The First Quenched Galaxies: When and How?

Xie 谢, Lizhi 利智; De Lucia, Gabriella; Fontanot, Fabio; Hirschmann, Michaela; Bahé, Yannick M.; Balogh, Michael L.; Muzzin, Adam; Vulcani, Benedetta; Baxter, Devontae C.; Forrest, Ben; Wilson, Gillian; Rudnick, Gregory H.; Cooper, M. C.; Rescigno, Umberto

doi:10.3847/2041-8213/ad380a

Cited by 8 publications

(3 citation statements)

References 59 publications

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“…However, we note that the SPHINX 20 simulation does not include black hole formation or AGN feedback due to its small volume (Katz et al 2023). AGN may be important in the quenching of high-redshift galaxies at a similar mass range as JADES-GS-z7-01-QU, as shown both theoretically and observationally by recent studies (Juodžbalis et al 2023;Xie et al 2024).…”

Section: Discussionmentioning

confidence: 88%

“…It is suggested that star formation can be quenched for good in lowmass dark matter halos during the epoch of reionization, giving rise to quiescent dwarf galaxies in the present day (e.g., Bullock et al 2000;Brown et al 2014). However, realistically, the SFH of galaxies at these masses is much more complex, and a purely passive evolution after a burst is unlikely given the large gas abundances at those early times (however, see Xie et al 2024 for theoretical evidence that most early quiescent galaxies stay quiescent for ∼1 Gyr). Dark-matter-halo-related quenching is not effective at low masses.…”

Section: Single Starburstmentioning

confidence: 99%

“…Since the galaxy is at a relatively low stellar mass (∼5 × 10 8 M e ), the most likely scenarios involve temporal quenching by star formation or AGN feedback (e.g., Gelli et al 2023;Lovell et al 2023) or galaxy-galaxy interactions (Asada et al 2023). A recent study found that the most dominant quenching mechanisms for low-mass high-redshift galaxies may be accretion disk feedback triggered by disk instabilities (Xie et al 2024). Alternatively, an unlucky geometric distribution of dust along the line of sight could attenuate the nebular emission and mimic quiescence.…”

Section: Introductionmentioning

confidence: 99%

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Dead or Alive? How Bursty Star Formation and Patchy Dust Can Cause Temporary Quiescence in High-redshift Galaxies

Faisst,

Morishita

2024

ApJ

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The recent discovery of a galaxy at z = 7.3 with undetected optical emission lines and a blue UV-to-optical continuum ratio in JWST spectroscopy is surprising and needs to be explained physically. Here, we explore two possibilities that could cause such a seemingly quiescent ∼5 × 108 M ⊙ galaxy in the early Universe: (i) stochastic variations in the star formation history (SFH) and (ii) the effect of spatially varying dust attenuation on the measured line and continuum emission properties. Both scenarios can play out at the same time to amplify the effect. A stochastic star formation model (similar to realistic SFHs from hydrodynamical simulations of similar-mass galaxies) can create such observed properties if star formation is fast-varying with a correlation time of <150 Myr given a reasonable burst amplitude of ∼0.6 dex. The total time spent in this state is less than 20 Myr, and the likelihood of such a state to occur over 500 Myr at z = 7 is ∼50% (consistent with current observations). On the other hand, we show that a spectrum with blue UV continuum and lack of emission lines can be reproduced by a blue+red composite spectrum. The UV continuum is emitted from dust-free density-bounded H ii regions (blue component), while the red component is a dust-obscured starburst with weakened emission lines due to strong differential dust attenuation between stellar and nebular emission. Future resolving far-infrared observations with the Atacama Large Millimeter/submillimeter Array will shed light on the latter scenario.

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Section: Discussionmentioning

confidence: 88%

Section: Single Starburstmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Dead or Alive? How Bursty Star Formation and Patchy Dust Can Cause Temporary Quiescence in High-redshift Galaxies

Faisst,

Morishita

2024

ApJ

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Tracing the quenching journey across cosmic time

De Lucia,

Fontanot,

Xie

et al. 2024

A&A

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We present the latest version of the GAlaxy Evolution and Assembly (GAEA) theoretical model of galaxy formation. Our new model now combines (i) an updated treatment of feedback from Active Galactic Nuclei (AGN), including an improved modelling of cold gas accretion on super-massive black holes and an explicit implementation of quasar winds; and (ii) a treatment for both cold and hot gas stripping from satellite galaxies. We show that our latest model version predicts specific star formation rate distributions that are in remarkable agreement with observational measurements in the local Universe. Our updated model predicts quenched fractions that are in very nice agreement with observational measurements up to $z 3-4$, and a turn-over of the number densities of quenched galaxies at low stellar masses that is in qualitative agreement with current observational estimates. We show that the main reasons for the improved behaviour with respect to previous renditions of our model are the updated treatment for satellites at low galaxy masses M sun $) and the inclusion of quasar winds at intermediate to large stellar masses ($>10^ M sun $). However, we show that the better treatment of the star formation threshold, due to our explicit partitioning of the cold gas in its atomic and molecular components, also plays an important role in suppressing excessive residual star formation in massive galaxies. While our analysis is based on a selection of quiescent galaxies that takes advantage of the information about their star formation rate, we demonstrate that the impact of a different (colour-colour) selection is not significant up to $z 3$, at least for galaxies above the completeness limits of current surveys. Our new model predicts number densities of massive quiescent galaxies at z > 3 that are the largest among recently published state-of-the-art models. Yet, our model predictions still appear to be below post-JWST observational measurements. We show that the expected cosmic variance is large, and can easily accommodate some of the most recent measurements.

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MAMBO: An empirical galaxy and AGN mock catalogue for the exploitation of future surveys

López-López,

Bolzonella,

Pozzetti

et al. 2024

A&A

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Current and future large surveys will produce unprecedented amounts of data. Realistic simulations have become essential for the design and development of these surveys, as well as for the interpretation of the results. We present MAMBO, a flexible and efficient workflow to build empirical galaxy and active galactic nucleus (AGN) mock catalogues that reproduce the physical and observational properties of these sources. We started with simulated dark matter (DM) haloes, to preserve the link with the cosmic web, and we populated them with galaxies and AGN using abundance matching techniques. We followed an empirical methodology, using stellar mass functions, host galaxy AGN mass functions, and AGN accretion rate distribution functions studied at different redshifts to assign, among other properties, stellar masses, the fraction of quenched galaxies, or the AGN activity (demography, obscuration, multiwavelength emission, etc.). As a proof test, we applied the method to a Millennium DM lightcone of 3.14 $ deg^2$ up to a redshift of $z=10$ and down to stellar masses of $ M \, M_ We show that the AGN population from the mock lightcone presented here reproduces with good accuracy various observables, such as state-of-the-art luminosity functions in the X-ray up to $z 7$ and in the ultraviolet up to $z 5$, optical/near-infrared colour-colour diagrams, and narrow emission line diagnostic diagrams. Finally, we demonstrate how this catalogue can be used to make useful predictions for large surveys. Using Euclid as a case example, we compute, among other forecasts, the expected surface densities of galaxies and AGN detectable in the Euclid $H_ E $ band. We find that Euclid might observe (on $H_ E $ only) about $10^ $ and $8 $ type 1 and 2 AGN, respectively, and $2 $ galaxies at the end of its $ deg^2$ Wide survey, in good agreement with other published forecasts.

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The First Quenched Galaxies: When and How?

Cited by 8 publications

References 59 publications

Dead or Alive? How Bursty Star Formation and Patchy Dust Can Cause Temporary Quiescence in High-redshift Galaxies

Dead or Alive? How Bursty Star Formation and Patchy Dust Can Cause Temporary Quiescence in High-redshift Galaxies

Tracing the quenching journey across cosmic time

MAMBO: An empirical galaxy and AGN mock catalogue for the exploitation of future surveys

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