Transverse clues on the kiloparsec-scale structure of the circumgalactic medium as traced by C IV absorption

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dc.article.numberA356
dc.catalogadorgjm
dc.contributor.authorLópez, Sebastián
dc.contributor.authorAfruni, A.
dc.contributor.authorZamora Hidalgo, Diego Amaro
dc.contributor.authorTejos, Nicolás
dc.contributor.authorLedoux, Cédric
dc.contributor.authorHernández Guajardo, Joaquín Alexis
dc.contributor.authorBerg, Trystyn A. M.
dc.contributor.authorCortés Muñoz, Hugo R.
dc.contributor.authorUrbina Jiménez, Francisco
dc.contributor.authorJohnston, E. J.
dc.contributor.authorBarrientos, Luis Felipe
dc.contributor.authorBayliss, M. B.
dc.contributor.authorCuellar, Rodrigo
dc.contributor.authorKrogager, Jens-Kristian
dc.contributor.authorNoterdaeme, Pasquier
dc.contributor.authorSolimano, Manuel
dc.date.accessioned2025-03-07T13:41:42Z
dc.date.available2025-03-07T13:41:42Z
dc.date.issued2024
dc.description.abstractThe kiloparsec-scale kinematics and density structure of the circumgalactic medium (CGM) is still poorly constrained observationally, which poses a problem for understanding the role of the baryon cycle in galaxy evolution. Here we present VLT/MUSE integral-field spectroscopy (R ≈ 1800) of four giant gravitational arcs exhibiting W0 ≳ 0.2 Å C IV absorption at eight intervening redshifts, zabs ≈ 2.0–2.5. We detected C IV absorption in a total of 222 adjacent and seeing-uncorrelated sight lines whose spectra sample beams of ("de-lensed") linear size ≈1 kpc. Our data show that (1) absorption velocities cluster at all probed transverse scales, Δr⊥ ≈ 0–15 kpc, depending on system; (2) the (transverse) velocity dispersion never exceeds the mean (line-of-sight) absorption spread; and (3) the (transverse) velocity autocorrelation function does not resolve kinematic patterns at the above spatial scales, but its velocity projection, ξarc(Δv), exhibits a similar shape to the known two-point correlation function toward quasars, ξQSO(Δv). An empirical kinematic model suggests that these results are a natural consequence of wide-beam observations of an unresolved clumpy medium. Our model recovers both the underlying velocity dispersion of the clumps (70–170 km s‑1) and the mean number of clumps per unit area (2–13 kpc‑2). The latter constrains the projected mean inter-clump distance to within ≈0.3–0.8 kpc, which we argue is a measure of clump size for a near-unity covering fraction. The model is also able to predict ξarc(Δv) from ξQSO(Δv), suggesting that the strong systems that shape ξarc(Δv) and the line-of-sight velocity components that define ξQSO(Δv) trace the same kinematic population. Consequently, the clumps must possess an internal density structure that generates both weak and strong components. We discuss how our interpretation is consistent with previous observations using background galaxies and multiple quasars as well as its implications for the connection between the small-scale kinematic structure of the CGM and galactic-scale accretion and feedback processes....
dc.fechaingreso.objetodigital2025-03-07
dc.format.extent17 páginas
dc.fuente.origenORCID
dc.identifier.doi10.1051/0004-6361/202451200
dc.identifier.urihttps://doi.org/10.1051/0004-6361/202451200
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/102427
dc.information.autorucInstituto de Astrofísica; Zamora Hidalgo, Diego Amaro; S/I; 1039073
dc.information.autorucInstituto de Astrofísica; Hernández Guajardo, Joaquín Alexis; S/I; 1064498
dc.information.autorucInstituto de Astrofísica; Barrientos, Luis Felipe; 0000-0003-0151-0718; 102167
dc.language.isoen
dc.nota.accesocontenido completo
dc.revistaAstronomy & Astrophysics
dc.rightsacceso abierto
dc.rights.licenseCC BY 4.0 Attribution 4.0 International
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.subjectgalaxies: evolution
dc.subjectgalaxies: halos
dc.subjectgalaxies: high-redshift
dc.subjectintergalactic medium
dc.subjectquasars: absorption lines
dc.subject.ddc520
dc.subject.deweyAstronomíaes_ES
dc.titleTransverse clues on the kiloparsec-scale structure of the circumgalactic medium as traced by C IV absorption
dc.typeartículo
dc.volumen691
sipa.codpersvinculados1039073
sipa.codpersvinculados1064498
sipa.codpersvinculados102167
sipa.trazabilidadORCID;2025-03-03
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