We propose a method for detecting gravitational magnification of distant sources, like quasars, due to absorber systems detected in their spectra. We first motivate the use of metal absorption lines rather than Lyman-$\alpha$ lines, then we show how to relate the observed moments of the source magnitude distribution to the mass distribution of absorbers. In order to illustrate the feasibility of the method, we use a simple model to estimate the amplitude of the effect expected for MgII absorption lines. Our model suggests that quasars behind strong MgII absorbers are in average brightened by $-0.05$ to $-0.2$ magnitude due to magnification. One must therefore revisit the claim that, in magnitude limited surveys, quasars with strong absorbers tend to be missed due to extinction effects. In addition to constraining the mass of absorber systems, applying our method will allow for the quantification of this bias.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Using an homogeneous sample of $v\sin i$ values for A-type main sequence stars (Royer et al. 2002), the equatorial velocity ($v$) distributions are determined as function of spectral class, from B9 to F2. The chemically peculiar and binary stars are discarded. These distributions of “normal” stars are discussed in terms of stellar formation and evolution, in particular the remaining bimodality observed for the earliest spectral types of the sample. We show that late B and early A-type main-sequence stars have genuine bimodal distributions of true equatorial rotational velocities probably due to the phenomena of angular momentum loss and of redistribution the star underwent before reaching the main sequence. A striking lack of slow rotators is noticed among intermediate and late A-type stars. The bimodal-like shape of their true equatorial rotational velocity distributions could be due to evolutionary effects.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present a direct detection of the growth of large-scale structure, using weak gravitational lensing and photometric redshift data from the COMBO-17 survey. Deep $R$-band imaging of two $0.5\times0.5$ square degree fields is used to provide shear estimates for over 52000 galaxies; these are combined with photometric redshift estimates from our 17 band survey, in order to obtain a 3-D shear field. We discuss how theoretical models for evolving matter power spectra and correlation functions cab be used to find a best fit to this 3-D shear field. We present the detection of the evolution of the power, and measurements of the rate of evolution for $0<z<1$. We discuss future refinements which will improve the accuracy with which the effect can be measured.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

PISKUNOV: I would like to start this discussion with evolutionary aspects. There are a few recent developments both observational and theoretical. So, some might disagree and others might agree that there are many things happening concerning the pre-Main sequence evolution of early A type and Ap stars and that is what makes them different. Would anybody like to comment?To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

NOELS: How is convection suppressed in model computations?

CUNHA: We do this in two different ways. One is just to make the mixing parameter smaller and smaller. As it approaches zero we are, in e.ect, suppressing convection. The other way is simply to use the equation for radiative energy transport throughout the envelope. The results are very similar.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We describe the first results of a systematic spectropolarimetric survey of the coolest magnetic Ap stars, undertaken with the MuSiCoS spectropolarimeter, with the aim of clarifying the magnetic field and atmospheric characteristics of these enigmatic objects.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Weak gravitational lensing can be combined with distance information from galaxy redshifts to great effect in 3-D weak lensing. With both shear and redshift information I show how the full 3-D dark matter distribution can be reconstructed and present a first application to the COMBO-17 data-set. In addition, I describe the Jain-Taylor geometric test, taking ratios of galaxy shear at different distances, as a probe of the dark energy in the universe and present a preliminary application to COMBO-17.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We describe an ongoing programme using the FORS1 spectropolarimeter on the ESO-VLT to search for magnetic fields in Herbig Ae/Be stars. Our aim is to identify the pre-Main Sequence progenitors of magnetic Ap stars, and to trace the evolution of their magnetic fields at the earliest possible stages.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

High $S/N$ high-resolution spectroscopic observations of seven bright well-known $\lambda$ Bootis stars: HD 31295, HD 91130, HD 110411, HD 125162, HD 183324, HD 192640, and HD 221756 are presented. Sharp absorption details observed in the bottoms of the Na-D lines in HD 192640 and HD 221756 do not show any radial velocity changes with an accuracy up to $1\,{\rm km\,s}^{-1}$. They are of interstellar origin. Manifestations of non-radial pulsation reported earlier in literature are observed both in the Na-D and the ${\rm H}\alpha$ line profiles. The Inglis-Teller formula was used to evaluate the electron density in the upper atmospheric layers ($\tau \sim 0.1$). The values obtained for $\log{N_e}$ are typical for normal A stars with similar effective temperatures and spectral classes.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We discuss the internal structure of stars in the mass range 1.5 to 4 $M_\odot$ from the PMS to the subgiant phase with a particular emphasis on the convective core and the convective superficial layers. Different physical aspects are considered such as overshooting, treatment of convection, microscopic diffusion and rotation. Their influence on the internal structure and on the photospheric chemical abundances is briefly described.

The role of binarity in determining the observed properties and as a tool to constrain the internal structure is also introduced and the current limits of theories of orbital evolution and of available binary datasets are discussed.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The parameter-free model of diffusion in the atmospheres of HgMn stars (Michaud 1986, Michaud et al. 1979) predicts that helium should sink below the $\hbox{He\,{\sc ii}}$ ionization zone that the diffusion of other elements may take place, and that all HgMn stars should have deficits of helium in their photospheres, with a minimum deficit of 0.3 dex. In this study, the Smith & Dworetsky (1993) sample of HgMn stars and normal comparison stars is examined, and the helium abundances determined by spectrum synthesis using échelle spectra taken at Lick Observatory and the AAT. The prediction is confirmed. All HgMn stars are deficient in He by as much as 1.5 dex. Also, two HgMn stars, HR 7361 and HR 7664, show clear evidence of helium stratification.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present results from weak lensing analyses of 20 high-redshift clusters in the ESO Distant Cluster Survey (EDisCS) from both deep optical VLT and HST/ACS imaging. We find that the EDisCS sample is composed primarily of clusters that are less massive than those in current X-ray selected samples at similar redshifts, but that all of the fields are likely to contain massive clusters rather than superpositions low mass groups. We find good agreement between the weak lensing measurements in the VLT and ACS images. Finally we determine the noise level in the shear measurements for the VLT fields as a function of exposure time and seeing and demonstrate that future ground-based surveys which plan to perform deep optical imaging for use in weak lensing measurements must achieve point-spread functions smaller than a median of $0\farcs 6$ FWHM.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The Michigan Catalogue (Vol. I – V) is an excellent database to study the distribution of CP2 stars in the galactic field in the Southern hemisphere. A cross-check with the Bidelman-Catalogue (1973) and the “Catalogue Général des Étoiles Ap et Am” (Renson 1991) shows that in the Michigan Catalogue 3.6% of all stars in the relevant spectral region are CP2 stars. Any discrepant classified stars could be verified photometrically in the $\Delta a$-system. The distribution of CP2 stars does not show any particular preferred region in the Southern hemisphere. The ages of these stars and an evolutionary dependence of the CP2 effect was another important question. We conclude that the CP2 stars occupy the full Main Sequence band.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We present samples from a spectroscopic atlas of the sharp-lined, magnetic Chemically Peculiar star HR 8216 (A6pCr) based on spectrograms obtained with the long camera of the 1.22-m telescope of the Dominion Astrophysical Observatory using a Reticon detector. For the spectral region $\lambda\lambda 3830-4770$ the inverse dispersion is $2.4\,\AA\,mm^{-1}$ with a 2 pixel resolution of 0.072 Å. At the continuum the mean signal-to-noise ratio is 200. The wavelengths in the laboratory frame, the equivalent widths, and the identifications of the various spectral features are given. This atlas should provide useful guidance for studies of similar stars and for atomic physicists interested in improving atomic line parameters.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The complicated and intricate time-dependent behavior of the magnetic field of $\beta$ Lyrae from 1980 to 2004 is discussed.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Gravitational microlensing is a powerful tool to detect compact matter on mass scales ranging from roughly $10^{-6} M_\odot$ to $10^6 M_\odot$ . Of particular importance is the fact that lensing is sensitive to both luminous and dark matter. There are two practically important regimes of microlensing: cosmological and Galactic. The former deals with the effect of stellar mass objects at cosmological distances on even more distant quasars, the latter treats stellar mass objects in the Milky Way or its Halo on stars in the Magellanic Clouds, the Galactic Bulge or M31. Microlensing has been detected in about ten quasars, roughly a dozen microlensing events towards stars in the Magellanic Clouds are on record, more than 1000 events have been measured towards stars in the Bulge. The large majority of microlensing events towards quasars and towards stars in the Magellanic Clouds or the Bulge can be explained by ordinary stellar mass objects. A small fraction of the Galactic microlensing events ($< 5 - 10$ %) could potentially be due to dark matter objects, including stellar mass Black Holes. Current and planned experiments will clarify the question whether any dark matter objects are necessary at all to explain microlensing events.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The use of the Four College Automatic Photometric Telescope at the Fairborn Observatory in Southern Arizona with its ability to observe stars every clear night and for continuous runs has played a major role in our very successful cooperative program of Strömgren differential uvby photometry of magnetic CP (mCP) stars. Out of about 100 stars observed only a few have variable light curves. But more may be found when additional observations are made. We review the published theoretical basis and observations as well as present new results for CU Vir, V1093 Ori, MW Vul, and HR 7224. We interpret some observations as possibly requiring a more robust theory of the variability of mCP star light curves.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

The paper emphasizes the connection between observations and theory in the Lower Instability Strip. It is argued that the $\delta$ Scuti and $\gamma$ Doradus pulsators are very close relatives in the sense that the $\gamma$ Doradus phenomenon can also be seen in the slightly hotter $\delta$ Scuti variables.

New developments and recent progress are reviewed. Arguments are given why all (or almost all) stars in the Lower Instability Strip are pulsators. Furthermore, the question of the so-called missing modes is answered as very extensive photometry campaigns have revealed a large number of pulsation modes with amplitudes less than one millimag. Arguments are given that the 500+ $\ell$ = 0 to 2 modes predicted for $\delta$ Scuti stars are actually present.

The progress made in developing reliable methods of pulsation mode identification is briefly discussed. The discovery of many close modes with small amplitudes sets severe requirements concerning the length of future studies.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We have developed a new code for measuring stellar magnetic fields by calculation using fast transforms of the Fourier cross-correlation function from spectra with reciprocal circular polarization. To test the code, spectra of stars with previously measured magnetic fields were used. In some cases, discrepancies between the field strength obtained by Babcock's classical technique and using our code occur.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

We have compiled all available measurements in the UV region for the group of $\lambda$ Bootis stars. These data are compared to those of F-weak stars and known spectroscopic binary systems. We also use synthetic photometric values from standard atmospheric models to comment on the proposed spectroscopic binary nature of members of the $\lambda$ Bootis group which can be found in the literature.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html