MAGELLAN AO SYSTEM z′, y S, and L′ OBSERVATIONS of the VERY WIDE 650 AU HD 106906 PLANETARY SYSTEM

Ya Lin Wu, Laird M Close, Vanessa P. Bailey, Timothy J. Rodigas, Jared R. Males, Katie M. Morzinski, Katherine B. Follette, Philip M Hinz, Alfio Puglisi, Runa Briguglio, Marco Xompero

Research output: Contribution to journalArticle

6 Citations (Scopus)

Abstract

We analyze archival data from Bailey and co-workers from the Magellan adaptive optics system and present the first 0.9 μm detection (z′ = 20.3 ±0.4 mag; Δz′ = 13.0 ±0.4 mag) of the 11 M Jup circumbinary planet HD 106906AB b, as well as 1 and 3.8 μm detections of the debris disk around the binary. The disk has an east-west asymmetry in length and surface brightness, especially at 3.8 μm where the disk appears to be one-sided. The spectral energy distribution of b, when scaled to the K S-band photometry, is consistent with 1800 K atmospheric models without significant dust reddening, unlike some young, very red, low-mass companions such as CT Cha B and 1RXS 1609 B. Therefore, the suggested circumplanetary disk of Kalas and co-workers might not contain much material, or might be closer to face-on. Finally, we suggest that the widest (a 100 AU) low mass ratio (M p/M ≡ q ≲ 0.01) companions may have formed inside protoplanetary disks but were later scattered by binary/planet interactions. Such a scattering event may have occurred for HD 106906AB b with its central binary star, but definitive proof at this time is elusive.

Original languageEnglish (US)
Article number24
JournalAstrophysical Journal
Volume823
Issue number1
DOIs
StatePublished - May 20 2016

Fingerprint

planetary systems
planet
planets
asymmetry
scattering
dust
protoplanetary disks
atmospheric models
S band
binary stars
spectral energy distribution
adaptive optics
debris
mass ratios
photometry
energy
brightness
detection
interactions
distribution

Keywords

  • circumstellar matter
  • instrumentation: adaptive optics
  • planets and satellites: individual (HD 106906AB b)
  • stars: individual (HD 106906AB)
  • techniques: high angular resolution

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

MAGELLAN AO SYSTEM z′, y S, and L′ OBSERVATIONS of the VERY WIDE 650 AU HD 106906 PLANETARY SYSTEM. / Wu, Ya Lin; Close, Laird M; Bailey, Vanessa P.; Rodigas, Timothy J.; Males, Jared R.; Morzinski, Katie M.; Follette, Katherine B.; Hinz, Philip M; Puglisi, Alfio; Briguglio, Runa; Xompero, Marco.

In: Astrophysical Journal, Vol. 823, No. 1, 24, 20.05.2016.

Research output: Contribution to journalArticle

Wu, YL, Close, LM, Bailey, VP, Rodigas, TJ, Males, JR, Morzinski, KM, Follette, KB, Hinz, PM, Puglisi, A, Briguglio, R & Xompero, M 2016, 'MAGELLAN AO SYSTEM z′, y S, and L′ OBSERVATIONS of the VERY WIDE 650 AU HD 106906 PLANETARY SYSTEM', Astrophysical Journal, vol. 823, no. 1, 24. https://doi.org/10.3847/0004-637X/823/1/24
Wu, Ya Lin ; Close, Laird M ; Bailey, Vanessa P. ; Rodigas, Timothy J. ; Males, Jared R. ; Morzinski, Katie M. ; Follette, Katherine B. ; Hinz, Philip M ; Puglisi, Alfio ; Briguglio, Runa ; Xompero, Marco. / MAGELLAN AO SYSTEM z′, y S, and L′ OBSERVATIONS of the VERY WIDE 650 AU HD 106906 PLANETARY SYSTEM. In: Astrophysical Journal. 2016 ; Vol. 823, No. 1.
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AB - We analyze archival data from Bailey and co-workers from the Magellan adaptive optics system and present the first 0.9 μm detection (z′ = 20.3 ±0.4 mag; Δz′ = 13.0 ±0.4 mag) of the 11 M Jup circumbinary planet HD 106906AB b, as well as 1 and 3.8 μm detections of the debris disk around the binary. The disk has an east-west asymmetry in length and surface brightness, especially at 3.8 μm where the disk appears to be one-sided. The spectral energy distribution of b, when scaled to the K S-band photometry, is consistent with 1800 K atmospheric models without significant dust reddening, unlike some young, very red, low-mass companions such as CT Cha B and 1RXS 1609 B. Therefore, the suggested circumplanetary disk of Kalas and co-workers might not contain much material, or might be closer to face-on. Finally, we suggest that the widest (a 100 AU) low mass ratio (M p/M ∗ ≡ q ≲ 0.01) companions may have formed inside protoplanetary disks but were later scattered by binary/planet interactions. Such a scattering event may have occurred for HD 106906AB b with its central binary star, but definitive proof at this time is elusive.

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