Probabilistic model for dynamic galaxy decomposition

Jagvaral, Yesukhei; Campbell, Duncan; Mandelbaum, Rachel; Rau, Markus

doi:10.1093/mnras/stab3104

Cited by 6 publications

(2 citation statements)

References 72 publications

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“…A step forward toward their better understanding might be possible through spectrophotometric and kinematical decomposition of IFS data (e.g., by extending the method by B20b by a dense grid of modexp models for 0 ≤ 1 ≤ 1, or other functional forms that allow for a centrally depressed exponential disk). A combined analysis of observational constraints gained from this task with galaxy simulations that incorporate detailed prescriptions for SFQ as well as Schwarzschild orbital superposition modeling (e.g., Zhu et al 2018a,b;Du et al 2020;Jagvaral et al 2022) would be of considerable interest.…”

Section: Effect Of δ Io On the Scatter And Slope Of Fundamental Scali...mentioning

confidence: 99%

Inside-out star formation quenching and the need for a revision of bulge-disk decomposition concepts for spiral galaxies

Papaderos

Breda

Humphrey

et al. 2022

A&A

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Our knowledge about the photometric and structural properties of bulges in late-type galaxies (LTGs) is founded upon image decomposition into a Sérsic model for the central luminosity excess of the bulge and an exponential model for the more extended underlying disk. We argue that the standard practice of adopting an exponential model for the disk all the way to its center is inadequate because it implicitly neglects the fact of star formation (SF) quenching in the centers of LTGs. Extrapolating the fit to the observable star-forming zone of the disk (outside the bulge) inwardly overestimates the true surface brightness of the disk in its SF-quenched central zone (beneath the bulge). We refer to this effect as δio. Using predictions from evolutionary synthesis models and by applying to integral field spectroscopy data REMOVEYOUNG, a tool that allows the suppression of stellar populations younger than an adjustable age cutoff we estimate the δio in the centers of massive SF-quenched LTGs to be up to ∼2.5 (0.7) B (K) mag. The primary consequence of the neglect of δio in bulge-disk decomposition studies is the oversubtraction of the disk underneath the bulge, leading to a systematic underestimation of the true luminosity of the latter. Secondary biases impact the structural characterization (e.g., Sérsic exponent η and effective radius) and color gradients of bulges, and might include the erroneous classification of LTGs with a moderately faint bulge as bulgeless disks. Framed in the picture of galaxy downsizing and inside-out SF quenching, δio is expected to differentially impact galaxies across redshift and stellar mass ℳ⋆, thus leading to systematic and complex biases in the scatter and slope of various galaxy scaling relations. We conjecture that correction for the δio effect will lead to a down-bending of the bulge versus supermassive black hole relation for galaxies below log(ℳ⋆/M⊙) ∼ 10.7. A decreasing ℳ∙/ℳ⋆ ratio with decreasing ℳ⋆ would help to consistently explain the scarcity and weakness of accretion-powered nuclear activity in low-mass spiral galaxies. Finally, it is pointed out that a well-detectable δio (> 2 r mag) can emerge early on through inward migration of star-forming clumps from the disk in combination with a strong contrast of emission-line equivalent widths between the quenched protobulge and its star-forming periphery. Spatially resolved studies of δio with the James Webb Space Telescope, the Extremely Large Telescope, and Euclid could therefore offer key insights into the chronology and physical drivers of SF-quenching in the early phase of galaxy assembly.

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Section: Effect Of δ Io On the Scatter And Slope Of Fundamental Scali...mentioning

confidence: 99%

Inside-out star formation quenching and the need for a revision of bulge-disk decomposition concepts for spiral galaxies

Papaderos

Breda

Humphrey

et al. 2022

A&A

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“…Understanding galactic morphology presumes that one is capable of separating the stellar body of the galaxy into subcomponents based on the surface and/or brightness density, kinematics, metallicity, age, etc. Attempts to decompose galaxies into various morphological features have a long history and aims at quantifying their relative importance during galaxy evolution (e.g., Abadi et al 2003a,b;Governato et al 2007;Di Matteo et al 2008;Croft et al 2009;Marinacci et al 2014;Genel et al 2015;Jagvaral et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Emergence of Galactic Morphologies at Cosmic Dawn: Input from Numerical Modeling

Bi,

Shlosman,

Romano-Diaz

2021

Preprint

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We employ a series of high-resolution zoom-in cosmological simulations to analyze the emerging morphology of main galaxies in dark matter halos at redshifts 𝑧 > ∼ 2. We choose DM halos of similar masses of log 𝑀 vir /M ∼ 11.65 ± 0.05 at the target redshifts of 𝑧 f = 6, 4 and 2. The rationale for this choice, among others, allows us to analyze how the different growth rate in these DM halos propagates down to galaxy scales and affects their basic parameters. Halos were embedded in high or low overdensity regions, and two different versions of a galactic wind feedback have been employed -a strong one and energetically weak one. Our main results are: (1) Although our galaxies evolve in different epochs, their global parameters (e.g., baryonic masses and sizes) remain within a narrow range. Their morphology, kinematics and stellar populations differ substantially, yet all of them host sub-kpc stellar bars; (2) The star formation rates (SFRs) appear higher for larger 𝑧 f , in tandem with their energy and momentum feedback; (3) The stellar kinematics allowed separation of bulge from the stellar spheroid. The existence of disk-like bulges has been revealed based on stellar surface density and photometry, but displayed a mixed disk-like and classical bulges based on their kinematics. The bulge-to-total mass ratios appear independent of the last merger time for all 𝑧 f . The stellar spheroid-to-total mass ratios of these galaxies lie in the range of ∼ 0.5 − 0.8; (4) The synthetic redshifted, pixelized and PSF-degraded JWST images allow to detect stellar disks at all 𝑧 f . Some bars disappear in degraded images, but others remain visible; (5) Based on the kinematic decomposition, for stellar disks separated from bulges and spheroids. we observe that rotational support in disks depends on the feedback type, but increases with decreasing 𝑧 f ; (6) Finally, the ALMA images detect disks at all 𝑧 f , but their spiral structure is only detectable in 𝑧 f = 2 galaxies. We also find that the galaxies follow the Tully-Fisher relation most of their evolution, being separated only by the galactic wind feedback.

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Morphological decomposition of TNG50 galaxies: methodology and catalogue

Zana

Lupi

Bonetti

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present mordor (MORphological DecOmposeR, a new algorithm for structural decomposition of simulated galaxies based on stellar kinematics. The code measures the properties of up to five structural components (a thin/cold and a thick/warm disc, a classical and a secular bulge, and a spherical stellar halo), and determines the properties of a stellar bar (if present). A comparison with other algorithms presented in the literature yields overall good agreement, with mordor displaying a higher flexibility in correctly decomposing systems and identifying bars in crowded environments (e.g. with ongoing fly-bys, often observable in cosmological simulations). We use mordor to analyse galaxies in the TNG50 simulation and find the following: (i) the thick disc component undergoes the strongest evolution in the binding energy-circularity plane, as expected when disc galaxies decrease their turbulent-rotational support with cosmic time; (ii) smaller galaxies (with stellar mass, $10^{9} \lesssim M_{*}/~\rm M_{\odot }\le 5 \times 10^{9}$) undergo a major growth in their disc components after z ∼ 1, whereas (iii) the most massive galaxies ($5 \times 10^{10} < M_{*}/~\rm M_{\odot }\le 5\times 10^{11}$) evolve toward more spheroidal dominated objects down to z = 0 due to frequent gravitational interactions with satellites; (iv) the fraction of barred galaxies grows rapidly at high redshift and stabilizes below z ∼ 2, except for the most massive galaxies that show a decrease in the bar occupation fraction at low redshift; (v) galaxies with $M_{*} \sim 10^{11}~~\rm M_{\odot }$ exhibit the highest relative occurrence of bars at z = 0, in agreement with observational studies. We publicly release mordor and the morphological catalogue of TNG50 galaxies.

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Probabilistic model for dynamic galaxy decomposition

Cited by 6 publications

References 72 publications

Inside-out star formation quenching and the need for a revision of bulge-disk decomposition concepts for spiral galaxies

Inside-out star formation quenching and the need for a revision of bulge-disk decomposition concepts for spiral galaxies

Emergence of Galactic Morphologies at Cosmic Dawn: Input from Numerical Modeling

Morphological decomposition of TNG50 galaxies: methodology and catalogue

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