Pith. sign in

REVIEW 3 major objections 5 minor 56 references

The trans-Neptunian object (84922) 2003 VS2 through stellar occultations

T0 review · 3 major / 5 minor · reviewed 2026-08-14 · deepseek-v4-flash

Pith's one-line read Occultations give the Kuiper Belt object 2003 VS2 a shape that fluid equilibrium cannot explain.

desk verdict Solid occultation size and astrometry for 2003 VS2, but the headline non-Jacobi shape claim is conditional on an unmeasured albedo/shape partition and should be softened. read the letter →

arxiv 1908.06645 v1 pith:JKYUPMDX submitted 2019-08-19 astro-ph.EP

classification astro-ph.EP
keywords bodyobjectoccultationsobtainedoccultationatmospheredataderive
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

Using three occultation campaigns, the paper reconstructs the shape of the plutino (84922) 2003 VS2, a Kuiper Belt object in Neptune's 2:3 resonance. The key measurement is the multi-chord event of November 7, 2014, whose projected limb is an ellipse with equivalent radius 282.4 km; combined with a $0.141 \pm 0.009$ mag rotational light-curve amplitude, it yields a triaxial ellipsoid with $a = 313.8 \pm 7.1$ km, $b = 265.5^{+8.8}_{-9.8}$ km, and $c = 247.3^{+26.6}_{-43.6}$ km. The paper's central claim is that these axes are not consistent with a Jacobi triaxial equilibrium figure, the shape expected for a homogeneous fluid body rotating with the same period. If correct, this provides a direct measurement showing that a body of roughly 548 km diameter can preserve a non-equilibrium shape, with consequences for internal strength and collisional history. The same data set places a 3-$\sigma$ upper limit of 1 microbar on a pure-nitrogen atmosphere and finds no confirmed rings or satellites.

What carries the argument

The load-bearing model is a triaxial ellipsoid with axes $a > b > c$ and aspect angle $\theta$ between the $c$-axis and the observer. Two relations carry the argument: the projection equation $b'^2 = c^2 \sin^2\theta + b^2 \cos^2\theta$, which maps the true axes onto the observed limb ellipse, and the light-curve relation $\Delta m = -1.25\,\log_{10}\left[\frac{1+\gamma^2\tan^2\theta}{1+(\gamma/\beta)^2\tan^2\theta}\right]$, which ties rotational brightness variation to the axis ratios $\beta = b/a$ and $\gamma = c/a$. Because the occultation occurred at a brightness maximum, the apparent semi-major axis equals the true long axis, removing one unknown; the two equations then constrain $\beta$, $\gamma$, and $\theta$. The final step is to compare the allowed $\beta$--$\gamma$ pairs with the Jacobi equilibrium ellipsoid sequence, and the absence of an intersection is what produces the paper's central non-Jacobi conclusion.

What would settle it

A second multi-chord stellar occultation at a substantially different rotational phase would measure the projected ellipse again; if the published axes and aspect angle cannot reproduce the new ellipse, the shape-albedo decomposition fails. More directly, a thermal-infrared light curve taken over the full 7.4-hour rotation would show whether the optical brightness variation is geometric or albedo-driven, because thermal emission tracks projected area rather than surface albedo.

Watch

Extended reading notes

Core claim

The occultation shadow on November 7, 2014 is best matched by an ellipse with apparent semi-major axis $a' = 313.8 \pm 7.1$ km and apparent oblateness $\epsilon' = 0.190$, for an equivalent radius of 282.4 km. Photometry obtained a few days later, folded at the known 7.4175285-hour rotation period, shows a peak-to-peak amplitude of $0.141 \pm 0.009$ mag and places the occultation near a brightness maximum, so the longest physical axis $a$ is perpendicular to the line of sight and equals $a'$. Combining the projection relation between the apparent minor axis and the true axes with the light-curve amplitude formula, the paper derives $a = 313.8 \pm 7.1$ km, $b = 265.5^{+8.8}_{-9.8}$ km, and $c = 247.3^{+26.6}_{-43.6}$ km, with the $c$-axis tilted $\theta = 65^{+15}_{-10}$ degrees to the line of sight. These axes give a spherical volume-equivalent diameter of $548.3^{+29.5}_{-44.6}$ km and an implied geometric albedo near 0.13. Because the derived ratios $\beta = b/a = 0.846$ and $\gamma = c/a = 0.788$ never intersect the Jacobi equilibrium sequence for any aspect angle, the paper concludes that the body is not a Jacobi triaxial equilibrium figure. Under the alternative assumption that the body is an oblate Maclaurin spheroid, the rotation period implies a density of $1400^{+1000}_{-300}$ kg m$^{-3}$.

Load-bearing premise

The inference about the $b$ and $c$ axes, and therefore the claim that the shape is not a Jacobi equilibrium figure, assumes that the entire $0.141 \pm 0.009$ mag rotational light-curve amplitude comes from the body's triaxial shape rather than from darker or brighter surface patches; the paper itself shows that if only $\Delta m = 0.015$ mag is shape-driven, a Jacobi solution with $\beta = 0.908$, $\gamma = 0.553$, and $\theta = 75^\circ$ is allowed.

Editorial extensions

If this is right

  • If the triaxial solution is correct, 2003 VS2 becomes a benchmark object whose size, shape, and rotation are known geometrically rather than assumed from thermal models.
  • Under the shape-driven light-curve interpretation, the surface albedo must be relatively uniform at the level of the 0.141 mag amplitude; if bright or dark patches contribute significantly, the axes must be re-derived.
  • The 3-sigma upper limit of about 1 microbar for a pure-nitrogen atmosphere, together with the absence of confirmed rings or satellites, places this object in the class of bare, atmosphere-less Kuiper Belt bodies.
  • The Maclaurin-spheroid assumption yields a density of $1400^{+1000}_{-300}$ kg m$^{-3}$, consistent with an ice-rock composition, but the density estimate is degenerate with the assumed oblate shape.
  • The three occultations provide accurate astrometric positions that improve the ephemeris of 2003 VS2, making future event predictions more reliable.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the no-albedo assumption survives later tests, the non-Jacobi result implies that a body of only about 550 km can hold a non-fluid shape against gravity and rotation, which would push the practical threshold for hydrostatic relaxation in icy Kuiper Belt objects upward and favor interiors with finite strength or rubble-pile structure.
  • The albedo-versus-shape degeneracy exposed by the paper's sensitivity test could be broken observationally: a thermal-infrared light curve at the same rotation period would be dominated by projected area rather than albedo spots and would independently verify the inferred axes.
  • The 0.09 flux drop seen in only the NTT light curve, if real, points either to a close stellar companion or to diffuse material near 2003 VS2; the paper's own data cannot distinguish these, so a future high-cadence occultation is the decisive observation.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 5 minor

Summary. This paper reports three stellar occultations by the plutino (84922) 2003 VS2: two single-chord events in December 2013 and March 2014, used for astrometry, and a multi-chord event on 2014 November 7 with four positive detections, used to fit an apparent limb ellipse with semi-axes a'=313.8±7.1 km and b'=254.8(+25.0/-21.7) km, position angle 5±7°, and area-equivalent diameter 564.8 km. From the rotational light curve (peak-to-peak amplitude 0.141±0.009 mag) and the adopted rotation period, the authors derive principal semi-axes a=313.8±7.1 km, b=265.5(+8.8/-9.8) km, and c=247.3(+26.6/-43.6) km, with the c axis inclined at θ=65(+15/-10)°, and conclude that the shape is not consistent with a Jacobi triaxial equilibrium figure. Under an alternative Maclaurin-oblate assumption they derive a density of 1400(+1000/-300) kg m^-3, and they report a geometric albedo of 0.131(+0.024/-0.013) in the main text (0.123(+0.015/-0.014) in the abstract). The data also set an upper limit of about 1 microbar for a pure N2 atmosphere and reveal a marginal secondary event in one NTT light curve that cannot be confirmed.

Significance. The observational core is solid and valuable: the multi-chord limb fit is carefully modelled using a sharp-edge model convolved with Fresnel diffraction, finite stellar diameter, and finite integration time, giving χ² per degree of freedom of 0.78; the chord timings are reported transparently; and the two single-chord events provide useful astrometric positions. If the derived 3D shape is correct, this is one of the few direct deconvolved size/shape measurements of a TNO and would be physically interesting for testing hydrostatic-equilibrium expectations. The paper also gives useful upper limits on an atmosphere and on rings or satellites. However, the headline non-Jacobi conclusion is conditional on the unmeasured assumption that the entire 0.141 mag light-curve amplitude is shape-induced; the authors' own sensitivity check in Appendix A shows that a modest albedo contribution would restore a Jacobi solution. The numeric inconsistency in the quoted albedo and the internal inconsistency in the Appendix A sensitivity example must be fixed before the central claim can be accepted as stated.

major comments (3)
  1. [Abstract, §4.1, Appendix A] The headline conclusion that 2003 VS2 is 'not consistent with a Jacobi triaxial equilibrium figure' rests entirely on the assumption that the full 0.141 ± 0.009 mag rotational light-curve amplitude is produced by the changing projected area of a uniform-albedo triaxial ellipsoid. The paper itself shows in Appendix A that if only Δm = 0.015 mag is shape-induced, a Jacobi solution with β = 0.908 and γ = 0.553 exists; the remaining 0.126 mag is an entirely plausible albedo contribution, as the paper's own Maclaurin alternative invokes a roughly 100 km spot covering ~16% of the area. The available photometry therefore cannot distinguish a shape-induced amplitude of 0.141 mag from one of about 0.015 mag. The abstract and Section 5 should state the non-Jacobi claim with an explicit caveat, for example 'under the assumption that the full light-curve amplitude is shape-induced', or the conclusion should be weakened accordingly.
  2. [Appendix A (Eq. A2)] The numerical Jacobi example quoted for Δm = 0.015 mag is internally inconsistent. With a' = 313.8 km, b' = 254.8 km, β = 0.908, γ = 0.553, and θ = 75°, Eq. (A2) gives γ ≈ 0.80, not 0.553; a value of θ ≈ 35° would satisfy the equation. Please correct the quoted θ and any dependent statements, and re-verify the corresponding figures, because the sensitivity test as printed does not demonstrably reproduce the observed limb while yielding a Jacobi solution.
  3. [Abstract vs. §4.1 and Table 10] The geometric albedo quoted in the Abstract (0.123(+0.015/-0.014)) differs from the value derived in Section 4.1 and listed in Table 10 (0.131(+0.024/-0.013)). These numbers cannot both be the result of the same calculation; please reconcile them and state which absolute magnitude and uncertainty were used.
minor comments (5)
  1. [Section 2.1] The sentence 'refine the the astrometric positions' contains a duplicated article; please correct it.
  2. [Abstract and Section 2.3] The sentence 'The rotational light curve present a peak-to-peak amplitude' should be 'presents a peak-to-peak amplitude'; the manuscript would benefit from a careful proofreading pass.
  3. [Appendix A] The typos 'Jabobi-shape object' and 'Suplemmentary Information' should be corrected, and 'tg2θ' should be typeset as tan^2 θ.
  4. [Section 3.2] The abbreviation 'pdf' for 'per degree of freedom' is nonstandard and could be confused with probability density function; consider using 'dof' instead.
  5. [Section 4.1 and Table 10] The distinction between the area-equivalent diameter of the projected ellipse (564.8 km) and the volume-equivalent spherical diameter of the 3D body (548.3 km) should be stated explicitly where both numbers appear, to avoid apparent inconsistency.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the shape is derived from independent occultation geometry and photometry, with the albedo/shape partition explicitly caveated.

full rationale

The paper's central derivation chain is observational and self-contained. Chord timings (Table 8) give a best-fit ellipse a' = 313.8 ± 7.1 km, b' = 254.8 km (Section 3.2), an independent geometric measurement. The 3D axes are then obtained from Eqs. A1-A3 of Appendix A, using the measured light-curve amplitude Δm = 0.141 ± 0.009 mag and the assumption that the occultation occurred near maximum brightness, justified by the folded photometry of Section 2.3. The rotational period P = 7.4175285 ± 0.00001 h is cited from Santos-Sanz et al. (2017), a self-citation with overlapping authors, but it is an independently measured external quantity, also consistent with the present photometric data, and it is not fitted to the shape result; hence it does not force the conclusion. The headline 'not consistent with a Jacobi equilibrium figure' is conditional on the explicitly stated assumption that the full Δm is shape-induced with negligible albedo contribution. The paper itself flags this in Appendix A: 'In fact we are assuming that some of the light curve contribution is due to VS2's shape and some due to albedo variation in the surface. When we try values for Δm smaller than 0.141 the lines in Fig. 12 will move to the right... For Δm = 0.015 mag we find a Jacobi solution with β = 0.908 (b = 284.9 km), γ = 0.553 (c = 173.5 km) and θ = 75°.' This is a sensitivity analysis of a modeling assumption, not a circular reduction: the size, ellipse, albedo, and density estimates follow from distinct observable inputs (occultation geometry, photometry amplitude, period, absolute magnitude). No equation is defined in terms of the quantity it is used to predict, and no fitted parameter is renamed as a prediction. Therefore the appropriate finding is no significant circularity.

Assumptions & free parameters 6 free parameters · 6 assumptions · 0 invented entities

The fitted ellipse parameters and light-curve amplitude are standard measurements for this technique. The load-bearing interpretive assumptions are that the occultation occurred at rotational maximum and that the light curve is shape-dominated; these are stated in the paper but are not independently verified. No invented entities are introduced.

free parameters (6)
  • a' apparent semi-major axis of the limb ellipse = 313.8 ± 7.1 km
    Fitted to the 8 chord extremities from the four positive detections of the 2014-11-07 occultation (Section 3.2, Table 10).
  • b' apparent semi-minor axis of the limb ellipse = 254.8 (+25.0/-21.7) km
    Fitted oblateness epsilon' = 0.190 (+0.052/-0.060) to the same chords; b' is derived from a' and epsilon'.
  • P' position angle of the apparent pole = 5 ± 7 deg
    Fifth free parameter in the ellipse fit (Section 3.2).
  • (f_c, g_c) center offsets relative to ephemeris = (-1558.1 ± 8.1, -634.6 ± 11.0) km
    Ephemeris offset fitted in the ellipse model (Table 10).
  • Delta m rotational light curve peak-to-peak amplitude = 0.141 ± 0.009 mag
    Peak-to-peak amplitude from a second-order Fourier fit to 97 photometric images over three nights (Section 2.3).
  • theta aspect angle of the c-axis = 65 (+15/-10) deg
    Chosen so that the triaxial solution satisfies the joint constraints of the occultation ellipse and light-curve amplitude (Appendix A).
assumptions (6)
  • domain assumption Limb is a perfect ellipse
    The multi-chord fit assumes an elliptical limb, following Braga-Ribas et al. (2013) and Ortiz et al. (2017); local topographic deviations would bias a' and b'.
  • domain assumption Occultation happened at rotational maximum so a' = a
    Stated in Section 4.1: the light curve phase puts the 2014 occultation near maximum brightness, so the projected major axis equals the true 3D long axis, which is needed to derive b and c.
  • domain assumption Light curve amplitude is entirely shape-induced in the reference triaxial solution
    Eq. A3 (Sicardy et al. 2011) maps Delta m to axis ratios assuming a homogeneous triaxial body without albedo spots; Appendix A shows small albedo contributions change the Jacobi conclusion.
  • standard math Jacobi/Maclaurin equilibrium theory describes a strengthless fluid body
    The comparison to Jacobi ellipsoids uses Chandrasekhar (1969, 1987) integrals, an externally established theory, not derived in this paper.
  • domain assumption Rotation period of 7.4175285 h is correct and the light curve is stable across the 8 days from occultation to photometry
    The phase is computed by folding new photometry with the period from Santos-Sanz et al. (2017); any period drift would move the phase away from maximum and alter the a' = a identification.
  • domain assumption Star flux drops to zero during occultation; no residual light from the TNO
    Assumed in Section 3 when normalizing light curves; if the TNO contributed significant flux, the chord extremities would shift.

how reviews work

0 comments
Cite this review

Pith. "Pith review of The trans-Neptunian object (84922) 2003 VS2 through stellar occultations." pith.science (2026). https://pith.science/paper/JKYUPMDX

@misc{pith2026190806645,
  author       = {Pith},
  title        = {Pith review of: The trans-Neptunian object (84922) 2003 VS2 through stellar occultations},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/JKYUPMDX}},
  note         = {Machine review of arXiv:1908.06645}
}
abstract

We present results from three world-wide campaigns that resulted in the detections of two single-chord and one multi-chord stellar occultations by the Plutino object (84922) 2003~VS$_2$. From the single-chord occultations in 2013 and 2014 we obtained accurate astrometric positions for the object, while from the multi-chord occultation on November 7th, 2014, we obtained the parameters of the best-fitting ellipse to the limb of the body at the time of occultation. We also obtained short-term photometry data for the body in order to derive its rotational phase during the occultation. The rotational light curve present a peak-to-peak amplitude of 0.141 $\pm$ 0.009 mag. This allows us to reconstruct the three-dimensional shape of the body, with principal semi-axes $a = 313.8 \pm 7.1$ km, $b = 265.5^{+8.8}_{-9.8}$ km, and $c = 247.3^{+26.6}_{-43.6}$ km, which is not consistent with a Jacobi triaxial equilibrium figure. The derived spherical volume equivalent diameter of $548.3 ^{+29.5}_{-44.6}$ km is about 5\% larger than the radiometric diameter of 2003~VS$_2$ derived from Herschel data of $523 \pm 35$ km, but still compatible with it within error bars. From those results we can also derive the geometric albedo ($0.123 ^{+0.015}_{-0.014}$) and, under the assumption that the object is a Maclaurin spheroid, the density $\rho = 1400^{+1000}_{-300}$ for the plutino. The disappearances and reappearances of the star during the occultations do not show any compelling evidence for a global atmosphere considering a pressure upper limit of about 1 microbar for a pure nitrogen atmosphere, nor secondary features (e.g. rings or satellite) around the main body.

Figures

Figures reproduced from arXiv: 1908.06645 by the authors.

Figure 1
Figure 1. Post-occultation map for the December 12, 2013 occultation. North is up and East is right. Blue lines repre￾sent the object equivalent diameter from the November 07, 2014 occultation of 564.8 km. Red dots represent the posi￾tion of the center of the body spaced every 30 seconds, the bigger dot corresponding to 20:10:44 UTC. Direction of the shadow is shown by the arrow at the right corner. Green dot is the site posi… view at source ↗
Figure 2
Figure 2. Post-occultation map for the March 04, 2014 oc￾cultation. North is up and East is right. Blue lines represent the object equivalent diameter from the November 07, 2014 occultation of 564.8 km. Red dots represent the position of the center of the body spaced every 30 seconds, the bigger dot corresponding to 19:55:54 UTC. Direction of the shadow is shown by the arrow at the right corner. Green dot is the site position… view at source ↗
Figure 5
Figure 5. Normalized light curves of the positive detec￾tions of the stellar occultations – see Tables 4 and 5 for sites details. Top: single-chord event in December 12, 2013; Cen￾ter: single-chord event in March 04, 2014, showing the de￾tection with the two telescopes at the same site; Bottom: multi-chord event on November 2014. Chords are shifted in flux for better visualization. Vertical lines are the uncertain￾ties in pho… view at source ↗
Figures from the paper (9 more)
Figure 6
Figure 6. Figure 6: Best fit for the star disappearance (left) and reappearance (right) instants of the single-chord events – see [PITH_FULL_IMAGE:figures/full_fig_p011_6.png]
Figure 7
Figure 7. Figure 7: Best fit for the star disappearance (left) and reap￾pearance (right) instants of the multi-chord event of Novem￾ber 07, 2014 – see [PITH_FULL_IMAGE:figures/full_fig_p013_7.png]
Figure 8
Figure 8. Figure 8: Occultation chords (blue) and their uncertainties (red) from the multi-chord event of November 2014 with the best elliptical fit (black). The offsets in both axis are with respect to ephemeride positions obtained using JPL#30 and DE431. The arrow shows the direction of…
Figure 9
Figure 9. Figure 9: Light curve from the single-chord stellar occulta￾tion of March 04, 2014 obtained at Wise Observatory (black) and the two models for the isothermic pure nitrogen (red) and a Pluto-like (blue) atmospheres within a 3σ limit. particular value. The other model is a N2 atmo…
Figure 10
Figure 10. Figure 10: Light curve from the multi-chord stellar occul￾tation of November 07, 2014 obtained at La Silla/NTT. All the flux drops in the curve are due to the star being too close to the edge of the CCD or being influenced by the bad row of pixels in the center of the CCD. Note …
Figure 11
Figure 11. Figure 11: Relation between β = b/a and γ = c/a obtained using eq. A2. Black lines correspond to a value of θ between 5 and 90 degrees (from left to right), every 5 degrees. Orange line are the values for β = γ. Red dotted vertical line is the value of β 0 = 0.811, observed in o…
Figure 12
Figure 12. Figure 12: Relation between β = b/a and γ = c/a obtained using eq. A4. Black lines correspond to a value of θ between 0 and 90 degrees (from left to right), every 5 degrees. Orange line are the values for β = γ. Red dotted vertical line is the value of β 0 = 0.811, observed in o…
Figure 13
Figure 13. Figure 13: Relation between β = b/a and γ = c/a combining eq. A2 (black dotted lines – as in [PITH_FULL_IMAGE:figures/full_fig_p019_13.png]
Figure 14
Figure 14. Figure 14: Relation between  and density for a Maclaurin object with rotation period of 7.4175285 hours (black line). The oblateness obtained for VS2 (blue horizontal full and dotted lines) gives limits for the minimum value of the density of 1.4 g cm−3 . Blue dotted lines repr…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

56 extracted references · 55 canonical work pages

  1. [1]

    L.; et al., 2016, A&A, V

    Alvarez-Candal, A.; Pinilla-Alonso, N.; Ortiz, J. L.; et al., 2016, A&A, V. 586, id.A155

  2. [2]

    J., Ortiz, J

    Anglada, G., Amado, P. J., Ortiz, J. L., et al., 2017, ApJL, 850, L6 Assafin, M.; Camargo, J. I. B.; Vieira Martins, R.; et al., 2010, A&A, V. 515 Assafin, M.; Vieira-Martins, R.; Camargo, J. I. B.; et al., 2011, GAIA FUN-SSO workshop proccedings, 85, gfun.conf Assafin, M.; Camargo, J. I. B.; Vieira Martins, R.; et al., 2012, A&A, V. 541

  3. [3]

    M.; Brown, M

    Barkume, K. M.; Brown, M. E.; & Schaller, E. L., 2008,

  4. [4]

    A.; Dotto, E

    Barucci, M. A.; Dotto, E. & Levasseur-Regourd, A. C., 2011, A&A Rv, V.19, id.48

  5. [5]

    N.; Ortiz, J

    Belskaya, I. N.; Ortiz, J. L.; Rousselot, P.; et al., 2006,

  6. [6]

    W.; et al., 2016,

    Benedetti-Rossi, G.; Sicardy, B.; Buie, M. W.; et al., 2016,

  7. [7]

    152, Issue 6, id

    AJ, V. 152, Issue 6, id. 156 B´ erard, D.; Sicardy, B.; Camargo, J. I. B.; et al., 2017, AJ, V. 154, Issue 4, id. 144

  8. [8]

    P.; Farinella, P.; Zappala, V

    Binzel, R. P.; Farinella, P.; Zappala, V. & Cellino, A., 1989, in Asteroids II (eds Binzel, R. P. et al.), 416441, Univ. Arizona Press

Show all 56 references
  1. [9]

    L.; et al., 2013, ApJ, 773, id

    Braga-Ribas, F.; Sicardy, B.; Ortiz, J. L.; et al., 2013, ApJ, 773, id. 26

  2. [10]

    L.; et al., 2014, Nature, 508, 7494 Brandeker & Cataldi, 2019, A&A, 621, A86

    Braga-Ribas, F.; Sicardy, B.; Ortiz, J. L.; et al., 2014, Nature, 508, 7494 Brandeker & Cataldi, 2019, A&A, 621, A86

  3. [11]

    W.; Keller, J

    Buie, M. W.; Keller, J. M., 2016, AJ, V. 151, Issue 3

  4. [12]

    Camargo, J. I. B.; Vieira-Martins, R.; Assafin, M.; et al., 2014, A&A, V. 561, id.A37

  5. [13]

    Camargo, J. I. B.; Desmars, J.; Braga-Ribas, F., et al., 2018, Planet. Space Sci., V. 154, p. 59-62 Occultations by the TNO 2003 VS2 21

  6. [14]

    Chandrasekhar, S., 1969, Ellipsoidal Figures of

  7. [15]

    Chandrasekhar, S., 1987, Ellipsoidal Figures of Equilibrium (New York: Dover)

  8. [16]

    & Brunette, G., 2001, in Using NTP to Control and Synchronize System Clocks Part I: Introduction to NTP (Sun BluePrintsTM), OnLine 2001 July

    Deeths, D. & Brunette, G., 2001, in Using NTP to Control and Synchronize System Clocks Part I: Introduction to NTP (Sun BluePrintsTM), OnLine 2001 July

  9. [17]

    L.; et al., 2017, AJ, V

    Dias-Oliveira, A.; Sicardy, B.; Ortiz, J. L.; et al., 2017, AJ, V. 154, id. 22 Duffard, R.; Ortiz, J. L.; Santos Sanz, P.; et al., 2008, A&A, V. 479, Issue 3 Fern´ andez-Valenzuela, E.; Ortiz, J. L.; Duffard, R.; et al., 2016, MNRAS, 456, Issue 3 Fern´ andez-Valenzuela, E.; Orti...

  10. [18]

    Gladman, B.; Marsden, B. G. & Vanlaerhoven, C., 2008, in The Solar System Beyond Neptune, M. A. Barucci, H

  11. [19]

    et al., 2009,

    Guilbert, A.; Alvarez-Candal, A.; Merlin, F. et al., 2009,

  12. [20]

    A.; Moore, J

    Hamilton, Douglas P.; Stern, S. A.; Moore, J. M. et al., 2016, Nature, V. 540, Issue 7631, pp. 97-99

  13. [21]

    P., Linscott, I

    Hinson, D. P., Linscott, I. R., Young, L. A., et al., 2017, Icarus, 290, 96

  14. [22]

    & Luu, J., 1993, Nature, 362, 6422

    Jewitt, D. & Luu, J., 1993, Nature, 362, 6422

  15. [23]

    & Rauer, H., 2008, in Trans-Neptunian Objects and Comets, Saas-Fee Advanced Course 35, 2008, XII

    Jewitt, D.; Morbidelli, A. & Rauer, H., 2008, in Trans-Neptunian Objects and Comets, Saas-Fee Advanced Course 35, 2008, XII

  16. [24]

    C., 2007, AJ, V

    Lacerda, P.; Jewitt, D. C., 2007, AJ, V. 133, Issue 4, pp. 1393, id. 159

  17. [25]

    Leiva, R.; Sicardy, B.; Camargo, J. I. B.; et al., 2017, AJ, V. 154, Issue 4, id. 159

  18. [26]

    B.; Sicardy, B.; et al., 1986,

    Lellouch, E.; Hubbard, W. B.; Sicardy, B.; et al., 1986,

  19. [27]

    324, Nov

    Nature, V. 324, Nov. 20, 1986, p. 227-231

  20. [28]

    L.; et al., 2002, A&A, V

    Lellouch, E.; Moreno, R.; Ortiz, J. L.; et al., 2002, A&A, V. 391

  21. [29]

    Lellouch, E.; Santos-Sanz, P.; Lacerda, P.; et al., 2013, A&A, V. 557

  22. [30]

    S.; Mukai, T., 2008, AJ, 135, 4, 1161-1200 Minor Planet Center Electronic Circular 2006-X45

    Lykawka, P. S.; Mukai, T., 2008, AJ, 135, 4, 1161-1200 Minor Planet Center Electronic Circular 2006-X45

  23. [31]

    W.; Kiss, C.; et al., 2012, A&A, V

    Mommert, M.; Harris, A. W.; Kiss, C.; et al., 2012, A&A, V. 541, A93

  24. [32]

    Moorwood, A.; Cuby, J.-G.; Biereichel, P.; et al., 1998, The

  25. [33]

    Moorwood, A.; Cuby, J.-G.; Lidman, C., 1998, The

  26. [34]

    F.; & Gomes, R., 2008, in The Solar System Beyond Neptune, M

    Morbidelli, A.; Levison, H. F.; & Gomes, R., 2008, in The Solar System Beyond Neptune, M. A. Barucci, H

  27. [35]

    L.; Baumont, S.; Guti´ errez, P

    Ortiz, J. L.; Baumont, S.; Guti´ errez, P. J.; et al., 2002, A&A, V. 388

  28. [36]

    L.; Sota, A.; Moreno, R.; et al., 2004, A&A, V

    Ortiz, J. L.; Sota, A.; Moreno, R.; et al., 2004, A&A, V. 420

  29. [37]

    L.; Guti´ errez, P

    Ortiz, J. L.; Guti´ errez, P. J.; Santos-Sanz, P.; et al., 2006, A&A, V. 447, Issue 3

  30. [38]

    L.; Santos Sanz, P.; Guti´ errez, P

    Ortiz, J. L.; Santos Sanz, P.; Guti´ errez, P. J.; et al., 2007, A&A, V. 468, Issue 1

  31. [39]

    L.; Cikota, A.; Cikota, S.; et al., 2011, A&A, V

    Ortiz, J. L.; Cikota, A.; Cikota, S.; et al., 2011, A&A, V. 525, id. A31

  32. [40]

    L.; Sicardy, B.; Braga-Ribas, F.; et al., 2012,

    Ortiz, J. L.; Sicardy, B.; Braga-Ribas, F.; et al., 2012,

  33. [41]

    L.; Duffard, R.; Pinilla-Alonso, N.; et al., 2015, A&A, V

    Ortiz, J. L.; Duffard, R.; Pinilla-Alonso, N.; et al., 2015, A&A, V. 576, id. A18

  34. [42]

    L.; Santos-Sanz, P.; Sicardy, B.; et al., 2017, Nature, 550, 7675

    Ortiz, J. L.; Santos-Sanz, P.; Sicardy, B.; et al., 2017, Nature, 550, 7675

  35. [43]

    H., 2015, Icarus, 247, 112-125

    Parker, A. H., 2015, Icarus, 247, 112-125

  36. [44]

    A.; Fornasier, S.; et al., 2010, A&A, V

    Perna, D.; Barucci, M. A.; Fornasier, S.; et al., 2010, A&A, V. 510, id. A53

  37. [45]

    G.; Pinilla-Alonso, N.; et al., 2016, PASP, 128, 959, 018011

    Santos-Sanz, P.; French, R. G.; Pinilla-Alonso, N.; et al., 2016, PASP, 128, 959, 018011

  38. [46]

    Santos-Sanz, P.; Lellouch, E.; Groussin, O.; et al., 2017, A&A, V. 604, id. A95

  39. [47]

    S., 2007, AJ, 134, 787-798

    Sheppard, S. S., 2007, AJ, 134, 787-798

  40. [48]

    L.; Assafin, M.; et al., 2011, Nature, 478, 493

    Sicardy, B.; Ortiz, J. L.; Assafin, M.; et al., 2011, Nature, 478, 493

  41. [49]

    Stansberry, J.; Grundy, W.; Brown, M.; et al., 2008, in The Solar System Beyond Neptune, M. A. Barucci, H

  42. [50]

    Stern, A.; Bagenal, F.; Ennico, K.; et al., 2015, Science, 350, 6258, id.aad1815 S. A. Stern; H. A. Weaver; J. R. Spencer; et al., 2019,

  43. [51]

    99, 191-222

    Stetson, Peter B., 1987, PASP, V. 99, 191-222

  44. [52]

    & Favre, S

    Tancredi, G. & Favre, S. 2008, Icarus, V. 195, Issue 2

  45. [53]

    L.; Duffard, R.; et al., 2010, A&A, V

    Thirouin, A.; Ortiz, J. L.; Duffard, R.; et al., 2010, A&A, V. 522, id. A93

  46. [54]

    T., 1999, PASP, V

    Thirouin, A., 2013, Study of Trans-Neptunian Objects using photometric techniques and numerical simulations (Granada, Spain: Universidad de Granada) van Belle, G. T., 1999, PASP, V. 111, Issue 766 22 Benedetti-Rossi et al. van Leeuwen, F.; de Bruijne, J. H. J.; Arenou, F.; et ...

  47. [55]

    199, Issue 2

    Widemann, T.; Sicardy, B.; Dusser, R.; et al., 2009, Icarus, V. 199, Issue 2

  48. [56]

    G.; Levine, S

    Zacharias, N.; Monet, D. G.; Levine, S. E.; et al., 2004, AAS Meeting 205, id.48.15; Bulletin of the American Astronomical Society, Vol. 36, Icarus 228, 301314

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.