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
17-18 Feb 2014
1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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FISICA ACTIVITIES
17-18 Feb 2014
1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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FISICA ACTIVITIES
Science & Requirements Definition
Science & Requirements
Definition
Technology Activities
Instrument Simulator
Software
Dissemination and
Networking
17-18 Feb 2014
Technology
Activities
Satellite-related
Technology
Activities
Payload-related
An end-to-end Instrument Simulator
Network and Dissemination
1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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SCIENCE NEEDS
Near
Dust and Debris-discs
Star formation
The nearby universe
The evolving universe
Far
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1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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SCIENCE IN CONTEXT
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1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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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”.
17-18 Feb 2014
1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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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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1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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PAYLOAD-RELATED ACTIVITIES
A Double-Fourier Modulation test-bed for the 30-300um range
Grainger et al. 2012
17-18 Feb 2014
1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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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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1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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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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1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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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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1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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l frequencies.
In this operation the
FIINS (FAR INFRARED INSTRUMENT SIMULATOR) - 1
139
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]
17-18 Feb 2014
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
1st EU FP7-FISICA
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
127
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
17-18 Feb 2014
DISSEMINATION
1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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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
1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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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.
17-18 Feb 2014
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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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1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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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
17-18 Feb 2014
Diaphragms
Variable FP-etalon
1st EU FP7-FISICA Workshop - Roma 2014 – FISICA-FP7 Consortium
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CALIBRATION SOURCES (FROM SIMPLE
TO COMPLEX)
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