NGC 4096

{{Short description|Spiral galaxy in the constellation Ursa Major}}

{{Infobox galaxy

| name = NGC 4096

| image = NGC4096 - SDSS DR14.jpg

| caption = NGC 4096 by Sloan Digital Sky Survey

| epoch = J2000

| type = SAB(rs)c {{cite web

| title=NASA/IPAC Extragalactic Database

| work=Results for NGC 4096

| url=http://ned.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=NGC+4096

| access-date=2024-03-26 }}

| ra = {{RA|12|06|01.1}}

| dec = {{DEC|+47|28|43}}

| dist_ly = 37.5 ± 7.8 Mly (11.5 ± 2.4 Mpc)

| z = 0.001908 ± 0.000007

| h_radial_v = 572 ± 2 km/s

| appmag_v = 10.8{{cite web |title=Revised NGC Data for NGC 4096 |url=https://spider.seds.org/ngc/revngcic.cgi?NGC4096 |website=spider.seds.org |access-date=30 March 2024}}

| size_v = 4.39{{prime}} × 1.04{{prime}}

| constellation name = Ursa Major

| notes =

| names = UGC 7090, MCG +08-22-067, CGCG 243-043, IRAS 12034+4745, PGC 38361

}}

NGC 4096 is a spiral galaxy in the constellation Ursa Major. The galaxy lies about 35 million light years away from Earth, which means, given its apparent dimensions, that NGC 4096 is approximately 80,000 light years across. It was discovered by William Herschel on March 9, 1788.{{cite web |last1=Seligman |first1=Courtney |title=NGC 4096 (= PGC 38361) |url=https://cseligman.com/text/atlas/ngc40a.htm#4096 |website=Celestial Atlas |access-date=19 November 2018}}

NGC 4096 is a spiral galaxy visible with an inclination of 76°. Although the presence of a bar has been suggested, it hasn't been proven.{{cite journal |last1=Dullo |first1=B. T. |last2=Knapen |first2=J. H. |last3=Beswick |first3=R. J. |last4=Baldi |first4=R. D. |last5=Williams |first5=D. R. A. |last6=McHardy |first6=I. M. |last7=Gallagher |first7=J. S. |last8=Aalto |first8=S. |last9=Argo |first9=M. K. |last10=Gil de Paz |first10=A. |last11=Klöckner |first11=H.-R. |last12=Marcaide |first12=J. M. |last13=Mundell |first13=C. G. |last14=Mutie |first14=I. M. |last15=Saikia |first15=P. |title=LeMMINGs: V. Nuclear activity and bulge properties: A detailed multi-component decomposition of e -MERLIN Palomar galaxies with HST |journal=Astronomy & Astrophysics |date=July 2023 |volume=675 |pages=A105 |doi=10.1051/0004-6361/202345913|arxiv=2303.11154 |bibcode=2023A&A...675A.105D }} The galaxy has multiple well-defined thin arms.Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington NGC 4096 is asymmetric in the north–south axis, with the northern half having stronger CO emissions{{cite journal |last1=Sofue |first1=Yoshiaki |last2=Tutui |first2=Yoshinori |last3=Honma |first3=Mareki |last4=Tomita |first4=Akihiko |title=Nuclear Rotation Curves of Galaxies in the Co-Line Emission |journal=The Astronomical Journal |date=December 1997 |volume=114 |pages=2428 |doi=10.1086/118657|arxiv=astro-ph/9709115 |bibcode=1997AJ....114.2428S }} and asymmetric HI and H-alpha emissions following a lopsided spiral arm.{{cite journal |last1=Zheng |first1=Yun |last2=Wang |first2=Jing |last3=Irwin |first3=Judith |last4=English |first4=Jayanne |last5=Ma |first5=Qingchuan |last6=Wang |first6=Ran |last7=Wang |first7=Ke |last8=Wang |first8=Q Daniel |last9=Krause |first9=Marita |last10=Randriamampandry |first10=Toky H |last11=Li |first11=Jiangtao |last12=Beck |first12=Rainer |title=CHANG-ES XXV: H i imaging of nearby edge-on galaxies – Data Release 4 |journal=Monthly Notices of the Royal Astronomical Society |date=29 April 2022 |volume=513 |issue=1 |pages=1329–1353 |doi=10.1093/mnras/stac760|doi-access=free |arxiv=2203.07818 }} The total stellar mass of the galaxy is estimated to be {{val|6.13|0.1|e=9|ul=M_solar}}.{{cite journal |last1=Lu |first1=Li-Yuan |last2=Li |first2=Jiang-Tao |last3=Vargas |first3=Carlos J |last4=Beck |first4=Rainer |last5=Bregman |first5=Joel N |last6=Dettmar |first6=Ralf-Jürgen |last7=English |first7=Jayanne |last8=Fang |first8=Taotao |last9=Heald |first9=George H |last10=Li |first10=Hui |last11=Qu |first11=Zhijie |last12=Rand |first12=Richard J |last13=Stein |first13=Michael |last14=Wang |first14=Q Daniel |last15=Wang |first15=Jing |last16=Wiegert |first16=Theresa |last17=Zheng |first17=Yun |title=eDIG-CHANGES I: extended Hα emission from the extraplanar diffuse ionized gas (eDIG) around CHANG-ES galaxies |journal=Monthly Notices of the Royal Astronomical Society |date=17 January 2023 |volume=519 |issue=4 |pages=6098–6110 |doi=10.1093/mnras/stad006|doi-access=free |arxiv=2212.14824 }} The star formation rate of the galaxy is estimated to be between 0.22 and 0.43 {{solar mass}} per year.{{cite journal |last1=Manna |first1=Souvik |last2=Roy |first2=Subhashis |title=Magnetic Fields, Star Formation Rates, and Gas Densities at Sub-kiloparsec Scales in a Pilot Sample of Nearby Galaxies |journal=The Astrophysical Journal |date=1 February 2023 |volume=944 |issue=1 |pages=86 |doi=10.3847/1538-4357/acaf64|doi-access=free |arxiv=2301.03752 |bibcode=2023ApJ...944...86M }}

Two supernovae have been detected in NGC 4096.{{cite web |title=Bright Supernova pages - Most prolific galaxies |url=https://www.rochesterastronomy.org/snimages/sndupe.html |website=www.rochesterastronomy.org |access-date=12 April 2024}} SN 1960H was a type Ia-pec supernova which had an apparent magnitude of 14.5 at discovery.{{cite web |title=SN 1960H {{!}} Transient Name Server |url=https://www.wis-tns.org/object/1960H |website=www.wis-tns.org |access-date=12 April 2024}} SN 2014bi was a low-luminosity type II-P supernova with magnitude 18.2 upon discovery. The spectrum indicated it was about two weeks post maximum and significantly reddened.{{cite web |title=SN 2014bi {{!}} Transient Name Server |url=https://www.wis-tns.org/object/2014bi |website=www.wis-tns.org |access-date=12 April 2024}}{{cite journal |last1=Zhang |first1=Jujia |last2=Wang |first2=Xiaofeng |title=Spectroscopic Classification of PSN J12060299+4729335 as A Low-Luminosity Type II-P Supernova |journal=The Astronomer's Telegram |date=1 June 2014 |volume=6192 |pages=1 |bibcode=2014ATel.6192....1Z |url=https://www.astronomerstelegram.org/?read=6192}}

Garcia in 1993 considered the galaxy to be a member of LGG 269 group, along with NGC 4111, NGC 3938, NGC 4051, and NGC 4138.{{cite journal |last1=Garcia |first1=A. M. |title=General study of group membership. II. Determination of nearby groups. |journal=Astronomy and Astrophysics Supplement Series |date=1 July 1993 |volume=100 |pages=47–90 |url=https://cdsarc.cds.unistra.fr/ftp/J/A+AS/100/47/table2.dat |bibcode= 1993A&AS..100...47G |issn=0365-0138}} On the other hand, Makarov et al. consider the galaxy to be a member of the Messier 106 Group, along with Messier 106, NGC 4242, NGC 4248, NGC 4288 and NGC 4460.{{cite journal|last1=Makarov|first1=Dmitry|last2=Karachentsev|first2=Igor|title=Galaxy groups and clouds in the local (z~ 0.01) Universe|journal=Monthly Notices of the Royal Astronomical Society|date=21 April 2011|volume=412|issue=4|pages=2498–2520|doi=10.1111/j.1365-2966.2010.18071.x|doi-access=free |bibcode=2011MNRAS.412.2498M|arxiv=1011.6277|s2cid=119194025}} The group is part of the Local Supercluster.G. De Vaucouleurs, 1975. Nearby Groups of Galaxies, ch. 5. the nearer groups within 10 megaparsecs. Published in "Galaxies and the Universe," ed. by A. Sandage, M. Sandage and J. Kristian