IC 5337
{{Short description|Galaxy in the constellation Pegasus}}
{{Infobox galaxy|name=IC 5337|image=File:IC5337 IC5338 potw2312a.jpg|constellation name=Pegasus|caption=Hubble Space Telescope image of IC 5337 (lower right) and IC 5338 (upper left)|z=0.054988|dist_ly=800 Mly (245.2 Mpc)|type=S0, S?|h_radial_v=16,485 km/s|ra={{RA|23h|36|25.03}}|group_cluster=Abell 2626|size=175,000 ly (estimated)|appmag_v=0.17|names=PGC 71875, MCG +03-60-012, AGC 330572, 2MASX J23362506+2109028, LEDA 71875, Z455-25, JW100|epoch=J2000|dec={{DEC|+21|09|01.98}}|size_v=0.8' x 0.1'|appmag_b=0.23}}
IC 5337 or JW100, is a spiral galaxy located 800 million light-years away from the Solar System in the constellation of Pegasus.{{Cite web |title=Your NED Search Results |url=https://ned.ipac.caltech.edu/cgi-bin/objsearch?search_type=Obj_id&objid=54168&objname=1&img_stamp=YES&hconst=73.0&omegam=0.27&omegav=0.73&corr_z=1 |access-date=2024-04-20 |website=ned.ipac.caltech.edu}}{{Cite web |title=IC 5337 - Spiral Galaxy in Pegasus {{!}} TheSkyLive.com |url=https://theskylive.com/sky/deepsky/ic5337-object |access-date=2024-04-20 |website=theskylive.com}}
It was discovered by French astronomer, Stephane Javelle on November 25, 1897{{Cite web |title=Index Catalog Objects: IC 5300 - 5349 |url=https://cseligman.com/text/atlas/ic53.htm#ic5337 |access-date=2024-04-20 |website=cseligman.com}} and is probably gravitationally bound to IC 5338, the brightest cluster galaxy in Abell 2626. According to SIMBAD, IC 5337 is considered an emission-line galaxy.{{Cite web |title=IC 5337 |url=https://simbad.u-strasbg.fr/simbad/sim-basic |access-date=2024-04-20 |website=simbad.u-strasbg.fr}}
IC 5337 is a jellyfish galaxy, mainly due to ram pressure.{{Cite web |last=information@eso.org |title=Portrait of a galactic jellyfish |url=https://www.spacetelescope.org/images/potw2312a/ |access-date=2024-04-20 |website=www.spacetelescope.org |language=en}}{{Cite web |last=information@eso.org |title=Example of a jellyfish galaxy |url=https://www.eso.org/public/images/eso1725b/ |access-date=2024-04-20 |website=www.eso.org |language=en}}{{Cite journal |last1=Poggianti |first1=B. M. |last2=Fasano |first2=G. |last3=Omizzolo |first3=A. |last4=Gullieuszik |first4=M. |last5=Bettoni |first5=D. |last6=Moretti |first6=A. |last7=Paccagnella |first7=A. |last8=Jaffé |first8=Y. L. |last9=Vulcani |first9=B. |last10=Fritz |first10=J. |last11=Couch |first11=W. |last12=D'Onofrio |first12=M. |date=2016-03-01 |title=Jellyfish Galaxy Candidates at Low Redshift |journal=The Astronomical Journal |volume=151 |issue=3 |pages=78 |doi=10.3847/0004-6256/151/3/78 |doi-access=free |arxiv=1504.07105 |bibcode=2016AJ....151...78P |issn=0004-6256}} Star-forming gas are thrown about, as the galaxy penetrates through the thin gas layer and causing them to drip from the galaxy's disc, giving it its unique appearance of a cosmic jellyfish. It has a stellar mass of 3.2 × 1011 M⊙{{Cite journal |last1=Poggianti |first1=Bianca M. |last2=Ignesti |first2=Alessandro |last3=Gitti |first3=Myriam |last4=Wolter |first4=Anna |last5=Brighenti |first5=Fabrizio |last6=Biviano |first6=Andrea |last7=George |first7=Koshy |last8=Vulcani |first8=Benedetta |last9=Gullieuszik |first9=Marco |last10=Moretti |first10=Alessia |last11=Paladino |first11=Rosita |last12=Bettoni |first12=Daniela |last13=Franchetto |first13=Andrea |last14=Jaffé |first14=Yara L. |last15=Radovich |first15=Mario |date=2019-12-01 |title=GASP XXIII: A Jellyfish Galaxy as an Astrophysical Laboratory of the Baryonic Cycle |journal=The Astrophysical Journal |volume=887 |issue=2 |pages=155 |doi=10.3847/1538-4357/ab5224 |doi-access=free |arxiv=1910.11622 |bibcode=2019ApJ...887..155P |issn=0004-637X}} and contains an active galactic nucleus likely trigged by accretion of matter into its supermassive black hole.{{Cite journal |last1=Poggianti |first1=Bianca M. |last2=Jaffé |first2=Yara L. |last3=Moretti |first3=Alessia |last4=Gullieuszik |first4=Marco |last5=Radovich |first5=Mario |last6=Tonnesen |first6=Stephanie |last7=Fritz |first7=Jacopo |last8=Bettoni |first8=Daniela |last9=Vulcani |first9=Benedetta |last10=Fasano |first10=Giovanni |last11=Bellhouse |first11=Callum |last12=Hau |first12=George |last13=Omizzolo |first13=Alessandro |date=2017-08-01 |title=Ram-pressure feeding of supermassive black holes |url=https://ui.adsabs.harvard.edu/abs/2017Natur.548..304P |journal=Nature |volume=548 |issue=7667 |pages=304–309 |doi=10.1038/nature23462 |pmid=28816245 |arxiv=1708.09036 |bibcode=2017Natur.548..304P |issn=0028-0836}}
In addition, IC 5337 also shows an X-ray source.{{Cite journal |last1=Wong |first1=Ka-Wah |last2=Sarazin |first2=Craig L. |last3=Blanton |first3=Elizabeth L. |last4=Reiprich |first4=Thomas H. |date=2008-07-01 |title=XMM-Newton and Chandra Observations of Abell 2626: Interacting Radio Jets and Cooling Core with Jet Precession? |url=https://ui.adsabs.harvard.edu/abs/2008ApJ...682..155W |journal=The Astrophysical Journal |volume=682 |issue=1 |pages=155–174 |doi=10.1086/588272 |arxiv=0803.1680 |bibcode=2008ApJ...682..155W |issn=0004-637X}}