The Distribution of the Elements in the Galactic Disk

By R. E. Luck, V. Kovtyukh, S. Andrievsky. 2006

246 citations recorded by the source corpus.

This paper reports on the spectroscopic investigation of 54 Cepheids, deriving parameters and abundances. These Cepheids extend previous samples by about 35% in number and increase the amount of the Galactic disk coverage, especially in the direction of l ≈ 120°. We find that there exists in the Galactic disk at that longitude and at a solar distance of about 3-4 kpc a region that has enhanced abundances, ⟨Fe/H]⟩ ≈ +0.2, with respect to the local region. A simple linear fit to all Cepheid data now extant yields a gradient d[Fe/H]/dRG = -0.068 ± 0.003 dex kpc-1. After consideration of the spatial abundance inhomogeneities in the sample, we conclude that the best current estimate of the overall gradient is d[Fe/H]/dRG = -0.06 dex kpc-1.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/0705f7fd7fbf169b4c4d50e8530156161cdb5105

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

CHEMICAL CARTOGRAPHY WITH APOGEE: LARGE-SCALE MEAN METALLICITY MAPS OF THE MILKY WAY DISK (2013, background): “In the inner Galaxy, Henry et al. (2010) find that the slope of the radial gradient is shallower than at the solar circle using planetary nebula, but Cepheid observations (Luck & Lambert 2011; Genovali et al. 2013) find that the gradient is steepest in the inner Galaxy.”
Chemodynamical evolution of the Milky Way disk II: Variations with Galactic radius and height above the disk plane (2014, background): “2009; Luck and Lambert 2011; Lemasle et al. 2013), HII regions (e.g., Daflon and Cunha 2004; Stasińska et al. 2012 and references therein) and the more numerous young open clusters (e.g., Jacobson et al. 2011; Yong et al. 2012; Frinchaboy et al. 2013).”
ARGOS - III. Stellar populations in the Galactic bulge of the Milky Way (2012, background): “This weak abundance gradient is shallower than the gradient seen in the cepheids (Luck & Lambert 2011) and young (age6 1 Gyr) open clusters (Yong, Carney, & Friel 2012).”
A FIRST CONSTRAINT ON THE THICK DISK SCALE LENGTH: DIFFERENTIAL RADIAL ABUNDANCES IN K GIANTS AT GALACTOCENTRIC RADII 4, 8, AND 12 kpc (2011, methodology): “…2004) and Cepheids 1 This paper includes data gathered with the 6.5 meter Magellan Telescopes located at the Las Campanas Observatory, Chile (e.g., Luck et al. 2006), that trace the young disk stellar population, the only available data on the abundance structure of the inner Galactic disk is…”
Measuring Radial Orbit Migration in the Galactic Disk (2018, result): “This assumption is supported by observations of young stars in the Galaxy (e.g., Luck et al. 2006; Przybilla et al. 2008; Genovali et al. 2014).”
On the fine structure of the Cepheid metallicity gradient in the Galactic thin disk (2014, methodology): “We also included Cepheid iron abundances available in the literature: Yong et al. (2006); Sziládi et al. (2007); Luck & Lambert (2011); Luck et al. (2011) (322 objects, black circles).”
THE APOGEE RED-CLUMP CATALOG: PRECISE DISTANCES, VELOCITIES, AND HIGH-RESOLUTION ELEMENTAL ABUNDANCES OVER A LARGE AREA OF THE MILKY WAY'S DISK (2014, result): “1Gyr) have obtained mixed results, with some studies seeing variations (Davies et al. 2009), while others do not (Luck & Lambert 2011).”
Quantifying the uncertainties of chemical evolution studies II. Stellar yields (2010, methodology): “For the comparison with the observations, we use the homogeneous data for nearly 200 classical Cepheid variable stars presented in a series of papersby S. Andrievsky and collaborators (Andrievsky et al. 2002a,b,c; Luck et al. 2003; Andrievsky et al. 2004; Kovtyukh et al. 2005; Luck et al. 2006).”