Extended star-forming regions within galaxies in a dense proto-cluster core at <i>z</i> = 2.53

Suzuki, Tomoko L.; Minowa, Yosuke; Koyama, Yusei; Kodama, Tadayuki; Hayashi, Masao; Shimakawa, Rhythm; Tanaka, Ichi; Tadaki, Ken-ichi

doi:10.1093/pasj/psz047

Cited by 13 publications

(10 citation statements)

References 87 publications

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“…The compact dust emission in our ALMA sample appears to be inconsistent with previous results that showed that the Hα emission is more extended than the stellar continuum emission in less massive, less dusty SFGs at z∼2 (Suzuki et al 2019;Wilman et al 2020). Note that our targets are all massive SFGs with >…”

Section: Discussioncontrasting

confidence: 99%

“…The centrally rising sSFR profiles seem to be at odds with previous studies that have applied dust gradient corrections to translate Hα profiles to SFR profiles, finding that dustcorrected sSFR profiles are centrally dipping in massive SFGs at z∼2 (Tacchella et al 2015(Tacchella et al , 2018Suzuki et al 2019). This difference may be due to underestimates of the central dust extinction and/or the different sample selection.…”

Section: Spatially Resolved Stellar Mass and Sfrcontrasting

confidence: 75%

“…In the stellar mass range of M å <10 11 M ☉ , the majority of SFGs at z=2 have an extended disk with = R 2 5 kpc e -(e.g., Genzel et al 2006;Law et al 2012;van der Wel et al 2014;Förster Schreiber et al 2018) and form stars in the more extended disk (Tacchella et al 2015;van Dokkum et al 2015;Nelson et al 2016a;Suzuki et al 2019;Wilman et al 2020). This inside-out growth scenario is also supported by a positive slope in the stellar mass-size relation (van der Wel et al 2014).…”

Section: Introductionmentioning

confidence: 96%

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Structural Evolution in Massive Galaxies at z ∼ 2

Tadaki

Belli

Burkert

et al. 2020

ApJ

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We present 0 2 resolution Atacama Large Millimeter/submillimeter Array (ALMA) observations at 870 μm in a stellar mass-selected sample of 85 massive ( >  1kpc 10.5☉ , which is around the boundary between massive SFGs and QGs. These results suggest an outside-in transformation scenario in which a dense core is formed at the center of a more extended disk, likely via dissipative in-disk inflows. Synchronized observations at ALMA 870 μm and James Webb Space Telescope 3-4 μm will explicitly verify this scenario.

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Section: Discussioncontrasting

confidence: 99%

Section: Spatially Resolved Stellar Mass and Sfrcontrasting

confidence: 75%

Section: Introductionmentioning

confidence: 96%

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Structural Evolution in Massive Galaxies at z ∼ 2

Tadaki

Belli

Burkert

et al. 2020

ApJ

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“…These inverse gradients are contrary to what is observed in the majority of both SF and Q galaxies: there is in fact overwhelming evidence that most galaxies form in an inside-out fashion. Firstly, by comparing the size of the star-forming gas disc to the size of the stellar disc, the instantaneous radial growth rate of SF galaxies has been shown to be positive (Pezzulli et al 2015;Wang et al 2019;Nelson et al 2016;Paulino-Afonso et al 2017;Suzuki et al 2019). Secondly, the stellar populations of most SF and Q galaxies have negative age gradients with radius (e.g.…”

mentioning

confidence: 99%

Inverse stellar population age gradients of post-starburst galaxies at z = 0.8 with LEGA-C

D’Eugenio

Wel

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We use deep, spatially resolved spectroscopy from the LEGA-C Survey to study radial variations in the stellar population of 17 spectroscopically-selected post-starburst (PSB) galaxies. We use spectral fitting to measure two Lick indices, HδA and Fe4383, and find that, on average, PSB galaxies have radially decreasing HδA and increasing Fe4383 profiles. In contrast, a control sample of quiescent, non-PSB galaxies in the same mass range shows outwardly increasing HδA and decreasing Fe4383. The observed gradients are weak (≈−0.2Å/Re), mainly due to seeing convolution. A two-SSP model suggests intrinsic gradients are as strong as observed in local PSB galaxies (≈−0.8Å/Re). We interpret these results in terms of inside-out growth (for the bulk of the quiescent population) vs star formation occurring last in the centre (for PSB galaxies). At z ≈ 0.8, central starbursts are often the result of gas-rich mergers, as evidenced by the high fraction of PSB galaxies with disturbed morphologies and tidal features (40%). Our results provide additional evidence for multiple paths to quiescence: a standard path, associated with inside-out disc formation and with gradually decreasing star-formation activity, without fundamental structural transformation, and a fast path, associated with centrally-concentrated starbursts, leaving an inverse age gradient and smaller half-light radius.

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“…Moreover, they have shown that the difference of the light profiles has become larger with increasing stellar mass. Also at z > 2, Suzuki et al (2019) have revealed extended Hα profiles with AO-assisted imaging data. These results indicate at a fixed aperture size one potentially might miss Hα flux at large radii.…”

Section: Hα Luminosity Functionmentioning

confidence: 85%

A selection of Hα emitters at z = 2.1-2.5 using the Ks-band photometry of ZFOURGE

Terao¹,

Spitler²,

Motohara³

2022

Preprint

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Large and less-biased samples of star-forming galaxies are essential to investigate galaxy evolution. Hα emission line is one of the most reliable tracers of star-forming galaxies because its strength is directly related to recent star formation. However, it is observationally expensive to construct large samples of Hα emitters by spectroscopic or narrow-band imaging survey at high-redshifts. In this work, we demonstrate a method to extract Hα fluxes of galaxies at z = 2.1-2.5 from K s broadband photometry of ZFOURGE catalog. Combined with 25-39 other filters, we estimate the emission line fluxes by SED fitting with stellar population models that incorporate emission-line strengths. 2005 galaxies are selected as Hα emitters by our method and their fluxes show good agreement with previous measurements in the literature. On the other hand, there are more Hα luminous galaxies than previously reported. The discrepancy can be explained by extended Hα profiles of massive galaxies and a luminosity dependence of dust attenuation, which are not taken into account in the previous work. We also find that there are a large number of low-mass galaxies with much higher specific star formation rate (sSFR) than expected from the extrapolated star formation main sequence. Such lowmass galaxies exhibit larger ratios between Hα and UV fluxes compared to more massive high sSFR galaxies. This result implies that a "starburst" mode may differ among galaxies: low-mass galaxies appear to assemble their stellar mass via short-duration bursts while more massive galaxies tend to experience longer-duration (> 10 Myr) bursts.

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Extended star-forming regions within galaxies in a dense proto-cluster core at z = 2.53

Cited by 13 publications

References 87 publications

Structural Evolution in Massive Galaxies at z ∼ 2

Structural Evolution in Massive Galaxies at z ∼ 2

Inverse stellar population age gradients of post-starburst galaxies at z = 0.8 with LEGA-C

A selection of Hα emitters at z = 2.1-2.5 using the Ks-band photometry of ZFOURGE

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