Morphology of Galaxies in JWST Fields: Initial Distribution and Evolution of Galaxy Morphology

Lee, Jeong Hwan; Park, Changbom; Hwang, Ho Seong; Kwon, Minseong

doi:10.3847/1538-4357/ad3448

Cited by 2 publications

(1 citation statement)

References 91 publications

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“…Given the difficulties in correlating galaxy morphology with physical significance, it is remarkable that galaxy classification systems have proven as useful as they have. In a significant way, the jury is still out on galaxy classification systems and whether the characteristics chosen as the basis for the classification systems are fundamental to the galaxies themselves and particularly their evolution although the Hubble and JWST Space Telescopes have greatly illuminated this connection (Lee et al 2024;NASA 2024;Wijesinghe et al 2010).…”

Section: Galaxy Classificationmentioning

confidence: 99%

Discovery and Classification in Astronomy: Scientific and Philosophical Challenges and the Importance of a Comprehensive and Consistent Classification System

Dick

2024

Planet. Sci. J.

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Throughout history, the definition of “class” and the construction of astronomical classification systems has been a deep scientific and philosophical problem: scientific because facts such as physical composition ideally need to be known for proper classification but often are not, philosophical because astronomers need to understand the philosophical assumptions behind their attempts at classification, and because different philosophical ideas such as “natural kinds” often guide classification, even if unconsciously. The primary lesson of history is that the most useful classifications of celestial objects are optimally based on their physical nature. The second lesson is that because discovery is an extended process consisting of detection, interpretation, and understanding, initial classifications may be phenomenological, based on characteristics that may be useful in early “detection” stages of extended discovery. By contrast, final classifications of “the thing itself,” is achieved only after the “understanding” stage of discovery and must have a physical basis. A third lesson is that class status is best determined within a comprehensive classification system in order to determine taxon level, e.g., class, type, subtype. Such a system, encompassing all astronomical objects, illustrates the problems of class and classification, problems that may be applied to exoplanet discoveries.

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Section: Galaxy Classificationmentioning

confidence: 99%

Discovery and Classification in Astronomy: Scientific and Philosophical Challenges and the Importance of a Comprehensive and Consistent Classification System

Dick

2024

Planet. Sci. J.

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Gravitational waves from mergers of Population III binary black holes: roles played by two evolution channels

Liu,

Hartwig,

Sartorio

et al. 2024

Monthly Notices of the Royal Astronomical Society

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The gravitational wave (GW) signal from binary black hole (BBH) mergers is a promising probe of Population III (Pop III) stars. To fully unleash the power of the GW probe, one important step is to understand the relative importance and features of different BBH evolution channels. We model two channels, isolated binary stellar evolution (IBSE) and nuclear star cluster-dynamical hardening (NSC-DH), in one theoretical framework based on the semi-analytical code a-sloth, under various assumptions on Pop III initial mass function (IMF), initial binary statistics and high-z nuclear star clusters (NSCs). The NSC-DH channel contributes $\sim 8-95{{\%}}$ of Pop III BBH mergers across cosmic history, with higher contributions achieved by initially wider binary stars, more top-heavy IMFs, and more abundant high-z NSCs. The dimensionless stochastic GW background (SGWB) produced by Pop III BBH mergers has peak values $\Omega ^{\rm peak}_{\rm GW}\sim 10^{-11}-8\times 10^{-11}$ around observer-frame frequencies $\nu \sim 10-100\ \rm Hz$. The Pop III contribution can be a non-negligible ($\sim 2-32{{\%}}$) component in the total SGWB at $\nu \lesssim 10\ \rm Hz$. The estimated detection rates of Pop III BBH mergers by the Einstein Telescope are $\sim 6-230\ \rm yr^{-1}$ and $\sim 30-1230\ \rm yr^{-1}$ for the NSC-DH and IBSE channels, respectively. Pop III BBH mergers in NSCs are more massive than those from IBSE, so they dominate the Pop III SGWB below 20 Hz in most cases. Besides, the detection rate of Pop III BBH mergers involving at least one intermediate-mass BH above $100\ \rm M_\odot$ by the Einstein Telescope is $\sim 0.5-200\ \rm yr^{-1}$ in NSCs but remains below $0.1\ \rm yr^{-1}$ for IBSE.

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Morphology of Galaxies in JWST Fields: Initial Distribution and Evolution of Galaxy Morphology

Abstract: A recent study from the Horizon Run 5 (HR5) cosmological simulation has predicted that galaxies with log M * / … Show more

Cited by 2 publications

References 91 publications

Discovery and Classification in Astronomy: Scientific and Philosophical Challenges and the Importance of a Comprehensive and Consistent Classification System

Discovery and Classification in Astronomy: Scientific and Philosophical Challenges and the Importance of a Comprehensive and Consistent Classification System

Gravitational waves from mergers of Population III binary black holes: roles played by two evolution channels

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