Astrophysical Spectroscopy
Eugene Churazov Outline Astrophysically abundant elements Two examples of “Hydrogen” spectroscopy X-ray Astronomy Galaxy clusters and hot plasma LCDM Universe (Today)
WMAP PLANCK
PLANCK Abundance of elements in the Earth (crust)
https://en.wikipedia.org/wiki/Abundance_of_elements_in_Earth%27s_crust Abundance of elements in the Universe (today)
https://en.wikipedia.org/wiki/Nucleosynthesis Origin of elements
https://en.wikipedia.org/wiki/Nucleosynthesis#/media/File:Nucleosynthesis_periodic_table.svg Big Bang Nucleosynthesis Type Ia SN2014J Stellar evolution
Type II SN1987A
https://scioly.org/wiki/index.php/Astronomy/Stellar_Evolution GW170817 Typical abundances today (Sun photosphere) Element Abundance (by number) H 1.00e+0 1.00e+0 He 9.77e-2 9.77e-2 C 3.63e-4 3.98e-4 N 1.12e-4 1.00e-4 O 8.51e-4 8.51e-4 Ne 1.23e-4 1.29e-4 Na 2.14e-6 2.14e-6 Mg 3.80e-5 3.80e-5 Al 2.95e-6 2.95e-6 Si 3.55e-5 3.55e-5
S 1.62e-5 1.62e-5 https://en.wikipedia.org/wiki/Nuclear_binding_energy Cl 1.88e-7 1.88e-7 Ar 3.63e-6 4.47e-6 Ca 2.29e-6 2.29e-6 Cr 4.84e-7 4.84e-7 Fe 4.68e-5 3.24e-5 Ni 1.78e-6 1.78e-6 Co 8.60e-8 8.60e-8Our Universe is dominated by hydrogen +10% of He + small amount of other el. Hydrogen 21 cm line Hyperfine splitting of the ground state A ∼ 10−15 s−1 Lifetime ∼ 10 Myr kTs ≫ hν I = C × nH
https://www.mpifr-bonn.mpg.de/pressreleases/2016/13
Other elements? 14N7 and 57Fe26; For instance, [H]-like N, or [Li]-like Fe? Hydrogen Ly� (1215 Å) Forest http://www.astro.ucla.edu/~wright/Lyman-alpha-forest.html Gunn-Peterson Trough
Image: Bob Carswell 21 cm again
Bowman+18 X-ray astronomy & spectroscopy X-ray image of Coma cluster
The best 10 keV plasma in the Universe (almost) zero density limit (10-3 cm-3) (almost) optically thin (almost) pure collisional ionization (almost) Maxwellian X-ray astronomy
Atmosphere is transparent in optical band We are opaque in optical band Atmosphere is opaque to X-rays We are ~transparent for X-rays
X-ray astronomy is only possible from space It is difficult to reflect X-rays https://imagine.gsfc.nasa.gov/observatories/technology/xray_telescopes1.html X-ray history (of clusters)
First extragalactic X-ray source detected – M87/ Virgo (Byram et al., 1966, Bradt et al., 1967) – Aerobee rocket flight
UHURU satellite (1970-1973) (Kellog et al., 1972, Forman et al., 1972) 43-45 Many clusters, very powerful Lx~10 erg/s Extended!
Ariel-5 satellite (1974-1980) Lines in the spectra – thermal plasma! (Mitchell et al 1976)
…Einstein observatory, Rosat, ASCA, Chandra, XMM-Newton Major X-ray observatories (for clusters) today
Chandra XMM-Newton
Angular resolution <1” Effective area ~2500 cm2 ΔE ∼ 150 eV Gratings on XMM and Chandra
ΔE ∼ 4 eV http://www.mssl.ucl.ac.uk/www_xmm/ukos/onlines/uhb/XMM_UHB/node14.html (But only for compact sources and with small efficiency) ~100 cm2 For clusters - one needs non-dispersive spectrometer
Solution: cryogenic bolometers with <5 eV resolution Hitomi Hitomi Collaboration Galaxy clusters Clusters usually refer as
Clusters are the most massive gravitationally bound structures in the Universe….
Clusters are formed recently...
Clusters are powerful X-ray sources….
Clusters represent a fair sample of matter (which is able to cluster) in the Universe….
Clusters are great astrophysical plasma laboratories Optical image of a patch of the sky (Coma Berenices)
Count galaxies Estimate size of the region Line-of-sight velocities of galaxies Clusters and Dark Matter R ~ Mpc, σ ~ 1000 km/s −U = 2K GM ≈ v2 = 3σ 2 R 15 M ∼ 10 M⊙ While examining the Coma galaxy cluster in 1933, Zwicky was the first to use the virial theorem to infer the existence of unseen matter, what is now called dark matter. He obtained a cluster mass about 160 times greater than expected from galaxies luminosity, and proposed that most of the matter was dark. Radiation dominated (Dark) Matter dominated (Dark) Energy dominated Planck: Map of the CMB temperature fluctuations δT 1 ϕ ∼ T 3 c2
δT ∼ 10−5 T ρ − ρ δ = δ ≈1 ρ R, size δ >>1
δ <<1 [matter dominated Universe]
a, scale factor
δ ≈ 1 (ρ ≈ 2 ρ )
Spherical collapse model Growth of perturbations in EdS Universe [z=1-1000]
Z=1000
1 Z=0 a = δρ ∝ a 1+ z δ c ≈1
δ = 0 δ (z =1000)×1000 2 Density/potential fluctuations ⎧ δ c ⎫ N ∝ exp⎨− 2 ⎬ ⎩ σ ⎭ δ ∝ a
~2
Z=10
Z=100
Z=1000
Density amplitude
Mass first massive clusters
This is why clusters are the most massive systems in the Universe 15 (there are ~50 clusters in observable Universe with mass > 10 MSun) Linear evolution of gravitational potential δ ∝ a δM δ ϕ ∝ G ∝ ∼ const R a No DE R ∝ a
Nonlinear evolution of the potential M2 M2 1 M2 −G = − G + G Ri Rf 2 Rf 1 R ∼ R ⟹ ϕ ∼ 2ϕ f 2 i f i Big and deep potential well => Hot plasma => X-rays
δT δϕ ∼ ∼ 10−5 T c2 n=1
δϕmp ∼ 15 keV
δϕ Potential amplitude
Hotter Colder (DM+Baryons) Potential Well gas DM galaxies
kT ~ 10 keV
GM kT ≈ m ≈ m 3σ 2 p R p Dark matter Stars Hot gas
80 % few. % 15 %
baryons baryons gas + stars = ≈ 0.2 DM DM Universe Clusters Clusters usually refer as
Clusters are the most massive gravitationally bound structures in the Universe….
Clusters are formed recently...
Clusters are powerful X-ray sources….
Clusters are representing a fair sample of matter (which is able to cluster) in the Universe….
Clusters are great astrophysical plasma laboratories What we can learn from X-ray spectra
Bremsstrahlung + lines + recombination + 2-photon
Flux → density Curvature → temperature Line Energy → redshift Line Strength → abundance The only existing resolved He-like triplet of Iron from a cluster
Instrumental + Instrumental Hitomi Collaboration thermal Plasma in galaxy clusters
−3 −3 −1 ne ∼ 10 cm kTe ∼ 10 keV u ∼ 500 km c L ∼ 1 Mpc Spectroscopy Material properties
CEI, ti~10 Myr; Age~Gyr λ ∼ 10 kpc Re ∼ 10 tee~3 105 yr; tei~few 108 yr ~Maxwellian Pr ∼ 0.02 nkT Optically thin (free-free) β = 8π ∼ 100 B2 3 ρe ∼ 10 km ⋘ λ Are clusters optically thin?
Optical depth for free-free L 1045 erg/s X ≈ ≈10−32 4πR2σT 4 1077 erg/s
Thomson optical depth
−3 −2 τ T = σ T ne R ≈10 −10
Clusters are optically thin in X-rays (in continuum) Resonant scattering (absorption+emission)
1/ 2 π hrecfik v ⎡ 2kT ⎤ σ 0 = ; ΔED = E0 = E0 ⎢ ⎥ ; τ 0 = nilσ 0 E c Am c2 Δ D ⎣⎢ p ⎦⎥
1) Abundant elements; He-like ions; maximal oscillator strength 2) Heavy elements have narrow lines (if no turbulent motions) 3) Product of density and size Optical depth in lines
NGC4636; 0.6 keV M87; 1-3 keV Perseus; 3-7 keV Impact on the surface brightness
Line is suppressed in the core Photons are re-emitted at the outskirts Spectral shape of the line
Core of the line is suppressed Gas Velocities I
1/ 2 2 π hrecfik ⎡ 2kT Vturb ⎤ σ 0 = ; ΔED = E0 ⎢ + ⎥ E Am c2 c2 Δ D ⎣⎢ p ⎦⎥
FeXXV; 6.7 keV line; T=5 keV
Radiative width: 0.3 eV
Thermal width: 3 eV
Turbulence (300 km/s): 7 eV Gas Velocities F6.7 F Isotropic, radial, tangential thin
τ ↔ Ekin Optical depth strongly depends on the character of motions (and on the correlation length) Direct evidence for resonant scatterings from HITOMI Polarization I
Scattering phase function =
W2 x Rayleight + W1 x Isotropic
+
Polarization No Polarization
W2 (J1, J 2 ) Hamilton, 1947; [Chandrasekhar 1950]
2 1 1 He-like ions; 1s ( S0) – 1s2p ( P1) => W2=1 Polarization II Rayleigh phase function + Quadrupole = Polarization
100% polarized Center: 0% Outskirts: 10% Polarization II Rayleigh phase function + Quadrupole = Polarization
100% polarized Center: 0% Outskirts: 10% Transverse ICM velocities and polarization
Quadrupole component can be induced by gas motions!
Motion along l.o.s. Motion transverse l.o.s.
Doppler shift No Doppler shift No polarization Polarization
1) On average gas motions reduce optical depth 2) But can cause polarization in the cluster core What we want from X-ray spectroscopy? Density Temperature Abundances Velocities
Why? To accurately measure cluster masses To understand gas heating processes Cooling flows
Cooling time
3 nkT t = 2 ≈ 5108 years cool n2Λ(T )
Fastest cooling near the center
Cooling rate
• L M = X × µm ≈1000 M yr−1 (L =1045 erg/s) 3 p Θ X kT 2 Gas density Gas temperature
Surface brightness Temperature
The highest density is at the center => cools first! When densest gas cools it is compressed and becomes even denser! But What is the fate of cooled gas? Stars? 3 −1 10 M⊙ yr 3 10 13 10 × 10 yr ∼ 10 M⊙ Where are emission lines, characteristic for cool gas?
Or there is a source of energy that keeps the gas hot? Supermassive black hole nkT t = ≪ t cool n2Λ(T) Hubble
Hot plasma Clear evidence for the impact of relativistic plasma on thermal gas Bubbles of relativistic plasma inflated by SMBH How to measure the energy release rate?
Böhringer+, 1993 Simple numerical simulations
g
200x200 EC+2001
LAGN ∼ Lcooling How the gas is heated? Bubbles induce gas motions - motions dissipate into heat Identify perturbations in images Relate the amplitude of perturbations to velocities Getting gas velocity power spectrum from images
δI δρ v ⇒ P2D (k) = C× P3D (k) ⇒ ⇒ 2014 al., et Zhuravleva I ρ cs 2/3 −5/3 Heating rate E(k) = K0ε k
Cooling=n2Λ(T) 3 Heating = CρV1,kk Zhuravleva et al., 2014 al., et Zhuravleva “Outer region” spectrum of the Perseus cluster (He-like triplet)
Instrumental + Instrumental thermal Predicted velocity power spectra in Perseus and M87
164±10 km/s @ 30-40 kpc
2016 2014 2014 al., et Zhuravleva Cluster masses and X-ray spectroscopy
Mass profile of the cluster from X-ray data1 dP dϕ GM (< r) = − = − 2 [stationary, sph.sym.] µmp n dr dr r 1 d2 P dϕ GM (< r) 1 dnσ r = −dϕ = −GM (< r) [stationary, sph.sym.] 2 [stationary, sph.sym., isotr.] m n dr= − dr= − 2r nµ dp r dr r 1 dnσ 2 dϕ GM (< r) r = − Hydrostatic equilibrium equation= − [stationary, sph.sym., isotr.] n dr dr r 2 P(r) = n(r)kT(r)
P(r) = n(r)kT(r) Deprojection of X-ray data
Repeat the same exercise at all energies ε(r,E)=n(r)2S(E,T(r)) Deprojected X-ray data: gas temperature and density
ne (r), Te (r) P(r)
1 dP GM = − ρ dr r 2
r 2 1 dP M (< r) = G ρ dr Mass profile of a real cluster
DM : 80-85% Gas : 12-15% Stars : 2-5%
The results have to be corrected for gas velocities
Only possible with bolometers 2 Density/potential fluctuations ⎧ δ c ⎫ N ∝ exp⎨− 2 ⎬ ⎩ σ ⎭ δ ∝ a
~2
Z=10
Z=100
Z=1000
Density amplitude
Mass Number of massive clusters as a function of amplitude
2 ⎧ δ c ⎫ N ∝ exp⎨− 2 ⎬ ⎩ σ ⎭ σ8=0.9
σ8=0.6 σ 8 ∝ ln N dN = f (Ω , Λ, N , Σm ,....) dMdz m ν ν
σ8=0.79 -1 σ8 =RMS(Δρ/ρ) @ 8 h Mpc High-resolution X-ray spectroscopy is coming to astronomy
(EBIT in space)
Spectroscopy can solve many astrophysical problems
Clusters offer an opportunity to test your models