TIPS-JIM Meeting
19 October 2006, 10am, Auditorium
1.
The Final Flux Calibration of the STIS Echelle
Alessandra Aloisi
Modes
2.
ACS Status Update
Ken Sembach
3.
HST Instrument Capabilities after SM4
Jerry Kriss
Next TIPS Meeting will be held on 16 November 2006.
The Final Flux Calibration
of the STIS Echelle Modes
Alessandra Aloisi
(ESA/STScI)
• Description of the issues involved
• Data analysis and results
• Pipeline tools implemented for corrections
TIPS Meeting – 19 October 2006
1
The Final Flux Calibration
of the STIS Echelle Modes
Alessandra Aloisi
(ESA/STScI)
In collaboration with R. Bohlin & J. Kim-Quijano
• Description of the issues involved
• Data analysis and results
• Pipeline tools implemented for corrections
TIPS Meeting – 19 October 2006
1
Outstanding Issues
• Time dependent sensitivity
• Blaze function characterization
 Shifts vs. location (x,y) & t
 Shape vs. location (x,y) & t
• Updated F calibration of prime modes
• On-orbit F calibration of secondary modes
TIPS Meeting – 19 October 2006
2
Time Dependent Sensitivity (TDS)
BD+28D4211 — E140M (1425)
• Sensitivity
of MAMAs
decreases
with time
(contaminants)
1997.7
2000.9
2004.0
F errors < 15%
TIPS Meeting – 19 October 2006
3
Time Dependent Sensitivity (TDS)
• Analysis of Spectra with same MO & different t
= BD+28D4211 MO = (0,0)
Prime Modes E140H (1416)
E230H (2263)
t = 1997.7–2004
E140M (1425)
E230M (1978, 2707)
 Results
* Similar trend as first-order modes
TIPS Meeting – 19 October 2006
4
Time Dependent Sensitivity (TDS)
• Analysis of Spectra with same MO & different t
= BD+28D4211 MO = (0,0)
Prime Modes E140H (1416)
E230H (2263)
t = 1997.7–2004
E140M (1425)
E230M (1978, 2707)
 Results
* Similar trend as first-order modes
G140L
E140M (1425)
TIPS Meeting – 19 October 2006
4
Time Dependent Sensitivity (TDS)
• Analysis of Spectra with same MO & different t
= BD+28D4211 MO = (0,0)
Prime Modes E140H (1416)
E230H (2263)
t = 1997.7–2004
E140M (1425)
E230M (1978, 2707)
 Results
* Similar trend as first-order modes
* Some scatter due to:
temperature ?
mis-centering in small aperture ?
blaze shift correction ?
TIPS Meeting – 19 October 2006
4
Time Dependent Sensitivity (TDS)
• TDS correction
from first-order
modes
• New TDS files
delivered to
the pipeline
 Apr. 2005
BD+28D4211 — E140M (1425)
FOS
no TDS correction
TDS correction
2004.0
 F uncertainty < few %
TIPS Meeting – 19 October 2006
5
Blaze Function (BF)
BD+28D4211 — E140M (1425)
• BF leads to
ripples in
calibrated
spectra
1998
 saw-tooth F
calibration
errors < 20%
TIPS Meeting – 19 October 2006
6
Blaze Function (BF)
BD+28D4211 — E140M (1425)
• BF leads to
ripples in
calibrated
spectra
2000.4
 saw-tooth F
calibration
errors < 20%
TIPS Meeting – 19 October 2006
6
Blaze Function (BF)
BD+28D4211 — E140M (1425)
• BF leads to
ripples in
calibrated
spectra
2003.4
 saw-tooth F
calibration
errors < 20%
TIPS Meeting – 19 October 2006
6
BF Variations
• Changes with time (contaminants & optics)
& location on the detector (MOs)
 What type of changes ?
* BF Shift
* BF Shape
 What causes the changes ?
* Effects due to location (x,y)
* Effects due to time (t)
TIPS Meeting – 19 October 2006
7
BF Shift
• MO produces BF shift
• Algorithm already implemented into pipeline
Bowers & Lindler (2002)
TIPS Meeting – 19 October 2006
8
BF Shift
• MO produces BF shift
• Algorithm already implemented into pipeline
Bowers & Lindler (2002)
TIPS Meeting – 19 October 2006
8
BF Shift
Parameter Model
• MO produces BF 2shift
BZS = A∗Δx + B∗Δy
• Algorithm already implemented into pipeline
Bowers & Lindler (2002)
TIPS Meeting – 19 October 2006
8
BF Shift
Parameter Model
• MO produces BF 2shift
Residuals
vs. t + B∗Δy
BZS = A∗Δx
• Algorithm already implemented into pipeline
Bowers & Lindler (2002)
TIPS Meeting – 19 October 2006
8
BF Shift
Parameter Model
• MO produces BF 2shift
Residuals
vs. t= A∗Δx
BLZSHIFT
+ B∗Δy
3 Parameter
Model
• Algorithm already implemented
into pipeline
BZS = A∗Δx+B∗Δy+C∗t
Bowers & Lindler (2002)
TIPS Meeting – 19 October 2006
8
BF Shift
• MO produces BF shift
• Algorithm already implemented into pipeline
Bowers & Lindler (2002)
 CALSTIS 2.13b (Sep. 2002)
 BZS = A ∗ Δx + B ∗ Δy + C ∗ t
Δx & Δy from wavecals
A, B, & C from fit of data (1997-2001)
• MO switched off in Aug 2002
TIPS Meeting – 19 October 2006
8
BF Shape with Location
• Analysis of Spectra with different MO & same t
= BD+28D4211
5 MOs
t = Jul 2002
Prime Mode E230H (2513)
 Results
* No change in BF shape with location
* Average BF shift similar to pipeline BZS
once MO = (0,0) taken as reference
correct spatial BZS component
* No strong dependence on the order
TIPS Meeting – 19 October 2006
9
BF Shape with Location
E230H (2513)
• Analysis of Spectra with different MO & same t
= BD+28D4211
5 MOs
t = Jul 2002
Prime Mode E230H (2513)
 Results
* No change in BF shape with location
* Average BF shift similar to pipeline BZS
once MO = (0,0) taken as reference
correct spatial BZS component
* No strong dependence on the order
TIPS Meeting – 19 October 2006
9
BF with Time
• Analysis of Spectra with same MO & different t
Same datasets used for TDS
TIPS Meeting – 19 October 2006
10
BF with Time
• Analysis of Spectra with same MO & different t
Same datasets used for TDS
E140M (1425) – order 95
TIPS Meeting – 19 October 2006
10
BF with Time
• Analysis of Spectra with same MO & different t
Same datasets used for TDS
 Results
* No change in BF shape with time
TIPS Meeting – 19 October 2006
10
BF with Time
• Analysis of Spectra with same MO & different t
Same datasets used for TDS
 Results
* No change in BF shape with time
* BF shift linear with time
(once spatial component subtracted)
TIPS Meeting – 19 October 2006
10
BF with Time
• Analysis of Spectra with same MO & different t
Same datasets used for TDS
E140M (1425)
 Results
* No change in BF shape with time
* BF shift linear with time
(once spatial component subtracted)
TIPS Meeting – 19 October 2006
10
BF with Time
• Analysis of Spectra with same MO & different t
Same datasets used for TDS
 Results
* No change in BF shape with time
* BF shift linear with time
(once spatial component subtracted)
* Clear break between Side 1 and Side 2 operations
linear extrapolation of pipeline wrong
TIPS Meeting – 19 October 2006
10
BF with Time
• Analysis of Spectra with same MO & different t
Same datasets used forE140M
TDS (1425)
 Results
* No change in BF shape with time
* BF shift linear with time
(once spatial component subtracted)
* Clear break between Side 1 and Side 2 operations
linear extrapolation of pipeline wrong
TIPS Meeting – 19 October 2006
10
BF with Time
• Analysis of Spectra with same MO & different t
Same datasets used for TDS
 Results
* No change in BF shape with time
* BF shift linear with time
(once spatial component subtracted)
* Clear break between Side 1 and Side 2 operations
linear extrapolation of pipeline wrong
* Clear (linear) dependence of BF shift on order
average BF shift not correct
TIPS Meeting – 19 October 2006
10
BF with Time
• Analysis of Spectra with same MO & different t
Same datasets used for TDS
 Results
* No change in BF shape with time
* BF shift linear with time
(once spatial component subtracted)
* Clear break between Side 1 and Side 2 operations
linear extrapolation of pipeline wrong
* Clear (linear) dependence of BF shift on order
average BF shift not correct
* Similar behavior of E230M(1978) & E230M(2707)
extrapolation to other modes
TIPS Meeting – 19 October 2006
10
Implementation of New
Blaze Shift Correction
E140H (1416)
• Linear fit vs time
ΔBZS = α t + β
for every order
• Fit with zero- or firstorder polynomial of
α and β coeff. vs order
Side 1 & Side 2
TIPS Meeting – 19 October 2006
11
Implementation of New
Blaze Shift Correction
E140H (1416)
Constant
Linear Coeff.
E140H (1416)
Order
TIPS Meeting – 19 October 2006
E140M (1425)
Linear Coeff.
Constant
E140M (1425)
Order
12
Implementation of New
Blaze Shift Correction
E230H (2263)
Constant
Linear Coeff.
E230H (2263)
Order
TIPS Meeting – 19 October 2006
E230M (1978)
Linear Coeff.
Constant
E230M (1978)
Order
12
Implementation of New
Blaze Shift Correction
E230M (2707)
Constant
Linear Coeff.
E230M (2707)
Order
TIPS Meeting – 19 October 2006
E230M (1978)
Linear Coeff.
Constant
E230M (1978)
Order
12
Implementation of New
Blaze Shift Correction
BD+28D4211 – E230M (1978)
• Implementation
of new BZS vs
order and side
• New PHT files
FOS
Pipeline BZS
New BZS
will be delivered
to the pipeline
 delivery next week
2004.4
 F uncertainty from
~10% to < 1-2 %
TIPS Meeting – 19 October 2006
13
Updated Flux Calibration
of Prime Modes
• 2D algorithm for Scattered Light implemented
into the pipeline
Lindler & Bowers (2002)
 CALSTIS 2.9
(Dec. 2000)
 F uncertainty < 2%
(absorption lines)
ISR STIS 02-01
TIPS Meeting – 19 October 2006
14
Updated Flux Calibration
of Prime Modes
• Re-determination of Echelle flux calibration for
self-consistency
BD+28D4211 — E140M (1425)
 no changes due to SL
 2-7 % due to other
FOS
old PHT file
new PHT file
• New PHT files
delivered to
the pipeline
1997.7
 Apr. 2005
 F uncertainty < few%
TIPS Meeting – 19 October 2006
15
Updated Flux Calibration
of Prime Modes
• Multiple observations of 3 different standard stars
BD+75D325, BD+28D4211 & G191B2B at MO = (0,0)
< few % uncertainties introduced by:
averaging over different observation epochs (≠TDS and B shift)
use of standard stars with a lot of absorption lines
BD+75D325 & BD+28D4211
• Switched to a calibration that only averages over
exposures of the most suitable standard star
G191B2B, taken at the same time with MO ≠ (0,0)
• Same PHT file with new BZS correction
TIPS Meeting – 19 October 2006
16
On-Orbit Flux Calibration
of Secondary Modes
• Secondary Modes almost used
as often as Prime Modes
• Absolute F calibration of Secondary
Modes still based on pre-launch data
• TDS applied, but not BZS correction
TIPS Meeting – 19 October 2006
17
On-Orbit Flux Calibration
of Secondary Modes
• On-board data collected for G191B2B with MO≠(0,0)
All Prime & Secondary
Modes (Sep. 2001)
old PHT file
new PHT file
• On-orbit sensitivities
BZS correction
secondary modes
new PHT files
 relative F uncertainty
from ~ 30% to < 1-2 %
TIPS Meeting – 19 October 2006
and
introduced for
with
2003.4
HD158643 (pre-MS ) – E140H (1380)
18
ISRs in Preparation
“Time-Dependent Sensitivity of STIS Echelle Medium
and High-Resolution Modes” A. Aloisi
“Blaze Shift Correction for STIS Echelle Prime and
Secondary Modes”
A. Aloisi
“On-Board Sensitivity Calibration of STIS Echelle Secondary
Modes (and Revision of Prime Mode Sensitivities)”
A. Aloisi, R. Bohlin, & J. Kim Quijano
TIPS Meeting – 19 October 2006
19
TIPS-JIM Meeting
19 October 2006, 10am, Auditorium
1.
The Final Flux Calibration of the STIS Echelle
Alessandra Aloisi
Modes
2.
ACS Status Update
Ken Sembach
3.
HST Instrument Capabilities after SM4
Jerry Kriss
Next TIPS Meeting will be held on 16 November 2006.
ACS Status Update
STScI TIPS Meeting
19-October-2006
Ken Sembach
43
ACS/HRC Timeline
•
ACS Suspended Saturday, September 23, 2006
• Telemetry showed that the HRC ASPC2 board was missing its
+35V input
• This voltage is needed for CCD bias level and reset drain
operation.
• Loss of +35V believed to leave HRC unusable
• Lots of discussion about this - more on this if you want to know
• An ACS-free SMS was implemented the following week
• Thanks to scheduling team, PCs, and NICMOS Team for getting as much
science as possible planned for that week
• ARB was convened to determine cause of suspension
• Failure of A2/A3 contacts to close in K1 relay
• Solder joints from K1 relay to ASPC2 board
• Problem is unrelated to June 2006 Side-1 electronics failure
44
CEB Power Switching
All relays independent and switched by individual RIU commands
LVPS1
ASPC1
(video)
MEB2
ASPC2
(video)
Clock1
(CCD control)
MEB1
LVPS2
Clock2
(CCD control)
Timing
(main control)
CEB
All boards are needed for operation of the entire detector.
Simplified – multiple diode
busses in hardware
Legend:
5V only
45
K1 relay
ASPC2
(C,D half of CCD)
ASPC1
(A,B half of CCD)
46
Relay Operation
Pushes Telemetry Pole
D
C
Glass Beads:
Used to push on
movable contact
Glass Beads:
Used to push on
movable contact
Rocker Assembly
A
B
Pushes +35V Pole
Pivot point
Contact made by
spring action of
movable center arm to
relaxed state
Shown in LVPS2
Selection Position (X coil
commanded last)
(LVPS2 A3
+35V)
D1
A2
(LVPS1 A1
+35V)
D2
Contact made by
pushing action of
rocker arm
D3
47
ACS/HRC Timeline
•
WFC returned to service on October 1, 2006
• Not affected by HRC relay issue
•
HRC returned to service on October 15, 2006
• Single toggle of relay restored electrical contact
• ARB has recommended never toggling problematic relay again
•
SBC is functional but powered off
• ARB is examining options for bringing SBC on line
• Previous use of SBC required toggle of problematic HRC relay to allow HRC to
be turned off for SBC observations
• Power / current / thermal issues are being worked
• Option 1: CCDs and SBC on simultaneously
• Option 2: CCDs off when SBC is on
48
ACS/HRC Post Recovery Performance
•
Internal bias and dark exposures from ACS Daily Monitor
Program (10758) have been examined
•
•
•
•
•
Data were obtained after the ACS anneal on October 16, 2006
Data were read out through the C amplifier
Both GAIN=2 and GAIN=4 data were obtained.
Readnoise and dark current track historical averages
Bias levels are slightly higher than historical average, but this is
expected
• Bias level typically higher for a short time (few hours) after anneals
• Bias level is expected to drop back to historical average by next set of
observations
• No impact on science data or performance
•
Data look perfectly normal, with no anomalies noted (Marco
Sirianni)
49
ACS/HRC Bias Images (16-Oct-2006)
The two bias images above were obtained after resumption of HRC operations.
Both were obtained with GAIN= 2 after the ACS anneal. These bias images look
perfectly normal. The data were read out through the C amplifier.
50
ACS/HRC Readnoise and Bias Level (GAIN=2)
The above plots show the readnoise (left) and bias level (right) for historical
Side-2 data [blue points] and post-recovery data [yellow points]. The solid red
lines are the historical averages, and the dotted red lines indicate the historical
±3 sigma excursions.
51
ACS/HRC Readnoise and Bias Level (GAIN=4)
The above plots show the readnoise (left) and bias level (right) for historical
Side-2 data [blue points] and post-recovery data [yellow points]. The solid red
lines are the historical averages, and the dotted red lines indicate the historical
±3 sigma excursions.
52
ACS/HRC Post Recovery Performance
•
First post-recovery science data were obtained October 18, 2006
• G800L observations of SN1987A (Kirshner SAINTs program;
GO10867)
• Historical data were pulled for comparison
• Exposures dithered to remove cosmic rays
•
Data look perfectly normal, with no anomalies noted (Ron
Gilliland)
53
ACS/HRC Science Images (18-Oct-2006)
54
TIPS-JIM Meeting
19 October 2006, 10am, Auditorium
1.
The Final Flux Calibration of the STIS Echelle
Alessandra Aloisi
Modes
2.
ACS Status Update
Ken Sembach
3.
HST Instrument Capabilities after SM4
Jerry Kriss
Next TIPS Meeting will be held on 16 November 2006.
HST Instrument Capabilities after SM4
Jerry Kriss
STUC Meeting, October 2006
With input from Tom Brown (WFC3),
Ron Gilliland (ACS),
Diane Karakla (User Support),
Tony Keyes (COS),
Keith Noll & Roelof de Jong (NICMOS),
Charles Proffitt (STIS)
10/18/2006
Outline


The instrument complement after SM4
Summary of instrument modes and capabilities





Comparison of similar capabilities
Unique capabilities
Past usage history, and expected usage after SM4
Suggested levels of support
Instrument mode prioritization
STUC Meeting, October 2006
Jerry Kriss
/31
Instrument Complement after SM4

COS


WFC3





High-resolution Far-UV and Near-UV spectroscopy
High-spatial resolution UV and Visible spectroscopy
NICMOS




Wide-field Visible imaging
High-resolution Near-UV and Far-UV imaging
Near-UV and Visible Coronagraphy and Polarimetry
STIS


Wide-field Near-UV, Visible, and Near-IR imaging
ACS


High sensitivity, moderate & low resolution Far-UV and Near-UV
spectroscopy
Thermal-IR imaging (λ>1.8 µm)
High-resolution IR imaging
IR coronagraphy and polarimetry
FGS

Precision astrometry
STUC Meeting, October 2006
Jerry Kriss
/31
Standard Support for HST Instruments

Calibration




Data Processing


Pipeline improvements made as needed
Documentation




Regular monitoring observations
Calibration reference files continuously updated
Calibration plans updated each cycle
Instrument Science Reports (ISRs)
User Handbooks
Data Handbooks
User Support



Contact scientist program
Phase 2 proposal reviews
Help desk
STUC Meeting, October 2006
Jerry Kriss
/31
Suggested Instrument Support Categories
1. New instrument
•
•
Full SMOV activation and calibration of WFC3 and COS.
Full characterization and regular calibration of all WFC3 and COS modes.
2. Standard support
•
•
•
Unique capabilities
Clear usage request in approved proposals.
Full calibration. Update reference files regularly. Write ISRs on calibration.
3. Minimal support
•
•
•
•
Secondary or backup modes
Minimal expected proposal pressure to use these modes
Basic calibration observations.
Calibrations checked, but not fully analyzed.
4. No support (but available) (shared risk)
•
•
•
•
Secondary, backup, and “available-but-unsupported” modes
For these modes, no SNAPS or ToOs that require bright-object checking.
No expected proposal pressure to use these modes
If observations proposed, then calibration observations must also be proposed
and analyzed by users.
STUC Meeting, October 2006
Jerry Kriss
/31
COS Capabilities



The Cosmic Origins Spectrograph (COS) is uniquely suited to
address particular scientific questions via greatly enhanced low and
moderate resolution FUV capabilities for point sources.
COS exploits an element of “performance space” by providing >10x
the FUV throughput of STIS and up to 70x STIS observing speed.
COS employs an advanced FUV detector with significantly lower
backgrounds and routinely utilizes TIME-TAG and event pulse-height
recording.
FUV Detector:
• Two 16k x 1k delay line MCPs
• TIME-TAG; pulse-heights
• 3 gratings
• 300-800 Ǻ spectral coverage
• R=3000; 20,000
STUC Meeting, October 2006
NUV Detector :
• 1k x 1k MAMA
• TIME-TAG
• 4 gratings, 1 Mirror and filter
• 100-800 Ǻ spectral coverage
• R=2000; 20,000
Jerry Kriss
/31
COS Discovery Potential
10-15
S
O
C
QSO (Reionization)
Unexplored discovery space
QSO (z ~ 0.5)
10-14
10-13
Starburst galaxies
S
STI
Brightest QSO (3C 273)
Discovery potential
Fλ (erg cm-2 sec-1 Å-1)
10-16
Increasing # of objects
Limiting flux as function of exposure time to reach S/N=10
with spectral resolution λ/Δλ=20,000 at 1600 Å
OB stars in the Magellanic Clouds
0
20
STUC Meeting, October 2006
40
60
Texp (orbits)
80
100
Jerry Kriss
/31
COS FUV Spectroscopic Capabilities
FUV M Mode Limiting Flux for S/N=10 in 3600 sec (R~10,000 (0.15 _) binning)
STIS E140M
1.00E-13
R=45,000
-sec
-1
-1
-_
Ǻ )
1.00E-12
Flux (erg-cm
-2
STIS G140M
R~11,000-17,000
1.00E-14
COS G130M
R~20,000-24,000
COS G160M
R~20,000-24,000
1.00E-15
1000
STUC Meeting, October 2006
1100
1200
1300
1400
1500
1600
Wavelength
Jerry Kriss (_)
1700
1800
1900
2000
2100
/31
COS NUV Spectroscopic Capabilities
NUV M Mode Limiting Flux for S/N=10 in 3600 sec (R~10,000 (0.24 _) binning)
1.00E-12
Flux (erg-cm
-2
-1
-sec - 1 -_
Ǻ )
1.00E-13
STIS E230M
R=30,000
1.00E-14
STIS G230M
R~9000-17,000
1.00E-15
COS G285M
R~20,000-24,000
COS G225M
R~20,000-24,000
COS G185M
R~16,000-20,000
1.00E-16
1600
STUC Meeting, October 2006
1800
2000
2200
2400
2600
Jerry
Kriss (_)
Wavelength
2800
3000
3200
/31
COS UV Spectroscopic Capabilities
COS vs STIS in the UV
COS/FUV
COS/NUV
STIS/FUV
STIS/NUV
Spectral coverage (Ǻ)
1150-1775(M) 1700-3200
1230-2050(L)
1150-1700
1600-3200
Effective Area
1300 (FUV), 2500
(NUV)
2800 (M)
2400 (L)
400 (M)
1700 (L)
350 (M)
900 (L)
Resolution (λ/Δλ)
H
N/A
M 20000-24000
2400-3500
L
900 (M)
750 (L)
N/A
16000-24000
1500-2800
110000
110000
10000-40000
1000
110000
110000
10,000-30000
500
Number of pixels
along dispersion
32768
1024
1024 (2048)
1024 (2048)
Background (cts/resel)
4.3 e-5
1.9 e-3
350e-5
17e-3
Background equivalent
Fλ (erg cm-2 sec-1 Ǻ-1)
0.5-8 e-18
1.3-3.8 e-16
20e-18
13e-16
STUC Meeting, October 2006
Jerry Kriss
/31
WFC3 Capabilities



The Wide Field Camera 3 (WFC3) will provide wide-field
imaging with continuous spectral coverage from the ultraviolet
through the infrared.
WFC3 dramatically increases both the survey power and the
panchromatic science of HST.
WFC3 will provide advanced detectors with less radiation
damage (hot pixels, charge transfer inefficiency, etc.).
UVIS Channel:
• Two 2k x 4k CCDs
• 160”x160” field of view
• 62 filters, 1 grism
• 200-1000 nm bandpass
• 0.039” pixels
STUC Meeting, October 2006
IR Channel:
• 1k x 1k HgCdTe array
• 135”x135” field of view
• 15 filters, 2 grisms
• 800-1700 nm bandpass
• 0.132” pixels
Jerry Kriss
/31
COS/NUV
STUC Meeting, October 2006
Jerry Kriss
/31
STUC Meeting, October 2006
Jerry Kriss
/31
WFC3 Capabilities
WFC3 vs ACS in the optical (380 nm - 1000 nm)
WFC3/UVIS
ACS/WFC
ACS/HRC
FOV area
(arcsec2)
25600
40804
754
Broadband
throughput @ V, I
0.25, 0.14
0.35, 0.36
0.23, 0.16
Pixel scale (arcsec)
0.039
0.049
0.027
Number of pixels
4k x 4k
4k x 4k
1k x 1k
Read noise
3 e-
5 e-
4.7 e-
Number of filters
49
27
21*
(32 full-field, 17 quad)
(12 full-field, 15 ramp)
(13 full-field, 3 pol., 5 ramp)
*Some of these cover only the ACS/HRC FOV but can in principle be used in the ACS/WFC.
STUC Meeting, October 2006
Jerry Kriss
/31
WFC3 Capabilities
WFC3 / ACS / COS in the near-UV (200 nm - 330 nm)
WFC3/UVIS
ACS/HRC
COS/NUV
FOV area
(arcsec2)
25600
754
12.5
4.90 (un-vignetted)
Broadband
throughput
@ 230, 330 nm
0.07, 0.18
0.03, 0.10
0.07, 0.02
Pixel scale (arcsec)
0.039
0.027
.024
Number of pixels
4k x 4k
1k x 1k
166 (diameter)
100 (un-vignetted)
Read noise
3 e-
4.7 e-
none
(@ 230, 320 nm)
(dark equiv flux: ~5e-19 )
Number of filters
13
6
1
(10 full-field, 3 quad)
(3 full-field, 3 UV pol.*)
(broad-band, 1700-3200 Å.)
*These polarizers are optimized for the UV and the ACS/HRC FOV but can in principle be used with the ACS/WFC in the optical.
STUC Meeting, October 2006
Jerry Kriss
/31
WFC3 Capabilities
WFC3 vs NICMOS in the near-IR (800 nm - 2500 nm)
WFC3/IR
NIC3
NIC2
NIC1
FOV area
(arcsec2)
18225
2621
369
121
Broadband
throughput
@ 1.1, 1.6 microns
0.29, 0.33 0.13, 0.20 0.14, 0.20
Pixel scale (arcsec) 0.132
0.200
Number of pixels
1k x 1k
256 x 256 256 x 256
256 x 256
Eff. read noise
14
22
20
22
number of filters
15
16
19
19
(16 standard, 3 pol.)
(16 standard, 3 pol.)
STUC Meeting, October 2006
Jerry Kriss
0.075
0.12, 0.18
0.043
/31
WFC3 Capabilities
WFC3 UVIS Filters - Broadband
Name
F200LP
F218W
F225W
F275W
G280
F300X
F336W
F350LP
F390W
F438W
F475W
F475X
F555W
F600LP
F606W
F625W
F775W
F814W
F850LP
Description
Clear
ISM feature UV Wide
UV Wide
Grism
Extremely wide UV
U, Stromgren u
Long Pass Washington C
WFPC2 B SDSS g’
Extremely wide blue
WFPC2 V Long Pass WFPC2 Wide V
SDSS r’
SDSS i’
WFPC2 Wide I
SDSS z’
Wavelength (nm)
pivot
width
569
800
218
35
234
55
272
48
278
185
283
75
336
55
681
450
390
95
431
68
476
149
492
220
531
160
843
400
591
230
625
158
773
149
830
254
976
150
Nearest ACS Equivalent
HRC/F220W
HRC/F250W
HRC/PR200L
HRC/F330W
F435W (WFC & HRC)
F475W (WFC & HRC)
F555W (WFC & HRC)
F606W (WFC & HRC)
F625W (WFC & HRC)
F775W (WFC & HRC)
F814W (WFC & HRC)
F850LP (WFC & HRC)
⇒Fully covers the ACS complement, and then some.
STUC Meeting, October 2006
Jerry Kriss
/31
WFC3 Capabilities
WFC3 UVIS Filters - Medium and Narrow
Name
F390M
F410M
F467M
F547M
F621M
F689M
F763M
F845M
Description
CaII continuum
Stromgren v Stromgren b Stromgren y 11% passband
11% passband
11% passband
11% passband
Wavelength (nm)
pivot
width
389
21
411
18
468
22
544
71
622
63
689
71
764
80
847
89
F280N
F343N
F373N
F395N
F469N
F487N
F502N
F631N
F645N
F656N
F657N
F658N
F665N
F673N
F680N
F953N
MgII 2795,2802
[NeV] 3426 [OII] 3726/3729
CaII H&K
HeII 4686
Hβ 4861
[OIII] 5007 [OI] 6300
Continuum Hα 6563
Wide Hα+[NII]
[NII] 6583
z (Hα+[NII]) [SII] 6717,6731
z (Hα+[NII]) [SIII] 9532 233
344
373
395
469
487
501
630
645
656
657
659
665
676
688
953
STUC Meeting, October 2006
3
14
4
7
4
5
6
4
9
1
10
2
11
10
32
8
Jerry Kriss
Nearest ACS Equivalent
FR459M (ramp; WFC & HRC)
F550M (WFC & HRC)
WFC/FR647M (ramp)
-
HRC/F344N
FR388N (ramp; WFC & HRC)
WFC/FR462N (ramp)
F502N (WFC & HRC)
FR656N (ramp; WFC & HRC)
F658N (WFC & HRC)
F660N (WFC & HRC)
-
/31
WFC3 Capabilities
WFC3 UVIS Filters - Quad
Name
FQ232N
FQ243N
FQ378N
FQ387N
FQ422M
FQ436N
FQ437N
FQ492N
FQ508N
FQ575N
FQ619N
FQ634N
FQ672N
FQ674N
FQ727N
FQ750N
FQ889N
FQ906N
FQ924N
FQ937N
Description
CII] 2326
[NeIV] 2425 z ([OII] 3727) [NeIII] 3869 Continuum Hγ+[OIII] 4363
[OIII] 4363 z (Hβ)
z ([OIII] 5007)509
[NII] 5755
CH4 6194 6194 continuum
[SII] 6717
[SII] 6731
CH4 7270 7270 continuum
CH4 25/km-agt
CH4 2.5/km-agt
CH4 0.25/km-agt
CH4 0.025/km-agt
STUC Meeting, October 2006
Wavelength (nm)
pivot
width
233
3
242
3
379
9
387
2
422
11
437
4
437
2
493
10
12
576
1
620
6
635
7
672
1
673
1
727
6
750
7
889
9
906
9
925
9
937
9
Jerry Kriss
Nearest ACS Equivalent
WFC/FR423N (ramp)
FR505N (ramp; WFC & HRC)
WFC/FR601N (ramp)
WFC/FR716N (ramp)
WFC/FR782N (ramp)
HRC/F892N
FR914M (ramp; WFC & HRC)
WFC/FR931N (ramp)
/31
WFC3 Capabilities
WFC3 IR Filters
Name
F098M
G102
F105W
F110W
F125W
F126N
F127M
F128N
F130N
F132N
F139M
F140W
G141
F153M
F160W
F164N
F167N
Description
Blue grism reference
Blue grism (high res.)
Wide Y
Wide YJ
Wide J
[FeII]
Water/CH4 continuum
Paschen β Paschen β continuum
Paschen β redshifted
Water/CH4 line
JH gap
Red grism (low res.)
H20 & NH3 Blue-shifted H
[FeII]
[FeII] continuum
STUC Meeting, October 2006
Wavelength (nm)
pivot
width
983
169
1025
250
1049
292
1141
503
1246
302
1258
11
1274
69
1283
14
1301
13
1319
13
1384
65
1392
399
1410
600
1533
69
1541
288
1645
17
1667
17
Jerry Kriss
Nearest NICMOS Equivalent
NIC1/F090M
NIC3/G096
F110W (NIC1, NIC2, & NIC3)
NIC1/F145M
NIC3/F150W & NIC1/F140W
NIC3/G141
NIC1/F145M
F160W (NIC1, NIC2, & NIC3)
NIC3/F164N & NIC1/F164N
NIC3/F166N & NIC1/F166N
/31
Unique ACS Capabilities




High-throughput, wide-field Optical imaging
High-resolution Far-UV, Near-UV and Optical imaging
UV and Optical Coronagraphy
UV and Optical Polarimetry
STUC Meeting, October 2006
Jerry Kriss
/31
Unique ACS Filters


G800L -- grism for both WFC and HRC that provides R=100
spectroscopy over 5500-11000A. With the WFC this will
continue to provide a quite unique capability with excellent
response in the red.
Ramp filters which cover nearly all of the optical with either 2%
or 9% widths and a 70x70" FOV.




These are used by the community, but not heavily so.
Our calibrations have been minimal, and there is currently a caloutsourcing program for ramp flats.
Many wavelength settings that might be used would be covered by
specific WFC3 filters.
SBC/UV filters have no WFC3 counterparts:
F122M, F115LP, F125LP, F140LP, F150LP, F165LP
and PR110L and PR130L.
STUC Meeting, October 2006
Jerry Kriss
/31
Unique NICMOS Capabilities




Thermal IR Imaging at λ>1.8 µm.
High-resolution IR imaging
IR Coronagraphy
IR Polarimetry
STUC Meeting, October 2006
Jerry Kriss
/31
Unique NICMOS filters <1.8 micron
Name
F090M /NIC1
F095N /NIC1 F097N /NIC1 F108N /NIC1/3
F113N /NIC1/3
F145M /NIC1
F165M /NIC1/2
F170M /NIC1
F171M /NIC2
Description
[S III]
[S III] continuum
He I
He I continuum
Water
Wavelength (nm)
pivot
width
903
56
954
4
972
4
1082
4
1130
5
1455
59
1648
59
1706
60
1721
25
Nearest WFC3 Equivalent
F098M Blue grism reference
F139M Water/CH4 & F153M H20 & NH3
(No polarimetry filters listed)
WFC3 equivalents
Name
F098M
F139M
F153M
Description
Blue grism reference
Water/CH4 line
H20 & NH3 STUC Meeting, October 2006
Wavelength (nm)
pivot
width
983
169
1384
65
1533
69
Jerry Kriss
Nearest NICMOS Equivalent
NIC1/F090M
NIC1/F145M
NIC1/F145M
/31
Unique STIS Capabilities





Echelle modes have higher spectral resolution (up to
200,000 vs 24,000 maximum for COS).
Long slits can give high-spatial-resolution optical and UV
spectra even in crowded fields.
STIS NUV imaging is solar blind. (Dark rate after SM4 will
be reduced due to additional passive cooling.)
STIS time-tag has higher resolution (125 µs vs 32 ms for
COS).
STIS can observe objects too bright for COS. (COS ND
aperture degrades resolution by 3-5x.)
STUC Meeting, October 2006
Jerry Kriss
/31
HST Instrument Usage, Historical & Projected
Detector/Mode
Cycle 14&15 Est. Cycle 17* Comment
ACS
65%
33.3%
Wide field, high-res, pol., cor.
NICMOS
26%
4.3%
High-res, pol., cor., λ>1.8 µm
STIS
23%**
12.1%
Unique spatial & spectral resolution
FGS
1%
1%
Precision astrometry
COS
---
16%
High UV throughput
WFC3
---
33.3%
**Cycle 12&13
STUC Meeting, October 2006
High panchromatic throughput & FOV
*Biagetti et al. 2003
Jerry Kriss
/31
Imaging Instrument Historical Usage (by Exposure Time*)
Detector/Mode
Cycle 14&15
Est. Cycle 17
Comment
ACS/WFC
50.6%
18.3%
WFC3 surveys will take over
ACS/HRC
10.4%
3%
Will be mostly high-res + Cor.
ACS/SBC
4.2%
2%
Unique mode
NIC1
1.6%
1%
Will be mostly high-res
NIC2
8.6%
1%
Will be mostly high-res
NIC1,2 Polarization
0.4%
0.5%
Unique mode
NIC2 Coronagraphy
1.7%
1.5%
Unique mode
NIC3 (λ<1.8 µm)
14.0%
0%
NIC3 (λ>1.8 µm)
0.3%
0.3%
STIS/FUV-IMG
0.2%**
0%
Superceded by ACS/SBC
STIS/NUV-IMG
0.1%**
0%
Superceded by ACS/HRC
STIS/CCD-IMG
0.1%**
0.1%
1.1%
1%
FGS
STUC Meeting, October 2006
**Cycle 12&13.
Jerry Kriss
Superceded by WFC3
Unique mode
Mostly Target Acq Verification
Unique mode & science
*GO/GTO/DD programs at Phase 2 ingest.
/31
Spectroscopic Mode Historical Usage (by Exposure Time*)
Detector/Mode
Cycle 12&13
Est. Cycle 17
Comment
STIS/UV-*L,*M
8.0%
1%
Spatial resolution is unique
STIS/Echelle *M
5.6%
3%
R~40,000 is unique
STIS/Echelle *H
2.7%
3%
R~100,000 is unique
STIS/CCD-*L,*M
6.1%
5%
Spatial resolution is unique
STIS/NUV-Prism
0.5%
0%
Superceded by SBC & WFC3
*GO/GTO/DD programs at Phase 2 ingest.
STUC Meeting, October 2006
Jerry Kriss
/31
Projected Usage for WFC3 and COS
Detector/Mode
Est. Cycle 17*
COS Low Res
2%
Used only for the faintest objects
COS Med Res
14%
Supercedes most STIS UV
WFC3 UVIS
20%
Panchromatic surveys
WFC3 IR
13.3%
Comment
Supercedes NIC3; pan. surveys
*Biagetti et al. 2003
STUC Meeting, October 2006
Jerry Kriss
/31
Suggested Instrument Support Categories
1. New instrument
•
•
Full SMOV activation and calibration of WFC3 and COS.
Full characterization and regular calibration of all WFC3 and COS modes.
2. Standard support
•
•
•
Unique capabilities
Clear usage request in approved proposals.
Full calibration. Update reference files regularly. Write ISRs on calibration.
3. Minimal support
•
•
•
•
Secondary or backup modes
Minimal expected proposal pressure to use these modes
Basic calibration observations.
Calibrations checked, but not fully analyzed.
4. No support (but available) (shared risk)
•
•
•
•
Secondary, backup, and “available-but-unsupported” modes
No SNAPS or ToOs that require bright-object checking.
No expected proposal pressure to use these modes
If observations proposed, then calibration observations must also be proposed
and analyzed by users.
STUC Meeting, October 2006
Jerry Kriss
/31
Instrument Support Classification
1. New instrument
•
COS, WFC3
2. Standard support
•
•
•
•
ACS/WFC, ACS/SBC, ACS/HRC
STIS/E*H, STIS/E*M, STIS/CCD*L,*M
NIC2, NIC2/COR*, NIC3/(λ>1.8 µm)
FGS*
3. Minimal support
•
•
STIS/UV*L,*M, STIS/NUV-IMG, STIS/NUV-Prism*,
STIS/COR*
NIC1, NIC1,2/POL*
4. No support (but available)
•
STIS/FUV-IMG, STIS/CCD-IMG
STUC Meeting, October 2006
Jerry Kriss
*candidates for outsourcing
/31
Back-up slides follow
STUC Meeting, October 2006
Jerry Kriss
/31
STIS after SM4


STIS NUV dark rate had been about 0.0012 counts/
pixel/s; ~ 4X COS dark rate, but …
STIS MAMAs will get passive cooling added during
SM4.


Should maintain or even reduce STIS MAMA dark rate,
despite expected increase in aft-shroud temperatures.
Will need to check alignment and calibrations, but
expect most calibrations to need only minor
adjustments…
STUC Meeting, October 2006
Jerry Kriss
/31
STIS Echelle Modes




In cycle 12 & 13, Echelle H modes 3.2% of initially
approved GO expo time; Echelle M modes at 7.1%.
Expect ~4-5% total usage after SM4.
E140H and E230H spectral resolution is normally
~110,000, but can be up to 200,000 when using
smallest 0.1” × 0.03” aperture.
E140M (R=45,000) and E230M (R=30,000) resolution
modestly better than COS m-modes 16,000 – 24,000.
STUC Meeting, October 2006
Jerry Kriss
/31
STIS CCD Spectral Modes






In Cy 12 & 13 these modes averaged 7.5% of initially
approved GO exposure time.
No bright object constraints
0.05” spatial resolution of extended objects
Only long slit optical spectroscopy on HST
Aperture bars allow coronographic spectroscopy
Much higher resolution than slitless prisms and grisms
available with other HST detectors
STUC Meeting, October 2006
Jerry Kriss
/31
STIS 1st Order UV Modes




In Cy 12 & 13 these modes (G140L, G230L, G140M,
G230M) received 10% of expo time.
Long slits allow 0.025” spatial resolution spectra of
extended objects.
G*M modes have very short per-tilt λ coverage (55 Å
G140M, 90 Å for G230M).
G*L modes used to perform sensitivity monitoring for
most MAMA modes, so some calibration must continue.
STUC Meeting, October 2006
Jerry Kriss
/31
STIS NUV-PRISM



Averaged 0.6% of approved GO exposure time in
cycles 12 and 13.
Provides slitless multi-object spectroscopy covering
both NUV & FUV (1150 –3620 Å).
Throughput smaller than overlapping SBC or HRC
prism modes.
STUC Meeting, October 2006
Jerry Kriss
/31
STIS Coronagraphic Imaging



Last used in Cycle 11.
Suppression of light in PSF wings and PSF stability
inferior to HRC coronagraph.
Only supports unfiltered coronagraphic imaging.


Very broad band pass results in large color effects on
PSF, making subtraction of standard PSFs difficult
Narrowest 0.6” wedge position significantly smaller
than ACS small spot (1.8“), so may be preferred for
imaging very close material.
STUC Meeting, October 2006
Jerry Kriss
/31
STIS NUV Imaging


Only 0.1% of GO exposure time in Cy 12 & 13
Advantages versus HRC or WFC3 UV modes for observing
very faint targets

Much lower dark current

No read noise
Broader filters.


Disadvantages compared to HRC/WFC3



STIS PSF wider and less stable
STIS MAMA will often have bright object concerns
Narrower filters give HRC/WFC3 smaller color terms
STUC Meeting, October 2006
Jerry Kriss
/31
STIS FUV Imaging




Received 0.3% of exposure time in cy 12 &13
Less sensitive than comparable SBC modes
Fewer filter choices than SBC
Time-tag available for STIS FUV imaging, but not SBC imaging
STUC Meeting, October 2006
Jerry Kriss
/31
STIS CCD Imaging






About 0.9% of exposure time in C12/13. (Mostly
target confirmation images.)
Throughput inferior to broad band WFC3 and ACS/
WFC modes.
Only two very broad and two narrow filters (plus
little used ND filters).
PSF less stable than newer detectors
Broad filters give large color terms to photometry
and PSFs.
CTI much larger than for newer CCDs
STUC Meeting, October 2006
Jerry Kriss
/31
ACS Use (by Exposure Time in Ksec)
10/18/2006
Detector
Cycle 15
Cycle 14
ACS Totals
6144 (55.0%)**
7310 (66.2%) **
WFC *
77.6%
76.6%
HRC
11.2%
20.6%
SBC
11.2%
2.8%
WFC SNAPs
9.7%
24.5%
HRC SNAPs
5.5%
17.1%
POL filters
1.1%
1.7%
RAMP filters
0.6%
G800L
1.2%
0
7.2%
GO,GO/DD,GTO - prime and parallel
* Includes 5-10% coord. parallel usage
** Percent of all GO/GTO obs in cycle
NIC Instrument Use (by Exposure Time in Ksec)
Detector/Mode
Cycle 15
Cycle 14
NIC Totals
3239 (29.0 %)**
2194 (19.9%) **
NIC1
10.1%
1.5%
NIC2
42.7%
23.8%
NIC3
47.1%
74.5%
SNAPs
1.0%
0
NIC2/Coron
6.3%
7.7%
NIC1+2/Pol
2.5%
0.7%
NIC3/K-band
(>F175W)
2.8%
4.4%
GO,GO/DD,GTO - prime and parallel
** Percent of all proposed GO/GTO obs
STUC Meeting, October 2006
Jerry Kriss
/31
Relative Usage of Unique NIC Filters
(by Exp Time in Ksec)
Detector/Mode
Cycle 15
Cycle 14
NIC Totals
3239 (29.0 %)**
2194 (19.9%) **
Nic1/F095N
0
0
Nic1/F097N
0
0
Nic1+3/F108N
0.5%
0.1%
Nic1+3/F113N
0
0
Nic1/F145M
0
1.4%
Nic1+2/F165M
0
0
Nic1/F170M
0
1.4%
Nic2/F171M
0
0.1%
GO,GO/DD,GTO - prime and parallel
** Percent of all proposed GO/GTO obs
STUC Meeting, October 2006
Jerry Kriss
/31
WPC2 Use (by exposure time)
Total WFPC2
Cycle 15
Cycle 14
1728 (15.5%) *
1344 (12.2%) *
Primary
3.9%
5.6%
Parallel
96.1%
94.4%
0
0.3%
SNAPs
FGS Use (by exposure time)
Cycle 15
Total FGS
66 (0.5%) *
Cycle 14
186 (1.7%) *
GO,GO/DD,GTO - prime and parallel
* Value in Ksec and given in percent of all proposed
GO/GTO obs
STUC Meeting, October 2006
Jerry Kriss
/31
STIS Usage of Unique Modes
(by Exp Time)
STIS Mode
Cycle 12+13*
Echelle Hi-res
3.2%
Echelle Med-res
7.1%
CCD/Spectral
7.5%
G140L/M, G230L/M
10.0%
NUV Prism
0.6%
Coron
0
NUV Imaging
0.1%
FUV Imaging
0.3%
CCD Imaging
0.9%
STUC Meeting, October 2006
Jerry Kriss
GO,GO/DD,GTO prime and parallel
Percent of all
proposed GO/GTO obs
/31
TIPS-JIM Meeting
19 October 2006, 10am, Auditorium
1.
The Final Flux Calibration of the STIS Echelle
Alessandra Aloisi
Modes
2.
ACS Status Update
Ken Sembach
3.
HST Instrument Capabilities after SM4
Jerry Kriss
Next TIPS Meeting will be held on 16 November 2006.