Star Formation in Galaxies at z ∼ 4–5 from the SMUVS Survey: A Clear Starburst/Main-sequence Bimodality for Hα Emitters on the SFR–M* Plane

Caputi, K.; Deshmukh, S.; Ashby, M. L. N.; Cowley, William I.; Bisigello, Laura; Fazio, G. G.; Fynbo, J. P. U.; Fèvre, O. Le; Milvang-Jensen, B.; Ilbert, O.

doi:10.3847/1538-4357/aa901e

Cited by 87 publications

(170 citation statements)

References 92 publications

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“…The color-coding represents the best-fit dust attenuation value. We also draw the SFR-M * relation at z ∼ 4 reported by the previous works , Caputi et al 2017.…”

Section: Relation Between Intrinsic β and Intrinsic M Uvmentioning

confidence: 98%

The UV spectral slope β and stellar population of most active star-forming galaxies at z ∼ 4

Yamanaka

Yamada

2019

Publications of the Astronomical Society of Japan

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We investigate the stellar population of star-forming galaxies at z ∼ 4 by focusing on their slope of rest-frame ultraviolet (UV) continuum, β where f λ ∝ λ β . We investigate the sample of bright Lyman Break Galaxies (LBGs) with i' ≤ 26.0 in the Subaru/XMM-Newton Deep Survey field by using the SED fitting analysis. We find that the apparently redder (β obs > −1.73) LBGs tend to be dusty (Av > 1.0), have the young stellar population (β int < −2.42), and the intrinsically active star-forming galaxies (SFR > ∼ a few × 10 2 M ⊙ yr −1 ). It means that a significant fraction of the UV-selected LBGs at z ∼ 4 is on-going active and dust obscured star-forming galaxies. We compare the IR to UV luminosity ratio assuming the dust attenuation laws with the submillimeter observations from previous works. The result suggests that the Calzetti-like dust attenuation law is preferable for the active and dusty star-forming LBGs at z = 4. We also find that an extrapolation of the β int -M UV,int relation toward the fainter magnitude range below our sample magnitude limit intersects the β obs -M UV,obs relation previously obtained in the deeper narrow-area observations at M UV = −18.9 and β = −1.94, which coincides with the break point of β obs -M UV,obs relation observed so far. The coincidence suggest that we see the almost dust-free population at M UV,obs > ∼ −18.9.

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“…The color-coding represents the best-fit dust attenuation value. We also draw the SFR-M * relation at z ∼ 4 reported by the previous works , Caputi et al 2017.…”

Section: Relation Between Intrinsic β and Intrinsic M Uvmentioning

confidence: 98%

The UV spectral slope β and stellar population of most active star-forming galaxies at z ∼ 4

Yamanaka

Yamada

2019

Publications of the Astronomical Society of Japan

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“…Gray inverse-triangle are the contribution of bright ALESS sources . Gray filled circles are lower and upper limit of the contribution of Hα emitters obtained by Caputi et al (2017). Brown open diamonds indicate the contribution of the ALMA sources obtained by Dunlop et al (2017).…”

Section: Physical Propertiesmentioning

confidence: 99%

ALMA 26 arcmin² Survey of GOODS-S at 1 mm (ASAGAO): Near-infrared-dark Faint ALMA Sources

Yamaguchi

Kohno

Hatsukade

et al. 2019

ApJ

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We report detections of two 1.2 mm continuum sources (S 1.2mm ∼ 0.6 mJy) without any counterparts in the deep H-and/or K-band image (i.e., K-band magnitude 26 mag). These near-infrared-dark faint millimeter sources are uncovered by ASAGAO, a deep and wide-field (≃ 26 arcmin 2 ) Atacama Large Millimeter/submillimeter Array (ALMA) 1.2 mm survey. One has a red IRAC (3.6 and 4.5 µm) counterpart, and the other has been independently detected at 850 and 870 µm using SCUBA2 and ALMA Band 7, respectively. Their optical to radio spectral energy distributions indicate that they can lie at z 3-5 and can be in the early phase of massive galaxy formation. Their contribution to the cosmic star formation rate density is estimated to be ∼ 1 × 10 −3 M ⊙ yr −1 Mpc −3 if they lie somewhere in the redshift range of z ∼ 3-5. This value can be consistent with, or greater than that

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“…The UltraVISTA data considered here correspond to the third data release, 8 which reaches an average depth of =  K 24.9 0.1 s and =  H 25.1 0.1 (2 arcsec diameter, s 5 ). This paper forms part of a series of scientific studies that make use of SMUVS data, such as the search for strong Hα emitters at = -z 4 5 (Caputi et al 2017) and the study of galaxy structural properties for  z 5 (Hill et al 2017). A thorough description of the SMUVS multiwavelength source catalog construction and spectral energy distribution (SED) fitting is given in Deshmukh et al (2018), but we summarize the main details here.…”

Section: Survey Overviewmentioning

confidence: 99%

The Galaxy–Halo Connection for as Revealed by the Spitzer Matching Survey of the UltraVISTA Ultra-deep Stripes

Cowley

Caputi

Deshmukh

et al. 2018

ApJ

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The Spitzer Matching Survey of the UltraVISTA ultra-deep Stripes (SMUVS) provides unparalleled depth at 3.6 and 4.5 µm over ∼ 0.66 deg 2 of the COSMOS field, allowing precise photometric determinations of redshift and stellar mass. From this unique dataset we can connect galaxy samples, selected by stellar mass, to their host dark matter halos for 1.5 < z < 5.0, filling in a large hitherto unexplored region of the parameter space. To interpret the observed galaxy clustering we utilize a phenomenological halo model, combined with a novel method to account for uncertainties arising from the use of photometric redshifts. We find that the satellite fraction decreases with increasing redshift and that the clustering amplitude (e.g., comoving correlation length / large-scale bias) displays monotonic trends with redshift and stellar mass. Applying ΛCDM halo mass accretion histories and cumulative abundance arguments for the evolution of stellar mass content we propose pathways for the coevolution of dark matter and stellar mass assembly. Additionally, we are able to estimate that the halo mass at which the ratio of stellar to halo mass is maximized is 10 12.5 +0.10 −0.08 M at z ∼ 2.5. This peak halo mass is here inferred for the first time from stellar mass-selected clustering measurements at z 2, and implies mild evolution of this quantity for z 3, consistent with constraints from abundance-matching techniques.

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Star Formation in Galaxies at z ∼ 4–5 from the SMUVS Survey: A Clear Starburst/Main-sequence Bimodality for Hα Emitters on the SFR–M* Plane

Cited by 87 publications

References 92 publications

The UV spectral slope β and stellar population of most active star-forming galaxies at z ∼ 4

The UV spectral slope β and stellar population of most active star-forming galaxies at z ∼ 4

ALMA 26 arcmin² Survey of GOODS-S at 1 mm (ASAGAO): Near-infrared-dark Faint ALMA Sources

The Galaxy–Halo Connection for as Revealed by the Spitzer Matching Survey of the UltraVISTA Ultra-deep Stripes

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Star Formation in Galaxies at z ∼ 4–5 from the SMUVS Survey: A Clear Starburst/Main-sequence Bimodality for Hα Emitters on the SFR–M* Plane

Cited by 87 publications

References 92 publications

The UV spectral slope β and stellar population of most active star-forming galaxies at z ∼ 4

The UV spectral slope β and stellar population of most active star-forming galaxies at z ∼ 4

ALMA 26 arcmin2 Survey of GOODS-S at 1 mm (ASAGAO): Near-infrared-dark Faint ALMA Sources

The Galaxy–Halo Connection for as Revealed by the Spitzer Matching Survey of the UltraVISTA Ultra-deep Stripes

Contact Info

Product

Resources

About

ALMA 26 arcmin² Survey of GOODS-S at 1 mm (ASAGAO): Near-infrared-dark Faint ALMA Sources