HIGH-Z & MULTI-Λ

Multi-wavelength study of accretion onto black holes and its evolution during cosmic times

Coordinatore	MAX PLANCK GESELLSCHAFT ZUR FOERDERUNG DER WISSENSCHAFTEN E.V.    more  Organization address address: Hofgartenstrasse 8 city: MUENCHEN postcode: 80539 contact info Titolo: Mr. Nome: Bernhard Cognome: Scheiner Email: send email Telefono: 4989300000000 Fax: 4989300000000
Nazionalità Coordinatore	Germany [DE]
Totale costo	161˙968 €
EC contributo	161˙968 €
Programma	FP7-PEOPLE Specific programme "People" implementing the Seventh Framework Programme of the European Community for research, technological development and demonstration activities (2007 to 2013)
Code Call	FP7-PEOPLE-2012-IEF
Funding Scheme	MC-IEF
Anno di inizio	2013
Periodo (anno-mese-giorno)	2013-03-01   -   2015-02-28

 Partecipanti

#	participant	country	role	EC contrib. [€]
1	MAX PLANCK GESELLSCHAFT ZUR FOERDERUNG DER WISSENSCHAFTEN E.V.  Organization address address: Hofgartenstrasse 8 city: MUENCHEN postcode: 80539 contact info Titolo: Mr. Nome: Bernhard Cognome: Scheiner Email: send email Telefono: 4989300000000 Fax: 4989300000000	DE (MUENCHEN)	coordinator	161˙968.80

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 Obiettivo del progetto (Objective)

'The beginning of this century can be considered a golden age for X-ray astronomy, with the launch of XMM-Newton, Chandra and Suzaku, three cornerstones of the ESA, NASA and JAXA space programs. These observatories, although more than 10yr old, still deliver excellent science and X-ray astronomy now leads many fields of astronomical investigation. However, only small-medium class X-ray missions are planned to be launched in the next 10-15yr, thus shrinking the space for new discoveries in X-rays alone. The two years at MPE will allow to diversify my scientific expertise by: i) expanding my research field into: a) Optical-Infra Red (IR) bands; b) evolution of Active Galactic Nuclei (AGN) variability through cosmic time; ii) being granted access to Optical-IR facilities and new X-ray missions. The proposed project will allow to: 1) measure the evolution of AGN variability over cosmic time using large AGN samples, thus also assessing whether AGN can be used as standard candles; 2) measure SgrA*'s duty cycle, its past activity, the Molecular Cloud (MC) Galactic Center (GC) distribution, the level of GC cosmic rays, the irradiation induced MC chemistry; 3) if SgrA* will go into outburst (a gas cloud will reach SgrA* in mid 2013) we will lead the X-ray investigation of this major event (e.g. the switching on of an AGN, jet-disc creation) that will remain in astronomy records; 4) link (thanks to NuSTAR, the new NASA X-ray mission) the variability properties of the Compton reflection hump, the FeK line and the soft excess in AGN, to finally understand the origin of these components; 5) monitoring the evolution of the cross-correlation function and the spectral energy distribution, during an entire Galactic Black Hole (GBH) outburst, to echo-map and determine the transformation of the disc-jet-corona system geometry; 6) understand if GBH winds can keep the alpha-disc stable, constrain the connections between wind-jet-state in GBH and the connections between GBH and AGN winds.'