Talk detail

Participant	Zannoni, Mario
Institution	University of Milano Bicocca - Piazza della Scienza, 3 - Milano - - Italy

Session	CM5	Accepted	Yes	Order	3	Time	16:15	30'
Talk	Oral abstract	Title	The LSPE/STRIP project
Coauthors	Mario Zannoni, Giuseppe Addamo, Alessandro Ba, Paola M. Battaglia, Marco Bersanelli, Barbara Caccianiga, Silvia Caprioli, Francesco Cavaliere, Kieran A. Cleary, Francesco Cuttaia, Francesco Del Torto, Viviana Fafone, Cristian Franceschet, Ricardo T. GŽnova Santos, Todd C. Gaier, Massimo Gervasi, Federico Incardona, Simone Iovenitti, Mike Jones, Pekka Kangaslahti, Roberto Mainini, Davide Maino, Michele Maris, Patricio Mena, Aniello Mennella, Roc’o Molina, Gianluca Morgante, Andrea Passerini, Maria del Rosario Perez-de-Taoro, Oscar A. Peverini, Federico Pezzotta, Claudio Pincella, Sabrina Realini, Nicol‡s Reyes, Alessio Rocchi, JosŽ A. Rubi–o-Mart’n, Maura Sandri, Stefano Sartor, Mary Soria, Valeria Tapia, Luca Terenzi, Maurizio Tomasi, Elisabetta Tommasi, Daniele M. Vigan—, Fabrizio Villa, Giuseppe Virone, Angela Volpe, Bob Watkins, Andrea Zacchei
Abstract	We present here the status of the low frequency instrument (STRIP) of the Large Scale Polarization Explorer (LSPE). LSPE is a project that combines ground-based (STRIP) and balloon-borne (SWIPE) polarization measurements of the microwave sky on large angular scales, trying to detect the primordial ÒB-modesÓ of the Cosmic Microwave Background. STRIP will observe approximately 25% of the Northern sky from the Tenerife site in Canary Island, using an array of forty-nine cryogenic coherent polarimeters at 43 GHz, coupled to a 1.5 m telescope in crossed Dragone configuration. A second frequency channel with six-elements at 95 GHz will be exploited mainly as an atmospheric monitor. STRIP will be able to continuously spin around the azimuth azis at different elevations to reach the sky coverage and the celestial calibrators. The sensitivity of the two instruments, together with an efficient scanning strategy and an effective component separation, will allow us to constrain the tensor-to-scalar ratio to about 0.03.
Pdf file