Target star catalogue for Darwin: Nearby Habitable Star Systems

Kaltenegger, Lisa; Eiroa, C.; Stankov, A.; Fridlund, M.

doi:10.1017/s1743921306009148

Cited by 10 publications

(16 citation statements)

References 2 publications

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“…Currently, target catalogs for these survey missions have been started; for now, these are based on astrobiological interest and the few informed astro-engineering requirements available today, such as the existence of a secondary star too near and bright (Kaltenegger et al 2006) 3 . Surveys of exozodiacal dust levels of nearby stars are planned or in progress 4 ; the statistics of this unknown parameter alone may impose dramatic revision of the scale and cost of missions, even though elements in favor of optimism do exist (Beichman et al 2006).…”

Section: Discussionmentioning

confidence: 99%

“…5, and since the smallest considered θ HZ in is 0. 01 mas (Kaltenegger et al 2006), the spectral resolution must be better than ∼50.…”

Section: Spectral Resolutionmentioning

confidence: 99%

“…We have therefore extracted from the Improved Reprocessing of the IRAS Survey (IRIS) maps (Miville-Deschênes & Lagache 2005) 12.5 and 25 µm background emission levels for the target list of Kaltenegger et al (2006). Figure 6 shows the histogram for the emission at 12.5 µm.…”

Section: Galactic Interstellar Mediummentioning

confidence: 99%

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A scene model of exosolar systems for use in planetary detection and characterisation simulations

Belu¹,

Thiébaut

Ollivier

et al. 2007

A&A

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Context. Instrumental projects that will improve the direct optical finding and characterisation of exoplanets have advanced sufficiently to trigger organized investigation and development of corresponding signal processing algorithms. The first step is the availability of field-of-view (FOV) models. These can then be submitted to various instrumental models, which in turn produce simulated data, enabling the testing of processing algorithms. Aims. We aim to set the specifications of a physical model for typical FOVs of these instruments. Methods. The dynamic in resolution and flux between the various sources present in such a FOV imposes a multiscale, independent layer approach. From review of current literature and through extrapolations from currently available data and models, we derive the features of each source-type in the field of view likely to pass the instrumental filter at exo-Earth level. Results. Stellar limb darkening is shown to cause bias in leakage calibration if unaccounted for. Occurrence of perturbing background stars or galaxies in the typical FOV is unlikely. We extract galactic interstellar medium background emissions for current target lists. Galactic background can be considered uniform over the FOV, and it should show no significant drift with parallax. Our model specifications have been embedded into a Java simulator, soon to be made open-source. We have also designed an associated FITS input/output format standard that we present here.

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Section: Discussionmentioning

confidence: 99%

“…5, and since the smallest considered θ HZ in is 0. 01 mas (Kaltenegger et al 2006), the spectral resolution must be better than ∼50.…”

Section: Spectral Resolutionmentioning

confidence: 99%

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A scene model of exosolar systems for use in planetary detection and characterisation simulations

Belu¹,

Thiébaut

Ollivier

et al. 2007

A&A

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“…• , which corresponds to 36% more targets from the DARWIN target catalogue [6]. This advantage comes at the cost of severe instrumental dif culties.…”

Section: Spacecraft Formation and Beam Routingmentioning

confidence: 99%

“…To evaluate the science performance of the different aperture con gurations we calculated for each target of the DARWIN prime target catalogues [6] the integration time required to achieve a speci ed SNR for detection and for spectroscopy of the demodulated planet signal. We analyzed the most promising three and four aperture congurations, namely the orthogonal TTN with planar and non-planar spacecraft formation and the planar x-Array with an imaging to nulling baseline ratio of X B = 3.…”

Section: Science Performancementioning

confidence: 99%

DARWIN system concepts

Wallner¹,

Ergenzinger²,

Flatscher³

et al. 2017

International Conference on Space Optics — ICSO 2006

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The European DARWIN mission aims at the detection of Earth-like exo-planets and at the spectroscopic characterization of their atmospheres. By nulling interferometry in the mid-infrared wavelength regime the stellar ux may be rejected. By spatial and temporal modulation of the interferometer's receive characteristic the planet signal may be extracted from the background signals. The DARWIN instrument consists of a otilla of free-ying spacecraft, three to four spacecraft carrying the collector telescopes and one spacecraft carrying the control units and the beam recombination and detection unit. We present different system design concepts for the DARWIN instrument which have been elaborated within the DARWIN System Assessment Study. We discuss various aperture con gurations and beam routing schemes as well as modulation methods and and beam recombination schemes.

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Mission Requirements: How to Search for Extrasolar Planets

Fridlund

Kaltenegger

2007

Extrasolar Planets

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In this chapter we will discuss the motivation, scientific requirements and technical implementation of space-based search for extrasolar planets. We discuss current and planned future missions, with a focus on designs that will be able to collect photons and therefore spectral information of the atmospheres of planets. The interferometric nulling technique, as well as simulations of the observations, are discussed in detail. IntroductionToday, our generation is the first that possesses the technological ability to search for, and observe, planets orbiting other stars -so-called exoplanets. During the middle of the last century, a small number of scientists noted that this capability was emerging and suggested ways to implement it. Most notably, Struve [1] hypothesized that very large planets (Jupiter-sized or larger) could, if orbiting very close to a solar type star, be easily detected by the periodic change they would cause in the radial velocity (the stellar velocity along the line of sight) signature in their star's spectrum. Struve went on to point out that under these circumstances (a large planet close to its star), a percentage of the objects (of order 1%) would undergo eclipses which would also, in principle, be detectable using methods that were just becoming available around that time (e.g., modern photomultipliers as detectors). After these very astute predictions by Struve, almost 40 years were to pass before the hypothesis turned into observable fact when first Latham et al. [2] and then Mayor and Queloz [3] immediately followed by Butler and Marcy [4], discovered such bodies by detecting the radial velocity signature. By this time, the predictions by Struve had been more or less forgotten, and it came as somewhat of a surprise to find these very large planets close to their primary star. This "new" class of planets were then designated "hot Jupiters". Today they

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Target star catalogue for Darwin: Nearby Habitable Star Systems

Cited by 10 publications

References 2 publications

A scene model of exosolar systems for use in planetary detection and characterisation simulations

A scene model of exosolar systems for use in planetary detection and characterisation simulations

DARWIN system concepts

Mission Requirements: How to Search for Extrasolar Planets

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