739 observed NEAs and new 2-4 m survey statistics within the EURONEAR network
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739 observed NEAs and new 2-4 m survey statistics within the EURONEAR network. / Vaduvescu, O.; Birlan, M.; Tudorica, A.; Popescu, M.; Colas, F.; Asher, D. J.; Sonka, A.; Suciu, O.; Lacatus, D.; Paraschiv, A.; Badescu, T.; Tercu, O.; Dumitriu, A.; Chirila, A.; Stecklum, B.; Licandro, J.; Nedelcu, A.; Turcu, E.; Vachier, E.; Beauvalet, L.; Tanis, F.; Bouquillon, L.; Pozo Nunez, F.; Colque Saavedra, J. P.; Unda-Sanzana, E.; Karami, M.; Khosroshahi, H. G.; Toma, R.; Ledo, H.; Tyndall, A.; Patrick, L.; Foehring, D.; Muelheims, D.; Enzian, G.; Klaes, D.; Lenz, D.; Mahlberg, P.; Ordenes, Y.; Sendlinger, K.
In: Planetary and Space Science, Vol. 85, 01.09.2013, p. 299-311.Research output: Contribution to journal › Journal article › Research › peer-review
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TY - JOUR
T1 - 739 observed NEAs and new 2-4 m survey statistics within the EURONEAR network
AU - Vaduvescu, O.
AU - Birlan, M.
AU - Tudorica, A.
AU - Popescu, M.
AU - Colas, F.
AU - Asher, D. J.
AU - Sonka, A.
AU - Suciu, O.
AU - Lacatus, D.
AU - Paraschiv, A.
AU - Badescu, T.
AU - Tercu, O.
AU - Dumitriu, A.
AU - Chirila, A.
AU - Stecklum, B.
AU - Licandro, J.
AU - Nedelcu, A.
AU - Turcu, E.
AU - Vachier, E.
AU - Beauvalet, L.
AU - Tanis, F.
AU - Bouquillon, L.
AU - Pozo Nunez, F.
AU - Colque Saavedra, J. P.
AU - Unda-Sanzana, E.
AU - Karami, M.
AU - Khosroshahi, H. G.
AU - Toma, R.
AU - Ledo, H.
AU - Tyndall, A.
AU - Patrick, L.
AU - Foehring, D.
AU - Muelheims, D.
AU - Enzian, G.
AU - Klaes, D.
AU - Lenz, D.
AU - Mahlberg, P.
AU - Ordenes, Y.
AU - Sendlinger, K.
PY - 2013/9/1
Y1 - 2013/9/1
N2 - 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 square degrees near opposition, using the Wide Field Camera on the 25 m 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 4 m telescope, generated around 12000 observations of 2000 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 that the best selection method is our e-it model which checks solar elongation and sky motion and the MPCs NEO rating tool. Our new data show that on average 0.5 NEO candidates per square degree should be observable in a 2 m-class survey (in agreement with past results), while an average of 2.7 NEO candidates per square degree should be observable in a 4 m-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 2 m survey based on the INT data (in accordance with other results), while our two best ecliptic Blanco fields away from opposition lead to 135 MBAs (2 unknown to every 1 known) to R=23. (C) 2013 Elsevier Ltd. All rights reserved.
AB - 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 square degrees near opposition, using the Wide Field Camera on the 25 m 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 4 m telescope, generated around 12000 observations of 2000 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 that the best selection method is our e-it model which checks solar elongation and sky motion and the MPCs NEO rating tool. Our new data show that on average 0.5 NEO candidates per square degree should be observable in a 2 m-class survey (in agreement with past results), while an average of 2.7 NEO candidates per square degree should be observable in a 4 m-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 2 m survey based on the INT data (in accordance with other results), while our two best ecliptic Blanco fields away from opposition lead to 135 MBAs (2 unknown to every 1 known) to R=23. (C) 2013 Elsevier Ltd. All rights reserved.
KW - Minor planets
KW - Near Earth Asteroids
KW - Main belt asteroids
KW - Astrometry and orbits
KW - Follow-up and discovery
KW - Survey statistics
KW - DISTRIBUTIONS
KW - SIZE
U2 - 10.1016/j.pss.2013.06.026
DO - 10.1016/j.pss.2013.06.026
M3 - Journal article
VL - 85
SP - 299
EP - 311
JO - Planetary and Space Science
JF - Planetary and Space Science
SN - 0032-0633
ER -
ID: 281755880