J/ApJ/760/L12 WISE/NEOWISE NEOs preliminary thermal fits (Mainzer+, 2012)
Physical parameters of asteroids estimated from the WISE 3-Band data and NEOWISE
post-cryogenic survey.
Mainzer A., Grav T., Masiero J., Bauer J., Cutri R.M., McMillan R.S.,
Nugent C.R., Tholen D., Walker R., Wright E.L.
<Astrophys. J., 760, L12 (2012)>
=2012ApJ...760L..12M 2012ApJ...760L..12M
ADC_Keywords: Minor planets ; Infrared sources ; Surveys
Keywords: atlases; catalogs; minor planets, asteroids: general; surveys
Abstract:
Enhancements to the science data processing pipeline of NASA's
Wide-field Infrared Survey Explorer (WISE) mission, collectively known
as NEOWISE, resulted in the detection of >158000 minor planets in four
infrared wavelengths during the fully cryogenic portion of the
mission. Following the depletion of its cryogen, NASA's Planetary
Science Directorate funded a four-month extension to complete the
survey of the inner edge of the Main Asteroid Belt and to detect and
discover near-Earth objects (NEOs). This extended survey phase, known
as the NEOWISE Post-Cryogenic Survey, resulted in the detection of
∼6500 large Main Belt asteroids and 86 NEOs in its 3.4 and 4.6µm
channels. During the Post-Cryogenic Survey, NEOWISE discovered and
detected a number of asteroids co-orbital with the Earth and Mars,
including the first known Earth Trojan. We present preliminary thermal
fits for these and other NEOs detected during the 3-Band Cryogenic and
Post-Cryogenic Surveys.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 82 129 *Results for the 30 NEOs detected by NEOWISE during
the 3-Band Cryogenic Survey phase and the 86 NEOs
detected during the NEOWISE Post-Cryogenic Survey
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Note on table1.dat: We apply the Near-Earth Asteroid Thermal Model (NEATM;
Harris 1998Icar..131..291H 1998Icar..131..291H) to obtain estimates of the asteroids' physical
parameters. This model uses a beaming parameter, η, to account for the
tendency of surface features such as craters to "beam" radiation back to the
observer at low phase angles. See section 2.1.
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See also:
J/A+A/561/A45 : Asteroid (341843) 2008 EV5 WISE light curves (Ali-Lagoa+, 2014)
J/ApJ/759/L8 : WISE/NEOWISE obs. of MBAs: preliminary results (Masiero+, 2012)
J/ApJ/759/49 : Jovian Trojan asteroids with WISE/NEOWISE (Grav+, 2012)
J/ApJ/744/197 : WISE/NEOWISE observations of Hilda asteroids (Grav+, 2012)
J/ApJ/743/156 : NEOWISE obs. of NEOs: preliminary results (Mainzer+, 2011)
J/ApJ/742/40 : Jovian Trojans asteroids with WISE/NEOWISE (Grav+, 2011)
J/ApJ/741/68 : Main Belt asteroids with WISE/NEOWISE. I. (Masiero+, 2011)
J/A+A/511/A49 : Lightcurves of 12 NEAs (Kwiatkowski+, 2010)
J/A+A/511/A40 : Near Earth Asteroids positions (Birlan+, 2010)
J/A+A/509/A27 : Near-Earth asteroids + QSOs close approaches (Nedelcu+, 2010)
J/A+A/375/285 : Photometric observations of 9 Near-Earth Objects (Szabo+, 2001)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- MPC Trojan asteroid name, in MPC packed format
9- 13 F5.2 mag HMag [12.7/22.6] Absolute H band magnitude (1)
15- 18 F4.2 --- G Magnitude slope parameter (1)
20- 25 F6.3 km Diam [0.1/26.7] Diameter (1)
27- 31 F5.3 km e_Diam The 1σ uncertainty in Diam (1)
33- 37 F5.3 --- pV Visible geometrical albedo (1)
39- 43 F5.3 --- e_pV The 1σ uncertainty in pV (1)
45- 49 F5.3 --- eta Beaming parameter η (1)
51- 55 F5.3 --- e_eta The 1σ uncertainty in eta (1)
57- 61 F5.3 --- pIR Infrared geometrical albedo (1)
63- 67 F5.3 --- e_pIR The 1σ uncertainty in pIR (1)
69- 71 I3 --- N1 Number of WISE/W1 (3.4um) band observations
73- 75 I3 --- N2 Number of WISE/W2 (4.6um) band observations
77- 79 I3 --- N3 Number of WISE/W3 (11.6um) band observations
81- 82 I2 --- N4 Number of WISE/W4 (22.1um) band observations
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Note (1): The 1σ errors presented here were statistically generated
using Monte Carlo modeling. WISE fluxes, absolute magnitude H, and G
were varied by their 1σ error bars, as well as beaming (η)
and pIR when these two parameters could not be fitted. The quoted
precision for each parameter follows the object with the most
significant figures for the error on that value in the table. The
statistical errors on diameter and pV for each object in the table
should be added in quadrature to the ±20% and ±50% systematic
errors described in the text.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 31-Jul-2014