Nea Population Estimate With Detection/re-detection Method: Analysis Update

Details Nea Population Estimate With Detection/re-detection Method: Analysis Update Nea Population Estimate With Detection/re-detection Method: Analysis Update

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.5302b&link_type=abstract

American Astronomical Society, DPS meeting #38, #53.02; Bulletin of the American Astronomical Society, Vol. 38, p.581

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We present an update of the near-Earth asteroids (NEAs) population estimate obtained by comparing the number of re-detections of previously known asteroids of a given size with the number of new detections during a test interval of time, as described in D'Abramo et al. (Icarus 153, 214-217, 2001). We apply this method to the sample of NEA observations (discovery observations and observations from apparitions of previously known asteroids) made by the Lincoln Near-Earth Asteroids Research Project (LINEAR, observatory code 704) and by the Catalina Survey (703 and E12) within the period Jan. 1, 2004 to Dec. 31, 2005 as published by the Minor Planet Center. The increased number of discovered objects compared to the previous analysis allows us to extend the population estimate up to Absolute Magnitude H = 21.0 and also to have smaller error bars. Both LINEAR and Catalina data suggest a number of NEAs of H 1 km) of 1050 +/-60. As in the previous analysis, however, the expected biases of this method all work in the direction of underestimating the true population. Here we have tried to cope with the effects of some of the expected biases through a survey bias corrector developed for each of the surveys taken into account. A preliminary analysis of this bias results in a corrected estimate of the number of NEAs of H < 18.0 of 1200. The current best estimate of H magnitude versus diameter of NEAs is H = 17.75 is about equivalent to D = 1 km (Stuart, J. S., 2003, PhD Thesis, MIT; Morbidelli et al. 2002, Icarus 158, 329). Interpolating our results to mid-bin of magnitude leads to an estimate of N(H<17.75) of about 1100. This is essentially unchanged from the estimate of Stuart (2003), but with a smaller error bar of about +/-75.

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