A. Chalabaev

Outflows, Disks, and Stellar Content in a Region of High-Mass Star Formation: G5.89?0.39 with Adaptive Optics

We present adaptive optics (AO)-assisted near-infrared Fabry-Perot observations of both the H2 v=1-0 S(1) line in the area surrounding the shell-like ultracompact H II region (UCH II) G5.89-0.39 and the Brγ emission in the region of ionized gas. This work aims at investigating the near-IR counterpart to the widely debated massive outflow detected toward this source. We also study the connection of the outflow(s) with the possible driving source(s) to better constrain the stellar content within this UCH II region. Our data show evidence of a total of three outflows in this region, with distinct orientations and different driving sources. Two prominent bow-shock structures are identified in our H2 data in a north-south orientation. The molecular jet, likely associated with these features, is not compatible with the orientation of the outflow previously detected at high spatial resolution in SiO emission. Moreover, we propose the driving source of this jetlike structure as the O5 V star recently detected by Feldt and coworkers. However, we report the detection of a bipolar structure, separated by a dark lane, at the location of the 1.3 mm continuum source (i.e., the candidate source to power the SiO outflow). Finally, a third bipolar outflow is traced through the Brγ emission. The confirmation through CO interferometric observations of this outflow activity would therefore favor an accretion scenario for high-mass star formation. Based on observations made with ESO Telescopes at La Silla and Paranal under programs ID:64.I-0532 and ID:73.C-0178. Based on observations collected at the Centro Astronomico Hispano Aleman (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut fur Astronomie and the Instituto de Astrofisica de Andalucia (CSIC).

GriF: The New Three‐dimensional Spectroscopic Mode of PUEO, the Canada‐France‐Hawaii Telescope Adaptive Optics Bonnette: First Observations in the Fabry‐Pérot Scanning Mode

ABSTRACT Three‐dimensional spectroscopy has the advantage of providing (quasi‐) simultaneously both spatial and spectral information. Coupled to adaptive optics, it conjugates spectroscopic power with high angular resolution. GriF offers these capabilities in the near‐infrared. As a new observing mode of KIR, the camera behind PUEO, the Canada‐France‐Hawaii Telescope adaptive optics bonnette, it provides images at the diffraction limit of the telescope in the K band. Spectroscopy at a resolution of 2000 is provided by a Fabry‐Perot interferometer coupled with a grism, cooled to limit the background. This setup offers a large multiplex gain by observing simultaneously up to five monochromatic images. This article first describes the instrument and the calibration procedures. Next, we demonstrate GriF performances from its first observations, obtained on the Orion molecular cloud OMC‐1.

The EPICS project for the European Extremely Large Telescope: outcome of the Planet Finder concept study for OWL

The Exo-Planets Imaging Camera and Spectrograph (EPICS), is the Planet Finder Instrument concept for the European Extremely Large Telescope (ELT). The study made in the frame of the OWL 100-m telescope concept is being up-dated in direct relation with the re-baselining activities of the European Extremely Large Telescope.

The EPICS project: Exoplanets detection with OWL

This paper presents the status of the EPICS project, an Earth-like Planets Imaging Camera Spectrograph for OWL. We present the Top-Level-Requirements of the instrument and we describe the baseline of the Adaptive Optics system with optimized wave-front sensor. The expected performance in rejection of starlight in the near infrared and in the visible is given. The instruments concepts for detection and characterization of exo-planets will be briefly described. The Signal-to-Noise ratio estimation shows that Earth-like planets can be detected up to 20 pc in a reasonable amount of time. The extremely challenging requirements in terms of static residual errors and differential aberrations are discussed.

The GraF instrument for Imaging Spectroscopy with the Adaptive Optics

The GraF instrument using a Fabry-Perot interferometer cross-dispersed with a grating was one of the first integral-field and long-slit spectrographs built for and used with an adaptive optics system. We describe its concept, design, optimal observational procedures and the measured performances. The instrument was used in 1997–2001 at the ESO3.6 m telescope equipped with ADONIS adaptive optics and SHARPII+camera. The operating spectral range was 1.2–2.5 μm. We used the spectral resolution from 500 to 10 000 combined with the angular resolution of 0.1″–0.2″. The quality of GraF data is illustrated by the integral field spectroscopy of the complex0.9″ × 0.9″ central region of η Car in the1.7 μm spectral range at the limit of spectral and angular resolutions.

GriF: an infrared 3D spectroscopic mode for KIR/PUEO

When combined with Adaptive Optics, integral field spectroscopy, i.e. observation of a sky field simultaneously in a number of spectral passbands, is the most efficient way to perform spectro-imaging at high angular resolution. GriF will provide the CFHT community with such a capability in the near infrared K-band. This extension will be completed by means of two simple optical devices to be installed in the KIR cryostat (the infrared camera of PUEO): a cooled grism in the filter-wheel and a cold aperture on an entrance focal plane wheel. They will be completed by a room-temperature Fabry- Perot (FP) interferometer in front of KIR. The FP selects narrow bandpass images while the grism spatially separates them, giving a 3-D spectroscopic capacity within a compact and light design. At each exposure, several (up to 9) monochromatic images of a rectangular field of about 36 arcseconds X 4 arc-seconds will be simultaneously acquired, allowing a precise subtraction of continuum and background. The cooled grism will guarantee a low background environment, thus a good sensitivity at K. The medium spectral resolution (about 2600) will fit to a number of programs and will represent a considerable improvement on imaging with narrow- band filters. Thus, combining high angular resolution with the spectroscopic diagnosis, GriF will allow the study of a large class of compact objects or structures, especially in the extragalactic domain where its sensitivity should be unique.