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J/A+A/525/A124 Pal1-I elemental equivalent widths and abundances (Monaco+, 2011)

High resolution HDS/SUBARU chemical abundances of the young stellar cluster Palomar 1. Monaco L., Saviane I., Correnti M., Bonifacio P., Geisler D. <Astron. Astrophys. 525, A124 (2011)> =2011A&A...525A.124M
ADC_Keywords: Clusters, globular ; Stars, giant ; Abundances ; Equivalent widths Keywords: stars: abundances - Galaxy: abundances - globular clusters: individual: Palomar 1 Abstract: Palomar 1 is a peculiar globular cluster (GC). It is the youngest Galactic GC and it has been tentatively associated to several of the substructures recently discovered in the Milky Way (MW), including the Canis Major (CMa) overdensity and the Galactic Anticenter Stellar Structure (GASS). In order to provide further insights into its origin, we present the first high resolution chemical abundance analysis for one red giant in Pal 1. We obtained high resolution (R=30000) spectra for one red giant star in Pal 1 using the High Dispersion Spectrograph (HDS) mounted at the SUBARU telescope. We used ATLAS-9 model atmospheres coupled with the SYNTHE and WIDTH calculation codes to derive chemical abundances from the measured line equivalent widths of 18 among alpha, Iron-peak, light and heavy elements. The Palomar 1 chemical pattern is broadly compatible to that of the MW open clusters population and similar to disk stars. It is, instead, remarkably different from that of the Sagittarius (Sgr) dwarf spheroidal galaxy. If Pal 1 association with either CMa or GASS will be confirmed, this will imply that these systems had a chemical evolution similar to that of the Galactic disk. Description: Table A1. reports the line list and atomic parameters adopted for the Palomar 1 giant Pal1-I and the Sun. For the Mn and Co lines we adopted the hyperfine structures (HFS) tabulated by Prochaska et al. (2000AJ....120.2513P). The measured equivalent width and the corresponding abundance obtained for each line are also reported. Objects: --------------------------------------------------------- RA (2000) DE Designation(s) --------------------------------------------------------- 03 33 21.896 +79 35 38.76 Pal1-I = Cl* Palomar 1 RPS I --------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 51 205 Adopted line atomic parameters and elemental abundances and equivalent widths measured for Pal1-I and the Sun
Table 2: Atmospheric parameters adopted for Pal1-I and the Sun -------------------------------------------------------------------------------- Star Teff (K) logg Vturb (km/s) [M/H] -------------------------------------------------------------------------------- Pal1-I 5000 2.40 1.0 -0.5 Sun 5777 4.44 0.9 0.0 Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 2 A2 --- El Element 4- 5 A2 --- Ion Ionization degree 7- 14 F8.3 0.1nm lambda Wavelength of the line (Å) 16- 21 F6.3 --- loggf ? Oscillator strength of the line 22 A1 --- n_loggf [H] H for HFS (1) 24- 28 F5.3 eV chi ? Lower excitation potential of the transition 29 A1 --- n_chi [H] H for HFS (1) 31- 35 F5.1 0.1pm WPal1-I Line equivalent width for Pal1-I 37- 40 F4.2 --- epsPal1-I Abundance (eps=log(X/H)+12) obtained from this line for Pal1-I 42- 46 F5.1 0.1pm WSun ?=999.9 Line equivalent width for the Sun 48- 51 F4.2 --- epsSun ?=9.99 Abundance (eps=log(X/H)+12) obtained from this line for the Sun
Note (1): For Mn and Co lines the flag HFS is reported to indicate that the hyperfine structures tabulated by Prochaska et al. (2000AJ....120.2513P) were adopted.
Acknowledgements: Lorenzo Monaco, lmonaco(at)eso.org
(End) Patricia Vannier [CDS] 02-Dec-2010
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

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