View source for NGC 1427

{{Short description|Galaxy in the constellation Fornax}}
{{Infobox Galaxy
| image = NGC 1427 Hubble WikiSky.jpg
| image_size = 270px
| caption = [[Hubble Space Telescope]] image of NGC 1427
| name = [[New General Catalogue|NGC]] 1427
| epoch = [[J2000]]
| type = E5<ref name="ned">{{cite web
  | title=NASA/IPAC Extragalactic Database
  | work=Results for NGC 1427
  | url=http://nedwww.ipac.caltech.edu/
  | access-date=2006-12-13 }}</ref>
| ra = {{RA|03|42|19.4}}<ref name="ned" />
| dec = {{DEC|-35|23|33}}<ref name="ned" />
| dist_ly = [[1 E23 m|71 ± 8]] [[light-year|Mly]] (21.9 ± 2.4 [[parsec|Mpc]])<ref name="jensenetal2003">{{cite journal
  | author=Jensen, Joseph B. |display-authors=4  | author2=Tonry, John L. | author3=Barris, Brian J. | author4=Thompson, Rodger I. | author5=Liu, Michael C. | author6=Rieke, Marcia J. | author7=Ajhar, Edward A. | author8=Blakeslee, John P.
  | title=Measuring Distances and Probing the Unresolved Stellar Populations of Galaxies Using Infrared Surface Brightness Fluctuations
  | journal=Astrophysical Journal
  |date=February 2003
  | volume=583
  | issue=2
  | pages=712–726
  | bibcode=2003ApJ...583..712J
  | doi=10.1086/345430
 |arxiv = astro-ph/0210129 |s2cid=551714 }}</ref>
| z = 0.004630<ref name="ned" />
| appmag_v = 11.8<ref name="ned" />
| size = ~{{convert|33.49|kpc|ly|abbr=on|lk=on|order=flip}} (estimated)<ref name ="ned" />
| constellation name = [[Fornax]]
| notes =Low-luminosity elliptical galaxy 
| names = ESO 358- G 052, MCG -06-09-021, FCC 276, [[Principal Galaxies Catalogue|PGC]] 13609<ref name="ned" />
|h_radial_v=1388 ± 3 km/[[second|s]]<ref name="ned" />|size_v=3.6 x 2.5<ref name ="ned" />|mass=7.9{{e|10}} (Stellar mass)/9.4{{e|10}} (Total Mass)<ref name=":Amblard" />|absmag_v=−20.43<ref>{{Cite journal |last1=Capuzzo-Dolcetta |first1=R. |last2=Mastrobuono-Battisti |first2=A. |date=November 2009 |title=Globular cluster system erosion in elliptical galaxies |url=http://www.aanda.org/10.1051/0004-6361/200912255 |journal=Astronomy & Astrophysics |volume=507 |issue=1 |pages=183–193 |doi=10.1051/0004-6361/200912255 |issn=0004-6361|arxiv=0904.0526 }}</ref>|group_cluster=[[Fornax Cluster]]}}

'''NGC 1427''' is a low-luminosity [[elliptical galaxy]]<ref name=":0">{{Cite journal |last1=Forte |first1=Juan C. |last2=Geisler |first2=Doug |last3=Ostrov |first3=Pablo G. |last4=Piatti |first4=Andrés E. |last5=Gieren |first5=Wolfgang |date=2001-04-01 |title=The Globular Cluster System of the Low-Luminosity Elliptical Galaxy NGC 1427 |url=https://ui.adsabs.harvard.edu/abs/2001AJ....121.1992F |journal=The Astronomical Journal |volume=121 |issue=4 |pages=1992–2002 |doi=10.1086/319954 |bibcode=2001AJ....121.1992F |issn=0004-6256|hdl=11336/22471 |hdl-access=free }}</ref> located approximately 71 million [[light-years]] away from [[Earth]].<ref name="jensenetal2003"/> It was discovered by John Frederick William Herschel on November 28, 1837.<ref>{{Cite web |title=New General Catalog Objects: NGC 1400 - 1449 |url=https://cseligman.com/text/atlas/ngc14.htm#1427 |access-date=2024-07-08 |website=cseligman.com}}</ref> It is a member of the [[Fornax Cluster]].<ref>{{Cite journal |last=Ferguson |first=Henry C. |date=August 1989 |title=Population studies in groups and clusters of galaxies. II - A catalog of galaxies in the central 3.5 deg of the Fornax Cluster |url=http://adsabs.harvard.edu/cgi-bin/bib_query?1989AJ.....98..367F |journal=The Astronomical Journal |volume=98 |pages=367 |doi=10.1086/115152|bibcode=1989AJ.....98..367F }}</ref><ref name=Zhu/> The galaxy has a [[Star|stellar]] mass of 7.9 × 10<sup>10</sup> [[Solar mass|<var>M</var><sub>☉</sub>]], and a total mass of 9.4 × 10<sup>10</sup> [[Solar mass|<var>M</var><sub>☉</sub>]].<ref name=":Amblard">{{Cite journal |last1=Amblard |first1=A. |last2=Riguccini |first2=L. |last3=Temi |first3=P. |last4=Im |first4=S. |last5=Fanelli |first5=M. |last6=Serra |first6=P. |date=2014-03-01 |title=Star Formation Bimodality in Early-type Galaxies |url=https://ui.adsabs.harvard.edu/abs/2014ApJ...783..135A |journal=The Astrophysical Journal |volume=783 |issue=2 |pages=135 |doi=10.1088/0004-637X/783/2/135 |arxiv=1309.5418 |bibcode=2014ApJ...783..135A |issn=0004-637X}}</ref> However, the mass of the [[dark matter halo]] surrounding the galaxy is around 4.3 × 10<sup>12</sup> [[Solar mass|<var>M</var><sub>☉</sub>]].<ref>{{Cite journal |last1=Spitler |first1=Lee R. |last2=Forbes |first2=Duncan A. |last3=Strader |first3=Jay |last4=Brodie |first4=Jean P. |last5=Gallagher |first5=Jay S. |date=2008-03-01 |title=The connection between globular cluster systems and their host galaxy and environment: a case study of the isolated elliptical NGC 821 |journal=Monthly Notices of the Royal Astronomical Society |volume=385 |issue=1 |pages=361–380 |doi=10.1111/j.1365-2966.2007.12823.x |doi-access=free |arxiv=0712.1382 |bibcode=2008MNRAS.385..361S |issn=0035-8711}}</ref>

==Characteristics==
NGC 1427 is the brightest elliptical galaxy on the eastern side of the Fornax cluster, and is thought to have been accreted into the gravtional potential well of the cluster core more than 8 billion years ago.<ref name="Zhu" /> It is around 9 billion years old.<ref>{{Cite journal |last1=Lee |first1=Sang-Yoon |last2=Chung |first2=Chul |last3=Yoon |first3=Suk-Jin |date=2019-01-01 |title=Nonlinear Color-Metallicity Relations of Globular Clusters. VIII. Reproducing Color Distributions of Individual Globular Cluster Systems in the Virgo and Fornax Galaxy Clusters |journal=The Astrophysical Journal Supplement Series |volume=240 |issue=1 |pages=2 |doi=10.3847/1538-4365/aaecd4 |doi-access=free |arxiv=1811.00018 |bibcode=2019ApJS..240....2L |issn=0067-0049}}</ref>

In the galaxy, dust patches are observed,<ref>{{Cite journal |last1=Forbes |first1=Duncan A. |last2=Franx |first2=Marijn |last3=Illingworth |first3=Garth D. |date=1995-05-01 |title=Ellipticals with Kinematically Distinct Cores: WFPC1 Imaging of Nearby Ellipticals |url=https://ui.adsabs.harvard.edu/abs/1995AJ....109.1988F |journal=The Astronomical Journal |volume=109 |pages=1988 |doi=10.1086/117425 |bibcode=1995AJ....109.1988F |issn=0004-6256}}</ref> with the central region being host to a [[nuclear stellar disk]] with an estimated diameter of {{convert|16|pc|ly|abbr=on|lk=on|order=flip}}.<ref>{{Cite journal |last1=Ledo |first1=H. R. |last2=Sarzi |first2=M. |last3=Dotti |first3=M. |last4=Khochfar |first4=S. |last5=Morelli |first5=L. |date=2010-09-01 |title=A census of nuclear stellar discs in early-type galaxies |journal=Monthly Notices of the Royal Astronomical Society |volume=407 |issue=2 |pages=969–985 |doi=10.1111/j.1365-2966.2010.16990.x |doi-access=free |bibcode=2010MNRAS.407..969L |issn=0035-8711|hdl=2299/5422 |hdl-access=free }}</ref> NGC 1427 is surrounded by 71 observed [[planetary nebula]]e.<ref>{{Cite journal |last1=Spriggs |first1=T. W. |last2=Sarzi |first2=M. |last3=Galán-de Anta |first3=P. M. |last4=Napiwotzki |first4=R. |last5=Viaene |first5=S. |last6=Nedelchev |first6=B. |last7=Coccato |first7=L. |last8=Corsini |first8=E. M. |last9=Fahrion |first9=K. |last10=Falcón-Barroso |first10=J. |last11=Gadotti |first11=D. A. |last12=Iodice |first12=E. |last13=Lyubenova |first13=M. |last14=Martín-Navarro |first14=I. |last15=McDermid |first15=R. M. |date=2021-09-01 |title=The Fornax3D project: Planetary nebulae catalogue and independent distance measurements to Fornax cluster galaxies |url=https://ui.adsabs.harvard.edu/abs/2021A&A...653A.167S |journal=Astronomy and Astrophysics |volume=653 |pages=A167 |doi=10.1051/0004-6361/202141314 |issn=0004-6361|arxiv=2107.09680 |bibcode=2021A&A...653A.167S }}</ref>

The galaxy has a [[supermassive black hole]] with an estimated mass of 9.1 × 10<sup>7</sup> [[Solar mass|<var>M</var><sub>☉</sub>]].<ref>{{Cite journal |last1=Arzoumanian |first1=Zaven |last2=Baker |first2=Paul T. |last3=Brazier |first3=Adam |last4=Brook |first4=Paul R. |last5=Burke-Spolaor |first5=Sarah |last6=Becsy |first6=Bence |last7=Charisi |first7=Maria |last8=Chatterjee |first8=Shami |last9=Cordes |first9=James M. |last10=Cornish |first10=Neil J. |last11=Crawford |first11=Fronefield |last12=Cromartie |first12=H. Thankful |last13=Decesar |first13=Megan E. |last14=Demorest |first14=Paul B. |last15=Dolch |first15=Timothy |date=2021-06-01 |title=The NANOGrav 11 yr Data Set: Limits on Supermassive Black Hole Binaries in Galaxies within 500 Mpc |journal=The Astrophysical Journal |volume=914 |issue=2 |pages=121 |doi=10.3847/1538-4357/abfcd3 |doi-access=free |arxiv=2101.02716 |bibcode=2021ApJ...914..121A |issn=0004-637X}}</ref>

=== Globular clusters ===
NGC 1427 is surrounded by a population of around 470 [[globular cluster]]s, however estimates suggest that number may be as high as 510. It has a biomedial distribution of one population of metal-rich red clusters and another population of metal-poor blue clusters. The blue globular clusters have an abundance ratio of [Fe/H] = -1.02 ± 0.2, greater than that of the globular clusters in the halo of the [[Milky Way]], while the red globular clusters have an abundance ratio of [Fe/H] = -0.15 making them more metal rich than the globular clusters in the [[Galactic bulge|bulge]] of the Milky Way. This suggests that the red globular clusters have more similarities to the metal-rich globular clusters found in [[disk galaxies]] unlike in giant elliptical galaxies like [[Messier 87|M87]]. Therefore as the red globular clusters have a higher [[metallicity]] than the blue globular clusters, this suggests that red globular clusters are younger than the blue global clusters, possibly having formed from ether galaxy mergers or another local galactic processes.<ref name=":0" />

=== Galaxy mergers ===
[[Computer simulation]]s and observations of the inner [[stellar halo]] of NGC 1427,  by Zhu et al. suggest that the formation of the galaxy's stellar halo requires the [[Galaxy merger|merger]] of a massive satellite galaxy of around  {{solar mass|{{val|1.5|+1.6|-0.7|e=10}}|link=yes}} with NGC 1427 which is about one-fourth of its current stellar mass.

Also, the stars in NGC 1427's stellar halo are younger than most stars in the bulge; with these stars being the youngest in the galaxy. The stellar age distribution of the hot inner stellar halo of NGC 1427 indicates that this merger occurred within the last 8 billion years. Based on current understanding of galaxy evolution, stars in the inner halo of NGC 1427 should have formed before the massive merger ended, either in a preexisting disk of NGC 1427 or in the satellite galaxy before and during the merger, because of the triggering of [[star formation]].<ref name="Zhu">{{cite journal | doi=10.1051/0004-6361/202243109| title=The Fornax3D project: Discovery of ancient massive merger events in the Fornax cluster galaxies NGC 1380 and NGC 1427| year=2022| last1=Zhu| first1=Ling| last2=Van De Ven| first2=Glenn| last3=Leaman| first3=Ryan| last4=Pillepich| first4=Annalisa| last5=Coccato| first5=Lodovico| last6=Ding| first6=Yuchen| last7=Falcón-Barroso| first7=Jesús| last8=Iodice| first8=Enrichetta| last9=Navarro| first9=Ignacio Martin| last10=Pinna| first10=Francesca| last11=Corsini| first11=Enrico Maria| last12=Gadotti| first12=Dimitri A.| last13=Fahrion| first13=Katja| last14=Lyubenova| first14=Mariya| last15=Mao| first15=Shude| last16=McDermid| first16=Richard| last17=Poci| first17=Adriano| last18=Sarzi| first18=Marc| last19=De Zeeuw| first19=Tim| journal=Astronomy & Astrophysics| volume=664| pages=A115| arxiv=2203.15822| bibcode=2022A&A...664A.115Z| s2cid=247793082}}</ref>

==References==
{{reflist}}

==External links==
* {{commons category-inline}}
* {{WikiSky}}

{{Sky|03|42|19.4|-|35|23|34|71000000}}
{{NGC objects:1000-1499}}
{{Fornax}}

{{DEFAULTSORT:NGC 1427}}
[[Category:Elliptical galaxies]]
[[Category:Fornax Cluster]]
[[Category:Fornax]]
[[Category:NGC objects|1427]]
[[Category:Principal Galaxies Catalogue objects|13609]]
[[Category:Astronomical objects discovered in 1837]]