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

5.17 The distribution of local galaxies from Karachentsev et al. (2004), relative
to the g band BBDs for the deeper sample. The local galaxies are shown as
purpledots. Thetopfigureshowsthefittothemodified-modelfunction, the
bottom figure the fit to the Choloniewski function. The purple dots denotes
the region the SWML algorithm was limited to. The red line denotes the
region that has complete coverage within a 30000Mpc 3 volume. . . . . . . 187
5.18 The variation in νf(ν) with wavelength. Five datasets are shown. The orange
datapoints are derived by summing the luminosity density within the
bins the BBD sampled (this method therefore ignores all luminosity density
outside the sampled region). Red datapoints are taken from the integration
of the best fitting Choloniewski parameters (Table 5.12), blue datapoints
from the integration of the best fitting modified-model parameters (also Table
5.12), green datapoints from the GAMA CSED paper (Driver, in prep),
and black datapoints from the MGC-SDSS-UKIDSS sample of Chapter 3
(also shown in Table 5.13). Errors for the red dataset are shown, in order
to provide a guide to the uncertainty on each datapoint. . . . . . . . . . . . 190
5.19 Cosmic energy output from 0.1 to 3µm. The model line shows the SED of
a 13.2Gyr Sa-type galaxy from the spectral template library of Poggianti
(1997). Data shown is taken from Baldry et al. (2005), Bell et al. (2003),
Blanton et al. (2003), Budavári et al. (2005), Cole et al. (2001), Driver et al.
(2007), Eke et al. (2005), Jones et al. (2006), Huang et al. (2003), Kochanek
etal.(2001),Montero-Dortaetal.(2008),Norbergetal.(2002),Treyeretal.
(2005) and Zucca et al. (1997). The GAMA BBD dataset (green) uses the
νf(ν) results provided by the integration of the modified model function,
shown in Table 5.12. The MGC-SDSS-UKIDSS data (black) is taken from
Chapter 3. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 192
5.20 The variation in νf(ν) with wavelength, compared with predictions from
different CSFH+IMF combinations (Wilkins, priv. comm.), and datapoints
from other measurements. Hollow points show the position of the data
when it is corrected for the effects of dust attenuation, using multiplying
factors taken from Driver et al. (2008). Uncertainties are calculated from
the 90% confidence intervals on the best-fitting parameters. CSFH models
are taken from Wilkins et al. (2008a). IMF models come from Wilkins et al.
(2008b) (WTH08), or Hopkins & Beacom (2006) (HB06). Red datapoints
are taken from this paper (the modified-model parameters in Table 5.12),
green datapoints from the GAMA CSED paper (Driver, in prep), and black
datapoints from the MGC-SDSS-UKIDSS sample of Chapter 3. . . . . . . . 193
B.1 The effects of convolution and the change in passband of observations of
SDSS object 588848900968480848. . . . . . . . . . . . . . . . . . . . . . . . 207
C.1 Redshift completeness limits due to the GAMA Petrosian magnitude selection
in the M,µ X plane. The redshift limit colours range from z = 0.5
(red), to z = 0 (orange). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 213