<table><caption>**Table 6**
Summary of eFEDS Observations</caption><thead><tr><th rowspan="2">Plate Number</th><th rowspan="2">MJD</th><th rowspan="2">R.A. (deg)</th><th rowspan="2">Decl. (deg)</th><th rowspan="2">Quality</th><th colspan="4">SN2</th><th rowspan="2">Tile ID</th></tr><tr><th>G1</th><th>I1</th><th>G2</th><th>I2</th></tr></thead><tbody><tr><td>12525</td><td>58,932</td><td>130.27</td><td>-0.57</td><td>B</td><td>7.6</td><td>17.8</td><td>9.2</td><td>26.0</td><td>17693</td></tr><tr><td>12527</td><td>58,930</td><td>130.02</td><td>1.65</td><td>F</td><td>9.1</td><td>27.6</td><td>10.8</td><td>35.0</td><td>17694</td></tr><tr><td>12531</td><td>58,932</td><td>131.96</td><td>1.65</td><td>B</td><td>3.2</td><td>9.1</td><td>4.0</td><td>11.5</td><td>17696</td></tr><tr><td>12533</td><td>58,931</td><td>134.15</td><td>-0.57</td><td>B</td><td>0.4</td><td>0.9</td><td>0.6</td><td>1.4</td><td>17697</td></tr><tr><td>12544</td><td>58,928</td><td>137.79</td><td>1.65</td><td>F</td><td>9.3</td><td>21.9</td><td>9.8</td><td>29.7</td><td>17702</td></tr><tr><td>12545</td><td>58,930</td><td>140.02</td><td>-0.55</td><td>F</td><td>8.3</td><td>24.6</td><td>9.4</td><td>30.9</td><td>17703</td></tr><tr><td>12547</td><td>58,928</td><td>139.75</td><td>1.65</td><td>G</td><td>28.8</td><td>70.3</td><td>27.1</td><td>81.4</td><td>17704</td></tr></tbody></table>

**Note.** Plate: plate number. MJD: Modified Julian Date of the observations. R.A.: R.A. of the center of the plate (degrees). Decl.: decl. of the center of the plate (degrees). Quality: "G": good, "F": fair, and "B": bad. SN2: signal to noise reached in each spectrograph's arm.

epoch had a typical exposure time of 2 hr. The SDSS-RM program continued in SDSS-IV (Blanton et al. 2017), with ~12 epochs per year (2 per month) with a nominal exposure time of 1 hr each during 2015–2017, and ~6 epochs per year (monthly cadence) during 2018–2020. As of 2020 July, SDSS-RM has obtained a total of 90 spectroscopic epochs over a spectroscopic baseline of 7 yr (2014–2020). All SDSS spectroscopic data (pipeline reduced and calibrated) from SDSS-RM are included in the data releases of SDSS-III and SDSS-IV. The full technical details of SDSS-RM are provided in Shen et al. (2015a).

In addition to the optical BOSS spectroscopy, accompanying photometric data in the *g* and *i* bands are acquired with the 3.6 m Canada–France–Hawaii Telescope and the Steward Observatory 2.3 m Bok telescope (Kinemuchi et al. 2020). The final photometric baseline spans 11 yr (2010–2020) when including the 2010–2013 photometric light curves from the Pan-STARRS 1 (Kaiser et al. 2010) Medium Deep survey that covers the entire SDSS-RM field. The SDSS-RM sample includes 849 broad-line quasars with $i_{PSF} < 21.7$ and $0.1 < z < 4.5$ without any constraints on quasar properties. The detailed sample properties are described in Shen et al. (2019b).

The primary science goal of SDSS-RM is to measure RM lags of different broad emission lines covered by optical spectroscopy across the full range of the quasar luminosity and redshift probed by the sample. SDSS-RM has successfully measured short (<6 months) lags for the low-ionization broad lines (e.g., Hα, Hβ, and Mg II; Shen et al. 2016b; Grier et al. 2017) based on the 2014 data. Grier et al. (2019) reported results on C IV lags using the first four years (2014–2017) of imaging and spectroscopy from SDSS-RM (and for Mg II lags in Homayouni et al. 2020), where the lags are typically longer than one season in the observed frame. Lag measurements based on more extended light curves are reported in Shen et al. (2019a), and the analyses of the final SDSS-RM data set are underway.

In addition to the main science goal of RM measurements, SDSS-RM also enables a diverse range of quasar science. Some notable examples are the following: measurements of continuum lags to constrain quasar accretion disk sizes (Homayouni et al. 2019), constraints on the black hole mass —host galaxy correlations at $z > 0.3$ (Matsuoka et al. 2015; Shen et al. 2015b; Yue et al. 2018; Li et al. 2021), spectral and variability properties of quasar emission and absorption lines (Shen et al. 2016a; Sun et al. 2018; Hemler et al. 2019;

Wang et al. 2019, 2020), and extreme variability in quasars (Dexter et al. 2019).

The SDSS-RM field continues to be monitored with optical imaging and spectroscopy as part of the BHM program in SDSS-V (Kollmeier et al. 2017, and Section 8 below). With more extended light curves, this program will be able to measure broad-line RM lags for the most luminous quasars at high redshift.

## 8. Conclusions and Future Plans

This paper documents the final data release from the SDSS-IV collaboration, and the seventeenth data release from SDSS programs as a whole (DR17). With this paper, we make all SDSS-IV data public, concluding the program described in Blanton et al. (2017). In the rest of this section, we give an update of SDSS-V that is now actively observing.

### 8.1. SDSS-V

As SDSS-IV was wrapping up observations (in late 2020 at APO and early 2021 at LCO), the next generation of SDSS began—SDSS-V<fnref n="186" /> (Kollmeier et al. 2017), with its first data taken using the existing plug plate system at APO in late 2020. Building on the legacy of earlier generations, SDSS-V is a multi-epoch spectroscopic survey to observe nearly six million sources using the existing BOSS/APOGEE spectrographs and 2.5 m telescopes, as well as very large swathes of the interstellar medium (ISM) in the Milky Way and Local Group using new optical spectrographs and small telescopes. SDSS-V operates at both APO and LCO and will provide the first *panoptic* spectroscopic view of the entire sky, spanning a wide variety of target types, observing cadences, and science goals.

The scientific program is overseen by three “Mappers”:

1. The Milky Way Mapper (MWM) is targeting millions of stars and stellar remnants with both the APOGEE and BOSS spectrographs, probing stellar populations from the immediate solar neighborhood across the MW, to the far side of the Galactic disk and in the MW’s satellite companions. The MWM’s primary goals are to explore (1) the formation and evolution of the MW, (2) the interior physics and evolutionary pathways of stars across all $T_{eff}$ regimes, from combined asteroseismology and spectroscopy (e.g., Aerts 2021), and (3) the architecture of multi-star and planetary systems.

<footnote n="186">¹⁸⁶ www.sdss5.org</footnote>
2. The *BHM* is targeting nearly half a million accreting SMBHs and other X-ray sources, including newly discovered systems from the SRG/eROSITA mission, with the optical BOSS spectrographs. The BHM seeks to characterize the X-ray sky, improve our understanding of accretion physics, and trace the evolution and impact of supermassive black holes across cosmic time.

3. The LVM is using a wide-field optical IFU, with new optical spectrographs ($R \sim 4000$, $\lambda = 3600-9800$ Å) fed by a 16 cm telescope, to map $\sim 2800$ deg$^2$ of sky. With their tens of millions of spectra sampling the ISM and embedded stellar populations in the MW and satellite galaxies, the LVM's maps will reveal the physics of star formation and the ISM, the complex interplay between stars and the ISM, and the connections between interstellar processes on parsec-sized to galaxy-wide scales.

SDSS-V expands upon the operational infrastructure and data legacy of earlier SDSS iterations with several key developments. Among these are the installation of robotic fiber positioners in the focal planes of both 2.5 m telescopes at APO and LCO, which replace the now-retired SDSS plug plate system. In comparison to earlier SDSS surveys, these focal plane systems enable improved observing efficiency, larger target densities, and more complex observing cadences for the MWM and BHM programs. In addition, the LVM is constructing additional small telescopes at LCO (with longer-term plans to expand to APO) that are linked to new optical spectrographs based on the DESI design (Martini et al. 2018). SDSS-V is continuing the decades-long SDSS legacy of open data policies and efficient, well-documented public data access, boosted with the development of improved data distribution systems to serve its expansive time-domain, multi-object, and integral-field data set to the world. The eighteenth data release of the SDSS (DR18), which will include the first SDSS-V data, mostly targeting and other information, is currently anticipated for 2022.

SDSS-V will also build on the rich educational legacy established by the previous SDSS generations. This will include continuing to distribute as many SDSS plug plates to schools and science centers as possible, and broadening the reach of the SDSS Voyages suite of educational activities. SDSS's large online data sets are an ideal resource for supporting hands-on activities using real archival data, at a wide range of ability levels, and have the potential to act as a gateway for numerous data science and analysis topics.

After twenty-one years of Sloan Digital Sky Surveys, the data released by SDSS-IV in DR17 has made significant contributions to our understanding of the MW, galaxy evolution, and the universe as a whole, and it will continue to enable new research for years to come. The SDSS-IV project is now complete, but the new technology and exciting new surveys, coming as part of SDSS-V, mean that the future remains bright for the SDSS legacy.

Funding for the Sloan Digital Sky Survey IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS website is www.sdss.org.

SDSS-IV is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS

Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Center for Astrophysics | Harvard & Smithsonian, Instituto de Astrofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Korean Participation Group, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatório Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.

Coauthorship on SDSS-IV data papers is alphabetical by last name and offered to all collaboration members who have contributed at least 1 month FTE toward any of the surveys during the period up to the end of data collection; as well as to any formally approved external collaborator who has contributed at least 1 month FTE to work critical to the data release.

The documentation workshop for DR17 was held over Zoom (“DocuZoom”) in 2021 May. This event was the main venue for documentation updates for DR17 (including the start of this paper) and was attended by Anne-Marie Weijmans, Joel Brownstein, Mike Blanton, Karen Masters, Renbin Yan, Sten Hasselquist, Michael Talbot, Hannah Lewis, Christian Hayes, Ani Thaker, Gail Zasowski, David Law, Brian Cherinka, Kyle Westfall, Amy Jones, Lewis Hill, Jon Holtzman, José Sánchez-Gallego, Rachael Beaton, Scott Anderson, Jennifer Johnson, Caroline Swartz, Jordan Raddick, Julie Imig, and a Llama.

Figure 1 made by Joel Browstein; Figures 2 and 3 made by Christian Hayes; Figure 4 made by Jon Holtzman; Figure 5 made by José Sánchez-Gallego; Figure 6 made by Kyle Westfall; Figure 7 made by Brian Cherinka; Figure 8 made by Renbin Yan.

This publication uses data generated via the Zooniverse.org platform, development of which is funded by generous support, including a Global Impact Award from Google, and by a grant from the Alfred P. Sloan Foundation.

This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.

This work is based, in part, on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA.

This publication makes use of data products from the Wide-field Infrared Survey Explorer (Wright et al. 2010), which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of
Technology, funded by the National Aeronautics and Space Administration, and NEOWISE, which is a project of the Jet Propulsion Laboratory/California Institute of Technology. WISE and NEOWISE are funded by the National Aeronautics and Space Administration.

This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

This research has made use of NASA's Astrophysics Data System.

This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. The original description of the SIMBAD service was published in Wenger et al. (2000).

This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France (doi:10.26093/cds/vizier). The original description of the VizieR service was published in Ochsenbein et al. (2000).

This research makes use of data from the Green Bank Observatory. The Green Bank Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

This research made use of ASTROPY, a community-developed core PYTHON (http://www.python.org) package for astronomy (Robitaille et al. 2013); IPYTHON (Pérez & Granger 2007); MATPLOTLIB (Hunter 2007); NUMPY (van der Walt et al. 2011); SCIPY (Jones et al. 2001); and TOPCAT (Taylor 2005).

## ORCID iDs

Víctor Silva Aguirre https://orcid.org/0000-0002-6137-903X

Nikhil Ajgaonkar https://orcid.org/0000-0003-1469-8246

N. Filiz Ak https://orcid.org/0000-0003-3016-5490

Carlos Allende Prieto https://orcid.org/0000-0002-0084-572X

Brett H. Andrews https://orcid.org/0000-0001-8085-5890

Borja Anguiano https://orcid.org/0000-0001-5261-4336

Erik Aquino-Ortíz https://orcid.org/0000-0003-1083-9208

Alfonso Aragón-Salamanca https://orcid.org/0000-0001-8215-1256

Maria Argudo-Fernández https://orcid.org/0000-0002-0789-2326

Metin Ata https://orcid.org/0000-0002-5934-9018

Vladimir Avila-Reese https://orcid.org/0000-0002-3461-2342

Carles Badenes https://orcid.org/0000-0003-3494-343X

Kat Barger https://orcid.org/0000-0001-5817-0932

Jorge K. Barrera-Ballesteros https://orcid.org/0000-0003-2405-7258

Rachael L. Beaton https://orcid.org/0000-0002-1691-8217

Timothy C. Beers https://orcid.org/0000-0003-4573-6233

Francesco Belfiore https://orcid.org/0000-0002-2545-5752

Chad F. Bender https://orcid.org/0000-0003-4384-7220

Matthew A. Bershady https://orcid.org/0000-0002-3131-4374

Dmitry Bizyaev https://orcid.org/0000-0002-3601-133X

Guillermo A. Blanc https://orcid.org/0000-0003-4218-3944

Michael R. Blanton https://orcid.org/0000-0003-1641-6222

Médéric Boquien https://orcid.org/0000-0003-0946-6176

Jura Borissova https://orcid.org/0000-0002-5936-7718

Jo Bovy https://orcid.org/0000-0001-6855-442X

W. N. Brandt https://orcid.org/0000-0002-0167-2453

Joel R. Brownstein https://orcid.org/0000-0002-8725-1069

Marcella Brusa https://orcid.org/0000-0002-5059-6848

Johannes Buchner https://orcid.org/0000-0003-0426-6634

Kevin Bundy https://orcid.org/0000-0001-9742-3138

Joseph N. Burchett https://orcid.org/0000-0002-1979-2197

Martin Bureau https://orcid.org/0000-0003-4980-1012

Adam Burgasser https://orcid.org/0000-0002-6523-9536

Michele Cappellari https://orcid.org/0000-0002-1283-8420

Joleen K. Carlberg https://orcid.org/0000-0001-5926-4471

Yan-Ping Chen https://orcid.org/0000-0001-8821-0309

Brian Cherinka https://orcid.org/0000-0002-4289-7923

S. Drew Chojnowski https://orcid.org/0000-0001-9984-0891

Johan Comparat https://orcid.org/0000-0001-9200-1497

Luiz da Costa https://orcid.org/0000-0002-7731-277X

Kevin Covey https://orcid.org/0000-0001-6914-7797

Irene Cruz-Gonzalez https://orcid.org/0000-0002-2653-1120

Katia Cunha https://orcid.org/0000-0001-6476-0576

Y. Sophia Dai (戴昱) https://orcid.org/0000-0002-7928-416X

Jeremy Darling https://orcid.org/0000-0003-2511-2060

Roger Davies https://orcid.org/0000-0001-7897-3812

Kyle Dawson https://orcid.org/0000-0002-0553-3805

Nathan De Lee https://orcid.org/0000-0002-3657-0705

Mariana Cano-Díaz https://orcid.org/0000-0001-9553-8230

Daniel J. Eisenstein https://orcid.org/0000-0002-2929-3121

Eric Emsellem https://orcid.org/0000-0002-6155-7166

Mike Eracleous https://orcid.org/0000-0002-3719-940X

Stephanie Escoffier https://orcid.org/0000-0002-2847-7498

Xiaohui Fan https://orcid.org/0000-0003-3310-0131

Shuai Feng https://orcid.org/0000-0002-9767-9237

Diane Feuillet https://orcid.org/0000-0002-3101-5921

Sean P Fillingham https://orcid.org/0000-0002-8425-0351

Peter M. Frinchaboy https://orcid.org/0000-0002-0740-8346

Lluís Galbany https://orcid.org/0000-0002-1296-6887

D. A. García-Hernández https://orcid.org/0000-0002-1693-2721

Doug Geisler https://orcid.org/0000-0002-3900-8208

Joseph Gelfand https://orcid.org/0000-0003-4679-1058

Julian Goddy https://orcid.org/0000-0002-8933-9574

Diego Godoy-Rivera https://orcid.org/0000-0003-4556-1277

Paul J. Green https://orcid.org/0000-0002-8179-9445

Catherine J. Grier https://orcid.org/0000-0001-9920-6057

Emily Griffith https://orcid.org/0000-0001-9345-9977

Hong Guo https://orcid.org/0000-0003-4936-8247

Paul Harding https://orcid.org/0000-0003-3442-6248

Sten Hasselquist https://orcid.org/0000-0001-5388-0994

Fred Hearty https://orcid.org/0000-0002-1664-3102

David W. Hogg https://orcid.org/0000-0003-2866-9403

Jon A. Holtzman https://orcid.org/0000-0002-9771-9622

Bau-Ching Hsieh https://orcid.org/0000-0001-5615-4904

Daniel Huber https://orcid.org/0000-0001-8832-4488

Marc Huertas-Company https://orcid.org/0000-0002-1416-8483

Héctor J. Ibarra-Medel https://orcid.org/0000-0002-9790-6313
Julie Imig https://orcid.org/0000-0003-2025-3585

Tharindu Jayasinghe https://orcid.org/0000-0002-6244-477X

Xihan Ji https://orcid.org/0000-0002-1660-9502

Henrik Jönsson https://orcid.org/0000-0002-4912-8609

Ivan Katkov https://orcid.org/0000-0002-6425-6879

Karen Kinemuchi https://orcid.org/0000-0001-7908-7724

Marina Kounkel https://orcid.org/0000-0002-5365-1267

Kathryn Kreckel https://orcid.org/0000-0001-6551-3091

Dhanesh Krishnarao https://orcid.org/0000-0002-7955-7359

Ivan Lacerna https://orcid.org/0000-0002-7802-7356

Richard R. Lane https://orcid.org/0000-0003-1805-0316

David R. Law https://orcid.org/0000-0002-9402-186X

Hannah M. Lewis https://orcid.org/0000-0002-7871-085X

Cheng Li https://orcid.org/0000-0002-8711-8970

Lihwai Lin (林俐暉) https://orcid.org/0000-0001-7218-7407

Yen-Ting Lin https://orcid.org/0000-0001-7146-4687

Chris Lintott https://orcid.org/0000-0001-5578-359X

Penélope Longa-Peña https://orcid.org/0000-0001-9330-5003

Britt F. Lundgren https://orcid.org/0000-0002-6463-2483

Yuanze Luo https://orcid.org/0000-0002-0696-6952

Suvrath Mahadevan https://orcid.org/0000-0001-9596-7983

Steven R. Majewski https://orcid.org/0000-0003-2025-3147

Arturo Manchado https://orcid.org/0000-0002-3011-686X

Thomas Masseron https://orcid.org/0000-0002-6939-0831

Karen L. Masters https://orcid.org/0000-0003-0846-9578

Savita Mathur https://orcid.org/0000-0002-0129-0316

Richard M. McDermid https://orcid.org/0000-0002-8175-7229

Michael Merrifield https://orcid.org/0000-0002-4202-4727

Andrea Miglio https://orcid.org/0000-0001-5998-8533

Dante Minniti https://orcid.org/0000-0002-7064-099X

Antonela Monachesi https://orcid.org/0000-0003-2325-9616

Benoit Mosser https://orcid.org/0000-0002-7547-1208

John Mulchaey https://orcid.org/0000-0003-2083-5569

Seshadri Nadathur https://orcid.org/0000-0001-9070-3102

Kirpal Nandra https://orcid.org/0000-0002-7150-9192

Justus Neumann https://orcid.org/0000-0002-3289-8914

Jeffrey A. Newman https://orcid.org/0000-0001-8684-2222

David L. Nidever https://orcid.org/0000-0002-1793-3689

Farnik Nikakhtar https://orcid.org/0000-0002-3641-4366

Christian Nitschelm https://orcid.org/0000-0003-4752-4365

Julia E. O'Connell https://orcid.org/0000-0003-2321-950X

Yeisson Osorio https://orcid.org/0000-0001-5832-6933

Zachary J. Pace https://orcid.org/0000-0003-4843-4185

Kaike Pan https://orcid.org/0000-0002-2835-2556

Hsi-An Pan https://orcid.org/0000-0002-1370-6964

Karla Peña Ramírez https://orcid.org/0000-0002-5855-401X

Samantha Penny https://orcid.org/0000-0001-5703-7531

Marc Pinsonneault https://orcid.org/0000-0002-7549-7766

Frédérick Poidevin https://orcid.org/0000-0002-5391-5568

Rogemar A. Riffel https://orcid.org/0000-0003-0483-3723

Rogério Riffel https://orcid.org/0000-0002-1321-1320

Hans-Walter Rix https://orcid.org/0000-0003-4996-9069

Annie C. Robin https://orcid.org/0000-0001-8654-9499

Alexandre Roman-Lopes https://orcid.org/0000-0002-1379-4204

Carlos Román-Zúñiga https://orcid.org/0000-0001-8600-4798

Ashley J. Ross https://orcid.org/0000-0002-7522-9083

Kate H. R. Rubin https://orcid.org/0000-0001-6248-1864

Mara Salvato https://orcid.org/0000-0001-7116-9303

Sebastián F. Sánchez https://orcid.org/0000-0001-6444-9307

Robyn Sanderson https://orcid.org/0000-0003-3939-3297

Felipe Antonio Santana Rojas https://orcid.org/0000-0002-4023-7649

Conor Sayres https://orcid.org/0000-0002-4454-1920

Elizaveta Sazonova https://orcid.org/0000-0001-6245-5121

Ricardo Schiavon https://orcid.org/0000-0002-2244-0897

Donald P. Schneider https://orcid.org/0000-0001-7240-7449

Mathias Schultheis https://orcid.org/0000-0002-6590-1657

Axel Schwope https://orcid.org/0000-0003-3441-9355

Aldo Serenelli https://orcid.org/0000-0001-6359-2769

Javier Serna https://orcid.org/0000-0001-7351-6540

Zhengyi Shao https://orcid.org/0000-0001-8611-2465

Yue Shen https://orcid.org/0000-0003-1659-7035

Matthew Shetrone https://orcid.org/0000-0003-0509-2656

Joshua D. Simon https://orcid.org/0000-0002-4733-4994

Verne Smith https://orcid.org/0000-0002-0134-2024

Jennifer Sobeck https://orcid.org/0000-0002-4989-0353

David V. Stark https://orcid.org/0000-0002-3746-2853

Keivan G. Stassun https://orcid.org/0000-0002-3481-9052

Matthias Steinmetz https://orcid.org/0000-0001-6516-7459

Dennis Stello https://orcid.org/0000-0002-4879-3519

Thaisa Storchi-Bergmann https://orcid.org/0000-0003-1772-0023

Guy S. Stringfellow https://orcid.org/0000-0003-1479-3059

Amelia Stutz https://orcid.org/0000-0003-2300-8200

Jamie Tayar https://orcid.org/0000-0002-4818-7885

Daniel Thomas https://orcid.org/0000-0002-6325-5671

Nicholas W. Troup https://orcid.org/0000-0003-3248-3097

Jonathan R. Trump https://orcid.org/0000-0002-1410-0470

Sarah Tuttle https://orcid.org/0000-0002-7327-565X

José Antonio Vázquez-Mata https://orcid.org/0000-0001-8694-1204

Marica Valentini https://orcid.org/0000-0003-0974-4148

Octavio Valenzuela https://orcid.org/0000-0002-0523-5509

Sandro Villanova https://orcid.org/0000-0001-6205-1493

Fiorenzo Vincenzo https://orcid.org/0000-0002-0743-9994

David Wake https://orcid.org/0000-0002-6047-1010

Kyle B. Westfall https://orcid.org/0000-0003-1809-6920

Matthew C. Wilde https://orcid.org/0000-0003-1980-364X

John C. Wilson https://orcid.org/0000-0001-7828-7257

Robert F. Wilson https://orcid.org/0000-0002-4235-6369

Mikayla Wilson https://orcid.org/0000-0003-3008-1975

W. M. Wood-Vasey https://orcid.org/0000-0001-7113-1233

Olga Zamora https://orcid.org/0000-0003-2100-1638

Gail Zasowski https://orcid.org/0000-0001-6761-9359

Zheng Zheng https://orcid.org/0000-0003-1887-6732
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