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About OSSOS

All survey observations were acquired by the Canada France Hawaii Telescope and are stored and processed using the Canadian Advanced Network For Astronomical Research. For additional public information is available from our public web site

Refereed Journal Articles

  1. The Outer Solar System Origins Survey. I. Design and First-quarter Discoveries (2016) Bannister
  2. OSSOS. II. A Sharp Transition in the Absolute Magnitude Distribution of the Kuiper Belt’s Scattering Population (2016) Shankman
  3. OSSOS. III Resonant Trans-Neptunian Populations: Constraints from the first quarter of the Outer Solar System Origins Survey (2016) Volk
  4. OSSOS. IV. Discovery of a Dwarf Planet Candidate in the 9:2 Resonance with Neptune (2016) Bannister
  5. OSSOS. V. Diffusion in the Orbit of a High-perihelion Distant Solar System Object (2017) Bannister
  6. OSSOS. VI. Striking Biases in the Detection of Large Semimajor Axis Trans-Neptunian Objects (2017) Shankman
  7. OSSOS. VII. 800+ Trans-Neptunian Objects—The Complete Data Release (2018) Bannister
  8. OSSOS. VIII. The Transition between Two Size Distribution Slopes in the Scattering Disk (2018) Lawler
  9. OSSOS. IX. Two Objects in Neptune's 9:1 Resonance—Implications for Resonance Sticking in the Scattering Population (2018) Volk
  10. OSSOS: X. How to use a Survey Simulator: Statistical Testing of Dynamical Models Against the Real Kuiper Belt (2018) Lawler
  11. OSSOS. XI. No active centaurs in the Outer Solar System Origins Survey (2019) Cabral
  12. OSSOS. XII. Variability Studies of 65 Trans-Neptunian Objects Using the Hyper Suprime-Cam (2019) Alexandersen
  13. OSSOS. XIII. Fossilized Resonant Dropouts Tentatively Confirm Neptune’s Migration Was Grainy and Slow (2019) Lawler
  14. OSSOS. XIV. The Plane of the Kuiper Belt (2019) Van Laerhoven
  15. OSSOS. XV. Probing the Distant Solar System with Observed Scattering TNOs (2019) Kaib
  16. A dearth of small members in the Haumea family revealed by OSSOS (2020) Pike
  17. OSSOS. XVII. An upper limit on the number of distant planetary objects in the Solar System (2021) Ashton
  18. OSSOS. XVIII. Constraining Migration Models with the 2:1 Resonance Using the Outer Solar System Origins Survey (2019) Chen
  19. OSSOS. XIX. Testing Early Solar System Dynamical Models Using OSSOS Centaur Detections (2019) Nesvorný
  20. OSSOS XX: The Meaning of Kuiper Belt Colors (2020) Nesvorný
  21. OSSOS. XXI. Collision Probabilities in the Edgeworth-Kuiper Belt (2021) Abedin
  22. OSSOS: The eccentricity and inclination distributions of the stable Neptunian Trojans (2021) Lin
  23. OSSOS. XXIII. 2013 VZ70 and the Temporary Coorbitals of the Giant Planets (2021) Alexandersen
  24. OSSOS Finds an Exponential Cutoff in the Size Distribution of the Cold Classical Kuiper Belt (2021) Kavelaars
  25. OSSOS XXV: Large Populations and Scattering-Sticking in the Distant Trans-Neptunian Resonances (2022) Crompvoets
  26. OSSOS. XXVI. On the Lack of Catastrophic Collisions in the Present Kuiper Belt (2022) Abedin
  27. OSSOS. XXVII. Population Estimates for Theoretically Stable Centaurs between Uranus and Neptune (2023) Dorsey
  28. The Hot Main Kuiper Belt Size Distribution from OSSOS (2023) Petit
  29. OSSOS. XXIX. The Population and Perihelion Distribution of the Detached Kuiper Belt

Data Releases

Collaboration

The Teams will receive the object list for each semester's discoveries as a summary table of internal designations with orbital elements and uncertainties. At release, a typical object will have a semimajor axis uncertainty of 0.1-1%. Dynamical classification using the SSBN 2008 classification will be provided. Core will also provide access to the full astrometry and the imaging data for each detection.

Some topic teams will then wish to propose observations to other telescopes for next-semester studies of the sample; this will likely be the only time when the topic teams have a proposal advantage over the world. At the time of proposal, the ephemerides of most objects will be good to +/- < 30"; the half-year-later CFHT recovery of all objects will have dropped these uncertainties to a few arcseconds by the time P.I.-led exploitation observations occur.

Public

We aim to submit all observations of a given semester to the MPC 6 months after the end of the semester, except for the first semester (2013), which was delayed longer. This gives observers on quarterly systems a chance to propose for telescope deadlines a cycle later with no competition. It also gives the theory teams 5 months to work before the world sees the MPC release. Recovery observations will be sent as a batch to the MPC with the same time delay.

CFHT imaging becomes public a year after the end of each semester, e.g. on August 1, 2016, the 2015A CFHT imaging becomes public to the world.

Collaboration Teams

The principle contact for each team member should be their topic team's leader.

Team leaders can contact the Core.

Full list of OSSOS collaborators
Core
CFHT image acquisition, moving object detection, orbit linkage, characterisation. (Teleconference minutes)
- Classical Belt, structure and SDF
H-mag distributions, dependence on class. ABSORBED INTO CORE: Petit as leader.
Catalogs
Objects slower than OSSOS rate cut) + non-moving object variation (eg. variable stars). Leader: L. Jones.
Binaries
mutual orbits, separation, colours. Leader: K. Noll.
Cometary Activity
Search for coma. Leader: P. Rousselot.
Light curves
Time variable TNOs, phase curves. Leader: M. Schwamb.
Occultations
Predictions, observing campaigns. Leader: W. Fraser.
Resonant Populations
relative populations, libration amplitude distributions. Leader: R. Murray-Clay
Scattering
Centaurs, Scattering Disk, Oort cloud connection. Leader: N. Kaib
Surfaces
Colours, NIR spectra. Leader: A. Delsanti.

SUSPENDED OR MERGED OR DEFUNCT OR INCOMPLETE

Nearby objects
Search for and tracking of objects moving faster than OSSOS cuts (roughly, inside 8 AU). SUSPENDED.
Thermal Modeling
Thermal evolution of objects. Leader: A. Guilbert ALL FUNCTIONS MERGED INTO SURFACES
Jovian Trojans
Proposed Leader: F. Yoshida. Work tasks and worker list never finalized. Does not yet formally exists.

How to join OSSOS

See the main OSSOS web site: http://www.ossos-survey.org/get-involved.html

Publications and Proposals

Survey

Observations have concluded.

Original proposals: see the survey draft and the Accepted Proposal (access restricted to collaboration only).

Figures for presentations etc.

2013A

  • April 2013 preliminary field layout plot (here for reference. As in the proposal; varied very slightly from the observed location)
  • April 2013 observed plot - as the O and E fields have oppositions a month apart, the E field is shown at its 9 April moon-dark location, and the O field at its 8 May moon-dark location. The known TNOs plotted are for new moon, May 9.
  • 13AE discoveries plot - all positions for 9 April 2013

2013B

Calibration

Timeline

  • June 6/2012: OSSOS was number 1 ranked CFHT Large program. 560hr awarded.
  • Jan 2013: OSSOS began observation.
  • Oct 6/2013: Second OSSOS team meeting, at 2013 DPS meeting in Denver.
  • June 25-27 2014: OSSOS team workshop in Beaune, France. Meeting Website
  • Nov 2014: Third OSSOS team meeting, 2014 DPS in Tucson.
  • Nov 2015: Fourth OSSOS team meeting, 2015 DPS in Washington DC.
  • Oct 2016: Fifth OSSOS team meeting just before 2016 DPS/EPSC in Pasedena
  • Jan 31/2017: End of 4-year CFHT OSSOS LP allocation
  • July 2017: Sixth OSSOS team meeting in Belfast, UK.
  • Dec 2017: OSSOS concluded observation.


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