Wikipedia

Orion Arm

This article is about the galactic arm of the Milky Way Galaxy. For the stars which form the arm of the Orion asterism, see Orion (constellation). For other uses, see Arm of Orion (disambiguation).

The Orion Arm, also known as the Orion–Cygnus Arm, is a minor spiral arm within the Milky Way Galaxy spanning 3,500 light-years (1,100 parsecs) in width and extending roughly 20,000 light-years (6,100 parsecs) in length.[2] This galactic structure encompasses the Solar System, including Earth. It is sometimes referred to by alternate names such as the Local Arm or Orion Bridge, and it was previously identified as the Local Spur or the Orion Spur. It should not be confused with the outer terminus of the Norma Arm, known as the Cygnus Arm.

Figure 1.The observed structure of the Milky Way's spiral arms[1]

Naming and brightness

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The arm is named after the Orion Constellation, one of the most prominent constellations of the Northern Hemisphere in winter (or the Southern Hemisphere in summer). Some of the brightest stars in the sky as well as other well-known celestial objects of the constellation (e.g. Betelgeuse, Rigel, the three stars of Orion's Belt, and the Orion Nebula) are found within it, as shown on Orion Arm's interactive map.

Location

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The Orion arm is located between the Carina–Sagittarius Arm, the local portion of which projects toward the Galactic Center, and the Perseus Arm's local portion, which forms the main outer-most arm.

Scientists once believed the Orion arm to be a minor structure, namely a "spur" between Carina-Sagittarius and Perseus, but evidence presented in 2013 suggests the Orion Arm to be a branch of the Perseus Arm or possibly an independent arm segment.[3]

The Solar System is close to its inner rim, about halfway along the arm's length, in a relative cavity in the arm's interstellar medium, known as the Local Bubble. It is approximately 8,000 parsecs (26,000 light-years) from the Galactic Center.

Composition

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Recently, the BeSSeL Survey (Bar and Spiral Structure Legacy Survey) analyzed the parallax and proper motion of more than 30 methanol (6.7-GHz) and water (22-GHz) masers in high-mass, star-forming regions within a few kiloparsecs of the Sun. Their measurement has accuracy above ±10% and even 3%.[citation needed] The accurate locations of interstellar masers in HMSFRs (high-mass star-forming regions) suggests the Local Arm appears to be an orphan segment of an arm between the Sagittarius and Perseus arms that wraps around less than a quarter of the Milky Way. The segment has a length of ~20,000 ly in length and ~3,000 ly in width, with a pitch angle of 10.1° ± 2.7° to 11.6° ± 1.8°. These results suggest the Local Arm is larger than previously thought, and both its pitch angle and star formation rate are comparable to those of the Galaxy’s major spiral arms. The Local Arm is reasonably referred to as the fifth feature in the Milky Way.[4][5][6][7][8]

Form

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To understand the form of the Local Arm between the Sagittarius and Perseus arms, the stellar density of a specific population of stars with about 1 Gyr of age between 90° ≤ l ≤ 270° have been mapped using the Gaia DR2.[9] The 1 Gyr population have been employed because they are significantly more-evolved objects than the gas in HMSFRs tracing the Local Arm. Investigations have been carried out to compare both the stellar density and gas distribution along the Local Arm. Researchers have found a marginally significant arm-like stellar overdensity close to the Local Arm, identified with the HMSFRs, especially in the region of 90° ≤ l ≤ 190°.[8]

The researchers have concluded that the Local Arm segment is associated only with gas and star-forming clouds, showing a significant overdensity of stars. They have also found that the pitch angle of the stellar arm is slightly larger than the gas-defined arm, and there is an offset between the gas-defined and stellar arm. These differences in pitch angles and offsets between the stellar and HMSFR-defined spiral arms are consistent with the expectation that star formation lags behind gas compression in a spiral density wave that lasts longer than the typical star formation timescale of 107 − 108 years.[10]

Messier objects

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The Orion Arm contains a number of Messier objects:

Maps

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A rough artist's depiction of the Orion Arm within the Milky Way, with features marked.
 
Molecular clouds around the Sun inside the Orion-Cygnus Arm

Interactive maps

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 Rosette NebulaCrab NebulaOrion NebulaTrifid NebulaLagoon NebulaOmega NebulaEagle NebulaNorth America NebulaRigelOrion's BeltPolarisSunBetelgeuseDenebPerseus ArmOrion ArmSagittarius Arm
Orion and neighboring arms (clickable map)
 Rosette NebulaSeagull NebulaCone NebulaCalifornia NebulaHeart NebulaOrion NebulaSoul NebulaNorth America NebulaCocoon NebulaGamma Cygni NebulaVeil NebulaTrifid NebulaCrescent NebulaLagoon NebulaOmega NebulaEagle NebulaCat's Paw NebulaEta Carinae NebulaCrab NebulaMessier 37Messier 36Messier 38Messier 50Messier 46Messier 67Messier 34Messier 48Messier 41Messier 47Messier 44Messier 45Messier 39Messier 52Messier 93Messier 7Messier 6Messier 25Messier 23Messier 21Messier 18Messier 26Messier 11Messier 35NGC 2362IC 2395NGC 3114NGC 3532IC 1396IC 2602NGC 6087NGC 6025NGC 3766IC 4665IC 2581IC 2944NGC 4755NGC 3293NGC 6067NGC 6193NGC 6231NGC 6383Tr 14Tr 16Messier 103Messier 29HPerChi PerCol 228O VelPerseus ArmOrion ArmSagittarius ArmStar clusterNebula
The nearest nebulae and star clusters (clickable map)

See also

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References

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  1. ^ See the "Spiral Arms" part of this NASA animation for details.
  2. ^ Xu, Ye; Reid, Mark; Dame, Thomas; Menten, Karl; Sakai, Nobuyuki; Li, Jingjing; Brunthaler, Andreas; Moscadelli, Luca; Zhang, Bo; Zheng, Xingwu (28 September 2016). "The local spiral structure of the Milky Way". Science Advances. 2 (9): e1600878. arXiv:1610.00242. Bibcode:2016SciA....2E0878X. doi:10.1126/sciadv.1600878. PMC 5040477. PMID 27704048.
  3. ^ Dave Finley, Earth's Milky Way Neighborhood Gets More Respect, National Radio Astronomy Observatory, 3 June 2013.
  4. ^ Reid, Mark; Zheng, Xing-Wu (April 2020). "New View of the Milky Way". Scientific American. 322 (4): 28. doi:10.1038/scientificamerican0420-28. PMID 39014607.
  5. ^ Xu, Y.; Reid, M.; Dame, T.; Menten, K.; Sakai, N.; Li, J.; Brunthaler, A.; Moscadelli, L.; Zhang, B.; Zheng, X. (2016). "The local spiral structure of the Milky Way". Science Advances. 2 (9): e1600878. arXiv:1610.00242. Bibcode:2016SciA....2E0878X. doi:10.1126/sciadv.1600878. PMC 5040477. PMID 27704048.
  6. ^ Xu, Y.; Li, J. J.; Reid, M. J.; Menten, K. M.; Zheng, X. W.; Brunthaler, A.; Moscadelli, L.; Dame, T. M.; Zhang, B. (30 April 2013). "On the Nature of the Local Spiral Arm of the Milky Way". The Astrophysical Journal. 769 (1): 15. arXiv:1304.0526. Bibcode:2013ApJ...769...15X. doi:10.1088/0004-637X/769/1/15.
  7. ^ Reid, M. J.; Menten, K. M.; Brunthaler, A.; Zheng, X. W.; Dame, T. M.; Xu, Y.; Li, J.; Sakai, N.; Wu, Y.; Immer, K.; Zhang, B.; Sanna, A.; Moscadelli, L.; Rygl, K. L. J.; Bartkiewicz, A.; Hu, B.; Quiroga-Nuñez, L. H.; Van Langevelde, H. J. (2019). "Trigonometric Parallaxes of High-mass Star-forming Regions: Our View of the Milky Way". The Astrophysical Journal. 885 (2): 131. arXiv:1910.03357. Bibcode:2019ApJ...885..131R. doi:10.3847/1538-4357/ab4a11. S2CID 203904869.
  8. ^ a b Hirota, Tomoya; Nagayama, Takumi; Honma, Mareki; et al. (August 2020). "The First VERA Astrometry Catalog". Publications of the Astronomical Society of Japan. 72 (4). arXiv:2002.03089. doi:10.1093/pasj/psaa018.
  9. ^ Miyachi, Yusuke; Sakai, Nobuyuki; Kawata, Daisuke; Baba, Junichi; Honma, Mareki; Matsunaga, Noriyuki; Fujisawa, Kenta (2019). "Stellar Overdensity in the Local Arm in Gaia DR2". The Astrophysical Journal. 882 (1): 48. arXiv:1907.03763. Bibcode:2019ApJ...882...48M. doi:10.3847/1538-4357/ab2f86. S2CID 195847953.
  10. ^ Shen, Juntai; Zheng, Xing-Wu (October 2020). "The bar and spiral arms in the Milky Way: structure and kinematics". Research in Astronomy and Astrophysics. 20 (10): 159. arXiv:2012.10130. Bibcode:2020RAA....20..159S. doi:10.1088/1674-4527/20/10/159.
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