Updated:   5 January 2024


 to:  The Moon             to:  The Stars  




Planets and Comets



Transit of Mercury, 9 November 2006


Sunrise on November 9 occurred at 4.54 am. Soon after, starting at 5.19 am, Mercury was visible through the telescope as a black dot moving across the Sun’s disc. This 'transit of Mercury' lasted until 10.12 am. These transits are quite rare, and the next one will occur on 9 May, 2016. Unfortunately, the next five transits of Mercury will not be visible from Australia, and we will have to wait for 46 years to see the next one from Nambour. The November 9 event occurred on a cloudy morning with some rain, but despite the weather, the following images were captured at Starfield Observatory:





Phases of Venus

                           April 2017                              June 2017                         December 2017                      





Mars near the 2016 opposition


Mars photographed from Starfield Observatory, Nambour on June 29 and July 9, 2016, showing two
 different sides of the planet.  The north polar cap is prominent.


Brilliant Mars at left, shining at magnitude 0.9, passes in front of the dark molecular clouds in Sagittarius
 on October 15, 2014. At the top margin is the white fourth magnitude star 44 Ophiuchi. Its type is A3 IV:m.
 Below it and to the left is another star, less bright and orange in colour. This is the sixth magnitude star
SAO 185374, and its type is K0 III. To the right (north) of this star is a dark molecular cloud named B74.
A line of more dark clouds wends its way down through the image to a small, extremely dense cloud, B68,
just right of centre at the bottom margin. In the lower right-hand corner is a long dark cloud shaped like a figure 5.
This is the Snake Nebula, B72. Above the Snake is a larger cloud, B77.

These dark clouds were discovered by Edward Emerson Barnard at Mount Wilson in 1905. He catalogued
 370 of them, hence the initial 'B'. The bright centre of our Galaxy is behind these dark clouds, and is hidden
from view. If the clouds were not there, the galactic centre would be so bright that it would turn night into day.




Jupiter near opposition in 2017

Jupiter as photographed from Nambour on the evening of April 25, 2017. The images were taken, from left
to right,  at 9:10, 9:23, 9:49, 10:06 and 10:37 pm. The rapid rotation of this giant planet in a little under 10
hours is clearly seen. In the southern hemisphere, the Great Red Spot (bigger than the Earth) is prominent,
sitting within a 'bay' in the South Tropical Belt. South of it is one of the numerous White Spots. All of these
 are features in the cloud tops of Jupiter's atmosphere.

Jupiter as it appeared at 7:29 pm on July 2, 2017. The Great Red Spot is in a similar position near Jupiter's
 eastern limb (edge)  as in the fifth picture in the series above. It will be seen that in the past two months
the position of the Spot has drifted when  compared with the festoons in the Equatorial Belt, so must rotate
around the planet at a slower rate. In fact, the Belt enclosing  the Great Red Spot rotates around the planet
in 9 hours 55 minutes, and the Equatorial Belt takes five minutes less. This high rate of rotation has made
the planet quite oblate. The prominent 'bay' around the Red Spot in the five earlier images appears to be
 disappearing, and a darker streak along the northern edge of the South Tropical Belt is moving south.

Two new white spots have developed in the South Temperate Belt, west of the Red Spot. The five upper
images were taken near opposition, when the Sun was directly behind the Earth and illuminating all of
Jupiter's disc evenly. The July 2 image was  taken just four days before Eastern Quadrature, when the
angle from the Sun to Jupiter and back to the Earth was at its maximum  size. This angle means that
 we see a tiny amount of Jupiter's dark side, the shadow being visible around the limb of the planet on
 the left-hand side, whereas the right-hand limb is clear and sharp. Three of Jupiter's Galilean satellites
 are visible, Ganymede to  the left and Europa to the right. The satellite Io can be detected in a transit of
 Jupiter, sitting in front of the North Tropical Belt,  just to the left of its centre.

Jupiter at opposition on May 9, 2018


Jupiter reached opposition on May 9, 2018 at 10:21 hrs, and the above photographs were taken that evening,
some ten to twelve  hours  later. The first image above was taken at 9:03 pm, when the Great Red Spot was
approaching Jupiter's central meridian  and the satellite Europa was preparing to transit Jupiter's disc.
 Europa's transit began at 9:22 pm, one minute after its shadow  had touched Jupiter's cloud tops. The second
photograph was taken three minutes later at 9:25 pm, with the Great Red Spot very close to Jupiter's central meridian.

The third photograph was taken at 10:20 pm, when Europa was approaching Jupiter's central meridian.
Its dark shadow is behind it,  slightly below, on the clouds of the North Temperate Belt. The shadow is partially
 eclipsed by Europa itself. The fourth photograph  at 10:34 pm shows Europa and its shadow well past the
central meridian. Europa is the smallest of the Galilean satellites,  and has a diameter of 3120 kilometres.
It is  ice-covered, which accounts for its brightness and whitish colour. Jupiter's elevation above the horizon
 for the four photographs in order was 50º, 55º, 66º and 71º. As the evening progressed, the air temperature
 dropped a little and the planet gained altitude. The 'seeing' improved slightly, from Antoniadi IV to Antoniadi III.
At the time of the  photographs,  Europa's angular diameter was 1.57 arcseconds. Part of the final
 photograph is enlarged below.



Jupiter at 11:34 pm on May 18, ten days later. Changes in the rotating cloud patterns are apparent,
as some cloud bands rotate faster  than others and interact. Compare with the first photograph in
 the line of four taken on May 9. The Great Red Spot is ploughing a furrow through the clouds of the
South Tropical Belt, and is pushing up a turbulent bow wave.

Jupiter at opposition on June 11, 2019




Jupiter reached opposition on June 11, 2019 at 01:20 hrs, and the above photographs were taken that evening,
some twenty to twenty-two hours later. The first image above was taken at 10:01 pm, when the Great Red Spot
 was leaving Jupiter's  central meridian and the satellite Europa was preparing to transit Jupiter's disc.

Europa's transit began at 10:11 pm, and its  shadow touched Jupiter's cloud tops almost simultaneously.
Europa was fully in transit by 10:15 pm. The second photograph  was taken two minutes later at 10:17 pm,
with the Great Red Spot heading towards Jupiter's western limb.

The third photograph was taken at 10:41 pm, when Europa was about a third of its way across Jupiter.
Its dark shadow is  trailing it, slightly below, on the clouds of the North Temperate Belt. The shadow is
 partially eclipsed by Europa itself.  The fourth photograph at 10:54 pm shows Europa and its shadow about
 a quarter of the way across. This image is enlarged below. The fifth photograph shows Europa on Jupiter's
 central meridian at 11:24 pm, with the Great Red Spot on Jupiter's limb.
The sixth photograph taken at 11:45 pm shows Europa about two-thirds of the way through its transit,
and the Great Red Spot  almost out of sight. In this image, the satellite Callisto may be seen to the lower
 right of its parent planet. Jupiter's elevation  above the horizon for the six photographs in order was 66º, 70º,
 75º, 78º, 84º and 86º. As the evening progressed, the 'seeing'  proved quite variable.

There have been numerous alterations to Jupiter's belts and spots over the thirteen months since the 2018
 opposition. In particular,  there have been major disturbances affecting the Great Red Spot, which appears
 to be slowly  changing in size or "unravelling".




Left: Saturn showing the Rings when edge-on.
 Right: Over-exposed Saturn surrounded by its satellites Rhea, Enceladus, Dione, Tethys and Titan -
February 23/24, 2009.

Saturn with its Rings wide open on July 2, 2017. The shadow of its globe can be seen on the far side of
the Ring system. There are three  main concentric rings: Ring A is the outermost, and is separated from
the brighter Ring B by a dark gap known as the  Cassini Division, which is 4800 kilometres wide, enough
to drop Australia through. The innermost parts of Ring B are not as  bright as its outermost parts. Inside
Ring B is the faint Ring C, almost invisible but noticeable where it passes in front of the bright planet as a
dusky band. Spacecraft visiting Saturn have shown that there are at least four more Rings, too faint and
 tenuous to be observable from Earth, and some Ringlets. Some of these extend from the inner edge of
Ring C to Saturn's  cloudtops. The Rings are not solid, but are made up of countless small particles,
 mainly water ice with some rocky material,  all orbiting Saturn at different distances and speeds.
 The bulk of the particles range in size from dust grains to car-sized chunks.

The photograph above was taken when Saturn was close to opposition, with the Earth between Saturn
and the Sun. At that time, the shadow of Saturn's globe upon the Ring system was directly behind the
planet and hardly visible. The photograph below was taken on September 09, 2018, when Saturn was
17 days prior to eastern quadrature. At such a time, the angle from the Sun to Saturn and back to the
Earth is near its maximum, making the shadow fall at an  angle across the Rings as seen from Earth.
It may be seen falling across the far side of the Ring to the left side of the globe.

The photograph above was taken at 8:17 pm on November 03, 2022, when Saturn was again near eastern quadrature. The shadow of the planet once again falls across the far side of the rings, but in the intervening four years the angle of the rings as seen from Earth has been greatly reduced. The shadow of Ring B across the globe of Saturn is much darker from this angle.

The photograph above was taken at 7:41 pm on December 07, 2023, 14 days after eastern quadrature. The shadow of the planet once more falls across the far side of the rings, but in the intervening 13 months the angle of the rings as seen from Earth has lessened considerably. The light-coloured equatorial zone on Saturn shows through the gap known as the Cassini Division.

The change in aspect of Saturn's rings is caused by the plane of the ring system being aligned with Saturn's equator, which is itself tilted at an angle of 26.7 degrees to Saturn's orbit. As the Earth's orbit around the Sun is in much the same plane as Saturn's, and the rings are always tilted in the same direction in space, as we both orbit the Sun, observers on Earth see the configuration of the rings change from wide open (top large picture) to half-open (bottom large picture) and finally to edge on (small picture above). This cycle is due to Saturn taking 29.457 years to complete an orbit of the Sun, so the complete cycle from "edge-on (2009) → view of Northern hemisphere, rings half-open (2013) → wide-open (2017) → half-open (2022) → edge-on (2025) → view of Southern hemisphere, rings half-open (2029) → wide-open (2032) → half-open (2036) → edge-on (2039)" takes 29.457 years. The angle of the rings will continue to reduce until they are edge-on again in 2025. They will appear so thin that it will seem that Saturn has no rings at all. The rings will be wide-open again in 2032.



Neptune, photographed from Nambour on October 31, 2008







The movement of the dwarf planet Pluto in two days, between 13 and 15 September, 2008. Pluto is the
one object that has moved.  Width of field:   200 arcseconds

This is a stack of four images, showing the movement of Pluto over the period October 22 to 25, 2014.
Pluto's image for  each date appears as a star-like point at the upper right corner of the numerals.
The four are equidistant points on an almost- straight line. Four eleventh magnitude field stars are identified.
 A is GSC 6292:20, mv = 11.6.  B is GSC 6288:1587, mv = 11.9.  C is GSC 6292:171, mv = 11.2. 
D is GSC 6292:36, mv = 11.5.  (GSC = Guide Star Catalogue).
Pluto's position on October 24 (centre of image) was Right Ascension = 18 hours 48 minutes 13 seconds,
Declination =  -20
º 39' 11". 

The planet moved 2' 51" with respect to the stellar background during the three days between the first and
 last images,  or 57 arcseconds per day, or 1 arcsecond every 25¼ minutes.




Comet 17P / Holmes,   October - December 2007


Comet 17P/Holmes is an extremely faint periodic comet that returns every 6.88 years without anyone taking much notice. Its arrival last year gained it world-wide attention, for it exploded on 24 October 2007. A vast sphere of dust and debris was ejected in an ever-growing cloud. Though the comet’s head is only some tens of kilometres across, the cloud rapidly reached the size of Jupiter by November 9 grew larger than the Sun. It has continued to enlarge until it exceeded two million kilometres in diameter.

Before the eruption, the comet could only be seen through large telescopes, but the explosion caused it to brighten a millionfold within 36 hours, making it an obvious naked-eye object. It is possible that there could be a second explosion, as occurred in 1892 and led to its discovery by Edwin Holmes.

Since the explosion was first detected, the comet expanded dramatically, to become the largest object in the solar system. It reached a size in the night sky a little larger than the diameter of the Moon.  How a small comet could produce such an enormous cloud has not yet been explained.

In mid-November 2007, Comet Holmes experienced a ‘disconnection event’ - its faint, beautiful blue ion tail became detached from its head. Comet tails can be disconnected by gusts of solar wind which trigger magnetic storms around the comet similar to the geomagnetic storms which cause aurorae on Earth. Such a storm and disconnection was observed earlier this year in the tail of Comet Encke.

Was it really the largest object in the Solar System? In diameter, yes, but of course the Sun is the most massive object by several orders of magnitude. Some comets produce tails many millions of kilometres long, so they would be longer, but not 'bigger'. Photographs taken from Starfield Observatory, Nambour appear below.


This image and those following are all taken with the same equipment and have the same plate scale,
except  when indicated otherwise. They therefore show how the ejecta cloud surrounding the nucleus has
 expanded from night to night. The sphere of ejecta surrounding the comet's nucleus is most clearly defined
in the direction of the Sun, In the picture above this direction is towards the lower right. The magnitude 11.4
star GSC 3321:602 can be seen shining through the cloud at upper left. The diameter of the expanding
 cloud had reached 15 arcminutes and was still growing.

In the remaining images, the direction of the Sun is to the right. This image was taken ten nights later,
 on 13 November. The cloud of dust surrounding the nucleus is much larger - in fact the cloud itself was
 larger than the Sun and appeared in the sky about the same size as the Full Moon.


This image was taken three nights later, just after midnight on 17 November. The cloud of dust surrounding
the nucleus continues to grow, and the comet is now the largest object in the Solar System.  It appeared to
 the unaided eye like a faint ghost of the Full Moon. The bright star at lower left is Mirfak, a yellow-white F5
 star of magnitude 1.79.

This image was taken two nights later, on November 19. The coma of Comet Holmes appears to swallow
 the much more distant star Mirfak. At this stage the comet is fading, and becoming swamped by
moonlight from the waxing gibbous Moon.


This image was taken ten nights later, on November 29. The cloud is still expanding, and has reached
 a diameter of 46 arcminutes (cf approximately 30 arcminutes for the Full Moon. A newly developing tail
can be seen extending from the spherical cloud to the left-hand margin.


This image was taken at the prime focus of the RCOS reflector, and has a much larger plate scale than
the  other images above. It shows the interior of the ejecta cloud, which fills the frame and has now
become the comet's coma. The nucleus or head is just right of centre, and the beginnings of the tail
 stream off to the left. Image acquired on December 3.




Comet 2006 P1 (McNaught),   January - February 2007


Comet McNaught provided a magnificent display in early 2007, the best since the 1910 apparition of Halley's Comet. At its brightest, the head outshone nearby Venus, and the tail developed great fan-shaped streamers of dust and gas that spread over a large span of the night sky. The following images were taken on January 20 and 21, when there was a break in persistent overcast weather.  Thanks to Nambour Plaza's Digital Dog for careful processing.


Comet McNaught faintly appears out of the twilight shortly after sunset. Photographed from the Maleny-
Conondale Road on January 20.


As twilight fades, Comet McNaught becomes easily seen.


The comet becomes clearly visible as darkness falls.


The great tail does not become visible until twilight fades. Unfortunately this happens after the comet's
head has passed below the horizon. Photographed from Starfield Observatory in Nambour on January 21.
The house lights in the foreground are at Image Flat. The short curved lines in the sky are star trails
caused by the Earth's rotation.

The full extent of the tail is revealed after darkness falls. A faint line of dots crossing the frame is the
 trail left by the strobe lights of the local rescue helicopter on its flight path to the Nambour Hospital.


There are over a dozen synchronic bands or streamers visible in the comet's tail in this photograph.
The lights on  the skyline are private homes built on Kureelpa Falls Road, on the edge of the Highworth
Range escarpment. The Dulong Lookout is at the left margin. The brightest star trail at upper right was
 made by the first magnitude star Fomalhaut.  The bright star behind the comet's tail (above left centre
of photograph) is the star Al Nair in the constellation Grus. Taken from Starfield Observatory with a
 standard lens which has a field width of 43 degrees.

By February 6 the synchronic bands have merged into a wide, triangular fan tail covering an angle of
 about 55 degrees. The star just below the comet's coma (the glowing gas and dust surrounding the nucleus)
 is SAO 247006, magnitude 7.47. The faintest stars on this image are of magnitude 13. None of these
stars is visible to the unaided eye. Taken from Starfield Observatory - the field width is 4.5 degrees.




Comet 2007 N3 (Lulin),   February - March  2009


Comet Lulin was discovered in 2007 at Lulin Observatory by a collaborative team of Taiwanese and Chinese astronomers. It moved rapidly from Scorpius to Gemini, the head reaching a magnitude of 5. It had bright ion and dust tails, and an anti-tail. 

Comet Lulin at 11:30 pm on February 23, 2009, in Leo.



Comet Lulin at 11:25 pm on February 28, in Leo. The brightest star is Nu Leonis, magnitude 5.26.



Comet 46P / Wirtanen,   November - December 2018

In December 2018, Comet 46P/Wirtanen swept past Earth, making one of the ten closest approaches of a comet to our planet since 1960. It became faintly visible to the naked eye for weeks. Although Wirtanen's nucleus is only 560 metres across, its emerald green atmosphere appeared larger than the full Moon, and it was an increasingly easy target for binoculars and small telescopes. It reached its closest approach to the Sun (perihelion) on December 12, and then headed towards Earth. It passed the Earth at a distance of 11.5 million kilometres (30 times as far away as the Moon) on December 16. Its passage across the sky took it from the southern constellation of Fornax through Eridanus, Cetus, Taurus and Auriga, making it an all-night object for observers in the southern hemisphere. I
t reached magnitude 4 on December 15, appearing as a large, faint cloud about a degree across in the constellation of Taurus, near the Hyades and Pleiades star clusters.


Comet 46/P Wirtanen was photographed on November 29, 2018 between 9:45 and 9:47 pm.  The comet's
 position was Right Ascension = 2 hrs 30 min 11 secs, Declination = 21
º 43' 13", and it was heading towards
 the top of the picture. The nearest star to the comet's position, just to its left, is GSC 5862:549, magnitude 14.1.
The spiral galaxy near the right margin is NGC 908. The right-hand star in the yellow circle is SAO 167833,
magnitude 8.31.

Comet 46/P Wirtanen on November 30, 2018. This image is a stack of five exposures between 8:13 and
9:05 pm.  The comet's movement over the 52 minute period can be seen, the five images of the comet
merging into a short streak. It is heading towards the upper left corner of the image, and is brightening as
it approaches the Sun, with perihelion occurring on December 12. The images of the stars in the five
 exposures overlap each other precisely. The length of the streak indicates that the comet is presently
 moving against the starry background at 1.6º per day.

The comet at 9:05 pm was at Right Ascension = 2 hrs 32 min 56 secs, Declination = 20º 27' 20".
The upper star in the yellow circle is SAO 167833, magnitude 8.31, the same one circled in the preceding
picture but with higher magnification.
It enables the two photographs to be linked.

Comet 46/P Wirtanen at perihelion on December 12, 2018, at 00:55 am. It was faintly visible to the unaided
 eye, but easily visible through binoculars. 
The circled star has a magnitude of 15.77, and the brighter one
 just to its left is GSC 60:1162, magnitude 13.8. The comet is moving north-east, or to the right. Its position
 at the time of the photograph was RA = 3 hr 23 min 13 sec, Declination +4º 34' 31", at the boundary of the
 constellations Cetus and Taurus. The comet may brighten as it passes by the Earth on December 16.
Width of field = 18.6 arcminutes.





The Moon                                        to:  The Stars


Below is a picture of the Moon's Mare Imbrium taken forty years ago on Kodachrome II colour slide film by the writer at the East Warwick Observatory, using a Celestron 14. Following this is a set of pictures taken with a digital video camera at Nambour from 2017 to the present.


Mare Imbrium, with the large walled plain Plato (centre left, 100 km diameter) and the 130 km
long Alpine Valley (centre right).


The following are digital images taken with the Alluna RC-20 at Starfield Observatory. The video cameras used are a ZWO ASI 120MM-S, ZWO ASI 290MM and ZWO ASI 290 MC. The video streams of 2000 - 2500 frames are processed using AutoStakkert 3 and RegiStax 6.1 to produce still images. The most delicate details visible in these images include the tiny craterlets on the floors of Plato and Archimedes, the Schröter's Valley rille and the Alpine Valley rille which averages only 600 metres across and 75 metres deep.


Moon at 8 days after New. You may be able to find on this image some of the lunar features seen in
close-up in the following images.


Sunrise at the Moon's south pole.

Sunrise at the Moon's north pole.



This area was photographed from Starfield Observatory, Nambour on October 10, 2016. East (where the
Sun is rising) is to the right, north is to the top. The area is dominated by the large walled plain Plato at upper left,
and the impact crater Cassini at lower right. Between the two is a rugged mountainous area called the Alps,
to the west of which is a large basin filled with solidified lava, called Mare Imbrium (the Sea of Rains).
 Most of the craters on the Moon larger than about 8 kilometres are named, usually after famous philosophers
or scientists. In addition, the lava plains, mountain ranges, peaks, shallow valleys (called 'rilles'), and other
 notable features have also received names, sometimes after places on the Earth. As there are no rivers,
 cities or countries on the Moon, these names help observers to find their way around. The second picture
above shows some examples.

Plato in close-up. Five craterlets with diameters of 2 to 3 kilometres are visible inside it, as well as several smaller ones.

Sunrise over the 166 km long Vallis Alpes (Alpine Valley). It has a maximum width of 10 km. A delicate rille runs
along the entire length. The rille has an average width of 600 metres and an average depth of 78 metres.

 One day later.


This well-known trio dominates the south-eastern quadrant of Mare Imbrium. The craters are Archimedes (left),
Aristillus (top right) and Autolycus (lower right). The Fresnel Rilles and Hadley Rille are in the lower right-hand corner.
Some small craterlets dot the flat floor of Archimedes. The complex of mountains at upper left is called the Spitzbergen.

Close-up of Archimedes, 85 km in diameter. The smallest craterlets visible are less than 1 km in diameter.


Sunrise on the Apennines: the crater Eratosthenes and the Montes Apenninus on the Moon,
photographed  from Nambour on August 1, 2017.


This area was photographed from Starfield Observatory, Nambour on August 2, 2017. East (where
the Sun is rising) is to the right, north is to the top. Eratosthenes is the crater at top right, Copernicus
is at lower left. The damaged landscape and debris field caused by rubble from the Copernicus impact
is at centre, and the ghost crater Stadius can be faintly seen at lower right.

This image adjoins the one above. The young crater Copernicus has a diameter of 95 km and is
3.75 km deep.  Photographed on August 2, 2017.


This area shows Tranquility Base, site of the landing by Apollo 11's lunar module on July 21, 1969.
It was photographed from Starfield Observatory, Nambour on July 30, 2017. East (where the Sun is
rising) is to the right, north is to the top. The largest crater in the image above is near the centre of the
 left margin, and is called Delambre. The deformed crater towards bottom right is named Torricelli.

This is an enlargement of the previous image. The landing site is shown by an ' x '. Three craterlets have been
officially named after the astronauts. Armstrong is 4.6 km in diameter,
Collins is 2.4 km, and Aldrin is 3.4 km.
The lunar module's landing approach was from the east (right).

Hadley Rille and its environs, where Apollo 15 landed. The Rille varies between 1 and 1.5 km in width,
and is 80 km long.  There are many more rilles to the north.

Comparing the image above with the NASA image below, from Nambour we see the area slightly
foreshortened as we are at 27º South while Hadley Rille is at latitude 26º North.

A photograph of Hadley Rille from an Apollo spacecraft, in orbit around the Moon, cropped to cover the
same area as the previous photograph taken from Nambour, for comparison purposes. The circle
shows the exact landing site. The camera is looking vertically down, so there is no foreshortening.
This was the first mission to include an LRV (lunar roving vehicle).


Theophilus (top), Cyrillus and Catharina (bottom) were photographed from Starfield Observatory, Nambour
on  July 30, 2017.  East (where the Sun is rising) is to the right, north is at the top.

Of these three craters, Theophilus (top) is obviously the newest, for it is more clearly defined and overlaps
Cyrillus. Catharina is the oldest of the three, appearing much more degraded and damaged by continual impacts
 by small meteorites over billions of years, All three craters were named by Giovanni Riccioli in the mid-17th century.
He was a Jesuit priest who knew his history of astronomy and astronomers very well, and used this knowledge
when applying names to the lunar features. The names were not chosen at random, and the three above were
named after people connected with the lost Great Library of Alexandria.

Catharina has a diameter of 100 kilometres and a depth of 3130 metres. It has been damaged by a later impact
on its northern wall, which has produced a 46 kilometre wide crater, Catharina P. The walls of Catharina are
 quite steep in places, but the rugged floor is reasonably flat with no large, central mountains. The floor does
 contain some small hills and fissures, and is disrupted in the south by a 16 kilometre crater called Catharina S.
 Nearby, on the southern wall of Catharina, there is a small, bright, bowl-shaped crater 7 kilometres across, Catharina F.

This photograph was taken 23 minutes after the preceding one on July 30, 2017, which it adjoins. The
crater Catharina is at the top of the image. The Rupes Altai or Altai Mountains is a 450 km long cliff or
fault escarpment which runs in a huge curve from west of Catharina to the 90 km crater Piccolomini
at the lower-right corner. The cliff averages 700 to 1000 metres in height, with some summits approaching
2 km high. One peak is 4 km high.

The crater Petavius has a diameter of 182 kilometres and this photograph was taken from Starfield Observatory,
Nambour on September 14, 2018. East (where the Sun is rising)  is to the top, north is to the left. As Petavius is near
 the south-east limb of the Moon, we see the crater at an angle, which foreshortens its circular shape into an ellipse.
On the southern wall of Petavius (on the right in the picture above, is an 11 kilometre wide crater, Petavius C.
The most spectacular cleft on the Moon runs in a straight line from the central mountain group to the south-west wall.
In this view, the Great Cleft is seen to be relatively shallow in places.

In the foreground is the 60 kilometre wide crater Wrottesley. A peculiar double ridge 200 kilometres long passes
through Petavius C and skirts the end of the Great Cleft, terminating near Wrottesley. 
Behind Petavius (to the east)
is the 42 kilometre wide crater Palitzsch, with the 114 kilometre Vallis Palitzsch (Palitzsch Valley) running to the
north (left),  outside the far wall of Petavius.

The crater Langrenus has a diameter of 136 kilometres. Like Petavius above, this photograph was taken
from  Starfield Observatory, Nambour on September 14, 2018. The orientation and foreshortening of Langrenus
is similar to that of Petavius above, for they are near neighbours on the Moon. The central cluster of
mountain peaks averages one kilometre in height. The north-western area of the floor is rough, while the
southern half is much smoother. The walls have slumped down to make spectacular terraces. Outside
the crater, the landscape has been covered with melted rock from the impact.

This image of the south-western margin of the Moon's Mare Fecunditatis (Sea of Fertility) was taken at
 5:19 pm on 18 July 2018, just five minutes after sunset. A deep red filter was used to counteract the light
 of the sky. North is to the top, east (where the Sun is rising) is to the right. The central crater is 77 km
diameter Gutenberg. To its south-east is the 56 km crater Goclenius, which is crossed by numerous
clefts. Towards the lower left corner of the image is the 34 km crater Gauldibert, which has a very
unusual volcanic floor. The smallest craterlets clearly visible in this image, e.g. one just north of the
mountain at the centre of Goclenius, are less than 600 metres across. Smaller ones in the flat area
 due west of Goclenius may also be detected.

Aristarchus is the bright 41 km crater at right, Herodotus is the flooded 36 km crater to its left.
Vallis Schöteri
(Schröter's Valley) is the remarkable feature to their north, and is 165 km long. The valley
begins at a small crater in the highlands between Aristarchus and Herodotus, widens out and then narrows
again heading north, before zig-zagging to the north-west and then turning to the south-west, where it narrows
further and peters out.  It has been  described as like a snake, in particular as a cobra, and its widest area
near its starting point has become  known as the 'Cobra Head'. A delicate rille 200 metres wide like a dry
water course meanders along the valley, visible above for most of its length. There is a complex of
narrow, winding rilles in the north-eastern corner of  this image.

Gassendi was photographed from Starfield Observatory, Nambour on September 2, 2017. North is to the top,
west is to the left. Gassendi is a moderately large crater, with a diameter of 114 km. It is completely
 circular, but due to its position towards the Moon's west-south-western limb, we see it considerably
foreshortened. It is quite ancient, and since it was formed by the impact of a large meteor or small asteroid
about 3.9 billion years ago, a large more recent impact has deformed its northern wall (on the right-hand side
 in the image above). This later crater is called Gassendi A, and is 33 kilometres across.  Almost adjoining it
on its north-western side is Gassendi B, which is 26 kilometres across. The floor of Gassendi is flat, with a
group of mountains in the centre that average 1200 metres high. To the south  is a large, flat lava plain called
Mare Humorum (the Sea of Humours). The Mare Humorum was caused by an asteroid striking the Moon in
the epoch after Gassendi was formed.

This huge impact blasted out a crater 391 kilometres across, fracturing  the Moon's crust in the area. These
fractures released pressure on the hot rocky layers below, which immediately liquified, allowing hot magma
to come to the surface as lava, which filled up the crater that  had been formed,  resulting in the large, level
 lava plain that was discovered and named the "Sea" of Humours by Giovanni Riccioli in the mid-17th century.

As the lava spread out from the impact crater, much of it reached the southern wall of Gassendi, sweeping
over it and bursting in to pool on the southern end of Gassendi's floor (to the left as seen in the image above).
We can see a gap in Gassendi's southern ramparts where the wall has been completely demolished, and
other parts of the southern wall have been smoothed over by the lava. As the lava cooled, ripples in it became
solid, and can be seen close to the south and south-east walls of Gassendi. The eastern, northern and
western walls, unaffected by the lava flow, are rugged.

The three largest craters above, which once were called ‘walled plains’, are near the centre of the Moon’s
Above centre is the large walled plain, Ptolemæus, which has a diameter of 145 km.  Its flat floor
is marked by numerous craterlets. South of Ptolemæus is another crater plain, Alphonsus, which is
121 km in diameter and has a central peak protruding from a low 'spine'.

There are a number of ash volcanoes occurring along a cleft system around the inside rim of Alphonsus.
Each has a dark halo of ash. To the right of these two large craters is a third, Albategnius, 139 km in diameter.
Adjoining Alphonsus to the south-west is a 41 km crater called Alpetragius, which has an unusually large domed
mountain at its centre.

South of Alphonsus is a smaller crater with a diameter of 100 km called Arzachel. It has very steep slopes with
 terraces where the walls have slumped. There is an off-centre mountain mass which rises to a height of 1500 metres.
On the floor is a 10 km crater, Arzachel A. The southern slopes of this crater are deformed by a later impact
which left  a 4 km crater. Another 4 km crater, Arzachel K, is on the floor slightly to the south of Arzachel A.

A network of rilles curves around  the eastern part of Arzachel's floor. The whole area of  this image is damaged
by  material blasted across the surface by a cataclysmic explosion called the Imbrium Event.  The damage
appears as grooves crossing the image from north-north-west to south-south-east, and is called 'Imbrium sculpture'.
The photograph was taken on August 1, 2017.

At top centre is the 6 km wide crater Hyginus. Its northern wall is deformed by a 2 km wide smaller
crater. Passing through Hyginus is a notable valley or rille, rather disjointed in outline, appearing
in parts to be made up of chains of collapse craterlets. This area of the Moon shows numerous
clefts, extending south past the crater Triesnecker at lower centre.

The south-eastern quadrant of the Moon is covered with overlapping craters ranging in size from large to
tiny. There are no lava plains (known as "Maria" or "seas" in the area. The two largest craters in the image
above are Stöfler (left, deformed on its south-eastern rim by Faraday) and Maurolycus.

Dominating this area is the magnificent crater Clavius, 233 km in diameter.  The walls rise in places
over 3.6 km above the floor. The slopes at lower right exhibit massive land slips. A remarkable series
of five craters begins on the southern wall (top) and trends in ever-decreasing size towards the north,
 then west  (right). The floor of Clavius is covered with numerous craterlets and other delicate features.


Rupes Recta, or the Straight Wall, is a  long cliff in the Moon's Mare Nubium (Sea of Clouds). 100 km
 long and 1 to 1.5 kilometres wide, it is a fault scarp.
Despite its appearance under a low Sun as above,
it is neither particularly high nor steep. The eastern or right-hand side is about 250 metres higher than the
 western, near the wall's mid-section. The slope is actually quite gentle, some sources quoting as little as
seven degrees.

Also in the image are some craters. To the west (left) of the Wall, is the 17 km crater Birt, the eastern rim
of which is deformed by the later impact that created 6.8 km Birt A. Starting in a craterlet just to the west
of Birt is a curved rille called Rima Birt, which is 51 km long and turns to the north-west before fading out.
It has a gap in its middle and a slight S-bend.

The large crater to the right of the image is 60 km Thebit which has a rille on its floor which is unusual in that
it is composed of four straight sections joined at abrupt angles.  Most rilles are sinuous. Thebit A (20 km)
 has deformed the western rim of the larger crater, and is itself deformed by Thebit L (12 km).

The largest crater in this image is Pitatus which is 100 km in diameter. To its west (left) is its 44 km
diameter neighbour Hesiodus. Both of these craters have flat floors with multiple rilles around their
circumferences.  Pitatus has an off-centre mountain massif on its floor, while that of Hesiodus has two
newer impact craters, both bowl-shaped. There is an unusual valley joining the floors of Pitatus and
Hesiodus. A 12 km 'ghost crater', partially submerged by the lava flows from the north, is about 30 km
north of Pitatus, with another to the west. From the western ramparts of Hesiodus, the 309 km long rille
called Rima Hesiodus runs to the south-west and off the image. There are three craterlets visible on this
narrow and shallow valley. They are so well-aligned on the rille that they are probably volcanic vents associated
 with the creation of the rille. It is unlikely that random impacts from space could have landed together exactly
on the rille.


This image shows the crater Hesiodus (above centre) when the Sun was higher, reducing the shadows and flattening
the  contrast. Adjoining Hesiodus to the south-south-west is the 15 km bright crater Hesiodus A. This crater is
remarkable in that it contains two concentric rings like a bulls-eye. The rings only become visible when the Sun is
high enough  to shine over the steep walls and illuminate them. The picture was taken on September 2, 2017.
The rings are only partially visible in the larger picture above, which was taken on August 2, 2017.

The crater Tycho is probably the youngest large crater on the Moon. Its diameter is 88 km and it lies at the centre
of a spectacular system of light-coloured rays. The surroundings are covered with areas of rock melt and
large angular blocks. The central mountain has three peaks and is 1.5 km high.

Posidonius is a large crater 99 km in diameter with a heavily fractured level floor. This image was taken
on November 24, 2017. East is to the top, north to the left. There is a secondary rim  of mountains in the
 eastern interior. The largest crater inside Posidonius has a diameter of 11 km and near it is a fresh 3 km
crater and some smaller craterlets. There are also five volcanic domes inside Posidonius and three more
outside. Of interest is the very sinuous and narrow rille which starts just inside the northern rim and follows
the rim to its north-western curve, where the rille suddenly turns towards the interior and heads south,
aiming for the south-western wall. A branch turns to the right and heads directly to the western wall (lower
margin in the image above). Where the wall is breached near the bottom margin, shadow  reveals that
 the floor of Posidonius is higher than the level of Mare Serenitatis outside the wall.

This area was photographed from Starfield Observatory, Nambour on May 6, 2017. East (where the Sun
 is rising) is to the right, north is to the top. The largest crater in the image above is Milichius, which is a
 minor crater only 14 kilometres in diameter. Milichius is surrounded by a great number of volcanoes, in
the form of low domes. These are of a roughly circular shape, and average only 200 to 300 metres high.
At the summit of each one is a volcanic crater, but all appear to be either dormant or extinct.

Once it was thought that all the craters on the Moon were volcanic in origin, for that is how craters on the
 Earth are generally formed. Not until the beginning of the 19th century did astronomers become aware
 of huge rocky masses flying through space that could impact the Moon, the Earth and other planets.
These rocks, as big as a truck or as big as Tasmania, were called 'asteroids' (star-like) by William Herschel,
as in the telescope they are simply points of light, but they are now called SSSBs (Small Solar System
Bodies) a name they share with comets and meteors. 

More domes are found about 160 km south-east of Milichius in the area shown here, which adjoins the one
above it. The largest crater in this image is Hortensius, 15 km in diameter, towards the lower-left corner
and filled with shadow. There is a fine cluster of eight domes, most with volcanic vents at their summits,
 just north of Hortensius.
Most of these domes are 8 to 12 km in diameter, but are very low for their size.
Their heights range between 300 and 400 metres. Six of the domes are quite prominent - the other two a
little more difficult. There are another three domes elsewhere in the  image - can you find them?

These domes are only observable when the angle of sunlight is small, i.e. the Sun is low to the Moon's
horizon. This produces shadows which reveal the nature of the domes, which appear as low blisters.
As the Sun rises over the Moon, the shadows diminish and soon disappear entirely, the only remaining
features to be observable being the tiny crater vents at the top of most of them. These vents rarely exceed
1000 metres in diameter.

This photograph  of the Sinus Iridum (the Bay of Rainbows) and its environs was taken on December 29,
North is to the top and west is to the left. The Bay is a large semi-circular formation in the north-
western part of the Mare Imbrium, (the Sea of Rains).

The Sinus Iridum is a very large feature, and is visible with the smallest telescope. It is bounded on the
north-east by the Promontorium Laplace (Laplace Promontory) and on the south-west by the
Promontorium Heraclides
(Heraclides Promontory). The mountainous western rim of the Bay is
 called the Montes Jura or Jura Mountains, named after a range near the Alps, on the border between
 France and Switzerland.  The Bay is 411 kilometres across. It has been filled with molten lava from the
Imbrium Event about 3.8 billion years ago, which created the Mare Imbrium. As the lava cooled, waves in its
 surface solidified and can be seen in the image above as 'wrinkle ridges', of which there are more than ten.
The Bay was not completely filled, as its surface is about 600 metres lower than that of the adjoining Mare Imbrium.

There is a pair of remarkable impact craters in the south-eastern corner of the image. They are Helicon
 (left, 26 km across), and Le Verrier (20 km across). Helicon was a Greek Astronomer who was active around
400 BCE. Le Verrier was the man "who discovered Neptune by the point of his pen", i.e. by mathematical
calculation, not by using a telescope. 


For the latest photographs taken from Nambour, click on the

Lunar Feature of the Month Archive





The Stars


Sirius (Alpha Canis Majoris) is the brightest star in the night sky. It has been known for centuries as the
 Dog Star. It is a very hot A0 type star, larger than our Sun. It is bright because it is one of our nearest
 neighbours, being only 8.6 light years away. The four spikes are caused by the secondary mirror supports
in the telescope's top end. The faintest stars on this image are of magnitude 15. To reveal the companion
 Sirius B, which is currently 10.4 arcseconds from its brilliant primary, the photograph below was taken
 with a magnification of 375x, although the atmospheric seeing conditions in the current heatwave were more
turbulent. The exposure was much shorter to reduce the overpowering glare from the primary star.

Sirius is a binary, or double star. Whereas Sirius A is a main sequence star like our Sun, only larger,
 hotter and brighter, its companion Sirius B is very tiny, a white dwarf star nearing the end of its life.
Although small, Sirius B is very dense, having a mass about equal to the Sun's packed into a volume
about the size of the Earth. In other words, a cubic centimetre of Sirius B would weigh over a tonne.
 Sirius B was once as bright as Sirius A, but reached the end of its lifespan on the main sequence
 much earlier, whereupon it swelled into a red giant. Its outer layers were blown away, revealing the
incandescent core as a white dwarf. All thermonuclear reactions ended, and no fusion reactions
 have been taking place on Sirius B for many millions of years. Over time it will radiate its heat away
into space, becoming a black dwarf, dead and cold. Sirius B is 63000 times fainter than Sirius A.
Sirius B is seen at position angle 62º from Sirius A (roughly east-north-east, north is at the top), in
 the photograph above which was taken at Nambour on January 31, 2017.
 That date is exactly 155
 years after Alvan Graham Clark discovered Sirius B in 1862 with a brand new 18.5 inch (47 cm)
 telescope made by his father, which was the largest refractor existing at the time.


Rigel (Beta Orionis, left) is a binary star which is the seventh brightest star in the night sky. It is huge
 when compared with Sirius. Rigel A is a large white supergiant which is 500 times brighter than its
small companion, Rigel B. Yet Rigel B is itself composed or a very close pair of Sun-type stars that
orbit each other in less than 10 days. Each of the two stars comprising Rigel B is brighter in absolute
terms than Sirius. The Rigel B pair orbit Rigel A at the immense distance of 2200 Astronomical Units,
equal to 12 light-days. (An Astronomical Unit or AU is the distance from the Earth to the Sun.) 


Antares, a red supergiant star

The star which we call Antares is a binary system. It is dominated by the great red supergiant Antares A
which, if it swapped places with our Sun, would enclose all the planets out to Jupiter inside itself.
Antares A is accompanied by the much smaller Antares B at a distance of between 224 and 529 AU -
the estimates vary. (One AU or Astronomical Unit is the distance of the Earth from the Sun, or about
150 million kilometres.) Antares B is a bluish-white companion, which, although it is dwarfed by its huge
primary, is actually a main sequence star of type B2.5V, itself substantially larger and hotter than our
 Sun or Sirius.  Antares B is difficult to observe as it is less than three arcseconds from Antares A and
is swamped in the glare of its brilliant neighbour. It can be seen in the picture above, at position angle
 277 degrees (almost due west or to the left) of Antares A. Seeing at the time was about IV on the Antoniadi
 Scale, or in other words below fair. Image acquired at Starfield Observatory in Nambour on July 1, 2017.


The red supergiant star Betelgeuse (Alpha Orionis) is almost a twin of Antares, but has no companion.

Achernar is the ninth brightest star in the night sky. Its visual magnitude ( mv) is  0.45, and it is a hot
 blue-white star of B3 spectral type. The width of the field is 24 arcminutes and the faintest stars are mv 15. 
As it is in the extreme southern sky, it is the only first magnitude star unknown to the ancient Greeks.


Arcturus, an orange K2 giant star, magnitude -0.05.



Gamma Crucis is a red star at the top of the Southern Cross. It shines at magnitude 1.59, and is a giant
star of type M4. The white star seen just to lower right of the main star is a sixth magnitude companion,
 in orbit around the system's barycentre.


The star Regor, properly called Gamma Velorum. There are at least four stars in the system. The brightest
 star in the image above, Gamma Velorum A, is itself a binary or double star composed of a blue supergiant
and a massive Wolf-Rayet star. They are too close to be split optically, being closer than Mercury is to our Sun.
Their double nature is only revealed by examination of their combined spectrum.

The second component to its left, Gamma Velorum B, is also a spectroscopic binary, with a period of less
than two days. The main star in this pair is a blue-white giant, and it is so close to its companion that the
spectrum of the companion is swamped by the other. Wolf-Rayet stars have strong emission lines in their
spectra and will end their lives with Type 1b supernova explosions. The one in Gamma Velorum A is one of
the closest supernova candidates to the Sun. The star's name "Regor" is not ancient nor exotic, but honours
the Apollo astronaut Roger Chaffee, and is simply 'Roger' spelt backwards. It was devised by one of the other
astronauts, Virgil "Gus" Grissom, and is not officially approved. It is allowed to be used as both Chaffee and
 Grissom, along with the third crew member Ed White, died in the Apollo 1 pre-launch fire in 1967.

The optical double star Mu Scorpii, halfway along the body of Scorpius, is a useful test of keen eyesight,
 being only 6 arcminutes apart. Though the two components look similar, it is only a chance alignment,
 not a true binary system. The stars are not related in any way. The upper star of the two is an eclipsing
binary 822 light years distant, while the lower star, a blue-white subgiant, is only 517 light years away.


 A typical nebula, where hydrogen gas is condensing into stars. The Great Nebula in Orion, M42, with its
 smaller companion at left, M43.



The central section of the Great Nebula in Orion.



The brightest spot in the centre of the nebula is illuminated by a famous multiple star system.



Embedded in the centre of the nebula is a multiple star known as the Trapezium.


The Trapezium is composed of four bright white stars, two of which are binary stars with fainter red
 companions, giving a total of six. The hazy background is caused by the cloud of fluorescing hydrogen
 comprising the nebula.



 The spectrum of Vega, an A0
V type star.  This spectrum shows three dark Balmer lines: Hydrogen α,
β and Hydrogen γ. The Balmer series is very pronounced in the spectra of B and A type
 main sequence stars like Vega, Altair and Sirius.



 The spectrum of Beta Gruis, a type M5 III giant star, not on the main sequence. The Balmer lines of
hydrogen are faint, and there are other lines of metals*. The lines in each star's spectrum are unique
 to itself, and act like a bar-code. Each line represents an element present in the star's atmosphere.
 By identifying the lines (which is easily done), then the elements present in the star (what it is made of)
 can be identified.

When this discovery by Bunsen and Kirchhoff became known in 1859, by 1861 the English astronomer
and early lunar photographer Warren de la Rue felt confident enough to say, "If we were to go to the Sun
[or a
star], and to bring away some portions of it and analyse them in our laboratories, we could not
examine them more accurately than we can by this new mode of spectrum analysis.”

The stars in the M7 cluster (also shown below) all have similar spectra, as they were formed together
 out of a nebula and are of the same age and stage of evolution.



The galactic cluster in Scorpius, M7, is also known as Ptolemy's Cluster.


Whereas the stars have continuous spectra overlaid by dark lines, planetary nebulae such as M57 (the
Ring Nebula - also seen below) are composed of gases such as oxygen and nitrogen which are fluorescing
 from intense stellar radiation from the central white dwarf star, producing bright-line spectra.
This gives an image of the circular nebula for each element.

M57 is 0.7 kiloparsecs (2 300 light-years) from Earth. It has a visual magnitude of 8.8 and a photographic
magnitude of 9.7. Photographs taken over a period of 50 years show the rate of expansion of the nrbula
to be about 1 arcsecond per century, which corresponds to a speed of 20-30 kilometres per second.
M57 is illuminated by a central white dwarf or ‘planetary nebula nucleus’ (PNN) whose visual magnitude
is 15.75; its mass is approximately 1.2 solar masses. All the interior parts of this nebula have a blue-
green tinge that is caused to a small extent by the
Hydrogen β line at 486.1 nm, but predominantly by
 oxygen emission lines at 495.7 and 500.7 nm. These so-called ‘forbidden lines’ of doubly ionised
 oxygen occur only in conditions of very low density where there are only a few atoms per cubic centimetre.
In the outer region of the ring, part of the reddish hue is caused by
Hydrogen α emission at 656.3 nm,
the first of the Balmer Series of hydrogen lines. Forbidden lines of ionised nitrogen ( N
II ) contribute to the
 reddish colour at wavelengths of 654.8 and 658.3 nm. Each of these emission lines reveals itself as an image
of the whole nebula. The three brightest ones are easily seen, but there are three more very faint ones visible.

The Ring Nebula, M57, a planetary nebula.


The Trifid Nebula, M20, is a combination of blue reflection nebula, pink emission nebula, and dark molecular clouds.

A planetary nebula, the 'Ghost of Jupiter', NGC 3242, formed when the central star exploded.



 The 'Wishing Well Cluster', NGC 3532.



The Eagle Nebula, M16, a star-forming area.



 This nebula has almost entirely contracted to form a cluster of new, hot, blue stars. Small amounts of wispy
nebulosity remain around the brighter stars. This is the Pleiades star cluster, M45. Such clusters are called
 'open clusters' or 'galactic clusters'.


 Star clouds in Sagittarius, with the dark Snake Nebula obscuring the stars behind. A satellite trail crosses the image.



The cluster IC 2602, known as the 'Southern Pleiades'.


The globular cluster Omega Centauri


The central core of Omega Centauri



There are over 120 globular clusters like this one, on the outer fringes of our galaxy. They contain hundreds
 of thousands of old stars. This example is named NGC104, but is popularly known as 47 Tucanae.

The globular cluster NGC 6752 in the constellation Pavo.


 Proxima Centauri (circled) is an 11th magnitude red dwarf star 4.2 light years away. It is the nearest
 star to the Sun. It orbits the bright binary star Alpha Centauri (at left).

Close-up of the star field around Proxima Centauri


The binary star at the centre of the Alpha Centauri triple system. Both stars are solar types.


The binary star Albireo (Beta Cygni), which is well known for its colour contrast.

The central part of the Eta Carinae nebula, showing dark lanes, molecular clouds, and glowing clouds
of fluorescing hydrogen

The Keyhole, a dark cloud obscuring part of the Eta Carinae Nebula

The Homunculus, a tiny planetary nebula ejected by the eruptive variable star, Eta Carinae


 The Cat's Paw Nebula


 The star Zeta Scorpii and the open cluster Caldwell 76.


The Dumbbell Nebula, M27


The Lagoon Nebula, M8, in Sagittarius, adjacent to Scorpius


The eastern half of the Lagoon Nebula, M8, showing dark Bok globules where protostars are forming


The centre of the Lagoon Nebula

Nebulosity in Scorpius.

The two bright stars at centre form the sting of the Scorpion's tail. Their names are Shaula and Lesath.


Shaula and Lesath are both hot, blue B type stars.


This cluster of new, hot B type stars surrounds the star Theta Carinae, and is sometimes called the
 'Southern Pleiades'.


  Halley's Comet, photographed as it passed in front of the stars of Scorpius in April, 1986.



The Great Spiral M33 in Triangulum.



The Great Galaxy in Andromeda, M31, photographed at Starfield Observatory with an off-the-shelf digital
 camera on 16 November 2007.


NGC 4945, an edge-on spiral galaxy in Centaurus.




The Quasi-Stellar Object 3C-273 is extremely remote.  It lies at a distance of 2440 million light years, over
 one sixth of the way to the edge of the universe. It is 1000 times further away than the Andromeda Galaxy
 shown above.


NGC 5128 was once believed to be a dusty spiral galaxy in collision with an elliptical galaxy.


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