NGC 1530

NGC 1530
NGC 1530
Observation data (J2000 epoch)
Constellation	Camelopardalis
Right ascension	04h 23m 27.102s
Declination	+75° 17′ 44.05″
Redshift	0.008209±0.000013
Helio radial velocity	2,459 km/s
Galactocentric velocity	2,622 km/s
Distance	65 Mly (19.9 Mpc)
Apparent magnitude (V)	12.3
Apparent magnitude (B)	13.40
Characteristics
Type	SB(rs)bc
Apparent size (V)	4.6′ × 2.4′
Other designations
	2MASX J04232710+7517440, NGC 1530, UGC 3013, LEDA 15018, MCG +13-04-004

Last updated August 15, 2023

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]

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]

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The Black Eye Galaxy is a relatively isolated spiral galaxy 17 million light-years away in the mildly northern constellation of Coma Berenices. It was discovered by Edward Pigott in March 1779, and independently by Johann Elert Bode in April of the same year, as well as by Charles Messier the next year. A dark band of absorbing dust partially in front of its bright nucleus gave rise to its nicknames of the "Black Eye", "Evil Eye", or "Sleeping Beauty" galaxy. M64 is well known among amateur astronomers due to its form in small telescopes and visibility across inhabited latitudes.

NGC 4725 is an intermediate barred spiral galaxy with a prominent ring structure, located in the northern constellation of Coma Berenices near the north galactic pole. It was discovered by German-born astronomer William Herschel on April 6, 1785. The galaxy lies at a distance of approximately 40 megalight-years from the Milky Way.

NGC 2787 is a barred lenticular galaxy approximately 24 million light-years away in the northern constellation of Ursa Major. It was discovered on December 3, 1788 by German-born astronomer William Herschel. J. L. E. Dreyer described it as, "bright, pretty large, a little extended 90°, much brighter middle, mottled but not resolved, very small (faint) star involved to the southeast". The visible galaxy has an angular size of 2.5 × 1.5 arcminutes or 3.24 × 1.81 arcminutes and an apparent visual magnitude of 11.8.

NGC 2903 is an isolated barred spiral galaxy in the equatorial constellation of Leo, positioned about 1.5° due south of Lambda Leonis. It was discovered by German-born astronomer William Herschel, who cataloged it on November 16, 1784. He mistook it as a double nebula, as did subsequent observers, and it wasn't until the nineteenth century that the Third Earl of Rosse resolved into a spiral form. J. L. E. Dreyer assigned it the identifiers 2903 and 2905 in his New General Catalogue; NGC 2905 now designates a luminous knot in the northeastern spiral arm.

<span class="mw-page-title-main">NGC 2997</span> Galaxy in the constellation Antlia

NGC 2997 is a face-on unbarred spiral galaxy about 40 million light-years away in the faint southern constellation of Antlia. It was discovered March 4, 1793 by German-born astronomer William Herschel. J. L. E. Dreyer described it as, "a remarkable object, very faint, very large, very gradually then very suddenly bright middle and 4 arcsec nucleus. This is the brightest galaxy of the NGC 2997 group of galaxies, and was featured on the cover of the first edition of Galactic Dynamics by James Binney and Scott Tremaine.

NGC 5398 is a barred spiral galaxy in the southern constellation of Centaurus. It was discovered June 3, 1836 by John Herschel. Distance estimates range from 5.39 Mpc to 18.30 Mpc. The tip of the red-giant branch method yields a distance of 11.6 Mpc, while the Tully–Fisher relation shows values of around 8.5 Mpc. It is receding with a heliocentric radial velocity of 1,219 km/s.

NGC 4639 is a barred spiral galaxy located in the equatorial constellation of Virgo. It was discovered by German-born astronomer William Herschel on April 12, 1784. John L. E. Dreyer described it as "pretty bright, small, extended, mottled but not resolved, 12th magnitude star 1 arcmin to southeast". This is a relatively nearby galaxy, lying approximately 72 million light-years away from the Milky Way. It is a companion to NGC 4654, and the two appear to have interacted roughly 500 million years ago. NGC 4639 is a member of the Virgo Cluster.

NGC 1808 is a barred spiral galaxy located in the southern constellation of Columba, about two degrees to the south and east of Gamma Caeli. It was discovered by Scottish astronomer James Dunlop, who described it as a "faint nebula". The galaxy is a member of the NGC 1808 group, which is part of the larger Dorado Group.

NGC 5962 is a spiral galaxy in the equatorial constellation of Serpens Caput. It was discovered by the Anglo-German astronomer William Herschel on March 21, 1784. The NGC 5962 galaxy is located at a distance of 120 million light years and is receding with a heliocentric radial velocity of 1,957 km/s. It is the brightest member of the eponymously-named NGC 5962 group, which overlaps with the nearby NGC 5970 group; the two groups may be gravitationally bound.

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NGC 2397 is a flocculent spiral galaxy located in the southern Volans constellation, about one degree to the SSE of Delta Volantis. English astronomer John Herschel discovered the galaxy on February 21, 1835. It is located at a distance of approximately 69 million light years from the Sun, and is a member of the small NGC 2442 group that includes NGC 2434.

NGC 4178 is the New General Catalogue identifier for a barred spiral galaxy in the equatorial constellation of Virgo. It was discovered April 11, 1825 by English astronomer John Herschel. Located some 43.8 million light years away, this galaxy spans 2.3 × 0.4 arc minutes and is seen at a low angle, being inclined by 77° to the line of sight from the Earth. The morphological classification of NGC 4178 is SB(rs)dm, indicating that it has a bar feature at the core, and, per the '(rs)', has traces of a ring-like structure surrounding the bar. The 'dm' suffix indicates the spiral arms are diffuse, broken, and irregular in appearance with no bulge at the nucleus. This galaxy is a member of the Virgo Cluster, which is the richest nearby group of galaxies outside the Local Group and forms the core of the Virgo Supercluster.

<span class="mw-page-title-main">NGC 672</span> Galaxy in the constellation Triangulum

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NGC 3175 is a spiral galaxy located in the far eastern part of the southern constellation of Antlia at an approximate distance of 54 million light-years. NGC 3175 was discovered on March 30, 1835 by English astronomer John Herschel, whose notes described it as, "considerably bright, large, much extended NE-SW, very gradually little brighter middle". This galaxy is the namesake of the NGC 3175 group of galaxies, which includes the spiral galaxy NGC 3137.

References

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↑ 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.
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 .
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.
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.
↑ "NGC 1530", SIMBAD , Centre de données astronomiques de Strasbourg , retrieved 2023-02-22.
↑ 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.
↑ Sulentic, Jack W.; et al. (1973), The Revised New Catalogue of Nonstellar Astronomical Objects, Tucson: University of Arizona Press, Bibcode:1973rncn.book.....S.
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.
↑ 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.
↑ 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.
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.
↑ 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.
↑ 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.

NGC 1530

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