{"content":[{"text":"4Laboratoire de Physique des 2 Inﬁnis Irène Joliot-Curie (CNRS-IN2P3, Université Paris-Saclay), \n France \n 5Università degli studi di Milano, Milano, Italy \n 6INFN sezione di Milano, 20133 Milano, Italy \n 7National University of Ireland, Maynooth, Ireland \n 8Cardiﬀ University, UK \n 9INFN sezione di Pisa, 56127 Pisa, Italy \n 10Observatoire de Paris, Université Paris Science et Lettres, F-75014 Paris, France \n 11Università di Milano - Bicocca, Milano, Italy \n 12INFN sezione di Milano - Bicocca, 20216 Milano, Italy \n 13GEMA (Universidad Nacional de La Plata), Argentina \n 14Instituto de Tecnologías en Detección y Astropartículas (CNEA, CONICET, UNSAM), Argentina \n 15Centro Atómico Bariloche and Instituto Balseiro (CNEA), Argentina \n 16Institut de Recherche en Astrophysique et Planétologie, Toulouse (CNRS-INSU), France \n 17Department of Physics, University of Oxford, UK \n 18Centre de Nanosciences et de Nanotechnologies, Orsay, France \n 19Centro Atómico Constituyentes (CNEA), Argentina \n 20University of Richmond, Richmond, USA \n 21Università di Roma “Tor Vergata”, Roma, Italy \n 22INFN sezione di Roma2, 00133 Roma, Italy \n 23University of Surrey, UK \n 24Facultad de Ciencias Astronómicas y Geofísicas (Universidad Nacional de La Plata), Argentina \n 25University of Manchester, UK \n 26Escuela de Ciencia y Tecnología (UNSAM) and Centro Atómico Constituyentes (CNEA), Argentina \n 27IRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, France \n 28Institut d’Astrophysique Spatiale, Orsay (CNRS-INSU), France \n 29Italian Space Agency, Roma, Italy \n 30Pontiﬁcia Universidad Catolica de Chile, Chile \n 31Instituto Argentino de Radioastronomía (CONICET, CIC, UNLP), Argentina \n 32California Institute of Technology, USA \n 33CONICET, Argentina \n 34Institute of Technology, Carlow, Ireland \n 35University of Wisconsin, Madison, USA \n 36Brown University, Providence, USA \n E-mail: giuseppe.dalessandro@uniroma1.it, lorenzo.mele@roma1.infn.it, \n fabio.columbro@roma1.infn.it \n Abstract. \n Inﬂation Gravity Waves B-Modes polarization detection is the ultimate goal of modern large \n angular scale cosmic microwave background (CMB) experiments around the world. A great eﬀort \n is being spent in the deployment of many ground-based, balloon-borne and satellite experiments \n using diﬀerent methods to separate this faint polarized component from the incoming radiation. \n One of the largely used technique is the Stokes Polarimetry that uses a rotating half-wave plate and","bbox":{"left":0.141817,"top":0.099232,"width":0.73729,"height":0.74985}}],"images_bbox":[],"images_bbox_not_text_overlap":[]}