Telescope Optical Design - inaoe
Telescope Optical Design - inaoe Telescope Optical Design - inaoe
Resolving power SPM-Twin: Wide-Field Sampling & Integration (complementary limitations) 1.5° Field of View (5400”) = 1.77 square degrees Lots of sampling elements (“spaxels”): 2.4x10 7 squared arcsecs a) Full wavelength range with well-chosen spatial coverage (d-IFUs, fiber-bundles, starbugs) b) Full spatial coverage with a finite wavelength range (WFT tunable imager) 1800 OSIRIS TF: Available resolving powers 1600 1400 1200 1000 800 600 400 200 0 400 500 600 700 800 900 1000 Wavelength (nm) m = 2 l cos R = m N dR/R = dm/m = dl/l R: 100 - 1000 m: 4 – 40 l : 1.5 – 15 μm K.A.O.S. Purple Book 2002 GTC-OSIRIS
SPM-Twin WFT: 3 Spaxel Distributions for Spectroscopy High-Z & Stellar objects a. Super sloan-like surveys (DE, LSS, etc. basically redshifts) b. Stellar surveys (thick disk, Local group systems) c. GC & PN systems d. HII Regions in local galaxies Very large number of individual spaxels (sparse sampling) with limited patrol fields each) The Intermediate-z Universe and semi-crowded fields a. Indicative galaxy dynamics, gradients and size b. Indicative structure (notches, pair interaction, etc) A number of relatively small IFUs (sparse with limited-continuous sampling), relatively large patrol fields The “local” 150 Mpc Universe a. Large galaxies b. galactic extended sources Single Large IFU (continuous sampling), fixed patrol field
- Page 1 and 2: Synoptic All-Sky Infrared Survey Te
- Page 3 and 4: SASIR dedicated telescope A new lar
- Page 5 and 6: SPM-Twin: Competitiveness based on
- Page 7 and 8: FWHM ["] FWHM ["] SPM-Twin: 1.5°-2
- Page 9 and 10: Diameter [mm] SPM-Twin: WF Telescop
- Page 11 and 12: SPM-Twin: WFT Atmospheric Dispersio
- Page 13 and 14: 100 cm S P M 6.5m f/4.5 WFT Effecti
- Page 15 and 16: Infrared emission Mauna Kea atmosph
- Page 17: SASIR pre-conceptual design Tels ex
- Page 23 and 24: Normal Field 9’ FoV (0.075)
- Page 25 and 26: WFCAM (UKIDSS) ‣ 3.8 m UK InfraRe
- Page 27: f/2.5
- Page 32 and 33: Relevant issues to cover by the opt
- Page 34 and 35: Thanks!
- Page 36 and 37: ‣ Input from the community (diver
- Page 40 and 41: Sitios privilegiados para el visibl
- Page 42 and 43: Algunos de los primarios de hoy 67t
- Page 44 and 45: Basic Survey ‣ ~ 20 sec dithered
- Page 46: Technical Concept (Detectors)
- Page 49 and 50: M US$ 1 st order estimate Need IR-C
- Page 51 and 52: Detectors ‣ The cost of large for
- Page 53 and 54: Cost [FY2008 $Million] Telescopios
- Page 55 and 56: Cost [FY2008 $Million] Telescopios
- Page 57 and 58: Cost [FY2008 $Million] Very LargeTe
- Page 59 and 60: Cost [FY2008 $Million] Telescopios
- Page 61 and 62: Cost [FY2008 $Million] Cost-Apertur
- Page 63 and 64: Previous work $ ~ D 2.6 (Smith-Kale
- Page 65 and 66: Cost [FY2008 $Million] 1000.0 100.0
- Page 67 and 68: Distribución de costos de inversi
- Page 69: Operación ‣ Varían entre el 7%
SPM-Twin WFT:<br />
3 Spaxel Distributions for Spectroscopy<br />
High-Z & Stellar objects<br />
a. Super sloan-like surveys (DE, LSS, etc. basically redshifts)<br />
b. Stellar surveys (thick disk, Local group systems)<br />
c. GC & PN systems<br />
d. HII Regions in local galaxies<br />
Very large number of individual spaxels (sparse sampling) with limited patrol<br />
fields each)<br />
The Intermediate-z Universe and semi-crowded fields<br />
a. Indicative galaxy dynamics, gradients and size<br />
b. Indicative structure (notches, pair interaction, etc)<br />
A number of relatively small IFUs (sparse with limited-continuous sampling),<br />
relatively large patrol fields<br />
The “local” 150 Mpc Universe<br />
a. Large galaxies<br />
b. galactic extended sources<br />
Single Large IFU (continuous sampling), fixed patrol field
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