The SAMI galaxy survey: Mass-kinematics scaling relations

Dilyar Barat; Francesco D'Eugenio; Matthew Colless; Sarah Brough; Barbara Catinella; Luca Cortese; Scott M. Croom; Anne M. Medling; Sree Oh; Jesse Van De Sande; Sarah M. Sweet; Sukyoung K. Yi; Joss Bland-Hawthorn; Julia Bryant; Michael Goodwin; Brent Groves; Jon Lawrence; Matt S. Owers; Samuel N. Richards; Nicholas Scott

doi:10.1093/mnras/stz1439

The SAMI galaxy survey: Mass-kinematics scaling relations

Dilyar Barat, Francesco D'Eugenio, Matthew Colless, Sarah Brough, Barbara Catinella, Luca Cortese, Scott M. Croom, Anne M. Medling, Sree Oh, Jesse Van De Sande, Sarah M. Sweet, Sukyoung K. Yi, Joss Bland-Hawthorn, Julia Bryant, Michael Goodwin, Brent Groves, Jon Lawrence, Matt S. Owers, Samuel N. Richards, Nicholas Scott

Research output: Contribution to journal › Review article › peer-review

18 Citations (Scopus)

Abstract

We use data from the Sydney-AAO Multi-object Integral-field spectroscopy (SAMI) Galaxy Survey to study the dynamical scaling relation between galaxy stellar mass M_∗ and the general kinematic parameter S_K = √KV²_rot + σ² that combines rotation velocity Vrot and velocity dispersion σ. We show that the logM_∗ - logSK relation: (1) is linear above limits set by properties of the samples and observations; (2) has slightly different slope when derived from stellar or gas kinematic measurements; (3) applies to both early-type and late-type galaxies and has smaller scatter than either the Tully.Fisher relation (logM_∗ - log V_rot) for late types or the Faber.Jackson relation (logM_∗ - log σ) for early types; and (4) has scatter that is only weakly sensitive to the value of K, with minimum scatter for K in the range 0.4 and 0.7. We compare SK to the aperture second moment (the 'aperture velocity dispersion') measured from the integrated spectrum within a 3-arcsecond radius aperture (σ_3″ ). We find that while SK and σ_3″ are in general tightly correlated, the logM_∗ - log SK relation has less scatter than the logM_∗ - log σ_3″ relation.

Original language	English
Pages (from-to)	2924-2936
Number of pages	13
Journal	Monthly Notices of the Royal Astronomical Society
Volume	487
Issue number	2
DOIs	https://doi.org/10.1093/mnras/stz1439
Publication status	Published - 2019 Aug 1

Bibliographical note

Funding Information:
DB is supported by an Australia Government Research Training Program Scholarship and ASTRO 3D. FDE acknowledges funding through the H2020 ERC Consolidator Grant 683184. JBH is supported by an ARC Laureate Fellowship that funds JvdS and an ARC Federation Fellowship that funded the SAMI prototype. JJB acknowledges support of an Australian Research Council Future Fellowship (FT180100231). JvdS is funded under Bland-Hawthorn’s ARC Laureate Fellowship (FL140100278). NS acknowledges support of a University of Sydney Postdoctoral Research Fellowship. Parts of this research were conducted by ASTRO 3D, through project number CE170100013. LC is the recipient of an Australian Research Council Future Fellowship (FT180100066) funded by the Australian Government. SB acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140101166). SMC acknowledges the support of an Australian Research Council Future Fellowship (FT100100457). BG is the recipient of an Australian Research Council Future Fellowship (FT140101202). MSO acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140100255). Support for AMM is provided by NASA through Hubble Fellowship grant #HST-HF2-51377 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. SKY acknowledges support from the Korean National Research Foundation (2017R1A2A1A05001116) and by the Yonsei University Future Leading Research Initiative (2015-22-0064). This study was performed under the umbrella of the joint collaboration between Yonsei University Observatory and the Korean Astronomy and Space Science Institute.

Funding Information:
We thank the referee for their constructive report. 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. The SAMI input catalogue is based on data taken from the Sloan Digital Sky Survey, the Galaxy And Mass Assembly (GAMA) Survey and the VLT Survey Telescope (VST) ATLAS Survey. The SAMI Galaxy Survey is supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (AS-TRO 3D), through project number CE170100013, 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 sami-survey.org.

Publisher Copyright:
© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

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10.1093/mnras/stz1439

Cite this

Barat, D., D'Eugenio, F., Colless, M., Brough, S., Catinella, B., Cortese, L., Croom, S. M., Medling, A. M., Oh, S., Van De Sande, J., Sweet, S. M., Yi, S. K., Bland-Hawthorn, J., Bryant, J., Goodwin, M., Groves, B., Lawrence, J., Owers, M. S., Richards, S. N., & Scott, N. (2019). The SAMI galaxy survey: Mass-kinematics scaling relations. Monthly Notices of the Royal Astronomical Society, 487(2), 2924-2936. https://doi.org/10.1093/mnras/stz1439

@article{36084f770b574c9f8ca68c4ec106a9d2,

title = "The SAMI galaxy survey: Mass-kinematics scaling relations",

abstract = "We use data from the Sydney-AAO Multi-object Integral-field spectroscopy (SAMI) Galaxy Survey to study the dynamical scaling relation between galaxy stellar mass M∗ and the general kinematic parameter SK = √KV2rot + σ2 that combines rotation velocity Vrot and velocity dispersion σ. We show that the logM∗ - logSK relation: (1) is linear above limits set by properties of the samples and observations; (2) has slightly different slope when derived from stellar or gas kinematic measurements; (3) applies to both early-type and late-type galaxies and has smaller scatter than either the Tully.Fisher relation (logM∗ - log Vrot) for late types or the Faber.Jackson relation (logM∗ - log σ) for early types; and (4) has scatter that is only weakly sensitive to the value of K, with minimum scatter for K in the range 0.4 and 0.7. We compare SK to the aperture second moment (the 'aperture velocity dispersion') measured from the integrated spectrum within a 3-arcsecond radius aperture (σ3″ ). We find that while SK and σ3″ are in general tightly correlated, the logM∗ - log SK relation has less scatter than the logM∗ - log σ3″ relation.",

author = "Dilyar Barat and Francesco D'Eugenio and Matthew Colless and Sarah Brough and Barbara Catinella and Luca Cortese and Croom, {Scott M.} and Medling, {Anne M.} and Sree Oh and {Van De Sande}, Jesse and Sweet, {Sarah M.} and Yi, {Sukyoung K.} and Joss Bland-Hawthorn and Julia Bryant and Michael Goodwin and Brent Groves and Jon Lawrence and Owers, {Matt S.} and Richards, {Samuel N.} and Nicholas Scott",

note = "Funding Information: DB is supported by an Australia Government Research Training Program Scholarship and ASTRO 3D. FDE acknowledges funding through the H2020 ERC Consolidator Grant 683184. JBH is supported by an ARC Laureate Fellowship that funds JvdS and an ARC Federation Fellowship that funded the SAMI prototype. JJB acknowledges support of an Australian Research Council Future Fellowship (FT180100231). JvdS is funded under Bland-Hawthorn{\textquoteright}s ARC Laureate Fellowship (FL140100278). NS acknowledges support of a University of Sydney Postdoctoral Research Fellowship. Parts of this research were conducted by ASTRO 3D, through project number CE170100013. LC is the recipient of an Australian Research Council Future Fellowship (FT180100066) funded by the Australian Government. SB acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140101166). SMC acknowledges the support of an Australian Research Council Future Fellowship (FT100100457). BG is the recipient of an Australian Research Council Future Fellowship (FT140101202). MSO acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140100255). Support for AMM is provided by NASA through Hubble Fellowship grant #HST-HF2-51377 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. SKY acknowledges support from the Korean National Research Foundation (2017R1A2A1A05001116) and by the Yonsei University Future Leading Research Initiative (2015-22-0064). This study was performed under the umbrella of the joint collaboration between Yonsei University Observatory and the Korean Astronomy and Space Science Institute. Funding Information: We thank the referee for their constructive report. 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. The SAMI input catalogue is based on data taken from the Sloan Digital Sky Survey, the Galaxy And Mass Assembly (GAMA) Survey and the VLT Survey Telescope (VST) ATLAS Survey. The SAMI Galaxy Survey is supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (AS-TRO 3D), through project number CE170100013, 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 sami-survey.org. Publisher Copyright: {\textcopyright} 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.",

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doi = "10.1093/mnras/stz1439",

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Barat, D, D'Eugenio, F, Colless, M, Brough, S, Catinella, B, Cortese, L, Croom, SM, Medling, AM, Oh, S, Van De Sande, J, Sweet, SM, Yi, SK, Bland-Hawthorn, J, Bryant, J, Goodwin, M, Groves, B, Lawrence, J, Owers, MS, Richards, SN & Scott, N 2019, 'The SAMI galaxy survey: Mass-kinematics scaling relations', Monthly Notices of the Royal Astronomical Society, vol. 487, no. 2, pp. 2924-2936. https://doi.org/10.1093/mnras/stz1439

TY - JOUR

T1 - The SAMI galaxy survey

T2 - Mass-kinematics scaling relations

AU - Barat, Dilyar

AU - D'Eugenio, Francesco

AU - Colless, Matthew

AU - Brough, Sarah

AU - Catinella, Barbara

AU - Cortese, Luca

AU - Croom, Scott M.

AU - Medling, Anne M.

AU - Oh, Sree

AU - Van De Sande, Jesse

AU - Sweet, Sarah M.

AU - Yi, Sukyoung K.

AU - Bland-Hawthorn, Joss

AU - Bryant, Julia

AU - Goodwin, Michael

AU - Groves, Brent

AU - Lawrence, Jon

AU - Owers, Matt S.

AU - Richards, Samuel N.

AU - Scott, Nicholas

N1 - Funding Information: DB is supported by an Australia Government Research Training Program Scholarship and ASTRO 3D. FDE acknowledges funding through the H2020 ERC Consolidator Grant 683184. JBH is supported by an ARC Laureate Fellowship that funds JvdS and an ARC Federation Fellowship that funded the SAMI prototype. JJB acknowledges support of an Australian Research Council Future Fellowship (FT180100231). JvdS is funded under Bland-Hawthorn’s ARC Laureate Fellowship (FL140100278). NS acknowledges support of a University of Sydney Postdoctoral Research Fellowship. Parts of this research were conducted by ASTRO 3D, through project number CE170100013. LC is the recipient of an Australian Research Council Future Fellowship (FT180100066) funded by the Australian Government. SB acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140101166). SMC acknowledges the support of an Australian Research Council Future Fellowship (FT100100457). BG is the recipient of an Australian Research Council Future Fellowship (FT140101202). MSO acknowledges the funding support from the Australian Research Council through a Future Fellowship (FT140100255). Support for AMM is provided by NASA through Hubble Fellowship grant #HST-HF2-51377 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. SKY acknowledges support from the Korean National Research Foundation (2017R1A2A1A05001116) and by the Yonsei University Future Leading Research Initiative (2015-22-0064). This study was performed under the umbrella of the joint collaboration between Yonsei University Observatory and the Korean Astronomy and Space Science Institute. Funding Information: We thank the referee for their constructive report. 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. The SAMI input catalogue is based on data taken from the Sloan Digital Sky Survey, the Galaxy And Mass Assembly (GAMA) Survey and the VLT Survey Telescope (VST) ATLAS Survey. The SAMI Galaxy Survey is supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (AS-TRO 3D), through project number CE170100013, 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 sami-survey.org. Publisher Copyright: © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.

PY - 2019/8/1

Y1 - 2019/8/1

N2 - We use data from the Sydney-AAO Multi-object Integral-field spectroscopy (SAMI) Galaxy Survey to study the dynamical scaling relation between galaxy stellar mass M∗ and the general kinematic parameter SK = √KV2rot + σ2 that combines rotation velocity Vrot and velocity dispersion σ. We show that the logM∗ - logSK relation: (1) is linear above limits set by properties of the samples and observations; (2) has slightly different slope when derived from stellar or gas kinematic measurements; (3) applies to both early-type and late-type galaxies and has smaller scatter than either the Tully.Fisher relation (logM∗ - log Vrot) for late types or the Faber.Jackson relation (logM∗ - log σ) for early types; and (4) has scatter that is only weakly sensitive to the value of K, with minimum scatter for K in the range 0.4 and 0.7. We compare SK to the aperture second moment (the 'aperture velocity dispersion') measured from the integrated spectrum within a 3-arcsecond radius aperture (σ3″ ). We find that while SK and σ3″ are in general tightly correlated, the logM∗ - log SK relation has less scatter than the logM∗ - log σ3″ relation.

AB - We use data from the Sydney-AAO Multi-object Integral-field spectroscopy (SAMI) Galaxy Survey to study the dynamical scaling relation between galaxy stellar mass M∗ and the general kinematic parameter SK = √KV2rot + σ2 that combines rotation velocity Vrot and velocity dispersion σ. We show that the logM∗ - logSK relation: (1) is linear above limits set by properties of the samples and observations; (2) has slightly different slope when derived from stellar or gas kinematic measurements; (3) applies to both early-type and late-type galaxies and has smaller scatter than either the Tully.Fisher relation (logM∗ - log Vrot) for late types or the Faber.Jackson relation (logM∗ - log σ) for early types; and (4) has scatter that is only weakly sensitive to the value of K, with minimum scatter for K in the range 0.4 and 0.7. We compare SK to the aperture second moment (the 'aperture velocity dispersion') measured from the integrated spectrum within a 3-arcsecond radius aperture (σ3″ ). We find that while SK and σ3″ are in general tightly correlated, the logM∗ - log SK relation has less scatter than the logM∗ - log σ3″ relation.

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The SAMI galaxy survey: Mass-kinematics scaling relations

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