1999 KW4 Observing Campaign Status

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Presentation transcript:

1999 KW4 Observing Campaign Status 1999 KW4 on 27 April 2019 Earth distance: 0.361 AU Sun distance: 0.768 AU 28 days until close approach Rob Landis

1999 KW4 Previous meeting in February 2019 in Vienna, IAWN signatories agreed to make 1999 KW4, a binary NEA, the next observing campaign target An exercise to see what resources might be brought to bear on a relatively short notice While 1999 KW4 is relatively well-characterized binary system, could serve as a reasonable analog to prepare for other binary NEAs as well as fine- tuning plans to observe/support DART impact into Didymos system IAWN has set up observing campaign webpage Logistics Points of contact Disciplines Assets http://www.iawn.net/obscamp/1999KW4/

1999 KW4 Science coordination - Mike Kelley (NASA HQ) Direct imaging – Marco Micheli (ESA) VLT SPHERES (O. Hainaut (ESO) et al.) HST WFC3 (A. Storrs (Towson Univ.) et al.) Gemini South and North Alopeke & Zorro (S. Howell, NASA ARC) Photometric lightcurve – Petr Pravec (Ondřejov Observatory) KMTNet, OWL-net, various (Hong-Kyu Moon (KASI) et al.) 2.1-m, 0.77-m (Jose Valdes (INAOE)) LCO network (T. Lister (LCO)) 0.61-m/1.0-m (Masa Ishiguru (Seoul Nat’l Univ.) et al.) 0.65-m (P. Pravec, Ondřejov Obs’y) others … Radar – Patrick Taylor (LPI) Arecibo (P. Taylor (LPI) et al.) Goldstone (L. Banner (JPL) et al. and Green Bank) Spectroscopy – Vishnu Reddy (Univ. of Arizona) NASA IRTF (V. Reddy et al.) Modeling – Jessie Dotson (NASA ARC) DD time has been requested; proposals have been submitted

(66391) 1999 KW4 – at a glance Discovery (LINEAR) 20 May 1999 Provisional Designation 1999 KW4 (closest known binary to Sun) Perihelion 0.2000 AU (Mercury crosser) Aphelion 1.0845 AU Heliocentric semi-major axis (a) 0.6422 AU Eccentricity (e) 0.6886 Orbital period (about the Sun) 188 days Orbital heliocentric inclination (i) 38.884° Rotational period 2.7650 hours (primary body) Orbital period of moonlet ~17.4 hours Diameter of primary ~1.3 km (complex ‘muffin’ shape) Diameter of moonlet ~0.5 km (elongated triaxial ellipsoid) System mass 2.488 ± 0.054 × 1012 kg Density ~2 g/cm3 (50% porosity) Spectral type S-type Next close approach 2036

(speckle interferometry) 1999 KW4 (Direct Imaging) VLT (SPHERE) Gemini North (‘Alopeke) 216 Kleopatra (speckle interferometry) HST (WFC3) Gemini South (Zorro) (DD time requested)

1999 KW4 (Photometric lightcurves) KASI KMTNet OWL-Net LOAO SOAO LCO Ondřejov Observatory (Czech Republic) National Institute of Astrophysics, Optics & Electronics (Mexico) And others …

1999 KW4 (Planetary Radar) DSS-14 (Goldstone 70-m) Arecibo Klystron (install late-May?) DSS-13 (34-m) Bi-static with Green Bank Arecibo DSS-13 DSS-14

1999 KW4 (Spectroscopy) Observations will made from the NASA IRTF May 27th and May 30th HST Prism mode observations (0.7-2.5 µm) with SpeX Observations will be made remotely from Arizona Goal is to reduce the data in near-real time and get composition information to Jessie Dotson

1999 KW4 Probabilistic Asteroid Impact Risk Model The PAIR model will be used to perform a risk assessment of a hypothetical impactor based on available characterization of 1999 KW4 at 3 points during the exercise: Prior to the exercise, assuming we know H. Immediately following close approach using the results from rapid analysis. A month after close approach utilizing the final observation results. Mathias, Wheeler, & Dotson (2017) (Exercise, Knowledge Capture, Modeling, Lessons Learned)