The MUSE Deep Lensed Field on the Hubble Frontier Field MACS~J0416. (arXiv:2009.08458v1 [astro-ph.GA])

The MUSE Deep Lensed Field on the Hubble Frontier Field MACS~J0416. (arXiv:2009.08458v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Vanzella_E/0/1/0/all/0/1">E. Vanzella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caminha_G/0/1/0/all/0/1">G. B. Caminha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosati_P/0/1/0/all/0/1">P. Rosati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mercurio_A/0/1/0/all/0/1">A. Mercurio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Castellano_M/0/1/0/all/0/1">M. Castellano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meneghetti_M/0/1/0/all/0/1">M. Meneghetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grillo_C/0/1/0/all/0/1">C. Grillo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sani_E/0/1/0/all/0/1">E. Sani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bergamini_P/0/1/0/all/0/1">P. Bergamini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calura_F/0/1/0/all/0/1">F. Calura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caputi_K/0/1/0/all/0/1">K. Caputi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cristiani_S/0/1/0/all/0/1">S. Cristiani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cupani_G/0/1/0/all/0/1">G. Cupani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fontana_A/0/1/0/all/0/1">A. Fontana</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gilli_R/0/1/0/all/0/1">R. Gilli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grazian_A/0/1/0/all/0/1">A. Grazian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gronke_M/0/1/0/all/0/1">M. Gronke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mignoli_M/0/1/0/all/0/1">M. Mignoli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nonino_M/0/1/0/all/0/1">M. Nonino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pentericci_L/0/1/0/all/0/1">L. Pentericci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tozzi_P/0/1/0/all/0/1">P. Tozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Treu_T/0/1/0/all/0/1">T. Treu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Balestra_I/0/1/0/all/0/1">I. Balestra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dijkstra_M/0/1/0/all/0/1">M. Dijkstra</a>

Context: A census of faint and tiny star forming complexes at high redshift
is key for the understanding of the reionizing sources, galaxy growth and the
formation of globular clusters. Aims: We present the MUSE deep lensed field
(MDLF) program. Methods: Deep MUSE observations of 17.1 hours integration on a
single pointing over the Hubble Frontier Field galaxy cluster MACS~J0416 are
described. Results: We confirm 182 multiple images in the redshift range
0.9<z<6.6 (from the previously known 102), emerging from 66 families drawn from
48 individual background sources. We identify 116 clumps belonging to
background high-z galaxies; the majority of them are multiple images and span
magnitude, size and redshift intervals of [-18,-10], [~400-3] parsec and
1<z<6.6, respectively, with the faintest and/or most magnified ones probing
possible single gravitationally-bound star clusters. The depth of the MDLF
combined with lensing magnification lead us to reach a detection limit for
unresolved emission lines of a few 10$^{-20}$ erg/s/cm2, after correction for
lensing magnification. Ultraviolet high-ionization metal lines (and HeII1640)
are detected with S/N>10 for individual objects down to de-lensed magnitude
28-30 suggesting that they are common in such faint sources. Conclusions:Deep
MUSE observations, in combination with existing HST imaging, allowed us to: (1)
confirm redshifts for extremely faint high-z sources; (2) peer into their
internal clumps (down to 100-200 pc scale); (3) in some cases break down such
clumps into bound star clusters (<25 pc scale); (4) double the number of
constraints for the lens model, reaching an unprecedented set of 182 bona-fide
multiple images and confirming up to 213 galaxy cluster members. These results
demonstrate the power that JWST and future ELTs will have when combined to
study gravitational telescopes.[abridged]

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