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OULE3 - Time Domain Implementation & Validation Phase Isobel Hook Jean-Philippe Beaulieu 1.

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Presentation on theme: "OULE3 - Time Domain Implementation & Validation Phase Isobel Hook Jean-Philippe Beaulieu 1."— Presentation transcript:

1 OULE3 - Time Domain Implementation & Validation Phase Isobel Hook Jean-Philippe Beaulieu 1

2 Euclids time-domain data Euclids deep fields will be observed several times – Of order 40 sq deg, observed ~ 40 times – Cadence TBD – These may or may not be the same as the fields required for calibration of primary science goals Euclids wide survey will have overlap regions between adjacent fields – 1% overlaps (see Red Book) of 15,000 sq deg = 150sq deg – Imaged twice or sometimes more, time separation hours to years… Each exposure is made of 4 dithered frames – Timescale between dithers ~15 minutes Possibly also dedicated time-domain surveys – If survey time/scheduling permit 2

3 Euclids time-domain science Science goals include: – Solar system – Supernovae (Type Ia, II, ultraluminous…) – Exo-planets (detected via microlensing) – Variable QSOs – Other transients (GRBs…?) These are considered legacy science/ secondary cosmology They can drive goals (but not formal requirements on the mission) 3

4 Potential dedicated surveys SNIa cosmology: dedicated survey (6 months or longer) – Of order sq deg, observed ~ 40 times – Cadence of order 4-8 days – Focus on Y,J,H imaging, possibly with non-standard exposure times Euclid microlensing : dedicated survey (ideally 6-10 months) – Fields observable twice a year for 1 month – Continuous 1 month observation period of 3 fields in galactic bulge (17 min cadence) – Monitoring in H band, VIS images every 12 hours 4

5 Implementation WP Summary - Inputs [From v4.0 of WP descriptions] Preliminary EUCLID data on time-ordered images from OUEUC and OU-VIS Preliminary versions of the EUCLID catalogues from OUPHO, OU-SPE and OUMER for object identification [comment: should include external data] Comment: Should also include simulated data! 5

6 Implementation WP Summary - Outputs [From v4.0 of WP descriptions] Algorithms to produce a catalogue of orbital, time and position parameters for transient solar neighborhood objects Algorithms to produce a catalogue of light curves, time, redshift, magnitude parameters for transient supernovaelike objects. A catalogue of any stellar timedependent variation. Algorithms to produce a catalogue of microlensing events 6

7 Implementation WP Summary - Deliverables [From v4.0 of WP descriptions] Documentation describing the algorithms, their implementation and results on the tests. Prototypes of the algorithms for the computation of the catalogues for solar system, stellarlike transient and microlensing catalogues. Example simulated dataset used for the testing of the prototypes. Comment: What about verifying the LE3 data products themselves? 7

8 Implementation WP Summary – List of tasks [paraphrased From v4.0 of WP descriptions] Definition, development and testing of: [Solar system] – algorithms to detect transients – algorithms for cross matching with existing catalogues [Supernovae and other stellar-like transients] – algorithms to detect transients – algorithms for cross matching with existing catalogues [Exoplanets] – algorithms to generate photometry catalogues (image subtraction) – Algorithms to detect microlensing events – Algorithms to detect transiting planets 8

9 WP Summary - List of tasks [From v4.0 of WP descriptions] [Solar system] – Definition, development and testing of algorithms to detect transients ENOs, TNOs, asteroid belts and Trojan objects) in the solar neighbourhood (goal). – Definition, development testing of algorithms for cross matching of ENOs, TNOs, asteroid belts and Trojan objects with existing catalogues (goal). [Supernovae] – Definition, development and testing of algorithms to detect stellarlike transients including supernovae-like transient objects, including but not limited to Type Ia supernovae using externally observed colour and spectroscopic information for light curve fitting and redshift determination (goal). – Definition, development and testing of algorithms for cross matching of detected SNe and stellarlike transients with existing catalogues (goal). [Exoplanets] – Definition, development and testing of algorithms to generate compact body and exoplanet microlensing catalogues (goal). 9

10 Proposed sub-tasks [Example of SN case – based on input from the SN & transients SWG] Start from simulated raw data (see later slide for definition) Develop algorithms to do the following steps – Create an oversampled stacked image as a reference (will be done by OU-MER?) – Register new images to reference – PSF match of new & reference image (accounting for flux ratio) – Subtract images – Detect objects on the subtracted images – Do photometry on the detections – Select real transients based on quality cuts – Match detections with previous catalogues, including other Euclid data and external data – Classify the detections based on various levels of available data – Fit light curves – Enter detection data into a database for further use (including cutouts for visual inspection) 10

11 Proposed sub-tasks [Example of exoplanet case – based on input from exoplanet SWG very close to SN tasks] Start from simulated raw data Develop algorithms to do the following steps – Create an oversampled stacked image as a reference (will be done by OU- MER?) – Register new images to reference – PSF match of new & reference image (accounting for flux ratio) – Subtract images – Detect objects on the subtracted images – Do photometry on the detections – Select real transients based on quality cuts – Classify the detections (microlensing events, variable stars, transiting planets) – Modeling of anomalous microlensing (fitting light curves) 11 Note that there is a need for development of these image subtraction pipelines for both Legacy SN and exoplanets. It is not needed for core science.

12 WP members – old version Others interested : R. Carlberg + C. Pritchet (Canada – not yet in Euclid) - experience in SNe JJ Kavelaars (Canada) – experience in solar system Possibly some members of the SN & transients WG, depending on the boundary of SWG and LE3 work NameFTERelevant experience/interest Isobel Hook0.3 or postdoc (expected) SNe Alain Blanchard0.3 Andrew Jaffe0.1 Lucia Pozzetti0.3 Mark SullivanSNe Remi Cabanac 12

13 Implementation WP members Total FTE committed ~ 0.85FTE. Others interested : – R. Carlberg + C. Pritchet (Canada – not yet in Euclid) - experience in SNe – JJ Kavelaars (Canada) – experience in solar system – Possibly some members of the SN & transients WG, depending on the boundary of SWG and LE3 work(*) * Level of available effort depends on whether there is an interesting SN survey in Euclid! NameFTERelevant experience/interest Isobel Hook postdoc (expected) SNe(*) Pascal Fouque0.3microlensing Andrew Jaffe0.1 Mark Sullivan0.1?SNe(*) Remi Cabanac0.1microlensing on SL quasars 13

14 Implementaton WP Summary - List of tasks [paraphrased From v4.0 of WP descriptions] Definition, development and testing of: [Solar system] – 0.0 FTE – algorithms to detect transients – algorithms for cross matching with existing catalogues [Supernovae and other stellar-like transients] ~ 0.35FTE – algorithms to detect transients – algorithms for cross matching with existing catalogues [Exoplanets] – 0.4 FTE – algorithms to generate catalogues Low level of committed effort is a concern. 14

15 Required simulations Three main scientific areas require simulations: – Solar system (moving objects) – SNe (point-like transients on host galaxies) Include dithered exposures so that oversampled reference image can be created Simulated SNe should have realistic lightcurves, colours, and spatial distribution on host galaxies – Exo-planet microlensing (variable point sources in crowded fields) 15

16 Simulated data requirements Time series of VIS and NISP Y,J,H images (2D) – Possibly with non-standard exposure times and non-standard SAA (if dedicated SN or exoplanet surveys are carried out) – Images should have fake transients added, with realistic properties – Images should be pre-processed (bias corrected, flat fielded and sky subtracted) – Covering an area of ~1 sq deg (?) Simulated NISP spectroscopy of the field (IS THIS NEEDED?) Simulated photo-z catalogue of the field (required for SN case) 16

17 Pipeline requirements [Summary of document sent to legacy science coordinators from SN&T SWG] For transients, the real-time and final reductions have different requirements Not clear whether they will be the same software Real-time pipeline: – Mainly for triggering follow-up. Can be less precise, but must be able to filter out junk (requires colour info, z if available, vignettes for human inspection etc) – Software must be rapidly adaptable. Would not be compatible with long code review process Final reductions – Precision goal of 1% relative PSF photometry [But not for the entire Euclid dataset – only repeat-imaged areas]

18 Validation tasks (Beaulieu et al.) Goal : Validation of the algorithms to obtain catalogues for objects in the time domain for Euclid including solar system transients, supernovae, stellar transients and microlensing events. -Science working groups are setting up goals and requirements. -Implementation WP is proposing a road towards these goals & requirements. -Validation will use these two ingredients. Our approach will be to work closely with the implementation WP. Lets well define the implementation first. Sign in for implementation and/or validation WP. 18

19 The End 19


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