Orbital motion of the massive multiple stars  in the Orion Trapezium

Schertl, D.; Balega, Yu. Yu.; Preibisch, Thomas; Weigelt, G.

doi:10.1051/0004-6361:20030225

Cited by 51 publications

(90 citation statements)

References 28 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The saturation of θ 1 Orionis A and B does not allow us to provide any useful relative photometry in the broad band filters. Standard PSF photometry of the B4 companion gives H = 11.2 and Ks = 10.6 mag, consistent with the results of Simon et al (1999) and Schertl et al (2003). Four additional previously known binaries (TCC-101, TCC-094, TCC-075, and TCC-105, McCaughrean & Stauffer 1994) are resolved in the MAD images.…”

Section: Multiple Systemssupporting

confidence: 82%

Multi-conjugate adaptive optics images of the Trapezium cluster

Bouy¹,

Kolb

Marchetti

et al. 2007

A&A

View full text Add to dashboard Cite

Context. Multi-conjugate adaptive optics (MCAO) combine the advantages of both standard adaptive optics, which provide high contrast and high spatial resolution, and of wide field imaging (≈1 ). Up to recently, MCAO for astronomy was limited to laboratory experiments. In this paper, we present the first scientific results obtained with the first MCAO instrument. Aims. We present a new study of the Trapezium cluster using deep MCAO images with a field of view of 1 × 1 obtained at the VLT. Methods. We used deep J, H, and Ks images recently obtained with the prototype MCAO facility MAD at the VLT to search for new members and new multiple systems in the Trapezium cluster. On bright targets (Ks ≈ 9 mag), these images allow us to reach ∆Ks ≈ 6 mag as close as 0 . 4. Results. We report detection of 128 sources, including 10 new faint objects in the magnitude range between 16.1 < Ks < 17.9 mag. In addition to all previously known multiple systems with separations greater than 0 . 1, we confirm the multiplicity of TCC-055. We also report the detection in J, H, and Ks of a very red extended embedded protostellar object, HC 419, previously detected only in the thermal infrared. Conclusions. Analysis of the first MCAO images obtained on the sky demonstrates not only the technical feasibility of MCAO, but also its great potential and versatility in terms of scientific output.

show abstract

Section: Multiple Systemssupporting

confidence: 82%

Multi-conjugate adaptive optics images of the Trapezium cluster

Bouy¹,

Kolb

Marchetti

et al. 2007

A&A

View full text Add to dashboard Cite

show abstract

“…Since the relative velocity of A2 with respect to A1 is more than four times larger than this value it is highly unlikely that we see a random chance projection of unrelated stars. Furthermore, as discussed in Schertl et al (2003), the probability to see a chance projected star with a K-band magnitude of ≤9 at an angular separation of ≤1 to the position of A1 is only 0.4%. Thus, although the observed motion is still linear and shows no significant curvature, we conclude that it is probably part of an binary orbit seen under a relatively high inclination.…”

Section: θ 1 Ori Amentioning

confidence: 98%

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

Grellmann

Preibisch

Ratzka

et al. 2013

A&A

View full text Add to dashboard Cite

Context. The characterization of multiple stellar systems is an important ingredient for testing current star formation models. Stars are more often found in multiple systems, the more massive they are. A complete knowledge of the multiplicity of high-mass stars over the full range of orbit separations is thus essential to understand their still debated formation process. Aims. Infrared long baseline interferometry is very well suited to close the gap between spectroscopic and adaptive optics searches. Observations of the Orion Nebula Cluster (ONC) in general and the Trapezium Cluster in particular can help to answer the question about the origin and evolution of multiple stars. Earlier studies provide a good knowledge about the multiplicity of the stars at very small (spectroscopic companions) and large separations (AO, speckle companions) and thus make the ONC a good target for such a project. Methods. We used the near infrared interferometric instrument AMBER at ESOs Very Large Telescope Interferometer to observe a sample of bright stars in the ONC. We complement our data set by archival NACO observations of θ 1 Ori A to obtain more information about the orbit of the close visual companion. Results. Our observations resolve the known multiple systems θ 1 Ori C and θ 1 Ori A and provide new orbit points, which confirm the predicted orbit and the determined stellar parameters for θ 1 Ori C. Combining AMBER and NACO data for θ 1 Ori A we were able to follow the (orbital) motion of the companion from 2003 to 2011. We furthermore find hints for a companion around θ 1 Ori D, whose existence has been suggested already before, and a previously unknown companion to NU Ori. With a probability of ∼90% we can exclude further companions with masses of ≥3 M around our sample stars for separations between ∼2 mas and ∼110 mas. Conclusions. We conclude that the companion around θ 1 Ori A is most likely physically related to the primary star and not only a chance projected star. The newly discovered possible companions further increase the multiplicity in the ONC. For our sample of two O and three B-type stars we find on average 2.5 known companions per primary, which is around five times more than for low-mass stars.

show abstract

“…The high-mass population exhibits a higher binary frequency than the low-mass primaries (Preibisch et al 1999;Schertl et al 2003;Köhler et al 2006). For the ONC, we use the study of Reipurth et al (2007), who find 75 binaries and 3 triples among 781 ONC members.…”

Section: Orion Nebula Clustermentioning

confidence: 99%

Inverse dynamical population synthesis

Marks

Kroupa

2012

A&A

253

302

View full text Add to dashboard Cite

Binary populations in young star clusters show multiplicity fractions both lower and up to twice as high as those observed in the Galactic field. We follow the evolution of a population of binary stars in dense and loose star clusters starting with an invariant initial binary population and a formal multiplicity fraction of unity, and demonstrate that these models can explain the observed binary properties in Taurus, ρ Ophiuchus, Chamaeleon, Orion, IC 348, Upper Scorpius A, Praesepe, and the Pleiades. The model needs to consider solely different birth densities for these regions. The evolved theoretical orbital-parameter distributions are highly probable parent distributions for the observed ones. We constrain the birth conditions (stellar mass, M ecl , and half-mass radius, r h ) for the derived progenitors of the star clusters and the overall present-day binary fractions allowed by the present model. The results compare very well with properties of molecular cloud clumps on the verge of star formation. Combining these with previously and independently obtained constraints on the birth densities of globular clusters, we identify a weak stellar mass -half-mass radius correlation for cluster-forming cloud clumps, r h /pc ∝ (M ecl /M ) 0.13 ± 0.04 . The ability of the model to reproduce the binary properties in all the investigated young objects, covering present-day densities from 1−10 stars pc −3 (Taurus) to 2 × 10 4 stars pc −3 (Orion), suggests that environment-dependent dynamical evolution plays an important role in shaping the present-day properties of binary populations in star clusters, and that the initial binary properties may not vary dramatically between different environments.

show abstract

Orbital motion of the massive multiple stars in the Orion Trapezium

Cited by 51 publications

References 28 publications

Multi-conjugate adaptive optics images of the Trapezium cluster

Multi-conjugate adaptive optics images of the Trapezium cluster

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

Inverse dynamical population synthesis

Contact Info

Product

Resources

About