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NGC 346

From Wikipedia, the free encyclopedia
Open cluster in the constellation Tucana
NGC 346
Observation data (J2000epoch)
Right ascension00h 59m 05.090s[1]
Declination−72° 10′ 33.24″[1]
Distance210,000light-years
Physical characteristics
H II region
Other designationsESO 51-10,[2] N66
Associations
ConstellationTucana[3]
See also:Open cluster,List of open clusters

NGC 346 is a young[4]open cluster of stars with associatednebula located in theSmall Magellanic Cloud (SMC) that appears in the southernconstellation ofTucana. It was discovered August 1, 1826 by Scottish astronomerJames Dunlop.J. L. E. Dreyer described it as, "bright, large, very irregular figure, much brighter middle similar to double star, mottled but not resolved".[5] On the outskirts of the cluster is themultiple star systemHD 5980,[6] one of the brightest stars in the SMC.

Description

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This cluster is located near the center of the brightestH II region in the SMC, designated N66.[7] This is positioned in the northeast section of thegalactic bar.[8] Stellar surveys have identified 230 massiveOB stars in the direction of this cluster.[4] 33 of the cluster members areO-type stars, with 11 of type O6.5 orearlier.[8] The inner15 pc radius of the cluster appears centrally condensed, while the area outside that volume is more dispersed.[9] The youngest cluster members near the center have ages of less than two million years,[7] and observations suggests the cluster is still engaged in high massstar formation.[7] The cluster star formation rate is estimated at(4±1)×10−3 M yr−1.[9]

Image Gallery

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  • Image of NGC 346 with a 30 arcminute wide field of view showing the wispy nebular structure around it.
    Image of NGC 346 with a 30 arcminute wide field of view showing the wispy nebular structure around it.
  • NGC 346 imaged by the Hubble Space Telescope
    NGC 346 imaged by theHubble Space Telescope
  • James Webb Space Telescope image of star formation in NGC 346
    James Webb Space Telescope image of star formation in NGC 346
Prominent stars[10]
WalbornELSMPGNMCSSNSpectral
type
Effective
temperature (K)
Absolute
magnitude
Bolometric
magnitude
Mass
(M)
207758755
(HD 5980/AB5)
LBV
WN4
OI
45,000
45,000
34,000
−7.1
(−8.1) −6.8
−6.7
−11.135
−10.885
−9.885
61
66
34
1435267O5.5If43,400−6.7−10.791
17895O7If38,900−7−10.785
3355299O3V51,300−5.7−10.376
673243213O4V48,600−5.2−9.654
43423011O5.5V44,900−5.5−9.753
3682815O5.5V44,900−5−9.243
247025O8.5III35,700−5.4−8.934

See also

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References

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  1. ^abSturm, R.; et al. (October 2013). "The XMM-Newton survey of the Small Magellanic Cloud: The X-ray point-source catalogue".Astronomy & Astrophysics.558: 31.arXiv:1307.7594.Bibcode:2013A&A...558A...3S.doi:10.1051/0004-6361/201219935.S2CID 118620464. A3.
  2. ^"NGC 346".SIMBAD.Centre de données astronomiques de Strasbourg. Retrieved2007-04-17.
  3. ^"Hubble Heritage Site".Results for NGC 346. Retrieved2007-04-03.
  4. ^abDufton, P. L.; et al. (February 2020). "The NGC 346 massive star census. Nitrogen abundances for apparently single, narrow lined, hydrogen core burning B-type stars".Astronomy & Astrophysics.634: 15.arXiv:1912.07539.Bibcode:2020A&A...634A...6D.doi:10.1051/0004-6361/201936921.S2CID 209376523. A6.
  5. ^Seligman, Courtney."New General Catalogue objects: NGC 300–349".cseligman.com. Retrieved2020-09-17.
  6. ^Nazé, Y.; et al. (November 2002). "An X-Ray Investigation of the NGC 346 Field in the Small Magellanic Cloud I. The Luminous Blue Variable HD 5980 and the NGC 346 Cluster".The Astrophysical Journal.580 (1):225–234.arXiv:astro-ph/0208289.Bibcode:2002ApJ...580..225N.doi:10.1086/343079.S2CID 118907796.
  7. ^abcDufton, P. L.; et al. (June 2019). "A census of massive stars in NGC 346. Stellar parameters and rotational velocities".Astronomy & Astrophysics.626: 28.arXiv:1905.03359.Bibcode:2019A&A...626A..50D.doi:10.1051/0004-6361/201935415.S2CID 148571638. A50.
  8. ^abRubio, M.; et al. (July 2018). "Massive young stellar objects in the N 66/NGC 346 region of the SMC".Astronomy & Astrophysics.615: 9.arXiv:1803.10833.Bibcode:2018A&A...615A.121R.doi:10.1051/0004-6361/201730487.S2CID 119190580. A121.
  9. ^abHony, S.; et al. (April 2015)."Star formation rates from young-star counts and the structure of the ISM across the NGC 346/N66 complex in the SMC".Monthly Notices of the Royal Astronomical Society.448 (2):1847–1862.arXiv:1501.03634.Bibcode:2015MNRAS.448.1847H.doi:10.1093/mnras/stv107.
  10. ^Massey, Philip; Waterhouse, Elizabeth;DeGioia-Eastwood, Kathleen (May 2000). "The Progenitor Masses of Wolf–Rayet Stars and Luminous Blue Variables Determined from Cluster Turnoffs. I. Results from 19 OB Associations in the Magellanic Clouds".The Astronomical Journal.119 (5):2214–2241.arXiv:astro-ph/0002233.Bibcode:2000AJ....119.2214M.doi:10.1086/301345.ISSN 0004-6256.S2CID 16891188.

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