TY - JOUR
T1 - Evolution of spatially resolved star formation main sequence and surface density profiles in massive disc galaxies at 0 ≲ z ≲ 1
T2 - Inside-out stellar mass buildup and quenching
AU - Abdurro'uf,
AU - Akiyama, Masayuki
N1 - Funding Information:
We thanks anonymous referee for his/her comments which improve our paper. We thanks Dr. Takahiro Morishita and Dr. Sandro Tac-chella for their useful comments. We thanks Dr. Sandro Tacchella for providing the radial profile of quenching time-scale of massive galaxies at z ∼ 2. Abdurro’uf acknowledges the support from Japanese Government (Ministry of Education, Culture, Sports, Science and Technology or MEXT) scholarship for his studies.
Funding Information:
We thanks anonymous referee for his/her comments which improve our paper. We thanks Dr. Takahiro Morishita and Dr. Sandro Tacchella for their useful comments. We thanks Dr. Sandro Tacchella for providing the radial profile of quenching time-scale of massive galaxies at z ~ 2. Abdurro'uf acknowledges the support from Japanese Government (Ministry of Education, Culture, Sports, Science and Technology or MEXT) scholarship for his studies. This work is based on observations taken by the 3D- HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Thiswork is based on observations made with theNASAGALEX. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. This work has made use of SDSS data. Funding for the SDSS IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High- Performance Computing at the University of Utah. The SDSS web site is www.sdss.org. SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de Astrof ísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Institut für Astrophysik Potsdam, Max-Planck-Institut für Astronomie (Heidelberg), Max-Planck-Institut für Astrophysik (MPA, Garching), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.
Funding Information:
This work is based on observations made with the NASA GALEX. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. This work has made use of SDSS data. Funding for the SDSS IV has been provided by the Alfred P. Sloan Foundation, the U.S. Department of Energy Office of Science, and the Participating Institutions. SDSS-IV acknowledges support and resources from the Center for High-Performance Computing at the University of Utah. The SDSS web site is www.sdss.org. SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS Collaboration including the Brazilian Participation Group, the Carnegie Institution for Science, Carnegie Mellon University, the Chilean Participation Group, the French Participation Group, Harvard-Smithsonian Center for Astrophysics, Instituto de As-trofísica de Canarias, The Johns Hopkins University, Kavli Institute for the Physics and Mathematics of the Universe (IPMU)/University of Tokyo, Lawrence Berkeley National Laboratory, Leibniz Insti-tut für Astrophysik Potsdam, Max-Planck-Institut für Astronomie (Heidelberg), Max-Planck-Institut für Astrophysik (MPA, Garch-ing), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatories of China, New Mexico State University, New York University, University of Notre Dame, Ob-servatário Nacional/MCTI, The Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universidad Nacional Autónoma de México, University of Arizona, University of Colorado Boulder, University of Oxford, University of Portsmouth, University of Utah, University of Virginia, University of Washington, University of Wisconsin, Vanderbilt University, and Yale University.
Funding Information:
This work is based on observations taken by the 3D-HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555.
Publisher Copyright:
© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2018/10/1
Y1 - 2018/10/1
N2 - We investigate a relation between surface densities of star formation rate (SFR) and stellar mass (M*) at a ~1 kpc scale namely spatially resolved star formation main sequence (SFMS) in massive (log (M*/M⊙) > 10.5) face-on disc galaxies at 0.01 < z < 0.02 and 0.8 < z < 1.8 and examine evolution of the relation. The spatially resolved SFMS of z ~ 0 galaxies is discussed in a companion paper. For z ~ 1 sample, we use eight bands imaging data set from Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey and 3D- HST and perform a pixel-to-pixel spectral energy distribution fitting to derive the spatially resolved SFR and M*. We find a linear spatially resolved SFMS in the z ~ 1 galaxies that lie on the global SFMS, while a 'flattening' at high Σ* end is found in that relation for the galaxies that lie below the global SFMS. Comparison with the spatially resolved SFMS of the z ~ 0 galaxies shows smaller difference in the specific SFR (sSFR) at low Σ* than that at high Σ*. This trend is consistent with the evolution of the sSFR(r) radial profile, which shows a faster decrease in the central region than in the outskirt, agrees with the inside-out quenching scenario.We then derive an empirical model for the evolution of the Σ*(r), ΣSFR(r), and sSFR(r) radial profiles. Based on the empirical model, we estimate the radial profile of the quenching time-scale and reproduce the observed spatially resolved SFMS at z ~ 1 and ~0.
AB - We investigate a relation between surface densities of star formation rate (SFR) and stellar mass (M*) at a ~1 kpc scale namely spatially resolved star formation main sequence (SFMS) in massive (log (M*/M⊙) > 10.5) face-on disc galaxies at 0.01 < z < 0.02 and 0.8 < z < 1.8 and examine evolution of the relation. The spatially resolved SFMS of z ~ 0 galaxies is discussed in a companion paper. For z ~ 1 sample, we use eight bands imaging data set from Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey and 3D- HST and perform a pixel-to-pixel spectral energy distribution fitting to derive the spatially resolved SFR and M*. We find a linear spatially resolved SFMS in the z ~ 1 galaxies that lie on the global SFMS, while a 'flattening' at high Σ* end is found in that relation for the galaxies that lie below the global SFMS. Comparison with the spatially resolved SFMS of the z ~ 0 galaxies shows smaller difference in the specific SFR (sSFR) at low Σ* than that at high Σ*. This trend is consistent with the evolution of the sSFR(r) radial profile, which shows a faster decrease in the central region than in the outskirt, agrees with the inside-out quenching scenario.We then derive an empirical model for the evolution of the Σ*(r), ΣSFR(r), and sSFR(r) radial profiles. Based on the empirical model, we estimate the radial profile of the quenching time-scale and reproduce the observed spatially resolved SFMS at z ~ 1 and ~0.
KW - Galaxies: evolution
KW - Galaxies: formation
KW - Galaxies: fundamental parameters
KW - Galaxies: spiral
KW - Galaxies: star formation
KW - Galaxies: structure
UR - http://www.scopus.com/inward/record.url?scp=85051453967&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85051453967&partnerID=8YFLogxK
U2 - 10.1093/mnras/sty1771
DO - 10.1093/mnras/sty1771
M3 - Article
AN - SCOPUS:85051453967
SN - 0035-8711
VL - 479
SP - 5083
EP - 5100
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -