NGC 3137

{{Short description|Galaxy in the constellation Antlia}}

{{Infobox galaxy

| name = NGC 3137

| image = NGC 3137 PanS.jpg

| caption = NGC 3137 imaged by PanSTARRS

| epoch = J2000

| type = SA(s)d {{cite web

| website=NASA/IPAC Extragalactic Database

| publisher = NASA and Caltech

| title=Results for object NGC 3137

| url=https://ned.ipac.caltech.edu/byname?objname=NGC+3137

| access-date=2 March 2025 }}

| ra = {{RA|10|09|07.3775}}

| dec = {{DEC|-29|03|50.486}}

| dist_ly = 52.6 ± 9.1 Mly (16.1 ± 2.8 Mpc)

| z = 0.003683 ± 0.000002

| h_radial_v = 1,104 ± 1 km/s

| appmag_v = 11.5{{cite web |title=Revised NGC Data for NGC 3137 |url=https://spider.seds.org/ngc/revngcic.cgi?NGC3137 |website=spider.seds.org |access-date=30 March 2024}}

| size_v = 6.3{{prime}} × 2.2{{prime}}

| size = ~{{convert|42.2|kpc|ly|abbr=on|lk=on|order=flip}} (estimated){{r|ned}}

| constellation name = Antlia

| group_cluster = NGC 3175 Group

| notes =

| names = {{odlist | UGCA= 203 | name= ESO 435- G 047 | MCG= -05-24-024 | name2= AM 1006-284 | PGC= 29530}}

}}

NGC 3137 is a spiral galaxy in the constellation Antlia. The galaxy lies about 50 million light years away from Earth, which means, given its apparent dimensions, that NGC 3137 is approximately 140,000 light years across. It was discovered by John Herschel on February 5, 1837.{{cite web |last1=Seligman |first1=Courtney |title=NGC 3137 (= PGC 29530) |url=https://cseligman.com/text/atlas/ngc31.htm#3137 |website=Celestial Atlas |access-date=19 November 2018}}

NGC 3137 has a pretty bright nucleus. The spiral pattern is similar with NGC 3621 and the Pinwheel Galaxy and features many knots. The morphological classification of this galaxy is SA(s)d, which indicates the galaxy doesn't have a bar (SA), lacks an inner ring structure (s), and has loosely wound spiral arms (d). A star is superposed 0.3 arcminutes from the centre.Corwin, H. G.; de Vaucouleurs, A.; de Vaucouleurs, G (1985) Southern Galaxy Catalogue. University of Texas The galaxy is seen at an inclination of about 70°.

The star formation rate of the galaxy is estimated to be 0.5 {{solar mass}} per year based on the CO(2-1) radio emission detected by the Atacama Large Millimeter Array. The total hydrogen mass of the galaxy is estimated to be {{val|e=9.68|ul=M_solar}}. The stellar mass of the galaxy is comparable, at {{val|e=9.88|u=M_solar}}.{{cite journal |last1=Leroy |first1=Adam K. |last2=Schinnerer |first2=Eva |last3=Hughes |first3=Annie |last4=Rosolowsky |first4=Erik |last5=Pety |first5=Jérôme |last6=Schruba |first6=Andreas |last7=Usero |first7=Antonio |last8=Blanc |first8=Guillermo A. |last9=Chevance |first9=Mélanie |last10=Emsellem |first10=Eric |last11=Faesi |first11=Christopher M. |last12=Herrera |first12=Cinthya N. |last13=Liu |first13=Daizhong |last14=Meidt |first14=Sharon E. |last15=Querejeta |first15=Miguel |last16=Saito |first16=Toshiki |last17=Sandstrom |first17=Karin M. |last18=Sun 孙 |first18=Jiayi 嘉 懿 |last19=Williams |first19=Thomas G. |last20=Anand |first20=Gagandeep S. |last21=Barnes |first21=Ashley T. |last22=Behrens |first22=Erica A. |last23=Belfiore |first23=Francesco |last24=Benincasa |first24=Samantha M. |last25=Bešlić |first25=Ivana |last26=Bigiel |first26=Frank |last27=Bolatto |first27=Alberto D. |last28=den Brok |first28=Jakob S. |last29=Cao |first29=Yixian |last30=Chandar |first30=Rupali |last31=Chastenet |first31=Jérémy |last32=Chiang 江 |first32=I-Da 宜 達 |last33=Congiu |first33=Enrico |last34=Dale |first34=Daniel A. |last35=Deger |first35=Sinan |last36=Eibensteiner |first36=Cosima |last37=Egorov |first37=Oleg V. |last38=García-Rodríguez |first38=Axel |last39=Glover |first39=Simon C. O. |last40=Grasha |first40=Kathryn |last41=Henshaw |first41=Jonathan D. |last42=Ho |first42=I-Ting |last43=Kepley |first43=Amanda A. |last44=Kim |first44=Jaeyeon |last45=Klessen |first45=Ralf S. |last46=Kreckel |first46=Kathryn |last47=Koch |first47=Eric W. |last48=Kruijssen |first48=J. M. Diederik |last49=Larson |first49=Kirsten L. |last50=Lee |first50=Janice C. |last51=Lopez |first51=Laura A. |last52=Machado |first52=Josh |last53=Mayker |first53=Ness |last54=McElroy |first54=Rebecca |last55=Murphy |first55=Eric J. |last56=Ostriker |first56=Eve C. |last57=Pan |first57=Hsi-An |last58=Pessa |first58=Ismael |last59=Puschnig |first59=Johannes |last60=Razza |first60=Alessandro |last61=Sánchez-Blázquez |first61=Patricia |last62=Santoro |first62=Francesco |last63=Sardone |first63=Amy |last64=Scheuermann |first64=Fabian |last65=Sliwa |first65=Kazimierz |last66=Sormani |first66=Mattia C. |last67=Stuber |first67=Sophia K. |last68=Thilker |first68=David A. |last69=Turner |first69=Jordan A. |last70=Utomo |first70=Dyas |last71=Watkins |first71=Elizabeth J. |last72=Whitmore |first72=Bradley |display-authors= 1 |title=PHANGS–ALMA: Arcsecond CO(2–1) Imaging of Nearby Star-forming Galaxies |journal=The Astrophysical Journal Supplement Series |date=1 December 2021 |volume=257 |issue=2 |pages=43 |doi=10.3847/1538-4365/ac17f3|doi-access=free |arxiv=2104.07739 |bibcode=2021ApJS..257...43L }} In the centre of the galaxy lies a supermassive black hole, whose mass is estimated to be 10^{7.78 ± 0.20} (38 - 95 millions) {{solar mass}}, based on the pitch angle of the spiral arms.{{cite journal |last1=Davis |first1=Benjamin L. |last2=Berrier |first2=Joel C. |last3=Johns |first3=Lucas |last4=Shields |first4=Douglas W. |last5=Hartley |first5=Matthew T. |last6=Kennefick |first6=Daniel |last7=Kennefick |first7=Julia |last8=Seigar |first8=Marc S. |last9=Lacy |first9=Claud H. S. |title=The Black Hole Mass Function Derived from Local Spiral Galaxies |journal=The Astrophysical Journal |date=20 June 2014 |volume=789 |issue=2 |pages=124 |doi=10.1088/0004-637X/789/2/124|bibcode=2014ApJ...789..124D |arxiv=1405.5876 |s2cid=119302157 }}

NGC 3137 is a member of the NGC 3175 Group.{{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 |url=http://www.sao.ru/hq/dim/groups/galaxies.dat|bibcode=2011MNRAS.412.2498M|arxiv=1011.6277|s2cid=119194025|access-date=1 February 2025}} It is one of the two large spirals of the group, the other being NGC 3175.{{cite journal |last1=Kondapally |first1=Rohit |last2=Russell |first2=George A |last3=Conselice |first3=Christopher J |last4=Penny |first4=Samantha J |title=Faint satellite population of the NGC-3175 Group – a Local Group analogue |journal=Monthly Notices of the Royal Astronomical Society |date=1 December 2018 |volume=481 |issue=2 |pages=1759–1773 |doi=10.1093/mnras/sty2333|doi-access=free |arxiv=1808.09020 }} Other members of the group include NGC 3113, and NGC 3125.{{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|bibcode-access=free}}