Galaxy Environment: Difference between revisions
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The environment of a galaxy | The environment of a galaxy can be a [https://ui.adsabs.harvard.edu/abs/2013pss6.book..207V/abstract key factor] in determining the evolution of galaxies. The environment of a galaxy is a multi-faceted property and can be quantified and interpreted in a large number of different ways depending on observations available and given science goal. | ||
'''Partial List of Probes of Environment''' | |||
- N-th Nearest Neighbour | |||
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. | - Fixed Aperture Measures | ||
- Correlation Functions, power spectra, counts-in-cells | |||
- Identifying Groups, Clusters, Filaments, Voids | |||
- Complementary observations of local gas content etc. | |||
'''Galaxy Halo Connection''' | |||
One key perspective on environment is the [https://arxiv.org/abs/1804.03097 galaxy-halo connection]; how the dark matter halo that a galaxy is in affects its evolution and determines its properties. | |||
Typically this requires assuming some knowledge of the underlying dark matter halo 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: | This can be probed in a number of ways: | ||
- Galaxy number counts; | - Galaxy number counts; the comoving number density of galaxies | ||
- Galaxy-galaxy clustering; measuring the correlation function/power spectrum of galaxies, often in angular space | - Galaxy-galaxy clustering; measuring the correlation function/power spectrum of galaxies, often in angular space | ||
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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 | |||
Some broader notes about galaxy clustering and correlation functions: [[File:Clustering notes small PH.pdf]] | |||
'''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/2009.05548 Formation of S0s in extreme environments II: the star-formation histories of bulges, discs and lenses] | |||
[https://arxiv.org/abs/1909.03843 Comparing Galaxy Clustering in Horizon-AGN Simulated Lightcone Mocks and VIDEO Observations] | |||
[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/1810.08507 PKSB1740-517: An ALMA view of the cold gas feeding a distant interacting young radio galaxy] | |||
[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/ | [https://arxiv.org/abs/1511.05476 The galaxy-halo connection in the VIDEO Survey at 0.5<z<1.7] | ||
[https://arxiv.org/abs/1511.03067 Tracing the neutral gas environments of young radio AGN with ASKAP] | |||
[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] | |||
[https://arxiv.org/abs/1302.2010 Sample variance, source clustering and their influence on the counts of faint radio sources] | |||
[https://arxiv.org/abs/astro-ph/0312215 The environments of hyperluminous infrared galaxies at 0.44<z<1.55] | |||
Latest revision as of 18:35, 7 Haziran 2021
The environment of a galaxy can be a key factor in determining the evolution of galaxies. The environment of a galaxy is a multi-faceted property and can be quantified and interpreted in a large number of different ways depending on observations available and given science goal.
Partial List of Probes of Environment
- N-th Nearest Neighbour
- Fixed Aperture Measures
- Correlation Functions, power spectra, counts-in-cells
- Identifying Groups, Clusters, Filaments, Voids
- Complementary observations of local gas content etc.
Galaxy Halo Connection
One key perspective on environment is the galaxy-halo connection; how the dark matter halo that a galaxy is in affects its evolution and determines its properties.
Typically this requires assuming some knowledge of the underlying dark matter halo 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; 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
Some broader notes about galaxy clustering and correlation functions: File:Clustering notes small PH.pdf
Examples of Work by Current or Former Group Members in this Area
Comparing Galaxy Clustering in Horizon-AGN Simulated Lightcone Mocks and VIDEO Observations
The clustering and bias of radio-selected AGN and star-forming galaxies in the COSMOS field
PKSB1740-517: An ALMA view of the cold gas feeding a distant interacting young radio galaxy
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
Tracing the neutral gas environments of young radio AGN with ASKAP
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
Sample variance, source clustering and their influence on the counts of faint radio sources
The environments of hyperluminous infrared galaxies at 0.44<z<1.55