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The Keck Baryonic Structure Survey: Using foreground/background galaxy pairs to trace the structure and kinematics of circumgalactic neutral hydrogen at z ∼ 2

Chen, Yuguang and Steidel, Charles C. and Hummels, Cameron B. and Rudie, Gwen C. and Dong, Bili and Trainor, Ryan F. and Bogosavljević, Milan and Erb, Dawn K. and Pettini, Max and Reddy, Naveen A. and Shapley, Alice E. and Strom, Allison L. and Theios, Rachel L. and Faucher-Giguère, Claude-André and Hopkins, Philip F. and Kereš, Dušan (2020) The Keck Baryonic Structure Survey: Using foreground/background galaxy pairs to trace the structure and kinematics of circumgalactic neutral hydrogen at z ∼ 2. . (Unpublished) https://resolver.caltech.edu/CaltechAUTHORS:20200626-150116926

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Abstract

We present new measurements of the spatial distribution and kinematics of neutral hydrogen in the circumgalactic and intergalactic medium surrounding star-forming galaxies at z ~ 2. Using the spectra of ~ 3000 galaxies with redshifts <z> ± 0.4 from the Keck Baryonic Structure Survey (KBSS), we assemble a sample of more than 200,000 distinct foreground-background pairs with projected angular separations of 3 - 500 arcsec and spectroscopic redshifts, with <z_(fg)> = 2.23 and <z_(bg)> = 2.57. The ensemble of sightlines and foreground galaxies is used to construct a 2D map of the mean excess Lyα optical depth relative to the intergalactic mean as a function of projected galactocentric distance (20 < D_(tran)/pkpc ≾ 4000) and line-of-sight velocity. We provide information on the line-of-sight kinematics of H I gas as a function of projected distance D_(tran). We compare the map with cosmological zoom-in simulation, finding qualitative agreement between them. A simple two-component (accretion, outflow) analytical model generally reproduces the observed line-of-sight kinematics and projected spatial distribution of H I. The best-fitting model suggests that galaxy-scale outflows with initial velocity v_(out) ≃ 600 km s⁻¹ dominate the kinematics of circumgalactic H I out to Dtran ~ 50 kpc, while H I at D_(tran) ≳ 100 kpc is dominated by infall with characteristic v_(in) ≾ v_c, where v_c is the circular velocity of the host halo (M_h ~ 10¹² M_⊙). Over the impact parameter range 80 ≾ D_(tran)/pkpc < 200, the H I line-of-sight velocity range reaches a minimum, with a corresponding flattening in the rest-frame Lyα equivalent width. These observations can be naturally explained as the transition between outflow-dominated and accretion-dominated flows. Beyond D_(tran) ≃ 300 kpc, the line of sight kinematics are dominated by Hubble expansion.


Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/2006.13236arXivDiscussion Paper
http://ramekin.caltech.edu/KBSS/Related ItemData
ORCID:
AuthorORCID
Chen, Yuguang0000-0003-4520-5395
Steidel, Charles C.0000-0002-4834-7260
Hummels, Cameron B.0000-0002-3817-8133
Rudie, Gwen C.0000-0002-8459-5413
Trainor, Ryan F.0000-0002-6967-7322
Erb, Dawn K.0000-0001-9714-2758
Pettini, Max0000-0002-5139-4359
Reddy, Naveen A.0000-0001-9687-4973
Shapley, Alice E.0000-0003-3509-4855
Strom, Allison L.0000-0001-6369-1636
Theios, Rachel L.0000-0002-4236-1037
Faucher-Giguère, Claude-André0000-0002-4900-6628
Hopkins, Philip F.0000-0003-3729-1684
Kereš, Dušan0000-0002-1666-7067
Additional Information:Based on data obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This paper has included data obtained using Keck/LRIS (Oke et al. 1995; Steidel et al. 2004; Rockosi et al. 2010) and Keck/MOSFIRE (McLean et al. 2010, 2012). We thank the W.M. Keck Observatory staff for their assistance with the observations over two decades. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The following software packages have been crucial to preparing for this paper: the IDL Astronomy User's Library14, the Coyote IDL library15, Astropy (Price-Whelan et al. 2018), Emcee (Foreman-Mackey et al. 2013), the yt project (Turk et al. 2011), and Trident (Hummels et al. 2017). This work was supported in part by grant AST-1313472 from the U.S. NSF, and by a grant from the Caltech/JPL President's and Director's Program. CAFG was supported by NSF through grants AST-1517491, AST-1715216, and CAREER award AST-1652522, by NASA through grant 17-ATP17-0067, by STScI through grants HST-GO-14681.011, HST-GO-14268.022-A, and HST-AR-14293.001-A, and by a Cottrell Scholar Award from the Research Corporation for Science Advancement. YC would like to thank Hongjie Zhu, for her continuous encouragements when preparing for this paper. We would like to acknowledge YiqiuMa, E. Sterl Phinney, and Mateusz Matuszewski, for their constructive discussions. Finally, we thank collaborators Kurt L. Adelberger, Matthew P. Hunt, David R. Law, Olivera Rakic, and Monica L. Turner for their contributions to the KBSS survey over the course of nearly two decades.
Group:Astronomy Department, TAPIR
Funders:
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
NSFAST-1313472
JPL President and Director's FundUNSPECIFIED
NSFAST-1517491
NSFAST-1715216
NSFAST-1652522
NASA17-ATP17-0067
NASAHST-GO-14681.011
NASAHST-GO-14268.022-A
NASAHST-AR-14293.001-A
Cottrell Scholar of Research CorporationUNSPECIFIED
Subject Keywords:galaxies: evolution | galaxies: ISM | galaxies: high-redshift
Record Number:CaltechAUTHORS:20200626-150116926
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200626-150116926
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:104099
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:29 Jun 2020 15:45
Last Modified:29 Jun 2020 15:45

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