Spatially resolved signature of quenching in star-forming galaxies

Quai, Salvatore; Pozzetti, L.; Moresco, M.; Citro, Annalisa; Cimatti, A.; Brinchmann, Jarle; Gunawardhana, Madusha; Paalvast, Mieke

doi:10.1093/mnras/stz2771

Cited by 12 publications

(5 citation statements)

References 138 publications

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“…In addition, decreasing SFR at the center indicates that the suppression is not merely due to the increasing mass of the stellar bulge component, but is evidence for inside-out quenching. Similar findings in the literature show that transition galaxies with high stellar mass typically have central suppression in their sSFR profiles (González Delgado et al 2016;Coenda et al 2018;Ellison et al 2018;Liu et al 2018;Sánchez et al 2018;Spindler et al 2018;Quai et al 2019). Moreover, the fraction of inside-out quenching increases with stellar mass (Lin et al 2019), suggesting that the fraction of inside-out quenching is higher than the fraction of outside-in quenching at a given stellar mass and environment.…”

supporting

confidence: 66%

The impact of quenching on galaxy profiles in the Simba simulation

Appleby,

Davé,

Kraljic

et al. 2019

Preprint

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We study specific star formation rate (sSFR) and gas profiles of star forming and green valley galaxies in the Simba cosmological hydrodynamic simulation. Star-forming galaxy half-light radii (R half ) at z = 0 agree well with observations, but its evolution ∝ (1 + z) −1.1 is somewhat too rapid. We compare Simba z = 0 sSFR radial profiles for main sequence and green valley galaxies to observations (Belfiore et al. 2018). Simba shows strong central depressions in star formation rate (SFR), specific SFR, and gas fraction in green valley galaxies and massive star-forming systems, qualitatively as observed. This owes primarily to black hole X-ray feedback, which pushes dense central gas outwards; turning off X-ray feedback leads to centrally peaked sSFR profiles as found in other simulations. In conflict with observations, Simba yields green valley galaxies with strongly dropping SFR profiles beyond > ∼ R half , regardless of AGN feedback. The central depression owes to lowering the molecular gas content, while the drop in the outskirts owes to a reduced star formation efficiency. Simba's satellites have higher central sSFR and lower outskirts sSFR than centrals, in qualitative agreement with observations. At z = 2 Simba does not show strong central depressions in massive star-forming galaxies, whereas observations do, suggesting that Simba's X-ray feedback should be more active at high-z. Reproducing the central sSFR depression in z = 0 green valley galaxies represents a unique success of Simba, but the remaining discrepancies highlight the importance of SFR and gas profiles in constraining the physical mechanisms by which galaxies quench.

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supporting

confidence: 66%

The impact of quenching on galaxy profiles in the Simba simulation

Appleby,

Davé,

Kraljic

et al. 2019

Preprint

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“…This, however, stands in diametric contrast to the wellestablished phenomenon of star formation quenching (SFQ) in the centers of massive (L L ) late-type galaxies. A strong depression or complete cessation of star formation (SF) activity within the bulge radius R B of these systems has been documented through photometry (e.g., Balcells & Peletier 1994;Peletier & Balcells 1996;de Jong & van der Kruit 1994) and, more recently, the centrally decreasing SF surface density, sSFR, and Hα equivalent width, and increasing age within R B using integral field spectroscopy (IFS) data (Pérez et al 2013;Fang et al 2013;González-Delgado et al 2014;Catalán-Torrecilla et al 2017;Belfiore et al 2018;Zibetti et al 2017;Breda & Papaderos 2018;Quai et al 2019;Kalinova et al 2021).…”

Section: Introductionmentioning

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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“…Galaxies become 'quenched' when they are no longer able to form stars, either because they have depleted their reservoir of cold, dense gas (e.g., Quai et al 2019), or because their gas has been heated and/or removed by stellar and/or AGN feedback (e.g., Lynds 1967;Heckman et al 2000;Pettini et al 2000;Ohyama et al 2002;Kraft et al 2009;Feruglio et al 2010;Cicone et al 2012;Tombesi et al 2013;Teng et al 2014, see also Bower et al 2017; for theoretical studies). These feedback processes redistribute gas and metals with the galaxy, and galaxy mergers can also greatly affect stellar orbits.…”

Section: Introductionmentioning

confidence: 99%

Oxygen Loss from Simulated Galaxies and the Metal Flow Main Sequence: Predicting the Dependence on Mass and Environment

Taylor,

Kobayashi,

Kewley

2020

Preprint

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We predict the mass fraction of oxygen lost from galaxies in a cosmological simulation as a function of stellar mass and environment at the present day. The distribution with stellar mass is bimodal, separating star-forming and quenched galaxies. The metallicity of gas and stars is self-consistently calculated using a chemical evolution model that includes supernovae type II and Ia, hypernovae, and asymptotic giant branch stars. The mass of oxygen lost from each galaxy is calculated by comparing the existing oxygen in gas and stars in the galaxy to the oxygen that should have been produced by the present-day population of stars. More massive galaxies are able to retain a greater fraction of their metals (∼ 100 per cent) than low-mass galaxies (∼ 40 − 70 per cent). As in the star formation main sequence, star-forming galaxies follow a tight relationship also in terms of oxygen mass lost -a metal flow main sequence, ZFMS -whereas massive quenched galaxies tend to have lost a greater fraction of oxygen (up to 20 per cent), due to AGN-driven winds. The amount of oxygen lost by satellite galaxies depends on the details of their interaction history, and those in richer groups tend to have lost a greater fraction of their oxygen. Observational estimates of metal retention in galaxies will provide a strong constraint on models of galaxy evolution.

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Spatially resolved signature of quenching in star-forming galaxies

Cited by 12 publications

References 138 publications

The impact of quenching on galaxy profiles in the Simba simulation

The impact of quenching on galaxy profiles in the Simba simulation

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

Oxygen Loss from Simulated Galaxies and the Metal Flow Main Sequence: Predicting the Dependence on Mass and Environment

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