TIPS/JIM
October 18, 2012
Agenda:
INS Division News (Margaret Meixner)
COS FUV Lifetime Move (Rachel Osten) !
VoIP Update: New/Expanded Voice, Collaboration and Mobility Services for STScI
(Dave Liska) !
A Preliminary Cycle 1 Calibration Plan for the JWST Science Instruments
(James Muzerolle) !
Next TIPS/JIM: December 20, 2012

INS  News
TIP/JIM  Meeting
October  18,  2012
You  have  probably  already  heard  this  news  via  email  from  Danny  himself.      Danny
Lennon  has  accepted  the  position  as  Head  of  Science  Operations  at  ESAC,  the  ESA
Madrid  Facility.    We  will  miss  him  when  he  leaves.    You  might  be  thinking  he  has   left  already  because  I  am  leading  TIPS  today.      But  he  is  not  gone  yet  –  just  on   travel  now.    When  he  does  take  up  his  new  position,  he  will  be  back  as  part  of  his   new  role  and  for  science  research  projects  that  he  has  started  with  many  of  you.

TIPS/JIM
October 18, 2012
Agenda:
INS Division News (Margaret Meixner)
COS FUV Lifetime Move (Rachel Osten) !
VoIP Update: New/Expanded Voice, Collaboration and Mobility Services for STScI
(Dave Liska) !
A Preliminary Cycle 1 Calibration Plan for the JWST Science Instruments
(James Muzerolle) !
Next TIPS/JIM: December 20, 2012

Rachel Osten with input from: A. Aloisi, C. Oliveira, G. Kriss, D.
Sahnow, C. Proffitt, K. A. Bostroem, S. Penton, S.
Osterman, T. Wheeler, P. Sonnentrucker, J. Roman-Duval,
D. Massa, J. Debes, E. Elliott, J. Ely
TIPS talk
Oct. 18

• gain sag in the FUV detector limits the amount of charge that can be extracted from any position on the detector
• holes due to Lyman alpha airglow, plus sag in continuum from normal usage
• previous estimates were that by Sept. 2012 part of the continuum in FUVB will be lost (unrecoverable) due to gain sag; goal was to move before then
• lifetime move = change of location on detector where routinely acquired spectra fall
• brainstorming retreat on Dec. 9, 2011 led to adoption of (0,+3.5”) in (disp., cross disp.) as the next lifetime position (~35 pixels away from original lifetime position) -- Aloisi TIPS presentation on Nov. 17, 2011 + Oliveira TIPS presentation on Jan. 19, 2012
• initial plan (OP-01) was to move lifetime positions ~ every year.

programs in I. done once; programs in II. and III. repeated with each lifetime move
define lifetime positions, select second lifetime position
Oliveira Jan. 2012
TIPS talk required to enable science at new lifetime position support science at new lifetime position ** start of operations at new lifetime position
** does not include routine calibration activities (e.g. darks) requirements were drafted, based on SMOV4+on-orbit experience
(Osten et al. 2012 TIR): “spot-check” approach
3

Activity/PID Title
FENA1/12793
FENA2/12795
FENA3/12796
FENA4/12797
FCAL1
FCAL2/12805
FCAL3/12806
FCAL4/12807
FUV HV sweep
Orbits
Allocated
13In (3In)*
FUV aperture, spectrum placement 3Ex
FUV focus verification 6Ex (3Ex)*
FUV target acquisition parameter update
11Ex
Total for enabling
FUV λ scales
FUV resolution
FUV sensitivity & flat fields
FUV BOA operations
20Ex 13In
0Ex (2Ex)*
4Ex (4Ex)*
25Ex(4Ex)*
1Ex
Total for calibration 30Ex (10Ex)*
4
*contingency orbits

Activity/PID Title
FENA1/12793
FENA2/12795
FENA3/12796
FENA4/12797
FCAL1
FCAL2/12805
FCAL3/12806
FCAL4/12807
FUV HV sweep
Orbits
Allocated
13In (3In)*
Orbits
Executed
16In
FUV aperture, spectrum placement 3Ex 3Ex
FUV focus verification 6Ex (3Ex)*
FUV target acquisition parameter update
11Ex
Total for enabling
FUV λ scales
FUV resolution
FUV sensitivity & flat fields
FUV BOA operations
9Ex
11Ex+2Ex H
20Ex 13In 25Ex 16In
0Ex (2Ex)*
4Ex (4Ex)*
25Ex(4Ex)*
1Ex
0Ex
4Ex+3Ex
25Ex
1Ex
H
Total for calibration 30Ex (10Ex)* 33Ex
*contingency orbits
H additional orbits due to
HOPR
58 external orbits is comparable to a typical cycle’s calibration program
5

FENA2 FENA3 aperture, spectrum placement focus value
FENA1
FENA4 decision on operating HV value all visits of these programs except final confirmation visit of
FENA4 (target acquisition confirmation) executed prior to switch of operations to second lifetime position on July 23, 2012

FCAL2
FENA3
FENA3 overlap with FCAL1;
G140L spectra used for focus determination
(FUV4) and WCA-PSA offsets (FUV6.1)
FENA3 overlap with FCAL2;
G140L spectra used for focus determination (FUV4) and
FUV6.4, 6.5, 6.8
FCAL2 overlap with FCAL1;
FUV6.1, 6.4
FCAL1 spatial resolution of M modes; FUV6.5, 6.7
FCAL3
BOA G140L spectrum obtained in
FENA4 due to available space
FENA4 FCAL4 internal wavecal spectra
FUV6.2,
6.3, 6.7
Considerable synergies across lifetime calibration activities minimized the total number of orbits/exposures needed to accomplish the objectives
7

(HV sweep)
• voltage-PHA curves show the second lifetime position started out closer in behavior to the pre-scrub curve from ground testing.
• rapid evolution of voltage-PHA curve led to need for contingency orbits to sample the highest gains
• decision made to start operations at a modal PHA near 10 rather than lower
•
Y-walk corrections more complex than the linear function currently in use.
•
Y-walk appears to be independent of Y
•
X-walk is not currently accounted for. It is as dramatic as the Ywalk, with a much higher scientific impact.
•
X-walk is strongly dependent on X, and appears to be independent of Y.
➜

(spectrum & aperture placement)
•
+35 pixel shift (+2.94”) was too low; G160M/FUVB spectrum overlaps Lyman α airglow gain sag holes from original lifetime position
• offset changed to +3.5”, or +41 pixels
• stepping target across the aperture in positive, negative directions both along and across dispersion shows proper centering at (-0.05”,
+3.5”); changes added to SIAF file
➜

(focus sweep)
•
Ray trace models predicted best focus to be within ±200 focus steps of current location. Focus sweep performed on M mode gratings using 100 focus step increments near region of best focus, and 200 focus step increments outside of this region; best focus values for second lifetime position determined
•
M-mode gratings appeared to be offset by more than 100 focus steps from original position, so executed contingency orbits to do focus sweep of G140L grating. Best focus for G140L is strongly wavelength dependent, and focus curve is very asymmetric; focus value chosen was the minimum of the sampled points
➜

auto-correlation technique used to determine focus minimum; width of auto-correlation function reflects widths of lines in spectrum
G140L

(target acquisition parameter update)
•
TA subarrays, plate-scales, WCA-PSA offsets, confirmed; sign error in SIAF file corrected
•
ACQ/SEARCH algorithm verified
•
ACQ/PEAKD algorithm verified
•
ACQ/PEAKXD algorithm verified for each grating
• full TA sequence (ACQ/SEARCH+ACQ/PEAKXD+ACQ/PEAKD) and short TA sequence (PEAKXD+PEAKD) completed (after switch to operations at second lifetime position); offsets between expected and observed slews understandable
➜

(wavelength scales)
• preliminary comparison of COS and STIS spectra show offsets of 3 pixels or less
• initial results of extreme cenwave comparison appear to show offsets of 3 pixels or less, so no need to execute contingency orbits at this time
• currently no need to update dispersion relations, just zero point offsets.
➜

(resolution)
• examine unresolved lines and complex profiles in external target, compare against model LSF predictions
• preliminary results show that the resolution is within 10-15% of the value at the original lifetime position, as expected
• computation of new LSFs at the second lifetime position (including
MFWFEs and scattering wings) being performed; will be compared against observations and made available to community
➜

black=STIS E140M spectrum blue=STIS spectrum convolved with
COS LSF which includes scattering wings yellow=COS G130M/1291 red=COS G130M/1327

(flux, flat fields, TDS transfer)
• absolute flux calibration awaits updated wavelength calibration
• comparison of spectra at old/new position shows ratios slightly larger than one. This is probably due to the different HV values being used at the two lifetime positions
•
FUVA L-flat appears very similar to the one obtained at the original lifetime position
•
P-flats at original and second lifetime positions are distinct, as expected: sampling different detector regions
➜

G130M
Old/New

G140L

FUVA L-flat appears similar to one obtained at original lifetime position
P-flats (without grid wires) comparison between original location (red) and second lifetime position
(black).

(BOA Operations)
• test of auto-wavecals revealed an initial minor problem associating the wavecal files with G130M target spectrum; this has been fixed
• measured resolution is consistent between SMOV4 and FCAL4
• throughput for phot table had been improperly populated for BOA aperture; this is being corrected.
➜

•
•
•

TIPS/JIM
October 18, 2012
Agenda:
INS Division News (Margaret Meixner)
COS FUV Lifetime Move (Rachel Osten) !
VoIP Update: New/Expanded Voice, Collaboration and Mobility Services for STScI
(Dave Liska) !
A Preliminary Cycle 1 Calibration Plan for the JWST Science Instruments
(James Muzerolle) !
Next TIPS/JIM: December 20, 2012

“VoIP”  Update
New  /  expanded  voice,   collabora:on,  and  mobility  services   for  STScI

VoIP  project:  services
•   Improved  voice  services
–   Increased  reliability
–   Clearer  audio  (digital)
–   New  handsets
•   New  collabora;on  services
–   Screen  sharing  and  audio  conferencing
•   Jabber
•   WebEx  (pilot)
–   Chat  /  IM
–   File  transfer
–   Presence  informa;on
•   New  mobility  services
–   SoFphones
–   Mobile  clients  (pilot)

VoIP  project:  overview
•   September  go-­‐live  postponed
•   New  tenta;ve  go-­‐live  Thursday,  November  15 th
–   Date  depends  on  Telco  vendor  /  new  circuit  installs
•   New  date:
–   Significantly  reduces  cutover  risk
–   Enables  more  complete,  thorough  tes;ng
–   Expands  set  of  new  /  enhanced  services
–   Improves  training  &  communica;ons
–   Allows  for  inclusion  of  non-­‐ITSD  staff  pilot  /  feedback

Cisco  Jabber
Staff  directory  integra;on
Click  to  call—desk  phone,  computer,  cell
Audio  only  or  Audio  &  Video*
Chat  /  IM
Call  history
Voicemail
Calendar
Call  forwarding

Instant  messaging
Switch  to  voice  /   video*  call.
Screen  /  Desktop   sharing
Mul;-­‐user  chat
Transfer  files
5

Timeline
October   November
Office  Cabling
ITSD  Pilot
New  Circuit  Installs
Staff  Pilot
Phone
Placement
Full  System  Test
Training   Go
Live
Old  Phone
Pickup
6

Q UESTIONS ?
7

TIPS/JIM
October 18, 2012
Agenda:
INS Division News (Margaret Meixner)
COS FUV Lifetime Move (Rachel Osten) !
VoIP Update: New/Expanded Voice, Collaboration and Mobility Services for STScI
(Dave Liska) !
A Preliminary Cycle 1 Calibration Plan for the JWST Science Instruments
(James Muzerolle) !
Next TIPS/JIM: December 20, 2012

James Muzerolle

•   checkout of mechanisms, early calibrations to enable science
•   Commissioning activity requests (“CARs”) now written
•   Cycle 1: science obs begin as instrument modes are commissioned – need full calibrations

obtain all internal and celestial observations needed to fully calibrate the science instruments:
•   characterization of detector effects not done or completed on the ground
•   (spectro)photometric, astrometric calibration
•   monitoring/stability of key metrics and effects that may change
•   anything else not covered or completed during Commissioning begin defining a baseline plan by defining the set of likely programs and drafting program “ summaries ” use as input into the SODRM (Gordon et al.)

plan conceived and written by instrument leads:
NIRCam: Anton Koekemoer NIRSpec: James Muzerolle
NIRISS: Kevin Volk, Harry Ferguson MIRI: Karl Gordon status: all planned program summaries are complete
39 programs among the 4 SIs
available at https://confluence.stsci.edu/display/JWST/Cycle+1+Calibration+plans modified versions of all have been added to the SODRM

example program summary

grand total of 756 hours:
•   258 hrs likely to be done as parallels
•   82 hrs can be run during slews
(internals)

the vast majority of data volume will be obtained in parallel observations (all darks)
•   need to investigate at the visit level to verify within sufficient limits

data categories shared by most/all instruments
•   most common are darks, flats, flux calibration
•   many external observations share the same targets: astrometric calibration field, photometric standards

MIRI and NIRSpec dominate
•   more modes, monitoring, and standard stars

more than half of the programs are monitors
•   darks, lamp flats, (spectro)photometric calibration
•   cadences mostly notional at this point

•   dark reference files
•   bad pixel maps
•   read noise measurements
•   P- and L-flat reference files
•   Linearity reference files
•   astrometric solution and distortion reference files
•   PSF images/characterization
•   persistence maps
•   Spectral traces
•   LSF characterization
•   absolute photometric calibration conversion factors
•   relative throughput measures

The plan will be maintained by the new JWST Calibration &
Commissioning Working Group
•   check completeness of deliverables (Van Dixon reference file studies)
•   push further coordination with the Commissioning plan
­
many monitoring programs based on CARs (internals, astrometric & photometric calibration)
­   better define the boundaries between Commissioning and Cycle
1
•   update programs as new ground test results are obtained
•   plan ground-based preparatory observations (vetting of appropriate targets, etc)

approximate commissioning timeline:
L +
- expect to phase in Cycle 1 over L+5 to L+6 months