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arxiv: 1906.09828 · v1 · pith:6FNAQU7Inew · submitted 2019-06-24 · 🌌 astro-ph.SR · astro-ph.GA

The Gaia-ESO Survey: The inner disc, intermediate-age open cluster Pismis 18

D. Hatzidimitriou , E. V. Held , E. Tognelli , A. Bragaglia , L. Magrini , L. Bravi , K. Gazeas , A. Dapergolas
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A. Drazdauskas E. Delgado-Mena E.D. Friel R. Minkeviciute R. Sordo G. Tautvaisiene G. Gilmore S. Randich S. Feltzing A. Vallenari E. J. Alfaro E. Flaccomio A. C. Lanzafame E. Pancino R. Smiljanic A. Bayo M. Bergemann G. Carraro A. R. Casey M. T. Costado F. Damiani E. Franciosini A. Gonneau P. Jofre' J. Lewis L. Monaco L. Morbidelli C. C. Worley S. Zaggia
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Pith reviewed 2026-05-25 16:56 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GA
keywords open clusterPismis 18inner discchemical abundancesGaia-ESO Surveymetallicityradial velocityproper motion
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The pith

Six UVES spectra establish Pismis 18 as a 700-Myr-old inner-disc cluster with [Fe/H] = +0.23.

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

The paper applies Gaia-ESO Survey observations to the open cluster Pismis 18, which lies inside the solar circle. Radial velocities for 142 candidate stars plus Gaia DR2 proper motions isolate high-confidence members and fix the cluster's systemic velocity. Photometry of those members yields revised age, reddening and distance, while high-resolution spectra of six radial-velocity members supply abundances for 23 elements. The resulting parameters place the cluster at roughly 7 kpc Galactocentric distance and show super-solar metallicity together with mild alpha and neutron-capture enhancements that match patterns seen in other inner-disc clusters.

Core claim

Using Gaia-ESO Survey data, Pismis 18 has age 700+40−50 Myr, E(B−V) = 0.562+0.012−0.026 mag, de-reddened distance modulus DM0 = 11.96+0.10−0.24 mag, median [Fe/H] = +0.23 ± 0.05 dex, [α/Fe] = 0.07 ± 0.13, and slight s- and r-process enhancement, confirming its inner-disc location at about 7 kpc from the Galactic centre.

What carries the argument

Radial-velocity membership study of 142 stars on the upper main sequence and red clump, combined with Gaia DR2 proper motions to select high-confidence members, followed by detailed abundance analysis of six UVES high-resolution spectra.

Load-bearing premise

The six stars observed at high resolution are chemically representative of the entire cluster and radial-velocity plus proper-motion cuts cleanly exclude field-star contamination.

What would settle it

Abundance measurements of additional proper-motion and radial-velocity selected members that differ by more than 0.1 dex in [Fe/H] or [α/Fe] from the reported medians would show the six-star sample is not representative.

Figures

Figures reproduced from arXiv: 1906.09828 by A. Bayo, A. Bragaglia, A. C. Lanzafame, A. Dapergolas, A. Drazdauskas, A. Gonneau, A. R. Casey, A. Vallenari, C. C. Worley, D. Hatzidimitriou, E. Delgado-Mena, E.D. Friel, E. Flaccomio, E. Franciosini, E. J. Alfaro, E. Pancino, E. Tognelli, E. V. Held, F. Damiani, G. Carraro, G. Gilmore, G. Tautvaisiene, J. Lewis, K. Gazeas, L. Bravi, L. Magrini, L. Monaco, L. Morbidelli, M. Bergemann, M. T. Costado, P. Jofre', R. Minkeviciute, R. Smiljanic, R. Sordo, S. Feltzing, S. Randich, S. Zaggia.

Figure 1
Figure 1. Figure 1: Left panel: VPHAS+ colour magnitude diagram of Pismis 18 over the entire field of view of FLAMES, marked as small grey filled circles. The targets observed with UVES are marked with red filled squares, while targets observed with GIRAFFE are marked with blue filled circles. High confidence cluster members are indicated with black crosses and the possible binary star with a black filled triangle; Right pane… view at source ↗
Figure 2
Figure 2. Figure 2: Proper motions of stars in our Pismis 18 spectroscopic sample in common with the Gaia DR2. Red dots represent the probable members according to the analysis of Cantat-Gaudin et al. (2018a), with proper motion errors in the Gaia DR2. A blue square marks a suspect binary star observed with UVES (CNAME 13365001-6205376, see discussion in the text). Only a limited range of proper motions is shown here to highl… view at source ↗
Figure 3
Figure 3. Figure 3: Distribution of radial velocities of all 142 observed stars (in grey). The distribution of the GIRAFFE radial velocity members is shown in blue and that of the UVES radial velocity members in red. The patterned bars show the distribution of radial velocities of Galactic stars in the direction of Pismis 18 according to the Besançon star count model for the Galaxy. For the normalization of this curve see tex… view at source ↗
Figure 4
Figure 4. Figure 4: Distribution of stars with assigned cluster membership, on the RA-Dec plane. With small grey filled circles we indicate all observed stars, with large blue filled circles the GIRAFFE radial velocity mem￾bers, with red filled squares the UVES radial velocity members, with a green filled triangle the possible binary star discussed in the text and with a black cross we indicate the location of the cluster cen… view at source ↗
Figure 5
Figure 5. Figure 5: Comparison between the Pisa best isochrone (corresponding to τ = 700+40 −50 Myr, E(B − V) = 0.562+0.012 −0.026 mag and DM0 = 11.96+0.10 −0.24 mag) and the observations in several photometric bands, namely BV (Piatti et al. 1998), JHKs (2MASS), GBpGRpG (Gaia DR2), and gri (VPHAS+). The uncertainties in magnitude and colour are too small to show on the two right-most diagrams. No uncertainties were available… view at source ↗
Figure 8
Figure 8. Figure 8: Abundance ratios as a function of galactocentric distance (RGC) for Pismis 18 (green star) compared with the results of Magrini et al. (2017) for both clusters (grey circles –the youngest clusters, age<2 Gyr, and in blue the oldest ones) and models (red–present time– and blue – 5 Gyr ago – curves). models built on an inside-out scenario (see for example [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
Figure 7
Figure 7. Figure 7: Abundance of Li as a function of temperature (filled symbols with error bars indicate specific measured values, while empty triangles indicate upper limits. of [α/Fe]=0.07±0.13. The individual abundances and abundance ratios are provided in [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Distribution of [X/Fe] ratios as a function of [Fe/H] for 23 species includ￾ing light (cyan), α (green), Fe-peak (ma￾genta) and n-capture (red for s-process and blue for r-process) elements. The grey points correspond to field MW stars in GES (see text; it is noted that no Y measurements are available for them). in M18 are related to the more strict selection of stars included to compute the average value … view at source ↗
Figure 10
Figure 10. Figure 10: Histogram of the ratio between average error and standard dis￾persion for all species (Li excluded) measured for the high probability members of Pismis 18. has been performed for the GES cluster sample yet, we have not found any compelling indication of unexplained intrinsic spreads (see e.g. Cantat-Gaudin et al. 2014; Donati et al. 2014; Overbeek Article number, page 12 of 14 [PITH_FULL_IMAGE:figures/fu… view at source ↗
read the original abstract

Pismis 18 is a moderately populated, intermediate-age open cluster located within the solar circle at a Galactocentric distance of about 7 kpc. Few open clusters have been studied in detail in the inner disc region before the Gaia-ESO Survey. New data from the Gaia-ESO Survey allowed us to conduct an extended radial velocity membership study as well as spectroscopic metallicity and detailed chemical abundance measurements for this cluster. Gaia-ESO Survey data for 142 potential members, lying on the upper MS and on the red clump, yielded radial velocity measurements, which, together with proper motion measurements from the Gaia DR2, were used to determine the systemic velocity of the cluster and membership of individual stars. Photometry from Gaia DR2 was used to re-determine cluster parameters based on high confidence member stars only. Cluster abundance measurements of six radial-velocity member stars with UVES high-resolution spectroscopy are presented for 23 elements. According to the new estimates, based on high confidence members, Pismis 18 has an age of $700^{+40}_{-50}$ Myr, interstellar reddening of E(B-V) = $0.562^{+0.012}_{-0.026}$ mag and a de-reddened distance modulus of $DM_0 = 11.96^{+0.10}_{-0.24}$ mag. The median metallicity of the cluster (using the six UVES stars) is [Fe/H] = $+0.23 \pm 0.05$ dex, with [$\alpha$/Fe]= $0.07 \pm 0.13$ and a slight enhancement of s- and r- neutron-capture elements. With the present work, we fully characterized the open cluster Pismis 18, confirming its present location in the inner disc. We estimated a younger age than the previous literature values and gave, for the first time, its metallicity and its detailed abundances. Its [$\alpha$/Fe] and [s-process/Fe], both slightly super-solar, are in agreement with other inner-disc open clusters observed by the Gaia-ESO survey. [abridged]

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

1 major / 0 minor

Summary. The manuscript presents a characterization of the intermediate-age open cluster Pismis 18 based on Gaia-ESO Survey data. It performs a radial velocity membership study on 142 potential members combined with Gaia DR2 proper motions to identify high-confidence members, uses Gaia DR2 photometry to determine the cluster's age, reddening, and distance modulus via isochrone fitting, and reports detailed chemical abundances for 23 elements from six UVES spectra of radial-velocity members, yielding a median [Fe/H] = +0.23 ± 0.05 dex and confirming the cluster's location in the inner Galactic disc.

Significance. This work contributes to the growing sample of inner-disc open clusters with precise abundances from the Gaia-ESO Survey. The derived parameters, including a younger age than previous estimates and slightly super-solar [α/Fe] and s-process elements, align with expectations for the inner disc and provide a useful comparison point for Galactic chemical evolution models. The integration of spectroscopic radial velocities with astrometric proper motions for membership is a methodological strength.

major comments (1)
  1. [Membership determination] The description of the membership analysis does not include the measured velocity dispersion of the cluster, the specific outlier rejection criteria, or an estimate of the field star contamination fraction among the 142 candidates. Since the chemical abundances and cluster parameters rely on the selected high-confidence members, these details are necessary to assess the robustness of the results.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the positive assessment of our work and the recommendation of minor revision. We address the single major comment below.

read point-by-point responses

  1. Referee: [Membership determination] The description of the membership analysis does not include the measured velocity dispersion of the cluster, the specific outlier rejection criteria, or an estimate of the field star contamination fraction among the 142 candidates. Since the chemical abundances and cluster parameters rely on the selected high-confidence members, these details are necessary to assess the robustness of the results.

    Authors: We agree that these details improve the clarity and robustness assessment of the membership selection. In the revised manuscript we will add the measured radial-velocity dispersion of the high-confidence members, explicitly state the outlier rejection thresholds applied to the 142 candidates (including any sigma-clipping or combined RV+PM criteria), and provide a quantitative estimate of the field-star contamination fraction remaining after the joint selection. These additions will be placed in the membership section and will directly support the reliability of the six UVES stars used for abundances and the high-confidence sample used for the isochrone fit. revision: yes

Circularity Check

0 steps flagged

No significant circularity; parameters derived directly from survey data

full rationale

The paper reports direct observational measurements: radial velocities from Gaia-ESO spectra for 142 candidates, combined with Gaia DR2 proper motions for membership, photometry for age/reddening/distance, and median abundances from six UVES spectra. No equations, fitted parameters renamed as predictions, or self-citation chains reduce any claim to its own inputs by construction. The derivation chain consists of standard data reduction and median statistics on independent measurements, with no self-definitional loops or ansatz smuggling. This is a typical observational cluster characterization paper whose central results are falsifiable against external data.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central results rest on standard assumptions of stellar isochrone fitting, radial-velocity membership, and the representativeness of six high-resolution spectra. No new free parameters or invented entities are introduced beyond those implicit in the survey analysis.

axioms (2)
  • domain assumption The six UVES stars are chemically representative of the cluster and unaffected by atomic diffusion or other internal processes that could alter surface abundances.
    Invoked when reporting median [Fe/H] and abundance ratios from the six stars as cluster values.
  • domain assumption Gaia DR2 proper motions and Gaia-ESO radial velocities cleanly separate cluster members from field stars at this location.
    Used to select the high-confidence members for parameter determination.

pith-pipeline@v0.9.0 · 6145 in / 1535 out tokens · 20328 ms · 2026-05-25T16:56:20.739841+00:00 · methodology

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