), 1998, 214 p. et Abrégé de métapolitique , Paris, Seuil, (coll. « L’ordre philosophique »), 1998, 166 p.

Beaulieu, Alain

doi:10.7202/004897ar

Cited by 6 publications

(6 citation statements)

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“…The EROS collaboration: Observation of periodic variable stars Beaulieu et al 1995;Beaulieu & Sasselov 1996). We use the empirical function R cut 21 (P ) = 0.4 − (P/30 days) in order to separate these pulsation modes (see Fig.…”

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confidence: 99%

Observation of periodic variable stars towards the Galactic spiral arms by EROS II

Derue

Marquette

Lupone

et al. 2002

A&A

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Abstract. We present the results of a massive variability search based on a photometric survey of a six square degree region along the Galactic plane at (l = 305. This survey was performed in the framework of the EROS II (Expérience de Recherche d'Objets Sombres) microlensing program. The variable stars were found among 1 913 576 stars that were monitored between April and June 1998 in two passbands, with an average of 60 measurements. A new period-search technique is proposed which makes use of a statistical variable that characterizes the overall regularity of the flux versus phase diagram. This method is well suited when the photometric data are unevenly distributed in time, as is our case. 1362 objects whose luminosity varies were selected. Among them we identified 9 Cepheids, 19 RR Lyrae, 34 Miras, 176 eclipsing binaries and 266 Semi-Regular stars. Most of them are newly identified objects. The cross-identification with known catalogues has been performed. The mean distance of the RR Lyrae is estimated to be ∼4.9 ± 0.3 kpc undergoing an average absorption of ∼3.4 ± 0.2 mag. This distance is in good agreement with that of disc stars that contribute to the microlensing source star population. Our catalogue and light curves are available electronically from the CDS, Strasbourg and from our Web site * * .

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confidence: 99%

Observation of periodic variable stars towards the Galactic spiral arms by EROS II

Derue

Marquette

Lupone

et al. 2002

A&A

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“…During the "EROS" era, we have built catalogues of variable stars in the LMC and in the SMC using the CCD data from the 1991-1994 campaign. A differential study of about 550 Cepheids from the LMC and SMC has been conducted to derive constraints on stellar pulsation theory (position of resonance centers, and beat Cepheids) and to find a subtle metallicity effect on the P-L relation (Beaulieu et al 1995, 1997a, 1997b.…”

Section: The Cepheid Cataloguesmentioning

confidence: 99%

“…The Cepheid candidates were extracted using selection criteria in the color-magnitude plane and the period-luminosity plane. Using the Fourier coefficients determined above, it was possible to distinguish between classical Cepheids pulsating in fundamental mode (F), and s-Cepheids pulsating in a first overtone mode (10T) as done in Beaulieu et al (1995) following the suggestion of Antonello et al (1986). Finally, a visual inspection of the selected Cepheid candidate light curves was undertaken in order to remove the clearly non-Cepheid variables and stars with a low signal to noise ratio, and to check for the F or 10T…”

Section: The Cepheid Cataloguesmentioning

confidence: 99%

Cepheids from the EROS-2 Microlensing Survey

Beaulieu

Marquette

2000

International Astronomical Union Colloquium

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Using observations obtained in the pilot campaign of the EROS-2 microlensing survey we observed 290 Cepheids towards the LMC and 590 Cepheids towards the SMC. We present the constraints they give to stellar pulsation theory. We detect a statistically significant break in the slope of the period-luminosity relation for SMC fundamental mode Cepheids with periods shorter than 2 d and discuss its origin.

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“…We will give a short report of the results on variable stars by EROS. A differential study of about 550 Cepheids from LMC and SMC have been conducted, to derive constraints on stellar pulsation theory (position of resonance centers, and beat Cepheids) and to find a subtle metallicity effect on the Period Luminosity relation , 1997a, 1997b. A larger sample of Cepheids from LMC and SMC has been observed as a pilot project of the EROS-2 survey (Bauer et al, 1998, Marquette, Graff, Ripepi et al, this volume).…”

Section: Pulsating Variables Nova Eclipsing Binariesmentioning

confidence: 99%

Results from the EROS Microlensing Survey

Beaulieu¹,

Lamers²,

Wit³

1999

Symp. - Int. Astron. Union

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Abstract. We will present a status report of the EROS and the on going EROS-2 microlensing surveys to search for dark matter in the Galactic halo via microlensing effects on LMC/SMC stars. Microlensing surveys provide systematic observations for millions of stars over a long period in both Magellanic Clouds and give birth to very powerful database. We will quickly review the results obtained on pulsating stars and we will detail the similarity and differences of the Herbig Ae/Be stars in the Magellanic Clouds compared to their Galactic counterpart. Observations made by the EROS microlensing surveyEROS (Expérience de Recherche d'Objets Sombres) is a French collaboration between astronomers and particle physicists to search for baryonic dark matter in the Galactic Halo by microlensing ( Paczyǹski, 1986) on stars of the Magellanic Clouds (MCs). A compact object in the Galactic Halo passing close enough to the line of sight to a background star in the Magellanic Clouds induces an increase in the apparent brightness of the star. This phenomenon occurs owing to the alignment of the observer, the deflector and the background star. Assuming a standard corotating halo the time scale τ 0 of a microlensing event is given by the relation τ 0 = 70 M/M days where M is the mass of the deflector. In order to be sensitive to a wide range of mass for compact objects (10 −7 − 10 −1 M ) two complementary approaches have been developed.The first involved photographic monitoring of 6.4 million stars over a 5 × 5 degree field using the ESO Schmidt telescope from 1990 to 1994. About 380 plates were taken once a night if possible in two colours B J and R C . Isolated stars can be found down to magnitude 20 with typical photometric uncertainties of 0.3 mag.The second approach was to be sensitive to low mass compact objects. Between 1991 and 1994 about 15000 CCD images were taken with two broad bandpass filters B E and R E of an area of 1 x 0.4 degrees centered on the bar of the LMC. Another field of 1 x 0.4 degrees had been chosen in the SMC between 1993-1995 and about 6000 images where taken. Lightcurves of 270 000 stars exist with up to 48 points per night ! 1

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Cited by 6 publications

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Observation of periodic variable stars towards the Galactic spiral arms by EROS II

Observation of periodic variable stars towards the Galactic spiral arms by EROS II

Cepheids from the EROS-2 Microlensing Survey

Results from the EROS Microlensing Survey

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