NGC 3513

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

{{Infobox galaxy

| name = NGC 3513

| image = NGC3513-hst-R814G606B450.jpg

| caption = NGC 3513 imaged by Hubble Space Telescope

| epoch = J2000

| type = SB(s)c {{cite web

| website=NASA/IPAC Extragalactic Database

| publisher = NASA and Caltech

| title=Results for object NGC 3513

| url=https://ned.ipac.caltech.edu/byname?objname=NGC+3513

| access-date=15 February 2025 }}

| ra = {{RA|11|03|46.1628}}

| dec = {{DEC|-23|14|44.196}}

| dist_ly = 40.2 ± 13.0 Mly (12.3 ± 4.0 Mpc)

| z = 0.003979 ± 0.000020

| h_radial_v = 1,163 ± 6 km/s

| appmag_v = 11.1{{cite web |title=Revised NGC Data for NGC 3513 |url=https://spider.seds.org/ngc/revngcic.cgi?NGC3513 |website=spider.seds.org |access-date=30 March 2024}}

| size_v = 2.8{{prime}} × 2.2{{prime}}

| size = ~{{convert|14.3|kpc|ly|abbr=on|lk=on|order=flip}} (estimated){{r|ned}}

| constellation name = Crater

| group_cluster = NGC 3511 Group

| notes =

| names = {{odlist | UGCA= 224 | name= ESO 502- G 014 | name2= AM 1101-225 | MCG= -04-26-021 | IRAS= 11013-2258 | PGC= 33410 }}{{r|ned}}

}}

NGC 3513 is a barred spiral galaxy in the constellation Crater. The galaxy lies about 40 million light years away from Earth, which means, given its apparent dimensions, that NGC 3513 is approximately 45,000 light years across. It was discovered by William Herschel on December 21, 1786.{{cite web |last1=Seligman |first1=Courtney |title=NGC 3513 (= PGC 33410) |url=https://cseligman.com/text/atlas/ngc35.htm#3513 |website=Celestial Atlas |access-date=19 November 2018}}

NGC 3513 is a barred galaxy with a thin high-surface-brightness bar. At the end of the bar there are slightly offset ansae from which emerge two well defined spiral arms. The arms are patchy, featuring many star formation knots and HII regions. The southern arm is more open, while the northern features more vigorous star formation. The arms can be followed by a bit over half a revolution.{{cite journal |last1=Eskridge |first1=Paul B. |last2=Frogel |first2=Jay A. |last3=Pogge |first3=Richard W. |last4=Quillen |first4=Alice C. |last5=Berlind |first5=Andreas A. |last6=Davies |first6=Roger L. |last7=DePoy |first7=D. L. |last8=Gilbert |first8=Karoline M. |last9=Houdashelt |first9=Mark L. |last10=Kuchinski |first10=Leslie E. |last11=Ramirez |first11=Solange V. |last12=Sellgren |first12=K. |last13=Stutz |first13=Amelia |last14=Terndrup |first14=Donald M. |last15=Tiede |first15=Glenn P. |title=Near-Infrared and Optical Morphology of Spiral Galaxies |journal=The Astrophysical Journal Supplement Series |date=November 2002 |volume=143 |issue=1 |pages=73–111 |doi=10.1086/342340|arxiv=astro-ph/0206320 |bibcode=2002ApJS..143...73E }} The total star formation rate of the galaxy is estimated to be 0.2 {{solar mass}} per year. The brightest stars of the galaxy can be resolved and have an apparent magnitude of 21.5. Ionised outflows have been observed near the nucleus. The galaxy is seen at an inclination of 39°.{{cite journal |last1=Zhu |first1=Hanjue |last2=Boettcher |first2=Erin |last3=Chen |first3=Hsiao-Wen |title=Spatially resolved properties of extraplanar diffuse ionized gas in NGC 3511 and NGC 3513 |journal=Monthly Notices of the Royal Astronomical Society |date=19 July 2024 |volume=532 |issue=3 |pages=3252–3267 |doi=10.1093/mnras/stae1708|doi-access=free }}

NGC 3513 forms a pair with NGC 3511, which lies 10.5 arcminutes away.Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington There is a faint narrow hydrogen bridge apparently connecting the two galaxies.{{cite journal |last1=Eibensteiner |first1=Cosima |last2=Sun |first2=Jiayi |last3=Bigiel |first3=Frank |last4=Leroy |first4=Adam K. |last5=Schinnerer |first5=Eva |last6=Rosolowsky |first6=Erik |last7=Kurapati |first7=Sushma |last8=Pisano |first8=D. J. |last9=de Blok |first9=W. J. G |last10=Barnes |first10=Ashley T. |last11=Thorp |first11=Mallory |last12=Colombo |first12=Dario |last13=Koch |first13=Eric W. |last14=Chiang |first14=I-Da |last15=Ostriker |first15=Eve C. |last16=Murphy |first16=Eric J. |last17=Zabel |first17=Nikki |last18=Laudage |first18=Sebstian |last19=Maccagni |first19=Filippo M. |last20=Healy |first20=Julia |last21=Sekhar |first21=Srikrishna |last22=Utomo |first22=Dyas |last23=den Brok |first23=Jakob |last24=Cao |first24=Yixian |last25=Chevance |first25=Mélanie |last26=Dale |first26=Daniel A. |last27=Faesi |first27=Christopher M. |last28=Glover |first28=Simon C. O. |last29=He |first29=Hao |last30=Jeffreson |first30=Sarah |last31=Jiménez-Donaire |first31=María J. |last32=Klessen |first32=Ralf |last33=Neumann |first33=Justus |last34=Pan |first34=Hsi-An |last35=Pathak |first35=Debosmita |last36=Querejeta |first36=Miguel |last37=Teng |first37=Yu-Hsuan |last38=Usero |first38=Antonio |last39=Williams |first39=Thomas G. |display-authors = 1|title=PHANGS-MeerKAT and MHONGOOSE HI observations of nearby spiral galaxies: Physical drivers of the molecular gas fraction, R mol |journal=Astronomy & Astrophysics |date=November 2024 |volume=691 |pages=A163 |doi=10.1051/0004-6361/202449944|arxiv=2407.01716 }} The two galaxies form a small group, known as the NGC 3511 group, which also includes the galaxy ESO 502-024.{{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}}