ASTR 1230 (O'Connell) Lecture Notes

1. INTRODUCTION TO THE NIGHT SKY
AND CONSTELLATIONS

Astronomy is primarily an observational science. It is driven more by new observational discoveries than by interpretive insights. Few important astronomical discoveries were predicted, and many were actually accidental. The human imagination has never been a match for the universe.

Astronomical discovery began with the simplest of observations: people looking at the night sky and trying to understand what they were seeing. In the past, most people were well acquainted with the basic features of the night sky. We are unfamiliar with the sky in modern times mainly because of the advent of artificial lighting, which makes it difficult to see the night sky in urban areas (and also unnecessary to know the sky as a pathfinder).

This lecture introduces you to the basic features of the night sky which are visible to the unaided eye and prepares you for the Constellation Laboratory.

A. NAKED-EYE ASTRONOMY

"Naked eye" observations (i.e. without optical aid from lenses or mirrors) were the only kind possible for most of human history! Telescopes were not invented until 1608 AD.

Nonetheless, great accomplishments were possible without telescopes, e.g.:

Determination of the size and shape of the Earth and Moon (Greeks, 500 BC - 200 AD)
Discovery of Earth's motion around the Sun (Copernicus, 1513)
Kepler's Laws of Planetary Motion (1609, based on Tycho's observations), which led to Newton's Laws of Motion and the modern scientific revolution

The human eye is a remarkably capable astronomical instrument. Follow this link for background information on its function and the important observing considerations of dark adaptation and averted vision.

B. MOTIVATIONS TO OBSERVE THE SKY

Astronomy is the "oldest science." Systematic observations of the sky, ranging from crude to sophisticated, were made by nearly all historical cultures, pre-literate and literate.

Initial motivations:

Curiosity---the most enduring motivation for trying to understand nature
Aesthetics
Fear/Religious Belief:
- E.g.: Astrology. This is the idea that the motions of the Sun, Moon, and planets against the stellar background can be used to predict the future and can influence human personalities. It derived from the ancient belief that these objects are living gods, who betray their intentions by their movements. This was obviously a powerful motivation for observing the sky. In the carving shown at the right the Egyptian Pharaoh Akhenaton (ca. 1350 BC) and his family are communing with the Sun god Aten, the source of Akhenaton's power.
  As our scientific understanding grew, astrology lost its interest for most people. We realized that the Sun, Moon, and planets are inanimate objects, moving in highly regular and predictable patterns in response to the well understood force of gravity. Constellations and the Zodiac were recognized to lack physical significance (see below). New planetary bodies were discovered that astrologers had somehow failed to detect. Statistical tests showed no correlation between "sun signs" and personality or personal history. There is no evidence, theoretical or empirical, for astrology. Astrology lingers only as a form of pseudo-science. But it, and related ideas, did play an important historical role in encouraging the systematic observations of the sky that ultimately led to the scientific interpretation of the solar system.

Study of the sky quickly reveals the existence of regular cycles in time of the Sun, Moon, & planets. These became the central concern of early astronomers because of their immense practical value for:

Navigation: on land & sea
Time Keeping
Calendar Keeping: tracking the date & seasons
For early societies (e.g. the Polynesians), these could be critical survival technologies.

C. NAKED EYE MEASUREMENTS

Only a few types of measurements are possible with the naked eye:

1. Angular Separations

Studying the geometry of the sky by measuring angles is the most basic form of astronomy. Apart from time tracking, this was the only accurate quantitative measurement possible before the advent of modern instrumentation.
Measured angles can be all-celestial ("sky", e.g. star-to-star) or celestial-terrestrial. They can be between different celestial objects, between a celestial object and a reference point on Earth, or across a celestial object.
Modern Units: Degrees, minutes, seconds of arc

Full circle = 360 degrees of arc;
1 degree = 60 minutes of arc;
1 arcmin = 60 seconds of arc
Don't confuse these angular units with units of time! Always use the "arc" terminology for clarity.

Examples:

Angles subtended by a quarter at distance D:
[Note: the symbol ~ means "approximately"]

1 degree @ D = 56 in

1 arcmin @ D = 270 feet

1 arcsec @ D = 3 miles

The bowl of the "Big Dipper" is ~ 10 degrees long.

Angular scales of "pan" of Big Dipper

The human eye has 1-2 arcmin resolution---i.e. it cannot distinguish two stars separated by less than 1-2 arcmin.

The Hubble Space Telescope, for comparison, has better than 0.1 arcsec resolution; i.e. it can resolve a quarter at a distance of 30 miles

"Hand-y" measuring scale (see illustration):

1 degree = width of index finger @ arm's length
10 degrees = width of closed fist @ arm's length
20 degrees = distance thumb to little finger on outstretched hand @ arm's length
Example: the diameter of the Sun or Moon is about 0.5 degree. You can block out either with your index finger held @ arm's length. Try it!

2. Brightnesses

Astronomers quote star brightnesses on the magnitude scale. This scale has ancient roots. It was based originally on simply ranking the stars by their apparent brightness as seen with the unaided eye. Without instruments, this kind of ranking is about the best observers can do.
Today, the scale has been quantified in terms of the light power deposited by an individual star per unit area and tied to telescopic measurements made with electronic detectors.
The magnitude scale is logarithmic, open-ended, and runs "backwards" (like a sports ranking scale).
Brighter objects have smaller magnitudes.
The brightest stars are about 0 magnitude; the faintest visible to the naked eye are about 5-6 magnitude. The brighter planets and most familiar stars have magnitudes in the range -4 to +2. There are only 11 stars brighter than magnitude 1 visible from Charlottesville but 1630 stars brighter than magnitude 5.

The faintest objects yet detected (by the Hubble Space Telescope) are 30th magnitude, or over 1 billion times fainter than visible to eye.

The human eye can make only rough measures of magnitudes; accuracy was only possible after the invention of photography and electronics. Magnitudes are discussed further in the notes on Stellar Astronomy.

3. Colors, Shapes (in some cases)
4. Time

Even crude measures of angles and brightnesses, if made systematically over days, months, or years, immediately reveal the presence of repeating time cycles in the motions of the Sun, Moon, and planets. As mentioned above, these were important for their practical value. But they also showed there was order in the universe, even if the origin of the motions was mysterious. They provided strong intellectual stimulus for investigations of the structure of the universe.

D. EASILY VISIBLE PHENOMENA

STARS: form the backdrop or "reference frame" against which other objects' motions are measured. About 2000-5000 are visible to the eye (depending on eyesight) over the whole sky. About 1000 are visible on a dark, clear night from a given location. The brighter stars form conspicuous patterns which seem unchanging (to the eye).

Motion: stars move in lockstep across sky from East to West. Patterns come back to the same location in the sky after slightly less than 24 hours. Star locations in the sky at a given time of night change systematically throughout the year.

Can you see all the stars that exist? NO! There are vast numbers of stars that are invisible to the eye. With our 8" telescopes, we can see stars about 800 times fainter than the naked eye limit---and there are 5 million of these over the whole sky. But our star system (the Milky Way Galaxy) contains about 100 billion stars, and there are billions of galaxies!

SUN: The most obvious astronomical object (and most important for us!). Steady brightness. Has a slow eastward motion relative to the stars (about 1^o per day; we have to infer the Sun's position since the stars are invisible in daylight). Returns to the same place against the star background in one year (365.25 days).

MOON: Very bright, but much fainter than the Sun. More rapid eastward motion relative to the stars (about 13^o per day).

Shows a drastic change in brightness and phase (bright part as a fraction of a full circle) during each cycle, from totally dark to fully illuminated. Takes 29.5 days to return to the same phase (e.g. "full"). This is the cycle we have formalized in our calendar as the month ("moonth"). There are 12 lunar cycles per year.
Note: Moonlight was of enormous practical value before electrical lighting was invented, so the phases of the Moon were closely followed in earlier times.

PLANETS: Less obvious. 5 bright, starlike objects; have a slow, complex motion relative to the stars. In order of speed of motions (fastest to slowest): Mercury, Venus, Mars, Jupiter, Saturn. Two of these (Mercury, Venus) are always found relatively near the Sun; others can be up to 180 degrees away. Although all the planets have perceptible disks in telescopes, the naked eye cannot discern these.

Other, less conspicuous, features visible to the eye (with the modern interpretation):

METEORS: sudden streaks of light in sky; typical rate 5-10 per hour. Small pieces of ice or rock, burning up in Earth's atmosphere. Often called, but are definitely not, "falling stars." Concentrations of debris (from comets) produce "meteor showers," e.g. the Leonids, lasting up to several days.

COMETS: occasional (once every few years) flamelike objects moving slowly through sky over several weeks. Large (~ 1 km) chunks of ice moving through Solar System, heated by Sun. E.g. Hale-Bopp (1997).

STAR CLUSTERS: compact groups of stars, all formed together. E.g. Pleiades, Hyades, M13 (at right). Since all stars in a given cluster have the same age, clusters became the keys to understanding stellar evolution.

DIFFUSE NEBULAE: clouds of interstellar gas lit up by hot stars. A handful are visible without telescopes. E.g. the Great Nebula in Orion. These mark the birthplaces of young stars. Smaller "planetary nebulae" mark the death of old stars.

MILKY WAY: appears as a faint, diffuse band of light arcing across the sky. It is the combined light of millions of distant stars in the plane of our own Galaxy (a massive, flattened star system), seen edge-on.

EXTERNAL GALAXIES: other star systems like our Galaxy. 4 are visible to the eye, 2 of these are in the northern hemisphere. E.g. the Andromeda Galaxy---the most distant object you can see without a telescope. It is 2 million light years from us, meaning that the light you see from it tonight started its journey 2 million years ago. For more discussion of this lookback effect, see this ASTR 121 page.

Interference: sky brightness: your view of the sky is strongly affected by background sky light, both natural and man-made. During the day, sunlight scattered by molecules in the Earth's atmosphere produces the "blue sky" that completely obscures almost all other cosmic objects from our eyesight (though the Moon is often easy to see in daylight, and you can detect Venus if you know where to look). Likewise, near full moon, only the brightest objects are visible in the night sky because of atmospheric scattering of moonlight. City lights create enough local "light pollution" to rival or exceed the effects of the full moon.

E. ORIENTATION IN THE NIGHT SKY
It is important, but difficult, to try to visualize your situation when you look into the sky at night. You are standing on a spherical, spinning, moving planet. What you can see in the sky is determined by the Earth's orientation and position in its orbit around the Sun. Your view of the sky is always made in your "local reference frame".

The local "horizon plane" is the (ideal, imaginary) plane "tangent" to (just touching) the Earth at your location; you can see objects above the plane but not below. The horizon plane sweeps across the sky as Earth spins; it determines the rising and setting of objects. The horizon plane is different at each location on Earth.
The Celestial Sphere (CS) is a geometric construct used to vizualize the positions of astronomical objects.

The celestial sphere is an imaginary hollow sphere centered on Earth. It is shown shaded in the illustration above. Directions to key orienting positions and to each astronomical object are imagined to be marked on the surface of sphere.
Exactly one-half of the celestial sphere (one hemisphere) is always above your local horizon.

The zenith is the point directly overhead on the CS. It is equidistant from all points on the horizon.
The north and south celestial poles are the points on the CS where the projection of Earth's rotation axis pierces the CS. These are fixed points.
The celestial equator is the outward projection of Earth's equator to the CS. It is a "great circle" (i.e. a circle drawn on the celestial sphere with its center coincident with the center of the sphere).
Your meridian is the great circle on the CS that passes through both celestial poles AND your zenith. It runs from due North to due South, splitting the celestial hemisphere in half. The meridian is not marked on the drawing above; instead, see this figure.

The diurnal motion: The daily spin of the Earth on its axis produces an apparent counter-rotation of the CS and its "attached" stars across your local sky. One complete rotation around its axis with respect to the stars takes 23h56m (note--not quite 24 hours). The Earth rotates eastward, so the sky appears to rotate continuously westward. Objects "rise" in the east or "set" in the west when they cross your local horizon plane. See the figure above.

An astronomical object is said to transit when it crosses the meridian. At this time it is farthest from the horizon and highest in the sky.

F. NIGHT SKY SIMULATIONS
We will use the "Starry Night" planetarium software to simulate the appearance and motions of the night sky.

G. CONSTELLATIONS
The stars are not uniformly distributed on the sky. Many of the brighter stars form conspicuous patterns. To the eye, the patterns seem unchanging: the stars appear "fixed" relative to one another. Historically, the patterns were very useful for orientation, navigation, and determining the time of night or the date and so were given names.

(The human brain is wired for this kind of pattern recognition: people who could recognize the tiger lurking in the forest shadows survived better than those who could not.)
Each named pattern is called a constellation. Constellations are associated with mythological figures, animals, instruments, and other features from the natural, human, or religious worlds. An example of the stick-figure pattern associated with "Orion the hunter" is shown at right.

History

It was natural for people to seek deeper meaning in these remote, silent, but majestic figures at the limit of the visible world. So, the constellations often were given important mythological or religious associations. These were, however, strongly culture-dependent, and the same patterns can have very different interpretations in different cultures.

Some associations we recognize today are very ancient, going back to around 2000 BC (e.g. Leo the lion, Scorpio the scorpion. See the carved stone at right; click for enlargement.) Some are new (Microscopium). Few resemble their namesake closely.

The Greeks (500 BC - 200 AD) added rich mythological associations and fanciful stories (e.g. Taurus, Perseus, Andromeda). Aratus' epic poem The Phaenomena (ca. 270 BC) describes the constellations as a memory aid to navigators. Ptolemy's Almagest (135 AD) listed positions of 1022 stars in 48 constellations. His catalogue was used for the next 1400 years(!)

The Romans inherited Greek myths. Names of most constellations are Latin.

Arab astronomers were active 700-1600 AD, and many modern star names have Arabic roots: Algol ("the demon star"), Aldebaran ("the follower"), Betelgeuse ("armpit of the Central One").

1600+: new constellations were added to fill in blanks, mostly in the Southern Hemisphere. E.g. Telescopium, Pyxis (compass). Elaborate & beautiful printed atlases of classical associations appear (an illustration of the north polar constellations from an atlas by Cellerius is shown below).

In 1930 the International Astronomical Union established formal boundaries for 88 constellations that cover the entire celestial sphere. 74 are visible from Charlottesville. Click here for an illustration of the boundaries for Orion.

Significance of the constellations:

Constellations have no physical significance. The associations are arbitrary & man-made. Constellations are not natural groups of stars. The fainter stars in a constellation don't participate in the pattern. Stars in a given constellation lie near the same line of sight from Earth but are not necessarily close to one another in space. (Click here for an illustration in the case of Orion.) Shapes are specific to the Earth's location in 3-D space (a fact not recognized when ancient astrological systems, which attached significance to the shapes, were developed).

The stars are all moving with respect to one another, even though the changes would not be apparent to the eye except over thousands of years. Therefore, constellation patterns are transitory. The changing appearance of the "Big Dipper" (part of Ursa Major) now and 100,000 years from now is shown below. Here is an animation of the motion of the Big Dipper stars over 200,000 years.

Modern astronomers use constellations only as a convenient "address" to roughly locate objects in the sky.

Terminology:

The zodiac ("circle of animals") is the set of constellations through which the Sun passes in the course of a year. The Sun's path is called the ecliptic, and the Moon and bright planets also stay near this path. Given the modern boundaries of the constellations, there are 13 ecliptic constellations. But in classical astronomy (and current-day astrology) there are only 12---one for each month. The ecliptic, and hence zodiac, is determined by the accidental orientation of the plane of Earth's orbit. Most zodiacal constellations are faint and uninteresting (e.g. Libra, Capricorn, Aquarius).

Constellation names: Latin, often translated from Greek

Star names: the brighter stars have "common" names derived from a mix of Greek, Latin, & Arabic. Most stars brighter than 14th magnitude have catalog numbers. Fainter stars---i.e. most stars---are largely uncataloged.

Bright stars have many synonyms since they appear in many catalogs

E.g: the star at the mouth of Canis Major (the large dog); brightest star in the sky

Sirius ("the scorched one" in Greek) --- common name

= Alpha Canis Majoris --- Bayer listing

= 9 Canis Majoris --- Flamsteed listing

= HD 48915 --- Henry Draper Catalog listing

= BD -16 1591 --- Bonner Durchmusterung listing

= SAO 151881 --- Smithsonian Astrophysical Observatory (SAO) listing

= 0645-16 --- Right Ascension/Declination coordinate listing

Bayer's Uranometria (1603) assigned Greek letters: alpha, beta, gamma, etc. to stars, usually in order of brightness, in each constellation; about 1300 stars have Bayer designations.
Flamsteed (1712): numbered stars in each constellation in "Right Ascension" (west to east) order: e.g. 61 Cygni, 40 Eri, etc.; used today for brighter stars without Bayer designations.
SAO catalog numbers are needed to locate stars in the database stored in your Celestron telescope computers.
Modern catalogs contain up to 100 million stars (but this is still only a small fraction of all stars in our galaxy). Most list objects in Right Ascension order.

There are also many catalogues of non-stellar objects, such as nebulae, star clusters, and galaxies. The three you will most frequently encounter are the New General Catalogue ("NGC"), the Messier Catalogue ("M"), and the The Caldwell Catalog of Deep-Sky Objects (an updated version of the Messier Catalogue).

H. COMPLETING LABORATORY 1 AND THE CONSTELLATION QUIZ

Read the Lab 1 chapter in the Manual.

The Lab will be given on the first two usable nights on or after the night of this lecture. You can come to either night. Check the Observatory status via the recorded message (924-7238) after 6:30 PM.

You will work in groups. Each group will be assigned a set of stars and constellations to learn from the required list in the Lab 1 description. After a group has mastered these, they will teach the other groups.

Advice on learning constellations:

Review and disregard the misconceptions about the sky that are listed in Ten Things to Forget About Astronomy.

Because not all objects on the Constellation Quiz are identified by name on your Sky Wheel, consult the following sky charts, which contain labeled objects for the Quiz:

Spring semester skychart

Fall semester skychart

Find the "North Star," Polaris (in Ursa Minor = "the Little Dipper"). Polaris is near to, but not exactly coincident with, the North Celestial Pole. It is not a very bright star. Easiest method is to use the two "pointers" at the end of the bowl of Ursa Major (the Big Dipper). See the sketch below. Alternatively, if Ursa Major is low in the sky, you can use the stars in Cassiopeia as pointers. See this illustration.

Then orient yourself N/S/E/W. When you face Polaris, your right arm is toward the East and your left is toward the West.

Find your zenith and your meridian.

Orient your sky wheel to match the time of night by aligning the date and time tickmarks. (Note: time marked is always Standard---not Daylight Savings--- time.) Using the wheel and pattern recognition, "hop" to other bright stars and groups. Use brighter, more conspicuous constellations to locate others. Practice locating all the constellations, stars, and other features on the Manual list for this semester.

Difficulties with using charts:

The scale of the real sky is very different from a chart

Brightnesses can't be represented well on paper. Relative brightnesses of real stars look very different.

Poor sky transparency, city lights, or moonlight reduce visibility.

Practice using averted vision to find fainter objects: rather than looking directly at the target, stare about 15 degrees away, but concentrate on target location. (This puts the image on a more sensitive part of your retina.)

After you have had time to learn the constellations, you will be examined individually by a TA on your knowledge of the sky. You will be expected to be able to identify 20 constellations, bright stars, or other features of the sky.

Assignment

The Constellation Lab (Lab I) will take place on the next two usable lab nights, starting Monday, 9/5. You must attend one of the two sessions. Whether the Observatory will be open will be announced on the recorded message (924-7238) by 6:30 PM. We will also send an email alert to the class.

It would be a good idea to become familiar with the various forecasts on the ASTR 1230 Weather Page in planning for this and later labs.

To prepare for the Constellation Lab: read Lab 1 description (Secs. 1.1 to 1.8); consult constellation descriptions (Sec. 1.9) as needed.

Download, print, & read lecture notes for Lec 1

Take Review Quiz--Week 2 on the Collab site.

Web links:

ASTR 1230 Link Page. A good starting point.
Ten Things to Forget About Astronomy (R. O'Connell)
The Human Eye as a Detector (R. O'Connell)
Astronomy Without a Telescope (introduction to naked-eye astronomy by N. Strobel)
The Sky Tonight (Sky & Telescope)
Constellation charts and information (International Astronomical Union)
General information on constellations--guides, charts, illustrations (C. Dolan)
Stars & Constellations (J. Kaler)
Heavens Above Charts for Charlottesville

Heavens Above Constellation Charts/Data

Your Sky, an interactive sky-chart maker (J. Walker)
A "live" night sky of your own ("Starry Night" planetarium software)
Ian Ridpath's Star Tales, constellation history & mythology
Constellation Myths (Coldwater Schools)
The Golden Age of the Celestial Atlas (exhibition) (Linda Hall Library)
Historical Celestial Atlases on the Web (R. van Gent)

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Last modified September 2011 by rwo
Text copyright © 1998-2011 Robert W. O'Connell. All rights reserved. Opening fisheye lens picture of comet Hale-Bopp and night sky from Ujue, Spain, April 1997, copyright © J. C. Casado. Illustrations of the celestial sphere copyright © by Nick Strobel. Image of M13 copyright © by J. Ware. These notes are intended for the private, noncommercial use of students enrolled in Astronomy 1230 at the University of Virginia.