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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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670 / 27 INCIDENTAL TABLES
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
n,(K
luw
erA
cade
mic
,D
ordr
echt
),p.
1124
.H
artle
y,M
.,&
Daw
e,J.
A.1
981,
Pro
c.A
stro
n.So
c.A
ustr
alia
,4,2
5125
.P
rope
rM
otio
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tic
Ast
rono
my,
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Rob
erta
M.H
umph
reys
,ASP
Con
f.Se
ries
127
26.
Las
ker,
B.M
.,St
urch
,C.R
.,M
cLea
n,B
.,R
usse
ll,J.
L.,
Jenk
ner,
H.,
&Sh
ara,
M.1
990,
AJ,
99,2
019
27.
Urb
an,
S.E
.,C
orbi
n,T.
E.,
&W
ycof
f,G
.L.,
1997
,U
.S.
Nav
alO
bser
vato
ry,
Ast
rogr
aphi
cC
atal
ogue
posi
tions
rere
duce
dus
ing
the
AC
RS
and
then
plac
edon
the
Hip
parc
ossy
stem
28.
IAU
Sym
posi
um14
1,19
91,I
nert
ialC
oord
inat
eSy
stem
onth
eSk
y,ed
ited
byJ.
H.L
iesk
ean
dV
.K.A
bala
kin,
(Klu
wer
Aca
dem
ic,D
ordr
echt
)29
.Tr
ansa
ctio
nsof
the
IAU
,XX
IB19
91,e
dite
dby
J.B
erge
ron
(Klu
wer
Aca
dem
ic,D
ordr
echt
)30
.Sw
arth
mor
e:W
orks
hop
onD
atab
ases
for
Gal
acti
cSt
ruct
ure,
1993
,ed
ited
byA
.G.
Dav
isPh
ilip,
B.
Hau
ck,
and
A.R
.U
pgre
n(L
.D
avis
Pres
s,Sc
hene
ctad
y)31
.D
igit
ized
Opt
ical
Sky
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eys,
edite
dby
H.T
.Mac
Gill
ivra
yan
dE
.B.T
hom
son
(Klu
wer
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dem
ic,D
ordr
echt
)32
.M
onet
,D.G
.199
6,U
SN
aval
Obs
erva
tory
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(10
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Ms)
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Tabl
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ajor
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Sp.-V/AQuan/1999/10/27:16:16 Page 683
684 / 27 INCIDENTAL TABLESN
otes
aE
xpla
nati
onof
the
colu
mns
:T
heco
lum
nsin
this
tabl
elis
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rfor
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atis
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27.1
0,an
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and
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nclu
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decl
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cent
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for
the
surv
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eth
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isch
ange
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me
ofth
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betw
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inko
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ical
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IIof
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stem
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ited
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per
and
B.
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urst
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POSS
=Pa
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ones
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and
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rees
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nstit
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uyte
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uyte
n,W
.J.1
963–
87,P
rope
rM
otio
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rvey
with
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y-E
ight
Inch
Schm
idtT
eles
cope
(Uni
vers
ityof
Min
neso
ta,M
inne
apol
is);
Luy
ten:
Luy
ten,
W.J
.198
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yFi
rst7
2Y
ears
ofA
stro
nom
ical
Res
earc
h,M
inne
apol
is,p
p.26
–28
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oess
el,J
.G.e
tal.
1979
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SP,9
1,41
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lom
arIn
frar
edsu
rvey
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aske
r,B
.M.e
tal.
1990
,AJ,
99,2
019
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eid,
I.N
.eta
l.19
91,P
ASP
,103
,661
7.M
onet
,D.G
.,&
Wes
terh
out,
G.1
989,
inD
igit
ized
Opt
ical
Sky
Surv
eys,
edite
dby
C.J
asch
ek,i
nB
ull.
d’In
fo.d
uC
DS,
No.
37,(
Obs
.de
Stra
sbou
rg,S
tras
bour
g),
p.75
.T
heU
SNO
QJ
isa
two-
min
ute
expo
sure
onun
hype
rsen
sitiz
edII
Ia-J
emul
sion
sto
beus
edfo
rth
ede
term
inat
ion
ofpo
sitio
nsof
brig
htst
ars.
8.W
est,
R.M
.,&
Schu
ster
,H.-
E.1
982,
AA
S,49
,577
9.W
est,
R.M
.198
4,in
IAU
Col
loq.
No.
78,p
.13.
10.
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non,
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.198
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No.
78,A
stro
nom
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ith
Schm
idtT
eles
cope
s,ed
ited
byM
.Cap
acci
oli(
Rei
del,
Dor
drec
ht),
p.25
11.
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.
12.
Har
tley,
M.,
&D
awe,
J.A
.198
1,P
roc.
Ast
ron.
Soc.
Aus
tral
ia,4
,251
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
Sp.-V/AQuan/1999/10/27:16:16 Page 689
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.
Sp.-V/AQuan/1999/10/27:16:16 Page 690
27.9 THE WORLD’ S LARGEST OPTICAL TELESCOPES / 691Ta
ble
27.1
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orld
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)
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ach
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and
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1)Fo
urse
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ctor
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beus
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er;fi
rstu
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ecam
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1998
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rors
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m
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ated
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rol
Sp.-V/AQuan/1999/10/27:16:16 Page 691
692 / 27 INCIDENTAL TABLESTa
ble
27.1
4.(C
onti
nued
.)
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ufac
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Lat
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eles
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(nor
th)
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tAst
rono
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ter
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(sou
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r-A
mer
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8,6
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ries
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ount
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uth
LO
MO
43◦ 3
9′N
41◦ 2
6′E
2100
m
1975
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ary
mir
ror
repl
aced
inab
out1
984,
and
ath
ird
mad
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llgl
ass
was
figur
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Geo
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ale
Tele
scop
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ount
ain,
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if.,
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inch
)
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-mm
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nder
son
f/3.
3,16
,30
Hor
sesh
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kem
ount
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tingh
ouse
33◦ 2
1′N
116◦
52′ W
1706
m
1948
Cal
ifor
nia
Inst
itute
ofTe
chno
logy
;rib
bed
prim
ary
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ngPy
rex
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iam
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chos
La
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irro
r— G
rubb
–Par
sons
f/2.
5,11
Alta
zim
uth
Gru
bb–P
arso
ns28
◦ 46′
N17
◦ 53′
W23
32m
1987
Ope
rate
dby
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Roy
alG
reen
wic
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bser
vato
ry;
prim
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ror
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wen
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tor
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roTo
lolo
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r-A
mer
ican
Obs
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erro
Tolo
lo,C
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er)
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ror
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hey–
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etie
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PNO
Opt
ical
Shop
f/2.
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0
Hor
sesh
oeeq
uato
rial
Wes
tern
Gea
rC
orp.
30◦ 1
0′S
70◦ 4
9′W
2215
m
1976
Cer
-Vit
prim
ary
mir
ror
Ang
lo-A
ustr
alia
nTe
lesc
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lo-A
ustr
alia
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bser
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ding
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tral
ia(A
AT
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ror
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bb–P
arso
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,36
Hor
sesh
oeeq
uato
rial
Mits
ubis
hi31
◦ 17′
S14
9◦04
′ E11
49m
1975
Cer
-Vit
prim
ary
mir
ror
Sp.-V/AQuan/1999/10/27:16:16 Page 692
27.9 THE WORLD’ S LARGEST OPTICAL TELESCOPES / 693Ta
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
Nic
hola
sU
.May
allR
eflec
tor
Kitt
Peak
Nat
iona
lObs
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ittPe
ak,A
rizo
na,U
S(K
ittPe
ak4
m)
3.81
-mm
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rR
itche
y–C
hret
ien
KPN
OO
ptic
alSh
opf/
2.7,
8,15
.7IR
,190
Hor
sesh
oeeq
uato
rial
Wes
tern
Gea
rC
orp.
31◦ 5
8′N
111◦
36′ W
2120
m
1973
Fuse
d-qu
artz
prim
ary
mir
ror
Uni
ted
Kin
gdom
Infr
ared
Tele
scop
eJo
intA
stro
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yC
entr
eM
auna
Kea
,Haw
aii,
US
(UK
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)
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2-m
mir
ror
Cas
segr
ain
Gru
bb–P
arso
nsf/
2.5,
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Eng
lish-
yoke
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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