3,617 research outputs found
Bridges and Watersheds; a narrative analysis of water management in England, Wales and the Netherlands
No full textItem does not contain fulltextKatholieke Universiteit Nijmegen, 09 november 2001Promotores : Godfroij, A.J.A., Albrow, M.273 p
The Global Age. State and society beyond modernity
No full textItem does not contain fulltextM. Albrow The Global Age. State and society beyond modernity Cambridge/Oxford:Polity Press ,2000 0-7456-1189-
Diffractive interactions: Experimental summary
No full textExperimental results on diffraction, which were presented at the 7th International Workshop on Deep Inelastic Scattering and QCD (DIS99), are summarized
Fast timing detectors for forward protons at the LHC
No full textThe author discusses the development of high precision timing detectors for high momentum protons at the LHC, and their application in studying exclusive Higgs boson production
A brown dwarf orbiting an M-dwarf: MOA 2009–BLG–411L
No full textContext. Caustic crossing is the clearest signature of binary lenses in microlensing. In the present context, this signature is diluted by the large source star but a detailed analysis has allowed the companion signal to be extracted. Aims. MOA 2009-BLG-411 was detected on August 5, 2009 by the MOA-Collaboration. Alerted as a high-magnification event, it was sensitive to planets. Suspected anomalies in the light curve were not confirmed by a real-time model, but further analysis revealed small deviations from a single lens extended source fit. Methods. Thanks to observations by all the collaborations, this event was well monitored. We first decided to characterize the source star properties by using a more refined method than the classical one: we measure the interstellar absorption along the line of sight in five different passbands (VIJHK). Secondly, we model the lightcurve by using the standard technique: make (s, q, α) grids to look for local minima and refine the results by using a downhill method (Markov chain Monte Carlo). Finally, we use a Galactic model to estimate the physical properties of the lens components. Results. We find that the source star is a giant G star with radius 9 R . The grid search gives two local minima, which correspond to the theoretical degeneracy s ≡ s−1. We find that the lens is composed of a brown dwarf secondary of mass MS = 0.05 M orbiting a primary M-star of mass MP = 0.18 M . We also reveal a new mass-ratio degeneracy for the central caustics of close binaries. Conclusions. As far as we are aware, this is the first detection using the microlensing technique of a binary system in our Galaxy composed of an M-star and a brown dwarf
Estimating the parameters of globular cluster M 30 (NGC 7099) from time-series photometry
No full textAims. We present the analysis of 26 nights of V and I time-series observations from 2011 and 2012 of the globular cluster M 30 (NGC 7099). We used our data to search for variable stars in this cluster and refine the periods of known variables; we then used our variable star light curves to derive values for the cluster's parameters. Methods. We used difference image analysis to reduce our data to obtain high-precision light curves of variable stars. We then estimated the cluster parameters by performing a Fourier decomposition of the light curves of RR Lyrae stars for which a good period estimate was possible. We also derived an estimate for the age of the cluster by fitting theoretical isochrones to our colour-magnitude diagram (CMD). Results. Out of 13 stars previously catalogued as variables, we find that only 4 are bona fide variables. We detect two new RR Lyrae variables, and confirm two additional RR Lyrae candidates from the literature. We also detect four other new variables, including an eclipsing blue straggler system, and an SX Phoenicis star. This amounts to a total number of confirmed variable stars in M 30 of 12. We perform Fourier decomposition of the light curves of the RR Lyrae stars to derive cluster parameters using empirical relations. We find a cluster metallicity [Fe/H]ZW =-2.01 ± 0.04, or [Fe/H]UVES =-2.11 ± 0.06, and a distance of 8.32 ± 0.20 kpc (using RR0 variables), 8.10 kpc (using one RR1 variable), and 8.35 ± 0.42 kpc (using our SX Phoenicis star detection in M 30). Fitting isochrones to the CMD, we estimate an age of 13.0 ± 1.0 Gyr for M 30. © 2013 ESO
Views from the experiments R410 and R413
No full text(front) D. Corder, M.-I. Sundell, ? (2nd row) L. Carroll, M. Albrow, H.B. Jensen, E. Lillethun, P. Herbsleb, (3rd row) G. Jarlskog, S. Almehe
- …
