TY - JOUR
T1 - Different higher order kinematics between star-forming and quiescent galaxies based on the SAMI, MAGPI, and LEGA-C surveys
AU - D'eugenio, Francesco
AU - Van Der Wel, Arjen
AU - Derkenne, Caro
AU - Van Houdt, Josha
AU - Bezanson, Rachel
AU - Taylor, Edward N.
AU - Van De Sande, Jesse
AU - Baker, William M.
AU - Bell, Eric F.
AU - Bland-Hawthorn, Joss
AU - Bluck, Asa F.L.
AU - Brough, Sarah
AU - Bryant, Julia J.
AU - Colless, Matthew
AU - Cortese, Luca
AU - Croom, Scott M.
AU - Van Dokkum, Pieter
AU - Fisher, Deanne
AU - Foster, Caroline
AU - Fraser-Mckelvie, Amelia
AU - Gallazzi, Anna
AU - De Graaff, Anna
AU - Groves, Brent
AU - Del P. Lagos, Claudia
AU - Looser, Tobias J.
AU - Maiolino, Roberto
AU - Maseda, Michael
AU - Mendel, J. Trevor
AU - Nersesian, Angelos
AU - Pacifici, Camilla
AU - Piotrowska, Joanna M.
AU - Poci, Adriano
AU - Remus, Rhea Silvia
AU - Sharma, Gauri
AU - Sweet, Sarah M.
AU - Thater, Sabine
AU - Tran, Kim Vy
AU - Übler, Hannah
AU - Valenzuela, Lucas M.
AU - Wisnioski, Emily
AU - Zibetti, Stefano
N1 - Funding Information:
The Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation Grant No. AST-1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation.
Funding Information:
Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/ .
Funding Information:
GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT, and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http://www.gama-survey.org/ .
Funding Information:
We thank the anonymous referee for insightful comments that greatly improved this article. FDE and AvdW acknowledge funding through the H2020 ERC Consolidator Grant 683184. FDE and RM ackwoledge funding through the ERC Advanced grant 695671 ‘QUENCH’ and support by the Science and Technology Facilities Council (STFC). JvdS acknowledges support of an Australian Research Council Discovery Early Career Research Award (project number DE200100461) funded by the Australian Government. SB acknowledges funding support from the Australian Research Council through a Future Fellowship (FT140101166) ORCID 0000-0002-9796-1363. JJB acknowledges support of an Australian Research Council Future Fellowship (FT180100231). CF is the recipient of an Australian Research Council Future Fellowship (project number FT210100168) funded by the Australian Government. HÜ gratefully acknowledges support by the Isaac Newton Trust and by the Kavli Foundation through a Newton-Kavli Junior Fellowship. LMV acknowledges support by the COMPLEX project from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program grant agreement ERC-2019-AdG 882679.
Funding Information:
The SAMI Galaxy Survey is based on observations made at the Anglo-Australian Telescope. The Sydney-AAO Multi-object Integral-field spectrograph (SAMI) was developed jointly by the University of Sydney and the Australian Astronomical Observatory, and funded by ARC grants FF0776384 (Bland-Hawthorn) and LE130100198. The SAMI input catalogue is based on data taken from the Sloan Digital Sky Survey, the GAMA Survey, and the VST ATLAS Survey. The SAMI Galaxy Survey is funded by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020, and other participating institutions. The SAMI Galaxy Survey website is http://sami-survey.org/ .
Publisher Copyright:
© 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
PY - 2023/10/1
Y1 - 2023/10/1
N2 - We present the first statistical study of spatially integrated non-Gaussian stellar kinematics spanning 7 Gyr in cosmic time. We use deep, rest-frame optical spectroscopy of massive galaxies (stellar mass) at redshifts z = 0.05, 0.3, and 0.8 from the SAMI, MAGPI, and LEGA-C surveys, to measure the excess kurtosis h4 of the stellar velocity distribution, the latter parametrized as a Gauss-Hermite series. We find that at all redshifts where we have large enough samples, h4 anticorrelates with the ratio between rotation and dispersion, highlighting the physical connection between these two kinematic observables. In addition, and independently from the anticorrelation with rotation-to-dispersion ratio, we also find a correlation between h4 and M, potentially connected to the assembly history of galaxies. In contrast, after controlling for mass, we find no evidence of independent correlation between h4 and aperture velocity dispersion or galaxy size. These results hold for both star-forming and quiescent galaxies. For quiescent galaxies, h4 also correlates with projected shape, even after controlling for the rotation-to-dispersion ratio. At any given redshift, star-forming galaxies have lower h4 compared to quiescent galaxies, highlighting the link between kinematic structure and star-forming activity.
AB - We present the first statistical study of spatially integrated non-Gaussian stellar kinematics spanning 7 Gyr in cosmic time. We use deep, rest-frame optical spectroscopy of massive galaxies (stellar mass) at redshifts z = 0.05, 0.3, and 0.8 from the SAMI, MAGPI, and LEGA-C surveys, to measure the excess kurtosis h4 of the stellar velocity distribution, the latter parametrized as a Gauss-Hermite series. We find that at all redshifts where we have large enough samples, h4 anticorrelates with the ratio between rotation and dispersion, highlighting the physical connection between these two kinematic observables. In addition, and independently from the anticorrelation with rotation-to-dispersion ratio, we also find a correlation between h4 and M, potentially connected to the assembly history of galaxies. In contrast, after controlling for mass, we find no evidence of independent correlation between h4 and aperture velocity dispersion or galaxy size. These results hold for both star-forming and quiescent galaxies. For quiescent galaxies, h4 also correlates with projected shape, even after controlling for the rotation-to-dispersion ratio. At any given redshift, star-forming galaxies have lower h4 compared to quiescent galaxies, highlighting the link between kinematic structure and star-forming activity.
KW - galaxies: elliptical and lenticular, cD
KW - galaxies: evolution
KW - galaxies: formation
KW - galaxies: fundamental parameters
KW - galaxies: structure
UR - http://www.scopus.com/inward/record.url?scp=85172904155&partnerID=8YFLogxK
U2 - 10.1093/mnras/stac3536
DO - 10.1093/mnras/stac3536
M3 - Article
AN - SCOPUS:85172904155
SN - 0035-8711
VL - 525
SP - 2765
EP - 2788
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -