X-RAY INTERACTION WITH MATTER. COLLIMATE OR NOT TO COLLIMATE?! SCATTER.
Maria Grazia Pia, INFN Genova Precision Electromagnetic Physics in Geant4: the Atomic Relaxation Models A. Mantero, B. Mascialino, Maria Grazia Pia, S.
Nuclear physics experiments for the astrophysical p process A. Sauerwein, IKP, Universität zu Köln, AG Zilges A. Sauerwein*, J. Hasper, A. Hennig*, L.
Image quality and spectroscopic characteristics of different silicon pixel imaging systems M. G. Bisogni, D.Bulajic, M. Boscardin, G. F. Dalla Betta, P.
EROSITA: The German Quest for Galaxy Clusters Christian Schmid & Ingo Kreykenbohm Dr. Remeis-Sternwarte Bamberg / ECAP Tautenburg, May 03, 2013 on behalf.
D retention in O-covered and pure beryllium Motivation Experimental results Interpretation 1.Retention 2.Sample characterisation 3.Mechanisms Outlook Outline:
The EDELWEISS-II experiment Silvia SCORZA Université Claude Bernard- Institut de Physique nucléaire de Lyon CEA-Saclay DAPNIA/DRECAM (FRANCE), CNRS/CRTBT.
Radiation Protection Service University of Glasgow Lecture 2: Detecting Radiation Detecting Ionising Radiation James Gray University RPA.
Objectives By the end of this section you should: understand the concept of diffraction in crystals be able to derive and use Braggs law know how X-rays.
Why diffraction? Learning Outcomes By the end of this section you should: understand what we are looking at with diffraction and why we need diffraction.
Pulsars High Energy Astrophysics [email protected]
UK HEP Forum, May 03 UKDMC - roland lüscher - RAL/PPD Double Beta Potential of Zeplin Zeplin: brief summary of DM programme Doing bb-search with a DM detector?