SDSS-V : The Local Volume Mapper A panchromatic 1-steradian IFU survey of sub-parsec Starformation
E. Pellegrini, N. Drory, J. Kollmeier, G. Blan, K. Kreckle
Universitat Heidelber, McDonald Observatory, Carnegie, Carnegie, Universitat Heidelberg
It is clear that the feedback from recently formed stars to the surrounding interstellar medium must be a central regulatory process in galaxy formation. But by what processes, over what time- and length-scales actually transfer energy and momentum from young stars (and supernovae) to the gas is inarguably less well-understood than the dark-matter driven hierarchical assembly dynamics of galaxies. The ideal observational basis to tackle this fundamental problem of galaxy formation would be a contiguous and high-resolution map of the gas' physical state and kinematics across an entire galaxy, along with a comprehensive mapping of the individual young and energetic stars: this is what SDSS-V's Local Volume Mapper (LVM) sets out to do for the Milky Way and Magellanic Clouds. LVM will directly probe the physical scales from which the global correlations arise, to witness the physics of galaxy formation at the ``energy injection scale''. The LVM move us towards the ``spectral panopticon'', a full spectroscopic image of the sky, resolving SF structures, GMCs, HII regions and young stellar clusters, over the bulk of the MW disk at 0.1-1~pc resolution, the Magellanic Clouds at 10~pc resolution using ~4000, fiber-fed, IFU spectrographs covering the full optical wavelength range. These clusters will be fed by a suite of small to medium aperture telescopes with very wide field-of-view (FOV) the southern hemispheres. LVM's coverage of ~3000 sqrdeg in the Milky Way, and 100 sqrdeg in the Magellanic Clouds is 3--4 orders of magnitude larger than any existing IFU dataset. Combined with the information on young stars from existing photometric surveys for the local group, we can map, model, and understand where the feedback energy and momentum are produced and where they are absorbed, with observations on the critical sub-parsec-scales.