A Survey of Star Clusters in the M31 Southwest Field:<i>UBVRI</i>Photometry and Multiband Maps

Narbutis, D.; Vansevičius, Vladas; Kodaira, Keiichi; Bridžius, A.; Stonkutė, R.

doi:10.1086/586736

Cited by 16 publications

(29 citation statements)

References 21 publications

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“…Hence we see here that the cluster sample is dominated by the magnitude fading until log 10 (t/yr) ∼ 8.5 and that after the cluster disruption phase takes over. This typical lifetime scale is comparable to that derived for the star cluster population in the southwest field of the M 31 galaxy by Vansevičius et al (2009) using a star cluster sample photometry from Narbutis et al (2008).…”

Section: Derived Physical Parameters Of Clusterssupporting

confidence: 80%

Deriving physical parameters of unresolved star clusters

Meulenaer

Narbutis

Mineikis

et al. 2015

A&A

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Context. When trying to derive the star cluster physical parameters of the M 33 galaxy using broad-band unresolved ground-based photometry, previous studies mainly made use of simple stellar population models, shown in the recent years to be oversimplified. Aims. In this study, we aim to derive the star cluster physical parameters (age, mass, and extinction; metallicity is assumed to be LMC-like for clusters with age below 1 Gyr and left free for older clusters) of this galaxy using models that take stochastic dispersion of cluster integrated colors into account. Methods. We use three recently published M 33 catalogs of cluster optical broad-band photometry in standard UBVRI and in CFHT/MegaCam u * g r i z photometric systems. We also use near-infrared JHK photometry that we derive from deep 2MASS images. We derive the cluster parameters using a method that takes into account the stochasticity problem, presented in previous papers of this series. Results. The derived differential age distribution of the M 33 cluster population is composed of a two-slope profile indicating that the number of clusters decreases when age gets older. The first slope is interpreted as the evolutionary fading phase of the cluster magnitudes, and the second slope as the cluster disruption. The threshold between these two phases occurs at ∼300 Myr, comparable to what is observed in the M 31 galaxy. We also model by use of artificial clusters the ability of the cluster physical parameter derivation method to correctly derive the two-slope profile for different photometric systems tested.

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Section: Derived Physical Parameters Of Clusterssupporting

confidence: 80%

Deriving physical parameters of unresolved star clusters

Meulenaer

Narbutis

Mineikis

et al. 2015

A&A

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“…Seventy-seven star clusters from our catalog are located in the HST archive frames. For object selection, photometry, and multiband image details, see Narbutis et al (2008).…”

Section: Datamentioning

confidence: 99%

Compact Star Clusters in the M31 Disk

Vansevičius

Kodaira

Narbutis

et al. 2009

ApJ

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We have carried out a survey of compact star clusters (apparent size 3 ′′ ) in the southwest part of the M31 galaxy, based on the high-resolution Suprime-Cam images (17.5 ′ × 28.5 ′ ), covering ∼15% of the deprojected galaxy disk area. The U BV RI photometry of 285 cluster candidates (V 20.5 mag) was performed using frames of the Local Group Galaxies Survey. The final sample, containing 238 high probability star cluster candidates (typical half-light radius r h ∼ 1.5 pc), was selected by specifying a lower limit of r h 0.15 ′′ ( 0.6 pc). We derived cluster parameters based on the photometric data and multiband images by employing simple stellar population models. The clusters have a wide range of ages from ∼5 Myr (young objects associated with 24 µm and/or Hα emission) to ∼10 Gyr (globular cluster candidates), and possess mass in a range of 3.0 log(m/m ⊙ ) 4.3 peaking at m ∼ 4000 m ⊙ . Typical age of these intermediate-mass clusters is in the range of 30 Myr t 3 Gyr, with a prominent peak at ∼70 Myr. These findings suggest a rich intermediate-mass star cluster population in M31, which appears to be scarce in the Milky Way galaxy.

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“…However, there are 42 clusters for which we cannot obtain accurate photometric measurements with different reasons as following, a) some clusters have one or more nearby very bright objects; b) some clusters are very close to other objects; c) some clusters are very faint and the signal-to-noise ratio (SNR) is low; d) some clusters are superimposed onto a bright background; e) some clusters are superimposed onto a strongly variable background. In addition, There are several remarkable clusters with "adhered" (Vansevičius et al 2009) objects in our images, such as M088 and its neighbor M089, and G099 and C037-G099x (see also Narbutis et al 2008). In a previous paper, Ma et al (2011) presented the SEDs in 15 intermediate-band filters of the BATC photometric system for one YMC VDB0-B195D and determined its age and mass by comparing its SEDs with the theoretical evolutionary population synthesis models.…”

Section: Sample Of Star Clustersmentioning

confidence: 77%

Age and Mass Studies for Young Star Clusters in M31 From Seds-Fit

Wang

Zhang

et al. 2012

The Astronomical Journal

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In this paper, we present photometry for young star clusters in M31, which are selected from Caldwell et al. These star clusters have been observed as part of the Beijing-Arizona-Taiwan-Connecticut (BATC) Multicolor Sky Survey from 1995 February to 2008 March. The BATC images including these star clusters are taken with 15 intermediate-band filters covering 3000-10000Å. Combined with photometry in the GALEX far-and near-ultraviolet, broad-band U BV RI, SDSS ugriz, and infrared JHK s of Two Micron All Sky Survey, we obtain their accurate spectral energy distributions (SEDs) from 1538 − 20000Å. We derive these star clusters' ages and masses by comparing their SEDs with stellar population synthesis models. Our results are in good agreement with previous determinations. The mean value of age and mass of young clusters (< 2 Gyr) is about 385 Myr and 2 × 10 4 M ⊙ , respectively. There are two distinct peaks in the age distribution, a highest peak at age ∼ 60 Myr and a secondary peak around 250 Myr, while the mass distribution shows a single peak around 10 4 M ⊙ . A few young star clusters have two-body relaxation times greater than their ages, indicating that those clusters have not been well dynamically relaxed and therefore have not established the thermal equilibrium. There are several regions showing aggregations of young star clusters around the 10 kpc ring and the outer ring, indicating that the distribution of the young star clusters is well correlated with M31's star-forming regions. The young massive star clusters (age ≤ 100 Myr and mass ≥ 10 4 M ⊙ ) show apparent concentration around the ring splitting region, suggesting a recent passage of a satellite galaxy (M32) through M31 disk.

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A Survey of Star Clusters in the M31 Southwest Field:UBVRIPhotometry and Multiband Maps

Cited by 16 publications

References 21 publications

Deriving physical parameters of unresolved star clusters

Deriving physical parameters of unresolved star clusters

Compact Star Clusters in the M31 Disk

Age and Mass Studies for Young Star Clusters in M31 From Seds-Fit

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