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Astronomy & Astrophysics manuscript no. MBOSS2 April 26, 2012

c ESO 2012

Colours of Minor Bodies in the Outer Solar System
II - A Statistical Analysis, Revisited
O. R. Hainaut1 , H. Boehnhardt2 , and S. Protopapa3
1

2 3

European Southern Observatory (ESO), Karl Schwarzschild Straúe, 85 748 Garching bei Munchen, Germany ¨ e-mail: ohainaut@eso.org Max-Planck-Institut fur Sonnensystemforschung, Max-Planck Straúe 2, 37 191 Katlenburg¨ Lindau, Germany Department of Astronomy, University of Maryland, College Park, MD 20 742-2421, USA

Received --; accepted --
ABSTRACT

We present an update of the visible and near-infrared colour database of Minor Bodies in the outer Solar System (MBOSSes), now including over 2000 measurement epochs of 555 objects, extracted from 100 articles. The list is fairly complete as of December 2011. The database is now large enough that dataset with a high dispersion can be safely identified and rejected from the analysis. The method used is safe for individual outliers. Most of the rejected papers were from the early days of MBOSS photometry. The individual measurements were combined so not to include possible rotational artefacts. The spectral gradient over the visible range is derived from the colours, as well as the R absolute magnitude M (1, 1). The average colours, absolute magnitude, spectral gradient are listed for each object, as well as their physico-dynamical classes using a classification adapted from Gladman et al., 2008. Colour-colour diagrams, histograms and various other plots are presented to illustrate and investigate class characteristics and trends with other parameters, whose significance are evaluated using standard statistical tests. Except for a small discrepancy for the J - H colour, the largest objects, with M (1, 1) < 5, are not distinguishable from the smaller ones. The larger are slightly bluer than the smaller ones in J - H . The Plutinos and other Resonant Objects, hot Classical Disk Objects, Scattered Disk Objects and Detached Disk Objects have similar properties in the visible, while the cold Classical Disk Objects and the Jupiter Trojans form two separate groups for their spectral properties in the visible wavelength range. The well known colour bimodality of Centaurs is confirmed. The hot Classical Disk Objects with large inclination, or with large orbital excitation are found bluer than the others, a result that was also previously known. Additionally, the hot Classical Disk Objects with a smaller perihelion distance are bluer than those which do not come as close to the Sun. The bluer hot Classical Disk Objects and Resonant Objects have fainter absolute magnitudes than the redder ones from the same class. Finally, we discuss possible scenariis for the origin of the colour diversity observed in MBOSSes, i.e. colouration due to evolutionary processes and due to formation. The colour tables and all the plots are available on-line at http://www.eso.org/ ohainaut/MBOSS, which will be updated when new measurements are published.
Key words. Comets: general ­ Kuiper Belt: general ­ Methods: photometry ­ Methods: statis-

tical ­

1. Introduction
Minor bodies in the outer Solar System (MBOSSes) comprise objects in the Kuiper Belt (KB) and more generally in the Transneptunian (TN) region, as well as small bodies in the giant planets region that came from the KB or TN regions, but are now no longer immediate member of these environments. Centaurs are considered escapees (Gladman et al. 2008; Kavelaars et al. 2008), scattered from the KB and TN environment towards the Sun, possibly also representing a major source of the short-periodic comets (SPCs). Some MBOSSes might also be found among the satellites of the giant planets since they may have been stranded there by gravitational capturing from the Centaur population (Duncan and Levison 1997). Another large population of MBOSSes can be found as long-periodic (LPCs) or Oort Cloud comets. These objects are believed to have formed in the region of the giant planets and be scattered afterwards into the very distant domains of the
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O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

Solar System (Dones et al. 2004), although presently it cannot be excluded that contaminators of extra-solar comets (Levison et al. 2010) may exist among the Oort Cloud population. MBOSSes in the planetary system environment are formed and have evolved in the region of the giant planets. They are considered remnants of the planetesimal population, however, not necessarily in the distance range where they are found today. Nonetheless, they may contain valuable information on the environment and the physical conditions at the time of their formation. On the other side, the long presence in the distant region of the planets and beyond may have caused alterations of physical properties of MBOSSes: for instance, high energy and particle radiation is suspected to modify colours and albedos of materials in space (de Bergh et al. 2008) and collisions can affect the body as a whole (fragmentation or growth) or in parts (resurfacing by excavated material). It can also not be excluded that intrinsic activity may have changed the surface constitution of the MBOSSes, since a number of ices, believed or known to be present in these objects, can sublimate at very large distances from the Sun (Delsemme 1982; Meech and Svoren 2004, for instance C H4 , CO, and N2 up to about 45, 65 and 80AU, respectively;). Last, but not least, larger MBOSSes may have experienced alteration of their internal structure (McKinnon et al. 2008). It is thus of interest to characterize population properties and to explore possible connections with the origin of the bodies and/or their evolutionary pathways in the Solar System. With this study we focus on photometric properties of MBOSSes and the characterization of different dynamical populations among them. The photometric properties comprise of published measurements of photometric brightnesses and filter colours of the objects or of spectral slopes of the reflected continuum light in the visible and near-infrared (IR) wavelength regions (Doressoundiram et al. 2008). The brightness of the objects is a first indicator on their size and albedo while filter colours allow a coarse characterization of the spectral energy distribution of reflected light from the objects and may provide constraints on the surface properties, i.e. the wavelength dependant reflectivity and in exceptional cases possibly also on surface chemistry. The visible and near-IR wavelength region up to 5µm show surface reflected sunlight, i.e. essentially a bluish, neutral or reddened solar spectrum, occasionally with imprinted absorptions from specific surface materials. Continuum colours and gradients are well defined, maybe with the exception of the H K (L M ) bands for objects with very strong ice absorption features (Trujillo et al. 2011). Photometric parameters of MBOSSes and their correlations with dynamical and other properties of the bodies were analysed in the past using various different datasets and statistical methods (for a review, see Doressoundiram et al. 2008, and references therein). Key findings are: the TNOs cover a wide range of colours and spectral slopes in the visible from slightly bluish (-5 to -10%/100 nm) to very red (40 to 55%/100 nm) while in the near-IR they display a fairly narrow dispersion around solar colours. Differences in the wavelength dependent surface reflectivity were noted for dynamically hot and cold Classical Disk Objects (CDOs), with the latter representing a very red population in the Solar System. An anti-correlation with high significance between the surface reddening and inclination and excentricity among the hot CDOs was interpreted as indicator for evolutionary changes due to impacts and cosmic radiation (Trujillo and Brown 2002; Peixinho et al. 2008). Centaurs may have a bimodal colour distribution with a neutral to slightly red and a very red sub-population (Tegler et al. 2008). A number of weaker correlations between photometric and dynamical properties of KBOs are addressed in literature. However, no clear convincing picture with quantitative modeling results has evolved, although various attempts of a qualitative understanding of the surface colours as results of evolutionary processes of the surface in the outer space environment have been published (for a brief review see Doressoundiram et al. 2008). In many cases the published colour and spectral gradient analyses rely on different datasets collected at different telescopes/instruments and by different groups. The sample sizes were growing with time reaching meanwhile more than 100 TNOs and Centaurs. A summarizing database of MBOSS colours comprising data from many different papers were first compiled and analyzed by Hainaut and Delsanti (2002, hereafter Paper I) and was publicly accessible through the internet; it is still available at http://www.eso.org/~ohainaut/MBOSS/ , but is superseded by this work. In this paper we provide a version of this MBOSS colour database that has been updated both in terms of populations and collected data. It can be used either for population-wide analysis, as done in this paper, or to support other works on specific objects or group of objects, either relying on the averaged data presented here (e.g. to get the colour of a given object), or by going back to the original publications which are listed for each objects. We present new statistical analyses of the MBOSS populations, based upon an enhanced database of photometric brightness and colour measurements of the object published in literature and applying qualified selection criteria to the data. The content of the database, both in terms of populations and collected data, is up-to-date for end of 2011. The qualifying criterion of the data are described in Section 2. Section 3 introduces the statistical methods and their application goals for the MBOSS analysis and outlines the results achieved. Possible interpretations of the findings related to their formation and evolutionary pathways are discussed in Section 4. The paper ends with a brief summary of the major findings and of open and/or controversial issues as well as prospects for their clarification in Section 5.
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O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

2. Description of the database
The database collects photometric information of MBOSSes, namely of objects in the Kuiper Belt (KBOs) and in the immediate Transneptunian region, of the Centaurs, of short-periodic (SPCs), long-periodic and Oort Cloud comets and of Jupiter Trojans. It does not contain information on satellites of the giant planets as far as they are considered to be captured MBOSSes, nor of Trojans of other planets. The objects are listed under their current official designation, i.e. number and name if available, or number and provisional designation, or provisional designation only. For objects presenting cometary activity, the measurements collected here refer to the nucleus, not to the dust and gas component. In the case of objects with satellites, measurements for the whole system are listed under the main designation (e.g. 26308 = 1998SM165), while an individual member of the system is indicated by a suffix (+B for the first satellite, for instance 134340-Pluto+B refers to Charon). In the statistical analysis, the satellites are not given a special status: they just count as individual objects. The photometric information in the database comprises magnitudes or filter colours in the U BV RI J H K L broadband filter system for the visible and the near-infrared. In rare cases also spectral gradients and/or colours measured from spectroscopic data of MBOSSes were entered, relying on the spectrum to colours conversion presented in the original paper. All flavours of the main filters are considered together without any conversion. For instance, in this database, Bessell R, Kron-Cousin R and r are directly listed as R. Most authors calibrate their system using Landolt (1992), thereby naturally unifying these subtly different systems. More exotic filters are included in the database, but not used in this study. The literature is searched for relevant papers, using the SAO/NASA ADS1 , the distant EKO newsletter2 , the Neese (2011) compilation of TNO and Centaurs at the Planetary Data System3 , the astroPh preprints from arXiv4 . Only magnitude measurements that are explicitly presented as simultaneous are considered as a single epoch. This means that the individual filters must have been observed in a sequence, so that no more than 1h elapsed during a colour measurement. The only exception was for average colours obtained from full light-curves. By default spectral gradients and colours obtained from spectroscopy fulfill the "simultaneity" criterion. Photometric measurements obtained non simultaneously are listed as separate data, and are not used for the average colour estimates. The method used to carefully combine measurements from different epochs without introducing colour artifacts from a possible lightcurve is the same as in Paper I. The original database, described in Paper I, contained information on only 104 objects. We did not have the means of evaluating the quality of the measurements, nor the luxury to reject some of them. The online-version continuously grew, listing up to 400 objects. The current version of the MBOSS database includes over 550 objects, with over 2000 measurements extracted from about 100 papers. We can now afford to reject some measurements, based upon a careful and quantifiable approach. The process of cleaning data is dangerous, as it could potentially select against special or interesting objects. We developed a method to evaluate the quality of a data-set that is robust against genuine outliers. As first noticed by Boehnhardt et al. (2001), and discussed later in this paper, most objects present a fairly linear reflectivity spectrum over the visible wavelength range; we used this characteristics to assess the quality of a set of measurements. For each individual measurement, the distance between the data point in a colour-colour diagram and the Reddening line (locus of the objects with a linear reflection spectrum, see Section 2.3) is computed as follows. Let (C x, C y) be the colours of the object, and (C x, F y), (F x, C y) the two points on the reddening line that have the same x and y as the data point, respectively. The distance estimator is defined as
n

d=
i=1

(Ci - Fi )2 , n

(1 )

where the Ci and Fi terms are the coordinates in the B - V /V - R and V - R/R - I colour-colour diagrams where available, and n the number of coordinates available (2 or 4). The overall quality estimator for a data-set is
N

D=
k =1

2 dk , N

(2 )

where dk are the individual distances, and N the number of measurement sets in the considered paper. D behaves like an error on the photometry, expressed in magnitude. Each of the papers
1 2 3 4

ht ht ht ht

t t t t

p: p: p: p:

//adswww.harvard.edu/ //www.boulder.swri.edu/ekonews/ //sbn.psi.edu/pds/resource/tnocencol.html //arxiv.org/archive/astro-ph 3


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

with D > 0.25 was scrutinized. The faintest objects were flagged out and D re-estimated. If D remained above 0.25, the process was iterated. In some cases, this brought D below 0.25, and the remaining measurements are retained, considering that those rejected were affected by low S/N. In other cases, the dispersion of the measurements is not correlated with magnitude, and the full data-set is flagged out; we consider that a problem affected the whole paper. This happened for instance to some papers from the early time of MBOSS photometry. Before flagging a data-set or a measurements out, the colours were compared with other measurements of the same object, if available, so to preserve objects with intrinsic unusual spectra. Also, it must be noted that the majority of the objects do have a linear spectrum, so even a few objects with non linear spectrum do not affect much the overall D estimator of a paper (thanks to the quadratic average), and these objects are then preserved in the database. This method obviously works only for measurements in the visible range. On the 102 papers considered, 33 did not have suitable data, and 7 were globally rejected. For each data-set (including IR-only papers), outliers were individually considered. Only the points that we have a strong reason to believe were affected by a problem were rejected (for instance if a note in the paper reports a problem). Also, some papers that concentrate on objects with exceptional spectra were obviously preserved. We believe that this statistical approach to the cleaning process with a careful and conservative a posteriori assessment ensures a better quality of the global data-set. The database as presented in this paper, is available online5 , together with all the plots related to this static version of the database, as a reference. In parallel, as the database is evolving with addition of new measurements, another up-to-date version6 is also available, also with all plots and tables. The former should be used only in direct reference to this paper, while the dynamically updated version can be used for further generic studies on MBOSSes. The updated version is produced exactly as the static one presented in this paper, with additional objects and measurements processed as described above.
2.1. Content of the database

Internally, each record lists the object designation as on the original publication (i.e. typically using the temporary designation for early papers, and the final number in later papers). These are converted to the current official designation, i.e. number and name if available, or number and provisional designation, or provisional designation only. The internal database lists the measurements for each epoch. One record is constituted by the name of the target, the epoch of the measurements, the reference to the original paper, and the list of measurements for that epoch as they appear in the paper, ie as magnitudes, colours, or a combination. The orbital elements are retrieved from the MPCORB file, regularly updated from the MInor Planets Center (MPC) website7 . These elements are used to compute the position of the object at the epoch of the observations (if available). The orbit semimajor axis a, perihelion q, eccentricity e, inclination i, orbital excitation defined as E = sin2 i + e2 , and the helio- and geocentric distances r and as well as the solar phase at the time of the observations are stored with the individual measurements. The measurements are averaged as in Paper I: For a given epoch, the matrix of all possible colours is populated from the magnitudes and colours available at that epoch ­ but not mixing different epochs. The average colours for an object are then obtained as a weighted average of the corresponding colours, using 1/ as the weight, where is either the reported or propagated error on the individual colour measurements. Additionally, for each epoch, we convert the R magnitude (either reported, or obtained from another magnitude together with the corresponding colour index) into an absolute M (1, 1, ) magnitude with the computed r and using M (1, 1, ) = R - 5 log(r). As in Paper I, we do not make any assumption on the solar phase function, and do not correct for solar phase effect. The M (1, 1, ) obtained for different epochs are then averaged into a final absolute R magnitude, which is reported as M (1, 1) in Table 2. The solar phase effects are not considered. Indeed, the observations are obtained at small solar phase angles because of the distance of the objects, and because most of the observations are acquired close to opposition. The colours of the objects, whose study is at the core of this paper, are even less affected than the absolute magnitude. We also do not make any assumption on the albedo of the object, and therefore do not convert the absolute magnitudes into diameters. For each object, the slope of the (very low resolution) reflectivity spectrum obtained from the average colour indices (Jewitt and Meech 1986) is computed as in Paper I, via a linear regression
5 6 7

http://www.eso.org/~ohainaut/MBOSS/MBOSS2 reference http://www.eso.org/~ohainaut/MBOSS http://www.minorplanetcenter.net/iau/Ephemerides/

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O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

over the B - V - R - I range (assigning a lower weight to the B reflectivity), where most objects display a linear reflectivity spectrum (Boehnhardt et al. 2001). This gradient, S, is expressed in percent of reddening per 100 nm.
2.2. Physico-dynamical classes

Since the publication of Paper I, the understanding of the dynamical classes in the outer Solar System has greatly progressed. Paper I used fairly arbitrary definitions of the dynamical classes; moreover, the fairly small number of objects in each class did not allow for a fine-grained classification. In this paper, we use the dynamical classes defined by Gladman et al. (2008) (now so-called the SSBN08 classification, from the book in which it is published). The membership of the object is allocated using a combination of integration of the orbit over time together with cut-off in the orbital element space. For this paper, we relied on the membership list published by Gladman et al. (2008), to which about 200 objects have been added from a list generated by C. Ejeta and H. Boehnhardt (private communication) in the context of the Herschel Key Program "TNOs are Cool" (Muller et al. 2009). ¨ This list was completed by the MPC catalogue of Jupiter Trojans8 . For the objects not included in these lists, we determine the dynamical class using a simplified method: objects with an obvious designation (Long Period Comets, Short Period Comets) are first flagged as such, then for the remaining few objects (26 objects in the current database), we used algorithm based only on the osculating orbital elements, without integration of the orbit, directly inspired by the flow-chart Fig. 1 in Gladman et al. (2008). Furthermore, we split the classical TNOs between dynamically hot classical disk objects (with i 5 ) and dynamically cold classical disk objects (i < 5 ). The arguments for this separation of CDOs come from the analysis of the orbital properties, although the first indications for the presence of different sub-populations among the classical TNOs came from a photometric study of TNOs by Tegler and Romanishin (2000) and were further evaluated in papers by Trujillo and Brown (2002) and Doressoundiram et al. (2002). The dynamical aspects are addressed in Morbidelli et al. (2008) and Gladman et al. (2008). We have chosen an inclination of 5 for the separation of the two populations. A split based around orbital excitation E = 0.12 gives similar results (only 3 objects over the 89 cold Classical TNOs change class). Also following Gladman et al. (2008), we distinguish TNOs as member of the scattered disk (SDOs) and of the detached disk (DDOs). The majority of 'Resonant' objects belongs to the class of Plutinos in 3:2 resonance with Neptune. Objects belonging to other resonances are summarized as 'Res.others' objects in the analysis below. Finally, some of the Short Period Comets with Centaur-like orbital elements, as defined in Gladman et al. (2008) are re-assigned to that class, following Jewitt (2009a) and Tegler et al. (2008): 29P/Schwassmann-Wachmann 1, 30P/Oterma, 165P/LINEAR, 166P/2001 T4, ´ 167P/2004 PY42 174P aka 60558 Echeclus, C/2001 M10 (NEAT), P/2004 A1 (LONEOS), and P/2005 T3 (Read).
2.3. The database

Table 1 lists the classes considered and the number of objects in each class. Table 2 provides examples of individual objects, listing the object identification and its dynamical class together with the main average colours, the spectral gradient S, and the absolute R magnitude M (1, 1). The full table is available in the online supplement.

8

http://www.minorplanetcenter.net/iau/lists/JupiterTrojans.html 5


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System Table 1. Object physico-dynamical classes (see text for the definitions) and number of objects in each class, and some statistics about the overall database. Class Jupiter Trojans Resonant (3:2) Resonant (others) Long-periodic Comets LPCs Short-periodic Comets SPCs Centaurs Scattered Disk Objects SDOs Detached Disk Objects DDOs Cold Classical Disk Objects (cold CDOs) Hot Classical Disk Objects (hot CDOs) Database Objects Epochs Papers Number 80 47 28 14 136 35 30 28 89 68 555 2045 100

6


Table 2. Object class and colour data for some example objects. The full table is available in the online supplement Object 1P/Halley 9P/Tempel 1 1172-Aneas 1994 ES2 1997 SZ10 1999 CF119 1999 CX131 2003 HX56 2060-Chiron 5145-Pholus 12917-1998 TG16 15760-1992 QB1 15809-1994 JS 19308-1996 TO66 20000-Varuna 20161-1996 TR66 24835-1995 SM55 35671-1998 SN165 42355-Typhon 42355-Typhon+B 50000-Quaoar 52747-1998 HM151 90377-Sedna 90482-Orcus 134340-Pluto 134340-Pluto+B 134340-Pluto+C 134340-Pluto+D 136108-Haumea 136199-Eris 136472-Makemake ... Class(1) SP Comet SP Comet J.Trojan Classic Cold Res.(other) Detached Res.(other) Classic Hot Centaur Centaur J.Trojan Classic Cold Res.(other) Classic Hot Classic Hot Res.(other) Classic Hot Classic Cold Scattered Scattered Classic Hot Classic Cold Detached Res. 3:2 Res. 3:2 Res. 3:2 Res. 3:2 Res. 3:2 Classic Hot Detached Classic Hot Epochs( 2 14 2 1 1 3 3 1 34 41 2 5 2 16 8 1 10 6 12 1 4 1 3 6 4 1 1 1 3 64 1
2)

M11 ± 13.558 ± 0.596 14.560 ± 0.460 8.729 ± 0.042 7.509 ± 0.130 8.148 ± 0.060 6.933 ± 0.133 6.910 ± 0.107 7.030 ± 0.209 6.092 ± 0.069 7.165 ± 0.076 11.388 ± 0.073 6.979 ± 0.094 7.479 ± 0.160 4.520 ± 0.042 3.455 ± 0.090 -- 4.332 ± 0.040 5.679 ± 0.320 7.252 ± 0.054 -- 2.220 ± 0.029 7.417 ± 0.100 1.077 ± 0.065 1.982 ± 0.099 -0.881 ± 0.400 -- -- -- 0.217 ± 0.030 -1.462 ± 0.036 --

Gr t ± 4.266 ± 2.015 9.959 ± 0.826 9.261 ± 0.863 -- 28.167 ± 2.909 14.704 ± 4.163 19.521 ± 4.293 -1.963 ±13.676 0.114 ± 0.996 48.354 ± 1.930 11.839 ± 1.962 27.538 ± 4.806 28.194 ± 6.000 2.077 ± 2.168 26.843 ± 1.917 -- 0.272 ± 1.805 6.857 ± 3.068 12.657 ± 1.354 9.763 ± 0.000 29.224 ± 1.706 24.891 ± 4.691 32.954 ± 2.972 2.761 ± 1.831 7.607 ± 0.681 3.334 ± 0.000 -2.234 ± 0.000 18.074 ± 0.000 -0.010 ± 0.850 3.866 ± 0.823 4.693 ± 0.900

B -V ± 0.720 ± 0.040 -- 0.727 ± 0.030 -- 1.140 ± 0.080 -- 0.918 ± 0.124 -- 0.700 ± 0.020 1.261 ± 0.121 0.724 ± 0.042 0.869 ± 0.143 -- 0.671 ± 0.057 0.906 ± 0.052 -- 0.652 ± 0.032 0.712 ± 0.095 0.758 ± 0.039 -- 0.958 ± 0.035 0.930 ± 0.090 1.131 ± 0.079 0.664 ± 0.041 0.867 ± 0.016 0.710 ± 0.002 0.644 ± 0.028 0.907 ± 0.031 0.631 ± 0.025 0.805 ± 0.015 0.828 ± 0.022

V-R ± 0.410 ± 0.030 0.468 ± 0.010 0.510 ± 0.022 -- 0.650 ± 0.030 0.622 ± 0.115 0.664 ± 0.128 0.350 ± 0.226 0.361 ± 0.017 0.788 ± 0.036 0.537 ± 0.042 0.707 ± 0.093 0.760 ± 0.170 0.389 ± 0.043 0.637 ± 0.040 -- 0.357 ± 0.043 0.444 ± 0.078 0.525 ± 0.022 -- 0.650 ± 0.020 0.620 ± 0.050 0.686 ± 0.077 0.370 ± 0.039 0.515 ± 0.035 -- -- -- 0.370 ± 0.020 0.389 ± 0.049 --

R -I ± 0.390 ± 0.060 0.469 ± 0.013 0.400 ± 0.030 -- -- 0.365 ± 0.106 0.434 ± 0.105 0.260 ± 0.459 0.325 ± 0.023 0.822 ± 0.054 0.410 ± 0.069 0.651 ± 0.166 0.480 ± 0.149 0.356 ± 0.053 0.628 ± 0.040 -- 0.356 ± 0.052 0.437 ± 0.083 0.414 ± 0.053 -- 0.610 ± 0.028 -- 0.657 ± 0.067 0.390 ± 0.045 0.400 ± 0.010 -- -- -- 0.320 ± 0.020 0.363 ± 0.061 --

1.

1. 2. 1. 0. 2. 1. 1. 1. 2. 2. 1.

1. 0.

V-J ± -- -- 577 ± 0.036 -- -- -- -- -- 199 ± 0.110 612 ± 0.048 707 ± 0.066 -- -- 997 ± 0.101 010 ± 0.050 -- 010 ± 0.050 270 ± 0.050 560 ± 0.045 -- 180 ± 0.058 -- 320 ± 0.060 070 ± 0.042 -- -- -- -- 051 ± 0.020 849 ± 0.108 --

J-H ± -- -- 0.430 ± 0.042 -- -- 0.380 ± 0.226 0.370 ± 0.238 -- 0.294 ± 0.079 0.391 ± 0.047 0.475 ± 0.086 -- 0.460 ± 0.705 -- 0.564 ± 0.070 0.470 ± 0.296 -0.270 ± 0.163 -- 0.406 ± 0.087 -- 0.360 ± 0.050 -- 0.290 ± 0.222 0.120 ± 0.051 -- -- -- -- -0.044 ± 0.037 0.080 ± 0.072 --

H- K ± -- -- 0.135 ± 0.036 -- -- -- -- -- 0.065 ± 0.094 -0.037 ± 0.047 0.205 ± 0.081 -- -- -- -0.038 ± 0.105 -- -- -- 0.160 ± 0.071 -- 0.030 ± 0.057 -- 0.050 ± 0.314 0.053 ± 0.055 -- -- -- -- -0.111 ± 0.048 -0.280 ± 0.085 --

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

(1) Classes refer to Gladman et al, SSBN07. M11 is the absolute R magnitude (2) Number of epochs. 7


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System Table 3. For some objects, list of the references used, and number of epochs. The full table is available in the online supplement Object 1994 ES2 7066-Nessus References Green et al. (1997) Davies et al. (1998) Romanishin and Tegler (1999) Bauer et al. (2003) Davies (2000) Tegler and Romanishin (1998) Jewitt and Luu (2001) Tegler and Romanishin (2000) Boehnhardt et al. (2001) Benecchi et al. (2011) Romanishin et al. (1997) Jewitt et al. (2007) Jewitt and Luu (1998) Romanishin and Tegler (1999) Hainaut et al. (2000) Gil-Hutton and Licandro (2001) Davies et al. (2000) Jewitt and Luu (2001) Boehnhardt et al. (2001) Sheppard (2010) Barucci et al. (1999) Davies (2000) Tegler and Romanishin (1998) Nr. 1

17

15760-1992 QB

1

5

19308-1996 TO

66

16

...

Table 3 shows examples for the list of references per object that were included in this study; the information for all objects is given in the online supplement. Figure 3 shows examples of the coarse reflectivity spectra for a set of objects obtained from their filter photometry. All of them are available on the MBOSS site. Figure 1 presents some of the representative colour-colour diagrams. As a reference, the solar colours are indicated by a red star (see Paper I, Table 2 for a list of the solar colours and their references). The red Reddening line, introduced in Paper I, marks the locus of objects with a perfectly linear reflectivity spectrum over the considered colours, with a tick mark every 10 units of S. For colour diagrams in the visible range, the distance from a data point to the reddening line therefore indicates a bent in the reflectivity spectrum. The symbols used indicate the dynamical class, and are explained in Fig. 2. The other colour-colour diagrams are available on the MBOSS site. Figure 7 displays the spectral gradient S as a function of the main orbital elements, the orbital excitation, and the M (1, 1) magnitude of the objects. Other similar plots, for all the colours, are available online. The symbols indicate the dynamical class. Figure 4 shows the histogram and the cumulative distribution for an example colour, for the spectral gradient, and for the absolute magnitude. Other similar plots are available on-line.

3. Results from the statistical analysis of the enhanced MBOSS database
3.1. Statistical tools

Comparing distribution by comparing their histograms "by eye" is unreliable: the size of the bins can cause artifacts or hide real features, and what appears as a strong difference can actually be of no significance. Similarly, the eye is a very powerful tool to detect alignments and clustering, even when these are not significant. The colour, spectral gradient and M (1, 1) distributions of the various MBOSS populations were therefore compared using a set of simple statistical tests that quantifies the significance of the apparent differences, i.e. the t-test, the f -test and the Kolmogorov-Smirnov test. The tests are described in detail in Appendix B of Paper I and references therein; in brief: ­ The Student t-test indicates whether the mean values of the two distributions are statistically different. The implementation used here deals properly with distributions with different variances. ­ The f -test considers whether two distributions have significantly different variances. ­ Finally, the Kolmogorov-Smirnov (KS) test uses the whole information contained in the distributions (and not just their means and variances) to estimate whether they are different.
8


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

Fig. 1. Selected colour-colour diagrams of the objects. The physico-dynamical class of the objects is identified by their symbols, which are explained in Fig. 2. The red star indicates the solar colours, and the red line is the locus of objects with a flat reflection spectrum. The other colour combinations are available on the MBOSS2 site.

For these tests to give meaningful results, the samples compared must be sufficiently large. We set the threshold at 15 units for t- and f-tests, and at 20 units for the KS test.
3.2. The case of the brightest objects

Large KBOs have non-typical surface properties (eg, high albedo ­Stansberry et al. (2008), or flatter spectral gradients) that are likely influenced by or the result of intrinsic processes overwriting the surface signatures from formation and/or from the evolution due to their environment. For instance, Pluto is known to have a tenuous, but captured atmosphere that can re-deposit on the surface (Stern and Tholen 1998; Protopapa et al. 2008) while (136199) Eris has an extremely high albedo (Sicardy et al. 2011). We therefore decided to remove the intrinsically brightest objects from the database for some studies, so that their potentially different characteristics does not pollute the colour distributions of the other, "normal" MBOSSes. In order to select a cut-off value, we estimated the radius of the objects whose escape velocity vesc is equal to the velocity of material ejection via cometary activity vej . The escape velocity is given by v
es c

=

2G M , R

(3 )

where G is the gravitational constant, M the mass of the object, and R its radius. Assuming a density 1000kg m-1 to get the mass from the volume of the object, v
es c

7 .5 1 0

-4

R,

(4 )

in IS units. To estimate the velocity of material ejection, vej (in m s-1 ), we use the relation ve j = 5 8 0 r
-0.5

µ0 , µ

(5 )

9


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

Fig. 2. Legend of the symbols used thorough this paper. Table 4. Averge colour and dispersion of all MBOSSes (excluding Trojans), comparing those with M (1, 1) < 5 with those with the others. Colour J-H H-K Aver./ M (1, 1) < 5 22 0.27± 0.25 16 0.04± 0.07 N Aver./ M (1, 1) 5 84 0.41± 0.20 31 0.07± 0.12 N t - Prob 0.025 0.279 f - Prob 0.149 0.036

Notes: The q cut-off is set at the median value; N is the number of measurements; t - Prob and f - Prob are the probabilities that the two sub-samples are randomly extracted from the same distibution, evaluated with the t- and f -tests. The other colours show insignificant differences.

where r is the heliocentric distance in AU, and µo /µ the ratio of the molecular mass of the species driving the activity to that of water. This relation was obtained by measuring the expansion of cometary comae, and is supported by a theoretical analysis --see Delsemme (1982) for a discussion. That velocity is the terminal velocity of the gas in the case of a small comet; it is directly controlled by the thermal velocity of the sublimating gas. For the TNOs, we use µo /µ = 0.64 for CO. Equaling vej and vesc , we obtain a critical radius Rc above which an object is likely to retain some of the material ejected by cometary activity, Rc 6 .2 1 0 5 . r (6 ) Rc with different species = 17 AU and 100 km at ts with the Spitzer Space use p = 0.2 to convert Rc (7 )

Rc is in m and r in AU. Delsanti et al. (2004) discuss the evolution of and distance. For our purpose, it is enough to say that Rc 150 km at r 43 AU. Stansberry et al. (2008), based on their large set of measuremen Telescope, indicate that large TNOs have higher than average albedo. We in an absolute magnitude, leading to M (1, 1) 1.9 + 2.5 log r,

again with r in AU. This give M (1, 1) 5 at r = 17 AU, and 6 at 43 AU. In what follow, we will then take M (1, 1) = 5 as a conservative limit, below which objects are likely to keep at least part of their atmosphere in the Centaur and TN regions, therefore to be potentially affected by different resurfacing processes. Clearly, that choice is partly arbitrary. We performed the following analysis with different cut-off values, leading to similar results. In order to verify whether we were justified to separate the bright M (1, 1) objects from the others, we compared their colours and gradient with those of the faint objects. The Trojans were not considered in this test, whose results are summarized in Table 4
10


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

1995DC2 2000CQ114

123509-2000WK183

15789-1993SC 2000FS53 1999OJ4+B

2000CN105 24978-1998HJ151 47171-1999TC36 1998WX31

44594-1999OX3 79983-1999DF9 1999RC215

50000-Quaoar 1998WY24

84522-2002TC302 55576-Amycus 1999CB119 66652-Borasisi 79360-1997CS29 33001-1997CU29 119979-2002WC19

2005CB79 2004PB108+B 2000CF105+B 2004PB108+B 2000CF105+B 45P/HMP 24835-1995SM55 107P/WH 2060-Chiron 33340-1998VG44 90568-2004GV9 144897-2004UX10 3548-Eurybates 26375-1999DE9 15883-1997CR29 138537-2000OK67 143P/KM 138537-2000OK67 9818-Eurymachos 55636-2002TX300 39285-2001BP75 55636-2002TX300 145453-2005RR43 136108-Haumea 53469-2000AX8

Fig. 3. Examples for reflectivity spectra for a set of objects. The reflectivity is normalized to unity for the V filter, and the spectra are shifted for clarity. The physico-dynamical class of the objects is identified by their symbols, which are explained in Fig. 2. The spectra for all the objects are available online on the MBOSS2 site.

With the exception of the J - H colour, the bright and the faint objects have compatible mean colours and overall distribution. In the infrared, the bright objects have marginally bluer colour ( J - H = 0.27 ± 0.25) than the faint ones (( J - H = 0.41 ± 0.20); this has only a probability of 2.5% to occur by chance, i.e. this difference is marginally significant. Similarly, the bright objects have a slightly broader distribution of H - K colour than the fainter ones (at the 3% level). When performing these tests on individual or group of classes, the result remains with a slightly stronger significance for the resonant objects, but cannot be tested on the other groups, which don't have enough bright objects. Nevertheless, removing the non-resonant objects increased the significance of the result for the resonant objects. Additionally, one must consider the possibility that the larger dispersion in H - K for the fainter object is connected to the poorer signal-to-noise ratio in K , as the sky is much brighter in this band and the instruments tend to be less sensitive there. Considering the colours of the various dynamical classes in the visible wavelength range for the bright ( M (1, 1) < 5) and faint objects, the colour distributions of the bright objects are undistinguishable from those of the fainter ones, indicating that the object populations might be rather uniform despite that some larger objects may differ in some surface properties (for instance albedo) and that intrinsic activity may play a role for resurfacing the bodies. It is, however, noted that the near-IR colours of individual KBOs can differ from mean values if the surfaces are covered to a significant amount with ices that display strong absorptions (like C H4 ), namely in H and K bands like Pluto, Eris and 2005 F Y9 (see Brown 2008). The presence of such ice absorptions can be inferred from an unusual negative slope for near-IR spectral gradients (i.e. from J to H and K bands). In summary, the infrared colours of the objects with bright absolute magnitudes are slightly different than those of the fainter objects. We will therefore keep them separate for most colour tests, but we will also re-incorporate them for some tests on the visible colours where more objects are helpful. Based on these results, one might consider to re-include the intrinsically brighter objects for the remainder of the study. However, we decided not to: If they are indeed similar, they would only marginally increase the size of the sample, not changing the conclusions. If they eventually turn out
11


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

Fig. 4. R - I (top) and spectral gradient (bottom) cumulative distributions (left) and histogram (right). Solar value is indicated by a dotted line. Similar plots are available on-line for the other colours.

to be different, as possibly suggested by the near-IR colours, we did the right thing keeping them separate.
3.3. Global characteristics of individual classes

The MBOSS2 database that we analyze contains photometric measurements of 10 different dynamical classes (see Fig. 2), i.e. the short-periodic comets (SPC), the long-periodic comets (LPC), the Jupiter Trojans, Kuiper Belt objects in 3:2 (Plutinos = Res. 3:2) and in other orbital resonances (Res.others) with Neptune, the Classical Disk objects (CDOs) in two flavors as dynamically 'hot' and 'cold' CDOs, the Scattered Disk objects (SDOs) and the Detached Disk objects (DDOs). Selected colour-colour diagrams of MBOSSes are shown in Fig. 1. Colour distributions of the various classes of objects are displayed in Fig. 4, for a selection of colours and for the spectral gradient S. At first sight, the ranges of visible colours are similar for the several dynamical groups (Plutinos and Resonants, CDOs, SDOs, Centaurs), ranging from slightly bluish (-10%/100 nm) compared to the Sun to very red (55%/100 nm). Jupiter Trojans do not appear to contain any very red objects (i.e. with spectral gradient > 20%/100 nm) as the other groups do. For LPCs the number of measured objects (14) may be too small to provide representative results for the total population, although it is noted that the available data indicate spectral gradients between about 0 and 10 %/100nm, well in agreement with the other groups. The mean colours (and corresponding variances) for the various dynamical classes are listed in Table 7, top panel, using all data in the MBOSS2 database, and the values for the restricted dataset of objects with M (1, 1) 5 mag are in Table 7, bottom panel. Many of these means are based on only a small number of objects, and their general representative should be taken with care. The average characteristics of the dynamical classes are also displayed as reflectivity spectra in Fig. 5. The red slope in the visible wavelength range, although different for individual groups, levels off in the near-IR with transition between I and J or H bands.
12


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

Cold_CDO Res._(others) Resonant_(3:2) Centaurs Scattered Hot_CDO Detached SPComets Jupiter_Trojans LPComets

a

Cold_CDO Resonant_(3:2) Detached_DO Scattered_DO Centaurs Hot_CDO SPComets LPComets Jupiter_Trojans

b

Cold_CDO Res._(others) Resonant_(3:2) Centaurs Scattered Detached Hot_CDO SPComets LPComets Jupiter_Trojans

c Fig. 5. Average reflectivity spectra for the different physico-dynamical classes. a: small objects ( M (1, 1) > 5 mag), b: large objects only ( M (1, 1) < 5 mag), c: all the objects 13


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System Table 5. Statistical comparisons of the spectral gradient distributions of pairs of MBOSS populations: t-test, f-test, KS test Resonant (Others) N Resonant 3:2 Resonant others Classical Cold Classic Hot Scattered Disk Objects Detached Disk Objects Centaurs 15 0.701 0.367 0.810 Indist. . Classical Cold 43 0.002 0.209 0.000 Not comp. 0.019 0.986 0.019 Marginal . Classical Hot 28 0.713 0.505 0.817 Indist. 0.485 0.166 0.680 Indist. 0.002 0.051 0.006 . Scattered Disk Objects 23 0.340 0.777 0.612 Indist. 0.211 0.523 0.183 Indist. 0.000 0.402 0.000 Not comp. 0.602 0.377 0.161 Indist. . Detached Disk Objects 17 0.056 0.264 0.023 Marginal 0.034 0.881 0.009 Marginal 0.000 0.839 0.000 Not comp. 0.160 0.106 0.002 Marginal 0.355 0.406 0.280 Indist. . Centaurs Short Period Comets 44 0.006 0.334 0.072 Marginal 0.005 0.810 0.020 Marginal 0.000 0.747 0.000 Not comp. 0.039 0.094 0.040 Marginal 0.114 0.569 0.359 Indist. 0.583 0.662 0.444 Indist. 0.015 0.014 0.035 Marginal Long Period Comets 0 Trojans

31

t f KS t f KS t f KS t f KS t f KS t f KS t f KS t f KS

15

43

28

23

17

26 0.768 0.163 0.438 Indist. 0.968 0.057 0.101 Indist. 0.038 0.006 0.000 Not comp. 0.560 0.471 0.284 Indist. 0.286 0.125 0.358 Indist. 0.064 0.031 0.182 Indist. .

-/-

-/-

-/-

-/-

-/-

-/-

26

-/-

Short Period Comets

44

. -/f -tests and the KS test. The number N indicate how many probability that the two distributions are randomly extracted whether the populations are significantly different, marginally text for details).

60 0.000 0.000 0.000 Not comp. 0.000 0.000 0.000 Not comp. 0.000 0.000 0.000 Not comp. 0.000 0.000 0.000 Not comp. 0.001 0.000 0.000 Not comp. 0.020 0.000 0.000 Not comp. 0.000 0.000 0.000 Not comp. 0.090 0.000 0.000 Not comp.

Notes: The three tests are the Student t- and objects have measurements. The result is the from the same population. The label indicates different, or statistically undistinguishable (see

3.4. Comparisons between classes

In the comparison of the photometric properties between the dynamical classes all groups are considered except long-periodic comets LPCs, since the number statistics of LPCs seems to be too sparse to expect firm conclusions.
3.4.1. Colours and spectral gradients

Comparing the colour distribution of the different physico-dynamical classes, it appears (see Fig. 4) that: ­ The distributions of the colours and of the spectral gradients in the visible wavelength range differ among the groups, in extend, shape and peak location. Taking the spectral gradients as an example, the peak level increases starting with the Jupiter Trojans (5-10%/100 nm), over the SPCs, Centaurs, DDOs, SDOs, Plutinos (and possibly the resonant objects) (10-20%/100 nm), to the hot CDOs (20-30%/100 nm) and finally to the cold CDOs as the reddest objects (2535%/100 nm) among the MBOSSes. Colour ranges and distribution width are well noticeable in the cumulative distribution functions (see left panels of Fig. 4). ­ Relevant secondary peaks in the frequency distributions may exist for Centaurs and Plutinos at higher reddening. At least for Centaurs, statistical arguments for a bimodal surface colour distribution were presented in numerous papers (Tegler and Romanishin 1998, 2003; Peixinho et al. 2003; Delsanti et al. 2006; Tegler et al. 2008, eg). Tegler et al. (2008) presented a detailed analysis of the Centaurs' bimodality, based on a sample of 26 objects, ie almost as large as the
14


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System Table 6. Statistical comparisons of the J - H colour distributions of pairs of MBOSS populations: t-test, f-test, KS test Classic cold 28 0.498 0.000 0.449 Not comp. Classic hot 34 0.119 0.961 0.677 Indist. 0.121 0.000 0.710 Not comp. Centaurs 17 0.308 0.000 0.984 Not comp. 0.332 0.703 0.284 Indist. 0.271 0.000 0.499 Not comp.

Resonant 3:2 Classic cold Classic hot

N 21

t f KS t f KS t f KS

28

34

-

Notes: The three tests are the Student t- and f -tests and the KS test. The N number indicate how many objects have measurements. The classes that are not listed do not have sufficiently measurements for these tests to be performed. The result is the probability that the two distributions are randomly extracted from the same population. The label indicates whether the populations are significantly different, marginally different, or statistically undistinguishable (see text for details).

one presented here (29 objects, so we do not present a new analysis). They conclude that the B - R distribution is bimodal with a confidence level of 99.5%, with 10 red centaurs and 16 gray ones. The red ones have marginally smaller orbital inclinations, and higher albedo at the 99% confidence level. ­ The frequency distribution in J - H instead gives a rather uniform picture for all dynamical groups with respect to colour range and peak position (with a few singular exceptions for Plutinos and CDOs). This global characterization indicates that parameters of the visible spectral energy distribution are better diagnostics for the global surface reflectivity and differences among MBOSSes compared to the near-IR colours. However, it is noted that near-IR spectral information of MBOSSes is more sensitive to specific and pronounced compositional differences than visible one, because stronger absorption bands, in particular of icy compounds, are found in the near-IR wavelength domain (Barucci et al. 2008).

15


16

Table 7. Mean colours, and variances, for the MBOSS populations: all objects colour Full database U-B B-V V -R V-I V-J R-I J-H H-K Gr t M (1, 1) Res. 3:2 Res.others 2 0.273±0.090 16 0.975±0.142 21 0.603±0.109 23 1.181±0.164 5 2.138±0.327 19 0.554±0.090 13 0.437±0.065 4 0.052±0.023 25 23.471±9.362 21 6.235±1.393 Classic cold 3 0.593±0.123 41 0.996±0.140 49 0.630±0.086 73 1.220±0.159 5 1.960±0.421 36 0.588±0.095 28 0.398±0.082 4 0.079±0.030 82 25.515±9.217 46 6.600±0.614 Classic hot 11 0.258±0.168 38 0.864±0.163 41 0.510±0.145 51 1.010±0.249 13 1.509±0.431 35 0.506±0.139 34 0.316±0.290 8 0.077±0.117 56 15.387±11.887 45 5.928±1.703 Scattered 7 0.334±0.144 27 0.858±0.153 25 0.536±0.096 28 1.037±0.189 9 1.753±0.481 22 0.544±0.108 13 0.400±0.124 8 0.060±0.151 29 15.258±9.974 24 7.168±1.225 Detached 2 0.180±0.156 22 0.869±0.109 23 0.519±0.083 24 1.039±0.170 4 1.614±0.601 21 0.515±0.099 10 0.381±0.126 4 0.035±0.228 26 15.459±8.873 23 5.718±2.181 J.Trojans 0 ---- 74 0.091 80 0.048 80 0.090 12 0.120 80 0.057 12 0.064 12 0.041 80 3.786 60 1.057 Centaurs 0 ---- 28 0.892±0.195 30 0.567±0.131 26 1.077±0.252 10 1.769±0.498 26 0.525±0.151 17 0.375±0.075 15 0.085±0.143 30 19.320±13.842 29 9.456±1.654 SP Comets 0 ---- 17 0.209 43 0.105 22 0.112 1 0.000 23 0.101 1 0.000 1 0.000 43 8.307 134 1.667 LP Comets 0 ---- 1 0.000 2 0.045 1 0.000 0 ---- 1 0.000 0 ---- 0 ---- 2 3.692 13 3.601

0 ---- 38 0.868±0.170 38 0.558±0.101 40 1.101±0.202 16 1.838±0.493 36 0.536±0.122 21 0.442±0.285 11 0.043±0.059 45 18.633±10.659 38 6.680±1.981

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

0.777± 0.445± 0.861± 1.551± 0.416± 0.434± 0.139± 7.024± 11.356±

0.863± 0.494± 0.947± 1.630± 0.447± 0.360± 0.140± 11.483± 16.131±

0.810± 0.422± 0.878±

0.430±

5.188± 13.550±


Table 7. Mean colours, and variances, for the MBOSS populations, continued: Objects with M (1, 1) > 5mag colour Res. 3:2 Res.others Classic cold Classic hot Scattered Detached Objects with M (1, 1) 5 mag U-B 0 1 2 3 7 2 ---- 0.210±0.000 0.525±0.049 0.187±0.103 0.334±0.144 0.180±0.156 B-V 26 10 34 22 23 15 0.858±0.175 0.943±0.131 1.011±0.139 0.919±0.167 0.876±0.143 0.836±0.084 V -R 31 15 42 29 23 16 0.555±0.102 0.590±0.102 0.642±0.082 0.523±0.152 0.532±0.098 0.513±0.077 V-I 31 13 37 25 22 15 1.098±0.205 1.114±0.162 1.226±0.145 1.050±0.258 1.068±0.186 1.010±0.159 V-J 9 1 4 2 6 1 1.912±0.528 2.295±0.000 1.932±0.480 1.807±0.024 1.796±0.369 1.646±0.000 R-I 30 13 33 25 20 14 0.538±0.127 0.521±0.084 0.578±0.090 0.529±0.137 0.549±0.113 0.510±0.104 J-H 14 5 17 17 9 5 0.518±0.319 0.467±0.064 0.401±0.071 0.342±0.296 0.417±0.133 0.414±0.026 H-K 6 1 3 0 5 1 0.056±0.076 0.080±0.000 0.070±0.030 ---- -0.004±0.114 0.260±0.000 Gr t 31 15 43 28 23 17 19.051±10.558 20.240±8.496 26.488±8.567 17.795±12.258 16.526±10.121 13.971±8.172 M (1, 1) 32 15 45 34 23 17 7.392±0.802 6.974±0.795 6.635±0.571 6.717±0.833 7.275±1.124 6.746±0.572 Notes: The number of objects included in each average is indicated. Grt is the spectral gradient S. M (1, 1) is the R absol J.Trojans 0 ---- 60 0.789±0.092 60 0.461±0.040 60 0.898±0.062 12 1.551±0.120 60 0.437±0.044 12 0.434±0.064 12 0.139±0.041 60 8.538±2.759 60 11.356±1.057 ute magnitude. Centaurs 0 ---- 28 0.892±0.195 30 0.567±0.131 26 1.077±0.252 10 1.769±0.498 26 0.525±0.151 17 0.375±0.075 15 0.085±0.143 30 19.320±13.842 29 9.456±1.654 SP Comets 0 ---- 16 0.872±0.213 43 0.494±0.105 22 0.947±0.112 1 1.630±0.000 23 0.447±0.101 1 0.360±0.000 1 0.140±0.000 43 11.483±8.307 134 16.131±1.667 LP Comets 0 ---- 1 0.000 2 0.045 1 0.000 0 ---- 1 0.000 0 ---- 0 ---- 2 3.692 13 3.601

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

0.810± 0.422± 0.878±

0.430±

5.188± 13.550±

17


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

We now want to compare populations using the statistical tests described in section 3.1. First of all, it must be stressed that a common feature among the statistical tests applied is to output a probability that the two populations compared are not randomly extracted from the same population. In other words, the statistical tests can very firmly establish that two populations are significantly different. A contrario, no statistical test can prove that two populations are identical. For instance, the colour distributions of the Centaurs and Jupiter Trojans (see Tab. 5) are radically different with a very high significance level: It is totally improbable that these two populations were randomly extracted from the same reservoir. However, the spectral gradient distributions of SDOs and DDOs indicate these objects could have been randomly extracted from a same pool -- but it is absolutely possible that this is a coincidence. Table 5 summarizes the results of the comparison between the spectral gradient S distribution of the MBOSS populations using these tests. Following the discussion in Section 3.2, the tests were restricted to the objects with M (1, 1) > 5 mag. For each pair, the table lists the probabilities that the two classes were randomly extracted from a common population, based on the mean spectral gradient (t-test), the spectral gradient variance ( f -test), and the overall spectral gradient distribution (KS test). Low probabilities indicate that the two considered distributions are not compatible. The pairs for which at least one of the tests returns a probability < 0.001 were flagged as not compatible, indicating they are significantly different. Those where a test indicates a probability < 0.05 are marked as marginally different, suggesting that there is a difference, but that it is not very strongly significant. The others are statistically undistinguishable using these tests. Again, it does not mean that the objects are similar, just that these tests cannot prove they are different. Similar tests were performed on the individual colours, with similar results. We discuss here only the spectral gradients, as it encompasses most of the information present in the visible spectrum r an g e. In the infrared, the tests are possible only in J - H , and only some of the classes have enough measurements for the tests to be meaningful. The results are presented in Table 6. The statistical tests indicate: ­ The spectral gradient distributions of the various resonant classes are statistically indistinguishable. In order to increase the size of the sample, all the resonant objects are split only between Plutinos (3:2) and Other Resonant Objects. ­ The spectral gradient distributions of Plutinos and other Resonant Objects, SDOs, hot CDOs, and Centaurs are indistinguishable, ­ Additionally, the Plutinos and the hot CDOs had indistinguishable J - H distributions. ­ The spectral gradient distribution of DDOs is indistinguishable from that of SDOs and only marginally distinguishable from that of Plutinos and resonant objects, as well as hot CDOs. ­ The spectral gradient distribution of cold CDOs is not compatible with the ones of hot CDOs, Plutinos, SDOs, DDOs and Centaurs, and it is only marginally compatible with that of the resonant objects. ­ Additionally, the cold CDOs J - H distribution is not compatible with that of the Plutinos and the hot CDOs. ­ The spectral gradient distribution of Jupiter Trojans clearly indicates complete incompatibility with all other MBOSS populations. ­ The spectral gradient distribution of SPCs is significantly different from that of the Jupiter Trojans and cold CDOs. It is only marginally different from that of the hot CDOs, Plutinos and other resonant objects as well as Centaurs, and it cannot be distinguished from that of SDOs, DDOs. ­ The J - H colours of the Centaurs is not compatible with those of the Plutinos and of the hot CDOs. In conclusion: Plutinos, other Resonant Objects, hot CDOs, SDOs and DDOs may be rather similar for their spectral gradients in the visible, while cold CDOs and Jupiter Trojans form two separate groups for their spectral properties in the visible wavelength range. The peak in the spectral gradient distribution of hot CDOs seems to be shifted slightly to higher reddening, for the moment a suggestion not yet at statistical significance level. SPCs may agree with the first populations mentioned above.
3.4.2. Absolute magnitude

The absolute magnitude M (1, 1) of an object depends on the reflectivity function across the surface, i.e. in a first order approximation on the object size, the geometric albedo and the photometric phase function. Given the relationship between M (1, 1), size, albedo and phase function one can assume that the M (1, 1) distribution is dominated by the effects of the size, except for the largest bodies which often have high albedoes (Stansberry et al. 2008). The solar phase angle for KBOs is always
18


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

Fig. 6. R absolute magnitude M (1, 1) cumulative distributions (logarithmic, left) and histogram (right).

relatively small, and the phase function is moderately steep, so the effect on M (1, 1) hardly exceeds 0.2-0.3mag. Hence, we assume that the M (1, 1) distribution of KBOs reflects ­at least to zeroth order­ the size distribution of the objects, with the understatement that a detailed analysis requires more accurate size estimates of the objects. Such a careful study can be found in Stansberry et al. (2 0 0 8 ). The M (1, 1) distributions are strongly biased by cumulative selection effects: while there are few bright and large objects in a given class, they are more easy to discover, and also more easy to observe, so they are likely to be represented in this data set. A contrario, the discovery surveys are not complete for fainter objects, and faint objects are less likely to be picked by observers performing colour measurements. Consequently, the M (1, 1) distributions are likely to be fairly complete at the bright end, but to have complex non-completeness at the faint end. Meech et al. (2004) discussed and simulated many of these selection effects.
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O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

Fig. 6 shows the frequency histogram and cumulative distribution function of M (1, 1) for the various MBOSS groups, now covering all objects in the MBOSS database (i.e. not excluding those with M (1, 1) > 5 mag). The selection bias against small KBOs is clear, with no object fainter than M (1, 1) 8.5 in the distant classes ­ this corresponds to actual magnitudes fainter than 23.5 for Plutinos, and even fainter for CDOs, i.e. about the limiting magnitude for colour observations performed with fairly short exposures on a 8 meter class telescope. On the other hand, Centaurs and SPCs may be seen as a sample of smaller KBOs that is scattered towards the inner planetary system. Meech et al. (2004) found that the shape of the short period comet size distribution is incompatible with that of the other TNOs. The slope k of the logarithmic cumulative M (1, 1) distribution relates to the power law q of the cumulative radius distribution Nc (a) a-q as q = 5k. Measuring the k slopes on the straight parts of the distributions in Fig. 6 leads to values q 0.8 for the SPCs, the Centaurs, the SDOs, the DDOs, the hot CDOs and the Resonant objects; the steep slope of the cold CDOs and the DDOs corresponds to q 2. Only the steepest part of the SP Comets distribution reaches q 3. The analysis based on controled samples designed for size analysis lead to much steeper q = 3.0 (Trujillo et al. 2001) to 3.5 (Kenyon and Bromley 2004), i.e. much richer in small/faint objects. This confirms that the sample used for colour measurements is heavily biased against faint objects ­only the brightest SPCs might be fairly complete. Therefore, the size distributions in Fig. 6 should only be used for internal comparison, with the hope that the selection effects were affecting them in a similar way, and/or restricting the analysis to the bright end of the distributions. Clearly, the observed Jupiter Trojans ( M (1, 1) between 8 and 13 mag) are smaller than KBOs (that cover the M (1, 1) range from about 0 to 9 mag). The bulk of that shift corresponds to the fact that the geometry gives an advantage of 4 mag for the Trojans. It is noteworthy that cold CDOs display a rather peaked M (1, 1) distribution and do not contain objects with M (1, 1) brighter than about 5 mag, while Plutinos, hot CDOs and DDOs contain objects of 2 to -1mag. The rather steep slope in the cumulative distribution function of M (1, 1) of the cold CDOSs reflects the likely difference in the size range of these KBOs. In particular, it is different from that of hot CDOs which should be exposed to very similar selection effects, i.e. it is real. The brightest resonant objects reach M (1, 1) of about 3mag, while the SDOs are more of the brightness of cold CDOs, however with a much less pronounced peak level on a bit wider distribution plateau. From the M (1, 1) distributions of MBOSSes we conclude that the absence of larger bodies among the cold CDOs and their presence among other populations of the Kuiper Belt may suggest different formation environments for both groups of objects that may have favored the growth of larger bodies for Plutinos, SDOs, DDOs and possibly hot CDOs compared to cold CDOs. Jupiter Trojans are a population of smaller size bodies, again arguing for a formation environment and evolution scenario that were distinct from that of the other MBOSSes (now including cold CDOs). Since it is very likely that the large bodies in these groups may have survived impact events widely unaffected for their sizes over the lifetime of the Solar System, one can assume that they represent the original population of planetesimals. The Centaurs reach the magnitude/size range where the vast majority of larger KBOs are detected, but they do not include one of the rare big ones. This might well be compatible with the scattering scenario for Centaurs but needs quantitive confirmation by dynamical calculations. Altogether, the M (1, 1) distributions give the impression that the MBOSSes may have been formed in at least 3 (maybe 4) different environments, i.e. one for the Jupiter Trojans, one for the cold CDOs, maybe one for the hot CDOs and one for the rest of the bodies. Since KBOs are now and were for very long time residing in the same distance range, one may consider Plutinos, resonant objects, hot CDOs, and SDOs as immigrant population of the Kuiper Belt compared to the cold CDOs that may represent "aborigines KBOs". Interestingly, also the DDOs appear to be `sizewise' in accord with the Kuiper Belt "immigrants", although they are found in a much more distant location.
3.5. Dependencies with dynamical parameters

The colour distribution (say, the B - V distribution) of a class of objects (say, the Centaurs) is considered as a function of another parameter of the objects (say, the perihelion distance q) to search for correlations as possible indicators for physical dependencies. The traditional Pearson correlation factor is not robust for non-linear dependencies, so a simpler and more robust estimator was used: The sample is divided in two sub-samples, using the median value of the independent variable (in the example, the median q of the Centaurs, i.e. 16.22 AU). The colour distribution
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O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System

a [AU]

q [AU]

i

e

M(1,1)

E

Fig. 7. The spectral gradient S of the objects [%/100 nm] as a function of the main orbital elements, and of the orbital excitation E and the absolute R magnitude M (1, 1). Similar plots are available on-line for the various colours. Table 8. Averge colour and dispersion for the cold CDOs, comparing those with smaller a (or q) with those with large values. Colour B B B V V B B B V V - - - - - - - - - - V R I R I V R I R I N 16 16 9 21 17 17 16 13 19 18 Aver./ a < 43.95 0.99±0.16 1.59±0.26 2.18±0.37 0.63±0.10 1.20±0.16 q < 40.91 0.95±0.17 1.56±0.25 2.15±0.30 0.61±0.08 1.20±0.18 N 18 17 14 21 20 17 17 10 23 19 Aver./ a 43.95 1.03±0.11 1.69±0.09 2.27±0.15 0.65±0.06 1.24±0.14 q 40.91 1.07±0.06 1.72±0.07 2.34±0.13 0.67±0.08 1.25±0.10 t - Prob 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 148 151 489 310 395 013 024 060 033 278 f - Prob 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 148 000 003 034 538 000 000 017 802 010

Notes: The a and q cut-off are set at the median value; N is the number of measurements; t - Prob and f - Prob are the probabilities that the two sub-samples are randomly extracted from the same distibution, evaluated with the t- and f -tests. The other colours show insignificant differences.

of the two sub-samples are then compared through t-test and f -test and the Pearson correlation parameter is also estimated. Visually, this can be done by comparing the left-hand side with the right-hand side of all the sub-panels of Figure 7.
For cold CDOs: The variances of colours B - V , B - R and B - I are different for the inner (smaller variance) and the outer (larger variance) population among the cold CDOs (considering both their semi-major axis and perihelion distance). These differences have a good level of significance, as listed in Tab. 8. The effect is only marginally observed in V - R and V - I . The average colours of the sub-samples are undistinguishable: only the breaths of the distributions are different Since similar results are not found in other colours nor for the spectral gradients in the visible, it might be related with a wavelength dependent phenomenon that is mostly restricted to the B filter, like for instance a stronger unknown continuum absorber in the outer cold CDOs. For hot CDOs: Hot CDOs with a perihelion closer to the Sun are significantly bluer than the ones

that do not get close, ee Tab. 9 . This result is visible in the B - V , B - R and B - I colours (eg
21


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System Table 9. Averge colour and dispersion for the hot CDO, comparing those with smaller q with those with large values. Colour B B B V V - - - - - V R I R I N 10 10 8 14 12 Aver./ q < 39.39 0.80±0.12 1.28±0.21 1.71±0.28 0.47±0.14 0.94±0.24 N 12 12 9 15 13 Aver./ q 39.39 1.02±0.13 1.64±0.18 2.37±0.27 0.57±0.15 1.15±0.24 t - Prob 0. 0. 0. 0. 0. 000 000 001 071 037 f - Prob 0. 0. 0. 0. 0. 795 666 838 792 967

Notes: The q cut-off is set at the median value; N is the number of measurements; t - Prob and f - Prob are the probabilities that the two sub-samples are randomly extracted from the same distibution, evaluated with the t- and f -tests. The other colours show insignificant differences. Table 10. Averge colour and dispersion for the hot CDOs, comparing those with smaller i with those with large values. Colour B B B V V G -V -R -I -R -I rad. N 14 14 11 15 13 15 Aver./ i < 17.0 0.99±0.16 1.60±0.21 2.14±0.33 0.61±0.08 1.20±0.15 24.59±7.99 N 8 8 6 14 12 13 Aver./ i 17.0 0.80±0.09 1.26±0.20 1.70±0.31 0.43±0.16 0.89±0.26 9.95±11.80 t - Prob 0. 0. 0. 0. 0. 0. 002 002 020 001 002 001 f - Prob 0. 0. 0. 0. 0. 0. 096 940 978 012 064 165

Notes: The q cut-off is set at the median value; N is the number of measurements; t - Prob and f - Prob are the probabilities that the two sub-samples are randomly extracted from the same distibution, evaluated with the t- and f -tests. The other colours show insignificant differences.

B - V = 0.80 ± 0.12 for q < 39.4 AU, and B - V = 1.02 ± 0.13 mag for the others). This result is based on fairly small samples, which decreases the strength of its significance. Hot CDOs with high inclinations or with large orbital excitation parameter are bluer than the others, see Tab. 10, a finding seen for several colours ( B - V , B - R, V - R, V - I ) as well as for the spectral gradient in the visible. The sample sizes are small, but sufficient. This result was already known (Trujillo and Brown 2002; Doressoundiram et al. 2008) and is generally expressed as anticorrelation between reddening of the objects and their orbital energy E. The usual interpretation scenario is colour changes due to resurfacing by impact ejecta if during a collision between a hot CDO and another KBO subsurface material with different colour properties is ejected and deposited on the surface by impact excavations. Since cold CDOs do not display such an anti-correlation despite the fact that they occupy the same distance range as the hot CDOs do, it may be more an effect due to orbital energy, i.e. collision energy rather than collision frequency.
For others: Other combinations of dynamical parameters and colours, spectral gradient and

M (1, 1) data of different dynamical classes do not show any statistically significant signal indicating possible correlations and physical dependencies.
3.6. Absolute magnitude
3.6.1. Absolute magnitude vs orbital parametres

For the comparison between M (1, 1) and dynamical parameters we consider the small objects ( M (1, 1) 5 mag) only and we find: For Centaurs, SDOs and DDOs, when considered together, objects with small semi-major axis a and perihelion distance q display a significantly fainter absolute magnitude M (1, 1) than the distant ones. While this is a statistically strong result, it disappears when the three classes are considered separately. Thus, it can simply be seen as the selection bias which makes the more distant and thus fainter objects harder to measure than the closer ones.
3.6.2. Absolute magnitude of the blue objects, vs red objects:

Next, we compare the absolute magnitude M (1, 1) distribution of a class of objects in function of their colour, in order to explore whether the redder objects have the same M (1, 1) distribution as the bluer objects. Considering only the small objects ( M (1, 1) 5 mag), the blue hot CDOs and the
22


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System Table 11. Averge M (1, 1) and dispersions for the hot CDOs, comparing those with blue vs red colours. Colour Colour cut-off hot TNOs B-V 0.92 B-R 1.55 B-I 1.92 V -R 0.56 V-I 1.10 R-I 0.54 Resonant Objects B-V 0.88 B-R 1.40 B-I 1.89 V -R 0.56 V-I 1.06 R-I 0.51 N Aver./ Blue 6. 7. 7. 6. 6. 6. 7. 7. 7. 7. 7. 7. 92± 09± 13± 88± 87± 85± 0. 0. 0. 0. 0. 0. 67 45 52 61 61 53 81 81 84 72 72 78 N Aver./ Red 6. 6. 6. 6. 6. 6. 6. 6. 6. 7. 7. 7. 54± 37± 41± 34± 29± 30± 0. 0. 0. 0. 0. 0. 62 64 67 62 65 72 78 78 81 88 91 83 t - Prob 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 183 007 025 026 031 039 004 004 052 073 170 065

11 11 8 14 12 12 18 18 15 23 22 21

11 11 9 15 13 13 18 18 16 23 22 22

61± 61± 40± 48± 42± 47±

0. 0. 0. 0. 0. 0.

79± 79± 79± 04± 08± 01±

0. 0. 0. 0. 0. 0.

Notes: The objects with M (1, 1) < 5 were excluded from this test; the colour cut-off is set at the median value for the considered colour; N is the number of measurements; t - Prob are the probabilities that the two sub-samples are randomly extracted from the same distibution, evaluated with the t-test. The other colours show insignificant differences.

blue Resonant Objects have fainter absolute magnitudes than the redder objects of the same type (see Tab. 11).
3.6.3. Others Parameters

Other combinations of the absolute magnitude with other parameters do not show any statistically significant signal.

4. Interpretation scenarios
In the following discussion we try to elaborate and understand the results from the statistical analysis described in Section 3 in the framework of two rather different scenarios, i.e. surface colouration by on-going external processes and surface colours as a result from the primordial constitution of the bodies.
4.1. Surface colouration by external processes

Colour diversity of MBOSSes was originally attributed to the action of external processes on their surfaces. These process included: resurfacing by impacts, expected to produce neutral-bluish colours due to fresh ice excavated and spread over the surface, and an irradiation process, producing red colours via radiation aging (eg Luu and Jewitt 1996, for a model). When restricting our MBOSS database samples to objects with M (1, 1) 5 mag, as done during most of our analysis, a third process, i.e. resurfacing due to atmospheric deposits of material from intrinsic activity, is considered less important for the subsequent discussion, since it should affect large size bodies only, the smaller ones losing the material into space A critical argument for significant changes in the surface reflectivity due to impacts comes from lightcurve analysis of MBOSSes: asymmetric or partial impact resurfacing of the body surfaces should cause colour variegations over rotation phase of the bodies that are, however, usually not seen (Sekiguchi et al. 2002, S. Sonnett, priv. comm., J. L. Ortiz, priv. comm.,) However, other authors report colour changes with rotation phase, eg for Haumea (Lacerda et al. 2008). So, strong variegation is certainly not wide-spread. In the colouration scenario due to external processes DDOs are expected to represent the end state of radiation reddening of the surface, since one can assume that, for these objects, impact resurfacing is not happening at a significant level, simply because spatial number density of DDOs seems very low and collisions should therefore happen extremely rarely over the lifetime of the Solar System. From our statistical analysis we find that DDOs are not the reddest objects among MBOSSes. Instead cold CDOs show by far the reddest surface colours. In order to explain the smaller reddening of DDOs in this colouring scenario one has to assume that cold CDOs are not representing the end state of radiation reddening (despite showing the reddest colours), but high radiation doses, as collected by DDOs, decrease the spectral gradients again. Laboratory experiments
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(de Bergh et al. 2008) have found materials that display such a behaviour although the end state of the material shows rather neutral spectral gradients in the visible wavelength range. However, it remains open whether such materials exist in DDOs and, if not, whether the laboratory results apply more generally to more or even all possible surface compounds considered to exist in DDOs. It is also noteworthy to mention the coincidence of the peaks in the spectral gradient distributions of DDOs and for instance SDOs, Plutinos and resonant objects as well as Centaurs; this may be by chance despite the different importance of collisional resurfacing for these groups. The colour cascade, with peaks in the colour histograms decreasing in reddening from cold CDOs over hot CDOs, to SDOs, Plutinos, resonant objects and parts of the Centaurs must be attributed to increasing importance of impact resurfacing. However, Centaurs live in a rather empty zone of the planetary system; hence, impact resurfacing must contribute less to their evolution. Here, the peak in the spectral gradient diagram could be attributed to resurfacing from intrinsic activity. Instead, the very red Centaurs represent the inactive objects that are subject to radiation reddening only, though not with extremely high doses (otherwise they could be expected to show similar reddening as DDOs). Currently, over the 6 known Centaurs showing cometary activity, only one has red colours. A larger sample of colours of cometary active Centaurs is therefore needed. Jupiter Trojans differ in their surface reddening from the MBOSSes. It is remarkable, that Jupiter Trojans do not show very 'red' surfaces like objects in all MBOSS populations do, despite higher radiation doses from the Sun (due to their closer distance; factor of about 100). So, we conclude that this difference may be due to different material properties compared to MBOSSes. An interesting behaviour is seen for the SPCs: Here, the population peak is well in the range of those for SDOs, Plutinos, moderately red Centaurs as well as for DDOs. Impact resurfacing should be negligible for SPCs and instead resurfacing due to activity could be the explaining reason. On the other side, due to the fast, continuous mass loss on short time scales (lifetime for active SPCs is estimated to be 100 000 years and less) the surface deposits should represent the intrinsic colour of the cometary material. Radiation aging is unimportant over the lifetime of SPC nuclei in the inner planetary system since cometary activity will result in fast and continuous resurfacing of the body. Hence, SPCs give the impression that their nuclei may consist ­on a global scale­ of material with rather homogeneous colour properties. As SPCs to a large extend originate from the Kuiper Belt (Gomes et al. 2008; Morbidelli et al. 2008) and because of their colour similarity to the immediate dynamical relatives therein (SDOs, Plutinos) and to the Centaurs from where SPCs are captured, it is attractive to assume that also the colours of these relatives should be globally uniform throughout the bodies. Jewitt (2002a) discusses the missing very red SPCs, suggesting that the red surfaces are rapidly buried while water ice sublimation starts at r < 6 AU.
4.2. Global colouration in the formation era

An alternative interpretation for the global findings on colour distributions and the M (1, 1) histogram of MBOSSes results from the scenario that the measured colours reflect global properties that apply for the material throughout the bodies. The motivation for this hypothesis comes from the interpretation of SPC colours and from the similarities of the peaks in the colour distribution of the MBOSS populations. We note that Brown et al. (2011) have recently introduced a similar hypothesis for the colour diversity among Kuiper Belt objects on the background of sublimation properties of supervolatile ices. What is described below can in parts be seen as arguments in support of such a 'primordial' colouration scheme for MBOSSes in the planetary system. 'Primordial' addresses the implicit assumption that the colours of the body materials are original from the time before the body was formed, i.e. they range back to the formation period of the planetary system and remained widely unaltered ever since. An additional assumption of the hypothesis is that the surface materials are not - or at least not by a large amount - affected by external processes like reddening due to cosmic radiation. The global character of the material colours implies also that impact resurfacing would reproduce the original pre-impact surface colours of the bodies and large-scale colour diversities on the surface should not occur. Intrinsic activity in MBOSSes will expel gaseous species and solids of which at least the solids may resemble the original colours while the gases, if not lost to interplanetary space, may condense on the body as surface frost, in which case the surface colour may change. However, our selection criterion to use only objects with M (1, 1) > 5 mag for the statistical analysis should significantly reduce the possibility that MBOSSes that may display intrinsic activity 'contaminate' the study results. On the background of the primordial colouration scenario, the findings from our statistical analysis of the MBOSS colours allow interesting conclusions: ­ At least 4 different colour populations may have existed in the protoplanetary disk, i.e. the cold CDOs, the hot CDOs, the SDO/DDO/Plutino population and the Jupiter Trojans. The four
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­

­

­

­

populations are characterize by different surface colours and spectral gradients of decreasing amplitude in the visible wavelength region, but may have very similar colours in the near-IR. The colour diversities among MBOSS populations with different surface colours call for formation environments at different and disjunct distances from the Sun. Migration transport may have shifted the original populations to their current locations in the planetary system. Namely, migration may have placed cold and hot CDOs in the same distance range. Various papers have studied the dynamical aspects of such a migration process in the planetary system (Morbidelli et al. 2008). However, DDOs may represent a challenge for migration scenarios, in particular if one wants to include the aspects of colour similarities with other MBOSS populations. Similar colour properties among MBOSS populations at different locations in the outer planetary system may indicate a common formation region of the bodies. If so, it could apply for Plutinos and DDOs, objects nowadays found at rather different distances from the Sun. Again, migration (for the Plutinos) and scattering (for the DDOs) may have been involved in separating the bodies formed in a common source region. The migration and scattering processes have kept population of the same formation origin together and shifted them to confined destination regions with no obvious signs of intermixing from other sides. This conclusion suggests that the migration and scattering processes in the outer Solar System may not have had a very violent nature since they kept colour characteristics as population entities. The colour distributions for the populations with 'temporary' dynamical object association, i.e. SDOs, Centaurs, and SPCs, should reflect the efficiency of the injection and ejection processes of bodies from the various feeding populations, i.e. Plutinos, hot and cold CDOs.

There are supportive and also critical arguments from the statistical analysis for the conclusions above. In particular, the similarities and differences in the M (1, 1) distributions provide compatible evidences: The disjunct M (1, 1) distributions of the Jupiter Trojans and of the hot and cold CDOs (Doressoundiram et al. 2008, the latter is already noted in various papers and summarized in) may call for different formation environments at different solar distances. On the other side, the existence of large objects with M (1, 1) < 3 mag among Plutinos and DDOs could be seen as a supportive argument for a common source region. Despite a possibly different formation environment for Plutinos and DDOs on one side and of the hot CDOs on the other side as suggested by their colour differences, the presence of large objects ( M (1, 1) < 3 mag) in all three populations suggests that the planetesimal formation and destruction processes were similarly efficient. On the other side, no obvious explanation - except an ad-hoc assumption as an outcome from the formation - can be offered for the anti-correlation between surface colours and excitation parameter as well as inclination among the hot CDO population, since the migration process should be 'colour-blind'. While the existence of very red objects among hot CDOs, DDOs, and Plutinos could be attributed to contaminations from the cold CDOs, the presence of bodies with blue and neutral surface in all populations except for cold CDOs and DDOs may call for colour contaminants either from the primordial environment or due to dynamical injection during a later phase.

5. A summarizing discussion
The MBOSS database first published in 2003 was updated using magnitude and colour measurements of TNOs, Centaurs, Jupiter Trojans, short- and long- periodic comets published since. A qualifying criterion was applied to the data in the database in order to distinguish `problematic' measurement sets from more consistent ones. A new statistical analysis of the qualified colours, spectral gradient and absolute R magnitudes M (1, 1) data in the database was performed with the aim to identify group properties among the various dynamical MBOSS populations, i.e. for the hot and cold classical disk objects (CDOs), the scattered disk objects (SDOs), the Plutinos and resonant objects, as well as for related objects outside of the Kuiper belt like detached disk objects (DDOs), Centaurs, and short-periodic comets (SPCs), using a classification based on the SSBN08 system Gladman et al. (2008). Furthermore Jupiter Trojans are included in the analysis since, from all that is known, these objects are unrelated to the MBOSSes although representing an abundant population at the border of this region in the Solar System. In order to avoid or at least to reduce impacts on the surface colours due to intrinsic activity, the statistical sample was restricted to objects with normalized (but not yet phase corrected) brightness M (1, 1) 5 mag. Our statistical analysis shows indications for indistinguishable and incompatible colour distributions and for differences and similarities in the M (1, 1) parameters among the MBOSS populations. These results suggest a scheme of 4 different colour (and M (1, 1)) groups in the MBOSS regime, i.e. (1) cold CDOs, (2) hot CDOs, (3) Plutinos, resonant objects, SDOs, DDOs, Centaurs and SPCs, and (4) Jupiter Trojans. Additional correlations between photometric and dynamical parameters of the various populations were searched for, but only a single well-established one
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is found in the data of the hot CDOs (colour anti-correlates with inclination and collision energy parameter). The statistical results are discussed on the background of two basic interpretation scenarios, i.e. explaining the surface colours of the MBOSSes (1) as being due to the interplay of resurfacing of impact ejecta (blue colour shift) and radiation reddening (red colour shift) and (2) as being of primordial nature imposed by the material properties of the formation environment. The two scenarios have the principle capability to explain our findings from the analysis of the MBOSS database. However, they are also challenged, each of them in a different way. The resurfacing scenario has to work out whether and under which assumption it is able to reproduce the actually observed colour, spectral gradient and M (1, 1) distributions of the MBOSSes and in particular that it can explain the reddening of the DDOs in this picture. To this respect, further lab measurements on the radiation reddening of reference materials under high dose levels can play an important role. The primordial surface colour scenario has a strong argument in the apparent uniformity of surface colours among SPCs despite cometary activity should be able to excavate material layers of different colours if they exist throughout the nuclei. The primordial surface colour scenario works with ad hoc assumptions in the interpretation of colour, spectral gradient and M (1, 1) parameter distributions which require supportive justifications. Brown et al. (2011) have indicated some first arguments to this respect. However, beyond that the scenario interpretation relies on object migration for the transport of the MBOSSes from their formation environment to the various regions where they are found today. Object migration in the early planetary system was already introduced to explain the existence of the hot CDOs in the immediate neighborhood of the cold CDOs in the Kuiper Belt (for a review see Morbidelli et al., 2008). The primordial colouration scenario requires more than the shift of one or both CDO populations; it also asks for a detailed understanding of the dynamical processes and to which extend they may have affected the distribution of the measurements of the physical and surface parameters of the MBOSSes.
Acknowledgements. H. Boehnhardt wants to thank the European Southern Observatory for support of this work during his research stay in September and November 2011 at ESO Headquarters in Garching/Germany. This research has made use of NASA's Astrophysics Data System.

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Weintraub, D. A., Tegler, S. C., and Romanishin, W. (1997). Visible and Near-Infrared Photometry of the Centaur Objects 1995 GO and 5145 Pholus. Icarus, 128:456­463.

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O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 1

Appendix A: Online material


Table A.1. Object class and colour data Object 1P/Halley 2P/Encke 4P/Faye 6P/dArrest 7P/PW 8P/Tuttle 9P/Tempel 1 10P/Tempel 2 14P/Wolf 15P/Finlay 16P/Brooks2 17P/Holmes 19P/Borrelly 21P/GZ 22P/Kopff 24P/Schaumasse 26P/GS 28P/Neujmin1 29P/SW1 30P/Reinmuth1 31P/SW2 32P/ComasSola 33P/Daniel 36P/Whipple 37P/Forbes 39P/Oterma 40P/Vaisala1 41P/TG 42P/Neujmin3 43P/WH 44P/Reinmuth2 45P/HMP 46P/Wirtanen 47P/AJ 48P/Johnson Class(1) SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet Centaurs SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet Centaurs SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet Epochs( 2 6 2 3 2 2 14 10 2 1 1 2 1 2 4 1 2 11 3 1 1 1 1 1 2 3 1 1 1 1 2 2 3 2 1
2)

13. 15. 16. 16. 15. 12. 14. 14. 15. 17. 16. 16. 15. 17. 16. 17. 16. 12. 11. 14. 14. 14. 17. 15. 17. 12. 15. 18. 17. 15. 16. 17. 18. 15. 14.

M11 ± 558 ± 0.596 207 ± 0.596 020 ± 0.009 239 ± 0.009 185 ± 0.009 799 ± 0.009 560 ± 0.460 287 ± 0.304 423 ± 0.009 488 ± 0.009 107 ± 0.009 094 ± 0.009 860 ± 0.009 259 ± 0.009 093 ± 0.156 744 ± 0.009 642 ± 0.136 580 ± 0.009 322 ± 0.009 602 ± 0.009 803 ± 0.009 478 ± 0.009 053 ± 0.009 432 ± 0.009 348 ± 0.009 464 ± 0.009 983 ± 0.009 034 ± 0.009 259 ± 0.009 983 ± 0.009 225 ± 0.009 744 ± 0.009 369 ± 0.009 024 ± 0.009 970 ± 0.009

Gr t ± 4.266 ± 2.015 5.117 ± 2.574 7.951 ± 0.000 13.264 ± 2.147 4.264 ± 2.620 15.869 ± 2.326 9.959 ± 0.826 13.740 ± 1.578 17.666 ± 3.210 -- -- 18.608 ± 0.000 -- 12.661 ± 2.057 12.577 ± 2.730 -- 5.227 ± 0.000 9.967 ± 4.007 14.948 ± 1.099 -- -- -- -- -- 3.181 ± 2.015 3.094 ± 3.964 -- -- -- -- 24.892 ± 0.000 0.768 ± 2.444 4.079 ± 0.000 3.454 ± 7.417 --

B -V ± 0.720 ± 0.040 0.780 ± 0.020 -- 0.770 ± 0.040 -- 0.890 ± 0.040 -- 0.800 ± 0.020 -- -- -- -- -- 0.800 ± 0.030 0.795 ± 0.056 -- -- -- 0.790 ± 0.030 -- -- -- -- -- -- 0.890 ± 0.070 -- -- -- -- -- 1.080 ± 0.050 -- 0.780 ± 0.080 --

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

0. 0.

0. 0. 0. 0.

V-R ± 410 ± 0.030 424 ± 0.053 450 ± 0.040 563 ± 0.067 400 ± 0.050 530 ± 0.040 468 ± 0.010 521 ± 0.037 570 ± 0.070 -- -- 560 ± 0.020 -- 500 ± 0.020 519 ± 0.046 -- 420 ± 0.139 494 ± 0.072 536 ± 0.030 -- -- -- -- -- 290 ± 0.030 386 ± 0.063 -- -- -- -- 620 ± 0.080 440 ± 0.050 407 ± 0.081 400 ± 0.080 --

R -I ± 0.390 ± 0.060 0.408 ± 0.060 -- 0.450 ± 0.040 0.410 ± 0.060 0.530 ± 0.060 0.469 ± 0.013 0.520 ± 0.030 0.510 ± 0.060 -- -- -- -- -- 0.450 ± 0.055 -- -- 0.440 ± 0.079 0.497 ± 0.025 -- -- -- -- -- 0.660 ± 0.060 0.412 ± 0.114 -- -- -- -- -- 0.210 ± 0.050 -- -- --

V-J ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

J-H ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

H- K ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 2


Table A.1. continued. Object 49P/AR 50P/Arend 51P/Harrington 52P/HA 53P/VanBiesbroec 55P/TT 56P/SB 57P/dTND 58P/JN 59P/KK 60P/Tsuchinshan2 61P/SS 62P/Tsuchinshan1 63P/Wild1 64P/SG 65P/Gunn 67P/CG 68P/Klemola 69P/Taylor 70P/Kojima 71P/Clark 72P/DF 73P/SW3 73P/SW3C 74P/SC 75P/Kohoutek 76P/WKI 77P/Longmore 78P/Gehrels2 79P/dTH 81P/Wild2 82P/Gehrels3 84P/Giclas 86P/Wild3 87P/Bus 88P/Howell C SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP lass(1) Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Epochs( 3 2 1 1 2 2 1 1 1 2 1 1 1 2 1 1 2 1 1 2 2 1 1 1 1 1 1 1 1 1 1 1 2 3 2 1
2)

14. 17. 15. 16. 14. 15. 16. 16. 18. 17. 17. 18. 17. 16. 16. 13. 15. 15. 14. 15. 18. 17. 16. 18. 15. 15. 19. 15. 16. 16. 15. 17. 17. 19. 20. 15.

M11 ± 120 ± 0.277 371 ± 0.009 648 ± 0.009 690 ± 0.009 647 ± 0.009 543 ± 0.482 294 ± 0.009 239 ± 0.009 369 ± 0.009 771 ± 0.009 744 ± 0.009 229 ± 0.009 744 ± 0.009 453 ± 0.009 239 ± 0.009 853 ± 0.009 754 ± 0.009 547 ± 0.009 947 ± 0.009 912 ± 0.009 097 ± 0.009 744 ± 0.009 850 ± 0.050 097 ± 0.009 518 ± 0.009 754 ± 0.009 667 ± 0.009 358 ± 0.009 498 ± 0.009 529 ± 0.009 754 ± 0.009 943 ± 0.009 488 ± 0.009 092 ± 0.009 024 ± 0.009 866 ± 0.009

Gr t ± 9.452 ± 2.141 24.132 ± 4.627 -- -- -2.672 ± 0.000 10.765 ± 2.444 -- -- -- 12.937 ± 3.558 -- -- -- 10.054 ± 2.273 -- -- 13.630 ± 0.000 -- -- 22.758 ± 0.000 27.065 ± 0.000 -- 10.751 ± 0.000 -- -- -- -- -- -- -- -- -- -3.328 ± 0.000 18.211 ±35.399 16.889 ± 0.000 --

B -V ± 0.770 ± 0.030 -- -- -- -- 0.750 ± 0.050 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 1.580 ± 0.080 -- --

V-R ± 0.471 ± 0.032 0.810 ± 0.100 -- -- 0.328 ± 0.081 0.510 ± 0.050 -- -- -- 0.620 ± 0.070 -- -- -- 0.500 ± 0.050 -- -- 0.510 ± 0.060 -- -- 0.600 ± 0.090 0.640 ± 0.070 -- 0.480 ± 0.235 -- -- -- -- -- -- -- -- -- 0.320 ± 0.030 0.555 ± 0.385 0.543 ± 0.020 --

R -I ± 0.444 ± 0.064 0.260 ± 0.090 -- -- -- 0.420 ± 0.050 -- -- -- 0.270 ± 0.080 -- -- -- 0.420 ± 0.040 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

V-J ± 1.630 ± 0.200 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

J-H ± 0.360 ± 0.141 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

H- K ± 0.140 ± 0.141 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 3


Table A.1. continued. Object 89P/Russell2 90P/Gehrels1 91P/Russell3 92P/Sanguin 93P/HL 94P/Russell4 96P/Machholz1 97P/MB 98P/Takamizawa 99P/Kowal1 100P/Hartley1 101P/Chernykh 103P/Hartley2 104P/Kowal2 105P/SB 106P/Schuster 107P/WH 109P/ST 110P/Hartley3 111P/HRC 112P/UN 113P/Spitaler 114P/WS 115P/Maury 116P/Wild4 117P/HRA 118P/SL 119P/PH 120P/Mueller1 121P/SH 123P/WH 124P/Mrkos 125P/Spacewatch 126P/IRAS 128P/SH 129P/SL C SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP SP lass(1) Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Comet Epochs( 1 1 1 2 1 1 2 1 1 1 1 1 1 1 1 2 6 2 2 1 2 1 2 1 1 1 1 1 1 1 1 1 1 1 1 1
2)

16. 14. 16. 16. 15. 14. 16. 14. 13. 16. 15. 17. 17. 17. 17. 15. 12. 15. 18. 17. 17. 17. 17. 14. 14. 15. 15. 16. 16. 15. 16. 17. 16. 15. 15.

M11 ± 864 ± 0.009 602 ± 0.009 690 ± 0.009 882 ± 0.009 -- 866 ± 0.009 734 ± 0.009 107 ± 0.009 418 ± 0.009 853 ± 0.009 690 ± 0.009 358 ± 0.009 744 ± 0.009 259 ± 0.009 259 ± 0.009 394 ± 0.009 865 ± 0.220 002 ± 0.376 597 ± 0.009 369 ± 0.009 488 ± 0.009 053 ± 0.009 799 ± 0.009 033 ± 0.009 539 ± 0.009 304 ± 0.009 358 ± 0.009 270 ± 0.009 379 ± 0.009 212 ± 0.009 547 ± 0.009 239 ± 0.009 744 ± 0.009 280 ± 0.009 451 ± 0.009 358 ± 0.009

Gr t ± -- -- -- 16.937 ± 1.982 -7.552 ± 0.000 -- 6.036 ± 0.000 -- -- -- -- -- -- -- -- 12.396 ± 2.913 0.119 ± 4.538 18.608 ± 0.000 30.401 ± 0.000 -- 15.593 ± 0.000 -- 12.158 ± 1.087 -- -- -- -- -- -- -- -- -- -- -- -- --

B -V ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 1.010 ± 0.060 0.674 ± 0.089 -- -- -- -- -- 0.850 ± 0.030 -- -- -- -- -- -- -- -- -- -- -- -- --

0. 0. 0.

0. 0. 0. 0. 0. 0.

V-R ± -- -- -- 540 ± 0.040 267 ± 0.075 -- 429 ± 0.027 -- -- -- -- -- -- -- -- 520 ± 0.060 361 ± 0.048 560 ± 0.050 670 ± 0.090 -- 530 ± 0.040 -- 460 ± 0.020 -- -- -- -- -- -- -- -- -- -- -- -- --

R -I ± -- -- -- 0.540 ± 0.040 -- -- -- -- -- -- -- -- -- -- -- 0.450 ± 0.060 -- -- -- -- -- -- 0.540 ± 0.020 -- -- -- -- -- -- -- -- -- -- -- -- --

V-J ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

J-H ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

H- K ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 4


Table A.1. continued. Object 130P/McNH 131P/Mueller2 132P/HRA 134P/KV 135P/SL 136P/Mueller3 137P/SL 138P/SL 139P/VO 140P/BS 141P/Machholz2 143P/KM 144P/Kushida 147P/KM 148P/AL 152P/HL 154P/Brewington 166P/2001T4 204P/Wild2 1172-Aneas 1173-Anchises 1647-Menelaus 1871-Astyanax 1993 RO 1994 ES2 1994 EV3 1994 TA 1995 DB2 1995 DC2 1995 FB21 1995 HM5 1995 WY2 1996 KV1 1996 RQ20 1996 RR20 1996 TC68 Class(1) SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet SP Comet Centaurs SP Comet J.Trojan J.Trojan J.Trojan J.Trojan Res. 3:2 Classic Cold Classic Cold Centaurs Classic Cold Classic Cold Classic Cold Res. 3:2 Classic Cold Classic Hot Classic Hot Res. 3:2 Classic Hot Epochs( 1 1 1 1 1 1 1 1 1 1 1 5 1 1 1 1 1 2 1 2 1 1 3 2 1 4 2 2 5 4 8 2 1 7 4 1
2)

15. 17. 17. 16. 16. 15. 14. 17. 15. 15. 17. 13. 16. 20. 15. 13. 16.

M11 ± 983 ± 0.009 744 ± 0.009 488 ± 0.009 529 ± 0.009 239 ± 0.009 866 ± 0.009 947 ± 0.009 744 ± 0.009 185 ± 0.009 451 ± 0.009 259 ± 0.009 598 ± 0.009 864 ± 0.009 648 ± 0.009 648 ± 0.009 946 ± 0.009 379 ± 0.009 -- -- 8.729 ± 0.042 8.793 ± 0.059 -- 11.149 ± 0.093 8.612 ± 0.134 7.509 ± 0.130 7.048 ± 0.178 11.421 ± 0.126 8.058 ± 0.120 6.809 ± 0.204 7.017 ± 0.099 7.849 ± 0.109 6.935 ± 0.149 -- 6.872 ± 0.100 6.811 ± 0.252 6.734 ± 0.073

Gr t ± -- -- -- -- -- -- -- -- -- -- -- 20.354 ± 1.102 -- -- -- -- -- 36.293 ± 1.976 -- 9.261 ± 0.863 4.286 ± 1.443 6.803 ± 1.630 7.777 ± 2.485 24.485 ± 4.231 -- 30.400 ± 7.250 31.545 ± 6.243 54.335 ± 0.000 35.475 ± 7.654 -- 9.432 ± 3.661 19.923 ±11.862 -- 22.364 ± 4.307 36.280 ± 5.193 22.758 ± 0.000

0.

0. 0. 0. 0. 0. 1. 1.

0. 1. 0. 1.

B -V ± -- -- -- -- -- -- -- -- -- -- -- 820 ± 0.023 -- -- -- -- -- 870 ± 0.040 -- 727 ± 0.030 811 ± 0.034 -- 716 ± 0.071 850 ± 0.070 -- 065 ± 0.110 261 ± 0.139 -- -- -- 649 ± 0.102 030 ± 0.280 -- 935 ± 0.141 143 ± 0.106 --

0.

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

V-R ± -- -- -- -- -- -- -- -- -- -- -- 580 ± 0.020 -- -- -- -- -- 695 ± 0.030 -- 510 ± 0.022 402 ± 0.035 428 ± 0.043 456 ± 0.053 590 ± 0.137 -- 588 ± 0.156 672 ± 0.080 -- 770 ± 0.160 -- 460 ± 0.097 600 ± 0.230 -- 558 ± 0.096 730 ± 0.095 600 ± 0.078

0.

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

R -I ± -- -- -- -- -- -- -- -- -- -- -- 560 ± 0.021 -- -- -- -- -- 735 ± 0.060 436 ± 0.093 400 ± 0.030 403 ± 0.052 438 ± 0.061 424 ± 0.089 480 ± 0.113 -- 800 ± 0.126 740 ± 0.210 -- 580 ± 0.160 -- 428 ± 0.126 510 ± 0.280 -- 591 ± 0.109 628 ± 0.125 --

V-J ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 1.577 ± 0.036 -- -- 1.422 ± 0.103 -- -- -- -- -- -- -- -- -- -- -- -- --

0. 0.

1. 0. 0.

J-H ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 430 ± 0.042 -- -- 373 ± 0.053 -- -- -- -- -- -- -- 180 ± 0.470 -- 430 ± 0.256 380 ± 0.226 -- --

H- K ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 0.135 ± 0.036 -- -- 0.123 ± 0.040 -- -- -- -- -- -- -- -- -- -- -- -- --

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 5


Table A.1. continued. Object 1996 TK66 1996 TS66 1997 CT29 1997 CV29 1997 GA45 1997 QH4 1997 RL13 1997 RT5 1997 RX9 1997 SZ10 1998 FS144 1998 KG62 1998 KS65 1998 KY61 1998 UR43 1998 UU43 1998 WS31 1998 WU24 1998 WV24 1998 WV31 1998 WW31 1998 WW31 1998 WX24 1998 WX31 1998 WY24 1998 WZ31 1998 XY95 1999 CB119 1999 CD158 1999 CF119 1999 CH119 1999 CJ119 1999 CL119 1999 CQ133 1999 CX131 1999 HJ12 Class(1) Classic Cold Classic Hot Classic Cold Classic Hot Classic Hot Classic Hot Classic Hot Classic Hot Classic Hot Res.(other) Classic Hot Classic Cold Classic Cold Classic Cold Res. 3:2 Res.(other) Res. 3:2 Scattered Classic Cold Res. 3:2 Classic Hot Classic Hot Classic Cold Classic Cold Classic Cold Res. 3:2 Detached Classic Hot Res.(other) Detached Classic Hot Classic Cold Classic Hot Classic Hot Res.(other) Classic Cold Epochs( 4 7 4 2 1 4 1 4 1 1 4 5 2 1 4 2 2 1 2 2 1 1 2 3 2 3 2 1 5 3 1 1 2 1 3 2
2)

6. 5. 6. 7. 7. 7. 9. 6. 7. 8. 6. 6. 7. 8. 6. 7. 7. 7. 6. 6. 6. 8. 6. 6. 4. 6. 5. 6.

+B

M11 ± 190 ± 0.116 947 ± 0.130 452 ± 0.173 154 ± 0.030 744 ± 0.500 128 ± 0.175 361 ± 0.300 951 ± 0.379 802 ± 0.100 148 ± 0.060 717 ± 0.105 367 ± 0.283 166 ± 0.040 -- 124 ± 0.134 925 ± 0.110 931 ± 0.203 -- 126 ± 0.067 639 ± 0.072 -- -- 241 ± 0.099 159 ± 0.095 441 ± 0.086 045 ± 0.115 438 ± 0.143 737 ± 0.076 822 ± 0.099 933 ± 0.133 -- -- 699 ± 0.072 -- 910 ± 0.107 --

29. 26. 32. 28.

Gr t ± 906 ± 4.054 561 ± 4.871 698 ± 4.508 171 ± 2.056 -- 27.144 ± 4.569 -- 15.015 ± 4.506 -- 28.167 ± 2.909 23.851 ± 3.089 24.857 ± 3.762 26.149 ± 1.858 -- 14.454 ± 7.356 14.799 ± 3.950 18.738 ± 6.008 12.934 ± 1.361 11.777 ± 3.357 13.835 ± 4.507 8.864 ± 0.000 2.628 ± 0.000 30.875 ± 3.793 29.252 ± 3.312 29.095 ± 3.185 6.687 ± 4.513 41.429 ± 5.409 33.869 ± 2.678 16.860 ± 2.607 14.704 ± 4.163 -- -- 19.530 ± 3.359 -- 19.521 ± 4.293 30.391 ± 0.000

B -V ± 0.993 ± 0.062 1.028 ± 0.079 -- 1.210 ± 0.010 -- 1.088 ± 0.143 -- 1.075 ± 0.121 -- 1.140 ± 0.080 0.950 ± 0.044 1.039 ± 0.105 1.090 ± 0.040 -- 0.784 ± 0.101 -- 0.726 ± 0.080 0.780 ± 0.034 0.770 ± 0.010 0.790 ± 0.099 -- -- 1.090 ± 0.050 -- -- 0.727 ± 0.093 0.930 ± 0.233 1.212 ± 0.102 0.864 ± 0.056 -- -- -- -- -- 0.918 ± 0.124 --

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

V-R ± 680 ± 0.067 672 ± 0.106 762 ± 0.105 650 ± 0.020 -- 641 ± 0.092 -- 474 ± 0.107 -- 650 ± 0.030 588 ± 0.060 609 ± 0.095 640 ± 0.020 -- 583 ± 0.120 610 ± 0.120 606 ± 0.102 530 ± 0.037 502 ± 0.058 521 ± 0.075 -- -- 727 ± 0.086 638 ± 0.083 620 ± 0.092 489 ± 0.114 720 ± 0.145 714 ± 0.076 520 ± 0.053 622 ± 0.115 -- -- 497 ± 0.077 -- 664 ± 0.128 --

R -I ± 0.551 ± 0.097 0.637 ± 0.088 0.490 ± 0.120 -- -- 0.631 ± 0.107 -- 0.539 ± 0.091 -- -- 0.510 ± 0.085 0.610 ± 0.078 -- -- 0.354 ± 0.175 0.400 ± 0.114 0.439 ± 0.172 0.460 ± 0.051 0.450 ± 0.106 0.481 ± 0.144 -- -- 0.500 ± 0.092 0.653 ± 0.081 0.680 ± 0.078 0.339 ± 0.114 0.752 ± 0.126 0.645 ± 0.062 0.575 ± 0.064 0.365 ± 0.106 -- -- 0.665 ± 0.094 -- 0.434 ± 0.105 --

V-J ± -- 1.824 ± 0.178 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 1.670 ± 0.043 -- -- -- -- -- -- -- -- -- -- 1.862 ± 0.076 -- -- -- -- -- -- --

0. 0. 0.

0. 0. 0. 0. 0. 0.

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

J-H ± -- 650 ± 0.071 410 ± 0.238 360 ± 0.243 -- -- -- 380 ± 0.231 -- -- 390 ± 0.228 410 ± 0.231 -- 350 ± 0.278 -- 490 ± 0.273 -- 430 ± 0.125 -- -- -- -- -- 400 ± 0.235 400 ± 0.240 400 ± 0.234 -- -- 423 ± 0.135 380 ± 0.226 320 ± 0.266 450 ± 0.265 450 ± 0.282 460 ± 0.282 370 ± 0.238 480 ± 0.598

H- K ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 0.240 ± 0.189 -- -- -- -- -- -- -- -- -- -- 0.048 ± 0.116 -- -- -- -- -- -- --

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 6


Table A.1. continued. Object 1999 HS11 1999 HV11 1999 OD4 1999 OE4 1999 OH4 1999 OJ4 1999 OJ4+ B 1999 OM4 1999 RC215 1999 RT214 1999 RX214 1999 RY214 1999 TR11 1999 XY143 2000 AF255 2000 CE105 2000 CF105 2000 CF105+ B 2000 CG105 2000 CK105 2000 CL104 2000 CN105 2000 CO105 2000 CP104 2000 CQ105 2000 CQ114 2000 CQ114+ B 2000 FS53 2000 FV53 2000 FZ53 2000 GV146 2000 KK4 2000 KL4 2000 OU69 2000 PD30 2000 PE30 Class(1) Classic Cold Classic Cold Classic Hot Classic Cold Classic Hot Classic Cold Classic Cold Classic Cold Classic Cold Classic Cold Classic Cold Classic Hot Res. 3:2 Classic Hot Detached Classic Cold Classic Cold Classic Cold Classic Hot Res. 3:2 Classic Cold Classic Cold Classic Hot Classic Hot Detached Classic Cold Classic Cold Classic Cold Res. 3:2 Centaurs Classic Cold Classic Hot Classic Hot Classic Cold Classic Cold Detached Epochs( 3 1 1 4 2 5 1 1 2 1 3 2 2 1 1 2 6 1 3 2 4 4 2 2 5 3 1 2 1 2 1 3 1 3 2 7
2)

M11 ± 6.331 ± 0.079 7.003 ± 0.050 -- 6.831 ± 0.177 6.321 ± 0.123 6.912 ± 0.062 -- 7.502 ± 0.100 6.571 ± 0.126 -- 6.413 ± 0.052 7.010 ± 0.065 8.144 ± 0.152 5.924 ± 0.065 -- -- -- -- 6.124 ± 0.311 6.370 ± 0.118 6.642 ± 0.229 5.261 ± 0.072 5.594 ± 0.078 -- 5.965 ± 0.049 6.660 ± 0.147 -- 7.300 ± 0.080 7.550 ± 0.087 10.990 ± 0.085 -- 5.982 ± 0.103 -- 6.839 ± 0.120 -- 5.796 ± 0.081

Gr t ± 31.102 ± 3.766 21.706 ± 2.057 -- 13.989 ± 7.765 -7.656 ± 9.026 26.192 ± 3.113 34.360 ± 0.000 18.976 ± 3.909 33.893 ± 4.703 35.732 ± 0.000 20.207 ± 2.817 18.063 ± 3.131 37.094 ± 4.048 26.014 ± 2.399 -- 14.512 ± 0.000 24.245 ± 0.000 21.377 ± 0.000 -- 25.479 ± 4.225 23.634 ± 4.673 29.677 ± 1.174 22.327 ± 2.904 18.106 ± 0.000 7.864 ± 2.902 34.780 ± 4.289 33.683 ± 0.000 34.603 ± 1.976 17.018 ± 4.070 14.413 ± 3.939 35.732 ± 0.000 17.292 ± 2.477 27.864 ± 0.000 10.128 ± 0.000 19.719 ± 0.000 2.353 ± 3.158

B -V ± 1.121 ± 0.082 1.110 ± 0.060 -- 1.103 ± 0.236 -- 1.098 ± 0.157 -- 1.137 ± 0.135 -- -- 1.054 ± 0.072 0.693 ± 0.087 1.020 ± 0.080 -- -- -- -- -- -- -- 1.223 ± 0.167 1.100 ± 0.020 -- -- 0.671 ± 0.023 -- -- 1.060 ± 0.040 -- -- -- 0.910 ± 0.040 -- -- -- 0.752 ± 0.069

V-R ± 0.698 ± 0.056 0.590 ± 0.020 -- 0.567 ± 0.159 0.200 ± 0.134 0.668 ± 0.072 -- 0.602 ± 0.104 0.810 ± 0.134 -- 0.593 ± 0.065 0.565 ± 0.080 0.750 ± 0.097 0.590 ± 0.071 -- -- -- -- 0.107 ± 0.246 0.590 ± 0.127 0.600 ± 0.119 0.636 ± 0.072 0.620 ± 0.085 -- 0.449 ± 0.038 0.690 ± 0.156 -- 0.710 ± 0.020 0.448 ± 0.094 0.686 ± 0.090 -- 0.580 ± 0.102 -- 0.473 ± 0.130 -- 0.373 ± 0.077

R -I ± 0.600 ± 0.090 -- -- 0.414 ± 0.180 0.430 ± 0.335 0.549 ± 0.073 -- 0.499 ± 0.088 0.520 ± 0.120 -- 0.530 ± 0.066 0.530 ± 0.084 0.650 ± 0.122 0.660 ± 0.064 -- -- -- -- 0.293 ± 0.265 0.650 ± 0.114 0.612 ± 0.128 0.640 ± 0.020 0.550 ± 0.078 -- 0.346 ± 0.101 0.650 ± 0.134 -- -- 0.679 ± 0.116 0.238 ± 0.103 -- 0.640 ± 0.064 -- -- -- 0.410 ± 0.049

V-J ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 1.790 ± 0.106 -- -- -- 1.646 ± 0.080

0. 0. 0. 0. 0.

0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

0. 0. 0.

J-H ± -- -- 460 ± 0.282 360 ± 0.216 330 ± 0.328 230 ± 0.197 -- -- 320 ± 0.225 -- -- -- -- -- 460 ± 0.265 160 ± 0.184 400 ± 0.266 -- 510 ± 0.298 390 ± 0.256 450 ± 0.285 -- 380 ± 0.228 440 ± 0.289 420 ± 0.262 420 ± 0.403 -- -- -- -- -- -- -- 400 ± 0.235 560 ± 0.336 452 ± 0.114

H- K ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 0.260 ± 0.072

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 7


Table A.1. continued. Object 2000 PH30 2000 QL251 2000 QL251+ B 2001 FL185 2001 FM194 2001 FU172 2001 KA77 2001 KB77 2001 KD77 2001 KG77 2001 KY76 2001 OG109 2001 OK108 2001 QC298 2001 QC298+ B 2001 QD298 2001 QF298 2001 QX322 2001 XR254 2001 XR254+ B 2001 XU254 2001 XZ255 2002 CB249 2002 DH5 2002 GB32 2002 PP149 2003 FZ129 2003 GH55 2003 HB57 2003 HX56 2003 QA92 2003 QD112 2003 QK91 2003 QQ91 2003 QW111 2003 QW111+ B Class(1) Detached Classic Cold Classic Cold Classic Cold Detached Res. 3:2 Classic Hot Res. 3:2 Res. 3:2 Scattered Res. 3:2 Classic Cold Classic Cold Classic Hot Classic Hot Classic Hot Res. 3:2 Detached Classic Cold Classic Cold Classic Hot Centaurs Centaurs Centaurs Scattered Classic Hot Detached Classic Cold Scattered Classic Hot Classic Cold Centaurs Detached Classic Hot Res.(other) Res.(other) Epochs( 1 1 1 1 1 1 4 6 9 1 1 1 1 3 1 1 8 3 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1
2)

M11 ± -- -- -- -- 7.582 ± 0.040 8.165 ± 0.181 5.050 ± 0.094 7.373 ± 0.063 5.926 ± 0.104 8.340 ± 0.120 -- -- -- 6.421 ± 0.030 -- 6.185 ± 0.170 5.128 ± 0.126 6.388 ± 0.080 -- -- -- 10.800 ± 0.080 10.587 ± 0.109 10.190 ± 0.061 7.637 ± 0.010 7.256 ± 0.030 6.982 ± 0.020 5.949 ± 0.050 7.389 ± 0.020 7.030 ± 0.209 -- 11.641 ± 0.030 6.967 ± 0.030 -- -- --

Gr t ± -- 6.266 ± 0.000 12.082 ± 0.000 23.082 ± 0.000 7.035 ± 2.909 22.552 ± 8.420 37.759 ± 3.264 11.050 ± 3.211 24.005 ± 2.575 7.034 ± 5.595 -- -- -- 10.333 ± 2.434 6.266 ± 0.000 30.399 ± 8.330 2.287 ± 2.687 18.862 ± 5.260 15.011 ± 0.000 16.024 ± 0.000 -- 39.753 ± 6.501 5.278 ± 4.487 4.151 ± 2.833 18.001 ± 1.087 -6.534 ± 3.793 10.329 ± 1.812 25.973 ± 5.595 13.225 ± 1.525 -1.963 ±13.676 25.973 ± 3.793 -- 11.829 ± 1.812 13.624 ± 7.416 27.864 ± 0.000 30.391 ± 0.000

0. 1. 1. 0.

0. 0. 0. 0.

1. 0. 0. 0. 0. 1. 0. 1. 0. 0.

B -V ± -- -- -- -- 760 ± 0.030 -- 104 ± 0.107 -- 123 ± 0.054 810 ± 0.040 -- -- -- 750 ± 0.080 -- 970 ± 0.130 644 ± 0.070 914 ± 0.058 -- -- -- 170 ± 0.020 -- 663 ± 0.072 880 ± 0.028 850 ± 0.100 840 ± 0.057 120 ± 0.050 830 ± 0.042 -- 040 ± 0.030 -- 870 ± 0.057 670 ± 0.060 -- --

0. 0. 0. 0. 0. 0.

0. 0. 0. 0.

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

V-R ± -- -- -- -- 440 ± 0.030 670 ± 0.192 704 ± 0.064 434 ± 0.083 624 ± 0.070 440 ± 0.060 -- -- -- 490 ± 0.030 -- 670 ± 0.090 381 ± 0.062 563 ± 0.056 -- -- -- 750 ± 0.070 492 ± 0.116 391 ± 0.069 510 ± 0.020 280 ± 0.040 480 ± 0.040 630 ± 0.060 480 ± 0.030 350 ± 0.226 630 ± 0.040 -- 500 ± 0.040 510 ± 0.080 -- --

0. 0. 0. 0.

0. 0.

0. 0. 0. 0. 0. 0. 0.

R -I ± -- -- -- -- -- 470 ± 0.225 716 ± 0.120 548 ± 0.089 565 ± 0.069 -- -- -- -- 480 ± 0.040 -- -- 360 ± 0.085 -- -- -- -- -- 300 ± 0.114 416 ± 0.081 610 ± 0.020 -- 460 ± 0.030 -- 540 ± 0.030 260 ± 0.459 -- -- 470 ± 0.030 -- -- --

V-J ± -- -- -- -- -- -- -- -- 2.294 ± 0.092 -- -- -- -- -- -- -- 1.126 ± 0.124 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

J-H ± 0.550 ± 0.361 -- -- -- -- -- -- -- 0.366 ± 0.141 -- 0.390 ± 0.228 0.350 ± 0.300 0.430 ± 0.275 0.430 ± 0.323 -- -- 0.317 ± 0.172 0.410 ± 0.247 -- -- 0.370 ± 0.226 -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

H- K ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 0.165 ± 0.113 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- --

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 8


Table A.1. continued. Object 2003 QW90 2003 QY90 2003 QY90+ B 2003 SQ317 2003 TH58 2003 TJ58 2003 TJ58+ B 2003 UY291 2003 UZ117 2003 YL179 2004 OJ14 2004 PB108 2004 PB108+ B 2004 PT107 2004 PY42 2004 VN112 2004 XR190 2005 CB79 2005 EO297 2005 EO304 2005 EO304+ B 2005 GE187 2005 PU21 2005 SD278 2006 SQ372 2007 TG422 2007 VJ305 2008 KV42 2008 OG19 2008 YB3 2060-Chiron 2223-Sarpedon 2357-Phereclos 3548-Eurybates 4035-1986 WD 4829-Sergestus Class(1) Res. 3:2 Classic Cold Classic Cold Classic Hot Res. 3:2 Classic Cold Classic Cold Classic Cold Classic Hot Classic Cold Detached Classic Hot Classic Hot Classic Hot 1 Detached Detached Classic Hot Detached Classic Cold Classic Cold Res. 3:2 Scattered Detached Scattered Scattered Detached Scattered Detached SP Comet Centaurs J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan Epochs( 2 1 1 1 1 1 1 1 4 1 1 1 1 1 -- 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 34 1 1 1 2 1
2)

M11 ± -- -- -- 6.161 ± 0.020 7.007 ± 0.045 -- -- -- 4.961 ± 0.020 -- 6.991 ± 0.020 -- -- 5.847 ± 0.010 17.581 ± 1.360 -- 3.937 ± 0.030 4.375 ± 0.028 7.220 ± 0.030 -- -- 7.214 ± 0.030 6.091 ± 0.020 5.916 ± 0.020 7.667 ± 0.020 6.186 ± 0.010 6.713 ± 0.020 8.565 ± 0.040 4.611 ± 0.010 9.715 ± 0.010 6.092 ± 0.069 9.265 ± 0.046 8.817 ± 0.078 -- 9.489 ± 0.080 11.122 ± 0.068

Gr t ± 15.349 ± 0.000 32.348 ± 0.000 32.348 ± 0.000 -- 5.615 ± 2.028 19.719 ± 0.000 18.639 ± 0.000 20.163 ± 3.383 -0.537 ± 1.824 7.953 ± 9.243 15.681 ± 1.525 19.177 ± 0.000 21.377 ± 0.000 -- 0.770 ± 0.030 12.396 ± 2.913 10.679 ± 1.982 1.054 ± 1.574 13.673 ± 2.955 38.554 ± 0.000 33.683 ± 0.000 -- 30.943 ± 1.087 17.797 ± 1.087 24.677 ± 1.702 13.918 ± 1.982 14.913 ± 1.525 8.461 ± 2.913 18.921 ± 0.677 10.549 ± 0.677 0.114 ± 0.996 8.785 ± 1.244 7.601 ± 1.876 -0.087 ± 1.847 10.259 ± 1.995 4.196 ± 1.856

0. 0. 0. 0. 0.

0. 0. 0. 0. 0.

1. 0. 1. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

B -V ± -- -- -- -- 610 ± 0.064 -- -- 880 ± 0.099 676 ± 0.031 810 ± 0.040 900 ± 0.042 -- -- -- 550 ± 0.030 900 ± 0.085 790 ± 0.057 740 ± 0.036 840 ± 0.071 -- -- -- 140 ± 0.028 970 ± 0.028 030 ± 0.042 880 ± 0.057 920 ± 0.042 820 ± 0.085 940 ± 0.014 800 ± 0.014 700 ± 0.020 753 ± 0.032 718 ± 0.059 677 ± 0.052 752 ± 0.040 851 ± 0.050

0. 0. 0. 0. 0.

0. 0. 0. 0. 0.

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

V-R ± -- -- -- -- 380 ± 0.045 -- -- 510 ± 0.070 350 ± 0.028 450 ± 0.100 520 ± 0.030 -- -- -- 540 ± 0.020 520 ± 0.060 450 ± 0.040 350 ± 0.036 480 ± 0.050 -- -- -- 650 ± 0.020 560 ± 0.020 590 ± 0.030 510 ± 0.040 520 ± 0.030 470 ± 0.060 530 ± 0.010 460 ± 0.010 361 ± 0.017 465 ± 0.025 427 ± 0.045 352 ± 0.045 484 ± 0.043 420 ± 0.039

0. 0. 0. 0.

0. 0. 0. 0.

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

R -I ± -- -- -- -- 480 ± 0.045 -- -- 670 ± 0.070 334 ± 0.039 -- 540 ± 0.030 -- -- -- -- 450 ± 0.060 520 ± 0.040 380 ± 0.036 570 ± 0.080 -- -- -- 680 ± 0.020 530 ± 0.020 650 ± 0.040 510 ± 0.040 520 ± 0.030 420 ± 0.060 590 ± 0.010 490 ± 0.010 325 ± 0.023 440 ± 0.041 463 ± 0.068 339 ± 0.067 451 ± 0.069 372 ± 0.065

V-J ± 1.930 ± 0.162 -- -- -- 1.160 ± 0.098 -- -- -- -- -- -- -- -- -- -- -- -- 1.040 ± 0.076 -- -- -- -- -- -- -- -- -- -- -- -- 1.199 ± 0.110 -- -- -- -- --

J-H ± -- -- -- -0.450 ± 0.197 1.280 ± 0.201 -- -- -- -- -- -- -- -- 0.540 ± 0.228 -- -- -- -0.510 ± 0.175 -- -- -- 0.660 ± 0.144 -- -- -- -- -- -- -- -- 0.294 ± 0.079 -- -- -- -- --

H- K ± -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 0.065 ± 0.094 -- -- -- -- --

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 9


Table A.1. continued. Object 5130-Ilioneus 5145-Pholus 5244-Amphilochos 5258-1989 AU1 5511-Cloanthus 6545-1986 TR6 6998-Tithonus 7066-Nessus 7352-1994 CO 8405-Asbolus 9030-1989 UX5 9430-Erichthonio 9818-Eurymachos 10199-Chariklo 10370-Hylonome 11089-1994 CS8 11351-1997 TS25 11488-1988 RM11 11663-1997 GO24 12917-1998 TG16 12921-1998 WZ5 13463-Antiphos 13862-1999 XT160 14707-2000 CC20 15094-1999 WB2 15502-1999 NV27 15535-2000 AT177 15760-1992 QB1 15788-1993 SB 15789-1993 SC 15807-1994 GV9 15809-1994 JS 15810-1994 JR1 15820-1994 TB 15836-1995 DA2 15874-1996 TL66 Class(1) J.Trojan Centaurs J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan Centaurs J.Trojan Centaurs J.Trojan J.Trojan J.Trojan Centaurs Centaurs J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan Classic Cold Res. 3:2 Res. 3:2 Classic Cold Res.(other) Res. 3:2 Res. 3:2 Res.(other) Scattered Epochs( 1 41 1 1 1 1 1 17 1 43 1 1 1 64 25 1 1 2 1 2 2 2 1 2 3 3 4 5 6 17 1 2 9 15 6 16
2)

M11 ± 9.656 ± 0.048 7.165 ± 0.076 -- -- 10.287 ± 0.047 10.219 ± 0.073 11.284 ± 0.059 9.054 ± 0.075 9.873 ± 0.056 8.999 ± 0.059 11.121 ± 0.047 11.306 ± 0.106 -- 6.508 ± 0.016 9.257 ± 0.159 10.681 ± 0.098 10.793 ± 0.076 11.524 ± 0.194 10.838 ± 0.052 11.388 ± 0.073 10.948 ± 0.073 11.083 ± 0.066 -- 11.410 ± 0.112 11.582 ± 0.118 9.943 ± 0.075 10.555 ± 0.075 6.979 ± 0.094 8.026 ± 0.143 6.740 ± 0.077 6.813 ± 0.091 7.479 ± 0.160 6.873 ± 0.079 7.499 ± 0.116 7.809 ± 0.091 5.208 ± 0.131

Gr t ± 9.188 ± 1.378 48.354 ± 1.930 3.187 ± 1.754 8.233 ± 1.590 10.774 ± 1.229 10.572 ± 1.962 8.155 ± 1.282 39.777 ± 3.448 4.815 ± 1.629 12.765 ± 1.370 11.783 ± 1.115 10.723 ± 3.060 -0.162 ± 1.824 13.595 ± 0.883 9.668 ± 6.478 4.732 ± 2.619 9.325 ± 2.033 6.507 ± 2.832 6.580 ± 1.438 11.839 ± 1.962 3.492 ± 1.876 7.093 ± 1.913 2.203 ± 1.754 4.232 ± 1.902 5.186 ± 2.495 7.368 ± 1.724 9.836 ± 2.098 27.538 ± 4.806 12.407 ± 4.044 34.698 ± 4.012 38.552 ± 0.000 28.194 ± 6.000 15.313 ± 4.751 37.669 ± 3.728 16.356 ± 5.630 1.451 ± 2.858

B -V ± 0.763 ± 0.034 1.261 ± 0.121 -- -- 0.906 ± 0.027 0.734 ± 0.041 0.787 ± 0.040 1.090 ± 0.040 0.713 ± 0.036 0.738 ± 0.038 0.887 ± 0.024 0.742 ± 0.079 0.673 ± 0.052 0.802 ± 0.049 0.690 ± 0.110 0.689 ± 0.073 0.739 ± 0.044 0.777 ± 0.110 0.837 ± 0.030 0.724 ± 0.042 0.673 ± 0.040 0.692 ± 0.045 -- 0.752 ± 0.041 0.652 ± 0.065 0.766 ± 0.047 0.739 ± 0.043 0.869 ± 0.143 0.802 ± 0.071 1.045 ± 0.117 -- -- 1.010 ± 0.180 1.107 ± 0.126 -- 0.687 ± 0.072

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

V-R ± 481 ± 0.026 788 ± 0.036 407 ± 0.044 466 ± 0.041 442 ± 0.027 499 ± 0.042 455 ± 0.032 763 ± 0.059 417 ± 0.034 508 ± 0.053 493 ± 0.027 488 ± 0.060 339 ± 0.046 491 ± 0.016 469 ± 0.154 423 ± 0.056 498 ± 0.044 436 ± 0.062 409 ± 0.030 537 ± 0.042 403 ± 0.047 449 ± 0.034 381 ± 0.044 412 ± 0.035 477 ± 0.065 445 ± 0.036 470 ± 0.049 707 ± 0.093 475 ± 0.077 688 ± 0.074 740 ± 0.099 760 ± 0.170 614 ± 0.114 697 ± 0.075 550 ± 0.110 369 ± 0.052

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

R -I ± 424 ± 0.046 822 ± 0.054 363 ± 0.064 425 ± 0.059 526 ± 0.042 436 ± 0.069 438 ± 0.046 689 ± 0.087 397 ± 0.056 505 ± 0.038 480 ± 0.039 456 ± 0.109 355 ± 0.067 520 ± 0.014 496 ± 0.189 384 ± 0.094 402 ± 0.072 420 ± 0.103 463 ± 0.049 410 ± 0.069 380 ± 0.068 412 ± 0.066 370 ± 0.064 385 ± 0.067 322 ± 0.094 430 ± 0.060 461 ± 0.082 651 ± 0.166 514 ± 0.114 697 ± 0.093 -- 480 ± 0.149 538 ± 0.098 739 ± 0.099 500 ± 0.160 370 ± 0.077

2.

2. 1.

1. 1.

1. 1. 1. 1. 1. 2.

2. 1.

V-J ± -- 612 ± 0.048 -- -- -- -- -- 290 ± 0.040 -- 654 ± 0.048 -- -- -- 685 ± 0.110 310 ± 0.100 -- -- -- -- 707 ± 0.066 -- 417 ± 0.048 -- -- 401 ± 0.066 565 ± 0.046 681 ± 0.045 -- -- 236 ± 0.200 -- -- -- 368 ± 0.162 -- 452 ± 0.114

0.

0. 0.

0. 0.

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

J-H ± -- 391 ± 0.047 -- -- -- -- -- 309 ± 0.268 -- 386 ± 0.103 -- -- -- 414 ± 0.046 180 ± 0.085 -- -- -- -- 475 ± 0.086 -- 343 ± 0.055 -- -- 342 ± 0.062 492 ± 0.041 500 ± 0.048 -- 450 ± 0.253 412 ± 0.240 -- 460 ± 0.705 430 ± 0.242 428 ± 0.119 -- 267 ± 0.144

H- K ± -- -0.037 ± 0.047 -- -- -- -- -- -0.089 ± 0.385 -- 0.170 ± 0.171 -- -- -- 0.097 ± 0.048 0.270 ± 0.092 -- -- -- -- 0.205 ± 0.081 -- 0.103 ± 0.052 -- -- 0.095 ± 0.058 0.152 ± 0.034 0.123 ± 0.047 -- -- -0.040 ± 0.197 -- -- -- 0.120 ± 0.120 -- -0.018 ± 0.138

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 10


Table A.1. continued. Object 158751588315977166841741618060181371826818493189401925519299193081952120000201082016120738235492369424233243412438024390244202442624444244522446724835249522497825347261812630826308Class(1) Res. 3:2 Classic Hot J.Trojan Classic Cold J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan Classic Cold Res. 3:2 Classic Hot Classic Hot Classic Hot Res. 3:2 Res.(other) J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan J.Trojan Classic Hot Res. 3:2 Classic Cold J.Trojan Res.(other) Res.(other) Res.(other) Epochs( 7 3 1 8 1 1 1 1 2 1 4 5 16 13 8 3 1 2 1 1 1 1 1 2 1 1 1 1 1 10 4 2 1 8 8 1
2)

1996 TP66 1997 CR29 1998 MA11 1994 JQ1 1988 RR10 1999 XJ156 2000 OU30 Dardanos Demoleon 2000 QV49 1994 VK8 1996 SZ4 1996 TO66 Chaos Varuna 1995 QZ9 1996 TR66 1999 XG191 Epicles 1997 KZ3 1999 XD94 2000 AJ87 2000 AA160 2000 AD177 2000 BU22 2000 CR12 2000 OP32 2000 QU167 2000 SS165 1995 SM55 1997 QJ4 1998 HJ151 1999 RQ116 1996 GQ21 1998 SM165 1998 SM165

+B

M11 ± 6.958 ± 0.076 7.076 ± 0.135 10.610 ± 0.046 6.646 ± 0.113 12.739 ± 0.097 -- 11.131 ± 0.057 12.080 ± 0.070 10.813 ± 0.083 11.615 ± 0.097 7.016 ± 0.163 8.330 ± 0.166 4.520 ± 0.042 4.503 ± 0.090 3.455 ± 0.090 7.889 ± 0.399 -- 11.536 ± 0.073 11.812 ± 0.118 11.340 ± 0.053 11.433 ± 0.071 12.013 ± 0.067 -- 11.595 ± 0.066 -- -- 11.395 ± 0.093 11.776 ± 0.099 11.800 ± 0.104 4.332 ± 0.040 7.622 ± 0.194 7.008 ± 0.050 11.545 ± 0.075 4.796 ± 0.051 5.549 ± 0.107 --

Gr t ± 30.636 ± 3.598 20.484 ± 7.048 8.770 ± 1.049 31.346 ± 4.713 12.134 ± 2.732 3.456 ± 1.719 9.115 ± 1.218 12.538 ± 1.495 3.154 ± 2.460 8.449 ± 2.608 24.540 ± 5.861 13.725 ± 4.694 2.077 ± 2.168 23.292 ± 2.396 26.843 ± 1.917 14.511 ± 3.460 -- 10.132 ± 1.962 7.916 ± 2.720 8.337 ± 1.151 9.103 ± 1.978 2.026 ± 1.928 1.556 ± 1.804 12.512 ± 1.913 2.931 ± 1.742 5.604 ± 1.660 6.264 ± 2.536 6.333 ± 2.377 11.221 ± 2.463 0.272 ± 1.805 4.696 ± 4.772 29.628 ± 2.427 10.900 ± 2.252 37.628 ± 1.969 31.425 ± 2.295 31.037 ± 0.000

1. 0. 0. 1. 0. 0. 0. 0. 0. 0. 1. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 1. 0. 1. 0.

B -V ± 031 ± 0.112 750 ± 0.152 748 ± 0.033 134 ± 0.068 742 ± 0.071 758 ± 0.056 733 ± 0.039 795 ± 0.042 703 ± 0.073 709 ± 0.072 010 ± 0.060 754 ± 0.100 671 ± 0.057 932 ± 0.054 906 ± 0.052 880 ± 0.040 -- 776 ± 0.041 800 ± 0.071 723 ± 0.035 704 ± 0.051 713 ± 0.043 734 ± 0.055 700 ± 0.042 937 ± 0.066 717 ± 0.054 712 ± 0.071 872 ± 0.056 927 ± 0.079 652 ± 0.032 763 ± 0.114 110 ± 0.030 618 ± 0.058 011 ± 0.068 989 ± 0.114 --

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

V-R ± 655 ± 0.076 538 ± 0.157 465 ± 0.025 736 ± 0.101 488 ± 0.055 412 ± 0.043 496 ± 0.031 529 ± 0.040 395 ± 0.047 465 ± 0.055 659 ± 0.095 522 ± 0.061 389 ± 0.043 608 ± 0.041 637 ± 0.040 515 ± 0.050 -- 472 ± 0.042 485 ± 0.068 474 ± 0.029 481 ± 0.037 369 ± 0.035 391 ± 0.048 513 ± 0.034 441 ± 0.042 414 ± 0.043 437 ± 0.053 441 ± 0.056 460 ± 0.060 357 ± 0.043 431 ± 0.114 710 ± 0.030 488 ± 0.042 726 ± 0.043 641 ± 0.056 --

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

R -I ± 673 ± 0.086 620 ± 0.182 441 ± 0.036 650 ± 0.123 498 ± 0.097 364 ± 0.063 409 ± 0.044 451 ± 0.056 380 ± 0.087 429 ± 0.093 490 ± 0.255 446 ± 0.154 356 ± 0.053 571 ± 0.087 628 ± 0.040 -- -- 467 ± 0.069 387 ± 0.101 418 ± 0.041 418 ± 0.069 390 ± 0.067 336 ± 0.068 462 ± 0.066 304 ± 0.063 424 ± 0.062 409 ± 0.090 406 ± 0.087 513 ± 0.091 356 ± 0.052 396 ± 0.102 -- 461 ± 0.079 694 ± 0.056 666 ± 0.072 --

V-J ± 2.309 ± 0.060 -- -- -- -- -- -- -- 1.383 ± 0.045 -- -- -- 0.997 ± 0.101 1.835 ± 0.087 2.010 ± 0.050 -- -- 1.593 ± 0.062 -- 1.657 ± 0.033 -- -- -- 1.684 ± 0.048 -- -- -- -- -- 1.010 ± 0.050 -- -- -- 2.438 ± 0.062 2.295 ± 0.087 --

J-H ± 0.170 ± 0.078 0.490 ± 0.320 -- -- -- -- -- -- 0.384 ± 0.046 -- 0.520 ± 0.297 -- -- 0.400 ± 0.095 0.564 ± 0.070 -- 0.470 ± 0.296 0.520 ± 0.084 -- 0.493 ± 0.033 -- -- -- 0.461 ± 0.055 -- -- -- -- -- -0.270 ± 0.163 -- -- -- 0.497 ± 0.082 0.546 ± 0.086 --

H- K ± 0.020 ± 0.092 -- -- -- -- -- -- -- 0.091 ± 0.040 -- -- -- -- 0.033 ± 0.094 -0.038 ± 0.105 -- -- 0.113 ± 0.081 -- 0.211 ± 0.028 -- -- -- 0.140 ± 0.052 -- -- -- -- -- -- -- -- -- 0.055 ± 0.096 0.080 ± 0.071 --

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 11


Table A.1. continued. Object 263752895828978299813069831820318213182432430325323261532794329293300133128333403478535671380833808438628392854031442301423554235543212445944580247171471714793247967482494825248639Class(1) Res.(other) J.Trojan Res. 3:2 Scattered J.Trojan J.Trojan J.Trojan Centaurs J.Trojan Centaurs J.Trojan J.Trojan Classic Cold Classic Cold Scattered Res. 3:2 J.Trojan Classic Cold Classic Hot Res.(other) Res. 3:2 J.Trojan Scattered Res.(other) Scattered Scattered J.Trojan Scattered Classic Cold Res. 3:2 Res. 3:2 Res. 3:2 J.Trojan J.Trojan J.Trojan Scattered Epochs( 13 1 8 18 3 1 1 14 1 221 1 1 5 6 9 12 1 6 1 3 58 1 5 6 12 1 1 30 2 23 1 13 1 1 1 4
2)

1999 DE9 2001 CQ42 Ixion 1999 TD10 Hippokoon 1999 RT186 1999 RK225 Elatus 2000 RQ83 Thereus 2001 QU277 1989 UE5 1995 QY9 1997 CU29 1998 BU48 1998 VG44 2001 RG87 1998 SN165 Rhadamanth 1999 HB12 Huya 2001 BP75 1999 KR16 2001 UR163 Typhon Typhon+B 2000 AL113 1999 OX3 2000 PV29 1999 TC36 1999 TC36+ B 2000 GN171 2000 SL298 2001 SY345 2001 TL212 1995 TL8

M11 ± 4.809 ± 0.045 -- 3.429 ± 0.050 8.693 ± 0.039 11.977 ± 0.125 12.450 ± 0.168 11.849 ± 0.173 10.462 ± 0.122 12.293 ± 0.074 9.218 ± 0.015 11.405 ± 0.050 12.744 ± 0.094 7.365 ± 0.062 6.216 ± 0.104 6.861 ± 0.137 6.322 ± 0.073 12.513 ± 0.076 5.679 ± 0.320 7.430 ± 0.063 6.632 ± 0.079 4.678 ± 0.099 -- 5.612 ± 0.092 3.799 ± 0.102 7.252 ± 0.054 -- -- 7.052 ± 0.085 -- 4.858 ± 0.060 -- 6.183 ± 0.045 11.843 ± 0.113 12.550 ± 0.072 12.719 ± 0.153 4.664 ± 0.087

Gr t ± 20.625 ± 1.625 -2.591 ± 1.987 22.481 ± 2.259 12.194 ± 1.263 7.486 ± 2.170 10.495 ± 4.232 8.202 ± 3.877 27.348 ± 1.859 8.679 ± 1.818 10.537 ± 1.186 9.346 ± 1.235 6.794 ± 2.116 18.741 ±10.170 28.823 ± 3.429 26.535 ± 4.487 20.986 ± 3.166 4.113 ± 1.599 6.857 ± 3.068 11.286 ± 3.072 15.815 ± 3.668 22.400 ± 2.192 -0.195 ± 1.869 42.033 ± 2.385 44.811 ± 2.993 12.657 ± 1.354 9.763 ± 0.000 2.314 ± 1.748 34.216 ± 2.104 -- 29.334 ± 1.738 19.177 ± 0.000 26.540 ± 1.817 11.415 ± 2.726 11.716 ± 1.707 8.694 ± 3.314 22.529 ± 6.004

0. 0. 1. 0. 0. 0. 0. 1. 0. 0. 0. 0. 0. 1. 1. 0. 0. 0. 0. 0. 0. 0. 1. 1. 0. 1. 1. 0. 0. 0. 0. 1.

B -V ± 967 ± 0.043 730 ± 0.054 009 ± 0.051 808 ± 0.095 715 ± 0.067 889 ± 0.093 980 ± 0.111 020 ± 0.060 772 ± 0.038 763 ± 0.072 807 ± 0.052 923 ± 0.065 740 ± 0.200 157 ± 0.145 044 ± 0.071 930 ± 0.055 728 ± 0.050 712 ± 0.095 650 ± 0.085 893 ± 0.064 963 ± 0.042 810 ± 0.059 123 ± 0.083 290 ± 0.109 758 ± 0.039 -- -- 138 ± 0.067 -- 029 ± 0.047 -- 924 ± 0.059 899 ± 0.058 758 ± 0.050 949 ± 0.100 008 ± 0.159

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

V-R ± 579 ± 0.036 364 ± 0.045 610 ± 0.030 502 ± 0.032 458 ± 0.048 520 ± 0.091 440 ± 0.097 620 ± 0.048 474 ± 0.045 501 ± 0.016 452 ± 0.028 393 ± 0.056 561 ± 0.110 645 ± 0.066 631 ± 0.101 573 ± 0.047 386 ± 0.043 444 ± 0.078 527 ± 0.069 544 ± 0.065 609 ± 0.090 381 ± 0.044 738 ± 0.057 840 ± 0.048 525 ± 0.022 -- 402 ± 0.043 705 ± 0.056 -- 693 ± 0.032 -- 622 ± 0.038 489 ± 0.069 530 ± 0.037 467 ± 0.093 621 ± 0.091

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

R -I ± 568 ± 0.043 230 ± 0.071 580 ± 0.040 511 ± 0.051 412 ± 0.079 396 ± 0.153 461 ± 0.145 630 ± 0.038 425 ± 0.067 488 ± 0.036 474 ± 0.043 486 ± 0.080 -- 634 ± 0.092 644 ± 0.104 598 ± 0.098 419 ± 0.060 437 ± 0.083 412 ± 0.075 481 ± 0.094 593 ± 0.055 291 ± 0.067 750 ± 0.040 673 ± 0.121 414 ± 0.053 -- 343 ± 0.064 642 ± 0.066 -- 619 ± 0.049 -- 617 ± 0.054 476 ± 0.102 420 ± 0.060 436 ± 0.129 551 ± 0.120

V-J ± 1.717 ± 0.193 -- 1.590 ± 0.064 1.790 ± 0.057 1.527 ± 0.074 -- -- -- -- 1.350 ± 0.050 -- -- 2.027 ± 0.201 -- 2.275 ± 0.059 -- -- 1.270 ± 0.050 -- -- 1.970 ± 0.050 -- -- 2.381 ± 0.058 1.560 ± 0.045 -- -- 2.217 ± 0.127 -- 2.215 ± 0.101 -- 1.711 ± 0.079 -- -- -- 2.420 ± 0.050

J-H ± 0.327 ± 0.106 -- 0.277 ± 0.069 0.425 ± 0.093 0.396 ± 0.080 -- -- 0.392 ± 0.062 -- 0.442 ± 0.074 -- -- -- 0.410 ± 0.238 0.505 ± 0.098 0.398 ± 0.128 -- -- -- -- 0.330 ± 0.109 -- 0.560 ± 0.071 0.476 ± 0.115 0.406 ± 0.087 -- -- 0.399 ± 0.105 0.428 ± 0.291 0.337 ± 0.092 -- 0.365 ± 0.108 -- -- -- 0.412 ± 0.131

H- K ± 0.025 ± 0.108 -- -0.010 ± 0.071 -- 0.183 ± 0.069 -- -- 0.020 ± 0.086 -- 0.110 ± 0.074 -- -- -- -- -0.157 ± 0.105 0.010 ± 0.078 -- -- -- -- -- -- 0.020 ± 0.071 -- 0.160 ± 0.071 -- -- -0.023 ± 0.090 -- 0.009 ± 0.090 -- 0.060 ± 0.099 -- -- -- -0.020 ± 0.085

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 12


Table A.1. continued. Object 490365000051359527475287252975534695452054598555655557655636556375563856968585345853459358604546045860458605586060860620606216325265150652256548965489664526665266652699866998769988Class(1) Centaurs Classic Hot J.Trojan Classic Cold Centaurs Centaurs J.Trojan Scattered Centaurs Classic Hot Centaurs Classic Hot Classic Hot Res. 3:2 J.Trojan Classic Cold Classic Cold Scattered Classic Cold Detached Detached Centaurs Scattered Res.(other) Res.(other) Centaurs J.Trojan J.Trojan Scattered Scattered Classic Cold Classic Cold Classic Cold Res. 3:2 Classic Cold Res.(other) Epochs( 3 4 1 1 18 9 1 1 15 9 19 8 8 2 1 7 1 1 2 2 1 8 3 3 3 10 1 1 3 1 3 7 1 3 1 2
2)

Pelion Quaoar 2000 SC17 1998 HM151 Okyrhoe Cyllarus 2000 AX8 2000 PJ30 Bienor 2002 AW197 Amycus 2002 TX300 2002 UX25 2002 VE95 2000 SA92 Logos Logos+B 1999 CL158 2000 CH105 2000 CM114 2000 CM114+ Echeclus 2000 EE173 2000 FD8 2000 FE8 2001 BL41 2002 CA126 2002 EK44 Ceto Ceto+B 1999 OF4 Borasisi Borasisi+B 1998 WW24 1998 WA25 1998 WA31

B

M11 ± 10.420 ± 0.247 2.220 ± 0.029 11.985 ± 0.233 7.417 ± 0.100 10.768 ± 0.093 8.634 ± 0.100 -- -- 7.573 ± 0.104 3.087 ± 0.038 7.774 ± 0.047 3.237 ± 0.043 3.497 ± 0.020 -- 11.534 ± 0.059 6.758 ± 0.181 -- 6.653 ± 0.090 6.376 ± 0.093 6.972 ± 0.040 -- 9.555 ± 0.155 8.147 ± 0.180 6.507 ± 0.221 6.510 ± 0.062 11.278 ± 0.063 -- -- 6.286 ± 0.041 -- 6.323 ± 0.080 5.418 ± 0.056 -- 7.963 ± 0.085 -- 7.352 ± 0.122

Gr t ± 8.735 ± 3.519 29.224 ± 1.706 7.745 ± 5.725 24.891 ± 4.691 10.846 ± 2.450 32.286 ± 3.654 0.771 ± 1.818 -- 8.793 ± 2.427 22.129 ± 1.429 33.885 ± 1.517 -0.195 ± 1.513 15.518 ± 1.290 36.638 ± 2.876 13.013 ± 1.374 26.351 ± 4.789 17.578 ± 0.000 5.546 ± 2.064 25.350 ± 3.158 11.545 ± 1.858 13.041 ± 0.000 10.399 ± 3.404 13.198 ± 1.827 30.813 ± 3.016 11.433 ± 1.500 13.807 ± 2.421 3.241 ± 1.724 1.982 ± 1.783 15.666 ± 0.871 13.527 ± 0.000 26.708 ± 3.878 33.830 ± 2.714 41.482 ± 0.000 17.966 ± 2.895 17.056 ± 0.000 13.652 ± 6.704

0. 0. 0. 0. 0. 1. 0. 0. 0. 1. 0. 1. 1. 0. 0. 0. 1. 0. 0. 0. 1. 0. 0. 0. 0. 0. 1. 0. 0. 0.

B -V ± 746 ± 0.080 958 ± 0.035 864 ± 0.201 930 ± 0.090 743 ± 0.065 096 ± 0.095 663 ± 0.051 -- 711 ± 0.059 913 ± 0.041 112 ± 0.041 679 ± 0.038 007 ± 0.043 127 ± 0.074 986 ± 0.040 990 ± 0.127 -- 800 ± 0.060 019 ± 0.086 730 ± 0.020 -- 854 ± 0.081 665 ± 0.032 151 ± 0.110 750 ± 0.024 718 ± 0.049 651 ± 0.051 693 ± 0.052 860 ± 0.030 -- 032 ± 0.106 820 ± 0.170 -- 756 ± 0.112 -- 786 ± 0.129

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

V-R ± 556 ± 0.078 650 ± 0.020 447 ± 0.131 620 ± 0.050 486 ± 0.061 680 ± 0.085 356 ± 0.045 -- 476 ± 0.046 602 ± 0.031 702 ± 0.030 359 ± 0.024 540 ± 0.030 -- 494 ± 0.033 729 ± 0.120 -- 390 ± 0.040 643 ± 0.096 500 ± 0.020 -- 465 ± 0.076 488 ± 0.029 664 ± 0.078 480 ± 0.020 509 ± 0.044 377 ± 0.044 401 ± 0.044 560 ± 0.030 -- 673 ± 0.083 646 ± 0.058 -- 463 ± 0.081 -- 492 ± 0.133

R -I ± 0.368 ± 0.102 0.610 ± 0.028 0.438 ± 0.210 -- 0.474 ± 0.070 0.669 ± 0.090 0.361 ± 0.067 -- 0.400 ± 0.079 0.581 ± 0.037 0.668 ± 0.039 0.323 ± 0.041 -- -- 0.509 ± 0.049 0.602 ± 0.119 -- 0.470 ± 0.060 0.583 ± 0.095 -- -- 0.486 ± 0.095 0.543 ± 0.056 0.648 ± 0.070 0.500 ± 0.050 0.381 ± 0.160 0.407 ± 0.064 0.334 ± 0.065 -- -- 0.601 ± 0.080 0.647 ± 0.062 -- 0.659 ± 0.104 -- 0.530 ± 0.183

2.

2. 1. 1.

2.

1.

2.

V-J ± -- 180 ± 0.058 -- -- -- 425 ± 0.077 -- -- 684 ± 0.091 740 ± 0.054 -- -- -- 220 ± 0.057 -- -- -- -- -- -- -- 480 ± 0.072 -- -- -- -- -- -- -- -- -- 010 ± 0.067 -- -- -- --

0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

0. 0. 0.

0. 0.

J-H ± -- 360 ± 0.050 -- -- 457 ± 0.068 450 ± 0.092 -- 410 ± 0.304 379 ± 0.078 329 ± 0.070 299 ± 0.077 -- 404 ± 0.049 400 ± 0.057 -- 498 ± 0.340 -- -- -- -- -- 466 ± 0.125 -- -- 470 ± 0.277 365 ± 0.071 -- -- -- -- 380 ± 0.253 457 ± 0.162 -- -- -- --

H- K ± -- 0.030 ± 0.057 -- -- 0.159 ± 0.080 -0.100 ± 0.085 -- -- 0.153 ± 0.099 0.215 ± 0.094 0.004 ± 0.064 -- -- 0.020 ± 0.064 -- -- -- -- -- -- -- 0.340 ± 0.083 -- -- -- 0.255 ± 0.101 -- -- -- -- -- 0.100 ± 0.094 -- -- -- --

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 13


Table A.1. continued. Object 69990-1998 WU31 73480-2002 PN34 76804-2000 QE 79360-1997 CS29 79360-1997 CS29+ B 79978-1999 CC158 79983-1999 DF9 80806-2000 CM105 82075-2000 YW134 82155-2001 FZ173 82158-2001 FP185 83982-Crantor 84522-2002 TC302 84709-2002 VW120 85627-1998 HP151 85633-1998 KR65 86047-1999 OY3 86177-1999 RY215 87269-2000 OO67 87555-2000 QB243 88269-2001 KF77 88611-Teharonhia 88611-Teharonhia+B 90377-Sedna 90482-Orcus 90568-2004 GV9 91133-1998 HK151 91205-1998 US43 91554-1999 RZ215 95626-2002 GZ32 99328-2001 UY123 105685-2000 SC51 111113-2001 VK85 118228-1996 TQ66 118379-1999 HC12 118702-2000 OM67 Class(1) Res. 3:2 Scattered J.Trojan Classic Cold Classic Cold Res.(other) Classic Hot Classic Cold Res.(other) Scattered Scattered Centaurs Res.(other) J.Trojan Classic Cold Classic Cold Classic Hot Classic Hot Scattered Scattered Centaurs Classic Cold Classic Cold Detached Res. 3:2 Classic Hot Res. 3:2 Res. 3:2 Scattered Centaurs J.Trojan J.Trojan J.Trojan Res. 3:2 Classic Hot Detached Epochs( 1 10 1 15 1 2 1 2 14 9 7 17 2 1 1 4 5 3 3 6 1 1 1 3 6 2 6 2 1 18 1 1 1 7 3 1
2)

M11 ± 8.204 ± 0.073 8.506 ± 0.030 12.095 ± 0.135 4.990 ± 0.060 -- 5.355 ± 0.097 5.797 ± 0.110 -- 4.382 ± 0.046 5.813 ± 0.024 5.947 ± 0.054 8.662 ± 0.056 3.719 ± 0.020 12.446 ± 0.158 -- 6.596 ± 0.206 6.396 ± 0.147 7.429 ± 0.077 9.027 ± 0.155 8.437 ± 0.129 10.038 ± 0.020 -- -- 1.077 ± 0.065 1.982 ± 0.099 -- 6.940 ± 0.075 7.851 ± 0.078 8.069 ± 0.079 6.733 ± 0.156 12.610 ± 0.103 12.721 ± 0.097 12.760 ± 0.086 7.245 ± 0.195 7.856 ± 0.125 7.075 ± 0.030

Gr t ± 23.278 ± 3.272 12.613 ± 1.134 7.871 ± 2.878 28.475 ± 2.382 31.690 ± 0.000 24.869 ± 2.974 33.944 ± 2.164 32.348 ± 0.000 16.483 ± 2.187 15.975 ± 1.446 16.009 ± 2.281 39.225 ± 1.992 28.979 ± 1.356 12.795 ± 3.419 25.429 ± 0.000 30.583 ± 2.821 -3.527 ± 2.148 3.839 ± 3.476 26.481 ± 2.592 5.554 ± 5.948 37.355 ± 1.301 5.020 ± 0.000 4.612 ± 0.000 32.954 ± 2.972 2.761 ± 1.831 20.819 ± 1.099 9.775 ± 2.589 4.463 ± 3.403 19.081 ± 3.401 16.992 ± 2.947 12.496 ± 2.292 8.131 ± 2.099 13.245 ± 1.864 38.250 ± 4.976 12.620 ± 6.899 14.444 ± 1.982

0. 0. 0. 1. 0. 0. 0. 0. 0. 1. 1. 0. 1. 0. 0. 1. 0. 1. 1. 0. 0. 0. 0. 0. 0. 0. 1. 0. 1. 0. 0.

B -V ± 720 ± 0.089 818 ± 0.095 803 ± 0.082 055 ± 0.079 -- 996 ± 0.066 920 ± 0.060 -- 922 ± 0.053 864 ± 0.023 820 ± 0.048 105 ± 0.042 120 ± 0.028 855 ± 0.087 -- 095 ± 0.080 726 ± 0.037 719 ± 0.123 080 ± 0.092 763 ± 0.086 080 ± 0.040 -- -- 131 ± 0.079 664 ± 0.041 843 ± 0.028 645 ± 0.121 691 ± 0.102 771 ± 0.097 674 ± 0.043 890 ± 0.058 016 ± 0.055 822 ± 0.063 186 ± 0.118 894 ± 0.163 820 ± 0.057

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

V-R ± 505 ± 0.086 520 ± 0.020 446 ± 0.070 666 ± 0.054 -- 611 ± 0.052 710 ± 0.050 -- 503 ± 0.052 546 ± 0.026 572 ± 0.038 761 ± 0.039 640 ± 0.020 462 ± 0.090 -- 628 ± 0.066 345 ± 0.046 358 ± 0.090 654 ± 0.081 383 ± 0.083 730 ± 0.010 -- -- 686 ± 0.077 370 ± 0.039 -- 520 ± 0.062 446 ± 0.095 575 ± 0.090 576 ± 0.054 537 ± 0.056 444 ± 0.059 462 ± 0.048 670 ± 0.096 490 ± 0.138 470 ± 0.040

R -I ± 0.722 ± 0.087 -- 0.443 ± 0.106 0.609 ± 0.057 -- 0.619 ± 0.075 0.650 ± 0.060 -- 0.581 ± 0.059 0.508 ± 0.036 0.458 ± 0.078 0.667 ± 0.055 0.660 ± 0.020 0.548 ± 0.130 -- 0.790 ± 0.081 0.277 ± 0.076 0.631 ± 0.185 0.593 ± 0.055 0.729 ± 0.198 -- -- -- 0.657 ± 0.067 0.390 ± 0.045 -- 0.390 ± 0.061 0.347 ± 0.094 0.539 ± 0.091 0.538 ± 0.067 0.434 ± 0.084 0.452 ± 0.081 0.558 ± 0.069 0.746 ± 0.113 0.343 ± 0.125 0.590 ± 0.040

2.

1.

2. 1. 1. 1.

2.

V-J ± -- -- -- 073 ± 0.134 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 480 ± 0.108 -- -- -- 320 ± 0.060 070 ± 0.042 570 ± 0.058 570 ± 0.092 -- -- -- -- -- -- 435 ± 0.128 -- --

J-H ± -- 0.425 ± 0.105 -- 0.356 ± 0.150 -- -- -- 0.360 ± 0.256 0.358 ± 0.153 0.171 ± 0.118 -- 0.380 ± 0.067 -- -- -- -- -0.380 ± 0.256 0.470 ± 0.286 -- 0.592 ± 0.152 -- -- -- 0.290 ± 0.222 0.120 ± 0.051 0.340 ± 0.094 -- -- -- 0.442 ± 0.113 -- -- -- -- 0.490 ± 0.298 --

H- K ± -- -- -- 0.104 ± 0.176 -- -- -- -- -- -- -- -0.140 ± 0.064 -- -- -- -- -- -- -- -- -- -- -- 0.050 ± 0.314 0.053 ± 0.055 0.140 ± 0.094 -- -- -- -- -- -- -- -- -- --

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 14


Table A.1. continued. Object 119068119070119315119951119979120061120132120178120347120347120348120453121725123509123509124729127546129772130391131695134340134340134340134340134860134860135182136108136199136472137294137295138537144897145451145452Class(1) Res.(other) Res.(other) Centaurs Classic Cold Res.(other) Centaurs Detached Classic Hot Classic Hot Classic Hot Res. 3:2 J.Trojan Centaurs Classic Cold Classic Cold J.Trojan Scattered Classic Cold Res.(other) Res.(other) Res. 3:2 Res. 3:2 Res. 3:2 Res. 3:2 Classic Cold Classic Cold Classic Cold Classic Hot Detached Classic Hot Classic Cold Res.(other) Classic Cold Res. 3:2 Scattered Classic Hot Epochs( 1 1 1 3 1 11 3 1 1 1 1 1 10 1 1 1 1 1 1 1 4 1 1 1 5 1 1 3 64 1 3 1 5 1 2 2
2)

2001 KC77 2001 KP77 2001 SQ73 2002 KX14 2002 WC19 2003 CO1 2003 FY128 2003 OP32 Salacia Salacia+B 2004 TY364 1988 RE12 1999 XX143 2000 WK183 2000 WK183 2001 SB173 2002 XU93 1999 HR11 2000 JG81 2001 XS254 Pluto Pluto+B Pluto+C Pluto+D 2000 OJ67 2000 OJ67+ B 2001 QT322 Haumea E ri s Makemake 1999 RE215 1999 RB216 2000 OK67 2004 UX10 2005 RM43 2005 RN43

+B

M11 ± 6.822 ± 0.030 -- 8.885 ± 0.030 -- -- 9.208 ± 0.040 4.476 ± 0.010 -- -- -- -- 13.202 ± 0.189 8.522 ± 0.123 -- -- 12.556 ± 0.107 7.943 ± 0.010 -- 7.755 ± 0.115 -- -0.881 ± 0.400 -- -- -- 6.001 ± 0.120 -- -- 0.217 ± 0.030 -1.462 ± 0.036 -- 6.415 ± 0.187 7.670 ± 0.087 6.082 ± 0.083 -- -- --

Gr t ± 18.607 ± 1.301 -- 8.875 ± 1.301 26.057 ± 1.557 28.487 ± 0.000 11.701 ± 2.057 21.441 ± 1.266 3.135 ± 2.090 7.116 ± 0.000 7.982 ± 0.000 28.425 ± 3.958 6.453 ± 3.884 30.600 ± 5.205 29.751 ± 0.000 26.029 ± 0.000 10.320 ± 2.774 5.447 ± 1.087 28.264 ± 4.298 3.743 ± 4.431 -- 7.607 ± 0.681 3.334 ± 0.000 -2.234 ± 0.000 18.074 ± 0.000 26.378 ± 3.102 33.683 ± 0.000 15.584 ±11.076 -0.010 ± 0.850 3.866 ± 0.823 4.693 ± 0.900 30.557 ± 3.448 14.468 ± 2.704 20.354 ± 3.262 20.664 ± 2.909 1.330 ± 1.474 16.523 ±-9.000

B -V ± 0.910 ± 0.010 -- 0.670 ± 0.020 1.050 ± 0.030 -- 0.740 ± 0.030 1.050 ± 0.028 0.698 ± 0.052 -- -- 1.059 ± 0.089 0.826 ± 0.132 1.060 ± 0.089 -- -- 0.992 ± 0.060 0.760 ± 0.028 0.920 ± 0.120 -- -- 0.867 ± 0.016 0.710 ± 0.002 0.644 ± 0.028 0.907 ± 0.031 1.050 ± 0.060 -- 0.710 ± 0.060 0.631 ± 0.025 0.805 ± 0.015 0.828 ± 0.022 1.003 ± 0.130 0.897 ± 0.122 0.821 ± 0.123 0.950 ± 0.020 0.590 ± 0.038 --

V-R ± 0.560 ± 0.010 -- 0.460 ± 0.010 0.610 ± 0.020 -- 0.490 ± 0.020 0.600 ± 0.020 -- -- -- -- 0.388 ± 0.108 0.648 ± 0.116 -- -- 0.503 ± 0.064 0.440 ± 0.020 0.530 ± 0.100 0.370 ± 0.128 -- 0.515 ± 0.035 -- -- -- 0.670 ± 0.050 -- 0.530 ± 0.120 0.370 ± 0.020 0.389 ± 0.049 -- 0.710 ± 0.074 0.522 ± 0.073 0.583 ± 0.072 0.580 ± 0.030 -- --

0.

0. 0. 0. 0. 0. 0. 0.

0. 0. 0. 0. 0. 0.

R -I ± -- -- -- -- -- -- 550 ± 0.030 -- -- -- -- 483 ± 0.151 679 ± 0.123 -- -- 424 ± 0.101 380 ± 0.020 800 ± 0.070 430 ± 0.134 -- 400 ± 0.010 -- -- -- 600 ± 0.070 -- -- 320 ± 0.020 363 ± 0.061 -- 571 ± 0.089 506 ± 0.061 524 ± 0.079 -- -- --

1.

1. 0.

2. 0. 1.

V-J ± -- -- -- -- -- -- 640 ± 0.058 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 051 ± 0.020 849 ± 0.108 -- -- -- 421 ± 0.088 -- 910 ± 0.067 550 ± 0.058

J-H ± -- 0.370 ± 0.235 -- -- -- 0.326 ± 0.091 0.360 ± 0.078 -- -- -- -- -- -- -- -- -- -- -- -- 0.420 ± 0.260 -- -- -- -- 0.305 ± 0.162 -- -- -0.044 ± 0.037 0.080 ± 0.072 -- -- -- 0.455 ± 0.145 -- 0.200 ± 0.085 0.310 ± 0.071

H- K ± -- -- -- -- -- -- 0.110 ± 0.085 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 0.070 ± 0.139 -- -- -0.111 ± 0.048 -0.280 ± 0.085 -- -- -- 0.040 ± 0.078 -- 0.280 ± 0.092 0.190 ± 0.071

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 15


Table A.1. continued. Object 145453145480148209148780148780150642163135163216168700168703181708181855181867181871181874181902182397182933192388192929208996Class(1) Classic Hot Detached Detached Classic Hot Classic Hot Classic Hot J.Trojan J.Trojan Res. 3:2 Classic Cold Classic Hot Classic Hot Res.(other) Classic Cold Detached Detached Classic Hot Detached J.Trojan J.Trojan Res. 3:2 Epochs( 3 1 3 1 1 1 1 1 1 5 8 3 1 1 2 2 1 1 1 1 9
2)

2005 2005 2000 Al t j i r Al t j i r 2001 2002 2002 2000 2000 1993 1998 1999 1999 1999 1999 2001 2002 1996 2000 2003

R R 43 T B 190 C R 105 a a+B C Z 31 C T 22 E N6 8 GE 1 4 7 GP 1 8 3 FW W T 31 C V1 1 8 C O1 5 3 HW 1 1 R D2 1 5 QW 2 9 7 GZ 3 1 R D2 9 AT44 AZ 8 4

4. 6.

8. 5. 6. 7. 7. 6. 7. 6.

3.

M11 ± -- 169 ± 0.020 228 ± 0.040 -- -- -- -- -- 002 ± 0.110 756 ± 0.060 527 ± 0.122 440 ± 0.088 186 ± 0.063 -- 672 ± 0.077 860 ± 0.079 660 ± 0.050 -- -- -- 227 ± 0.050

Gr t ± 0.109 ± 3.025 18.632 ± 1.525 14.424 ± 3.398 29.751 ± 0.000 35.732 ± 0.000 -- 1.927 ± 1.789 4.392 ± 1.713 16.667 ± 3.950 8.353 ± 2.654 18.980 ± 3.484 10.112 ± 6.721 31.744 ± 2.469 38.554 ± 0.000 12.562 ± 2.766 7.547 ± 0.000 25.220 ± 3.210 33.013 ± 0.000 4.691 ± 1.684 -0.624 ± 1.876 23.884 ± 2.812

B -V ± 0.790 ± 0.076 0.980 ± 0.042 0.771 ± 0.082 -- -- -- 0.690 ± 0.053 -- -- 0.669 ± 0.074 1.023 ± 0.069 0.751 ± 0.144 -- -- 0.840 ± 0.042 -- 1.020 ± 0.099 -- 0.741 ± 0.055 0.707 ± 0.053 0.757 ± 0.146

0. 0.

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

V-R ± -- 560 ± 0.030 509 ± 0.048 -- -- -- 382 ± 0.045 443 ± 0.042 550 ± 0.120 445 ± 0.053 583 ± 0.070 502 ± 0.121 733 ± 0.067 -- 499 ± 0.073 -- 580 ± 0.070 -- 421 ± 0.042 354 ± 0.045 620 ± 0.030

0. 0.

0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0. 0.

R -I ± -- 550 ± 0.030 590 ± 0.090 -- -- -- 360 ± 0.066 347 ± 0.062 520 ± 0.114 463 ± 0.066 439 ± 0.104 416 ± 0.166 582 ± 0.062 -- 493 ± 0.083 498 ± 0.058 670 ± 0.060 -- 388 ± 0.062 318 ± 0.068 560 ± 0.042

V-J ± 1.020 ± 0.067 -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- -- 1.210 ± 0.054

0. 0.

0.

0.

J-H ± -- -- 410 ± 0.297 -- -- 550 ± 0.099 -- -- -- -- 400 ± 0.250 -- -- -- -- -- -- -- -- -- 188 ± 0.165

H- K ± -- -- -- -- -- 0.160 ± 0.099 -- -- -- -- -- -- -- -- -- -- -- -- -- -- 0.060 ± 0.071

O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 16


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 17

List of Objects
`C/1983 H1 IRAS-Araki-Alcock' on page 18 `C/1983 J1 Sugano-Saigusa-Fujikawa' on page 18 `C/1984 K1 Shoemaker' on page 18 `C/1984 U1 Shoemaker' on page 18 `C/1986 P1 Wilson' on page 18 `C/1987 A1 Levy' on page 18 `C/1987 H1 Shoemaker' on page 18 `C/1988 B1 Shoemaker' on page 18 `C/1988 C1 Maury-Phinney' on page 18 `C/1995 O1 Hale-Bopp' on page 18 `C/1996 B2 Hyakutake' on page 18 `C/1999 S4 LINEAR' on page 18 `C/2000 B4 LINEAR' on page 18 `C/2001 M10 NEAT' on page 18 `C/2001 OG108 LONEOS' on page 18 `P/1991 L3 Levy' on page 18 `P/1993 W1 Mueller' on page 18 `P/1994 A1 Kushida' on page 18 `P/1994 J3 Shoemaker' on page 18 `P/1995 A1 Jedicke' on page 18 `P/1996 A1 Jedicke' on page 18 `P/1997 C1 Gehrels' on page 18 `P/1997 G1 Montani' on page 18 `P/1997 V1 Larsen' on page 18 `P/1998 S1 LM' on page 18 `P/1999 D1 Hermann' on page 18 `P/1999 RO28 LONEOS' on page 18 `P/2004 A1' on page 18 `1P/Halley' on page 18 `2P/Encke' on page 18 `4P/Faye' on page 18 `6P/d'Arrest' on page 18 `7P/Pons-Winnecke' on page 18 `8P/Tuttle' on page 18 `9P/Tempel 1' on page 18 `10P/Tempel 2' on page 18 `14P/Wolf ' on page 18 `15P/Finlay' on page 18 `16P/Brooks2' on page 18 `17P/Holmes' on page 18 `19P/Borrelly' on page 18 `21P/GZ' on page 18 `22P/Kopff ' on page 18 `24P/Schaumasse' on page 18 `26P/GS' on page 18 `28P/Neujmin 1' on page 19 `29P/Schwassmann-Wachmann 1' on page 19 `30P/Reinmuth1' on page 19 `31P/Schwassmann-Wachmann 2' on page 19 `32P/ComasSola' on page 19 `33P/Daniel' on page 19 `36P/Whipple' on page 19 `37P/Forbes' on page 19 `39P/Oterma' on page 19 `40P/Vaisala 1' on page 19 `42P/Neujmin 3' on page 19 `43P/Wolf-Harrington' on page 19 `44P/Reinmuth 2' on page 19 `45P/Honda-Mrkos-Pajdusakova' on page 19 ^´ ´ `46P/Wirtanen' on page 19 `47P/Ashbrook-Jackson' on page 19

` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` `

4 4 5 5 5 5 5 5 5 5 5 6 6 6 6 6 6 6 6 6 7 7 7 7 7 7 7 7 7 7 7 8 8 8 8 8 8 8 9 9 9 9 9 9 9 9 9 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

8 9 0 1 2 3 5 6 7 8 9 0 1 2 3 4 5 7 8 9 0 1 2 3 3 4 5 6 7 8 9 1 2 4 6 7 8 9 0 1 2 3 4 6 7 8 9 0 0 0 0 0 0 0 0 1 1 1 1 1 1 1 1 1

P/Johnson' on page 19 P/Arend-Rigaux' on page 19 P/Arend' on page 19 P/Harrington' on page 19 P/Harrington-Abell' on page 19 P/Van Biesbroeck' on page 19 P/Tempel-Tuttle' on page 19 P/Slaughter-Burnham' on page 19 P/du Toit-Neujmin-Delporte' on page 19 P/Jackson-Neujmin' on page 19 P/Kearns-Kwee' on page 19 P/Tsuchinshan 2' on page 19 P/Shajn-Schaldach' on page 19 P/Tsuchinshan 1' on page 19 P/Wild 1' on page 19 P/Swift-Gehrels' on page 19 P/Gunn' on page 19 P/Churyumov-Gerasimenko' on page 19 P/Klemola' on page 19 P/Taylor' on page 19 P/Kojima' on page 19 P/Clark' on page 19 P/Denning-Fujikawa' on page 19 P/Schwassmann-Wachmann 3' on page 19 P/Schwassmann-Wachmann 3 C' on page 19 P/Smirnova-Chernykh' on page 19 P/Kohoutek' on page 20 P/West-Kohoutek-Ikemura' on page 20 P/Longmore' on page 20 P/Gehrels 2' on page 20 P/du Toit-Hartley' on page 20 P/Wild 2' on page 20 P/Gehrels 3' on page 20 P/Giclas' on page 20 P/Wild 3' on page 20 P/Bus' on page 20 P/Howell' on page 20 P/Russell 2' on page 20 P/Gehrels 1' on page 20 P/Russell 3' on page 20 P/Sanguin' on page 20 P/Lovas 1' on page 20 P/Russell 4' on page 20 P/Machholz 1' on page 20 P/Metcalf-Brewington' on page 20 P/Takamizawa' on page 20 P/Kowal 1' on page 20 0P/Hartley 1' on page 20 1P/Chernykh' on page 20 3P/Hartley 2' on page 20 4P/Kowal 2' on page 20 5P/Singer-Brewster' on page 20 6P/Schuster' on page 20 7P/Wilson-Harrington' on page 20 9P/Swift-Tuttle' on page 20 0P/Hartley 3' on page 20 1P/Helin-Roman-Crockett' on page 20 2P/Urata-Niijima' on page 20 3P/Spitaler' on page 20 4P/Wiseman-Skiff ' on page 20 5P/Maury' on page 20 6P/Wild 4' on page 20 7P/Helin-Roman-Alu 1' on page 20 8P/Shoemaker-Levy 4' on page 20


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 18 Table A.2. References used for each object, and number of epochs. Object C/1983 C/1983 C/1984 C/1984 C/1986 C/1987 C/1987 C/1988 C/1988 C/1995 C/1996 C/1999 C/2000 C/2001 C/2001 P/1991 P/1993 P/1994 P/1994 P/1995 P/1996 P/1997 P/1997 P/1997 P/1998 P/1999 P/1999 P/2004 1P/Hall References Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Bauer et al. (2003) Jewitt (2009b) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Jewitt (2009b) Lamy et al. (2004) Keller and Thomas (1989) Jewitt (2002b) Meech et al. (2004) Lamy et al. (2004) Luu and Jewitt (1990) Lamy et al. (2004) Lamy and Toth (2009) Meech et al. (2004) Jewitt (2002b) Lamy et al. (2004) Snodgrass et al. (2005) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Meech et al. (2004) Lamy et al. (2004) Jewitt and Luu (1989) Meech et al. (2004) Lamy et al. (2004) Jewitt and Meech (1988) Lamy and Toth (2009) Snodgrass et al. (2005) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lamy et al. (2004) Luu (1993) Meech et al. (2004) Lamy et al. (2004) Lamy et al. (2002) Lamy and Toth (2009) Lamy et al. (2004) Boehnhardt et al. (1999) Lamy et al. (2004) Nr. 1 1 1 1 1 1 1 1 1 2 1 1 6 2 1 1 1 1 1 1 1 1 1 1 1 1 1 1 2

H1 IRAS-Araki-Alcock J1 Sugano-Saigusa-Fujikawa K1 Shoemaker U1 Shoemaker P1 Wilson A1 Levy H1 Shoemaker B1 Shoemaker C1 Maury-Phinney O1 Hale-Bopp B2 Hyakutake S 4 L I NE AR B 4 L I NE AR M10 NEAT OG108 LONEOS L3 Levy W1 Mueller A1 Kushida J3 Shoemaker A1 Jedicke A1 Jedicke C1 Gehrels G1 Montani V1 Larsen S 1 LM D1 Hermann RO28 LONEOS A1 ey

2P/Encke

6 2 3 2 2 14

4P/Faye 6P/d'Arrest 7P/Pons-Winnecke 8P/Tuttle 9P/Tempel 1 10P/Tempel 2

10 2 1 1 2 1 2

14P/Wolf 15P/Finlay 16P/Brooks2 17P/Holmes 19P/Borrelly 21P/GZ 22P/Kopff

24P/Schaumasse 26P/GS

4 1 2


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 19 Table A.2. Continued Object 28P/Neujmin 1 References Jewitt and Meech (1988) Delahodde et al. (2001) Meech et al. (2004) Lamy et al. (2004) Campins et al. (1987) Bauer et al. (2003) Jewitt (2009b) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Bauer et al. (2003) Jewitt (2009b) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lamy and Toth (2009) Meech et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lowry et al. (2003) Lamy et al. (2004) Millis et al. (1988) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lamy et al. (2004) Meech et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Boehnhardt et al. (1999) Lamy et al. (2004) Lamy et al. (2004) Nr.

11 3 1 1 1 1 1 2 3 1 1 1 1 2 2 3 2 1 3 2 1 1 2 2 1 1 1 2 1 1 1 2 1 1 2 1 1 2 2 1 1 1 1

29P/Schwassmann-Wachmann 1 30P 31P 32P 33P 36P 37P /Reinmuth1 /Schwassmann-Wachmann 2 /ComasSola /Daniel /Whipple /Forbes

39P/Oterma 40P 41P 42P 43P 44P /Vaisala 1 /Tuttle-Giacobini-Kresak /Neujmin 3 /Wolf-Harrington /Reinmuth 2

45P/Honda-Mrkos-Pajdusakova ^´ ´ 46P/Wirtanen 47P/Ashbrook-Jackson 48P/Johnson 49P/Arend-Rigaux 50P/Arend 51P/Harrington 52P/Harrington-Abell 53P/Van Biesbroeck 55P/Tempel-Tuttle 56P 57P 58P 59P 60P 61P 62P 63P /Slaughter-Burnham /du Toit-Neujmin-Delporte /Jackson-Neujmin /Kearns-Kwee /Tsuchinshan 2 /Shajn-Schaldach /Tsuchinshan 1 /Wild 1

64P/Swift-Gehrels 65P/Gunn 67P/Churyumov-Gerasimenko 68P/Klemola 69P/Taylor 70P/Kojima 71P/Clark 72P 73P 73P 74P /Denning-Fujikawa /Schwassmann-Wachmann 3 /Schwassmann-Wachmann 3 C /Smirnova-Chernykh


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 20 Table A.2. Continued Object 75P/Kohoutek 76P/West-Kohoutek-Ikemura 77P/Longmore 78P/Gehrels 2 79P/du Toit-Hartley 81P/Wild 2 82P/Gehrels 3 84P/Giclas 86P/Wild 3 87P/Bus 88P 89P 90P 91P 92P /Howell /Russell 2 /Gehrels 1 /Russell 3 /Sanguin References Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Meech et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Meech et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Snodgrass et al. (2005) Lamy et al. (2004) Meech et al. (2004) Lamy et al. (2004) Meech et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Meech et al. (2004) Lowry and Weissman (2003) Lamy et al. (2004) Chamberlin et al. (1996) Green et al. (1997) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lamy et al. (2004) Lamy and Toth (2009) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Nr. 1 1 1 1 1 1 1 2 3 2 1 1 1 1 2 1 1 2 1 1 1 1 1 1 1 1 2

93P/Lovas 1 94P/Russell 4 96P/Machholz 1 97P/Metcalf-Brewington 98P/Takamizawa 99P/Kowal 1 100P/Hartley 1 101P/Chernykh 103P/Hartley 2 104P/Kowal 2 105P/Singer-Brewster 106P/Schuster 107P/Wilson-Harrington

6 2 2 1 2 1 2 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

109P/Swift-Tuttle 110P/Hartley 3 111P/Helin-Roman-Crockett 112P/Urata-Niijima 113P/Spitaler 114P/Wiseman-Skiff 115P 116P 117P 118P 119P 120P 121P 123P 124P 125P 126P 128P 129P 130P 131P 132P 134P 135P 136P 137P 138P 139P /Maury /Wild 4 /Helin-Roman-Alu 1 /Shoemaker-Levy 4 /Parker-Hartley /Mueller 1 /Shoemaker-Holt 2 /West-Hartley /Mrkos /Spacewatch /IRAS /Shoemaker-Holt 1 /Shoemaker-Levy 3 /McNaught-Hughes /Mueller 2 /Helin-Roman-Alu 2 /Koval-Vavrova ´ ´ /Shoemaker-Levy 8 /Mueller 3 /Shoemaker-Levy 2 /Shoemaker-Levy 7 /Vaisala-Oterma ¨ ¨¨


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 21 Table A.2. Continued Object 140P/BS 141P/Machholz2 143P/KM 144P/Kushida 147P/Kushida-Muramatsu 148P/Anderson-LINEAR 152P/Helin-Lawrence 154P/Brewington 166P/NEAT 204P/Wild 2 1172-Aneas 1173-Anchises 1647-Menelaus 1871-Astyanax 1993 RO 1994 ES2 1994 EV3 1994 TA 1995 DB
2

1995 DC2 1995 FB21 1995 HM5

1995 WY2 1996 KV1 1996 RQ20

1996 RR

20

1996 TC68 1996 TK66

1996 TS

66

1997 CT

29

1997 CV

29 45 4

1997 GA 1997 QH

1997 RL

13

References Lamy et al. (2004) Lamy et al. (2004) Jewitt (2002b) Jewitt et al. (2003) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Lamy et al. (2004) Jewitt (2009b) Meech et al. (2004) Fornasier (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Boehnhardt et al. (2001) Tegler and Romanishin (2000) Green et al. (1997) Boehnhardt et al. (2001) Gil-Hutton and Licandro (2001) Boehnhardt et al. (2002) Tegler and Romanishin (2000) Jewitt and Luu (2001) Green et al. (1997) Benecchi et al. (2011) Green et al. (1997) Green et al. (1997) Romanishin and Tegler (1999) Gil-Hutton and Licandro (2001) Boehnhardt et al. (2001) Benecchi et al. (2011) Barucci et al. (2000) Tegler and Romanishin (1998) Jewitt and Luu (2001) Benecchi et al. (2011) Romanishin and Tegler (1999) Jewitt and Luu (2001) Boehnhardt et al. (2001) Delsanti et al. (2001) Benecchi et al. (2011) Tegler and Romanishin (1998) Jewitt and Luu (2001) Tegler and Romanishin (2000) Boehnhardt et al. (2002) Benecchi et al. (2011) Gil-Hutton and Licandro (2001) Tegler and Romanishin (2000) Jewitt and Luu (2001) Doressoundiram et al. (2002) Benecchi et al. (2011) Jewitt and Luu (1998) Romanishin and Tegler (1999) Davies et al. (2000) Jewitt and Luu (2001) Tegler and Romanishin (1998) Tegler and Romanishin (2000) Benecchi et al. (2011) Barucci et al. (2000) Tegler and Romanishin (2003) Benecchi et al. (2011) Gladman et al. (1998) Tegler and Romanishin (2000) Jewitt and Luu (2001) Delsanti et al. (2001) Boehnhardt et al. (2002) Gladman et al. (1998)

Nr. 1 1 5 1 1 1 1 1 2 1 2 1 1 3 2 1 4 2 2 5 4

8 2 1

7

4 1

4

7 4 2 1

4 1


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 22 Table A.2. Continued Object 1997 RT References Gladman et al. (1998) Boehnhardt et al. (2002) Benecchi et al. (2011) Gladman et al. (1998) Tegler and Romanishin (2000) Tegler and Romanishin (2003) Benecchi et al. (2011) Barucci et al. (2000) Gil-Hutton and Licandro (2001) Boehnhardt et al. (2002) Benecchi et al. (2011) Doressoundiram et al. (2001) Tegler and Romanishin (2003) Benecchi et al. (2011) Benecchi et al. (2011) Gil-Hutton and Licandro (2001) Delsanti et al. (2001) Benecchi et al. (2011) Benecchi et al. (2011) Benecchi et al. (2011) Peixinho et al. (2004) Davies et al. (2001) Tegler and Romanishin (2000) Benecchi et al. (2011) Delsanti et al. (2001) Peixinho et al. (2004) Benecchi et al. (2009) Benecchi et al. (2009) Tegler and Romanishin (2000) Benecchi et al. (2011) Delsanti et al. (2001) Benecchi et al. (2011) Benecchi et al. (2011) Benecchi et al. (2011) Peixinho et al. (2004) Boehnhardt et al. (2001) Benecchi et al. (2011) Peixinho et al. (2004) Delsanti et al. (2004) Doressoundiram et al. (2002) Delsanti et al. (2006) Benecchi et al. (2011) Delsanti et al. (2001) Benecchi et al. (2011) Benecchi et al. (2011) Benecchi et al. (2011) Peixinho et al. (2004) Benecchi et al. (2011) Benecchi et al. (2011) Benecchi et al. (2011) Peixinho et al. (2004) Benecchi et al. (2011) Tegler and Romanishin (2003) Peixinho et al. (2004) Doressoundiram et al. (2001) Tegler and Romanishin (2003) Benecchi et al. (2011) Peixinho et al. (2004) Benecchi et al. (2011) Benecchi et al. (2011) Snodgrass et al. (2010) Peixinho et al. (2004) Benecchi et al. (2011) Benecchi et al. (2009) Benecchi et al. (2009) Boehnhardt et al. (2002) Benecchi et al. (2011) Nr.

5

1997 RX9 1997 SZ10 1998 FS144 1998 KG

4 1 1 4

62

5 2 1 4 2 2 1 2 2 1 1 2 3 2 3 2 1

1998 KS

65

1998 KY61 1998 UR43 1998 UU43 1998 WS31 1998 WU 1998 WV 1998 WV
24 24 31

1998 WW31 1998 WW31 1998 WX24 1998 WX
31

+B

1998 WY24 1998 WZ31 1998 XY
95

1999 CB119 1999 CD158

5 3 1 1 2 1 3 2 3 1 1 4 2 5 1 1 2

1999 CF

119

1999 CH119 1999 CJ119 1999 CL119 1999 CQ 1999 CX
133 131

1999 HJ12 1999 HS11 1999 HV1 1999 OD4 1999 OE4 1999 OH 1999 OJ4 1999 OJ4+ B 1999 OM4 1999 RC215
4

1


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 23 Table A.2. Continued Object 1999 RT214 1999 RX214 1999 RY21 1999 TR11 1999 2000 2000 2000
4

XY1 4 3 AF 2 5 5 C E 105 C F 105

2000 CF105+ 2000 CG105 2000 CK105 2000 CL104 2000 CN

B

105

2000 CO105 2000 CP104 2000 CQ105

2000 CQ

114 4+ B

2000 CQ11 2000 FS53 2000 2000 2000 2000

F V5 3 F Z 53 GV1 4 KK4

6

2000 KL4 2000 OU6

9

2000 PD30 2000 PE30

2000 2000 2000 2001 2001 2001 2001

P H3 0 QL 2 5 1 QL 2 5 1 + F L 185 FM194 F U1 7 2 KA7 7

B

2001 KB77 2001 KD77

2001 2001 2001 2001 2001

K K O O Q

G7 7 Y7 6 G1 0 9 K1 0 8 C 298

2001 QC

298+ B

References Benecchi et al. (2009) Peixinho et al. (2004) Benecchi et al. (2011) Peixinho et al. (2004) Tegler and Romanishin (2000) Benecchi et al. (2011) Benecchi et al. (2011) Benecchi et al. (2011) Benecchi et al. (2011) Tegler et al. (2003) Benecchi et al. (2011) Benecchi et al. (2009) Benecchi et al. (2009) Benecchi et al. (2011) Snodgrass et al. (2010) Benecchi et al. (2011) Boehnhardt et al. (2002) Benecchi et al. (2011) Peixinho et al. (2004) Peixinho et al. (2004) Jewitt et al. (2007) Benecchi et al. (2011) Benecchi et al. (2011) Benecchi et al. (2011) Peixinho et al. (2004) Tegler et al. (2003) Jewitt et al. (2007) Benecchi et al. (2011) Benecchi et al. (2009) Benecchi et al. (2009) Tegler and Romanishin (2003) Benecchi et al. (2011) Peixinho et al. (2004) Peixinho et al. (2004) Benecchi et al. (2011) McBride et al. (2003) Tegler and Romanishin (2003) Benecchi et al. (2011) Benecchi et al. (2011) Peixinho et al. (2004) Benecchi et al. (2011) Benecchi et al. (2011) Delsanti et al. (2006) Doressoundiram et al. (2007) Benecchi et al. (2011) Sheppard (2010) Doressoundiram et al. (2001) Benecchi et al. (2011) Benecchi et al. (2009) Benecchi et al. (2009) Benecchi et al. (2009) Tegler et al. (2003) Snodgrass et al. (2010) Doressoundiram et al. (2002) Peixinho et al. (2004) Doressoundiram et al. (2005b) Peixinho et al. (2004) Doressoundiram et al. (2002) Peixinho et al. (2004) Doressoundiram et al. (2007) Benecchi et al. (2011) Tegler et al. (2003) Benecchi et al. (2011) Benecchi et al. (2011) Benecchi et al. (2011) Benecchi et al. (2011) Jewitt et al. (2007) Benecchi et al. (2009) Benecchi et al. (2009)

Nr. 1 3 2 2 1 1 2 6 1 3 2 4 4 2 2

5 3 1 2 1 2 1 3 1 3 2

7 1 1 1 1 1 1 4 6

9 1 1 1 1 3 1


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 24 Table A.2. Continued Object 2001 QD298 2001 QF298 References Doressoundiram et al. (2005b) Doressoundiram et al. (2007) Fornasier et al. (2004) Delsanti et al. (2006) Doressoundiram et al. (2005b) Tegler et al. (2003) Benecchi et al. (2011) Jewitt et al. (2007) Benecchi et al. (2009) Benecchi et al. (2009) Benecchi et al. (2011) Tegler et al. (2003) Peixinho et al. (2004) Peixinho et al. (2004) Sheppard (2010) Jewitt et al. (2007) Sheppard (2010) Jewitt et al. (2007) Sheppard (2010) Snodgrass et al. (2010) Romanishin et al. (2010) Jewitt (2009b) Sheppard (2010) Romanishin et al. (2010) Benecchi et al. (2009) Benecchi et al. (2009) DeMeo et al. (2009) Benecchi et al. (2009) Benecchi et al. (2009) Snodgrass et al. (2010) Snodgrass et al. (2010) Benecchi et al. (2009) Benecchi et al. (2009) Sheppard (2010) Jewitt et al. (2007) DeMeo et al. (2009) Romanishin et al. (2010) Sheppard (2010) Benecchi et al. (2009) Benecchi et al. (2009) Snodgrass et al. (2010) Jewitt (2009b) Sheppard (2010) Sheppard (2010) Snodgrass et al. (2010) Sheppard (2010) Benecchi et al. (2009) Benecchi et al. (2009) Snodgrass et al. (2010) Sheppard (2010) Sheppard (2010) Sheppard (2010) Sheppard (2010) Sheppard (2010) Sheppard (2010) Sheppard (2010) Sheppard (2010) Hartmann et al. (1981) Davies et al. (1998) Parker et al. (1997) Jewitt (2002b) Bauer et al. (2003) Doressoundiram et al. (2007) Green et al. (1997) Fornasier (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Nr. 1

8 3 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 2 1 1 1 1 1 1 1 4 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

2001 QX 2001 2001 2001 2001 2002 2002 2002 2002 2003 2003 2003 2003 2003 2003 2003 2003 2003 2003 2003 2003 2003 2003 2003 2003 2003 2003 2003

322

XR 2 5 4 XR 2 5 4 + B XU2 5 4 XZ 2 5 5 C B 249 DH5 GB 3 2 P P 149 F Z 129 GH5 5 HB 5 7 HX5 6 QA9 2 QD1 1 2 QK9 1 QQ9 1 QW 1 1 1 QW 1 1 1 + B QW 9 0 QY9 0 QY9 0 + B S Q3 1 7 T H5 8 TJ58 TJ58+ B UY2 9 1 UZ 1 1 7

2003 YL179 2004 OJ14 2004 PB108 2004 PB108+ B 2004 PT107 2004 PY42 2004 VN112 2004 XR190 2005 CB79 2005 EO297 2005 EO304 2005 EO304+ B 2005 GE187 2005 PU21 2005 SD278 2006 SQ372 2007 TG422 2007 VJ305 2008 KV42 2008 OG19 2008 YB3 2060-Chiron

22232357354840354829-

Sarpedon Phereclos Eurybates 1986 WD Sergestus

34 1 1 1 2 1


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 25 Table A.2. Continued Object 5130-Ilioneus 5145-Pholus References Fornasier (2007) Binzel (1992) Mueller et al. (1992) Davies et al. (1993) Davies et al. (1998) Romanishin and Tegler (1999) Weintraub et al. (1997) Bauer et al. (2003) Doressoundiram et al. (2007) Buie and Bus (1992) Davies (2000) Fink et al. (1992) Green et al. (1997) Tegler and Romanishin (1998) Fornasier (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Davies et al. (1998) Romanishin and Tegler (1999) Bauer et al. (2003) Davies (2000) Tegler and Romanishin (1998) Fornasier (2007) Weintraub et al. (1997) Brown and Luu (1997) Davies et al. (1998) Bauer et al. (2003) Romon-Martin et al. (2002) Davies (2000) Rabinowitz et al. (2007) Tegler and Romanishin (1998) Fornasier (2007) Fornasier (2007) Fornasier (2007) Davies et al. (1998) Jewitt and Kalas (1998) Romanishin and Tegler (1999) N. McBride and Foster (1999) Jewitt and Luu (2001) Peixinho et al. (2001) Bauer et al. (2003) DeMeo et al. (2009) Davies (2000) Tegler and Romanishin (1998) Davies et al. (1998) Romanishin and Tegler (1999) Bauer et al. (2003) Doressoundiram et al. (2002) Delsanti et al. (2006) Davies (2000) Tegler and Romanishin (1998) Fornasier (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Dotto (2005) Fornasier (2007) Fornasier (2007) Dotto (2005) Fornasier (2007) Fornasier (2007) Fornasier (2007) Dotto (2005) Fornasier (2007) Fornasier (2007) Dotto (2005) Nr. 1

524452585511654569987066-

Amphilochos 1989 AU1 Cloanthus 1986 TR6 Tithonus Nessus

41 1 1 1 1 1

7352-1994 CO 8405-Asbolus

17 1

9030-1989 UX5 9430-Erichthonio 9818-Eurymachos 10199-Chariklo

43 1 1 1

64

10370-Hylonome

1108911351114881166312917-

1994 1997 1988 1997 1998

CS 8 T S 25 RM11 GO2 4 T G1 6
5

25 1 1 2 1 2 2 2 1 2 3 3 4

12921-1998 WZ 13463-Antiphos

13862-1999 XT16 14707-2000 CC20 15094-1999 WB2

0

15502-1999 NV27 15535-2000 AT177


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 26 Table A.2. Continued Object 15760-1992 QB References Jewitt and Luu (2001) Tegler and Romanishin (2000) Boehnhardt et al. (2001) Benecchi et al. (2011) Romanishin et al. (1997) Gil-Hutton and Licandro (2001) Jewitt and Luu (2001) Tegler and Romanishin (2000) McBride et al. (2003) Delsanti et al. (2001) Benecchi et al. (2011) Davies et al. (1997) Romanishin and Tegler (1999) Jewitt and Luu (1998) Davies et al. (2000) Jewitt and Luu (2001) Benecchi et al. (2011) Luu and Jewitt (1996) Romanishin et al. (1997) Tegler and Romanishin (1998) Gil-Hutton and Licandro (2001) Benecchi et al. (2011) Green et al. (1997) Romanishin and Tegler (1999) Benecchi et al. (2011) Barucci et al. (1999) Tegler and Romanishin (1998) Davies et al. (2000) Jewitt and Luu (2001) Delsanti et al. (2001) Delsanti et al. (2004) Delsanti et al. (2006) Doressoundiram et al. (2007) Barucci et al. (1999) Davies (2000) Romanishin et al. (1997) Tegler and Romanishin (1998) Green et al. (1997) Benecchi et al. (2011) Jewitt et al. (2007) Jewitt and Luu (1998) Romanishin and Tegler (1999) Boehnhardt et al. (2001) Davies et al. (2000) Jewitt and Luu (2001) Benecchi et al. (2011) Doressoundiram et al. (2007) Barucci et al. (1999) Davies (2000) Tegler and Romanishin (1998) Jewitt and Luu (1998) Romanishin and Tegler (1999) Boehnhardt et al. (2001) Davies et al. (2000) Jewitt and Luu (2001) Barucci et al. (1999) Jewitt and Luu (2001) Doressoundiram et al. (2001) Benecchi et al. (2011) Fornasier (2007) Green et al. (1997) Gil-Hutton and Licandro (2001) Boehnhardt et al. (2002) Tegler and Romanishin (2003) Benecchi et al. (2011) Fornasier (2007) Fornasier (2007) Nr.

1

5

15788-1993 SB

6

15789-1993 SC

15807-1994 GV 15809-1994 JS 15810-1994 JR1

9

17 1 2

9

15820-1994 TB

15 6

15836-1995 DA 15874-1996 TL

2

66

16

15875-1996 TP

66

7 3 1

15883-1997 CR

29

15977-1998 MA 16684-1994 JQ1

11

17416-1988 RR10 18060-1999 XJ156

8 1 1


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 27 Table A.2. Continued Object 1813718268184931894019255References Fornasier (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Tegler and Romanishin (2000) Doressoundiram et al. (2001) Benecchi et al. (2011) Jewitt and Luu (2001) Tegler and Romanishin (2000) McBride et al. (2003) Boehnhardt et al. (2002) Jewitt et al. (2007) Jewitt and Luu (1998) Romanishin and Tegler (1999) Hainaut et al. (2000) Gil-Hutton and Licandro (2001) Davies et al. (2000) Jewitt and Luu (2001) Boehnhardt et al. (2001) Sheppard (2010) Barucci et al. (1999) Davies (2000) Tegler and Romanishin (1998) Davies et al. (2000) Tegler and Romanishin (2000) Boehnhardt et al. (2001) Delsanti et al. (2004) Doressoundiram et al. (2002) Benecchi et al. (2011) Doressoundiram et al. (2007) Barucci et al. (2000) Doressoundiram et al. (2002) Hainaut (2001) Jewitt and Sheppard (2002) McBride et al. (2003) Doressoundiram et al. (2007) Jewitt et al. (2007) Rabinowitz et al. (2007) Gil-Hutton and Licandro (2001) Tegler and Romanishin (2000) Benecchi et al. (2011) Benecchi et al. (2011) Fornasier (2007) Dotto (2005) Fornasier (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Dotto (2005) Fornasier (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Gil-Hutton and Licandro (2001) Boehnhardt et al. (2001) Delsanti et al. (2001) McBride et al. (2003) Delsanti et al. (2004) Doressoundiram et al. (2002) Benecchi et al. (2011) Jewitt et al. (2007) Doressoundiram et al. (2007) Rabinowitz et al. (2008) Nr. 1 1 2 1 4

2000 OU30 Dardanos Demoleon 2000 QV49 1994 VK8

19299-1996 SZ

4

5

19308-1996 TO

66

16

19521-Chaos

13

20000-Varuna

8 3 1 2 1 1 1 1 1 2 1 1 1 1 1

20108-1995 QZ

9

20161-1996 TR66 20738-1999 XG19 235492369424233243412438024390244202442624444244522446724835Epicl 1997 1999 2000 2000 2000 2000 2000 2000 2000 2000 1995 es K X A A A Z3 D9 J87 A1 D1

1

4 60 77

BU22 C R 12 OP 3 2 QU167 S S 165 SM55

10


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 28 Table A.2. Continued Object 24952-1997 QJ4 References Gil-Hutton and Licandro (2001) Jewitt and Luu (2001) Delsanti et al. (2001) Boehnhardt et al. (2002) Tegler and Romanishin (2003) Benecchi et al. (2011) Fornasier (2007) McBride et al. (2003) Boehnhardt et al. (2002) Delsanti et al. (2006) Doressoundiram et al. (2003) Doressoundiram et al. (2007) Tegler and Romanishin (2000) McBride et al. (2003) Delsanti et al. (2004) Doressoundiram et al. (2007) Jewitt et al. (2007) Benecchi et al. (2009) Benecchi et al. (2009) Jewitt and Luu (2001) Delsanti et al. (2001) Doressoundiram et al. (2002) McBride et al. (2003) Delsanti et al. (2006) Doressoundiram et al. (2003) Tegler et al. (2003) Benecchi et al. (2011) Doressoundiram et al. (2007) DeMeo et al. (2009) Rabinowitz et al. (2007) Fornasier (2007) Doressoundiram et al. (2002) Doressoundiram et al. (2007) DeMeo et al. (2009) Rabinowitz et al. (2007) Delsanti et al. (2001) McBride et al. (2003) Doressoundiram et al. (2002) Doressoundiram et al. (2007) Consolmagno et al. (2000) Rabinowitz et al. (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Peixinho et al. (2001) Delsanti et al. (2004) Doressoundiram et al. (2002) Doressoundiram et al. (2007) Gutierrez et al. (2001) ´ Fornasier (2007) Farnham and Davies (2003) Tegler et al. (2003) Barucci et al. (2002) Bauer et al. (2003) Doressoundiram et al. (2007) DeMeo et al. (2009) Rabinowitz et al. (2007) Fornasier (2007) Fornasier (2007) Gil-Hutton and Licandro (2001) Davies et al. (2000) Barucci et al. (1999) Tegler and Romanishin (2000) Jewitt and Luu (2001) Doressoundiram et al. (2001) Benecchi et al. (2011) Barucci et al. (2000) Nr.

4 2 1

24978-1998 HJ1

51

25347-1999 RQ116 26181-1996 GQ21

8

26308-1998 SM1

65

26308-1998 SM1 26375-1999 DE9

65+ B

8 1

28958-2001 CQ 28978-Ixion

42

13 1

8

29981-1999 TD

10

30698318203182131824-

Hippokoon 1999 RT186 1999 RK225 Elatus

18 3 1 1

32430-2000 RQ 32532-Thereus

83

14 1

32615-2001 QU27 32794-1989 UE5 32929-1995 QY9 33001-1997 CU

7

221 1 1 5

29

6


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 29

` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` `

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 2 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

1 2 2 2 2 2 2 2 2 3 3 3 3 3 3 3 3 3 4 4 4 4 4 4 5 5 6 0 1 1 6 8 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9

9 0 1 3 4 5 6 8 9 0 1 2 4 5 6 7 8 9 0 1 3 4 7 8 2 4 6 4 7 7 4 7 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9

P/Parker-Hartley' on page 20 P/Mueller 1' on page 20 P/Shoemaker-Holt 2' on page 20 P/West-Hartley' on page 20 P/Mrkos' on page 20 P/Spacewatch' on page 20 P/IRAS' on page 20 P/Shoemaker-Holt 1' on page 20 P/Shoemaker-Levy 3' on page 20 P/McNaught-Hughes' on page 20 P/Mueller 2' on page 20 P/Helin-Roman-Alu 2' on page 20 P/Koval-Vavrova' on page 20 ´ ´ P/Shoemaker-Levy 8' on page 20 P/Mueller 3' on page 20 P/Shoemaker-Levy 2' on page 20 P/Shoemaker-Levy 7' on page 20 P/Vaisala-Oterma' on page 20 ¨ ¨¨ P/BS' on page 21 P/Machholz2' on page 21 P/KM' on page 21 P/Kushida' on page 21 P/Kushida-Muramatsu' on page 21 P/Anderson-LINEAR' on page 21 P/Helin-Lawrence' on page 21 P/Brewington' on page 21 P/NEAT' on page 21 P/Wild 2' on page 21 2-Aneas' on page 21 3-Anchises' on page 21 7-Menelaus' on page 21 1-Astyanax' on page 21 3 RO' on page 21 4 ES2 ' on page 21 4 E V3 ' o n p a g e 2 1 4 TA' on page 21 5 DB2 ' on page 21 5 DC2 ' on page 21 5 FB21 ' on page 21 5 HM 5 ' o n p a g e 2 1 5 WY2 ' on page 21 6 KV1 ' o n p a g e 2 1 6 RQ20 ' on page 21 6 RR20 ' on page 21 6 TC68 ' on page 21 6 TK66 ' on page 21 6 TS66 ' on page 21 7 CT29 ' on page 21 7 CV29 ' on page 21 7 GA45 ' on page 21 7 QH4 ' o n p a g e 2 1 7 RL13 ' on page 21 7 RT5 ' on page 22 7 RX9 ' on page 22 7 SZ10 ' on page 22 8 FS144 ' on page 22 8 KG62 ' on page 22 8 KS65 ' on page 22 8 KY61 ' on page 22 8 UR43 ' on page 22 8 UU43 ' on page 22 8 WS31 ' on page 22 8 WU24 ' on page 22 8 WV24 ' on page 22

` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` `

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2

9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0

9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0

8 8 8 8 8 8 8 8 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 9 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 1 1 1 1 1 1 1 1

WV31 ' on page 22 WW31 ' on page 22 WW31+B ' on page 22 WX24 ' on page 22 WX31 ' on page 22 WY24 ' on page 22 WZ31 ' on page 22 XY95 ' on page 22 CB119 ' on page 22 CD158 ' on page 22 CF119 ' on page 22 CH119 ' on page 22 CJ119 ' on page 22 CL119 ' on page 22 CQ133 ' on page 22 CX131 ' on page 22 HJ12 ' on page 22 HS11 ' on page 22 HV11 ' on page 22 OD4 ' o n p a g e 2 2 OE 4 ' o n p a g e 2 2 OH4 ' o n p a g e 2 2 OJ4 ' on page 22 OJ4+B ' on page 22 OM 4 ' o n p a g e 2 2 RC215 ' on page 22 RT214 ' on page 23 RX214 ' on page 23 RY214 ' on page 23 TR11 ' on page 23 XY143 ' on page 23 AF255 ' on page 23 CE105 ' on page 23 CF105 ' on page 23 CF105+B ' on page 23 CG105 ' on page 23 CK105 ' on page 23 CL104 ' on page 23 CN105 ' on page 23 CO105 ' on page 23 CP104 ' on page 23 CQ105 ' on page 23 CQ114 ' on page 23 CQ114+B ' on page 23 FS53 ' on page 23 FV53 ' on page 23 FZ53 ' on page 23 GV146 ' on page 23 KK4 ' o n p a g e 2 3 KL 4 ' o n p a g e 2 3 OU69 ' on page 23 PD30 ' on page 23 PE30 ' on page 23 PH30 ' on page 23 QL251 ' on page 23 QL251+B ' on page 23 FL185 ' on page 23 FM194 ' on page 23 FU172 ' on page 23 KA77 ' on page 23 KB77 ' on page 23 KD77 ' on page 23 KG77 ' on page 23 KY76 ' on page 23


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 30

` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` `

2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 3 4 4 5 5 5

0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 2 3 5 0 8 1 1 2

0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 0 6 2 5 4 3 2 3 4 4

1 1 1 1 1 1 1 1 1 1 1 2 2 2 2 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 4 4 4 4 4 4 4 5 5 5 5 5 5 5 6 7 7 8 8 8 0 3 7 8 5 9 0 5 4

OG109 ' on page 23 OK108 ' on page 23 QC298 ' on page 23 QC298+B ' on page 23 QD298 ' on page 24 QF298 ' on page 24 QX322 ' on page 24 XR254 ' on page 24 XR254+B ' on page 24 XU254 ' on page 24 XZ255 ' on page 24 CB249 ' on page 24 DH5 ' o n p a g e 2 4 GB32 ' on page 24 PP149 ' on page 24 FZ129 ' on page 24 GH55 ' on page 24 HB57 ' on page 24 HX56 ' on page 24 QA92 ' on page 24 QD112 ' on page 24 QK91 ' on page 24 QQ91 ' on page 24 QW111 ' on page 24 QW111+B ' on page 24 QW90 ' on page 24 QY90 ' on page 24 QY90+B ' on page 24 SQ317 ' on page 24 TH58 ' on page 24 TJ58 ' on page 24 TJ58+B ' on page 24 UY291 ' on page 24 UZ117 ' on page 24 YL179 ' on page 24 OJ14 ' on page 24 PB108 ' on page 24 PB108+B ' on page 24 PT107 ' on page 24 PY42 ' on page 24 VN112 ' on page 24 XR190 ' on page 24 CB79 ' on page 24 EO297 ' on page 24 EO304 ' on page 24 EO304+B ' on page 24 GE187 ' on page 24 PU21 ' on page 24 SD278 ' on page 24 SQ372 ' on page 24 TG422 ' on page 24 VJ305 ' on page 24 KV42 ' on page 24 OG19 ' on page 24 YB3 ' on page 24 -Chiron' on page 24 -Sarpedon' on page 24 -Phereclos' on page 24 -Eurybates' on page 24 -1986 WD' on page 24 -Sergestus' on page 24 -Ilioneus' on page 25 -Pholus' on page 25 -Amphilochos' on page 25

` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` `

5 5 6 6 7 7 8 9 9 9 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2

2 5 5 9 0 3 4 0 4 8 0 0 1 1 1 1 2 2 3 3 4 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 6 7 8 8 8 8 8 9 9 9 9 0 0 0 0 3 3 4 4 4 4 4 4 4 4 4 4 4

5 1 4 9 6 5 0 3 3 1 1 3 0 3 4 6 9 9 4 8 7 0 5 5 7 7 7 8 8 8 8 8 8 8 8 9 6 4 0 1 2 4 9 2 2 3 5 0 1 1 7 5 6 2 3 3 3 4 4 4 4 4 8 9

8 1 5 8 6 2 5 0 0 8 9 7 8 5 8 6 1 2 6 6 0 9 0 3 6 8 8 0 0 1 2 3 7 7 8 7 8 1 6 3 6 9 4 5 9 0 2 0 0 6 3 4 9 3 4 8 9 2 2 4 5 6 3 5

-1989 AU1 ' on page 25 -Cloanthus' on page 25 -1986 TR6 ' on page 25 -Tithonus' on page 25 -Nessus' on page 25 -1994 CO' on page 25 -Asbolus' on page 25 - 1 9 8 9 UX5 ' o n p a g e 2 5 -Erichthonio' on page 25 -Eurymachos' on page 25 9-Chariklo' on page 25 0-Hylonome' on page 25 9-1994 CS8 ' on page 25 1-1997 TS25 ' on page 25 8-1988 RM11 ' on page 25 3-1997 GO24 ' on page 25 7-1998 TG16 ' on page 25 1-1998 WZ5 ' on page 25 3-Antiphos' on page 25 2-1999 XT160 ' on page 25 7-2000 CC20 ' on page 25 4-1999 WB2 ' on page 25 2-1999 NV27 ' on page 25 5-2000 AT177 ' on page 25 0-1992 QB1 ' on page 26 8-1993 SB' on page 26 9-1993 SC' on page 26 7 - 1 9 9 4 GV9 ' o n p a g e 2 6 9-1994 JS' on page 26 0-1994 JR1 ' on page 26 0-1994 TB' on page 26 6-1995 DA2 ' on page 26 4-1996 TL66 ' on page 26 5-1996 TP66 ' on page 26 3-1997 CR29 ' on page 26 7-1998 MA11 ' on page 26 4-1994 JQ1 ' on page 26 6-1988 RR10 ' on page 26 0-1999 XJ156 ' on page 26 7-2000 OU30 ' on page 27 8-Dardanos' on page 27 3-Demoleon' on page 27 0-2000 QV49 ' on page 27 5 - 1 9 9 4 VK8 ' o n p a g e 2 7 9-1996 SZ4 ' on page 27 8-1996 TO66 ' on page 27 1-Chaos' on page 27 0-Varuna' on page 27 8 - 1 9 9 5 QZ 9 ' o n p a g e 2 7 1-1996 TR66 ' on page 27 8-1999 XG191 ' on page 27 9-Epicles' on page 27 4 - 1 9 9 7 KZ 3 ' o n p a g e 2 7 3-1999 XD94 ' on page 27 1-2000 AJ87 ' on page 27 0-2000 AA160 ' on page 27 0-2000 AD177 ' on page 27 0-2000 BU22 ' on page 27 6-2000 CR12 ' on page 27 4-2000 OP32 ' on page 27 2-2000 QU167 ' on page 27 7-2000 SS165 ' on page 27 5-1995 SM55 ' on page 27 2-1997 QJ4 ' on page 28


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 31

` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` `

2 2 2 2 2 2 2 2 2 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 4 4 4 4 4 4 4 4 4 4 4 4 4 4 4 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 5 6 6 6 6 6

4 5 6 6 6 6 8 8 9 0 1 1 1 2 2 2 2 2 3 3 3 4 5 8 8 8 9 0 2 2 2 3 4 5 7 7 7 7 8 8 8 9 0 1 2 2 2 3 4 4 5 5 5 5 5 6 8 8 9 0 0 0 0 0

9 3 1 3 3 3 9 9 9 6 8 8 8 4 5 6 7 9 0 1 3 7 6 0 0 6 2 3 3 3 3 2 5 8 1 1 9 9 2 2 6 0 0 3 7 8 9 4 5 5 5 5 6 6 6 9 5 5 3 4 4 4 5 6

7 4 8 0 0 7 5 7 8 9 2 2 2 3 3 1 9 2 0 2 4 8 7 8 8 2 8 1 0 5 5 1 9 0 7 7 3 6 4 5 3 3 0 5 4 7 7 6 2 9 6 7 3 3 3 6 3 3 5 5 5 5 5 0

8 7 1 8 8 5 8 8 1 8 0 1 4 0 2 5 4 9 1 8 0 5 1 3 4 8 5 4 1 5 5 2 4 2 1 1 2 7 9 2 9 6 0 9 7 2 5 9 0 8 5 6 6 7 8 8 4 4 8 4 8 8 8 8

-

1998 HJ151 ' on page 28 1999 RQ116 ' on page 28 1996 GQ21 ' on page 28 1998 SM165 ' on page 28 1998 SM165+B ' on page 28 1 9 9 9 DE 9 ' o n p a g e 2 8 2001 CQ42 ' on page 28 Ixion' on page 28 1999 TD10 ' on page 28 Hippokoon' on page 28 1999 RT186 ' on page 28 1999 RK225 ' on page 28 Elatus' on page 28 2000 RQ83 ' on page 28 Thereus' on page 28 2001 QU277 ' on page 28 1 9 8 9 UE 5 ' o n p a g e 2 8 1 9 9 5 QY9 ' o n p a g e 2 8 1997 CU29 ' on page 28 1998 BU48 ' on page 33 1998 VG44 ' on page 33 2001 RG87 ' on page 33 1998 SN165 ' on page 33 Rhadamanth' on page 33 1999 HB12 ' on page 33 Hu y a ' o n p a g e 3 3 2001 BP75 ' on page 33 1999 KR16 ' on page 33 2001 UR163 ' on page 33 Typhon' on page 33 Typhon+B' on page 33 2000 AL113 ' on page 33 1999 OX3 ' on page 33 2000 PV29 ' on page 33 1999 TC36 ' on page 34 1999 TC36+B ' on page 34 2000 GN171 ' on page 34 2000 SL298 ' on page 34 2001 SY345 ' on page 34 2001 TL212 ' on page 34 1 9 9 5 T L 8 ' o n p ag e 3 4 Pelion' on page 34 Qu a o a r ' o n p a g e 3 4 2000 SC17 ' on page 34 1998 HM151 ' on page 34 Okyrhoe' on page 34 Cyllarus' on page 34 2 0 0 0 AX8 ' o n p a g e 3 4 2000 PJ30 ' on page 34 Bienor' on page 34 2002 AW197 ' on page 34 Amycus' on page 34 2002 TX300 ' on page 34 2002 UX25 ' on page 35 2002 VE95 ' on page 35 2000 SA92 ' on page 35 Logos' on page 35 Logos+B' on page 35 1999 CL158 ' on page 35 2000 CH105 ' on page 35 2000 CM114 ' on page 35 2000 CM114+B ' on page 35 Echeclus' on page 35 2000 EE173 ' on page 35

` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` `

6 6 6 6 6 6 6 6 6 6 6 6 6 6 7 7 7 7 7 7 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 8 9 9 9 9 9 9 9 9 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1

0 0 3 5 5 5 5 6 6 6 9 9 9 9 3 6 9 9 9 9 0 2 2 2 3 4 4 5 5 6 6 7 7 8 8 8 0 0 0 1 1 1 5 9 0 1 1 1 1 1 1 1 1 1 2 2 2 2 2 2 2 2 2 2

6 6 2 1 2 4 4 4 6 6 9 9 9 9 4 8 3 3 9 9 8 0 1 1 9 5 7 6 6 0 1 2 5 2 6 6 3 4 5 1 2 5 6 3 5 1 8 8 8 9 9 9 9 9 0 0 0 0 0 0 0 1 3 3

2 2 5 5 2 8 8 5 5 5 8 8 8 9 8 0 6 6 7 8 0 7 5 5 8 2 0 2 3 4 7 6 5 6 1 1 7 8 6 3 0 5 2 2 6 1 2 3 7 0 0 3 9 9 0 1 1 3 3 3 4 7 5 5

0 1 2 0 5 9 9 2 2 2 6 7 8 0 0 4 0 0 8 3 6 5 5 8 2 2 9 7 3 7 7 9 5 9 1 1 7 2 8 3 5 4 6 8 8 1 2 7 0 6 7 1 5 7 6 3 7 4 4 4 5 2 0 0

-2000 FD8 ' on page 35 -2000 FE8 ' on page 35 -2001 BL41 ' on page 35 -2002 CA126 ' on page 35 -2002 EK44 ' on page 35 -Ceto' on page 35 -Ceto+B' on page 35 -1999 OF4 ' on page 35 -Borasisi' on page 35 -Borasisi+B' on page 35 -1998 WW24 ' on page 35 -1998 WA25 ' on page 35 -1998 WA31 ' on page 35 -1998 WU31 ' on page 35 -2002 PN34 ' on page 35 - 2 0 0 0 QE ' o n p a g e 3 5 -1997 CS29 ' on page 36 -1997 CS29+B ' on page 36 -1999 CC158 ' on page 36 -1999 DF9 ' on page 36 -2000 CM105 ' on page 36 -2000 YW134 ' on page 36 -2001 FZ173 ' on page 36 -2001 FP185 ' on page 36 -Crantor' on page 36 -2002 TC302 ' on page 36 -2002 VW120 ' on page 36 -1998 HP151 ' on page 36 -1998 KR65 ' on page 36 -1999 OY3 ' on page 36 -1999 RY215 ' on page 36 -2000 OO67 ' on page 36 -2000 QB243 ' on page 36 -2001 KF77 ' on page 36 -Teharonhia' on page 36 -Teharonhia+B' on page 36 -Sedna' on page 36 -Orcus' on page 36 - 2 0 0 4 GV9 ' o n p a g e 3 6 -1998 HK151 ' on page 37 -1998 US43 ' on page 37 -1999 RZ215 ' on page 37 -2002 GZ32 ' on page 37 -2001 UY123 ' on page 37 5-2000 SC51 ' on page 37 3-2001 VK85 ' on page 37 8-1996 TQ66 ' on page 37 9-1999 HC12 ' on page 37 2-2000 OM67 ' on page 37 8-2001 KC77 ' on page 37 0-2001 KP77 ' on page 37 5-2001 SQ73 ' on page 37 1-2002 KX14 ' on page 37 9-2002 WC19 ' on page 37 1-2003 CO1 ' on page 37 2-2003 FY128 ' on page 37 8-2003 OP32 ' on page 37 7-Salacia' on page 37 7-Salacia+B' on page 37 8-2004 TY364 ' on page 37 3-1988 RE12 ' on page 37 5-1999 XX143 ' on page 37 9-2000 WK183 ' on page 37 9-2000 WK183+B ' on page 37


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 32

` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` ` `

1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 2

2 2 2 3 3 3 3 3 3 3 3 3 3 3 3 3 3 3 4 4 4 4 4 4 4 4 5 6 6 6 6 8 8 8 8 8 8 8 8 9 9 0

4 7 9 0 1 4 4 4 4 4 4 5 6 6 6 7 7 8 4 5 5 5 5 8 8 8 0 3 3 8 8 1 1 1 1 1 1 2 2 2 2 8

7 5 7 3 6 3 3 3 3 8 8 1 1 1 4 2 2 5 8 4 4 4 4 2 7 7 6 1 2 7 7 7 8 8 8 8 9 3 9 3 9 9

2 4 7 9 9 4 4 4 4 6 6 8 0 9 7 9 9 3 9 5 5 5 8 0 8 8 4 3 1 0 0 0 5 6 7 7 0 9 3 8 2 9

9 6 2 1 5 0 0 0 0 0 0 2 8 9 2 4 5 7 7 1 2 3 0 9 0 0 2 5 6 0 3 8 5 7 1 4 2 7 3 8 9 6

-

2001 SB173 ' on page 37 2002 XU93 ' on page 37 1999 HR11 ' on page 37 2000 JG81 ' on page 37 2001 XS254 ' on page 37 Pluto' on page 37 Pluto+B' on page 37 Pluto+C' on page 37 Pluto+D' on page 37 2000 OJ67 ' on page 37 2000 OJ67+B ' on page 37 2001 QT322 ' on page 37 Ha u m e a ' o n p a g e 3 7 Eris' on page 37 Makemake' on page 38 1999 RE215 ' on page 38 1999 RB216 ' on page 38 2000 OK67 ' on page 38 2004 UX10 ' on page 38 2005 RM43 ' on page 38 2005 RN43 ' on page 38 2005 RR43 ' on page 38 2005 TB190 ' on page 38 2000 CR105 ' on page 38 Altjira' on page 38 Altjira+B' on page 38 2001 CZ31 ' on page 38 2002 CT22 ' on page 38 2002 EN68 ' on page 38 2000 GE147 ' on page 38 2000 GP183 ' on page 38 1993 FW' on page 38 1998 WT31 ' on page 38 1999 CV118 ' on page 38 1999 CO153 ' on page 38 1999 HW11 ' on page 38 1999 RD215 ' on page 38 2001 QW297 ' on page 38 2002 GZ31 ' on page 38 1996 RD29 ' on page 38 2000 AT44 ' on page 38 2003 AZ84 ' on page 38


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 33 Table A.2. Continued Object 33128-1998 BU References Delsanti et al. (2004) Doressoundiram et al. (2002) Delsanti et al. (2006) Bauer et al. (2003) Boehnhardt et al. (2001) Doressoundiram et al. (2001) McBride et al. (2003) Doressoundiram et al. (2002) Delsanti et al. (2006) Benecchi et al. (2011) Doressoundiram et al. (2007) Fornasier (2007) Jewitt and Luu (2001) Gil-Hutton and Licandro (2001) Delsanti et al. (2001) McBride et al. (2003) Fornasier et al. (2004) Doressoundiram et al. (2001) Boehnhardt et al. (2002) Benecchi et al. (2011) Peixinho et al. (2004) Doressoundiram et al. (2001) Ferrin et al. (2001) Jewitt and Luu (2001) Schaefer and Rabinowitz (2002) Boehnhardt et al. (2002) McBride et al. (2003) Doressoundiram et al. (2007) Doressoundiram et al. (2001) Rabinowitz et al. (2007) Fornasier (2007) Jewitt and Luu (2001) Delsanti et al. (2006) Boehnhardt et al. (2002) Jewitt et al. (2007) Doressoundiram et al. (2007) Doressoundiram et al. (2005b) Benecchi et al. (2011) Peixinho et al. (2004) Tegler et al. (2003) Doressoundiram et al. (2007) Jewitt et al. (2007) DeMeo et al. (2009) Benecchi et al. (2009) Rabinowitz et al. (2007) Benecchi et al. (2009) Fornasier (2007) Tegler and Romanishin (2000) Bauer et al. (2003) Delsanti et al. (2001) McBride et al. (2003) Boehnhardt et al. (2002) Doressoundiram et al. (2002) Peixinho et al. (2004) Doressoundiram et al. (2005b) Doressoundiram et al. (2007) Delsanti et al. (2006) Jewitt et al. (2007) Sheppard (2010) Doressoundiram et al. (2001) Benecchi et al. (2011) Nr.

48

9

33340-1998 VG

44

34785-2001 RG87 35671-1998 SN165

12 1

38083-Rhadamanth 38084-1999 HB12 38628-Huya

6 1 3

39285-2001 BP75 40314-1999 KR16

58 1

5 6

42301-2001 UR 42355-Typhon

163

42355-Typhon+B 43212-2000 AL113 44594-1999 OX3

12 1 1

45802-2000 PV

29

30 2


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 34 Table A.2. Continued Object 47171-1999 TC References Boehnhardt et al. (2001) Delsanti et al. (2001) McBride et al. (2003) Delsanti et al. (2004) Dotto et al. (2003) Tegler et al. (2003) Doressoundiram et al. (2007) Protopapa et al. (2009) DeMeo et al. (2009) Benecchi et al. (2009) Doressoundiram et al. (2001) Rabinowitz et al. (2007) Benecchi et al. (2009) McBride et al. (2003) Boehnhardt et al. (2002) Doressoundiram et al. (2007) DeMeo et al. (2009) Rabinowitz et al. (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Delsanti et al. (2004) Doressoundiram et al. (2002) Benecchi et al. (2011) Sheppard (2010) Tegler and Romanishin (2000) Boehnhardt et al. (2002) Doressoundiram et al. (2002) Fornasier et al. (2004) Tegler et al. (2003) DeMeo et al. (2009) Rabinowitz et al. (2007) Fornasier (2007) Tegler and Romanishin (2003) Bauer et al. (2003) Delsanti et al. (2001) Dotto et al. (2003) Delsanti et al. (2006) Doressoundiram et al. (2007) Doressoundiram et al. (2001) Boehnhardt et al. (2001) Delsanti et al. (2004) Bauer et al. (2003) Doressoundiram et al. (2002) Tegler et al. (2003) Fornasier (2007) Benecchi et al. (2011) Delsanti et al. (2004) Doressoundiram et al. (2002) Tegler et al. (2003) Dotto et al. (2003) Bauer et al. (2003) Doressoundiram et al. (2007) DeMeo et al. (2009) Rabinowitz et al. (2007) Doressoundiram et al. (2005a) Fornasier et al. (2004) Jewitt et al. (2007) DeMeo et al. (2009) Rabinowitz et al. (2007) Peixinho et al. (2004) Bauer et al. (2003) Fornasier et al. (2004) Doressoundiram et al. (2005a) Doressoundiram et al. (2007) Tegler et al. (2003) Doressoundiram et al. (2005b) Jewitt et al. (2007) Ortiz et al. (2004) Rabinowitz et al. (2008) Rabinowitz et al. (2007) Nr.

36

47171-1999 TC36+ B 47932-2000 GN171

23 1

47967482494825248639-

2000 2001 2001 1995

S L 298 S Y3 4 5 T L 212 TL8

13 1 1 1

4 3

49036-Pelion 50000-Quaoar

51359-2000 SC17 52747-1998 HM1 52872-Okyrhoe

51

4 1 1

18

52975-Cyllarus

53469-2000 AX8 54520-2000 PJ30 54598-Bienor

9 1 1

15

55565-2002 AW

197

9

55576-Amycus

19

55636-2002 TX

300

8


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 35 Table A.2. Continued Object 55637-2002 UX References Jewitt et al. (2007) Doressoundiram et al. (2007) DeMeo et al. (2009) Rabinowitz et al. (2007) Rabinowitz et al. (2007) Barucci et al. (2006) Fornasier (2007) Jewitt and Luu (2001) Boehnhardt et al. (2001) Gil-Hutton and Licandro (2001) Benecchi et al. (2011) Barucci et al. (2000) Benecchi et al. (2009) Benecchi et al. (2009) Doressoundiram et al. (2002) Peixinho et al. (2004) Benecchi et al. (2011) Tegler et al. (2003) Benecchi et al. (2009) Benecchi et al. (2009) Boehnhardt et al. (2002) Delsanti et al. (2006) Bauer et al. (2003) Jewitt (2009b) DeMeo et al. (2009) Boehnhardt et al. (2002) Benecchi et al. (2011) Tegler et al. (2003) Boehnhardt et al. (2002) Benecchi et al. (2011) Peixinho et al. (2004) Doressoundiram et al. (2002) Benecchi et al. (2011) Tegler et al. (2003) Bauer et al. (2003) Doressoundiram et al. (2003) Peixinho et al. (2004) Tegler et al. (2003) Fornasier (2007) Fornasier (2007) Tegler et al. (2003) Jewitt et al. (2007) Benecchi et al. (2009) Benecchi et al. (2009) Peixinho et al. (2004) Benecchi et al. (2011) Delsanti et al. (2001) McBride et al. (2003) Delsanti et al. (2006) Benecchi et al. (2011) Benecchi et al. (2009) Doressoundiram et al. (2001) Benecchi et al. (2009) Doressoundiram et al. (2002) Peixinho et al. (2004) Benecchi et al. (2011) Benecchi et al. (2011) Peixinho et al. (2004) Peixinho et al. (2004) Tegler et al. (2003) Doressoundiram et al. (2007) Rabinowitz et al. (2007) Fornasier (2007) Nr.

25

8 2 1

55638-2002 VE 56968-2000 SA 58534-Logos

95

92

58534-Logos+B 59358-1999 CL158 60454-2000 CH105 60458-2000 CM1 60458-2000 CM1 60558-Echeclus
14 14+ B

7 1 1 2 2 1

8 3 3 3

60608-2000 EE

173

60620-2000 FD 60621-2000 FE

8

8

63252-2001 BL

41

65150-2002 CA12 65225-2002 EK44 65489-Ceto 65489-Ceto+B 66452-1999 OF 66652-Borasisi

6

10 1 1 3 1 3

4

66652-Borasisi+B 69986-1998 WW24 69987-1998 WA 69988-1998 WA
25 31 1

7 1 3 1 2 1 10 1

69990-1998 WU3 73480-2002 PN34 76804-2000 QE


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 36 Table A.2. Continued Object 79360-1997 CS References Romanishin and Tegler (1999) Jewitt and Luu (2001) Davies et al. (2000) Boehnhardt et al. (2001) Delsanti et al. (2006) Benecchi et al. (2011) Jewitt et al. (2007) Barucci et al. (2000) Benecchi et al. (2009) Tegler and Romanishin (1998) Benecchi et al. (2009) Delsanti et al. (2001) Doressoundiram et al. (2002) Doressoundiram et al. (2002) Benecchi et al. (2011) Benecchi et al. (2009) Peixinho et al. (2004) Benecchi et al. (2011) Doressoundiram et al. (2005b) Doressoundiram et al. (2007) Jewitt et al. (2007) Sheppard (2010) Benecchi et al. (2009) Peixinho et al. (2004) Tegler et al. (2003) Doressoundiram et al. (2007) Jewitt et al. (2007) Peixinho et al. (2004) Doressoundiram et al. (2005b) Tegler et al. (2003) Jewitt et al. (2007) Peixinho et al. (2004) Bauer et al. (2003) Tegler et al. (2003) Doressoundiram et al. (2005a) Fornasier et al. (2004) Doressoundiram et al. (2007) DeMeo et al. (2009) Sheppard (2010) Rabinowitz et al. (2008) Fornasier (2007) Benecchi et al. (2011) Boehnhardt et al. (2002) Tegler and Romanishin (2003) Benecchi et al. (2011) Tegler and Romanishin (2000) Boehnhardt et al. (2002) Doressoundiram et al. (2002) Benecchi et al. (2011) Jewitt et al. (2007) Boehnhardt et al. (2002) Benecchi et al. (2011) Doressoundiram et al. (2001) Tegler et al. (2003) Benecchi et al. (2011) Sheppard (2010) Peixinho et al. (2004) Doressoundiram et al. (2007) Tegler et al. (2003) Benecchi et al. (2009) Benecchi et al. (2009) Barucci et al. (2005) Sheppard (2010) Rabinowitz et al. (2007) Rabinowitz et al. (2004) de Bergh et al. (2005) Rabinowitz et al. (2007) DeMeo et al. (2009) Rabinowitz et al. (2008) Nr.

29

79360-1997 CS29+ 79978-1999 CC158 79983-1999 DF9 80806-2000 CM1 82075-2000 YW

B

15 1 2 1 2

05

134

14

82155-2001 FZ

173

9

82158-2001 FP

185

7

83982-Crantor

17 2 1 1 4

84522-2002 TC

302 0

84709-2002 VW12 85627-1998 HP151 85633-1998 KR65 86047-1999 OY

3

5 3 3 6 1 1 1 3 6 2

86177-1999 RY

215

87269-2000 OO 87555-2000 QB 88269886118861190377-

67

243

2001 KF77 Teharonhia Teharonhia+B Sedna

90482-Orcus 90568-2004 GV

9


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 37 Table A.2. Continued Object 91133-1998 HK References Boehnhardt et al. (2001) McBride et al. (2003) Doressoundiram et al. (2002) Benecchi et al. (2011) Doressoundiram et al. (2001) Peixinho et al. (2004) Boehnhardt et al. (2002) Doressoundiram et al. (2005b) Bauer et al. (2003) Tegler et al. (2003) Fornasier et al. (2004) Doressoundiram et al. (2007) Rabinowitz et al. (2007) Fornasier (2007) Fornasier (2007) Fornasier (2007) Romanishin and Tegler (1999) Davies et al. (2000) Gil-Hutton and Licandro (2001) Jewitt and Luu (2001) Benecchi et al. (2011) Tegler and Romanishin (1998) Boehnhardt et al. (2002) Benecchi et al. (2011) Sheppard (2010) Tegler et al. (2003) Benecchi et al. (2011) Tegler et al. (2003) DeMeo et al. (2009) Rabinowitz et al. (2007) Romanishin et al. (2010) Benecchi et al. (2009) Tegler et al. (2003) Doressoundiram et al. (2007) DeMeo et al. (2009) Sheppard (2010) Rabinowitz et al. (2008) Benecchi et al. (2009) Benecchi et al. (2009) Rabinowitz et al. (2007) Fornasier (2007) Bauer et al. (2003) Doressoundiram et al. (2002) Peixinho et al. (2004) Benecchi et al. (2009) Benecchi et al. (2009) Fornasier (2007) Sheppard (2010) Doressoundiram et al. (2001) Benecchi et al. (2011) Benecchi et al. (2011) Buratti et al. (2003) Jewitt and Luu (2001) Buie et al. (2006) Buie et al. (2006) Buie et al. (2006) Buie et al. (2006) Doressoundiram et al. (2002) Delsanti et al. (2006) Benecchi et al. (2011) Benecchi et al. (2009) Benecchi et al. (2009) Romanishin et al. (2010) Jewitt et al. (2007) Rabinowitz et al. (2007) Trujillo et al. (2007) Carraro et al. (2006) DeMeo et al. (2009) Rabinowitz et al. (2007) Nr.

151

91205-1998 US43 91554-1999 RZ215 95626-2002 GZ32

6 2 1

99328-2001 UY123 105685-2000 SC51 111113-2001 VK85 118228-1996 TQ66

18 1 1 1

7 3 1 1 1 1 3 1 11 3 1 1 1 1 1 10 1 1 1 1 1 1 1 4 1 1 1

118379-1999 HC 1187021190681190701193151199512000 2001 2001 2001 2002

12

OM67 KC 7 7 KP 7 7 S Q7 3 KX1 4

119979-2002 WC1 120061-2003 CO1 120132-2003 FY 120178120347120347120348120453121725123509123509124729127546129772130391131695134340134340134340134340134860-

9

128

2003 OP32 Salacia Salacia+B 2004 TY364 1988 RE12 1999 XX143 2000 2000 2001 2002 1999 2000 2001 Pluto W K1 8 W K1 8 S B 173 XU9 3 HR 1 1 JG81 XS 2 5 4

3 3+ B

Pluto+B Pluto+C Pluto+D 2000 OJ6

7

134860-2000 OJ67+ B 135182-2001 QT322 136108-Haumea 136199-Eris

5 1 1 3 64


O. R. Hainaut et al.: Colours of Minor Bodies in the Outer Solar System, Online Material p 38 Table A.2. Continued Object 136472-Makemake 137294-1999 RE215 137295-1999 RB216 138537-2000 OK67 References Rabinowitz et al. (2007) Boehnhardt et al. (2002) Benecchi et al. (2011) Boehnhardt et al. (2002) Delsanti et al. (2001) Delsanti et al. (2004) Doressoundiram et al. (2002) Benecchi et al. (2011) Romanishin et al. (2010) DeMeo et al. (2009) Rabinowitz et al. (2008) DeMeo et al. (2009) DeMeo et al. (2009) Rabinowitz et al. (2008) Sheppard (2010) Tegler et al. (2003) Benecchi et al. (2011) Sheppard (2010) Benecchi et al. (2009) Benecchi et al. (2009) Delsanti et al. (2006) Fornasier (2007) Fornasier (2007) Benecchi et al. (2011) Doressoundiram et al. (2002) Benecchi et al. (2011) Peixinho et al. (2004) Green et al. (1997) Tegler and Romanishin (2003) Benecchi et al. (2011) Barucci et al. (2000) Romanishin et al. (1997) Peixinho et al. (2004) Snodgrass et al. (2010) Peixinho et al. (2004) Benecchi et al. (2011) Benecchi et al. (2011) Sheppard (2010) Boehnhardt et al. (2002) Benecchi et al. (2011) Sheppard (2010) Benecchi et al. (2009) Fornasier (2007) Fornasier (2007) Fornasier et al. (2004) Doressoundiram et al. (2007) DeMeo et al. (2009) Rabinowitz et al. (2008) Nr. 1 3 1

144897-2004 UX10 145451-2005 RM43 145452-2005 RN43 145453-2005 RR43 145480-2005 TB190 148209-2000 CR105 148780148780150642163135163216168700168703Al t j i r Al t j i r 2001 2002 2002 2000 2000 a a+B C Z 31 C T 22 E N6 8 GE 1 4 7 GP 1 8 3

5 1 2 2 3 1 3 1 1 1 1 1 1 5

181708-1993 FW

8 3 1 1 2 2 1 1 1 1

181855-1998 WT

31

181867-1999 CV118 181871-1999 CO153 181874-1999 HW11 181902-1999 RD 1823971829331923881929292089962001 2002 1996 2000 2003
215 7

QW 2 9 GZ 3 1 R D2 9 AT44 AZ 8 4

9