The MAGPI Survey — science goals, design, observing strategy, early results and theoretical framework. (arXiv:2011.13567v2 [astro-ph.GA] UPDATED)

The MAGPI Survey — science goals, design, observing strategy, early results and theoretical framework. (arXiv:2011.13567v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Foster_C/0/1/0/all/0/1">C. Foster</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mendel_J/0/1/0/all/0/1">J. T. Mendel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lagos_C/0/1/0/all/0/1">C. D. P. Lagos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wisnioski_E/0/1/0/all/0/1">E. Wisnioski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yuan_T/0/1/0/all/0/1">T. Yuan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DEugenio_F/0/1/0/all/0/1">F. D'Eugenio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Barone_T/0/1/0/all/0/1">T. M. Barone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harborne_K/0/1/0/all/0/1">K. E. Harborne</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vaughan_S/0/1/0/all/0/1">S. P. Vaughan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schulze_F/0/1/0/all/0/1">F. Schulze</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Remus_R/0/1/0/all/0/1">R.-S. Remus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gupta_A/0/1/0/all/0/1">A. Gupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Collacchioni_F/0/1/0/all/0/1">F. Collacchioni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khim_D/0/1/0/all/0/1">D. J. Khim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taylor_P/0/1/0/all/0/1">P. Taylor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bassett_R/0/1/0/all/0/1">R. Bassett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Croom_S/0/1/0/all/0/1">S. M. Croom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McDermid_R/0/1/0/all/0/1">R. M. McDermid</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Poci_A/0/1/0/all/0/1">A. Poci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battisti_A/0/1/0/all/0/1">A. J. Battisti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bland_Hawthorn_J/0/1/0/all/0/1">J. Bland-Hawthorn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bellstedt_S/0/1/0/all/0/1">S. Bellstedt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Colless_M/0/1/0/all/0/1">M. Colless</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Davies_L/0/1/0/all/0/1">L. J. M. Davies</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Driver_S/0/1/0/all/0/1">S. Driver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferre_Mateu_A/0/1/0/all/0/1">A. Ferré-Mateu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fisher_D/0/1/0/all/0/1">D. B. Fisher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gjergo_E/0/1/0/all/0/1">E. Gjergo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnston_E/0/1/0/all/0/1">E. J. Johnston</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khalid_A/0/1/0/all/0/1">A. Khalid</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kobayashi_C/0/1/0/all/0/1">C. Kobayashi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Oh_S/0/1/0/all/0/1">S. Oh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peng_Y/0/1/0/all/0/1">Y. Peng</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Robotham_A/0/1/0/all/0/1">A. S. G. Robotham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sweet_S/0/1/0/all/0/1">S. M. Sweet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Taylor_E/0/1/0/all/0/1">E. N. Taylor</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tran_K/0/1/0/all/0/1">K.-V. H. Tran</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Trayford_J/0/1/0/all/0/1">J. W. Trayford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sande_J/0/1/0/all/0/1">J. van de Sande</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yi_S/0/1/0/all/0/1">S. K. Yi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zanisi_L/0/1/0/all/0/1">L. Zanisi</a>

We present an overview of the Middle Ages Galaxy Properties with Integral
Field Spectroscopy (MAGPI) survey, a Large Program on the European Southern
Observatory Very Large Telescope. MAGPI is designed to study the physical
drivers of galaxy transformation at a lookback time of 3-4 Gyr, during which
the dynamical, morphological, and chemical properties of galaxies are predicted
to evolve significantly. The survey uses a combination of new medium-deep
adaptive optics aided Multi Unit Spectroscopic Explorer (MUSE) observations and
publicly available ultraviolet-to-infrared imaging from the Galaxy And Mass
Assembly (GAMA) survey. With these data, MAGPI will map the kinematic and
chemical properties of stars and ionised gas for a sample of 60 massive ($> 7
times 10^{10} M_odot$) central galaxies at $0.25 < z <0.35$ in a
representative range of environments. The spatial resolution delivered by MUSE
with Ground Layer Adaptive Optics (GLAO, $0.6-0.8$ arcsec FWHM) will facilitate
a direct comparison with Integral Field Spectroscopy surveys of the nearby
Universe, such as SAMI and MaNGA, and at higher redshifts using adaptive
optics. In addition to the primary (central) galaxy sample, MAGPI will deliver
resolved and unresolved spectra for as many as 150 satellite galaxies at $0.25
< z <0.35$, as well as hundreds of emission-line sources at $z < 6$. This paper
outlines the science goals, survey design, and observing strategy of MAGPI. We
also present a first look at the MAGPI data, and the theoretical framework to
they will be compared using the current generation of cosmological
hydrodynamical simulations. Our results show that cosmological hydrodynamical
simulations make discrepant predictions in the spatially resolved properties of
galaxies at $zapprox 0.3$. MAGPI observations will place new constraints and
allow for tangible improvements in galaxy formation theory.

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