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Double Star Measurements at the Southern Sky with a 50 Cm Reflector in 2017

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Double Star Measurements at the Southern Sky with a 50 Cm Reflector in 2017 Vol. 15 No. 3 July 1, 2019 Journal of Double Star Observations Page 336 Double Star Measurements at the Southern Sky with a 50 cm Reflector in 2017 Rainer Anton Altenholz/Kiel, Germany e-mail: rainer.anton”at”ki.comcity.de Abstract: A 50 cm Ritchey-Chrétien reflector was used in October 2017 for recordings of double stars with a CCD webcam, which were analyzed with “lucky imaging”. Data from the Gaia catalogs DR1 and DR2 were used for calibration of the image scale. Also, parallax and proper motion data were checked for estimating the probability of physical relation for some systems with doubtful status. About one third of the 92 pairs investigated here are not re- solved or not listed in Gaia, either because of too close separations and/or too bright compo- nents. For several binaries, deviations from currently assumed orbits were found. Some imag- es of noteworthy systems are also presented. Introduction with a red or near infrared filter, which reduce effects “Lucky imaging” is an alternative method to speck- from atmospheric dispersion, seeing, as well as from le interferometry for beating the seeing, and is especial- chromatic aberrations of the Barlow lens. Only the best ly suitable for small to medium sized telescopes. By frames, typically several tens and up to more than 100, using short exposure times, and selection of only the were selected, registered, and stacked. The pixel size of best images for stacking, one can obtain virtually dif- 2.4 µm square results in a nominal resolution of 0.061 fraction limited images. More details of this technique arc sec/pixel. A more accurate value was obtained with are described, for example, in reference [1]. The accu- reference systems, as was already indicated above, and racy of position measurements depends on mainly three as will be explained in more detail below. In any case, factors: the seeing, the size and resolution of the tele- the accuracy of position measurements is typically bet- scope, and the calibration factor of the image scale. ter by more than one order of magnitude. Images were This applies equally well for speckle and lucky imag- re-sampled before stacking, as registering can be done ing, only the method of image analyzing differs. In fact, with sub-pixel accuracy, which results in smoothening given the telescope, the precision of position measure- of the intensity profiles, and better definition of the ments should be the same. As in earlier work, a rather peak centroids. Position angles were obtained by re- accurate calibration was obtained with data from the cording star trails with the telescope drive switched off, Gaia satellite mission, which delivered highly accurate from which the east-west direction was determined. star positions [2]. Statistical analysis resulted in an s.d. of about ± 0.1 de- grees. Instrumental The 50 cm Ritchey-Chrétien telescope is located at Calibration the “Internationale Amateursternwarte” on a guest The image scale was adjusted by using data from farm in Namibia [3], which I have already used in 2014 the Gaia DR1 and DR2 catalogs, which were released and 2016 for double star work [4]. The primary focal in 2016 and 2018, respectively. For 59 pairs out of the length of 4.1 m was extended by a 2x Barlow lens, re- total of 92 investigated here, values for right ascension sulting in an f-ratio of about f/16. Series of 1000 to and declination of the components were found, with 2000 images were taken with a b/w-CMOS camera of error margins typically smaller than 0.001 arc sec, from type “QHY 5 III 178” with exposure times ranging which separations and position angles were calculated. from less than a millisecond to several tenths of a sec- These are marked in table 1 below with shaded lines. ond, depending on the star brightness, on the filter be- Star positions in DR1 and DR2 refer to the epoch ing used, and on the seeing. Recordings were made 2015.0 and 2015.5, respectively, and were extrapolated Vol. 15 No. 3 July 1, 2019 Journal of Double Star Observations Page 337 Double Star Measurements at the Southern Sky with a 50 cm Reflector in 2017 to the epoch of my own recordings. However, in several cases, this turned out as ambiguous, mostly due to large scatter of other literature data. Also, in cases, where one or both components are close doubles, which are not resolved by Gaia, their positions are deemed as less accurate (see below). In total, 47 pairs were found suit- able for reference. These are indicated with darker shading. The image scale was adjusted by statistical evaluation of the residuals of the reference systems, such that the mean value and the standard deviation (s.d.) were minimized. As a result, the range of residu- als extended from -0.008 to +0.009 arc sec (this can be seen in Figure 1), the mean was less than 0.0001 arc sec, the s.d. was ± 0.005 arc sec, and the scale factor Figure 1. Plot of the residuals delta rho vs. rho of the refer- became 0.06488 arc sec/pixel with an estimated error of ence systems used for calibration of the image scale. The less than ± 0.1 per cent. mean value for the 47 pairs is less than 0.001 arc sec, and the standard deviation amounts to ± 0.005 arc sec. Results All measurements are listed in Table 1. Names, or too large a scatter. The table is followed by individu- nominal positions, and magnitudes are adopted from al notes, which are numbered with RA values. There the WDS [5]. Residuals refer to extrapolated literature are several pairs with unclear physical status, either data, mainly from the so-called “speckle catalog” [6], truly binary or merely optical. These were checked with as well as from Gaia, and for binaries, to ephemeris parallax and proper motion data from Gaia, and are data from the Sixth Catalog of Orbits of Visual Binary commented in the notes. Stars [7]. In several cases, no reasonable residuals could be given, because of too few literature data and/ (Text continues on page 343) Table 1: List of measurements. Position angles (PA) are in degrees, separations (rho) in arc seconds. N is the number of recordings. Shaded lines indicate pairs, for which data have been found in Gaia DR1 and/or DR2. Darker shadings mark pairs used for calibration of the image scale. Residuals (delta PA, delta rho) are given, when reasonable. Asterisks in column “Pair” refer to figures shown below. Pair RA & Dec Mags PA rho Date N delta PA delta rho Table 2. List of binaries with significant deviations from currently as- BU 391 AB 00 09.4 -27 59 6.13 6.24 258.2 1.328 2017.791 1 ~0 0.003 sumed orbits. In most cases, deviations are confirmed by Gaia, except * LCL 119 AC 00 31.5 -62 57 4.28 4.51 167.8 27.15 2017.797 2 -0.4 0.150 for I 264AB, BU 205AB, I 253AB, and I 22AB, which are not listed, * I 260 CD „ 4.60 6.54 347.0 0.350 „ 2 -2.5 0.035 incomplete, or not resolved in Gaia. See also corresponding notes. HDO 182 00 42.7 -38 28 6.60 7.01 23.7 0.665 2017.792 1 1.3 -0.017 HJ 3416 AB 01 03.3 -60 06 7.58 7.67 129.1 5.115 2017.797 1 0.1 0.008 * SLR 1 AB 01 06.1 -46 43 4.10 4.19 79.3 0.573 2017.795 3 -0.8 -0.046 HJ 3423 AB 01 15.8 -68 53 5.00 7.74 315.1 4.601 2017.792 2 -0.4 -0.007 STF 113 AB 01 19.8 -00 31 6.45 6.99 21.3 1.613 2017.792 2 ~0 -0.007 HJ 2036 01 20.0 -15 49 7.40 7.61 337.4 2.373 2017.792 1 0.5 -0.003 * I 264 AB 01 31.6 -53 22 8.36 8.84 25.8 0.793 2017.789 1 -1.5 -0.101 STF 138 AB 01 36.0 +07 39 5.97 7.35 60.0 1.727 2017.795 1 0.3 -0.007 DUN 4 01 38.8 -53 26 7.15 8.49 104.5 10.300 2017.800 1 0.1 0.002 DUN 5 01 39.8 -56 12 5.78 5.90 186.3 11.410 2017.800 2 ~0 -0.003 HJ 3461 AB 01 45.6 -25 03 5.38 8.50 17.9 4.957 2017.789 1 ~0 0,002 HJ 3475 01 55.3 -60 19 7.18 7.23 78.3 2.481 2017.800 2 -0.5 -0.001 * STF 186 01 55.9 +01 51 6.79 6.84 71.5 0.655 2017.792 1 -1.1 -0.034 Table 1 continues on the next page. Vol. 15 No. 3 July 1, 2019 Journal of Double Star Observations Page 338 Double Star Measurements at the Southern Sky with a 50 cm Reflector in 2017 Table 1 (continued). List of measurements. Position angles (PA) are in degrees, separations (rho) in arc seconds. N is the number of record- ings. Shaded lines indicate pairs, for which data have been found in Gaia DR1 and/or DR2. Darker shadings mark pairs used for calibration of the image scale. Residuals (delta PA, delta rho) are given, when reasonable.
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