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Vol. 8 No. 1 January 1, 2012 Journal of Double Star Observations Page 32 Divinus Lux Observatory Bulletin: Report #24 Dave Arnold Program Manager for Double Star Research 2728 North Fox Run Drive Flagstaff, AZ 86004 Email: [email protected] Abstract: This report contains theta/rho measurements from 109 different double star sys- tems. The time period spans from 2010.616 to 2011.679. Measurements were obtained using a 20-cm Schmidt-Cassegrain telescope and an illuminated reticle micrometer. This report represents a portion of the work that is currently being conducted in double star astronomy at Divinus Lux Observatory in Flagstaff, Arizona. This article contains a listing of double star nents, since 2001, is the cause for this shift. measurements that are part of a series, which have Two additional variances in the theta values for been continuously reported at Divinus Lux Observa- two more double stars are being noted. First, proper tory, since the spring of 2001. Beginning with this motion by the “A” component, for the BU 483 multi- article, the selected double star systems, which ap- ple star system, appears to have caused significant pear in the table below, have been taken exclusively increases in the theta values for AC and AD during from the 2006.5 version of the Washington Double the past 10 years. Increases of over three degrees are Star Catalog (WDS), with published measurements being reported for both components. Secondly, the that are no more recent than ten years ago. There theta value for STF 140 AC, which appears in the are also some noteworthy items that are discussed, table, is 2.5 degrees greater than the 1998 WDS which pertain to a few of the measured systems. value. Proper motion doesn’t appear to be the cause As in previous articles, this report contains some in this case, but since this double star has few previ- double stars with noteworthy theta/rho shifts be- ous measurements, perhaps additional measure- cause of the effects of proper motion by one or both of ments will help bring more accuracy to this parame- the components. To begin with, proper motion by ter. In a similar context, the rho measurement in both component stars, for ES 1015 AB, has caused a this report, for HJ 3437, lines up more closely with 4% rho value increase during the past decade. Like- the listing for 1836 than it does for the one in 2002. wise, proper motion by both components, for STF Additional measures of this pair might also be useful 2944 AC, is responsible for a 4% rho value increase, Some possible corrections are being suggested for but this occurred in just the last 5 years. Next, the 2006.5 version of the WDS catalog. First of all, proper motion by the companion star, for GRV 440, the 2005 theta value for STF 3008 (23238-0828) caused a 2 degrees theta value decrease during the might contain a typo, since the proper motion vectors past 10 years. A rho value decrease of 5% is being imply a theta value increase rather than a decrease. reported for HJ 1927. Proper motion by both compo- Based upon measurements for this report, it appears Vol. 8 No. 1 January 1, 2012 Journal of Double Star Observations Page 33 Divinus Lux Observatory Bulletin: Report #24 that this value might be 159 degrees instead of 150 to either confirm the 2001 catalog values or the ones degrees. Secondly, the 2000 theta value for HJ 5547 obtained for this report. (22204+1102) reveals a 2 degrees increase from the In a similar context, the historical data in the 1991 value, when the proper motion vectors suggest WDS catalog seems to suggest a position angle in- just the opposite. The theta measurement appearing crease, over time, for S 799AB (21434+3817) but the in this report seems to validate a decreasing theta position angle measurement obtained for this article value. is more closely in line with the value listed for 1824. Another unexplained discrepancy from catalog Again, others may want to consider making addi- values pertains to STF 431 (03424+3358). The WDS tional position angle measurements of this pair in catalog lists the parameters for this double star as order to help verify the actual value. 249 degrees and 25.6” in 2001, but measurements of Finally, the rho measurement in the catalog for this pair on 2010.847 yielded theta/rho values of ARY 9 (00116+5813), for 2002, appears to possibly be 243.8 degrees and 19.75 seconds. Proper motion shifts in error. The rho measurement in this report, for this are not significant enough to account for this and no double star, is much more closely aligned with the other pairs with similar parameters or magnitudes measurements in 1910, rather than the 2002 meas- appear in this part of the sky. Perhaps other re- urements. searchers might consider measuring this double star NAME RA DEC MAGS PA SEP DATE NOTES STF2688 20308+1347 9.2 10.4 174.3 7.67 2010.616 1 GRV 440 21157+2355 10.6 10.6 297.9 43.94 2010.616 2 ES 1012 21467+5523 10.5 10.6 5.5 4.44 2010.616 3 ES 1015AB 21584+5245 10.4 10.7 238.7 7.90 2010.616 4 POP 145AB-CD 22042+4633 9.5 9.8 94.1 30.61 2010.616 5 STT 465 AB 22120+5012 7.3 10.5 317.3 12.84 2010.616 6 BU 477 22159+3125 9.5 10.3 40.8 6.42 2010.616 7 HJ 5547 22204+1102 7.5 10.1 300.9 40.98 2010.616 8 STF2944AC 22478-0414 7.2 8.5 87.1 60.24 2010.616 9 STF3008 23238-0828 7.1 7.6 159.2 5.93 2010.616 10 ARG 47 00027+5958 9.3 10.3 290.4 9.88 2010.638 11 HJ 1927 00032+4508 9.1 10.1 73.4 9.88 2010.638 12 BU 483AC 00091+4051 6.9 7.5 270.4 158.00 2010.734 13 BU 483AD 00091+4051 6.9 10.4 275.3 227.13 2010.734 13 HJ 1953AC 00194-0849 3.5 10.3 190.7 107.14 2010.638 14 HJ 1981A-BC 00310-1005 6.9 8.4 88.1 78.51 2010.638 15 STF 104 01170+3828 7.9 9.8 321.6 13.33 2010.638 16 HDO 45 01172+0201 7.2 9.5 102.6 38.02 2010.638 17 H 23AC 01201+5814 5.0 7.0 231.0 134.30 2010.638 18 H 23AD 01201+5814 5.0 10.2 287.8 178.74 2010.638 18 H 23AE 01201+5814 5.0 10.3 239.0 170.84 2010.638 18 H 23CE 01201+5814 7.0 10.3 265.3 41.97 2010.638 18 Table continues on next page. Vol. 8 No. 1 January 1, 2012 Journal of Double Star Observations Page 34 Divinus Lux Observatory Bulletin: Report #24 NAME RA DEC MAGS PA SEP DATE NOTES WEI 3 01201+3639 8.9 9.7 188.4 4.94 2010.638 19 S 398 01284+0758 6.2 8.0 99.5 69.13 2010.658 20 HJ 2052 01316-1901 6.8 7.4 113.9 80.98 2010.658 21 STF 135AB-C 01341+3612 8.0 10.5 260.4 7.90 2010.658 22 STF 135AB-D 01341+3612 8.0 10.6 51.0 50.86 2010.658 22 STT 33AB 01374+5838 7.3 8.8 77.1 26.66 2010.658 23 DOB 2AC 01374+5838 7.3 10.2 109.3 106.65 2010.658 23 STF 140AC 01390+4104 9.2 9.9 322.5 195.53 2010.734 24 STF 150 01434-0705 7.7 8.2 195.8 36.04 2010.658 25 ENG 8 01496-1041 4.7 6.7 250.4 183.68 2010.658 26 STF 4AB 01562+3715 5.7 5.9 297.5 202.44 2010.658 27 BU 1368Bb 01562+3715 5.9 9.6 258.2 204.41 2010.658 27 STF 245Aa-B 02186+4017 7.2 8.0 293.9 11.36 2010.658 28 STT 27AB 02268+1034 6.7 8.3 31.9 73.57 2010.658 29 STF 431 03424+3358 5.0 10.0 243.8 19.75 2010.847 30 WEB 4 05290-0442 9.8 10.0 232.9 47.89 2010.978 31 STF 785AB 05459+2555 7.3 8.3 347.8 14.32 2010.978 32 STT 116AD 05459+2555 7.3 10.2 10.5 201.45 2010.978 32 BU 93AB 05489+2101 9.0 10.2 122.1 60.24 2010.978 33 H 125AB 05506+5655 6.5 10.4 128.0 26.19 2010.978 34 BRT1188 05596+1312 10.0 10.1 354.6 5.43 2010.978 35 GUI 10AC 06117+1723 7.5 9.0 35.9 73.08 2010.978 36 STF 889AB 06199+2501 7.4 9.9 243.2 21.23 2010.978 37 WAL 43AC 06199+2501 7.4 10.1 322.2 38.51 2010.978 37 A 2720AC 06234+1432 9.3 9.6 28.6 67.15 2010.978 38 STF1174AB-C 08047+4717 8.9 9.3 215.0 5.93 2011.118 39 WFC 81 09133+0540 10.2 10.4 76.5 8.39 2011.118 40 A 2367AB 10100+1623 9.9 10.6 85.0 60.74 2011.118 41 STF1435 10280+1950 10.3 10.7 203.2 8.89 2011.173 42 STF1442 10320+2202 8.2 8.5 156.8 13.33 2011.118 43 STF1447 10338+2321 7.5 8.8 124.4 4.44 2011.118 44 BU 111AC 10512-0906 10.0 9.4* 130.7 64.19 2011.173 45 STF3072 11309-0643 7.7 9.9 331.1 9.88 2011.173 46 ES 626 15409+5009 9.2 9.2 275.1 7.90 2011.367 47 STF 29AB 16224+3348 5.2 5.4 164.2 356.49 2011.367 48 Table continues on next page.
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  • Ground-Based Follow-Up Observations of TRAPPIST-1 Transits in the Near-Infrared

    Ground-Based Follow-Up Observations of TRAPPIST-1 Transits in the Near-Infrared

    MNRAS 000,1{21 (2019) Preprint 16 May 2019 Compiled using MNRAS LATEX style file v3.0 Ground-based follow-up observations of TRAPPIST-1 transits in the near-infrared A. Y. Burdanov,1? S. M. Lederer2, M. Gillon1, L. Delrez3, E. Ducrot1, J. de Wit4, E. Jehin5, A. H. M. J. Triaud6, C. Lidman7, L. Spitler8;9, B.-O. Demory10, D. Queloz3 and V. Van Grootel5 1Astrobiology Research Unit, Universit´ede Li`ege, All´ee du 6 Ao^ut19C, 4000 Li`ege, Belgium 2NASA Johnson Space Center, 2101 NASA Parkway, Houston, TX 77058, USA 3Cavendish Laboratory, JJ Thomson Avenue, Cambridge, CB3 0H3, UK 4Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA 5Space Sciences, Technologies and Astrophysics Research (STAR) Institute, Universit´ede Li`ege, All´eedu 6 Ao^ut19C, 4000 Li`ege, Belgium 6School of Physics & Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK 7The Research School of Astronomy and Astrophysics, Australian National University, ACT 2601, Australia 8Research Centre for Astronomy, Astrophysics & Astrophotonics, Macquarie University, Sydney, NSW 2109, Australia 9Department of Physics & Astronomy, Macquarie University, Sydney, NSW 2109, Australia 10University of Bern, Center for Space and Habitability, Sidlerstrasse 5, CH-3012 Bern, Switzerland Accepted 2019 May 14. Received 2019 May 9; in original form 2019 April 3 ABSTRACT The TRAPPIST-1 planetary system is a favorable target for the atmospheric charac- terization of temperate earth-sized exoplanets by means of transmission spectroscopy with the forthcoming James Webb Space Telescope (JWST). A possible obstacle to this technique could come from the photospheric heterogeneity of the host star that could affect planetary signatures in the transit transmission spectra.