View source for NGC 300

{{Short description|Galaxy in the constellation Sculptor}}
{{Infobox galaxy
| name = [[New General Catalogue|NGC]] 300
| image = View of the southern spiral NGC 300.jpg
| caption = NGC 300 imaged by ESO's [[La Silla Observatory]] 
| epoch = [[J2000]]
| type = SA(s)d<ref name="ned">
 {{cite web
  |title=NASA/IPAC Extragalactic Database|url=http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=NGC+300&img_stamp=yes&extend=no
  |work=Results for NGC 300
  |access-date=2006-11-18
 }}</ref>
| ra = {{RA|00|54|53.48}}<ref name="ned" />
| dec = {{DEC|-37|41|03.8}}<ref name="ned" />
| dist_ly = 6.07 ± 0.23 [[light-years|Mly]] (1.86 ± 0.07 [[parsec|Mpc]])<ref name="Rizzietal2006" />{{Ref_label|A|a|none}}
| z = 0.000480 <ref name="ned" />
| h_radial_v = 144 ± 1 km/[[second|s]]<ref name="ned" />
| appmag_v = 9.0<ref name="ned" />
| size_v = {{Val|21.9|×|15.5|u=arcminute}}<ref name="ned" />
| size = 55,200 [[Light-Year|ly]] (16.92 [[kiloparsec|kpc]]) (estimated)<ref name ="ned" />
| mass = (2.9 ± 0.2) × 10<sup>10</sup>
| constellation name = [[Sculptor (constellation)|Sculptor]]
| notes =
| names = {{ odlist | PGC= 3238 | name=ESO 295- G 020 | MCG= -06-03-005 | 2MASX= J00545347-3741037 | IRAS= 00525-3757}}, [[Caldwell catalogue|Caldwell]] 70<ref name="ned" />
}}

'''NGC 300''' (also known as '''Caldwell 70''' or the '''Sculptor Pinwheel Galaxy'''<ref name="interstellarum">{{cite book|last1=Stoyan|first1=Ronald|last2=Schurig|first2=Stephan|title=interstellarum Deep Sky Atlas|publisher=Cambridge University Press; Oculum-Verlag GmbH|publication-place=Erlangen|date=2014|isbn=978-1-107-50338-0|oclc=920437579|url=http://www.deep-sky-atlas.com/}}</ref>) is a [[spiral galaxy]] in the [[constellation]] [[Sculptor (constellation)|Sculptor]]. It was discovered on 5 August 1826 by [[Scotland|Scottish]] astronomer [[James Dunlop]].<ref name="selig">{{cite web | url = https://cseligman.com/text/atlas/ngc3.htm#300 | title = New General Catalogue Objects: NGC{{nbsp}}300| last = Seligman | first = Courtney | website = Celestial Atlas | access-date = 30 August 2024}}</ref> It is one of the closest galaxies to the [[Local Group]], and it most likely lies between the latter and the [[Sculptor Group]].  It is the brightest of the five main spirals in the direction of the Sculptor Group.<ref name="Rizzietal2006" /> It is inclined at an angle of 42° when viewed from [[Earth]] and shares many characteristics of the [[Triangulum Galaxy]].<ref name="Vlajićetal2009"> 
{{cite journal
 |author1=Vlajić, M. |author2=Bland-hawthorn, J. |author3=Freeman, K.C.
 |date=2009
 |title=The Abundance Gradient in the Extremely Faint Outer Disk of NGC 300
 |journal=[[The Astrophysical Journal]]
 |volume=697 |issue=1 |pages=361&ndash;372
 |bibcode=2009ApJ...697..361V
 |doi=10.1088/0004-637X/697/1/361
|arxiv = 0903.1855 |s2cid=15805386 }}</ref> It is about 55,000 light-years in diameter, somewhat smaller than the [[Milky Way]], and has an estimated mass of (2.9 ± 0.2) × 10<sup>10</sup> {{solar mass}}.<ref name="West">{{Cite journal|last1=Westmeier|first1=T.|last2=Braun|first2=R.|last3=Koribalski|first3=B. S.|date=2011-02-01|title=Gas and dark matter in the Sculptor group: NGC 300|journal=Monthly Notices of the Royal Astronomical Society|volume=410|issue=4|pages=2217–2236|doi=10.1111/j.1365-2966.2010.17596.x|doi-access=free |arxiv=1009.0317|bibcode=2011MNRAS.410.2217W|s2cid=119264221}}</ref><ref>{{Cite web|url=http://annesastronomynews.com/photo-gallery-ii/galaxies-clusters/ngc-300/|title = NGC 300, a spiral galaxy in Sculptor|date = 8 July 2014}}</ref>

==Nearby galaxies and group information==
NGC&nbsp;300 and the [[Magellanic spiral galaxy|Magellanic type]] [[barred spiral galaxy]] [[NGC 55|NGC&nbsp;55]] have traditionally been identified as members of the [[Sculptor Group]], a nearby [[group of galaxies]] in the constellation of the same name.  However, recent distance measurements indicate that these two galaxies actually lie in the foreground.<ref name="karachentsevetal2003">
{{cite journal
 |author1=Karachentsev, I.D. |display-authors=4 |author2=Grebel, E.K. |author3=Sharina, M.E.
 |author4=Dolphin, A.E. |author5=Geisler, D. |author6=Guhathakrta, P.
 |author7=Hodge, P.W. |author8=Karachentseva, V.E. |author9=Sarajedini, A.
 |author10=Seitzer, P.
 |date=2003
 |title=Distances to nearby galaxies in Sculptor
 |journal=[[Astronomy and Astrophysics]]
 |volume=404 |pages=93–111
 |bibcode=2003A&A...404...93K
 |doi=10.1051/0004-6361:20030170
|arxiv = astro-ph/0302045 |s2cid=54977869 }}</ref> It is likely that NGC&nbsp;300 and NGC&nbsp;55 form a gravitationally bound pair.<ref name = "vandesteeneetal2006">
{{Cite journal
 |last1=van de Steene |first1=G.C. |last2=Jacoby |first2=G.H. |last3=Praet |first3=C.
 |last4=Ciardullo |first4=R. |last5=Dejonghe |first5=H.
 |title=Distance determination to NGC 55 from the planetary nebula luminosity function
 |journal=Astronomy and Astrophysics
 |date=2006
 |volume=455 |issue=3 |pages=891–896
 |bibcode=2006A&A...455..891V
 |doi=10.1051/0004-6361:20053475
|doi-access=free }}</ref>

The dwarf galaxy [[Sculptor C]] is located about 6.65 million light-years (2.04 [[megaparsec]]s) away from the Sun, and is very likely a [[satellite galaxy]] of NGC 300. Sculptor C has an absolute magnitude of about &minus;9.1 which is typical for other recently discovered ultra-faint dwarf galaxies.<ref name=Sand2024>{{cite journal|bibcode=2024ApJ...977L...5S|arxiv=2409.16345|doi=10.3847/2041-8213/ad927c|doi-access=free |title=Three Quenched, Faint Dwarf Galaxies in the Direction of NGC 300: New Probes of Reionization and Internal Feedback |date=2024 |last1=Sand |first1=David J. |last2=Mutlu-Pakdil |first2=Burçin |last3=Jones |first3=Michael G. |last4=Karunakaran |first4=Ananthan |last5=Andrews |first5=Jennifer E. |last6=Bennet |first6=Paul |last7=Crnojević |first7=Denija |last8=Donatiello |first8=Giuseppe |last9=Drlica-Wagner |first9=Alex |last10=Fielder |first10=Catherine |last11=Martínez-Delgado |first11=David |last12=Martínez-Vázquez |first12=Clara E. |last13=Spekkens |first13=Kristine |last14=Doliva-Dolinsky |first14=Amandine |last15=Hunter |first15=Laura C. |last16=Carlin |first16=Jeffrey L. |last17=Cerny |first17=William |last18=Hai |first18=Tehreem N. |last19=McQuinn |first19=Kristen B.W. |last20=Pace |first20=Andrew B. |last21=Smercina |first21=Adam |journal=The Astrophysical Journal Letters |volume=977 |issue=1 |pages=L5 }}</ref>

==Distance estimates==
In 1986, [[Allan Sandage]] estimated the distance to NGC 300 to be 5.41&nbsp;[[lightyear|Mly]] (1.66&nbsp;[[Megaparsec|Mpc]]).<ref name="Sandage1986">
{{cite journal
 |last=Sandage |first=A.
 |date=1986
 |title=The redshift-distance relation. IX – Perturbation of the very nearby velocity field by the mass of the Local Group
 |journal=[[Astrophysical Journal]]
 |volume=307 |pages=1–19
 |doi=10.1086/164387
 |bibcode=1986ApJ...307....1S
|doi-access=free
 }}</ref> By 1992, this had been updated to 6.9&nbsp;Mly (2.1&nbsp;Mpc) by Freedman et al.<ref name="Rizzietal2006">
{{cite journal
 |author1=Rizzi, L. |display-authors=4 |author2=Bresolin, F. |author3=Kudritzki, R.-P.
 |author4=Gieren, W. |author5=Pietrzyński, G.
 |date=2006
 |title=The Araucaria Project: The Distance to NGC 300 from the Red Giant Branch Tip Using HST ACS Imaging
 |journal=[[The Astrophysical Journal]]
 |volume=638 |issue=2 |pages=766–771
 |doi=10.1086/498705
 |bibcode=2006ApJ...638..766R
|arxiv = astro-ph/0510298 |s2cid=15632452 }}</ref> In 2006, this was revised by Karachentsev et al. to be {{val|7.0|0.3|u=Mly}} ({{val|2.15|0.10|u=Mpc}}).<ref name="Karachentsevetal2006">
{{cite journal
 |author1=Karachentsev, I.D. |author2=Kashibadze, O.G.
 |date=2006
 |title=Masses of the local group and of the M81 group estimated from distortions in the local velocity field
 |journal=[[Astrophysics (journal)|Astrophysics]]
 |volume=49 |issue=1 |pages=3–18
 |doi=10.1007/s10511-006-0002-6
 |bibcode=2006Ap.....49....3K
|s2cid=120973010
 }}</ref> At about the same time, the [[tip of the red giant branch]] (TRGB) method was used to produce an estimate of {{val|5.9|0.4|u=Mly}} ({{val|1.82|0.13|u=Mpc}}) using edge detection and {{val|6.1|0.4|u=Mly}} ({{val|1.87|0.12|u=Mpc}}) using maximum likelihood.<ref name="Rizzietal2006" />  These results were consistent with estimates using near-infrared photometry of [[Cepheid variable]]s by Gieren et al. 2005 that provided an estimate of {{val|6.1|0.2|u=Mly}} ({{val|1.88|0.07|u=Mpc}}).<ref name="Rizzietal2006" /> Combining the recent TRGB and Cepheid estimates the distance to NGC&nbsp;300 is estimated at {{val|6.07|0.23|u=Mly}} ({{val|1.86|0.07|u=Mpc}}).{{Ref_label|A|a|none}}

==NGC 300-OT==
On a [[Charge-coupled device|CCD]] image obtained on 14 May 2008, amateur astronomer L.A.G. Berto Monard discovered a bright [[optical transient]] (OT) in NGC&nbsp;300 that is designated NGC&nbsp;300-OT.<ref>{{cite journal|bibcode=2008IAUC.8946....1M |title=Luminous Transient in NGC 300 |last1=Monard |first1=L. A. G. |journal=International Astronomical Union Circular |date=2008 |issue=8946 |page=1 | url=http://www.cbat.eps.harvard.edu/iauc/08900/08946.html#Item1}}</ref><ref name="PrietoEtAl2009" /> It is located at [[Right ascension|RA]]:&nbsp;{{RA|00|54|34.552}} and [[Declination|DEC]]:&nbsp;{{DEC|-37|38|31.79}}<ref name="Gogartenetal2009">
{{cite journal
 |author1=Gogarten, S.M. |display-authors=4 |author2=Dalcanton, J.J. |author3=Murphy, J.W.
 |author4=Williams, B.F. |author5=Gilbert, K. |author6=Dolphin, A.
 |date=2009
 |title=The NGC 300 Transient: An Alternative Method for Measuring Progenitor Masses
 |journal=[[The Astrophysical Journal]]
 |volume=703 |issue=1 |pages=300&ndash;310
 |doi=10.1088/0004-637X/703/1/300
 |bibcode=2009ApJ...703..300G
|arxiv = 0907.0710 |s2cid=8131611 }}</ref> in a [[spiral arm]] containing active star formation.<ref name="Bondetal2009" /> Its broad-band magnitude was 14.3 in that image.  An earlier image (from 24 April 2008), taken just after NGC&nbsp;300 reemerged from behind the [[Sun]], evidenced an already brightening OT at ~16.3 magnitude.<ref name="Bondetal2009">
{{cite journal
 |author1=Bond, H.E. |display-authors=4 |author2=Bedin, L.R. |author3=Bonanos, A.Z.
 |author4=Humphreys, R.M. |author5=Monard, L.A.G.B. |author6=Prieto, J.L.
 |author7=Water, F.M.
 |title=The 2008 Luminous Optical Transient in the Nearby Galaxy NGC 300
 |date=2009
 |journal=[[The Astrophysical Journal Letters]]
 |volume=695 |issue=2 |pages=L154–L158
 |doi=10.1088/0004-637X/695/2/L154
 |bibcode=2009ApJ...695L.154B
|arxiv = 0901.0198 |s2cid=15953172 }}</ref> No brightening was detected on a 8 February 2008 image, nor on any earlier ones.<ref name="Bondetal2009" /> The transient's peak measured magnitude was 14.69 on 15 May 2008.<ref name="Bondetal2009" />

At discovery, the transient had an absolute magnitude of {{nowrap|MV ≈ &minus;13}}, making it faint in comparison to a typical [[core-collapse supernova]] but bright in comparison to a [[classical nova]].<ref name="PrietoEtAl2009" /><ref name="Bondetal2009" /> Additionally, the photometric and spectroscopic properties of the OT imply that it is not a [[luminous blue variable]] either.<ref name="Bondetal2009" /> Since its peak, brightness dropped smoothly through September 2008 while becoming continuously redder.<ref name="Bondetal2009" /> After September 2008, brightness continued to fall at a lower rate in the optical spectrum but with strong [[hydrogen alpha|Hα]] emissions.<ref name="Bondetal2009" /> Further, the optical spectrum is mostly made up of fairly narrow [[Hydrogen Balmer]] and Ca&nbsp;II emission lines coupled with strong Ca&nbsp;II H&K absorption.<ref name="PrietoEtAl2009" />  Research into historical [[Hubble Space Telescope|Hubble]] images provide an accurate upper bound on the progenitor star's brightness.<ref name="PrietoEtAl2009" /> This suggested a low-mass [[main sequence]] star as progenitor with the transient resulting from a stellar merger similar to red Galactic nova [[V838 Monocerotis]].<ref name="PrietoEtAl2009">
{{cite journal
 |date=2009
 |title=A Spitzer/IRS Spectrum of the 2008 Luminous Transient in NGC 300: Connection to Proto-Planetary Nebulae
 |last1=Prieto   | first1=J.L.
 |last2=Sellgren |first2=K.
 |last3=Thompson | first3=T.A.
 |last4=Kochanek | first4=C.S.
 |doi=10.1088/0004-637X/705/2/1425
 |journal=The Astrophysical Journal
 |volume=705
 |issue=2
 |pages=1425–1432
 |arxiv=0907.0230
|bibcode = 2009ApJ...705.1425P |s2cid=15627891
 }}</ref> Analysis of historical images of the area of the OT suggest with 70% certainty that the progenitor formed in a burst of stars around 8&ndash;13&nbsp;Myr ago and implies the progenitor's mass to be 12&ndash;25&nbsp;[[solar mass|M<sub>⊙</sub>]] assuming the OT is due to an evolving massive star.<ref name="Gogartenetal2009" />

[[File:NGC 300 Hubble.jpg|thumb|NGC 300 zoom-in by the [[Hubble Space Telescope]]]]
[[file:Composite Image of NGC 300.jpg|thumb|NGC 300 by [[GALEX]], in ultraviolet light]]
However, in 2008 a bright [[mid-infrared]] progenitor to the transient was discovered in historical [[Spitzer Space Telescope|Spitzer]] data. This was a star that was obscured by dust, with energy distribution analogous to a [[black-body]] of {{nowrap|''R'' ≈ 300}} [[astronomical units|AU]] and radiating at {{nowrap|''T'' ≈ 300}} [[kelvin|K]] with {{nowrap|''L''<sub>bol</sub> ≈ {{e|6|4}} [[solar luminosity|''L''<sub>⊙</sub>]]}}. This demonstrated that the transient was associated with an energetic explosion of a low-mass ≈&nbsp;10&nbsp;M<sub>⊙</sub> star. The transient's low luminosity as compared to typical core-collapse supernova, combined with its spectral attributes and dust covered properties, make it nearly identical to [[NGC 6946|NGG&nbsp;6946]]'s [[SN 2008S|SN&nbsp;2008S]].<ref name="PrietoEtAl2009" />

The spectrum of NGC&nbsp;300-OT observed with Spitzer shows strong, broad emission features at 8&nbsp;μm and 12&nbsp;μm.  Such features are also seen in Galactic [[carbon star|carbon-rich]] [[protoplanetary nebulae]].<ref name="PrietoEtAl2009" />

On 19 April 2025, NGC&nbsp;300-OT was classified as an Intermediate-Luminosity Red Transient (ILRT).<ref>{{cite web | website=Transient Name Server | title=Classification certificate for object 2008jd | url=https://www.wis-tns.org/object/2008jd/classification-cert | publisher = [[International Astronomical Union|IAU]] | access-date=19 April 2025}}</ref>

==SN 2010da==
SN 2010da (type LBV, mag. 16) was discovered by Monard on 23 May 2010.<ref>{{cite journal|bibcode=2010CBET.2289....1M |title=Supernova 2010da in NGC 300 |last1=Monard |first1=L. A. G. |journal=Central Bureau Electronic Telegrams |date=2010 |issue=2289 |page=1 | url=http://www.cbat.eps.harvard.edu/iau/cbet/002200/CBET002289.txt}}</ref><ref name=atel2640>{{cite journal|bibcode=2010ATel.2640....1B |title=Optical Photometry of the New Optical Transient SN 2010da in NGC 300 |last1=Bond |first1=Howard E. |journal=The Astronomer's Telegram |date=2010-05-26 |volume=2640 |page=1 | url=http://www.astronomerstelegram.org/?read=2640}}</ref> The optical transient was detected 15".9 west and 16".8 north the center of the galaxy at coordinates 00 55 04.86 −37 41 43.7.<ref>{{cite web | website=Transient Name Server | title=SN{{nbsp}}2010da | url=https://www.wis-tns.org/object/2010da | publisher = [[International Astronomical Union|IAU]] | access-date=7 June 2025}}</ref>

Two sets of independent follow-up spectroscopy data suggested that this was again another optical transient rather than a supernova, possibly an outbursting [[luminous blue variable]] star according to one spectrum,<ref name=atel2636>{{cite journal|bibcode=2010ATel.2636....1E |title=SN 2010da is a SN "impostor" |last1=Elias-Rosa |first1=N. |last2=Mauerhan |first2=J. C. |last3=Van Dyk |first3=S. D. |journal=The Astronomer's Telegram |date=2010-05-25 |volume=2636 |page=1 | url=http://www.astronomerstelegram.org/?read=2636}}</ref><ref name=atel2637>{{cite journal|bibcode=2010ATel.2637....1C |title=Spectroscopy of SN 2010da in NGC 300 |last1=Chornock |first1=Ryan |last2=Berger |first2=Edo |journal=The Astronomer's Telegram |date=2010-05-25 |volume=2637 |page=1 |url=http://www.astronomerstelegram.org/?read=2637}}</ref> as earlier predicted from the nature of the candidate mid-infrared progenitor.<ref name=atel2632>{{cite journal|bibcode=2010ATel.2632....1K |title=Mid-IR progenitor of SN 2010da in NGC 300 |last1=Khan |first1=R. |last2=Stanek |first2=K. Z. |last3=Kochanek |first3=C. S. |last4=Thompson |first4=T. A. |last5=Prieto |first5=J. L. |journal=The Astronomer's Telegram |date=2010-05-24 |volume=2632 |page=1 |url=http://www.astronomerstelegram.org/?read=2632}}</ref>  The transient faded by 0.5–0.7 mag in 9 days, much faster than the 2008 transient in NGC 300.<ref name=atel2660>{{cite journal|bibcode=2010ATel.2660....1P |title=Optical and Near-IR Follow-up of SN 2010da: Evidence for Warm Dust |last1=Prieto |first1=J. L. |last2=Bond |first2=H. E. |last3=Kochanek |first3=C. S. |last4=Khan |first4=R. |last5=Stanek |first5=K. Z. |last6=Thompson |first6=T. A. |journal=The Astronomer's Telegram |date=2010-06-04|volume=2660 |page=1 |url=http://www.astronomerstelegram.org/?read=2660}}</ref>

== Other Novae, Supernovae, and Transients ==

AT 2019qyl was discovered by the ''Distance Less Than 40 Mpc Survey'' (DLT40) on 26 September 2019, at magnitude 17.1.  It was initially classified as a type IIn/LBV,<ref>{{cite web | website=Transient Name Server | title=Classification certificate for object 2019qyl | url=https://www.wis-tns.org/object/2019qyl/classification-cert |publisher = [[International_Astronomical_Union|IAU]] | access-date=17 August 2024}}</ref> but later analysis classified the star as a classical [[nova]].<ref>{{cite web | website=Transient Name Server | title=AT 2019qyl | url=https://www.wis-tns.org/object/2019qyl |publisher = [[International_Astronomical_Union|IAU]] | access-date=16 August 2024}}</ref>

SN 2020acli ([[Type II supernova|type&nbsp;IIn-pec]], mag. 18.4205) was discovered by the ''Distance Less Than 40 Mpc Survey'' (DLT40) on 12 December 2020.<ref>{{cite web | website=Transient Name Server | title=SN{{nbsp}}2020acli | url=https://www.wis-tns.org/object/2020acli | publisher = [[International Astronomical Union|IAU]] | access-date=15 January 2025}}</ref>

AT 2024oth (type unknown, mag. 19.85) was discovered by [[BlackGEM]] on 27 June 2024.<ref>{{Cite web |title=2024oth {{!}} Transient Name Server |url=https://www.wis-tns.org/object/2024oth |access-date=2025-01-02 |website=www.wis-tns.org}}</ref>

AT 2024txt (type unknown, mag. 19.77) was discovered by [[Pan-STARRS]] on 29 July 2024.<ref>{{Cite web |title=2024txt {{!}} Transient Name Server |url=https://www.wis-tns.org/object/2024txt |access-date=2025-01-02 |website=www.wis-tns.org}}</ref>

==Binary black hole system==
An [[x-ray astronomy|x-ray]] source in NGC&nbsp;300 is designated NGC&nbsp;300&nbsp;X-1.<ref name = "Barnardetal2008" />  Astronomers speculate that NGC&nbsp;300&nbsp;X-1 is a new kind of [[Wolf–Rayet star|Wolf-Rayet]] + [[stellar black hole]] [[binary system (astronomy)|binary system]] similar to the confirmed such system [[IC 10|IC&nbsp;10]]&nbsp;X-1.<ref name = "Barnardetal2008">
{{cite journal
 |author1=Barnard, R. |author2=Clark, J.S. |author3=Kolb, U.C.
 |date=2008
 |title=NGC 300 X-1 and IC 10 X-1: a new breed of black hole binary?
 |journal=[[Astronomy and Astrophysics]]
 |volume=488 |issue=2 |pages=697–703
 |doi=10.1051/0004-6361:20077975
 |bibcode=2008A&A...488..697B
|arxiv = 0807.0606 |s2cid=1234999 }}</ref> Their shared properties include an [[orbital period]] of 32.8 hours. The black hole has a mass of 17 ± 4 {{Solar mass|link=true}} and the WR star has a mass of {{Val|26|7|5}} {{Solar mass}}. Both objects orbit each other at a distance of about 18.2 {{Solar radius|link=true}}.<ref>{{Cite journal |last1=Binder |first1=Breanna A. |last2=Sy |first2=Janelle M. |last3=Eracleous |first3=Michael |last4=Christodoulou |first4=Dimitris M. |last5=Bhattacharya |first5=Sayantan |last6=Cappallo |first6=Rigel |last7=Laycock |first7=Silas |last8=Plucinsky |first8=Paul P. |last9=Williams |first9=Benjamin F. |date=2021-03-01 |title=The Wolf–Rayet + Black Hole Binary NGC 300 X-1: What is the Mass of the Black Hole? |journal=The Astrophysical Journal |volume=910 |issue=1 |pages=74 |doi=10.3847/1538-4357/abe6a9 |doi-access=free |arxiv=2102.07065 |bibcode=2021ApJ...910...74B |issn=0004-637X}}</ref>

== WO star ==
There is an oxygen-sequence Wolf–Rayet star (WO4 type), known as STWR 13, located in one of the bright H II regions in NGC 300.<ref>{{Cite journal |last1=Breysacher |first1=J. |last2=Azzopardi |first2=M. |last3=Testor |first3=G. |last4=Muratorio |first4=G. |date=1997-10-01 |title=Wolf–Rayet stars detected in five associations of NGC 300. |url=https://ui.adsabs.harvard.edu/abs/1997A&A...326..976B |journal=Astronomy and Astrophysics |volume=326 |pages=976–981 |bibcode=1997A&A...326..976B |issn=0004-6361}}</ref>

==Notes==
{{refbegin}}
<ol type="a"><li>{{Note_label|A|a|none}}Average ({{val|1.845|0.125}}, {{val|1.86|0.07}}) = ((1.845 + 1.86) / 2) ± ((0.125<sup>2</sup> + 0.07<sup>2</sup>)<sup>0.5</sup> / 2) = 1.86 ± 0.07</li></ol>
{{refend}}

== See also ==
* [[List of NGC objects (1–1000)]]

==References==
{{reflist|30em}}

==External links==
{{commons category}}
*{{WikiSky}}
*Confirmation image of [https://web.archive.org/web/20110927114126/http://www.supernovae.net/sn2010/n300s2.jpg SN 2010da] (2010-05-24) / [http://www.wikisky.org/?ra=0.9161420290060076&de=-37.694394782755666&zoom=11&show_grid=1&show_constellation_lines=1&show_constellation_boundaries=1&show_const_names=0&show_galaxies=1&show_box=1&box_ra=0.9180167&box_de=-37.695473&box_width=50&box_height=50&img_source=DSS2 Wikisky DSS2 zoom-in of same region]

{{Sky|00|54|53.5|-|37|41|04|7000000}}
{{Catalogs|NGC=300|C=70|PGC=3238}}
{{Caldwell catalogue}}
{{Ngc5}}
{{Sculptor (constellation)}}
{{Portalbar|Astronomy}}

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{{DEFAULTSORT:NGC 0300}}
[[Category:Unbarred spiral galaxies]]
[[Category:Sculptor (constellation)]]
[[Category:NGC objects|0300]]
[[Category:Principal Galaxies Catalogue objects|003238]]
[[Category:Caldwell objects|070b]]
[[Category:IRAS catalogue objects|00525-3757]]
[[Category:MCG objects|-06-03-005]]
[[Category:Astronomical objects discovered in 1826|18260805]]
[[Category:Articles containing video clips]]
[[Category:Virgo Supercluster]]
[[Category:Discoveries by James Dunlop]]