# Barium abundances in Cepheids

S.M. Andrievsky, J. Lépine, S. Korotin, R. Luck, V. Kovtyukh, W. Maciel

► To cite this version:

S.M. Andrievsky, J. Lépine, S. Korotin, R. Luck, V. Kovtyukh, et al.. Barium abundances in Cepheids. Monthly Notices of the Royal Astronomical Society, 2013, 428 (4), pp.3252-3261. 10.1093/mn-ras/sts270. hal-02612462

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# Barium abundances in Cepheids

S. M. Andrievsky,<fnref n="1" />,<fnref n="2" />,<fnref n="3" />* J. R. D. Lépine,<fnref n="1" /> S. A. Korotin,<fnref n="2" /> R. E. Luck,<fnref n="4" />
V. V. Kovtyukh<fnref n="2" /> and W. J. Maciel<fnref n="1" />

Accepted 2012 October 22. Received 2012 October 21; in original form 2012 August 28

## ABSTRACT

We derived the barium atmospheric abundances for a large sample of Cepheids, comprising 270 stars. The sample covers a large range of Galactocentric distances, from about 4 to 15 kpc, so it is appropriate to investigate the existence of radial barium abundance gradients in the Galactic disc. In fact, this is the first time that such a comprehensive analysis of the distribution of barium abundances in the Galactic disc has been carried out. As a result, we conclude that the Ba abundance distribution can be characterized by a zero gradient. This result is compared with derived gradients for other elements, and some reasons are briefly discussed for the independence of the barium abundances from Galactocentric distances.

**Key words:** stars: abundances – stars: variables: Cepheids – Galaxy: disc – Galaxy: evolution.

## 1 INTRODUCTION

In our extensive studies of the elemental distributions in the galac-
tic disc based on studies of Cepheid spectra (Andrievsky et al.
2002a,b,c, 2004; Luck et al. 2003; Luck, Kovtyukh & Andrievsky
2006; Luck & Lambert 2011; Luck et al. 2011), we have avoided
the determination of barium abundances. Although three Ba II lines
are available in the observed spectral domain, all are very strong
in Cepheid spectra with equivalent widths ranging from 200 to
600 mA. A simple local thermodynamic equilibrium (LTE) analy-
sis of such strong lines could produce incorrect abundance results
due to non-local thermodynamic equilibrium (NLTE) effects in the
atomic populations, and more importantly, due to strong saturation
effects making the analysis particularly sensitive to the microturbu-
lence.

The great majority of studies devoted to the barium abundance
in the galactic disc are based on the LTE approximation, and most
focus on nearby stars. Recently, a more sophisticated method, i.e.
NLTE, has been applied to the galactic disc stars, but as in the case
of older studies, only for those stars situated near the solar region
(Korotin et al. 2010).

The present-day barium abundance distribution in galactic disc
results from a variety of processes. The different processes in-
clude nucleosynthesis in asymptotic giant branch stars, Type II
supernovae, as well as dynamical processes involving radial gas
flows that lead to large-scale mixing of the interstellar medium.

The barium abundance distribution in the galactic disc [as well as
distributions of the heavy r-/($r+s$)-process elements like La, Ce and
Nd] is necessary to constrain models of the Milky Way chemical
evolution. Existing data on the barium content in objects situated at
large distances from the Sun are scarce, and apparently insufficient
to check the validity of model predictions (see e.g. fig. 9 in Cescutti
et al. 2007).

To investigate the barium abundances in distant stars we use the
sample of Cepheids investigated in our previous works: Andrievsky
et al. (2002a,b,c) and Luck et al. (2003, 2006, 2011). In those papers,
one can find information about the atmospheric parameters of the
programme stars and their spectra. For some stars, we have used the
multiphase observations described in Luck & Andrievsky (2004),
Kovtyukh et al. (2005), Andrievsky, Luck & Kovtyukh (2005) and
Luck et al. (2008). The reasons for studying these stars are many.
These stars are luminous, allowing them to serve as probes of distant
regions. The methods of the abundance analysis of the stars of F–G
spectral classes are well established; and finally, Cepheids are rather
young stars, and thus they reflect the present-day characteristics of
the galactic disc even though they had time to migrate.

## 2 BARIUM ATOMIC MODEL AND METHOD
OF ABUNDANCE DETERMINATION

Andrievsky et al. (2009) describe our model of barium atom in de-
tail. Briefly, it consists of 31 levels of Ba I, 73 levels of Ba II and
the ground level of Ba III. 91 bound–bound transitions between the
first 28 levels of Ba II with *n* < 12 and *l* < 5 are computed in detail.
The remaining levels are used for particle number conservation.

<footnote n="1">¹Instituto de Astronomia, Geofísica e Ciências Atmosféricas da Universidade de São Paulo, Cidade Universitária, CEP 05508-900 São Paulo, SP, Brazil</footnote>

<footnote n="2">²Department of Astronomy and Astronomical Observatory, Odessa National University, and Isaac Newton Institute of Chile Odessa branch Shevchenko Park, 65014 Odessa, Ukraine</footnote>

<footnote n="3">³GEPI, Observatoire de Paris-Meudon, F-92125 Meudon Cedex, France</footnote>

<footnote n="4">⁴Department of Astronomy, Case Western Reserve University, Cleveland, OH 44106, USA</footnote>

<footnote>*E-mail: scan@deneb1.odessa.ua</footnote>
For two levels, 5d²D and 6p²P₀, fine structure was taken into account. Oscillator strengths, photoionization cross-sections, collisional rates, broadening parameters and test calculations are found in the above-mentioned paper.

Atomic level populations were determined using the MULTI code of Carlsson (1986) with modifications as given in Korotin, Andrievsky & Luck (1999). MULTI calculates the line profile for each line considered in detail. The line profile computed assuming either LTE or NLTE depends upon many parameters: the effective temperature of the model, the surface gravity, the microturbulent velocity and the line damping as well as the populations in the appropriate levels. Departure coefficients, defined as the ratio of NLTE to LTE level populations, are also computed by MULTI, and they depend only on the model atom and model stellar atmosphere. Specifically, they are independent of the total abundance, the damping and the microturbulence.

Barium atom has seven isotopes. Isotopic shifts are very small (about 2 mÅ). For two odd isotopes ¹³⁵Ba and ¹³⁷Ba the hyperfine structure is quite important, and this produces additional complication in the line structure (several line components of the odd isotopes shifted relatively to the lines of even isotopes). This produces the shifts between the line components formed by odd and even isotopes. It is known that the most pronounced effect is seen in the Ba II line 4554.03 Å (out of our spectral region).

In principle, this effect has some influence on the profile of the 6496.91-Å line. The components of the odd isotopes constitute two compact groups that are shifted by -4 and +9 mÅ relative to the components of the even isotopes. For the rest of our two lines the corresponding shifts are too small to affect their line profiles.

As it was showed in the work of Mashonkina, Gehren & Bikmaev (1999) for the adequate barium line modelling, it is sufficient to use the three-component model suggested by Rutten (1978). For the calculations of the Ba line profiles in the spectra of young stars one can use the even-to-odd abundance ratio of 82:18 (Cameron 1982).

Since the equivalent widths of our programme barium lines are larger than 250 mÅ, we can state that HFS does not have in this case any significant influence on the line profiles.

Three Ba II lines are available in our program spectra for the abundance analysis: 5853.68, 6141.71 and 6496.91 Å. The barium abundance was derived by fitting calculated profiles to the observed profiles. All of the available barium lines are blended with lines of other elements (iron lines, in particular). The blending effect is more significant for the 6141.71- and 6496.91-Å lines (for 5853.68-Å line, this effect is negligible). Proper comparison of the observed and computed profiles thus requires a multi-element synthesis. For this process, we fold the NLTE (MULTI) calculations into the LTE synthetic spectrum code SYNTHV (Tsymbal 1996). With these programs, we calculated synthetic spectra for each Ba II line region taking into account all the lines in each region listed in the VALD<fnref n="1" /> data base. For the barium lines, the corresponding departure coefficients (the so-called b-factors: $b = n_i/n_i^*$ – the ratio of NLTE-to-LTE level populations) are input to SYNTHV, where they are used in the calculation of the line source function and barium line profiles. Figs 1 and 2 show the quality of fit achieved by this process.

In Fig. 3 we show how blending lines together with Ba II lines form the resulting profile of 6141.71- and 6496.91-Å lines (an example for Cepheid DL Cas). We can see that the contribution from the blending lines (Fe I 6141.732 Å for 6141.71 Å, and Fe I 6496.467 Å for 6496.91 Å) is not extremely large (we have also to note that

<figure><img src="image_3.png" /><figcaption>**Figure 1.** Profile fitting of the Ba II line in the DL Cas spectrum. Observed spectrum – dots; pure NLTE MULTI profile – dotted line; and combined synthetic spectrum – smooth line.</figcaption></figure>

<figure><img src="image_4.png" /><figcaption>**Figure 2.** The same as Fig. 1, but for DT Cyg.</figcaption></figure>

<figure><img src="image_5.png" /><figcaption>**Figure 3.** Ba II lines, blending lines and resulting profiles in DL Cas spectrum. Dots – observed spectrum; smooth line – combined calculated profile; dotted line – pure Ba II line profile; and dashed line – blending spectral line.</figcaption></figure>

there are also two weak lines in the wings of 6141.71-Å line – Fe II 6141.033 Å and Si I 6142.483 Å). If spectral synthesis is properly done, then this contribution is adequately accounted. For blending lines we used the reliable atomic data from the VALD data base (see the reference above), while abundances of elements producing those lines are taken from the series of our previous papers, i.e. they were fixed. In particular, in this case the VALD data are based on the original data from Fuhr & Wiese (2006). In fact, we always relied more on the barium abundance derived from 5853.68-Å line. In a few cases, this line was not available in our spectra, or its profile was spoiled due to some reasons. In those cases, only the rest two lines were used in abundance analysis. As a rule, the barium abundances derived from 5853.68-Å line and from the other two lines agree well between themselves. If there was a significant deviation of barium abundance from one of the 6141.71- and 6496.91-Å lines, then the corresponding line was not considered in the final statistics.

Stellar parameters for all stars were taken from our previous works (for a compendium, see Luck et al. 2011). These parameters were determined from a combined LTE excitation and ionization balance analysis. In particular, the microturbulent velocity depends solely on Fe II lines. In our syntheses, we used previously published (see Luck et al. 2011) abundances of elements whose lines were treated in SYNTHV, i.e. blending lines and lines situated in the vicinity of barium lines.

In some cases, our programme Cepheids exhibit asymmetric line profiles due to dynamic phenomena associated with pulsation. In such cases, our profile fitting cannot be applied, and thus spectra with greatly asymmetric lines were excluded from the analysis. A few exceptions were allowed in which we used the 5853.68-Å line alone to derive NLTE barium abundance. This line is not heavily blended, and its equivalent width is measurable by direct integration.

<footnote n="1">¹ http://ams.astro.univie.ac.at/vald/</footnote>
## 3 RESULTS OF THE NLTE BARIUM ABUNDANCE DETERMINATION AND SOURCES OF ABUNDANCE ERRORS

Table 3 contains the list of programme stars, phases for the selected spectra, adopted atmosphere parameters, galactocentric distances (based on $R_{\text{Sun}} = 7.9$ kpc), NLTE barium abundances, $\sigma$ values and the number of analysed barium line profiles. In some cases, adjacent echelle orders contain the same barium lines, and each profile was analysed independently. For some stars, we have multiphase observations; therefore, the number of analysed barium line profiles is the number of available spectra multiplied by the number of available barium lines in each spectrum (this number is listed in Table 3).

We have investigated the parameter sensitivity of the derived Ba abundance. Our initial parameters were $T_{\text{eff}} = 6000$ K, $\log g = 2.0$ and $V_t = 4.0$ km s$^{-1}$, with [Fe/H] = 0. We then generated lines assuming $\log \epsilon(\text{Ba}) = 2.17$ and matched them using parameter sets that vary one parameter at a time. An increase of 150 K in effective temperature changes the Ba abundance by +0.1 dex, a 0.2-dex increase in $\log g$ gives a change of +0.06 and a microturbulent velocity increase and decrease of 0.5 km s$^{-1}$ yield a decrease and increase in abundance of -0.23 and +0.28 dex, respectively. The formal parameter-related uncertainty is thus about $\pm 0.3$ dex. However, note that at lower microturbulent velocities the dependence of the barium abundance on $V_t$ is much stronger.

In Figs 4–8, we show the derived barium abundances as a function of the pulsation phase, effective temperature, surface gravity and microturbulent velocity. As one can see, there is no significant dependence on phase $\phi$ (for three stars where we used multiphase observations, Fig. 5 shows such a dependence), $T_{\text{eff}}$ or $\log g$, but there is quite a clear variation with microturbulent velocity (Fig. 8). This relation is quite disconcerting as it means that we are dealing with strong saturation in the lines, and hence the dramatic dependence of abundance on assumed microturbulent velocity.

<figure><img src="image_6.png" /><figcaption>**Figure 4.** Barium abundance versus phase for programme stars spectra. Combined plot.</figcaption></figure>

<figure><img src="image_7.png" /><figcaption>**Figure 5.** Barium abundance versus phase for programme stars spectra with multiphase observations.</figcaption></figure>

<figure><img src="image_8.png" /><figcaption>**Figure 6.** Barium abundance versus effective temperature.</figcaption></figure>

<figure><img src="image_9.png" /><figcaption>**Figure 7.** Same as Fig. 6, but for surface gravity.</figcaption></figure>

<figure><img src="image_10.png" /><figcaption>**Figure 8.** Same as Fig. 6, but for microturbulent velocity.</figcaption></figure>

To illustrate this, we give in Table 1 the dependence of the Ba abundance on microturbulent velocity for UX Car.

In the case of UX Car (Table 1), the Fe II-derived $V_t$ (4.7 km s$^{-1}$) yields excellent agreement between the three Ba II lines. This is not surprising as this $V_t$ is in the region of $V_t$ versus Ba abundance (see Fig. 8) where there is no obvious dependence between abundance and $V_t$. This suggests that it might be possible to find the proper $V_t$ value for Ba II by forcing the three lines to yield the same Ba abundance using $V_t$ as a free parameter. The result of this approach for IR Cep is shown in Table 2. The idea behind this attempt is that each Ba II feature has a constant contribution from Ba that is defined by the best-fitting synthesis. One then uses the best-fitting

<table><caption>**Table 1.** NLTE abundances for UX Car.</caption><thead><tr><th></th><th colspan="4">V<sub>t</sub> (km s<sup>-1</sup>)</th></tr></thead><tbody><tr><td>Line</td><td>3.5</td><td>4.0</td><td>4.7</td><td>5.3</td></tr><tr><td>5853</td><td>2.58</td><td>2.37</td><td>2.19</td><td>2.09</td></tr><tr><td>6141</td><td>2.84</td><td>2.53</td><td>2.19</td><td>1.99</td></tr><tr><td>6496</td><td>2.81</td><td>2.50</td><td>2.19</td><td>2.01</td></tr></tbody></table>
<table><caption>**Table 2.** Abundances for IR Cep.</caption><thead><tr><th rowspan="2">Line</th><th rowspan="2">EW<br>(mÅ)</th><th colspan="7">V<sub>t</sub> (km s<sup>-1</sup>)</th></tr><tr><th>2.0</th><th>2.5</th><th>3.0</th><th>3.5</th><th>4.0</th><th>4.5</th><th>5.0</th><th>6.0</th><th>7.0</th></tr></thead><tbody><tr><td>LTE</td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td><td></td></tr><tr><td>5853</td><td>196</td><td>3.23</td><td>2.81</td><td>2.46</td><td>2.18</td><td>1.97</td><td>1.83</td><td>1.73</td><td>1.58</td><td>1.50</td></tr><tr><td>6141</td><td>270</td><td>3.17</td><td>2.89</td><td>2.54</td><td>2.22</td><td>1.94</td><td>1.72</td><td>1.53</td><td>1.26</td><td>1.09</td></tr><tr><td>6496</td><td>280</td><td>3.30</td><td>2.96</td><td>2.59</td><td>2.29</td><td>2.04</td><td>1.83</td><td>1.67</td><td>1.43</td><td>1.28</td></tr><tr><td>NLTE</td><td></td><td></td><td>2.75</td><td></td><td>2.08</td><td></td><td></td><td></td><td></td><td></td></tr></tbody></table>

abundance to the profile to calculate the unblended Ba equivalent width. One then matches the equivalent width for each selected microturbulent velocity. In this test, we have matched the equivalent widths using an LTE approach, as the primary problem we are trying to overcome now is not level populations but saturation effects. While there is a range of equivalent widths in the Ba II lines, all lines are saturated, and it is not possible to obtain a clear-cut indication of a better value to use for $V_t$. In this case, the Fe II $V_t$ is 2.9 km s$^{-1}$, which gives a spread of about 0.13 dex between the Ba II lines. The spread at 4.0 km s$^{-1}$ is marginally better at 0.10 dex, but given the overall uncertainties does not significantly improve the confidence level of the abundance determination. It is also of interest that above about 6 km s$^{-1}$, the lines become only weakly dependent on $V_t$, i.e. they are desaturated and behave as weak lines. Also included in Table 2 is the best-fitting Ba abundance for the NLTE analysis. The NLTE corrections for these lines are not especially large, averaging around -0.1 dex.

The origin of the dependence of the Ba abundance of $V_t$ as shown in Fig. 8 could arise in a velocity stratification in the atmosphere of Cepheids. The solar atmosphere exhibits an increasing microturbulent velocity with height (Stodilka & Malynch 2006), and it would not be surprising if similar temperature but higher luminosity objects showed the same phenomenon. Quite strong barium lines have effective depth of formation high in the atmosphere, while weaker (on average) iron lines used for microturbulence determination must be formed deeper in the atmosphere at a lower $V_t$.

Since there is no straightforward method to account for the dependence seen in Fig. 8, we simply divide the barium abundance data into two parts based on the microturbulent velocity. From Fig. 8, one can estimate that the break in the (Ba/H)$-V_t$ relation roughly corresponds to $V_t = 3.8$ km s$^{-1}$.

## 4 THE BARIUM RADIAL ABUNDANCE DISTRIBUTION

Our primary interest in previous Cepheid abundance studies has been the distribution of the elements in the galactic disc, and the motivation for this study of Ba abundances is no exception. While there is uncertainty about the abundances themselves, we shall persevere and consider the abundance distribution found from our Ba data.

In Fig. 9 we show the radial barium abundance distribution in galactic disc as derived from the total sample of the stars and from the sample with $V_t > 3.8$ km s$^{-1}$ (the distances are given in Table 3). With the exception of a few deviant stars (such as EE Mon at $R_G = 15$ kpc), the barium abundance distribution looks essentially flat. The mean value for the total sample is $\langle(Ba/H)\rangle = 2.29 \pm 0.15$. If we use barium abundance data for the part of the sample with $V_t > 3.8$ km s$^{-1}$, then the mean value is $\langle(Ba/H)\rangle = 2.25 \pm 0.13$. Both

<figure><img src="image_11.png" /><figcaption>**Figure 9.** (Ba/H) data versus Galactocentric distance. Upper plot – the total sample of stars; lower plot – part of the sample with $V_t > 3.8$ km s$^{-1}$.</figcaption></figure>

values are the same within the estimated errors. What is important to note is that in both cases we have almost zero gradient.

## 5 DISCUSSION

As a first approach to the Ba gradient, a linear regression was fitted to the data of Fig. 9, with the formal result being (Ba/H) = +0.0066 $R_G + 2.2345$ (the total sample) and (Ba/H) = +0.0003 $R_G + 2.2456$ ($V_t > 3.8$ km s$^{-1}$). From this, we conclude the following.

(i) Barium abundances appear to be the same with quite a large scatter around the mean in the region spanning Galactocentric distances from 4 to 15 kpc.

(ii) The mean (Ba/H) value for the solar neighbourhood is near the solar barium abundance. The Cepheid mean values are 2.29 for the total sample and 2.25 for the stars with $V_t > 3.8$ km s$^{-1}$ versus a solar (NLTE) barium abundance of 2.17.

What could be the origin of a homogeneous distribution of barium in the galactic radius? Let us consider the iron distribution in the disc presented in Fig. 10 (data from Luck et al. 2011). This figure shows that the mean iron abundance in the range of galactocentric distances from 9 to 14 kpc is about 0.2 dex lower than in the solar
<table><caption>**Table 3.** Programme stars, their phase parameters and barium abundance.</caption><thead><tr><th>Star</th><th>Phase</th><th>T<sub>eff</sub> (K)</th><th>log g</th><th>V<sub>t</sub> (km s<sup>-1</sup>)</th><th>[Fe/H]</th><th>R<sub>G</sub> (kpc)</th><th>log ε(Ba)<sub>NLTE</sub></th><th>σ(Ba)</th><th>N lines</th></tr></thead><tbody><tr><td>AA Gem</td><td>0.625</td><td>5126</td><td>1.40</td><td>4.40</td><td>-0.24</td><td>11.550</td><td>2.32</td><td>0.18</td><td>2</td></tr><tr><td>AA Mon</td><td>0.106</td><td>6261</td><td>2.10</td><td>4.00</td><td>-0.21</td><td>11.364</td><td>2.17</td><td>0.12</td><td>3</td></tr><tr><td>AC Mon</td><td>0.081</td><td>6075</td><td>1.90</td><td>4.80</td><td>-0.22</td><td>10.121</td><td>2.27</td><td>0.12</td><td>3</td></tr><tr><td>AC Mon</td><td>0.919</td><td>6121</td><td>2.20</td><td>5.80</td><td>-0.07</td><td>10.121</td><td>2.27</td><td>0.12</td><td>3</td></tr><tr><td>AD Cru</td><td>0.030</td><td>6000</td><td>2.00</td><td>4.00</td><td>0.06</td><td>6.987</td><td>2.32</td><td>0.13</td><td>3</td></tr><tr><td>AD Gem</td><td>0.818</td><td>5784</td><td>2.15</td><td>4.30</td><td>-0.19</td><td>10.481</td><td>2.24</td><td>0.18</td><td>2</td></tr><tr><td>AE Tau</td><td>0.377</td><td>5981</td><td>2.30</td><td>4.00</td><td>-0.19</td><td>11.326</td><td>2.27</td><td>0.13</td><td>3</td></tr><tr><td>AE Vel</td><td>0.732</td><td>5460</td><td>1.70</td><td>4.50</td><td>0.05</td><td>7.983</td><td>2.25</td><td>0.20</td><td>3</td></tr><tr><td>AG Cru</td><td>0.039</td><td>6628</td><td>2.20</td><td>4.70</td><td>-0.13</td><td>7.346</td><td>1.95</td><td>0.13</td><td>3</td></tr><tr><td>AH Vel</td><td>0.383</td><td>6037</td><td>2.20</td><td>4.30</td><td>0.10</td><td>7.996</td><td>2.35</td><td>0.13</td><td>3</td></tr><tr><td>AO Aur</td><td>0.707</td><td>5459</td><td>1.70</td><td>3.60</td><td>-0.14</td><td>11.813</td><td>2.32</td><td>0.18</td><td>2</td></tr><tr><td>AP Pup</td><td>0.052</td><td>6233</td><td>2.10</td><td>4.20</td><td>0.06</td><td>8.189</td><td>2.34</td><td>0.13</td><td>3</td></tr><tr><td>AP Sgr</td><td>0.093</td><td>6328</td><td>2.02</td><td>3.46</td><td>0.10</td><td>7.101</td><td>2.41</td><td>0.15</td><td>6</td></tr><tr><td>AQ Car</td><td>0.998</td><td>5815</td><td>1.90</td><td>4.90</td><td>0.06</td><td>7.631</td><td>2.22</td><td>0.13</td><td>3</td></tr><tr><td>AQ Pup</td><td>0.756</td><td>4937</td><td>0.60</td><td>5.50</td><td>-0.14</td><td>9.487</td><td>2.12</td><td>0.13</td><td>3</td></tr><tr><td>AQ Pup</td><td>0.798</td><td>4958</td><td>0.60</td><td>5.70</td><td>-0.14</td><td>9.487</td><td>2.05</td><td>0.15</td><td>3</td></tr><tr><td>AS Per</td><td>0.580</td><td>5550</td><td>1.72</td><td>3.35</td><td>0.10</td><td>9.154</td><td>2.49</td><td>0.15</td><td>5</td></tr><tr><td>AT Pup</td><td>0.658</td><td>6455</td><td>2.10</td><td>5.00</td><td>-0.14</td><td>8.412</td><td>2.05</td><td>0.15</td><td>3</td></tr><tr><td>AV Cir</td><td>0.207</td><td>6169</td><td>2.10</td><td>3.30</td><td>0.10</td><td>7.516</td><td>2.30</td><td>0.13</td><td>3</td></tr><tr><td>AV Sgr</td><td>0.982</td><td>5875</td><td>1.75</td><td>4.90</td><td>0.34</td><td>5.475</td><td>2.13</td><td>0.15</td><td>3</td></tr><tr><td>AW Per</td><td>0.295</td><td>5989</td><td>1.90</td><td>3.60</td><td>0.00</td><td>8.622</td><td>2.30</td><td>0.13</td><td>5</td></tr><tr><td>AW Per</td><td>0.451</td><td>5836</td><td>2.00</td><td>3.70</td><td>0.00</td><td>8.622</td><td>2.30</td><td>0.13</td><td>6</td></tr><tr><td>AX Cir</td><td>0.119</td><td>5761</td><td>1.80</td><td>3.70</td><td>-0.05</td><td>7.530</td><td>2.16</td><td>0.13</td><td>3</td></tr><tr><td>AX Cir</td><td>0.745</td><td>5648</td><td>1.90</td><td>4.50</td><td>-0.07</td><td>7.530</td><td>2.20</td><td>0.12</td><td>3</td></tr><tr><td>AY Cen</td><td>0.999</td><td>5933</td><td>2.10</td><td>4.50</td><td>0.01</td><td>7.424</td><td>2.25</td><td>0.10</td><td>3</td></tr><tr><td>AZ Cen</td><td>0.947</td><td>6425</td><td>2.30</td><td>4.00</td><td>-0.05</td><td>7.413</td><td>2.21</td><td>0.10</td><td>3</td></tr><tr><td>BB Cen</td><td>0.183</td><td>6202</td><td>2.30</td><td>4.60</td><td>0.13</td><td>7.126</td><td>2.24</td><td>0.13</td><td>3</td></tr><tr><td>BB Gem</td><td>0.589</td><td>6035</td><td>2.40</td><td>3.00</td><td>-0.09</td><td>10.641</td><td>2.49</td><td>0.18</td><td>2</td></tr><tr><td>BB Her</td><td>0.259</td><td>5750</td><td>1.80</td><td>4.20</td><td>0.16</td><td>6.054</td><td>2.28</td><td>0.13</td><td>6</td></tr><tr><td>BB Her</td><td>0.389</td><td>5556</td><td>1.70</td><td>4.20</td><td>0.13</td><td>6.054</td><td>2.28</td><td>0.14</td><td>6</td></tr><tr><td>BB Sgr</td><td>0.878</td><td>5859</td><td>1.87</td><td>4.47</td><td>0.08</td><td>7.138</td><td>2.34</td><td>0.17</td><td>5</td></tr><tr><td>BC Pup</td><td>0.062</td><td>6695</td><td>2.00</td><td>3.50</td><td>-0.20</td><td>12.440</td><td>2.29</td><td>0.13</td><td>3</td></tr><tr><td>BC Pup</td><td>0.341</td><td>5879</td><td>1.90</td><td>3.30</td><td>-0.24</td><td>12.440</td><td>2.33</td><td>0.14</td><td>3</td></tr><tr><td>BD Cas</td><td>0.772</td><td>6200</td><td>2.50</td><td>5.00</td><td>-0.07</td><td>8.574</td><td>1.97</td><td>0.18</td><td>3</td></tr><tr><td>BD Cas</td><td>0.073</td><td>6075</td><td>2.30</td><td>4.50</td><td>-0.07</td><td>8.574</td><td>1.97</td><td>0.17</td><td>3</td></tr><tr><td>β Dor</td><td>0.128</td><td>5618</td><td>1.60</td><td>4.30</td><td>-0.01</td><td>7.896</td><td>2.10</td><td>0.13</td><td>6</td></tr><tr><td>BF Oph</td><td>0.033</td><td>6246</td><td>2.30</td><td>4.60</td><td>0.05</td><td>7.121</td><td>2.09</td><td>0.10</td><td>3</td></tr><tr><td>BF Oph</td><td></td><td>5541</td><td>1.90</td><td>4.10</td><td>-0.01</td><td>7.121</td><td>2.07</td><td>0.11</td><td>3</td></tr><tr><td>BG Cru</td><td>0.150</td><td>6309</td><td>2.30</td><td>4.20</td><td>0.06</td><td>7.694</td><td>2.25</td><td>0.16</td><td>3</td></tr><tr><td>BG Cru</td><td>0.188</td><td>6101</td><td>2.00</td><td>3.80</td><td>-0.02</td><td>7.694</td><td>2.25</td><td>0.15</td><td>6</td></tr><tr><td>BG Lac</td><td>0.147</td><td>5923</td><td>1.90</td><td>3.80</td><td>0.01</td><td>8.158</td><td>2.44</td><td>0.13</td><td>5</td></tr><tr><td>BG Lac</td><td>0.332</td><td>5625</td><td>1.85</td><td>3.60</td><td>0.02</td><td>8.158</td><td>2.44</td><td>0.13</td><td>6</td></tr><tr><td>BG Vel</td><td>0.849</td><td>5727</td><td>1.90</td><td>5.30</td><td>-0.01</td><td>7.922</td><td>2.18</td><td>0.13</td><td>3</td></tr><tr><td>BM Per</td><td>0.344</td><td>5313</td><td>0.54</td><td>3.40</td><td>0.10</td><td>10.851</td><td>2.64</td><td>0.18</td><td>5</td></tr><tr><td>BN Pup</td><td>0.396</td><td>5105</td><td>1.00</td><td>3.50</td><td>0.01</td><td>9.920</td><td>2.40</td><td>0.15</td><td>3</td></tr><tr><td>BP Cir</td><td>0.033</td><td>6533</td><td>2.40</td><td>3.70</td><td>-0.06</td><td>7.431</td><td>1.75</td><td>0.15</td><td>3</td></tr><tr><td>CD Cyg</td><td>0.376</td><td>5211</td><td>1.00</td><td>3.50</td><td>0.10</td><td>7.474</td><td>2.40</td><td>0.13</td><td>6</td></tr><tr><td>CD Cyg</td><td>0.434</td><td>5108</td><td>1.10</td><td>4.00</td><td>0.15</td><td>7.474</td><td>2.37</td><td>0.14</td><td>6</td></tr><tr><td>CD Cyg</td><td>0.519</td><td>4979</td><td>1.00</td><td>4.00</td><td>0.08</td><td>7.474</td><td>2.37</td><td>0.13</td><td>6</td></tr><tr><td>CE Cas A</td><td>0.732</td><td>5817</td><td>1.73</td><td>3.81</td><td>0.18</td><td>9.549</td><td>2.30</td><td>0.20</td><td>5</td></tr><tr><td>CE Pup</td><td>0.804</td><td>5846</td><td>1.30</td><td>5.80</td><td>-0.04</td><td>14.739</td><td>2.24</td><td>0.13</td><td>3</td></tr><tr><td>CF Cas</td><td>0.584</td><td>5454</td><td>1.70</td><td>4.30</td><td>0.01</td><td>9.702</td><td>2.40</td><td>0.15</td><td>6</td></tr><tr><td>CF Cas</td><td>0.980</td><td>6115</td><td>2.00</td><td>4.00</td><td>-0.03</td><td>9.702</td><td>2.44</td><td>0.16</td><td>6</td></tr><tr><td>CF Cas</td><td>0.238</td><td>5704</td><td>1.90</td><td>3.70</td><td>0.02</td><td>9.702</td><td>2.40</td><td>0.15</td><td>6</td></tr><tr><td>CH Cas</td><td>0.108</td><td>6319</td><td>1.80</td><td>5.50</td><td>-0.08</td><td>9.601</td><td>2.43</td><td>0.17</td><td>5</td></tr><tr><td>CN Car</td><td>0.066</td><td>6331</td><td>2.20</td><td>4.30</td><td>0.06</td><td>7.802</td><td>2.22</td><td>0.13</td><td>3</td></tr><tr><td>CP Cep</td><td>0.243</td><td>5150</td><td>1.30</td><td>4.10</td><td>-0.14</td><td>9.600</td><td>2.35</td><td>0.17</td><td>3</td></tr><tr><td>CR Cep</td><td>0.634</td><td>5443</td><td>1.33</td><td>4.02</td><td>-0.06</td><td>8.442</td><td>2.39</td><td>0.15</td><td>6</td></tr><tr><td>CS Ori</td><td>0.679</td><td>6539</td><td>2.50</td><td>3.60</td><td>-0.26</td><td>11.738</td><td>2.35</td><td>0.15</td><td>3</td></tr><tr><td>CU Mon</td><td>0.655</td><td>5677</td><td>1.90</td><td>4.50</td><td>-0.25</td><td>14.451</td><td>2.20</td><td>0.15</td><td>3</td></tr><tr><td>CV Mon</td><td>0.178</td><td>5897</td><td>2.00</td><td>4.10</td><td>-0.03</td><td>9.461</td><td>2.00</td><td>0.15</td><td>3</td></tr><tr><td>CX Vel</td><td>0.003</td><td>6251</td><td>2.20</td><td>5.30</td><td>0.06</td><td>8.360</td><td>2.07</td><td>0.13</td><td>3</td></tr><tr><td>CY Car</td><td>0.095</td><td>6042</td><td>2.20</td><td>4.00</td><td>0.10</td><td>7.471</td><td>2.32</td><td>0.13</td><td>3</td></tr><tr><td>CY Cas</td><td>0.391</td><td>5369</td><td>0.85</td><td>3.45</td><td>0.06</td><td>10.062</td><td>2.27</td><td>0.18</td><td>5</td></tr></tbody></table>
<table><caption>Table 3 – continued</caption><thead><tr><th>Star</th><th>Phase</th><th>T<sub>eff</sub> (K)</th><th>log g</th><th>V<sub>t</sub> (km s<sup>-1</sup>)</th><th>[Fe/H]</th><th>R<sub>G</sub> (kpc)</th><th>log ϵ (Ba)<sub>NLTE</sub></th><th>σ(Ba)</th><th>N lines</th></tr></thead><tbody><tr><td>DD Cas</td><td>0.039</td><td>5901</td><td>1.80</td><td>4.50</td><td>0.04</td><td>9.602</td><td>2.35</td><td>0.18</td><td>5</td></tr><tr><td>DF Cas</td><td>0.401</td><td>5644</td><td>2.20</td><td>4.65</td><td>0.13</td><td>9.718</td><td>2.19</td><td>0.18</td><td>3</td></tr><tr><td>DK Vel</td><td>0.009</td><td>6448</td><td>2.20</td><td>3.70</td><td>-0.02</td><td>8.126</td><td>2.23</td><td>0.13</td><td>3</td></tr><tr><td>DL Cas</td><td>0.105</td><td>5860</td><td>1.70</td><td>4.70</td><td>-0.01</td><td>8.846</td><td>2.15</td><td>0.13</td><td>6</td></tr><tr><td>DL Cas</td><td>0.229</td><td>5786</td><td>1.70</td><td>4.20</td><td>-0.01</td><td>8.846</td><td>2.19</td><td>0.13</td><td>6</td></tr><tr><td>DL Cas</td><td>0.473</td><td>5438</td><td>1.40</td><td>4.00</td><td>-0.01</td><td>8.846</td><td>2.15</td><td>0.14</td><td>6</td></tr><tr><td>DR Vel</td><td>0.165</td><td>5482</td><td>1.50</td><td>3.80</td><td>0.08</td><td>8.036</td><td>2.40</td><td>0.13</td><td>3</td></tr><tr><td>DT Cyg</td><td>0.651</td><td>6406</td><td>2.60</td><td>3.70</td><td>0.16</td><td>7.805</td><td>2.37</td><td>0.13</td><td>6</td></tr><tr><td>DT Cyg</td><td>0.705</td><td>6286</td><td>2.35</td><td>3.10</td><td>0.10</td><td>7.805</td><td>2.45</td><td>0.13</td><td>6</td></tr><tr><td>DT Cyg</td><td>0.769</td><td>6339</td><td>2.45</td><td>3.40</td><td>0.13</td><td>7.805</td><td>2.40</td><td>0.13</td><td>6</td></tr><tr><td>DX Gem</td><td>0.353</td><td>6096</td><td>1.90</td><td>2.80</td><td>-0.02</td><td>10.755</td><td>2.69</td><td>0.20</td><td>2</td></tr><tr><td>DY Car</td><td>0.956</td><td>6533</td><td>2.30</td><td>5.30</td><td>-0.07</td><td>7.686</td><td>2.00</td><td>0.13</td><td>3</td></tr><tr><td>EE Mon</td><td>0.209</td><td>6134</td><td>1.80</td><td>4.50</td><td>-0.51</td><td>15.018</td><td>1.60</td><td>0.18</td><td>3</td></tr><tr><td>EK Mon</td><td>0.918</td><td>6001</td><td>2.00</td><td>4.50</td><td>-0.10</td><td>10.191</td><td>2.10</td><td>0.20</td><td>3</td></tr><tr><td>ER Car</td><td>0.872</td><td>5874</td><td>2.10</td><td>6.00</td><td>0.03</td><td>7.597</td><td>2.07</td><td>0.13</td><td>3</td></tr><tr><td>η Aql</td><td>0.263</td><td>5800</td><td>1.90</td><td>4.00</td><td>0.09</td><td>7.713</td><td>2.35</td><td>0.13</td><td>6</td></tr><tr><td>η Aql</td><td>0.404</td><td>5612</td><td>1.75</td><td>3.90</td><td>0.10</td><td>7.713</td><td>2.39</td><td>0.13</td><td>6</td></tr><tr><td>η Aql</td><td>0.462</td><td>5508</td><td>1.80</td><td>4.00</td><td>0.08</td><td>7.713</td><td>2.39</td><td>0.13</td><td>6</td></tr><tr><td>EU Tau</td><td>0.172</td><td>6203</td><td>2.00</td><td>3.00</td><td>-0.06</td><td>8.933</td><td>2.30</td><td>0.13</td><td>6</td></tr><tr><td>EU Tau</td><td>0.641</td><td>6014</td><td>2.20</td><td>3.30</td><td>-0.06</td><td>8.933</td><td>2.34</td><td>0.13</td><td>6</td></tr><tr><td>EW Sct</td><td>0.572</td><td>5655</td><td>1.70</td><td>3.40</td><td>0.04</td><td>7.568</td><td>2.36</td><td>0.13</td><td>6</td></tr><tr><td>EW Sct</td><td>0.722</td><td>5728</td><td>1.80</td><td>3.50</td><td>0.04</td><td>7.568</td><td>2.36</td><td>0.13</td><td>6</td></tr><tr><td>EX Vel</td><td>0.954</td><td>5902</td><td>2.00</td><td>5.00</td><td>0.05</td><td>8.872</td><td>2.34</td><td>0.13</td><td>3</td></tr><tr><td>FF Aql</td><td>0.219</td><td>6172</td><td>2.15</td><td>4.30</td><td>0.00</td><td>7.629</td><td>2.32</td><td>0.18</td><td>6</td></tr><tr><td>FF Aql</td><td>0.846</td><td>6328</td><td>2.10</td><td>5.20</td><td>0.09</td><td>7.629</td><td>2.32</td><td>0.17</td><td>6</td></tr><tr><td>FF Aql</td><td>0.995</td><td>6425</td><td>2.10</td><td>4.90</td><td>0.02</td><td>7.629</td><td>2.22</td><td>0.18</td><td>6</td></tr><tr><td>FG Mon</td><td>0.523</td><td>5626</td><td>1.60</td><td>3.00</td><td>-0.20</td><td>13.944</td><td>2.47</td><td>0.15</td><td>3</td></tr><tr><td>FG Vel</td><td>0.756</td><td>5411</td><td>1.50</td><td>4.40</td><td>-0.05</td><td>8.286</td><td>2.34</td><td>0.18</td><td>3</td></tr><tr><td>FI Car</td><td>0.215</td><td>5215</td><td>1.20</td><td>3.80</td><td>-0.01</td><td>8.107</td><td>2.29</td><td>0.13</td><td>6</td></tr><tr><td>FI Mon</td><td>0.356</td><td>5938</td><td>2.00</td><td>3.50</td><td>-0.18</td><td>13.106</td><td>2.45</td><td>0.15</td><td>6</td></tr><tr><td>FM Aql</td><td>0.432</td><td>5590</td><td>1.60</td><td>3.70</td><td>0.06</td><td>7.290</td><td>2.54</td><td>0.15</td><td>6</td></tr><tr><td>FM Cas</td><td>0.669</td><td>5395</td><td>1.60</td><td>4.20</td><td>-0.12</td><td>8.941</td><td>2.27</td><td>0.15</td><td>5</td></tr><tr><td>FN Vel</td><td>0.221</td><td>5809</td><td>1.90</td><td>3.70</td><td>0.06</td><td>7.850</td><td>2.32</td><td>0.15</td><td>3</td></tr><tr><td>FR Car</td><td>0.011</td><td>5905</td><td>2.00</td><td>5.00</td><td>0.02</td><td>7.387</td><td>2.33</td><td>0.13</td><td>6</td></tr><tr><td>GH Car</td><td>0.965</td><td>6336</td><td>2.00</td><td>5.50</td><td>-0.01</td><td>7.414</td><td>2.27</td><td>0.13</td><td>3</td></tr><tr><td>GH Lup</td><td>0.142</td><td>5460</td><td>1.60</td><td>4.60</td><td>0.08</td><td>6.944</td><td>2.22</td><td>0.13</td><td>3</td></tr><tr><td>GQ Ori</td><td>0.074</td><td>6002</td><td>1.80</td><td>4.10</td><td>0.01</td><td>10.226</td><td>2.54</td><td>0.18</td><td>5</td></tr><tr><td>GU Nor</td><td>0.145</td><td>6036</td><td>2.20</td><td>3.60</td><td>0.15</td><td>6.553</td><td>2.35</td><td>0.13</td><td>3</td></tr><tr><td>GX Car</td><td>0.996</td><td>6297</td><td>2.20</td><td>5.30</td><td>0.01</td><td>7.762</td><td>2.04</td><td>0.13</td><td>3</td></tr><tr><td>HW Car</td><td>0.947</td><td>5671</td><td>2.00</td><td>5.20</td><td>0.04</td><td>7.556</td><td>2.24</td><td>0.13</td><td>3</td></tr><tr><td>HW Pup</td><td>0.432</td><td>5869</td><td>1.55</td><td>3.60</td><td>-0.15</td><td>12.332</td><td>2.33</td><td>0.15</td><td>3</td></tr><tr><td>IO Car</td><td>0.072</td><td>6145</td><td>1.80</td><td>6.00</td><td>-0.05</td><td>8.078</td><td>2.07</td><td>0.15</td><td>3</td></tr><tr><td>IR Cep</td><td>0.385</td><td>6104</td><td>2.10</td><td>2.90</td><td>0.11</td><td>8.037</td><td>2.50</td><td>0.15</td><td>6</td></tr><tr><td>IT Car</td><td>0.950</td><td>5794</td><td>1.80</td><td>4.70</td><td>0.06</td><td>7.451</td><td>2.17</td><td>0.13</td><td>3</td></tr><tr><td>KK Cen</td><td>0.012</td><td>5894</td><td>1.90</td><td>5.50</td><td>0.12</td><td>7.542</td><td>2.32</td><td>0.13</td><td>3</td></tr><tr><td>KN Cen</td><td>0.488</td><td>4870</td><td>1.70</td><td>4.50</td><td>0.35</td><td>6.404</td><td>2.55</td><td>0.18</td><td>3</td></tr><tr><td>KQ Sco</td><td>0.940</td><td>5058</td><td>1.10</td><td>5.70</td><td>0.16</td><td>5.409</td><td>2.15</td><td>0.17</td><td>3</td></tr><tr><td>L Car</td><td>0.094</td><td>5298</td><td>1.10</td><td>4.50</td><td>0.05</td><td>7.794</td><td>2.37</td><td>0.15</td><td>3</td></tr><tr><td>LR TrA</td><td>0.086</td><td>5943</td><td>2.20</td><td>4.40</td><td>0.25</td><td>7.291</td><td>2.35</td><td>0.13</td><td>3</td></tr><tr><td>MM Per</td><td>0.358</td><td>5746</td><td>2.15</td><td>3.40</td><td>-0.01</td><td>10.304</td><td>2.49</td><td>0.18</td><td>2</td></tr><tr><td>MW Cyg</td><td>0.458</td><td>5522</td><td>1.65</td><td>4.00</td><td>0.05</td><td>7.553</td><td>2.24</td><td>0.15</td><td>5</td></tr><tr><td>MY Pup</td><td>0.114</td><td>6317</td><td>2.20</td><td>4.80</td><td>-0.14</td><td>8.028</td><td>2.32</td><td>0.13</td><td>3</td></tr><tr><td>MZ Cen</td><td>0.207</td><td>5816</td><td>1.90</td><td>5.20</td><td>0.20</td><td>6.531</td><td>2.23</td><td>0.15</td><td>3</td></tr><tr><td>NT Pup</td><td>0.219</td><td>5561</td><td>1.20</td><td>4.00</td><td>-0.15</td><td>12.416</td><td>2.25</td><td>0.13</td><td>3</td></tr><tr><td>QY Cen</td><td>0.004</td><td>6205</td><td>2.00</td><td>6.30</td><td>0.16</td><td>6.638</td><td>2.30</td><td>0.20</td><td>1</td></tr><tr><td>R Cru</td><td>0.100</td><td>6203</td><td>2.00</td><td>4.00</td><td>0.08</td><td>7.539</td><td>2.25</td><td>0.13</td><td>3</td></tr><tr><td>R Mus</td><td>0.184</td><td>5985</td><td>2.00</td><td>4.00</td><td>0.10</td><td>7.502</td><td>2.32</td><td>0.13</td><td>3</td></tr><tr><td>R TrA</td><td>0.167</td><td>6121</td><td>2.20</td><td>3.80</td><td>0.06</td><td>7.475</td><td>2.22</td><td>0.13</td><td>3</td></tr><tr><td>RR Lac</td><td>0.518</td><td>5646</td><td>1.80</td><td>4.10</td><td>0.00</td><td>8.554</td><td>2.13</td><td>0.15</td><td>5</td></tr><tr><td>RS Ori</td><td>0.831</td><td>5934</td><td>1.85</td><td>5.10</td><td>-0.02</td><td>9.363</td><td>2.29</td><td>0.15</td><td>3</td></tr><tr><td>RS Pup</td><td>0.905</td><td>5068</td><td>1.00</td><td>5.00</td><td>0.20</td><td>8.540</td><td>2.38</td><td>0.13</td><td>3</td></tr><tr><td>RS Pup</td><td>0.935</td><td>5073</td><td>1.00</td><td>4.70</td><td>0.16</td><td>8.540</td><td>2.38</td><td>0.13</td><td>3</td></tr><tr><td>RT Aur</td><td>0.535</td><td>5696</td><td>2.15</td><td>3.30</td><td>0.05</td><td>8.304</td><td>2.30</td><td>0.13</td><td>6</td></tr><tr><td>RT Aur</td><td>0.583</td><td>5686</td><td>1.85</td><td>3.40</td><td>0.07</td><td>8.304</td><td>2.28</td><td>0.14</td><td>6</td></tr></tbody></table>
<table><caption>Table 3 – continued</caption><thead><tr><th>Star</th><th>Phase</th><th>T<sub>eff</sub> (K)</th><th>log g</th><th>V<sub>t</sub> (km s<sup>-1</sup>)</th><th>[Fe/H]</th><th>R<sub>G</sub> (kpc)</th><th>log ε(Ba)<sub>NLTE</sub></th><th>σ (Ba)</th><th>N lines</th></tr></thead><tbody><tr><td>RT Mus</td><td>0.204</td><td>6236</td><td>2.40</td><td>4.00</td><td>0.02</td><td>7.426</td><td>2.08</td><td>0.13</td><td>3</td></tr><tr><td>RV Sco</td><td>0.914</td><td>6172</td><td>2.30</td><td>5.40</td><td>0.03</td><td>6.734</td><td>2.05</td><td>0.13</td><td>3</td></tr><tr><td>RX Aur</td><td>0.135</td><td>6165</td><td>2.00</td><td>4.70</td><td>0.04</td><td>9.397</td><td>2.39</td><td>0.15</td><td>3</td></tr><tr><td>RX Aur</td><td>0.334</td><td>5677</td><td>1.40</td><td>3.70</td><td>-0.06</td><td>9.397</td><td>2.33</td><td>0.14</td><td>3</td></tr><tr><td>RX Cam</td><td>0.212</td><td>5971</td><td>1.95</td><td>4.10</td><td>0.07</td><td>8.614</td><td>2.40</td><td>0.15</td><td>6</td></tr><tr><td>RX Cam</td><td>0.461</td><td>5485</td><td>1.60</td><td>3.50</td><td>0.05</td><td>8.614</td><td>2.44</td><td>0.14</td><td>6</td></tr><tr><td>RY CMa</td><td>0.897</td><td>6096</td><td>2.10</td><td>4.30</td><td>0.02</td><td>8.781</td><td>2.44</td><td>0.20</td><td>2</td></tr><tr><td>RY Sco</td><td>0.746</td><td>5519</td><td>1.50</td><td>6.30</td><td>0.04</td><td>6.668</td><td>2.13</td><td>0.20</td><td>6</td></tr><tr><td>RY Vel</td><td>0.412</td><td>5466</td><td>1.30</td><td>4.60</td><td>0.10</td><td>7.731</td><td>2.32</td><td>0.13</td><td>3</td></tr><tr><td>RZ Gem</td><td>0.325</td><td>5906</td><td>2.20</td><td>3.10</td><td>-0.12</td><td>9.838</td><td>2.55</td><td>0.20</td><td>2</td></tr><tr><td>RZ Vel</td><td>0.037</td><td>6669</td><td>1.55</td><td>6.50</td><td>-0.03</td><td>8.225</td><td>2.24</td><td>0.15</td><td>3</td></tr><tr><td>RZ Vel</td><td>0.988</td><td>6549</td><td>1.65</td><td>6.80</td><td>-0.11</td><td>8.225</td><td>2.12</td><td>0.14</td><td>3</td></tr><tr><td>S Cru</td><td>0.983</td><td>6464</td><td>2.10</td><td>4.10</td><td>-0.12</td><td>7.553</td><td>2.20</td><td>0.13</td><td>3</td></tr><tr><td>S Mus</td><td>0.106</td><td>5752</td><td>1.80</td><td>4.40</td><td>-0.02</td><td>7.564</td><td>2.34</td><td>0.13</td><td>3</td></tr><tr><td>S Nor</td><td>0.124</td><td>5859</td><td>2.00</td><td>5.00</td><td>0.07</td><td>7.169</td><td>2.23</td><td>0.13</td><td>3</td></tr><tr><td>S Sge</td><td>0.295</td><td>5887</td><td>1.80</td><td>3.90</td><td>0.10</td><td>7.552</td><td>2.41</td><td>0.18</td><td>3</td></tr><tr><td>S Sge</td><td>0.345</td><td>5661</td><td>1.90</td><td>4.40</td><td>0.10</td><td>7.552</td><td>2.30</td><td>0.17</td><td>3</td></tr><tr><td>S Sge</td><td>0.463</td><td>5476</td><td>1.60</td><td>3.90</td><td>0.10</td><td>7.552</td><td>2.30</td><td>0.16</td><td>3</td></tr><tr><td>S Sge</td><td>0.502</td><td>5412</td><td>1.55</td><td>3.75</td><td>0.10</td><td>7.552</td><td>2.37</td><td>0.18</td><td>3</td></tr><tr><td>S Sge</td><td>0.820</td><td>5799</td><td>2.10</td><td>5.50</td><td>0.10</td><td>7.552</td><td>2.25</td><td>0.19</td><td>3</td></tr><tr><td>S Sge</td><td>0.911</td><td>6115</td><td>2.00</td><td>5.00</td><td>0.07</td><td>7.552</td><td>2.34</td><td>0.17</td><td>3</td></tr><tr><td>S Sge</td><td>0.935</td><td>6198</td><td>2.10</td><td>5.00</td><td>0.08</td><td>7.552</td><td>2.21</td><td>0.16</td><td>3</td></tr><tr><td>S Sge</td><td>0.940</td><td>6239</td><td>2.20</td><td>4.10</td><td>0.10</td><td>7.552</td><td>2.25</td><td>0.17</td><td>3</td></tr><tr><td>S TrA</td><td>0.176</td><td>5976</td><td>2.10</td><td>4.20</td><td>0.12</td><td>7.283</td><td>2.22</td><td>0.13</td><td>3</td></tr><tr><td>S Vul</td><td>0.516</td><td>5166</td><td>0.50</td><td>6.40</td><td>-0.04</td><td>7.067</td><td>2.24</td><td>0.18</td><td>6</td></tr><tr><td>S Vul</td><td>0.557</td><td>5123</td><td>0.50</td><td>6.60</td><td>-0.01</td><td>7.067</td><td>2.24</td><td>0.17</td><td>6</td></tr><tr><td>ST Tau</td><td>0.132</td><td>6268</td><td>2.00</td><td>3.50</td><td></td><td>8.834</td><td>2.41</td><td>0.15</td><td>6</td></tr><tr><td>ST Tau</td><td>0.869</td><td>6519</td><td>2.50</td><td>4.40</td><td></td><td>8.834</td><td>2.41</td><td>0.16</td><td>6</td></tr><tr><td>ST Vel</td><td>0.978</td><td>6255</td><td>2.10</td><td>4.30</td><td>0.00</td><td>8.183</td><td>2.34</td><td>0.13</td><td>3</td></tr><tr><td>SU Cas</td><td>0.405</td><td>6162</td><td>2.35</td><td>3.00</td><td>0.08</td><td>8.127</td><td>2.40</td><td>0.15</td><td>6</td></tr><tr><td>SU Cas</td><td>0.616</td><td>6112</td><td>2.30</td><td>2.80</td><td>0.06</td><td>8.127</td><td>2.59</td><td>0.14</td><td>6</td></tr><tr><td>SU Cas</td><td>0.855</td><td>6520</td><td>2.60</td><td>3.30</td><td>0.06</td><td>8.127</td><td>2.40</td><td>0.15</td><td>6</td></tr><tr><td>SU Cas</td><td>0.926</td><td>6603</td><td>2.80</td><td>3.50</td><td>0.02</td><td>8.127</td><td>2.31</td><td>0.15</td><td>6</td></tr><tr><td>SU Cyg</td><td>0.415</td><td>5956</td><td>2.10</td><td>3.20</td><td>0.00</td><td>7.603</td><td>2.39</td><td>0.17</td><td>6</td></tr><tr><td>SU Cyg</td><td>0.917</td><td>6197</td><td>2.20</td><td>4.25</td><td>-0.03</td><td>7.603</td><td>2.32</td><td>0.18</td><td>6</td></tr><tr><td>SU Cyg</td><td>0.940</td><td>6314</td><td>2.40</td><td>4.50</td><td>-0.03</td><td>7.603</td><td>2.32</td><td>0.18</td><td>6</td></tr><tr><td>SV Mon</td><td>0.047</td><td>6141</td><td>1.50</td><td>4.60</td><td>-0.05</td><td>10.143</td><td>2.39</td><td>0.18</td><td>5</td></tr><tr><td>SV Mon</td><td>0.223</td><td>5464</td><td>1.10</td><td>4.20</td><td>0.06</td><td>10.143</td><td>2.39</td><td>0.15</td><td>6</td></tr><tr><td>SV Mon</td><td>0.352</td><td>5204</td><td>0.90</td><td>3.30</td><td>-0.01</td><td>10.143</td><td>2.54</td><td>0.17</td><td>6</td></tr><tr><td>SV Mon</td><td>0.559</td><td>4924</td><td>1.10</td><td>4.50</td><td>0.00</td><td>10.143</td><td>2.20</td><td>0.17</td><td>3</td></tr><tr><td>SV Mon</td><td>0.784</td><td>5263</td><td>1.35</td><td>7.00</td><td>-0.07</td><td>10.143</td><td>2.39</td><td>0.18</td><td>6</td></tr><tr><td>SV Mon</td><td>0.851</td><td>5522</td><td>1.50</td><td>6.00</td><td>-0.05</td><td>10.143</td><td>2.39</td><td>0.17</td><td>6</td></tr><tr><td>SV Mon</td><td>0.916</td><td>5482</td><td>1.40</td><td>4.90</td><td>-0.04</td><td>10.143</td><td>2.39</td><td>0.18</td><td>6</td></tr><tr><td>SV Per</td><td>0.894</td><td>5734</td><td>1.70</td><td>4.30</td><td>-0.05</td><td>10.088</td><td>2.35</td><td>0.15</td><td>5</td></tr><tr><td>SV Vel</td><td>0.939</td><td>6064</td><td>2.00</td><td>6.00</td><td>0.08</td><td>7.594</td><td>2.07</td><td>0.15</td><td>3</td></tr><tr><td>SV Vul</td><td>0.070</td><td>5856</td><td>1.20</td><td>5.90</td><td>0.11</td><td>7.261</td><td>2.10</td><td>0.13</td><td>6</td></tr><tr><td>SV Vul</td><td>0.414</td><td>5005</td><td>0.65</td><td>5.00</td><td>-0.01</td><td>7.261</td><td>2.10</td><td>0.14</td><td>6</td></tr><tr><td>SW Cas</td><td>0.791</td><td>5749</td><td>2.00</td><td>5.10</td><td>0.02</td><td>8.747</td><td>2.14</td><td>0.20</td><td>2</td></tr><tr><td>SW Vel</td><td>0.348</td><td>5010</td><td>1.00</td><td>4.40</td><td>0.00</td><td>8.427</td><td>2.22</td><td>0.15</td><td>3</td></tr><tr><td>SX Car</td><td>0.943</td><td>6513</td><td>2.10</td><td>4.50</td><td>-0.09</td><td>7.586</td><td>2.17</td><td>0.13</td><td>3</td></tr><tr><td>SX Vel</td><td>0.852</td><td>6280</td><td>2.00</td><td>4.50</td><td>0.00</td><td>8.245</td><td>2.25</td><td>0.13</td><td>3</td></tr><tr><td>SY Cas</td><td>0.985</td><td>5718</td><td>2.00</td><td>4.30</td><td>-0.06</td><td>8.928</td><td>2.20</td><td>0.15</td><td>6</td></tr><tr><td>SY Nor</td><td>0.164</td><td>5641</td><td>1.80</td><td>4.70</td><td>0.31</td><td>6.442</td><td>2.28</td><td>0.20</td><td>3</td></tr><tr><td>SZ Aql</td><td>0.015</td><td>6559</td><td>2.00</td><td>6.00</td><td>0.13</td><td>6.421</td><td>2.32</td><td>0.13</td><td>6</td></tr><tr><td>SZ Aql</td><td>0.402</td><td>5147</td><td>1.10</td><td>3.85</td><td>0.25</td><td>6.421</td><td>2.35</td><td>0.14</td><td>6</td></tr><tr><td>SZ Cas</td><td>0.694</td><td>6157</td><td>1.60</td><td>4.30</td><td>0.02</td><td>9.832</td><td>2.50</td><td>0.20</td><td>5</td></tr><tr><td>SZ Cyg</td><td>0.293</td><td>5109</td><td>1.30</td><td>3.90</td><td>0.06</td><td>8.059</td><td>2.27</td><td>0.15</td><td>6</td></tr><tr><td>SZ Tau</td><td>0.296</td><td>6037</td><td>2.20</td><td>3.60</td><td>0.08</td><td>8.394</td><td>2.45</td><td>0.13</td><td>6</td></tr><tr><td>SZ Tau</td><td>0.426</td><td>5867</td><td>2.00</td><td>3.30</td><td>0.08</td><td>8.394</td><td>2.48</td><td>0.13</td><td>6</td></tr><tr><td>T Ant</td><td>0.173</td><td>6265</td><td>2.10</td><td>4.40</td><td>-0.24</td><td>8.384</td><td>2.14</td><td>0.12</td><td>2</td></tr><tr><td>T Cru</td><td>0.958</td><td>5940</td><td>2.20</td><td>5.10</td><td>0.09</td><td>7.546</td><td>2.25</td><td>0.13</td><td>3</td></tr></tbody></table>
<table><caption>Table 3 – continued</caption><thead><tr><th>Star</th><th>Phase</th><th>T<sub>eff</sub> (K)</th><th>log g</th><th>V<sub>t</sub> (km s<sup>-1</sup>)</th><th>[Fe/H]</th><th>R<sub>G</sub> (kpc)</th><th>log ε(Ba)<sub>NLTE</sub></th><th>σ (Ba)</th><th>N lines</th></tr></thead><tbody><tr><td>T Mon</td><td>0.562</td><td>4853</td><td>0.80</td><td>4.20</td><td>0.21</td><td>9.150</td><td>2.43</td><td>0.13</td><td>3</td></tr><tr><td>T Mon</td><td>0.600</td><td>4828</td><td>1.10</td><td>4.70</td><td>0.11</td><td>9.150</td><td>2.40</td><td>0.14</td><td>3</td></tr><tr><td>T Vel</td><td>0.827</td><td>5692</td><td>2.00</td><td>4.80</td><td>-0.02</td><td>8.054</td><td>2.26</td><td>0.15</td><td>3</td></tr><tr><td>T Vul</td><td>0.201</td><td>6077</td><td>2.00</td><td>3.55</td><td>0.02</td><td>7.760</td><td>2.35</td><td>0.18</td><td>6</td></tr><tr><td>T Vul</td><td>0.302</td><td>5899</td><td>2.00</td><td>3.30</td><td>0.03</td><td>7.760</td><td>2.43</td><td>0.17</td><td>6</td></tr><tr><td>TT Aql</td><td>0.457</td><td>5080</td><td>1.10</td><td>3.60</td><td>0.12</td><td>7.099</td><td>2.37</td><td>0.13</td><td>6</td></tr><tr><td>TT Aql</td><td>0.920</td><td>5630</td><td>1.60</td><td>5.10</td><td>0.09</td><td>7.099</td><td>2.37</td><td>0.14</td><td>6</td></tr><tr><td>TW CMa</td><td>0.059</td><td>6142</td><td>1.80</td><td>3.90</td><td>-0.18</td><td>9.764</td><td>2.37</td><td>0.20</td><td>2</td></tr><tr><td>TW Mon</td><td>0.167</td><td>5770</td><td>1.70</td><td>4.00</td><td>-0.24</td><td>13.608</td><td>2.38</td><td>0.13</td><td>3</td></tr><tr><td>TW Nor</td><td>0.094</td><td>5979</td><td>2.00</td><td>5.60</td><td>0.28</td><td>5.843</td><td>2.25</td><td>0.15</td><td>3</td></tr><tr><td>TX Cyg</td><td>0.936</td><td>6054</td><td>2.00</td><td>5.60</td><td>0.08</td><td>7.869</td><td>2.20</td><td>0.15</td><td>6</td></tr><tr><td>TX Del</td><td>0.005</td><td>6217</td><td>1.80</td><td>6.00</td><td>0.24</td><td>6.820</td><td>2.11</td><td>0.15</td><td>3</td></tr><tr><td>TX Mon</td><td>0.122</td><td>5871</td><td>1.80</td><td>4.90</td><td>-0.14</td><td>11.742</td><td>2.05</td><td>0.18</td><td>3</td></tr><tr><td>TZ Mon</td><td>0.817</td><td>5008</td><td>2.20</td><td>1.50</td><td>-0.03</td><td>11.439</td><td>2.29</td><td>0.13</td><td>3</td></tr><tr><td>TZ Mus</td><td>0.024</td><td>6348</td><td>2.10</td><td>4.60</td><td>-0.01</td><td>7.063</td><td>2.17</td><td>0.15</td><td>3</td></tr><tr><td>U Car</td><td>0.968</td><td>4934</td><td>0.80</td><td>5.80</td><td>0.01</td><td>7.537</td><td>2.27</td><td>0.15</td><td>3</td></tr><tr><td>U Nor</td><td>0.476</td><td>5426</td><td>1.40</td><td>3.60</td><td>0.15</td><td>6.815</td><td>2.33</td><td>0.10</td><td>3</td></tr><tr><td>U Vul</td><td>0.290</td><td>5965</td><td>1.85</td><td>4.10</td><td>0.13</td><td>7.584</td><td>2.43</td><td>0.13</td><td>6</td></tr><tr><td>U Vul</td><td>0.415</td><td>5655</td><td>1.75</td><td>4.00</td><td>0.10</td><td>7.584</td><td>2.43</td><td>0.14</td><td>6</td></tr><tr><td>UU Mus</td><td>0.041</td><td>6175</td><td>1.80</td><td>5.40</td><td>0.05</td><td>7.054</td><td>2.34</td><td>0.15</td><td>3</td></tr><tr><td>UW Car</td><td>0.035</td><td>6618</td><td>2.10</td><td>4.30</td><td>-0.06</td><td>7.617</td><td>2.05</td><td>0.12</td><td>3</td></tr><tr><td>UX Car</td><td>0.902</td><td>6442</td><td>2.60</td><td>4.70</td><td>0.02</td><td>7.663</td><td>2.19</td><td>0.12</td><td>3</td></tr><tr><td>UY Car</td><td>0.946</td><td>6376</td><td>2.40</td><td>5.70</td><td>0.03</td><td>7.548</td><td>2.05</td><td>0.15</td><td>3</td></tr><tr><td>UY Mon</td><td>0.674</td><td>6181</td><td>2.20</td><td>2.70</td><td>-0.08</td><td>10.085</td><td>2.47</td><td>0.18</td><td>2</td></tr><tr><td>UZ Car</td><td>0.044</td><td>6079</td><td>2.00</td><td>4.30</td><td>0.07</td><td>7.544</td><td>2.31</td><td>0.15</td><td>2</td></tr><tr><td>UZ Sct</td><td>0.455</td><td>5127</td><td>1.50</td><td>3.30</td><td>0.33</td><td>5.125</td><td>2.69</td><td>0.15</td><td>3</td></tr><tr><td>V Car</td><td>0.889</td><td>5906</td><td>2.10</td><td>5.20</td><td>0.01</td><td>7.877</td><td>2.22</td><td>0.12</td><td>2</td></tr><tr><td>V Cen</td><td>0.236</td><td>5705</td><td>2.10</td><td>3.90</td><td>0.01</td><td>7.426</td><td>2.15</td><td>0.12</td><td>3</td></tr><tr><td>V Cen</td><td>0.781</td><td>5616</td><td>1.80</td><td>4.80</td><td>0.01</td><td>7.426</td><td>1.95</td><td>0.12</td><td>3</td></tr><tr><td>V Cen</td><td>0.952</td><td>6427</td><td>2.30</td><td>4.60</td><td>0.01</td><td>7.426</td><td>2.15</td><td>0.13</td><td>3</td></tr><tr><td>V Lac</td><td>0.098</td><td>6470</td><td>1.90</td><td>3.60</td><td>-0.05</td><td>8.485</td><td>2.40</td><td>0.18</td><td>5</td></tr><tr><td>V Vel</td><td>0.043</td><td>6364</td><td>2.10</td><td>5.00</td><td>-0.23</td><td>7.849</td><td>2.00</td><td>0.13</td><td>3</td></tr><tr><td>V335 Aur</td><td>0.622</td><td>5750</td><td>2.20</td><td>3.50</td><td>-0.27</td><td>9.193</td><td>2.28</td><td>0.20</td><td>1</td></tr><tr><td>V339 Cen</td><td>0.142</td><td>5923</td><td>2.00</td><td>5.30</td><td>0.04</td><td>6.774</td><td>2.12</td><td>0.13</td><td>3</td></tr><tr><td>V340 Ara</td><td>0.167</td><td>5472</td><td>1.50</td><td>4.00</td><td>0.31</td><td>4.344</td><td>2.30</td><td>0.15</td><td>3</td></tr><tr><td>V340 Nor</td><td>0.193</td><td>5595</td><td>1.75</td><td>4.50</td><td>0.08</td><td>6.306</td><td>2.15</td><td>0.13</td><td>3</td></tr><tr><td>V340 Nor</td><td>0.430</td><td>5733</td><td>2.00</td><td>5.30</td><td>0.08</td><td>6.306</td><td>2.17</td><td>0.14</td><td>3</td></tr><tr><td>V350 Sgr</td><td>0.468</td><td>5557</td><td>1.90</td><td>3.70</td><td>0.15</td><td>7.065</td><td>2.34</td><td>0.15</td><td>6</td></tr><tr><td>V351 Cep</td><td>0.301</td><td>6005</td><td>2.10</td><td>3.30</td><td>0.03</td><td>8.313</td><td>2.27</td><td>0.18</td><td>3</td></tr><tr><td>V351 Cep</td><td>0.425</td><td>5944</td><td>2.50</td><td>4.30</td><td>0.03</td><td>8.313</td><td>2.21</td><td>0.18</td><td>2</td></tr><tr><td>V367 Sct</td><td></td><td>5891</td><td>2.10</td><td>4.25</td><td>-0.01</td><td>6.431</td><td>2.05</td><td>0.20</td><td>3</td></tr><tr><td>V378 Cen</td><td>0.131</td><td>6184</td><td>2.00</td><td>4.70</td><td>-0.02</td><td>7.054</td><td>2.35</td><td>0.13</td><td>3</td></tr><tr><td>V379 Cas</td><td>0.515</td><td>5943</td><td>2.00</td><td>3.50</td><td>0.04</td><td>8.592</td><td>2.50</td><td>0.15</td><td>6</td></tr><tr><td>V379 Cas</td><td>0.740</td><td>5969</td><td>2.00</td><td>3.50</td><td>0.01</td><td>8.592</td><td>2.50</td><td>0.14</td><td>6</td></tr><tr><td>V381 Cen</td><td>0.896</td><td>6224</td><td>2.30</td><td>5.10</td><td>0.02</td><td>7.236</td><td>2.20</td><td>0.13</td><td>3</td></tr><tr><td>V386 Cyg</td><td>0.961</td><td>6284</td><td>2.20</td><td>4.60</td><td>-0.04</td><td>7.888</td><td>2.27</td><td>0.15</td><td>6</td></tr><tr><td>V397 Car</td><td>0.903</td><td>6036</td><td>2.30</td><td>4.80</td><td>0.03</td><td>7.674</td><td>2.16</td><td>0.13</td><td>3</td></tr><tr><td>V402 Cyg</td><td>0.514</td><td>5518</td><td>1.55</td><td>3.70</td><td>-0.06</td><td>7.600</td><td>2.27</td><td>0.18</td><td>6</td></tr><tr><td>V419 Cen</td><td>0.905</td><td>6276</td><td>2.10</td><td>5.60</td><td>0.07</td><td>7.411</td><td>2.27</td><td>0.13</td><td>3</td></tr><tr><td>V440 Per</td><td>0.275</td><td>6048</td><td>2.20</td><td>4.80</td><td>-0.02</td><td>8.478</td><td>2.43</td><td>0.18</td><td>6</td></tr><tr><td>V440 Per</td><td>0.807</td><td>6041</td><td>2.00</td><td>4.80</td><td>-0.02</td><td>8.478</td><td>2.43</td><td>0.17</td><td>6</td></tr><tr><td>V465 Mon</td><td>0.373</td><td>6088</td><td>2.30</td><td>3.70</td><td>-0.04</td><td>10.088</td><td>2.45</td><td>0.18</td><td>6</td></tr><tr><td>V473 Lyr</td><td>0.559</td><td>6113</td><td>2.60</td><td>4.50</td><td>-0.06</td><td>7.726</td><td>2.35</td><td>0.15</td><td>3</td></tr><tr><td>V473 Lyr</td><td>0.793</td><td>6163</td><td>2.45</td><td>4.20</td><td>-0.06</td><td>7.726</td><td>2.45</td><td>0.16</td><td>3</td></tr><tr><td>V482 Sco</td><td>0.113</td><td>6129</td><td>2.20</td><td>4.00</td><td>0.07</td><td>6.945</td><td>2.31</td><td>0.13</td><td>3</td></tr><tr><td>V495 Mon</td><td>0.622</td><td>5591</td><td>1.60</td><td>4.00</td><td>-0.26</td><td>12.105</td><td>2.35</td><td>0.18</td><td>3</td></tr><tr><td>V496 Aql</td><td>0.043</td><td>5841</td><td>1.70</td><td>4.00</td><td>0.06</td><td>6.884</td><td>2.35</td><td>0.15</td><td>6</td></tr><tr><td>V496 Aql</td><td>0.910</td><td>5822</td><td>1.70</td><td>4.25</td><td>0.03</td><td>6.884</td><td>2.35</td><td>0.16</td><td>6</td></tr><tr><td>V496 Cen</td><td>0.025</td><td>6194</td><td>2.15</td><td>3.80</td><td>0.00</td><td>7.059</td><td>2.32</td><td>0.15</td><td>3</td></tr><tr><td>V500 Sco</td><td>0.051</td><td>5999</td><td>1.80</td><td>4.30</td><td>0.06</td><td>6.530</td><td>2.36</td><td>0.15</td><td>6</td></tr><tr><td>V500 Sco</td><td>0.340</td><td>5356</td><td>1.25</td><td>3.60</td><td>0.02</td><td>6.530</td><td>2.33</td><td>0.16</td><td>6</td></tr><tr><td>V504 Mon</td><td>0.714</td><td>6370</td><td>2.00</td><td>3.50</td><td>-0.31</td><td>10.676</td><td>2.13</td><td>0.13</td><td>3</td></tr><tr><td>V508 Mon</td><td>0.742</td><td>5566</td><td>1.60</td><td>4.00</td><td>-0.25</td><td>10.710</td><td>2.05</td><td>0.15</td><td>3</td></tr><tr><td>V510 Mon</td><td>0.232</td><td>5842</td><td>1.40</td><td>3.80</td><td>-0.19</td><td>12.956</td><td>2.48</td><td>0.15</td><td>3</td></tr></tbody></table>
<table><caption>Table 3 – continued</caption><thead><tr><th>Star</th><th>Phase</th><th>T<sub>eff</sub> (K)</th><th>log g</th><th>V<sub>t</sub> (km s<sup>-1</sup>)</th><th>[Fe/H]</th><th>R<sub>G</sub> (kpc)</th><th>log ϵ (Ba)<sub>NLTE</sub></th><th>σ (Ba)</th><th>N lines</th></tr></thead><tbody><tr><td>V526 Mon</td><td>0.674</td><td>6464</td><td>2.40</td><td>3.50</td><td></td><td>9.325</td><td>2.52</td><td>0.20</td><td>3</td></tr><tr><td>V532 Cyg</td><td>0.599</td><td>5960</td><td>2.00</td><td>3.10</td><td>0.08</td><td>7.981</td><td>2.47</td><td>0.15</td><td>6</td></tr><tr><td>V600 Aql</td><td>0.457</td><td>5604</td><td>1.70</td><td>4.00</td><td>-0.02</td><td>6.831</td><td>2.30</td><td>0.15</td><td>6</td></tr><tr><td>V636 Cas</td><td>0.151</td><td>5562</td><td>1.50</td><td>4.10</td><td>0.07</td><td>8.337</td><td>2.33</td><td>0.15</td><td>6</td></tr><tr><td>V636 Cas</td><td>0.270</td><td>5473</td><td>1.50</td><td>3.80</td><td>0.06</td><td>8.337</td><td>2.39</td><td>0.15</td><td>6</td></tr><tr><td>V636 Sco</td><td>0.969</td><td>5348</td><td>1.60</td><td>4.30</td><td>0.07</td><td>7.148</td><td>2.01</td><td>0.15</td><td>3</td></tr><tr><td>V659 Cen</td><td>0.856</td><td>6067</td><td>2.20</td><td>5.40</td><td>0.07</td><td>7.447</td><td>2.17</td><td>0.15</td><td>3</td></tr><tr><td>V733 Aql</td><td>0.699</td><td>5435</td><td>1.70</td><td>4.70</td><td>-0.01</td><td>6.187</td><td>2.02</td><td>0.15</td><td>5</td></tr><tr><td>V737 Cen</td><td>0.967</td><td>5865</td><td>2.00</td><td>4.50</td><td>0.13</td><td>7.335</td><td>2.45</td><td>0.13</td><td>3</td></tr><tr><td>V924 Cyg</td><td>0.702</td><td>5910</td><td>1.80</td><td>5.00</td><td>-0.09</td><td>7.529</td><td>2.10</td><td>0.20</td><td>3</td></tr><tr><td>V950 Sco</td><td>0.126</td><td>6322</td><td>2.20</td><td>4.20</td><td>0.11</td><td>7.099</td><td>2.22</td><td>0.13</td><td>3</td></tr><tr><td>V1154 Cyg</td><td>0.120</td><td>5840</td><td>1.80</td><td>4.10</td><td>-0.12</td><td>7.704</td><td>2.37</td><td>0.15</td><td>6</td></tr><tr><td>V1334 Cyg</td><td>0.253</td><td>6203</td><td>2.10</td><td>3.50</td><td>0.03</td><td>7.856</td><td>2.30</td><td>0.15</td><td>6</td></tr><tr><td>V1334 Cyg</td><td>0.295</td><td>6203</td><td>2.10</td><td>3.40</td><td>0.06</td><td>7.856</td><td>2.30</td><td>0.18</td><td>6</td></tr><tr><td>V1726 Cyg</td><td>0.109</td><td>6349</td><td>2.20</td><td>5.20</td><td>-0.02</td><td>8.177</td><td>2.14</td><td>0.20</td><td>3</td></tr><tr><td>VW Cru</td><td>0.175</td><td>5880</td><td>2.10</td><td>4.40</td><td>0.10</td><td>7.275</td><td>2.23</td><td>0.13</td><td>3</td></tr><tr><td>VW Pup</td><td>0.617</td><td>5586</td><td>1.90</td><td>4.60</td><td>-0.19</td><td>10.340</td><td>2.05</td><td>0.15</td><td>3</td></tr><tr><td>VX Cyg</td><td>0.411</td><td>5015</td><td>0.80</td><td>3.70</td><td>0.10</td><td>8.064</td><td>2.49</td><td>0.18</td><td>6</td></tr><tr><td>VX Per</td><td>0.709</td><td>5999</td><td>1.80</td><td>4.20</td><td>-0.03</td><td>9.627</td><td>2.52</td><td>0.20</td><td>6</td></tr><tr><td>VX Per</td><td>0.800</td><td>5992</td><td>1.80</td><td>4.20</td><td>-0.04</td><td>9.627</td><td>2.52</td><td>0.18</td><td>6</td></tr><tr><td>VX Pup</td><td>0.813</td><td>6159</td><td>2.50</td><td>3.50</td><td>-0.13</td><td>8.638</td><td>2.30</td><td>0.20</td><td>2</td></tr><tr><td>VY Car</td><td>0.169</td><td>4895</td><td>1.60</td><td>5.20</td><td>0.26</td><td>7.582</td><td>2.64</td><td>0.20</td><td>3</td></tr><tr><td>VY Cyg</td><td>0.370</td><td>5743</td><td>1.80</td><td>4.10</td><td>-0.02</td><td>7.885</td><td>2.27</td><td>0.15</td><td>6</td></tr><tr><td>VY Sgr</td><td>0.394</td><td>5144</td><td>1.25</td><td>3.30</td><td>0.26</td><td>5.584</td><td>2.50</td><td>0.15</td><td>3</td></tr><tr><td>VZ Cma</td><td>0.777</td><td>6542</td><td>2.50</td><td>3.60</td><td>-0.06</td><td>8.753</td><td>2.57</td><td>0.20</td><td>2</td></tr><tr><td>VZ Cyg</td><td>0.365</td><td>5670</td><td>1.80</td><td>3.30</td><td>-0.07</td><td>8.132</td><td>2.52</td><td>0.18</td><td>6</td></tr><tr><td>VZ Pup</td><td>0.980</td><td>6070</td><td>2.20</td><td>4.70</td><td>-0.16</td><td>10.404</td><td>2.25</td><td>0.19</td><td>3</td></tr><tr><td>W Gem</td><td>0.029</td><td>6416</td><td>2.25</td><td>5.00</td><td>-0.02</td><td>8.776</td><td>2.30</td><td>0.13</td><td>6</td></tr><tr><td>W Gem</td><td>0.136</td><td>6032</td><td>1.85</td><td>4.05</td><td>-0.01</td><td>8.776</td><td>2.35</td><td>0.14</td><td>6</td></tr><tr><td>W Gem</td><td>0.524</td><td>5475</td><td>1.70</td><td>3.90</td><td>-0.01</td><td>8.776</td><td>2.39</td><td>0.13</td><td>6</td></tr><tr><td>W Sgr</td><td>0.302</td><td>5927</td><td>1.85</td><td>3.70</td><td>0.04</td><td>7.512</td><td>2.40</td><td>0.15</td><td>6</td></tr><tr><td>W Sgr</td><td>0.462</td><td>5535</td><td>1.70</td><td>3.80</td><td>0.03</td><td>7.512</td><td>2.40</td><td>0.14</td><td>6</td></tr><tr><td>WW Car</td><td>0.852</td><td>5858</td><td>2.10</td><td>5.30</td><td>-0.07</td><td>7.515</td><td>1.87</td><td>0.13</td><td>3</td></tr><tr><td>WW Mon</td><td>0.750</td><td>6166</td><td>2.20</td><td>5.10</td><td>-0.29</td><td>12.943</td><td>2.30</td><td>0.15</td><td>3</td></tr><tr><td>WW Pup</td><td>0.722</td><td>5550</td><td>1.60</td><td>4.20</td><td>-0.18</td><td>10.068</td><td>2.07</td><td>0.15</td><td>3</td></tr><tr><td>WZ Car</td><td>0.009</td><td>5770</td><td>1.80</td><td>6.80</td><td>0.03</td><td>7.573</td><td>2.17</td><td>0.15</td><td>3</td></tr><tr><td>WZ Sgr</td><td>0.335</td><td>5077</td><td>1.10</td><td>3.80</td><td>0.20</td><td>5.964</td><td>2.40</td><td>0.15</td><td>3</td></tr><tr><td>WZ Sgr</td><td>0.942</td><td>6130</td><td>1.85</td><td>5.70</td><td>0.10</td><td>5.964</td><td>2.40</td><td>0.15</td><td>3</td></tr><tr><td>X Cru</td><td>0.125</td><td>5948</td><td>2.00</td><td>4.20</td><td>0.14</td><td>7.201</td><td>2.32</td><td>0.13</td><td>3</td></tr><tr><td>X Lac</td><td>0.328</td><td>5890</td><td>1.85</td><td>3.30</td><td>-0.01</td><td>8.477</td><td>2.42</td><td>0.18</td><td>5</td></tr><tr><td>X Pup</td><td>0.175</td><td>5848</td><td>1.30</td><td>5.00</td><td>-0.01</td><td>9.730</td><td>2.25</td><td>0.15</td><td>6</td></tr><tr><td>X Pup</td><td>0.213</td><td>5654</td><td>1.10</td><td>4.40</td><td>0.01</td><td>9.730</td><td>2.32</td><td>0.16</td><td>6</td></tr><tr><td>X Vul</td><td>0.062</td><td>6260</td><td>2.00</td><td>4.20</td><td>0.13</td><td>7.532</td><td>2.17</td><td>0.15</td><td>6</td></tr><tr><td>X Vul</td><td>0.220</td><td>5870</td><td>1.90</td><td>4.25</td><td>0.12</td><td>7.532</td><td>2.12</td><td>0.15</td><td>6</td></tr><tr><td>XX Car</td><td>0.692</td><td>5942</td><td>1.60</td><td>4.50</td><td>0.11</td><td>7.382</td><td>2.29</td><td>0.13</td><td>3</td></tr><tr><td>XX Cen</td><td>0.116</td><td>5953</td><td>2.00</td><td>5.00</td><td>0.16</td><td>6.997</td><td>2.40</td><td>0.13</td><td>3</td></tr><tr><td>XX Mon</td><td>0.704</td><td>5533</td><td>1.70</td><td>4.20</td><td>-0.18</td><td>11.946</td><td>2.20</td><td>0.15</td><td>3</td></tr><tr><td>XX Sgr</td><td>0.584</td><td>5557</td><td>1.60</td><td>3.20</td><td>0.05</td><td>6.632</td><td>2.53</td><td>0.18</td><td>6</td></tr><tr><td>XX Vel</td><td>0.011</td><td>6521</td><td>2.20</td><td>4.90</td><td>-0.05</td><td>7.708</td><td>2.10</td><td>0.13</td><td>3</td></tr><tr><td>XY Car</td><td>0.242</td><td>5738</td><td>1.70</td><td>4.60</td><td>0.04</td><td>7.356</td><td>2.07</td><td>0.13</td><td>3</td></tr><tr><td>XY Cas</td><td>0.603</td><td>5542</td><td>1.50</td><td>3.80</td><td>0.02</td><td>8.979</td><td>2.28</td><td>0.15</td><td>5</td></tr><tr><td>XZ Car</td><td>0.072</td><td>6170</td><td>2.10</td><td>5.70</td><td>0.14</td><td>7.414</td><td>2.32</td><td>0.15</td><td>1</td></tr><tr><td>Y Lac</td><td>0.858</td><td>6006</td><td>1.70</td><td>4.45</td><td>-0.08</td><td>8.419</td><td>2.17</td><td>0.18</td><td>6</td></tr><tr><td>Y Lac</td><td>0.936</td><td>6330</td><td>2.00</td><td>4.00</td><td>-0.10</td><td>8.419</td><td>2.17</td><td>0.17</td><td>6</td></tr><tr><td>Y Sgr</td><td>0.319</td><td>5733</td><td>1.65</td><td>3.80</td><td>0.11</td><td>7.425</td><td>2.43</td><td>0.18</td><td>6</td></tr><tr><td>Y Sgr</td><td>0.427</td><td>5605</td><td>1.60</td><td>3.70</td><td>0.04</td><td>7.425</td><td>2.45</td><td>0.18</td><td>6</td></tr><tr><td>YZ Car</td><td>0.860</td><td>5655</td><td>1.60</td><td>6.50</td><td>0.02</td><td>7.629</td><td>2.12</td><td>0.13</td><td>3</td></tr><tr><td>YZ Sgr</td><td>0.249</td><td>5507</td><td>1.40</td><td>3.65</td><td>0.06</td><td>6.799</td><td>2.24</td><td>0.15</td><td>6</td></tr><tr><td>YZ Sgr</td><td>0.775</td><td>5913</td><td>1.90</td><td>4.80</td><td>0.08</td><td>6.799</td><td>2.27</td><td>0.15</td><td>6</td></tr><tr><td>Z Lac</td><td>0.204</td><td>5722</td><td>1.50</td><td>3.80</td><td>0.05</td><td>8.564</td><td>2.37</td><td>0.15</td><td>6</td></tr><tr><td>Z Lac</td><td>0.930</td><td>5899</td><td>1.70</td><td>4.30</td><td>0.01</td><td>8.564</td><td>2.37</td><td>0.15</td><td>6</td></tr></tbody></table>
<figure><img src="image_12.png" /><figcaption>**Figure 10.** [Fe/H] versus Galactocentric distance from Luck & Lambert (2011) – Fig. 1.</figcaption></figure>

vicinity. This difference would be about 0.3 dex if we adopt the metallicity distribution with a step at corotation as proposed by Lépine et al. (2011) based on a study of open clusters. One could expect to detect lower barium abundance in the region 9–14 kpc relative to the solar value, but this is not the case, as one can see in Fig. 9.

If one adopts for lanthanum, praseodymium, neodymium, samarium and europium the main s- and r-process dissection provided by Simmerer et al. (2004), and plot their r-process fractions versus abundance gradients derived for these elements by Luck & Lambert (2011), then one can note the slight (and quite loose) slope in the ‘abundance gradient–r-process fraction’ dependence. Using this dependence together with barium r-process fraction 0.15, one can derive the expected barium abundance gradient of about –0.03 dex kpc⁻¹, which is in contrast to the zero slope from the present paper.

This discrepancy between observed and expected abundance gradient for Ba abundance requires either a peculiar s-process pattern with lower ‘r’-process fraction for all the above-considered elements, or there is a systematic error in the Ba abundance analysis, an odd error that is not revealed by the temperature, gravity or phase-dependent spectra.

Another possibility could be connected to some yet unaccounted effect, which may be hidden in the literature, La, Ce, Nd and Eu LTE abundance data derived for Cepheids and the respective gradients based on them. For instance, the NLTE deviations for these elements may be different for the stars with (even slightly) different metallicities located at different galactocentric distances.

Since there are no other large studies, in the literature, of the barium abundance distributions in the disc, and thus there is no possibility to compare our barium data with the results of other specialists, we prefer to leave a detailed discussion of this problem for future studies, until the new observational and theoretical data

on barium and other heavy s-process element distributions in the Galactic disc appear.

## ACKNOWLEDGMENTS

SMA acknowledges the Universidade de São Paulo (USP) and Instituto de Astronomia, Geofísica e Ciências Atmosféricas da USP for support and hospitality during his stay in Brazil. SAK thanks the SCOPES grant no. IZ73Z0-128180/1 for partial financial support. The authors thank anonymous referee for his/her comments.

## REFERENCES

* Andrievsky S. M. et al., 2002a, A&A, 381, 32

* Andrievsky S. M., Bersier D., Kovtyukh V. V., Luck R. E., Maciel W. J., Lépine J. R. D., Beletsky Yu. V., 2002b, A&A, 384, 140

* Andrievsky S. M., Kovtyukh V. V., Luck R. E., Lépine J. R. D., Maciel W. J., Beletsky Yu. V., 2002c, A&A, 392, 491

* Andrievsky S. M., Luck R. E., Martin P., Lépine J. R. D., 2004, A&A, 413, 159

* Andrievsky S. M., Luck R. E., Kovtyukh V. V., 2005, AJ, 130, 1880

* Andrievsky S. M., Spite M., Korotin S. A., Spite F., Francois P., Bonifacio P., Cayrel R., Hill V., 2009, A&A, 494, 1083

* Cameron A. G. W., 1982, Ap&SS, 82, 123

* Carlsson M., 1986, Uppsala Astron. Obser. Rep., 33

* Cescutti G., Matteucci F., Francois P., Chiappini C., 2007, A&A, 462, 943

* Fuhr J. R., Wiese W. L., 2006, J. Phys. Chem. Reference Data, 35, 1669

* Korotin S. A., Andrievsky S. M., Luck R. E., 1999, A&A, 351, 168

* Korotin S., Mishenina T., Gorbaneva T., Soubiran C., 2010, Proceedings of the 11th Symposium on Nuclei in the Cosmos. Proceedings of Science

* Kovtyukh V. V., Andrievsky S. M., Belik S. I., Luck R. E., 2005, AJ, 129, 433

* Lépine J. R. D. et al., 2011, MNRAS, 417, 698

* Luck R. E., Andrievsky S. M., 2004, AJ, 128, 343

* Luck R. E., Lambert D. L., 2011, AJ, 142, 136

* Luck R. E., Gieren W. P., Andrievsky S. M., Kovtyukh V. V., Fouqué P., Pont F., Kienzle F., 2003, A&A, 401, 939

* Luck R. E., Kovtyukh V. V., Andrievsky S. M., 2006, AJ, 132, 902

* Luck R. E., Andrievsky S. M., Fokin A., Kovtyukh V. V., 2008, AJ, 136, 98

* Luck R. E., Andrievsky S. M., Kovtyukh V. V., Gieren W., Graczyk D., 2011, AJ, 142, 51

* Mashonkina L., Gehren T., Bikmaev I., 1999, A&A, 343, 519

* Rutten R. J., 1978, Solar Phys., 56, 237

* Simmerer J., Sneden C., Cowan J. J., Collier J., Woolf V. M., Lawler J. E., 2004, ApJ, 617, 1091

* Stodilka M. I., Malynch S. Z., 2006, MNRAS, 373, 1523

* Tsymbal V. V., 1996, in Adelman S. J., Kupka F., Weiss W. W., eds, ASP Conf. Ser. Vol. 108, Model Atmospheres and Spectrum Synthesis. Astron. Soc. Pac., San Francisco, p. 198

This paper has been typeset from a TEX/LATEX file prepared by the author.