A5018008347- Adaptive optics and wavefront sensing
- Stellar, planetary, and galactic studies
- Galaxies: Formation, Evolution, Phenomena
- Astrophysics and Star Formation Studies
- Advanced optical system design
- Astronomy and Astrophysical Research
- Optical Systems and Laser Technology
- CCD and CMOS Imaging Sensors
- Astrophysics and Cosmic Phenomena
- Advanced Vision and Imaging
- Optical measurement and interference techniques
- Astrophysical Phenomena and Observations
- Radio Astronomy Observations and Technology
- Atomic and Subatomic Physics Research
- Image Processing Techniques and Applications
- Historical Geography and Cartography
- Geophysics and Sensor Technology
- Maritime Navigation and Safety
- Astronomical Observations and Instrumentation
- Calibration and Measurement Techniques
- Magnetic Field Sensors Techniques
University of Turin
2023-2024
Osservatorio Astrofisico di Torino
2023-2024
Universidad de La Laguna
2011-2022
Instituto de Astrofísica de Canarias
2016-2017
We analyse Near-Infrared Integral Field Spectrograph (NIFS) observations of the type-2 quasar (QSO2) SDSS J094521.33+173753.2 to investigate its warm molecular and ionized gas kinematics. This QSO2 has a bolometric luminosity 10 45.7 erg s −1 redshift z = 0.128. The K -band spectra provided by NIFS cover range 1.99–2.40 μm where low ionization (Pa α Br δ ), high ([S XI] λ 1.920 [Si VI] 1.963 μm), lines (from H 2 1-0S(5) 1-0S(1)) are detected, allowing us study multi-phase Our analysis...
We report high spatial resolution i' band imaging of the multiple T Tauri system LkHα 262/LkHα 263 obtained during first commissioning period Adaptive Optics Lucky Imager (AOLI) at 4.2-m William Herschel Telescope, using its Imaging mode. AOLI images have provided photometry for each two components A and B (0.41 arcsec separation) marginal evidence an unresolved binary or a disc in 262. The data combined with previously available newly optical infrared show that three are comoving, there is...
AOLI (Adaptive Optics Lucky Imager) is a state-of-art instrument that combines adaptive optics (AO) and lucky imaging (LI) with the objective of obtaining diffraction limited images in visible wavelength at mid- big-size ground-based telescopes. The key innovation development use new TP3-WFS (Two Pupil Plane Positions Wavefront Sensor). TP3-WFS, working band, represents an advance over classical wavefront sensors such as Shack-Hartmann WFS (SH-WFS) because it can theoretically fainter...
Plenoptic cameras have been developed the last years as a passive method for 3d scanning, allowing focal stack capture from single shot. But data recorded by this kind of sensors can also be used to extract wavefront phases associated atmospheric turbulence in an astronomical observation. The terrestrial atmosphere degrades telescope images due diffraction index changes turbulence. Na artificial Laser Guide Stars (Na-LGS, 90km high) must obtain reference phase and Optical Transfer Function...
Plenoptic cameras have been developed over the last years as a passive method for 3d scanning. Several superresolution algorithms proposed in order to increase resolution decrease associated with lightfield acquisition microlenses array. A number of multiview stereo also applied extract depth information from plenoptic frames. Real time systems implemented using specialized hardware Graphical Processing Units (GPUs) and Field Programmable Gates Arrays (FPGAs). In this paper, we will present...
Since the beginning of development Gran Telescopio Canarias (GTC), an Adaptive Optics (AO) system was considered necessary to exploit full diffraction-limited potential telescope. The GTC AO designed during last years is based on a single deformable mirror conjugated telescope pupil, and Shack-Hartmann wavefront sensor with 20 x subapertures, using OCAM2 camera. GTCAO will provide corrected beam Strehl Ratio (SR) 0.65 in K-band bright natural guide stars. Most subsystems have been...
The CAFADIS camera project has consisted in building a to measure wave-front phases and distances under different scenarios (from microns kilometres), using highly specialised electronic technology, namely Graphics Processing Units (GPUs) Field Programmable Gate Arrays (FPGAs). It is passive method of depth extraction, it uses incoherent light (natural light). In this paper we will present our new developments.
In this paper we present the Adaptive Optics Lucky Imager (AOLI), a state-of-the-art instrument which makes use of two well proved techniques for extremely high spatial resolution with ground-based telescopes: Imaging (LI) and (AO). AOLI comprises an AO system, including low order non-linear curvature wavefront sensor together 241 actuators deformable mirror, science array four 1024x1024 EMCCDs, allowing 120x120 down to 36x36 arcseconds field view, calibration subsystem powerful LI software....
The study of ionized gas kinematics in high- z active galaxies plays a key part our understanding galactic evolution, an age where nuclear activity was widespread and star formation close to its peak. We present TXS 0952−217, radio galaxy at = 2.95, using VLT/MUSE integral field optical spectroscopy as project aimed studying the properties high redshift (HzRGs). Ly α line profile this object presents various emission absorption components. By utilizing Voronoi binning, we obtained...
The study of ionized gas kinematics in high-z active galaxies plays a key part our understanding galactic evolution, an age where nuclear activity was widespread and star formation close to its peak. We present TXS 0952-217, radio galaxy at z=2.95, using VLT/MUSE integral field optical spectroscopy as project aimed studying the properties high redshift (HzRGs). Lyman $\alpha$ line profile this object presents various emission absorption components. By utilizing Voronoi binning, we obtained...
This paper presents a method to recover the wavefront phase at telescope pupil, distorted because of atmosphere action, and its use command deformable mirror compensate for optical aberrations in real time (AOLI instrument). For this purpose, an evolution geometric sensor [1] was used restore from two defocused images. Furthermore, by using specialized hardware computations can be performed time, within stability atmosphere.
Abstract Spatially resolved observations of active galactic nuclei (AGN) host galaxies undergoing feedback processes are one the most relevant avenues through which evolution can be studied, given long-lasting effects AGN has on gas reservoirs, star formation, and environments at all scales. Within this context, we report results from Very Large Telescope/MUSE integral field optical spectroscopy TN J1049-1258, powerful radio sources known, a redshift 3.7. We detected extended (∼18 kpc) Ly α...
Spatially resolved observations of AGN host galaxies undergoing feedback processes are one the most relevant avenues through which galactic evolution can be studied, given long lasting effects has on gas reservoirs, star formation, and environments at all scales. Within this context we report results from VLT/MUSE integral field optical spectroscopy TN J1049-1258, powerful radio sources known, a redshift 3.7. We detected extended ($\sim$ 18 kpc) Lyman $\alpha$ emission, spatially aligned...