Structural Evolution in Massive Galaxies at z similar to 2

Tadaki, Ken-ichi; Belli, Sirio; Burkert, Andreas; Dekel, Avishai; Foerster Schreiber, Natascha M.; Genzel, Reinhard; Hayashi, Masao; Herrera-Camus, Rodrigo; Kodama, Tadayuki; Kohno, Kotaro; Koyama, Yusei; Lee, Minju M.; Lutz, Dieter; Mowla, Lamiya; Nelson, Erica J.; Renzini, Alvio; Suzuki, Tomoko L.; Tacconi, Linda J.; Uebler, Hannah; Wisnioski, Emily und Wuyts, Stijn (2020): Structural Evolution in Massive Galaxies at z similar to 2. In: Astrophysical Journal, Bd. 901, Nr. 1, 74

Abstract

We present 0.'' 2 resolution Atacama Large Millimeter/submillimeter Array (ALMA) observations at 870 mu m in a stellar mass-selected sample of 85 massive (M-* > 10(11)M(circle dot)) star-forming galaxies (SFGs) at z = 1.9-2.6 in the CANDELS/3D-Hubble Space Telescope fields of UDS and GOODS-S. We measure the effective radius of the rest-frame far-infrared (FIR) emission for 62 massive SFGs. They are distributed over wide ranges of FIR size from R-e,R-FIR = 0.4 kpc to R-e,R-FIR = 6 kpc. The effective radius of the FIR emission is smaller by a factor of 2.3(-1.0)(+1.9) than the effective radius of the optical emission and is smaller by a factor of 1.9(-1.0)(+1.9) than the half-mass radius. Taking into account potential extended components, the FIR size would change only by similar to 10%. By combining the spatial distributions of the FIR and optical emission, we investigate how galaxies change the effective radius of the optical emission and the stellar mass within a radius of 1 kpc, M-1kpc. The compact starburst puts most of the massive SFGs on the mass-size relation for quiescent galaxies (QGs) at z similar to 2 within 300 Myr if the current star formation activity and its spatial distribution are maintained. We also find that within 300 Myr, similar to 38% of massive SFGs can reach the central mass of M-1kpc = 10(10.5) M-circle dot, which is around the boundary between massive SFGs and QGs. These results suggest an outside-in transformation scenario in which a dense core is formed at the center of a more extended disk, likely via dissipative in-disk inflows. Synchronized observations at ALMA 870 mu m and James Webb Space Telescope 3-4 mu m will explicitly verify this scenario.

• Dokumententyp: Zeitschriftenartikel
• Fakultät: Physik
• Themengebiete: 500 Naturwissenschaften und Mathematik > 530 Physik
• ISSN: 0004-637X
• Sprache: Englisch