View source for Messier 77

{{Short description|Galaxy in the constellation Cetus}}
{{Use dmy dates|date=March 2021}}
{{Infobox Galaxy
 | name       = [[Messier object|Messier]] 77
 | image      = Messier 77 spiral galaxy by HST.jpg
 | caption    = M77 imaged by the [[Hubble Space Telescope]]
 | epoch      = [[J2000]]
 | ra         = {{RA|02|42|40.771}}<ref name=Skrutskie2006/>
 | dec        = {{DEC|−00|00|47.84}}<ref name=Skrutskie2006/>
 | dist_ly    = {{cvt|14.4|Mpc|Mly|order=flip|lk=on}}<ref name="xiv"/>
 | z          = 0.003793<ref name="ned" />
 | h_radial_v = {{Val|1137|3|u=km/s|fmt=commas}}<ref name="ned" />
 | appmag_v   = 8.9<ref>{{cite web |url=https://messier.seds.org/m/m077.html |title=Messier 77 |access-date=30 April 2022 |website=SEDS Messier Catalog}}</ref>
 | type       = (R)SA(rs)b<ref name=vaucoulerus1991/>
 | size       = {{convert|27.70|kpc|ly|-3|abbr=off|lk=on}}<ref name="ned" /><br />(diameter; [[Galaxy#Isophotal diameter|D<sub>25</sub> isophote]])
 | size_v     = {{Val|7.1|×|6.0|u=arcminute}}{{r|ned}}
 | constellation name = [[Cetus (constellation)|Cetus]]
 | mass       = ~1{{e|12}}<ref name=messier/>
 | notes      = One of the biggest galaxies of [[Charles Messier|Messier]]'s catalog. Inclination estimated to be 40°.<ref name="xiv"/>
 | names      = {{odlist | name= Cetus&nbsp;A, | NGC= 1068 | name2= [[Third Cambridge Catalogue of Radio Sources|3C]] 71 | name3= [[Fourth Cambridge Survey|4C]] -00.13 | Arp= 37 | UGC= 2188 | PGC= 10266 | CGCG= 388-098 | MCG= +00-07-083 | IRAS= 02401-0013}}<ref name="simbad" />
}}

'''Messier 77''' ('''M77'''), also known as '''[[New General Catalogue|NGC]] 1068''' or the '''Squid Galaxy''', is a [[barred spiral galaxy]] in the [[constellation]] [[Cetus (constellation)|Cetus]]. It is about {{convert|47|e6ly|Mpc|lk=on}} away from Earth, and was discovered by [[Pierre Méchain]] in 1780, who originally described it as a nebula.  Méchain then communicated his discovery to [[Charles Messier]], who subsequently listed the object in his [[Messier Catalogue|catalog]].<ref name="jonesbook1991"/> Both Messier and [[William Herschel]] described this galaxy as a star cluster.<ref name="jonesbook1991" /> Today, however, the object is known to be a galaxy. It is one of the brightest [[Seyfert galaxy|Seyfert galaxies]] visible from Earth and has a [[Galaxy#Isophotal diameter|D<sub>25</sub> isophotal diameter]] of about {{convert|27.70|kpc|ly|-3|abbr=off|lk=on}}.<ref name="ned" />

== Morphology ==
The [[Galaxy morphological classification|morphological classification]] of NGC 1068 in the [[Gérard de Vaucouleurs|De Vaucouleurs]] system is (R)SA(rs)b,<ref name=vaucoulerus1991/> where the '(R)' indicates an outer ring-like structure, 'SA' denotes a non-barred spiral, '(rs)' means a transitional inner ring/spiral structure, and 'b' says the spiral arms are moderately wound.<ref name=deVaucouleurs1963/> Ann [[et al.]] (2015) gave it a class of SAa,<ref name=Ann2015/> suggesting tightly wound arms. However, [[infrared astronomy|infrared]] images of the inner part of the galaxy reveal a prominent bar not seen in visual light,<ref name=Thronson1989/> and for this reason it is now considered a barred spiral.<ref name=Alexander2000/> Messier 77 is the largest member of a small group of galaxies,<ref>{{cite web |last1=Normandin |first1=George |title=Spiral Galaxy M-77 (NGC 1068) in Cetus |url=https://www.kopernik.org/images/archive/m77.htm |website=www.kopernik.org |publisher=Kopernik Observatory & Science Center |access-date=24 January 2025}}</ref> which includes [[NGC 1055]], an edge-on spiral galaxy likely twisted by gravitational interactions with Messier 77, and five small irregular galaxies.<ref>{{cite web |last1=Hook |first1=Richard |title=A Galaxy on the Edge |url=https://www.eso.org/public/news/eso1707/ |website=www.eso.org |publisher=European Southern Observatory |access-date=24 January 2025 |language=en}}</ref>  

Messier 77 is an [[active galaxy]] with an [[active galactic nucleus]] (AGN), which is obscured from view by astronomical dust at visible wavelengths. The diameter of the molecular disk and hot plasma associated with the obscuring material was first measured at radio wavelengths by the [[Very Long Baseline Array|VLBA]] and [[Very Large Array|VLA]]. The hot dust around the nucleus was subsequently measured in the mid-infrared by the [[Mid-IR Interferometric instrument|MIDI]] instrument at the [[Very Large Telescope|VLT]]I. It is the brightest<ref name="deVaucouleurs1973"/> and one of the closest and best-studied<ref name=Alexander2000/> type 2 [[Seyfert galaxy|Seyfert galaxies]],<ref name="xiv"/> forming a prototype of this class.<ref name=Alexander2000/>

== Research ==
Messier 77 is of key interest to scientists due to its relative proximity and [[luminosity]], allowing for study of its [[active galactic nucleus]].<ref>{{Cite journal |last1=Isbell |first1=J. W. |last2=Ertel |first2=S. |last3=Pott |first3=J. -U. |last4=Weigelt |first4=G. |last5=Stalevski |first5=M. |last6=Leftley |first6=J. |last7=Jaffe |first7=W. |last8=Petrov |first8=R. G. |last9=Moszczynski |first9=N. |last10=Vermot |first10=P. |last11=Hinz |first11=P. |last12=Burtscher |first12=L. |last13=Gámez Rosas |first13=V. |last14=Becker |first14=A. |last15=Carlson |first15=J. |date=2025-01-01 |title=Direct imaging of active galactic nucleus outflows and their origin with the 23 m Large Binocular Telescope |url=https://ui.adsabs.harvard.edu/abs/2025NatAs.tmp...15I/abstract |journal=Nature Astronomy |volume=9 |issue=3 |page=417 |doi=10.1038/s41550-024-02461-y |issn=2397-3366|arxiv=2502.01840 |bibcode=2025NatAs...9..417I }}</ref> This section contains relevant scientific discoveries that have been made as a result of studying M77.

It has been proposed that type 2 Seyfert galaxies are the same class of object as type 1 Seyfert galaxies, viewed from such an angle that the type 1 core is hidden from view.<ref>{{Cite journal |last1=Krips |first1=M. |last2=Eckart |first2=A. |last3=Neri |first3=R. |last4=Schödel |first4=R. |last5=Leon |first5=S. |last6=Downes |first6=D. |last7=García-Burillo |first7=S. |last8=Combes |first8=F. |date=2006-01-01 |title=Continuum emission in NGC 1068 and NGC 3147: indications for a turnover in the core spectra |url=https://www.aanda.org/articles/aa/abs/2006/04/aa3729-05/aa3729-05.html |journal=Astronomy & Astrophysics |language=en |volume=446 |issue=1 |pages=113–120 |doi=10.1051/0004-6361:20053729 |issn=0004-6361|arxiv=astro-ph/0509825 |bibcode=2006A&A...446..113K }}</ref> An analysis of NGC 1068's spectra using [[interferometry]] by Tacconi et al. (1994) suggested that the galaxy's Seyfert 1 core was obstructed by a thick [[molecular cloud]] region.<ref>{{Cite journal |last1=Tacconi |first1=L. J. |last2=Genzel |first2=R. |last3=Blietz |first3=M. |last4=Cameron |first4=M. |last5=Harris |first5=A. I. |last6=Madden |first6=S. |date=1994-05-01 |title=The Nature of the Dense Obscuring Material in the Nucleus of NGC 1068 |url=https://ui.adsabs.harvard.edu/abs/1994ApJ...426L..77T/abstract |journal=The Astrophysical Journal |volume=426 |pages=L77 |doi=10.1086/187344 |bibcode=1994ApJ...426L..77T |issn=0004-637X}}</ref>

X-ray source 1H 0244+001 in Cetus has been identified as Messier 77.<ref name=Wood/>

It has a radio jet consisting of a northeast and a southwest region, caused by interactions with the interstellar medium.<ref>{{Cite journal |last1=Gallimore |first1=J. F. |last2=Baum |first2=S. A. |last3=O'Dea |first3=C. P. |last4=Pedlar |first4=A. |date=1996-02-01 |title=The Subarcsecond Radio Structure in NGC 1068. I. Observations and Results |url=https://ui.adsabs.harvard.edu/abs/1996ApJ...458..136G |journal=The Astrophysical Journal |volume=458 |page=136 |doi=10.1086/176798 |bibcode=1996ApJ...458..136G |issn=0004-637X}}</ref>The presence of bow shocks in the northeast region due to these interactions overlap with the edges of molecular outflow, suggesting that the jet is responsible for the outflow.<ref>{{Citation |last1=Mutie |first1=Isaac M. |title=Radio jets in NGC 1068 with e-MERLIN and VLA: structure and morphology |date=2023-12-15 |arxiv=2312.09722 |last2=Williams-Baldwin |first2=David |last3=Beswick |first3=Robert J. |last4=Bempong-Manful |first4=Emmanuel K. |last5=Baki |first5=Paul O. |last6=Muxlow |first6=Tom W. B. |last7=Gallimore |first7=Jack F. |last8=Aalto |first8=Susanne E. |last9=Dullo |first9=Bililign T.|journal=Monthly Notices of the Royal Astronomical Society |volume=527 |issue=4 |page=11756 |doi=10.1093/mnras/stad3864 |doi-access=free |bibcode=2024MNRAS.52711756M }}</ref> 

In February 2022 astronomers reported a cloud of cosmic dust, detected through [[infrared]] [[interferometry]] observations, located at the centre of Messier 77 that is hiding a [[supermassive black hole]].<ref>{{cite press release |author=<!--Not stated--> |title=Supermassive black hole caught hiding in a ring of cosmic dust |url=https://www.eso.org/public/news/eso2203/ |publisher=European Southern Observatory |date=16 February 2022 |access-date=2024-11-08}}</ref><ref>{{cite journal |display-authors=5 |last1=Gámez Rosas |first1=Violeta |last2=Isbell |first2=Jacob W. |last3=Jaffe |first3=Walter |last4=Petrov |first4=Romain G. |last5=Leftley |first5=James H. |last6=Hofmann |first6=Karl-Heinz |last7=Millour |first7=Florentin |last8=Burtscher |first8=Leonard |last9=Meisenheimer |first9=Klaus |last10=Meilland |first10=Anthony |last11=Waters |first11=Laurens B. F. M. |last12=Lopez |first12=Bruno |last13=Lagarde |first13=Stéphane |last14=Weigelt |first14=Gerd |last15=Berio |first15=Philippe |last16=Allouche |first16=Fatme |last17=Robbe-Dubois |first17=Sylvie |last18=Cruzalèbes |first18=Pierre |last19=Bettonvil |first19=Felix |last20=Henning |first20=Thomas |last21=Augereau |first21=Jean-Charles |last22=Antonelli |first22=Pierre |last23=Beckmann |first23=Udo |last24=van Boekel |first24=Roy |last25=Bendjoya |first25=Philippe |last26=Danchi |first26=William C. |last27=Dominik |first27=Carsten |last28=Drevon |first28=Julien |last29=Gallimore |first29=Jack F. |last30=Graser |first30=Uwe |last31=Heininger |first31=Matthias |last32=Hocdé |first32=Vincent |last33=Hogerheijde |first33=Michiel |last34=Hron |first34=Josef |last35=Impellizzeri |first35=Caterina M. V. |last36=Klarmann |first36=Lucia |last37=Kokoulina |first37=Elena |last38=Labadie |first38=Lucas |last39=Lehmitz |first39=Michael |last40=Matter |first40=Alexis |last41=Paladini |first41=Claudia |last42=Pantin |first42=Eric |last43=Pott |first43=Jörg-Uwe |last44=Schertl |first44=Dieter |last45=Soulain |first45=Anthony |last46=Stee |first46=Philippe |last47=Tristram |first47=Konrad |last48=Varga |first48=Jozsef |last49=Woillez |first49=Julien |last50=Wolf |first50=Sebastian |last51=Yoffe |first51=Gideon |last52=Zins |first52=Gerard |title=Thermal imaging of dust hiding the black hole in NGC 1068 |journal=Nature |date=February 2022 |volume=602 |issue=7897 |pages=403–407 |doi=10.1038/s41586-021-04311-7 |pmid=35173340 |arxiv=2112.13694 |url=https://www.nature.com/articles/s41586-021-04311-7 |bibcode=2022Natur.602..403G}}</ref>

In November 2022, the [[IceCube Neutrino Observatory|IceCube]] collaboration announced the detection of a [[neutrino]] source emitted by the active galactic nucleus of Messier 77.<ref>{{cite journal |collaboration=IceCube Collaboration |display-authors=1 |last1=Abbasi |first1=R. |last2=Ackermann |first2=M. |last3=Adams |first3=J. |last4=Aguilar |first4=J. A. |last5=Ahlers |first5=M. |last6=Ahrens |first6=M. |last7=Alameddine |first7=J. M. |last8=Alispach |first8=C. |last9=Alves |first9=A. A. |last10=Amin |first10=N. M. |last11=Andeen |first11=K. |last12=Anderson |first12=T. |last13=Anton |first13=G. |last14=Argüelles |first14=C. |last15=Ashida |first15=Y. |last16=Axani |first16=S. |last17=Bai |first17=X. |last18=Balagopal V. |first18=A. |last19=Barbano |first19=A. |last20=Barwick |first20=S. W. |last21=Bastian |first21=B. |last22=Basu |first22=V. |last23=Baur |first23=S. |last24=Bay |first24=R. |last25=Beatty |first25=J. 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G. |last312=Schumacher |first312=L. |last313=Schwefer |first313=G. |last314=Sclafani |first314=S. |last315=Seckel |first315=D. |last316=Seunarine |first316=S. |last317=Sharma |first317=A. |last318=Shefali |first318=S. |last319=Silva |first319=M. |last320=Skrzypek |first320=B. |last321=Smithers |first321=B. |last322=Snihur |first322=R. |last323=Soedingrekso |first323=J. |last324=Soldin |first324=D. |last325=Spannfellner |first325=C. |last326=Spiczak |first326=G. M. |last327=Spiering |first327=C. |last328=Stachurska |first328=J. |last329=Stamatikos |first329=M. |last330=Stanev |first330=T. |last331=Stein |first331=R. |last332=Stettner |first332=J. |last333=Steuer |first333=A. |last334=Stezelberger |first334=T. |last335=Stokstad |first335=R. |last336=Stürwald |first336=T. |last337=Stuttard |first337=T. |last338=Sullivan |first338=G. W. |last339=Taboada |first339=I. |last340=Ter-Antonyan |first340=S. |last341=Tilav |first341=S. |last342=Tischbein |first342=F. |last343=Tollefson |first343=K. |last344=Tönnis |first344=C. |last345=Toscano |first345=S. |last346=Tosi |first346=D. |last347=Trettin |first347=A. |last348=Tselengidou |first348=M. |last349=Tung |first349=C. F. |last350=Turcati |first350=A. |last351=Turcotte |first351=R. |last352=Turley |first352=C. F. |last353=Twagirayezu |first353=J. P. |last354=Ty |first354=B. |last355=Unland Elorrieta |first355=M. A. |last356=Valtonen-Mattila |first356=N. |last357=Vandenbroucke |first357=J. |last358=van Eijndhoven |first358=N. |last359=Vannerom |first359=D. |last360=van Santen |first360=J. |last361=Verpoest |first361=S. |last362=Walck |first362=C. |last363=Watson |first363=T. B. |last364=Weaver |first364=C. |last365=Weigel |first365=P. |last366=Weindl |first366=A. |last367=Weiss |first367=M. J. |last368=Weldert |first368=J. |last369=Wendt |first369=C. |last370=Werthebach |first370=J. |last371=Weyrauch |first371=M. |last372=Whitehorn |first372=N. |last373=Wiebusch |first373=C. H. |last374=Williams |first374=D. R. |last375=Wolf |first375=M. |last376=Woschnagg |first376=K. |last377=Wrede |first377=G. |last378=Wulff |first378=J. |last379=Xu |first379=X. W. |last380=Yanez |first380=J. P. |last381=Yoshida |first381=S. |last382=Yu |first382=S. |last383=Yuan |first383=T. |last384=Zhang |first384=Z. |last385=Zhelnin |first385=P. |title=Evidence for neutrino emission from the nearby active galaxy NGC 1068 |journal=Science |date=4 November 2022 |volume=378 |issue=6619 |pages=538–543 |doi=10.1126/science.abg3395 |url=https://www.science.org/doi/10.1126/science.abg3395 |pmid=36378962 |arxiv=2211.09972 |bibcode=2022Sci...378..538I |hdl=2013/ULB-DIPOT:oai:dipot.ulb.ac.be:2013/360290 |s2cid=253320297 |issn=0036-8075}}</ref><ref>{{Cite web |last=Staff |title=IceCube neutrinos give us first glimpse into the inner depths of an active galaxy |url=https://icecube.wisc.edu/news/press-releases/2022/11/icecube-neutrinos-give-us-first-glimpse-into-the-inner-depths-of-an-active-galaxy/ |access-date=2022-11-23 |website=IceCube |date=3 November 2022 |language=en-US}}</ref> It is the second detection by IceCube after [[TXS 0506+056]], and only the fourth known source including [[SN1987A]] and [[Solar neutrino|solar neutrinos]]. A potential candidate for the source of these neutrinos is the magnetic corona surrounding the active galactic nucleus, providing powerful enough particle acceleration to cause neutron radiation phenomena.<ref>{{Cite journal |last1=Fiorillo |first1=Damiano F. G. |last2=Comisso |first2=Luca |last3=Peretti |first3=Enrico |last4=Petropoulou |first4=Maria |last5=Sironi |first5=Lorenzo |date=2024-10-01 |title=A Magnetized Strongly Turbulent Corona as the Source of Neutrinos from NGC 1068 |journal=The Astrophysical Journal |volume=974 |issue=1 |page=75 |doi=10.3847/1538-4357/ad7021 |doi-access=free |arxiv=2407.01678 |bibcode=2024ApJ...974...75F |issn=0004-637X}}</ref> To explain the combination of Messier 77 being an energetic neutrinos source and a weak gamma rays source, a mechanism was suggested whereby helium nuclei collide with ultraviolet photons emitted by the galaxy's central region and break up, releasing neutrons that eventually decay into neutrinos without producing gamma rays.<ref>{{Cite journal |last1=Yasuda |first1=Koichiro |last2=Sakai |first2=Nobuyuki |last3=Inoue |first3=Yoshiyuki |last4=Kusenko |first4=Alexander |date=2025-04-18 |title=Neutrinos and Gamma Rays from Beta Decays in an Active Galactic Nucleus NGC 1068 Jet |url=https://journals.aps.org/prl/abstract/10.1103/PhysRevLett.134.151005 |journal=Physical Review Letters |volume=134 |issue=15 |article-number=151005 |doi=10.1103/PhysRevLett.134.151005|pmid=40315530 |arxiv=2405.05247 |bibcode=2025PhRvL.134o1005Y |osti=2560524 }}</ref>

==Supernova==
One [[supernova]] has been observed in Messier 77. '''SN 2018ivc''' ([[Type II Supernova|Type II]], mag. 14.6523) was discovered  by the DLT40 Survey on 24 November 2018.<ref name="King"/><ref>{{cite web | website=Transient Name Server | title=SN 2018ivc | url=https://www.wis-tns.org/object/2018ivc | publisher = [[International Astronomical Union|IAU]] | access-date=11 April 2025}}</ref>

==Gallery==
<gallery mode=packed heights=200px style="text-align:left">
File:The squid and the whale (potw2515a).jpg|M77 imaged by the [[Hubble Space Telescope]]|alt="A close-up of a spiral galaxy, seen face-on. Its center is a bright glowing From the sides of the galaxy's core emerge spiral arms which wind through the round disc of the galaxy, filled with shining pink spots where stars are forming and more dark-red dust. Some faint stars can be seen around the galaxy, as well as a particularly bright star in the lower left of the image."
File:Dazzling galaxy Messier 77.jpg|M77 imaged by ESO's Very Large Telescope (VLT)<ref name=eso />
File:M77 Clr SuperNova 2.jpg|M77 with SN 2018ivc, November 2018
</gallery>

==See also==
* [[List of Messier objects]]
* [[NGC 1106]] Another galaxy with an active galactic nucleus.

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<ref name="King">{{cite news |last1=King |first1=Bob |title=Supernova Discovered in the Bright Galaxy M77 |url=https://www.skyandtelescope.com/observing/supernova-discovered-in-the-bright-galaxy-m77/?k=Pg%2FjMopAjLuymaFqJZqBEJMUEcArttgJ8%2B6vHkAwjlw%3D&cid=DM88427&bid=879626371 |website=Sky & Telescope |access-date=30 November 2018|date=2018-11-29 }}</ref>

<ref name=eso>{{cite web | title=Dazzling galaxy Messier 77 | url=https://www.eso.org/public/images/eso1720a/ | website=www.eso.org | access-date=5 July 2017}}</ref>
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==External links==
{{commons category|Messier 77}}
* {{WikiSky}}
* [https://web.archive.org/web/20110722021432/http://blackholes.stardate.org/directory/factsheet.php?p=M77 "StarDate: M77 Fact Sheet"]
* [http://messier.seds.org/m/m077.html Spiral Galaxy M77 @ SEDS Messier pages]
* [https://www.vlba.nrao.edu/imgmonth/N1068/ VLBA image of the month: radio continuum and water masers of NGC 1068]
* [https://web.archive.org/web/20050306093230/http://www.eso.org/outreach/press-rel/pr-2004/pr-10-04.html Press release about VLTI observations of NGC 1068]
* [https://www.eso.org/public/unitedkingdom/news/eso1720/?lang ESO:Dazzling Spiral with an Active Heart] incl. Potos & Animation
* {{cite web|last=Gray|first=Meghan|title=M77 – Globular Cluster|url=http://www.deepskyvideos.com/videos/messier/M77.html|work=Deep Sky Videos|publisher=[[Brady Haran]]|author2=Hardy, Liam}}
* {{APOD |date=10 May 2013 |title=Messier 77}}

{{Sky|02|42|40.7|-|00|00|48|47000000}}
{{Portal bar|Astronomy|Stars|Outer space}}
{{Ngc15}}
{{Catalogs|M=77|NGC=1068|UGC=2188|PGC=10266|Arp=37}}
{{Messier objects}}
{{List of Seyfert galaxies}}
{{Cetus}}
{{Authority control}}

{{DEFAULTSORT:Messier 077}}
[[Category:Barred spiral galaxies]]
[[Category:Seyfert galaxies]]
[[Category:Radio galaxies]]
[[Category:Luminous infrared galaxies]]
[[Category:Cetus]]
[[Category:Messier objects|077]]
[[Category:NGC objects]]
[[Category:UGC objects|02188]]
[[Category:Principal Galaxies Catalogue objects|010266]]
[[Category:Arp objects|041]]
[[Category:Astronomical objects discovered in 1780]]
[[Category:3C objects|071]]
[[Category:4C objects]]
[[Category:Discoveries by Pierre Méchain]]
[[Category:MCG objects|+00-07-083]]
[[Category:IRAS catalogue objects|02401-0013]]