Andromeda Galaxy#Nucleus

File:Auv0175.png in The Book of Fixed Stars (from around 964 CE) in a manuscript from 1009–1010 CE{{cite web | title=Andromeda Galaxy al-Sufi | website=Ian Ridpath | url=http://www.ianridpath.com/startales/andromeda-alsufi.html | access-date=2024-11-22}}{{cite web | title=The earliest image of another galaxy | website=Ivan Debono | date=2015-09-16 | url=http://www.idebono.eu/2015/09/16/the-earliest-image-of-another-galaxy/ | access-date=2024-11-22}}]]

The Andromeda Galaxy is visible to the naked eye in dark skies. 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". Star charts of that period labeled it as the Little Cloud. In 1612, the German astronomer Simon Marius gave an early description of the Andromeda Galaxy based on telescopic observations. Pierre Louis Maupertuis conjectured in 1745 that the blurry spot was an island universe. 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. 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 {{cvt|18000|ly|kpc|lk=on}}.

In 1850, William Parsons, 3rd Earl of Rosse, made a drawing of Andromeda's spiral structure.{{Cite journal |last=Payne-Gaposchkin |first=Cecilia H. |year=1953 |title=Why do Galaxies have a Spiral Form? |journal=Scientific American |volume=189 |issue=3 |pages=89–99 |bibcode=1953SciAm.189c..89P |doi=10.1038/scientificamerican0953-89 |issn=0036-8733 |jstor=24944338 }}{{better source needed|date=January 2024}}

In 1864, William Huggins noted that the spectrum of Andromeda differed from that of a gaseous nebula. 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. At the time, it was called "Nova 1885"—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.{{citation needed|date=October 2023}}

File:Andromeda_Nebula_-_Isaac_Roberts,_29_December_1888 (cropped).jpg to the upper right), by Isaac Roberts (29 December 1888)]]

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.

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 {{cvt|300|km/s}}.

File:Andromeda_constellation_map.svg

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.{{cite web |title=Seite:Allgemeine Naturgeschichte und Theorie des Himmels.djvu/41 – Wikisource |url=https://de.wikisource.org/wiki/Seite:Allgemeine_Naturgeschichte_und_Theorie_des_Himmels.djvu/41?useskin=vector |website=de.wikisource.org |language=de}}

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 {{convert|500000|ly|e9AU|abbr=unit}}. 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). Curtis became a proponent of the so-called "island universes" hypothesis: that spiral nebulae were actually independent galaxies.

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. 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 {{cvt|450|kpc}}. 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 {{convert|100|in|m|adj=on}} 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.

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. 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.) 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.

In 1950, radio emissions from the Andromeda Galaxy were detected by Robert Hanbury Brown and Cyril Hazard at the Jodrell Bank Observatory. The first radio maps of the galaxy were made in the 1950s by John Baldwin and collaborators at the Cambridge Radio Astronomy Group. 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 WalkerPASP 1960, p.72 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 Walker1962 Astrophysical Journal, 136, p.692 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.

File:Largest Mosaic of Andromeda by Hubble jan 16 2025-extra details.jpg

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.

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.

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.

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.

File:Andromeda Galaxy 560mm FL.jpg to highlight its star-forming regions]]

A major merger occurred 2 to 3 billion years ago at the Andromeda location, involving two galaxies with a mass ratio of approximately 4.{{cite journal |last1=Hammer |first1=F |last2=Yang |first2=Y B |last3=Wang |first3=J L |last4=Ibata |first4=R |last5=Flores |first5=H |last6=Puech |first6=M |title=A 2–3 billion year old major merger paradigm for the Andromeda galaxy and its outskirts |journal=Monthly Notices of the Royal Astronomical Society |date=1 April 2018 |volume=475 |issue=2 |pages=2754–2767 |doi=10.1093/mnras/stx3343|doi-access=free |arxiv=1801.04279 }}{{cite journal |last1=D’Souza |first1=Richard |last2=Bell |first2=Eric F. |title=The Andromeda galaxy's most important merger about 2 billion years ago as M32's likely progenitor |journal=Nature Astronomy |date=September 2018 |volume=2 |issue=9 |pages=737–743 |doi=10.1038/s41550-018-0533-x |arxiv=1807.08819 |bibcode=2018NatAs...2..737D |s2cid=256713163 |url=https://www.nature.com/articles/s41550-018-0533-x |language=en |issn=2397-3366}}

The discovery of a recent merger in the Andromeda galaxy was first based on interpreting its anomalous age-velocity dispersion relation,{{Cite journal |last1=Dorman |first1=Claire E. |last2=Guhathakurta |first2=Puragra |last3=Seth |first3=Anil C. |last4=Weisz |first4=Daniel R. |last5=Bell |first5=Eric F. |last6=Dalcanton |first6=Julianne J. |last7=Gilbert |first7=Karoline M. |last8=Hamren |first8=Katherine M. |last9=Lewis |first9=Alexia R. |last10=Skillman |first10=Evan D. |last11=Toloba |first11=Elisa |last12=Williams |first12=Benjamin F. |date=9 April 2015 |title=A clear age-velocity dispersion correlation in Andromeda's stellar disk |journal=The Astrophysical Journal |volume=803 |issue=1 |pages=24 |arxiv=1502.03820 |bibcode=2015ApJ...803...24D |doi=10.1088/0004-637X/803/1/24 |s2cid=119223754}} as well as the fact that 2 billion years ago, star formation throughout Andromeda's disk was much more active than today.{{Cite journal |last1=Williams |first1=Benjamin F. |last2=Dalcanton |first2=Julianne J. |last3=Dolphin |first3=Andrew E. |last4=Weisz |first4=Daniel R. |last5=Lewis |first5=Alexia R. |last6=Lang |first6=Dustin |last7=Bell |first7=Eric F. |last8=Boyer |first8=Martha |last9=Fouesneau |first9=Morgan |last10=Gilbert |first10=Karoline M. |last11=Monachesi |first11=Antonela |last12=Skillman |first12=Evan |date=5 June 2015 |title=A Global Star-forming Episode in M31 2-4 Gyr Ago |journal=The Astrophysical Journal |volume=806 |issue=1 |pages=48 |arxiv=1504.02120 |bibcode=2015ApJ...806...48W |doi=10.1088/0004-637X/806/1/48 |s2cid=118435748}}

Modeling of this violent collision shows that it has formed most of the galaxy's (metal-rich) galactic halo, including the Giant Stream,{{cite journal |last1=Ibata |first1=Rodrigo |last2=Irwin |first2=Michael |last3=Lewis |first3=Geraint |last4=Ferguson |first4=Annette M. N. |last5=Tanvir |first5=Nial |title=A giant stream of metal-rich stars in the halo of the galaxy M31 |journal=Nature |date=July 2001 |volume=412 |issue=6842 |pages=49–52 |doi=10.1038/35083506|pmid=11452300 |arxiv=astro-ph/0107090 |bibcode=2001Natur.412...49I |s2cid=4413139 }} 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.{{cite journal |last1=Patel |first1=Ekta |last2=Besla |first2=Gurtina |last3=Sohn |first3=Sangmo Tony |title=Orbits of massive satellite galaxies – I. A close look at the Large Magellanic Cloud and a new orbital history for M33 |journal=Monthly Notices of the Royal Astronomical Society |date=1 February 2017 |volume=464 |issue=4 |pages=3825–3849 |doi=10.1093/mnras/stw2616|doi-access=free |hdl=10150/623269 |hdl-access=free }}

File:Milky Way and Andromeda in space, to scale.jpg

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 {{convert|2.57|+/-|0.06|e6ly|e9AU|lk=on|abbr=unit}} was derived. A 2004 Cepheid variable method estimated the distance to be 2.51 ± 0.13 million light-years (770 ± 40 kpc).

In 2005, an eclipsing binary star was discovered in the Andromeda Galaxy. The binary{{efn|name=M31VJ}} 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 {{convert|2.52|+/-|0.14|e6ly|e9AU|abbr=unit}} and the whole Andromeda Galaxy at about {{convert|2.5|e6ly|e9AU|abbr=unit}}. 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 {{convert|2.56|+/-|0.08|e6ly|e9AU|abbr=unit}}. Averaged together, these distance estimates give a value of {{convert|2.54|+/-|0.11|e6ly|e9AU|abbr=unit}}.{{efn|name=avg dist}}

File:Hubble Finds Giant Halo Around the Andromeda Galaxy.jpg

Until 2018, mass estimates for the Andromeda Galaxy's halo (including dark matter) gave a value of approximately {{Solar mass|1.5{{e|12}}|link=y}}, compared to {{Solar mass|8{{e|11}}}} 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 {{Solar mass|8{{e|11}}}}. In 2006, the Andromeda Galaxy's spheroid was determined to have a higher stellar density than that of the Milky Way, and its galactic stellar disk was estimated at twice the diameter of that of the Milky Way. The total mass of the Andromeda Galaxy is estimated to be between {{Solar mass|8{{e|11}}}} and {{Solar mass|1.1{{e|12}}}}. The stellar mass of M31 is {{Solar mass|10–15{{e|10}}}}, with 30% of that mass in the central bulge, 56% in the disk, and the remaining 14% in the stellar halo. 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 {{Solar mass|0.8{{e|12}}}}, which is only half of the Milky Way's newer mass, calculated in 2019 at {{Solar mass|1.5{{e|12}}}}.

In addition to stars, the Andromeda Galaxy's interstellar medium contains at least {{Solar mass|7.2{{e|9}}}} in the form of neutral hydrogen, at least {{Solar mass|3.4{{e|8}}}} as molecular hydrogen (within its innermost 10 kiloparsecs), and {{Solar mass|5.4{{e|7}}}} of dust.

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.

The estimated luminosity of the Andromeda Galaxy, {{Solar luminosity|~2.6{{e|10}}|link=y}}, is about 25% higher than that of our own galaxy. 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, with an absolute magnitude of around −22.21{{efn|name=bright m31}} or close).

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,{{efn|name=blue mag}} compared to −20.9 for the Milky Way), and a total luminosity in that wavelength of {{Solar luminosity|3.64{{e|10}}}}.

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. 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. 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.

{{Wide image|Andromeda Galaxy M31 - Heic1502a Full resolution.jpg|600px|Zooming In on the Andromeda Galaxy – A panorama of foreground stars and the Andromeda Galaxy's nucleus. The image is the largest ever taken by the Hubble Space Telescope.}}

File:A Swift Tour of M31.ogv team]]

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. 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.

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.{{Cite web|url=https://ned.ipac.caltech.edu/level5/PROPERTIES/dog.html|title=Dimensions of Galaxies|website=ned.ipac.caltech.edu}} The Third Reference Catalogue of Bright Galaxies (RC3) used this standard for Andromeda in 1991, yielding an isophotal diameter of {{convert|46.56|kpc|ly|sigfig=3|abbr=off}} at a distance of 2.5 million light-years. An earlier estimate from 1981 gave a diameter for Andromeda at {{convert|54|kpc|ly|sigfig=3|abbr=off}}.{{Cite web|url=https://ned.ipac.caltech.edu/level5/ANDROMEDA_Atlas/frames.html|title=Atlas of the Andromeda Galaxy|website=ned.ipac.caltech.edu}}

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. 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. This diffuse halo extends outwards away from Andromeda's main disc with the diameter of {{convert|67.45|kpc|ly|sigfig=3|abbr=off}}.

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. 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 {{cvt|225|km/s}} at {{convert|1300|ly|e6AU|lk=on|abbr=unit}} from the core, and it has its minimum possibly as low as {{cvt|50|km/s}} at {{convert|7000|ly|e6AU|abbr=unit}} from the core. Further out, rotational velocity rises out to a radius of {{convert|33000|ly|e9AU|abbr=unit}}, where it reaches a peak of {{cvt|250|km/s}}. The velocities slowly decline beyond that distance, dropping to around {{cvt|200|km/s}} at {{convert|80000|ly|e9AU|abbr=unit}}. These velocity measurements imply a concentrated mass of about {{Solar mass|6{{e|9}}|link=y}} in the nucleus. The total mass of the galaxy increases linearly out to {{convert|45000|ly|e9AU|abbr=unit}}, then more slowly beyond that radius.

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. His descriptions of the spiral structure, as each arm crosses the major axis of the Andromeda Galaxy, are as follows^{§pp1062§pp92}:

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 {{convert|13000|ly|e6AU|lk=on|abbr=unit}} and that can be followed outward from a distance of roughly {{convert|1600|ly|e6AU|abbr=unit}} from the core. Alternative spiral structures have been proposed such as a single spiral arm or a flocculent pattern of long, filamentary, and thick spiral arms.

The most likely cause of the distortions of the spiral pattern is thought to be interaction with galaxy satellites M32 and M110. This can be seen by the displacement of the neutral hydrogen clouds from the stars.

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 {{cvt|32000|ly|kpc}} from the core, nicknamed by some astronomers the ring of fire. 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.

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.

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.

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.

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. 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. 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.

File:M31 nucleus (labels).jpg image of the Andromeda Galaxy core showing P1, P2 and P3, with P3 containing M31*. NASA/ESA photo]]

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 {{cvt|1.5|pc|lk=on}}. 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, containing many UV-bright A-stars and the supermassive black hole, called M31*.{{Cite journal |last1=Garcia |first1=Michael R. |last2=Hextall |first2=Richard |last3=Baganoff |first3=Frederick K. |last4=Galache |first4=Jose |last5=Melia |first5=Fulvio |last6=Murray |first6=Stephen S. |last7=Primini |first7=F. A. |last8=Sjouwerman |first8=Loránt O. |last9=Williams |first9=Ben |date=1 February 2010 |title=X-ray and Radio Variability of M31*, The Andromeda Galaxy Nuclear Supermassive Black Hole |url=https://ui.adsabs.harvard.edu/abs/2010ApJ...710..755G |journal=The Astrophysical Journal |volume=710 |issue=1 |pages=755–763 |arxiv=0907.4977 |bibcode=2010ApJ...710..755G |doi=10.1088/0004-637X/710/1/755 |hdl=1721.1/96091 |issn=0004-637X}}{{Cite journal |last1=Yang |first1=Yang |last2=Li |first2=Zhiyuan |last3=Sjouwerman |first3=Loránt O. |last4=Yuan |first4=Feng |last5=Shen |first5=Zhi-Qiang |date=1 August 2017 |title=Very Large Array Multiband Monitoring Observations of M31* |journal=The Astrophysical Journal |volume=845 |issue=2 |pages=140 |arxiv=1707.08317 |bibcode=2017ApJ...845..140Y |doi=10.3847/1538-4357/aa8265 |doi-access=free |issn=0004-637X}} The black hole is classified as a low-luminosity AGN (LLAGN) and it was detected only in radio wavelengths and in x-rays. It was quiescent in 2004–2005, but it was highly variable in 2006–2007. An additional x-ray flare occurred in 2013.{{Cite journal |last1=DiKerby |first1=Stephen |last2=Zhang |first2=Shuo |last3=Irwin |first3=Jimmy |date=2025-03-01 |title=Fifteen Years of M31* X-Ray Variability and Flares |journal=The Astrophysical Journal |volume=981 |issue=1 |pages=50 |arxiv=2502.01365 |bibcode=2025ApJ...981...50D |doi=10.3847/1538-4357/adb1d5 |doi-access=free |issn=0004-637X}} The mass of M31* was measured at 3–5 × 10⁷ {{Solar mass}} in 1993, and at 1.1–2.3 × 10⁸ {{Solar mass}} in 2005. The velocity dispersion of material around it is measured to be ≈ {{cvt|160|km/s|round=10|lk=on}}.

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. 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.{{Cite journal |last1=Akiba |first1=Tatsuya |last2=Madigan |first2=Ann-Marie |date=1 November 2021 |title=On the Formation of an Eccentric Nuclear Disk following the Gravitational Recoil Kick of a Supermassive Black Hole |journal=The Astrophysical Journal Letters |volume=921 |issue=1 |pages=L12 |doi=10.3847/2041-8213/ac30d9 |arxiv=2110.10163 |bibcode=2021ApJ...921L..12A |s2cid=239049969 |issn=2041-8205 |doi-access=free }} 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.

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, 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.

File:PIA20061 - Andromeda in High-Energy X-rays, Figure 1.jpg

Apparently, by late 1968, no X-rays had been detected from the Andromeda Galaxy. A balloon flight on 20 October 1970 set an upper limit for detectable hard X-rays from the Andromeda Galaxy. 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.

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. An observation campaign of NuSTAR space mission identified 40 objects of this kind in the galaxy.

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 {{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.

File:Star cluster in the Andromeda galaxy.jpg

There are approximately 460 globular clusters associated with the Andromeda Galaxy. 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. 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. The cluster with the greatest apparent brightness is G76 which is located in the southwest arm's eastern half.

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; however, other studies have shown it is actually similar in properties to Mayall II.

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.

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.

The most massive globular cluster in the Andromeda Galaxy, B023-G078, likely has a central intermediate black hole of almost 100,000 solar masses.{{cite journal | last1=Pechetti | first1=Renuka | last2=Seth | first2=Anil | last3=Kamann | first3=Sebastian | last4=Caldwell | first4=Nelson | last5=Strader | first5= Jay |title=Detection of a 100,000 M ⊙ black hole in M31's Most Massive Globular Cluster: A Tidally Stripped Nucleus |journal=The Astrophysical Journal |date=January 2022 |volume=924 |issue=2 |pages=13 |doi=10.3847/1538-4357/ac339f | arxiv=2111.08720 | bibcode=2022ApJ...924...48P | s2cid=245876938 | doi-access=free }}

{{Main|PA-99-N2}}

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.

{{Main|Andromeda's satellite galaxies}}

File:M31, the Andromeda Galaxy, Killarney Provincial Park Observatory.jpg M32 (center left above the galactic nucleus) and M110 (center right below the galaxy)]]

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.{{cite journal|doi=10.1093/mnras/stab1754|title=Solo dwarfs IV: Comparing and contrasting satellite and isolated dwarf galaxies in the Local Group|year=2021|last1=Higgs|first1=C. R.|last2=McConnachie|first2=A. W.|journal=Monthly Notices of the Royal Astronomical Society|volume=506|issue=2|pages=2766–2779|doi-access=free |arxiv=2106.12649}} 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.

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. M110 does contain a dusty lane, which may indicate recent or ongoing star formation. M32 has a young stellar population as well.

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.{{cite web |url=http://www.messier.seds.org/m/m033.html |title=Messier 33 |access-date=22 July 2024 |website=SEDS Messier Catalog}}

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.

{{Main|Andromeda–Milky Way collision}}

File:Collision paths of our Milky Way galaxy and the Andromeda galaxy.jpg

The Andromeda Galaxy is approaching the Milky Way at about {{convert|110|km|abbr=off}} per second. It has been measured approaching relative to the Sun at around {{cvt|300|km/s}} as the Sun orbits around the center of the galaxy at a speed of approximately {{cvt|225|km/s}}. This makes the Andromeda Galaxy one of about 100 observable blueshifted galaxies. 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 or possibly large disc galaxy. 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.

File:Moon over Andromeda (rotated).jpg

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.){{Cite web|last=Garner|first=Rob|date=20 February 2019|title=Messier 33 (The Triangulum Galaxy)|url=https://www.nasa.gov/feature/goddard/2019/messier-33-the-triangulum-galaxy|access-date=6 August 2021|website=NASA}}{{cite book |last=Harrington |first=Philip S. |date=2010 |title=Cosmic Challenge: The Ultimate Observing List for Amateurs |publisher=Cambridge University Press |pages=28–29 |isbn=9781139493680 |quote=But can [M81's] diffuse 7.9-magnitude glow actually be glimpsed without any optical aid? The answer is yes, but with a few important qualifications. Not only must the observing site be extraordinarily dark and completely absent of any atmospheric interferences, either natural or artificial, but the observer must have exceptionally keen vision.}}

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.

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. An amateur telescope can reveal Andromeda's disk, some of its brightest globular clusters, dark dust lanes, and the large star cloud NGC 206.

• List of Messier objects
• List of galaxies
• New General Catalogue

{{notelist

| notes =

{{efn

| name = avg dist

| 1 = average(787 ± 18, 770 ± 40, 772 ± 44, 783 ± 25) = ((787 + 770 + 772 + 783) / 4) ± (18² + 40² + 44² + 25²)^0.5 / 2 = 778 ± 33.

}}

{{efn

| name = M31VJ

| 1 = J00443799+4129236 is at celestial coordinates R.A. {{RA|00|44|37.99}}, Dec. {{DEC|+41|29|23.6}}.

}}

{{efn

| name = blue mag

| 1 = Blue absolute magnitude of −20.89 – Color index of 0.63 = −21.52

}}

{{efn

| name = bright m31

| 1 = Blue absolute magnitude of −21.58 (see reference) – Color index of 0.63 = absolute visual magnitude of −22.21

}}

}}

{{clear}}

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{{cite journal | last1=Gordon |first1=Karl D. | last2=Bailin|first2=J. | last3=Engelbracht |first3=Charles W. | display-authors=3 | last4=Rieke |first4=George H. | last5=Misselt|first5=K. A. | last6=Latter|first6=W. B. | last7=Young|first7=E. T. | last8=Ashby |first8=Matthew L. N. | last9=Barmby |first9=Pauline | last10=Gibson|first10=B. K. | last11=Hines|first11=D. C. | last12=Hinz |first12=Joannah L. | last13=Krause|first13=O. | last14=Levine|first14=D. A. | last15=Marleau|first15=F. R. | last16=Noriega-Crespo|first16=A. | last17=Stolovy|first17=S. | last18=Thilker |first18=David A. | last19=Werner|first19=M. W. | title=Spitzer MIPS Infrared Imaging of M31: Further Evidence for a Spiral-Ring Composite Structure | journal=The Astrophysical Journal | date=2006 | volume=638 | pages=L87–L92 | bibcode=2006ApJ...638L..87G | doi=10.1086/501046|arxiv = astro-ph/0601314 | issue=2 |s2cid=15495044}}

{{cite journal | last1=Block |first1=David L. | last2=Bournaud |first2=Frédéric | last3=Combes |first3=Françoise | display-authors=3 | last4=Groess |first4=Robert | last5=Barmby |first5=Pauline | last6=Ashby |first6=Matthew L. N. | last7=Fazio |first7=Giovanni G. | last8=Pahre |first8=Michael A. | last9=Willner |first9=Steven P. | title=An almost head-on collision as the origin of the two off-centre rings in the Andromeda galaxy | journal=Nature | date=2006 | volume=443 | pages=832–834 | bibcode=2006Natur.443..832B | doi=10.1038/nature05184|arxiv = astro-ph/0610543 | issue=1 | pmid=17051212|s2cid=4426420}}

{{cite news |title=Microquasar in Andromeda Galaxy Amazes Astronomers |url=http://www.sci-news.com/astronomy/article00779.html |agency= Sci-News.com |date=14 December 2012 |first= Sergio |last= Prostak}}

{{cite journal |date = 2006 |title = A 'super' star cluster grown old: the most massive star cluster in the Local Group |journal = Monthly Notices of the Royal Astronomical Society |pages =1443–1450 |volume =368 |bibcode= 2006MNRAS.368.1443M |last1=Ma|first1=Jun |last2= de Grijs |first2=Richard |last3= Yang|first3=Yanbin |display-authors=3 |last4= Zhou|first4=Xu |last5= Chen|first5=Jiansheng |last6= Jiang|first6=Zhaoji |last7= Wu|first7=Zhen-Yu |last8= Wu|first8=Jianghua |doi = 10.1111/j.1365-2966.2006.10231.x |issue = 3 |doi-access = free |arxiv = astro-ph/0602608|s2cid = 15947017}}

{{cite journal |last = Cohen|first=Judith G. |date = 2006 |title = The Not So Extraordinary Globular Cluster 037-B327 in M31 |journal = The Astrophysical Journal |pages = L21–L23 |volume = 653 |issue=1 |bibcode = 2006ApJ...653L..21C |doi = 10.1086/510384 |arxiv = astro-ph/0610863|s2cid=1733902 |url = http://authors.library.caltech.edu/7276/1/COHapjl06.pdf}}

{{cite journal |date= 2004 |title = Globular Cluster and Galaxy Formation: M31, the Milky Way, and Implications for Globular Cluster Systems of Spiral Galaxies |journal = Astrophysical Journal |pages = 158–166 |volume = 614 |issue = 1 |bibcode = 2004ApJ...614..158B |last1= Burstein|first1=David |last2= Li|first2=Yong |last3= Freeman|first3=Kenneth C. |display-authors=3 |last4= Norris|first4=John E. |last5= Bessell|first5=Michael S. |last6= Bland-Hawthorn|first6=Joss |last7= Gibson|first7=Brad K. |last8= Beasley|first8=Michael A. |last9= Lee|first9=Hyun-chul |last10=Barbuy|first10=Beatriz |last11=Huchra|first11=John P. |last12=Brodie|first12=Jean P. |last13=Forbes|first13=Duncan A. |doi = 10.1086/423334 |arxiv = astro-ph/0406564 |s2cid = 56003193}}

{{Cite journal |last1=Rudenko |first1=Pavlo |last2=Worthey |first2=Guy |last3=Mateo |first3=Mario |date=December 2009 |title=Intermediate age clusters in the field containing M31 and M32 stars |journal=The Astronomical Journal |volume=138 |issue=6 |pages=1985–1989 |bibcode=2009AJ....138.1985R |doi=10.1088/0004-6256/138/6/1985 |issn=0004-6256 |doi-access=free}}

"The median values of the Milky Way and Andromeda masses are M_G = {{val|0.8|0.4|0.3|e=12|u=solar mass}} and M_A = {{val|1.5|0.5|0.4|e=12|u=solar mass}} at a 68% level" {{cite journal | first1=Jorge |last1=Peñarrubia | first2=Yin-Zhe |last2=Ma | first3=Matthew G. |last3=Walker | first4=Alan W. |last4=McConnachie | title=A dynamical model of the local cosmic expansion | journal=Monthly Notices of the Royal Astronomical Society | volume=433 | issue=3 | date=29 July 2014 | pages=2204–2222 | bibcode= 2014MNRAS.443.2204P | doi=10.1093/mnras/stu879|doi-access=free |arxiv = 1405.0306 |s2cid=119295582}}, but compare "[we estimate] the virial mass and radius of the galaxy to be {{cvt|0.8|+/-|0.1|e12solar mass|kg|lk=on}}" {{cite journal | first1 = Prajwal R. |last1=Kafle | first2 = Sanjib |last2=Sharma | first3 = Geraint F. |last3=Lewis | display-authors=3 | first4 = Aaron S. G. |last4=Robotham | first5 = Simon P. | last5=Driver | title = The Need for Speed: Escape velocity and dynamical mass measurements of the Andromeda Galaxy | journal = Monthly Notices of the Royal Astronomical Society | volume = 475 | issue = 3 | date = 1 February 2018 | pages=4043–4054 | bibcode = 2018MNRAS.475.4043K | issn=0035-8711 | doi = 10.1093/mnras/sty082|doi-access=free |arxiv = 1801.03949 |s2cid=54039546}}

{{Cite web |date=11 March 2019 |title=Milky Way tips the scales at 1.5 trillion solar masses |url=https://astronomynow.com/2019/03/11/milky-way-tips-the-scales-at-1-5-trillion-solar-masses/ |access-date=2024-09-11 |website=Astronomy Now |language=en-US}}

{{cite journal|last1=Schiavi|first1=Riccardo|last2=Capuzzo-Dolcetta|first2=Roberto|last3=Arca-Sedda|first3=Manuel|last4=Spera|first4=Mario|title=Future merger of the Milky Way with the Andromeda galaxy and the fate of their supermassive black holes|journal=Astronomy & Astrophysics|date=October 2020|volume=642|pages=A30|doi=10.1051/0004-6361/202038674|bibcode=2020A&A...642A..30S|arxiv=2102.10938|s2cid=224991193}}

{{cite web |url=https://messierobjects101.com/messier-object-m31-m32-m110-andromeda-galaxy/ |title=M 31, M 32 & M 110 |date=15 October 2016}}

{{Cite thesis | last= Hafez | first= Ihsan | date= 2010 | title= Abd al-Rahman al-Sufi and his book of the fixed stars: a journey of re-discovery. | url= http://eprints.jcu.edu.au/28854/ | type= PhD Thesis | publisher= James Cook University | access-date= 23 June 2016 | bibcode= 2010PhDT.......295H}}

{{Cite book |last=Kant |first=Immanuel |author-link=Immanuel Kant |url=https://archive.org/details/universalnatural0000kant |title=Universal natural history and theory of the heavens |date=1969 |publisher=University of Michigan Press}}

{{Cite journal |last=Roberts |first=I. |year=1888 |title=Photographs of the Nebulae M 31, h 44, and h 51 Andromedae, and M 27 Vulpeculae |journal=Monthly Notices of the Royal Astronomical Society |language=en |volume=49 |issue=2 |pages=65–66 |bibcode=1888MNRAS..49...65R |doi=10.1093/mnras/49.2.65 |issn=0035-8711 |doi-access=free}}

{{Cite web|url=https://www.space.com/15590-andromeda-galaxy-m31.html|title=The Andromeda Galaxy (M31): Location, Characteristics & Images|website=Space.com|date=10 January 2018 }}

{{Cite web|url=https://www.sciencephoto.com/media/480378/view/andromeda-galaxy-19th-century|title=Andromeda Galaxy, 19th century – Stock Image – C014/5148|first=ROYAL ASTRONOMICAL SOCIETY/SCIENCE PHOTO|last=LIBRARY|website=Science Photo Library}}

{{cite web|title=Hubble Finds Giant Halo Around the Andromeda Galaxy|url=http://www.spacetelescope.org/images/opo1515a/|access-date=14 June 2015}}

{{Cite journal |arxiv = 1801.03949|doi = 10.1093/mnras/sty082|title = The need for speed: Escape velocity and dynamical mass measurements of the Andromeda galaxy|journal = Monthly Notices of the Royal Astronomical Society|volume = 475|issue = 3|pages = 4043–4054|year = 2018|last1 = Kafle|first1 = Prajwal R.|last2 = Sharma|first2 = Sanjib|last3 = Lewis|first3 = Geraint F.|last4 = Robotham|first4 = Aaron S G.|last5 = Driver|first5 = Simon P.| doi-access=free |bibcode = 2018MNRAS.475.4043K|s2cid = 54039546}}

{{cite web|url=https://www.icrar.org/cosmic-collision/|title=Milky Way ties with neighbour in galactic arms race|date=15 February 2018}}

{{cite web|url=https://www.space.com/39751-andromeda-galaxy-not-bigger-than-milky-way.html|title=The Andromeda Galaxy Is Not Bigger Than the Milky Way After All|first1=Samantha Mathewson 2018-02-20T19:05:26Z|last1=Science|last2=Astronomy|website=Space.com|date=20 February 2018 }}

{{cite journal|title=The Need for Speed: Escape velocity and dynamical mass measurements of the Andromeda galaxy|year=2018|doi=10.1093/mnras/sty082|arxiv=1801.03949|last1=Kafle|first1=Prajwal R.|last2=Sharma|first2=Sanjib|last3=Lewis|first3=Geraint F.|last4=Robotham|first4=Aaron S G.|last5=Driver|first5=Simon P.|journal=Monthly Notices of the Royal Astronomical Society|volume=475|issue=3|pages=4043–4054|doi-access=free |bibcode=2018MNRAS.475.4043K|s2cid=54039546}}

{{Cite web|url=https://scitechdaily.com/hubble-gaia-reveal-weight-of-the-milky-way-1-5-trillion-solar-masses/|title=Hubble & Gaia Reveal Weight of the Milky Way: 1.5 Trillion Solar Masses|first1=Bethany|last1=Downer|first2=ESA/Hubble|last2=Telescope|date=10 March 2019}}

{{Cite web|title = HubbleSite – NewsCenter – Hubble Finds Giant Halo Around the Andromeda Galaxy (05/07/2015) – The Full Story|url = http://hubblesite.org/newscenter/archive/releases/2015/15/full/|website = hubblesite.org|access-date = 7 May 2015}}

{{Cite web |title = Hubble finds massive halo around the Andromeda Galaxy |url = https://news.nd.edu/news/hubble-finds-halo-around-the-andromeda-galaxy/ |website = University of Notre Dame News |date = 7 May 2015 |first=Marissa |last=Gebhard}}

{{Cite journal |title = Evidence for a Massive, Extended Circumgalactic Medium Around the Andromeda Galaxy |journal = The Astrophysical Journal |arxiv = 1404.6540 |date = 25 April 2014 |first1 = Nicolas |last1 = Lehner |first2 = Chris |last2 = Howk |first3 = Bart |last3 = Wakker |doi=10.1088/0004-637x/804/2/79 |bibcode=2015ApJ...804...79L |volume=804 |issue = 2 |pages=79 |s2cid = 31505650}}

{{Cite web|title = NASA's Hubble Finds Giant Halo Around the Andromeda Galaxy |url = http://www.nasa.gov/feature/goddard/nasa-s-hubble-finds-giant-halo-around-the-andromeda-galaxy|access-date = 7 May 2015|date = 7 May 2015}}

{{cite journal |doi=10.1088/0004-637X/736/2/84 |title=The Mid-life Crisis of the Milky Way and M31 |date=2011 |last1=Mutch |first1=Simon J. |last2=Croton | first2=Darren J. |last3=Poole | first3=Gregory B. |journal=The Astrophysical Journal |volume=736 |issue=2 |bibcode = 2011ApJ...736...84M |arxiv = 1105.2564 |pages=84 |s2cid=119280671}}

{{cite web|title=Andromeda Galaxy Scanned with High-Energy X-ray Vision|website = Jet Propulsion Laboratory|url=https://www.jpl.nasa.gov/news/news.php?feature=4811 |date=5 January 2016 |access-date=22 September 2018}}

{{cite web|title=Star cluster in the Andromeda galaxy|url=http://www.spacetelescope.org/images/opo1518a/ |publisher=ESA |date=4 September 2015 |access-date=7 September 2015}}

{{cite journal | last1=An | first1=Jin H. | last2=Evans | first2=N. W. | last3=Kerins | first3=E. | last4=Baillon | first4=P. | last5=Calchi Novati | first5=S. | last6=Carr | first6=B. J. | last7=Creze | first7=M. | last8=Giraud-Heraud | first8=Y. | last9=Gould | first9=A. | last10=Hewett | first10=P. | last11=Jetzer | first11=Ph. | last12=Kaplan | first12=J. | last13=Paulin-Henriksson | first13=S. | last14=Smartt | first14=S. J. | last15=Tsapras | first15=Y. | last16=Valls-Gabaud | first16=D. | title=The Anomaly in the Candidate Microlensing Event PA-99-N2 | journal=The Astrophysical Journal | volume=601 | issue=2 | year=2004 | issn=0004-637X | doi=10.1086/380820 | pages=845–857| arxiv=astro-ph/0310457 | bibcode=2004ApJ...601..845A | s2cid=8312033 }}

{{cite web|url=http://www.spaceanswers.com/deep-space/apart-from-andromeda-are-any-other-galaxies-moving-towards-us/|title=Apart from Andromeda, are any other galaxies moving towards us? |first=Jonathan |last=O'Callaghan |date=14 May 2018 |work=Space Facts |access-date=3 April 2016}}

{{cite web|url=https://starchild.gsfc.nasa.gov/docs/StarChild/questions/question15.html|title=Can you see other galaxies without a telescope?|website=starchild.gsfc.nasa.gov}}

{{cite news|url=http://www.skyandtelescope.com/observing/how-to-see-the-farthest-thing-you-can-see090920150909/|title=How to See the Farthest Thing You Can See |work=Sky & Telescope |first=Bob |last=King |date=9 September 2015}}

{{cite web |title=Observing the Andromeda Galaxy |url=http://www.physics.ucla.edu/~huffman/m31.html |website=University of California}}

{{cite news|url=http://www.skyandtelescope.com/observing/watch-andromeda-blossom-in-binoculars091620151609/|title=Watch Andromeda Blossom in Binoculars |work=Sky & Telescope |first=Bob |last=King |date=16 September 2015}}

{{cite web|url=http://www.backyard-astro.com/focusonarchive/m31/m31.html#Anchor-11481|title=Observing M31, the Andromeda Galaxy|access-date=5 October 2016|archive-date=5 August 2020|archive-url=https://web.archive.org/web/20200805132930/http://backyard-astro.com/focusonarchive/m31/m31.html#Anchor-11481|url-status=dead}}

{{Cite web|url=https://www.astronomy-mall.com/Adventures.In.Deep.Space/gcm31.htm|title=Globular Clusters in the Andromeda Galaxy|website=www.astronomy-mall.com}}

}}

{{Commons}}

• {{WikiSky|name=The Andromeda Galaxy}}
• [https://web.archive.org/web/20110722021459/http://blackholes.stardate.org/directory/factsheet.php?p=M31 StarDate: M31 Fact Sheet]
• [http://www.messier.seds.org/m/m031.html Messier 31, SEDS Messier pages]
• Astronomy Picture of the Day
• [https://apod.nasa.gov/apod/ap981017.html A Giant Globular Cluster in M31] 1998 October 17.
• [https://apod.nasa.gov/apod/ap040718.html M31: The Andromeda Galaxy] 2004 July 18.
• [https://apod.nasa.gov/apod/ap051222.html Andromeda Island Universe] 2005 December 22.
• [https://apod.nasa.gov/apod/ap100109.html Andromeda Island Universe] 2010 January 9.
• [https://apod.nasa.gov/apod/ap100219.html WISE Infrared Andromeda] 2010 February 19.
• [https://apod.nasa.gov/apod/ap130801.html M31's angular size compared with full Moon] 2013 August 1.
• [http://www.beskeen.com/gallery/galaxy/m31/m31.shtml M31 and its central Nuclear Spiral]
• [http://www.starpointing.com/ccd/m31.html Amateur photography – M31]
• [http://astro.neutral.org/imagehtml/20050903_m31.html Globular Clusters in M31] at The Curdridge Observatory
• [https://web.archive.org/web/20181116120359/http://www.astronomy.com/news/2005/11/first-direct-distance-to-andromeda First direct distance to Andromeda] − Astronomy magazine article
• [http://www.solstation.com/x-objects/andromeda.htm Andromeda Galaxy] at SolStation.com
• [https://www.daviddarling.info/encyclopedia/A/Andromeda.html Andromeda Galaxy at The Encyclopedia of Astrobiology, Astronomy, & Spaceflight]
• [http://www.nightskyinfo.com/archive/m31_galaxy M31, the Andromeda Galaxy] at NightSkyInfo.com
• {{cite news |last=Than |first=Ker |title=Strange Setup: Andromeda's Satellite Galaxies All Lined Up |url=http://space.com/scienceastronomy/060123_andromeda_plane.html |work=Space.com |date=23 January 2006}}
• [https://web.archive.org/web/20110719204305/http://cbat.eps.harvard.edu/CBAT_M31.html M31 (Apparent) Novae Page] (IAU)
• [http://herschel.esac.esa.int/Images/2011/M31_COMPO_A.jpg Multi-wavelength composite]
• [https://www.zooniverse.org/projects/zooniverse/andromeda-project Andromeda Project] (crowd-source)
• {{cite web |title=M31 – Andromeda Galaxy|url=http://www.deepskyvideos.com/videos/messier/M31_andromeda.html |work=Deep Sky Videos |publisher=Brady Haran |last1=Gray |first1=Meghan| last2=Szymanek |first2=Nik |author2-link=Nik Szymanek |last3=Merrifield |first3=Michael}}
• [https://hubblesite.org/contents/news-releases/2015/news-2015-02.html Hubble's High-Definition Panoramic View of the Andromeda Galaxy]
• [https://hubblesite.org/contents/media/images/2022/027/01G4NM6207PRA9YES60C5RKKA5 Infrared-Radio Image of the Andromeda Galaxy (M31)]
• [https://rockchucksummit.com/m31-andromeda-galaxy/ Creative Commons Astrophotography M31 Andromeda image download & processing guide]

{{Andromeda galaxy}}

{{Messier objects}}

{{NGC objects:1-499}}

{{Stars of Andromeda}}

{{Authority control}}

{{Portal bar|Astronomy|Stars|Outer space}}

{{Good article}}

{{Sky|00|42|44.3|+|41|16|9|2540000}}

{{DEFAULTSORT:Andromeda Galaxy}}

Category:Andromeda (constellation)

Category:Andromeda Subgroup

Category:Articles containing video clips

Category:Astronomical objects known since antiquity

Category:Barred spiral galaxies

00400+4059

Category:Local Group

+07-02-016

Category:Messier objects

Category:NGC objects

002557

00454