Chapter27

Incidental Tables

Alan D. Fiala, William F. Van Altena,Stephen T. Ridgway, and Roger W. Sinnott

27.1 The Julian Date. . . . . . . . . . . . . . . . . . . . . . 667

27.2 Standard Epochs. . . . . . . . . . . . . . . . . . . . . . 668

27.3 Reduction for Precession. . . . . . . . . . . . . . . . . 669

27.4 Solar Coordinates and Related Quantities. . . . . . . 670

27.5 Constellations. . . . . . . . . . . . . . . . . . . . . . . 672

27.6 The Messier Objects. . . . . . . . . . . . . . . . . . . . 674

27.7 Astrometry . . . . . . . . . . . . . . . . . . . . . . . . . 677

27.8 Optical and Infrared Interferometry. . . . . . . . . . . 687

27.9 The World’s Largest Optical Telescopes. . . . . . . . 689

27.1 THE JULIAN DATEby A.D. Fiala

The Julian Day Number (JD) is a sequential count that begins at Noon 1 Jan. 4713 B.C. Julian Calendar.

27.1.1 Julian Dates of Specific Years

Noon 1 Jan. 4713 B.C.= JD 0.0Noon 1 Jan. 1 B.C.= Noon 1 Jan. 0 A.D.= JD 172 1058.0Noon 1 Jan. 1 A.D.= JD 172 1424.0A Modified Julian Day (MJD) is defined as JD− 240 0000.5.Table 27.1 gives the Julian Day of some centennial and decennial dates in the Gregorian Calendar.

667

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Table 27.1. Julian date of selected years in the Gregorian calendar [1, 2].

Julian day at noon (UT) on 0 January, Gregorian calendarJan. 0.5 JD Jan. 0.5 JD Jan. 0.5 JD Jan. 0.5 JD

1500 226 8923 1910 241 8672 1960 243 6934 2010 245 51971600 230 5447 1920 242 2324 1970 244 0587 2020 245 88491700 234 1972 1930 242 5977 1980 244 4239 2030 246 25021800 237 8496 1940 242 9629 1990 244 7892 2040 246 61541900 241 5020 1950 243 3282 2000 245 1544 2050 246 9807

Century years evenly divisible by 400 (e.g., 1600, 2000) are leap years. Others are not.

References1. Explanatory Supplement to the Astronomical Almanac. 1992, edited by P.K. Seidelmann

(University Science Books, Mill Valley, CA), pp. 55, 56, 580, 581, 600–6042. Explanatory Supplement to the Astronomical Ephemeris and the American Ephemeris and

Nautical Almanac. 1961, (Her Majesty’s Stationery Office, London), pp. 434–439

27.1.2 Conversion Algorithms

Several algorithms for converting among Julian Calendar Date, Gregorian Calendar Date, IslamicTabular Calendar Date, Indian Civil Calendar, and Julian Day Number, and computing day of theweek, are given in [1]. Probably the most useful of these is the conversion from Gregorian CalendarDate to Julian Day Number, as follows [2]:

Julian Day Numbers run from noon to noon. Define the following integer variables:

JD = Julian Day Number,

Y = calendar year,

M = month,

D = day of month.

Given Y , M , D, compute JD:

JD = (1461 × (Y + 4800 + (M − 14)/12))/4 + (367 × (M − 2 − 12 × ((M − 14)/12)))/12

− (3 × ((Y + 4900 + (M − 14)/12)/100))/4 + D − 32075.

JD ≥ 0, that is, the date is after −4713 November 23.

27.2 STANDARD EPOCHSby A.D. Fiala

The beginning of the Besselian (fictitious) solar year is the instant when the right ascension of thefictitious mean sun, affected by aberration and measured from the mean equinox, is 18h40m.

The Julian year begins at noon on January 0.Table 27.2 gives the Julian Date of several years.

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27.3 REDUCTION FOR PRECESSION / 669

Table 27.2. Julian dates of Julian and Besselian years [1, 2].

Julian year Besselian year

JY JD BY JD

B1850.0 239 6758.203J1900.0 241 5020.0 B1900.0 241 5020.313J1950.0 243 3282.5 B1950.0 243 3282.423

B1975.0 244 2413.478J2000.0 245 1545.0 B2000.0 245 1544.533

B2025.0 246 0675.588J2050.0 246 9807.5 B2050.0 246 9806.643J2100.0 248 8070.0 B2100.0 248 8068.753

References1. Explanatory Supplement to the Astronomical Ephemeris and

the American Ephemeris and Nautical Almanac. 1961, (HerMajesty’s Stationery Office, London), pp. 434–439

2. Explanatory Supplement to the Astronomical Almanac. 1992,edited by P.K. Seidelmann (University Science Books, MillValley, CA), p. 8

27.3 REDUCTION FOR PRECESSIONby A.D. Fiala

Approximate formulas for the reduction of coordinates and orbital elements referred to the meanequinox and equator or ecliptic of date (t) are as follows, as given in the Astronomical Almanac [3],page B19, in all years since 1984:

For reduction to J2000.0 For reduction from J2000.0

α0 = α − M − N sin αm tan δm α = α0 + M + N sin αm tan bmδ0 = δ − N cos αm δ = δ0 + N cos αmλ0 = λ − a + b cos(λ + c′) tan β0 λ = λ0 + a − b cos(λ0 + c) tan β

β0 = β − b sin(λ + c′) β = β0 + b sin(λ0 + c)�0 = � − a + b cos(� + c′) cot i0 � = �0 + a − b sin(�0 + c) cot ii0 = i − b cos(� + c′) i = i0 + b cos(�0 + c)

ω0 = ω − b sin(� + c′) csc i0 ω = ω0 + b sin(�0 + c) csc i

where α and δ are the right ascension and declination; λ and β are the ecliptic longitude and latitude;and �, i , and ω are the orbital elements (referred to the ecliptic) longitude of the node, inclination, andargument of perihelion; the subscript zero refers to epoch J2000.0; and αm and δm refer to the meanepoch.

With sufficient accuracy:

αm = α − 12 (M + N sin α tan δ),

δm = δ − 12 N cos αm,

αm = α0 + 12 (M + N sin α0 tan δ0),

δm = δ0 + 12 N cos αm.

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The precessional constants M, N, etc., are given by

M = 1.◦281 2323T + 0.◦000 3879T 2 + 0.◦000 0101T 3

N = 0.◦556 7530T − 0.◦000 1185T 2 − 0.◦000 0116T 3

a = 1.◦396 971T + 0.◦000 3086T 2

b = 0.◦013 056T − 0.◦000 0092T 2

c = 5.◦123 62 + 0.◦241 614T + 0.◦000 1122T 2

c′ = 5.◦123 62 − 1.◦155 358T − 0.◦000 1964T 2

where T = (t − 2000.0)/100 = (JD − 245 1545.0)/36 525.

27.4 SOLAR COORDINATES AND RELATED QUANTITIESby A.D. Fiala

27.4.1 The Sun’s Coordinates and the Equation of Time:Low-Precision Formulas

The following formulas from any recent Astronomical Almanac [3], page C24, give the apparentcoordinates of the Sun to a precision of 0.◦01 and the equation of time to a precision of 0.m1 between1950 and 2050; on this page the time argument n is the number of days from J2000.0.

n = JD − 245 1545.0

= −2557.5 + day of year (B2-B3) + fraction of day from 0h UT.

The mean longitude of the Sun, corrected for aberration, is

L = 280.◦460 + 0.◦985 647 4n.

The mean anomaly is g = 357.◦528 + 0.◦985 600 3n.

Put L and g in the range 0◦ to 360◦ by adding multiples of 360◦.

The ecliptic longitude is λ = L + 1.◦915 sin g + 0.◦20 sin 2g.

The ecliptic latitude is β = 0◦.The obliquity of ecliptic is ε = 23.◦439 − 0.◦000 000 4n.

The right ascension (in the same quadrant as λ) is α = tan−1(cos ε tan λ).

Alternatively, α may be calculated directly from

α = λ − f t sin 2λ + ( f/2)t2 sin 4λ,

wheref = 180/π and t = tan2(ε/2).

The declination is δ = sin−1(sin ε sin λ).

The distance of the Sun from the Earth, in AU, is

R = 1.000 14 − 0.016 71 cos g − 0.000 14 cos 2g.

The equatorial rectangular coordinates of the Sun, in AU, is

x = R cos λ, y = R cos ε sin λ, z = R sin ε sin λ.

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27.4 SOLAR COORDINATES AND RELATED QUANTITIES / 671

The equation of time (apparent time minus mean time) is

E(in minutes of time) = 4(L − α), where L − α is in degrees.

The horizontal parallax is 0.◦0024.The semidiameter is 0.◦2666/R.The light time is 0.d0058.Similar formulas for the Moon are given in any recent Astronomical Almanac [3], page D46.

27.4.2 The Sun’s Coordinates and the Equation of Time: Tables

In Table 27.3 the Sun’s position and the equation of time are evaluated to low precision to represent atypical year. In addition, the UT of the transit of Aries is given and also the right ascension of Ariesat 0h UT; i.e., the Universal Time of the beginning of the sidereal day, and the sidereal time of thebeginning of the civil day.

The quantities are calculated using the reference in the table. They are the approximate mean ofvalues over a four-year cycle, with range on the order of two units in the last significant digit.

Table 27.3. Sun’s coordinates and equation of time [1].

Date

Sun’s geocentric apparent

α δ Long. Dist.(h m) (deg) (deg) (AU)

Equationof time =

app − meanE − 12h

(m)

Transitof Aries

(h m)

RA ofmidnightmeridian

∼= R(h m)

Jan. 1 18 44 −23.0 280.2 0.9833 −3.2 17 16 6 41Jan. 16 19 50 −21.0 295.5 0.9837 −9.5 16 17 7 40Feb. 1 20 57 −17.3 311.8 0.9853 −13.5 15 14 8 43Feb. 16 21 57 −12.5 327.0 0.9878 −14.1 14 15 9 43Mar. 1 22 47 −7.7 340.3 0.9908 −12.5 13 23 10 35Mar. 16 23 43 −1.9 355.3 0.9947 −8.8 12 24 11 34Apr. 1 0 41 +4.4 11.2 0.9992 −4.0 11 21 12 37Apr. 16 1 36 +10.0 25.9 1.0035 +0.1 10 22 13 36May 1 2 32 +15.0 40.5 1.0075 +2.9 9 23 14 35May 16 3 31 +19.0 55.0 1.0110 +3.7 8 24 15 34Jun. 1 4 35 +22.0 70.4 1.0140 +2.3 7 22 16 37Jun. 16 5 37 +23.3 84.8 1.0158 −0.5 6 23 17 37Jul. 1 6 39 +23.1 99.1 1.0167 −3.7 5 24 18 36Jul. 16 7 41 +21.4 113.4 1.0164 −6.0 4 25 19 35Aug. 1 8 44 +18.1 128.6 1.0150 −6.3 3 22 20 38Aug. 16 9 41 +13.8 143.0 1.0126 −4.4 2 23 21 37Sep. 1 10 40 +8.4 158.5 1.0093 −0.1 1 20 22 40Sep. 16 11 34 +2.8 173.0 1.0054 +5.0 0 21 23 39Oct. 1 12 28 −3.0 187.7 1.0012 +10.2 23 18 0 38Oct. 16 13 23 −8.8 202.5 0.9969 +14.3 22 19 1 38Nov. 1 14 24 −14.3 218.5 0.9926 +16.4 21 16 2 41Nov. 16 15 25 −18.7 233.5 0.9889 +15.3 20 17 3 40Dec. 1 16 28 −21.7 248.7 0.9861 +11.1 19 18 4 39Dec. 16 17 33 −23.3 263.9 0.9842 +4.6 18 19 5 38

Reference1. MICA (Multiyear Interactive Computer Almanac), 1990–2005. 1998, U.S. Naval Obser-

vatory (Willmann-Bell, Richmond, VA).

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With quantities from the table, for a given longitude λeast, the local hour angle HA of the Sun orHA∗ of a star that has right ascension RA∗ is found as follows:

HA∗ = UT + R − RA∗ + λeast,

HA = UT + E + λeast.

27.4.3 The Sun’s Disk

Table 27.4 gives positions on the solar disk for some times during the year. These mean values areaveraged over a four-year cycle 1991–1994.

P = position of North point of Sun’s axis measured eastward from North point of disk.

B0 = heliographic latitude of Earth or central point of disk.

Table 27.4. Sun’s disk [1].

Date P (degrees) B0 (degrees)

Jan. 6 −0.2 −3.6Feb. 5 −13.6 −6.3Mar. 7 −22.9 −7.25Apr. 6 −26.3 −6.3May 6 −23.3 −3.7Jun. 5 −14.1 −0.2Jul. 7 0.0 3.5Aug. 6 12.7 6.1Sep. 5 22.0 7.2Oct. 5 26.2 6.5Nov. 4 24.0 4.1Dec. 4 15.0 0.5

Reference1. MICA (Multiyear Interactive Computer Almanac),

1990–2005. 1998, U.S. Naval Observatory(Willmann-Bell, Richmond, VA).

27.5 CONSTELLATIONSby A.D. Fiala

Table 27.5 lists data for the constellations in the sky.

Table 27.5. Constellation names, genitive endings, English meaning, three-letter contractions,approximate positions, and areas on the sky [1–4].

Genitive α δ AreaConstellation ending Meaning Contraction (h) (deg) (deg2)

Andromeda -dae Chained maiden And 1 40 N 722Antlia -liae Air pump Ant 10 35 S 239Apus -podis Bird of paradise Aps 16 75 S 206Aquarius -rii Water bearer Aqr 23 15 S 980

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27.5 CONSTELLATIONS / 673

Table 27.5. (Continued.)

Genitive α δ AreaConstellation ending Meaning Contraction (h) (deg) (deg2)

Aquila -lae Eagle Aql 20 5 N 652Ara -rae Altar Ara 17 55 S 237Aries -ietis Ram Ari 3 20 N 441Auriga -gae Charioteer Aur 6 40 N 657Bootes -tis Herdsman Boo 15 30 N 907Caelum -aeli Chisel Cae 5 40 S 125Camelopardus -di Giraffe Cam 6 70 N 757Cancer -cri Crab Cnc 9 20 N 506Canes Venatici -num -corum Hunting dogs CVn 13 40 N 465Canis Major -is -ris Great dog CMa 7 20 S 380Canis Minor -is -ris Small dog CMi 8 5 N 183Capricornus -ni Sea goat Cap 21 20 S 414Carina -nae Keel Car 9 60 S 494Cassiopeia -peiae Lady in chair Cas 1 60 N 598Centaurus -ri Centaur Cen 13 50 S 1060Cepheus -phei King Cep 22 70 N 588Cetus -ti Whale Cet 2 10 S 1231Chamaeleon -ntis Chamaeleon Cha 11 80 S 132Circinus -ni Compasses Cir 15 60 S 93Columba -bae Dove Col 6 35 S 270Coma Berenices -mae -cis Berenice’s hair Com 13 20 N 386Corona Australis -nae -lis S crown CrA 19 40 S 128Corona Borealis -nae -lis N crown CrB 16 30 N 179Corvus -vi Crow Crv 12 20 S 184Crater -eris Cup Crt 11 15 S 282Crux -ucis S cross Cru 12 60 S 68Cygnus -gni Swan Cyg 21 40 N 804Delphinus -ni Dolphin Del 21 10 N 189Dorado -dus Dorado fish Dor 5 65 S 179Draco -onis Dragon Dra 17 65 N 1083Equuleus -lei Small horse Equ 21 10 N 72Eridanus -ni River Eridanus Eri 3 20 S 1138Fornax -acis Furnace For 3 30 S 398Gemini -norum Heavenly twins Gem 7 20 N 514Grus -ruis Crane Gru 22 45 S 366Hercules -lis Kneeling giant Her 17 30 N 1225Horologium -gii Clock Hor 3 60 S 249Hydra -drae Water monster Hya 10 20 S 1303Hydrus -dri Sea serpent Hyi 2 75 S 243Indus -di Indian Ind 21 55 S 294Lacerta -tae Lizard Lac 22 45 N 201Leo -onis Lion Leo 11 15 N 947Leo Minor -onis-ris Small lion LMi 10 35 N 232Lepus -poris Hare Lep 6 20 S 290Libra -rae Scales Lib 15 15 S 538Lupus -pi Wolf Lup 15 45 S 334Lynx -ncis Lynx Lyn 8 45 N 545Lyra -rae Lyre Lyr 19 40 N 286Mensa -sae Table (mountain) Men 5 80 S 153Microscopium -pii Microscope Mic 21 35 S 210Monoceros -rotis Unicorn Mon 7 5 S 482Musca -cae Fly Mus 12 70 S 138Norma -mae Square (level) Nor 16 50 S 165Octans -ntis Octant Oct 22 85 S 291Ophiuchus -chi Serpent bearer Oph 17 0 948Orion -nis Hunter Ori 5 5 N 594Pavo -vonis Peacock Pav 20 65 S 378

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Table 27.5. (Continued.)

Genitive α δ AreaConstellation ending Meaning Contraction (h) (deg) (deg2)

Pegasus -si Winged horse Peg 22 20 N 1121Perseus -sei Champion Per 3 45 N 615Phoenix -nisis Phoenix Phe 1 50 S 469Pictor -ris Painter’s easel Pic 6 55 S 247Pisces -cium Fishes Psc 1 15 N 889Piscis Austrinus -is -ni S fish PsA 22 30 S 245Puppis -ppis Poop (stern) Pup 8 40 S 673Pyxis (=Malus) -xidis Compass Pyx 9 30 S 221Reticulum -li Net Ret 4 60 S 114Sagitta -tae Arrow Sge 20 10 N 80Sagittarius -rii Archer Sgr 19 25 S 867Scorpius -pii Scorpion Sco 17 40 S 497Sculptor -ris Sculptor Scl 0 30 S 475Scutum -ti Shield Sct 19 10 S 109Serpens (Caput and -ntis Serpent, Head Ser 16 10 N 429

Cauda Tail 18 5 S +208Sextans -ntis Sextant Sex 10 0 314Taurus -ri Bull Tau 4 15 N 797Telescopium -pii Telescope Tel 19 50 S 252Triangulum -li Triangle Tri 2 30 N 132Triangulum Australe -li -lis S Triangle TrA 16 65 S 110Tucana -nae Toucan Tuc 0 65 S 295Ursa Major -sae -ris Great Bear UMa 11 50 N 1280Ursa Minor -sae -ris Small Bear UMi 15 70 N 256Vela -lorum Sails Vel 9 50 S 500Virgo -ginis Virgin Vir 13 0 1294Volans -ntis Flying fish Vol 8 70 S 141Vulpecula -lae Small fox Vul 20 25 N 268

References1. Transactions I.A.U., 1, 158 (for names and coordinates)2. Davis, G.A., Barton, S.G., & McHugh, D.J. 1943, Pop. Astron., 50, 356 (for meanings and

pronunciations)3. Oravec, E.G. 1958, Sky & Tel., 17, 220 (for meanings and pronunciations)4. Levin, A.E. 1935, in Handbook of the British Astronomical Association, 34 (for constellation area)

27.6 THE MESSIER OBJECTSby A.D. Fiala

Table 27.6 gives information for the Messier objects.

Table 27.6. The Messier objects [1].

α δ

Messier NGC 2000.0 2000.0M IC Typea Con. (h m) (◦ ′) mV Name, etc.

1 1952 Crab Tau 5 34.5 +22 01 8.4 Crab nebula2 7089 Glob Aqr 21 33.5 − 0 49 6.53 5272 Glob CVn 13 42.2 +28 23 6.44 6121 Glob Sco 16 23.6 −26 32 5.95 5904 Glob Ser 15 18.6 + 2 05 5.86 6405 Op Cl Sco 17 40.1 −32 13 4.2 Butterfly

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27.6 THE MESSIER OBJECTS / 675

Table 27.6. (Continued.)

α δ

Messier NGC 2000.0 2000.0M IC Typea Con. (h m) (◦ ′) mV Name, etc.

7 6475 Op Cl Sco 17 53.9 −34 49 3.38 6523 Neb Sgr 18 03.8 −24 23 5.8 Lagoon nebula9 6333 Glob Oph 17 19.2 −18 31 7.9

10 6254 Glob Oph 16 57.1 − 4 06 6.611 6705 Op Cl Sct 18 51.1 − 6 16 5.8 Wild duck cluster12 6218 Glob Oph 16 47.2 − 1 57 6.613 6205 Glob Her 16 41.7 +36 28 5.9 Hercules14 6402 Glob Oph 17 37.6 − 3 15 7.615 7078 Glob Peg 21 30.0 +12 10 6.416 6611 Op Cl Ser 18 18.8 −13 47 6.0 Eagle nebula17 6618 Neb Sgr 18 20.8 −16 11 7.5 Swan or Omega nebula18 6613 Op Cl Sgr 18 19.9 −17 08 6.919 6273 Glob Oph 17 02.6 −26 16 7.220 6514 Neb Sgr 18 02.6 −23 02 8.5 Trifid nebula21 6531 Op Cl Sgr 18 04.6 −22 30 5.922 6656 Glob Sgr 18 36.4 −23 54 5.123 6494 Op Cl Sgr 17 56.8 −19 01 5.524 6603 Op Cl Sgr 18 16.9 −18 29 4.525 I 4725 Op Cl Sgr 18 31.6 −19 15 4.626 6694 Op Cl Sct 18 45.2 − 9 24 8.027 6853 Plan Vul 19 59.6 +22 43 8.1 Dumbbell nebula28 6626 Glob Sgr 18 24.5 −24 52 6.929 6913 Op Cl Cyg 20 23.9 +38 32 6.630 7099 Glob Cap 21 40.4 −23 11 7.531 224 Gal Sb And 0 42.7 +41 16 3.4 Andromeda nebula32 221 Gal E And 0 42.7 +40 52 8.233 598 Gal Sc Tri 1 33.9 +30 39 5.734 1039 Op Cl Per 2 42.0 +42 47 5.235 2168 Op Cl Gem 6 08.9 +24 20 5.136 1960 Op Cl Aur 5 36.1 +34 08 6.037 2099 Op Cl Aur 5 52.4 +32 33 5.638 1912 Op Cl Aur 5 28.7 +35 50 6.439 7092 Op Cl Cyg 21 32.2 +48 26 4.640 2 stars UMa 12 22.4 +58 05 8.0 Winnecke 441 2287 Op Cl CMa 6 46.1 −20 46 4.542 1976 Neb Ori 5 35.4 − 5 27 4.0 Orion nebula43 1982 Neb Ori 5 35.6 − 5 16 9.0 Orion nebula44 2632 Op Cl Cnc 8 40.2 +19 43 3.1 Praesepe (Beehive)45 Op Cl Tau 3 47.0 +24 07 1.2 Pleiades46 2437 Op Cl Pup 7 41.8 −14 49 6.147 2422 Op Cl Pup 7 36.6 −14 30 4.448 2548 Op Cl Hya 8 13.8 − 5 48 5.849 4472 Gal E Vir 12 29.8 + 8 00 8.450 2323 Op Cl Mon 7 02.8 − 8 23 5.951 5194 Gal Sc CVn 13 29.9 +47 12 8.1 Whirlpool52 7654 Op Cl Cas 23 24.2 +61 35 6.953 5024 Glob Com 13 12.9 +18 10 7.754 6715 Glob Sgr 18 55.1 −30 29 7.755 6809 Glob Sgr 19 40.0 −30 58 7.056 6779 Glob Lyr 19 16.6 +30 11 8.257 6720 Plan Lyr 18 53.6 +33 02 9.0 Ring nebula58 4579 Gal SBb Lyr 12 37.7 +11 49 9.859 4621 Gal E Vir 12 42.0 +11 39 9.860 4649 Gal E Vir 12 43.7 +11 33 8.861 4303 Gal Sc Vir 12 21.9 + 4 28 9.762 6266 Glob Oph 17 01.2 −30 07 6.6

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Table 27.6. (Continued.)

α δ

Messier NGC 2000.0 2000.0M IC Typea Con. (h m) (◦ ′) mV Name, etc.

63 5055 Gal Sb CVn 13 15.8 +42 02 8.6 Sunflower64 4826 Gal Sb Com 12 56.7 +21 41 8.5 Black Eye65 3623 Gal Sa Leo 11 18.9 +13 05 9.366 3627 Gal Sb Leo 11 20.2 +12 59 9.067 2682 Op Cl Cnc 8 51.4 +11 49 6.968 4590 Glob Hya 12 39.5 −26 45 8.269 6637 Glob Sgr 18 31.4 −32 21 7.770 6681 Glob Sgr 18 43.2 −32 18 8.171 6838 Glob Sge 19 53.8 +18 47 8.372 6981 Glob Aqr 20 53.5 −12 32 9.473 6994 Op Cl Aqr 20 58.9 −12 38 4 stars74 628 Gal Sc Psc 1 36.7 +15 47 9.275 6864 Glob Sgr 20 06.1 −21 55 8.676 650 Plan Per 1 42.4 +51 34 11.5 Little Dumbbell77 1068 Gal Sb Cet 2 42.7 − 0 01 8.878 2068 Neb Ori 5 46.7 + 0 03 8.079 1904 Glob Lep 5 24.5 −24 33 8.080 6093 Glob Sco 16 17.0 −22 59 7.281 3031 Gal Sb UMa 9 55.6 +69 04 6.882 3034 Gal Irr UMa 9 55.8 +69 41 8.483 5236 Gal Sc Hya 13 37.0 −29 52 10.184 4374 Gal E Vir 12 25.1 +12 53 9.385 4382 Gal So Com 12 25.4 +18 11 9.386 4406 Gal E Vir 12 26.2 +12 57 9.287 4486 Gal Ep Vir 12 30.8 +12 24 8.6 Radio gal88 4501 Gal Ep Com 12 32.0 +14 25 9.589 4552 Gal E Vir 12 35.7 +12 33 9.890 4569 Gal Sb Vir 12 36.8 +13 10 9.591 4548 Gal S Com 12 35.4 +14 30 10.292 6341 Glob Her 17 17.1 +43 08 6.593 2447 Op Cl Pup 7 44.6 −23 52 6.294 4736 Gal Sb CVn 12 50.9 +41 07 8.195 3351 Gal SBb Leo 10 44.0 +11 42 9.796 3368 Gal Sa Leo 10 46.8 +11 49 9.297 3587 Plan UMa 11 14.8 +55 01 11.2 Owl nebula98 4192 Gal Sb Com 12 13.8 +14 54 10.199 4254 Gal Sc Com 12 18.8 +14 25 9.8

100 4321 Gal Sc Com 12 22.9 +15 49 9.4101 5457 Gal Sc UMa 14 03.2 +54 21 7.7 Pinwheel102 5866 Gal Sa Dra 15 06.5 +55 46 10.0103 581 Op Cl Cas 1 33.2 +60 42 7.4104 4594 Gal Sa Vir 12 40.0 −11 37 8.3 Sombrero105 3379 Gal E Leo 10 47.8 +12 35 9.3106 4258 Gal Sb CVn 12 19.0 +47 18 8.3107 6171 Glob Oph 16 32.5 −13 03 8.1108 3556 Gal Sb UMa 11 11.5 +55 40 10.0109 3992 Gal SBc UMa 11 57.6 +53 23 9.8

NoteaOp Cl = open cluster; Glob = globular cluster; Plan = planetary nebula; Neb = diffuse nebula;

Gal = galaxy (with classification).

Reference1. The Observer’s Handbook—1991, (Royal Astronomical Society of Canada), p. 209

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27.7 ASTROMETRY / 677

27.7 ASTROMETRYby W.F. van Altena

27.7.1 Astrometric Catalogues

Summary statistics and bibliographies for astrometric catalogs are given in Table 27.7. Newly plannedcatalogs are described in Table 27.8. Table 27.9 lists the major Schmidt telescope astrometric surveys.Table 27.10 summarizes the data available to the authors on the status of the major Schmidt telescopesurveys and the process of their digitization as of May 1993. See also the paper and table byMorgan [4].

Tables 27.11–27.13 summarize data on catalogs providing surveys of relative proper motions,catalogs compiling stars with proper motions larger than some limit, and catalogs that compile varietiesof data for a specific type of star, e.g., all bright stars, stars nearer than some distance, etc. The columnsin each table are similar and list, respectively, a reference to the source where the catalog may be found,an acronym for the catalog, number of stars, declination coverage, date of publication (Tpub), magnitudelimit, parallax limit (π ), proper motion or some other kind of limit (µ limit), and a brief description ofthe catalog. More detailed compilations may be found in [5–10].

Most of the acronyms used in the tables are: FK3 = Third Catalogue of the AstronomischesGesellshaft; FK5 = Fifth Fundamental Catalogue; IRS = International Reference Stars; KSZ = FaintStar Catalogue; ACRS = Astrographic Catalogue Reference Stars; PPM = Positions and ProperMotions; CPC = Cape Photographic Catalogue; BKAT = Bright Star Catalogue; NPM = NorthernProper Motion survey; SPM = Southern Proper Motion survey; HIC = Hipparcos Input Catalogue;FHST = Fixed Head Star Tracker catalogue; SAOSC = Smithsonian Astrophysical ObservatoryStar Catalogue; FASTT = Flagstaff Astrometric Scanning Transit Telescope; POSS = PalomarObservatory Sky Survey; AAO-SES = Anglo Australia Observatory Second Epoch Survey; SERC-I/SR = Science and Engineering Research Council Infrared and Short Red survey; GSC = HubbleSpace Telescope Guide Star Catalogue; GAC = HST CGS second epoch positions; IFRS =Intermediate Fundamental Reference Stars; FON = Four-Fold Coverage of Northern Sky; EKAT =Equatorial Catalogue; DENIS = Deep Near Infrared Southern Sky Survey; ESO-B = EuropeanSouthern Observatory Blue Survey; ESO-R; ESO Red Survey; SERC-J/R = Science and EngineeringResearch Council J and R Survey; STSCIdig = Space Telescope Science Institute digitization;ROEdig = Royal Observatory Edinburgh digitization; CAMdig = Cambridge digitization; APS =University of Minnesota Automated Plate Scanner; USN PMM = U.S. Naval Observatory PrecisionPlate Measuring Machine; BPM = Bruce Proper Motion Survey; Lowell N = Lowell ProperMotion Survey Northern Hemisphere Catalogue; Lowell S = Lowell Proper Motion Survey SouthernHemisphere Catalogue; LP = Luyten Palomar Proper Motion Survey; Calan = Cerro CalanObservatory, Chile; NLTT = New Luyten Catalogue of stars with proper motions greater than TwoTenths of an arc second; LHS = Luyten Half Second Catalogue; BSC V = Yale Bright Star Catalogue;BSC Supp. = Yale Bright Star supplement; CNS 3 = Catalogue of Nearby Stars, Heidelberg;CNSG = Catalogue of Nearby Stars with Ground-based parallaxes; CNSH = Catalogue of NearbyStars with Hipparcos-based parallaxes; YPC = Yale Parallax Catalogue; WDS = Washington DoubleStars; CHARA = Center for High Angular Resolution. Georgia State; Orbits = Visual double StarOrbit Catalogue; ADC CDL = Astronomical Data Center CD-ROM.

Machine-readable versions of all catalogues may be obtained at the Astronomical Data Center atGoddard Space Flight Center [11], at Data Centers in other countries, and normally at World Wide Websites at each institution. Recent reviews are also given by van Altena [12] and [13, 14]. Astrometricdata and references for open clusters, globular clusters, and radio astrometry may be found in [15],pages 215 and 250.

Sp.-V/AQuan/1999/10/27:16:16 Page 677

678 / 27 INCIDENTAL TABLESTa

ble

27.7

.Cat

alog

ues

ofpo

siti

ons

and

prop

erm

otio

ns.a

Num

ber

σp

σp

Ref

eren

ceC

atal

ogue

star

sC

over

age

T pub

m(T

pub)

(200

0)σ

µD

escr

iptio

n

[1]

Hip

parc

os11

821

8A

llsk

y19

9112

.40.

86.

20.

7O

nth

eIC

RS/

ICR

Fb,c

syst

em[1

]Ty

cho

105

833

2A

llsk

y19

9111

.525

······

On

the

Hip

parc

ossy

stem

[2]

AC

2000

462

183

6A

llsk

y19

0711

.522

0···

2.7

Re-

redu

ced

Ast

rogr

aphi

cC

atal

ogue

onH

ippa

rcos

syst

em[2

]A

CT

988

758

All

sky

1991

11.5

2536

2.7

Prop

erm

otio

nsfr

om[1

,2]

onH

ippa

rcos

syst

em[3

]FK

51

535

All

sky

1950

7.0

2040

0.7

The

fund

amen

talr

efer

ence

fram

e[4

]FK

5E

xt.

311

7A

llsk

y19

449.

555

156

2.6

Fain

text

ensi

onto

the

FK5

[4]

IRS

I29

163

All

sky

1950

9.5

8022

54.

2In

tern

atio

nalR

efer

ence

Star

s[5

]IR

SII

706

4A

llsk

y19

509.

512

034

66.

5L

ower

prec

isio

nex

tens

ion

ofIR

SI

[6]

KSZ

2181

7δ

≥−3

019

609

150

······

Incl

uded

inth

eIR

SC

atal

ogue

[4,5

][7

]A

CR

SI

250

052

All

sky

1950

10.5

8825

34.

7Po

sitio

nsan

dpr

oper

mot

ions

[8]

AC

RS

II70

159

All

sky

1950

10.5

140d

404

7.5d

Low

erpr

ecis

ion

exte

nsio

nof

AC

RS

I[9

]PP

MN

181

731

Nor

th19

3110

.510

031

34.

3Po

sitio

nsan

dpr

oper

mot

ions

,nor

th[1

0]PP

MS

197

179

Sout

h19

6210

.573

135

3.0

Posi

tions

and

prop

erm

otio

ns,s

outh

[11]

CPC

227

613

1So

uth

1967

10.5

54···

···Po

sitio

nalc

atal

ogue

[12]

CPC

454

875

Sout

hV

ar.

10V

ar.

Var

.V

ar.

The

Cap

ePh

otog

raph

icC

atal

ogue

sfo

r19

50[1

3]Y

ale

Zon

e22

133

8A

llsk

yV

ar.

10V

ar.

Var

.V

ar.

The

Yal

eZ

one

Cat

alog

ues,

inte

grat

edve

rsio

nav

aila

ble

[14]

AG

K3

183

173

Nor

th19

4410

.521

058

910

Posi

tions

;mot

ions

from

AG

K3–

AG

K2

[15]

AG

K3U

170

464

Nor

th19

5110

.511

830

85.

8Po

sitio

ns;m

otio

nsfr

omA

GK

3,A

GK

2,an

dth

ere

vise

d[2

5][1

6]B

KA

T4

949

All

sky

1969

5.9

8096

1.7

Bri

ghts

tar

cata

logu

eof

posi

tions

and

prop

erm

otio

ns[1

7]N

PM1

148

940

+90

to−2

319

6818

150

200

5A

bsol

ute

prop

erm

otio

nsw

ithre

spec

tto

gala

xies

,out

side

Milk

yW

ay,p

ositi

oner

ror

for

1950

[18]

SPM

-1.0

5000

0−2

2to

−45

1980

1839

824

Abs

olut

epr

oper

mot

ions

with

resp

ectt

oga

laxi

esT

heSo

uth

Gal

actic

Pole

[19]

HIC

118

209

All

sky

Var

.12

.5···

300

4H

ippa

rcos

Inpu

tC

atal

ogue

(pos

ition

aler

ror

for

1990

)[2

0]FH

ST21

985

9A

llsk

yV

ar.

9.0

Var

.V

ar.

Var

.H

STst

artr

acke

rca

talo

gue,

com

plet

eto

8.5

[21]

SAO

SC25

899

7A

llsk

y19

309

200

1070

15A

ccur

acy

atpu

blic

atio

nda

te,

notm

ean

epoc

h

Sp.-V/AQuan/1999/10/27:16:16 Page 678

27.7 ASTROMETRY / 679Ta

ble

27.7

.(C

onti

nued

.)

Num

ber

σp

σp

Ref

eren

ceC

atal

ogue

star

sC

over

age

T pub

m(T

pub)

(200

0)σ

µD

escr

iptio

n

[22]

SKY

2000

300

000

All

sky

1991

90.

8–25

6.2–

360.

7–2.

7N

ASA

oper

atio

nsca

talo

gue;

data

from

[1,2

][2

3]SK

YM

AP

248

558

All

sky

1930

920

010

7015

NA

SAop

erat

ions

cata

logu

e[2

4]M

SXIR

177

860

All

sky

Var

.8

Var

.V

ar.

Var

.R

efer

ence

cata

logu

efo

rin

frar

ed,

mag

.lim

it≥

8in

K[2

5]H

STG

SC2

×10

7A

llsk

y19

8016

250

······

HST

Gui

deSt

arC

atal

ogue

,Tab

le27

.9[3

,9,1

0][2

6]U

SNO

-A1.

04.

9×

108

All

sky

Var

.20

–21

250

······

USN

OPM

MSt

arC

atal

ogue

,N

orth

from

[30,

31]

Sout

hfr

om[3

2,33

][2

7]U

SNO

-A2.

04.

7×

108

All

sky

······

150

······

USN

OA

1.0

onth

eIC

RS

syst

emb

[28]

USN

O-T

AC

N70

567

9δ

≥−1

819

8112

90···

···U

SNO

Twin

Ast

rogr

aph

Cat

alog

ue[2

9]U

SNO

-FA

STT

661

591

Equ

ator

ial

1995

17.8

45···

···C

CD

tran

sit

tele

scop

eca

talo

gue,

|δ|<

1.6

degr

ees

Not

esa

T cis

the

cent

rale

poch

,mth

em

agni

tude

limit,

σp(T

c)th

eer

ror

inm

illi-

arcs

ec(m

as)

ofa

posi

tion

atth

ece

ntra

lepo

ch,σ

p(2

000)

the

erro

rof

apo

sitio

nin

mas

at20

00,σ

µth

eer

ror

ofa

prop

erm

otio

nin

mas

/yr.

bT

heex

trag

alac

ticre

fere

nce

syst

emof

the

Inte

rnat

iona

lEar

thR

otat

ion

Serv

ice

(IC

RS)

,Ari

as,E

.F.e

tal.

1995

,A&

A,3

03,6

04.T

heIC

RS

defin

esth

eax

esof

the

syst

emus

ing

212

ofth

ebe

st-o

bser

ved

extr

agal

actic

sour

ces.

The

seax

esar

eto

bem

aint

aine

dby

the

Inte

rnat

iona

lEar

thR

otat

ion

Serv

ice.

c Defi

niti

onan

dR

eali

zati

onof

the

Inte

rnat

iona

lCel

esti

alR

efer

ence

Syst

emby

VL

BI,

Ast

rom

etry

ofE

xtra

gala

ctic

Obj

ects

,edi

ted

byM

a,C

.and

Feis

selM

.,IE

RS

Tech

nica

lNot

e23

,199

7.T

heIC

RF

isa

larg

erse

tof

sour

ces

(abo

ut61

0)th

atpr

ovid

eth

efid

ucia

lpoi

nts

for

the

syst

em.

dE

stim

ated

valu

e.

Ref

eren

ces

1.E

SA-S

P12

00,1

997;

Pro

ceed

ings

ofth

eH

ippa

rcos

’97

Veni

ceC

onfe

renc

e,E

SASP

-402

1997

2.U

rban

,S.E

.,C

orbi

n,T.

E.,

&W

ycof

f,G

.L.,

1997

,U.S

.Nav

alO

bser

vato

ry,A

stro

grap

hic

Cat

alog

uepo

sitio

nsre

redu

ced

usin

gth

eA

CR

San

dth

enpl

aced

onth

eH

ippa

rcos

syst

em[1

].Pr

oper

mot

ions

from

[1,2

].3.

Fric

ke,W

.eta

l.19

88,F

ifth

Fun

dam

enta

lCat

alog

ue(F

K5)

,Par

tI:T

heB

asic

Fun

dam

enta

lSta

rs(V

erof

f.A

stro

n.R

eche

n-In

stitu

ts,H

eide

lber

g),3

24.

Fric

ke,W

.eta

l.19

91,T

heF

K5

Ext

ensi

on:

New

Fun

dam

enta

lSta

rs(V

erof

f.A

stro

n.R

eche

n-In

stitu

ts,H

eide

lber

g),3

35.

Cor

bin,

T.19

91,U

.S.N

aval

Obs

erva

tory

.IR

Slo

wer

prec

isio

nda

ta6.

Thi

sin

com

plet

eca

talo

gue

was

inco

rpor

ated

into

the

IRS

[5]

7.C

orbi

n,T.

,&

Urb

an,

S.E

.19

91,

U.S

.N

aval

Obs

erva

tory

.T

his

cata

logu

ean

d[8

]w

ere

used

for

the

rere

duct

ion

ofth

eA

stro

grap

hic

Cat

alog

ue[2

],so

they

cont

ain

noA

Cpo

sitio

nsan

dem

phas

ize

the

incl

usio

nof

earl

yep

och

posi

tions

;bot

hhe

mis

pher

esar

eav

erag

edto

geth

erto

form

the

aver

age

erro

rs8.

Cor

bin,

T.,&

Urb

an,S

.E.1

991,

U.S

.Nav

alO

bser

vato

ry.

9.R

oser

,S.

,&

Bas

tian,

U.

1991

,P

PM

Star

Cat

alog

ue,

Vol

s.I

and

II,

(Ast

ron.

Rec

hen-

Inst

ituts

,H

eide

lber

g).

Thi

sca

talo

gue

and

[10]

are

inte

nded

toin

clud

eal

lav

aila

ble

data

and

henc

epr

ovid

eth

em

ost

prec

ise

posi

tions

and

prop

erm

otio

ns;

all

data

are

aver

aged

togi

veth

eav

erag

eer

rors

rath

erth

anhi

gh-

and

low

-pre

cisi

onda

tase

para

tely

,as

for

[7]

and

[8].

10.

Ros

er,S

.,&

Bas

tian,

U.1

993

PP

MSt

arC

atal

ogue

(The

Sout

hern

Hem

isph

ere)

(Ast

ron.

Rec

hen-

Inst

ituts

,Hei

delb

erg)

Sp.-V/AQuan/1999/10/27:16:16 Page 679

680 / 27 INCIDENTAL TABLES11

.de

Veg

t,C

.eta

l.19

92,A

&A

S,97

,985

;Zac

hari

as,N

.199

5,A

J,10

9,18

8012

.Pu

blic

atio

nsof

the

Roy

alO

bser

vato

ry,C

ape

ofG

ood

Hop

e13

.Y

ale

Phot

ogra

phic

Cat

alog

ues.

1926

–83,

Tran

s.A

stro

n.O

bs.Y

ale

Uni

vers

ity,

Vol

s.3–

32;a

ndY

ale

Zon

eC

atal

ogue

s—In

tegr

ated

Ver

sion

14.

Die

ckvo

ss,W

.eta

l.19

75,T

heA

GK

3C

atal

ogue

ofPo

siti

ons

and

Pro

per

Mot

ions

Nor

thof

−2.5

Dec

lina

tion

,Vol

s.1–

8,(H

ambu

rgB

erge

dorf

).15

.B

ucci

arel

li,B

.eta

l.19

92,A

J,10

3,16

89.

AG

K3U

=U

pdat

eto

[14]

usin

ga

rere

duct

ion

of[2

5]fo

rth

ird

epoc

hpo

sitio

ns16

.C

hrut

skay

a,E

.V.1

985,

Sov.

Ast

ron.

J.,6

2,60

5.17

.H

anso

n,R

.B.,

1988

,P

rope

rM

otio

nsan

dG

alac

tic

Ast

rono

my,

edite

dby

Rob

erta

M.

Hum

phre

ys,

ASP

Con

f.Se

ries

127:

Kle

mol

a,A

.R.,

Jone

s,B

.F.,

&H

anso

n,R

.B.1

987,

AJ,

94,5

01.S

eeal

so[3

4],p

.235

;Cam

brid

ge:

Gal

actic

and

Sola

rSy

stem

Opt

ical

Ast

rom

etry

,199

5(h

eld

atR

obin

son

Col

lege

,Cam

brid

geU

nive

rsity

inJu

ne19

93),

edite

dby

L.V

.Mor

riso

nan

dG

.Gilm

ore,

(Klu

wer

Aca

dem

ic,D

ordr

echt

),p.

20;a

nd[3

5],p

.45

18.

Gir

ard,

T.M

.et

al.

1998

,A

J,11

5,85

5;an

d19

97,

BA

AS,

29,

1383

;Pl

atai

s,I.

etal

.19

98,

A&

A,

331,

1119

;va

nA

ltena

,W

.F.

etal

.19

90,

The

Yale

-San

Juan

Sout

hern

Pro

per

Mot

ion

Pro

gram

(SPM

),in

IAU

Sym

posi

um14

1,19

91,

Iner

tial

Coo

rdin

ate

Syst

emon

the

Sky,

edite

dby

J.H

.L

iesk

ean

dV

.K.

Aba

laki

n,(K

luw

erA

cade

mic

,Dor

drec

ht),

p.41

9:va

nA

ltena

,W.F

.eta

l.in

Cam

brid

ge:

Gal

actic

and

Sola

rSy

stem

Opt

ical

Ast

rom

etry

,199

5(h

eld

atR

obin

son

Col

lege

,C

ambr

idge

Uni

vers

ityin

June

1993

),ed

ited

byL

.V.M

orri

son

and

G.G

ilmor

e(K

luw

erA

cade

mic

,Dor

drec

ht),

p.26

19.

Tur

on,C

.eta

l.19

92,a

ndin

[35]

,p.7

7,T

heH

ippa

rcos

Inpu

tCat

alog

ue,E

SASP

-113

6(E

STE

C,N

oord

wijk

)20

.Y

ang,

T.-g

.eta

l.19

92.

FHST

,AN

ewFi

xed

Hea

dSt

arT

rack

erC

atal

ogue

for

the

HST

,in

[34]

,p.2

3521

.Sm

ithso

nian

Inst

itutio

n19

66.

22.

NA

SAG

odda

rdSp

ace

Flig

htC

ente

r,G

reen

belt.

Maj

orre

visi

onan

dex

pans

ion

ofSK

YM

AP

[23]

oper

atio

nsca

talo

gue

for

guid

ance

and

trac

king

NA

SAsp

acec

raft

.A

stro

met

ric

data

deri

ved

from

Hip

parc

osan

dTy

cho

cata

logu

es.

23.

NA

SAG

odda

rdSp

ace

Flig

htC

ente

r,G

reen

belt.

An

oper

atio

nsca

talo

gue

for

guid

ance

and

trac

king

NA

SAsp

acec

raft

24.

Ega

n,M

.P.,

&Pr

ice,

S.D

.,19

96,

AJ,

112,

2862

.A

stro

met

ric

posi

tions

for

infr

ared

obje

cts

have

been

colle

cted

into

aca

talo

gue

desi

gned

toai

din

the

dete

rmin

atio

nof

posi

tions

ofob

ject

sfo

und

inin

frar

edsu

rvey

s;61

,242

ofth

eob

ject

sha

vebe

enid

entifi

edin

infr

ared

cata

logu

es.

25.

Las

ker,

B.M

.eta

l.19

90,A

J,99

,201

9,an

dC

D-R

OM

asG

SC1.

0;an

upda

ted

vers

ion

GSC

1.1

was

issu

edon

CD

-RO

Mon

1A

ugus

t199

2.Po

sitio

nale

rror

isth

eav

erag

elo

calp

reci

sion

26.

Mon

et,D

.G.1

996,

US

Nav

alO

bser

vato

ry,W

ashi

ngto

n,D

C:U

SNO

(10

CD

RO

Ms)

.D

eriv

edfr

omsc

ans

ofth

ein

dica

ted

surv

eys

with

the

USN

O’s

Prec

isio

nM

easu

ring

Mac

hine

(PM

M)

atFl

agst

aff.

Red

uced

into

the

syst

emof

the

HST

GSC

27.

Mon

et,D

.G.,

the

USN

O-A

1.0

cata

logu

ere

duce

din

toth

esy

stem

ofth

eA

CT

28.

Zac

hari

as,

N.e

tal

.199

6,A

J,11

2,23

36.

Obs

erve

dph

otog

raph

ical

lyin

the

blue

and

visu

alba

ndpa

sses

.H

ighe

rac

cura

cyan

ticip

ated

once

the

cata

logu

eha

sbe

enre

redu

ced

into

the

Hip

parc

ossy

stem

.29

.St

one,

R.C

.,19

97,

AJ,

114,

2811

;Si

xtee

nas

trom

etri

cca

libra

tion

equa

tori

alre

gion

sw

ithdi

men

sion

sof

7.6

×3.

2de

gree

ses

tabl

ishe

dw

ithth

eU

SN

aval

Obs

erva

tory

’sFl

agst

aff

Ast

rom

etri

cSc

anni

ngT

rans

itTe

lesc

ope

(FA

STT

)in

the

mag

nitu

dera

nge

9.5

<R

<17

.8.

30.

Min

kow

ski,

R.L

.,&

Abe

ll,G

.O.1

963,

inB

asic

Ast

rono

mic

alD

ata,

edite

dby

K.A

a.St

rand

;V

ol.I

IIof

Star

san

dSt

ella

rSy

stem

s,ed

ited

byG

.Kui

per

and

B.

Mid

dleh

urst

,p.4

8131

.W

hite

oke,

J.19

69,W

hite

oke

Fie

lds

atD

ecli

nati

onZ

ones

−36

and

−42

Deg

rees

(Cal

if.I

nstit

.Tec

h.,P

asad

ena)

32.

Las

ker,

B.M

.,&

Can

non,

R.D

.198

9,in

Dig

itiz

edO

ptic

alSk

ySu

rvey

s,ed

ited

byC

.Jas

chek

,in

Bul

l.d’

Info

.du

CD

S,N

o.37

(Obs

.de

Stra

sbou

rg,S

tras

bour

g),

p.13

;and

Mor

gan,

D.H

.eta

l.19

92,i

nD

igit

ized

Opt

ical

Sky

Surv

eys,

edite

dby

H.T

.Mac

Gill

ivra

yan

dE

.B.T

hom

son

(Klu

wer

Aca

dem

ic,D

ordr

echt

),p.

11.

33.

Har

tley,

M.,

&D

awe,

J.A

.198

1,P

roc.

Ast

ron.

Soc.

Aus

tral

ia,4

,251

.34

.IA

UX

XIB

:Tra

nsac

tion

sof

the

IAU

XX

IB19

91,e

dite

dby

J.B

erge

ron

(Klu

wer

Aca

dem

ic,D

ordr

echt

)35

.IA

U16

6:IA

USy

mpo

sium

166,

Ast

rono

mic

alan

dA

stro

phys

ical

Obj

ecti

ves

ofSu

b-M

illi

arcs

econ

dO

ptic

alA

stro

met

ry,e

dite

dby

E.H

oeg

and

P.K

.Sei

delm

ann

(Klu

wer

Aca

dem

ic,D

ordr

echt

)

Sp.-V/AQuan/1999/10/27:16:16 Page 680

27.7 ASTROMETRY / 681Ta

ble

27.8

.Fut

ure

cata

logu

esan

dsu

rvey

sin

prog

ress

.a

Num

ber

σp

σp

Ref

eren

ceC

atal

ogue

star

sC

over

age

T pub

m(T

pub)

(200

0)σµ

Des

crip

tion

[1]

Tych

o-E

xt.

300

000

0A

llsk

y19

9112

100

······

Ext

ensi

onof

the

Tych

oC

atal

ogue

from

Hip

parc

os[2

]G

AC

400

000

0A

llsk

y19

5412

.520

035

07

[11]

plus

[3]

[3]

IFR

S3

000

All

sky

···13

······

···In

term

edia

teFu

nd.

Star

s(9

.5≤

V≤

13)

(find

ing

list)

[4]

NPM

215

000

0+9

0to

−23

1968

1812

020

05

Abs

olut

epr

oper

mot

ions

with

resp

ectt

oga

laxi

es,

insi

deM

ilky

Way

[5]

SPM

-2.0

250

000

−22

to−4

819

8018

3982

4A

bsol

ute

prop

erm

otio

nsE

xten

sion

ofSP

M1.

0[6

]SP

M-3

.010

7−1

7to

−90

1985

1830

553

Abs

olut

epr

oper

mot

ions

Com

plet

ion

ofSP

M[7

]FO

N36

000

000

+90

to−1

519

90?

1615

0···

···Po

ssib

lyco

mpl

eted

byye

ar20

00[8

]E

KA

T1

000

000

+20

to−2

019

93?

1215

0···

···E

quat

oria

lcat

alog

ue,

obse

rvat

ions

60%

com

plet

ed[9

]A

C2

400

000

0A

llsk

y?

1315

0?

?Fi

rste

poch

is[3

]+

new

epoc

h;pr

ojec

ton

hold

[10]

HST

GSC

II10

9N

orth

1988

20–2

147

823

µfr

om[1

8–22

]So

uth

1973

21–2

247

926

µfr

om[2

3,24

][1

1]U

SNO

-B1.

010

9N

orth

1988

20–2

147

823

µfr

om[1

8-22

]So

uth

1973

21–2

247

926

µfr

om[2

3,24

]U

SN

aval

Obs

erva

tory

PMM

Cat

alog

ue[1

2]U

CA

C-S

40×

106

−2to

−90

1999

16.5

70···

···U

SNO

Sout

hern

CC

Dsu

rvey

[13]

DE

NIS

109

−2to

−88

1998

18.5

1000

······

Nea

r-In

frar

edSk

ySu

rvey

see

refs

.fo

rde

taile

dlim

its[1

4]2M

ASS

??A

llsk

y20

0014

.320

0···

···In

frar

edA

llSk

ySu

rvey

[15]

Sloa

nD

SS10

9N

.Pol

arC

ap20

0222

.550

······

Sloa

nD

igita

lSky

Surv

ey[1

6]Q

uest

-I:

8×

106

1619

9920

100

······

Qua

sar

Equ

ator

ialS

urve

yTe

am[1

7]Q

uest

-II:

108

122

2002

2110

0···

···E

xten

sion

ofQ

uest

-Iw

ithne

wca

mer

a

Not

ea

See

Tabl

e27

.7fo

ra

desc

ript

ion

ofth

eco

lum

nhe

adin

gs.

Sour

ces

for

new

posi

tion

s:Se

eT

rien

nial

Rep

orts

ofIA

UC

omm

issi

ons

8an

d24

,W

orld

Wid

eW

ebsi

tes

and

the

publ

icat

ions

ofth

ere

spec

tive

obse

rvat

orie

s.M

erid

ian

circ

les:

Car

lsbe

rgA

utom

atic

Mer

idia

nC

ircl

e(−

45to

+90,

La

Palm

a,Is

las

Can

aria

s,pu

blis

hed

annu

ally

byC

open

hage

nU

niv.

Obs

.,R

oyal

Gre

enw

ich

Obs

.,an

dR

eal

Inst

.yO

bs.d

ela

Arm

ada,

San

Fern

ando

);U

.S.N

aval

Obs

erva

tory

(all

sky,

Was

hing

ton

and

Bla

ckB

irch

,N

.Z.)

;ad

ditio

nal

nort

hern

mer

idia

nci

rcle

sin

Bel

grad

e,B

orde

aux,

Pulk

ova,

San

Fern

ando

,Sp

ain

(tra

nsfe

rred

toE

lL

eonc

ito,

Arg

entin

ain

1996

),Sh

angh

ai,

Yun

nan

(Chi

na)

and

sout

hern

mer

idia

nci

rcle

sin

San

Juan

(Arg

entin

a)an

dSa

ntia

go(C

hile

).

Sp.-V/AQuan/1999/10/27:16:16 Page 681

682 / 27 INCIDENTAL TABLESA

stro

labe

s:N

orth

ern

astr

olab

esex

isti

nB

eijin

g(c

urre

ntly

inSa

nJu

an,A

rgen

tina)

,Bel

grad

e,B

ucha

rest

,CE

RG

A(F

ranc

e),P

aris

,Pul

kova

,San

Fern

ando

(Spa

in),

Shan

ghai

,Was

hing

ton,

and

Yun

nan

(Chi

na),

whi

leso

uthe

rnas

trol

abes

exis

tin

Rio

Gra

nde

and

San

Juan

(Arg

entin

a),S

antia

go(C

hile

),an

dSa

oPa

ulo

(Bra

zil)

.

Ref

eren

ces

1.H

og,E

.,19

97,E

SASP

-402

,Hip

parc

osVe

nice

’97

(EST

EC

,Noo

rdw

ijk),

p.25

.E

xpec

ted

posi

tiona

lerr

orat

V=

11is

50m

as.

2.U

rban

,S.E

.199

3,in

[25]

,p.1

45.

[26]

seco

ndep

och

posi

tions

with

Ast

rogr

aphi

cC

atal

ogue

first

epoc

hpo

sitio

nsA

C20

00in

[27]

3.C

orbi

n,T.

E.,

&U

rban

,S.E

.199

0,Fa

intR

efer

ence

Star

s,in

[28]

,p.4

33.S

eeal

soR

epor

tof

the

Wor

king

Gro

upon

Star

Lis

ts,i

n[2

9]p.

142.

Not

eth

atth

isis

afin

ding

listf

orob

serv

ers

and

nota

cata

logu

e.IF

RS

=In

term

edia

teFu

ndam

enta

lRef

eren

ceSt

ars

4.H

anso

n,R

.B.,

1997

,in

[30]

,p.2

3.Se

eN

PM1

for

othe

rre

fere

nces

.T

his

isth

eex

tens

ion

ofth

eN

PM1

into

the

gala

ctic

plan

e.5.

See

SPM

-1.0

for

refe

renc

es.

Thi

sis

anex

tens

ion

ofth

eSP

M-1

.0ou

tsid

eth

ega

lact

icpl

ane

for

the

−35

and

−40

degr

eein

addi

tion

tofie

lds

with

seco

nd-e

poch

plat

es.

6.Se

eSP

M-1

.0an

d-2

.0fo

rre

fere

nces

.T

his

isth

epl

anne

dex

tens

ion

toth

eso

uth

cele

stia

lpo

leus

ing

CC

Ds

asde

tect

ors

toob

tain

the

seco

nd-e

poch

expo

sure

s.7.

Kol

chin

sky,

I.G

.,G

arilo

v,I.

V.,

&O

negi

na,A

.B.1

978,

inIA

UC

ollo

q.48

,Mod

ern

Ast

rom

etry

,edi

ted

byF.

V.P

roch

azka

and

R.H

.Tuc

ker

(Uni

v.O

bs.,

Vie

nna)

,p.4

798.

Polo

jent

sev,

D.D

.,Po

tter,

H.I

.,Y

agud

in,

L.I

.,&

Zal

les,

R.F

.199

1,in

Pro

ceed

ings

ofth

eF

irst

Spai

n–U

SSR

Wor

ksho

pon

Posi

tion

alA

stro

nom

yan

dC

eles

tial

Mec

hani

cs,e

dite

dby

A.L

opez

Gar

cia,

R.F

.Lop

ezM

achi

,and

A.G

.Sok

olsk

y(U

niv.

Val

enci

aO

bs.A

stro

n.,V

alen

cia)

,p.6

3.9.

Prop

osed

byH

.I.P

otte

r.T

his

cata

logu

ew

illus

eth

eA

stro

grap

hic

Cat

alog

ueas

the

first

epoc

han

dne

wob

serv

atio

nsw

ithsi

mila

ras

trog

raph

sfo

rth

ese

cond

epoc

h.T

hepr

ojec

thas

been

susp

ende

dfo

rth

etim

ebe

ing

10.

Las

ker,

B.M

.in

1991

,[31

],p.

8711

.M

onet

,D.G

.in

[30]

,see

also

[32,

33]

12.

Gau

ss,F

.G.e

tal.

1996

,BA

AS,

28,1

282;

Obs

erva

tions

for

star

sbr

ight

erth

an14

have

anav

erag

eac

cura

cyof

20m

as.

13.

Epc

htei

n,N

.eta

l.19

97,T

heD

eep

Nea

r-In

frar

edSo

uthe

rnSk

ySu

rvey

(DE

NIS

),T

heE

SOM

esse

nger

,No.

87,2

7;E

pcht

ein,

N.,

1997

,Pro

c.w

orks

hop

on“

The

Impa

ctof

Lar

geSc

ale

Nea

r-IR

Sky

Surv

eys”

,hel

dat

Puer

tode

laC

ruz

(Ten

erif

e),A

pr.6

,Klu

wer

ASS

LSe

r.21

0,p.

15.

Lim

iting

mag

nitu

dein

Ks-

band

(18.

5),

I(1

6.3)

,an

dJ

(14)

.D

etec

tions

ofst

ars

inI,

109,

and

108

inK

s;of

gala

xies

inI,

5×

106,

J,2.

5×

106

and

Ks,

105.

Posi

tiona

lac

cura

cym

aybe

impr

oved

infin

alpr

oces

sing

14.

Two-

Mic

ron

All

Sky

Surv

ey(2

MA

SS).

Lim

iting

mag

nitu

deis

inth

eK

band

15.

Hin

dsle

y,R

.,[3

0],p

.33.

The

limiti

ngm

agni

tude

isin

the

r′ba

nd,a

ndth

esu

rvey

will

cove

rab

out

1st

erad

ian

cent

ered

onth

eN

orth

Gal

actic

Pole

;sp

ectr

aw

illbe

obta

ined

for

abou

t1m

illio

nga

laxi

esan

d50

000

star

s,in

addi

tion

toph

otom

etry

infiv

epa

ssba

nds

for

allo

fth

est

ars.

16.

Snyd

er,

J.et

al.

1998

,in

Pro

ceed

ings

ofSP

IE,

Vol

.33

55(A

stro

nom

ical

Tele

scop

esan

dIn

stru

men

tatio

n,K

ona,

HI,

20–2

8M

arch

1998

),pa

per

36.

Phas

eI

limiti

ngm

ag.i

nV

for

asi

gnal

-to-

nois

eof

10;s

urve

yco

vers

abou

t400

0sq

uare

degr

ees

athi

ghga

lact

icla

titud

esw

ithin

abou

t6de

gree

sof

the

cele

stia

lequ

ator

.17

.Se

ere

fere

nce

for

Que

st-I

.Pha

seII

ispl

anne

dw

ithim

prov

edde

tect

ors

cove

ring

ala

rger

area

.18

.M

inko

wsk

i,R

.L.,

&A

bell,

G.O

.196

3,in

Bas

icA

stro

nom

ical

Dat

a,ed

ited

byK

.Aa.

Stra

nd;V

ol.I

IIof

Star

san

dSt

ella

rSy

stem

s,ed

ited

byG

.Kui

per

and

B.M

iddl

ehur

st,p

.481

.PO

SS=

Palo

mar

Obs

erva

tory

Sky

Surv

ey19

.W

hite

oke,

J.19

69,W

hite

oke

Fie

lds

atD

ecli

nati

onZ

ones

−36

and

−42

Deg

rees

(Cal

if.I

nstit

.Tec

h.,P

asad

ena)

20.

Rei

d,I.

N.1

991,

PASP

,103

,661

21.

Mon

et,D

.G.,

&W

este

rhou

t,G

.198

9,in

Dig

itiz

edO

ptic

alSk

ySu

rvey

s,ed

ited

byC

.Jas

chek

,in

Bul

l.d’

Info

.du

CD

S,N

o.37

,(O

bs.d

eSt

rasb

ourg

,St

rasb

ourg

),p.

75.

The

USN

OQ

Jis

atw

o-m

inut

eex

posu

reon

unhy

pers

ensi

tized

IIIa

-Jem

ulsi

ons

tobe

used

for

the

dete

rmin

atio

nof

posi

tions

ofbr

ight

star

s.

Sp.-V/AQuan/1999/10/27:16:16 Page 682

27.7 ASTROMETRY / 68322

.W

est,

R.M

.,&

Schu

ster

,H.-

E.1

982,

AA

S,49

,577

23.

Las

ker,

B.M

.,&

Can

non,

R.D

.198

9,in

Dig

itiz

edO

ptic

alSk

ySu

rvey

s,ed

ited

byC

.Jas

chek

,in

Bul

l.d’

Info

.du

CD

S,N

o.37

,(O

bs.d

eSt

rasb

ourg

,St

rasb

ourg

),p.

13;a

ndM

orga

n,D

.H.e

tal.

1992

,in

Dig

itiz

edO

ptic

alSk

ySu

rvey

s,ed

ited

byH

.T.M

acG

illiv

ray

and

E.B

.Tho

mso

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Sp.-V/AQuan/1999/10/27:16:16 Page 684

27.7 ASTROMETRY / 685

Table 27.10. Digitization of Schmidt plates (prepared in collaboration with Barry M. Lasker).a

Site Survey Pixel Status Reference Distribution Net access

STScI 2, 5, 12, 13 1.7 Done [1] CD-ROM Yes6–8, 15 1.0 Scanning [1] CD-ROM Yes

ROE 12, 13, 16 1.1 Done [2, 3] CD-ROM Yes1, 6–8, 14, 15 0.5 Scanning [1] CD-ROM Yes

Cam 1, 2, 12, 13 0.5 Done [4] Via collaboration No6–8, 15 0.5 Scanning [4] Via collaboration No

Minn 1, 2, 3 0.5 Done [5, 6] ADS Yes6–8 0.5 Scanning [6] ADS Yes

USNO 1, 2, 11, 12 0.9 Done [7] CD-ROM Yes6–9, 15 0.9 Scanning [7] CD-ROM Yes

NoteaExplanation of the columns: This table summarizes the status of Schmidt plate digitization known to the authors as of

April 1998. The columns list information for each digitization center, giving an acronym for the center (“Site” ); the surveysbeing digitized (the number refers to the survey number given in Table 27.9) the digitization pixel size is in arcseconds; thestatus of the project (either completed or in the process of being scanned); references to the project, listed below; plans fordistribution of the data; and whether or not the data will be available over electronic networks of some kind (“Net access” ).For more details, see [8, 9, 10, 11].

References1. STScI dig.: Lasker, B.M. 1992 in Digitized Optical Sky Surveys, edited by H.T. MacGillivray and E.B. Thomson, (Kluwer

Academic, Dordrecht), p. 87; see also Lasker, B.M. 1993, in Workshop on Databases for Galactic Structure, edited by A.G.Davis, B. Hauck, and A.R. Upgren (L. Davis Press, Schenectady), p. 77; and Sturch, C.R. et al. in Workshop on Databasesfor Galactic Structure, edited by A.G. Davis, B. Hauck, and A.R. Upgren (L. Davis Press, Schenectady), p. 201.

2. ROE dig.: Yentis, D.J. et al. 1992, in Digitized Optical Sky Surveys, edited by H.T. MacGillivray and E.B. Thomson(Kluwer Academic, Dordrecht), p. 67

3. ROE dig.: Working Group on Wide-Field Imaging. 1992, Newsletter 2, p. 104. Cam. dig.: Irwin, M.J., & McMahon, R. 1992, Working Group on Wide-Field Imaging, Newsletter 2, p. 31. Plans to scan

POSS II and AAO SES indicated in private communication.5. Minn APS: Pennington, R.L. et al. 1993, PASP, 105, 521; see also Pennington, R.L. et al. 1992, in Digitized Optical Sky

Surveys, edited by H.T. MacGillivray and E.B. Thomson (Kluwer Academic, Dordrecht), p. 77. Minn.6. Minn APS: Humphreys, R.M. 1993, in Workshop on Databases for Galactic Structure, edited by A.G. Davis, B. Hauck,

and A.R. Upgren (L. Davis Press, Schenectady), p. 87, and Humphreys, R.M. et al. in Workshop on Databases for GalacticStructure, edited by A.G. Davis, B. Hauck, and A.R. Upgren (L. Davis Press, Schenectady), p. 197; see also Odewahn,S.C. et al. 1992, AJ, 103, 318; and Annual Reports for the University of Minnesota 1993, BAAS, 25, 320

7. USN PMM: Monet, D.G., & Westerhout, G. 1989, in Digitized Optical Sky Surveys, edited by C. Jaschek, in Bull. d’ Info.du CDS, No. 37 (Obs. de Strasbourg, Strasbourg), p. 75. The USNO QJ is a two-minute exposure on unhypersensitizedIIIa-J emulsions to be used for the determination of positions of bright stars.

8. Morgan, D.H., & Tritton, S.B. 1988, in Mapping the Sky, IAU Colloq. 133, edited by S. Debarbat, J.A. Eddy, H.K.Eichhorn, and A.R. Upgren (Kluwer Academic, Dordrecht), p. 349

9. Digitized Optical Sky Surveys Newsletter and IAU Working Group on Wide-Field Imaging Newsletters, both edited by H.T.MacGillivray (ROE)

10. Lasker, B.M. 1995, PASP, 107, 763; and 1995, in Future Utilization of Schmidt Telescopes, edited by R.D. Cannon et al.(ASP, San Francisco)

11. Workshop on Databases for Galactic Structure, 1993, edited by A.G. Davis, B. Hauck, and A.R. Upgren (L. Davis Press,Schenectady), pp. 215 and 250

Table 27.11. Modern relative proper motion surveys.

Reference Catalogue No. stars Coverage Tpub m µ limit Description

[1] BPM 94 263 South + 1963 15 0.10 Bruce Proper Motion Survey,1928–63

[2] Lowell 8 991 North 1971 16 0.26 Lowell Proper Motion Survey,1958–70

[3] Lowell 2 758 South 1978 16 0.20 Lowell Southern section, 1959–78

Sp.-V/AQuan/1999/10/27:16:16 Page 685

686 / 27 INCIDENTAL TABLES

Table 27.11. (Continued.)

Reference Catalogue No. stars Coverage Tpub m µ limit Description

[4] LP 450 000 North − 1979 21 0.08 Luyten Palomar 48-Inch SchmidtSurvey, 1963–77

[5] Calan 830 South 1998 21 0.15 Selected regions, Maksutov atCerro El Roble, Chile

References1. Luyten, W.J. 1963, University of Minnesota, Minneapolis. Mostly Southern hemisphere, but includes some in the

north2. Giclas, H.L., Burnham Jr., R., & Thomas, N.G. 1971, Lowell Proper Motion Survey, Northern Hemisphere

Catalogue, Lowell Obs., Flagstaff3. Giclas, H.L., Burnham Jr., R., & Thomas, N.G. 1978, Lowell Obs. Bull. No. 164, Vol. VIII, p. 894. Luyten, W.J. 1963–87, Proper Motion Survey with the Forty-Eight inch Schmidt Telescope, University of

Minnesota, Minneapolis; and 1987, My First 72 Years of Astronomical Research, Minneapolis, pp. 26–28. ProperMotion Survey. Mostly Northern Hemisphere, but includes some in the south

5. Wroblewski, H., & Torres, C. 1997, A&AS, 122, 447; 1998, A&AS, 128, 457

Table 27.12. Relative proper motion summary catalogues.

Reference Catalogue No. stars Coverage Tpub m µ limit Description

[1] NLTT 58 855 All sky 1979 All 0.18 Stars with µ ≥ 0.18 arcsec/yr[2] LHS Cat. 4 447 All sky 1979 All 0.50 Stars with µ ≥ 0.50 arcsec/yr,

2nd ed.[3] LHS Atlas 3 040 All sky 1979 All 0.50 Stars with µ ≥ 0.50 arcsec/yr,

Finding Charts for LHS Catalogue

References1. Luyten, W.J. 1979, 80, New Luyten Catalogue of Stars with Proper Motions Larger than Two Tenths of an Arcsecond

(University of Minnesota, Minneapolis)2. Luyten, W.J. 1979, Luyten Half-Second Catalogue (University of Minnesota, Minneapolis)3. Luyten, W.J., & Albers, H. 1979, Luyten Half-Second Atlas (University of Minnesota, Minneapolis). Finding charts

for stars without published charts

Table 27.13. Stellar compilation catalogues.

Reference Catalogue No. stars Coverage Tpub m Limits Description

[1] BSC Va 9 110 All sky 1998 6.5 V ≤ 6.5 The Bright Star Catalogue, 5th ed.;Stars with V ≤ 6.5

[2] BSC Supp. 2 603 All sky 1983 7.1 V ≤ 7.1 The BSC Supplement; Stars withV ≤ 7.1 photoelectric

[3] CNS 3 3 803 All sky 1996 All π ≥ 0.040 Catalogue of Nearby Stars, 3rdprelim. ed.; stars with π ≥ 0.040

[4] CNSG 2 542 All sky 1997 All π ≥ 0.040 Catalogue of Nearby Stars,Ground-based parallaxes

[5] CNSH 2 678 All sky 1997 9 π ≥ 0.040 Catalogue of Nearby Stars,Hipparcos-based parallaxes

[6] YPC 8 112 All sky 1995 All · · · Gen. Cat. Trig. Parallaxes; all starswith measured π

[7] WDS 78 100 All sky 1984/96 All · · · Washington Double StarCatalogue; all measures

[8] CHARA 7 598 All sky 1998 10 · · · Interferometric measures of doublestars; 3rd catalogue

[9] Orbits 847 All Sky 1984 All · · · Visual Double Star Orbit Catalogue

Sp.-V/AQuan/1999/10/27:16:16 Page 686

27.8 OPTICAL AND INFRARED INTERFEROMETRY / 687

NoteaAn electronic version of the Bright Star Catalogue, often referred to as the BSC V, has circulated, but the final BSC V will

not be released until late 1998 or 1999.

References1. Hoffleit, E.D., & Warren Jr., W.H. 1998, The Bright Star Catalogue, 5th rev. ed. (NASA Astronomical Data Center,

Greenbelt); see also Hoffleit, E.D. (with the collaboration of Jaschek, C.) 1982, The Bright Star Catalogue, 4th rev. ed.(Yale Univ. Obs., New Haven), and [10]

2. Hoffleit, E.D., Saladyga, M., & Wlasuk, P. 1983, A Supplement to the Bright Star Catalogue (Yale Univ. Obs., New Haven),and [10]

3. Jahreiß, H., & Gliese, W. 1996, The Catalogue of Nearby Stars, 3rd ed. (Veroff. Astron. Rechen-Instituts, Heidelberg); seealso [10] for the 1991 Preliminary Edition

4. Jahreiß, H., & Wielen, R. 1997, Hipparcos-Venice ’97, ESA SP-402 (ESTEC, Noordwijk), p. 675. This version of the CNSis derived from ground-based parallaxes and is probably more complete.

5. Jahreiß, H., & Wielen, R. 1997, Hipparcos-Venice ’97, ESA SP-402 (ESTEC, Noordwijk), p. 675. This version of theCNS is derived from Hipparcos-based parallaxes and is biased by the bright limiting magnitude of Hipparcos, but it is moreaccurate in identifying which stars are included within the 25 pc limit.

6. van Altena, W.F., Lee, J.T., & Hoffleit, E.D. 1995, General Catalogue of Trigonometric Parallaxes, 4th ed. (Yale Univ. Obs.,New Haven); see also [10] for the 1991 Preliminary Edition, and van Altena et al. for a discussion of the system of the YPCin [11], p. 65 and [12], p. 50.

7. Worley, C.E., & Douglass, G.G. 1984, Washington Catalog of Visual Double Stars (U.S. Naval Obs., Washington, DC); seeWeb site for up-to-date version.

8. McAlister, H.A., Hartkopf, W.I., & Mason, B. 1997, Third Catalog of Interferometric Measurements of Binary Stars; seeWeb site for up-to-date version.

9. Worley, C.E., & Heintz, W.D. 1984, Fourth Catalog of Orbits of Visual Binary Stars, Publ. U.S. Naval Obs. (2) 24, Part VII;see Web site.

10. Brotzman, L.E. et al. 1991, Astronomical Data Center CD-ROM Selected Astronomical Catalogs, Vol. I, (NASA GoddardSpace Flight Center, Greenbelt). See also subsequent volumes in this series.

11. Swarthmore: Workshop on Databases for Galactic Structure, edited by A.G. Davis, B. Hauck, and A.R. Upgren (L. DavisPress, Schenectady), p. 1993

12. Cambridge: Galactic and Solar System Optical Astrometry (held at Robinson College, Cambridge University in June 1993);1995, edited by L.V. Morrison and G. Gilmore (Kluwer Academic, Dordrecht)

27.8 OPTICAL AND INFRARED INTERFEROMETRYby S.T. Ridgway

Optical interferometry is qualitatively similar to radio interferometry, though differing in manyquantitative details related to atmospheric turbulence and detection. Optical interferometry has nowreached a state of development similar to radio interferometry of about 30 years ago.

Independent telescopes functioning as an interferometer, with a telescope separation of B,operating at wavelength λ, will enable angular resolution up to spatial frequency B/λ and the capabilityof resolving structures with angular extent of order λ/B. This will allow model-dependent sizemeasures of sources smaller than λ/B by a factor approximately equal to the signal-to-noise ratio.

Interferometers measure the mutual coherence of light from the source by detecting the interferencefringes formed in the combined light beams from two or more apertures. Pairs of telescopes can beemployed, as in the classical Michelson experiment, to determine the modulus of the fringe visibility.Three or more telescopes can additionally measure (in part) the complex visibility and subject to certainapproximations, images can be obtained by numerical manipulation of the mutual coherence data,using most of the techniques developed for image restoration at radio wavelengths [17].

The implementation of interferometry is constrained by the requirement to detect the fringes ina time short enough to “ freeze” the fringes in the presence of optical path drifts. In practice, thesensitivity of an interferometer will be limited by the number of source photons in the coherencevolume, �2cT δλ, depending on the maximum collecting aperture � and time T over which photons inbandwidth δλ may be combined coherently for a measurement [18].

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688 / 27 INCIDENTAL TABLES

Figure 27.1. The effective magnitude per resolution element versus log θ diagram shows how the surfacebrightness and size are related through the radiometric temperature for various sources [22]

The atmosphere limits � to approximately r0, the Fried length, which is

r0 ≈ 0.1

(λ

0.5 µm

)1.2

m. (1)

The atmosphere limits T to times of order r0/v, where v is a weighted mean wind speed in theturbulent atmosphere. Values of a few milliseconds are common in the visible range. Furthermore,δλ is constrained by the residual optical path differences to the source and the source and observinggeometry.

There does not appear to be any fundamental limit to the use of optical interferometry from theground, though the practical difficulties are severe. Interferometry with r0 size apertures can be carriedout on bright sources (M ≈ 10). In order to reach faint limits several techniques are available. � can beincreased to the aperture size of the available telescope by use of adaptive optics (phasing a telescope).T can be increased by actively stabilizing the optical path differences (cophasing telescopes). Throughcoherencing [19] and/or absolute metrology [20] it should be possible to maintain a condition ofapproximate cophasing for any point on the sky. With laser reference beacons, it may be possibleto achieve adaptive phasing and cophasing with faint reference sources. The practical performancelimits for optical interferometry from the ground are still a matter of some speculation, as these areintimately tied to the effective implementation of adaptive telescopes with large aperture telescopes,and this effort is itself in an early stage of development. However, extension of interferometry toimaging of complex sources and sources much fainter than M = 18 may be exceedingly difficult.

In space, the problems of phasing and cophasing should be ameliorated. Instrument changes dueto thermal or tidal effects should be relatively benign and can be monitored with internal metrology.The wavefront quality and optical path difference to the source can be monitored with bright reference

Sp.-V/AQuan/1999/10/27:16:16 Page 688

27.9 THE WORLD’ S LARGEST OPTICAL TELESCOPES / 689

Figure 27.2. Overview of science topics for optical interferometry showing the typical apparent sizes of varioustypes of sources. The angular resolution at 1 µm wavelength, for several telescope separations, is shown on theright-hand side of the figure (for a different wavelength, shift the baseline scale as shown).

stars at large angle from the source of interest. Potentially, T can be greatly increased. However,this gain must be traded against the loss in collecting aperture compared to possible ground-basedinterferometers [21].

The amount of image information collected in an interferometer is related to the number ofindependent baselines in the array, which can be as large as N (N − 1)/2 for N telescopes, providingmost radio interferometers a quadratic improvement with number of telescopes. However, in theabsence of noiseless optical amplifiers, optical interferometry imposes a signal-to-noise penalty forthe combination of multiple beams. For more than about N = 5, the gain in observing efficiency willbe approximately linear with N .

The most important parameters in an interferometric measurement are the source brightness perspatial resolution element, and the required telescope separation. Figures 27.1 and 27.2 show aschematic representation of this information.

Ground-based interferometry has been used to achieve wide-angle astrometry with errors of a fewmilliarcseconds, and may be extended to achieve errors as small as tens of microarcseconds for very-narrow-angle astrometry [24]. Interferometry from space is expected to achieve absolute astrometricprecision of a few microarcseconds [25] for wide- and narrow-angle measurements. This advantage ofspace over ground appears to be fundamental. See also [26] and [27].

27.9 THE WORLD’S LARGEST OPTICAL TELESCOPESby Roger W. Sinnott and Kari Parker

Table 27.14 lists the largest telescopes designed to observe the sky at visible and infrared wavelengths.The instruments are grouped into three main categories and arranged in descending order of aperture.Included are the biggest reflecting telescopes, Schmidt cameras, and refracting telescopes currently in

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690 / 27 INCIDENTAL TABLES

use or in an advanced stage of construction or planning. Important note: Many additional reflectorsare in use with apertures between 1.3 and 2.3 m; they have been omitted from the table, even thoughthey exceed the existing Schmidt and refracting telescopes in light-gathering power.

Large reflectors stand at the forefront of astronomical research today. They collect starlight usingeither a single concave monolithic mirror, a segmented-mirror mosaic, or several separate mirrorsarranged to send their beams to a combined focus. Generally their angular coverage is small (only a fewarcminutes), but such a field is well suited to the needs of spectroscopy and the small physical size ofmodern electronic detectors, such as the charge-coupled devices (CCDs) that have largely supersededphotographic plates on this class of instrument.

Schmidt telescopes are photographic cameras providing exquisite star images on a curved focalsurface centered within the tube. Because light first enters through a corrector lens, the diameter of thislens determines the overall light grasp. The primary mirror is always made substantially larger thanthe corrector so the instrument can photograph an unvignetted field spanning 5◦ or more.

Refractors have a two-element objective lens instead of a primary mirror to collect light. Thedifficulty of manufacturing glass with the necessary purity and homogeneity in large sizes has seta natural limit to refractor size—a limit that, in fact, was attained around the turn of the twentiethcentury. Yet many of these venerable instruments remain in service; they have been of particular valuein high-accuracy astrometry.

The first column of Table 27.14 gives the official telescope name, the observatory to which itbelongs, and the geographical site, along with the instrument’s common name (if any). Sometimes thecommon name quotes a mirror size that differs slightly from the clear aperture.

The second column lists the clear aperture in meters, the optical design, and the main person(s)or firm(s) involved in making the optics, along with the available focal ratios (that is, effective focallength divided by aperture). In the case of reflectors, the smallest focal ratio usually refers to theprimary mirror itself; some of the instruments have wide-field correctors for prime-focus work, andthese correctors may alter the focal ratio slightly. Additional focal ratios refer to Cassegrain, Nasmyth,or coude foci, where IR means a focus used for infrared observations.

Next comes the style of the telescope’s mounting and the firm(s) associated with its manufacture.Here, as in the second column, no attempt has been made to recognize the full hierarchy of contractorsby which these complex instruments have come into being. Among the abbreviations used, LOMOrefers to Leningrad Optical Equipment Works, Russia; SNACRP is the Societe Nouvelle des Atelierset Chantiers de La Rochelle-la-Pallice, France; REOSC is Recherches et Etudes d’Optique et desSciences Connexes, France; KPNO is Kitt Peak National Observatory, Arizona, US; NOAO is theNational Optical Astronomy Observatories, Arizona, US.

The listed latitude and longitude refer to the telescope, as opposed to the observatory headquarters.These values have been rounded off to the nearest arcminute in all cases, and elevations above sea levelare expressed in meters. In a few cases accurate values were not available; a colon (:) signifies that thevalue is uncertain.

The year refers either to an official commissioning ceremony, “fi rst light” through the instrument,or the start of regular observations. For telescopes still under construction at the time this table wascompiled (mid-1998), the projected year of completion is given in parentheses. For such telescopes,not only the year but also the instrument’s specifications may change as the project unfolds.

The final column gives additional comments, such as the glass type used for the primary mirror andother notes about the instrument.

We are grateful to the staffs at dozens of observatories for returning the questionnaires we sentout in mid-1992. These responses were our primary source of information. Also very helpful was anearlier compilation [28]. Whenever possible, telescope coordinates have been taken from the extensivelistings in the Astronomical Almanac [3] for 1981–84 (US Naval Observatory and Royal GreenwichObservatory). Telephone calls, electronic mail, and published articles have filled in additional details,especially for instruments still under construction.

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27.9 THE WORLD’ S LARGEST OPTICAL TELESCOPES / 691Ta

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Sp.-V/AQuan/1999/10/27:16:16 Page 691

692 / 27 INCIDENTAL TABLESTa

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27.9 THE WORLD’ S LARGEST OPTICAL TELESCOPES / 693Ta

ble

27.1

4.(C

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equa

tori

alH

adfie

lds

Ltd

.(Sh

effie

ld)

19◦ 5

0′N

155◦

28′ W

4194

m

1978

Cer

-Vit

prim

ary

mir

ror;

used

for

infr

ared

wor

kon

ly

Can

ada–

Fran

ce–H

awai

iTel

esco

peC

anad

a–Fr

ance

–Haw

aiiT

eles

cope

Cor

p.M

auna

Kea

,Haw

aii,

US

(CFH

T)

3.58

-mm

irro

r··· D

omin

ion

Ast

roph

ys.

Obs

.f/

3.8,

8,20

,35

Hor

sesh

oe-y

oke

equa

tori

alSN

AC

RP

19◦ 4

9′N

155◦

28′ W

4200

m

1979

Cer

-Vit

prim

ary

mir

ror

Tele

scop

ioN

azio

nale

Gal

ileo

Obs

.del

Roq

uede

los

Muc

hach

osL

aPa

lma,

Can

ary

Isla

nds

(Gal

ileo)

3.58

-mm

irro

rR

itche

y–C

hret

ien

Zei

ssf/

2.5,

6,11

Alta

zim

uth

28◦ 4

5′N

17◦ 5

4′W

2370

m

(199

8)Z

erod

urm

irro

r

ESO

3.6-

met

erTe

lesc

ope

Eur

opea

nSo

uthe

rnO

bser

vato

ryL

aSi

lla,C

hile

(ESO

3.6

m)

3.57

-mm

irro

r··· R

EO

SCf/

3.0,

8.1,

32

Hor

sesh

oe-f

ork

equa

tori

alC

reus

ot-L

oire

29◦ 1

6′S

70◦ 4

4′W

2387

m

1977

Fuse

d-si

lica

prim

ary

mir

ror

New

Tech

nolo

gyTe

lesc

ope

Eur

opea

nSo

uthe

rnO

bser

vato

ryL

aSi

lla,C

hile

(NT

T)

3.50

-mm

irro

rR

itche

y–C

hret

ien

Zei

ssf/

2.2,

11

Alta

zim

uth

29◦ 1

6′S

70◦ 4

4′W

2353

m

1989

Thi

nZ

erod

urpr

imar

ym

irro

r;fig

ure

cont

rolle

dby

78ac

tive

supp

orts

3.5-

met

erTe

lesc

ope

Cal

arA

ltoO

bser

vato

ryC

alar

Alto

,Spa

in···

3.50

-mm

irro

rR

itche

y–C

hret

ien

Zei

ss(O

ber.)

f/3.

5,3.

9,10

,35

Hor

sesh

oeyo

keV

oith

,Hei

denh

eim

;Z

eiss

(Obe

r.)

37◦ 1

3′N

2◦32

′ W21

68m

1984

Ope

rate

dby

Ger

man

–Spa

nish

Ast

rono

mic

alC

ente

r;Z

erod

urpr

imar

ym

irro

r

Ast

roph

ysic

alR

esea

rch

Con

sort

ium

Tele

scop

eA

pach

ePo

int,

New

Mex

ico,

US

(AR

C3.

5m

)

3.5-

mm

irro

r··· R

.Ang

el,B

.Mar

tinf/

1.75

Alta

zim

uth

32◦ 4

7′:

N10

5◦49

′ :W

2800

m

1994

Spin

-cas

tbo

rosi

licat

eho

ney-

com

bpr

imar

ym

irro

r(O

hara

E6)

Sp.-V/AQuan/1999/10/27:16:16 Page 693

694 / 27 INCIDENTAL TABLESTa

ble

27.1

4.(C

onti

nued

.)

Tele

scop

eO

bser

vato

ryPl

ace

(Com

mon

Nam

e)

Cle

arap

ertu

reO

ptic

alde

sign

Mak

erFo

calr

atio

sM

ount

ing

Man

ufac

ture

r

Lat

itude

Lon

gitu

deE

leva

tion

Yea

rN

otes

Wis

cons

in–I

ndia

na–Y

ale–

NO

AO

Tel.

WIY

NO

bser

vato

ryK

ittPe

ak,A

rizo

na,U

S(W

IYN

3.5

m)

3.5-

mm

irro

r··· C

harl

esH

arm

er/N

OA

O(f

/1.7

5)f/

6.3

Alta

zim

uth

L&

FIn

dust

ries

31◦ 5

7′N

111◦

36′ W

2089

m

1994

Spin

-cas

tbor

osili

cate

prim

ary

mir

ror

bySt

ewar

dO

bser

vato

ryM

irro

rL

ab(R

.A

ngel

)

C.D

onal

dSh

ane

Tele

scop

eL

ick

Obs

erva

tory

Mou

ntH

amilt

on,C

alif

.,U

S(1

20in

ch)

3.05

-mm

irro

rC

asse

grai

nD

onO

.Hen

drix

f/5,

17,3

6

Equ

ator

ial

fork

Juds

onPa

cific

–Mur

phy

Cor

p.37

◦ 21′

N12

1◦38

′ W12

90m

1959

Pyre

xpr

imar

ym

irro

r

NA

SAIn

frar

edTe

lesc

ope

Faci

lity

Mau

naK

eaO

bser

vato

ryM

auna

Kea

,Haw

aii,

US

(NA

SAIR

TF)

3.00

-mm

irro

rC

asse

grai

nK

PNO

Opt

ical

Shop

f/2.

5,35

,120

IR

Eng

lish

yoke

equa

tori

alde

Bar

tolo

mei

s19

◦ 50′

N15

5◦28

′ W42

08m

1979

Infr

ared

tele

scop

e;C

er-V

itpr

imar

ym

irro

r

Har

lan

J.Sm

ithTe

lesc

ope

McD

onal

dO

bser

vato

ryM

ount

Loc

ke,T

exas

,US

(107

inch

)

2.72

-mm

irro

rR

itche

y–C

hret

ien

Dav

idso

nO

ptro

nics

f/3.

9,8.

8,18

Cro

ss-a

xis

equa

tori

alW

estin

ghou

se30

◦ 40′

N10

4◦01

′ W20

75m

1969

Fuse

d-si

lica

prim

ary

mir

ror

UB

C–L

aval

Tele

scop

eU

niv.

ofB

.C.a

ndL

aval

Uni

v.V

anco

uver

,BC

,Can

ada

(LM

T)

2.7-

mm

irro

r(l

iqui

d)Pa

rabo

loid

,fiel

dco

rr.

P.H

icks

onf/

1.88

7

Fixe

dve

rtic

alm

ount

Uni

v.of

Bri

tish

Col

.49

◦ 07′

N12

2◦35

′ :W

50m

1992

Mer

cury

prim

ary

mir

ror

(rot

atin

g);v

iew

sa

21′ fi

eld

atlo

cal

zeni

th(c

ente

red

onde

clin

atio

n+4

9◦1)

Shaj

n2.

6-m

Refl

ecto

rC

rim

ean

Ast

roph

ysic

alO

bs.

Nau

chny

,Ukr

aine

(Cri

mea

n10

2in

ch)

2.64

-mm

irro

r··· ··· f/

3.8,

15.7

,16.

4,40

Fork

equa

tori

al44

◦ 44′

N34

◦ 00′

E···

1960

···

Byu

raka

n2.

6-m

eter

Refl

ecto

rB

yura

kan

Obs

erva

tory

Mou

ntA

raga

tz,A

rmen

ia(B

yura

kan

102

inch

)

2.64

-mm

irro

r··· ··· f/

3.6,

16,4

0

Fork

equa

tori

alL

OM

O40

◦ 20′

N44

◦ 18′

E15

00m

1976

···

Nor

dic

Opt

ical

Tele

scop

eO

bs.d

elR

oque

delo

sM

ucha

chos

La

Palm

a,C

anar

yIs

land

s(N

OT

)

2.56

-mm

irro

rC

asse

grai

nO

ptic

sL

abs

(Tar

tu)

(f/2

.0),

11.0

Alta

zim

uth

mou

ntin

rota

ting

build

ing

28◦ 4

5′N

17◦ 5

3′W

2382

m

1989

Zer

odur

prim

ary

mir

ror

Sp.-V/AQuan/1999/10/27:16:16 Page 694

27.9 THE WORLD’ S LARGEST OPTICAL TELESCOPES / 695Ta

ble

27.1

4.(C

onti

nued

.)

Tele

scop

eO

bser

vato

ryPl

ace

(Com

mon

Nam

e)

Cle

arap

ertu

reO

ptic

alde

sign

Mak

erFo

calr

atio

sM

ount

ing

Man

ufac

ture

r

Lat

itude

Lon

gitu

deE

leva

tion

Yea

rN

otes

Iren

eedu

Pont

Tele

scop

eL

asC

ampa

nas

Obs

erva

tory

Las

Cam

pana

s,C

hile

(du

Pont

100

inch

)

2.54

-mm

irro

rR

itche

y–C

hret

ien

Don

ald

A.L

oom

isf/

3.0

Fork

equa

tori

alB

ruce

H.R

ule

29◦ 0

0′S

70◦ 4

2′W

2282

m

1976

Ow

ned

byC

arne

gie

Inst

.of

Was

hing

ton;

fuse

d-si

lica

prim

ary

mir

ror

Hoo

ker

Tele

scop

eM

ount

Wils

onO

bser

vato

ryM

ount

Wils

on,C

alif

.,U

S(1

00in

ch)

2.5-

mm

irro

rC

asse

grai

nG

.W.R

itche

yf/

5,16

,30

Eng

lish

mou

ntF.

G.P

ease

and

Fore

Riv

erSh

ipya

rds

34◦ 1

3′N

118◦

03′ W

1742

m

1917

Plat

e-gl

ass

prim

ary

mir

ror

from

Sain

t-G

obai

n(P

aris

);te

lesc

ope

out

ofse

rvic

e19

85–9

2

Isaa

cN

ewto

nTe

lesc

ope

Obs

.del

Roq

uede

los

Muc

hach

osL

aPa

lma,

Can

ary

Isla

nds

(Isa

acN

ewto

n98

inch

)

2.5-

mm

irro

r··· G

rubb

–Par

sons

f/3,

15

Pola

r-di

skeq

uato

rial

Gru

bb–P

arso

ns28

◦ 46′

N17

◦ 53′

W23

36m

1984

Ope

rate

dby

Roy

alG

reen

wic

hO

bser

vato

ry;o

rigi

nally

setu

pin

Eng

land

in19

67

Sloa

nD

igita

lSky

Surv

eyTe

l.A

stro

phys

.Res

.Con

sort

ium

Obs

.A

pach

ePo

int,

New

Mex

ico,

US

(Slo

an2.

5m

)

2.5-

mm

irro

rR

itche

y–C

hret

ien

Alta

zim

uth

L&

FIn

dust

ries

and

Uni

vers

ityof

Was

hing

ton

32◦ 4

7′N

105◦

49′ W

2800

m

(199

8)To

take

CC

Dim

ager

yof

aqu

arte

rof

sky

in5

colo

rs(u

,g,r

,i,z

)an

dm

easu

rere

dshi

fts

of1

mill

ion

gala

xies

Hub

ble

Spac

eTe

lesc

ope

Spac

eTe

lesc

ope

Scie

nce

Inst

.B

altim

ore,

Mar

ylan

d,U

S(H

ST)

2.4-

mm

irro

rR

itche

y–C

hret

ien

Perk

inE

lmer

f/12

.9,3

0,48

,96

3-ax

is-s

tabi

lized

spac

ecra

ftL

ockh

eed

(Ear

thor

bit)

1990

Prim

ary

isof

Cor

ning

UL

Egl

ass

Hilt

ner

Tele

scop

eM

ichi

gan–

Dar

tmou

th–M

ITO

bs.

Kitt

Peak

,Ari

zona

,US

(Hilt

ner

2.3

m)

2.34

-mm

irro

rR

itche

y–C

hret

ien

Con

trav

es(U

SA)

f/2.

07,1

3.5

Equ

ator

ialf

ork,

fric

tion-

disk

driv

esD

FME

ngin

eeri

ng,

L&

FIn

dust

ries

31◦ 5

7′N

111◦

37′ W

1938

m

1986

Mir

rors

repo

lishe

d19

91;C

er-V

itpr

imar

ym

irro

r

2.3-

met

erTe

lesc

ope

Vai

nuB

appu

Obs

erva

tory

Kav

alur

,Tam

ilN

adu,

Indi

a(V

ainu

Bap

pu2.

3m

)

2.33

-mm

irro

r··· In

dian

Inst

.A

stro

phys

.f/

3.25

,13,

43

Hor

sesh

oeeq

uato

rial

Wal

chan

dnag

arIn

dust

ries

12◦ 3

5′N

78◦ 5

0′E

725

m

1985

Zer

odur

prim

ary

mir

ror

Mou

ntSt

rom

lo2.

3-m

eter

Mt.

Stro

mlo

and

Sidi

ngSp

ring

Obs

.Si

ding

Spri

ngM

tn.,

Aus

tral

ia···

2.3-

mm

irro

r··· N

orm

anC

ole

f/2.

09,1

8

Alta

zim

uth

Aus

tral

ian

Nat

iona

lUni

v.,

New

cast

leD

ocky

ard

31◦ 1

6′S

149◦

03′ E

1149

m

1984

Cer

-Vit

prim

ary

mir

ror

Sp.-V/AQuan/1999/10/27:16:16 Page 695

696 / 27 INCIDENTAL TABLESTa

ble

27.1

4.(C

onti

nued

.)

Tele

scop

eO

bser

vato

ryPl

ace

(Com

mon

Nam

e)

Cle

arap

ertu

reO

ptic

alde

sign

Mak

erFo

calr

atio

sM

ount

ing

Man

ufac

ture

r

Lat

itude

Lon

gitu

deE

leva

tion

Yea

rN

otes

SCH

MID

TT

EL

ESC

OP

ES

2-m

eter

Tele

scop

eK

arlS

chw

arzs

child

Obs

erva

tori

umTa

uten

berg

,Ger

man

y(T

aute

nber

gSc

hmid

t)

1.34

-mco

rrec

tor

Schm

idt

Zei

ss(J

ena)

f/3.

00

Equ

ator

ialf

ork

Zei

ss(J

ena)

50◦ 5

9′N

11◦ 4

3′E

331

m

1960

2-m

prim

ary

mir

ror

ofSc

hott

ZK

-7gl

ass;

can

also

beus

edin

Cas

segr

ain

and

coud

em

odes

Osc

hin

48-i

nch

Tele

scop

ePa

lom

arO

bser

vato

ryPa

lom

arM

ount

ain,

Cal

if.,

US

(Osc

hin

Schm

idt)

1.24

-mco

rrec

tor

Schm

idt

Don

O.H

endr

ixf/

2.47

Equ

ator

ial

fork

mad

eat

Cal

ifor

nia

Inst

itute

ofTe

chno

logy

33◦ 2

1′N

116◦

51′ W

1706

m

1948

1.83

-mpr

imar

ym

irro

r;a

new

achr

omat

icco

rrec

tor

plat

e(G

rubb

–Par

sons

)w

asin

stal

led

inab

out1

984

Uni

ted

Kin

gdom

Schm

idtT

el.U

nit

Roy

alO

bser

vato

ry,E

dinb

urgh

Sidi

ngSp

ring

Mtn

.,A

ustr

alia

(U.K

.Sch

mid

t)

1.24

-mco

rrec

tor

Schm

idt

Gru

bb–P

arso

nsf/

2.5

··· Gru

bb–P

arso

ns31

◦ 16′

S14

9◦04

′ E11

45m

1973

Cer

-Vit

1.83

-mpr

imar

ym

irro

r

Kis

oSc

hmid

tTel

esco

peK

iso

Obs

erva

tory

Kis

o,Ja

pan

···

1.05

-mco

rrec

tor

Schm

idt

Nik

onf/

3.1

Equ

ator

ialf

ork

Nik

on35

◦ 48′

N13

7◦38

′ E11

30m

1975

Ope

rate

dby

Uni

v.of

Toky

o;C

er-V

it1.

5-m

prim

ary

mir

ror;

alte

rnat

ese

cond

ary

mir

ror

offe

rsan

f/22

.6C

ass.

focu

s

3TA

-10

Schm

idtT

eles

cope

Byu

raka

nA

stro

phys

ical

Obs

erva

tory

Mou

ntA

raga

tz,A

rmen

ia(B

yura

kan

Schm

idt)

1.00

-mco

rrec

tor

Schm

idt

LO

MO

f/2.

13

··· LO

MO

40◦ 2

0′N

44◦ 3

0′E

1450

m

1961

1.5-

mpr

imar

ym

irro

r;th

iste

lesc

ope

has

thre

e1-

mob

ject

ive

pris

ms

Kvi

stab

erg

Schm

idtT

eles

cope

Upp

sala

Uni

vers

ityO

bser

vato

ryK

vist

aber

g,Sw

eden

(Upp

sala

Schm

idt)

1.00

-mco

rrec

tor

Schm

idt

Upp

sala

Uni

v.O

bs.

f/3.

00

··· Var

ious

Swed

ish

fact

orie

s59

◦ 30′

N17

◦ 36′

E33

m

1963

1.35

-mpr

imar

ym

irro

r

ESO

1-m

eter

Schm

idtT

eles

cope

Eur

opea

nSo

uthe

rnO

bser

vato

ryL

aSi

lla,C

hile

(ESO

Schm

idt)

1.00

-mco

rrec

tor

Schm

idt

Zei

ss(O

ber.)

f/3.

06

··· Hei

denr

eich

&H

arbe

ck29

◦ 15′

S70

◦ 44′

W23

18m

1972

1.6-

mpr

imar

ym

irro

rof

Scho

ttD

uran

50

Ven

ezue

la1-

met

erSc

hmid

tC

entr

o“F

.J.D

uart

e”L

lano

delH

ato,

Mer

ida,

Ven

ezue

la···

1.00

-mco

rrec

tor

Con

cent

ric

Schm

idt

Ask

ania

f/3.

0

Ben

t-yo

keeq

uato

rial

Ask

ania

8◦47

′ N70

◦ 52′

W36

10m

1978

1.52

-mpr

imar

ym

irro

r;ha

sa

1-m

obje

ctiv

epr

ism

Sp.-V/AQuan/1999/10/27:16:16 Page 696

27.9 THE WORLD’ S LARGEST OPTICAL TELESCOPES / 697Ta

ble

27.1

4.(C

onti

nued

.)

Tele

scop

eO

bser

vato

ryPl

ace

(Com

mon

Nam

e)

Cle

arap

ertu

reO

ptic

alde

sign

Mak

erFo

calr

atio

sM

ount

ing

Man

ufac

ture

r

Lat

itude

Lon

gitu

deE

leva

tion

Yea

rN

otes

Tel

esco

pede

Schm

idt

Obs

erva

toir

ede

Cal

ern

Cal

ern,

Fran

ce(C

aler

nSc

hmid

t)

0.90

-mco

rrec

tor

Schm

idt

Jean

Texe

reau

f/3.

5

··· C.M

.G—

Pari

s43

◦ 45′

N6◦

56′ W

1270

m

1981

Cer

-Vit

1.52

-mpr

imar

y

Tel

esco

peC

ombi

nede

Schm

idt

Obs

erva

toir

eR

oyal

deB

elgi

que

Ucc

le,B

ruxe

lles,

Bel

gium

···

0.84

-mco

rrec

tor

Schm

idt

Cox

,Har

grea

ves,

Tho

mso

nf/

2.5

··· Zei

ss(J

ena)

50◦ 4

8′N

4◦21

′ E10

5m

1958

1.2-

mbo

rosi

licat

epr

imar

ym

irro

r

Schm

idtT

eles

cope

Rad

ioas

trop

hysi

calO

bser

vato

ryR

iga,

Lat

via

···

0.80

-mco

rrec

tor

Schm

idt

Zei

ss(J

ena)

f/3.

0

··· Zei

ss(J

ena)

56◦ 4

7′N

24◦ 2

4′E

75m

1968

Ope

rate

dby

the

Lat

vian

Aca

dem

yof

Scie

nces

;1.2

-mpr

imar

ym

irro

r

Cal

ar-A

lto-S

chm

idts

pieg

elC

alar

Alto

Obs

erva

tory

Cal

arA

lto,S

pain

(Cal

arA

ltoSc

hmid

t)

0.80

-mco

rrec

tor

Schm

idt

Zei

ss(J

ena)

f/3.

0

Equ

ator

ialf

ork

Gru

bb–P

arso

ns37

◦ 13′

N2◦

32′ W

2168

m

1980

Tub

ean

dop

tics

mov

edfr

omH

ambu

rg,

Ger

man

y,w

here

the

inst

rum

enth

adbe

enin

use

sinc

e19

55;1

.2-m

prim

ary

mir

ror

RE

FR

AC

TO

RS

Yer

kes

40-i

nch

Ref

ract

orY

erke

sO

bser

vato

ryW

illia

ms

Bay

,Wis

cons

in,U

S(4

0in

ch)

1.01

6-m

doub

let

Vis

ualr

efra

ctor

Alv

anC

lark

&So

nsf/

19.0

4

Ger

man

equa

tori

alW

arne

ran

dSw

asey

42◦ 3

4′N

88◦ 3

3′W

334

m

1897

Uni

vers

ityof

Chi

cago

;afo

calr

educ

eral

sopr

ovid

esan

f/3

focu

s

36-i

nch

Ref

ract

orL

ick

Obs

erva

tory

Mou

ntH

amilt

on,C

alif

.,U

S(3

6in

ch)

0.89

5-m

doub

let

Vis

ualr

efra

ctor

Alv

anC

lark

&So

nsf/

19.7

Ger

man

equa

tori

alW

arne

ran

dSw

asey

37◦ 2

0′N

121◦

39′ W

1290

m

1888

Fron

tsur

face

ofcr

own

elem

entr

efigu

red

in19

87

Meu

don

Ref

ract

orO

bser

vato

ire

dePa

ris

Meu

don,

Fran

ce(3

3in

ch)

0.83

-mdo

uble

tV

isua

lref

ract

orH

enry

brot

hers

f/19

.5

··· P.G

autie

r48

◦ 48′

N2◦

14′ E

162

m

1889

Pots

dam

Ref

ract

orZ

entr

alin

stitu

tfur

Ast

roph

ysik

Tele

graf

enbe

rg,P

otsd

am,G

erm

any

···

0.80

-mdo

uble

tV

isua

lref

ract

orC

.A.S

tein

heil

f/15

.0

··· Rep

sold

52◦ 2

3′N

13◦ 0

4′E

107

m

1899

Sp.-V/AQuan/1999/10/27:16:16 Page 697

698 / 27 INCIDENTAL TABLESTa

ble

27.1

4.(C

onti

nued

.)

Tele

scop

eO

bser

vato

ryPl

ace

(Com

mon

Nam

e)

Cle

arap

ertu

reO

ptic

alde

sign

Mak

erFo

calr

atio

sM

ount

ing

Man

ufac

ture

r

Lat

itude

Lon

gitu

deE

leva

tion

Yea

rN

otes

The

Tha

wR

efra

ctor

Alle

ghen

yO

bser

vato

ryPi

ttsbu

rgh,

PA,U

S(3

0in

ch)

0.76

-mdo

uble

tR

ed-l

ight

refr

acto

rR

.E.S

umne

rf/

18.6

Ger

man

equa

tori

alW

arne

ran

dSw

asey

40◦ 2

9′N

80◦ 0

1′W

380

m

1985

Ori

gina

llyha

da

Bra

shea

rvi

sual

obje

ctiv

e(1

914)

;pr

esen

tone

isco

rrec

ted

for

red

light

Lun

ette

Bis

chof

fsch

eim

Obs

erva

toir

ede

Nic

eM

ontG

ros,

Fran

ce···

0.74

-mdo

uble

tV

isua

lref

ract

orH

enry

Bro

ther

sf/

24.2

Ger

man

equa

tori

alP.

Gau

tier

43◦ 4

3′N

7◦18

′ E37

2m

1886

28-i

nch

Vis

ualR

efra

ctor

Old

Roy

alO

bser

vato

ryG

reen

wic

h,L

ondo

n,E

ngla

nd(G

reen

wic

hre

frac

tor)

0.71

1-m

doub

let

Vis

ualr

efra

ctor

Gru

bbf/

11.9

Eng

lish

equa

tori

alR

anso

mes

and

Sim

s51

◦ 29′

N00

◦ 00′

47m

1894

Dom

eun

der

repa

irin

1992

Gro

sser

Ref

rakt

orA

rche

nhol

d-St

ernw

arte

Alt

Tre

ptow

,Ber

lin,G

erm

any

···

0.68

-mdo

uble

tV

isua

lref

ract

orC

.A.S

tein

heil

f/30

.9

Ger

man

equa

tori

alH

oppe

–Ber

lin52

◦ 29′

N13

◦ 29′

E41

m

1896

Gro

sser

Ref

rakt

orA

stro

nom

isch

esIn

st.,

Uni

v.O

bs.

Vie

nna,

Aus

tria

···

0.67

-mdo

uble

tV

isua

lref

ract

orG

rubb

f/15

.7

Ger

man

equa

tori

alG

rubb

48◦ 1

4′N

16◦ 2

0′E

241

m

1880

McC

orm

ick

Ref

ract

orL

eand

erM

cCor

mic

kO

bser

vato

ryC

harl

otte

svill

e,V

A,U

S(2

6in

ch)

0.66

7-m

doub

let

Vis

ualr

efra

ctor

Alv

anC

lark

&So

nsf/

14.9

Ger

man

equa

tori

alW

arne

ran

dSw

asey

38◦ 0

2′N

78◦ 3

1′W

264

m

1883

26-i

nch

Equ

ator

ial

US

Nav

alO

bser

vato

ryW

ashi

ngto

n,D

C,U

S(2

6in

ch)

0.66

-mdo

uble

tV

isua

lref

ract

orA

lvan

Cla

rk&

Sons

f/15

.0

Ger

man

equa

tori

alW

arne

ran

dSw

asey

38◦ 5

5′N

77◦ 0

4′W

92m

1873

Tho

mps

onR

efra

ctor

Roy

alG

reen

wic

hO

bser

vato

ryH

erst

mon

ceux

,Sus

sex,

Eng

land

···

0.66

-mdo

uble

tV

isua

lref

ract

orG

rubb

f/10

.4

Ger

man

equa

tori

alG

rubb

50◦ 5

2′N

0◦20

′ E34

m

1897

Sp.-V/AQuan/1999/10/27:16:16 Page 698

27.9 THE WORLD’ S LARGEST OPTICAL TELESCOPES / 699

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