NGC 1546 is alenticular galaxy in the constellationDorado. The galaxy lies about 55 millionlight years away from Earth, which means, given its apparent dimensions, that NGC 1546 is approximately 60,000 light years across.[1] It was discovered byJohn Herschel on December 5, 1834.[3] It is a member of theDorado Group.[4]
The galaxy is seen nearly edge-on, with an inclination of 70°. The galaxy has a high surface brightnessspiral arm pattern. The multiple spiral arms are in a pattern that is similar to that of an Scspiral galaxy. In older images that disk appeared to have no structure, leading the galaxy to be categorised as a lenticular galaxy.[5] TheH-alpha and [N II] emission is distributed in a flocculent pattern.[6] The galaxy features an inner ring, with a radius of 26 arcseconds, and an outer pseudoring 0.96 arcminutes across, which have both been detected ininfrared and far ultraviolet.[7][8] There areH II regions at both rings.[6] The total star formation rate of the galaxy is estimated to be 0.83M☉ per year.[9]
A series of dust lanes, some of which are backlit by the galaxy's core. This dust absorbs light from the core, reddening it and making the dust appear rusty-brown. The core itself glows brightly in a yellowish light indicating an older population of stars. Brilliant-blue regions of active star formation sparkle through the dust.[10] The galaxy doesn't show evidence of an outflow from the nucleus.[11] It has diffuse far ultraviolet emission from the outer regions of the galaxy and a diffuse halo. A faint shell is visible south-east of the galaxy.[7]
^Maia, M. A. G.; da Costa, L. N.; Latham, David W. (April 1989). "A catalog of southern groups of galaxies".The Astrophysical Journal Supplement Series.69: 809.Bibcode:1989ApJS...69..809M.doi:10.1086/191328.
^Sandage, A., Bedke, J. (1994),The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington
^abRampazzo, R.; Ciroi, S.; Mazzei, P.; Mille, F. Di; Congiu, E.; Cattapan, A.; Bianchi, L.; Iodice, E.; Marino, A.; Plana, H.; Postma, J.; Spavone, M. (1 November 2020). "Dorado and its member galaxies - Hα imaging of the group backbone".Astronomy & Astrophysics.643: A176.arXiv:2009.14731.Bibcode:2020A&A...643A.176R.doi:10.1051/0004-6361/202038996.
^abcRampazzo, R.; Mazzei, P.; Marino, A.; Bianchi, L.; Postma, J.; Ragusa, R.; Spavone, M.; Iodice, E.; Ciroi, S.; Held, E. V. (August 2022). "Dorado and its member galaxies: III. Mapping star formation with FUV imaging from UVIT".Astronomy & Astrophysics.664: A192.arXiv:2206.01578.Bibcode:2022A&A...664A.192R.doi:10.1051/0004-6361/202243726.
^Comerón, S.; Salo, H.; Laurikainen, E.; Knapen, J. H.; Buta, R. J.; Herrera-Endoqui, M.; Laine, J.; Holwerda, B. W.; Sheth, K.; Regan, M. W.; Hinz, J. L.; Muñoz-Mateos, J. C.; Gil de Paz, A.; Menéndez-Delmestre, K.; Seibert, M.; Mizusawa, T.; Kim, T.; Erroz-Ferrer, S.; Gadotti, D. A.; Athanassoula, E.; Bosma, A.; Ho, L. C. (February 2014). "ARRAKIS: atlas of resonance rings as known in the S 4 G".Astronomy & Astrophysics.562: A121.arXiv:1312.0866.doi:10.1051/0004-6361/201321633.
^Neumann, Lukas; Gallagher, Molly J; Bigiel, Frank; Leroy, Adam K; Barnes, Ashley T; Usero, Antonio; den Brok, Jakob S; Belfiore, Francesco; Bešlić, Ivana; Cao, Yixian; Chevance, Mélanie; Dale, Daniel A; Eibensteiner, Cosima; Glover, Simon C O; Grasha, Kathryn; Henshaw, Jonathan D; Jiménez-Donaire, María J; Klessen, Ralf S; Kruijssen, J M Diederik; Liu, Daizhong; Meidt, Sharon; Pety, Jérôme; Puschnig, Johannes; Querejeta, Miguel; Rosolowsky, Erik; Schinnerer, Eva; Schruba, Andreas; Sormani, Mattia C; Sun, Jiayi; Teng, Yu-Hsuan; Williams, Thomas G (23 March 2023)."The ALMOND survey: molecular cloud properties and gas density tracers across 25 nearby spiral galaxies with ALMA".Monthly Notices of the Royal Astronomical Society.521 (3):3348–3383.arXiv:2302.03042.doi:10.1093/mnras/stad424.
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This article incorporates text from this source, which is in thepublic domain."NASA Releases Hubble Image Taken in New Pointing Mode - NASA Science".science.nasa.gov. NASA. 18 June 2024. Retrieved8 February 2025.
