The Apache Point Observatory Galactic Evolution Experiment (APOGEE) high-resolution near-infrared multi-object fiber spectrograph

Wilson, John C.; Hearty, Fred; Skrutskie, Michael F.; Majewski, Steven R.; Schiavon, Ricardo P.; Eisenstein, Daniel J.; Gunn, J. E.; Blank, Basil; Henderson, C.; Smee, Stephen A.; Barkhouser, Robert H.; Harding, Albert; Fitzgerald, Greg; Stolberg, Todd M.; Arns, Jim; Nelson, Matt; Brunner, Sophia; Burton, Adam; Walker, E.; Lam, Charles R.; Maseman, Paul; Barr, Jordan G.; Léger, F.; Carey, Larry N.; MacDonald, Nick; Horne, T. B. Van; Young, Erick T.; Rieke, G. H.; Rieke, M. J.; O'Brien, Tom; Hope, Steve; Krakula, John; Crane, Jeff; Zhao, Bo; Carr, M.; Harrison, Craig; Stoll, Robert D.; Vernieri, M.; Holtzman, Jon A.; Shetrone, Matthew; Allende-Prieto, Carlos; Johnson, Jennifer A.; Frinchaboy, Peter M.; Zasowski, Gail; Bizyaev, Dmitry; Gillespie, Bruce; Weinberg, David H.

doi:10.1117/12.856708

Cited by 114 publications

(31 citation statements)

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“…Going beyond its structural properties, the dynamical structure of the bar-bulge has been most clearly elucidated by spectroscopic studies. The line-of-sight mean velocities from the Bulge Radial Velocity Assay (BRAVA, Kunder et al 2012), Abundances and Radial velocity Galactic Origins Survey (ARGOS, Ness et al 2013b), Apache Point Observatory Galactic Evolution Experiment (APOGEE, Wilson et al 2010;Abolfathi et al 2018), Giraffe Inner Bulge Survey (GIBS, Zoccali et al 2014) and the Gaia-ESO survey (Gilmore et al 2012) all demonstrate the cylindrical rotation expected for a dynamically-formed bulge (Howard et al 2009). Furthermore, dissection of the populations by spectroscopic metallicity suggest the presence of a classical bulge component for metal-poor populations (Ness et al 2013a), whilst the metal-rich population is characterised by orbits typical of buckled bars (e.g., Williams et al 2016).…”

Section: Introductionmentioning

confidence: 94%

Transverse kinematics of the Galactic bar-bulge from VVV and Gaia

Sanders

Smith

Evans

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We analyse the kinematics of the Galactic bar-bulge using proper motions from the ESO public survey Vista Variables in the Via Lactea (VVV) and the second Gaia data release. Gaia has provided some of the first absolute proper motions within the bulge and the near-infrared VVV multi-epoch catalogue complements Gaia in highly-extincted low-latitude regions. We discuss the relative-to-absolute calibration of the VVV proper motions using Gaia. Along lines of sight spanning −10 < / deg < 10 and −10 < b/ deg < 5, we probabilistically model the density and velocity distributions as a function of distance of ∼ 45 million stars. The transverse velocities confirm the rotation signature of the bar seen in spectroscopic surveys. The differential rotation between the double peaks of the magnitude distribution confirms the X-shaped nature of the bar-bulge. Both transverse velocity components increase smoothly along the near-side of the bar towards the Galactic centre, peak at the Galactic centre and decline on the far-side. The anisotropy is σ /σ b ≈ 1.1 − 1.3 within the bulk of the bar, reducing to 0.9 − 1.1 when rotational broadening is accounted for, and exhibits a clear Xshaped signature. The vertex deviation in and b is significant | ρ b | 0.2, greater on the nearside of the bar and produces a quadrupole signature across the bulge indicating approximate radial alignment. We have re-constructed the 3D kinematics from the assumption of triaxiality, finding good agreement with spectroscopic survey results. In the co-rotating frame, we find evidence of bar-supporting x1 orbits and tangential bias in the in-plane dispersion field.

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Section: Introductionmentioning

confidence: 94%

Transverse kinematics of the Galactic bar-bulge from VVV and Gaia

Sanders

Smith

Evans

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…The first APOGEE phase was in SDSS-III and collected data between 2011 and 2014 July, obtaining highresolution (R∼22,500) spectra with a typical signal-to-noise 100 using a multiobject infrared spectrograph coupled to the 2.5 m SDSS telescope at the Apache Point Observatory (Gunn et al 2006;Wilson et al 2010). The targets map the Galactic disk, bulge, and halo (Zasowski et al 2013).…”

Section: Samplementioning

confidence: 99%

Disentangling the Galactic Halo with APOGEE. II. Chemical and Star Formation Histories for the Two Distinct Populations

Fernández-Alvar

Carigi

Schuster

et al. 2018

ApJ

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The formation processes that led to the current Galactic stellar halo are still under debate. Previous studies have provided evidence for different stellar populations in terms of elemental abundances and kinematics, pointing to different chemical and star formation histories (SFHs). In the present work, we explore, over a broader range in metallicity (-Fe H 0.5), the two stellar populations detected in the first paper of this series from metal-poor stars in DR13 of the Apache Point Observatory Galactic Evolution Experiment (APOGEE). We aim to infer signatures of the initial mass function (IMF) and the SFH from the two α-to-iron versus iron abundance chemical trends for the most APOGEE-reliable α-elements (O, Mg, Si, and Ca). Using simple chemical-evolution models, we infer the upper mass limit (M up ) for the IMF and the star formation rate, and its duration for each population. Compared with the low-α population, we obtain a more intense and longer-lived SFH, and a topheavier IMF for the high-α population.

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“…The APOGEE instrument is a cryogenic multifiber spectrograph (300 fibers; Wilson et al 2010) on the SDSS 2.5 m telescope at the Apache Point Observatory (Gunn et al 2006). The survey observations consist of high-resolution (R= λ/Δλ ∼ 22,500) spectra of stars, primarily red giants but also stars in other evolutionary stages (see Zasowski et al 2013), in the NIR (∼λ1.50-λ1.70 μm) with the ultimate goal of exploring the chemical evolution of the stellar populations in the Milky Way.…”

Section: The Apogee Spectra and The Samplementioning

confidence: 99%

Chemical Abundances of Main-sequence, Turnoff, Subgiant, and Red Giant Stars from APOGEE Spectra. I. Signatures of Diffusion in the Open Cluster M67

Souto

Cunha

Smith

et al. 2018

ApJ

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Detailed chemical abundance distributions for 14 elements are derived for eight high-probability stellar members of the solar metallicity old open cluster M67 with an age of ∼4 Gyr. The eight stars consist of four pairs, with each pair occupying a distinct phase of stellar evolution: two G dwarfs, two turnoff stars, two G subgiants, and two red clump (RC) K giants. The abundance analysis uses near-IR high-resolution spectra (λ1.5-1.7 μm) from the Apache Point Observatory Galactic Evolution Experiment survey and derives abundances for C, N, O, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, and Fe. Our derived stellar parameters and metallicity for 2M08510076+1153115 suggest that this star is a solar twin, exhibiting abundance differences relative to the Sun of 0.04 dex for all elements. Chemical homogeneity is found within each class of stars (∼0.02 dex), while significant abundance variations (∼0.05-0.20 dex) are found across the different evolutionary phases; the turnoff stars typically have the lowest abundances, while the RCs tend to have the largest. Non-LTE corrections to the LTE-derived abundances are unlikely to explain the differences. A detailed comparison of the derived Fe, Mg, Si, and Ca abundances with recently published surface abundances from stellar models that include chemical diffusion provides a good match between the observed and predicted abundances as a function of stellar mass. Such agreement would indicate the detection of chemical diffusion processes in the stellar members of M67.

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The Apache Point Observatory Galactic Evolution Experiment (APOGEE) high-resolution near-infrared multi-object fiber spectrograph

Cited by 114 publications

References 0 publications

Transverse kinematics of the Galactic bar-bulge from VVV and Gaia

Transverse kinematics of the Galactic bar-bulge from VVV and Gaia

Disentangling the Galactic Halo with APOGEE. II. Chemical and Star Formation Histories for the Two Distinct Populations

Chemical Abundances of Main-sequence, Turnoff, Subgiant, and Red Giant Stars from APOGEE Spectra. I. Signatures of Diffusion in the Open Cluster M67

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