<i>WISE</i>/<i>NEOWISE</i>OBSERVATIONS OF THE JOVIAN TROJAN POPULATION: TAXONOMY

Grav, T.; Mainzer, Amy; Bauer, J. M.; Masiero, J.; Nugent, C.

doi:10.1088/0004-637x/759/1/49

Cited by 107 publications

(185 citation statements)

References 51 publications

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“…For the spectrum from 0.4 to 2.5 μm we use the mean red and less-red spectra of Emery et al (2011) scaled to the mean measured visible albedos from Grav et al (2012). From 2.2 to 3.8 μm we use our average spectra for the red and less-red spectral types, scaled to match the small 2.2-2.5 μm overlap region.…”

Section: Spectral Modelingmentioning

confidence: 99%

“…The "red" and "less-red" populations differ in their optical and near-infrared colors, their infrared reflectivities measured from the WISE spacecraft, and in their size distributions (Emery et al 2011;Grav et al 2012;Wong et al 2014;Wong & Brown 2015), yet seem completely mixed dynamically. It is not known whether these two color populations represent distinct source populations, distinct dynamical pathways, distinct collision histories, or some other set of mechanisms.…”

Section: Introductionmentioning

confidence: 99%

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THE 3–4 μm SPECTRA OF JUPITER TROJAN ASTEROIDS

Brown

2016

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To date, reflectance spectra of Jupiter Trojan asteroids have revealed no distinctive absorption features. For this reason, the surface composition of these objects remains a subject of speculation. Spectra have revealed, however, that the Jupiter Trojan asteroids consist of two distinct sub-populations that differ in the optical to near-infrared colors. The origins and compositional differences between the two sub-populations remain unclear. Here, we report the results from a 2.2-3.8 μm spectral survey of a collection of 16 Jupiter Trojan asteroids, divided equally between the two sub-populations. We find clear spectral absorption features centered around 3.1 μm in the less-red population. Additional absorption consistent with that expected from organic materials might also be present. No such features are see in the red population. A strong correlation exists between the strength of the 3.1 μm absorption feature and the optical to near-infrared color of the objects. While, traditionally, absorptions such as these in dark asteroids are modeled as being due to fine-grain water frost, we find it physically implausible that the special circumstances required to create such fine-grained frost would exist on a substantial fraction of the Jupiter Trojan asteroids. We suggest, instead, that the 3.1 μm absorption on Trojans and other dark asteroids could be due to N-H stretch features. Additionally, we point out that reflectivities derived from WISE observations show a strong absorption beyond 4 μm for both populations. The continuum of 3.1 μm features and the common absorption beyond 4 μm might suggest that both sub-populations of Jupiter Trojan asteroids formed in the same general region of the early solar system.

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Section: Spectral Modelingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

THE 3–4 μm SPECTRA OF JUPITER TROJAN ASTEROIDS

Brown

2016

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“…We gratefully acknowledge the helpful inputs from referees M. Delbo and A. Harris of DLR. Grav et al 2011aGrav et al , 2012b to the optically-selected sample observed by Spitzer (light gray squares Fernández et al 2009); the solid and dashed lines give the running medians for the NEOWISE and Spitzer samples, respectively. Fig.…”

Section: Acknowledgmentsmentioning

confidence: 99%

Space-Based Thermal Infrared Studies of Asteroids

Mainzer¹,

Usui²,

Trilling³

2015

Asteroids IV

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Large-area surveys operating at mid-infrared wavelengths have proven to be a valuable means of discovering and characterizing minor planets. Through the use of radiometric models, it is possible to derive physical properties such as diameters, albedos, and thermal inertia for large numbers of objects. Modern detector array technology has resulted in a significant improvement in spatial resolution and sensitivity compared with previous generations of spacebased infrared telescopes, giving rise to a commensurate increase in the number of objects that have been observed at these wavelengths. Space-based infrared surveys of asteroids therefore offer an effective method of rapidly gathering information about small body populations orbital and physical properties. The AKARI, WISE/NEOWISE, Spitzer, and Herschel missions have significantly increased the number of minor planets with well-determined diameters and albedos.

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“…As in Bauer et al (2011Bauer et al ( , 2012, we performed blackbody temperature fits to the dust coma region surrounding the nucleus, extracting the W3 and W4 measured nucleus flux contribution from the thermal signal. We also estimated the W1 and W2 nucleus contribution, based on the thermal fit results for the size and albedo computed using W3 and W4 and scaling the reflected light contribution to the appropriate phase angle, assuming an IR albedo twice that of the visual-wavelength albedo (Grav et al 2011). W3 and W4 fluxes from the nucleus represent less than 11% of the total signal in the 11-arcsec aperture photometry for VA.…”

Section: Dust Photometry and Co/co 2 Productionmentioning

confidence: 99%

WISE/NEOWISE PRELIMINARY ANALYSIS AND HIGHLIGHTS OF THE 67P/CHURYUMOV-GERASIMENKO NEAR NUCLEUS ENVIRONS

Bauer

Kramer

Stevenson

et al. 2012

ApJ

Self Cite

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On 2010 January 18-19 and June 28-29, the Wide-field Infrared Survey Explorer (WISE) spacecraft imaged the Rosetta mission target, comet 67P/Churyumov-Gerasimenko. We present a preliminary analysis of the images, which provide a characterization of the dust environment at heliocentric distances similar to those planned for the initial spacecraft encounter, but on the outbound leg of its orbit rather than the inbound. Broadband photometry yields low levels of CO 2 production at a comet heliocentric distance of 3.32 AU and no detectable production at 4.18 AU. We find that at these heliocentric distances, large dust grains with mean grain diameters on the order of a millimeter or greater dominate the coma and evolve to populate the tail. This is further supported by broadband photometry centered on the nucleus, which yield an estimated differential dust particle size distribution with a power-law relation that is considerably shallower than average. We set a 3σ upper limit constraint on the albedo of the large-grain dust at 0.12. Our best estimate of the nucleus radius (1.82 ± 0.20 km) and albedo (0.04 ± 0.01) are in agreement with measurements previously reported in the literature.

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WISE/NEOWISEOBSERVATIONS OF THE JOVIAN TROJAN POPULATION: TAXONOMY

Cited by 107 publications

References 51 publications

THE 3–4 μm SPECTRA OF JUPITER TROJAN ASTEROIDS

THE 3–4 μm SPECTRA OF JUPITER TROJAN ASTEROIDS

Space-Based Thermal Infrared Studies of Asteroids

WISE/NEOWISE PRELIMINARY ANALYSIS AND HIGHLIGHTS OF THE 67P/CHURYUMOV-GERASIMENKO NEAR NUCLEUS ENVIRONS

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