EXERCISES AND PROBLEM SETS
QUASAR ABSORPTION LINES
Volume 1, Part 3
Chapter 16
Groups and Clusters
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Review Questions
When multiple galaxies might be contributing to a single absorber, it is challenging to assign which galaxy is giving rise to the absorption. What are five possible strategies for selecting which galaxy to assign as the galaxy-absorber pair? What are some pros and cons to such "arbitrary" assignments?
Describe the French-Wakker likelihood parameter. What are some shortcomings of adopting this approach?
Is it reasonable to conclude that an absorber in a group environment does not arise from the CGM of any single galaxy or even from the CGM of any of the galaxies in the group? If so, give an example scenario and explain.
For MgII absorbers, describe the key findings about how the absorption strengths and kinematics differ in group environments as compared to in the CGM of "isolated" galaxies? What are some possible interpretations explaining these differences?
Repeat Question 4 for OVI absorbers. Review/describe the evidence that OVI absorbers may have a "mixed" origin in group environments?
Describe that nature of observed HI absorption in and around clusters, including the column density, equivalent width, and covering fraction distributions as a function of impact parameter in units of virial radii. Consider Figure 16.7(c) and the predicted fraction of gas phases as a function of impact parameter in units of virial radii. Compare and contrast the observed HI distributions with the theoretical predictions. Do they align with one another, or do they seem to be in conflict? Explain.
Repeat Question 6, but for MgII absorption.
Repeat Question 6, but for CIV and OVI absorption.
Consider the TNG100 simulations presented in Figure 16.14. In terms of spatial distributions and halo masses, describe where would you the expect to find OVI distributed within the cluster environment, as opposed to OVII and OVIII. For Figure 16.14(c,d), explain how the flattening of the cumulative bound mass of OVI bearing gas with increasing halo mass is consistent with the peak in the average column density of OVI at a halo mass of 1012 solar masses.
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