Galaxy and mass assembly (GAMA): the mass-metallicity relationship

C. Foster; A. M. Hopkins; M. Gunawardhana; M. A. Lara-López; R. G. Sharp; O. Steele; E. N. Taylor; S. P. Driver; I. K. Baldry; S. P. Bamford; J. Liske; J. Loveday; P. Norberg; J. A. Peacock; M. Alpaslan; A. E. Bauer; J. Bland-Hawthorn; S. Brough; E. Cameron; M. Colless; C. J. Conselice; S. M. Croom; C. S. Frenk; D. T. Hill; D. H. Jones; L. S. Kelvin; K. Kuijken; R. C. Nichol; M. S. Owers; H. R. Parkinson; K. A. Pimbblet; C. C. Popescu; M. Prescott; A. S G Robotham; A. R. Lopez-Sanchez; W. J. Sutherland; D. Thomas; R. J. Tuffs; E. Van Kampen; D. Wijesinghe

doi:10.1051/0004-6361/201220050

Galaxy and mass assembly (GAMA): the mass-metallicity relationship

C. Foster^*, A. M. Hopkins, M. Gunawardhana, M. A. Lara-López, R. G. Sharp, O. Steele, E. N. Taylor, S. P. Driver, I. K. Baldry, S. P. Bamford, J. Liske, J. Loveday, P. Norberg, J. A. Peacock, M. Alpaslan, A. E. Bauer, J. Bland-Hawthorn, S. Brough, E. Cameron, M. CollessC. J. Conselice, S. M. Croom, C. S. Frenk, D. T. Hill, D. H. Jones, L. S. Kelvin, K. Kuijken, R. C. Nichol, M. S. Owers, H. R. Parkinson, K. A. Pimbblet, C. C. Popescu, M. Prescott, A. S G Robotham, A. R. Lopez-Sanchez, W. J. Sutherland, D. Thomas, R. J. Tuffs, E. Van Kampen, D. Wijesinghe

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

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Abstract

Context. The mass-metallicity relationship (MMR) of star-forming galaxies is well-established, however there is still some disagreement with respect to its exact shape and its possible dependence on other observables. Aims.We measure the MMR in the Galaxy And Mass Assembly (GAMA) survey. We compare our measured MMR to that measured in the Sloan Digital Sky Survey (SDSS) and study the dependence of the MMR on various selection criteria to identify potential causes for disparities seen in the literature. Methods.We use strong emission line ratio diagnostics to derive oxygen abundances. We then apply a range of selection criteria for the minimum signal-to-noise in various emission lines, as well as the apparent and absolute magnitude to study variations in the inferred MMR. Results. The shape and position of the MMR can differ significantly depending on the metallicity calibration and selection used. After selecting a robust metallicity calibration amongst those tested, we find that the mass-metallicity relation for redshifts 0.061 ≲ z ≲ 0.35 in GAMA is in reasonable agreement with that found in the SDSS despite the difference in the luminosity range probed. Conclusions. In view of the significant variations of the MMR brought about by reasonable changes in the sample selection criteria and method, we recommend that care be taken when comparing the MMR from different surveys and studies directly. We also conclude that there could be a modest level of evolution over 0.06 ≤ z ≤ 0.35 within the GAMA sample.

Original language	English
Article number	A79
Pages (from-to)	1-9
Number of pages	9
Journal	Astronomy and Astrophysics
Volume	547
DOIs	https://doi.org/10.1051/0004-6361/201220050
Publication status	Published - 2012

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Foster, C., Hopkins, A. M., Gunawardhana, M., Lara-López, M. A., Sharp, R. G., Steele, O., Taylor, E. N., Driver, S. P., Baldry, I. K., Bamford, S. P., Liske, J., Loveday, J., Norberg, P., Peacock, J. A., Alpaslan, M., Bauer, A. E., Bland-Hawthorn, J., Brough, S., Cameron, E., ... Wijesinghe, D. (2012). Galaxy and mass assembly (GAMA): the mass-metallicity relationship. Astronomy and Astrophysics, 547, 1-9. Article A79. https://doi.org/10.1051/0004-6361/201220050

@article{36a80fd18b62402c8c54f1c7c68c643c,

title = "Galaxy and mass assembly (GAMA): the mass-metallicity relationship",

abstract = "Context. The mass-metallicity relationship (MMR) of star-forming galaxies is well-established, however there is still some disagreement with respect to its exact shape and its possible dependence on other observables. Aims.We measure the MMR in the Galaxy And Mass Assembly (GAMA) survey. We compare our measured MMR to that measured in the Sloan Digital Sky Survey (SDSS) and study the dependence of the MMR on various selection criteria to identify potential causes for disparities seen in the literature. Methods.We use strong emission line ratio diagnostics to derive oxygen abundances. We then apply a range of selection criteria for the minimum signal-to-noise in various emission lines, as well as the apparent and absolute magnitude to study variations in the inferred MMR. Results. The shape and position of the MMR can differ significantly depending on the metallicity calibration and selection used. After selecting a robust metallicity calibration amongst those tested, we find that the mass-metallicity relation for redshifts 0.061 ≲ z ≲ 0.35 in GAMA is in reasonable agreement with that found in the SDSS despite the difference in the luminosity range probed. Conclusions. In view of the significant variations of the MMR brought about by reasonable changes in the sample selection criteria and method, we recommend that care be taken when comparing the MMR from different surveys and studies directly. We also conclude that there could be a modest level of evolution over 0.06 ≤ z ≤ 0.35 within the GAMA sample.",

author = "C. Foster and Hopkins, {A. M.} and M. Gunawardhana and Lara-L{\'o}pez, {M. A.} and Sharp, {R. G.} and O. Steele and Taylor, {E. N.} and Driver, {S. P.} and Baldry, {I. K.} and Bamford, {S. P.} and J. Liske and J. Loveday and P. Norberg and Peacock, {J. A.} and M. Alpaslan and Bauer, {A. E.} and J. Bland-Hawthorn and S. Brough and E. Cameron and M. Colless and Conselice, {C. J.} and Croom, {S. M.} and Frenk, {C. S.} and Hill, {D. T.} and Jones, {D. H.} and Kelvin, {L. S.} and K. Kuijken and Nichol, {R. C.} and Owers, {M. S.} and Parkinson, {H. R.} and Pimbblet, {K. A.} and Popescu, {C. C.} and M. Prescott and Robotham, {A. S G} and Lopez-Sanchez, {A. R.} and Sutherland, {W. J.} and D. Thomas and Tuffs, {R. J.} and {Van Kampen}, E. and D. Wijesinghe",

year = "2012",

doi = "10.1051/0004-6361/201220050",

language = "English",

volume = "547",

pages = "1--9",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Foster, C, Hopkins, AM, Gunawardhana, M, Lara-López, MA, Sharp, RG, Steele, O, Taylor, EN, Driver, SP, Baldry, IK, Bamford, SP, Liske, J, Loveday, J, Norberg, P, Peacock, JA, Alpaslan, M, Bauer, AE, Bland-Hawthorn, J, Brough, S, Cameron, E, Colless, M, Conselice, CJ, Croom, SM, Frenk, CS, Hill, DT, Jones, DH, Kelvin, LS, Kuijken, K, Nichol, RC, Owers, MS, Parkinson, HR, Pimbblet, KA, Popescu, CC, Prescott, M, Robotham, ASG, Lopez-Sanchez, AR, Sutherland, WJ, Thomas, D, Tuffs, RJ, Van Kampen, E & Wijesinghe, D 2012, 'Galaxy and mass assembly (GAMA): the mass-metallicity relationship', Astronomy and Astrophysics, vol. 547, A79, pp. 1-9. https://doi.org/10.1051/0004-6361/201220050

TY - JOUR

T1 - Galaxy and mass assembly (GAMA)

T2 - the mass-metallicity relationship

AU - Foster, C.

AU - Hopkins, A. M.

AU - Gunawardhana, M.

AU - Lara-López, M. A.

AU - Sharp, R. G.

AU - Steele, O.

AU - Taylor, E. N.

AU - Driver, S. P.

AU - Baldry, I. K.

AU - Bamford, S. P.

AU - Liske, J.

AU - Loveday, J.

AU - Norberg, P.

AU - Peacock, J. A.

AU - Alpaslan, M.

AU - Bauer, A. E.

AU - Bland-Hawthorn, J.

AU - Brough, S.

AU - Cameron, E.

AU - Colless, M.

AU - Conselice, C. J.

AU - Croom, S. M.

AU - Frenk, C. S.

AU - Hill, D. T.

AU - Jones, D. H.

AU - Kelvin, L. S.

AU - Kuijken, K.

AU - Nichol, R. C.

AU - Owers, M. S.

AU - Parkinson, H. R.

AU - Pimbblet, K. A.

AU - Popescu, C. C.

AU - Prescott, M.

AU - Robotham, A. S G

AU - Lopez-Sanchez, A. R.

AU - Sutherland, W. J.

AU - Thomas, D.

AU - Tuffs, R. J.

AU - Van Kampen, E.

AU - Wijesinghe, D.

PY - 2012

Y1 - 2012

N2 - Context. The mass-metallicity relationship (MMR) of star-forming galaxies is well-established, however there is still some disagreement with respect to its exact shape and its possible dependence on other observables. Aims.We measure the MMR in the Galaxy And Mass Assembly (GAMA) survey. We compare our measured MMR to that measured in the Sloan Digital Sky Survey (SDSS) and study the dependence of the MMR on various selection criteria to identify potential causes for disparities seen in the literature. Methods.We use strong emission line ratio diagnostics to derive oxygen abundances. We then apply a range of selection criteria for the minimum signal-to-noise in various emission lines, as well as the apparent and absolute magnitude to study variations in the inferred MMR. Results. The shape and position of the MMR can differ significantly depending on the metallicity calibration and selection used. After selecting a robust metallicity calibration amongst those tested, we find that the mass-metallicity relation for redshifts 0.061 ≲ z ≲ 0.35 in GAMA is in reasonable agreement with that found in the SDSS despite the difference in the luminosity range probed. Conclusions. In view of the significant variations of the MMR brought about by reasonable changes in the sample selection criteria and method, we recommend that care be taken when comparing the MMR from different surveys and studies directly. We also conclude that there could be a modest level of evolution over 0.06 ≤ z ≤ 0.35 within the GAMA sample.

AB - Context. The mass-metallicity relationship (MMR) of star-forming galaxies is well-established, however there is still some disagreement with respect to its exact shape and its possible dependence on other observables. Aims.We measure the MMR in the Galaxy And Mass Assembly (GAMA) survey. We compare our measured MMR to that measured in the Sloan Digital Sky Survey (SDSS) and study the dependence of the MMR on various selection criteria to identify potential causes for disparities seen in the literature. Methods.We use strong emission line ratio diagnostics to derive oxygen abundances. We then apply a range of selection criteria for the minimum signal-to-noise in various emission lines, as well as the apparent and absolute magnitude to study variations in the inferred MMR. Results. The shape and position of the MMR can differ significantly depending on the metallicity calibration and selection used. After selecting a robust metallicity calibration amongst those tested, we find that the mass-metallicity relation for redshifts 0.061 ≲ z ≲ 0.35 in GAMA is in reasonable agreement with that found in the SDSS despite the difference in the luminosity range probed. Conclusions. In view of the significant variations of the MMR brought about by reasonable changes in the sample selection criteria and method, we recommend that care be taken when comparing the MMR from different surveys and studies directly. We also conclude that there could be a modest level of evolution over 0.06 ≤ z ≤ 0.35 within the GAMA sample.

UR - http://www.scopus.com/inward/record.url?scp=84868314594&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201220050

DO - 10.1051/0004-6361/201220050

M3 - Article

AN - SCOPUS:84868314594

SN - 0004-6361

VL - 547

SP - 1

EP - 9

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A79

ER -

Galaxy and mass assembly (GAMA): the mass-metallicity relationship

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