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CRIRES - VLT High-Resolution IR Echelle Spectrometer

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CRIRES
High-Resolution IR Echelle Spectrometer

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Crires Optical Design
Click on the image for a full sized display

 

Table of Content

Instrument Name

CRIRES

ESO Responsible

H.U. Käufl

Instrument Scientist

R. Siebenmorgen

Location

Nasmyth UT1 (ANTU)

Status

Commissioning

Science Team

B. Gustafsson, C. de Bergh, A. Hatzes, K. Hinkle, E. van Dishoeck


 

Instrument Status

CRIRES first commissioning was successfully performed in June 2006.

First light images and spectra and more information is available : HERE

A second and third commissioning is scheduled in August and October 2006.

Our goal is to be able to release the instrument for the next call for proposals.
 

Science Verification

The science verification (SV) for CRIRES is carried out following the: VLT   Science Verification Policy and Procedures .

SV runs are interleaved with commissioning and test activities, taking place between August 2006 and April 2007.

SV observer shall submit their proposals using the Science Verification proposal template Proposers are asked to provide at least a short summary of the science goal, coordinates and magnitudes of GS and science target, a finding chart, the observing wavelength ID, as specified in appendix A of the UM and DIT, NDIT settings of science detectors as computed with the exposure time calculator (see below).

Useful Links and manuals


 

Science Objectives

A cryogenic high-resolution IR spectrograph has been conceived for the VLT in order to exploit the enormously enhanced sensitivity provided by a dispersive instrument with a large detector array at an 8 m telescope. The gain entails a quantitative and qualitative improvement of the observational capabilities. It can boost all scientific applications aiming at fainter objects, higher spatial (extended sources), spectral and temporal resolution.

The IR spectrograph will make previously inaccessible phenomena and objects available for spectroscopic studies. Table 1 presents a list of science objectives.

Table 1: Science Objectives

Extra-Solar Planets

Radial velocities studies

Direct spectroscopic detection and characterization: CO, CH4.

 

Solar System

Chemistry/phys. conditions/velocity fields/structure

Giant planets/Titan

H3+, CH4, NH3, CH3D, AsH3, H2O,C2H2,C2H6, PH3, CH3, NH3, HCN, C2H2, C2H6, PH3, CH3, NH3, HCN

Terrestrial planets

CO, HCL, HF, HDO, H2O, OCS
Mars imaging (0.1"- 40 Km) spectr. of CO depletion.

Io

spatial/time mapping of volcanic activity (SO2)

Pluto/Charon/Triton

search tenous CO, CH4 atmos.

Comets

(resolve nuclei), H2O abundance, temperature, velocities, minor species.

 

Stars

Stellar evolution/nucleosynthesis (OB, AGB stars, cluster red giants, cool MS, C & S stars in galaxy, S/LMC, nearby glaxies), CNO isotopic abundances unique in IR.

Stellar mass:atom/mol. lines from secondaries

Stellar winds/mass loss, OB, WR, AGB stars in galaxy and S/LMC, CO,SiO,C2H2, HCN

Atmospheric structure & oscillations in cool stars

Magnetic fields

 

Star Formation Regions/ISM

Accretion/Outflow from embedded YSOs

ISM chemistry/ cloud structure, H3+, H2O, CH4, C2H2, NH3

 

Extragalactic

AGN

Velocity structure of BLR, NLR, CLR & molecular clouds, H recombination, [FeII], [SiIV], H2 lines suffering low dust extinction

 

Instrument Concept and Capabilities

The cryogenic echelle will provide for:

Functionally, the instrument can be divided into four units. The fore-optics section provides for field de-rotation, cold pupil and field stops, curvature sensing adaptive optics, and slit viewing. The prism predisperser isolates one echelle order and minimizes the total amount of light entering into the high-resolution section. The high-resolution section comprises the collimator, the echelle which is tilt-tuned for wavelength selection, the camera providing the 0.1 arcsec/pixel plate scale, and the detector(s). The calibration unit outside the cryogenic environment contains light sources for flux/wavelength calibration and detector flatfielding.

Observational capabilities and predicted performance are given in Tables 2 and 3.

Table 2: Cryogenic Echelle Main Characteristics

Parameter

Value

Focus

Nasmyth

Configuration

stationary

Wavelenght range

1-5 µm

Slit width-res. power product

20,000-40,000 (Rmax = 100.000)

Echelle

40 cm length, 31.6 lines/mm

Optics

reflective

Detector

3 x 1024 x 1024 InSb arrays

Pixel size

0.1 arcsec

Spectral format

single order

Slit length

~ 50"

Operating temperature

60-80 °K

Detector temperature

~30 °K

background subtraction

nodding

Istantaneous wavelength coverage

lambda/70

 

Table 3: Performance Limits

Limiting magnitudes ( for S/N = 3 in 1 hr)

Wavelength (µm)

1.2

1.6

2.2

3.3

4.2

4.7

mag

17

16.5

16

13.5

12.5

11

Integration times (required for S/N=100 on a 5th mag. star)

Wavelength (µm)

1.2

1.6

2.2

3.3

4.2

4.7

T [sec], mag=5

< 5

5

10

10

15

30


Send comments to Ralf Siebenmorgen
Last update: 07/07/06

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