State of the Art of High-Energy Astronomy E>100eV=1.6x10-10erg, kT>106 K, λ<100Å
Presented by Jan-Uwe Ness Matteo Guainazzi, Maria Santos-Lleo, Michael Parker, Gabi Matzeu, Felix Fürst, Richard Saxton, Maggie Lieu, Erik Kuulkers, Celia Sanchez, Guillaume Belanger, Peter Kretschmar, Achille Nucita
Cherenkov Telescope Array (CTA) High-Energy Astrophysics started and continues on the ground
Huge Diversity of Activities: => Impossible to cover all
● Solar System Sun ==> Talk by David Williams, Moon, Planets, Comets: Magnetic activity, Reflection, fluorescence, Aurorae, Charge Exchange
● Stars: Magnetic Dynamos, activity cycles, stellar winds, Exo-planets
● Star Formation: Deeply embedded proto stars
● Planetary Nebulae: Increased rotation due to past common envelope phase
● Globular Clusters: Binding Energy in form of binaries
● Accreting White Dwarfs (CVs), Neutron Stars, Black Holes (Low-mass, High-mass X-ray binaries), Ultra-luminous X-ray sources (ULX) ==> Talk by Felix Fürst
● Stellar- and intermediate mass black holes
● Supermassive Black Holes (Active Galactic Nuclei = AGN) ==> Talks by Michael Parker, Ricardo Pérez Martinez, Gabriele Matzeu
● Supernova explosions and remnants: Heavy Element production
● Gamma-ray bursts
● Nature of Dark Matter
● Galaxy Clusters ==> Talks by Maggie Lieu, Bruno Altieri
● Distribution of matter in the Universe ==> alk by Bruno Altieri
● Cosmic X-ray Background
In half an hour ?!? ----- Don’t worry, made a selection…... XRISM
NASA Missions
Other High-Energy Missions
● Astrosat (India): Multi-wavelength
● MAXI (JAXA): X-ray monitor mounted to ISS
● HXMT-Insight (China): Hard X-ray Modulation Telescope
● DAMPE (China, Switzerland, Italy): DArk Matter Particle Explorer
● eROSITA/Спектра-РГ (German/Russian): Спектра-РГ (German/Спектра-РГ(German/Russian):Russian): All-sky X-ray Survey
● Einstein Probe (China/Спектра-РГ (German/Russian):ESA):X-ray Large-field Monitor
● SMILE (China/Спектра-РГ (German/Russian):NASA/Спектра-РГESA)Solar wind Magnetosphere Ionosphere Link Explorer
● GECAM (China): High-energy Electromagnetic Counterpart All-sky Monitor
“When you have this kind of opportunity you can’t handle it like a normal mission, with selection and review taking 10 or 20 years” Xiong Shaolin, Chinese Academy of Science, Institute of High Energy Physics, Beijing
X-ray Cosmic background
NuSTAR resolves into discrete sources
X-ray Cosmic background
● 3rd brightest X-ray source ● Apparently homogeneous over entire sky → Extragalactic ● Peak at 30keV → One of the core NuSTAR science activities ● 80% currently resolved in discrete sources
● Diverse sources (mostly AGN) ← this talk… ● INTEGRAL resolved 100% of soft -ray (20-300keV) X-ray background into compact sources 훾 Lebrun et al. 2004, Nature 428, 293
Photon Limit ● Since each photon has high energy, number of photons is usually small
● Consequences:
● Long exposure durations => Long mission durations ;-) ● Limited image/Спектра-РГ (German/Russian): spectralresolution(talkbyGuillaumeBelanger, Bruno Altieri)
● Importance of upper limits (see poster #5 by R. Saxton)
Photon Limit ● Since each photon has high energy, number of photons is usually small
● Consequences:
● Long exposure durations => Long mission durations ;-) ● Limited image/Спектра-РГ (German/Russian): spectralresolution
1974, Quarterly Journal of the Royal Astronomical Society Vol. 15, p.141
Photon Limit ● Since each photon has high energy, number of photons is usually small
● Consequences:
● Long exposure durations => Long mission durations ;-) ● Limited image/Спектра-РГ (German/Russian): spectralresolution
1974, Quarterly Journal of the Royal Astronomical Society Vol. 15, p.141
Photon Limit ● Since each photon has high energy, number of photons is usually small
● Consequences:
● Long exposure durations => Long mission durations ;-) ● Limited image/Спектра-РГ (German/Russian): spectralresolution
1974, Quarterly Journal of the Royal Astronomical Society Vol. 15, p.141
Photon Limit ● Since each photon has high energy, number of photons is usually small
● Consequences:
● Long exposure durations => Long mission durations ;-) ● Limited image/Спектра-РГ (German/Russian): spectralresolution
1974, Quarterly Journal of the Royal Astronomical Society Vol. 15, p.141
Photon Limit ● Since each photon has high energy, number of photons is usually small
● Consequences:
● Long exposure durations => Long mission durations ;-) ● Limited image/Спектра-РГ (German/Russian): spectralresolution XMM grating spectrum of same source at same time! XMM CCD spectrum Many of these emission Lines unknown!
Resonant Scattering: Hitomi spectrum of Intra Cluster Medium of Perseus Cluster:
- Photons of certain energies Resonant scattering in the FeXXV (Heα Resonance) absorbed in resonant transitions and re-emitted into random directions => Into and out of line of sight !
RS is sensitive to anisotropies of the velocity field, and small-scale motions and density inhomogeneities Imaging: Resolve structures e.g. Supernova remnants, Light echoes from imaging monitoring
Galaxy Clusters
● Covered by talks by Ivan Valtchanov, Maggie Lieu, Bruno Altieri
Extragalactic Astronomy Perseus Cluster TurbulenceTurbulence seenseen withwith ChandraChandra VigorousVigorous AGNAGN FeedbackFeedback
Extragalactic Astronomy Perseus Cluster TurbulenceTurbulence seenseen withwith ChandraChandra VigorousVigorous AGNAGN FeedbackFeedback
=>=> ShouldShould seesee broadenedbroadened emissionemission lines,lines, butbut ● XMM-NewtonXMM-Newton upperupper limitslimits narrowernarrower thanthan whatwhat isis neededneeded ● HitomiHitomi observed:observed:
StateState ofof thethe Art:Art: PuzzlingPuzzling resultresult …...…...
Warm-Hot Intergalactic Medium (WHIM)
Nicastro et al. 2018, Nature 558, 406 Warm-Hot Intergalactic Medium
● Number of Baryons in Universe predicted by Big-Bang Nucleosynthesis models and seen in very early Universe (Lyα forest) ● => 30-40% missing in observations probing more recent Universe ● Theory: Missing baryons in hot, tenuous plasma
● But: H ionized, need to rely on higher-Z elements ● OVII in right temperature regime
● Search for absorption in a quasar at redshift >0.4
Nicastro et al. 2018, Nature 558, 406 Warm-Hot Intergalactic Medium
=> FOU ND!
Nicastro et al. 2018, Nature 558, 406 Active Galactic Nuclei
Inactive Galacic Nuclei: Sgr A* ● Like 90% of all Galactic Central Black Holes, the one in our own Galaxy is relatively inactive ● 4 Million Solar Masses ● Much more active some 300 years ago ● <= Deduced from delayed X-ray reflections!
Reverberation Mapping Time delayed reflections depending on frequency or energy 1) Mass of central source (e.g. Black Hole BH) 2) Localize emission (Geometry) 3) Relations between various emitting regions
Also applied to a) Active Galacti Nuclei (AGN) b) Ultra Luminous X-ray Sources (ULX) c) Tidal Disruption Events (TDEs) d) X-ray Binaries
Slide from Erin Kara, given at “The X-ray Universe 2017”
Reverberation Mapping Time delayed reflections depending on frequency or energy 1) Mass of central source (e.g. Black Hole BH) 2) Localize emission (Geometry) 3) Relations between various emitting regions
Results AGN: 1) Several Million Solar Masses 2) X-rays from central regions, few gravitational radii
=> Probing how matter behaves in highly relativistic environment: A RARE OPPORTUNITY! From Jiachen Jiang Nardini et al. 2015, Science 347, 860
AGN Feedback
● Ultra-fast outflows @ several fractions of the speed of light! ● High kinetic power in outflows that impacts star formation history of the host galaxy!
● Known from large fraction of AGN with outflows (large solid angle) ● Active BH quenches star formation ● Feedback also influences host Galaxy Cluster (see Perseus)
Extragalactic Astronomy Perseus Cluster TurbulenceTurbulence seenseen withwith ChandraChandra VigorousVigorous AGNAGN FeedbackFeedback
Tidal Disruption Events
(CO=Compact Object)
From A. Levan Schwarzschild Radius (no light from inside can escape)
From A. Levan Tidal Disruption Events
● ~ Solar-mass star swallowed by Black Hole that is not supermassive (intermediate mass?) ● About 1% of mass converted to radiation. Where are the other 99% going?
● Winds seen (blue shifted absorption lines) but not enough mass in winds ● Accretion disk: Would radiate for decades but not enough evidence so far
Unified TDE model
Reprocessing models Strubbe&Murray 2011 Guillochon+ 2014 Metzger&Stone 2016 Roth+ 2016
All TDE are same.
Characteristics due to viewing angle.
Predictions:
- Some X-ray TDE with high absorption
- X-rays visible when debris screen clears
Dai et al. 2018 Gravitational Waves: Association to electromagnetic (EM) counterpart
Gravitational Waves: Association to electromagnetic (EM) counterpart
Progenitors are X-ray binaries: Also important field of high-E Astronomy X-ray Binaries
X-ray Binaries
● Stellar scale ● Accretion physics similar to AGN, but on much smaller and faster scales ● Relatively nearby => bright sources (more photons) => detailed, time resolved comparison with models possible ● Different components to be studied (e.g., stellar wind, accretion disk, jets, flow to surface) covering many orders of magnitude in size. ● Very active field for spectral, timing and multi- wavelength analysis.
No time for more …..
Supernovae Ia
● Cosmic Distance ladder
● Supernovae Ia occur when a white dwarf collapses after growing beyond 1.4 solar masses:
● => Central density grows => Pauli Principle not sustainable => Further collapse => Nuclear fusion chain reactions => Energy production => Explosion
Supernovae Ia
● INTEGRAL detected radioactive decay of 56Co into 56Fe in a Type Ia supernova: SN2014J in M82 Churazov et al,2014, Nature 512, 406 => Direct proof of concept for first time!
Juno: In situ measurements of physical Processes (talk by Japheth Yates) XMM-Newton and Chandra: Remote X-ray observations
Tandem: Once in a generation opportunity [email protected]
Independent pulsations of Jupiter's northern and southern X-ray aurorae
Dunn et al. 2017 Nature Astronomy 1, 758 High-Energy Astrophysics Highlights
● Jupiter: Uncorrelated pulses in Northern and Southern Aurorae ● Tidal Disruption Events: Black Hole swallows star: Young field, a way to discover unknown black holes of intermediate mass. With a lot more, distribution of black holes in galaxy could be determined. ● Active Galactic Nuclei: 10% of Central Black Holes are active, powered by accretion, complex reflection patterns, strong feedback into host galaxy and even host Galaxy Cluster! ● Intergalactic Medium: Missing Baryons found! ● Supernovae Ia: Important isotope found by INTEGRAL => Observational proof of concept! ● Galaxy Clusters: Going to largest distances to determine distribution of matter in the Universe (talk by Bruno Altieri)