Near-infrared interferometry of <i>η</i> Carinae with spectral resolutions of 1 500 and 12 000 using AMBER/VLTI

Weigelt, G.; Kraus, Stefan; Driebe, T.; Petrov, R.; Hofmann, K.-H.; Millour, F.; Chesneau, O.; Schertl, D.; Malbet, Fabien; Hillier, John; Gull, Theodore R.; Davidson, Kris; Souza, A. Domiciano de; Antonelli, P.; Beckmann, U.; Bresson, Y.; Chelli, A.; Dugué, M.; Duvert, G.; Gennari, S.; Glück, L.; Kern, P.; Lagarde, S.; Coarer, E. Le; Lisi, F.; Perraut, K.; Puget, P.; Rantakyrö, F.; Robbe-Dubois, S.; Roussel, Alain; Tatulli, E.; Zins, G.; Accardo, M.; Acke, B.; Agabi, Karim; Altariba, E.; Arezki, B.; Aristidi, Éric; Baffa, C.; Behrend, J.; Blöcker, T.; Bonhomme, S.; Busoni, S.; Cassaing, F.; Clausse, J. M.; Colin, J.; Connot, C.; Delboulbé, A.; Feautrier, Philippe; Ferruzzi, D.; Forveille, T.; Fossat, E.; Foy, R.; Fraix-Burnet, Didier; Gallardo, Aurelio; Giani, E.; Gil, C.; Glentzlin, A.; Heiden, M.; Heininger, M.; Utrera, O. Hernández; Kamm, D.; Kiekebusch, M.; Contel, D. Le; Contel, J. M. Le; Lesourd, T.; López, B.; López, M.; Magnard, Y.; Marconi, A.; Mars, G.; Martinot-Lagarde, G.; Mathias, P.; Mège, P.; Monin, Jean‐Louis; Mouillet, D.; Mourard, D.; Nußbaum, E.; Ohnaka, K.; Pacheco, J. A. de Freitas; Perrier, C.; Rabbia, Yves; Rebattu, S.; Reynaud, François; Richichi, A.; Robini, A.; Sacchettini, M.; Schöller, M.; Solscheid, W.; Spang, A.; Stee, Philippe; Stefanini, P.; Tallon, Michel; Tallon–Bosc, I.; Tasso, D.; Testi, L.; Vakili, F.; Lühe, O. von der; Valtier, J. C.; Vannier, M.; Ventura, N.; Weis, Karsten; Wittkowski, M.

doi:10.1051/0004-6361:20065577

Cited by 87 publications

(76 citation statements)

References 42 publications

(98 reference statements)

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“…Furthermore, only 20% of the frames with the highest signal-to-noise ratio were taken into account to avoid degrading the fringe signal. This percentage is slightly more constraining than the value used in different previous studies using AMBER (e.g., Weigelt et al 2007). …”

Section: Observations With Ambermentioning

confidence: 82%

Multiwavelength interferometric observations and modeling of circumstellar disks

Schegerer

Ratzka

Schuller

et al. 2013

A&A

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Aims. We investigate the structure of the innermost region of three circumstellar disks around pre-main sequence stars HD 142666, AS 205 N, and AS 205 S. We determine the inner radii of the dust disks and, in particular, search for transition objects where dust has been depleted and inner disk gaps have formed at radii of a few tenths of AU up to several AU. Methods. We performed interferometric observations with IOTA, AMBER, and MIDI in the infrared wavelength ranges 1.6−2.5 μm and 8−13 μm with projected baseline lengths between 25 m and 102 m. The data analysis was based on radiative transfer simulations in 3D models of young stellar objects (YSOs) to reproduce the spectral energy distribution and the interferometric visibilities simultaneously. Accretion effects and disk gaps could be considered in the modeling approach. Results from previous studies restricted the parameter space. Results. The objects of this study were spatially resolved in the infrared wavelength range using the interferometers. Based on these observations, a disk gap could be found for the source HD 142666 that classifies it as transition object. There is a disk hole up to a radius of R in = 0.30 AU and a (dust-free) ring between 0.35 AU and 0.80 AU in the disk of HD 142666. The classification of AS 205 as a system of classical T Tauri stars could be confirmed using the canonical model approach, i.e., there are no hints of disk gaps in our observations.

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Section: Observations With Ambermentioning

confidence: 82%

Multiwavelength interferometric observations and modeling of circumstellar disks

Schegerer

Ratzka

Schuller

et al. 2013

A&A

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“…The wavelength calibration was performed using telluric lines. We used the same method as described in Appendix A of Weigelt et al (2007).…”

Section: Observations and Data Processingmentioning

confidence: 99%

“…The calibrated continuum visibilities were fit with a twodimensional exponential function in Fourier space, because the measured visibilities and the Fourier transform of the Hillier continuum model curves are approximately exponential functions (van Boekel et al 2003;Kervella 2007;Weigelt et al 2007). From this visibility, we derived an axis ratio of 1.07 ± 0.14 and a PA of the major axis of 159.5 ± 47 • .…”

Section: Observations and Data Processingmentioning

confidence: 99%

“…The inclination of the polar axis of the Homunculus nebula with the line-of-sight is ∼41 • Smith 2006), and the position angle (PA) of the projected Homunculus axis is ∼132 • (Davidson & Humphreys 1997;Davidson et al 2001;Smith 2006). Using ESO's Very Large Telescope Interferometer (VLTI), the diameter of η Car's wind region was measured to be about 5 mas (50% encircled-intensity diameter measured in the fieldof-view, FOV, of 70 mas) in the K-band continuum (van Boekel et al 2003;Kervella 2007;Weigelt et al 2007). The measured visibilities are in good agreement with the predictions from the detailed spectroscopic model by Hillier & Miller (1998) and Hillier et al (2001Hillier et al ( , 2006.…”

Section: Introductionmentioning

confidence: 99%

“…Studies of the binary or binary wind-wind collision zone were reported by many authors (e.g., Damineli 1996;Damineli et al 1997Damineli et al , 1998Damineli et al , 2000Damineli et al , 2008bDavidson 1997;Davidson et al 2005Davidson et al , 2015Smith & Gehrz 2000;Smith et al 2004;Smith 2010;Pittard & Corcoran 2002;Corcoran et al 1997Corcoran et al , 2001Corcoran 2005;Ishibashi et al 1999;Soker 2003Soker , 2007Weis et al 2005;Gull et al 2006Gull et al , 2009Gull et al , 2011Gull et al , 2016Nielsen et al 2007;Weigelt et al 2007; Kashi & Soker 2007, 2009aParkin et al 2009;Groh et al 2010Groh et al , 2012bMadura & Owocki 2010;Madura et al 2012Madura et al , 2013Mehner et al 2010aMehner et al , 2011Mehner et al , 2012Mehner et al , 2015Richardson et al 2010;Teodoro et al 2013Teodoro et al , 2016Clementel et al 2015a,b;Hamaguchi et al 2016). The X-ray...…”

Section: Introductionmentioning

confidence: 99%

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VLTI-AMBER velocity-resolved aperture-synthesis imaging ofηCarinae with a spectral resolution of 12 000

Weigelt

Hofmann

Schertl

et al. 2016

A&A

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Context. The mass loss from massive stars is not understood well. η Carinae is a unique object for studying the massive stellar wind during the luminous blue variable phase. It is also an eccentric binary with a period of 5.54 yr. The nature of both stars is uncertain, although we know from X-ray studies that there is a wind-wind collision whose properties change with orbital phase. Aims. We want to investigate the structure and kinematics of η Car's primary star wind and wind-wind collision zone with a high spatial resolution of ∼6 mas (∼14 au) and high spectral resolution of R = 12 000. Methods. Observations of η Car were carried out with the ESO Very Large Telescope Interferometer (VLTI) and the AMBER instrument between approximately five and seven months before the August 2014 periastron passage. Velocity-resolved aperture-synthesis images were reconstructed from the spectrally dispersed interferograms. Interferometric studies can provide information on the binary orbit, the primary wind, and the wind collision.Results. We present velocity-resolved aperture-synthesis images reconstructed in more than 100 different spectral channels distributed across the Brγ 2.166 µm emission line. The intensity distribution of the images strongly depends on wavelength. At wavelengths corresponding to radial velocities of approximately −140 to −376 km s −1 measured relative to line center, the intensity distribution has a fan-shaped structure. At the velocity of −277 km s −1 , the position angle of the symmetry axis of the fan is ∼126 • . The fan-shaped structure extends approximately 8.0 mas (∼18.8 au) to the southeast and 5.8 mas (∼13.6 au) to the northwest, measured along the symmetry axis at the 16% intensity contour. The shape of the intensity distributions suggests that the obtained images are the first direct images of the innermost wind-wind collision zone. Therefore, the observations provide velocity-dependent image structures that can be used to test three-dimensional hydrodynamical, radiative transfer models of the massive interacting winds of η Car.

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Combining optical spectroscopy and interferometry

Kraus

2014

Astron Nachr

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Modern optical spectrographs and optical interferometers push the limits in the spectral and spatial regime, providing important new tools for the exploration of the universe. In this contribution I outline the complementary nature of spectroscopic & interferometric observations and discuss different strategies for combining such data. Most remarkable, the latest generation of "spectro-interferometric" instruments combine the milliarcsecond angular resolution achievable with interferometry with spectral capabilities, enabling direct constraints on the distribution, density, kinematics, and ionization structure of the gas component in protoplanetary disks. I will present some selected studies from the field of star- & planet formation and hot star research in order to illustrate these fundamentally new observational opportunities.Comment: Proceedings article for the "10th Potsdam Thinkshop". Accepted for publication in Astronomische Nachrichte

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Near-infrared interferometry of η Carinae with spectral resolutions of 1 500 and 12 000 using AMBER/VLTI

Cited by 87 publications

References 42 publications

Multiwavelength interferometric observations and modeling of circumstellar disks

Multiwavelength interferometric observations and modeling of circumstellar disks

VLTI-AMBER velocity-resolved aperture-synthesis imaging ofηCarinae with a spectral resolution of 12 000

Combining optical spectroscopy and interferometry

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