Physical Properties of Sub-galactic Clumps at 0.5 ≤ Z ≤ 1.5 in the UVUDF

Soto, Emmaris; Mello, D. F. de; Rafelski, Marc; Gardner, Jonathan P.; Teplitz, Harry I.; Koekemoer, Anton M.; Ravindranath, Swara; Grogin, Norman A.; Scarlata, Claudia; Kurczynski, Peter; Gawiser, Eric

doi:10.3847/1538-4357/aa5da3

Cited by 53 publications

(81 citation statements)

References 90 publications

(161 reference statements)

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“…We choose rest-frame NUV because it is observed by HST filters for the whole GOODS-S field across the redshift range of z 0.5 3.0  < . Some clumps are brighter and more prominent in rest-frame far-UV ( 1500 Å), as found by Soto et al (2017), which makes far-UV also an efficient band to detect active starforming clumps. However, deep far-UV observations are only available for about one-third of the area of GOODS-S for galaxies at z 0.5 1.5  <…”

Section: Clump Samplementioning

confidence: 67%

“…These clumps are seen in deep and high-resolution rest-frame UV and optical images (e.g., Conselice et al 2004;Elmegreen & Elmegreen 2005;Elmegreen et al 2007Elmegreen et al , 2009aFörster Schreiber et al 2011;Guo et al 2012bGuo et al , 2015Wuyts et al 2012;Murata et al 2014;Tadaki et al 2014;Shibuya et al 2016;Soto et al 2017). They are also detected in highresolution emission-line maps of Hα (e.g., Genzel et al 2008Genzel et al , 2011Wisnioski et al 2011;Livermore et al 2012Livermore et al , 2015Mieda et al 2016;Fisher et al 2017a) and CO (e.g., Jones et al 2010;Swinbank et al 2010;Dessauges-Zavadsky et al 2017b).…”

Section: Overview: Clumps and Their Formation And Evolutionmentioning

confidence: 93%

“…The clumps appear to be much larger, brighter, and more massive than local star-forming regions. Their typical stellar mass (M * ) is M 10 10 7 9  -(e.g., Elmegreen et al 2007;Guo et al 2012b;Soto et al 2017). Their actual sizes are uncertain due to the resolution limit of current observations, ranging from ∼1 kpc (e.g., Elmegreen et al 2007;Förster Schreiber et al 2011) to a few hundred pc (e.g., Livermore et al 2012).…”

Section: Overview: Clumps and Their Formation And Evolutionmentioning

confidence: 99%

“…After PSF matching to the F160W resolution, some clumps may disappear due to the reduced contrast between clumps and the background. Moreover, some intrinsically blue clumps are almost "invisible" in red bands (e.g., F160W), again due to small clump-background contrasts (e.g., see clumps in Figure 2 and discussion in Soto et al 2017). For these clumps, we fix their centers as those detected in the non-PSF-matched NUV bands to measure the aperture photometry.…”

Section: Tablementioning

confidence: 99%

“…Current facilities enable us to resolve distant galaxies and study their spatially resolved physical properties, including (I) substructures (e.g., Elmegreen & Elmegreen 2005;Elmegreen et al 2007Elmegreen et al , 2009aElmegreen et al , 2009bGenzel et al 2008Genzel et al , 2011Förster Schreiber et al 2011;Guo et al 2012bGuo et al , 2015Wuyts et al 2012;Tadaki et al 2014;Shibuya et al 2016;Soto et al 2017), (II) color variation (e.g., Menanteau et al 2004;McGrath et al 2008;Tortora et al 2010;Gargiulo et al 2011Gargiulo et al , 2012Guo et al 2011;Szomoru et al 2011;Boada et al 2015;Tacchella et al 2015b;Chan et al 2016;Liu et al 2016), (III) star formation variation (e.g., Wuyts et al 2013;Hemmati et al 2014Hemmati et al , 2015Tacchella et al 2015a;Barro et al 2016;Mieda et al 2016;Nelson et al 2016aNelson et al , 2016b, and (IV) mass distribution and central concentration (e.g., Saracco et al 2012;Szomoru et al 2013;Lang et al 2014;van Dokkum et al 2014;Barro et al 2017;Mosleh et al 2017).…”

Section: Overview: Clumps and Their Formation And Evolutionmentioning

confidence: 99%

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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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108

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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: Clump Samplementioning

confidence: 67%

Section: Overview: Clumps and Their Formation And Evolutionmentioning

confidence: 93%

Section: Overview: Clumps and Their Formation And Evolutionmentioning

confidence: 99%

Section: Tablementioning

confidence: 99%

Section: Overview: Clumps and Their Formation And Evolutionmentioning

confidence: 99%

See 3 more Smart Citations

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

Guo

Rafelski

Bell

et al. 2018

ApJ

Self Cite

108

150

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The cold gas supply through cosmic time: insights on the galaxy assembly at early epochs

Aravena

2021

Proc. IAU

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Abstract.Remarkable progress has been made in the last few years in understanding the global properties of galaxies and how they evolve through cosmic time. Major focus has been given to studies of how the availability of molecular gas regulates star-forming activity and galaxy growth, the eventual quenching of star formation, and how these mechanisms evolve through cosmic time. Most of these advances have been made thanks to ALMA and the upgraded capabilities of NOEMA. In this contribution, I briey review the latest constraints on the molecular gas content based on dierent tracers of the interstellar medium (ISM; dust continuum and CO, [CI] and [CII] line emission), including recent determinations of the molecular gas fraction, gas depletion timescales, and molecular gas cosmic density provided by the recent ALMA programs out to z ∼ 7. Finally, I concentrate on recent and ongoing studies aiming to spatially and kinematically resolve the cold ISM and star formation activity down to kpc scales in galaxies out to z ∼ 6 – 7, which represent an unprecedented view of the galaxy assembly and feedback processes in the early universe.

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The nature of giant clumps in distant galaxies probed by the anatomy of the cosmic snake

et al. 2017

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Giant stellar clumps are ubiquitous in high-redshift galaxies. 1,2 They are thought to play an important role in the build-up of galactic bulges 3 and as diagnostics of star formation feedback in galactic discs. M and linear sizes > ∼ 1 kpc. 5,6 Recently, gravitational lensing has also been used to get higher spatial resolution. [7][8][9] However, both recent lensed observations 10,11 and models 12,13 suggest that the clumps properties may be overestimated by the limited resolution of standard imaging techniques. A definitive proof of this observational bias is nevertheless still missing. Here we investigate 1 arXiv:1711.03977v1 [astro-ph.GA] 10 Nov 2017 directly the effect of resolution on clump properties by analysing multiple gravitationallylensed images of the same galaxy at different spatial resolutions, down to 30 pc. We show that the typical mass and size of giant clumps, generally observed at ∼1 kpc resolution in high-redshift galaxies, are systematically overestimated. The high spatial resolution data, only enabled by strong gravitational lensing using currently available facilities, support smaller scales of clump formation by fragmentation of the galactic gas disk via gravitational instabilities.The multiply imaged galaxy situated behind the central region of the cluster MACSJ1206.2-084747 14 (Figure 1a) is the perfect target for our experiment. Figure 1b shows two images of this galaxy: a strongly lensed one whose peculiar shape led us to name it the "Cosmic Snake", and a more regular and less amplified one (the "Counterimage"). For the source galaxy we have estimated, from spectral energy distribution (SED) fitting (see Methods), a total stellar mass M * ∼ 4×10 10 M , and total SFR∼ 30M yrThis places the galaxy on the main sequence of star-forming galaxies at z ∼ 1-2, providing a target with physical properties comparable to typical high redshift clumpy galaxies. 15,16 According to our tailored lensing model (see Methods) the Cosmic Snake is composed by four elongated and stretched images (Figure 1c) of the southern half of the source galaxy, imaged with magnifications covering a wide range from a few to hundreds times ( Figure 1d). In contrast, the Counterimage is located in a region of nearly constant amplification, with an average magnification of µ 4.5, and shows the entire source galaxy. These extremely different magnifications allow us to inspect features of the galaxy on very different intrinsic physical scales.Using high-quality data from the Cluster Lensing And Supernova survey with Hubble (CLA-SH; 17), we have identified clumps in the Cosmic Snake and the Counterimage starting from the rest-frame UV band (HST-WFC3 filter F390W). This filter shows clumps with a high 2 Figure 1 | Overview of the Cosmic Snake and the Counterimage. a, Portion of the HST field of view showing an RGB color composite image (R = F160W, G = F110W, B =F606W) of the cluster MACSJ1206.2-0847 including the giant arc (Cosmic Snake) and its Counterimage. b, Zoomed view of the Cosmic Snake (bottom) and the Counterimage(to...

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Physical Properties of Sub-galactic Clumps at 0.5 ≤ Z ≤ 1.5 in the UVUDF

Cited by 53 publications

References 90 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

The cold gas supply through cosmic time: insights on the galaxy assembly at early epochs

The nature of giant clumps in distant galaxies probed by the anatomy of the cosmic snake

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