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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 421523.0, MPI für Astronomie / Publikationen_mpia
IMAGES. II. A surprisingly low fraction of undisturbed rotating spiral disks at z ~ 0.6 The morpho-kinematical relation 6 Gyr ago
Authors:Neichel, B.; Hammer, F.; Puech, M.; Flores, H.; Lehnert, M.; Rawat, A.; Yang, Y.; Delgado, R.; Amram, P.; Balkowski, C.; Cesarsky, C.; Dannerbauer, H.; Fuentes-Carrera, I.; Guiderdoni, B.; Kembhavi, A.; Liang, Y. C.; Nesvadba, N.; Östlin, G.; Pozzetti, L.; Ravikumar, C. D.; di Serego Alighieri, S.; Vergani, D.; Vernet, J.; Wozniak, H.
Date of Publication (YYYY-MM-DD):2008
Title of Journal:Astronomy and Astrophysics
Start Page:159
End Page:172
Review Status:Peer-review
Audience:Experts Only
Abstract / Description:We present a first combined analysis of the morphological and dynamical properties for the intermediate-mass Galaxy Evolution Sequence (IMAGES) sample. It is a representative sample of 52 zËœ0.6 galaxies with M_stell from 1.5 to 15 × 1010~Mo that possesses 3D resolved kinematics and HST deep imaging in at least two broad band filters. We aim at evaluating the evolution of rotating spirals robustly since zËœ 0.6, as well as at testing the different schemes for classifying galaxies morphologically. We used all the information provided by multi-band images, color maps, and 2D light fitting to assign a morphological class to each object. We divided our sample into spiral disks, peculiar objects, compact objects, and mergers. Using our morphological classification scheme, 4/5 of the identified spirals are rotating disks, and more than 4/5 of identified peculiar galaxies show complex kinematics, while automatic classification methods such as concentration-asymmetry and GINI-M20 severely overestimate the fraction of relaxed disk galaxies. Using this methodology, we find that the fraction of undisturbed rotating spirals has increased by a factor ~2 during the past 6 Gyr, a much higher fraction than was found previously based on morphologies alone. These rotating spiral disks are forming stars very rapidly, even doubling their stellar masses over the past 6 Gyr, while most of their stars were formed a few Gyr earlier, which reveals a large gas supply. Because they are the likely progenitors of local spirals, we can conjecture how their properties are evolving. Their disks show some evidence of inside-out growth, and the gas supply/accretion is not random since the disk needs to be stable in order to match the local disk properties. Intermediate-mass Galaxy Evolution Sequence. Table 4 and Fig. 12 are only available in electronic form at
Free Keywords:galaxies: formation; galaxies: evolution; galaxies: kinematics and dynamics; galaxies: fundametal parameters
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL: [ID No:1]
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