Epsilon Eridani's planetary debris disk: Structure and dynamics based on spitzer and Caltech Submillimeter Observatory observations

D. Backman, M. Marengo, K. Stapelfeldt, K. Su, D. Wilner, C. D. Dowell, D. Watson, J. Stansberry, George H. Rieke, T. Megeath, G. Fazio, M. Werner

Research output: Contribution to journalArticle

93 Citations (Scopus)

Abstract

Spitzer and Caltech Submillimeter Observatory images and spectrophotometry of ε Eridani at wavelengths from 3.5 to 350 μm reveal new details of its bright debris disk. The 350 μm map confirms the presence of a ring at r = 11″-28″(35-90 AU), observed previously at longer sub-mm wavelengths. The Spitzer mid-IR and far-IR images do not show the ring, but rather a featureless disk extending from within a few arcsec of the star across the ring to r 34″ (110 AU). The spectral energy distribution (SED) of the debris system implies a complex structure. A model constrained by the surface brightness profiles and the SED indicates that the sub-mm ring emission is primarily from large (a 135 μm) grains, with smaller (a 15 μm) grains also present in and beyond the ring. The Spitzer Infrared Spectrograph and Multiband Imaging Photometer for Spitzer SED-mode spectrophotometry data clearly show the presence of spatially compact excess emission at λ ≳ 15 μm that requires the presence of two additional narrow belts of dust within the sub-mm ring's central void. The innermost belt at r 3 AU is composed of silicate dust. A simple dynamical model suggests that dust produced collisionally by a population of about 11 M of planetesimals in the sub-mm ring could be the source of the emission from both in and beyond the sub-mm ring. Maintaining the inner belts and the inner edge to the sub-mm ring may require the presence of three planets in this system including the candidate radial velocity object.

Original languageEnglish (US)
Pages (from-to)1522-1538
Number of pages17
JournalAstrophysical Journal
Volume690
Issue number2
DOIs
StatePublished - 2009

Fingerprint

debris
observatories
observatory
spectrophotometry
dust
rings
wavelength
energy
planetesimal
photometer
spectral energy distribution
void
planet
silicate
distribution
protoplanets
wavelengths
radial velocity
spectrographs
photometers

Keywords

  • Circumstellar matter
  • Infrared: stars
  • Planetary systems
  • Stars: individual (epsilon Eridani)

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Epsilon Eridani's planetary debris disk : Structure and dynamics based on spitzer and Caltech Submillimeter Observatory observations. / Backman, D.; Marengo, M.; Stapelfeldt, K.; Su, K.; Wilner, D.; Dowell, C. D.; Watson, D.; Stansberry, J.; Rieke, George H.; Megeath, T.; Fazio, G.; Werner, M.

In: Astrophysical Journal, Vol. 690, No. 2, 2009, p. 1522-1538.

Research output: Contribution to journalArticle

Backman, D, Marengo, M, Stapelfeldt, K, Su, K, Wilner, D, Dowell, CD, Watson, D, Stansberry, J, Rieke, GH, Megeath, T, Fazio, G & Werner, M 2009, 'Epsilon Eridani's planetary debris disk: Structure and dynamics based on spitzer and Caltech Submillimeter Observatory observations', Astrophysical Journal, vol. 690, no. 2, pp. 1522-1538. https://doi.org/10.1088/0004-637X/690/2/1522
Backman, D. ; Marengo, M. ; Stapelfeldt, K. ; Su, K. ; Wilner, D. ; Dowell, C. D. ; Watson, D. ; Stansberry, J. ; Rieke, George H. ; Megeath, T. ; Fazio, G. ; Werner, M. / Epsilon Eridani's planetary debris disk : Structure and dynamics based on spitzer and Caltech Submillimeter Observatory observations. In: Astrophysical Journal. 2009 ; Vol. 690, No. 2. pp. 1522-1538.
@article{3bc0627aceb548fc8db52916031ac16c,
title = "Epsilon Eridani's planetary debris disk: Structure and dynamics based on spitzer and Caltech Submillimeter Observatory observations",
abstract = "Spitzer and Caltech Submillimeter Observatory images and spectrophotometry of ε Eridani at wavelengths from 3.5 to 350 μm reveal new details of its bright debris disk. The 350 μm map confirms the presence of a ring at r = 11″-28″(35-90 AU), observed previously at longer sub-mm wavelengths. The Spitzer mid-IR and far-IR images do not show the ring, but rather a featureless disk extending from within a few arcsec of the star across the ring to r 34″ (110 AU). The spectral energy distribution (SED) of the debris system implies a complex structure. A model constrained by the surface brightness profiles and the SED indicates that the sub-mm ring emission is primarily from large (a 135 μm) grains, with smaller (a 15 μm) grains also present in and beyond the ring. The Spitzer Infrared Spectrograph and Multiband Imaging Photometer for Spitzer SED-mode spectrophotometry data clearly show the presence of spatially compact excess emission at λ ≳ 15 μm that requires the presence of two additional narrow belts of dust within the sub-mm ring's central void. The innermost belt at r 3 AU is composed of silicate dust. A simple dynamical model suggests that dust produced collisionally by a population of about 11 M ⊕ of planetesimals in the sub-mm ring could be the source of the emission from both in and beyond the sub-mm ring. Maintaining the inner belts and the inner edge to the sub-mm ring may require the presence of three planets in this system including the candidate radial velocity object.",
keywords = "Circumstellar matter, Infrared: stars, Planetary systems, Stars: individual (epsilon Eridani)",
author = "D. Backman and M. Marengo and K. Stapelfeldt and K. Su and D. Wilner and Dowell, {C. D.} and D. Watson and J. Stansberry and Rieke, {George H.} and T. Megeath and G. Fazio and M. Werner",
year = "2009",
doi = "10.1088/0004-637X/690/2/1522",
language = "English (US)",
volume = "690",
pages = "1522--1538",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

TY - JOUR

T1 - Epsilon Eridani's planetary debris disk

T2 - Structure and dynamics based on spitzer and Caltech Submillimeter Observatory observations

AU - Backman, D.

AU - Marengo, M.

AU - Stapelfeldt, K.

AU - Su, K.

AU - Wilner, D.

AU - Dowell, C. D.

AU - Watson, D.

AU - Stansberry, J.

AU - Rieke, George H.

AU - Megeath, T.

AU - Fazio, G.

AU - Werner, M.

PY - 2009

Y1 - 2009

N2 - Spitzer and Caltech Submillimeter Observatory images and spectrophotometry of ε Eridani at wavelengths from 3.5 to 350 μm reveal new details of its bright debris disk. The 350 μm map confirms the presence of a ring at r = 11″-28″(35-90 AU), observed previously at longer sub-mm wavelengths. The Spitzer mid-IR and far-IR images do not show the ring, but rather a featureless disk extending from within a few arcsec of the star across the ring to r 34″ (110 AU). The spectral energy distribution (SED) of the debris system implies a complex structure. A model constrained by the surface brightness profiles and the SED indicates that the sub-mm ring emission is primarily from large (a 135 μm) grains, with smaller (a 15 μm) grains also present in and beyond the ring. The Spitzer Infrared Spectrograph and Multiband Imaging Photometer for Spitzer SED-mode spectrophotometry data clearly show the presence of spatially compact excess emission at λ ≳ 15 μm that requires the presence of two additional narrow belts of dust within the sub-mm ring's central void. The innermost belt at r 3 AU is composed of silicate dust. A simple dynamical model suggests that dust produced collisionally by a population of about 11 M ⊕ of planetesimals in the sub-mm ring could be the source of the emission from both in and beyond the sub-mm ring. Maintaining the inner belts and the inner edge to the sub-mm ring may require the presence of three planets in this system including the candidate radial velocity object.

AB - Spitzer and Caltech Submillimeter Observatory images and spectrophotometry of ε Eridani at wavelengths from 3.5 to 350 μm reveal new details of its bright debris disk. The 350 μm map confirms the presence of a ring at r = 11″-28″(35-90 AU), observed previously at longer sub-mm wavelengths. The Spitzer mid-IR and far-IR images do not show the ring, but rather a featureless disk extending from within a few arcsec of the star across the ring to r 34″ (110 AU). The spectral energy distribution (SED) of the debris system implies a complex structure. A model constrained by the surface brightness profiles and the SED indicates that the sub-mm ring emission is primarily from large (a 135 μm) grains, with smaller (a 15 μm) grains also present in and beyond the ring. The Spitzer Infrared Spectrograph and Multiband Imaging Photometer for Spitzer SED-mode spectrophotometry data clearly show the presence of spatially compact excess emission at λ ≳ 15 μm that requires the presence of two additional narrow belts of dust within the sub-mm ring's central void. The innermost belt at r 3 AU is composed of silicate dust. A simple dynamical model suggests that dust produced collisionally by a population of about 11 M ⊕ of planetesimals in the sub-mm ring could be the source of the emission from both in and beyond the sub-mm ring. Maintaining the inner belts and the inner edge to the sub-mm ring may require the presence of three planets in this system including the candidate radial velocity object.

KW - Circumstellar matter

KW - Infrared: stars

KW - Planetary systems

KW - Stars: individual (epsilon Eridani)

UR - http://www.scopus.com/inward/record.url?scp=62549094048&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=62549094048&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/690/2/1522

DO - 10.1088/0004-637X/690/2/1522

M3 - Article

AN - SCOPUS:62549094048

VL - 690

SP - 1522

EP - 1538

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

ER -