A comparison of observed and simulated absorption from H <scp>i</scp>, C <scp>iv</scp>, and Si <scp>iv</scp>around<i>z</i> ≈ 2 star-forming galaxies suggests redshift–space distortions are due to inflows

Turner, Monica L.; Schaye, Joop; Crain, Robert A.; Rudie, Gwen C.; Steidel, Charles C.; Strom, Allison L.; Theuns, Tom

doi:10.1093/mnras/stx1616

Cited by 88 publications

(79 citation statements)

References 61 publications

(88 reference statements)

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“…On ∼ 1 pMpc scale, the clumpy neutral gas inflow onto galaxies causes the squashing of the effective optical depth map along the line-of-sight direction. Such large-scale inflow of the gas on to galaxies has been detected in observations (Rakic et al 2012;Bielby et al 2017) in a consistent matter with cosmological simulations (Turner et al 2017). A higher velocity dispersion introduces a more line-of-sight elongation in the redshift-space anisotropy.…”

Section: D Redshift-space Galaxy-lyα Forest Clustering: the Imprintssupporting

confidence: 78%

A new model framework for circumgalactic Lyα radiative transfer constrained by galaxy-Lyα forest clustering

Kakiichi

Dijkstra

2018

Monthly Notices of the Royal Astronomical Society

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We present a new perturbative approach to "constrained Lyα radiative transfer" (RT) through the circum-and inter-galactic medium (CGM and IGM). We constrain the H I content and kinematics of the CGM and IGM in a physically motivated model, using the galaxy-Lyα forest clustering data from spectroscopic galaxy surveys in QSO fields at z ∼ 2 − 3. This enables us to quantify the impact of the CGM/IGM on Lyα emission in an observationally constrained, realistic cosmological environment. Our model predicts that the CGM and IGM at these redshifts transmit ≈ 80 % of Lyα photons after having escaped from galaxies. This implies that while the inter-stellar medium primarily regulates Lyα escape, the CGM has a non-negligible impact on the observed Lyα line properties and the inferred Lyα escape fraction, even at z ∼ 2 − 3. Lyα scattering in the CGM and IGM further introduces an environmental dependence in the (apparent) Lyα escape fraction, and the observed population of Lyα emitting galaxies: the CGM/IGM more strongly suppresses direct Lyα emission from galaxies in overdense regions in the Universe, and redistributes this emission into brighter Lyα haloes. The resulting mean surface brightness profile of the Lyα haloes is generally found to be a powerlaw ∝ r −2.4 . Although our model still contains arbitrariness, our results demonstrate how (integral field) spectroscopic surveys of galaxies in QSO fields constrain circumgalactic Lyα RT, and we discuss the potential of these models for studying CGM physics and cosmology.

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Section: D Redshift-space Galaxy-lyα Forest Clustering: the Imprintssupporting

confidence: 78%

A new model framework for circumgalactic Lyα radiative transfer constrained by galaxy-Lyα forest clustering

Kakiichi

Dijkstra

2018

Monthly Notices of the Royal Astronomical Society

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“…The EAGLE simulations successfully reproduce a broad range of observed galaxy properties and scalings, such as the evolution of the stellar masses and sizes (Furlong et al 2017) of galaxies, their luminosities and colours (Trayford et al 2015), their cold gas properties (Lagos et al 2015(Lagos et al , 2016Bahé et al 2016;Marasco et al 2016;Crain et al 2017), and the properties of circumgalactic and intergalactic absorption systems (Rahmati et al 2015;Oppenheimer et al 2016;Rahmati et al 2016;Turner et al 2016Turner et al , 2017.…”

Section: The Eagle Simulations Of Galaxy Formationmentioning

confidence: 90%

The E-MOSAICS project: simulating the formation and co-evolution of galaxies and their star cluster populations

Pfeffer

Kruijssen

Crain

et al. 2017

Monthly Notices of the Royal Astronomical Society

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260

472

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We introduce the MOdelling Star cluster population Assembly In Cosmological Simulations within EAGLE (E-MOSAICS) project. E-MOSAICS incorporates models describing the formation, evolution and disruption of star clusters into the EAGLE galaxy formation simulations, enabling the examination of the co-evolution of star clusters and their host galaxies in a fully cosmological context. A fraction of the star formation rate of dense gas is assumed to yield a cluster population; this fraction, and the population's initial properties, are governed by the physical properties of the natal gas. The subsequent evolution and disruption of the entire cluster population is followed accounting for two-body relaxation, stellar evolution, and gravitational shocks induced by the local tidal field. This introductory paper presents a detailed description of the model and initial results from a suite of 10 simulations of ∼ L galaxies with disc-like morphologies at z = 0. The simulations broadly reproduce key observed characteristics of young star clusters and globular clusters (GCs), without invoking separate formation mechanisms for each population. The simulated GCs are the surviving population of massive clusters formed at early epochs (z 1 − 2), when the characteristic pressures and surface densities of star-forming gas were significantly higher than observed in local galaxies. We examine the influence of the star formation and assembly histories of galaxies on their cluster populations, finding that (at similar present-day mass) earlier-forming galaxies foster a more massive and disruption-resilient cluster population, while galaxies with late mergers are capable of forming massive clusters even at late cosmic epochs. We find that the phenomenological treatment of interstellar gas in EAGLE precludes the accurate modelling of cluster disruption in low-density environments, but infer that simulations incorporating an explicitly-modelled cold interstellar gas phase will overcome this shortcoming.

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“…Due to their young ages and high star-formation rates, they exhibit comparatively Fe-poor stellar populations which have a 1-4 Ryd ionizing spectrum that is harder than is typical in the local universe, but likely common at high redshift Strom et al 2017;Steidel et al 2016). Clustering analysis of the parent sample suggests these galaxies occupy dark matter halos with median halo masses M halo = 10 11.9 M ⊙ (Trainor & Steidel 2012;Rakic et al 2013;Turner et al 2017) corresponding to a typical virial radius of ∼ 100 pkpc at these redshifts.…”

Section: Observationsmentioning

confidence: 99%

“…2013; Turner et al 2017), of galaxies in the KBSS sample. All the galaxies included in this analysis have QSO spectroscopy covering at least two Lyman series transitions so that the H I column is well constrained.…”

Section: Observationsmentioning

confidence: 99%

Column Density, Kinematics, and Thermal State of Metal-bearing Gas within the Virial Radius of z ∼ 2 Star-forming Galaxies in the Keck Baryonic Structure Survey

Rudie

Steidel

Pettini

et al. 2019

ApJ

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109

135

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We present results from the Keck Baryonic Structure Survey (KBSS) including the first detailed measurements of the column densities, kinematics, and internal energy of metal-bearing gas within the virial radius (35-100 physical kpc) of eight ∼ L * galaxies at z ∼ 2. From our full sample of 130 metal-bearing absorbers, we infer that halo gas is kinematically complex when viewed in singly, doubly, and triply ionized species. Broad O VI and C IV absorbers are detected at similar velocities to the lower-ionization gas but with very different kinematic structure indicating that the circumgalactic medium (CGM) is multi-phase. There is a high covering fraction of metal-bearing gas within 100 kpc including highly ionized gas such as O VI; however, observations of a single galaxy probed by a lensed background QSO suggest the size of metal-bearing clouds is small (< 400 pc for all but the O VI-bearing gas). The mass in metals found within the halo is substantial, equivalent to 25% of the metal mass within the interstellar medium. The gas kinematics unambiguously show that 70% of galaxies with detected metal absorption have some unbound metal-enriched gas, suggesting galactic winds may commonly eject gas from halos at z ∼ 2. Significant thermal broadening is detected in CGM absorbers which dominates the internal energy of the gas. 40% of the detected gas has temperatures in the range 10 4.5−5.5 K where cooling times are short, suggesting the CGM is dynamic, with constant heating and/or cooling to produce this short-lived thermal phase.

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A comparison of observed and simulated absorption from H i, C iv, and Si ivaroundz ≈ 2 star-forming galaxies suggests redshift–space distortions are due to inflows

Cited by 88 publications

References 61 publications

A new model framework for circumgalactic Lyα radiative transfer constrained by galaxy-Lyα forest clustering

A new model framework for circumgalactic Lyα radiative transfer constrained by galaxy-Lyα forest clustering

The E-MOSAICS project: simulating the formation and co-evolution of galaxies and their star cluster populations

Column Density, Kinematics, and Thermal State of Metal-bearing Gas within the Virial Radius of z ∼ 2 Star-forming Galaxies in the Keck Baryonic Structure Survey

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