Due to their high vsini, early-type main-sequence stars have been considered as unsuitable targets for radial-velocity surveys. Knowing about the presence of planets around those stars is however a key issue to understand the impact of the mass of the central star on the way planets form and evolve. We developped in recent years a method that allows to search for planets around those stars and started radial-velocity surveys focused on these targets. We report here some results obtained so far in terms of performances and detection.

A large fraction of the energy released during solar flares is carried by accelerated electrons and ions. At present the most direct diagnostics of accelerated electrons are the radio emission produced from the microwave to the sub-millimeter domains by gyrosynchrotron emission and the hard X-ray/gamma-ray continuum from electron bremsstrahlung. These diagnostics have brought valuable information on the electron energetics, but the characteristics of relativistic electrons are still poorly known, although they provide the most stringent constraints for acceleration models. This is, at least partly, because radio diagnostics were usually obtained below 100 GHz and gamma-ray measurements were restricted to energies below 100 MeV. Recent radio observations in the 200–400 GHz range have revealed a new spectral component, the origin of which is not yet understood. Observations at higher frequencies are necessary in order to discriminate between different possibilities. Although solar observations in the far infrared domain have not yet been performed, this spectral region contains key information on both relativistic electrons and the response of the low atmosphere to energy deposition from the flare. The combination of observations obtained in the far infrared continuum (2–10 THz) with measurements of high energy gamma-rays (up to 500–600 MeV) will not suffer from the limitations of the present diagnostics and thus provide new constraints on acceleration and energy transport processes.

We discuss four questions dealing with massive star evolution. The first one is about the origin of slowly rotating, non-evolved, nitrogen rich stars. We propose that these stars may originate from initially fast rotating stars whose surface has been braked down. The second question is about the evolutionary status of α-Cygni variables. According to their pulsation properties, these stars should be post red supergiant stars. However, some stars at least present surface abundances indicating that they should be pre red supergiant stars. How to reconcile these two contradictory requirements? The third one concerns the various supernova types which are the end point of the evolution of stars with initial masses between 18 and 30M⊙, i.e. the most massive stars which go through a red supergiant phase during their lifetime. Do they produce types IIP, IIL, IIn, IIb or Ib supernovae or do they end without producing any SN event? Finally, we shall discuss reasons why so few progenitors of type Ibc supernovae have yet been detected?

Numerical simulations have become one of the main tools in the researchon stellar convection zones and they can be expected to become veryimportant for the study of the convection-diffusion interaction as well.In this review, I will first provide some historical background andthen select a few sample problems where numerical simulations of stellarconvection have provided useful results or are expected to do so inthe near future: solar granulation, interacting convection zones, andsemi-convection.

Magnetic field generation in the Universe is still an open problem. Possible mechanisms involve the Weibel instability, due to anisotropic phase-space distributions, as well as the Biermann battery, due to misaligned density and temperature gradients. These mechanisms can be reproduced in scaled laboratory experiments. In this contribution we estimate the relative importance of these two processes and explore the laser-energy requirements for producing Weibel dominated shocks.

In this paper, we describe two fully Bayesian algorithms that have been previously proposed to unmix hyperspectral images. These algorithms relies on the widely admitted linear mixing model, i.e. each pixel of the hyperspectral image is decomposed as a linear combination of pure endmember spectra. First, the unmixing problem is addressed in a supervised framework, i.e., when the endmembers are perfectly known, or previously identified by an endmember extraction algorithm. In such scenario, the unmixing problem consists of estimating the mixing coefficients under positivity and additivity constraints. Then the previous algorithm is extended to handle the unsupervised unmixing problem, i.e., to estimate the endmembers and the mixing coefficients jointly. This blind source separation problem is solved in a lower-dimensional space, which effectively reduces the number of degrees of freedom of the unknown parameters. For both scenarios, appropriate distributions are assigned to the unknown parameters, that are estimated from their posterior distribution. Markov chain Monte Carlo (MCMC) algorithms are then developed to approximate the Bayesian estimators.

Traces of heavy metal in cool DZ white dwarfs may be attributed to the accretion of circumstellar dust. This dust is thought to originate from the tidal disruption of some rocky material, they provide a unique opportunity to study the composition of extra-solar planetary systems. The determinations of precise atmospheric parameters and abundances require accurate description of the line profiles of the identified features. We present absorption spectra of Na-He and Ca+-He for the conditions prevailing in cool white dwarfs.

Some general features of indirect approaches for determining cross sectionsof astrophysically relevant reactions at low energies are discussed from a theoretical point of view. The methodsof Coulomb dissocation (CD), of the asymptotic normalization coefficient(ANC) and the Trojan-horse method (THM) are considered.

The operation of any base or expedition to Antarctica is regulatedby the mutual agreement among nations in the “Antarctic Treaty”.This treaty deals with the major aspects of life in Antarctica andits main principles and provisions are described in what follows.

As of today over 40 planetary systems have been discovered in binary star systems. In all cases the configuration appears to be circumstellar, where the planets orbit around one of the stars, the secondary acting as a perturber. The formation of planets in binary star systems is more difficult than around single stars due to the gravitational action of the companion on the dynamics of the protoplanetary disk. In this contribution we first briefly present the relevant observational evidence for planets in binary systems. Then the dynamical influence that a secondary companion has on a circumstellar disk will be analyzed through fully hydrodynamical simulations. We demonstrate that the disk becomes eccentric and shows a coherent precession around the primary star. Finally, fully hydrodynamical simulations of evolving protoplanets embedded in disks in binary star systems are presented. We investigate how the orbital evolution of protoplanetary embryos and their mass growth from cores to massive planets might be affected in this very dynamical environment. We consider, in particular, the planet orbiting the primary in the system γ Cephei.

Optical Interferometry has had an impressive 30-year run of innovation, prototyping and implementation. Some half-dozen arrays are now in operation. Publications are increasing exponentially. In a future phase of advanced facility development, interferometry could move in any of several directions: increased sensitivity, higher resolution, better imaging. What role may the Antarctic have in the future?

Some recent observations of Classical Cepheids, RR Lyrae and Mira variables are used to illustrate their continued importance as standard candles. Gaia will provide a calibration of these stars as distance indicators which should lead to a greatly improved understanding of the formation and evolution of our Galaxy as well as a vital calibration of the extra-galactic distance scale. The importance of infrared observations, as well as a deeper understanding of interstellar reddening and photometric systems, will play a part if the Gaia calibration is to be put to good use.

Dwarf galaxies are currently enjoying wide popularity as more sensitive telescopes are able to unveil their dust emission properties in the mid-infrared to submillimetre wavelengths. Once thought to be an insignificant component of their ISM, the dust in dwarf galaxies can now be studied in greater detail with ISO and Spitzer and soon, Herschel, as well as new ground-based submillimetre telescopes. The mid-infrared to millimetre spectral energy distributions reveal global dust properties which look to be different from more metal-rich starburst galaxies, or our own Galaxy: a) deficit of PAHs; b) abundant very small grains; c) excess submillimetre emission that has been interpreted as very cold (<10 K) dust, thus containing up to 50% of the dust mass of the galaxies. The molecular clouds, and the morphology of the ISM appear to differ dramatically. These properties can be explained by the low metallicity environments and the young massive star formation activity, supernovae activity and chemical abundances.

Near-infrared spectro-photometry, at a spectral resolution of ~100, allows to characterize a great variety of stellar sources, from late-typegiants to emission line stars. Various components of the inter-stellar medium can also be traced. This technique can therefore be very fruitful, in addition, for studies of star forming regions, the Milky Way and external galaxies.The outstanding environmental conditions that are expected at Dome C should be favorable to carry out spectro-photometric surveys in the 1 to 2.5 μm region, that would usefully complement space-borne projects.

Herschel is the fourth cornerstone mission in the European Space Agency (ESA) science programme. It will perform imaging photometry and spectroscopy in the far infrared and submillimetre part of the spectrum, covering approximately the 55–672 µmm range and thus bridging the traditional space infrared range with the groundbased capabilities.
The key science objectives emphasize fundamental issues connected to the formation and evolution of galaxies and stars and stellar systems. However, Herschel will be an observatory facility and its unique capabilities will be available to the entire astronomical community for a wide range of observations. Herschel is equipped with a passively cooled 3.5 m diameter classical Cassegrain telescope. The science payload complement – two cameras/medium resolution spectrometers (PACS and SPIRE) and a very high resolution heterodyne spectrometer (HIFI) – is housed in a superfluid helium cryostat. The ground segment is jointly developed by the ESA, the three instrument consortia, and NASA/IPAC. Herschel is scheduled to be launched into a transfer trajectory towards its operational orbit around the Earth-Sun L2 point by an Ariane 5 ECA (shared with the ESA cosmic background mapping mission Planck) in 2009. Once operational about half a year after launch, Herschel will offer 3 years of routine science operations. Almost 20 000 hours of observing time will nominally be made available for astronomy, 32% is guaranteed time, the remainder is open time which is offered to the worldwide general astronomical community through a standard competitive proposal procedure.

This paper concentrates on a first demonstrator, a 23 NbSi superconducting thermometer array, developed in the DCMB collaboration. Firstly, the NbSi thin film alloy is described then the 23 TES array topology is presented. After that, DC and noise cryogenic measurement is reported. The cryogenic readout chain is also presented and finally, the multiplexing scheme developed for the readout of the 23 pixels array is described.


The science case for an ELT covers a very wide range of topics fromthe study of exo-planets to fundamental parameters of theUniverse. Here the case is summarised, and areas where an Antarctic sitewould provide advantages or limitations are considered. Simple scalingarguments are used to suggest that a “Moderately Extremely LargeTelescope” (or “MELT”) of order 15–20 m diameter in Antarctica wouldbe capable of carrying out some (but not all) of theobservations currently envisaged for a $\sim $40 m class ELT at atemperate site. It is suggested that any such Antarctic telescopeshould be dedicated to a small number of specific science goals,chosen to complement ELTs at temperate sites.

ISOGAL, one of the most important programs observed by ISO, is a7-15 μm ISOCAM survey, with 6" pixels and sensitivity around 15 mJy,of ≈18 deg2 in the Galactic Plane mostly interior to |l| = 30°. In combination with near-infraredDENIS data, ISOGAL data allow detailed studies of cold stellar populationsand Galactic structure in regions highly obscured throughout the innerGalaxy. Version 1 of the ISOGAL Point Source Catalogue is submitted forpublication and will be available through CDS. It contains about 105 stars,with associated KJI DENIS data for most of them. Most of these sources areAGB stars and red giants, with a number of dusty young stars.

We are planning three space astrometry missions as a series of JASMINE missions; Nano-JASMINE, Small-JASMINE and (Medium-sized)JASMINE. JASMINE is an abbreviation of Japan Astrometry Satellite Mission of INfrared Exploration. The JASMINE mission will measure in an infrared band annual parallaxes, positions on the celestial sphere, and proper motions of many stars in the bulge of the Milky Way (the Galaxy) with high accuracies. A target launch date is the first half of the 2020s. Before the launch of JASMINE, we are planning Nano-JASMINE and Small-JASMINE. Nano-JASMINE uses a very small nano-satellite and it is determined to be launched in 2011. Small-JASMINE is a downsized version of the JASMINE satellite, which observes toward restricted small regions of the Galactic bulge. A target launch date is around 2016. A completely new “map” of the Galactic bulge given by Small-JASMINE and JASMINE will bring us many exciting scientific results.

A short description of Dynamic Eclipse Mapping methodology is given. These tools are designed for mapping the surface patterns of non-radial oscillations on eclipsing binary components, using the effective surface sampling of the eclipses. I present two approaches to the problem, an image reconstruction (EM) and a direct model fitting (DF) method, review their capabilities and limitations, then report about the status of their application on real data, with emphasis on the encountered difficulties and caveats.