A critical survey of atomic transition probabilities for CuI

Biełski, A.

doi:10.1016/0022-4073(75)90065-5

Cited by 91 publications

(21 citation statements)

References 16 publications

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“…We also compare our derived abundance ratios with those presented in Marino et al After accounting for the different sets of log(gf ) values, S.S. abundances (see Marino et al 2009), and line-by-line mean offsets (see Appendix), the abundance offsets for most [Fe/H] and [X/Fe] ratios can be immediately accounted for. Offsets in other species (Ti i, Cu i, Zn i, La ii, and Nd ii) are unexplained by these factors but probably result from the S/N and small numbers of features available in the spectra of Marino et al For Kurucz & Bell (1995); (4) Blackwell et al (1982a,b), increased by 0.056 dex according to Grevesse et al (1989); (5) Pickering et al (2001), with corrections given in Pickering et al (2002); (6) Whaling et al (1985), using HFS from Kurucz & Bell (1995) Nitz et al (1999), using HFS from Kurucz & Bell (1995); (14) Cardon et al (1982), using HFS from Kurucz & Bell (1995); (15) Wickliffe & Lawler (1997a); (16) Bielski (1975), using HFS from Kurucz & Bell (1995); (17) Biémont & Godefroid (1980) Note. -The full version of this table is available in the online edition of the journal.…”

Section: Abundance Analysismentioning

confidence: 99%

CHARACTERIZING THE HEAVY ELEMENTS IN GLOBULAR CLUSTER M22 AND AN EMPIRICALs-PROCESS ABUNDANCE DISTRIBUTION DERIVED FROM THE TWO STELLAR GROUPS

Roederer

Marino

Sneden

2011

ApJ

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We present an empirical s-process abundance distribution derived with explicit knowledge of the r-process component in the low-metallicity globular cluster M22. We have obtained high-resolution, high signal-to-noise spectra for 6 red giants in M22 using the MIKE spectrograph on the Magellan-Clay Telescope at Las Campanas Observatory. In each star we derive abundances for 44 species of 40 elements, including 24 elements heavier than zinc (Z = 30) produced by neutron-capture reactions. Previous studies determined that 3 of these stars (the "r + s group") have an enhancement of sprocess material relative to the other 3 stars (the "r-only group"). We confirm that the r + s group is moderately enriched in Pb relative to the r-only group. Both groups of stars were born with the same amount of r-process material, but s-process material was also present in the gas from which the r + s group formed. The s-process abundances are inconsistent with predictions for AGB stars with M ≤ 3 M ⊙ and suggest an origin in more massive AGB stars capable of activating the 22 Ne(α,n) 25 Mg reaction. We calculate the s-process "residual" by subtracting the r-process pattern in the r-only group from the abundances in the r + s group. In contrast to previous r-and s-process decompositions, this approach makes no assumptions about the r-and s-process distributions in the solar system and provides a unique opportunity to explore s-process yields in a metal-poor environment.

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Section: Abundance Analysismentioning

confidence: 99%

CHARACTERIZING THE HEAVY ELEMENTS IN GLOBULAR CLUSTER M22 AND AN EMPIRICALs-PROCESS ABUNDANCE DISTRIBUTION DERIVED FROM THE TWO STELLAR GROUPS

Roederer

Marino

Sneden

2011

ApJ

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“…In particular, we used the atomic data by Martin et al (1988) for the Mn I lines at 4030, 4033, 4034, 4041, and 4055 Å; the NIST 4 atomic data for the Ba II lines at 4934, 5853, 6141, and 6496 Å; the atomic data by Lawler et al (2001) for the La II lines at 3988, 4086, 4123, and 4238 Å; and the atomic data by Bielski (1975) for the 5105 Å Cu I line 5 . For the CH and CN molecular bands, we used the Kurucz molecular linelists 6 , but we had to revise the log g f values of C downwards 4 http://physics.nist.gov/PhysRefData/ASD/index.html 5 We could not use the 5872 Å Cu I line since it falls into the gap between the two UVES red CCDs.…”

Section: Equivalent Widths and Atomic Datamentioning

confidence: 99%

The subgiant branch ofω Centauri seen through high-resolution spectroscopy

Pancino¹,

Mucciarelli²,

Sbordone³

et al. 2011

A&A

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We analysed high-resolution UVES spectra of six stars belonging to the subgiant branch of ω Centauri, and derived abundance ratios of 19 chemical elements (namely Al, Ba, C, Ca, Co, Cr, Cu, Fe, La, Mg, Mn, N, Na, Ni, Sc, Si, Sr, Ti, and Y). A comparison with previous abundance determinations for red giants provided remarkable agreement and allowed us to identify the sub-populations to which our targets belong. We found that three targets belong to a low-metallicity population at [Fe/H] -2.0 dex, [α/Fe] +0.4 dex and [s/Fe] 0 dex. Stars with similar characteristics were found in small amounts by past surveys of red giants. We discuss the possibility that they belong to a separate sub-population that we name VMP (very metal-poor, at most 5% of the total cluster population), which -in the self-enrichment hypothesis -is the best-candidate first stellar generation in ω Cen. Two of the remaining targets belong to the dominant metal-poor population (MP) at [Fe/H] -1.7 dex, and the last one to the metal-intermediate (MInt) one at [Fe/H] -1.2 dex. The existence of the newly defined VMP population could help to understand some puzzling results based on low-resolution spectroscopy for age differences determinations, because the metallicity resolution of these studies was probably not enough to detect the VMP population. The VMP could also correspond to some of the additional substructures of the subgiant-branch region found in the latest HST photometry. After trying to correlate chemical abundances with substructures in the subgiant branch of ω Cen, we found that the age difference between the VMP and MP populations should be small (0 ± 2 Gyr), while the difference between the MP and MInt populations could be slightly larger (2 ± 2 Gyr).

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“…1 at 324.7 nm and 327.3 nm. The log g f values were taken from Bielski (1975) and the hyperfine structure and isotopic shifts for the 63 Cu and 65 Cu isotopes from Kurucz (1999). We used the same sources for the two lines of Mult.…”

Section: Atomic Datamentioning

confidence: 99%

Cu i resonance lines in turn-off stars of NGC 6752 and NGC 6397

Bonifacio

Caffau

Ludwig

2010

A&A

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Context.Copper is an element whose interesting evolution with metallicity is not fully understood. Observations of copper abundances rely on a very limited number of lines, the strongest are the Cu i lines of Mult. 1 at 324.7 nm and 327.3 nm which can be measured even at extremely low metallicities. Aims. We investigate the quality of these lines as abundance indicators. Methods. We measure these lines in two turn-off (TO) stars in the Globular Cluster NGC 6752 and two TO stars in the Globular Cluster NGC 6397 and derive abundances with 3D hydrodynamical model atmospheres computed with the CO5BOLD code. These abundances are compared to the Cu abundances measured in giant stars of the same clusters, using the lines of Mult. 2 at 510.5 nm and 578.2 nm. Results. The abundances derived from the lines of Mult. 1 in TO stars differ from the abundances of giants of the same clusters. This is true both using CO5BOLD models and using traditional 1D model atmospheres. The LTE 3D corrections for TO stars are large, while they are small for giant stars.Conclusions. The Cu i resonance lines of Mult. 1 are not reliable abundance indicators. It is likely that departures from LTE should be taken into account to properly describe these lines, although it is not clear if these alone can account for the observations. An investigation of these departures is indeed encouraged for both dwarfs and giants. Our recommendation to those interested in the study of the evolution of copper abundances is to rely on the measurements in giants, based on the lines of Mult. 2. We caution, however, that NLTE studies may imply a revision in all the Cu abundances, both in dwarfs and giants.

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A critical survey of atomic transition probabilities for CuI

Cited by 91 publications

References 16 publications

CHARACTERIZING THE HEAVY ELEMENTS IN GLOBULAR CLUSTER M22 AND AN EMPIRICALs-PROCESS ABUNDANCE DISTRIBUTION DERIVED FROM THE TWO STELLAR GROUPS

CHARACTERIZING THE HEAVY ELEMENTS IN GLOBULAR CLUSTER M22 AND AN EMPIRICALs-PROCESS ABUNDANCE DISTRIBUTION DERIVED FROM THE TWO STELLAR GROUPS

The subgiant branch ofω Centauri seen through high-resolution spectroscopy

Cu i resonance lines in turn-off stars of NGC 6752 and NGC 6397

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