Probes of rain and turbulence in hot halos - Massimo (Max) Gaspari Princeton University - ESA
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probes of rain and turbulence in
hot halos
Massimo (Max) Gaspari
Princeton University
Lyman Spitzer Jr. Fellow
… and smbh co-evolution
Massimo (Max) Gaspari
Princeton University
Lyman Spitzer Jr. Fellow
“black hole weather”
program
r vir
AC K
EDB 0.1 r v
ir
FE 4. r co re
⇡ tcool > tage
diffuse
c phase
⇠ kp
3 r vir POUT
3. 10
8 r vir entrainment
10
10
9 .3 r vir ṀOUT 5.
Ṁout
SMBH galaxy, group, cluster
Ṁcool
Ṁ• 5 rS
100 r
S
CCA
colli
2. sion
s 10 7 rS
Ṁcool
Lx
CCA
cond cold phase
ensa
tion
FEE 1. 10 9 r
DIN S
G 10 10
rS
GOAL 1: first-principle multi-scale simulations
GOAL 2: test detailed synthetic models with multi-λ data
MG+2011-2019
“black hole weather”
program
r vir
0.1 r v
ir
⇡ tcool > tage
r co re
diffuse
c phase
⇠ kp
3 r vir POUT
10
8 r vir entrainment
10
9 .3 r vir ṀOUT
10
Ṁout
SMBH galaxy, group, cluster
Ṁcool
Ṁ• 5 rS
2. m 100 r
FEE icro
S
CCA
colli Ṁcool
DIN sion
s 10 7 rS Lx
G 1. m CCA
FEE acro
cond cold phase
ensa
tion
DIN 10 9 r
G S
10 10
r
multiphase condensation cascade (“raining”) S
CCA = CHAOTIC COLD ACCRETION
MG+2011-2019
raining on black holes
a.k.a. Chaotic Cold Accretion [CCA] — Gaspari et al. 2013
TURBULENCE > ROTATION
Tat < 1
COOLING ~ AGN HEATING
chaotic streamlines => recurrent turbulence ~150 km/s, as
multiphase gas interactions found (a posteriori) by Hitomi
MG+17
RGB surface density: plasma (blue), warm gas (red), cold gas (green)
Since 2013, CCA has been corroborated by several independent observational and theoretical/simulation studies: e.g.,
Voit & Donahue 2015, Voit 2015, 2017, 2018; Werner+2014; David+2014, Li & Bryan 2014, 2015; Wong+2014; Russell+2015;
Valentini & Brighenti 2015; Yang+2015-2016; Meece+2016; Tremblay+2015, 2016, 2018; Prasad+2016; David+2017;
McDonald+18; Maccagni+18; Nagai+19; Rose+19a,b; Storchi-Bergmann+19 (review)
TOP-DOWN MULTIPHASE GAS CONDENSATION RAIN
hard X-ray soft X-ray
central massive galaxy (e.g., N5044)
ultra high-resolution (0.8 pc) SIM:
hydrodynamics + gravity + turbulence +
AGN heating + multiphase radiative cooling
cold gas/molecular warm gas/neutral warm gas/ionized
radio optical/IR UV
Gaspari et al. 2017
kinematic tracers
multiphase rain
“shaken snow globes”
Gaspari et al. 2018
self-regulated
AGN jet feedback run
ENSEMBLE beam
(R < 50 kpc,
arcmin scale)
novel method to constrain Perseus
turbulence in the hot phase
global turbulence
spectral line broadening kinematics:
= turbulent motions ensemble warm phase
and hot/plasma phase
are linearly related
similar can be shown for UV - IR - radio (molecular) phases:
multiwavelength synergies: ATHENA - ALMA - JWST/ELT - VLT/MUSE, SINFONI - SKA
kinematic tracers - rain/cca
observational tests
(massive galaxies in groups and clusters)
spectral line broadening = turbulent motions vs. line shift = bulk motions
MG+18
1-3 sigma SIMS
1-3 sigma SIMS
VIMOS IFU single spectra
HI, CO absorption
ALMA, VLA, WSRT
substantial line broadening and small scatter large line shifts and narrow broadening: accreting clouds
red points: ~80 systems (Hα+[NII], HI, CO, [CII] lines) — contours: SIMS lognormal distributions
• r < 100 pc funneling of clouds with 100s km/s
(recently probed by ALMA, e.g., N5044, A2597)
kinematic tracers - rain/cca
observational tests
(massive galaxies in groups and clusters)
spectral line broadening = turbulent motions vs. line shift = bulk motions
MG+18
1-3 sigma SIMS
1-3 sigma SIMS
VIMOS IFU single spectra
HI, CO absorption
ALMA, VLA, WSRT
ALMA A2597
CO absorption Tremblay+16-18
substantial line broadening and small scatter large line shifts and narrow broadening: accreting clouds
red points: ~80 systems (Hα+[NII], HI, CO, [CII] lines) — contours: SIMS lognormal distributions
• r < 100 pc funneling of clouds with 100s km/s
(recently probed by ALMA, e.g., N5044, A2597)
athena x-ifu
synthetic observations
“real”
(3D hydro sims)
synthetic
586 Voronoi
tessellation
(125 arcsec2),
exp. ~ 400 ks
Roncarelli, Gaspari, Ettori, et al., 2018 Coma-like cluster - subsonic turbulence (L~500 kpc)“black hole weather”
program
r vir
0.1 r v
ir
⇡ tcool > tage
r co re
diffuse
c phase
⇠ kp
3 r vir POUT
10
8 r vir entrainment
10
9 .3 r vir ṀOUT
10
Ṁout outskirt hot halo
SMBH
Ṁcool
Ṁ• 5 rS
100 r
S
CCA
colli Ṁcool
sion
s 10 7 rS Lx
CCA
cond cold phase
ensa
tion
10 9 r
S
10 10
rS
5. self-regulation Gaspari et al. 2019x-ray halo scaling relations of smbhs
Gaspari et al. 2019
Bayesian analysis:
85 galaxies,
groups, clusters
ETGs (blue), S0s
(green), Ss (cyan)
DIRECT BH
MASSES, e.g., Rg ⇠ 0.03 R500
OPTICAL “TEMP” Kormendy+13, X-RAY TEMP
vBosch+16
X-ray scalings
lower scatter and
larger correlation
Rg ⇠ 0.03 R500
OPTICAL LUM X-RAY LUMx-ray halo scaling relations of smbhs
Gaspari et al. 2019
Bayesian analysis:
85 galaxies,
groups, clusters
ETGs (blue), S0s
(green), Ss (cyan)
DIRECT BH
MASSES, e.g., Rcore ⇠ 0.1 R500
OPTICAL “TEMP” Kormendy+13, X-RAY TEMP
vBosch+16
X-ray scalings
lower scatter and
larger correlation
Rcore ⇠ 0.1 R500
OPTICAL LUM X-RAY LUMx-ray halo scaling relations of smbhs
Gaspari et al. 2019
red: BCGs
magenta: BGGs
grey: isolated/field/satellitesx-ray halo scaling relations of smbhs
(indirect properties) Gaspari et al. 2019 all within core region
gas DENSITY gas MASS TOT MASS (stars+gas+DM)
gas PRESSURE Compton parameter gas fractionsAGN feedback MG+2012
cycle
(> kpc)
L>H z (kpc)
nonlinear
condensation
DENS
x (kpc)
CCA rain
feed SMBH
Logn n
Log
feedback boosted
PHASE PLOT
Lx-ray halo scaling relations of smbhs
(models)
CCA(gas)-driven BH growth vs. merger-driven BH growth
ALL SMBHs
sub-dominant
growth channel
Gaspari et al. 2019 total
predicts well the observed BH mass ONLY
BCGs major mergers
low N mergers + steady scatter also rule out non-causal models (CLT)“Black Hole
Weather” tight X-ray halo Roncarelli, Gaspari, Ettori+2018
discussed results scalings of SMBHs merger-driven
Gaspari+2019 turbulence (Athena)
Gaspari+2017
CCA
0.1 r v
ir
⇡
4. r co re
c
⇠ kp
3 r vir POUT
10
ows
outfl
3. 10
8 r vir entrainm
ent
10
9 .3 r vir core hot plasma 5.
hot plasma halo rvir
SMBH
cold phase
Ṁ• 5 rS warm phase
100 r
2.
S
CCA
colli
sion
s 10 7 r
S
CCA
cond
1. ensa
tion
10 9 r
S
10 10
r
S
molecular clouds Gaspari+2018
feeding
BH shadows warm filaments/hot gas turbulent hot halos
correlations Gaspari+2017EXTRAS
x-ray halo scaling relations of smbhs
fundamental planes
Gaspari et al. 2019
optical FP X-ray FPx-ray halo scaling relations of smbhs
multivariate correlations
Gaspari et al. 2019
optical “fundamental plane” X-ray “fundamental plane”You can also read
