WDS method codes: A = adaptive optics Ac = CHARA adaptive optics Ad = adaptive optics spectral deconvolution technique Ag = laser-guided AO Al = adaptive optics imaging, keeping only selected images ("lucky imaging") Am = adaptive optics with aperture mask Ao = adaptive optics coronagraph As = AO + dark speckle coronagraph Aw = adaptive optics with coronagraph and "well-corrected subaperture" C = CCD or other two-dimensional electronic imaging Ca = Area scanner Cc = IR coronagraph Ce = Electronographic camera Ci = IR direct imaging Cl = short-exposure CCD imaging, keeping only selected images ("lucky imaging") Cp = IR imaging polarimetry Cs = IR one-dimensional slit scanning Cu = USNO CCD imaging (speckle-style reduction) D = Heliometer E = Wide-field CCD or other two-dimensional electronic imaging E2 = 2MASS (Two Micron All-Sky Survey) Ed = DENIS (Deep Near-Infrared Survey) Ek = UKIDSS (UKIRT Infrared Deep Sky Survey) Es = SDSS (Sloan Digital Sky Survey) Eu = UCAC3/UCAC4 H = Hipparcos/Tycho, HST, Spitzer, or other space-based technique Hc = Chandra Ha = HST + ACS He = Einstein Hf = HST + Fine Guidance Sensor Hh = Hipparcos Hi = Spitzer Space Telescope + IRAC (Infrared Array Camera) Hm = Spitzer Space Telescope + MIPS (Multiband Imaging Photometer for Spitzer) Hn = HST + NICMOS IR direct imaging Ho = HST + Faint Object Camera Hp = HST + WFPC2 Planetary Camera Hs = HST + STIS Ht = Tycho Hw = WISE (Wide-field Infrared Survey Explorer) satellite (IR imaging) Hx = Spitzer Space Telescope + SpeX spectrometer and slit-viewing camera I = interferometric technique Ig = phase grating interferometer Im = Michelson interferometer J = visual interferometer Jm = Mount Wilson 100-inch telescope rotating interferometer (Anderson, Merrill) Jp = Mount Wilson 20-foot beam interferometer (Pease) K = long-baseline visual/IR/radio interferometer K2 = CERGA 2-telescope interferometer Ka = VLTI/AMBER Kb = BIMA Kc = CHARA Array Ke = European VLBI network Kf = CHARA Array (separated fringe packet data) Kg = global VLBI array Ki = IOTA Kk = Keck interferometer Kl = VLA/VLBA Km = Mark III Kn = NPOI (Navy Prototype/Precision Optical Interferometer) Kp = PTI (Palomar Testbed Interferometer) Kr = radio/IR aperture synthesis technique Ks = SUSI (Sydney University Stellar Interferometer) Ku = Pulkovo Stellar Interferometer M = micrometry technique Ma = micrometer with refractor Mb = micrometer with reflector Mc = Comparison image micrometer Md = Visual measures with a double-image micrometer Mr = RGO use of micrometer plus comparison image micrometer on same star O = occultation P = photographic technique Pa = photographic, with astrograph Pc = Astrographic Catalog Pe = ESO Schmidt astrograph Pk = AGK Catalog Po = photographic, with medium or long-focus technique or with ocular enlargement Pp = Palomar Observatory Sky Survey (POSS-I/POSS-II) Pu = UK Schmidt Southern Survey S = speckle interferometric technique Sa = aperture masking technique (MAPPIT, etc.) Sb = bispectrum speckle interferometric technique Sc = CHARA speckle Si = IR speckle Sp = speckle polarimetry Ss = shift-and-add technique St = Tokovinin speckle camera (SOAR) Su = USNO speckle T = Transit circle / Meridian circle Tm = "Eyepiece micrometer" transit/chronometric technique V = visual estimate X = spectroscopic technique Xg = Visual estimate made with an objective grating Xh = high-resolution spectroscopy Xl = low-resolution spectroscopy Xr = resolved spectroscopy Xs = spectrophotometry Z = photometric technique Zc = CCD photometry Zd = Photocell with diaphragm in focal plane Zp = Visual photometry with a double-image or polarizing photometer Zw = Wedge photometer =========================== Observation codes: F Too faint, not seen, or not located G This measure is not in the published paper but is a vector combination of measured pairs by this author for a pair already in the WDS. I Identification, or question about such L Original PA given as n, nf, f, sf, s, sp, p, or np (n = north, f = following, s = south, p = preceeding), and converted to 0, 45, 90, 135, 180, 225, 270, or 315, respectively. Also, a PA given as e or w (e = east, w = west) is converted to 90 or 270 respectively. Due to the small number of single letter codes (n, f, s, and p), the PA is assumed accurate only to the nearest quadrant (i.e., +/- 45 deg). M Mean of multiple measures of same photographic plate or CCD. N Identification error, position error, or misprint in publication, corrected. O Optical P Corrected by author V No. of nights varies 50% or more between angle and separation measures X Identification error, position error, or misprint in publication, NOT corrected. Code "X" data are not included in the summary line. The X code is also used to indicate measures superceded by later reductions of the same data (for example, reprocessing of Astrographic Catalog data for the WFC). Z Measurer other than author(s)