Review Questions

1. Consider Figure 14.1, which shows HI, SiII, SiIII, SiIV, CII, CIV, and OVI absorption over a range of impact parameters through many galaxies.  (i) What are some general insights we gain from this figure?  (ii) What can the relative strengths of SiII, SiIII, and SiIV tell us? (iii) What type of gas (density, temperature) and ionization conditions in the CGM do we learn about if we focus on SiII and CII absorption? If we focus on SiIV and CIV absorption?  If we focus on OVI absorption? 

2. As discussed at length in Sections 14.1-14.4 in this chapter, many investigations of the CGM for z < 2 have focused on several individual ion: (1) HI, (2) MgII, (3) CIV, (4) OVI, and (5) NeVIII.  Absorption properties of each ion are studied spatially around galaxies as a function of (1) impact parameter, (ii) galaxy stellar mass, (3) halo mass, (4) star formation rate, (5) specific star formation rate, and (6) redshift. Construct a table with 6 rows, one for each ion, and 4 columns, one for each galaxy property. In each table cell, briefly summarize the key highlight(s) of what has been observationally documented/learned about the CGM and galaxy properties. [The point of this question is not to detail every observation; it is to consider all observations and synthesize them into a concise "10,000 foot" narrative that captures the most important astrophysical connections between the CGM seen in these ions and their host galaxies.]

3. In the spirit of Question2 above, now do the same for the observations described in Section 14.5 for z > 2 galaxy-absorber pairs, LBGs, and LAEs.

4. Describe what "morphokinematic analysis" is. What measured galaxy and absorption quantities are required in order undertake morphokinematic analysis?  What are some key results from such studies?

5. Describe what "morphospatial analysis" is. What are some key results from such studies?

Problems

1. Under construction