The Sejong Open Cluster Survey (SOS). VII. A Photometric Study of the Young Open Cluster IC 1590

Kim, Seulgi; Lim, Beomdu; Bessell, M. S.; Kim, Jinyoung Serena; Sung, Hwankyung

doi:10.3847/1538-3881/ac0fd9

Cited by 6 publications

(2 citation statements)

References 75 publications

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“…Searching for mass segregation in the youngest clusters can address the question of whether mass segregation may be primordial or largely attributed to dynamical and relaxation processes. Some of the youngest clusters that have been studied observationally for mass segregation include NGC 2264 (3 Myr; Nony et al 2021), NGC 6231 (3-4 Myr;Raboud & Mermilliod 1998), IC 1590 Myr; Kim et al 2021), NGC 2516 (100 Myr; Pera et al 2022), and the Hyades (680 Myr; Evans & Oh 2022).…”

Section: Introductionmentioning

confidence: 99%

Tracing the Origins of Mass Segregation in M35: Evidence for Primordially Segregated Binaries

Motherway,

Geller,

Childs

et al. 2024

ApJL

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M35 is a young open cluster and home to an extensive binary population. Using Gaia Data Release 3, Pan-STARRS, and Two Micron All Sky Survey photometry with the Bayesian statistical software, BASE-9, we derive precise cluster parameters, identify single and binary cluster members, and extract their masses. We identify 571 binaries down to Gaia G = 20.3 and a lower limit on the binary frequency of f b = 0.41 ± 0.02. We extend the binary demographics by many magnitudes faint-ward of previous (radial-velocity) studies of this cluster and further away from the cluster center (1.°78, roughly 10 core radii). We find the binary stars to be more centrally concentrated than the single stars in the cluster. Furthermore, we find strong evidence for mass segregation within the binary population itself, with progressively more-massive binary samples becoming more and more centrally concentrated. For the single stars, we find weaker evidence for mass segregation; only the most massive single stars (>2.5M ⊙) appear more centrally concentrated. Given the cluster age of ∼200 Myr, and our derived half-mass relaxation time for the cluster of 230 ± 84 Myr, we estimate ∼47% of the binary stars and ∼12% of single stars in the cluster have had time to become dynamically mass segregated. Importantly, when we investigate only stars with mass segregation timescales greater than the cluster age, we still find the binaries to be more centrally concentrated than the singles, suggesting the binaries may have formed with a primordially different spatial distribution from that of the single stars.

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Section: Introductionmentioning

confidence: 99%

Tracing the Origins of Mass Segregation in M35: Evidence for Primordially Segregated Binaries

Motherway,

Geller,

Childs

et al. 2024

ApJL

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“…Lim et al (2015a) summarize the findings of several papers that were already published by members of the SOS surveys(Sung & Bessell 2004Hur et al 2012;Sung et al 2013b;Lim et al 2013Lim et al , 2014aLim et al , 2014bLim et al , 2015bLim et al , 2015cHur et al 2015) and others which appeared later(Sung et al 2017;Kim et al 2021). …”

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confidence: 99%

Variation of the High-mass Slope of the Stellar Initial Mass Function: Theory Meets Observations

Dib

2023

ApJ

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We present observational evidence of a correlation between the high-mass slope of the stellar initial mass function (IMF) in young star clusters and their stellar surface density, σ *. When the high-mass end of the IMF is described by a power law of the form dN / d log M * ∝ M * − Γ , the value of Γ is seen to decrease weakly with increasing σ *, following a Γ = 1.31 σ * − 0.095 relation. We also present a model that can explain these observations. The model is based on the idea that the coalescence of protostellar cores in a protocluster-forming clump is more efficient in high-density environments where cores are more closely packed. The efficiency of the coalescence process is calculated as a function of the parental clump properties, in particular the relation between its mass and radius as well as its core formation efficiency. The main result of this model is that the increased efficiency of the coalescence process leads to shallower slopes of the IMF, in agreement with the observations of young clusters, and the observations are best reproduced with compact protocluster-forming clumps. These results have significant implications for the shape of the IMF in different Galactic and extragalactic environments and have very important consequences for galactic evolution.

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A statistical approach to polarimetric and photometric investigation of the intermediate-age open cluster NGC 1912

Biswas,

Medhi,

Deb

et al. 2024

Monthly Notices of the Royal Astronomical Society

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This paper presents a comprehensive multiwavelength investigation of the intermediate-age open cluster NGC 1912. We identified 401 member stars for NGC 1912 using K-nearest neighbour and Gaussian Mixture Model machine learning techniques. The fundamental parameters determined for the cluster are metallicity (z) = 0.0141 $\pm$ 0.0006, log(age) = 8.519 $\pm$ 0.040, binary fraction ($b_{\text{frac}}$) = 0.445 $\pm$ 0.035, visual extinction ($A_V$) = 0.864 $\pm$ 0.033 mag, total-to-selective extinction ratio ($R_V$) = 3.007 $\pm$ 0.096, distance = 1096 $\pm$ 15 pc. The central density ($\rho _o$), core radius ($r_c$), tidal radius ($r_t$), and background density ($\rho _{\mathrm{bg}}$) for the cluster are obtained as 0.643 $\pm$ 0.067 stars arcmin$^{-2}$, 7.743 $\pm$ 0.784 arcmin, 84.633 $\pm$ 7.188 arcmin, and 0.001 $\pm$ 0.000 stars arcmin$^{-2}$, respectively. Dynamical mass segregation study revealed a concentration of some apparently massive stars towards the cluster centre. Polarimetric analysis of 90 stars in $BVR_cI_c$ wavelength bands revealed that the observed polarization in NGC 1912 is not solely attributed to interstellar dust. The Galactic magnetic field is dominant in this region. Dust grain sizes within the intracluster region are found to be relatively smaller than that of the general ISM. The extinction map revealed the existence of a potential ‘interstellar bubble’ located close to the cluster region. Towards the periphery of the probable bubble region, which displays an ovoid-like geometry, 16 probable young stellar objects have been detected, suggesting the ongoing triggering of secondary star formation events in this region.

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The Sejong Open Cluster Survey (SOS). VII. A Photometric Study of the Young Open Cluster IC 1590

Cited by 6 publications

References 75 publications

Tracing the Origins of Mass Segregation in M35: Evidence for Primordially Segregated Binaries

Tracing the Origins of Mass Segregation in M35: Evidence for Primordially Segregated Binaries

Variation of the High-mass Slope of the Stellar Initial Mass Function: Theory Meets Observations

A statistical approach to polarimetric and photometric investigation of the intermediate-age open cluster NGC 1912

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