Report on the 29 th General Assembly of the International Astronomical Union 2015 Oct. 17, Las Vegas, Nevada International Occultation Timing Association - Annual Meeting David & Joan Dunham

August 2 – 14, we returned to the USA, but only to Honolulu, Hawaii, to attend the 29 th General Assembly (GA) of the International Astronomical Union (IAU). IAU GA’s take place every three years and last for two five-day sessions spread over two weeks. Previously, I attended IAU GA’s in 1967 (Prague, Czechoslovakia), 1970 (Brighton, UK), 1976 (Grenoble, France), 1979 (Montreal, Quebec), 1982 (Patras, Greece), and 1988 (Baltimore, Maryland). They provide a unique opportunity for astronomers worldwide working in all fields of astronomy to come together. In addition to the core administrative meetings, the General Assembly also includes a substantial and attractive scientific program. This usually comprises two series of three Symposia each lasting for three days, and scheduled during the first and second weeks, respectively. Fifteen to twenty more specialized "Focus Meetings" are also held, with up to five topics running in parallel. In addition, two full days are reserved for Division Meetings, with no overlap with the general program.

Symposia of the 29 th IAU GA included: IAUS 315 – From Interstellar Clouds to Star-forming Galaxies: Universal Processes? IAUS 316 – Formation, Evolution, and Survival of Massive Star Clusters IAUS 317 – The General Assembly of Galaxy Halos: Structure, Origin and Evolution IAUS 318 – Asteroids: New Observations, New Models IAUS 319 – Galaxies at High Redshift and Their Evolution Over Cosmic Time IAUS 320 – Solar and Stellar Flares and Their Effects on Planets A special session described first results from Gaia (first year obs.) Symposia programs & other IAU details are at

Focus Meetings of the 29 th IAU GA included: FM 1 – Dynamical Problems in Extrasolar Planets Science FM 2 – Astronomical Heritage: Progressing the UNESCO–IAU Initiative FM 3 – Scholarly Publication in Astronomy: Evolution or Revolution? FM 4 – Planetary Nebulae as Probes of Galactic Structure and Evolution FM 5 – The Legacy of Planck FM 6 – X-ray Surveys of the Hot and Energetic Cosmos FM 7 – Stellar Physics in Galaxies Throughout the Universe FM 8 – Statistics and Exoplanets FM 9 – Highlights in the Exploration of Small Worlds (results from Rosetta, Dawn, New Horizons) FM 10 – Stellar Explosions in an Ever-Changing Environment FM 11 – Global Coordination of Ground and Space Astrophysics and Heliophysics FM 12 – Bridging Laboratory Astrophysics and Astronomy FM 13 – Brightness Variations of the Sun and Sun-like Stars FM 14 – The Gravitational Wave Symphony of Structure Formation FM 15 – Search for Water and Life's Building Blocks in the Universe FM 16 – Stellar Behemoths - Red Supergiants Across the Local Universe FM 17 – Advances in Stellar Physics from Asteroseismology FM 18 – Scale-free Processes in the Universe FM 19 – Communicating Astronomy with the Public in the Big Data Era FM 20 – Astronomy for Development FM 21 – Mitigating Threats of Light Pollution & Radio Frequency Interference FM 22 – The Frontier Fields: Transforming our Understanding of Cluster and Galaxy Evolution

On behalf of IOTA, I gave four poster presentations, all during the first week: 1.Results from Asteroidal Occultations (Josef Durech was there) 2.Double star results from occultations 3.Solar diameter results from total and annular solar eclipses 4.Plans for the 2017 August 21 st total solar eclipse In the following, I give at least the title slide of each; the full posters (Power Point files) will be given in a subfolder in the IOTA meeting presentations section

S318p.15 – Sizes, Shapes, and Satellites of Asteroids from Occultations David W. Dunham*, David Herald, Steve Preston, Bradley Timerson, & Paul Maley, International Occultation Timing Association (IOTA); Eric Frappa, IMCCE, Paris; Tsutomu Hayamizu, Japanese Occultation Information Network; John Talbot, RASNZ Occ’n Section; and Atila Poro, IOTA/Middle East Section, Iran * Cell phone International Astronomical Union - General Assembly Honolulu, Hawaii, 2015 August 3 – 7 - Control ID For 40 years, the sizes and shapes of dozens of asteroids have been determined from observations of asteroidal occultations. Some of the first evidence for satellites of asteroids was obtained from the early efforts; now, the orbits and sizes of some satellites discovered by other means have been refined from occultation observations. Also, several close binary stars have been discovered, and the angular diameters of some stars have been measured from analysis of these observations. The International Occultation Timing Association (IOTA) coordinates this activity worldwide, from predicting and publicizing the events, to accurately timing the occultations from as many stations as possible, and publishing and archiving the observations.

Occult Watcher Planning Tool Used by observers to find potential occultations that they can observe, filtered by distance (larger distances for mobile observers), star mag., etc., and give event details, including links to star charts, etc. Through a Web interface, mobile observers can then set up to fill gaps in coverage by those at fixed observatories.

Lightcurve from Dunham Station #3 for 2011 Dec. 28th occ’n of SAO = HIP by (407) Arachne e. of Huntsville, TX Video analyzed by Scotty Degenhardt. The site was a graze near the n. limit; the star disappeared completely behind 3 features on the edge of the asteroid.

Still the record, Scotty observed from 14 stations in Oklahoma ! Scotty & I agreed before that I would cover the n. side & he the s. side, so each of us could deploy more stations across a shorter distance. This time, the path shifted s. so he hit the jackpot. 3 LA region fixed observers expected no event, but ended up defining the southern part of Hertha.

2011 July 19 occultation of LQ Aquarii by the binary asteroid (90) Antiope observed in western USA Above is the best direct image of Antiope, by Bill Merline using AO with Keck 3d before the occultation; it allowed a good pre- diction of the objects’ orientation.

Sky-plane plot, 2012 Jan. 19 th (911) Agamemnon occultation Above: Agamemnon: Axes  0.9 by  1.5 km, PA minor axis   1.3 , center X  0.4 km, Y  0.6 km; Disappearances are on the right side. The probable satellite is plotted as 9-km circle (but it’s more likely about 4 km across)  (278 km in the plane) from Agamemnon’s center in PA 93.8  Below: Light curve by Steve Conard (sta. 6) using a 14-in. SCT at his observatory at Gamber, Maryland

RASC Observer’s Handbook and The RASC Observer’s Handbook contains predictions of the  70 best asteroidal occultations visible from North America and Hawaii during the year. Many occultation YouTube videos are linked to from: Listed on this web page are, in groups from top to bottom, Lunar Occultation Videos; Asteroidal Occultation Videos; Jupiter/Saturn Satellite Events Miscellaneous Events (most of them are solar eclipse videos made near the edges of total and annular solar eclipse paths)

DGp Close Double Stars from Occultation Video Recordings David W. Dunham, Anthony George, Brian Loader, and David Herald, International Occultation Timing Association (IOTA) and high-speed CCD observations by Andrea Richichi, National Astronomical Research Institute of Thailand International Astronomical Union - General Assembly Honolulu, Hawaii, 2015 August 3 – 7 Control ID

Long History of Double Star Discoveries from Lunar Occultations; Antares was 1st Duplicity of Antares discovered during a lunar occultation observed at Vienna by Johann Tobias Bürg on 1819 April 13. I observed a graze of Antares by the thin crescent Moon on 1969 January 25 Contrast of the red giant star and its 5 th -mag. blue companion was striking I recorded an Antares graze with a color video camera and 12cm SCT from Western Australia on 2009 Feb. 17 Show events of both components, 19:44:10 to 19:44:25 and 19:47:00 to 19:47:30

Reduction profile by Dr. Mitsuru Sôma at the National Observatory, Japan. The lunar mean limb is the horizontal line at 0  and heights are in units of  at the Moon’s mean distance (1  then is 1.86 km). “Axis Angle” is position angle measured relative to the Moon’s axis of rotation. For each observer (and each stellar component), the star follows a parabolic arc. Cloud interference, esp. near the end, resulted in some spurious events. Kaguya & LRO laser altimeter profiles are very accurate.

IOTA’s Efforts to Catalog Possible Double Star Discoveries from Lunar Occultations In the early 1970’s, I worked with David Evans’ group at the Univ. of Texas to analyze hundreds of photoelectric lunar occultation observations I worked with a student, Don Stockbauer, to create a list of possible doubles from lunar occultations using: - Photoelectric occultations, Univ. of Texas and other published obs. - Grazing occultations observed since Total occultations, both current and from published obs. - Spectroscopic binaries (including 1-line) were included to encourage observation of their occultations. Too many dubious events were included; especially visual observers often reported “gradual” events more likely due to Fresnel diffraction, and sometimes stellar angular diameter Codes that indicated “certain, events in clear steps”, “probable”, and “possible” were lost when transferred to currently-used lists, for occultation predictions but also even the Washington interferometric catalog

IOTA’s Recent Double Star Efforts We now strongly encourage observation with relatively inexpensive video equipment to better quantify the observations, and obtain at least approximate photometric information using specially-developed software for analyzing video records, esp. Limovie from Japan and Tangra from Australia We encourage observation of stars with a past claim of duplicity; Over 90% of those show no evidence of duplicity with the new video obs. We encourage observations of the same occultation of a suspected double from widely- separated locations with real-time coordination using “Occult Watcher” Web software. If the same lunar occultation is observed from widely-separated locations (with the contacts at different position angles), the separation and position angle (P.A.) can be uniquely determined; otherwise, Only a “vector separation” in the P.A. of the occultation is found If orbital motion slow, “vector separations” from events a few months apart can give approximate double star separation and P.A. Results are published in JDSO periodically, including lists where the new observations indicate “probably single” for previous occ’n duplicity claims We have begun a collaboration with the current Kepler2 ecliptic program, to obtain (or find past) occultation lightcurves of their program stars, to help assess close stellar duplicity that might affect Kepler’s analysis for exoplanet transits. We are starting to collect and archive new and past occultation lightcurves.

Multiple events of 2 close components from a video recording of a lunar grazing occultation observed in Australia

X63280, 2014 Dec 31 23

Professional Work Is mainly coordinated now by Andrea Richichi at the National Astronomical Research Institute of Thailand, He worked before for a long time at the European Southern Observatory, where he still makes most of his observations Most observations are recorded in the infrared, allowing higher S/N and even some daytime observations Observations are concentrated on times when the Moon traverses the Galactic center region, an area of obvious high interest; a hundred occultations might be recorded in a single night Passages over the Pleiades and other interesting clusters are also observed The equipment is set up so that it can be used during “dead times” between other astronomical observations

2.4m f/10 TNT, alt. 2400m since Mar Instruments & Detectors  Photometers, photomultipliers, InSb diodes  APD, SPAD  CCD (drift scanning)  NIR Arrays (subwindow)  Specialized small format arrays (AO)

Lightcurve of occultation of SAO by (160) Una recorded by Dennis DiCicco at his observatory in Sudbury, Mass., 2011 January 24 Video at

FM13p.21 – Solar Diameter Measurements from Eclipses as a Solar Variability Proxy David W. Dunham*, Internat’l Occultation Timing Assoc. (IOTA); Sabatino Sofia, Yale Univ. – retired; Konrad Guhl, IOTA/European Section; and David Herald, IOTA * Cell phone International Astronomical Union - General Assembly Honolulu, Hawaii, 2015 August 3 – 7 - Control ID Since thermal relaxation times for the Sun are thousands of years, small variations of the Solar intensity are proportional to small variations of the Solar diameter on decadal time scales. In a combination between observations and theory, reliable values of the relation constant W are known, that allow transformation of historical variations of radius into variations of the solar luminosity. During the past 45 years, members of the International Occultation Timing Association (IOTA) have observed 20 annular and total solar eclipses from locations near the path edges. Baily’s beads, whose occurrence and duration are considerably prolonged as seen from path edge locations, were first timed visually, mostly using projection techniques.

Overview IOTA’s long term solar radius measurement research Observations near central eclipse path edges since 1970 Analysis of historical obs. back to 1715; look for more Re-analyze all obs. with accurate profile data- eg, LRO These large tasks manageable with some help from others in and outside of IOTA

30 Solar Radius Determinations from Solar Eclipses The radius correction, delta-R, is relative to the standard value at 1 A.U., arc seconds. All have been reduced using David Herald’s WinOccult program and analyzed with the Solrad programs. The Delta-R values are from 2-parameter solutions using bead events within 30° of the poles to use the better accuracy of the lunar polar profile as explained in a previous slide.

Summary of Remaining Work Search publications and local university archives for past observations to analyze Work remains to be done, for example, on the rather well- observed US eclipses of 1806 and 1869 The Internet facilitates connection with local historians who can often find information about past observations. Google Earth and other GIS tools make position determination much easier than using topo maps Re-analyze all obs. with accurate profile data- eg, LRO New observations with previous and modern techniques, especially at the 2017 eclipse, are needed to calibrate the earlier observations Anyone near a university or a central eclipse path, or even with just internet access, can help

DEp.1.08 – Plans to Observe the 2017 Total Solar Eclipse from near the Path Edges David W. Dunham* and Richard Nugent, International Occultation Timing Association (IOTA); Konrad Guhl and Hans-Joachim Bode, IOTA/European Section * Cell phone International Astronomical Union - General Assembly Honolulu, Hawaii, 2015 August 3 – 7 - Control ID The August 21 st, 2017 solar eclipse provides a good opportunity, to time the totality contacts, other Baily’s bead phenomena, and observe other dynamic edge phenomena, from locations near the edges of the path of totality. A good network of roads and generally favorable weather prospects means that more observers will likely be able to deploy more equipment than during most previous eclipses. The value of contact and Baily’s bead timings of total solar eclipses, for determining solar diameter and intensity variations, was described in an earlier presentation in Focus Meeting 13. This poster will concentrate on how observations of different types that have been used during past eclipses can be made by different observers,

Unique opportunity to deploy greater resources than usual

Primary goals for this eclipse Continuation for IOTA’s long term solar radius measurement research Standardization of video equipment Standardization of solar filters Co-located use of previous techniques (visual, telescopic projected image, filtered telescopic video) 2nd use of narrow band filters (1 st was for the May 20, 2012 annular eclipse) Desired Results: calibrate with Picard satellite data and with methods used at previous central eclipses

IOTA Standardization Attempted for the May 2012 Annular Eclipse Equipment Specifications Telescope aperture: 75mm – 100mm Field of View – 15' - 20' Solar filter – Baader brand – in sheets Narrow band filters – Wratten #23, #56 Attempt to observe in Picard wavelengths Video camera: PC164C(EX-2), Watec 902H

Ted Swift, S. Limit of May 2012 Annular Eclipse 15 sec interval Unfortunately, clouds prevented observation near the northern limit.

January 24, 1925 Total Solar Eclipse – Boy Scouts and Con Ed workers found the southern limit by observing at one-block intervals across Manhattan. Similar efforts might be made at towns straddling the limits of the August 2017 TSE, a public outreach opportunity

Two occultations during the GA Aug. 5, grazing occultation of 6.5-mag. 96 Piscium across southern Honolulu with path only a mile south of our hotel (first graze where we walked to the graze zone). We brought a 120mm maxi and due to the 73  altitude, we brought & used a paver mount. John Broughton plans to make lighter versions of those for better air transport. Aug. 13, possible occultation of 9.6-mag. star by (1197) Rhodesia – I thank Ernie Iverson for the pre-point charts for this & all AU events

August 5, 4:25am HST, graze of 6.5-mag. 96 Piscium 7  from northern cusp of 67% sunlit Moon, altitude 73 

Possible Oahu occultation of 9.6-mag. PPM by (1197) Rhodesia predicted on 2015 August 13 at 7:53 pm HST = PPM Predicted size of (1197) is 49 km. The expected central Duration is 3.3s with a 5-mag. drop. The Predicted altitude is 24  in the east. = PPM More about this event will be posted here on Thurs. & Friday. Contact David Dunham if you might try to observe this. Cell The target star is in northern Aquarius at J2000 RA 21h 09m 46.2s Dec +01  07’ 18” Northern limit if 1-  shift to north Predicted northern limit Predicted southern limit Predicted central line

Note published in IAU GA Newspaper

Rhodesia Occultation Results On target, cloud moved over FOV few seconds after the predicted time, a miss, but Sherrod’s AR miss (purple) was closer. Bart Billard recorded his first positive at Fredericksburg, VA with a CCD drift scan.