A relation between the characteristic stellar ages of galaxies and their intrinsic shapes
Stellar population and stellar kinematic studies provide unique but complementary insights into how galaxies build-up their stellar mass and angular momentum1,2,3. A galaxy's mean stellar age reveals when stars were formed, but provides little constraint on how the galaxy's mass was assemb...
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ftanucanberra:oai:openresearch-repository.anu.edu.au:1885/205941 2024-01-14T10:10:21+01:00 A relation between the characteristic stellar ages of galaxies and their intrinsic shapes van de Sande, J. Scott, Nicholas Bland-Hawthorn, J. Brough, Sarah Bryant, J. J. Colless, Matthew Cortese, L. Croom, Scott M. D'Eugenio, Francesco Foster, Caroline Goodwin, Michael Konstantopoulos, I. S. Medling, Anne Sharp, Rob application/pdf http://hdl.handle.net/1885/205941 https://doi.org/10.1038/s41550-018-0436-x https://openresearch-repository.anu.edu.au/bitstream/1885/205941/3/jvds_sami_vsp_arxiv.pdf.jpg en_AU eng Nature Publishing Group http://purl.org/au-research/grants/arc/CE1101020 http://purl.org/au-research/grants/arc/CE170100013 http://purl.org/au-research/grants/arc/FL140100278 http://purl.org/au-research/grants/arc/FT140101166 http://purl.org/au-research/grants/arc/FT140100255 2397-3366 http://hdl.handle.net/1885/205941 doi:10.1038/s41550-018-0436-x https://openresearch-repository.anu.edu.au/bitstream/1885/205941/3/jvds_sami_vsp_arxiv.pdf.jpg © 2018 Macmillan Publishers Limited, part of Springer Nature. Nature Astronomy Journal article ftanucanberra https://doi.org/10.1038/s41550-018-0436-x 2023-12-15T09:33:46Z Stellar population and stellar kinematic studies provide unique but complementary insights into how galaxies build-up their stellar mass and angular momentum1,2,3. A galaxy's mean stellar age reveals when stars were formed, but provides little constraint on how the galaxy's mass was assembled. Resolved stellar dynamics4 trace the change in angular momentum due to mergers, but major mergers tend to obscure the effect of earlier interactions5. With the rise of large multi-object integral field spectroscopic surveys, such as SAMI6 and MaNGA7, and single-object integral field spectroscopic surveys (for example, ATLAS3D (ref. 8), CALIFA9, MASSIVE10), it is now feasible to connect a galaxy′s star formation and merger history on the same resolved physical scales, over a large range in galaxy mass, morphology and environment4,11,12. Using the SAMI Galaxy Survey, here we present a combined study of spatially resolved stellar kinematics and global stellar populations. We find a strong correlation of stellar population age with location in the (V/σ, ϵe) diagram that links the ratio of ordered rotation to random motions in a galaxy to its observed ellipticity. For the large majority of galaxies that are oblate rotating spheroids, we find that characteristic stellar age follows the intrinsic ellipticity of galaxies remarkably well. The SAMI Galaxy Survey is based on observations made at the Anglo-Australian Telescope. The Sydney–Australian Astronomical Observatory Multi-object Integral field spectrograph (SAMI) was developed jointly by the University of Sydney and the Australian Astronomical Observatory. 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. Parts of this research were conducted by the Australian Research Council Centre of Excellence for ... Article in Journal/Newspaper sami Australian National University: ANU Digital Collections Nature Astronomy 2 6 483 488 |
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Australian National University: ANU Digital Collections |
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ftanucanberra |
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English |
description |
Stellar population and stellar kinematic studies provide unique but complementary insights into how galaxies build-up their stellar mass and angular momentum1,2,3. A galaxy's mean stellar age reveals when stars were formed, but provides little constraint on how the galaxy's mass was assembled. Resolved stellar dynamics4 trace the change in angular momentum due to mergers, but major mergers tend to obscure the effect of earlier interactions5. With the rise of large multi-object integral field spectroscopic surveys, such as SAMI6 and MaNGA7, and single-object integral field spectroscopic surveys (for example, ATLAS3D (ref. 8), CALIFA9, MASSIVE10), it is now feasible to connect a galaxy′s star formation and merger history on the same resolved physical scales, over a large range in galaxy mass, morphology and environment4,11,12. Using the SAMI Galaxy Survey, here we present a combined study of spatially resolved stellar kinematics and global stellar populations. We find a strong correlation of stellar population age with location in the (V/σ, ϵe) diagram that links the ratio of ordered rotation to random motions in a galaxy to its observed ellipticity. For the large majority of galaxies that are oblate rotating spheroids, we find that characteristic stellar age follows the intrinsic ellipticity of galaxies remarkably well. The SAMI Galaxy Survey is based on observations made at the Anglo-Australian Telescope. The Sydney–Australian Astronomical Observatory Multi-object Integral field spectrograph (SAMI) was developed jointly by the University of Sydney and the Australian Astronomical Observatory. 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. Parts of this research were conducted by the Australian Research Council Centre of Excellence for ... |
format |
Article in Journal/Newspaper |
author |
van de Sande, J. Scott, Nicholas Bland-Hawthorn, J. Brough, Sarah Bryant, J. J. Colless, Matthew Cortese, L. Croom, Scott M. D'Eugenio, Francesco Foster, Caroline Goodwin, Michael Konstantopoulos, I. S. Medling, Anne Sharp, Rob |
spellingShingle |
van de Sande, J. Scott, Nicholas Bland-Hawthorn, J. Brough, Sarah Bryant, J. J. Colless, Matthew Cortese, L. Croom, Scott M. D'Eugenio, Francesco Foster, Caroline Goodwin, Michael Konstantopoulos, I. S. Medling, Anne Sharp, Rob A relation between the characteristic stellar ages of galaxies and their intrinsic shapes |
author_facet |
van de Sande, J. Scott, Nicholas Bland-Hawthorn, J. Brough, Sarah Bryant, J. J. Colless, Matthew Cortese, L. Croom, Scott M. D'Eugenio, Francesco Foster, Caroline Goodwin, Michael Konstantopoulos, I. S. Medling, Anne Sharp, Rob |
author_sort |
van de Sande, J. |
title |
A relation between the characteristic stellar ages of galaxies and their intrinsic shapes |
title_short |
A relation between the characteristic stellar ages of galaxies and their intrinsic shapes |
title_full |
A relation between the characteristic stellar ages of galaxies and their intrinsic shapes |
title_fullStr |
A relation between the characteristic stellar ages of galaxies and their intrinsic shapes |
title_full_unstemmed |
A relation between the characteristic stellar ages of galaxies and their intrinsic shapes |
title_sort |
relation between the characteristic stellar ages of galaxies and their intrinsic shapes |
publisher |
Nature Publishing Group |
url |
http://hdl.handle.net/1885/205941 https://doi.org/10.1038/s41550-018-0436-x https://openresearch-repository.anu.edu.au/bitstream/1885/205941/3/jvds_sami_vsp_arxiv.pdf.jpg |
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sami |
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Nature Astronomy |
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http://purl.org/au-research/grants/arc/CE1101020 http://purl.org/au-research/grants/arc/CE170100013 http://purl.org/au-research/grants/arc/FL140100278 http://purl.org/au-research/grants/arc/FT140101166 http://purl.org/au-research/grants/arc/FT140100255 2397-3366 http://hdl.handle.net/1885/205941 doi:10.1038/s41550-018-0436-x https://openresearch-repository.anu.edu.au/bitstream/1885/205941/3/jvds_sami_vsp_arxiv.pdf.jpg |
op_rights |
© 2018 Macmillan Publishers Limited, part of Springer Nature. |
op_doi |
https://doi.org/10.1038/s41550-018-0436-x |
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Nature Astronomy |
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2 |
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6 |
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483 |
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488 |
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