TIPS/JIM
June 21, 2012
Agenda:
INS Division News (Danny Lennon)
Voice Over Internet Protocol (Gary Gladney)!
NIRISS NRM Bad Pixel Tolerance Analysis (Anand Sivaramakrishnan)!
The Infrared Sky: Background Considerations for JWST (Dean Hines)!
Next TIPS/JIM: July 19, 2012
INS STATUS June 21, 2012 Staffing Amber Armstrong to the Observation and Planning Branch -­‐ we wish her well. Audrey DiFelice has joined the instrument engineering team in MESA. Gerry Kriss will take over as Head of NIRCam in October. Operations COS is back to normal science operations. TIPS/JIM
June 21, 2012
Agenda:
INS Division News (Danny Lennon)
Voice Over Internet Protocol (Gary Gladney)!
NIRISS NRM Bad Pixel Tolerance Analysis (Anand Sivaramakrishnan)!
The Infrared Sky: Background Considerations for JWST (Dean Hines)!
Next TIPS/JIM: July 19, 2012
Voice over Internet Protocol at Space Telescope Science Ins3tute •  What is VoIP? •  What will be VoIP services will be offered at STScI? –  Basic VoIP Features (see user and administra3ve features and benefits) –  Voicemail –  SoC Phone (Cisco Jabber for Macs and Windows laptops) and Mobility ( iPhones, iPads, Androids and BlackBerrys) •  Scalability of STScI VoIP infrastructure What is Voice over Internet Protocol
(VoIP) Analog Digital Signal Digital Signal Cisco Call Manager Analog Cisco VoIP features Summary of user features for Cisco VoIP Ø Call connection
Ø Impromptu audio conference (up to 6
internal participants)
Ø Caller ID (at this time only for Internal calls)
Ø Hands free, full duplex Speaker phone
Ø Headset (uses RJ11 type connector)
Ø Message Waiting Indicator (MWI)
Ø Hold
Ø Transfer
Summary of user features for Cisco VoIP Ø  Dialed number display
Ø  Intercom
Ø  Use of reground and recyclable products in
manufacturing handsets (Cisco phone only)
Ø  Supported encryption for voice traffic, TLS/
SRTP
Ø  Call forwarding to either another local number
or external number
Ø  Self service website to allow user to configure
their desktop phone remotely.
Summary of user features for Cisco VoIP Ø  Call Park and pickup
Ø  Direct Inward dialing and Direct Outward
dialing
Ø  Directory dial from phone: Corporate directory
(AD) and personal directory (contacts address
book)
Ø  Mute capability
Ø  On-hook dialing
Ø  Multiple speed dials
Ø  Pre-record messages
Summary of features managing your Voice communica5ons remotely Ø Desktop voice communica3on can be managed using a WEB browser. Ø Customize Do Not Disturb op3ons Ø Set call forwarding per line Ø Change the Voice Message Indicator seQng per line Ø Change the Audible Voice Message Indicator seQng per line Ø Change ring seQng per line Ø Set speed dial buRons on your desktop phone Ø Change your PIN Ø Add a New Remote des3na3on Summary of user features for Cisco voicemail
Ø
Ø
Ø
Ø
Ø
Ø
Ø
Ø
Ø
Ø
Ø
Ø
You can select conversation type; full or brief prompts are supported.
You can change prompt and message playback speed.
You can address and then record a message, or record and then address a message.
You can record up to five personal greetings (alternate, busy, internal, off-hours, or
standard).
You can specify the order in which messages are presented over the phone, by
message type (voice, fax, or email), urgency, or LIFO/FIFO.
You can set an expiration date for any personal greeting.
You can manage an alternate greeting, require callers to listen to the full greeting, or
notify users when a greeting is on.
With a cascade message-notification feature, you can send additional notification
types if a message is not retrieved.
You can select whether or not message counts are announced; options include type,
totals, saved, and new counts.
You can specify Call Forward to a personal greeting or busy greeting.
You can provide message notification for new messages through devices such as
Simple Mail Transfer Protocol (SMTP) text, pagers, and phone destinations.
You can use your desktop telephone to manage, listen or record messages
Summary of features using Cisco’s Jabber application
Ø Use a single, intuitive interface for instant messaging with individuals and
groups, IP telephony, visual voicemail, voice and web conferencing,
desktop sharing1, communication history, and integrated directories.
Ø Presence (if you are online or Do Not Disturb)
Ø View real-time availability of co-workers and colleagues within and
outside the enterprise network.
Ø Exchange and display presence availability information and instant
messages with other Cisco Jabber users, Cisco Unified Personal
Communicator, Cisco WebEx Connect®, Microsoft Office Communicator
and Lync, IBM Lotus Sametime, AOL, GoogleTalk, and many other
XMPP-compatible clients.
Ø Exchange presence information with mobile handsets using Cisco Jabber
or third-party XMPP-compatible clients.
Ø Display customized availability messages.
Ø Your status is updated automatically when you are in a Cisco WebEx
meeting or sharing an application.
What does the user interface for Cisco Jabber look like Scalability of STScI VoIP Infrastructure Ø  Call manager server pair will support up to 10,000 subscribers.
Ø  Unity server (voicemail) can support up to 15000 users and a
maximum of 250,000 users per clusters.
Ø  Maximum number of subscribers for Cisco Call Manager cluster
can support up to 30,000 users.
Ø  Cisco IP Telephony solution can support multiple Call Manager
clusters.
Ø  Adding services is accomplished by adding more application
servers for example if we wanted to provision Cisco Mobile
Communicator as a service. We would add the application server
to our voice network. Below is the features of Cisco mobility.
Ø  Cisco has delivered Unified Communications in modular
architecture, as services are needed the can be added to the
overall Unified Communication architecture.
Ø  In the future we may use external Session Initiation Protocol (SIP)
trunks instead of connecting to the public telephone network. This
will help reduce our cost for external call and long distance calls.
Impact to the network with the deployment of VoIP Stsci.edu Cisco Unified IP Presence server (used for Cisco Jabber) STScI internal router Internet STScI VPN server Internet Cisco Unity server (voicemail) Cisco Call Manager MicrosoC Exchange server Cisco Voice Gateway Public Telephone Network STScI VoIP Deployment model
Single site deployment
More informa3on about Cisco’s IP Telephony can be found at – hRp://www.cisco.com/en/US/products/sw/voicesw/products_category_buyers_guide.html More informa3on about the Interna3onal Telecommunica3ons Union (ITU) and voice standards can be found at – hRp://www.itu.int/ITU-­‐T/50/docs/ITU-­‐T_50.pdf TIPS/JIM
June 21, 2012
Agenda:
INS Division News (Danny Lennon)
Voice Over Internet Protocol (Gary Gladney)!
NIRISS NRM Bad Pixel Tolerance Analysis (Anand Sivaramakrishnan)!
The Infrared Sky: Background Considerations for JWST (Dean Hines)!
Next TIPS/JIM: July 19, 2012
NIRISS NRM bad pixel tolerance analysis
David Lafrenière
2012 February 21
Simulation description
•  Master PSF
•  OTE phase maps RevV
•  NRM mask G7S6SC
•  Polychromatic, using F430M filter profile
•  Created with oversampling of 11x11 compared to NIRISS
pixels
•
Soummer, Pueyo, Sivaramakrishnan, Vanderbei OpEx 2007, same as WebbPSF algo)
•  Pointing
•  Telescope pointing error for acquisition and dithers: 15 mas
•
•
RMS
Telescope pointing jitter while guiding: 5 mas RMS
Simulated at 0.01 pixel precision using oversampled PSFs
Simulation description
•  Detector
•  Pixel flat field error: 0.1%
•  Non-uniform intra-pixel sensitivity
•  1 at pixel center, decreasing to a mean of 0.8 at pixel corner
(with RMS of 0.05)
•  Gaussian shape
•  21 e- read noise per CDS
•  Mean dark current of 0.012 e-/sec
•  Inter-pixel capacitive coupling included
•  Bad pixels included (see later for details)
Simulation description
•  Observation
•  L’=7.5 mag star
•  256x256 subarray (tframe=0.66 s)
•  Read mode, TFIRAPID, Nframe=1, Ngroup=14
•  Peak pixel kept at <70000 e- in last read
•  9 dithers on a 3x3 grid with 4” step
•  Assumed that the central 7x7 pixel box at each dither
position was free of bad pixels
•  121 integrations at each dither position
•  3 hour clock-time total on target
•  plus a similar sequence on a calibrator
•  12 min exposure on each of target and calibrator
Bad pixels
•
•
•
Varied fraction of bad pixels from 0% to 5%
Randomly distributed, assumed that 5/6th of bad pixels are
grouped in a “cross pattern” while 1/6th are individual pixels
Bad pixels assumed completely unusable
128x128
subarray
Bad pixel fraction 1%
Bad pixel fraction 5%
Bad pixels overlaid on PSF
•  A single exposure, on a log display scale
Bad pixel fraction 1%
Bad pixel fraction 5%
Analysis
1.  Mask bad pixels. Using integer shifts only, center all PSFs such
that their brightest pixel is aligned
2.  Average all images together to obtain a “clean” PSF image
3.  For each image, shift the “clean” PSF image by fraction of pixel
to align it precisely with the image, then substitute bad pixels for
the corresponding values from the shifted “clean” image.
4.  Apply a fractional shift to all images to precisely register them to
a common center.
5.  Average all images to obtain a new, and better, “clean” PSF.
6.  Repeat 3 & 4 using the new “clean” PSF image to substitute
bad pixels.
7.  Apply the usual procedure to extract the CP and SqV from each
image, then average them.
Results – detection limits
•
Limiting contrast (in difference of magnitude) as a function of
angular separation
0.06”
0.08”
0.10”
0.20”
0.30”
0.40”
0%
7.75
8.26
8.54
8.89
8.93
8.98
0.5%
7.66
8.17
8.45
8.76
8.73
8.79
1%
7.66
8.16
8.43
8.72
8.67
8.75
2%
7.42
7.92
8.19
8.49
8.42
8.49
3%
7.12
7.63
7.92
8.24
8.18
8.24
4%
6.93
7.45
7.74
8.08
8.02
8.08
5%
6.66
7.20
7.50
7.86
7.81
7.85
Results – detection limits
•
Magnitude loss in contrast compared with 0% bad pixels
0.06”
0.08”
0.10”
0.20”
0.30”
0.40”
0%
0.00
0.00
0.00
0.00
0.00
0.00
0.5%
-0.09
-0.09
-0.09
-0.13
-0.20
-0.19
1%
-0.09
-0.10
-0.11
-0.17
-0.26
-0.23
2%
-0.33
-0.34
-0.35
-0.40
-0.51
-0.49
3%
-0.63
-0.63
-0.62
-0.65
-0.75
-0.74
4%
-0.82
-0.81
-0.80
-0.81
-0.91
-0.90
5%
-1.09
-1.06
-1.04
-1.03
-1.12
-1.13
Results – detection limits
•
Factor of loss in contrast compared with 0% bad pixels
0.06”
0.08”
0.10”
0.20”
0.30”
0.40”
0%
1.00
1.00
1.00
1.00
1.00
1.00
0.5%
1.09
1.09
1.09
1.13
1.20
1.19
1%
1.09
1.10
1.11
1.17
1.27
1.24
2%
1.36
1.37
1.38
1.45
1.60
1.57
3%
1.79
1.79
1.77
1.82
2.00
1.98
4%
2.13
2.11
2.09
2.11
2.31
2.29
5%
2.73
2.65
2.61
2.58
2.81
2.83
Conclusion
•  Relatively good tolerance to bad pixels using dithers
•  To limit the loss in contrast at any separation to less
than 0.5 mag compared with 0% bad pixels, the bad
pixel fraction should be less than 3%
TIPS/JIM
June 21, 2012
Agenda:
INS Division News (Danny Lennon)
Voice Over Internet Protocol (Gary Gladney)!
NIRISS NRM Bad Pixel Tolerance Analysis (Anand Sivaramakrishnan)!
The Infrared Sky: Background Considerations for JWST (Dean Hines)!
Next TIPS/JIM: July 19, 2012
JWST/MIRI
The Infrared Sky: Background
Considerations for JWST"
Dean C. Hines & Christine Chen!
MIRI Instrument Team"
DCH-1
Space Telescope Science Institute
7/3/12
JWST/MIRI
The Visible (Optical) Sky"
DCH-2
Space Telescope Science Institute
7/3/12
JWST/MIRI
The Visible vs the Infrared Sky"
DCH-3
Space Telescope Science Institute
7/3/12
JWST/MIRI
The Visible vs the Infrared Sky"
DCH-4
Space Telescope Science Institute
7/3/12
JWST/MIRI
Infrared Background Sources"
u
Three primary sources of diffuse light in the astronomical sky"
–  Extragalactic – light from unresolved objects (galaxies and QSOs)!
–  Galactic – mostly star-light reprocessed by material in the Interstellar
Medium (ISM)!
–  Solar System – sun light reprocessed by material within the solar system!
u
These astronomical components are highly wavelength
dependent"
–  Visible and near-Infrared (NIR) – dominated by scattered/reflected
light but with some thermal NIR emission from very hot dust !
–  Longer wavelengths – dominated by thermal emission from warm dust
and by broad solid-state and giant molecular emission features!
u
Emission from the telescope and stray light also contribute to
the background"
–  Not a large issue for HST (except for NICMOS λ > 1.8µm)!
–  For JWST, this is an issue for most wavelengths, and becomes a
dominant source for MIRI!
DCH-5
Space Telescope Science Institute
7/3/12
JWST/MIRI
HST vs JWST!
Because JWST operates much colder than HST (~39-46K vs ~290K), diffuse!
galactic and zodiacal emission dominate the background for λ ≤ 16µm!
JWST!
HST!
HST Thermal"
Emission!
Diffuse Galactic + Zodi!
NICMOS Instrument Handbook!
DCH-6
Glasse et al. (2010)!
Space Telescope Science Institute
7/3/12
JWST/MIRI
COBE/DIRBE"
Blue = 1.25 µm"
Green = 2.2 µm"
Red = 3.5 µm"
Zodi + Galaxy + Exgal!
!
All of the images use 4
decade logarithmic color
scales. "
"
The lowest level is 3.95 kJy/sr
at 3.5 microns, 6.67 kJy/sr at
2.2 microns, and 7.08 kJy/sr
at 1.25 microns for the upper
and middle images, but 0.395
kJy/sr for the lower image."
DCH-7
Galaxy + Exgal!
Exgal!
Space Telescope Science Institute
7/3/12
JWST/MIRI
Thermal Emission from Zodi Dust"
Blue = 12 µm; Green = 60 µm; Red = 100 µm"
IRAS!
DCH-8
Space Telescope Science Institute
7/3/12
JWST/MIRI
Thermal Emission from Zodi Dust"
Blue = 12 µm; Green = 60 µm; Red = 100 µm"
IRAS!
DCH-9
Space Telescope Science Institute
7/3/12
JWST/MIRI
Thermal Emission from Zodi Dust"
Blue = 65 µm; Green = 90 µm; Red = 140 µm"
Akari!
DCH-10
Space Telescope Science Institute
7/3/12
JWST/MIRI
Zodi Dust Bands (IRAS)"
DCH-11
Space Telescope Science Institute
7/3/12
JWST/MIRI
Zodi Bands & Spectrum"
Optical!
DCH-12
Space Telescope Science Institute
7/3/12
JWST/MIRI
Taurus Spitzer 24µm"
Residual Zodiacal Dust
Band Emission after
subtraction of a smooth
zodiacal background
model based on COBE/
DIRBE data.!
Zodiacal"
Dust Bands !
DCH-13
Space Telescope Science Institute
7.7˚!
7/3/12
JWST/MIRI
Galactic ISM (COBE)"
Blue = 60 µm; Green = 100 µm; Red = 240 µm"
DCH-14
Space Telescope Science Institute
7/3/12
JWST/MIRI
Galactic ISM (COBE)"
Green = 100 µm; Red = 240 µm"
DCH-15
Space Telescope Science Institute
7/3/12
JWST/MIRI
PAH Emission from the ISM"
PAH Emission Features — 3.29, 6.2, 7.7, 8.7, 11.3, and 12.7 µm!
Wavelength (µm)!
DCH-16
Space Telescope Science Institute
7/3/12
JWST/MIRI
Emission from the Galaxy"
PAH Emission Features — 3.29, 6.2, 7.7, 8.7, 11.3, and 12.7 µm!
DCH-17
Space Telescope Science Institute
7/3/12
JWST/MIRI
Zodi + Galactic"
DCH-18
Space Telescope Science Institute
7/3/12
JWST/MIRI
Zodi + Galactic"
DCH-19
Space Telescope Science Institute
7/3/12
JWST/MIRI
Conclusions"
u
u
u
u
u
u
DCH-20
The Infrared Sky is much different in structure and brightness
compared the visible sky"
At visible wavelengths, the background is dominated by light
scattered from dust in the solar system (HST also contends
with geocoronal emission and earthshine)"
The infrared background is dominated by emission from dust
in the solar system and the galaxy, plus broad-band emission
features from PAHs associated with diffuse galactic dust"
These astronomical background sources will dominate the
JWST background for λ ≤ 16µm, and will still be important for
longer wavelengths"
The background will vary in time as our view of the zodiacal
emission changes during the year"
STScI is working with the Spitzer Science Center (SSC) to
develop a background model appropriate for JWST"
Space Telescope Science Institute
7/3/12
JWST/MIRI
Fin!
DCH-21
Space Telescope Science Institute
7/3/12
JWST/MIRI
WISE"
DCH-22
Space Telescope Science Institute
7/3/12
JWST/MIRI
DCH-23
u
All of the images use 4 decade logarithmic color scales. The
lowest level is 3.95 kJy/sr at 3.5 microns, 6.67 kJy/sr at 2.2
microns, and 7.08 kJy/sr at 1.25 microns for the upper and
middle images, but 0.395 kJy/sr for the lower image."
u
The lowest level is 223.2 kJy/sr at 240 microns, 555.3 kJy/sr at
100 microns, and 508.2 kJy/sr at 60 microns for the upper and
middle images, but 30.7 kJy/sr for the lower image."
Space Telescope Science Institute
7/3/12