Andromeda Galaxy
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The Andromeda Galaxy is a barred spiral galaxy and is the nearest major galaxy to the Milky Way. It was originally named the Andromeda Nebula and is cataloged as Messier 31, M31, and NGC 224. Andromeda has a D25 isophotal diameter of about Template:Convert<ref name=RC3/> and is approximately Template:Convert from Earth. The galaxy's name stems from the area of Earth's sky in which it appears, the constellation of Andromeda, which itself is named after the princess who was the wife of Perseus in Greek mythology.<ref name="RC3"/>
The virial mass of the Andromeda Galaxy is of the same order of magnitude as that of the Milky Way, at Template:Convert. The mass of either galaxy is difficult to estimate with any accuracy, but it was long thought that the Andromeda Galaxy was more massive than the Milky Way by a margin of some 25% to 50%.<ref name="Kafle2018"/> However, this has been called into question by early-21st-century studies indicating a possibly lower mass for the Andromeda Galaxy<ref name="Kafle2018"/> and a higher mass for the Milky Way.<ref>Template:Cite journal</ref><ref name="As-Now"/> The Andromeda Galaxy has a diameter of about Template:Cvt, making it the largest member of the Local Group of galaxies in terms of extension.<ref name="As-Now"/>
The Milky Way and Andromeda galaxies are expected to collide with each other in around 4–5 billion years,<ref name="Schiavi"/> merging to potentially form a giant elliptical galaxy<ref name="milky-way-collide"/> or a large lenticular galaxy.<ref name="Ueda2014"/>
With an apparent magnitude of 3.4, the Andromeda Galaxy is among the brightest of the Messier objects,<ref name="Frommert & Kronberg 2007"/> and is visible to the naked eye from Earth on moonless nights,<ref name="Messie"/> even when viewed from areas with moderate light pollution.<ref name="RC3"/>
Observation historyEdit
The Andromeda Galaxy is visible to the naked eye in dark skies.<ref name="firstName"/> Around the year 964 CE, the Persian astronomer Abd al-Rahman al-Sufi described the Andromeda Galaxy in his Book of Fixed Stars as a "nebulous smear" or "small cloud".<ref name="Hafez"/> Star charts of that period labeled it as the Little Cloud.<ref name="NSOG"/> In 1612, the German astronomer Simon Marius gave an early description of the Andromeda Galaxy based on telescopic observations.<ref name="Aati"/> Pierre Louis Maupertuis conjectured in 1745 that the blurry spot was an island universe.<ref name="Kant"/> Charles Messier cataloged Andromeda as object M31 in 1764 and incorrectly credited Marius as the discoverer despite it being visible to the naked eye. In 1785, the astronomer William Herschel noted a faint reddish hue in the core region of Andromeda.<ref name="Messie"/> He believed Andromeda to be the nearest of all the "great nebulae," and based on the color and magnitude of the nebula, he incorrectly guessed that it was no more than 2,000 times the distance of Sirius, or roughly Template:Cvt.<ref name="Herschel 1785"/>
In 1850, William Parsons, 3rd Earl of Rosse, made a drawing of Andromeda's spiral structure.<ref>Template:Cite journal</ref>Template:Better source needed
In 1864, William Huggins noted that the spectrum of Andromeda differed from that of a gaseous nebula.<ref name="Huggins & Miller 1864"/> The spectrum of Andromeda displays a continuum of frequencies, superimposed with dark absorption lines that help identify the chemical composition of an object. Andromeda's spectrum is very similar to the spectra of individual stars, and from this, it was deduced that Andromeda has a stellar nature. In 1885, a supernova (known as S Andromedae) was seen in Andromeda, the first and so far only one observed in that galaxy.<ref name="Öpik 1922"/> At the time, it was called "Nova 1885"<ref name="Backhouse 1888"/>—the difference between "novae" in the modern sense and supernovae was not yet known. Andromeda was considered to be a nearby object, and it was not realized that the "nova" was much brighter than ordinary novae.Template:Citation needed
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In 1888, Isaac Roberts took one of the first photographs of Andromeda, which was still commonly thought to be a nebula within our galaxy. Roberts mistook Andromeda and similar "spiral nebulae" as star systems being formed.<ref name="NebPix"/><ref name="sciPho"/>
In 1912, Vesto Slipher used spectroscopy to measure the radial velocity of Andromeda with respect to the Solar System—the largest velocity yet measured, at Template:Cvt.<ref name="Slipher 1913"/>
"Island universes" hypothesisEdit
As early as 1755, the German philosopher Immanuel Kant proposed the hypothesis that the Milky Way is only one of many galaxies in his book Universal Natural History and Theory of the Heavens. Arguing that a structure like the Milky Way would look like a circular nebula viewed from above and like an ellipsoid if viewed from an angle, he concluded that the observed elliptical nebulae like Andromeda, which could not be explained otherwise at the time, were indeed galaxies similar to the Milky Way, not nebulae, as Andromeda was commonly believed to be.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>
In 1917, Heber Curtis observed a nova within Andromeda. After searching the photographic record, 11 more novae were discovered. Curtis noticed that these novae were, on average, 10 magnitudes fainter than those that occurred elsewhere in the sky. As a result, he was able to come up with a distance estimate of Template:Convert. Although this estimate is about fivefold lower than the best estimates now available, it was the first known estimate of the distance to Andromeda that was correct to within an order of magnitude (i.e., to within a factor of ten of the current estimates, which place the distance around 2.5 million light-years<ref name="Karachentsevetal2006"/><ref name="karachentsevetal2004"/><ref name="Ribas2005"/><ref name="McConnachieetal2005"/>). Curtis became a proponent of the so-called "island universes" hypothesis: that spiral nebulae were actually independent galaxies.<ref name="Curtis 1988"/>
In 1920, the Great Debate between Harlow Shapley and Curtis took place concerning the nature of the Milky Way, spiral nebulae, and the dimensions of the universe.<ref name="Hubble 1929"/> To support his claim that the Great Andromeda Nebula is, in fact, an external galaxy, Curtis also noted the appearance of dark lanes within Andromeda that resembled the dust clouds in our own galaxy, as well as historical observations of the Andromeda Galaxy's significant Doppler shift. In 1922, Ernst Öpik presented a method to estimate the distance of Andromeda using the measured velocities of its stars. His result placed the Andromeda Nebula far outside our galaxy at a distance of about Template:Cvt.<ref name="Öpik 1922"/> Edwin Hubble settled the debate in 1925 when he identified extragalactic Cepheid variable stars for the first time on astronomical photos of Andromeda. These were made using the Template:Convert Hooker telescope, and they enabled the distance of the Great Andromeda Nebula to be determined. His measurement demonstrated conclusively that this feature was not a cluster of stars and gas within our own galaxy, but an entirely separate galaxy located a significant distance from the Milky Way.<ref name="Hubble 1929"/>
In 1943, Walter Baade was the first person to resolve stars in the central region of the Andromeda Galaxy. Baade identified two distinct populations of stars based on their metallicity, naming the young, high-velocity stars in the disk Type I and the older, red stars in the bulge Type II.<ref name="Baade 1944"/> This nomenclature was subsequently adopted for stars within the Milky Way and elsewhere. (The existence of two distinct populations had been noted earlier by Jan Oort.)<ref name="Baade 1944"/> Baade also discovered that there were two types of Cepheid variable stars, which resulted in doubling the distance estimate to Andromeda, as well as the remainder of the universe.<ref name="Gribbin 2001"/>
In 1950, radio emissions from the Andromeda Galaxy were detected by Robert Hanbury Brown and Cyril Hazard at the Jodrell Bank Observatory.<ref name="Brown & Hazard 1950"/><ref name="Brown & Hazard 1951"/> The first radio maps of the galaxy were made in the 1950s by John Baldwin and collaborators at the Cambridge Radio Astronomy Group.<ref name="van der Kruit & Allen 1976"/> The core of the Andromeda Galaxy is called 2C 56 in the 2C radio astronomy catalog.
In 1959 rapid rotation of the semi-stellar nucleus of M31 was discovered by Andre Lallemand, M. Duschene and Merle Walker<ref>PASP 1960, p.72</ref> at the Lick Observatory, using the 120-inch telescope, coudé Spectrograph, and Lallemand electronographic camera. They estimated the mass of the nucleus to be about 1.3 x 107 solar masses. The second example of this phenomenon was found in 1961 in the nucleus of M32 by M.F Walker<ref>1962 Astrophysical Journal, 136, p.692</ref> at the Lick Observatory, using the same equipment as used for the discovery of the nucleus of M31. He estimated the nuclear mass to be between 0.8 and 1 x 107 solar masses. Such rotation is now considered to be evidence of the existence of supermassive black holes in the nuclei of these galaxies.
21st centuryEdit
In 2009, an occurrence of microlensing—a phenomenon caused by the deflection of light by a massive object—may have led to the first discovery of a planet in the Andromeda Galaxy.<ref name="Ingrosso 2009"/>
In 2020, observations of linearly polarized radio emission with the Westerbork Synthesis Radio Telescope, the Effelsberg 100-m Radio Telescope, and the Very Large Array revealed ordered magnetic fields aligned along the "10-kpc ring" of gas and star formation.<ref name="Beck 2020"/>
In 2025, NASA published a huge mosaic made by the Hubble Space Telescope, assembled from approximately 600 separate overlapping fields of view taken over 10 years of Hubble observation. Hubble resolves an estimated 200 million stars that are hotter than our Sun, but still a fraction of the galaxy’s total estimated stellar population.
GeneralEdit
The estimated distance of the Andromeda Galaxy from our own was doubled in 1953 when it was discovered that there is a second, dimmer type of Cepheid variable star. In the 1990s, measurements of both standard red giants as well as red clump stars from the Hipparcos satellite measurements were used to calibrate the Cepheid distances.<ref name="Holland 1998"/><ref name="Stanek & Garnavich 1998"/>
Formation and historyEdit
A major merger occurred 2 to 3 billion years ago at the Andromeda location, involving two galaxies with a mass ratio of approximately 4.<ref name="Hammer et al. 2018">Template:Cite journal</ref><ref name="D'Souza and Bell">Template:Cite journal</ref>
The discovery of a recent merger in the Andromeda galaxy was first based on interpreting its anomalous age-velocity dispersion relation,<ref name="Dorman et al. 2014">Template:Cite journal</ref> as well as the fact that 2 billion years ago, star formation throughout Andromeda's disk was much more active than today.<ref name="Williams et al. 2015">Template:Cite journal</ref>
Modeling<ref name="Hammer et al. 2018"/> of this violent collision shows that it has formed most of the galaxy's (metal-rich) galactic halo, including the Giant Stream,<ref name="Ibata et al. 2001">Template:Cite journal</ref> and also the extended thick disk, the young age thin disk, and the static 10 kpc ring. During this epoch, its rate of star formation would have been very high, to the point of becoming a luminous infrared galaxy for roughly 100 million years. Modeling also recovers the bulge profile, the large bar, and the overall halo density profile.
Andromeda and the Triangulum Galaxy (M33) might have had a very close passage 2–4 billion years ago, but it seems unlikely from the last measurements from the Hubble Space Telescope.<ref name="Patel et al. 2017">Template:Cite journal</ref>
Distance estimateEdit
At least four distinct techniques have been used to estimate distances from Earth to the Andromeda Galaxy. In 2003, using the infrared surface brightness fluctuations (I-SBF) and adjusting for the new period-luminosity value and a metallicity correction of −0.2 mag dex−1 in (O/H), an estimate of Template:Convert was derived. A 2004 Cepheid variable method estimated the distance to be 2.51 ± 0.13 million light-years (770 ± 40 kpc).<ref name="Karachentsevetal2006"/><ref name="karachentsevetal2004"/>
In 2005, an eclipsing binary star was discovered in the Andromeda Galaxy. The binaryTemplate:Efn is made up of two hot blue stars of types O and B. By studying the eclipses of the stars, astronomers were able to measure their sizes. Knowing the sizes and temperatures of the stars, they were able to measure their absolute magnitude. When the visual and absolute magnitudes are known, the distance to the star can be calculated. The stars lie at a distance of Template:Convert and the whole Andromeda Galaxy at about Template:Convert.<ref name="Ribas2005"/> This new value is in excellent agreement with the previous, independent Cepheid-based distance value. The TRGB method was also used in 2005 giving a distance of Template:Convert.<ref name="McConnachieetal2005"/> Averaged together, these distance estimates give a value of Template:Convert.Template:Efn
Mass estimatesEdit
Until 2018, mass estimates for the Andromeda Galaxy's halo (including dark matter) gave a value of approximately Template:Solar mass,<ref name="Jorge Peñarrubia2014"/> compared to Template:Solar mass for the Milky Way. This contradicted even earlier measurements that seemed to indicate that the Andromeda Galaxy and Milky Way are almost equal in mass. In 2018, the earlier measurements for equality of mass were re-established by radio results as approximately Template:Solar mass.<ref name="Kafle et al. 2018"/><ref name="Need4Speed-1"/><ref name="cosmic"/><ref name="Space.com"/> In 2006, the Andromeda Galaxy's spheroid was determined to have a higher stellar density than that of the Milky Way,<ref name="Kalirai et al 2006"/> and its galactic stellar disk was estimated at twice the diameter of that of the Milky Way.<ref name="Chapman et al 2006"/> The total mass of the Andromeda Galaxy is estimated to be between Template:Solar mass<ref name="Kafle et al. 2018"/> and Template:Solar mass.<ref name="Barmby 2006"/><ref name="Barmby2007"/> The stellar mass of M31 is Template:Solar mass, with 30% of that mass in the central bulge, 56% in the disk, and the remaining 14% in the stellar halo.<ref name="Tamm2012"/> The radio results (similar mass to the Milky Way Galaxy) should be taken as likeliest as of 2018, although clearly, this matter is still under active investigation by several research groups worldwide.
As of 2019, current calculations based on escape velocity and dynamical mass measurements put the Andromeda Galaxy at Template:Solar mass,<ref name="Need4Speed"/> which is only half of the Milky Way's newer mass, calculated in 2019 at Template:Solar mass.<ref name="daily"/><ref name="SA-20190308"/><ref name="ARX-20190208"/>
In addition to stars, the Andromeda Galaxy's interstellar medium contains at least Template:Solar mass<ref name="BraunThilkerWalterbosCorbelli2009"/> in the form of neutral hydrogen, at least Template:Solar mass as molecular hydrogen (within its innermost 10 kiloparsecs), and Template:Solar mass of dust.<ref name="Andromedandust"/>
The Andromeda Galaxy is surrounded by a massive halo of hot gas that is estimated to contain half the mass of the stars in the galaxy. The nearly invisible halo stretches about a million light-years from its host galaxy, halfway to our Milky Way Galaxy. Simulations of galaxies indicate the halo formed at the same time as the Andromeda Galaxy. The halo is enriched in elements heavier than hydrogen and helium, formed from supernovae, and its properties are those expected for a galaxy that lies in the "green valley" of the Galaxy color-magnitude diagram (see below). Supernovae erupt in the Andromeda Galaxy's star-filled disk and eject these heavier elements into space. Over the Andromeda Galaxy's lifetime, nearly half of the heavy elements made by its stars have been ejected far beyond the galaxy's 200,000-light-year-diameter stellar disk.<ref name="Hubble-halo-a"/><ref name="Massive"/><ref name="Evidence"/><ref name="HaloFind"/>
Luminosity estimatesEdit
The estimated luminosity of the Andromeda Galaxy, Template:Solar luminosity, is about 25% higher than that of our own galaxy.<ref name="vdb"/><ref name="Moskvitch 2010"/> However, the galaxy has a high inclination as seen from Earth, and its interstellar dust absorbs an unknown amount of light, so it is difficult to estimate its actual brightness and other authors have given other values for the luminosity of the Andromeda Galaxy (some authors even propose it is the second-brightest galaxy within a radius of 10 megaparsecs of the Milky Way, after the Sombrero Galaxy,<ref name="Karachentsev2004"/> with an absolute magnitude of around −22.21Template:Efn or close<ref name="McCall2014"/>).
An estimation done with the help of Spitzer Space Telescope published in 2010 suggests an absolute magnitude (in the blue) of −20.89 (that with a color index of +0.63 translates to an absolute visual magnitude of −21.52,Template:Efn compared to −20.9 for the Milky Way), and a total luminosity in that wavelength of Template:Solar luminosity.<ref name="Tempel2010"/>
The rate of star formation in the Milky Way is much higher, with the Andromeda Galaxy producing only about one solar mass per year compared to 3–5 solar masses for the Milky Way. The rate of novae in the Milky Way is also double that of the Andromeda Galaxy.<ref name="Liller & Mayer 1987"/> This suggests that the latter once experienced a great star formation phase, but is now in a relative state of quiescence, whereas the Milky Way is experiencing more active star formation.<ref name="vdb"/> Should this continue, the luminosity of the Milky Way may eventually overtake that of the Andromeda Galaxy.
According to recent studies, the Andromeda Galaxy lies in what is known in the galaxy color–magnitude diagram as the "green valley", a region populated by galaxies like the Milky Way in transition from the "blue cloud" (galaxies actively forming new stars) to the "red sequence" (galaxies that lack star formation). Star formation activity in green valley galaxies is slowing as they run out of star-forming gas in the interstellar medium. In simulated galaxies with similar properties to the Andromeda Galaxy, star formation is expected to extinguish within about five billion years, even accounting for the expected, short-term increase in the rate of star formation due to the collision between the Andromeda Galaxy and the Milky Way.<ref name="MWAY"/>
StructureEdit
Based on its appearance in visible light, the Andromeda Galaxy is classified as an SA(s)b galaxy in the de Vaucouleurs–Sandage extended classification system of spiral galaxies.<ref name="ned"/> However, infrared data from the 2MASS survey and the Spitzer Space Telescope showed that Andromeda is actually a barred spiral galaxy, like the Milky Way, with Andromeda's bar major axis oriented 55 degrees anti-clockwise from the disc major axis.<ref name="Beaton 2006"/>
There are various methods used in astronomy in defining the size of a galaxy, and each method can yield different results concerning one another. The most commonly employed is the D25 standard, the isophote where the photometric brightness of a galaxy in the B-band (445 nm wavelength of light, in the blue part of the visible spectrum) reaches 25 mag/arcsec2.<ref name="GalaxySize">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref> The Third Reference Catalogue of Bright Galaxies (RC3) used this standard for Andromeda in 1991, yielding an isophotal diameter of Template:Convert at a distance of 2.5 million light-years.<ref name="RC3"/> An earlier estimate from 1981 gave a diameter for Andromeda at Template:Convert.<ref name="AtlasofAndromeda">{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>
A study in 2005 by the Keck telescopes shows the existence of a tenuous sprinkle of stars, or galactic halo, extending outward from the galaxy.<ref name="Chapman et al 2006"/> The stars in this halo behave differently from the ones in Andromeda's main galactic disc, where they show rather disorganized orbital motions as opposed to the stars in the main disc having more orderly orbits and uniform velocities of 200 km/s.<ref name="Chapman et al 2006"/> This diffuse halo extends outwards away from Andromeda's main disc with the diameter of Template:Convert.<ref name="Chapman et al 2006"/>
The galaxy is inclined an estimated 77° relative to Earth (where an angle of 90° would be edge-on). Analysis of the cross-sectional shape of the galaxy appears to demonstrate a pronounced, S-shaped warp, rather than just a flat disk.<ref name="UC Santa Cruz 2001"/> A possible cause of such a warp could be gravitational interaction with the satellite galaxies near the Andromeda Galaxy. The Galaxy M33 could be responsible for some warp in Andromeda's arms, though more precise distances and radial velocities are required.
Spectroscopic studies have provided detailed measurements of the rotational velocity of the Andromeda Galaxy as a function of radial distance from the core. The rotational velocity has a maximum value of Template:Cvt at Template:Convert from the core, and it has its minimum possibly as low as Template:Cvt at Template:Convert from the core. Further out, rotational velocity rises out to a radius of Template:Convert, where it reaches a peak of Template:Cvt. The velocities slowly decline beyond that distance, dropping to around Template:Cvt at Template:Convert. These velocity measurements imply a concentrated mass of about Template:Solar mass in the nucleus. The total mass of the galaxy increases linearly out to Template:Convert, then more slowly beyond that radius.<ref name="Rubin & Ford 1970"/>
The spiral arms of the Andromeda Galaxy are outlined by a series of HII regions, first studied in great detail by Walter Baade and described by him as resembling "beads on a string". His studies show two spiral arms that appear to be tightly wound, although they are more widely spaced than in our galaxy.<ref name="Arp 1964"/> His descriptions of the spiral structure, as each arm crosses the major axis of the Andromeda Galaxy, are as follows<ref name="Bergh1991"/>§pp1062<ref name="Hodge1966"/>§pp92:
| Arms (N=cross M31's major axis at north, S=cross M31's major axis at south) | Distance from center (arcminutes) (N*/S*) | Distance from the center (kpc) (N*/S*) | Notes |
|---|---|---|---|
| N1/S1 | 3.4/1.7 | 0.7/0.4 | Dust arms with no OB associations of HII regions |
| N2/S2 | 8.0/10.0 | 1.7/2.1 | Dust arms with some OB associations |
| N3/S3 | 25/30 | 5.3/6.3 | As per N2/S2, but with some HII regions too |
| N4/S4 | 50/47 | 11/9.9 | Large numbers of OB associations, HII regions, and little dust |
| N5/S5 | 70/66 | 15/14 | As per N4/S4 but much fainter |
| N6/S6 | 91/95 | 19/20 | Loose OB associations. No dust is visible. |
| N7/S7 | 110/116 | 23/24 | As per N6/S6 but fainter and inconspicuous |
Since the Andromeda Galaxy is seen close to edge-on, it is difficult to study its spiral structure. Rectified images of the galaxy seem to show a fairly normal spiral galaxy, exhibiting two continuous trailing arms that are separated from each other by a minimum of about Template:Convert and that can be followed outward from a distance of roughly Template:Convert from the core. Alternative spiral structures have been proposed such as a single spiral arm<ref name="Simien1978"/> or a flocculent<ref name="Haas2000"/> pattern of long, filamentary, and thick spiral arms.<ref name="ned"/><ref name="Walterbos1988"/>
The most likely cause of the distortions of the spiral pattern is thought to be interaction with galaxy satellites M32 and M110.<ref name="Gordon2006"/> This can be seen by the displacement of the neutral hydrogen clouds from the stars.<ref name="Braun 1991"/>
In 1998, images from the European Space Agency's Infrared Space Observatory demonstrated that the overall form of the Andromeda Galaxy may be transitioning into a ring galaxy. The gas and dust within the galaxy are generally formed into several overlapping rings, with a particularly prominent ring formed at a radius of Template:Cvt from the core,<ref name="ESA 1998-10-14"/> nicknamed by some astronomers the ring of fire.<ref name="M31youngclusters"/> This ring is hidden from visible light images of the galaxy because it is composed primarily of cold dust, and most of the star formation that is taking place in the Andromeda Galaxy is concentrated there.<ref name="Andromedan10kpcring"/>
Later studies with the help of the Spitzer Space Telescope showed how the Andromeda Galaxy's spiral structure in the infrared appears to be composed of two spiral arms that emerge from a central bar and continue beyond the large ring mentioned above. Those arms, however, are not continuous and have a segmented structure.<ref name="Gordon2006"/>
Close examination of the inner region of the Andromeda Galaxy with the same telescope also showed a smaller dust ring that is believed to have been caused by the interaction with M32 more than 200 million years ago. Simulations show that the smaller galaxy passed through the disk of the Andromeda Galaxy along the latter's polar axis. This collision stripped more than half the mass from the smaller M32 and created the ring structures in Andromeda.<ref name="Harvard-Smithsonian 2006-10-18"/> It is the co-existence of the long-known large ring-like feature in the gas of Messier 31, together with this newly discovered inner ring-like structure, offset from the barycenter, that suggested a nearly head-on collision with the satellite M32, a milder version of the Cartwheel encounter.<ref name="Block2006"/>
Studies of the extended halo of the Andromeda Galaxy show that it is roughly comparable to that of the Milky Way, with stars in the halo being generally "metal-poor", and increasingly so with greater distance.<ref name="Kalirai et al 2006"/> This evidence indicates that the two galaxies have followed similar evolutionary paths. They are likely to have accreted and assimilated about 100–200 low-mass galaxies during the past 12 billion years.<ref name="Bullock & Johnston 2005"/> The stars in the extended halos of the Andromeda Galaxy and the Milky Way may extend nearly one-third the distance separating the two galaxies.
NucleusEdit
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The Andromeda Galaxy is known to harbor a dense and compact star cluster at its very center, similar to the Milky Way galaxy. A large telescope creates a visual impression of a star embedded in the more diffuse surrounding bulge. In 1991, the Hubble Space Telescope was used to image the Andromeda Galaxy's inner nucleus. The nucleus consists of two concentrations separated by Template:Cvt. The brighter concentration, designated as P1, is offset from the center of the galaxy. The dimmer concentration, P2, falls at the true center of the galaxy and contains an embedded star cluster, called P3,<ref name="Bender et al 2005"/> containing many UV-bright A-stars and the supermassive black hole, called M31*.<ref name=":0">Template:Cite journal</ref><ref name=":1">Template:Cite journal</ref> The black hole is classified as a low-luminosity AGN (LLAGN) and it was detected only in radio wavelengths and in x-rays.<ref name=":1"/> It was quiescent in 2004–2005, but it was highly variable in 2006–2007.<ref name=":0"/> An additional x-ray flare occurred in 2013.<ref>Template:Cite journal</ref> The mass of M31* was measured at 3–5 × 107 Template:Solar mass in 1993,<ref name="Lauer"/> and at 1.1–2.3 × 108 Template:Solar mass in 2005.<ref name="Bender et al 2005"/> The velocity dispersion of material around it is measured to be ≈ Template:Cvt.<ref name="Gebhardt et al 2000"/>
It has been proposed that the observed double nucleus could be explained if P1 is the projection of a disk of stars in an eccentric orbit around the central black hole.<ref name="Tremaine 1995"/> The eccentricity is such that stars linger at the orbital apocenter, creating a concentration of stars. It has been postulated that such an eccentric disk could have been formed from the result of a previous black hole merger, where the release of gravitational waves could have "kicked" the stars into their current eccentric distribution.<ref>Template:Cite journal</ref> P2 also contains a compact disk of hot, spectral-class A stars. The A stars are not evident in redder filters, but in blue and ultraviolet light they dominate the nucleus, causing P2 to appear more prominent than P1.<ref name="hubblesite 1993-07-20"/>
While at the initial time of its discovery it was hypothesized that the brighter portion of the double nucleus is the remnant of a small galaxy "cannibalized" by the Andromeda Galaxy,<ref name="Schewe & Stein 1993"/> this is no longer considered a viable explanation, largely because such a nucleus would have an exceedingly short lifetime due to tidal disruption by the central black hole. While this could be partially resolved if P1 had its own black hole to stabilize it, the distribution of stars in P1 does not suggest that there is a black hole at its center.<ref name="Tremaine 1995"/>
Discrete sourcesEdit
Apparently, by late 1968, no X-rays had been detected from the Andromeda Galaxy.<ref name="Fujimoto et al 1969"/> A balloon flight on 20 October 1970 set an upper limit for detectable hard X-rays from the Andromeda Galaxy.<ref name="Peterson 1973"/> The Swift BAT all-sky survey successfully detected hard X-rays coming from a region centered 6 arcseconds away from the galaxy center. The emission above 25 keV was later found to be originating from a single source named 3XMM J004232.1+411314, and identified as a binary system where a compact object (a neutron star or a black hole) accretes matter from a star.<ref name="Marelli et al. 2017"/>
Multiple X-ray sources have since been detected in the Andromeda Galaxy, using observations from the European Space Agency's (ESA) XMM-Newton orbiting observatory. Robin Barnard et al. hypothesized that these are candidate black holes or neutron stars, which are heating the incoming gas to millions of kelvins and emitting X-rays. Neutron stars and black holes can be distinguished mainly by measuring their masses.<ref name="Barnard Kolb & Osborne 2005"/> An observation campaign of NuSTAR space mission identified 40 objects of this kind in the galaxy.<ref name="And-Scand"/> In 2012, a microquasar, a radio burst emanating from a smaller black hole was detected in the Andromeda Galaxy. The progenitor black hole is located near the galactic center and has about 10 Template:Solar mass. It was discovered through data collected by the European Space Agency's XMM-Newton probe and was subsequently observed by NASA's Swift Gamma-Ray Burst Mission and Chandra X-Ray Observatory, the Very Large Array, and the Very Long Baseline Array. The microquasar was the first observed within the Andromeda Galaxy and the first outside of the Milky Way Galaxy.<ref name="prostak-2012"/>
Globular clustersEdit
There are approximately 460 globular clusters associated with the Andromeda Galaxy.<ref name="Barmby & Huchra 2001"/> The most massive of these clusters, identified as Mayall II, nicknamed Globular One, has a greater luminosity than any other known globular cluster in the Local Group of galaxies.<ref name="hubblesite 1996-04-24"/> It contains several million stars and is about twice as luminous as Omega Centauri, the brightest known globular cluster in the Milky Way. Mayall II (also known as Globular One or G1) has several stellar populations and a structure too massive for an ordinary globular. As a result, some consider Mayall II to be the remnant core of a dwarf galaxy that was consumed by Andromeda in the distant past.<ref name="Meylan et al 2001"/> The cluster with the greatest apparent brightness is G76 which is located in the southwest arm's eastern half.<ref name="NSOG"/> Another massive globular cluster, named 037-B327 (also known as Bol 37) and discovered in 2006 as is heavily reddened by the Andromeda Galaxy's interstellar dust, was thought to be more massive than Mayall II and the largest cluster of the Local Group;<ref name="SuperStr"/> however, other studies have shown it is actually similar in properties to Mayall II.<ref name="Cohen06"/>
Unlike the globular clusters of the Milky Way, which show a relatively low age dispersion, Andromeda Galaxy's globular clusters have a much larger range of ages: from systems as old as the galaxy itself to much younger systems, with ages between a few hundred million years to five billion years.<ref name="Formations"/>
In 2005, astronomers discovered a completely new type of star cluster in the Andromeda Galaxy. The new-found clusters contain hundreds of thousands of stars, a similar number of stars that can be found in globular clusters. What distinguishes them from the globular clusters is that they are much larger—several hundred light-years across—and hundreds of times less dense. The distances between the stars are, therefore, much greater within the newly discovered extended clusters.<ref name="Huxor et al 2005"/>
The most massive globular cluster in the Andromeda Galaxy, B023-G078, likely has a central intermediate black hole of almost 100,000 solar masses.<ref name="central black hole">Template:Cite journal</ref>
PA-99-N2 event and possible exoplanet in galaxyEdit
{{#invoke:Labelled list hatnote|labelledList|Main article|Main articles|Main page|Main pages}} PA-99-N2 was a microlensing event detected in the Andromeda Galaxy in 1999. One of the explanations for this is the gravitational lensing of a red giant by a star with a mass between 0.02 and 3.6 times that of the Sun, which suggested that the star is likely orbited by a planet. This possible exoplanet would have a mass 6.34 times that of Jupiter. If finally confirmed, it would be the first ever found extragalactic planet. However, anomalies in the event were later found.<ref name="Better needed"/>
Nearby and satellite galaxiesEdit
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Like the Milky Way, the Andromeda Galaxy has smaller satellite galaxies, consisting of over 20 known dwarf galaxies. The Andromeda Galaxy's dwarf galaxy population is very similar to the Milky Way's, but the galaxies are much more numerous.<ref>Template:Cite journal</ref> The best-known and most readily observed satellite galaxies are M32 and M110. Based on current evidence, it appears that M32 underwent a close encounter with the Andromeda Galaxy in the past. M32 may once have been a larger galaxy that had its stellar disk removed by M31 and underwent a sharp increase of star formation in the core region, which lasted until the relatively recent past.<ref name="Bekki et al 2001"/>
M110 also appears to be interacting with the Andromeda Galaxy, and astronomers have found in the halo of the latter a stream of metal-rich stars that appear to have been stripped from these satellite galaxies.<ref name="Ibata et al 2001"/> M110 does contain a dusty lane, which may indicate recent or ongoing star formation.<ref name="Young 2000"/> M32 has a young stellar population as well.<ref name="Rudenko"/>
The Triangulum Galaxy is a non-dwarf galaxy that lies 750,000 light-years from Andromeda. It is currently unknown whether it is a satellite of Andromeda.<ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref>
In 2006, it was discovered that nine of the satellite galaxies lie in a plane that intersects the core of the Andromeda Galaxy; they are not randomly arranged as would be expected from independent interactions. This may indicate a common tidal origin for the satellites.<ref name="Koch & Grebel 2006"/>
Collision with the Milky WayEdit
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The Andromeda Galaxy is approaching the Milky Way at about Template:Convert per second.<ref name="nature"/> It has been measured approaching relative to the Sun at around Template:Cvt<ref name="ned"/> as the Sun orbits around the center of the galaxy at a speed of approximately Template:Cvt. This makes the Andromeda Galaxy one of about 100 observable blueshifted galaxies.<ref name="Answers"/> Andromeda Galaxy's tangential or sideways velocity concerning the Milky Way is relatively much smaller than the approaching velocity and therefore it is expected to collide directly with the Milky Way in about 2.5–4 billion years. A likely outcome of the collision is that the galaxies will merge to form a giant elliptical galaxy<ref name="Cox & Loeb 2008"/> or possibly large disc galaxy.<ref name="Ueda2014"/> Such events are frequent among the galaxies in galaxy groups. The fate of Earth and the Solar System in the event of a collision is currently unknown. Before the galaxies merge, there is a small chance that the Solar System could be ejected from the Milky Way or join the Andromeda Galaxy.<ref name="Cain 2007"/>
Amateur observationEdit
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Under most viewing conditions, the Andromeda Galaxy is one of the most distant objects that can be seen with the naked eye, due to its sheer size. (M33 and, for observers with exceptionally good vision, M81 can be seen under very dark skies.)<ref name="StarChild"/><ref name="S&T-obs"/><ref>{{#invoke:citation/CS1|citation |CitationClass=web }}</ref><ref>Template:Cite book</ref> The constellation of Andromeda, in which the galaxy is located, is usually found with the aid of the constellations Cassiopeia or Pegasus, which are usually easier to recognize at first glance. Andromeda is best seen during autumn nights in the Northern Hemisphere when it passes high overhead, reaching its highest point around midnight in October, and two hours earlier each successive month. In the early evening, it rises in the east in September and sets in the west in February.<ref name=physics/> From the Southern Hemisphere the Andromeda Galaxy is visible between October and December, best viewed from as far north as possible. Binoculars can reveal some larger structures of the galaxy and its two brightest satellite galaxies, M32 and M110.<ref name="S&T"/> An amateur telescope can reveal Andromeda's disk, some of its brightest globular clusters, dark dust lanes, and the large star cloud NGC 206.<ref name=Backyard/><ref name="A-Mall"/>
See alsoEdit
NotesEdit
ReferencesEdit
External linksEdit
- Template:WikiSky
- StarDate: M31 Fact Sheet
- Messier 31, SEDS Messier pages
- Astronomy Picture of the Day
- A Giant Globular Cluster in M31 1998 October 17.
- M31: The Andromeda Galaxy 2004 July 18.
- Andromeda Island Universe 2005 December 22.
- Andromeda Island Universe 2010 January 9.
- WISE Infrared Andromeda 2010 February 19.
- M31's angular size compared with full Moon 2013 August 1.
- M31 and its central Nuclear Spiral
- Amateur photography – M31
- Globular Clusters in M31 at The Curdridge Observatory
- First direct distance to Andromeda − Astronomy magazine article
- Andromeda Galaxy at SolStation.com
- Andromeda Galaxy at The Encyclopedia of Astrobiology, Astronomy, & Spaceflight
- M31, the Andromeda Galaxy at NightSkyInfo.com
- Template:Cite news
- M31 (Apparent) Novae Page (IAU)
- Multi-wavelength composite
- Andromeda Project (crowd-source)
- {{#invoke:citation/CS1|citation
|CitationClass=web }}
- Hubble's High-Definition Panoramic View of the Andromeda Galaxy
- Infrared-Radio Image of the Andromeda Galaxy (M31)
- Creative Commons Astrophotography M31 Andromeda image download & processing guide
Template:Andromeda galaxy Template:Messier objects Template:NGC objects:1-499 Template:Stars of Andromeda Template:Portal bar Template:Authority control Template:Sky