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Galaxy and Mass Assembly: FUV, NUV, ugrizYJHK Petrosian, Kron and Sérsic photometry

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Galaxy and Mass Assembly : FUV, NUV, ugrizYJHK Petrosian, Kron and Sérsic photometry. / Hill, David T.; Kelvin, Lee S.; Driver, Simon P.; Robotham, Aaron S. G.; Cameron, Ewan; Cross, Nicholas J. G.; Andrae, Ellen; Baldry, Ivan K.; Bamford, Steven P.; Bland-Hawthorn, Joss; Brough, Sarah; Conselice, Christopher J.; Dye, Simon; Hopkins, Andrew M.; Liske, Jochen; Loveday, Jon; Norberg, Peder; Peacock, John A.; Croom, Scott M.; Frenk, Carlos S.; Graham, Alister W.; Jones, David Heath; Kuijken, Konrad; Madore, Barry F.; Nichol, Robert C.; Parkinson, Hannah R.; Phillipps, Steven; Pimbblet, Kevin A.; Popescu, Cristina C.; Prescott, Matthew; Seibert, Mark; Sharp, Robert G.; Sutherland, Will J.; Thomas, Daniel; Tuffs, Richard J.; Van Kampen, Eelco.

In: Monthly Notices of the Royal Astronomical Society, Vol. 412, No. 2, 01.04.2011, p. 765-769.

Research output: Contribution to journalArticle

Harvard

Hill, DT, Kelvin, LS, Driver, SP, Robotham, ASG, Cameron, E, Cross, NJG, Andrae, E, Baldry, IK, Bamford, SP, Bland-Hawthorn, J, Brough, S, Conselice, CJ, Dye, S, Hopkins, AM, Liske, J, Loveday, J, Norberg, P, Peacock, JA, Croom, SM, Frenk, CS, Graham, AW, Jones, DH, Kuijken, K, Madore, BF, Nichol, RC, Parkinson, HR, Phillipps, S, Pimbblet, KA, Popescu, CC, Prescott, M, Seibert, M, Sharp, RG, Sutherland, WJ, Thomas, D, Tuffs, RJ & Van Kampen, E 2011, 'Galaxy and Mass Assembly: FUV, NUV, ugrizYJHK Petrosian, Kron and Sérsic photometry', Monthly Notices of the Royal Astronomical Society, vol. 412, no. 2, pp. 765-769. https://doi.org/10.1111/j.1365-2966.2010.17950.x

APA

Hill, D. T., Kelvin, L. S., Driver, S. P., Robotham, A. S. G., Cameron, E., Cross, N. J. G., Andrae, E., Baldry, I. K., Bamford, S. P., Bland-Hawthorn, J., Brough, S., Conselice, C. J., Dye, S., Hopkins, A. M., Liske, J., Loveday, J., Norberg, P., Peacock, J. A., Croom, S. M., ... Van Kampen, E. (2011). Galaxy and Mass Assembly: FUV, NUV, ugrizYJHK Petrosian, Kron and Sérsic photometry. Monthly Notices of the Royal Astronomical Society, 412(2), 765-769. https://doi.org/10.1111/j.1365-2966.2010.17950.x

Vancouver

Hill DT, Kelvin LS, Driver SP, Robotham ASG, Cameron E, Cross NJG et al. Galaxy and Mass Assembly: FUV, NUV, ugrizYJHK Petrosian, Kron and Sérsic photometry. Monthly Notices of the Royal Astronomical Society. 2011 Apr 1;412(2):765-769. https://doi.org/10.1111/j.1365-2966.2010.17950.x

Author

Hill, David T. ; Kelvin, Lee S. ; Driver, Simon P. ; Robotham, Aaron S. G. ; Cameron, Ewan ; Cross, Nicholas J. G. ; Andrae, Ellen ; Baldry, Ivan K. ; Bamford, Steven P. ; Bland-Hawthorn, Joss ; Brough, Sarah ; Conselice, Christopher J. ; Dye, Simon ; Hopkins, Andrew M. ; Liske, Jochen ; Loveday, Jon ; Norberg, Peder ; Peacock, John A. ; Croom, Scott M. ; Frenk, Carlos S. ; Graham, Alister W. ; Jones, David Heath ; Kuijken, Konrad ; Madore, Barry F. ; Nichol, Robert C. ; Parkinson, Hannah R. ; Phillipps, Steven ; Pimbblet, Kevin A. ; Popescu, Cristina C. ; Prescott, Matthew ; Seibert, Mark ; Sharp, Robert G. ; Sutherland, Will J. ; Thomas, Daniel ; Tuffs, Richard J. ; Van Kampen, Eelco. / Galaxy and Mass Assembly : FUV, NUV, ugrizYJHK Petrosian, Kron and Sérsic photometry. In: Monthly Notices of the Royal Astronomical Society. 2011 ; Vol. 412, No. 2. pp. 765-769.

Bibtex

@article{c7e07e9b90a34f7f8c345e1483160d30,
title = "Galaxy and Mass Assembly: FUV, NUV, ugrizYJHK Petrosian, Kron and S{\'e}rsic photometry",
abstract = "In order to generate credible 0.1–2 μm spectral energy distributions, the Galaxy and Mass Assembly (GAMA) project requires many gigabytes of imaging data from a number of instruments to be reprocessed into a standard format. In this paper, we discuss the software infrastructure we use, and create self-consistent ugrizYJHK photometry for all sources within the GAMA sample. Using UKIDSS and SDSS archive data, we outline the pre-processing necessary to standardize all images to a common zero-point, the steps taken to correct for the seeing bias across the data set and the creation of gigapixel-scale mosaics of the three 4 × 12 deg2 GAMA regions in each filter. From these mosaics, we extract source catalogues for the GAMA regions using elliptical Kron and Petrosian matched apertures. We also calculate S{\'e}rsic magnitudes for all galaxies within the GAMA sample using sigma, a galaxy component modelling wrapper for galfit 3. We compare the resultant photometry directly and also calculate the r-band galaxy luminosity function for all photometric data sets to highlight the uncertainty introduced by the photometric method. We find that (1) changing the object detection threshold has a minor effect on the best-fitting Schechter parameters of the overall population (M*± 0.055 mag, α± 0.014, ϕ*± 0.0005 h3 Mpc−3); (2) there is an offset between data sets that use Kron or Petrosian photometry, regardless of the filter; (3) the decision to use circular or elliptical apertures causes an offset in M* of 0.20 mag; (4) the best-fitting Schechter parameters from total-magnitude photometric systems (such as SDSS modelmag or S{\'e}rsic magnitudes) have a steeper faint-end slope than photometric systems based upon Kron or Petrosian measurements; and (5) our Universe{\textquoteright}s total luminosity density, when calculated using Kron or Petrosian r-band photometry, is underestimated by at least 15 per cent. ",
author = "Hill, {David T.} and Kelvin, {Lee S.} and Driver, {Simon P.} and Robotham, {Aaron S. G.} and Ewan Cameron and Cross, {Nicholas J. G.} and Ellen Andrae and Baldry, {Ivan K.} and Bamford, {Steven P.} and Joss Bland-Hawthorn and Sarah Brough and Conselice, {Christopher J.} and Simon Dye and Hopkins, {Andrew M.} and Jochen Liske and Jon Loveday and Peder Norberg and Peacock, {John A.} and Croom, {Scott M.} and Frenk, {Carlos S.} and Graham, {Alister W.} and Jones, {David Heath} and Konrad Kuijken and Madore, {Barry F.} and Nichol, {Robert C.} and Parkinson, {Hannah R.} and Steven Phillipps and Pimbblet, {Kevin A.} and Popescu, {Cristina C.} and Matthew Prescott and Mark Seibert and Sharp, {Robert G.} and Sutherland, {Will J.} and Daniel Thomas and Tuffs, {Richard J.} and {Van Kampen}, Eelco",
year = "2011",
month = apr,
day = "1",
doi = "10.1111/j.1365-2966.2010.17950.x",
language = "English",
volume = "412",
pages = "765--769",
journal = "MNRAS",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "2",

}

RIS

TY - JOUR

T1 - Galaxy and Mass Assembly

T2 - FUV, NUV, ugrizYJHK Petrosian, Kron and Sérsic photometry

AU - Hill, David T.

AU - Kelvin, Lee S.

AU - Driver, Simon P.

AU - Robotham, Aaron S. G.

AU - Cameron, Ewan

AU - Cross, Nicholas J. G.

AU - Andrae, Ellen

AU - Baldry, Ivan K.

AU - Bamford, Steven P.

AU - Bland-Hawthorn, Joss

AU - Brough, Sarah

AU - Conselice, Christopher J.

AU - Dye, Simon

AU - Hopkins, Andrew M.

AU - Liske, Jochen

AU - Loveday, Jon

AU - Norberg, Peder

AU - Peacock, John A.

AU - Croom, Scott M.

AU - Frenk, Carlos S.

AU - Graham, Alister W.

AU - Jones, David Heath

AU - Kuijken, Konrad

AU - Madore, Barry F.

AU - Nichol, Robert C.

AU - Parkinson, Hannah R.

AU - Phillipps, Steven

AU - Pimbblet, Kevin A.

AU - Popescu, Cristina C.

AU - Prescott, Matthew

AU - Seibert, Mark

AU - Sharp, Robert G.

AU - Sutherland, Will J.

AU - Thomas, Daniel

AU - Tuffs, Richard J.

AU - Van Kampen, Eelco

PY - 2011/4/1

Y1 - 2011/4/1

N2 - In order to generate credible 0.1–2 μm spectral energy distributions, the Galaxy and Mass Assembly (GAMA) project requires many gigabytes of imaging data from a number of instruments to be reprocessed into a standard format. In this paper, we discuss the software infrastructure we use, and create self-consistent ugrizYJHK photometry for all sources within the GAMA sample. Using UKIDSS and SDSS archive data, we outline the pre-processing necessary to standardize all images to a common zero-point, the steps taken to correct for the seeing bias across the data set and the creation of gigapixel-scale mosaics of the three 4 × 12 deg2 GAMA regions in each filter. From these mosaics, we extract source catalogues for the GAMA regions using elliptical Kron and Petrosian matched apertures. We also calculate Sérsic magnitudes for all galaxies within the GAMA sample using sigma, a galaxy component modelling wrapper for galfit 3. We compare the resultant photometry directly and also calculate the r-band galaxy luminosity function for all photometric data sets to highlight the uncertainty introduced by the photometric method. We find that (1) changing the object detection threshold has a minor effect on the best-fitting Schechter parameters of the overall population (M*± 0.055 mag, α± 0.014, ϕ*± 0.0005 h3 Mpc−3); (2) there is an offset between data sets that use Kron or Petrosian photometry, regardless of the filter; (3) the decision to use circular or elliptical apertures causes an offset in M* of 0.20 mag; (4) the best-fitting Schechter parameters from total-magnitude photometric systems (such as SDSS modelmag or Sérsic magnitudes) have a steeper faint-end slope than photometric systems based upon Kron or Petrosian measurements; and (5) our Universe’s total luminosity density, when calculated using Kron or Petrosian r-band photometry, is underestimated by at least 15 per cent.

AB - In order to generate credible 0.1–2 μm spectral energy distributions, the Galaxy and Mass Assembly (GAMA) project requires many gigabytes of imaging data from a number of instruments to be reprocessed into a standard format. In this paper, we discuss the software infrastructure we use, and create self-consistent ugrizYJHK photometry for all sources within the GAMA sample. Using UKIDSS and SDSS archive data, we outline the pre-processing necessary to standardize all images to a common zero-point, the steps taken to correct for the seeing bias across the data set and the creation of gigapixel-scale mosaics of the three 4 × 12 deg2 GAMA regions in each filter. From these mosaics, we extract source catalogues for the GAMA regions using elliptical Kron and Petrosian matched apertures. We also calculate Sérsic magnitudes for all galaxies within the GAMA sample using sigma, a galaxy component modelling wrapper for galfit 3. We compare the resultant photometry directly and also calculate the r-band galaxy luminosity function for all photometric data sets to highlight the uncertainty introduced by the photometric method. We find that (1) changing the object detection threshold has a minor effect on the best-fitting Schechter parameters of the overall population (M*± 0.055 mag, α± 0.014, ϕ*± 0.0005 h3 Mpc−3); (2) there is an offset between data sets that use Kron or Petrosian photometry, regardless of the filter; (3) the decision to use circular or elliptical apertures causes an offset in M* of 0.20 mag; (4) the best-fitting Schechter parameters from total-magnitude photometric systems (such as SDSS modelmag or Sérsic magnitudes) have a steeper faint-end slope than photometric systems based upon Kron or Petrosian measurements; and (5) our Universe’s total luminosity density, when calculated using Kron or Petrosian r-band photometry, is underestimated by at least 15 per cent.

U2 - 10.1111/j.1365-2966.2010.17950.x

DO - 10.1111/j.1365-2966.2010.17950.x

M3 - Article

VL - 412

SP - 765

EP - 769

JO - MNRAS

JF - MNRAS

SN - 0035-8711

IS - 2

ER -

ID: 1436094