Interferometric data reduction with AMBER/VLTI.  Principle,
 estimators, and illustration

Tatulli, E.; Millour, F.; Chelli, A.; Duvert, G.; Acke, B.; Utrera, O. Hernández; Hofmann, Karl H.; Kraus, Stefan; Malbet, Fabien; Mège, P.; Petrov, R.; Vannier, M.; Zins, G.; Antonelli, P.; Beckmann, U.; Bresson, Y.; Dugué, M.; Gennari, S.; Glück, L.; Kern, P.; Lagarde, S.; Coarer, E. Le; Lisi, F.; Perraut, K.; Puget, P.; Rantakyrö, F.; Robbe-Dubois, S.; Roussel, Alain; Weigelt, G.; Accardo, M.; 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.; Souza, A. Domiciano de; Driebe, T.; 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.; 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.; 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.; Schertl, D.; 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.; Ventura, N.

doi:10.1051/0004-6361:20064799

Cited by 216 publications

(178 citation statements)

References 28 publications

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“…The absolute differential visibility is estimated, as in the power spectrum method, by calibrating the high frequency energy with the low frequency energy of W 12 ( f ). This method has been extensively described in Berio et al (1999) and Tatulli et al (2007). One advantage of this method is to correctly permit measurements at the spectral resolution of VEGA.…”

Section: Cross-spectrum Methodsmentioning

confidence: 99%

VEGA: Visible spEctroGraph and polArimeter for the CHARA array: principle and performance

Mourard

Clausse

Marcotto

et al. 2009

A&A

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140

183

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Context. Among optical stellar interferometers, the CHARA Array located at Mt Wilson in California offers the potential of very long baselines (up to 330 m) and the prospect of coupling multiple beam combiners. This paper presents the principle and the measured performance of VEGA, Visible spEctroGraph and polArimeter installed in September 2007 at the coherent focus of the array. Aims. With 0.3 ms of arc of spatial resolution and up to 30 000 of spectral resolution, VEGA intends to measure fundamental parameters of stars, to study stellar activities and to image and analyze circumstellar environments. We describe the observing modes that have been implemented for this spectro-polarimeter and show actual performances measured on the sky during the first observing runs. Methods. The astrophysical programs are described in relation to the observing modes of the instrument, the presentation of the spectrograph and of the interface table is shown and finally the data is presented. We discuss the perspectives of further development in the framework of the CHARA Array. Results. We show that VEGA/CHARA is fully operational. The current limiting magnitude is nearly 7 but the results depend on the observing conditions (seeing, spectral resolution, etc.). We have validated the stability of the instrumental visibility at the level of 1 to 2% over half an hour and of the instrumental polarization for various declinations. Some examples of squared visibility and differential visibility are presented. Conclusions. The spectro-polarimeter VEGA has been installed and successfully tested on CHARA. It will permit stellar physics studies at unprecedented spectral and spatial resolutions.

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Section: Cross-spectrum Methodsmentioning

confidence: 99%

VEGA: Visible spEctroGraph and polArimeter for the CHARA array: principle and performance

Mourard

Clausse

Marcotto

et al. 2009

A&A

Self Cite

140

183

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“…We recorded H-and K-band interferograms in the low spectral resolution mode (R ∼ 35) with a detector integration time (DIT) of 50 ms. For data reduction, we employed the software library amdlib v3.0.5 1 . We selected 20% of the frames with the highest fringe signal-to-noise ratio (S/N; Tatulli et al 2007) and applied a histogram equalization method for piston correction . The observation log is shown in Table 1.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Resolving the inner disk of UX Orionis

Kreplin

Madlener

Chen

et al. 2016

A&A

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Aims. The cause of the UX Ori variability in some Herbig Ae/Be stars is still a matter of debate. Detailed studies of the circumstellar environment of UX Ori objects (UXORs) are required to test the hypothesis that the observed drop in photometry might be related to obscuration events. Methods. Using near-and mid-infrared interferometric AMBER and MIDI observations, we resolved the inner circumstellar disk region around UX Ori. Results. We fitted the K-, H-, and N-band visibilities and the spectral energy distribution (SED) of UX Ori with geometric and parametric disk models. The best-fit K-band geometric model consists of an inclined ring and a halo component. We obtained a ring-fit radius of 0.45 ± 0.07 AU (at a distance of 460 pc), an inclination of 55.6 ± 2.4 • , a position angle of the system axis of 127.5 ± 24.5 • , and a flux contribution of the over-resolved halo component to the total near-infrared excess of 16.8 ± 4.1%. The best-fit N-band model consists of an elongated Gaussian with a HWHM ∼ 5 AU of the semi-major axis and an axis ration of a/b ∼ 3.4 (corresponding to an inclination of ∼72 • ). With a parametric disk model, we fitted all near-and mid-infrared visibilities and the SED simultaneously. The model disk starts at an inner radius of 0.46 ± 0.06 AU with an inner rim temperature of 1498 ± 70 K. The disk is seen under an nearly edge-on inclination of 70 ± 5 • . This supports any theories that require high-inclination angles to explain obscuration events in the line of sight to the observer, for example, in UX Ori objects where orbiting dust clouds in the disk or disk atmosphere can obscure the central star.

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“…The data reduction was done using the amdlib-2.2 package, which employs the P2VM algorithm (Tatulli et al 2007). In a first step, the instrumental calibration matrix with the standard calibration files provided by ESO was computed.…”

Section: Interferometrymentioning

confidence: 99%

“…This ratio provides the most stable transfer function, see discussion in Tatulli et al (2007) and Millour et al (2007). -The transfer function was estimated by averaging all observations of the calibration stars.…”

Section: Interferometrymentioning

confidence: 99%

Cyclic variability of the circumstellar disk of the Be starζ Tauri

Štefl¹,

Rivinius²,

Carciofi

et al. 2009

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Context. Emission lines formed in decretion disks of Be stars often undergo long-term cyclic variations, especially in the violet-to-red (V/R) ratio of their primary components. The underlying structural and dynamical variations of the disks are only partly understood. From observations of the bright Be-shell star ζ Tau, the possibly broadest and longest data set illustrating the prototype of this behaviour was compiled from our own and archival observations. It comprises optical and infrared spectra, broad-band polarimetry, and interferometric observations. Aims. The dense, long-time monitoring permits a better separation of repetitive and ephemeral variations. The broad wavelength coverage includes lines formed under different physical conditions, i.e. different locations in the disk, so that the dynamics can be probed throughout much of the disk. Polarimetry and interferometry constrain the spatial structure. All together, the objective is a better understand the dynamics and life cycle of decretion disks. Methods. Standard methods of data acquisition, reduction, and analysis were applied. Results. From 3 V/R cycles between 1997 and 2008, a mean cycle length in Hα of 1400-1430 days was derived. After each minimum in V/R, the shell absorption weakens and splits into two components, leading to 3 emission peaks. This phase may make the strongest contribution to the variability in cycle length. There is no obvious connection between the V/R cycle and the 133-day orbital period of the not otherwise detected companion. V/R curves of different lines are shifted in phase. Lines formed on average closer to the central star are ahead of the others. The shell absorption lines fall into 2 categories differing in line width, ionization/excitation potential, and variability of the equivalent width. They seem to form in separate regions of the disk, probably crossing the line of sight at different times. The interferometry has resolved the continuum and the line emission in Brγ and HeI 2.06. The phasing of the Brγ emission shows that the photocenter of the line-emitting region lies within the plane of the disk but is offset from the continuum source. The plane of the disk is constant throughout the observed V/R cycles. The observations lay the foundation for the fully self-consistent, one-armed, disk-oscillation model developed in Paper II.

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Interferometric data reduction with AMBER/VLTI. Principle, estimators, and illustration

Cited by 216 publications

References 28 publications

VEGA: Visible spEctroGraph and polArimeter for the CHARA array: principle and performance

VEGA: Visible spEctroGraph and polArimeter for the CHARA array: principle and performance

Resolving the inner disk of UX Orionis

Cyclic variability of the circumstellar disk of the Be starζ Tauri

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