A comprehensive photometric and kinematical characteristic of the newly discovered QCs clusters with Gaia EDR3

Elsanhoury, W. H.; Amin, Magdy Y.; Haroon, A. A.; Awad, Z.

doi:10.48550/arxiv.2201.04015

Cited by 2 publications

(2 citation statements)

References 39 publications

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“…The IMF controls the efficiency of star formation in molecular clouds (Dib et al 2011(Dib et al ,2013Hony et al 2015), the radiative and mechanical feedback from stars into the large-scale interstellar medium (Dib et al 2006(Dib et al ,2021Martizzi et al 2016;Silich & Tenorio-Tagle 2017), and the dynamical and chemical evolution of galaxies (Côté et al 2016). Significant efforts have been devoted to the determination of the shape of the IMF in a variety of environments, including the Galactic field (Salpeter 1955;Bochanski et al 2010;Rybizki & Just 2015;Mor et al 2019;Sollima 2019), the Galactic bulge (Zoccali et al 2000;Wegg et al 2017), and globular clusters (GCs;Da Costa & Freeman 1976;De Marchi & Paresce 1997;Covino & Ortolani 1997;Marconi et al 1998;Paresce & De Marchi 2000;Sollima et al 2007;Balbinot et al 2009;Sollima & Baumgardt 2017;Cadelano et al 2020), as well as in many young open clusters and associations (Dib 2014;Weisz et al 2015;Maia et al 2016;Dib et al 2017;Jose et al 2017;Madaan et al 2020;Bisht et al 2021;Damian et al 2021;Elsanhoury et al 2022). The existence of IMF variations in clusters has significant consequences for the galaxy-wide IMF and for galactic evolution (Dib & Basu 2018;...…”

Section: Introductionmentioning

confidence: 99%

Stellar collisions in globular clusters: Constraints on the initial mass function of the first generation of stars

Dib

Kravtsov

Haghi

et al. 2022

A&A

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Globular clusters display an anticorrelation between the fraction of the first generation of stars (N(G1)/N(tot)) and the slope of the present-day mass function of the clusters (α pd ), which is particularly significant for massive clusters. In the framework of the binarymediated collision scenario for the formation of the second-generation stars in globular clusters, we test the effect of a varying stellar initial mass function (IMF) of the G1 stars on the (N(G1)/N(tot)) −α pd anticorrelation. We use a simple collision model that has only two input parameters, the shape of the IMF of G1 stars and the fraction of G1 stars that coalesce to form second-generation stars. We show that a variable efficiency of the collision process is necessary in order to explain the (N(G1)/N(tot)) −α pd anticorrelation; however, the scatter in the anticorrelation can only be explained by variations in the IMF, and in particular by variations in the slope in the mass interval ≈ (0.1-0.5) M ⊙ . Our results indicate that in order to explain the scatter in the (N(G1)/N(tot)) −α pd relation, it is necessary to invoke variations in the slope in this mass range between ≈ −0.9 and ≈ −1.9. Interpreted in terms of a Kroupa-like broken power law, this translates into variations in the mean mass of between ≈ 0.2 and 0.55 M ⊙ . This level of variation is consistent with what is observed for young stellar clusters in the Milky Way and may reflect variations in the physical conditions of the globular cluster progenitor clouds at the time the G1 population formed or may indicate the occurrence of collisions between protostellar embryos before stars settle on the main sequence.

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Section: Introductionmentioning

confidence: 99%

Stellar collisions in globular clusters: Constraints on the initial mass function of the first generation of stars

Dib

Kravtsov

Haghi

et al. 2022

A&A

View full text Add to dashboard Cite

show abstract

“…The IMF controls the efficiency of star formation in molecular clouds (Dib et al 2011(Dib et al ,2013Hony et al 2015), the radiative and mechanical feedback from stars into the large scale interstellar medium (Dib et al 2006(Dib et al ,2021Martizzi et al 2016;Silich & Tenorio-Tagle 2017) and the dynamical and chemical evolution of galaxies (Côté et al 2016). Significant efforts have been devoted to the determination of the shape of the IMF in a variety of environments, from the Galactic field (Salpeter 1955;Bochanski et al 2010;Rybizki & Just 2015;Mor et al 2019;Sollima 2019), the Galactic bulge (Wegg et al 2017) and in galactic open clusters both old and young (Dib 2014;Weisz et al 2015;Maia et al 2016;Dib et al 2017;Jose et al 2017;Madaan et al 2020;Bisht et al 2021;Damian et al 2021;Elsanhoury et al 2022). In the galactic ecosystem, globular clusters (GCs) stand out as relics of early star formation (Pfeffer et al 2018) and it is well established that GCs in the Milky Way and in the Magellanic clouds harbor two or more stellar populations (d'Antona & Caloi 2008;Milone et al 2010;Sbordone et al 2011;Gratton et al 2012;Cummings et al 2014;Piotto et al 2015;Lee 2015;Oldham & Auger 2016;Mucciarelli et al 2016;Massari et al 2016;Dalessandro et al 2016;Bowman et al 2017;…”

Section: Introductionmentioning

confidence: 99%

Stellar collisions in globular clusters: Constraints on the initial mass function of the first generation of stars

Dib,

Kravtsov,

Haghi

et al. 2022

Preprint

View full text Add to dashboard Cite

Globular clusters display an anti-correlation between the fraction of the first generation of stars (N(G1)/N(tot)) and the slope of the present-day mass function of the clusters (α pd ), which is particularly significant for massive clusters. In the framework of the binarymediated collision scenario for the formation of the second generation stars in globular clusters, we test the effect of a varying initial stellar mass function (IMF) of the G1 stars on the (N(G1)/N(tot)) − α pd anti-correlation. We use a simple collision model which has only two inputs, the IMF of G1 stars and the fraction of G1 stars that coalesce to form G2 stars. We show that a variable efficiency of the collision process is necessary in order to explain the (N(G1)/N(tot)) − α pd anti-correlation, however, the scatter in the anticorrelation can only be explained by variations in the IMF, and in particular by variations of the slope in the mass interval ≈ (0.1-0.5) M ⊙ . Our results indicate that in order to explain the scatter in the (N(G1)/N(tot)) − α pd relation, it is necessary to invoke variations of the slope in this mass range between ≈ −0.9 and ≈ −1.9. Interpreted in terms of a Kroupa-like broken power law, this translates into variations of the mean mass between ≈ 0.2 and 0.55 M ⊙ . This level of variations is consistent with what is observed for young stellar clusters in the Milky Way and may reflect variations in the physical conditions of the globular clusters progenitor clouds at the time the G1 population has formed or to the occurrence of collisions between protostellar embryos before stars settle on the Main Sequence.

show abstract

A comprehensive photometric and kinematical characteristic of the newly discovered QCs clusters with Gaia EDR3

Cited by 2 publications

References 39 publications

Stellar collisions in globular clusters: Constraints on the initial mass function of the first generation of stars

Stellar collisions in globular clusters: Constraints on the initial mass function of the first generation of stars

Stellar collisions in globular clusters: Constraints on the initial mass function of the first generation of stars

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