I Ecuadorian School of Radio Astronomy
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1 Day 1: Wednesday (11 January) 11:00am 11:00am - 11:50am 11:50am - 12:40pm 14:00pm - 14:50pm Day 1 begins Welcome Ceremony (Ericson López) Lecture 1: Introduction to Radio Astronomy (Wladimir Banda) - The Radio Sky - The Electromagnetic Spectrum - Why do we observe at radio wavelengths? - Brief history of radio astronomy - Basic concepts and definitions - Brightness Temperature - Flux Density Lecture 2: Radio Emission Mechanisms ( Ericson López) - Atomic transitions - Atomic tracers - Hyperfine splitting - The 21cm Line - Free particle emission - Cerenkov Emission - Thermal Bremsstrahlung - Magneto-bremsstrahlung - Other mechanisms - Plasma emission - Electron-cyclotron emission Lecture 3: Overview of Radio Telescopes - Overview of Radio Instrumentation - Optical vs. Radio telescopes - Single-dish instruments - Interferometers - Future Arrays - Australian Radio Telescopes - How does interferometry work? - How do we apply for observing time? - How do we observe? Day 1 ends
2 Day 2: Thursday (12 January) 9:00am 9:00am - 9:50am 9:50am - 10:40am 10:40am - 11:00am 11:00am - 12:40pm Day 2 begins Lecture 4: Overview of Radio Sources (Mario Llerena) - Radio-emitting Objects in our Solar System - Stellar Radio Emission - Solar Emission - Pulsars - Galactic Objects - Supernovae - Masers - Neutral hydrogen in Galaxies - Radio Emission in AGNs Lecture 5: Molecular Tracers (Jairo Armijos) - Overview of Interstellar Molecules - Molecular Spectroscopy - Density Probes - Temperature Probes - Optical Depth Probes - Studies of Star formation - Studies of Chemical Abundances - Kinematic Studies - Biomolecules Morning Tea Colloquium: A wide-field investigation into the HI content of galaxies Abstract: The environment of a galaxy can play a major role in its evolution. Late-type gas-rich galaxies can be transformed into gas-poor early-type galaxies in dense environments. Observations show that spiral galaxies in galaxy cluster tend to have on average less neutral hydrogen (HI) than galaxies of the same type and size in the field. Recently there is accumulating evidence that HI-deficient galaxies are also relatively frequent in galaxy groups and that galaxy transformation can already start in the group environment. In this talk I will investigate how the environment influences the HI content of galaxies, and which mechanisms are responsible for the gas deficiency in galaxy groups?
3 14:00pm - 14:50pm Lecture 6: Radiative Transfer (Ericson López) - Propagation of Radiation - Emission - External Absorption and Self-Absorption - Equation of Radiative Transfer - Absorption and emission coefficients - Line broadening - Equivalent width and curve of growth - Observations of optical and UV lines - Opacity - Free-free Emission - Gyro-resonance Emission - Gyro-synchrotron Emission Lecture 7: Synthetic Radio Emission Maps (Wladimir Banda) - Hydro and Magnetohydrodynamic Simulations - General Overview - Example of wind-shock interactions - Output parameters - Radio Emission Calculations - H I Emission - Synchrotron Emission - Ray-tracing Techniques and Visualisation Day 2 ends
4 Day 3: Thursday (13 January) 9:00am 9:00am - 9:50am 9:50am - 10:15am 10:15am - 10:40am 10:40am - 11:00am 11:00am - 11:50am Day 3 begins Science Talk 1: Radio Mapping of the Milky Way (Franklin Aldás) Abstract: Hydrogen is the most abundant element in the interstellar medium (ISM) and neutral hydrogen (HI) atoms are abundant and ubiquitous in low-density regions of the ISM. They are detectable in the 21 cm hyperfine line. HI is considered to be an extremely sensitive tracer of the Galactic mass distribution and of the dynamics of Galactic systems as a whole. We intend to discuss global aspects of the HI distribution in the Milky Way, in particular the region out of the Galactic disk where the halo is located. In this lecture we will cover the process to get and process data from SALSA telescope to get a map of our Galaxy halo. Student Talk 1: Blast Waves in the Cosmos (Patricio Salazar) - The dynamics of blast waves - Supernova Remnants: Examples - A numerical study of blast waves in the interstellar medium - Shock acceleration - Synchrotron emission Student Talk 2: Cosmic bullets as Radio Sources (Emily Franco) - Shock-cloud interactions in the interstellar medium - Cosmic bullets and wind-swept clouds: Examples - A numerical study of shock-cloud interactions - Cloud disruption - HI emission Morning Tea Science Talk 2: Cold Gas in the Galaxy Abstract: To gain a better understanding of star formation it is important to know how the interstellar medium (ISM) transitions from the atomic gas into molecular clouds and how much molecular gas is there in our Galaxy. Based on gamma ray and dust temperature measurements, we know that there is some hidden 'dark gas' in the Milky Way, that can not be traced by HI or CO emission. This gas could be optically thick atomic hydrogen (HI), molecular hydrogen (H2) or a combination of these to. To investigate the nature of the dark gas, I will present new, more accurate measurements of the molecular hydrogen content of the Galaxy.
5 11:50am - 12:40pm 14:00pm - 14:50pm Lecture 8: EMD study case: Pulsars (Christian Vásconez) Abstract: Empirical mode decomposition (EMD) has been widely employed to analyzing nonlinear and nonstationary signals. The EMD algorithm find the intrinsic mode functions based on the intrinsic frequency, reducing the complexity of a signal and enhancing the interpretability of its components. Then, the information embedded in a signal can be easily recovered. On the other hand, Pulsars are highly-magnetized rotating neutron stars. During this rapid rotation, radio waves are emanated from above its poles, which are received on the Earth instruments as a sort of flashes from a lighthouse. In this case of study, we will use the EMD to investigate the time variation of the main components of some extensively studied Pulsars. Lecture 9: LTE Data Analysis (Jairo Armijos) Abstract: Based on several assumptions of astrophysical sources we can used the Local Thermodynamic Equilibrium (LTE) approach to study the excitation temperature and column density of molecules. During the talk I will show the main equations used in the LTE approach, and I will use a software in a case study of data analysis under LTE conditions. Tutorial: H I data analysis - Hands-on demonstration of how to use H I data cubes. A comprehensive description on how to make moment maps in miriad, how to extract spectra from data cubes, and how to calculate the H I mass of galaxies, will be presented. - Required programs: - Miriad - CASA - Recommended programs: - kvis (from the Karma package) - ds9 - An assignment on the tutorial will be given to participants who wish to get a certificate of approval. Day 3 ends
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