NGC 3175
| NGC 3175 | |
|---|---|
 NGC 3175 taken by the Hubble Space Telescope[1] | |
| Observation data (J2000[2] epoch) | |
| Constellation | Antlia |
| Right ascension | 10h 14m 42.111s[3] |
| Declination | −28° 52′ 19.42″[3] |
| Redshift | 0.003613[2] |
| Heliocentric radial velocity | 1,081.1 km/s[4] |
| Distance | 53.9 Mly (16.52 Mpc)[5] |
| Group or cluster | NGC 3175 group[6] |
| Apparent magnitude (B) | 12.08[5] |
| Characteristics | |
| Type | SAB(s)b[7] |
| Mass | (7.34±0.85)×1010[6] M☉ |
| Mass/Light ratio | 7.13+1.78 −1.98[6] M☉/L☉ |
| Apparent size (V) | 5′.0 × 1′.3[8] |
| Other designations | |
| IRAS 1012-286P13, 2MASX J10144211-2852194, NGC 3175, LEDA 29892, MCG -05-24-028[2] | |
NGC 3175 is a spiral galaxy located in the far eastern part of the southern constellation of Antlia[8] at an approximate distance of 54 million light-years.[5] NGC 3175 was discovered on March 30, 1835 by English astronomer John Herschel,[9] whose notes described it as, "considerably bright, large, much extended NE-SW, very gradually little brighter middle".[10] This galaxy is the namesake of the NGC 3175 group of galaxies,[6] which includes the spiral galaxy NGC 3137.[11]
The morphological classification of this galaxy is SAB(s)b,[7] which indicates a weakly-barred spiral galaxy (SAB) with no inner ring structure (s), and somewhat tightly wound spiral arms (b). It spans an angular size of 5′.0 × 1′.3,[8] with the major axis aligned along a position angle of 56°. The plane of the galaxy is inclined at an angle of 77° to the line of sight from the Earth,[12] and thus is being viewed close to edge on.
A study of the galaxy using the Australia Telescope Compact Array found that the outer disk of this galaxy, beyond a radius of 3.5 kpc from the core, is free of neutral hydrogen emission. This is an indication that no star formation is occurring, which is peculiar for a spiral galaxy. In contrast, the central region is undergoing star formation and contains 5.8×108 M☉ of neutral hydrogen. There are no nearby galaxies that could explain the stripping of hydrogen gas from the outer part of the galaxy.[6]
See also
[edit]References
[edit]- ^ "Galactic Diversity". www.spacetelescope.org. Retrieved 10 December 2019.
- ^ a b c "NGC 3175". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-12-10.
- ^ a b Skrutskie, Michael F.; et al. (February 1, 2006). "The Two Micron All Sky Survey (2MASS)". The Astronomical Journal. 131 (2): 1163–1183. Bibcode:2006AJ....131.1163S. doi:10.1086/498708. ISSN 0004-6256. S2CID 18913331.
- ^ Meyer, M. J.; et al. (June 2004). "The HIPASS catalogue - I. Data presentation". Monthly Notices of the Royal Astronomical Society. 350 (4): 1195–1209. arXiv:astro-ph/0406384. Bibcode:2004MNRAS.350.1195M. doi:10.1111/j.1365-2966.2004.07710.x. S2CID 10336076.
- ^ a b c Tully, R. Brent; et al. (August 2016). "Cosmicflows-3". The Astronomical Journal. 152 (2): 21. arXiv:1605.01765. Bibcode:2016AJ....152...50T. doi:10.3847/0004-6256/152/2/50. S2CID 250737862. 50.
- ^ a b c d e Dahlem, M.; et al. (May 2001). "The mysterious H I deficiency of NGC 3175". Astronomy and Astrophysics. 371: 45–51. arXiv:astro-ph/0103086. Bibcode:2001A&A...371...45D. doi:10.1051/0004-6361:20010313. S2CID 15035948.
- ^ a b Dahlem, M.; et al. (October 2006). "Dependence of radio halo properties on star formation activity and galaxy mass". Astronomy and Astrophysics. 457 (1): 121–131. arXiv:astro-ph/0607102. Bibcode:2006A&A...457..121D. doi:10.1051/0004-6361:20054787. S2CID 18292843.
- ^ a b c Streicher, Magda (June 2010). "Antlia, the Machine Pneumatique". Monthly Notes of the Astronomical Society of South Africa. 69 (5 and 6): 107–112. Bibcode:2010MNSSA..69..107S.
- ^ Seligman, C. "NGC 3175 (= PGC 29892 = PGC 736480)". Celestial Atlas. Retrieved 2021-12-18.
- ^ Aranda, Ted (November 25, 2011). 3,000 Deep-Sky Objects, An Annotated Catalogue. Springer New York. p. 221. ISBN 9781441994196.
- ^ Kondapally, Rohit; Russell, George A.; Conselice, Christopher J.; Penny, Samantha J. (December 2018). "Faint satellite population of the NGC-3175 Group - a Local Group analogue". Monthly Notices of the Royal Astronomical Society. 481 (2): 1759–1773. arXiv:1808.09020. Bibcode:2018MNRAS.481.1759K. doi:10.1093/mnras/sty2333.
- ^ Mathewson, D. S.; Ford, V. L. (November 1996). "Parameters of 2447 Southern Spiral Galaxies for Use in the Tully-Fisher Relation". Astrophysical Journal Supplement. 107: 97. Bibcode:1996ApJS..107...97M. doi:10.1086/192356.
External links
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