Transcript fisica - First Fisica Workshop

FISICA: FAR-INFRARED SPACE
INTERFEROMETER CRITICAL ASSESSMENT.
SCIENCE DRIVERS DEFINITION
AND
TECHNOLOGY DEVELOPMENT
Giorgio Savini on behalf of the FP7-FISICA Consortium
17-18 Feb 2014
1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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THE CONSORTIUM
Nicola Baccichet, Roser Juanola-Parramon, Giorgio Savini, Bruce Swinyard,
Amelie Guisseau
Peter Ade, Matt Griffin, Pete Hargrave, Georgina Klemencic, Enzo Pascale,
Rashmi Sudiwala.
Rob Ivison à Wayne Holland, John Lightfoot
Martyn Jones , David Walker
Colm Bracken, Anthony Donohoe, Anthony Murphy, Creidhe O’Sullivan,
Neal Trappe
Brad Gom, David Naylor, Locke Spencer, Ian Veenendaal
Kjetil Dohlen , Joel Lemerrer, Fabrice Madec, Eddy Rakotonimbahy, Christel
Rossin, Sebastien Vives, Annie Zavagno
Scige’ Liu, Stefano Pezzutto, Luigi Spinoglio.
Valerio Iafolla, Carlo Lefevre, Carmelo Magnafico, Diana Martella, Simone
Pini, Daniele Schito
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FISICA ACTIVITIES
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FISICA ACTIVITIES
Science & Requirements Definition
Science & Requirements
Definition
Technology Activities
Instrument Simulator
Software
Dissemination and
Networking
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Technology
Activities
Satellite-related
Technology
Activities
Payload-related
An end-to-end Instrument Simulator
Network and Dissemination
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SCIENCE NEEDS
Near
Dust and Debris-discs
Star formation
The nearby universe
The evolving universe
Far
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SCIENCE IN CONTEXT
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DATA PRODUCTS
Initial numbers were based on an ideal-element sensitivity model
Consistent with a scaled version of the NASA-concept SPIRIT.
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INSTRUMENT REQUIREMENTS
The Sensitivity Spreadsheet
Inter-connected sections with mutual dependencies.
Final Performances are gathered in the “performance sheet”.
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SATELLITE-RELATED ACTIVITIES
Study of tolerances and other implications of
CFRPs for light-weight deployable mirrors
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SATELLITE-RELATED ACTIVITIES
Satellite motion tolerances based on
accelerometer control loop
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SATELLITE-RELATED ACTIVITIES
Nano-satellite test-bench validation
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PAYLOAD-RELATED ACTIVITIES
A Double-Fourier Modulation test-bed for the 30-300um range
Grainger et al. 2012
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PAYLOAD-RELATED ACTIVITIES
Study of alternative techniques
Direct images
Visibility function
van der Avoort et al. (2007)
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PAYLOAD-RELATED ACTIVITIES
Cryogenic (4K) delay-line metrology
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PAYLOAD-RELATED ACTIVITIES
Complex Calibration Sources
Polypropilene based copper dissipator
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FIINS (FAR INFRARED INSTRUMENT SIMULATOR) - 1
Based on the original work of Roser JuanolaParramon (Doctoral Thesis)
Sky Simulator Instrument Model Data Processing Product Comparison
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l frequencies.
In this operation the
FIINS (FAR INFRARED INSTRUMENT SIMULATOR) - 1
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5.2. Data synthesis algorithms
40
−2
30
FOV [arcsec]
10
v [1/λ]
0.9
0.8
20
0
−1
0.7
0.6
0
0.5
y
Based on the
work of Roser
Juanola- have been
e used.
Iforiginal
pointing
errors
−10
−20
0.3
0.2
−30
−40
−40
0.4
1
2
−20
0
u [1/λ]
20
40
0.1
−2
−1
Parramon (Doctoral Thesis)
0
1
FOVx [arcsec]
2
Figure 5.14: uv-map coverage for a Fixed Angle baselines configuration (left) and the corre4.5.
sponding normalised dirty beam (right).
109
Instrument Model
cordingly for each baseline position.
−2
30
−10
−1
0
u [1/λ]
Instrument Model 20
40
−2
−1
0
1
FOVx [arcsec]
2
W
M
1
M
0
FOVx [arcsec]
1
2
Cold%Op(cs%
In general, if possible one selectsM3the uv-map W
coverage
to create
a beam suitable
for a
M3
W
4
D
M
F,BS
Det
M
Det
F,BS
Det
−3shows the simulated pointing position with an absolute pointing
−3error (left) in
Fig.4.7
M
OSL4
The restoration of the Master sky map has been kindly performed by Dr. Danielle Fenechrelative
100
200
Wavenumbers [cm −1]
126
6
here ⌦point is the point source solid angle and ⌦pixel is the pixel solid angle. With
1.1
3.
−2
−2
−2
−1
0
Noise reduction and time domain interpolation
FOVx [arcsec]
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the interferometric dirty beam.
1
2
10
rms
v
u n
u1 X
=t
[N ( i )]2
n
(5.3)
j=0 k=0
where n is the number of samples.
Given the number of scans N
for a given baseline and assuming that the signal
|SkyC(✓
2⇡⌫.k (b · ✓)]
p
x,i , ✓y,j ; ⌫k )| cos[2⇡⌫k
and noise are uncorrelated, by averaging them the DR is increased by N
scans
scans
9
x 10
5
x 10
0.4
θ=(0,0) arcsec
where
SkyC(✓x , ✓y ; ⌫) = SkyS(✓x , ✓y ; ⌫)Beam(✓
5
x , ✓y ; ⌫)td0 (⌫), I1 and I2 are the to
tensity of the sky map
4 on each of the
4
−5
−5
NX
N
F OV NX
F OV X
i=0
9
−1
3
0
θx [arcsec]
5
0.2
0
θ=(0,1.03) arcsec
telescope
θ=(1.03,0)dishes,
arcsec and
−0.2
0.4
b · ✓ is the projection
Position [cm]
0
−5
0 , ✓ )5on the
10 baseline vector (b , b ), this is
sky−10map vector
(✓
∆θx [arcsec]
x y
x y
3
3
Figure 4.7: Simulated pointing position with an absolute pointing error (left) and the absolute
pointing error distribution in the x direction (right) including a gaussian fit to the data with p = 2
b · ✓ = |b||✓| cos[arctan(by /bx )
arcsec.
2
2
2
0.2
0
−0.2
0.4
Position [cm]
arctan(✓y /✓x )]
0.2
0
−0.2
By observing Eq.4.28, it can be noted that the FTS contribution and the interfero
1
−0.2
1
−0.15
−0.1
−0.05
0
Position [cm]
0.05
0.1
0.15
0.2
contribution at the cosine arguments: the spectroscopic modulation is due to the term
1
0
0
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improve the dynamic range (DR) achievable in an interferogram, signal-averaging tech-
pp
the root-mean-square value of the noise, computed as
Ig( , b) = I1 + I2 + 2
0
5
4
e current configuration and with the defined astronomical distances, for this simulation
' 10
Data Processing i=1
5
2
FOVy [arcsec]
y
(5.1)
20
Nrms
x 10
Product Comparison
0
0
urce size is smaller than the pixel size on the sky grid, an emissivity parameter ✏ has to
−1.5
the4Double Fourier Modulation
observed. As expected, the point 15source is being detected with a diameter smaller than
−3
The
urce can be considered a protostar at ⇠ 50pc and with a radius ⇠ RSun . As the point
−1
0 performs
2
that
FOVx [arcsec]
FOV [arcsec]
baseline b.
Intensity [W/m /sr/cm ]
FOV [arcsec]
2
1.
0.5
⇠ 300pc but with a different orientation with respect to the observer plane. The point
−0.5
Double Fourier Module
x
pointing error, are user defined
parameters and can be modified.
5
200AU at ⇠ 150pc. The gaussian source can also be a circumstellar disk of ⇠ 80AU
⌦point
✏=
⌦pixel
M
application of Fourier Transform Spectroscopy and Interferometry simultaneously.
5.1. Datacube reconstruction from detected interferograms
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from UCL using the Astronomical Image Processing System AIPS [92] . AIPS is a package
Figure 5.17: Result of the wavenumber integration of the CLEAN datacube (left) and its logaAbsolute Pointing Error
Absolute
Pointing
Error Distribution
x
the sky
map
SkyS
a set ofininterferograms
are
computed,
for
each andinterfero
where Ig
S is the
peak to
peak power of the signalone
at the zero
path difference,
N
is
300
400
rithm (right).
1 could correspond to a circumstellar disk with an envelope size of
The elliptical source
introduced, this is
4.5.7
M
−4deviation−2
0 pointing
2 error,
−4 for the
−2
The standard
for the absolute
as4well as
This
module
isthe
thepercentage
analytical
module
Master sky map restoration with CLEAN
d the elliptical1.5
source is a blackbody at 50K and an absorption line at 80cm
ectra of the three sources is shown in Fig.5.2 (right).
−2
OSL3
the ✓x and
−4 ✓y space and the corresponding distribution (right, only in the
−4 x direction).
gure 5.2: The Master sky map. A gaussian source, a point source and an elliptical source
positioned on the sky grid (left). Spectrally (right) the gaussian source is a blackbody with
brightness temperature of 100 K and an emission line at 60 cm 1 (blue); the point source
responds to a blackbody at 2000 K (green), and the elliptical source is a blackbody at 50 K and
absorption line at 80 cm 1 (red).
2
2
2
2
N EPph,background = N EPph,instrument + N EPph,CM
B + N EPph,CIB + N EPph,Zodi
2
OSL3
−2
Det
M
given observation.
3
0
0
M
Det
OSL2
Intensity [A.U.]
−1
1
D
M
M
OSL4
θy [arcsec]
−2
−2
1
plus the CMB, CIB, and Zodiacal light
Det
1
5.1. Datacube reconstruction from detected interferograms
−1.5
W
NFD
Figure W4.6: Pointing of aMtwo-telescope
interferometer. If the pointing is ideal, the light coming
M
M3
M
deviation
corresponding
to the
10% of Dthe absolute
pointing error.
M
M
modulation appears in the dirty image.
1
where k indicates the source of the noise being computed. Finally, the total backg
p
2 Hz) is the addition of all the contributions from the instr
NEP (in units of W/
NFD
Det
will
the same
telescope beam (left) with a given delay. If the telescope
126uv-map coverage for a Spiral baselines configuration (left) and the correspondingfrom a givenOSLdirection
Figure 5.15:
D see F,BS
M
M
M
normalised dirty beam (right).
baseline is tilted, light coming from a given directionOSLwill see the same telescope beam, but the
corresponding to two orM1more different sources interfere constructively and hence a strong
4
2
2
FOVy [arcsec]
−20
3
Ideal Pointing
0.1
4
T2
T1
3
Telescope Pointing Error
Intensity [pW]
−0.5
2
T2
T1
Full Spacecraft Pointing Error
T2
Intensity [pW]
0
T1
Intensity [pW]
Intensity [W/m2/sr/cm−1]
FOVy [arcsec]
0.5
0.3
Det
but the circular symmetry has been lost. This feature could be useful in the case of sourcesto the other telescope,
M
theD lightF,BScoming from a givenM OSL
direction will see a different telescope beam
M2
M2
−1
−1
2
2
D
M
M
positioned in spatial harmonics, this is, when the ripples of the interferometric beams(right).
M
x 10
5
1
4
0.4
Intensity [A.U.]
1.5
0.5
0
0
delay will have changed (centre). If the pointing of one of the telescopes is different with respect
−3
6
4.5. Instrument Model
0.6
0.2
−30
2
0.7
0
1
−20
Sky Simulator −1
y
0
FOVy [arcsec]
FOV [arcsec]
v [1/λ]
10
1. Datacube reconstruction from detected interferograms
0.9
0.8
20
−40
−40
141
5.2. Data synthesis algorithms
40
0
50
Figure 5.3: Interferograms generated by FIInS for the Master simulation with a baseline length
of 18m: the raw or ideal interferogram Igraw (top), the noisy interferogram Ignoisy (centre) and
the averaged interferogram Ignoisy,av (bottom).
100
150and
−1
Wavenumbers ν [cm ]
0
the
is due
· ✓). 200
The longer the baseline separ
k5.3(b
200interferometric delay
50
100 to 2⇡⌫
Fig.150
shows interferograms
generated by FIInS for the Master simulation with a
−1
length]of 18m: the raw or ideal interferogram Ig
(top), the noisy interferogram
Wavenumbers baseline
ν [cm
the longer the delay between cosine modulations,
the more separated the interfero
Ig
(centre) which is the result of the addition of the instrumental, background and
raw
noisy
Figure 5.18: Spectral results of the
Master simulation
aftersources
restoration
with the CLEAN algocorresponding
to different
will appear.
100
200
300
400
rithm for
−1the central pixel of the gaussian source (blue), the point source (green) and the central
Wavenumbers
[cm
]2014
elliptical
source–(red)
(left). DetectedConsortium
spectra for three positions in the sky where no source
Workshop
- pixel
Roma
FISICA-FP7
intensity is expected (right).
4.5.8
ques must be used. The dynamic range is defined as
Figure
5.2: The Master sky map. A gaussian source, a point source and an elliptical source
Detector Noise Module
17
EU - NETWORK
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DISSEMINATION
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EU - NETWORK
DISSEMINATION
Yearly workshop as a reference and to allow
focused approach
Bringing Fundamental Astrophysical
Processes Into Focus: A Community
Workshop to Plan the Future of Far-Infrared
Space Astrophysics, Goddard
2017
The next opportunities:
-) pathfinders
-) technology demonstrators
-) Mission design study
Mid-decadal review,
somewhere here
2016
2015
2014
17-18 Feb 2014
London Early 2016
(Focus on Technology)
Maynooth Workshop, Early 2015
(Focus on Instrument Simulation)
WE ARE HERE
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CONCLUSIONS
Ø 2013 has been an exciting (not all good) year for the far-infrared
§ “Death” of Herschel, but not of its science
§ L2/L3 call – pooling of ideas and resources
§ The SPICA next step...
Ø FISICA-FP7 will focus on the identification and definition of the key data
products required from the science + analysis of the requirements of a space
interferometer to achieve these.
Ø Technological activities relevant to satellite and instrument have commenced
Ø While the program cannot be comprehensive of all techniques and existing
technology groups interested in the FIR, the Networking and Dissemination
elements allow for a regular note-comparing exercise in order to keep focus
Ø For information on the Consortium (and future related workshops):
www.fp7-fisica.eu
Ø There is a plan (not yet implemented) to use the webpage as a repository of FarInfrared science and mission concepts to allow the community to access relevant
information as required.
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...
THANKS FOR
YOUR KIND
ATTENTION
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ADDITIONAL MATERIAL
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DOUBLE-FOURIER MODULATION (DFM)
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A TEST-BED FOR THE FIRI OPTICS
DEVELOPMENT
Spectral
arm
Input ports
Output
ports
Variable
baseline
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TEST-BED UPGRADES PLANNED - MID &
FAR INFRARED
Detailed optical modelling
Upgrade metrology
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TEST-BED UPGRADES PLANNED - MID &
FAR INFRARED
A wide-band beam splitter
(or maybe two)
10 14 24 32
55
340
Wavenumbers (cm-1)
Optical bench conversion
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TEST-BED UPGRADES PLANNED – 3 BEAMS?
Detector planes
With additional
K-mirrors for
image rotation.
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CALIBRATION SOURCES (FROM SIMPLE TO COMPLEX)
Grainger et al. 2012
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CALIBRATION SOURCES (FROM SIMPLE TO
COMPLEX)
x13
x12
x23
1
3
Potentially covered by
2
Filters
d3
d1 d 2
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Diaphragms
Variable FP-etalon
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CALIBRATION SOURCES (FROM SIMPLE
TO COMPLEX)
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