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Kalliope sings rock and metal

Chrysa Avdellidou, Ullas Bhat, Kieran Bujdoso, Marco Delbo, Michael
Marsset, Pierre Vernazza

► To cite this version:

Chrysa Avdellidou, Ullas Bhat, Kieran Bujdoso, Marco Delbo, Michael Marsset, et al. Kalliope sings rock and metal. Monthly Notices of the Royal Astronomical Society, 2025, 539, pp.3534-3550. 10.1093/mnras/staf640. insu-05099855

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# Kalliope sings rock and metal

Chrysa Avdellidou<sup>1,★</sup>, Ullas Bhat,<sup>1</sup> Kieran Bujdoso,<sup>1</sup> Marco Delbo,<sup>1,2</sup> Michael Marsset<sup>3</sup>
and Pierre Vernazza<sup>4</sup>

Accepted 2025 April 15. Received 2025 April 14; in original form 2025 March 16

## ABSTRACT

Asteroid (22) Kalliope is the densest known asteroid in the main belt, with a density of $\rho = 4.4 \pm 0.46$ g cm$^{-3}$, suggesting that it is differentiated. Kalliope has recently been identified as the parent body of a family of collisional fragments, which is located in the so-called ‘pristine zone’ of the outer main belt, between 2.825 and 2.955 au. Kalliope’s spectroscopic classification has been uncertain, but it has been broadly associated with iron meteorites. We combined visible reflectance spectra from the Gaia Data Release 3, visible SDSS spectrophotometry, and new near-infrared spectroscopic observations from the SpeX instrument at NASA’s Infrared Telescope Facility for 22 Kalliope family members, which were mostly classified as X or Xk-types. Considering the spectral slope and 0.9 µm absorption band variations, we divided the family members into three spectral groups. By analysing the spectra and geometric visible albedo data, we identified the best matches for Kalliope family members as iron and pallasite meteorites. The absence of crustal material among family members makes the nature of Kalliope’s parent body unclear, whether it was a fully or partially differentiated planetesimal and whether it originated in the inner or outer Solar system.

**Key words:** methods: observational – techniques: spectroscopic – minor planets, asteroids: general.

## 1 INTRODUCTION

During the early stages of the formation and evolution of the Solar system, <sup>26</sup>Al was still abundant. Its decay within newly accreted planetesimals served as the primary heating source, causing their initial material to melt and differentiate. With a half-life of 0.7 Myr, <sup>26</sup>Al is thought to have caused differentiation in planetesimals that accreted within the first few million years (Weiss & Elkins-Tanton 2013). According to the classical theory of full planetesimal differentiation, such bodies would form an iron-rich core, an olivine-dominated mantle, and a basaltic crust enriched in pyroxene (Weiss & Elkins-Tanton 2013). In cases of partial differentiation – typical of planetesimals that accreted slightly later – the crust would retain its original chondritic composition. This theory is supported by evidence showing that iron meteorites are older than chondritic ones (Kruijer et al. 2014; Hellmann et al. 2019; Hellmann, Van Orman & Kleine 2024). The detection and study of remnants of differentiated planetesimals can constrain models of early thermal evolution and help link them to known meteorites (Henke et al. 2012; Avdellidou et al. 2022; Trieloff, Hopp & Gail 2022).

The best locations to search for differentiation are families of asteroid fragments formed by large collisional events. Analysis of the physical properties of asteroid family members, such as visible (VIS) and near-infrared (NIR) spectra, geometric visible albedo ($p_V$), radar

albedos, and densities ($\rho$), provides insights into the composition and internal structure of their parent bodies. To date, the most compelling evidence for a differentiated planetesimal is asteroid (4) Vesta and its family, which formed following the impacts that created the Rheasilvia and Veneneia basins (Marchi et al. 2012). Using data from NASA’s Dawn mission (Russell et al. 2012), as well as ground-based spectra and $p_V$ measurements from space telescopes, Vesta and its family – classified as V-types in the Bus–DeMeo taxonomy (DeMeo et al. 2009) – have been linked to howardite–eucrite–diogenite meteorites, which correspond to the upper layers of a differentiated planetesimal.

Spectroscopic searches for differentiated material across the main belt, such as olivine-rich asteroids (classified as A-types), have yielded significant results. Ground-based NIR surveys, informed by Sloan Digital Sky Survey (SDSS) data, showed that olivine-rich material is rare in the main belt (0.16 per cent abundance for main-belt objects larger than 2 km in diameter) and unassociated with any known asteroid family (DeMeo et al. 2019). However, Gaia Data Release 3 data (Gaia DR3) led to the discovery of the first concentration of olivine-rich asteroids in the pristine zone of the outer main belt (Brož et al. 2013),<fnref n="1" /> associated with the (36256)

<footnote n="1"><sup>1</sup>School of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UK</footnote>

<footnote n="2"><sup>2</sup>Observatoire de la Côte d'Azur, Université Côte d'Azur, CNRS – Lagrange, 96 Bd de l'Observatoire, CS 34229, F-06304 NICE Cedex 4, France</footnote>

<footnote n="3"><sup>3</sup>European Southern Observatory (ESO), Alonso de Cordova 3107, 1900 Casilla Vitacura, Santiago, Chile</footnote>

<footnote n="4"><sup>4</sup>Laboratoire d'Astrophysique de Marseille, Aix-Marseille University, CNRS, LAM, 38 rue Frederic Joliot Curie, F-13388 Marseille, France</footnote>

<footnote n="1"><sup>1</sup>According to Broz et al. the pristine zone of the outer main belt is located between the 5:2 and 7:3 mean motion resonances with Jupiter. It was thought that due to the lack of very small asteroids compared to the other regions of the main belt this zone could preserve the initial asteroid belt population, hence its name.</footnote>

<footnote>*E-mail: ca337@leicester.ac.uk</footnote>
1999 XT17 asteroid family (Galinier et al. 2024). This family might have formed from the breakup of a partially differentiated parent body or an olivine-rich body. In the latter scenario, the parent body could represent mantle material from a differentiated planetesimal that fragmented elsewhere in the Solar system, with at least one of its fragments, e.g. the parent body of the (36256) 1999 XT17 family, dynamically implanted into the main belt, as suggested for the case of enstatite meteorites of type EL (Avdellidou et al. 2024). These findings indicate that planetesimal differentiation and its remnants in the main belt may be more common than previously thought.

In addition to basaltic and olivine material, metallic asteroids have also been identified. Large asteroids with high radar albedo, attributed to high surface densities from metal content, and/or high ρ, are considered likely remnants of differentiated planetesimal cores. Some of the planetesimals from the non-carbonaceous (NC) and carbonaceous chondrite (CC) reservoirs, which are thought to have been spatially separated in the protoplanetary disc, differentiated, producing iron cores and, consequently, iron meteorites (Kruijer et al. 2017). The study of iron meteorites provides evidence that planetesimals from the NC differentiated earlier than those from the CC reservoirs (Spitzer et al. 2021).

The forthcoming NASA's Psyche mission aims to characterize the main belt asteroid (16) Psyche, which resides in the pristine zone of the outer main belt and has been proposed to be an exposed metallic core of a differentiated body (Elkins-Tanton et al. 2022). Psyche has a high radar albedo of 0.34±0.08 (Shepard et al. 2021) and is spectroscopically classified as an Xk-type in the X-complex (DeMeo et al. 2009). High-precision volume measurements agree within uncertainties (Hanuš et al. 2017; Viikinkoski et al. 2018; Ferrais et al. 2020; Shepard et al. 2021), while recent mass measurements from close encounters with other asteroids suggest a moderate-to-high density of 4.17 g cm⁻³ (Farnocchia et al. 2024). NIR observations from both ground-based (Takir et al. 2017) and space-based (Jarmak et al. 2024) studies have detected a 3 µm hydration band. The latter could indicate that the surface of Psyche is not igneous, and thus the body was not fully differentiated. However, it remains unclear whether this hydration is endogenous or due to exogenous impact contamination (Avdellidou, Delbo' & Fienga 2018). Unfortunately, no collisional family has yet been detected around Psyche that could help characterize its different layers (Davis, Farinella & Marzari 1999). Other asteroids with high radar albedos are (69) Esperia, (92) Undine, (110) Lydia, (201) Penelope, (129) Antigone, (216) Kleopatra, (347) Pariana, (413) Edburga, and (758) Mancunia (Shepard et al. 2015), while asteroids with moderate-to-high density include (22) Kalliope, (30) Urania, and (216) Kleopatra (Vernazza et al. 2021). Apart from (22) Kalliope, none of these asteroids is associated with a known collisional family (Nesvorny, Broz & Carruba 2015; Nesvorny et al. 2024).

Asteroid (22) Kalliope is the densest known asteroid, with $\rho = 4.4 \pm 0.46$ g cm⁻³ (Ferrais et al. 2022). Its low radar albedo (0.18±0.05, Shepard et al. 2015) suggests a lower metal content on its surface compared to Psyche, with a surface density of 2.3 g cm⁻³. However, its very high bulk density indicates a differentiated and possibly a metal-rich interior. Kalliope is a binary system with Linus the smaller component of the system, supporting the hypothesis that its parent body experienced a major collisional event. This is because moons of large asteroids are expected to have formed from debris of giant impacts on their parent bodies (Brož et al. 2022, and references therein). Recently, Kalliope was associated with a family in the outer main belt (hereafter the Kalliope family) that contains 302 asteroids (Brož et al. 2022), previously identified as the San Marcello family (Nesvorny et al. 2015).

In this work, we investigated the properties of the Kalliope family. In Section 2, we present the available literature data and our new NIR observations. In Section 3, we describe the analysis in family identification, the spectral classification, and band analysis as well as the match with meteorites. Finally, in Section 4, we discuss our findings.

## 2 DATA

### 2.1 Literature data

Based on the Kalliope family membership defined by Brož et al. (2022), we initially searched for spectral and spectrophotometric data available in the literature. Of the 302 family members, only (22) Kalliope has a complete VNIR spectrum, obtained from various studies over the years (Zellner, Tholen & Tedesco 1985; Xu et al. 1995; Rivkin et al. 2000; Burbine et al. 2002; Bus & Binzel 2002; Bell et al. 2005; DeMeo et al. 2009; Fornasier et al. 2010; Ockert-Bell et al. 2010; Hardersen et al. 2011; Reddy & Sanchez 2016; Usui et al. 2019). The Gaia DR3 data set (Gaia Collaboration 2023) includes VIS reflectance spectra between 0.33 and 1.05 µm for over 60 000 Solar system objects. From this, we retrieved spectra for 37 members of the Kalliope family. The SDSS MOC4 data set (Ivezic et al. 2002) contains spectrophotometric data for 24 family members, providing magnitudes in five spectral bands (u', g', r', i', z') centred at 0.354, 0.477, 0.623, 0.763, and 0.913 µm, respectively (Carvano et al. 2010; Gayon-Markt et al. 2012). We converted the SDSS magnitudes into reflectance values following the procedure of DeMeo & Carry (2013), excluding the u' magnitudes due to their large associated errors. Additionally, we obtained proper orbital elements ($a_p, e_p, i_p$), diameters, and $p_V$ for Kalliope family members from the Minor Planet Physical Properties Catalogue<fnref n="2" /> (MP3C; Delbo et al. 2022). For objects with multiple diameter and $p_V$ values in the literature, we report a best value calculated as the weighted average (the weights are equal to the inverse of the square of the formal diameter uncertainties). For asteroids (22) and (14012) we performed a further data selection where $p_V$ derived using the NEATM (Harris 1998) is preferred over the STM (Lebofsky & Spencer 1989), since the latter neglects the effect of the thermal inertia (Delbó & Harris 2002), which is non-negligible for main belt asteroids (Delbo et al. 2015; Hung et al. 2022). Moreover, concerning WISE data we preferred values that were derived during the cryogenic phase of the mission, when the two longer wavelength bands, W3 and W4, were functional, thus providing better wavelength coverage for thermal model fitting. Diameters and $p_V$ were recovered for 48 of the 302 nominal family members, including 18 of the 22 asteroids observed in this study (Fig. 1; see Table A1 for details on references).

### 2.2 NIR observations

To characterize the Kalliope family, we conducted new spectroscopic observations in the NIR wavelength range for 22 family members, following the methodologies of our previous studies (Avdellidou et al. 2021, 2022; Galinier et al. 2024). The primary criterion for target selection was the availability of VIS data in Gaia DR3 to minimize the possible interlopers in the family and to cover the full wavelength range of diagnostic mineralogical features. Observations were performed using the SpeX instrument (Rayner et al. 2003) with the MORIS high-accuracy guider (Gulbis et al. 2011) at

<footnote n="2">²mp3c.oca.eu</footnote>
<figure><img src="image_3.png" /><figcaption>**Figure 1.** The *p*<sub>V</sub> distribution of the Kalliope family members (dark grey) and the ones we study here (light grey). We note that asteroid (21741) with the outlying *p*<sub>V</sub>=0.319 is an Sq-type.</figcaption></figure>

NASA's Infrared Telescope Facility. The instrument was configured in PRISM mode with a slit size of 0.8 × 15 arcsec, providing coverage across wavelengths from 0.7 to 2.5 µm and a spectral resolution of approximately 200 in a single set-up. For each target, we observed a nearby G2-type star within 250 arcsec of the asteroid to ensure optimal telluric correction. Additionally, when possible, we observed a well-studied solar analogue star at a similar airmass to correct for the spectral slope. SpeX data were reduced using the IDL-based spectral reduction tool Spextool (v4.1, Cushing, Vacca & Rayner 2004). A summary of the observation details is provided in Table A2.

3 ANALYSIS AND RESULTS

**3.1 Kalliope family V-shape identification and age**

At the time of the asteroid family formation, the asteroid fragments
are clustered in the proper orbital element space, but due to the
Yarkovsky effect, the *a*<sub>p</sub> values of the family fragments disperses
with time (Vokrouhlicky et al. 2015). The rate da<sub>p</sub>/dt is proportional
to the inverse diameter 1/D of the objects, with da<sub>p</sub>/dt > 0 for
the objects rotating prograde and da<sub>p</sub>/dt < 0 for those rotating
retrograde. Thus, over time, the members of the family form a ‘V-
shape’ in the (*a*<sub>p</sub>, 1/D) space. The V-shape identification method has
been successfully used to discover old families (Bolin et al. 2017;
Delbo et al. 2017; Delbo, Avdellidou & Morbidelli 2019; Ferrone
et al. 2023). Before identifying the V-shape for the Kalliope family,
the first step was to remove known families of the pristine zone (as
given in Nesvorny et al. 2015) to reduce disturbance in the V-shape
searching method caused by asteroids belonging to other families.
However, these family definitions, which were produced using a
hierarchical clustering method that links family fragments to the
core, are conservative, with several families having ‘haloes’ that are
not linked to them (see fig. 6 in Parker et al. 2008). To achieve a better
family removal from the pristine zone (see Fig. A1), we followed the
V-shape constrained hierarchical clustering method (see section 3.1
of Ferrone et al. 2023). Since the edges of a family V-shape are
formed by the members experiencing the maximum Yarkovsky drift,
if other effects are not considered, ideally all family members should
lie within this V-shape. By reclustering within a family’s V-shape
using a higher velocity cut-off, we can account for these haloes
while still minimizing false positives (see fig. 5 in Ferrone et al.

2023). In the (*a*<sub>p</sub>, 1/*D*) plane, the V-shape is given by the relation
1/*D* = *K*|*a*<sub>p</sub> − *a*<sub>c</sub>|, where *K* and *a*<sub>c</sub> are the slope and the vertex of
the V-shape, respectively. By shifting the V-shape by a factor *a*<sub>w</sub>, two
other V-shapes are generated such that an interior and exterior lobe
are formed given by the expressions 1/*D* = *K*(|*a*<sub>p</sub> − *a*<sub>c</sub>| ± *a*<sub>w</sub>). A
score function of *s* = *N*<sub>int</sub><sup>2</sup>/*N*<sub>ext</sub> is used to define the edges of the
family’s V-shape, where *N*<sub>int</sub> and *N*<sub>ext</sub> are the number of bodies in
the interior and exterior lobes, respectively (for further details see
Ferrone et al. 2023).

To find the slope and the vertex for the V-shape of the Kalliope
family, we performed a search in a large domain of K between 1
and 5 km⁻¹ au⁻¹ and a_c between 2.82 and 2.96 au. An enhancement
in scores around (K, a_c) ≈ (2 km⁻¹au⁻¹, 2.9 au) is visually evident
when using values for a_w between 0.01 and 0.02 au (see Fig. 2).
The value of a_p for (22) Kalliope is very close to this vertex, with
a_p Kalliope = 2.9096 au. We improved the slope and vertex of the
V-shape estimate by performing a narrower search in a restricted
domain of K between 1.6 and 2.4 km⁻¹ au⁻¹ and a_c between 2.9075
and 2.915 au. We created a 64x64 grid of K and a_c values in this
restricted domain and calculated the score for all combinations of K
and a_c for 30 values of a_w between 0.01 and 0.045 au.

Using the diameter uncertainties, we performed a Monte Carlo
analysis to propagate them to the V-shape of the Kalliope family.
To do this, we randomly generated 1000 diameter realizations for
the family-removed background population of the pristine zone
assuming a normal distribution centred at the mean diameter value
and with a standard deviation equal to the diameter uncertainties
as obtained by MP3C (see Section 2.1). With this, we obtain
30 000x(64x64) score maps. Each score map is then normalized
using Z-score normalization given as *s*<sub>*ij*</sub>' = (*s*<sub>*ij*</sub> − *μ*)/*σ*, where *s*
and *s*' are the scores before and after normalization respectively,
*ij* is the index in the 64x64 grid, and *μ* and *σ* are the mean and
standard deviation of scores in each score map, and the enhanced
region is found by taking all combinations of *K* and *a*<sub>*c*</sub> with *s*<sub>*ij*</sub>' > 2
(more than two standard deviations above the mean). The optimum
*K* and *a*<sub>*c*</sub> of the family in each score map is found by taking the
centre of enhancement calculated as the mean *K*<sub>*ij*</sub> and *a*<sub>*cij*</sub> for all *ij*
corresponding to *s*<sub>*ij*</sub>' > 2. This returned a collection of 30 000 *K*s and
*a*<sub>*c*</sub>s of Kalliope's V-shape. We report the mean of this distribution as
the best-fitting V-shape and the standard deviation as the uncertainty
with *K* = 2.069 ± 0.173 km⁻¹ au⁻¹ and *a*<sub>*c*</sub> = 2.910 ± 0.002 au.

Given the K-value and its uncertainty, it is possible to estimate the
age of the family. For this, we used equation (2) of Ferrone et al.
(2023), which is derived from Nesvorny et al. (2015). Assuming that
family members have ρ = 4.1 g cm⁻³ to maintain consistency with
Brož et al. (2022), we obtained an age of 3.64 ± 0.31 Gyr, which is
in agreement within the uncertainty with the age estimated by Brož
et al. (2022) using only Yarkovsky V-shape methods. Here, we note
that in theory, the collisional fragments of a differentiated body may
have a range of densities; thus, a more complex age estimation may
be needed. This may be due to the sampling of materials at different
depths of the parent body and also due to the re-accumulation of the
fragments into rubble piles, maintaining macroporosity that reduces
the initial material density.

**3.2 Spectra classification and band analysis**

An initial inspection of Gaia DR3 reflectance spectra revealed that
the family members belong to the X-complex (Fig. A2). The NIR
spectra were smoothed using a running average method with a 20
data point window. The outliers in each window were identified
by calculating their distance from the median and removing points
<figure><img src="image_4.png" /><figcaption>**Figure 2.** Left: the score map for detecting the V-shape for the Kalliope family. Right: the best-fitting V-shape of the Kalliope family and availability of physical properties. The majority of family members do not have measured diameters, thus we estimated the values using their H-mag and the average *p*<sub>V</sub> of the population that we observed.</figcaption></figure>

with distances greater than twice the median absolute deviation in the window. We followed the same procedure outlined in Avdellidou et al. (2022). Namely, we combined the NIR spectra with the VIS data from Gaia DR3 and, where applicable, the SDSS data (Fig. A3) at 0.85 µm. We then classified the reflectance spectra of each asteroid within the Bus–DeMeo taxonomy (DeMeo et al. 2009). This was achieved by performing reflectance curve matching, minimizing the χ² value between the observed spectrum and the Bus–DeMeo spectral class templates for each part of the spectrum independently, i.e. Gaia DR3, NIR observations, and SDSS. Finally, the χ² results for each object were summed to determine the two best classification matches (Table A3).

Of the 22 family members, 21 were classified as X-complex asteroids, while one was identified as Sq-type. Among the 21 X-complex asteroids, 18 were classified as X-types, two as Xk-types, and one as an Xc-type (Table A3).

Next, we investigated the presence of Band I (BI) and Band II (BII) in the spectra of X and Xk-type family members. We followed established methods (Vernazza et al. 2005) by adding an additional initial step of removing the slope in the spectra in the range 0.7–1.5 µm, making it easier to isolate the BI shoulder around 1.5 µm and the BI centre around 0.9 µm. We also calculated the BI depth as the relative difference between the BI continuum and the reflectance at the BI centre. The same was repeated for BII around 1.9 µm (Table A3). The tentative presence of BII should be treated with caution as it is located in the spectral region that is affected by the telluric band, while further investigation would be needed.

Based on spectral classification and the presence of the bands, we divided the asteroids into three groups: Group 1 includes 10 objects classified as X-types, characterized by red slopes and no evidence of BI and/or BII. Group 2 includes eight objects classified as X-types but with present BI (all objects) and BII (two objects). Finally, Group 3 includes two Xk-type objects that display BI (Table A3). Changes in spectral slope (that are not due to measurement artefacts; see Marsset et al. 2020) can be attributed to variations in grain sizes (Hasegawa et al. 2018) and/or to the exposure of fresher non-irradiated material (Fornasier et al. 2007; Avdellidou et al. 2021). Therefore, Groups 2 and 3 may correspond to the same composition but the surfaces of Group 2 may be either younger or covered by finer-grained material.

The spectra of each group were averaged by resampling the combined spectra at 750 linearly spaced wavelengths and taking the mean and standard deviation of the spectra at each wavelength sampled (Fig. 3). The general average of the Kalliope family was also computed in the same way (Fig. A4).

## 3.3 Meteorite matching

The spectroscopic X-complex encompasses a diversity of asteroid compositions (Cloutis et al. 1990; Gaffey, Reed & Kelley 1992; Vernazza et al. 2009; DeMeo et al. 2015). To gain a better understanding of the composition of the Kalliope family, we performed a meteorite matching analysis using reflectance spectra from the RELAB (Brown University) and the Planetary Spectrophotometer Facility (University of Winnipeg). This process followed the methodology described in Avdellidou et al. (2022), where the Athor family was uniquely linked to the EL enstatite chondrite meteorites.

For each asteroid, we conducted 10⁵ Monte Carlo simulations, where at each iteration, the asteroid’s reflectance spectrum was varied within its uncertainty and compared to all meteorite reflectance spectra. The meteorite spectra that represented 99 per cent of the cumulative probability of matching a given family member were then selected. Using these spectra, we identified potential meteorite types corresponding to members of the Kalliope family: iron, stony iron (pallasites and mesosiderites), and CM and C-type carbonaceous chondrites. We note that Psyche has been proposed as analogue to CB and CH meteorites (Shepard et al. 2021). However, in the case of Kalliope these meteorite types were not shortlisted during the matching process, although samples from both are included in the spectral data bases.

Curve matching alone is not always sufficient to establish definitive links between asteroids and meteorites. Asteroid *p*<sub>V</sub> and meteorite absolute reflectances must also be considered. To address this, we retrieved all meteorite spectra corresponding to the identified types from RELAB and PSF and applied a process similar to that used in Avdellidou et al. (2022). Specifically, when necessary, meteorite absolute reflectances were corrected to correspond to a phase angle, as outlined in equation (2) of Beck et al. (2021), to allow comparison
<figure><img src="image_5.png" /><figcaption>**Figure 3.** Average spectrum of each Kalliope family group and its standard deviation in comparison to the closest spectral classes from the Bus–DeMeo taxonomy.</figcaption></figure>

<figure><img src="image_6.png" /><figcaption>**Figure 5.** Composite plot of the available spectra for asteroid (22) Kalliope, compared with Bus–DeMeo spectral classes.</figcaption></figure>

**Figure 4.** 1.8/0.8 µm reflectance ratio versus the geometric visible albedo of the Kalliope family members and the average values from meteorite groups that achieved a curve-matching with Kalliope in the first step of the analysis. The properties of the Kalliope family members (as a whole and of each spectral group) and the iron/pallasites overlap, whereas the other meteorite classes are clearly distinct. Errorbars are $1\sigma$.

with asteroid geometric visible albedos. Following a well-established method (Cloutis et al. 2010), we created a plot of the 1.8/0.8 µm reflectance ratio against the 0.56 µm absolute reflectance for both meteorites and the average spectra of the three Kalliope family groups (Fig. 4). Our analysis indicates that Kalliope family members are best matched with iron or pallasite meteorites.

# 4 DISCUSSION

## 4.1 Family composition and planetesimal origin

Before this study, the asteroid (22) Kalliope was the only member of its family with known VIS and NIR spectra. The spectrum of Kalliope has shown some variability. Specifically, it has been classified either as X (DeMeo et al. 2009) or Xk-type (Fornasier et al. 2010). This ambiguous classification arises primarily from the detection or not of BI (Fig. 5). In this study, we observed NIR spectra of Kalliope family members that are classified as X (Group 1) and Xk-types (Group 3), while another population (Group 2) seems to have an intermediate spectra signature: the slope aligns with the X-type, but BI, characteristic of Xk-types is also detected. The literature and present spectra of asteroid Kalliope (see Fig. 5) are found to match with Group 1 (DeMeo et al. 2009; Hardersen et al. 2011), Group 2

(this study; Burbine & Binzel 2002; Fornasier et al. 2010; Ockert-Bell et al. 2010; Reddy & Sanchez 2016), and Group 3 (Bell et al. 2005). The presence on BI in Groups 1 and 3 is also stated in the original studies.

The presence of the three spectral groups we identified within the Kalliope family together with their identification on Kalliope surface itself explains asteroid Kalliope’s variability and supports the hypothesis that Kalliope is a metallic core with a low-Fe pyroxene mantle material veneer. In this scenario, Kalliope family members re-accumulated core and mantle material in varying proportions, accounting for the observed spectral diversity. The presence of pyroxene as the dominant mafic mineral over olivine can be inferred from the location of the BI centre (see fig. 3 in Cloutis et al. 1986). The variability is also reflected in the wide range of family members’ $p_V$ values, further supporting the conclusion that the Kalliope parent body was differentiated.

Additional evidence of differentiation comes from the low radar albedo of Kalliope, suggesting that the metal content on its surface is lower than what its bulk density indicates. Moreover, the anticorrelation between Kalliope’s radar albedo and millimetre emissivity points to spatial variability in its metal content (de Kleer et al. 2024).
Linus, Kalliope's moon, exhibits a lower metal content than Kalliope itself (Kleer et al. 2024).

Asteroid Kalliope has long been associated with laboratory spectra of iron meteorites (Fornasier et al. 2010). Our linking of the Kalliope family to iron and/or stony-iron (pallasite) meteorites corroborates this previous association and extends it to all observed family members. However, with current data, an origin from either the CC or NC reservoir of planetesimal formation cannot be inferred. Rivkin et al. (2000) detected a 3 µm hydration band, while Usui et al. (2019) detected a 2.78 µm band similar to what has been detected also on Psyche (Jarmak et al. 2024). These detections could suggest an initially primitive nature for (22) Kalliope, supporting its origin beyond the snow line and its formation within the CC reservoir. Considering the conclusions of Ferrais et al. (2022) and Kleer et al. (2024) we cannot argue against the case that (22) Kalliope has a surface of a differentiated body exposing material from different compositional layers of the parent body. In that case, the presence of the hydration band could be either due to an exogenous origin of hydration through impacts, as was proposed for (16) Psyche (Avdellidou et al. 2018), or due to the impact of the solar wind as it occurs on the lunar surface (Sunshine et al. 2009). In the latter case, if the surface of Kalliope has a silicate component then the detected absorption band can form when solar-wind protons interact with the oxygen-rich surfaces (Pieters et al. 2009). On the other hand, if the surface is metal-dominated then this mechanism should be less efficient due to much lower oxygen content but still may not be impossible. The rotational variation of the hydration band (Rivkin et al. 2000) can be explained either by an exogenous origin scenario via impacts or a breakup and re-accumulation scenario, resulting in an inhomogeneous surface with both metallic and silicate components.

Similarly, if the Kalliope family originated from a fully or partially differentiated planetesimal, crustal basaltic or chondritic material should be present among its members. The presence of the S-complex asteroid within the family members could indicate the existence of undifferentiated chondritic material from the crust, suggesting an origin from the NC reservoir in the inner Solar system. However, such a hypothesis is weak, as it is based on a single object that could be an interloper to the family.

## 4.2 Kalliope's daughters among NEAs

The near-Earth asteroid (6178) 1986 DA was observed to exhibit a red slope and a weak absorption band at 0.9 µm (Sanchez et al. 2021), indicating a potentially metallic composition. Asteroid (6178) has a high radar albedo, which varies significantly between 0.18 and 0.78 (Ostro et al. 1991). Assuming a diameter of 2.8 km (Harris & Drube 2014), this results in a wide range of densities, from 2.3 to 6.5 g cm⁻³. This large variation in radar albedo is more likely to be caused by surface irregularities on metallic asteroids than on rocky ones (Shepard et al. 2010). The irregular shape and the broad range of densities strongly suggest that (6178) could be a collisional fragment from a differentiated parent body, having reaccumulated materials of varying densities (and hence depths) from its parent body. Furthermore, asteroid (6178) originates from the outer main belt, with a 76 per cent probability of having escaped from the 5:2 mean motion resonance (MMR) with Jupiter (Sanchez et al. 2021). Near-Earth asteroids predominantly originate from collisional asteroid families. Considering the high likelihood of (6178) coming from the 5:2 MMR, Sanchez et al. (2021) proposed that one of the four families adjacent to the 5:2 resonance – Kalliope, Phaeo, Brasilia, and (15477) 1999 CG1 – could be its source. However, the Phaeo and (15477) 1999 CG1 families have very low *p*<sub>V</sub> values,

with family averages of 0.064±0.025 and 0.098±0.035, respectively, ruling them out as likely sources. The Brasilia family has a moderate average *p*<sub>V</sub> of 0.173± 0.060, but it has not been yet characterized. The spectrum of (6178) aligns well with Group 2 of the Kalliope family, exhibiting a red slope typical of X-types and a shallow 0.9 µm band (Fig. A5). Based on this evidence, we propose that the Kalliope family is the most plausible source of (6178), since it can feed that size of objects to the 5:2 MMR (see Fig. 2).

## 4.3 Note on Athor family's link to EL enstatite chondrite meteorites

The 3-Gyr-old Athor family was recently discovered (Delbo et al. 2019) and spectroscopically characterized as an Xc-type family (Avdellidou et al. 2022). Extensive spectroscopic investigations, combined with independent corroborating evidence, concluded that Athor is the source of the EL enstatite chondrite meteorites (Avdellidou et al. 2022). In the same study, the Kalliope family (then referred to as the San Marcello family), using the membership defined by Nesvorny et al. (2015), was found to have an average *p*<sub>V</sub> value of 0.177, which is within the range of EL meteorites. However, the Kalliope family was not further considered as the potential source of ELs for several reasons, including the potential metallic composition of its parent body, as EL meteorites cannot originate from a differentiated planetesimal. The NIR slopes (Fig. A6) and spectral classifications obtained in this work do not match those of the Athor family and the respective properties of the EL meteorites. Our present findings reinforce the conclusions of Avdellidou et al. (2022, 2024) – that the Athor family is the unique source of the EL meteorites.

## 5 CONCLUSIONS

We report the discovery of the first metallic asteroid family formed from the catastrophic collision of a differentiated parent body: the Kalliope family. The Kalliope family resides in the pristine zone of the outer main belt, exhibiting significant variability in geometric visible albedo values and some variability in X-complex spectral classes among its members. Kalliope family members are best matched with iron and/or stony-iron (pallasite) meteorites and are a source of metallic fragments that are delivered to near-Earth space. Future spectroscopic observations of smaller family members could reveal whether Kalliope is fully or partially differentiated. In the latter case, such observations may help determine whether it originated from the CC or NC population of planetesimals.

## ACKNOWLEDGEMENTS

We thank Sunao Hasegawa for his constructive comments that improved this work. CA and MD acknowledge support from ANR ORIGINS (ANR-18-CE31-0014). UB acknowledges funding from an STFC PhD studentship. This work has used data from the European Space Agency (ESA) Gaia mission (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work is based on data provided by the Minor Planet Physical Properties Catalogue (MP3C) of the Observatoire de la Côte d'Azur. CA and MD were Visiting Astronomers at the Infrared Telescope Facility, which is operated by the University of Hawaii under contract 80HQTR19D0030 with the
National Aeronautics and Space Administration. This research used the ALICE High Performance Computing facility at the University of Leicester.

DATA AVAILABILITY

Orbits, albedos, and diameters were obtained from the Minor Planet Physical Properties Catalogue (mp3c.oca.eu). The Gaia DR3 asteroid reflectance spectra were obtained from the archive website https://archives.esac.esa.int/gaia. The new raw NIR spectra can be found in the NASA IRTF Data Archive when they become publicly available https://irtfweb.ifa.hawaii.edu/research/irtf_data Archive.php. The reduced NIR spectra can be available upon request from the corresponding author.

REFERENCES

Alí-Lagoa V., Müller T. G., Usui F., Hasegawa S., 2018, A&A, 612, A85

Avdellidou C., Delbo' M., Fienga A., 2018, MNRAS, 475, 3419s

Avdellidou C. et al., 2021, A&A, 656, L18

Avdellidou C. et al., 2022, A&A, 665, L9

Avdellidou C., Delbo' M., Nesvorný D., Walsh K. J., Morbidelli A., 2024, Science, 384, 348

Beck P., Schmitt B., Potin S., Pommerol A., Brissaud O., 2021, Icarus, 354, 114066

Bell J. F., Owensby P. D., Hawke B. R., Brown R. H., Cruikshank D., Hartmann W. K., 2005, 52-color Asteroid Survey. NASA Planetary Data System, id. EAR-A-RDR-3-52COLOR-V2.1

Bolin B. T., Delbo M., Morbidelli A., Walsh K. J., 2017, Icarus, 282, 290

Brož M., Morbidelli A., Bottke W. F., Rozehnal J., Vokrouhlický D., Nesvorný D., 2013, A&A, 551, A117

Brož M., Ferrais M., Vernazza P., Ševeček P., Jutzi M., 2022, A&A, 664, A69

Burbine T. H., Binzel R. P., 2002, Icarus, 159, 468

Burbine T. H., McCoy T. J., Meibom A., Gladman B., Keil K., 2002, in Bottke W. F., Jr, et al. eds, Asteroids III. University of Arizona Press, Tucson, p. 653

Bus S. J., Binzel R. P., 2002, Icarus, 158, 106

Carvano J. M., Hasselmann P. H., Lazzaro D., Mothé-Diniz T., 2010, A&A, 510, A43

Cloutis E. A., Gaffey M. J., Jackowski T. L., Reed K. L., 1986, J. Geophys. Res., 91, 11641

Cloutis E. A., Gaffey M. J., Smith D. G. W., Lambert R. S. J., 1990, J. Geophys. Res., 95, 8323

Cloutis E. A., Hardersen P. S., Bish D. L., Bailey D. T., Gaffey M. J., Craig M. A., 2010, Meteorit. Planet. Sci., 45, 304

Cushing M. C., Vacca W. D., Rayner J. T., 2004, PASP, 116, 362

Davis D. R., Farinella P., Marzari F., 1999, Icarus, 137, 140

de Kleer K., Cambioni S., Butler B., Shepard M., 2024, Planet. Sci. J., 5, 230

DeMeo F. E., Carry B., 2013, Icarus, 226, 723

DeMeo F. E., Binzel R. P., Slivan S. M., Bus S. J., 2009, Icarus, 202, 160

DeMeo F. E., Alexander C. M. O., Walsh K. J., Chapman C. R., Binzel R. P., 2015, in Michel P. E., DeMeo F. Bottke W. F., eds, Asteroids IV. Arizona University Press, Tucson, p. 13

DeMeo F. E., Polishook D., Carry B., Burt B. J., Hsieh H. H., Binzel R. P., Moskovitz N. A., Burbine T. H., 2019, Icarus, 322, 13

Delbo M., Harris A. W., 2002, Meteorit. Planet. Sci., 37, 1929

Delbo M., Mueller M., Emery J. P., Rozitis B., Capria M. T., 2015, in Michel P., et al. eds, Asteroids IV. University of Arizona Press, Tucson, p. 107

Delbo M., Walsh K., Bolin B., Avdellidou C., Morbidelli A., 2017, Science, 357, 1026

Delbo M., Avdellidou C., Morbidelli A., 2019, A&A, 624, A69

Delbo M., Avdellidou C., Bruot N., Erard S., 2022, in European Planetary Science Congress, Palacio de Congresos de Granada, Spain. p. EPSC2022–323

Delbo M., Avdellidou C., Walsh K. J., 2023, A&A, 680, A10

Descamps P. et al., 2008, Icarus, 196, 578

Ďurech J. et al., 2011, Icarus, 214, 652

Elkins-Tanton L. T. et al., 2022, Space Sci. Rev., 218, 17

Farnocchia D., Fuentes-Muñoz O., Park R. S., Baer J., Chesley S. R., 2024, AJ, 168, 21

Ferrais M. et al., 2020, A&A, 638, L15

Ferrais M. et al., 2022, A&A, 662, A71

Ferrone S., Delbo M., Avdellidou C., Melikyan R., Morbidelli A., Walsh K., Deienno R., 2023, A&A, 676, A5

Fornasier S., Dotto E., Hainaut O., Marzari F., Boehnhardt H., De Luise F., Barucci M. A., 2007, Icarus, 190, 622

Fornasier S., Clark B. E., Dotto E., Migliorini A., Ockert-Bell M., Barucci M. A., 2010, Icarus, 210, 655

Gaffey M. J., Reed K. L., Kelley M. S., 1992, Icarus, 100, 95

Gaia Collaboration, 2023, A&A, 674, A35

Galinier M., Delbo M., Avdellidou C., Galluccio L., 2024, A&A, 683, L3

Gayon-Markt J., Delbo M., Morbidelli A., Marchi S., 2012, MNRAS, 424, 508

Gulbis A. A. S. et al., 2011, PASP, 123, 461

Hanuš J. et al., 2013, A&A, 559, A134

Hanuš J. et al., 2017, A&A, 601, A114

Hardersen P. S., Cloutis E. A., Reddy V., Mothé-Diniz T., Emery J. P., 2011, Meteorit. Planet. Sci., 46, 1910

Harris A. W., 1998, Icarus, 131, 291

Harris A. W., Drube L., 2014, ApJ, 785, L4

Hasegawa S. et al., 2018, PASJ, 70, 114

Hellmann J. L., Kruijter T. S., Van Orman J. A., Metzler K., Kleine T., 2019, Geochim. Cosmochim. Acta, 258, 290

Hellmann J. L., Van Orman J. A., Kleine T., 2024, Earth Planet. Sci. Lett., 626, 118518

Henke S., Gail H. P., Trieloff M., Schwarz W. H., Kleine T., 2012, A&A, 545, A135

Hung D., Hanuš J., Masiero J. R., Tholen D. J., 2022, Planet. Sci. J., 3, 56

Ivezic Z., Juric M., Lupton R. H., Tabachnik S., Quinn T., 2002, in Tyson J. A., Wolff S. C., eds, Proc. SPIE Conf. Ser. Vol. 4836, Survey and Other Telescope Technologies and Discoveries. Sidney. pp. 98

Jarmak S. G. et al., 2024, Planet. Sci. J., 5, 183

Knežević Ž., Milani A., 2003, A&A, 403, 1165

Kruijter T. S., Touboul M., Fischer-Gödde M., Bermingham K. R., Walker R. J., Kleine T., 2014, Science, 344, 1150

Kruijter T. S., Burkhardt C., Budde G., Kleine T., 2017, Proc. Natl. Acad. Sci., 114, 6712

Lebofsky L. A., Spencer J. R., 1989, in Binzel R. P., Gehrels T., Matthews M. S., eds, Asteroids II. University of Arizona Press, Tucson. p. 128

Marchi S. et al., 2012, Planet. Space Sci., 66, 87

Marchis F., Descamps P., Baek M., Harris A. W., Kaasalainen M., Berthier J., Hestroffer D., Vachier F., 2008, Icarus, 196, 97

Marchis F. et al., 2012, Icarus, 221, 1130

Marsset M. et al., 2020, ApJS, 247, 73

Masiero J. R. et al., 2011, ApJ, 741, 68

Masiero J. R., Mainzer A. K., Grav T., Bauer J. M., Cutri R. M., Nugent C., Cabrera M. S., 2012, ApJ, 759, L8

Nesvorny D., Broz M., Carruba V., 2015, in Michel P. et al., eds, Asteroids IV. University of Arizona Press, Tucson, p. 297

Nesvorny D., Roig F., Vokrouhlický D., Brož M., 2024, ApJS, 274, 25

Ockert-Bell M. E., Clark B. E., Shepard M. K., Isaacs R. A., Cloutis E. A., Fornasier S., Bus S. J., 2010, Icarus, 210, 674

Ostro S. J., Campbell D. B., Chandler J. F., Hine A. A., Hudson R. S., Rosema K. D., Shapiro I. I., 1991, Science, 252, 1399

Parker A., Ivezić Ž., Jurić M., Lupton R., Sekora M. D., Kowalski A., 2008, Icarus, 198, 138

Pieters C. M. et al., 2009, Science, 326, 568

Rayner J. T., Toomey D. W., Onaka P. M., Denault A. J., Stahlberger W. E., Vacca W. D., Cushing M. C., Wang S., 2003, PASP, 115, 362

Reddy V., Sanchez J. A., 2016, Reddy Main Belt Asteroid Spectra V1.0. NASA Planetary Data System, id. EAR-A-I0046-3-REDDYMBSPEC-V1.0
Rivkin A. S., Howell E. S., Lebofsky L. A., Clark B. E., Britt D. T., 2000, *Icarus*, 145, 351

Russell C. T. et al., 2012, *Science*, 336, 684

Sanchez J. A., Reddy V., Bottke W. F., Battle A., Sharkey B., Kareta T., Pearson N., Cantillo D. C., 2021, *Planet. Sci. J.*, 2, 205

Shepard M. K. et al., 2010, *Icarus*, 208, 221

Shepard M. K. et al., 2015, *Icarus*, 245, 38

Shepard M. K. et al., 2021, *Planet. Sci. J.*, 2, 125

Spitzer F., Burkhardt C., Nimmo F., Kleine T., 2021, *Earth Planet. Sci. Lett.*, 576, 117211

Sunshine J. M., Farnham T. L., Feaga L. M., Groussin O., Merlin F., Milliken R. E., A’Hearn M. F., 2009, *Science*, 326, 565

Takir D., Reddy V., Sanchez J. A., Shepard M. K., Emery J. P., 2017, *AJ*, 153, 31

Trieloff M., Hopp J., Gail H.-P., 2022, *Icarus*, 373, 114762

Usui F. et al., 2011, *PASJ*, 63, 1117

Usui F., Hasegawa S., Ootsubo T., Onaka T., 2019, *PASJ*, 71, 1

Vernazza P., Mothé-Diniz T., Barucci M. A., Birlan M., Carvano J. M., Strazzulla G., Fulchignoni M., Migliorini A., 2005, *A&A*, 436, 1113

Vernazza P., Binzel R. P., Rossi A., Fulchignoni M., Birlan M., 2009, *Nature*, 458, 993

Vernazza P. et al., 2021, *A&A*, 654, A56

Viikinkoski M. et al., 2018, *A&A*, 619, L3

Vokrouhlický D., Bottke W. F., Chesley S. R., Scheeres D. J., Statler T. S., 2015, in Michel P. et al., eds, University of Arizona Press, Tucson, p. 509

Weiss B. P., Elkins-Tanton L. T., 2013, *Annu. Rev. Earth Planet. Sci.*, 41, 529

Xu S., Binzel R. P., Burbine T. H., Bus S. J., 1995, *Icarus*, 115, 1

Zellner B., Tholen D. J., Tedesco E. F., 1985, *Icarus*, 61, 355

## APPENDIX A: TABLES AND FIGURES

<figure><img src="image_7.png" /><figcaption>**Figure A1.** The asteroid population of the pristine zone (with $p_V>0.12$ per cent) before (A) and after (B) family removal. Families are indicated by their number.</figcaption></figure>

<figure><img src="image_8.png" /><figcaption>**Figure A2.** Gaia DR3 spectral profile of Kalliope family. To calculate the family average we followed the method that was described in Delbo, Avdellidou & Walsh (2023). S-complex asteroid 21741 is excluded from the average.</figcaption></figure>
<figure><img src="image_9.png" /><figcaption>**Figure A3.** NIR spectra (black points) were obtained from our survey and are presented after we applied a 2σ clipping in order to eliminate the scattered data points inside the telluric bands (grey areas) by as much as possible. NIR spectra were combined with Gaia DR3 (red points) and SDSS (blue points), where available.</figcaption></figure>
<figure><img src="image_10.png" /><figcaption>**Figure A4.** Average spectrum of Kalliope family members and its standard deviation in comparison to the closest spectral classes from the Bus–DeMeo taxonomy.</figcaption></figure>

<figure><img src="image_11.png" /><figcaption>**Figure A5.** Comparison of NEAs (6178) and 2016 ED85 with Kalliope spectral Group 2. Asteroid 2016 ED85 is also proposed by Sanchez et al. (2021) to be a metallic NEA; however, its spectrum is much redder than Kalliope family and similar to primitive D-type asteroids. In addition, its orbit places it externally to the pristine zone and far from the 5:2 MMR. Radar and geometric visible albedo data are required to constrain its nature.</figcaption></figure>

<figure><img src="image_12.png" /><figcaption>**Figure A6.** NIR slopes of the Kalliope family members.</figcaption></figure>
<table><caption>**Table A1.** Orbits and physical properties of Kalliope family members are taken from mp3c.oca.eu. MP3C reports proper elements from 'The Asteroid Family Portal' of the Department of Astronomy, University of Belgrade, Serbia, where proper elements were computed numerically by means of a synthetic theory by Knežević & Milani (2003). Diameters, albedos, and their uncertainties originally reported in Descamps et al. (2008), Marchis et al. (2008), Usui et al. (2011), Đurech et al. (2011), Masiero et al. (2011), Masiero et al. (2012), Marchis et al. (2012), Hanuš et al. (2013), Hanuš et al. (2017), Alí-Lagoa et al. (2018). Refs. (a) Gaia Collaboration (2023), (b) Zellner et al. (1985), (c) Xu et al. (1995), (d) Bus & Binzel (2002), (e) Bell et al. (2005), (f) Fornasier et al. (2010), (g) Rivkin et al. (2000), (h) Burbine & Binzel (2002), (i) DeMeo et al. (2009), (j) Ockert-Bell et al. (2010), (k) Hardersen et al. (2011), (l) Reddy & Sanchez (2016), (m) Usui et al. (2019), and (n) This work.</caption><thead><tr><th>Number</th><th>Name</th><th>a<sub>p</sub></th><th>e<sub>p</sub></th><th>i<sub>p</sub></th><th>D<br>km</th><th>D<sub>err</sub><br>km</th><th>p<sub>V</sub></th><th>p<sub>Verr</sub></th><th>VIS</th><th>NIR</th><th>SDSS</th></tr></thead><tbody><tr><td>22</td><td>Kalliope</td><td>2.9096</td><td>0.0879</td><td>0.2182</td><td>154.16</td><td>1.4</td><td>0.173</td><td>0.0151</td><td>a,b,c,d,e,f</td><td>f,g,h,i,j,k,l,m,n</td><td>-</td></tr><tr><td>7481</td><td>San Marcello</td><td>2.9222</td><td>0.0767</td><td>0.2177</td><td>11.17</td><td>1.99</td><td>0.17</td><td>0.074</td><td>a</td><td>n</td><td>Y</td></tr><tr><td>12573</td><td>1999 NJ53</td><td>2.9399</td><td>0.0794</td><td>0.219</td><td>-</td><td>-</td><td>-</td><td>-</td><td>a</td><td>n</td><td>-</td></tr><tr><td>14012</td><td>Amedee</td><td>2.868</td><td>0.0843</td><td>0.2214</td><td>10.59</td><td>0.124</td><td>0.205</td><td>0.0096</td><td>a</td><td>n</td><td>-</td></tr><tr><td>14338</td><td>Shibakoukan</td><td>2.9445</td><td>0.0792</td><td>0.2181</td><td>8.85</td><td>0.058</td><td>0.247</td><td>0.0224</td><td>a</td><td>n</td><td>Y</td></tr><tr><td>16367</td><td>Astronomiasvecia</td><td>2.8647</td><td>0.0896</td><td>0.2233</td><td>5.85</td><td>0.23</td><td>0.247</td><td>0.0454</td><td>a</td><td>-</td><td>-</td></tr><tr><td>17845</td><td>1998 HY112</td><td>2.863</td><td>0.095</td><td>0.2175</td><td>10.14</td><td>0.54</td><td>0.13</td><td>0.021</td><td>a</td><td>n</td><td>-</td></tr><tr><td>17994</td><td>1999 JF70</td><td>2.9339</td><td>0.088</td><td>0.2183</td><td>10.82</td><td>0.128</td><td>0.199</td><td>0.0159</td><td>a</td><td>n</td><td>-</td></tr><tr><td>18733</td><td>1998 KV31</td><td>2.8703</td><td>0.0522</td><td>0.2169</td><td>-</td><td>-</td><td>-</td><td>-</td><td>a</td><td>-</td><td>-</td></tr><tr><td>21216</td><td>1994 UZ1</td><td>2.9029</td><td>0.0748</td><td>0.2168</td><td>8.33</td><td>0.125</td><td>0.161</td><td>0.0144</td><td>a</td><td>n</td><td>Y</td></tr><tr><td>21741</td><td>1999 RN162</td><td>2.8666</td><td>0.08</td><td>0.2299</td><td>5.39</td><td>0.118</td><td>0.319</td><td>0.0388</td><td>a</td><td>n</td><td>-</td></tr><tr><td>22087</td><td>2000 AZ175</td><td>2.8593</td><td>0.093</td><td>0.2176</td><td>-</td><td>-</td><td>-</td><td>-</td><td>a</td><td>n</td><td>-</td></tr><tr><td>22108</td><td>2000 PD</td><td>2.9465</td><td>0.0775</td><td>0.2201</td><td>10.49</td><td>0.123</td><td>0.232</td><td>0.0479</td><td>a</td><td>n</td><td>Y</td></tr><tr><td>24879</td><td>1996 KO5</td><td>2.9326</td><td>0.075</td><td>0.22</td><td>-</td><td>-</td><td>-</td><td>-</td><td>a</td><td>n</td><td>Y</td></tr><tr><td>25631</td><td>2000 AJ55</td><td>2.9486</td><td>0.0842</td><td>0.2178</td><td>6.8</td><td>0.312</td><td>0.2</td><td>0.0387</td><td>a</td><td>n</td><td>Y</td></tr><tr><td>26023</td><td>4538 P-L</td><td>2.8648</td><td>0.0565</td><td>0.2179</td><td>3.86</td><td>0.515</td><td>0.13</td><td>0.0341</td><td>-</td><td>-</td><td>-</td></tr><tr><td>26213</td><td>Ayani</td><td>2.8675</td><td>0.0947</td><td>0.2196</td><td>6.11</td><td>0.158</td><td>0.109</td><td>0.0106</td><td>a</td><td>-</td><td>-</td></tr><tr><td>27916</td><td>1996 VX1</td><td>2.8842</td><td>0.0808</td><td>0.2103</td><td>-</td><td>-</td><td>-</td><td>-</td><td>a</td><td>-</td><td>-</td></tr><tr><td>28089</td><td>1998 RD17</td><td>2.8576</td><td>0.0786</td><td>0.2205</td><td>6.66</td><td>0.2</td><td>0.19</td><td>0.0244</td><td>a</td><td>n</td><td>-</td></tr><tr><td>31064</td><td>1996 TP11</td><td>2.9438</td><td>0.075</td><td>0.2166</td><td>-</td><td>-</td><td>-</td><td>-</td><td>a</td><td>-</td><td>-</td></tr><tr><td>31709</td><td>1999 JD51</td><td>2.8583</td><td>0.096</td><td>0.2156</td><td>6.18</td><td>0.26</td><td>0.153</td><td>0.0235</td><td>a</td><td>n</td><td>-</td></tr><tr><td>32646</td><td>3010 P-L</td><td>2.9394</td><td>0.0789</td><td>0.2157</td><td>6.01</td><td>0.14</td><td>0.234</td><td>0.0332</td><td>a</td><td>-</td><td>Y</td></tr><tr><td>34565</td><td>2000 SY292</td><td>2.9439</td><td>0.0794</td><td>0.2219</td><td>5.95</td><td>0.264</td><td>0.138</td><td>0.0286</td><td>a</td><td>-</td><td>-</td></tr><tr><td>37292</td><td>2001 AN34</td><td>2.8732</td><td>0.0826</td><td>0.2204</td><td>5.57</td><td>0.327</td><td>0.172</td><td>0.029</td><td>a</td><td>-</td><td>-</td></tr><tr><td>37669</td><td>1994 TH1</td><td>2.9338</td><td>0.0785</td><td>0.2176</td><td>-</td><td>-</td><td>-</td><td>-</td><td>a</td><td>n</td><td>Y</td></tr><tr><td>41358</td><td>2000 AJ54</td><td>2.9343</td><td>0.0801</td><td>0.2191</td><td>8.79</td><td>0.271</td><td>0.173</td><td>0.0246</td><td>a</td><td>n</td><td>-</td></tr><tr><td>41930</td><td>2000 WO175</td><td>2.898</td><td>0.0757</td><td>0.2199</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td></tr><tr><td>46212</td><td>2001 FD162</td><td>2.9424</td><td>0.0734</td><td>0.2145</td><td>4.4</td><td>0.473</td><td>0.275</td><td>0.051</td><td>a</td><td>-</td><td>-</td></tr><tr><td>46272</td><td>2001 HO64</td><td>2.8575</td><td>0.079</td><td>0.2251</td><td>3.89</td><td>1.039</td><td>0.243</td><td>0.1324</td><td>-</td><td>-</td><td>-</td></tr><tr><td>47061</td><td>1998 XZ43</td><td>2.8797</td><td>0.0953</td><td>0.2191</td><td>7.52</td><td>0.155</td><td>0.187</td><td>0.026</td><td>a</td><td>n</td><td>-</td></tr><tr><td>47898</td><td>2000 GA47</td><td>2.9281</td><td>0.0825</td><td>0.2184</td><td>8.2</td><td>0.148</td><td>0.107</td><td>0.0069</td><td>a</td><td>n</td><td>-</td></tr><tr><td>50806</td><td>2000 FH28</td><td>2.9387</td><td>0.0788</td><td>0.2175</td><td>6.27</td><td>0.192</td><td>0.163</td><td>0.0088</td><td>a</td><td>n</td><td>Y</td></tr><tr><td>51259</td><td>2000 JY59</td><td>2.8746</td><td>0.0886</td><td>0.2242</td><td>-</td><td>-</td><td>-</td><td>-</td><td>a</td><td>-</td><td>Y</td></tr><tr><td>53350</td><td>1999 JD65</td><td>2.9414</td><td>0.0807</td><td>0.2166</td><td>5.22</td><td>1.343</td><td>0.196</td><td>0.0645</td><td>-</td><td>-</td><td>Y</td></tr><tr><td>54280</td><td>2000 JF47</td><td>2.9216</td><td>0.074</td><td>0.2139</td><td>4.14</td><td>0.519</td><td>0.345</td><td>0.0716</td><td>a</td><td>-</td><td>-</td></tr><tr><td>54908</td><td>2001 OY80</td><td>2.8724</td><td>0.0873</td><td>0.2211</td><td>9.04</td><td>0.197</td><td>0.18</td><td>0.0255</td><td>a</td><td>n</td><td>-</td></tr><tr><td>55418</td><td>Bianciardi</td><td>2.9364</td><td>0.0788</td><td>0.2183</td><td>-</td><td>-</td><td>-</td><td>-</td><td>a</td><td>-</td><td>-</td></tr><tr><td>62032</td><td>2000 RG58</td><td>2.858</td><td>0.077</td><td>0.223</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td></tr><tr><td>68222</td><td>2001 CQ47</td><td>2.8514</td><td>0.0795</td><td>0.2229</td><td>4.09</td><td>1.368</td><td>0.265</td><td>0.2092</td><td>a</td><td>-</td><td>-</td></tr><tr><td>71357</td><td>2000 AJ122</td><td>2.8393</td><td>0.0798</td><td>0.2296</td><td>-</td><td>-</td><td>-</td><td>-</td><td>a</td><td>-</td><td>Y</td></tr><tr><td>71396</td><td>2000 AV166</td><td>2.8804</td><td>0.0758</td><td>0.2169</td><td>4.5</td><td>1.02</td><td>0.2</td><td>0.0897</td><td>a</td><td>n</td><td>-</td></tr><tr><td>73446</td><td>2002 NX12</td><td>2.871</td><td>0.0745</td><td>0.2186</td><td>5.5</td><td>0.236</td><td>0.146</td><td>0.0322</td><td>-</td><td>-</td><td>-</td></tr><tr><td>82711</td><td>2001 PC45</td><td>2.8445</td><td>0.0806</td><td>0.2243</td><td>-</td><td>-</td><td>-</td><td>-</td><td>a</td><td>-</td><td>Y</td></tr><tr><td>82731</td><td>2001 PQ59</td><td>2.9359</td><td>0.08</td><td>0.2186</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td></tr><tr><td>82787</td><td>2001 QP22</td><td>2.947</td><td>0.0778</td><td>0.2179</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>Y</td></tr><tr><td>85417</td><td>1996 XQ3</td><td>2.875</td><td>0.0828</td><td>0.2108</td><td>3.07</td><td>0.622</td><td>0.225</td><td>0.0835</td><td>-</td><td>-</td><td>-</td></tr><tr><td>94038</td><td>2000 XX48</td><td>2.9438</td><td>0.0814</td><td>0.2178</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td></tr><tr><td>94199</td><td>2001 BM16</td><td>2.9176</td><td>0.0717</td><td>0.2125</td><td>4.84</td><td>0.274</td><td>0.173</td><td>0.0418</td><td>-</td><td>-</td><td>-</td></tr><tr><td>95912</td><td>2003 HN40</td><td>2.8958</td><td>0.085</td><td>0.2124</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td></tr><tr><td>104173</td><td>2000 EE83</td><td>2.9444</td><td>0.0805</td><td>0.2177</td><td>4.72</td><td>0.114</td><td>0.199</td><td>0.0391</td><td>a</td><td>-</td><td>-</td></tr><tr><td>110549</td><td>2001 TC101</td><td>2.9427</td><td>0.0801</td><td>0.2173</td><td>4.09</td><td>1.021</td><td>0.167</td><td>0.0482</td><td>-</td><td>-</td><td>-</td></tr><tr><td>111144</td><td>2001 VH99</td><td>2.8571</td><td>0.0685</td><td>0.2145</td><td>3.77</td><td>0.558</td><td>0.197</td><td>0.0482</td><td>a</td><td>-</td><td>Y</td></tr><tr><td>111199</td><td>2001 WW21</td><td>2.8895</td><td>0.0773</td><td>0.219</td><td>4.69</td><td>0.246</td><td>0.127</td><td>0.0125</td><td>-</td><td>-</td><td>-</td></tr><tr><td>112430</td><td>2002 NJ51</td><td>2.9301</td><td>0.0785</td><td>0.218</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>Y</td></tr><tr><td>112631</td><td>2002 PT77</td><td>2.8882</td><td>0.0785</td><td>0.2209</td><td>3.13</td><td>0.838</td><td>0.261</td><td>0.2436</td><td>-</td><td>-</td><td>Y</td></tr><tr><td>114664</td><td>2003 FO15</td><td>2.8705</td><td>0.0852</td><td>0.2172</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td><td>-</td></tr></tbody></table>
<table><caption>Table A1 – continued</caption><thead><tr><th>Number</th><th>Name</th><th>a<sub>p</sub></th><th>e<sub>p</sub></th><th>i<sub>p</sub></th><th>D<br>km</th><th>D<sub>err</sub><br>km</th><th>p<sub>V</sub></th><th>p<sub>Verr</sub></th><th>VIS</th><th>NIR</th><th>SDSS</th></tr></thead><tbody><tr><td>116170</td><td>2003 XW2</td><td>2.8527</td><td>0.0948</td><td>0.2215</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>Y</td></tr><tr><td>119834</td><td>2002 CK3</td><td>2.9317</td><td>0.0792</td><td>0.2158</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>Y</td></tr><tr><td>131265</td><td>2001 FD43</td><td>2.8563</td><td>0.086</td><td>0.2206</td><td>3.6</td><td>0.484</td><td>0.103</td><td>0.0305</td><td>—</td><td>—</td><td>—</td></tr><tr><td>140031</td><td>2001 SP64</td><td>2.9096</td><td>0.0838</td><td>0.2182</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>140108</td><td>2001 SA135</td><td>2.8799</td><td>0.0647</td><td>0.2159</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>141200</td><td>2001 XP203</td><td>2.8751</td><td>0.0758</td><td>0.2195</td><td>3.12</td><td>0.824</td><td>0.181</td><td>0.0445</td><td>—</td><td>—</td><td>—</td></tr><tr><td>150541</td><td>2000 ST142</td><td>2.8542</td><td>0.0924</td><td>0.2193</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>152341</td><td>2005 UE67</td><td>2.935</td><td>0.0797</td><td>0.2197</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>152606</td><td>1995 WL19</td><td>2.8871</td><td>0.0819</td><td>0.2222</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>Y</td></tr><tr><td>153086</td><td>2000 RX41</td><td>2.8673</td><td>0.0915</td><td>0.2238</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>154059</td><td>2002 CA168</td><td>2.8669</td><td>0.0969</td><td>0.221</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>159032</td><td>2004 TK67</td><td>2.8949</td><td>0.0819</td><td>0.2202</td><td>2.68</td><td>0.536</td><td>0.224</td><td>0.0426</td><td>—</td><td>—</td><td>Y</td></tr><tr><td>161396</td><td>2003 UR132</td><td>2.8854</td><td>0.0773</td><td>0.2186</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>161565</td><td>2005 AD62</td><td>2.8857</td><td>0.0758</td><td>0.2188</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>Y</td></tr><tr><td>161837</td><td>2006 XZ63</td><td>2.8697</td><td>0.0843</td><td>0.2189</td><td>2.68</td><td>0.494</td><td>0.246</td><td>0.1</td><td>—</td><td>—</td><td>Y</td></tr><tr><td>164369</td><td>2005 ED49</td><td>2.8743</td><td>0.086</td><td>0.2307</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>166751</td><td>2002 UZ2</td><td>2.8784</td><td>0.0948</td><td>0.2185</td><td>2.82</td><td>0.616</td><td>0.185</td><td>0.0393</td><td>—</td><td>—</td><td>Y</td></tr><tr><td>171194</td><td>2005 JJ27</td><td>2.8817</td><td>0.0761</td><td>0.2181</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>175716</td><td>1996 XW24</td><td>2.9304</td><td>0.077</td><td>0.2163</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>177128</td><td>2003 HU24</td><td>2.8829</td><td>0.0891</td><td>0.2223</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>178329</td><td>1995 SO36</td><td>2.8771</td><td>0.0769</td><td>0.2205</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>180960</td><td>2005 MX34</td><td>2.8697</td><td>0.0809</td><td>0.2208</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>181005</td><td>2005 NX48</td><td>2.8643</td><td>0.0706</td><td>0.2104</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>190114</td><td>2004 VH12</td><td>2.8784</td><td>0.0574</td><td>0.2276</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>196897</td><td>2003 TR6</td><td>2.8672</td><td>0.0853</td><td>0.2243</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>196974</td><td>2003 UC64</td><td>2.9204</td><td>0.0799</td><td>0.2192</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>203800</td><td>2002 TA110</td><td>2.9113</td><td>0.0806</td><td>0.2187</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>206688</td><td>2003 YO154</td><td>2.8751</td><td>0.0875</td><td>0.2236</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>216530</td><td>2001 OF111</td><td>2.8783</td><td>0.0751</td><td>0.2186</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>217802</td><td>2000 US96</td><td>2.8524</td><td>0.0589</td><td>0.2177</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>226746</td><td>2004 RF23</td><td>2.9413</td><td>0.0767</td><td>0.2179</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>227719</td><td>2006 DK197</td><td>2.8675</td><td>0.0836</td><td>0.2219</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>228284</td><td>2000 AJ176</td><td>2.8651</td><td>0.0659</td><td>0.2138</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>229227</td><td>2004 XE18</td><td>2.8427</td><td>0.081</td><td>0.2281</td><td>2.92</td><td>0.429</td><td>0.273</td><td>0.0828</td><td>—</td><td>—</td><td>—</td></tr><tr><td>232543</td><td>2003 SF129</td><td>2.845</td><td>0.0583</td><td>0.219</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>237969</td><td>2002 RA197</td><td>2.8441</td><td>0.0863</td><td>0.2273</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>245390</td><td>2005 GS131</td><td>2.9384</td><td>0.0856</td><td>0.2156</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>246484</td><td>2007 XY7</td><td>2.9405</td><td>0.0873</td><td>0.2189</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>248020</td><td>2004 FX40</td><td>2.8792</td><td>0.0791</td><td>0.222</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>250675</td><td>2005 OV25</td><td>2.9188</td><td>0.0821</td><td>0.2182</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>254820</td><td>2005 QQ131</td><td>2.8758</td><td>0.0663</td><td>0.2196</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>254988</td><td>2005 SY266</td><td>2.9433</td><td>0.0818</td><td>0.2178</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>261583</td><td>2005 XV10</td><td>2.871</td><td>0.0918</td><td>0.221</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>267786</td><td>2003 SN168</td><td>2.8852</td><td>0.0791</td><td>0.2217</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>277936</td><td>2006 OO</td><td>2.9383</td><td>0.0796</td><td>0.2155</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>279504</td><td>2011 AC52</td><td>2.8927</td><td>0.0834</td><td>0.2144</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>280659</td><td>2005 EZ20</td><td>2.9457</td><td>0.0768</td><td>0.2173</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>284640</td><td>2007 VM323</td><td>2.8631</td><td>0.0884</td><td>0.2216</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>285991</td><td>2001 SH15</td><td>2.8881</td><td>0.0828</td><td>0.2171</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>286015</td><td>2001 SU141</td><td>2.9305</td><td>0.076</td><td>0.2211</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>295381</td><td>2008 HR68</td><td>2.8466</td><td>0.0867</td><td>0.228</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>296463</td><td>2009 HT83</td><td>2.8579</td><td>0.077</td><td>0.219</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>296943</td><td>2010 DN45</td><td>2.9225</td><td>0.0762</td><td>0.2183</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>304544</td><td>2006 UP285</td><td>2.8574</td><td>0.0911</td><td>0.2184</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>305259</td><td>2007 YP14</td><td>2.9289</td><td>0.0817</td><td>0.2212</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>306388</td><td>1994 JX7</td><td>2.8777</td><td>0.0935</td><td>0.22</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>316440</td><td>2010 UL17</td><td>2.9235</td><td>0.0721</td><td>0.2127</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>318919</td><td>2005 UC62</td><td>2.9431</td><td>0.0836</td><td>0.2141</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>319447</td><td>2006 KJ65</td><td>2.9327</td><td>0.0775</td><td>0.2153</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>322682</td><td>1999 VY53</td><td>2.9</td><td>0.0788</td><td>0.2156</td><td>2.94</td><td>0.578</td><td>0.142</td><td>0.0468</td><td>—</td><td>—</td><td>—</td></tr><tr><td>325905</td><td>2010 UP57</td><td>2.8677</td><td>0.0927</td><td>0.2222</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>326039</td><td>2010 XM65</td><td>2.9088</td><td>0.0768</td><td>0.2174</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>327530</td><td>2006 BK137</td><td>2.8607</td><td>0.0565</td><td>0.22</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr></tbody></table>
<table><caption>Table A1 – continued</caption><thead><tr><th>Number</th><th>Name</th><th>a<sub>p</sub></th><th>e<sub>p</sub></th><th>i<sub>p</sub></th><th>D<br>km</th><th>D<sub>err</sub><br>km</th><th>p<sub>V</sub></th><th>p<sub>Verr</sub></th><th>VIS</th><th>NIR</th><th>SDSS</th></tr></thead><tbody><tr><td>328400</td><td>2008 SM30</td><td>2.8567</td><td>0.0855</td><td>0.2175</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>329280</td><td>1999 VD141</td><td>2.8545</td><td>0.0916</td><td>0.218</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>331508</td><td>1999 XC261</td><td>2.8944</td><td>0.0807</td><td>0.2152</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>331810</td><td>2003 SZ93</td><td>2.8717</td><td>0.0807</td><td>0.2311</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>333674</td><td>2008 TC52</td><td>2.9175</td><td>0.0702</td><td>0.2124</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>334501</td><td>2002 QJ107</td><td>2.9254</td><td>0.0823</td><td>0.2178</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>334874</td><td>2003 UJ212</td><td>2.898</td><td>0.0787</td><td>0.2199</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>338276</td><td>2002 TZ309</td><td>2.8584</td><td>0.0903</td><td>0.2217</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>351859</td><td>2006 RT104</td><td>2.8401</td><td>0.0892</td><td>0.2184</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>357736</td><td>2005 RJ40</td><td>2.9062</td><td>0.0785</td><td>0.2176</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>360902</td><td>2005 SX177</td><td>2.9336</td><td>0.0831</td><td>0.2192</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>361395</td><td>2006 VM140</td><td>2.8647</td><td>0.0667</td><td>0.2147</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>363398</td><td>2003 JC3</td><td>2.8792</td><td>0.0813</td><td>0.2077</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>366347</td><td>1998 OO2</td><td>2.9347</td><td>0.0836</td><td>0.212</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>368462</td><td>2003 SC101</td><td>2.9096</td><td>0.0829</td><td>0.2162</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>368809</td><td>2005 YP134</td><td>2.8716</td><td>0.0692</td><td>0.2175</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>378902</td><td>2008 UZ45</td><td>2.9402</td><td>0.0823</td><td>0.2196</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>380475</td><td>2003 WC101</td><td>2.8666</td><td>0.0693</td><td>0.2201</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>387687</td><td>2002 TW309</td><td>2.8851</td><td>0.0572</td><td>0.2218</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>396582</td><td>2000 RM78</td><td>2.8483</td><td>0.0964</td><td>0.2211</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>400928</td><td>2010 UA43</td><td>2.8816</td><td>0.0774</td><td>0.2207</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>403919</td><td>2011 YH68</td><td>2.8673</td><td>0.082</td><td>0.2179</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>404857</td><td>2014 KF17</td><td>2.863</td><td>0.0895</td><td>0.2225</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>409327</td><td>2004 TL367</td><td>2.9251</td><td>0.0824</td><td>0.217</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>410858</td><td>2009 RU46</td><td>2.934</td><td>0.0739</td><td>0.217</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>413399</td><td>2004 RB325</td><td>2.8416</td><td>0.0886</td><td>0.2281</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>414629</td><td>2009 VX24</td><td>2.8499</td><td>0.0904</td><td>0.2264</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>415732</td><td>1999 VY104</td><td>2.8566</td><td>0.0685</td><td>0.2127</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>420228</td><td>2011 HN45</td><td>2.861</td><td>0.075</td><td>0.2195</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>423037</td><td>2003 UK74</td><td>2.8932</td><td>0.0829</td><td>0.2185</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>426532</td><td>2013 RY64</td><td>2.9031</td><td>0.0781</td><td>0.2151</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>427317</td><td>2014 WH292</td><td>2.8484</td><td>0.0673</td><td>0.2116</td><td>3.81</td><td>0.866</td><td>0.101</td><td>0.0999</td><td>—</td><td>—</td><td>—</td></tr><tr><td>428933</td><td>2008 WG118</td><td>2.9138</td><td>0.08</td><td>0.2175</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>430340</td><td>2013 YV65</td><td>2.86</td><td>0.0794</td><td>0.2182</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>440414</td><td>2005 QY62</td><td>2.8699</td><td>0.0949</td><td>0.2213</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>444625</td><td>2006 VU170</td><td>2.8729</td><td>0.0834</td><td>0.2322</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>454161</td><td>2013 EL119</td><td>2.8622</td><td>0.0592</td><td>0.217</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>454418</td><td>2014 NJ57</td><td>2.8918</td><td>0.0924</td><td>0.2197</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>462450</td><td>2008 UR114</td><td>2.9234</td><td>0.0753</td><td>0.2168</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>464107</td><td>2014 WA428</td><td>2.9488</td><td>0.0778</td><td>0.2186</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>464304</td><td>2016 AU100</td><td>2.9034</td><td>0.0832</td><td>0.2184</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>464612</td><td>2016 CJ140</td><td>2.9261</td><td>0.0823</td><td>0.2177</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>472463</td><td>2015 BR416</td><td>2.9311</td><td>0.0767</td><td>0.2176</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>477110</td><td>2009 BQ177</td><td>2.9379</td><td>0.0881</td><td>0.2182</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>483146</td><td>2015 OA57</td><td>2.8489</td><td>0.0868</td><td>0.2189</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>485768</td><td>2012 CP24</td><td>2.9134</td><td>0.0775</td><td>0.2198</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>487450</td><td>2014 SQ24</td><td>2.8511</td><td>0.093</td><td>0.2199</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>488123</td><td>2015 VU107</td><td>2.8556</td><td>0.0691</td><td>0.2208</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>492163</td><td>2013 PA38</td><td>2.8481</td><td>0.0878</td><td>0.2202</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>501370</td><td>2013 YN45</td><td>2.8629</td><td>0.0812</td><td>0.2184</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>503314</td><td>2016 AO127</td><td>2.8625</td><td>0.0735</td><td>0.219</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>505186</td><td>2012 TW114</td><td>2.8466</td><td>0.0767</td><td>0.2195</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>505266</td><td>2012 VL1</td><td>2.861</td><td>0.0548</td><td>0.2145</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>507356</td><td>2011 VE23</td><td>2.9012</td><td>0.0833</td><td>0.2165</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>510489</td><td>2011 XA4</td><td>2.9105</td><td>0.0778</td><td>0.2169</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>515640</td><td>2014 MZ32</td><td>2.924</td><td>0.0813</td><td>0.2181</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>518825</td><td>2010 CM169</td><td>2.9476</td><td>0.0804</td><td>0.2176</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>520740</td><td>2014 QB474</td><td>2.8882</td><td>0.0788</td><td>0.2094</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>521968</td><td>2015 VG161</td><td>2.9001</td><td>0.0836</td><td>0.2138</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>523413</td><td>2017 DN122</td><td>2.929</td><td>0.0827</td><td>0.2184</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>526488</td><td>2006 RN91</td><td>2.8693</td><td>0.0859</td><td>0.2194</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>529676</td><td>2010 JN79</td><td>2.8543</td><td>0.0573</td><td>0.2169</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>532317</td><td>2013 QD93</td><td>2.8547</td><td>0.0769</td><td>0.2199</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr></tbody></table>
<table><caption>Table A1 – continued</caption><thead><tr><th>Number</th><th>Name</th><th>a<sub>p</sub></th><th>e<sub>p</sub></th><th>i<sub>p</sub></th><th>D<br>km</th><th>D<sub>err</sub><br>km</th><th>p<sub>V</sub></th><th>p<sub>Verr</sub></th><th>VIS</th><th>NIR</th><th>SDSS</th></tr></thead><tbody><tr><td>532409</td><td>2013 RP103</td><td>2.8636</td><td>0.0697</td><td>0.2171</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>533253</td><td>2014 DM154</td><td>2.8648</td><td>0.0702</td><td>0.2161</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>536305</td><td>2015 CX66</td><td>2.9245</td><td>0.0803</td><td>0.2135</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>538932</td><td>2016 HY24</td><td>2.8634</td><td>0.0715</td><td>0.2173</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>539027</td><td>2016 LN58</td><td>2.9225</td><td>0.0809</td><td>0.218</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>539263</td><td>2016 PJ72</td><td>2.8548</td><td>0.0859</td><td>0.2206</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>545524</td><td>2011 OP65</td><td>2.8435</td><td>0.0665</td><td>0.2128</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>546186</td><td>2010 TA176</td><td>2.8565</td><td>0.0893</td><td>0.2171</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>549084</td><td>2011 BA182</td><td>2.8449</td><td>0.0796</td><td>0.219</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>551844</td><td>2013 NO3</td><td>2.8816</td><td>0.082</td><td>0.2113</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>555164</td><td>2013 RS123</td><td>2.8487</td><td>0.0883</td><td>0.2185</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>559437</td><td>2015 DH12</td><td>2.9377</td><td>0.0744</td><td>0.2145</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>560485</td><td>2015 FY420</td><td>2.9077</td><td>0.0794</td><td>0.2191</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>562647</td><td>2016 AM128</td><td>2.9283</td><td>0.0743</td><td>0.2234</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>562836</td><td>2016 AW241</td><td>2.8636</td><td>0.0868</td><td>0.2295</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>563578</td><td>2016 CG314</td><td>2.8856</td><td>0.0775</td><td>0.209</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>563959</td><td>2016 EN202</td><td>2.9282</td><td>0.0785</td><td>0.218</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>564493</td><td>2016 GM217</td><td>2.932</td><td>0.0829</td><td>0.2156</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>566962</td><td>2018 VJ83</td><td>2.8538</td><td>0.0912</td><td>0.2194</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>569114</td><td>2005 JR174</td><td>2.9225</td><td>0.0818</td><td>0.2184</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>569157</td><td>2005 NR47</td><td>2.882</td><td>0.0793</td><td>0.2105</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>571468</td><td>2007 RY185</td><td>2.8515</td><td>0.0943</td><td>0.2199</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>573702</td><td>2009 RF48</td><td>2.8758</td><td>0.0831</td><td>0.2138</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>576659</td><td>2012 TG333</td><td>2.8458</td><td>0.0869</td><td>0.2202</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>576709</td><td>2012 UC23</td><td>2.8588</td><td>0.0799</td><td>0.2207</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>576969</td><td>2012 XW101</td><td>2.8748</td><td>0.0567</td><td>0.2212</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>581697</td><td>2015 KZ82</td><td>2.9135</td><td>0.0758</td><td>0.214</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>582004</td><td>2015 MO138</td><td>2.9427</td><td>0.0846</td><td>0.2116</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>582022</td><td>2015 NM</td><td>2.8475</td><td>0.0601</td><td>0.2191</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>583589</td><td>2016 KU5</td><td>2.8755</td><td>0.0564</td><td>0.2251</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>583772</td><td>2016 PJ3</td><td>2.9284</td><td>0.0767</td><td>0.2174</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>588322</td><td>2007 VQ154</td><td>2.868</td><td>0.085</td><td>0.2205</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>590269</td><td>2011 UF336</td><td>2.8444</td><td>0.0918</td><td>0.2205</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>590279</td><td>2011 UJ400</td><td>2.8972</td><td>0.0755</td><td>0.212</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>594884</td><td>2019 GH7</td><td>2.8576</td><td>0.0735</td><td>0.2206</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>598037</td><td>2008 CW225</td><td>2.9202</td><td>0.0807</td><td>0.2182</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>600315</td><td>2011 UB4</td><td>2.8555</td><td>0.0799</td><td>0.2267</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>601088</td><td>2012 UR184</td><td>2.9402</td><td>0.0778</td><td>0.2177</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>601468</td><td>2013 EL54</td><td>2.9018</td><td>0.0779</td><td>0.2141</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>604253</td><td>2015 NX26</td><td>2.9293</td><td>0.0726</td><td>0.2124</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>608932</td><td>2004 KB20</td><td>2.8679</td><td>0.0719</td><td>0.2213</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>609997</td><td>2005 VY137</td><td>2.9475</td><td>0.0758</td><td>0.2138</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>611557</td><td>2006 YF37</td><td>2.9235</td><td>0.0808</td><td>0.2165</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>611813</td><td>2007 FY54</td><td>2.9325</td><td>0.0792</td><td>0.218</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>616522</td><td>2005 WN116</td><td>2.8439</td><td>0.0831</td><td>0.2271</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>618644</td><td>2002 RC265</td><td>2.9482</td><td>0.0783</td><td>0.2188</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>628817</td><td>2016 EL258</td><td>2.9387</td><td>0.0849</td><td>0.218</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>632719</td><td>2008 UH232</td><td>2.895</td><td>0.0846</td><td>0.2098</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>634560</td><td>2011 UO420</td><td>2.8685</td><td>0.0755</td><td>0.22</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>1999 FS99</td><td>2.8585</td><td>0.0691</td><td>0.2156</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2000 SX379</td><td>2.8627</td><td>0.0692</td><td>0.2193</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2002 CB315</td><td>2.8653</td><td>0.0679</td><td>0.2163</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2005 TY83</td><td>2.8353</td><td>0.0574</td><td>0.2193</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2007 EQ145</td><td>2.9423</td><td>0.0823</td><td>0.2178</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2007 RU52</td><td>2.951</td><td>0.0835</td><td>0.2123</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2007 VX305</td><td>2.8639</td><td>0.0767</td><td>0.2195</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2007 VN347</td><td>2.9433</td><td>0.0784</td><td>0.2215</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2008 EW42</td><td>2.8554</td><td>0.0879</td><td>0.217</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2008 JF12</td><td>2.8908</td><td>0.0812</td><td>0.2112</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2008 SM319</td><td>2.8464</td><td>0.0785</td><td>0.2189</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2008 TC197</td><td>2.9085</td><td>0.0754</td><td>0.22</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2009 SA113</td><td>2.9236</td><td>0.0785</td><td>0.214</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2010 RS77</td><td>2.8651</td><td>0.0809</td><td>0.2156</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr></tbody></table>
<table><caption>**Table A1 – continued**</caption><thead><tr><th>Number</th><th>Name</th><th>a<sub>p</sub></th><th>e<sub>p</sub></th><th>i<sub>p</sub></th><th>D<br>km</th><th>D<sub>err</sub><br>km</th><th>p<sub>V</sub></th><th>p<sub>Verr</sub></th><th>VIS</th><th>NIR</th><th>SDSS</th></tr></thead><tbody><tr><td></td><td>2010 TT192</td><td>2.8773</td><td>0.0572</td><td>0.2196</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2010 YY3</td><td>2.9217</td><td>0.0816</td><td>0.2184</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2011 CW125</td><td>2.8849</td><td>0.0929</td><td>0.221</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2011 FR66</td><td>2.8444</td><td>0.0914</td><td>0.2253</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2012 BG62</td><td>2.8609</td><td>0.0514</td><td>0.2163</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2012 GG42</td><td>2.8627</td><td>0.0605</td><td>0.2159</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2012 XM102</td><td>2.8667</td><td>0.0667</td><td>0.219</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2013 HS125</td><td>2.9</td><td>0.0823</td><td>0.2125</td><td>2.7</td><td>0.797</td><td>0.042</td><td>0.035</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2013 VA36</td><td>2.8757</td><td>0.0623</td><td>0.2144</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2014 EG244</td><td>2.9018</td><td>0.0793</td><td>0.2187</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2014 MO66</td><td>2.9245</td><td>0.0704</td><td>0.2148</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2014 NZ22</td><td>2.8803</td><td>0.0961</td><td>0.2197</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2014 QN72</td><td>2.9201</td><td>0.0811</td><td>0.2181</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2014 QZ103</td><td>2.8804</td><td>0.0793</td><td>0.2202</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2014 QH248</td><td>2.8685</td><td>0.0775</td><td>0.231</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2014 QX473</td><td>2.8455</td><td>0.0884</td><td>0.2267</td><td>2.58</td><td>0.487</td><td>0.067</td><td>0.0217</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2014 RL31</td><td>2.8397</td><td>0.0776</td><td>0.2199</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2014 SV118</td><td>2.8694</td><td>0.0607</td><td>0.2142</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2014 XX3</td><td>2.8678</td><td>0.0847</td><td>0.2268</td><td>2.77</td><td>0.529</td><td>0.145</td><td>0.08</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 BR379</td><td>2.8641</td><td>0.0723</td><td>0.2104</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 DH253</td><td>2.9175</td><td>0.0812</td><td>0.2202</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 DO258</td><td>2.9376</td><td>0.0833</td><td>0.2101</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 GZ21</td><td>2.8972</td><td>0.0832</td><td>0.2117</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 HG4</td><td>2.9208</td><td>0.0792</td><td>0.2139</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 KB83</td><td>2.8766</td><td>0.0608</td><td>0.2136</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 KD83</td><td>2.9282</td><td>0.0826</td><td>0.2184</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 MP57</td><td>2.9119</td><td>0.0762</td><td>0.2126</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 SQ24</td><td>2.8384</td><td>0.0566</td><td>0.2171</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 TH272</td><td>2.8977</td><td>0.0754</td><td>0.2184</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 UH30</td><td>2.948</td><td>0.0787</td><td>0.2167</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 VU85</td><td>2.9493</td><td>0.0843</td><td>0.2181</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 XQ277</td><td>2.8702</td><td>0.0675</td><td>0.2141</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 XG358</td><td>2.8844</td><td>0.0771</td><td>0.2176</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 XB413</td><td>2.8506</td><td>0.0864</td><td>0.2156</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2016 AO141</td><td>2.9432</td><td>0.0744</td><td>0.2152</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2016 KT10</td><td>2.8781</td><td>0.0655</td><td>0.2138</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2016 QV66</td><td>2.8555</td><td>0.0891</td><td>0.2242</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2016 UF8</td><td>2.9407</td><td>0.0816</td><td>0.2079</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2017 BD122</td><td>2.8649</td><td>0.0683</td><td>0.2123</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2017 UJ49</td><td>2.9354</td><td>0.073</td><td>0.2148</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2018 LS17</td><td>2.9157</td><td>0.0797</td><td>0.2202</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2018 OK1</td><td>2.8595</td><td>0.0588</td><td>0.2186</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 VZ37</td><td>2.8743</td><td>0.0833</td><td>0.2283</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>628785</td><td>2016 CP87</td><td>2.9142</td><td>0.0713</td><td>0.2112</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>629730</td><td>2003 SE228</td><td>2.8698</td><td>0.0802</td><td>0.2316</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>630600</td><td>2006 CW31</td><td>2.8378</td><td>0.0757</td><td>0.221</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td>637756</td><td>2015 MZ90</td><td>2.86</td><td>0.0568</td><td>0.2142</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2007 TX459</td><td>2.9336</td><td>0.0807</td><td>0.2203</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2008 KB45</td><td>2.9167</td><td>0.0773</td><td>0.2185</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2010 FU140</td><td>2.8431</td><td>0.0798</td><td>0.2192</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2011 EX91</td><td>2.8771</td><td>0.0565</td><td>0.224</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2012 UY194</td><td>2.9263</td><td>0.0807</td><td>0.2179</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2014 HH165</td><td>2.9235</td><td>0.0815</td><td>0.2185</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2014 QV508</td><td>2.9193</td><td>0.0799</td><td>0.2184</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2014 WO214</td><td>2.8959</td><td>0.0756</td><td>0.2216</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2015 FH411</td><td>2.9096</td><td>0.0826</td><td>0.2171</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr><tr><td></td><td>2017 SM30</td><td>2.8657</td><td>0.0962</td><td>0.2159</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td><td>—</td></tr></tbody></table>
<table><caption>**Table A2.** NIR observations for 22 Kalliope family members.</caption><thead><tr><th>Asteroid</th><th>Date (UT)</th><th>SA trusted</th><th>SA local</th></tr></thead><tbody><tr><td>22Kalliope</td><td>24-04-2023</td><td>SA 102-1081</td><td>HD 111606</td></tr><tr><td>7481San Marcello</td><td>24-04-2023</td><td>SA 107-684</td><td>HD 156114</td></tr><tr><td>7481San Marcello</td><td>01-06-2023</td><td>SA 107-684</td><td>HD 151526</td></tr><tr><td>7481San Marcello</td><td>13-06-2023</td><td>SA 107-684</td><td>HD 151526</td></tr><tr><td>125731999NJ53</td><td>24-04-2023</td><td>SA 102-1081</td><td>HD 121610</td></tr><tr><td>14012Amedee</td><td>02-02-2023</td><td>Hyades 64</td><td>HD 19061</td></tr><tr><td>14338Shibakoukan</td><td>10-12-2023</td><td>SA 98-978</td><td>–</td></tr><tr><td>14338Shibakoukan</td><td>01-06-2024</td><td>SA 98-978</td><td>–</td></tr><tr><td>14338Shibakoukan</td><td>28-01-2024</td><td>SA 98-978</td><td>–</td></tr><tr><td>178451998HY112</td><td>13-10-2024</td><td>SA 115-271</td><td>HD 7716</td></tr><tr><td>179941999JF70</td><td>02-02-2023</td><td>SA 98-978</td><td>HD 62487</td></tr><tr><td>212161994UZ1</td><td>03-08-2023</td><td>SA 115-271</td><td>HD 217254</td></tr><tr><td>217411999RN162</td><td>03-08-2023</td><td>SA 115-271</td><td>HD 217254</td></tr><tr><td>220872000AZ175</td><td>06-12-2023</td><td>Hyades 64</td><td>–</td></tr><tr><td>221082000PD</td><td>02-02-2023</td><td>SA 102-1081</td><td>–</td></tr><tr><td>248791996KO5</td><td>22-10-2023</td><td>SA 93101</td><td>–</td></tr><tr><td>256312000AJ55</td><td>29-07-2023</td><td>SA 120-13333</td><td>HD 217890</td></tr><tr><td>280891998RD17</td><td>06-12-2023</td><td>Hyades 64</td><td>–</td></tr><tr><td>317091999JD51</td><td>24-04-2023</td><td>SA 102-1081</td><td>HD 121610</td></tr><tr><td>376691994TH1</td><td>01-10-2024</td><td>SA 115-271</td><td>HD 3083</td></tr><tr><td>413582000AJ54</td><td>22-10-2023</td><td>SA 93101</td><td>–</td></tr><tr><td>470611998XZ43</td><td>19-01-2024</td><td>SA 102-1081</td><td>HD 95331</td></tr><tr><td>470611998XZ43</td><td>28-01-2024</td><td>SA 102-1081</td><td>–</td></tr><tr><td>478982000GA47</td><td>19-01-2024</td><td>SA 98-978</td><td>–</td></tr><tr><td>508062000FH28</td><td>10-12-2023</td><td>Hyades 64</td><td>–</td></tr><tr><td>549082001OY80</td><td>02-02-2023</td><td>SA 102-1081</td><td>HD 76241</td></tr><tr><td>713962000AV166</td><td>06-12-2023</td><td>Hyades 64</td><td>–</td></tr></tbody></table>
<table><caption>**Table A3.** Spectroscopic classification of Kalliope family members in the Bus–DeMeo taxonomic scheme.</caption><thead><tr><th>Asteroid Number</th><th>Asteroid Designation</th><th>Class 1</th><th>Class 2</th><th>Group</th><th>BI centre ±0.01</th><th>BI depth ±0.002</th><th>BII centre</th><th>BII depth</th></tr></thead><tbody><tr><td>7481</td><td>San Marcello</td><td>X</td><td>Xk</td><td>1</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>12573</td><td>1999NJ53</td><td>X</td><td>T</td><td>1</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>14338</td><td>Shibakoukan</td><td>X</td><td>Xk</td><td>1</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>24879</td><td>1996KO5</td><td>X</td><td>Xk</td><td>1</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>25631</td><td>2000AJ55</td><td>X</td><td>Xk</td><td>1</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>37669</td><td>1994TH1</td><td>X</td><td>Xk</td><td>1</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>41358</td><td>2000AJ54</td><td>X</td><td>T</td><td>1</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>47061</td><td>1998XZ43</td><td>X</td><td>T</td><td>1</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>47898</td><td>2000GA47</td><td>X</td><td>Xk</td><td>1</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>50806</td><td>2000FH28</td><td>X</td><td>T</td><td>1</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>22</td><td>Kalliope</td><td>X</td><td>T</td><td>2</td><td>0.93</td><td>0.037</td><td>–</td><td>–</td></tr><tr><td>14012</td><td>Amedee</td><td>X</td><td>T</td><td>2</td><td>0.89</td><td>0.041</td><td>–</td><td>–</td></tr><tr><td>17845</td><td>1998HY112</td><td>X</td><td>T</td><td>2</td><td>0.93</td><td>0.023</td><td>–</td><td>–</td></tr><tr><td>17994</td><td>1999JF70</td><td>X</td><td>T</td><td>2</td><td>0.97</td><td>0.046</td><td>–</td><td>–</td></tr><tr><td>22108</td><td>2000PD</td><td>X</td><td>Xk</td><td>2</td><td>0.89</td><td>0.030</td><td>–</td><td>–</td></tr><tr><td>31709</td><td>1999JD51</td><td>X</td><td>T</td><td>2</td><td>0.93</td><td>0.007</td><td>–</td><td>–</td></tr><tr><td>54908</td><td>2001OY80</td><td>X</td><td>T</td><td>2</td><td>0.90</td><td>0.045</td><td>2.03±0.24</td><td>0.061±0.036</td></tr><tr><td>71396</td><td>2000AV166</td><td>X</td><td>T</td><td>2</td><td>0.89</td><td>0.022</td><td>1.97±0.06</td><td>0.056±0.001</td></tr><tr><td>22087</td><td>2000AZ175</td><td>Xk</td><td>Cgh</td><td>3</td><td>0.88</td><td>0.014</td><td>–</td><td>–</td></tr><tr><td>28089</td><td>1998RD17</td><td>T</td><td>Xk</td><td>3</td><td>0.87</td><td>0.061</td><td>–</td><td>–</td></tr><tr><td>21216</td><td>1994UZ1</td><td>Xc</td><td>Xe</td><td>–</td><td>–</td><td>–</td><td>–</td><td>–</td></tr><tr><td>21741</td><td>1999RN162</td><td>Sq</td><td>S</td><td>–</td><td>–</td><td>–</td><td>–</td><td>–</td></tr></tbody></table>

This paper has been typeset from a *TEX/LATEX* file prepared by the author.