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The surface of Pluto-twin TNOs 2005 FY 9 and 2003 UB 313

The surface of Pluto-twin TNOs 2005 FY 9 and 2003 UB 313. Javier Licandro (1,2) , N. Pinilla-Alonso (3) , M. Pedani (3) , E. Oliva (3) , P. Leisy (1) , G.P. Tozzi (4) and W. Grundy (5). (1)Isaac Newton Group of Telescopes (2)Instituto de Astrofísica de Canarias (3)Fundación Galileo Galilei

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The surface of Pluto-twin TNOs 2005 FY 9 and 2003 UB 313

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  1. The surface of Pluto-twin TNOs 2005 FY9 and 2003 UB313 Javier Licandro(1,2), N. Pinilla-Alonso(3), M. Pedani(3), E. Oliva(3), P. Leisy(1), G.P. Tozzi(4) and W. Grundy(5) (1)Isaac Newton Group of Telescopes (2)Instituto de Astrofísica de Canarias (3)Fundación Galileo Galilei (4)INAF-Oss di Arcetri (5)Lowel Observatory

  2. Pluto’s spectrum • deep CH4 ice bands, shifted by about 15A respect to laboratory. • weak N2 (2.15 microns) and CO (1.58, 2.35 microns) • no deep water ice or CO2 • red in the visible  organics (tholins, irradiated CH4)?

  3. 2005 FY9 Observed simultaneously with the TNG and WHT at La Palma on Aug. 1st, 2005. Deep CH4 ice bands, some of them not seen in Pluto’s spectrum ( e.g. 0.63 microns) Red colour in the visible, similar to Pluto Licandro et al. 2006

  4. 2003 UB313 Brown et al. 2005 Near infrared spectrum of 2003 UB313 similar to our 2005 FY9 spectrum Licandro et al. 2006

  5. 2003 UB313 • Observed with the WHT on Oct. 20th, 2005. Licandro et al. 2006, in preparation

  6. COLOURS All present slightly red slope in the visible S’ measured using the 0.59 and 0.825 microns reflectance S’(UB313)= 4 %/1000A S’(FY9)= 8.9 %/1000A S’(Pluto)= 8.9 %/1000A Posible organics in the surface, probably irradiated methane (Brunetto et al. this meeting). Less abuntant in 2003 UB313 Licandro et al. 2006, in preparation

  7. Band depths Indicative of abundance and/or grain sizes FY9/Pluto (0.73) = 6 FY9/Pluto (0.89) = 3 FY9/UB313 (0.73)= 1.9 FY9/UB313 (0.89)= 1.1 Licandro et al. 2006, in preparation

  8. Band depths • In the infrared the differences are smaller but consistent, • light reflected from the 3 objects samples different mean optical pathlengths • Saturation of deeper bands Different concentration of CH4 and or thickness of the CH4 layers

  9. Band depths and saturation effects In the infrared the bands are highly saturated  visible spectral range is very important Weaker bands sample deeper layers

  10. Band shifts: 2005 FY9 Band shifts respect to laboratory pure CH4 ones indicative of dilusion in N2 Shifts < 5 A  high concetration of CH4 or no N2 on 2005 FY9 surface Atmosphere? Crucial to determine if there is some N2 Licandro et al. 2005

  11. Band shifts: 2003 UB313 SHIFTED ?

  12. Band shifts: 0.73 micron band Pluto CH4 (0.05cm) 2005 FY9 CH4 (4.5cm) 2003 UB313 CH4 (1.5cm)

  13. Band shifts: 0.89 micron bands Pluto CH4 (0.05cm) 2005 FY9 CH4 (4.5cm) 2003 UB313 CH4 (1.5cm) Problems with wl calibration? NO!!!! Uncertainties on Sky lines < 1A

  14. Band shifts: 2003 UB313 2003 UB313 shifted by 15 A CH4 (1.5cm) Narower?

  15. Band shifts: 2003 UB313 There is CH4 diluted in N2 ice in the surface of 2003 UB313 Weaker bands sample deeper layers  evidence of a vertical compositional gradient ? Colapse of the atmosphere?

  16. Charons

  17. Band shifts

  18. Band shifts

  19. Band shifts

  20. La atmósfera de Plutón atmósfera de CH4, N2 y CO Condiciones suficientes de tamaño, masa, y temperatura

  21. La atmósfera de Caronte? No se ha detectado

  22. La superficie de Plutón • bandas desplazadas  metano diluido en N2 • inhomogeneidades superficiales relacionadas con diferente composición y albedo

  23. Observations Visible 4.2 William Herschel Telescope ISIS Infrarred 3.6 m Telescopio Nazionale Galileo NICS

  24. Los TNOs grandes

  25. Diferent composition or diferent surface evolution?

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