Ices on (90377) Sedna

Confirmation and compositional constraints

J. P. Emery, C. M. Dalle Ore, D. P. Cruikshank, Y. R. Fernández, David E Trilling, J. A. Stansberry

Research output: Contribution to journalArticle

22 Citations (Scopus)

Abstract

We report measurements of reflectances of 90377 Sedna at λ> 2.5 μm using the Infrared Array Camera (IRAC) on the Spitzer Space Telescope. Sedna orbits well beyond even the Kuiper Belt, with a perihelion distance of 76 AU, and is therefore very faint as viewed from Earth, despite its relatively large size. Previously published near-infrared spectra show possible signatures of CH4 and N2 at ∼2.3 and ∼2.15 μm, respectively. These and other ices also exhibit much stronger absorptions at λ> 2.5 μm, providing the motivation for the present work. We detected flux from Sedna at 3.6 and 4.5 μm, but not at 5.8 or 8.0 μm. The measured IRAC fluxes are converted to geometric albedos and combined with previous measurements of the visible and near-infrared spectra. Strong absorption at both 3.6 and 4.5 μm (relative to the 2.0-2.5 μm region) is readily apparent, confirming the presence of ices on the surface of Sedna. Spectral modeling of the full wavelength range (0.4-4.5 μm) provides further constraints. We find that CH4 is required to fit the new data points, but that these new data points can not be adequately described with models containing CH4 and N2 as the only ices. We suggest that H2O ice is also present. Several characteristics of the spectrum of Sedna suggest an absence of atmospheric volatile transport, in contrast to the large objects Eris and 2005 FY9.

Original languageEnglish (US)
Pages (from-to)395-398
Number of pages4
JournalAstronomy and Astrophysics
Volume466
Issue number1
DOIs
StatePublished - Apr 2007
Externally publishedYes

Fingerprint

ice
near infrared
infrared spectra
cameras
Kuiper belt
Space Infrared Telescope Facility
albedo
reflectance
signatures
wavelength
orbits
wavelengths
modeling

Keywords

  • Infrared: solar system
  • Kuiper Belt
  • Planets and satellites: individual: Sedna
  • Solar system: general

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Emery, J. P., Dalle Ore, C. M., Cruikshank, D. P., Fernández, Y. R., Trilling, D. E., & Stansberry, J. A. (2007). Ices on (90377) Sedna: Confirmation and compositional constraints. Astronomy and Astrophysics, 466(1), 395-398. https://doi.org/10.1051/0004-6361:20067021

Ices on (90377) Sedna : Confirmation and compositional constraints. / Emery, J. P.; Dalle Ore, C. M.; Cruikshank, D. P.; Fernández, Y. R.; Trilling, David E; Stansberry, J. A.

In: Astronomy and Astrophysics, Vol. 466, No. 1, 04.2007, p. 395-398.

Research output: Contribution to journalArticle

Emery, JP, Dalle Ore, CM, Cruikshank, DP, Fernández, YR, Trilling, DE & Stansberry, JA 2007, 'Ices on (90377) Sedna: Confirmation and compositional constraints', Astronomy and Astrophysics, vol. 466, no. 1, pp. 395-398. https://doi.org/10.1051/0004-6361:20067021
Emery JP, Dalle Ore CM, Cruikshank DP, Fernández YR, Trilling DE, Stansberry JA. Ices on (90377) Sedna: Confirmation and compositional constraints. Astronomy and Astrophysics. 2007 Apr;466(1):395-398. https://doi.org/10.1051/0004-6361:20067021
Emery, J. P. ; Dalle Ore, C. M. ; Cruikshank, D. P. ; Fernández, Y. R. ; Trilling, David E ; Stansberry, J. A. / Ices on (90377) Sedna : Confirmation and compositional constraints. In: Astronomy and Astrophysics. 2007 ; Vol. 466, No. 1. pp. 395-398.
@article{bed040980f5f429397d22472f84e3628,
title = "Ices on (90377) Sedna: Confirmation and compositional constraints",
abstract = "We report measurements of reflectances of 90377 Sedna at λ> 2.5 μm using the Infrared Array Camera (IRAC) on the Spitzer Space Telescope. Sedna orbits well beyond even the Kuiper Belt, with a perihelion distance of 76 AU, and is therefore very faint as viewed from Earth, despite its relatively large size. Previously published near-infrared spectra show possible signatures of CH4 and N2 at ∼2.3 and ∼2.15 μm, respectively. These and other ices also exhibit much stronger absorptions at λ> 2.5 μm, providing the motivation for the present work. We detected flux from Sedna at 3.6 and 4.5 μm, but not at 5.8 or 8.0 μm. The measured IRAC fluxes are converted to geometric albedos and combined with previous measurements of the visible and near-infrared spectra. Strong absorption at both 3.6 and 4.5 μm (relative to the 2.0-2.5 μm region) is readily apparent, confirming the presence of ices on the surface of Sedna. Spectral modeling of the full wavelength range (0.4-4.5 μm) provides further constraints. We find that CH4 is required to fit the new data points, but that these new data points can not be adequately described with models containing CH4 and N2 as the only ices. We suggest that H2O ice is also present. Several characteristics of the spectrum of Sedna suggest an absence of atmospheric volatile transport, in contrast to the large objects Eris and 2005 FY9.",
keywords = "Infrared: solar system, Kuiper Belt, Planets and satellites: individual: Sedna, Solar system: general",
author = "Emery, {J. P.} and {Dalle Ore}, {C. M.} and Cruikshank, {D. P.} and Fern{\'a}ndez, {Y. R.} and Trilling, {David E} and Stansberry, {J. A.}",
year = "2007",
month = "4",
doi = "10.1051/0004-6361:20067021",
language = "English (US)",
volume = "466",
pages = "395--398",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",
number = "1",

}

TY - JOUR

T1 - Ices on (90377) Sedna

T2 - Confirmation and compositional constraints

AU - Emery, J. P.

AU - Dalle Ore, C. M.

AU - Cruikshank, D. P.

AU - Fernández, Y. R.

AU - Trilling, David E

AU - Stansberry, J. A.

PY - 2007/4

Y1 - 2007/4

N2 - We report measurements of reflectances of 90377 Sedna at λ> 2.5 μm using the Infrared Array Camera (IRAC) on the Spitzer Space Telescope. Sedna orbits well beyond even the Kuiper Belt, with a perihelion distance of 76 AU, and is therefore very faint as viewed from Earth, despite its relatively large size. Previously published near-infrared spectra show possible signatures of CH4 and N2 at ∼2.3 and ∼2.15 μm, respectively. These and other ices also exhibit much stronger absorptions at λ> 2.5 μm, providing the motivation for the present work. We detected flux from Sedna at 3.6 and 4.5 μm, but not at 5.8 or 8.0 μm. The measured IRAC fluxes are converted to geometric albedos and combined with previous measurements of the visible and near-infrared spectra. Strong absorption at both 3.6 and 4.5 μm (relative to the 2.0-2.5 μm region) is readily apparent, confirming the presence of ices on the surface of Sedna. Spectral modeling of the full wavelength range (0.4-4.5 μm) provides further constraints. We find that CH4 is required to fit the new data points, but that these new data points can not be adequately described with models containing CH4 and N2 as the only ices. We suggest that H2O ice is also present. Several characteristics of the spectrum of Sedna suggest an absence of atmospheric volatile transport, in contrast to the large objects Eris and 2005 FY9.

AB - We report measurements of reflectances of 90377 Sedna at λ> 2.5 μm using the Infrared Array Camera (IRAC) on the Spitzer Space Telescope. Sedna orbits well beyond even the Kuiper Belt, with a perihelion distance of 76 AU, and is therefore very faint as viewed from Earth, despite its relatively large size. Previously published near-infrared spectra show possible signatures of CH4 and N2 at ∼2.3 and ∼2.15 μm, respectively. These and other ices also exhibit much stronger absorptions at λ> 2.5 μm, providing the motivation for the present work. We detected flux from Sedna at 3.6 and 4.5 μm, but not at 5.8 or 8.0 μm. The measured IRAC fluxes are converted to geometric albedos and combined with previous measurements of the visible and near-infrared spectra. Strong absorption at both 3.6 and 4.5 μm (relative to the 2.0-2.5 μm region) is readily apparent, confirming the presence of ices on the surface of Sedna. Spectral modeling of the full wavelength range (0.4-4.5 μm) provides further constraints. We find that CH4 is required to fit the new data points, but that these new data points can not be adequately described with models containing CH4 and N2 as the only ices. We suggest that H2O ice is also present. Several characteristics of the spectrum of Sedna suggest an absence of atmospheric volatile transport, in contrast to the large objects Eris and 2005 FY9.

KW - Infrared: solar system

KW - Kuiper Belt

KW - Planets and satellites: individual: Sedna

KW - Solar system: general

UR - http://www.scopus.com/inward/record.url?scp=34347346270&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=34347346270&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:20067021

DO - 10.1051/0004-6361:20067021

M3 - Article

VL - 466

SP - 395

EP - 398

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

IS - 1

ER -