Composition of KBO (50000) Quaoar

Ore, C. M. Dalle; Barucci, Maria Antonietta; Emery, Joshua P.; Cruikshank, D. P.; Ore, L. V. Dalle; Merlin, F.; Álvarez-Candal, A.; Bérgh, C. de; Trilling, David E.; Perna, D.; Fornasier, S.; Mastrapa, Rachel M. E.; Dotto, E.

doi:10.1051/0004-6361/200911752

Cited by 52 publications

(36 citation statements)

References 36 publications

(60 reference statements)

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“…The spectra are compared with a previously obtained spectrum (Q2008 in Fig. 1) also acquired at the VLT-ESO facility, but with different instruments (FORS for the visible, ISAAC for the J-band, and SINFONI for the H-and K-bands) whose spectra were adjusted by means of photometric colours (Dalle Ore et al 2009). The advantage of the X-Shooter spectrograph is in the simultaneous spectrum acquisition from the visible to the NIR, resulting in the more accurate spectral information needed to investigate surface composition.…”

Section: Discussionmentioning

confidence: 99%

“…Both are indicative of a young surface possibly refreshed by cryo-volcanic activity. The accurate fitting model by Dalle Ore et al (2009) on high quality data reported a surface composition containing crystalline water ice, CH 4 , as well as possibly C 2 H 6 and organic materials, products of irradiation of CH 4 . The band at 2.2 μm was present in the observations of Dalle Ore et al (2009) and was fitted by their model.…”

Section: Introductionmentioning

confidence: 99%

“…The accurate fitting model by Dalle Ore et al (2009) on high quality data reported a surface composition containing crystalline water ice, CH 4 , as well as possibly C 2 H 6 and organic materials, products of irradiation of CH 4 . The band at 2.2 μm was present in the observations of Dalle Ore et al (2009) and was fitted by their model. However, it was attributed to CH 4 , as previously done by Schaller & Brown (2007a), instead of ammonia hydrates.…”

Section: Introductionmentioning

confidence: 99%

“…The data are complemented by previously published photometric observations (Dalle Ore et al 2009) obtained in the NIR (3.6, 4.5 μm) with the Spitzer Space Telescope. Along with the updated visible albedo determined by Fornasier et al (2013), the Spitzer data provide an extra set of constraints in the model calculation process.…”

Section: Introductionmentioning

confidence: 99%

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(50000) Quaoar: Surface composition variability

Barucci

Ore

Perna

et al. 2015

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Aims. The goal of this work is to investigate the composition of the surface of (50000) Quaoar and its spatial variability. Methods. We present new continuous spectra from the visible to near-IR (0.3−2.3 μm) obtained with the X-Shooter instrument at the VLT-ESO at four different epochs on the surface of Quaoar. The data represent the highest spectral resolution data ever obtained for this object and the first near-IR dataset acquired in a single exposure over the entire wavelength range. They are complemented by previously published photometric observations obtained in the near-IR (3.6, 4.5 μm) with the Spitzer Space Telescope, which provide an extra set of constraints in the model calculation. Spectral modelling was performed for the entire wavelength range by means of a code based on the Shkuratov radiative transfer formulation and of an updated value of albedo obtained from recent Herschel observations. Results. We obtained compositional information for different observed areas that can cover about 40% of the assumed rotational period of 8.84 h. Our analysis helps to prove the presence of CH 4 and C 2 H 6 , as previously reported, along with indications of the possible presence of NH 3 ·H 2 O. New evidence of N 2 is inferred from the shift in the CH 4 bands. The albedo at the two Spitzer bands suggests there may be CO diluted in N 2 , and CO 2 for one of the surface locations. Conclusions. The spectral similarities indicate the overall homogeneity of the surface composition of one hemisphere of Quaoar, while some subtle variations are apparent when modelling. The presence of NH 3 ·H 2 O would support the idea that Quaoar's surface may be relatively young.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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(50000) Quaoar: Surface composition variability

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Perna

et al. 2015

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“…Similarly, tholins are an effective coloring agent in models of solid surfaces (e.g., Hoffman et al 1993;Dalle Ore et al 2009;Owen et al 2001;and Cruikshank et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Organic materials in planetary and protoplanetary systems: nature or nurture?

Ore

Fulchignoni

Cruikshank

et al. 2011

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Aims. The objective of this work is to summarize the discussion of a workshop aimed at investigating the properties, origins, and evolution of the materials that are responsible for the red coloration of the small objects in the outer parts of the solar system. Because of limitations or inconsistencies in the observations and, until recently, the limited availability of laboratory data, there are still many questions on the subject. Our goal is to approach two of the main questions in a systematic way: -Is coloring an original signature of materials that are presolar in origin ("nature") or stems from post-formational chemical alteration, or weathering ("nurture")? -What is the chemical signature of the material that causes spectra to be sloped towards the red in the visible? We examine evidence available both from the laboratory and from observations sampling different parts of the solar system and circumstellar regions (disks). Methods. We present a compilation of brief summaries gathered during the workshop and describe the evidence towards a primordial vs. evolutionary origin for the material that reddens the small objects in the outer parts of our, as well as in other, planetary systems. We proceed by first summarizing laboratory results followed by observational data collected at various distances from the Sun. Results. While laboratory experiments show clear evidence of irradiation effects, particularly from ion bombardment, the first obstacle often resides in the ability to unequivocally identify the organic material in the observations. The lack of extended spectral data of good quality and resolution is at the base of this problem. Furthermore, that both mechanisms, weathering and presolar, act on the icy materials in a spectroscopically indistinguishable way makes our goal of defining the impact of each mechanism challenging. Conclusions. Through a review of some of the workshop presentations and discussions, encompassing laboratory experiments as well as observational data, we infer that both "nature" and "nurture" are instrumental in the coloration of small objects in the outer parts Article published by EDP Sciences A98, page 1 of 14 A&A 533, A98 (2011) of the solar system. While in the case of some observations it is clear that the organic reddening material originated before the solar nebula (i.e. presolar grains found in meteorites), for many other cases pointers are not as clear and indicate a concurrence of both processes.

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