Found 20 talks width keyword spectrographs

Tuesday November 23, 2021
Dr. Dainis Dravins
Lund Observatory (Sweden)


The new generation of spectrometers designed for extreme precision radial velocities enable correspondingly precise stellar spectroscopy. It is now fruitful to theoretically explore what the information content would be if stellar spectra could be studied with spectral resolutions of a million or more, and to deduce what signatures remain at lower resolutions. Hydrodynamic models of stellar photospheres predict how line profiles shapes, asymmetries, and convective wavelength shifts vary from disk center to limb. Corresponding high-resolution spectroscopy across spatially resolved stellar disks is now practical using differential observations during exoplanet transits, thus enabling the testing of such models. A most demanding task is to understand and to model spectral microvariability toward the radial-velocity detection of also low-mass planets in Earth-like orbits around solar-type stars. Observations of the Sun-as-a-star with extreme precision spectrometers now permit searches for spectral-line modulations on the level of a part in a thousand or less, feasible to test against hydrodynamic models of various solar features.

Friday September 17, 2021
Nicolás A. Rodríguez Linares, Pablo Estevez Alonso


Automatización del POTEC

Explicación del problema de automatización del criostato de pruebas para la preóptica de Harmoni. Integración de diferentes protocolos de comunicación mediante el uso de lenguajes de alto nivel y un manejo de los errores que posibilite su integración dentro de un proceso industrial robusto acelerando el tiempo de prototipado y testeo. Uso de Python para la adquisición de datos y la supervisión del proceso en tiempo de ejecución.


Desarrollo de un sistema de medida optoelectrónico para la caracterización  de fotodetectores basado en un monocromador

Creación de una aplicación Python para el control de un sistema óptico y la toma de datos de dos picoamperímetros conectados a sendos fotodiodos que miden la intensidad de la radiación emitida. Esto nos servirá para la caracterización del fotodetectores


Tema: Seminario de Instrumentación: Presentaciones Becarios de Verano

Hora: 17 sept. 2021 12:00 p. m. Atlantic/Canary


Unirse a la reunión Zoom



Tuesday July 20, 2021
Dr. Sergey Yurchenko
University College of London


The ExoMol project ( provides comprehensive spectroscopic data (line lists) for the study of atmospheres of exoplanets and other hot bodies.  These line lists serve as input for models of radiative transport through hot atmospheres and are useful for a variety of terrestrial applications. The basic form of the database is extensive line lists; these are supplemented with partition functions, state lifetimes, cooling functions, Landé g-factors, temperature-dependent cross sections, opacities, k-coefficients and pressure broadening parameters. Currently containing 80 molecules and 190 isotopologues totaling over 700 billion transitions, the database covers infrared, visible and UV wavelengths. The field of the HR spectroscopy of exoplanets is growing extremely fast and urgently demands molecular data of high precision. Failure to detect molecules in atmospheres of exoplanets is often attributed to the lack of the underlying quality of
the line positions.  These developments have led us to begin a systematic attempt to improve the accuracy of the line positions for the line lists contained in the database. Our new ExoMolHD project aims to provide comprehensive line lists to facilitate their use in characterization of exoplanets using high resolution Doppler shift spectroscopy. Progress on this objective will be presented.

Tuesday June 8, 2021
Dr. Hector Socas-Navarro


In this talk I'll present results from a recent paper in which we have developed a new analysis technique for solar spectra based on artificial neural networks. Our first test applications yielded some unexpected and interesting results. The fine-scale network of temperature enhancements in the quiet middle and upper photosphere have a reversed pattern. Hot pixels in the middle photosphere, possibly associated with small-scale magnetic elements, appear cool at higher levels (log(tau)=-3 and -4), and vice versa. We also find hot arcs on the limb side of magnetic pores, which we interpret as the first direct observational evidence of the "hot wall" effect. Hot walls are a prediction of theoretical models from the 1970s which had not been observed until now.

Friday June 4, 2021
Manuel Amate Plasencia


En los ultimos años hemos visto el desarrollo de instrumentación para la búsqueda de exoplanetas por el método de la Velocidad Radial.

La tendencia es que cada generación de espectrógrafos ultra-estables sea un orden de magnitud mejor que la anterior. Pero ¿qué tienen en común estos intrumentos?, ¿Qué los distingue del resto?

El IAC participa en instrumentos de tres generacines: HARPS3, ESPRESSO y HIRES; en esta charla, aprovechando la experiencia adquirida, se hablará de las estrategias que han permitido a estos instrumentos tener alta resolución, alta estabilidad y alta repetibilidad.

Friday February 19, 2021
Pablo Alberto Fuerte Rodríguez


Durante este seminario se hará un recorrido sobre la instrumentación dentro del proyecto QUIJOTE, desde de los instrumentos ya existentes y su problemática hasta el estado actual de los instrumentos de nueva generación y los posibles desarrollos a futuro.



Friday February 12, 2021
Prof. Caroline Kulcsár
Université Paris-Saclay


In this talk, I will start by briefly presenting the Institut d'Optique Graduate School and the Laboratoire Charles Fabry, where I conduct my research. Then I will explain the principle of adaptive optics and discuss some issues related to the control of AO systems. This will lead to the general ideas behind high-performance control. In particular, I will explain why high-performance control can outperform the standard integrator. Some results of on-sky experiments will be shown, and I will conclude the talk by presenting our PhD students working through research collaborations.



Friday December 11, 2020
María F. Gómez Reñasco


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.

Thursday February 21, 2019
Dr. Hans Zinnecker
Severo Ochoa senior researcher



Tuesday February 19, 2019
Dr. Hans Zinnecker
Deutsches SOFIA Institut, Univ. of Stuttgart, Germany (retired)



SOFIA, short for Stratospheric Observatory for Infrared Astronomy,
is a 2.7m telescope flying on a Boeing 747SP at altitudes of 12-14km,
to detect and study mid- and far-infrared radiation that is blocked
by water vapor in the earth's atmosphere and cannot reach the
ground. It is the successor to the Kuiper Airborne Observatory (1974-1995)
and currently the only access to and platform for astronomical observations
in the far-infrared (30-300 microns), except for balloon-borne telescopes.
SOFIA normally flies out of California, but once a year also
deploys to the Southern Hemisphere (usually to Christchurch,
New Zealand), benefitting from the excellent wintertime
stratospheric conditions to study the rich southern skies.
Although a bilateral project (80:20)
between USA (NASA/USRA) and Germany (DLR/DSI), it is open for
proposals from the world-wide astronomical community at large.
It addresses many science questions that ESA's successful but
now extinct Herschel Observatory has left unanswered and
offers observational opportunities similar to and beyond Herschel.
SOFIA also has many synergies with ALMA and APEX, as well as IRAM
and other submm and radio telescopes.

In part I of this SOFIA lecture, I will introduce the observatory 
in general, the plane, the telescope, the mode of operation, and 
in particular the current and future instrumentation.

In part II (later this week),  I will present a glimpse of SOFIA science
highlights and discoveries in its first 6 years of operation
(since 2012), including the most recent astrophysical and astrochemical 
results. I will also address its future ISM and star formation potential.  

SOFIA is a unique observatory, different from ground-based and
space platforms, which will serve the mid- and far-infrared 
astronomical community for many years to come.
It is a fascinating experience to fly on SOFIA! 

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