Found 23 talks width keyword spectrographs

HORUS (High ResolUtion Spectrograph) es un espectrógrafo de alta resolución, instrumento visitante en GTC y disponible para la comunicad científica desde prinicipios de 2019. Instalado en la plataforma Nasmyth B, detrás de OSIRIS, comparte foco con él. En esta charla se describe su software de control, resaltando la implementación realizada para ser un instrumento visitante de GTC y cómo se ha resuelto el problema del apuntado de un objeto.

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We present the discovery of a small 0.2'' (60 pc) radius kinematically decoupled core, as well as an outflow jet, in the archetypical AGN-starburst "composite" galaxy NGC 7130 from integral field data obtained with the adaptive optics-assisted MUSE-NFM instrument on the VLT. Correcting the already good natural seeing at the time of our science verification observations with the four-laser GALACSI AO system we reach an unprecedented spatial resolution of around 0.15''. We confirm the existence of star-forming knots arranged in an 0.58'' (185 pc) radius ring around the nucleus, previously observed from UV and optical  Hubble Space Telescope and CO(6-5) ALMA imaging. We determine the position of the nucleus as the location of a peak in gas velocity dispersion. A plume of material extends towards the NE from the nucleus until at least the edge of our FOV at 2'' (640 pc) radius which we interpret as an outflow jet originating in the AGN. The plume is not visible morphologically, but is clearly characterised in our data by emission lines ratios characteristic of AGN emission, enhanced gas velocity dispersion, and distinct non-circular gas velocities. Its orientation is roughly perpendicular to line of nodes of the rotating host galaxy disk. An 0.2''-radius circumnuclear area of positive and negative velocities indicates a tiny inner disk, which can only be seen after combining the integral field spectroscopic capabilities of MUSE with adaptive optics.

Tigre is a 1.2m f:8 RC robotic telescope designed to do spectroscopic monitoring of dynamical processes, mainly in stellar astrophysics, for objects of less than 2" of size and brighter than magnitude 10...11. Its 2-channel (red/blue) echelle spectrograph HEROS has a resolution of 20,000 and covers simultaneously almost the whole range from the near IR to near UV (8800-3800A). It can also be used to determine the exact physical properties of stellar samples of interest, comparing high s/n (80-120) spectra with PHOENIX models and iSpec analysis. The large amount of spectroscopic data ideally serves a large variety of undergraduate and graduate thesis projects. This presentation gives a brief insight into this dedicated, yet economic international project of the universities of Hamburg, Guanajuato and Liege and the opportunities it has to offer to the international community.

MUSE (Multi Unit Spectroscopic Explorer) is a 2nd generation Integral Field facility for the VLT. With a field of view of 1x1 arcmin, fine sampling, intermediate spectral resolution and large spectral coverage in the visible, it uses a complex image slicer, twenty-four parallel spectrographs and a large detector area. In addition, MUSE is conceived to work assisted by the Adaptive Optics Facility (AOF), which will enhance notably its performance. MUSE is the result of ten years of design and development by the MUSE consortium — headed by the Centre de Recherche Astrophysique de Lyon, France and the partner institutes Leibniz-Institut für Astrophysik Potsdam (AIP, Germany),  Institut für Astrophysik Göttingen (IAG, Germany),  Institute for Astronomy ETH Zurich (Switzerland), L'Institut de Recherche en Astrophysique et Planétologie (IRAP, France), Nederlandse Onderzoekschool voor de Astronomie (NOVA, the Netherlands) and ESO.
MUSE has been successfully installed on ESO’s Very Large Telescope (VLT). In this talk it will be presented the instrument, its design and challenges, the integration (both in Europe and Paranal), the first light and first commissioning results.

CARMENES (Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and optical Échelle Spectrographs) is a next-generation instrument being built for the 3.5m telescope at the Calar Alto Observatory by a consortium of German and Spanish institutions. It consists of two separated spectrographs covering the wavelength ranges from 0.5 to 1.0 mum and from 1.0 to 1.7 mum with spectral resolutions R = 82,000, each of which shall perform high-accuracy radial-velocity measurements (~1 m/s) with long-term stability. The fundamental science objective of CARMENES is to carry out a survey of ~300 late-type main-sequence stars with the goal of detecting low-mass planets in their habitable zones. We aim at being able to detect 2 MEarth planets in the habitable zone of M5V stars. The CARMENES first light is expected to occur in Spring 2014.

The vision for the use of the WHT in the coming decade is taking shape.   A key element is the construction and deployment of WEAVE, a wide-field massive-multiplex spectrograph.  With 1000 fibres and spectral resolutions of 5000 and 20000, the opportunities for discovery are tremendous.  Three key fields will be: Milky-Way and Local Group archaeology linked to the   Gaia mission; cosmology redshift surveys; and galaxy evolution studies linked to photometric surveys such as VISTA, UKIDSS, LOFAR, EUCLID, and  others. IAC has the opportunity to get involved in this important instrument for ORM from the beginning.

The 2nd generation VLT instrument Multi Unit Spectroscopic Explorer(MUSE) is going to be an integral field spectrograph with wide field of view and high spatial sampling. It is currently being built by a European consortium to see first light end of 2012. I will describe instrumental properties, show some details of the optomechanical design, present the data processing, and give some examples for possible scientific use.

VIMOS is visible multi-object spectrometer operating on the VLT.  The high multiplex of the VLT visible imager and multi object/integral-field spectrometer, VIMOS, makes it a powerful instrument for large-scale spectroscopic surveys of faint sources. Following community input and recommendations by ESO's Science and Technology Committee, it was decided to upgrade the instrument in phases. The first phase of the upgrade is described and included changing the shutters, installing an active flexure compensation system, replacing the detectors with CCDs with a far better red sensitivity and less fringing, and improving the data reduction pipeline.