| Palomar 5 | |
|---|---|
.jpg) | |
| Observation data ( J2000 epoch) | |
| Class | XII |
| Constellation | Serpens |
| Right ascension | 15h 16m 05.3s [1] |
| Declination | –00° 06′ 41″ [1] |
| Distance | 76 kly (23 kpc) [2] |
| Apparent magnitude (V) | +11.75 |
| Apparent dimensions (V) | 6.9′ |
| Physical characteristics | |
| Mass | 3.00×104 [3] M☉ |
| Radius | 76 ly [4] |
| Estimated age | 11.5±1.0 Gyr [5] |
| Notable features | Erroneously thought to be a dwarf galaxy |
| Other designations | UGC 9792, GCl 32 [1] |
Palomar 5 is a globular cluster and a member of the Palomar Globular Clusters group. It was discovered by Walter Baade in 1950, and independently found again by Albert George Wilson in 1955. After the initial name of Serpens, it was subsequently catalogued as Palomar 5.
There is a process of disruption acting on this cluster because of the gravitation of the Milky Way – in fact there are many stars leaving this cluster in the form of a stellar stream. The stream has a mass of 5000 solar masses and is 30,000 light years long. [6] The cluster is currently 60.6 kly (18.6 kpc) from the Galactic Center. It shows a noticeable amount of flattening, with an aspect ratio of 0.62 ± 0.23 between its semimajor axis and semiminor axis. [7]
See also
References
- ^ a b c "SIMBAD Astronomical Database". Results for Palomar 5. Retrieved 2006-11-17.
- ^ Hessels, J. W. T.; et al. (November 2007), "A 1.4 GHz Arecibo Survey for Pulsars in Globular Clusters", The Astrophysical Journal, 670 (1): 363–378, arXiv: 0707.1602, Bibcode: 2007ApJ...670..363H, doi: 10.1086/521780, S2CID 16914232.
- ^ Boyles, J.; et al. (November 2011), "Young Radio Pulsars in Galactic Globular Clusters", The Astrophysical Journal, 742 (1): 51, arXiv: 1108.4402, Bibcode: 2011ApJ...742...51B, doi: 10.1088/0004-637X/742/1/51, S2CID 118649860.
- ^ distance × sin( diameter_angle / 2 ) = 76 ly. radius
- ^ Martell, S. L.; Smith, G. H.; Grillmair, C. J. (2002). "A New Age Measurement for Palomar 5". American Astronomical Society, 201st AAS Meeting, #07.11; Bulletin of the American Astronomical Society. 34: 1103. Bibcode: 2002AAS...201.0711M.
- ^ Ibata, Rodrigo; Gibson, Brad (April 2007). "The Ghosts of Galaxies Past". Scientific American. 296 (4): 40–45. Bibcode: 2007SciAm.296d..40I. doi: 10.1038/scientificamerican0407-40. ISSN 0036-8733. PMID 17479629.
- ^ Chen, C. W.; Chen, W. P. (October 2010), "Morphological Distortion of Galactic Globular Clusters", The Astrophysical Journal, 721 (2): 1790–1819, Bibcode: 2010ApJ...721.1790C, doi: 10.1088/0004-637X/721/2/1790
External links
- SEDS Palomar 5
- Palomar 5 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
- Gieles, Mark; Erkal, Denis; Antonini, Fabio; Balbinot, Eduardo; Peñarrubia, Jorge (2021), N-body simulation of the Galactic globular cluster Palomar 5 and its stream, arXiv: 2102.11348, doi: 10.1038/s41550-021-01392-2, S2CID 256703405, archived from the original on 2021-12-18, retrieved 2021-07-08
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Milky Way →
Milky Way subgroup →
Local Group →
Local Sheet →
Virgo Supercluster →
Laniakea Supercluster →
Local Hole →
Observable universe →
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 | This star cluster–related article is a stub. You can help Wikipedia by expanding it. |
| Palomar 5 | |
|---|---|
|
| |
| Observation data ( J2000 epoch) | |
| Class | XII |
| Constellation | Serpens |
| Right ascension | 15h 16m 05.3s [1] |
| Declination | –00° 06′ 41″ [1] |
| Distance | 76 kly (23 kpc) [2] |
| Apparent magnitude (V) | +11.75 |
| Apparent dimensions (V) | 6.9′ |
| Physical characteristics | |
| Mass | 3.00×104 [3] M☉ |
| Radius | 76 ly [4] |
| Estimated age | 11.5±1.0 Gyr [5] |
| Notable features | Erroneously thought to be a dwarf galaxy |
| Other designations | UGC 9792, GCl 32 [1] |
Palomar 5 is a globular cluster and a member of the Palomar Globular Clusters group. It was discovered by Walter Baade in 1950, and independently found again by Albert George Wilson in 1955. After the initial name of Serpens, it was subsequently catalogued as Palomar 5.
There is a process of disruption acting on this cluster because of the gravitation of the Milky Way – in fact there are many stars leaving this cluster in the form of a stellar stream. The stream has a mass of 5000 solar masses and is 30,000 light years long. [6] The cluster is currently 60.6 kly (18.6 kpc) from the Galactic Center. It shows a noticeable amount of flattening, with an aspect ratio of 0.62 ± 0.23 between its semimajor axis and semiminor axis. [7]
See also
References
- ^ a b c "SIMBAD Astronomical Database". Results for Palomar 5. Retrieved 2006-11-17.
- ^ Hessels, J. W. T.; et al. (November 2007), "A 1.4 GHz Arecibo Survey for Pulsars in Globular Clusters", The Astrophysical Journal, 670 (1): 363–378, arXiv: 0707.1602, Bibcode: 2007ApJ...670..363H, doi: 10.1086/521780, S2CID 16914232.
- ^ Boyles, J.; et al. (November 2011), "Young Radio Pulsars in Galactic Globular Clusters", The Astrophysical Journal, 742 (1): 51, arXiv: 1108.4402, Bibcode: 2011ApJ...742...51B, doi: 10.1088/0004-637X/742/1/51, S2CID 118649860.
- ^ distance × sin( diameter_angle / 2 ) = 76 ly. radius
- ^ Martell, S. L.; Smith, G. H.; Grillmair, C. J. (2002). "A New Age Measurement for Palomar 5". American Astronomical Society, 201st AAS Meeting, #07.11; Bulletin of the American Astronomical Society. 34: 1103. Bibcode: 2002AAS...201.0711M.
- ^ Ibata, Rodrigo; Gibson, Brad (April 2007). "The Ghosts of Galaxies Past". Scientific American. 296 (4): 40–45. Bibcode: 2007SciAm.296d..40I. doi: 10.1038/scientificamerican0407-40. ISSN 0036-8733. PMID 17479629.
- ^ Chen, C. W.; Chen, W. P. (October 2010), "Morphological Distortion of Galactic Globular Clusters", The Astrophysical Journal, 721 (2): 1790–1819, Bibcode: 2010ApJ...721.1790C, doi: 10.1088/0004-637X/721/2/1790
External links
- SEDS Palomar 5
- Palomar 5 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
- Gieles, Mark; Erkal, Denis; Antonini, Fabio; Balbinot, Eduardo; Peñarrubia, Jorge (2021), N-body simulation of the Galactic globular cluster Palomar 5 and its stream, arXiv: 2102.11348, doi: 10.1038/s41550-021-01392-2, S2CID 256703405, archived from the original on 2021-12-18, retrieved 2021-07-08
| Stars |
| ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| |||||||||||||
|
Star clusters |
| ||||||||||||
| Nebulae |
| ||||||||||||
| Galaxies |
| ||||||||||||
| |||||||||||||
| |||||||||||||
| Location |
Milky Way →
Milky Way subgroup →
Local Group →
Local Sheet →
Virgo Supercluster →
Laniakea Supercluster →
Local Hole →
Observable universe →
Universe Each arrow (→) may be read as "within" or "part of". | | |||||
|---|---|---|---|---|---|---|---|
| Structure |
| ||||||
|
Satellite galaxies | |||||||
| Related | |||||||
|
| This star cluster–related article is a stub. You can help Wikipedia by expanding it. |