Transcript 1 - astro1.snu.ac.kr

2011-30128 서우영
GRAN TELESCOPIO CANARIAS
Contents
 Introduction
 Observatory & Mirrors
 Instruments : Feature and Scientific goal
 Osiris : Tunable Filter
 Science of GTC
 How To Use
Introduction : Basic info.
 Observatorio del Roque de los Muchachos
(ORM) on the island of La Palma in Canaries.
 10.4m primary mirror.
(formed by 36 hexagonal components)
 Each mirror is 8cm thick, 470kg, and 1.9m.
Introduction : Basic info.
 1.6m focal length
 Mounting is Altitude/Azimuth.
 First science observations on Mar. 16th, 2009
 Produce first Scientific data : July 2010
Introduction : Basic info.
 GTC will be the last of the so called
generation of 8-10 meter telescopes.
 And the Largest (single mirror) telescope.
 Active optics & Adaptive optics.
 Segmented Ritchey–Chrétien telescope
Introduction : The Site
 La Palma, One of Canary islands.
 706km2 / 2423m height.
 The Sky Law : approved on 13th Mar. 1992
(Law for the Protection of the Astronomical Quality)
 Light pollution
 Radioelectrical pollution
 Atmospheric pollution
 Aviation routes
Introduction : The Site
Introduction : The Site
Introduction : The Site
 Second best location for optical and infrared astronomy in the
Northern Hemisphere.














17m MAGIC gamma-ray imaging Cherenkov telescope
10.4m GTC
4.2m WHT (William Herschel Telescope)
3.5m TNG (Telescopio Nazionale Galileo)
2.56m NOT (Nordic Optical Telescope)
2.5m INT (Isaac Newton Telescope)
2.0m LT (Liverpool Telescope)
1.2m Mercator Telecope
1.0m SST (Swedish Solar Telescope)
1.0m JKT (Jacobus KapteynTelescope)
0.45m DOT (Dutch Open Telescope)
0.18m CMT (Carlsberg Meridian Telescope)
SuperWASP (Wide Angle Search for Planets
HEGRA (High-Energy-Gamma-Ray Astronomy)
NOT, WHT, DOT, SST, INT, JKT
Introduction :
Astrophotography
 Three color composition image of M51
 Using the instrument OSIRIS at the GTC
 Exposure time : 120 sec
Introduction :
Astrophotography
 M56, using OSIRIS
Observatory - dome
Observatory - Telescope
Two Nasmyth foci
Four Folded
Casserain foci
Cassegrain focus
Observatory - Telescope
Mirrors
 Primary
 Secondary
 Tertiary
Primary Mirror
 Formed by 36 hexagonal components.
 Each mirror is 8cm thick, 470kg, and 1.9m.
 Maximum D is 11.4m, effective D is 10.4m.
 Coated with Aluminum.
 Margin of error is 15nm.
Primary Mirror
Secondary Mirror
 Quasi-hexagonal shape
 About 1.2m / 55kg
 Made of beryllium
substrate.
 Coated with Nickel.
Tertiary Mirror
 Job to deflect the beam of light to the
4 folded Cassegrain and 2 Nasmyth foci.
Instruments
 Day-One Scientific instruments :
 OSIRIS
 CanariCam
 Post-Day-One instrumentation :
 EMIR
 CIRCE
 FRIDA
 New generation of instruments :
 GO-IRS, MEGARA, MIRADAS, NIRINTS
Instruments : CanariCam
 Mid-infrared (7.5 ~ 25micron) imager with spectroscopic,
coronagraphic, and polarimetric capabilities.
 Nasmyth focus.
 Feb. 2011 : Preparing GTC for CanariCam
Instruments : CanariCam
Spectral range
7.5 ~ 25μm
Field of View
25.6’’ x 19.2’’
Plate Scale
0.08’’, Nyquist sampled at 8 μm
Detector
Raytheon CRC-774 320x240 Si:As IBC
Physical Pixel Size
50 x 50 μm (0.08arcsec)
Image Quality
EER80 < 2pic (0.16’’) in imaging mode
Diffraction limited at λ > 8μm
Observing
Modes
Imaging
Filters: (N,Q) and Narrow Band (18)
Spectroscopy
Slit length : 19.2’’, width : 0.17-1.04’’
R=175, 1313 (8-14 μm); 120, 891 (16-26 μm)
Coronography
10 micron window (8-14 μm)
Polarimetry
10 micron window (8-14 μm)
Instruments : CanariCam
 Scientific goal
 Sub-stellar objects
 Circumstellar disks
 Active galaxies, Ultra High Infrared Luminosity
Galaxies and Starbursts
Instruments : OSIRIS
 Optical System for Imaging and low Resolution





Integrated Spectroscopy
To obtain direct images of the sky
To carry out spectroscopy of a number of different
objects simultaneously.
located in the Nasmyth-B focus
Tunable Filter
OSIRIS covers the wavelength range
from 0.365 to 1.05 µm with a field of view of 7.8 x
8.5 arcmin and 8 x 5.2 arcmin, for direct imaging
and low resolution spectroscopy respectively.
Instruments : OSIRIS
 Available
 Broad band imaging
 Narrow band imaging with the red-optimized TF
 Long-slit spectroscopy
 Remain some uncertainty
 Multi-object spectroscopy mode
 Frame transfer high-speed photometric modes
 blue-optimized TF
Instruments : OSIRIS
Spectral range
3650~10000Å
Field of View
7.8’ x 8.5’
Plate Scale
0.125’’
Detector
2048x4098 Marconi CCD42-82 (x2 with 9.2’’ gap)
Pixel Size
15 μm / pixel
Quantum Efficiency
50%(400nm), 90(600), 80(800), 40 (900)
Image Quality
EER80 < 0.15’’ (Imaging mode).
Distortion < 2% in all the detector.
Instruments : OSIRIS
Instruments : OSIRIS
 Main science programs












Asteroids and Comets
Variable stars
Stellar activity cycles in open cluster stars
Stellar populations in remote parts of the galaxy
Brown dwarfs
White dwarfs in star clusters
HII Regions in Galaxies
Black Hole Hunting
Surveys of galaxies
AGN-Normal galaxies link
AGN Unification Models
AGN components
Instruments : OSIRIS
 Main science programs
 Optical counterparts of radiojets
 Optical counterparts of GRBs
 The Origin of the X-ray Background
 QSOs
 The Environments of QSO at z>1
 Clustering around radio sources
 Evolution of low-redshift galaxies
 Determination of redshifts of faint objects
 Probing Dark Matter
 Microlensing
 OTELO survey (deepest emission line survey to date)
Instruments : EMIR
 Wide field camera and near-infrared multi-object medium





resolution spectrograph.
Nasmyth focus.
Spectral range : 0.9 ~ 2.5 μm
ZJH(R=4000), K(R=3500)
Array format : 2048 x 2048 pixelsLimiting magnitude : J=25.5
H=24.5 K=23.5 (para S/N=5; t=5hours)
Imaging mode



FOV : 6’ x 6’
Plate scale : 0.2’’ / pixel
Filters : Broad band(ZJHK / K’), Narrow band
 Multi-object spectroscopy mode


FOV : 6’ x 4’
Multi-slit Masks Exchanger
Instruments : EMIR
 General Scientific Goals




Search for low-mass stars.
Survey and nature of IR objects embedded in molecular clouds.
CO abundances in nearby early-type galaxies.
Nature of AGN central sources and their interaction with
circumnuclear gas.
 IR spectroscopic follow-up of radio, IR, X-ray Sky Surveys.
 Distant clusters of galaxies.
 GOYA Project Scientific Goals

Carry out a comprehensive study of the rest-frame optical properties of
1000 galaxies at, including: morphology, structure, kinematics, dust
content, SFR , metallicity, luminosity and mass functions, clustering,
and large scale-structure.
 The fundamental questions that we are attempting to answer include :
What is the nature of the galaxy population at z>2?
What are their local counterparts?
Instruments : CIRCE
 Canary InfraRed Camera Experiment
 Nasmyth / Cassegrain focus
 0.9 ~ 2.4 micron infrared camera.
 Bridge the gap in the near-infrared instrumentation between
‘day-one’ and EMIR.
 Hawaii II 2048 x 2048 pixel detector.
 Scale : 0.25’’ / pixel
 Observing modes





Broad band imaging : JHK ; FOV 3.4’ x 3.4’
Narrow band imaging : FOV 3.4’ x 3.4’
Spectroscopy : 3 long-slits(0.4,0.7,1.0’’), 2 grisms (R=410, 725)
Imaging polarimetry : FOV 2’ x 50’’ (divided into 3 slots of 50’’x12’’)
Spectropolarimetry : Same grisms and slits widths as standard
spectroscopy. FOV 2’ x 50’’ (divided into 3 slots of 50’’x12’’)
 50% faster and 3 times greater FOV than NIRI/Gemini
Instruments : CIRCE
 Proposed Science Projects







NIR obervations of microquasars
Emission-line surveys for massive star clusters
Transient observations : GRB and X-ray flash
Deep JHK Photometry of Galactic Globular Clusters
The distance Scale of Local Group Dwarf Galaxies
Metal Abundance Gradients in M31 and M33
The Stellar Masses of Galaxies over Cosmological Timescales
Instruments : FRIDA







inFRared Imager and Dissector for Adaptive optics
Imaging / Integral Field Spectroscopy
First instrument of the GTC to make use of the AO system.
Nasmyth platform at the output focus of GTCAO
0.9 ~ 2.5 μm
Hawaii II 2048 x 2048 pixel detector.
Imaging mode


Scale : 0.01’’/pix , 0.02’’/pix , 0.04’’/pix
FOV : 20’’ x 20’’ , 40’’ x 40’’
 Integral field mode

30 slices with 66 pixels/slice in the spatial direction and 2 pixels per
‘resolution element’ in the spectral direction
 FOV : 0.60’’ x 0.66’’ , 1.2’’ x 1.32’’ , 2.4’’ x 2.64’’
 Spectral resolution : 1300 (H+K), 4000 (ZJHK), 20000 (HK 1.4~2.4 μm)
Instruments : FRIDA
 Science drivers

High redshift at kpc scales with FRIDA
 FRIDA and the nearest Universe
 FRIDA in our galaxy at sub-parsec scale.
OSIRIS : Tunable Filter
Tunable imaging
Spectroscopy
1 or few spectral lines
Wide spectral range (at low R)
2D spectral features
1D (long slit) or very small area (IFU)
All targets in FOV
Number of spectra per mask limited
Reliable flux calibration
Uncertain (LS,IFU), unreliable (MOS) flux
calibration
Low spectral resolution
Velocity fields & line profiles (at high R)
Approximate redshift should be known
Redshift knowledge not required
Position not required (survey)
On-the-fly observations enabled
(ex : Galaxy clusters)
TF pre-imaging avoid IFU mosaic
Position required
(pre-imaging. This introduce biases)
Drilling masks overheads
OSIRIS : Tunable Filter
Image of Ne spectral lamp
Scientific result of GTC/OSIRIS
 12 GTC Publications (using OSIRIS)









2011 (10) , 2011 (2)
Exoplanet (3)
Gamma Ray Burst (2)
Soft Gamma Ray (2)
Galaxy encounter
Faint L subdwarf
Comet
Substellar object
Black hole (X-ray transient)
Scientific result of GTC/OSIRIS
 GTC OSIRIS transiting exoplanet atmospheric
survey: detection of potassium in XO-2b form
narrowband spectrophotometry
(D.K.Sing et al., 2011)
 Hot-Jupiter exoplanets
 Identification of atmospheric contents
(one of the first steps for understanding the nature of exoplanetary atmospheres)
 XO-2B (host star of XO-2b) is 3.5 mag fainter in the
optical than those of the well studied transiting hot
Jupiters HD 189733b and HD 209458b.
Scientific result of GTC/OSIRIS
 GTC OSIRIS transiting exoplanet atmospheric
survey: detection of potassium in XO-2b form
narrowband spectrophotometry
(D.K.Sing et al., 2011)
 GTC OSIRIS transiting exoplanet atmospheric
survey: detection of potassium in XO-2b form
narrowband spectrophotometry
(D.K.Sing et al., 2011)
Science with the GTC
 The Solar System
 Extrasolar planets, substellar objects ans





faint stars
Protostellear objects and stellar formation
Compact objects and black holes
External galaxies
Axtive galaxies, ultraluminous galaxies and
primaeval galaxies
Cosmology
Observing with the GTC
 Member of a group with Guaranteed Time.
 Member of the GTC community: Spain,
Mexico and the University of Florida.
 Collaborative time under agreements
between Spain and Mexico, and Spain and
University of Florida.
 CCI International Time Programs.