STAR FORMATION IN GALAXIES ALONG THE HUBBLE SEQUENCE
Open accessAbstract
▪ Abstract Observations of star formation rates (SFRs) in galaxies provide vital clues to the physical nature of the Hubble sequence and are key probes of the evolutionary histories of galaxies. The focus of this review is on the broad patterns in the star formation properties of galaxies along the Hubble sequence and their implications for understanding galaxy evolution and the physical processes that drive the evolution. Star formation in the disks and nuclear regions of galaxies are reviewed separately, then discussed within a common interpretive framework. The diagnostic methods used to measure SFRs are also reviewed, and a self-consistent set of SFR calibrations is presented as an aid to workers in the field.
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The FUV emission is weighted most strongly toward short-lived O and B stars with lifetimes shorter than 100 Myr, with a strong weighting toward ages of 30-50 Myr.
“Physically, the FUV emission is weighted most strongly toward short lived O and B stars with lifetimes shorter than 100 Myr, with a strong weighting toward ages of 30-50 Myr”
From The Panchromatic Hubble Andromeda Southern Treasury (PHAST). II. The Spatially Resolved Recent Star Formation History in M31 (2026) · cites this paper as Kennicutt 1998
The FUV is sensitive not just to the averaged rate of star formation over some time interval, but also depends on the detailed timing of star formation within that interval.
“the failure of either constant SFR model to explain the observed FUV emission is due to the fact that the FUV is sensitive not just to the averaged rate of star formation over some time interval, but also depends on the detailed timing of star formation within that interval.”
From The Panchromatic Hubble Andromeda Southern Treasury (PHAST). II. The Spatially Resolved Recent Star Formation History in M31 (2026) · cites this paper as Kennicutt 1998
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“The High-density Regime The two regimes discussed above were able to reproduce all of the early observations of the large-scale star formation law by Kennicutt (1989, 1998b) and Martin & Kennicutt (2001).”
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“This timescale is chosen to match what is generally considered the characteristic sensitivity window of the FUV+24 µ m tracer (e.g., Kennicutt 1998; Kennicutt & Evans 2012) and to remain within the regime where the SFHs are best constrained.”
Influential
- Authors
- Kennicutt, R. C.
- Affiliations
- University of Arizona (US)
- Corresponding author
- Kennicutt, Robert C.
- Venue
- Annual Review of Astronomy and Astrophysics
- Publisher
- Annual Reviews
- Published
- 1998-09
- Volume
- 36
- Issue
- 1
- Pages
- 189-231
- ISSN
- 0066-4146 (ISSN-L)
- 1545-4282
- OpenAlex
- W2131522386
- Cited by
- 6,578
- References
- 2
- Citations by year
- 2026: 178 · 2025: 249 · 2024: 252 · 2023: 235 · 2022: 280 · 2021: 287 · 2020: 279 · 2019: 287 · 2018: 281 · 2017: 287 · 2016: 386 · 2015: 318 · 2014: 287 · 2013: 353 · 2012: 332
- FWCI
- 7.65
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Locations
- Annual Review of Astronomy and Astrophysics (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Keywords
- star formation rate, Hubble sequence, galaxy evolution, disk galaxies, nuclear star formation, SFR calibration, star formation rate surface density
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