Abstract
The discovery that Cosmic Infra-red Background (CIB, e.g. Puget et al. (1996), Fixsen et al. 1998) had a similar energy density to the UV optical background implies that a significant proportion of the star formation over the history of the Universe has been obscured by dust.
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Notes
- 1.
The content of this Chapter (with the exception of Sect. 4.4.4) is based on the article Cowley et al. ‘The clustering evolution of dusty star-forming galaxies’, Monthly Notices of the Royal Astronomical Society, Volume 461, Issue 2, p.1621–1641, published 6 May 2016. Reproduced with permission. All rights reserved, https://doi.org/10.1093/mnras/stw1069. The content of Sect. 4.4.4 is based on the article Cowley et al. ‘Blending bias impacts the host halo masses derived from a cross correlation analysis of bright submillimetre galaxies’, Monthly Notices of the Royal Astronomical Society, Volume 469, Issue 3, p.3396–3404, published 19 April 2017. Reproduced with permission. All rights reserved, https://doi.org/10.1093/mnras/stx928.
- 2.
Large APEX (Atacama Pathfinder EXperiment) Bolometer Camera Array (LABOCA) Extended Chandra Deep Field South (ECDFS) Sub-millimetre Survey.
- 3.
The luminosity at which the infra-red luminosity functions predicted by our model become dominated by starburst galaxies is dependent on redshift. For example, at \(z=0\) the luminosity function is dominated by starbursts for \(L_\mathrm{IR}\gtrsim 10^{11.3}\)Â \(h^{-2}\)Â L\(_{\odot }\), at \(z=4.9\) this limit is \(L_\mathrm{IR}\gtrsim 10^{10.5}\)Â \(h^{-2}\)Â L\(_{\odot }\).
- 4.
Analogously to the spatial case, at \(\theta =0\) the correlation function is described by a Dirac delta function, \(\delta ^\mathrm{D}(\theta )/\eta \), which is referred to as the shot noise term.
- 5.
This does not include any treatment of gravitational lensing.
- 6.
In Chap. 3 we showed that this confusion effect boosts the cumulative 850 \(\upmu \)m number counts by a factor of \(\sim 2\) at \(S_{850\upmu \mathrm m}=4\) mJy for a 15 arcsec FWHM beam. See also Hayward et al. (2013) and Muñoz Arancibia et al. (2015) who investigate the effect of coarse angular resolution on the observed sub-mm number counts.
- 7.
Here we use a limit of 2, rather than 4 mJy, so we have enough objects for a robust determination of \(w_\mathrm{cross}\). We do not expect the result to be sensitive to this given that the auto-correlation of galaxies is roughly independent of flux over this flux range.
- 8.
United Kingdom Infra-red Telescope (UKIRT) Infra-red Deep Sky Survey – Ultra Deep Survey.
- 9.
In principle these could be derived from lightcone catalogues giving essentially identical results, however we prefer using Limber’s equation as it utilises all of the clustering information available in our simulation volume.
- 10.
In this Section, for ease of reading, and as here we are only considering a single band (850Â \(\upmu \)m), we suppress the explicit frequency dependence in our notation. For example, we write the mean intensity at a given observed frequency \(\nu \), \(\langle I_\nu \rangle \), as \(\langle I\rangle \).
- 11.
We use this convention as it is the standard practice for angular power spectra of CIB anisotropies (e.g. Gautier et al. 1992; Viero et al. 2009). Under this convention the angular wavenumber is related to the multipole index, \(\ell \), by \(\ell =2\pi k_{\theta }\) (when angles are measured in radians).
- 12.
Imposing the limit \(S_\mathrm{cut}\) is necessary as for Euclidean number counts (\(\mathrm{d}\eta /\mathrm{d}S\propto S^{-2.5}\)) the integral in equation (4.5.23) does not converge.
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Cowley, W. (2017). The Clustering Evolution of Dusty Star-Forming Galaxies. In: The Nature of Dusty Star-Forming Galaxies. Springer Theses. Springer, Cham. https://doi.org/10.1007/978-3-319-66748-5_4
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DOI: https://doi.org/10.1007/978-3-319-66748-5_4
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