Shaping massive galaxies: their morphology and kinematics at z = 1-3

Details Shaping massive galaxies: their morphology and kinematics at z = 1-3 Shaping massive galaxies: their morphology and kinematics at z = 1-3

Nov 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011hsa6.conf..154b&link_type=abstract

Highlights of Spanish Astrophysics VI, Proceedings of the IX Scientific Meeting of the Spanish Astronomical Society (SEA), held

Astronomy and Astrophysics

Astrophysics

Scientific paper

Massive (M_* ≥ 10^{11} M_&sun;) galaxies at high redshift (z ≥ 1.5) remain mysterious objects. Their extremely small sizes (effective radii of 1-2 kpc) make them as dense as modern globular clusters. It is thought that a highly dissipational merger is needed to create such compact galaxies. Within this proceedings, we discuss this issue, along with state-of-the-art morphological and kinematic observations of these objects. In the present day Universe massive galaxies contain large sizes, and harbour old and metal-rich stellar populations. In order to explore their development, we present near-IR IFU observations with SINFONI@VLT for ten massive galaxies at z ˜ 1.4 solely selected by their high stellar mass which allows us to retrieve velocity dispersions, kinematic maps and dynamical masses. We combine this with data from the GOODS NICMOS Survey, the largest sample of massive galaxies (80 objects) with high-resolution imaging at high redshift (1.7 < z < 3) acquired to date. As a result, we show how massive galaxy morphology changes possibly result through elusive minor merging.

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