HIGH ENERGY - XMM-Newton Science Operations Centre

Report
Basic scientific idea of eROSITA ….
to extend the ROSAT all-sky survey up to 10 keV
with an XMM-Newton type sensitivity
eROSITA: ready for launch ….
fall of
2011
2009
2010
2014
Mission scenario & Instrument specification
• 3 month calibration & science verification phase
• 4 yrs all-sky survey (8 sky coverages)
• 2.7 yrs pointed observations
• Energy range ~ 0.2 - 10 keV
• FOV: 1 degree
• All-sky survey sensitivity ~ 6 x10-14 erg cm-2 s-1 ~ (10 – 30) x ROSAT
~ 100 x HEAO/RXTE (hard band)
• Deep survey field(s) (~100 sqdeg) with 5×10-15 erg cm-2 s-1
• Temporal resolution ~ 50 ms
• Energy resolution ~ 130 ev @ 6 keV / 80 ev @ 1.5 keV
• Angular resolution ~ 15” (20” survey)
eROSITA on Spectrum-RG
ART-XC
( IKI )
eROSITA ( MPE )
Navigator
(NPO Lavochkin)
Launch from Baikonur with Zenit-Fregat, fall of 2014
Zenit-Fregat-Navigator = standard configuration,
also used for Elektro-L (Jan 2011) and Radiastron (Jul 2011).
eROSITA: Navigator and Booster
Navigator
Fregat
Booster
eROSITA Telescope Array
Mirror Systems
• 7 aligned X-ray mirror modules
• 54 nested gold-coated nickel-shells
• Aeff ~ 2400 cm2 (1 keV, on-axis)
• 7 pn-CCD Cameras
eROSITA: effective area 2400 cm2 @ 1keV
eROSITA: Grasp @ 1keV
eROSITA: Advanced XMM pn-CCD
384 amplifiers
Frame
store
Imaging
– 7 individual cameras
• 256 × 256 pixel, 75µm
• frame store area
• faster read-out
eROSITA pn-CCD flight devices
• 40% reduced out-oftime events
• temporal res. 50 ms
eROSITA Status: Cameras
eROSITA: Telescope
eROSITA: Mission geometry during all-sky survey
eROSITA L2 halo-orbit
SRG is continuously rotating around the z-axis which always points to the earth
- during the survey ~4 hr / revolution -- 6 scans per day
- 4 years all-sky survey (8 sky passages), 3 yrs pointings
eROSITA: Exposure Map
~ 2.5 ksec in the plane
eROSITA: Sky division ….
IKI/Ru
MPE/D
How many pulsars will be detected in the all sky survey?
Crab-like pulsars (< 104 yrs)
Cooling neutron stars
Old pulsars (106 - 108 yrs)
( ~105 - 106 yrs)
Simulations:
•
for pulsars detected in X-rays we adopted their observed spectral parameters
• for pulsars not detected by now we used:
1. Pulsar parameters (e.g. age, distance,
E ) from the ATNF-Catalog (Manchster & Hobbs)
2. Thermal surface component: Neutron star cooling model (Tsuruta et al 2007)
3. Thermal hot-spot component : Polar cap model from Harding (2002)
4. Non-thermal component: assuming Lx = 10-3
E+
power-law spectrum with a=1.8
How many pulsars will be detected in the all sky survey?
those pulsars will be detected
with a photon statistics sufficient
to perform a detailed spectral
and timing analysis !
Fermi:
Currently 600 unidentified gamma-ray sources
eROSITA will be fundamental to cover all Fermi
error boxes in an identification campaign
Temperature upper limits for all neutron stars in the survey
Becker et al. 1995
eROSITA on
Supernova Remnants?
eROSITA: Supernova research
see the poster by Prinz & Becker
~270 known
Galactic SNRs
RASS: 215 SNR candidates
Supernova research with eROSITA: G296.7-0.9
Supernova remnant candidates in the RASS
eROSITA: on extended supernova remnants …
eROSITA: Data Rights and Policies (MPE)
“Policy Document”
• German eROSITA data will be made public after a 2 yr proprietary
period
• Periodic data releases envisaged (e.g. 24, 30, 36,42, 48 months)
• Access to proprietary data via eROSITA_DE collaboration
(consortium)
• Projects/Papers regulated by Working Groups
• Individual External Collaborations
• Group External Collaborations
eROSITA: Data Rights and Policies (MPE)
„Science Working Groups“:
Chairs
Clusters and Cosmology
AGN, Blazars
Normal Galaxies
H. Böhringer, J. Mohr, T. Reiprich
K. Nandra
F. Haberl
Compact Objects
A. Schwope, A. Santangelo
Diffuse Emission, SNR
W. Becker, M. Freyberg, M. Sasaki
Stars
Solar System
J. Robrade, J. Schmitt
K. Dennerl
„Infrastructure Working Groups“:
Time Domain Astrophysics
Data analysis, source extraction, catalogs
Multi-wavelength follow-up
Calibration
Background
J. Wilms, I. Kreykenbohm
H. Brunner
J. Mohr
K. Dennerl
M. Freyberg
eROSITA Collaboration
Core Institutes (DLR funding):
MPE, Garching/D
Universität Erlangen-Nürnberg/D
IAAT (Universät Tübingen)/D
SB (Universität Hamburg)/D
Astrophysikalisches Institut 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
K. Nandra, A. Merloni, P.P.
Instrument Design, Manufacturing, Integration & Test
Data Handling & Processing, Archive etc.

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