David Thomas Hill PhD Thesis - Research@StAndrews:FullText ...

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1.1. A brief history of galaxy detection As survey astronomy extended its range beyond visible light, it was a small step to define spectroscopic surveys using other parts of the electromagnetic spectrum. The IRAS redshift survey sample (Fisher et al., 1995) was defined using 60µm observations, producing a coherent sample across the entire sky, including the optical ”zone of avoidance”. Further advances were made in optical astronomy. The Las Campanas Survey (Oemler etal.,1993),utilisedafibre-fedspectrographthatcouldsimultaneouslymeasurespectrafor 100 objects. The 2dF galaxy redshift survey (2dFGRS, Colless et al. 2001) went further, utilising the AAT’s 2dF multifibre spectrograph to simultaneously observe 400 sources. The 2dFGRS sample was taken from the APM galaxy catalogue (Maddox et al., 1990). Over 200 thousand galaxy spectra were observed, within 2000sqdeg of sky, to a limiting magnitude of mbj = 19.45mag. SDSS (York et al., 2000), as well as being a large area photometric survey, also produced spectra for over 1.6million sources, including 930 thousand galaxies (Strauss et al., 2002), with their main sample complete to mr = 17.77mag. Within 20 years, the number of galaxy redshifts detected had increased by 2 orders of magnitude. The sky distribution of bright sources had become well measured. However, extragalactic astronomy, particular theories of groups and mergers, always needs observations that are deeper, in order to examine clusters of galaxies in greater detail. The MGC (Liske et al., 2003) was a deeper survey, covering a 37.5sqdeg area within both 2dF and SDSS surveys. A highly complete (> 99%) photometric survey covering all galaxies brighter than mB = 20mag, the MGC combined redshifts from the literature (including 2dF and SDSS sources) with its own specific redshift survey (Driver et al., 2005). Its purpose was to examine a segment of the local Universe to a depth beyond the capabilities of 2dF and SDSS, and to deduce any inaccuracy within those datasets (Cross et al., 2004). MGC data is used within this thesis (in Chapter 3), and the survey is discussed in further detail in Section 2.1. The GAMA survey (Driver et al., 2010) is a larger, slightly deeper follow up to the MGC survey. Providing spectra for an highly complete (∼ 98%), magnitude limited (mr < 19.4mag) sample of over 100 thousand galaxies over 144sqdeg of sky, GAMA is an attempt to probe deeper than SDSS whilst still limiting the effects of cosmic variance. GAMA’s region of coverage is also within the area probed by SDSS and 2dF (with partial coverage by MGC), with over 17 thousand sources within its sample having existing spectroscopy. GAMA data is used within this thesis, and the survey is discussed in further detail in Section 2.4. 9
Chapter 1. Introduction: The luminosity distribution and total luminosity density of galaxies Figure 1.3: The sky position of the GAMA, SDSS main redshift survey, MGC and 2dFGRS datasets. Taken from Driver et al. (2010), with the author’s permission. 10
Page 1 and 2: THE OPTICAL AND NIR LUMINOUS ENERGY
Page 4: Declaration I, David Thomas Hill, h
Page 8: Abstract Theories of how galaxies f
Page 11 and 12: the American Museum of Natural Hist
Page 13 and 14: 3.4 The CSED points from the MGC-SD
Page 15 and 16: 2.1 Coverage of the equatorial regi
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Page 21 and 22: 5.12 A comparison between the best-
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Page 26 and 27: List of Tables 2.1 The Absolute mag
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B MGC − K MGC B MGC − H MGC 6 5
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3.2. Generation of the luminosity d
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N dm (deg −2 (0.5mag) −1 ) 0.1
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3.2.3 Normalisation 3.2. Generation
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3.3. ugrizYJHK luminosity functions
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3.3. ugrizYJHK luminosity functions
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-1.4 -1.2 -1 -0.8 -0.6 Smith et al
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3.4. The CSED points from the MGC-S
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4 The GAMA ugrizYJHK sample: Creati
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Frequency Frequency Frequency Frequ
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4.1. Consistent NIR and optical pho
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4.1. Consistent NIR and optical pho
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4.2. Photometry used to cut the lon
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4.2. Photometry Figure 4.4: A compa
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4.2. Photometry will be missed desp
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N(m) dm 5000 1000 500 100 50 Detect
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4.3. Testing the GAMA catalogues de
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4.3. Testing the GAMA catalogues so
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4.3. Testing the GAMA catalogues Ba
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4.3. Testing the GAMA catalogues Ty
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4.4. Properties of the catalogues s
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4.4. Properties of the catalogues B
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uSDSS − ur defined AUTO gSDSS −
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uSDSS − uself defined PETRO gSDSS
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uSDSS,cmodel − uSersic gSDSS,cmod
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Colour Photometry σ1 σ2 (mag) (ma
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4.4. Properties of the catalogues F
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4.5. Final GAMA photometry apparent
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4.5. Final GAMA photometry Figure 4
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4.5.2 ‘Fixed aperture’ Sérsic
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strip. The SExtractor error is calc
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σ SDSS, all Auto and all Petro mag
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4.5. Final GAMA photometry A deviat
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4.5. Final GAMA photometry u (mag)
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4.5. Final GAMA photometry J (mag)
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4.5. Final GAMA photometry Figure 4
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5 The GAMA ugrizYJHK sample: Statis
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5.1. The impact of the photometric
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143 Magnitude system Sources M ∗
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5.1. The impact of the photometric
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5.2. The effects of surface brightn
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Spectroscopic completeness 5.2. The
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e μPetro,r,50(mag arcsec −2 ) 5.
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165 Photometry Sources M ∗ −5lo
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μ r (mag arcsec −2 ) 16 18 20 22
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μ r (mag arcsec −2 ) μ r (mag a
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5.3. Comparisons with previous surv
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5.3. Comparisons with previous surv
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μ g (mag arcsec −2 ) 18 20 22 5.
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Quality of modified-model fits 5.3.
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5.4. Calculation of total luminosit
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185 Photometry M ∗ −5log 10(h)
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μ g (mag arcsec −2 ) μ g (mag a
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Band MGC-SDSS-UKIDSS LF j (×108h L
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6 Summary In this chapter I outline
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6.1. Results 0.001h 3 Mpc −3 ). H
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6.2. Further work enough, particula
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Deeper data 6.2. Further work Unfor
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In this appendix I derive Equation
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B Variation between passbands In th
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Figure B.1: The effects of convolut
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C Visibility theory In this appendi
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C.2 Modifications for GAMA C.2. Mod
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e μPetro,r,50(mag arcsec −2 ) M
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fibermag aperture: h(r) = � r=1.5
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D BBDs from the data and the best f
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μ g (mag arcsec −2 ) μ g (mag a
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μ z (mag arcsec −2 ) μ z (mag a
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μ J (mag arcsec −2 ) μ J (mag a
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μ K (mag arcsec −2 ) μ K (mag a
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[1] - http://www.eso.org/∼jliske/
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Benson, A. J., Bower, R. G., Frenk,
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Diehl, R. et al. 2006, Nature, 439,
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Hoskin, M. A. 1976, Journal for the
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Martin, N. F., Ibata, R. A., Bellaz
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Shapley, H., & Ames, A. 1932, Annal
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