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Title: Gas kinematics, morphology and angular momentum in the FIRE simulations

Abstract

We report on the z = 0 gas kinematics, morphology and angular momentum content of isolated galaxies in a suite of cosmological zoom-in simulations from the FIRE project spanning Mstar = 106–11 M. Gas becomes increasingly rotationally supported with increasing galaxy mass. In the lowest mass galaxies (Mstar < 108M), gas fails to form a morphological disc and is primarily dispersion and pressure supported. At intermediate masses (Mstar = 108–10 M), galaxies display a wide range of gas kinematics and morphologies, from thin, rotating discs to irregular spheroids with negligible net rotation. All the high-mass (Mstar = 1010–11 M) galaxies form rotationally supported gas discs. Many of the haloes whose galaxies fail to form discs harbour high angular momentum gas in their circumgalactic medium. The ratio of the specific angular momentum of gas in the central galaxy to that of the dark matter halo increases significantly with galaxy mass, from $$\langle$$jgas$$\rangle$$$\langle$$jDM$$\rangle$$ ~ 0.1 at Mstar=106--7M⊙ to$$\langle$$gas$$\rangle$$/$$\langle$$jDM$$\rangle$$ ~ 2 at Mstar = 1010–11 M. The reduced rotational support in the lowest mass galaxies owes to (a) stellar feedback and the UV background suppressing the accretion of high angular momentum gas at late times, and (b) stellar feedback driving large non-circular gas motions. We broadly repeat the observed scaling relations between galaxy mass, gas rotation velocity, size and angular momentum, but may somewhat underpredict the incidence of disky, high angular momentum galaxies at the lowest observed masses (Mstar = (106-2× 107) M). Stars form preferentially from low angular momentum gas near the galactic centre and are less rotationally supported than gas. The common assumption that stars follow the same rotation curve as gas thus substantially overestimates the simulated galaxies’ stellar angular momentum, particularly at low masses.

Authors:
ORCiD logo [1];  [1];  [2]; ORCiD logo [3]; ORCiD logo [1];  [4];  [5];  [5];  [4];  [6]; ORCiD logo [3]
  1. Univ. of California, Berkeley, CA (United States)
  2. California Inst. of Technology (CalTech), Pasadena, CA (United States); Observatories of the Carnegie Inst. for Science, Pasadena, CA (United States); Univ. of California, Davis, CA (United States)
  3. California Inst. of Technology (CalTech), Pasadena, CA (United States)
  4. Univ. of California, San Diego, CA (United States)
  5. Univ. of Texas, Austin, TX (United States)
  6. Northwestern Univ., Evanston, IL (United States)
Publication Date:
Research Org.:
Lawrence Berkeley National Lab. (LBNL), Berkeley, CA (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1523825
Grant/Contract Number:  
AC02-05CH11231
Resource Type:
Accepted Manuscript
Journal Name:
Monthly Notices of the Royal Astronomical Society
Additional Journal Information:
Journal Volume: 473; Journal Issue: 2; Journal ID: ISSN 0035-8711
Publisher:
Royal Astronomical Society
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; galaxies: dwarf; galaxies: irregular; galaxies: kinematics and dynamics

Citation Formats

El-Badry, Kareem, Quataert, Eliot, Wetzel, Andrew, Hopkins, Philip F., Weisz, Daniel R., Chan, T. K., Fitts, Alex, Boylan-Kolchin, Michael, Kereš, Dušan, Faucher-Giguère, Claude-André, and Garrison-Kimmel, Shea. Gas kinematics, morphology and angular momentum in the FIRE simulations. United States: N. p., 2017. Web. doi:10.1093/mnras/stx2482.
El-Badry, Kareem, Quataert, Eliot, Wetzel, Andrew, Hopkins, Philip F., Weisz, Daniel R., Chan, T. K., Fitts, Alex, Boylan-Kolchin, Michael, Kereš, Dušan, Faucher-Giguère, Claude-André, & Garrison-Kimmel, Shea. Gas kinematics, morphology and angular momentum in the FIRE simulations. United States. doi:https://doi.org/10.1093/mnras/stx2482
El-Badry, Kareem, Quataert, Eliot, Wetzel, Andrew, Hopkins, Philip F., Weisz, Daniel R., Chan, T. K., Fitts, Alex, Boylan-Kolchin, Michael, Kereš, Dušan, Faucher-Giguère, Claude-André, and Garrison-Kimmel, Shea. Tue . "Gas kinematics, morphology and angular momentum in the FIRE simulations". United States. doi:https://doi.org/10.1093/mnras/stx2482. https://www.osti.gov/servlets/purl/1523825.
@article{osti_1523825,
title = {Gas kinematics, morphology and angular momentum in the FIRE simulations},
author = {El-Badry, Kareem and Quataert, Eliot and Wetzel, Andrew and Hopkins, Philip F. and Weisz, Daniel R. and Chan, T. K. and Fitts, Alex and Boylan-Kolchin, Michael and Kereš, Dušan and Faucher-Giguère, Claude-André and Garrison-Kimmel, Shea},
abstractNote = {We report on the z = 0 gas kinematics, morphology and angular momentum content of isolated galaxies in a suite of cosmological zoom-in simulations from the FIRE project spanning Mstar = 106–11 M⊙. Gas becomes increasingly rotationally supported with increasing galaxy mass. In the lowest mass galaxies (Mstar < 108M⊙), gas fails to form a morphological disc and is primarily dispersion and pressure supported. At intermediate masses (Mstar = 108–10 M⊙), galaxies display a wide range of gas kinematics and morphologies, from thin, rotating discs to irregular spheroids with negligible net rotation. All the high-mass (Mstar = 1010–11 M⊙) galaxies form rotationally supported gas discs. Many of the haloes whose galaxies fail to form discs harbour high angular momentum gas in their circumgalactic medium. The ratio of the specific angular momentum of gas in the central galaxy to that of the dark matter halo increases significantly with galaxy mass, from $\langle$jgas$\rangle$$\langle$jDM$\rangle$ ~ 0.1 at Mstar=106--7M⊙ to$\langle$gas$\rangle$/$\langle$jDM$\rangle$ ~ 2 at Mstar = 1010–11 M⊙. The reduced rotational support in the lowest mass galaxies owes to (a) stellar feedback and the UV background suppressing the accretion of high angular momentum gas at late times, and (b) stellar feedback driving large non-circular gas motions. We broadly repeat the observed scaling relations between galaxy mass, gas rotation velocity, size and angular momentum, but may somewhat underpredict the incidence of disky, high angular momentum galaxies at the lowest observed masses (Mstar = (106-2× 107) M⊙). Stars form preferentially from low angular momentum gas near the galactic centre and are less rotationally supported than gas. The common assumption that stars follow the same rotation curve as gas thus substantially overestimates the simulated galaxies’ stellar angular momentum, particularly at low masses.},
doi = {10.1093/mnras/stx2482},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 2,
volume = 473,
place = {United States},
year = {2017},
month = {9}
}

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Cited by: 51 works
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Figures / Tables:

Table 1 Table 1: Summary of the simulations at $z$ = 0.

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