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Figuring Out Gas & Galaxies in Enzo (FOGGIE). I. Resolving Simulated Circumgalactic Absorption at 2 ≤ z ≤ 2.5

Peeples, Molly S. and Corlies, Lauren and Tumlinson, Jason and O’Shea, Brian W. and Lehner, Nicolas and O’Meara, John M. and Howk, J. Christopher and Earl, Nicholas and Smith, Britton D. and Wise, John H. and Hummels, Cameron B. (2019) Figuring Out Gas & Galaxies in Enzo (FOGGIE). I. Resolving Simulated Circumgalactic Absorption at 2 ≤ z ≤ 2.5. Astrophysical Journal, 873 (2). Art. No. 129. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20190313-131244125

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Abstract

We present simulations from the new "Figuring Out Gas & Galaxies in Enzo" (FOGGIE) project. In contrast to most extant simulations of galaxy formation, which concentrate computational resources on galactic disks and spheroids with fluid and particle elements of fixed mass, the FOGGIE simulations focus on extreme spatial and mass resolution in the circumgalactic medium (CGM) surrounding galaxies. Using the Enzo code and a new refinement scheme, FOGGIE reaches spatial resolutions of 381 comoving h^(−1) pc and resolves extremely low masses (≾1–100 M⊙) out to 100 comoving h^(−1) kpc from the central halo. At these resolutions, cloud and filament-like structures giving rise to simulated absorption are smaller, and better resolved, than the same structures simulated with standard density-dependent refinement. Most of the simulated absorption arises in identifiable and well-resolved structures with masses ≾10^4 M⊙, well below the mass resolution of typical zoom simulations. However, integrated quantities such as mass surface density and ionic covering fractions change at only the ≾30% level as resolution is varied. These relatively small changes in projected quantities—even when the sizes and distribution of absorbing clouds change dramatically—indicate that commonly used observables provide only weak constraints on the physical structure of the underlying gas. Comparing the simulated absorption features to the KODIAQ (Keck Observatory Database of Ionized Absorption toward Quasars) survey of z ~ 2–3.5 Lyman limit systems, we show that high-resolution FOGGIE runs better resolve the internal kinematic structure of detected absorption and better match the observed distribution of absorber properties. These results indicate that circumgalactic medium resolution is key in properly testing simulations of galaxy evolution with circumgalactic observations.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/ab0654DOIArticle
https://arxiv.org/abs/1810.06566arXivDiscussion Paper
ORCID:
AuthorORCID
Peeples, Molly S.0000-0003-1455-8788
Corlies, Lauren0000-0002-0646-1540
Tumlinson, Jason0000-0002-7982-412X
O’Shea, Brian W.0000-0002-2786-0348
Lehner, Nicolas0000-0001-9158-0829
O’Meara, John M.0000-0002-7893-1054
Howk, J. Christopher0000-0002-2591-3792
Earl, Nicholas0000-0003-1714-7415
Smith, Britton D.0000-0002-6804-630X
Wise, John H.0000-0003-1173-8847
Hummels, Cameron B.0000-0002-3817-8133
Additional Information:© 2019 The American Astronomical Society. Received 2018 October 11; revised 2019 January 23; accepted 2019 January 26; published 2019 March 13. This study was primarily funded by the National Science Foundation via NSF AST-1517908, which helped support the contributions of L.C., B.W.O., N.L., J.O.M., and J.C.H. L.C. was additionally supported in part by HST AR #15012. B.W.O. was supported in part by NSF grants PHY-1430152, AST-1514700, and OAC-1835213, by NASA grants NNX12AC98G and NNX15AP39G, and by HST AR #14315. N.L. was also supported by NASA ADAP grant NNX16AF52G. N.E. was supported by HST AR #13919, HST GO #14268, and HST AR #14560. B.D.S. was supported by NSF AST-1615848. J.H.W. was supported by NSF grants AST-1614333 and OAC-1835213, NASA grant NNX17AG23G, and HST-AR-14326. C.B.H. was supported by HST AR #13917, HST AR #13919, and an NSF AAPF. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center and were sponsored by NASA's Science Mission Directorate; we are grateful for the superb user support provided by NAS. Resources were also provided by the Blue Waters sustained-petascale computing project, which is supported by the NSF (award No. ACI 1238993 and ACI-1514580) and the state of Illinois. Blue Waters is a joint effort of the University of Illinois at Urbana-Champaign and its NCSA. This work benefited from the dancing penguin and all the things emojis on Slack. The data presented herein were 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 research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. 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. We have made extensive use of the Python libraries Astropy, a community-developed core Python package for Astronomy (The Astropy Collaboration et al. 2018, http://www.astropy.org), datashader and holoviews from Anaconda (datashader.org), pandas (McKinney 2010), and seaborn. Computations described in this work were performed using the publicly available Enzo code, which is the product of a collaborative effort of many independent scientists from numerous institutions around the world. Facilities: NASA Pleiades - , Blue Waters - , Keck (HIRES) - . Software: astropy (The Astropy Collaboration et al. 2018), Cloudy (Ferland et al. 2013), Enzo (Bryan et al. 2014), grackle (Smith et al. 2017), yt (Turk et al. 2011), Trident (Hummels et al. 2017), ytree (Smith & Lang 2018).
Funders:
Funding AgencyGrant Number
NSFAST-1517908
NASAAR-15012
NSFPHY-1430152
NSFAST-1514700
NSFOAC-1835213
NASANNX12AC98G
NASANNX15AP39G
NASAAR-14315
NASANNX16AF52G
NASAAR-13919
NASAAR-14268
NASAAR-14560
NSFAST-1615848
NSFAST-1614333
NSFOAC-1835213
NASANNX17AG23G
NASAAR14326
NASAAR-13917
NASAAR-13919
NSF Astronomy and Astrophysics FellowshipUNSPECIFIED
NSFACI-1238993
NSFACI-1514580
State of IllinoisUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
Subject Keywords:galaxies: evolution – hydrodynamics – intergalactic medium – quasars: absorption lines
Record Number:CaltechAUTHORS:20190313-131244125
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20190313-131244125
Official Citation:Molly S. Peeples et al 2019 ApJ 873 129
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:93784
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:13 Mar 2019 21:14
Last Modified:13 Mar 2019 21:14

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