Sub-damped Lyman α systems in the XQ-100 survey – II. Chemical evolution at 2.4 ≤ <i>z</i> ≤ 4.3

Berg, Trystyn A. M.; Fumagalli, Michele; D’Odorico, V.; Ellison, Sara L.; López, Sebastián; Becker, George D.; Christensen, L.; Cupani, G.; Denney, K. D.; Sánchez-Ramírez, R.; Worseck, G.

doi:10.1093/mnras/stab184

Cited by 16 publications

(21 citation statements)

References 109 publications

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“…We note that the Magellan DLA survey by Jorgenson et al (2013) has essentially the same metallicity distribution as R12-DLA in our redshift of interest 2.2 z 3.6 (see below). The recent XQ-100 survey of SLLSs by Berg et al (2021) shows also the same metallicity distributions as in HD-LLS.…”

Section: Search For H I Absorbers In the Kodiaq Databasementioning

confidence: 54%

“…In Fig. 26, we show the neutral fraction of the absorbers estimated from the Cloudy models as a function of N H I from log N H I 14.6 to 20 from KODIAQ-Z and HD-LLS (see §5.2, and see also the recent work for the SLLSs from Berg et al 2021). There is a clear correlation between f H I and N H I .…”

Section: Neutral Fractionsmentioning

confidence: 87%

“…Since we do not have SLLSs with log N H I > 20 in our sample, we use the result from the HD-LLS survey where Fumagalli et al (2016b) derived Ω m = 1.6 × 10 −6 for the SLLSs. For reasons (sample variance, using the arithmetic mean) discussed in detail in Fumagalli et al, these values are uncertain by a factor ∼ 3 (see also discussion in Berg et al 2021). We note that the comoving metal-mass density can be estimated via ρ m = Ω m /ρ c (e.g., Péroux & Howk 2020).…”

Section: Cosmological Metal Budgetmentioning

confidence: 94%

“…At high redshift, much of the effort has focused on the metal enrichment of the most diffuse regions probed by the LYAF (e.g., Cowie et al 1995;Songaila 1998;Ellison et al 2000;Schaye et al 2000Schaye et al , 2003Aguirre et al 2004;Simcoe et al 2004;Simcoe 2011) and the densest regions of the universe probed by DLAS (e.g., Pettini et al 1997Pettini et al , 1999Prochaska 1999;Prochaska et al 2003;Rafelski et al 2012;Jorgenson et al 2013). The HD-LLS survey (Prochaska et al 2015;Fumagalli et al 2016b, and see also Berg et al 2021 for the XQ-100 survey of SLLSs) has surveyed lower H I column density absorbers mostly in the range 17.8 log N H I < 20.3. With KODIAQ-Z (this work, and earlier KODIAQ surveys Lehner et al 2014Lehner et al , 2016, we bridge the gap between the DLA/SLLS regimes and the LYAF.…”

Section: Insights From Foggie Simulationsmentioning

confidence: 99%

“…18), and the XQ-100 survey only reports one supersolar SLLS at z ∼ 2.5 (see Fig. 2 in Berg et al 2021; we exclude poorly-constrained upper limits on the metallicity that are above solar in that survey). Adding that supersolar pLLS to the KODIAQ-Z+HD-LLS survey would imply that only 1 out 242 absorbers has a supersolar metallicity at 2.2 z 3.6, i.e., 0.41% +1.42% −0.32% (90% CI) of the absorbers have [X/H] > 0.…”

Section: Extreme Metallicities and Metal-rich Gasmentioning

confidence: 99%

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KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2

Lehner,

Kopenhafer,

O'Meara

et al. 2021

Preprint

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We present the KODIAQ-Z survey aimed to characterize the cool, photoionized gas at 2.2 z 3.6 in 202 H Iselected absorbers with 14.6 ≤ log N H I < 20, i.e., the gaseous interface between galaxies and the intergalactic medium (IGM). We find that the 14.6 ≤ log N H I < 20 gas at 2.2 z 3.6 can be metal-rich gas (−1.6 [X/H] −0.2) as seen in damped Lyα absorbers (DLAs); it can also be very metal-poor ([X/H] < −2.4) or even pristine gas ([X/H] < −3.8) not observed in DLAs, but commonly observed in the IGM. For 16 < log N H I < 20 absorbers, the frequency of pristine absorbers is about 1%-10%, while for 14.6 ≤ log N H I ≤ 16 absorbers it is 10%-20%, similar to the diffuse IGM. Supersolar gas is extremely rare (< 1%) in this gas. The factor of several thousand spread from the lowest to highest metallicities and large metallicity variations (a factor of a few to > 100) between absorbers separated by less than ∆v < 500 km s −1 imply that the metals are poorly mixed in 14.6 ≤ log N H I < 20 gas. We show that these photoionized absorbers contribute to about 10% of the cosmic baryons and 30% of the cosmic metals at 2.2 z 3.6. We find the mean metallicity increases with N H I , consistent with what is found in z < 1 gas. The metallicity of gas in this column density regime has increased by a factor ∼8 from 2.2 z 3.6 to z < 1, but the contribution of the 14.6 ≤ log N H I < 19 absorbers to the total metal budget of the universe at z < 1 is half that at 2.2 z 3.6, indicating a substantial shift in the reservoirs of metals between these two epochs. We compare the KODIAQ-Z results to FOGGIE cosmological zoom simulations. The simulations show an evolution of [X/H] with N H I similar to our observational results. Very metal-poor absorbers with [X/H] < −2.4 at z ∼ 2-3 in these simulations are excellent tracers of inflows, while higher metallicity absorbers are a mixture of inflows and outflows.

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Section: Search For H I Absorbers In the Kodiaq Databasementioning

confidence: 54%

Section: Neutral Fractionsmentioning

confidence: 87%

Section: Cosmological Metal Budgetmentioning

confidence: 94%

Section: Insights From Foggie Simulationsmentioning

confidence: 99%

Section: Extreme Metallicities and Metal-rich Gasmentioning

confidence: 99%

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KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2

Lehner,

Kopenhafer,

O'Meara

et al. 2021

Preprint

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Cosmic metal density evolution in neutral gas: insights from observations and cosmological simulations

Yates

Péroux

Nelson

2021

Monthly Notices of the Royal Astronomical Society

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We contrast the latest observations of the cosmic metal density in neutral gas ($\rho _{\rm {met,neu}}$) with three cosmological galaxy evolution simulations: L-Galaxies 2020, TNG100, and EAGLE. We find that the fraction of total metals that are in neutral gas is <40 per cent at 3 ≲ z ≲ 5 in these simulations, whereas observations of damped Lyman-α (DLA) systems suggest ≳ 85 per cent. In all three simulations, hot, low-density gas is also a major contributor to the cosmic metal budget, even at high redshift. By considering the evolution in cosmic SFR density ($\rho _{\rm {\small {SFR}}}$), neutral gas density ($\rho _{\rm {HI}}$), and mean gas-phase metallicity ($[\langle {}\rm {M/H}\rangle ]_{\rm {neu}}$), we determine two possible ways in which the absolute $\rho _{\rm {met,neu}}$ observed in DLAs at high redshift can be matched by simulations: (a) the $\rho _{\rm {\small {SFR}}}$ at z ≳ 3 is greater than inferred from current FUV observations, or (b) current high-redshift DLA metallicity samples have a higher mean host mass than the overall galaxy population. If the first is correct, TNG100 would match the ensemble data best, however there would be an outstanding tension between the currently observed $\rho _{\rm {\small {SFR}}}$ and $\rho _{\rm {met,neu}}$. If the second is correct, L-Galaxies 2020 would match the ensemble data best, but would require an increase in neutral gas mass inside subhaloes above z ∼ 2.5. If neither is correct, EAGLE would match the ensemble data best, although at the expense of over-estimating $[\langle {}\rm {M/H}\rangle ]_{\rm {neu}}$. Modulo details related to numerical resolution and Hi mass modelling in simulations, these incompatibilities highlight current tensions between key observed cosmic properties at high redshift.

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MUSE Analysis of Gas around Galaxies (MAGG) – IV. The gaseous environment of z ∼ 3–4 Ly α emitting galaxies

Lofthouse

Fumagalli

Fossati

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We study the link between galaxies and H i-selected absorption systems at z ∼ 3 − 4 in the MUSE Analysis of Gas around Galaxies (MAGG) survey, an ESO large programme consisting of integral field spectroscopic observations of 28 quasar fields hosting 61 strong absorbers with $\rm N_{\rm HI}\gtrsim 10^{16.5}~\rm cm^{-2}$. We identify 127 Lyα emitting galaxies (LAEs) around the absorbers, corresponding to a detection rate of 82±16 per cent. The luminosity function of these LAEs is ≈5 times higher in normalization than the field population and we detect a significant clustering of galaxies with respect to the gas, confirming that high column density absorbers and LAEs trace each other. Between 30 and 40 per cent of the absorbers are associated with multiple LAEs, which lie preferentially along filaments. Galaxies in groups also exhibit a three times higher covering factor of optically-thick gas compared to isolated systems. No significant correlations are identified between the emission properties of LAEs and the absorption properties of optically-thick gas clouds, except for a weak preference of brighter and multiple galaxies to reside near broad absorbers. Based on the measured impact parameters and the covering factor, we conclude that the near totality of optically-thick gas in the Universe can be found in the outer circumgalactic medium (CGM) of LAEs or in the intergalactic medium (IGM) in proximity to these galaxies. Thus, LAEs act as tracers of larger scale structures within which both galaxies and optically-thick clouds are embedded. The patchy and inhomogeneous nature of the CGM and IGM explains the lack of correlations between absorption and emission properties. This implies that very large samples are needed to unveil the trends that encode the properties of the baryon cycle.

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Sub-damped Lyman α systems in the XQ-100 survey – II. Chemical evolution at 2.4 ≤ z ≤ 4.3

Cited by 16 publications

References 109 publications

KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2

KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2

Cosmic metal density evolution in neutral gas: insights from observations and cosmological simulations

MUSE Analysis of Gas around Galaxies (MAGG) – IV. The gaseous environment of z ∼ 3–4 Ly α emitting galaxies

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