Athena+, ESA’s next generation X-ray observatory Gregor Rauw High-Energy Astrophysics Group Liège...
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Athena+, ESA’s next generation X-ray observatory Gregor Rauw High-Energy Astrophysics Group Liège University on behalf of the Athena+ coordination group
Athena+, ESAs next generation X-ray observatory Gregor Rauw
High-Energy Astrophysics Group Lige University on behalf of the
Athena+ coordination group
Slide 2
The X-ray Universe today
Slide 3
X-ray astrophysics provides a complementary view of the
Universe, revealing highly energetic phenomena. Crab Nebula Sirius
B Orion Moon
Slide 4
XMM-Newton (ESA) and Chandra (NASA) are now in orbit for more
than 10 years and have deeply changed our view of the X-ray
Universe. Among the many discoveries: Establishing charge-exchange
as the mechanism for X-ray emission of comets Quantitative
diagnostics of hot plasma in the coronae and winds of stars Images
of the particle acceleration shocks in supernova remnants Direct
measurement of rotation of black holes and neutron stars Resolving
the cosmic X-ray background into discrete sources, mostly AGN
Contributions to the study of dark matter and dark energy via
observations of galaxy clusters. Cas AM82NGC6231Cen A
Slide 5
Where are the hot baryons and how do they evolve? The science
to be addressed by Athena+ How do black holes grow and shape the
Universe? The life cycle of matter and energy in the local Universe
High z groups and clusters. Evolution of hot baryons. Missing
baryons at low z. Physics of clusters and groups. High z groups and
clusters. Evolution of hot baryons. Missing baryons at low z.
Physics of clusters and groups. AGN feedback. Accretion physics.
Obscured accretion and galaxy formation. Growth of SMBHs. AGN
feedback. Accretion physics. Obscured accretion and galaxy
formation. Growth of SMBHs. Star formation and evolution. Compact
Objects SNRs and the ISM Solar System and exo- planets. Star
formation and evolution. Compact Objects SNRs and the ISM Solar
System and exo- planets. Diagnose hot/energetic cosmic plasmas in a
wide variety of astrophysical environments using spatially resolved
medium and high-resolution X-ray spectroscopy
Slide 6
Where are the hot baryons and how do they evolve? Reveal and
map the first virialized baryonic structures Determine their
dynamical, thermal and chemical evolution E.g. measure the chemical
composition of the hot plasma in galaxy clusters as a function of
z. Complete the census of baryons in the local Universe Trace
large-scale-structures and detect the WHIM via high resolution
X-ray spectroscopy Understand the physics of clusters and groups
Determine intra-cluster gas velocities as a function of z via
imaging X-ray spectroscopy. Cosmic Web Cluster Physics
Slide 7
Accretion physics High z SMBH Cosmic FeedbackObscured accretion
Reveal the causes and effects of AGN feedback Understand the
physics of accretion onto compact objects X-ray tomography of inner
accretion disk, determination of the spin rate of black holes (Fe K
line shape), hot spot tracking (short-term variability of Fe K
line). Track obscured accretion through the ages Perform a census
of black hole growth at high redshift How do black holes grow and
shape the Universe?
Slide 8
Life cycle of matter and energy in the local Universe Star
formation and evolution Young stars, stellar winds, stellar
activity End points of stellar evolution X-ray binaries, neutron
star, pulsars, white dwarfs Supernova remnants and the interstellar
medium Disentangle the 3-D structure of SNR via high-resolution
integral field spectroscopy, study the acceleration of particles by
the SNR shock through the resulting non-thermal emission. The Solar
System and exo-planets Charge ExchangeStellar ActivityCompact
Objects SNRs
Slide 9
A few more specific examples Wind-wind collisions in massive
binaries: dynamics of hot gas well traced by Fe K line. E.g.
colliding winds in WR140: diagnose the physics of the innermost
parts of the wind-wind interaction. But also: study X-ray emission
and variability of single massive stars, Doppler-map their
magnetospheres,
Slide 10
A few more specific examples X-ray emission from planets of the
Solar System. E.g. Jupiter (emission due to charge exchange, solar
X-ray scattering and electron bremsstrahlung) Integral field
spectroscopy with Athena+ will resolve the disk and auroral charge
exchange emissions and resolve the charge exchange ions (hence
specify their origin) But also: look for Saturns auroral X-rays,
Mars: solar X-ray scattering in the atmosphere, charge-exchange in
the exosphere
Slide 11
Athena+ mission concept Focal plane Mirror Assembly Service
Module 12m Fixed Focal Length Sensitivity ~ 30 times better than
XMM: stacked Si pore optics, 5 (3) resolution Payload: Wide Field
Imager (WFI), X-ray Integral Field Unit (X-IFU) microcalorimeter.
L2 orbit, 5yr nominal lifetime (starting 2028)
Slide 12
Athena+ requirements RequirementDriver Effective Area2m 2 @ 1
keV (goal 2.5m 2 ) 0.25m 2 @ 6 keV (goal 0.3m 2 ) Hot Baryons Black
hole evolution Accretion Physics Angular Resolution5 (goal of
3)Black Hole Evolution Hot Baryons Fields of viewWFI: 40 diameter
(goal 50) X-IFU: 5 x 5 (goal 7 x 7) Hot Baryons Black Hole
Evolution Spectral resolution150 eV @ 6 keV (WFI) 2.5 eV (X-IFU)
goal 1.5 eV Black Hole Evolution Hot Baryons Count rate capability
>1 CrabAccretion Physics Timing resolution 50 s Accretion
Physics TOO response8 hours (2 hours goal)Hot Baryons
Slide 13
Find out more about Athena+:
http://www.the-athena-x-ray-observatory.euhttp://www.the-athena-x-ray-observatory.eu
And sign up to support the project! Athena+ Open Meeting:1-2 July
in Paris Athena+ white paper in response to ESA call for L2/L3
currently in preparation (due 24 May). Athena+ will be the most
sensitive X-ray observatory ever. It will lead to substantial
breakthroughs in many different fields of astrophysics.