This is one of two chapters that describe the methods used to extract closure phase from CLIMB data and visibility amplitude from both the CLASSIC and CLIMB beam combiners. In this, the second chapter, I describe the pipeline software.

The dynamical state of a multiple planet system reflects the underlying processes of planet formation and orbital evolution. Radial velocity planet searches have yielded several systems that appear to be in or near a low-order mean-motion resonance, including several near a 2:1 mean-motion ratio. Still more systems apparently contain one eccentric planet. We demonstrate that many of these systems are indistinguishable from a system with two planets in a 2:1 mean-motion ratio, and outline a framework for determining how often the observed, apparently-single planets are likely to have such a second planet present.

This chapter is a review of the dynamics of two-planet systems. It includes the study of averaged models of both secular and resonant planetary configurations. The introduction describes our understanding of long-term planetary behavior and stability. The next section introduces the presently known sample of 31 extra-solar systems and the classification of these systems with respect to their dynamical behavior. Their secular dynamics are described in Section 3, where we also introduce the main techniques commonly used for exploring dynamical features. We conclude this section by describing the effects of the proximity of a secular system to mean-motion resonances. Finally, phenomena related to mean-motion resonances are presented in Section 4.

This review presents a general overview of the magnetic fields foundin main sequence A and B stars, and of some of the phenomenaassociated with this magnetism. An attempt is made to place theobserved magnetic fields into an evolutionary context.

Thick layers of warm, low density ionized hydrogen (i.e., the warm ionized medium or WIM) in spiral galaxies provide direct evidence for an interaction between the disk and halo. The wide-spread ionization implies that a significant fraction of the Lyman continuum photons from O stars, produced primarily in isolated star forming regions near the midplane and often surrounded by opaque clouds of neutral hydrogen, is somehow able to propagate large distances through the disk and into the halo. Moreover, even though O stars are the source of the ionization, the temperature and ionization state of the WIM differ significantly from what is observed in the classical O star H ii regions. Therefore, the existence of the WIM and observations of its properties provide information about the structure of the interstellar medium and the transport of energy away from the midplane as well as place significant constraints on models.

We focus our analysis on an event which occurred at the W-limb on May 30, 2003. The dynamical behavior of the filament, including damped oscillations, was investigated with the CDS and EIT (SoHO) experiments, as well as with Hα filtergrams (movies). The eruptive phase is analyzed taking into account the approximate phasing with other eruptive phenomena occurring at the same time or before, called homologous flares and eruptions.

We summarize the current discussions towards astronomical time-series observations at Dome C and emphasize some near-future projects. We define time-series as the continuous process of data taking that takes advantage of the unique time windows and observing conditions at Dome C. We emphasize that most of the current approaches to time-series astrophysics require a dedicated flux collector. In addition, some specific scientific topics may proceed with significant fractions of time on multi-purpose facilities. We consider only on those ideas and projects that were presented at least once during the various ARENA workshops and conferences. Topics of solar science are not considered in detail here.

This paper reviews the overall principles of astronomical spectrographs and the design rules that cover low, medium, and high spectral resolution instruments. Several examples of spectrograph designs are described that are easy to build and are optimised for amateur telescopes. Results are given for each of these instruments. Despite the modest size of amateur telescopes, we show that high performance spectrographs in the hands of amateur astronomers provide access to some specialised areas where the amateur could contribute to useful astrophysical work.

A new analitycally approximated interior metric for a stationary compact perfect fluid withequation of state µ+(1–n)p = µ0 is presented. Also, it is concluded that an object of this kindcan be a source of Wahlquist's metric.

The optical spectra of L- and T-type dwarfs exhibit a continuum dominated by the far wings of the absorption profiles of the Na 3s-3p and K 4s-4p doublets perturbed by molecular hydrogen and helium. We examine the K resonance line wing and core with a unified line profile theory and compare to laboratory experiments and observations of the cool brown dwarf ϵ Indi Ba,b.

The PAMELA satellite-borne experiment was launched from the Baikonur launch site on the 15th of June 2006. Since July 2006 it is daily delivering to ground 16 GBytes of data. The instrument is composed by a magnetic spectrometer, a time-of-flight system, a silicon-tungsten electromagnetic calorimeter, a neutron detector and anticoincidence scintillators. The primary scientific goal is to searching for evidence of dark matter particle annihilations studying antiparticles fluxes. Preliminary results concerning antiproton-proton and positron-electron ratios are presented.

Due to the recent interest shown by astronomers towards the Antarctic Plateauas a potential site for large astronomical facilities, we assistedin the last years to a strengthening of site testing activities in this region, particularly at Dome C. Most of the results collected so far concern meteorologic parameters and optical turbulence measurements based on different principles using different instruments. At present we have several elements indicating that, above the first $20{-}30$ m, the quality of the optical turbulence above Dome C is better than above whatever other site in the world. The challenging question, crucial to know which kind of facilities to build on, is to establish how much better the Dome C is than a mid-latitude site. In this contribution we will provide some complementary elements and strategies of analysis aiming to answer to this question. We will try to concentrate the attention on critical points, i.e. open questions that still require explanation/attention.

This paper describes a general methodology for simulating varioustypes of coronagraphs, especially in the context of their relativecomparison in terms of performance. Some critical points arediscussed such as sampling problems, numerical dynamic range andcomputation errors which could hamper the results. Moreover,comparing the performance of these High Dynamic Range Imaging(HDRI) instruments is not straightforward, so I will define anddiscuss some criteria and their significance.

Multi-epoch, high-resolution (R ∼ 50 000) optical spectrosco-py of the O-type (O9 III – IV) star HD 152246 suggests that it is a triple system where a close inner pair (Aa–Ab) with a circular orbit and a period of 6 days is in a 53–d eccentric orbit (e = 0.68) with a third component Ac. The mass ratios for the inner and outer system are 0.10 and 0.96, respectively. The strengths of various He lines classify Aa and Ac as late O-type stars while Ab is invisible in our spectra.

We discuss the various post-main sequence phases of massive stars,focusing on Wolf-Rayet stars, Luminous Blue Variables, plus connectionswith other early-type and late-type supergiants. End states for massive stars are also investigated, emphasising connections between Supernovae originating fromcore-collapse massive stars and Gamma Ray Bursts.

The Large Magellanic Cloud (LMC) is the closest large satellite of the Milky Way (MW) and the first step of the extragalactic distance scale, hence knowing the distance to the LMC and its three-dimensional structure contributes to the definition of the entire cosmic distance ladder. RR Lyrae stars are old objects which trace the halo of the LMC. They can be used as distance indicators because they follow a period-luminosity-metallicity (PLKsZ) relation in the Ks passband. The purpose of this study was the derivation of a new PLKsZ relation for RR Lyrae stars in the LMC based on the multi-epoch Ks photometry obtained by the VISTA survey of the Magellanic Clouds system (VMC, Cioni et al. 2011).

The first suite of instruments and associated science cases for a larger facilityat Dome C are mainly targeted towards imaging and surveys.While the potential advantages for astronomical observations fromAntarctica are applicable to both imaging and spectroscopy,spectrographs are more complex to build and harder to use in afully automatic and remote operation.However, the innovative technique of 3D-Spectroscopy (3DS) offersimaging and spectroscopic capabilities simultaneously withapplications to a wide range of astronomical programmes.Furthermore, 3DS provides several operational benefits, that are well suited for a location such as Antarctica.

Two exercises are proposed to illustrate the simple linear regression. The first one is based on the famous Galton's data set on heredity. We use the lm R command and get coefficients estimates, standard error of the error, R2, residuals …In the second example, devoted to data related to the vapor tension of mercury, we fit a simple linear regression, predict values, and anticipate on multiple linear regression.

This pratical session is an excerpt from practical exercises proposed by A. Dalalyan at EPNC (see Exercises 1 and 2 of http://certis.enpc. fr/∼dalalyan/Download/TP_ENPC_4.pdf).

In this paper the present status of theoretical understanding - mostlyrelying on mean-field dynamo models - of global magnetic activity oflate-type stars with convective envelopes is reviewed. The principlesof the mean-field dynamo theory are introduced, and a discussion onsome of the present-day problems and challenges is presented. Theremaining sections are devoted to discuss the current status of solarand stellar dynamo models.

One of the key aspects of the upcoming Ultra-Fast Flash Observatory (UFFO) pathfinder forGamma Ray Bursts (GRBs) identification is the UFFO Burst Alert & Trigger Telescope(UBAT). The scientific propose of UBAT is to detect and locate as fast as possible theGRBs in the sky. This is achieved by using a coded mask aperture camera scheme with a widefield of view (FOV) and selecting a X-ray detector of high quantum efficiency and largedetection area. This X-ray detector of high quantum efficiency and large detection area iscalled the UBAT detector. The UBAT detector consists of 48 × 48 Yttrium Oxyorthosilicate(YSO) scintillator crystal arrays and Multi Anode Photomultiplier Tubes (MAPMTs), analogelectronics equipped with ASIC chips, digital electronics equipped with Field ProgrammableGate Array (FPGA) chips, and a mechanical structure that supports all components of theUBAT detector. The total number of the pixels in the UBAT detector is 2304, and the totaleffective detection area is 191 cm2. We will present the design andconstruction, and performance of the UBAT detector including the responses of the UBATdetector to X-ray sources.