High-resolution images of orbital motion in the Orion Trapezium cluster with the LBT AO system

Laird M Close, A. Puglisi, J. R. Males, C. Arcidiacono, A. Skemer, J. C. Guerra, L. Busoni, G. Brusa, E. Pinna, D. L. Miller, A. Riccardi, Donald W Mccarthy, M. Xompero, C. Kulesa, F. Quiros-Pacheco, J. Argomedo, J. Brynnel, S. Esposito, F. Mannucci, K. BoutsiaL. Fini, D. J. Thompson, J. M. Hill, C. E. Woodward, R. Briguglio, T. J. Rodigas, R. Briguglio, P. Stefanini, G. Agapito, Philip M Hinz, K. Follette, R. Green

Research output: Contribution to journalArticle

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Abstract

The new 8.4m LBT adaptive secondary AO system, with its novel pyramid wavefront sensor, was used to produce very high Strehl (≳ 75% at 2.16 μm) near-infrared narrowband (Brγ: 2.16 μm and [Fe II]: 1.64 μm) images of 47young (∼1 Myr) Orion Trapezium θ1 Ori cluster members. The inner ∼41 × 53″ of the cluster was imaged at spatial resolutions of ∼0″.050 (at 1.64 μm). A combination of high spatial resolution and high S/N yielded relative binary positions to ∼0.5 mas accuracies. Including previous speckle data, we analyze a 15year baseline of high-resolution observations of this cluster. We are now sensitive to relative proper motions of just ∼0.3 mas yr-1 (0.6kms-1 at 450 pc); this is a ∼7 × improvement in orbital velocity accuracy compared to previous efforts. We now detect clear orbital motions in the θ1 Ori B2 B3 system of 4.9 ± 0.3kms-1 and 7.2 ± 0.8kms-1 in the θ1 Ori A1 A2 system (with correlations of P.A. versus time at >99% confidence). All five members of the θ1 Ori B system appear likely a gravitationally bound "mini-cluster." The very lowest mass member of the θ1 Ori B system (B4; mass ∼0.2 M) has, for the first time, a clearly detected motion (at 4.3 ± 2.0kms-1; correlation = 99.7%) w.r.t. B1. However, B4 is most likely in a long-term unstable (non-hierarchical) orbit and may "soon" be ejected from this "mini-cluster." This "ejection" process could play a major role in the formation of low-mass stars and brown dwarfs.

Original languageEnglish (US)
Article number180
JournalAstrophysical Journal
Volume749
Issue number2
DOIs
StatePublished - Apr 20 2012

Fingerprint

image resolution
orbits
high resolution
spatial resolution
speckle
near infrared
orbital velocity
sensor
proper motion
pyramids
ejection
narrowband
confidence
stars
sensors

Keywords

  • binaries: general
  • brown dwarfs
  • instrumentation: adaptive optics
  • stars: evolution
  • stars: formation
  • stars: low-mass

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Close, L. M., Puglisi, A., Males, J. R., Arcidiacono, C., Skemer, A., Guerra, J. C., ... Green, R. (2012). High-resolution images of orbital motion in the Orion Trapezium cluster with the LBT AO system. Astrophysical Journal, 749(2), [180]. https://doi.org/10.1088/0004-637X/749/2/180

High-resolution images of orbital motion in the Orion Trapezium cluster with the LBT AO system. / Close, Laird M; Puglisi, A.; Males, J. R.; Arcidiacono, C.; Skemer, A.; Guerra, J. C.; Busoni, L.; Brusa, G.; Pinna, E.; Miller, D. L.; Riccardi, A.; Mccarthy, Donald W; Xompero, M.; Kulesa, C.; Quiros-Pacheco, F.; Argomedo, J.; Brynnel, J.; Esposito, S.; Mannucci, F.; Boutsia, K.; Fini, L.; Thompson, D. J.; Hill, J. M.; Woodward, C. E.; Briguglio, R.; Rodigas, T. J.; Briguglio, R.; Stefanini, P.; Agapito, G.; Hinz, Philip M; Follette, K.; Green, R.

In: Astrophysical Journal, Vol. 749, No. 2, 180, 20.04.2012.

Research output: Contribution to journalArticle

Close, LM, Puglisi, A, Males, JR, Arcidiacono, C, Skemer, A, Guerra, JC, Busoni, L, Brusa, G, Pinna, E, Miller, DL, Riccardi, A, Mccarthy, DW, Xompero, M, Kulesa, C, Quiros-Pacheco, F, Argomedo, J, Brynnel, J, Esposito, S, Mannucci, F, Boutsia, K, Fini, L, Thompson, DJ, Hill, JM, Woodward, CE, Briguglio, R, Rodigas, TJ, Briguglio, R, Stefanini, P, Agapito, G, Hinz, PM, Follette, K & Green, R 2012, 'High-resolution images of orbital motion in the Orion Trapezium cluster with the LBT AO system', Astrophysical Journal, vol. 749, no. 2, 180. https://doi.org/10.1088/0004-637X/749/2/180
Close, Laird M ; Puglisi, A. ; Males, J. R. ; Arcidiacono, C. ; Skemer, A. ; Guerra, J. C. ; Busoni, L. ; Brusa, G. ; Pinna, E. ; Miller, D. L. ; Riccardi, A. ; Mccarthy, Donald W ; Xompero, M. ; Kulesa, C. ; Quiros-Pacheco, F. ; Argomedo, J. ; Brynnel, J. ; Esposito, S. ; Mannucci, F. ; Boutsia, K. ; Fini, L. ; Thompson, D. J. ; Hill, J. M. ; Woodward, C. E. ; Briguglio, R. ; Rodigas, T. J. ; Briguglio, R. ; Stefanini, P. ; Agapito, G. ; Hinz, Philip M ; Follette, K. ; Green, R. / High-resolution images of orbital motion in the Orion Trapezium cluster with the LBT AO system. In: Astrophysical Journal. 2012 ; Vol. 749, No. 2.
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abstract = "The new 8.4m LBT adaptive secondary AO system, with its novel pyramid wavefront sensor, was used to produce very high Strehl (≳ 75{\%} at 2.16 μm) near-infrared narrowband (Brγ: 2.16 μm and [Fe II]: 1.64 μm) images of 47young (∼1 Myr) Orion Trapezium θ1 Ori cluster members. The inner ∼41 × 53″ of the cluster was imaged at spatial resolutions of ∼0″.050 (at 1.64 μm). A combination of high spatial resolution and high S/N yielded relative binary positions to ∼0.5 mas accuracies. Including previous speckle data, we analyze a 15year baseline of high-resolution observations of this cluster. We are now sensitive to relative proper motions of just ∼0.3 mas yr-1 (0.6kms-1 at 450 pc); this is a ∼7 × improvement in orbital velocity accuracy compared to previous efforts. We now detect clear orbital motions in the θ1 Ori B2 B3 system of 4.9 ± 0.3kms-1 and 7.2 ± 0.8kms-1 in the θ1 Ori A1 A2 system (with correlations of P.A. versus time at >99{\%} confidence). All five members of the θ1 Ori B system appear likely a gravitationally bound {"}mini-cluster.{"} The very lowest mass member of the θ1 Ori B system (B4; mass ∼0.2 M⊙) has, for the first time, a clearly detected motion (at 4.3 ± 2.0kms-1; correlation = 99.7{\%}) w.r.t. B1. However, B4 is most likely in a long-term unstable (non-hierarchical) orbit and may {"}soon{"} be ejected from this {"}mini-cluster.{"} This {"}ejection{"} process could play a major role in the formation of low-mass stars and brown dwarfs.",
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AU - Close, Laird M

AU - Puglisi, A.

AU - Males, J. R.

AU - Arcidiacono, C.

AU - Skemer, A.

AU - Guerra, J. C.

AU - Busoni, L.

AU - Brusa, G.

AU - Pinna, E.

AU - Miller, D. L.

AU - Riccardi, A.

AU - Mccarthy, Donald W

AU - Xompero, M.

AU - Kulesa, C.

AU - Quiros-Pacheco, F.

AU - Argomedo, J.

AU - Brynnel, J.

AU - Esposito, S.

AU - Mannucci, F.

AU - Boutsia, K.

AU - Fini, L.

AU - Thompson, D. J.

AU - Hill, J. M.

AU - Woodward, C. E.

AU - Briguglio, R.

AU - Rodigas, T. J.

AU - Briguglio, R.

AU - Stefanini, P.

AU - Agapito, G.

AU - Hinz, Philip M

AU - Follette, K.

AU - Green, R.

PY - 2012/4/20

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N2 - The new 8.4m LBT adaptive secondary AO system, with its novel pyramid wavefront sensor, was used to produce very high Strehl (≳ 75% at 2.16 μm) near-infrared narrowband (Brγ: 2.16 μm and [Fe II]: 1.64 μm) images of 47young (∼1 Myr) Orion Trapezium θ1 Ori cluster members. The inner ∼41 × 53″ of the cluster was imaged at spatial resolutions of ∼0″.050 (at 1.64 μm). A combination of high spatial resolution and high S/N yielded relative binary positions to ∼0.5 mas accuracies. Including previous speckle data, we analyze a 15year baseline of high-resolution observations of this cluster. We are now sensitive to relative proper motions of just ∼0.3 mas yr-1 (0.6kms-1 at 450 pc); this is a ∼7 × improvement in orbital velocity accuracy compared to previous efforts. We now detect clear orbital motions in the θ1 Ori B2 B3 system of 4.9 ± 0.3kms-1 and 7.2 ± 0.8kms-1 in the θ1 Ori A1 A2 system (with correlations of P.A. versus time at >99% confidence). All five members of the θ1 Ori B system appear likely a gravitationally bound "mini-cluster." The very lowest mass member of the θ1 Ori B system (B4; mass ∼0.2 M⊙) has, for the first time, a clearly detected motion (at 4.3 ± 2.0kms-1; correlation = 99.7%) w.r.t. B1. However, B4 is most likely in a long-term unstable (non-hierarchical) orbit and may "soon" be ejected from this "mini-cluster." This "ejection" process could play a major role in the formation of low-mass stars and brown dwarfs.

AB - The new 8.4m LBT adaptive secondary AO system, with its novel pyramid wavefront sensor, was used to produce very high Strehl (≳ 75% at 2.16 μm) near-infrared narrowband (Brγ: 2.16 μm and [Fe II]: 1.64 μm) images of 47young (∼1 Myr) Orion Trapezium θ1 Ori cluster members. The inner ∼41 × 53″ of the cluster was imaged at spatial resolutions of ∼0″.050 (at 1.64 μm). A combination of high spatial resolution and high S/N yielded relative binary positions to ∼0.5 mas accuracies. Including previous speckle data, we analyze a 15year baseline of high-resolution observations of this cluster. We are now sensitive to relative proper motions of just ∼0.3 mas yr-1 (0.6kms-1 at 450 pc); this is a ∼7 × improvement in orbital velocity accuracy compared to previous efforts. We now detect clear orbital motions in the θ1 Ori B2 B3 system of 4.9 ± 0.3kms-1 and 7.2 ± 0.8kms-1 in the θ1 Ori A1 A2 system (with correlations of P.A. versus time at >99% confidence). All five members of the θ1 Ori B system appear likely a gravitationally bound "mini-cluster." The very lowest mass member of the θ1 Ori B system (B4; mass ∼0.2 M⊙) has, for the first time, a clearly detected motion (at 4.3 ± 2.0kms-1; correlation = 99.7%) w.r.t. B1. However, B4 is most likely in a long-term unstable (non-hierarchical) orbit and may "soon" be ejected from this "mini-cluster." This "ejection" process could play a major role in the formation of low-mass stars and brown dwarfs.

KW - binaries: general

KW - brown dwarfs

KW - instrumentation: adaptive optics

KW - stars: evolution

KW - stars: formation

KW - stars: low-mass

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