1. Astronomical Observational Techniques Prof. F.M. Walter
AST 443 / PHY 517
Astronomical Observational Techniques
Prof. F.M. Walter

2. I. The Basics The 3 basic measurements: WHERE something is
WHEN something happened
HOW BRIGHT something is
Since this is science, let’s be quantitative!

3. Where
Positions:
2-dimensional projections on celestial sphere (theta, phi)
Theta, phi are angular measures: radians, or degrees, minutes, arcsec
3-dimensional position in space (x,y,z) or (theta, phi, r).
(x,y,z) are linear positions within a right-handed rectilinear coordinate system.
R is a distance (spherical coordinates)
Galactic positions are sometimes presented in cylindrical coordinates, of galactocentric radius, height above the galactic plane, and azimuth.

4. Coordinate Systems
"What good are Mercator's North Poles and Equators Tropics, Zones, and Meridian Lines?" So the Bellman would cry, and the crew would reply "They are merely conventional signs" L. Carroll -- The Hunting of the Snark
Celestial (equatorial): based on terrestrial longitude & latitude
Ecliptic: based on solar system
Altitude-Azimuth (alt-az): local
Galactic: based on Milky Way
Supergalactic: based on supergalactic plane

5. Reference points
Celestial coordinates (Right Ascension α, Declination δ)
δ = 0: projection of terrestrial equator
(α, δ) = (0,0): where ascending node of the ecliptic intersects the celestial equator (the first point of Aries = γ)

6. Reference points Ecliptic coordinates (λ,β)
β = 0: plane of the Earth’s orbit around the Sun
(λ,β) = (0,0) at γ
ε: inclination of the ecliptic to the celestial equator, ε=23o26'21" ".82T - 0".0006T2 + 0".0018T3, (T in Julian Centuries from 2000AD)
north ecliptic pole: 18h +66o33' (J2000)

7. Reference points Altitude-Azimuth (theta, phi)
Theta measured east of north
Azimuth phi measured from horizon to zenith

8. Reference points Galactic (lII, bII)
(lII, bII) = (0,0) is at α=17h42m24s, δ=-28o55'.
North galactic pole: (α,δ) =12h49m, +27o24' (B1950.0).
The galactic equator is inclined to the celestial equator by 62.6o.

9. When
Solar time
Terrestrial time
Sidereal time

10. The Second
The atomic second is the duration of 9,192,631,770 periods of the radiation corresponding to the transition between two hyperfine levels of the ground state of cesium 133.
The solar second is 1/86,400 of the length of one solar day, This second is variable in duration, a consequence of the irregular and unpredictable rotation rate of the Earth.
The ephemeris second is one/31,556, of the length of the tropical year 1900 (vernal equinox to vernal equinox).
The atomic second is the same length as the ephemeris second. The mean solar second equalled the atomic second in 1820.

11. Solar time
Local time.
The Sun transits (crosses the meridian) at noon, local time.
The length of the day varies throughout the year.

12. Civil Time the mean angular velocity of the Sun is 15o per hour.
Civil time consists of 24 time zones, each nominally 15o wide, centered on lines of longitude which are multiples of 15o (there are local variations).
The Eastern time zone is centered on 75o west longitude. Noon EST occurs when the fictitious mean Sun crosses the 75th degree of longitude.
The fictitious mean Sun differs from the true Sun in that it has a constant angular velocity across the sky. The difference (in time) between the true Sun and the fictitious mean Sun, the Equation of Time, reaches nearly +/-15 minutes.

13. The Equation of Time

14. Universal Time
UT is the civil time at 0o longitude (the standard meridian), which passes through Greenwich, England.
UT is also known as Greenwich mean time (GMT), and is military time Zulu (Z).
UT is based on the fictitious mean Sun. UT = 12h + the Greenwhich hour angle (GHA) or Right Ascension of the fictitious mean Sun.
UT1 is UT corrected for the motion of the geographic poles (the Chandler wobble and similar phenomena).
UT2 is UT1 with an extrapolated correction for the spindown of the Earth.
UTC (Coordinated Universal time) is basically UT1, rounded off. Leap seconds are added to keep UTC within 0.9 sec of UT1. UTC is broadcast by WWV radio. You can see this time on the seismograph in the ESS lobby.

15. Atomic Time Kept by atomic clocks since 1958 Stable to 1 part in 1014
Unaffected by the vagaries of the Solar System

16. Ephemeris Time
ET based on the fictitious mean Sun, with the angular velocity of the Sun on January. The RA of the fictitious mean Sun = RA=18h38m45.836s + 8,640, s TE s TE2
ET-UT = s sTE sTE2
Ephemeris time was formally abolished in 1984, and replaced with Terrestrial Time (TT; formerly Terrestrial Dynamical Time (TDT) and Terrestrial Barycentric Time (TBT).
For all practical purposes, TT = UT1.
TT - TAI = 32s.184
TE = (JD )/36525, the number of Julian Centuries since 1900 January 0.5

17. Heliocentric Time Time at the center of the Sun
UT corrected for the light travel time (up to 8.3 minutes)

18. Terrestrial Barycentric Time
TDB = TT sin(g) sin(2g) seconds, where
g = 357o o (JD )
g is the mean anomaly of the Earth in its orbit around the Sun.
TBD is referred to the barycenter of the Solar System. It is an ideal time calculated for an ideal Earth in a circular orbit around the Sun.
The 1.7 ms periodic deviation is a general relativistic effect due to the variation in the gravitational potential around the Earth's orbit.
TCB: ideal time corrected for GR effects in a flat space-time frame far from the Solar System. Due to gravitational time dilation, TCB is 49 sec/century faster than TDB.

19. Keeping it all together
On 1 January 1958:
0:00:00 TAI = 0:00:00 UT2 = 0:00:32.15 ET

20. The Year
Tropical Year: The interval between two transits of the mean Sun through the mean equinoxes x10-6T days. The length of the Tropical Year decreases by 5.36 seconds per century due to precession of the equinoxes. (now considered obsolete)
Sidereal Year: The interval for the Sun to return to the same point on the ecliptic x10-7T days
Anomalistic Year: The time between successive perihelia x10-6T days The Anomalistic Year is 4.5 minutes longer than the sidereal year because the perihelion advances.
Julian Year days.
Gregorian Year days. (accurate to 1 day in 3000 years)
T : number of Julian centuries since 1900 January 0.5 (12h UT). A Julian Century is ephemeris days.

21. Julian Days
the number of ephemeris days elapsed since 12h UT on 1 January, 4713 BC (-4712 AD).
1 ephemeris day = sec
Modified Julian Day (MJD) = JD
1 January 2013, 0:00 UT: JD=
The algorithm:
JD = fix(365.25*f) + fix( *(g+1)) + d + A + 1,720,994.5 where y is the year, m is the month, d is the day of the month, f=y for m>2 and f=y-1 for m<3 g=m for m>2 and g=m+12 for m<3 A=2-fix(f/100) + fix(f/400).
Gregorian civil calendar dates only.

22. Sidereal Time
based on the Earth's sidereal rotation period (rotation with respect to the stars).
sidereal day = 24 sidereal hours, or 23h56m4s Solar time. The difference is due to the angular motion of the earth around the Sun.
The sidereal time is a measured locally.
The local sideral time (LST) is RA of the zenith.
The hour angle HA of an object with right ascension RA is given by HA=LST-RA
GMST (Greenwich Mean Sidereal Time) at 0h UT = TU TU x10-6TU3 seconds
GAST (Greenwich Apparent Sidereal Time) = GMST + the equation of the equinoxes. The Equation of the Equinoxes is the total nutation in longitude time the cosine of the true obliquity of the ecliptic. It ranges from +0.8 to +1.2 seconds.
LAST (Local Apparent Sidereal Time): hour angle of the ascending node of the ecliptic.
LMST (Local Mean Sidereal Time) = GMST - geodetic longitude.
Note 1: both the sideral and solar days are 86,400 seconds long. The sidereal second is shorter than the solar second by x10-10TE
Note 2: TU = (JD )/36525 is the number of Julian Centuries since J2000.0

23. The Inconstancy of Time
Ephemeris time, which is referred to the fictitious mean Sun and the mean Equinox is uniform.
True local time varies from ephemeris time because of:
Periodic variations in the Sun-Earth distance.
Secular changes, including:
Tidal friction, which causes the length of the day to increase by sec/century. dt/t = 4.5x10-8 sec/day, with an acceleration term proportional to t2.
Irregular variations in the Earth's rotation due to small changes in the moment of inertia. The effect is cumulative but unpredictable. Relative to 1972, the effect was seconds in 1871, and seconds in 1907.
Seasonal variations in I due to weather.
man-made changes from reservoirs (increasing I)
sea-level changes

24. How Time Affects Position
Because of
motions of the measurement frame (the precession of the equinoxes) and
intrinsic motions (proper motions),
coordinates specified in the Equatorial coordinate system are strictly valid at only one instant of time.
Therefore, it is necessary to supplement the coordinates with two more pieces of information:
the epoch of the measurement. This is the time at which the position was measured. If one knows the intrinsic motions of a moving object, one can then extrapolate to predict the position at other epochs.
the equinox of the coordinates, which makes the RA and DEC of a stationary object change with time. One reduces the measured position to a standard equinox (e.g., B1950 or J2000), essentially by adding or subtracting the expected precessional shifts. Equinox B1950 was standard prior to about 1980; now J2000 is the standard epoch.
Note that the terms "equinox" and "epoch" are often confused; the correct term can often be discerned from its context. An observation made in 1984 and precessed to J2000 coordinates should be referred to as Epoch 1984, Equinox J2000, but is often simply referred to as "Epoch 2000". If proper motions are negligable, the difference is inconsequential.

25. How Bright
Later…