STT Doubles with Large ΔM – Part VI: Cygnus Multiples

Vol. 12 No. 6 October 1, 2016 Journal of Double Star Observations Page 519

Wilfried R.A. Knapp

John Nanson

Star Splitters Double Star Blog Manzanita, Oregon [email protected]

Abstract: The results of visual double star observing sessions suggested a pattern for STT doubles with large delta_M of being harder to resolve than would be expected based on the WDS catalog data. It was felt this might be a problem with expectations on one hand, and on the other might be an indication of a need for new precise measurements, so we decided to take a closer look at a selected sample of STT doubles and do some research. Of these objects we found three rather complex multiples in Cygnus of special interest so we decided to write a separate report to have more room to include the non STT components as well. Again like for the other objects covered so far several of the components show parameters quite different from the current WDS data.

research sources were used for this section of this pa- Change in Procedure per, the first of which was W.J. Hussey’s Micrometrical With the availability of URAT1 for plate solving in Observations of the Double Stars Discovered at the northern skies we decided to switch from UCAC4 Pulkowa, published in 1901, which provided prelimi- to URAT1 to get results of higher precision and avoid nary historical information on each of the stars. Hus- problems with proper motion issues. We changed fur- sey’s book includes his observations and measures of ther the plate solving setup from Linear Fit to 4th-Order all the stars originally listed in Otto Wilhelm Struve’s Fit resulting in a substantial reduction of the average 1845 Pulkovo Catalog, as well as data beginning with plate solving error due to better adaption to the Correct- the date of first measure and continuing through the ed Dell-Kirkham optics used for imaging. following years up to 1900. That data, plus inclusion of Introduction the background for the Pulkovo Catalog, makes Hus- As follow up to our previous STT reports, we con- sey’s book a valuable source of reference. Also con- tinue in the constellation of Cygnus with 3 multiples sulted was S.W. Burnham’s A General Catalogue of with a rather complex structure (see Table 1). All val- Double Stars Within 121° of the North Pole, Part II, for ues are based on WDS data as of the beginning of 2016. information on each of the three stars. In addition, Bill Hartkopf of the USNO graciously provided the text Further Research files for 425 and STT 433. Following the procedure for the earlier parts of our STT 425 Otto Struve measured the first two report we concluded again that the best approach would discovered components of STT 425 in 1847 (27.7° and be to check historical data on all objects, observe them 12.18"), which he designated AB. However S.W. visually with the target of comparing with the existing Burnham discovered a much closer companion in 1890 data and obtain as many images as possible suitable for (119.9° and 2.30") with the Lick 36 inch refractor (also photometry. observed by Hussey with the Lick 12 inch refractor), Historical Research and Catalog Comparisons and that pair became the new AB, while the pair Otto Each of the three multiple stars in this survey have Struve discovered became AC. The star now designat- notable aspects worth further investigation. Three main

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STT Doubles with Large ΔM – Part VI: Cygnus Multiples

Table 1. WDS catalog Data at the Beginning of 2016 for the Selected STT Objects

Name ID RA Dec Sep PA M1 M2 ΔM BU449 AB 21395+4144 21:39:28.710 +41:43:36.00 6.2 14 7.67 12.70 5.03 STT447 AC 21395+4144 21:39:28.710 +41:43:36.00 13.7 176 7.67 12.20 4.53 BU449 AD 21395+4144 21:39:28.710 +41:43:36.00 18.7 248 7.67 13.00 5.33 STT447 AE 21395+4144 21:39:28.710 +41:43:36.00 28.6 45 7.67 8.48 0.81 ABH148 AG 21395+4144 21:39:28.710 +41:43:36.00 33.8 337 7.67 14.80 7.13 ABH148 AH 21395+4144 21:39:28.710 +41:43:36.00 74.2 263 7.67 13.79 6.12 ABH148 AI 21395+4144 21:39:28.710 +41:43:36.00 92.7 271 7.67 11.65 3.98 ABH148 AJ 21395+4144 21:39:28.710 +41:43:36.00 71.3 94 7.67 13.88 6.21 ABH148 AK 21395+4144 21:39:28.710 +41:43:36.00 75.0 49 7.67 11.65 3.98 FOX262 EF 21395+4144 21:39:30.520 +41:43:36.00 42.0 46 8.48 11.56 3.08 STT433 AB 21179+3454 21:17:55.070 +34:53:48.80 14.2 222 4.36 10.00 5.64 STT433 AC 21179+3454 21:17:55.070 +34:53:48.80 21.2 181 4.36 9.95 5.59 SLE382 AD 21179+3454 21:17:55.070 +34:53:48.80 57.0 308 4.36 12.00 7.64 BU9011 AE 21179+3454 21:17:55.070 +34:53:48.80 34.2 67 4.36 10.00 5.64 STT433 BC 21179+3454 21:17:54.290 +34:53:37.10 10.1 141 10.00 10.00 0.00 BU1210 AB 21001+4841 21:00:06.610 +48:40:45.90 1.4 104 7.34 12.20 4.86 STT425 AC 21001+4841 21:00:06.610 +48:40:45.90 17.9 27 7.34 10.80 3.46 STT425 AE 21001+4841 21:00:06.610 +48:40:45.90 44.9 16 7.34 10.61 3.27 STT425 CD 21001+4841 21:00:07.409 +48:41:01.707 4.5 132 10.5 10.90 0.40 ed as the D component was discovered by Struve in Table 2. Data for STT 425 AB (BU 1851, which he measured from the star he had previ- 1210) from the WDS ously designated as B (now C) at a position angle of 135°, but didn’t include a separation, although Hussey Date PA Sep (1901, p. 174) includes a comment that Struve came up 1890.630 119.9 2.30 with a distance of 4.11". That leaves the E component, 1898.420 117.2 2.35 which was first measured by S.W. Burnham in 1898 at 1898.600 120.2 2.54 18° and 45.17". 1901.623 117.2 2.40 The last two measures of the AB pair discovered in 1903.550 118.6 2.03 1890 by Burnham were made in 1924 and shows a sur- 1924.810. 117.1 2.24 prising difference in position angle and separation, as 1924.900 103.9 1.43 seen in Table 2. We were able to track down the publi- cation containing the 1924.900 measure, verified the data listed in the WDS text file matched the published Table 3. Data for STT 425 AC from the WDS data, and also found it was made using the 28 inch re- Date PA Sep fractor at Greenwich by R.T. Cullen. Because of the 1847.490 27.7 12.18 4.86 magnitude differential between the two compo- 1867.000 29.9 12.72 nents, the secondary is so well hidden in the glare of the 1868.430 29.7 12.81 primary that it has not been detected in the numerous 1890.630 28.6 13.80 photographic surveys we’ve checked (NOMAD-1, 1898.450 28.0 13.80 UCAC4, URAT1, Hipparcos, GSC 2.3, Tycho, and US- 1898.548 45.2 13.37 NO A-2 and B-1). Our efforts at photographing the 1898.582 46.8 13.55 secondary met with the same results. A new measure 1898.600 28.0 13.98 of the AB pair would be welcome if for no other reason 1900.640 26.9 14.35 than to verify that the 1924.900 PA is an anomaly. 1901.623 27.8 14.13 A comparison of the various components of STT 1902.540 28.4 14.33 425 shows very little change in PA and separation with 1903.570 29.1 14.08 the exception of the AC pair (Table 3). Since O. 1907.880 28.2 14.44 Struve’s 1847 discovery, the pair has widened from 1924.810 27.4 14.91 12.18" to 17.85" as of the most recent measure in the 1999.470 26.7 17.79 WDS (2003). Our measure for the pair was 18.142", 2000.690 27.6 17.53 2003.488 26.9 17.85

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STT Doubles with Large ΔM – Part VI: Cygnus Multiples

which indicates the separation has continued to widen. after 2006. The two position angles of 1898.548 and 1898.582 The component which is now designated as E was stand out as anomalous in the data in Table 3. The first noticed by S.W. Burnham in 1874 (Burnham, WDS text file shows those measures were made by 1874, p. 46). He estimated the distance and PA of what Hussey and are from his 1901 book used as a reference is now the AE pair, and repeated those comments in his for this paper. A look at Hussey’s data on p. 174 of that 1906 catalog (shown in Figure 1, where he used a des- book shows three 1898 measures with PA’s of 28.1°, ignation of D). It appears he never returned to make 29.2°, and 28.4°, which average out to the 28.6° num- specific measures of the two stars. The out of sequence ber he lists in the book for 1898.57. His three 1898 9011 number was added by the WDS at some point af- separation measures were 14.10", 13.97", and 13.92", ter 2006. (A first look at the 1874 source referred to in which average out to the 14.0" number listed in the the WDS text file failed to turn up Burnham‘s observa- book for the 1898.57 date. Consequently it appears the tion, but a closer look at the MNRAS titles in the SAO/ PA’s of 45.2° and 46.8° in the WDS text file are incor- NASA ADS catalog led to the discovery that Burn- rect. ham’s article had been split into two parts, with the second part listed under an erroneous title. We’ve includ- STT 433 (Upsilon Cygni) This is a complex mul- ed both ADS bibliographic codes in the sources section tiple star with a complex past, comprised of five com- of this paper.). ponents and two additional WDS designations beyond STT 433: SLE 382 for the AD pair and BU 9011 for STT 447 With a total of eleven components you the AE pair. almost need a scorecard to keep track of all the mem- The AB pair was first seen by John Herschel in bers of this system, especially since the designations 1827, who provided estimated measures of 210° and have been frequently revised as new components were 21". Otto Struve added the first specific measures in added. Table 4 shows the designations in use in 1898 1849, which were 219.4° and 14.91”. John Herschel when Hussey published his Micrometrical Observations was also the first to look at the AC components, again of the Double Stars Discovered at Pulkowa and the in 1827, and again estimated the measures (180° and changes made in 1906 by Burnham (which are also the 30"), followed by Otto Struve with actual measures in designations currently used in the WDS) in his General 1849 (177.6° and 21.16"). The AD/SLE 382 pair is Catalogue of Double Stars. credited to G. Soulie, but the WDS text file data shows The observational history of STT 447 goes back to it was first noticed by Philip Fox in 1912. However, September 17, 1783, when William Herschel cataloged our search through the WDS source could only turn up it as H III 110. He measured what are now the AC and this short comment by Fox: “Star (12.5) in 309° : AE pairs, but also described H III 110 as quadruple. 1’ ” (Fox, 1915, p. 199). Soulie’s astrographic Although he didn’t provide any measures for it, the measures were made in 1982 according to the text file, fourth star to which he referred – “Position almost in and it appears Fox’s observation was added to the WDS line with the two largest.” (Herschel, 1784, p. 90) – can

Figure 1. Burnham's entry for STT 433.A

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STT Doubles with Large ΔM – Part VI: Cygnus Multiples

Table 4. Changes in STT 447 Designa- been made from photographic plates since the WDS tions Between 1898 and 1906 date of first measure is 1895. The AG, AH, AI, AJ, and AK pairs are all designated as ABH 148. Hussey Current There has been very little change in the separations Designation Designation of the eleven components of this system, which is not AD AB surprising considering the distance of STT 447 A is 815 light years. The WDS Catalog assigns a code of “U” to AC AC each of the STT 447 components, which characterizes AE AD all members as non-physical. Visual Observations AB AE Both Nanson and Knapp made visual observations of the stars included in this report. Nanson used a be identified by looking at Figure 2, where AB and E 152mm f/10 refractor, while Knapp utilized 140mm (Herschel’s two “largest” stars) are in line with the star and 185mm refractors as well as a masking device to now labeled as F. evaluate what could be seen at lesser apertures. In addition to the STT 447 designation, there are three more WDS designations within the group. S.W. STT 425 (Cyg): Knapp looked at STT 425 twice. Burnham discovered and measured the B and D compo- During the first observation, using the masking device nents in 1876 with the 18 ½ inch refractor at the Dear- he could detect C with the aperture limited to 60mm, born Observatory. The AB and AD pairs are designat- suggesting it’s slightly brighter than the WDS value of ed as BU 449. Philip Fox brought William Herschel’s 10.80. The limiting aperture during the second obser- fourth star into the system in 1895 when he measured vation was 80mm, which would indicate a confirmation the distance and position angle between it and the E of the WDS magnitude. Nanson observed STT 425 component, resulting in EF being designated as Fox once with the six inch refractor and found C (10.80) 262. and E (WDS magnitude 10.61) appeared to be about the That leaves the last five components, G through K, same magnitude, both of which were slightly brighter which were added in 1987 by H.A.Abt, although the than a comparison star with a Vmag of 11.586, indicat- first measures of the AI and AK pairs appear to have ing the WDS magnitudes are about right.

Figure 2. Aladin image of STT 447 with all components labeled.

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STT Doubles with Large ΔM – Part VI: Cygnus Multiples

The CD pair (separation of 4.5", WDS magnitudes then plate solved with Astrometrica with URAT1 refer- of 10.80 and 10.90) were resolved at 152x and 304x. D ence stars with Vmags in the range 10.5 to 14.5mag. appeared to be about half a magnitude fainter than C. It The RA/Dec coordinates resulting from plate solving was obvious the CD pair is not the evenly matched pair with URAT1 reference stars in the 10.5 to 14.5mag indicated by the WDS magnitudes. range were used to calculate Sep and PA using the for- mula provided by R. Buchheim (2008). Err_Sep is cal- STT 433 (Cyg): Nanson observed STT 433 once culated as SQRT(dRA^2+dSep^2) with dRA and dDec and was able to see B and C clearly at 84x, but lost both as average RA and Dec plate solving errors. Err_PA is of them in the glare of the primary when adding addi- the error estimation for PA calculated as arctan tional magnification because of poor seeing conditions. (Err_Sep/Sep) in degrees assuming the worst case that Both of those stars were close matches for a compari- Err_Sep points in the right angle to the direction of the son star with a Vmag of 9.901, suggesting their WDS separation means perpendicular to the separation vec- magnitudes (10.0 and 9.95, respectively) should be rea- tor. Mag is the photometry result based on UCAC4 ref- sonably close. He spent several minutes searching for erence stars with Vmags between 10.5 and 14.5mag. D and finally saw it at 253x with averted vision, leading th Err_Mag is calculated as square root of (dVmag^2 + to the conclusion that it may be close to 13 magnitude (2.5*Log10(1+1/SNR))^2) with dVmag as the average since it should have been easier to see if the WDS mag- Vmag error over all used reference stars and SNR is the nitude of 12.0 is correct. He searched repeatedly for E, signal to noise ratio for the given star. The results are but never saw it, suggesting the WDS magnitude of shown in Table 5. 10.0 is incorrect. Knapp observed STT 433 twice. During the first Summary observation he could detect B at 200x with the aperture Tables 6 and 7 compare the final results of our re- reduced to 93mm, suggesting B is at least half a magni- search with the WDS data that was current at the time tude fainter than the WDS’s 10.0. C could be seen at we began working on our current group of stars. 200x with the aperture reduced to 80mm, also suggest- In Table 6 the results of our photometry have been ing it may be half a magnitude fainter than the WDS’s averaged for each star. Because we’re aware that both 9.95. During the second observation, B was visible at the NOMAD-1 and the UCAC4 catalogs are frequently 180x with the aperture reduced to 90mm, again sug- consulted when making WDS evaluations of magni- gesting it may be fainter than the WDS value of 10.0. tudes changes, the data from those catalogs has also

STT 447 (Cyg): Knapp observed this complex been included for each of the stars. multiple star twice. Using the aperture mask, each time Red type has been used in Tables 6 and 7 to call he found C appeared to be about a magnitude brighter attention to significant differences from the WDS data. than the WDS value of 12.20. Nanson looked at STT With regard to Table 6, those magnitudes that differ by 447 once during conditions of poor transparency. Us- two tenths of a magnitude or more from the WDS val- ing magnifications of 152x and 253x on the six inch ues have been highlighted. In Table 7 differences in refractor, he also found C to be about a magnitude separation in excess of two-tenths of an arc second are brighter than the WDS value based on comparison with highlighted, as are all position angles which differ by the 11.56 magnitude F component. C was a bit easier more than a degree. to see than I (WDS magnitude of 11.65). Subsequent to our measures, as a quality check for Looking at the other components, he concluded the our astrometry results we turned to the URAT1 catalog WDS magnitude of the I component is correct or very for the most recent precise professional measurements close to correct based on a comparison star with a available. We used its coordinates to calculate the Sep Vmag of 11.244. The I component seemed to be fainter and PA for all objects in this report for which URAT1 than 11.56 magnitude F, but the combined brightness of data was available and compared these values with our F and K (WDS value of 11.65) very likely makes F ap- results, which are shown below in Table 8. pear brighter than it is (K was hidden in the glare of F). Acknowledgements D was glimpsed once with averted vision – given the The following tools and resources have been used poor transparency, it’s possible D is slightly brighter for this research: than the WDS value of 13.0.  Washington Double Star Catalog as data source for Photometry and Astrometry Results the selected objects Several hundred images taken with iTelescope re-  iTelescope: Images were taken with mote telescopes were in a first step plate solved and stacked with AAVSO VPhot. The stacked images were (Continued on page 534)

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STT Doubles with Large ΔM – Part VI: Cygnus Multiples

1 2 3 4 5 6 7 8 9 5 6 7 9

Notes Notes Notes

N 5 5 5 N 5 5 5 5 N 5 5 5 5

15 20 20

images (usually (usually images

621 632 639 630 621 632 700 639 648 621 632 700 639 648

ine below the indi- the below ine

and exposure time time exposure and

rr values. The N N The values. rr

Date Date Date

e l e

es es

l E l

0.07 0.05 0.08 0.07 0.05 0.09 0.08 0.07 0.05 0.09 0.08

dVmag dVmag dVmag

SNR SNR SNR

14.97 17.00 15.34 69.08 52.78 42.06 40.65 24.88 19.52

339.58 400.85 284.05 339.58 102.48 400.85 102.83 309.59 284.05 339.58 400.85 309.59 284.05

Err Err Mag Err Mag Err Mag

0.070 0.099 0.050 0.080 0.080 0.105 0.068 0.095 0.070 0.071 0.050 0.051 0.090 0.091 0.080 0.083 0.074 0.075 0.070 0.075 0.050 0.057 0.090 0.100 0.080 0.097 0.074 0.084

Mag Mag Mag

7.475 7.491 7.494 7.487 7.475 7.491 7.291 7.494 7.438 7.475 7.491 7.291 7.494 7.438

12.662 12.480 12.733 12.625 11.204 11.222 11.140 11.167 11.183 13.120 13.091 13.127 13.144 13.121

PA PA PA

Err Err Err Err

0.805 0.614 0.812 0.750 0.346 0.261 0.523 0.350 0.382 0.257 0.194 0.387 0.260 0.283

PA PA PA

13.718 13.878 14.084 13.894

176.570 176.398 176.477 176.307 176.438 247.894 247.963 248.144 247.782 247.945

Err Err Sep Err Sep Err Sep

0.085 0.064 0.086 0.079 0.085 0.064 0.128 0.086 0.094 0.085 0.064 0.128 0.086 0.094

Sep Sep Sep

6.042 5.974 6.073 6.030

14.035 14.078 14.027 14.079 14.055 18.946 18.949 18.937 18.962 18.949

dDec 0.06 0.04 0.05 dDec 0.06 0.04 0.10 0.05 dDec 0.06 0.04 0.10 0.05

0.051 0.067 0.067

dRA dRA dRA

0.06 0.05 0.07 0.06 0.05 0.08 0.07 0.06 0.05 0.08 0.07

0.061 0.066 0.066

Dec Dec Dec

41 43 36.03 43 41 41.90 43 41 36.04 43 41 41.84 43 41 36,04 43 41 41.93 43 41 36.04 43 41 41.89 43 41 36.03 43 41 22.02 43 41 36.04 43 41 21.99 43 41 35.84 43 41 21.84 43 41 36,04 43 41 21.99 43 41 35.99 43 41 21.96 43 41 36.03 43 41 28.90 43 41 36.04 43 41 28.93 43 41 35.84 43 41 28.79 43 41 36,04 43 41 28.87 43 41 35.99 43 41 28.87 43 41

RA RA RA

21 39 28.727 39 21 28.855 39 21 28.727 39 21 28.855 39 21 28.723 39 21 28.855 39 21 28.726 39 21 28.855 39 21 28.727 39 21 28.802 39 21 28.727 39 21 28.806 39 21 28.729 39 21 28.806 39 21 28.723 39 21 28.804 39 21 28.727 39 21 28.805 39 21 28.727 39 21 27.159 39 21 28.727 39 21 27.158 39 21 28.729 39 21 27.159 39 21 28.723 39 21 27.155 39 21 28.727 39 21 27.158 39 21

A B A B A B A B A C A C A C A C A C A D A D A D A D A D

BU 449 BU 449 BU

STT 447 STT

Table 5. Photometry and astrometry results for the selected STT objects. Date is the Bessel epoch in 2015 and N is the number the is N and 2015 in epoch Bessel the Dateis objects. STT selected the for results astrometry and Photometry 5. Table imag of number with used telescope the indicates column Notes the in iT values. reported the used for time) 1s exposure with th in given are images used all over results The average Acknowledgements). See telescopes: used the of given (Specifications individua the over square mean root as calculated is images used all over estimation error The bold. and red in stacks vidual epoch. Bessel average the Date and used images of number total the gives line summary the in column

Table 5 continues on next page.

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STT Doubles with Large ΔM – Part VI: Cygnus Multiples

11 12 13 14 15 16 17 18 19 20 21 22 23 24 25

Notes Notes Notes

N 5 5 5 5 N 5 5 5 5 N 5 5 5 5

20 20 20

621 632 700 639 648 621 632 700 639 648 621 632 700 639 648

Date Date Date

0.07 0.05 0.09 0.08 0.07 0.05 0.09 0.08 0.07 0.05 0.09 0.08

dVmag dVmag dVmag

SNR SNR SNR

8.26

13.22 12.91 10.44 26.61 27.19 15.68 12.21

339.58 341.74 400.85 318.26 309.59 242.38 284.05 184.05 339.58 400.85 309.59 284.05 339.58 400.85 309.59 284.05

Err Err Mag Err Mag Err Mag

0.070 0.070 0.050 0.050 0.090 0.090 0.080 0.080 0.074 0.074 0.070 0.106 0.050 0.095 0.090 0.153 0.080 0.128 0.074 0.122 0.070 0.081 0.050 0.064 0.090 0.112 0.080 0.117 0.074 0.096

Mag Mag Mag

7.475 8.453 7.491 8.459 7.291 8.275 7.494 8.459 7.438 8.412 7.475 7.491 7.291 7.494 7.438 7.475 7.491 7.291 7.494 7.438

14.598 14.766 14.798 14.308 14.618 13.782 13.733 14.055 13.885 13.864

PA PA PA

Err Err Err Err

0.167 0.127 0.253 0.170 0.185 0.144 0.109 0.218 0.146 0.159 0.065 0.049 0.099 0.066 0.072

PA PA PA

44.206 44.565 44.464 44.566 44.450

336.611 336.321 336.601 336.561 336.523 262.476 262.550 262.768 262.459 262.563

Err Err Sep Err Sep Err Sep

0.085 0.064 0.128 0.086 0.094 0.085 0.064 0.128 0.086 0.094 0.085 0.064 0.128 0.086 0.094

Sep Sep Sep

29.142 28.956 28.976 28.971 29.011 33.841 33.784 33.658 33.744 33.757 74.460 74.346 74.434 74.373 74.403

dDec 0.06 0.04 0.10 0.05 dDec 0.06 0.04 0.10 0.05 dDec 0.06 0.04 0.10 0.05

0.067 0.067 0.067

dRA dRA dRA

0.06 0.05 0.08 0.07 0.06 0.05 0.08 0.07 0.06 0.05 0.08 0.07

0.066 0.066 0.066

Dec Dec Dec

41 43 36.03 43 41 56.92 43 41 36.04 43 41 56.67 43 41 35.84 43 41 56.52 43 41 36,04 43 41 56.68 43 41 35.99 43 41 56.70 43 41 36.03 43 41 07.09 44 41 36.04 43 41 06.98 44 41 35.84 43 41 06.73 44 41 36,04 43 41 07.00 44 41 35.99 43 41 06.95 44 41 36.03 43 41 26.28 43 41 36.04 43 41 26.40 43 41 35.87 43 41 26.50 43 41 36,04 43 41 26.28 43 41 36.00 43 41 26.37 43 41

RA RA RA

21 39 28.727 39 21 30.542 39 21 28.727 39 21 30.542 39 21 28.729 39 21 30.542 39 21 28.723 39 21 30.539 39 21 28.727 39 21 30.541 39 21 28.727 39 21 27.527 39 21 28.727 39 21 27.515 39 21 28.729 39 21 27.535 39 21 28.723 39 21 27.524 39 21 28.727 39 21 27.525 39 21 28.727 39 21 22.133 39 21 28.727 39 21 22.142 39 21 28.731 39 21 22.135 39 21 28.723 39 21 22.137 39 21 28.727 39 21 22.137 39 21

A E A E A E A E A E A G A G A G A G A G A H A H A H A H A H

STT 447 STT 148 ABH 148 ABH Table 5 (continued). Photometry and astrometry results for the selected STT objects. ... objects. STT selected the for results astrometry and Photometry (continued). 5 Table

Table 5 continues on next page.

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STT Doubles with Large ΔM – Part VI: Cygnus Multiples

5 6 7 8 9 5 6

26 27 28 29 30 31 32

Notes Notes Notes

N 5 5 5 5 N 5 5 5 5 N 5 5 5

20 20 15

621 632 700 639 648 621 632 700 639 648 621 632 639 630

Date Date Date

0.07 0.05 0.09 0.08 0.07 0.05 0.09 0.08 0.07 0.05 0.08

dVmag dVmag dVmag

SNR SNR SNR

4.86 7.19 3.09

68.15 72.26 43.32 34.96 21.60 25.34 12.34 10.13

339.58 400.85 309.59 284.05 339.58 400.85 309.59 284.05 339.58 400.85 284.05

Err Err Mag Err Mag Err Mag

0.070 0.072 0.050 0.052 0.090 0.093 0.080 0.086 0.074 0.077 0.070 0.086 0.050 0.065 0.090 0.124 0.080 0.130 0.074 0.105 0.070 0.215 0.050 0.150 0.080 0.315 0.068 0.236

Mag Mag Mag

7.475 7.491 7.291 7.494 7.438 7.475 7.491 7.291 7.494 7.438 7.475 7.491 7.494 7.487

12.033 12.056 12.050 12.036 12.044 13.989 13.874 14.053 14.037 13.988 15.715 15.486 15.577 15.593

PA PA PA

Err Err Err Err

0.052 0.039 0.079 0.053 0.058 0.068 0.052 0.103 0.069 0.075 0.065 0.049 0.066 0.061

PA PA PA

94.654 94.499 94.369 94.503 94.506 48.760 48.667 48.358 48.595

271.270 271.234 271.283 271.241 271.257

Err Err Sep Err Sep Err Sep

0.085 0.064 0.128 0.086 0.094 0.085 0.064 0.128 0.086 0.094 0.085 0.064 0.086 0.079

Sep Sep Sep

92.952 92.883 92.908 92.839 92.895 71.110 71.139 71.149 71.207 71.151 74.588 74.679 74.946 74.737

dDec 0.06 0.04 0.10 0.05 dDec 0.06 0.04 0.10 0.05 dDec 0.06 0.04 0.05

0.067 0.067 0.051

dRA dRA dRA

0.06 0.05 0.08 0.07 0.06 0.05 0.08 0.07 0.06 0.05 0.07

0.066 0.066 0.061

Dec Dec Dec

41 43 36.03 43 41 38.09 43 41 36.04 43 41 38.04 43 41 35.84 43 41 37.92 43 41 36,04 43 41 38.05 43 41 35.99 43 41 38.03 43 41 36.03 43 41 30.26 43 41 36.04 43 41 30.46 43 41 35.84 43 41 30.42 43 41 36,04 43 41 30.45 43 41 35.99 43 41 30.40 43 41 36.03 43 41 25.20 44 41 36.04 43 41 25.36 44 41 36,04 43 41 25.84 44 41 36.04 43 41 25.47 44 41

RA RA RA

21 39 28.727 39 21 20.426 39 21 28.727 39 21 20.432 39 21 28.729 39 21 20.432 39 21 28.723 39 21 20.432 39 21 28.727 39 21 20.430 39 21 28.727 39 21 35.058 39 21 28.727 39 21 35.062 39 21 28.729 39 21 35.066 39 21 28.723 39 21 35.064 39 21 28.727 39 21 35.062 39 21 28.727 39 21 33.737 39 21 28.727 39 21 33.736 39 21 28.723 39 21 33.726 39 21 28.726 39 21 33.733 39 21

A I A I A I A I A I A J A J A J A J A J A K A K A K A K

ABH 148 ABH 148 ABH 148 ABH Table 5 (continued). Photometry and astrometry results for the selected STT objects. ... objects. STT selected the for results astrometry and Photometry (continued). 5 Table

Table 5 continues on next page.

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STT Doubles with Large ΔM – Part VI: Cygnus Multiples

5 6 7 8 5 6 7 8 5 6 7 8

33 34 34

Notes Notes Notes

N 5 5 5 5 N 5 5 5 5 N 5 5 5 5

20 20 20

621 632 700 639 648 621 632 639 700 648 621 632 639 700 648

Date Date Date

0.07 0.05 0.09 0.08 0.05 0.05 0.07 0.10 0.05 0.05 0.07 0.10

dVmag dVmag dVmag

SNR SNR SNR

87.57 89.24 57.53 43.54 99.15 58.41 65.29 99.15 69.15 96.94

341.74 318.26 242.38 184.05 126.84 125.30 107.40 657.46 217.38 126.84 140.12 120.34 657.46 217.38

Err Err Mag Err Mag Err Mag

0.070 0.071 0.050 0.051 0.090 0.092 0.080 0.084 0.074 0.076 0.051 0.051 0.051 0.051 0.070 0.072 0.100 0.101 0.071 0.072 0.051 0.051 0.051 0.051 0.070 0.072 0.100 0.101 0.071 0.071

Mag Mag Mag

8.453 8.459 8.275 8.459 8.412 6.239 6.037 4.684 5.126 5.522 6.239 6.037 4.684 5.126 5.522

11.611 11.621 11.562 11.590 11.596 10.818 10.829 10.803 10.674 10.781 10.654 10.665 10.659 10.440 10.605

PA PA PA

Err Err Err Err

0.117 0.088 0.176 0.118 0.129 0.158 0.216 0.294 0.463 0.304 0.110 0.148 0.204 0.315 0.209

PA PA PA

46.341 46.062 45.984 46.084 46.117

219.488 219.527 220.170 217.987 219.295 183.977 183.539 184.269 182.729 183.627

Err Err Sep Err Sep Err Sep

0.085 0.064 0.128 0.086 0.094 0.042 0.057 0.078 0.122 0.081 0.042 0.057 0.078 0.122 0.081

Sep Sep Sep

41.529 41.708 41.778 41.739 41.688 15.342 15.039 15.220 15.111 15.177 22.173 21.922 21.981 22.225 22.074

dDec 0.06 0.04 0.10 0.05 dDec 0.03 0.04 0.05 0.10 dDec 0.03 0.04 0.05 0.10

0.067 0.061 0.061

dRA dRA dRA

0.06 0.05 0.08 0.07 0.03 0.04 0.06 0.07 0.03 0.04 0.06 0.07

0.066 0.052 0.052

Dec Dec Dec

41 43 56.92 43 41 25.59 44 41 56.67 43 41 25.61 44 41 56.52 43 41 25.55 44 41 56.68 43 41 25.63 44 41 56.70 43 41 25.60 44 41 49.05 53 34 37.21 53 34 48.83 53 34 37.23 53 34 48.83 53 34 37.20 53 34 48.99 53 34 37.08 53 34 48.93 53 34 37.18 53 34 49.05 53 34 26.93 53 34 48.83 53 34 26.95 53 34 48.83 53 34 26.91 53 34 48.99 53 34 26.79 53 34 48.93 53 34 26.90 53 34

RA RA RA

21 39 30.542 39 21 33.226 39 21 30.542 39 21 33.225 39 21 30.542 39 21 33.226 39 21 30.539 39 21 33.225 39 21 30.541 39 21 33.225 39 21 55.096 17 21 54.303 17 21 55.082 17 21 54.304 17 21 55.102 17 21 54.304 17 21 55.059 17 21 54.303 17 21 55.085 17 21 54.303 17 21 55.096 17 21 54.971 17 21 55.082 17 21 54.972 17 21 55.102 17 21 54.969 17 21 55.059 17 21 54.973 17 21 55.085 17 21 54.971 17 21

E F E F E F E F E F A B A B A B A B A B A C A C A C A C A C

FOX 262 FOX 433 STT 433 STT Table 5 (continued). Photometry and astrometry results for the selected STT objects. ... objects. STT selected the for results astrometry and Photometry (continued). 5 Table

Table 5 continues on next page.

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STT Doubles with Large ΔM – Part VI: Cygnus Multiples

5 6 7 8 5 6 5 6 8 7

34 35 36 34

Notes Notes Notes

N 5 5 5 5 N 5 5 5 5 N 5 5 5 5

20 20 20

621 632 639 700 648 621 632 639 700 648 621 632 639 700 648

Date Date Date

0.05 0.05 0.07 0.10 0.05 0.05 0.07 0.10 0.05 0.05 0.07 0.10

dVmag dVmag dVmag

SNR SNR SNR

51.53 99.15 45.48 21.66 25.09 36.95 99.15 36.95 13.50 17.92 58.41 69.15 65.29 96.94

126.84 657.46 217.38 126.84 657.46 217.38 125.30 140.12 107.40 120.34

Err Err Mag Err Mag Err Mag

0.051 0.054 0.051 0.055 0.070 0.085 0.100 0.109 0.071 0.079 0.051 0.058 0.051 0.058 0.070 0.104 0.100 0.116 0.071 0.088 0.051 0.051 0.051 0.051 0.018 0.072 0.017 0.101 0.038 0.071

Mag Mag Mag

6.239 6.037 4.684 5.126 5.522 6.239 6.037 4.684 5.126 5.522

13.086 13.099 13.020 13.186 13.098 13.678 13.674 13.799 13.696 13.712 10.818 10.654 10.829 10.665 10.803 10.659 10.674 10.440 10.781 10.605

PA PA PA

Err Err Err Err

0.043 0.057 0.078 0.123 0.081 0.071 0.094 0.131 0.202 0.134 0.185 0.247 0.340 0.530 0.351

PA PA PA

67.526 67.267 67.216 67.668 67.420

306.973 307.222 307.056 307.125 307.094 141.359 141.403 141.512 141.302 141.394

Err Err Sep Err Sep Err Sep

0.042 0.057 0.078 0.122 0.081 0.042 0.057 0.078 0.122 0.081 0.042 0.057 0.078 0.122 0.081

Sep Sep Sep

57.146 57.134 57.286 56.814 57.095 34.270 34.468 34.241 34.661 34.410 13.161 13.115 13.146 13.185 13.152

dDec 0.03 0.04 0.05 0.10 dDec 0.03 0.04 0.05 0.10 dDec 0.03 0.04 0.05 0.10

0.061 0.061 0.061

dRA dRA dRA

0.03 0.04 0.06 0.07 0.03 0.04 0.06 0.07 0.03 0.04 0.06 0.07

0.052 0.052 0.052

Dec Dec Dec

34 53 49.05 53 34 23.42 54 34 48.83 53 34 23.39 54 34 48.83 53 34 23.35 54 34 48.99 53 34 23.28 54 34 48.93 53 34 23.36 54 34 49.05 53 34 02.15 54 34 48.83 53 34 02.15 54 34 48.83 53 34 02.09 54 34 48.99 53 34 02.16 54 34 48.93 53 34 02.14 54 34 37.21 53 34 26.93 53 34 37.23 53 34 26.98 53 34 37.20 53 34 26.91 53 34 37.08 53 34 26.79 53 34 37.18 53 34 26.90 53 34

RA RA RA

21 17 55.096 17 21 51.385 17 21 55.082 17 21 51.384 17 21 55.102 17 21 51.386 17 21 55.059 17 21 51.377 17 21 55.085 17 21 51.383 17 21 55.096 17 21 57.670 17 21 55.082 17 21 57.666 17 21 55.102 17 21 57.668 17 21 55.059 17 21 57.665 17 21 55.085 17 21 57.667 17 21 54.303 17 21 54.971 17 21 54.304 17 21 54.969 17 21 54.304 17 21 54.969 17 21 54.303 17 21 54.973 17 21 54.303 17 21 54.971 17 21

A D A D A D A D A D A E A E A E A E A E B C B C B C B C B C

Table 5 (continued). Photometry and astrometry results for the selected STT objects. ... objects. STT selected the for results astrometry and Photometry (continued). 5 Table

SLE 382 SLE 9011 BU 433 STT

Table 5 concludes on next page.

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7 9 5 6 9 7 8 5 6 9 7 8 5 6

37 38 35 35

Notes Notes Notes Notes

N 5 5 5 5 5 N N 5 5 5 5 5 N 5 5 5 5 5

25 25 25 25

700 639 615 620 632 641 641 700 639 615 620 632 641 700 639 615 620 632 641

Date Date Date Date

0.10 0.07 0.05 0.04 0.04 0.10 0.07 0.05 0.04 0.04 0.10 0.07 0.05 0.04 0.05

dVmag dVmag dVmag dVmag

SNR SNR SNR SNR

85.82 59.83 93.94 57.76 85.82 29.59 59.83 29.03 48.38 48.55 52.29

383.39 292.92 368.32 106.91 308.64 102.75 393.42 110.29 383.39 292.92 368.32 118.04 308.64 124.96 393.42 120.64 106.91 102.75 110.29

Err Err Mag Err Mag Err Mag Err Mag

0.100 0.101 0.070 0.072 0.050 0.051 0.040 0.041 0.040 0.041 0.064 0.065 0.064 0.100 0.101 0.070 0.072 0.050 0.051 0.040 0.041 0.040 0.041 0.064 0.065 0.101 0.106 0.072 0.079 0.010 0.055 0.011 0.046 0.051 0.054 0.060 0.071

Mag Mag Mag Mag

7.111 7.251 7.301 7.287 7.287 7.247 7.247 7.111 7.272 7.301 7.287 7.287 7.252

10.753 10.860 10.902 10.902 10.893 10.862 10.595 10.928 10.884 10.901 10.925 10.847 10.753 12.317 10.860 12.212 10.902 12.283 10.902 12.296 10.893 12.264 10.862 12.274

PA PA PA PA

Err Err Err Err Err

0.385 0.341 0.268 0.268 0.335 0.323 0.154 0.137 0.107 0.107 0.134 0.129 1.591 1.485 1.140 1.113 1.414 1.363

PA PA PA PA

27.142 27.227 27.143 27.201 27.100 27.163 15.728 15.834 15.779 15.885 15.792 15.804

128.749 131.604 131.588 131.954 131.437 131.055

Err Err Sep Err Sep Err Sep Err Sep

0.122 0.108 0.085 0.085 0.106 0.102 0.122 0.108 0.085 0.085 0.106 0.102 0.122 0.108 0.085 0.085 0.106 0.102

Sep Sep Sep Sep

4.394 4.172 4.264 4.368 4.306 4.300

18.171 18.162 18.149 18.113 18.175 18.154 45.379 45.372 45.380 45.269 45.383 45.356

dDec 0.10 0.06 0.06 0.06 0.07 dDec dDec 0.10 0.06 0.06 0.06 0.07 dDec 0.10 0.06 0.06 0.06 0.07

0.072 0.072 0.072 0.072

dRA dRA dRA dRA

0.07 0.09 0.06 0.06 0.08 0.07 0.09 0.06 0.06 0.08 0.07 0.09 0.06 0.06 0.08

0.073 0.073 0.073 0.073

Dec Dec Dec Dec

48 40 45.91 40 48 02.08 41 48 46.11 40 48 02.26 41 48 46.06 40 48 02.21 41 48 46.12 40 48 02.23 41 48 46.05 40 48 02.23 41 48 46.05 40 48 02.20 41 48 46.05 40 48 45.91 40 48 29.59 41 48 46.11 40 48 29.76 41 48 46.06 40 48 29.73 41 48 46.12 40 48 29.66 41 48 46.05 40 48 29.72 41 48 46.05 40 48 29.69 41 48 02.08 41 48 59.33 40 48 02.21 41 48 59.44 40 48 02.21 41 48 59.38 40 48 02.23 41 48 59.31 40 48 02.23 41 48 59.38 40 48 02.19 41 48 59.37 40 48

RA RA RA RA

21 00 06.628 00 21 07.465 00 21 06.627 00 21 07.466 00 21 06.634 00 21 07.470 00 21 06.628 00 21 07.464 00 21 06.635 00 21 07.471 00 21 06.630 00 21 07.467 00 21 06.630 00 21 06.628 00 21 07.870 00 21 06.627 00 21 07.877 00 21 06.634 00 21 07.880 00 21 06.628 00 21 07.879 00 21 06.635 00 21 07.882 00 21 06.630 00 21 07.878 00 21 07.465 00 21 07.811 00 21 07.465 00 21 07.780 00 21 07.470 00 21 07.792 00 21 07.464 00 21 07.792 00 21 07.471 00 21 07.797 00 21 07.467 00 21 07.794 00 21

A C A C A C A C A C A C A B A E A E A E A E A E A E C D C D C D C D C D C D

Table 5 (conclusion). Photometry and astrometry results for the selected STT objects. ... objects. STT selected the for results astrometry and Photometry (conclusion). 5 Table

STT 425 STT 1210 BU 425 STT 425 STT

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Notes to Table 5. 20. A too bright for reliable photometry. SNR G < 20. 1. iT24 stack 5x3s. SNR B < 20. 21. iT24 stack 5x3s. Elongation indicates this being a dou- 2. i24 stack 5x3s_2. SNR B < 20. ble itself. 3. iT18 stack 5x3s. SNR B < 20. 22. iT24 stack 5x3s_2. No elongation. 4. A too bright for reliable photometry. SNR B < 20. 23. iT21 stack 5 x 3s. SNR H < 20. 5. iT24 stack 5x3s. 24. iT18 stack 5x3s. SNR H < 20. 6. iT24 stack 5x3s_2. 25. A too bright for reliable photometry. SNR H < 20. Indi- cation of H being a double itself only in one image, thus 7. iT21 stack 5x3s. not confirmed. 8. iT18 stack 5x3s. 26. iT21 stack 5x3s. SNR J < 20. 9. A too bright for reliable photometry. 27. iT18 stack 5x3s. SNR J < 20. 10. iT18 stack 5x3s. SNR D < 20. 28. A too bright for reliable photometry. SNR J < 20. 11. iT24 stack 5x3s. A and B too bright for reliable pho- 29. iT24 stack 5x3s. SNR K < 5. tometry. 30. it24 stack 5x3s_2. SNR K < 10. 12. iT24 stack 5x3s_2. A and B too bright for reliable photometry. 31. iT18 stack 5x3s. SNR K < 5. 13. iT21 stack 5x3s. A and B too bright fro reliable pho- 32. A too bright for reliable photometry. SNR K < 5. tometry. 33. E too bright for reliable photometry. 14. iT18 stack 5x3s. A and B too bright fro reliable pho- 34. A too bright for reliable photoemetry and photometry 1) tometry. 35. iT18 stack 5x3s. SNR E < 20. 15. A and B too bright for reliable photometry. 36. iT21 stack 5x3s. SNR E < 20. 16. iT24 stack 5x3s. SNR G < 20. 37. iT24 stack 5x3s_3 17. IT24 stack 5x3s_2. SNR G < 20. 38. 38. Components too close, no resolution. A too bright 18. iT21 stack 5x3s. SNR G < 10. for reliable photometry. 19. iT18 stack 5x3s. SNR G < 20.

1) The very bright primary of STT433 poses in our setup besides the usual photometry issue with bright stars also an astrometry challenge as the star disk gets huge and the large central area is populated with ADU values per pixel near the saturation limit sea- soned with random effects up and down making the centroid calculation quite difficult. This leads to the curious effect that 2 image stacks of very good quality with a rather small average plate solving error from the same telescope deliver a position for A different by ~0.3” but at the same time a nearly identical position for the other components. Another side effect of the bright STT433 primary are heavy sparks also dis- turbing measurements of components The difficulty of getting precise positions for very bright stars is also demonstrated by the results in the AAVSO Bright Star Monitor (BSM) Epoch Photome- try Database (EPD) v3.0 (released October 22, 2015) with an average scatter of ~0.3” around the current URAT1 position of STT433A. That astrometry for bright stars is somewhat difficult is also demonstrated by the fact that special efforts were taken in the URAT1 survey to access stars as bright as 3rd magnitude by taking short exposures with an objec- tive grating (Zacharias 2015) Figure 3. STT433 ADU Readings iT24 showing the scatter in the center of the star disk

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Table 6.: Photometry and Visual Results Compared to WDS Average of WDS NOMAD-1 UCAC4 UCAC4 Photometry Results of Visual Observations Mag VMag VMa f. mag Measures BU 449 B 12.70 - - - 12.625 Not seen. Three observations pointing to C STT 447 C 12.20 - - 11.231 11.183 being a magnitude brighter than the WDS value. Glimpsed with averted vision, BU 449 D 13.00 - - 12.696 13.121 hinting D may be slightly brighter than the WDS value. STT 447 E 8.48 8.373 9.015 8.782 8.412 No observations recorded.

ABH 148 G 14.80 14.20 - 14.192 14.618 No observations recorded.

ABH 148 H 13.79 13.670 - 13.442 13.864 Not seen. One observation indicating the magnitude of I is close to the ABH 148 I 11.65 11.595 12.063 12.034 12.044 WDS value based on comparison star. ABH 148 J 13.88 13.570 13.840 13.693 13.988 Not seen.

ABH 148 K 11.65 - - 14.614 15.593 Not seen. One observation which concluded K FOX 262 F 11.56 11.120 11.559 11.285 11.596 may cause F to appear brighter than it is. One observation indicating B was close to the WDS value, two ob- STT 433 B 10.00 - - - 10.781 servations suggesting B is half a magnitude fainter. One observation concluded C is reasonably close to the WDS val- STT 433 C 9.95 10.847 9.952 - 10.605 ue, one suggested it’s half a magnitude fainter. One observation that concluded D SLE 382 D 12.00 12.950 - 12.937 13.098 is close to 13th magnitude based on difficulty. One observation which concluded BU 9011 E 10.00 - - 13.379 13.712 E is 13th magnitude or fainter because it wasn’t visible. BU 1210 B 12.20 - - - - Not seen. Two observations suggesting the WDS magnitude was about right, STT 425 C 10.80 - 10.801 10.577 10.862 one suggesting C is half a magnitude brighter than WDS mag. One observation which concluded E STT 425 E 10.61 10.515 10.516 10.113 10.847 is the same magnitude as C. One observation which found D is STT 425 D 10.90 - - 12.206 12.274 about half a magnitude fainter than C.

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Table 7. Astrometry Results Compared to WDS Astrometry Astrometry WDS Coordinates WDS Sep WDS PA Astrometry PA Coordinates Sep 21:39:28.710 21 39 28.726 BU 449 AB 6.2 14 6.030 13.894 +41:43:36.00 +41 43 36.04 21:39:28.710 21 39 28.727 STT 447 AC 13.7 176 14.055 176.438 +41:43:36.00 +41 43 35.99 21:39:28.710 21 39 28.727 BU 449 AD 18.7 248 18.949 247.945 +41:43:36.00 +41 43 35.99 21:39:28.710 21 39 28.727 STT 447 AE 28.6 45 29.011 44.450 +41:43:36.00 +41 43 35.99 21:39:28.710 21 39 28.727 ABH 148 AG 33.8 337 33.757 336.523 +41:43:36.00 +41 43 35.99 21:39:28.710 21 39 28.727 ABH 148 AH 74.2 263 74.403 262.563 +41:43:36.00 +41 43 36.00 21:39:28.710 21 39 28.727 ABH 148 AI 92.7 271 92.895 271.257 +41:43:36.00 +41 43 35.99 21:39:28.710 21 39 28.727 ABH 148 AJ 71.3 94 71.151 94.506 +41:43:36.00 +41 43 35.99 21:39:28.710 21 39 28.726 ABH 148 AK 75.0 49 74.737 48.595 +41:43:36.00 +41 43 36.04 21:39:30.520 21 39 30.541 FOX 262 EF 42.0 46 41.688 46.117 +41:43:56.50 +41 43 56.70 21:17:55.070 21 17 55.085 STT 433 AB 14.2 222 15.177 1) 219.295 1) +34:53:48.80 +34 53 48.93 21:17:55.070 21 17 55.085 STT 433 AC 21.2 181 22.074 1) 183.627 1) +34:53:48.80 +34 53 48.93 21:17:55.070 21 17 55.085 SLE 382 AD 57.0 308 57.095 1) 307.094 1) +34:53:48.80 +34 53 48.93 21:17:55.070 21 17 55.085 BU 9011 AE 34.2 67 34.410 1) 67.420 1) +34:53:48.80 +34 53 48.93 21:00:06.610 21 00 06.630 BU 1210 AB 1.4 104 - - +48:40:45.90 +48 40 46.05 21:17:54.290 21 17 54.303 STT 433 BC 10.1 141 13.152 141.394 +34:53:37.10 +34 53 37.18 21:00:06.610 21 00 06.630 STT 425 AC 17.9 27 18.154 27.163 +48:40:45.90 +48 40 46.05 21:00:06.610 21 00 06.630 STT 425 AE 44.9 16 45.356 15.804 +48:40:45.90 +48 40 46.05 21:00:07.410 21 00 07.467 STT 425 CD 4.5 132 4.300 131.055 +48:41:01.71 +48 41 02.19

1) These results have to be taken with caution due to the astrometry issue with the bright primary. For explanation see Note 1 below Table 5.

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Table 8. Astrometry Results Compared with URAT1 Coordinates

Within Within iTelescope Object URAT1 Sep Err Sep Error URAT1 PA iTelescope PA Err PA Error Sep Range? Range? STT 447 AC 14.047 14.055 0.094 Yes 176.401 176.438 0.382 Yes

BU 449 AD 18.907 18.949 0.094 Yes 247.878 247.945 0.283 Yes

STT 447 AE 28.976 29.011 0.094 Yes 44.490 44.450 0.185 Yes ABH 148 AG 33.731 33.757 0.094 Yes 336.598 336.523 0.159 Yes ABH 148 AH 74.371 74.403 0.094 Yes 262.562 262.563 0.072 Yes

ABH 148 AI 92.849 92.895 0.094 Yes 271.252 271.257 0.058 Yes

ABH 148 AJ 71.190 71.151 0.094 Yes 94.496 94.506 0.075 Yes

ABH 148 AK 74.661 74.737 0.079 Yes 48.571 48.595 0.061 Yes

FOX 262 EF 41.751 41.688 0.094 Yes 46.120 46.117 0.129 Yes

STT 433 AB 15.090 15.177 0.081 No 1) 222.080 219.295 0.304 No 1)

STT 433 AC 21.864 22.074 0.081 No 1) 183.970 183.627 0.209 No 1)

SLE 382 AD 57.273 57.095 0.081 No 1) 307.235 307.094 0.081 No 1)

BU 9011 AE 34.444 34.410 0.081 Yes 67.107 67.420 0.134 No 1)

STT 433 BC 13.140 13.152 0.081 Yes 141.373 141.394 0.351 Yes

STT 425 AC 18.069 18.154 0.102 Yes 26.884 27.163 0.323 Yes

STT 425 AE 45.382 45.356 0.102 Yes 15.704 15.804 0.129 Yes

STT 425 CD 4.318 4.300 0.102 Yes 131.433 131.055 1.363 Yes

1) “No” with only minor delta to calculated error estimation for Sep and the respective PA with the exception of PA for STT 433 AB – here we have a measurement error of ~3° far beyond any calculated error estimation. This is the consequence of a STT433A plate solving error of as little as 0.008 RA seconds while STT433B is plate solved with virtually no difference compared to URAT1. For explanation see Note 1 below Table 2.3.1. It should also be noted that there is a difference of 0.240” for the position of STT433A between UCAC4 and URAT1 and 0.291” between WDS catalog data and URAT1 most probably due to proper motion. According to URAT1 the 2013.711 J2000 position is 21:17:55.093 +34:53:48.73

Vol. 12 No. 6 October 1, 2016 Journal of Double Star Observations Page 534

STT Doubles with Large ΔM – Part VI: Cygnus Multiples

(Continued from page 523) Fox, Philip, 1915, Annals of The Dearborn Observatory  iT24: 610mm CDK with 3962mm focal of Northwestern University, Vol 1, p. 199. length. CCD: FLI-PL09000. Resolution Greaney, Michael, 2012, "Some Useful Formulae" in 0.62 arcsec/pixel. V-filter. Located in Au- R.W. Argyle, Observing and Measuring Visual berry, California. Elevation 1405m Double Stars, 2nd Edition, Springer, New York.  iT11: 510mm CDK with 2280mm focal length. CCD: FLI ProLine PL11002M. Herschel, William, 1785, Catalogue of Double Stars, Resolution 0.81 arcsec/pixel. B- and V- Philosophical Transactions, Vol. 75, pp. 40-127. Filter. Located in Mayhill, New Mexico. Hussey, W.J., 1901, Micrometrical Observations of the Elevation 2225m Double Stars Discovered at Pulkowa Made with the  iT18: 318mm CDK with 2541mm focal Thirty-Six-Inch and Twelve-Inch Refractors of Lick length. CCD: SBIG-STXL-6303E. Resolu- Observatory, pp. 14-16, A.J. Johnston, Sacramento. tion 0.73 arcsec/pixel. V-filter. Located in Nerpio, Spain. Elevation 1650m Knapp, Wilfried; Nanson, John; Smith, Steven, 2015,  iT21: 431mm CDK with 1940mm focal "STT Doubles with Large Delta_M – Part I: Gem length. CCD: FLI-PL6303E. Resolution and Part II Leo and UMa", Journal of Double Star 0.96 arcsec/pixel. V-filter. Located in Observations, 11, 184-195. Mayhill, New Mexico. Elevation 2225m Knapp, Wilfried; Nanson, John; Smith, Steven, "2016,  AAVSO VPhot for initial plate solving STT Doubles with Large Delta_M – Part II: Leo  AAVSO APASS providing Vmags for faint refer- and UMa", Journal of Double Star Observations, ence stars (indirect via UCAC4) 12, 111-127.  UCAC4 catalog (online via the University of Hei- delberg website and Vizier and locally from USNO Knapp, Wilfried; Nanson, John, 2016, "STT Doubles DVD) for counterchecks with Large Delta_M – Part III: Vir, Ser, CrB, Com and Boo", Journal of Double Star Observations, 12,  URAT1 catalog for high precision plate solving 128-142.  Aladin Sky Atlas v8.0 for counterchecks  SIMBAD, VizieR for counterchecks Knapp, Wilfried; Nanson, John, 2016, "STT Doubles  2MASS All Sky Catalog for counterchecks with Large Delta_M – Part IV: Oph and Her", Jour-  URAT1 Survey (preliminary) for counterchecks nal of Double Star Observations, 12, 361-373.  AstroPlanner v2.2 for object selection, session Knapp, Wilfried; Nanson, John, 2016, "STT Doubles planning and for catalog based counterchecks with Large Delta_M – Part V: Aql, Del, Cyg and  MaxIm DL6 v6.08 for plate solving on base of the Aqr, Journal of Double Star Observing", 12, 474- UCAC4 catalog 487.  Astrometrica v4.9.1.420 for astrometry and photometry measurements Zacharias, Norbert, 2015, "Bright Star Astrometry with URAT", proceedings of invited talk at 2014 ADe- References LA meeting in Santiago, Chile, accepted by Revista Buchheim, Robert, 2008, "CCD Double-Star Measure- Mexicana de Astronomia y Astrofisica. ments at Altimira Observatory in 2007", Journal of Double Star Observations, 4, 27-31. Burnham, S.W., 1874, "A Fifth Catalogue of 71 New Double Stars", Monthly Notices of the Royal As- tronomical Society, 35, 31-48. (ADS bibliographic codes 1874MNRAS..35...31B and 1874MNRAS..35...40). Burnham, S.W., 1906, A General Catalogue of Double Stars Within 120° of the North Pole, Part II, Uni- versity of Chicago Press, Chicago. Cullen, R.T., 1937, Observations Made at the Royal Observatory, Greenwich, in the Year 1935, London, (ADS bibliographic code 1937GOAM…11B…1J).