NGC 663

NGC 663 (also known as Caldwell 10) is young open cluster of about 400 stars in the Cassiopeia constellation. It has an estimated 400 stars and spans about a quarter of a degree across the sky. It can reportedly be detected with the unaided eye, although a telescope is recommended for best viewing. The brightest members of the cluster can be viewed with binoculars. Although the listed visual magnitude is 7.1, several observers have reported higher estimates.[1]

NGC 663
NGC 663 in Cassiopeia
Observation data (J2000 epoch)
ConstellationCassiopeia
Right ascension01h 46.0m
Declination+61° 15′
Distance6,850 ly (2,100 pc)
Apparent magnitude (V)7.1
Apparent dimensions (V)16.0′
Physical characteristics
Other designationsCaldwell 10, Cr 20

After adjusting for reddening due to interstellar dust, the distance modulus is estimated as 11.6 magnitudes. It is located about 2,100 parsecs distant with an estimated age of 20–25 million years.[2] This means that stars of spectral class B2 or higher (in the sense of higher mass), are reaching the end of their main sequence lifespan.[3] This cluster appears to be located in front of a molecular cloud, although the two are not physically associated. This cloud has the effect of blocking background stars from the visual image of the cluster as it lies at a distance of 300 parsecs.[4]

This cluster is of interest because of the high number of Be stars, with a total of about 24 discovered. These are spectral class B stars that show prominent emission lines of hydrogen in their spectrum. Most of the Be stars in the cluster lie between spectral class B0 and B3.[2] A candidate member of the cluster, LS I +61° 235, is a Be star with an X-ray binary component that has a period of about three years.[5] There are at least five blue stragglers in the cluster. These are stars that formed by the merger of two other stars.[3] Two of the cluster's star systems are likely eclipsing binaries with periods of 0.6 and 1.03 days.[6] NGC 663 also has two red supergiant stars, both located on its periphery[7][8]

The star cluster is assumed to form part of the stellar association Cassiopeia OB8, that is located in the Perseus arm of the Milky Way, along with the open clusters M103, NGC 654, NGC 659, and some supergiant stars scattered between them, all of them having similar ages and distances.[9][10]

  • NGC663 LRGB Using PlaneWave CDK 12.5 from Talent, OR
gollark: To save you from problems they're withheld until I can recalculate safe ones.
gollark: My guesses accidentally contained a proof of the inconsistency of arithmetic.
gollark: No, it's because I'm everyone's alt and I have an IQ of 205 octillion.
gollark: None are safe, broadly speaking.
gollark: Compute the main and variance then multiply and add until you get back to the definition of IQ.

References
  1. O'Meara, S. J. (2002). The Caldwell objects, Deep-sky companions. Cambridge University Press. pp. 50–51. ISBN 978-0-521-82796-6.
  2. Pigulski, A.; Kopacki, G.; Kolaczkowski, Z. (2001). "The young open cluster NGC 663 and its Be stars". Astronomy & Astrophysics. 376 (1): 144–153. Bibcode:2001A&A...376..144P. doi:10.1051/0004-6361:20010974.
  3. Marco, A.; Negueruela, I.; Motch, C. (2007). "Blue Stragglers, Be Stars and X-ray Binaries in Open Clusters". ASP Conference Series. 361: 388. Bibcode:2007ASPC..361..388M.
  4. Phelps, Randy L.; Janes, Kenneth A. (1993). "Young open clusters as probes of the star-formation process. 2: Mass and luminosity functions of young open clusters". Astronomical Journal. 106 (5): 1870–1884. Bibcode:1993AJ....106.1870P. doi:10.1086/116772.
  5. Reig, P.; Fabregat, J.; Coe, M. J.; Roche, P.; et al. (1997). "The Be/X-ray binary LS I +61 235/RX J0146.9+6121: physical parameters and V/R variability" (PDF). Astronomy and Astrophysics. 322 (1): 183–192. Bibcode:1997A&A...322..183R. Archived from the original (PDF) on 2016-03-04. Retrieved 2012-04-17.
  6. Pietrzynski, G. (1996). "Variable Stars in the Young Open Cluster NGC 663". Acta Astronomica. 46: 357–360. Bibcode:1996AcA....46..357P.
  7. Mermilliod, J. C.; Mayor, M.; Udry, S. (2008). "Red giants in open clusters. XIV. Mean radial velocities for 1309 stars and 166 open clusters". Astronomy & Astrophysics. 485 (1): 303–314. Bibcode:2008A&A...485..303M. CiteSeerX 10.1.1.30.7545. doi:10.1051/0004-6361:200809664.
  8. Pandey, A. K.; Upadhyay, K.; Ogura, K.; Sagar, Ram; et al. (2005). "Stellar contents of two young open clusters: NGC 663 and 654". Monthly Notices of the Royal Astronomical Society. 358 (4): 1290–1308. Bibcode:2005MNRAS.358.1290P. doi:10.1111/j.1365-2966.2005.08784.x.
  9. Negueruela, I.; González-Fernández, C.; Marco, A.; Clark, J. S. (2011). "A massive association around the obscured open cluster RSGC3". Astronomy & Astrophysics. 528: A59. arXiv:1102.0028. Bibcode:2011A&A...528A..59N. doi:10.1051/0004-6361/201016102.
  10. Humphreys, R. M. (1978). "Studies of luminous stars in nearby galaxies. I. Supergiants and O stars in the Milky Way". Astrophysical Journal Supplement Series. 38: 309–350. Bibcode:1978ApJS...38..309H. doi:10.1086/190559.


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