. "Practical numerical astronomy course"@en . . "8" . "no data" . . "Presential"@en . "TRUE" . . "Practical course in observation-oriented astronomy"@en . . "8" . "no data" . . "Presential"@en . "TRUE" . . "Emphasis in astronomy"@en . . "24" . "no data" . . "Presential"@en . "TRUE" . . "Radio astronomy"@en . . "6" . "In this course you learn critical aspects of radio astronomy, allowing you to relate radio observations to the astrophysical sources they probe. We thus deal with both the electromagnetic processes in the Universe that produce radio emission, as well as the workings of the telescopes that measure this radio emission.\nThe course consists of presentation- and discussion sessions, complemented by written exercises and practical computer classes, where you are coached to process state-of-the-art radio interferometry data. The course covers the whole spectrum from Mega-Hertz to sub-millimetre radiation and from the cosmic dawn to galactic star formation, focusing on how to interpret data with different frequency- and spatial resolution.\n\nIn particular, the following aspects are covered:\n\nDetection of radio waves, telescope and receiver characteristics\nThe workings of interferometers and their response\nData processing techniques, such as image deconvolution and self-calibration\nThe AGN phenomena and the brightest radio sources\nRadio properties of the cold and warm interstellar medium\nSpecial radio sources, such as pulsars and masers\nDesign and data flow characteristics for interferometers like LOFAR, VLBI, ALMA, SKA\nSpectral line observation of molecules and HI throughout the universe\n\nOutcome:\nAfter this course you are ready to engage in scientific discussions that concern radio observations of astrophysical phenomena. You can compare how various radio telescopes and observing modes can be used optimally to investigate the astrophysical processes that generate long wavelength emission.\n\nAfter this course you can:\n\nWrite a clear, concise report describing a radio-interferometric data reduction and subsequent image analysis;\nDevelop a data reduction process from raw radio interferometric data to science-quality images;\nWrite an observing proposal for an appropriate radio telescope to answer a scientific question;\nAnalyse quantitatively how radio interferometric concepts affect a specific scientific result;\nExplain if and why certain radio image features are astrophysical or not;\nAnalyse to what extent signals are mutually coherent;\nIdentify common radio-astronomical data visualizations with their axis labels removed;\nIdentify the type of astrophysical object visualized in a figure;\nPerform basic Fourier-analyses, such as deriving a SINC function andqualitatively predicting the telescope’s response to a small collection of elementary shapes;\nDescribe (the function of) common components involved in a telescope’s signal processing;" . . "Presential"@en . "TRUE" . . "Astronomical spectroscopy"@en . . "3" . "Astronomical observation is a subject combining astronomy, quantum mechanics, and experimental spectroscopy. To accurately interpret and optimize the knowledge and societal impact of the obtained telescope data in various spectral ranges, it is crucial to have a rigorous understanding of the principles of theoretical and laboratory works.\r\nIn this course, you will learn to understand and apply atomic and molecular spectroscopy in an astronomical context. The course covers the basics of absorption spectroscopy and the history of astronomical spectroscopy. You will learn how to interpret spectra and what is needed to simulate molecular spectra for electronic, vibrational, and rotational transitions. The course highlights the synergy between observational and laboratory spectroscopy in astronomical research.\r\nThis course starts with general principles of quantum mechanics, and from these derives the principles behind atomic and molecular spectroscopy of molecules commonly found in the interstellar medium. You will apply the newly learned theory to the spectral simulation using the Pgopher software and compare them with observational data. Finally, general laboratory spectroscopy will be introduced to demonstrate how a typical molecular spectrum is measured in fully controlled experimental conditions.\n\nOutcome:\nUpon completion of this course, you will be able to:\r\n1. Read spectroscopic notation, and interpret and simulate (interstellar) spectra\r\n2. Explain the origin of atomic and molecular spectra\r\n3. Reproduce and simulate the typical shape of molecular spectra\r\n4. Calculate/explain physical parameters from spectra\r\n5. Read and summarize the literature on spectroscopy with astronomical applications\r\n6. Explain solid state and gas phase spectra obtained in the laboratory" . . "Presential"@en . "FALSE" . . "Astronomy student colloquium"@en . . "0" . "All Astronomy Master's Research Projects are concluded with a public presentation, referred to as a Student or MSc Colloquium. This presentation will be graded by the Student Colloquium coordinator for your presentation skills and not for the scientific content or the way you conducted your research. Prepare your talk well using these presenting tips and action plan for your presentation, and practice your talk well in advance within your research group. Immediately after your talk, you will receive feedback on your presentation and a pass/fail grade.\r\nNote: in the specialisations Astronomy and Business Studies, and, Astronomy and Science Communication and Society, the Student Colloquium can be given on either the Master's Research Project or on the internship or research project carried out for the BS/SCS component of the programme, with a preference for the former. Note that the Student Colloquium requirement is separate from any other presentations that may be required for these specialisations.\r\n\r\nAs an Astronomy master's student, you have to plan your own Student Colloquium, which will be held in the format of an Astronomy master's colloquium conference three times per year (October, January and June, as shown in your schedule). You will get the opportunity to register for a colloquium slot approximately two weeks before the start of each conference, via a link that will be sent to your @strw email address.\n\nOutcome: Not Provided" . . "Presential"@en . "TRUE" . . "Radio astronomy"@en . . "6" . "In this course you learn critical aspects of radio astronomy, allowing you to relate radio observations to the astrophysical sources they probe. We thus deal with both the electromagnetic processes in the Universe that produce radio emission, as well as the workings of the telescopes that measure this radio emission.\r\nThe course consists of presentation- and discussion sessions, complemented by written exercises and practical computer classes, where you are coached to process state-of-the-art radio interferometry data. The course covers the whole spectrum from Mega-Hertz to sub-millimetre radiation and from the cosmic dawn to galactic star formation, focusing on how to interpret data with different frequency- and spatial resolution.\r\n\r\nIn particular, the following aspects are covered:\r\n\r\nDetection of radio waves, telescope and receiver characteristics\r\n\r\nThe workings of interferometers and their response\r\n\r\nData processing techniques, such as image deconvolution and self-calibration\r\n\r\nThe AGN phenomena and the brightest radio sources\r\n\r\nRadio properties of the cold and warm interstellar medium\r\n\r\nSpecial radio sources, such as pulsars and masers\r\n\r\nDesign and data flow characteristics for interferometers like LOFAR, VLBI, ALMA, SKA\r\n\r\nSpectral line observation of molecules and HI throughout the universe\n\nOutcome:\nAfter this course you are ready to engage in scientific discussions that concern radio observations of astrophysical phenomena. You can compare how various radio telescopes and observing modes can be used optimally to investigate the astrophysical processes that generate long wavelength emission.\r\n\r\nAfter this course you can:\r\n\r\nWrite a clear, concise report describing a radio-interferometric data reduction and subsequent image analysis;\r\n\r\nDevelop a data reduction process from raw radio interferometric data to science-quality images;\r\n\r\nWrite an observing proposal for an appropriate radio telescope to answer a scientific question;\r\n\r\nAnalyse quantitatively how radio interferometric concepts affect a specific scientific result;\r\n\r\nExplain if and why certain radio image features are astrophysical or not;\r\n\r\nAnalyse to what extent signals are mutually coherent;\r\n\r\nIdentify common radio-astronomical data visualizations with their axis labels removed;\r\n\r\nIdentify the type of astrophysical object visualized in a figure;\r\n\r\nPerform basic Fourier-analyses, such as deriving a SINC function andqualitatively predicting the telescope’s response to a small collection of elementary shapes;\r\n\r\nDescribe (the function of) common components involved in a telescope’s signal processing;" . . "Presential"@en . "TRUE" . . "Astronomical spectroscopy"@en . . "3" . "Astronomical observation is a subject combining astronomy, quantum mechanics, and experimental spectroscopy. To accurately interpret and optimize the knowledge and societal impact of the obtained telescope data in various spectral ranges, it is crucial to have a rigorous understanding of the principles of theoretical and laboratory works.\r\nIn this course, you will learn to understand and apply atomic and molecular spectroscopy in an astronomical context. The course covers the basics of absorption spectroscopy and the history of astronomical spectroscopy. You will learn how to interpret spectra and what is needed to simulate molecular spectra for electronic, vibrational, and rotational transitions. The course highlights the synergy between observational and laboratory spectroscopy in astronomical research.\r\nThis course starts with general principles of quantum mechanics, and from these derives the principles behind atomic and molecular spectroscopy of molecules commonly found in the interstellar medium. You will apply the newly learned theory to the spectral simulation using the Pgopher software and compare them with observational data. Finally, general laboratory spectroscopy will be introduced to demonstrate how a typical molecular spectrum is measured in fully controlled experimental conditions\n\nOutcome:\nUpon completion of this course, you will be able to:\r\n1. Read spectroscopic notation, and interpret and simulate (interstellar) spectra\r\n2. Explain the origin of atomic and molecular spectra\r\n3. Reproduce and simulate the typical shape of molecular spectra\r\n4. Calculate/explain physical parameters from spectra\r\n5. Read and summarize the literature on spectroscopy with astronomical applications\r\n6. Explain solid state and gas phase spectra obtained in the laboratory" . . "Presential"@en . "FALSE" . . "Astronomy student colloquium"@en . . "0" . "All Astronomy Master's Research Projects are concluded with a public presentation, referred to as a Student or MSc Colloquium. This presentation will be graded by the Student Colloquium coordinator for your presentation skills and not for the scientific content or the way you conducted your research. Prepare your talk well using these presenting tips and action plan for your presentation, and practice your talk well in advance within your research group. Immediately after your talk, you will receive feedback on your presentation and a pass/fail grade.\r\nNote: in the specialisations Astronomy and Business Studies, and, Astronomy and Science Communication and Society, the Student Colloquium can be given on either the Master's Research Project or on the internship or research project carried out for the BS/SCS component of the programme, with a preference for the former. Note that the Student Colloquium requirement is separate from any other presentations that may be required for these specialisations.\r\n\r\nAs an Astronomy master's student, you have to plan your own Student Colloquium, which will be held in the format of an Astronomy master's colloquium conference three times per year (October, January and June, as shown in your schedule). You will get the opportunity to register for a colloquium slot approximately two weeks before the start of each conference, via a link that will be sent to your @strw email address.\n\nOutcome: Not Provided" . . "Presential"@en . "TRUE" . . "Galactic and extra-galactic astronomy (1)"@en . . "6" . "spherical astronomy – galactic coordinates and proper motions in galactic coordinates; Solar motion, Local standard of rest (LSR); theory of galactic rotation; Oort’s equations and constants; rotation curve, dark matter; spiral structure of the Galaxy; galactic bar; stellar dynamics; regular and irregular forces in stellar systems; basic equation of stellar dynamics; characteristics of trajectories of stars; perturbations: epicyclic motion in the galactic plane and cyclic motion in a plane normal to the galactic plane; dark matter dynamics and generalized gravity, apparent distribution of stars, differential and integral function of brightness, luminosity function, interstellar absorption.\n\nOutcome:\nTo gain basic knowledge of the Galactic structure and the motions of Galactic objects. Students will be able to study and understand the-state-of-the-art scientific papers and/or be able to independently recalculate the published results." . . "Presential"@en . "TRUE" . . "Galactic and extra-galactic astronomy (2)"@en . . "4" . "Models of the Galaxy; Galactic structures: spiral arms, galactic warp and flare, stellar streams; resonances in the Galaxy; classification of galaxies, their structure, and properties; methods of\r\n\r\ndetermining galactic masses and distances; radial galactic velocities, redshift, and Hubble’s law; galactic gas; space distribution of galaxies, local group of galaxies, clusters of galaxies; basics of galactic evolution; galactic mergers and interaction with intergalactic gas; active galaxies, galactic nuclei, quasars.\n\nOutcome:\nTo gain basic knowledge about galaxies in the Universe, their structure, kinematic and dynamic. Students will be able to study and understand the-state-of-the-art scientific papers." . . "Presential"@en . "TRUE" . . "Spectroscopy in astronomy"@en . . "3" . "Hartree-Fock theory of atom and molecule. Atomic and molecular orbitals. Energy levels of atoms and molecules. Born - Oppenheimer approximation. Rotational and vibrational states of diatomic molecules. Rotational levels of polyatomic molecules. Vibration of polyatomic molecules. Electron states and electron spectra. atoms and molecules Symmetry of transitions, selection rules. Spin-orbital coupling. Summary of quantum mechanical theory of rotational moment. Spectroscopic methods in astronomy, modeling of synthetic spectra and fitting methods. Emission, absorption and reflectance spectroscopy in stellar, galactic and interplanetary astronomy.\n\nOutcome:\nGaining a basic overview of the energy states of atoms and molecules, their spectral characteristics, quantum-chemical description of rotational and vibrational motions, basic types of molecular spectroscopy, selection rules, their origin. To provide an overview of methods and applications of spectroscopic research in astronomy." . . "Presential"@en . "TRUE" . . "Computers in astronomy (1)"@en . . "4" . "Work with Python libraries such as installation, basic set-up, input parameters, usage of functions, programming own scripts. Work with FITS images covering image calibration, segmentation and astrometric reduction. Calculation of object’s ephemerides, coordinates transformation, own scripts development. Usage of Python libraries Python libraries AstroPy, SciPy, NumPy, matplotlib, rebound, SourceExtractor, and sgp4.\n\nOutcome:\nStudents will acquire basic skills for work with astronomical libraries in Python. These skills will cover areas like FITS image processing, object’s ephemeris prediction on celestial sphere, application of numerical integration in astronomy and visualization of obtained scientific data." . . "Presential"@en . "TRUE" . . "Selected topics in history of astronomy"@en . . "3" . "Origin of astronomy; Astronomy of ancient cultures; Astronomy of Greek philosofers: Aristarchos, Hipparchos; Almagest; Ptolemaios and the geocentric conception of the world; Astronomy in the middle ages; Copernicus and the heliocentric system; Gaileo Galilei; Kepler; Newton and development of celestial mechanics. Development of astrophysics.\n\nOutcome: Not Provided" . . "Presential"@en . "FALSE" . . "Computers in astronomy (2)"@en . . "4" . "Solving astronomical problems on a computer: time measurement, coordinate systems, planetary motion, Kepler and perturbation ephemeris. Use of programming in C / C ++ and Linux OS.\n\nOutcome:\nStudents will be able to solve simple astronomical problems on a computer, work with documentation, use existing libraries in their programs, work with Linux." . . "Presential"@en . "FALSE" . . "Galactic and extra-galactic astronomy - state exams"@en . . "2" . "Galactic coordinates and proper motions in galactic coordinates; Solar motion, Local standard of rest (LSR); theory of galactic rotation; Oort’s equations and constants; rotation curve, dark matter; spiral structure of the Galaxy; galactic bar; stellar dynamics; regular and irregular forces in stellar systems; basic equation of stellar dynamics; characteristics of trajectories of stars; perturbations: epicyclic motion in the galactic plane and cyclic motion in a plane normal to the galactic plane; dark matter dynamics and generalized gravity, apparent distribution of stars, differential and integral function of brightness, luminosity function, interstellar absorption. Models of the Galaxy; Galactic structures: spiral arms, galactic warp and flare, stellar streams; resonances in the Galaxy; classification of galaxies, their structure, and properties; methods of determining galactic masses and distances; radial galactic velocities, redshift, and Hubble’s law; galactic gas; space distribution of galaxies, local group of galaxies, clusters of galaxies; basics of galactic evolution; galactic mergers and interaction with intergalactic gas; active galaxies, galactic nuclei, quasars.\n\nOutcome:\nThe students will gain and proof the overview and understanding of the-state-of-the-art knowledge in the field of galactic and extragalactic astronomy." . . "Presential"@en . "TRUE" . . "Specialised topics in astronomical techniques"@en . . "6" . "• To understand the basic concepts of observational astronomy beyond the visible domain.\n• To get acquainted with techniques used in the mm and radio domain\n• To get acquainted with techniques used in high-energy astrophysics\n• To understand the basic concepts of interferometry\n• To be trained in reduction and interpretation of optical interferometric data\n• To be trained in reduction and interpretation of radio interferometric data\n• To be trained in advanced image processing techniques used in astronomical research" . . "Presential"@en . "TRUE" . . "Specialised topics in astronomical techniques"@en . . "6" . "no data" . . "Presential"@en . "FALSE" . . "Time series analysis in astronomy"@en . . "5" . "LEARNING OUTCOMES\nThe students will learn the theory, the application and the programming of different period finding methods that can be used to analyse astronomical data.\n\nCONTENT\nThe following methods are taught: the Discrete Chi Square Methods, the power spectrum method and other statistical methods. All these will be programmed and applied to real data" . . "Presential"@en . "FALSE" . . "Observational course in astronomy"@en . . "5" . "Description of qualifications\nThe objective of the course is to give the students an introduction to the central elements in preparation, execution and data reduction relating observations at a modern astrophysical observatory.\n\nThe student will after having passed the course be able to:\n\n- apply for observing time (although there is no guarantee that time will be granted)\n\n- prepare an observing run. This includes determining when a given target can be observed during the year and on a given night, how long the target should be observed to reach a specified signal-to-noise ratio, establishing which calibration data are needed, and interact with the observatory staff about which instrumental setup is needed for the run.\n\n- Carry out astrophysical observations in an efficient and careful manner.\n\n- Extract the astrophysically relevant information from a dataset and write up a report presenting the conclusions in a clear and comprehensive manner.\n\nContents\nThe course has three elements: 1) a preparation phase, 2) the actual observations at the telescope, and 3) a data reduction and report writing phase.\n\n- phase 1: application for observing time, astronomical instruments, preparation of observing runs (target visibility, finding charts, signal-to-noise considerations). It is mandatory to take part in this phase, which is expected to take ~5 days. The time for this will be agreed with the students.\n\n- phase 2: execution of astrophysical observations at the Nordic Optical Telescope. When possible we will also visit other telescopes on Roque del los Muchachos (e.g., the Swedish solar telescope, the Isaac Newton Group telescopes or the Spanish GTC).\n\n- phase 3: reduction and presentation of data." . . "Presential"@en . "FALSE" . . "Galactic astronomy"@en . . "5" . "General structure of the Galaxy. Interchange of matter between stars and ISM. Forms of\nISM: gas and dust, extinction, reddening. Stellar clusters: globular and open, moving cluster.\nMilky Way in near and far infrared. Velocity of the Sun with respect to neighbouring stars:\napex, centroid. LSR and peculiar velocities. Determination of Solar LSR velocity in respect to\nthe Galaxy centre. Determination of the peculiar velocity of the Sun. Simple model of the\nGalaxy rotation: velocity vector of a star in respect to the Sun. Oort's approach to the Galaxy\nrotation. Oort's constants. Differential rotation of the Galaxy: geometric interpretation.\nGalactic rotation curve from radio observations of HI clouds. Determination of the Sun –\ngalactic center distance. Estimation of the Galaxy mass from Oort's constants. Models of\nmass distribution in the Galaxy. Surface brightness of galaxies. Visual versus dynamical mass\nof the Galaxy. Dark matter. Distribution of stellar velocities: fast and slow stars, orbits.\nDistribution of components of peculiar velocities for slow stars: ellipsoid and dispersion.\nRelationship between velocity dispersion, spectral type and metallicity. Asymetric distribution\nof the rotational component of the peculiar velicities. Scattering of the stellar orbits leading\nto the increase of the peculiar velocity dispersion. Disc and halo kinematics. Star counts\nmethodology. Relation between star-counts and their space distribution. Kapteyn's universe.\nLF, ILF and SFR functions. LF for galactic disc and for stars in GC. Height scale and its\ndependence on spectral type. Discovery of spiral arms in the Galaxy. Stability of spiral arms\nand density waves. Mechanism of star formation in spiral arms. Discovery of galactic bar.\nStellar populations of the Galaxy. Thin and thick discs. Gas and dust distribution in the\nGalaxy. ELS model of the Galaxy orogin: free infall and energy dissipation. SZ model of the\nGalaxy formation: acrection. Chemical evolution of the Galaxy. Age and spatial distribution\nof globular clusters. Origin of the thick disc. Centre of the Galaxy with a black hole." . . "Presential"@en . "FALSE" . . "Extragalactic astronomy"@en . . "5" . "Components of the Milky Way Galaxy: stars vs interstellar matter, central object, rotation\ncurve, populations, chemical composition and kinematics. Classification of normal galaxies,\nHubble sequence, different galaxy classification systems. Global parameters of galaxies:\nmasses, sizes, luminosities, composition, stellar populations. Observational evidence for the\nexistence of dark matter. Spectra of galaxies versus their composition. Methods for\ndetermining distances to galaxies. Formation of galaxies, galaxy evolution scenarios, the\nimportance of collisions and mergers of galaxies in their evolution. The Local Group,\ncomponents and characteristics. The nearest galaxies: Sagittarius dwarf galaxy, Magellanic\nClouds, M31 and M33. Dwarf galaxies: types and properties. Virgo and Coma clusters of\ngalaxies, the large-scale structure of the Universe. The unified model of the AGN, Seyfert\ngalaxies, blazars, radio galaxies. Active galaxies, sources of non-thermal radiation in active\ngalaxies. Quasars and their spectra, interpretation of quasar spectra. Supermassive black\nholes, relations between supermassive black hole masses and other galaxy parameters.\nGravitational lensing: conditions and examples of the formation of Einstein rings, double and\nmultiple images. Weak lensing and microlensing." . . "Presential"@en . "FALSE" . . "Astronomy"@en . . "4" . "-" . . "no data"@en . "FALSE" . . "Astronomical informaion technology"@en . . "2" . "Review of programming skills:\n\nalgorithms\nC / C++ programming language\nIntroducion to astronomical image processing:\n\ntechnical images (bias/dark/lat)\nastronomical image format (its)\nIntroducion to IDL (Interactive Data Language) programming language:\n\nIDL used for data input/output/analysis\nIDL used for its image format - IDL used for scieniic visualizaion\nusing the IDL Astronomy Users Library (http://idlastro.gsfc.nasa.gov)" . . "Presential"@en . "TRUE" . . "Astronomical spectroscopy 1-2"@en . . "4" . "Electromagneic radiation, astronomical sources in the visible and other spectral ranges\nHistory and basics of astronomical spectroscopy\nSpectroscopes, how they work and their applicaion in astrophysics\nInfrared and ultraviolet spectra of stars, interstellar medium, galaxies, AGN-s\nX-ray sources and their spectra\nSpectral analysis sotware tools: IDL, IRAF, and CLASS (GILDAS)\nReducion and analysis of HI 21cm, CO (J=1-0) 2,6mm and NH3 (1,1) 1,3cm spectra\nReducion and analysis of opical spectra of stars, spectral classiicaion\nReducion and analysis of opical spectra of galaxies, determinaion of redshit\nWriing spectroscopic observaion proposals for measurements with facility telescopes: one for the visible and one outside the visible range" . . "Presential"@en . "TRUE" . . "Seminar in modern astronomy 1-4"@en . . "8" . "Students gain experience in giving scieniic presentaions and in reading/processing scientific papers.\nAstronomical Seminar 1:\ngiving a 15-20 minutes long presentaion, based on a short scieniic paper Astronomical\nSeminar 2:\ngiving a 15-20 minutes long presentaion, based on a long (min. 10 pages) scieniic paper Astronomical\nSeminar 3:\ngiving a 20-40 minutes long presentaion, based on one or more scieniic papers of total lebgth exceeding 10 pages, in the form of a free review of the subject Astronomical\nSeminar 4:\ngiving a 20-40 minutes long presentaion, based on one or more scieniic papers of total lebgth exceeding 10 pages, in the form of a free review of the subject" . . "Presential"@en . "TRUE" . . "Galactic astronomy 1-4"@en . . "8" . "1st semester:\r\nHistory of radio astronomy, atmospheric radio window\r\nBasic deiniions and terms, radio emission mechanisms\r\nInstrumentaion: single-dish radio telescopes and interferometers\r\nVery Long Baseline Interferometry networks, data processing, image reconstrucion; applicaions in astrophysics, astrometry and geodesy\r\nNext-generaion radio astronomy instruments\r\n2nd semester:\r\nClassiicaion of celesial radio sources\r\nRadio astronomy in the Solar System\r\nGalacic radio astronomy, the Galacic Centre\r\nExtragalacic radio sources, acive galacic nuclei\r\n Cosmological applicaions\r\nCosmic microwave background radiaion" . . "Presential"@en . "TRUE" . . "Radio astronomy 1-2"@en . . "4" . "N.A." . . "Presential"@en . "FALSE" . . "Infrared astronomy 1-2"@en . . "4" . "N.A." . . "Presential"@en . "FALSE" . . "Advanced astronomical informaion technology 1-2"@en . . "4" . "Semester 1: Review of programming skills: algorithms, C or C++ programming languages. Overview of the basic numerical methods; implemening Euler's method; implemening Runge-Kuta methods; elements of parallel programming; CUDA / OpenMP / MPI\r\n\r\nSemester 2: overview of astronomical image processing; IDL (Interacive Data Language) programming language; data analysis using IDL; image processing using IDL; IDL Astronomy Users Library (http://idlastro.gsfc.nasa.gov)" . . "Presential"@en . "FALSE" . . "Astronomy from space 1-2"@en . . "4" . "Motivaion for space research, scieniic and social environment, poliical and legal issues\nPhases of space missions, criical points and examples\nChronology and milestones of lunar and planetary exploraion\nHigh energy and infrared astronomy and space applicaions\nSpace observatories and observaions\nOrbits, trajectories and maneuvers\nRocket engines and fuels and their use\nLaunch vehicles, and spaceports\nOn-board systems\nHungarian space research, achievements and science teams\nMajor space research and technology insituions and organizaions (ESA, NASA, JAXA)" . . "Presential"@en . "FALSE" . . "The history of astronomy 1-2"@en . . "4" . "N.A." . . "Presential"@en . "FALSE" . . "Introduction to astronomy 1-4"@en . . "8" . "N.A." . . "Presential"@en . "FALSE" . . "Information technology in astronomy 1-3"@en . . "6" . "no data" . . "Presential"@en . "FALSE" . . "Radio astronomy"@en . . "5" . "no data" . . "Presential"@en . "TRUE" . . "Radioastronomy"@en . . "6" . "At the end of the course, the student will gain a deeper knowledge of the concepts regarding the synchrotron radiation and its relation with other processes of the production of radiation in astrophysics. Various astrophysical bodies will be analysed, ranging from interstellar gas, star formation and end-products, generation of radio jets on various scales, processes at the centre of galaxies and in the intergalactic medium, relativistic particle acceleration and re-accelerating, etc. The student will have advanced knowledge on both classical as well as new topics in radioastronomy, in the general framework of modern astrophysical research. The student will be able to understand and present in a critical manner research papers on arguments discussed during the course." . . "no data"@en . "FALSE" . . "astronomy"@en . . "no data" . "no data" . . "Presential"@en . "FALSE" . . "Astronomical and space-based systems engineering"@en . . "no data" . "no data" . . "Presential"@en . "FALSE" . . "Space astronomy"@en . . "6" . "Not found" . . "Presential"@en . "TRUE" . . "Radio astronomy"@en . . "6" . "Specific Competition\nCE1 - Understand the basic conceptual schemes of Astrophysics\nCE2 - Understand the structure and evolution of stars\nCE9 - Understand the instrumentation used to observe the Universe in the different frequency ranges\nGeneral Competencies\nCG2 - Understand the technologies associated with observation in Astrophysics and instrumentation design\nCG4 - Evaluate the orders of magnitude and develop a clear perception of physically different situations that show analogies allowing the use, to new problems, of synergies and known solutions\nBasic skills\nCB6 - Possess and understand knowledge that provides a basis or opportunity to be original in the development and/or application of ideas, often in a research context\nCB7 - That students know how to apply the knowledge acquired and their ability to solve problems in new or little-known environments within broader contexts\nCB8 - That students are able to integrate knowledge and face the complexity of formulating judgments based on information that, being incomplete or limited, includes reflections on the social and ethical responsibilities linked to the application of their knowledge and judgments\nCB10 - That students possess the learning skills that allow them to continue studying in a way that will be largely self-directed or autonomous\nExclusive to the Specialty in Observation and Instrumentation\nCX11 - Understand the techniques used by radio astronomy\n6. Subject contents\nTheoretical and practical contents of the subject\nIntroduction and basic concepts (6 hours)\nHistorical perspective. Main discoveries.\nThe atmospheric window of radio waves. Main astrophysical processes of radio emission.\nBasic definitions. Specific intensity. Flux density. Total intensity. Total flow. Spectral luminosity. bolometric luminosity.\nBlack body emission. Planck's Law. RJ approach. Brightness temperature.\nRadiative transport equation.\nAtmospheric absorption and emission.\nRadio telescopes and radiometers (8 hours)\nGeneral design of a radio telescope. Mount, optics, front-end, back-end.\nReception diagram. Main lobe, lateral lobes. Angular resolution. Antenna solid angle, main lobe, and beam efficiency.\nReciprocity theorem.\nGain and directivity. Effective opening and opening efficiency.\nAntenna temperature and system temperature. Flow measured by the antenna. Antenna sensitivity.\nDissipated noise in a radiometer. White noise and 1/f noise. Gain fluctuations. Nyquist's theorem. noise temperature.\nEquation of the ideal radiometer. Real radiometer equation. Sensitivity and signal to noise.\nBroadcasting processes in the radio-continuum (8 hours)\nBlackbody thermal emission. Equilibrium temperature. Astrophysical applications: radio emission of the calm Sun, planets, Moon.\nPseudothermal emission from interstellar dust.\nFree-free issue. Emission produced by an accelerated charge (Larmor equation). Optically thin and optically thick regime. Astrophysical applications: H II regions.\nSynchrotron emission. Total power emitted. Spectrum. Astrophysical applications: supernova remnants.\nCosmic Microwave Background. Sunyaev-Zel'dovich effect in galaxy clusters.\nOther general astrophysics applications. Streaming from our galaxy. Global galaxy emission. Population from extragalactic sources.\nSpectral lines (8 hours)\nRadiative transport in lines. Einstein coefficients. Excitation temperature.\nAtomic lines. 21cm line of the H I. Recombination lines in radius. Astrophysical applications: rotation curves, interactions, reionization tomography, line intensity mapping , determination of relative abundances.\nMolecular lines. Issuance processes. CO and isotopes line. H2, H2O and other molecular lines. Astrophysical applications: study of molecular clouds, mapping of the Milky Way with H2 and CO." . . "Presential"@en . "FALSE" . . "An introduction to astronomy"@en . . "5.5" . "Description in Bulgarian" . . "Presential"@en . "TRUE" . . "General astronomy I"@en . . "4,5" . "Description in Bulgarian" . . "Presential"@en . "TRUE" . . "An introduction to radio astronomy"@en . . "6,0" . "Description in Bulgarian" . . "Presential"@en . "FALSE" . . "General astronomy II"@en . . "4,5" . "Description in Bulgarian" . . "Presential"@en . "TRUE" . . "Extragalactic astronomy"@en . . "2.0" . "Description in Bulgarian" . . "Presential"@en . "FALSE" . . "History of astronomy"@en . . "3.0" . "Description in Bulgarian" . . "Presential"@en . "FALSE" . . "Practice in astronomy"@en . . "5.0" . "Description in Bulgarian" . . "Presential"@en . "TRUE" . . "Spectroscopy and photometry in astronomy"@en . . "6.0" . "### Teaching language\n\nEnglish \n_Obs.: As aulas serão em português caso todos dominem esta língua._\n\n### Objectives\n\nIt is intended that students understand the workings and characteristics of detectors and instruments of observation in modern astronomy, in particular in the optical waveband and including CCD cameras and spectrographs. They should also acquire the basic knowledge enabling them to reduce photometric and spectroscopic data, analyze the results and infer conclusions on practical applications in research.\n\n### Learning outcomes and competences\n\nFamiliarization with the basic signals in Astronomy (photometry, spectroscopy), detectors and their operation in order to be able to reduce the respective data. Acquisition of basic knowledge on data reduction. Ability to handle specific software and analyse the results of its application to real data.\n\n### Working method\n\nPresencial\n\n### Program\n\n1\\. Instrumentation in Astronomy - Cameras and detectors. - Noise and artifacts recorded on a CCD and their correction. - Filter and magnitude systems in the optical. - The spectrograph and the dipersor - gratings. - Resolving power of a spectrograph. - Quick reference to multi-object spectroscopy and integral field spectroscopy. 2. Reduction of low-resolution spectroscopic observations - The treatment of thermal noise and sensitivity analysis of the detector. - Removal of the effects of cosmic rays in the images. - Calibration of the spectra in wavelength. - Calibration of spectra in flux using standard reference stars. - Analysis 3. Reduction of observations in several photometric filters - The treatment of thermal noise and sensitivity analysis of the detector. - PSF analysis and detection of objects in the image. - Aperture photometry. - Photometry calibration using standard stars.\n\n### Mandatory literature\n\nSterken Chr.; [Astronomical photometry](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000228193 \"Astronomical photometry (Opens in a new window)\"). ISBN: 0-7923-1776-9 \nKitchin C. R.; [Astrophysical techniques](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000193071 \"Astrophysical techniques (Opens in a new window)\"). ISBN: 0-85274-461-7 \nGray David F.; [The observation and analysis of stellar photospheres](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000268080 \"The observation and analysis of stellar photospheres (Opens in a new window)\"). ISBN: 0-521-85186-6 \n\n### Complementary Bibliography\n\nSutton Edmund C.; [Observational astronomy](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000295338 \"Observational astronomy (Opens in a new window)\"). ISBN: 9781107010468 \n\n### Comments from the literature\n\nSupport documents regarding the software used for data reduction will be made available or indicated to the students. Published scientific papers will also be given as bibliographic material, when/if required.\n\n### Teaching methods and learning activities\n\nPractical work with computer during classes, enabling the reduction of real astronomical data using the adopted software. These classes will be supplemented with lectures on the fundamentals of data processing. The final exam will use the computer, in order to reduce real observations, both spectroscopic and photometric.\n\n### Software\n\nAstropy \n\n### keywords\n\nPhysical sciences > Astronomy \n\n### Evaluation Type\n\nDistributed evaluation with final exam\n\n### Assessment Components\n\nTest: 100,00%\n\n### Amount of time allocated to each course unit\n\nEstudo autónomo: 106,00 hours\nFrequency of lectures: 56,00 hours\n\n**Total:**: 162,00 hours\n\n### Eligibility for exams\n\nStudents should participate in, at least, 50% of the practical classes.\n\n### Calculation formula of final grade\n\nStudetns can choose between two alternative assessment systems: \n \nA- With continuous assessment \nA1. \\[50%\\] Intermediate written test on Photometry \nA2. \\[50%\\] Intermediate written test on Spectroscopy \n \nB- Without continuous assessment \nAppeal exam with two components: Photometry \\[50%\\] + Spectroscopy \\[50%\\]\n\n### Classification improvement\n\nBy exam, in the \"época de recurso\" (appeal). The appeal exam will have two components: a module on spectroscopy and another one on photometry. If the student wishes, he/she can improve the grade in only one of the modules.\n\nMore information at: https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=498802" . . "Presential"@en . "TRUE" . . "Extragalactic astronomy"@en . . "6.0" . "### Teaching language\n\nEnglish \n_Obs.: As aulas serão em português caso todos dominem esta língua._\n\n### Objectives\n\nThe aim of this course is that students acquire a thorough knowledge about different types of galaxies, their composition and the physical mechanisms responsible for the variety of observed properties and their evolution in different environments. Alongside the theoretical approach, existing observational evidence will be presented, and the major ongoing and future projects with scientific impact in this area will be mentioned.\n\n### Learning outcomes and competences\n\nIt is intended that students acquire a thorough knowledge about different types of galaxies, their composition and the physical mechanisms responsible for the variety of observed properties and their evolution in different environments. Alongside the theoretical approach, it is expected that students develop skills of reasoning and understanding, critical analysis and exposition of different results available in the literature and, if possible, experience a brief approach to research in this topic. \n\n### Working method\n\nPresencial\n\n### Program\n\nI. The Milky Way - structure, dimensions, main constituents (stars, interstellar medium, dark matter). \n \nII. Galaxy classification schemes and main properties of the different galaxy types. \n \nIII. Disks and spheroids - dynamics, total mass estimates, scaling relations and statistical properties. Star formation in disks. \n \nIV. Spectral synthesis: main types, ingredients and equations. \n \nV. Groups and clusters of galaxies: dimensions, constituents and main properties. \n \nVI. Physical mechanisms responsible for galactic evolution in groups and clusters: dynamical friction, ram-pressure stripping, tidal stripping, mergers. \n \nVII. Active galaxy nuclei - emission; different types of AGN and the unification scheme. Estimates of the mass of the central supermassive black hole. \n \nVIII. High redshift galaxies and evolutionary studies: techniques and types of distant galaxies; K and E corrections; observational biases; evolution in color, morphology, star formation rate and stellar mass function.\n\n### Mandatory literature\n\nPeter Schneider; Extragalactic Astronomy and Cosmology, Springer. ISBN: 978-3-642-54082-0/978-3-642-54083-7 (eBook) \nMo Houjun; [Galaxy formation and evolution](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000295217 \"Galaxy formation and evolution (Opens in a new window)\"). ISBN: 9780521857932 \n\n### Complementary Bibliography\n\nCarroll Bradley W.; [An introduction to modern astrophysics](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000228181 \"An introduction to modern astrophysics (Opens in a new window)\"). ISBN: 0-201-54730-9 \nB.W. Carrol, D.A. Ostlie; An Introduction to Modern Galactic Astrophysics and Cosmology, Addison-Wesley, 2007 \nSparke Linda S.; [Galaxies in the universe](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000260230 \"Galaxies in the universe (Opens in a new window)\"). ISBN: 0-521-59740-4 \nPeterson Bradley M.; [An introduction to active galactic nuclei](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000228123 \"An introduction to active galactic nuclei (Opens in a new window)\"). ISBN: 0-521-47911-8 (pbk) \nA.K. Kembhavi, J.V. Narlikar; Quasars and Active Galactic Nuclei, Cambridge University Press, 1999 \nKrolik Julian H.; [Active galactic nuclei](http://catalogo.up.pt/F/-?func=find-b&local_base=FCUP&find_code=SYS&request=000259815 \"Active galactic nuclei (Opens in a new window)\"). ISBN: 0-691-01151-6 \n\n### Comments from the literature\n\nThroughout the semester, references for scientific papers dealing with the subjects taught will be provided.\n\n### Teaching methods and learning activities\n\nClasses involve the exposure by the lecturer of the contents of the program - including the discussion of scientific results based on relevant and/or recent papers -, with the help of multimedia materials, followed by examples of application and problem solving when appropriate. \n\n### Software\n\nO trabalho prático requer conhecimentos básicos de python. \n\n### keywords\n\nPhysical sciences > Astronomy > Astrophysics \n\n### Evaluation Type\n\nDistributed evaluation with final exam\n\n### Assessment Components\n\nExam: 50,00%\nOral exam: 5,00%\nPractical assignment or project: 40,00%\nwritten assignment: 5,00%\n**Total:**: 100,00%\n\n### Amount of time allocated to each course unit\n\nAutonomous study: 120,00 hours\nFrequency of lectures: 42,00 hours\n\n**Total:**: 162,00 hours\n\n### Eligibility for exams\n\nThe exam is compulsory and has a minimum grade - see **Formula of final grade. \n \n**\n\n### Calculation formula of final grade\n\nThe assessment in this curricular unit consists of: \n\\- a final exam - which is compulsory - that contributes with a weight of 50% to the final classification; \n\\- exercises to be solved at home and presented by the students in class orally, and delivered afterwards in writing, which contribute with 10% for the final classification; \n\\- a practical assignment that contributes with 40% to the final grade. \nThe formula to compute the final classification is as follows: Nf=Ex+Q+TP where Nf is the final grade, Ex is the exam grade (rated 0-10, and required to be no less than 4/10), Q are the exercises (oral presentation + written work, rated 0 to 2) and TP is the assignment (rated 0 to 8).\n\n### Classification improvement\n\nThe improvement of the classification can be made on the written exam component only, that will still weigh 50% of the final mark.\n\nMore information at: https://sigarra.up.pt/fcup/en/ucurr_geral.ficha_uc_view?pv_ocorrencia_id=498807" . . "Presential"@en . "TRUE" . . "Astronomy from space"@en . . "3.0" . "Learning objectives\n\nReferring to knowledge\n\nReceive advanced academic training in the fields of Astronomy from spacecraft and of Space Weather by the study of selected areas in these fields. These subjectes provide the student with basic and updated knowledge to properly prepare them for a subsequent research career in the field. For those who do not seek a career in research, the knowledge acquired in these subjects will contribute in boosting their skills and experience.\nTo understand the basic concepts involved in astrophysical measurements from space and their limitations. Review the conditions and requirements needed in the design of a space mission via the description and anlysis of several scientific missions of the European Space Agency (ESA) and of the Unitated States’ National Aeronautics and Space Administration (NASA).\nTo understand the basic concepts in the fields of Heliophysics, and in particular of the Solar-Terrestrial relations, including: solar activity, interplanetary space, and the Earth’s magnetosphere. To understand the basic concepts of Space Weather, its effects on the geospace and on human activity in the short term, and its applications.\n\nTeaching blocks\n\n \n\n1. Space Based Astronomy\n1.1. Elements of a mission\n\nOrbit. Launch windows. Payload. Subsystems and Launchers.\n\n1.2. Space mission analysis and design\n\nDevelopment phases. Analysis. Selection and implementation. The main agencies: ESA and NASA. ESA’s Cosmic Vision 2015−2025\n\n1.3. Astronomy from the space\n\nScientific goals. Missions: Types and payloads. Data bases and explotation. Future missions (CHEOPS, Juice, Euclid, Plato, etc.).\n\n2. Space Weather\n2.1. Space Weather\n\nDefinition and goals. Effects of solar storms on spacecraft and Earth. Extreme stormy events. Prediction. Radiation risks. The Space Weather programme of ESA/EU and the US National Space Weather programme.\n\n2.2. Heliophysics\n\n\na) Solar wind plasma and interplanetary magnetic field. The Earth’s magnetosphere and magnetospheric storms.\n\nb) Solar activity: flares and coronal mass ejections. The solar activity cycle.\n\nc) Solar energetic particle events.\n\n2.3. Heliophysics and space weather missions\n\nStudy of different scientific missions: Ulysses, SOHO, ACE, STEREO, SDO, Parker Solar Probe and Solar Orbiter. Data and in-situ instrumentation.\n\n \n\n \n\nTeaching methods and general organization\n\n \n\n\nLecturers explain the topics of the programme with the support of electronic material and internet resources, among others. Students are given the material presented in each lecture in electronic format mainly via the Campus Virtual. Personal assignments: the student will deepen in some of the aspects of the subjects explained, prepare a report to be submitted and/or an oral presentation to prove the comprehension of the knowledge acquired. It is intended that these assignments have and important practical component, based as much as possible in actual space missions.\n\n\nGenre perspective will be taken into account in the development and activities of this subject, as much as possible.\n\nThe degree of attendance and assessment activities may be modified in the event of a health crisis, like it was during COVID-19. If this is the case, any changes will be informed to the students in due course through the usual channels.\n \n\n \n\nOfficial assessment of learning outcomes\n\n \n\nThe evaluation criteria are as follows:\n\nThe understanding of the fundamental concepts will be evaluated through the student’s personal work. Students will have elaborated different assignments consisting on short reports and/or oral presentations in English. Pro-active participation in the lecture sessions will be considered. In those cases where there is a reasonable doubt about the student’s gained knowledge, he/she will take a written or oral examination. The corresponding percentages are:\n\nBrief written assignments: 30%\nPreparation and oral presentations of given topics: 50%\nParticipation: 20%\n\n\nFor the re-evaluation there will be an oral presentation and a test-type exam. There is no need to repeat the brief written assignment if it was evaluated positively.\n \n\nExamination-based assessment\n\nOral presentation of a previously agreed topic: 60%\n\nExam: 40% (the same of the oral presentation).\n\n \n\n \n\nReading and study resources\n\nCheck availability in Cercabib\n\nBook\n\nSpacecraft systems engineering. 4th ed. Chichester ; New York : Wiley, 2011 Enllaç\n\n\nSpace mission analysis and design., Wiley J. Larson & James R. Wertz, Kluwer Academic, 1999 Enllaç\n\n\nOrbital Motion, A. E. Roy, 2nd ed., Ed. Hilger, 1982 Enllaç\n\n\nSpace physics : an introduction to plasmas and particles in the heliosphere and magnetospheres, Kallenrode, May-Britt, 3rd ed. Berlin : Springer, 2004 Enllaç\n\n\nIntroduction to space physics. Eds. Kivelson and Russel, Cambridge : Cambridge University Press, 1995 Enllaç\n\n\nSolar Particle Radiation Storms Forecasting and Analysis, Eds. Malandraki, O.E. & Crosby, N.B., Astrophysics and Space Science Library, 444, Springer, 2018, ISBN 978-3-319-60051-2 (eBook)\n\n \tIntroduction to particle radiation from the Sun in Chapters 1 to 6. https://link.springer.com/book/10.1007/978-3-319-60051-2\n\nPhysics of Space Storms. From the Solar Surface to the Earth. H. E. J. Koskinen (Springer Praxis, 2011). ISBN 978-3-6-00310-3\n\n\nHeliophysics. Space Storms and radiation: causes and effects. C.J. Schrijver and G.L. Siscoe. Cambridge Univeristy Press, 2010. Enllaç\n\n\nElectronic text\n\nSpace radiation hazards and the vision for space exploration Enllaç\n\n\nMore information at: http://grad.ub.edu/grad3/plae/AccesInformePDInfes?curs=2023&assig=568434&ens=M0D0B&recurs=pladocent&n2=1&idioma=ENG" . . "Presential"@en . "FALSE" . . "Galactic astronomy"@en . . "6.0" . "Learning objectives\n\nReferring to knowledge\n\n— Acquire a basic understanding of the structure, kinematics and dynamics of the Milky Way.\n\n— Advance in the knowledge of processes of formation and evolution of spiral galaxies.\n\n— Become familiar with the physical properties of the interstellar medium and of the stellar components of the Milky Way.\n\n— Understand which observables properties are available to us. Understand the precision in what can be attained today, focusing on the Gaia mission of the European Space Agency\n\n— Acquire knowledge of statistical analysis techniques.\n\n \n\n \n\nTeaching blocks\n\n \n\n1. Introduction\n1.1. Galaxies and their place in the Universe\n\n1.2. History of galactic astronomy\n\n1.3. Overview of galaxies: current knowledge\n\n2. Astronomical units\n2.1. Stellar component\n\n2.2. Interstellar matter\n\n2.3. Catalogues and large surveys\n\n2.4. Interstellar extinction\n\n3. Stellar statistics\n3.1. Apparent distribution of stars\n\n3.2. Fundamental equation of stellar statistics\n\n3.3. Luminosity function of stars\n\n3.4. The initial mass function and the star formation rate\n\n3.5. Galaxy models for predicting stellar recounts\n\n4. Galactic Kinematics\n4.1. Kinematics of stars in the solar neighbourhood\n\n4.2. Large scale kinematics\n\n5. The orbits of the stars in the galactic potential\n5.1. Integrals of motion\n\n5.2. Energy and angular momentum: Lindblad’s diagram\n\n5.3. The orbital structure in spherical, asymmetrical and non-asymmetric potentials\n\n5.4. Force and movement perpendicular to the galactic disc\n\n6. Fundamental equations of stellar dynamics\n6.1. Poisson’s equation\n\n6.2. Boltzmann equations without collisions\n\n7. Introduction to the chemical evolution of galaxies\n7.1. Observational evidence\n\n7.2. Gas surface density, rate of supernova explosions, enrichment\n\n7.3. Basic elements of a chemical evolution model: star birth rate and rate of fall of matter\n\n7.4. Some simplified models\n\n8. Collisions and encounters of star systems\n \n\n \n\nTeaching methods and general organization\n\n \n\n— Lectures.\n\n— Presentation of assignments by students to the rest of the class.\n\n— Practical exercises with laptop\n\n— Reading and discussion of recent articles\n\nNote: The degree of attendance to the University for the teaching and evaluation activities may be modified depending on the restrictions arising from the health crisis. If this is the case, any changes will be informed in due course through the usual channels.\n\n \n\n \n\nOfficial assessment of learning outcomes\n\n \n\nAssignments proposed to students, oral presentation in front of the class and hands-on activities. This part counts for the 40% of the final mark of the course. \n\nThe evaluation at the end of the course consists of a written examination to assess the students progress that counts for the 60% of the final mark (with the requirement of passing the exam).\n\nReevaluation: For students who do not pass the exam, a second written exam takes place in June to assess the improvement in the student progress. The final mark includes the 40% of the course activities as well.\n\n \n\nExamination-based assessment\n\nThe evaluation at the end of the course consists of a written examination to assess the students progress.\n\n \n\n \n\nReading and study resources\n\nCheck availability in Cercabib\n\nBook\n\nBINNEY, JAMES, 1950- ; MERRIFIELD, MICHAEL..\n\nGalactic astronomy. Princeton : Princeton University\n\nPress, cop. 1998\n\n Enllaç\n\nBINNEY, JAMES, 1950- ; TREMAINE, SCOTT, 1950-.\n\nGalactic dynamics. (2nd ed. Princeton : Princeton\n\nUniversity Press, 2008\n\n Enllaç\n1a ed. Enllaç\n\nMIHALAS, DIMITRI, 1939-. ; BINNEY, J.AMES, 1950-.\n\nGalactic astronomy: structre and kinematics. 2nd ed.\n\nSan Francisco : Freeman, cop. 1981\n\nhttps://cercabib.ub.edu/discovery/search?vid=34CSUC_UB:VU1&search_scope=MyInst_and_CI&query=any,contains,b1105403* Enllaç\n\nSCHEFFLER, HELMUT ; ELSÄSSER, HANS, 1929-.\n\nPhysics of the galaxy and interstellar matter.\n\nBerlin : Springer, 1988" . . "Presential"@en . "FALSE" . . "Astronomy"@en . . "6.0" . "http://grad.ub.edu/grad3/plae/AccesInformePDInfes?curs=2023&assig=569097&ens=M0D0G&recurs=pladocent&n2=1&idioma=ENG" . . "Presential"@en . "FALSE" . . "Introduction in astronomy"@en . . "4" . "no data" . . "Presential"@en . "TRUE" . . "Bachelor seminar on astronomy"@en . . "10" . "no data" . . "Presential"@en . "TRUE" . . "Extragalactic astronomy"@en . . "8" . "no data" . . "Presential"@en . "TRUE" . . "Other Astronomy Kas"@en . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .