UVI colour gradients of 0.4 &lt; z &lt; 1.4 star-forming main-sequence galaxies in CANDELS: dust extinction and star formation profiles

Wang, Weichen; Faber, S. M.; Liu, F. S.; Guo, Y.; Pacifici, Camilla; Koo, David C.; Kassin, Susan; Mao, Shude; Fang, Jerome J.; Chen, Zhu; Koekemoer, Anton M.; Kocevski, Dale D.

doi:10.1093/mnras/stx1148

Cited by 41 publications

(34 citation statements)

References 99 publications

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“…We also find marginal evidence (through a linear fit) that the slope of intra-clump regions' color gradient becomes steeper with galaxy M * at z 1  . This result is consistent with recent studies of the color gradient of integrated light in galaxies, e.g., Liu et al (2016), Tacchella et al (2017), and Wang et al (2017). Figure 8 implies that clumps' color gradient at z 2 < would be changed if the colors were measured by using the fluxes without background subtraction.…”

Section: Radial Variation Of Clump Color (Color Gradient)supporting

confidence: 92%

“…We compare our measurements (brown lines in Figure 10) with those of Wang et al (2017;green dashed lines) and Tacchella et al (2017;purple dashed line). The methods used by Wang et al and Tacchella et al are different from ours.…”

Section: Dust Extinction Gradientsupporting

confidence: 54%

“…Similar to Figure 9, but for the radial gradient of dust extinction, E(B−V ), of clumps. Green and purple dashed lines show the E(B−V ) profiles measured by Wang et al (2017) and Tacchella et al (2017).…”

Section: Dust Extinction Gradientmentioning

confidence: 89%

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Clumpy Galaxies in CANDELS. II. Physical Properties of UV-bright Clumps at 0.5 ≤ z < 3

Guo

Rafelski

Bell

et al. 2018

ApJ

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Studying giant star-forming clumps in distant galaxies is important to understand galaxy formation and evolution. At present, however, observers and theorists have not reached a consensus on whether the observed "clumps" in distant galaxies are the same phenomenon that is seen in simulations. In this paper, as a step to establish a benchmark of direct comparisons between observations and theories, we publish a sample of clumps constructed to represent the commonly observed "clumps" in the literature. This sample contains 3193 clumps detected from 1270 galaxies at z 0.5 3.0  < . The clumps are detected from rest-frame UV images, as described in our previous paper. Their physical properties (e.g., rest-frame color, stellar mass (M * ), star formation rate (SFR), age, and dust extinction) are measured by fitting the spectral energy distribution (SED) to synthetic stellar population models. We carefully test the procedures of measuring clump properties, especially the method of subtracting background fluxes from the diffuse component of galaxies. With our fiducial background subtraction, we find a radial clump U−V color variation, where clumps close to galactic centers are redder than those in outskirts. The slope of the color gradient (clump color as a function of their galactocentric distance scaled by the semimajor axis of galaxies) changes with redshift and M * of the host galaxies: at a fixed M * , the slope becomes steeper toward low redshift, and at a fixed redshift, it becomes slightly steeper with M * . Based on our SED fitting, this observed color gradient can be explained by a combination of a negative age gradient, a negative E(B−V ) gradient, and a positive specific SFR gradient of the clumps. We also find that the color gradients of clumps are steeper than those of intra-clump regions. Correspondingly, the radial gradients of the derived physical properties of clumps are different from those of the diffuse component or intra-clump regions.

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Section: Radial Variation Of Clump Color (Color Gradient)supporting

confidence: 92%

Section: Dust Extinction Gradientsupporting

confidence: 54%

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Clumpy Galaxies in CANDELS. II. Physical Properties of UV-bright Clumps at 0.5 ≤ z < 3

Guo

Rafelski

Bell

et al. 2018

ApJ

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102

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“…For example, Wuyts et al (2011b) shows that galaxies on the main sequence at a fixed stellar mass have a larger size on average at z ∼ 0.1 than at z ∼1. Due to this evolution, and the fact that opacity also varies with radius in galaxies out to at least z < 2 (Tacchella et al 2017;Wang et al 2017), we cannot interpret the slopes of the attenuation-inclination relation reported in this paper in the context of an evolutionary picture for particular galaxies. Instead, we emphasise that the inclination dependence of the UV attenuation in the largest and most massive star-forming disk galaxies at z ∼ 0.7 (which are not necessarily the same galaxies that will end up in our sample at z = 0.07), behaves similarly to that in galaxies selected to have the same stellar mass and radius at z ∼ 0.…”

Section: Evolution Of Disk Opacitymentioning

confidence: 73%

Probing star formation and ISM properties using galaxy disk inclination

Leslie

Sargent

Schinnerer

et al. 2018

A&A

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Disk galaxies at intermediate redshift (z ∼ 0.7) have been found in previous work to display more optically thick behaviour than their local counterparts in the rest-frame B-band surface brightness, suggesting an evolution in dust properties over the past ∼6 Gyr. We compare the measured luminosities of face-on and edge-on star-forming galaxies at different wavelengths (Ultraviolet (UV), midinfrared (MIR), far-infrared (FIR), and radio) for two well-matched samples of disk-dominated galaxies: a local Sloan Digital Sky Survey (SDSS)-selected sample at z ∼ 0.07 and a sample of disks at z ∼ 0.7 drawn from Cosmic Evolution Survey (COSMOS). We have derived correction factors to account for the inclination dependence of the parameters used for sample selection. We find that typical galaxies are transparent at MIR wavelengths at both redshifts, and that the FIR and radio emission is also transparent as expected. However, reduced sensitivity at these wavelengths limits our analysis; we cannot rule out opacity in the FIR or radio. Ultra-violet attenuation has increased between z ∼ 0 and z ∼ 0.7, with the z ∼ 0.7 sample being a factor of ∼3.4 more attenuated. The larger UV attenuation at z ∼ 0.7 can be explained by more clumpy dust around nascent star-forming regions. There is good agreement between the fitted evolution of the normalisation of the SFR UV versus 1-cos(i) trend (interpreted as the clumpiness fraction) and the molecular gas fraction/dust fraction evolution of galaxies found out to z < 1.

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“…It appears that some C-SFB objects have moved up into the green valley, or even merged with the quenched clump using this color. The combination of red g − z plus blue NUV −r could mean dust (e.g., Williams et al 2009;Patel et al 2011;Brammer et al 2011) or composite stellar populations (Wang et al 2017). ∆Σ 1 appears slightly tighter than ∆ µ e in the G09 sample.…”

Section: ∆ µ E and ∆σ 1 Compared To Stellar-population Parametersmentioning

confidence: 88%

Structural and stellar-population properties versus bulge types in Sloan Digital Sky Survey central galaxies

Luo

Faber

Rodríguez-Puebla

et al. 2020

Monthly Notices of the Royal Astronomical Society

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This paper studies pseudo-bulges (P-bulges) and classical bulges (C-bulges) in Sloan Digital Sky Survey central galaxies using the new bulge indicator ∆Σ 1 , which measures relative central stellar-mass surface density within 1 kpc. We compare ∆Σ 1 to the established bulge-type indicator ∆ µ e from Gadotti (2009) and show that classifying by ∆Σ 1 agrees well with ∆ µ e . ∆Σ 1 requires no bulge-disk decomposition and can be measured on SDSS images out to z = 0.07. Bulge types using it are mapped onto twenty different structural and stellar-population properties for 12,000 SDSS central galaxies with masses 10.0 < log M * /M < 10.4. New trends emerge from this large sample. Structural parameters show fairly linear log-log relations vs. ∆Σ 1 and ∆ µ e with only moderate scatter, while stellar-population parameters show a highly non-linear "elbow" in which specific star-formation rate remains roughly flat with increasing central density and then falls rapidly at the elbow, where galaxies begin to quench. P-bulges occupy the low-density end of the horizontal arm of the elbow and are universally star-forming, while C-bulges occupy the elbow and the vertical branch and exhibit a wide range of star-formation rates at fixed density. The nonlinear relation between central density and star-formation rate has been seen before, but this mapping onto bulge class is new. The wide range of star-formation rates in C-bulges helps to explain why bulge classifications using different parameters have sometimes disagreed in the past. The elbow-shaped relation between density and stellar indices suggests that central structure and stellar-populations evolve at different rates as galaxies begin to quench.

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UVI colour gradients of 0.4 < z < 1.4 star-forming main-sequence galaxies in CANDELS: dust extinction and star formation profiles

Cited by 41 publications

References 99 publications

Clumpy Galaxies in CANDELS. II. Physical Properties of UV-bright Clumps at 0.5 ≤ z < 3

Clumpy Galaxies in CANDELS. II. Physical Properties of UV-bright Clumps at 0.5 ≤ z < 3

Probing star formation and ISM properties using galaxy disk inclination

Structural and stellar-population properties versus bulge types in Sloan Digital Sky Survey central galaxies

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