COMMISSIONS 27 AND 42 OF THE IAU INFORMATION BULLETIN ON VARIABLE STARS Number 3855 Konkoly Observatory Budapest 8 March 1993 HU ISSN 0374 - 0676 NEW VARIABLE STARS IN CYGNUS, LYRA AND VULPECULA The following work is an evaluation of an area of 20d x 15d centred at 19h46m +30d in my series of 32 fields in the Milky Way. Two fields are previously described in IBVS (Dahlmark, 1982,1986). Twenty-one plate pairs (103aD +GG 11 and 103aO) exposed between 1967 and 1982 were collected and treated in the same way as described previously (Dahlmark, 1982). In addition, 86 exposures of the field were made on Technical Pan film 4415+Schott 495 (1mm) during the period 1985-1992. Two 4"x5" images of one hour exposure were taken immediately after each other with the Perkin-Elmer lens 65/305 mm. During 1990, 4 exposures were made on IIIaJ plates without filter and simultaneously with TP film. TP films and IIIaJ plates were always hypersensitized. During 1987 and 1990 the area was exposed with a 200/210/300 mm Schmidt camera and a casette with 10d field (TP film+Wr 9 filter). 16 stars were photographed twice with my Newtonian reflector (210/1660 mm) and an image intensifier camera of the micro channel type. Filter combination was Schott BG 12 (2 mm)+BG 28 (1 mm) for B magnitudes and Schott GG 495 (1 mm)+BG 38 (2 mm) for V magnitudes (T Max 400 film was used). All magnitude estimations were made with a step scale under the films in a stereomicroscope. The scale is calibrated with the magnitudes obtained from NGC 6823, 6834, 6871 and 6882/5 in the publication of Hoag et al. (1961). Around each new variable the magnitudes of about 10 comparison stars were estimated mainly from the 103aD plates and the Schmidt exposures. Six Schmidt negatives covering the area were enlarged (with negative images) to the scale 1d=60 mm. A grid of epoch 1950 was drawn from the positions from SAO catalog. The coordinates of the new variables were determined from this grid. For 60 stars my coordinates were compared with those from IRAS. The average deviation in both R.A. and decl. is +-13". In this survey 80 stars are published. 73 of them are quite new variables. The results are based on more than 8700 magnitude estimations. Rough B-V color estimations could be made for 44 stars. 24 stars have only a lower limit for B-V. 12 stars are without B-V estimations. The average uncertainty is estimated to be +-0.2. It depends mainly on the fact that the B magnitudes are very close to the plate limit. Three different methods are used for the B-V estimations. 1. 34 stars from 103aO and 103aG +GG 11 plates 2. 21 stars from IIIaJ and TP+S 495 plates and films 3. 16 stars on T Max 400 film from the image intensifier camera Table 1. New variables in Cyg, Lyr and Vul. Plate centre 19h46m -30d. No R.A. Decl. m_V B-V Type Epoch P Notes (1950) (1950) max min 2440000 (d) LD 106 190122 +3353.5 11.2 <15.0 1.7 M 7560 459 c LD 107 190415 +2530.0 12.5 <16.0 0.5 M? 6910 338 c LD 108 190523 +3138.0 12.6 14.4 2.0 SR 6985 308? LD 109 190538 +3541.7 12.0 13.0 1.2 IB - - LD 110 190602 +3618.3 11.9 13.5 1.6 IB - - 1 LD 111 190710 +3248.3 11.3 12.3 1.5 SR 6990 457 LD 112 190806 +2315.9 13.2 <15 0 ? 7315 234 c 1 LD 113 190908 +2439.4 12.7 16.0 1.2 M 6620 302 c LD 114 191035 +2305.5 11.8 <15 - M 5620 335 c 1 LD 115 191117 +2653.6 13.8 <15.3 - M 7060 282 c 1 LD 116 191251 +3655.8 11.5 14.8 1.5 M 6650 290 1 LD 117 191954 +2300.8 12.2 15.2 2.3 M 6945 180 c LD 118 191959 +2616.7 13.4 <16.2 - SR 6740 395 LD 119 192037 +2552.8 12.5 <15.2 >0.5 M 7085 292 c LD 120 192109 +2421.7 10.5 13.2 3.3 M 6740 342 c 2 LD 121 192146 +2621.3 13.3 14.7 0.8 IB - - 1 LD 122 192228 +3213.3 11.7 <15.2 2 SR 6620 531 3,1 LD 123 192352 +2632.3 13.2 <15.2 1 SR 6930 407 1 LD 124 192412 +3456.9 11.6 <15.2 1.7 M 7280 405 LD 125 192518 +3517.3 11.6 <15.2 1.6 M 7015 247 4 LD 126 192541 +2436.4 11.9 15.2 1.7 M 6945 182 c 1 LD 127 192813 +2803.2 12.4 <15.2 >2 M 6953 370 2,1 LD 128 192903 +2324.0 11.4 15.2 2.4 M 6920 363 LD 129 192942 +2844.0 12.7 14.5 1.3 SR - - LD 130 193359 +3409.2 12.3 15.2 >2 M 6700 358 1 LD 131 193713 +2337.5 11.7 <15.0 >1.3 M 7300 292 c 1 LD 132 193813 +2326.0 14.0 15.0 - I - - LD 133 193858 +2445.6 12.1 <15.2 2.1 M 7300 260 LD 134 194009 +3006.6 12.0 <15.2 2.0 M 6700 362 11 LD 135 194141 +3421.9 10.4 13.0 3.0 SR 6730 560 5,2 LD 136 194155 +3222.2 10.2 14.7 4.0 M 6990 562 c 1,2 LD 137 194427 +3132.8 11.9 15.0 2.3 M 6700 371 c LD 138 194446 +2801.1 12.1 <15.2 >1.8 M 6890 227 1,6 LD 139 194527 +3538.4 12.7 14.6 0.8 SRA? 6680 304 c 1 LD 140 194712 +2230.2 13.0 <15.5 1.3 M 7000 470 c 1 LD 141 194713 +2924.0 10.0 12.6 2.7 M 7380 523 2 LD 142 194757 +3541.3 11.4 <15.2 1 M? 6640 452 1 LD 143 194758 +2225.0 13.2 <15.2 >0.7 M 7280 400 LD 144 194808 +2618.8 13.0 15.0 >1.5 - - 1,7 LD 145 194910 +2602.9 12.7 <15.2 - M? 7133 444 11 LD 146 194933 +3240.0 13.0 <15.1 >0.9 M 6650 394 c LD 147 194958 +2701.5 12.0 15.0 1.6 SR 6650 480 8 LD 148 195149 +2300.7 13.0 15.0 1.3 6950 200 9 LD 149 195303 +2223.3 12.1 <15.0 >1.3 M 6945 294 10,11 LD 150 195347 +2213.1 11.3 14.5 0.7 SRD? 6885 478 c 1 LD 151 195419 +2308.4 12.4 14.2 1.4 SRB 7350 404 LD 152 195607 +3146.7 14.1 <15.2 >0.6 M 7400 600 LD 153 195613 +2933.1 12.6 <15.2 1.5 M 6670 386 1 LD 154 195710 +3105.1 11.9 15.1 >2.8 M 7040 288 c 1 LD 155 200029 +2943.3 11.8 15.1 >2 M 7086 585 c LD 156 200113 +3115.6 12.8 13.7 1.2 I - - LD 157 200123 +2946.6 11.8 13.6 2.0 SR - - LD 158 200414 +2518.9 12.5 <15.2 1.8 M 7005 204 c LD 159 200420 +3509.0 12.6 15.1 >1.8 M 7310 460 11,2 LD 160 200443 +3349.4 12.5 15.1 >1.4 M 6920 355 12 LD 161 200621 +2527.3 13.8 <15.2 - I - - 11 LD 162 200744 +3149.9 13.0 <15.2 >1 M 6925 437 c 1 LD 163 200756 +2529.2 11.8 15.1 1.6 M 6720 214 c 1 LD 164 200851 +2243.0 12.8 15.0 1.5 M 7355 284 1,13 LD 165 201030 +2427.8 12.4 <15.2 1.8 M 7050 263 c LD 166 201334 +2517.7 10.3 <15.2 2.8 M 6660 262 c 1,2 LD 167 201357 +2404.4 11.6 <15.2 >1.8 M 6720 452 LD 168 201930 +3015.1 13.0 <15.2 >0.5 SR 6645 403 1 LD 169 201931 +2905.1 12.4 15.0 - SR 6620 420? LD 170 201957 +2213.8 13.0 14.9 0.7 SRD 6640 148 1 LD 171 202403 +2759.7 12.8 <15.0 - 6945 430? 14 LD 172 202518 +2407.5 12.0 <16.0 1.8 M 6760 440 15 LD 173 191555 +3420.4 12.0 14.8 1.9 M 7375 269 c LD 174 191940 +2437.4 12.9 <15.8 - SR 7730 323 1 LD 175 192809 +2404.0 14.2 <16.0 - M 6980 250 LD 176 194635 +3158.6 13.0 15.1 - M 6650 275 LD 177 194844 +2921.3 12.8 15.2 >1 M 6930 317 c 1 LD 178 195023 +3042.4 12.5 14.2 >1.7 M 7050 250 16 LD 179 195229 +3356.7 12.5 <15.2 1.4 M 7056 230 c 1 LD 180 135417 +3522.2 13.1 <15.0 >0.8 M 6980 382 17 LD 181 195531 +3035.0 13.9 <15.2 - SR 6690 375 1 LD 182 195553 +2241.3 13.0 14.7 >1 I - - 1 LD 183 195624 +3535.1 12.3 14.8 >2 SRB 6619 103 18 LD 184 201616 +2629.8 11.8 <15.2 >1.6 M 6715 345 c LD 185 201633 +2825.7 13.5 15.0 >0.7 M 7715 298 c Notes 1. Close faint star (5" -30" ) may influence the magnitude estimations at minimum. 2. Possibly carbon star. 3. Small light variations in 1967-82. 4. P changes +-5 days. 5. P changes between 450 and 560 d. 6. P changes between 215-240 d, average 227 d. LD 138=AI Vul. 7. Light variations only in 1967-70, max 2440030. 8. Long intervals constant 15.0 at min. 9. P between 195-205 d. Fast variations of 0.3 magn in one hour. 10. P increases from 288 to 300 d between 1986 and 1992. 11. Not found on 103aD plates in 1967-82. 12. P changes from 362 to 355 days between 1970 and 1990. 13. 0.5 magn variations in one hour. 14. Nova-like? Only one sharp max 2446945. Nothing in 1967-82. 15. P change +-30 d. 16. P change (between 240-290 days). 17. LD 180=V1460 Cyg. P increases from 367 days (1968) to 382 days (1990). 18. LD 183=V1464 Cyg. V1460 and V1464 are given with wrong coordinates in GCVS (3' and 5'). c means that the period P is constant between 1967 and 1992. <15.2 means that the star is fainter than 15.2m. LD 120=TAV 1921+24=CCS 2728. The Astronomer, Vol. 28, No. 332,182,1991. LD 135=TAV 1941+34. The Astronomer, Vol. 26, No. 311, 237,1990. LD 142=V1000 Cyg. LD 164=HX Vul. In GCVS given with 10' wrong coordinates. [FIGURE 1] [FIGURE 2] [FIGURE 3] and Newtonian telescope. I cannot find significant differences between the three methods. It is curious that IIIaJ and TP gives almost the same values as 103aO and 103aD. Perhaps the reason is that both IIIaJ and TP have their sensibility shifted about 500 angstrom to the red compared with 103aO and 103aD. From 6720 magnitude estimations on TP film (1985-1992) the light curves of 80 variable stars have been drawn. From these curves the types, epoch and period (P) are estimated. The shape of these curves is correct, but the Technical Pan "V" magnitudes could be too bright, especially for red stars. To find out the correction to be made I exposed a TP 2415 Hy film +Wr 9 with the Newtonian telescope on NGC 6866. This cluster has about 22 stars close to magn 13.5 with B-V from 0.15 to 1.85 (Hoag et al., 1961). I found a roughly linear connection between V and B-V for TP film and yellow filter corr. =0.4 (B-V). This means that the carbon stars with B-V=3 or 4 could be 1 to 1.5 magn. too bright in the Table. For instance V=10.2-14.7 and B-V=4 is given for the star LD 136. Perhaps it is more correct with V=11.8-16.3. But no corrections have been made in the table nor in the graphs, while B-V are rough and only known for 44 stars. The finding charts were obtained with the Schmidt camera in September 1987. Lennart DAHLMARK Montlaux F-04230 St Etienne les Orgues France References: Dahlmark, L., 1982, I.B.V.S., No. 2157 Dahlmark, L., 1986, I.B.V.S., No. 2878 Hoag, A. et al., 1961, Publ. U.S. Naval Obs., 17, 7 [BIBCODE 1961PUSNO..17....1H ]