Galaxy And Mass Assembly (GAMA): The galaxy stellar mass function to z = 0.1 from the r-band selected equatorial regions

A. H. Wright, A. S.G. Robotham, S. P. Driver, M. Alpaslan, S. K. Andrews, Ivan K. Baldry, J. Bland-Hawthorn, S. Brough, M. J.I. Brown, M. Colless, E. Da Cunha, L. J.M. Davies, Alister W. Graham, B. W. Holwerda, A. M. Hopkins, P. R. Kafle, L. S. Kelvin, J. Loveday, S.J. Maddox, M. J. Meyer & 7 others A. J. Moffett, P. Norberg, S. Phillipps, K. Rowlands, E. N. Taylor, L. Wang, S. M. Wilkins

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Abstract

We derive the low-redshift galaxy stellar mass function (GSMF), inclusive of dust corrections, for the equatorial Galaxy And Mass Assembly (GAMA) data set covering 180 deg2. We construct the mass function using a density-corrected maximum volume method, using masses corrected for the impact of optically thick and thin dust. We explore the galactic bivariate brightness plane (M*-μ), demonstrating that surface brightness effects do not systematically bias our mass function measurement above 107.5 M. The galaxy distribution in the M-μ plane appears well bounded, indicating that no substantial population of massive but diffuse or highly compact galaxies are systematically missed due to the GAMA selection criteria. The GSMF is fitted with a double Schechter function, with M* = 1010.78±0.01±0.20 M, φ1* = (2.93 ± 0.40) × 10-3 h70 3 Mpc-3, α1 =-0.62 ± 0.03 ± 0.15, φ2* = (0.63 ± 0.10) × 10-3 h70 3 Mpc-3 and α2 =-1.50 ± 0.01 ± 0.15. We find the equivalent faint end slope as previously estimated using the GAMA-I sample, although we find a higher value of M*. Using the full GAMA-II sample, we are able to fit the mass function to masses as low as 107.5 M, and assess limits to 106.5 M. Combining GAMA-II with data from G10-COSMOS, we are able to comment qualitatively on the shape of the GSMF down to masses as low as 106 M. Beyond the well-known upturn seen in the GSMF at 109.5, the distribution appears to maintain a single power-law slope from 109 to 106.5. We calculate the stellar mass density parameter given our best-estimate GSMF, finding Ω* = 1.66-0.23 +0.24 ± 0.97 h 70 -1 × 10-3, inclusive of random and systematic uncertainties.

Original languageEnglish
Article numberstx1149
Pages (from-to)283-302
Number of pages20
JournalMonthly Notices of the Royal Astronomical Society
Volume470
Issue number1
DOIs
Publication statusPublished - Aug 2017

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equatorial regions
stellar mass
assembly
galaxies
brightness
dust
slopes
compact galaxies
coverings

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Wright, A. H. ; Robotham, A. S.G. ; Driver, S. P. ; Alpaslan, M. ; Andrews, S. K. ; Baldry, Ivan K. ; Bland-Hawthorn, J. ; Brough, S. ; Brown, M. J.I. ; Colless, M. ; Da Cunha, E. ; Davies, L. J.M. ; Graham, Alister W. ; Holwerda, B. W. ; Hopkins, A. M. ; Kafle, P. R. ; Kelvin, L. S. ; Loveday, J. ; Maddox, S.J. ; Meyer, M. J. ; Moffett, A. J. ; Norberg, P. ; Phillipps, S. ; Rowlands, K. ; Taylor, E. N. ; Wang, L. ; Wilkins, S. M. / Galaxy And Mass Assembly (GAMA) : The galaxy stellar mass function to z = 0.1 from the r-band selected equatorial regions. In: Monthly Notices of the Royal Astronomical Society. 2017 ; Vol. 470, No. 1. pp. 283-302.
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abstract = "We derive the low-redshift galaxy stellar mass function (GSMF), inclusive of dust corrections, for the equatorial Galaxy And Mass Assembly (GAMA) data set covering 180 deg2. We construct the mass function using a density-corrected maximum volume method, using masses corrected for the impact of optically thick and thin dust. We explore the galactic bivariate brightness plane (M*-μ), demonstrating that surface brightness effects do not systematically bias our mass function measurement above 107.5 M⊙. The galaxy distribution in the M-μ plane appears well bounded, indicating that no substantial population of massive but diffuse or highly compact galaxies are systematically missed due to the GAMA selection criteria. The GSMF is fitted with a double Schechter function, with M* = 1010.78±0.01±0.20 M⊙, φ1* = (2.93 ± 0.40) × 10-3 h70 3 Mpc-3, α1 =-0.62 ± 0.03 ± 0.15, φ2* = (0.63 ± 0.10) × 10-3 h70 3 Mpc-3 and α2 =-1.50 ± 0.01 ± 0.15. We find the equivalent faint end slope as previously estimated using the GAMA-I sample, although we find a higher value of M*. Using the full GAMA-II sample, we are able to fit the mass function to masses as low as 107.5 M⊙, and assess limits to 106.5 M⊙. Combining GAMA-II with data from G10-COSMOS, we are able to comment qualitatively on the shape of the GSMF down to masses as low as 106 M⊙. Beyond the well-known upturn seen in the GSMF at 109.5, the distribution appears to maintain a single power-law slope from 109 to 106.5. We calculate the stellar mass density parameter given our best-estimate GSMF, finding Ω* = 1.66-0.23 +0.24 ± 0.97 h 70 -1 × 10-3, inclusive of random and systematic uncertainties.",
keywords = "Galaxies: evolution, Galaxies: fundamental parameters, Galaxies: general, Galaxies: luminosity function, mass function, Galaxies: stellar content",
author = "Wright, {A. H.} and Robotham, {A. S.G.} and Driver, {S. P.} and M. Alpaslan and Andrews, {S. K.} and Baldry, {Ivan K.} and J. Bland-Hawthorn and S. Brough and Brown, {M. J.I.} and M. Colless and {Da Cunha}, E. and Davies, {L. J.M.} and Graham, {Alister W.} and Holwerda, {B. W.} and Hopkins, {A. M.} and Kafle, {P. R.} and Kelvin, {L. S.} and J. Loveday and S.J. Maddox and Meyer, {M. J.} and Moffett, {A. J.} and P. Norberg and S. Phillipps and K. Rowlands and Taylor, {E. N.} and L. Wang and Wilkins, {S. M.}",
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journal = "Monthly Notices of the Royal Astronomical Society",
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Wright, AH, Robotham, ASG, Driver, SP, Alpaslan, M, Andrews, SK, Baldry, IK, Bland-Hawthorn, J, Brough, S, Brown, MJI, Colless, M, Da Cunha, E, Davies, LJM, Graham, AW, Holwerda, BW, Hopkins, AM, Kafle, PR, Kelvin, LS, Loveday, J, Maddox, SJ, Meyer, MJ, Moffett, AJ, Norberg, P, Phillipps, S, Rowlands, K, Taylor, EN, Wang, L & Wilkins, SM 2017, 'Galaxy And Mass Assembly (GAMA): The galaxy stellar mass function to z = 0.1 from the r-band selected equatorial regions' Monthly Notices of the Royal Astronomical Society, vol. 470, no. 1, stx1149, pp. 283-302. https://doi.org/10.1093/mnras/stx1149

Galaxy And Mass Assembly (GAMA) : The galaxy stellar mass function to z = 0.1 from the r-band selected equatorial regions. / Wright, A. H.; Robotham, A. S.G.; Driver, S. P.; Alpaslan, M.; Andrews, S. K.; Baldry, Ivan K.; Bland-Hawthorn, J.; Brough, S.; Brown, M. J.I.; Colless, M.; Da Cunha, E.; Davies, L. J.M.; Graham, Alister W.; Holwerda, B. W.; Hopkins, A. M.; Kafle, P. R.; Kelvin, L. S.; Loveday, J.; Maddox, S.J.; Meyer, M. J.; Moffett, A. J.; Norberg, P.; Phillipps, S.; Rowlands, K.; Taylor, E. N.; Wang, L.; Wilkins, S. M.

In: Monthly Notices of the Royal Astronomical Society, Vol. 470, No. 1, stx1149, 08.2017, p. 283-302.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Galaxy And Mass Assembly (GAMA)

T2 - The galaxy stellar mass function to z = 0.1 from the r-band selected equatorial regions

AU - Wright, A. H.

AU - Robotham, A. S.G.

AU - Driver, S. P.

AU - Alpaslan, M.

AU - Andrews, S. K.

AU - Baldry, Ivan K.

AU - Bland-Hawthorn, J.

AU - Brough, S.

AU - Brown, M. J.I.

AU - Colless, M.

AU - Da Cunha, E.

AU - Davies, L. J.M.

AU - Graham, Alister W.

AU - Holwerda, B. W.

AU - Hopkins, A. M.

AU - Kafle, P. R.

AU - Kelvin, L. S.

AU - Loveday, J.

AU - Maddox, S.J.

AU - Meyer, M. J.

AU - Moffett, A. J.

AU - Norberg, P.

AU - Phillipps, S.

AU - Rowlands, K.

AU - Taylor, E. N.

AU - Wang, L.

AU - Wilkins, S. M.

PY - 2017/8

Y1 - 2017/8

N2 - We derive the low-redshift galaxy stellar mass function (GSMF), inclusive of dust corrections, for the equatorial Galaxy And Mass Assembly (GAMA) data set covering 180 deg2. We construct the mass function using a density-corrected maximum volume method, using masses corrected for the impact of optically thick and thin dust. We explore the galactic bivariate brightness plane (M*-μ), demonstrating that surface brightness effects do not systematically bias our mass function measurement above 107.5 M⊙. The galaxy distribution in the M-μ plane appears well bounded, indicating that no substantial population of massive but diffuse or highly compact galaxies are systematically missed due to the GAMA selection criteria. The GSMF is fitted with a double Schechter function, with M* = 1010.78±0.01±0.20 M⊙, φ1* = (2.93 ± 0.40) × 10-3 h70 3 Mpc-3, α1 =-0.62 ± 0.03 ± 0.15, φ2* = (0.63 ± 0.10) × 10-3 h70 3 Mpc-3 and α2 =-1.50 ± 0.01 ± 0.15. We find the equivalent faint end slope as previously estimated using the GAMA-I sample, although we find a higher value of M*. Using the full GAMA-II sample, we are able to fit the mass function to masses as low as 107.5 M⊙, and assess limits to 106.5 M⊙. Combining GAMA-II with data from G10-COSMOS, we are able to comment qualitatively on the shape of the GSMF down to masses as low as 106 M⊙. Beyond the well-known upturn seen in the GSMF at 109.5, the distribution appears to maintain a single power-law slope from 109 to 106.5. We calculate the stellar mass density parameter given our best-estimate GSMF, finding Ω* = 1.66-0.23 +0.24 ± 0.97 h 70 -1 × 10-3, inclusive of random and systematic uncertainties.

AB - We derive the low-redshift galaxy stellar mass function (GSMF), inclusive of dust corrections, for the equatorial Galaxy And Mass Assembly (GAMA) data set covering 180 deg2. We construct the mass function using a density-corrected maximum volume method, using masses corrected for the impact of optically thick and thin dust. We explore the galactic bivariate brightness plane (M*-μ), demonstrating that surface brightness effects do not systematically bias our mass function measurement above 107.5 M⊙. The galaxy distribution in the M-μ plane appears well bounded, indicating that no substantial population of massive but diffuse or highly compact galaxies are systematically missed due to the GAMA selection criteria. The GSMF is fitted with a double Schechter function, with M* = 1010.78±0.01±0.20 M⊙, φ1* = (2.93 ± 0.40) × 10-3 h70 3 Mpc-3, α1 =-0.62 ± 0.03 ± 0.15, φ2* = (0.63 ± 0.10) × 10-3 h70 3 Mpc-3 and α2 =-1.50 ± 0.01 ± 0.15. We find the equivalent faint end slope as previously estimated using the GAMA-I sample, although we find a higher value of M*. Using the full GAMA-II sample, we are able to fit the mass function to masses as low as 107.5 M⊙, and assess limits to 106.5 M⊙. Combining GAMA-II with data from G10-COSMOS, we are able to comment qualitatively on the shape of the GSMF down to masses as low as 106 M⊙. Beyond the well-known upturn seen in the GSMF at 109.5, the distribution appears to maintain a single power-law slope from 109 to 106.5. We calculate the stellar mass density parameter given our best-estimate GSMF, finding Ω* = 1.66-0.23 +0.24 ± 0.97 h 70 -1 × 10-3, inclusive of random and systematic uncertainties.

KW - Galaxies: evolution

KW - Galaxies: fundamental parameters

KW - Galaxies: general

KW - Galaxies: luminosity function, mass function

KW - Galaxies: stellar content

UR - http://www.scopus.com/inward/record.url?scp=85021787881&partnerID=8YFLogxK

U2 - 10.1093/mnras/stx1149

DO - 10.1093/mnras/stx1149

M3 - Article

VL - 470

SP - 283

EP - 302

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 1

M1 - stx1149

ER -