Galaxy And Mass Assembly (GAMA): spectroscopic analysis

A. M. Hopkins, S. P. Driver, S. Brough, M. S. Owers, A. E. Bauer, M. L P Gunawardhana, M. E. Cluver, M. Colless, C. Foster, M. A. Lara-López, I. Roseboom, R. Sharp, O. Steele, D. Thomas, I. K. Baldry, M. J I Brown, J. Liske, P. Norberg, A. S G Robotham, S. Bamford & 62 others J. Bland-Hawthorn, M. J. Drinkwater, J. Loveday, M. Meyer, J. A. Peacock, R. Tuffs, N. Agius, M. Alpaslan, E. Andrae, E. Cameron, S. Cole, J. H Y Ching, L. Christodoulou, C. Conselice, S. Croom, N. J G Cross, R. De Propris, J. Delhaize, L. Dunne, S. Eales, S. Ellis, C. S. Frenk, Alister W. Graham, M. W. Grootes, B. Häußler, C. Heymans, D. Hill, B. Hoyle, M. Hudson, M. Jarvis, J. Johansson, D. H. Jones, E. van Kampen, L. Kelvin, K. Kuijken, A. López-Sánchez, S. Maddox, B. Madore, C. Maraston, T. McNaught-Roberts, R. C. Nichol, S. Oliver, H. Parkinson, S. Penny, S. Phillipps, K. A. Pimbblet, T. Ponman, C. C. Popescu, M. Prescott, R. Proctor, E. M. Sadler, A. E. Sansom, M. Seibert, L. Staveley-Smith, W. Sutherland, E. Taylor, L. Van Waerbeke, J. A. Vázquez-Mata, S. Warren, D. B. Wijesinghe, V. Wild, S. Wilkins

Research output: Contribution to journalArticleResearchpeer-review

Abstract

The Galaxy And Mass Assembly (GAMA) survey is a multiwavelength photometric and spectroscopic survey, using the AAOmega spectrograph on the Anglo-Australian Telescope to obtain spectra for up to ~300 000 galaxies over 280 deg2, to a limiting magnitude of rpet < 19.8 mag. The target galaxies are distributed over 0 < z ≲ 0.5 with a median redshift of z ≈ 0.2, although the redshift distribution includes a small number of systems, primarily quasars, at higher redshifts, up to and beyond z = 1. The redshift accuracy ranges from σv ≈ 50 km s-1 to σv ≈ 100 km s-1 depending on the signal-to-noise ratio of the spectrum. Here we describe the GAMA spectroscopic reduction and analysis pipeline. We present the steps involved in taking the raw two-dimensional spectroscopic images through to flux-calibrated one-dimensional spectra. The resulting GAMA spectra cover an observed wavelength range of 3750 λ 8850Å at a resolution of R ≈ 1300. The final flux calibration is typically accurate to 10-20 per cent, although the reliability is worse at the extreme wavelength ends, and poorer in the blue than the red. We present details of the measurement of emission and absorption features in the GAMA spectra. These measurements are characterized through a variety of quality control analyses detailing the robustness and reliability of the measurements. We illustrate the quality of the measurements with a brief exploration of elementary emission line properties of the galaxies in the GAMA sample. We demonstrate the luminosity dependence of the Balmer decrement, consistent with previously published results, and explore further how Balmer decrement varies with galaxy mass and redshift. We also investigate the mass and redshift dependencies of the [NII]/Hα versus [OIII]/Hβ spectral diagnostic diagram, commonly used to discriminate between star forming and nuclear activity in galaxies.

LanguageEnglish
Pages2047-2066
Number of pages20
JournalMonthly Notices of the Royal Astronomical Society
Volume430
Issue number3
DOIs
Publication statusPublished - 2013

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spectroscopic analysis
assembly
galaxies
wavelength
analysis
quality control
signal-to-noise ratio
diagram
calibration
wavelengths
quasars
spectrographs
signal to noise ratios
diagrams
luminosity
telescopes
stars

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Hopkins, A. M., Driver, S. P., Brough, S., Owers, M. S., Bauer, A. E., Gunawardhana, M. L. P., ... Wilkins, S. (2013). Galaxy And Mass Assembly (GAMA): spectroscopic analysis. Monthly Notices of the Royal Astronomical Society, 430(3), 2047-2066. https://doi.org/10.1093/mnras/stt030
Hopkins, A. M. ; Driver, S. P. ; Brough, S. ; Owers, M. S. ; Bauer, A. E. ; Gunawardhana, M. L P ; Cluver, M. E. ; Colless, M. ; Foster, C. ; Lara-López, M. A. ; Roseboom, I. ; Sharp, R. ; Steele, O. ; Thomas, D. ; Baldry, I. K. ; Brown, M. J I ; Liske, J. ; Norberg, P. ; Robotham, A. S G ; Bamford, S. ; Bland-Hawthorn, J. ; Drinkwater, M. J. ; Loveday, J. ; Meyer, M. ; Peacock, J. A. ; Tuffs, R. ; Agius, N. ; Alpaslan, M. ; Andrae, E. ; Cameron, E. ; Cole, S. ; Ching, J. H Y ; Christodoulou, L. ; Conselice, C. ; Croom, S. ; Cross, N. J G ; De Propris, R. ; Delhaize, J. ; Dunne, L. ; Eales, S. ; Ellis, S. ; Frenk, C. S. ; Graham, Alister W. ; Grootes, M. W. ; Häußler, B. ; Heymans, C. ; Hill, D. ; Hoyle, B. ; Hudson, M. ; Jarvis, M. ; Johansson, J. ; Jones, D. H. ; van Kampen, E. ; Kelvin, L. ; Kuijken, K. ; López-Sánchez, A. ; Maddox, S. ; Madore, B. ; Maraston, C. ; McNaught-Roberts, T. ; Nichol, R. C. ; Oliver, S. ; Parkinson, H. ; Penny, S. ; Phillipps, S. ; Pimbblet, K. A. ; Ponman, T. ; Popescu, C. C. ; Prescott, M. ; Proctor, R. ; Sadler, E. M. ; Sansom, A. E. ; Seibert, M. ; Staveley-Smith, L. ; Sutherland, W. ; Taylor, E. ; Van Waerbeke, L. ; Vázquez-Mata, J. A. ; Warren, S. ; Wijesinghe, D. B. ; Wild, V. ; Wilkins, S. / Galaxy And Mass Assembly (GAMA) : spectroscopic analysis. In: Monthly Notices of the Royal Astronomical Society. 2013 ; Vol. 430, No. 3. pp. 2047-2066.
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abstract = "The Galaxy And Mass Assembly (GAMA) survey is a multiwavelength photometric and spectroscopic survey, using the AAOmega spectrograph on the Anglo-Australian Telescope to obtain spectra for up to ~300 000 galaxies over 280 deg2, to a limiting magnitude of rpet < 19.8 mag. The target galaxies are distributed over 0 < z ≲ 0.5 with a median redshift of z ≈ 0.2, although the redshift distribution includes a small number of systems, primarily quasars, at higher redshifts, up to and beyond z = 1. The redshift accuracy ranges from σv ≈ 50 km s-1 to σv ≈ 100 km s-1 depending on the signal-to-noise ratio of the spectrum. Here we describe the GAMA spectroscopic reduction and analysis pipeline. We present the steps involved in taking the raw two-dimensional spectroscopic images through to flux-calibrated one-dimensional spectra. The resulting GAMA spectra cover an observed wavelength range of 3750 λ 8850{\AA} at a resolution of R ≈ 1300. The final flux calibration is typically accurate to 10-20 per cent, although the reliability is worse at the extreme wavelength ends, and poorer in the blue than the red. We present details of the measurement of emission and absorption features in the GAMA spectra. These measurements are characterized through a variety of quality control analyses detailing the robustness and reliability of the measurements. We illustrate the quality of the measurements with a brief exploration of elementary emission line properties of the galaxies in the GAMA sample. We demonstrate the luminosity dependence of the Balmer decrement, consistent with previously published results, and explore further how Balmer decrement varies with galaxy mass and redshift. We also investigate the mass and redshift dependencies of the [NII]/Hα versus [OIII]/Hβ spectral diagnostic diagram, commonly used to discriminate between star forming and nuclear activity in galaxies.",
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year = "2013",
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volume = "430",
pages = "2047--2066",
journal = "Monthly Notices of the Royal Astronomical Society",
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Hopkins, AM, Driver, SP, Brough, S, Owers, MS, Bauer, AE, Gunawardhana, MLP, Cluver, ME, Colless, M, Foster, C, Lara-López, MA, Roseboom, I, Sharp, R, Steele, O, Thomas, D, Baldry, IK, Brown, MJI, Liske, J, Norberg, P, Robotham, ASG, Bamford, S, Bland-Hawthorn, J, Drinkwater, MJ, Loveday, J, Meyer, M, Peacock, JA, Tuffs, R, Agius, N, Alpaslan, M, Andrae, E, Cameron, E, Cole, S, Ching, JHY, Christodoulou, L, Conselice, C, Croom, S, Cross, NJG, De Propris, R, Delhaize, J, Dunne, L, Eales, S, Ellis, S, Frenk, CS, Graham, AW, Grootes, MW, Häußler, B, Heymans, C, Hill, D, Hoyle, B, Hudson, M, Jarvis, M, Johansson, J, Jones, DH, van Kampen, E, Kelvin, L, Kuijken, K, López-Sánchez, A, Maddox, S, Madore, B, Maraston, C, McNaught-Roberts, T, Nichol, RC, Oliver, S, Parkinson, H, Penny, S, Phillipps, S, Pimbblet, KA, Ponman, T, Popescu, CC, Prescott, M, Proctor, R, Sadler, EM, Sansom, AE, Seibert, M, Staveley-Smith, L, Sutherland, W, Taylor, E, Van Waerbeke, L, Vázquez-Mata, JA, Warren, S, Wijesinghe, DB, Wild, V & Wilkins, S 2013, 'Galaxy And Mass Assembly (GAMA): spectroscopic analysis' Monthly Notices of the Royal Astronomical Society, vol. 430, no. 3, pp. 2047-2066. https://doi.org/10.1093/mnras/stt030

Galaxy And Mass Assembly (GAMA) : spectroscopic analysis. / Hopkins, A. M.; Driver, S. P.; Brough, S.; Owers, M. S.; Bauer, A. E.; Gunawardhana, M. L P; Cluver, M. E.; Colless, M.; Foster, C.; Lara-López, M. A.; Roseboom, I.; Sharp, R.; Steele, O.; Thomas, D.; Baldry, I. K.; Brown, M. J I; Liske, J.; Norberg, P.; Robotham, A. S G; Bamford, S.; Bland-Hawthorn, J.; Drinkwater, M. J.; Loveday, J.; Meyer, M.; Peacock, J. A.; Tuffs, R.; Agius, N.; Alpaslan, M.; Andrae, E.; Cameron, E.; Cole, S.; Ching, J. H Y; Christodoulou, L.; Conselice, C.; Croom, S.; Cross, N. J G; De Propris, R.; Delhaize, J.; Dunne, L.; Eales, S.; Ellis, S.; Frenk, C. S.; Graham, Alister W.; Grootes, M. W.; Häußler, B.; Heymans, C.; Hill, D.; Hoyle, B.; Hudson, M.; Jarvis, M.; Johansson, J.; Jones, D. H.; van Kampen, E.; Kelvin, L.; Kuijken, K.; López-Sánchez, A.; Maddox, S.; Madore, B.; Maraston, C.; McNaught-Roberts, T.; Nichol, R. C.; Oliver, S.; Parkinson, H.; Penny, S.; Phillipps, S.; Pimbblet, K. A.; Ponman, T.; Popescu, C. C.; Prescott, M.; Proctor, R.; Sadler, E. M.; Sansom, A. E.; Seibert, M.; Staveley-Smith, L.; Sutherland, W.; Taylor, E.; Van Waerbeke, L.; Vázquez-Mata, J. A.; Warren, S.; Wijesinghe, D. B.; Wild, V.; Wilkins, S.

In: Monthly Notices of the Royal Astronomical Society, Vol. 430, No. 3, 2013, p. 2047-2066.

Research output: Contribution to journalArticleResearchpeer-review

TY - JOUR

T1 - Galaxy And Mass Assembly (GAMA)

T2 - Monthly Notices of the Royal Astronomical Society

AU - Hopkins,A. M.

AU - Driver,S. P.

AU - Brough,S.

AU - Owers,M. S.

AU - Bauer,A. E.

AU - Gunawardhana,M. L P

AU - Cluver,M. E.

AU - Colless,M.

AU - Foster,C.

AU - Lara-López,M. A.

AU - Roseboom,I.

AU - Sharp,R.

AU - Steele,O.

AU - Thomas,D.

AU - Baldry,I. K.

AU - Brown,M. J I

AU - Liske,J.

AU - Norberg,P.

AU - Robotham,A. S G

AU - Bamford,S.

AU - Bland-Hawthorn,J.

AU - Drinkwater,M. J.

AU - Loveday,J.

AU - Meyer,M.

AU - Peacock,J. A.

AU - Tuffs,R.

AU - Agius,N.

AU - Alpaslan,M.

AU - Andrae,E.

AU - Cameron,E.

AU - Cole,S.

AU - Ching,J. H Y

AU - Christodoulou,L.

AU - Conselice,C.

AU - Croom,S.

AU - Cross,N. J G

AU - De Propris,R.

AU - Delhaize,J.

AU - Dunne,L.

AU - Eales,S.

AU - Ellis,S.

AU - Frenk,C. S.

AU - Graham,Alister W.

AU - Grootes,M. W.

AU - Häußler,B.

AU - Heymans,C.

AU - Hill,D.

AU - Hoyle,B.

AU - Hudson,M.

AU - Jarvis,M.

AU - Johansson,J.

AU - Jones,D. H.

AU - van Kampen,E.

AU - Kelvin,L.

AU - Kuijken,K.

AU - López-Sánchez,A.

AU - Maddox,S.

AU - Madore,B.

AU - Maraston,C.

AU - McNaught-Roberts,T.

AU - Nichol,R. C.

AU - Oliver,S.

AU - Parkinson,H.

AU - Penny,S.

AU - Phillipps,S.

AU - Pimbblet,K. A.

AU - Ponman,T.

AU - Popescu,C. C.

AU - Prescott,M.

AU - Proctor,R.

AU - Sadler,E. M.

AU - Sansom,A. E.

AU - Seibert,M.

AU - Staveley-Smith,L.

AU - Sutherland,W.

AU - Taylor,E.

AU - Van Waerbeke,L.

AU - Vázquez-Mata,J. A.

AU - Warren,S.

AU - Wijesinghe,D. B.

AU - Wild,V.

AU - Wilkins,S.

PY - 2013

Y1 - 2013

N2 - The Galaxy And Mass Assembly (GAMA) survey is a multiwavelength photometric and spectroscopic survey, using the AAOmega spectrograph on the Anglo-Australian Telescope to obtain spectra for up to ~300 000 galaxies over 280 deg2, to a limiting magnitude of rpet < 19.8 mag. The target galaxies are distributed over 0 < z ≲ 0.5 with a median redshift of z ≈ 0.2, although the redshift distribution includes a small number of systems, primarily quasars, at higher redshifts, up to and beyond z = 1. The redshift accuracy ranges from σv ≈ 50 km s-1 to σv ≈ 100 km s-1 depending on the signal-to-noise ratio of the spectrum. Here we describe the GAMA spectroscopic reduction and analysis pipeline. We present the steps involved in taking the raw two-dimensional spectroscopic images through to flux-calibrated one-dimensional spectra. The resulting GAMA spectra cover an observed wavelength range of 3750 λ 8850Å at a resolution of R ≈ 1300. The final flux calibration is typically accurate to 10-20 per cent, although the reliability is worse at the extreme wavelength ends, and poorer in the blue than the red. We present details of the measurement of emission and absorption features in the GAMA spectra. These measurements are characterized through a variety of quality control analyses detailing the robustness and reliability of the measurements. We illustrate the quality of the measurements with a brief exploration of elementary emission line properties of the galaxies in the GAMA sample. We demonstrate the luminosity dependence of the Balmer decrement, consistent with previously published results, and explore further how Balmer decrement varies with galaxy mass and redshift. We also investigate the mass and redshift dependencies of the [NII]/Hα versus [OIII]/Hβ spectral diagnostic diagram, commonly used to discriminate between star forming and nuclear activity in galaxies.

AB - The Galaxy And Mass Assembly (GAMA) survey is a multiwavelength photometric and spectroscopic survey, using the AAOmega spectrograph on the Anglo-Australian Telescope to obtain spectra for up to ~300 000 galaxies over 280 deg2, to a limiting magnitude of rpet < 19.8 mag. The target galaxies are distributed over 0 < z ≲ 0.5 with a median redshift of z ≈ 0.2, although the redshift distribution includes a small number of systems, primarily quasars, at higher redshifts, up to and beyond z = 1. The redshift accuracy ranges from σv ≈ 50 km s-1 to σv ≈ 100 km s-1 depending on the signal-to-noise ratio of the spectrum. Here we describe the GAMA spectroscopic reduction and analysis pipeline. We present the steps involved in taking the raw two-dimensional spectroscopic images through to flux-calibrated one-dimensional spectra. The resulting GAMA spectra cover an observed wavelength range of 3750 λ 8850Å at a resolution of R ≈ 1300. The final flux calibration is typically accurate to 10-20 per cent, although the reliability is worse at the extreme wavelength ends, and poorer in the blue than the red. We present details of the measurement of emission and absorption features in the GAMA spectra. These measurements are characterized through a variety of quality control analyses detailing the robustness and reliability of the measurements. We illustrate the quality of the measurements with a brief exploration of elementary emission line properties of the galaxies in the GAMA sample. We demonstrate the luminosity dependence of the Balmer decrement, consistent with previously published results, and explore further how Balmer decrement varies with galaxy mass and redshift. We also investigate the mass and redshift dependencies of the [NII]/Hα versus [OIII]/Hβ spectral diagnostic diagram, commonly used to discriminate between star forming and nuclear activity in galaxies.

KW - galaxies: evolution

KW - galaxies: formation

KW - galaxies: general

UR - http://www.scopus.com/inward/record.url?scp=84876798195&partnerID=8YFLogxK

U2 - 10.1093/mnras/stt030

DO - 10.1093/mnras/stt030

M3 - Article

VL - 430

SP - 2047

EP - 2066

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -