The eROSITA X-ray Survey Telescope

The eROSITA X-ray Survey Telescope
The eROSITA X-ray Survey Telescope
Vadim Burwitz
Max-Planck-Institut für extraterrestrische Physik, Germany
On behalf of the eROSITA Team
2014 September 25, The International Center Goa, India
Spektr-Rentgen-Gamma
eROSITA
(MPE/D)
ART-XC
(IKI/Ru)
Pavlinsky et al, 9144-65
Gubarev et al., 9144-66
Navigator
(Lavochkin Ass.)
Fregat-SB Booster
Vadim Burwitz, ICG, Goa, India 2014-09-25
Spektr-Rentgen-Gamma
Launch from Baikonur with Zenit-Fregat, 2016 (March 26)
- 3 months: flight to L2, verification and calibration phase
- 4 years: 8 all sky surveys (scanning mode: 6 rotations/day, 1 degree advance per day)
- 3 years: pointed observation phase, including ~20% of GTO. 1 AO per year
Vadim Burwitz, ICG, Goa, India 2014-09-25
L2 insertion orbit, correction burns
Vadim Burwitz, ICG, Goa, India 2014-09-25
Sky Division
IKI/Ru
MPE/D
Vadim Burwitz, ICG, Goa, India 2014-09-25
Data Rights and Policies (MPE)
• German eROSITA data made public after 2 yr proprietary period
• Periodic data releases envisaged (e.g. 6, 24, 48 months)
• Proprietary data via eROSITA_DE collaboration (consortium)
• Projects/Papers regulated by Working Groups
• Individual External Collaborations
• Group External Collaborations
Science Working Groups:
Clusters and Cosmology
AGN, Blazars
Normal Galaxies
Compact objects
Diffuse emission, SNR
Stars, Solar System
Infrastructure Working Groups:
Time Domain Astrophysics
Data analysis, source extraction, catalogs
Multi-wavelength follow-up
Calibration
Background
Vadim Burwitz, ICG, Goa, India 2014-09-25
Redshift from Surveys
Ru
split
D
Vadim Burwitz, ICG, Goa, India 2014-09-25
eROSITA Collaboration
Core Institutes (DLR funding):
MPE, Garching/D
Universität Erlangen-Nürnberg/D
IAAT (Universät Tübingen)/D
SB (Universität Hamburg)/D
Leibniz Institut für Astrophysik Potsdam/D
Associated Institutes:
MPA, Garching/D
IKI, Moscow/Ru
USM (Universität München)/D
AIA (Universität Bonn)/D
Industry:
Media Lario/I
Mirrors, Mandrels
Kayser-Threde/D Mirror Structures
Carl Zeiss/D
ABRIXAS-Mandrels
Invent/D
Telescope Structure
pnSensor/D
CCDs
IberEspacio/E
Heatpipes
RUAG/A
Mechanisms
HPS/D,P
MLI
Moog/USA
Valves
MAP/F
Painting
Laserjob/D
X-ray Baffles
NPOL/Ru
Spacecraft, Mission
+ many other (small) companies
MPE: Scientific Lead Institute, Project Management
Instrument Design, Manufacturing, Integration & Test
Data Handling & Processing, Archive etc.
eROSITA
Telescope Front Cover
2 Star Sensors
7 X-ray Baffles
7 Mirror Modules
2 Sun Sensors
7 Electron Deflectors
2 Camera Cooling Radiators
7 Filter-Wheels
7 CCD-Cameras
7 Camera Electronics
2 Control Electronics
Hexapod = I/F with S/C
2 E-Box Cooling Radiators
7 identical Mirror Modules
54 nested Mirror Shells each
7 identical pnCCD Cameras
Field of View
Angular Resolution HEW
Energy Range
Vadim Burwitz, ICG, Goa, India 2014-09-25
1° Ø
~16‘‘ on-axis
~28‘‘ survey
~0.3 - 10 keV
ART-XC & eROSITA
On-axis Effective Area & Grasp
2500 см2 @ 1.4 keV
1100 см2 deg2 @ 1.4 keV
450 см2 @ 8 keV
45 см2 deg2 @ 8 keV
Vadim Burwitz, ICG, Goa, India 2014-09-25
Performance
Effective Area @ 1keV
Angular Resolution (survey)
Spectral Resolution
Field of View
Survey Duration
Pointed Observation Duration
Point sources
eROSITA
2000 cm2
30 arcsec
~100eV
1° Ø
4 years
3 years
ROSAT
350cm2
60 arcsec
~400eV
2° Ø
½ year
1 year +7½ years
Extended sources
Point source sensitivity:
~30 times better than ROSAT (soft band 0.5-2 keV)
~100 times better than HEAO/RXTE (hard band 2-10 keV)
Chandra
~ 30 pointings
~ 2 Msec
eROSITA
~ 1 pointing
~ 80 ksec
Vadim Burwitz, ICG, Goa, India 2014-09-25
Churazov, IKI, MPA
Cluster Cosmology
Design Driving Science
+
WL
+
Vikhlinin et al., 2009
COSMOS Field
XMM-Newton
Wm
WMAP: Spergel et al. 2003
ROSAT: Schuecker et al. 2003
Clusters of galaxies are the largest
gravitationally bound entities in the
universe.
In X-rays we see clusters as one
continuous entity.
Detectability of 100.000 Clusters of Galaxies, z < 1.5:
–
All-sky survey with sensitivity 6×10-14 erg cm-2 s-1
–
Deep survey field(s) (~100 sqdeg) with 1×10-14 erg cm-2 s-1
–
Individual pointed observations
–
Moderate angular resolution (< 28 arcsec, aver. over FoV)
–
–
–
Large collecting area (> 2000 cm2 @ 1keV)
Large FoV (1° Ø)
Long duration (survey 4 years   1/2 year (ROSAT)
Evolution of Cluster Mass Function
court. Churazov/MPA
z=0
z = 0.5
z = 1.4
Number of most massive clusters is extremely sensitive to cosmology
Will eROSITA detect all Clusters?
Vadim Burwitz, ICG, Goa, India 2014-09-25
… and all other Science Targets
Charge Exchange
Cool Stars
Interstellar Dust
Supernova Remnants
~0.7 Mio stars
Vaughan et al., 2003
Lisse et al., 1996
Isolated NS
Aschenbach et al., 1995
SMBH
Tidal Disruption
~3 Mio AGN
Walter et al., 1997
Brusa et al. 2009
Komossa et al., 2006
Vadim Burwitz, ICG, Goa, India 2014-09-25
eROSITA Sensitivity to variables
Vadim Burwitz, ICG, Goa, India 2014-09-25
19
Transient X-ray sources in eROSITA
Vadim Burwitz, ICG, Goa, India 2014-09-25
HW-Status: Overview FM
Telescope Structure, Front Cover incl. Mechanism
MLI
Mirror System
FM-1
FM-2, 3, 4, 5, 6, 7, 8
X-ray Baffle
FM-1, 3, 4, 5, 6, 7, 8, 9
Mirror Assemblies (Mirror + X-ray Baffle)
FM-1, 2, 3, 4, 5, 6, 7, 8
ready, tested (qualified)
ready, some parts to be refurbished
ready with X-ray Baffle, tested (acc, baf, vib, ptv, tel)
ready with X-ray Baffle, tested (acceptance)
ready, integrated on each mirror module
Electron Deflector FM 1-8
E-Box Radiators (2)
Camera Radiators
Heatpipe System Camera
Heatpipe System Electronics
ready, all still need to be calibrated in X-rays together with QM camera
ready, tested (acceptance)
ready, tested (qualified)
ready after modification
Integrated for test
integrated for test next week
Cameras (Meidinger et al. SPIE 8859-10)
CCDs
Detector
Electronics
Interface & Thermal Control Electronics
Harnesses
QM test completed
QM test close to completion
QM close to completion
EM tests in progress
completed
Vadim Burwitz, ICG, Goa, India 2014-09-25
Fürmetz et al, 9144-192
eROSITA CCD Cameras and E-Boxes
Vadim Burwitz, ICG, Goa, India 2014-09-25
CCD Camera Design
completed
completed
Vadim Burwitz, ICG, Goa, India 2014-09-25
Cameras and Electronics
,,,
7×
Filterwheels
CCDs
Cameras
Camera Electronics
60 printed circuit boards
~35.000 electronics components
(radhard, highrel)
Complex Cooling pipe system for 7 CCDs
Vadim Burwitz, ICG, Goa, India 2014-09-25
The eROSITA Mirrors and Calibration
Each of the 8 Mirror Modules (7 FMs and 1 spare)
will go through the following procedure:
• an X-ray acceptance test
– HEW and effective area
• Integration of the baffle unit
• X-ray test after baffle integration
– HEW and effective area
• Environmental tests (thermal cycling and vibration)
• Final calibration tests to measure the:
– PSF on-axis / off-axis in the energy range 0.18 – 8.04 keV
– effective area in the energy range 0.18 – 8.04 keV
– contribution of scattering
Vadim Burwitz, ICG, Goa, India 2014-09-25
The MPE PANTER X-ray Test Facility
•
•
•
The X-ray test Facility
• Length 132 m extendible to 145 m
• Main intrument chamber 3.5 m diameter
• Large cleanroom for handling X-ray optics
Detectors
• PSPC :
Position Sensitive Proportional Counter
• TRoPIC :
Single photon counting CCD camera
• PIXI :
Integrating CCD Camera
X-ray Sources
•
Beam Monitors
• Multi target electron
• Proportional counters
impact source
• Drift Chamber
• Seifert closed X-ray source
•
Manipulators
• X-ray Monochromators
• X, Y, Z translation stages
•
PIXI
TRoPIC
PSPC
Tip-tilt, rotation stages
X-ray
source
13 m
extension
Instrument
Chamber &
Clean Room
Pumping
Station 3
Pumping
Station 2
Pumping
Station 1
28
eROSITA Mirror Development and Testing
Two single mirror units ready for testing.
Demonstrator mirror module with X-ray baffle.
8 12’ 16’
’
Flight mirror module FM3 with 39 Shells
On- and off-axis PSFs for FM1a
X-Ray Baffle Performance
with baffle
without baffle
X-Ray Test (QM)
Vadim Burwitz, ICG, Goa, India 2014-09-25
PSFs of the eROSITA Flight Mirror Modules
Mirrors shells produced and integrated at Media Lario Technologies and the X-ray Baffles at MPE
Photon
energy
Goal
Measurement
FM 1 FM 2
FM 3
FM 4
FM 5
FM6
FM7
FM 8
HEW Al-K
≤15’’
(1.49 keV)
16.1
±0.2
16.8
±0.3
15.7
±0.3
16.0
±0.3
16.2
±0.3
16.3
±0.3
15.6
±0.3
17.0
±0.3
HEW Cu-K
(8.04 keV)
15.2
±0.1
15.4
±0.3
16.7
±0.4
16.3
±0.3
16.2
±0.3
16.2
±0.3
16.6
±0.3
18.4
±0.4
≤
20’’
The of Axis PSF of eROSITA (Survey PSF)
+30
+25
+20
+15
+10
+5
0
-30 -25 -20 -15 -10 -5 0 +5 +10 +15 +20 +25 +30
Half the focal plane scanned In 5 arcmin steps
Vadim Burwitz, ICG, Goa, India 2014-09-25
Single eROSITA telescope in PANTER
Vadim Burwitz, ICG, Goa, India 2014-09-25
Space Simulation with Cooling Shroud
Vadim Burwitz, ICG, Goa, India 2014-09-25
eROSITA „End to End“ Test at PANTER
• The last „end to end test“ of the eROSITA telescope before
delivery to Russia will be performed at PANTER. In this
critical test all systems, both hardware and software, will
be checked out.
• As eROSITA will be placed upright into PANTER the on
board Fe55 calibration sources will be used to illuminate
the CCDs.
• The PANTER X-ray Test Facility is ideally suited for this „end
to end“ test because it is the cleanest large vacuum
chamber available to us for such a test that also provides
the cooling capability for the radiators.
Vadim Burwitz, ICG, Goa, India 2014-09-25
eROSITA Ground Segment
•
•
•
•
•
•
eROSITA Data Centre
Mission Planning
Science Cooperations
Follow-up Observations
Simulation
Calibration
Vadim Burwitz, ICG, Goa, India 2014-09-25
eROSITA data processing pipeline









Vadim Burwitz, ICG, Goa, India 2014-09-25

NRTA & SASS & Catalogues
 NRTA (Near Real Time Analysis)
 SASS (Standard Analysis Software System)
Vadim Burwitz, ICG, Goa, India 2014-09-25
Simulations
ROSAT
eROSITA
Schmid, Clerc, Pace, Roncarelli
Vadim Burwitz, ICG, Goa, India 2014-09-25
Calibration
Vadim Burwitz, ICG, Goa, India 2014-09-25
court. K. Dennerl
Calibration of spatial resolution
Vadim Burwitz, ICG, Goa, India 2014-09-25
Calibration of spectral resolution
Vadim Burwitz, ICG, Goa, India 2014-09-25
eROSITA status Summary
• A sturdy mission emerged after many changes
in the profile at the beginnings
– redesign of electronics, cooling system
orbit change from LEO to L2
• All is set for a delivery to Russia 3rd quarter
2015
• Launch March 26, 2016 from Baikanur
,, India 2014-09-25
Vadim Burwitz, ICG, Goa,
Important Lessons
• Prior to Mission launch Discussions between instrument builders and
future observers should be fomented and pursued.
Creation of Science and Instrument Working Groups on specific topics
(object classes) to optimize the use of the observatory is important (from
eROSITA experience).
• Observers and Theorists should be aware when analysing data that they
should interact with the instrument calibrators to achieve the best solid
results.
Believing in “Black Boxes” is dangerous.
• Cross-calibration between X-ray instruments and other observatories has
to have a high priority
 the IACHEC effort over the last 10 years has led to vast improvements
also providing new standard candles
In 2016 the IACHEC meeting takes place in India
,,
Important Lessons
• Prior to Mission launch Discussions between instrument builders and
future observers should be fomented and pursued.
Creation of Science and Instrument Working Groups on specific topics
(object classes) to optimize the use of the observatory is important (from
eROSITA experience).
• Observers and Theorists should be aware when analysing data that they
should interact with the instrument calibrators to achieve the best solid
results.
Believing in “Black Boxes” is dangerous.
• Cross-calibration between X-ray instruments and other observatories has
to have a high priority
 the IACHEC effort over the last 10 years has led to vast improvements
also providing new standard candles
In 2016 the IACHEC meeting takes place in India
,,

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