A Deep Large Binocular Telescope View of the Canes Venatici I Dwarf Galaxy

Martín, Nicolás F.; Coleman, Matthew G.; Jong, J. T. A. de; Rix, Hans-Walter; Bell, Eric F.; Sand, David J.; Hill, John M.; Thompson, D. J.; Burwitz, V.; Giallongo, E.; Ragazzoni, Roberto; Diolaiti, Emiliano; Gasparo, F.; Grazian, A.; Pedichini, Fernando; Bechtold, Jill

doi:10.1086/525559

Cited by 45 publications

(62 citation statements)

References 20 publications

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“…However, the SFH reveals the presence of both an old, metal-poor, as well as a younger ( 3 Gyr) and more metal-rich population. This is consistent with the findings of Ibata et al (2006), who detect two kinematically distinct populations in CVn I which differ in age and metallicity, and the detection of a young component by Martin et al (2007b) in deeper photometry. The SFH of UMa II also shows a peak at an age of ∼5 Gyr, which supports suggestion of multiple populations in this object by Zucker et al (2006b), who find the MSTO width of UMa II to be too large to be explained by photometric errors alone.…”

Section: Discussionsupporting

confidence: 92%

“…135 stars along the HB. This detection of an old and intermediateage population with these metallicities confirms the findings of Ibata et al (2006) and Martin et al (2007b). Furthermore, Zucker et al (2006a) note the presence of a carbon star very close to the center of CVn I and its heliocentric radial velocity of 36 ± 20 km s −1 is consistent with the radial velocities that Belokurov et al (2007) due to the presence of HB stars.…”

Section: Satellite Propertiessupporting

confidence: 86%

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Numerical Color-Magnitude Diagram Analysis of Sloan Digital Sky Survey Data and Application to the New Milky Way Satellites

Jong

Rix

Martín

et al. 2008

The Astronomical Journal

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We have tested the application to Sloan Digital Sky Survey (SDSS) data of the software package MATCH, which fits color-magnitude diagrams (CMDs) to estimate stellar population parameters and distances. These tests on a set of six globular clusters show that these techniques recover their known properties. New ways of using the CMD-fitting software enable us to deal with an extended distribution of stars along the line-of-sight, to constrain the overall properties of sparsely populated objects, and to detect the presence of stellar overdensities in wide-area surveys. We then also apply MATCH to CMDs for 12 recently discovered Milky Way satellites to derive in a uniform fashion their distances, ages, and metallicities. While the majority of them appear consistent with a single stellar population, CVn I, UMa II, and Leo T exhibit (from SDSS data alone) a more complex history with multiple epochs of star formation.

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Section: Discussionsupporting

confidence: 92%

Section: Satellite Propertiessupporting

confidence: 86%

Numerical Color-Magnitude Diagram Analysis of Sloan Digital Sky Survey Data and Application to the New Milky Way Satellites

Jong

Rix

Martín

et al. 2008

The Astronomical Journal

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“…It is possible to simply exclude putative blue stragglers from the CMD fitting process a priori. However, it is not always clear whether stars in the blue plume of early-type galaxies are blue stragglers or main sequence stars (e.g., Martin et al 2008;Sand et al 2010;Okamoto et al 2012). If they are main sequence stars, excluding them would remove critical information about interesting late time star formation in early-type galaxies.…”

Section: Measuring the Star Formation Historiesmentioning

confidence: 99%

THE STAR FORMATION HISTORIES OF LOCAL GROUP DWARF GALAXIES. I.HUBBLE SPACE TELESCOPE/WIDE FIELD PLANETARY CAMERA 2 OBSERVATIONS

Weisz¹,

Dolphin²,

Skillman³

et al. 2014

ApJ

450

561

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We present uniformly measured star formation histories (SFHs) of 40 Local Group (LG) dwarf galaxies based on color-magnitude diagram (CMD) analysis from archival Hubble Space Telescope imaging. We demonstrate that accurate SFHs can be recovered from CMDs that do not reach the oldest main sequence turn-off (MSTO), but emphasize that the oldest MSTO is critical for precisely constraining the earliest epochs of star formation. We find that: (1) the average lifetime SFHs of dwarf spheroidals (dSphs) can be approximated by an exponentially declining SFH with τ ∼ 5 Gyr; (2) lower luminosity dSphs are less likely to have extended SFHs than more luminous dSphs; (3) the average SFHs of dwarf irregulars (dIrrs), transition dwarfs, and dwarf ellipticals can be approximated by the combination of an exponentially declining SFH (τ ∼ 3-4 Gyr) for lookback ages >10-12 Gyr ago and a constant SFH thereafter; (4) the observed fraction of stellar mass formed prior to z = 2 ranges considerably (80% for galaxies with M < 10 5 M to 30% for galaxies with M > 10 7 M ) and is largely explained by environment; (5) the distinction between "ultra-faint" and "classical" dSphs is arbitrary; (6) LG dIrrs formed a significantly higher fraction of stellar mass prior to z = 2 than the Sloan Digital Sky Survey galaxies from Leitner and the SFHs from the abundance matching models of Behroozi et al. This may indicate higher than expected star formation efficiencies at early times in low mass galaxies. Finally, we provide all the SFHs in tabulated electronic format for use by the community.

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“…From the tip of the red giant branch, they concluded that the Galaxy was at a distance of 220 kpc. The first deep color−magnitude diagrams of the Canes Venatici I (CVn I) dwarf galaxy were provided by Martin et al (2008) from observations with the wide-field Large Binocular Camera on the Large Binocular Telescope. Interestingly, their analysis revealed a dichotomy in the stellar populations of CVn I which harbors an old (≥10 Gyr), metal-poor ([Fe/H] −2.0 dex), and spatially extended population along with a much younger, more metalrich, and spatially more concentrated population.…”

Section: Canes Venatici Imentioning

confidence: 99%

Abundance ratios of red giants in low-mass ultra-faint dwarf spheroidal galaxies

François

Monaco

Bonifacio

et al. 2016

A&A

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Context. Low-mass dwarf spheroidal galaxies are key objects for our understanding of the chemical evolution of the pristine Universe and the Local Group of galaxies. Abundance ratios in stars of these objects can be used to better understand their star formation and chemical evolution. Aims. We report on the analysis of a sample of 11 stars belonging to five different ultra-faint dwarf spheroidal galaxies (UfDSph) that is based on X-Shooter spectra obtained at the VLT. Methods. Medium-resolution spectra have been used to determine the detailed chemical composition of their atmosphere. We performed a standard 1D LTE analysis to compute the abundances. Results. Considering all the stars as representative of the same population of low-mass galaxies, we found that the [α/Fe] ratios vs.s [Fe/H] decreases as the metallicity of the star increases in a way similar to that which is found for the population of stars that belong to dwarf spheroidal galaxies. The main difference is that the solar [α/Fe] is reached at a much lower metallicity for the UfDSph than for the dwarf spheroidal galaxies. We report for the first time the abundance of strontium in CVn II. The star we analyzed in this galaxy has a very high [Sr/Fe] and a very low upper limit of barium which makes it a star with an exceptionally high [Sr/Ba] ratio.

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A Deep Large Binocular Telescope View of the Canes Venatici I Dwarf Galaxy

Cited by 45 publications

References 20 publications

Numerical Color-Magnitude Diagram Analysis of Sloan Digital Sky Survey Data and Application to the New Milky Way Satellites

Numerical Color-Magnitude Diagram Analysis of Sloan Digital Sky Survey Data and Application to the New Milky Way Satellites

THE STAR FORMATION HISTORIES OF LOCAL GROUP DWARF GALAXIES. I.HUBBLE SPACE TELESCOPE/WIDE FIELD PLANETARY CAMERA 2 OBSERVATIONS

Abundance ratios of red giants in low-mass ultra-faint dwarf spheroidal galaxies

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