Morphology and molecular gas fractions of local luminous infrared galaxies as a function of infrared luminosity and merger stage

We present a new, detailed analysis of the morphologies and molecular gas fractions (MGFs) for a complete sample of 65 local luminous infrared galaxies from Great Observatories All-Sky Luminous Infrared Galaxies (LIRG) Survey using high resolution I-band images from The Hubble Space Telescope, the U...

Descripción completa

Guardado en:
Detalles Bibliográficos
Publicado: 2016
Materias:
galaxies: evolution
galaxies: interactions
infrared: galaxies
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v825_n2_p_Larson
http://hdl.handle.net/20.500.12110/paper_0004637X_v825_n2_p_Larson
Aporte de:
Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id paper:paper_0004637X_v825_n2_p_Larson
record_format dspace
spelling paper:paper_0004637X_v825_n2_p_Larson2023-06-08T14:29:17Z Morphology and molecular gas fractions of local luminous infrared galaxies as a function of infrared luminosity and merger stage galaxies: evolution galaxies: interactions infrared: galaxies We present a new, detailed analysis of the morphologies and molecular gas fractions (MGFs) for a complete sample of 65 local luminous infrared galaxies from Great Observatories All-Sky Luminous Infrared Galaxies (LIRG) Survey using high resolution I-band images from The Hubble Space Telescope, the University of Hawaii 2.2 m Telescope and the Pan-STARRS1 Survey. Our classification scheme includes single undisturbed galaxies, minor mergers, and major mergers, with the latter divided into five distinct stages from pre-first pericenter passage to final nuclear coalescence. We find that major mergers of molecular gas-rich spirals clearly play a major role for all sources with L IR > 10 11.5 L ⊙ ; however, below this luminosity threshold, minor mergers and secular processes dominate. Additionally, galaxies do not reach L IR > 10 12.0 L ⊙ until late in the merger process when both disks are near final coalescence. The mean MGF (MGF = M H2 /(M ∗ +M H2 )) for non-interacting and early-stage major merger LIRGs is 18 ± 2%, which increases to 33 ± 3%, for intermediate stage major merger LIRGs, consistent with the hypothesis that, during the early-mid stages of major mergers, most of the initial large reservoir of atomic gas (HI) at large galactocentric radii is swept inward where it is converted into molecular gas (H 2 ). © 2016. The American Astronomical Society. All rights reserved. 2016 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v825_n2_p_Larson http://hdl.handle.net/20.500.12110/paper_0004637X_v825_n2_p_Larson
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic galaxies: evolution
galaxies: interactions
infrared: galaxies
spellingShingle galaxies: evolution
galaxies: interactions
infrared: galaxies
Morphology and molecular gas fractions of local luminous infrared galaxies as a function of infrared luminosity and merger stage
topic_facet galaxies: evolution
galaxies: interactions
infrared: galaxies
description We present a new, detailed analysis of the morphologies and molecular gas fractions (MGFs) for a complete sample of 65 local luminous infrared galaxies from Great Observatories All-Sky Luminous Infrared Galaxies (LIRG) Survey using high resolution I-band images from The Hubble Space Telescope, the University of Hawaii 2.2 m Telescope and the Pan-STARRS1 Survey. Our classification scheme includes single undisturbed galaxies, minor mergers, and major mergers, with the latter divided into five distinct stages from pre-first pericenter passage to final nuclear coalescence. We find that major mergers of molecular gas-rich spirals clearly play a major role for all sources with L IR > 10 11.5 L ⊙ ; however, below this luminosity threshold, minor mergers and secular processes dominate. Additionally, galaxies do not reach L IR > 10 12.0 L ⊙ until late in the merger process when both disks are near final coalescence. The mean MGF (MGF = M H2 /(M ∗ +M H2 )) for non-interacting and early-stage major merger LIRGs is 18 ± 2%, which increases to 33 ± 3%, for intermediate stage major merger LIRGs, consistent with the hypothesis that, during the early-mid stages of major mergers, most of the initial large reservoir of atomic gas (HI) at large galactocentric radii is swept inward where it is converted into molecular gas (H 2 ). © 2016. The American Astronomical Society. All rights reserved.
title Morphology and molecular gas fractions of local luminous infrared galaxies as a function of infrared luminosity and merger stage
title_short Morphology and molecular gas fractions of local luminous infrared galaxies as a function of infrared luminosity and merger stage
title_full Morphology and molecular gas fractions of local luminous infrared galaxies as a function of infrared luminosity and merger stage
title_fullStr Morphology and molecular gas fractions of local luminous infrared galaxies as a function of infrared luminosity and merger stage
title_full_unstemmed Morphology and molecular gas fractions of local luminous infrared galaxies as a function of infrared luminosity and merger stage
title_sort morphology and molecular gas fractions of local luminous infrared galaxies as a function of infrared luminosity and merger stage
publishDate 2016
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_0004637X_v825_n2_p_Larson
http://hdl.handle.net/20.500.12110/paper_0004637X_v825_n2_p_Larson
_version_ 1768542916645486592

Ejemplares similares