2003/02/11 by Jayanne English, K. C. Freeman, Ken C. Freeman · 1 citation
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Galaxies: Formation, Evolution, Phenomena #Galaxy #Globular cluster #Physics #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/367915
Jpeg images; colour images are meant to only appear on monitors, not printout. 19 pages, 3 figures, and 3 tables. To be published in Astronomical Journal Mar. 2003
arxiv created 2003/02/11 · openalex publication_date 2003/03/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
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 Hα luminosity greater than 1.5 × 10 40 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 ≥ M R136 .