IIA Sept 2006 1

UVIT gratings and science

Science meeting Sept 2006

J. Hutchings

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Photek tube resolution

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Photek tube resolution

1”

.5”

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Image quality expected

• Final PSF combined from

tube resolution (0.5-1”)

telescope optics (<1”)

spacecraft jitter (<0.5”)

• Final resolution may be 1.0” to 1.5”

worst at short wavelengths

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FUVDescription Remark PassbandLiF Maximum Coverage and

Sensitivity120 – 180 nm

MgF2 120 – 180 nmCaF2 Default 125 – 180 nmBaF2 Block OI lines 135 – 180 nmSapphire CIV 154.9 nm line 145 – 180 nmFused Silica(UV Grade) HeII 164 nm line 160 – 180 nmBroadband FUVF1 Continuum 125 – 150 nmClosed Safety

NUVDescription Remark PassbandMgF2 Backup for FUV 120 – 300 nmFused Silica(UV Grade) Default 160 – 300 nmNarrowband NUVFC3 CIII 191 nm line filter 191 +/- 4 nmNarrowband NUVFMg2 MgII 280 nm line filter 280 +/- 10 nmNarrowbandNUVFUVHump

Absorption Band 215 +/- 15 nm

NUVFAGN1 AGN Continuum 268 +/- 15 nmNUVFAGN2 AGN Continuum 183 +/- 15 nmClosed Safety

VISDescription Remark PassbandBK7 Default 300 – 600 nmSDSSg Sloan Survey Filter 380 – 550 nmACS435W HST Survey Filter 380 – 480 nmACS555W HST Survey Filter 470 – 600 nmV Johnson Filter 520 – 590 nmClosed Safety

UVIT filters w/o gratings

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Filter passbands

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Filter throughput

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UVIT gratings

• 400 grooves per mm

• Second order in FUV (35 microns/nm)

• First order in NUV (18 microns/nm)

• Deflection is 6mm at 300nm

(~4 arcmin of 30 arcmin field)

• Deflection 2.2mm (1.5arcmin) at 130nm

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Grating specs

• Blaze peak 140nm in FUV

• Blaze peak 270nm in NUV

• 70% efficiency at peaks

• Resolution 1nm (10A) in FUV (R~140)

2nm (20A) in NUV (R~130)

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UVIT grating blaze

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Detector QE

Spec Measured

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Total sensitivity UVIT + gratings

--10 sq cm

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Grating PSF at 150nm

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Grating PSF at 250nm

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Grating spectra summary

• UVIT eff area approx 100 sq cm in NUV 50 sq cm in FUV Similar to FUSE• Signal/px ~80 times less than open direct image (3-4 magnitudes less sensitive than filter image)• PSF of 1.5” ~35microns • Grating spectra ~2.1mm for full FUV/NUV range This is 5% of detector diameter Sky bgnd in spectrum ~1 count per 1000 sec

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Hot stars in solar neighbourhood

Spectra of local hot objects add to imaging information

• Census of WD population for missing mass• Pulsating stars over wide wavelength range• Accretion disk SEDs in close binaries• WR star variability in UV• OB star SEDs and temperatures• UV photometry of flare events

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Hot stars in nearby galaxies

Good spatial resolution important in crowded fields

• Hot stars measure star formation and dominate the energy output of galaxies

• UV imaging will resolve the hot stars, free of crowding by cool stars in the visible

• UV interstellar extinction in different environments• Detailed studies of Magellanic Clouds• Global young star populations in different galaxies• IMF in local group galaxies• LBVs in distant galaxies for distance scale work• Spectra will reveal UV extinction laws

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LMC star clusters with UIT

Our nearest neighbourGalaxy

UVIT resolution4 times better -needed to resolvecrowded fields

UV spectra of manyBright OB stars

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M31, M33 OB stars

OB associations show up in Galex and UIT images

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Galex UV image of NGC5474 in M101 group

UVIT willimage thesestructureswith 4 timesthe resolution

Grating spectraof bright clumps

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Lyman alpha surveys On and off band images : shortest FUV bandpass desirable

Or use gratings for isolated hot objects.

• Strongest emission line in the universe• Used for high z galaxy and QSO surveys• Gas distribution in galaxy groups & clusters• Gas morphology in local galaxies• Calibrate L alpha in high z objects• AGN luminosity function in z=1 to 2

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Canadian UVIT science interests

UVIT science was peer-reviewed as CUVIT by CSA Scisat program

• Massive star populations in local galaxies

• Stellar cycles and variability

• Starburst galaxies and AGN

• WD and other evolved stars

• UV morphology of galaxies

• Deep UV survey for cosmic SF history

• GALEX survey follow-on

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Canadian science team

David Ballantyne (CITA) GalaxiesPhil Bennett (StMary’s & Colorado) Cool starsPat Cote (HIA) * Galaxy popsMichael De Robertis (York) AGNLaurent Drissen (Laval) Hot starsJean Dupuis (CSA) * WDAlex Fullerton (UVIC and STScI) Hot starsMike Hudson (Waterloo) (*) CosmologyJohn Hutchings (HIA) * AGN, XRBVicky Kaspi (McGill) (*) NSDenis Leahy (Calgary) (*) XRBJaymie Matthews (UBC) (*) SeismologyGene Milone (Calgary) (*) BinariesTony Moffatt (Montreal) Hot starsCarmelle Robert (Laval) * Hot starsSamar Safi-Harb (Manitoba) (*) NS, SNRPeter Stetson (HIA) Stellar pops

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UV Deep survey

100,000sec over 6 filter FUV + NUV bands

• UV light from distant galaxies and UV background of the universe

• Ionisation and opacity of IGM• Galaxy counts at z=0.5 to 2.5 - gap in

ground-based window• Cosmic star formation history peak

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CASCA 2005 poster

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Thank you

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Channel I Channel II Optical ChannelPassband 120-250nm 200-320nm 400-650nm

Aperture 380mm 380mm -

Configuration RC with focal plane RC with focal plane Beam obtained from Corrector * Corrector Channel II with

Correction for opticalFinal f/ratio 13 13 13Corrected field 0.5o 0.5o 0.5o90% of energy < 1 “ < 1” < 1”on axis

Microroughness 15Ao 15Ao 15AoOn mirrors

Reflectivity per >80% >90% >90%Surface

UVIT 3 channels – FUV, NUV, Optical

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1 LiF (Continuum) Crystalline 1.996 mm 120 – 180 nm 80

2 MgF2 (Continuum) Crystalline 3.0 mm 120 – 180 nm 80

3 CaF2 (Continuum) Crystalline 2.497 mm 125 – 180 nm 80

4 BaF2 (Continuum) Crystalline 2.405 mm 135 – 180 nm 80

5 Sapphire (CIV 155) Crystalline 1.995 mm 145 – 180 nm 80

6 Fused Silica (HeII 164) Crystalline 160 – 180 nm 80

7 FUVF1 (Continuum) Interference 125 – 150 nm 10

8 Fused Silica (Contm) Crystalline 3.0 mm 160 – 320 nm 80

9 MgF2 (Continuum) Crystalline 2.815 mm 120 – 320 nm 80

10 NUVFC3 (CIII 191) Interference 187 – 195 nm 40

11 NUVFMg2 (MgII 280) Interference 3.277 mm 275 – 285 nm 40

12 NUVFUVHump Interference 2.979 mm 200 –230 nm 40

13 NUVFAGN1 Interference 2.689 mm 250 – 280 nm 40

14 NUVFAGN2 Interference 3.238 mm 170 – 200 nm 40

15 BK7 Window 3.0 mm 300 – 600 nm 90

16 SDSSg Interference 3.049 mm 380 – 550 nm 90

17 ACS435W Interference 2.988 mm 380 – 480 nm 85

18 ACS555W Interference 3.122 mm 470 – 600 nm 85

19 V Interference 3.141 mm 520 – 590 nm 85

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FUV1 LiF (Continuum) Crystalline 1.996 mm 120 – 180 nm 802 MgF2 (Continuum) Crystalline 3.0 mm 120 – 180 nm 803 CaF2 (Continuum) Crystalline 2.497 mm 125 – 180 nm 804 BaF2 (Continuum) Crystalline 2.405 mm 135 – 180 nm 805 Sapphire (CIV 155) Crystalline 1.995 mm 145 – 180 nm 806 Fused Silica (HeII 164) Crystalline 3.0 mm 160 – 180 nm 807 FUVB1ontinuum) Interference 3.0 mm 125 – 150 nm >15

NUV8 Fused Silica (Contm) Crystalline 3.0 mm 160 – 320 nm 809 NUVN1 (Narrowband) Interferen ce 2.5 6 mm 187 – 19 5 nm >5010 NUVB1 (Broadband) Interferen ce 2.5 6 mm 170 – 20 0 nm >5011 NUVB2 (Broadband) Interferen ce 2.9 7 mm 200 – 23 0 nm >5012 NUVB3 (Broadband) Interferen ce 3.1 5 mm 230 – 25 0 nm >5013 NUVB4 (Broadband) Interferen ce 3.3 3 mm 250 – 28 0 nm >6014 NUVN2 (Narrowband) Interferen ce 3.3 8 mm 275 – 28 5 nm >60

VIS15 BK7 Windo w 3.0 mm 300 – 60 0 nm 9016 VIS1 Interferen ce 3.0 mm 320 – 36 0 nm >8517 VIS2 Interferen ce 3.0 mm 370 – 41 0 nm >8518 B Interferen ce 3.0 mm 390 – 47 0 nm >8519 VIS3 Interferen ce 3.0 mm 400 – 53 0 nm >85

UVIT filters - w/o NUV + UV gratings

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Visible and UIT image of NGC4736

UV image reveals circumnuclearstar-formation

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UIT image of NGC6752

Distribution ofhot stars differsfrom overallcluster

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UV morphology of galaxies

Multi-filter imaging for stellar pops

• 4 times the detail of Galex

• Galex catalogue for sample selection

• Evolution of stellar populations

• UV upturn location

• Mergers and star formation

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