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Andromeda Galaxy
M31 Lanoue.png
A visible light image of the Andromeda Galaxy.
Observation data (J2000 epoch)
Pronunciation /ænˈdrɒmədə/
Constellation Andromeda
Right ascension 00h 42m 44.3s[1]
Declination +41° 16′ 9″[1]
Redshift −301 ± 1 km/s[2]
Distance 2.54 ± 0.06 Mly
(778 ± 17 kpc)[3][2][4][5][6][a]
Type SA(s)b[1]
Apparent dimensions (V) 190′ × 60′[1]
Apparent magnitude (V) 3.44[7][8]
Other designations
M31, NGC 224, UGC 454, PGC 2557, 2C 56 (Core)[1], LEDA 2557
See also: Galaxy, List of galaxies

The Andromeda Galaxy is a spiral galaxy approximately 2,500,000 light-years (1.58×1011 AU) away[4] in the constellation Andromeda. It is also known as Messier 31, M31, or NGC 224, and is often referred to as the Great Andromeda Nebula in older texts. Andromeda is the nearest spiral galaxy to our own, the Milky Way. As it is visible as a faint smudge on a moonless night, it is one of the farthest objects visible to the naked eye, and can be seen even from urban areas with binoculars. It is named after the princess Andromeda (Greek: Ανδρομέδη – Andromédē) in Greek mythology. Andromeda is the largest galaxy of the Local Group, which consists of the Andromeda Galaxy, the Milky Way Galaxy, the Triangulum Galaxy, and about 30 other smaller galaxies. Although the largest, Andromeda may not be the most massive, as recent findings suggest that the Milky Way contains more dark matter and may be the most massive in the grouping.[9] The 2006 observations by the Spitzer Space Telescope revealed that M31 contains one trillion (1012) stars,[10] more than the number of stars in our own galaxy, which is estimated to be c. 200-400 billion.[11]

While the 2006 estimates put the mass of the Milky Way to be ~80% of the mass of Andromeda, which is estimated to be 7.1 × 1011 solar masses,[2] a 2009 study concluded that Andromeda and the Milky Way are about equal in mass.[12]

At an apparent magnitude of 3.4, the Andromeda Galaxy is notable for being one of the brightest Messier objects,[13] making it easily visible to the naked eye even when viewed from areas with moderate light pollution. Although it appears more than six times as wide as the full moon when photographed through a larger telescope, only the brighter central region is visible with the naked eye.

Contents

Observation history

Great Andromeda Nebula by Isaac Roberts.

The earliest recorded observation of the Andromeda Galaxy was in 964 CE by the Persian astronomer, Abd al-Rahman al-Sufi (Azophi),[14] who described it as a "small cloud" in his Book of Fixed Stars. Other star charts of that period have it labeled as the Little Cloud.[14] The first description of the object based on telescopic observation was given by Simon Marius[14] in 1612. Charles Messier catalogued it as object M31 in 1764 and incorrectly credited Marius as the discoverer, unaware of Al Sufi's earlier work. In 1785, the astronomer William Herschel noted a faint reddish hue in the core region of the M31. He believed it 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.[15]

William Huggins in 1864 observed the spectrum of M31 and noted that it differed from a gaseous nebula.[16] The spectra of M31 displayed a continuum of frequencies, superimposed with dark absorption lines that help identify the chemical composition of an object. The Andromeda nebula was very similar to the spectra of individual stars, and from this it was deduced that M31 had a stellar nature. In 1885, a supernova (known as "S Andromedae") was seen in M31, the first and so far only one observed in that galaxy. At the time M31 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".[17]

The first photographs of M31 were taken in 1887 by Isaac Roberts from his private observatory in Sussex, England. The long-duration exposure allowed the spiral structure of the galaxy to be seen for the first time.[18] However, at the time this object was commonly believed to be a nebula within our galaxy, and Roberts mistakenly believed that M31 and similar spiral nebulae were actually solar systems being formed, with the satellites nascent planets. The radial velocity of this object with respect to our solar system was measured in 1912 by Vesto Slipher at the Lowell Observatory, using spectroscopy. The result was the largest velocity recorded at that time, at 300 kilometres per second (190 mi/s), moving in the direction of the Sun.[19]

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Island universe

M31 in proximity to Pegasus constellation.

In 1917, Heber Curtis observed a nova within M31. Searching the photographic record, 11 more novae were discovered. Curtis noticed that these novae were, on average, 10 magnitudes fainter than those that occurred within our Galaxy. 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.[20]

In 1920 the Great Debate between Harlow Shapley and Heber Curtis took place, concerning the nature of the Milky Way, spiral nebulae, and the dimensions of the universe. To support his claim that Great Andromeda Nebula (M31) was an external galaxy, Curtis also noted the appearance of dark lanes resembling the dust clouds in our own Galaxy, as well as the significant Doppler shift. In 1922 Ernst Öpik presented a very elegant and simple astrophysical method to estimate the distance of M31, his result put Andromeda Nebula far outside our Galaxy at a distance of about 450 kpc (kilo parsec), which is about 1,500 kly (kilo lightyears).[21] Edwin Hubble settled the debate in 1925 when he identified extragalactic Cepheid variable stars for the first time on astronomical photos of M31. These were made using the 2.5 metres (98 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 Galaxy, but an entirely separate galaxy located a significant distance from our own.[22]

Andromeda plays an important role in galactic studies, since it is the nearest spiral galaxy (although not the nearest galaxy). In 1943, Walter Baade was the first person to resolve stars in the central region of the Andromeda Galaxy. Based on his observations of this galaxy, he was able to discern 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.)[23] Dr. Baade also discovered that there were two types of Cepheid variables, which resulted in a doubling of the distance estimate to M31, as well as the remainder of the Universe.[24]

Radio emission from the Andromeda Galaxy was first detected by Grote Reber in 1940. The first radio maps of the galaxy were made in the 1950s by John Baldwin and collaborators at the Cambridge Radio Astronomy Group.[25] The core of the Andromeda Galaxy is called 2C 56 in the 2C radio astronomy catalogue. In 2009, the first planet may have been discovered in the Andromeda Galaxy. This candidate was detected using a technique called microlensing, which is caused by the deflection of light by a massive object.[26]

General

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

The measured distance to the Andromeda Galaxy 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.[27][28]

Recent distance estimate

The Andromeda Galaxy pictured in ultraviolet light by GALEX.

At least four distinct techniques have been used to measure distances to the Andromeda Galaxy.

In 2003, using the infrared surface brightness fluctuations (I-SBF) and adjusting for the new period-luminosity value of Freedman et al. 2001 and using a metallicity correction of -0.2 mag dex−1 in (O/H), an estimate of 2.57 ± 0.06 megalight-years (790 ± 18 kpc) was derived.

Using the Cepheid variable method, an estimate of 2.51 ± 0.13 Mly (770 ± 40 kpc) was achieved in 2004.[3][2]

In 2005, a group of astronomers consisting of Ignasi Ribas (CSIC, Institute for Space Studies of Catalonia (IEEC)) and his colleagues announced the discovery of an eclipsing binary star in the Andromeda Galaxy. The binary star, designated M31VJ00443799+4129236,[c] has two luminous and hot blue stars of types O and B. By studying the eclipses of the stars, which occur every 3.54969 days, the astronomers were able to measure their sizes. Knowing the sizes and temperatures of the stars they were able to measure the absolute magnitude of the stars. When the visual and absolute magnitudes are known, the distance to the star can be measured. The stars lie at the distance of 2.52 ± 0.14 megalight-years (770 ± 43 kpc) and the whole Andromeda Galaxy at about 2.5 Mly (770 kpc).[4] This new value is in excellent agreement with the previous, independent Cepheid-based distance value.

Andromeda is close enough that the Tip of the Red Giant Branch (TRGB) method may also be used to estimate its distance. The estimated distance to M31 using this technique in 2005 yielded 2.56 ± 0.08 Mly (780 ± 25 kpc).[5]

Averaged together, all these distance measurements give a combined distance estimate of 2.54 ± 0.06 Mly (780 ± 18 kpc).[a] Based upon the above distance, the diameter of M31 at the widest point is estimated to be 141 ± 3 kly (43,000 ± 920 pc).[d] Applying trigonometry (arctangent), that figures to extending at an apparent 3.18° angle in the sky.

Mass and luminosity estimates

Mass estimates for the Andromeda halo (including dark matter) give a value of approximately 1.23 × 1012 M[29] (or 1.2 million million solar masses) compared to 1.9 × 1012 M for the Milky Way. Thus M31 may be less massive than our own galaxy, although the error range is still too large to say for certain. Even so, the masses of the Milky Way and M31 are comparable, and M31's spheroid actually has a higher stellar density than that of the Milky Way.[30]

In particular, M31 appears to have significantly more common stars than the Milky Way, and the estimated luminosity of M31, ~2.6 × 1010 L, is about 25% higher than that of our own galaxy.[31] However the rate of star formation in the Milky Way is much higher, with M31 only producing about one solar mass per year compared to 3–5 solar masses for the Milky Way. The rate of supernovae in the Milky Way is also double that of M31.[32] This suggests that M31 has experienced a great star formation phase in its past, but is now relatively quiescent, whereas the Milky Way is experiencing more active star formation.[31] Should this continue, the luminosity in the Milky Way may overtake that of M31 in the future.

Sextans B Sextans A Milky Way Leo I (dwarf galaxy) Canes Dwarf Leo II (dwarf galaxy) NGC 6822 Phoenix Dwarf Tucana Dwarf Wolf-Lundmark-Melotte Cetus Dwarf IC 1613 SagDIG Aquarius Dwarf Triangulum Galaxy NGC 185 NGC 147 IC 10 Andromeda Galaxy Messier 110 Leo A NGC 3109 Antlia Dwarf LGS 3 Pegasus Dwarf Andromeda II Andromeda III Andromeda I
About this image
Local group (clickable map)

Structure

The Andromeda Galaxy seen in infrared by the Spitzer Space Telescope, one of NASA's four Great Space Observatories.
Image of Andromeda Galaxy (M31) taken by Spitzer in infrared, 24 micrometres (0.00094 in) (Credit:NASA/JPLCaltech/K. Gordon (University of Arizona)
A Swift Tour of M31.OGG
A Swift Tour of M31.

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 the bulge of M31 has a box-like appearance, which implies that the galaxy is actually a barred galaxy with the bar viewed almost directly along its long axis.[33]

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.[34] This means that the spiral disk of stars in Andromeda 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 pc) in diameter. Previously, estimates of Andromeda'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 the 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.[35] A possible cause of such a warp could be gravitational interaction with the satellite galaxies near M31. The galaxy M33 could be responsible for some warp in M31's arms, though more precise distances and radial velocities are required.

Spectroscopic studies have provided detailed measurements of the rotational velocity of M31 at various radii from the core. In the vicinity of the core, the rotational velocity climbs to a peak of 225 kilometres per second (140 mi/s) at a radius of 1,300 light-years (82,000,000 AU) light-years, then descends to a minimum at 7,000 light-years (440,000,000 AU) where the rotation velocity may be as low as 50 kilometres per second (31 mi/s). Thereafter the velocity steadily climbs again 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.[36]

The spiral arms of Andromeda are outlined by a series of H II regions that Baade described as resembling "beads on a string". They appear to be tightly wound, although they are more widely spaced than in our galaxy.[37] Rectified images of the galaxy show a fairly normal spiral galaxy with the arms wound up in a clockwise direction. There are two continuous trailing arms that are separated from each other by a minimum of about 13,000 light-years (8.2E+8 AU). These can be followed outward from a distance of roughly 1,600 light-years (100,000,000 AU) from the core. The most likely cause of the spiral pattern is thought to be interaction with M32. This can be seen by the displacement of the neutral hydrogen clouds from the stars.[38]

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 Andromeda 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) from the core.[39] This ring is hidden from visible light images of the galaxy because it is composed primarily of cold dust.

Close examination of the inner region of Andromeda 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 Andromeda 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.[40]

Studies of the extended halo of M31 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.[41] This evidence indicates that the two galaxies have followed similar evolutionary paths. They are likely to have accreted and assimilated about 1–200 low-mass galaxies during the past 12 billion years.[42] The stars in the extended halos of M31 and the Milky Way may extend nearly one-third the distance separating the two galaxies.

Nucleus

HST image of 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. The luminosity of the nucleus is in excess of the most luminous globular clusters.[citation needed]

Using the orbiting Chandra X-ray telescope, astronomers have imaged the center of our near-twin island universe, finding evidence for an object so bizarre it would have impressed many 1960s science fiction writers (and readers). Like the Milky Way, Andromeda's galactic center appears to harbor an X-ray source characteristic of a black hole of a million or more solar masses. Seen above, the false-color X-ray picture shows a number of X-ray sources, likely X-ray binary stars, within Andromeda's central region as yellowish dots. The blue source located right at the galaxy's center is coincident with the position of the suspected massive black hole. While the X-rays are produced as material falls into the black hole and heats up, estimates from the X-ray data show Andromeda's central source to be surprisingly cool - only a million degrees or so compared to the tens of millions of degrees indicated for Andromeda's X-ray binaries. Credit: S. Murray, M. Garcia, et al., (CfA) SAO, CXO, and NASA

In 1991 Tod R. Lauer used WFPC, then on board the Hubble Space Telescope, to image Andromeda'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 3-5x107 M black hole.[43]

Scott Tremaine has 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.[44] 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.[45]

While at the initial time of its discovery it was hypothesized that the brighter portion of the double nucleus was the remnant of a small galaxy "cannibalized" by Andromeda,[46] this is no longer considered to be a viable explanation. The primary reason is that 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.[44]

Discrete sources

Artist's concept of Andromeda galaxy core showing a view across a mysterious disk of young, blue stars encircling a supermassive black hole. NASA/ESA photo.

Multiple X-ray sources have been detected in the Andromeda Galaxy, using observations from the ESA's XMM-Newton orbiting observatory. Robin Barnard et al. hypothesized that these are candidate black holes or neutron stars, which are heating 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.[47]

There are approximately 460 globular clusters associated with the Andromeda galaxy.[48] 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.[49] 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 M31 in the distant past.[50] The globular with the greatest apparent brightness is G76 which is located in the south-west arm's eastern half.[14]

In 2005, astronomers discovered a completely new type of star cluster in M31. 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.[51]

Satellites

Like the Milky Way, 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 M31 (Andromeda) 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.[52]

M110 also appears to be interacting with M31, and astronomers have found a stream of metal-rich stars in the halo of M31 that appears to have been stripped from these satellite galaxies.[53] M110 does contain a dusty lane, which may indicate recent or ongoing star formation.[54]

In 2006 it was discovered that nine of these galaxies lay along a plane that intersects the core of the Andromeda Galaxy, rather than being randomly arranged as would be expected from independent interactions. This may indicate a common tidal origin for the satellites.[55]

Future collision of the Milky Way with Andromeda

The Andromeda Galaxy is approaching the Sun at about 100 to 140 kilometres per second (62 to 87 mi/s),[56] so it is one of the few blue shifted galaxies. The Andromeda Galaxy and the Milky Way are thus expected to collide in perhaps 2.5 billion years, although the details are uncertain since Andromeda's tangential velocity with respect to the Milky Way is only known to within about a factor of two.[57] A likely outcome of the collision is that the galaxies will merge to form a giant elliptical galaxy.[58] 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 are presently unknown. If the galaxies do not merge, there is a small chance that the Solar System could be ejected from the Milky Way or join Andromeda.[59]

See also

The Andromeda galaxy on a German postage stamp of 1999.

Notes

  1. ^ average(787 ± 18, 770 ± 40, 772 ± 44, 783 ± 25) = ((787 + 770 + 772 + 783) / 4) ± ((182 + 402 + 442 + 252)0.5 / 4) = 778 ± 17
  2. ^ Apparent Magnitude of 4.36 – distance modulus of 24.4 = −20.0
  3. ^ J00443799+4129236 is at celestial coordinates R.A. 00h 44m 37.99s, Dec. +41° 29′ 23.6″.
  4. ^ distance × tan( diameter_angle = 190′ ) = 141 ± 3 kly diameter

References

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External links

Coordinates: Sky map 00h 42.44m 30s, +41° 16′ 10″


Simple English

File:M31
The Andromeda Galaxy.

The Andromeda Galaxy is the nearest big galaxy to the Milky Way, which is the galaxy Earth is in. It is sometimes called M31 or NGC 324 by astronomers. It is about 2.9 million light years away from Earth.[1] The Andromeda Galaxy is a Spiral galaxy like the Milky Way,[2] although it is about as twice as massive.[3] Scientists estimate it has over a trillion stars.[4]

Andromeda is about 2.2 million light years away from our galaxy. This huge gap gets smaller by 500,000 kilometres every hour. Eventually, in about 2 billion years, it will collide with the Milky Way.[5]

Being both large and very bright, it is one of the farthest objects that can be seen without a telescope or binoculars.[6]

Observation history

The Persian astronomer Abd-al-Rahman Al Sufi was the first man to record seeing the Andromeda Galaxy. He called the Galaxy 'a small cloud' in his book, 'The Book of Fixed Stars', which was written in 964 AD.[7] The first person to look at the galaxy with a telescope was Simon Marius in 1612.[8] In Charles Messier put it into his catalogue of astronomical objects. He called it M31 and gave the credit for its discovery to Marius, as he didn't know that Al Sufi had seen it over a thousand years previously.[9] In 1751 William Herschel estimated the distance to the Andromeda 'Nebula' as 'no more than 2000 times the distance to Sirius. This works out at around 17,200 light years[10] which which is far from the modern best estimate of 2.54 million light years.[11]

References


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