arXiv subjects

Tsutomu T. Takeuchi

Publications and source records attributed to Tsutomu T. Takeuchi.

At least 19 recordsLinked to original sources

arXiv2026

Topological Signatures of AGN Feedback in the Simba Simulations

Active galactic nuclei (AGN) feedback can alter the abundance and spatial distribution of galaxies within large-scale structure. We apply topological data analysis (TDA) to Simba hydrodynamical simulations with varying AGN feedback at $z=0$ to determine which galaxy populations, environments, and spatial scales are most affected. The galaxy two-point correlation function is most sensitive to feedback at $r<1 h^{-1} Mpc$. We then use Betti curves, persistence diagrams, and the 2-Wasserstein distance to quantify feedback-dependent changes in topology. Persistence diagrams show clearer differences than Betti curves, particularly for satellite galaxies. For satellites, loop-like features show significant differences at $α=0.1$--$0.4 h^{-1} Mpc$ for all feedback channels, together with a weaker cumulative difference at $α=1$--$3 h^{-1} Mpc$. The differences are strongest for satellites in quenched halos with $M_h\gtrsim10^{12} M_\odot$. Optimal matching shows that they are driven mainly by shifts in the birth and death scales of loop-like features rather than by their appearance or disappearance. These results indicate that persistent homology can provide complementary constraints on AGN feedback and environmental quenching in galaxy surveys.

astro-ph.GA↗

arXiv2026

Curvature-Conditioned Measures for Cosmological Peak Statistics: A Transport-Geometric Framework

We develop a transport-geometric theory of cosmological peak statistics based on optimal transport and entropy geometry. The density field is treated as a probability measure in Wasserstein space, and its local structure is characterized by a logarithmic curvature tensor obtained as the localized response of an entropy functional. Peaks are thereby defined as positive-curvature stationary points, and their abundance is formulated as a curvatureconditioned measure on local tensor space. In the Gaussian-linear limit, this measure admits a finite-dimensional closure in terms of the spectral moments of the density field. The resulting peak abundance reduces exactly to the classical BBKS formula, identifying BBKS as a solvable Gaussian closure of a more general geometric structure. This formulation separates peak statistics into three fundamental ingredients: the probability distribution of local variables, the positive-curvature constraint, and the induced geometric measure. The theory extends naturally beyond the Gaussian approximation. Nonlinear evolution appears as a deformation of the logarithmic curvature geometry, while primordial non-Gaussianity is interpreted as a deformation of the curvature-conditioned measure itself. We further formulate two- and three-point peak statistics as higher-order curvature-conditioned measures and show that the resulting hierarchy can be organized as response functions to long-wavelength background modes, with conventional peak bias emerging as the lowest-order response coefficient. These results provide a unified description linking optimal transport, curvature geometry, peak statistics, and cosmological observables, and establish a systematic framework for studying nonlinearity, scale dependence, primordial non-Gaussianity, and higher-order peak correlations.

astro-ph.CO↗

arXiv2026

Estimating Galaxy Star Formation Rates from Murchison Widefield Array Radio Continuum Emission

We investigate the frequency dependence of the low-frequency infrared (IR)--radio correlation for nearby galaxies drawn from the {\sl Herschel} Reference Survey (HRS), using radio continuum observations from the GaLactic and Extragalactic All-sky MWA (GLEAM) survey obtained with the Murchison Widefield Array (MWA). The GLEAM survey provides densely sampled flux densities across 20 sub-bands spanning 72--231 MHz, allowing detailed characterization of the low-frequency radio spectral energy distribution (SED). We analyze 18 nearby galaxies detected by GLEAM and examine the frequency dependence of the IR--radio correlation coefficient $q_ν$. Among these galaxies, three sources show Seyfert or LINER signatures and may contain non-negligible AGN contributions to the radio continuum emission. We therefore use the remaining 15 predominantly star-forming galaxies as the primary sample for deriving the main calibration results. For the majority of the sample, the low-frequency radio continuum is well described by a single power-law spectral model from the GLEAM frequency range up to 1.5 GHz, with a median spectral index of $γ=-0.63$. The ensemble-averaged $q_ν$ relation and its intrinsic scatter provide a practical calibration for converting low-frequency radio luminosities into star formation rates (SFRs), while explicitly quantifying the associated systematic uncertainty. Our results indicate that the low-frequency IR--radio correlation remains stable across the MWA bands for nearby star-forming galaxies, supporting the use of low-frequency radio continuum as a dust-unbiased tracer of star formation in the local Universe. These results provide a local benchmark for interpreting low-frequency radio continuum surveys and for future studies of radio-based SFR tracers with next-generation facilities such as the Square Kilometre Array (SKA).

astro-ph.GA↗

arXiv2026

Dipole Anisotropy in Newly Sampled AGN Population: Still in Tension with CMB Dipole

We revisit the all-sky survey data, the Wide-field Infrared Survey Explorer (WISE) catalog, with an improved galaxy-selection criterion to investigate the inconsistency between the dipole anisotropy in the galaxy number count and the kinematic CMB dipole anisotropy. We apply a set of active galactic nuclei (AGN) selection criteria composed of a flux cut and multiple color cuts, and formulate an appropriate adaptation of the original Ellis & Baldwin (1984) formalism for our photometric survey samples whose spectral energy distributions deviate from a pure power-law form. We find that the newly sampled AGNs from the WISE catalog still bears an anomalous number-count dipole anisotropy, whose amplitude is ~ 2.5 times as large as that of the purely kinematic origin at a 5.3 sigma confidence level. We also find that the direction of our WISE-AGN dipole is ~ 3 sigma away from that of the CMB dipole. We discuss its possible cosmological implications: nonlinearity of the nearby universe and mismatch of matter-rest frame and the CMB-rest frame.

astro-ph.CO↗

arXiv2026

Joint State-and-Dynamics Inference for Galaxy Population Evolution on an Effective Manifold

Galaxy surveys provide noisy, incomplete, selection-affected population snapshots rather than complete evolutionary histories. We formulate galaxy evolution as joint inference of effective physical states, their population intensity, and cross-epoch dynamics. An effective state is a coarse-grained description defined by predictive adequacy and distinguished from measured variables and learned representations. The intrinsic population is a finite non-negative measure evolving through one-galaxy transport, source and removal terms, and nonlocal two-to-one merger jumps. A sub-probability observational kernel maps this population to survey catalogs and supplies the likelihood for state inference. Projected luminosity and stellar-mass functions generally do not obey closed dynamics and cannot identify the underlying channels alone. In a restricted IllustrisTNG proof of concept, a finite-time non-merger kernel and reduced merger operator are calibrated on training root merger trees and evaluated on held-out lineages. Dynamical propagation improves the normalized later mass--sSFR distribution relative to a static baseline, while the merger channel captures number loss from disappearing secondary progenitors. Under noisy and censored mock observations, the propagated prior improves posterior-stacked reconstruction of the latent population relative to a frozen-static prior. The framework provides an observation-directed, simulation-assisted route to galaxy state-and-dynamics inference.

astro-ph.GA↗

arXiv2026

Wasserstein Distance in Cosmological Structure Formation: An Optimal Transport Perspective

Cosmological large-scale structure is usually characterized by statistics such as the power spectrum and correlation function, which describe fluctuation amplitudes but not the spatial redistribution of matter. We formulate structure formation as a transport problem between mass distributions using the Wasserstein distance of optimal transport theory. The generative process from the initial linear density field to an observed galaxy catalog is represented as a hierarchical mapping from a continuous matter field to a galaxy point process. Under the small-fluctuation approximation, we derive an approximate Wasserstein distance that decomposes into three physically distinct contributions: gravitational mass transport, galaxy formation bias, and shot noise from discrete galaxy sampling. The gravitational term is expressed as an integral of the matter power spectrum, whereas the galaxy formation term is given by a transport-weighted integral of the galaxy correlation function. The sampling term reduces to Poisson shot noise. Unlike conventional volume-weighted clustering statistics, the correlation contribution measures cumulative matter displacements and is naturally connected to baryon acoustic oscillation smearing. This framework provides a transport-geometric description of large-scale structure formation and introduces the Wasserstein distance as a statistical link between continuous density fields and observed galaxy catalogs.(abridged)

astro-ph.CO↗

arXiv2026

Insights into Jet-Induced Cloud Disruption in NGC 1316: ALMA Reveals a Spatially Extended Molecular Gas

We present ALMA CO($J=1-0$) observations of a nearby radio galaxy NGC1316 at a 100-pc resolution to investigate the impact of AGN jets on the molecular gas. The molecular gas exhibits complex spatial and kinematic distributions, with broad CO line widths ($>50$ km s$^{-1}$) observed in several regions. The interferometric CO flux is only 34%-38% compared to single-dish data, indicating a large fraction of spatially extended molecular gas, especially in the central regions. We identified 24 Giant Molecular Clouds Associations (GMAs) primarily within the ``NW Shell'' and the ``SE Blob''; these GMAs show velocity dispersions approximately twice as high as those in typical star-forming galaxies for their sizes. Analysis of archival ALMA CO($J=2-1$) and CO($J=3-2$) data reveals elevated line ratios ($R_{21} \sim 1$ and $R_{31} \sim 1$) in gas near the jet, whereas, away from the jet, typical values ($R_{21} \sim 0.7$, $R_{31} \sim 0.3$). A multi-wavelength comparison reveals a $\sim$5 kpc warm ionized gas shell that encompasses the molecular NW Shell. The observed energetics and bubble morphology are consistent with an expanding bubble model driven by the jet assuming a jet power of $1.6\times10^{43}$~erg~s$^{-1}$. We propose that the high extended gas fraction results from the destruction of molecular clouds due to interactions with the jet plasma. NGC1316 may be a good example of jet-induced negative feedback through the ablation, dispersal, and rarification of dense molecular clouds through jet-ISM interactions.

astro-ph.GA↗

arXiv2026

Exploring the Cosmic Dawn through the 21 cm Forest and High-redshift Radio Sources with the SKA

The 21~cm forest, seen as absorption features in the spectra of distant radio sources, is produced by intervening neutral hydrogen and offers a direct probe of the neutral intergalactic medium during the epoch of reionization (EoR). Because it is sensitive to small-scale structure and gas temperature, it can constrain the thermal history of the early Universe and physics that affects structure formation. Detecting individual absorption lines is challenging, mainly because of their weakness and the scarcity of high-redshift radio-bright sources. Recent progress, however, has made 21~cm forest studies increasingly feasible: new statistical observables can improve sensitivity within realistic observing times, updated radio-source counts have revised expectations for suitable background quasars, and deep-learning methods can extract physical information more efficiently. In addition, new approaches have been developed to separate astrophysical effects from early galaxies from fundamental-physics effects on small-scale structure. With the Square Kilometre Array (SKA), the 21~cm forest will therefore provide a promising route to study early heating, possible exotic energy injection, dark matter properties, neutrino mass, the running spectral index, and baryon--dark-matter relative velocity. This chapter reviews recent developments in 21~cm forest research and discusses observational strategies and prospects for constraining the first galaxies and fundamental physics with SKA-Low.

astro-ph.CO↗

arXiv2026

Revisiting Marked Galaxy Clustering from a Joint Point Process Perspective

Marked correlation functions, in which galaxy properties such as luminosity or stellar mass are treated as marks, are widely used to test models of galaxy formation. In astronomy, however, these statistics are typically implemented as summary measures that do not preserve the joint structure of mark pairs conditioned on separation. In this work, we formulate galaxies as points $(x,m)$ on the product space $\mathbb{R}^3\times\mathcal{M}$, where $x$ denotes position and $m$ a mark, and introduce the joint pair correlation function $g(r;m_1,m_2)$ as the fundamental quantity describing mark-dependent clustering. We further define a diagnostic quantity $Δ_{\mathrm{ind}}(r;m_1,m_2)$ that locally quantifies deviations from the independence hypothesis relative to spatial clustering alone, thereby providing a projection-free description of which mark pairs are over- or underrepresented at a given separation scale. Within this framework, commonly used diagnostics such as the inhomogeneous cross-$J$ function are naturally interpreted as summary statistics obtained through averaging over mark sets and geometric-event-based reductions of the joint structure. This perspective clarifies that previously discussed marked effects, including assembly bias, correspond to projections of an underlying joint dependence, and that observationally accessible information is the existence of non-factorizable joint structure itself. The present formulation provides both a fundamental quantity and practical diagnostics for its characterization.

astro-ph.GA↗

arXiv2026

A General Formulation of the Kinematic Dipole as a Functional of Selection and Source Properties: Beyond the Ellis--Baldwin Approximation

The dipole anisotropy in galaxy and QSO number counts induced by the motion of the observer (the kinematic dipole) provides an important test of cosmological isotropy and a comparison with the Cosmic Microwave Background (CMB) dipole. Traditionally, the Ellis \& Baldwin expression,$\mathcal{A}=2+x(1+α)$, has been widely adopted, assuming power-law number counts and a single power-law spectral energy distribution (SED). Realistic surveys, however, involve a range of non-ideal effects, including diverse SEDs, finite instrumental bandpasses, non-power-law number counts, multi-band photometry and photo-$z$ selections, and direction-dependent or stochastic detection limits. In this paper, we incorporate these effects explicitly at the theoretical level and present a unified formulation of the kinematic dipole for a general parent population and a general multi-dimensional selection function. We show that the dipole amplitude is not described by a single index, but is instead given by a functional, $\mathcal{A}[\mathcal{W},f]$, defined as the Doppler response of the selection function acting on the underlying population. We demonstrate that the classical Ellis--Baldwin result is recovered as a special limiting case of this formalism, and clarify the relation between the theoretical coefficient $\mathcal{A}$ and the dipole vector estimated from finite catalogs, separating theoretical response from statistical uncertainty. This framework provides a basis for reinterpreting reported discrepancies in kinematic dipole measurements across surveys and is directly applicable to future wide-area, multi-band observations.

astro-ph.CO↗

arXiv2026

A Measure-Theoretic Transport Formulation of Galaxy Evolution on the Galaxy Manifold: Geometric Constraints

We develop a measure-theoretic framework for galaxy evolution in which galaxy populations are described as probability measures on a state space. Galaxy evolution is represented as the time evolution of a measure $ν_t$, governed by the sum of a continuous transport term and a jump operator. The transport term describes internal galaxy evolution, while the jump operator captures discrete events such as mergers and interactions, yielding a unified reaction--transport system on the space of measures. We further equip the space of probability measures with the Wasserstein distance and impose a curvature--dimension condition CD$(K,\infty)$ to reveal the geometric structure of the dynamics. In this setting, the transport term is interpreted as a gradient flow of a free-energy functional, whereas the jump operator generates nonlinear rearrangements induced by many-body interactions. In the low-density limit, these interactions reduce effectively to two-body processes, leading to a closed dynamical system. A central consequence is that galaxy evolution is not arbitrary, but constrained by a variational structure, curvature bounds, and an interaction hierarchy. Admissible trajectories are restricted by energy dissipation, geometric contractivity, and effective interaction closure. The framework also separates intrinsic galaxy dynamics from observational projection, treating observables as pushforwards of measures. It thus provides a unified foundation for structure formation and galaxy evolution as a geometrically constrained reaction--transport process.

physics.gen-ph↗

arXiv2026

Resolving the Dust Budget Crisis at $z \sim 8$ with Optically Thick, High-Density Molecular Clumps: MACS0416_Y1

Dust plays a crucial role in galaxy evolution by shaping the spectral energy distribution (SED) and star formation history. However, standard models often underestimate the infrared luminosity of high-redshift galaxies ($z \sim 8$), leading to the so-called dust budget crisis. In this work, we modify the theoretical framework by focusing on compact star-forming clumps in the interstellar medium. Motivated by the observed compactness of high-z galaxies, we treat the cold neutral medium density as a free parameter. Our analysis reveals that the ISM must reach extreme densities ($n_{\text{H,CNM}} \sim 7.5 \times 10^3 \, \mathrm{cm}^{-3}$). This enhances UV photon trapping, accelerates dust processing in dense gas, and reduces dust destruction by supernova shocks. Our model successfully reproduces the observed UV-to-FIR SED of MACS0416_Y1 ($z = 8.312$). A grain-size-resolved treatment further shows that the warm IR emission is dominated by intermediate-size grains ($a = 0.01$ - $0.1\,μ$m), which contribute about 89% of the luminosity near the SED peak and in the ALMA Band~9 continuum. These grains are nearly in thermal equilibrium at characteristic temperatures of $\sim 70$ K, while the largest grains remain cooler and the smallest grains exhibit a high-temperature tail with low probability. We conclude that extreme ISM densities can alleviate the dust budget crisis by promoting efficient UV photon trapping and rapid dust evolution, thereby increasing dust mass and producing a multi-temperature grain population.

astro-ph.GA↗

arXiv2026

A Geometric Theory of Cosmological Structure via Entropic Curvature in Wasserstein Space

We construct a geometric framework for cosmological large-scale structure based on optimal transport theory and Wasserstein geometry. In this framework, Ricci curvature on the probability measure space $\mathcal{P}_2(M)$ is characterized by the geodesic convexity of entropy and is formulated as the response of probability distributions to optimal transport. We introduce effective Ricci curvatures $K_{\mathrm{eff}}^{(\infty)}$ and $K_{\mathrm{eff}}^{(N)}$ associated with Kullback--Leibler-type and Rényi-type entropies, corresponding respectively to the curvature-dimension conditions CD$(K,\infty)$ and CD$(K,N)$. By localizing these curvatures to finite scales using local and reference measures, we construct curvature indicators applicable to observational data. Under a local quadratic approximation, the effective curvature reduces to the Hessian of the log-density, showing that conventional Hessian-based structure classifications arise as a limiting case of the present framework. We further show that effective curvature depends on observational scale and formulate this dependence as a scale flow, distinct from Ricci flow because it describes a change of resolution rather than a time evolution of geometry. Treating curvature as a random field then extends the statistical description of density fields: curvature statistics are given by higher-order weighted integrals of the power spectrum and by spatial derivatives of the correlation function, emphasizing geometric rather than amplitude information. This framework provides a unified connection between optimal transport geometry and cosmological structure analysis, and offers a new perspective on multiscale structure and nonlinear statistics.

astro-ph.CO↗

arXiv2026

Rigorous Formulation of Finite-Sample and Finite-Window Effects in Galaxy Clustering

Galaxy surveys provide finite catalogs of objects observed within bounded volumes, yet clustering statistics are often interpreted using theoretical frameworks developed for infinite point processes. In this work, we formulate key statistical quantities directly for finite point processes and examine the structural consequences of finite-number and finite-window constraints. We show that several well-known features of galaxy survey analysis arise naturally from finiteness alone. In particular, non-vanishing higher-order connected correlations can occur even in statistically independent samples when the total number of points is fixed, and the integral constraint in two-point statistics appears as an exact identity implied by the finite-number condition rather than as an estimator artifact. We further demonstrate that counts-in-cells and point-centered environmental measures correspond to distinct statistical ensembles. Using Palm conditioning, we derive an exact relation between random-cell and point-centered statistics, showing that the latter probe a tilted version of the underlying distribution. These results provide a probabilistic framework for separating structural effects imposed by finite sampling from correlations reflecting genuine astrophysical processes. The formulation presented here remains valid for realistic survey geometries and finite data sets and clarifies the interpretation of commonly used clustering statistics in galaxy surveys.

astro-ph.GA↗

arXiv2026

A Potential Link between Nuclear Winds and Cold Gas Outflows on Kiloparsec Scales in Reionization-Era Quasars

Feedback from accreting supermassive black holes may regulate galaxy evolution, but statistical evidence linking nuclear winds to kiloparsec-scale cold gas outflows remains limited in the early universe. Here we report statistical evidence for such a connection in a sample of luminous quasars at $z \sim 5.5$. We compare stacked [C II] 158 $μ$m emission profiles from ALMA observations, which trace galactic-scale neutral gas, for quasars with and without broad absorption lines (BALs) that indicate powerful nuclear winds on sub-kiloparsec scales. A total of 5 BAL and 11 non-BAL quasar spectra are included in the stacking analysis. The BAL quasar stack exhibits a potential blueshifted broad component in the [C II] line profile, with a velocity offset of $Δv_{\rm b} = -2.1 \times 10^2\,\rm km\,s^{-1}$ and a full width at half maximum of $1.18 \times 10^3\,\rm km\,s^{-1}$, whereas the non-BAL stack shows no obvious broad component. Using a conservative ``clean-stack'' selection that excludes quasars with partial [C II] spectral coverage, the BAL broad residual is reduced to a hint-level feature. We estimate that up to a few percent to one-quarter of the nuclear wind energy may be transferred to cold neutral gas on kiloparsec scales. Although the sample size is limited, these results suggest a potential link between BAL winds and cold gas feedback in quasar host galaxies. These results provide empirical motivation for future tests of how multiphase outflows relate to the diversity of quasar host properties, including $M_{\rm BH}/M_*$.

astro-ph.GA↗

arXiv2026

Cosmic Dipole as a Symmetry Response: From the Ellis--Baldwin Formula to Correlation Function Dipoles

The cosmic dipole in galaxy number counts is traditionally described by the Ellis--Baldwin (EB) formula under simplifying assumptions of power-law source counts and flux-limited selection. We reformulate the EB dipole as a symmetry response of observed counts to a Lorentz boost, leading to the general expression $D=βR$, where $R=\partial\ln N/\partial\lnβ$ encodes the underlying population and selection effects. The classical EB formula is recovered as a limiting case. We show that this response framework extends beyond one-point statistics: Lorentz boosts induce a dipole component in the two-point correlation function and, more generally, a hierarchy of responses in $n$-point statistics. We further clarify the relation to redshift-space distortions and relativistic galaxy clustering, and provide a unified description in which observer- and source-induced dipoles contribute to the same multipole component. This establishes the cosmic dipole as a symmetry response of finite-sample point-process statistics, offering a new perspective on dipole anisotropies and their observational interpretation.

astro-ph.CO↗

arXiv2026

A New Framework for Multi-Line Analysis Combined Kernel PCA and Kernel SHAP: A Case of NGC 1068 ALMA Band 3 Data

We present a new framework for multi-line analysis that combines kernel principal component analysis (Kernel PCA), an unsupervised machine-learning method, and Kernel SHapley Additive exPlanations (Kernel SHAP), an explainable artificial intelligence (XAI) technique. To enable a comparison with PCA-based studies, which have been widely used in multi-line analyses, we apply our framework to integrated intensity maps of 13 molecular lines from Atacama Large Millimeter/submillimeter Array (ALMA) Band 3 archival data of the nearby galaxy NGC 1068. Previous PCA-based studies of NGC 1068 reported that physically meaningful structures are mainly captured up to the second component. In contrast, our framework can interpret physically meaningful features up to the fourth component. Furthermore, by comparing the results obtained from our framework with molecular column densities derived from local thermodynamical equilibrium (LTE) analysis, we suggest that the abundance of HCO+ is relatively enhanced in the molecular outflow region extending to a radius of about 400 pc from the galactic center, likely due to the effects of ultraviolet radiation and highly dense gas. These results show that our framework can provide data-driven insights into physical and chemical features that have not been clearly identified in previous studies. It also provides an efficient tool for interpreting the rapidly increasing amount of multi-line observational data.

astro-ph.GA↗

arXiv2025

CO Multi-line Imaging of Nearby Galaxies (COMING). XI. Azimuthally averaged star formation rate and stellar mass relation with molecular gas amount

This study investigated the relation between the surface density of star formation rate (SFR) ($Σ_{\mathrm{SFR}}$), stellar mass ($Σ_{M_{\ast}}$), and molecular gas mass ($Σ_{M_\mathrm{mol}}$) on nearly 1 kpc scales averaged over concentric tilted rings using the $^{12}$CO $J=1-0$ mapping data of 92 nearby galaxies obtained in the CO Multi-line Imaging of Nearby Galaxies (COMING) project. We categorized these galaxies into three groups based on the deviation of each global SFR from the star-forming main sequence (MS), $Δ$MS: upper MS (UMS), MS, and lower MS (LMS). UMS galaxies tend to be less massive or barred spiral galaxies, exhibiting molecular gas fraction ($f_{\mathrm{gas}}$) comparable to those of MS galaxies but higher star formation efficiency (SFE). In contrast, the LMS galaxies tend to be massive or active galaxies hosting an active galactic nucleus (AGN). Their $f_{\mathrm{gas}}$ values are lower than those of MS galaxies, and their SFEs are slightly lower or comparable to those of MS galaxies in the inner region. These trends indicate that enhanced SFE contributes to higher $Δ$MS values, whereas reduced $f_{\mathrm{gas}}$ results in lower $Δ$MS values. The less prominent bulge or the presence of a bar structure in UMS galaxies induces disk-wide star formation, consequently increasing the SFE. In LMS galaxies, the molecular gas is exhausted, and their star formation activity is low. Environmental effects, such as tidal gas stripping, may also reduce gas supply from the outer regions. Furthermore, our sample galaxies show that both the specific star formation rate (sSFR) and $f_{\mathrm{gas}}$ decrease in the central region in LMS galaxies but did not change in the same region in UMS galaxies. These results seem to support the inside-out quenching of star formation although the dominant cause of depletion remains uncertain.

astro-ph.GA↗