SDSS-V
I have a number of funded projects related to each of the SDSS-V Mappers, including both data analysis (intended for research publications) and data visualization (for webapp and api development) and data software frameworks (to prepare for future data releases).

Milky Way Mapper (MWM)

MWM is a multi-object spectroscopic survey to obtain near-infrared and/or optical spectra of more than 4 million stars throughout the Milky Way and Local Group. The stellar parameters and elemental abundances derived from these data will enable a unique global map of the Milky Way’s fossil records that survive in its stars and interstellar material. The entire hierarchy of structure and chemo-dynamical patterns will be sampled throughout the disk- and bulge-dominated regions of the Milky Way. The data collected from both Apache Point Observatory, New Mexico and Las Campanas Observatory, Chile will allow us to test models of galaxy formation.

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Black Hole Mapper (BHM)

BHM is a multi-object spectroscopic survey that emphasizes optical spectra (often also with multiple epochs of spectrosopy) for more than 300,000 quasars to jointly understand the masses, accretion physics, and growth and evolution over cosmic time of supermassive black holes, and will take observations on the 2.5m telescopes at both Apache Point Observatory, New Mexico and Las Campanas Observatory, Chile.

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Local Volume Mapper (LVM)

LVM is an optical, integral-field spectroscopic survey that will target the Milky Way, Small and Large Magellanic Clouds, and other Local Volume galaxies, and will collect ~20 million contiguous spectra over 2,500 square degrees of sky, including the midplane of the Milky Way, Orion, and the Magellanic Clouds from Las Campanas Observatory, Chile.

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SDSS-V White Paper:
 arXiv:1711.03234
 337 Citations
SDSS-V: Pioneering Panoptic Spectroscopy
SDSS-V will be an all-sky, multi-epoch spectroscopic survey of over six million objects. It is designed to decode the history of the Milky Way, trace the emergence of the chemical elements, reveal the inner workings of stars, and investigate the origin of planets. It will also create an integral-field spectroscopic map of the gas in the Galaxy and the Local Group that is 1,000x larger than the current state of the art and at high enough spatial resolution to reveal the self-regulation mechanisms of galactic ecosystems. SDSS-V will pioneer systematic, spectroscopic monitoring across the whole sky, revealing changes on timescales from 20 minutes to 20 years. The survey will thus track the flickers, flares, and radical transformations of the most luminous persistent objects in the universe: massive black holes growing at the centers of galaxies. The scope and flexibility of SDSS-V will be unique among extant and future spectroscopic surveys: it is all-sky, with matched survey infrastructures in both hemispheres; it provides near-IR and optical multi-object fiber spectroscopy that is rapidly reconfigurable to serve high target densities, targets of opportunity, and time-domain monitoring; and it provides optical, ultra-wide-field integral field spectroscopy. SDSS-V, with its programs anticipated to start in 2020, will be well-timed to multiply the scientific output from major space missions (e.g., TESS, Gaia, eROSITA) and ground-based projects. SDSS-V builds on the 25-year heritage of SDSS's advances in data analysis, collaboration infrastructure, and product deliverables. The project is now refining its science scope, optimizing the survey strategies, and developing new hardware that builds on the SDSS-IV infrastructure. We present here an overview of the current state of these developments as we seek to build our worldwide consortium of institutional and individual members.

SDSS-V Schematic (Image From Mark Seibert)
SDSS-V Schematic