Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682)

Pancino, E.; Carrera, R.; Rossetti, E.; Gallart, Carme

doi:10.1051/0004-6361/200912965

Cited by 194 publications

(265 citation statements)

References 197 publications

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“…The gradients defined by OCs have been the subject of previous studies. The current picture suggests a gradient for [Fe/H] of about −0.06 dex kpc −1 (Friel et al 2002;Pancino et al 2010) to −0.20 dex kpc −1 (Frinchaboy et al 2013) in the radial range 5 to 10 kpc with a nearly flat trend (−0.02 dex kpc −1 ) over the entire radial extent of the disc at Rgc >12 kpc, with a break occurring around 11 kpc Pancino et al 2010;Yong et al 2012;Frinchaboy et al 2013). We show in figure 4, the run of [Fe/H] versus Rgc (top panel) and [α/Fe] versus Rgc (bottom panel) for the present homogeneous sample of 79 OCs (a total of 28 OCs from our study and 51 OCs from the literature).…”

Section: Radial Abundance Distribution Of Ocs and The Field Starsmentioning

confidence: 80%

“…Abundance gradients in the Milky Way can be measured using a wide variety of tracers including the young population of H ii regions, OB stars, and Cepheid variables, and planetary nebulae of different ages, cool unevolved stars and red giants in the field (see for example, Magrini et al 2010;Cheng et al 2012;Hayden et al 2014) and in open clusters (OCs; Friel et al 2002Friel et al , 2010Magrini et al 2010;Pancino et al 2010;Yong et al 2012;Frinchaboy et al 2013). The cooler main sequence stars or red giants which are members of OCs provide not only abundance estimates for elements sampling all the major processes of stellar nucleosynthesis -but a collection of stars whose age, distance, kinematics and metallicity can be measured with greater certainty than for field stars.…”

Section: Introductionmentioning

confidence: 99%

“…All these clusters save NGC 2099, NGC 2287, NGC 2632 and NGC 6633 are analysed for the first time. The chemical content of NGC 2099 was previously measured for the elements Na, Al, α-elements (Mg, Si, Ca, and Ti), iron-peak elements (Sc, V, Cr, Fe, Co, and Ni), and the s-process elements (Y, Ba, La, and Nd) by Pancino et al (2010). The chemical composition of NGC 2632 was estimated previously for the elements Na, Al, Si, Ca, Ti, Cr, Fe and Ni by Pace, Pasquini & François (2008), and for 17 elements in the range from O to Ba by Yang, Chen & Zhao (2015).…”

Section: Introductionmentioning

confidence: 99%

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The evolution of the Milky Way: new insights from open clusters

Reddy¹,

Lambert²,

Giridhar³

2016

Mon. Not. R. Astron. Soc.

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We have collected high-dispersion echelle spectra of red giant members in the twelve open clusters (OCs) and derived stellar parameters and chemical abundances for 26 species by either line equivalent widths or synthetic spectrum analyses. We confirm the lack of an age−metallicity relation for OCs but argue that such a lack of trend for OCs arise from the limited coverage in metallicity compared to that of field stars which span a wide range in metallicity and age. We confirm that the radial metallicity gradient of OCs is steeper (flatter) for R gc < 12 kpc (>12 kpc). We demonstrate that the sample of clusters constituting a steep radial metallicity gradient of slope −0.052±0.011 dex kpc −1 at R gc < 12 kpc are younger than 1.5 Gyr and located close to the Galactic midplane (| z| < 0.5 kpc) with kinematics typical of the thin disc. Whereas the clusters describing a shallow slope of −0.015±0.007 dex kpc −1 at R gc > 12 kpc are relatively old, thick disc members with a striking spread in age and height above the midplane (0.5 < | z| < 2.5 kpc). Our investigation reveals that the OCs and field stars yield consistent radial metallicity gradients if the comparison is limited to samples drawn from the similar vertical heights. We argue via the computation of Galactic orbits that all the outer disc clusters were actually born inward of 12 kpc but the orbital eccentricity has taken them to present locations very far from their birthplaces.

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Section: Radial Abundance Distribution Of Ocs and The Field Starsmentioning

confidence: 80%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The evolution of the Milky Way: new insights from open clusters

Reddy¹,

Lambert²,

Giridhar³

2016

Mon. Not. R. Astron. Soc.

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“…Finally the spectra were summed -after correcting for radial velocity shifts -to produce one single spectrum for each of the six observed stars. Radial velocities were obtained with DAOSPEC 2 (Stetson & Pancino 2008) and the procedure described by Pancino et al (2010). In short, the laboratory wavelength of selected absorption lines (Sect.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

The subgiant branch ofω Centauri seen through high-resolution spectroscopy

Pancino¹,

Mucciarelli²,

Sbordone³

et al. 2011

A&A

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

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“…These studies have confirmed the steep slope in the gradient for 7 kpc < R GC < 11 kpc and have shown that the distribution becomes flatter for Galactocentric distances (R GC ) above 11−12 kpc (cf. Magrini et al 2009, hereafter M09, but see Pancino et al 2010 for a different view).…”

Section: Introductionmentioning

confidence: 99%

Open clusters towards the Galactic centre: chemistry and dynamics

Magrini

Randich

Zoccali

et al. 2010

A&A

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Context. In the framework of the study of the Galactic metallicity gradient and its time evolution, we present new high-resolution spectroscopic observations obtained with FLAMES and the fiber link to UVES at VLT of three open clusters (OCs) located within ∼7 kpc from the Galactic centre (GC): NGC 6192, NGC 6404, NGC 6583. We also present new orbit determination for all OCs with Galactocentric distances (R GC ) ≤ 8 kpc and metallicity from high-resolution spectroscopy. Aims. We aim to investigate the slope of the inner disc metallicity gradient as traced by OCs and to discuss its implication for the chemical evolution of our Galaxy. Methods. We have derived memberships of a group of evolved stars for each clusters, obtaining a sample of 4, 4, and 2 member stars in NGC 6192, NGC 6404, and NGC 6583, respectively. Using standard LTE analysis we derived stellar parameters and abundance ratios for the iron-peak elements Fe, Ni, Cr, and for the α-elements Al, Mg, Si, Ti, Ca. We calculated the orbits of the OCs currently located within 8 kpc from the GC, and discuss their implication on the present-time radial location. Results. The average metallicities of the three clusters are all oversolar: [Fe/H] = +0.12±0.04 (NGC 6192), +0.11±0.04 (NGC 6404), +0.37 ± 0.03 (NGC 6583). They are in qualitative agreement with their Galactocentric distances, because they are all internal OCs, and expected to be more metal rich than the solar neighbourhood. The abundance ratios of the other elements over iron [X/Fe] are consistent with solar values. Conclusions. The clusters we have analysed confirm, together with other OC and Cepheid data, a steep gradient in the inner disc, a signature of an evolutionary rate that is different from the one in the outer disc.

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Chemical abundance analysis of the open clusters Cr 110, NGC 2099 (M 37), NGC 2420, NGC 7789, and M 67 (NGC 2682)

Cited by 194 publications

References 197 publications

The evolution of the Milky Way: new insights from open clusters

The evolution of the Milky Way: new insights from open clusters

The subgiant branch ofω Centauri seen through high-resolution spectroscopy

Open clusters towards the Galactic centre: chemistry and dynamics

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