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1. Chemical abundances of the young inner-disk open cluster NGC 6705 observed by APOGEE: sodium-rich and not $\alpha$-enhanced

Author

Loaiza-Tacuri, V., Cunha, K., Souto, D., Smith, V. V., Guerço, R., Chiappini, C., Silva, J. V. Sales, Horta, D., Prieto, C. Allende, Beaton, R., Bizyaev, D., Daflon, S., Frinchaboy, P., Hasselquist, S., Hayes, C. R., Holtzman, J. A., Jönsson, H., Majewski, S. R., Mészáros, S., Nidever, D. L., Pinsonneault, M., and Zasowski, G.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Previous results in the literature have found the young inner-disk open cluster NGC 6705 to be mildly $\alpha$-enhanced. We examined this possibility via an independent chemical abundance analysis for 11 red-giant members of NGC 6705. The analysis is based on near-infrared APOGEE spectra and relies on LTE calculations using spherical model atmospheres and radiative transfer. We find a mean cluster metallicity of $\rm [Fe/H] = +0.13 \pm 0.04$, indicating that NGC 6705 is metal-rich, as may be expected for a young inner-disk cluster. The mean $\alpha$-element abundance relative to iron is $\rm \langle [\alpha/Fe]\rangle =-0.03 \pm 0.05$, which is not at odds with expectations from general Galactic abundance trends. NGC 6705 also provides important probes for studying stellar mixing, given its turn-off mass of M$\sim$3.3 M$_\odot$. Its red giants have low $^{12}$C abundances ([$^{12}$C/Fe]=$-$0.16) and enhanced $^{14}$N abundances ([$^{14}$N/Fe]=+0.51), which are key signatures of the first dredge-up on the red giant branch. An additional signature of dredge-up was found in the Na abundances, which are enhanced by [Na/Fe]=+0.29, with a very small non-LTE correction. The $^{16}$O and Al abundances are found to be near-solar. All of the derived mixing-sensitive abundances are in agreement with stellar models of approximately 3.3 M$_{\odot}$ evolving along the red giant branch and onto the red clump. As found in young open clusters with similar metallicities, NGC 6705 exhibits a mild excess in the s-process element cerium, with $\rm [Ce/Fe] = +0.13\pm0.07$., Comment: 17 pages, 10 figures, 6 tables

Published
2023
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2. Open Cluster Chemical Homogeneity Throughout the Milky Way

Author

Poovelil, Vijith Jacob, Zasowski, G., Hasselquist, S., Seth, A., Donor, John, Beaton, Rachael L., Cunha, K., Frinchaboy, Peter M., García-Hernández, D. A., Hawkins, K., Kratter, K. M., Lane, Richard R., and Nitschelm, C.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The chemical homogeneity of surviving stellar clusters contains important clues about interstellar medium (ISM) mixing efficiency, star formation, and the enrichment history of the Galaxy. Existing measurements in a handful of open clusters suggest homogeneity in several elements at the 0.03 dex level. Here we present (i) a new cluster member catalog based only on APOGEE radial velocities and Gaia-DR2 proper motions, (ii) improved abundance uncertainties for APOGEE cluster members, and (iii) the dependence of cluster homogeneity on Galactic and cluster properties, using abundances of eight elements from the APOGEE survey for ten high-quality clusters. We find that cluster homogeneity is uncorrelated with Galactocentric distance, |Z|, age, and metallicity. However, velocity dispersion, which is a proxy for cluster mass, is positively correlated with intrinsic scatter at relatively high levels of significance for [Ca/Fe] and [Mg/Fe]. We also see a possible positive correlation at a low level of significance for [Ni/Fe], [Si/Fe], [Al/Fe], and [Fe/H], while [Cr/Fe] and [Mn/Fe] are uncorrelated. The elements that show a correlation with velocity dispersion are those that are predominantly produced by core-collapse supernovae (CCSNe). However, the small sample size and relatively low correlation significance highlight the need for follow-up studies. If borne out by future studies, these findings would suggest a quantitative difference between the correlation lengths of elements produced predominantly by Type~Ia SNe versus CCSNe, which would have implications for Galactic chemical evolution models and the feasibility of chemical tagging., Comment: Accepted for publication in ApJ; 21 pages (plus appendix), 21 figures, 4 tables

Published
2020
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3. Cool stars in the Galactic Center as seen by APOGEE: M giants, AGB stars and supergiant stars/candidates

Author

Schultheis, M., Rojas-Arriagada, A., Cunha, K., Zoccali, M., Chiappini, C., Queiroz, A. B. A., Minniti, D., Fritz, T., García-Hernández, D. A., Nitschelm, C., Zamora, O., Hasselquist, S., Fernández-Trincado, J. G., and Munoz, R. R.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The Galactic Center region, including the nuclear disk, has until recently been largely avoided in chemical census studies because of extreme extinction and stellar crowding. Making use of the latest APOGEE data release (DR16), we are able for the first time to study cool AGB stars and supergiants in this region. The stellar parameters of five known AGB stars and one supergiant star (VR 5-7) show that their location is well above the tip of the RGB.We study metallicities of 157 M giants situated within 150 pc of the Galactic center from observations obtained by the APOGEE survey with reliable stellar parameters from the APOGEE/ASPCAP pipeline making use of the cool star grid down to 3200 K. Distances, interstellar extinction values, and radial velocities were checked to confirm that these stars are indeed situated in the Galactic Center region. We detect a clear bimodal structure in the metallicity distribution function, with a dominant metal-rich peak of [Fe/H] ~ +0.3 dex and a metal-poor peak around [Fe/H]= -0.5 dex, which is 0.2 dex poorer than Baade's Window. The alpha-elements Mg, Si, Ca, and O show a similar trend to the Galactic Bulge. The metal-poor component is enhanced in the alpha-elements, suggesting that this population could be associated with the classical bulge and a fast formation scenario. We find a clear signature of a rotating nuclear stellar disk and a significant fraction of high velocity stars with $\rm v_{gal} > 300\,km/s$; the metal-rich stars show a much higher rotation velocity ($\rm \sim 200\,km/s$) with respect to the metal-poor stars ($\rm \sim 140\,km/s$). The chemical abundances as well as the metallicity distribution function suggest that the nuclear stellar disc and the nuclear star cluster show distinct chemical signatures and might be formed differently., Comment: 12 pages, accepted for Astronomy&Astrophysics

Published
2020
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4. How Many Components? Quantifying the Complexity of the Metallicity Distribution in the Milky Way Bulge with APOGEE

Author

Rojas-Arriagada, A., Zasowski, G., Schultheis, M., Zoccali, M., Hasselquist, S., Chiappini, C., Cohen, R. E., Cunha, K., Fernández-Trincado, J. G., Fragkoudi, F., García-Hernández, D. A., Geisler, D., Lian, J., Majewski, S., Minniti, D., Nitschelm, C., and Queiroz, A. B. A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We use data of $\sim$13,000 stars from the SDSS/APOGEE survey to study the shape of the bulge MDF within the region $|\ell|\leq11^\circ$ and $|b|\leq13^\circ$, and spatially constrained to ${\rm R_{GC}\leq3.5}$ kpc. We apply Gaussian Mixture Modeling and Non-negative Matrix Factorization decomposition techniques to identify the optimal number and the properties of MDF components. We find the shape and spatial variations of the MDF (at ${\rm [Fe/H]\geq-1}$ dex) are well represented as a smoothly varying contribution of three overlapping components located at [Fe/H]=+$0.32$, $-0.17$ and $-0.66$ dex. The bimodal MDF found in previous studies is in agreement with our trimodal assessment once the limitations in sample size and individual measurement errors are taken into account. The shape of the MDF and its correlations with kinematics reveal different spatial distributions and kinematical structure for the three components co-existing in the bulge region. We confirm the consensus physical interpretation of metal-rich stars as associated with the secularly evolved disk into a boxy/peanut X-shape bar. On the other hand, metal-intermediate stars could be the product of in-situ formation at high redshift in a gas-rich environment characterized by violent and fast star formation. This interpretation would help to link a present-day structure with those observed in formation in the center of high redshift galaxies. Finally, metal-poor stars may correspond to the metal-rich tail of the population sampled at lower metallicity from the study of RR Lyrae stars. Conversely, they could be associated with the metal-poor tail of the early thick disc., Comment: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society, Published by Oxford University Press on behalf of the Royal Astronomical Society. 21 pages, 19 Figures

Published
2020
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5. The Milky Way bar and bulge revealed by APOGEE DR16 and Gaia EDR3

Author

Queiroz, A. B. A., Chiappini, C., Perez-Villegas, A., Khalatyan, A., Anders, F., Barbuy, B., Santiago, B. X., Steinmetz, M., Cunha, K., Schultheis, M., Majewski, S. R., Minchev, I., Minniti, D., Beaton, R. L., Cohen, R. E., da Costa, L. N., Fernández-Trincado, J. G., Garcia-Hernández, D. A., Geisler, D., Hasselquist, S., Lane, R. R., Nitschelm, C., Rojas-Arriagada, A., Roman-Lopes, A., Smith, V., and Zasowski, G.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We investigate the inner regions of the Milky Way with a sample of unprecedented size and coverage thanks to APOGEE DR16 and Gaia EDR3 data. Our inner Galactic sample has more than 26,000 stars within $|X_{\rm Gal}| <5$ kpc, $|Y_{\rm Gal}| <3.5$ kpc, $|Z_{\rm Gal}| <1$ kpc, and we also make the analysis for a foreground-cleaned sub-sample of 8,000 stars more representative of the bulge-bar populations. The inner Galaxy shows a clear chemical discontinuity in key abundance ratios [$\alpha$/Fe], [C/N], and [Mn/O], probing different enrichment timescales, which suggests a star formation gap (quenching) between the high- and low-$\alpha$ populations. For the first time, we are able to fully characterize the different populations co-existing in the innermost regions of the Galaxy via joint analysis of the distributions of rotational velocities, metallicities, orbital parameters and chemical abundances. The chemo-kinematic analysis reveals the presence of the bar; of an inner thin disk; of a thick disk, and of a broad metallicity population, with a large velocity dispersion, indicative of a pressure supported component. We find and characterize chemically and kinematically a group of counter-rotating stars, which could be the result of a gas-rich merger event or just the result of clumpy star formation during the earliest phases of the early disk, which migrated into the bulge. Finally, based on the 6D information we assign stars a probability value of being on a bar orbit and find that most of the stars with large bar orbit probabilities come from the innermost 3 kpcs. Even stars with a high probability of belonging to the bar show the chemical bimodality in the [$\alpha$/Fe] vs. [Fe/H] diagram. This suggests bar trapping to be an efficient mechanism, explaining why stars on bar orbits do not show a significant distinct chemical abundance ratio signature., Comment: 25 pages, 25 figures, Accepted for publication on A&A, in press

Published
2020
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6. APOGEE DR14/DR15 Abundances in the Inner Milky Way

Author

Zasowski, G., Schultheis, M., Hasselquist, S., Cunha, K., Sobeck, J., Johnson, J. A., Rojas-Arriagada, A., Majewski, S. R., Andrews, B. H., Jonsson, H., Beers, T. C., Chojnowski, S. D., Frinchaboy, P. M., Holtzman, J. A., Minniti, D., Nidever, D. L., and Nitschelm, C.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present an overview of the distributions of 11 elemental abundances in the Milky Way's inner regions, as traced by APOGEE stars released as part of SDSS Data Release 14/15 (DR14/DR15), including O, Mg, Si, Ca, Cr, Mn, Co, Ni, Na, Al, and K. This sample spans ~4000 stars with R_GC<4 kpc, enabling the most comprehensive study to date of these abundances and their variations within the innermost few kiloparsecs of the Milky Way. We describe the observed abundance patterns ([X/Fe]-[Fe/H]), compare to previous literature results and to patterns in stars at the solar Galactic radius, and discuss possible trends with DR14/DR15 effective temperatures. We find that the position of the [Mg/Fe]-[Fe/H] "knee" is nearly constant with R_GC, indicating a well-mixed star-forming medium or high levels of radial migration in the early inner Galaxy. We quantify the linear correlation between pairs of elements in different subsamples of stars and find that these relationships vary; some abundance correlations are very similar between the alpha-rich and alpha-poor stars, but others differ significantly, suggesting variations in the metallicity dependencies of certain supernova yields. These empirical trends will form the basis for more detailed future explorations and for the refinement of model comparison metrics. That the inner Milky Way abundances appear dominated by a single chemical evolutionary track and that they extend to such high metallicities underscore the unique importance of this part of the Galaxy for constraining the ingredients of chemical evolution modeling and for improving our understanding of the evolution of the Galaxy as a whole., Comment: Submitted to AAS Journals; revised after referee report

Published
2018
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7. A chemical and kinematical analysis of the intermediate-age open cluster IC 166 from APOGEE and Gaia DR2

Author

Schiappacasse-Ulloa, J., Tang, B., Fernández-Trincado, J. G., Zamora, O., Geisler, D., Frinchaboy, P., Schultheis, M., Dell'Agli, F., Villanova, S., Masseron, T., Mészáros, Sz., Souto, D., Hasselquist, S., Cunha, K., Smith, V. V., García-Hernández, D. A., Vieira, K., Robin, A. C., Minniti, D., Zasowski, G., Moreno, E., Pérez-Villegas, A., Lane, R. R., Ivans, I. I., Pan, K., Nitschelm, C., Santana, F. A., Carrera, R., and Roman-Lopes, A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

IC 166 is an intermediate-age open cluster ($\sim 1$ Gyr) which lies in the transition zone of the metallicity gradient in the outer disc. Its location, combined with our very limited knowledge of its salient features, make it an interesting object of study. We present the first high-resolution spectroscopic and precise kinematical analysis of IC 166, which lies in the outer disc with $R_{GC} \sim 12.7$ kpc. High resolution \textit{H}-band spectra were analyzed using observations from the SDSS-IV Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey. We made use of the Brussels Automatic Stellar Parameter (BACCHUS) code to provide chemical abundances based on a line-by-line approach for up to eight chemical elements (Mg, Si, Ca, Ti, Al, K, Mn and Fe). The $\alpha-$element (Mg, Si, Ca and whenever available Ti) abundances, and their trends with Fe abundances have been analysed for a total of 13 high-likelihood cluster members. No significant abundance scatter was found in any of the chemical species studied. Combining the positional, heliocentric distance, and kinematic information we derive, for the first time, the probable orbit of IC 166 within a Galactic model including a rotating boxy bar, and found that it is likely that IC 166 formed in the Galactic disc, supporting its nature as an unremarkable Galactic open cluster with an orbit bound to the Galactic plane., Comment: 16 pages, 7 tables, 8 figures, accepted for publication in AJ

Published
2018
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8. The Fifteenth Data Release of the Sloan Digital Sky Surveys: First Release of MaNGA-derived Quantities, Data Visualization Tools, and Stellar Library

Author

Aguado, DS, Ahumada, R, Almeida, A, Anderson, SF, Andrews, BH, Anguiano, B, Ortiz, EA, Aragón-Salamanca, A, Argudo-Fernández, M, Aubert, M, Avila-Reese, V, Badenes, C, Barboza Rembold, S, Barger, K, Barrera-Ballesteros, J, Bates, D, Bautista, J, Beaton, RL, Beers, TC, Belfiore, F, Bernardi, M, Bershady, M, Beutler, F, Bird, J, Bizyaev, D, Blanc, GA, Blanton, MR, Blomqvist, M, Bolton, AS, Boquien, M, Borissova, J, Bovy, J, Nielsen Brandt, W, Brinkmann, J, Brownstein, JR, Bundy, K, Burgasser, A, Byler, N, Cano Diaz, M, Cappellari, M, Carrera, R, Cervantes Sodi, B, Chen, Y, Cherinka, B, Doohyun Choi, P, Chung, H, Coffey, D, Comerford, JM, Comparat, J, Covey, K, Da Silva Ilha, G, Da Costa, L, Sophia Dai, Y, Damke, G, Darling, J, Davies, R, Dawson, K, De Sainte Agathe, V, Deconto Machado, A, Del Moro, A, De Lee, N, Diamond-Stanic, AM, Dominguez Sánchez, H, Donor, J, Drory, N, Du Mas Des Bourboux, H, Duckworth, C, Dwelly, T, Ebelke, G, Emsellem, E, Escoffier, S, Fernández-Trincado, JG, Feuillet, D, Fischer, JL, Fleming, SW, Fraser-Mckelvie, A, Freischlad, G, Frinchaboy, PM, Fu, H, Galbany, L, Garcia-Dias, R, Garcia-Hernández, DA, Alberto Garma Oehmichen, L, Antonio Geimba Maia, M, Gil-Marin, H, Grabowski, K, Gu, M, Guo, H, Ha, J, Harrington, E, Hasselquist, S, Hayes, CR, Hearty, F, Hernandez Toledo, H, Hicks, H, Hogg, DW, Holley-Bockelmann, K, Holtzman, JA, Hsieh, BC, and Hunt, JAS

Subjects
atlases, catalogs, surveys, astro-ph.IM, Astronomy & Astrophysics, Astronomical and Space Sciences, Organic Chemistry, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

Twenty years have passed since first light for the Sloan Digital Sky Survey (SDSS). Here, we release data taken by the fourth phase of SDSS (SDSS-IV) across its first three years of operation (2014 July-2017 July). This is the third data release for SDSS-IV, and the 15th from SDSS (Data Release Fifteen; DR15). New data come from MaNGA - we release 4824 data cubes, as well as the first stellar spectra in the MaNGA Stellar Library (MaStar), the first set of survey-supported analysis products (e.g., stellar and gas kinematics, emission-line and other maps) from the MaNGA Data Analysis Pipeline, and a new data visualization and access tool we call "Marvin." The next data release, DR16, will include new data from both APOGEE-2 and eBOSS; those surveys release no new data here, but we document updates and corrections to their data processing pipelines. The release is cumulative; it also includes the most recent reductions and calibrations of all data taken by SDSS since first light. In this paper, we describe the location and format of the data and tools and cite technical references describing how it was obtained and processed. The SDSS website (www.sdss.org) has also been updated, providing links to data downloads, tutorials, and examples of data use. Although SDSS-IV will continue to collect astronomical data until 2020, and will be followed by SDSS-V (2020-2025), we end this paper by describing plans to ensure the sustainability of the SDSS data archive for many years beyond the collection of data.

Published
2019

9. Target Selection for the Apache Point Observatory Galactic Evolution Experiment (APOGEE)

Author

Zasowski, G., Johnson, Jennifer A., Frinchaboy, P. M., Majewski, S. R., Nidever, D. L., Pinto, H. J. Rocha, Girardi, L., Andrews, B., Chojnowski, S. D., Cudworth, K. M., Jackson, K., Munn, J., Skrutskie, M. F., Beaton, R. L., Blake, C. H., Covey, K., Deshpande, R., Epstein, C., Fabbian, D., Fleming, S. W., Hernandez, A. Garcia, Herrero, A., Mahadevan, S., Meszaros, Sz., Schultheis, M., Sellgren, K., Terrien, R., van Saders, J., Prieto, C. Allende, Bizyaev, D., Burton, A., Cunha, K., da Costa, L. N., Hasselquist, S., Hearty, F., Holtzman, J., Perez, A. E. Garcia, Maia, M. A. G., O'Connell, R. W., O'Donnell, C., Pinsonneault, M., Santiago, B. X., Schiavon, R. P., Shetrone, M., Smith, V., and Wilson, J. C.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The Apache Point Observatory Galactic Evolution Experiment (APOGEE) is a high-resolution infrared spectroscopic survey spanning all Galactic environments (i.e., bulge, disk, and halo), with the principal goal of constraining dynamical and chemical evolution models of the Milky Way. APOGEE takes advantage of the reduced effects of extinction at infrared wavelengths to observe the inner Galaxy and bulge at an unprecedented level of detail. The survey's broad spatial and wavelength coverage enables users of APOGEE data to address numerous Galactic structure and stellar populations issues. In this paper we describe the APOGEE targeting scheme and document its various target classes to provide the necessary background and reference information to analyze samples of APOGEE data with awareness of the imposed selection criteria and resulting sample properties. APOGEE's primary sample consists of ~100,000 red giant stars, selected to minimize observational biases in age and metallicity. We present the methodology and considerations that drive the selection of this sample and evaluate the accuracy, efficiency, and caveats of the selection and sampling algorithms. We also describe additional target classes that contribute to the APOGEE sample, including numerous ancillary science programs, and we outline the targeting data that will be included in the public data releases., Comment: Accepted to AJ. 31 pages, 11 figures

Published
2013
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10. The tenth data release of the Sloan digital sky survey: First spectroscopic data from the SDSS-iii apache point observatory galactic evolution experiment

Author

Gott, JR, Mack, CE, Ahn, CP, Alexandroff, R, Allende Prieto, C, Anders, F, Anderson, SF, Anderton, T, Andrews, BH, Aubourg, E, Bailey, S, Bastien, FA, Bautista, JE, Beers, TC, Beifiori, A, Bender, CF, Berlind, AA, Beutler, F, Bhardwaj, V, Bird, JC, Bizyaev, D, Blake, CH, Blanton, MR, Blomqvist, M, Bochanski, JJ, Bolton, AS, Borde, A, Bovy, J, Bradley, AS, Brandt, WN, Brauer, D, Brinkmann, J, Brownstein, JR, Busca, NG, Carithers, W, Carlberg, JK, Carnero, AR, Carr, MA, Chiappini, C, Chojnowski, SD, Chuang, CH, Comparat, J, Crepp, JR, Cristiani, S, Croft, RAC, Cuesta, AJ, Cunha, K, Da Costa, LN, Dawson, KS, De Lee, N, Dean, JDR, Delubac, T, Deshpande, R, Dhital, S, Ealet, A, Ebelke, GL, Edmondson, EM, Eisenstein, DJ, Epstein, CR, Escoffier, S, Esposito, M, Evans, ML, Fabbian, D, Fan, X, Favole, G, Femenía Castellá, B, Fernández Alvar, E, Feuillet, D, Filiz Ak, N, Finley, H, Fleming, SW, Font-Ribera, A, Frinchaboy, PM, Galbraith-Frew, JG, García-Hernández, DA, Pérez, AEG, Ge, J, Génova-Santos, R, Gillespie, BA, Girardi, L, González Hernández, JI, Gunn, JE, Guo, H, Halverson, S, Harding, P, Harris, DW, Hasselquist, S, Hawley, SL, Hayden, M, Hearty, FR, Herrero Davó, A, Ho, S, Hogg, DW, Holtzman, JA, Honscheid, K, Huehnerhoff, J, Ivans, II, Jackson, KM, Jiang, P, and Johnson, JA

Subjects
atlases, catalogs, surveys, astro-ph.IM, astro-ph.CO, astro-ph.GA, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract

The Sloan Digital Sky Survey (SDSS) has been in operation since 2000 April. This paper presents the Tenth Public Data Release (DR10) from its current incarnation, SDSS-III. This data release includes the first spectroscopic data from the Apache Point Observatory Galaxy Evolution Experiment (APOGEE), along with spectroscopic data from the Baryon Oscillation Spectroscopic Survey (BOSS) taken through 2012 July. The APOGEE instrument is a near-infrared R 22,500 300 fiber spectrograph covering 1.514-1.696 μm. The APOGEE survey is studying the chemical abundances and radial velocities of roughly 100,000 red giant star candidates in the bulge, bar, disk, and halo of the Milky Way. DR10 includes 178,397 spectra of 57,454 stars, each typically observed three or more times, from APOGEE. Derived quantities from these spectra (radial velocities, effective temperatures, surface gravities, and metallicities) are also included. DR10 also roughly doubles the number of BOSS spectra over those included in the Ninth Data Release. DR10 includes a total of 1,507,954 BOSS spectra comprising 927,844 galaxy spectra, 182,009 quasar spectra, and 159,327 stellar spectra selected over 6373.2 deg2. © 2014. The American Astronomical Society. All rights reserved..

Published
2014

11. Chemical abundances of the young inner-disc open cluster NGC 6705 observed by APOGEE: sodium-rich and not α-enhanced

Author

Loaiza-Tacuri, V, primary, Cunha, K, additional, Souto, D, additional, Smith, V V, additional, Guerço, R, additional, Chiappini, C, additional, Sales-Silva, J V, additional, Horta, D, additional, Prieto, C Allende, additional, Beaton, R, additional, Bizyaev, D, additional, Daflon, S, additional, Frinchaboy, P, additional, Hasselquist, S, additional, Hayes, C R, additional, Holtzman, J A, additional, Jönsson, H, additional, Majewski, S R, additional, Mészáros, S, additional, Nidever, D L, additional, Pinsonneault, M, additional, and Zasowski, G, additional

Published
2023
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12. High-velocity Stars in SDSS/APOGEE DR17

Author

Quispe-Huaynasi, F., primary, Roig, F., additional, McDonald, D. J., additional, Loaiza-Tacuri, V., additional, Majewski, S. R., additional, Wanderley, F. C., additional, Cunha, K., additional, Pereira, C. B., additional, Hasselquist, S., additional, and Daflon, S., additional

Published
2022
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13. Quantifying radial migration in the Milky Way: Inefficient over short time-scales but essential to the very outer disc beyond ∼15 kpc

Author

Lian, J, Lian, J, Zasowski, G, Hasselquist, S, Holtzman, JA, Boardman, N, Cunha, K, Fernández-Trincado, JG, Frinchaboy, PM, Garcia-Hernandez, DA, Nitschelm, C, Lane, RR, Thomas, D, Zhang, K, Lian, J, Lian, J, Zasowski, G, Hasselquist, S, Holtzman, JA, Boardman, N, Cunha, K, Fernández-Trincado, JG, Frinchaboy, PM, Garcia-Hernandez, DA, Nitschelm, C, Lane, RR, Thomas, D, and Zhang, K

Abstract

Stellar radial migration plays an important role in reshaping a galaxy's structure and the radial distribution of stellar population properties. In this work, we revisit reported observational evidence for radial migration and quantify its strength using the age-[Fe/H] distribution of stars across the Milky Way with APOGEE data. We find a broken age-[Fe/H] relation in the Galactic disc at r > 6 kpc, with a more pronounced break at larger radii. To quantify the strength of radial migration, we assume stars born at each radius have a unique age and metallicity, and then decompose the metallicity distribution function (MDF) of mono-age young populations into different Gaussian components that originated from various birth radii at rbirth < 13 kpc. We find that, at ages of 2 and 3 Gyr, roughly half the stars were formed within 1 kpc of their present radius, and very few stars (<5 per cent) were formed more than 4 kpc away from their present radius. These results suggest limited short-distance radial migration and inefficient long-distance migration in the Milky Way during the last 3 Gyr. In the very outer disc beyond 15 kpc, the observed age-[Fe/H] distribution is consistent with the prediction of pure radial migration from smaller radii, suggesting a migration origin of the very outer disc. We also estimate intrinsic metallicity gradients at ages of 2 and 3 Gyr of-0.061 and-0.063 dex kpc-1, respectively.

Published
2022

14. The Milky Way bar and bulge revealed by APOGEE and Gaia EDR3

Author

Queiroz, A. B. A., primary, Chiappini, C., additional, Perez-Villegas, A., additional, Khalatyan, A., additional, Anders, F., additional, Barbuy, B., additional, Santiago, B. X., additional, Steinmetz, M., additional, Cunha, K., additional, Schultheis, M., additional, Majewski, S. R., additional, Minchev, I., additional, Minniti, D., additional, Beaton, R. L., additional, Cohen, R. E., additional, da Costa, L. N., additional, Fernández-Trincado, J. G., additional, Garcia-Hernández, D. A., additional, Geisler, D., additional, Hasselquist, S., additional, Lane, R. R., additional, Nitschelm, C., additional, Rojas-Arriagada, A., additional, Roman-Lopes, A., additional, Smith, V., additional, and Zasowski, G., additional

Published
2021
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15. Final Targeting Strategy for the Sloan Digital Sky Survey IV Apache Point Observatory Galactic Evolution Experiment 2 North Survey

Author

Beaton, RL, Beaton, RL, Oelkers, RJ, Hayes, CR, Covey, KR, Chojnowski, SD, De Lee, N, Sobeck, JS, Majewski, SR, Cohen, RE, Fernández-Trincado, J, Longa-Pea, P, O'Connell, JE, Santana, FA, Stringfellow, GS, Zasowski, G, Aerts, C, Anguiano, B, Bender, C, Caas, CI, Cunha, K, Donor, J, Fleming, SW, Frinchaboy, PM, Feuillet, D, Harding, P, Hasselquist, S, Holtzman, JA, Johnson, JA, Kollmeier, JA, Kounkel, M, Mahadevan, S, Price-Whelan, AM, Rojas-Arriagada, A, Román-Zúiga, C, Schlafly, EF, Schultheis, M, Shetrone, M, Simon, JD, Stassun, KG, Stutz, AM, Tayar, J, Teske, J, Tkachenko, A, Troup, N, Albareti, FD, Bizyaev, D, Bovy, J, Burgasser, AJ, Comparat, J, Downes, JJ, Geisler, D, Inno, L, Manchado, A, Ness, MK, Pinsonneault, MH, Prada, F, Roman-Lopes, A, Simonian, GVA, Smith, VV, Yan, R, Zamora, O, Beaton, RL, Beaton, RL, Oelkers, RJ, Hayes, CR, Covey, KR, Chojnowski, SD, De Lee, N, Sobeck, JS, Majewski, SR, Cohen, RE, Fernández-Trincado, J, Longa-Pea, P, O'Connell, JE, Santana, FA, Stringfellow, GS, Zasowski, G, Aerts, C, Anguiano, B, Bender, C, Caas, CI, Cunha, K, Donor, J, Fleming, SW, Frinchaboy, PM, Feuillet, D, Harding, P, Hasselquist, S, Holtzman, JA, Johnson, JA, Kollmeier, JA, Kounkel, M, Mahadevan, S, Price-Whelan, AM, Rojas-Arriagada, A, Román-Zúiga, C, Schlafly, EF, Schultheis, M, Shetrone, M, Simon, JD, Stassun, KG, Stutz, AM, Tayar, J, Teske, J, Tkachenko, A, Troup, N, Albareti, FD, Bizyaev, D, Bovy, J, Burgasser, AJ, Comparat, J, Downes, JJ, Geisler, D, Inno, L, Manchado, A, Ness, MK, Pinsonneault, MH, Prada, F, Roman-Lopes, A, Simonian, GVA, Smith, VV, Yan, R, and Zamora, O

Abstract

The Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2) is a dual-hemisphere, near-infrared (NIR), spectroscopic survey with the goal of producing a chemodynamical mapping of the Milky Way. The targeting for APOGEE-2 is complex and has evolved with time. In this paper, we present the updates and additions to the initial targeting strategy for APOGEE-2N presented in Zasowski et al. (2017). These modifications come in two implementation modes: (i) "Ancillary Science Programs"competitively awarded to Sloan Digital Sky Survey IV PIs through proposal calls in 2015 and 2017 for the pursuit of new scientific avenues outside the main survey, and (ii) an effective 1.5 yr expansion of the survey, known as the Bright Time Extension (BTX), made possible through accrued efficiency gains over the first years of the APOGEE-2N project. For the 23 distinct ancillary programs, we provide descriptions of the scientific aims, target selection, and how to identify these targets within the APOGEE-2 sample. The BTX permitted changes to the main survey strategy, the inclusion of new programs in response to scientific discoveries or to exploit major new data sets not available at the outset of the survey design, and expansions of existing programs to enhance their scientific success and reach. After describing the motivations, implementation, and assessment of these programs, we also leave a summary of lessons learned from nearly a decade of APOGEE-1 and APOGEE-2 survey operations. A companion paper, F. Santana et al. (submitted; AAS29036), provides a complementary presentation of targeting modifications relevant to APOGEE-2 operations in the Southern Hemisphere.

Published
2021

16. Open Cluster Chemical Homogeneity throughout the Milky Way

Author

Poovelil, Vijith Jacob, primary, Zasowski, G., additional, Hasselquist, S., additional, Seth, A., additional, Donor, John, additional, Beaton, Rachael L., additional, Cunha, K., additional, Frinchaboy, Peter M., additional, García-Hernández, D. A., additional, Hawkins, K., additional, Kratter, K. M., additional, Lane, Richard R., additional, and Nitschelm, C., additional

Published
2020
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17. Cool stars in the Galactic center as seen by APOGEE

Author

Schultheis, M., primary, Rojas-Arriagada, A., additional, Cunha, K., additional, Zoccali, M., additional, Chiappini, C., additional, Zasowski, G., additional, Queiroz, A. B. A., additional, Minniti, D., additional, Fritz, T., additional, García-Hernández, D. A., additional, Nitschelm, C., additional, Zamora, O., additional, Hasselquist, S., additional, Fernández-Trincado, J. G., additional, and Munoz, R. R., additional

Published
2020
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18. APOGEE Chemical Abundances of the Large Magellanic Cloud

Author

Hasselquist, S., Nidever, D., Hayes, C., Anguiano, B., Majewski, S., Sobeck, J., Stringfellow, G., Beers, T., Jonsson, H., Lian, J., Cohen, R., Zasowski, G., Mackereth, J., Battaglia, G., Weinberg, D., Lane, R., Long-Pena, P., Gallart, C., Villanova, S., Rix, H., Andrews, B., Cunha, K., Smith, V., Choi, Y., Geisler, D., Carrera, R., Almeida, A., and Fernandez-Trincado, J.

Abstract

To date, the SDSS-IV APOGEE survey has obtained S/N > 70 spectra for over 2,500 red giant stars distributed across much of the Large Magellanic Cloud (LMC), allowing for the characterization of the detailed abundance patterns for 10+ chemical elements. In this project, we interpret the chemical abundance patterns of the LMC by comparing them to the chemical abundance patterns of the Sagittarius Dwarf Galaxy (Sgr) and the Milky Way (MW), as well as by invoking chemical evolution models (such as flexCE and chempy) that include the LMC's star formation history. Preliminary results show that the LMC shares [Ni/Fe] and [Al/Fe] deficiencies with Sgr, but exhibits alpha-element abundances ([O/Fe], [Mg/Fe], and [Si/Fe]) that are near-solar. There is also a correlation with [O/Fe] and [Mg/Fe] with [Fe/H] at [Fe/H] > -1.0. These results suggest that the LMC exhibited low star formation efficiency (as compared to Sgr and the MW) at early times, but has since experienced several starbursts which spawned the stars with [Fe/H] > -1.0. Using these APOGEE chemical abundance patterns as constraints, we use chemical evolution models to better characterize the nature (strength, time, duration, IMF, etc.) of these starbursts.

Published
2019

19. H-band discovery of additional second-generation stars in the Galactic bulge globular cluster NGC 6522 as observed by APOGEE and Gaia

Author

Fernández-Trincado, J. G., primary, Zamora, O., additional, Souto, Diogo, additional, Cohen, R. E., additional, Dell’Agli, F., additional, García-Hernández, D. A., additional, Masseron, T., additional, Schiavon, R. P., additional, Mészáros, Sz., additional, Cunha, K., additional, Hasselquist, S., additional, Shetrone, M., additional, Schiappacasse Ulloa, J., additional, Tang, B., additional, Geisler, D., additional, Schleicher, D. R. G., additional, Villanova, S., additional, Mennickent, R. E., additional, Minniti, D., additional, Alonso-García, J., additional, Manchado, A., additional, Beers, T. C., additional, Sobeck, J., additional, Zasowski, G., additional, Schultheis, M., additional, Majewski, S. R., additional, Rojas-Arriagada, A., additional, Almeida, A., additional, Santana, F., additional, Oelkers, R. J., additional, Longa-Peña, P., additional, Carrera, R., additional, Burgasser, A. J., additional, Lane, R. R., additional, Roman-Lopes, A., additional, Ivans, I. I., additional, and Hearty, F. R., additional

Published
2019
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20. APOGEE DR14/DR15 Abundances in the Inner Milky Way

Author

Zasowski, G., primary, Schultheis, M., additional, Hasselquist, S., additional, Cunha, K., additional, Sobeck, J., additional, Johnson, J. A., additional, Rojas-Arriagada, A., additional, Majewski, S. R., additional, Andrews, B. H., additional, Jönsson, H., additional, Beers, T. C., additional, Chojnowski, S. D., additional, Frinchaboy, P. M., additional, Holtzman, J. A., additional, Minniti, D., additional, Nidever, D. L., additional, and Nitschelm, C., additional

Published
2019
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21. A Chemical and Kinematical Analysis of the Intermediate-age Open Cluster IC 166 from APOGEE and Gaia DR2

Author

Schiappacasse-Ulloa, J., primary, Tang, B., additional, Fernández-Trincado, J. G., additional, Zamora, O., additional, Geisler, D., additional, Frinchaboy, P., additional, Schultheis, M., additional, Dell’Agli, F., additional, Villanova, S., additional, Masseron, T., additional, Mészáros, Sz., additional, Souto, D., additional, Hasselquist, S., additional, Cunha, K., additional, Smith, V. V., additional, García-Hernández, D. A., additional, Vieira, K., additional, Robin, A. C., additional, Minniti, D., additional, Zasowski, G., additional, Moreno, E., additional, Pérez-Villegas, A., additional, Lane, R. R., additional, Ivans, I. I., additional, Pan, K., additional, Nitschelm, C., additional, Santana, F. A., additional, Carrera, R., additional, and Roman-Lopes, A., additional

Published
2018
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23. CHEMICAL TAGGING CAN WORK: IDENTIFICATION of STELLAR PHASE-SPACE STRUCTURES PURELY by CHEMICAL-ABUNDANCE SIMILARITY

Author

Hogg, DW, Casey, AR, Ness, M, Rix, HW, Foreman-Mackey, D, Hasselquist, S, Ho, AYQ, Holtzman, JA, Majewski, SR, Martell, SL, Mészáros, S, Nidever, DL, Shetrone, M, Hogg, DW, Casey, AR, Ness, M, Rix, HW, Foreman-Mackey, D, Hasselquist, S, Ho, AYQ, Holtzman, JA, Majewski, SR, Martell, SL, Mészáros, S, Nidever, DL, and Shetrone, M

Abstract

Chemical tagging promises to use detailed abundance measurements to identify spatially separated stars that were, in fact, born together (in the same molecular cloud) long ago. This idea has not yielded much practical success, presumably because of the noise and incompleteness in chemical-abundance measurements. We have succeeded in substantially improving spectroscopic measurements with The Cannon, which has now delivered 15 individual abundances for stars observed as part of the APOGEE spectroscopic survey, with precisions around 0.04 dex. We test the chemical-tagging hypothesis by looking at clusters in abundance space and confirming that they are clustered in phase space. We identify (by the k-means algorithm) overdensities of stars in the 15-dimensional chemical-abundance space delivered by The Cannon, and plot the associated stars in phase space. We use only abundance-space information (no positional information) to identify stellar groups. We find that clusters in abundance space are indeed clusters in phase space, and we recover some known phase-space clusters and find other interesting structures. This is the first-ever project to identify phase-space structures at the survey-scale by blind search purely in abundance space; it verifies the precision of the abundance measurements delivered by The Cannon; the prospects for future data sets appear very good.

Published
2016

24. TARGET SELECTION FOR THE APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT (APOGEE)

Author

Zasowski, G., primary, Johnson, Jennifer A., additional, Frinchaboy, P. M., additional, Majewski, S. R., additional, Nidever, D. L., additional, Pinto, H. J. Rocha, additional, Girardi, L., additional, Andrews, B., additional, Chojnowski, S. D., additional, Cudworth, K. M., additional, Jackson, K., additional, Munn, J., additional, Skrutskie, M. F., additional, Beaton, R. L., additional, Blake, C. H., additional, Covey, K., additional, Deshpande, R., additional, Epstein, C., additional, Fabbian, D., additional, Fleming, S. W., additional, Hernandez, D. A. Garcia, additional, Herrero, A., additional, Mahadevan, S., additional, Mészáros, Sz., additional, Schultheis, M., additional, Sellgren, K., additional, Terrien, R., additional, van Saders, J., additional, Prieto, C. Allende, additional, Bizyaev, D., additional, Burton, A., additional, Cunha, K., additional, da Costa, L. N., additional, Hasselquist, S., additional, Hearty, F., additional, Holtzman, J., additional, García Pérez, A. E., additional, Maia, M. A. G., additional, O'Connell, R. W., additional, O'Donnell, C., additional, Pinsonneault, M., additional, Santiago, B. X., additional, Schiavon, R. P., additional, Shetrone, M., additional, Smith, V., additional, and Wilson, J. C., additional

Published
2013
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25. Efficacy of ceftriaxone in serious bacterial infections

Author

Epstein, J S, Hasselquist, S M, and Simon, G L

Abstract

Ceftriaxone is a new semisynthetic cephalosporin with broad-spectrum in vitro activity and an unusually long serum half-life. The clinical efficacy of ceftriaxone was evaluated in 35 infections in 34 patients; 12 of these patients had skin and soft tissue infections, 10 had infections of the urinary tract, 8 had pneumonia, 2 had biliary tract infections, 1 had sinusitis, 1 had diverticulitis, and 1 had a retroperitoneal abscess. Of the 35 infections, 9 were bacteremic. The bacteria isolated included Staphylococcus aureus, Staphylococcus epidermidis, Streptococcus pneumoniae, Streptococcus faecalis, other streptococcal species, Escherichia coli, Proteus mirabilis, Klebsiella pneumoniae, Serratia marcescens, Enterobacter cloacae, Haemophilus influenzae, Pseudomonas aeruginosa, Bacteroides fragilis, other Bacteroides species, and anaerobic cocci. Improvement or cure occurred in 32 episodes, for a response rate of 91%. There were three treatment failures in patients with soft tissue infections. No serious drug toxicities were observed. At a dosage regimen of 1 g every 12 h the peak and trough serum antibiotic concentrations were well above the minimal inhibitory concentrations of most pathogens. Our findings suggest that ceftriaxone is a safe and effective antibiotic for therapy of serious bacterial infections.

Published
1982
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26. The 16th Data Release of the Sloan Digital Sky Surveys : First Release from the APOGEE-2 Southern Survey and Full Release of eBOSS Spectra

Author

Romina Ahumada, Carlos Allende Prieto, Andrés Almeida, Friedrich Anders, Scott F. Anderson, Brett H. Andrews, Borja Anguiano, Riccardo Arcodia, Eric Armengaud, Marie Aubert, Santiago Avila, Vladimir Avila-Reese, Carles Badenes, Christophe Balland, Kat Barger, Jorge K. Barrera-Ballesteros, Sarbani Basu, Julian Bautista, Rachael L. Beaton, Timothy C. Beers, B. Izamar T. Benavides, Chad F. Bender, Mariangela Bernardi, Matthew Bershady, Florian Beutler, Christian Moni Bidin, Jonathan Bird, Dmitry Bizyaev, Guillermo A. Blanc, Michael R. Blanton, Médéric Boquien, Jura Borissova, Jo Bovy, W. N. Brandt, Jonathan Brinkmann, Joel R. Brownstein, Kevin Bundy, Martin Bureau, Adam Burgasser, Etienne Burtin, Mariana Cano-Díaz, Raffaella Capasso, Michele Cappellari, Ricardo Carrera, Solène Chabanier, William Chaplin, Michael Chapman, Brian Cherinka, Cristina Chiappini, Peter Doohyun Choi, S. Drew Chojnowski, Haeun Chung, Nicolas Clerc, Damien Coffey, Julia M. Comerford, Johan Comparat, Luiz da Costa, Marie-Claude Cousinou, Kevin Covey, Jeffrey D. Crane, Katia Cunha, Gabriele da Silva Ilha, Yu Sophia Dai, Sanna B. Damsted, Jeremy Darling, James W. Davidson, Roger Davies, Kyle Dawson, Nikhil De, Axel de la Macorra, Nathan De Lee, Anna Bárbara de Andrade Queiroz, Alice Deconto Machado, Sylvain de la Torre, Flavia Dell’Agli, Hélion du Mas des Bourboux, Aleksandar M. Diamond-Stanic, Sean Dillon, John Donor, Niv Drory, Chris Duckworth, Tom Dwelly, Garrett Ebelke, Sarah Eftekharzadeh, Arthur Davis Eigenbrot, Yvonne P. Elsworth, Mike Eracleous, Ghazaleh Erfanianfar, Stephanie Escoffier, Xiaohui Fan, Emily Farr, José G. Fernández-Trincado, Diane Feuillet, Alexis Finoguenov, Patricia Fofie, Amelia Fraser-McKelvie, Peter M. Frinchaboy, Sebastien Fromenteau, Hai Fu, Lluís Galbany, Rafael A. Garcia, D. A. García-Hernández, Luis Alberto Garma Oehmichen, Junqiang Ge, Marcio Antonio Geimba Maia, Doug Geisler, Joseph Gelfand, Julian Goddy, Violeta Gonzalez-Perez, Kathleen Grabowski, Paul Green, Catherine J. Grier, Hong Guo, Julien Guy, Paul Harding, Sten Hasselquist, Adam James Hawken, Christian R. Hayes, Fred Hearty, S. Hekker, David W. Hogg, Jon A. Holtzman, Danny Horta, Jiamin Hou, Bau-Ching Hsieh, Daniel Huber, Jason A. S. Hunt, J. Ider Chitham, Julie Imig, Mariana Jaber, Camilo Eduardo Jimenez Angel, Jennifer A. Johnson, Amy M. Jones, Henrik Jönsson, Eric Jullo, Yerim Kim, Karen Kinemuchi, Charles C. Kirkpatrick IV, George W. Kite, Mark Klaene, Jean-Paul Kneib, Juna A. Kollmeier, Hui Kong, Marina Kounkel, Dhanesh Krishnarao, Ivan Lacerna, Ting-Wen Lan, Richard R. Lane, David R. Law, Jean-Marc Le Goff, Henry W. Leung, Hannah Lewis, Cheng Li, Jianhui Lian, Lihwai Lin, Dan Long, Penélope Longa-Peña, Britt Lundgren, Brad W. Lyke, J. Ted Mackereth, Chelsea L. MacLeod, Steven R. Majewski, Arturo Manchado, Claudia Maraston, Paul Martini, Thomas Masseron, Karen L. Masters, Savita Mathur, Richard M. McDermid, Andrea Merloni, Michael Merrifield, Szabolcs Mészáros, Andrea Miglio, Dante Minniti, Rebecca Minsley, Takamitsu Miyaji, Faizan Gohar Mohammad, Benoit Mosser, Eva-Maria Mueller, Demitri Muna, Andrea Muñoz-Gutiérrez, Adam D. Myers, Seshadri Nadathur, Preethi Nair, Kirpal Nandra, Janaina Correa do Nascimento, Rebecca Jean Nevin, Jeffrey A. Newman, David L. Nidever, Christian Nitschelm, Pasquier Noterdaeme, Julia E. O’Connell, Matthew D. Olmstead, Daniel Oravetz, Audrey Oravetz, Yeisson Osorio, Zachary J. Pace, Nelson Padilla, Nathalie Palanque-Delabrouille, Pedro A. Palicio, Hsi-An Pan, Kaike Pan, James Parker, Romain Paviot, Sebastien Peirani, Karla Peña Ramŕez, Samantha Penny, Will J. Percival, Ismael Perez-Fournon, Ignasi Pérez-Ràfols, Patrick Petitjean, Matthew M. Pieri, Marc Pinsonneault, Vijith Jacob Poovelil, Joshua Tyler Povick, Abhishek Prakash, Adrian M. Price-Whelan, M. Jordan Raddick, Anand Raichoor, Amy Ray, Sandro Barboza Rembold, Mehdi Rezaie, Rogemar A. Riffel, Rogério Riffel, Hans-Walter Rix, Annie C. Robin, A. Roman-Lopes, Carlos Román-Zúñiga, Benjamin Rose, Ashley J. Ross, Graziano Rossi, Kate Rowlands, Kate H. R. Rubin, Mara Salvato, Ariel G. Sánchez, Laura Sánchez-Menguiano, José R. Sánchez-Gallego, Conor Sayres, Adam Schaefer, Ricardo P. Schiavon, Jaderson S. Schimoia, Edward Schlafly, David Schlegel, Donald P. Schneider, Mathias Schultheis, Axel Schwope, Hee-Jong Seo, Aldo Serenelli, Arman Shafieloo, Shoaib Jamal Shamsi, Zhengyi Shao, Shiyin Shen, Matthew Shetrone, Raphael Shirley, Víctor Silva Aguirre, Joshua D. Simon, M. F. Skrutskie, Anže Slosar, Rebecca Smethurst, Jennifer Sobeck, Bernardo Cervantes Sodi, Diogo Souto, David V. Stark, Keivan G. Stassun, Matthias Steinmetz, Dennis Stello, Julianna Stermer, Thaisa Storchi-Bergmann, Alina Streblyanska, Guy S. Stringfellow, Amelia Stutz, Genaro Suárez, Jing Sun, Manuchehr Taghizadeh-Popp, Michael S. Talbot, Jamie Tayar, Aniruddha R. Thakar, Riley Theriault, Daniel Thomas, Zak C. Thomas, Jeremy Tinker, Rita Tojeiro, Hector Hernandez Toledo, Christy A. Tremonti, Nicholas W. Troup, Sarah Tuttle, Eduardo Unda-Sanzana, Marica Valentini, Jaime Vargas-González, Mariana Vargas-Magaña, Jose Antonio Vázquez-Mata, M. Vivek, David Wake, Yuting Wang, Benjamin Alan Weaver, Anne-Marie Weijmans, Vivienne Wild, John C. Wilson, Robert F. Wilson, Nathan Wolthuis, W. M. Wood-Vasey, Renbin Yan, Meng Yang, Christophe Yèche, Olga Zamora, Pauline Zarrouk, Gail Zasowski, Kai Zhang, Cheng Zhao, Gongbo Zhao, Zheng Zheng, Guangtun Zhu, Hu Zou, Department of Physics, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofisica de Canarias (IAC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Universidad Nacional Autónoma de México (UNAM), Department of Astrophysical Sciences [Princeton], Princeton University, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Department of Astronomy, Yale University [New Haven], University of Notre Dame [Indiana] (UND), Department of Physics and Astronomy [Philadelphia], University of Pennsylvania [Philadelphia], University of Wisconsin-Madison, Texas Tech University Health Sciences Center, Texas Tech University [Lubbock] (TTU), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), California Institute of Technology (CALTECH), Sub-department of Astrophysics [Oxford], Department of Physics [Oxford], University of Oxford [Oxford]-University of Oxford [Oxford], Center for Astrophysics and Space Sciences [La Jolla] (CASS), University of California [San Diego] (UC San Diego), University of California-University of California, Department of Psychology, St John's University, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Departamento de FisicaTeorica e IFT-UAM/CSIC, Universidad Autonoma de Madrid (UAM), Lowell Observatory [Flagstaff], Observatorio Nacional [Rio de Janeiro], Vernalis (R&D) Ltd, Special Care Dentistry, UCLH Eastman Dental Hospital, University of Utah, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universidad de La Laguna [Tenerife - SP] (ULL), University of Virginia [Charlottesville], University of Wyoming (UW), School of Physics and Astronomy, University of Birmingham [Birmingham], Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Arizona State University [Tempe] (ASU), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Max-Planck-Institut für Astronomie (MPIA), Texas Christian University (TCU), Department of Physics and Astronomy [Irvine], University of California [Irvine] (UCI), Department of Physics and Astronomy [Pittsburgh], University of Pittsburgh (PITT), Pennsylvania Commonwealth System of Higher Education (PCSHE)-Pennsylvania Commonwealth System of Higher Education (PCSHE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), New York University [New York] (NYU), NYU System (NYU), Research Institute of Forest Resource Information Techniques, Chinese Academy of Forestry, New Mexico State University, Pennsylvania State University (Penn State), Penn State System, Princess Margaret Hospital, University of Toronto, Cognition, Langues, Langage, Ergonomie (CLLE-ERSS), École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Toulouse - Jean Jaurès (UT2J)-Université Bordeaux Montaigne-Centre National de la Recherche Scientifique (CNRS), J. A. Baker Institute, Cornell University [New York], Institute of Infection, Immunity & Inflammation, University of Glasgow, Sainsbury Laboratory Cambridge University (SLCU), University of Cambridge [UK] (CAM), Ecole Polytechnique Fédérale de Lausanne (EPFL), Carnegie Observatories, Carnegie Institution for Science [Washington], Institute of Science and Technology [Austria] (IST Austria), Universidad de Atacama, Department of Chemical and Biomolecular Engineering, Universidad de Antofagasta, Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Institute of cosmology and gravitation, University of Portsmouth, Institut d'Astronomie et d'Astrophysique [Bruxelles] (IAA), Université libre de Bruxelles (ULB), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Max-Planck-Institut für Astrophysik (MPA), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département des Sciences et Gestion de l'Environnement/Océanologie [Liège], Université de Liège, Universidad Andrés Bello [Santiago] (UNAB), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Montana State University (MSU), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Astronomy (Ohio State University), Ohio State University [Columbus] (OSU), Institut Lagrange de Paris, Sorbonne Université (SU), The Wellcome Trust Centre for Human Genetics [Oxford], University of Oxford [Oxford], Liverpool John Moores University (LJMU), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institute of Space Sciences [Barcelona] (ICE-CSIC), Spanish National Research Council [Madrid] (CSIC), Chinese Academy of Sciences [Beijing] (CAS), McDonald Observatory, University of Texas at Austin [Austin], Astronomy Centre, University of Sussex, Department of Physics and Astronomy [Aarhus], Aarhus University [Aarhus], University of Washington [Seattle], Vanderbilt University [Nashville], Stellar Astrophysics Centre [Aarhus] (SAC), University of Colorado [Boulder], Laboratoire de Biochimie Médicale (LBM), CHU Rouen, Normandie Université (NU)-Normandie Université (NU), University of St Andrews [Scotland], Instituto de Astronomıa, universidad catolica del Norte, Institut d'Astrophysique et de Géophysique [Liège], Laboratoire de Physique des Solides (LPS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Department of Computer Science and Engineering [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Dunlap Institute for Astronomy and Astrophysics [Toronto], World Bank, State Key Laboratory in Computer Science [Beijing] (SKLCS), Institute of Software Chinese Academy of Sciences [Beijing], Nanjing University of Information Science and Technology (NUIST), Laboratoire de Chimie - UMR5182 (LC), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon)-Institut de Chimie du CNRS (INC), Johns Hopkins University (JHU), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of Pennsylvania, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of Oxford-University of Oxford, University of California (UC)-University of California (UC), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universidad Autónoma de Madrid (UAM), University of Virginia, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), University of California [Irvine] (UC Irvine), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), École Pratique des Hautes Études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Bordeaux Montaigne (UBM)-Centre National de la Recherche Scientifique (CNRS), Carnegie Institution for Science, Institute of Science and Technology [Klosterneuburg, Austria] (IST Austria), Harvard University-Smithsonian Institution, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of Oxford, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Ahumada R., Prieto C.A., Almeida A., Anders F., Anderson S.F., Andrews B.H., Anguiano B., Arcodia R., Armengaud E., Aubert M., Avila S., Avila-Reese V., Badenes C., Balland C., Barger K., Barrera-Ballesteros J.K., Basu S., Bautista J., Beaton R.L., Beers T.C., Benavides B.I.T., Bender C.F., Bernardi M., Bershady M., Beutler F., Bidin C.M., Bird J., Bizyaev D., Blanc G.A., Blanton M.R., Boquien M., Borissova J., Bovy J., Brandt W.N., Brinkmann J., Brownstein J.R., Bundy K., Bureau M., Burgasser A., Burtin E., Cano-Diaz M., Capasso R., Cappellari M., Carrera R., Chabanier S., Chaplin W., Chapman M., Cherinka B., Chiappini C., Doohyun Choi P., Chojnowski S.D., Chung H., Clerc N., Coffey D., Comerford J.M., Comparat J., Da Costa L., Cousinou M.-C., Covey K., Crane J.D., Cunha K., Ilha G.D.S., Dai Y.S., Damsted S.B., Darling J., Davidson J.W., Davies R., Dawson K., De N., De La Macorra A., De Lee N., Queiroz A.B.D.A., Deconto Machado A., De La Torre S., Dell'Agli F., Du Mas Des Bourboux H., Diamond-Stanic A.M., Dillon S., Donor J., Drory N., Duckworth C., Dwelly T., Ebelke G., Eftekharzadeh S., Davis Eigenbrot A., Elsworth Y.P., Eracleous M., Erfanianfar G., Escoffier S., Fan X., Farr E., Fernandez-Trincado J.G., Feuillet D., Finoguenov A., Fofie P., Fraser-Mckelvie A., Frinchaboy P.M., Fromenteau S., Fu H., Galbany L., Garcia R.A., Garcia-Hernandez D.A., Oehmichen L.A.G., Ge J., Maia M.A.G., Geisler D., Gelfand J., Goddy J., Gonzalez-Perez V., Grabowski K., Green P., Grier C.J., Guo H., Guy J., Harding P., Hasselquist S., Hawken A.J., Hayes C.R., Hearty F., Hekker S., Hogg D.W., Holtzman J.A., Horta D., Hou J., Hsieh B.-C., Huber D., Hunt J.A.S., Chitham J.I., Imig J., Jaber M., Angel C.E.J., Johnson J.A., Jones A.M., Jonsson H., Jullo E., Kim Y., Kinemuchi K., Kirkpatrick Iv C.C., Kite G.W., Klaene M., Kneib J.-P., Kollmeier J.A., Kong H., Kounkel M., Krishnarao D., Lacerna I., Lan T.-W., Lane R.R., Law D.R., Le Goff J.-M., Leung H.W., Lewis H., Li C., Lian J., Lin L., Long D., Longa-Peña P., Lundgren B., Lyke B.W., Ted Mackereth J., Macleod C.L., Majewski S.R., Manchado A., Maraston C., Martini P., Masseron T., Masters K.L., Mathur S., McDermid R.M., Merloni A., Merrifield M., Meszaros S., Miglio A., Minniti D., Minsley R., Miyaji T., Mohammad F.G., Mosser B., Mueller E.-M., Muna D., Muñoz-Gutierrez A., Myers A.D., Nadathur S., Nair P., Nandra K., Do Nascimento J.C., Nevin R.J., Newman J.A., Nidever D.L., Nitschelm C., Noterdaeme P., O'Connell J.E., Olmstead M.D., Oravetz D., Oravetz A., Osorio Y., Pace Z.J., Padilla N., Palanque-Delabrouille N., Palicio P.A., Pan H.-A., Pan K., Parker J., Paviot R., Peirani S., Ramrez K.P., Penny S., Percival W.J., Perez-Fournon I., Perez-Rafols I., Petitjean P., Pieri M.M., Pinsonneault M., Poovelil V.J., Povick J.T., Prakash A., Price-Whelan A.M., Raddick M.J., Raichoor A., Ray A., Rembold S.B., Rezaie M., Riffel R.A., Riffel R., Rix H.-W., Robin A.C., Roman-Lopes A., Roman-Zuñiga C., Rose B., Ross A.J., Rossi G., Rowlands K., Rubin K.H.R., Salvato M., Sanchez A.G., Sanchez-Menguiano L., Sanchez-Gallego J.R., Sayres C., Schaefer A., Schiavon R.P., Schimoia J.S., Schlafly E., Schlegel D., Schneider D.P., Schultheis M., Schwope A., Seo H.-J., Serenelli A., Shafieloo A., Shamsi S.J., Shao Z., Shen S., Shetrone M., Shirley R., Aguirre V.S., Simon J.D., Skrutskie M.F., Slosar A., Smethurst R., Sobeck J., Sodi B.C., Souto D., Stark D.V., Stassun K.G., Steinmetz M., Stello D., Stermer J., Storchi-Bergmann T., Streblyanska A., Stringfellow G.S., Stutz A., Suarez G., Sun J., Taghizadeh-Popp M., Talbot M.S., Tayar J., Thakar A.R., Theriault R., Thomas D., Thomas Z.C., Tinker J., Tojeiro R., Toledo H.H., Tremonti C.A., Troup N.W., Tuttle S., Unda-Sanzana E., Valentini M., Vargas-Gonzalez J., Vargas-Magaña M., Vazquez-Mata J.A., Vivek M., Wake D., Wang Y., Weaver B.A., Weijmans A.-M., Wild V., Wilson J.C., Wilson R.F., Wolthuis N., Wood-Vasey W.M., Yan R., Yang M., Yeche C., Zamora O., Zarrouk P., Zasowski G., Zhang K., Zhao C., Zhao G., Zheng Z., Zhu G., Zou H., Alfred P. Sloan Foundation, and Department of Energy (US)

Subjects
Optical telescopes, SAMPLE, Astrophysics, 01 natural sciences, Astronomi, astrofysik och kosmologi, Infrared astronomy, Observatory, Astronomy, Astrophysics and Cosmology, Astrophysics::Solar and Stellar Astrophysics, REDSHIFT 0.8, redshift surveys, stellar spectral lines, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, Astronomy databases, Redshift surveys, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, stellar properties, CATALOG, astro-ph.CO, astronomy databases, Data release, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], infrared astonomy, TELESCOPE, astro-ph.GA, media_common.quotation_subject, Astrophysics::Cosmology and Extragalactic Astrophysics, MASS, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Galactic abundances, Stellar properties, 0103 physical sciences, Astrophysics::Galaxy Astrophysics, DISTANCES, Stellar spectral lines, 010308 nuclear & particles physics, Astronomy and Astrophysics, optical telescopes, 115 Astronomy, Space science, Galaxy, GALAXY, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], STELLAR, 13. Climate action, Space and Planetary Science, Sky, [SDU]Sciences of the Universe [physics], galactic abundances, MILKY, astro-ph.IM, SDSS-IV MANGA
Abstract

This paper documents the 16th data release (DR16) from the Sloan Digital Sky Surveys (SDSS), the fourth and penultimate from the fourth phase (SDSS-IV). This is the first release of data from the Southern Hemisphere survey of the Apache Point Observatory Galactic Evolution Experiment 2 (APOGEE-2); new data from APOGEE-2 North are also included. DR16 is also notable as the final data release for the main cosmological program of the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), and all raw and reduced spectra from that project are released here. DR16 also includes all the data from the Time Domain Spectroscopic Survey and new data from the SPectroscopic IDentification of ERosita Survey programs, both of which were co-observed on eBOSS plates. DR16 has no new data from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey (or the MaNGA Stellar Library "MaStar"). We also preview future SDSS-V operations (due to start in 2020), and summarize plans for the final SDSS-IV data release (DR17)., 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.

Published
2020

27. PET scanning in sarcoidosis.

Author

Jain V, Hasselquist S, and Delaney MD

Subjects
Humans, Sarcoidosis pathology, Positron-Emission Tomography methods, Sarcoidosis diagnosis
Abstract

Sarcoidosis is a multisystem granulomatous disorder that most commonly presents with pulmonary involvement. The diagnosis is suggested on the basis of clinical and radiologic manifestations and is supported by the histological demonstration of noncaseating granulomas in affected tissues. Different imaging modalities, including chest radiography, X-rays, computed tomography, magnetic resonance imaging, and (67) Ga scintigraphy are currently employed to help diagnose and help plan treatment strategy in sarcoidosis patients. Here, we discuss the potential role of positron emission tomography in the diagnosis, assessment of disease activity, and management of patients with sarcoidosis. We also point out some of the limitations of this technique., (© 2011 New York Academy of Sciences.)

Published
2011
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28. Disseminated pneumocystosis presenting as a pleural effusion.

Author

Jayes RL, Kamerow HN, Hasselquist SM, Delaney MD, and Parenti DM

Subjects
Administration, Inhalation, Adult, Humans, Injections, Intravenous, Male, Pentamidine administration & dosage, Pentamidine therapeutic use, Pleural Effusion drug therapy, Pleural Effusion pathology, Pneumocystis Infections drug therapy, Pleural Effusion microbiology, Pneumocystis Infections pathology
Abstract

Extrapulmonary pneumocystosis recently has been reported in a number of tissues. Most cases occurred in patients receiving aerosolized pentamidine prophylaxis. We report a case of disseminated pneumocystosis presenting as a large pleural effusion without apparent lung involvement where Pneumocystis carinii was the only pathogen identified. The absence of parenchymal lesions on chest x-ray film, the lack of hypoxemia and the minimal uptake of gallium all argue against significant lung involvement. The patient was successfully treated with chest tube drainage, intravenous and inhaled pentamidine and orally administered dapsone and trimethoprim. The addition of inhaled pentamidine to intravenously administered pentamidine may have increased pleural fluid levels substantially and its use coincided with the patient's improvement.

Published
1993
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