A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at <i>z</i> ∼ 1.7

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dc.contributor.authorShaban, Ahmed
dc.contributor.authorBordoloi, Rongmon
dc.contributor.authorChisholm, John
dc.contributor.authorSharma, Soniya
dc.contributor.authorSharon, Keren
dc.contributor.authorRigby, Jane R.
dc.contributor.authorGladders, Michael G.
dc.contributor.authorBayliss, Matthew B.
dc.contributor.authorBarrientos, L. Felipe
dc.contributor.authorLopez, Sebastian
dc.contributor.authorTejos, Nicolas
dc.contributor.authorLedoux, Cedric
dc.contributor.authorFlorian, Michael K.
dc.date.accessioned2025-01-20T21:02:53Z
dc.date.available2025-01-20T21:02:53Z
dc.date.issued2022
dc.description.abstractWe image the spatial extent of a cool galactic outflow with fine-structure Fe ii* emission and resonant Mg ii emission in a gravitationally lensed star-forming galaxy at z = 1.70347. The Fe ii* and Mg ii (continuum-subtracted) emissions span out to radial distances of similar to 14.33 and 26.5 kpc, respectively, with maximum spatial extents of similar to 21 kpc for Fe ii* emission and similar to 30 kpc for Mg ii emission. Mg ii emission is patchy and covers a total area of similar to 184 kpc(2), constraining the minimum area covered by the outflowing gas to be similar to 13% of the total area. Mg ii emission is asymmetric and shows similar to 21% more extended emission along the decl. direction. We constrain the covering fractions of the Fe ii* and Mg ii emission as a function of radial distance and characterize them with a power-law model. The Mg ii 2803 emission line shows two kinematically distinct emission components and may correspond to two distinct shells of outflowing gas with a velocity separation of Delta v similar to 400 km s(-1). By using multiple images with different magnifications of the galaxy in the image plane, we trace the Fe ii* and Mg ii emissions around three individual star-forming regions. In all cases, both the Fe ii* and Mg ii emissions are more spatially extended compared to the star-forming regions traced by the [O ii] emission. These findings provide robust constraints on the spatial extent of the outflowing gas and, combined with outflow velocity and column density measurements, will give stringent constraints on mass-outflow rates of the galaxy.
dc.fuente.origenWOS
dc.identifier.doi10.3847/1538-4357/ac7c65
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://doi.org/10.3847/1538-4357/ac7c65
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/93096
dc.identifier.wosidWOS:000848500500001
dc.issue.numero1
dc.language.isoen
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.titleA 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at <i>z</i> ∼ 1.7
dc.typeartículo
dc.volumen936
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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