View source for Sculptor Galaxy

{{Short description|Intermediate spiral galaxy in the constellation Sculptor}}
{{Distinguish|text = the [[Sculptor Dwarf Galaxy]] or the [[Sculptor Dwarf Irregular Galaxy]]}}
{{Infobox Galaxy
| name = Sculptor Galaxy
| image = NGC 253 - Sculptor.png
| caption = The Sculptor Galaxy is particularly known for its exceptionally high rate of [[star formation]]
| epoch = [[Epoch (astronomy)#Julian years and J2000|J2000]]
| ra = {{RA|00|47|33.13}}<ref name="ned">{{cite web | title=NASA/IPAC Extragalactic Database | work=Results for NGC 253 | url=https://ned.ipac.caltech.edu/byname?objname=ngc+253 | access-date=2006-11-25}}</ref>
| dec = {{DEC|-25|17|17.1}}<ref name="ned" />
| constellation name = [[Sculptor (constellation)|Sculptor]]
| z = 0.000807<ref name="ned" />
| h_radial_v = {{nowrap|242 ± 1 [[Metre per second|km/s]]}} <ref name="ned" />
| dist_ly = 11.4 ± 0.7 [[light year|Mly]]<br />&nbsp;&nbsp;&nbsp;(3.5 ± 0.2 [[parsec|Mpc]])<ref name="Rekolaetal2005" />
| type = SAB(s)c<ref name="ned" />
| appmag_v = 8.0<ref name="ned" />
| size_v = 27′.5 × 6′.8<ref name="ned" />
| size = {{convert|36.96|kpc|ly|-2|abbr=off|lk=on}}<br />(diameter; [[Galaxy#Isophotal diameter|D<sub>27</sub> isophote]])
| notes =
| names = Silver Coin Galaxy,<ref name="ned" /> Silver Dollar Galaxy,<ref name="apod-2006-04-21">{{Cite APOD
  | title = NGC 253: Dusty Island Universe
  | date = 2006-04-21
  | access-date = 2010-12-04
}}</ref> [[New General Catalogue|NGC]] 253,<ref name="ned" /> UGCA 13,<ref name="ned" /> [[Principal Galaxies Catalogue|PGC]] 2789<ref name="ned" /> [[Caldwell catalogue|Caldwell]]&nbsp;65
}}

The '''Sculptor Galaxy''' (also known as the '''Silver Coin Galaxy''', '''Silver Dollar Galaxy''', '''NGC 253''', or '''Caldwell 65''') is an [[intermediate spiral galaxy]] in the [[constellation]] [[Sculptor (constellation)|Sculptor]]. The Sculptor Galaxy is a [[starburst galaxy]], which means that it is currently undergoing a period of intense star formation.

==Observation==

===Observational history===
The galaxy was discovered by [[Caroline Herschel]] in 1783 during one of her systematic [[comet]] searches.<ref name="Dreyer1888">{{cite journal|last=Dreyer|first=J. L. E.|author-link=John Louis Emil Dreyer|date=1888|title=A New General Catalogue of Nebulae and Clusters of Stars, being the Catalogue of the late Sir John F.W. Herschel, Bart., revised, corrected, and enlarged|journal=[[Memoirs of the Royal Astronomical Society]]|volume=49|pages=1–237|bibcode=1888MmRAS..49....1D}}</ref><ref name="Burnhams">{{cite book|title=Burnham's Celestial Handbook: An Observer's Guide to the Universe Beyond the Solar System|last=Burnham|first=Robert|date=1978|publisher=Dover Publications, Inc.|isbn=978-0-486-24065-7|volume=Three, Pavo Through Vulpecula|page=[https://archive.org/details/burnhamscelestia03burn/page/1736 1736]|author-link=Robert Burnham Jr.|url=https://archive.org/details/burnhamscelestia03burn/page/1736}}</ref> Many years later, [[John Herschel]] observed it using his 18-inch metallic mirror [[reflecting telescope|reflector]] at the [[Cape of Good Hope]].<ref name="Burnhams" /> He wrote: "very bright and large (24′ in length); a superb object.... Its light is somewhat streaky, but I see no stars in it except 4 large and one very small one, and these seem not to belong to it, there being many near..."<ref name="Burnhams" />

In 1961, [[Allan Sandage]] wrote in the ''Hubble Atlas of Galaxies'' that the Sculptor Galaxy is "the prototype example of a special subgroup of Sc systems....photographic images of galaxies of the group are dominated by the dust pattern. [[Dust lane]]s and patches of great complexity are scattered throughout the surface. Spiral arms are often difficult to trace.... The arms are defined as much by the dust as by the spiral pattern."<ref name="Sandage1961">{{cite book|title=The Hubble Atlas of Galaxies|last=Sandage|first=Allan|date=1961|publisher=Washington: Carnegie Institution|isbn=978-0-87279-629-4|bibcode=1961hag..book.....S|author-link=Allan Sandage}}</ref> [[Bernard Y. Mills]], working out of [[Sydney]], discovered that the Sculptor Galaxy is also a fairly strong [[Radio sources|radio source]].<ref name="Burnhams" />

In 1998, the [[Hubble Space Telescope]] took a detailed image of NGC 253.<ref name="hubb">{{cite web | title=HubbleSite NewsCenter | work=Results for NGC 253 | url=http://hubblesite.org/newscenter/archive/releases/1998/42/image/a | access-date=2007-04-05}}</ref>

===Amateur===
As one of the brightest galaxies in the sky, the Sculptor Galaxy can be seen through [[binoculars]] and is near the star [[Beta Ceti]]. It is considered one of the most easily viewed spiral galaxies in the sky after the [[Andromeda Galaxy]].<ref name="Burnhams"/><ref name="NSOG">{{cite book|title=The Night Sky Observer's Guide|last1=Kepple|first1=George Robert|last2=Sanner|first2=Glen W.|publisher=Willmann-Bell, Inc.|year=1998|isbn=978-0-943396-60-6|volume=2|pages=365, 371}}</ref>

The Sculptor Galaxy is a good target for observation with a telescope with a 300&nbsp;mm diameter or larger.<ref name="NSOG" /> In such telescopes, it appears as a galaxy with a long, oval bulge and a mottled [[galactic disc]].<ref name="NSOG" /> Although the bulge appears only slightly brighter than the rest of the galaxy, it is fairly extended compared to the disk.<ref name="NSOG" /> In 400&nbsp;mm scopes and larger, a dark dust lane northwest of the [[Active galactic nucleus|nucleus]] is visible, and over a dozen faint stars can be seen superimposed on the bulge.<ref name="NSOG" /> Some people claim to have observed the galaxy with the unaided eye under exceptional viewing conditions.

==Features==
[[File:MUSE view of the Sculptor Galaxy (eso2510a).jpg|left|thumb|The Sculptor Galaxy as seen by the [[Multi-unit spectroscopic explorer|MUSE]] instrument at the [[Very Large Telescope]].]]
[[Image:Three-dimensional view of ALMA observations of the outflows from NGC 253.jpg|thumb|Three-dimensional simulation of [[Atacama Large Millimeter Array|ALMA]] observations of the outflows.<ref>{{cite news|url=https://www.eso.org/public/news/eso1334/|title=Starburst to Star Bust|date=24 July 2013|access-date=15 August 2013|publisher=[[European Southern Observatory]]}}</ref>]]
[[Image:NGC 253.jpg|thumb|Detail of NGC 253 by [[Hubble Space Telescope]]. (Credit: HST/[[NASA]]/[[ESA]]).]]
The Sculptor Galaxy is located at the center of the [[Sculptor Group]], one of the nearest [[galaxy group|groups of galaxies]] to the [[Milky Way]].<ref name="karachentsev2005">{{cite journal|last=Karachentsev|first=I. D.|date=2005|title=The Local Group and Other Neighboring Galaxy Groups|journal=[[The Astronomical Journal]]|volume=129|issue=1|pages=178–188|arxiv=astro-ph/0410065|bibcode=2005AJ....129..178K|doi=10.1086/426368|s2cid=119385141 }}</ref> The Sculptor Galaxy (the brightest galaxy in the group and one of the [[Intrinsic brightness|intrinsically brightest]] galaxies in the vicinity of ours, only surpassed by the Andromeda Galaxy and the [[Sombrero Galaxy]]<ref name="Karachentsev2004">{{cite journal|last1=Karachentsev|first1=Igor D.|last2=Karachentseva|first2=Valentina E.|last3=Huchtmeier|first3=Walter K.|last4=Makarov|first4=Dmitry I.|date=2003|title=A Catalog of Neighboring Galaxies|journal=[[The Astronomical Journal]]|volume=127|issue=4|pages=2031–2068|bibcode=2004AJ....127.2031K|doi=10.1086/382905|doi-access=free}}</ref>) and the companion galaxies [[NGC 247]], [[PGC 2881]], [[PGC 2933]], [[Sculptor-dE1]], and [[UGCA 15]] form a gravitationally-bound core near the center of the group. Most other galaxies associated with the Sculptor Group are only weakly gravitationally bound to this core.<ref name="karachentsev2005" /><ref name="karachentsevetal2003">{{cite journal|last1=Karachentsev|first1=I. D.|last2=Grebel|first2=E. K.|last3=Sharina|first3=M. E.|last4=Dolphin|first4=A. E.|author5=D. Geisler|author6=P. Guhathakrta|author7=P. W. Hodge|author8=V. E. Karachentseva|author9=A. Sarajedini|display-authors=4|date=2003|title=Distances to nearby galaxies in Sculptor|journal=[[Astronomy and Astrophysics]]|volume=404|issue=1|pages=93–111|arxiv=astro-ph/0302045|bibcode=2003A&A...404...93K|doi=10.1051/0004-6361:20030170|author10=P. Seitzer|s2cid=54977869}}</ref>

===Starburst===
NGC 253's starburst has created several [[super star cluster]]s on NGC 253's center (discovered with the aid of the Hubble Space Telescope): one with a mass of {{val|1.5|e=6}} [[solar mass]]es, and [[absolute magnitude]] of at least −15, and two others with {{val|5|e=4}} solar masses and absolute magnitudes around −11;<ref name="Watson1996">{{cite journal|last1=Watson|first1=A. M.|last2=Gallagher|first2=J. S. III|last3=Holtzman|first3=J. A.|last4=Hester|first4=J. J.|author5=Mould, J. R.|author6=Ballester, G. E.|author7=Burrows, C. J.|author8=Casertano, S.|author9=Clarke, J. T.|display-authors=4|date=1996|title=The Discovery of Young, Luminous, Compact Stellar Clusters in the Starburst Galaxy NGC 253|url=https://authors.library.caltech.edu/53645/1/1996AJ____112__534W.pdf|journal=[[The Astronomical Journal]]|volume=112|issue=2|page=534|bibcode=1996AJ....112..534W|doi=10.1086/118032|author10=Crisp, D.|author11=Evans, R.|author12=Griffiths, R. E.|author13=Hoessel, J. G.|author14=Scowen, P. A.|author15=Stapelfeldt, K. R.|author16=Trauger, J. T.|author17=Westphal, J. A.}}</ref> later studies have discovered an even more massive cluster heavily obscured by NGC 253's [[Cosmic dust|interstellar dust]] with a mass of {{val|1.4|e=7}} solar masses, an age of around {{val|5.7|e=6}} years, and rich in [[Wolf–Rayet star]]s.<ref name="Kornei2009">{{cite journal|last1=Kornei|first1=Katherine A.|last2=McCrady|first2=Nate|date=2009|title=A Young Super Star Cluster in the Nuclear Region of NGC 253|journal=[[The Astrophysical Journal]]|volume=697|issue=2|pages=1180–1186|arxiv=0902.4027|bibcode=2009ApJ...697.1180K|doi=10.1088/0004-637X/697/2/1180|s2cid=18960325}}</ref> The super star clusters are arranged in an ellipse around the center of NGC 253, which from the Earth's perspective appears as a flat line.<ref>{{cite journal |arxiv= 2206.04700|doi= 10.3847/1538-4357/ac7b7a|title= The Morpho-kinematic Architecture of Super Star Clusters in the Center of NGC 253|year= 2022|last1= Levy|first1= Rebecca C.|last2= Bolatto|first2= Alberto D.|last3= Leroy|first3= Adam K.|last4= Sormani|first4= Mattia C.|last5= Emig|first5= Kimberly L.|last6= Gorski|first6= Mark|last7= Lenkić|first7= Laura|last8= Mills|first8= Elisabeth A. C.|last9= Tarantino|first9= Elizabeth|last10= Teuben|first10= Peter|last11= Veilleux|first11= Sylvain|last12= Walter|first12= Fabian|journal= The Astrophysical Journal|volume= 935|issue= 1|page= 19|bibcode= 2022ApJ...935...19L|s2cid= 249605852|doi-access= free}}</ref>

[[Star formation]] is also high in the northeast of NGC 253's disk, where a number of [[red supergiant star]]s can be found, and in its [[Galactic halo|halo]] there are young stars as well as some amounts of [[neutral hydrogen]]. This, along with other peculiarities found in NGC 253, suggest that a gas-rich [[dwarf galaxy]] collided with it 200 million years ago, disturbing its disk and starting the present starburst.<ref name="Davidge2010">{{cite journal|last=Davidge|first=T. J.|date=2010|title=Shaken, Not Stirred: The Disrupted Disk of the Starburst Galaxy NGC 253|journal=[[The Astrophysical Journal]]|volume=725|issue=1|pages=1342–1365|arxiv=1011.3006|bibcode=2010ApJ...725.1342D|doi=10.1088/0004-637X/725/1/1342|s2cid=118649411}}</ref>

As happens in other galaxies suffering strong star formation such as [[Messier 82]], [[NGC 4631]], or [[NGC 4666]], the [[stellar wind]]s of the massive stars produced in the starburst as well as their deaths as [[supernova]]e have blown out material to NGC 253's halo in the form of a [[galactic superwind|superwind]] that seems to be inhibiting star formation in the galaxy.<ref name="Bolatto2013">{{cite journal|last1=Bolatto|first1=Alberto D.|last2=Warren|first2=Steven R.|last3=Leroy|first3=Adam K.|last4=Walter|first4=Fabian|author5=Veilleux, Sylvain|author6=Ostriker, Eve C.|author7=Ott, Jürgen|author8=Zwaan, Martin|author9=Fisher, David B.|display-authors=4|date=2013|title=Suppression of star formation in the galaxy NGC 253 by a starburst-driven molecular wind|journal=[[Nature (journal)|Nature]]|volume=499|issue=7459|pages=450–453|arxiv=1307.6259|bibcode=2013Natur.499..450B|doi=10.1038/nature12351|pmid=23887428|author10=Weiss, Axel|author11=Rosolowsky, Erik|author12=Hodge, Jacqueline|s2cid=4366091}}</ref>

===Novae and Supernovae===
Although supernovae are generally associated with starburst galaxies, only one has been detected within the Sculptor Galaxy. SN 1940E (type unknown, mag. 14.5) was discovered by [[Fritz Zwicky]] on 22 November 1940, located approximately 54″ southwest of the galaxy's nucleus.<ref>{{cite journal | url = http://www.cbat.eps.harvard.edu/IAUCs/IAUC0848.png | title = Circular No. 848 : Nova in N. G. C. 253 | last = Strömgren | first = Elis | date = 4 February 1941 | journal = Central Bureau for Astronomical Telegrams | volume = 848 | pages = 1 | publisher = Observatory Copenhagen, [[International Astronomical Union|IAU]] | access-date = 18 June 2025}}</ref><ref>{{cite web | website=Transient Name Server | title=SN{{nbsp}}1940E | url=https://www.wis-tns.org/object/1940E | publisher = [[International Astronomical Union|IAU]] | access-date=27 November 2024}}</ref><ref name="barbonetal1984">{{cite journal | last1=Barbon| first1=R.| last2=Cappellaro| first2=E.| last3=Ciatti| first3=F.| last4=Turatto| first4=M.| last5=Kowal| first5=C. T.| date=1984| title=A revised supernova catalogue| journal=[[Astronomy & Astrophysics Supplement Series]]| volume=58| pages=735–750| bibcode=1984A&AS...58..735B}}</ref>

NGC 253 is close enough that classical [[nova]]e can also be detected.  The first confirmed nova in this galaxy was discovered by [[BlackGEM]] at magnitude 19.6 on 12 July 2024, and designated AT 2024pid.<ref>{{cite web | website=Transient Name Server | title=AT{{nbsp}}2024pid | url=https://www.wis-tns.org/object/2024pid | publisher = [[International Astronomical Union|IAU]] | access-date=27 November 2024}}</ref>

===Central black hole===
Research suggests the presence of a [[supermassive black hole]] in the center of this galaxy with a mass estimated to be 5 million times that of the Sun, which is slightly heavier than [[Sagittarius A*]].<ref>{{Cite web|url=https://www.jpl.nasa.gov/news/news.php?release=2013-198|title=Black Hole Naps Amidst Stellar Chaos|date=June 11, 2013|website=[[Jet Propulsion Laboratory]]|publisher=[[NASA]]}}</ref>

===Distance estimates===
At least two techniques have been used to measure distances to Sculptor in the past ten years.

Using the [[planetary nebula luminosity function]] (PNLF) method, an estimate of 10.89 {{±|0.85|1.24}} million light years (or Mly; 3.34 {{±|0.26|0.38}} [[parsec|Megaparsec]]s, or Mpc) was achieved in 2005.<ref name="Rekolaetal2005">
{{cite journal|last1=Rekola|first1=R.|last2=Richer|first2=M. G.|last3=McCall|first3=Marshall L.|last4=Valtonen|first4=M. J.|last5=Kotilainen|first5=J. K.|last6=Flynn|first6=Chris|date=2005|title=Distance to NGC 253 based on the planetary nebula luminosity function|journal=[[Monthly Notices of the Royal Astronomical Society]]|volume=361|issue=1|pages=330–336|bibcode=2005MNRAS.361..330R|doi=10.1111/j.1365-2966.2005.09166.x|doi-access=free}}</ref>

A recent study analyzing [[Multi-unit spectroscopic explorer|MUSE]] observations of the galaxy have identified over 500 [[planetary nebulae]] (PNe) in the galaxy, enabling a revision of the distance via the [[planetary nebula luminosity function|PNLF]]. This work derived a distance of 4.1 {{±|0.07|0.09}} Mpc, about 0.76 Mpc larger than what obtained previously with the same technique. The discrepancy was attributed to the misclassification of the brighter object in the first study sample. In addition, the distance is also 0.6 Mpc larger than the typically accepted distance coming mostly from [[tip of the red-giant branch]] (TRGB) measurements. In this case, the discrepancy is attributed to the extinction produced by the dusty [[interstellar medium]] of the galaxy. Modelling suggests that this dust, likely distributed vertically due to starburst-driven outflows, dims the PNe enough to bias the PNLF-based distance estimates. This analysis highlights the limitations of PNLF as a distance indicator in dusty, inclined galaxies like NGC 253.<ref>{{cite web|url=https://arxiv.org/pdf/2506.14921|title=The MUSE view of the Sculptor galaxy: survey overview and the planetary nebulae luminosity function|access-date=2025-06-22}}</ref>

The Sculptor Galaxy is close enough that the [[tip of the red-giant branch|TRGB]] method may also be used to estimate its distance. The estimated distance to Sculptor using this technique in 2004 yielded {{val|12.8|1.2|u=Mly}} ({{val|3.94|0.37|u=Mpc}}).<ref name="karachentsevetal2004">{{cite journal|last1=Karachentsev|first1=Igor D.|last2=Karachentseva|first2=Valentina E.|last3=Hutchmeier|first3=Walter K.|last4=Makarov|first4=Dmitry I.|date=2004|title=A Catalog of Neighboring Galaxies|journal=[[The Astronomical Journal]]|volume=127|issue=4|pages=2031–2068|bibcode=2004AJ....127.2031K|doi=10.1086/382905|doi-access=free}}</ref><ref name="Karachentsevetal2006">{{cite journal|author=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|bibcode=2006Ap.....49....3K|doi=10.1007/s10511-006-0002-6|s2cid=120973010}}</ref>

A weighted average of the most reliable distance estimates gives a distance of {{val|11.4|0.7|u=Mly}} ({{val|3.5|0.2|u=Mpc}}).<ref name="Rekolaetal2005" />

==Satellite galaxies==
An international team of researchers has used the [[Subaru Telescope]] to identify a faint dwarf galaxy disrupted by NGC 253. The [[satellite galaxy]] is called NGC 253-dw2 and may not survive its next passage by its much larger host. The host galaxy may suffer some damage too if the dwarf is massive enough.<ref>{{cite web|url=https://www.subarutelescope.org/Pressrelease/2016/02/08/index.html|title=Galactic Space Oddity Discovered|date=February 8, 2016|website=[[Subaru Telescope]]|publisher=[[National Astronomical Observatory of Japan]]|access-date=February 9, 2016}}</ref> The interplay between the two galaxies is responsible for the disturbance in NGC 253's structure.<ref>{{cite journal|last1=Romanowsky|first1=Aaron J.|last2=Martínez-Delgado|first2=David|last3=Martin|first3=Nicolas F.|last4=Morales|first4=Gustavo|last5=Jennings|first5=Zachary G.|last6=GaBany|first6=R. Jay|last7=Brodie|first7=Jean P.|last8=Grebel|first8=Eva K.|last9=Schedler|first9=Johannes|display-authors=4|title=Satellite accretion in action: a tidally disrupting dwarf spheroidal around the nearby spiral galaxy NGC 253|journal=[[Monthly Notices of the Royal Astronomical Society]]|volume=456|issue=1|pages=103–107|arxiv=1512.03815|bibcode=2016MNRAS.457L.103R|doi=10.1093/mnrasl/slv207|first10=Michael|last10=Sidonio|year=2016|doi-access=free }}</ref>

Until 2020, 12 satellite galaxies were known to exist within the region of influence of NGC 253: NGC 247, NGC 7793 and its companions PGC 704814 and ESO 349–031, DDO 6, ESO 349-03, ESO 540-032, KDG 2, Sc22, LVJ0055-2310, Scl-MM-Dw1, Scl-MM-Dw2.<ref>{{Cite journal |last=Karachentsev |first=Igor D. |last2=Kaisina |first2=Elena I. |last3=Makarov |first3=Dmitry I. |date=2013-12-03 |title=SUITES OF DWARFS AROUND NEARBY GIANT GALAXIES |url=https://iopscience.iop.org/article/10.1088/0004-6256/147/1/13 |journal=The Astronomical Journal |volume=147 |issue=1 |pages=13 |doi=10.1088/0004-6256/147/1/13 |issn=0004-6256}}</ref>

In June 2021, the discovery of three new satellite galaxies, named Donatiello II, Donatiello III, and Donatiello IV, was reported by Italian amateur astronomer [[Giuseppe Donatiello]]. Donatiello II is the third-closest satellite to NGC 253. Donatiello III, approximately 340,000 parsecs from NGC 253, is one of the outer members of the satellite group. Donatiello IV, along with the irregular dwarf galaxy ESO 540-032, forms a subgroup around NGC 247.<ref>{{Cite journal |last=Martínez-Delgado |first=David |last2=Makarov |first2=Dmitry |last3=Javanmardi |first3=Behnam |last4=Pawlowski |first4=Marcel S. |last5=Makarova |first5=Lidia |last6=Donatiello |first6=Giuseppe |last7=Lang |first7=Dustin |last8=Román |first8=Javier |last9=Vivas |first9=Kathy |last10=Carballo-Bello |first10=Julio A. |date=2021-08-01 |title=Tracing satellite planes in the Sculptor group - I. Discovery of three faint dwarf galaxies around NGC 253 |url=https://www.aanda.org/articles/aa/abs/2021/08/aa41242-21/aa41242-21.html |journal=Astronomy & Astrophysics |language=en |volume=652 |pages=A48 |doi=10.1051/0004-6361/202141242 |issn=0004-6361}}</ref>

In August 2021, another team of astronomers announced the discovery of three additional new satellite galaxies, designated Scl-MM-dw3, Scl-MM-dw4, and Scl-MM-dw5; however, the object Scl-MM-dw3, as the study authors specified, corresponds to the previously reported Donatiello II. Observed with the Hubble Space Telescope, they are 3.48, 4.10, and 3.90 Mpc away, respectively, and can be classified as ultra-faint dwarf galaxies (UFDs).<ref>{{Citation |last=Mutlu-Pakdil |first=Burçin |title=Hubble Space Telescope Observations of NGC 253 Dwarf Satellites: Discovery of Three Ultra-faint Dwarf Galaxies |date=2021-08-20 |url=http://arxiv.org/abs/2108.09312 |access-date=2025-11-02 |publisher=arXiv |doi=10.48550/arXiv.2108.09312 |id=arXiv:2108.09312 |last2=Sand |first2=David J. |last3=Crnojević |first3=Denija |last4=Jones |first4=Michael G. |last5=Caldwell |first5=Nelson |last6=Guhathakurta |first6=Puragra |last7=Seth |first7=Anil C. |last8=Simon |first8=Joshua D. |last9=Spekkens |first9=Kristine}}</ref>

Observations with the Hubble Space Telescope also determined the distances of the Donatiello III and Donatiello IV galaxies at 3.37 and 3.94 Mpc, respectively, confirming their membership in the NGC 253 satellite system. The object designated dw0036m2828, estimated at 3.76 Mpc, was also confirmed as belonging to the NGC 253 satellite system. The same study also ruled out the possibility that the dwarf galaxy reported as SculptorSR is in the NGC 253 group, being approximately 19 Mpc away and possibly interacting with NGC 150.<ref>{{Citation |last=Mutlu-Pakdil |first=Burçin |title=The Faint Satellite System of NGC 253: Insights into Low-Density Environments and No Satellite Plane |date=2024-01-25 |url=http://arxiv.org/abs/2401.14457 |access-date=2025-11-02 |publisher=arXiv |doi=10.48550/arXiv.2401.14457 |id=arXiv:2401.14457 |last2=Sand |first2=David J. |last3=Crnojević |first3=Denija |last4=Bennet |first4=Paul |last5=Jones |first5=Michael G. |last6=Spekkens |first6=Kristine |last7=Karunakaran |first7=Ananthan |last8=Zaritsky |first8=Dennis |last9=Caldwell |first9=Nelson}}</ref>

In March 2024, an international team announced the discovery of a new satellite galaxy named NGC253-SNFC-dw1. It is a very diffuse and faint object, revealed using deep stellar photometry obtained as part of the Subaru Near-Field Cosmology Survey using the Hyper Suprime-Cam on the Subaru Telescope. The distance has been estimated at 3.62 Mpc.<ref>{{Cite web |title=Uncovering the Ghostly Remains of an Extremely Diffuse Satellite in the Remote Halo of NGC 253 1footnote 11footnote 1This research is based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. |url=https://arxiv.org/html/2403.16011v1 |access-date=2025-11-02 |website=arxiv.org |language=en}}</ref>

In May 2024, the discovery of five more dwarf satellite galaxies was reported, also discovered by [[Giuseppe Donatiello]]. In accordance with the nomenclature used, they have been named Donatiello V, Donatiello VI, Donatiello VII, Donatiello VIII, and Donatiello IX. The new discoveries weaken the hypothesis of a coplanar distribution of the satellites.<ref>{{Citation |last=Martinez-Delgado |first=David |title=Tracing satellite planes in the Sculptor group: II. Discovery of five faint dwarf galaxies in the DESI Legacy Survey |date=2025-10-08 |url=http://arxiv.org/abs/2405.03769 |access-date=2025-11-02 |publisher=arXiv |doi=10.48550/arXiv.2405.03769 |id=arXiv:2405.03769 |last2=Stein |first2=Michael |last3=Pawlowski |first3=Marcel S. |last4=Sakowska |first4=Joanna D. |last5=Makarov |first5=Dmitry |last6=Makarova |first6=Lidia |last7=Donatiello |first7=Giuseppe |last8=Lang |first8=Dustin}}</ref>

NGC 59, NGC 625, DDO 226, and UGCA 442 are instead considered to be peripheral galaxies and not related to NGC 253, despite being in the same group.

==See also==
* Globular cluster [[NGC 288]], located 1.8° south-southeast of the Sculptor Galaxy.
* [[2MASX J00482185-2507365 occulting pair]], discovered while photographing NGC 253

==References==
{{Reflist}}

==External links==
{{commons category}}
* [http://hubblesite.org/newscenter/newsdesk/archive/releases/1995/10/ STScI news release: Hubble Probes the Violent Birth of Stars in Galaxy NGC 253]
* [http://hubblesite.org/newscenter/newsdesk/archive/releases/1998/42/ STScI news release: Behind a Dusty Veil Lies a Cradle of Star Birth]
{{WikiSky|1=NGC 253}}
* [http://messier.seds.org/xtra/ngc/n0253.html SEDS] – NGC 253

{{Sky|00|47|33.13|-|25|17|17.1|11400000}}
{{Catalogs|NGC=253|C=65|PGC=2789}}
{{Caldwell catalogue}}
{{NGC objects: 1-1000}}
{{Sculptor (constellation)}}

{{DEFAULTSORT:Galaxy, Sculptor}}
[[Category:Starburst galaxies]]
[[Category:Intermediate spiral galaxies]]
[[Category:Sculptor (constellation)]]
[[Category:Sculptor Group]]
[[Category:NGC objects]]
[[Category:Principal Galaxies Catalogue objects|02789]]
[[Category:Caldwell objects|065b]]
[[Category:Astronomical objects discovered in 1783|17830923]]
[[Category:UGCA objects|013]]
[[Category:Discoveries by Caroline Herschel]]