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See detail(Erratum) Further observational evidence that MG J0414+0534 is a gravitational mirage.
Angonin-Willaime, M.-C.; Vanderriest, C.; Hammer, F. et al

in Astronomy and Astrophysics (1994), 292

In Sect. 3.3, the identifications of components A1 and A2 for the optical data were inadvertently inverted. This does not change substantially the discussion; just read A1 for A2 and vice versa. In ... [more ▼]

In Sect. 3.3, the identifications of components A1 and A2 for the optical data were inadvertently inverted. This does not change substantially the discussion; just read A1 for A2 and vice versa. In particular, the ratio A2/A1 = 0.3 cannot be made compatible with the radio value without one or several of the mechanisms we suggested. We apologize for the error and thank Dr S. Mao for bringing it to our attention. Erratum to Astron. Astrophys. 281, 388-394 (1994) [less ▲]

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See detailErratum.
Swings, Polydore ULg

in Astrophysical Journal (1941), 94

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See detailErratum: "Envelope solitons associated with electromagnetic waves in a magnetized pair plasma" [vol 12, pg 012319, 2005]
Cattaert, Tom ULg; Kourakis, I.; Shukla, P. K.

in Physics of Plasmas (2005), 12(5), 1

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See detailERRATUM: "Physical Properties of the 0.94 Day Period Transiting Planetary System WASP-18" (2009, ApJ, 707, 167)
Southworth, John; Hinse, T. C.; Dominik, M. et al

in Astrophysical Journal (2010), 723(2), 1829

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See detailErratum: "the Transit Light Curve Project. VII. The Not-So Exoplanet HAT-P-1B" (2007, AJ, 134, 1707)
Winn, Joshua N; Holman, Matthew J; Bakos, Gaspar Á et al

in Astronomical Journal (The) (2008), 136

Two of the midtransit times that were given in Table 3 of Winn et al. 2007 (AJ, 134, 1707-1712) are incorrect. The first entry was incorrect because a trend in the out-of-transit flux had not been removed ... [more ▼]

Two of the midtransit times that were given in Table 3 of Winn et al. 2007 (AJ, 134, 1707-1712) are incorrect. The first entry was incorrect because a trend in the out-of-transit flux had not been removed as described in the text. The sixth entry gave an incorrect epoch, and a midtransit time that was too small by one orbital period, because of a rounding error in the computer code that generated the table. The corrected times are given below in a revised version of Table 3. With these revisions, the ephemeris parameters given in the text following Equation (4) are changed slightly, to T[SUB]c[/SUB] (0) = 2453997.79252(32) (HJD) and P = 4.46543(13) days, where the numbers in parentheses indicate the 1sigma uncertainty in the last two digits. We note that a more precise ephemeris has been calculated by Johnson et al. (2008), based on a combination of the data presented here and more recent transit observations. [less ▲]

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See detailErratum: Characterization of multi-walled carbon nanotube dispersion in resorcinol-formaldehyde aerogels (Microporous and Mesoporous Materials (2014) 184 (97-104))
Haghgoo, M.; Yousefi, A. A.; Zohouriaan Mehr, M. J. et al

in Microporous and Mesoporous Materials (2014), 195

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See detailErratum: High-energy forward scattering and the Pomeron: Simple pole versus unitarized models [Phys. Rev. D 61, 034019 (2000)]
Cudell, Jean-René ULg; Ezhela, V.; Kang, K. et al

in Physical Review. D : Particles and Fields (2001), 63

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See detailErratum: Multipartite-entanglement monotones and polynomial invariants
Eltschka, Christopher; Bastin, Thierry ULg; Osterloh, Andreas et al

in Physical Review. A (2012), 85

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See detailErratum: SN 2007uy − metamorphosis of an aspheric Type Ib explosion
Roy, Rupak ULg

in Monthly Notices of the Royal Astronomical Society (2014)

The supernovae (SNe) of Type Ibc are rare and the detailed characteristics of these explosions have been studied only for a few events. Unlike Type II SNe, the progenitors of Type Ibc have never been ... [more ▼]

The supernovae (SNe) of Type Ibc are rare and the detailed characteristics of these explosions have been studied only for a few events. Unlike Type II SNe, the progenitors of Type Ibc have never been detected in pre-explosion images. So, to understand the nature of their progenitors and the characteristics of the explosions, investigation of proximate events are necessary. Here we present the results of multi-wavelength observations of Type Ib \sn\ in the nearby ($\sim$ 29.7 Mpc) galaxy NGC 2770. Analysis of the photometric observations revealed this explosion as an energetic event with peak absolute $R$ band magnitude $-18.5\pm0.16$, which is about one mag brighter than the mean value ($-17.6\pm0.6$) derived for well observed Type Ibc events. The SN is highly extinguished, \ebv\ = 0.63$\pm$0.15 mag, mainly due to foreground material present in the host galaxy. From optical light curve modeling we determine that about 0.3 \msun\ radioactive $^{56}$Ni is produced and roughly 4.4 \msun\ material is ejected during this explosion with liberated energy $\sim 15\times10^{51}$ erg, indicating the event to be an energetic one. Through optical spectroscopy, we have noticed a clear aspheric evolution of several line forming regions, but no dependency of asymmetry is seen on the distribution of $^{56}$Ni inside the ejecta. The SN shock interaction with the circumburst material (CSM) is clearly noticeable in radio follow-up, presenting a Synchrotron Self Absorption (SSA) dominated light curve with a contribution of Free Free Absorption (FFA) during the early phases. Assuming a Wolf-Rayet (WR) star, with wind velocity $\ga 10^3 {\rm km~s}^{-1}$, as a progenitor, we derive a lower limit to the mass loss rate inferred from the radio data as $\dot{M} \ga 2.4\times10^{-5}$ \msun\,~yr$^{-1}$, which is consistent with the results obtained for other Type Ibc SNe bright at radio frequencies. [less ▲]

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See detailErratum: The XMM Large-Scale Structure survey: an initial sample of galaxy groups and clusters to a redshift z < 0.6
Willis, J. P.; Pacaud, F.; Valtchanov, I. et al

in Monthly Notices of the Royal Astronomical Society (2005), 364

We present X-ray and optical spectroscopic observations of twelve galaxy groups and clusters identified within the XMM Large-Scale Structure (LSS) survey. Groups and clusters are selected as extended X ... [more ▼]

We present X-ray and optical spectroscopic observations of twelve galaxy groups and clusters identified within the XMM Large-Scale Structure (LSS) survey. Groups and clusters are selected as extended X-ray sources from a 3.5 deg2 XMM image mosaic above a flux limit 8e-15 ergs/s/cm2 in the [0.5-2] keV energy band. Deep BVRI images and multi-object spectroscopy confirm each source as a galaxy concentration located within the redshift interval 0.29<z<0.56. We combine line-of-sight velocity dispersions with the X-ray properties of each structure computed from a two-dimensional surface brightness model and a single temperature fit to the XMM spectral data. The resulting distribution of X-ray luminosity, temperature and velocity dispersion indicate that the XMM-LSS survey is detecting low-mass clusters and galaxy groups to redshifts z < 0.6. Confirmed systems display little or no evidence for X-ray luminosity evolution at a given X-ray temperature compared to lower redshift X-ray group and cluster samples. A more complete understanding of these trends will be possible with the compilation of a statistically complete sample of galaxy groups and clusters anticipated within the continuing XMM-LSS survey. [less ▲]

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See detailErratum: VLT + UVES spectroscopy of the low-ionization intrinsic absorber in SDSS J001130.56+005550.7
Hutsemekers, Damien ULg; Hall, Patrick; Brinkmann, J.

in Astronomy and Astrophysics (2004), 422

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See detailL'erreur totale pour le transfert de méthodes
Rozet, Eric ULg

Conference (2010)

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See detailL'erreur totale pour le transfert de méthodes
Rozet, Eric ULg

Conference (2009)

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See detailL'erreur, matière première de l'apprentissage d'une langue
Defays, Jean-Marc ULg

Conference given outside the academic context (2008)

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See detailErreurs de catégorie et erreur de catégoriser
Leclercq, Bruno ULg

Conference (2000, May 06)

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See detailErreurs de classification dans les tables de contingence
Magis, David ULg

Scientific conference (2003, December)

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See detailErreurs de désignations d'Etoiles Ap ou Am
Renson, Pierre ULg

in Bulletin d'Information du Centre de Données Stellaires (1988), 34

A table of erroneous designations which appeared in the literature for Ap and Am stars is given. The number of stars erroneously designated at least once is of the order of 2% of the total number of known ... [more ▼]

A table of erroneous designations which appeared in the literature for Ap and Am stars is given. The number of stars erroneously designated at least once is of the order of 2% of the total number of known or probable Ap and Am stars. [less ▲]

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See detailLes erreurs humaines en anesthésie
De Keyser, Véronique ULg; Nyssen, Anne-Sophie ULg

in Travail Humain (Le) (1993), 56(2-3), 243-266

Human errors in anesthesia - with due respect to the French-speaking tradition, human error is studied in field work, here in anesthesia. The authors specify the social context, compare the process of ... [more ▼]

Human errors in anesthesia - with due respect to the French-speaking tradition, human error is studied in field work, here in anesthesia. The authors specify the social context, compare the process of anesthesia to a continuous process, present a cognitive analyse of the task, emphasizing temporal characteristics and cognitive demands regarding the cognitive aspects of human behavior. Referring to the dictinction made by Hollnagel (1991) between reliability, robustness and adaptiveness of the system (man and machine), they present and analyse some human errors which reveal the importance of variation elements and the dynamic dimension of the environment. Influenced by Time Psychology, they postulate the existence of different systems of temporal reference and of external synchronizers connected to these systems, which would allow an individual to adaptively respond to the demands for synchronization in the face of events and actions whose evolutions cannot be calibrated in clock time. Inadequate systems of temporal reference and the absence of synchronizers can make this adaptation to the evolution and the dynamicity of the environment fail. The prevention integrates different measures (technological, ergonomic, social, organizational, of expertise development, etc.) and relies on collection and in-depth analysis of human error. This paper is dedicated to J. Leplat. [less ▲]

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