J/MNRAS/418/284 s-process in low-metallicity stars. II. (Bisterzo+, 2011)
The s-process in low-metallicity stars.
II. Interpretation of high-resolution spectroscopic observations with asymptotic
giant branch models.
Bisterzo S., Gallino R., Straniero O., Cristallo S., Kappeler F.
<Mon. Not. R. Astron. Soc., 418, 284-319 (2011)>
=2011MNRAS.418..284B 2011MNRAS.418..284B
ADC_Keywords: Stars, giant ; Abundances
Keywords: nuclear reactions, nucleosynthesis, abundances -
stars: AGB and post-AGB - stars: carbon - stars: Population II
Abstract:
High-resolution spectroscopic observations of 100 metal-poor carbon
and s-rich stars (CEMP-s) collected from the literature are compared
with the theoretical nucleosynthesis models of the asymptotic giant
branch (AGB) presented in Paper I, Cat. J/MNRAS/404/1529.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 132 57 Abundances for CEMP-s and CEMP-s/r stars with a
major number of observations
table3.dat 134 41 Abundances for CEMP-s and CEMP-s/r stars with a
limited number of spectroscopic observations
among the characteristic s-process elements
tablea1.dat 83 34 *Binarity status of the star sample
tablea2.dat 18 12 Solar meteoritic abundance
refs.dat 112 41 References
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Note on tablea1.dat: For the stars not listed here there are no measurements
available so far.
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See also:
J/MNRAS/404/1529 : s-process in low-metallicity stars (Bisterzo+, 2010)
Byte-by-byte Description of file: table[23].dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Star Star name
18 A1 --- n_Star [a] disc stars (1)
20- 32 A13 --- Ref Reference(s), in refs.dat file
34- 37 A4 --- FDU [yes no?] First dredge-up ?
39- 43 F5.2 [Sun] [Fe/H] Metallicity, [Fe/H] (2)
44 A1 --- --- [,]
45- 49 F5.2 [Sun] [Fe/H]2 ? Second value for metallicity [Fe/H]
51- 55 F5.2 [-] [Na/Fe] ?=- Abundance [Na/Fe] (2)
56 A1 --- --- [,]
57- 59 A3 [-] [Na/Fe]2 ? Second value for abundance [Na/Fe]
60- 64 F5.2 [-] [Mg/Fe] ?=- Abundance [Mg/Fe] (2)
65 A1 --- --- [,]
66- 69 F4.2 [-] [Mg/Fe]2 ?=- Second value for abundance [Mg/Fe]
72- 76 F5.2 [-] [ls/Fe] ?=- light-s abundance [ls/Fe] (3)
78- 81 F4.2 [-] [hs/Fe] high-s abundance [hs/Fe] (3)
83- 87 F5.2 [-] [hs/ls] ?=- high to low s-elements ratio [hs/ls] (3)
89- 90 A2 --- l_[Pb/Fe] [≤ ] Limit flag on [Pb/Fe]
91- 94 F4.2 [-] [Pb/Fe] ?=- Abundance [Pb/Fe] (2)
96- 97 A2 --- l_[Pb/hs] [≤ ] Limit flag on [Pb/hs]
98-102 F5.2 [-] [Pb/hs] ?=- Abundance [Pb/hs] (2)
103 A1 --- l_[La/Fe] Limit flag on [La/Fe]
104-107 F4.2 [-] [La/Fe] ?=- Abundance [La/Fe] (2)
109-110 A2 --- l_[Eu/Fe] [≤ ] Limit flag on [Eu/Fe]
111-115 F5.2 [-] [Eu/Fe] ?=- Abundance [Eu/Fe] (2)
116 A1 --- u_[Eu/Fe] Uncertainty flag on [Eu/Fe]
117-118 A2 --- l_[La/Eu] [≥ ] Limit flag on [La/Eu]
119-123 F5.2 [-] [La/Eu] ?=- Abundance [La/Eu] (2)
124 A1 --- u_[La/Eu] Uncertainty flag on [La/Eu]
126-134 A9 --- Type Type (4)
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Note (1): disc star which will be discussed in Paper III:
* in table2: HD 26 ([Fe/H]=-1.0), HD 206983 ([Fe/H]=-1.0), and
HE 1152-0355 ([Fe/H]=-1.3)
* in table3: CS 29503-010 ([Fe/H]=-1.1) and HE 0507-1653 ([Fe/H] =-1.4)
Note (2): Range:
-----------------------------
El table2 table3
-----------------------------
[Fe/H] -1.0-3.3 , -1.1-3.2
[Na/Fe] -0.1-2.3 , -0.5-2.7
[Mg/Fe] 0.0-1.7 , 0.2-1.4
[ls/Fe] -0.1-2.2 , 0.2-2.3
[hs/Fe] 0.5-2.9 , 0.4-3.4
[hs/ls] -0.4-1.4 , -1.0-1.5
[Pb/Fe] 0.9-3.7 , 1.3-3.7
[Pb/hs] -0.4-1.6 , -0.4-2.0
[La/Fe] 0.4-2.9 , 0.6-2.1
[Eu/Fe] -0.5-2.0 , 0.0-1.7
[La/Eu] 0.0-1.1 , -0.2-0.7
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Note (3): "ls" = light s-process (neutron-capture for N=50: Sr, Y, Zr)
and "hs" = heavy s-process (neutron-capture for N=82 [Ba, La, Ce, Nd, Sm]
or N=126 (Pb).
In table3, [ls/Fe]=[Sr/Fe] in all these stars, with only one exception,
SDSS 2047+00, for which Y and Zr are detected.
[hs/Fe]=[Ba/Fe], with the exception of those stars with La measurement
([La/Eu]), and for HE 0131-3953 for which both La and Nd have been detected.
Note (4): We distinguish between stars with high s-process enhancement,
[hs/Fe]≳1.5, called CEMP-sII (or CEMP-sII/rII and CEMP-sII/rI depending
on the r-process enhancement; see text and Section 3.3), and stars with a
mild s enrichment, [hs/Fe]< 1.5, called CEMP-sI. The two classes are labelled
with 'sII' (or 'sII/rII' and 'sII/rI') and 'sI'. The labels 'sI/-' and
'sII/-' apply for stars without europium detection.
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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- 17 A17 --- Star Star name
20- 41 A22 --- Bin Binarity status (1)
43- 44 A2 --- l_Per [≥ ] Limit flag on Per
45- 51 F7.2 d Per ? Period
52- 55 F4.1 d e_Per ? rms uncertainty in Per
57- 62 F6.1 d Per2 ? Second period value
64- 83 A20 --- Ref References, in refs.dat files
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Note (1): "no confirmation" means that the velocity amplitude is too low to
confirm binary motion (The velocity amplitude detected is ∼2km/s. Several
phenomena, as spots, pulsation and planetary companions, may result in velocity
variations of comparable amplitude, and they do not have necessarily to be
produced by binary motion), while "p. v. v.?" (= possible velocity variable)
indicates possible long period binaries with too short observation time
(Tsangarides, 2005, PhD Thesis, Open Unviversity (United Kingdom)).
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 2 A2 --- El Element (1)
4- 7 F4.2 --- AG89m Abundance determination by
Anders & Grevesse (1989) (2)
9- 12 F4.2 --- L09ph Abundance determination by
Lodders et al. (2009) (2)
14- 18 F5.2 --- AG89m-L09ph Abundance difference
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Note (1): Only heavy elements with differences higher than 0.05dex are listed
here (Sr, Y and Zr show negligible differences, ≤0.03). The difference
between the two iron values is Δ(logε(Fe))=7.51-7.45=0.06.
Note (2): Anders & Grevesse, 1989, Geochimica Cosmochimica Acta, 53, 197;
Lodders et al., 2009, ed., Landolt-Bornstein - Group VI Astronomy and
Astrophysics Numerical Data and Functional Relationships in Science and
Technology, 4B: Solar System, 4.4. Springer-Verlag, Berlin.
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Byte-by-byte Description of file:refs.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Ref Reference code
7- 25 A19 --- BibCode BibCode
27- 46 A20 --- Aut Author's name
49-112 A64 --- Com Comments
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History:
From electronic version of the journal
References:
Bisterzo et al., Paper I 2010MNRAS.404.1529B 2010MNRAS.404.1529B
(End) Patricia Vannier [CDS] 11-May-2012