Revisiting the Color–Color Selection: Submillimeter and AGN Properties of NUV–r–J Selected Quiescent Galaxies

Hwang, Yu-Hsuan; Wang, Weihao; Chang, Yu-Yen; Lim, Chen-Fatt; Chen, Chian-Chou; Gao, Zhen-Kai; Dunlop, James; Gao, Yu; Ho, Luis C.; Hwang, Ho Seong; Koprowski, M. P.; Michalowski, Michal; Peng, Yingjie; Shim, Hyunjin; Simpson, J. M.; Toba, Yoshiki

doi:10.3847/1538-4357/abf11a

“…Finally, we discuss the choice of a synthetic u s filter over an ultraviolet one (e.g., rest-frame NUV ). NUV − r or FUV − V color selection, for instance, is a better discriminator of current versus past star formation activity than that of U − V (Arnouts et al 2007;Martin et al 2007;Ilbert et al 2010Ilbert et al , 2013Man et al 2016;Leja et al 2019b;Hwang et al 2021). Similarly, the FUV − V color has also been shown to have a much stronger correlation with specific SFR (Leja et al 2019b).…”

Section: The Ideal Filter Combinationmentioning

confidence: 99%

“…Similarly, the FUV − V color has also been shown to have a much stronger correlation with specific SFR (Leja et al 2019b). NUVrJselected quiescent samples have also been shown to have low contamination (10%-15%) from dusty star-forming galaxies at z 3 (Man et al 2016;Hwang et al 2021). These are all reasons to choose an ultraviolet filter over an optical u filter.…”

Section: The Ideal Filter Combinationmentioning

confidence: 99%

Beyond UVJ: Color Selection of Galaxies in the JWST Era

Antwi-Danso

¹

,

Papovich

²

,

Leja

³

et al. 2023

ApJ

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We present a new rest-frame color–color selection method using synthetic u s − g s and g s − i s , (ugi) s colors to identify star-forming and quiescent galaxies. Our method is similar to the widely used U − V versus V − J (UVJ) diagram. However, UVJ suffers known systematics. Spectroscopic campaigns have shown that UVJ-selected quiescent samples at z ≳ 3 include ∼10%–30% contamination from galaxies with dust-obscured star formation and strong emission lines. Moreover, at z > 3, UVJ colors are extrapolated because the rest-frame band shifts beyond the coverage of the deepest bandpasses at <5 μm (typically Spitzer/IRAC 4.5 μm or future JWST/NIRCam observations). We demonstrate that (ugi) s offers improvements to UVJ at z > 3, and can be applied to galaxies in the JWST era. We apply (ugi) s selection to galaxies at 0.5 < z < 6 from the (observed) 3D-HST and UltraVISTA catalogs, and to the (simulated) JAGUAR catalogs. We show that extrapolation can affect (V − J)0 color by up to 1 mag, but changes ( g s − i s ) 0 color by ≤0.2 mag, even at z ≃ 6. While (ugi) s -selected quiescent samples are comparable to UVJ in completeness (both achieve ∼85%–90% at z = 3–3.5), (ugi) s reduces contamination in quiescent samples by nearly a factor of 2, from ≃35% to ≃17% at z = 3, and from ≃60% to ≃33% at z = 6. This leads to improvements in the true-to-false-positive ratio (TP/FP), where we find TP/FP ≳2.2 for (ugi) s at z ≃ 3.5 − 6, compared to TP/FP < 1 for UVJ-selected samples. This indicates that contaminants will outnumber true quiescent galaxies in UVJ at these redshifts, while (ugi) s will provide higher-fidelity samples.

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“…This would be expected if the rest-frame fluxes were measured directly from the template, but in this case they are weighted by the observed fluxes, and so the conclusion is that the different selections are generally measuring the same observed SED shape. Hwang et al (2021), who compared NUVrJ-and UVJ-selected samples at 0 < z < 3 in COSMOS2015, found a similar overlap (∼85%). This suggests that the choice of rest-frame color diagram selection at z < 3 is not crucial, although modifications to both UVJ and NUVrJ color selections may be in order.…”

Section: Comparing Gmm/nuv − Vj To Uvj and Nuvrj Color Selectionsmentioning

confidence: 70%

“…We could simply use this value to decide what to classify as quiescent, however this does not account for the errors in a galaxy's colors. To assign each galaxy a probability of belonging to the quiescent group, which is identified by eye as the component in the quiescent area of UVJ space, we instead take the following approach, inspired by Hwang et al (2021). Each galaxy has rest-frame fluxes in the NUV, U, V, and J bands, and associated errors.…”

Section: Defining the Separatormentioning

confidence: 99%

“…These selections were originally designed to separate galaxy populations at low redshift, but as newer data have emerged demonstrating that the bimodality in populations clearly extends to higher redshift (e.g., Whitaker et al 2011;Ilbert et al 2013;Muzzin et al 2013;Straatman et al 2014), the selections and variations thereof are now often adopted at z > 2 (e.g., Whitaker et al 2012;Straatman et al 2014;Hwang et al 2021;Ji & Giavalisco 2022;Suzuki et al 2022). In sum, restframe color-color diagrams are ideal to select quiescent populations as they are computationally cheap and straightforward.…”

Section: Introductionmentioning

confidence: 99%

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COSMOS2020: Exploring the Dawn of Quenching for Massive Galaxies at 3 < z < 5 with a New Color-selection Method

Gould

¹

,

Brammer

²

,

Valentino

³

et al. 2023

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We select and characterize a sample of massive (log(M */M ⊙) > 10.6) quiescent galaxies (QGs) at 3 < z < 5 in the latest Cosmological Evolution Survey catalog (COSMOS2020). QGs are selected using a new rest-frame color-selection method, based on their probability of belonging to the quiescent group defined by a Gaussian mixture model (GMM) trained on rest-frame colors (NUV − U, U − V, V − J) of similarly massive galaxies at 2 < z < 3. We calculate the quiescent probability threshold above which a galaxy is classified as quiescent using simulated galaxies from the shark semi-analytical model. We find that, at z ≥ 3 in shark, the GMM/NUVU − VJ method outperforms classical rest-frame UVJ selection and is a viable alternative. We select galaxies as quiescent based on their probability in COSMOS2020 at 3 < z < 5, and compare the selected sample to both UVJ- and NUVrJ-selected samples. We find that, although the new selection matches UVJ and NUVrJ in number, the overlap between color selections is only ∼50%–80%, implying that rest-frame color commonly used at lower-redshift selections cannot be equivalently used at z > 3. We compute median rest-frame spectral energy distributions for our sample and find the median QG at 3 < z < 5 has a strong Balmer/4000 Å break, and residual NUV flux indicating recent quenching. We find the number densities of the entire quiescent population (including post-starbursts) more than doubles from 3.5 ± 2.2 × 10−6 Mpc−3 at 4 < z < 5 to 1.4 ± 0.4 × 10−5 Mpc−3 at 3 < z < 4, confirming that the onset of massive galaxy quenching occurs as early as 3 < z < 5.

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The structure of massive star-forming galaxies from JWST and ALMA: Dusty, high-redshift disc galaxies

Gillman,

Smail,

Gullberg

et al. 2024

A&A

1

0

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We present an analysis of the NIRCam and MIRI morphological and structural properties of 80 massive ($ (M_ M_ odot )$\,=\,11.2\,pm \,0.1) dusty star-forming galaxies at $, identified as sub-millimetre galaxies (SMGs) by ALMA, which have been observed as part of the PRIMER project. To compare the structure of these massive, active galaxies to more typical, less actively star-forming galaxies, we defined two comparison samples. The first of 850 field galaxies matched in specific star formation rate and redshift and the second of 80 field galaxies matched in stellar mass . From the visual classification of the SMGs, we have identified 20\,pm \,5<!PCT!> as candidate late-stage major mergers, a further 40\,pm \,10<!PCT!> as potential minor mergers, and 40\,pm \,10<!PCT!> that have comparatively undisturbed disc-like morphologies, with no obvious massive neighbours on lesssim \,20\,--\,30\,kpc (projected) scales. These rates are comparable to those for the field samples and indicate that the majority of the sub-millimetre-detected galaxies are not late-stage major mergers, but have interaction rates similar to the general field population at $z$\,sim \,2--3. Through a multi-wavelength morphological analysis, using parametric and non-parametric techniques, we establish that SMGs have comparable near-infrared, mass-normalised sizes to the less active population, $ F444W $\,=\,2.7\,pm \,0.2\,kpc versus $ F444W $\,=\,3.1\,pm \,0.1\,kpc, but exhibit lower S\'ersic indices, consistent with bulge-less discs: F444W $\,=\,1.1\,pm \,0.1, compared to F444W $\,=\,1.9\,pm \,0.1 for the less active field galaxies and $n_ F444W $\,=\,2.8\,pm \,0.2 for the most massive field galaxies . The SMGs exhibit greater single-S\'ersic fit residuals and their morphologies are more structured at 2 relative to 4 when compared to the field galaxies. This appears to be caused by significant structured dust content in the SMGs and we find evidence for dust reddening as the origin of the morphological differences by identifying a strong correlation between the F200W$-$F444W pixel colour and the 870 surface brightness using high-resolution ALMA observations. We conclude that SMGs and both massive and less massive star-forming galaxies at the same epochs share a common disc-like structure, but the weaker bulge components (and potentially lower black hole masses) of the SMGs result in their gas discs being less stable. Consequently, the combination of high gas masses and instabilities triggered either secularly or by minor external perturbations results in higher levels of activity (and dust content) in SMGs compared to typical star-forming galaxies.

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Revisiting the Color–Color Selection: Submillimeter and AGN Properties of NUV–r–J Selected Quiescent Galaxies

Cited by 6 publications

References 91 publications

Beyond UVJ: Color Selection of Galaxies in the JWST Era

Beyond UVJ: Color Selection of Galaxies in the JWST Era

COSMOS2020: Exploring the Dawn of Quenching for Massive Galaxies at 3 < z < 5 with a New Color-selection Method

The structure of massive star-forming galaxies from JWST and ALMA: Dusty, high-redshift disc galaxies

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