1. BAA VSS Oct 14th 2011

2.  Data collected from 25/10/2003 to 30/3/2008  This during 76 nights  In between Cygnus work of higher priority  25,000 images, 21,000 pass quality tests  Longest night 11-1/2/2006- 12 hrs 31mins  Start at el=45.6° to 79.9° and down to 16.7° BAA VSS Oct 14th 2011

3. Location in Auriga 05 18 +41 50 capella BAA VSS Oct 14th 2011

5.  Started October 2000 - first two years gaining experience  66,400 quality-filtered images since Aug 2003 in main Cygnus area (area ‘a’)  But also some data in 8 contiguous areas in Cygnus (10,000)- Each 2.8 degrees square, 7.84 sq. Degrees  Plus 25,000 in Auriga (total area 86 sq. degrees)  The area ‘a’ has more than 220,000 measurable stars  17,000 of those have 5 year light curves  1022 variable stars found in area ‘a’ so far BAA VSS Oct 14th 2011

6.  Outline of data pipeline  Ways of finding variable stars with examples  So far (11/10/11) I’ve found 178  63 eclipsing binaries, 64 slow variables  37 fast variables, 1 Cepheid, 13 misc  Six of those are in the GCVS BAA VSS Oct 14th 2011

7.  Collect data- 1 image every 46seconds  Rename files- Fits convert-extract time info  Convert to APL, x10, dark subtraction, flat division  Find brightest 6,000 stars, quality assessment, log data -vimp  Calculate picture coefficients (144 stars, 4 th order poly, 16 coefficients)  Probe images at starlist ra, dec positions* (60,000 or 28,000)  Collect pixel sets for each star, add to previous and store- singlesets  Collect average sets, 2401 per image, 20 images averaged *Probing by ra and dec allows us to make average sets centred at fixed ra/dec and also to observe any large-enough proper motions. BAA VSS Oct 14th 2011

8.  Store Fits and processed images  Probe pixel-sets to create diameter sets  Each star is measured at in 14 diameters  3x3 pix and 4 to 16 diameter  Noise is measured in quiet dates and optimum diameter evaluated  Each star is then ratioed to each of 10 local comparison stars BAA VSS Oct 14th 2011

9.  At this point a number of obvious variable stars pop out  So, re-evaluate the star ratios  Repeat a few times  End result: good light curves for all stars with several comparison stars for each BAA VSS Oct 14th 2011

10.  For the Auriga data these are 20,086 x14 magnitude values from 76 dates  From a nominal 28,738 stars  8.08 billion data values  Explain nominal! BAA VSS Oct 14th 2011

11.  Fast noise  Slow noise  Scattery noise  Spiky noise  Overlay analysis  Fourier Analysis  Star colour hints BAA VSS Oct 14th 2011

12. 735 data points- rms 14.5 mmag BAA VSS Oct 14th 2011 This is the image to image variation

13. 735 data points BAA VSS Oct 14th 2011

15. SD 15.8mmag

16. SD 3.1 mmag BAA VSS Oct 14th 2011

17. Mag 13.8 not var Mag 13.8 varMag 15.4 var

18. 0345678910111213141516 14855483124181411 12141923 3761621389560382014 1516 1718 380124114109108106 105104 103104 105 418191150881041441982222172111711311026451 diameter star BAA VSS Oct 14th 2011 In mmags

19. BAA VSS Oct 14th 2011

20. Star 380 101 pixels square star 418 BAA VSS Oct 14th 2011

21. Each of 76 dots is the average of one night The rms variation over those 1619 days is 12mmag BAA VSS Oct 14th 2011 2003/4 2005/6 2006/7 2007/8

22. BAA VSS Oct 14th 2011

24. GCVS Variable Stars in Stan’s Auriga Area StarTypem P (d) Sp. myid SX AurEB8.38-9.141.2100855B3 V+ B5 V 41 SY AurDCEP8.74-9.4010.14465F5-F8 61 ER AurDCEP11.17-11.8015.6973 742 V414 Aur Be8.20-8.30 B2 Vne 27 V425 AurEB7.62-7.901.568583 B5 12 V489 AurLB:12.5-13.3 876 BAA VSS Oct 14th 2011

26. My range is 0.519- gcvs is 0.66 BAA VSS Oct 14th 2011

27. Range 0.46mag---- gcvs is 0.63 mag BAA VSS Oct 14th 2011

29. 35 0.260 632 0.190 STARE 1697 0.390 4006 0.460 47 0.590 iras 665 0.180 STARE 1843 0.330 4048 0.470 141 0.210 761 0.130 2107 0.250 4055 0.150 184 0.086 825 0.130 2174 0.590 4761 0.660 CGCS 206 0.450 iras 876 0.870 2253 0.000 8016 0.660 258 0.041 963 0.420 2292 0.960 8402 0.290 264 0.612 1021 0.600 2309 0.250 8463 0.460 356 0.250 STARE 1154 0.380 CGCS 2366 0.440 CGCS 8904 0.600 382 0.166 1165 0.170 2381 0.570 10812 0.800 384 0.250 STARE 1217 0.420 2533 0.250 11404 0.180 409 0.500 1239 0.110 2541 1.340 CGCS 13694 0.650 459 0.122 1311 0.240 STARE 2585 0.120 15009 0.920 495 0.810 1318 0.760 STARE 2686 0.410 15268 1.030 536 0.312 1389 0.250 STARE 2855 0.410 19924 0.850 548 0.280 1421 0.150 STARE 3362 0.500 22947 0.930 588 0.270 STARE 1490 0.180 3775 0.000 26863 0.500 CGCS BAA VSS Oct 14th 2011 64 found so far

30. 2541 1.340 CGCS 47 0.590 iras 1154 0.380 CGCS 665 0.180 STARE 15268 1.030 2174 0.590 1843 0.330 1490 0.180 2292 0.960 2381 0.570 536 0.312 11404 0.180 22947 0.930 409 0.500 8402 0.290 1165 0.170 15009 0.920 3362 0.500 548 0.280 382 0.166 876 0.870 26863 0.500 CGCS 588 0.270 STARE 1421 0.150 STARE 19924 0.850 4048 0.470 35 0.260 4055 0.150 495 0.810 4006 0.460 356 0.250 STARE 761 0.130 10812 0.800 8463 0.460 384 0.250 STARE 825 0.130 1318 0.760 STARE 206 0.450 iras 1389 0.250 STARE 459 0.122 4761 0.660 CGCS 2366 0.440 CGCS 2107 0.250 2585 0.120 8016 0.660 963 0.420 2309 0.250 1239 0.110 13694 0.650 1217 0.420 2533 0.250 184 0.086 264 0.612 2686 0.410 1311 0.240 STARE 258 0.041 1021 0.600 2855 0.410 141 0.210 2253 0.000 8904 0.600 1697 0.390 632 0.190 STARE 3775 0.000 BAA VSS Oct 14th 2011

31. Carbon star CGCS 878 BAA VSS Oct 14th 2011

33. 11459 5.3 16783 5 1055 3.47 V407 6077 1.81 V575? 14833 1.81 955 1.72 V573 12001 1.69 11293 1.58 2086 1.37 V362 4851 1.32 3403 1.29 18915 1.28 17886 1.25 11496 1.11 2550 1.07 Slow Red Variables in Cygnus area ‘a’ Star id magr starid magr BAA VSS Oct 14th 2011

34.  Fast noise  Slow noise  Scattery noise  Spiky noise --------  Overlay analysis  Fourier Analysis  Star colour hints BAA VSS Oct 14th 2011

37. 4 years data BAA VSS Oct 14th 2011

38. 4 years data BAA VSS Oct 14th 2011

39. 4 years data BAA VSS Oct 14th 2011

43. 1.210090

44. 12030.300769811.114126462.3676812520 30460.32084911.197991732.43417260 243770.40048411.2099126162.575817390 90620.4112124171.31368201172.656524720 41560.477371971.359942203.216327650 3800.54648641.44931003.2176637490 23490.55862571.51428833.56138110 28240.6048121.568419404.226146300 44530.620847231.626868404.245450880 21470.6568530331.6522207235.4559858030 29010.71764104811.68961076.98661580 124970.82487651.776417469.6162190 163810.89934142981.787576083.9373280 110090.9508134242.010350074430 59261.003888042.22796132076230 206101.049873032.3468044200132630 star period star period star period star

45.  Good at the fast ones  Only one long night needed  But three is better  I used 2170 2202 and 2211 which are  10/12/2005 and 11/1, 20/1 2006  11.8 12.5 and 11.6hrs long  Longest: el=45.6° to 79.9° down to 16.7°  It’s very quick – 28,000 stars in 40mins BAA VSS Oct 14th 2011

46. 867 6 0 0 12 0 0 7 5 0 14 13 0 6 5 0 13 12 0 1 0 1864 6 0 0 7 0 0 10 0 0 7 0 0 0 0 0 0 0 0 1 0 yes 3678 6 0 0 6 0 0 0 0 0 0 0 0 15 7 0 2 4 0 0 1 5323 5 0 0 6 0 0 5 0 0 4 0 0 14 5 0 2 4 0 0 1 5507 9 6 0 8 9 0 10 0 0 12 0 0 10 0 0 10 0 0 0 1 8990 5 0 0 11 0 0 9 5 0 3 2 0 0 0 0 0 0 0 0 0 9911 19 7 0 6 5 0 12 7 0 6 7 0 16 0 0 6 0 0 1 0 yes 11503 5 0 0 7 0 0 0 0 0 0 0 0 5 0 0 4 0 0 1 0 yes First, I tried looking at those where 6th or higher harmonic dominated: 37 found so far- incomplete BAA VSS Oct 14th 2011

47. Auto scan criterion: peak> 5 times 90%rms BAA VSS Oct 14th 2011

49. 11.0932 cycles/day amplitude 29mmags BAA VSS Oct 14th 2011

51. 9.90947 cycles/day amplitude 137 mmags BAA VSS Oct 14th 2011

52. ER Auriga --DCEP BAA VSS Oct 14th 2011

53. 4 yr plot BAA VSS Oct 14th 2011

54. 1171 Red squares-Cepheid Green Triangle –W VIR

55. BAA VSS Oct 14th 2011

57. According to the Catalogue of Components of Double and Multiple Stars (CCDM) of Dommanget et al. (2002), this is a visual binary star with r = 0.2”, q = 16°, and with V 1 = V 2 = 9.5.///// Hartkopf et al. (1994), in ‘ICCD speckle observations of binary stars’ give r = 0.211”, q = 356.7° for the epoch 1991.9049. ///////The Washington Visual Double Star Catalogue (Mason et al., 2001-11) gives r = 0.3”, q = 27° for the epoch 1907. This yields dq / dt = -0.357°/yr  P ~ 1000 yr. On the present information, we see the visual binary orbit roughly face-on (i « 90°), so the orbit is not co- planar with the orbit of the eclipsing binary, which, of course, must be nearly edge-on (i ~ 90°).

58. BAA VSS Oct 14th 2011 THE END