Theoretical isochrones in several photometric systems. II. The Sloan Digital Sky Survey ugriz system

By L. Girardi, E. Grebel, M. Odenkirchen, C. Chiosi. 2004

218 citations recorded by the source corpus.

Following Paper I, we provide extended tables of bolometric corrections, extinction coeffi cients, stellar isochrones, and integrated magnitudes and colours of single-burst stellar populations, for the Sloan Digital Sky Survey (SDSS) ugriz photometric system. They are tested on comparisons with DR1 data for a few stellar systems, namely the Palomar 5 and NGC 2419 globular clusters and the Draco dSph galaxy.

View Paper: https://www.semanticscholar.org/paper/c79452bd02847f04f1fdfe307286ef2ab769f451

How researchers see this paper

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

Citations in the corpus

RINGS AND RADIAL WAVES IN THE DISK OF THE MILKY WAY (2015, methodology): “We checked these isochrones against those of Girardi et al. (2004) and found that they are in good agreement for mainsequence stars with (g−r) < 0.8, so our distances are apparently not very model dependent.”
Empirical color transformations between SDSS photometry and Other photometric systems. (2005, background): “A recent theoretical transformation was carried out by Girardi et al. (2004).”
A COMPLETE SPECTROSCOPIC SURVEY OF THE MILKY WAY SATELLITE SEGUE 1: THE DARKEST GALAXY (2010, background): “A small number of stars located near a metal-poor asymptotic giant branch isochrone from Girardi et al. (2004) were also selected.”
A New Milky Way Dwarf Galaxy in Ursa Major (2005, background): “Because SDSS does not resolve Sextans’ main sequence turnoff, we instead overplot the theoretical isochrone of an [Fe/H] = -1.7, 13 Gyr old population (Girardi et al. 2004) projected to 100 kpc.”
The Accretion Origin of the Milky Way’s Stellar Halo (2007, background): “Firstly, for old populations such as those in globular clusters it is clear that the color of the main sequence turn-off (MSTO) is a metallicity indicator (this point is discussed in more detail for SDSS isochrones in Girardi et al. 2004).”
MAPPING THE STELLAR STRUCTURE OF THE MILKY WAY THICK DISK AND HALO USING SEGUE PHOTOMETRY (2009, methodology): “The color of the MSTO is a useful proxy for the metallicity of the dominant population at a given distance (e.g. see the discussion about this for SDSS isochrones in Girardi et al. 2004).”
A New Milky Way Companion: Unusual Globular Cluster or Extreme Dwarf Satellite? (2004, background): “However, those stars are bluer relative to the detected turnoff than subgiant stars of a young (<10 Gyr) stellar population (see isochrones in Girardi et al. 2004).”
Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems (2014, background): “…synthetic magnitudes, besides being more convenient given the dependence of the asinh magnitudes9 on a softening parameter (survey dependent) and the difficulty of defining quantities such as bolometric corrections and absolute magnitudes in the asinh formulation (see e.g., Girardi et al. 2004).”
A Keck/DEIMOS spectroscopic survey of faint Galactic satellites: searching for the least massive dwarf galaxies (2007, methodology): “On the other hand, the color difference of the Girardi et al. (2004) isochrones for an old population with metallicities ranging from [Fe/H] = −2.3 to [Fe/H] = −0.7 indicates that such a metallicity spread in the satellite could explain the broadness of the main sequence observed in the satellite.”
A Spectroscopic Study of the Ancient Milky Way: F- and G-Type Stars in the Third Data Release of the Sloan Digital Sky Survey (2005, methodology): “Using isochrones from Girardi et al. (2004), we have determined the loci of the turnoff as a function of metallicity for different ages, accounting for the enhanced [ /Fe] ratios using equation (9).”
The Sloan Digital Sky Survey monitor telescope pipeline (2006, methodology): “These data may be used to verify the recent age and metallicity models of Girardi et al. (2004) and the prior work of Lenz et al. (1998), and to verify and expand upon theu′g′r′i′z′ to UBV RcIc transformations presented in the standard star paper (Smith et al. 2002).”
Distances to Galactic High-Velocity Clouds. I. Cohen Stream, Complex GCP, Cloud g1 (2007, methodology): “The determined stellar parameters (TeA, log g, and [Fe/H]) are then used to estimate absolute magnitudes MV by placing the star on the theoretical isochrones of Girardi et al. (2004).”
The Haunted Halos of Andromeda and Triangulum: A Panorama of Galaxy Formation in Action (2007, methodology): “Instead we chose to adopt the Padova isochrones (Girardi et al. 2004), which conveniently have been calculated in the Sloan passbands.”
CHEMICAL EVOLUTION IN HIERARCHICAL MODELS OF COSMIC STRUCTURE. II. THE FORMATION OF THE MILKY WAY STELLAR HALO AND THE DISTRIBUTION OF THE OLDEST STARS (2009, methodology): “These models adopt the isochrones of Girardi et al. (2002) and Girardi et al. (2004) for the UBVRIJHK and SDSS ugriz systems, respectively, as published on the Padova group website3.”
A REVISED EFFECTIVE TEMPERATURE SCALE FOR THE KEPLER INPUT CATALOG (2011, methodology): “We used a 1 Gyr old Padova models at solar abundance (Girardi et al. 2004).”
THE UNIVERSAL STELLAR MASS–STELLAR METALLICITY RELATION FOR DWARF GALAXIES (2013, methodology): “For photometry in the SDSS filter set, we used Padova isochrones (Girardi et al. 2004), which were computed with SDSS filter transmission curves.”
Stellar SEDs from 0.3 to 2.5 μm: Tracing the Stellar Locus and Searching for Color Outliers in the SDSS and 2MASS (2007, background): “…Hawley et al. (2002), West et al. (2005), Bilir et al. (2005), Davenport et al. (2006), Bochanski et al. (2007) and Golimowski et al. (2007) present science-grade empirical measurements, while Girardi et al. (2004) and Dotter & Chaboyer (2006) provide stellar models with SDSS and 2MASS photometry.”