Abstract
Galactic accretion interacts in complex ways with gaseous halos, including galactic winds. As a result, observational diagnostics typically probe a range of intertwined physical phenomena. Because of this complexity, cosmological hydrodynamic simulations have played a key role in developing observational diagnostics of galactic accretion. In this chapter, we review the status of different observational diagnostics of circum-galactic gas flows, in both absorption (galaxy pair and down-the-barrel observations in neutral hydrogen and metals; kinematic and azimuthal angle diagnostics; the cosmological column density distribution; and metallicity) and emission (Lyα; UV metal lines; and diffuse X-rays). We conclude that there is no simple and robust way to identify galactic accretion in individual measurements. Rather, progress in testing galactic accretion models is likely to come from systematic, statistical comparisons of simulation predictions with observations. We discuss specific areas where progress is likely to be particularly fruitful over the next few years.
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Notes
- 1.
Galactic disks are better traced by damped Lyα absorbers (DLAs; N HI ≥ 2 × 1020 cm−2; e.g., Wolfe et al. 2005; Neeleman et al. 2015). At very high redshift, the increased cosmic mean density and declining cosmic ultraviolet background (UVB) cause absorbers of fixed HI column to probe structures more closely associated with the low-density IGM with increasing redshift (e.g., McQuinn et al. 2011). As a result, LLSs become associated with structures such as intergalactic filaments and some DLAs may arise in the CGM. There rapid increase in LLS incidence observed at \(z\gtrsim 3.5\) suggests that LLSs commonly arise outside galaxy halos at these redshifts (Fumagalli et al. 2013) while the rapid evolution of the DLA metallicity distribution at \(z\gtrsim 5\) suggest that DLAs at these redshifts commonly arise outside galaxies (Rafelski et al. 2014).
- 2.
See the FIRE project web site at http://fire.northwestern.edu.
- 3.
- 4.
In galaxy pair experiments, an outflowing absorber located behind the foreground galaxy would also appear redshifted. This introduces a generic ambiguity in the interpretation of absorption lines transverse to foreground galaxies.
- 5.
Absent hydrodynamic interactions and angular momentum, the radial velocity would be simply equal to the velocity of free fall into halo. Current cosmological simulations indicate that asymptotic cold stream radial velocities are typically closer to half the halo circular velocity (Kereš et al. 2005; Goerdt and Ceverino 2015).
- 6.
If the stellar light of a galaxy were concentrated in a point source and the ISM were rotating in perfectly circular motion around the center, then the ISM would move purely tangentially with respect to the light source and could not mimic infalling gas. In real galaxies, stellar light is, however, spatially extended and the internal dynamics and morphology of the ISM can be quite complex. For example, at z ∼ 2 the nebular line emission of galaxies is often very clumpy (e.g., Förster Schreiber et al. 2009). These effects could cause some ISM gas to appear as infalling.
- 7.
Note, however, that the two types of observations are not equivalent since down-the-barrel spectra are always sensitive to high-density material near (or within) the target galaxy, while transverse spectra only probe the CGM at distances from the galaxy equal to the impact parameter or greater.
- 8.
This is not to say that infalling cool gas solely determines the angular momentum of disk galaxies. In an analysis of the Illustris simulation, Zjupa and Springel (2017) identify the important roles of specific angular momentum transfer from dark matter onto gas during mergers and from feedback expelling low specific angular momentum gas from halos.
- 9.
In the updated z ≤ 1 metallicity analysis of Wotta et al. (2016), the statistical evidence for a bimodality is strongest for a subsample restricted to partial LLSs, with 16. 2 ≤ logN HI ≤ 17. 2.
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Acknowledgements
We are grateful to many colleagues and collaborators who have helped shape our views on galactic accretion, including: Chuck Steidel, Gwen Rudie, Alice Shapley, Xavier Prochaska, Joe Hennawi, Michele Fumagalli, Nicolas Lehner, Chris Howk, Lars Hernquist, Joop Schaye, Freeke van de Voort, Andrey Kravtsov, Cameron Liang, Mark Dijkstra, Norm Murray, Eliot Quataert, Dusan Kereš, Phil Hopkins, Alexander Muratov, Daniel Anglés-Alcázar, and Zach Hafen. Our research on galactic accretion has been supported by NSF and NASA.
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Faucher-Giguère, CA. (2017). Observational Diagnostics of Gas Flows: Insights from Cosmological Simulations. In: Fox, A., Davé, R. (eds) Gas Accretion onto Galaxies . Astrophysics and Space Science Library, vol 430. Springer, Cham. https://doi.org/10.1007/978-3-319-52512-9_12
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