Absorption-based circumgalactic medium line emission estimates

Piacitelli, Daniel; Solhaug, Erik; Faerman, Yakov; McQuinn, Matthew

doi:10.1093/mnras/stac2390

Cited by 4 publications

(7 citation statements)

References 65 publications

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“…Katz et al 2019;Mitchell et al 2021;Byrohl et al 2021), and analytical models (e.g. Faerman et al 2020;Piacitelli et al 2022). Recently, Nelson et al (2021) explored the Mg emission from haloes around a statistical sample of thousands of galaxies with stellar mass in the range log(𝑀 * /𝑀 ) = 7.5 − 11.0 over the redshift range 0.3 < 𝑧 < 2, using the TNG50 cosmological magnetohydrodynamical simulation (Nelson et al 2019a,b;Pillepich et al 2019) from the IllustrisTNG project.…”

Section: Comparison With Simulationsmentioning

confidence: 99%

“…The metal-enriched halo gas has been more challenging to detect (Rickards Vaught et al 2019), as expected from theoretical grounds due to their lower SB (Bertone & Schaye 2012;Frank et al 2012;Piacitelli et al 2022). This technique has nevertheless seen many recent successes, such as the detection of extended nebulae in [O ] and [O ] emission around quasars (Johnson et al 2018(Johnson et al , 2022Helton et al 2021), galaxy groups and clusters (Epinat et al 2018;Boselli et al 2019;Chen et al 2019), and ultraluminous galaxies (Rupke et al 2019) at 𝑧 < 1.…”

Section: Introductionmentioning

confidence: 99%

“…To put robust constraints on galaxy formation models (e.g. Corlies & Schiminovich 2016;Nelson et al 2021;Piacitelli et al 2022), it is imperative to spatially resolve and map the metal line emission from gaseous haloes around more normal galaxies, and conduct complete systematic studies in larger samples. While detection of metal-emitting haloes around individual galaxies at 𝑧 1 is still challenging, the average metal emission around a population of galaxies can be studied through stacking the IFU data of a statistical sample of galaxies.…”

Section: Introductionmentioning

confidence: 99%

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Metal line emission from galaxy haloes at z~1

Dutta¹,

Fossati²,

Fumagalli³

et al. 2023

Preprint

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We present a study of the metal-enriched halo gas, traced using Mg and [O ] emission lines, in two large, blind galaxy surveys conducted using Multi Unit Spectroscopic Explorer (MUSE) optical integral field unit observations, namely the MUSE Analysis of Gas around Galaxies (MAGG) and the MUSE Ultra Deep Field (MUDF). By stacking a sample of ≈600 galaxies with stellar masses M * ≈ 10 6−12 M (median M * ≈ 2 × 10 9 M ) at redshifts 𝑧 = 0.7 − 1.5 (median 𝑧 ≈ 1), we characterize for the first time the average metal line emission from a general population of galaxy haloes. The Mg and [O ] line emission extends farther out than the stellar continuum emission around galaxies, on average out to ≈25 kpc and ≈45 kpc, respectively, at a surface brightness (SB) level of 10 −20 erg s −1 cm −2 arcsec −2 . The radial profile of the Mg SB is shallower than that of the [O ], suggesting that the resonant Mg emission is affected by dust and radiative transfer effects. The [O ] to Mg SB ratio is ≈ 3 over ≈ 20 − 40 kpc, also indicating a significant in situ origin of the extended metal emission in the inner halo. The average profiles are intrinsically brighter by a factor ≈ 2 − 3 and more radially extended by a factor of ≈ 1.3 at 1.0 < 𝑧 ≤ 1.5 than at 0.7 ≤ 𝑧 ≤ 1.0. The average extent of the metal emission also increases independently with increasing stellar mass and in overdense group environments. When considering individual detections, we find extended [O ] emission up to ≈ 50 kpc around ≈ 30 − 40 percent of the group galaxies, and extended (≈ 30 − 40 kpc) Mg emission around two 𝑧 ≈ 1 quasars in groups, which could arise from outflows or environmental processes.

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Section: Comparison With Simulationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Metal line emission from galaxy haloes at z~1

Dutta¹,

Fossati²,

Fumagalli³

et al. 2023

Preprint

View full text Add to dashboard Cite

show abstract

“…Recent decades have seen significant progress in observational studies of the cool CGM. At low redshift, this phase is observed mainly in UV absorption, using the Hubble Space Telescope (HST) Cosmic Origins Spectrograph (COS; e.g., Prochaska et al 2011;Stocke et al 2013;Tumlinson et al 2013;Werk et al 2013; and see Piacitelli et al 2022 for emission predictions). Measurements include both hydrogen transitions and metal lines, allowing estimation of the gas metallicity (e.g., Prochaska et al 2017;Chen et al 2018;Wotta et al 2019;Berg et al 2023) and showing that it is significantly metal-enriched.…”

Section: Introductionmentioning

confidence: 99%

The Cool Circumgalactic Medium of Low-redshift Star-forming Galaxies. I. Empirical Model and Mean Properties

Faerman,

Werk

2023

ApJ

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We present an analytic model for the cool, T ∼ 104 K, circumgalactic medium (CGM), describing the gas distribution, and thermal and ionization states. Our model assumes (total) pressure equilibrium with the ambient warm/hot CGM, photoionization by the metagalactic radiation, and allows for nonthermal pressure support, parameterized by the ratio of thermal pressures, η = P hot,th/P cool,th. We apply the model to the COS-Halos measurements and find that a nominal model with η = 3, gas distribution out to r ≈ 0.6R vir, and M cool = 3 × 109 M ⊙, corresponding to a volume filling fraction of f V,cool ≈ 1%, reproduces the H i and low/intermediate metal ions (C ii, C iii, Si ii, Si iii, and Mg ii) mean column densities. Variation of ±0.5 dex in η or M cool encompasses ∼2/3 of the scatter between objects. Our nominal model underproduces the measured C iv and Si iv columns, and these can be reproduced with (i) a cool phase with M cool ∼ 1010 M ⊙ and η ≈ 5, or (ii) cooling or mixing gas at intermediate temperatures, with M ∼ 1.5 × 1010 M ⊙ and occupying ∼1/2 of the total CGM volume. For cool gas with f V,cool ≈ 1%, we estimate an upper limit on the cloud sizes, R cl ≲ 0.5 kpc. Our results suggest that for the average galaxy CGM, the mass and nonthermal support in the cool phase are lower than previously estimated, and extreme scenarios are not necessary. We estimate the rates of cool gas depletion and replenishment, and find accretion onto the galaxy can be offset, allowing M ̇ cool ≈ 0 over long timescales.

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“…The metal-enriched halo gas has been more challenging to detect (Rickards Vaught et al 2019 ), as expected from theoretical grounds due to their lower SB (Bertone & Schaye 2012 ;Frank et al 2012 ;Piacitelli et al 2022 ). This technique has nevertheless seen many recent successes, such as the detection of extended nebulae in [O II ] and [O III ] emission around quasars (Johnson et al 2018(Johnson et al , 2022Helton et al 2021 ), galaxy groups and clusters (Epinat et al 2018 ;Boselli et al 2019 ;Chen et al 2019 ), and ultraluminous galaxies (Rupke et al 2019 ) at z < 1.…”

mentioning

confidence: 99%

Metal line emission from galaxy haloes at z ≈ 1

Dutta

Fossati

Fumagalli

et al. 2023

Monthly Notices of the Royal Astronomical Society

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We present a study of the metal-enriched halo gas, traced using Mg ii and [O ii] emission lines, in two large, blind galaxy surveys – the MUSE (Multi Unit Spectroscopic Explorer) Analysis of Gas around Galaxies (MAGG) and the MUSE Ultra Deep Field (MUDF). By stacking a sample of ≈600 galaxies (stellar masses $\rm M_*$ ≈106 − 12 $\rm M_\odot$), we characterize for the first time the average metal line emission from a general population of galaxy haloes at 0.7 ≤ z ≤ 1.5. The Mg ii and [O ii] line emission extends farther out than the stellar continuum emission, on average out to ≈25 kpc and ≈45 kpc, respectively, at a surface brightness (SB) level of 10−20 $\rm erg\, s^{-1}\, cm^{-2}\, arcsec^{-2}$. The radial profile of the Mg ii SB is shallower than that of the [O ii], suggesting that the resonant Mg ii emission is affected by dust and radiative transfer effects. The [O ii] to Mg ii SB ratio is ≈3 over ≈20 − 40 kpc, also indicating a significant in situ origin of the extended metal emission. The average SB profiles are intrinsically brighter by a factor ≈2 − 3 and more radially extended by a factor of ≈1.3 at 1.0 < z ≤ 1.5 than at 0.7 ≤ z ≤ 1.0. The average extent of the metal emission also increases independently with increasing stellar mass and in overdense group environments. When considering individual detections, we find extended [O ii] emission up to ≈50 kpc around ≈30–40 per cent of the group galaxies, and extended (≈30 − 40 kpc) Mg ii emission around two z ≈ 1 quasars in groups, which could arise from outflows or environmental processes.

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Absorption-based circumgalactic medium line emission estimates

Cited by 4 publications

References 65 publications

Metal line emission from galaxy haloes at z~1

Metal line emission from galaxy haloes at z~1

The Cool Circumgalactic Medium of Low-redshift Star-forming Galaxies. I. Empirical Model and Mean Properties

Metal line emission from galaxy haloes at z ≈ 1

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