TY - JOUR
T1 - First ranked galaxies of non-elliptical morphology
AU - Li, Yen Ting
AU - Chen, Lin Wen
N1 - Funding Information:
We thank the referee for providing substantial and detailed suggestions on our work, and for pointing out that our sample should use FRG as a more suitable name to represent the correct target in which we are interested. Y-TL thanks E. Tempel for a helpful discussion on the error estimate of the cluster total mass. He also thanks Yen-Ting Lin, Li-Hwai Lin and Tzi-hong Chiueh for suggestions to improve the quality of the paper. Funding for the SDSS IV has been provided by the Alfred P. Sloan Foundation, the US 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 IV 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, In-stituto de Astrofísica de Canarias, 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 (AIP), Max-Planck-Institut für Astronomie (MPIA Heidelberg), Max-Planck-Institut für Astrophysik (MPA Garching), Max-Planck-Institut für Extrater-restrische Physik (MPE), National Astronomical Observatory of China, New Mexico State University, New York University, University of Notre Dame, Observatário Nacional/MCTI, Ohio State University, Pennsylvania State University, Shanghai Astronomical Observatory, United Kingdom Participation Group, Universi-dad 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.
Publisher Copyright:
© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2019/1/21
Y1 - 2019/1/21
N2 - In the local Universe, the major morphology for first ranked galaxies (FRGs) is elliptical. However, FRGs might not be limited to elliptical or central dominant galaxies. We select galaxies from galaxy group/cluster catalogues based on the Sloan Digital Sky Survey Data Release 10, and we find that more than 35 per cent of FRG morphologies are classified as unclear or even spiral. Spiral FRGs (spFRGs) have several distinctive features. The stellar mass of spFRGs is as massive as the majority of elliptical galaxies and their luminosity is between the elliptical FRGs (elFRGs) and their elliptical member galaxies. There are also non-negligible differences in star formation rate and colour between (both field and member) spirals and spFRGs, and spFRGs show a relatively young formation age compared to elFRGs. In comparison to elFRG hosts, spFRG hosts are poorer and less massive, and spFRGs have large offsets from the luminosity-weighted group/cluster centre. spFRG also has large seperaration between spFRGs and the closest members with r-band absolute magnitude is ≤−19 (mag + 5 log10h). From the analysis, we propose a possible formation scenario for spFRGs. The galaxy number density around spFRGs and the mass ratio between spFRGs and their closest members rule out the possibility of a formation scenario from the galaxy-galaxy minor interaction. This implies that a galaxy has the potential to become the brightest group galaxy or a low-mass brightest cluster galaxy without galaxy-galaxy interactions but instead growing mass by gentle processes. We suggest that the halo cold gas accretion mechanism is plausible for spFRGs to assemble their mass.
AB - In the local Universe, the major morphology for first ranked galaxies (FRGs) is elliptical. However, FRGs might not be limited to elliptical or central dominant galaxies. We select galaxies from galaxy group/cluster catalogues based on the Sloan Digital Sky Survey Data Release 10, and we find that more than 35 per cent of FRG morphologies are classified as unclear or even spiral. Spiral FRGs (spFRGs) have several distinctive features. The stellar mass of spFRGs is as massive as the majority of elliptical galaxies and their luminosity is between the elliptical FRGs (elFRGs) and their elliptical member galaxies. There are also non-negligible differences in star formation rate and colour between (both field and member) spirals and spFRGs, and spFRGs show a relatively young formation age compared to elFRGs. In comparison to elFRG hosts, spFRG hosts are poorer and less massive, and spFRGs have large offsets from the luminosity-weighted group/cluster centre. spFRG also has large seperaration between spFRGs and the closest members with r-band absolute magnitude is ≤−19 (mag + 5 log10h). From the analysis, we propose a possible formation scenario for spFRGs. The galaxy number density around spFRGs and the mass ratio between spFRGs and their closest members rule out the possibility of a formation scenario from the galaxy-galaxy minor interaction. This implies that a galaxy has the potential to become the brightest group galaxy or a low-mass brightest cluster galaxy without galaxy-galaxy interactions but instead growing mass by gentle processes. We suggest that the halo cold gas accretion mechanism is plausible for spFRGs to assemble their mass.
KW - Galaxies: clusters: general
KW - Galaxies: elliptical and lenticular, cD
KW - Galaxies: evolution
KW - Galaxies: groups: general
KW - Galaxies: kinematics and dynamics
KW - Galaxies: spiral
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U2 - 10.1093/mnras/sty2408
DO - 10.1093/mnras/sty2408
M3 - Article
AN - SCOPUS:85066929474
SN - 0035-8711
VL - 482
SP - 4084
EP - 4095
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -