Calibration of the cosmic origins spectrograph
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Calibration of the Cosmic Origins Spectrograph. James C. Green University of Colorado. The CU COS Instrument Team. Project Scientist: Cynthia Froning Instrument Scientist: Steve Osterman Steve Penton St é phane B é land Detector Scientist: Jason McPhate (Berkeley) Gone – but not forgotten

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Calibration of the Cosmic Origins Spectrograph

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Calibration of the cosmic origins spectrograph

Calibration of the Cosmic Origins Spectrograph

James C. Green

University of Colorado


The cu cos instrument team

The CU COS Instrument Team

Project Scientist: Cynthia Froning

Instrument Scientist: Steve Osterman

Steve Penton

Stéphane Béland

Detector Scientist: Jason McPhate (Berkeley)

Gone – but not forgotten

Erik Wilkinson

Ken Brownsberger

John Andrews

Jon Morse

Dennis Ebbets

Dave Sahnow


Calibration of the cosmic origins spectrograph

NUV MAMA

Detector

(STIS spare)

Calibration

Platform

OSM2: G185M, G225M,

G285M, G230L, TA1

  • COS has 2 channels to provide low and medium

    resolution UV spectroscopy

    • FUV: 1150-1775Å, NUV: 1700-3200Å

  • FUV gratings: G130M, G160M, G140L

  • NUV gratings: G185M, G225M, G285M, G230L

    • M gratings have spectral resolution of R ~ 20,000

FUV XDL

Detector

Aperture Mechanism:

Primary Science Aperture,

Bright Object Aperture

OSM1: G130M,

G160M, G140L,

NCM1

Optical bench

(not shown):

re-use of GHRS

bench


Cos fuv spectroscopic modes

COS FUV Spectroscopic Modes

Nominal WavelengthResolving Power

Grating Wavelength Range (R = l/Dl) b

Coverage a per Exposure

G130M1150 - 1450 Å 300 Å 20,000 - 24,000

G160M1405 - 1775 Å 375 Å 20,000 - 24,000

G140L1230 - 2050 Å > 820 Å 2400 - 3500

a Nominal Wavelength Coverage is the expected usable spectral range delivered by each grating mode. The G140L grating disperses the 100 - 1100 Å region onto one FUV detector segment and 1230 - 2400 Å onto the other. The sensitivity to wavelengths longer than 2050 Å or shorter than 1150 Å will be very low.

b The lower values of the Resolving Power shown are delivered at the shortest wavelengths covered, and the higher values at longer wavelengths. The resolution increases roughly linearly between the short and long wavelengths covered by each grating mode.


Calibration of the cosmic origins spectrograph

* N2 purge data through FUV detector door window.

* Portion of FUV detector flat-field obtained during component-level testing.


Cos nuv spectroscopic modes

COS NUV Spectroscopic Modes

Nominal WavelengthResolving Power

Grating Wavelength Range (R = l/Dl) b

Coverage a per Exposure

G185M 1700 - 2100 Å 3 x 35 Å 16,000 - 20,000

G225M 2100 - 2500 Å 3 x 35 Å 20,000 - 24,000

G285M 2500 - 3200 Å 3 x 41 Å 20,000 - 24,000

G230L 1700 - 3200 Å(1 or 2) x 400 Å 1500 - 2800

a Nominal Wavelength Coverage is the expected usable spectral range delivered by each grating mode, in three non-contiguous strips for the medium-resolution modes. The G230L grating disperses the 1st-order spectrum between 1700 - 3200 Å along the middle strip on the NUV detector. G230L also disperses the 400 - 1400 Å region onto one of the outer spectral strips and the 3400 - 4400 Å region onto the other. The shorter wavelengths will be blocked by an order separation filter and the longer will have low thruput on the solar blind detector. The G230L 2nd-order spectrum between 1700 - 2200 Å will be detected along the long wavelength strip.

b The lower values of the Resolving Power shown are delivered at the shortest wavelengths covered, and the higher values at longer wavelengths. The resolution increases roughly linearly between the short and long wavelengths covered by each grating mode.


Calibration of the cosmic origins spectrograph

Point source Spectra

Calibration Stripes

NCM3a

NCM3a

NCM3b

NCM3c

NCM3b

NCM3c

Increasing Wavelength

25.60 square

1.45

5.75

2.25

4.95

2.80

2.80

All dimensions in mm

  • NUV spectra projected onto the NUV MAMA detector


Wavelength accuracy

Wavelength Accuracy

Extragalactic moderate resolution programs generally require absolute wavelength accuracy of ~ +/- 1 resel ( = +/- 15 km/s), with relative accuracy of 1/3 resel rms across the spectrum.

Some programs that require higher accuracy can use “tricks” to obtain needed calibration - e.g., using known wavelengths of ISM lines along sight-line.

  • The aberrated HST PSF centered in the COS Primary Science Aperture.

Target Acquisition

  • COS is a “slitless” spectrograph, so the precision of target acquisition (placement of target relative to calibration aperture) is the largest uncertainty for determining the absolute wavelength scale.

  • Goal is to center targets routinely in science apertures to a precision of

  • +/- 0.1 arcsec (= +/- 10 km/s).

  • Throughput is relatively insensitive to centering due to large size of science apertures; centering of +/- 0.3 arcsec necessary for >98% slit throughput.


Fundamental design priorities

Fundamental Design Priorities

1: Sensitivity

2: Bandpass

3: Spectral Resolution


High sensitivity

High Sensitivity

High throughput achieved through a minimum of reflections - ion etched blazed holographic gratings - windowless, opaque photocathode (NUV)

COS throughput measured by direct comparison to RASCAL reference detector – effective areas calculated by multiplying by HST area and reflectivity


Calibration of the cosmic origins spectrograph

For Comparison - COS Throughputs:G130M @ 1216 Å (peak) = 19.7%, @1430 Å = 9.0%G160M @ 1430 Å = 11.7%, @1669 Å = 5.8%G140L @ 1248 Å = 10.7%, @1723 Å = 0.65%G185M @1777 Å = 3.9%, @2085 Å = 2.3%G225 M @ 2262 Å = 2.7%, @ 2497 Å = 2.8%G285M @ 2659 Å = 2.2%, @ 2998 = 1.0%G230L @ 1846 Å = 3.0%, @ 2998 Å = 0.8%


Spectral resolution

Spectral Resolution

Spectral Resolution determined by measuring the FWHM of best Gaussian fit to emission lines:

FWHM (m) * dispersion (Å/m) = 

/ = Resolution

This technique will underestimate the true resolution if the emission line is not monochromatic


Cos has an imaging mode

COS has an imaging mode

  • TA1 : implemented for target acquisition and correction of initial installation errors

  • Broad Band Imaging in the NUV – no filters – response dictated by the MAMA QE curve


Cos imaging

COS Imaging

Plate scale = 0.024″ / pixel

FWHM resolution (radial)  2.7 pixels = 0.064″ (FWHM is ~ 78% encircled energy)

Field of View = 2.5″ - 3″ (fuzzy edge)

(40 resol diameter - 105 pixel diameter image)

For comparison, ACS WFC/HRC has 80/82% encircled energy in 0.25″


Cos flat fielding

COS Flat Fielding

  • NUV MAMA – classic flat filed techniques yield high signal/noise capabilities


Cos flat fielding1

COS Flat Fielding

  • FUV detector show hex pattern consistent with MCP manufacturing process –

  • Stable geometric distortion map can be developed and applied

  • Classic flat field techniques do not fully remove the structure - redistribution


Cos bonus feature

COS Bonus Feature

Potential capability from 912 - 1150Å

G140L places these wavelengths on the detector with spectral resolution of ~ 1000

Grating efficiency at 1048Å measured – implying 20-50 cm2 effective area at 1048Å – assuming that HST mirror coatings behave as grating coating


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