6 This source is interesting because the UV bright star is surrounded by
  6 nebulosity. The star is hidden from view by the nebulosity on both the PSS
  6 blue and red prints. The nebulosity itself is much more prominent on the
  6 PSS print. The Catalogue of Galactic Planetary Nebulae (Perek and Kohoutek
  6 1967) was searched but no object was found at this position. Present
  6 evidence, however, is too limited to suggest this source is a planetary.
  6 Its importance here is directed principally to the strong UV excess of the
  6 coincident stellar source. No estimate of the blue magnitude was attempted
  6 because of the apparent association with nebulosity. Strong UV excess of
  6 south preceding star, surrounded by nebulosity. No blue magnitude estimate
  6 is given because of contamination of the image by the nebulosity.
 10 see Horne, Lanning, Gomer (1982ApJ...252..681H)
 15 This is a high-latitude source b = +37.4 deg) approximately 1 degree south
 15 of the Hercules X-ray source, which is probably too far from the X-ray
 15 error box to be associated with that source. The object has a very large
 15 UV excess ((U-B) < -1.0) and has been suggested as the optical
 15 identification of the Bologna radio source B2 1656+34 by Grueff and
 15 Vigotti (1972A&AS....6....1G). Its estimated blue magnitude is approximately
 15 18.5 mag.
 16 Located in the Omega Nebula (M17). The AGK1 m(V)=9.6. No estimate of the
 16 blue magnitude was attempted due to the heavy nebulosity in the field.
 16 = BD-16 4818
 17 This faint source is variable. It was very prominent on the two-color
 17 plate as a result of its large UV excess. In addition, the image appeared
 17 to be nebulous in character. The most striking nature of the object,
 17 however, was the absence of any image on the PSS blue print plate. An
 17 image near the plate limit on the PSS red print was measured and compared
 17 to the two-color print, and is believed to be the same object. A
 17 subsequent two-color print plate partially overlapping the first was
 17 taken 13 months later and shows no trace of the UV object.
 18 Luyten (1963)
 25 Attention is drawn to the peculiar object east of no 25, and designated by
 25 the arrow on the chart in the printed paper. This source does not show any
 25 UV excess but was of interest because of its nebulous image, apparent on
 25 both the red and blue PSS prints and the two-color plate. The 1950
 25 coordinates for this object are: RA = 02:25:16; Dec = +63:03:20.
 31 Observed near minimum. Kukarkin et al. (1970) gives m(pg) = 11.7 - 14.0;
 31 eclipsing (Algol)-spectral type - B9. = RY Aur
 33 DEC error in Paper corrected for WWW
 36 Central star of 195-0 1 (Perek & Kohoutek 1967) Planetary Neb.
 41 Possible QSO; Moderately bright UV with emission feature at 3740A
 42 Moderate UV excess (-05 >/= U-B > -0.8). Very Faint.
 43 HD 173637. Photoelectric B magnitude (Blanco et al. 1970); U-B = -0.66;
 43 B1 IV. = BD-8 4702 = HD 173637.
 46 Photoelectric B magnitude (Blanco et al. 1970); U-B = -0.86; WDA. = EG 134
 46 = G142-50
 47 Central star of planetary nebulae NGC 6842 (Perek & Kohoutek 1967).
 50 Photoelectric B magnitude (Blanco et al. 1970); U-B =-0.72; WDA. = EG 136
 50 = (WZ Sge)
 51 Suspected white dwarf (Giclas et al. 1971). = G231-40
 65 = +36 1030
 68 = +37 1122
 77 Noted as good moderately bright uv candidate. No emission detected.
 78 Rapid irregular variable (Kukarkin et al. 1970); m(pg) = 13.0 - 14.5. HZ
 78 Her has been suggested as the possible optical identification of Her X-1
 78 (Liller 1972).
 82 Giclas et al. (1971) = G231-43.
 85 Although a much fainter companion is slightly overlapping this image to
 85 the southwest, the identification of this object as a marginal to moderate
 85 UV source is firm.
 87 Strong UV excess? Dense core in UV This source is the center star of a
 87 close, nearly overlapping, string of three stars. The UV image appears to
 87 be very strong with a dense core, but the proximity of the other stars and
 87 possible offset in orientation make confirmation questionable. No other
 87 images on the Palomar Sky Survey prints suggest the presence of any
 87 overlapping images which would contribute to the apparent UV excess.
 90 = V1776 Cyg. During the initial quick-look survey of selected UV-bright
 90 sources from this survey by Shafter (private communication), this 17th
 90 magnitude source was noted to exhibit the spectrum of a cataclysmic
 90 variable, as was later reported by Shafter, Lanning, and Ulrich
 90 (1983PASP...95..206S). The authors presented evidence suggesting the system
 90 was an eclipsing CV. Garnavich, et al. (1990ApJ...365..696G), determined
 90 that Lanning 90 (V1776 Cyg) is indeed eclipsing. An orbital period of 3h57m
 90 was obtained, and variations in the shape of the eclipse were detected along
 90 with brightness changes of more than a magnitude in less than one day
 90 outside eclipse. A re-examination of the original two-color plate suggests
 90 the blue magnitude of this UV source was approximately 19 at the time of
 90 detection.
 91 No emission was detected. The U-B suggests this is a very blue source.
 93 = LSIII 46 -7 = BD+46 2948
100 Very near plate limit in B
103 = LSIII 47 -13 = BD+46 3023
106 This source was noted by Shafter to be of ~13-14th magnitude. Narrow
106 absorption lines were detected.
111 Central star of PK93+5 1
112 = GD393
116 Normally sources brighter than 10th magnitude were ignored due to
116 saturation of the image and merging of the UV and B images. Magnitude and
116 color estimates are very difficult to establish. The source was noted
116 because it had appeared at first inspection to be in the marginal range
116 with a U-B ~ -0.2. The magnitudes noted in the SIMBAD database for this
116 8th magnitude star, however, indicate a U-B = +0.15 suggesting the source
116 may be variable. = HD201033
118 Although this source is near the plate limit, the object appears
118 noticeably blue.
120 This source is overlapped with another star which is slightly fainter.
120 However, the orientation between the two is such that the blue nature of
120 the UV source seems evident with a moderate strength, i.e. U-B ~ -0.8. A
120 quantitative value for this source, however, cannot accurately be
120 provided.
122 The plate examined in Paper II was an overlapping field with a plate in
122 Paper I. The 12.5 magnitude source is coincident with Lanning 51 and was
122 also detected by Downes (1986), KPD2117+5400. Although placed into the
122 marginal detection category with a U-B of only ~ -0.4 in this survey,
122 Lanning 51 has been previously identified as the DA white dwarf G231-40
122 (Lanning 1973).
124 Central star of PK116+8 1
130 Re-examination of plate suggests overlapping image. Not UV.
134 The plate on which this source was detected in part II is also an
134 overlapping plate from Paper I. This ~18th magnitude source is coincident
134 with Lanning 1 and appeared in Paper I to be a very strong UV source. On
134 the plate examined for the second segment of the survey, the source
134 detection appears marginal with a U-B estimate of only ~ -0.4.
149 The position for this source coincides with the center of the planetary
149 nebula HFG 1 (PN G136.3+05.5) discovered by Heckathorn, Fesen, and Gull
149 (1982A&A...114..414H). They detected the nebula in [OIII] interference-
149 filter imagery showing it to be approximately 15 arcmin in diameter, but
149 asymmetric. No nebulosity was visible on the two-color plate examined in 
149 this survey. The 14th magnitude central star is noted by Bond (1994) as a
149 reflection effect binary (V664 Cas) based on the photometric variations of
149 this short period (13h57m) binary (Grauer et al 1987). The central star
149 examined on the two-color plate in this study was estimated to have a 
149 U-B ~ -0.6 and a m(B) ~ 13.
159 The color of this source appears slightly blue at U-B ~-0.3 . The image is
159 much brighter than other stars in the immediate field of view. However, on
159 the Palomar Observatory Sky Survey (POSS) Blue print, the object is of
159 comparable or slightly fainter brightness. The UV image of the candidate
159 source overlaps with the B image of an adjacent star to the west. This
159 overlapping star, however, is very faint on the POSS Blue print (near the
159 plate limit), and noticeably redder on the Red plate, suggesting a small
159 UV contribution, if any. Therefore, the UV identification of Lanning 159
159 is believed to be valid and suggests the source is probably variable. The
159 object could be a nova-like source which was brighter in the UV at the
159 time the two-color plate was exposed, or perhaps an eclipsing binary
159 caught during eclipse allowing the blue component to dominate during the
159 exposure. Neither case would be unprecedented. Paper I describes two such
159 sources, Lanning 17, an apparent nova which was observed to be very blue
159 on the two-color plate but was coincident with a faint red source on the
159 POSS E plate, and Lanning 31, which was noted to be the eclipsing algol RY
159 Aur observed during eclipse. The plate on which this source was detected
159 was taken JD2440506.8440 (12 Oct. 1969 UT).
165 This source is identified as the (m(B) = 14.17) DA2/DAwk white dwarf WD
165 0147+674 = GD 421 (McCook and Sion 1987, Greenstein 1984). The estimated
165 blue magnitude on the two-color plate is only slightly beyond the
165 estimated errors at m(B) ~ 13.5, and does not necessarily suggest the
165 source is variable. This source has also been detected by ROSAT, RE
165 J0151+673 (Pounds, et al. 1993).
179 The central star of PN G144.1+06.1 = NGC 1501
180 This source is identified as AG+60 431 (BD+60 806). Normally, a source as
180 bright as this object, m(B) ~ 10.5, is not given a value for the U-B color
180 in this survey due to the uncertainty of accurate measurements for merged
180 images. However, the color of the object on this plate appeared blue and
180 was therefore given a U-B estimate of ~-0.5:. The SIMBAD database
180 indicates the spectral type is F5. Bidelman (private communication)
180 confirms the spectral type identification from a Case survey plate, noting
180 also that the star appears to be weak-lined.
181 Located in the same field as Lanning 180
182 Bidelman (private communication) found that this object is SS 14 = VES 779
182 (Stephenson and Sanduleak 1977). The star is classified as OB- r:w, i.e. a
182 reddened OB-type star with weak Hydrogen emission. Spectra obtained by
182 Shafter (private communication) with the grism spectrograph of the Mt.
182 Laguna Observatory 1.0-m telescope and Schultz (private communication)
182 with IUE support this classification.
187 Coincident with the planetary nebula PN G142.1+03.4 (Acker 1992), the
187 nebulous images on the plate definitely indicate a blue object on the
187 two-color plate. The U-B is estimated to be ~-0.5. However, no stellar
187 source within the nebular image was evident. [incorrectly identified in
187 published text; is really Lanning 187, not 188.]
189 Identified as LS I +59 193; OB-. [incorrect ID in published paper...should
189 be associated with Lanning 189, not 190; = HHL 110695]
196 BD +59 117, LS I +59 53; B2
198 BD +59 208, LS I +59 65; B5 (U-B=-0.46)
200 UBV 721; B7 (U-B=-0.11)
202 BD +58 142, LS I +59 59; B0 (U-B=-0.62)
204 UBV 1209; B2 (U-B=-0.37)
208 BD +58 188; B7 (U-B=-0.28)
210 UBV 723; B6 (U-B=-0.16)
213 Correction for LAN 213 Brian Skiff (2003, private communication) reported
213  that the identification for Lanning 213 was likely incorrect on the
213  published finding chart in Lanning & Meakes (1998PASP..110..586L Paper IV).
213  We have confirmed the object was indeed incorrectly marked. Additionally,
213  the J2000.0 positions provided in the table were measured for the wrong
213  star. The correct UV-bright source is the brighter star 20" to the north.
213  The correct J2000.0 positions and star identification have been updated on 
213  the Web site devoted to this survey. The correct J2000.0 coordinates are
213  RA=01:05:30.8, DE=+59:10:34.9. (instead of 01:05:31.1 +59:10:13.7)
215 LS I +58 28; EM*
222 CCDM J01154+5831A
224 BD +57 153, LS I +58 18; B0
226 BD +57 219; G0 (poss. contamination?)
227 BD +57 227, LS I 57 9; B5
231 BD +56 213; B5
232 LS I +57 8
237 BD +56 87, HD 236471; Ap
238 BD +56 109, HD 236497; B8
248 LS I +56 15
267 This source was verified to be the same as KPD 0054+5406. The B magnitude
267 was estimated at 14.5 with U-B=-0.6, in close agreement with the
267 photometric values provided by Downes (1986), where V=14.12, B-V=-0.07,
267 and U-B=-0.9. He places the object in his category of sdB stars.
270 BD +60 682, LS I +60 305; (U-B=-0.21)
271 LS I +60 278; B (U-B=-0.50)
274 LS I +59 191; B (U-B=-0.44)
275 LS I +59 173, BD +59 608; B2 III (U-B=-0.4)
277 HD 20295; B5 III (U-B=-0,39)
281 The SIMBAD search identified this source as AF Cam. The identification was
281 verified by examining the chart provided by Downes & Shara 
281 (1993PASP..105..127D). AF Cam is classified as a U Gem-type dwarf nova with
281 a range in V magnitude of 13.4-17.0.
283 LS I +58 97; B (U-B=-0.44)
285 BD +58 623, LS I +58 127; B8 (U-B=-0.64)
302 Although it appears only the blue image is present on the plate and the
302 source may not necessarily be a UV-bright object, it was very interesting
302 in that it looked, initially, very characteristic of a comet. A dense core
302 image was surrounded by more nebulous material with an apparent small tail
302 trailing off to the southeast. No image was noted at this location on the
302 Digitized Sky Survey. Further investigation, however, revealed that the
302 apparent tail was nearly 1000 from that expected given the position of the
302 Sun at the time of observation. An alternative explanation may suggest the
302 object is, actually, a nova-like system that, upon brightening, ionized
302 the nonsymmetrically oriented gas in the immediate neighborhood of the
302 nova, making it visible for a short time. Upon fading, the gas and the
302 star were then no longer visible. A search of the Palomar Sky Survey E
302 and O prints revealed no source at the reported position. Plates taken in
302 1983 by R. Downes (1997, private communication) in the U and B were also
302 examined and provided no evidence of a source at this position. The object
302 is clearly a transient source. The position listed in Table 1 is the
302 precessed position of the object as determined from the original plate.
302 The epoch of the plate was JD=2,440,507.8187. Given the nebulous
302 surroundings, the magnitude estimate of 14 is uncertain.
307 LS I +56 90; B (U-B=-0.32)
310 LS V +56 57
313 LS V +55 14; B
317 BD +55 838, LS I +55B 58; B3 Ib (U-B=-0.1)
323 LS V +53 19; B EM*
332 BD +51 815, LS V +52 16; B6 V
333 BD +51 819; B1 IV
338 LS V +51 15; B
345 LS V +51 13; 06 (U-B=-0.1); exciting star of H II region
345 [L89b] 150.590-00.950
346 FO Per (Z Cam-type dwarf nova); -0.6. Exhibiting a relatively strong blue
346 color, U-B~-0.6, this source was identified as FO Per and verified from
346 the Downes & Shara (1993PASP..105..127D) chart. FO Per is also a dwarf nova
346 of U Gem type, subclass Z Cam. It is noted by Downes & Shara to range
346 from 11.8v to 16.2p. The B magnitude on the two-color plate for this
346 paper was estimated at B~13.0.
349 LS V +51 17; B
351 WD 0402+543; DAs
361 This source is coincident with the previously identified DA white dwarf
361 found by Downes (1986ApJS...61..569D), KPD 2046+3940 (DAw). Both the B
361 magnitude and U-B color fell within the 0.5 mag uncertainty for this very
361 blue source. Downes gave an estimate of U-B~-1.20; the estimate from this
361 study was ~-0.9.
390 Estimated at mB~11.0 and U-B~-0.3, this source is within 2' of the reported
390 position of the transient X-ray source Cyg X-4. However, the position for
390 Cyg X-4 is very uncertain given the 1deg^2^ error box (Amnuel, Guseinov &
390 Rakhamimov, 1982Ap&SS..82....3A). Three rocket observations are listed by
390 Amnuel which suggest a slow decline of the X-ray source of about a factor of
390 8 in 3 years. The X-ray source has not been seen since the last observation
390 in 1968 (Amnuel, Guseinov & Rakhamimov, 1979ApJS...41..327A). It seems
390 highly unlikely that an 11th magnitude star close to the center of the error
390 box would not have been observed during previous searches for the optical
390 counterpart to the X-ray source. No optical candidate for Cyg X-4 has ever
390 been identified.
430 WD 2119+58 (DA) is the third white dwarf recovered during this part of the
430 survey analysis. McCook & Sion (1987ApJS...65..603M) list the white dwarf
430 as a DA6 with a photographic B mag of 16.0. The B and U-B estimates
430 determined in this study are 17.0 and -0.5, respectively.
456 Located in the field of the transient X-ray source H2116+55. The X-ray
456 source, detected in 1978 with HEAO 1, was a transient event which lasted
456 about 200s (Connors, Serlemitsos & Swank, 1986ApJ...303..769C). Although
456 the position of the UV source is within 5' of the center position reported
456 for the X-ray source, the position is not well determined. Based upon the
456 intensity of the X-ray source event and optical flare statistics, Conners
456 et al. indicated the source was likely to be a dMe or dKe star undergoing a
456 strong flaring episode. If so, the correlation of Lanning 456 with the X-ray
456 source is purely coincidental and cannot be confirmed as the optical
456 identification of the X-ray source.
496 This strong UV source is the central star of the planetary nebula IC 289
496  (PN G138.8+02.8). The B magnitude reported on SIMBAD is 16.8. The estimate
496  from this study gives an m_B_=17.0, although some uncertainty can be
496  expected as a result of the associated nebulosity, and a U-B of -0.8.
497 The source is coincident with the dwarf nova FT Cam. FT Cam is a UG-type
497  dwarf nova discovered by Antipin (1999IBVS.4673....1A) on Moscow archive
497  plates. The nova is characterized by short-term variations at minimum, with
497  outbursts of short duration and a total range in B of 14.0-17.6. On this
497  plate, the m_B_ was estimated to be 17.5 with a U-B=-0.9. The epochs of the
497  Sandage two-color plate U and B images were JD 2,440,507.89132 and
497  JD 2,440,507.91708, respectively.
502 This source is coincident with the ROSAT B0 X-ray source RX J0440.9+4431,
502  also known as VES 826. The X-ray source was suggested as a new massive
502  X-ray binary (Motch et al., 1997A&A...323..853M7) and was found by
502  comparing sources from the ROSAT all-sky survey with SIMBAD OB* catalogs.
502  A recent study by Reig & Roche (1999MNRAS.306..100R) describes the source
502  as a new persistent slow rotating X-ray pulsar. The epochs of the Sandage
502  two-color plate U and B images were JD 2,440,510.93576 and
502  JD 2,440,510.96157, respectively.
505 This blue source is within ~2" of the infrared source IRAS 04398+4411.
505  Examination of the Sandage two-color plate does suggest the presence of
505  some nebulosity in the B image. Perhaps this UV source is the exciting star
505  of this gas in the immediate vicinity.
515 An estimate for the U-B=-0.4 suggests that this source is in the marginal
515  range of detection as a UV source. However, the coincident star is noted as
515  HD 276118 with a spectral type of K5 and an m_B_=9.9. An m_B_=11.0 was
515  estimated on this plate. The inconsistency of the magnitudes and colors as
515  well as the spectral type suggest that this star may be a binary system
515  with an early-type companion observed during minimum or eclipse. The epochs
515  of the Sandage two-color plate U and B images were JD 2,440,510.93576
515  and JD 2,440,510.96157, respectively.
529 Coordinates were switched with  Lan 533 [from B. Skiff, June 2012]
533 Coordinates were switched with  Lan 529 [from B. Skiff, June 2012]
534 This source is coincident with the previously identified DA white dwarf
534  KPD 0416+4015 (Downes, 1986ApJS...61..569D). Downes listed the m_B_=16.0
534  and U-B=-1.09. The estimate from this study placed the m_B_ at 15.5 and
534  the U-B=-0.7, in reasonably good agreement with Downes.
537 is HD 276727 (not HD 176727) [from B. Skiff, June 2012]
540 This is another UV source coincident with a ROSAT X-ray source,
540  1RXS J041638.8+400236. The m_B_ was estimated to be 17.0 with the U-B=-1.0.
540  Information related to this survey including published papers, finding
540  charts, updated tables, etc., may be viewed on the World Wide Web site
540  devoted to the survey, http://www.stsci.edu/~lanning/index.html.
575 This UV-bright source is faint but very strong, with an estimated m_B_=19.2
575  and U-B=-0.6. We also note that the source exhibits a significant proper
575  motion. The source was notably displaced between the POSS red image
575  extracted (epoch 1953.8) and the GASP Quick-V image (1983.8). We have
575  measured both positions, determining a rate of motion of ~0.264"/yr.
575  The J2000.0 positions determined for both images are:
575  POSS red: RA=02:10:22.9, DE=+65:00:33.6;
575  GASP Quick-V: RA=02:10:23.8, DE=+65:00:28.1.
575  The proper motions tabulated in the USNO-B catalog confirm this source
575  exhibits significant motion with pm_RA_=188mas/yr and pm_DE_=-90mas/yr.
575  The very blue nature of this source, along with the high proper motion,
575  strongly suggest it is a white dwarf.
606 Another very strong UV-bright source, with m_B_=19.0 and U-B=-0.9, was noted
606  be 1.5' south of the X-ray source 1RXS J014206.4+592508.
607 A single image was detected that appears, in image character, to be similar
607  to typical planetary nebulae. A search of the SIMBAD database failed to
607  provide any corresponding identification with a previously cataloged
607  planetary nebula (PN), suggesting this may be a new PN.
608 This is another single-image source, similar to Lanning 607. This source,
608  however, was confirmed to be the planetary nebula PN G130.4+03.1.
614 The 11mag source Lanning 614 was found to be at the same position as that of
614   1RXS J051330.0+321353.
617 A large proper motion value was reported in the USNO-B catalog for the most
617  likely corresponding candidate for this UV-bright source (U-B=-0.9). The
617  values may be suspect, however, because of the faintness of the source
617  (B=20.0, near the plate limit). Very large uncertainties are noted in the
617  USNO-B tables. Another field star that was included in the table is
617  consistent with what was observed on the two-color survey plate. Thus, the
617  confidence in the identification is high, and the proper motion is probably
617  significant, but one should use caution in accepting the reported magnitude
617  of the motion.
627 The X-ray source 1RXS J052406.7+293742 is located within about 20" of the
627  very strong source Lanning 627 (U-B=-0.9).
652 The 17mag UV-bright source Lanning 652, estimated at U-B=-0.6, was confirmed
652  to be the previously identified Nova T Aur (Nova Aur 1891). The source
652  ranges in photographic magnitude from 4.2 to 15.2 and exhibits a period of
652  0.2 days (Downes, 1986ApJS...61..569D). The times of observation for the
652  source on this plate were JD2440507.00914 (UV image) and JD2440507.02992
652  (B image).
659 This strong UV-bright source (on the same survey plate as Lanning 652) was
659  identified as the U Gem-type dwarf nova FS Aur. The dwarf nova is noted
659  to have a range in V magnitude from 14.4 to 16.2, with a period of 0.06days
659  (Downes, 1986ApJS...61..569D). The magnitude and color estimates from
659  this work are m_B_=15.5 and U-B=-0.9. The times of observation for the
659  source on this plate were JD2440507.00914 (UV image) and JD2440507.02992
659  (B image).
663 This source is coincident with the previously identified DA white dwarf
663  WD 0544+280 (Kirkpatrick & McGraw, 1989, IAU Colloq. 114, 167). The source
663  is exceptionally bright in the UV, with an estimate of m_B_=20.0 and
663  U-B=-1.2. The verification of the source proved difficult, since the
663  details, including a finding chart and positional information, were never
663  published. The Kirkpatrick & McGraw reference only provided a summary of
663  the survey program and some discussion. J. D. Kirkpatrick (2004, private
663  communication) kindly provided a finding chart for the white dwarf.
663  However, even this could not be verified. Ensuing discussion resulted in
663  the discovery that the equinox implied by the CCD transit instrument (CTI)
663  survey name CTI 054438.5+280224 and reported as 1950 in the McCook & Sion
663  catalog (Cat. <III/210>) of white dwarfs was not 1950. It was instead
663  1987.5. Once the position was precessed to J2000.0, the discovery finding
663  chart was verified and the white dwarf was confirmed to be identical to the
663  very blue source Lanning 663. The J2000.0 coordinates measured in this
663  survey analysis are listed in lanning.dat table.
663  J. D. Kirkpatrick also provided a copy of the spectrum of this source,
663  obtained as part of the CTI survey, and has very kindly given his
663  permission to include that spectrum in this work. The spectrum (Fig. 12)
663  clearly exhibits the characteristics of a DA white dwarf with a strong
663  blue continuum and the typical broad hydrogen absorption lines.
666 The U Gem-type variable UZ Ser was found to be coincident with the source
666  Lanning 666. UZ Ser is noted to have a range in V magnitude from 11.9 to
666  16.0, with a period of 0.17 days (Downes, 1986ApJS...61..569D). The
666  variable was estimated at m_B_=16.5 and U-B=-0.3 on the Sandage two-color
666  plate. The times of observation for the source on this plate were
666  JD2440412.79201 (UV image) and JD2440412.76667 (B image). The values of
666  proper motion included in lanning.dat table suggest substantial motion for
666  this source, with pm_RA_=88mas/yr and pm_DE_=-46mas/yr. However, there
666  also appears to be some confusion of sources in the USNO-B catalog, perhaps
666  due to the different epochs of plates scanned. McCook & Sion (<III/210>)
666  list the proper motion of this source as ~253mas/yr.