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The CSQCD conference will take place at the Gran Sasso Science Institute (GSSI) in L'Aquila (Italy). GSSI is an international PhD school and a center for research and higher education. On May 25 the CSQCD conference will take place at the Gran Sasso National Laboratories (LNGS). LNGS is one of the four national laboratories of INFN (National Institute for Nuclear Physics). It is the largest underground laboratory in the world for experiments in particle physics, particle astrophysics and nuclear astrophysics. Participants to the conference will be picked up at the hotels and transported to LNGS. An underground guided tour will take place that day.
— Advances in understanding high-energy sources (compact objects, accreting binary sources and active galactic nuclei, supernova explosions, gamma-ray bursts) with two complementary courses on clusters of galaxies and applications in fundamental physics.
— State of the art and technological advances in terms of telescopes and detectors. These courses are intended for astrophysicists (particularly those that might later carry instrumental projects) so that they are well aware of the capabilities, but also the limitations of the current techniques and their future developments.
— Data analysis through tutorials on real data. This is particularly important for non-specialists who may get lost in the jargon and specific procedures. Each attendant will have followed at least once all the stages of the analysis with a specialist, making sure that no critical step is forgotten.
astrochemistry. Additionally, during the symposium, we will have two hands-on workshops: One focused in experimental astrochemistry and other focused on observations. The hands-on workshops will have activities on the proposal submissions to the LNLS (Brazilian Synchrotron Light Laboratory) laboratory, data reduction and to LLAMA (Large Latin American Millimeter Array) and ALMA (Atacama Large Millimeter Array) radio observatories. During this meeting we will also have an opportunity to follow a real astrochemical experiment (in real time) at one of the beamlines of the LNLS that simulates the interaction between UV and soft X-rays with
astrophysical ice analogs.
In recent years there has been significant improvement in our knowledge of both the distribution of galaxies through comprehensive redshift surveys and the deviant motions of galaxies through measurements of distances. These observational advances have stimulated interest in methods of interpretation. The constraints on the distribution of matter and cosmological parameters are becoming increasingly precise. Yet major questions remain.
The conference will consist of plenary sessions for in depth oral presentations (review talks and specialized talks on specific topics) and posters. The contributions are either solicited or selected among submitted abstracts. The program will be available after the deadline of abstracts submission (March 3rd, 2016).
Students will be given the opportunity to present their own research work by bringing a poster to the School. The School provides an opportunity for the young researchers to network with fellow students and lecturers, thereby promoting awareness of areas outside the main specialization of the student, and potential cross-fertilization of techniques and concepts.
The School covers two scientific topics that share many synergies and resources: Asteroseismology and Exoplanets. Therefore, the program aims at building opportunities for cooperation and sharing of methods that will benefit both communities. This cooperation has experienced great success in the context of past space missions such as CoRoT and Kepler. Upcoming photometry and astrometry from space, as well as complementary data from ground-based networks, will continue to foster this cooperation. Observations of bright stars and clusters in the ecliptic plane are being made by the repurposed K2 mission, and NASA's TESS and ESA's CHEOPS missions will soon start obtaining similar data over the entire sky. ESA's PLATO mission will then build upon these successes by providing photometric light curves on a wealth of stars. Ground-based spectroscopy from the Stellar Observations Network Group (SONG) will complement the satellite data for the brightest stars in the sky, as will also be the case with the new generation of high-precision spectrographs being developed for the ESO, like the Echelle SPectrograph for Rocky Exoplanets and Stable Spectroscopic Observations (ESPRESSO).
• Fundamental aspects, structure and spectroscopy
• Collisions with electrons, ions, atoms and molecules
• Interaction with clusters, surfaces and solids
• Interaction with photons and plasmas
• Strong field and ultrafast processes
• Production, experimental developments and applications
Dernière mise à jour: 31 Janvier 2016