X-ray astronomy (100 eV to 100 keV) was historically the starting point of high-energy astronomy, and many categories of astrophysical sources (from stars to all accretion phenomena and to clusters of galaxies) emit X-rays. The "X-ray view" of an object is therefore required for understanding the physical phenomenon. In particular X-ray astronomy remains a reference for all gamma-ray astronomy, since we have to turn to X-rays to study in details the sources detected at higher energy. Recent observational developments renew the X-ray astronomy landscape. NASA’s NuSTAR telescope, launched in 2012, extends the domain of imaging telescopes beyond 10 keV into hard X-rays. The Japanese Astro-H telescope, which will be launched in 2016, opens fine spectroscopy to faint and extended sources. The Russian-German SRG satellite will be launched in 2017 and its main instrument eROSITA will conduct a survey of all X-ray sources in the sky 20 times more sensitive than the previous one (ROSAT, twenty years ago). The NICER detector will reach the ISS in October 2016 to study the X-ray emission of neutron stars. Starting from 2021 the French-Chinese SVOM mission will relay Swift to monitor the sky in hard X-rays to search for gamma-ray bursts and other transient sources. In 2014, ESA has selected the next large X-ray observatory ATHENA for launch in 2028. This is the next-generation multi-purpose X-ray observatory, successor to XMM-Newton, launched in 1999. In this evolving context it is the right time to take stock of the prospects in X-ray astronomy. |
Training goals A survey on the occasion
of the recent CNES prospective (Dubus et al 2014)
has shown a growing interest in X-rays from communities that are not
frequent X-ray observers, but for which X-rays are an important
complement. This school should meet their expectations by showing the
type of diagnostics that can be obtained in X-rays, how to analyze data
to achieve it, and what are the current and future instrumental
opportunities. Our aim is that X-ray astronomy can optimize use of
observatories at other wavelengths (Herschel, ALMA, VLT) or beyond
electromagnetism (VIRGO/LIGO, ICECUBE/KM3Net), insofar as understanding
a source requires its broadband spectrum, including X-rays.
This school is primarily targeted at scientists, post-doctoral fellows and PhD students in the fields of astroparticle physics, astronomy, theoretical physics and high energy physics, willing to acquire complementary skills and/or to change their research topic. Scientists from other fields are welcome if the topic appeals to them. A PhD level either in Astronomy, Astrophysics, Theoretical Physics or Particle Physics.
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PHYSICS Radiative mechanisms, thermal process of transfer and absorption | Accretion/ejection flows associated with stellar black holes | Super massive black holes | Neutron stars, pulsars, PWNe, magnetars | Supernovae, supernova remnants, hot interstellar medium | GRBs | Fundamental Physics | Galaxy clusters, the cosmological aspects | Radiative mechanisms, thermal process, transfer and absorption DATA ANALYSIS Catalogs, archives | Imaging | Spectroscopy | Variability INSTRUMENT ON PRESENT AND FUTURE X-ray telescopes (general principles and specific solutions for high-resolution, surface area, high power) | Collimators hubs and associated detectors | Coded masks and sky monitoring | Semiconductor detectors (CCD, DePFETs) | Spectroscopy (networks, bolometers) | Polarimetry |
X-ray Astronomy * Black Holes * Gamma-ray bursts * Galaxies clusters * Supernovæ * Astrophysical jets * Neutrons stars * Fundamental Physics |
Jean Ballet (IRFU/CEA), Michel Boer
(ARTEMIS), Josè Busto(CPPM), Paschal Coyle (CPPM), Bernard Degrange (LLR), Yves Gallant (LUPM), Berrie Giebels
(LLR), René Goosmann (UNISTRA), Stavros Katsanevas (APC), Jürgen Knödlseder (IRAP), Julien Lavalle (LUPM), Benoit Lott (CENBG), Jean Orloff (LPC CLERMONT), Etienne Parizot (APC), Guy Pelletier (IPAG), Pierre Salati (LAPTH), Roland Triay (CPT)
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