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See detailErratum for : primary structure of the streptomyces R61 extracellular DD-peptidase. 1. Cloning into Streptomyces lividans and nucleotide sequence of the gene
Duez, Colette ULg; Piron-Fraipont, C.; Joris, Bernard ULg et al

in European Journal of Biochemistry (1994), 224(3), 1079

This is the correction of the fig. 5 of Primary structure of the Streptomyces R61 extracellular DD-peptidase. 1. Cloning into Streptomyces Zividuns and nucleotide sequence of the gene, by C. Duez, C ... [more ▼]

This is the correction of the fig. 5 of Primary structure of the Streptomyces R61 extracellular DD-peptidase. 1. Cloning into Streptomyces Zividuns and nucleotide sequence of the gene, by C. Duez, C. Piron-Fraipont, B. Joris, J. Dusart, M. S. Urdea, J. A. Martial, J.-M. Frère and J.-M. Ghuysen. European Journal of Biochemistry Volume 162, Issue 3, pages 509–518, February 1987 [less ▲]

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See detailErratum to "Accurate Spitzer infrared radius measurement for the hot Neptune GJ 436b"
Gillon, Michaël ULg; Demory, B*-O; Barman, T. et al

in Astronomy and Astrophysics (2008), 490

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See detailErratum to : A complete fuzzy decision tree technique (vol 138, pg 221, 2003)
Olaru, C.; Wehenkel, Louis ULg

in Fuzzy Sets and Systems (2003), 140(3), 563-565

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See detailErratum to : Recommendations for the health economics analysis to be performed with a drug to be registered in prevention or treatment of osteoporosis
Dere, W; Avouac, B; Boers, M et al

in Calcified Tissue International (2013), 93

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See detailErratum to: Vitamin D Status and Bone Mineral Density Changes During Alendronate Treatment in Postmenopausal Osteoporosis.
Roux, Christian; Binkley, Neil; Boonen, Steven et al

in Calcified tissue international (2013)

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See detailErratum to: “Perturbative evolution and Regge behaviour”: [Phys. Lett. B 448 (1999) 281]
Cudell, Jean-René ULg; Donnachie, A.; Landshoff, P.

in Physics Letters B (2002), 528

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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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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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