# Andromeda Galaxy

Andromeda Galaxy
The Andromeda Galaxy
Observation data (J2000 epoch)
Pronunciation /ænˈdrɒmɪdə/
Constellation Andromeda
Right ascension 00h 42m 44.3s[1]
Declination +41° 16′ 9″[1]
Redshift z = −0.001001
(minus sign
indicates blueshift)[1]
Helio radial velocity −301 ± 1 km/s[2]
Distance 2.54 ± 0.11 Mly
(778 ± 33 kpc)[2][3][4][5][6][a]
Apparent magnitude (V) 3.44[7][8]
Absolute magnitude (V) −21.5[b][4]
Characteristics
Type SA(s)b[1]
Mass

~0.8-1.5×1012[9]

[10] M
Number of stars ~1 trillion (1012)[12]
Size ~220 kly (diameter)[11]
Apparent size (V) 3.167° × 1°[1]
Other designations
M31, NGC 224, UGC 454, PGC 2557, 2C 56 (Core),[1] CGCG 535-17, MCG +07-02-016, IRAS 00400+4059, 2MASX J00424433+4116074, GC 116, h 50, Bode 3, Flamsteed 58, Hevelius 32, Ha 3.3, IRC +40013

The Andromeda Galaxy (/ænˈdrɒmɪdə/), also known as Messier 31, M31, or NGC 224, is a spiral galaxy approximately 780 kiloparsecs (2.5 million light-years) from Earth, and the nearest major galaxy to the Milky Way.[4] Its name stems from the area of the sky in which it appears, the constellation of Andromeda.

The 2006 observations by the Spitzer Space Telescope revealed that the Andromeda Galaxy contains approximately one trillion stars,[10] more than twice the number of the Milky Way's estimated 200 to 400 billion stars.,[13] though a 2018 study found that the Andromeda Galaxy's mass is roughly the same as the Milky Way's.[14] The Andromeda Galaxy, spanning approximately 220,000 light-years, is the largest galaxy in our Local Group, which is also home to the Triangulum Galaxy and other minor galaxies. The Andromeda Galaxy's mass is estimated to be around 1.76 times that of the Milky Way Galaxy (~0.8-1.5×1012 solar masses [9][10] vs the Milky Way's 8.5×1011 solar masses).

The Milky Way and Andromeda galaxies are expected to collide in ~4.5 billion years, merging to form a giant elliptical galaxy[15] or a large disc galaxy.[16] With an apparent magnitude of 3.4, the Andromeda Galaxy is among the brightest of the Messier objects[17]—making it visible to the naked eye on moonless nights,[18] even when viewed from areas with moderate light pollution.

## Observation history

Great Andromeda Nebula by Isaac Roberts, 1899.

Around the year 964, the Persian astronomer Abd al-Rahman al-Sufi described the Andromeda Galaxy, in his Book of Fixed Stars as a "nebulous smear".[19]

Star charts of that period labeled it as the Little Cloud.[20] In 1612, the German astronomer Simon Marius gave an early description of the Andromeda Galaxy based on telescopic observations.[21] The German philosopher Immanuel Kant in 1755 in his work Universal Natural History and Theory of the Heavens conjectured that the blurry spot was an island universe. In 1764, Charles Messier cataloged Andromeda as object M31 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 is no more than 2,000 times the distance of Sirius.[22] In 1850, William Parsons, 3rd Earl of Rosse, saw and made the first drawing of Andromeda's spiral structure.

In 1864, William Huggins noted that the spectrum of Andromeda differs from a gaseous nebula.[23] The spectra 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 Andromeda was considered to be a nearby object, so the cause was thought to be a much less luminous and unrelated event called a nova, and was named accordingly; "Nova 1885".[24]

In 1887, Isaac Roberts took 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 solar systems being formed.[citation needed] In 1912, Vesto Slipher used spectroscopy to measure the radial velocity of Andromeda with respect to our Solar System—the largest velocity yet measured, at 300 kilometres per second (190 miles per second).[25]

### Island universe

Location of the Andromeda Galaxy (M31) in the Andromeda constellation.

In 1917, Heber Curtis observed a nova within Andromeda. 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 500,000 light-years (3.2×1010 AU). He became a proponent of the so-called "island universes" hypothesis, which held that spiral nebulae were actually independent galaxies.[26]

Andromeda Galaxy above the Very Large Telescope.[27] The Triangulum Galaxy is visible on the top.

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 of the Great Andromeda Nebula being, in fact, an external galaxy, Curtis also noted the appearance of dark lanes within Andromeda which resembled the dust clouds in our own galaxy, as well as historical observations of 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 450,000 parsecs (1,500,000 light-years).[28] 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 2.5-metre (8 ft 2 in) Hooker telescope, and they enabled the distance of 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.[29]

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.)[30] Baade also discovered that there were two types of Cepheid variables, which resulted in a doubling of the distance estimate to Andromeda, as well as the remainder of the Universe.[31]

In 1950, radio emission from the Andromeda Galaxy was detected by Hanbury Brown and Cyril Hazard at Jodrell Bank Observatory.[32][33] The first radio maps of the galaxy were made in the 1950s by John Baldwin and collaborators at the Cambridge Radio Astronomy Group.[34] The core of the Andromeda Galaxy is called 2C 56 in the 2C radio astronomy catalog. In 2009, the first planet may have been discovered in the Andromeda Galaxy. This was detected using a technique called microlensing, which is caused by the deflection of light by a massive object.[35]

## General

The estimated distance of the Andromeda Galaxy from our own was doubled in 1953 when it was discovered that there is another, dimmer type of Cepheid. 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.[36][37]

### Formation and history

The Andromeda Galaxy as seen by NASA's Wide-field Infrared Survey Explorer.

The Andromeda Galaxy was formed roughly 10 billion years ago from the collision and subsequent merger of smaller protogalaxies.[38]

This violent collision formed most of the galaxy's (metal-rich) galactic halo and extended disk. 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. Andromeda and the Triangulum Galaxy had a very close passage 2–4 billion years ago. This event produced high rates of star formation across the Andromeda Galaxy's disk—even some globular clusters—and disturbed M33's outer disk.

Over the past 2 billion years, star formation throughout Andromeda's disk is thought to have decreased to the point of near-inactivity. There have been interactions with satellite galaxies like M32, M110, or others that have already been absorbed by Andromeda Galaxy. These interactions have formed structures like Andromeda's Giant Stellar Stream. A galactic merger roughly 100 million years ago is believed to be responsible for a counter-rotating disk of gas found in the center of Andromeda as well as the presence there of a relatively young (100 million years old) stellar population.[citation needed]

### Distance estimate

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 2.57 ± 0.06 million light-years (1.625×1011 ± 3.8×109 astronomical units) was derived. A 2004 Cepheid variable method estimated the distance to be 2.51 ± 0.13 million light-years (770 ± 40 kpc).[2][3] In 2005, an eclipsing binary star was discovered in the Andromeda Galaxy. The binary[c] is 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 measured. The stars lie at a distance of 2.52×106 ± 0.14×106 ly (1.594×1011 ± 8.9×109 AU) and the whole Andromeda Galaxy at about 2.5×106 ly (1.6×1011 AU).[4] 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 2.56×106 ± 0.08×106 ly (1.619×1011 ± 5.1×109 AU).[5] Averaged together, these distance estimates give a value of 2.54×106 ± 0.11×106 ly (1.606×1011 ± 7.0×109 AU).[a] And, from this, the diameter of Andromeda at the widest point is estimated to be 220 ± 3 kly (67,450 ± 920 pc).[original research?] Applying trigonometry (angular diameter), this is equivalent to an apparent 4.96° angle in the sky.

### Mass and luminosity estimates

#### Mass

The Andromeda Galaxy pictured in ultraviolet light by GALEX.
Illustration showing both the size of each galaxy and the distance between the two galaxies, to scale.
Giant halo around Andromeda Galaxy.[39]

Mass estimates for the Andromeda Galaxy's halo (including dark matter) give a value of approximately 1.5×1012 M[10] (or 1.5 trillion solar masses) compared to 8×1011 M for the Milky Way. This contradicts earlier measurements, that seem to indicate that Andromeda Galaxy and the Milky Way are almost equal in mass. Even so, Andromeda Galaxy's spheroid actually has a higher stellar density than that of the Milky Way[40] and its galactic stellar disk is about twice the size of that of the Milky Way.[11] The total stellar mass of Andromeda Galaxy is estimated to be between 1.1×1011 M.,[41][42] (i.e., around twice as massive as that of the Milky Way) and 1.5×1011 M, with around 30% of that mass in the central bulge, 56% in the disk, and the remaining 14% in the halo.[43]

In addition to it, Andromeda Galaxy's interstellar medium contains at least around 7.2×109 M[44] in the form of neutral hydrogen, at least 3.4×108 M as molecular hydrogen (within its innermost 10 kiloparsecs), and 5.4×107 M of dust.[45]

Andromeda Galaxy is surrounded by a large and 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 Andromeda Galaxy's star-filled disk and eject these heavier elements into space. Over 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.[46][47][48][49][50]

#### Luminosity

Compared to the Milky Way, the Andromeda Galaxy appears to have predominantly older stars with ages >7×109 years.[43][clarification needed] The estimated luminosity of Andromeda Galaxy, ~2.6×1010 L, is about 25% higher than that of our own galaxy.[51] 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 mega-parsecs of the Milky Way, after the Sombrero Galaxy,[52] with an absolute magnitude of around -22.21[d] or close[53]).

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,[b] compared to −20.9 for the Milky Way), and a total luminosity in that wavelength of 3.64×1010 L.[54]

The rate of star formation in the Milky Way is much higher, with 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 Andromeda Galaxy.[55] 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.[51] Should this continue, the luminosity of the Milky Way may eventually overtake that of Andromeda Galaxy.

According to recent studies, the Andromeda Galaxy lies in what in the galaxy color–magnitude diagram is known 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 Andromeda Galaxy, star formation is expected to extinguish within about five billion years from the now, even accounting for the expected, short-term increase in the rate of star formation due to the collision between Andromeda Galaxy and the Milky Way.[56]

## Structure

The Andromeda Galaxy seen in infrared by the Spitzer Space Telescope, one of NASA's four Great Space Observatories.
Image of the Andromeda Galaxy taken by Spitzer in infrared, 24 micrometres (Credit:NASA/JPLCaltech/K. Gordon, University of Arizona).
A Swift Tour of Andromeda Galaxy.
A Galaxy Evolution Explorer image of the Andromeda Galaxy. The bands of blue-white making up the galaxy's striking rings are neighborhoods that harbor hot, young, massive stars. Dark blue-grey lanes of cooler dust show up starkly against these bright rings, tracing the regions where star formation is currently taking place in dense cloudy cocoons. When observed in visible light, Andromeda Galaxy's rings look more like spiral arms. The ultraviolet view shows that these arms more closely resemble the ring-like structure previously observed in infrared wavelengths with NASA's Spitzer Space Telescope. Astronomers using the latter interpreted these rings as evidence that the galaxy was involved in a direct collision with its neighbor, M32, more than 200 million years ago.

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.[1] However, data from the 2MASS survey showed that Andromeda is actually a barred spiral galaxy, like the Milky Way, with Andromeda's bar oriented along its long axis.[57]

In 2005, astronomers used the Keck telescopes to show that the tenuous sprinkle of stars extending outward from the galaxy is actually part of the main disk itself.[11] This means that the spiral disk of stars in the Andromeda Galaxy is three times larger in diameter than previously estimated. This constitutes evidence that there is a vast, extended stellar disk that makes the galaxy more than 220,000 light-years (67,000 parsecs) in diameter. Previously, estimates of the Andromeda Galaxy's size ranged from 70,000 to 120,000 light-years (21,000 to 37,000 pc) across.

The galaxy is inclined an estimated 77° relative to Earth (where an angle of 90° would be viewed directly from the side). Analysis of the cross-sectional shape of the galaxy appears to demonstrate a pronounced, S-shaped warp, rather than just a flat disk.[58] 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 225 kilometres per second (140 mi/s) at 1,300 light-years (82,000,000 astronomical units) from the core, and it has its minimum possibly as low as 50 kilometres per second (31 mi/s) at 7,000 light-years (440,000,000 AU) from the core. Further out, rotational velocity rises out to a radius of 33,000 light-years (2.1×109 AU), where it reaches a peak of 250 kilometres per second (160 mi/s). The velocities slowly decline beyond that distance, dropping to around 200 kilometres per second (120 mi/s) at 80,000 light-years (5.1×109 AU). These velocity measurements imply a concentrated mass of about 6×109 M in the nucleus. The total mass of the galaxy increases linearly out to 45,000 light-years (2.8×109 AU), then more slowly beyond that radius.[59]

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.[60] His descriptions of the spiral structure, as each arm crosses the major axis of the Andromeda Galaxy, are as follows[61]§pp1062[62]§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 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 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 13,000 light-years (820,000,000 astronomical units) and that can be followed outward from a distance of roughly 1,600 light-years (100,000,000 AU) from the core. Alternative spiral structures have been proposed such as a single spiral arm[63] or a flocculent[64] pattern of long, filamentary, and thick spiral arms.[1][65]

The most likely cause of the distortions of the spiral pattern is thought to be interaction with galaxy satellites M32 and M110.[66] This can be seen by the displacement of the neutral hydrogen clouds from the stars.[67]

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 is generally formed into several overlapping rings, with a particularly prominent ring formed at a radius of 32,000 light-years (2.0×109 AU) (10 kiloparsecs) from the core,[68] nicknamed by some astronomers the ring of fire.[69] 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.[70]

Later studies with the help of the Spitzer Space Telescope showed how 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.[66]

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.[71] 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.[72]

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.[40] 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.[73] 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.

## Nucleus

Hubble image of the Andromeda Galaxy core showing possible double structure. NASA/ESA photo.

M31 is known to harbor a dense and compact star cluster at its very center. In a large telescope it creates a visual impression of a star embedded in the more diffuse surrounding bulge. In 1991, the Hubble Space Telescope was used to image Andromeda Galaxy's inner nucleus. The nucleus consists of two concentrations separated by 1.5 parsecs (4.9 ly). 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 a black hole measured at 3–5 × 107 M in 1993,[74] and at 1.1–2.3 × 108 M in 2005.[75] The velocity dispersion of material around it is measured to be ≈ 160 km/s.[76]

Chandra X-ray telescope image of the center of Andromeda Galaxy. A number of X-ray sources, likely X-ray binary stars, within the galaxy's central region appear as yellowish dots. The blue source at the center is at the position of the supermassive black hole.

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.[77] The eccentricity is such that stars linger at the orbital apocenter, creating a concentration of stars. 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.[78]

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 Andromeda Galaxy,[79] 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.[77]

## Discrete sources

The Andromeda Galaxy in high-energy X-ray and ultraviolet light (released 5 January 2016).
Artist's concept of the Andromeda Galaxy core showing a view across a disk of young, blue stars encircling a supermassive black hole. NASA/ESA photo.

Apparently, by late 1968, no X-rays had been detected from the Andromeda Galaxy.[80] A balloon flight on October 20, 1970, set an upper limit for detectable hard X-rays from the Andromeda Galaxy.[81]

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. The spectrum of the neutron stars is the same as the hypothesized black holes but can be distinguished by their masses.[82]

There are approximately 460 globular clusters associated with the Andromeda Galaxy.[83] 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.[84] It contains several million stars, and is about twice as luminous as Omega Centauri, the brightest known globular cluster in the Milky Way. Globular One (or G1) has several stellar populations and a structure too massive for an ordinary globular. As a result, some consider G1 to be the remnant core of a dwarf galaxy that was consumed by Andromeda in the distant past.[85] The globular with the greatest apparent brightness is G76 which is located in the south-west arm's eastern half.[20] Another massive globular cluster, named 037-B327 and discovered in 2006 as is heavily reddened by the Andromeda Galaxy's interstellar dust, was thought to be more massive than G1 and the largest cluster of the Local Group;[86] however, other studies have shown it is actually similar in properties to G1.[87]

Star clusters in the Andromeda Galaxy.[88]

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.[89]

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.[90]

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 ${\displaystyle {\begin{smallmatrix}M_{\odot }\end{smallmatrix}}}$. Discovered through a data collected by the European Space Agency's XMM-Newton probe, and 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.[91]

## Satellites

Messier 32 is to the left of the center, Messier 110 is to the bottom-right of the center.

Like the Milky Way, the Andromeda Galaxy has satellite galaxies, consisting of 14 known dwarf galaxies. 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.[92]

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.[93] M110 does contain a dusty lane, which may indicate recent or ongoing star formation.[94]

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.[95]

## Collision with the Milky Way

The Andromeda Galaxy is approaching the Milky Way at about 110 kilometres per second (68 miles per second).[96] It has been measured approaching relative to our Sun at around 300 km/s (190 mi/s)[1] as the Sun orbits around the center of our galaxy at a speed of approximately 225 km/s (140 mi/s). This makes the Andromeda Galaxy one of about 100 observable blueshifted galaxies.[97] Andromeda Galaxy's tangential or sideways velocity with respect to 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 4 billion years. A likely outcome of the collision is that the galaxies will merge to form a giant elliptical galaxy[98] or perhaps even a large disc galaxy.[16] Such events are frequent among the galaxies in galaxy groups. The fate of the 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.[99]

## Amateur observing

The Andromeda Galaxy is bright enough to be seen with the naked eye, even with some light pollution.[100] Andromeda is best seen during autumn nights in the Northern Hemisphere, when from mid-latitudes the galaxy reaches zenith (its highest point at midnight) so can be seen almost all night. From the Southern Hemisphere, it is most visible at the same months, that is in spring, and away from our equator does not reach a high altitude over the northern horizon, making it difficult to observe. Binoculars can reveal some larger structures and its two brightest satellite galaxies, M32 and M110.[101] An amateur telescope can reveal Andromeda's disk, some of its brightest globular clusters, dark dust lanes and the large star cloud NGC 206.[102][103]

## Notes

1. ^ a b average(787 ± 18, 770 ± 40, 772 ± 44, 783 ± 25) = ((787 + 770 + 772 + 783) / 4) ± (182 + 402 + 442 + 252)0.5 / 2 = 778 ± 33.
2. ^ a b Blue absolute magnitude of −20.89 – Color index of 0.63 = −21.52
3. ^ J00443799+4129236 is at celestial coordinates R.A. 00h 44m 37.99s, Dec. +41° 29′ 23.6″.
4. ^ Blue absolute magnitude of −21.58 (see reference) – Color index of 0.63 = absolute visual magnitude of −22.21

## References

1. "Results for Messier 31". NASA/IPAC Extragalactic Database. NASA/IPAC. Retrieved 2006-11-01.
2. ^ a b c Karachentsev, I. D.; Kashibadze, O. G. (2006). "Masses of the Local Group and of the M81 group estimated from distortions in the local velocity field". Astrophysics. 49 (1): 3–18. Bibcode:2006Ap.....49....3K. doi:10.1007/s10511-006-0002-6.
3. ^ a b Karachentsev, I. D.; et al. (2004). "A Catalog of Neighboring Galaxies". Astronomical Journal. 127 (4): 2031–2068. Bibcode:2004AJ....127.2031K. doi:10.1086/382905.
4. ^ a b c d Ribas, I.; et al. (2005). "First Determination of the Distance and Fundamental Properties of an Eclipsing Binary in the Andromeda Galaxy". Astrophysical Journal Letters. 635 (1): L37–L40. arXiv:. Bibcode:2005ApJ...635L..37R. doi:10.1086/499161.
5. ^ a b McConnachie, A. W.; et al. (2005). "Distances and metallicities for 17 Local Group galaxies". Monthly Notices of the Royal Astronomical Society. 356 (4): 979–997. arXiv:. Bibcode:2005MNRAS.356..979M. doi:10.1111/j.1365-2966.2004.08514.x.
6. ^ Jensen, J. B.; et al. (2003). "Measuring Distances and Probing the Unresolved Stellar Populations of Galaxies Using Infrared Surface Brightness Fluctuations". Astrophysical Journal. 583 (2): 712–726. arXiv:. Bibcode:2003ApJ...583..712J. doi:10.1086/345430.
7. ^ "M 31".
8. ^ Armando, G. P.; et al. (2007). "The GALEX Ultraviolet Atlas of Nearby Galaxies". Astrophysical Journal. 173 (2): 185–255. arXiv:. Bibcode:2007ApJS..173..185G. doi:10.1086/516636.
9. ^ a b Prajwal R. Kafle; Sanjib Sharma; Geraint F. Lewis; Aaron S. G. Robotham (1 February 2018). "The Need for Speed: Escape velocity and dynamical mass measurements of the Andromeda Galaxy". Monthly Notices of the Royal Astronomical Society (3): 66. arXiv:. Bibcode:2018MNRAS.475.4043K. doi:10.1093/mnras/sty082.
10. ^ a b c d Jorge Peñarrubia; Yin-Zhe Ma; Matthew G. Walker; Alan McConnachie (29 July 2014). "A dynamical model of the local cosmic expansion". Monthly Notices of the Royal Astronomical Society. 433 (3): 2204–2222. arXiv:. Bibcode:2014MNRAS.443.2204P. doi:10.1093/mnras/stu879.
11. ^ a b c Chapman, S. C.; et al. (2006). "A kinematically selected, metal-poor spheroid in the outskirts of M31". Astrophysical Journal. 653 (1): 255–266. arXiv:. Bibcode:2006ApJ...653..255C. doi:10.1086/508599. Also see the press release, "Andromeda's Stellar Halo Shows Galaxy's Origin to Be Similar to That of Milky Way" (Press release). Caltech Media Relations. February 27, 2006. Archived from the original on 9 May 2006. Retrieved 2006-05-24.
12. ^ Young, K. (June 6, 2006). "The Andromeda Galaxy hosts a trillion stars". New Scientist. Retrieved 2014-10-06.
13. ^ Frommert, H.; Kronberg, C. (August 25, 2005). "The Milky Way Galaxy". SEDS. Archived from the original on 2007-05-12. Retrieved 2007-05-09.
14. ^ Kafle, Prajwal R.; Sharma, Sanjib; Lewis, Geraint F.; Robotham, Aaron S. G.; Driver, Simon P. (2018-04-11). "The Need for Speed: Escape velocity and dynamical mass measurements of the Andromeda galaxy". Monthly Notices of the Royal Astronomical Society. 475 (3): 4043–4054. doi:10.1093/mnras/sty082. ISSN 0035-8711.
15. ^ "NASA's Hubble Shows Milky Way is Destined for Head-On Collision". NASA. 31 May 2012. Archived from the original on 4 June 2014. Retrieved 12 July 2012.
16. ^ a b Ueda, Junko; et al. "Cold molecular gas in merger remnants. I. Formation of molecular gas disks". The Astrophysical Journal Supplement Series. 214 (1). arXiv:. Bibcode:2014ApJS..214....1U. doi:10.1088/0067-0049/214/1/1.
17. ^ Frommert, H.; Kronberg, C. (August 22, 2007). "Messier Object Data, sorted by Apparent Visual Magnitude". SEDS. Archived from the original on 2007-07-12. Retrieved 2007-08-27.
18. ^ "M 31, M 32 & M 110". 15 October 2016.
19. ^ Hafez, Ihsan (2010). "Abd al-Rahman al-Sufi and his book of the fixed stars: a journey of re-discovery". Ph.D. thesis, James Cook University. Retrieved June 23, 2016.
20. ^ a b Kepple, G. R.; Sanner, G. W. (1998). The Night Sky Observer's Guide. Vol. 1. Willmann-Bell. p. 18. ISBN 978-0-943396-58-3.
21. ^ Davidson, Norman (1985). Astronomy and the imagination: a new approach to man's experience of the stars. Routledge Kegan & Paul. p. 203. ISBN 978-0-7102-0371-7.
22. ^ Herschel, W. (1785). "On the Construction of the Heavens". Philosophical Transactions of the Royal Society of London. 75 (0): 213–266. doi:10.1098/rstl.1785.0012.
23. ^ Huggins, W.; Miller, W. A. (1864). "On the Spectra of Some of the Nebulae". Philosophical Transactions of the Royal Society of London. 154 (0): 437–444. Bibcode:1864RSPT..154..437H. doi:10.1098/rstl.1864.0013.
24. ^ Backhouse, T. W. (1888). "nebula in Andromeda and Nova, 1885". Monthly Notices of the Royal Astronomical Society. 48: 108–110. Bibcode:1888MNRAS..48..108B. doi:10.1093/mnras/48.3.108.
25. ^ Slipher, V. M. (1913). "The Radial Velocity of the Andromeda Nebula". Lowell Observatory Bulletin. 1: 56–57. Bibcode:1913LowOB...2...56S.
26. ^ Curtis, H. D. (1988). "Novae in Spiral Nebulae and the Island Universe Theory". Publications of the Astronomical Society of the Pacific. 100: 6. Bibcode:1988PASP..100....6C. doi:10.1086/132128.
27. ^ "Two naked-eye galaxies above the VLT". ESO Picture of the Week. Retrieved 22 October 2013.
28. ^ Öpik, E. (1922). "An estimate of the distance of the Andromeda Nebula". Astrophysical Journal. 55: 406–410. Bibcode:1922ApJ....55..406O. doi:10.1086/142680.
29. ^ Hubble, E. P. (1929). "A spiral nebula as a stellar system, Messier 31". Astrophysical Journal. 69: 103–158. Bibcode:1929ApJ....69..103H. doi:10.1086/143167.
30. ^ Baade, W. (1944). "The Resolution of Messier 32, NGC 205, and the Central Region of the Andromeda Nebula". Astrophysical Journal. 100: 137. Bibcode:1944ApJ...100..137B. doi:10.1086/144650.
31. ^ Gribbin, J. R. (2001). The Birth of Time: How Astronomers Measure the Age of the Universe. Yale University Press. p. 151. ISBN 978-0-300-08914-1.
32. ^ Brown, R. Hanbury; Hazard, C. (1950). "Radio-frequency Radiation from the Great Nebula in Andromeda (M.31)". Nature. 166 (4230): 901–902. Bibcode:1950Natur.166..901B. doi:10.1038/166901a0.
33. ^ Brown, R. Hanbury; Hazard, C. (1951). "Radio emission from the Andromeda nebula". MNRAS. 111: 357–367. Bibcode:1951MNRAS.111..357B. doi:10.1093/mnras/111.4.357.
34. ^ van der Kruit, P. C.; Allen, R. J. (1976). "The Radio Continuum Morphology of Spiral Galaxies". Annual Review of Astronomy and Astrophysics. 14 (1): 417–445. Bibcode:1976ARA&A..14..417V. doi:10.1146/annurev.aa.14.090176.002221.
35. ^ Ingrosso, G.; et al. (2009). "Pixel-lensing as a way to detect extrasolar planets in M31". Monthly Notices of the Royal Astronomical Society. 399 (1): 219–228. arXiv:. Bibcode:2009MNRAS.399..219I. doi:10.1111/j.1365-2966.2009.15184.x.
36. ^ Holland, S. (1998). "The Distance to the M31 Globular Cluster System". Astronomical Journal. 115 (5): 1916–1920. arXiv:. Bibcode:1998AJ....115.1916H. doi:10.1086/300348.
37. ^ Stanek, K. Z.; Garnavich, P. M (1998). "Distance to M31 With the HST and Hipparcos Red Clump Stars". Astrophysical Journal Letters. 503 (2): 131–141. arXiv:. Bibcode:1998ApJ...503L.131S. doi:10.1086/311539.
38. ^ Davidge, T. J.; McConnachie, A. W.; Fardal, M. A.; Fliri, J.; Valls-Gabaud, D.; Chapman, S. C.; Lewis, G. F.; Rich, R. M. (2012). "The Recent Stellar Archeology of M31 – The Nearest Red Disk Galaxy". The Astrophysical Journal. 751 (1): 74. arXiv:. Bibcode:2012ApJ...751...74D. doi:10.1088/0004-637X/751/1/74.
39. ^ "Hubble Finds Giant Halo Around the Andromeda Galaxy". Retrieved 14 June 2015.
40. ^ a b Kalirai, J. S.; et al. (2006). "The Metal-Poor Halo of the Andromeda Spiral Galaxy (M31)". Astrophysical Journal. 648 (1): 389–404. arXiv:. Bibcode:2006ApJ...648..389K. doi:10.1086/505697.
41. ^ Barmby, P.; Ashby, M. L. N.; Bianchi, L.; Engelbracht, C. W.; Gehrz, R. D.; Gordon, K. D.; Hinz, J. L.; Huchra, J. P.; Humphreys, R. M.; Pahre, M. A.; Pérez-González, P. G.; Polomski, E. F.; Rieke, G. H.; Thilker, D. A.; Willner, S. P.; Woodward, C. E. (2006). "Dusty Waves on a Starry Sea: The Mid-Infrared View of M31". The Astrophysical Journal. 650 (1): L45–L49. arXiv:. Bibcode:2006ApJ...650L..45B. doi:10.1086/508626.
42. ^ Barmby, P.; Ashby, M. L. N.; Bianchi, L.; Engelbracht, C. W.; Gehrz, R. D.; Gordon, K. D.; Hinz, J. L.; Huchra, J. P.; Humphreys, R. M.; Pahre, M. A.; Pérez-González, P. G.; Polomski, E. F.; Rieke, G. H.; Thilker, D. A.; Willner, S. P.; Woodward, C. E. (2007). "Erratum: Dusty Waves on a Starry Sea: The Mid-Infrared View of M31". The Astrophysical Journal. 655 (1): L61–L61. Bibcode:2007ApJ...655L..61B. doi:10.1086/511682.
43. ^ a b Tamm, A.; Tempel, E.; Tenjes, P.; Tihhonova, O.; Tuvikene, T. (2012). "Stellar mass map and dark matter distribution in M 31". Astronomy & Astrophysics. 546: A4. arXiv:. Bibcode:2012A&A...546A...4T. doi:10.1051/0004-6361/201220065.
44. ^ Braun, R.; Thilker, D. A.; Walterbos, R. A. M.; Corbelli, E. (2009). "A Wide-Field High-Resolution H I Mosaic of Messier 31. I. Opaque Atomic Gas and Star Formation Rate Density". The Astrophysical Journal. 695 (2): 937–953. arXiv:. Bibcode:2009ApJ...695..937B. doi:10.1088/0004-637X/695/2/937.
45. ^ Draine, B. T.; Aniano, G.; Krause, Oliver; Groves, Brent; Sandstrom, Karin; Braun, Robert; Leroy, Adam; Klaas, Ulrich; Linz, Hendrik; Rix, Hans-Walter; Schinnerer, Eva; Schmiedeke, Anika; Walter, Fabian (2014). "Andromeda's Dust". The Astrophysical Journal. 780 (2): 172. arXiv:. Bibcode:2014ApJ...780..172D. doi:10.1088/0004-637X/780/2/172.
46. ^ "HubbleSite - NewsCenter - Hubble Finds Giant Halo Around the Andromeda Galaxy (05/07/2015) - The Full Story". hubblesite.org. Retrieved 2015-05-07.
47. ^ Dame, ENR/PAZ. "Hubble finds massive halo around the Andromeda Galaxy // News // Notre Dame News // University of Notre Dame". news.nd.edu. Retrieved 2015-05-07.
48. ^ "Hubble finds a massive halo around the Andromeda Galaxy // News // Department of Physics // University of Notre Dame". physics.nd.edu. Retrieved 2015-05-07.
49. ^ Lehner, Nicolas; Howk, Chris; Wakker, Bart (2014-04-25). "Evidence for a Massive, Extended Circumgalactic Medium Around the Andromeda Galaxy". The Astrophysical Journal. 804: 79. arXiv: [astro-ph]. Bibcode:2015ApJ...804...79L. doi:10.1088/0004-637x/804/2/79.
50. ^ "NASA's Hubble Finds Giant Halo Around the Andromeda Galaxy". Retrieved 2015-05-07.
51. ^ a b van den Bergh, S. (1999). "The local group of galaxies". Astronomy and Astrophysics Review. 9 (3–4): 273–318. Bibcode:1999A&ARv...9..273V. doi:10.1007/s001590050019.
52. ^ Karachentsev, Igor D.; Karachentseva, Valentina E.; Huchtmeier, Walter K.; Makarov, Dmitry I. (2003). "A Catalog of Neighboring Galaxies". The Astronomical Journal. 127 (4): 2031–2068. Bibcode:2004AJ....127.2031K. doi:10.1086/382905.
53. ^ McCall, Marshall L. (2014). "A Council of Giants". Monthly Notices of the Royal Astronomical Society. 440 (1): 405–426. arXiv:. Bibcode:2014MNRAS.440..405M. doi:10.1093/mnras/stu199.
54. ^ Tempel, E.; Tamm, A.; Tenjes, P. (2010). "Dust-corrected surface photometry of M 31 from Spitzer far-infrared observations". Astronomy and Astrophysics. 509: A91. arXiv:. Bibcode:2010A&A...509A..91T. doi:10.1051/0004-6361/200912186. wA91.
55. ^ Liller, W.; Mayer, B. (1987). "The Rate of Nova Production in the Galaxy". Publications of the Astronomical Society of the Pacific. 99: 606–609. Bibcode:1987PASP...99..606L. doi:10.1086/132021.
56. ^ Mutch, S.J.; Croton, D.J.; Poole, G.B. (2011). "The Mid-life Crisis of the Milky Way and M31". The Astrophysical Journal. 736 (2): 84. arXiv:. Bibcode:2011ApJ...736...84M. doi:10.1088/0004-637X/736/2/84.
57. ^ Beaton, R. L.; et al. (2006). "Unveiling the Boxy Bulge and Bar of the Andromeda Spiral Galaxy". Astrophysical Journal Letters. 658 (2): L91. arXiv:. Bibcode:2007ApJ...658L..91B. doi:10.1086/514333.
58. ^ "Astronomers Find Evidence of an Extreme Warp in the Stellar Disk of the Andromeda Galaxy" (Press release). UC Santa Cruz. January 9, 2001. Archived from the original on 19 May 2006. Retrieved 2006-05-24.
59. ^ Rubin, V. C.; Ford, W. K. J. (1970). "Rotation of the Andromeda Nebula from a Spectroscopic Survey of Emission". Astrophysical Journal. 159: 379. Bibcode:1970ApJ...159..379R. doi:10.1086/150317.
60. ^ Arp, H. (1964). "Andromeda Nebula from a Spectroscopic Survey of Emission". Astrophysical Journal. 139: 1045. Bibcode:1964ApJ...139.1045A. doi:10.1086/147844.
61. ^ van den Bergh, Sidney (1991). "The stellar populations of M31". Publications of the Astronomical Society of the Pacific. 103: 1053–1068. Bibcode:1991PASP..103.1053V. doi:10.1086/132925.
62. ^ Hodge, P .W. (1966). Galaxies and Cosmology. McGraw Hill.
63. ^ Simien, F.; Pellet, A.; Monnet, G.; Athanassoula, E.; Maucherat, A.; Courtes, G. (1978). "The spiral structure of M31 – A morphological approach". Astronomy and Astrophysics. 67: 73–79. Bibcode:1978A&A....67...73S.
64. ^ Haas, M. (2000). "Cold dust in M31 as mapped by ISO". The interstellar medium in M31 and M33. Proceedings 232. WE-Heraeus Seminar: 69–72. Bibcode:2000immm.proc...69H.
65. ^ Walterbos, R. A. M.; Kennicutt, R. C., Jr. (1988). "An optical study of stars and dust in the Andromeda galaxy". Astronomy and Astrophysics. 198: 61–86. Bibcode:1988A&A...198...61W.
66. ^ a b Gordon, K. D.; Bailin, J.; Engelbracht, C. W.; Rieke, G. H.; Misselt, K. A.; Latter, W. B.; Young, E. T.; Ashby, M. L. N.; Barmby, P.; Gibson, B. K.; Hines, D. C.; Hinz, J.; Krause, O.; Levine, D. A.; Marleau, F. R.; Noriega-Crespo, A.; Stolovy, S.; Thilker, D. A.; Werner, M. W. (2006). "Spitzer MIPS Infrared Imaging of M31: Further Evidence for a Spiral-Ring Composite Structure". The Astrophysical Journal. 638 (2): L87–L92. arXiv:. Bibcode:2006ApJ...638L..87G. doi:10.1086/501046.
67. ^ Braun, R. (1991). "The distribution and kinematics of neutral gas, HI region in M31". Astrophysical Journal. 372: 54–66. Bibcode:1991ApJ...372...54B. doi:10.1086/169954.
68. ^ "ISO unveils the hidden rings of Andromeda" (Press release). European Space Agency. October 14, 1998. Retrieved 2006-05-24.
69. ^ Morrison, Heather; Caldwell, Nelson; Harding, Paul; Kriessler, Jeff; Rose, James A.; Schiavon, Ricardo (2008). "Young Star Clusters in M 31". Galaxies in the Local Volume, Astrophysics and Space Science Proceedings: 227–230. arXiv:. Bibcode:2008ASSP....5..227M. doi:10.1007/978-1-4020-6933-8_50.
70. ^ Pagani, L.; Lequeux, J.; Cesarsky, D.; Donas, J.; Milliard, B.; Loinard, L.; Sauvage, M. (1999). "Mid-infrared and far-ultraviolet observations of the star-forming ring of M 31". Astronomy & Astrophysics. 351: 447–458. arXiv:. Bibcode:1999A&A...351..447P.
71. ^ "Busted! Astronomers Nab Culprit in Galactic Hit-and-Run". Harvard-Smithsonian Center for Astrophysics. October 18, 2006. Archived from the original on 8 October 2014. Retrieved 2014-10-06.
72. ^ Block, D. L.; Bournaud, F.; Combes, F.; Groess, R.; Barmby, P.; Ashby, M. L. N.; Fazio, G. G.; Pahre, M. A.; Willner, S. P. (2006). "An almost head-on collision as the origin of the two off-centre rings in the Andromeda galaxy". Nature. 443 (1): 832–834. arXiv:. Bibcode:2006Natur.443..832B. doi:10.1038/nature05184. PMID 17051212.
73. ^ Bullock, J. S.; Johnston, K.V. (2005). "Tracing Galaxy Formation with Stellar Halos I: Methods". Astrophysical Journal. 635 (2): 931–949. arXiv:. Bibcode:2005ApJ...635..931B. doi:10.1086/497422.
74. ^ Lauer, T. R.; et al. (1993). "Planetary camera observations of the double nucleus of M31". Astronomical Journal. 106 (4): 1436–1447, 1710–1712. Bibcode:1993AJ....106.1436L. doi:10.1086/116737.
75. ^ Bender, Ralf; et al. (2005). "HST STIS Spectroscopy of the Triple Nucleus of M31: Two Nested Disks in Keplerian Rotation around a Supermassive Black Hole". Astrophysical Journal. 631 (1): 280–300. arXiv:. Bibcode:2005ApJ...631..280B. doi:10.1086/432434.
76. ^ Gebhardt, Karl; Bender, Ralf; Bower, Gary; Dressler, Alan; Faber, S. M.; Filippenko, Alexei V.; Green, Richard; Grillmair, Carl; Ho, Luis C.; Kormendy, John; Lauer, Tod R.; Magorrian, John; Pinkney, Jason; Richstone, Douglas; Tremaine, Scott (June 2000). "A Relationship between Nuclear Black Hole Mass and Galaxy Velocity Dispersion" (PDF). The Astrophysical Journal. Chicago, Illinois, USA: The University of Chicago Press. 539 (1): L13–L16. arXiv:. Bibcode:2000ApJ...539L..13G. doi:10.1086/312840. Retrieved March 10, 2010.
77. ^ a b Tremaine, S. (1995). "An Eccentric-Disk Model for the Nucleus of M31". Astronomical Journal. 110: 628–633. arXiv:. Bibcode:1995AJ....110..628T. doi:10.1086/117548.
78. ^ "Hubble Space Telescope Finds a Double Nucleus in the Andromeda Galaxy" (Press release). Hubble News Desk. July 20, 1993. Retrieved 2006-05-26.
79. ^ Schewe, Phillip F.; Stein, Ben (July 26, 1993). "The Andromeda Galaxy has a Double Nucleus". Physics News Update. American Institute of Physics. Archived from the original on August 15, 2009. Retrieved 2009-07-10.
80. ^ Fujimoto, M.; Hayakawa, S.; Kato, T. (1969). "Correlation between the Densities of X-Ray Sources and Interstellar Gas". Astrophysics and Space Science. 4 (1): 64–83. Bibcode:1969Ap&SS...4...64F. doi:10.1007/BF00651263.
81. ^ Peterson, L. E. (1973). "Hard Cosmic X-Ray Sources". In Bradt, H.; Giacconi, R. X- and Gamma-Ray Astronomy, Proceedings of IAU Symposium no. 55 held in Madrid, Spain, 11–13 May 1972. International Astronomical Union. pp. 51–73. Bibcode:1973IAUS...55...51P.
82. ^ Barnard, R.; Kolb, U.; Osborne, J. P. (2005). "Timing the bright X-ray population of the core of M31 with XMM-Newton". arXiv: [astro-ph].
83. ^ Barmby, P.; Huchra, J. P. (2001). "M31 Globular Clusters in the Hubble Space Telescope Archive. I. Cluster Detection and Completeness". Astronomical Journal. 122 (5): 2458–2468. arXiv:. Bibcode:2001AJ....122.2458B. doi:10.1086/323457.
84. ^ "Hubble Spies Globular Cluster in Neighboring Galaxy" (Press release). Hubble news desk STSci-1996-11. April 24, 1996. Archived from the original on 1 July 2006. Retrieved 2006-05-26.
85. ^ Meylan, G.; et al. (2001). "G1 in M31 – Giant Globular Cluster or Core of a Dwarf Elliptical Galaxy?". Astronomical Journal. 122 (2): 830–841. arXiv:. Bibcode:2001AJ....122..830M. doi:10.1086/321166.
86. ^ Ma, J.; De Grijs, R.; Yang, Y.; Zhou, X.; Chen, J.; Jiang, Z.; Wu, Z.; Wu, J. (2006). "A 'super' star cluster grown old: the most massive star cluster in the Local Group". Monthly Notices of the Royal Astronomical Society. 368 (3): 1443–1450. arXiv:. Bibcode:2006MNRAS.368.1443M. doi:10.1111/j.1365-2966.2006.10231.x.
87. ^ Cohen, Judith G. (2006). "The Not So Extraordinary Globular Cluster 037-B327 in M31". The Astrophysical Journal. 653: L21–L23. arXiv:. Bibcode:2006ApJ...653L..21C. doi:10.1086/510384.
88. ^ "Star cluster in the Andromeda galaxy". Retrieved 7 September 2015.
89. ^ Burstein, David; Li, Yong; Freeman, Kenneth C.; Norris, John E.; Bessell, Michael S.; Bland-Hawthorn, Joss; Gibson, Brad K.; Beasley, Michael A.; Lee, Hyun-chul; Barbuy, Beatriz; Huchra, John P.; Brodie, Jean P.; Forbes, Duncan A. (2004). "Globular Cluster and Galaxy Formation: M31, the Milky Way, and Implications for Globular Cluster Systems of Spiral Galaxies". Astrophysical Journal. 614: 158–166. arXiv:. Bibcode:2004ApJ...614..158B. doi:10.1086/423334.
90. ^ Huxor, A. P.; et al. (2005). "A new population of extended, luminous, star clusters in the halo of M31". Monthly Notices of the Royal Astronomical Society. 360 (3): 993–1006. arXiv:. Bibcode:2005MNRAS.360.1007H. doi:10.1111/j.1365-2966.2005.09086.x.
91. ^ Prostak, Sergio (2012-12-14). "Microquasar in Andromeda Galaxy Amazes Astronomers". Sci-News.com.
92. ^ Bekki, K.; et al. (2001). "A New Formation Model for M32: A Threshed Early-type Spiral?". Astrophysical Journal Letters. 557 (1): L39–L42. arXiv:. Bibcode:2001ApJ...557L..39B. doi:10.1086/323075.
93. ^ Ibata, R.; et al. (2001). "A giant stream of metal-rich stars in the halo of the galaxy M31". Nature. 412 (6842): 49–52. arXiv:. doi:10.1038/35083506. PMID 11452300.
94. ^ Young, L. M. (2000). "Properties of the Molecular Clouds in NGC 205". Astronomical Journal. 120 (5): 2460–2470. arXiv:. Bibcode:2000AJ....120.2460Y. doi:10.1086/316806.
95. ^ Koch, A.; Grebel, E. K. (March 2006). "The Anisotropic Distribution of M31 Satellite Galaxies: A Polar Great Plane of Early-type Companions". Astronomical Journal. 131 (3): 1405–1415. arXiv:. Bibcode:2006AJ....131.1405K. doi:10.1086/499534.
96. ^ Cowen, Ron (2012). "Andromeda on collision course with the Milky Way". Nature. doi:10.1038/nature.2012.10765. Retrieved 2014-10-06.
97. ^
98. ^ Cox, T. J.; Loeb, A. (2008). "The collision between the Milky Way and Andromeda". Monthly Notices of the Royal Astronomical Society. 386 (1): 461–474. arXiv:. Bibcode:2008MNRAS.386..461C. doi:10.1111/j.1365-2966.2008.13048.x.
99. ^ Cain, F. (2007). "When Our Galaxy Smashes Into Andromeda, What Happens to the Sun?". Universe Today. Archived from the original on 17 May 2007. Retrieved 2007-05-16.
100. ^ "How to See the Farthest Thing You Can See - Sky & Telescope". 9 September 2015.
101. ^ "Watch Andromeda Blossom in Binoculars - Sky & Telescope". 16 September 2015.
102. ^
103. ^