Euclid Mission: Survey Model Consortium J. Amiaux, R. Scaramella, - - PowerPoint PPT Presentation

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Euclid Mission: Survey Model Consortium J. Amiaux, R. Scaramella, - - PowerPoint PPT Presentation

Jun 09, 2023 364 likes •846 views

Euclid Euclid Mission: Survey Model Consortium J. Amiaux, R. Scaramella, Y. Mellier, B. Altieri, C. Burigana, A. Da Silva, P. Gomez, J. Hoar, R. Laureijs, E. Maiorano, D. Magalhes Oliveira, F. Renk, G. Saavedra Criado, I. Tereno, J.L.

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:1

Euclid Consortium

  • J. Amiaux, R. Scaramella, Y. Mellier, B. Altieri, C. Burigana, A. Da Silva, P. Gomez, J. Hoar, R. Laureijs, E.

Maiorano, D. Magalhães Oliveira, F. Renk, G. Saavedra Criado, I. Tereno, J.L. Auguères, J. Brinchmann, M. Cropper, L. Duvet, A. Ealet, P. Franzetti, B. Garilli, P. Gondoin, L. Guzzo, H. Hoekstra, R. Holmes, K. Jahnke,

  • T. Kitching, M. Meneghetti, W. Percival, S. Warren, and the Euclid collaboration

Euclid Mission: Survey Model

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:2

Euclid Consortium

What is Reference Survey?

Survey used to demonstrate feasibility of Mission Top Level Science Requirements:

  • 15 000 square degrees Wide survey + 40 square degrees Deep Survey
  • 30 galaxies / arcmin² in imaging for Weak Lensing
  • 3500 galaxies / deg² in spectroscopy for Galaxy Clustering

2 instruments – 3 modes:

  • Visible Imaging
  • NIR Photometry
  • NIR Spectroscopy

Wide Field observations > 0.5 square degrees Step and Stare mode: 4500 s per fields Observe « Best Square Degrees » to limit

  • Extinction
  • Zodiacal Light
  • Star Density
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OUSIM / Barcelona iss 1.0 10/07/12 – VG:3

Euclid Consortium

What is Reference Survey?

Survey used to demonstrate feasibility of Mission Top Level Science Requirements:

  • 15 000 square degrees Wide survey + 40 square degrees Deep Survey
  • 30 galaxies / arcmin² in imaging for Weak Lensing
  • 3500 galaxies / deg² in spectroscopy for Galaxy Clustering

2 instruments – 3 modes:

  • Visible Imaging
  • NIR Photometry
  • NIR Spectroscopy

Wide Field observations > 0.5 square degrees Step and Stare mode: 4500 s per fields Observe « Best Square Degrees » to limit

  • Extinction
  • Zodiacal Light
  • Star Density

E(b-v)<0.08 Core Preferred Area

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SLIDE 4

OUSIM / Barcelona iss 1.0 10/07/12 – VG:4

Euclid Consortium

What is Reference Survey?

Survey used to demonstrate feasibility of Mission Top Level Science Requirements:

  • 15 000 square degrees Wide survey + 40 square degrees Deep Survey
  • 30 galaxies / arcmin² in imaging for Weak Lensing
  • 3500 galaxies / deg² in spectroscopy for Galaxy Clustering

2 instruments – 3 modes:

  • Visible Imaging
  • NIR Photometry
  • NIR Spectroscopy

Wide Field observations > 0.5 square degrees Step and Stare mode: 4500 s per fields Observe « Best Square Degrees » to limit

  • Extinction
  • Zodiacal Light|
  • Star Density

GAL lat>|25|

ECL lat>|15| Core Preferred Area E(b-v)<0.08

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SLIDE 5

OUSIM / Barcelona iss 1.0 10/07/12 – VG:5

Euclid Consortium

What is Reference Survey?

Survey used to demonstrate feasibility of Mission Top Level Science Requirements:

  • 15 000 square degrees Wide survey + 40 square degrees Deep Survey
  • 30 galaxies / arcmin² in imaging for Weak Lensing
  • 3500 galaxies / deg² in spectroscopy for Galaxy Clustering

2 instruments – 3 modes:

  • Visible Imaging
  • NIR Photometry
  • NIR Spectroscopy

Wide Field observations > 0.5 square degrees Step and Stare mode: 4500 s per fields Observe « Best Square Degrees » to limit

  • Extinction

E(b-v)<0.08

  • Zodiacal Light

ECL lat>|15|

  • Star Density

GAL lat>|25|

GAL lat>|25| Core Preferred Area ECL lat>|15| E(b-v)<0.08

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SLIDE 6

OUSIM / Barcelona iss 1.0 10/07/12 – VG:6

Euclid Consortium

What is Reference Survey?

Survey used to demonstrate feasibility of Mission Top Level Science Requirements:

  • 15 000 square degrees Wide survey + 40 square degrees Deep Survey
  • 30 galaxies / arcmin² in imaging for Weak Lensing
  • 3500 galaxies / deg² in spectroscopy for Galaxy Clustering

2 instruments – 3 modes:

  • Visible Imaging
  • NIR Photometry
  • NIR Spectroscopy

Wide Field observations > 0.5 square degrees Step and Stare mode: 4500 s per fields Observe « Best Square Degrees » to limit

  • Extinction

E(b-v)<0.08

  • Zodiacal Light

ECL lat>|15|

  • Star Density

GAL lat>|25|

GAL lat>|20| Extended Preferred Area E(b-v)<0.15 ECL lat>|15|

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:7

Euclid Consortium

What is Reference Survey?

Survey used to size the spacecraft within Mission Constraints Main Mission Constraints:

  • 6 years mission
  • Mass / Volume Compatible with Soyouz Launcher
  • Limited Solar Aspect Angle variation to ensure high thermal Mechanical Stability
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OUSIM / Barcelona iss 1.0 10/07/12 – VG:8

Euclid Consortium

Observation Constraints

Spacecraft Constraints: Solar Aspect Angle variation: +0° to +10°

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:9

Euclid Consortium

Observation Constraints

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:10

Euclid Consortium

Observation Constraints

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:11

Euclid Consortium

Observation Constraints

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:12

Euclid Consortium

Observation Constraints

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:13

Euclid Consortium

Observation Constraints

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:14

Euclid Consortium

Observation Constraints

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:15

Euclid Consortium

Associated Performance

WL GC

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:16

Euclid Consortium

Main Survey: year 1

Euclid Sky Survey Planning Tool developped by ESAC

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:17

Euclid Consortium

Main Survey: year 2

Euclid Sky Survey Planning Tool developped by ESAC

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:18

Euclid Consortium

Main Survey: year 3

Euclid Sky Survey Planning Tool developped by ESAC

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:19

Euclid Consortium

Main Survey: year 4

Euclid Sky Survey Planning Tool developped by ESAC

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:20

Euclid Consortium

Main Survey: year 5

Euclid Sky Survey Planning Tool developped by ESAC

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:21

Euclid Consortium

Main Survey: year 6

Euclid Sky Survey Planning Tool developped by ESAC

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:22

Euclid Consortium

Survey Covered area

After 5.5 years:

  • 15 500 square degrees covered
  • 14 500 square degrees on the « core preferred area »
  • This include all required calibrations (~15% of survey time)
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OUSIM / Barcelona iss 1.0 10/07/12 – VG:23

Euclid Consortium

Calibrations fields

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:24

Euclid Consortium

Calibrations fields

Monthly dense star field Allocation for VIS PSF calibration

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:25

Euclid Consortium

Calibrations fields

Allocation for NISP spectroscopy wavelength calibration Planetary Nebulae:

  • Twice a year

Open Cluster:

  • Once a year
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OUSIM / Barcelona iss 1.0 10/07/12 – VG:26

Euclid Consortium

Calibrations fields

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:27

Euclid Consortium

Calibrations fields

Allocation for NISP spectroscopy photometric calibration HST standard stars or reference transfered to the Deep Field:

  • Twice a year
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OUSIM / Barcelona iss 1.0 10/07/12 – VG:28

Euclid Consortium

Calibrations fields

Deep Field North allocation 20 square degrees with 40 revisits

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:29

Euclid Consortium

Calibrations fields

Allocation for HST field visit (VIS color gradient calibration)

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:30

Euclid Consortium

Calibrations fields

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:31

Euclid Consortium

Calibrations fields

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:32

Euclid Consortium

Calibrations fields

Deep Field South allocation 20 square degrees with 40 revisits

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:33

Euclid Consortium

Calibrations fields

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:34

Euclid Consortium

Calibrations fields

Allocation for 2 additional HST fields (VIS color gradient calibration)

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:35

Euclid Consortium

Calibrations fields

NIR Photometry Cross calibration (relative photometry) Monthly revisit of same field at Northern Ecliptic Pole

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:36

Euclid Consortium

Field Sequence

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:37

Euclid Consortium

Field Sequence

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:38

Euclid Consortium

Field Sequence

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:39

Euclid Consortium

Field Sequence

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:40

Euclid Consortium

Field Sequence

Main Reference Survey composed of ~41 500 field observations

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:41

Euclid Consortium

Field Sequence

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Euclid Consortium

Field Sequence

Each field will be > 0.5 square degrees

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:43

Euclid Consortium

Field Sequence

Each field will be > 0.5 square degrees

Frame 01 Frame 02 Frame 03 Frame 04 Dither 01 Dither 02 Dither 03 Slew To Next Field

75 s 75 s 75 s 35O s

VIS NISP

Shutter 10 s NISP S 565 s VIS 565 s Shutter 10 s FWA 10 s Y 121 s FWA 10 s J 116 s FWA 10 s H 81 s GWA 10 s

Frame = 973 s

Stab 10 s Stab 10 s Stab 10 s

Reference Case = 4 x 973 s + 3 x 75 s + 350 s = 4467 s

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:44

Euclid Consortium

Field Sequence

Integration time map for observed fields with dithering pattern VIS:

  • >95% of pixels sees at least 3 frames
  • 50% of pixels sees more than 4 frames
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OUSIM / Barcelona iss 1.0 10/07/12 – VG:45

Euclid Consortium

Field Sequence

Integration time map for observed fields with dithering pattern VIS:

  • >95% of pixels sees at least 3 frames
  • 50% of pixels sees more than 4 frames
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OUSIM / Barcelona iss 1.0 10/07/12 – VG:46

Euclid Consortium

Solar Aspect Angle Variation

This will contribute to the PSF variation along the survey The Opto-mechanical PSf can be related to history f pointing

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OUSIM / Barcelona iss 1.0 10/07/12 – VG:47

Euclid Consortium The reference survey will be updated before end of year Tools are being upgraded and developped There is Survey group: Italy + France + Portugal + ESA This group can evaluate scenario and provide the Survey Model