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Annual Review of Astronomy and Astrophysics

Volume 60, 2022

Photodissociation and X-Ray-Dominated Regions

Abstract

The radiation from stars and active galactic nuclei (AGNs) creates photodissociation regions (PDRs) and X-ray-dominated regions (XDRs), where the chemistry or heating is dominated by far-ultraviolet (FUV) radiation or X-ray radiation, respectively. PDRs include a wide range of environments, from the diffuse interstellar medium (ISM) to dense star-forming regions. XDRs are found in the center of galaxies hosting AGNs, in protostellar disks, and in the vicinity of X-ray binaries. In this review, we describe the dominant thermal, chemical, and radiation transfer processes in PDRs and XDRs, as well as give a brief description of models and their use for analyzing observations. We then present recent results from Milky Way, nearby extragalactic, and high-redshift observations.

Several important results include the following:

  • ▪  Velocity-resolved PDR lines reveal the kinematics of the neutral atomic gas and provide constraints on the stellar feedback process. Their interpretation is, however, in dispute, as observations suggest a prominent role for stellar winds, whereas they are much less important in theoretical models.
  • ▪  A significant fraction of molecular mass resides in CO-dark gas especially in low-metallicity and/or highly irradiated environments.
  • ▪  The CO ladder and [C]/[C] ratios can determine if FUV or X rays dominate the ISM heating of extragalactic sources.
  • ▪  With Atacama Large Millimeter/submillimeter Array, PDR and XDR tracers are now routinely detected on galactic scales over cosmic time. This makes it possible to link the star-formation history of the Universe to the evolution of the physical and chemical properties of the gas.
Keyword(s): active galactic nuclei, infrared emission, interstellar medium, star-forming regions
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2022-08-18
2025-06-13
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Photodissociation and X-Ray-Dominated Regions
Annual Review of Astronomy and Astrophysics 60, 247 (2022); https://doi.org/10.1146/annurev-astro-052920-010254
/content/journals/10.1146/annurev-astro-052920-010254
/content/journals/10.1146/annurev-astro-052920-010254
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Supplementary Data

  • Supplemental Video 1: Video of the [Cɪɪ] velocity channel maps of the Orion region. Several distinct kinematic structures are seen, including the expanding Veil shell in the south, the interaction with the molecular ridge (at v ～ 8 – 10 km s-1), and the expanding shell in the north surrounding NGC1977 (v ～ 12 km s-1). Video from Universität zu Koln/NASA/SOFIA, Pabst et al. (2020) and Higgins et al. (2021).

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