Chemical abundances in Leo I and II dSph : J/MNRAS/378/318

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Authors : Bosler T.L. orcid , Smecker-Hane T.A., Stetson P.B. (hide) , Smecker-Hane T.A., Stetson P.B. et..al

VizieR DOI : 10.26093/cds/vizier.73780318
Bibcode : 2007MNRAS.378..318B (ADS) (Simbad) (Objects)
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CDS Keywords : Galaxies, nearby; Abundances; Equivalent widths
UAT : Galaxies, Chemical abundances, Line intensities

Observation (OC)

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Inserted into VizieR : 14-Jan-2008
Last modification : 04-Jul-2024

The chemical abundances of the stellar populations in the Leo I and II dSph galaxies. (2007)

Keywords : stars abundances - galaxies: abundances - galaxies: dwarf - galaxies: evolution - galaxies: individual: Leo I dSph, Leo II dSph

Abstract:We have obtained calcium abundances and radial velocities for 102 red giant branch (RGB) stars in the Leo I dwarf spheroidal galaxy (dSph) and 74 RGB stars in the Leo II dSph using the low-resolution spectrograph (LRIS) on the Keck I 10-m telescope. We report on the calcium abundances [Ca/H] derived from the strengths of the Ca ii triplet absorption lines at 8498, 8542 and 8662{AA} in the stellar spectra using a new empirical Ca II triplet calibration to [Ca/H]. ...(more)
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Monthly Notices policies
The photometry and astrometry for Leo I and II were obtained as part of a larger program to provide homogeneous photometry for star clusters and nearby resolved galaxies (e.g. Stetson, Hesser & Smecker-Hane 1998, Cat. <J/PASP/110/533>; Stetson 2000PASP..112..925S). The present photometry is based upon a large database of CCD images acquired by ourselves and collaborators, images obtained from the archives of the Canada-France-Hawaii Telescope and the Isaac Newton Group and images privately donated by other astronomers.

  • J/A+AS/121/95 : Atmospheric parameters for 24 clusters (Carreta+ 1997)
  • J/PASP/109/883 : Globular metallicity scale. I. (Rutledge+ 1997)
  • J/PASP/110/533 : BR photometry of Fornax bright stars (Stetson+ 1998)

                


                

                    

                


                

                    

                


                

                    
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