The Milky Way Tomography with SDSS. II. Stellar Metallicity

By Željko Ivezic´, B. Sesar, Mario Juric, Nicholas A. Bond, J. J. Dalcanton, C. Rockosi, Brian Yanny, Heidi Jo Newberg, Timothy C. Beers, C. A. Prieto and 43 more. 2008

464 citations recorded by the source corpus.

Using effective temperature and metallicity derived from SDSS spectra for ~60,000 F- and G-type main-sequence stars (0.2 < g − r < 0.6), we develop polynomial models for estimating these parameters from the SDSS u − g and g − r colors. These photometric estimates have similar error properties as those determined from SDSS spectra. We apply this method to SDSS photometric data for over 2 million F/G stars and measure the unbiased metallicity distribution for a complete volume-limited sample of stars at distances between 500 pc and 8 kpc. The metallicity distribution can be exquisitely modeled using two components with a spatially varying number ratio, which correspond to disk and halo. The two components also possess the kinematics expected for disk and halo stars. The metallicity of the halo component is spatially invariant, while the median disk metallicity smoothly decreases with distance from the Galactic plane from –0.6 at 500 pc to –0.8 beyond several kiloparsecs. The absence of a correlation between metallicity and kinematics for disk stars is in a conflict with the traditional decomposition in terms of thin and thick disks. We detect coherent substructures in the kinematics-metallicity space, such as the Monoceros stream, which rotates faster than the LSR, and has a median metallicity of [Fe/H] = −0.95, with an rms scatter of only ~0.15 dex. We extrapolate our results to the performance expected from the Large Synoptic Survey Telescope (LSST) and estimate that LSST will obtain metallicity measurements accurate to 0.2 dex or better, with proper-motion measurements accurate to ~0.5 mas yr−1, for about 200 million F/G dwarf stars within a distance limit of ~100 kpc (g < 23.5).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4f2c86ea720e79d531e9499bf401cfb695592c0a

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Citations in the corpus

CHEMICAL CARTOGRAPHY WITH APOGEE: LARGE-SCALE MEAN METALLICITY MAPS OF THE MILKY WAY DISK (2013, background): “The nature of the vertical structure continues to be debated, with some studies suggesting that the thin and thick-disks are distinct populations, while others report that there is just a single component with a continuous distribution of properties (e.g., Ivezic et al. 2008; Bovy et al. 2012a,b,c).”
KINEMATICAL AND CHEMICAL VERTICAL STRUCTURE OF THE GALACTIC THICK DISK. II. A LACK OF DARK MATTER IN THE SOLAR NEIGHBORHOOD, (2012, background): “Nevertheless, this will be eventually gathered by modern extensive surveys such as the Sloan Digital Sky Survey (SDSS; York et al. 2000), GAIA (Wilkinson et al. 2005), and Large Synoptic Survey Telescope (LSST; Ivezic et al. 2008).”
The Galaxy in Context: Structural, Kinematic, and Integrated Properties (2016, methodology): “This survey gave rise to three major studies based on photometric parallax ( Jurić et al. 2008), photometric metallicities (Ivezić et al. 2008), and kinematics (Bond et al. 2010) discussed in the next two sections.”
LIGHT CURVE TEMPLATES AND GALACTIC DISTRIBUTION OF RR LYRAE STARS FROM SLOAN DIGITAL SKY SURVEY STRIPE 82 (2009, methodology): “The results from Ivezić et al. (2008) and the results presented here seem to support this prediction.”
J-PLUS: The Javalambre Photometric Local Universe Survey (2015, background): “It is anticipated that estimates of metallicity down to [Fe/H]∼ −3.5 will be achieved, which would represent a major improvement from previous broad-band photometric methods, where SDSS photometry reached saturation at [Fe/H] < −2 (e.g., Ivezić et al. 2008), or [Fe/H] < −2.7 (An et al. 2015).”
Cosmological simulations of the formation of the stellar haloes around disc galaxies (2011, unknown): “…Richardson et al. (2009), and Koch et al. (2008) from the solar abundances of Asplund et al. (2005), which we use to normalise the simulated profiles. neighbourhood out to ≈ 30 − 40 kpc (Carollo et al. 2007; Ivezić et al. 2008; Carollo et al. 2010; de Jong et al. 2010, but see Sesar et al. 2011).”
THE PRISM MULTI-OBJECT SURVEY (PRIMUS). I. SURVEY OVERVIEW AND CHARACTERISTICS (2010, result): “We then compared the observed position of the stellar locus (corrected for Galactic reddening; Schlegel et al. 1998; O’Donnell 1994) to the locus predicted by the Pickles (1998) stellar library for metal-poor dwarfs (i.e., similar to stars in the Galactic halo; Ivezić et al. (2008) ).”
Dynamics for galactic archaeology (2013, background): “Ivezic et al. (2008) analysed the kinematics of these stars as a function of metallicity and showed that the sample divides naturally into a metal-poor halo and a metal-richer disc with distinct kinematics.”
The age structure of stellar populations in the solar vicinity Clues of a two-phase formation history of the Milky Way disk (2013, result): “…in the last years has lead to conflicting results both in the predictions of models and in the data analysis and interpretation (see, for example, Ivezić et al. 2008; Schönrich & Binney 2009b; Spagna et al. 2010; Navarro et al. 2011; Loebman et al. 2011; Lee et al. 2011; Curir et al. 2012).”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, background): “Galactic chemo-dynamic studies are now entering a new realm with current (e.g., RAVE Steinmetz et al. 2006; SDSS Ivezić et al. 2008) and forthcoming (e.g., SkyMapper, APOGEE, HERMES, LSST, Gaia) large photometric, spectroscopic and astrometric surveys targeting different and fainter components of t”
The Milky Way’s stellar disk (2013, background): “But ‘imaging’ and ‘spectroscopic’ surveys are only seemingly disjoint categories, because multi-band photometry may be re-interpreted as a (very) low resolution spectrum and some stellar parameters (e.g., Teff and [Fe/H]) can be constrained by photometry and/or spectra (e.g., Ivezić et al. 2008).”
FORMATION AND EVOLUTION OF THE DISK SYSTEM OF THE MILKY WAY: [α/Fe] RATIOS AND KINEMATICS OF THE SEGUE G-DWARF SAMPLE (2011, background): “…Casetti-Dinescu et al. (2011),−25 km s−1 kpc−1, based on∼4400 red clump metal-rich thick-disk stars covering the metallicity range−0.6 < [Fe/H]< +0.5, that of Ivezíc et al. (2008) from their SDSS sample (−29 km s−1 kpc−1), that of Girard et al. (2006), who 7.0 7.5 8.0 8.5 9.0 9.5 R…”
THE MILKY WAY TOMOGRAPHY WITH SDSS. III. STELLAR KINEMATICS (2009, background): “The results presented here will be greatly extended by several upcoming large-scale, deep optical surveys, including the Dark Energy Survey (Flaugher 2008), Pan-STARRS (Kaiser et al. 2002), and the Large Synoptic Survey Telescope (LSST; Ivezić et al. 2008b).”
THE SEGUE STELLAR PARAMETER PIPELINE. IV. VALIDATION WITH AN EXTENDED SAMPLE OF GALACTIC GLOBULAR AND OPEN CLUSTERS (2010, unknown): “N/A Ivezić et al. (2008) Notes.”
Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems (2014, background): “…metallicity ([Fe/H]) and (to a lesser extent) surface gravity (log g) also play a role, especially towards the near ultraviolet (UV) and the Balmer discontinuity (e.g., Eggen et al. 1962; Ridgway et al. 1980; Bell & Gustafsson 1989; Alonso et al. 1996; Ivezić et al. 2008; Casagrande et al. 2010).”
A compendium of distances to molecular clouds in the Star Formation Handbook (2020, background): “…our underlying parameters θ incorporates previous work on the luminosity, number density, and metallicity of stars in the Galaxy (Bressan et al. 2012; Ivezić et al. 2008; Jurić et al. 2008) as well as the variation of the optical-infrared extinction curve across the Milky Way disk (Schlafly et…”
Co-formation of the disc and the stellar halo (2018, methodology): “We estimate the stars’ distances using equations (A2), (A3) and (A7) in Ivezić et al. (2008).”