Euclid Euclid OU-SIR / OU-SPE Simulation needs P. Franzetti - - PowerPoint PPT Presentation

Euclid Euclid OU-SIR / OU-SPE Simulation needs

• P. Franzetti

&

• B. Garilli

Euclid Euclid

Why simulated data

Each OU-SIR/OU-SPE WPs requires

• testing of existing tools to Euclid data
• and/or adaptation of existing tools to Euclid data
• and/or development of new ‘classical’ tools
• and/or development of innovative tools

How much can we re-use? How much do we need to develop from scratch? ONLY simulated data can answer to THESE questions

Euclid Euclid

TIMELINE

Timeline (from SIP) June 2014: delivery of pipeline Bread Board Model (2 years from now) November 2015: delivery of pipeline Demonstration Model Given the unknown amount of development required time is not

• verabundant, work on algorithms has to start NOW!

Even if the input of each WP is essentially the output of the previous WP, WPs cannot start their work sequentially they have to proceed in parallel, Simulated data are needed NOW

Euclid Euclid

OU-SIR Relevant WPs

• Basic Processing
• Spectra Identification
• Background Subtraction
• De-contamination
• Calibrations
• Extraction

A survey of needs has been made c/o WP managers The input of each WP is essentially the output of the previous WP, but WPs cannot start their work sequentially, they have to proceed in parallel, so globally the simulation needs are the sum

• f all inputs

Euclid Euclid

OU-SIR Required data

2D “RAW DATA” N pointings with simulated data for all the detectors and dithers (i.e. 16*4 images per pointing)

• 0th and 1st orders spectra
• higher orders spectra (2nd, -1st … )

with various contributions (that can be added or excluded)

• Signal noise
• Sky background
• Dark
• Flat-field
• Bad pixels and detector cosmetics effects
• Cosmic rays

RED: NOW GREEN: SPRING 2013

Euclid Euclid

OU-SIR Required data

CALIBRATIONS

• Instrument Model
• Optics
• Distorsions
• Dispersion relation
• FPA description
• Detectors characteristic (RON, QE)
• PSF
• Dark images
• Flat images
• Calibration fields (as 2D raw data)

RED: NOW GREEN: SPRING 2013

Euclid Euclid

OU-SIR Required data

OBJECTS CATALOG

• Input catalog
• alpha,delta
• redshift
• spectral type
• lines fluxes and ew
• shape parameters (rdisk, rbulge, axratio,pa)
• VIS,J,H,K magnitudes
• “Processed” catalogs J, H, K, J+H+K (+ direct images)
• “real” detection procedure
• grism re-positioning errors
• OU-MER data

RED: NOW GREEN: SPRING 2013

Euclid Euclid

OU-SIR Data Size

9 pointings, i.e. a contiguous area of ~ 4.4 sq deg (3x3 pointings) 25 sq degrees

RED: NOW GREEN: SPRING 2013

Euclid Euclid

OU-SPE Relevant WPs

• Spectra Combination
• Lines Identification and Redshift Measurement
• Spectral Features Measurement
• Redshift Quality Determination
• Rest-frame Parameters
• Spectro-photometric Classification
• A survey of needs has been made c/o WP managers

The input of each WP is essentially the output of the previous WP, but WPs cannot start their work sequentially, they have to proceed in parallel, so globally the simulation needs are the sum of all inputs

Euclid Euclid

OU-SPE Required data

Data kind Notes

• bserved 1D spectra

contamination free 1/grism/roll

• bserved 2D spectra

1/grism/roll

• bserved 1D spectra,

contamination free Combined all grisms all rolls

• bserved 2D spectra

Combined all grisms all rolls error spectrum Contamination mask source infos as from simulations input catalog Line flux, redshift, mag, galaxy type…..

• bserved uncontaminated

spectrum Can be replaced by incident spectrum photometric redshift Or photoz uncertainty and %

• f catastrophs per

redshift bin

Euclid Euclid

OU-SPE size required and time scales

Algorithms have to be tested with meaningful statistics (statistical uncertainties less than 5%) i.e. ~ 1000 galaxies For each

• redshift bin : e.g. z bin of width 0.1 between 0.7 and 2, and 0.25

below and above (up to z=4) i.e. ~20 bins

• galaxy type: emitter/non emitter i.e. 2 bins
• line fluxes bin: e.g. <1,1-3,3-4,4-6,6-8,8-12,>12 e-16 erg/cm2/

s i.e. 12 bins 20x2x12~500 bins x1000 galaxies per bin= ~500k spectra Assuming a galaxy density of the order of 20k gals per sq.deg Simulations of ~ 25 sq. deg. are required 1/10 of it (2.5 sq.deg.) is enough to begin work. Larger areas will be needed in 6/9 months time

Euclid Euclid

Additional requirements

What listed before applies to the Wide survey ONLY (products, sizes etc) Something similar (same products) should also be made available for the DEEP survey, rescaling areas accordingly (1 full square degree), on a slightly longer time scale (end of 2013) Also to be considered in the near future are special needs for rare

• bjects

EXAMPLE: Surface density of QSOs or primeval galaxies is very low. In order to study what Euclid can do, we need dedicated simulations in which the surface densities of these objects is artificially increased by some order of magnitude, so that meaningful statistics can be collected with a moderately small simulation This will be the subject of more detailed requirements in the near future (if OU-SIM has dead lines for this topic, please say so now)

Euclid Euclid

Note about EMA, DataModel etc

OU’s in general, and OU-SIR/SPE in particular, does NOT need a working EMA or an established Data model to start algorithms development and testing Nor OUs should worry about EMA etc, that is a task for SDCs Instead OU-SIR/SPE (all OU’s?) NEED simulated data NOW A provisional way to generate and distribute simulated data should be put in place

Euclid Euclid

Who?

OU-SIR/OU-SPE does NOT have a dedicated WP to provide simulated data The NISP Science Simulation group cannot provide 25 sq. deg

• Not large enough input catalog (not even for 2.5 sq. deg)
• Not enough computer power
• No disk storage
• No manpower to produce the required data products (2 people in

total, also with other responsibilities)

Euclid Euclid

Who?

Also OU-SIM does NOT have dedicated WPs to provide some of these data; just one WP for pixel simulation New WPs ?

• pixel level simulation
• reduction level simulation
• final spectra simulation