Results from a triple chord stellar occultation and far-infrared photometry of the trans-Neptunian object (229762) 2007 UK<sub>126</sub>

Schindler, Karsten; Wolf, Jürgen; Bardecker, J.; Olsen, Aart M.; Müller, Thomas; Kiss, Csaba; Ortiz, J. L.; Braga-Ribas, F.; Camargo, J. I. B.; Herald, D.; Krabbe, A.

doi:10.1051/0004-6361/201628620

Cited by 20 publications

(16 citation statements)

References 55 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Recent works with this TPM code (e.g. Pál et al 2015Pál et al , 2016Schindler et al 2017;Fornasier et al 2013) have shown that a combined analysis of Herschel and Spitzer thermal measurements enable us to constrain the spin-axis orientation of TNOs. Following up on this expertise, we also applied this code in the case of 2003 AZ 84 , assuming a spherical shape model and a constant emissivity of 0.9 at all MIPS and PACS wavelengths (emissivity effects are only expected at longer wavelengths, see Fornasier et al 2013).…”

Section: Analysis Of 2003 Az 84 Resultsmentioning

confidence: 99%

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

Santos-Sanz

Lellouch

Groussin

et al. 2017

A&A

Self Cite

View full text Add to dashboard Cite

Context. Time series observations of the dwarf planet Haumea and the Plutinos 2003 VS 2 and 2003 AZ 84 with Herschel/PACS are presented in this work. Thermal emission of these trans-Neptunian objects (TNOs) were acquired as part of the "TNOs are Cool" Herschel Space Observatory key programme. Aims. We search for the thermal light curves at 100 and 160 µm of Haumea and 2003 AZ 84 , and at 70 and 160 µm for 2003 VS 2 by means of photometric analysis of the PACS data. The goal of this work is to use these thermal light curves to obtain physical and thermophysical properties of these icy Solar System bodies. Methods. When a thermal light curve is detected, it is possible to derive or constrain the object thermal inertia, phase integral and/or surface roughness with thermophysical modeling. Results. Haumea's thermal light curve is clearly detected at 100 and 160 µm. The effect of the reported dark spot is apparent at 100 µm. Different thermophysical models were applied to these light curves, varying the thermophysical properties of the surface within and outside the spot. Although no model gives a perfect fit to the thermal observations, results imply an extremely low thermal inertia (<0.5 J m −2 s −1/2 K −1 , hereafter MKS) and a high phase integral (>0.73) for Haumea's surface. We note that the dark spot region appears to be only weakly different from the rest of the object, with modest changes in thermal inertia and/or phase integral. The thermal light curve of 2003 VS 2 is not firmly detected at 70 µm and at 160 µm but a thermal inertia of (2 ± 0.5) MKS can be derived from these data. The thermal light curve of 2003 AZ 84 is not firmly detected at 100 µm. We apply a thermophysical model to the mean thermal fluxes and to all the Herschel/PACS and Spitzer/MIPS thermal data of 2003 AZ 84 , obtaining a close to pole-on orientation as the most likely for this TNO. Conclusions. For the three TNOs, the thermal inertias derived from light curve analyses or from the thermophysical analysis of the mean thermal fluxes confirm the generally small or very small surface thermal inertias of the TNO population, which is consistent with a statistical mean value Γ mean = 2.5 ± 0.5 MKS.

show abstract

Section: Analysis Of 2003 Az 84 Resultsmentioning

confidence: 99%

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

Santos-Sanz

Lellouch

Groussin

et al. 2017

A&A

Self Cite

View full text Add to dashboard Cite

show abstract

“…Considering this, we also plot all known objects. The observed population is taken from the Minor Planet Center (on 10th October 2017), with measured radii from occulations (Elliot et al 2010;Sicardy et al 2011;Braga-Ribas et al 2013;Alvarez-Candal et al 2014;Dias-Oliveira et al 2017;Schindler et al 2017), direct imaging (Nimmo et al 2017), thermal modelling (Lim et al 2010;Müller et al 2010;Mommert et al 2012;Pál et al 2012;Santos-Sanz et al 2012;Vilenius et al 2012;Fornasier et al 2013;Lellouch et al 2013;Vilenius et al 2014), or by assuming albedos of (D/250 km) 2 + 6 % per Fraser et al (2014), in that order of priority. Masses for objects with satellites were taken from Benecchi et al (2010); Brown (2013); Brown & Schaller (2007); Carry et al (2011);Fraser et al (2013); Grundy et al (2007Grundy et al ( , 2008Grundy et al ( , 2009Grundy et al ( , 2011Grundy et al ( , 2012Grundy et al ( , 2015; Kovalenko et al (2017); Margot et al (2004); Parker et al (2011); Ragozzine & Brown (2009);Sheppard, Ragozzine & Trujillo (2012); Stansberry et al (2012); Stern et al (2015); Veillet et al (2002).…”

Section: Observations and Our Inferences Of The Pastmentioning

confidence: 99%

Limits on the number of primordial Scattered disc objects at Pluto mass and higher from the absence of their dynamical signatures on the present-day trans-Neptunian Populations

Shannon

Dawson

2018

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Today, Pluto and Eris are the largest and most massive Trans-Neptunian Objects respectively. They are believed to be the last remnants of a population of planetesimals that has been reduced by > 99% since the time of its formation. This reduction implies a primordial population of hundreds or thousands of Pluto-mass objects, and a mass-number distribution that could have extended to hundreds of Lunas, dozens of Mars, and several Earths. Such lost protoplanets would have left signatures in the dynamics of the present-day Trans-Neptunian Populations, and we statistically limit their primordial number by considering the survival of ultra-wide binary TNOs, the Cold Classical Kuiper belt, and the resonant population. We find that if the primordial mass-number distribution extended to masses greater than Pluto ∼ 10 −3 M ⊕ , it must have turned downwards to be no more top-heavy than roughly equal mass per log size, a significant deviation from the distribution observed between 10 −5 M ⊕ and 10 −3 M ⊕ . We compare these limits to the predicted mass-number distribution of various planetesimal and proto-planet growth models. The limits derived here provide a test for future models of planetesimal formation.

show abstract

“…Our analysis is based on the data obtained during the "TNOs are cool" program, which contains 28 binary and 2 triple systems A&A 608, A19 (2017) Schindler et al (2017) 3.79 --…”

Section: Datasetmentioning

confidence: 99%

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

Kovalenko

Doressoundiram

Lellouch

et al. 2017

A&A

Self Cite

View full text Add to dashboard Cite

Context. Gravitationally bound multiple systems provide an opportunity to estimate the mean bulk density of the objects, whereas this characteristic is not available for single objects. Being a primitive population of the outer solar system, binary and multiple trans-Neptunian objects (TNOs) provide unique information about bulk density and internal structure, improving our understanding of their formation and evolution. Aims. The goal of this work is to analyse parameters of multiple trans-Neptunian systems, observed with Herschel and Spitzer space telescopes. Particularly, statistical analysis is done for radiometric size and geometric albedo, obtained from photometric observations, and for estimated bulk density. Methods. We use Monte Carlo simulation to estimate the real size distribution of TNOs. For this purpose, we expand the dataset of diameters by adopting the Minor Planet Center database list with available values of the absolute magnitude therein, and the albedo distribution derived from Herschel radiometric measurements. We use the 2-sample Anderson-Darling non-parametric statistical method for testing whether two samples of diameters, for binary and single TNOs, come from the same distribution. Additionally, we use the Spearman's coefficient as a measure of rank correlations between parameters. Uncertainties of estimated parameters together with lack of data are taken into account. Conclusions about correlations between parameters are based on statistical hypothesis testing. Results. We have found that the difference in size distributions of multiple and single TNOs is biased by small objects. The test on correlations between parameters shows that the effective diameter of binary TNOs strongly correlates with heliocentric orbital inclination and with magnitude difference between components of binary system. The correlation between diameter and magnitude difference implies that small and large binaries are formed by different mechanisms. Furthermore, the statistical test indicates, although not significant with the sample size, that a moderately strong correlation exists between diameter and bulk density.

show abstract

Results from a triple chord stellar occultation and far-infrared photometry of the trans-Neptunian object (229762) 2007 UK₁₂₆

Cited by 20 publications

References 55 publications

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

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

Limits on the number of primordial Scattered disc objects at Pluto mass and higher from the absence of their dynamical signatures on the present-day trans-Neptunian Populations

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

Contact Info

Product

Resources

About

Results from a triple chord stellar occultation and far-infrared photometry of the trans-Neptunian object (229762) 2007 UK126

Cited by 20 publications

References 55 publications

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

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

Limits on the number of primordial Scattered disc objects at Pluto mass and higher from the absence of their dynamical signatures on the present-day trans-Neptunian Populations

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

Contact Info

Product

Resources

About

Results from a triple chord stellar occultation and far-infrared photometry of the trans-Neptunian object (229762) 2007 UK₁₂₆