NGC 1530
Observation data (J2000 epoch)
ConstellationCamelopardalis
Right ascension04h 23m 27.102s[1]
Declination+75° 17′ 44.05″[1]
Redshift0.008209±0.000013[2]
Heliocentric radial velocity2,459 km/s[3]
Galactocentric velocity2,622 km/s[4]
Distance65 Mly (19.9 Mpc)[3]
Apparent magnitude (V)12.3[5]
Apparent magnitude (B)13.40[1]
Characteristics
TypeSB(rs)bc[5]
Apparent size (V)4.6′ × 2.4′[5]
Other designations
2MASX J04232710+7517440, NGC 1530, UGC 3013, LEDA 15018, MCG +13-04-004[6]

NGC 1530 is a barred spiral galaxy in the northern constellation of Camelopardalis. It was discovered by German astronomer W. Tempel in 1876.[7] Danish astronomer J. L. E. Dreyer in 1888 described it only as large and pretty bright.[8] NGC 1530 has an apparent visual magnitude of 12.3[5] and an angular size of 4.6′ × 2.4′.[5] The plane of the galactic disk is inclined at an angle of 55° to the line of sight from the Earth.[9] This galaxy is located at an estimated distance of 65 million light years,[3] with a recessional velocity of 2,622 km/s relative to the Milky Way galaxy.[4] It is a relatively isolated galaxy with its nearest neighbor being NGC 1530A at an angular separation of 19′.[5]

HST partial image of NGC 1530 showing the central region and part of the bar

NGC 1530 has a morphological classification of type SB(rs)bc[5] in the de Vaucouleurs system, which means it is a barred spiral galaxy (SB) with a transitional outer ring structure (rs) that joins somewhat loosely wound arms (bc). The bar structure in this galaxy is unusually large and strong, spanning an angular size of 100″. It includes a clumpy, star-forming nuclear ring structure with a radius of 21″.[9] Star formation is particularly high in the nucleus region and at the ends of the bar, but weak in between these locations.[10] This activity appears to be taking place primarily on the trailing side of the bar where gas pressure is highest.[11] Two linear dust lanes are visible along the bar, which outline shock fronts in the flow of gas.[12]

Mass is flowing into the nuclear ring from the bar at the rate of one solar mass per year[13] with infall velocities of up to 100 km/s.[12] The central region has over 25% of the free gaseous hydrogen in the galaxy.[12] There was some suggestion that the galaxy has a second, inner bar, but this instead appears to be an inner spiral structure. This spiral has one arm brighter than the other, appearing lopsided.[14]

References

  1. 1 2 3 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.
  2. ↑ De Vaucouleurs, Gerard; et al. (1991), Third Reference Catalogue of Bright Galaxies, 9, New York: Springer–Verlag, Bibcode:1991rc3..book.....D, doi:10.1007/978-1-4757-4363-0, ISBN 978-1-4757-4365-4.
  3. 1 2 3 Sorce, J. G.; et al. (October 2014), "From Spitzer Galaxy photometry to Tully–Fisher distances", Monthly Notices of the Royal Astronomical Society, 444 (1): 527–541, arXiv:1408.0729, Bibcode:2014MNRAS.444..527S, doi:10.1093/mnras/stu1450.
  4. 1 2 Tully, R. Brent; et al. (October 2013), "Cosmicflows-2: The Data", The Astronomical Journal, 146 (4): 25, arXiv:1307.7213, Bibcode:2013AJ....146...86T, doi:10.1088/0004-6256/146/4/86, S2CID 118494842, 86.
  5. 1 2 3 4 5 6 7 König, Michael; Binnewies, Stefan (September 7, 2017), The Cambridge Photographic Atlas of Galaxies, Cambridge University Press, p. 89, Bibcode:2017cpag.book.....K, ISBN 9781107189485.
  6. ↑ "NGC 1530", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2023-02-22.
  7. ↑ Steinicke, Wolfgang (2010), Observing and Cataloguing Nebulae and Star Clusters, From Herschel to Dreyer's New General Catalogue, Cambridge University Press, p. 266, ISBN 9781139490108.
  8. ↑ Sulentic, Jack W.; et al. (1973), The Revised New Catalogue of Nonstellar Astronomical Objects, Tucson: University of Arizona Press, Bibcode:1973rncn.book.....S.
  9. 1 2 Regan, Michael W.; et al. (August 1995), "Dust and Molecular Gas in the Barred Spiral Galaxy NGC 1530", Astrophysical Journal, 449: 576, Bibcode:1995ApJ...449..576R, doi:10.1086/176081.
  10. ↑ Reynaud, D.; Downes, D. (September 1998), "Kinematics of the gas in a barred galaxy: do strong shocks inhibit star formation?", Astronomy and Astrophysics, 337: 671–680, Bibcode:1998A&A...337..671R.
  11. ↑ Zurita, A.; et al. (June 2008), Knapen, J. H.; et al. (eds.), "New Clues to Unveiling the Recent Massive Star Formation History in the Bar of NGC 1530", Pathways Through an Eclectic Universe ASP Conference Series, Vol. 390, proceedings of the conference held 23-27 April, 2007 at Santiago del Teide, Tenerife, Spain, San Francisco: Astronomical Society of the Pacific, vol. 390, p. 328, Bibcode:2008ASPC..390..328Z.
  12. 1 2 3 Reynaud, D.; Downes, D. (March 1997), "Shocks and ring in the barred spiral galaxy NGC 1530", Astronomy and Astrophysics, 319: 737–746, Bibcode:1997A&A...319..737R.
  13. ↑ Regan, Michael W.; et al. (June 1997), "The Mass Inflow Rate in the Barred Galaxy NGC 1530", The Astrophysical Journal, 482 (2): L143–L147, arXiv:astro-ph/9704009, Bibcode:1997ApJ...482L.143R, doi:10.1086/310717, S2CID 8750099.
  14. ↑ Erwin, Peter (March 2004), "Double-barred galaxies. I. A catalog of barred galaxies with stellar secondary bars and inner disks", Astronomy and Astrophysics, 415 (3): 941–957, arXiv:astro-ph/0310806, Bibcode:2004A&A...415..941E, doi:10.1051/0004-6361:20034408, S2CID 12717503.

Further reading

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