Massive quiescent galaxies at <i>z</i> &amp;gt; 3 in the Millennium simulation populated by a semi-analytic galaxy formation model

Yu, Rong; Jing, Yingjie; Gao, Liang; Guo, Qi; Wang, Jie; Sun, Shuangpeng; Wang, Lin; Pan, Jun

doi:10.1093/mnrasl/slx099

Cited by 12 publications

(7 citation statements)

References 58 publications

(77 reference statements)

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“…This research has made use of the NASA Astrophysics Data System Bibliographic Services, the NASA Extragalactic Database, PYTHON/EMCEE v.2.2.1 (Foreman-Mackey et al 2013,https:// emcee.readthedocs.io/en/v2.2.1/) package, GALFIT (Peng et al 2002(Peng et al , 2010, and ds9 (a tool for data visualization supported by the Chandra X-ray Science Center and the High Energy Astrophysics Science Archive Center with support from the James Webb Space Telescope Mission office at the Space Telescope Science Institute for 3D visualization). We also acknowledge the related literature of Goodman & Weare (2010), Jones et al (2001), Rong et al (2017bRong et al ( , 2018b, Astropy Collaboration et al (2013), andHunter (2007).…”

Section: Summary and Discussionmentioning

confidence: 96%

Intrinsic Morphology of Ultra-diffuse Galaxies

Dong

Puzia

et al. 2020

ApJ

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With the published data of apparent axis ratios for 1109 ultra-diffuse galaxies (UDGs) located in 17 low-redshift (z ∼ 0.020-0.063) galaxy clusters and 84 UDGs in two intermediate-redshift (z ∼ 0.308-0.348) clusters, we take advantage of a Markov Chain Monte Carlo approach and assume a triaxial model to investigate the intrinsic morphologies of UDGs. In contrast to the conclusion of Burkert, i.e., the underlying shapes of UDGs are purely prolate (C=B<A), we find that the data favor the oblate-triaxial models (i.e., thick disks with <  C B A) over the nearly prolate ones. We also find that the intrinsic morphologies of UDGs are related to their stellar masses/ luminosities, environments, and redshifts. First, the more luminous UDGs have puffier morphologies compared with the less luminous counterparts; the UDG morphologic dependence on luminosity is distinct from that of the typical quiescent dwarf ellipticals (dEs) and dwarf spheroidals (dSphs); in this sense, UDGs may not be simply treated as an extension of the dE/dSph class with similar evolutionary histories; they may differ not only in size. Second, the UDGs with smaller clustercentric distances are more puffed up, compared with the counterparts with larger clustercentric distances; in combination with the UDG thickness dependence on luminosity, the puffier morphologies of UDGs with high luminosities or located in the denser environments are very likely to be attributed to tidal interactions with massive galaxies. Third, we find that the intermediate-redshift UDGs are more flattened, compared with the low-redshift counterparts, which plausibly suggests a "disky" origin for the high-redshift, newly born UDGs.

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Section: Summary and Discussionmentioning

confidence: 96%

Intrinsic Morphology of Ultra-diffuse Galaxies

Dong

Puzia

et al. 2020

ApJ

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“…More recently, Rong et al (2017) used an earlier version of this SAM (Guo et al 2011) to study analogs of ZF-COS-20115, the z = 3.7 quiescent galaxy discussed in G17. While they were indeed able to find quiescent galaxies at these redshifts, their predicted space density was comparably low: 7.5 × 10 −8 Mpc −3 for galaxies with sSFR < sSFR Q and M * > 10 11 M ⊙ , a factor 30 lower than we observe for this same mass threshold (i.e., (2.2 ± 1.1) × 10 −6 Mpc −3 ).…”

Section: Number Densities Predicted By Semi-analytic Modelsmentioning

confidence: 99%

Near infrared spectroscopy and star-formation histories of 3 ≤ z ≤ 4 quiescent galaxies

Schreiber

Glazebrook

Nanayakkara

et al. 2018

A&A

221

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We present Keck-MOSFIRE H and K spectra for a sample of 24 candidate quiescent galaxies at 3 < z < 4, identified from their rest-frame UV J colors and photometric redshifts in the ZFOURGE and 3DHST surveys. With median integration times of one hour in H and five in K, we obtain spectroscopic redshifts for half of the sample, using either Balmer absorption lines or nebular emission lines. We confirm the high accuracy of the photometric redshifts for this spectroscopically-confirmed sample, with a median |z phot − z spec |/(1 + z spec ) of 1.2%. Two galaxies turn out to be dusty Hα emitters at lower redshifts (z < 2.5), and these are the only two detected in the sub-mm with ALMA. High equivalent-width [O iii] emission is observed in two galaxies, contributing up to 30% of the K-band flux and mimicking the UV J colors of an old stellar population. This implies a failure rate of only 20% for the UV J selection at these redshifts. Lastly, Balmer absorption features are identified in four galaxies, among the brightest of the sample, confirming the absence of OB stars. We then modeled the spectra and photometry of all quiescent galaxies with a wide range of star-formation histories. We find specific star-formation rates (sSFR) lower than 0.15 Gyr −1 (a factor of ten below the main sequence) for all but one galaxy, and lower than 0.01 Gyr −1 for half of the sample. These values are consistent with the observed Hβ and [O ii] luminosities, and the ALMA non-detections. The implied formation histories reveal that these galaxies have quenched on average 300 Myr prior to being observed, between z = 3.5 and 5, and that half of their stars were formed by z ∼ 5.5 with a mean SFR ∼ 300 M ⊙ /yr. We finally compared the UV J selection to a selection based instead on the sSFR, as measured from the photometry. We find that galaxies a factor of ten below the main sequence are 40% more numerous than UV J-selected quiescent galaxies, implying that the UV J selection is pure but incomplete. Current models fail at reproducing our observations, and underestimate either the number density of quiescent galaxies by more than an order of magnitude, or the duration of their quiescence by a factor two. Overall, these results confirm the existence of an unexpected population of quiescent galaxies at z > 3, and offer the first insights on their formation histories.

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“…This allowed us to precisely trace back the star-formation history of this galaxy, which we estimated must have stopped at z > 5 and required a large peak SFR ∼ 1000 M /yr. While some models can accommodate quenched galaxies this early in the history of the Universe (e.g., Rong et al 2017;Qin et al 2017), none is able to produce them in numbers large enough to match observations. Despite its apparently quenched star-formation history, faint sub-millimeter emission was detected toward the galaxy ZF-COSMOS-20115 with ALMA (Schreiber et al 2017b), with a spatial offset of 0.4 ± 0.1 .…”

Section: Introductionmentioning

confidence: 99%

Jekyll & Hyde: quiescence and extreme obscuration in a pair of massive galaxies 1.5 Gyr after the Big Bang

Schreiber

Labbé

Glazebrook

et al. 2018

A&A

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We obtained ALMA spectroscopy and deep imaging to investigate the origin of the unexpected sub-millimeter emission toward the most distant quiescent galaxy known to date, ZF-COSMOS-20115 at z = 3.717. We show here that this sub-millimeter emission is produced by another massive (M * ∼ 10 11 M ), compact (r 1/2 = 0.67 ± 0.14 kpc) and extremely obscured galaxy (A V ∼ 3.5), located only 0.43 (3.1 kpc) away from the quiescent galaxy. We dub the quiescent and dusty galaxies Jekyll and Hyde, respectively. No dust emission is detected at the location of the quiescent galaxy, implying SFR < 13 M /yr which is the most stringent upper limit ever obtained for a quiescent galaxy at these redshifts. The two sources are spectroscopically confirmed to lie at the same redshift thanks to the detection of [C ii] 158 in Hyde (z = 3.709), which provides one the few robust redshifts for a highly-obscured "H-dropout" galaxy (H − [4.5] = 5.1 ± 0.8). The [C ii] line shows a clear rotating-disk velocity profile which is blueshifted compared to the Balmer lines of Jekyll by 549 ± 60 km/s, demonstrating that it is produced by another galaxy. Careful de-blending of the Spitzer imaging confirms the existence of this new massive galaxy, and its non-detection in the Hubble images requires extremely red colors and strong attenuation by dust. Full modeling of the UV-to-far-IR emission of both galaxies shows that Jekyll has fully quenched at least 200 Myr prior to observation and still presents a challenge for models, while Hyde only harbors moderate star-formation with SFR 120 M /yr, and is located at least a factor 1.4 below the z ∼ 4 main sequence. Hyde could also have stopped forming stars less than 200 Myr before being observed; this interpretation is also suggested by its compactness comparable to that of z ∼ 4 quiescent galaxies and its low [C ii]/FIR ratio, but significant on-going star-formation cannot be ruled out. Lastly, we find that despite its moderate SFR, Hyde hosts a dense reservoir of gas comparable to that of the most extreme starbursts. This suggests that whatever mechanism has stopped or reduced its star-formation must have done so without expelling the gas outside of the galaxy. Because of their surprisingly similar mass, compactness, environment and star-formation history, we argue that Jekyll and Hyde can be seen as two stages of the same quenching process, and provide a unique laboratory to study this poorly understood phenomenon.

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Massive quiescent galaxies at z > 3 in the Millennium simulation populated by a semi-analytic galaxy formation model

Cited by 12 publications

References 58 publications

Intrinsic Morphology of Ultra-diffuse Galaxies

Intrinsic Morphology of Ultra-diffuse Galaxies

Near infrared spectroscopy and star-formation histories of 3 ≤ z ≤ 4 quiescent galaxies

Jekyll & Hyde: quiescence and extreme obscuration in a pair of massive galaxies 1.5 Gyr after the Big Bang

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Massive quiescent galaxies at z &gt; 3 in the Millennium simulation populated by a semi-analytic galaxy formation model

Cited by 12 publications

References 58 publications

Intrinsic Morphology of Ultra-diffuse Galaxies

Intrinsic Morphology of Ultra-diffuse Galaxies

Near infrared spectroscopy and star-formation histories of 3 ≤ z ≤ 4 quiescent galaxies

Jekyll & Hyde: quiescence and extreme obscuration in a pair of massive galaxies 1.5 Gyr after the Big Bang

Contact Info

Product

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Massive quiescent galaxies at z > 3 in the Millennium simulation populated by a semi-analytic galaxy formation model