Download Mauna Kea Site Monitoring Working Group 1998 Activities

Ground-based Observatories Instrumentation and Detector Systems
Doug Simons (Gemini Observatory)
Paola Amico (Keck Observatory)
Scientific Detector Workshop - 2005
Photo Courtesy Akihiko Miyashita, Subaru Telescope
Coauthor List
Poster
Oral
Dietrich Baade, European Southern Observatory
Sam Barden, Anglo Australian Observatory
Randall Campbell,W.M. Keck Observatory
Gert Finger, European Southern Observatory
Kirk Gilmore, Stanford/SLAC
Roland Gredel, Calar Alto Observatory
Paul Hickson, University of British Colombia
Steve Howell, National Optical Astronomy Observatory
Norbert Hubin, European Southern Observatory
Andreas Kaufer, European Southern Observatory
Ralk Kohley, GranTeCan/ Instituto de Astrofisica de Canarias
Philip MacQueen, University of Texas
Sergej Markelov, Russian Academy of Sciences
Mike Merrill, National Optical Astronomy Observatory
Satoshi Miyazaki, Subaru Telescope
Hidehiko Nakaya, Subaru Telescope
Darragh O'Donoghue, South African Astronimical Observatory
Tino Oliva, INAF/ Telescopio Nazionale Galileo
Andrea Richichi, European Southern Observatory
Derrick Salmon,Canada France Hawaii Telescope
Ricardo Schmidt, National Optical Astronomy Observatory
Homgjun Su, National Astronomical Observatory of China
Simon Tulloch, ISAAC Newton Group/ Instituto de Astrofisica de Canarias
Mark Wagner, Large Binocular Telescope
Olivier Wiecha, Lowell Observatory
Binxun Ye, National Astronomical Observatory of China
2
A World-wide Sample of Instruments
3
Summary
 Survey conducted world-wide to develop a “snap
shot” of instrumentation used today and planned for
tomorrow
 Intent is to use this database to
 Explore “where we are” now in astronomy
 Extrapolate to the future
 Help bridge gap between astronomical community and
manufacturers about what types of detectors are needed
 Not intended to be a detailed description of any
institution’s instruments
 No single observatory is large enough to “dominate” the
database
4
Survey Details
 Instrument name
 Observing Modes
 Start of operations
 Wavelength Coverage
 Field of View
 Instrument cost
 Multiplex gain
 Spatial [“]/Spectral
resolution
 # Detectors
 Detector Format
 Detector size
 Buttability
 Pixel size
 Pixel scale
 Electronics
 Noise
 Readout Time
 Dark Current
 Full well
 Cost per pixel
 Comments or additional
parameters
5
Survey Details
 25 institutions polled as part of a world-wide
survey of ground-based instrumentation
 Compiled instrumentation database for telescopes with
3.5 m aperture
 Compiled data on ~200 instruments through this
survey
 Enough to probe various trends in instrumentation and the
detector systems in use today at major astronomy facilities,
worldwide
 Detailed results will be published via the Proceedings of
this conference
 Represents a unique source of information about
instrumentation in astronomy, both existing and planned
6
Wavelength Coverage
Instrument Number
Instrumement
 The “great divide”
between optical and
infrared is obvious
 Basically a bimodal
distribution, separated
at 1 µm
 This divide is artificial
- it’s technology
driven, not science
driven
180
90
1
0.1
11
10
Wavelength (µm)
100
7
Optical, Near-Infrared, or Mid-Infrared?
50
40
30
20
10
0
MIR
NIR
OPT
Wavelength Coverage
Percent
 The next-generation of
instruments will consist
of nearly equal numbers
of optical and NIR
instruments
NOW
60
Percent
 Currently astronomy is
pretty heavily dominated
by optical instruments,
with ~2 out of 3
instruments using CCDs
70
50
45
40
35
30
25
20
15
10
5
0
FUTURE
MIR
NIR
Wavelength Coverage
OPT
8
Optical, Near-Infrared, or Mid-Infrared?
 This is due to many reasons
including
70
50
40
30
20
10
 A relatively small MIR
community
 A historically specialized
field technically to get into
 The need for special telescope
systems (chopping), etc.
0
MIR
NIR
OPT
Wavelength Coverage
Percent
 The lack of MIR
instruments reflects a
relatively “untapped”
science frontier, not lack of
scientific importance
NOW
60
Percent
 In both cases MIR
instruments occupy a very
small part of the “market”
50
45
40
35
30
25
20
15
10
5
0
FUTURE
MIR
NIR
Wavelength Coverage
OPT
9
What Modes are Most Commonly Used?
 Most spectrometers also have an
imaging mode, at least to support a
target acquisition mode, so imaging
systems are important
70
60
50
Percent
 Spectrometers remain the most
popular type of instrument in
astronomy (~60%), with imagers a
distant second (~25%)
30
20
10
0
Imager
Spectrometer
Other
Primary Instrument Modes
 Among the spectrometers built, not
surprisingly the most popular type
remains the “simple” long slit
spectrometer
80
70
60
Percent
 An equal number of MOS and IFU
based systems are either built or
planned
 Given the large multiplex gain of
these systems, MOS and IFU
spectrometers tend to require the
largest focal planes
40
50
40
30
20
10
0
MOS
IFU
Long Slit
Spectrometer in Use
10
Current Market Share by Various
Manufacturers
30
20
15
10
E2V
Other
E2V
Other
Rockwell
Raytheon
SITe
Rockwell
Manufacturer
Raytheon
50
45
40
35
30
25
20
15
10
5
0
SITe
0
MIT/LL
5
MIT/LL
 Bottom plot tallies all detectors
sampled in survey so is a true
“head count” of detectors in use
Percent of
Instruments
 Effectively assumes 1 detector per
instrument
 “Others” are in many cases are oneoff devices in specialized
instruments which together
account for ~20% of all instruments
25
Percent of
Detectors
 Top histogram shows dominant
manufacturers used in various
instruments
Manufacturer
11
Current Market Share by Various
Manufacturers
30
 Regardless of how market share is
assessed, E2V detectors are the most
commonly used in ground-based
astronomy
20
15
10
Other
E2V
Rockwell
Raytheon
SITe
0
MIT/LL
5
Manufacturer
Other
E2V
Rockwell
Raytheon
50
45
40
35
30
25
20
15
10
5
0
SITe
Manufacturer
MIT/LL
Percent of
Detectors
 Nearly half of all science detectors in
instruments sampled are made by E2V
 Linked to previous plots
demonstrating popularity of optical
instruments in astronomy
 Large CCD mosaics that have been
built no doubt enable E2V market
share compared to NIR
manufacturers, where comparably
large mosaics have not been built
Percent of
Instruments
25
12
Plate Scale and Field of View
15
10
 Can’t correct over large fields
1
0.9
0.8
0.7
0.6
0.5
0.4
0.3
Plate Scale (arcsec/pixel)
40
35
30
Percent
 Extremely small fields are
pretty much exclusively domain
of AO
0
0.2
 Clearly a “sweet spot” in field
size of instruments for fields in the
10-100 arcmin2 range
0.1
5
0
 Lack of >1” pixels is probably
due to not sampling small
telescopes which often have
large fields
20
Percent
 Most instruments use
(surprisingly) small pixels, most
at ~0.1”
25
25
20
15
10
Field of View (arcmin2)
1E+06
1E+05
10000
1000
100
10
1
0
0.1
5
0.01
Extremely large fields on the right
are mainly due to future ultra wide
field instruments involving enormous
CCD focal planes
14
 Drives builders to faster optical
systems and reduced tolerances
which may be non-trivial to
achieve in cryogenic instruments
50
45
40
35
30
25
20
15
10
5
0
CURRENT
18.5
27
30
40
50
75
Pixel Size (µm)
70
FUTURE
60
50
Percent
 NIR instruments have pretty much
locked into 18-27 µm pixel format
 The the future, pixels of this size
will remain popular
 Likewise MIR instruments have
adopted pixels 2-3 times bigger,
consistent with larger point spread
function at these longer
wavelengths
 Shifting to considerably smaller
pixels to reach larger array formats
may pose problems for optical
designs of infrared instruments
Percent
Typical Infrared Pixel Size Now and
Tomorrow…
40
30
20
10
0
18.5
20
27
40
Pixel Size (µm)
50
15
Typical CCD Pixel Size Now and
Tomorrow…
45
40
30
25
20
15
10
 86% of current instruments use
13-15 µm pixels
 In all cases 15 um is the most
often used, with
5
0
6.5
13
13.5
15
16
24
Pixel Size (µm)
60
50
Percent
 73% of future instruments
sampled will use 13-15 um
pixels
CURRENT
35
Percent
 Similarly, current and future
optical instruments have
pretty much “standardized”
on 13-15 µm pixels
FUTURE
40
30
20
10
0
9
10
12
13
13.5
Pixel Size (µm)
15
24
16
Typical Infrared Array Format, Now and
Tomorrow…
 1024x1024 is the “standard”
format used in NIR arrays today
 In the future, the community
clearly wants to switch to larger
format device, with 75% of the
future instruments sampled
going with 2k NIR arrays
 Again, astronomers will take
advantage of larger format IR
detectors, when they become
available
Percent
50
CURRENT
40
30
20
10
0
128x128
240x320
256x256
512x512
1024x1024
2048x2048
Detector Format
80
70
FUTURE
60
Percent
 2048x2048x devices likely have
not been around long enough to
become well established, with
only ~15% of the market share
60
50
40
30
20
10
0
256x256
240x320
1024x1024
Detector Format
2048x2048
17
Typical CCD Format, Now and
Tomorrow…
60
 77% of future instruments
expect to use either 2x4k or
4x4k CCDs
 Clearly astronomers are eager
to use ever larger CCDs…
Percent
50
CURRENT
40
30
20
10
0
1024x1024
2048x2048
2048x4096
Other
Detector Format
45
40
35
Percent
 2x4k building block is, not
surprisingly, by far the most
popular current CCD format
 Future planned instruments
will baseline 4x4k detectors
as much as the more
established 2x4k detectors
FUTURE
30
25
20
15
10
5
0
1024x1024 2048x2048 2048x4096 4096x4096
Detector Format
Other
18
Optical
Infrared
Number of Pixels in Focal Plane (10 6)
18
16
More
100
90
80
70
60
50
40
30
20
10
CURRENT
0
50
45
40
35
30
25
20
15
10
5
0
FUTURE
14
12
10
8
Number of Pixels in Focal Plane (10 6)
More
100
90
80
70
60
50
40
30
20
2
0
10
6
4
0
 Essentially all IR focal
planes are <10 Mpixel
 Most optical focal planes are
also <10 Mpixel, though
some are much larger
 Have merged NIR+MIR into
“Infrared”
Number of Focal Planes
 Total of ~1.9 Gpixels
found in current
instruments sampled by
this survey
Number of Focal Planes
Total Pixel “Inventory”, Now and
Tomorrow…
19
Optical
Infrared
18
16
More
100
90
80
70
60
50
40
30
20
10
CURRENT
0
50
45
40
35
30
25
20
15
10
5
0
Number of Pixels in Focal Plane (10 6)
FUTURE
14
12
10
8
Number of Pixels in Focal Plane (10 6)
More
100
90
80
70
60
50
40
30
20
2
0
10
6
4
0
Number of Focal Planes
 The future looks similar in the
infrared with most instruments
having modest size focal planes
 The future at optical
wavelengths include a lot more
large focal planes
 The future market includes
~7.7Gpixels of science grade
detectors, >90% of which is in the
form of CCDs in the future
“More” category (>100 Mpixel
focal planes)
 Note that lack of planned IR
large format focal planes isn’t
due to lack of ambition on the
part of IR astronomers - it’s due
to lack of money…
Number of Focal Planes
Total Pixel “Inventory”, Now and
Tomorrow…
20
Controller Types
25
20
15
10
MPI
Monsoon
MCE
SDSU
IRACE
FIERA
0
ARCON
5
AAO2
Percent
 Includes all instruments
(current and future) in survey
 SDSU clearly the most
commonly used controller in
astronomy, with ~1 in 4
controllers being an SDSU
system
 Huge range in controllers being
used - total of 44 different
controllers identified in survey
 This is an area where we would
all benefit from an “industry
standard”
Manufacturer
 Closest thing we have is SDSU
21
Instrument Costs
 Most participants in the survey did not include a
cost and, in general, it is difficult to make a detailed
“apples to apples” comparisons due to various
assumptions
 Does cost include labor, overhead, all parts, etc?
 Instead, have only assessed median costs of current
and future instruments to look for basic trends
Median Instrument Cost Summary
Optical
Infrared
Current
$400,000
$3,750,000
Future
$6,600,000
$5,000,000
22
Future Trends in Science and
Technology…
“Cosmic Convergence”
 Tracing the physical origin,
evolution, and large scale
structure of matter and
energy, from the Big Bang, to
present, remains one of
highest priority research areas
in all of science
 Many organizations are
working in this field in a
global effort to unravel the
most fundamental aspects of
the universe
24
Key Epochs in the Early Universe
Photons from this scattering surface are what we now
see as the Cosmic Microwave Background (CMB)
Universe Neutral
Universe Ionized
Reionization in the Early Universe
25
“First Light” in a Dark Universe
 Using current and/or next-gen
telescopes, we will, for the first
time, detect the first luminous
objects in the universe – the
“First Light”
 The discovery and analysis of
the first stars is arguably one of
the “holy grails” in astronomy
 The light from these distant
objects is red shifted to 1-2 µm,
hence the need for large format,
low noise, NIR detectors in the
future
Simulation of an Ultra Deep
NIR Image of the First Stars
26
Boundaries on Research Frontiers
Astronomy is fundamentally a
technology driven and limited field of
science and detectors always have and
always will play a central role in what
we can learn about the universe
As an example…
27
The Galactic Center: Discovery Strip
Chart
28
The Galactic Center: Becklin &
Neugebauer 1975
29
The Galactic Center: Forrest et al. 1986
30
The Galactic Center: Rigaut et al. 1997
31
The Galactic Center: Recent ESO Results
Zeroing in on a Massive Black Hole…
32
 Our basic understanding of
key areas in astronomy is
clearly a function of current
technology
 What took us perhaps 25
years to achieve before, may
only take ~10 years with the
rapid acceleration of
technology available to
astronomers
 Advancements in science
detectors have made this all
possible…
25 yrs
The 25 Year “Evolution” of the Galactic
Center...
33
Boundaries on Research Frontiers
ELT’s and the next generation of ultra wide
field instruments are examples of nextgeneration ground-based facilities that will
revolutionize our understanding of the
universe
The years ahead in astronomy will include
explorations of very large and very small
structures
In either case, large scale, high performance,
affordable optical and infrared science
detectors will be necessary
34
The Future is Both Large and Small
 The next generation of ELT’s
will provide unprecedented
“views” of the universe
 Given the extreme apertures of
these telescopes, when coupled
with AO systems that allow
ELT’s to work at their
diffraction limits, they will
yield data with spatial
resolutions far greater than
what is possible with the
current generation of 8-10 m
telescopes
OWL
TMT
35
The ELT’s Window
on the Universe...
~1”
~1”
Target: Galactic Cores
Objective: Detect signatures
of black holes in compact
galactic nuclei
Target: Io
Objective: Remote seismic
monitoring & planetary
mineralogy
Target: Forming Planetary
Systems
Objective: Measure SED of
forming stars, planets &
surrounding gas, binary
fractions, disk evolution,
Dust & gas dynamics, MF,
etc.
Target: First Stars
Objective: Morphology,
spectra, and luminosity
of first luminous objects
in the universe
Target: -ray bursters
Objective: Identify and
measure distance & SED
of hosts; detect the “first”
GRBs in the universe
Target: Extra-solar planets
Objective: Direct imaging
and spectroscopy of
planetary systems beyond
our own
Future Wide Field Facilities
LAMOST Project
The Large Sky Area Multi-Object
Fiber Spectroscopic Telescope
Pan-STARRS
LSST
Hyper-SUPRIME + WFMOS
44
Future Research
 These facilities will be used to perform enormous
surveys to answer major questions in astronomy and
fundamental physics, of interest to all of humanity
Galaxy Genesis
Dark Matter
Dark Energy
45
The Destiny of the Universe
Matter/Gravity Overcome the
Initial Expansion from the Big Bang
46
The Destiny of the Universe
Universe “Coasts” Outward, with Matter/Gravity
In Approximate Equilibrium with Big Bang Expansion
47
The Destiny of the Universe
Expansion of the Universe Accelerates, Ultimately
Shredding Its Material Contents
48
The Destiny of the Universe
With the discovery of Dark Energy
this now appears to be possible.
Next-generation detectors will
play a key role in solving this mystery
Expansion of the Universe Accelerates, Ultimately
Shredding Its Material Contents
49
Summary Thoughts
Detectors in 180 instruments in use today have
been surveyed to perform a “bottom-up”
assessment of detector systems in use now or
planned in the near future in astronomy
Optical detectors currently dominate those used in
ground-based astronomy, and will remain the most
commonly used detector throughout the next ~decade
Planned future instruments will need Gpixel class
optical focal planes and many are migrating to 40962
format
Most infrared detectors used now have a 10242 format,
but many instrument builders are migrating to the
buttable 20482 format detectors now available
50
Summary Thoughts
 A “top-down” approach is used to forecast the
future in ground based astronomy (~5-15 years)
 ELTs: Large infrared focal planes will be needed to sample
diffraction limited fields of enormous telescopes of the
future
 Wide Field Facilities: Large optical focal planes will be
used to survey millions of stars and galaxies at modest to
high spectral resolution
 Cosmology: Frontier science is being red shifted to the
near-infrared as telescopes get larger, which will drive NIR
detectors to have low noise and low dark current in often
“photon starved” applications
 The science horizon in astronomy is exciting and
compelling, but our discoveries will only be as
remarkable as the science detectors we use to
explore the universe
51