Darwin—an experimental astronomy mission to search for extrasolar planets
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As a response to ESA call for mission concepts for its Cosmic Vision 2015–2025 plan, we propose a mission called Darwin. Its primary goal is the study of terrestrial extrasolar planets and the search for life on them. In this paper, we describe different characteristics of the instrument.
KeywordsInterferometer Nulling interferometry Direct imaging of exoplanets Exoplanets Habitable zone
1 The Darwin mission goals
The discovery of extra-solar planets is one of the greatest achievements of modern astronomy. There are now more than 200 such objects known, and the recent detection of planets with masses approximately five times that of Earth demonstrates that extra-solar planets of low mass exist. In addition to providing a wealth of scientific information on the formation and structure of planetary systems, these discoveries capture the interest of both scientists and the wider public with the profound prospect of the search for life in the Universe.
We propose an L-type mission, called Darwin, whose primary goal is the study of terrestrial extrasolar planets and the search for life on them. By its very nature, Darwin advances the first Grand Theme of ESA’s Cosmic Vision. Accomplishing the mission objectives will require collaborative science across disciplines ranging from planet formation and atmospheres to chemistry and biology, and these disciplines will reap rewards from their contributions to the Darwin mission.
Darwin is designed to detect rocky planets similar to the Earth and perform spectroscopic analysis of them at mid-infrared wavelengths (6 to 20 μm), where the most advantageous contrast ratio between star and planet occurs. The spectroscopy will characterize the physical and chemical state of the planetary atmospheres and search for evidence of biological activity.
2 The Darwin mission profile
2.1 Baseline mission scope
The Darwin mission consists of two phases, search and spectral characterization, whose relative duration can be adjusted to optimize scientific return. During the search phase of the mission (nominally 2 years), the mission will examine nearby stars for evidence of terrestrial planets in their habitable zone (HZ). An identified planet should be observed at least three times during the mission in order to characterize its orbit. The number of stars that can be searched depends on the level of zodiacal light in the system and the diameter of the collector telescopes. As a baseline, we estimate this number under the assumption of a mean exozodiacal density three times that in the solar system and collecting diameters of 2 m. Over 200 stars can be screened under these conditions (Section 3.3.3). The mission focuses on solar type stars, including the F, G, K and some M spectral types.
The number of expected planetary detections depends upon the mean number of terrestrial planets in the HZ, per star, ηEarth. Our present understanding of terrestrial planet formation (Section 2.3) and our solar system, where there are two such planets (Earth and Mars) and one close to the HZ (Venus), point to a fairly high abundance of terrestrial planets. We assume hereafter that ηEarth = 1. The COROT mission should reveal the abundance of small hot planets, and Kepler will evaluate ηEarth as well as the size distribution of these objects several years before Darwin flies. These inputs will allow refinement of Darwin’s observing strategy well in advance of launch.
During the characterization phase of the mission (nominally 3 years), Darwin will acquire spectra of each detected planet at a resolution of 20 and with sufficient signal-to-noise to measure the equivalent widths of CO2, H2O, and O3 with a precision of 20% if they are in abundances similar to those in the Earth’s atmosphere.
Spectroscopy is more time consuming than detection. With ηEarth = 1, only a fraction of the detected planets can be studied spectroscopically. As shown in Section 3.3.3 for Earth-sized planets, Darwin can perform spectroscopy of CO2 and O3 on about 50 planets and of H2O on about 25 planets during the nominal 3-year characterization phase. Note that the mission profile retains flexibility, and optimization of the spectroscopy phase will be possible based on early results from the detection phase.
The general astrophysics program, if adopted, will comprise 10% to 20% of the mission time.
The primary science segment would then be reduced accordingly, with limited impact on its outcome.
2.2 Extended mission scope
An extension of the mission to 10 years will depend on the results gathered during the first 5 years. Such an extension could be valuable to observe more M stars, only 10% of the baseline time is attributed to them, search for big planets around a significantly larger sample of stars, and carry out additional measurements on the most interesting targets already studied.
2.3 Darwin target catalogue
3 Mission design
3.1 The Darwin concept and its evolution
In order to disentangle the faint emission of an Earth-like planet from the overwhelming flux of its host star, the planetary system needs to be spatially resolved. This, in turn, requires an instrument up to 100 m in diameter when operating at mid-IR wavelengths since the angular size of the habitable zones around Darwin target stars ranges between 10 and 100 mas. A monolithic telescope of this size is presently not feasible, particularly since the observatory must be space-borne and cooled to provide continuous coverage and sensitivity between 6 and 20 μm.
Residual star light, referred to as stellar leakage, caused by the finite size of the stellar photosphere and by imperfect efficiency of the interferometer;
The local zodiacal background, produced by the disk of warm dust particles that surround our Sun and radiate at infrared wavelengths;
The exozodiacal light, arising from the dust disk around the target star;
The instrumental background produced by thermal emission within the instrument.
Breaking the symmetry of the array to cancel all centro-symmetric sources, including the stellar leakage, the local and exozodiacal emissions;
Performing faster modulation of the planet signal via internal modulation between the outputs of sub-interferometers
Because the modulation efficiency varies across the field-of-view, the planet can only be localised and characterised through an additional level of modulation, provided by array rotation with a typical period of one day. The variation of the chopped planet photon rate with the rotation angle of the array appears at the extreme right of Figure 3. These data must be inverted to obtain the fluxes and locations of any planets that are present. The most common approach is correlation mapping, which is closely related to the Fourier transform used for standard image synthesis. The result is a correlation map, displayed for a single point source in the low right part of the figure. This represents the point spread function (PSF) of the array.
This process, illustrated here for a single wavelength, is repeated across the waveband, and the maps are co-added to obtain the net correlation map. The broad range of wavelengths planned for Darwin greatly extends the spatial frequency coverage of the array, suppressing the side lobes of the PSF (Section 3.3.4).
A dozen array configurations using phase chopping have been proposed and studied at ESA and NASA during the past decade. In 2004, the two agencies agreed on common figures of merit to evaluate their performance. The most important criteria are the modulation efficiency of the beam combination scheme, the structure of the PSF and its associated ability to handle multiple planets, the overall complexity of beam routing and combination, and finally, the number of stars that can be surveyed during the mission lifetime (Section 3.3.3). Among the many configurations studied, the X-array has been identified as the most promising for the Darwin mission.
3.2 Mission architecture
Two observing modes: nulling for extrasolar planet detection and spectroscopy, and constructive imaging for general astrophysics;
Placement at L2 for passive cooling and low ambient forces;
Launch with a single Ariane 5 rocket or two Soyuz-ST/Fregat vehicles;
The ability to search at least 225 candidate stars with an exozodiacal background of one zodi,1 or 150 stars with an exozodiacal background of 10 zodis;
Detection and measurement of terrestrial atmosphere biosignatures as described in Section 2.2 for at least 25 stars (with one zodi) or 15 stars (with 10 zodis; 2 m collectors);
Time allocation of search as follows: G stars 50%, K stars 30%, F and M stars 10% each.
The effort to turn these requirements into a workable mission culminated in 2005–2006 with two parallel assessment studies of the Darwin mission. Two array architectures have been thoroughly investigated during these studies: the four-telescope X-array and the three-telescope TTN. These studies included the launch requirements, payload spacecraft, and the ground segment during which the actual mission science would be executed. Almost simultaneously, NASA/JPL initiated a similar study in the context of the Terrestrial Planet Finder Interferometer (TPF-I).
These efforts on both sides of the Atlantic have resulted in a convergence and consensus on mission architecture. The baseline for Darwin is a non-coplanar, or Emma2-type X-array, with four collector spacecraft (CS) and a single beam combiner spacecraft (BCS). This process also identified a back-up option, in case unforeseen technical obstacles appear: a planar X-array.
3.2.1 The Emma X-array architecture
The X-array configuration separates the nulling and imaging functions, thus allowing independent optimal tuning of the shorter dimension of the array for starlight suppression and that of the longer dimension for resolving the planet. Most other configurations are partially degenerate for these functions. The X-array also lends itself naturally to techniques for removing instability noise, a key limit to the sensitivity of Darwin (Section 3.3.2). The assessment studies settled on an imaging to nulling baseline ratio of 3:1, based on scientific and instrument design constraints. A somewhat larger ratio of 6:1 may improve performance by simplifying noise reduction in the post-processing of science images (Section 3.3.2).
Each of the collector spacecraft (CS) contains a spherical mirror and no additional science-path optics (some components may be needed for configuration control). The four CS fly in formation to synthesize part of a larger paraboloid—the Emma configuration is a single, sparsely filled aperture. Flexing of the CS primary mirrors or deformable optics within the beam combiner spacecraft will conform the individual spheres to the larger paraboloid.
Transfer optics and BCS/CS metrology;
Correction and modulation, including optical delay lines, tip-tilt, deformable mirrors;
Mirrors, wavefront sensors, and beam switching;
Possibly, spectral separation to feed the science photons into two separate channels;
Phase shifting, beam mixing;
Recombination, spectral dispersion and detection
The collector and beam combiner spacecrafts use sunshades for passive cooling to <50 K.
An additional refrigerator within the BCS cools the detector assembly to below 10 K.
Key Darwin parameters
Value or comment
Collector spacecraft (CS)
4 free-flyers, passively cooled to <50 K
Lightweight spherical mirrors, diameter about 2.0 m, no deployables
CS array configuration
X-array with aspect ratio 3:1–6:1 (to be optimized)
7 to 168 m nulling, 20 to 500 m imaging option
Beam combiner (BCS)
1 free flying spacecraft, passively cooled to <50 K
Beam combiner optics
Transfer, modulation, beam-mixing, recombination, spectroscopy
Mid-IR detector about 500 × 8 pixels for nulling, (300 × 300 for imaging option), cooled to < 10 K
Low vibration refrigerator, e.g. absorption coolers
Require about 1 GBit/s, direct downlink from BCS
6–20 μm, includes H2O, O3, CH4, CO2 signatures
Field of view
Typically 1 arcsec at 10 μm
10 − 5, stable over ∼5 days
5 milliarcsec at 10 μm for a 500 m baseline, scales inversely
25 (possibly 300) for exo-planets; 300 for general astrophysics
Field of regard
Annular region between 46° and 83° from anti-sun direction at a date, 99% over one year
F, G, K, M, at least 150 (10 exo-zodis) or 220 (3 exo-zodi)
5 years baseline, extendable to 10 years
Nominal 2 years detection, 3 years spectroscopy, flexible
L2 halo orbit
Radio frequency and laser controlled
Field effect electric propulsion (FEEP) or cold gas
Single Ariane 5 ECA or 2 Soyuz-ST/Fregat
3.3 Mission performance
3.3.1 Detecting earths
For a given integration time, the signal is proportional to the number of planetary photons, and the quantum noise increases with the square root of the number of extraneous photons (Fig. 6). As described in the next section, additional noise arises from imperfections in the system such as stellar leakage. In order not to dominate the quantum noise, these imperfections must be very stable, with a flat power spectral density, i.e. white noise, allowing the signal to noise ratio on the planet to increase as the square root of the integration time.
3.3.2 Instability noise
To estimate mission performance in a realistic way, we must take into account the possible imperfections of the instrument. In the case of Darwin, the main imperfections result from vibrations and thermal drifts of the spacecraft, which in turn generate small fluctuations in the phase and amplitude of the input light beams. This produces instabilities in the interferometric null, a process similar to speckle noise in a coronagraph. The associated time-variable leakage of stellar photons, called instability noise, is generally not removed by phase chopping [2, 7].
Reducing the contribution of instability noise to a harmless level, that is below other unavoidable noises, places strict requirements on configuration control: path length and amplitude variations should be less than 1.5 nm and 0.1%, respectively.
This is only marginally compliant with state-of-the-art active control. Therefore, two techniques have been proposed and investigated to mitigate the influence of instability noise on mission performance.
The first solution, known as spectral fitting , is closely related to the particular arrangement of the X-array, where the nulling baselines are decoupled from the resolution baselines. Stretching the array while keeping the nulling baselines unchanged shrinks the fringe pattern considerably. Because the overall transmission pattern scales as the wavelength, the transmitted planet signal becomes a rapidly oscillating function of wavelength, an effect which can be used to disentangle it from the slowly varying instability noise pattern. The ability of the Emma architecture to adjust the aspect ratio of the X-array is valuable to implement this technique in an optimal way.
The second solution, known as post-nullingcalibration, also relies heavily on the geometry of the X-array. The constructive outputs of the pair-wise nulling beam combiners, which contain mostly stellar light, can be used as reference beams to calibrate the final output of the interferometer. Only the stellar component of the output signal produces fringes when combined with these reference beams, and hence the stellar glare can be isolated .
These two mitigation techniques represent a decisive advantage of the X-array concept compared to other architectures.
3.3.3 Search strategy and performance
Darwin mission performance can be expressed in terms of the number of stars that can be screened for the presence of habitable planets, and the number of follow-up spectroscopic observations that are possible.
The nominal mission is 5 years, with 2 years allocated to detection and 3 years for spectroscopy (possibly reduced by 10% to 20% if the imaging capability in constructive mode is implemented—see Section 2.1). About 70% of mission time is spent collecting data, with the remainder dedicated to overheads, for example, moving the spacecraft to change the interferometer geometry. In order to secure an accurate identification in the search phase, we require that the probability for detecting an Earth-like planet in the HZ at a signal-to-noise ratio (SNR) of 5 be 90% or larger. We assume that the IR luminosity of planets in the HZ are identical to Earth’s, independent of the distance to the host star. Detection is most efficient with a single, optimised array length.
ESA has conducted performance simulations for each star in the target catalogue, using the DarwinSim software to assess the required integration time to reach the required signal to noise ratio (SNR) for detection and spectroscopy. These requirements are a SNR of 5 on the whole band for imaging in nulling mode, and a SNR of 10 from 7.2 to 20 μm for H2O, CO2 and O3 spectroscopy, using a spectral resolution λ/Δλ ≥ 20.3
The level of exozodiacal emission is an important input parameter to these simulations. The amount of such emission around typical main sequence stars is presently largely unknown. There are successful ongoing programs using the Spitzer spacecraft and Keck-I interferometer to evaluate the zodiacal emission for stars with rather large emission, e.g. young stars, and relate these emissions to stellar parameters. They will be valuable to pre-screen the Darwin targets and avoid object with severe zodiacal emission. The LBT-I interferometer, and a possible future interferometer in Antarctica, will contribute to this effort, in due time before the launch.
Under the assumption that the exozodiacal emission is symmetric around the target star, the chopping process will suppress it, and the exo-zodi will only contribute to the quantum noise. The simulations presented below assume an exozodiacal density of three zodis.4
Number of stars and planets that can be studied
Assuming that each nearby cool dwarf is surrounded by one rocky planet of one Earth radius within its habitable zone, we estimate that only a fraction of the detected planets can be fully characterised (i.e., examined for the presence of H2O, CO2 and O3) during the subsequent 3-year spectroscopic phase. This number would be doubled or quadrupled for planets with radii 1.5 and 2 times that of the Earth, respectively. A comparable simulation effort at NASA using star count models confirms these predictions.
The diameter of the telescopes has an important incidence on the overall mission performance. With 1-m telescopes, the number of targets screened would be reduced to about 75, while with 3-m mirrors, almost the complete star catalogue could be surveyed, at constant performance per object.
3.3.4 Image reconstruction in the nulling mode
3.3.5 Visibility measurements with a bright source in the field
For imaging in the constructive mode, the presence of a bright source in the field makes cophasing the sub-pupils of the interferometer much easier. The nature of the target and the science goal will determine the required instrumentation. We consider three different cases: few visibility measurements with a bright source in the field of view, imaging with a bright source, and imaging without a bright source.
With minimal impact on the nulling recombiner, Darwin can carry out visibility (V2) science with JWST-like sensitivity, as long as there is a K ≤ 13 magnitude source in the field of view to stabilize the array. The modulus of the visibility provides simple size information about the target, for example, its radius assuming spherical morphology. The phase of the visibility gives shape information, such as deviations from spherical symmetry.
If the target spectrum is smooth a few visibility measurements can be obtained rapidly, because Darwin can work simultaneously at several wavelengths (see below). The baseline recombiner could perform such measurements with very modest modification, and hence, with minimum impact on the cost of the mission. Therefore, a capability for basic visibility measurement should be implemented. Unfortunately, a limited number of V2 observations provide useful information for only a limited number of targets.
3.3.6 Aperture synthesis for targets with a bright source
Aperture synthesis imaging requirements for Darwin
Maximum baseline (m)
Minimum baseline (m)
Field of view (resolution elements)
Spectral range (μm)
The 5σ, 1 h, point source sensitivities for Darwin in 20% wide bands centred at 8, 10, 13 and 17 μm are approximately 0.1, 0.25, 0.5 and 0.8 μJy, respectively. These sensitivities are comparable to those of JWST.
The maximum foreseen baselines are 500 m, corresponding to a spatial resolution of 5 mas at 10 μm.
With a stability time scale of 10 s for the array (Alcatel Study, 2000), the sensitivity limit for self-fringe-tracking is about 10 mJy at 10 μm in a 0.5 arcsec aperture. This performance gives access to virtually all of the sources in the Spitzer SWIRE survey.
3.3.7 Aperture synthesis for targets with no bright source
For targets with no bright source in the field, the preferred option for co-phasing is the use of a nearby off-axis bright reference star (K ≤ 13). One way of doing this is to feed the K-band light of this star along with the 6–18 μm light of the target to the beam combiner satellite, a so-called dual field configuration. Another option is to make the interferometer optically rigid using kilometric optical gyros. These devices can maintain the phasing of the array between pointings at a reference star and the target field.
Clearly, this additional instrumentation may be much more demanding and expensive. A decision whether or not to add this capability to Darwin will depend on an analysis undertaken during the study phase and available fundings.
4 Science operations and archiving
4.1 Data science operations architecture and share of responsibilities
The Science Operations Center (SOC) will be responsible for science mission planning, data processing, and data product distribution to the Darwin science team and the wider scientific community. Because the data acquisition and calibration requirements are very different for the planetary (nulling) and general astrophysics (imaging) missions, options for the SOC beyond ESOC need to be considered. Computer networking and remote presence through videoconferencing will play a central role, allowing responsibilities to be spread among a variety of network-nodes at several institutes throughout Europe.
4.2 Archive approach
The site for active and legacy archives is to be determined. The archive should include values of the nulling transmission, visibilities, and reduced image data, including the accompanying calibration files. A quick-look facility will allow rapid assessment and review of the data. Compared to other contemporary missions, Darwin’s data volume will be relatively modest and should present no storage challenges.
4.3 Propriety data policy
Although the detailed rules of data access are still to be determined, we anticipate that there may be different policies for the primary science and general astrophysics programs. Specifically, the baseline mission (nulling interferometry) will be conducted by ESA in cooperation with a dedicated team of Darwin scientists. Data rights would then follow guidelines adopted by ESA for missions similar in character (e.g., GAIA). In general, the science team is obliged to reduce the data and make the results public within a stipulated time. A peer-review process will almost certainly determine the general astrophysics targets. Following a call for Open Time observations, ESA will accept proposals from a Lead Scientist, who will act as the contact point between the Agency and the proposing community. In this case, the commonly adopted proprietary period is one year from the time of data release.
5 Technology and mission roadmap for Darwin
5.1 Darwin’s technology roadmap
5.1.1 Essential technology developments for Darwin
Formation flying of several spacecrafts with relative position control of a few centimetres
The feasibility of nulling interferometry in the 6–20 μm range. Based on the expected star/planet contrast (1.5 × 10 − 7 at 10 μm and 10 − 6 at 18 μm for an Sun–Earth analogue) and on evaluations of instability noise (Section 3.3.2), the common conclusion of the industrial studies is that the null depth must be 10 − 5 on average, and that it must be sufficiently stable on the timescale of days so that the signal to noise ratio improves essentially as the square root of time. This stability requirement translates into tight instrument control specifications, which can however be relaxed by means of the two instability noise mitigation techniques presented in Section 3.3.2. A thorough evaluation of the these techniques and of the resulting instrumental stability requirements will be a key component of the technology development programme.
5.1.2 Current status of technology development
Europe has devoted considerable resources, both intellectual and financial, to these technological issues since the initial Alcatel study. ESA has invested approximately 20 M€ since 2000, with a significant ramp-up in the last 2 years. Several tens of Technology Research Programs (TRPs) have been issued. NASA has run a parallel program in the USA. Most of the key technologies have been addressed and significant progress achieved.
Selection of the baseline interferometer configuration. Significant effort in this area since 2000, backed by independent studies in the USA and Europe, has identified the non-planar Emma X-Array as the optimal choice (see Section 3.2);
Achromatic phase shifters (APS), which allow broadband destructive interference between beams, have reached TRL 4. A comparative study currently running in Europe should identify the preferred approach;
Space-qualified delay lines to balance the different optical paths to nanometre accuracy have been demonstrated to TRL 5. A breadboard at TNO-TPD has achieved this performance at 40K and may be included as a test payload in the PROBA 3 space mission (Section 5.2);
Single mode fibres, or integrated optics modal filters that enable broadband nulling are now at TRL 4. Chalcogenide fibres have demonstrated the required performance of 40% throughput and 30 dB rejection of higher order spatial modes in the 6–12 μm band. On going work is emphasizing silver halide single-mode filters, which will operate in the 12–20 μm band. Photonic crystal fibres that can cover the whole spectral domain in a single optical channel are considered;
Detector arrays with appropriate read noise and dark current are at TRL 5/6. The Si:As impurity band conductor (IBC) arrays developed for JWST appear to be fully compliant with Darwin requirements. A reduced-size version of the JWST 1,024 × 1,024 detector, e.g. 512 × 8 (300 × 300 for the general astrophysics program), could be read out at the required rate with a dissipation of a few tens to hundreds of μW. These devices exhibit high quantum efficiency (80%), low read noise (19 e − ), and minimal dark current (0.03 e − /s at 6.7 K). Such performance permits sensitive observations, even at moderately high spectral resolution (Res = 300);
Low vibration Cryo-coolers for the detector system are now at TRL 4. A European TRP has led to a prototype absorption cooler providing 5 mW of cooling power at 4.5 K. JPL scientists have demonstrated a system with 30 mW of cooling at 6 K.
5.1.3 Future plans
The message from the last decade of Darwin technology development is clear: if the research and technology effort that has been pursued in both Europe and the USA continues vigorously, Darwin’s technology will reach TRL 5/6 by 2010, allowing it to be selected as ESA’s first L mission for launch in 2018–2020.
In addition to the European and American teams, the Japanese space agency (JAXA) has expressed interest in the mission and in participating in the technology effort. Japan has considerable expertise in several key fields, including cryogenics with the AKARI mission, and mirror engineering.
5.2 Precursor missions
5.2.1 Exoplanet discovery and statistics
COROT (in operation)
Kepler (under implementation)
5.2.2 Formation flying
The Darwin interferometer relies on formation flying (FF) technology to control the four collector spacecrafts and one beam combiner. Section 3 describes how this strategy offers significant advantages. As with any new approach, however, FF should be validated in space. Europe has initiated several precursor missions:
The PROBA-3 mission is the next logical step after PRISMA. This mission builds on PRISMA’s achievements, in addition to RF metrology, will demonstrate optical metrology sensors to TRL 8/9, providing 30 μm relative positioning accuracy. PROBA 3 could be launched in 2010, but it is not yet fully funded. This mission is not essential for Darwin, but we favour its completion, because it would provide further in-space demonstration of FF technologies.
Pegase is a single Bracewell interferometer that was proposed in the framework of the 2004 call by CNES for its formation flying demonstrator mission. The main scientific goal of Pegase is the high-angular resolution study of extrasolar giant planets at near-infrared wavelengths (2.5 to 5 μm). The mission could be extended to the study of brown dwarfs, circumstellar disks and dust tori around active galactic nuclei (AGN). CNES performed a Phase 0 study, but the mission was not selected for budgetary reasons. The construction of a mission breadboard, called PERSEE, is under consideration to increase our understanding of nulling interferometers. Note that, in order to ensure knowledge transfer to ESA, Pegase is being proposed as an M mission within the Cosmic Vision programme. An attractive possibility would be a merger with PROBA 3, with additional European and possibly international participation. This would allow the inclusion of stellar interferometry into the mission.
6 Cost plan and international cooperation
6.1 Cost estimate
Darwin is proposed as an L mission. Darwin will be one of the most ambitious missions that ESA has ever undertaken, and we emphasize that a phase A study is needed to derive an accurate cost estimate. Here, we present a preliminary estimate, based on information from Alcatel (now Thales Alenia Space, TAS), Astrium, and a recent study of the Emma X-array by JPL.
The introduction of the Emma concept [4, 17] provides a major simplification of the instrument, eliminating all deployable components except the antennas. The optics of the collecting spacecrafts (CS) is reduced to a single mirror (Section 3.2). Note that the CS cost scales as a function of the mirror diameter, because it is the main component of the spacecraft.
Estimated total cost and science performance for Darwin with different collector spacecraft mirror diameters
Total cost (M€)
Planets O3, CO2 sp.
Planets H2O sp.a
Further cost savings may be achievable in the design of the beam combiner spacecraft (BCS). For instance, the current baseline design requires two distinct optical paths, because of the limited spectral range of existing single-mode fibres. However in the near future, Photonic Crystal fibres may allow operation over the entire 6–18 μm range with a single optical path.
Flight elements. We use the JPL estimate of spacecraft masses plus a 20% margin, and apply a mean cost of 220 k€ per payload kg, which includes 15% contingency. These values are typical for scientific payloads (Earth and astronomical observations) as well as for telecommunication satellites, (information supplied by a European prime contractor). Total, 845 M€.
Launcher. Ariane V ECA, 6.6 tons deliverable to L2: 125 M€ (CV Annex 4).
Ground segment (5 years operations). Considering the volume of communications, a prime contractor estimates the ground segment cost at 55 M€, which seems conservative when compared to that of GAIA (48 M€).
Pre-implementation and Space Agency internal costs. We apply 1% and 11% of the total, respectively, as required in CV Annex 4.
Contingency. This is already included: 20% on mass plus 15% on cost per kilogram.
Table 4 presents cost and performance estimates for different CS mirror sizes, using a conservative scaling dependence of the collecting mirror mass with their diameter, M∝ D2.
6.2 International cooperation
Darwin science has worldwide appeal. At present, both NASA and the Japan space agency, JAXA, have indicated their interest in the mission and their willingness to participate in the study phase (letters of commitment has been sent). Their letters also indicate a possible participation in the construction and operation phases. Contacts with other agencies are being cultivated.
A “zodi” is defined as the density of our local zodiacal dust disk and acts as a scaling factor for the integrated brightness of exozodiacal dust disks.
The required SNR of 10 for water vapour detection has still to be consolidated. For CO2 and O3, an SNR of 5 would actually be sufficient for a secure detection.
In practice, exozodiacal densities below 10 times our local zodiacal cloud barely affect the overall shot noise level, while higher densities would significantly increase the required integration times.
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