An update on Archeops Jacques Delabrouille on behalf of the - - PowerPoint PPT Presentation

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An update on Archeops Jacques Delabrouille on behalf of the - - PowerPoint PPT Presentation

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An update on Archeops Jacques Delabrouille on behalf of the Archeops Collaboration JENAM, September 5th, 2002 Porto (Portugal) Archeops An update on Archeops 2 The Archeops collaboration France CESR, CRTBT, CSNSM, IAP, IAS, ISN, LAL,

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SLIDE 1

An update on Archeops

Jacques Delabrouille

  • n behalf of

the Archeops Collaboration

JENAM, September 5th, 2002 Porto (Portugal)

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SLIDE 2

An update on Archeops 2

Archeops

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SLIDE 3

An update on Archeops 3

The Archeops collaboration

  • France
  • Italy
  • U.K.
  • U.S.A.

CESR, CRTBT, CSNSM, IAP, IAS, ISN, LAL, LAOG, PCC/CdF, OMP, SPP/CEA

  • Univ. La Sapienza (Rome), IROE CNR

QMW CALTECH, JPL, Univ. Of Minnesota

http://www.archeops.org

  • Russia

Landau Ins. of Theoretical Physics

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SLIDE 4

An update on Archeops 4

Outline

  • The Archeops concept
  • The instrument
  • Archeops flights
  • Data and processing pipelines
  • Science with Archeops data
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SLIDE 5

An update on Archeops 5

Outline

  • The Archeops concept
  • The instrument
  • Archeops flights
  • The data and the processing pipelines
  • Science with Archeops data
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SLIDE 6

An update on Archeops 6

Published CMB spectrum data

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SLIDE 7

An update on Archeops 7

The Archeops concept

  • Large sky coverage : 20-30%
  • High angular resolution : ~ 8-12 arcmin

Constraints on low ! (>10) Constraints on high ! (<800)

  • Concept similar to Planck HFI
  • Dilution cryostat cooling bolometers to 100 mK
  • Spider web bolometers
  • Off-axis Gregorian telescope
  • Scanning the sky along large circles

Testbed for Planck

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SLIDE 8

An update on Archeops 8

The Archeops gondola

  • 1.5 meter primary
  • Altitude : 30-40 km
  • Elevation : 41°
  • Rotation speed : 2 rpm
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SLIDE 9

An update on Archeops 9

Scan strategy

Objective : a 24-hour flight during the arctic night

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SLIDE 10

An update on Archeops 10

The Archeops concept (cont’d)

  • 22 bolometers
  • Multiband photometer
  • 4 frequency bands : 143, 217, 353, 545 GHz

Good redundancy foreground sep.

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SLIDE 11

An update on Archeops 11

Outline

  • The Archeops concept
  • The instrument
  • Archeops flights
  • The data and the processing pipelines
  • Science with Archeops data
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SLIDE 12

An update on Archeops 12

Archeops

(ready to fly)

Stellar sensor Main baffle Crash pads Cryostat Magnetometer Battery box

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SLIDE 13

An update on Archeops 13

  • Helium tank at T= 4.2K
  • Open circuit dilution fridge

– Similar to that built for Planck – 3He et 4He tanks – Mixture pumped with a charcoal pump – Temperature reached : 75 mK

  • Big input window (Ø 160mm)

– First stage cooled to about 10K with4He vapour (7.5K during flight) – Flexible polypropylene window – Protection valve opening only at low outside pressure

The!ARCHEOPS cooling system

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SLIDE 14

An update on Archeops 14

The focal plane

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SLIDE 15

An update on Archeops 15

Bolometers

  • Spider Web bolometers
  • Low heat capacity
  • Large photon collecting area
  • Little sensitivity to cosmic rays

(Mauskopf et al.Appl. Opt., 36, 1997)

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SLIDE 16

An update on Archeops 16

Archeops horns

QMW horns

  • Back to Back corrugated horns

(QMW) on the 10 K stage

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SLIDE 17

An update on Archeops 17

Archeops baffling system

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SLIDE 18

An update on Archeops 18

  • Stellar sensor

– ‘!Small!’ (40cm) optical telescope with a photodiode array (Italy) – Stars identified a posteriori with a dedicated matching software (LAL)

  • Additional information: GPS, gyroscopes, magnetometer

– The GPS gives balloon position (longitude, latitude, altitude) – The gyroscopes give the rotation speed and pendulation – The magnetometer gives phase information (magnetic north)

Pointing and attitude monitoring

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SLIDE 19

An update on Archeops 19

Outline

  • The Archeops concept
  • The instrument
  • Archeops flights
  • Data and processing pipelines
  • Science with Archeops data
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SLIDE 20

An update on Archeops 20

Trapani Test flight

From Trapani (Sicily) to Granada (Spain) 6 bolometers in the focal plane

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SLIDE 21

An update on Archeops 21

Test flight from Trapani

July 1999

  • 4 hours of night-time data
  • 4 bolometers worked well

(143, 217, 353 GHz)

  • On board recorder OK
  • Cryostat OK
  • Stellar sensor OK
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SLIDE 22

An update on Archeops 22

Scientific flights

  • Two campains
  • december 2000 - january 2001
  • december 2001 - january 2002
  • During Arctic night

Long duration

  • From ESRANGE (SSC, CNES)

base near Kiruna (Sweden)

  • To somewhere in Northern Russia...
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SLIDE 23

An update on Archeops 23

Getting ready : ARCHEOPS ground calibration

Sensitivity measurements Mirror alignment

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SLIDE 24

An update on Archeops 24

Gondola supported by auxiliary balloons (and held by the Archeops team !)

Launch with auxiliary balloons

Filling the main balloon

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SLIDE 25

An update on Archeops 25

Launch !!!

!

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SLIDE 26

An update on Archeops 26

  • Requirements to fly :

– Not too much wind on ground ( < 2 m/s ) – Not too much snowing (avoid filling the mirror with snow !) – Stratospheric winds towards east and not too strong – Moon, Sun to be avoided, Jupiter to be seen – Agreements and contracts with Russians signed...

  • Four flights from Kiruna :

Archeops flights from Kiruna

12 january 2001 // Problem with a flow-meter 29 january 2001 7h low altitude because of excessive winds 19 january 2002 2h Balloon valve blocked 7 february 2002 19h 12.5 h of excellent night-time data

Flight duration at ceiling ! Date!

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SLIDE 27

An update on Archeops 27

  • Early failure of a flow rate meter
  • Quick landing in Finland

First Flight january 12th 2001

Fast recovery ...

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SLIDE 28

An update on Archeops 28

First Scientific Flight (KS1)

  • from the ESRANGE base

(SSC, CNES) in Kiruna (Sweden)

  • to Syktyvkar (Russia)

Ceiling altitude : 31.5 km

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SLIDE 29

An update on Archeops 29

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SLIDE 30

An update on Archeops 30

Archeops coverage (KS1 flight)

temperature always < 100 mK during the 7.5 hours of scientific data 22 bolometers on board: 8 143 GHz 6 217 GHz 6 353 GHz 2 545 GHz

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SLIDE 31

An update on Archeops 31

Balloon launched at 12h44 UT February 7th Balloon landed at 10h20 UT February 8th

Landing close to Noril’sk (Siberia)

Ceiling altitude: 34 km

Third Scientific Flight (KS3)

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SLIDE 32

An update on Archeops 32

February 2002 flight : sky coverage

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SLIDE 33

An update on Archeops 33

Archeops coverage (Kiruna, 7 february 2002) 12.5 hours of night data at ceiling

+ 6.5 hours during the day 21 bolometers on board: 8 @ 143 GHz 6 @ 217 GHz 6 @ 353 GHz 1 @ 545 GHz

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SLIDE 34

An update on Archeops 34

Outline

  • The Archeops concept
  • The instrument
  • Archeops flights
  • The data and the processing pipelines
  • Science with Archeops data
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SLIDE 35

An update on Archeops 35

Data processing pipeline

  • Cleaning the data
  • Pointing reconstruction
  • Calibration
  • Map-making
  • Component separation
  • Cl spectrum estimation
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SLIDE 36

An update on Archeops 36

A look at Archeops timelines

Archeops signal Dipole signal Independent calibration on the dipole, on Galaxy crossings, and on Jupiter 5 minutes

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SLIDE 37

An update on Archeops 37

  • Very low frequencies (1 minute to 1 hour)
  • Correct for slow gain drifts
  • Decorrelate slow signals proportional to airmass!(altitude , elevation)
  • Decorrelate 0.1K, 1.6K 10K temperature fluctuations
  • High frequency (1 - 100 Hz)
  • Remove cosmic-ray hits (glitches)
  • Remove correlated EM noise
  • Remove microphonic bursts
  • Remove noise synchronous with acquisition frequency
  • A spinning frequency (30 sec)
  • separate!ozone cloud emission using multi-band data
  • Flag all bad data

Data cleaning

Macias-Perez, Madet, Filliatre, Renault, Désert et al.

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SLIDE 38

An update on Archeops 38

Azimuth (arcmin) Elevation (arcmin) Beam shape and focal plane geometry reconstructed using Jupiter crossings

Pointing

Position from GPS, attitude reconstruction using stellar sensor data (matched with a catalog of known stars)

Couchot, Bourrachot et al., Hamilton, Versillé, et al.

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SLIDE 39

An update on Archeops 39

Calibration

217 GHz

About 20% systematic discrepancy between methods still being investigated Final absolute calibration error expected to be better than ~ 5%

Lagache et al., Désert et al., Benoit et al.

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SLIDE 40

An update on Archeops 40

MAIN ISSUE Residual low frequency drifts below ~1 Hz + insufficient scan crossings lead to significant striping SOLUTIONS Method 1 : strong filtering followed by weighted co-addition Method 2 (MAPCUMBA) : multi-resolution implementation of optimal map making Method 3 (MIRAGE) : a combination of filtering and optimal map making

Map making

Yvon, Mayet et al., Teyssier, Prunet, Doré, Vibert et al.

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SLIDE 41

An update on Archeops 41

THREE METHODS

  • MASTER method (Hivon et al.) :
  • Use sub-optimal maps obtained by filtering and co-addition
  • Use maps only from the best tree bolometers (1-143 & 2-217)
  • Make a stringent galactic cut (use only b>30°)
  • Correct for filtering effects on Cl by Monte-Carlo methods
  • Optimal Map method :
  • Make optimal maps with e.g. MAPCUMBA
  • Cl estimation on maps with, e.g. SPICE (Szapudi et al.)
  • Blind spectral matching method

Power spectrum extraction

NEW ! Current baseline... In progress Amblard et al. Vibert, Doré,Prunet et al. Patanchon et al.

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SLIDE 42

An update on Archeops 42

LINEAR MODEL : each detector’s map is a linear superposition of a number of components (sources)

Blind spectral matching method

yd(k) = Adc. sc(k) + nd(k)

maps (alm) for detectors d unknown maps

  • f components c

Unknown noise maps unknown mixing matrix Cardoso et al.

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SLIDE 43

An update on Archeops 43

Blind spectral matching method (cont!’d)

<yy†> = A <ss†> A† + <nn†>

  • Find by minimising the mismatch between Y and ASA† + N
  • the mixing matrix A
  • a band-power parameterised model of S
  • a white noise model of N

The data autocorrelation can be written as

Y = ASA† + N

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SLIDE 44

An update on Archeops 44

Component separation s = [A†N-1A + S-1]-1 A†N-1 y

Knowing A, S and N, the best estimated component maps are obtained by Wiener filtering :

This can be done using estimated values of A, S and N obtained by spectral matching (blind component separation)

^

Patanchon et al. Bouchet et al.

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SLIDE 45

An update on Archeops 45

Outline

  • The Archeops concept
  • The instrument
  • Archeops flights
  • The data and the processing pipelines
  • Science with Archeops data
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SLIDE 46

An update on Archeops 46

Half of the galactic plane mapped at 143, 217, 353 and 545 GHz Constraints on foreground polarisation at 353 GHz CMB fluctuations detected ! Good measurement of the CMB power spectrum in the l=10-800 range

Science with Archeops data

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SLIDE 47

An update on Archeops 47

First-order KS3 maps around Galactic plane

143 GHz 217 GHz 353 GHz 545 GHz Maps covers 1/3 of the galactic plane

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SLIDE 48

An update on Archeops 48

NB :

  • Non-optimal version of the pipeline
  • No Wiener filtering

Comparison 143-217 GHz (best detectors)

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SLIDE 49

An update on Archeops 49

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SLIDE 50

An update on Archeops 50

Preliminary blind separation results

far from galactic plane, high-redundancy region Two-component separation using 18 maps (143-353 GHz)

  • One of the recovered components is

compatible with CMB (frequency channel dependence flat in units of !KCMB, power spectrum displaying a clear peak at l~200)

  • The other component is correlated

detector noise (essentially low-level residual stripes)

  • No detectable galactic foreground

contamination in this region at this stage Wiener filtered recovered component map about 40 deg.

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SLIDE 51

An update on Archeops 51

Component 1 Component 2 Component 3

Preliminary KS3 component maps

  • btained by blind separation with Wiener filtering

Patanchon et al.

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SLIDE 52

An update on Archeops 52

Component 1

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SLIDE 53

An update on Archeops 53

Component 2

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SLIDE 54

An update on Archeops 54

Component 3

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SLIDE 55

An update on Archeops 55

Estimated Cl sensitivity

Full optimal processing with actual noise levels Present processing on 3 best bolometers with the MASTER method (to be published soon)