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Giant H II Regions in the Merging System NGC 3256: Are they the birthplaces of globular clusters?

English, Jayanne; Freeman, Kenneth

Description

CCD images and spectra of ionized hydrogen in the merging system NGC 3256 were acquired as part of a kinematic study to investigate the formation of globular clusters (GCs) during the interactions and mergers of disk galaxies. This paper focuses on the proposition by Kennicutt & Chu that giant H II regions (GHRs), with an Ha luminosity greater than 1.5 × 1040 ergs s-1, are birthplaces of young populous clusters (YPCs). Although, compared with some other interacting systems, NGC 3256 has...[Show more]

dc.contributor.authorEnglish, Jayanne
dc.contributor.authorFreeman, Kenneth
dc.date.accessioned2015-12-13T23:09:19Z
dc.identifier.issn0004-6256
dc.identifier.urihttp://hdl.handle.net/1885/86944
dc.description.abstractCCD images and spectra of ionized hydrogen in the merging system NGC 3256 were acquired as part of a kinematic study to investigate the formation of globular clusters (GCs) during the interactions and mergers of disk galaxies. This paper focuses on the proposition by Kennicutt & Chu that giant H II regions (GHRs), with an Ha luminosity greater than 1.5 × 1040 ergs s-1, are birthplaces of young populous clusters (YPCs). Although, compared with some other interacting systems, NGC 3256 has relatively few (seven) giant H II complexes, these regions are comparable in total flux to about 85 30 Doradus-like giant H II regions (GHRs). The bluest, massive YPCs (Zepf et al.) are located in the vicinity of observed 30 Dor GHRs, contributing to the notion that some fraction of 30 Dor GHRs do cradle massive YPCs, as 30 Dor harbors R136. If interactions induce the formation of 30 Dor GHRs, the observed luminosities indicate that almost 900 30 Dor GHRs would form in NGC 3256 throughout its merger epoch. In order for 30 Dor GHRs to be considered GC progenitors, this number must be consistent with the specific frequencies of globular clusters estimated for elliptical galaxies formed via mergers of spirals (Ashman & Zepf). This only requires that about 10% of NGC 3256's 900 30 Dor GHRs harbor YPCs, which survive several gigayears and have masses ≥MR136.
dc.publisherUniversity of Chicago Press
dc.sourceAstronomical Journal
dc.subjectKeywords: Galaxies: individual (NGC 3256); Galaxies: interactions; Globular clusters: general
dc.titleGiant H II Regions in the Merging System NGC 3256: Are they the birthplaces of globular clusters?
dc.typeJournal article
local.description.notesImported from ARIES
local.description.refereedYes
local.identifier.citationvolume125
dc.date.issued2003
local.identifier.absfor020110 - Stellar Astronomy and Planetary Systems
local.identifier.ariespublicationMigratedxPub16014
local.type.statusPublished Version
local.contributor.affiliationEnglish, Jayanne, College of Physical and Mathematical Sciences, ANU
local.contributor.affiliationFreeman, Kenneth, College of Physical and Mathematical Sciences, ANU
local.description.embargo2037-12-31
local.bibliographicCitation.startpage1124
local.bibliographicCitation.lastpage1133
local.identifier.doi10.1086/367915
dc.date.updated2015-12-12T08:18:36Z
local.identifier.scopusID2-s2.0-0242624497
CollectionsANU Research Publications

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