Galaxy Environment: Difference between revisions
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Very broadly, measurements of clustering contain information about information about galaxy environment on small (~<1Mpc) scales, and information about cosmology on large (~>1Mpc) scales | |||
'''Examples of Work by Current or Former Group Members in this Area''' | |||
[https://arxiv.org/abs/2009.01817 Cross-correlating radio continuum surveys and CMB lensing: constraining redshift distributions, galaxy bias and cosmology] | |||
[https://arxiv.org/abs/1711.05201 The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field] | |||
[https://arxiv.org/abs/1702.03309 The environment and host haloes of the brightest z~6 Lyman-break galaxies] | [https://arxiv.org/abs/1702.03309 The environment and host haloes of the brightest z~6 Lyman-break galaxies] | ||
[https://arxiv.org/abs/1606.08989 Environmental Quenching and Galactic Conformity in the Galaxy Cross-Correlation Signal] | |||
[https://arxiv.org/abs/1511.05476 The galaxy-halo connection in the VIDEO Survey at 0.5<z<1.7] | |||
[https://arxiv.org/abs/ | [https://arxiv.org/abs/1403.0882 Evolution in the bias of faint radio sources to z ~ 2.2] | ||
[https://arxiv.org/abs/1402.5654 Galaxy and Mass Assembly (GAMA): The evolution of bias in the radio source population to z ~ 1.5] | |||
Revision as of 15:00, 18 November 2020
The environment of a galaxy is a key factor in determining the evolution of galaxies. This can be measured in a number of ways
One key is the galaxy-halo connection; how the dark matter halo that a galaxy is in affects its evolution.
Typically this requires assuming some knowledge of the underlying dark matter distribution, and then measuring some properties of the galaxy population and constraining what the relationship could be.
This can be probed in a number of ways:
- Galaxy number counts; if the comoving number density of galaxies
- Galaxy-galaxy clustering; measuring the correlation function/power spectrum of galaxies, often in angular space
- Galaxy-galaxy lensing; measure the correlation between galaxies and the shear on background galaxies from gravitational lensing
Very broadly, measurements of clustering contain information about information about galaxy environment on small (~<1Mpc) scales, and information about cosmology on large (~>1Mpc) scales
Examples of Work by Current or Former Group Members in this Area
The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field
The environment and host haloes of the brightest z~6 Lyman-break galaxies
Environmental Quenching and Galactic Conformity in the Galaxy Cross-Correlation Signal
The galaxy-halo connection in the VIDEO Survey at 0.5<z<1.7
Evolution in the bias of faint radio sources to z ~ 2.2
Galaxy and Mass Assembly (GAMA): The evolution of bias in the radio source population to z ~ 1.5