Major ground-based observing inastructures for Astronomy and

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Major ground-based observing in"astructures for Astronomy
and Astrophysics: optical and in"ared wavelengths
María Rosa Zapatero Osorio (CAB, INTA-CSIC)
La Astronomía y los desarrollos tecnológicos, Univ. Politécnica de Cartagena, Julio 2012
Thursday, July 26, 2012
Presentation focuses on the major facilities to which astronomers in Spanish-based
institutions and research centers have (and will have) access.
Paranal Observatory
La Silla Observatory
Calar Alto Observatory
Roque de los Muchachos Observatory
European Extremely Large Telescope
With some exceptions (indicated), all pictures have been taken by the speaker or any of
her collaborators during observing runs through the last 5 years.
Daybreak on Roque de los Muchachos, La Palma
Geographical location
Calar Alto
Roque de los Muchachos
Paranal
La Silla
Excellent sky coverage of northern and southern astronomical objects.
Major ground-based infrastructures: optical and infrared. M. R. Zapatero Osorio
Paranal Observatory: Very Large Telescope (VLT)
ESO
Cerro Paranal (Chile), 2635 m, operated by European Southern Observatory (ESO), inauguration 1996.
Four 8.2-m telescopes (UTs), four 1.8-m auxiliary telescopes (ATs), one 4-m imaging telescope (VISTA)
Paranal Observatory
Atacama Desert is commonly known as the driest place in the world, especially at
about 100 km south of Antofagasta city (Chile). Average rainfall: 1 mm/yr.
Sodium nitrate may be used as a
Atacama soil has been compared to that of Mars.
The desert has rich deposits of copper and the world’s largest
sodium nitrate.
constituent of fertilizers, pyrotechnics
and smoke bombs, glass and pottery
enamels, as a food preservative and
naturala supply
ofpropellant. It has been
solid rocket
mined extensively for these purposes.
Paranal Observatory
UT3
Melipal
(South Cross)
UT1
Antú (Sun)
UT4
Yepún (Venus)
UT2
Kueyén (Moon)
Monolithic mirrors.
Paranal Observatory
Auxiliary Units (ATs) are dedicated to interferometry. The transporter section runs on
tracks, so the ATs can be moved to 30 different observing locations.
Paranal Observatory
Auxiliary Units (ATs) are dedicated to interferometry. The transporter section runs on
tracks, so the ATs can be moved to 30 different observing locations.
ESO
Paranal Observatory: VLT
Each UT provides on Cassegrain and two Nasmyth focus stations for instruments. One Nasmyth focus is
available for visitor instruments. In addition, each UT is equipped with a Coudé focus station from
which the incoming light can be combined in the interferometric focus.
Today there are 11 instruments operating at optical and/or infrared wavelengths for science
observations.
ESO
Paranal Observatory: VLT
Plans for future state-of-the-art instrumentation.
KMOS on UT1: NIR IFU spectrograph (R=1800-4200), star and galaxy
formation at both high and low redshift. Commissioning in November 2012. PI:
Ray Sharples (Durham Univ., UK).
KMOS consortium
MUSE: adaptive optics IFU spectrograph operating at visible wavelength range. PI: R. Bacon (Lyon, France).
Star and galaxy formation, solar system. Expected first light: 2012.
SPHERE: PI J.-L. Beuzit (France). Discovery and study of new extrasolar giant planets orbiting nearby
stars by direct imaging of their circumstellar environment. The challenge consists in the very large
contrast between the host star and the planet, larger than 12.5 magnitudes of 105 in flux ratio) at very
small angular separations. Observing modes: imaging, dual-band imaging, polarimetric imaging, long-slit
spectroscopy.
Paranal Observatory: X-Shooter at VLT
ESO
X-SHOOTER is the first of the second generation
instruments at VLT. It is mounted on the Cassegrain focus of
UT2, and is one of the most demanded instruments in the
astronomical community.
X-SHOOTER provides a large wavelength spectroscopic
coverage (0.3-2.5 µm) in one single shot.
It was built by a Consortium of Institutes in Denmark,
France, Italy and The Netherlands together with ESO.
ESO
Paranal Observatory: ESPRESSO
1.5 m
ESPRESSO consortium
1.51 m
4.1 m
ESPRESSO (Echelle SPectrograph for
Rocky Exoplanets and Stable
Spectroscopic Observations) will
deliver radial velocities with a precision
of 10 cm/s. For this, a laser frequency
comb is envisaged for wavelength
calibration across the visible
wavelengths. The first operational
laser comb was recently tested on the
3.6-m telescope (La Silla) using HARPS.
Paranal Observatory: residence for astronomers and ESO staff
It is built half into the mountain with the concrete colored to blend into the landscape.
Located 200 m below the VLT and at a distance of 3 km.
Paranal Observatory: residence for astronomers and ESO staff
Contrasting with the natural landscape, the interior of the “residencia” contains two
gardens and a swimming pool. They help maintain humidity inside the building.
La Silla, also in Atacama desert (Chile), 2400 m, partly operated by (ESO), inauguration 1969.
Among many telescopes, there are the ESO 3.6 m and NTT.
La Silla, also in Atacama desert (Chile), 2400 m, partly operated by (ESO), inauguration 1969.
Among many telescopes, there are the ESO 3.6 m and NTT.
HARPS, the High Accuracy Radial velocity Planet Searcher, operates on the 3.6 m teles. of La Silla Observatory.
It is a fiber-fed echelle spectrograph that has a long record of planet discoveries (Swiss team).
Geneva Univ.
Geneva Univ.
3.6-m telescope
Sierra de los Filabres (Almería, Spain), 2168 m, operated jointly by the Max-Planck-Institut für
Astronomie (MPIA) in Heidelberg, Germany, and the Instituto de Astrofísica de Andalucía (CSIC) in
Granada/Spain. Three telescopes with apertures of 1.23m, 2.2m and 3.5m. A 1.5 m-telescope is
operated under the control of the Observatory of Madrid. Inaugurated in 1975.
3.5 m Calar Alto
CARMENES (Calar Alto high-Resolution search for M dwarfs with Exoearths with Near-infrared and
optical Échelle Spectrographs), is a next-generation instrument to be built for the 3.5 m telescope by a
consortium of German and Spanish institutions. Two separated spectrographs: 0.5 to 1.0 µm and 1.0 to
1.7 µm, spectral resolutions R = 82,000. The spectrographs will be fed by fibres from the Cassegrain
focus of the telescope, housed in a temperature-stabilised environment in vacuum tanks, calibrated
using simultaneous emission lamps, and optimised for exoearth searches around M dwarfs.
La Palma Island (Spain), 2396 m, operated by European partners, inauguration 1985.
The two largest optical and infrared facilities are the 10.4-m Gran Telescopio de Canarias (GTC) and
the 4.2-m William Herschel Telescope (WHT).
TNG
GTC
New state-of-the-art instrumentation is arriving to these two telescopes.
HARPS-North (planet hunter) is starting operations on the Telescope Nazionale Galileo (TNG).
OSIRIS and Canaricam are available on the GTC.
Roque de los Muchachos Observatory: WHT
Imaging and spectroscopic instrumentation: ACAM, LIRIS, Naomi/Ingrid, ISIS, Autofib2/WYFFOS.
Roque de los Muchachos Observatory: GTC
Inaugurated in 2009.
Partners: Spain, IA-UAM and INAOE of Mexico, and University of Florida (USA).
Sky over GTC (webcam).
http://www.gtc.iac.es/pages/multimedia/webcams-en-el-orm.php#
http://www.gtc.iac.es/pages/multimedia/panoramictour.php
Segmented mirror telescope: 36 hexagonal pieces.
Acquisition and guiding camera
IAC
OSIRIS is an imager and spectrograph for the optical wavelength range, located in the
Nasmyth-B focus of GTC. It covers the wavelength range from 0.365 to 1.05 µm with a
field of view of 7.8 x 7.8 arcmin2 (unvignetted, imaging), and 8 x 5.2 arcmin2
(spectroscopy).
Univ. Florida
CanariCam is a mid-infrared (7.5-25 µm) imager with spectroscopic, coronographic, and
polarimetric capabilities, which is mounted at one of the Nasmyth foci of the GTC. The
cryostat is cooled down to 28 K (-265º C) using a He cryo-cooler system. Temperature
control of the detector ensures that its optimum operating temperature (9 K, -264 K) is
stable in the mK range.
The Infrared Multi-Object Spectrograph (EMIR) is taking shape (construction phase).
This instrument will operate in the wavelength interval 0.9-2.5 µm.
IAC
EMIR cryostat put together for the first time (November 2011)
Minutes before sunrise. Teide volcano (Tenerife island) silhouette is clearly seen.
Picture taken from the Nordic Optical Telescope.
European Extremely Large Telescope (E-ELT)
Since 2005 ESO has been working together with its user community of European
astronomers to define the new giant telescope needed by the middles of the next decade.
Mirror size: 39.3 m, the world’s biggest eye on the sky.
Science goals: high redshift galaxies, star formation, exoplanets and protoplanetary systems.
Current design of the dome. ESO
Primary mirror: >800 segments of 1.4 m wide, but only 50 mm thick.
The optical design calls for an immense secondary mirror 4.2 m in diameter.
It will go to Cerro Armazones (Atacama desert, Chile), 3064 m,
350 cloudless nights a year.
E-ELT two first-light instruments have been identified:
MICADO, a diffraction-limited near-infrared imager, a
HARMONI, a single-field near-infrared wide-band integral
field spectrograph operating at visible and near-infrared
wavelengths.
ESO
Thank you very much!
¡Muchas gracias!

Major ground-based observing inastructures for Astronomy and

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