The surface of Pluto-twin TNOs 2005 FY
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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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The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

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


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

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)?


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

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


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

2003 UB313

Brown et al. 2005

Near infrared spectrum of 2003 UB313 similar to our 2005 FY9 spectrum

Licandro et al. 2006


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

2003 UB313

  • Observed with the WHT on Oct. 20th, 2005.

Licandro et al. 2006, in preparation


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

  • 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


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

  • 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


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

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


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

Band depths and saturation effects

In the infrared the bands are highly saturated  visible spectral range is very important

Weaker bands sample deeper layers


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

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


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

Band shifts: 2003 UB313

SHIFTED ?


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

Band shifts: 0.73 micron band

Pluto

CH4 (0.05cm)

2005 FY9

CH4 (4.5cm)

2003 UB313

CH4 (1.5cm)


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

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


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

Band shifts: 2003 UB313

2003 UB313 shifted by 15 A

CH4 (1.5cm)

Narower?


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

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?


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

Charons


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

Band shifts


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

Band shifts


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

Band shifts


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

La atmósfera de Plutón

atmósfera de CH4, N2 y CO

Condiciones suficientes de tamaño, masa, y temperatura


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

La atmósfera de Caronte?

No se ha detectado


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

La superficie de Plutón

  • bandas desplazadas  metano diluido en N2

  • inhomogeneidades superficiales relacionadas con diferente composición y albedo


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

Observations

Visible

4.2 William Herschel Telescope

ISIS

Infrarred

3.6 m Telescopio Nazionale Galileo

NICS


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

Los TNOs grandes


The surface of pluto twin tnos 2005 fy 9 and 2003 ub 313

Diferent composition or diferent surface evolution?


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