Thursday, December 3, 2009

Time Crystal


here’s a disaster at CERN in Switzerland and two men are absorbed by a black hole. Moments later time stops everywhere in the Universe except near fragments of mysterious blue crystal. Each one is surrounded by a bubble of time. Hold a crystal and you’re alive. Without it you’re frozen in time. Fourteen-year-old Catriona O’Brien is visiting CERN when the disaster happens. She is given a crystal and hears one of the two absorbed men saying that if she can collect all the crystal fragments and bring them down something called the ‘Time Tunnel’ then he can restart time.

So begins an adventure that will take Catriona back thru the history of the Universe to the Big Bang and beyond!

But there are other things, mysterious and dangerous things, coming up the Time Tunnel, things which want to use the people of Earth for their own evil purposes. Time Crystal, the greatest adventure in the history of the Universe, written and read by me, Wyken Seagrave. Visit www.timecrystal.c o.uk for free podcast, role-playing on-line games, competitions, prizes and far far more!

So begins Wyken Seagrave’s epic adventure which will take Catriona on a journey through time back to the Big Bang and beyond.

Time Crystal is Unique

It is the first work of fiction to:
  1. use the history of the Universe as its stage
  2. allow listeners to influence the next episode
  3. describe a novel mechanism for the creation of a black hole
  4. explore the science and art underlying the work in a simultaneous sister podcast
  5. cost the author US$ 1 million to develop

This is truly the greatest adventure in the history of the Universe!

Click on the links above to visit the parts of this site, or click the links at the side to subscribe free either via iTunes or Podiobooks.

The Art & Science of Time Crystal describes the writing, development, characters and science behind the story.

http://www.timecrystal.co.uk/

Jupiter

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Jupiter is the largest planet in the solar system, the 5th from the Sun. It is not quite as bright as Venus when seen from Earth.
Measured across, Jupiter is ten times the size of the Earth and one-tenth the size of the Sun. Like the Sun and Saturn, it is mostly hydrogen and helium. There may be a small core of rock and perhaps ice at the center. This is surrounded by an ocean of liquid hydrogen and helium in the form of a metal. Above this is a layer of liquid hydrogen and helium, and above this a thick atmosphere.

Jupiter is radiating energy, possibly as a result of radioactivity. The most famous feature is the Great Red Spot, which may be a huge storm in the atmosphere. If so it must be quite a storm, as it has been recorded for 300 years!

Jupiter also has a faint ring made of dust which was only recently discovered.
Far more easy to see are the moons. The four largest of these were seen by Galileo when he made one of the first telescopes. The way they moved round the planet convinced him that the old idea, that everything moves round the Earth, must be wrong.

The following was kindly contributed by Russell Odell

The sun contains 99.9 percent of the mass in the solar system. The remaining 0.1 percent make up the other planets and their moons, and Jupiter took most of that mass. If Jupiter were a shell, all the other planets and their moons could fit inside with room to spare. Jupiter could hold 317 of our earth's.

Jupiter's diameter is 88,000 miles, thirty times the width of the United States. It orbits the sun at 8.1 miles per second (mps), or 19,160 miles per hour (mph). It is 485 million miles from the sun making it a very cold planet in the range of minus 240 degrees F. However, due to the enormous pressure of its mass, the center is estimated to be 54,000 degrees F., or five times hotter than the surface of the sun. (The interior of the sun is 40 million ºF.)

The earth rotates on its axis in 24 hours establishing day and night. Jupiter rotates in 9 hours, 54 minutes, giving it the shortest day and night of any of the planets. The surface speed of the earth at its equator is a little over 1,000 mph. Jupiter's surface speed at its equator is 30,000 mph.

Jupiter is in full view six months of the year. It is very bright. Only the planet Venus is brighter. If you compare the brightness of Jupiter to the stars, only one star, Sirius, is brighter.

Jupiter, like Saturn, Uranus and Neptune is a ball of gas while the other four planets are solid (Mercury, Venus, Earth & Mars).

Galileo discovered Jupiter and three of its moons on January 7, 1610. Six nights later, January 13th , he discovered the fourth moon. He named them, J1, J2, J3, and J4.

A few nights later the Dutch astronomer Simon Marius, quite independently, saw the moons through his telescope. Marius gave them names from mythology after the sons and daughters of the Greek gods naming them Io, Europa, Gannymede and Callisto. Later, when Marius announced his discovery he was ridiculed by the followers of the great Galileo who was a patron of the Grand Duke of Tuscany. Marius was ostracized and no one would honor the names he had given to the moons. As other moons were discovered Galileo's method of numbering prevailed over giving names to the moons. These first four moons of Jupiter are known as the Galilean Moons. However, later, to recognize the work of Marius, the names he gave the moons are the names we know them by today.

The 14th moon was discovered in October, 1975, by the American astronomer Charles T. Kowal. Its distance from the planet has not yet been determined.

Jupiter's 12th moon is the incredible distance of 14, 880,000 miles from the planet. With such a distance, it takes the moon two years to orbit its planet.

The 16 moons of Jupiter is a story by itself. For example, its four outer most moons are 15 million miles from the planet and orbit in the opposite direction of Jupiter’s other moons. .

One of the mysteries of Jupiter is its big red spot. The Space Probe Pioneer Ten flew by Jupiter on December 3, 1973. It was followed a year later by Pioneer Eleven. In March of 1979 Voyager One sent back pictures of the big Red Spot. Voyager Two sent back additional pictures in July (1974). The Red Spot was first reported by Robert Hooke in 1664. Several years later it was also noted by Cassini, the Italian-French astronomer. Drawings of it appeared in 1831 by William Dawes and later by other astronomers. We have known about the great Red Spot of Jupiter for more than 300 years.

We do not know why this Red Spot grows and diminishes in size from 7000 miles wide and 13,000 to 30,000 miles long. We know it rises and sinks in the gaseous clouds but don't know why. Neither do we know why it drifts east and west but never north or south.

Did you ever wonder how or why the planet Jupiter came into existence? What or who determined its size? What keeps it rotating, where does the energy come from to keep it zooming around the sun at 19,160 mph? Why does it rotate on its axis anti-clockwise while the planet Venus rotates clockwise? Why does Jupiter have 16 moons but Mercury and Venus have none? Science says this all happened purely by chance over a period of billions of years.

However, we have many theories that explain its creation from many different viewpoints, but, which theory is right?

The gravitational fields of Jupiter are so strong they disintegrated the Shoemaker-Levy 9 Comet into 20 fragments before it hit the planet.

Revealing the mysteries of galaxy formation

Revealing the mysteries of galaxy formation

This image provides a view of the Large Magellanic Cloud in visible light. The distribution of stars can be clearly seen in this image. The red outlined area corresponds to AKARI's far-infrared image. The green area shows the location of the near- and mid-infrared image. AKARI's far-infrared image reveals that interstellar clouds cover the entire galaxy, while the stellar distribution is concentrated in the lower part of the image. This galaxy is located in the constellation Dorado, in the southern sky. When looking at the night sky, the Large Magellanic Cloud can be seen with a smaller neighbouring galaxy, called the Small Magellanic Cloud. Both appear as dim clouds in the sky. The name 'Magellanic' is taken from the great 16th century navigator Magellan, who observed the two 'clouds' during his voyage around the world. Credits: Mr. Motonori Kamiya

As the AKARI satellite nears completion of its All Sky Survey, it has released two stunning images of the Large Magellanic Cloud. AKARI is an infrared astronomical satellite from the Japan Aerospace Exploration Agency (JAXA) with involvement from the UK, the Netherlands and the European Space Agency.

Mars, The Stars & Planets - Did the Universe from from - God? New Angle on a Tired Old Debate - CosmicFingerprints.com

Dr Stephen Serjeant of the Open University, commenting on the new images said, "AKARI has given us a superb view of the Large Magellanic Cloud - a dwarf galaxy which our own galaxy is consuming. All galaxies cannibalize each other; in time, our own galaxy will be subsumed within the Andromeda galaxy."

The Large Magellanic Cloud is a dwarf galaxy orbiting our own galaxy. It lies at a distance of about 160,000 light years, having about 1/20 the diameter of our galaxy and 1/10 the number of stars. It is believed that the LMC was once a barred spiral galaxy that was disrupted by the Milky Way to become somewhat irregular.

The Large Magellanic Cloud contains about 10 billion stars and is at a distance of 160,000 light years, extremely close by astronomical standards. The Large Magellanic Cloud is located in the constellation Dorados in the southern sky. The name "Magellanic" is taken from the great 16th century navigator Magellan who observed the clouds during his voyage around the world.

Revealing the mysteries of galaxy formation

This false-colour view of the Large Magellanic Cloud is a composite of images taken by AKARI at far-infrared wavelengths (60, 90 and 140 microns). The Large Magellanic Cloud is a neighbour galaxy to the Milky Way. Interstellar clouds in which new stars are forming are distributed over the entire galaxy. The bright region in the bottom-left is known as the 'Tarantula Nebula' and is a very productive factory of stars. This figure is a part of a data set covering a sky portion of about 17 000 by 17 000 light-years. Credits: JAXA

AKARI (formerly known as ASTRO-F) was launched in February 2006 and began its All Sky Survey in May. It is the first new infrared survey satellite since the 1980s and the data it collects will shed new light on the dusty Universe – such as areas where stars are born and die.

Dr Chris Pearson, European Space Agency support astronomer for AKARI, said, "The spectacular images of the Large Magellanic Cloud in the Far-Infrared give us a first mouth watering taste of what we can expect from the AKARI All-Sky Survey as the satellite continues to sweep out great swathes of the sky."

Dr Seb Oliver of the University of Sussex added "AKARI has now mapped virtually the whole sky. This is a tremendous achievement by all concerned. These examples show the impressive quality that we can expect from the first far infrared sky survey for 20 years."

During the survey observations, AKARI investigated one of the most important targets for studies of the formation of galaxies, the Large Magellanic Cloud, over more wavelength bands than has ever been possible in the past. Using the data taken by AKARI astronomers will be able to unlock the secrets of how both the Large Magellanic Cloud and our own Galaxy have formed and have grown to their current state.

Your Zodiac Horoscope - Insert Your Birthdate & Get Answers about Past-Present and Future. Free - AboutAstro.com/horoscope

Professor Glenn White of the Open University / CCLRC Rutherford Appleton Laboratory said "this stunning AKARI image traces the far -infrared emission from a noticeable bar of stars, some of which, including S Doradus, are extremely luminous. The Large Magellanic Cloud is rich in a variety of diffuse nebulae, including the spectacular Tarantula Nebula, planetary nebulae, open clusters, globular clusters, which suggest that it has experienced early and late bursts of star formation."

Since most stars are formed deep in dusty clouds of interstellar gas, their starlight is not directly visible in the optical, but light from the young stars heats the surrounding dust, which in turn radiates at infrared wavelengths that can escape the dusty clouds. However, if dust is very widespread and thick throughout galaxies, the stars which heat the surrounding dust may not be just the young stars, so the observed infrared radiation would not be the good measure of star formation rates that it is usually assumed to be. Clarifying the dust content of typical galaxies is important to understanding how they evolve over time, as interstellar gas is transformed into stars. These AKARI far infrared surveyor observations are designed to trace the distribution of warm dust close to hot stars, and the associated star-formation rate. Understanding this in one of the Local Group galaxies in our own backyard is crucial to our understanding of the formation and evolution of more distant galaxies.

Dr Rich Savage of the University of Sussex said, "These latest images are a great example of the new views of the cosmos that AKARI is giving us."

Dr Elysandra Figueredo of the Open University said, "I'm really very impressed with these images but much more impressed about the superb scientific insights this data bring. It's very exciting to see the structure and the content of the compact star-forming regions distributed throughout our neighbour galaxy. These regions are crowded with newly born stars that are probably still inside their cocoons. This is a new view Large Magellanic Cloud and it will certainly help us a great deal in understanding the birth of stars like our Sun, and also bring new insights about our own Galaxy."

Dr David Clements from Imperial College London said, 'The last all sky far infrared survey, made by the IRAS satellite, was completed in 1983 but astronomers still refer to it on a daily basis. These early results from AKARI show just how much of an advance the new survey is going to be - we'll be using AKARI data daily for at least the next 20 years!'

http://www.physorg.com/news81599877.html

The Galaxies

Galaxies

The Milky Way system

The Sombrero Galaxy (M104)The Sombrero Galaxy (M104), an almost edge-on spiral galaxy in the constellation of Virgo.
© Peter Barthel (Kapteyn Institute), Very Large Telescope, European Southern Observatory.
On a dark night we can often see a band of light stretching across the sky. If we look at this band with binoculars or a small telescope we see that it is partially resolved into stars. This band we call the Milky Way and indeed it is composed of a band of stars most of which are too faint to be resolved so that we see their combined light as a faint glow.

This band is the plane of the disk of our galaxy. The Sun is one, rather faint, example of approximately 200,000,000,000 stars that make up our galaxy. These stars are mostly grouped into a flattened disk which has a bulge at its centre. The Sun is in this disk about two thirds of the way from its centre to its edge. When we look at the night sky we see the Milky Way when we look along the plane of this disk whereas when we look in other directions, out of the plane, we see far fewer stars.

There is a spherical component to our galaxy which contains very old stars and spherical clusters of old stars. These are often referred to as Population 2 objects. Population 1 being the objects found in the disk.

The size of our galaxy is huge; light would take about 100,000 years to cross the Galaxy.

Spiral galaxies

NGC 253NGC 253, a nearly edge-on spiral galaxy (type Sc) in the constellation Sculptor. NGC 253 lies about 8 million light years away. © European Southern Observatory Wide Field Imager, Max-Planck-Institut für Astronomie, Osservatorio Astronomico di Capodimonte. Our galaxy has arms of younger stars and gas that appear to spiral out from the centre. In fact the objects in these spiral arms are in almost circular orbits about the centre of the Galaxy. The Sun takes about 200 million years to complete one orbit around the centre. About 30 percent of all galaxies have spiral arms. Some have arms that spiral directly from the nucleus while others have a linear feature, called a bar, from whose ends the arms originate.

Spiral galaxies are rich in gas and dust. Some are viewed face-on so that the spiral arms are easily seen whereas others are viewed edge-on. These show the presence of dust lanes which obscure the starlight coming from near the midline of the disk. We see this in our galaxy where the Milky Way is divided into two portions for much of its length. Indeed the centre of the Milky Way galaxy is invisible in ordinary light because the interstellar dust in that direction is so thick. Infrared light, however, penetrates the dust and recent measures have allowed astronomers to `see' the Galactic centre.

Elliptical galaxies

The majority of galaxies show no spiral features, nor are they flattened disks; they take the form of ellipsoids. They show only small evidence for young stars, dust or gas. They are very different in size ranging from giant ellipticals with masses of about 1 million million times that of the Sun to dwarf ellipticals with masses closer to those of the globular clusters.

Irregular galaxies

NGC 253NGC 253, a nearly edge-on spiral galaxy (type Sc) in the constellation Sculptor. NGC 253 lies about 8 million light years away. © European Southern Observatory Wide Field Imager, Max-Planck-Institut für Astronomie, Osservatorio Astronomico di Capodimonte. Some galaxies are neither ellipsoidal nor are they spirals. Some of these are obviously objects which have been tidally distorted by the presence of another near-by galaxy but there are some, such as the Magellanic Clouds (see below), which have little symmetry to their structure.

Active galaxies

Some galaxies show evidence for the generation of enormous amounts of energy from the vicinity of their nucleus. These are often strong radio emitters and often show complex lobe structure extending for millions of light years. Other galaxies have such energetic nuclei that we only see the bright nucleus and not the underlying galaxy; we call these objects quasars (quasi-stellar objects).

The presence of black holes at the centres of these objects is thought necessary by many astronomers to explain their nature. Because they are the brightest objects known in the universe it is not surprising that quasars are the objects that have been traced out furthest from us. The furthest known are so far away that the light we see coming from them must have originated when the Universe was only one tenth of its present age.

Clusters of galaxies

There are many clusters of galaxies. Members of some of the closest can be seen with a small telescope in the constellations Virgo and Coma Berenices. We can trace clusters of galaxies out to the furthest distances that we can reach. Some of these clusters contain thousands of galaxies. Near their centres giant ellipticals are often found and it is thought that these arise from the collision of several galaxies which have combined.

X-ray studies have shown that there is very hot gas between the galaxies in a cluster but this gas does not solve one of the great puzzles in astronomy which is that these clusters require a certain total mass to explain how they are held together but we only can account for one tenth of this mass. This is known as the `missing mass problem'.

Nearby galaxies

Unfortunately those of us who live in the northern hemisphere cannot see the two closest galaxies, called the Magellanic Clouds, which are rather like two satellite galaxies to the Milky Way.

They can easily be seen by the naked-eye and their brightest stars can be seen with binoculars. These two galaxies are much smaller than the Milky Way and are about 200,000 light years away.

In the northern sky we can see two galaxies with the naked-eye. The Andromeda galaxy, M31, is a faint fuzzy patch that appears, with binoculars, as a lens shaped object. It is a galaxy rather like ours at a distance of about 2 million light years. It has two dwarf elliptical satellites which can be seen with a small telescope.

The other galaxy (M33 in Triangulum) is much harder to see although it is at a similar distance to the Andromeda galaxy. This is because it is smaller and less bright intrinsically. It too is a spiral galaxy.

ANDROMEDA GALAXY PART 2

  • GALEX Team, CalTech, NASA




    Larger ultraviolet image.




    This ultraviolet image highlights
    a 150,000-ly-wide ring of young
    and hot, blue stars that surrounds
    Andromeda's central bulge (more
    from APOD and GALEX).


    On October 18, 2006, astronomers using NASA's Spitzer Space Telescope announced the discovery of two dust rings (or "holes") in Andromeda's dust disk using infrared light that provide evidence of an ancient head-on collision with neighboring dwarf galaxy along its polar axis Messier 32 (M32) some 210 million years ago. Computer simulations support the hypothesis that the passage of the much smaller galaxy created violent waves of gravitational interactions that left rings of gas and dust propagating outward from the site of the impact. Since Andromeda is much more massive than M32, the larger galaxy was not substantially disrupted, but M32 lost more than half its initial mass in the course of the collision (more).



    Pauline Barmby, CfA, JPL, NASA -- larger infrared image

    Holes in Andromeda's disk may be from an ancient collision with satellite galaxy M32 (more).


  • Active Galactic Nucleus


    STScI, NASA


    Larger image.



    The central 30 light-years of Andromeda
    contains two galactic nuclei, which suggests
    that the great spiral consumed a major
    galactic companion whose substance has
    been mostly merged except for its central
    core (more from APOD and STScI).


    In the 1990s, astronomers using the Hubble Space Telescope found that Andromeda has a nucleus with a double structure. The "nuclear hot-spots" are located close together, considering that the galaxy's spiral disk has been estimated to be anywhere from 150,000 to more than 200,000 ly across while the observed central area measures only around 30 ly wide. Subsequent ground-based observations led some astronomers to speculate that two galactic nuclei do indeed exist, are moving with respect to each other, and that one nucleus is slowly disrupting the other through tidal forces. As a result, some astronomers believed that that one nucleus may be the remains a smaller satellite galaxy that was "eaten" by Andromeda (Corbin et al, 2001; Gerssen et al, 1995; and Lauer et al, 1993). In 2005, astronomers using the Hubble Space Telecope announced that the two two bright blobs are actually composed of an elliptical ring of older red stars and a smaller, brighter, and denser disk of young blue stars of around 200 million years old around the galaxy's central black hole (NASA press release).


    Michael Garcia, Stephen Murray,
    Palomar Sky Survey





    Larger image.





    The black square in the center
    of Andromeda's spiral disk has
    been observed with x-rays to
    reveal a supermassive black
    hole, as as well as smaller
    ones (more from CXC).


    Andromeda's core has a supermassive central black hole of around 140 million Solar-masses (latest NASA press release). Recent observations with the Chandra X-Ray Observatory also reveal numerous other bright X-ray sources, most of which are probably due to binary systems where a star is feeding gas into a neutron star and black hole. A very cool X-ray source has been identified about 10 light years south of the galactic center. A second, hotter X-ray source was found to be at a position consistent with the position of the super-massive black hole.


    Garcia et al, 2001;
    T. Brown et al, 2001;
    CXC, SAO, NASA



    Larger x-ray image.



    The blue dot is an unusually "cool"
    million degree X-ray source that
    lies just below an black hole
    (yellow) that may be X-ray bright
    from matter swirling toward a
    supermassive black hole of 30
    million Solar-masses (more
    from CXC).


    Andromeda's satellite (or "companion") galaxies include M32 and M110, two bright dwarf elliptical galaxies that are the brightest of a swarm of smaller companions. By late 1999, however, at least 10 satellite galaxies of Andromeda were known, including NGC 185 (which was discovered by William Herschel), and NGC 147 (discovered by Heinrich Ludwig d'Arrest, 1822-1875) as well as the very faint dwarf systems And I, And II, And III, possibly And IV (which may be a cluster or a remote background galaxy), And V, And VI (also called the Pegasus dwarf), and And VII (also the Cassiopeia dwarf).

    Satellite galaxy M32 may be interacting to distort the disk structure of Andromeda itself, whose spiral arms of neutral hydrogen are displaced from those consisted of stars by around 4,000 light-years and so cannot be continuously followed in the area closest to its smaller neighbor. Computer simulations have shown that such disturbances can be modelled by assuming a recent close encounter with a small companion of the mass of M32, which also suggest M32 has lost many stars from such an encounter to be spread out in Andromeda's halo.


  • Very Large Galactic Halo

    Using the Hubble Space Telescope, astronomers had previously announced in 2003 that they had obtained the deepest visible-light image ever taken of the sky to resolve approximately 300,000 stars in Andromeda's luminous halo. By capturing both faint dwarf stars and bright giant stars, astronomers were able to estimate the age of many members of Andromeda's halo population by analyzing color and brightness distributions. Describing an initial hypothesis subsequently contested in January 2007, the astronomers indicated that they had found many stars spanning a wide range of ages from six to 13 billion years old, which is much wider than that of the stellar population of the Milky Way's halo where 11- to 13-billion-year-old, metal-poor stars reside. (More discussion and close-up images from Alan M. MacRobert at Sky and Telescope).


    STScI, NASA




    Larger image.




    Although Andromeda's luminous halo
    was thought to include many younger
    stars around six to 13 billion years
    old in 2003, new observations of
    old red giant, halo stars up to
    500,000 light-years away from
    Andromeda's core were announced
    in 2007 (2003; and 2007 findings).


    On January 7, 2007, astronomers announced finding old low-metallicity, red giant stars up to some 500,000 light-years from Andromeda's center which suggests that the galaxy is up to five times larger than originally thought, so that its luminous halo may actually overlap with that of the Milky Way. The new finding also suggests that previous observers mis-identified relatively metal-rich red giants in Andromeda's galactic bulge as halo stars. Based on observations of the Milky Way and other galaxies, the metallicity of stars farther from the galactic center should fall with distance from the core (more).


    Ann Feild, STScI, NASA




    Larger image.





    Although a 2003 study of 300,000 stars
    in Andromeda's halo indicated that their
    age range was wider than those found in
    the Milky Way's (more from STScI and
    APOD), this observation has been revised
    by subsequent observations that suggest
    that Andromeda's luminosity may be five
    times larger than originally thought (more).


    In addition, a giant stream of metal-rich stars was recently detected in Andromeda's halo (Ibata et al, 2001). The presence of younger stars in Andromeda's halo may the result of a more violent phase of the galaxy past involving mergers with smaller satellite galaxies. Furthermore, numerical simulations of the movements of Andromeda and the Milky Way suggest that the two big spiral galaxies themselves may eventually collide and merge within five to 10 billion years.


  • Old but Bright Globular Cluster

    A small and compact satellite of Andromeda, G1 is the brightest globular star cluster in the Local Group. Also known as Mayall II, G1 contains at least 300,000 old stars. Despite its globular appearance, however, G1 may actualy be the stripped down core of a dwarf spheroidal galaxy (like SagDEG, the Milky Way's satellite) that has been "shredded" by its larger host. G1 may have at least 10 to 18 million Solar-masses, at least twice the mass of Omega Centauri, the Milky Way's largest globular (Meylan et al, 1998). It is located around 130,000 to 170,000 ly from Andromeda's nucleus.


    Michael Rich, Kenneth Mighell,
    James D. Neill, Wendy Freedman,
    Columbia University, Carnegie
    Observatories
    , STScI, NASA


    Larger image.



    One of Andromeda's more compact satellites
    is G1, the brightest globular star cluster in
    the Local Group (more from STScI and APOD).


    G1 appears to be nearly as old as the oldest of the roughly 250 known globulars in the Milky Way Galaxy and so probably was formed shortly after the birth of the first stars at the beginning of the universe. Unlike many other globulars, it has a "rather high mean metallicity of [Fe/H] = --0.95, somewhat similar to 47 Tucanae" which may be the result of self enrichment during an early phase of cluster evolution (Meylan et al, 2001). Recently, some astronomers detected a 20,000 Solar-mass black hole in G1's core (more from STScI and Gebhardt et al, 2002).


  • Satellite Galaxies

    On January 11, 2006, astronomers announced their discovery that many of Andromeda's faint companion galaxies lie within a thin sheet running perpendicular through the galaxy's Andromeda disk. Nine out of 14 low-mass satellites lying with 1.3 million light-years from Andromeda are found within this sheet, whose typical width is only 52,000 light years (about two percent of the distance between Milky Way and Andromeda). The sheet runs through Andromeda's core and is almost exactly aligned with its polar axis.


    Eva Grebel,
    Andreas Koch,
    University of Basel,
    NOAO/AURA/NSF,
    Keck Observatory


    Larger illustration.


    Many of Andromeda's
    satellite galaxies
    are located within
    a plane pendicular
    to its disk (more).


    Similar polar planes containing contain many of the Milky Way's companion galaxies were found around three decades ago by William Kunkel and Donald Lynden-Bell. One hypothesis is that such satellite galaxies are tiny left-overs from the break-up of a more massive galaxy which has since been swallowed by their host but still move within the orbital plane of their predecessor, as galactic mergers are believed to be a main mechanism of galactic growth. A second possibility is that the observed alignment with the poles of spiral galaxies' disks traces the otherwise invisible distribution of non-luminous, so-called dark matter around these massive galaxies. Finally, it is also possible that the observed orientation along a plane is a consequence of the infall of satellites along dark matter filaments, as cosmological models predict density fluctuations or matter concentrations which would attract neighboring clumps and continued growth that lead to streams of dark and luminous matter along filamentary features of the so-called cosmic web. Small galaxies forming in dark matter streams could end up in preferred sheets determined by their infall direction toward massive galaxies. Indeed, the Andromeda satellite plane points to the nearby spiral galaxy M33 as well as to the M81 group of galaxies (more).


  • Other Information


  • http://www.solstation.com/x-objects/andromeda.htm

ANDROMEDA GALAXY PART 1

© Robert Gendler,
Astroimaging Gallery
(Used with permission)

Larger mosaic (more).


Andromeda is the
largest member of
the Local Group of
galaxies, which
includes the Milky
Way and its satellite
galaxies. Andromeda's
own satellites include
M32, at center left, and
M110, at lower right
(more from APOD).


  • Breaking News


    Stefan Immler,
    Erin Grand, Swift,
    GSFC, NASA

    Larger UV image.

    This new high-resolution
    UV image highlights the
    hottest and youngest stars
    and energetic stellar
    remnants in Andromeda's
    spiral arms, densest
    clusters, and violent
    core around its central
    black hole (more).


    On September 16, 2009, NASA's Swift Satellite Mission released the highest resolution ultra-violet (UV) image of Andromeda available. Covering an area some 200,000 light-years (ly) wide and 100,000 ly high, the image was compiled from 330 UV images made at wavelengths of 192.8, 224.6, and 260 nanometers. The result covers some 20,000 UV sources among the hottest and youngest stars and stellar remnants in Andromeda's spiral arms, densest clusters, and violent core around its central, supermassive black hole (more from NASA and Astronomy Picture of the Day).


    McConnachie et al, 2009;
    PAndAS




    Larger composite image and
    composite illustration
    .




    Andromeda has been growing
    by pulling stars (as well as
    gas) from smaller satellite
    galaxies, such as bright
    neighbor Triangulum (more).


    On September 2, 2009, a team of astronomers (using the Canada-France Hawaii Telescope for the Pan-Andromeda Archaeological Survey or PAndAS) announced the discovery of stars and coherent structures that are almost certainly remnants of dwarf galaxies destroyed by the tidal field of Andromeda (M31). They also found that the halo of the giant spiral galaxy has non-native stars and "coherent structures" (such as stellar streams or "tidal tails" and a gaseous as well as stellar warp in its spiral disk). M31's nearest bright neighbor, satellite galaxy Triangulum (M33), moreover, has a stellar structure (including a warped disk) suggestive of a recent encounter with M31 around 2.5 billion years ago, and model simulations indicate that the two galaxies will have an even more violent encounter in about 2 billion years). Their observations supports the hierarchical galaxy formation model through the apparent interactions of M31 and M33 in the continuing growth of galaxies in the modern era (more from PAndAS; UBC news release; Lisa Grossman, New Scientist, September 2, 2009; McConnachie et al, 2009; and Martin et al, 2009).



    Courtesy of PAndAS





    Larger illustration (more).





    The two galaxies will have an
    even more violent encounter
    in about 2 billion years (more).


  • A Large Spiral Galaxy

    Wider and possibly brighter than our own Milky Way, the Andromeda Galaxy was once thought to be the dominant member of the Local Group of galaxies. Although it is Milky Way's nearest large galactic neighbor, this large spiral galaxy (type Sb with two arms) lies around 2.52 ± 0.14 million light-years (ly) from the Solar System (Ribas et al, 2005). It can be found in (0:40:27+40:40:12, J2000; and 0:42:44.3+41:16:9.4, ICRS 2000) Constellation Andromeda, the Chained Maiden. It is located northwest of Mu and Beta Andromedae (Mirach); west of Nu Andromedae; northeast of Theta and Sigma Andromedae; north of Pi, Delta, and Epsilon Andromedae; and south of Theta and Omega Cassiopeiae. Andromeda can be seen by Human eyes from Earth without a telescope as a "little cloud" (see Akira Fujii's photo to better relate the galaxy's location to the brightest stars of Constellation Andromeda).

    Andromeda has a bright disk that is now believed to span as much as 228,000 ly in width (Chapman et al, 2005). In 2005, astronomers announced that Andromeda's disk actally extends far further out, so that the disk spans at least 260,000 light-years -- almost twice the size of the bright disk seen in photographs (Ibata et al, 2005). The outer disk emits nearly 10 percent of the galaxy's total light and may be comprised of metal-poor stars stripped from smaller galaxies that strayed too close. On January 7, 2007, a team of astronomers announced the discovery of low-metallicity, red giant stars up to some 500,000 light-years from Andromeda's core which suggests that the galaxy is much larger than originally thought, so that Andromeda's luminous halo may actually overlap with that of the Milky Way (BBC News -- more below).


    © Jason Ware,
    www.galaxyphoto.com
    (Used with permission)




    Larger image (more).




    Andromeda has a bright
    yellowish nucleus, dark
    winding dustlanes, and
    bluish spiral arms and
    star clusters (more
    from APOD).


    In the venerable Star Names: Their Lore and Meaning, Richard Hinckley Allen noted that: "... the Great Nebula, the Queen of the Nebulae, ..., is said to have been known as far back as A.D. 905; was described by [Abd-al-Rahman] Al Sufi as the Little Cloud before 986; and appeared on a Dutch star-map of 1500." According to Robert Burnham, Jr. (1931-93): "The first hint of the true nature of the Andromeda Galaxy came late in 1923 when several [C]epheid variable stars were identified in the system [by Edwin Powell Hubble (1889-1953) who thus] ... definitively established the great spiral as an extra-galactic object ...."The galaxy is frequently referred to as M31 because it was the 31st object in the Messier Catalogue of diffuse objects that Charles Messier (1730-1817) found not to be comets. Subsequently, the "nebula" was also designated as NGC 224 by John Louis Emil Dreyer (1852-1926) in his New General Catalogue (NGC) of Nebulae and Clusters of Stars, which was first published in 1887 and later supplemented with Index Catalogue (IC) I in 1895 and IC II in 1907.


    Bill Schoening, Vanessa Harvey,
    REU program, NOAO/AURA/NSF




    Larger red, green, and blue composite image.





    Recent observations indicate that,
    although the spiral disk of Andromeda
    may be much larger than that of the
    Milky Way, the galaxy appears to be
    much less dense, with a smaller mass
    counting its dark matter halo (box
    view at page bottom -- more at NOAO).


    Careful estimates of Andromeda's angular diameter obtained using 2-inch binoculars by Robert Jonckhere from 1952 to 1953 indicated that Andromeda's disk had a diameter of over 200,000 ly (assuming a distance of 2.9 million ly). Hence, Andromeda's spiral disk may as much as twice as large as the Milky Way's. Although Andromeda was long thought to be the most massive galaxy in the Local Group, recent data suggest that Andromeda's visible mass may total around 300 to 400 billion Solar-masses. This is considerably less than more recent estimates of the Milky Way's visible mass of as much as 600 billion or more Solar-masses, which suggests that the Milky Way may be much denser than Andromeda. These results apparently have been confirmed by recent estimates of the total halo masses of the two spirals that account for the gravitational effects of their invisible dark matter, which suggest that Andromeda has a total of around 700 billion to 1.2 trillion Solar-masses compared to 0.93 to 1.9 trillion or more for the Milky Way (more discussion from (Xue et al, 2008; Evans et al, 2000; and Evans and Wilkinson, 2000).


    IRAS, IPAC, NASA




    Larger infrared image.






    Young stars are probably being born
    in many dusty regions of Andromeda
    that are bright in infrared wavelengths,
    with many short-lived but massive, blue
    stars in the more intense white and
    yellow areas (more from IPAC).


    The brightest star cloud in Andromeda has its own NGC number, NGC 206. One of the largest star-forming regions known in the Local Group of galaxies, Sir William Friedrich Wilhelm Herschel (1738-1822, portrait) noted it in his catalog as H V.36 on his discovery of the diffuse object on October 17, 1786. Located next to a dark nebula towards the southwestern, outer edge of Andromeda's spiral disk (another photo), the cloud's bright blue stars give an indication of the massive star cluster's youth (more from Astronomy Picture of the Day).


    B.J. Mochejska (Warsaw University),
    The DIRECT Project, FLWO, MDM



    Larger blue, visual, and infrared,
    composite image.




    One of the largest clusters of young blue stars
    in the Local Group of galaxies, NGC 206 is
    located in one of Andromeda's dusty spiral arms
    (more from APOD and CfA).


    So far, only one supernova has been recorded in the Andromeda Galaxy, but it was the first to be detected outside the Milky Way. Known as Supernova 1885 for the year of its appearance, it has also been designated as S Andromedae. Ernst Albrecht Hartwig (1851-1923) observed it on August 20, 1885 at Dorpat Observatory in Estonia. While found independently by several other observers, only Hartwig realized its significance. The supernova reached a magnitude of six between August 17th and 20th but then faded to magnitude 16 by February 1890.



    Philip Choi, Puragra Guhathakurta, UCSC, KPNO -- larger blue and infrared image.

    Andromeda has an "extreme" warp in its outer spiral disk, possibly from interactions
    with satellite galaxies (more from UCSC and UCOLICK), as well as debris trails
    from past mergers with other galaxies (more).


    Astronomers have been finding evidence of a warp in Andromeda's spiral disk for some time. The faint outer parts of a spiral galaxy are more susceptible to warping because they are less strongly bound by the gravitational and other forces that keep disk stars in a plane and are also more susceptible to the influence of neighboring galaxies. As a result, the outer regions of a rotating body of stars and gas can deviate from the plane of the disk, like an old record album exposed to too much heat. Such a warp tends to occur at the outer edges, while the inner part of the spiral disk continues to look reasonably flat. Andromeda's warp is especially pronounced on the northeast (left) side of its major axis. Such galactic warps are very difficult to demonstrate conclusively because the outer portions of a spiral disk are extremely faint compared to their bright central regions. However, the warp in Andromeda may be the most extreme case of a warped spiral galaxy found thus far. Possible causes of the warp include interactions between Andromeda and its smaller satellite galaxies (more discussion).


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