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Title: The Relation between Galaxy ISM and Circumgalactic Ovi Gas Kinematics Derived from Observations and ΛCDM Simulations

Journal Article · · The Astrophysical Journal (Online)
 [1];  [2]; ORCiD logo [1]; ORCiD logo [3]; ORCiD logo [1]; ORCiD logo [4]; ORCiD logo [5];  [4];  [4]; ORCiD logo [6];  [2]
  1. Swinburne Univ. of Technology, VIC (Australia)
  2. Swinburne Univ. of Technology, VIC (Australia); New Mexico State Univ., Las Cruces, NM (United States)
  3. Leiden Univ. (Netherlands)
  4. New Mexico State Univ., Las Cruces, NM (United States)
  5. Heidelberg Univ. (Germany)
  6. Pennsylvania State Univ., University Park, PA (United States)
+ Show Author Affiliations

We introduce the first galaxy–Ovi absorption kinematic study for 20 absorption systems (EW > 0.1 Å) associated with isolated galaxies (0.15 ≤ z ≤ 0.55) that have accurate redshifts and rotation curves obtained using Keck/ESI. Our sample is split into two azimuthal angle bins: major axis (Φ < 25°) and minor axis (Φ > 33°). O vi absorption along the galaxy major axis is not correlated with galaxy rotation kinematics, with only 1/10 of systems that could be explained with rotation/accretion models. This is in contrast to corotation commonly observed for Mg ii absorption. Ovi along the minor axis could be modeled by accelerating outflows, but only for small opening angles, while the majority of the Ovi is decelerating. Along both axes, stacked Ovi profiles reside at the galaxy systemic velocity with the absorption kinematics spanning the entire dynamical range of their galaxies. The Ovi found in AMR cosmological simulations exists within filaments and in halos of ~50 kpc surrounding galaxies. Simulations show that major-axis Ovi gas inflows along filaments and decelerates as it approaches the galaxy, while increasing in its level of corotation. Minor-axis outflows in the simulations are effective within 50–75 kpc; beyond that they decelerate and fall back onto the galaxy. While the simulations show clear Ovi kinematic signatures, they are not directly comparable to observations. When we compare kinematic signatures integrated through the entire simulated galaxy halo, we find that these signatures are washed out owing to full velocity distribution of Ovi throughout the halo. We illustrate that Ovi alone does not serve as a useful kinematic indicator of gas accretion, outflows, or star formation and likely best probes the halo virial temperature.

Research Organization:
Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States). National Energy Research Scientific Computing Center (NERSC)
Sponsoring Organization:
Australian Research Council; NASA; National Science Foundation (NSF); USDOE
OSTI ID:
1544076
Journal Information:
The Astrophysical Journal (Online), Journal Name: The Astrophysical Journal (Online) Journal Issue: 2 Vol. 870; ISSN 1538-4357
Publisher:
Institute of Physics (IOP)Copyright Statement
Country of Publication:
United States
Language:
English

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Metal-enriched, sub-kiloparsec gas clumps in the circumgalactic medium of a faint z = 2.5 galaxy text January 2014
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Cited By (9)

Evolution of neutral oxygen during the epoch of reionization and its use in estimating the neutral hydrogen fraction journal August 2019
Quasar Sightline and Galaxy Evolution (QSAGE) survey – I. The galaxy environment of O vi absorbers up to z = 1.4 around PKS 0232−04 journal March 2019
Kinematics of Circumgalactic Gas: Feeding Galaxies and Feedback journal June 2019
Relationship between the Metallicity of the Circumgalactic Medium and Galaxy Orientation journal September 2019
Kinematics of the O vi Circumgalactic Medium: Halo Mass Dependence and Outflow Signatures journal November 2019
The Relationship between Galaxy ISM and Circumgalactic Gas Metallicities journal November 2019
Quasar Sightline and Galaxy Evolution (QSAGE) Survey - I. The Galaxy Environment of OVI Absorbers up to z=1.4 around PKS 0232-04 text January 2018
Kinematics of the OVI Circumgalactic Medium: Halo Mass Dependence and Outflow Signatures text January 2019
The Relationship Between Galaxy ISM and Circumgalactic Gas Metallicities text January 2019

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79 ASTRONOMY AND ASTROPHYSICS
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