eROSITA: Status & Scientific Prospects - PowerPoint Presentation

Slide1

eROSITA:

Status & Scientific Prospects

Slide2

t

o

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

Basic scientific idea of eROSITA ….

Slide3

2009

2010

2011

fall of

2014

eROSITA: ready for launch ….

Slide4

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

Slide5

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).

Slide6

Fregat

Booster

Navigator

eROSITA: Navigator and Booster

Slide7

Mirror Systems 7 aligned X-ray mirror modules54 nested gold-coated nickel-shells

Aeff ~ 2400 cm

2 (1 keV, on-axis

)

7

pn-CCD Cameras

eROSITA Telescope Array

Slide8

eROSITA: effective area 2400 cm

2

@ 1keV

Slide9

eROSITA: Grasp @ 1keV

Slide10

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

Slide11

eROSITA Status: Cameras

Slide12

eROSITA: Telescope

Slide13

Slide14

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

Slide15

eROSITA: Exposure Map

~

2.5

ksec

in the plane

Slide16

eROSITA: Sky division ….

IKI/

Ru

MPE/D

Slide17

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

Crab-like

pulsars

(< 10

4

yrs)

Cooling

neutron

stars

( ~10

5

- 10

6

yrs

)

Old

pulsars

(10

6

- 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 L

x

= 10

-3

+

power-law spectrum with

a

=1.8

Slide18

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

Slide19

Temperature upper limits for all neutron stars in the survey

Becker et al. 1995

Slide20

eROSITA on

Supernova Remnants?

Slide21

eROSITA: Supernova

research

~270 known

Galactic SNRs

RASS: 215 SNR candidates

see

the

poster

by

Prinz & Becker

Slide22

Supernova research with

eROSITA

: G296.7-0.9

ROSAT RASS image + MOST (contour lines

)

new young SNRs in RASS

ATCA (20 cm)

image

Slide23

Supernova

remnant candidates in the RASS

Slide24

eROSITA: on extended supernova remnants …

Slide25

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

Slide26

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

O

bjects

A

.

Schwope, A. Santangelo Diffuse Emission, SNR

W

. Becker, M. Freyberg, M. SasakiStars 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

Slide27

Core Institutes (DLR

funding

):MPE, Garching/DUniversität Erlangen-Nürnberg/DIAAT (Universät Tübingen)/DSB (Universität Hamburg)/DAstrophysikalisches Institut Potsdam/DAssociated Institutes:MPA, Garching/DIKI, Moscow/

RuUSM (Universität München)/DAIA (Universität Bonn)/D

Industry

:Media Lario/I Mirrors, Mandrels

Kayser-Threde/D Mirror StructuresCarl Zeiss/D

ABRIXAS-MandrelsInvent/D Telescope StructurepnSensor/D CCDs

IberEspacio

/E

Heatpipes

RUAG/A

Mechanisms

HPS/D,P

MLI

Moog/USA

Valves

MAP/F Painting

Laserjob/D X-ray BafflesNPOL/Ru Spacecraft, Mission+ many

other (small) companieseROSITA Collaboration

MPE: Scientific Lead Institute, Project Management

K.

Nandra, A. Merloni, P.P.Instrument Design, Manufacturing, Integration & TestData Handling & Processing, Archive etc.