Category: Guide to Space

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The small constellation of Telescopium is located just south of the ecliptic plane and was originally charted by Abbe Nicolas Louis de Lacaille who named it. It was later adopted by the IAU as one of the modern 88 constellations. Telescopium spans 252 square degrees of sky – ranking 57th in size. It has 2 primary stars in its asterism and 13 Bayer Flamsteed designated stars within its confines. Telescopium is bordered by the constellations of Ara, Corona Australis, Indus, Microscopium, Pavo and Sagittarius. It is visible to observers located at latitudes between +40° and -90° and its primary stars are best seen at culmination during the month of August.

Since Telescopium is considered a “new” constellation, there is no mythology associated with it – only Abbe Nicolas Louis de Lacaille’s love of all things science and what Telescopium is meant to represent – the telescope of Sir William Herschel. In Lacaille’s time, it was called “Beta Telescopii” and when represented on Johann Bode’s charts, it pointed northwards, towards Sagittarius and Corona Australis. Since Bode actually depicted it clear up into Ophichus, he also changed the name to “Tubus Astronomicus” as well. Later, both the name – and the constellation – became more abbreviated as it was adopted by the International Astronomical Union.

Let’s begin our binocular tour of Telescopium with its brightest star – Alpha – the “a” symbol on our chart. While Alpha is far from bright to our vision, this class B (B3) blue subgiant star shines more than 900 times brighter than our own Sun from a distance of 250 light years away. It is a young star, just beginning to evolve away from a core-hydrogen-fusing dwarf. While it is rotating very slowing, Alpha is also chemically peculiar, because it is a helium rich star with very strong stellar magnetic fields. It is believed that it may someday evolve into a massive white dwarf like Sirius-B.

Now aim your binoculars towards Delta – the “8” symbol. It won’t take long to discover this designation is shared by two stars! That’s right, we’re looking at an optical double star. Delta 1 and Delta 2 are both blue-white B-type subgiant stars, but Delta 1 (slightly brighter) is approximately 800 light years from Earth, while Delta 2 is closer to 1,100 light years distant!

Are you ready for Kappa? That’s the “k” symbol on our chart. Kappa Telescopii is also a visual double star. It is a yellow G-type giant star located 293 light years from our solar system.

Get out large binoculars or a small telescope for a look at a very rare type of variable star – RR Telescopii (RA 20 04 18.54 Dec -55 43 33.2). Here we have an example of what is called a Symbiotic Nova. According to the work of F.L. Crawford: “The optical spectrum of RR Tel is very rich in emission. By comparing the results of this study with previous publications on the subject, it is found that the RR Tel system is advancing towards higher degrees of excitation. It is also shown that several nebular lines (for example, [OIII] 4363 Angstroms and NeIV 4714 Angstroms) demonstrate component structure, perhaps caused by the different densities of the emitting plasmas.” Also, infrared and optical photometric and spectroscopic observations of the symbiotic nova RR Telecopii are used to study the effects and properties of dust in symbiotic binaries containing a cool Mira component, as well as showing “obscuration events” of increased absorption, which are typical for such Mira-type variable stars. RR Telescopii erupted in 1944 and took nearly 1600 days to reach maximum. At its lowest, RR can be as dim as magnitude 11 – or as bright as magnitude 7!

Keep a telescope handy to have a look at globular cluster NGC 6584 (RA 18 : 18.6 Dec -52 : 13). At around magnitude 9, this 8 arc minute sized globular will delight you. Discovered by James Dunlop on June 5, 1826 and cataloged originally as Dunlop 376, you will pull a lot of nice resolution out of the core region with larger aperture. A lot of photometry work has been done on this particular star cluster – looking for calcium abundances, blue straggler stars and hot stars located in the galactic halo region.

Now aim your large telescope towards challenging planetary nebula IC 4699 (RA 18 : 18.5 Dec -45 : 59) At magnitude 12 and nearly stellar in size, this particular planetary nebula will be difficult to distinguish from the field without the aid of a nebula filter which will aid in revealing the small disc.

Sources:
SEDS
Wikipedia
Chart Courtesy of Your Sky.

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Jupiter has the fastest rotation of all the planets in the Solar System, completing one rotation on its axis every 9.9 hours. It sounds like a simple question: what’s the rotation of Jupiter? But finding out the answer was surprisingly complicated.

Why was it so difficult to figure out Jupiter’s rotation? Unlike the inner terrestrial planets, Jupiter is a ball of almost entirely hydrogen and helium. Unlike Mars or Mercury, Jupiter has no surface features that you track to measure the rotation speed; there are no craters or mountains that rotate into view after a specific amount of time.

Jupiter has the fastest rotation of all the planets in the Solar System. This is quite a feat when you consider that Jupiter is also the largest planet in the Solar System; it’s turning a lot of mass very quickly. The rapid rotation causes the planet’s equator to bulge out. Instead of being a perfect sphere, Jupiter looks more like a squashed ball. The bulge at the equator is even visible in small, backyard telescopes.

This bulge dramatically effects the diameter of Jupiter, depending on whether you measure it from the center of Jupiter to the equator or to the poles. The polar radius of Jupiter is 66,800 km, while the equatorial radius is 71,500 km. In other words, points along Jupiter’s equator are actually 4,700 km more distant from the planet’s center.

Jupiter is a ball of gas, and so it actually experiences differential rotation. The rotation takes different amounts of time depending on where you are on the planet. The rotation of Jupiter at its poles takes about 5 minutes longer than the rotation of Jupiter at its equator. So the commonly quoted 9.9 hours is actually an average amount for the entire planet.

Scientists actually use three different systems to calculate the rotation of Jupiter. System 1 is for latitudes 10 degrees north and south of Jupiter’s equator – the rotation is 9 hours 50 minutes. System II is for latitudes north and south of this region, and the rotation rate is 9 hours, 55 minutes. These rates are measured by how long it takes for specific storms to come back into view. The final system, System III, measures the rotation speed of Jupiter’s magnetosphere and is usually considered the official rotation rate.

We have written many articles about Jupiter for Universe Today. Here’s an article about how Jupiter has Van Allen Belts, just like Earth. And here’s an article about how Jupiter is buffeted by the Solar wind.

Want more information on Jupiter? Here’s a link to Hubblesite’s News Releases about Jupiter, and here’s NASA’s Solar System Exploration Guide.

We have recorded a podcast just about Jupiter for Astronomy Cast. Click here and listen to Episode 56: Jupiter.

Reference:
NASA

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If you look up into the night sky on a very clear night, in an area with very little light pollution, you will see a band of stars splashed across the sky. That band is the Milky Way, the spiral galaxy in which our Solar System lies, and where almost every object you can see with your naked eye calls home.

The Solar System is inside the disk of the Milky Way, and orbits in one of the spiral arms at 26,000 light years from the center of the galaxy. We can’t see the spiral structure of the galaxy from our planet because we are inside the disk and have no means of taking images from above or below the galaxy. Images of the Milky Way’s spiral structure are created from computer modeling based on information from stars as they orbit the galaxy.

Much of the Milky Way is invisible to us because we have to look through the plane of its disk – a lot of the Milky Way is on the other side of the galaxy, and there is so much dust and so many bright stars closer to us that we can’t see the stars behind all of this matter. Of the 5,000 to 8,000 stars in the Milky Way visible to the human eye from Earth, one can usually only see about 2,500 at a time. In fact, the few thousand stars we can see of the Milky Way with our naked eye are only about 0.000003% of the 200-400 billion stars that inhabit the spiral!

To see a picture of the entire Milky Way from the surface of the Earth at once, you have to create a mosaic of photographs taken at different times. This is because the Milky Way moves overhead at night with the rotation of the Earth, so can’t be viewed all at once from one spot. Many panoramas of our galaxy can be found on the web, but here’s a few to get you started:  NASA’s Astronomy Picture of the Day, the Spitzer Space Telescope’s very detailed, very large (55-meters long when printed) mosaic available for your perusal here – it’s a large image, so give it a little time to load – and a drawing by Knut Lundmark of over 7,000 stars in the Milky Way made in the 1950s.

To learn more about the Milky Way, visit the rest of the section here at the Guide to Space, listen to Episode 99 of Astronomy Cast, or visit the Students for the Exploration and Development of Space.

Source: NASA

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The ancient zodiacal constellation of Taurus was one of Ptolemy’s original 48 constellations and remains today as part of the official 88 modern constellations recognized by the IAU. It is perhaps one of the oldest constellations of all and may have even been recognized prehistorically. Taurus spreads over 797 square degrees of sky and contains 7 main stars in its asterism with 130 Bayer Flamsteed designated stars located within its confines. It is bordered by the constellations of Auriga, Perseus, Aries, Cetus, Eridanus, Orion and Gemini. Taurus is visible to all observers located at latitudes between +90° and ?65° and is best seen at culmination during the month of January.

There is one major annual meteor shower associated with the constellation of Taurus, the annual Taurids, which peak on or about November 5 of each year and have a duration period of about 45 days. The maximum fall rate for this meteor shower is about 10 meteors per hour average, with many bright fireballs often occuring when the parent comet – Encke – has passed near perihelion. Look for the radiant, or point of origin, to be near the Pleiades.

Taurus is considered by some to be one of the oldest recognized constellations known, and may have even been depicted with the Pleiades in cave paints dating back to 13,000 BC. According to Greek myth, Taurus was the god Zeus, transformed into a bull in order to woo princess Europa, and perhaps could represent one of the Cretean Bull of Herculean fame. The ancient Egyptians also worshiped a bull-god for which this constellation might represent, just as the Arabs also considered it to be bovine by nature. The Hyades cluster was meant to represent the sisters of Hyas, a great hunter, placed in the sky to honor their mourning for the loss of their brother – just as the Pleiades represent the seven sisters of Greek mythology – as well as many other things in many other cultural beliefs. The Persians called this group of stars “Taura”, just as the Arabs referred to it as “Al Thaur”. No matter what way you want to look at it, this handsome collection of stars contains many fine deep sky objects to pique your interest!

Let’s begin our binocular and telescope tour of Taurus with its brightest star- Alpha – the “a” symbol on our map. Known to the Arabs as Al Dabaran, or “the Follower,” Alpha Tauri got its name because it appears to follow the Pleiades across the sky. In Latin it was called Stella Dominatrix, yet the Olde English knew it as Oculus Tauri, or very literally the “eye of Taurus.” No matter which source of ancient astronomical lore we explore, there are references to Aldebaran.

As the 13th brightest star in the sky, it almost appears from Earth to be a member of the V-shaped Hyades star cluster, but this association is merely coincidental, since it is about twice as close to us as the cluster is. In reality, Aldebaran is on the small end as far as K5 stars go, and like many other orange giants, it could possibly be a variable. Aldebaran is also known to have five close companions, but they are faint and very difficult to observe with backyard equipment. At a distance of approximately 68 light-years, Alpha is “only” about 40 times larger than our own Sun and approximately 125 times brighter. To try to grasp such a size, think of it as being about the same size as Earth’s orbit! Because of its position along the ecliptic, Aldebaran is one of the very few stars of first magnitude that can be occulted by the Moon.

Now, head off to Beta Tauri – the “B” symbol on our chart. Located 131 light years from our solar system, El Nath, or Gamma Aurigae, is a main sequence star about to evolve into a peculiar giant star – one high in manganese content, but low in calcium and magnesium. While you won’t find anything else spectacular about El Nath, there is a good reason to remember its position – it, too, get frequently occulted by the Moon. Such occultations occur when the moon’s ascending node is near the vernal equinox. Most occultations are visible only in parts of the Southern Hemisphere, because the star lies at the northern edge of the lunar occultation zone and occasionally it may be occulted as far north as southern California.

Now, turn your binoculars or small telescopes towards Omicron – the “o”. Omicron is sometimes called Atirsagne, meaning the “Verdant One”, but there’s nothing green about this 212 light year distant yellow G-type giant star, only that it has a great optical companion! Be sure to take a look at Kappa Tau, too… the “k”. Kappa is also a visual double star – but a whole lot more. Located 153 light years from Earth, this Hyades cluster member is dominated by white A-type subgiant star K1 and white A-type main sequence dwarf star, K2. They are 5.8 arcminutes, or at least a quarter light year apart. Between the two bright stars is a binary star made up of two 9th magnitude stars, Kappa Tauri C and Kappa Tauri D, which are 5.3 arcseconds from each other and 183 arcseconds from K1 Tau. Two more 12th magnitude companions fill out the star system, Kappa Tauri E, which is 136 arcseconds from K1 Tau, and Kappa Tauri F, 340 arcseconds away from K2 Tau. Still more? Then have a look at 37 Tauri, an orange giant star with a faint optical companion star… or 10 Tauri! 10 Tauri is only 45 light years away, and while it just slightly larger and brighter than our Sun, its almost the same age. It is believed to be a spectroscopic binary star, but you’ll easily see it’s optical companion. What’s more, thanks to noticing a huge amount of infrared radiation being produced by 10, we know it also has a dusty debris disk surrounding it!

Now, let’s have a go at variable stars – starting with Lambda, the upside down “Y” on our map. Al Thaur is in reality a binary star system as well as being an eclipsing variable star. The primary is a blue-white B-type main sequence dwarf star located about 370 light years away. However, located at a distance of 0.1 AU away from it is a white A-type subgiant star, too… and a third player even further away. Watch over a period of 3.95 days as first one, then the other passes in front of the primary star, dimming it by almost a full stellar magnitude! Don’t forget to check out HU Tauri, too. It is also an eclipsing binary star that drops by a magnitude every 2.6 days!

Ready to take a look at Messier 45? Visible to the unaided eye, small binoculars and every telescope, the Pleiades bright components will resolve easily to any instrument and is simply stunning. The recognition of the Pleiades dates back to antiquity and they’re known by many names in many cultures. The Greeks and Romans referred to them as the “Starry Seven,” the “Net of Stars,” “The Seven Virgins,” “The Daughters of Pleione” and even “The Children of Atlas.” The Egyptians referred to them as “The Stars of Athyr,” the Germans as “Siebengestiren” (the Seven Stars), the Russians as “Baba” after Baba Yaga, the witch who flew through the skies on her fiery broom. The Japanese call them “Subaru,” Norsemen saw them as packs of dogs and the Tongans as “Matarii” (the Little Eyes). American Indians viewed the Pleiades as seven maidens placed high upon a tower to protect them from the claws of giant bears, and even Tolkien immortalized the stargroup in The Hobbit as “Remmirath.” The Pleiades have even been mentioned in the Bible! So, you see, no matter where we look in our “starry” history, this cluster of seven bright stars has been part of it.

The date of the Pleiades culmination (its highest point in the sky) has been celebrated through its rich history by being marked with various festivals and ancient rites — but there is one particular rite that really fits this occasion! What could be spookier on this date than to imagine a bunch of Druids celebrating the Pleiades’ midnight “high” with Black Sabbath? This night of “unholy revelry” is still observed in the modern world as “All Hallows Eve” or more commonly as “Halloween.” Although the actual date of the Pleiades’ midnight culmination is now on November 21 instead of October 31. Thanks to its nebulous regions M45 looks wonderfully like a “ghost” haunting the starry skies. Binoculars give an incredible view of the entire region, revealing far more stars than are visible with the naked eye. Small telescopes at lowest power will enjoy M45’s rich, icy-blue stars and fog-like nebulae. Larger telescopes and higher power reveal many pairs of double stars buried within its silver folds. No matter what you chose, the Pleiades definitely rocks!

Our next most famous Messier catalog object in Taurus is M1 – the “Crab Nebula”. Although M1 was discovered by John Bevis in 1731, it became the first object on Charles Messier’s astronomical list. He rediscovered M1 while searching for the expected return of Halley’s Comet in late August 1758 and these “comet confusions” prompted Messier to start cataloging. It wasn’t until Lord Rosse gathered enough light from M1 in the mid-1840’s that the faint filamentary structure was noted (although he may not have given the Crab Nebula its name). To have a look for yourself, locate Zeta Tauri and look about a finger-width northwest. You won’t see the “Crab legs” in small scopes – but there’s much more to learn about this famous “supernova remnant”.

Factually, we know the “Crab Nebula” to be the remains of an exploded star recorded by the Chinese in 1054. We know it to be a rapid expanding cloud of gas moving outward at a rate of 1,000 km per second, just as we understand there is a pulsar in the center. We also know it as first recorded by John Bevis in 1758, and then later cataloged as the beginning Messier object – penned by Charles himself some 27 years later to avoid confusion while searching for comets. We see it revealed beautifully in timed exposure photographs, its glory captured forever through the eye of the camera — but have you ever really taken the time to truly study the M1? Then you just may surprise yourself… In a small telescope, the “Crab Nebula” might seem to be a disappointment – but do not just glance at it and move on. There is a very strange quality to the light which reaches your eye, even though at first it may just appear as a vague, misty patch. To small aperture and well-adjusted eyes, the M1 will appear to have “living” qualities – a sense of movement in something that should be motionless. This aroused my curiosity to study and by using a 12.5″ scope, the reasons become very clear to me as the full dimensions of the M1 “came to light”.

The “Crab” Nebula holds true to so many other spectroscopic studies I have enjoyed over the years. The concept of differing light waves crossing over one another and canceling each other out – with each trough and crest revealing differing details to the eye – is never more apparent than during study. To truly watch the M1 is to at one moment see a “cloud” of nebulosity, the next a broad ribbon or filament, and at another a dark patch. When skies are perfectly stable you may see an embedded star, and it is possible to see six such stars. It is sometimes difficult to “see” what others understand through experience, but it can be explained. It is more than just the pulsar at its center teasing the eye, it is the “living” quality of which I speak -TRUE astronomy in action. There is so much information being fed into the brain by the eye!

I believe we are all born with the ability to see spectral qualities, but they just go undeveloped. From ionization to polarization – our eye and brain are capable of seeing to the edge of infra-red and ultra-violet. How about magnetism? We can interpret magnetism visually – one only has to view the “Wilson Effect” in solar studies to understand. What of the spinning neutron star at its heart? We’ve known since 1969 the M1 produces a “visual” pulsar effect! We are now aware that about once every five minutes, changes occurring in the neutron star’s pulsation effect the amount of polarization, causing the light waves to sweep around like a giant “cosmic lighthouse” and flash across our eyes. For now, l’ll get down of my “physics” soapbox and just let it suffice to say that the M1 is much, much more than just another Messier. Capture it tonight!!

Since we’ve studied the “death” of a star, why not take the time tonight to discover the “birth” of one? Get out your telescope! Our journey will start by identifying Aldeberan (Alpha Tauri) and moving northwest to bright Epsilon. Hop 1.8 degrees west and slightly to the north for an incredibly unusual variable star – T Tauri. Discovered by J.R. Hind in October 1852, T Tauri and its accompanying nebula, NGC 1554/55 set the stage for discovery with a pre-main sequence variable star. Hind reported the nebula, but also noted that no catalog listed such an object in that position. His observance also included a 10th magnitude uncharted star and he surmised that the star in question was a variable. On either account, Hind was right and both were followed by astronomers for several years until they began to fade in 1861. By 1868, neither could be seen and it wasn’t until 1890 that the pair was re-discovered by E.E. Barnard and S.W. Burnham. Five years later? They vanished again.

T Tauri is the prototype of this particular class of variable stars and is itself totally unpredictable. In a period as short as a few weeks, it might move from magnitude 9 to 13 and other times remain constant for months on end. It is about average to our own Sun in temperature and mass – and its spectral signature is very similar to Sol’s chromosphere – but the resemblance ends there. T Tauri is a star in the initial stages of birth! So what exactly are T Tauri stars? They may be very similar in ways to our own Sun but they are far more luminous and rotate much faster. For the most part, they are located near molecular clouds and produce massive outflows of this material in accretion as evidenced by the variable nebula, NGC 1554/55. Like Sol, they produce X-ray emissions, but a thousand times more strong! We know they are young because of the spectra – high in lithium – which is not present at low core temperatures. T Tauri has not reached the point yet where proton to proton fusion is possible! Perhaps in a few million years T Tauri will ignite in nuclear fusion and the accretion disk become a solar system. And just think! We’re lucky enough to see them both…

For a large telescope challenge, let’s try NGC 1514 (RA 4 : 09.2 +30 : 47). This magnitude 10 planetary nebula is fairly small and dim… and it was discovered by William Herschel on November 13, 1790. If he could do it over 300 years ago, so can you! Chances are this particular nebula is a gaseous envelope which surrounds a tight double star, but revealing it was what startled Herschel the most. In his reports he writes: “A most singular phenomena… surrounded with a faintly luminous atmosphere… judgement I may venture to say, will be, that the nebulosity about the star is not of a starry nature”.

Planetary nebulae were first described as “planetary” by William Herschel in 1785. Before then, all were simply considered “nebulae.” It was once thought they were made of stars, but today we know planetaries are created from material given off by a single star. Many show well-defined rings of one type or another. Others – like M1 – are irregularly shaped supernova remnants. NGC 1514’s material is slowly boiled off over time, rather than caused by a violent explosion. It would be very hard to find the neutron central star in M1, but almost any scope can make out NGC 1514’s 10th magnitude fueling star as it quietly cooks away gases to feed its nebulous shroud. Because it is so bright, it can easily overwhelm the eye. This makes NGC 1514 similar to the famous “Blinking Planetary” – NGC 6826 – in Cygnus.

Are you ready for some galactic star clusters? Then let’s head for NGC 1647 (RA 4 : 46.0 Dec +19 : 04). At nearly unaided eye visibility and large enough to be easily seen in small binoculars and telescope, this widely scattered star cluster contains several dozen well resolved members and lots of double stars. The brighter stars are A or B-type main sequence stars, however there are also a few colorful orange giants to delight the eye, and the two brightest are located on the southern edge of the cluster.

Another bright, big and beautiful open star cluster for all optics is NGC 1746 (RA 5 : 03.6 Dec +23 : 49). It contains about two dozen members and although its not very compressed to the telescope, makes a very nice showing in binoculars or a rich field telescope. What’s clever about this particular cluster, is there is also two other open clusters which are superimposed on top! Look for NGC 1750 and NGC 1758 as part of this region as well. While it was debated for many years that Sir William Herschel was crazy when he designated three separate clusters for this region, later science proved him right!

How about another pair of open star clusters? Then have a look at NGC 1817 (RA 5 : 12.1 Dec +16 : 42) and NGC 1807 (RA 5 : 10.7 Dec +16 : 32). Both can be squeezed in the same field in binoculars and resolved very well to the telescope. Found a little less than a hand span northwest of Betelguese, NGC 1807 and NGC 1817 aren’t exactly twins. Both clusters are of similar magnitude and can be seen as faint patches in binoculars. Through a telescope, NGC 1817 appears far more populated with stars than its neighbor. Studies based on stellar motion reveal that NGC 1817 has far more stars than the brighter NGC 1807. Although the two are quite distant from one another in space, we get to see them both as close friends…

Sources:
Chandra Observatory
SEDS
Wikipedia
Chart Courtesy of Your Sky.

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Located just south of the ecliptic plane, the small, dim constellation of Sextans was originally introduced in the 17th century by astronomer Johannes Hevelius. It covers 314 square degrees of sky and ranks 47th in constellation size. Sextans has 3 primary stars in its asterism and 28 Bayer Flamsteed designated stars within its confines. It is bordered by the constellations of Leo, Hydra and Crater. Sextans is visible to all observers located at latitudes between +80° and ?80° and is best seen at culmination during the month of April.

There is one annual meteor shower associated with Sextans which occurs during the daytime. The Sextantids begin their activity on or about September 9 and last through October 9 of each year with the peak date occurring on or about September 27. This daytime radio meteor stream can produce up to three or four per hour at maximum rate.

Since Sextans is considered a relatively “new” constellation, it has no mythology associated with it – only the object which it represents. Its original name – Sextans Uranae – is Latin for the astronomical sextant, an instrument which Johannes Hevelius made frequent use of in his stellar observations. Although the constellation is very faint, its angles do resemble this particular tool with which the ancient astronomer measured and charted star positions and it was adopted as the constellation Sextans by the International Astronomical Union as one of the 88 modern constellations.

Let’s begin our binocular tour with its brightest star – Alpha – the “a” symbol on our map. Just barely visible to the unaided eye and standing right on the celestial equator, Alpha Sextantis shines 122 times brighter than our Sun and is about 3 times larger. Little wonder it appears so dim, considering that its about 285 light years from Earth! At an estimated 300 million years old, Alpha is nearing the end of its hydrogen fusing lifetime and is about to become an orange giant star – one with its pole pointed right at us. Take note of Alpha’s position in the sky… Because thanks to Earth’s nutation, it was 7 arc seconds more to the north a century ago!

Now, shift your attention towards Beta – the “B” symbol. Beta is a a blue-white B-type main sequence dwarf star located about 345 light years from our solar system. While it looks very ordinary… It isn’t. Beta is a Alpha 2 Canum Venaticorum variable star – one that varies its magnitude ever so slightly just about every 15 days or so.

Ready to go to the telescope? Then aim it at Gamma – the “Y” symbol on our chart. Gamma Sextantis is a triple star system approximately 262 light years from Earth. Its two primary components, A and B, are approximately 0.38 arcseconds apart or approximately 30 Astronomical Units With apparent magnitudes of +5.8 and +6.2 this close proximity means you better have a big telescope and some super resolution to pull this pair apart! However, orbiting the binary star pair at a distance of 36 arcseconds, or roughly a hundred times farther out, is Gamma Sextantis C, a 12th magnitude companion that is also gravitationally bound to the system. Faint… But far enough away to be seen!

Before you give up on Sextans, be sure to turn your telescope or big binoculars towards NGC 3115 (RA 10 : 05.2 Dec -07 : 43). With a magnitude of 9 and more than 8 arc minutes of size, the “Spindle Galaxy” is sure to please everyone! This lenticular galaxy was discovered by William Herschel on February 22, 1787. At about 32 million light-years away from us, it might not look large in the eyepiece, but in reality it is several times bigger than our own Milky Way Galaxy. In 1992, a supermassive black hole was observed in NGC 3115 – the largest found to that date. With an estimated mass of 2 billion times the mass of the Sun, astronomers have kept a close eye on activity since its discovery. The galaxy itself appears to be comprised of mostly old stars and the growth of the black hole hasn’t increased in size since it was first observed.

The Chandra X-Ray Telescope has maintained its vigil and according to its press releases: “This is the best black hole candidate that is massive enough to have powered a quasar.”

These findings strengthen the popular view that quasars – the brightest objects in the Universe – are powered by accretion onto massive black holes. Quasars can be seen farther away than any other object. In many cases, their light has been traveling toward us for most of the age of the Universe. Therefore we see quasars as they were long ago. As a result, astronomers can infer how the quasar population evolved with time. They find that quasars were numerous when the Universe was 1/4 of its present age. Now they have mostly died out. So dead quasars should be hiding in many nearby galaxies. Quasar energies imply that the dead remnants should have masses of a billion Suns. The discovery of a supermassive black hole is a crucial confirmation of the black hole accretion theory of quasars.

Ironically, NGC 3115 is otherwise undistinguished. It’s name comes from its listing as object number 3115 in J. Dreyer’s “New General Catalog” of nebulae and star clusters, published in 1888. The galaxy is visible in moderate-sized amateur telescopes as a faint fuzzy patch in the constellation Sextans, The Sextant. But at a distance of 30 million light years, NGC 3115 is more than ten times farther from us than Andromeda or M32. In reality, it is several times bigger than our own Milky Way. But its stars are mostly old, it contains virtually no gas, and little is going on now apart from the stately orbits of its stars. In particular, its nucleus is extremely inactive. The growth of the black hole and the nuclear activity that it feeds are over, unless additional stars wander too close to the center. Whenever that happens, the nucleus is expected to experience a brief but energetic rebirth.

Although these findings support our general picture of quasars, they also highlight a number of unresolved issues. “We have only a very speculative idea of how supermassive black holes form,” Richstone said. “The processes that control their feeding, make them shine, and later turn them off are also poorly understood.” Finding nearby black holes is crucial to further progress. NGC 3115 provides a billion-solar-mass example.”

Sources:
Wikipedia
University of Illinois
Chart Courtesy of Your Sky.

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The constellation of Serpens is unique – being the only one to be divided into two parts. Serpens Cauda represents the eastern half. Serpens was one of the 48 constellations listed by the 1st century astronomer Ptolemy and it remains one of the 88 modern constellations. The entire constellation spans 637 square degrees of sky and contains 9 main stars within its asterism and 57 Bayer Flamsteed designated stars within its confines. Serpens Caput is bordered by the constellations of Aquila, Sagittarius, Scutum and separated from its counterpart by Ophiuchus. Serpens Cauda can be seen by all observers located at latitudes between +80° and -80° and is best seen at culmination during the month of July.

In mythology, Serpens represents a huge snake held by the constellation Ophiuchus. It can either be referred to as simply “Serpens” or by its western half (Caput – the “Snake’s Head”) or its eastern half (Cauda – the “Snake’s Tail”). Ophiuchus was believed to have been the son of Apollo and a healer. According to legend, the snake is also meant to represent healing as it sheds its skin in rebirth.

Let’s begin our binocular tour of Serpens Cauda with its brightest star – Eta Serpentis – the “n” symbol on our map. Eta Serpentis is approximately 61 light years from Earth and it is an orange K-type giant star about 15 times more luminous than our Sun. Don’t forget Xi, the squiggle at the southern border, either… while it’s strictly a visual double star, this 105 light year distant group is very attractive in binoculars!

Are you ready for more? Then let’s head to M16 (RA 18 : 18.8 Dec -13 : 47). While the attendant open cluster NGC 6611 was discovered by Cheseaux in 1745-6, it was Charles Messier who cataloged the object as Messier 16. And he was the first to note the nearby nebula IC 4703, now commonly known as the Eagle. At 7000 light-years distant, this roughly 7th magnitude cluster and nebula can be spotted in binoculars, but at best it is only a hint. As part of the same giant cloud of gas and dust as neighboring M17, the Eagle is also a place of starbirth illuminated by these hot, high energy stellar youngsters which are only about five and a half million years old.

In small to mid-sized telescopes, the cluster of around 20 brighter stars comes alive with a faint nebulosity that tends to be brighter in three areas. For larger telescopes, low power is essential for Messier 16. With good conditions, it is very possible to see areas of dark obscuration and the wonderful notch where the “Pillars of Creation” are located. Immortalized by the Hubble Space Telescope, they won’t be nearly as grand or as colorful as the HST saw them, but what a thrill to know they are there!

For binoculars and all telescopes, let’s take a look a IC 4756 (RA 18 : 39.0 Dec +05 : 27). This huge, 5th magnitude open star cluster is sometimes referred to as “Graff’s Cluster”. Located about about 13,000 light years away from our solar system, you will see far more stars than you can count in this terrific field!

Sources:
Wikipedia
Chandra Observatory
SEDS
Chart Courtesy of Your Sky.

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The constellation of Serpens is unique – being the only one to be divided into two parts. Serpens Caput represents the western half. Serpens was one of the 48 constellations listed by the 1st century astronomer Ptolemy and it remains one of the 88 modern constellations. The entire constellation spans 637 square degrees of sky and contains 9 main stars within its asterism and 57 Bayer Flamsteed designated stars within its confines. Serpens Caput is bordered by the constellations of Hercules, Corona Borealis, Virgo, Libra, Bootes and separated from its counterpart by Ophiuchus. Serpens Caput can be seen by all observers located at latitudes between +80° and ?80° and is best seen at culmination during the month of July.

In mythology, Serpens represents a huge snake held by the constellation Ophiuchus. It can either be referred to as simply “Serpens” or by its western half (Caput – the “Snake’s Head”) or its eastern half (Cauda – the “Snake’s Tail”). Ophiuchus was believed to have been the son of Apollo and a healer. According to legend, the snake is also meant to represent healing as it sheds its skin in rebirth.

Let’s begin our binocular tour of Serpen Caput with its brightest star – Alpha Serpentis – the “a” symbol on our map. Alpha Serpentis goes by the proper name Unukalhai, meaning loosely the “heart of the serpent”. Alpha Serpentis is approximately 73.2 light years from Earth and it is a great binary star for a small telescope. The primary, Alpha Serpentis A is an orange K-type giant star about 15 times larger than our Sun and its 11th magnitude B star is about 58 arcseconds from the primary. But don’t stop there! If skies are steady, power up and keep looking for the 13th magnitude C star located 2.3 arcminutes from A.

Now, aim your telescope towards Theta – the “8” symbol on our chart. Theta Serpentis is located 132 light years from our solar system and goes by the name of Alya, which means “fat tail”. Guess what? It’s also a great multiple star system! Both Theta-1 Serpentis and Theta-2 Serpentis are white A-type main sequence dwarf stars, very close in magnitude and separated by 22 arcseconds, but Theta Serpentis C is a yellow G-type star that is widely separated from this par by about 7 arc minutes.

For binoculars and all telescopes, let’s take a look a Messier 5 (RA 15 : 18.6 Dec +02 : 05). At nearly unaided eye visible, you’ll like this one! This fifth brightest globular cluster in the sky is considered one of the most ancient at 13 billion years old. Located further away from the dusty galactic center, resolution explodes as we move up in aperture. Easily seen as a round ball of unresolved stars in binoculars, small scopes begin to pick up individual stellar points at higher magnifications. Careful attention shows that M5 is not perfectly round. Its brightest 11th and 12th magnitude stars actually are randomly distributed but seem to array themselves in great arcs.

For a big telescope challenge, try NGC 6118 (RA 16 : 21.8 Dec -02 : 17). It is a very low surface brightness, 13th magnitude spiral galaxy, and although its fairly large, it’s pretty hard to see in small telescopes. This quality has given rise to the nickname the “Blinking Galaxy”, since it only seems to appear during averted vision – only to disappear if the angle isn’t right. About 80 million light-years away, NGC 6118 is a grand-design spiral seen at an angle, with a very small central bar and tightly wound spiral arms. Thank to imagining by the VLA, we know more about this galaxy than ever. In 2004 a supernova event was caught near the galaxy’s center – believed to be the collision of two binary stars!

Sources:
SEDS
Chandra Observatory
Wikipedia
Chart Courtesy of Your Sky.

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The small constellation of Scutum was originally created by Johannes Hevelius in 1683 and was later adopted as a permanent constellation by the IAU. It resides just north of the ecliptic plane or about 10 degrees south of the celestial equator and spans 109 square degrees of sky, ranking 84th in constellation size. There are 2 main stars in Scutum’s asterism and it contains 7 Bayer Flamsteed designated stars within its confines. It is bordered by the Aquila constellation, Sagittarius and Serpens Cauda. Scutum is visible to all observers located at latitudes between +80° and ?90° and is best seen at culmination during the month of August.

There is one annual meteor shower associated with the constellation of Scutum – the June Scutiids. Beginning on or about June 2 and ending about July 29th, we pass into the meteoroid stream which brings on the activity. The peak date for this meteor shower is on or about June 27 and the maximum fall rate is 2-4 meteors per hour.

The constellation of Scutum wasn’t named for a mythological figure – but rather for an object to honor a classical one. In, 1683, Johannes Hevelius, who originally named it Scutum Sobiescianum (the shield of Sobieski), did to commemorate the victory of the Polish forces led by King John III Sobieski in the Battle of Vienna, and thus the name refers to Sobieski’s Janina Coat of Arms. Rather fitting, since this particular king helped Hevelius rebuild his observatory after it was destroyed by fire! It’s Latin name means “shield” and the name was later shortened to Scutum when it was adopted as a permanent constellation by the International Astronomical Union.

Let’s begin our binocular tour of Scutum with its brightest star – Alpha – the “a” symbol on our map. Alpha Scuti is an orange class K giant star located about 175 light years from Earth. While it is not uncommon for this type of star to be over 130 times brighter than our Sun and more than 20 times larger – what’s unusual is the way it has evolved. According to its mass, Alpha should be about 2 billion years old and beginning to fuse helium to carbon… However, it has been discovered that Alpha is slightly variable – meaning it could be shedding its outer layer and on the way to becoming a white dwarf star!

Now, have a look at Delta – the “8” symbol on our chart. Here’s a peculiar star if there ever was one… A star so strange that it’s the prototype of its class. Delta is a giant star – but it is also a variable star. Located 187 light years from our solar system, this metal-rich oddity shines 33 times brighter than our Sun, but it’s only about twice as big. Deep inside, it has stopped fusing hydrogen and it is on its way to becoming a red giant star. But, it’s pulsing like a heartbeat… Changing its magnitude by about 20% every 5 to 65 hours. Added to this are periods of 2.79 hours, 2.28 hours, 2.89 hours, and 20.11 hours. All of this adds up to a very complex rhythm which makes Delta unique! Now, take a look in a telescope, too… Because Delta isn’t alone – it is also a binary star. Look for a 12th magnitude companion 15.2 seconds of arc away from the primary and a 9th component 52.2 seconds away.

For binoculars and small telescopes, head off to Messier 11 (RA 18 : 51.1 Dec -06 : 16)! This incredible galactic star cluster was discovered in 1681 by German astronomer Gottfried Kirch at the Berlin Observatory, M11 was later cataloged by Charles Messier in 1764 and first dubbed the “Wild Duck” by Admiral Smyth. To our modern telescopes and binoculars, there is little doubt as to how this rich galactic cluster earned its name – for it has a distinctive wedge-shaped pattern that closely resembles a flight of ducks. This fantastic open cluster of several thousand stars (about 500 of them are magnitude 14 or brighter) is approximately 250 million years old. M11 is easily located by identifying Altair, the brightest star in Aquila. By counting two stars down the “body” of Aquila and stopping on Lambda, you will find your starhop guide. Near Lambda you will see three stars, the centermost is Eta Scuti. Now just aim! Even small binoculars will have no problem finding M11, but a telescope is required to start resolving individual stars. The larger the telescope’s aperture the more stars will be revealed in this most concentrated of all open clusters!

Keep binoculars and rich field telescopes handy as you shift over to Alpha Scutum and check east-northeast for neighboring 7.8 magnitude open cluster NGC 6664 (RA 18 : 36.7 Dec -08 : 13) . Compare the view to Scutum’s other Messier open cluster – similar sized M26 (RA 18 : 45.2 Dec -09 : 24). As one of the faintest Messier clusters, it’s surprising his scope was able to reveal it at all! To locate Messier 26 shift a little less than 3 degrees south-southeast of Alpha. Those with larger scopes should look for a strange void in the middle of the cluster.

Now, let’s go with a large telescope and have a look at globular cluster NGC 6712 (RA 18 : 53.1 Dec -08 : 42). At magnitude 8, it can be captured with smaller aperture, but requires some muscle to resolve! NGC 6712 was probably discovered by Le Gentil on July 9, 1749 when investigating the Milky Way star cloud in Aquila, but we know it was independently discovered by William Herschel on June 16, 1784. As for its nature? That took John Herschel, who was the first to described it as a “globular star cluster” during his observations in the 1830s!

Last, but not least, let’s do something that you don’t even need a telescope for – R Scuti. This terrific red variable star ranges from 4th to 8th magnitude in 142 days. Chances are, R is probably a red supergiant star, surrounded by a shell of material thousands of times bigger than the interior star itself. One day, it will drop its envelope – turning into a planetary nebula and the star into a white dwarf… But until then? We can simply enjoy this beautiful mystery star!

Sources:
Wikipedia
SEDS
Chandra Observatory
Chart Courtesy of Your Sky.

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The small constellation of Sculptor is located south of the ecliptic plane. It was originally charted by Abbe Nicolas Louis de Lacaille who named it “Apparatus Sculptoris” – the Sculptor’s Studio. It was later adopted by the International Astronomical Union as one of the 88 modern constellations and its name shortened to Sculptor. It covers 475 square degrees of sky and ranks 36th in constellation size. Sculptor has 4 main stars in its asterism and contains 18 Bayer Flamsteed designated stars within its boundaries. It is bordered by the constellations of Cetus, Aquarius, Piscis Austrinus, Grus, Phoenix and Fornax. Sculptor is visible to all observers located at latitudes between +50° and ?90° and is best seen at culmination during the month of November.

Since Sculptor is considered a “new” constellation, there is no mythology associated with it – only the story of how its name came to be. French astronomer Nicolas Louis de Lacaille charted the southern hemisphere skies from the Cape of Good Hope during the time period of 1751-1752 and his love of all objects in art and science were portrayed in the names he assigned to his newly created constellations. Depicted on his chart as a fanciful tripod with a carved bust and the artist’s tools, ” l’Atelier du Sculpteur” was later shortened to the simpler term – Sculptor – and adopted by the International Astronomical Union as a permanent constellation.

Let’s begin our binocular tour of Sculptor with its brightest star – Alpha – the “a” symbol on our map. Located approximately 680 light years from Earth, Alpha Sculptoris is a blue-white B-type giant classified as an SX Arietis type variable star and its magnitude varies by 0.01. While changes in brightness and spectral composition that small would never be detectable to the human eye, at one time it was believed to be caused by orbiting black hole – but were later identified to chemical variations in its atmosphere. While Alpha doesn’t appear to be much, take a closer look… It still shines over 1700 times brighter than our own Sun – yet is only 7 times larger! It is one of the weirdest stars you will ever see – a helium weak star that rotates ever-so-slowly. Thanks to this creeping motion, Alpha can generate a huge stellar magnetic field which allows it to concentrate its chemicals in certain areas – and even flip its magnetic poles!

For other binocular attractions, take a look at Beta Sculptoris – the “B” symbol. It’s a a blue-white B-type subgiant star positioned approximately 178 light years from our solar system. Or Gamma – the “Y” symbol – it’s an an orange K-type giant that is 179 light years away… or even Delta – the “8” symbol. Delta is is a triple star system that’s 139 light years distant and the primary component, Delta Sculptoris A, is a white A-type main sequence dwarf star! Take out the telescope and look for a faint, 11th magnitude companion, Delta Sculptoris B, 4 arcseconds, or more than 175 AU, away from it. Orbiting this pair at the much greater separation of 74 arcseconds, is the third player in this drama, the yellow G-type Delta Sculptoris C, which has an apparent stellar magnitude of 9.4.

For telescope observers, one of the greatest challenges you will ever encounter is the Sculptor Dwarf Galaxy (RA 01 : 00.0 Dec -33 : 42). Discovered by Harlow Shapley on photographic plates in 1937, this extreme low surface brightness elliptical galaxy is a member of our own local galaxy group and is about 290,000 light-years away. Use at least a 150mm telescope and an absolute minimum of magnification to spot just a compression in the starfield at this location!

Now, let’s take a look at the Sculptor Group – a a loose group of galaxies near the south galactic pole and one of the closest groups of galaxies to the Milky Way Local Group. At the head of this class is the Sculptor Galaxy – NGC 253 – is an intermediate spiral galaxy (RA 0 : 47.6 Dec -25 : 17). Discovered by Caroline Herschel, this brilliant magnitude 7 beauty is a starburst galaxy, undergoing periods of intense star formation, and can easily be seen with a small telescope or binoculars. However, companion galaxies NGC 247, PGC 2881, PGC 2933, Sculptor-dE1, and UGCA 15 will need much more aperture! This association forms a gravitationally bound core near the center of the group and most other galaxies associated with the Sculptor Group are only weakly gravitationally bound to this core.

While there, drop south and take a look at NGC 288 (RA 00:52:47.5 Dec -26:35:24). This 8th magnitude globular cluster was discovered by Sir William Herschel and can often be spotted in the same binocular field as NGC 253. While this small globular doesn’t appear to be worthy of much attention, think again… In the late 1980’s it was discovered that it is about 3 billion years older than other globular clusters!

Need to take a look at the home of a supernova? The stop by NGC 150 (RA 0 : 34.3 Dec -27 : 48). Home to an event in 1990, this spiral galaxy is also a great radio emitter, too. Even though it will require a larger telescope to catch anything at magnitude 11, it will still give a nice oblong presentation with a bright core region.

For another binocular and small telescope galaxy, take a look at NGC 55 (RA 0 : 14.9 Dec -39 : 11). This huge, magnitude 8 irregular galaxy gives a great, near edge-on presentation and is believed to be very similar to the Large Magellanic Cloud (LMC). Spanning about 50,000 light-years, large telescopes will be able to resolve out brighter regions of emission nebulae – large star forming regions producing new stars.

For an unusual mid-size telescope challenge, take a look at NGC 7793 (RA 23 : 57.8 Dec -32 : 35). At magnitude 9 and about 9 arc minutes in size, you’ll find 10 million light year distant Bennett 130 to be a beautiful spiral with a sharp nucleus and round, hazy spiral galaxy structure. It was discovered by James Dunlop and it is also part of the Sculptor Group. In 2005, the Spitzer Space Telescope was able to pierce through its clouds and take a closer look at star formation driving the evolution of the galaxy.

Don’t forget while you’re in Sculptor to take on large telescope challenges like NGC 7713 (RA 23 : 36.5 Dec -37 : 56) – a 12th magnitude spiral galaxy, NGC 7755 (RA 23 : 47.9 Dec -30 : 31), also 12th magnitude, but a much smaller elliptical galaxy. How about small and faint NGC 24 (RA 0 : 09.9 Dec -24 : 58) or far easier NGC 134 (RA 0 : 30.4 Dec -33 : 15). There’s galaxies galore just waiting to be carved out of Sculptor and enjoyed!

Sources:
SEDS
Chandra Observatory
Wikipedia
Chart Courtesy of Your Sky.