The popularisation of science is central to the culture of the citizen, and if astronomy make poets dream (and many others), astrophysics attracts young and old talents to science. To reveal in simple terms the stellar bestiary from the black holes to the quasars proceeds along this line. Black hole is still the object which is subject to most questions in any public talk on astronomy. How indeed does contemporary physics link the black hole, this stellar gravitational tomb, with the quasar, a galaxy gone mad? The tale is worth telling and makes indeed a beautiful story for contemporary young audience. Can it be told to our high school students with their modest scientific background? This is what we intend to do in this paper, spicing the sauce at the end with some new insights on the unified model of AGN.

Recent attempts to constrain cosmological variation in the fine structure constant, α, using quasar absorption lines have yielded two statistical samples which initially appear to be inconsistent. One of these samples was subsequently demonstrated to not pass consistency tests; it appears that the optimisation algorithm used to fit the model to the spectra failed. Nevertheless, the results of the other hinge on the robustness of the spectral fitting program VPFIT, which has been tested through simulation but not through direct exploration of the likelihood function. We present the application of Markov Chain Monte Carlo (MCMC) methods to this problem, and demonstrate that VPFIT produces similar values and uncertainties for Δα/α, the fractional change in the fine structure constant, as our MCMC algorithm, and thus that VPFIT is reliable.

We present preliminary results from the largest-ever survey of high-resolution associated absorption line (AAL) region metallicities and physical properties in a sample of high redshift (z > 3) quasars.

In this paper, we describe the role astronomy has played in interesting students towards taking physics as a major subject during their final year in Mbarara University of Science and Technology (MUST). This has resulted into some former students from MUST taking up postgraduate studies in Astrophysics and Space Science in South African Universities. The plans to strengthen and develop Astronomy in Uganda are also discussed, and in particular, the strategies for organizing the IYA2009 are outlined.

The values of the fundamental physical constants determine the nature of our universe from the height of mountains on earth to the evolution of the universe over its history. One of these constants is μ = MP/Me the ratio of the proton to electron mass. Astronomical observations provide a determination of this ratio in the early universe through observations of molecular absorption and emission lines in distant objects. Observations of molecular hydrogen in distant damped Lyman Alpha clouds provide a measurement of μ at a time when the universe was only 20% of its present age. To date there is no evidence for a change in μ at the level of 1 part in 105. This limit produces an observational constraint on quintessence theories for the evolution of the universe and Super Symmetric theories of elementary particles.

Feedback from AGN is a key component in most current models of galaxy formation and evolution. For the most massive galaxies, heating and removal of gas by the AGN could precipitate an abrupt quenching of star formation during a dramatic blow-out phase. The “smoking gun” for such a scenario would be direct evidence of powerful outflows associated with the jet. I present some preliminary results of a program to look for these in high-z radio galaxies (HzRGs). Recent observations of the z = 1.5 radio galaxy 3C 230 obtained with the NIFS integral-field spectrograph and Altair laser adaptive optics facility on Gemini North are shown. These reveal with unprecedented resolution the complex kinematics of this system in redshifted Hα and [N ii] emission. The bi-polar velocity field is aligned with the jet axis, with a kinematic center associated with the radio core itself, and turbulent edges approaching the galaxy's escape velocity. This suggests a gas mass of roughly 1011M⊙ has been propagating outwards for 107 to 108 years, corresponding to a mass loss of roughly 102–3M⊙ yr−1, based on its velocity and spatial extent. This is in good agreement with the energetics and typical ages of radio jets, and likely heralds the onset of the “red and dead” stage for this HzRG.

Cosmology contributes a good deal to the investigation of variation of fundamental physical constants. High resolution data is available and allows for detailed analysis over cosmological distances and a multitude of methods were developed. The raised demand for precision requires a deep understanding of the limiting errors involved. The achievable accuracy is under debate and current observing proposals max out the capabilities of today's technology. The question for self-consistency in data analysis and effective techniques to handle unknown systematic errors is of increasing importance. This work is motivated by numerous findings of different groups that partially are in disagreement witch each other. A large part of these discrepancies reflects the different methods of handling systematic errors. Evidently systematics are not yet under control or fully understood. We try to emphasize the importance to take these errors, namely calibration issues, into account and put forward some measures adapted to the problem. Alternative approaches for some of the steps involved are introduced.

Seventy per cent of Aboriginal students drop out of school before the end of their secondary school years and very few go on to do science at the Higher School Certificate level. As a result of this statistics reveal that only 0.003% of the 9000 university science graduates in 2005 in Australia were of Aboriginal origin. This paper discusses an astronomy project which seeks to improve the scientific literacy of Aboriginal students so as to motivate them to take up careers in science and engineering.

Recent detailed studies of narrow absorption line (NAL) systems in QSO spectra have revealed that at least 50% of QSOs have NALs associated with the central engine, and in most cases they are found to be outflowing. Will studies of NALs provide the much sought-after evidence for ubiquitous QSO feedback that can halt the formation of stars in galaxies? I present new results on the distribution of line-of-sight velocity offsets between Mg ii absorbers and their background QSOs, based on a large catalogue of absorbers from SDSS DR6 and greatly improved QSO redshift estimates. The analysis reveals high velocity Mg ii NALs out to at least 6000 km s−1 from the QSO, which cannot be ascribed to the clustering of local galaxies, similar to that observed for C iv absorbers. The existence of such low-ionization, high-velocity gas clouds in the intense ionixing field of the QSO suggests that we may indeed be witnessing the mechanical expulsion of gas, alongside the heating previously observed. We also find an excess of low-velocity Mg ii NALs in radio-loud QSOs compared to radio-quiet QSOs, consistent with their different clustering amplitudes.

I describe ways in which state-of-the-art cosmological simulations are modeling the growth and evolution of supermassive black holes (feeding), and the impact of the energy that they release on galaxies and their surroundings (feedback). I then discuss how this new picture of interconnected co-evolution of galaxies and black holes provides plausible explanations for several of the mysteries that have long vexed theorists studying galaxy formation within the hierarchical cold dark matter paradigm.

Molecular transitions recently discovered at redshift zabs=2.059 toward the bright background quasar J2123-0050 are analysed to limit cosmological variation in the proton-to-electron mass ratio, μ ≡ mp/me. Observed with the Keck telescope, the optical spectrum has the highest resolving power and largest number (86) of H2 transitions in such analyses so far. Also, (7) HD transitions are used for the first time to constrain μ-variation. These factors, and an analysis employing the fewest possible free parameters, strongly constrain μ's relative deviation from the current laboratory value: Δμ/μ =(+5.6±5.5stat±2.7sys)×10−6. This is the first Keck result to complement recent constraints from three systems at zabs>2.5 observed with the Very Large Telescope.

The history, current situation, education and future directions of modern Mongolian space science and astronomy is reviewed. This paper discusses recent efforts to develop astronomy education and research capacity in Mongolia with cooperation of the International Astronomical Union. Various capacity-building initiatives in space science including remote sensing in Mongolia are discussed.

In the radio domain, absorption lines in front of quasars of CO, HI, OH, HCO+, HCN, up to NH3 and CII are providing interesting constraints on fundamental constant variation (α and μ). With more absorbing systems, and a wider redshift range, they could be more competitive than optical studies. This could come with ALMA, with more than one order of magnitude in sensitivity.

Up to now, at intermediate and high redshift, between z = 0.25 to z = 0.89, only four absorption lines systems have been detected in the millimeter range and a fifth system at 0.765, at the OH-18cm lines (Kanekar et al. 2005). Out of these 5 systems, 3 are intervening lensing galaxies (and the background quasar is multiply imaged), and 2 correspond to an absorption of the host (PKS1413+135, B3-1504+377, for an overview see Combes & Wiklind 1996; Wiklind & Combes 1994 to 1998).

A global comparison of all molecular lines observed with the HI-21cm absorption lines in PKS1413 and B0218 systems, the two narrowest line systems, have given quite stringent constraints on y = α2gp μ, Δ y/y = (-0.20 ± 0.44) 10−5 and Δ y/y = (-0.16 ± 0.54) 10−5 respectively (Murphy et al. 2001). The precision is comparable to the MM method (Murphy et al. 2003), with a limited number of absorbing systems.

The high sensitivity if the NH3 inversion lines to variation in the μ ratio (Flambaum & Kozlov 2007) was used by Henkel et al. (2009) in a recent multi-line study of PKS1830 at z ~ 0.9, and Murphy et al. (2008) for B0218 at z ~ 0.7. They find a limit of Δμ/μ < 1.4 10−6 and Δμ/μ < 1.8 10−6 respectively.

Clearly, the radio method suffers from the rarity of the objects, and the fact that they have not yet been discovered at high redshift. The main caveats are that the lines compared come from different molecules, which might have intrinsic velocity offsets, due to several reasons, chemistry, excitation, temperature, density etc. . . When very different frequencies are compared (HI to CO for instance), the background continuum source has different sizes, and the absorbing medium is not the same. Also, the continuum source varies in both intensity and shape, and the compared lines are not always observed simultaneously. Only large statistics could smooth the errors down.

On the positive side, the radio domain is favoured by the high spectral resolution and the very narrow lines due to cold gas, the exquisite precision of the frequency calibration, and the well-known rest frequencies. Also, the sensitivity of the line position to the variation of constants is much higher (by a factor 100 for NH3).

Fortunately, the sensitivity of ALMA will be able to detect many more continuum sources, to search for absorption lines, and at larger redshifts. ALMA will have a much wider bandwidth, allowing the search of absorption, even if not previously detected in the optical or HI-21cm. The redshift will be obtained directly in the millimeter.

It is possible to predict the number of continuum sources that can be selected as targets for absorption searches with ALMA. The density of flat-spectrum quasars has been shown to follow the same curve as optical quasars, a curve peaking at z ~ 2, very similar to the star formation history (Wall et al. 2005). They are still of significant density at z ~ 3.

The merging of astronomy and physics into one subject in Kazakhstan's schools has hampered the knowledge of astronomy that had been established over tha past years. It is necessary to create a new system of aspace education for schoolchildren and the system of additional education should be leading this work. Additional education of astronomy in Kazakhstan began with astronomical clubs in the 1960s. In this paper a new system of additional education of astronomy in Kazakhstan is proposed.

Recent observations of tight correlations between supermassive black hole masses and the properties of their host galaxies demonstrate that black holes and bulges are co-eval and have motivated theoretical models in which feedback from AGN activity regulates the black hole and host galaxy evolution. Combining simulations, analytic models, and recent observations, answers to a number of questions are starting to take shape: how do AGN get triggered? How long do they live? What are typical light curves and what sets them? Is feedback necessary and/or sufficient to regulate BH growth? What effects does that feedback have on the host galaxy? On the host halo? All of this also highlights questions that remain wide open: how does gas get from a few pc to the AGN? What are the actual microphysical mechanisms of feedback? What is the tradeoff between stellar and AGN feedback? And, if there are different “modes” of feedback, where/when are each important?

I report new results from radio studies of fundamental constant evolution, using comparisons between (1) conjugate satellite OH lines, and (2) inversion and rotational lines.

The study of the conditions and the kinematics of the gas in the central region of AGN provides important information on the relevance of feedback effects connected to the nuclear activity. Quantifying these effects is key for constraining galaxy evolution models. Here we present a short summary of our recent efforts to study the occurrence and the impact of gas outflows in radio-loud AGN that are in their first phase of their evolution. Clear evidence for AGN-induced outflows has been found for the majority of these young radio sources. The outflows are detected both in (warm) ionized as well in (cold) atomic neutral gas, and they are likely to be driven (at least in most of the cases) by the interaction between the expanding jet and the medium. The mass outflow rates of the cold gas (Hi) appear to be systematically higher than those of the ionized gas. The former reach up to ~50 M⊙ yr−1 and are in the same range as “mild” starburst-driven superwinds in ULIRGs, whilst the latter are currently estimated to be a few solar masses per year. However, the kinetic powers associated with these gaseous outflows are a relatively small fraction (a few × 10−4) of the Eddington luminosity of the galaxy. Thus, they do not appear to match the requirements of the galaxy evolution feedback models.

We describe briefly the current state of astronomical education in Ukraine, namely the secondary, higher, and post-graduating education systems. A special attention is paid to so called “scientific schools”, non-formal groups of scientists formed by recognised astronomers, which have played and continue to play an important rôle in development of the astronomy education system. Among the founders of scientific schools were the well-known professors Alexander Ya. Orlov (Odessa University), Nikolai P. Barabashov (Kharkiv University), Sergei K. Vsekhsvyatsky (Kyiv University), Semen Ya. Braude (Kharkiv Polytechnical Institute), and Vladimir P. Tsesevich (Odessa University). We also give a general review on the history of astronomy education during the 16th-18th centuries. In 2000 astronomy was reinstated into the current 12-year secondary education curriculum of Ukraine. At present, some elements of astronomical knowledge are included in the lessons of “Natural Sciences” for pupils in the 5th – 10th grades. Astronomy is included as a basic course both in general (non-specialised) schools (17 academic hours in the last 11th or 12th grade) and in lyceums of the natural sciences (34 academic hours in the 12th grade). It is included also as an optional course in the educational program of gymnasiums in humanities. Every year about 75 young persons enter the Ukrainian universities to become astronomers. Results of our monitoring of the efficiency of astronomical higher educational system indicate that about 80% of the entered university students finish their education in 5 years; 50% of those who finished the cursus were working in astronomy. Since 1992 more then 100 astronomers defend Theses of Cand. Sci. (similar to Ph.D) and about 40 astronomers defend Theses of Dr. Sci. (topmost scientific degree, similar to Dr. Hab.). One of our present-day problems is a brain drain of young scientists. About 50% of those who obtained Cand. Sci. degree work outside Ukraine. At the same time in Ukraine we have a lack of experienced persons to work in astronomical instrumentation and observations.

Microwave and far infrared (FIR) spectra of atoms and molecules are in general more sensitive to the variation of the fundamental constants than optical spectra. For example, FIR transitions between levels of the ground state multiplet 3PJ of Carbon-like ions are sensitive to α-variation, (Levshakov et al. (2008)). Moreover, sensitivities of the transitions (1-0) and (2-1) are different, (Kozlov et al. (2008)). This allows to study α-variation by comparing apparent redshifts for these two transitions of the same ion and significantly reduce systematic errors from the Doppler noise.

The centre of astronomy in Tajikistan is the Institute of Astrophysics of the Academy of Sciences of Tajikistan. This institute carries out scientific research and contributes to the preparation of the astronomical staff and to astronomical education. The reform of education in Tajikistan continues and now astronomy is studied in schools (together with physics) and at universities. The Tajik State Pedagogical University resumed in 2007 the training of teachers in physics and astronomy. Since 1999 the Tajik National University (TNU) offers a a specialty in astronomy. In 2006 is restored the Small Academy of Sciences (SAS) of Tajikistan. There is a planetarium in Khujand and in 2006 the Institute of Astrophysics, TNU and the Astronomical Society of Tajikistan, along with the support IBSP/UNESCO, organised the Training Methodical Center (TMC) “TAJASTRO” at the Hisar astronomical observatory for students, graduate students, young scientists, and teachers at secondary schools.