Probing the cold magnetized Universe with SPICA-POL (B-BOP). (arXiv:1905.03520v1 [astro-ph.GA])

Probing the cold magnetized Universe with SPICA-POL (B-BOP). (arXiv:1905.03520v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Andre_P/0/1/0/all/0/1">Ph. André</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_A/0/1/0/all/0/1">A. Hughes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guillet_V/0/1/0/all/0/1">V. Guillet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boulanger_F/0/1/0/all/0/1">F. Boulanger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bracco_A/0/1/0/all/0/1">A. Bracco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ntormousi_E/0/1/0/all/0/1">E. Ntormousi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arzoumanian_D/0/1/0/all/0/1">D. Arzoumanian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maury_A/0/1/0/all/0/1">A.J. Maury</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernard_J/0/1/0/all/0/1">J.-Ph. Bernard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bontemps_S/0/1/0/all/0/1">S. Bontemps</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ristorcelli_I/0/1/0/all/0/1">I. Ristorcelli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Girart_J/0/1/0/all/0/1">J.M. Girart</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Motte_F/0/1/0/all/0/1">F. Motte</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tassis_K/0/1/0/all/0/1">K. Tassis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pantin_E/0/1/0/all/0/1">E. Pantin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Montmerle_T/0/1/0/all/0/1">T. Montmerle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnstone_D/0/1/0/all/0/1">D. Johnstone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gabici_S/0/1/0/all/0/1">S. Gabici</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Efstathiou_A/0/1/0/all/0/1">A. Efstathiou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basu_S/0/1/0/all/0/1">S. Basu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bethermin_M/0/1/0/all/0/1">M. Béthermin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beuther_H/0/1/0/all/0/1">H. Beuther</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Braine_J/0/1/0/all/0/1">J. Braine</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Francesco_J/0/1/0/all/0/1">J. Di Francesco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Falgarone_E/0/1/0/all/0/1">E. Falgarone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferriere_K/0/1/0/all/0/1">K. Ferrière</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fletcher_A/0/1/0/all/0/1">A. Fletcher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Galametz_M/0/1/0/all/0/1">M. Galametz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giard_M/0/1/0/all/0/1">M. Giard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hennebelle_P/0/1/0/all/0/1">P. Hennebelle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_A/0/1/0/all/0/1">A. Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kepley_A/0/1/0/all/0/1">A.A. Kepley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kwon_J/0/1/0/all/0/1">J. Kwon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lagache_G/0/1/0/all/0/1">G. Lagache</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lesaffre_P/0/1/0/all/0/1">P. Lesaffre</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Levrier_F/0/1/0/all/0/1">F. Levrier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_D/0/1/0/all/0/1">D. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_Z/0/1/0/all/0/1">Z.-Y. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mao_S/0/1/0/all/0/1">S.A. Mao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nakagawa_T/0/1/0/all/0/1">T. Nakagawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Onaka_T/0/1/0/all/0/1">T. Onaka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Paladino_R/0/1/0/all/0/1">R. Paladino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peretto_N/0/1/0/all/0/1">N. Peretto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poglitsch_A/0/1/0/all/0/1">A. Poglitsch</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reveret_V/0/1/0/all/0/1">V. Revéret</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodriguez_L/0/1/0/all/0/1">L. Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sauvage_M/0/1/0/all/0/1">M. Sauvage</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soler_J/0/1/0/all/0/1">J.D. Soler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spinoglio_L/0/1/0/all/0/1">L. Spinoglio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tabatabaei_F/0/1/0/all/0/1">F. Tabatabaei</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tritsis_A/0/1/0/all/0/1">A. Tritsis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tak_F/0/1/0/all/0/1">F. van der Tak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ward_Thompson_D/0/1/0/all/0/1">D. Ward-Thompson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wiesemeyer_H/0/1/0/all/0/1">H. Wiesemeyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ysard_N/0/1/0/all/0/1">N. Ysard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_H/0/1/0/all/0/1">H. Zhang</a>

SPICA, the cryogenic infrared space telescope recently pre-selected for a
`Phase A’ concept study as one of the three remaining candidates for ESA’s
fifth medium class (M5) mission, is foreseen to include a far-infrared
polarimetric imager (SPICA-POL, now called B-BOP), which would offer a unique
opportunity to resolve major issues in our understanding of the nearby, cold
magnetized Universe. This paper presents an overview of the main science
drivers for B-BOP, including high dynamic range polarimetric imaging of the
cold interstellar medium (ISM) in both our Milky Way and nearby galaxies.
Thanks to a cooled telescope, B-BOP will deliver wide-field 100-350 micron
images of linearly polarized dust emission in Stokes Q and U with a resolution,
signal-to-noise ratio, and both intensity and spatial dynamic ranges comparable
to those achieved by Herschel images of the cold ISM in total intensity (Stokes
I). The B-BOP 200 micron images will also have a factor ~30 higher resolution
than Planck polarization data. This will make B-BOP a unique tool for
characterizing the statistical properties of the magnetized interstellar medium
and probing the role of magnetic fields in the formation and evolution of the
interstellar web of dusty molecular filaments giving birth to most stars in our
Galaxy. B-BOP will also be a powerful instrument for studying the magnetism of
nearby galaxies and testing galactic dynamo models, constraining the physics of
dust grain alignment, informing the problem of the interaction of cosmic rays
with molecular clouds, tracing magnetic fields in the inner layers of
protoplanetary disks, and monitoring accretion bursts in embedded protostars.

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