First light of SINFONI AO-module at VLT

Bonnet, Henri; Conzelmann, Ralf; Delabre, B.; Donaldson, Robert H.; Fedrigo, Enrico; Hubin, N.; Kissler-Patig, M.; Lizon, Jean-Louis; Paufique, J.; Rossi, Silvio; Stroebele, Stefan; Tordo, Sebastien

doi:10.1117/12.551187

Cited by 47 publications

(30 citation statements)

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“…The results presented in Meshkat et al (2015) find HD 984 B at a separation of 0 19±0 02 (9.0 ± 1.0 au) based on the L¢ observations with NaCo (Lenzen et al 2003;Rousset et al 2003) in 2012 July and the H+K band observations with SINFONI (Eisenhauer et al 2003;Bonnet et al 2004) in 2014 September. These two instruments are both mounted on UT4 on the Very Large Telescope at Cerro Paranal, Chile.…”

Section: Introductionmentioning

confidence: 86%

Integral Field Spectroscopy of the Low-mass Companion HD 984 B with the Gemini Planet Imager

Johnson-Groh

Marois

Rosa

et al. 2017

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We present new observations of the low-mass companion to HD 984 taken with the Gemini Planet Imager (GPI) as a part of the GPI Exoplanet Survey campaign. Images of HD 984 B were obtained in the J (1.12-1.3 μm) and H (1.50-1.80 μm) bands. Combined with archival epochs from 2012 and 2014, we fit the first orbit to the companion to find an 18 au (70-year) orbit with a 68% confidence interval between 14 and 28 au, an eccentricity of 0.18 with a 68% confidence interval between 0.05 and 0.47, and an inclination of 119°with a 68% confidence interval between 114°and 125°. To address the considerable spectral covariance in both spectra, we present a method of splitting the spectra into low and high frequencies to analyze the spectral structure at different spatial frequencies with the proper spectral noise correlation. Using the split spectra, we compare them to known spectral types using field brown dwarf and low-mass star spectra and find a best-fit match of a field gravity M6.5±1.5 spectral type with a corresponding temperature of 2730 180 120 -+ K. Photometry of the companion yields a luminosity of L log bol ( /L 2.88 0.07 = - ) ☉ dex with DUSTY models. Mass estimates, again from DUSTY models, find an age-dependent mass of 34±1 to 95±4M Jup . These results are consistent with previous measurements of the object.

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Section: Introductionmentioning

confidence: 86%

Integral Field Spectroscopy of the Low-mass Companion HD 984 B with the Gemini Planet Imager

Johnson-Groh

Marois

Rosa

et al. 2017

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“…In the framework of the SINS survey (see Förster Schreiber et al 2006;Förster Schreiber et al 2009;Genzel et al 2006Genzel et al , 2008Bouché et al 2007;Shapiro et al 2008), we used the SINFONI NIR integral field spectrograph on the ESO VLT (Eisenhauer et al 2003;Bonnet et al 2004) to measure the dynamics of the warm gas in a substantial sample of over 60 redshift 1.5-3.5 massive star-forming galaxies, as traced by their Hα emission redshifted into the H band (z ∼ 1.5) and K band (z ∼ 2.2), or by [O iii] at z > 2.8.…”

Section: Sample and Observationsmentioning

confidence: 99%

THE SINS SURVEY: MODELING THE DYNAMICS OFz∼ 2 GALAXIES AND THE HIGH-zTULLY-FISHER RELATION

Cresci

Hicks

Genzel

et al. 2009

ApJ

284

543

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We present the modeling of SINFONI integral field dynamics of 18 star-forming galaxies at z ∼ 2 from Hα line emission. The galaxies are selected from the larger sample of the SINS survey, based on the prominence of ordered rotational motions with respect to more complex merger-induced dynamics. The quality of the data allows us to carefully select systems with kinematics dominated by rotation, and to model the gas dynamics across the whole galaxy using suitable exponential disk models. We obtain a good correlation between the dynamical mass and the stellar mass, finding that large gas fractions (M gas ≈ M * ) are required to explain the difference between the two quantities. We use the derived stellar mass and maximum rotational velocity V max from the modeling to construct for the first time the stellar mass Tully-Fisher relation at z ∼ 2.2. The relation obtained shows a slope similar to what is observed at lower redshift, but we detect an evolution of the zero point. We find that at z ∼ 2.2 there is an offset in log(M * ) for a given rotational velocity of 0.41 ± 0.11 with respect to the local universe. This result is consistent with the predictions of the latest N-body/hydrodynamical simulations of disk formation and evolution, which invoke gas accretion onto the forming disk in filaments and cooling flows. This scenario is in agreement with other dynamical evidence from SINS, where gas accretion from the halo is required to reproduce the observed properties of a large fraction of the z ∼ 2 galaxies.

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“…SINFONI is composed of an integral field spectrograph SPIFFI fed by the adaptive optics module MACAO (Eisenhauer et al 2003;Bonnet et al 2004). The instrument was operated with the J-band grating yielding a spectral resolution of ∼2000 over the 1.1-1.35 μm range.…”

Section: Noema 13 MM Continuum Imagingmentioning

confidence: 99%

An Upper Limit on the Mass of the Circumplanetary Disk for DH Tau b^*

Wolff

Ménard

Cáceres

et al. 2017

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DHTau is a young (∼1 Myr) classical TTauri star. It is one of the few young PMS stars known to be associated with a planetary mass companion, DHTaub, orbiting at large separation and detected by direct imaging. DHTaub is thought to be accreting based on copious a H emission and exhibits variable Paschen Beta emission. NOEMA observations at 230 GHz allow us to place constraints on the disk dust mass for both DHTaub and the primary in a regime where the disks will appear optically thin. We estimate a disk dust mass for the primary,, which gives a disktostar mass ratio of 0.014 (assuming the usual gas todust mass ratio of 100 in the disk). We find a conservative disk dust mass upper limit of 0.42 M ⊕ for DHTaub, assuming that the disk temperature is dominated by irradiation from DH Tau b itself. Given the environment of the circumplanetary disk, variable illumination from the primary or the equilibrium temperature of the surrounding cloud would lead to even lower disk mass estimates. AMCFOST radiative transfer model, including heating of the circumplanetary disk by DHTaub and DHTauA, suggests that a mass-averaged disk temperature of 22 K is more realistic, resulting in a dust disk mass upper limit of 0.09 M ⊕ for DHTaub. We place DHTaub in context with similar objects and discuss the consequences for planet formation models.

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First light of SINFONI AO-module at VLT

Cited by 47 publications

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Integral Field Spectroscopy of the Low-mass Companion HD 984 B with the Gemini Planet Imager

Integral Field Spectroscopy of the Low-mass Companion HD 984 B with the Gemini Planet Imager

THE SINS SURVEY: MODELING THE DYNAMICS OFz∼ 2 GALAXIES AND THE HIGH-zTULLY-FISHER RELATION

An Upper Limit on the Mass of the Circumplanetary Disk for DH Tau b^*

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First light of SINFONI AO-module at VLT

Cited by 47 publications

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Integral Field Spectroscopy of the Low-mass Companion HD 984 B with the Gemini Planet Imager

Integral Field Spectroscopy of the Low-mass Companion HD 984 B with the Gemini Planet Imager

THE SINS SURVEY: MODELING THE DYNAMICS OFz∼ 2 GALAXIES AND THE HIGH-zTULLY-FISHER RELATION

An Upper Limit on the Mass of the Circumplanetary Disk for DH Tau b*

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An Upper Limit on the Mass of the Circumplanetary Disk for DH Tau b^*