Movatterモバイル変換

• Top
• Abstract
• 1. Introduction
• 2. Observations and data reduction
• 3. Abundance analysis
• 4. Results of abundance analysis
• 5. Fundamental parameters of NGC 4337
• 6. Discussion and conclusions
• Acknowledgments
• References
• List of tables
• List of figures

© ESO, 2014

1. Introduction

Recently, Carraro et al. (2014a) have drawn the attention to the open star cluster NGC 4337, located at,. It was identified as a particularly relevant object, being a rare example of an old (~1.5–2.0 Gyr) cluster located inside the solar ring at a Galacto-centric distanceR_GC ~ 7.5 kpc. As such, NGC 4337 can help us to improve our knowledge of the inner disc radial abundance gradient and its temporal evolution (Magrini et al.2010,2014).

This evidence came from the analysis of a deep photometric data-set in theU,B,V, andI passbands, and using the classical old open IC 4651 (Anthony-Twarog et al.2009) ridge-line as comparison. Previous shallow photoelectric optical photometry had missed the cluster, but more recently, it was recovered by Froebrich et al. (2010) in their search for star clusters across the Galactic plane using 2MASS.

Carraro et al. (2014a) assumed that NGC 4337 shares the same metallicity as IC 4651 from simply comparing the distribution of stars in the colour-magnitude diagram (CMD). Based on this, preliminary estimates of the reddening (E(B −V) ~ 0.26) and the apparent distance modulus ((m −M)_V ~ 13.00) were derived.

With this preliminary fundamental parameter set, NGC 4337 is shown to be an extremely interesting object, sharing the same age and hence turn-off (TO) mass as IC 4651, NGC 3680, and NGC 752. These text-book clusters have routinely been studied to probe the behaviour of H-burning in the TO mass range 1.1–1.4M_⊙, where convective overshooting is expected to take place. Because NGC 4337 is much richer in stars than these clusters, it is an ideal target to compare its CMD with stellar models (Bertelli et al.1992; Carraro et al.1993,1994). The NGC 4337 clump is also particularly rich and well defined, allowing for direct comparisons with stellar models of the He-burning phase in this critical mass range (Girardi et al.2000).

In this paper we follow the study of Carraro et al. (2014a) up and present for the first time high-resolution spectroscopy obtained with the FLAMES-UVES spectrograph at ESO Paranal. These data are used to measure the abundance of several elements (such asα, neutron-capture, and iron peak) for the stars in the red clump of NGC 4337. The knowledge of the metal abundance, in turn, allows us to provide more solid estimates of the cluster fundamental parameters (mostly age and distance), and discuss its properties in the framework of the Milky Way structure and chemical evolution.

The paper is organised as follows: in Sect. 2 we present the observational material and describe how radial velocities are derived. Section 3 is devoted to the abundance analysis, while in Sect. 4 we discuss the results of our analysis in detail. Section 5 summarises our findings.

2. Observations and data reduction

Observations were taken in service mode on the night of March 30, 2014 using the multi-object fibre-fed FLAMES facility mounted at the ESO-VLT/UT2 telescope at the Paranal Observatory (Chile). Two 2775 s exposures were taken simultaneously with the GIRAFFE medium-resolution spectrograph, and the red arm of the UVES high-resolution spectrograph. GIRAFFE was configured in Medusa mode in the setup HR15N, which covers the wavelength range 6470–6790 Å  at a resolution ofR = 17 000. This set-up was chosen because it simultaneously includes the Li resonance doublet and the H_αline. The analysis of this data-set will be presented in a forthcoming paper.

The UVES spectrograph was, instead, set up around a 5800 Å  central wavelength, thus covering the 4760–6840 Å  wavelength range and providing a resolution ofR ≃ 47 000.

Here we discuss the UVES data. The UVES fivers were placed on probable red-clump targets, and are shown on top of the cluster’sV vs.V −I CMD in Fig.1. Table1 presents the target star IDs, coordinates, andB,V, andI photometry from Carraro et al. (2014a). The data were reduced using the ESO CPL based FLAMES-UVES pipeline version 5.3.0¹ to extrac the individual fibre spectra.

The spectra were eventually normalised using the standard IRAF taskcontinuum. Radial velocities were computed using the IRAF/fxcortask to cross-correlate the observed spectra with a synthetic spectrum from the library of Coelho et al. (2005) with stellar parametersT_eff = 4750 K,log g = 2.0, solar metallicity, and noα-enhancement. The IRAFrvcorrecttask was used to calculate the correction from geocentric velocities to heliocentric.

The seven stars observed with UVES have the same heliocentric radial velocity within the uncertainty (see Table1), supporting the idea that they are all cluster members. Therefore, the mean heliocentric radial velocity of NGC 4337RV = −17.75 ± 0.81 km s^-1.

Fig. 1 Colour–magnitude diagram of NGC 4337. Red filled circles identify the seven red clump stars observed with UVES.

3. Abundance analysis

The chemical abundances for Na, Mg, Al, Si, Ca, Ti, Cr, Fe, and Ni were obtained using the equivalent widths of species transition lines (EW method, as detailed in Marino et al.2008). For C, N, O, Y, Ba, La, and Eu, whose lines are affected by blending, we used the spectrum-synthesis method. For this purpose we calculated five synthetic spectra with different abundances for the elements, and estimated the best-fitting value as the one that minimises the rms scatter. Only lines un-contaminated by telluric lines were used. ATLAS9 (Kurucz1970) model atmospheres were used for the EW and spectrum-synthesis methods. The initial atmospheric parameters for the model atmosphere were assumed to be those typical for an RGB star of an open cluster, that isT_eff = 4500 K, log g = 2.5,v_t = 1.20 km s^-1, and[Fe/H] = 0.0. We then refined them during the abundance analysis. As a first step, atmospheric models were calculated using ATLAS9 (Kurucz1970) with the initial estimates ofT_eff,log g,v_t, and [Fe/H].

The values ofT_eff,v_t, andlog g were adjusted and new atmospheric models calculated in an interactive way to remove trends in excitation potential (EP) and equivalent widthvs. abundance forT_eff andv_t, respectively, and to satisfy the ionisation equilibrium forlog g. Fe iand Fe iiwere used for this purpose. The [Fe/H] value of the model was changed at each iteration according to the output of the abundance analysis (see Table2). The local thermodynamic equilibrium (LTE) program MOOG (Sneden1973) was used for the abundance analysis.

In all the analysis, we closely followed Carraro et al. (2014b). We therefore refer to this study for additional details. We briefly recall that typical internal errors areΔ(T_eff) = 50 K,Δlog g = 0.2 dex,Δv_t = 0.10 km s^-1, andΔ [Fe/H] = 0.05 dex.

The line lists for the chemical analysis were obtained from many sources (Gratton et al. 2003, VALD & NIST²; McWilliam & Rich1994; McWilliam1998, SPECTRUM³, and SCAN⁴), and the log gf were calibrated using the solar-inverse technique and by the spectral synthesis method, as discussed in full detail by Villanova et al. (2009). For this purpose we used the high-resolution, high signal-to-noise ratio NOAO solar spectrum (Kurucz et al.1984). The solar abundances we obtained with our line list are reported in Table4, together with those given by Grevesse & Sauval (1998) for comparison. We emphasise that all the line-lists were calibrated on the Sun, including those used for the spectral synthesis. We provided the line list as a long table in Carraro et al. (2014b). In addition, the C content was obtained from the C₂ system at 563.2 nm, and N from the CN lines at 634 nm.

Abundances for C, N, and O were determined all together in an interactive way to take into account any possible molecular coupling of these three elements. Our targets are objects evolved off the main sequence, so some evolutionary mixing is expected. This can affect the primordial C and N abundances separately, but not the total C+N+O content because these elements are transformed one into the other during the CNO cycle.

Fig. 2 Comparison between NGC 4337 meanα-element ratios (black solid square) including error bars derived from Table 5, with data from old open clusters in the inner disc from Magrini et al. (2010; blue triangles) and inner disc giants from Bensby et al. (2010; grey dots). The black solid circle indicates Trumpler 20 from Carraro et al. (2014b), and the red circles are NGC 4815 and NGC 6705 from Magrini et al. (2014).

4. Results of abundance analysis

In this section, we discuss in detail the outcome of the abundance analysis and its impact on the determination of the cluster parameters.

4.1. Metallicity andα elements

Table2 lists the metallicity, measured as [Fe/H], of the seven clump stars we observed with UVES. The mean value is[Fe/H] = 0.12 ± 0.01, with very small dispersion (see also Table4). This is the very first estimate of the metallicity of NGC 4337 , and the value we obtained is well within the expectations for a cluster located inside the solar ring (Magrini et al.2010,2014). It is indeed quite similar to Trumpler 20 (Carraro et al.2014b; Magrini et al.2014), an open cluster located very close to NGC 4337.

In Fig.2 we plot the trend of averagedα-element abundance of NGC 4337 versus metallicity, an compare them with different objects, The comparison is against K giants in the inner disc taken from Bensby et al. (2010) study. Besides, we also show a few inner disc open clusters: Trumpler 20 (Carraro et al.2014b), NGC 4815 and NGC 6705 (Magrini et al.2014), and NGC 6404, NGC 6503, and NGC 6192 (Magrini et al.2010). Solar abundances are indicated with dotted lines.

The agreement is in general very good, and all these clusters appear to be members of the same stellar population. The exception is [Mg/Fe], which shows a quite significant scatter. This was also reported present in Magrini et al. (2014), because Trumpler 20 shows a Mg under-abundance with respect to the Sun, similar to the clusters studied in Magrini et al. (2010). NGC 4337, instead, comfortably lies in the general trend defined by K giants. This is true not only for Mg, but for all the otherα-elements.

4.2. Iron peak elements

We culled from the literature the abundances of thin- and thick-disc stars iron peak element (Ni and Cr, Reddy et al.2003,2006) and compare them with our results for NGC 4337 in Fig.3. We also considered, as in Fig.2, old open clusters in the inner disc. The upper panel shows Cr abundance ratio, while the lower show Ni. Solar abundances are indicated with dotted lines.

As emphasised already in the past (Carraro et al.2014b), the sample of Reddy et al. do not have many stars with the same metallicity as inner disc star clusters. In spite of this limitation, clusters and stars shows essentially the same trend. NGC 4337, however, shows a significant overabundance in [Ni/Fe], compared to other clusters. In [Cr/Fe], lastly, it shows a basically solar abundance.

Fig. 3 Mean Ni (lower panel), and Cr (upper panel) abundance ratios for NGC 4337 giants (filled black squares), compared with thin-disc stars (large red open circles), thick-disc stars (grey symbols), and inner disc open clusters (Magrini et al.2010, blue triangles), Magrini et al. (2014, green empty circles), and Trumpler 20 (black filled circle).

4.3. Neutron-capture elements

There currently is a lively discussion on the Ba and the Y overabundance in star clusters and associations and its origin. According to recent studies (Mishenina et al.2013), star clusters for which Ba and Y were measured tend to exhibit a Ba overabundance with respect to the Sun, and this overabundance correlates with age, namely it increases at decreasing age. In addition, for clusters younger than 3–4 Gyr, the Ba abundance shows a large scatter.

Our results are shown in Fig.4, where NGC 4337 is compared with Trumpler 20 and the sample of old open clusters from Mishenina et al. (2013). Thin- and thick-disc stars from Reddy et al. (2003,2006) are also plotted. Both NGC 4337 and Trumpler 20 are underabundant in Y, and are the only open clusters known to shown such underabundance above solar metallicity. NGC 4337 appears to be Ba underabundant with respect to the Sun. This behaviour is unique among open clusters more metal-rich than the Sun.

Fig. 4 Mean Ba (lower panel) and Y (upper panel) abundance ratios for NGC 4337 giants (filled black squares), compared with thin-disc stars (large red open circles), thick-disc stars (grey symbols), and old open clusters (blue triangles, from Mishenina et al.2013). Lastly, the filled black circle indicate Trumpler 20.

5. Fundamental parameters of NGC 4337

We derive in this section updated estimates of the basic parameters of NGC 4337 based on the results of the previous section. To this aim we generate isochrones using the stellar models from the Padova group (Bressan et al.2012) by adopting a metal content[Fe/H] = 0.12 ± 0.05, which translates intoZ = 0.025. We generated several isochrones, and obtained the best fit for an age of1.6 ± 0.1 Gyr. The quality of the fit was judged by visually inspecting the CMD, with particular attention on the main sequence (MS) turn-off (TO) region, the MS slope, and the red clump. The best fit is shown in Fig.5.

As a result, we estimate the reddening towards NGC 4337 to beE(B −V) = 0.23 ± 0.05, and its apparent distance modulus(m −M)_V = 12.80 ± 0.15. This implies a heliocentric distance of2.6 ± 0.2 kpc, which places the cluster at 200 pc above the Galactic plane and 7.6 kpc from the Galactic centre.

Having a more solid handle on the cluster metallicity and reddening, we re-compute – as an internal sanity check – the stars’T_eff using Alonso et al. (1999) calibrations for(B −V) colours. We find that the differences inT_eff do not exceed 80K, and are in most case smaller than 20 K. This is because the reddening adopted to deriveT_eff estimates in Table2 is only 0.03 mag larger (0.26, Carraro et al.2014a) than the reddening estimated in this paper, and the metallicity only marginally super-solar.

Fig. 5 V/B −V CMD of NGC 4337 stars within 5 arcmin from the cluster centre. Super-imposed (red line) areZ = 0.025 metallicity isochrones for the ages of 1.5, 1.6, and 1.7 Gyr. The inferred reddening and apparent distance modulus areE(B −V) = 0.23 ± 0.05 and(m −M)V = 12.80 ± 0.15.

Fig. 6 Inner disc radial abundance gradient from Magrini et al. (2010,2014; blue and red symbols, respectively) with the addition of Trumpler 20 (black circle) and NGC 4337 (black square). The dotted line is a weighted least square fit to the points, that yields− 0.12 as value of the slope.

In Fig.6 we show an updated version of the radial metallicity gradient in the inner disc. Differently to Carraro et al. (2014b) we added NGC 4337 (solid square) and NGC 6705 and NGC 4815 from Magrini et al. (2014, red symbols). NGC 4337 follows the trend defined by Magrini et al. (2010) sample, and Trumpler 20 very well. Including of NGC 4815 and NGC 6705, which clearly seem do deviate from the main relation, significantly decreases the slope of the gradient to d[Fe/H]/dR = −0.12 ± 0.10 dex/kpc, and increases the metallicity scatter at any distance. We caution, however, that these two clusters are significantly younger. Lastly, we note that an almost flat gradient would result if the two most metal-rich clusters, namely NGC 6583 and NGC 6253, were removed.

6. Discussion and conclusions

We have presented the first high-resolution spectroscopic study of the inner disc, old open cluster NGC 4337. Our main results are as follows:

(i): NGC 4337 has a marginally super-solar metalcontent([Fe/H] = 0.12 ± 0.05) – theα-elements are essentially solar, while we detect a significant underabundance of Ba, unexpected in a star cluster with this metallicity. Y is also underabundant, similarly to Trumpler 20, and at odds with other clusters;

(ii): we refine the results of Carraro et al. (2014a), and estimate an age of1.6 ± 0.1 Gyr for the cluster.

(iii): with this metallicity, and a Galacto-centric distance of 7.6 kpc, NGC 4337 fits in the inner disc radial metallicity gradient very well.

Now that we independently estimate the age and metallicity of NGC 4337, we can compare it again with IC 4651. According to Anthony-Twarog et al.2009), IC 4651 is 1.5 Gyr old for a metallicity[Fe/H] = 0.12 (see also Carretta et al.2004), identical to the metallicity of NGC 4337. It has a reddeningE(B −V) ~ 0.12, and an apparent distance modulus(m −M) ~ 10.40.

Fig. 7 Comparison of NGC 4337 (right panel) with IC 4651 (left panel). The dashed line indicates the TO magnitude of IC 4651, which NGC 4337 has been shifted to for comparison purposes. The blue segment shows the estimate of the parameterΔV. Best-fit values for the clusters’ fundamental parameters are written in the top of the panels.

We compare the two clusters in Fig.7. The blue segment shows the estimate of the parameterΔV, defined as the magnitude difference between the blue TO and the red clump magnitude. This parameter is a very well-known relative age indicator (Carraro & Chiosi1994), independent on reddening, and with some dependence on metallicity. A higherΔV values means an older age. In this case, theΔV for IC 4651 and NGC 4337 are 2.1 and 1.6 mag.

Fig. 8 Comparison of NGC 4337 (right panel) with NGC 752 (left panel). The dashed line indicates the TO magnitude of NGC 752, which NGC 4337 has been shifted to for comparison purposes. Best-fit values for the clusters’ fundamental parameters are written in the top of the panels.

Super-imposed on the NGC 4337 stars is the best-fit isochrone discussed in Sect. 5. Since NGC 4337 and IC 4651 have the very same metallicity, we super-imposed the same isochrone on top of IC 4651. A 1.6 Gyr isochrone misses the clump, which is clearly brighter and at the same time does not reproduce the TO curvature and extension well.

This evidence, in tandem with the higher value ofΔV, suggests that IC 4651 is significantly older than NGC 4337. In our scale (the Padova models), IC 4651 would in fact be about 1.9 Gyr old. This age would be consistent with a lower reddeningE(B −V) ~ 0.09 mag, and a smaller apparent distance modulus(m −M)_V ~ 10.15 mag.

Therefore, although they share the same metallicity, NGC 4337 and IC 4651 do have significantly different ages.

We found NGC 752 (Anthony-Twarog & Twarog2006) to be a stronger case for a NGC 4337 twin. NGC 752 has a marginally lower metallicity ([Fe/H] = 0.08 ± 0.04, Carrera & Pancino2011) which appears to be very similar to NGC 4337 one within the uncertainties, however.

The comparison is illustrated in Fig.8, where the CMD of NGC 4337 is compared to the CMD of NGC 752 from Francic (1989). We adopted for both cluster the same metallicity ([Fe/H] = 0.012) and the same age (1.6 Gyr). The fit is remarkably good in both cases, strongly suggesting that these two clusters share the same chemical and evolutionary phase.

While the clump in both clusters is equally populated and possibly delineates the same evolutionary phase (Girardi et al.2000), the real difference among these two clusters is in the MS, which for NGC 752 shows a significant star-smearing immediately below the TO. It is indeed impossible to follow the cluster MS belowV ~ 11.50 mag. This is interpreted as a signature that NGC 752 has undergone quite a strong dynamical evolution and is on the verge of dissolving into the general Galactic field. Since the two clusters are coeval, this suggests that either NGC 4337 formed as a more massive cluster than NGC 752, or that the latter experienced a much stronger tidal interaction with the Milky Way than the former.

Because it is more massive, and hence has retained more stars, NGC 4337 is an ideal object in which to compare the star distribution in the CMD against stellar evolution models in a statistical manner.

Acknowledgments

S. Villanova gratefully acknowledges the support provided by FONDECYT program N. 1130721. G. Carraro expresses his gratitude to B. Twarog for his very useful comments. The ESO Director General is deeply thanked for granting time to this project via the Director General Discretionary Time (DDT).

References

All Tables

All Figures

	Fig. 1 Colour–magnitude diagram of NGC 4337. Red filled circles identify the seven red clump stars observed with UVES.
In the text

Fig. 2 Comparison between NGC 4337 meanα-element ratios (black solid square) including error bars derived from Table 5, with data from old open clusters in the inner disc from Magrini et al. (2010; blue triangles) and inner disc giants from Bensby et al. (2010; grey dots). The black solid circle indicates Trumpler 20 from Carraro et al. (2014b), and the red circles are NGC 4815 and NGC 6705 from Magrini et al. (2014).

In the text

	Fig. 3 Mean Ni (lower panel), and Cr (upper panel) abundance ratios for NGC 4337 giants (filled black squares), compared with thin-disc stars (large red open circles), thick-disc stars (grey symbols), and inner disc open clusters (Magrini et al.2010, blue triangles), Magrini et al. (2014, green empty circles), and Trumpler 20 (black filled circle).
In the text

	Fig. 4 Mean Ba (lower panel) and Y (upper panel) abundance ratios for NGC 4337 giants (filled black squares), compared with thin-disc stars (large red open circles), thick-disc stars (grey symbols), and old open clusters (blue triangles, from Mishenina et al.2013). Lastly, the filled black circle indicate Trumpler 20.
In the text

	Fig. 5 V/B −V CMD of NGC 4337 stars within 5 arcmin from the cluster centre. Super-imposed (red line) areZ = 0.025 metallicity isochrones for the ages of 1.5, 1.6, and 1.7 Gyr. The inferred reddening and apparent distance modulus areE(B −V) = 0.23 ± 0.05 and(m −M)V = 12.80 ± 0.15.
In the text

	Fig. 6 Inner disc radial abundance gradient from Magrini et al. (2010,2014; blue and red symbols, respectively) with the addition of Trumpler 20 (black circle) and NGC 4337 (black square). The dotted line is a weighted least square fit to the points, that yields− 0.12 as value of the slope.
In the text

	Fig. 7 Comparison of NGC 4337 (right panel) with IC 4651 (left panel). The dashed line indicates the TO magnitude of IC 4651, which NGC 4337 has been shifted to for comparison purposes. The blue segment shows the estimate of the parameterΔV. Best-fit values for the clusters’ fundamental parameters are written in the top of the panels.
In the text

	Fig. 8 Comparison of NGC 4337 (right panel) with NGC 752 (left panel). The dashed line indicates the TO magnitude of NGC 752, which NGC 4337 has been shifted to for comparison purposes. Best-fit values for the clusters’ fundamental parameters are written in the top of the panels.
In the text

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.