NGC 1553
Galaxy in the constellation Dorado
title: "NGC 1553" type: doc version: 1 created: 2026-02-28 author: "Wikipedia contributors" status: active scope: public tags: ["lenticular-galaxies", "interacting-galaxies", "dorado", "dorado-group", "ngc-objects", "principal-galaxies-catalogue-objects"] description: "Galaxy in the constellation Dorado" topic_path: "science/astronomy" source: "https://en.wikipedia.org/wiki/NGC_1553" license: "CC BY-SA 4.0" wikipedia_page_id: 0 wikipedia_revision_id: 0
::summary Galaxy in the constellation Dorado ::
::data[format=table title="Infobox Galaxy"]
| Field | Value |
|---|---|
| name | NGC 1553 |
| image | NGC 1553 Hubble.jpg |
| image_size | 250px |
| caption | NGC 1553 core by HST, 0.3′ view |
| epoch | J2000 |
| type | SA(rl)00{{cite web |
| title | NASA/IPAC Extragalactic Database |
| work | Results for NGC 1553 |
| url | http://nedwww.ipac.caltech.edu/ |
| access-date | 2008-07-06}} |
| ra | |
| dec | |
| dist_ly | 78.9 Mly(24.2 Mpc) |
| z | 1080 ± 11 km/s |
| appmag_v | 10.3 |
| size_v | 4′.5 × 2′.8 |
| constellation name | Dorado |
| names | PGC 14765, IRAS 04150-5554, ESO 157-17, and AM 0415-555 |
| :: |
| name = NGC 1553 | image = NGC 1553 Hubble.jpg | image_size = 250px | caption = NGC 1553 core by HST, 0.3′ view | credit = | epoch = J2000 | type = SA(rl)00{{cite web | title=NASA/IPAC Extragalactic Database | work=Results for NGC 1553 | url=http://nedwww.ipac.caltech.edu/ | access-date=2008-07-06}} | ra = | dec = | dist_ly = 78.9 Mly(24.2 Mpc) | z = 1080 ± 11 km/s | appmag_v = 10.3 | size_v = 4′.5 × 2′.8 | constellation name = Dorado | notes = | names = PGC 14765, IRAS 04150-5554, ESO 157-17, and AM 0415-555
NGC 1553 is a prototypical{{citation | bibcode = 2003MNRAS.343..819R | title = Warm gas kinematics in shell galaxies
| date = August 2003 | journal = Monthly Notices of the Royal Astronomical Society | volume = 343 | issue = 3 | pages = 819–830 | doi = 10.1046/j.1365-8711.2003.06721.x | author = Rampazzo, R. |display-authors=4 | author2 =Plana, H. | author3 =Longhetti, M. | author4 =Amram, P. | author5 =Boulesteix, J. | author6 =Gach, J.-L. | author7 =Hernandez, O. | doi-access = free}} lenticular galaxy in the constellation Dorado. It is the second brightest member of the Dorado Group of galaxies.{{citation | bibcode = 1990AJ....100....1F | title = Population studies in groups and clusters of galaxies. III - A catalog of galaxies in five nearby groups
| date = July 1990 | last1 = Ferguson | first1 = Henry C. | last2 = Sandage | first2 = Allan | author-link2 = Allan Sandage | journal = Astronomical Journal | volume = 100 | pages = 1–31 | doi = 10.1086/115486 | doi-access = free | bibcode = 2006MNRAS.372.1856F
| date = November 2006 | title = Kinematics, substructure and luminosity-weighted dynamics of six nearby galaxy groups | journal = Monthly Notices of the Royal Astronomical Society | volume = 372 | issue = 4 | pages = 1856–1868 | doi = 10.1111/j.1365-2966.2006.10993.x | author = Firth, P. |display-authors=4 | author2 =Evstigneeva, E. A. | author3 =Jones, J. B. | author4 =Drinkwater, M. J. | author5 =Phillipps, S. | author6 =Gregg, M. D. | doi-access = free |arxiv = astro-ph/0608584 | s2cid = 18646500 | bibcode = 2005MNRAS.356...77K | title = A Wide-Field HI Study of the NGC 1566 Group
| date = January 2005 | journal = Monthly Notices of the Royal Astronomical Society | volume = 356 | issue = 1 | pages = 77–88 | doi = 10.1111/j.1365-2966.2004.08450.x | author = Virginia A. Kilborn |display-authors=4 | author2 =Bärbel S. Koribalski | author2-link =Bärbel Koribalski | author3 =Duncan A. Forbes | author4 =David G. Barnes | author5 =Ruth C. Musgrave | doi-access=free |arxiv = astro-ph/0409743 }} British astronomer John Herschel discovered NGC 1553 on December 5, 1834 using an 18.7 inch reflector.{{citation |url = http://www.ngcic.org/ngcicdb.asp |archive-url = https://web.archive.org/web/20010904223152/http://www.ngcic.org/ngcicdb.asp |url-status = dead |archive-date = 2001-09-04 |title = The NGC/IC Project: NGC 1553 |author = Robert E. Erdmann Jr. |place = Prescott, Arizona
Interacting galaxy
It forms a pair of interacting galaxies together with elliptical NGC 1549 which lies 11′.8 away from it in the sky.{{citation | bibcode = 2001ApJ...552..106B
| date = May 2001 | title = Diffuse Gas and Low-Mass X-Ray Binaries in the Chandra Observation of the S0 Galaxy NGC 1553 | journal = The Astrophysical Journal | volume = 552 | issue = 1 | pages = 106–119 | doi = 10.1086/320461 | author = Blanton, Elizabeth L. |author-link=Elizabeth Blanton| author2 =Sarazin, Craig L. | author3 =Irwin, Jimmy A. |arxiv = astro-ph/0012481 | s2cid = 15308561 | bibcode = 1990AJ.....99.1100B | title = Globular clusters in the interacting galaxies NGC 1549 and NGC 1553
| date = April 1990 | journal = Astronomical Journal | volume = 99 | pages = 1100–1107, 1340, 1341 | doi = 10.1086/115399 | author = Bridges, Terry J. | author2 =Hanes, David A.
Characteristics
NGC 1553 is an early type galaxy with a luminosity of 4 L⊙. It has been detected{{citation | bibcode = 1991rc3..book.....D | title = Third Reference Catalogue of Bright Galaxies | date = 1991 | author1 = de Vaucouleurs, Gerard |display-authors=4 | author2 =de Vaucouleurs, Antoinette | author3 =Corwin, Herold G. Jr. | author4 =Buta, Ronald J. | author5 =Paturel, Georges | author6 =Fouque, Pascal | publisher = Springer-Verlag | place = Berlin / Heidelberg / New York | isbn = 978-3-540-97552-6 | volume = 1-3
NGC 1553 has an especially well developed lens (~36″) component of nearly constant surface brightness that is found between the bulge and the exponential disk.{{citation | bibcode = 1975IAUS...69..367F | title = Comparison with Observations of Disk Galaxies (invited Paper) | publication-date = 1975 | date = September 9–13, 1974 | journal = Dynamics of Stellar Systems: Proceedings from IAU Symposium | series = 69 | place = Besançon, France | editor-last = Hayli | editor-first = Avram | page = 367 | author = Freeman, K. C. | volume = 69 | bibcode = 1982SAAS...12..115K | title = Observations of galaxy structure and dynamics | last1 = Kormendy | first1 = John | journal = IN: Morphology and Dynamics of Galaxies; Proceedings of the Twelfth Advanced Course | volume = 12 | place = Saas-Fee, Switzerland | date = March 29 – April 3, 1982 | pages = 113–288 | bibcode = 1984ApJ...286..116K
| date = November 1, 1984 | title = The velocity dispersion in the disk of the S0 galaxy NGC 1553 | last1 = Kormendy | first1 = John | journal = Astrophysical Journal, Part 1 | volume = 286 | pages = 116–131 | doi = 10.1086/162581 | doi-access = free
NGC 1553 has associated with itself cool gas and dust. It can also be seen in infrared and is a weak radio source. Hubble observations in 2000 revealed an inner torus-like dust lane about 3″ across at the galaxy's center.
Chandra X-ray imaging of NGC 1553 show diffuse hot gas making up 70% of the emissions, dotted with many point-like sources (low-mass X-ray binaries) making up the rest. Similarly to NGC 4697 and Messier 60, these bright spots are due to binary star systems of black holes and neutron stars most of which are located in globular clusters and reflect this old galaxy's very active past.{{citation | title = Distant Galaxies Had Wild Youth | url = http://vnweb.hwwilsonweb.com/hww/jumpstart.jhtml?recid=0bc05f7a67b1790e050a2140da939dde29bfd13582719af6525c53bb2a79cc3dc929177cf486840a&fmt=H
| date = October 2002 | issn = 0091-6358 | journal = Astronomy | last1 = Talcott | first1 = Richard | volume = 30 | issue = 10 | page = 22 | url = https://chandra.harvard.edu/photo/2002/1058 | title = NGC 1553: Black Holes in Distant Galaxy Points to Wild Youth | publisher = Harvard-Smithsonian Center for Astrophysics | place = Cambridge, MA
| date = August 30, 2006 | author = NASA/CXC/UVa/E.Blanton |display-authors=etal
Globular clusters
Globular clusters have been resolved in the galaxy by the Hubble Space Telescope. There are an estimated 600 globulars in NGC 1553. Like Messier 87, there is a central deficit of globulars with respect to the underlying luminosity.
Spiral feature
NGC 1553 has a roughly symmetrical X-ray spiral feature (not detected in visible light) with a possible 10″ inner bar in the diffuse emission near the center of the galaxy. This feature is probably due to adiabatic or shock compression of ambient gas perhaps due to interaction with the radio source. Hα emission also has spiral structure which is surprisingly similar to the X-ray spiral.
References
::callout[type=info title="Wikipedia Source"] This article was imported from Wikipedia and is available under the Creative Commons Attribution-ShareAlike 4.0 License. Content has been adapted to SurfDoc format. Original contributors can be found on the article history page. ::