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UVIT gratings and
science
Science meeting Sept 2006
J. Hutchings
1
IIA Sept 2006
Photek tube resolution
2
IIA Sept 2006
Photek tube resolution
1”
.5”
3
IIA Sept 2006
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
4
IIA Sept 2006
UVIT filters w/o gratings
FUV
Description
LiF
MgF2
CaF2
BaF2
Sapphir e
Fused Sil ica(UV Grade)
Broadband FUVF1
Closed
NUV
Description
MgF2
Fused Sil ica(UV Grade)
Narrowband NUVFC3
Narrowband NUVFMg2
Narrowband
NUVFUVHu mp
NUVFAGN1
NUVFAGN2
Closed
VIS
Description
BK7
SDSSg
ACS435W
ACS555W
V
IIA Sept 2006 Closed
Remark
Maximum Coverage and
Sens iti vit y
Default
Block OI li nes
CIV 154.9 nm li ne
HeII 164 nm li ne
Continuu m
Safety
Passband
120 – 180 nm
120 – 180 nm
125 – 180 nm
135 – 180 nm
145 – 180 nm
160 – 180 nm
125 – 150 nm
Remark
Backup for FUV
Default
CIII 191 nm l ine fil ter
MgII 280 nm li ne filt er
Absorption Band
Passband
120 – 300 nm
160 – 300 nm
191 +/- 4 nm
280 +/- 10 nm
215 +/- 15 nm
AGN Continuu m
AGN Continuu m
Safety
268 +/- 15 nm
183 +/- 15 nm
Remark
Default
Sloan Survey Filt er
HST Surv ey Filt er
HST Surv ey Filt er
John son Filt er
Safety
Passband
300 – 600 nm
380 – 550 nm
380 – 480 nm
470 – 600 nm
520 – 590 nm
5
Filter passbands
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IIA Sept 2006
Filter throughput
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IIA Sept 2006
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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IIA Sept 2006
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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IIA Sept 2006
UVIT grating blaze
10
IIA Sept 2006
Detector QE
Spec
Measured
11
IIA Sept 2006
Total sensitivity UVIT + gratings
--10 sq cm
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IIA Sept 2006
13
IIA Sept 2006
Grating PSF at 150nm
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IIA Sept 2006
Grating PSF at 250nm
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IIA Sept 2006
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
16
IIA Sept 2006
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
17
IIA Sept 2006
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
18
IIA Sept 2006
LMC star clusters with UIT
Our nearest neighbour
Galaxy
UVIT resolution
4 times better needed to resolve
crowded fields
UV spectra of many
Bright OB stars
19
IIA Sept 2006
M31, M33 OB stars
OB associations show up in
Galex and UIT images
20
IIA Sept 2006
Galex UV image of NGC5474 in M101 group
UVIT will
image these
structures
with 4 times
the resolution
Grating spectra
of bright clumps
21
IIA Sept 2006
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
IIA Sept 2006
22
Canadian UVIT
science interests
UVIT science was peer-reviewed as CUVIT by CSA Scisat program
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•
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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IIA Sept 2006
Canadian science team
David Ballantyne (CITA)
Phil Bennett (StMary’s & Colorado)
Pat Cote (HIA)
*
Michael De Robertis (York)
Laurent Drissen (Laval)
Jean Dupuis (CSA)
*
Alex Fullerton (UVIC and STScI)
Mike Hudson (Waterloo)
(*)
John Hutchings (HIA)
*
Vicky Kaspi (McGill)
(*)
Denis Leahy (Calgary)
(*)
Jaymie Matthews (UBC)
(*)
Gene Milone (Calgary)
(*)
Tony Moffatt (Montreal)
Carmelle Robert (Laval)
*
Samar Safi-Harb (Manitoba)
(*)
Peter Stetson (HIA)
IIA Sept 2006
Galaxies
Cool stars
Galaxy pops
AGN
Hot stars
WD
Hot stars
Cosmology
AGN, XRB
NS
XRB
Seismology
Binaries
Hot stars
Hot stars
NS, SNR
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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IIA Sept 2006
CASCA 2005 poster
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IIA Sept 2006
Thank you
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IIA Sept 2006
UVIT 3 channels – FUV, NUV, Optical
Passband
Channel I
120-250nm
Aperture
380mm
Configuration
RC with focal plane
Corrector *
Channel II
200-320nm
380mm
RC with focal plane
Corrector
Optical Channel
400-650nm
Beam obtained from
Channel II with
Correction for optical
13
0.5o
< 1”
Final f/ratio
Corrected field
90% of energy
on axis
13
0.5o
<1“
13
0.5o
< 1”
Microroughness
On mirrors
15Ao
15Ao
15Ao
Reflectivity per
Surface
>80%
>90%
>90%
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IIA Sept 2006
Crystalline
1.996 mm
120 – 180 nm
80
(Continuum)
Crystalline
3.0
mm
120 – 180 nm
80
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
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
1
LiF
2
MgF2
3
(Continuum)
(Continuum)
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IIA Sept 2006
UVIT filters - w/o NUV + UV gratings
1
2
3
4
5
6
7
FUV
LiF
(C ontinuum)
MgF2
(Continuum)
CaF2 (Continuum)
BaF2
(Continuum)
Sapphire (CIV 155)
Fused Silica (HeII 164)
FUVB1ontinuum)
Crystalline
Crystalline
Crystalline
Crystalline
Crystalline
Crystalline
Int erference
1.996 mm
3.0 mm
2.497 mm
2.405 mm
1.995 mm
3.0 mm
3.0 mm
120 Р 180 nm
120 Р 180 nm
125 Р 180 nm
135 Р 180 nm
145 Р 180 nm
160 Р 180 nm
125 Р 150 nm
80
80
80
80
80
80
>15
8
9
10
11
12
13
14
NUV
Fused Silica (Contm)
NUVN1 (Narrowband )
NUVB1 (Broadband )
NUVB2 (Broadband )
NUVB3 (Broadband )
NUVB4 (Broadband )
NUVN2 (Narrowband )
Crystalline
Int erference
Int erference
Int erference
Int erference
Int erference
Int erference
3.0
2.56
2.56
2.97
3.15
3.33
3.38
mm
mm
mm
mm
mm
mm
mm
160 Р 320 nm
187 Р 195 nm
170 Р 200 nm
200 Р 230 nm
230 Р 250 nm
250 Р 280 nm
275 Р 285 nm
80
>50
>50
>50
>50
>60
>60
15
16
17
18
19
VIS
BK7
VIS 1
VIS 2
B
VIS 3
Window
Int erference
Int erference
Int erference
Int erference
3.0
3.0
3.0
3.0
3.0
mm
mm
mm
mm
mm
300 Р 600 nm
320 Р 360 nm
370 Р 410 nm
390 Р 470 nm
400 Р 530 nm
90
>85
>85
>85
>85
IIA Sept 2006
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Visible and UIT image of NGC4736
UV image
reveals
circumnuclear
star-formation
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IIA Sept 2006
UIT image of NGC6752
Distribution of
hot stars differs
from overall
cluster
32
IIA Sept 2006
UV morphology of galaxies
Multi-filter imaging for stellar pops
•
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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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IIA Sept 2006
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IIA Sept 2006