2018ApJ...861....7F -
Astrophys. J., 861, 7-7 (2018/July-1)
ALMA 26 arcmin2 survey of GOODS-S at one millimeter (ASAGAO): average morphology of high-z dusty star-forming galaxies in an exponential disk (n ≃ 1).
FUJIMOTO S., OUCHI M., KOHNO K., YAMAGUCHI Y., HATSUKADE B., UEDA Y., SHIBUYA T., INOUE S., OOGI T., TOFT S., GOMEZ-GUIJARRO C., WANG T., ESPADA D., NAGAO T., TANAKA I., AO Y., UMEHATA H., TANIGUCHI Y., NAKANISHI K., RUJOPAKARN W., IVISON R.J., WANG W.-H., LEE M.M., TADAKI K.-I., TAMURA Y. and DUNLOP J.S.
Abstract (from CDS):
We present morphological properties of dusty star-forming galaxies at z = 1-3 determined with the high-resolution (FWHM ∼ 0.''19) Atacama Large Milllimeter/submillimeter Array (ALMA) 1 mm map of our ASAGAO survey covering a 26 arcmin2 area in GOODS-S. In conjunction with the ALMA archival data, our sample consists of 45 ALMA sources with infrared luminosity (LIR) range of ∼1011-1013 L☉. To obtain an average rest-frame far-infrared (FIR) profile, we perform individual measurements and careful stacking of the ALMA sources using the uv-visibility method that includes positional-uncertainty and smoothing-effect evaluations through Monte Carlo simulations. We find that our sample has an average FIR-wavelength Sersic index and effective radius of nFIR = 1.2 ± 0.2 and Re,FIR = 1.0-1.3 kpc, respectively, additionally with a point-source component at the center, indicative of the existence of active galactic nuclei. The average FIR profile agrees with a morphology of an exponential disk clearly distinguished from a de Vaucouleurs spheroidal profile (Sersic index of 4). We also examine the rest-frame optical Sersic index nopt and effective radius Re,opt with deep Hubble Space Telescope (HST) images. Interestingly, we obtain nopt = 0.9 ± 0.3 (≃nFIR) and Re,opt = 3.2 ± 0.6 kpc (>Re,FIR), suggesting that the dusty disk-like structure is embedded within a larger stellar disk. The rest-frame UV and FIR data of HST and ALMA provide us with a radial profile of the total star formation rate (SFR), where the infrared SFR dominates over the UV SFR at the center. Under the assumption of a constant SFR, a compact stellar distribution in z ∼ 1-2 compact quiescent galaxies (cQGs) is well reproduced, while a spheroidal stellar morphology of cQGs (nopt = 4) is not, suggestive of other important mechanism(s) such as dynamical dissipation.
Abstract Copyright:
© 2018. The American Astronomical Society. All rights reserved.
Journal keyword(s):
galaxies: evolution - galaxies: formation - galaxies: high-redshift - galaxies: starburst - galaxies: star formation
Nomenclature:
Table 1: [FOK2018] NNN N=42 among (Nos 1-613).
Simbad objects:
53
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