SDSS-V: Pioneering Panoptic Spectroscopy

By Juna A. Kollmeier, G. Zasowski, Hans-Walter Rix, M. Johns, S. Anderson, N. Drory, Jennifer A. Johnson, R. Pogge, J. Bird, G. Blanc and 40 more. 2017

188 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Yule-Simpson’s paradox in Galactic Archaeology (2019, methodology): “We expect to get those form the K2 (Howell et al. 2014), TESS (Ricker et al. 2015) and PLATO (Rauer et al. 2014) asteroseismic missions in the near future, as well as isochrone age determination from spectroscopic surveys, such as GALAH (De Silva et al. 2015), Gaia-ESO (Gilmore et al. 2012), APOGEE,”
The GALAH+ survey: Third data release (2020, background): “Upcoming surveys like SDSS-V (Kollmeier et al. 2017), WEAVE (Dalton et al. 2018), 4MOST (de Jong et al. 2019), and PFS (Takada et al. 2014) will certainly continue to broaden our capabilities and understanding surrounding our galaxy’s physical and chemical evolution.”
The Payne: Self-consistent ab initio Fitting of Stellar Spectra (2018, unknown): “…surveys, such as DESI (DESI Collaboration et al. 2016), 4MOST (de Jong et al. 2014), WEAVE (Dalton et al. 2016), MOONS (Cirasuolo et al. 2014), and SDSS-V (Kollmeier et al. 2017), will boost sample sizes at both high and low spectral resolution by another order of magnitude, toward ∼107 stars.”
The GALAH Survey: Second Data Release (2018, background): “Several even larger highresolution spectroscopic surveys of the Milky Way are expected to commence over the next decade, including WEAVE (Dalton et al. MNRAS 000, 1–38 (2018) The GALAH Survey: Second Data Release 3 2014), 4MOST (de Jong et al. 2014), and SDSS5 (Kollmeier et al. 2017).”
Estimating stellar birth radii and the time evolution of Milky Way’s ISM metallicity gradient (2018, methodology): “…surveys GALAH (De Silva et al. 2015) and GaiaESO (Gilmore et al. 2012) within 2-3 kpc from the Sun, and APOGEE, SDSS-V’s Milky Way Mapper (MWM, Kollmeier et al. 2017), WEAVE (Dalton et al. 2012), and 4MOST (de Jong et al. 2012) up to ∼ 6 − 7 kpc from the Sun, combined with Gaia astrometry…”
AGaiaData Release 2 catalogue of white dwarfs and a comparison with SDSS (2018, background): “With large multi-fibre spectroscopic facilities approaching first light in both hemispheres (e.g., WEAVE, 4MOST, DESI, SDSS-V, Dalton et al. 2014; de Jong et al. 2014; DESI Collaboration et al. 2016; Kollmeier et al. 2017), our catalogue represents a key resource for future white dwarf studies.”