eROSITA: Status & Scientific Prospects

to extend the ROSAT all-sky survey up to 10 keVwith an XMM-Newton type sensitivity

Basic scientific idea of eROSITA ….

200920102011fall of

2014

eROSITA: ready for launch ….

• 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)

Mission scenario & Instrument specification

• 3 month calibration & science verification phase

• 4 yrs all-sky survey (8 sky coverages)

• 2.7 yrs pointed observations

eROSITA ( MPE )ART-XC

( IKI )

eROSITA on Spectrum-RG

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).

Fregat Booster

Navigator

eROSITA: Navigator and Booster

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 Telescope Array

eROSITA: effective area 2400 cm2 @ 1keV

eROSITA: Grasp @ 1keV

eROSITA pn-CCD flight devices

Frame store

Imaging

384 amplifiers

eROSITA: Advanced XMM pn-CCD

– 7 individual cameras

• 256 × 256 pixel,

75µm

• frame store area

• faster read-out

• 40% reduced out-of-

time events

• temporal res. 50 ms

eROSITA Status: Cameras

eROSITA: Telescope

eROSITA: Mission geometry during all-sky survey

SRG is continuously rotating around the z-axis which always points to the earth

eROSITA L2 halo-orbit

- 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

( ~105 - 106 yrs)

Old pulsars (106 - 108 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, ) 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 + power-law spectrum with a=1.8

those pulsars will be detected with a photon statistics sufficient

to perform a detailed spectral and timing analysis !

How many pulsars will be detected in the all sky survey?

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

~270 knownGalactic SNRs

RASS: 215 SNR candidates

see the poster by Prinz & Becker

Supernova research with eROSITA: G296.7-0.9

ROSAT RASS image + MOST (contour lines)

new young SNRs in RASS

ATCA (20 cm) image

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 H. Böhringer, J. Mohr, T. Reiprich AGN, Blazars K. Nandra Normal Galaxies F. Haberl

Compact Objects A. Schwope, A. Santangelo

Diffuse Emission, SNR W. Becker, M. Freyberg, M. Sasaki

Stars J. Robrade, J. Schmitt Solar System K. Dennerl

„Infrastructure Working Groups“:

Time Domain Astrophysics J. Wilms, I. Kreykenbohm Data analysis, source extraction, catalogs H. Brunner Multi-wavelength follow-up J. Mohr Calibration K. Dennerl Background M. Freyberg

Core Institutes (DLR funding):MPE, Garching/DUniversität Erlangen-Nürnberg/DIAAT (Universät Tübingen)/DSB (Universität Hamburg)/DAstrophysikalisches Institut Potsdam/D

Associated Institutes:MPA, Garching/DIKI, Moscow/RuUSM (Universität München)/DAIA (Universität Bonn)/D

Industry:Media Lario/I Mirrors, MandrelsKayser-Threde/D Mirror StructuresCarl Zeiss/D ABRIXAS-MandrelsInvent/D Telescope StructurepnSensor/D CCDsIberEspacio/E HeatpipesRUAG/AMechanismsHPS/D,P MLIMoog/USA ValvesMAP/F PaintingLaserjob/D X-ray BafflesNPOL/RuSpacecraft, Mission+ many other (small) companies

eROSITA Collaboration

MPE: Scientific Lead Institute, Project Management K. Nandra, A. Merloni, P.P.

Instrument Design, Manufacturing, Integration & TestData Handling & Processing, Archive etc.