Baltic Astronomy, vol. 2, 171-213, 1993.

INTERSTELLAR EXTINCTION IN THE VICINITY OF THE NORTH AMERICA AND PELICAN NEBULAE. II.

V. Straizys1, A. Kazlauskas1, V. Vansevicius2 and K. Cernis1 1 Institute of Theoretical Physics and Astronomy, Gostauto 12, Vilnius 2600, Lithuania 2 National Astronomical Observatory, Mitaka, Tokyo 181, Japan* Received October 5, 1993.

Abstract. The results of photoelectric photometry of 564 stars in the Vilnius seven-colour system in three areas near the North America and Pelican Nebulae are given. Photometric spectral types, absolute magnitudes, colour excesses, interstellar extinctions and distances of the stars are determined. We find that the dark cloud separating both nebulae is at 580 pc distance. A number of stars immersed into the dark cloud have been found. It seems that the dark cloud extends to south down to 40° declination. The area southwest of α Cygni in the declination zones 42° and 43° is comparatively transparent at least up to 1 kpc. Key words: North America Nebula - Pelican Nebula - interstellai extinction - dark clouds - Vilnius photometric system - classification of stars

1. Introduction

In our previous papers (Straizys et al., 1989a, b) we have start«·

* Visiting astronomer from the Institute of Physics, Gostauto 12, Vtlnin- 2600, Lithuania 172 V. Straizys, A. Kazlauskas, V. Vansevicius and K. Öemis The Vicinity of the North America and Pelican Nebulae 173 the results of photoelectric photometry of 249 stars, their two- dimensional classification, colour excesses, interstellar extinctions and distancies have been given. In the second paper (Straizys et al., 1989b, Paper II) we have investigated interstellar extinction in the area including the North America Nebula., the Pelican Nebula, the dark cloud separating both the nebulae (Lynds 935) and the nearby area south of a Cygni. The distance of the dark cloud was found to be 550 pc. and the area west of the Pelican Nebula, and south of a Cygni was found to be comparatively transparent at least up to 700 pc. Trying to find more stars embedded into the dark cloud and to investigate the interstellar extinction in the wider area south and west of a Cygni, observations of new stars have been made. They include 212 stars in the area, of the dark cloud and 352 stars in two rectangular areas extending west and south the area, investigated in Papers I and II. Coordinate limits of all three areas are given in Table 1. Their positions are shown in Fig. 1. The broken lines limit the area investigated in Papers I and II. The BD 40°-41° area, contains the open cluster NGC 6910. The results of photometry of 17 stars in the cluster area were published earlier (Va.nsevicius, 1992). Table 1. Coordinates of the investigated areas

No. Area α(1950) £(1950) Vlim Ν 1. Dark cloud 20h47I?17 - 20h58'.T13 +42°27'- +44°39' 12.5 212 2. BD 40°- 41° 201,15I."2 - 21h03"16 +40°24'- +42°19' 10.0 255 3. BD 42°- 43° 20h14!"8 - 20h35'.n0 +42°22'- +44°14' 10.0 97 2. Observations and results

The observations have been obtained in 1989-1991 with the 1-meter telescope of the Institute of Theoretical Physics and Astro- nomy at the Maidanak Observatory in Uzbekistan. The standard set of filters of the Vilnius photometric system has been used. The observed magnitudes and colour indices were transformed outside the atmosphere by the Nikonov's method modified by Zdanavicius

Fig. 1. Boundaries of the investigated areas: (1) the dark cloud area, (2) the BD 40°- 41° area, (3) the BD 42°- 43°area, (4) the area investigated in Papers I and II. The map is from Tirion et al. (1987). The coordinates are for 2000.0. 174 V. Straizys, A. Kazlauskas, V. Vansevicius and K. Öemis

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Fig. 2. The map of the dark cloud area.

(1975). The standard star HD 197037 = BD+41°3845 (F8 V, V = 6.79), situated in the same area, has been used. Its a(1950) = 20h37m45s and <5(1950) = +42°04.'3. Magnitude V and colour in- dices of this star in the Vilnius system are published in Paper I. Transformation equations from the instrumental to the standard sys- tem were based on observations of 15 stars of luminosity classes V The Vicinity of the North America and Pelican Nebulae 175 and III of different spectral types from the Cygnus Standard Region (Zdanavicius and Cerniene, 1985). The results of photometry of 564 stars are presented in Tables 2, 3 and 4. Table 2 gives BD numbers, numbers from Metik (1960), equatorial coordinates, spectral types from literature and those ob- tained in this paper, V magnitudes* and colour indices U-P, P-X, X-Y, Y-Z, Z-V and V-S in the Vilnius system, η is the number of independent observations. Tables 3 and 4 give BD and HD numbers, other columns are the same as in Table 2. Coordinates of the stars were taken from the SAO or AGK3 catalogues or have been mea- sured from copies of the Papadopoulos and Scovil (1980) atlas with the accuracy of Is in a and O.'l in 6. Mean square error σ of one pho- tometric observation is of the order of ±0.01 mag. Stars of the dark cloud are identified in Fig. 2. In the chart, the stars investigated in Paper I are not numerated. The remarks at the end of the tables give information on du- plicity, variability and the classification difficulties. For the binaries with separation of their components < 5', both components were measured together. For the wider binaries, the information is given, how they are measured, separately or together.

3. Photometric classification of stars and their interstellar extinction

Spectral classes, luminosity classes and absolute magnitudes of the stars, given in Tables 5-7, have been determined from the pho- tometric data by three different methods: (1) the reddening-free diagrams QUPY, QPYV', QUPY, QXYV', QUXY, QUPYV, QUPY, Qxzs and Qxzs·, QXYZ calibrated in terms of spectral class and absolute magnitude by Straizys et al. (1982); (2) the OQ method based on matching of ten different reddening- free Q-parameters of a program star to those of about 7000 standard stars of different spectral and luminosity classes. (3) the semi-automatic classification with a program CLASS (Vansevicius and Bridzius, 1993).

* The V magnitude of the Vilnius system is a medium band analogue of the V magnitude of the UBV system (see Straizys, 1992). Both V magnitudes coincide within 0.01 mag for normal O-B-A—F-G-K stars. For M, S, R and N-type stars, as well as for stars with emission spectra differences of both magnitudes can be significant. 176 V. Straizys, A. Kazlauskas, V. Vansevicius and K. Öernis

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Remarks to Table 3. 1. +40°4103, visual binary, ADS 13672 AB, sep=2"7, Δπι=2.5, 09+B2. 2. +40M115, elliptical variable V470 Cyg, SB, B2+B2. If both compo- nents are of the same absolute magnitude their apparent magnitudes are 7.66 and the distance 432 pc. 7. +40°4124, Herbig Ae/Be star. II. +40M136, SB, G5 III+A. 37-38. +40M197, visual binary, BDS 10274, sep=14'/0, measured sepa- rately. 49. +40°4220, V729 Cyg, eclipsing binary, sep=l'/5, Am«4.0. 52. +40°4227, visual binary ADS 14000 AB, sep=9'/6, Am« 1.0. 69. +40°4266, visual binary ADS 14126 AB, sep=0'/6, Bp (Jaschek and Egret, 1982). 108. +40°4354, visual binary ADS 14413 AB, sep=5'/8, Δηι«4.0. III. +40M358, visual binary ADS 14435 AB, sep=670, Am«3.5. 115. +40°4372, detemination of My uncertain, Ay ss 1.3 mag. 125. +40M393, suspected variable YZ Cyg. 127. +40M399, visual binary ADS 14605 AB, sep=678, Am«3.5. 152. +41°3728, visual binary. 154. +41°3731, Herbig Ae/Be star. 158. +41°3737, visual binary ADS 13832 AB, sep=7'/3, Am«5.0, measured together. 165. +41°3752, visual binary ADS 13869 AB, sep = l'/4, Am»0.2. 184. +41°3796, visual binary ADS 13985 AB, sep=l"5, Am«0.8. 185. +41°3799, SB. 193. +41°3815, photometrically peculiar, Ay «2.2 mag. 201. +41°3844, visual binary ADS 14130 AB, sep=0'/8, Am«2.0. 215. +41°3884A, visual binary ADS 14295 AC, sep=5'.'6, Am«3.5. 216. +41°3884B, visual binary ADS 14295 B, about 10" from component A. 217. +41°3889, visual binary ADS 14306 AB, sep=(V/4, Am«1.0. 218. +41°3890, visual binary ADS 14308 AB, sep=4'.'5, Am«3.5. 232. +41°3932, visual binary ADS 14432 AB, sep=2"9, Äm»2.5. 244. +41°3962, also possible classification as sdF5. 245. +41°3962a, a star ~30" from the BD+41°3962 star. 251. +41°3986, visual binary BDS 10719 BC, sep=773, Am«4.0 . 252. +41°3987, visual binary component BDS 10719 A. 194 V. Straizys, A. Kazlauskas, V. Vansevicius and K. Gernis

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Table 5. Results of quantification, extinction and distance determination in the dark cloud area.

No. Sp. Mv V r 1. F5 V +3.6: 11.24 0.23 300 3. F6 V +3.7: 10.36 0.15 200 4. F5 V +3.6: 11.12 0.18 290 5. GO IV +3.0 11.28 0.50 360 6. K0 III + 1.2 10.93 0.14 830 7. A6 V +2.2 9.79 0.74 230 8. F9 V +4.3: 11.04 0.00 220 9. A7 V +3.0 10.91 0.72 270 10. F0 V +2.8: 11.66 0.36 500 11. K1 III -0.6 10.11 0.00 1390 13. F5 V +3.6: 11.45 0.05 360 15. K0 IV +2.8 10.82 0.04 390 16. F9 V +4.3: 11.80 0.09 300 17. A7 V +2.8 11.59 0.81 390 18. K1 III +0.7 9.53 0.23 530 19. GO IV-V +3.7 10.89 0.09 260 20. A9 V +3.0 10.29 0.20 260 21. A5 V +2.1 10.41 0.63 340 22. K0.5 III +1.4 10.00 0.18 480 23. F6 V +3.7: 11.01 0.29 250 24. F5 V +3.6: 11.81 0.36 370 25. A6 V +2.3 10.83 0.52 400 26. F8 IV-V +3.5: 11.33 0.34 320 27. GO V +4.4: 11.18 0.04 220 28. K1.5 III + 1.7 10.45 0.63 420 29. G9 V +5.8 11.94: 0.25 151 30. K0 III-IV +1.5 10.55 0.65 480 31. F5 V +3.6: 10.74 0.09 260 32. F7 V +4.0 12.40 0.39 400 33. GO IV-V +3.5 12.66 0.27 600 34. F0 V +3.0 10.85 0.63 280 36. GO V +4.4 12.66 0.22 400 38. A7 V +3.0 11.76 0.45 460 39. K0 in +0.9 9.42 0.13 480 40. F5 V +3.6 11.42 0.23 330 41. F7 V +4.0 12.43 0.12 460 42. K2.5 V +6.5 12.58 0.14 154 43. F4 V +3.5: 11.45 0.31 340 44. B6:V +0.3: 11.02 2.47 450 45. F0 V +2.8 11.78 0.54 490 46. Al V + 1.1: 10.81 0.63 650 47. F8 V +4.1 12.05 0.18 360 48. F8 V +3.8 11.21 0.18 280 49. F2 V +3.1 11.05 0.45 320 50. G5 V +5.1: 10.42 0.45 94 The Vicinity of the North America and Pelican Nebulae 199

Table 5 (continued)

No. Sp. Mv V Av r 51. G2 IV +3.5 10.80 0.04 280 52. B2 V -1.6 11.18 3.82 620 54. F5 V +3.6 11.68 0.50 330 55. K2 IV +3.6 12.25 0.72 390 57. :B2 V -2.0 12.49 4.95 810: 58. F8 V +3.8 11.29 0.31 270 59. F8 V +3.8 12.62 0.32 500 60. G5 V +5.1 12.66 0.23 290 61. A6 V +2.1 10.13 0.29 350 62. F6 V +3.7 11.56 0.38 310 63. F8 V +4.1 11.68 0.23 300 64. F7 V +4.0 11.32 0.00 290 65. F2 V +3.1 10.51 0.18 280 66. Gl III-IV +2.0 11.91 0.00 960 67. K0 III +0.9 9.49 0.18 480 68. F7 V +4.0 10.94 0.03 240 69. K1 III -0.3 9.58 0.99 600 70. K0 III +0.7 10.34 0.27 750 71. F5 V +3.6 12.48 0.45 490 72. K0 III-IV +2.0 12.21 1.19 640 73. F6 V: +3.7 12.27 0.11 490 74. F5 V +3.6 12.04 0.18 450 75. F5 IV +2.5 11.46 0.36 520 76. F5 V +3.6 11.96 0.27 410 77. F7 V +4.0 12.09 0.08 400 78. F5 V +3.6 11.07 0.14 290 79. GO IV-V +3.5 12.63 0.63 500 80. A7 V +3.0 11.40 0.49 380 81. G8 IV-V +4.0 10.61 0.36 178 82. F8 V +4.1 11.86 0.09 340 85. F5:V +3.5 10.66 0.00 270 87. F5 V +3.6 11.67 0.27 360 88. G3 IV +3.0 10.68 0.00 340 90. F5 V +3.6 11.93 0.36 390 92. GO V +4.4 13.24 0.36 500 93. GO IV-V +3.3 12.11 0.31 500 97. F6:V +3.7 12.87 0.38: 570: 98. Gl V +4.6 11.08 0.16 184 99. A9 V +3.0 11.02 0.33 350 100. G9.5 III-IV +2.0 11.21 0.00 700 101. F5 V +3.6 11.50 0.27 340 102. G2 V +4.7 11.64 0.00 240 104. A9 V +3.0 11.53 0.78 350 105. F5 V +3.6 13.09 0.72 570 106. KOIV-V +4.1 9.92 0.18 134 200 V. Straizys, A. Kazlauskas, V. Vansevicius and K. Öernis

Table 5 (continued)

No. Sp. Mv V Av r 107. GO V +4.5 13.28 0.18 520 108. F8 V +4.1 10.60 0.00 200 109. F2 V +3.1 11.60 0.22 450 110. A7 V +3.0 11.36 0.54 370 111. F5 IV-V +3.1 11.46 0.09 450 112. F5 V +3.6 11.31 0.00 350 113. GO V +4.4 12.26 0.36 320 114. F5 V +3.6 11.80 0.00 440 115. F0 V +2.8 10.88 0.32 360 116. F2 V +3.1 12.34 0.95 460 117. AO V +0.8 9.76 0.36 520 118. K0 III +0.8 10.37 0.50 650 119. G9 IV-V +4.2 12.28 0.38 350 120. K0 III-IV +2.0 10.54 0.29 450 124. F6 III +0.8 12.56 0.57 1730 125. A5 V +2.2 11.69 0.58 600 127. GO V +4.0 12.00 0.09 380 129. GO IV +3.2 11.77 0.23 470 130. FO V +2.9 11.61 1.04 340 131. F8 V +4.0 12.15 0.04 420 132. F7 V +3.8 10.79 0.00 250 133. F2 V +3.1 10.97 0.23 340 134. G5 V +5.1 11.66 0.36 174 135. A6 V +2.5 11.33 0.34 500 136. F5 V +3.6 10.60 0.09 240 138. F5 V +3.6 10.72 0.09 250 139. F8 V +4.1 11.39 0.00 290 140. G7 V +5.5 11.24 0.28 124 142. F2 V +3.1 11.93 0.54 450 143. F8 IV +3.3 11.23 0.18 350 145. F9 V +4.2 12.34 0.36 360 146. A7 V +2.9 9.87 0.58 190 147. F8 V +4.1 12.17 0.14 390 149. AO V +1.5 10.87 0.67 550 151. G5 V +5.1 11.29 0.36 146 152. GO IV +3.2 11.14 0.54 300 153. F8 V +4.1 11.63 0.00 320 154. KO III +0.8 9.12 0.04 450 155. F9 V +4.3 10.71 0.00 191 156. Gl IV-V +3.5 12.69 0.20 630 157. FO V +2.8 10.72 0.59 290 158. F5 IV-V +3.0 12.23 0.23 630 159. A4 V +1.7 10.76 0.72 470 160. A9 V +2.7 12.02 0.73 520 161. GO V +4.4 12.64 0.36 380 The Vicinity of the North America and Pelican Nebulae 201

Table 5 (continued)

No. Sp. Mv V Av r 162. F6 V +3.7 11.94 0.11 420 164. A4 V +1.7 11.08 0.54 590 166. F2 III +1.8 10.50 0.76 390 167. F3 V +3.2 11.86 0.27 480 168. K0.5 IV +2.7 10.39 0.00 350 169. F3 V +3.2 11.84 0.31 460 170. A7 V +2.9 11.63 0.54 430 171. F8 IV +3.0 11.77 0.72 410 172. F5 V +3.6 11.39 0.27 320 174. A8 II -3.0 10.92 3.22 1380 175. G5 V +5.1 12.70 0.14 310 176. Gl V +4.5 13.17 0.02 540 177. F5 V +3.6 10.13 0.09 194 178. AO V +1.6 12.28 2.29 480 179. K4 III +0.8 10.21 1.26 430 180. K0.5 III +0.8 11.23 0.23 1100 181. G5 V +5.1 13.18 0.36 350 182. A5 V +2.2 10.55 0.18 430 183. Gl V +4.5 12.16 0.11 320 185. F5 V +3.6 11.85 0.72 320 186. A9 V +2.7 10.47 0.78 250 187. F5 V +3.6 12.79 0.59 530 189. F7 V +3.9 10.58 0.44 177 190. A6 V +2.1 12.81 1.15 820 191. B9 IV +0.2 10.04 1.08 560 192. F5 V +3.6 11.65 0.50 320 193. G3 IV +3.6 11.98 0.39 400 194. A3 V +1.9 11.37 0.76 550 195. GO V +4.4 9.87 0.23 112 196. A2 V +1.5 11.31 1.22 520 198. B9 III -0.5 11.34 2.79 650 199. A8 V +2.5 11.52 0.61 480 200. F0 V +2.8 11.68 0.77 420 201. F5 V +3.6 11.39 0.45 290 202. F8 V +4.1 11.36 0.04 280 203. A4 V + 1.7 10.58 0.86 400 204. F8 V +4.1 12.50 0.23 430 205. A7 V +2.5 11.90 1.08 460 207. F5 III +1.2 12.42 1.76 780 208. G3 V +4.8 11.96 0.30 240 209. A5 V +1.7 12.02 1.13 690 210. GO V +4.4 10.82 0.04 189 211. F7 V +3.9 11.74 0.21 340 212. F6 V +3.7 10.29 0.15 194 202 V. Straizys, A. Kazlauskas, V. Vansevicius and K. Öernis

Table β. Results of quantification, extinction and distance determination in the BD 40° - 41° area.

No. BD Sp. Mv V Av r

3. +40° 4116 B9 IV 0.0 7.76 0.31 310 4. +40° 4119 B2 V -1.7: 8.85 1.98 520: 5. +40° 4120 A8.5 V +2.4 8.91 0.22 180 6. +40° 4121 Al V + 1.1: 7.15 0.09 160 8. +40° 4129 B9.5 II-III -2.1 7.96 0.58: 790 9. +40° 4132 B0 V -4.0: 8.51 3.10 760 10. +40° 4135 K4 III +0.6 8.93 0.58 350 12. +40° 4137 B0.5 III -4.2: 8.24 1.48 1560 13. +40° 4139 B1.5 IV -3.5: 8.10 1.12 1250 14. +40° 4141 K5 III +0.3 5.94 0.45 110 15. +40° 4144 Kl.5 III +0.6 7.38 0.27 200 16. +40° 4147 06 III -5.9: 8.51 3.87 1280: 17. +40° 4150 B2 Ia -7.2: 7.03 3.78 1230: 18. +40° 4151 K0.5 III + 1.2 9.42 0.14 410 19. +40° 4152 AO V +0.8: 9.60 0.22 520 20. +40° 4155 K2 III +0.2 8.28 0.22 370 21. +40° 4157 A0.5 V + 1.0: 9.30 0.18 420 22. +40° 4160 A7 V +2.9 8.53 0.36 • 115 23. +40° 4163 B7.5 IV -0.5 8.70 0.54 540 24. +40° 4164 B2 II -4.8: 7.69 1.58 1520 25. +40° 4165 B0.5 Ia -7.2: 7.49 3.78 1520 26. +40° 4171 G7 IV +3.2 8.91 0.32 120 27. +40° 4176 A2 V + 1.3: 9.13 0.18 340 28. +40° 4177 G7 V +5.3 8.95 0.00 54 29. +40° 4178 A2 V + 1.8 8.73 0.40 200 30. +40° 4181 A3 V + 1.5: 9.10 0.09 320 31. +40° 4183 B9.5 III -0.2 7.97 0.18 400 32. +40° 4186 Al V + 1.7: 9.01 0.22 260 33. +40° 4187 07 -5.2: 8.76 3.78 1090: 34. +40° 4188 Al.5 V + 1.3 7.92 0.14 200 35. +40° 4194 AO V + 1.3 8.84 0.18 300 36. +40° 4195 Gl V +4.5: 10.02 0.09 120 37. +40° 4197A A7 V +3.0 9.17 0.32 150 38. +40° 4197B G9 III-IV +2.0 9.96 0.32: 340 39. +40° 4199 A2 V + 1.3: 9.41 0.18 380 40 +40° 4200 A7 V +2.3: 9.45 0.32 230 41. +40° 4201 A4 V +2.1: 9.63 0.00 320 43. +40° 4205 B7.5 V +0.4 7.97 0.18 300 44. +40° 4209 B8.5 V + 1.0 8.76 0.18 330 45. +40° 4211 G9 III + 1.0 7.44 0.18 180 46. +40° 4213 F5 V +3.6: 9.11 0.00 125 47. +40° 4214 F4 V +3 2 8.56 0.18 110 48. +40° 4218 B8 V +0 7 9.64 0.36 520 50. +40° 4225 F8 V +4.1: 7.24 0.00 42 51. +40° 4226 B9 V +0.7 8.22 0.14 300 53. +40° 4228 K0 III + 1.3 9.24 0.14 360 The Vicinity of the North America and Pelican Nebulae 203

Table 6 (continued)

No. BD Sp Mv V Av r

54. +40° 4229 F2 V +3.2 9.44 0.28 155 55. +40° 4230 K0 IV +3.1 8.63 0.09 120 56. +40° 4231 G8 III-IV +1.9 9.51 0.32 290 57. +40° 4236 B8 V +0.8 8.71 0.09 370 58. +40° 4239 Al V + 1.7: 8.94 0.22 250 59. +40° 4240 K4 III +0.5 6.66 0.22 155 60. +40° 4246 A4 V +1.8: 7.87 0.09 155 61. +40° 4247 K0.5 III +0.6 9.77 0.14 640 62. +40° 4248 K0 III +0.6 9.30 0.14 520 63. +40° 4250 Al V +1.7: 9.28 0.00 330 64. +40° 4251 F6 V +3.9: 7.79 0.00 60 65. +40° 4255 A5 V +2.4 9.13 0.14 210 66. +40° 4257 G7 IV +2.7 8.98 0.32 155 67. +40° 4260 F9 V +4.3: 9.70 0.22 110 68. +40° 4261 F5 V +3.6: 9.38 0.00 145 70. +40° 4267 B9.5 V + 1.3 8.74 0.09 300 71. +40° 4274 A5 V +2.7 9.74 0.32 220 72. +40° 4275 G9 IV +2.5 9.63 0.40 220 73. +40° 4276 B9 V +0.6 6.98 0.09 145 74. +40° 4277 A4 V +2.1 9.83 0.09 340 75. +40° 4279 AO V + 1.0 9.24 0.32 380 76. +40° 4282 A7 V +2.4 9.58 0.45 220 77. +40° 4283 AO IV +0.2 9.28 0.18 600 78. +40° 4286 G7 III +0.3 9.10 0.54 450 79. +40° 4289 A9 III + 1.6 8.12 0.09 195 80. +40° 4290 B9 V +0.8 8.52 0.12 330 82. +40° 4297 F8 IV-V +3.6: 9.93 0.00 185 83. +40° 4300 A4 V +2.3 9.97 0.08 330 84. +40° 4301 AO.5 V +0.7 9.40 0.16 510 85. +40° 4305 A7 V +3.0 9.61 0.54 165 86. +40° 431OA K2 III +0.7 9.59 0.50 480 87. +40° 4310B G3 V +5.0 11.80 0.04 225 88. +40° 4313 Kl III + 1.0 9.76 0.27 500 89. +40° 4322 B8 V 0.0 9.77 0.54 700 90. +40° 4324 Kl III + 1.2 8.94 0.00 350 91. +40° 4325 A5 V +2.3 10.38 0.09 400 92. +40° 4328 F8 IV +3.0 7.72 0.18 81 93. +40° 4329 F5 V +3.6: 8.41 0.00 92 94. +40° 4331 A4 III-IV + 1.1 8.90 0.24 325 95. +40° 4333 A8 V +3.0 9.42 0.40 160 96. +40° 4335 G8 V +5.5 9.96 0.14 73 97. +40° 4336 KO III +0.8 8.89 0.18 380 99. +40° 4343 Al.5 V +1.7: 9.38 0.27 300 100. +40° 4345 Al V + 1.7: 10.00 0.50 360 101. +40° 4346 B5.5 V 0.0 7.56 0.18 300 102. +40° 4347 A3 V +2.2 9.59 0.13 280 204 V. Straizys, A. Kazlauskas, V. Vansevicius and K. Cemis

Table 6 (continued)

No. BD Sp Mv V Av r

IU3. +40° 4349 K0 III + 1.1 8.61 0.18 290 104. +40° 4348 A7 IV + 1.5 8.75 0.31 245 105. +40° 4350 A2 V + 1.8: 8.38 0.40 170 106. +40° 4352 K1.5 III + 1.3 9.44 0.09 410 108. +40° 4354 B7 III -1.5 6.66 0.18 400 109. +40° 4356 Al.5 V + 1.7: 8.86 0.32 230 110. +40° 4357 F5 V +3.6: 9.25: 0.00 135 111. +40° 4358 F5 III +2.1 9.77 0.45 280 112. +40° 4362 AO.5 V +2.0 8.96 0.05 240 113. +40° 4363 A6 IV + 1.7 8.63 0.36 210 114. +40° 4369 A3 V + 1.5: 8.48 0.14 230 116. +40° 4373 K5:III: +0.1 7.11 0.37 210 117. +40° 4374 F2 V +3.1 7.97 0.00 95 118. +40° 4378 K0 III +0.3 6.99 0.18 200 119. +40° 4380 GO V +4.4: 8.90 0.00 79 121. +40° 4382 A3 V +2.0 8.70 0.04 215 122. +40° 4385 G8 III + 1.0 9.03 0.28 355 123. +40° 4389 F6 V +3.8: 7.15 0.00 47 124. +40° 4391 G9 III + 1.4 9.14 0.14 330 125. +40° 4393 B8 V +0.1: 8.55 0.32 420 126. +40° 4397 G8 III -0.4 9.31 0.27 770 128. +40° 4401 AO III -0.1 8.24 0.40 390 129. +40° 4402 K3 III + 1.0 8.89 0.40 315 130. +40° 4403 :F8 V +4.1: 10.78 0.06 210 131. +40° 4404 A6 V + 1.8 9.80 0.49 320 132. +40° 4405 K0 III + 1 1 10.28 0.26 610 133. +40° 4406 A8 V +3.0 10.08 0.18 240 134. +40° 4407 Al V + 1.1: 8.89 0.22 330 135. +41° 3687 K2 IV +2.9 7.93 0.28 89 137. +41° 3691 K0 III 0.0 9.52 0.25 710 138. +41° 3693 B9 IV 0.0 9.06 0.31 560 139. +41° 3700 Al.5 V + 1.2: 9.83 0.40 440 140. +41° 3703 B7.5 III -1.4 8.09 0.45 640 141. +41° 3705 G9 V +5.3 9.91 0.00 84 142. +41° 3707 G8.5 III + 1.8 9.24 0.22 280 143. +41° 3709 A7 V +2.8 9.73 0.40 200 144. +41° 3711 AO V + 1.6: 9.72 0.27 370 145. +41° 3712 B9 V + 1.4 8.28 0.27 210 146. +41° 3715 A7 V +3.0 9.15 0.54 130 147. +41° 3716 B5 V -0.7 9.21 1.35 515 148. +41° 3718 K2 III 0.0 9.40 0.50 600 149. +41° 3720 Al V + 1.7 9.35 0.22 310 150. +41° 3721 A2.5 V + 1.8: 8.49 0.18 200 151. +41° 3725 B8.5 V +0.6 9.19 0.36 440 153. +41° 3729 KO IV +2.7 9.32 0.09 200 154. +41° 3731 B3 V -1.0: 9.84 0.94 950: The Vicinity of the North America and Pelican Nebulae 205

Table 6 (continued)

No. BD Sp Mv V Av r

155. +41° 3732 B9 V + 1.2 9.35 0.27 380 156. +41° 3734 K3 III +1.5 8.96 0.58 240 158. +41° 3737 B3 V -1.0: 9.22 1.08 670 159. +41° 3739 A9 V +2.8 7.81 0.40 84 160. +41° 3742 A6 V +2.3 7.09 0.27 80 161. +41° 3748b F7 V +4.0: 10.73 0.00 220 162. +41° 3748a B8 V +0.7 10.56 0.72 670 163. +41° 3749 A2 V + 1.8: 9.61 0.18 335 164. +41° 3751 F5 V +3.6: 9.22 0.00 135 166. +41° 3754 B6 IV-V -0.7 8.67 0.86 500 167. +41° 3756 B9 IV +0.2 9.32 0.36 560 168. +41° 3757 A4 V + 1.7: 9.04 0.00 290 169. +41° 3758 B2 IV -2.1 7.30 0.76 530 170. +41° 3761 B7 V +0.3 9.19 0.32 520 171. +41° 3764 G5 V +4.9 8.56 0.18 50 172. +41° 3765 BO.5 III -4.7 7.64 1.58 1420 173. +41° 3769 B9.5 V + 1.3 8.81 0.14 300 174. +41° 3770 G3 IV +3.2: 8.00 0.00 91 175. +41° 3773 F5 V +3.6 9.00 0.00 120 176. +41° 3775 K0 III +0.7 8.24 0.00 320 177. +41° 3776 F5:V +3.7: 9.73 0.00 160 178. +41° 3782 K5 III +0.4 9.29 0.90 400 179. +41° 3783 G5 IV-V +4.5 9.64 0.00 105 180. +41° 3789 B9 V +1.3 8.54 0.18 260 181. +41° 3790 B6.5 V -0.4: 9.81 1.26 620 182. +41° 3791 B8 V +0.9 8.89 0.27 350 183. +41° 3792 B8.5 III -1.9 8.67 0.81 890 186. +41° 3800 AO.5 V +0.9: 9.46 0.27 455 187. +41° 3805 K0 III-IV + 1.7 6.51 0.18 84 188. +41° 3809 A9 V +3.0 9.32 0.36 155 189. +41° 3810 Al III -1.2: 10.14 1.26 1040 190. +41° 3811 A4 III-IV +1.0 7.96 0.32 210 191. +41° 3813 A3 V +1.9: 10.21 0.50 360 192. +41° 3814 B6 V 0.0 7.57 0.27 290 194. +41° 3818 G8 III +1.6 6.64 0.09 98 195. +41° 3820 B7 V 0.0 9.27 0.54 560 196. +41° 3823 K2 III +1.5 9.45 0.14 360 197. +41° 3824 Al V +1.5 10.10 0.50 420 199. +41° 3836 K4 II-III -2.0 7.58 1.55 580 200. +41° 3841 B9.5 V +1.2 9.09 0.22 340 202. +41° 3845 F7:V +4.1 6.82 0.00 35 203. +41° 3846 G9 III +1.9 9.36 0.00 310 204. +41° 3853 F9 IV-V +3.5 9.07' 0.18 120 205. +41° 3855 F8 III +2.0 7.94 0.22 140 206. +41° 3856 B6 IV -0.9 5.63 0.22 185 207. +41° 3858 Kl III +1.2 8.72 0.14 300 206 V. Straizys, A. Kazlauskas, V. Vansevicius and K. Cemis

Table 6 (continued)

No. BD Sp Mv V Av r

•208. +41° 3859 GO.5 V +4.5 9.66 0.00 110 209. +41° 3865 K3 III + 1.2 9.43 0.09 425 210. +41° 3868 B7 IV-V -0.4 8.44 0.32 510 211. +41° 3872 K0.5 IV +3.0 8.46 0.09 120 212. +41° 3878 A2 V + 1.8 9.59 0.45 290 '213. +41° 3879 A5 IV + 1.5 9.91 0.27 420 214. +41° 3881 K5 III +0.1 8.60 0.02 490 •215 +41° 3884A B6 V -0.5 7.44 0.32 335 216. +41° 3884B Al V + 1.8 8.97 0.08 245 217. +41° 3889 AOIV-V +0.2 7.52 0.12 275 218. +41° 3890 F5 V: +3.6 9.44 0.00 145 219. +41° 3893 G8.5 III + 1.6 8.07 0.14 185 220. +41° 3894 F4 V +3.5 9.18 0.18 125 221. +41° 3895 GO V +4.5 8.15 0.18 49 222. +41° 3896 B5 III -2.0 9.47 2.55 610 223. +41° 3897 G6 III +0.5 7.40 0.14 225 224. +41° 3901 B8 V +0.4 8.83 0.14 450 225. +41° 3904 A6 V +2.5 9.12 0.28 185 226. +41° 3906 AO V + 1.6 9.54 0.28 340 227. +41° 3913 AO V + 1.6 9.85 0.09 430 228. +41° 3916 Al V + 1.1 7.84 0.09 210 229. +41° 3918 A2 V + 1.7 9.86 0.68 310 230. +41° 3928 B8 V +0.6 9.00 0.58 370 231. +41° 3929 Kl.5 III +0.5 7.48 0.09 240 233. +41° 3933 A6 V +3.0 9.45 0.32 170 234 +41° 3935 Al V + 1.1 9.73 0.18 490 235. +41° 3937 Kl III -0.5 8.96 0.90 520 236. +41° 3940 GO V +4.4 9.81 0.00 120 237. +41° 3941 GO V +4.4 9.20 0.00 91 238. +41° 3943 A3 V + 1.7 7.32 0.14 125 239 +41° 3946 A6 V +2.7 9.09 0.09 180 240. +41° 3949 B6 V +0.4 6.12 0.22 125 241. +41° 3951 F5 la -5.0 8.40 3.20 1100 242. +41° 3955 A2.5 V + 1.4 9.93 0.40 420 243. +41° 3961 A3 V + 1.9 10.03 0.45 340 246. +41° 3963 A2 V + 1.8 9.15 0.18 270 247. +41° 3972 A6 V +2.6 9.02 0.50 155 248. +41° 3973 F5 V +3.6 9.46 0.09 140 249. +41° 3976 F6 V +3.8 8.75 0.00 98 250. +41° 3985 B2 V -1.6 9.07 1.98 550 251. +41° 3986 F6 V +3.7 8.79 0.00 105 252. +41° 3987 F0 IV +2.5 6.32 0.22 52 253. +41° 3991 M3 III +0.5 7.71 0.58: 210: 254. +41° 3993 Kl.5 III +0.8 8.35 0.22 290 255. +41° 3995 K3.5 III +0.6 9.23 0.40 440 The Vicinity of the North America and Pelican Nebulae 207

Table 7. Results of quantification, extinction and distance determination in the BD 42° - 43° area.

No. BD SP My V Αν r

1. +42° 3665 K0 III +1.5 8.51 0.14 240 2. +42° 3666 B9.5 V + 1.0: 8.68 0.11 325 3. +42° 3670 K4 II -2.5: 6.31 0.45 470 4. +42° 3671 G9 III +0.1 9.84 0.07 860 5. +42° 3672 A5 V + 1.9 8.77 0.00 240 6. +42° 3677 K0 III +0.5 9.30 0.04 565 7. +42° 3683 F2 III +2.0: 9.21 0.27 245 9. +42° 3685 B9 V + 1.4: 8.65 0.27 250 10. +42° 3692 B8.5 Ib-II -4.8 8.06 3.33 800 11. +42° 3695 F5 V +3.6: 9.37 0.00 143 12. +42° 3699 AO V +1.2: 9.16 0.22 350 13. +42° 3700 AO V +1.3 9.19 0.13 355 14. +42° 3702 B9 V +0.7 8.65 0.22 350 15. +42° 3703 B2 V -2.5 8.92 2.07 740 16. +42° 3704 B8 V +0.4 8.54 0.31 370 17. +42° 3705 F0 III-IV +2.0 8.77 0.18 210 18. +42° 3706 B9.5 V +1.0 9.67 0.34 460 19. +42° 3714 A8 V +2.5 9.23 0.39 185 20. +42° 3716 K1 III +0.2 8.76 0.45 420 21. +42° 3718 B8 V +0.4 8.73 0.22 420 22. +42° 3719 G7 IV +2,1 9.91 0.41 265 23. +42° 3721 G9 III + 1.0 6.23 0.02 110 24. +42° 3723 F6 V +3.7: 9.51 0.19 133 25. +42° 3724 A2 III 0.0 8.02 0.27 355 26. +42° 3725 K3 III +0.1 8.81 0.36 460 27. +42° 3736 M3 III -1.0 9.34 0.81 800 28. +42° 3737 G8 III + 1.0 8.18 0.27 240 29. +42° 3740 F6 III +2.0 6.90 0.00 95 30. +42° 3741 B2 IV -3.0 9.52 2.43 1040 31. +42° 3743 A5 II -2.8 8.39 1.17 1010 32. +42° 3747 A3 V + 1.5 9.31 0.27 320 34. +42° 3749 AL V + 1.5: 8.95 0.09 295 35. +42° 3750 A7 V +2.5 8.98 0.22 178 36. +42° 3752 B7 V +0.2 7.66 0.36 260 37. +42° 3753 KL III +0.1 7.92 0.36 310 38. +42° 3754 G8 III-IV + 1.9 7.59 0.00 137 39. +42° 3757 A2 V + 1.5 9.40 0.09 365 40. +42° 3761 GO V +4.4: 9.53 0.23 96 41. +42° 3762 B9 V +0.5 9.54 0.18 590 42. +42° 3763 G8 V +4.9 8.86 0.00 62 43. +42° 3764 F7 V +3.6: 9.04 0.17 114 44. +42° 3767 G9 III -0.1 9.00 0.47 530 45. +42° 3768 A4 V + 1.5 7.62 0.22 151 46. +42° 3769 A3 V + 1.5: 9.70 0.18 400 47. +42° 3775 B7 V +0.8 9.15 0.18 430 208 V. Straizys, A. Kazlauskas, V. Vansevicius and K. Cernis

Table 7 (continued)

No. BD Sp Mv V Av r

48. +42° 3779 A2 V + 1.3: 10.46 0.23 610 49. +42° 3782 B8 V +0.2 9.79 0.86 560 50. +42° 3783 G8 III +0.9 8.85 0.31 340 51. +42° 3784 G8 IV +2.6 9.45 0.36 200 52. +42° 3790 Fl IV +2.5 10.01 0.38 265 53. +43° 3549 F7 IV +3.0 7.85 0.11 89 54. +43° 3550 G9 III +0.7 8.86 0.29 375 55. +43° 3552 A3 III +0.7 7.95 0.50 225 56. +43° 3553 G3 III-IV +2.4 8.69 1.08 110 57. +43° 3561 F3 V +3.5: 9.70 0.00 174 58. +43° 3562 G8 IV +2.8 9.92 0.41 220 59. +43° 3566 F5 V +3.6: 7.57 0.05 61 60. +43° 3568 K7 III? +0.7: 9.11 0.57 370 63. +43° 3576 AO V +1.0: 7.86 0.04 230 64. +43° 3579 G8 III +1.4 9.35 0.27 345 65. +43° 3580 A5 V +2.0 9.77 0.09 345 66. +43° 3581 A3 V +1.9 9.05 0.14 255 67. +43° 3584 K0 III +0.9 9.72 0.04 570 68. +43° 3585 Kl III +0.7 9.94 0.14 660 69. +43° 3586 K0 III +0.6 9.48 0.13 560 70. +43° 3587A G5 V +5.0 9.77 0.04 88 71. +43° 3587B G9 III +0.4 10.48 0.29 910 73. +43° 3599 B7 V -0.2 9.43 0.50 670 74. +43° 3600 B8 III -0.5 9.58 0.54 810 75. +43° 3601 A3 V +1.7: 8.81 0.49 210 76. +43° 3602 K3.5 III -0.2 9.16 0.81 510 77. +43° 3606 A5 V +2.3 9.29 0.23 225 78. +43° 3608 G9 III +0.1 9.22 0.29 580 79. +43° 3609 B6 V 0.0 8.30 0.45 370 80. +43° 3613 G9 III +0.1 9.70 0.34 710 81. +43° 3617 K5 III: +0.3: 9.35 0.72 460 82. +43° 3620 AO V +1.5 7.70 0.04 170 83. +43° 3626 F8 IV +2.7: 9.15 0.72 140 84. +43° 3627A A2 V +1.5: 9.91 0.27 420 85. +43° 3627B F0 V +3.1 10.13 0.50 203 86. +43° 3630 09.5 Ia -7.1 7.11 3.46 1410 88. +43° 3638 G8 III +0.6 8.59 0.45 320 89. +43° 3648 B7 V +0.3 9.63 0.45 600 90. +43° 3650 A6 V +2.0 9.74 0.52 280 91. +43° 3655 Fl V +3.0 9.44 0.40 161 92. +43° 3656 G8 II -2.0 8.99 1.76 700 93. +43° 3660 Kl III +0.8 9.46 0.36 460 94. +43° 3662 A7 V +2.5 7.32 0.41 76 95. +43° 3663 F8 V +4.0 9.71 0.04 136 96. +43° 3664 F5 V +3.6 8.83 0.00 111 97. +43° 3666 G2 II -3.0 9.91 1.53 1890 The Vicinity of the North America and Pelican Nebulae 209

All the three methods give similar spectral and luminosity classes and absolute magnitudes: the differences usually do not exceed 1 or 2 subclasses and ±0.5 mag. In this paper, we decided to use the quantification results for normal stars obtained by the Q, Q diagrams (as it was done in Paper I). Intercomparison and critical evaluation of different quantification methods will be given elsewhere. For a part of A-F-G stars of luminosity class V, the Q, Q dia- grams cannot give sufficiently precise value of My due to necessity of extrapolation of the My isolines. For these stars, the average My for a given MK type is ascribed. Such My values in Tables 5-7 are marked by a colon. Colons are also placed to the uncertain spectral types and absolute magnitudes. If the colon stands in front of spec- tral class, this means uncertainty both in spectral and luminosity class. For recognition of peculiar stars of different types we have used the following diagrams: QXYV, Y- V for Am-type stars, QYZS,Y~S for Ap-type stars, QUPYV,Qxzs for carbon-rich stars and the para- meter QYSYV for M-type stars (QYSYV < 0.12 for K-type stars and > 0.12 for M-type stars). The stars with different peculiarities or with a low accuracy of classification are not included into Tables 5-7. Colour excesses Εγ-y, interstellar extinctions Ay and dis- tances of stars r, given in Tables 5-7, have been determined as described in Paper I. The normal interstellar extinction law with R = Ay/Εγ-ν = 4.5 or Ay/Eß-v = 3.15 has been used. The decision to use the normal value of R is based on investigation of Amax of interstellar polarization for some stars in the area of the North America and Pelican Nebulae (Straizys and Goldberg, 1991). The probable errors are ±0.03 mag for Εγ-y, ±0.1 mag for Ay and ±25% for distance. The distances r > 200 pc are rounded to the nearest number multiple to 10.

4. Interstellar extinction in the dark cloud

Fig. 3 shows the plot of extinction versus distance for the dark cloud between the North America and Pelican Nebulae. The stars from Table 5 and the heavily reddened (Ay > 1 mag) stars from Pa- per I which are projected on the dark cloud have been plotted. Fig. 3 is similar to Fig. 2 of Paper II but shows more numerous reddened stars which start to appear at the distance of 430 pc. These stars are probably embedded into the dust cloud and they are important 210 V. jStraizys, A. Kazlauskas, V. Vansevicius and K. Öernis

5

4

3

2

1

0 Ο 300 600 900 1200 1500 1800 r, pc Fig. 3. Dependence of interstellar extinction on distance in the dark cloud area. In addition to the stars from Table 5, stars Nos. 112, 131, 140, 141, 148, 153, 163, 176, 177, 185, 195, 224, 238 and 245 with Ay > 1 mag from Paper I are also plotted. for distance determination of the cloud. The distance error of 25% at 550 pc, the expected distance of the cloud, corresponds to ±140 pc. Due to this error it is not possible to estimate which stars are at the front edge of the cloud and which are behind the cloud. How- ever, the cloud seems to be very dense, and it is safe to assume that all heavily reddened stars are inside it; the stars of the dark cloud background probably are too faint to be measured with our limiting magnitude. If the depth of the cloud is of the same order as the linear extent on the sky plane of the star forming complex 2? 5 or 25 pc), the thickness of the dust layer must not exceed 25 pc. This allows us to consider that all stars within 430 pc and 800 pc can be the cloud objects scattered by the distance determination errors. The average distance of 24 stars with Ay > 1 mag is 580± 100 pc. This value within the error bar coincides with that determined in Paper II, being larger by only 30 pc. The stars of foreground closer than 400 pc, projected on the dust cloud, seem to behave in the same way as the stars in the surroun- ding fields: in general, extinction values of these stars are scattered between zero and 1.0 mag with slight increase with increasing dis- tance. The Vicinity of the North America and Pelican Nebulae 211

Special attention must be paid to the stars which exhibit too small interstellar extinction for their distances. Such stars are: No. 66 (V = 11.91, Gl III-IV, Av = 0.00, r = 0.96 kpc), No. 180 (V = 11.23, K0 III, Av = 0.23, r = 1.1 kpc), No. 11 (V = 10.11, Kl III, Av = 0.00, r = 1.4 kpc) and No. 124 (V = 12.56, F6 III, Av = 0.57, r = 1.7 kpc). These stars are either observed in the transparent windows in the dust cloud or are of peculiar types, not recognized photometrically. Spectroscopic investigation of these stars would be recommended.

5. Interstellar extinction in other areas

Figs. 4 and 5 show the plot of extinction versus distance for the other two areas listed in Table 1. Both these areas up to 500 pc distance show similar run of extinction with distance: the stars are scattered between Av values from 0.0 to ~ 0.5 mag. The slight increase of maximum extinction with distance is observed. Many stars show very small or no interstellar reddening up to 600 pc: this means that numerous transparent windows are present between dust clouds. Some stars, such as +43°3553 and +43°3626 exhibit too large extinction for their distance. Probably, these stars are either unresolved binaries of close spectral types or peculiar objects. In the BD 40°- 41° ctrCcl} cl number of heavily reddened stars start to appear at r > 500 pc. In this respect the area seems to be similar to the area of the dark cloud (Fig. 3). This probably means that the dark cloud extends far to south. This conclusion seems to be confirmed by a glance to long exposure photographs of the area: the extension of the dark cloud is observable south of the North America Nebula, the Pelican Nebula and a Cygni down to the 40° declination. It is an impression that the BD 40°- 41° area shows a dichotomy in the Av,r dependence at r > 600 pc: a part of stars extend the low extinction sequence up to 1.5 kpc and the other part of stars exhibit extinctions of the order of 3 to 4 mag. If this dichotomy is real, then it would be a reason to suggest the presence of a dust cloud system which shades the upper group of stars while the stars of lower group are seen in the windows. Both strongly reddened and mildly reddened stars are scattered in the whole field. On the other hand, this conclusion seems to contradict with our result of Paper II where the area south of a Cygni has been found to be transparent up to 700 pc distance. However, in that area the stars between 500 and 700 pc were not sufficiently represented. To solve 212 V. Straizys, A. Kazlauskas, V. Vansevicius and K. Öernis

τ r ~l ι ι ι ι I I I I 1 1 1 Γ

4 ο ο ο 3 h

2

1 0 * * ° ο ° ° ο 0 fo Ρ I J I I I L 300 600 900 1200 1500 1800 r, pc

Fig. 4. Dependence of interstellar extinction on distance in the BD 40°- 41° area.

1 1 1 5 π ι ι ι ι ι ι ι ι ι ι ρ I ι Ζ

Ar

4

3

2

1

0 0 300 600 900 1200 1500 1800 r, pc

Fig. 5. Dependence of interstellar extinction on distance in the BD 42°- 43° area. this problem, more observations with fainter limiting magnitude in the area south of a Cygni would be important. In the BD 42°- 43° area (Fig. 5) the jump of extinction at » 700 pc also takes place but here the reddened stars are less numerous and the conclusions are not so definite. The Vicinity of the North America and Pelican Nebulae 213

Acknowledgments. The authors are indebted to Miss S. Barta- siüte for her help in observations. One of us (V.V.) acknowledges the support by the Japan Society for Promotion of Science.

References

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