BlueMUSE: Project Overview and Science Cases. (arXiv:1906.01657v1 [astro-ph.IM])

BlueMUSE: Project Overview and Science Cases. (arXiv:1906.01657v1 [astro-ph.IM])
<a href="http://arxiv.org/find/astro-ph/1/au:+Richard_J/0/1/0/all/0/1">Johan Richard</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Bacon_R/0/1/0/all/0/1">Roland Bacon</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Blaizot_J/0/1/0/all/0/1">Jérémy Blaizot</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Boissier_S/0/1/0/all/0/1">Samuel Boissier</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Boselli_A/0/1/0/all/0/1">Alessandro Boselli</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+NicolasBouch%5C%27e/0/1/0/all/0/1">NicolasBouché</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Brinchmann_J/0/1/0/all/0/1">Jarle Brinchmann</a> (3,4), <a href="http://arxiv.org/find/astro-ph/1/au:+Castro_N/0/1/0/all/0/1">Norberto Castro</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Ciesla_L/0/1/0/all/0/1">Laure Ciesla</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Crowther_P/0/1/0/all/0/1">Paul Crowther</a> (6), <a href="http://arxiv.org/find/astro-ph/1/au:+Daddi_E/0/1/0/all/0/1">Emanuele Daddi</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Dreizler_S/0/1/0/all/0/1">Stefan Dreizler</a> (8), <a href="http://arxiv.org/find/astro-ph/1/au:+Duc_P/0/1/0/all/0/1">Pierre-Alain Duc</a> (9), <a href="http://arxiv.org/find/astro-ph/1/au:+Elbaz_D/0/1/0/all/0/1">David Elbaz</a> (7), <a href="http://arxiv.org/find/astro-ph/1/au:+Epinat_B/0/1/0/all/0/1">Benoit Epinat</a> (2), <a href="http://arxiv.org/find/astro-ph/1/au:+Evans_C/0/1/0/all/0/1">Chris Evans</a> (10), <a href="http://arxiv.org/find/astro-ph/1/au:+Fossati_M/0/1/0/all/0/1">Matteo Fossati</a> (11), <a href="http://arxiv.org/find/astro-ph/1/au:+Fumagalli_M/0/1/0/all/0/1">Michele Fumagalli</a> (11), <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_M/0/1/0/all/0/1">Miriam Garcia</a> (12), <a href="http://arxiv.org/find/astro-ph/1/au:+Garel_T/0/1/0/all/0/1">Thibault Garel</a> (1,13), <a href="http://arxiv.org/find/astro-ph/1/au:+Hayes_M/0/1/0/all/0/1">Matthew Hayes</a> (14), <a href="http://arxiv.org/find/astro-ph/1/au:+Herrero_A/0/1/0/all/0/1">Artemio Herrero</a> (15,16), <a href="http://arxiv.org/find/astro-ph/1/au:+Humphrey_A/0/1/0/all/0/1">Andrew Humphrey</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Jablonka_P/0/1/0/all/0/1">Pascale Jablonka</a> (17), <a href="http://arxiv.org/find/astro-ph/1/au:+Kamann_S/0/1/0/all/0/1">Sebastian Kamann</a> (18), <a href="http://arxiv.org/find/astro-ph/1/au:+Kaper_L/0/1/0/all/0/1">Lex Kaper</a> (19), <a href="http://arxiv.org/find/astro-ph/1/au:+Kelz_A/0/1/0/all/0/1">Andreas Kelz</a> (5), <a href="http://arxiv.org/find/astro-ph/1/au:+Kneib_J/0/1/0/all/0/1">Jean-Paul Kneib</a> (17), <a href="http://arxiv.org/find/astro-ph/1/au:+Koter_A/0/1/0/all/0/1">Alex de Koter</a> (19,20), <a href="http://arxiv.org/find/astro-ph/1/au:+Kudritzki_R/0/1/0/all/0/1">Rolf-Peter Kudritzki</a> (21), <a href="http://arxiv.org/find/astro-ph/1/au:+Langer_N/0/1/0/all/0/1">Norbert Langer</a> (22), <a href="http://arxiv.org/find/astro-ph/1/au:+Lardo_C/0/1/0/all/0/1">Carmela Lardo</a> (17), <a href="http://arxiv.org/find/astro-ph/1/au:+Leclercq_F/0/1/0/all/0/1">Floriane Leclercq</a> (13), <a href="http://arxiv.org/find/astro-ph/1/au:+Lennon_D/0/1/0/all/0/1">Danny Lennon</a> (15), <a href="http://arxiv.org/find/astro-ph/1/au:+Mahler_G/0/1/0/all/0/1">Guillaume Mahler</a> (23), <a href="http://arxiv.org/find/astro-ph/1/au:+Martins_F/0/1/0/all/0/1">Fabrice Martins</a> (24), <a href="http://arxiv.org/find/astro-ph/1/au:+Massey_R/0/1/0/all/0/1">Richard Massey</a> (11), <a href="http://arxiv.org/find/astro-ph/1/au:+Mitchell_P/0/1/0/all/0/1">Peter Mitchell</a> (4), et al. (21 additional authors not shown)

We present the concept of BlueMUSE, a blue-optimised, medium spectral
resolution, panoramic integral field spectrograph based on the MUSE concept and
proposed for the Very Large Telescope. With an optimised transmission down to
350 nm, a larger FoV (1.4 x 1.4 arcmin$^2$) and a higher spectral resolution
compared to MUSE, BlueMUSE will open up a new range of galactic and
extragalactic science cases allowed by its specific capabilities, beyond those
possible with MUSE. For example a survey of massive stars in our galaxy and the
Local Group will increase the known population of massive stars by a factor
$>$100, to answer key questions about their evolution. Deep field observations
with BlueMUSE will also significantly increase samples of Lyman-alpha emitters,
spanning the era of Cosmic Noon. This will revolutionise the study of the
distant Universe: allowing the intergalactic medium to be detected
unambiguously in emission, enabling the study of the exchange of baryons
between galaxies and their surroundings. By 2030, at a time when the focus of
most of the new large facilities (ELT, JWST) will be on the infra-red, BlueMUSE
will be a unique facility, outperforming any ELT instrument in the Blue/UV. It
will have a strong synergy with ELT, JWST as well as ALMA, SKA, Euclid and
Athena.

http://arxiv.org/icons/sfx.gif