THE SPATIALLY RESOLVED NUV–r COLOR OF LOCAL STAR-FORMING GALAXIES AND CLUES FOR QUENCHING

Pan, Zhifen; Zheng, Xianzhong; Lin, Weipeng; Li, Jinrong; Wang, Jing; Fan, Lulu; Kong, Xu

doi:10.3847/0004-637x/819/2/91

Cited by 20 publications

(19 citation statements)

References 101 publications

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“…In NUV−u, the median of the colour difference is 0.23 mag; in u−i, the median of the colour difference is 0.19 mag. This negative colour offset is consistent with previous work (Pan et al 2014(Pan et al , 2016 where the authors found similar negative gradient in the NUV−optical colours in local galaxies. Nevertheless, there is a small fraction of galaxies having blue star-forming outer part but red quiescent inner part.…”

Section: Colour Distributionsupporting

confidence: 93%

Inside-out growth or inside-out quenching? Clues from colour gradients of local galaxies

Lian

Yan

Blanton

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We constrain the spatial gradient of star formation history within galaxies using the colour gradients in NUV−u and u − i for a local spatially-resolved galaxy sample. By splitting each galaxy into an inner and an outer part, we find that most galaxies show negative gradients in these two colours. We first rule out dust extinction gradient and metallicity gradient as the dominant source for the colour gradient. Then using stellar population models, we explore variations in star formation history to explain the colour gradients. As shown by our earlier work, a two-phase SFH consisting of an early secular evolution (growth) phase and a subsequent rapid evolution (quenching) phase is necessary to explain the observed colour distributions among galaxies. We explore two different inside-out growth models and two different inside-out quenching models by varying parameters of the SFH between inner and outer regions of galaxies. Two of the models can explain the observed range of colour gradients in NUV−u and u − i colours. We further distinguish them using an additional constraint provided by the u − i colour gradient distribution, under the assumption of constant galaxy formation rate and a common SFH followed by most galaxies. We find the best model is an inside-out growth model in which the inner region has a shorter e-folding time scale in the growth phase than the outer region. More spatially resolved ultraviolet (UV) observations are needed to improve the significance of the result.

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Section: Colour Distributionsupporting

confidence: 93%

Inside-out growth or inside-out quenching? Clues from colour gradients of local galaxies

Lian

Yan

Blanton

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Histories of stellar mass assembly for galaxies are mainly classified into two distinct modes: "inside-out" and "outsidein" (Pan et al 2016;). In the "inside-out" assembly mode, star formation quenching takes place first in the center region of a galaxy, which may be due to AGN feedback depleting, heating or blowing out the gas in galactic center (e.g., Kauffmann et al 2004, Croton et al 2006, Fabian 2012, Dekel & Burkert 2014 or the bulge stabilizing gas in the disk from collapsing (i.e., so-called "morphological quenching"; Martig et al 2009).…”

Section: Structure Transformation and Quenchingmentioning

confidence: 99%

The Mass Dependence of Structure, Star Formation Rate, and Mass Assembly Mode at 0.5 < z < 2.5

Fang

Yuan

et al. 2019

ApJ

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To investigate the mass dependence of structural transformation and star formation quenching, we construct three galaxy samples using massive (M * > 10 10 M ⊙ ) red, green, and blue galaxy populations at 0.5 < z < 2.5 in five 3D-HST/CANDELS fields. The structural parameters, including effective radius (r e ), galaxy compactness (Σ 1.5 ), and second order moment of 20% brightest pixels (M 20 ) are found to be correlated with stellar mass. Sérsic index (n), concentration (C), and Gini coefficient (G) seem to be insensitive to stellar mass. The morphological distinction between blue and red galaxies is found at a fixed mass bin, suggesting that quenching processes should be accompanied with transformations of galaxy structure and morphology. Except for r e and Σ 1.5 at high mass end, structural parameters of green galaxies are intermediate between red and blue galaxies in each stellar mass bin at z < 2, indicating green galaxies are at a transitional phase when blue galaxies are being quenched into quiescent statuses. The similar sizes and compactness for the blue and green galaxies at high-mass end implies that these galaxies will not appear to be significantly shrunk until they are completely quenched into red QGs. For the green galaxies at 0.5 < z < 1.5, a morphological transformation sequence of bulge buildup can be seen as they are gradually shut down their star formation activities, while a faster morphological transformation is verified for the green galaxies at 1.5 < z < 2.5.

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“…Galaxies appear to assemble their stellar mass mainly in two distinct modes: the "inside-out" and the "outside-in" mode (Pan et al 2016;Pérez et al 2013;Ibarra-Medel et al 2016;Goddard et al 2017). In the inside-out assembly mode, star formation cessation occurs first in galactic center with respect to the outskirts, which may be due to active galactic nucleus feedback (e.g.…”

Section: Introductionmentioning

confidence: 99%

The Properties of the Massive Star-forming Galaxies with an Outside-in Assembly Mode

Wang

Kong

Wang

et al. 2017

ApJ

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Previous findings show that massive (M * > 10 10 M ⊙ ) star-forming (SF) galaxies usually have an "inside-out" stellar mass assembly mode. In this paper, we have for the first time selected a sample of 77 massive SF galaxies with an "outside-in" assembly mode (called "targeted sample") from the Mapping Nearby Galaxies at the Apache Point Observatory (MaNGA) survey. For comparison, two control samples are constructed from MaNGA sample matched in stellar mass: a sample of 154 normal SF galaxies and a sample of 62 quiescent galaxies. In contrast to normal SF galaxies, the targeted galaxies appear to be more smooth-like and bulge-dominated, and have smaller size, higher concentration, higher star formation rate and higher gas-phase metallicity as a whole. However, they have larger size and lower concentration than quiescent galaxies. Unlike normal SF sample, the targeted sample exhibits a slightly positive gradient of 4000Å break and a pronounced negative gradient of Hα equivalent width. Further more, their median surface mass density profile is between that of normal SF sample and quiescent sample, indicating that the gas accretion of quiescent galaxies is not likely to be the main approach for the outside-in assembly mode. Our results suggest that the targeted galaxies are likely in the transitional phase from normal SF galaxies to quiescent galaxies, with rapid on-going central stellar mass assembly (or bulge growth). We discuss several possible formation mechanisms for the outside-in mass assembly mode.

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THE SPATIALLY RESOLVED NUV–r COLOR OF LOCAL STAR-FORMING GALAXIES AND CLUES FOR QUENCHING

Cited by 20 publications

References 101 publications

Inside-out growth or inside-out quenching? Clues from colour gradients of local galaxies

Inside-out growth or inside-out quenching? Clues from colour gradients of local galaxies

The Mass Dependence of Structure, Star Formation Rate, and Mass Assembly Mode at 0.5 < z < 2.5

The Properties of the Massive Star-forming Galaxies with an Outside-in Assembly Mode

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