Access to Astronomical Catalogues

← Click to display the menu
J/A+A/538/A100     Abundances red giants in Carina dSph      (Lemasle+, 2012)

VLT/FLAMES spectroscopy of red giant branch stars in the Carina dwarf spheroidal galaxy. Lemasle B., Hill V., Tolstoy E., Venn K.A., Shetrone M.D., Irwin M.J., de Boer T.J.L., Starkenburg E., Salvadori S. <Astron. Astrophys. 538, A100 (2012)> =2012A&A...538A.100L
ADC_Keywords: Galaxies, nearby ; Stars, giant ; Abundances ; Radial velocities ; Equivalent widths ; Photometry, UBVRI ; Photometry, infrared Keywords: stars: abundances - galaxies: individual (Carina Dwarf Spheroidal) - galaxies: evolution Abstract: The ages of individual Red Giant Branch stars can range from 1Gyr old to the age of the Universe, and it is believed that the abundances of most chemical elements in their photospheres remain unchanged with time (those that are not affected by the first dredge-up). This means that they trace the interstellar medium in the galaxy at the time the star formed, and hence the chemical enrichment history of the galaxy. Colour-Magnitude Diagram analysis has shown the Carina dwarf spheroidal to have had an unusually episodic star formation history and this is expected to be reflected in the abundances of different chemical elements. Description: We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode (R∼20000) to measure the abundances of several chemical elements, including Fe, Mg, Ca and Ba, in a sample of 35 individual Red Giant Branch stars in the Carina dwarf spheroidal galaxy. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation episodes the stars in our sample belong to, and thus to define the relationship between star formation and chemical enrichment during these two episodes. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 88 98 Photometric information for our FLAMES targets table4.dat 36 3360 List of all spectral lines, their atomic parameters and their measured EWs for all the 35 RGB stars in the Carina dSph table7.dat 86 35 The abundances and errors of iron and α-elements in our sample of RGB stars in the Carina dSph table8.dat 73 35 The abundances and errors of iron-peak and heavy elements in our sample of RGB stars in the Carina dSph table9.dat 98 8 The abundances and errors for elements that could be measured from single lines in only a handful of stars
See also: J/AJ/130/2677 : Stars in the Carina dSph galaxy field (Majewski+, 2005) J/ApJ/649/201 : Velocities & Washington photometry in Carina dSph (Munoz+ 2006) J/AJ/135/1580 : Element abundances in ten red giants of Car dSph (Koch+, 2008) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Name Name MKVNNNN 9- 10 I2 h RAh Right ascension (J2000) 12- 13 I2 min RAm Right ascension (J2000) 15- 19 F5.2 s RAs Right ascension (J2000) 21 A1 --- DE- Declination sign (J2000) 22- 23 I2 deg DEd Declination (J2000) 25- 26 I2 arcmin DEm Declination (J2000) 28- 32 F5.2 arcsec DEs Declination (J2000) 34- 39 F6.3 mag Vmag ESO-WFI V magnitude 41- 46 F6.3 mag Imag ESO-WFI I magnitude 48- 53 F6.3 mag Jmag ? ESO-SOFI J magnitude (1) 55- 60 F6.3 mag Hmag ? ESO-SOFI H magnitude (1) 62- 67 F6.3 mag Kmag ? ESO-SOFI K magnitude (1) 69- 73 F5.1 km/s HRV Heliocentric radial velocity (2) 75- 77 F3.1 km/s e_HRV rms uncertainty on HRV (2) 79- 88 A10 --- Memb Membership
Note (1): From M. Gullieuszik (private communication) Note (2): our measured radial velocities
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Name Star name 9- 15 F7.2 0.1nm lambda Wavelength 17- 19 A3 --- El Element 21- 25 F5.3 eV ExPot Excitation potential 27- 32 F6.3 [-] loggf Oscillator strength 34- 36 I3 0.1pm EW ?=- Equivalent width
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Name Star name 9- 13 F5.2 [-] [Fe1/H] Abundance [FeI/H] 15- 18 F4.2 [-] e_[Fe1/H] rms uncertainty on [FeI/H] 20- 21 I2 --- o_[Fe1/H] Number of line used for [FeI/H] 23- 27 F5.2 [-] [Fe2/H] ?=- Abundance [FeII/H] 29- 32 F4.2 [-] e_[Fe2/H] ?=- rms uncertainty on [FeII/H] 34 I1 --- o_[Fe2/H] ?=- Number of line used for [FeII/H] 36- 40 F5.2 [-] [Mg1/H] ?=- Abundance [MgI/H] 42- 45 F4.2 [-] e_[Mg1/H] ?=- rms uncertainty on [MgI/H] 47 I1 --- o_[Mg1/H] ?=- Number of line used for [MgI/H] 49- 53 F5.2 [-] [Ca1/H] ?=- Abundance [CaI/H] 55- 58 F4.2 [-] e_[Ca1/H] ?=- rms uncertainty on [CaI/H] 60 I1 --- o_[Ca1/H] ?=- Number of line used for [CaI/H] 62- 66 F5.2 [-] [Ti1/H] ?=- Abundance [TiI/H] 68- 71 F4.2 [-] e_[Ti1/H] ?=- rms uncertainty on [TiI/H] 73 I1 --- o_[Ti1/H] ?=- Number of line used for [TiI/H] 75- 79 F5.2 [-] [Ti2/H] ?=- Abundance [TiII/H] 81- 84 F4.2 [-] e_[Ti2/H] ?=- rms uncertainty on [TiII/H] 86 I1 --- o_[Ti2/H] ?=- Number of line used for [TiII/H]
Byte-by-byte Description of file: table8.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Name Star name 9- 13 F5.2 [-] [Fe1/H] Abundance [FeI/H] 15- 18 F4.2 [-] e_[Fe1/H] rms uncertainty on [FeI/H] 20- 21 I2 --- o_[Fe1/H] Number of line used for [FeI/H] 23- 27 F5.2 [-] [Cr1/H] ?=- Abundance [CrI/H] 29- 32 F4.2 [-] e_[Cr1/H] ?=- rms uncertainty on [CrI/H] 34 I1 --- o_[Cr1/H] ?=- Number of line used for [CrI/H] 36- 40 F5.2 [-] [Co1/H] ?=- Abundance [CoI/H] 42- 45 F4.2 [-] e_[Co1/H] ?=- rms uncertainty on [CoI/H] 47 I1 --- o_[Co1/H] ?=- Number of line used for [CoI/H] 49- 53 F5.2 [-] [Ni1/H] ?=- Abundance [NiI/H] 55- 58 F4.2 [-] e_[Ni1/H] ?=- rms uncertainty on [NiI/H] 60 I1 --- o_[Ni1/H] ?=- Number of line used for [NiI/H] 62- 66 F5.2 [-] [Ba2/H] ?=- Abundance [BaII/H] 68- 71 F4.2 [-] e_[Ba2/H] ?=- rms uncertainty on [BaII/H] 73 I1 --- o_[Ba2/H] ?=- Number of line used for [BaII/H]
Byte-by-byte Description of file: table9.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Name Star name 9- 13 F5.2 [-] [Na1/H] ?=- Abundance [NaI/H] 15- 18 F4.2 [-] e_[Na1/H] ?=- rms uncertainty on [NaI/H] 20 I1 --- o_[Na1/H] ?=- Number of line used for [NaI/H] 22- 26 F5.2 [-] [Si1/H] ?=- Abundance [SiI/H] 28- 31 F4.2 [-] e_[Si1/H] ?=- rms uncertainty on [SiI/H] 33 I1 --- o_[Si1/H] ?=- Number of line used for [SiI/H] 35- 39 F5.2 [-] [Sc2/H] ?=- Abundance [ScII/H] 41- 44 F4.2 [-] e_[Sc2/H] ?=- rms uncertainty on [ScII/H] 46 I1 --- o_[Sc2/H] ?=- Number of line used for [ScII/H] 48- 52 F5.2 [-] [Y2/H] ?=- Abundance [YII/H] 54- 57 F4.2 [-] e_[Y2/H] ?=- rms uncertainty on [YII/H] 59 I1 --- o_[Y2/H] ?=- Number of line used for [YII/H] 61- 65 F5.2 [-] [La2/H] ?=- Abundance [LaII/H] 67- 70 F4.2 [-] e_[La2/H] ?=- rms uncertainty on [LaII/H] 72 I1 --- o_[La2/H] ?=- Number of line used for [LaII/H] 74- 78 F5.2 [-] [Nd2/H] ?=- Abundance [NdII/H] 80- 83 F4.2 [-] e_[Nd2/H] ?=- rms uncertainty on [NdII/H] 85 I1 --- o_[Nd2/H] ?=- Number of line used for [NdII/H] 87- 91 F5.2 [-] [Eu2/H] ?=- Abundance [EuII/H] 93- 96 F4.2 [-] e_[Eu2/H] ?=- rms uncertainty on [EuII/H] 98 I1 --- o_[Eu2/H] ?=- Number of line used for [EuII/H]
Acknowledgements: Bertrand Lemasle, lemasle(at)astro.rug.nl References: Venn et al. Companion Paper. 2012ApJ...751..102V Cat. J/ApJ/751/102
(End) Bertrand Lemasle [Kapteyn Inst.], Patricia Vannier [CDS] 16-Dec-2011
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© UDS/CNRS

Contact