Browsing
     by title


0-9 A B C D E F G H I J K L M N O P Q R S T U V W X Y Z

or enter first few letters:   
OK
Full Text
Peer Reviewed
See detailLes offrandes liées à la fécondité et à la maternité dans la Gaule romaine
Nissen, Cécile ULg

in Revue du Praticien (La) (2006), 56(7), 804-9

Detailed reference viewed: 23 (2 ULg)
See detailOffre foncière et demande pour les activités économiques en 2015
Halleux, Jean-Marie ULg; Kessler, L.; Klinkenberg, A.-C. et al

Conference (2002, November 14)

Detailed reference viewed: 3 (0 ULg)
Full Text
Peer Reviewed
See detailOGLE 2008-BLG-290: an accurate measurement of the limb darkening of a galactic bulge K Giant spatially resolved by microlensing
Fouqué, P.; Heyrovský, D.; Dong, S. et al

in Astronomy and Astrophysics (2010), 518

Context. Not only is gravitational microlensing a successful tool for discovering distant exoplanets, but it also enables characterization of the lens and source stars involved in the lensing event. <BR ... [more ▼]

Context. Not only is gravitational microlensing a successful tool for discovering distant exoplanets, but it also enables characterization of the lens and source stars involved in the lensing event. <BR /> Aims: In high-magnification events, the lens caustic may cross over the source disk, which allows determination of the angular size of the source and measurement of its limb darkening. <BR /> Methods: When such extended-source effects appear close to maximum magnification, the resulting light curve differs from the characteristic Paczyński point-source curve. The exact shape of the light curve close to the peak depends on the limb darkening of the source. Dense photometric coverage permits measurement of the respective limb-darkening coefficients. <BR /> Results: In the case of the microlensing event OGLE 2008-BLG-290, the K giant source star reached a peak magnification at about 100. Thirteen different telescopes have covered this event in eight different photometric bands. Subsequent light-curve analysis yielded measurements of linear limb-darkening coefficients of the source in six photometric bands. The best-measured coefficients lead to an estimate of the source effective temperature of about 4700[SUP]+100[/SUP][SUB]-200[/SUB] K. However, the photometric estimate from colour-magnitude diagrams favours a cooler temperature of 4200 ± 100 K. <BR /> Conclusions: Because the limb-darkening measurements, at least in the CTIO/SMARTS2 V_s- and I_s-bands, are among the most accurate obtained, the above disagreement needs to be understood. A solution is proposed, which may apply to previous events where such a discrepancy also appeared. [less ▲]

Detailed reference viewed: 42 (5 ULg)
Full Text
Peer Reviewed
See detailOGLE-2008-BLG-510: first automated real-time detection of a weak microlensing anomaly - brown dwarf or stellar binary?
Bozza, V.; Dominik, M.; Rattenbury, N. J. et al

in Monthly Notices of the Royal Astronomical Society (2012), 424

The microlensing event OGLE-2008-BLG-510 is characterized by an evident asymmetric shape of the peak, promptly detected by the Automated Robotic Terrestrial Exoplanet Microlensing Search (ARTEMiS) system ... [more ▼]

The microlensing event OGLE-2008-BLG-510 is characterized by an evident asymmetric shape of the peak, promptly detected by the Automated Robotic Terrestrial Exoplanet Microlensing Search (ARTEMiS) system in real time. The skewness of the light curve appears to be compatible both with binary-lens and binary-source models, including the possibility that the lens system consists of an M dwarf orbited by a brown dwarf. The detection of this microlensing anomaly and our analysis demonstrate that: (1) automated real-time detection of weak microlensing anomalies with immediate feedback is feasible, efficient and sensitive, (2) rather common weak features intrinsically come with ambiguities that are not easily resolved from photometric light curves, (3) a modelling approach that finds all features of parameter space rather than just the 'favourite model' is required and (4) the data quality is most crucial, where systematics can be confused with real features, in particular small higher order effects such as orbital motion signatures. It moreover becomes apparent that events with weak signatures are a silver mine for statistical studies, although not easy to exploit. Clues about the apparent paucity of both brown-dwarf companions and binary-source microlensing events might hide here. Based in part on data collected by MiNDSTEp with the Danish 1.54m telescope at the ESO La Silla Observatory. [less ▲]

Detailed reference viewed: 24 (3 ULg)
Peer Reviewed
See detailOGLE-2009-BLG-092/MOA-2009-BLG-137: A Dramatic Repeating Event with the Second Perturbation Predicted by Real-time Analysis
Ryu, Y*-H; Han, C.; Hwang, K*-H et al

in Astrophysical Journal (2010), 723(1), 81-88

We report the result of the analysis of a dramatic repeating gravitational microlensing event OGLE-2009-BLG-092/MOA-2009-BLG-137, for which the light curve is characterized by two distinct peaks with ... [more ▼]

We report the result of the analysis of a dramatic repeating gravitational microlensing event OGLE-2009-BLG-092/MOA-2009-BLG-137, for which the light curve is characterized by two distinct peaks with perturbations near both peaks. We find that the event is produced by the passage of the source trajectory over the central perturbation regions associated with the individual components of a wide-separation binary. The event is special in the sense that the second perturbation, occurring ~100 days after the first, was predicted by the real-time analysis conducted after the first peak, demonstrating that real-time modeling can be routinely done for binary and planetary events. With the data obtained from follow-up observations covering the second peak, we are able to uniquely determine the physical parameters of the lens system. We find that the event occurred on a bulge clump giant and it was produced by a binary lens composed of a K- and M-type main-sequence stars. The estimated masses of the binary components are M [SUB]1[/SUB] = 0.69 ± 0.11 M [SUB]sun[/SUB] and M [SUB]2[/SUB] = 0.36 ± 0.06 M [SUB]sun[/SUB], respectively, and they are separated in projection by r [SUB]bottom[/SUB] = 10.9 ± 1.3 AU. The measured distance to the lens is D [SUB]L[/SUB] = 5.6 ± 0.7 kpc. We also detect the orbital motion of the lens system. [less ▲]

Detailed reference viewed: 42 (8 ULg)
Full Text
Peer Reviewed
See detailOGLE-TR-211 - a new transiting inflated hot Jupiter from the OGLE survey and ESO LP666 spectroscopic follow-up program
Udalski, A.; Pont, F.; Naef, D. et al

in Astronomy and Astrophysics (2008), 482

We present results of the photometric campaign for planetary and low-luminosity object transits conducted by the OGLE survey in the 2005 season (Campaign #5). About twenty of the most promising candidates ... [more ▼]

We present results of the photometric campaign for planetary and low-luminosity object transits conducted by the OGLE survey in the 2005 season (Campaign #5). About twenty of the most promising candidates discovered in these data were subsequently verified spectroscopically with the VLT/FLAMES spectrograph. One of the candidates, OGLE-TR-211, reveals clear changes of radial velocity with a small amplitude of 82 m/s, varying in phase with photometric transit ephemeris. Further analysis confirms the planetary nature of this system. Follow-up precise photometry of OGLE-TR-211 with VLT/FORS, together with radial velocity spectroscopy, supplemented with high-resolution, high S/N VLT/UVES spectra allowed us to derive parameters of the planet and host star. OGLE-TR-211b is a hot Jupiter orbiting an F7-8 spectral type dwarf star with a period of 3.68 days. The mass of the planet is equal to 1.03±0.20 M_Jup, while its radius 1.36[SUP]+0.18[/SUP][SUB]-0.09[/SUB] R_Jup. The radius is about 20% larger than the typical radius of hot Jupiters of similar mass. OGLE-TR-211b is, then, another example of inflated hot Jupiters - a small group of seven exoplanets with large radii and unusually low densities - objects that are a challenge to the current models of exoplanets. Based on observations made with the FORS1 camera and the FLAMES/UVES spectrograph at the VLT, ESO, Chile (program 07.C-0706, 076.C-0122, and 177.C-0666) and 1.3-m Warsaw Telescope at Las Campanas Observatory, Chile. [less ▲]

Detailed reference viewed: 42 (2 ULg)
Full Text
See detailOgling Jhumpa Lahiri at Southbank
Munos, Delphine ULg

Article for general public (2013)

Detailed reference viewed: 27 (2 ULg)
See detailLes OGM sous l'angle économique
Burny, Philippe ULg

Conference given outside the academic context (2003)

Detailed reference viewed: 4 (0 ULg)
Peer Reviewed
See detailOGO-4 observations of the ultraviolet auroral spectrum
Gérard, Jean-Claude ULg; Barth, C. A.

in Planetary and Space Science (1976), 24

Auroral ultraviolet spectra in the range from 1200 to 3200 A have been obtained by the spectrometer on board the OGO-4 satellite. Emissions of N2, H, O, and N are readily identified. Atomic and molecular ... [more ▼]

Auroral ultraviolet spectra in the range from 1200 to 3200 A have been obtained by the spectrometer on board the OGO-4 satellite. Emissions of N2, H, O, and N are readily identified. Atomic and molecular intensities are deduced from the comparison with a synthetic spectrum and compare reasonably well with some previous measurements and calculations. A feature at 2150 A is assigned to the (1-0) NO gamma band. Taking into consideration the various excitation mechanisms of NO(A2 Sigma), it is proposed that energy transfer from N2 metastable molecules to oxygen accounts for the excitation of the NO gamma bands. In particular, it is suggested that the resonant reaction between O2 and highly metastable N2 molecules may be a major source of NO(A2 Sigma). [less ▲]

Detailed reference viewed: 12 (0 ULg)
Peer Reviewed
See detailThe OH Venus nightglow : morphology and relation to ozone in the upper atmosphere
Soret, Lauriane ULg; Gérard, Jean-Claude ULg; Piccioni, G. et al

Conference (2011, October)

Detailed reference viewed: 13 (5 ULg)
Full Text
Peer Reviewed
See detailThe OH Venus nightglow spectrum: intensity and vibrational composition from VIRTIS-Venus Express observations
Soret, Lauriane ULg; Gérard, Jean-Claude ULg; Piccioni, Giuseppe et al

in Planetary and Space Science (2012), 73(1),

Limb spectra of the OH nightglow emission corresponding to the ∆v=1 and ∆v=2 sequences have been collected with the VIRTIS infrared imaging spectrograph on board Venus Express between April 2006 and ... [more ▼]

Limb spectra of the OH nightglow emission corresponding to the ∆v=1 and ∆v=2 sequences have been collected with the VIRTIS infrared imaging spectrograph on board Venus Express between April 2006 and October 2008. A detailed statistical analysis shows that the peak intensity and altitude of the two vibrational sequences are significantly correlated, with a mean intensity ratio of the two sequences of 0.38±0.37. The altitude of the maximum of the ∆v=2 emission is located ~1 km lower than ∆v=1. A spectral analysis shows that the Δv=1 sequence is composed at 44.6% by the (1–0) band, 9.3% by the (3–2) band and 7.1% by the (4–3) band. The Δv=2 emission is best fitted if solely including the (2–0) band. A non-LTE model of OH vibrational population by the O3+H reaction including radiative and collisional relaxation has been used to compare the expected spectral distribution, the altitude of the emission peak and the emission rate under different assumptions on the quenching processes to those observed with VIRTIS. The adopted carbon dioxide, atomic oxygen and ozone densities are based on recent Venus Express remote sensing measurements. We find that the “sudden death” quenching scheme by CO2 produces inadequate spectral distribution between the various bands and insufficient airglow brightness. Instead, the observed spectral distribution and the total emission intensity are reasonably well reproduced with the single quantum jump model, a O density profile peaking at 103.5 km with a maximum value of 1.9×1011 cm−3, a O3 density profile peaking at 5.8×106 cm−3 at 96.5 km and a H density profile close to 108 cm−3 between 90 and 120 km, in agreement with several photochemical models. [less ▲]

Detailed reference viewed: 17 (2 ULg)
Full Text
See detail"Oh wow. Oh wow. Oh wow."
Choffray, Jean-Marie ULg

E-print/Working paper (2011)

Pour les enseignants/chercheurs universitaires, et autres scientifiques, de ma génération, il y a incontestablement un « avant » et un « après » Apple II !... Plus que tout autre, au travers de sa ... [more ▼]

Pour les enseignants/chercheurs universitaires, et autres scientifiques, de ma génération, il y a incontestablement un « avant » et un « après » Apple II !... Plus que tout autre, au travers de sa créativité, de son ingéniosité, et de son sens de l’entreprise, Steve Jobs a durablement créé de nouvelles opportunités de développement intellectuel et professionnel. [less ▲]

Detailed reference viewed: 169 (49 ULg)
See detailOh, Monsieur Gaston, comme vous parlez bien! : une étude des variations sociolinguistiques dans Gaston Lagaffe
Lafontaine, Dominique ULg

in Enjeux : Revue de Formation Continuée et de Didactique du Français (1984), 5

Detailed reference viewed: 47 (1 ULg)
Full Text
See detailUn oikèma appelé Erechtheion (Pausanias, I, 26, 5)
Pirenne-Delforge, Vinciane ULg

in Carlier, Pierre; Lerouge-Cohen, Charlotte (Eds.) Paysage et religion en Grèce antique. Mélanges offerts à Madeleine Jost (2010)

A close reading of Pausanias’ visit of the north side of the Athenian Acropolis suggests that the present identification of the Erechtheion, which dates back to the seventeenth century, is highly doubtful ... [more ▼]

A close reading of Pausanias’ visit of the north side of the Athenian Acropolis suggests that the present identification of the Erechtheion, which dates back to the seventeenth century, is highly doubtful, as some very few scholars have concluded during the last three decades. The present analysis addresses the word "oikema" used by Pausanias in his description of the Acropolis, comparing this use with all the other places where it appears in the Periegesis. We may conclude that the asymetrical Ionic temple was completely devoted to Athena Polias. Therefore, the so-called Erechtheion has still to be found. [less ▲]

Detailed reference viewed: 118 (6 ULg)
See detailOil bioremediation in sub-antarctic region : a field study at Kerguelen Islands
Delille, D; Delille, Bruno ULg; Prevot, C et al

Conference (1999, April)

Detailed reference viewed: 6 (0 ULg)
Full Text
Peer Reviewed
See detailOil field subsidence phenomena
Charlier, Robert ULg; Schroeder, Christian ULg; Radu, Jean-Pol ULg et al

in Revue Française de Génie Civil (2001), 5(6), 857-866

Subsidence of an chalky oil field is described. The mechanical behaviour of the chalk partly saturated by oil and water is described and allows to model the compaction occurring within a simple reservoir ... [more ▼]

Subsidence of an chalky oil field is described. The mechanical behaviour of the chalk partly saturated by oil and water is described and allows to model the compaction occurring within a simple reservoir model during the depletion as well as during the water injection. [less ▲]

Detailed reference viewed: 81 (11 ULg)
Peer Reviewed
See detailOiled seabirds at the belgian coast
Jauniaux, Thierry ULg; Coignoul, Freddy ULg

in annual proceeding (1993)

Detailed reference viewed: 9 (2 ULg)
Full Text
Peer Reviewed
See detailUn oiseau nouveau au Burundi: le Moineau domestique Passer domesticus
Nasasagare, Régine Pacis ULg

in Malimbus (2011), 33(1), 57-58

Detailed reference viewed: 39 (2 ULg)
Full Text
See detailOiseau, d'où viens-tu?
Pierard, Sébastien ULg; Franchimont, Claudine ULg; Pierard, Gérald ULg

in Association des Géologues Amateurs de Belgique Minibul (1998), 31(8), 20-22

Detailed reference viewed: 31 (2 ULg)