J/AJ/131/1766 Abundances and equivalent widths in NGC 2808 (Carretta, 2006)
Abundances in red giant stars of NGC 2808 and correlations between chemical
anomalies and global parameters in globular clusters.
Carretta E.
<Astron. J., 131, 1766-1783 (2006)>
=2006AJ....131.1766C 2006AJ....131.1766C
ADC_Keywords: Clusters, globular ; Stars, population II ; Abundances ;
Equivalent widths
Keywords: globular clusters: general -
globular clusters: individual (NGC 2808) - stars: abundances -
stars: evolution - stars: Population II
Abstract:
We present the abundance analysis of stars from the tip of the red
giant branch (RGB) to below the RGB bump in the globular cluster NGC
2808 based on high-resolution echelle spectra. We derive abundances of
Al, α-process elements (SiI, CaI, TiI, and TiII), and Fe-group
elements (ScII, VI, CrI, CrII, MnI, CoI, and NiI). Apart from Mg being
somewhat reduced, likely because it has been depleted at the expense
of Al in the MgAl cycle, the other α-element ratios show the
overabundance typical of halo stars of similar metallicity.
Description:
The program stars were observed during the FLAMES Science Verification
program at the ESO Paranal Observatory on 2003 January 24-25. All the
stars were observed with the fiber-fed red arm of the high-resolution
Ultraviolet and Visual Echelle Spectrograph (UVES; R∼47000, fibers of
1"; entrance aperture, grating centered at 5800Å with spectral
coverage of about 2000Å).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 53 20 Adopted atmospheric parameters and Fe abundances
table2.dat 35 6973 Measured equivalent widths for stars in NGC 2808
table34.dat 166 19 Abundances of Al, α-elements and Fe-group
elements in stars of NGC 2808
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See also:
J/A+A/413/343 : RGB stars in NGC 2808 (Cacciari+, 2004)
J/A+A/417/597 : Radial velocities in 4 globular clusters (Recio-Blanco+, 2004)
J/A+AS/84/59 : Photometry of NGC 2808 (Ferraro+, 1990)
J/ApJ/562/368 : UV photometry in NGC 2808 (Brown+, 2001)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- Star Star identification number
(Cl* NGC 2808 PIOTT NNNNN in Simbad)
6 A1 --- f_Star [a] Unreliable equivalent widths (1)
7- 9 I3 --- S/N Signal-to-noise ratio
11- 14 I4 K Teff Effective temperature
16- 19 F4.2 [cm/s2] log(g) Surface gravity
21- 24 F4.2 km/s Vt Microturbulent velocity
26- 28 I3 --- o_[Fe/HI] Number of lines used
30- 34 F5.2 [Sun] [Fe/HI] Abundance ratio
36- 39 F4.2 [Sun] e_[Fe/HI] The 1σ rms on [Fe/HI]
41- 42 I2 --- o_[Fe/HII] Number of lines used
44- 48 F5.2 [Sun] [Fe/HII] Abundance ratio
50- 53 F4.2 [Sun] e_[Fe/HII] The 1σ rms on [Fe/HII]
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Note (1): "a" indicates that for Star 34013 measurements of EWs were scarcely
reliable; hence, this star is disregarded from further discussion
and is reported here only for the sake of completeness.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- Star Star identification number
(Cl* NGC 2808 PIOTT NNNNN in Simbad)
7- 10 A4 --- Ion Ion designation
12- 18 F7.2 0.1nm lambda Wavelength in Angstroms
20- 23 F4.2 eV ExPot Excitation potential
25- 29 F5.2 [-] log(gf) Log of the oscillator strength
31- 35 F5.1 10-13m EW ? Equivalent width (in units of milliAngstroms)
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Byte-by-byte Description of file: table34.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- Star Star identification number
(Cl* NGC 2808 PIOTT NNNNN in Simbad)
7 I1 --- o_[Al/Fe] Number of measured lines
9- 13 F5.2 [Sun] [Al/Fe] ? Abundance ratio
15- 18 F4.2 [Sun] e_[Al/Fe] ? The 1σ rms on [Al/Fe]
20 I1 --- o_[Mg/Fe] Number of measured lines
22- 26 F5.2 [Sun] [Mg/Fe] Abundance ratio
28- 31 F4.2 [Sun] e_[Mg/Fe] ? The 1σ rms [Mg/Fe]
33 I1 --- o_[Si/Fe] Number of measured lines
35- 39 F5.2 [Sun] [Si/Fe] Abundance ratio
41- 44 F4.2 [Sun] e_[Si/Fe] ? The 1σ rms [Si/Fe]
46- 47 I2 --- o_[Ca/Fe] Number of measured lines
49- 53 F5.2 [Sun] [Ca/Fe] Abundance ratio
55- 58 F4.2 [Sun] e_[Ca/Fe] The 1σ rms [Ca/Fe]
60- 61 I2 --- o_[Ti/FeI] Number of measured lines
63- 67 F5.2 [Sun] [Ti/FeI] Abundance ratio
69- 72 F4.2 [Sun] e_[Ti/FeI] The 1σ rms [Ti/FeI]
74 I1 --- o_[Ti/FeII] Number of measured lines
76- 80 F5.2 [Sun] [Ti/FeII] ? Abundance ratio
82- 85 F4.2 [Sun] e_[Ti/FeII] ? The 1σ rms [Ti/FeII]
87 I1 --- o_[Sc/FeII] Number of measured lines
89- 93 F5.2 [Sun] [Sc/FeII] Abundance ratio
95- 98 F4.2 [Sun] e_[Sc/FeII] ? The 1σ rms [Sc/FeII]
100-101 I2 --- o_[V/Fe] Number of measured lines
103-107 F5.2 [Sun] [V/Fe] Abundance ratio
109-112 F4.2 [Sun] e_[V/Fe] The 1σ rms [V/Fe]
114-115 I2 --- o_[Cr/FeI] Number of measured lines
117-121 F5.2 [Sun] [Cr/FeI] Abundance ratio
123-126 F4.2 [Sun] e_[Cr/FeI] The 1σ rms [Cr/FeI]
128 I1 --- o_[Cr/FeII] Number of measured lines
130-134 F5.2 [Sun] [Cr/FeII] ? Abundance ratio
136-139 F4.2 [Sun] e_[Cr/FeII] ? The 1σ rms [Cr/FeII]
141 I1 --- o_[Mn/Fe] Number of measured lines
143-147 F5.2 [Sun] [Mn/Fe] Abundance ratio
149-152 F4.2 [Sun] e_[Mn/Fe] The 1σ rms [Mn/Fe]
154-155 I2 --- o_[Ni/Fe] Number of measured lines
157-161 F5.2 [Sun] [Ni/Fe] Abundance ratio
163-166 F4.2 [Sun] e_[Ni/Fe] The 1σ rms [Ni/Fe]
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Marianne Brouty [CDS] 19-Jul-2007