Photometric and kinematic studies of open star clusters

Sanner, J.; Brunzendorf, J.; Will, J. M.; Geffert, M.

doi:10.1051/0004-6361:20010196

Cited by 60 publications

(136 citation statements)

References 35 publications

(52 reference statements)

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“…The almost 3σ discrepancy between the cluster's proper motion results obtained by this work, D06, and Sanner et al (2000), may be caused by the different materializations of the HIPPARCOS reference system. As for UCAC2, PM2000 is linked to HIPPARCOS as materialized by Tycho-2.…”

Section: Ngc 2194contrasting

confidence: 56%

“…NGC 2194 is an open cluster located in a moderately rich field projected along the Galactic anti-centre direction, which has been studied by Kyeong et al (2005), Piatti et al (2003), and Sanner et al (2000). Only the final of these three aforementioned studies deals with proper motions.…”

Section: Ngc 2194mentioning

confidence: 99%

“…Only the final of these three aforementioned studies deals with proper motions. Sanner et al (2000) were the first to analyse this object's proper motion. In their study, proper motions were obtained by using photographic plates from the Bonn Doppelrefraktor (first plate from 14.02.1917) and from CCD observations performed at the 1.23 m telescope at the Calar Alto Observatory (15.10.1998).…”

Section: Ngc 2194mentioning

confidence: 99%

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Kinematic parameters and membership probabilities of open clusters in the Bordeaux PM2000 catalogue

Krone-Martins

Soubiran

Ducourant

et al. 2010

A&A

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Aims. We derive lists of proper-motions and kinematic membership probabilities for 49 open clusters and possible open clusters in the zone of the Bordeaux PM2000 proper motion catalogue (+11 • ≤ δ ≤ +18 • ). We test different parametrisations of the proper motion and position distribution functions and select the most successful one. In the light of those results, we analyse some objects individually. Methods. We differenciate between cluster and field member stars, and assign membership probabilities, by applying a new and fully automated method based on both parametrisations of the proper motion and position distribution functions, and genetic algorithm optimization heuristics associated with a derivative-based hill climbing algorithm for the likelihood optimization.Results. We present a catalogue comprising kinematic parameters and associated membership probability lists for 49 open clusters and possible open clusters in the Bordeaux PM2000 catalogue region. We note that this is the first determination of proper motions for five open clusters. We confirm the non-existence of two kinematic populations in the region of 15 previously suspected non-existent objects.

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Section: Ngc 2194contrasting

confidence: 56%

Section: Ngc 2194mentioning

confidence: 99%

Section: Ngc 2194mentioning

confidence: 99%

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Kinematic parameters and membership probabilities of open clusters in the Bordeaux PM2000 catalogue

Krone-Martins

Soubiran

Ducourant

et al. 2010

A&A

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“…Feast (1963) 0 .48 ± 0.01 11.86 ± 0.14 2360 · · · Kennedy (1966) 0.46 11.9 Becker & Fenkart (1971) 0.31 Perry et al (1976) 0 .40 ± 0.01 11.8 ± 0.2 · · · 7 Shobbrook (1984) 0 . 3 8 1 1 .4 ± 0.1 Sanner et al (2001) 0 .36 ± 0.02 11.6 ± 0.2 2100 ± 200 10 ± 5 McSwain & Gies (2005) 0.38 11.80 2290 7 This work 0.30 12.10 ± 0.39 2630 ± 475 11…”

Section: (B8 V)mentioning

confidence: 84%

Open clusters

Aidelman

Cidale

Zorec

et al. 2012

A&A

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Context. Spectroscopic investigations of galactic open clusters are scarce and limited to a reduced sample of cluster members. Aims. We intend to perform a complete study of the physical parameters of two galactic clusters as well as of their individual members. Methods. To carry out this study, we used the BCD (Barbier-Chalonge-Divan) spectrophotometric system, which is based on the study of the Balmer discontinuity and is independent of interstellar and circumstellar extinction. Additional physical properties were derived from the line profiles (FWHM) and stellar evolution models. We analyzed low-resolution spectra around the Balmer discontinuity for normal B-type and Be stars in two open clusters: NGC 3766 and NGC 4755. We determined the stellar fundamental parameters, such as effective temperatures, surface gravities, spectral types, luminosity classes, absolute and bolometric magnitudes, and color gradient excesses. The stellar rotation velocity was also determined. Complementary information, mainly stellar mass, age, and radius of the star population were calculated using stellar evolution models. In some cases, the stellar fundamental parameters were derived for the first time. The obtained results allowed us also to determine the reddening, age, and distance to the clusters. Results. The cluster parameters obtained through the BCD method agree very well with those derived from classical methods based on photometric data. The BCD system also provides physical properties of the star members. This study enables us to test the good behavior of M bol (λ 1 , D)-calibrations and detect systematic discrepancies between log g estimates from model atmospheres and those derived from stellar evolution models. To improve our knowledge on the formation and evolution of the clusters, more statistical studies on the initial mass luminosity and angular momentum distributions should be addressed. Therefore, the BCD spectrophotometric system could be a powerful tool for studying far galactic and extragalactic clusters with the generation of large telescopes and the multi-object technique.

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“…The slope is Γ ∼ 1.3 − 1.4 out to stellar masses greater than 100 M ⊙ (Massey & Hunter 1998). In addition, h and χ Persei (Slesnick, Hillenbrand & Massey 2002), NGC 604 in M33 (González Delgado & Pérez 2000), NGC 1960 and NGC 2194 (Sanner et al 2000), NGC 6611 (Belikov et al 2000) and many other clusters have Salpeter IMFs (e.g., Sakhibov & Smirnov 2000;Sagar, Munari, & de Boer 2001). Massey & Hunter (1998) concluded that the Salpeter IMF occurs in star-forming regions spanning a factor of 200 in density.…”

Section: Clustersmentioning

confidence: 99%

The Initial Mass Function in Starbursts

Elmegreen

2005

Starbursts

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The history of the IMF in starburst regions is reviewed. The IMFs are no longer believed to be top-heavy, although some superstar clusters, whether in starburst regions or not, could be. Introduction: History of Starburst IMFsEarly starburst observations suggested the luminous mass from young massive stars is comparable to the dynamical mass from the rotation curve (see reviews in Telesco 1988; Scalo 1990; Zinnecker 1996; Leitherer 1999). This implied there was a deficit in low mass stars. The nearby starburst galaxy, M82, was one of the best cases. Rieke et al. (1980Rieke et al. ( , 1993 modeled M82's gas mass, luminous star mass, rotation curve mass, 2.2 µm flux, Lyman continuum flux, CO index for supergiants, and the Brα/Brγ ratio, giving an extinction A V = 25 mag. They concluded that only the usual IMF models with lower mass limits M L > 3 − 6 M ⊙ worked. Kronberg et al. (1985) used the Lyman continuum flux from radio emission in M82 to determine the star formation rate, and used the total gas mass combined with an efficiency estimate to conclude that the IMF is top-heavy compared to the Miller & Scalo (1979) IMF. Bernlohr (1992 fit the same M82 properties as Rieke et al., plus the heavy element abundance and FIR line ratios, and concluded that either the IMF slope is shallower than the Scalo (1986) IMF by 1, or there is a lower mass cutoff greater than 1.5-2

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Photometric and kinematic studies of open star clusters

Cited by 60 publications

References 35 publications

Kinematic parameters and membership probabilities of open clusters in the Bordeaux PM2000 catalogue

Kinematic parameters and membership probabilities of open clusters in the Bordeaux PM2000 catalogue

Open clusters

The Initial Mass Function in Starbursts

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