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 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 2000AJ....120.2513P). The measured equivalent width and the
corresponding abundance obtained for each line are also reported.
Objects:
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RA (2000) DE Designation(s)
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03 33 21.896 +79 35 38.76 Pal1-I = Cl* Palomar 1 RPS I
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File Summary:
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FileName Lrecl Records Explanations
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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
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Table 2: Atmospheric parameters adopted for Pal1-I and the Sun
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Star Teff (K) logg Vturb (km/s) [M/H]
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Pal1-I 5000 2.40 1.0 -0.5
Sun 5777 4.44 0.9 0.0
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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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
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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 2000AJ....120.2513P) were adopted.
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Acknowledgements:
Lorenzo Monaco, lmonaco(at)eso.org
(End) Patricia Vannier [CDS] 02-Dec-2010