The multiplicity of massive stars in the Orion Nebula Cluster as seen with long-baseline interferometry

Grellmann, R.; Preibisch, Thomas; Ratzka, Thorsten; Kraus, Stefan; Hełminiak, K. G.; Zinnecker, H.

doi:10.1051/0004-6361/201220192

Cited by 33 publications

(35 citation statements)

References 44 publications

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“…The Galactic O Star Catalog (GOSC-v2, Sota et al 2008) lists 147 O-type stars fulfilling these criteria. Rejecting the Orion stars that have already been observed by the VLTI (Grellmann et al 2013), we are left with 138 possible targets. Twelve of these are flagged as runaway stars in the GOSC and are handled separately from the main target list.…”

Section: Observational Samplementioning

confidence: 99%

Southern Massive Stars at High Angular Resolution: Observational Campaign and Companion Detection

Sana

Bouquin

Lacour

et al. 2014

ApJS

Self Cite

584

476

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Multiplicity is one of the most fundamental observable properties of massive O-type stars and offers a promising way to discriminate between massive star formation theories. Nevertheless, companions at separations between 1 and 100 milli-arcsec (mas) remain mostly unknown due to intrinsic observational limitations. At a typical distance of 2 kpc, this corresponds to projected physical separations of 2-200 AU. The Southern MAssive Stars at High angular resolution survey (smash+) was designed to fill this gap by providing the first systematic interferometric survey of Galactic massive stars. We observed 117 O-type stars with VLTI/PIONIER and 162 O-type stars with NACO/SAM, respectively probing the separation ranges 1-45 and 30-250 mas and brightness contrasts of ∆H < 4 and ∆H < 5. Taking advantage of NACO's field-of-view, we further uniformly searched for visual companions in an 8 -radius down to ∆H = 8. This paper describes the observations and data analysis, reports the discovery of almost 200 new companions in the separation range from 1 mas to 8 and presents the catalog of detections, including the first resolved measurements of over a dozen known long-period spectroscopic binaries.Excluding known runaway stars for which no companions are detected, 96 objects in our main sample (δ < 0 • ; H < 7.5) were observed both with PIONIER and NACO/SAM. The fraction of these stars with at least one resolved companion within 200 mas is 0.53. Accounting for known but unresolved spectroscopic or eclipsing companions, the multiplicity fraction at separation ρ < 8 increases to f m = 0.91 ± 0.03. The fraction of luminosity class V stars that have a bound companion reaches 100% at 30 mas while their average number of physically connected companions within 8 is f c = 2.2 ± 0.3. This demonstrates that massive stars form nearly exclusively in multiple systems. The nine non-thermal radio emitters observed by smash+ are all resolved, including the newly discovered pairs HD 168112 and CPD−47 • 2963. This lends strong support to the universality of the wind-wind collision scenario to explain the non-thermal emission from O-type stars.

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Section: Observational Samplementioning

confidence: 99%

Southern Massive Stars at High Angular Resolution: Observational Campaign and Companion Detection

Sana

Bouquin

Lacour

et al. 2014

ApJS

Self Cite

584

476

View full text Add to dashboard Cite

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“…One of the components has been detected through adaptive optics and Very Large Telescope Interferometer (VLTI) imaging (Close et al 2013;Grellmann et al 2013), with a projected separation of~ 0. 2 or ∼70 au.…”

Section: Appendix a λ Ori Scatteringmentioning

confidence: 99%

The Gould’s Belt Distances Survey (Gobelins). Ii. Distances and Structure Toward the Orion Molecular Clouds

Kounkel

Hartmann

Loinard

et al. 2017

ApJ

225

179

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We present the results of the Gould's Belt Distances Survey of young star-forming regions toward the Orion Molecular Cloud Complex. We detected 36 young stellar objects (YSOs) with the Very Large Baseline Array, 27 of which have been observed in at least three epochs over the course of two years. At least half of these YSOs belong to multiple systems. We obtained parallax and proper motions toward these stars to study the structure and kinematics of the Complex. We measured a distance of 388±5 pc toward the Orion Nebula Cluster, 428±10 pc toward the southern portion L1641, 388±10 pc toward NGC 2068, and roughly ∼420 pc toward NGC 2024. Finally, we observed a strong degree of plasma radio scattering toward λ Ori.

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“…with spectral types B0.5V. Both are also binary systems with a lower mass companion 43 . θ 1 Ori B is only 7 M !…”

Section: Sofia Observationsmentioning

confidence: 99%

Three-Dimensional Hydrodynamic Simulations of Multiphase Galactic Disks With Star Formation Feedback. I. Regulation of Star Formation Rates

Kim

Ostriker

Kim

2013

ApJ

226

257

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Mechanical and radiative energy input by massive stars stir up the environment, heat the gas, produce cloud & intercloud phases in the interstellar medium and disrupt molecular clouds, the birthsites of new stars 1,2 . Ionization by UV photons, stellar wind action and supernova explosions control molecular clouds lifetimes 3,4,5,6,7 . Theoretical studies predict that momentum injection by radiation dominates by far over momentum injected by a stellar wind 8 , but this has hitherto been difficult to assess observationally. Velocity-resolved large-scale images in the fine structure line of ionized carbon ([CII]) provide an observational diagnostic of the radiative energetics and the dynamics of the ISM in the immediate vicinity of massive stars. Here, we present the [CII] 1.9 THz (158 µm) study of ~1 square degree region (~7pc in diameter) at a resolution of 16" (0.03pc) of the nearest region of massive star formation, Orion. The results reveal that the stellar wind originating from the star, θ 1 Ori C, has created a ~2pc sized bubble by sweeping up a 2600 M ! shell expanding at 13 km/s. This shows that the stellar wind mechanical energy is coupled very efficiently to the molecular core and its action dominates over photoionization/evaporation or future supernova explosions.We have surveyed one square degree of the Orion Molecular cloud, centered on the Trapezium cluster and the Orion Molecular Core 1 (OMC-1) behind it, in the 1.9 THz (158µm) [CII] fine-structure line with the 14 pixel upGREAT heterodyne highspectral resolution spectrometer 9 on board of the Stratospheric Observatory For Infrared Astronomy (SOFIA) (see method). Figure 1 compares the [CII] integrated intensity map with the mid-IR and far-IR maps due to UV-pumped fluorescence by polycyclic aromatic hydrocarbon (PAHs) molecules and thermal dust continuum emission, respectively. Each map clearly shows the direct interaction of the Trapezium cluster with the dense molecular core (center), the large, wind-blown bubble, associated with the Orion Veil (South), and the bubble created by the B stars illuminating the reflection nebulae, NGC 1973, 1975. Here, we focus on the prominent Veil bubble associated with the stellar wind from θ 1 Ori C. This shell consists of neutral atomic (H) gas and is very prominent in the [CII] map but there is no detectable counterpart in carbon monoxide, H 2 , or other molecular tracers as the shell is too tenuous for these species to persist; e.g., H 2 /H fraction <2x10 -4 and C/C + =10 -4 10,11 . Likewise, the complex pattern of absorption and emission features and the presence of multiple (foreground) components preclude recognition of the large scale structure of the shell in 21cm HI studies 12 . X-ray observations 13 have shown that this bubble is filled with tenuous (~1cm -3 ) hot (2x10 6 K) gas created by the strong stellar wind (mechanical luminosity, L w =8x10 35 erg/s 14,15 ) from the most massive star in the region, θ 1 Ori C (see Extended Data Figure 5).While each IR image ( Fig. 1) traces the Veil morphology, only [...

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The multiplicity of massive stars in the Orion Nebula Cluster as seen with long-baseline interferometry

Cited by 33 publications

References 44 publications

Southern Massive Stars at High Angular Resolution: Observational Campaign and Companion Detection

Southern Massive Stars at High Angular Resolution: Observational Campaign and Companion Detection

The Gould’s Belt Distances Survey (Gobelins). Ii. Distances and Structure Toward the Orion Molecular Clouds

Three-Dimensional Hydrodynamic Simulations of Multiphase Galactic Disks With Star Formation Feedback. I. Regulation of Star Formation Rates

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