Rotationally resolved spectroscopy of dwarf planet (136472) Makemake

Lorenzi, V.; Pinilla-Alonso, N.; Licandro, J.

doi:10.1051/0004-6361/201425575

Cited by 20 publications

(20 citation statements)

References 37 publications

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“…The spectral properties of Pluto, compared to those of Makemake and Eris, support that Pluto's surface holds a similar amount of solid complex organics (the coloring agent) as Makemake, while Eris's surface has a lesser amount of organics than them both, as previously suggested (e.g., Licandro et al 2006b;Alvarez-Candal et al 2011;Lorenzi et al 2015). On the other hand, our spectra confirm that methane is less abundant in the Pluto's surface than on those of Eris and Makemake, as previously reported by Licandro et al (2006b).…”

Section: Discussionsupporting

confidence: 76%

The spectrum of Pluto, 0.40–0.93μm

Lorenzi

Pinilla-Alonso

Licandro

et al. 2016

A&A

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Context. During the past 30 years the surface of Pluto has been characterized and its variability monitored through continuous nearinfrared spectroscopic observations. But in the visible range only a few data are available. Aims. The aim of this work is to define Pluto's relative reflectance in the visible range to characterize the different components of its surface, and to provide ground based observations in support of the New Horizons mission. Methods. We observed Pluto on six nights between May and July 2014 with the imager/spectrograph ACAM at the William Herschel Telescope (La Palma, Spain). The six spectra obtained cover a whole rotation of Pluto (P rot = 6.4 days). For all the spectra, we computed the spectral slope and the depth of the absorption bands of methane ice between 0.62 and 0.90 μm. To search for shifts in the center of the methane bands, which are associated with dilution of CH 4 in N 2 , we compared the bands with reflectances of pure methane ice. Results. All the new spectra show the methane ice absorption bands between 0.62 and 0.90 μm. Computation of the depth of the band at 0.62 μm in the new spectra of Pluto and in the spectra of Makemake and Eris from the literature, allowed us to estimate the Lambert coefficient at this wavelength at temperatures of 30 K and 40 K, which has never been measured before. All the detected bands are blueshifted with respect to the position for pure methane ice, with minimum shifts correlated to the regions where the abundance of methane is higher. This could be indicative of a dilution of CH 4 :N 2 that is more saturated in CH 4 . The longitudinal and secular variations in the parameters measured in the spectra are in accordance with results previously reported in the literature and with the distribution of the dark and bright materials that show the Pluto's color maps from New Horizons.

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Section: Discussionsupporting

confidence: 76%

The spectrum of Pluto, 0.40–0.93μm

Lorenzi

Pinilla-Alonso

Licandro

et al. 2016

A&A

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“…Such mixtures are representative of the main composition for methane and nitrogenrich surfaces of the dwarf planet Pluto (Cruikshank et al 2015;Grundy et al 2016) and are also relevant for some surfaces on other dwarf planets (e.g. Eris, Makemake, see Licandro et al 2006;Lorenzi et al 2015). Thousands of smaller objects in the Kuiper belt and Oort cloud regions should possess the same kind of surface composition, but their spectra are not yet accessible owing to their magnitudes that are too low.…”

Section: Methodsmentioning

confidence: 99%

“…Indeed because of the presence of abundant water ice in protoplanetary disk and dense interstellar environments, the matter recovered should present some features related to a higher amount of incorporated oxygen atoms in the solid network, whereas the organic matter of UCAMMs exhibits a low O/C ratio. In the last two scenarios, the formation of nitrogenrich organic matter in the outermost regions of the solar system can be explained, since nitrogen and methane rich ices are condensed at the surface of icy bodies (Protopapa et al 2016;Grundy et al 2016;Licandro et al 2006;Lorenzi et al 2015;Cruikshank et al 2015), and water ice is buried and protected from the ambient radiation fields. These scenarios are favoured to explain the formation of N-rich organic matter because of the expected final organic matter composition and the volume of irradiated material.…”

Section: Introductionmentioning

confidence: 99%

Irradiation of nitrogen-rich ices by swift heavy ions

Augé

Dartois

Engrand

et al. 2016

A&A

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Context. Extraterrestrial materials, such as meteorites and interplanetary dust particles, provide constraints on the formation and evolution of organic matter in the young solar system. Micrometeorites represent the dominant source of extraterrestrial matter at the Earth's surface, some of them originating from large heliocentric distances. Recent analyses of ultracarbonaceous micrometeorites recovered from Antarctica (UCAMMs) reveal an unusually nitrogen-rich organic matter. Such nitrogen-rich carbonaceous material could be formed in a N 2 -rich environment, at very low temperature, triggered by energetic processes. Aims. Several formation scenarios have been proposed for the formation of the N-rich organic matter observed in UCAMMs. We experimentally evaluate the scenario involving high energy irradiation of icy bodies subsurface orbiting at large heliocentric distances. Methods. The effect of Galactic cosmic ray (GCR) irradiation of ices containing N 2 and CH 4 was studied in the laboratory. The N 2 -CH 4 (90:10 and 98:2) ice mixtures were irradiated at 14 K by 44 MeV Ni 11+ and 160 MeV Ar 15+ swift heavy ion beams. The evolution of the samples was monitored using in-situ Fourier transform infrared spectroscopy. The evolution of the initial ice molecules and new species formed were followed as a function of projectile fluence. After irradiation, the target was annealed to room temperature. The solid residue of the whole process left after ice sublimation was characterized in-situ by infrared spectroscopy, and the elemental composition was measured ex-situ. Results. The infrared bands that appear during irradiation allow us to identify molecules and radicals (HCN, CN − , NH 3 , ...). The infrared spectra of the solid residues measured at room temperature show similarities with that of UCAMMs. The results point towards the efficient production of a poly-HCN-like residue from the irradiation of N 2 -CH 4 rich surfaces of icy bodies. The room temperature residue provides a viable precursor for the N-rich organic matter found in UCAMMs.

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“…The bulk density of the 2007 OR 10 system would also be of significant interest, especially in comparison with that of Makemake, an object of very similar size (D ≈ 1430km), but with much higher albedo (0.4, vs. 0.09 for 2007 OR 10 ) and covered in volatile CH 4 ice (Brown et al 2015;Lorenzi et al 2015). Facilities: HST(STIS) …”

Section: Possible Orbits Of the Satellitementioning

confidence: 99%

Discovery of a Satellite of the Large Trans-Neptunian Object (225088) 2007 OR₁₀

Kiss

Márton

Farkas-Takács

et al. 2017

ApJL

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ABSTRACT2007 OR 10 is currently the third largest known dwarf planet in the Transneptunian region, with an effective radiometric diameter of ∼1535 km. It has a slow rotation period of ∼45 h that was suspected to be caused by tidal interactions with a satellite undetected at that time. Here we report on the discovery of a likely moon of 2007 OR 10 , identified on archival Hubble Space Telescope WFC3/UVIS system images. Although the satellite is detected at two epochs, this does not allow an unambiguous determination of the orbit and the orbital period. A feasible 1.5-5.8·10 21 kg estimate for the system mass leads to a likely 35 to 100 d orbital period. The moon is about 4. m 2 fainter than 2007 OR 10 in HST images that corresponds to a diameter of 237 km assuming equal albedos with the primary. Due to the relatively small size of the moon the previous size and albedo estimates for the primary remains unchanged. With this discovery all trans-Neptunian objects larger than 1000 km are now known to harbour satellites, an important constraint for moon formation theories in the young Solar system.

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Rotationally resolved spectroscopy of dwarf planet (136472) Makemake

Cited by 20 publications

References 37 publications

The spectrum of Pluto, 0.40–0.93μm

The spectrum of Pluto, 0.40–0.93μm

Irradiation of nitrogen-rich ices by swift heavy ions

Discovery of a Satellite of the Large Trans-Neptunian Object (225088) 2007 OR₁₀

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Rotationally resolved spectroscopy of dwarf planet (136472) Makemake

Cited by 20 publications

References 37 publications

The spectrum of Pluto, 0.40–0.93μm

The spectrum of Pluto, 0.40–0.93μm

Irradiation of nitrogen-rich ices by swift heavy ions

Discovery of a Satellite of the Large Trans-Neptunian Object (225088) 2007 OR10

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Product

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Discovery of a Satellite of the Large Trans-Neptunian Object (225088) 2007 OR₁₀