Table 1
Finding List of UV Sources
Source No. RA(J2000) DEC(J2000) m(B) U-B Notes
Lanning 83 20 11 15.0 +49 10 37.0 20.5 -1.3
Lanning 84 20 12 27.3 +47 29 20.7 12 -0.8
Lanning 85 20 14 57.6 +45 52 20.4 18 -0.7
Lanning 86 20 14 51.2 +49 13 03.7 19 -1.1
Lanning 87 20 16 25.0 +49 52 07.7 21 strong? dense core in UV
Lanning 88 20 17 21.9 +45 52 50.5 20.5 -1.2
Lanning 89 20 17 55.0 +47 51 43.5 20.5 -1.4
Lanning 90 20 23 30.5 +46 31 29.7 19 -1.2 =V1776 Cyg
Lanning 91 20 24 35.2 +45 05 28.7 18.5 -1.0 no emission (see
text)
Lanning 92 20 27 58.6 +47 14 50.6 19 -0.9
Lanning 93 20 29 20.2 +46 39 59.2 10.5 -0.9 LSIII 46 -7 =
BD+46 2948
Lanning 94 20 32 28.9 +48 01 48.1 19 -0.6
Lanning 95 20 34 54.7 +47 23 02.6 20.5 -1.0
Lanning 96 20 40 36.9 +55 26 47.5 21 -0.3
Lanning 97 20 40 45.1 +53 03 46.1 20.5 -0.7
Lanning 98 20 42 20.0 +51 42 14.4 20.5 -0.5
Lanning 99 20 43 48.1 +53 58 14.0 21 -0.8
Lanning 100 20 43 51.7 +53 13 25.8 21.5 -0.9 very near plate
limit in B
Lanning 101 20 42 51.2 +47 09 06.8 20.5 -1.0
Lanning 102 20 46 00.1 +55 04 14.7 21 -1.0
Lanning 103 20 43 31.6 +47 26 00.4 10.5 -0.8 LSIII 47 -13 =
BD+46 3023
Lanning 104 20 46 56.5 +55 21 20.7 21 -0.6
Lanning 105 20 45 33.9 +48 31 43.2 16 -0.9
Lanning 106 20 46 07.9 +46 36 05.1 13 -0.8 narrow abs. (see
text)
Lanning 107 20 47 17.8 +45 10 03.7 10 -0.8
Lanning 108 20 54 12.3 +55 04 09.1 20 -0.5
Lanning 109 20 55 21.0 +50 14 07.4 21 -1.0
Lanning 110 20 58 19.2 +50 12 07.2 15 -0.6
Lanning 111 21 00 32.8 +54 32 35.5 14 -0.6 central star of
PK93+5 1
Lanning 112 21 00 31.4 +50 51 19.2 15.5 -0.4 GD393
Lanning 113 21 02 46.4 +55 30 18.5 20.5 -1.4
Lanning 114 21 01 54.5 +51 38 56.6 21 -0.6
Lanning 115 21 04 35.3 +55 57 39.4 21 -1.2
Lanning 116 21 04 48.8 +55 35 15.9 8 -0.2 HD201033
Lanning 117 21 03 44.9 +50 02 29.2 18.5 -0.5
Lanning 118 21 06 20.7 +50 05 38.0 21.5 -0.5 near plate limit
Lanning 119 21 12 23.0 +55 55 24.6 20.5 -0.5
Lanning 120 21 14 05.7 +49 51 17.0 19 moderate (see text)
Lanning 121 21 17 17.7 +50 44 06.0 15 -0.6
Lanning 122 21 18 56.4 +54 12 38.5 13 -0.6 Lanning 51
(G231-40)
Lanning 123 23 26 58.9 +71 00 19.1 20.5 -1.5
Lanning 124 23 31 53.1 +70 22 10.8 20.5 -0.8 central star of
PK116+8 1
Lanning 125 23 35 56.3 +71 13 11.3 20 -0.6
Lanning 126 23 39 10.5 +66 51 45.6 19.5 -0.8
Lanning 127 23 39 45.5 +67 46 54.9 20.5 -1.0
Lanning 128 23 47 07.2 +65 34 18.7 20 -0.6
Lanning 129 23 50 53.7 +69 24 37.6 19.5 -0.5
Lanning 130 23 59 55.6 +65 12 59.7 21.5 ... re-examination of
plate suggests
overlapping image.
Not UV.
Lanning 131 00 01 50.6 +66 07 01.4 21.5 -0.3
Lanning 132 00 04 45.1 +71 30 31.2 21.5 -0.8
Lanning 133 00 12 24.8 +65 28 53.6 21 -0.6
Lanning 134 00 21 30.4 +68 15 15.8 20.5 -0.4 = Lanning 1
Lanning 135 20 47 57.5 +48 42 12.5 19.5 -0.8
III. THE FINDING CHARTS
Finding charts are given in Figures 1-6 for all the sources listed in Table 1. For the purposes of any subsequent surveys of these sources, it was deemed appropriate to provide all relevant information and charts in a self-contained reference. All the charts have been reproduced from the STScI GASP system. Images retrieved from the guide star image archive were transferred to a Celco film writer and reproduced by the on-site photolab. The scale is approximately 11 arcsecond/mm, with a full field of 8 arcminutes on a side. Identified sources are centered in a 20 arcsec circle. The circle for some charts, however, has been increased due to the brighter magnitude of the sources, or in order to prevent obstructing a nearby field star which may need to be used for identification. For UV sources in fields which contain close companions, or which may be merged with other field stars, an arrow has been overlaid to point to the UV source. In all charts north is up and east is to the left.
IV. DISCUSSION
Among the sources listed in Table 1, a number warrant special mention. Also, in 1982, a spectroscopic survey of a few of the stars listed here was undertaken by Allen Shafter with charts provided by the author. This survey was accomplished using the Mt. Lemmon 1.5m telescope with the Image Dissecting Scanner (IDS) attached to a low resolution spectrograph yielding ~11 A resolution. Followup observations of Lanning 90 were completed with the Lick Observatory Shane 3-meter and an IDS. Information noted by Shafter (private communiation) on Lanning 90, 91, and 106 is provided below. No spectra were recorded for later analysis. Other sources from this survey are also discussed.
-
Lanning 85: Although a much fainter companion is slightly overlapping this
image to the southwest, the identification of this object as a
marginal to moderate UV source is firm.
Lanning 87: This source is the center star of a close, nearly overlapping, string of three stars. The UV image appears to be very strong with a dense core, but the proximity of the other stars and possible offset in orientation make confirmation questionable. No other images on the Palomar Sky Survey prints suggest the presence of any overlapping images which would contribute to the apparent UV excess.
Lanning 90: During the initial quick-look survey of selected UV-bright sources from this survey by Shafter (private communication), this 17th magnitude source was noted to exhibit the spectrum of a cataclysmic variable, as was later reported by Shafter, Lanning, and Ulrich (1983). The authors presented evidence suggesting the system was an eclipsing CV. Garnavich, et al. (1990), determined that Lanning 90 (V1776 Cyg) is indeed eclipsing. An orbital period of 3h57m was obtained, and variations in the shape of the eclipse were detected along with brightness changes of more than a magnitude in less than one day outside eclipse. A re-examination of the original two-color plate suggests the blue magnitude of this UV source was approximately 19 at the time of detection.
Lanning 91: No emission was detected. The U-B noted in Table 1 suggests this is a very blue source.
Lanning 106: This source was noted by Shafter to be of ~13-14th magnitude. Narrow absorption lines were detected.
Lanning 116: Normally sources brighter than 10th magnitude were ignored due to saturation of the image and merging of the UV and B images. Magnitude and color estimates are very difficult to establish. The source was noted because it had appeared at first inspection to be in the marginal range with a U-B ~ -0.2. The magnitudes noted in the SIMBAD database for this 8th magnitude star, however, indicate a U-B = +0.15 suggesting the source may be variable.
Lanning 118: Although this source is near the plate limit, the object appears noticeably blue.
Lanning 120: This source is overlapped with another star which is slightly fainter. However, the orientation between the two is such that the blue nature of the UV source seems evident with a moderate strength, i.e. U-B ~ -0.8. A quantitative value for this source, however, cannot accurately be provided.
Lanning 122: The plate examined in this survey was an overlapping field with a plate in Paper I. The 12.5 magnitude source is coincident with Lanning 51 and was also detected by Downes (1986), KPD2117+5400. Although placed into the marginal detection category with a U-B of only ~ -0.4 in this survey, the star has been previously identified as the DA white dwarf G231-40 (Lanning 1973).
Lanning 134: The plate on which this source was detected is also an overlapping plate from Paper I. This ~18th magnitude source is coincident with Lanning 1 and appeared in Paper I to be a very strong UV source. On the plate examined for this segment of the survey, the source detection appears marginal with a U-B estimate of only ~ -0.4.
V. PREVIOUSLY IDENTIFIED SOURCES
Since publication of Paper I , several sources have have been investigated independently or have been been noted in more recent references. One of these, Lanning 15, was originally noted in Paper I as a very blue source and coincident with the object associated with Bologna radio source B2 1656+34 (Grueff and Vigotti 1972). The source was first noted to be a confirmed QSO by Pauliny-Toth, et al. (1972). Upon re-examination of associated plates in the same region from the Case Low-Dispersion Northern Sky Survey (Pesch and Sanduleak 1982), Pesch also indicated the source had been logged as a QSO (private communication). The category was listed as IIe QSO, where II signifies blue and/or emission-line stellar objects.
A re-examination of other Lanning objects in the region by Pesch (private communication) indicated that Lanning 41 was noted as a possible QSO with category IIe. A single emission feature was measured at ~3740 A. Lanning 42 was not originally logged as part of the Case survey. It was noted as rather faint upon re-examination, but a category II has been assigned. Lanning 77 was also not picked up by the Case survey originally, but has subsequently been designated as a very good candidate for category II. The source contains no emission features. Updated positions for these sources have been provided in Table 2. The original estimated blue magnitudes from Paper I are also noted. All the sources noted in this section were located in the vicinity of the x-ray/optical binary HZ Her.
Table 2
Previously Identified Sources - Updated Positions
Source No. RA(J2000) DEC(J2000) m(B) Notes (see text)
Lanning 41 17 01 24.8 +35 11 57.1 20: Possible QSO; Category IIe;
Emission feature at 3740 A
Lanning 42 17 09 58.8 +34 21 30.6 20: Category II. Very Faint.
Lanning 77 16 56 14.0 +35 10 14.6 19: Noted as good category II.
No emission detected.
Downes, R. A. 1986, ApJS, 61, 569
Garnavich, P. M., Szkody, P., Mateo, M., Feinswog, L., Booth, J., Goodrich, B., Miller, H. R., Carini, M. T., and Wilson, J. W. 1990, ApJ, 365, 696
Grueff, G., and Vigotti, M. 1972, A&AS 6, 1 (No. 1)
Hoag, A. A., Johnson, H. L., Iriate, B., Mitchell, R. I., Hallman, K. L., and Sharpless, S. 1961, Pub. U.S. Naval Obs. 17 (part 7), 345 (2nd series)
Haro, G. and Herbig, G.H. 1955, Bol. Obs. Tonantzintla y Tacubaya, 12, 33
Lanning, H. H. 1973, PASP, 85, 70
Pauliny-Toth, I.I.K., Kellerman, K.I., Davis, M.M., Fomalont, E.B., and Shaffer, D.B. 1972, AJ, 77, 265
Pesch, P. and Sanduleak, N. 1982, ApJS, 51, 171
Russell, J.L., Lasker, B.M., McLean, B.J., Sturch, C.R., and Jenkner, H. 1990, AJ, 99, 2059
Shafter, A. W., Lanning, H. H., and Ulrich, R. K. 1983, PASP, 95, 206
UV Survey Intro Page