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dc.contributor.authorVasan, G., C, K.
dc.contributor.authorJones, T.
dc.contributor.authorSanders, R.L.
dc.contributor.authorEllis, R.S.
dc.contributor.authorStark, D.P.
dc.contributor.authorKacprzak, G.G.
dc.contributor.authorBarone, T.M.
dc.contributor.authorTran, K.H.
dc.contributor.authorGlazebrook, K.
dc.contributor.authorJacobs, C.
dc.date.accessioned2024-03-26T06:52:13Z
dc.date.available2024-03-26T06:52:13Z
dc.date.issued2023-12-13
dc.identifier.citationKeerthi Vasan G. C. et al 2023 ApJ 959 124
dc.identifier.issn0004-637X
dc.identifier.doi10.3847/1538-4357/acf462
dc.identifier.urihttp://hdl.handle.net/10150/671897
dc.description.abstractWe study the kinematics of the interstellar medium (ISM) viewed “down the barrel” in 20 gravitationally lensed galaxies during cosmic noon (z = 1.5-3.5). We use moderate-resolution spectra (R ∼ 4000) from Keck’s Echellette Spectrograph and Imager and Magellan/MagE to spectrally resolve the ISM absorption in these galaxies into ∼10 independent elements and use double Gaussian fits to quantify the velocity structure of the gas. We find that the bulk motion of gas in this galaxy sample is outflowing, with average velocity centroid v cent = − 141 km s−1 (±111 km s−1 scatter) measured with respect to the systemic redshift. A total of 16 out of the 20 galaxies exhibit a clear positive skewness, with a blueshifted tail extending to ∼ −500 km s−1. We examine scaling relations in outflow velocities with galaxy stellar mass and star formation rate, finding correlations consistent with a momentum-driven wind scenario. Our measured outflow velocities are also comparable to those reported for FIRE-2 and TNG50 cosmological simulations at similar redshift and galaxy properties. We also consider implications for interpreting results from lower-resolution spectra. We demonstrate that while velocity centroids are accurately recovered, the skewness, velocity width, and probes of high-velocity gas (e.g., v 95) are subject to large scatter and biases at lower resolution. We find that R ≳ 1700 is required for accurate results for the gas kinematics of our sample. This work represents the largest available sample of well-resolved outflow velocity structure at z > 2 and highlights the need for good spectral resolution to recover accurate properties. © 2023. The Author(s). Published by the American Astronomical Society.
dc.language.isoen
dc.publisherInstitute of Physics
dc.rights© 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.
dc.rights.urihttps://creativecommons.org/licenses/by/4.0
dc.titleResolved Velocity Profiles of Galactic Winds at Cosmic Noon
dc.typeArticle
dc.typetext
dc.contributor.departmentSteward Observatory, University of Arizona
dc.identifier.journalAstrophysical Journal
dc.description.noteOpen access journal
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.
dc.eprint.versionFinal Published Version
dc.source.journaltitleAstrophysical Journal
refterms.dateFOA2024-03-26T06:52:13Z


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© 2023. The Author(s). Published by the American Astronomical Society.  Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.
Except where otherwise noted, this item's license is described as © 2023. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence.