![]() (greater then 1500M/yr), and they exhibit behaviour similar to sub-mm galaxies. With those sources with continuum measurements, high SFRs were found ![]() That environmental processes are already at work. Have gas fractions that fall below what is seen in field galaxies. These galaxies are undergoing a period of extreme star formation. These gas fractions fall below expected scaling relations, and could show that The CO spectra) and stellar masses (from Spitzer IRAC data) I find gas fractions of Is the progenitor to a Coma like cluster. ~570 km/s, which corresponds to a mass of ~2.5x10^13M. With 10 sources being a part of the structure.įrom the cluster members I estimate a velocity dispersion for the cluster of Using velocity dispersions I assign proto-cluster membership, To all the sources, I identified an over-density at redshift 3.64, which I take as the Identify any potential spectral lines in the ALMA data, and identified 57 detections with a S/N greater than 4 (six of these are associated with continuum sources). I used a match filter technique to try and Using band 3 ALMA spectral scans, I searched for a potential proto-cluster inĪn over-density of red Herschel sources. Mass has an effect on the galaxies that reside within it. Since the mass of JKCS041 is significantly larger then otherĬlusters at this redshift, it could show some of the first direct evidence that a clusters JKCS041 on the other handĭeviates significantly. Seems to follow expected scaling relations for clusters. When comparing these clusters to other high redshift clusters, I see that CLJ1449 Galaxies within are being quenched and the environment is having a profound effect. With very few galaxies exhibiting star-burst behaviour. For JKCS041, the majority of galaxies lie below the main sequence, The lowest stellar masses, which could indicate environmental influences quenching Thereĭoes appear to be a radial trend, with those galaxies closest to the cluster core showing Main sequence, or just above it in a region dominated by star burst galaxies. For CLJ1449, I find that all the cluster galaxies either exist on the galaxy When I look at the SFR-stellar mass relation I find a deviation between the twoĬlusters. Regions of the cluster (opposed to what happens in local clusters). ![]() Of these clusters, and the majority of the star formation is occurring in the densest This indicates that there is indeed a reversal in the SFR-density relation in both Which are five orders of magnitude greater then expected field values. When converted to a SFR-density this gives In the central 0.5Mpc region I find SFRs of 800 +/- 200 M/yr for CLJ1449,Īnd 770 +/- M/yr for JKCS041. Star formation rates (SFRs) between 12-1600M/yr over the entire 3Mpc radial Rates and stellar masses for all our cluster members. ![]() Using archival opticalĪnd near-infrared data with the energy-balance code CIGALE I calculate star formation The Bayesian inference tool XID+ to estimate fluxes for them. Using high-resolution Atacama Large Millimetre Array (ALMA)Īnd Jansky Very Large Array data I identify potentially confused galaxies, and use Of two mature, high redshift galaxy clusters, CLJ1449 (at redshift two) and JKCS041 Using SCUBA-2 and Herschel data I investigate the star forming properties Processes effect the evolutionary path a galaxy is on. Potential environmental effects on cluster galaxies, and see if and how these (FIR) and Sub-millimeter (sub-mm) observations. This thesis aims to investigate high redshift galaxy clusters, focusing on Far Infrared PDF (Cardiff University Electronic Publication Form) Available under License Creative Commons Attribution No Derivatives.
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