Some entries in the following charts and tables are dependent upon a diameter
that is roughly inferred from the object’s estimated absolute magnitude (H) and
its assumed reflectivity, or albedo. The absolute magnitude (H) of a near-Earth
asteroid (NEA) is a measure of the object's brightness one astronomical unit from
the sun and Earth and at zero phase angle (i.e., the angle between the sun and
Earth, as seen from the NEA, is zero). The absolute magnitude (H) for a particular
NEA is computed from the observed apparent magnitudes of the object at various
times when the phase angles and the distances from the sun and Earth are known.
An effective diameter is the diameter of a hypothetical spherical NEA that would
provide the same apparent brightness as the observed NEA, whose actual shape is
unknown.
Since most NEAs do not have a known reflectivity, or albedo, this albedo must be
estimated before the H values, representing intrinsic brightness, can be converted to
an approximate diameter. Pravec et al (2012) determined that, for their sample of
583 main-belt asteroids and NEAs, the mean albedos and their standard deviations
are 0.057 (±0.013) for the Tholen/Bus/DeMeo C/G/B/F/P/D types and 0.197
(±0.051) for the S/A/L types. Since the albedos for NEAs are most likely to be either
approximately 6% for asteroids of the C-type and associated taxonomic classes or
20% for asteroids of the more populous S-type and associated taxonomic classes,
we have used an approximate mean value of 14% albedo and an H value of 17.75
to represent a one kilometer spherical NEA. Since the determined H values are
uncertain, and likely biased by a few tenths (see Pravec et al., 2012, Icarus) and the
single 14% albedo is only a rough mean representing a bimodal albedo distribution,
the estimated numbers of one kilometer and larger sized objects in the tables below
are very rough. However, these statistics are useful for monitoring the annual NEA
discovery progress.
Using near-infrared data provided by the WISE spacecraft in 2010 and early 2011,
Mainzer et al (2011) were able to determine diameters and albedos for 250 NEAs
with a minimum uncertainty of 10% and 20% respectively. Hence they were able to
determine the albedo distribution of these objects with known diameters and this
distribution was then used to compute diameters for previously known NEOs with
known H values but unknown diameters or albedos. They provided an estimate of
981 (±19) NEAs as the total population of NEAs one kilometer and larger.
At the time of their analysis (Spring 2011), they also estimated that 911 (±17)
of these large NEAs had already been discovered. While this latter estimate is
both higher and more accurate than the estimated numbers given for Spring 2011
in the following tables, this statistical technique cannot be easily employed for
day-to-day estimates of the population of NEAs one kilometer and larger.
In the following tables, we will continue to use the simpler method described
in the previous paragraph.
Mainzer, A. et al. (2011). NEOWISE observations of near-Earth objects: Preliminary
Results. Astrophysical Journal. 743:156.
Pravec, P., A.W. Harris, P. Kusnirak, A. Galad, K. Hornoch (2012). Absolute
magnitudes of asteroids and a revision of asteroid albedo estimates from WISE
thermal observations. Icarus (submitted 6/2012).
Stuart, J.S. (2003). Observational constraints on the number, albedos, sizes
and impact hazards of the near-Earth asteroids. Ph.D. thesis, MIT.
All Asteroids
Table 1. NEAs Discovered by Site
Half Year Intervals |
LINEAR (704) |
NEAT (566,608,644) |
Spacewatch (691,291) |
LONEOS (699) |
Catalina (703,E12,G96) |
Pan-STARRS (F51) |
Other | Cumulative Total |
1995 (1) | 0 | 0 | 14 | 0 | 0 | 0 | 4 | 335 |
1995 (2) | 0 | 0 | 12 | 0 | 0 | 0 | 2 | 349 |
1996 (1) | 1 | 5 | 18 | 0 | 0 | 0 | 4 | 377 |
1996 (2) | 0 | 5 | 10 | 0 | 0 | 0 | 2 | 394 |
1997 (1) | 3 | 2 | 10 | 0 | 0 | 0 | 4 | 413 |
1997 (2) | 14 | 9 | 4 | 0 | 0 | 0 | 7 | 447 |
1998 (1) | 44 | 9 | 19 | 1 | 1 | 0 | 7 | 528 |
1998 (2) | 92 | 2 | 15 | 6 | 2 | 0 | 5 | 650 |
1999 (1) | 74 | 0 | 12 | 6 | 11 | 0 | 1 | 754 |
1999 (2) | 87 | 0 | 7 | 7 | 19 | 0 | 3 | 877 |
2000 (1) | 108 | 2 | 14 | 21 | 13 | 0 | 4 | 1039 |
2000 (2) | 150 | 14 | 12 | 17 | 0 | 0 | 8 | 1240 |
2001 (1) | 95 | 28 | 7 | 22 | 0 | 0 | 2 | 1394 |
2001 (2) | 184 | 64 | 15 | 20 | 0 | 0 | 4 | 1681 |
2002 (1) | 158 | 56 | 16 | 14 | 1 | 0 | 6 | 1932 |
2002 (2) | 128 | 89 | 6 | 7 | 0 | 0 | 5 | 2167 |
2003 (1) | 102 | 30 | 23 | 33 | 0 | 0 | 9 | 2364 |
2003 (2) | 133 | 38 | 33 | 21 | 8 | 0 | 8 | 2605 |
2004 (1) | 167 | 19 | 41 | 14 | 25 | 0 | 6 | 2877 |
2004 (2) | 137 | 7 | 29 | 25 | 60 | 0 | 6 | 3141 |
2005 (1) | 78 | 8 | 29 | 22 | 116 | 0 | 10 | 3404 |
2005 (2) | 59 | 30 | 54 | 19 | 193 | 0 | 10 | 3769 |
2006 (1) | 44 | 4 | 45 | 13 | 197 | 0 | 3 | 4075 |
2006 (2) | 52 | 17 | 54 | 7 | 199 | 0 | 5 | 4409 |
2007 (1) | 38 | 4 | 20 | 7 | 200 | 0 | 3 | 4681 |
2007 (2) | 74 | 0 | 25 | 5 | 266 | 0 | 7 | 5058 |
2008 (1) | 74 | 0 | 43 | 1 | 281 | 0 | 5 | 5462 |
2008 (2) | 66 | 0 | 43 | 0 | 278 | 0 | 11 | 5860 |
2009 (1) | 50 | 0 | 32 | 0 | 261 | 0 | 18 | 6221 |
2009 (2) | 58 | 0 | 31 | 0 | 314 | 0 | 17 | 6641 |
2010 (1) | 29 | 0 | 21 | 0 | 257 | 0 | 97 | 7045 |
2010 (2) | 75 | 0 | 22 | 0 | 345 | 18 | 52 | 7557 |
2011 (1) | 40 | 0 | 17 | 0 | 332 | 68 | 15 | 8029 |
2011 (2) | 30 | 0 | 15 | 0 | 253 | 105 | 23 | 8455 |
2012 (1) | 25 | 0 | 13 | 0 | 353 | 120 | 7 | 8973 |
2012 (2) | 29 | 0 | 13 | 0 | 277 | 131 | 26 | 9449 |
2013 (1)* | 3 | 0 | 4 | 0 | 105 | 36 | 7 | 9604 |
* Incomplete half-year (based on discovery data through 2013-Feb-14 06:05 local)
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Large Asteroids
Table 2. Large NEAs Discovered by Site
Half Year Intervals |
LINEAR (704) |
NEAT (566,608,644) |
Spacewatch (691,291) |
LONEOS (699) |
Catalina (703,E12,G96) |
Pan-STARRS (F51) |
Other | Cumulative Total |
1995 (1) | 0 | 0 | 3 | 0 | 0 | 0 | 2 | 180 |
1995 (2) | 0 | 0 | 4 | 0 | 0 | 0 | 1 | 185 |
1996 (1) | 0 | 2 | 2 | 0 | 0 | 0 | 0 | 189 |
1996 (2) | 0 | 2 | 0 | 0 | 0 | 0 | 0 | 191 |
1997 (1) | 0 | 1 | 2 | 0 | 0 | 0 | 1 | 195 |
1997 (2) | 2 | 3 | 1 | 0 | 0 | 0 | 2 | 203 |
1998 (1) | 7 | 4 | 2 | 1 | 0 | 0 | 2 | 219 |
1998 (2) | 24 | 2 | 1 | 3 | 0 | 0 | 3 | 252 |
1999 (1) | 15 | 0 | 2 | 4 | 4 | 0 | 0 | 277 |
1999 (2) | 24 | 0 | 1 | 1 | 2 | 0 | 2 | 307 |
2000 (1) | 31 | 2 | 1 | 1 | 4 | 0 | 1 | 347 |
2000 (2) | 39 | 2 | 3 | 5 | 0 | 0 | 4 | 400 |
2001 (1) | 24 | 8 | 0 | 4 | 0 | 0 | 0 | 436 |
2001 (2) | 25 | 5 | 0 | 4 | 0 | 0 | 1 | 471 |
2002 (1) | 32 | 4 | 2 | 3 | 0 | 0 | 1 | 513 |
2002 (2) | 21 | 11 | 0 | 1 | 0 | 0 | 1 | 547 |
2003 (1) | 15 | 3 | 1 | 6 | 0 | 0 | 2 | 574 |
2003 (2) | 17 | 5 | 1 | 4 | 2 | 0 | 1 | 604 |
2004 (1) | 16 | 5 | 1 | 2 | 3 | 0 | 1 | 632 |
2004 (2) | 9 | 1 | 0 | 1 | 13 | 0 | 0 | 656 |
2005 (1) | 10 | 0 | 2 | 1 | 9 | 0 | 1 | 679 |
2005 (2) | 6 | 5 | 5 | 0 | 10 | 0 | 1 | 706 |
2006 (1) | 3 | 0 | 2 | 1 | 9 | 0 | 0 | 721 |
2006 (2) | 1 | 0 | 2 | 0 | 12 | 0 | 0 | 736 |
2007 (1) | 2 | 0 | 3 | 0 | 9 | 0 | 1 | 751 |
2007 (2) | 5 | 0 | 1 | 0 | 7 | 0 | 0 | 764 |
2008 (1) | 2 | 0 | 1 | 0 | 8 | 0 | 0 | 775 |
2008 (2) | 3 | 0 | 1 | 0 | 5 | 0 | 0 | 784 |
2009 (1) | 1 | 0 | 0 | 0 | 9 | 0 | 0 | 794 |
2009 (2) | 6 | 0 | 0 | 0 | 6 | 0 | 2 | 808 |
2010 (1) | 0 | 0 | 1 | 0 | 5 | 0 | 3 | 817 |
2010 (2) | 1 | 0 | 0 | 0 | 1 | 0 | 4 | 823 |
2011 (1) | 1 | 0 | 0 | 0 | 6 | 1 | 0 | 831 |
2011 (2) | 0 | 0 | 1 | 0 | 6 | 4 | 0 | 842 |
2012 (1) | 0 | 0 | 0 | 0 | 9 | 1 | 0 | 852 |
2012 (2) | 1 | 0 | 0 | 0 | 5 | 2 | 0 | 860 |
2013 (1)* | 0 | 0 | 0 | 0 | 1 | 0 | 0 | 861 |
* Incomplete half-year (based on discovery data through 2013-Feb-14 06:05 local)
NOTE: In the year 2010, the "Other" site category was exclusively WISE.
A separate table of WISE discoveries is available.
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Data compiled by Alan Chamberlin.
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