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J/ApJ/792/30      NEOWISE magnitudes for near-Earth objects     (Mainzer+, 2014)

Initial performance of the NEOWISE reactivation mission. Mainzer A., Bauer J., Cutri R.M., Grav T., Masiero J., Beck R., Clarkson P., Conrow T., Dailey J., Eisenhardt P., Fabinsky B., Fajardo-Acosta S., Fowler J., Gelino C., Grillmair C., Heinrichsen I., Kendall M., Kirkpatrick J.D., Liu F., Masci F., McCallon H., Nugent C.R., Papin M., Rice E., Royer D., Ryan T., Sevilla P., Sonnett S., Stevenson R., Thompson D.B., Wheelock S., Wiemer D., Wittman M., Wright E., Yan L. <Astrophys. J., 792, 30 (2014)> =2014ApJ...792...30M (SIMBAD/NED BibCode)
ADC_Keywords: Minor planets ; Comets ; Photometry, infrared ; Surveys Keywords: comets: general - infrared: general - minor planets, asteroids: general - space vehicles - surveys Abstract: NASA's Wide-field Infrared Survey Explorer (WISE) spacecraft has been brought out of hibernation and has resumed surveying the sky at 3.4 and 4.6 µm. The scientific objectives of the NEOWISE reactivation mission are to detect, track, and characterize near-Earth asteroids and comets. The search for minor planets resumed on 2013 December 23, and the first new near-Earth object (NEO) was discovered 6 days later. As an infrared survey, NEOWISE detects asteroids based on their thermal emission and is equally sensitive to high and low albedo objects; consequently, NEOWISE-discovered NEOs tend to be large and dark. Over the course of its three-year mission, NEOWISE will determine radiometrically derived diameters and albedos for ∼2000 NEOs and tens of thousands of Main Belt asteroids. The 32 months of hibernation have had no significant effect on the mission's performance. Image quality, sensitivity, photometric and astrometric accuracy, completeness, and the rate of minor planet detections are all essentially unchanged from the prime mission's post-cryogenic phase. Description: Regular survey operations, including the moving object processing pipeline, began on 2013 December 23; the first new NEO was discovered 6 days later. The NEOWISE operational cadence remains identical to that employed during the prime mission (Wright et al. 2010AJ....140.1868W; Heinrichsen & Wright 2006SPIE.6270E..1CH). The telescope scans continuously along great circles with approximately constant ecliptic longitude, while a scan mirror freezes the sky on the focal planes for 9.9 s and returns to its starting position 1.1 s later. While the sky is fixed on the focal planes, simultaneous exposures are collected in the W1 and W2 bands through the use of beamsplitters every 11 s with an exposure time of 7.7 s. Based on its present rate of NEO observations, over the course of its three year mission, NEOWISE is expected to observe ∼2000 NEOs, roughly 700-800 of which will be detected in single-exposure images, with the remainder being recoverable through stacking. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 84 59 Thermal Fit Results for the NEO Detections Reported in this Work table1.dat 51 806 Preliminary NEOWISE magnitudes for the NEOs shown in Figure 15 at each observation's modified Julian date
See also: II/311 : WISE All-Sky Data Release (Cutri+ 2012) J/A+A/375/285 : Photometric observations of 9 Near-Earth Objects (Szabo+, 2001) J/ApJ/743/156 : NEOWISE observations of NEOs: preliminary results (Mainzer+, 2011) J/ApJ/760/L12 : WISE/NEOWISE NEOs preliminary thermal fits (Mainzer+, 2012) J/ApJ/784/110 : NEOWISE observations of 105 near-Earth objects (Mainzer+, 2014) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Name Identifier 9- 18 A10 --- OName Other name 20- 24 F5.2 mag H H magnitude 26- 29 F4.2 -- G Phase curve slope parameter 31- 35 F5.3 km D Diameter 37- 41 F5.3 km e_D rms uncertainty on D 43- 47 F5.3 --- pV Visible albedo 49- 53 F5.3 --- e_pV rms uncertaitny on pV (1) 55- 59 F5.3 --- eta Beaming parameter 61- 65 F5.3 --- e_eta rms uncertaitny on eta (1) 67- 71 F5.3 --- pIR Infrared albedo 73- 77 F5.3 --- e_pIR rms uncertaitny on pIR (1) 79- 80 I2 --- NobsW1 Number of observations in NEOWISE W1 band 82- 84 I3 --- NobsW2 Number of observations in NEOWISE W2 band
Note (1): The 1σ errors presented here were statistically generated using Monte Carlo modeling. NEOWISE magnitudes, absolute magnitude H, and G were varied by their 1σ error bars, as well as beaming (eta) and pIR when these two parameters could not be fit. The statistical errors on diameter and pV for each object in the table should be added in quadrature to the systematic errors described in the text and discussed in Mainzer et al. (2012ApJ...745....7M).
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Name Identifier 9- 21 F13.7 d MJD Modified Julian Date of observation 23 A1 --- l_3.4mag The 2σ upper limit flag on 3.4mag (1) 25- 30 F6.3 mag 3.4mag NEOWISE 3.4 micron band magnitude 32- 36 F5.3 mag e_3.4mag ? Uncertainty in 3.4mag 38- 43 F6.3 mag 4.6mag NEOWISE 4.6 micron band magnitude 45- 49 F5.3 mag e_4.6mag Uncertainty in 4.6mag 51 I1 --- FAper [0] flag for aperture radius used for photometry (2)
Note (1): See Cutri et al. 2012, cat II/311 ( Note (2): Flag for aperture radius as follows: 0 = pipeline profile fit photometry was used.
History: From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 05-Apr-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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