The trans-neptunian object UB313 is larger than Pluto

Bertoldi, F.; Altenhoff, W. J.; Weiß, A.; Menten, K. M.; Thum, C.

doi:10.1038/nature04494

Cited by 58 publications

(29 citation statements)

References 7 publications

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“…Prior to our measurements, Eris' size and albedo have been determined by several groups and methods. The first measurement was achieved by Bertoldi et al (2006) who used IRAM thermal observations at 1200 μm and obtained D = 3000 +300 −100 km and p V = 60 ± 10%. Subsequently, Brown et al (2006) (1-σ) of which have an effective diameter of 2330 ± 180 km.)…”

Section: Ormentioning

confidence: 99%

“TNOs are Cool”: A survey of the trans-Neptunian region

Santos-Sanz

Lellouch

Fornasier

et al. 2012

A&A

145

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Context. Physical characterization of trans-Neptunian objects, a primitive population of the outer solar system, may provide constraints on their formation and evolution. Aims. The goal of this work is to characterize a set of 15 scattered disk (SDOs) and detached objects, in terms of their size, albedo, and thermal properties. Methods. Thermal flux measurements obtained with the Herschel-PACS instrument at 70, 100 and 160 μm, and whenever applicable, with Spitzer-MIPS at 24 and 70 μm, are modeled with radiometric techniques, in order to derive the objects' individual size, albedo and when possible beaming factor. Error bars are obtained from a Monte-Carlo approach. We look for correlations between these and other physical and orbital parameters. Results. Diameters obtained for our sample range from 100 to 2400 km, and the geometric albedos (in V band) vary from 3.8% to 84.5%. The unweighted mean V geometric albedo for the whole sample is 11.2% (excluding Eris); 6.9% for the SDOs, and 17.0% for the detached objects (excluding Eris). We obtain new bulk densities for three binary systems: Ceto/Phorcys, Typhon/Echidna and Eris/Dysnomia. Apart from correlations clearly due to observational bias, we find significant correlations between albedo and diameter (more reflective objects being bigger), and between albedo, diameter and perihelion distance (brighter and bigger objects having larger perihelia). We discuss possible explanations for these correlations.

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Section: Ormentioning

confidence: 99%

“TNOs are Cool”: A survey of the trans-Neptunian region

Santos-Sanz

Lellouch

Fornasier

et al. 2012

A&A

145

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“…More recent observations from the Institut de Radioastronomie Millimétrique (IRAM) telescope succeeded in detecting a flux of 1.27 ‫ע‬ mJy at 1.2 mm, suggesting a size between 2600 and 0.29 3400 km and an albedo between 42% and 72% (Bertoldi et al 2006). An object of this size would have an angular diameter seen from the Earth of between 37 and 48 mas, similar to or larger than Quaoar, and thus should be directly resolvable from HST observations.…”

Section: Introductionmentioning

confidence: 99%

Direct Measurement of the Size of 2003 UB313 from theHubble Space Telescope

Brown

Schaller

Roe

et al. 2006

ApJ

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We have used the Hubble Space Telescope to directly measure the angular size of the large Kuiper Belt object 2003 UB313. By carefully calibrating the point-spread function of a nearby field star, we measure the size of 2003 UB313 to be mas, corresponding to a diameter of km or a size ∼5% larger than 34.3 ‫ע‬ 1.4 2400 ‫ע‬ 100 Pluto. The V-band geometric albedo of 2003 UB313 is . The extremely high albedo is consistent with 86% ‫ע‬ 7% the frosty methane spectrum, the lack of red coloring, and the lack of observed photometric variation on the surface of 2003 UB313. Methane photolysis should quickly darken the surface of 2003 UB313, but continuous evaporation and redeposition of surface ices appears capable of maintaining the extreme albedo of this body.

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“…with pericenter decoupled from Neptune (Gladman et al 2007). The first diameter estimation was determined by Bertoldi et al (2006) by combining optical brightness measurements with millimeter wavelength observations. Based on the measured thermal emission, Bertoldi et al derived a diameter of 3000 ± 300 km and a visible albedo of 0.60 ± 0.10.…”

Section: Introductionmentioning

confidence: 99%

Surface composition of the largest dwarf planet 136199 Eris (2003 UB${_{313}}$)

Dumas¹,

Merlin²,

Barucci³

et al. 2007

A&A

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Aims. The surface composition of the largest TNO, the dwarf planet 136199 Eris, is studied and compared to Pluto's. Methods. High signal-to-noise visible and near-infrared reflectance spectra were obtained at the TNG and ESO-VLT observatories. The nature and properties of the compounds present on the surface of Eris are investigated by applying Hapke and Shkuratov radiative transfer models to our spectra. Results. The surface of Eris can be modeled using two areas of distinct composition: about 50% appears to be covered with pure methane ice, while the rest of its surface would be made of an intimate mixture of methane, nitrogen and water ices, and ice tholin. The use of nitrogen in our model is shown to improve significantly the data fit, in particular for high surface albedo values. The icy grains are found to be large, from sub-mm to a few tens of mm in size.

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The trans-neptunian object UB313 is larger than Pluto

Cited by 58 publications

References 7 publications

“TNOs are Cool”: A survey of the trans-Neptunian region

“TNOs are Cool”: A survey of the trans-Neptunian region

Direct Measurement of the Size of 2003 UB313 from theHubble Space Telescope

Surface composition of the largest dwarf planet 136199 Eris (2003 UB${_{313}}$)

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