pith. sign in

arxiv: 1906.09824 · v1 · pith:V73TQRXTnew · submitted 2019-06-24 · 🌌 astro-ph.SR · astro-ph.GA

Chemical abundances in the metal-intermediate GC NGC 6723

Juliana Crestani , Alan Alves-Brito , Giuseppe Bono , Arthur A. Puls , Javier Alonso-Garc\'ia This is my paper

Pith reviewed 2026-05-25 16:59 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GA
keywords globular clusterNGC 6723chemical abundancesmetallicityalpha elementsred giant branchspectral analysismetal-intermediate
0
0 comments X

The pith

NGC 6723 chemical abundances match metal-intermediate globular clusters and show no metal-rich transition signs.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper measures detailed chemical abundances from high-resolution spectra of eleven red giant branch stars in the inner-halo globular cluster NGC 6723. It reports a mean metallicity of [Fe/H] = -0.93 dex, alpha-element enrichment of roughly 0.39, and standard patterns for light elements, Fe-peak elements, neutron-capture elements, and the Na-O and Mg-Al anti-correlations. These values place the cluster with metal-intermediate and lower-metallicity systems rather than at the start of metal-rich behavior, even though NGC 6723 sits at the minimum of the globular-cluster metallicity distribution and has an extended horizontal branch. A reader would care because the result clarifies where the chemical shift between metallicity regimes actually occurs in these ancient systems.

Core claim

High-resolution spectral analysis of eleven red giant branch stars yields [Fe/H] = -0.93 ± 0.05 dex and [α/Fe] ≈ 0.39, together with typical abundances for Na, Al, V, Cr, Mn, Co, Ni, Cu, Ba, and Eu and the expected Na-O and Mg-Al anticorrelations. These patterns align NGC 6723 with metal-intermediate globular clusters and their lower-metallicity counterparts, showing no chemical prodrome of the metal-rich regime.

What carries the argument

High-resolution spectroscopy (R ≈ 22000-48000) of red giant branch stars to derive abundances of light, alpha, Fe-peak, and neutron-capture elements.

If this is right

  • NGC 6723 reinforces the separation between metallicity regimes in the bimodal globular-cluster distribution.
  • The cluster can serve as a reference point for chemical-evolution models at the metal-intermediate boundary.
  • Other clusters near the same metallicity minimum should display similar abundance patterns if the conclusion holds.
  • The presence of an extended horizontal branch and many RR Lyrae stars remains compatible with the observed chemical properties.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • The transition to metal-rich chemical signatures may occur at metallicities higher than NGC 6723's value.
  • Multiple stellar populations within the cluster could still harbor abundance variations not fully sampled by these eleven stars.
  • Similar abundance work on additional transitional clusters would test whether NGC 6723 is typical or an outlier.

Load-bearing premise

The eleven selected red giant branch stars give a representative view of the cluster's chemical composition without large selection biases or unaccounted systematic errors in the abundance measurements.

What would settle it

A larger sample of stars or an independent analysis method that returns a clearly different mean [α/Fe] or altered anti-correlation strengths would contradict the reported alignment with metal-intermediate clusters.

Figures

Figures reproduced from arXiv: 1906.09824 by Alan Alves-Brito, Arthur A. Puls, Giuseppe Bono, Javier Alonso-Garc\'ia, Juliana Crestani.

Figure 1
Figure 1. Figure 1: Finding chart for the analyzed stars, which are indi￾cated by red circles. The dashed and full line black cirles represent the core and half-light radius, respectively (Harris 1996, 2010 edi￾tion). Image from the ESO Digitized Sky Survey. lan telescopes on Cerro Manqui at the Las Campanas Obser￾vatory, at a resolution of R ≈ 22000. These data were reduced using the MIKE pipeline, with continuum normalizati… view at source ↗
Figure 2
Figure 2. Figure 2: Color-magnitude diagram for NGC 6723 (L14). The analyzed stars are indicated by red crosses. 3 ANALYSIS 3.1 Photometric Parameters Adopting the typical value RV = 3.1, E(B −V) = 0.063 mag (L14), and AKs = 0.117 (Gontcharov 2017; Rieke & Lebofsky 1985), we un-reddened the BV (L14) and Ks (2MASS) mag￾nitudes. With the intrinsic colors, we used two empirical color-temperature relations. The first employs the … view at source ↗
Figure 3
Figure 3. Figure 3: Final result of iterative process to compute the spec￾troscopic atmospheric parameters for star a1. Circles and triangles represent, respectively, FeI and FeII lines. Any trends have been eliminated to slopes equal to or smaller than ±0.001. See text for details. manually tweaked the [X/Fe] abundance of each line until the synthetic profile matched the observed profile ( [PITH_FULL_IMAGE:figures/full_fig_… view at source ↗
Figure 4
Figure 4. Figure 4: Black dots: portion of the observed spectra for the whole sample, ordered by temperature. Each star is indicated, alongside its atmospheric parameters Te f f /log(g)/[Fe /H ]/ξt in K, dex, dex, and kms−1 units, respectively. Red line: the correspond￾ing modelled manganese lines. sition of our sample. Thus, each line for each star has a corresponding σTe f f which refers to its response to ∆Te f f , and sim… view at source ↗
Figure 5
Figure 5. Figure 5: Difference between atmospheric parameters in this work and those of RA16. The difference between our values and those of Ram´ırez & Allende Prieto (2011) for Arcturus is also shown as a quality test for our line list and methodology. In the abscissa, values for Arcturus are represented as Arc, and for stars b1 to b7 as 1 through 7. Our microturbulence velocities are con￾sistently higher than those of RA16,… view at source ↗
Figure 6
Figure 6. Figure 6: Red cirles: this work. Black filled square: stars 1 to 7 as computed by RA16. Blue star: 47 Tucanae (Cordero et al. 2014). Blue triangle: NGC 6266 (M62, Yong et al. 2014). Blue up￾side down triangle: NGC 6528 (Carretta et al. 2001). Blue circle: NGC 6522 (Barbuy et al. 2014). Blue square: NGC 6553 (Alves￾Brito et al. 2006). Blue diamond: NGC 6366 (Puls et al. 2018). Black empty squares: GCs from Carretta e… view at source ↗
Figure 7
Figure 7. Figure 7: Red cirles: this work. Black square: stars 1 to 7 as computed by RA16. Blue star: 47 Tucanae (Cordero et al. 2014). Blue square: NGC 6838 (Cordero et al. 2015). Blue triangle: NGC 6266 (M62, Yong et al. 2014). Blue upside down triangle: NGC 6528 (Carretta et al. 2001). Blue diamond: NGC 6366 (Puls et al. 2018). Grey crosses and ’x’: Bulge field stars from Alves-Brito et al. (2010) and Johnson et al. (2014)… view at source ↗
Figure 9
Figure 9. Figure 9: Red cirles: this work. Black square: stars 1 to 7 as com￾puted by RA16. Blue triangle: NGC 6266 (M62, Yong et al. 2014). Blue upside down triangle: NGC 6528 (Carretta et al. 2001). Blue diamond: NGC 6366 (Puls et al. 2018). Blue star, square, dot, cir￾cle, triangle to the right, triangle to the left: 47 Tucanae, NGC 6553, NGC 6528, HP 1, NGC 6552, NGC 6558, respectively (Er￾nandes et al. 2018). Grey crosse… view at source ↗
Figure 10
Figure 10. Figure 10: Red cirles: this work, with a black cross over a red circle marking star b6 due to its lower SNR. Black square: stars 1 to 7 as computed by RA16. Grey circles: HB stars from NGC 6723 (Gratton et al. 2015). Blue triangle: NGC 6266 (M62, Yong et al. 2014). Blue upside down triangle: NGC 6528 (Carretta et al. 2001). Blue diamond: NGC 6366 (Puls et al. 2018). Blue star: 47 Tucanae (Cordero et al. 2014). Blue … view at source ↗
Figure 12
Figure 12. Figure 12: Final abundance pattern for NGC 6723. Boxes repre￾sent the interquartile ranges (IQR), whiskers the 1.5×IQR limits (approximately 2.7× the standard deviation in the star-to-star spread σ∗), black lines the means, red lines the medians, red cir￾cles the outliers. b1 and b4, appear as Na-depleted and O-enhanced in our study, and are recognized as CN-weak photometrically by Lim et al. (2016), confirming them… view at source ↗
Figure 11
Figure 11. Figure 11: Different HB morphology parameters as a function of metallicity: τHB index (Torelli et al. 2019) with a red line indicat￾ing the best fit and blue lines the 1.5σ levels, L1 and L2 (Milone et al. 2014), and the HBR (Lee et al. 1988). Black cirles: GCs with available τHB index, with metallicities from (Carretta et al. 2009c). Red square: NGC 6723 considering [Fe/H] = −1.10 dex. Red triangle: NGC 6723 consid… view at source ↗
read the original abstract

We have performed a detailed spectral analysis of the inner halo Galactic globular cluster (GC) NGC 6723 using high resolution (R$\approx$ 22000-48000) spectra for for eleven red giant branch stars collected with MIKE (Magellan) and FEROS (MPG/ESO). This globular is located at the minimum of the bimodal metallicity distribution of GCs suggesting that it might be an excellent transitional system between metal-intermediate and metal-rich GCs. In spite of its metal-intermediate status, it is characterized by an extended horizontal branch and by a large number of RR Lyrae stars. We investigated abundances of a variety of species including light, $\alpha$-, Fe-peak, and neutron capture elements. We found a mean metallicity $[Fe/H]=-0.93 \pm 0.05$ dex, and a typical $\alpha$ -enrichment ($[\alpha/Fe] \approx 0.39$) that follows the trend of metal-poor and metal-intermediate GCs. The same outcome applies for light metals (Na, Al), Fe-peak (V, Cr, Mn, Fe, Co, Ni, Cu), $s$/$r$-process elements (Ba, Eu) and for the classical anti-correlation: Na-O and Mg-Al. The current findings further support the evidence that the chemical enrichment of NGC 6723 is in more line with metal-intermediate GCs and their lower metallicity counterparts, and it does not bring forward the prodrome of the metal-rich regime.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper reports a high-resolution spectroscopic analysis (R≈22000-48000) of 11 red giant branch stars in the inner-halo globular cluster NGC 6723 observed with MIKE and FEROS. It derives a mean metallicity [Fe/H]=−0.93±0.05, [α/Fe]≈0.39, abundances for light, α, Fe-peak and neutron-capture elements, and the presence of Na-O and Mg-Al anticorrelations. The central claim is that these patterns align NGC 6723 with metal-intermediate and lower-metallicity GCs rather than foreshadowing the metal-rich regime, despite its location at the metallicity bimodality minimum and its extended horizontal branch.

Significance. If the abundances are accurate and representative, the work supplies a well-sampled abundance set at a key transitional metallicity, reinforcing the chemical continuity between metal-poor and metal-intermediate GCs. The dual-instrument dataset and coverage of s/r-process ratios plus classical anticorrelations are useful additions to the GC abundance literature.

major comments (2)
  1. [Abstract and results] Abstract and results section: The claim that NGC 6723 shows no prodrome of the metal-rich regime rests on abundances derived from only 11 RGB stars. The manuscript must demonstrate that this sample is representative of the cluster (e.g., by quantifying selection effects from the inner-halo location or RGB evolutionary stage and by comparing the observed spread to literature samples of similar size).
  2. [Methods and error analysis] Methods and error analysis: The quoted [Fe/H] uncertainty of ±0.05 dex and the [α/Fe] value are used to place NGC 6723 relative to other GCs, yet the abstract (and presumably the methods) provides no explicit information on line selection, model-atmosphere assumptions (1D LTE), or the full error budget including possible NLTE effects on Na, O, or neutron-capture elements. Without these, systematic offsets >0.1 dex cannot be ruled out and would affect the alignment conclusion.
minor comments (2)
  1. [Abstract] Abstract: duplicate word “for for eleven”; “in more line with” should read “more in line with”.
  2. [Abstract] The term “prodrome” is non-standard in this context; consider “precursor signatures” or “indications”.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed and constructive report. We address the major comments point-by-point below, agreeing that additional clarifications are beneficial. The manuscript will be revised to incorporate these improvements.

read point-by-point responses

  1. Referee: [Abstract and results] Abstract and results section: The claim that NGC 6723 shows no prodrome of the metal-rich regime rests on abundances derived from only 11 RGB stars. The manuscript must demonstrate that this sample is representative of the cluster (e.g., by quantifying selection effects from the inner-halo location or RGB evolutionary stage and by comparing the observed spread to literature samples of similar size).

    Authors: We note that samples of 10-15 stars are common in high-resolution GC abundance studies. Our stars were chosen from the inner regions but span the RGB as shown in the CMD figure. The measured spreads in [Fe/H] and other elements are similar to those in comparable literature samples. To better demonstrate representativeness, we will add text in Section 3 (Results) quantifying the selection and comparing the observed dispersions to those in other GCs with similar sample sizes and metallicities. revision: yes

  2. Referee: [Methods and error analysis] Methods and error analysis: The quoted [Fe/H] uncertainty of ±0.05 dex and the [α/Fe] value are used to place NGC 6723 relative to other GCs, yet the abstract (and presumably the methods) provides no explicit information on line selection, model-atmosphere assumptions (1D LTE), or the full error budget including possible NLTE effects on Na, O, or neutron-capture elements. Without these, systematic offsets >0.1 dex cannot be ruled out and would affect the alignment conclusion.

    Authors: The full methods section (Section 2) details the line list used, the adoption of 1D LTE ATLAS9 models and MOOG, and the error estimation from parameter variations and EW uncertainties. However, we agree that an explicit statement on these assumptions and a discussion of potential NLTE effects would improve the paper. We will add a paragraph in the methods section outlining the assumptions and error budget. For NLTE, we will note that for the relevant elements at [Fe/H] ~ -1, the effects are generally small and do not alter the conclusion that the abundances align with metal-intermediate GCs rather than metal-rich ones. We cite supporting literature for this. revision: partial

Circularity Check

0 steps flagged

Observational abundance study with no derivations or self-referential reductions

full rationale

This is a purely observational paper: high-resolution spectra of 11 RGB stars are reduced to elemental abundances via standard spectral analysis, then compared to literature trends for other GCs. No equations, predictions, fitted parameters renamed as outputs, or load-bearing self-citations appear in the derivation chain. The central claim (alignment with metal-intermediate GCs) rests on direct measurements and external comparisons, not on any step that reduces to its own inputs by construction.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Central claim rests on fitted mean abundances from spectral analysis of a small stellar sample plus standard assumptions of stellar spectroscopy; no invented entities.

free parameters (2)
  • mean [Fe/H] = -0.93 ± 0.05
    Determined by fitting spectral lines of 11 RGB stars
  • [alpha/Fe] = 0.39
    Average alpha-element enhancement from multiple species
axioms (2)
  • domain assumption The 11 observed RGB stars are chemically representative of the entire cluster
    Implicit when reporting cluster-wide means and anti-correlations
  • domain assumption Standard 1D LTE model atmospheres and line formation suffice for abundance derivation
    Common in the field but not explicitly validated in abstract

pith-pipeline@v0.9.0 · 5824 in / 1283 out tokens · 27868 ms · 2026-05-25T16:59:23.253962+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

94 extracted references · 94 canonical work pages · 4 internal anchors

  1. [1]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

    work page

  2. [2]

    Alca \' no G., Liller W., Alvarado F., Mironov A., Ipatov A., Piskunov A., Samus N., Smirnov O., 1999, @doi [ ] 10.1051/aas:1999228 , http://adsabs.harvard.edu/abs/1999A

    work page doi:10.1051/aas:1999228 1999

  3. [3]

    L., and Asplund , M

    Allende Prieto C., Lambert D. L., Asplund M., 2001, @doi [ ] 10.1086/322874 , http://adsabs.harvard.edu/abs/2001ApJ...556L..63A 556, L63

    work page doi:10.1086/322874 2001

  4. [4]

    Alonso A., Arribas S., Mart \' nez-Roger C., 1999, @doi [ ] 10.1051/aas:1999521 , http://adsabs.harvard.edu/abs/1999A

    work page doi:10.1051/aas:1999521 1999

  5. [5]

    Alonso A., Arribas S., Mart \' nez-Roger C., 2001, @doi [ ] 10.1051/0004-6361:20011095 , http://adsabs.harvard.edu/abs/2001A

    work page doi:10.1051/0004-6361:20011095 2001

  6. [6]

    Alves-Brito A., et al., 2006, @doi [ ] 10.1051/0004-6361:20065488 , http://adsabs.harvard.edu/abs/2006A

    work page doi:10.1051/0004-6361:20065488 2006

  7. [7]

    Alves-Brito A., Mel \'e ndez J., Asplund M., Ram \' rez I., Yong D., 2010, @doi [ ] 10.1051/0004-6361/200913444 , http://adsabs.harvard.edu/abs/2010A

    work page doi:10.1051/0004-6361/200913444 2010

  8. [8]

    J., Scott P., 2009, @doi [ ] 10.1146/annurev.astro.46.060407.145222 , http://adsabs.harvard.edu/abs/2009ARA

    Asplund M., Grevesse N., Sauval A. J., Scott P., 2009, @doi [ ] 10.1146/annurev.astro.46.060407.145222 , http://adsabs.harvard.edu/abs/2009ARA

    work page doi:10.1146/annurev.astro.46.060407.145222 2009

  9. [9]

    Barbuy B., et al., 2013, @doi [ ] 10.1051/0004-6361/201322380 , http://adsabs.harvard.edu/abs/2013A

    work page doi:10.1051/0004-6361/201322380 2013

  10. [10]

    Barbuy B., et al., 2014, @doi [ ] 10.1051/0004-6361/201424311 , http://adsabs.harvard.edu/abs/2014A

    work page doi:10.1051/0004-6361/201424311 2014

  11. [11]

    Barbuy B., Chiappini C., Gerhard O., 2018, preprint, http://adsabs.harvard.edu/abs/2018arXiv180501142B ( @eprint arXiv 1805.01142 )

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  12. [12]

    Bastian N., Lardo C., 2015, @doi [ ] 10.1093/mnras/stv1661 , http://adsabs.harvard.edu/abs/2015MNRAS.453..357B 453, 357

    work page doi:10.1093/mnras/stv1661 2015

  13. [13]

    Bastian N., Lardo C., 2018, @doi [ ] 10.1146/annurev-astro-081817-051839 , http://adsabs.harvard.edu/abs/2018ARA

    work page doi:10.1146/annurev-astro-081817-051839 2018

  14. [14]

    R., Piotto G., Anderson J., King I

    Bedin L. R., Piotto G., Anderson J., King I. R., Cassisi S., Momany Y., 2004, Memorie della Societa Astronomica Italiana Supplementi, http://adsabs.harvard.edu/abs/2004MSAIS...5..105B 5, 105

    work page 2004

  15. [15]

    Bergemann M., Cescutti G., 2010, @doi [ ] 10.1051/0004-6361/201014250 , http://adsabs.harvard.edu/abs/2010A

    work page doi:10.1051/0004-6361/201014250 2010

  16. [16]

    Bergemann M., Gehren T., 2008, @doi [ ] 10.1051/0004-6361:200810098 , http://adsabs.harvard.edu/abs/2008A

    work page doi:10.1051/0004-6361:200810098 2008

  17. [17]

    R., 2009, @doi [ ] 10.1111/j.1365-2966.2009.15167.x , http://adsabs.harvard.edu/abs/2009MNRAS.398..607V 398, 607

    Bergemann M., Pickering J. C., Gehren T., 2010, @doi [ ] 10.1111/j.1365-2966.2009.15736.x , http://adsabs.harvard.edu/abs/2010MNRAS.401.1334B 401, 1334

    work page doi:10.1111/j.1365-2966.2009.15736.x 2010

  18. [18]

    A., Gunnels S

    Bernstein R., Shectman S. A., Gunnels S. M., Mochnacki S., Athey A. E., 2003, in Iye M., Moorwood A. F. M., eds, Vol. 4841, Instrument Design and Performance for Optical/Infrared Ground-based Telescopes. pp 1694--1704, @doi 10.1117/12.461502

    work page doi:10.1117/12.461502 2003

  19. [19]

    Bica E., Bonatto C., Barbuy B., Ortolani S., 2006, @doi [ ] 10.1051/0004-6361:20054351 , https://ui.adsabs.harvard.edu/\#abs/2006A&A...450..105B 450, 105

    work page doi:10.1051/0004-6361:20054351 2006

  20. [20]

    H., Brodie J

    Buonanno R., 1993, in Smith G. H., Brodie J. P., eds, Astronomical Society of the Pacific Conference Series Vol. 48, The Globular Cluster-Galaxy Connection. p. 131

    work page 1993

  21. [21]

    G., 1997, @doi [ ] 10.1051/aas:1997116 , http://adsabs.harvard.edu/abs/1997A

    Carretta E., Gratton R. G., 1997, @doi [ ] 10.1051/aas:1997116 , http://adsabs.harvard.edu/abs/1997A

    work page doi:10.1051/aas:1997116 1997

  22. [22]

    G., Gratton R

    Carretta E., Cohen J. G., Gratton R. G., Behr B. B., 2001, @doi [ ] 10.1086/322116 , http://adsabs.harvard.edu/abs/2001AJ....122.1469C 122, 1469

    work page doi:10.1086/322116 2001

  23. [23]

    Carretta E., et al., 2009a, @doi [ ] 10.1051/0004-6361/200912096 , http://adsabs.harvard.edu/abs/2009A

    work page doi:10.1051/0004-6361/200912096

  24. [24]

    Carretta E., Bragaglia A., Gratton R., Lucatello S., 2009b, @doi [ ] 10.1051/0004-6361/200912097 , http://adsabs.harvard.edu/abs/2009A

    work page doi:10.1051/0004-6361/200912097

  25. [25]

    Carretta E., Bragaglia A., Gratton R., D'Orazi V., Lucatello S., 2009c, @doi [ ] 10.1051/0004-6361/200913003 , http://adsabs.harvard.edu/abs/2009A

    work page doi:10.1051/0004-6361/200913003

  26. [26]

    Carretta E., Bragaglia A., Gratton R., Lucatello S., Bellazzini M., D'Orazi V., 2010, @doi [ ] 10.1088/2041-8205/712/1/L21 , http://adsabs.harvard.edu/abs/2010ApJ...712L..21C 712, L21

    work page doi:10.1088/2041-8205/712/1/l21 2010

  27. [27]

    G., Kurucz R

    Castelli F., Gratton R. G., Kurucz R. L., 1997, , http://adsabs.harvard.edu/abs/1997A

    work page 1997

  28. [28]

    Catelan M., 2009, @doi [ ] 10.1007/s10509-009-9987-8 , http://adsabs.harvard.edu/abs/2009Ap

    work page doi:10.1007/s10509-009-9987-8 2009

  29. [29]

    A., Glushkova E

    Chemel A. A., Glushkova E. V., Dambis A. K., Rastorguev A. S., Yalyalieva L. N., Klinichev A. D., 2018, @doi [Astrophysical Bulletin] 10.1134/S1990341318020049 , http://adsabs.harvard.edu/abs/2018AstBu..73..162C 73, 162

    work page doi:10.1134/s1990341318020049 2018

  30. [30]

    J., Pilachowski C

    Cordero M. J., Pilachowski C. A., Johnson C. I., McDonald I., Zijlstra A. A., Simmerer J., 2014, @doi [ ] 10.1088/0004-637X/780/1/94 , http://adsabs.harvard.edu/abs/2014ApJ...780...94C 780, 94

    work page doi:10.1088/0004-637x/780/1/94 2014

  31. [31]

    J., Pilachowski C

    Cordero M. J., Pilachowski C. A., Johnson C. I., Vesperini E., 2015, @doi [ ] 10.1088/0004-637X/800/1/3 , http://adsabs.harvard.edu/abs/2015ApJ...800....3C 800, 3

    work page doi:10.1088/0004-637x/800/1/3 2015

  32. [32]

    J., 1966, in Hubenet H., ed., IAU Symposium Vol

    Deutsch A. J., 1966, in Hubenet H., ed., IAU Symposium Vol. 26, Abundance Determinations in Stellar Spectra. p. 112

    work page 1966

  33. [33]

    V., Da Costa G

    Dias B., Barbuy B., Saviane I., Held E. V., Da Costa G. S., Ortolani S., Gullieuszik M., V \'a squez S., 2016, @doi [ ] 10.1051/0004-6361/201526765 , http://adsabs.harvard.edu/abs/2016A

    work page doi:10.1051/0004-6361/201526765 2016

  34. [34]

    I., Girard T

    Dinescu D. I., Girard T. M., van Altena W. F., L \'o pez C. E., 2003, @doi [ ] 10.1086/367801 , http://adsabs.harvard.edu/abs/2003AJ....125.1373D 125, 1373

    work page doi:10.1086/367801 2003

  35. [35]

    W., 2008, @doi [ ] 10.1086/589654 , http://adsabs.harvard.edu/abs/2008ApJS..178...89D 178, 89

    Dotter A., Chaboyer B., Jevremovi \'c D., Kostov V., Baron E., Ferguson J. W., 2008, @doi [ ] 10.1086/589654 , http://adsabs.harvard.edu/abs/2008ApJS..178...89D 178, 89

    work page doi:10.1086/589654 2008

  36. [36]

    Dotter A., et al., 2010, @doi [ ] 10.1088/0004-637X/708/1/698 , http://adsabs.harvard.edu/abs/2010ApJ...708..698D 708, 698

    work page doi:10.1088/0004-637x/708/1/698 2010

  37. [37]

    Iron-peak elements Sc, V, Mn, Cu and Zn in Galactic bulge globular clusters

    Ernandes H., Barbuy B., Alves-Brito A., Friaca A., Siqueira-Mello C., Allen D. M., 2018, preprint, http://adsabs.harvard.edu/abs/2018arXiv180106157E ( @eprint arXiv 1801.06157 )

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  38. [38]

    C., Norris J., 1981, @doi [ ] 10.1146/annurev.aa.19.090181.001535 , http://adsabs.harvard.edu/abs/1981ARA

    Freeman K. C., Norris J., 1981, @doi [ ] 10.1146/annurev.aa.19.090181.001535 , http://adsabs.harvard.edu/abs/1981ARA

    work page doi:10.1146/annurev.aa.19.090181.001535 1981

  39. [39]

    K., Carney B

    Fullton L. K., Carney B. W., 1996, in Morrison H. L., Sarajedini A., eds, Astronomical Society of the Pacific Conference Series Vol. 92, Formation of the Galactic Halo...Inside and Out. p. 265

    work page 1996

  40. [40]

    Gaia Collaboration et al., 2016, @doi [ ] 10.1051/0004-6361/201629272 , http://adsabs.harvard.edu/abs/2016A

    work page doi:10.1051/0004-6361/201629272 2016

  41. [41]

    Gaia Collaboration Brown A. G. A., Vallenari A., Prusti T., de Bruijne J. H. J., Babusiaux C., Bailer-Jones C. A. L., 2018, preprint, http://adsabs.harvard.edu/abs/2018arXiv180409365G ( @eprint arXiv 1804.09365 )

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  42. [42]

    A., 2017, @doi [Astronomy Letters] 10.1134/S1063773717070039 , http://adsabs.harvard.edu/abs/2017AstL...43..472G 43, 472

    Gontcharov G. A., 2017, @doi [Astronomy Letters] 10.1134/S1063773717070039 , http://adsabs.harvard.edu/abs/2017AstL...43..472G 43, 472

    work page doi:10.1134/s1063773717070039 2017

  43. [43]

    I., Bonifacio P., 2009, @doi [ ] 10.1051/0004-6361/200810904 , http://adsabs.harvard.edu/abs/2009A

    Gonz \'a lez Hern \'a ndez J. I., Bonifacio P., 2009, @doi [ ] 10.1051/0004-6361/200810904 , http://adsabs.harvard.edu/abs/2009A

    work page doi:10.1051/0004-6361/200810904 2009

  44. [44]

    Gratton R., Sneden C., Carretta E., 2004, @doi [ ] 10.1146/annurev.astro.42.053102.133945 , http://adsabs.harvard.edu/abs/2004ARA

    work page doi:10.1146/annurev.astro.42.053102.133945 2004

  45. [45]

    G., Carretta E., Bragaglia A., 2012, @doi [ ] 10.1007/s00159-012-0050-3 , http://adsabs.harvard.edu/abs/2012A

    Gratton R. G., Carretta E., Bragaglia A., 2012, @doi [ ] 10.1007/s00159-012-0050-3 , http://adsabs.harvard.edu/abs/2012A

    work page doi:10.1007/s00159-012-0050-3 2012

  46. [46]

    G., et al., 2015, @doi [ ] 10.1051/0004-6361/201424393 , http://adsabs.harvard.edu/abs/2015A

    Gratton R. G., et al., 2015, @doi [ ] 10.1051/0004-6361/201424393 , http://adsabs.harvard.edu/abs/2015A

    work page doi:10.1051/0004-6361/201424393 2015

  47. [47]

    G., Plez B., 2003, in Hubeny I., Mihalas D., Werner K., eds, Astronomical Society of the Pacific Conference Series Vol

    Gustafsson B., Edvardsson B., Eriksson K., Mizuno-Wiedner M., J rgensen U. G., Plez B., 2003, in Hubeny I., Mihalas D., Werner K., eds, Astronomical Society of the Pacific Conference Series Vol. 288, Stellar Atmosphere Modeling. p. 331

    work page 2003

  48. [48]

    E., 1996, @doi [ ] 10.1086/118116 , http://adsabs.harvard.edu/abs/1996AJ....112.1487H 112, 1487

    Harris W. E., 1996, @doi [ ] 10.1086/118116 , http://adsabs.harvard.edu/abs/1996AJ....112.1487H 112, 1487

    work page doi:10.1086/118116 1996

  49. [49]

    E., Canterna R., 1979, @doi [ ] 10.1086/182997 , http://adsabs.harvard.edu/abs/1979ApJ...231L..19H 231, L19

    Harris W. E., Canterna R., 1979, @doi [ ] 10.1086/182997 , http://adsabs.harvard.edu/abs/1979ApJ...231L..19H 231, L19

    work page doi:10.1086/182997 1979

  50. [50]

    N., Chiba M., Aoki W., 2012, @doi [ ] 10.1088/0004-637X/753/1/64 , http://adsabs.harvard.edu/abs/2012ApJ...753...64I 753, 64

    Ishigaki M. N., Chiba M., Aoki W., 2012, @doi [ ] 10.1088/0004-637X/753/1/64 , http://adsabs.harvard.edu/abs/2012ApJ...753...64I 753, 64

    work page doi:10.1088/0004-637x/753/1/64 2012

  51. [51]

    I., Rich R

    Johnson C. I., Rich R. M., Kobayashi C., Kunder A., Koch A., 2014, @doi [ ] 10.1088/0004-6256/148/4/67 , http://adsabs.harvard.edu/abs/2014AJ....148...67J 148, 67

    work page doi:10.1088/0004-6256/148/4/67 2014

  52. [52]

    Jurcsik J., Kovacs G., 1996, , http://adsabs.harvard.edu/abs/1996A

    work page 1996

  53. [53]

    I., Lattanzio J

    Karakas A. I., Lattanzio J. C., 2014, @doi [ ] 10.1017/pasa.2014.21 , http://adsabs.harvard.edu/abs/2014PASA...31...30K 31, e030

    work page doi:10.1017/pasa.2014.21 2014

  54. [54]

    Kobayashi C., Umeda H., Nomoto K., Tominaga N., Ohkubo T., 2006, @doi [ ] 10.1086/508914 , http://adsabs.harvard.edu/abs/2006ApJ...653.1145K 653, 1145

    work page doi:10.1086/508914 2006

  55. [55]

    A., Andrievsky S

    Korotin S. A., Andrievsky S. M., Hansen C. J., Caffau E., Bonifacio P., Spite M., Spite F., Fran c ois P., 2015, @doi [ ] 10.1051/0004-6361/201526558 , http://adsabs.harvard.edu/abs/2015A

    work page doi:10.1051/0004-6361/201526558 2015

  56. [56]

    P., Ivans I

    Kraft R. P., Ivans I. I., 2003, @doi [ ] 10.1086/345914 , http://adsabs.harvard.edu/abs/2003PASP..115..143K 115, 143

    work page doi:10.1086/345914 2003

  57. [57]

    Lardo C., Salaris M., Bastian N., Mucciarelli A., Dalessandro E., Cabrera-Ziri I., 2018, @doi [ ] 10.1051/0004-6361/201832999 , http://adsabs.harvard.edu/abs/2018A

    work page doi:10.1051/0004-6361/201832999 2018

  58. [58]

    E., Wickliffe M

    Lawler J. E., Wickliffe M. E., den Hartog E. A., Sneden C., 2001, @doi [ ] 10.1086/323407 , http://adsabs.harvard.edu/abs/2001ApJ...563.1075L 563, 1075

    work page doi:10.1086/323407 2001

  59. [59]

    Lee Y.-W., Demarque P., Zinn R., 1988, in Philip A. G. D., ed., Calibration of Stellar ages. pp 149--162

    work page 1988

  60. [60]

    Lee Y.-W., Demarque P., Zinn R., 1994, @doi [ ] 10.1086/173803 , http://adsabs.harvard.edu/abs/1994ApJ...423..248L 423, 248

    work page doi:10.1086/173803 1994

  61. [61]

    L., Walker A., 2014, @doi [ ] 10.1088/0067-0049/210/1/6 , http://adsabs.harvard.edu/abs/2014ApJS..210....6L 210, 6

    Lee J.-W., L \'o pez-Morales M., Hong K., Kang Y.-W., Pohl B. L., Walker A., 2014, @doi [ ] 10.1088/0067-0049/210/1/6 , http://adsabs.harvard.edu/abs/2014ApJS..210....6L 210, 6

    work page doi:10.1088/0067-0049/210/1/6 2014

  62. [62]

    Lim D., Lee Y.-W., Pasquato M., Han S.-I., Roh D.-G., 2016, @doi [ ] 10.3847/0004-637X/832/2/99 , http://adsabs.harvard.edu/abs/2016ApJ...832...99L 832, 99

    work page doi:10.3847/0004-637x/832/2/99 2016

  63. [63]

    H., Fraquelli D

    Martins D. H., Fraquelli D. A., 1987, @doi [ ] 10.1086/191218 , http://adsabs.harvard.edu/abs/1987ApJS...65...83M 65, 83

    work page doi:10.1086/191218 1987

  64. [64]

    McWilliam A., 2016, @doi [ ] 10.1017/pasa.2016.32 , http://adsabs.harvard.edu/abs/2016PASA...33...40M 33, e040

    work page doi:10.1017/pasa.2016.32 2016

  65. [65]

    Mel \'e ndez J., et al., 2008, @doi [ ] 10.1051/0004-6361:200809398 , http://adsabs.harvard.edu/abs/2008A

    work page doi:10.1051/0004-6361:200809398 2008

  66. [66]

    P., et al., 2014, @doi [ ] 10.1088/0004-637X/785/1/21 , http://adsabs.harvard.edu/abs/2014ApJ...785...21M 785, 21

    Milone A. P., et al., 2014, @doi [ ] 10.1088/0004-637X/785/1/21 , http://adsabs.harvard.edu/abs/2014ApJ...785...21M 785, 21

    work page doi:10.1088/0004-637x/785/1/21 2014

  67. [67]

    P., et al., 2017, @doi [ ] 10.1093/mnras/stw2531 , http://adsabs.harvard.edu/abs/2017MNRAS.464.3636M 464, 3636

    Milone A. P., et al., 2017, @doi [ ] 10.1093/mnras/stw2531 , http://adsabs.harvard.edu/abs/2017MNRAS.464.3636M 464, 3636

    work page doi:10.1093/mnras/stw2531 2017

  68. [68]

    Nomoto K., Tominaga N., Umeda H., Kobayashi C., Maeda K., 2006, @doi [Nuclear Physics A] 10.1016/j.nuclphysa.2006.05.008 , http://adsabs.harvard.edu/abs/2006NuPhA.777..424N 777, 424

    work page doi:10.1016/j.nuclphysa.2006.05.008 2006

  69. [69]

    Osborn W., 1971, The Observatory, http://adsabs.harvard.edu/abs/1971Obs....91..223O 91, 223

    work page 1971

  70. [70]

    Piotto G., et al., 2007, @doi [ ] 10.1086/518503 , http://adsabs.harvard.edu/abs/2007ApJ...661L..53P 661, L53

    work page doi:10.1086/518503 2007

  71. [71]

    X., McWilliam A., 2000, @doi [ ] 10.1086/312749 , http://adsabs.harvard.edu/abs/2000ApJ...537L..57P 537, L57

    Prochaska J. X., McWilliam A., 2000, @doi [ ] 10.1086/312749 , http://adsabs.harvard.edu/abs/2000ApJ...537L..57P 537, L57

    work page doi:10.1086/312749 2000

  72. [72]

    X., Naumov S

    Prochaska J. X., Naumov S. O., Carney B. W., McWilliam A., Wolfe A. M., 2000, @doi [ ] 10.1086/316818 , http://adsabs.harvard.edu/abs/2000AJ....120.2513P 120, 2513

    work page doi:10.1086/316818 2000

  73. [73]

    A., Alves-Brito A., Campos F., Dias B., Barbuy B., 2018, @doi [ ] 10.1093/mnras/sty267 , http://adsabs.harvard.edu/abs/2018MNRAS.476..690P 476, 690

    Puls A. A., Alves-Brito A., Campos F., Dias B., Barbuy B., 2018, @doi [ ] 10.1093/mnras/sty267 , http://adsabs.harvard.edu/abs/2018MNRAS.476..690P 476, 690

    work page doi:10.1093/mnras/sty267 2018

  74. [74]

    Ram \' rez I., Allende Prieto C., 2011, @doi [ ] 10.1088/0004-637X/743/2/135 , http://adsabs.harvard.edu/abs/2011ApJ...743..135R 743, 135

    work page doi:10.1088/0004-637x/743/2/135 2011

  75. [75]

    G., 2006, @doi [ ] 10.1051/0004-6361:20053006 , http://adsabs.harvard.edu/abs/2006A

    Recio-Blanco A., Aparicio A., Piotto G., de Angeli F., Djorgovski S. G., 2006, @doi [ ] 10.1051/0004-6361:20053006 , http://adsabs.harvard.edu/abs/2006A

    work page doi:10.1051/0004-6361:20053006 2006

  76. [76]

    M., et al., 1997, @doi [ ] 10.1086/310758 , http://adsabs.harvard.edu/abs/1997ApJ...484L..25R 484, L25

    Rich R. M., et al., 1997, @doi [ ] 10.1086/310758 , http://adsabs.harvard.edu/abs/1997ApJ...484L..25R 484, L25

    work page doi:10.1086/310758 1997

  77. [77]

    H., Lebofsky M

    Rieke G. H., Lebofsky M. J., 1985, @doi [ ] 10.1086/162827 , http://adsabs.harvard.edu/abs/1985ApJ...288..618R 288, 618

    work page doi:10.1086/162827 1985

  78. [78]

    Rojas-Arriagada A., Zoccali M., V \'a squez S., Ripepi V., Musella I., Marconi M., Grado A., Limatola L., 2016, @doi [ ] 10.1051/0004-6361/201527351 , http://adsabs.harvard.edu/abs/2016A

    work page doi:10.1051/0004-6361/201527351 2016

  79. [79]

    A., Hesser J

    Rutledge G. A., Hesser J. E., Stetson P. B., Mateo M., Simard L., Bolte M., Friel E. D., Copin Y., 1997, @doi [ ] 10.1086/133958 , http://adsabs.harvard.edu/abs/1997PASP..109..883R 109, 883

    work page doi:10.1086/133958 1997

  80. [80]

    Salaris M., Chieffi A., Straniero O., 1993, @doi [ ] 10.1086/173105 , http://adsabs.harvard.edu/abs/1993ApJ...414..580S 414, 580

    work page doi:10.1086/173105 1993

Showing first 80 references.