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

Australian Astronomical Optics

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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 - Aug 2019

Bibliographical note

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society, Volume 487, Issue 2, August 2019, Pages 2924–2936, https://doi.org/10.1093/mnras/stz1439. Copyright 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

Keywords

Galaxy stellar content
Galaxy structure
Galaxy: kinematics and dynamics

Access to Document

10.1093/mnras/stz1439

Publisher version (open access)Final published version, 11.1 MBLicence: Other

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{a950151f2fba43e0acf47f7684a7d66d,

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.",

keywords = "Galaxy stellar content, Galaxy structure, Galaxy: kinematics and dynamics",

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 = "This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society, Volume 487, Issue 2, August 2019, Pages 2924–2936, https://doi.org/10.1093/mnras/stz1439. Copyright 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.",

year = "2019",

month = aug,

doi = "10.1093/mnras/stz1439",

language = "English",

volume = "487",

pages = "2924--2936",

journal = "Monthly Notices of the Royal Astronomical Society: Letters",

issn = "1745-3925",

publisher = "Oxford University Press",

number = "2",

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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 - This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society, Volume 487, Issue 2, August 2019, Pages 2924–2936, https://doi.org/10.1093/mnras/stz1439. Copyright 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

PY - 2019/8

Y1 - 2019/8

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.

KW - Galaxy stellar content

KW - Galaxy structure

KW - Galaxy: kinematics and dynamics

UR - http://www.scopus.com/inward/record.url?scp=85071155577&partnerID=8YFLogxK

UR - http://purl.org/au-research/grants/arc/CE1101020

UR - http://purl.org/au-research/grants/arc/CE170100013

UR - http://purl.org/au-research/grants/arc/FT140100255

U2 - 10.1093/mnras/stz1439

DO - 10.1093/mnras/stz1439

M3 - Article

AN - SCOPUS:85071155577

VL - 487

SP - 2924

EP - 2936

JO - Monthly Notices of the Royal Astronomical Society: Letters

JF - Monthly Notices of the Royal Astronomical Society: Letters

SN - 1745-3925

IS - 2

ER -

The SAMI Galaxy Survey: mass-kinematics scaling relations

Abstract

Bibliographical note

Keywords

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The impact of impact: what stops star formation in cluster galaxies?

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The SAMI Galaxy Survey: mass-kinematics scaling relations

Abstract

Bibliographical note

Keywords

Access to Document

Other files and links

Fingerprint

Projects

The impact of impact: what stops star formation in cluster galaxies?

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