Photometric Investigation of the California Nebula Region: Catalogs

Baltic Astronomy, vol. 10, 319-347, 2001.

PHOTOMETRIC INVESTIGATION OF THE CALIFORNIA NEBULA REGION: CATALOGS

V. Straizys1, K. Cernis1 and S. Bartasiute1'2

1 Institute of Theoretical Physics and Astronomy, Gostauto 12, Vilnius 2600, Lithuania 2 Vilnius University Observatory, Giurlionio 29, Vilnius 2009, Lithuania Received May 10, 2000.

Abstract. Vilnius seven-color photometry has been obtained for 238 stars down to 13th mag in the area of the California Nebula in Perseus. For nearly all of the stars photometric spectral classes, luminosity classes, absolute magnitudes, interstellar reddenings, extinctions and distances are determined. The present paper contains the results of photometry and the parameters of the stars. Key words: methods: observational - techniques: photometric: Vilnius photometric system - stars: fundamental parameters - interstellar medium: dust, extinction - nebulae: individual: California Nebula or NGC 1499

1. INTRODUCTION

This paper is an extension of the program of investigation of the Taurus-Auriga-Perseus-Aries dark clouds by photoelectric photometry in the Vilnius seven-color system. The earlier investigations included a number of areas in Taurus and southern Perseus: the Taurus area containing the Lynds dark clouds L 1538, L 1528, L1521 and L1495 (Straizys & Meistas 1980, Straizys 1982, Straizys et al. 1982a,b, 1985), the Taurus area containing the Lynds daxk clouds L1551, L1546 and L1543 (Meistas & Straizys 1981), the area around the variable star RV Tau (Straizys & Meistas 1981), the Merope dark cloud in the Pleiades (Cernis 1987), the area around the reflection 320 V. Straizys, K. Cernis, S. Bartasiute nebula NGC 1333 (Cernis 1990), the area around the open cluster IC 348 and in the Per OB2 association (Cernis 1993), the area around the open clusters NGC 1750 and NGC 1758 (Straizys et al. 1992). The area investigated in this paper includes the California Neb- ula (NGC 1499) and is bounded by the following 2000.0 coordinates: RA from 3h48m to 4h10^ and DEC from +35° to +39°. The northern part of this area is covered by the dark cloud Khavtassi 257 (Khav- tassi 1960). The Lynds (1962) catalog separates several smaller dark clouds in the area: L 1449, L 1456 and L 1459. In the present paper we describe the methods of observation and reductions, and the determination of spectral classes, absolute magnitudes, color excesses, interstellar extinctions and distances of the stars. The catalogs present the observed magnitudes and color indices (Table 2) and the physical properties and distances of the stars (Table 3). Investigation of interstellar extinction in the area will be described elsewhere (Straizys, Cernis & Bartasiute 2001).

2. OBSERVATIONS, REDUCTIONS AND THE CATALOG

Photoelectric photometry of 238 stars in the standard passbands of the Vilnius system (Table 1) was performed in 1994-1996 with the 1 m telescope of the Institute of Theoretical Physics and Astronomy situated at the Maidanak Observatory in Uzbekistan. In the area al- most all stars down to 10th mag were measured. In the dark clouds north of California we observed a number of fainter stars down to 13th mag. In all cases we tried to reach the accuracy of flux measurements better than ±0.01 mag, so at least 10 000 pulses were usually counted in each filter. For the faintest stars this condition was some- times disobeyed, and the accuracy of their magnitudes and color indices can be somewhat lower, especially in the ultraviolet filters for red or reddened stars. The extinction coefficients of the atmosphere for every moment of observation were determined by the Nikonov (1976) method adjusted to the Vilnius system by Zdanavicius (1975, 1996). The star HD 23609 (V=6.97, F9 IV) in the Pleiades was used for the extinction determination. Transformation equations from the instrumental to the standard system were determined from observations of about 20 stars in the Cygnus Standard Region (Zdanavicius & Cerniene 1985). Details on the instrumentation and reduction procedures are given by Bartasiute (1999). California Nebula region: catalogs 321

Table 1. Mean wavelengths and half-widths of the passbands of the Vilnius photometric system.

Passband U P X Y Z V S

Ao (nm) 345 374 405 466 516 544 656 AA (nm) 40 26 22 26 21 26 20

The catalog of V magnitudes and color indices in the standard Vilnius system for the observed stars is given in Table 2. The number of independent observations for each star, n, used to take the average values of magnitudes and color indices, is given in the last column. The identification numbers correspond to Figs. 1-4. BD numbers are also given in the Table. HD and other numbers, as well as information on duplicity and variability, are presented in the Notes.

3. CLASSIFICATION OF STARS

For the determination of spectral classes and absolute magnitudes of stars the following two independent methods were used.

(1) Interstellar reddening-free diagrams QUPY,QPYV', QUPY, QXYV; QUXY,QUPYV) QUPY,QXZS and QXZS,QXYZ calibrated in terms of MK spectral classes and absolute magnitudes My by Straizys et al. (1982c). Here the reddening-free Q-parameters are defined by the equation:

m m £?1234 = ( i - 2) - (Ei2/E34)(m3 - m4), (1) and

EK,E = (MK — m^)reddened — (FNK — raf)intrinsic- (2) This method gives the accuracy of spectral class ±1 decimal spectral subclass. The accuracy of MY depends on spectral type and varies from ±0.3 to ±0.5 mag. Absolute magnitudes are adjusted to the modern distance scale based on the Hyades distance modulus V — MV = 3.3 mag (Perryman et al. 1998). 322 V. Straizys, K. Cernis, S. Bartasiute

Table 2. Results of photometry.

No. BD RA(2000) DEC(2000) V U-V P-V X-V Y-V Z-V V-S n h m s oi

1. +38 810 3 49 28 39 07.1 9.74 2.76 1.96 1.10 0.51 0.19 0.45 2 2. * +38 811 3 49 36 38 59.0 9.15 2.97 2.05 1.09 0.51 0.19 0.50 2 3. +35 750 3 49 41 35 47.3 9.88 2.30 1.76 1.10 0.47 0.19 0.46 1 4. +38 812 3 49 43 39 11.6 10.07 2.30 1.87 1.32 0.54 0.21 0.57 4 5. * +35 751 3 49 49 35 36.0 9.51 2.32: 1.85: 1.07 0.42 0.16 0.26 1 6. * +37 833 3 50 03 37 52.4 6.63 2.17 1.60 0.86 0.33 0.12 0.32 2 7. +35 753 3 50 08 35 34.0 9.55 5.41 4.57 3.21 1.18 0.53 1.12 2 8. +37 834 3 50 18 38 20.1 10.11 2.23 1.75 1.14 0.49 0.18 0.49 2 9. * +35 752 3 50 34 36 16.5 10.73 2.63 2.06 1.37 0.62 0.25 0.58 1 10. +36 762 3 51 16 37 21.6 9.64 4.61 3.87 2.71 1.09 0.47 1.04 2 11. +36 765a 3 51 17 37 07.4 10.51 4.32 3.67 2.52 0.98 0.38 0.93 1 12. +36 763 3 51 19 37 12.3 9.12 2.22 1.68 0.96 0.40 0.15 0.38 1 13. 3 51 22 37 06.2 11.91 2.48 1.96 1.35 0.62 0.25 0.56 1 14. +35 754 3 51 25 35 33.1 8.25 5.14 4.34 3.11 1.21 0.48 1.02 2 15. 3 51 25 37 05.7 12.50 4.07: 3.66 2.50 0.98 0.40 0.89 1 16. * +36 764 3 51 26 37 26.6 8.88 2.25 1.73 1.10 0.47 0.18 0.46 1 17. +38 814 3 51 32 38 43.0 10.07 4.00 3.31 2.34 1.01 0.39 0.95 4 18. +36 765 3 51 32 37 04.7 10.11 3.83 3.22 2.24 0.90 0.35 0.87 1 19. +36 766 3 51 43 36 51.6 8.57 5.52 4.70 3.35 1.33 0.59 1.26 2 20. +35 755 3 51 47 35 42.5 8.89 3.50 2.87 1.98 0.81 0.32 0.77 2 21. +36 767 3 52 02 36 39.2 10.56 4.20 3.59 2.43 1.00 0.39 0.90 1 22. +36 768 3 52 14 36 31.3 8.95 2.84 2.42 1.65 0.63 0.28 0.65 1 23. +38 815 3 52 23 38 50.8 9.02 4.21 3.57 2.46 0.99 0.39 0.92 3 24. +35 756 3 52 24 36 12.3 10.55 2.25 1.71 0.82 0.35 0.12 0.28 1 25. +38 816 3 52 41 38 32.4 9.28 2.39 1.81 1.13 0.50 0.19 0.48 4 26. +35 757 3 52 42 35 47.5 10.15 2.53 1.83 0.95 0.42 0.16 0.39 1 27. +36 769 3 52 54 36 51.3 9.78 2.46 1.76 0.87 0.42 0.17 0.37 1 28. * +35 759 3 52 55 35 32.3 10.77 2.56 2.00 1.23 0.57 0.23 0.56 1 29. +37 835 3 52 58 38 15.2 9.50 3.92 3.27 2.26 0.95 0.36 0.90 2 30. +35 760 3 53 05 35 35.8 10.67 3.90 3.23 2.26 0.89 0.36 0.86 1 31. +38 817 3 53 13 38 55.7 10.10 2.53 2.04 1.36 0.55 0.21 0.55 3 32. * +35 761 3 53 16 36 20.3 9.61 5.01 4.25 2.95 1.12 0.47 1.03 1 33. * +36 770 3 53 18 36 49.4 8.21 4.61 3.82 2.72 1.17 0.45 1.07 2 34. * +35 763 3 53 22 35 33.3 8.71 1.41 1.05 0.51 0.24 0.09 0.20 1 35. * +35 762 3 53 25 36 24.8 8.73 4.03 3.36 2.29 0.91 0.36 0.87 2 36. +35 764 3 53 25 35 48.0 9.47 1.68 1.24 0.59 0.29 0.10 0.23 1 37. +36 771 3 53 32 37 21.6 10.31 2.46 2.09 1.42 0.57 0.24 0.58 2 38. +35 765 3 53 48 35 39.6 10.52 6.79: 4.65: 3.13 1.50 0.45 1.56 2 39. +38 818 3 53 54 39 03.0 10.02 2.65 2.18 1.49 0.61 0.24 0.59 2 40. +36 772 3 53 55 36 58.7 9.77 2.25 1.80 1.25 0.51 0.19 0.54 1 California Nebula region: catalogs 323

Table 2 (continued)

No. BD RA(2000) DEC(2000) V U-V P-V X-V Y-V Z-V V-S n h m s oi

41. +37 838 3 53 56 37 27.4 10.66 2.58 2.12 1.44 0.58 0.22 0.62 2 42. * +38 819 3 54 04 38 32.9 8.29 2.35 1.72 0.91 0.35 0.14 0.29 3 43. * +38 820 3 54 05 38 31.6 8.87 2.23 1.63 0.81 0.32 0.12 0.27 3 44. * +36 774 3 54 18 36 40.9 8.72 4.00 3.37 2.28 0.89 0.36 0.85 1 45. +37 839 3 54 19 38 26.4 10.60 2.77 2.27 1.51 0.60 0.23 0.63 2 46. +36 773 3 54 20 37 17.1 10.96 2.37 1.85 1.22 0.54 0.20 0.53 1 47. * +36 775 3 54 39 36 43.6 8.48 5.18 4.40 3.03 1.14 0.48 1.04 1 48. +37 840 3 54 55 38 11.6 9.77 2.61 2.15 1.43 0.58 0.22 0.57 2 49. +35 768 3 55 03 35 33.6 10.31 4.08 3.45 2.34 0.92 0.37 0.87 1 50. +36 778 3 55 05 37 02.6 11.54 2.69 2.03 1.07 0.50 0.19 0.40 2 51. +36 776 3 55 06 37 15.0 10.25 3.32 2.85 1.91 0.71 0.35 0.74 1 52. +36 777 3 55 13 36 27.5 10.42 4.08 3.47 2.39 0.94 0.39 0.88 2 53. +37 841 3 55 22 38 12.6 9.77 2.50 2.00 1.38 0.60 0.23 0.58 2 54. * +36 779 3 55 28 36 34.9 8.43 3.98 3.30 2.32 0.97 0.40 0.85 1 55. * +37 842 3 55 31 38 18.9 8.85 2.24 1.79 1.21 0.50 0.19 0.51 4 56. +36 780 3 55 40 37 00.1 11.31 2.43 1.93 1.28 0.58 0.20 0.55 1 57. +36 781 3 55 54 37 23.9 10.74 2.51 1.99 1.41 0.67 0.21 0.56 1 58. +35 769 3 55 57 36 16.2 9.79 5.25 4.41 3.08 1.19 0.51 1.11 1 59. +36 782 3 56 00 36 41.0 9.66 3.91 3.23 2.20 0.87 0.35 0.87 2 60. +36 784 3 56 10 37 01.0 10.99 2.79 2.23 1.53 0.65 0.25 0.64 1 61. 3 56 15 38 50.5 11.50 2.82 2.11 1.37 0.66 0.24 0.51 1 62. 3 56 16 38 58.2 11.43 2.66 2.01 1.34 0.63 0.26 0.55 1 63. 3 56 22 38 55.5 11.55 5.95: 4.52 2.89 1.27 0.48 1.15 1 64. +35 770 3 56 22 36 09.1 11.20 2.41 1.87 1.27 0.59 0.22 0.55 1 65. 3 56 27 39 07.2 11.42 5.80 4.94 3.42 1.42 0.59 1.28 1 66. +36 786 3 56 34 37 09.5 9.13 3.56 2.93 2.05 0.85 0.32 0.82 2 67. +36 787 3 56 40 37 16.2 9.93 3.65 3.08 2.18 0.90 0.34 0.87 1 68. +38 822 3 56 45 38 43.7 9.73 3.31 2.74 1.90 0.78 0.30 0.76 4 69. * +35 771 3 56 45 36 00.2 8.31 2.19 1.74 1.18 0.49 0.18 0.51 2 70. +38 823b 3 56 46 38 28.3 10.86 2.61 2.13 1.43 0.59 0.23 0.57 1 71. +38 823a 3 56 49 38 28.0 9.50 2.15 1.68 1.10 0.46 0.17 0.48 4 72. 3 56 52 38 41.7 12.42 6.94: 5.94 4.36 1.84 0.80 1.66 2 73. +38 824 3 56 53 38 50.3 9.37 2.70 2.25 1.52 0.60 0.25 0.61 4 74. 3 57 00 38 46.1 11.78 2.67 2.21 1.57 0.65 0.27 0.65 2 75. +37 843 3 57 03 37 58.4 10.68 2.33 1.83 1.25 0.53 0.18 0.55 2 76. +36 788 3 57 13 37 02.0 9.72 2.28 1.77 1.17 0.50 0.19 0.48 2 77. 3 57 17 38 56.4 10.98 2.72 2.07 1.37 0.65 0.25 0.61 2 78. +36 789 3 57 17 36 58.0 10.03 5.06 4.29 3.02 1.16 0.48 1.09 1 79. +38 825 3 57 19 38 36.7 10.90 5.45: 4.59 3.17 1.28 0.52 1.18 4 80. +36 790 3 57 19 36 35.2 9.44 2.57 1.94 1.23 0.54 0.21 0.53 1 324 V. Straizys, K. Cernís, S. Bartasiutè

Table 2 (continued)

No. BD RA(2000) DEC(2000) V U-V P-V X-V Y-V Z-V V-S n h m s oí

81. 3 57 23 38 46.9 12.49 3.76 3.19 2.18 0.75 0.44 0.85 2 82. +36 791 3 57 30 36 54.0 9.72 2.05 1.57 1.14 0.50 0.18 0.48 1 83. * +36 792 3 57 35 36 29.5 6.70 2.09 1.62 1.04 0.43 0.16 0.44 2 84. +35 772 3 57 39 35 58.5 8.98 4.55 3.85 2.70 1.07 0.44 0.98 2 85. +37 844 3 57 42 37 32.2 9.74 4.49 3.82 2.63 1.06 0.41 0.98 1 86. 3 57 45 38 31.8 12.30 5.34 4.70 3.32 1.33 0.58 1.17 2 87. 3 57 48 38 41.9 12.35 3.08 2.61 1.78 0.70 0.31 0.69 2 88. +36 793 3 57 51 36 36.6 8.03 5.09 4.32 2.94 1.08 0.47 1.01 2 89. +36 794 3 57 53 37 16.6 10.33 6.41 5.50 3.79 1.51 0.62 1.40 1 90. 3 57 54 38 56.3 12.83 5.48 4.63 3.37 1.42 0.56 1.29 2 91. * +38 826 3 57 56 38 41.2 10.05 1.99 1.57 1.17 0.64 0.22 0.73 4 92. 3 57 59 38 44.0 11.43 2.68 2.07 1.40 0.64 0.23 0.60 2 93. +36 795 3 58 03 36 32.7 9.52 2.31 1.74 0.99 0.41 0.16 0.39 2 94. 3 58 06 38 39.8 12.21 2.65 2.19 1.54 0.63 0.25 0.65 2 95. 3 58 06 38 39.8 11.99 2.74 2.13 1.47 0.69 0.24 0.63 2 96. +37 845 3 58 12 37 45.3 10.31 2.79 2.39 1.62 0.63 0.29 0.64 1 97. 3 58 14 38 50.8 12.46 3.60 2.67 1.62 0.77 0.29 0.63 2 98. 3 58 16 38 57.3 10.42: 3.21: 2.47 1.70 0.73 0.27 0.67 2 99. 3 58 16 38 42.2 10.81 2.86 2.32 1.57 0.65 0.25 0.61 2 100. 3 58 25 38 46.8 12.50 3.20 2.39 1.39 0.67 0.24 0.57 2 101. * +38 827 3 58 29 38 50.6 6.30 3.85 3.23 2.19 0.81 0.33 0.78 3 102. * +36 796 3 58 37 37 07.7 8.91 2.42 1.88 1.25 0.53 0.19 0.54 1 103. 3 58 41 38 28.3 12.57 3.49 2.63 1.78 0.86 0.33 0.72 2 104. 3 58 44 38 59.1 12.34 3.48 2.59 1.56 0.78 0.25 0.64 2 105. +37 846 3 58 45 37 41.3 9.23 2.43 1.89 1.27 0.55 0.21 0.54 1 106. * +35 773 3 58 49 36 22.5 10.09 2.40 1.76 0.88 0.43 0.17 0.33 1 107. 3 58 54 38 49.5 12.96 4.80 3.79 2.81 1.29 0.49 1.16 2 108. * +35 775 3 58 58 35 47.5 4.04 0.74 0.58 0.47 0.27 0.10 0.24 2 109. +35 774b 3 59 01 36 23.3 11.43 2.29 1.71 0.83 0.37 0.15 0.25 1 110. +35 774a 3 59 03 36 22.4 10.47 2.32 1.76 1.06 0.47 0.18 0.44 1 111. +35 776 3 59 10 35 50.1 9.99 2.29 1.79 1.19 0.52 0.20 0.49 3 112. * +36 797 3 59 26 36 33.2 10.48 2.90 2.09 1.10 0.51 0.20 0.45 1 113. * +35 778 3 59 28 36 19.1 7.99 3.47 2.91 2.02 0.81 0.32 0.77 2 114. +35 777 3 59 30 35 51.6 10.50 2.30 1.80 1.16 0.53 0.21 0.48 2 115. +37 848 3 59 34 37 27.7 9.66 2.82 2.05 1.08 0.51 0.18 0.42 2 116. 3 59 37 38 57.6 12.27 3.27 2.66 1.82 0.79 0.32 0.73 1 117. +38 828 3 59 40 38 55.0 9.84: 4.96 4.18 2.90 1.15 0.51 1.10 2 118. * +38 829 3 59 40 38 49.2 6.48 2.15 1.43 0.60 0.28 0.11 0.23 5 119. 3 59 49 38 49.7 11.48 3.54 3.03 2.01 0.72 0.42 0.80 2 120. * +36 798 3 59 49 36 47.6 8.96 2.16 1.69 1.08 0.47 0.18 0.44 1 California Nebula region: catalogs 325

Table 2 (continued)

No. BD RA(2000) DEC(2000) V U-V P-V X-V Y-V Z-V V-S n h m s oi

121. * +37 849b 3 59 50 38 01.6 11.67 3.18 2.36 1.27 0.61 0.22 0.48 1 122. * +37 849a 3 59 51 38 01.0 10.72 3.07 2.36 1.47 0.65 0.24 0.58 2 123. +36 799 3 59 51 37 18.0 10.29 4.54 3.76 2.64 1.13 0.42 1.11 1 124. 3 59 52 38 51.6 11.02 2.33: 1.80: 1.21 0.57 0.19 0.52 1 125. 3 59 53 38 34.9 11.62 2.67 2.14 1.45 0.68 0.24 0.57 2 126. * +35 779 3 59 53 36 01.0 8.54 2.42 1.78 1.00 0.43 0.16 0.39 2 127. 3 59 56 38 49.6 12.03 3.86 2.75 1.67 0.84 0.29 0.68 2 128. +35 780 3 59 57 36 01.0 9.78 2.27 1.64 0.77 0.36 0.13 0.26 1 129. 3 59 58 38 38.0 12.21 2.73 2.35 1.73 0.72 0.28 0.65 2 130. +36 800 3 59 58 36 43.5 10.09 4.94 4.15 2.85 1.12 0.45 1.04 1 131. +38 830 3 59 59 39 03.9 10.84 2.75 2.06 1.23 0.57 0.21 0.47 2 132. +38 831a 4 00 00 38 32.1 10.19 2.35 1.83 1.24 0.54 0.21 0.51 2 133. +37 850 4 00 02 37 41.6 9.47 2.46 1.83 0.92 0.42 0.15 0.34 1 134. 4 00 04 38 52.3 10.13 6.38: 5.38: 4.00: 1.77 0.71 1.65 2 135. * +35 781 4 00 04 35 47.5 9.91 2.37 1.75 0.85 0.39 0.15 0.28 1 136. +38 831b 4 00 06 38 30.6 9.72 6.62 5.62 3.98 1.58 0.65 1.42 1 137. 4 00 09 38 56.2 10.77 2.71 2.14 1.48 0.67 0.26 0.62 3 138. +37 851 4 00 16 37 59.1 9.49 2.29 1.82 1.26 0.52 0.20 0.55 1 139. +37 852 4 00 18 37 54.6 9.81 2.55 2.03 1.36 0.56 0.23 0.55 2 140. +35 783 4 00 23 36 11.6 9.14 4.37 3.69 2.55 1.01 0.41 0.93 1 141. +37 853 4 00 27 38 06.7 9.32 2.20 1.75 1.17 0.49 0.18 0.49 2 142. 4 00 29 38 55.7 11.71 3.29 2.68 1.87 0.84 0.32 0.77 2 143. +37 854 4 00 42 37 48.9 9.94 2.95 2.44 1.63 0.66 0.27 0.64 3 144. +36 801 4 00 47 37 08.8 10.23 2.29 1.78 1.26 0.64 0.23 0.62 3 145. +37 856 4 00 47 38 16.7 10.24 2.25 1.76 1.16 0.51 0.18 0.49 2 146. +35 784b 4 00 51 35 51.0 10.66 3.45 2.98 2.02 0.74 0.38 0.74 1 147. * +35 785 4 00 51 36 17.7 9.48 2.33 1.80 0.99 0.40 0.17 0.36 1 148. 4 00 53 38 39.0 12.27 2.50 2.09 1.55 0.69 0.26 0.62 2 149. +35 786 4 01 04 36 04.1 10.12 2.56 1.90 0.99 0.43 0.16 0.37 1 150. * +37 857 4 01 05 38 22.6 7.51 4.57 3.88 2.59 0.94 0.41 0.86 2 151. +36 803 4 01 08 36 44.9 11.07 2.61 2.14 1.49 0.61 0.25 0.63 2 152. 4 01 12 38 36.0 11.14 3.29 2.43 1.40 0.71 0.26 0.56 3 153. +36 804 4 01 12 37 07.6 8.43 3.56 2.98 2.03 0.81 0.31 0.77 1 154. +37 858 4 01 13 37 30.7 9.59 2.21 1.70 1.08 0.45 0.17 0.44 1 155. * +36 805 4 01 15 36 59.4 6.41 1.77 1.21 0.47 0.20 0.07 0.16 2 156. +35 787 4 01 23 36 18.0 10.88 3.96 3.35 2.29 0.93 0.35 0.87 1 157. 4 01 25 36 34.6 9.95 5.41 4.55 3.18 1.23 0.53 1.12 1 158. * +38 832b 4 01 33 38 40.1 9.16 3.04 2.54 1.77 0.71 0.29 0.70 4 159. * +38 832a 4 01 35 38 40.0 7.79 5.74 4.86 3.40 1.31 0.56 1.20 4 160. +38 833 4 01 44 39 09.6 10.33 2.56 2.06 1.43 0.59 0.23 0.60 2 326 V. Siraizys, K. Cernís, S. Bartasiuté

Table 2 (continued)

No. BD RA(2000) DEC(2000) V U-V P-V X-V Y-V Z-V V-S n h m s oí

161. 4 01 50 39 05.8 12.77 3.46 3.33 1.98 0.77 0.35 0.74 1 162. 4 01 53 38 40.6 10.91 2.72 2.24 1.55 0.63 0.26 0.62 2 163. +36 806 4 01 55 36 47.9 10.07 2.40 1.83 1.16 0.52 0.20 0.49 1 164. 4 02 03 39 10.3 11.93 2.74 2.34 1.56 0.60 0.20 0.65 1 165. 4 02 04 39 06.2 11.55 2.58: 2.15: 1.36 0.68 0.28 0.58 1 166. 4 02 05 38 38.0 12.45: 3.69: 2.80: 1.75 0.77 0.29 0.73 2 167. 4 02 06 38 41.5 12.44 3.35 2.61 1.57 0.80 0.26 0.71 2 168. +36 807 4 02 14 37 10.0 10.70 2.30 1.63 0.83 0.35 0.15 0.36 2 169. +37 859 4 02 16 37 29.7 9.58 2.34 1.74 0.91 0.39 0.15 0.34 2 170. +36 809 4 02 18 37 19.3 10.84 6.20 5.19 3.65 1.41 0.62 1.32 1 171. * +36 808 4 02 22 36 27.4 9.10 3.68 3.10 2.13 0.86 0.34 0.80 1 172. • +38 834 4 02 29 39 05.8 7.70 2.18 1.59 0.85 0.34 0.14 0.31 2 173. +35 789 4 02 35 36 11.8 11.12 2.99 2.17 1.23 0.56 0.20 0.48 2 174. * +37 862 4 02 48 37 56.7 8.74 2.23 1.65 0.82 0.32 0.12 0.27 2 175. +37 864 4 02 54 37 38.3 9.70 2.57 1.91 1.05 0.45 0.17 0.40 2 176. * +37 863 4 02 55 37 57.6 9.14 2.28 1.72 1.03 0.44 0.16 0.43 2 177. * +36 810 4 03 10 37 07.3 7.26 3.60 3.02 2.06 0.80 0.31 0.78 2 178. * +37 866 4 03 11 38 03.3 7.89 1.69 1.20 0.55 0.21 0.09 0.15 2 179. +38 835 4 03 13 38 58.4 9.90 2.40 1.81 1.16 0.50 0.18 0.49 2 180. * +37 867 4 03 48 37 58.3 8.42 2.03 1.48 0.63 0.24 0.09 0.19 2 181. +35 792 4 03 50 35 53.5 10.18 4.86 4.13 2.86 1.10 0.47 1.05 2 182. +35 791 4 03 52 36 11.0 10.29 4.17 3.45 2.44 1.00 0.38 0.96 2 183. +37 868 4 03 56 37 26.6 11.25 3.33: 2.68 1.91 0.85 0.34 0.82 2 184. +37 869 4 04 03 37 29.9 11.14: 2.67 2.20 1.53 0.63 0.29 0.67 2 185. +36 811 4 04 04 36 57.0 9.30 2.42 1.88 1.24 0.53 0.20 0.51 2 186. * +37 870 4 04 07 37 36.7 8.60 2.17 1.70 1.15 0.49 0.18 0.51 2 187. +37 871 4 04 14 37 59.6 9.93 2.74 2.29 1.57 0.61 0.26 0.62 2 188. +35 793 4 04 16 35 49.1 9.46 3.99 3.32 2.29 0.93 0.36 0.79 1 189. * +38 836 4 04 24 38 47.8 7.48 2.16 1.56 0.80 0.32 0.12 0.30 3 190. +37 872 4 04 31 37 33.8 9.14 2.31 1.85 1.25 0.52 0.20 0.53 2 191. * +35 796 4 04 34 35 55.2 7.98 2.08 1.44 0.66 0.31 0.11 0.24 2 192. +38 837 4 04 37 38 51.9 9.47 2.29 1.78 1.20 0.53 0.20 0.51 2 193. +36 812 4 04 39 36 30.2 9.81 2.35 1.83 1.25 0.55 0.20 0.52 2 194. * +38 838 4 04 44 38 54.0 8.15 2.62 1.92 1.18 0.50 0.19 0.59 3 195. * +36 813b 4 04 54 37 05.4 9.52 4.33 3.70 2.50 0.95 0.40 0.89 2 196. * +37 873 4 04 57 37 27.3 8.73 2.30 1.74 1.09 0.47 0.17 0.45 2 197. * +36 813a 4 04 58 37 05.2 8.02 2.14 1.57 0.71 0.27 0.09 0.20 2 198. * +36 814 4 04 59 36 44.0 9.45 2.08 1.54 0.68 0.28 0.08 0.23 2 199. +37 874 4 05 03 37 35.5 10.02 3.35 2.71 1.91 0.83 0.33 0.79 4 200. +38 839 4 05 33 38 38.2 10.36 3.41 2.94 1.98 0.70 0.38 0.76 2 California Nebula region: catalogs 327

Table 2 (continued)

No. BD RA(2000) DEC(2000) V U-V P-V X-V Y-V Z-V V-S n h m s 01

201. * +37 876 4 05 40 37 45.3 7.87 2.38 1.74 1.02 0.43 0.16 0.42 4 202. +35 799 4 06 53 36 02.0 10.71 2.74 2.31 1.56 0.64 0.25 0.63 1 203. +35 800b 4 07 04 36 19.9 10.44 4.52: 3.88: 2.69: 1.03 0.44 0.97 2 204. * +35 800a 4 07 07 36 20.6 9.30 2.17 1.57 0.72 0.29 0.11 0.22 2 205. * +38 841 4 07 08 38 27.3 9.02 2.18 1.65 0.97 0.40 0.15 0.36 2 206. * +36 818 4 07 13 37 17.2 7.93 3.72 3.13 2.12 0.82 0.33 0.77 2 207. +36 819 4 07 15 36 26.9 11.10 4.99 4.39 2.93 1.14 0.45 1.04 2 208. * +37 877 4 07 23 38 01.4 8.50 4.55 3.82 2.72 1.08 0.48 1.03 5 209. * +37 878 4 07 34 38 04.5 7.08 3.04 2.59 1.74 0.67 0.31 0.74 4 210. +36 821 4 07 38 36 34.0 10.83 2.77 2.27 1.57 0.65 0.27 0.64 2 211. * +35 802 4 07 41 35 42.1 9.91 2.37 1.75 0.96 0.42 0.14 0.40 1 212. * +37 879 4 07 45 38 09.5 9.89 2.51 1.89 1.09 0.45 0.18 0.42 3 213. * +36 823 4 07 46 37 05.9 9.11 2.27 1.80 1.22 0.52 0.21 0.49 2 214. +38 842 4 07 47 39 15.0 9.63 3.84 3.23 2.23 0.85 0.35 0.82 1 215. • +37 880 4 07 47 37 26.3 9.92 2.62 2.03 1.37 0.60 0.23 0.57 2 216. +35 803 4 07 54 35 27.8 10.14 3.41 2.78 1.98 0.88 0.36 0.86 2 217. +38 843a 4 08 05 38 45.8 10.23 2.16 1.63 1.04 0.45 0.16 0.46 2 218. +38 843b 4 08 05 38 45.6 11.81 2.29 1.82 1.30 0.57 0.23 0.56 2 219. +36 824 4 08 06 36 45.3 9.11 3.76 3.15 2.15 0.85 0.33 0.79 2 220. * +36 825 4 08 07 36 58.0 9.04 2.28 1.60 0.76 0.36 0.12 0.28 2 221. * +36 826 4 08 07 36 35.7 9.40 5.82 4.92 3.43 1.26 0.55 1.21 2 222. * +37 881 4 08 15 37 43.6 6.05 3.40 2.88 1.92 0.72 0.30 0.71 2 223. +35 804 4 08 17 35 34.0 9.91 4.64 3.90 2.64 1.05 0.42 0.98 1 224. +36 827 4 08 20 37 15.0 10.08 2.65 2.17 1.45 0.59 0.23 0.58 2 225. +35 805 4 08 21 35 59.4 9.82 4.06 3.58 2.46 0.83 0.52 0.93 3 226. • +37 882 4 08 36 38 02.4 5.51 2.27 1.79 1.20 0.49 0.19 0.50 4 227. +36 828 4 08 47 36 54.6 9.54 3.29 2.76 1.90 0.78 0.31 0.76 3 228. * +38 844 4 08 49 38 40.8 10.67 2.60 2.05 1.40 0.60 0.23 0.60 2 229. +35 806 4 08 53 35 43.2 8.73 4.29 3.64 2.45 0.93 0.41 0.88 1 230. +38 845 4 09 03 39 17.7 9.10 3.77 3.13 2.18 0.90 0.34 0.86 2 231. +36 831 4 09 09 37 23.3 10.79 3.56 2.87 1.92 0.85 0.34 0.83 2 232. * +36 829 4 09 12 36 25.7 7.74: 6.01: 4.99 3.47 1.34 0.50 1.40 2 233. +36 830a 4 09 22 36 30.5 11.10 2.41 1.80 0.88 0.40 0.15 0.29 3 234. * +35 807 4 09 23 36 02.1 7.77 2.28 1.76 1.15 0.49 0.18 0.47 2 235. +35 808 4 09 25 35 56.8 10.02 3.88 3.24 2.24 0.93 0.36 0.87 1 236. +36 832 4 09 28 36 44.4 9.80 2.36 1.86 1.27 0.56 0.22 0.54 2 237. +38 846 4 09 33 39 22.1 10.04 2.35 1.74 0.84 0.37 0.13 0.30 2 238. * +35 809 4 09 43 35 58.6 8.00 3.16 2.63 1.81 0.72 0.30 0.71 2 328 V. Straizys, K. Cemis, S. Bartasiutè

NOTES:

2. XY Per. Variable star of the Orion type (In). Kmax/Kmin = 9.2/10.6. CCDM 03496+3859 AB: PA 74°, Sep 1.3", VA/KB = 9.6/9.9. 5. V498 Per. Variable star of a2 CVn type. 6. HD 23885 (F0). 9. Suspected duplicity from Tycho data analysis (ESA 1997). 16. HD 24051 (F5). 28. Double or multiple star. CCDM 03529+3532 AB: PA 220°, Sep 4.6", VA/VB = 10.6/11.4. IDS 03464+3514 AB. 32. Strong evidence of variability in the Tycho data (ESA 1997). 33. HD 24286 (ICO). Variability suspected in the Tycho data (ESA 1997). 34. HD 24300 (AO). 35. HD 24299 (K2). 42. HD 24353 (A3). 43. HD 24354 (A). 44. HD 24397 (K0). Double or multiple star. CCDM 03543+3641 AB: PA 248°, Sep 2.8", VA/VB = 8.8/12.3. IDS 03478+3624 AB. 47. HD 24433 (K2). 54. HD 24517 (K2). 55. HD 24516 (G5). 69. HD 24664 (F8). 83. HD 24747 (F0). 91. Emission-line star: EM*MWC 729. 101. HD 24843 (K0). 102. HD 24855 (F8). 106. Apparent variability in the Tycho data; weak indication of duplicity, combined with indication of variability (ESA 1997). 108. HD 24912 (Oe5). £ Per. CSV 100364. NSV 1427. Micro-variable: Vmax/Vmin = 4.0/4.1. Emission-line star: EM*CDS 401. 112. Double star: Sep 4-5" (this paper). 113. HD 24960 (K0). 118. HD 24982 (AO). Double or multiple star. CCDM 03597+3849 AB: PA 320°, Sep 1.5", VA/VB = 6.5/9.2. IDS 03530+3832 AB, ADS 2910 AB. Duplicity induced variability from Hipparcos analysis (ESA 1997). 120. HD 24995 (F5). 121. -122. Visual binary. 126. HD 25023 (A2). California Nebula region: catalogs 329

135. Apparent variability in the Tycho data; weak indication of duplicity, combined with indication of variability (ESA 1997). 147. Variability suspected in the Tycho data (ESA 1997). Double or mul-

tiple star. CCDM 04009+3618 AB: PA 13°, Sep 0.2", VA/VB = 9.5/9.5. IDS 03543+3601 AB. 150. HD 25136 (K5). 155. HD 25152 (B9). 158. Star in triple system. CCDM 04015+3840 B: PA 287°, Sep 26.1". IDS 03549+3823 B. ADS 2932 B. 159. HD 25184 (K2). Star in triple system. CCDM 04015+3840 A. IDS 03549+3823 A. ADS 2932 A. Duplicity induced variability from Hip- parcos analysis (ESA 1997). 171. Star in double system. CCDM 04024+3627 A. Component B: PA

259°, Sep 10.1", Vk/VB = 9.6/12.5. IDS 03558+3611 A. 172. HD 25271 (A3). Possibly micro-variable from Hipparcos analysis: Hp (ma,x) I Hp (min) = 7.77/7.82 (ESA 1997). 174. HD 25307 (AO). 176. HD 25321 (G). 177. HD 25338 (G5). 178. HD 25354 (AOp). V280 Per. Periodic variable (ACV), P = 3.90 d, Hp(m&x)/Hp(mm) = 7.85/7.89 (ESA 1997). 180. HD 25411 (AO). Variable star of a2 CVn type. Hp (max)/Hp (mm) = 8.41/8.46, spurious variability due to duplicity (ESA 1997). CCDM 04038+3758 AB: PA 266°, Sep 4.4", VA/VB = 7.8/9.9. IDS 03572+3742. 186. HD 25454 (GO). 189. HD 25476 (A3). Probable astrometric binary from Hipparcos analysis (ESA 1997). 191. HD 25508 (AO). 194. HD 25518 (F5). 195. The star in a double system. CCDM 04049+3705 B: PA 278°, Sep 49.2", VA/VB = 8.2/9.6. IDS 03584+3648 B. 196. HD 25552 (F8). 197. HD 25538 (AO). Star in double system. CCDM 04049+3705 A. IDS 03584+3648 A. 198. HD 25553 (AO). Variability suspected in the Tycho data (ESA 1997). Star in double system. CCDM 04050+3644 A. Comp. B: PA 58°, Sep 6.5", VA/VB = 8.8/12.3. IDS 03584+3628 A. 201. HD 25643 (F0). 204. HD 25822 (AO). 205. HD 25821 (F0). 330 V. Straizys, K. Oemis, S. Bartasiute

206. HD 25847 (K0). 208. HD 25866 (KO). Double or multiple system. CCDM 04075+3803 CD (4 components). Comp. C: PA 210, Sep 233.1"; Comp. D: PA 307°, Sep 1.0"; VAIVBIVCIVV = 7.3/9.0/8.0/11.5. ADS 2992 AB. 209. HD 25893 (G5). V491 Per. NSV 1463. Variable of BY Dra type. //p(max)/Hp (mm) = 7.25/7.28, spurious variability due to duplicity (ESA 1997). CCDM 04075+3803 AB (4 components): VA/VB = 7.3/9.0. IDS 04009+3749 AB. ADS 2995 AB. 211. Apparent variability and suspected duplicity in the Tycho data (ESA 1997). 212. Suspected duplicity from Tycho data analysis (ESA 1997). 213. HD 25919 (GO). Apparent variability in the Tycho data. Weak indication of duplicity, combined with indication of variability (ESA 1997). 215. Variability suspected in the Tycho data (ESA 1997). 220. HD 25950 (AO). 221. Suspected duplicity from Tycho data analysis (ESA 1997). 222. HD 25975 (G5). 49 Per. High proper-motion star. 226. HD 25998 (F8). V582 Per. Periodic variable, P = 3.05 d, Hp [max) I Hp {mm) = 5.62/5.65 (ESA 1997). New Gamma Doradus star candidate (Aerts et al. 1998). Probable astrometric binary from Hipparcos analysis (ESA 1997). Physical multiple system (4 components): G1 161.1 + 160.1 AB; IDS 04019+3746. (Tokovinin A. A. 1997, A&AS, 124, 75 (Multiple Star Catalogue)). 228. Suspected duplicity from Tycho data analysis (ESA 1997). 232. HD 26080 (Ma). NSV 1475. CSV 100369. Periodic variable, P= 7.28 d, Hp (max)/Hp (mm) = 7.70/7.78 (ESA 1997). Suspected non-single star from Hipparcos analysis (ESA 1997). 234. HD 26103 (F8). 238. HD 26140 (K0).

(2) The trQ-method of matching 14 different reddening-free Q- parameters of a program star to those of about 7000 standard stars of various spectral and luminosity classes, metallicities and peculiar- ity types. This method does not give quantitative values of stellar parameters but selects instead some standard stars with a set of Q- parameters most similar to those of the program star. The degree of similarity is characterized by crQ, the standard deviation of the Q differences between the standard and the program stars. If the crQ value is sufficiently small, the parameters of the closest standard star may be prescribed to the program star. For photometry of normal California Nebula region: catalogs 331

Fig. 1. Identification chart for the California Nebula area (south-west section). 332 V. Straizys, K. Cernis, S. Bartasiute

Fig. 2. Identification chart for the California Nebula area (north-west section). California Nebula region: catalogs 333

0>n °o oW- l so fVOl miri + + +

Fig. 3. Identification chart for the California Nebula area (south-east section). 334 V. Straiiys, K. Oernis, S. Bartasiute

o ou- i o o< o OS 00 0r«01 + + + +

P. .*•

• •; S • » O • T oe K • • BO - o «0 • •• • n • • * 2 ¿0 ' ,2 00" . 3 — s; / • w * • Pt r- * s -o i —• o g^. • o - 8. i * • * : • I • •• • S s p • .S- i r.8 7 • • I eo e .t-i* "-00 • o o m S • is• a* i oo r- • (N V « • ' • •

e(S . ft* -—r • •

Fig. 4. Identification chart for the California Nebula area (north-east section). California Nebula region: catalogs 335 stars with 1% accuracy, AQ is usually of the order of ±0.01 — 0.02 mag for B-A-F-G stars and of ±0.02 - 0.03 mag for K-M stars. For the successful application of both methods we should be sure that Q-parameters of the standard stars are calculated with the color-excess-ratios which are valid for the given area. For the general Galactic dust layer and for dust clouds of moderate density, the so-called normal interstellar extinction law is applicable. In the vicinities of O-type stars and in the densest dust clouds, consider- able deviations from the normal law are found (for a discussion, see Straizys 1992). Consequently, before we begin doing the photometric classification of stars in any area, we must investigate its interstellar extinction law, i.e. the ratios of color excesses and the ratio of extinction to color excesses. The interstellar extinction law in the area north of the California Nebula has not been investigated in this respect so far. However, the area is at the edge of the Per OB2 association which was the sub- ject of several extinction law studies. Coyne, Gehrels & Serkowski (1974) have found that the stars £ Per and ( Per show normal values of the wavelength of maximum polarization, Amax at 0.59 and 0.58 /zm. This wavelength is proportional to the ratio R = AV/EB-V and gives R 3.2-3.3, which is close to the ratio for the normal interstellar extinction law. By application of the variable extinction and the color-difference methods Guetter (1977) has obtained a similar value (R « 3.2) for the Per OB2 association. Rossiger (1971) finds normal R ratio in the Per OB2 association from star counts in two colors. Friedemann (1973) finds the extinction bump at 220 nm to be normal for the stars £ Per, £ Per and e Per. At the same time, higher values of R were obtained in the area of the young open cluster IC 348. From UBVHKL photometry, Strom, Strom & Carrasco (1974) find by the color-difference method that in this area R increases from 3.0 to 4.1 with increasing reddening. In the region of the reflection nebula NGC 1333 Cernis (1990) has found R values from 3.5 to 4.0 by the maximum polarization method, using the observations by Turnshek et al. (1980). Bhatt (1986) has found larger than normal Amax polarization in the dust cloud B5, located 5° south-west from the California Nebula. In the California Nebula area the character of interstellar reddening law can be estimated from analysis of color indices in various photometric systems of the star £ Per (HD 24912, 07.5 III), the exciting star of the nebula. Its color excess is EB-V = 0.33, and 336 V. Straizys, K. Öernis, S. Bartasiute

Table 3. The interstellar extinction law for £ Per compared with the normal law from Straizys (1992).

EU—Y EP-Y EX -V EZ—V EY _S EY—V EY—V EY—V EY—V EY—V

£ Per 2.74±0.20 2.15±0.10 1.74±0.02 0.37±0,01 0.89±0.01 Normal law 2.62 2.14 1.76 0.36 0.84

the ratio R = 1.1 EY-K/EB-V is 3.4, i.e. slightly larger than is expected for the normal extinction law (i? = 3.15). However, the ratio EU-B/EB-V — 0.67 is very close to the normal ratio 0.72, determined from observations of 0-type stars (Straizys 1992). The UBV data taken are from Nicolet (1978) and K is taken from Castor & Simon (1983). The observed color indices of £ Per in the Vilnius system are given in Table 2. Since the intrinsic color indices of 07-08 stars in this system are zeros, all color excesses are equal to observed color indices. Table 3 gives the ratios of color excesses for £ Per and for the normal interstellar extinction law (Straizys 1992). The rms errors listed are typical of the photometric determination of color-excess- ratios and are taken from Straizys, Corbally & Laugalys (1999). The conclusion is that £ Per exhibits the normal extinction law within the errors of determination. The larger ratio of Ey-s/Ey-v most probably is the result of some emission in the Ha line on which the S passband is centered. The normal interstellar extinction law for £ Per was also found by Goy (1972) from its observation in the Geneva seven-color system. Consequently, there are no firm indications that the interstellar extinction law in the California area is abnormal. This conclusion is also expected from general considerations of the causes of grain size modification: (1) the area does not contain regions with very high dust density where the coalescence of dust grains could take place, and (2) no hot luminous stars are present, whose radiation would be capable to remove small dust grains. Therefore, in our calculation of Q-parameters we use the normal ratios of color excesses and in the calculation of interstellar extinction from color excesses we use the normal R ratio. California Nebula region: catalogs 337

Fig. 5. A comparison of the photometric distances of 23 stars with the distances determined from the Hipparcos parallaxes. Error boxes for all stars are shown. For the photometric distance determinations the following errors are taken: 25 % for B-A-F-G stars and 15 % for K stars.

The two methods applied for the determination of spectral classes and absolute magnitudes give compatible results. Spectral classes usually agree within 1 decimal subclass. Luminosity classes usually are the same when determined by both methods. The color excesses Ey-v were calculated as differences between the observed Y-V and the intrinsic (y-V)o taken from Straizys (1992) for stars of various spectral and luminosity classes. Distances of stars were derived as usual:

51ogr = V-Mv+ 5 - REy-v, where R = 4.16 for the normal interstellar extinction law. 338 V. Straizys, K. Cernis, S. Bartasiute

Table 4. Results of photometric classification, determination of color excesses, extinctions and distances of the stars.

No. Photom. Other MV EY-V AV r A sp. type sp. type pc mag

1. A5V A4 +1.4 0.25 1.04 290 0.02 2.* A3 IV A2, A2II + B6 3. F2V F5 +3.0 0.07 0.29 210 0.01 4. GOV F9 +4.3 0.01 0.04 140 0.02 5. Ap Ap (Si,Sr) 6. A7V F0, F0 +2.2 0.06 0.25 68 0.01 7. K4III K5 +0.9 0.19 0.79 370 0.02 8. F5V F8 +3.5 0.03 0.12 200 0.01 9. F5IV-V F5, GO +3.1: 0.16 0.66 260 0.01 10. K2III K2 +1.9 0.24 1.00 220 0.02 11. KOIII K0 -0.3 0.21 0.87 970 0.02 12. FOV A7V.A9V +2.7 0.06 0.25 171 0.01 13. F5V +3.5 0.16 0.66 360 0.01 14. * K1 Il-Ib K2,R0 -3.6 0.21 0.87 1570 0.03 15. KOIII 0.0 0.21 0.87 2120 0.05 16. F4V F2, F5: +2.5 0.03 0.12 179 0.01 17. G8IV K0 +2.5 0.36 1.50 163 0.01 18. KOIV +1.8 0.20 0.83 310 0.01 19. K2III K5 +0.6 0.48 2.00 156 0.02 20. G8III GO, G5 +0.8 0.09 0.37 350 0.02 21. KOIII I<2 +0.7 0.23 0.96 600 0.03 22. G8V G5,K0 +5.6 0.02 0.08 47 0.02 23. KOIII KO +0.4 0.22 0.92 350 0.01 24. A3 V A1 V, A1IV +1.4 0.13 0.54 530 0.03 25. F2V F5 +3.0 0.10 0.42 149 0.01 26. A4V A2, Am +1.6 0.18 0.75 360 0.01 27. AO V AO, A2,A0V +0.7 0.25 1.04 410 0.02 28.* A6 V FO, GO 29. G8IV I<2 +2.7 0.30 1.25 129 0.01 30. KOIII KO +1.9 0.12 0.50 450 0.01 31. G2V GO +4.6 0.00 0.00 126 0.01 32. K2III I<5, K2 0.0 0.27 1.12 500 0.02 33. G9III KO +0.7 0.42 1.75 142 0.01 34. B7V AO, B6 V -0.3 0.14 0.58 480 0.02 35. KOIII K0,K2 +1.0 0.14 0.58 270 0.02 36. B8V AO, B8, B9.5 V +0.7 0.17 0.71 410 0.02 37. G3V GO +4.7 0.00 0.00 132 0.02 38.* M5: III 39. G3V GO +4.7 0.05 0.21 105 0.01 40. F9V F8 +4.2 0.00 0.00 130 0.01 California Nebula region: catalogs 339

Table 4 (continued)

No. Photom. Other My Ey-V Av r a sp. type sp. type pc mag

41. G3V F8 +4.7 0.02 0.08 150 0.02 42. A3 IV A3, A7: +0.8 0.13 0.54 240 0.01 43. A5V A, A5: +1.8 0.06 0.25 230 0.01 44. KOIII K0 +1.0 0.12 0.49 280 0.01 45. G4V G5 +4.9 0.03 0.12 131 0.02 46. F5V: F2 +3.5 0.08 0.33 270 0.01 47. K3III K2 -0.5 0.23 0.96 400 0.03 48. G5V GO +5.0 0.01 0.04 88 0.02 49. K0.5 III K2 +1.2 0.13 0.54 520 0.01 50. A2V AO +1.2 0.30 1.25 660 0.02 51. K1.5V I<2 +6.2 0.04 0.17 60 0.02 52. K0.5III K5 +1.2 0.16 0.66 520 0.02 53. F8V GO +4.0 0.09 0.37 120 0.01 54. G9III K0, K2 +0.6 0.22 0.92 240 0.03 55. F8V G5 +4.0 0.00 0.00 93 0.01 56. F5V GO +3.5 0.12 0.49 290 0.01 57. F6V +3.7 0.19 0.79 178 0.04 58. K2.5III K2 +0.5 0.31 1.29 400 0.01 59. KOIV KO +2.3 0.17 0.71 210 0.02 60. GOV GO +4.3 0.12 0.50 173 0.02 61. A7: V A7 +2.2 0.39 1.62 340 0.03 62. F2V +3.0 0.23 0.96 310 0.02 63.* G8: III 64. F4V F5, F8 +3.4 0.15 0.62 270 0.01 65. K2.5III +0.3 0.54 2.25 590 0.02 66. G8IV KO +3.1 0.20 0.83 110 0.01 67. G8IV G5 +2.5 0.25 1.04 190 0.03 68. G6IV KO +3.0 0.17 0.71 160 0.01 69. F8V F8,F8V +4.0 0.00 0.00 73 0.01 70. G3V +4.7 0.03 0.12 161 0.02 71. F6V F8 +3.6 0.00 0.00 151 0.01 72. K4III +0.9 0.85 3.54 400 0.03 73. G6V GO +4.7 0.02 0.08 83 0.01 74. G5V +5.0 0.08 0.33 195 0.02 75. F7V F8 +3.9 0.04 0.17 210 0.02 76. F5V F5 +3.5 0.04 0.17 162 0.01 77. FOV GO +2.7 0.31 1.29 250 0.02 78. K2.5III K +0.1 0.28 1.16 570 0.03 79. K2 III K5 +0.6 0.43 1.79 500 0.03 80. F2V F5,F8 +3.0 0.14 0.58 148 0.01 340 V. Straizys, K. Cernís, S. Bartaêiutè

Table 4 (continued)

No. Photom. Other Mv EY-V Ay r a sp. type sp. type pc mag

81. K3.5V +6.9 0.03 0.12 124 0.05 82. F5V F2,F5 +3.5 0.04 0.17 162 0.01 83. F5V F0, F2 III +3.5 0.00 0.00 44 0.01 84. K1III K2, K5 +0.4 0.26 1.08 320 0.02 85. K1III K2 +0.4 0.25 1.04 460 0.02 86. K3III +0.5 0.42 1.75 1020 0.04 87. G9V +5.7 0.07 0.29 190 0.01 88. K3III K2,K5 -0.3 0.17 0.71 330 0.02 89.* M2: III K5 90. K2III +0.6 0.57 2.37 940 0.03 91. B2 Ve 07:, B5, Be -2.3 0.60 2.50 980 0.03 92. F5 V +3.5 0.18 0.75 270 0.01 93. A8V A5,F0, A7V +2.3 0.12 0.50 220 0.01 94. G3V +4.7 0.07 0.29 280 0.01 95. F5V +3.5 0.23 0.96 320 0.02 96. G9V G5 +5.9 0.00 0.00 76 0.01 97. A2V A5 +1.2 0.57 2.37 600 0.02 98. G4: V F2 0.02 99. G2IV A5 +3.4 0.10 0.42 250 0.01 100. A3 V B9 +1.4 0.45 1.87 700 0.01 101. KO.5 III KO.gKl +0.7 0.02 0.08 127 0.01 102. F8IV F8, GO +2.9 0.03 0.12 151 0.01 103. Fl IV +2.2 0.50 2.08 460 0.02 104. A3 V +1.4 0.56 2.33 530 0.02 105. F5V F8 +3.5 0.09 0.37 118 0.01 106. AO V AO, A2,B9 V +0.7 0.26 1.08 460 0.03 107.* G 108. O-BO 07 Ve, 07.5 Illf -5.2 0.27 1.12 420 0.01 109. A2 V A, B9 V +1.2 0.17 0.71 800 0.03 110. A7 V F5, A7 V +2.2 0.20 0.83 310 0.02 111. F5V F8 +3.5 0.06 0.25 177 0.01 112. A3 V A2, AO V +1.4 0.29 1.21 380 0.01 113. G9III G5, KO +0.8 0.06 0.25 240 0.01 114. F3V F5 +3.2 0.11 0.46 230 0.02 115. A2V AO, A2, A1V +1.2 0.31 1.29 270 0.01 116. G4: V +5.0: 0.22: 0.92: 200: 0.02 117. K2 III +0.9: 0.30: 1.25: 350: 0.02 118.* AO V AO, Al, Al Vp: 119. K3V +6.6 0.02 0.08 91 0.04 120. F4V F5 +3.4 0.03 0.12 122 0.01 California Nebula region: catalogs 341

Table 4 (continued)

No. Photom. Other My EY-V AV r A sp. type sp. type pc mag

121.* A2p? A2 122.* A8m? A5 123. G8III K5 +1.6 0.41 1.70 250 0.02 124.* F5: 125. F6V F0 +3.7 0.20 0.83 260 0.02 126. A7V A2, A5, A7V +2.2 0.16 0.67 136 0.01 127. A3 III B9, A5 +0.3 0.63 2.62 670 0.03 128. AO V AO, A2, AO V +0.7 0.19 0.79 460 0.01 129. G5V +5.0 0.15 0.62 210 0.03 130. K1.5III K7 0.0 0.29 1.21 600 0.03 131. A7V F5 +2.2 0.30 1.25 300 0.01 132. F6V F5 +3.6 0.06 0.25 186 0.01 133. Al V AO, AO V +1.0 0.23 0.96 320 0.01 134.* M3: III 135. Al V AO V, Al V +1.0 0.20 0.83 410 0.01 136. K5 III K5 +0.2 0.51 2.12 300 0.05 137. F7V F +3.9 0.18 0.75 167 0.01 138. F8V F5, GO +4.0 0.01 0.04 123 0.01 139. GO IV F8, GO +3.1 0.03 0.12 210 0.02 140. Kl III G5, KO +1.7 0.20 0.83 210 0.01 141. F8V F5,F8 +4.0 0.00 0.00 116 0.01 142. G2V +4.0 0.28 1.16 200 0.02 143. G6IV-V G5, KO +3.7 0.06 0.25 158 0.02 144.* B5 V: B5 -0.5 0.54 2.24 500 0.03 145. F5V +3.5 0.05 0.21 200 0.01 146. K2V F8,K2 +6.4 0.06 0.25 63 0.03 147.* A A3, A5, A5 V 148. GOV +4.3 0.16 0.66 290 0.04 149. A5V A2, A5V +1.8 0.17 0.71 330 0.01 150. K2 III K5 -0.3 0.09 0.37 310 0.03 151. G2V F2 +4.6 0.05 0.21 179 0.01 152. A2V B9 +1.2 0.51 2.12 370 0.01 153. G5 III GO, G5 +1.7 0.14 0.58 170 0.01 154. F5V F0,F2 +3.5 0.00 0.00 165 0.01 155. B9.5V B9.5 V, AO V +0.7 0.02 0.08 134 0.01 156. G9 III K2 +1.1 0.18 0.75 640 0.02 157. K3 III K7 +0.5 0.32 1.33 420 0.02 158. G8IV K2 +3.1 0.06 0.25 145 0.01 159. K3 II-III K2 -0.6 0.40 1.66 220 0.02 160. GOV GO +4.3 0.06 0.25 143 0.01 342 V. Straizys, K. Cernís, S. Bartasiuté

Table 4 (continued)

No. Photom. Other Mv Ey-v Ay r a sp. type sp. type pc mag

161. Kl V: +6.1: 0.12 0.50 171 0.05 162. G5V +4.7 0.06 0.25 156 0.02 163. F2V A5,F0 +3.0 0.12 0.50 210 0.01 164. G7V +5.4 0.00 0.00 200 0.03 165.* A-F 166.* A7 A8 167. A3 V A5 +1.8 0.58 2.41 440 0.03 168. A3 V A2 +1.4 0.13 0.54 560 0.02 169. A5V A3, A5, A6 V +1.8 0.13 0.54 280 0.02 170.* M2: III 171. G9III-IV G5, K0 +1.8 0.15 0.62 220 0.01 172. A7V A3 +2.2 0.07 0.20 115 0.02 173. A5V A5 +1.8 0.30 1.25 410 0.01 174. A5V AO, A2 III +1.8 0.06 0.25 220 0.01 175. A5V A5, A7 V +1.8 0.19 0.79 260 0.01 176. FOV F0,F2 +2.7 0.10 0.42 160 0.01 177. G9III-IV G5 +1.4 0.08 0.33 128 0.01 178.* A AO, AOp 179. F5V F2 +3.5 0.04 0.17 180 0.01 180.* A2 AOp, AI III 181. K2 III K7 +0.9 0.25 1.04 440 0.02 182. G9III KO +1.2 0.25 1.04 410 0.02 183. G2IV +2.9 0.30 1.25 260 0.02 184. G5V GO +5.0 0.06 0.25 150 0.03 185. F5V F5 +3.5 0.07 0.29 126 0.01 186. F7V F5, GO +3.9 0.00 0.00 87 0.01 187. G7V GO, KO +5.4 0.00 0.00 80 0.01 188. G8III KO -0.4 0.21 0.87 630 0.02 189. A7V A3 +2.5 0.05 0.21 90 0.01 190. F9V F8 +4.2 0.00 0.00 97 0.01 191. B9V AO, B8 V +0.4 0.17 0.71 240 0.01 192. F6V F8 +3.6 0.05 0.21 136 0.01 193. F7V F8, AO +3.9 0.06 0.25 136 0.01 194. F2III F5, F5IV +1.7 0.10 0.42 160 0.04 195. K2 III K2 +0.8 0.10 0.42 460 0.02 196. F2V F5,F8 +3.0 0.07 0.29 122 0.01 197. A4 V AO, A5 V +1.6 0.03 0.12 182 0.01 198. Al V AO +1.0 0.09 0.37 410 0.01 199. G2V G5 0.02 200. K3V K7 +6.6 0.00 0.00 56 0.01 California Nebula region: catalogs 343

Table 4 (continued)

No. Photom. Other Mv Ey-v Ay r a sp. type sp. type pc mag

201. F0 III FO +1.4 0.08 0.33 169 0.01 202. G7V GO, G5 +5.4 0.04 0.17 107 0.02 203. K2III +1.0 0.18 0.75 550 0.02 204. A3 V AO, A2, A3 +1.4 0.07 0.29 330 0.01 205. F0V A7, FO +2.7 0.06 0.25 164 0,01 206. K0 III KO + 1.1 0.05 0.21 210 0.01 207. * K2III: 208. * K2 III KO, K2 209. * G9 V G5, K2 210. G4V GO +4.9 0.08 0.33 132 0.01 211. A5V A2, A5 V +1.8 0.16 0.67 310 0.02 212. * A A2, A5 213. F8V GO +4.0 0.01 0.04 103 0.01 214. K0 III KO +0.7 0.08 0.33 520 0.01 215. F6V F5, GO +3.6 0.13 0.54 143 0.01 216. G5IV GO +2.9 0.29 1.21 161 0.02 217. F4V A7 +3.4 0.01 0.04 230 0.01 218. F8V +4.0 0.06 0.25 320 0.02 219. G9III G5, KO +0.5 0.10 0.42 430 0.01 220. AO V AO, A2,B8 V +0.7 0.19 0.79 320 0.02 221. K4III K5 -1.6 0.27 1.12 950 0.02 222. KOIV G5, Kl III +2.2 0.02 0.08 57 0.01 223. Kl III K5 +0.2 0.24 1.00 550 0.02 224. G3IV F8 +4.7 0.03 0.12 113 0.02 225. K4V K7 +6.9 226. F8V F8, F7 V +4.0 0.00 0.00 20 0.01 227. G8IV G5 +3.8 0.13 0.54 110 0.01 228. F8V GO +4.0 0.09 0.37 182 0.01 229. K2III-IV KO +1.7 0.11 0.46 210 0.01 230. G8III-IV KO +1.9 0.22 0.92 180 0.01 231. GO III A7, KO +2.9 0.28 1.16 220 0.03 232. * M3: III MO, Ml 233. Al IV AO, A2 V +1.0 0.23 0.96 670 0.01 234. F7IV F8 +2.7 0.01 0.04 101 0.01 235. G9III-IV G8 +2.1 0.22 0.92 250 0.01 236. F5V F8 +3.5 0.10 0.42 150 0.01 237. A2V AO +1.2 0.17 0.71 420 0.01 238. G9IV KO +2.9 0.05 0.21 95 0.01 344 V. Straizys, K. Cernis, S. Bartasiute

NOTES: 2. Variable and binary (see Notes to Table 2). 14. HDE 279088 (K2). The star photometrically seems like a luminous K1 giant. AGK3 and PPM catalogs give the spectral class R0. How- ever, we do not find any indication in the literature that the star is carbon-rich. The Vilnius diagram QuPYV,Qxzs, which is used for the identification of late-type carbon-rich stars, also shows no indication of the carbon enrichment. 28. Binary (see Notes to Table 2). 38. Classification uncertain. UV color indices of low accuracy. 63. Classification uncertain. UV color indices of low accuracy. 89. Classification uncertain. 107. Classification uncertain. Probably, color indices are of low accuracy. 118. Multiple (see Notes to Table 2). 121. -122. Visual binary, classification of both stars uncertain. 124. Classification uncertain. UV color indices of low accuracy. 134. Classification uncertain. Ultraviolet and violet color indices of low accuracy. 144. Alternative classification: sdF7; however, in this case the reddening of the star contradicts its distance. 147. Multiple star (see Notes to Table 2). 165. Classification uncertain. UV color indices of low accuracy. 166. Classification uncertain. UV color indices of low accuracy. 170. Accurate absolute magnitude determination impossible. 178. Variable (see Notes to Table 2). 180. Binary and variable (see Notes to Table 2). 207. Classification uncertain. 208. Multiple star (see Notes to Table 2). 209. Multiple and variable (see Notes to Table 2). 212. Suspected binary (see Notes to Table 2). 232. Classification uncertain. Variable (see Notes to Table 2).

Table 4 gives the results of photometric classification: spectral types, absolute magnitudes, color excesses Ey-v, extinctions Ay, distances r in parsecs and, in the last column, the classification accuracy aQ discussed in p. 12. The expected rms errors are: ±0.03 mag for Ey-v, ±0.1 mag for Ay and 15-25% for distance. In Table 4, the values of distances at r > 200 pc are rounded to the nearest number multiple of 10. We collected spectral types determined for the stars in the area by other authors. In most cases, only spectral classes determined California Nebula region: catalogs 345 from low dispersion objective-prism spectra are available. The data were taken from the HD catalogue, the HDE catalogue (Cannon & Mayall 1949, Nesterov et al. 1995), Seyfert et al. (1960), Voroshilov et al. (1985), Ungerer et al. (1985), the PPM catalogue (Róser & Bastian 1991) and the Hipparcos and Tycho catalogues (ESA 1997). For some of the stars in the area Guetter (1977) gives more precise spectral types in the MK system determined from slit spectra. All these spectral types are given in the column named "Other sp. type". Evidently, most of them are of considerably lower accuracy than the spectral types determined in this paper. We have found 23 stars in the area which are nearer than 250 pc and for which Hipparcos parallax measurements are available. Dis- tances of these stars are intercompared in Fig. 5. Differences of the photometric and trigonometric distances are within the error boxes (the standard deviation ±25 pc), and no systematic effects are seen. A comparison of absolute magnitudes determined photometrically and from the trigonometric parallaxes (with interstellar extinction taken into account) gives the standard deviation ±0.42 mag and no systematic difference.

ACKNOWLEDGMENT. We are grateful to O. Paupers for observation of some stars in the area.

REFERENCES

Aerts C., Eyer L., Kestens E. 1998, A&A, 337, 790 Bartasiüté S. 1999, Baltic Astronomy, 8, 443 Bhatt H. C. 1986, MNRAS, 222, 383 Cannon A. J., Mayall M. W. 1949, The Henry Draper Extension, Annals of Harvard College Obs., Vol. 112 Castor J. I., Simon T. 1983, ApJ, 265, 304 Cernis K. 1987, Ap&SS, 133, 355 Cernis K. 1990, Ap&SS, 166, 315 Cernis K. 1993, Baltic Astronomy, 2, 214 Coyne G. V., Gehrels T., Serkowski K. 1974, AJ, 79, 581 ESA 1997, The Hipparcos and Tycho Catalogues, ESA SP-1200 Friedemann C. 1973, AN, 294, 257 Goy G. 1972, A&A, 21, 11 346 V. Straizys, K. Cernis, S. Bartasiute

Guetter H. H. 1977, AJ, 82, 598 Khavtassi J. Sh. 1960, Atlas of Galactic Dark Nebulae, Abastumani Ob- servatory, Tbilisi, Georgia Lynds B. T. 1962, ApJS, 7, 1 Meistas E., Straizys V. 1981, Acta Astron., 31, 85 Nesterov V.V., Kuzmin A. V., Ashimbaeva N.T., Volchkov A.A., Röser S., Bastian U. 1995, The Henry Draper Extension Charts: a Catalogue of Accurate Positions, Proper Motions, Magnitudes and Spectral Types of 86 933 stars, A&AS, 110, 367 Nicolet B. 1978, A&AS, 34, 1 Nikonov V. B. 1976, Izvestija Crimean Obs., 54, 3 Perryman M. A. C., Brown A. G. A., Lebreton Y. et al. 1998, A&A, 331, 81 Röser S., Bastian U. 1991, PPM Star Catalogue, Vol. 1, Astron. Rechen- Institut Heidelberg Rössiger S. 1971, AN, 293, 211 Seyfert C. K., Hardie R. H., Grenchik R. T. 1960, ApJ, 132, 58 Straizys V. 1982, Pisma AZh, 8, 481 Straizys V. 1992, Multicolor Stellar Photometry, Pachart Publishing House, Tucson, Arizona Straizys V., Cernis K., Meistas E. 1992, Baltic Astronomy, 1, 125 Straizys V., Cernis K., Hayes D. S. 1985, Ap&SS, 112, 251 Straizys V., Cernis K., Bartasiute S. 2001, A&A (accepted) Straizys V., Corbally C. J., Laugalys V. 1999, Baltic Astronomy, 8, 355 Straizys V., Glagolevskij Y. V., Romanyuk I. I., Bychkov V. D. 1982a, Pisma AZh, 8, 183 Straizys V., Kuriliene G., Jodinskiene E. 1982c, Bull. Vilnius Obs., No. 60, 3 Straizys V., Meistas E. 1980, Acta Astron., 30, 541 Straizys V., Meistas E. 1981, AZh, 58, 367 = Soviet Astron. 25 No. 2 Straizys V., Wisniewski W.Z., Lebofsky M.J. 1982b, Ap&SS, 85, 271 Strom S. E., Strom K. M., Carrasco L. 1974, PASP, 86, 798 Turnshek D. A., Turnshek D.E., Craine E. R. 1980, AJ, 85, 1638 Ungerer V., Mauron N., Brillet J., Rieu N.-Q. 1985, A&A, 146, 123 Voroshilov V. I., Guseva N. G., Kalandadze N. B., Kolesnik L. N., Kuznetsov V.l., Metreveli M. D., Shapovalov A.N. 1985, California Nebula region: catalogs 347

Catalogue of BV Magnitudes and Spectral Classes of 6000 Stars, Naukova Dumka Publishers, Kiev Zdanavicius K. 1975, Bull. Vilnius Obs., No. 41, 3 Zdanavicius K. 1996, Baltic Astronomy, 5, 549 Zdanavicius K., Cerniene E. 1985, Bull. Vilnius Obs., No. 69, 3