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CHEOPS IN A NUTSHELL CHEOPS IN A NUTSHELL → KEY PERFORMANCE METRICS → MORE INFORMATION ... CHEOPS

Photometric Performance → CHARACTERISING SciReq 1.1 (G5V, 5500K) SciReq 1.2 (K5V, 4500K) ESA’S FIRST SMALL SCIENCE MISSION 100 100 85 ppm total total photon photon

] stray light ] stray light

-1/2 instrument -1/2 instrument [ppm (6h) [ppm (3h) [ppm

σ 20 ppm σ

10 10 6 8 10 12 6 8 10 12

1-sigma photometric precision (in parts per million) for two sizing cases. Left: precision foreseen after a total on-source integration time of 6 hours (duration of CHEOPS is an ESA mission implemented in partnership with Switzerland transit of planet with of 50 days). Right: precision foreseen after a through the . The University of Bern leads a Consortium total on-source integration time of 3 hours (duration of transit of planet with orbital period of 13 days). The dashed horizontal lines denote requirements. of 11 ESA member states contributing to the mission and represented in the CHEOPS Science Team. Bandpass

1 1 TESS Austria CHEOPS is the next European Space Community contribution 0.8 0.8 COROT Belgium to the long-term international effort of finding life beyond our

0.6 0.6 France Solar System. The mission will use the technique of ultra-high CHEOPS CHEOPS Germany precision transit to measure accurate sizes of large 0.4 0.4 Hungary MOST Normalised Response Normalised Response samples of to Neptune-sized planets, targeting individual

Kepler Italy 0.2 0.2 bright stars already known to host . Portugal

0 Spain 400 600 800 1000 0 400 600 800 1000 Sweden By combining measurements of radius made with CHEOPS with Wavelength (mm) Wavelength (mm) Switzerland existing mass determinations, it will be possible to determine Left: Normalised spectral response of CHEOPS and selected exoplanet space United Kingdom the mean density of the planets and thus to start to constrain missions. Cyan = spectral energy distribution (SED) of a Teff~5500K dwarf; pink their internal structure and composition. These constraints = SED of Teff~4500K dwarf. Right: Normalised spectral response of CHEOPS and GAIA, compared with the bandpasses of the BVRI filter set (Bessell, 1990, PASP, will be combined with key parameters of the host stars and 102, 118 with data taken from http://spiff.rit.edu/classes/phys440/lectures/filters/ For further details, see the following websites: the planetary orbits to provide vital clues to how small planets filters.html). See https://www.cosmos.esa.int/web/cheops/cheops-performances for further details. form, migrate and evolve. Sky coverage CHEOPS will identify prime targets for searches for the finger-

De c Sep Jun De c Sep Jun 90 90 prints of key molecules in the planets’ atmospheres using facil- 10 80 2015 15 85 80 85 15 15 20 80 80 ities such as Webb Telescope and future ground-based facilities 15 60 1520 60 45 25 75 75 40 20 35 70 70 30 25 ] ] such as the European Extremely Large Telescope. It will also be 40 25 65 40 65 50 25 25 60 60 days days 20 55 55 [ 20 5 5 5 5 5 5 55 [ 65 e 10 20 e used to study the physical mechanisms driving energy transport 50 35 50 75 75 im 35 im 5 deg] 0 45 deg] 0 30 45 dt dt 70 40

c[ c[ 5 65 40 25 40 in the atmospheres of hot Jupiters, through measurements of 35 25 30 De De 40 − 20 35 − 20 15 5 35 70 30 20 10 15 30 60 2015 40 50 60 5 their phase curves. − 40 20 55 25 − 40 25 25 45 20 Accumulate 20 Accumulate 35 15 15 − 60 1520 10 − 60 30 10 10 10 20 10 510 15 5 − 80 10 5 5 − 80 5 0 0 To achieve these science objectives, the design and implemen- 12h 9h 6h 3h 0h 21h 18h 15h 12h 9h 6h 3h 0h 21h 18h 15h RA [hours ] RA [hours ] tation of CHEOPS has been optimised to achieve: Accessible sky (in days per year) for which the contribution to the noise budget from • Ultra-high precision photometry in the visible-NIR, over Earth stray light is ≤ 5 ppm /70 ppm for a V=9 G-type (T =5500K)/ V=12 K-type https://sci.esa.int/cheops https://cosmos.esa.int/cheops http://cheops.unibe.ch/ eff periods of up to 48 hours. (Teff=4500K) dwarf, and for which the maximum % of each spacecraft orbit that is free from interruptions due to Earth Occultation or passage through the South • High sampling cadence (up to 1 sample per minute). Atlantic Anomaly is 50% (left) or 80% (right). Solid black line: locus of the . • Large instantaneous and annual sky coverage. CHEOPS IN A NUTSHELL CHEOPS IN A NUTSHELL CHEOPS IN A NUTSHELL → MISSION OVERVIEW → PAYLOAD → OBSERVING WITH CHEOPS

Spacecraft/instrument Single ultra-high precision photometer covering 0.33 – 1.1 microns maintenance

Overview:

• First ESA small (S-) class science mission. Guaranteed Time Guest Observers Observing Programme Programme • Partnership with Switzerland with Defined by the CHEOPS Science Team Open to the whole contributions from 10 other member states. Science Community • Short development time (5 yrs), ESA

cost of 50M€ . Monitoring & characterisation • Responsibilities: activities ESA: mission architect + launch, space- Left: Fully-assembled flight model of the CHEOPS payload;Right: Cross-section through the Lifetime: 3.5 yrs baseline (5 yrs goal) craft procurement (delegated to ADS payload. Credit: University of Bern. Spain), instrument CCD, mission opera- • 10% of time per year top-sliced for spacecraft-/instrument-related activities, tion tools, Guest Observers Programme. Telescope Optics: together with programme to monitor and characterise CHEOPS performance. Consortium: instrument, mission/science • Ritchey Chrétien Telescope, primary mirror effective diameter 30cm, • 80% of remaining observing time allocated to the Guaranteed Time operations, science team, monitoring + CAD of the CHEOPS spacecraft. Credit: F/5 optics, effective length 1600 mm. Spain. Observing Programme (GTO), defined by the CHEOPS Science Team. evaluation of science performance. • De-focussed point spread function (PSF), radius (90% encircled energy) ~12 pixels. • 20% of remaining observing time - 1578 hours/946 orbits per year - • Plate scale of ~ 1 arcsec/pixel, 17’ x 17’ field of view (0.32 deg2). available to Community through the ESA-run CHEOPS Guest Observers (GO) Spacecraft: • Multiple baffles to minimise straylight. Programme. • Target list for the GTO Programme defined for full 3.5 year mission from outset: • Based on flight proven Airbus D&S - List frozen shortly before annual calls, updated over the course of the mission platform, with small modifications. according to agreed procedures. • ~ (1.5 m)3, 290 kg mass (wet). • Rolls around Line of Sight to ensure • ESA Guest Observers’ Programme. - Annual Announcements of Opportunity (AOs) – first call ~ 6 months before launch. radiators point to free-space (nadir - Open to all, regardless of nationality or country of employment. locked). - Any science that makes use of the capabilities of CHEOP eligible, however • 3-axis stabilised, “payload in the loop” targets on the GTO target list are blocked. to provide < 4 arcsec (rms) pointing - Proposals evaluated by an independent ESA-appointed Time Allocation stability. Committee (TAC), selected based on scientific merit and applicability of CHEOPS. - To allow newly discovered sources to be observed by Community, up to 25% • Design compatible with wide range of Left: White light PSF measured over 500 - 800 nm waveband during the on-ground of the GO time will be available via Discretionary Programme that can be launcher environments. The Intgrated CHEOPS flight hardware. applied to at any time of year. Opens shortly after launch. Credit: Airbus Defence and Space Spain. calibration campaign (x- and y-axes in pixels relative to bottom lower left pixel in a 200x200 pixel image frame, colour scale indicates fraction of total power in an individual pixel); Right: Cuts through the PSF at the specified value of x. Credit: University of Bern. • Same proprietary period applies for GTO data, and GO data from annual AOs. - 1 year after last visit of a given observation request has been made and Mission Profile: declared complete; will not exceed a period of 1.5 years that starts from time of Detector: successful completion of first visit of observation request. • Sun-synchronous orbit (~100 mins): • Single CCD 4720 (): back-illuminated, thinned, operating in - Proprietary time for Discretionary Programme component of GO up to that of -dusk (6 am), 700 km altitude. advanced inverted mode to minimise dark current. standard, annual call. • Shared launch on from ; • 13 micron square pixels, 1024 x 1024 pixel full-frame array, • All CHEOPS data reduced using pipeline running at Science Operations completion of satellite-level tests end frame transfer. Centre (SOC) in Geneva. Data accessed via CHEOPS archive at SOC. 2018, launch in 2019. • Cooled to -40 deg C, thermally stabilised to 10 mK. • Mission Operations Centre (MOC) - • Observations scheduled according to priorities set by the TAC (GO) and the INTA (Torrejòn, ES). Operations: Science Team (GTO), respecting the 20%:80% split between GO and GTO. • Science Operations Centre (SOC) - • Pointed observations of single targets, with the field of view rotating - Award of observing time does not guarantee that observations will be executed due to complexities of scheduling large numbers of time-critical observations. (CH). around the pointing centre. • 1 minute sampling cadence (eg. 200 x 200-pixel sub-frame rate), • 2-month commissioning period, 3.5 • Tools and documentation to support Guest Observers in proposal cadence of additional imagettes (eg. 15-pixel radius) can be up to one years nominal science operations preparation/submission and use of CHEOPS provided by the CHEOPS every few seconds. (goal: 5 years). Operational orbit of CHEOPS, on the Mission Consortium and ESA. day-night terminator. Credit: ESA. • Maximum exposure time of 60 s. • Standard ultrabright, bright and faint modes to cover wide target • Community support provided by ESA Project Scientist. range.