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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 276800.0, MPI für Astronomie / Publikationen_mpia
HST/WFPC2 morphologies and bar structures of field galaxies at 0.4 < z < 1
Authors:Zheng, X. Z.; Hammer, F.; Flores, H.; Assémat, F.; Rawat, A.
Date of Publication (YYYY-MM-DD):2005
Title of Journal:Astronomy and Astrophysics
Journal Abbrev.:Astronomy and Astrophysics
Start Page:507
End Page:519
Review Status:Peer-review
Audience:Not Specified
Abstract / Description:To address how the galaxy Hubble sequence is established and what physical processes are involved, we studied morphological properties and internal structures of field galaxies in the past (0.4<z<1). In addition to structural parameters derived from bulge+disk decomposition, Zheng et al. (2004, A&A, 421, 847) introduced color maps in recognizing galaxies and properly classified morphologies of 36 luminous infrared galaxies (LIRGs, L_IR(8{-}1000 mum) &geq; 1011 L_â_™). Here we presented morphological classification of a parallel 75 non-LIRG sample. Our examination revealed that a significant fraction of the galaxies shows remarkable morphological evolution, most likely related to the present-day spiral galaxies. Comparison of the morphological properties between LIRGs and non-LIRGs shows that the LIRGs contain a higher fraction of ongoing major mergers and systems with signs of merging/interaction. This suggests that the merging process is one of the major mechanisms to trigger star formation. We found that spiral LIRGs probably host much fewer bars than spiral non-LIRGs, suggesting that a bar is not efficient in triggering violent star formation. Differing from Abraham et al. (1999, MNRAS, 308, 569), no dramatic change of the bar frequency is detected up to redshift z~0.8. The bar frequency of the distant spirals is similar to (and may be higher than) the present-day spirals in the rest-frame B band. We conclude that bar-driven secular evolution is not a major mechanism to drive morphological evolution of field galaxies, especially their bulge formation, which is more likely related to multiple intense star formation episodes during which the galaxies appear as LIRGs (Hammer et al. 2005, A&A, 430, 115).
Free Keywords:galaxies: formation; galaxies: evolution; galaxies: structure
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/cgi-bin/nph- bib_query?b... [ID No:1]
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