IC 1182
{{Short description|Galaxy in the constellation Hercules}}
{{Infobox galaxy|name=IC 1182|image=File:IC1182 - SDSS DR14.jpg|caption=SDSS image of IC 1182|constellation name=Hercules|ra={{RA|16|05|36.8}}|dec={{DEC|+17|48|07.7}}|z=0.034210|h_radial_v=10,206 km/s|dist_ly=464 Mly (142.26 Mpc)|appmag_v=15.19|type=SAO+ pec, HII|size=135,000 ly|names=PGC 57084, UGC 10192, CGCG 108-126, MCG +03-41-104, Mrk 298, AGC 260184, NPM1G+17.0584, 2MASX J16053680+1748078, NVSS J160536+174804, 1RXS J160537.9+174740, KUG 1603+179B, SDSS J160536.78+174807.5, WBL 607-016, 2MASS J16053680+1748075, LEDA 57084|group_cluster=Hercules Cluster|epoch=J2000}}
IC 1182 is a type S0-a{{Cite web |title=HyperLeda -object description |url=http://atlas.obs-hp.fr/hyperleda/ledacat.cgi?o=IC%201182 |access-date=2024-04-30 |website=atlas.obs-hp.fr}} lenticular galaxy located in Hercules.{{Cite web |last=Ford |first=Dominic |title=IC1182 (Galaxy) |url=https://in-the-sky.org//data/object.php?id=IC1182 |access-date=2024-04-30 |website=In-The-Sky.org |language=en}} It is located 464 million light-years away from the Solar System{{Cite web |title=Your NED Search Results |url=https://ned.ipac.caltech.edu/cgi-bin/objsearch?search_type=Obj_id&objid=56010&objname=1&img_stamp=YES&hconst=73.0&omegam=0.27&omegav=0.73&corr_z=1 |access-date=2024-04-30 |website=ned.ipac.caltech.edu}} and was discovered on August 11, 1892, by Stephane Javelle.{{Cite web |title=Index Catalog Objects: IC 1150 - 1199 |url=https://cseligman.com/text/atlas/ic11a.htm#ic1182 |access-date=2024-04-30 |website=cseligman.com}} IC 1198 is a member of the Hercules Cluster, which is a part of the CfA 2 Great Wall.{{Cite web |title=Clusters and Superclusters of Galaxies |url=https://ned.ipac.caltech.edu/level5/Sept01/Bahcall2/Bahcall9_2.html |access-date=2024-04-30 |website=ned.ipac.caltech.edu}}
Description
IC 1182 was originally classified as a Seyfert type 2 galaxy but later, research shows it is an unusual and rare galaxy in some kind of merger event. A jet which is extending out from the center in an easterly direction is composed of kinetic material.{{Cite web |last=information@eso.org |title=The VLT Records Faint Structures in Colliding Galaxies |url=https://www.eso.org/public/news/eso9834/ |access-date=2024-04-30 |website=www.eso.org |language=es}} There is a broad, faint S-shaped plume and debris on the other side of the galaxy. IC 1182 radiates a lot of energy and ejects a substantial amount of material at high velocity. In its central region, clusters of O-type hot blue stars are present.
An ongoing merger?
IC 1182 shows high resolution broad and narrow band images and long slit spectroscopy. It reveals a distorted morphology with a heavily obscured disk-link structure with several knots in its regions.{{Cite journal |last1=Moles |first1=M. |last2=Bettoni |first2=D. |last3=Fasano |first3=G. |last4=Kjærgaard |first4=P. |last5=Varela |first5=J. |last6=Milvang-Jensen |first6=B. |date=2004-05-01 |title=The peculiar galaxy IC 1182: An ongoing merger? |url=https://www.aanda.org/articles/aa/abs/2004/17/aa0295/aa0295.html |journal=Astronomy & Astrophysics |language=en |volume=418 |issue=2 |pages=495–507 |doi=10.1051/0004-6361:20034295 |arxiv=astro-ph/0402219 |bibcode=2004A&A...418..495M |issn=0004-6361}} Some of the galactic material, in the form of two slender tails are detected beyond the main body of the galaxy. IC 1182 has color indices of an early type object which is significantly bluer than what is typical for this kind of galaxy. The narrow lines show this galaxy is a powerful emitter and the knots in the central region and inside the tail emerging eastward from the galaxy are luminous in Hα and have typical sizes of 1 kpc.
Additionally, IC 1182 contains large quantities of neural hydrogen which its distance-independent ratio of hydrogen mass to optical luminosity is equal to 0.7 times the solar ratio.{{Cite journal |last1=Bothun |first1=G. D. |last2=Stauffer |first2=J. R. |last3=Schommer |first3=R. A. |date=1981-07-01 |title=The peculiar galaxy IC 1182. |url=https://ui.adsabs.harvard.edu/abs/1981ApJ...247...42B |journal=The Astrophysical Journal |volume=247 |pages=42–47 |doi=10.1086/159007 |bibcode=1981ApJ...247...42B |issn=0004-637X}} This could indicate it might be involved in a collision involving a gas-rich spiral galaxy which gives rise to observed nuclear emission lines.