THE GALACTIC CENTER ENVIRONMENT
Abstract
▪ Abstract The central half kiloparsec region of our Galaxy harbors a variety of phenomena unique to the central environment. This review discusses the observed structure and activity of the interstellar medium in this region in terms of its inevitable inflow toward the center of the Galactic gravitational potential well. A number of dissipative processes lead to a strong concentration of gas into a “Central Molecular Zone” of about 200-pc radius, in which the molecular medium is characterized by large densities, large velocity dispersions, high temperatures, and apparently strong magnetic fields. The physical state of the gas and the resultant star formation processes occurring in this environment are therefore quite unlike those occurring in the large-scale disk. Gas not consumed by star formation either enters a hot X ray–emitting halo and is lost as a thermally driven galactic wind or continues moving inward, probably discontinuously, through the domain of the few parsec-sized circumnuclear disks and eventually into the central parsec. There, the central radio source SgrA*currently accepts only a tiny fraction of the inflowing material, likely as a result of a limit cycle wherein the continual inflow of matter provokes star formation, which in turn can temporarily halt the inflow via mass-outflow winds.
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The CMZ is a disk-like region of dense (≳10^3 cm^-3) gas within +1.7°≲l≲-1° (R≃200 pc, assuming Galactocentric radii 8.5 kpc), |b|≲0.5° (H≃75 pc), and |vrot|≲150 km/s.
“The CMZ is a disk-like region of dense ( ≳ 10 3 cm -3 ) gas within + 1 . 7 ◦ ≲ l ≲ -1 ◦ ( R ≃ 200 pc, assuming a Galactocentric radii of 8 . 5 kpc), | b | ≲ 0 . 5 ◦ ( H ≃ 75 pc), and | v rot | ≲ 150 km s -1 (Panel a of Fig 8; Sofue 1995; Morris & Serabyn 1996; Molinari et al. 2011; Henshaw et al. 2016, 2022; Sormani et al. 2022).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Morris & Serabyn 1996
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A DISK OF YOUNG STARS AT THE GALACTIC CENTER AS DETERMINED BY INDIVIDUAL STELLAR ORBITS
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ACOBEModel of the Galactic Bar and Disk
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The Large‐Scale Bipolar Wind in the Galactic Center
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The 511 keV emission from positron annihilation in the Galaxy
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Detection of amino acetonitrile in Sgr B2(N)
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What controls star formation in the central 500 pc of the Galaxy?
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EVIDENCE FOR WARPED DISKS OF YOUNG STARS IN THE GALACTIC CENTER
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The 6-GHz methanol multibeam maser catalogue - I. Galactic Centre region, longitudes 345° to 6°
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Observing Interstellar and Intergalactic Magnetic Fields
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HCN and HCO<sup>+</sup>Observations of the Galactic Circumnuclear Disk
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The Galactic Center: The Largest Oxygen‐bearing Organic Molecule Repository
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Surface brightness profile of the Milky Way’s nuclear star cluster
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Spectral analysis of the Galactic e+e- annihilation emission
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A Deep Submillimeter Survey of the Galactic Center
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Spatial distribution of interstellar gas in the innermost 3 kpc of our Galaxy
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Star formation rates and efficiencies in the Galactic Centre
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Gas flow models in the Milky Way embedded bars
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ASCA X‐Ray Source Catalog in the Galactic Center Region
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FADING HARD X-RAY EMISSION FROM THE GALACTIC CENTER MOLECULAR CLOUD Sgr B2
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Self-citationInfrared stellar populations in the central parts of the Milky Way galaxy
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The Origin of Diffuse X‐Ray and γ‐Ray Emission from the Galactic Center Region: Cosmic‐Ray Particles
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Impact of Low-Energy Cosmic Rays on Star Formation
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Sensitivity of the Cherenkov Telescope Array to a dark matter signal from the Galactic centre
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The Secrets of the Nearest Starburst Cluster. II. The Present-Day Mass Function in NGC 3603
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Evidence for a Long‐standing Top‐heavy Initial Mass Function in the Central Parsec of the Galaxy
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Wild at Heart:-The Particle Astrophysics of the Galactic Centre
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A STRONGLY MAGNETIZED PULSAR WITHIN THE GRASP OF THE MILKY WAY'S SUPERMASSIVE BLACK HOLE
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Early formation and recent starburst activity in the nuclear disk of the Milky Way
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- Authors
- Morris, M., & Serabyn, E.
- Affiliations
- University of California, Los Angeles (US)
- California Institute of Technology (US)
- Venue
- Annual Review of Astronomy and Astrophysics
- Publisher
- Annual Reviews
- Published
- 1996-09
- Volume
- 34
- Issue
- 1
- Pages
- 645-701
- ISSN
- 0066-4146 (ISSN-L)
- 1545-4282
- OpenAlex
- W2127604531
- Cited by
- 930
- References
- 344
- Citations by year
- 2026: 20 · 2025: 38 · 2024: 36 · 2023: 23 · 2022: 31 · 2021: 41 · 2020: 47 · 2019: 60 · 2018: 35 · 2017: 35 · 2016: 37 · 2015: 34 · 2014: 33 · 2013: 50 · 2012: 39
- FWCI
- 1.86
- Type
- journal article
- Language
- en
- Open access
- closed
- Locations
- Annual Review of Astronomy and Astrophysics (publishedVersion)
- CaltechAUTHORS (California Institute of Technology) (submittedVersion)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Keywords
- Galactic Center, interstellar medium, Central Molecular Zone, gas inflow, molecular gas, velocity dispersion, magnetic field, star formation, galactic winds, circumnuclear disk, Sgr A*, supermassive black holes
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
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