The Cosmic Baryon and Metal Cycles

Péroux, Céline; Howk, J. C.

doi:10.1146/annurev-astro-021820-120014

Cited by 242 publications

(221 citation statements)

References 236 publications

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“…Dust is not yet commonly modelled in cosmological simulations, and is not included in either EAGLE or TNG50. However, dust grains are thought to play a central role in catalyzing the formation of the molecules essential to star formation and hence metal production, and there is a tight relation between metallicity and dust content, as seen in the evolution of the dust-togas ratio with metallicity (Jenkins 2009;De Cia et al 2016;Péroux & Howk 2020). Hence, we expect the metallicity trend reported here to also appear versus dust or molecular content (see e.g.…”

Section: Discussion : I M P L I C At I O N S F O R O B S E Rsupporting

confidence: 51%

“…Overall, the normalization of the metallicity values are characteristically higher than most of the simulation correlations explored in Section 3.2.2. The lack of low metallicity measurements in the data does not reflect a detection limit of the observations, which are typically sensitive to metallicity down to log (Z/Z ) = −2.5 at z < 1.5 and as low as log (Z/Z ) = −3.5 at higher redshifts (Péroux & Howk 2020). The high metallicities found by the observations are in part related to the low impact parameters probed in the range b = 6 pkpc to b = 52 pkpc.…”

Section: Discussion : I M P L I C At I O N S F O R O B S E Rmentioning

confidence: 74%

“…In contrast, the CGM is commonly detected in absorption against bright background sources (Bouché et al 2007a). This offers a compelling method to study the distribution, chemical properties, and kinematics of the CGM down to relatively low gas densities (Péroux & Howk 2020). While individual absorption measurements have been limited to a pencil-beam along the line of sight, large statistical samples can constrain the mean properties of the CGM around galaxies, showing for example that cool gas is omnipresent around galaxies (Adelberger et al 2003;Prochaska, Hennawi & Simcoe 2013;Zhu et al 2014).…”

mentioning

confidence: 99%

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Predictions for the angular dependence of gas mass flow rate and metallicity in the circumgalactic medium

Péroux

Nelson

Voort

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We use cosmological hydrodynamical simulations to examine the physical properties of the gas in the circumgalactic media (CGM) of star-forming galaxies as a function of angular orientation. We utilise TNG50 of the IllustrisTNG project, as well as the EAGLE simulation to show that observable properties of CGM gas correlate with azimuthal angle, defined as the galiocentric angle with respect to the central galaxy. Both simulations are in remarkable agreement in predicting a strong modulation of flow rate direction with azimuthal angle: inflow is more substantial along the galaxy major axis, while outflow is strongest along the minor axis. The absolute rates are noticeably larger for higher ($\log {(M_\star / \rm {M}_\odot )} \sim 10.5$) stellar mass galaxies, up to an order of magnitude compared to $\dot{M} \lesssim 1$ M⊙ yr−1 sr−1 for $\log {(M_\star / \rm {M}_\odot )}\sim 9.5$ objects. Notwithstanding the different numerical and physical models, both TNG50 and EAGLE predict that the average metallicity of the CGM is higher along the minor versus major axes of galaxies. The angular signal is robust across a wide range of galaxy stellar mass $8.5 < \log {(M_\star / \rm {M}_\odot )} < 10.5$ at z < 1. This azimuthal dependence is particularly clear at larger impact parameters b ≥ 100 kpc. Our results present a global picture whereby, despite the numerous mixing processes, there is a clear angular dependence of the CGM metallicity. We make forecasts for future large survey programs that will be able to compare against these expectations. Indeed, characterising the kinematics, spatial distribution and metal content of CGM gas is key to a full understanding of the exchange of mass, metals, and energy between galaxies and their surrounding environments.

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Section: Discussion : I M P L I C At I O N S F O R O B S E Rsupporting

confidence: 51%

Section: Discussion : I M P L I C At I O N S F O R O B S E Rmentioning

confidence: 74%

mentioning

confidence: 99%

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Predictions for the angular dependence of gas mass flow rate and metallicity in the circumgalactic medium

Péroux

Nelson

Voort

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…A possible concern is that the local galaxy Hi measurements measure the gas within galaxies, while the absorption line measurements at higher redshifts probe gas in the galaxies, as well as in the CGM. We refer the reader to the article by Péroux & Howk (2020) in this volume for more details.…”

Section: Mass-integrated Evolutionmentioning

confidence: 99%

The Evolution of the Star-Forming Interstellar Medium Across Cosmic Time

Tacconi

Genzel

Sternberg

2020

Annu. Rev. Astron. Astrophys.

331

327

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Over the past decade, increasingly robust estimates of the dense molecular gas content in galaxy populations between redshift z = 0 and the peak of cosmic galaxy/star formation ( z ∼ 1–3) have become available. This rapid progress has been possible due to the advent of powerful ground- and space-based telescopes for the combined study of several millimeter to far-IR, line or continuum tracers of the molecular gas and dust components. The main conclusions of this review are as follows: ▪ Star-forming galaxies contained much more molecular gas at earlier cosmic epochs than at the present time. ▪ The galaxy-integrated depletion timescale for converting the gas into stars depends primarily on z or Hubble time and, at a given z, on the vertical location of a galaxy along the star-formation rate versus stellar mass main sequence (MS) correlation. ▪ Global rates of galaxy gas accretion primarily control the evolution of the cold molecular gas content and star-formation rates of the dominant MS galaxy population, which in turn vary with cosmological expansion. Another key driver may be global disk fragmentation in high- z, gas-rich galaxies, which ties local free-fall timescales to galactic orbital times and leads to rapid radial matter transport and bulge growth. The low star-formation efficiency inside molecular clouds is plausibly set by supersonic streaming motions and internal turbulence, which in turn may be driven by conversion of gravitational energy at high z and/or by local feedback from massive stars at low z. ▪ A simple gas regulator model is remarkably successful in predicting the combined evolution of molecular gas fractions, star-formation rates, galactic winds, and gas-phase metallicities. Expected final online publication date for the Annual Review of Astronomy, Volume 58 is August 18, 2020. Please see http://www.annualreviews.org/page/journal/pubdates for revised estimates.

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“…The outflowing and accreting gas interacts around galaxies on scales up to hundreds of kpc (the Circumgalactic Medium, CGM). Studying the CGM is fundamental to understand the cosmic baryon cycle [106,122,132,140] and it will provide key constraints on the question of galaxy formation and evolution. Absorption spectroscopy has already provided insights on the distribution and the chemical composition of the CGM gas from a statistical point of view, given that typically only one line of sight per galaxy can be studied due to the scarcity of background quasars in the vicinity of galaxies [7, 60,77,100,107,109,111].…”

Section: Probing the Emission Of The Circumgalactic Medium Around Galaxiesmentioning

confidence: 99%

Unveiling the faint ultraviolet Universe

et al. 2021

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With this paper we participate to the call for ideas issued by the European Space Agency to define the Science Program and plan for space missions from 2035 to 2050. In particular we present five science cases where major advancements can be achieved thanks to space-based spectroscopic observations at ultraviolet (UV) wavelengths. We discuss the possibility to (1) unveil the large-scale structures and cosmic web in emission at redshift $\lesssim 1.7$ ≲ 1.7 ; (2) study the exchange of baryons between galaxies and their surroundings to understand the contribution of the circumgalactic gas to the evolution and angular-momentum build-up of galaxies; (3) constrain the efficiency of ram-pressure stripping in removing gas from galaxies and its role in quenching star formation; (4) characterize the progenitor population of core-collapse supernovae to reveal the explosion mechanisms of stars; (5) target accreting white dwarfs in globular clusters to determine their evolution and fate. These science themes can be addressed thanks to UV (wavelength range $\lambda \sim 90 - 350$ λ ∼ 90 − 350 nm) observations carried out with a panoramic integral field spectrograph (field of view $\sim \!1 \times 1$ ∼ 1 × 1 arcmin2), and medium spectral (R = 4000) and spatial ($\sim \!1^{\prime \prime } - 3^{\prime \prime }$ ∼ 1 ′ ′ − 3 ′ ′ ) resolution. Such a UV-optimized instrument will be unique in the coming years, when most of the new large facilities such as the Extremely Large Telescope and the James Webb Space Telescope are optimized for infrared wavelengths.

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The Cosmic Baryon and Metal Cycles

Cited by 242 publications

References 236 publications

Predictions for the angular dependence of gas mass flow rate and metallicity in the circumgalactic medium

Predictions for the angular dependence of gas mass flow rate and metallicity in the circumgalactic medium

The Evolution of the Star-Forming Interstellar Medium Across Cosmic Time

Unveiling the faint ultraviolet Universe

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