NGC 330

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NGC 330
NGC330 - HST - Potw2126a.jpg
The star cluster NGC 330
Credit: Hubble Space Telescope
Observation data (J2000 epoch)
Right ascension 00h 56m 17.6s [1]
Declination −72° 27′ 47″ [1]
Distance 182000 [1]
Apparent magnitude  (V)9.60 [2]
Apparent dimensions (V)2.8′ × 2.5′ [3]
Physical characteristics
Mass5.4×104 [2]   M☉
Estimated age0.04±0.00 Gyr [2]
Other designations ESO 029-SC 024. [1]
Associations
Constellation Tucana
See also: Open cluster, List of open clusters

NGC 330 is an open cluster in the Small Magellanic Cloud. It is located in the constellation Tucana. It was discovered on 1 August 1826 by James Dunlop. It was described by Dreyer as "a globular cluster, very bright, small, a little extended, stars from 13th to 15th magnitude." [4] At an aperture of 31.0 arcseconds, the apparent V-band magnitude is 9.60, but at this wavelength, it also has 0.36 magnitudes of interstellar extinction. [2]

NGC 330 is quite young, at about 40 million years old, and has a large proportion of Be stars. [5] Its estimated mass is 5.4×104  M☉, and its total luminosity is 8.93×105  L☉, leading to a mass-to-luminosity ratio of 0.06 M☉/L☉. [2] All else equal, older star clusters have higher mass-to-luminosity ratios; that is, they have lower luminosities for the same mass. [2] About 34% of the massive star population in NGC 330 is estimated to be in a close binary star system; this is lower than clusters in the Large Magellanic Cloud and the Milky Way, but it is unknown if this is because NGC 330 is metal-poor or is older than the compared clusters. [5]

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<span class="mw-page-title-main">NGC 339</span> Globular cluster in the Small Magellanic Cloud

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<span class="mw-page-title-main">NGC 1783</span> Globular cluster in the constellation Dorado

NGC 1783 is a globular cluster within the Dorado constellation and part of the Large Magellanic Cloud, a satellite dwarf galaxy of the Milky Way. At an aperture of 50 arcseconds, its apparent V-band magnitude is 10.39, making it one of the brightest globular clusters in the LMC as viewed from Earth. It was discovered in 1835 by John Herschel. The compiler of the New General Catalogue, John Louis Emil Dreyer, described this cluster as "considerably bright, large, round, very gradually pretty much brighter middle, mottled but not resolved."

<span class="mw-page-title-main">AB8 (star)</span> Binary star located in the Small Magellanic Cloud in the constellation Hydrus

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<span class="mw-page-title-main">NGC 152</span> Open cluster in the constellation Tucana

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<span class="mw-page-title-main">NGC 361</span> Open star cluster in the Small Magellanic Cloud

NGC 361 is an open cluster in the Small Magellanic Cloud. It is located in the constellation Tucana. It was discovered on September 6, 1826, by James Dunlop. It was described by Dreyer as "very very faint, pretty large, very little extended, very gradually brighter middle." At an aperture of 31.0 arcseconds, its apparent V-band magnitude is 12.24, but at this wavelength, it has 0.40 magnitudes of interstellar extinction.

<span class="mw-page-title-main">NGC 1846</span> Globular cluster in the constellation Dorado

NGC 1846 is a globular cluster containing hundreds of thousands of stars in the outer halo of the Large Magellanic Cloud. It was discovered on November 6, 1826, by James Dunlop and is included in the New General Catalogue. At an aperture of 50 arcseconds, its apparent V-band magnitude is 10.68, but at this wavelength, it has 0.07 magnitudes of interstellar extinction.

<span class="mw-page-title-main">NGC 411</span> Globular cluster located in the constellation Tucana

NGC 411 is a globular cluster located approximately 55,000 pc (180,000 ly) from Earth in the constellation Tucana. It was discovered in 1826 by James Dunlop. It was described by Dreyer as "extremely faint, pretty large, round, gradually very little brighter middle". At a distance of about 180,000 light years (55,000 parsecs), it is located within the Small Magellanic Cloud. It has a mass of about 3.0×104 M☉, and a luminosity of about 8.0×104 L☉.

<span class="mw-page-title-main">NGC 416</span> Globular cluster located in the constellation Tucana

NGC 416 is a globular cluster located in the constellation Tucana. It was discovered on September 5, 1826, by James Dunlop. It was described by Dreyer as "faint, pretty small, round, gradually brighter middle". At a distance of about 199,000 ± 9,800 ly (61,000 ± 3,000 pc), it is located within the Small Magellanic Cloud. At an aperture of 31 arcseconds, its apparent V-band magnitude is 11.42, but at this wavelength, it has 0.25 magnitudes of interstellar extinction.

<span class="mw-page-title-main">NGC 419</span> Globular cluster located in the constellation Tucana

NGC 419 is a globular cluster located approximately 57,000 pc (190,000 ly) from Earth in the constellation Tucana. It was discovered on September 2, 1826, by James Dunlop. It was described by Dreyer as "pretty large, pretty bright, round, gradually brighter middle". At a distance of about 186,000 light years, it is located within the Small Magellanic Cloud. At an aperture of 50 arcseconds, its apparent V-band magnitude is 10.30, but at this wavelength, it has 0.15 magnitudes of interstellar extinction.

<span class="mw-page-title-main">NGC 458</span> Open cluster located in the constellation Tucana

NGC 458 is an open cluster located in the constellation Tucana. It was discovered on September 6, 1826, by James Dunlop. It was also observed by John Herschel and DeLisle Stewart. It was described by Dreyer as "pretty faint, large, round, very gradually brighter middle". It was also noted in the second Index Catalogue that it was "probably a cluster, extremely small, close, no nebulosity seen by D.S. ." At an aperture of 31 arcseconds, its apparent V-band magnitude is 11.73, but at this wavelength, it has 0.12 magnitudes of interstellar extinction.

<span class="mw-page-title-main">NGC 1978</span> Globular cluster in the constellation Dorado

NGC 1978 is an elliptical shaped globular cluster or open cluster in the constellation Dorado. It is located within the Large Magellanic Cloud. It was discovered by James Dunlop on November 6, 1826. At an aperture of 50 arcseconds, its apparent V-band magnitude is 10.20, but at this wavelength, it has 0.16 magnitudes of interstellar extinction. It appears 3.9 arcminutes wide. NGC 1978 has a radial velocity of 293.1 ± 0.9 km/s.

References

  1. 1 2 3 4 "NASA/IPAC Extragalactic Database". Results for NGC 0330. Retrieved September 2, 2016.
  2. 1 2 3 4 5 6 Song, Ying-Yi; Mateo, Mario; Bailey, John I.; Walker, Matthew G.; Roederer, Ian U.; Olszewski, Edward W.; Reiter, Megan; Kremin, Anthony (2021). "Dynamical masses and mass-to-light ratios of resolved massive star clusters – II. Results for 26 star clusters in the Magellanic Clouds". Monthly Notices of the Royal Astronomical Society. 504 (3): 4160–4191. arXiv: 2104.06882 . doi:10.1093/mnras/stab1065.
  3. ↑ "NGC 330". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved January 1, 2016.
  4. ↑ "New General Catalog Objects: NGC 300 - 349". Cseligman. Retrieved October 30, 2016.
  5. 1 2 Bodensteiner, J.; Sana, H.; Wang, C.; Langer, N.; Mahy, L.; Banyard, G.; de Koter, A.; de Mink, S. E.; Evans, C. J.; Götberg, Y.; Patrick, L. R.; Schneider, F. R. N.; Tramper, F. (2021). "The young massive SMC cluster NGC 330 seen by MUSE. II. Multiplicity properties of the massive-star population". Astronomy & Astrophysics. 652: 18. arXiv: 2104.13409 . Bibcode:2021A&A...652A..70B. doi:10.1051/0004-6361/202140507. S2CID   207852580. A70.


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