Galaxy redshift surveys with sparse sampling

Chi Ting Chiang, Philipp Wullstein, Donghui Jeong, Eiichiro Komatsu, Guillermo A. Blanc, Robin Ciardullo, Niv Drory, Maximilian Fabricius, Steven Finkelstein, Karl Gebhardt, Caryl Gronwall, Alex Hagen, Gary J. Hill, Inh Jee, Shardha Jogee, Martin Landriau, Erin Mentuch Cooper, Donald P. Schneide, Sarah Tuttle

Research output: Contribution to journalReview article

13 Citations (Scopus)

Abstract

Survey observations of the three-dimensional locations of galaxies are a powerful approach to measure the distribution of matter in the universe, which can be used to learn about the nature of dark energy, physics of inflation, neutrino masses, etc. A competitive survey, however, requires a large volume (e.g., V survey ∼ 10Gpc3) to be covered, and thus tends to be expensive. A ''sparse sampling'' method offers a more affordable solution to this problem: within a survey footprint covering a given survey volume, V survey, we observe only a fraction of the volume. The distribution of observed regions should be chosen such that their separation is smaller than the length scale corresponding to the wavenumber of interest. Then one can recover the power spectrum of galaxies with precision expected for a survey covering a volume of V survey (rather than the volume of the sum of observed regions) with the number density of galaxies given by the total number of observed galaxies divided by V survey (rather than the number density of galaxies within an observed region). We find that regularly-spaced sampling yields an unbiased power spectrum with no window function effect, and deviations from regularly-spaced sampling, which are unavoidable in realistic surveys, introduce calculable window function effects and increase the uncertainties of the recovered power spectrum. On the other hand, we show that the two-point correlation function (pair counting) is not affected by sparse sampling. While we discuss the sparse sampling method within the context of the forthcoming Hobby-Eberly Telescope Dark Energy Experiment, the method is general and can be applied to other galaxy surveys.

Original languageEnglish (US)
Article number030
JournalJournal of Cosmology and Astroparticle Physics
Volume2013
Issue number12
DOIs
StatePublished - Dec 1 2013

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sampling
galaxies
power spectra
dark energy
coverings
footprints
counting
neutrinos
universe
telescopes
deviation
physics

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics

Cite this

Chiang, Chi Ting ; Wullstein, Philipp ; Jeong, Donghui ; Komatsu, Eiichiro ; A. Blanc, Guillermo ; Ciardullo, Robin ; Drory, Niv ; Fabricius, Maximilian ; Finkelstein, Steven ; Gebhardt, Karl ; Gronwall, Caryl ; Hagen, Alex ; Hill, Gary J. ; Jee, Inh ; Jogee, Shardha ; Landriau, Martin ; Mentuch Cooper, Erin ; Schneide, Donald P. ; Tuttle, Sarah. / Galaxy redshift surveys with sparse sampling. In: Journal of Cosmology and Astroparticle Physics. 2013 ; Vol. 2013, No. 12.
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abstract = "Survey observations of the three-dimensional locations of galaxies are a powerful approach to measure the distribution of matter in the universe, which can be used to learn about the nature of dark energy, physics of inflation, neutrino masses, etc. A competitive survey, however, requires a large volume (e.g., V survey ∼ 10Gpc3) to be covered, and thus tends to be expensive. A ''sparse sampling'' method offers a more affordable solution to this problem: within a survey footprint covering a given survey volume, V survey, we observe only a fraction of the volume. The distribution of observed regions should be chosen such that their separation is smaller than the length scale corresponding to the wavenumber of interest. Then one can recover the power spectrum of galaxies with precision expected for a survey covering a volume of V survey (rather than the volume of the sum of observed regions) with the number density of galaxies given by the total number of observed galaxies divided by V survey (rather than the number density of galaxies within an observed region). We find that regularly-spaced sampling yields an unbiased power spectrum with no window function effect, and deviations from regularly-spaced sampling, which are unavoidable in realistic surveys, introduce calculable window function effects and increase the uncertainties of the recovered power spectrum. On the other hand, we show that the two-point correlation function (pair counting) is not affected by sparse sampling. While we discuss the sparse sampling method within the context of the forthcoming Hobby-Eberly Telescope Dark Energy Experiment, the method is general and can be applied to other galaxy surveys.",
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Chiang, CT, Wullstein, P, Jeong, D, Komatsu, E, A. Blanc, G, Ciardullo, R, Drory, N, Fabricius, M, Finkelstein, S, Gebhardt, K, Gronwall, C, Hagen, A, Hill, GJ, Jee, I, Jogee, S, Landriau, M, Mentuch Cooper, E, Schneide, DP & Tuttle, S 2013, 'Galaxy redshift surveys with sparse sampling', Journal of Cosmology and Astroparticle Physics, vol. 2013, no. 12, 030. https://doi.org/10.1088/1475-7516/2013/12/030

Galaxy redshift surveys with sparse sampling. / Chiang, Chi Ting; Wullstein, Philipp; Jeong, Donghui; Komatsu, Eiichiro; A. Blanc, Guillermo; Ciardullo, Robin; Drory, Niv; Fabricius, Maximilian; Finkelstein, Steven; Gebhardt, Karl; Gronwall, Caryl; Hagen, Alex; Hill, Gary J.; Jee, Inh; Jogee, Shardha; Landriau, Martin; Mentuch Cooper, Erin; Schneide, Donald P.; Tuttle, Sarah.

In: Journal of Cosmology and Astroparticle Physics, Vol. 2013, No. 12, 030, 01.12.2013.

Research output: Contribution to journalReview article

TY - JOUR

T1 - Galaxy redshift surveys with sparse sampling

AU - Chiang, Chi Ting

AU - Wullstein, Philipp

AU - Jeong, Donghui

AU - Komatsu, Eiichiro

AU - A. Blanc, Guillermo

AU - Ciardullo, Robin

AU - Drory, Niv

AU - Fabricius, Maximilian

AU - Finkelstein, Steven

AU - Gebhardt, Karl

AU - Gronwall, Caryl

AU - Hagen, Alex

AU - Hill, Gary J.

AU - Jee, Inh

AU - Jogee, Shardha

AU - Landriau, Martin

AU - Mentuch Cooper, Erin

AU - Schneide, Donald P.

AU - Tuttle, Sarah

PY - 2013/12/1

Y1 - 2013/12/1

N2 - Survey observations of the three-dimensional locations of galaxies are a powerful approach to measure the distribution of matter in the universe, which can be used to learn about the nature of dark energy, physics of inflation, neutrino masses, etc. A competitive survey, however, requires a large volume (e.g., V survey ∼ 10Gpc3) to be covered, and thus tends to be expensive. A ''sparse sampling'' method offers a more affordable solution to this problem: within a survey footprint covering a given survey volume, V survey, we observe only a fraction of the volume. The distribution of observed regions should be chosen such that their separation is smaller than the length scale corresponding to the wavenumber of interest. Then one can recover the power spectrum of galaxies with precision expected for a survey covering a volume of V survey (rather than the volume of the sum of observed regions) with the number density of galaxies given by the total number of observed galaxies divided by V survey (rather than the number density of galaxies within an observed region). We find that regularly-spaced sampling yields an unbiased power spectrum with no window function effect, and deviations from regularly-spaced sampling, which are unavoidable in realistic surveys, introduce calculable window function effects and increase the uncertainties of the recovered power spectrum. On the other hand, we show that the two-point correlation function (pair counting) is not affected by sparse sampling. While we discuss the sparse sampling method within the context of the forthcoming Hobby-Eberly Telescope Dark Energy Experiment, the method is general and can be applied to other galaxy surveys.

AB - Survey observations of the three-dimensional locations of galaxies are a powerful approach to measure the distribution of matter in the universe, which can be used to learn about the nature of dark energy, physics of inflation, neutrino masses, etc. A competitive survey, however, requires a large volume (e.g., V survey ∼ 10Gpc3) to be covered, and thus tends to be expensive. A ''sparse sampling'' method offers a more affordable solution to this problem: within a survey footprint covering a given survey volume, V survey, we observe only a fraction of the volume. The distribution of observed regions should be chosen such that their separation is smaller than the length scale corresponding to the wavenumber of interest. Then one can recover the power spectrum of galaxies with precision expected for a survey covering a volume of V survey (rather than the volume of the sum of observed regions) with the number density of galaxies given by the total number of observed galaxies divided by V survey (rather than the number density of galaxies within an observed region). We find that regularly-spaced sampling yields an unbiased power spectrum with no window function effect, and deviations from regularly-spaced sampling, which are unavoidable in realistic surveys, introduce calculable window function effects and increase the uncertainties of the recovered power spectrum. On the other hand, we show that the two-point correlation function (pair counting) is not affected by sparse sampling. While we discuss the sparse sampling method within the context of the forthcoming Hobby-Eberly Telescope Dark Energy Experiment, the method is general and can be applied to other galaxy surveys.

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