SINFONI data reduction software

Abuter, R.; Schreiber, J.; Eisenhauer, F.; Ott, T.; Horrobin, M.; Gillessen, S.

doi:10.1016/j.newar.2006.02.008

Cited by 101 publications

(90 citation statements)

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“…We reduced our dataset homogeneously with the ESO data reduction pipeline version 1.9.8 (Abuter et al 2006). We used in addition custom scripts to suppress several electronic effects (odd even effect affecting slitlet N • 25, negative rows) affecting our raw images.…”

Section: Data Reductionmentioning

confidence: 99%

A library of near-infrared integral field spectra of young M–L dwarfs

Bonnefoy

Chauvin

Lagrange

et al. 2014

A&A

147

204

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Context. At young ages, low surface gravity affects the atmospheric properties of ultracool dwarfs. The impact on medium-resolution near-infrared (NIR) spectra has only been slightly investigated at the M-L transition so far. Aims. We present a library of NIR (1.1-2.45 µm) medium-resolution (R ∼ 1500-2000) integral field spectra of 15 young M6−L0 dwarfs. We aim at deriving updated NIR spectral type, luminosity, and physical parameters (T eff , log g, M, L/L ) for each source. This work also aims at testing the latest generation of BT-SETTL atmospheric models. Methods. We estimated spectral types using spectral indices and the spectra of young objects classified in the optical. We used the 2010 and 2012 releases of the BT-SETTL synthetic spectral grid and cross-checked the results with the DRIFT-PHOENIX models to derive the atmospheric properties of the sources. Results. We do not find significant differences between the spectra of young companions and those of young isolated brown dwarfs in the same spectral type range. We derive infrared spectral types L0 ± 1, L0 ± 1, M9.5 ± 0.5, M9.5 ± 0.5, M9.25 ± 0.25, M8 +0.5 −0.75 , and M8.5 ± 0.5 for AB Pic b, Cha J110913-773444, USco CTIO 108B, GSC 08047-00232 B, DH Tau B, CT Cha b, and HR7329B, respectively. The BT-SETTL and DRIFT-PHOENIX models yield close T eff and log g estimates for each source. The models seem to show a 600 +600 −300 K drop in the effective temperature at the M-L transition. Assuming the former temperatures are correct, we then derive new mass estimates that confirm that DH Tau B, USco CTIO 108B, AB Pic b, KPNO Tau 4, OTS 44, and Cha1109 lie inside or at the boundary of the planetary mass range. We combine the empirical luminosities of the M9.5-L0 sources to the T eff to derive semi-empirical radii estimates that do not match "hot-start" evolutionary models predictions at 1-3 Myr. We use complementary data to demonstrate that atmospheric models are able to reproduce the combined optical and infrared spectral energy distribution, together with the NIR spectra of these sources simultaneously. But the models still fail to represent the dominant features in the optical. This issue raises doubts on the ability of these models to predict effective temperatures from NIR spectra alone. Conclusions. The library provides templates for characterizing other young and late type objects. The study advocates the use of photometric and spectroscopic information over a broad range of wavelengths to study the properties of very low-mass young companions to be detected with the planet imagers (Subaru/SCExAO, LBT/LMIRCam, Gemini/GPI, VLT/SPHERE).

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Section: Data Reductionmentioning

confidence: 99%

A library of near-infrared integral field spectra of young M–L dwarfs

Bonnefoy

Chauvin

Lagrange

et al. 2014

A&A

147

204

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“…We used the SINFONI data reduction pipeline version 2.0.5 offered by ESO (Jung et al 2006) with reduction routines developed by the SINFONI consortium (Abuter et al 2006). After standard reduction, including dark subtraction, flat fielding, distortion correction, and wavelength calibration, all nodding cycles were combined to a final data cube.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

First spectroscopic observations of the substellar companion of the young debris disk star PZ Telescopii

Schmidt

Mugrauer

Neuhäuser

et al. 2014

A&A

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Context. In 2010 a substellar companion to the solar analog pre-main sequence star PZ Tel and member of the approximately 12 Myr old β Pic moving group was found by high-contrast direct imaging independently by two teams. Aims. In order to determine the basic parameters of this companion more precisely and independent of evolutionary models, hence age-independent, we obtained follow-up spectroscopic observations of the primary and companion. Methods. We used the Spectrograph for INtegral Field Observations in the Near Infrared (SINFONI) at the Very Large Telescope Unit 4/Yepun of ESO's Paranal Observatory in the H + K band and processed the data using the spectral deconvolution technique. The resulting spectrum of the companion was then compared to a grid of Drift-Phoenix synthetic model spectra, a combination of a general-purpose model atmosphere code with a non-equilibrium, stationary cloud and dust model, using a χ 2 minimization analysis. Results. We find a best fitting spectral type of G6.5 for PZ Tel A. The extracted spectrum of the substellar companion, at a spatial position compatible with earlier orbit estimates, yields a temperature T eff = 2500 +138 −115 K, a visual extinction A V = 0.53 +0.84 −0.53 mag, a surface gravity of log g = 3.50 +0.51 −0.30 dex, and a metallicity at the edge of the grid of [M/H] = 0.30 −0.30 dex. Conclusions. We derive a luminosity of log(L bol /L ) = −2.66 +0.06 −0.08 , a radius of R = 2.42 +0.28 −0.34 R Jup , and a mass of M = 7.5 +16.9 −4.3 M Jup for the PZ Tel companion, which is consistent with most earlier estimates using photometry alone. Combining our results with evolutionary models, we find a best-fitting mass of about 21 Jupiter masses at an age corresponding to the recently determined lithium depletion age of 7 +4 −2 Myr. Hence, the PZ Tel companion is most likely a wide brown dwarf companion in the 12 +8 −4 Myr old β Pic moving group.

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“…The data were reduced using the SPRED (version 1.37) software developed by the MPE SINFONI consortium (Schreiber et al 2004;Abuter et al 2006). The procedure described by Davies (2007) was applied to remove the OH line residuals.…”

Section: Vlt-sinfoni Integral Field Spectroscopy Observationsmentioning

confidence: 99%

Different evolutionary stages in the massive star-forming region S255 complex

Wang

Beuther

Bik

et al. 2011

A&A

108

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Aims. Massive stars form in clusters, and they are often found in different evolutionary stages located close to each other. To understand evolutionary and environmental effects during the formation of high-mass stars, we observed three regions of massive star formation at different evolutionary stages, and all are found that in the same natal molecular cloud. Methods. The three regions, S255IR, S255N, and S255S, were observed at 1.3 mm with the submillimeter array (SMA), and followup short spacing information was obtained with the IRAM 30 m telescope. Near infrared (NIR) H + K-band spectra and continuum observations were taken for S255IR with VLT-SINFONI to study the different stellar populations in this region.Results. This combination of millimeter (mm) and near infrared data allow us to characterize different stellar populations within the young forming cluster in detail. While we find multiple mm continuum sources toward all regions, their outflow, disk, and chemical properties vary considerably. The most evolved source S255IR exhibits a collimated bipolar outflow visible in CO and H 2 emission, and the outflows from the youngest region S255S are still small and fairly confined in the regions of the mm continuum peaks. Also the chemistry toward S255IR is the most evolved, exhibiting strong emission from complex molecules, while much fewer molecular lines are detected in S255N, and in S255S we detect only CO isotopologues and SO lines. Also, rotational structures are found toward S255N and S255IR. Furthermore, a comparison of the NIR SINFONI and mm data from S255IR clearly reveal two different (proto) stellar populations with an estimated age difference of approximately 1 Myr. Conclusions. A multiwavelength spectroscopy and mapping study reveals different evolutionary phases of the star formation regions. We propose the triggered outside-in collapse star formation scenario for the bigger picture and the fragmentation scenario for S255IR.

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SINFONI data reduction software

Cited by 101 publications

References 0 publications

A library of near-infrared integral field spectra of young M–L dwarfs

A library of near-infrared integral field spectra of young M–L dwarfs

First spectroscopic observations of the substellar companion of the young debris disk star PZ Telescopii

Different evolutionary stages in the massive star-forming region S255 complex

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