Clark R. ChapmanClark R. ChapmanSouthwest Research Institute, Boulder CO, USASouthwest Research Institute, Boulder CO, USA

andandAlan W. HarrisAlan W. Harris

Space Science Institute, La Canada CA, USASpace Science Institute, La Canada CA, USA

Clark R. ChapmanClark R. ChapmanSouthwest Research Institute, Boulder CO, USASouthwest Research Institute, Boulder CO, USA

andandAlan W. HarrisAlan W. Harris

Space Science Institute, La Canada CA, USASpace Science Institute, La Canada CA, USA

7272ndnd Annual Meeting Annual MeetingThe Meteoritical SocietyThe Meteoritical Society

Nancy, France 16 July 2009Nancy, France 16 July 2009

7272ndnd Annual Meeting Annual MeetingThe Meteoritical SocietyThe Meteoritical Society

Nancy, France 16 July 2009Nancy, France 16 July 2009

Near-Earth Asteroid/Meteoroid Near-Earth Asteroid/Meteoroid Impacts: Prospects for Linking Impacts: Prospects for Linking Telescopic Observations with Telescopic Observations with

Recovered MeteoritesRecovered Meteorites

Asteroid 2008 TC3 = meteorite Almahata Sitta: Asteroid 2008 TC3 = meteorite Almahata Sitta:

Importance of Linking Asteroids and Meteorites A major goal of meteoritics has been to

determine the origin and nature of meteorite parent bodies.

Asteroids are meteorite parent bodies (or fragments of parent bodies).

Linking recovered meteorites to specific asteroids has been difficult. Orbits derived from fireball photos for

recovered meteorites are imprecise and would not identify the parent body anyway because orbits evolve

Reflectance spectra are not unique to particular asteroids

Groundbased telescopic data exist for tens of thousands of asteroids.

Calibration (either by in situ spacecraft missions to asteroids, or by cheaper identifications like TC3) can powerfully link meteorites to parent asteroids.

We can compare meteorite properties with asteroid taxonomic class, interpreted mineralogy, spin, size, shape, orbit, etc.

TC3 Reflectance Spectrum: Wm. Herschel Telescope (Fitzsimmons, Hsieh, Duddy & Ramsay)

TC3 Lightcurve (Clay Center Observatory)

2008 TC3 = Almahata Sitta Asteroid 2008 TC3 was the first

asteroid ever discovered and predicted to strike the Earth.

The predicted impact occurred, there are many records of its impact, and many resulting meteorites were collected on the ground (the Almahata Sitta ureilite, discussed in other talks).

Was this first-ever event unique and miraculous, or can we expect future opportunities to collect meteoritic samples from astronomically observed asteroids?

We show that we may expect future TC3-like events, especially if we proactively campaign for the required telescopic surveys.

Almahata Sitta fragment on ground in Sudan (P. Jenniskens)

TC3 atmospheric train (M. Mahir)

TC3 asteroid moving (W. Boschin, TNG)

2008 TC3: 20 Hour Warning!

NEA discovered by CSS 7 Oct. 2008, predicted to impact Sudan 20 hours later. Before impact, other telescopes observed TC3’s physical properties. Nearly 300 pieces of a rare, anomalous ureilite meteorite were recovered. TC3 was ~4 meters diameter, roughly an annual impact on Earth. Spaceguard Survey was expected to find only 1-in-1 million TC3-sized NEOs. Was it a miracle that we found beforehand what was plausibly the largest NEA

to impact Earth in 2008? NO! Astronomers overlooked Spaceguard’s short-term warning capability.

Short-Term Warning Capability of Tele-scopic Surveys: Nobody Got it Right

Analyses in the 1990s of the “Spaceguard Survey” only considered cataloging of near-Earth asteroids (NEAs); short-term warning was evaluated only for rare comets.

Thus it was believed that there was only a tiny chance that a dangerous 30-meter NEA would be found, let alone a “TC3”.

Short-term hazard warning was evaluated (NASA SDT 2003) for the “next generation” surveys, but not for meteorite recovery.

“Consider a 30–40-m office-building-sized object striking at 100 times the speed of a jetliner…. Even with the proposed augmented Spaceguard Survey, it is unlikely that such a small object would be discovered in advance; impact would occur without warning.” – C. Chapman, EPSL (2004).

““a short lead time for an NEO is extremely unlikely – a short lead time for an NEO is extremely unlikely – we can expect either decades of warning or none at we can expect either decades of warning or none at all”all” – Morrison, Harris, Sommer, Chapman & Carusi (“Asteroids III” 2002)

Capability for “Final Plunge” Detection by Current Survey

The Catalina Sky Survey (the telescope shown and a smaller Schmidt) dominates Spaceguard discoveries, followed by LINEAR, then others.

Sky coverage is to varying magnitude (size) limits, with spatial/temporal limits: Poor coverage south of -45 deg. declination Poor coverage near Milky Way No coverage within 60 deg. of the Sun Poor coverage during Ariz./N.Mex. summer

Half of “final plunge” objects are well placed to see, generally opposite the Sun; other half come from Sun’s direction.

Night-sky coverage repeats every 10 days: Most 30 m “dangerous” NEOs can be found

because they can be detected ~2 weeks out 5%-10% of TC3’s detected (1-2 days out)

Optimization might yield TC3 twice/decade.

1.6-meter Catalina Sky Survey telescope: discovered TC3

LINEAR telescope in New Mexico, part of Spaceguard Survey

Spaceguard Survey Sky Coverage

Charts show coverage of whole sky (different colors show different surveys) for 10-day intervals in Feb. and June 2009.

Red oval (centered at midnight along the ecliptic) shows approach directions for ~40% of asteroids on their final plunge (see next chart).

Feb. 19-28 is good coverage (>90% of red oval), while June 19-28 coverage is poor due to Milky Way and weather (<50% of red oval).

Searching for Final Plungers

Red box indicates general range surveyed by Spaceguard telescopes. Known Potentially Hazardous Asteroids (PHAs) were used to simulate

direction from which impactors come: 53% of them are well within the survey range, coming from the general anti-solar direction. There is a concentration within the red oval (which is plotted in sky coverage charts).

Maximum warning time (days to observe before impact) depends on asteroid brightness (size) and on limiting magnitude of survey (V~20.5 for Spaceguard, ~24 for next generation surveys).

Next generation surveys “could” find most night-time TC3s. But will they?

Will Pan-STARRS and LSST Actually Report TC3s?

Pan-STARRS prototype has recently been evaluated for ability to detect TC3’s [Vere et al., Icarus, in press 2009]; 25% chance of a TC3 in 4 years operation.

Both Pan-STARRS-4 and LSST serve many astrophysical survey projects and observing protocols have already been established many years before operation:

Design of observing “cadence” (how often images are taken of different parts of the sky) is fixed

Protocols for data analysis and reporting are nominally designed, but do not account for “short warning” situations: they could be changed…although there will be resistance to doing so

Real-time search for interesting objects (e.g. to alert other observers) is probably possible, converting weeks to days (true “Rapid Response”) for recognizing and warning of an incoming asteroid.

Even if the astrophysicists remain firm, after-impact searches would be possible to find data for an asteroid that resulted in an observed meteorite-producing bolide: This would NOT provide physical observations This WOULD provide a good orbit for the asteroid

Pan-STARRS #1, now operating Pan-STARRS #1, now operating in Maui; four are planned. in Maui; four are planned. “Panoramic Survey Telescope “Panoramic Survey Telescope and Rapid Response System”and Rapid Response System”

LSST: a major NSF astronomical LSST: a major NSF astronomical survey telescope; funding and survey telescope; funding and timeline uncertain. “Large timeline uncertain. “Large Synoptic Survey Telescope”Synoptic Survey Telescope”

Conclusions

2008 TC3/Almahata Sitta was not a fluke…we can expect another within a decade or so.

The current Spaceguard Survey could be optimized to perhaps double the chances.

The next generation surveys (e.g. Pan-STARRS and LSST) could find TC3s every year or two, starting around 2020, but…

The meteoritical community will have to speak up to change current plans, which now would analyze and report asteroid data only every few weeks.

Let’s find and observe the meteorite-yielding Let’s find and observe the meteorite-yielding asteroids BEFORE they hit!asteroids BEFORE they hit!

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