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Coordinates: Sky map 12h 36m 49.8s, +13° 09′ 46″
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{{Short description|Galaxy in the constellation Virgo}}
{{Use dmy dates|date=April 2012}}
{{Use dmy dates|date=June 2021}}
{{Galaxybox begin
{{Infobox galaxy
| name = [[Messier object|Messier]] 90
| name = [[Messier object|Messier]] 90
| image = [[File:Messier 90 - HST.png|300px]]
}}
| caption = Messier 90 taken by [[Hubble Space Telescope|Hubble]]
{{Galaxybox image
| image = [[File:Messier90 - SDSS DR14 (panorama).jpg|250px]]
⚫
| caption = [[Messier object|Messier]] 90 imaged by the [[Sloan Digital Sky Survey]]
}}
{{Galaxybox observe
| epoch = [[J2000]]
| epoch = [[J2000]]
| constell = [[Virgo (constellation)|Virgo]]<ref name="sinnott1988">
| constellation name = [[Virgo (constellation)|Virgo]]<ref name="sinnott1988">
{{cite book
{{cite book
| editor=R. W. Sinnott
| editor=R. W. Sinnott
Line 22: Line 19:
| work=Results for NGC 4569
| work=Results for NGC 4569
| url=http://nedwww.ipac.caltech.edu/
| url=http://nedwww.ipac.caltech.edu/
| accessdate=2006-02-01
| access-date=2006-02-01
}}</ref>
}}</ref>
| dec = {{DEC|+13|09|46}}<ref name="ned" />
| dec = {{DEC|+13|09|46}}<ref name="ned"/>
| appdim_v = 9.5 × 4.4 [[Minute of arc|moa]]<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>
| appmag_v = 10.26<ref name="ned" />
⚫
| 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]
}}
}}
{{Galaxybox character
⚫
| g_type = SAB(rs)ab,<ref name="ned" /> [[LINER]],<ref name="ned" /> Sy<ref name="ned" />
}}
{{Galaxybox astrometry
| h_radial_v = −235
⚫
| hrv_err = 4<ref name="ned" />
| z = -0.000784
⚫
| z_err = 0.000013<ref name="ned" />
| gal_v = −282
⚫
| gv_err = 4<ref name="ned" />
| g_dist = 58.7
| dist_err = 2.8
}}
{{Galaxybox catalog
⚫
| 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" />
}}
{{Galaxybox reference
| Simbad = M90 Search M90
}}
{{Galaxybox end}}


'''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">
'''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">
Line 68: Line 52:
| doi= 10.1086/113874
| doi= 10.1086/113874
| journal=The Astronomical Journal
| journal=The Astronomical Journal
}}</ref> being one of its largest and brightest spiral galaxies, with an [[absolute magnitude]] of around -22 (brighter than the [[Andromeda Galaxy]]).<ref name=Harris1991/> The galaxy is located approximately 1°.5 away from the subgroup centered on [[Messier 87]].<ref name="carnegieatlas">
}}</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
{{cite book
| author=A. Sandage | author2=J. Bedke
| author=A. Sandage | author2=J. Bedke
Line 75: Line 59:
| publisher=[[Carnegie Institution of Washington]]
| publisher=[[Carnegie Institution of Washington]]
| isbn=978-0-87279-667-6
| isbn=978-0-87279-667-6
}}</ref> As a consequence of the galaxy's interaction with the [[intracluster medium]] in the Virgo 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 galaxy's interstellar medium and [[star formation|star formation region]]s appear severely truncated compared to similar galaxies outside the Virgo Cluster<ref name="koopmannkenney2004">
}}</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
{{cite journal
| author=R. A. Koopmann | author2=J. D. P. Kenney
| author=R. A. Koopmann | author2=J. D. P. Kenney
| date=2004
| date=2004
| title=Hα Morphologies and Environmental Effects in Virgo Cluster Spiral Galaxies
| title=Hα Morphologies and Environmental Effects in Virgo Cluster Spiral Galaxies
| journal=[[Astrophysical Journal]]
| journal=[[The Astrophysical Journal]]
| volume=613
| volume=613
| issue= 2 | pages=866–885
| issue= 2 | pages=866–885
| bibcode=2004ApJ...613..866K
| bibcode=2004ApJ...613..866K
| doi= 10.1086/423191
| doi= 10.1086/423191
|arxiv = astro-ph/0406243 }}</ref> and there are even [[H II region]]s outside the [[galactic plane]],<ref name="koopmannkenney2004" /> as well as long (up to 80 k[[parsec|pc]]s, 260,000 light-years) tails of ionized gas that has been stripped of M90.<ref name="bosellietal2016">
|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
{{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.
| 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
| date=2016
| title=Spectacular tails of ionised gas in the Virgo cluster galaxy NGC 4569
| title=Spectacular tails of ionised gas in the Virgo cluster galaxy NGC 4569
| journal=[[Astronomy and Astrophysics]]
| journal=[[Astronomy & Astrophysics]]
| volume=587 | pages=A68 | bibcode=2016A&A...587A..68B
| volume=587 | pages=A68 | bibcode=2016A&A...587A..68B
|arxiv = 1601.04978| doi=10.1051/0004-6361/201527795| url=http://dro.dur.ac.uk/18073/1/18073.pdf?DDD25+pncg48+dul4eg}}</ref>
|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 ==
== 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>
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
{{cite journal
|last1=Bergh |first1=S.
|last1=Bergh |first1=S.
|date=1976
|date=1976
|title=A new classification system for galaxies
|title=A new classification system for galaxies
|journal=The Astrophysical Journal
|journal=The Astrophysical Journal
|volume=206 |pages=883–887
|volume=206 |pages=883–887
|bibcode=1976ApJ...206..883V
|bibcode=1976ApJ...206..883V
|doi=10.1086/154452
|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>
}}</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
{{cite journal
|last1=Moran |first1=S. M.
|last1=Moran |first1=S. M.
Line 114: Line 100:
|date=2007
|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
|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
|journal=The Astrophysical Journal
|volume=671 |issue=2
|volume=671 |issue=2
|pages=1503–1522
|pages=1503–1522
|bibcode=2007ApJ...671.1503M
|bibcode=2007ApJ...671.1503M
|doi=10.1086/522303
|doi=10.1086/522303
|arxiv = 0707.4173 }}</ref>
|arxiv = 0707.4173 |s2cid=14325264
}}</ref>


However, the center of Messier 90 appears to be a site of [[starburst galaxy|significant star formation activity]], where around 5*10<sup>4</sup> stars of spectral types [[O-type star|O]] and [[B-type star|B]] that formed around 5-6 million years ago<ref name="gabel2002">
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
{{cite journal
| author=Gabel, J. R. | author2=Bruhweiler, F. C.
| author=Gabel, J. R. | author2=Bruhweiler, F. C.
Line 131: Line 118:
| bibcode=2002AJ....124..737G
| bibcode=2002AJ....124..737G
| doi=10.1086/341376
| doi=10.1086/341376
|arxiv = astro-ph/0204371 }}</ref> are surrounded by a large amount of [[A-type star|A-type]] [[supergiant]]s that were born in other starburst that took place before the former, between 15 and 30 million years ago.<ref name="chyży2006">
|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
{{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.
| 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.
Line 141: Line 129:
| bibcode=2006A&A...447..465C
| bibcode=2006A&A...447..465C
| doi=10.1051/0004-6361:20053819
| doi=10.1051/0004-6361:20053819
| arxiv=astro-ph/0510392}}</ref>
| arxiv=astro-ph/0510392| s2cid=17027396 }}</ref>


Multiple [[supernovae]] (up to 10<sup>5</sup><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">
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
{{cite journal
| author=D. Tschöke | author2=D. J. Bomans | author3=G. Hensler | author4=N. Junkes
| first1=D. |last1=Tschöke |first2=D. J. |last2=Bomans |first3=G. |last3=Hensler |first4=N. |last4=Junkes
| date=2001
| date=2001
| title=Hot halo gas in the Virgo cluster galaxy NGC 4569
| title=Hot halo gas in the Virgo cluster galaxy NGC 4569
| journal=[[Astronomy and Astrophysics]]
| journal=[[Astronomy & Astrophysics]]
| volume=380
| volume=380
| issue=1 | pages=40–54
| issue=1 | pages=40–54
| bibcode=2001A&A...380...40T
| bibcode=2001A&A...380...40T
| doi=10.1051/0004-6361:20011354
| 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">
}}</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
{{cite journal
| author=Kenney, J. D. P. | author2=Crowl, H. | author3=van Gorkom, J. | author4=Vollmer, B.
| author=Kenney, J. D. P. | author2=Crowl, H. | author3=van Gorkom, J. | author4=Vollmer, B.
Line 161: Line 150:
| volume=217 | pages=370–375
| volume=217 | pages=370–375
| bibcode=2004IAUS..217..370K
| bibcode=2004IAUS..217..370K
|arxiv = astro-ph/0403129 | doi=10.1017/S0074180900197979 }}</ref>
|arxiv = astro-ph/0403129 | doi=10.1017/S0074180900197979 | s2cid=18764568 }}</ref>


== Blueshift ==
== Blueshift ==
The [[astronomical spectroscopy|spectrum]] of Messier 90 is [[blueshift]]ed, which indicates that it is moving towards the Earth.<ref name="ned" /> In contrast, the spectra of most other 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, the blueshift is thought to be evidence for the large range in velocities of objects within the Virgo Cluster itself.<ref name="carnegieatlas" />
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 ==
== Distance measurements ==
Low levels of [[H I]] gas prevents using the [[Tully-Fisher relation]] to estimate the distance to Messier 90.<ref name="tschokeetal2001" />
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 ==
== Companion galaxies ==
Messier 90 is rich in [[globular cluster]]s, with around 1,000 of them<ref name="Harris1991">{{cite web
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"/>
|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
|accessdate=2012-07-21}}</ref> and has a [[satellite galaxy]] ([[IC 3583]]), which is an [[irregular galaxy]]{{Citation needed|date=February 2007}}; both galaxies were thought to be [[interacting galaxies|interacting]],<ref name="chyży2006" /> however it is now thought they are too far away to be interacting at all.<ref name="bosellietal2016" />


== Gallery ==
== Gallery ==
<gallery>
<gallery heights=180 widths=180>
⚫
Messier90 - SDSS DR14 (panorama).jpg|[[Messier object|Messier]] 90 imaged by the [[Sloan Digital Sky Survey]]
Come a little closer Messier 90.jpg|Messier 90 taken by [[Hubble Space Telescope|Hubble]].<ref>{{cite web |title=Come a little closer |url=https://www.spacetelescope.org/images/potw1920a/ |website=www.spacetelescope.org |accessdate=20 May 2019 |language=en}}</ref>
Messier90 - GALEX.jpg | Messier 90 imaged by [[GALEX]]
</gallery>
</gallery>


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


== Notes ==
== Notes ==
<ol type="a">
<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>
<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>
</ol>


Line 193: Line 181:


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


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

Latest revision as of 00:04, 13 March 2024

Messier 90
Messier 90 taken by Hubble
Observation data (J2000 epoch)
ConstellationVirgo[1]
Right ascension12h 36m 49.8s[2]
Declination+13° 09′ 46″[2]
Redshift−0.000784±0.000013[2]
Heliocentric radial velocity−235±4 km/s[2]
Galactocentric velocity−282±4 km/s[2]
Distance58.7 ± 2.8 Mly (18.00 ± 0.86 Mpc)
Apparent magnitude (V)9.5[3]
Characteristics
TypeSAB(rs)ab,[2] LINER,[2] Sy[2]
Apparent size (V)9.5 × 4.4 moa[2]
Other designations
NGC 4569,[2] UGC 7786,[2] PGC 42089,[2] Arp 76[2]
References: SIMBAD: 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-years away[a] in the constellation Virgo. It was discovered by Charles Messier in 1781.[4]

Membership of the Virgo Cluster

[edit]

Messier 90 is a member of the Virgo Cluster,[5] being one of its largest and brightest spiral galaxies, with an absolute magnitude of around −22 (brighter than the Andromeda Galaxy).[6] The galaxy is found about 1.5° from the central subgroup of Messier 87.[7] 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[8] and there are even H II regions outside the galactic plane,[8] as well as long (up to 80,000-parsec—that is, 260,000-light-year) tails of ionized gas that has been stripped away.[9]

Star formation activity

[edit]

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,[8] which justifies why this galaxy, along with NGC 4921 in the Coma Cluster has been classified as the prototype of an anemic galaxy.[10] Some authors go even further and consider it is a passive spiral galaxy, similar to those found on galaxy clusters with high redshift.[11]

However, its center appears to host significant nebula and star formation, where around 50,000 stars of spectral types O and B that formed around 5 to 6 million years ago[12] are set amidst many A-type supergiants that were born in earlier starbursts, between 15 and 30 million years ago.[13]

Multiple supernovae (up to 100,000[13]) in the nucleus have produced 'superwinds' that are blowing the galaxy's interstellar medium outward into the intracluster medium[14] collimated in two jets, one of which is being disturbed by interaction with Virgo's intracluster medium as the galaxy moves through it.[15]

Blueshift

[edit]

The spectrum of Messier 90 is blueshifted, which indicates that, net of non-aligned vectors of motion, the gap between it and our galaxy is narrowing.[2] The spectra of most galaxies are redshifted. 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.[7]

Distance measurements

[edit]

Low levels of H I gas prevents using the Tully–Fisher relation to estimate the distance to Messier 90.[14]

Companion galaxies

[edit]

Messier 90 is rich in globular clusters, with around 1,000 of them.[6] The galaxy IC 3583 was once thought to be a satellite of Messier 90;[13] however, it is now thought they are too far away to be interacting at all.[9]

[edit]

See also

[edit]

Notes

[edit]
  1. ^ Tschöke et al. 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.

References

[edit]
  1. ^ R. W. Sinnott, ed. (1988). The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer. Sky Publishing Corporation/Cambridge University Press. ISBN 978-0-933346-51-2.
  2. ^ a b c d e f g h i j k l m n "NASA/IPAC Extragalactic Database". Results for NGC 4569. Retrieved 1 February 2006.
  3. ^ "Messier 90". SEDS Messier Catalog. Retrieved 30 April 2022.
  4. ^ K. G. Jones (1991). Messier's Nebulae and Star Clusters (2nd ed.). Cambridge University Press. ISBN 978-0-521-37079-0.
  5. ^ B. Binggeli; A. Sandage; G. A. Tammann (1985). "Studies of the Virgo Cluster. II - A catalog of 2096 galaxies in the Virgo Cluster area. V - Luminosity functions of Virgo Cluster galaxies". The Astronomical Journal. 90: 1681–1759. Bibcode:1985AJ.....90.1681B. doi:10.1086/113874.
  6. ^ a b "Globular Cluster Systems in Galaxies Beyond the Local Grup". NASA-IPAC Extragalactic Database (NED). Retrieved 21 July 2012.
  7. ^ a b A. Sandage; J. Bedke (1994). Carnegie Atlas of Galaxies. Carnegie Institution of Washington. ISBN 978-0-87279-667-6.
  8. ^ a b c R. A. Koopmann; J. D. P. Kenney (2004). "Hα Morphologies and Environmental Effects in Virgo Cluster Spiral Galaxies". The Astrophysical Journal. 613 (2): 866–885. arXiv:astro-ph/0406243. Bibcode:2004ApJ...613..866K. doi:10.1086/423191. S2CID 17519217.
  9. ^ a b Boselli, A.; Cuillandre, J. C.; Fossati, M.; Boissier, S.; Bomans, D.; Consolandi, G.; Anselmi, G.; Cortese, L.; Cote, P.; Durrell, P.; Ferrarese, L.; Fumagalli, M.; Gavazzi, G.; Gwyn, S.; Hensler, G.; Sun, M.; Toloba, E. (2016). "Spectacular tails of ionised gas in the Virgo cluster galaxy NGC 4569" (PDF). Astronomy & Astrophysics. 587: A68. arXiv:1601.04978. Bibcode:2016A&A...587A..68B. doi:10.1051/0004-6361/201527795. S2CID 53841566.
  10. ^ Bergh, S. (1976). "A new classification system for galaxies". The Astrophysical Journal. 206: 883–887. Bibcode:1976ApJ...206..883V. doi:10.1086/154452.
  11. ^ Moran, S. M.; Ellis, R. S.; Smith, G. P.; Rich, R. M.; et al. (2007). "A Wide-Field Survey of Two z ~ 0.5 Galaxy Clusters: Identifying the Physical Processes Responsible for the Observed Transformation of Spirals into S0s". The Astrophysical Journal. 671 (2): 1503–1522. arXiv:0707.4173. Bibcode:2007ApJ...671.1503M. doi:10.1086/522303. S2CID 14325264.
  12. ^ Gabel, J. R.; Bruhweiler, F. C. (2002). "The Central Starburst and Ionization Mechanism in the LINER/H II Region Transition Nucleus in NGC 4569". The Astronomical Journal. 124 (2): 737–750. arXiv:astro-ph/0204371. Bibcode:2002AJ....124..737G. doi:10.1086/341376. S2CID 119421698.
  13. ^ a b c Chyży, K. T.; Soida, M.; Bomans, D. J.; Vollmer, B.; et al. (2006). "Large-scale magnetized outflows from the Virgo Cluster spiral NGC 4569. A galactic wind in a ram pressure wind". Astronomy & Astrophysics. 447 (2): 465–472. arXiv:astro-ph/0510392. Bibcode:2006A&A...447..465C. doi:10.1051/0004-6361:20053819. S2CID 17027396.
  14. ^ a b Tschöke, D.; Bomans, D. J.; Hensler, G.; Junkes, N. (2001). "Hot halo gas in the Virgo cluster galaxy NGC 4569". Astronomy & Astrophysics. 380 (1): 40–54. Bibcode:2001A&A...380...40T. doi:10.1051/0004-6361:20011354.
  15. ^ Kenney, J. D. P.; Crowl, H.; van Gorkom, J.; Vollmer, B. (2004). "Spiral Galaxy - ICM Interactions in the Virgo Cluster". International Astronomical Union Symposium No. 217. 217: 370–375. arXiv:astro-ph/0403129. Bibcode:2004IAUS..217..370K. doi:10.1017/S0074180900197979. S2CID 18764568.
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