View source for Messier 90

{{Short description|Galaxy in the constellation Virgo}}
{{Use dmy dates|date=June 2021}}
{{Infobox galaxy
| name = [[Messier object|Messier]] 90
| image = [[File:Messier 90 - HST.png|300px]]
| caption = Messier 90 taken by [[Hubble Space Telescope|Hubble]]
| epoch = [[J2000]]
| constellation name = [[Virgo (constellation)|Virgo]]<ref name="sinnott1988">
{{cite book
 | editor=R. W. Sinnott
 | title= The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer
 | date=1988
 | publisher=[[Sky Publishing Corporation]]/[[Cambridge University Press]]
 | isbn=978-0-933346-51-2
}}</ref>
| ra = {{RA|12|36|49.8}}<ref name="ned">
{{cite web
 | title=NASA/IPAC Extragalactic Database
 | work=Results for NGC 4569
 | url=http://nedwww.ipac.caltech.edu/
 | access-date=2006-02-01
}}</ref>
| dec = {{DEC|+13|09|46}}<ref name="ned"/>
| size_v = 9.5 × 4.4 [[Minute and second of arc|moa]]<ref name="ned"/>
| appmag_v = 9.5<ref>{{cite web |url=https://messier.seds.org/m/m090.html |title=Messier 90 |access-date=30 April 2022 |website=SEDS Messier Catalog}}</ref>
| type = SAB(rs)ab,<ref name="ned"/> [[LINER]],<ref name="ned"/> Sy<ref name="ned"/>
 | h_radial_v = {{val|−235|4|u=km/s}}<ref name="ned"/>
|z = {{val|-0.000784|0.000013}}<ref name="ned"/>
 | gal_v = {{val|−282|4|u=km/s}}<ref name="ned"/>
|dist_ly = {{convert|58.7|+/-|2.8|Mly|Mpc|2|lk=on|abbr=on}}
| names = [[New General Catalogue|NGC]] 4569,<ref name="ned"/> [[Uppsala General Catalogue|UGC]] 7786,<ref name="ned"/> [[Principal Galaxies Catalogue|PGC]] 42089,<ref name="ned"/> [[Atlas of Peculiar Galaxies|Arp]] 76<ref name="ned"/>
| references = [[SIMBAD]]: [http://simbad.u-strasbg.fr/simbad/sim-id?Ident=M90 Search M90]
}}

'''Messier 90''' (also known as '''M90''' and '''NGC 4569''') is an [[intermediate spiral galaxy]] exhibiting a weak inner ring structure about 60 million [[light-year]]s away{{Ref label|A|a|none}} in the [[constellation]] [[Virgo (constellation)|Virgo]]. It was discovered by [[Charles Messier]] in 1781.<ref name="jones1991">
{{cite book
 | author=K. G. Jones
 | date=1991 | edition= 2nd
 | title=Messier's Nebulae and Star Clusters
 | publisher=[[Cambridge University Press]]
 | isbn=978-0-521-37079-0
}}</ref>

== Membership of the Virgo Cluster ==
Messier 90 is a member of the [[Virgo Cluster]],<ref name="binggelietal1985">
{{cite journal
 | author=B. Binggeli | author2=A. Sandage | author3=G. A. Tammann
 | date=1985
 | title=Studies of the Virgo Cluster. II - A catalog of 2096 galaxies in the Virgo Cluster area. V - Luminosity functions of Virgo Cluster galaxies
 | volume=90 | pages=1681–1759
 | bibcode=1985AJ.....90.1681B
 | doi= 10.1086/113874
 | journal=The Astronomical Journal
}}</ref> being one of its largest and brightest spiral galaxies, with an [[absolute magnitude]] of around &minus;22 (brighter than the [[Andromeda Galaxy]]).<ref name=Harris1991/> The galaxy is found about 1.5° from the central subgroup of [[Messier 87]].<ref name="carnegieatlas">
{{cite book
 | author=A. Sandage | author2=J. Bedke
 | date=1994
 | title=Carnegie Atlas of Galaxies
 | publisher=[[Carnegie Institution of Washington]]
 | isbn=978-0-87279-667-6
}}</ref> Due to the galaxy's interaction with the [[intracluster medium]] in its cluster, the galaxy has lost much of its [[interstellar medium]]. As a result of this process, which is referred to as [[ram-pressure stripping]], the medium and [[star formation]] regions appear severely truncated compared to similar galaxies outside the Virgo Cluster<ref name="koopmannkenney2004">
{{cite journal
 | author=R. A. Koopmann | author2=J. D. P. Kenney
 | date=2004
 | title=Hα Morphologies and Environmental Effects in Virgo Cluster Spiral Galaxies
 | journal=[[The Astrophysical Journal]]
 | volume=613
 | issue= 2 | pages=866–885
 | bibcode=2004ApJ...613..866K
 | doi= 10.1086/423191
|arxiv = astro-ph/0406243 | s2cid=17519217
 }}</ref> and there are even [[H II region]]s outside the [[galactic plane]],<ref name="koopmannkenney2004"/> as well as long (up to 80,000-[[parsec]]—that is, 260,000-light-year) tails of ionized gas that has been stripped away.<ref name="bosellietal2016">
{{cite journal
 | author=Boselli, A. | author2=Cuillandre, J. C. | author3=Fossati, M. | author4=Boissier, S. | author5=Bomans, D. | author6=Consolandi, G. | author7=Anselmi, G. | author8=Cortese, L. | author9=Cote, P. | author10=Durrell, P. | author11=Ferrarese, L. | author12=Fumagalli, M. | author13=Gavazzi, G. | author14=Gwyn, S. | author15=Hensler, G. | author16=Sun, M. | author17=Toloba, E.
 | date=2016
 | title=Spectacular tails of ionised gas in the Virgo cluster galaxy NGC 4569
 | journal=[[Astronomy & Astrophysics]]
 | volume=587 | pages=A68 | bibcode=2016A&A...587A..68B
 |arxiv = 1601.04978| doi=10.1051/0004-6361/201527795| s2cid=53841566 | url=http://dro.dur.ac.uk/18073/1/18073.pdf?DDD25+pncg48+dul4eg}}</ref>

== Star formation activity ==
As stated above, the [[star formation]] in Messier 90 appears truncated. Consequently, the galaxy's spiral arms appear to be smooth and featureless, rather than knotted like galaxies with extended star formation,<ref name="koopmannkenney2004"/> which justifies why this galaxy, along with [[NGC 4921]] in the [[Coma Cluster]] has been classified as the prototype of an [[anemic galaxy]].<ref name=Bergh1976>
{{cite journal
 |last1=Bergh |first1=S.
 |date=1976
 |title=A new classification system for galaxies
 |journal=The Astrophysical Journal
 |volume=206 |pages=883–887
 |bibcode=1976ApJ...206..883V
 |doi=10.1086/154452
|doi-access=free
 }}</ref> Some authors go even further and consider it is a [[Anemic galaxy#Passive spiral galaxies|passive spiral galaxy]], similar to those found on galaxy clusters with high [[redshift]].<ref name=Moran2007>
{{cite journal
 |last1=Moran |first1=S. M.
 |display-authors=4
 |last2=Ellis |first2=R. S.
 |last3=Smith |first3=G. P.
 |last4=Rich |first4=R. M.
 |last5=Smail |first5=J.
 |date=2007
 |title=A Wide-Field Survey of Two z ~ 0.5 Galaxy Clusters: Identifying the Physical Processes Responsible for the Observed Transformation of Spirals into S0s
 |journal=The Astrophysical Journal
 |volume=671 |issue=2
 |pages=1503–1522
 |bibcode=2007ApJ...671.1503M
 |doi=10.1086/522303
|arxiv = 0707.4173 |s2cid=14325264
 }}</ref>

However, its center appears to host [[starburst galaxy|significant nebula and star formation]], where around 50,000 stars of spectral types [[O-type star|O]] and [[B-type star|B]] that formed around 5 to 6 million years ago<ref name="gabel2002">
{{cite journal
 | author=Gabel, J. R. | author2=Bruhweiler, F. C.
 | date=2002
 | title=The Central Starburst and Ionization Mechanism in the LINER/H II Region Transition Nucleus in NGC 4569
 | journal=[[The Astronomical Journal]]
 | volume=124
 | issue=2 | pages=737–750
 | bibcode=2002AJ....124..737G
 | doi=10.1086/341376
|arxiv = astro-ph/0204371 | s2cid=119421698
 }}</ref> are set amidst many [[A-type star|A-type]] [[supergiant]]s that were born in earlier starbursts, between 15 and 30 million years ago.<ref name="chyży2006">
{{cite journal
 | author=Chyży, K. T. | display-authors=4 | author2=Soida, M. | author3=Bomans, D. J. | author4=Vollmer, B. | author5=Balkowski, Ch. | author6=Beck, R. | author7=Urbanik, M.
 | date=2006
 | title=Large-scale magnetized outflows from the Virgo Cluster spiral NGC 4569. A galactic wind in a ram pressure wind
 | journal=[[Astronomy & Astrophysics]]
 | volume=447
 | issue=2 | pages=465–472
 | bibcode=2006A&A...447..465C
 | doi=10.1051/0004-6361:20053819
| arxiv=astro-ph/0510392| s2cid=17027396 }}</ref>

Multiple [[supernova]]e (up to 100,000<ref name="chyży2006"/>) in the nucleus have produced 'superwinds' that are blowing the galaxy's interstellar medium outward into the [[intracluster medium]]<ref name="tschokeetal2001">
{{cite journal
 | first1=D. |last1=Tschöke |first2=D. J. |last2=Bomans |first3=G. |last3=Hensler |first4=N. |last4=Junkes
 | date=2001
 | title=Hot halo gas in the Virgo cluster galaxy NGC 4569
 | journal=[[Astronomy & Astrophysics]]
 | volume=380
 | issue=1 | pages=40–54
 | bibcode=2001A&A...380...40T
 | doi=10.1051/0004-6361:20011354
| doi-access=free
 }}</ref> collimated in two jets, one of which is being disturbed by interaction with Virgo's intracluster medium as the galaxy moves through it.<ref name="Kenney2004">
{{cite journal
 | author=Kenney, J. D. P. | author2=Crowl, H. | author3=van Gorkom, J. | author4=Vollmer, B.
 | date=2004
 | title=Spiral Galaxy - ICM Interactions in the Virgo Cluster
 | journal=International Astronomical Union Symposium No. 217
 | volume=217 | pages=370–375
 | bibcode=2004IAUS..217..370K
|arxiv = astro-ph/0403129 | doi=10.1017/S0074180900197979 | s2cid=18764568 }}</ref>

== Blueshift ==
The [[astronomical spectroscopy|spectrum]] of Messier 90 is [[blueshift]]ed, which indicates that, net of [[proper motion|non-aligned vectors of motion]], the gap between it and our galaxy is narrowing.<ref name="ned"/> The spectra of most galaxies are [[redshift]]ed. The blueshift was originally used to argue that Messier 90 was actually an object in the foreground of the Virgo Cluster. However, since the phenomenon was limited mostly to galaxies in the same part of the sky as the Virgo Cluster, it appeared that this inference based on the blueshift was incorrect. Instead, many blueshifts exhibit the large range in velocities of objects within the Virgo Cluster.<ref name="carnegieatlas"/>

== Distance measurements ==
Low levels of [[H I region|H I]] gas prevents using the [[Tully–Fisher relation]] to estimate the distance to Messier 90.<ref name="tschokeetal2001"/>

== Companion galaxies ==
Messier 90 is rich in [[globular cluster]]s, with around 1,000 of them.<ref name="Harris1991">
{{cite web |title=Globular Cluster Systems in Galaxies Beyond the Local Grup. |publisher=NASA-IPAC Extragalactic Database (NED) |url=http://ned.ipac.caltech.edu/level5/Harris/Harris2.html#Table%201 |access-date=2012-07-21}}</ref> The galaxy [[IC 3583]] was once thought to be a [[satellite galaxy|satellite]] of Messier 90;<ref name="chyży2006"/> however, it is now thought they are too far away to be [[interacting galaxies|interacting]] at all.<ref name="bosellietal2016"/>

== Gallery ==
<gallery heights=180 widths=180>
Messier90 - SDSS DR14 (panorama).jpg|[[Messier object|Messier]] 90 imaged by the [[Sloan Digital Sky Survey]]
Messier90 - GALEX.jpg | Messier 90 imaged by [[GALEX]]
</gallery>

==See also==
* [[List of Messier objects]]
*[[Black Eye Galaxy]] (Messier 64), a similar spiral galaxy

== Notes ==
<ol type="a">
<li>{{Note label|A|a|none}}{{Harvnb|Tschöke|Bomans|Hensler|Junkes|2001}} uses a [[Hubble constant]] of 75 (km/s)/Mpc to estimate a distance of 16.8 Mpc to NGC 4569. Adjusting for the 2006 value of 70{{±|2.4|3.2}} (km/s)/Mpc we get a distance of 18.0{{±|0.9|0.6}} Mpc.</li>
</ol>

== References ==
{{Reflist|30em}}

== External links ==
{{commons category}}
* [http://messier.seds.org/m/m090.html SEDS: Spiral Galaxy M90]
* {{WikiSky}}

{{Portal bar|Astronomy|Stars|Outer space}}
{{Catalogs|M=90|UGC=7786|PGC=42089|NGC=4569|Arp=76}}
{{Virgo}}
{{Messier objects}}
{{Ngc50}}

{{Sky|12|36|49.8|+|13|09|46|58700000}}

{{DEFAULTSORT:Messier 090}}
[[Category:Intermediate spiral galaxies]]
[[Category:Virgo Cluster]]
[[Category:Virgo (constellation)]]
[[Category:Messier objects|090]]
[[Category:NGC objects]]
[[Category:UGC objects|07786]]
[[Category:Principal Galaxies Catalogue objects|42089]]
[[Category:Arp objects|076]]
[[Category:Astronomical objects discovered in 1781]]
[[Category:Discoveries by Charles Messier]]