J/AJ/157/94 Col-OSSOS: Properties of outer solar system objects (Marsset+, 2019)
Col-OSSOS: color and inclination are correlated throughout the Kuiper Belt.
Marsset M., Fraser W.C., Pike R.E., Bannister M.T., Schwamb M.E., Volk K.,
Kavelaars J.J., Alexandersen M., Chen Y.-T., Gladman B.J., Gwyn S.D.J.,
Lehner M.J., Peixinho N., Petit J.-M., Wang S.-Y.
<Astron. J., 157, 94 (2019)>
=2019AJ....157...94M 2019AJ....157...94M (SIMBAD/NED BibCode)
ADC_Keywords: Solar system ; Minor planets ; Photometry ; Optical ; Surveys
Keywords: Kuiper belt: general - minor planets, asteroids: general - surveys
Abstract:
Both physical and dynamical properties must be considered to constrain
the origins of the dynamically excited distant solar system populations.
We present high-precision (g-r) colors for 25 small (Hr>5) dynamically
excited trans-Neptunian objects (TNOs) and centaurs acquired as part
of the Colours of the Outer Solar System Origins Survey. We combine our
data set with previously published measurements and consider a set of
229 colors of outer solar system objects on dynamically excited orbits.
The overall color distribution is bimodal and can be decomposed into
two distinct classes, termed gray and red, that each has a normal color
distribution. The two color classes have different inclination
distributions: red objects have lower inclinations than the gray ones.
This trend holds for all dynamically excited TNO populations. Even in
the worst-case scenario, biases in the discovery surveys cannot account
for this trend; it is intrinsic to the TNO population. Considering that
TNOs are the precursors of centaurs, and that their inclinations are
roughly preserved as they become centaurs, our finding solves the conundrum
of centaurs being the only outer solar system population identified so
far to exhibit this property. The different orbital distributions of
the gray and red dynamically excited TNOs provide strong evidence that
their colors are due to different formation locations in a disk of
planetesimals with a compositional gradient.
Description:
All of the new color measurements presented in this paper were acquired
through the Col-OSSOS large program (PI: W. Fraser) on Gemini North between
2014 August and 2016 November. Col-OSSOS collects near-simultaneous g-, r-,
and J-band photometry of a magnitude-limited (r<23.6) subset of the OSSOS
sample. Optical measurements were acquired with the Gemini Multi-Object
Spectrograph (GMOS; Hook et al. 2004PASP..116..425H 2004PASP..116..425H), and the J-band
sequence was obtained with the Near InfraRed Imager and Spectrometer (NIRI;
Hodapp et al. 2003PASP..115.1388H 2003PASP..115.1388H). We observed using a rgJgr sequence
to account for any brightness variation due to light-curve effects.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 79 229 Orbit, magnitude, and measured spectral slope
of the outer solar system objects studied in
this work
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See also:
B/astorb : Orbits of Minor Planets (Bowell+ 2014)
J/A+A/380/347 : BVRI photometry of 27 Kuiper Belt Objects (Delsanti+, 2001)
J/A+A/389/641 : Col. of Minor Bodies in Outer Solar System (Hainaut+, 2002)
J/A+A/407/1139 : RVB photom. of Kuiper-Belt object 1999 TD10 (Rousselot+, 2003)
J/AJ/127/3023 : R magnitudes of Kuiper Belt object 2001QG298 (Sheppard+, 2004)
J/AJ/135/55 : NIR spectra of Centaurs & Kuiper Belt objects (Barkume+, 2008)
J/ApJ/720/1691 : Observations of the distant Kuiper belt (Schwamb+, 2010)
J/A+A/546/A86 : R absolute magnitudes of Kuiper Belt objects (Peixinho+, 2012)
J/A+A/546/A115 : Colors of minor bodies in outer solar system (Hainaut+, 2012)
J/A+A/577/A35 : Visible colors of Centaurs and KBOs (Peixinho+, 2015)
J/AJ/152/70 : Outer Solar System Origins Survey (OSSOS) (Bannister+, 2016)
J/AJ/152/221 : New extreme trans-Neptunian objects (Sheppard+, 2016)
http://www.minorplanetcenter.net/ : Minor Planet Center
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- Planet [2060/511555]? Minor Planet Center (MPC)
number designation
8- 17 A10 --- Name Target name
19- 30 A12 --- OName Other designation
32- 35 A4 --- Class Orbit classification (1)
37 A1 --- f_Class [*i] Flag on Class (2)
39- 43 F5.2 mag Hr [5.02/10.89] Absolute r-band magnitude (3)
45- 50 F6.2 AU a [10.64/799.41] Semi-major axis
52- 55 F4.2 --- e [0.01/0.97] Eccentricity
57- 61 F5.2 deg Inc [5.05/44.89] Inclination
63- 67 F5.2 10-4nm-1 Slope [-2.6/52.82] Spectral slope (in %/103Å)
69- 73 F5.2 10-4nm-1 e_Slope [0.48/11.89] Uncertainty in Slope
(in %/103Å)
75- 79 A5 --- Ref Reference code(s) (4)
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Note (1): Dynamical classification:
cla = Classical belt;
sca = Scattering disk;
cen = Centaur;
det = Detached;
x:y = Resonators, where x and y indicate the specific mean motion resonance.
Orbital elements are in the barycentric referential and were computed using
the Bernstein & Khushalani (2000AJ....120.3323B 2000AJ....120.3323B) orbit-fitting procedure.
Dynamical classification uses the Gladman et al. (2008ssbn.book...43G 2008ssbn.book...43G)
classification scheme. See Bannister et al. (2016, J/AJ/152/70) for additional
information.
Note (2): Flag as follows:
* = 2007JK43 is nearly on a Uranus crossing orbit and has a semi-major axis
that falls within the classical belt. It is classified as "detached"
because no close encounter happens during the 10 My integration of its
orbit;
i = Insecure classification.
Note (3): Converted to r-band using the Synphot/STSDAS tool. Peixinho et al.
(2015, J/A+A/577/A35) do not report absolute magnitude for several objects in
their dataset. We retrieved these magnitudes from the Minor Bodies in the
Outer Solar System (MBOSS) database (Hainaut et al. 2012, J/A+A/546/A115) when
available, or from the original papers (Boehnhardt et al. 2002A&A...395..297B 2002A&A...395..297B;
Sheppard 2010AJ....139.1394S 2010AJ....139.1394S; Benecchi et al. 2009Icar..200..292B 2009Icar..200..292B,
2011Icar..213..693B 2011Icar..213..693B) otherwise.
Note (4): Reference code as follows:
1 = Col-OSSOS (Pike et al. 2017AJ....154..101P 2017AJ....154..101P, Schwamb et al.
2018arXiv180908501S 2018arXiv180908501S and this work);
2 = Peixinho et al. (2015, J/A+A/577/A35) and references herein;
3 = Fraser & Brown (2012ApJ...749...33F 2012ApJ...749...33F), Fraser et al. (2015ApJ...804...31F 2015ApJ...804...31F);
4 = Tegler et al. (2016AJ....152..210T 2016AJ....152..210T).
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(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 29-May-2019