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| {{Galaxybox begin
| | == Nike Free 5.0 V4 i|Also i|In addition == |
| | name = Virgo A
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| {{Galaxybox image
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| | image = [[File:Messier 87 Hubble WikiSky.jpg|250px]]
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| | caption = The Messier 87 galaxy.
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| }}
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| {{Galaxybox observe
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| | epoch = [[Epoch (astronomy)#Julian years and J2000|J2000]]
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| | constell = [[Virgo (constellation)|Virgo]]
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| | ra = {{RA|12|30|49.42338}}<ref name=aaa493_1/>
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| | dec = {{DEC|+12|23|28.0439}}<ref name=aaa493_1/>
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| | appdim_v = 8.3 × 6.6 [[Minute of arc|moa]]<ref name=ned/>
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| | appmag_v = 9.59<ref name=ned/>
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| }}
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| {{Galaxybox character
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| | g_type = E+0-1 pec, NLRG Sy<ref name=ned/>
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| {{Galaxybox astrometry
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| | h_radial_v = 1307
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| | hrv_err = 7<ref name=ned/>
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| | z = 0.004360
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| | z_err = 0.000022<ref name=ned/>
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| | gal_v = 1254
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| | gv_err = 7<ref name=ned/>
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| | g_dist = 53.5
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| | dist_err = 1.63 | |
| | dist_ref = <ref name=aaa524_1/> | |
| }}
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| {{Galaxybox catalog
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| | names = Virgo A, Virgo X-1, [[New General Catalogue|NGC]] 4486, [[Uppsala General Catalogue|UGC]] 7654, [[Principal Galaxies Catalogue|PGC]] 41316, VCC 1316, [[Atlas of Peculiar Galaxies|Arp]] 152, [[Third Cambridge Catalogue of Radio Sources|3C]] 274,<ref name=ned/> 3U 1228+12.<ref name=mnras170/>
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| {{Galaxybox reference
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| | Simbad = M87 Search M87
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| '''Messier 87''' (also known as '''M87''', '''Virgo A''' or '''NGC 4486''') is a supergiant [[elliptical galaxy]]. It was discovered in 1781 by the French astronomer [[Charles Messier]], who cataloged it as a nebulous feature. The second brightest galaxy within the northern [[Virgo Cluster]], it is located about 16.4 million [[parsec]]s (53.5 million [[light-year]]s) from [[Earth]].<ref name=aaa524_1/><ref name=aj94/> Unlike a disk-shaped [[spiral galaxy]], Messier 87 has no distinctive [[dust lanes]] and it has an almost featureless, [[ellipsoid]]al shape that diminishes in luminosity with distance from the center. At the core is a [[supermassive black hole]], which forms the primary component of an [[active galactic nucleus]]. This object is a strong source of multiwavelength radiation, particularly [[radio wave]]s. A jet of energetic [[plasma (physics)|plasma]] originates at the core and extends outward at least {{Convert|1,500|pc|ly|abbr=off|sigfig=1}}.<ref name=apj119/>
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| The [[star]]s in this galaxy form about one sixth of Messier 87's mass. They have a nearly spherically symmetric distribution, while the density of stars decreases with increasing distance from the core. The galactic envelope extends out to a radius of about {{Convert|150|kpc|kly|abbr=on}}, where it has been truncated—possibly by an encounter with another galaxy. Between the stars is a diffuse [[interstellar medium]] of gas that has been chemically enriched by elements emitted from [[Stellar evolution|evolved stars]]. Any dust formed within the galaxy is destroyed within 46 million years by the [[X-ray]] emission from the core, although optical filaments of dust have been observed. Orbiting the galaxy is an abnormally large population of about 12,000 [[globular clusters]], compared to 150-200 globular clusters orbiting the [[Milky Way]].
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| ==Observation history== | | == Jordan Shoes Effexor XR effexor. == |
| In 1781, French astronomer [[Charles Messier]] published a [[Messier object|catalogue]] of 103 objects that had a nebulous appearance. This list was intended to identify objects that might be confused with [[comet]]s. In subsequent use, each item in the catalogue was prefixed with an 'M'. Thus, M87 was the eighty seventh member of Messier's catalogue.<ref name=basu03/> During the 1880s, this nebula was included in the ''[[New General Catalogue]]'' as NGC 4486. This compilation of nebulae and star clusters was assembled by the Danish-Irish astronomer [[John Louis Emil Dreyer|John Dreyer]] based primarily on the observations of English astronomer [[John Herschel]].<ref name=mras49/>
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| In 1918, American astronomer [[Heber Curtis]] of [[Lick Observatory]] observed that there was no spiral structure in Messier 87 and he noticed a "curious straight ray ... apparently connected with the nucleus by a thin line of matter." The ray appeared brightest at the inner end.<ref name=plo13/> The following year, a [[supernova]] within Messier 87 reached a peak [[photographic magnitude]] of 21.5, although this event was not reported until photographic plates were examined by the Russian astronomer [[Innokentii A. Balanowski]] in 1922.<ref name=pasp35_207/><ref name=sa24/>
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| American astronomer [[Edwin Hubble]] categorized Messier 87 as one of the brighter globular nebulae, as it lacked any spiral structure but appeared to belong to the same family of non-galactic nebulae as spiral nebulae.<ref name=apj56/> In 1926 he produced a new categorization of nebulae, with Messier 87 being classified as a type of elliptical extra-galactic nebula with no apparent elongation (class E0).<ref name=apj64/> By 1931, Hubble had identified Messier 87 as a member of the [[Virgo cluster]], for which he gave a provisional estimate of 1.8 million [[parsecs]] from Earth. At the time it was the only known example of an elliptical nebula for which individual stars could be resolved.<ref name=apj74/> Messier 87 continued to be called an extragalactic nebula for many years thereafter, but by 1956 it had been identified as an E0-type galaxy.<ref name=apj124_416/>
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| In 1947, a prominent [[radio astronomy|radio]] source was identified overlapping the location of Messier 87, and this was labeled Virgo-A.<ref name=ajsra3/> This source was confirmed to be Messier 87 by 1953, and the linear [[Relativistic jet|jet]] emerging from the core of this extragalactic nebula was suggested as the cause. This jet extended from the core at a [[position angle]] of 260° to an [[angular distance]] of 20″ with an angular width of 2″.<ref name=apj119/> German-American astronomer [[Walter Baade]] found that the light from this jet is [[plane polarized]], which suggested that the energy was being generated by the acceleration of electrons moving at [[relativistic velocities]] in a [[magnetic field]]. The total energy output of these electrons was estimated as {{nowrap|5 × 10<sup>56</sup> [[Electron volt|eV]]}}.<ref name=observatory76/> In 1969-70, a strong component of the radio emission was found to closely align with the optical source of the jet.<ref name=mnras170/>
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| [[File:Hubble follows spiral flow of black-hole-powered jet.jpg|thumb|Hubble follows spiral flow of black-hole-powered jet.<ref>{{cite news|title=Hubble follows spiral flow of black-hole-powered jet|url=http://www.spacetelescope.org/images/opo1332a/|accessdate=6 September 2013|newspaper=ESA/Hubble Press Release}}</ref> ]]
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| The [[US Naval Research Laboratory]] group launched an [[Aerobee]] 150 during April, 1965 that was equipped with a pair of [[geiger counter]]s.<ref name=HEASARC1965/> This flight discovered seven candidate X-ray sources, including the first extragalactic X-ray source; designated Virgo X-1 as the first X-ray source detected in Virgo.<ref name=charles95/> A later [[Aerobee]] rocket launched from [[White Sands Missile Range]] on July 7, 1967, yielded further evidence that the source Virgo X-1 was the radio galaxy Messier 87.<ref name=bradt68/> Subsequent X-ray observations by the [[HEAO 1]] and [[Einstein Observatory]] showed a complex source that included the [[active galactic nucleus]] of Messier 87.<ref name=apj262/> However, there is little central concentration of the X-ray emission.<ref name=mnras170/>
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| <div style="position: relative; float: right; border: solid #CCCCCC 1px; padding: 4px;">[[File:Virgo constellation map.svg|250px|alt=The location of M87 (upper right) in Virgo]] | | |
| <div style="position: absolute; left: 162px; top: 43px">[[File:Cercle rouge 100%.svg|12px]]</div>
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| <div style="font-size: 90%; ">The location of M87 (upper right) in Virgo</div> | |
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| Messier 87 is located near the high [[declination]] border of the Virgo, next to the constellation of [[Coma Berenices]]. It lies along a line between the stars [[Epsilon Virginis]] and [[Denebola]].<ref name=midway/> At an [[apparent magnitude]] of 9.59, this galaxy can be readily observed using a small telescope with a {{Convert|6|cm|in|abbr=on}} [[aperture]]. Visually, the galaxy extends across an angular area of 7′.2 × 6′.8, with a bright, 45″ core.<ref name=luginbuhl_skiff98/> Viewing the jet feature is a challenge without the aid of photography.<ref name=cooke2005/> Up through 1990, the only known visual observation of the jet had been by Russian-American astronomer [[Otto Struve]] using the {{Convert|254|cm|in|abbr=on}} [[Hooker telescope]].<ref name=clark90/> In recent years, however, it has been observed in larger amateur telescopes under excellent conditions.<ref name=astromall/>
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| In the modified [[Hubble sequence]] [[galaxy morphological classification]] scheme of French astronomer [[Gérard de Vaucouleurs]], Messier 87 is categorized as an E0p galaxy. The E0 designation is used for an [[elliptical galaxy]] that displays no flattening—that is, it appears spherical in profile.<ref name=jass4_1/> A 'p' suffix indicates a [[peculiar galaxy]] that does not fit cleanly into the classification scheme; in this case, the peculiarity is caused by the presence of a [[relativistic jet]] emerging from the core.<ref name=jass4_1/><ref name=jones_lambourne04/> Messier 87 is considered a [[type-cD galaxy]], which is a supergiant D class galaxy.<ref name=aj121_6/><ref name=mnras377_1/> The latter category, first proposed by American astronomer [[William Wilson Morgan|William W. Morgan]] in 1958, is a galaxy that has an elliptical-like nucleus surrounded by an extensive, dustless, diffuse envelope.<ref name=apj209/><ref name=whitmore89/>
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| The distance to Messier 87 has been estimated using several independent techniques. These include measuring the luminosity of [[planetary nebula]]e, comparison with nearby galaxies whose distance has been estimated using [[standard candle]]s such as [[cepheid variable]]s, the linear size distribution of [[globular cluster]]s, and the [[tip of the red giant branch]] method using individually resolved [[red giant]] stars. These measurements are consistent with each other, and their [[weighted average]] yields a distance estimate of {{Convert|16.7|+/-|0.5|Mpc|Mly|abbr=on|sigfig=3}}.<ref name=aaa524_1/>
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| {| class="wikitable" style="float: right; text-align: center; margin-left: 0.5em;"
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| |+ Enclosed mass
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| |- style="background-color: #eeeeee;"
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| | '''Mass'''<br>×10<sup>12</sup> M<sub>☉</sub>
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| | '''Radius'''<br>kpc
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| | 2.4<ref name=apj643_1/> || 32
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| | 3.0<ref name=apj486/> || 44
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| | 5.7<ref name=apj729_2/> || 47
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| |-
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| | 6.0<ref name=apj106_6/> || 50
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| |}
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| This galaxy is one of the most massive in the [[Virgo Supercluster|local Universe]].<ref name=apj729_2/> The mass of Messier 87 within a radius of {{Convert|9|-|40|kpc|kly|abbr=on}} from the core steadily increases roughly [[Proportionality (mathematics)|in proportion]] to ''r''<sup>1.7</sup>, where ''r'' is the radius from the core.<ref name=apj486/> Within a radius of {{Convert|32|kpc|kly|abbr=on}}, the mass is {{nowrap|(2.4 ± 0.6) × 10<sup>12</sup>}} times the [[solar mass|mass of the Sun]],<ref name=apj643_1/> which is double the mass of the [[Milky Way]] galaxy.<ref name=mnras364/> However, only a fraction of this mass is in the form of stars, as Messier 87 has an estimated mass to luminosity ratio of {{nowrap|6.3 ± 0.8}}. That is, about one part in six of the galaxy's mass is in the form of stars that are radiating energy.<ref name="apj700_2_1690"/> The total mass of Messier 87 may be 200 times that of the Milky Way.<ref name=leverington00/>
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| Gas is infalling into the galaxy at the rate of two to three solar masses per year, most of which may be accreted onto the core region.<ref name=aj86/> The extended stellar envelope of this galaxy reaches a radius of about {{Convert|150|kpc|kly|abbr=on}},<ref name=aaa502_3/><ref name=klotz090608/> compared to about {{Convert|100|kpc|kly|abbr=on}} for the Milky Way.<ref name=science287_5450_79/> Beyond that distance the outer edge of the galaxy has been truncated by some means; possibly by an earlier encounter with another galaxy.<ref name=aaa502_3/><ref name=klotz090608/> There is some evidence of linear streams of stars to the northwest of the galaxy, which may have been created by tidal stripping of orbiting galaxies, or by small satellite galaxies falling in toward Messier 87.<ref name=janowiecki10/> as well as a filament of hot, ionized gas in the northeastern outer part of this galaxy that has been proposed to be the remmant of a small, gas-rich galaxy that was disrupted by Messier 87 and that could be feeding its active nucleus.<ref name=aa361_1/>
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| ==Components==
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| [[Image:Supermassiveblackhole nasajpl.jpg|right|thumb|Artist's concept of a supermassive black hole and its [[accretion disk]]]]
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| At the core of this galaxy is a [[supermassive black hole]] (SMBH) with an estimated {{nowrap|(3.5 ± 0.8) × 10<sup>9</sup>}} times the mass of the Sun.<ref name=jwalsh/> This is one of the highest masses known for such an object. Surrounding the black hole is a rotating disk of ionized gas that is oriented roughly perpendicular to a [[relativistic jet]]. This disk is rotating at velocities of up to roughly 1,000 km/s,<ref name=apj489/> and spans a maximum diameter of {{Convert|0.12|pc|ly|abbr=on}}.<ref name=al37_3_154/> Gas is [[Bondi accretion|accreting]] onto the black hole at an estimated rate equal to the mass of the Sun every ten years.<ref name=apj582_1/>
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| Observations suggest that the black hole in M87 may be displaced from the galaxy center by a distance of about {{Convert|25|pc|ly|abbr=on}}.<ref name=apjl717_1_L6/> The displacement is in the opposite direction from the one-sided jet, which may indicate that the black hole has been accelerated away from the center by the jet. Another possibility is that the displacement occurred during the merger of two SMBH.<ref name=apjl717_1_L6/><ref name=sciencenews177_3_9/> However care has to be taken with these findings. The study does not include any spectroscopic discrimination between the stellar and active galactic nucleus component. It is therefore possible that the seeming position of the galaxy center with respect to the black hole is misinterpreted by an optical flare of the jet itself. In 2011, an analysis of M87 did not find any statistically significant displacement.<ref name=gebhardt2011/>
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| Active elliptical galaxies of a form similar to Messier 87 are believed to form as a result of one or more mergers between smaller galaxies.<ref name=dehnen1997/> There is now little dust remaining to form the [[diffuse nebula]]e where new stars are created, so the stellar population is dominated by old, [[population II]] stars that contain relatively low abundances of elements other than hydrogen and helium. The elliptical shape of this galaxy is maintained by random orbital motions of its member stars, in contrast to the more orderly rotational motions found in a [[spiral galaxy]] such as the Milky Way.<ref name=steinicke_jakiel2007/>
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| The space between the stars in the Messier 87 galaxy is filled with a diffuse [[interstellar medium]] of gas, which has been chemically enriched by the elements ejected from stars as they passed beyond the end of their [[main sequence]] lifetime. Carbon and nitrogen is being continuously supplied by intermediate mass stars as they pass through the [[asymptotic giant branch]]. The heavier elements from oxygen to iron are primarily produced by [[supernova]] explosions within the galaxy. About 60% of the abundance of these heavy elements was produced by [[core-collapse supernova]]e, while the remainder came from [[Type Ia supernova]]e. The distribution of these elements suggests that early enrichment was from core-collapse supernovae. However, the contribution from this source was much lower in abundance than in the Milky Way. Type Ia supernovae have provided a continuous contribution to the interstellar medium of Messier 87 throughout the history of the galaxy.<ref name=aaa459_2/>
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| Examination of Messier 87 at far [[infrared]] wavelengths shows an excess emission at wavelengths longer than 25 μm. Normally such emission may be an indication of [[thermal emission]] by warm dust.<ref name=apj655_2_781/> However, in the case of Messier 87, the emission appears to be fully explained by [[synchrotron radiation]] from the jet. Within the galaxy, silicate grains are expected to survive for no more than 46 million years because of the X-ray emission from the core.<ref name=aaa518_1/> This dust may be destroyed by the hostile environment or expelled from the galaxy.<ref name=aaa518_1/> The combined mass of dust in this galaxy is no more than 70,000 times the [[Solar mass|mass of the Sun]].<ref name=aaa518_1/> By comparison, the Milky Way contains about a hundred million (10<sup>8</sup>) solar masses worth of dust.<ref name=jones2004/>
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| Within a {{Convert|4|kpc|kly|abbr=on}} radius of the core, the abundance of elements other than hydrogen and helium—what astronomers term the [[metallicity]]—is about half the abundance in the [[Sun]]. Outside this radius, the abundance of metals steadily decreases with increasing distance from the core.<ref name=aj115_5/> Although this is classified as an elliptical galaxy and therefore lacks the dust lanes of a [[spiral galaxy]], optical filaments have been observed in Messier 87. These filaments have an estimated mass of about 10,000 times the mass of the Sun.<ref name=aj86/> Surrounding the galaxy is an extended corona with hot, low density gas.<ref name=aj115_5/>
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| Messier 87 has an abnormally large population of [[globular cluster]]s. A 2006 survey out to an [[angular distance]] of 25′ from its core estimates that there are {{nowrap|12,000 ± 800 globular clusters}} in orbit around Messier 87, as compared to the [[Milky Way]]'s 150–200.<ref name=mnras373_2/> These clusters are similar in size distribution to the globular clusters of the Milky Way, with most having an effective radius between 1 and 6 parsecs. The size of the Messier 87 clusters shows a gradual increase with distance from the galactic center.<ref name=apj705_1_237/>
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| ==Jet==
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| {{multiple image
| |
| | align = right
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| | direction = vertical
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| | width = 220
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| | image1 = M87 jet.jpg
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| | caption1 = This [[Hubble Space Telescope]] photograph shows the [[Relativistic jet|jet of matter]] ejected from M87 at nearly [[light speed]], as it stretches {{convert|1.5|kpc|kly|abbr=on|sigfig=1}} from the galactic core.
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| | image2 = M87 Super-Volcano.jpg
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| | caption2 = In this [[Chandra X-ray Observatory]] image, cold matter from the Virgo cluster falls toward the core of M87, where it's met by the relativistic jet, producing shock waves in the galaxy's interstellar medium.
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| }}
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| The [[relativistic jet]] of matter emerging from the core extends at least {{convert|1.5|kpc|kly|abbr=on|sigfig=1}} from the nucleus of Messier 87 and is made up of matter ejected from the galaxy by a [[supermassive black hole]]. This jet is highly [[Collimated light|collimated]], appearing constrained to an angle of 60° within {{convert|0.8|pc|ly|abbr=on}} of the core, about 16° at a distance of {{convert|2|pc|ly|abbr=on}} and an angle of 6–7° at a distance of {{convert|12|pc|ly|abbr=on}}.<ref name=Doeleman2012/> The jet's base has the diameter of {{nowrap|5.5 ± 0.4}} Schwarzschild radii. The jet is probably powered by a [[Direct motion|prograde]] accretion disk around a spinning supermassive black hole.<ref name=Doeleman2012>{{cite doi|10.1126/science.1224768}}</ref> It is surrounded by a lower velocity, non-relativistic component. There is evidence of a counter jet, but this feature remains unseen from the Earth due to [[relativistic beaming]].<ref name=apj668_1_L27/><ref name=nature355_804/> The jet is [[precession|precessing]], causing the outflow to form a helical pattern out to a distance of {{Convert|1.6|pc|ly|abbr=on}}.<ref name=al37_3_154/> Lobes of matter from the jet extend out to a distance of {{Convert|77|kpc|kly|abbr=on}}.<ref name=klein1997/>
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| In pictures taken by the [[Hubble Space Telescope]] in 1999, the motion of Messier 87's jet was measured at four to six times the speed of light. This motion may be an optical illusion caused by the relativistic velocity of the jet, and not true [[superluminal motion]]. However, detection of such motion supports the theory that [[quasar]]s, [[BL Lac object]]s and [[radio galaxies]] may all be the same phenomenon, known as [[active galactic nucleus|active galaxies]], viewed from different perspectives.<ref name=apj520_2/><ref name=hubble990106/> It has been proposed Messier 87 could actually be a BL Lacertae object (with a low-luminosity nuclei compared with the brightness of its host galaxy) seen from an unfavorable angle to appreciate the properties of that kind of galaxies.<ref name=arxiv_1997/><ref name=M87_blazar/>
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| Observations made by [[Chandra X-ray Observatory]] indicate the presence of loops and rings in the hot X-ray emitting gas that permeates the cluster and surrounds Messier 87. These loops and rings are generated by pressure waves. The pressure waves are caused by variations in the rate at which material is ejected from the supermassive black hole in jets. The distribution of loops suggests that minor eruptions occur every six million years. One of the rings, caused by a major eruption, is a shock wave {{convert|26|kpc|kly|abbr=on}} in diameter around the black hole. Other features observed include narrow X-ray emitting filaments up to {{convert|31|kpc|kly|abbr=on}} long, and a large cavity in the hot gas caused by a major eruption 70 million years ago. The regular eruptions prevent a huge reservoir of gas from cooling and forming stars, implying that M87’s evolution may have been seriously affected, preventing it from becoming a large [[spiral galaxy]]. The observations also imply the presence of sound waves, 56 octaves below [[middle C]] for the minor eruptions and 58 to 59 below middle C for the major eruptions.<ref name=roy_watzke0610/>
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| Messier 87 is a very strong source of [[gamma rays]], which are the most energetic rays of the electromagnetic spectrum. Gamma rays coming from Messier 87 have been observed since the late 1990s, but in 2006, using the [[HESS]] Cherenkov telescopes, scientists have measured the variations of the gamma ray flux coming from Messier 87, and found that the flux changes over a matter of days. This short period makes the immediate vicinity of the supermassive black hole in Messier 87 the most promising source for these gamma rays.<ref name=cain061027/> In general, the smaller the diameter of the emission source, the faster the variation in flux, and vice versa.
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| A knot of matter in the jet, designated HST-1, has been tracked by the [[Hubble Space Telescope]] and the [[Chandra X-ray Observatory]]. This knot is about {{Convert|65|pc|ly|abbr=on}} from the core. By 2006, the X-ray intensity of this knot had increased by a factor of 50 over a four-year period.<ref name=apj640_1/> This X-ray emission has since been decaying in a variable manner.<ref name=baas41/>
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| ==Cluster membership==
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| [[Image:ESO-M87.jpg|thumb|left|alt=A cluster of galaxies|The Virgo Cluster showing the diffuse light between the galaxies belonging to the cluster. Messier 87 is to lower left.]]
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| This supergiant elliptical galaxy is located near the center of the [[Virgo Cluster]].<ref name=mnras377_1/> This rich cluster has about 2,000 members<ref name=apjss153_1_223/> and it forms the core of the larger [[Virgo Supercluster]], of which the [[Local Group]], and hence the [[Milky Way]] galaxy, is an outlying member.<ref name=aaa502_3/> The cluster is organized into at least three distinct subsystems that are associated with the three galaxies Messier 87, [[Messier 49]] and [[Messier 86]], with the one centered around M87 known as ''Virgo A'' and the one around M49 as ''Virgo B''.<ref name="BinggeliNED">{{cite web
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| |title=VIRGO CLUSTER
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| |publisher=NASA-IPAC Extragalactic Database (NED)
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| |url=http://ned.ipac.caltech.edu/level5/ESSAYS/Binggeli/binggeli.html
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| |accessdate=2012-12-25}}</ref> In terms of mass, Messier 87 is a dominant member of the cluster, and hence appears to be moving very little relative to the cluster as a whole.<ref name=aaa502_3/> Indeed, Messier 87 is defined as the cluster center. The cluster has a sparse gaseous atmosphere that emits X-rays that decrease in temperature toward the middle, where Messier 87 is located.<ref name=apj655_2_781/> The combined mass of the cluster is estimated to be (0.15–1.5) × 10<sup>15</sup> [[solar mass]]es.<ref name=apjss153_1_223/>
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| Measurements of the motion of intracluster [[planetary nebula]]e between Messier 87 and Messier 86 suggest that these two galaxies are moving toward each other and this may be their first encounter. Messier 87 may have encountered [[Messier 84]] in the past, as evidenced by the truncation of the outer halo of the former from tidal effects. However, another possible cause of this truncation is a contraction due to an unseen mass falling into Messier 87 from the rest of the cluster, which, in particular, may be the hypothesized [[dark matter]]. A third possibility is that the halo formation was truncated as a result of early feedback from the active galactic nucleus at the core of Messier 87.<ref name=aaa502_3/>
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| == See also ==
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| * [[NGC 1316]]
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| * [[3C 66B]]
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| * [[Superluminal motion]]
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| | |
| == References ==
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| {{reflist|30em|refs=
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| <ref name=aaa493_1>{{cite journal | author=Lambert, S. B.; Gontier, A.-M. | title=On radio source selection to define a stable celestial frame | journal=Astronomy and Astrophysics | volume=493 | issue=1 | pages=317–323 |date=January 2009 | doi=10.1051/0004-6361:200810582 | bibcode=2009A&A...493..317L }}</ref>
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| <ref name=ned>{{cite web | title=Results for NGC 4486 | work=NASA/IPAC Extragalactic Database | publisher=California Institute of Technology | url=http://nedwww.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=M+87&img_stamp=yes&extend=no | accessdate=2006-10-22}} Select the "By Name" cell, then enter "NGC 4486" in the "Object Name:" field of the query form.</ref>
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| <ref name=apj119>{{cite journal | author=Baade, W.; Minkowski, R. | title=On the Identification of Radio Sources | journal=Astrophysical Journal | year=1954 | volume=119 | pages=215–231 | bibcode=1954ApJ...119..215B | doi=10.1086/145813}}</ref>
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| <ref name=aj94>{{cite journal | author=Binggeli, Bruno; Tammann, G. A.; Sandage, Allan | title=Studies of the Virgo cluster. VI - Morphological and kinematical structure of the Virgo cluster | journal=Astronomical Journal | volume=94 |date=August 1987 | pages=251–277 | doi=10.1086/114467 | bibcode=1987AJ.....94..251B }}</ref>
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| <ref name=apj643_1>{{cite journal | author=Wu, Xiaoan; Tremaine, Scott | title=Deriving the Mass Distribution of M87 from Globular Clusters | journal=The Astrophysical Journal | year=2006 | volume=643 | issue=1 | pages=210–221 | bibcode=2006ApJ...643..210W | doi=10.1086/501515 |arxiv = astro-ph/0508463 }}</ref>
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| <ref name=mnras373_2>{{cite journal | doi=10.1111/j.1365-2966.2006.11067.x | author=Tamura, Naoyuki; Sharples, Ray M.; Arimoto, Nobuo; Onodera, Masato; Ohta, Kouji; Yamada, Yoshihiko | title=A Subaru/Suprime-Cam wide-field survey of globular cluster populations around M87 - I. Observation, data analysis and luminosity function | journal=Monthly Notices of the Royal Astronomical Society | volume=373 | issue=2 | pages=588–600 | year=2006 | bibcode=2006MNRAS.373..588T |arxiv = astro-ph/0609067 }}</ref>
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| <ref name=apj520_2>{{cite journal | author=Biretta, J. A.; Sparks, W. B.; Macchetto, F. | title=Hubble Space Telescope Observations of Superluminal Motion in the M87 Jet | journal=The Astrophysical Journal | volume=520 | issue=2 | pages=621–626 |date=August 1999 | doi=10.1086/307499 | bibcode=1999ApJ...520..621B }}</ref>
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| <ref name=hubble990106>{{cite web | title=Hubble detects faster-than-light motion in Galaxy M87 | first=John | last=Biretta | publisher=Space Telescope Science Institute | location=[[Baltimore, Maryland]] | url=http://www.stsci.edu/ftp/science/m87/press.txt | date=January 6, 1999 | accessdate=2010-12-08 }}</ref>
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| <ref name=cain061027>{{cite news | first=Bernd | last=Wirsing | date=October 26, 2006 | title=Discovery of Gamma Rays from the Edge of a Black Hole | publisher=Max Planck Society | url=http://www.mpg.de/english/illustrationsDocumentation/documentation/pressReleases/2006/pressRelease20061025/ | accessdate=2010-12-03 }}</ref>
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| <ref name=roy_watzke0610>{{cite web | first=Steve | last=Roy | coauthors=Watzke, Megan |date=October 2006 | work=Chandra | title=Chandra Reviews Black Hole Musical: Epic But Off-Key | publisher=Harvard-Smithsonian Center for Astrophysics | url=http://chandra.harvard.edu/press/06_releases/press_100506.html | accessdate=2010-04-25 }}</ref>
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| <ref name=aaa502_3>{{cite journal | author=Doherty, M.; Arnaboldi, M.; Das, P.; Gerhard, O.; Aguerri, J. A. L.; Ciardullo, R.; Feldmeier, J. J.; Freeman, K. C.; Jacoby, G. H.; Murante, G. | title=The edge of the M 87 halo and the kinematics of the diffuse light in the Virgo cluster core | journal=Astronomy and Astrophysics | volume=502 | issue=3 | pages=771–786 |date=August 2009 | doi=10.1051/0004-6361/200811532 | bibcode=2009A&A...502..771D |arxiv = 0905.1958 }}</ref>
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| <ref name=klotz090608>{{cite news | title=Galaxy's Outer Halo Lopped Off | date=June 8, 2009 | first=Irene | last=Klotz | work=Discovery News | url=http://dsc.discovery.com/news/2009/06/08/galaxy-messier-star.html | accessdate=2010-04-25 }}</ref>
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| <ref name=basu03>{{cite journal | first=Baidyanath | last=Basu | title=An Introduction to Astrophysics | page=237 | publisher=PHI Learning Pvt. Ltd. | year=2003 | isbn=81-203-1121-3 }}</ref>
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| <ref name=mras49>{{cite journal | last=Dreyer | first=J. L. E. | year=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=Memoires of the Royal Astronomical Society | volume=49 | pages=1–237 | bibcode=1888MmRAS..49....1D }}</ref>
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| <ref name=plo13>{{cite journal | first=Heber Doust | last=Curtis | year=1918 | title=Descriptions of 762 Nebulae and Clusters Photographed with the Crossley Reflector | journal=Publications of the Lick Observatory | volume=13 | page=31 | url=http://books.google.com/?id=HYnnAAAAMAAJ | accessdate=2010-04-26 | publisher=University of California Press }}</ref>
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| <ref name=apj56>{{cite journal | last=Hubble | first=E. P. | title=A general study of diffuse galactic nebulae | journal=Astrophysical Journal | volume=56 | pages=162–199 |date=October 1922 | doi=10.1086/142698 | bibcode=1922ApJ....56..162H }}</ref>
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| <ref name=apj64>{{cite journal | last=Hubble | first=E. P. | title=Extragalactic nebulae | journal=Astrophysical Journal | volume=64 | pages=321–369 |date=December 1926 | doi=10.1086/143018 | bibcode=1926ApJ....64..321H }}</ref>
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| <ref name=pasp35_207>{{cite journal | title=Messier 87 and Belanowsky's Nova | last=Hubble | first=E. | journal=Publications of the Astronomical Society of the Pacific | volume=35 | issue=207 | page=261 |date=October 1923 | doi=10.1086/123332 | bibcode=1923PASP...35..261H }}</ref>
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| <ref name=sa24>{{cite journal | last=Shklovskii | first=I. S. | year=1980 | title=Supernovae in Multiple Systems | journal=Soviet Astronomy | volume=24 | page=387 | month=August | bibcode=1980SvA....24..387S | unused_data=year=1980 }}</ref>
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| <ref name=apj74>{{cite journal | title=The Velocity-Distance Relation among Extra-Galactic Nebulae | author=Hubble, Edwin; Humason, Milton L. | journal=Astrophysical Journal | volume=74 | page=43 |date=July 1931 | doi=10.1086/143323 | bibcode=1931ApJ....74...43H }}</ref>
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| <ref name=ajsra3>{{cite journal | author=Stanley, G. J.; Slee, O. B. | title=Galactic Radiation at Radio Frequencies. II. The Discrete Sources | journal=Australian Journal of Scientific Research A | volume=3 | page=234 |date=June 1950 | bibcode=1950AuSRA...3..234S | last2=Slee }}</ref>
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| <ref name=observatory76>{{cite journal | author=Baldwin, J. E.; Smith, F. G. | title=Radio emission from the extragalactic nebula M87 | journal=The Observatory | volume=76 | pages=141–144 |date=August 1956 | bibcode=1956Obs....76..141B | last2=Smith }}</ref>
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| <ref name=aj86>{{cite journal | title=A search for neutral hydrogen in D and cD galaxies | author=Burns, J. O.; White, R. A.; Haynes, M. P. | journal=Astronomical Journal | volume=86 | pages=1120–1125 |date=August 1981 | doi=10.1086/112992 | bibcode=1981AJ.....86.1120B }}</ref>
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| <ref name=jass4_1>{{cite journal | author=Park, Kyung-Suk; Chun, Mun-Suk | title=Dynamical Structure of NGC 4486 | journal=Journal of Astronomy and Space Science | volume=4 | issue=1 | pages=35–45 |date=June 1987 | bibcode=1987JASS....4...35P | last2=Chun }}</ref>
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| <ref name=jones_lambourne04>{{cite book | author=Jones, Mark H.; Lambourne, Robert J. | title=An introduction to galaxies and cosmology | publisher=Cambridge University Press | year=2004 | isbn=0-521-54623-0 | page=69 }}</ref>
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| <ref name=aj121_6>{{cite journal | author=Kundu, Arunav; Whitmore, Bradley C. | title=New Insights from HST Studies of Globular Cluster Systems. I. Colors, Distances, and Specific Frequencies of 28 Elliptical Galaxies | journal=The Astronomical Journal | volume=121 | issue=6 | pages=2950–2973 |date=June 2001 | doi=10.1086/321073 | bibcode=2001AJ....121.2950K |arxiv = astro-ph/0103021 }}</ref>
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| <ref name=apj209>{{cite journal | last=Oemler | first=A., Jr. | title=The structure of elliptical and cD galaxies | journal=Astrophysical Journal | volume=209 | pages=693–709 |date=November 1976 | doi=10.1086/154769 | bibcode=1976ApJ...209..693O }}</ref>
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| <ref name=whitmore89>{{cite conference | first=B. C. | last=Whitmore | title=Effect of the Cluster Environment on Galaxies | page=151 | booktitle=Clusters of galaxies: proceedings of the Clusters of Galaxies Meeting, Baltimore, 1989 May 15–17, Volume 1989 | volume=4 | series=Space Telescope Science Institute symposium series | location=Baltimore | date=May 15–17, 1989 | editors=William R. Oegerle, Michael J. Fitchett, Laura Danly | publisher=Cambridge University Press | isbn=0-521-38462-1 }}</ref>
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| | |
| <ref name=midway>Epsilon Virginis is at celestial coordinates α={{RA|13|02}}, δ={{DEC|+10|57}}; Denebola is at α={{RA|11|49}}, δ={{DEC|+14|34}}. The midpoint of the pair is at α={{RA|12|16}}, δ={{DEC|12|45}}. Compare to the
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| coordinates of Messier 87: α={{RA|12|31}}, δ={{DEC|+12|23}}.
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| </ref>
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| <ref name=luginbuhl_skiff98>{{cite book | author=Luginbuhl, Christian B.; Skiff, Brian A. | title=Observing Handbook and Catalogue of Deep-Sky Objects | page=266 | edition=2 | publisher=Cambridge University Press | year=1998 | isbn=0-521-62556-4 }}</ref>
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| <ref name=clark90>{{cite book | first=Roger Nelson | last=Clark | year=1990 | title=Visual astronomy of the deep sky | page=153 | publisher=CUP Archive | isbn=0-521-36155-9 }}</ref>
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| <ref name=charles95>{{cite book | author=Charles, P. A.; Seward, F. D. | title=Exploring the X-ray universe | publisher=Press Syndicate of the University of Cambridge | location=Cambridge, England | year=1995 | page=9 | isbn=0-521-43712-1 }}</ref>
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| <ref name=bradt68>{{cite journal | author=Bradt, H.; Naranan, S.; Rappaport, S.; Spada, G. |title=Celestial Positions of X-Ray Sources in Sagittarius | journal=Astrophysical Journal |date=June 1968 | volume=152 | issue=6 | pages=1005–13 | doi=10.1086/149613 | bibcode=1968ApJ...152.1005B }}</ref>
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| <ref name=apj262>{{cite journal | author=Lea, S. M.; Mushotzky, R.; Holt, S. S. | title=Einstein Observatory solid state spectrometer observations of M87 and the Virgo cluster | journal=Astrophysical Journal, Part 1 | volume=262 | pages=24–32 |date=November 1982 | doi=10.1086/160392 | bibcode=1982ApJ...262...24L }}</ref>
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| <ref name=mnras170>{{cite journal | last=Turland | first=B. D. |date=February 1975 | title=Observations of M87 at 5 GHz with the 5-km telescope | journal=Monthly Notices of the Royal Astronomical Society | volume=170 | pages=281–294 | bibcode=1975MNRAS.170..281T }}</ref>
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| <ref name=apj486>{{cite journal | title=The Dynamics of the M87 Globular Cluster System | author=Cohen, Judith G.; Ryzhov, Anton | journal=Astrophysical Journal | volume=486 | issue=1 | page=230 |date=September 1997 | doi=10.1086/304518 | bibcode=1997ApJ...486..230C |arxiv = astro-ph/9704051 }}</ref>
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| <ref name=janowiecki10>{{cite journal | first=Steven | last=Janowiecki | coauthors=''et al.'' | title=Diffuse Tidal Structures in the Halos of Virgo Ellipticals | journal=The Astrophysical Journal | volume=715 | issue=2 | pages=972–985 |date=June 2010 | bibcode=2010ApJ...715..972J | doi=10.1088/0004-637X/715/2/972 | arxiv=1004.1473 }}</ref>
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| <ref name=apj640_1>{{cite journal | title=The Outburst of HST-1 in the M87 Jet | author=Harris, D. E.; Cheung, C. C.; Biretta, J. A.; Sparks, W. B.; Junor, W.; Perlman, E. S.; Wilson, A. S. | journal=The Astrophysical Journal | volume=640 | issue=1 | pages=211–218 |date=March 2006 | doi=10.1086/500081 | bibcode=2006ApJ...640..211H |arxiv = astro-ph/0511755 }}</ref>
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| <ref name=baas41>{{cite journal | author=Harris, D. E.; Cheung, C. C.; Stawarz, L. | title=Variability Timescales in the M87 Jet: Signatures of E Squared Losses, Discovery of a Quasi-period in HST-1, and the Site of TeV Flaring | journal=Bulletin of the American Astronomical Society | volume=41 | page=393 |date=January 2009 | bibcode=2009AAS...21333207H | arxiv=0904.3925 | last2=Cheung | last3=Stawarz }}</ref>
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| <ref name=mnras377_1>{{cite journal | last=Chakrabarty | first=Dalia | title=Mass modelling with minimum kinematic information | journal=Monthly Notices of the Royal Astronomical Society | volume=377 | issue=1 | pages=30–40 |date=May 2007 | doi=10.1111/j.1365-2966.2007.11583.x | bibcode=2007MNRAS.377...30C |arxiv = astro-ph/0702065 }}</ref>
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| <ref name=apj106_6>{{cite journal | last=Merritt | first=David | authorlink=David Merritt |last2= Tremblay |first2=Benoit | title=The distribution of dark matter in the halo of M87 | journal=The Astronomical Journal | volume=106 | issue=6 | pages=2229–2242 |date=December 1993 | doi=10.1086/116796 | bibcode=1993AJ....106.2229M }}</ref>
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| <ref name=aaa459_2>{{cite journal | author=Werner, N.; Böhringer, H.; Kaastra, J. S.; de Plaa, J.; Simionescu, A.; Vink, J. | title=XMM-Newton high-resolution spectroscopy reveals the chemical evolution of M 87 | journal=Astronomy and Astrophysics | volume=459 | issue=2 | pages=353–360 |date=November 2006 | doi=10.1051/0004-6361:20065678 | bibcode=2006A&A...459..353W |arxiv = astro-ph/0608177 }}</ref>
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| <ref name=aj115_5>{{cite journal | author=Harris, William E.; Harris, Gretchen L. H.; McLaughlin, Dean E. | title=M87, Globular Clusters, and Galactic Winds: Issues in Giant Galaxy Formation | journal=The Astronomical Journal | volume=115 | issue=5 | pages=1801–1822 |date=May 1998 | doi=10.1086/300322 | bibcode=1998AJ....115.1801H |arxiv = astro-ph/9801214 }} The authors give a [[metallicity]] of:
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| :<math>\begin{smallmatrix}\left[\frac{Fe}{H}\right]\ =\ -0.3\end{smallmatrix}</math>
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| within a 3 kpc radius of the galactic core.</ref>
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| <ref name=mnras364>{{cite journal | author=Battaglia, G.; Helmi, A.; Morrison, H.; Harding, P.; Olszewski, E. W.; Mateo, M.; Freeman, K. C.; Norris, J.; Shectman, S. A. | title=The radial velocity dispersion profile of the Galactic halo: Constraining the density profile of the dark halo of the Milky Way | journal=Monthly Notices of the Royal Astronomical Society | year=2005 | volume=364 | pages=433–442 | doi=10.1111/j.1365-2966.2005.09367.x | bibcode=2005MNRAS.364..433B |arxiv = astro-ph/0506102 }}</ref>
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| <ref name=leverington00>{{cite book | first=David | last=Leverington | year=2000 | title=New cosmic horizons: space astronomy from the V2 to the Hubble Space Telescope | page=343 | publisher=Cambridge University Press | isbn=0-521-65833-0 }}</ref>
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| <ref name=apj489>{{cite journal | author=Macchetto, F.; Marconi, A.; [[David Axon|Axon, D. J.]]; Capetti, A.; Sparks, W.; Crane, P. | title=The Supermassive Black Hole of M87 and the Kinematics of Its Associated Gaseous Disk | journal=Astrophysical Journal | volume=489 | issue=2 | page=579 |date=November 1997 | doi=10.1086/304823 | bibcode=1997ApJ...489..579M |arxiv = astro-ph/9706252 }}</ref>
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| <ref name=apj582_1>{{cite journal | author=Di Matteo, Tiziana; Allen, Steven W.; Fabian, Andrew C.; Wilson, Andrew S.; Young, Andrew J. | title=Accretion onto the Supermassive Black Hole in M87 | journal=The Astrophysical Journal | volume=582 | issue=1 | pages=133–140 |date=January 2003 | doi=10.1086/344504 | bibcode=2003ApJ...582..133D |arxiv = astro-ph/0202238 }}</ref>
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| <ref name=jwalsh>{{cite journal | author=Walsh, Jonelle L.; Barth, Aaron J.; Ho, Luis C.; Sarzi, Marc | title=The M87 Black Hole Mass from Gas-dynamical Models of Space Telescope Imaging Spectrograph Observations | journal=The Astrophysical Journal | volume=770 | issue=2 | page=86 |date=June 2013 | doi= 10.1088/0004-637X/770/2/86 | bibcode= 2013ApJ...770...86W |arxiv = 1304.7273 }}</ref>
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| <ref name=sciencenews177_3_9>{{cite journal | first=Ron | last=Cowen | title=Black hole shoved aside, along with 'central' dogma | date=June 19, 2010 | journal=ScienceNews | volume=177 | issue=13 | page=9 | url=http://www.sciencenews.org/view/generic/id/59656/title/Black_hole_shoved_aside,_along_with_central_dogma | accessdate=2010-05-29 }}</ref>
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| <ref name=apjl717_1_L6>{{cite journal | author=Batcheldor, D.; Robinson, A.; Axon, D. J.; Perlman, E. S.; Merritt, D. | title=A Displaced Supermassive Black Hole in M87 | journal=The Astrophysical Journal Letters | volume=717 | issue=1 | pages=L6–L10 |date=July 2010 | doi=10.1088/2041-8205/717/1/L6 | bibcode=2010ApJ...717L...6B | arxiv=1005.2173 }}</ref>
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| <ref name="apj700_2_1690">{{cite journal | author=Gebhardt, Karl; Thomas, Jens | title=The Black Hole Mass, Stellar Mass-to-Light Ratio, and Dark Halo in M87 | journal=The Astrophysical Journal | volume=700 | issue=2 | pages=1690–1701 |date=August 2009 | doi=10.1088/0004-637X/700/2/1690 | bibcode=2009ApJ...700.1690G |arxiv = 0906.1492 }}</ref>
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| <ref name=klein1997>{{cite conference | last=Klein | first=Uli | title=The Large-Scale Structure of Virgo A | booktitle=The radio galaxy Messier 87 | series=Lecture notes in physics | volume=530 | location=Ringberg Castle, Tegernsee, Germany | date=September 15–19, 1997 | editors=Hermann-Josef Röser, Klaus Meisenheimer | publisher=Springer | doi=10.1007/BFb0106418 | bibcode=1999LNP...530...56K }}</ref>
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| <ref name=astromall>{{cite web | title=Visual observations of the M87 jet | work=Adventures in Deep Space | publisher=Astronomy-Mall | url=http://astronomy-mall.com/Adventures.In.Deep.Space/m87jet.htm | accessdate=2010-12-07 }}</ref>
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| <ref name=apj705_1_237>{{cite journal | author=Madrid, Juan P.; Harris, William E.; Blakeslee, John P.; Gómez, Matías | title=Structural Parameters of the Messier 87 Globular | journal=The Astrophysical Journal | volume=705 | issue=1 | pages=237–244 |date=November 2009 | doi=10.1088/0004-637X/705/1/237 | bibcode=2009ApJ...705..237M |arxiv = 0909.0272 }} See Fig. 6. for a plot of the effective cluster radius versus galactocentric distance.</ref>
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| <ref name=aaa518_1>{{cite journal | author=Baes, M. | coauthors=''et al.'' | title=The Herschel Virgo Cluster Survey. VI. The far-infrared view of M 87 | journal=Astronomy and Astrophysics | volume=518 | pages=1–4 |date=July 2010 | doi=10.1051/0004-6361/201014555 | bibcode=2010A&A...518L..53B |arxiv = 1005.3059 }}</ref>
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| <ref name=aaa524_1>{{cite journal | author=Bird, S.; Harris, W. E.; Blakeslee, J. P.; Flynn, C. | title=The inner halo of M 87: a first direct view of the red-giant population | journal=Astronomy and Astrophysics | volume=524 |date=December 2004 | pages=1–11 | doi=10.1051/0004-6361/201014876 | bibcode=2010A&A...524A..71B |arxiv = 1009.3202 }}</ref>
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| <ref name=apjss153_1_223>{{cite journal | author=Côté, Patrick | coauthors=''et al.'' | title=The ACS Virgo Cluster Survey. I. Introduction to the Survey | journal=The Astrophysical Journal Supplement Series | volume=153 | issue=1 | pages=223–242 |date=July 2004 | doi=10.1086/421490 | bibcode=2004ApJS..153..223C |arxiv = astro-ph/0404138 }}</ref>
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| <ref name=apj668_1_L27>{{cite journal | author=Kovalev, Y. Y.; Lister, M. L.; Homan, D. C.; Kellermann, K. I. | title=The Inner Jet of the Radio Galaxy M87 | journal=The Astrophysical Journal | volume=668 | issue=1 | pages=L27–L30 |date=October 2007 | doi=10.1086/522603 | bibcode=2007ApJ...668L..27K |arxiv = 0708.2695 }}</ref>
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| <ref name=apj124_416>{{cite journal | last=Burbidge | first=G. R. | title=On Synchrotron Radiation from Messier 87 | journal=The Astrophysical Journal | volume=124 | pages=416 |date=September 1956 | doi=10.1086/146237 | bibcode=1956ApJ...124..416B }}</ref>
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| <ref name=nature355_804>{{cite journal | title=A counterjet in the elliptical galaxy M87 | author=Sparks, William B.; Fraix-Burnet, D.; Macchetto, F.; Owen, F. N. | journal=Nature | volume=355 | issue=6363 | date=February 27, 1992 | pages=804–806 | doi=10.1038/355804a0 | bibcode=1992Natur.355..804S }}</ref>
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| <ref name=cooke2005>{{cite book | first=Antony | last=Cooke | year=2005 | title=Visual astronomy under dark skies: a new approach to observing deep space | pages=5–37 | series=Patrick Moore's practical astronomy series | publisher=Springer-Verlag | location=London | isbn=1-85233-901-2 }}</ref>
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| <ref name=science287_5450_79>{{cite journal | author=Bland-Hawthorn, Joss; Freeman, Ken | title=The Baryon Halo of the Milky Way: A Fossil Record of Its Formation | journal=Science | date=January 7, 2000 | volume=287 | issue=5450 | pmid=10615053 | pages=79–84 | doi=10.1126/science.287.5450.79
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| |bibcode = 2000Sci...287...79B }}</ref>
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| <ref name=aaa518_1>{{cite journal | author=Clemens, M. S. | coauthors=''et al.'' | title=The Herschel Virgo Cluster Survey. III. A constraint on dust grain lifetime in early-type galaxies | journal=Astronomy and Astrophysics | volume=518 |date=July 2010 | pages=1–4 | doi=10.1051/0004-6361/201014533 | bibcode=2010A&A...518L..50C |arxiv = 1005.3056 }}</ref>
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| <ref name=jones2004>{{cite book | author=Jones, Mark H.; Lambourne, Robert J.; Adams, David John | title=An introduction to galaxies and cosmology | page=13 | publisher=Cambridge University Press | year=2004 | isbn=0-521-54623-0 }}</ref>
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| <ref name=dehnen1997>{{cite conference | last=Dehnen | first=Walter | title=M 87 as a Galaxy | booktitle=The radio galaxy Messier 87: proceedings of a workshop | location=Ringberg Castle, Tegernsee, Germany | date=September 15–19, 1997 | editors=Hermann-Josef Röser, Klaus Meisenheimer | publisher=Springer | page=31 | doi=10.1007/BFb0106415 | bibcode=1999LNP...530...31D }}</ref>
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| <ref name=steinicke_jakiel2007>{{cite book | author=Steinicke, Wolfgang; Jakiel, Richard | title=Galaxies and how to observe them | year=2007 | series=Astronomers' observing guides | pages=32–33 | isbn=1-85233-752-4 | publisher=Springer }}</ref>
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| <ref name=gebhardt2011>{{cite journal | first=Karl | last=Gehbardt| coauthors=''et al.'' | title=The Black-Hole Mass in M87 from Gemini/NIFS Adaptive Optics Observations | journal=The Astrophysical Journal | volume=(accepted) | year=2011 | arxiv=1101.1954 |bibcode = 2011ApJ...729..119G |doi = 10.1088/0004-637X/729/2/119 | issue=2 | pages=119 }}</ref>
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| <ref name=HEASARC1965>{{Cite journal | first=Stephen A. | last1=Drake | title=A Brief History of High-Energy Astronomy: 1965 - 1969 | publisher=NASA HEASARC | url=http://heasarc.nasa.gov/docs/heasarc/headates/1965.html | accessdate=2011-10-28 | postscript=<!-- Bot inserted parameter. Either remove it; or change its value to "." for the cite to end in a ".", as necessary. -->{{inconsistent citations}} }}</ref>
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| <ref name=apj729_2>{{Cite journal | last1=Murphy | first1=Jeremy D. | last2=Gebhardt | first2=Karl | last3=Adams | first3=Joshua J. | title=Galaxy Kinematics with VIRUS-P: The Dark Matter Halo of M87 | journal=The Astrophysical Journal | volume=729 | issue=2 |date=March 2011 | doi=10.1088/0004-637X/729/2/129 | bibcode=2011ApJ...729..129M | pages=129 | postscript=<!-- Bot inserted parameter. Either remove it; or change its value to "." for the cite to end in a ".", as necessary. -->{{inconsistent citations}} |arxiv = 1101.1957 }}</ref>
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| <ref name=al37_3_154>{{Cite journal | last1=Matveyenko | first1=L. I. | last2=Seleznev | first2=S. V. | title=Fine core-jet structure of the galaxy M87 | journal=Astronomy Letters | volume=37 | issue=3 | pages=154–170 |date=March 2011 | doi=10.1134/S1063773711030030 | bibcode=2011AstL...37..154M | postscript=<!-- Bot inserted parameter. Either remove it; or change its value to "." for the cite to end in a ".", as necessary. -->{{inconsistent citations}} }}</ref>
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| <ref name=apj655_2_781>{{Cite journal | display-authors=1 | last1=Shi | first1=Y. | last2=Rieke | first2=G. H. | last3=Hines | first3=D. C. | last4=Gordon | first4=K. D. | last5=Egami | first5=E. | title=Thermal and Nonthermal Infrared Emission from M87 | journal=The Astrophysical Journal | volume=655 | issue=2 | pages=781–789 |date=February 2007 | doi=10.1086/510188 | bibcode=2007ApJ...655..781S | postscript=<!-- Bot inserted parameter. Either remove it; or change its value to "." for the cite to end in a ".", as necessary. -->{{inconsistent citations}} |arxiv = astro-ph/0610494 }}</ref>
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| <ref name=aa361_1>{{Cite journal | last1=Gavazzi | first1=G. | last2=Boselli | first2=A. | last3=Vílchez | first3=J. M. | last4=Iglesias-Paramo | first4=J. | last5=Bonfanti | first5=C. | title=The filament of ionized gas in the outskirt of M87 | journal=Astronomy & Astrophysics | volume=361 |date=September 2000 | bibcode=2000A&A...361....1G | pages=1–4|arxiv = astro-ph/0007323 }}</ref>
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| <ref name=M87_blazar>{{Cite journal | display-authors=1 | last1=Reimer | first1=A. | last2=Protheroe | first2=R. J. | last3=Donea | first3=A. .-C. | title=M87 as a Misaligned Synchrotron-Proton Blazar | journal=Proceedings of the 28th International Cosmic Ray Conference. | pages=2631 |date=July 2003 | bibcode=2003ICRC....5.2631R}}</ref>
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| <ref name=arxiv_1997>{{Cite journal | last1=Tsvetanov | first1=Zlatan I. | last2=Hartig | first2=George F. | last3=Ford | first3=Holland C. | last4=Dopita | first4=Michael A. | last5=Kriss | first5=Gerard A. | last6=Pei | first6=Yichuan C. | last7=Dressel | first7=Linda L. | last8=Harms | first8=Richard J. | title=M87: A Misaligned BL LAC? | journal=arXiv |date=November 1997 | arxiv= astro-ph/9711241|bibcode = 1997astro.ph.11241T }}</ref>
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| == External links ==
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| {{commons-inline|Messier 87|Messier 87}}
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| *[http://www.seds.org/messier/m/m087.html Messier 87], SEDS Messier pages
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| *[http://www.spacetelescope.org/news/html/heic0204.html ESA/Hubble News Release]
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| *[http://www.spacetelescope.org/images/archive/freesearch/m87/viewall/1 ESA/Hubble images of M87]
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| *[http://astro.neutral.org/imagehtml/20060304_m87.html Amateur Images of M87 Jet]
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| *[http://www.starshadows.com/gallery/display.cfm?imgID=284 Another amateur image showing M87 jet and M87 globulars]
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| *{{WikiSky}}
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| {{Sky|12|30|49.4|+|12|23|28|55000000}}
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| {{Virgo}}
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| {{Messier objects}}
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| {{Ngc45}}
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| {{good article}}
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| [[Category:Elliptical galaxies|Messier 087]]
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| [[Category:Peculiar galaxies|Messier 087]]
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| [[Category:Radio galaxies|Messier 087]]
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| [[Category:Virgo Cluster|Messier 087]]
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| [[Category:Virgo (constellation)|Messier 087]]
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| [[Category:Messier objects|087]]
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| [[Category:NGC objects|Messier 087]]
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| [[Category:UGC objects|07654]]
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| [[Category:PGC objects|41316]]
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| [[Category:Arp objects|152]]
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| [[Category:3C objects|274]]
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