Strong suppression of star formation and spiral arm formation in disc galaxies with counter-rotating gas discs

Omima Osman, Kenji Bekki

Research output: Contribution to journalArticle

Abstract

Galaxy-wide star formation can be quenched by a number of physical processes such as environmental effects (e.g. ram pressure stripping) and supernova feedback. Using numerical simulations, we here demonstrate that star formation can be severely suppressed in disc galaxies with their gas discs counter-rotating with respect to their stellar discs. This new mechanism of star formation suppression (or quenching) does not depend so strongly on model parameters of disc galaxies, such as bulge-to-disc ratios and gas mass fractions. Such severe suppression of star formation is largely due to the suppression of the gas density enhancing mechanism, i.e. spiral arm formation in disc galaxies with counter-rotating gas. Our simulations also show that molecular hydrogen and dust can be rather slowly consumed by star formation in disc galaxies with counter-rotating gas discs (i.e. long gas depletion time-scale). Based on these results, we suggest that spiral and S0 galaxies with counter-rotation can have rather low star formation rate for their gas densities. Also, we suggest that a minor fraction of S0 galaxies have no prominent spiral arms because they have a higher fraction of counter-rotating gas. We predict that poststarburst 'E+A' disc galaxies with cold gas could have counter-rotating gas.

LanguageEnglish
PagesL87-L91
Number of pages5
JournalMonthly Notices of the Royal Astronomical Society
Volume471
Issue number1
DOIs
StatePublished - Oct 2017

Cite this

@article{1c9f069ce63f48caa61e984376b691e1,
title = "Strong suppression of star formation and spiral arm formation in disc galaxies with counter-rotating gas discs",
abstract = "Galaxy-wide star formation can be quenched by a number of physical processes such as environmental effects (e.g. ram pressure stripping) and supernova feedback. Using numerical simulations, we here demonstrate that star formation can be severely suppressed in disc galaxies with their gas discs counter-rotating with respect to their stellar discs. This new mechanism of star formation suppression (or quenching) does not depend so strongly on model parameters of disc galaxies, such as bulge-to-disc ratios and gas mass fractions. Such severe suppression of star formation is largely due to the suppression of the gas density enhancing mechanism, i.e. spiral arm formation in disc galaxies with counter-rotating gas. Our simulations also show that molecular hydrogen and dust can be rather slowly consumed by star formation in disc galaxies with counter-rotating gas discs (i.e. long gas depletion time-scale). Based on these results, we suggest that spiral and S0 galaxies with counter-rotation can have rather low star formation rate for their gas densities. Also, we suggest that a minor fraction of S0 galaxies have no prominent spiral arms because they have a higher fraction of counter-rotating gas. We predict that poststarburst 'E+A' disc galaxies with cold gas could have counter-rotating gas.",
keywords = "galaxies: evolution, galaxies: ISM, galaxies: star formation, E+A GALAXIES, MOLECULAR-HYDROGEN, ATLAS(3D) PROJECT, IONIZED-GAS, S0 GALAXIES, COLD GAS, KINEMATICS, DUST, ACCRETION, EVOLUTION",
author = "Omima Osman and Kenji Bekki",
year = "2017",
month = "10",
doi = "10.1093/mnrasl/slx104",
language = "English",
volume = "471",
pages = "L87--L91",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "OXFORD UNIV PRESS UNITED KINGDOM",
number = "1",

}

TY - JOUR

T1 - Strong suppression of star formation and spiral arm formation in disc galaxies with counter-rotating gas discs

AU - Osman,Omima

AU - Bekki,Kenji

PY - 2017/10

Y1 - 2017/10

N2 - Galaxy-wide star formation can be quenched by a number of physical processes such as environmental effects (e.g. ram pressure stripping) and supernova feedback. Using numerical simulations, we here demonstrate that star formation can be severely suppressed in disc galaxies with their gas discs counter-rotating with respect to their stellar discs. This new mechanism of star formation suppression (or quenching) does not depend so strongly on model parameters of disc galaxies, such as bulge-to-disc ratios and gas mass fractions. Such severe suppression of star formation is largely due to the suppression of the gas density enhancing mechanism, i.e. spiral arm formation in disc galaxies with counter-rotating gas. Our simulations also show that molecular hydrogen and dust can be rather slowly consumed by star formation in disc galaxies with counter-rotating gas discs (i.e. long gas depletion time-scale). Based on these results, we suggest that spiral and S0 galaxies with counter-rotation can have rather low star formation rate for their gas densities. Also, we suggest that a minor fraction of S0 galaxies have no prominent spiral arms because they have a higher fraction of counter-rotating gas. We predict that poststarburst 'E+A' disc galaxies with cold gas could have counter-rotating gas.

AB - Galaxy-wide star formation can be quenched by a number of physical processes such as environmental effects (e.g. ram pressure stripping) and supernova feedback. Using numerical simulations, we here demonstrate that star formation can be severely suppressed in disc galaxies with their gas discs counter-rotating with respect to their stellar discs. This new mechanism of star formation suppression (or quenching) does not depend so strongly on model parameters of disc galaxies, such as bulge-to-disc ratios and gas mass fractions. Such severe suppression of star formation is largely due to the suppression of the gas density enhancing mechanism, i.e. spiral arm formation in disc galaxies with counter-rotating gas. Our simulations also show that molecular hydrogen and dust can be rather slowly consumed by star formation in disc galaxies with counter-rotating gas discs (i.e. long gas depletion time-scale). Based on these results, we suggest that spiral and S0 galaxies with counter-rotation can have rather low star formation rate for their gas densities. Also, we suggest that a minor fraction of S0 galaxies have no prominent spiral arms because they have a higher fraction of counter-rotating gas. We predict that poststarburst 'E+A' disc galaxies with cold gas could have counter-rotating gas.

KW - galaxies: evolution

KW - galaxies: ISM

KW - galaxies: star formation

KW - E+A GALAXIES

KW - MOLECULAR-HYDROGEN

KW - ATLAS(3D) PROJECT

KW - IONIZED-GAS

KW - S0 GALAXIES

KW - COLD GAS

KW - KINEMATICS

KW - DUST

KW - ACCRETION

KW - EVOLUTION

U2 - 10.1093/mnrasl/slx104

DO - 10.1093/mnrasl/slx104

M3 - Article

VL - 471

SP - L87-L91

JO - Monthly Notices of the Royal Astronomical Society

T2 - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 1

ER -