The Gemini NICI planet-finding campaign: The offset ring of HR 4796 A

Zahed Wahhaj, Michael C. Liu, Beth A. Biller, Eric L. Nielsen, Thomas L. Hayward, Marc Kuchner, Laird M Close, Mark Chun, Christ Ftaclas, Douglas W. Toomey

Research output: Contribution to journalArticle

15 Citations (Scopus)

Abstract

We present J,H, CH4 short (1.578 μm), CH4 long (1.652 μm) and Ks-band images of the dust ring around the 10 Myr old star HR 4796 A obtained using the Near Infrared Coronagraphic Imager (NICI) on the Gemini-South 8.1 m Telescope. Our images clearly show for the first time the position of the star relative to its circumstellar ring thanks to NICI's translucent focal plane occulting mask. We employ a Bayesian Markov chain Monte Carlo method to constrain the offset vector between the two. The resulting probability distribution shows that the ring center is offset from the star by 16.7 ± 1.3 milliarcseconds along a position angle of 26 ± 3°, along the PA of the ring, 26.47 ± 0.04°. We find that the size of this offset is not large enough to explain the brightness asymmetry of the ring. The ring is measured to have mostly red reflectivity across the JHKs filters, which seems to indicate micron-sized grains. Just like Neptune's 3:2 and 2:1 mean-motion resonances delineate the inner and outer edges of the classical Kuiper belt, we find that the radial extent of the HR 4796 A and the Fomalhaut rings could correspond to the 3:2 and 2:1 mean-motion resonances of hypothetical planets at 54.7 AU and 97.7 AU in the two systems, respectively. A planet orbiting HR 4796 A at 54.7 AU would have to be less massive than 1.6 MJup so as not to widen the ring too much by stirring.

Original languageEnglish (US)
Article numberA34
JournalAstronomy and Astrophysics
Volume567
DOIs
StatePublished - 2014

Fingerprint

planets
near infrared
planet
Neptune
rings
Markov chain
reflectivity
asymmetry
dust
filter
stars
hypothetical planets
Kuiper belt
Neptune (planet)
Markov chains
stirring
Monte Carlo method
brightness
masks
telescopes

Keywords

  • Infrared: planetary systems
  • Instrumentation: adaptive optics
  • Kuiper belt: general
  • Methods: statistical
  • Planet-disk interactions
  • Techniques: high angular resolution

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Wahhaj, Z., Liu, M. C., Biller, B. A., Nielsen, E. L., Hayward, T. L., Kuchner, M., ... Toomey, D. W. (2014). The Gemini NICI planet-finding campaign: The offset ring of HR 4796 A. Astronomy and Astrophysics, 567, [A34]. https://doi.org/10.1051/0004-6361/201323335

The Gemini NICI planet-finding campaign : The offset ring of HR 4796 A. / Wahhaj, Zahed; Liu, Michael C.; Biller, Beth A.; Nielsen, Eric L.; Hayward, Thomas L.; Kuchner, Marc; Close, Laird M; Chun, Mark; Ftaclas, Christ; Toomey, Douglas W.

In: Astronomy and Astrophysics, Vol. 567, A34, 2014.

Research output: Contribution to journalArticle

Wahhaj, Z, Liu, MC, Biller, BA, Nielsen, EL, Hayward, TL, Kuchner, M, Close, LM, Chun, M, Ftaclas, C & Toomey, DW 2014, 'The Gemini NICI planet-finding campaign: The offset ring of HR 4796 A', Astronomy and Astrophysics, vol. 567, A34. https://doi.org/10.1051/0004-6361/201323335
Wahhaj, Zahed ; Liu, Michael C. ; Biller, Beth A. ; Nielsen, Eric L. ; Hayward, Thomas L. ; Kuchner, Marc ; Close, Laird M ; Chun, Mark ; Ftaclas, Christ ; Toomey, Douglas W. / The Gemini NICI planet-finding campaign : The offset ring of HR 4796 A. In: Astronomy and Astrophysics. 2014 ; Vol. 567.
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AB - We present J,H, CH4 short (1.578 μm), CH4 long (1.652 μm) and Ks-band images of the dust ring around the 10 Myr old star HR 4796 A obtained using the Near Infrared Coronagraphic Imager (NICI) on the Gemini-South 8.1 m Telescope. Our images clearly show for the first time the position of the star relative to its circumstellar ring thanks to NICI's translucent focal plane occulting mask. We employ a Bayesian Markov chain Monte Carlo method to constrain the offset vector between the two. The resulting probability distribution shows that the ring center is offset from the star by 16.7 ± 1.3 milliarcseconds along a position angle of 26 ± 3°, along the PA of the ring, 26.47 ± 0.04°. We find that the size of this offset is not large enough to explain the brightness asymmetry of the ring. The ring is measured to have mostly red reflectivity across the JHKs filters, which seems to indicate micron-sized grains. Just like Neptune's 3:2 and 2:1 mean-motion resonances delineate the inner and outer edges of the classical Kuiper belt, we find that the radial extent of the HR 4796 A and the Fomalhaut rings could correspond to the 3:2 and 2:1 mean-motion resonances of hypothetical planets at 54.7 AU and 97.7 AU in the two systems, respectively. A planet orbiting HR 4796 A at 54.7 AU would have to be less massive than 1.6 MJup so as not to widen the ring too much by stirring.

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KW - Methods: statistical

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