The Low-mass Population in the Young Cluster Stock 8: Stellar Properties and Initial Mass Function

Jose, Jessy; Herczeg, Gregory J.; Samal, M. R.; Fang, Qiliang; Panwar, Neelam

doi:10.3847/1538-4357/836/1/98

Cited by 37 publications

(51 citation statements)

References 93 publications

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“…Kang et al (2012) discuss an old supernova remnant FVW 172.8+1.5 whose center and south-west arc coincide with the white dashed circle in our Figure 1. Jose et al (2017) also found this envelope on a Herschel-SPIRE image and study a star-formation in the south-western arc toward Sh2-234. So the filamentary structure could be an interesting example to test theoretical models by e.g.…”

Section: Introductionmentioning

confidence: 99%

Molecular gas in high-mass filament WB673

et al. 2017

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Abstract:We studied the distribution of dense gas in a filamentary molecular cloud containing several dense clumps. The center of the filament is given by the dense clump WB 673. The clumps are high-mass and intermediate-mass starforming regions. We observed CS (2-1), 13 CO (1-0), C 18 O (1-0), and methanol lines at 96 GHz toward WB 673 with the Onsala Space Observatory 20-m telescope. We found CS (2-1) emission in the inter-clump medium so the clumps are physically connected and the whole cloud is indeed a filament. Its total mass is 10 4 M ⊙ and mass-to-length ratio is 360 M ⊙ pc −1 from 13 CO (1-0) data. Mass-to-length ratio for the dense gas is 3.4 − 34 M ⊙ pc −1 from CS (2-1) data. The PV-diagram of the filament is V-shaped. We estimated physical conditions in the molecular gas using methanol lines. Location of the filament on the sky between extended shells suggests that it could be a good example to test theoretical models of formation of the filaments via multiple compression of interstellar gas by supersonic waves.

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Section: Introductionmentioning

confidence: 99%

Molecular gas in high-mass filament WB673

et al. 2017

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“…We derived the KLF resulting from field star decontamination in H − K/H colour-magnitude diagram (CMD) of the cluster (see Jose et al 2017, for details of the field star decontamination). Figure 9 reflects the KLF of cluster members.…”

Section: Luminosity Function and Mass Of The Clusters Associated Withmentioning

confidence: 99%

“…In contrast, we find no young Class I sources around S147 and most of Class I sources around S148 are co-spatial with the Class II sources located near the centre of the ionized gas. Since young clusters often harbor Class III to Class I sources as a part of cluster formation process (e.g., Jose et al 2017;Panwar et al 2017Panwar et al , 2018, thus the Class I YSOs of the S148 are most likely part of the central cluster responsible for the ionization of S148. Given the fact that the H ii region S149 located near the boundary of S148 and smaller in size, one can argue that S149 might have been influenced by S148.…”

Section: Star Formation Processes In Pg1083mentioning

confidence: 99%

“…Schneider et al 2012;Kirk et al 2013). As molecular clouds are often comprised of H ii regions, bubbles, and dense filamentary structures (Bieging et al 2009;Mallick et al 2013;Samal et al 2015;Bieging et al 2016;Jose et al 2017), therefore, understanding what shapes the molecular clouds to dense and massive enough to form a young cluster is of great inter-est. Additionally, the initial cloud configuration decides the future location of cluster formation (e.g.…”

Section: Introductionmentioning

confidence: 99%

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The Planck Cold Clump G108.37-01.06: A Site of Complex Interplay between H ii Regions, Young Clusters, and Filaments

Dutta

Mondal

Samal

et al. 2018

ApJ

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The Planck Galactic Cold Clumps (PGCCs) are the possible representations of the initial conditions and the very early stages of star formation. With an objective to understand better the star and star cluster formation, we probe the molecular cloud associated with PGCC G108.37-01.06 (hereafter, PG108.3), which can be traced in a velocity range −57 to −51 km s −1 . The IPHAS images reveal Hα emission at various locations around PG108.3, and optical spectroscopy of the bright sources in those zones of Hα emission disclose two massive ionizing sources with spectral type O8-O9V and B1V. Using the radio continuum, we estimate ionizing gas parameters and find the dynamical ages of H ii regions associated with the massive stars in the range 0.5−0.75 Myr. Based on the stellar surface density map constructed from the deep near-infrared CHFT observations, we find two prominent star clusters in PG108.3; of which, the cluster associated with H ii region S148 is moderately massive (∼ 240 M⊙). A careful inspection of JCMT 13 CO(3−2) molecular data exhibits that the massive cluster is associated with a number of filamentary structures. Several embedded young stellar objects (YSOs) are also identified in the PG108.3 along the length and junction of filaments. We find the evidence of velocity gradient along the length of the filaments. Along with kinematics of the filaments and the distribution of ionized, molecular gas and YSOs, we suggest that the cluster formation is most likely due to the longitudinal collapse of the most massive filament in PG108.3.

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“…This work put forth the now-classic model for the IMF, a power law with a finite upper bound equal to the physical maximum mass of a star that could form in a cluster (Salpeter, 1955). More recent studies continue to use this power law form for the IMF, especially for stars of mass greater than half that of our sun (e.g., Massey 2003;Bastian, Covey and Meyer 2010;Da Rio et al 2012;Lim et al 2013;Weisz et al 2013Weisz et al , 2015Jose et al 2017). Similar models have been proposed and used in the astronomical literature for inference of the stellar IMF; these will be discussed in the next section.…”

Section: Introductionmentioning

confidence: 99%

A preferential attachment model for the stellar initial mass function

Cisewski-Kehe

Weller²,

Schafer

2019

Electron. J. Statist.

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Accurate specification of a likelihood function is becoming increasingly difficult in many inference problems in astronomy. As sample sizes resulting from astronomical surveys continue to grow, deficiencies in the likelihood function lead to larger biases in key parameter estimates. These deficiencies result from the oversimplification of the physical processes that generated the data, and from the failure to account for observational limitations. Unfortunately, realistic models often do not yield an analytical form for the likelihood. The estimation of a stellar initial mass function (IMF) is an important example. The stellar IMF is the mass distribution of stars initially formed in a given cluster of stars, a population which is not directly observable due to stellar evolution and other disruptions and observational limitations of the cluster. There are several difficulties with specifying a likelihood in this setting since the physical processes and observational challenges result in measurable masses that cannot legitimately be considered independent draws from an IMF. This work improves inference of the IMF by using an approximate Bayesian computation approach that both accounts for observational and astrophysical effects and incorporates a physically-motivated model for star cluster formation. The methodology is illustrated via a simulation study, demonstrating that the proposed approach can recover the true posterior in realistic situations, and applied to observations from astrophysical simulation data.

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The Low-mass Population in the Young Cluster Stock 8: Stellar Properties and Initial Mass Function

Cited by 37 publications

References 93 publications

Molecular gas in high-mass filament WB673

Molecular gas in high-mass filament WB673

The Planck Cold Clump G108.37-01.06: A Site of Complex Interplay between H ii Regions, Young Clusters, and Filaments

A preferential attachment model for the stellar initial mass function

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