Morphological analysis of open clusters’ properties

Tadross, A. L.; Werner, PN; Osman, Anas; Marie, M.

doi:10.1016/s1384-1076(02)00172-0

Cited by 50 publications

(95 citation statements)

References 20 publications

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“…12 (panel a), similar to what has already been observed by, e.g. Lyngå (1982), Tadross et al (2002), and van den Bergh et al (1991). Although with more scatter, a similar relation occurs for cluster size and height over the Galactic plane |Z GC | (panel b).…”

Section: Relations With Cluster Sizesupporting

confidence: 87%

The wide variety of evolutionary stages among 34 unstudied Teutsch open clusters

Bonatto

Bica

2010

A&A

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Context. Close investigations of unstudied open-cluster candidates may improve the statistics of objects undergoing the dissolution phase. Aims. We plan to settle the nature and derive astrophysical (fundamental, structural, and stellar mass content) parameters for 34 unstudied open cluster candidates from the near-infrared Teutsch list. Methods. The analysis employs 2MASS photometry, field-star decontamination (to enhance the intrinsic colour-magnitude diagram morphology), and colour-magnitude filters (for high contrast in stellar radial density profiles). Results. We find 8 clusters younger than ∼30 Myr, 21 with ages within 100-900 Myr, 3 older than 1 Gyr, and possibly 1 as old as ∼7 Gyr. Part of the sample is affected by reddening as high as A V ∼ 9, and about half is located more than d ∼ 3 kpc away from the Sun, with a few reaching d = 6−9 kpc. The sample contains essentially low-luminosity clusters in the optical, with M V ≈ −3 ± 3. These properties are consistent with their near-infrared origin. Cluster size increases both with Galactocentric distance and height over the plane, which is consistent with the low level of tidal stress (and field contamination) associated with these regions. The average mass density falls off with cluster radius as ρ ∼ R −3 , which in clusters younger than ∼20 Myr and more massive than ∼10 3 M has been interpreted as diffusion-related cluster expansion. Conclusions. Besides the derivation of astrophysical parameters for a sample of unstudied open clusters, in this paper we identify a set of clusters older than several 10 2 Myr, with 4 of them having survived a few Gyr. Surveys of open cluster candidates should be further explored to fill in the gap between the detected and predicted number of clusters. An improved statistic, especially on the population of clusters in highly evolved phases, can be used to investigate cluster formation rates and constrain the dissolution-time scale in the Galaxy.

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Section: Relations With Cluster Sizesupporting

confidence: 87%

The wide variety of evolutionary stages among 34 unstudied Teutsch open clusters

Bonatto

Bica

2010

A&A

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“…(b) Averages of measurements by West (1967a), Jennens & Helfer (1975), Lyngå (1987), Mermilliod et al (1996), Twarog et al (1997), Kiss et al (2001), Kalirai et al (2001), Nilakshi & Sagar (2002), Grocholski & Sarajedini (2003), Bragaglia & Tosi (2006), and Hartman et al (2008). (c) Averages of measurements by McClure et al (1974), Barbaro & Pigatto (1984), Vandenberg (1985), Lyngå (1987), AnthonyTwarog et al (1990), Carraro & Chiosi (1994), Demarque et al (1994), Twarog et al (1997), Tadross et al (2002), and Grocholski & Sarajedini (2003). (d) Averages of measurements by Racine (1971), Barbaro & Pigatto (1984), Vandenberg (1985), Nissen et al (1987), Hobbs & Thorburn (1991), Gilliland & Brown (1992), Demarque et al (1992), Meynet et al (1993), Montgomery et al (1993), Carraro & Chiosi (1994), Dinescu et al (1995), Fan et al (1996), Twarog et al (1997), Sarajedini (1999), Tadross et al (2002), Grocholski & Sarajedini (2003), VandenBerg & Clem (2003)…”

Section: Linelist Atomic Data and Equivalent Widthsmentioning

confidence: 99%

“…(c) Averages of measurements by McClure et al (1974), Barbaro & Pigatto (1984), Vandenberg (1985), Lyngå (1987), AnthonyTwarog et al (1990), Carraro & Chiosi (1994), Demarque et al (1994), Twarog et al (1997), Tadross et al (2002), and Grocholski & Sarajedini (2003). (d) Averages of measurements by Racine (1971), Barbaro & Pigatto (1984), Vandenberg (1985), Nissen et al (1987), Hobbs & Thorburn (1991), Gilliland & Brown (1992), Demarque et al (1992), Meynet et al (1993), Montgomery et al (1993), Carraro & Chiosi (1994), Dinescu et al (1995), Fan et al (1996), Twarog et al (1997), Sarajedini (1999), Tadross et al (2002), Grocholski & Sarajedini (2003), VandenBerg & Clem (2003), Laugalys et al (2004), andSandquist (2004). (e) Averages of measurements by Burbidge & Sandage (1958), Arp (1962), Strom & Strom (1970), Jennens & Helfer (1975), Janes (1977), Claria (1979), Twarog & Tyson (1985), Lyngå (1987), Mazzei & Pigatto (1988)...…”

Section: Linelist Atomic Data and Equivalent Widthsmentioning

confidence: 99%

“…(d) Averages of measurements by Racine (1971), Barbaro & Pigatto (1984), Vandenberg (1985), Nissen et al (1987), Hobbs & Thorburn (1991), Gilliland & Brown (1992), Demarque et al (1992), Meynet et al (1993), Montgomery et al (1993), Carraro & Chiosi (1994), Dinescu et al (1995), Fan et al (1996), Twarog et al (1997), Sarajedini (1999), Tadross et al (2002), Grocholski & Sarajedini (2003), VandenBerg & Clem (2003), Laugalys et al (2004), andSandquist (2004). (e) Averages of measurements by Burbidge & Sandage (1958), Arp (1962), Strom & Strom (1970), Jennens & Helfer (1975), Janes (1977), Claria (1979), Twarog & Tyson (1985), Lyngå (1987), Mazzei & Pigatto (1988), Friel & Janes (1993), Martinez Roger et al (1994, Janes & Phelps (1994), Twarog et al (1997), Gim et al (1998b), Sarajedini (1999), Vallenari et al (2000), Tadross et al (2002), and Bartašiutė & Tautvaišienė (2004).…”

Section: Linelist Atomic Data and Equivalent Widthsmentioning

confidence: 99%

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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)

Pancino

Carrera

Rossetti

et al. 2010

A&A

194

206

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Context. The present number of Galactic Open Clusters that have high resolution abundance determinations, not only of [Fe/H], but also of other key elements, is largely insufficient to enable a clear modeling of the Galactic Disk chemical evolution. Aims. To increase the number of Galactic Open Clusters with high quality measurements. Methods. We obtained high resolution (R∼30 000), high quality (S/N∼50-100 per pixel), echelle spectra with the fiber spectrograph FOCES, at Calar Alto, Spain, for three red clump stars in each of five Open Clusters. We used the classical Equivalent Width analysis method to obtain accurate abundances of sixteen elements: Al,

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“…Kharchenko et al 2005;Tadross et al 2002), especially for cluster age. This occurs especially for young clusters in which field contamination has not been properly taken into account.…”

Section: Fundamental Parametersmentioning

confidence: 99%

Astrophysical parameters of 14 open clusters projected close to the Galactic plane

Camargo¹,

Bonatto²,

Bica³

2009

A&A

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Aims. Astrophysical parameters (age, reddening, distance, core and cluster radii) of 14 open clusters (OCs) projected close to the Galactic plane are derived with 2MASS photometry. The OCs are Be 63, Be 84, Cz 6, Cz 7, Cz 12, Ru 141, Ru 144, Ru 172, FSR 101, FSR 1430, FSR 1471, FSR 162, FSR 178, and FSR 198. The OCs Be 63, Be 84, Ru 141, Ru 144, and Ru 172 are studied in more detail than in previous works, while the others have astrophysical parameters derived for the first time. Methods. We analyse the colour−magnitude diagrams (CMDs) and stellar radial density profiles (RDPs) built after field-star decontamination and colour-magnitude filtered photometry. Field-star decontamination is applied to uncover the cluster's intrinsic CMD morphology, and colour−magnitude filters are used to isolate stars with a high probability of being cluster members in view of structural analyses.Results. The open clusters of the sample are located at d = 1.6−7.1 kpc from the Sun and at Galactocentric distances 5.5−11.8 kpc, with age in the range 10 Myr to 1.5 Gyr and reddening E(B−V) in the range 0.19−2.56 mag. The core and cluster radii are in the range 0.27−1.88 pc and 2.2−11.27 pc, respectively. Cz 6 and FSR 198 are the youngest OCs of this sample, with a population of pre-main sequence (PMS) stars, while FSR 178 is the oldest cluster.

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Morphological analysis of open clusters’ properties

Cited by 50 publications

References 20 publications

The wide variety of evolutionary stages among 34 unstudied Teutsch open clusters

The wide variety of evolutionary stages among 34 unstudied Teutsch open clusters

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

Astrophysical parameters of 14 open clusters projected close to the Galactic plane

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