The ESA Herschel Space Observatory was successfully launched on 14 May2009, and is currently operating in its routine science phase. Due to the rapidly evolvingnature of the mission at this point a short summary with pointers to more up-to-dateadditional information is provided here.

Large-scale shocks propagate in the interstellar medium of starburst and active galaxies, driven by the same mechanisms that regulate the evolution of the star formation and AGN episodes. The imprints of shocks in the chemical composition of the molecular gas provide useful means to identify those mechanisms and to asses their effects. We review some recent and on-going studies of the molecular gas chemistry in the nearby star-forming galaxies IC 342, NGC 253 and M 82, based on the well known shock tracer silicon monoxide (SiO). When mapped at high–spatial resolution the SiO emission reveals substantial differences among these galaxies. In particular, the location of shocks and their dominant driver are in correspondence with the evolutionary stage of the starburst episode. Complementary observations of other tracers of shock chemistry, like methanol (CH3OH), help us to improve the characterization of the shock mechanisms. We also present the first high-resolution observations of the SiO emission in the Seyfert 2 galaxy NGC 1068.

The analysis of hydrogen and metal absorption lines in the spectra of distant quasars (QSOs) has become a powerful method to study the distribution and physical properties of low-density gas situated in the extended halos and circumgalactic environment of galaxies at low and high redshift. We here review the overall properties of halo absorption-line systems seen in QSO spectra and discuss their connection to the Milky Way’s population of intermediate- and high-velocity clouds.

Supernovae are known to be the dominant energy source for driving turbulence in the interstellar medium. Yet, their effect on magnetic field amplification in spiral galaxies is still poorly understood. Analytical models based on the uncorrelated-ensemble approach predicted that any created field will be expelled from the disk before a significant amplification can occur. By means of direct simulations of supernova-driven turbulence, we demonstrate that this is not the case. Accounting for vertical stratification and galactic differential rotation, we find an exponential amplification of the mean field on timescales of 100 Myr. We highlight the importance of rotation in the generation of helicity by showing that a similar mechanism based on Cartesian shear does not lead to a sustained amplification of the mean magnetic field.

While the PAMELA collaboration has recently confirmed the cosmic ray positron excess, it is interesting to review the effects of dark matter subhalos on the predicted antimatter signals. We recall that, according to the general subhalo properties as inferred from theoretical cosmology, the enhancement cannot be larger than ~20 for the antimatter yield. This bound is obviously different from what is found for γ-rays. We also show some predictions for supersymmetric benchmark models observable at the LHC and derived in the cosmological N-body framework, but remind the existing discrepancy between the profiles derived from N-body experiments and the current observations.

This paper presents some statistical information about the Concordia turbulent surface inversion layer, regarding height and turbulent energy, its contribution to the peculiar local seeing, and the free atmosphere seeing encountered just above this surface layer.

In a recent study we have used a large sample of extragalactic radio sources to investigate the redshift evolution of the Rotation Measure (RM) of polarized quasars up to z ≈ 3.0. We found that the dispersion in the RM distribution of quasars increases at higher redshifts and hypothesized that MgII intervening systems were responsible for the observed trend. To test this hypothesis, we have recently obtained high-resolution UVES/VLT spectra for 76 quasars in our sample and in the redshift range 0.6 < z < 2.0. We found a clear correlation between the presence of strong MgII systems and large RMs. This implies that normal galaxies at z ≈ 1 already had large-scale magnetic fields comparable to those seen today.

This paper describes the damage occurring in CCDs exposed to solar radiation and explainsits implications for the Gaia measurements by focusing on the astrometric instrument. Itintroduces the strategy that will be used in the Gaia data processing to mitigate theradiation induced effects, and presents CEMGA (CTI effects Models for Gaia) amulti-purpose platform which hosts different models that simulate radiation effects onCCDs.

Testing instrument capabilities is a crucial issue for Gaia, where high levelperformances are expected. This activity involves many aspects: simulation of theinstrument through suitable modelling, comparison of the models with the actualinstrument, as well as producing evaluation methods, which are strictly related to the waydata will be processed and calibrated. In this paper I discuss the interconnections amongthese aspects, and provide some example from the current testing activities.

The era of high-precision astrometry has dawned upon us. The potential of Gaia μas-level precision in positional measuraments is about to be unleashed in the field of extrasolar planetary systems. The Gaia data hold the promise for much improved global characterization of planetary systems around stars of all types, ages, and chemical composition, particularly when synergistically combined with other indirect and direct planet detection and characterization programs.

Telescope pupils are usually not well suited for high dynamical range imaging. Central obstruction, telescope spiders, hard edges and sparseness (for interferometers) can make it very challenging to build a coronagraph. Fortunately, it is often possible to remap a telescope pupil to achieve high contrast imaging without loosing light. In the case of a monolithic telescope, pupil remapping can produce an apodized pupil with 2 aspheric mirrors which redistribute the light without introducing phase aberrations. Similarly, an interferometer pupil can be remapped into a tight configuration compatible with coronagraphic techniques.

An invariant classification scheme of algebraicallygeneral rotating dust with a purely electric Weyl tensor ispresented. It turns out that the vorticity vector of the dustcongruence is necessarily parallel to a Weyl principal vector, whichis moreover geodesic. An explicit metric expression can be obtainedfor the subclass of expanding models with one functionallyindependent zero-order Riemann invariant. The basic equations forthe general case, where there are two such invariants, are givenwithin a weighted 1+1+2 tetrad formalism.

The SIM-Lite mission has finished its technology programme and continues with anengineering risk reduction activity while waiting for the results of the 2010 decadalreview. One of the last remaining activities is work on the SCDU testbed, which isdesigned to calibrate the spectral bias in interferometric astrometry to 0.1 microarcsec.This talk will provide a summary of engineering activities on building flight-likeprototypes of the key interferometer subassemblies, as well as an overview of the types ofproblems one encounters when attempting to do astrometry below 1 microarcsec, as well astheir solution.

We describe recently proposed algorithms, denoted scaled gradient projection (SGP) methods, which provide efficient and accurate reconstructions of astronomical images. We restrict the presentation to the case of data affected by Poisson noise and of nonnegative solutions; both maximum likelihood and Bayesian approaches are considered. Numerical results are presented for discussing the practical behaviour of the SGP methods.

CASPER (Concordia Atmospheric SPectroscopy of Emitted Radiation)is a spectrometer proposed for installation at Dome C, devoted tomeasurements of atmospheric emission in the spectral regionbetween 180 μm and 3 mm (3–55 cm-1). Thisinstrument will be able to perform continuous spectral sampling atdifferent altitudes at angular scales of ~1°. From therecorded data it is possible to extract atmospheric transmittancewithin 1% in the whole wide operating band, together with watervapour content and O2 and O3 concentrations. CASPER willallow us to characterize the site for future FIR/mm telescopes.Atmospheric data recorded by CASPER will allow for correction ofastrophysical and cosmological observations without the need fortelescope-specific procedures and further loss of observation timewith more precision in the observations themselves. Calibration ofground-based telescopes on known sky sources is strongly affectedby atmospheric absorption. CASPER has this as its primary goal.The spectrometer is based on a Martin-Puplett interferometer. Twodata sampling solutions will be performed: phase modulation &fast scan strategy. Sky radiation is collected towards theinterferometer by an optical setup that allows the field of view,to explore the full 0° ÷ 90° range of elevation angles. Witha low spurious polarization instrument, monitoring of polarizedatmospheric contribution will be possible.

The NIR Ca II triplet has proven to be an important tool for quantitative spectroscopy. Here we present results of synthetic spectral analysis for the Ca II triplet for low-metallicity red giant stars, combined with observational data. Our results start to deviate strongly from the widely-used and linear empirical calibrations below [Fe/H] = −2. We provide a new calibration for Ca II triplet studies which is valid down until [Fe/H] = −4 and apply this new calibration to current data sets. We suggest that the classical dwarf galaxies are not so devoid of extremely low-metallicity stars as was previously thought and discuss preliminary results and possibilities for follow-up observations of these extremely low-metallicity candidates.

We report the discovery of a new class of non-radial pulsating stars that are the precursors of low-mass white dwarf stars.

We briefly review the observations of the solar photosphere and pinpoint some open questions related to the magnetohydrodynamics of this layer of the Sun. We then discuss the current modelling efforts, addressing among other problems, that of the origin of supergranulation.

Nebular emission lines are easy to observe, and their spectrum contains a lot of information. We explain the mechanisms of production of the emissions, and the relation between the intensity of the recombination and forbidden lines, and the physical parameters of the objects. A gallery of emission lines spectra is presented, and a rough analysis will clarify their differences. The case of Planetary Nebulae will be developed, in order to determine the extinction constant, the plasma parameters (electron density and temperature), the chemical abundances, and also the properties of the central star (temperature, mass, stellar wind velocity, age).

The main theme of this paper is truthful communication of scientific results. Therefore, concepts of truth, error, quality and value are elaborated.

The following bibliometric parameters are explained: the journal impact factor, the journal cited half-life, and the journal immediacy index, as well as paper counts, citation rates, citation index and the Hirsch index. These bibliometric indices and indicators are illustrated with examples derived from bibliometric analyses of the astronomical literature.

Scientific misconduct in the broadest sense is discussed by category: researcher misconduct, author misconduct, referee and grant-reviewer misconduct. But also publisher misconduct, editorial misconduct and mismanagement, and research supervisor misbehavior are dealt with. The overall signatures of scientific misconduct are focused on, as well as the causes and the cures. This is followed by a Section devoted to whistleblowing.

The biases of bibliometric indices, and the use and abuse of bibliometrics are illustrated. Moreover, suggestions for remediating the present defective system of bibliometric measurement and evaluation are worked out. Finally, the hopes and concerns of our students – either expressed during or after the lectures, or through subsequent private contacts – are passed on.