UBVI CCD photometry of M11 — II. New photometry and surface density profiles

Sung, Hwankyung; Bessell, M. S.; Lee, Hyun Chul; Kang, Yong-Woo; Lee, Sang Gak

doi:10.1046/j.1365-8711.1999.02961.x

Cited by 44 publications

(21 citation statements)

References 35 publications

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“…The photometry used to select the target stars is indicated as a footnote. Alcaino (1965); 2 Platais et al (2003); 3 Johnson (1953); 4 Harris & Harris (1977); 5 Pandey et al (2007); 6 Kiss et al (2001); 7 Anthony-Twarog et al (1990); 8 Choo et al (2003); 9 Montgomery et al (1993); 10 Harmer et al (2001); 11 Sung et al (1999); 12 Stetson et al (2003); 13 Rosvick & Vandenberg (1998); 14 Maciejewski & Niedzielski (2007); 15 Kharchenko et al (2005a); 16 Subramaniam & Bhatt (2007); 17 Mochejska & Kaluzny (1999); McNamara & Solomon (1981). a Salaris et al (2004); b Subramaniam & Sagar (1999); c Nilakshi & Sagar (2002); d Vogel et al (2003); e Jeffries et al (2002); f Cantat- ; g Andreuzzi et al (2004); h Kharchenko et al (2005b); i Subramaniam & Bhatt (2007); j Carraro et al (2016) It has only 4 stars in the RC but was included for observation in a night with non optimal weather conditions.…”

Section: Observational Materialsmentioning

confidence: 99%

OCCASO – II. Physical parameters and Fe abundances of red clump stars in 18 open clusters

Casamiquela

Carrera

Blanco-Cuaresma

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Open Clusters have long been used to study the chemo-dynamical evolution of the Galactic disk. This requires an homogeneously analysed sample covering a wide range of ages and distances. In this paper we present the OCCASO second data release. This comprises a sample of high-resolution (R > 65, 000) and high signal-to-noise spectra of 115 Red Clump stars in 18 Open Clusters. We derive atmospheric parameters (T eff , log g, ξ), and [Fe/H] abundances using two analysis techniques: equivalent widths and spectral synthesis. A detailed comparison and a critical review of the results of the two methods are made. Both methods are carefully tested between them, with the Gaia FGK Benchmark stars, and with an extensive sample of literature values. We perform a membership study using radial velocities and the resulting abundances. Finally, we compare our results with a chemo-dynamical model of the Milky Way thin disk concluding that the oldest Open Clusters are consistent with the models only when dynamical effects are taken into account. 65 HERMES 5147 ± 46 2.98 ± 0.07 1.15 ± 0.06 5106 ± 12 2.85 ± 0.04 1.43 ± 0.02 5126 29 28 2.92 0.06 0.09 0.08 ± 0.04 −0.02 ± 0.05 0.05 W119 18:28:17.64 +06:46:00.1 8.95 67 FIES 5138 ± 42 2.84 ± 0.06 1.28 ± 0.06 5203 ± 21 3.02 ± 0.04 1.47 ± 0.03 5170 31 46 2.93 0.05 0.13 0.03 ± 0.05 −0.02 ± 0.05 0.02 70 HERMES 5192 ± 56 3.03 ± 0.07 1.09 ± 0.05 5218 ± 18 3.08 ± 0.04 1.44 ± 0.02 5205 37 18 3.06 0.06 0.04 0.03 ± 0.04 −0.07 ± 0.05 0.05 W126 18:28:22.97 +06:42:29.3 8.77 95 FIES 5054 ± 50 2.55 ± 0.06 1.28 ± 0.09 5131 ± 12 2.80 ± 0.04 1.53 ± 0.02 5092 31 54 2.68 0.05 0.18 −0.01 ± 0.05 −0.04 ± 0.05 0.02 78 HERMES 5190 ± 37 3.07 ± 0.09 1.23 ± 0.05 5174 ± 12 2.92 ± 0.03 1.44 ± 0.02 5182 24

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Section: Observational Materialsmentioning

confidence: 99%

OCCASO – II. Physical parameters and Fe abundances of red clump stars in 18 open clusters

Casamiquela

Carrera

Blanco-Cuaresma

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…About 50 stars were brightened by 0.75 mag adopting the minimum binary fraction of 5 per cent. We found that the adopted U −V colour scale 50 appears to be, on average, about 0.05 bluer than the one 51 used in the reddening determination of the previous study 18 (see Supplementary Fig. 11).…”

Section: Methodsmentioning

confidence: 56%

“…A distance modulus (V − M V ) of 11.55 mag and mean reddening E(U −V ) of 0.74 from a previous study 18 were applied to the synthetic colour-magnitude diagram. Non-negligible differential reddening was found in M11 18 : E(B − V ) ranges from 0.38 to 0.48 mag with a standard deviation of 0.03 mag, which corresponds to 0.05 mag in E(U −V ). The differential reddening was randomly introduced to the synthetic colour-magnitude diagram assuming a Gaussian distribution with the standard deviation.…”

Section: Methodsmentioning

confidence: 99%

“…The differential reddening was randomly introduced to the synthetic colour-magnitude diagram assuming a Gaussian distribution with the standard deviation. The photometric errors in U − V and V provided from the published data 18 were averaged within each V magnitude bin of 1 mag. These mean errors were adopted as the dispersions of the Gaussian distributions.…”

Section: Methodsmentioning

confidence: 99%

“…M11 is an intermediate-age cluster (250 Myr) at 2 kpc distance 18 , having a total mass up to 11000 M ⊙ (Refs. 19 and 20).…”

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confidence: 99%

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Extended main sequence turn-off originating from a broad range of stellar rotational velocities

et al. 2018

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Star clusters have long been considered to comprise a simple stellar population, but this paradigm is being challenged, since apart from multiple populations in Galactic globular clusters 1,2 , a number of intermediate-age star clusters exhibit a significant colour spread at the main sequence turn-off (MSTO) 3,4,5,6,7,8,9,10,11 . A sequential evolution of multiple generations of stars formed over 100-200 million years is a natural explanation of this colour spread 12 . Another approach to explain this feature is to introduce the effect of stellar rotation 13 . However, its effectiveness has not yet been proven due to the lack of direct measurements of rotational velocities. Here we report the distribution of projected rotational velocities (V sin i) of stars in the Galactic open cluster M11, measured through a Fourier transform analysis. Cluster members display a broad V sin i distribution, and fast rotators including Be stars have redder colours than slow rotators. Monte Carlo simulations infer that cluster members have highly aligned spin axes and a broad distribution of equatorial velocities biased towards high velocities. Our findings demonstrate how stellar rotation affects the colours of cluster members, suggesting that the colour spread observed in populous clusters can be understood in the context of stellar evolution even without introducing multiple stellar populations.

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Why have no transiting planets been found in star clusters?

Janes¹,

Kim²

2008

Proc. IAU

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Abstract. Since the suggestion by Janes 1996 that star clusters might be attractive targets to search for transiting planets, there have been more than 20 searches in both open and globular clusters. To date, no confirmed hot Jupiter transiting planets have been found in clusters. We review the statistics for finding short-period planets and we summarize the open cluster work to date, including our own (so far negative) search in NGC 7789. While individually, the negative results are not surprising, the consistent failure to find planets in clusters may suggest differences in the formation or evolution of planetary systems in clusters.

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UBVI CCD photometry of M11 — II. New photometry and surface density profiles

Cited by 44 publications

References 35 publications

OCCASO – II. Physical parameters and Fe abundances of red clump stars in 18 open clusters

OCCASO – II. Physical parameters and Fe abundances of red clump stars in 18 open clusters

Extended main sequence turn-off originating from a broad range of stellar rotational velocities

Why have no transiting planets been found in star clusters?

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