J/A+A/572/A108 47 Tuc red giants chemical composition (Thygesen+, 2014)
The chemical composition of red giants in 47 Tucanae.
I: Fundamental parameters and chemical abundance patterns.
Thygesen A. O., Sbordone L., Andrievsky S., Korotin S., Yong D., Zaggia S.,
Ludwig H.-G., Collet R., Asplund M., Ventura P., D'Antona F., Melendez J.,
D'Ercole A.
<Astron. Astrophys. 572, A108 (2014)>
=2014A&A...572A.108T 2014A&A...572A.108T
ADC_Keywords: Milky Way ; Clusters, globular ; Abundances ; Stars, giant;
Radial velocities
Keywords: galaxy: globular clusters: individual - stars: abundances -
stars: fundamental parameters - methods: observational -
techniques: spectroscopic
Abstract:
The study of chemical abundance patterns in globular clusters is of
key importance to constrain the different candidates for intra-cluster
pollution of light elements. We aim at deriving accurate abundances
for a large range of elements in the globular cluster 47 Tucanae (NGC
104) to add new constraints to the pollution scenarios for this
particular cluster, expanding the range of previously derived element
abundances. Using tailored 1D LTE atmospheric models together with a
combination of equivalent width measurements, LTE, and NLTE synthesis
we derive stellar parameters and element abundances from
high-resolution, high signal-to-noise spectra of 13 red giant stars
near the tip of the RGB. We derive abundances of a total 27 elements
(O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Y, Zr,
Mo, Ru, Ba, La, Ce, Pr, Nd, Eu, Dy). Departures from LTE were taken
into account for Na, Al and Ba. We find a mean [Fe/H]=-0.78±0.07
and [alpha/Fe]=0.34±0.03 in good agreement with previous studies.
The remaining elements show good agreement with the literature, but
the inclusion of NLTE for Al has a significant impact on the behaviour
of this key element. We confirm the presence of an Na-O
anti-correlation in 47 Tucanae found by several other works. Our NLTE
analysis of Al shifts the [Al/Fe] to lower values, indicating that
this may be overestimated in earlier works. No evidence for an
intrinsic variation is found in any of the remaining elements.
Description:
Table 2 contains linelist of the non-HFS elements. These lines were
used for equivalent width measurements. Sorted by element number.
Table 5 contains all the lines used for HFS synthesis. With the
exception of Ba, all lines are split into individual HFS components,
including isotopes. log(gf) values reflect this. Solar isotope mixture
is assumed. Sorted by element number. Table 8 contains the fundamental
stellar parameters. Table 9 contains [Fe/H] as well as abundance
ratios [X/Fe] for all stars. All measurements have an associated
uncertainty sig[X/Fe] and the number of lines used in each individual
star. In cases where no measurement exist, the value "-9.99" is given.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 63 13 Properties of the observed targets
table8.dat 31 13 Fundamental stellar parameters
table9.dat 388 13 Abundance ratios [X/Fe], sigma and number of lines
table2.dat 27 150 Non-HFS lines used for abundance analysis
table5.dat 27 554 Hyperfine structure (HFS) linelist,
split into components (except Ba)
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See also:
J/A+A/435/657 : Equivalent widths of 5 giants in 47 Tuc (Alves-Brito+, 2005)
J/A+A/550/A34 : Abundances of red giants in M4 and 47 Tuc (Carretta+, 2013)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- ID ID number
6 A1 --- n_ID [*] * indicates polluted target
8- 9 I2 h RAh Right ascension (J2000)
11- 12 I2 min RAm Right ascension (J2000)
14- 18 F5.2 s RAs Right ascension (J2000)
20 A1 --- DE- Declination sign (J2000)
21- 22 I2 deg DEd Declination (J2000)
24- 25 I2 arcmin DEm Declination (J2000)
27- 31 F5.2 arcsec DEs Declination (J2000)
33- 36 F4.1 mag Vmag V magnitude (1)
38- 41 F4.1 mag Bmag B magnitude (1)
43- 46 F4.1 mag Imag I magnitude (1)
48- 51 F4.1 mag Umag U magnitude (1)
53- 58 F6.2 km/s RV [-29/-9] Radial velocity
60- 63 F4.2 km/s e_RV [0.1/0.4] rms uncertainty of RV
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Note (1): The uncertainties on the magnitudes are at the 3% level.
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- ID Star ID number
7- 10 I4 K Teff Effective temperature
12- 15 F4.2 [cm/s2] logg [0.3/1.45] Surface gravity
17- 20 F4.2 km/s Vt [1.1/1.9] Microturbulent velocity ξt
22- 26 F5.2 [Sun] [Fe/H] [-0.86/-0.66] Metallicity [Fe/H]
28- 31 F4.2 km/s Vmac [5/7] Macroturbulent velocity
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Byte-by-byte Description of file: table9.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- ID Star ID number
7- 11 F5.2 [Sun] [FeI/H] Abundance (26.0)
13- 16 F4.2 [Sun] e_[FeI/H] Uncertainty on measurement
18- 19 I2 --- NFeI Number of lines used
21- 25 F5.2 [Sun] [FeII/H] Abundance (26.1)
27- 30 F4.2 [Sun] e_[FeII/H] Uncertainty on measurement
32- 33 I2 --- NFeII Number of lines used
35- 39 F5.2 [Sun] [O/Fe] ?=-9.99 Abundance ratio (8.)
41- 45 F5.2 [Sun] e_[O/Fe] ?=-9.99 Uncertainty on measurement
47 I1 --- NO Number of lines used
49- 52 F4.2 [Sun] [Na/Fe] Abundance ratio (11.)
54- 57 F4.2 [Sun] e_[Na/Fe] Uncertainty on measurement
59 I1 --- NNa Number of lines used
61- 64 F4.2 [Sun] [Mg/Fe] Abundance ratio (12.)
66- 69 F4.2 [Sun] e_[Mg/Fe] Uncertainty on measurement
71 I1 --- NMg Number of lines used
73- 76 F4.2 [Sun] [Al/Fe] Abundance ratio (13.)
78- 81 F4.2 [Sun] e_[Al/Fe] Uncertainty on measurement
83 I1 --- NAl Number of lines used
85- 88 F4.2 [Sun] [Si/Fe] Abundance ratio (14.)
90- 93 F4.2 [Sun] e_[Si/Fe] Uncertainty on measurement
95 I1 --- NSi Number of lines used
97-100 F4.2 [Sun] [Ca/Fe] Abundance ratio (20.)
102-105 F4.2 [Sun] e_[Ca/Fe] Uncertainty on measurement
107 I1 --- NCa Number of lines used
109-113 F5.2 [Sun] [ScI/Fe] Abundance ratio (21.0)
115-118 F4.2 [Sun] e_[ScI/Fe] Uncertainty on measurement
120 I1 --- NScI Number of lines used
122-125 F4.2 [Sun] [ScII/Fe] Abundance ratio (21.1)
127-130 F4.2 [Sun] e_[ScII/Fe] Uncertainty on measurement
132-133 I2 --- NScII Number of lines used
135-138 F4.2 [Sun] [TiI/Fe] Abundance ratio (22.0)
140-143 F4.2 [Sun] e_[TiI/Fe] Uncertainty on measurement
145-146 I2 --- NTiI Number of lines used
148-151 F4.2 [Sun] [TiII/Fe] Abundance ratio (22.1)
153-156 F4.2 [Sun] e_[TiII/Fe] Uncertainty on measurement
158 I1 --- NTiII Number of lines used
160-163 F4.2 [Sun] [V/Fe] Abundance ratio (23.)
165-168 F4.2 [Sun] e_[V/Fe] Uncertainty on measurement
170-171 I2 --- NV Number of lines used
173-177 F5.2 [Sun] [Cr/Fe] Abundance ratio (24.)
179-182 F4.2 [Sun] e_[Cr/Fe] Uncertainty on measurement
184 I1 --- NCr Number of lines used
186-190 F5.2 [Sun] [Mn/Fe] Abundance ratio (25.)
192-195 F4.2 [Sun] e_[Mn/Fe] Uncertainty on measurement
197 I1 --- NMn Number of lines used
199-203 F5.2 [Sun] [Co/Fe] Abundance ratio (27.)
205-208 F4.2 [Sun] e_[Co/Fe] Uncertainty on measurement
210-211 I2 --- NCo Number of lines used
213-217 F5.2 [Sun] [Ni/Fe] Abundance ratio (28.)
219-222 F4.2 [Sun] e_[Ni/Fe] Uncertainty on measurement
224-225 I2 --- NNi Number of lines used
227-231 F5.2 [Sun] [Cu/Fe] Abundance ratio (29.)
233-236 F4.2 [Sun] e_[Cu/Fe] Uncertainty on measurement
238 I1 --- NCu Number of lines used
240-243 F4.2 [Sun] [Zn/Fe] Abundance ratio (30.)
245-248 F4.2 [Sun] e_[Zn/Fe] Uncertainty on measurement
250 I1 --- NZn Number of lines used
252-256 F5.2 [Sun] [YII/Fe] Abundance ratio (39.2)
258-261 F4.2 [Sun] e_[YII/Fe] Uncertainty on measurement
263 I1 --- NYII Number of lines used
265-268 F4.2 [Sun] [Zr/Fe] Abundance ratio (40.)
270-273 F4.2 [Sun] e_[Zr/Fe] Uncertainty on measurement
275 I1 --- NZr Number of lines used
277-280 F4.2 [Sun] [Mo/Fe] Abundance ratio (42.)
282-285 F4.2 [Sun] e_[Mo/Fe] Uncertainty on measurement
287 I1 --- NMo Number of lines used
289-292 F4.2 [Sun] [Ru/Fe] Abundance ratio (44.)
294-297 F4.2 [Sun] e_[Ru/Fe] Uncertainty on measurement
299 I1 --- NRu Number of lines used
301-304 F4.2 [Sun] [BaII/Fe] Abundance ratio (56.1)
306-309 F4.2 [Sun] e_[BaII/Fe] Uncertainty on measurement
311 I1 --- NBaII Number of lines used
313-317 F5.2 [Sun] [LaII/Fe] Abundance ratio (57.1)
319-322 F4.2 [Sun] e_[LaII/Fe] Uncertainty on measurement
324 I1 --- NLaII Number of lines used
326-330 F5.2 [Sun] [CeII/Fe] ?=-9.99 Abundance ratio (58.1)
332-336 F5.2 [Sun] e_[CeII/Fe] ?=-9.99 Uncertainty on measurement
338 I1 --- NCeII Number of lines used
340-344 F5.2 [Sun] [PrII/Fe] Abundance ratio (59.1)
346-349 F4.2 [Sun] e_[PrII/Fe] Uncertainty on measurement
351 I1 --- NPrII Number of lines used
353-357 F5.2 [Sun] [NdII/Fe] Abundance ratio (60.1)
359-362 F4.2 [Sun] e_[NdII/Fe] Uncertainty on measurement
364 I1 --- NNdII Number of lines used
366-369 F4.2 [Sun] [EuII/Fe] Abundance ratio (63.1)
371-374 F4.2 [Sun] e_[EuII/Fe] Uncertainty on measurement
376 I1 --- NEuII Number of lines used
378-381 F4.2 [Sun] [DyII/Fe] Abundance ratio (66.1)
383-386 F4.2 [Sun] e_[DyII/Fe] Uncertainty on measurement
388 I1 --- NDyII Number of lines used
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Byte-by-byte Description of file: table2.dat table5.dat
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Bytes Format Units Label Explanations
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1- 8 F8.3 0.1nm lambda [4800/6800] Wavelength λ (in Angstrom)
10- 13 F4.1 --- Ion Element ID. XX.0 neutral, XX.1 ionized species
15- 21 F7.3 --- loggf Oscillator strength
23- 27 F5.3 eV Elow Lower excitation potential
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Acknowledgements:
Anders Thygesen, a.thygesen(at)lsw.uni-heidelberg.de
Landessternwarte, Heidelberg, Germany
(End) A. Thygesen [Landessternwarte, Heidelberg], P. Vannier [CDS] 18-Sep-2014