VLT/SPHERE deep insight of NGC 3603’s core: Segregation or confusion?

Khorrami, Zeinab; Lanz, T.; Vakili, F.; Lagadec, E.; Langlois, M.; Brandner, W.; Chesneau, O.; Meyer, M. R.; Carbillet, Marcel; Abe, Lyu; Mouillet, D.; Beuzit, J. L.; Boccaletti, A.; Perrot, C.; Thalmann, Christian; Schmid, H. M.; Pavlov, A.; Costille, A.; Døhlen, K.; Mignant, D. Le; Petit, Cyril; Sauvage, J.-F.

doi:10.1051/0004-6361/201628107

Cited by 16 publications

(17 citation statements)

References 37 publications

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“…It has been shown by Ninkovic (1998) that the Schuster distribution with the slope β = 1.5 (see Equation 2) approximates well the King stellar surface density profile (King 1962). The King profile was originaly obtained for the globular clusters, however, it is also in a good agreement with the observed stellar surface density profiles of young massive clusters (e.g.…”

Section: Physical Modelsupporting

confidence: 62%

The Formation of Secondary Stellar Generations in Massive Young Star Clusters From Rapidly Cooling Shocked Stellar Winds

Wünsch

Palouš

Tenorio-Tagle

et al. 2017

ApJ

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We study a model of rapidly cooling shocked stellar winds in young massive clusters and estimate the circumstances under which secondary star formation, out of the reinserted winds from a first stellar generation (1G), is possible. We have used two implementations of the model: a highly idealized computationally inexpensive spherically symmetric semi-analytic model, and a complex three-dimensional radiation-hydrodynamic simulations, and they are in a good mutual agreement. The results confirm our previous findings that in a cluster with 1G mass 10 7 M and half-mass radius 2.38 pc, the shocked stellar winds become thermally unstable, collapse into dense gaseous structures that partially accumulate inside the cluster, self-shield against ionizing stellar radiation and form the second generation (2G) of stars. We have used the semi-analytic model to explore a subset of the parameter space covering a wide range of the observationally poorly constrained parameters: the heating efficiency, η he , and the mass loading, η ml . The results show that the fraction of the 1G stellar winds accumulating inside the cluster can be larger than 50% if η he 10% which is suggested by the observations. Furthermore, for low η he , the model provides a self-consistent mechanism predicting 2G stars forming only in the central zones of the cluster. Finally, we have calculated the accumulated warm gas emission in the H30α recombination line, analyzed its velocity profile and estimated its intensity for super star clusters in interacting galaxies NGC4038/9 (Antennae) showing that the warm gas should be detectable with ALMA.

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Section: Physical Modelsupporting

confidence: 62%

The Formation of Secondary Stellar Generations in Massive Young Star Clusters From Rapidly Cooling Shocked Stellar Winds

Wünsch

Palouš

Tenorio-Tagle

et al. 2017

ApJ

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“…A.3 middle). Using Starfinder we detected 408 and 288 stars in J and Ks images, respectively (Khorrami et al 2016). Using the same criteria for Starfinder, we only detected 109 and 52 sources in J and Ks images of NGC 3603 at the distance of R 136, which means that more than 70% of the stars cannot be detected.…”

Section: Discussionmentioning

confidence: 99%

Uncrowding R 136 from VLT/SPHERE extreme adaptive optics

Khorrami

Vakili

Lanz

et al. 2017

A&A

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This paper presents the sharpest near-IR images of the massive cluster R 136 to date, based on the extreme adaptive optics of the SPHERE focal instrument implemented on the ESO Very Large Telescope and operated in its IRDIS imaging mode. The crowded stellar population in the core of the R 136 starburst compact cluster remains still to be characterized in terms of individual luminosities, age, mass and multiplicity. SPHERE/VLT and its high contrast imaging possibilities open new windows to make progress on these questions. Stacking-up a few hundreds of short exposures in J and Ks spectral bands over a field of view (FoV) of 10.9 × 12.3 centered on the R 136a1 stellar component, enabled us to carry a refined photometric analysis of the core of R 136. We detected 1110 and 1059 sources in J and Ks images respectively with 818 common sources. Thanks to better angular resolution and dynamic range, we found that more than 62.6% (16.5%) of the stars, detected both in J and Ks data, have neighbours closer than 0.2 (0.1 ). The closest stars are resolved down to the full width at half maximum (FWHM) of the point spread function (PSF) measured by Starfinder. Among resolved and/or detected sources R 136a1 and R 136c have optical companions and R 136a3 is resolved as two stars (PSF fitting) separated by 59 ± 2 mas. This new companion of R 136a3 presents a correlation coefficient of 86% in J and 75% in Ks. The new set of detected sources were used to re-assess the age and extinction of R 136 based on 54 spectroscopically stars that have been recently studied with HST slit-spectroscopy (Crowther et al. 2016, MNRAS, 458, 624) of the core of this cluster. Over 90% of these 54 sources identified visual companions (closer than 0.2 ). We found the most probable age and extinction for these sources are 1.8 +1.2 −0.8 Myr, A J = (0.45 ± 0.5) mag and A K = (0.2 ± 0.5) mag within the photometric and spectroscopic error-bars. Additionally, using PARSEC evolutionary isochrones and tracks, we estimated the stellar mass range for each detected source (common in J and K data) and plotted the generalized histogram of mass (MF with error-bars). Using SPHERE data, we have gone one step further and partially resolved and studied the initial mass function covering mass range of (3-300) M at the age of 1 and 1.5 Myr. The density in the core of R 136 (0.1-1.4 pc) is estimated and extrapolated in 3D and larger radii (up to 6 pc). We show that the stars in the core are still unresolved due to crowding, and the results we obtained are upper limits. Higher angular resolution is mandatory to overcome these difficulties.

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“…comm. ; Khorrami et al 2016) to determine the pixel scale and the correction angle to align the images with the North direction. Since the IFS observations are performed simultaneously with the IRDIS observations, we calibrated the IFS data of HR 2562 using the IRDIS calibration and an additional angle offset accounting for the relative orientation between the two instrument fields of view.…”

Section: Observations and Data Analysismentioning

confidence: 99%

VLT/SPHERE astrometric confirmation and orbital analysis of the brown dwarf companion HR 2562 B

Maire

Rodet

Lazzoni

et al. 2018

A&A

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Context.A low-mass brown dwarf has recently been imaged around HR 2562 (HD 50571), a star hosting a debris disk resolved in the far infrared. Interestingly, the companion location is compatible with an orbit coplanar with the disk and interior to the debris belt. This feature makes the system a valuable laboratory to analyze the formation of substellar companions in a circumstellar disk and potential disk-companion dynamical interactions. Aims. We aim to further characterize the orbital motion of HR 2562 B and its interactions with the host star debris disk. Methods. We performed a monitoring of the system over ∼10 months in 2016 and 2017 with the VLT/SPHERE exoplanet imager. Results. We confirm that the companion is comoving with the star and detect for the first time an orbital motion at high significance, with a current orbital motion projected in the plane of the sky of 25 mas (∼0.85 au) per year. No orbital curvature is seen in the measurements. An orbital fit of the SPHERE and literature astrometry of the companion without priors on the orbital plane clearly indicates that its orbit is (quasi-)coplanar with the disk. To further constrain the other orbital parameters, we used empirical laws for a companion chaotic zone validated by N-body simulations to test the orbital solutions that are compatible with the estimated disk cavity size. Non-zero eccentricities (>0.15) are allowed for orbital periods shorter than 100 yr, while only moderate eccentricities up to ∼0.3 for orbital periods longer than 200 yr are compatible with the disk observations. A comparison of synthetic Herschel images to the real data does not allow us to constrain the upper eccentricity of the companion.

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VLT/SPHERE deep insight of NGC 3603’s core: Segregation or confusion?

Cited by 16 publications

References 37 publications

The Formation of Secondary Stellar Generations in Massive Young Star Clusters From Rapidly Cooling Shocked Stellar Winds

The Formation of Secondary Stellar Generations in Massive Young Star Clusters From Rapidly Cooling Shocked Stellar Winds

Uncrowding R 136 from VLT/SPHERE extreme adaptive optics

VLT/SPHERE astrometric confirmation and orbital analysis of the brown dwarf companion HR 2562 B

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