Fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies

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Context. Recent observational and theoretical works have suggested that the Tully-Fisher relation might be generalised to include dispersion-dominated systems by combining the rotation and dispersion velocity in the definition of the kinematical indicator. Mergers and interactions have been pointed...

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Autores principales: De Rossi, M.E., Tissera, P.B., Pedrosa, S.E.
Formato: Artículo publishedVersion
Lenguaje:Inglés
Publicado: 2012
Materias:
Galaxies: evolution
Galaxies: formation
Galaxies: structure
Evolution of galaxies
Galaxies: evolutions
Gas phase velocity
Joint actions
Multiphase model
Potential wells
Rotation curves
Rotation velocity
Simulated evolutions
Starbursts
Computer simulation
Dispersions
Galaxies
Kinematics
Mergers and acquisitions
Morphology
Rotation
Stars
Velocity
Gases
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_00046361_v546_n_p_DeRossi
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
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spelling paperaa:paper_00046361_v546_n_p_DeRossi2023-06-12T16:40:55Z Fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies Astron. Astrophys. 2012;546 De Rossi, M.E. Tissera, P.B. Pedrosa, S.E. Galaxies: evolution Galaxies: formation Galaxies: structure Evolution of galaxies Galaxies: evolutions Galaxies: formation Galaxies: structure Gas phase velocity Joint actions Multiphase model Potential wells Rotation curves Rotation velocity Simulated evolutions Starbursts Computer simulation Dispersions Galaxies Kinematics Mergers and acquisitions Morphology Rotation Stars Velocity Gases Context. Recent observational and theoretical works have suggested that the Tully-Fisher relation might be generalised to include dispersion-dominated systems by combining the rotation and dispersion velocity in the definition of the kinematical indicator. Mergers and interactions have been pointed out as responsible of driving turbulent and disordered gas kinematics, which could generate Tully-Fisher relation outliers. Aims. We investigated the gas kinematics of galaxies by using a simulated sample that includes gas-disc-dominated as well as spheroid-dominated systems. We paid particular attention to the scatter evolution of the Tully-Fisher relation. We also determined the gas-phase velocity indicator, which traces the potential well of the galaxy better. Methods. Cosmological hydrodynamical simulations that include a multiphase model and physically motivated supernova feedback were performed to follow the evolution of galaxies as they are assembled. We analysed the gas kinematics of the surviving gas discs to estimate all velocity indicators. Results. Both the baryonic and stellar Tully-Fisher relations for gas-disc-dominated systems are tight while, as more dispersion-dominated systems are included, the scatter increases. We found a clear correlation between σ/V rot and morphology, with dispersion-dominated systems exhibiting higher values (>0.7). Mergers and interactions can affect the rotation curves directly or indirectly, inducing a scatter in the Tully-Fisher relation larger than the simulated evolution since z ~ 3. Kinematical indicators, which combine rotation velocity and dispersion velocity, can reduce the scatter in the baryonic and the stellar mass-velocity relations. In particular, s 1.0 = (V rot 2 + σ 2) 0.5 seems to be the best tracer of the circular velocity at larger radii. Our findings also show that the lowest scatter in both relations is obtained if the velocity indicators are measured at the maximum of the rotation curve. Conclusions. In agreement with previous works, we found that the gas kinematics of galaxies is significantly regulated by mergers and interactions, which play a key role in inducing gas accretion, outflows and starbursts. The joint action of these processes within a hierarchical ΛCDM Universe generates a mean simulated Tully-Fisher relation in good agreement with observations since z ~ 3 but with a scatter depending on morphology. The rotation velocity estimated at the maximum of the gas rotation curve is found to be the best proxy for the potential well regardless of morphology. ©2012 ESO. Fil:De Rossi, M.E. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Tissera, P.B. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. Fil:Pedrosa, S.E. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. 2012 info:eu-repo/semantics/article info:ar-repo/semantics/artículo info:eu-repo/semantics/publishedVersion application/pdf eng info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_00046361_v546_n_p_DeRossi
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
language Inglés
orig_language_str_mv eng
topic Galaxies: evolution
Galaxies: formation
Galaxies: structure
Evolution of galaxies
Galaxies: evolutions
Galaxies: formation
Galaxies: structure
Gas phase velocity
Joint actions
Multiphase model
Potential wells
Rotation curves
Rotation velocity
Simulated evolutions
Starbursts
Computer simulation
Dispersions
Galaxies
Kinematics
Mergers and acquisitions
Morphology
Rotation
Stars
Velocity
Gases
spellingShingle Galaxies: evolution
Galaxies: formation
Galaxies: structure
Evolution of galaxies
Galaxies: evolutions
Galaxies: formation
Galaxies: structure
Gas phase velocity
Joint actions
Multiphase model
Potential wells
Rotation curves
Rotation velocity
Simulated evolutions
Starbursts
Computer simulation
Dispersions
Galaxies
Kinematics
Mergers and acquisitions
Morphology
Rotation
Stars
Velocity
Gases
De Rossi, M.E.
Tissera, P.B.
Pedrosa, S.E.
Fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies
topic_facet Galaxies: evolution
Galaxies: formation
Galaxies: structure
Evolution of galaxies
Galaxies: evolutions
Galaxies: formation
Galaxies: structure
Gas phase velocity
Joint actions
Multiphase model
Potential wells
Rotation curves
Rotation velocity
Simulated evolutions
Starbursts
Computer simulation
Dispersions
Galaxies
Kinematics
Mergers and acquisitions
Morphology
Rotation
Stars
Velocity
Gases
description Context. Recent observational and theoretical works have suggested that the Tully-Fisher relation might be generalised to include dispersion-dominated systems by combining the rotation and dispersion velocity in the definition of the kinematical indicator. Mergers and interactions have been pointed out as responsible of driving turbulent and disordered gas kinematics, which could generate Tully-Fisher relation outliers. Aims. We investigated the gas kinematics of galaxies by using a simulated sample that includes gas-disc-dominated as well as spheroid-dominated systems. We paid particular attention to the scatter evolution of the Tully-Fisher relation. We also determined the gas-phase velocity indicator, which traces the potential well of the galaxy better. Methods. Cosmological hydrodynamical simulations that include a multiphase model and physically motivated supernova feedback were performed to follow the evolution of galaxies as they are assembled. We analysed the gas kinematics of the surviving gas discs to estimate all velocity indicators. Results. Both the baryonic and stellar Tully-Fisher relations for gas-disc-dominated systems are tight while, as more dispersion-dominated systems are included, the scatter increases. We found a clear correlation between σ/V rot and morphology, with dispersion-dominated systems exhibiting higher values (>0.7). Mergers and interactions can affect the rotation curves directly or indirectly, inducing a scatter in the Tully-Fisher relation larger than the simulated evolution since z ~ 3. Kinematical indicators, which combine rotation velocity and dispersion velocity, can reduce the scatter in the baryonic and the stellar mass-velocity relations. In particular, s 1.0 = (V rot 2 + σ 2) 0.5 seems to be the best tracer of the circular velocity at larger radii. Our findings also show that the lowest scatter in both relations is obtained if the velocity indicators are measured at the maximum of the rotation curve. Conclusions. In agreement with previous works, we found that the gas kinematics of galaxies is significantly regulated by mergers and interactions, which play a key role in inducing gas accretion, outflows and starbursts. The joint action of these processes within a hierarchical ΛCDM Universe generates a mean simulated Tully-Fisher relation in good agreement with observations since z ~ 3 but with a scatter depending on morphology. The rotation velocity estimated at the maximum of the gas rotation curve is found to be the best proxy for the potential well regardless of morphology. ©2012 ESO.
format Artículo
Artículo
publishedVersion
author De Rossi, M.E.
Tissera, P.B.
Pedrosa, S.E.
author_facet De Rossi, M.E.
Tissera, P.B.
Pedrosa, S.E.
author_sort De Rossi, M.E.
title Fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies
title_short Fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies
title_full Fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies
title_fullStr Fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies
title_full_unstemmed Fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies
title_sort fingerprints of the hierarchical building-up of the structure on the gas kinematics of galaxies
publishDate 2012
url http://hdl.handle.net/20.500.12110/paper_00046361_v546_n_p_DeRossi
work_keys_str_mv AT derossime fingerprintsofthehierarchicalbuildingupofthestructureonthegaskinematicsofgalaxies
AT tisserapb fingerprintsofthehierarchicalbuildingupofthestructureonthegaskinematicsofgalaxies
AT pedrosase fingerprintsofthehierarchicalbuildingupofthestructureonthegaskinematicsofgalaxies
_version_ 1769810153682501632

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