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739 observed NEAs and new 2-4m survey statistics within the EURONEAR network | | O. Vaduvescu
; M. Birlan
; A. Tudorica
; M. Popescu
; F. Colas
; D. J. Asher
; A. Sonka
; O. Suciu
; D. Lacatus
; A. Paraschiv
; T. Badescu
; O. Tercu
; A. Dumitriu
; A. Chirila
; B. Stecklum
; J. Licandro
; A. Nedelcu
; E. Turcu
; F. Vachier
; L. Beauvalet
; F. Taris
; L. Bouquillon
; F. Pozo Nunez
; J. P. Colque Saavedra
; E. Unda-Sanzana
; M. Karami
; H. G. Khosroshahi
; R. Toma
; H. Ledo
; A. Tyndall
; L. Patrick
; D. Fohring
; D. Muelheims
; G. Enzian
; D. Klaes
; D. Lenz
; P. Mahlberg
; Y. Ordenes
; K. Sendlinger
; | | Date: |
26 Aug 2013 | | Abstract: | We report follow-up observations of 477 program Near-Earth Asteroids (NEAs)
using nine telescopes of the EURONEAR network having apertures between 0.3 and
4.2 m. Adding these NEAs to our previous results we now count 739 program NEAs
followed-up by the EURONEAR network since 2006. The targets were selected using
EURONEAR planning tools focusing on high priority objects. Analyzing the
resulting orbital improvements suggests astrometric follow-up is most important
days to weeks after discovery, with recovery at a new opposition also valuable.
Additionally we observed 40 survey fields spanning three nights covering 11 sq.
degrees near opposition, using the Wide Field Camera on the 2.5m Isaac Newton
Telescope (INT), resulting in 104 discovered main belt asteroids (MBAs) and
another 626 unknown one-night objects. These fields, plus program NEA fields
from the INT and from the wide field MOSAIC II camera on the Blanco 4m
telescope, generated around 12,000 observations of 2,000 minor planets (mostly
MBAs) observed in 34 square degrees. We identify Near Earth Object (NEO)
candidates among the unknown (single night) objects using three selection
criteria. Testing these criteria on the (known) program NEAs shows the best
selection methods are our epsilon-miu model which checks solar elongation and
sky motion and the MPC’s NEO rating tool. Our new data show that on average 0.5
NEO candidates per square degree should be observable in a 2m-class survey (in
agreement with past results), while an average of 2.7 NEO candidates per square
degree should be observable in a 4m-class survey (although our Blanco
statistics were affected by clouds). At opposition just over 100 MBAs (1.6
unknown to every 1 known) per square degree are detectable to R=22 in a 2m
survey based on the INT data, while our two best ecliptic Blanco fields away
from opposition lead to 135 MBAs (2 unknown to every 1 known) to R=23. | | Source: | arXiv, 1308.5594 | | Services: | Forum | Review | PDF | Favorites | |
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