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Annual Review of Astronomy and Astrophysics

Volume 55, 2017

The Circumgalactic Medium

Abstract

The gas surrounding galaxies outside their disks or interstellar medium and inside their virial radii is known as the circumgalactic medium (CGM). In recent years this component of galaxies has assumed an important role in our understanding of galaxy evolution owing to rapid advances in observational access to this diffuse, nearly invisible material. Observations and simulations of this component of galaxies suggest that it is a multiphase medium characterized by rich dynamics and complex ionization states. The CGM is a source for a galaxy's star-forming fuel, the venue for galactic feedback and recycling, and perhaps the key regulator of the galactic gas supply. We review our evolving knowledge of the CGM with emphasis on its mass, dynamical state, and coevolution with galaxies. Observations from all redshifts and from across the electromagnetic spectrum indicate that CGM gas has a key role in galaxy evolution. We summarize the state of this field and pose unanswered questions for future research.

Keyword(s): cosmology, galaxies, galaxy evolution, gas
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2017-08-18
2024-04-19
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/content/journals/10.1146/annurev-astro-091916-055240
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The Circumgalactic Medium
Annual Review of Astronomy and Astrophysics 55, 389 (2017); https://doi.org/10.1146/annurev-astro-091916-055240
/content/journals/10.1146/annurev-astro-091916-055240
/content/journals/10.1146/annurev-astro-091916-055240
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Supplemental Material

Supplementary Data

  • Download Supplemental Figure 1: Different circumgalactic medium observing techniques. The example emission line map is adapted from Corlies & Schiminovich (2016) with permission (PDF).

    Download Supplemental Figure 2: Same as Figure 3 but with options to scale fully within the virial radius and within 1 Mpc comoving. The halo has masses log Mhalo = 11.67, 12.0, 12.1, and 12.33 at z = 3, 2, 1, and 0, respectively (PDF).

    Download Supplemental Figure 4: Same as Figure 6 but broken down by element. Hovering over each ion gives the ionization energy for that species (higher ionization energies tend to trace hotter, more rarefied gas) and the wavelengths and oscillator strengths for a selection of strong and/or commonly observed lines (PDF).

    All of the above PDFs are best viewed in Adobe Acrobat Reader.

  • Article Type: Review Article

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