List of star-forming regions in the Local Group

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Composite image showing young stars in and around molecular cloud Cepheus B. Cepheus B.jpg
Composite image showing young stars in and around molecular cloud Cepheus B.

This is a list of star-forming regions in the Milky Way Galaxy and the Local Group. Star formation occurs in molecular clouds, which become unstable to gravitational collapse, and these complexes may contain clusters of young stars and regions of ionized gas called H II regions. Stars typically form in groups of many stars, rather than in isolation. [1]

Contents

Galactic star-forming regions

Extragalactic star-forming regions

NameRA [deg]Dec [deg]l [deg]b [deg]Distance [pc]Age [Myr]Earliest SpTyNumber of StarsCloud Mass [Mo]
30 Doradus 84.67665-69.10093279.4652-31.671949,000

See also

References

  1. ↑ Lada, C. J.; Lada, E. A. (2003). "Embedded Clusters in Molecular Clouds". Annual Review of Astronomy & Astrophysics. 41: 57–115. arXiv: astro-ph/0301540 . Bibcode:2003ARA&A..41...57L. doi:10.1146/annurev.astro.41.011802.094844. S2CID   16752089.
  2. 1 2 Shuping, R. Y.; et al. (2012). "Spectral Classification of the Brightest Objects in the Galactic Star-forming Region W40". Astronomical Journal. 144 (4): 116. arXiv: 1208.4648 . Bibcode:2012AJ....144..116S. doi:10.1088/0004-6256/144/4/116. S2CID   119227485.
  3. ↑ Getman, K. V.; et al. (2014). "Age Gradients in the Stellar Populations of Massive Star Forming Regions Based on a New Stellar Chronometer". Astrophysical Journal. 787 (2): 108. arXiv: 1403.2741 . Bibcode:2014ApJ...787..108G. doi:10.1088/0004-637X/787/2/108. S2CID   118626928.
  4. ↑ Kuhn, M. A.; et al. (2010). "A Chandra Observation of the Obscured Star-forming Complex W40". Astrophysical Journal. 725 (2): 2485–2506. arXiv: 1010.5434 . Bibcode:2010ApJ...725.2485K. doi:10.1088/0004-637X/725/2/2485. S2CID   119192761.
  5. ↑ Kuhn, M. A.; Getman, K. V.; Feigelson, E. D. (2015). "The Spatial Structure of Young Stellar Clusters. II. Total Young Stellar Populations". Astrophysical Journal. 802 (1): 60. arXiv: 1501.05300 . Bibcode:2015ApJ...802...60K. doi:10.1088/0004-637X/802/1/60. S2CID   119309858.
  6. ↑ Johnston, K. G.; Shepherd, D. S.; Robitaille, T. P.; Wood, K. (2013). "The standard model of low-mass star formation applied to massive stars: a multi-wavelength picture of AFGL 2591". Astronomy & Astrophysics. 551: A43, 1–23. arXiv: 1212.1719 . Bibcode:2013A&A...551A..43J. doi:10.1051/0004-6361/201219657. S2CID   54972885.
  7. ↑ Sanna, A.; Reid, M. J.; Carrasco-González, C.; et al. (2012). "Clustered star formation and outflows in AFGL 2591". The Astrophysical Journal. 745 (2): 191–200. arXiv: 1111.0843 . Bibcode:2012ApJ...745..191S. doi:10.1088/0004-637X/745/2/191. S2CID   118465380.
  8. ↑ Zhang, B.; et al. (2013). "Parallaxes for W49N and G048.60+0.02: Distant Star Forming Regions in the Perseus Spiral Arm". Astrophysical Journal. 775 (1): 79. arXiv: 1312.3856 . Bibcode:2013ApJ...775...79Z. doi:10.1088/0004-637X/775/1/79. S2CID   119257313.
  9. ↑ Wu, S.-W.; et al. (2014). "The discovery of a very massive star in W49". Astronomy & Astrophysics. 568: L13. arXiv: 1407.4804 . Bibcode:2014A&A...568L..13W. doi:10.1051/0004-6361/201424154. S2CID   55277847.
  10. ↑ Sample, Ian (7 January 2020). "Astronomers discover huge gaseous wave holding Milky Way's newest stars". The Guardian. ISSN   0261-3077 . Retrieved 2020-01-07– via www.theguardian.com.
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