Supermassive black hole
formation in the early universe
Kohei Inayoshi (稲吉恒平)
KIAA/PKU
21st September 2023 @DoA, PKU
Introduction &
Research background
Black Holes (BHs)
Three quantities to
characterize the object
Event horizon
M, Q, J
2GM
RSch = 2
c
singularity
for a non-rotating/
non-charged BH
（c.f. ~3km for M◉）
The theory of general relativity predicts that a sufficiently compact
mass can deform spacetime to form a black hole, where gravity is
so strong that nothing (even lights!) can escape from it.
Standard BH formation path
final products
or remnants
https://blackholecam.org/a-massive-star-collapsing-in-upon-itself-forms-a-black-hole/
stellar-mass BHs
(M~10-100 Msun)
Supermassive black holes (SMBH)
powerful engine!
M ~ 106-10 Msun
https://en.wikipedia.org/wiki/Messier_87
https://en.wikipedia.org/wiki/Quasar#
universal existence in galaxies
Artist's illustration of a supermassive black hole. Credit: NASA/JPL/CALTECH
Supermassive BH in Milky-Way
Our Milky-Way Galaxy
Young massive stars
around SgrA*
Supermassive BH in Milky-Way
The Nobel Prize in Physics 2020
R. Penrose
R. Genzel
“for the discovery that black hole
formation is a robust prediction of
the general theory of relativity"
A.Ghez
“for the discovery of a supermassive compact object at the
centre of our galaxy."
Black Hole mass
Early BH-galaxy coevolution
Cosmological coevolution?
Kormendy & Ho (2013)
Galaxy mass
artist’s illustration [ESA/Hubble, L. Calçada (ESO)]
Early BH-galaxy coevolution
Black Hole mass
Co-evolution diagram
?
seed BHs
Galaxy mass
?
History of the universe
Expanding universe:
δρ
T
inflation
cosmic microwave
background (CMB)
https://science.sciencemag.org/
content/319/5859/52
z ~ 10-30
z ~ 6-7
z=0 (today)
0.1-0.5 Gyrs
1 Gyrs
13.7 Gyrs
History of the universe
Dark ages
observable
universe
inflation
First Stars
First Galaxies
First SMBHs
cosmic microwave
background (CMB)
https://science.sciencemag.org/
content/319/5859/52
z ~ 10-30
z ~ 6-7
z=0 (today)
0.1-0.5 Gyrs
1 Gyrs
13.7 Gyrs
High-redshift monster BHs
Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs) X
Most distant z=7.54 Banados et al. (2017)
12
1.2
1.4
Observed wavelength (µm)
1.6
1.8
2.2
Subaru HSC, SHELLQs (Matsuoka et al. 2019)
2.4
2
2
C IV
9
1
cm
2.0
Ly
Å
1
)
1.0
7
0
2.3
f (10
3
Transmission
18
erg s
C III]
6
0.8
2.4
Mg II
0
0.4
zDE
J1
J
H
Ks
0.0
1.0
1.2
1.4
1.6
1.8
2.0
2.2
2.4
Observed wavelength (µm)
Figure 1. Photometry and combined Magellan/FIRE and Gemini/GNIRS near-infrared spectrum of the
Most massive M=10 M
Wu et al. (2015)
10 sun
quasar J1342+0928 at z = 7.54. The FIRE data were collected
on 11–12 March 2017 for a total integration time of
00
3.5 h. We used the 0.6 slit in the echellete mode, yielding a spectral resolution of around 6, 000 over the range
0.8 2.3 µm. The GNIRS spectrum was obtained on 31 March 2017 and 3 April 2017 with a total exposure time of
4.7 h. We used the 0.67500 slit in the cross-dispersion mode, yielding a spectral resolution of around 1, 800 over the
range 0.8 2.5 µm. The spectral flux density ( fl . black line) is shown at the GNIRS resolution, binned by a factor
of two. The 1s error is shown in grey and the orange line represents the best-fitting power-law continuum emission
Mg II
with fl µ l 1.58±0.02 . Regions with low sky transparency between the J H and H Ks bands
are not shown. The
Fe II The inset shows a
red circles show the follow-up photometry obtained with the Magellan/Fourstar infrared camera.
PL
0.4
Gaussian fit to the Mg II line, from which we derive a black-hole mass of 7.8 ⇥ 108 M . The bottom panel shows the
transmission of the Fourstar J1, J, H, Ks filters (red), and the DECam zDE filter (blue); the top panel shows
1000 ⇥ 1000 images of the quasar in the same filters, with
their respective AB magnitudes. The quasar is not detected
0.35
in the zDE image and its 3s -limiting magnitude (zDE,3s ) is reported.
2700
Figure 3:
2800
2900
3000
Figure 1. Discovery spectra of the first set of 11 quasars, displayed in decreasing order of redshift. The object name and the
7/16
estimated redshift (and the designation “NL” for the possible quasars with narrow Lyα emission) are indicated at the top left
corner of each panel. The blue dotted lines mark the expected positions of the Lyα and N V λ1240 emission lines, given the
High-z SMBH population
11
1011
1.0
11
0.8
Wu et al. (2015)
0.6
age (Gyr)
196 QSO samples (z>6)
SHELLQs/Subaru
Wang et al. (2021)
Yang et al. (2020)
10
SHELLQs/Subaru
DELS/DES
DELS/DES
Pan-STARS1
Pan-STARS1
CFHQ
CFHQ
log (M /Msun)
log (M /Msun)
BH mass (Msun)
10
1010
0.9
cosmic age (Gyr)
0.7
1099
SDSS
SDSS
others
others
9
GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
1088
8
1077
7
8 quasars (as of July 2021)
Discovery
J1342+0928
(Bañados+18)
J1007+2115
(Yang+20)
(←now)
*λEdd=1 is assumed for BHs
if not mass measurements
66
6
J0303-1806
BH’s record holders from PKU
7known at z>6 (<10
8 in Gpc-3 per9mag; MUV>-24)
• ~300
9
8
77
8
9
(past→)
redshift z 2
- Needredshift
>1000 deg
coverage rather than depth
z
redshift
KI, Visbal & Haimanetc.
(2020)
- SDSS/PS1/HSC/DES/UKIDSS/VIKING/WISE,
! ρ ! 10 g cm ). The cloud initially
of the densities (10
has a spherically symmetric density profile enhanced by a factor f (=1.6) above the critical Bonnor–Ebert (BE) distribution, an
isothermal sphere embedded in a pressurized medium and supported
in marginal hydrostatic equilibrium against gravitational collapse.
According to cosmological simulations (e.g. Wise et al. 2008), at
the centre of a first galaxy with virial temperature "104 K, forming
in an environment where the H2 formation is suppressed, a warm
(T ∼ 8000 K) cloud with ∼105 M# becomes gravitationally unstable at ρ ∼ 10−20 g cm−3 and collapses. Based on this, we set the
central density and temperature of the cloud to ρ c = 1.67 × 10−20 g
cm−3 and T = 8000 K, giving a mass and radius of 1.17 × 105 M#
and 10.8 pc, respectively. Although we here do not impose an external FUV radiation, H2 is collisionally dissociated for ρ " 10−20 g
cm−3 and T " 6000 K. Note that we neglect the dark-matter gravity since the cloud is already bound by the self-gravity of its gas.
Our simulation box size is (50 pc)3 and refinement is controlled by
insisting that one Jeans length is resolved by at least 64 grid cells
(e.g. Turk et al. 2012). Under this condition, the simulation uses 23
out of the allowed 25 refinement levels, ensuring we are resolved
by the above criteria at all times and giving a limiting resolution of
!0.1 au.
The development of turbulence in the central region of forming
first galaxies has been suggested by numerical simulations (e.g.
Wise & Abel 2007; Greif et al. 2008). In the initial phase of collapse with ∼10−20 g cm−3 , the turbulence is still subsonic in the
cloud. To consider the density and velocity perturbations due to the
turbulence, we initially impose a subsonic velocity field (the root
mean square of the velocity is set to 0.1cs ) with power spectrum
P(k) ∝ k−4 , which corresponds to the so-called Larson’s law for
the contemporary star-forming regions (Larson 1981). To ensure
that the turbulence is adequately resolved, we select the maximum
k-mode value of 1/10 of the number of cells across the cloud.
We consider the non-equilibrium primordial chemistry of 9
−
+
++
) and 13 hyspecies (H, H2 , e− , H+ , H+
2 , H , He, He , and He
drogen reactions selected to reproduce the correct thermal/chemical
evolution of the warm atomic-cooling cloud (reactions 3, 4, 7−10,
12, 15−18, 28, and 32 in table 2 of Omukai 2001). We adopt
the reaction rate coefficients updated by the following studies: 7–
10 (Coppola et al. 2011), 15 (Martin, Schwarz & Mandy 1996),
17 (Stibbe & Tennyson 1999), and 28 (Ferland et al. 1992). The
four helium reactions originally included in ENZO are also present,
although they are not relevant in our calculation. We initially assume a uniform distribution of ionization degree with 10−4 and H2
molecular fraction with 10−7 , respectively (e.g. Shang et al. 2010).
At high density, the chemical reactions proceed faster than the cloud
collapse and chemical equilibrium is achieved. To smoothly connect the non-equilibrium chemistry to that of equilibrium, we solve
which is approximately given by the Jeans length for th
symmetric cloud in the runaway collapse. Finally, not
not include the heating/cooling associated with the ch
tions because their effect is negligible during the therm
of the atomic-cooling clouds.
Rapid SMBH assembly
3 R E S U LT S
Fig. 1 shows the density distribution at the end of the
where the central density reaches ∼10−7 g cm−3 , for f
spatial scales; from the top-left clockwise, large-scal
bution (∼1 pc), the collapsing core (∼0.1 pc), the cen
region, and the protostar formed at the centre (∼10 au)
portion of the cloud undergoes the runaway collapse
lence forms filamentary structures that channel mate
central region (ρ ∼ 10−8 g cm−3 ), feeding the protos
bottom panel presents the density distribution around t
At the end of this simulation, the protostellar mass reac
and its radius &2 au. These values are consistent wi
of the stellar-structure calculation by Hosokawa et al.
assumed a steady and spherical accretion.
Fig. 2 shows the evolution of mass-weighted radia
(a) density, (b) temperature, and (c) H2 fraction. Dur
“The Assembly of the First Massive Black Holes”
Inayoshi, Visbal & Haiman, 2020, ARA&A, 58, 27
BH mass
109-10
bright QSOs
gas accretion
MBH,0
BH mergers
(GWs)
6-7
(tH ~ 1Gyr)
MNRASL 445, L109–L113 (2014)
redshift
seed BH
formation
Figure 1. Density distribution in the plane through the de
four spatial scales: from top-left, clockwise: the large-scale
tion (∼1 pc), a collapsing core by the H− free–bound conti
(∼0.1 pc), the central region around the protostar (∼100 au)
protostar (∼10 au).
10-20
Formation channels of early BHs
The mass of seed BHs would depend on the environments
Pop III BHs
20 < M/M☉< 140
1
GW recoils
Radiation feedback
101–2 M☉
PopIII BHs
Minihalo
4
Tvir <
~ 10 K
Collapsing
protogalaxy
Hyper-Eddington accretion
•
•
M >> MEdd
4
No H2 cooling
2
Pristine gas
JLW > Jcrit
High vbsm
Rapid merger
Atomic-cooling halo
4
Tvir >
~ 10 K
105–6 M☉
DCBHs
SMS
Star formation
(H2 cooling)
No
Prior star
formation
Yes
If N* > Ncrit
First galaxies
Runaway
collisions
3
103–4 M☉
IMBHs
igure 3
1 Pop III remnant BHs with a mass of M• ≈ 101–2 M! , ●
2 massive seed BHs
ormation pathways
of seed&
BHs
in early protogalaxies:
●
KI, Visbal
Haiman
(2020) ARA&A
ith M• ≈ 105–6 M! in ACHs under peculiar conditions such as strong LW radiation ( JLW > Jcrit ), high baryon-DM streaming
3
3–4
cal estio photo-
, (22)
1
Number fraction [M
revious
he mass
On the
crit , the
constant
because
nvelope
n. Note
by the
e upper
entum).
a mass
to disk
e upper
1
Nhalo
]
BH mass function in QSO host galaxies
10
High-z QSO progenitor haloes
w/o radiation feedback
2
Mini haloes (Hirano+2015)
10
3
10
4
10
5
M
high-z QSO seeds
1.3
M
10
6
10
7
101
102
103
M
104
2.8
GW sources
105
[M ]
FigureRHD
11. simulations
The mass distribution
function of
massive
stars
+ semi-analytical
model
for primordial
BH seeding
in a high-I
QSO progenitor halo (red histogram) obtained from the
(Li et al. 2021; Toyouchi et al. 2022; see also Sassano et al. 2021)
§ ⇤ i1HD "⇤,3RHD correlation (see Figure 10). The probability distribuh"
Numerical simulations + Observation data
Radiation-hydrodynamical simulations
ongoing/future multi-wavelength observations
Subaru HSC
JWST
powerful outflows
Lynx
Roman
ALMA
LISA
central BH
cosmological
gas inflows
Toward the understanding of the origin of
SMBH and galaxies in the early universe
Are you excited & motivated?
Gravitational waves
Black holes
(active galactic nuclei)
Astrophysics
Big Bang
General Relativity
first stars
first galaxies
SMBH
?
Cosmology
First SMBHs
Excavating the spectral signatures of
the first massive BHs with JWST
James Webb Space Telescope
JWST
sensitivity
JWST Imaging
Sensitivity
UV
optical
infrared
radio
JWST & Roman for hunting seed BHs
Observed wavelength 1.98µm [(1+z)/16]
Rest-frame ~ 10eV (0.124µm)
JWST cycle 1&2 approved
PI: M.Onoue
10nJy
How to find seed BHs from images?
galaxies
quasars/
seed BHs?
brown dwarfs
Credits: NASA, ESA, CSA,
and STScI
Spectra for fast growing seed BHs
The Astrophysical
Journal
Letters,
931:L25 (7pp), 2022 June 1
RHD
simulations
+ CLOUDY
4
Inayoshi et al.
Inayoshi, Onoue et al.+Ho (2022b)
Observed radiation flux density (nJy)
AB magnitude
(Watarai et al. 2000). Photoheating of th
22 of h
dominated
by
bound–free
absorption
z
=
8,
θ
obs
=
60
Hα
in the UV and soft X-ray bands but X-r
elements is subdominant in the low-meta
10 3
24
Paα
Hβ
Note that the hardness of the incident r
OI
Paβconditions for the onset
Lyα He II
affects Othe
I
Hγ
OI
26
2
accretion
(e.g.,
Takeo
et
al.
2019).
Furth
10
C II]
isotropic and anisotropic radiation fields
bolometric luminosity emitted from28the acc
SED2022). This mod
details in Inayoshi total
et al.
10
BH + equatorial
nebula
radiation flux to the
region (
disk affects the 30
Eddington flux and
therma
imaging sensitivity
F560W
F770W
accretion disk. The
reprocessed compon
1
considered to be the disk emission 32
(see bel
super-Eddington accretion
in excess
of the Eddington
value20.0
is inject
from a dense disk
0
5.0
10.0
15.0
thatwavelength
the flux (μm)
is collimated to the poles as
observed
The simulation domain is separated
2. Spectral
energy
distribution
of the
seed BH with
106 M at accreting
z = 8: the total
• 'luminous
Figure 1. Density structure of theFigure
accretion
flow onto
a seed
BH and
a growing
irradiated
by M
the
BH SE
a
radiation
flux
from
the
nuclear
BH
with
nebular
emission
lines
(magenta),
and
the
emission
from
the
dense
ac
schematic picture describing our SED modeling, which includes three
feeds the central BH. Here, we define the
r ⇠ 0.1 1from
pc (green).
The viewing
angle is
set to ✓obs = 60 . The imaging sensitivity curves with S/N=10 of JW
components: (1) the radiation flux produced
the unresolved
nuclear
disk
✦
regions
as
thatHβ
where
the
electron
fractio
(0.6–5
µm)
and
MIRI
(5–20 µm)
inparcels,
a 10 Hα
ks exposure
time
are Å,
overlaid
(the
open
square
symbol
indicates the
e↵ect
Strong
Balmer
lines
(e.g.,
= 1300
EW
=
100
Å)
of the BH, (2)
nebular emission
lines
emitted
from
irradiated
gasEW
and
of each
the transmission
curve of eachgives
filter atathe
bottom
(arbitrary units).
The filled
square
clear
separation
between
them
bes
(3) radiation from the dense accreting
disk filter),
in the along
RHD with
simulation
domain. The
the
filter-convolved
flux
density
at density
each filter.
The continuum
radiation
flux with several
prominent
lines than
with
,
Δs,
and
θ
are
the
number
of
physical
of
n,
T,
U,
x
path
at
the
ionization
front
is
shorter
✦ quantities
e
obs
Emission lines
of widths
neutral
due to Lyβ
of EWrestoxygen
> 7 Å is observable
NIRCamfluorescence
broad-band filters except for F070W and the
hydrogen nuclei, gas temperature,equivalent
ionization
parameter,
electron
fraction, with the
The
nebular
gas reprocesses emission line
filter. Intergalactic medium absorption is not included here.
thickness of gas parcels, and viewing angle, respectively. The quantities with
recombination of ionized atoms. The ion
brackets ⟨ · ⟩ are the mass-weighted values along the vertical direction (see
10
4
The first AGN discovered with JWST
A z = 5 AGN in CEERS
5
JWST NIRCam
HST + CFHT + Spitzer
Figure 1. The z = 5 AGN candidate presented in this paper, CEERS-AGN-z5-1. (Top:) The snapshot images of seven
Onoue,Optical-to-NIR
Inayoshi & Ding
(2023)
NIRCam filters employed in CEERS. The image size of each panel is 100 .5 ⇥ 100 .5. (Bottom:)
SED of
CEERSAGN-z5-1. The NIRCam flux densities based on model magnitudes are presented in red. CEERS-AGN-z5-1 has a entry in
0
0
0
0
1670
3210
3210 Av = 4
(mag)
(1043 erg s-1 )
-19.4 ± 0.05 4.48 ± 0.08
See text
See text
(1042 erg s-1 )
1.64 ± 0.21
1.67 ± 0.16
34.4 ± 3.4
(km s-1 )
2060 ± 290
1800 ± 200
1800 ± 200
(107 M )
1.3 ± 0.4
0.90 ± 0.22
4.7 ± 1.2
0.15 ± 0.04
0.29 ± 0.08
3.5 ± 0.9
(109 M )
< 6.0
< 60.0
< 60.0
3.9 ± 0.5
5.3 ± 2.1
5.3 ± 2.1
The first AGN discovered with JWST
OTE —The
BH mass for CEERS 1670 uses L5100 estimated from the photometric SED and the line width of broad H↵ (FWHMH↵,broad )
Hidden Little Monsters:
Spectroscopic Identification
of Low-Mass,
Broad-Line AGN at z > 5 with CEERS
quation 1), while for CEERS
3210 we use FWHM
and line luminosity
of broad H↵ (Equation 2). The bolometric luminosity is also
CEERS: L OW-M ASS , B ROAD -L INE AGN AT Z >5H↵,broad
5
nverted from LH↵ for
CEERS 3210.
In the third
row, we show
the case
CEERS
heavily+dust-reddened
with
AV = 4. The H↵
D. Kocevski,
M. Onoue,
K. Inayoshi,
J. Trump,
P. when
Arrabal
Haro3210
et al.is(KIAA
JWST CEERS
team)
minosities are reported as observed, with no correction for potential slit losses.
48
HSC (z=6-7)
Shen+19 (z~6)
Willott+10 (z~6)
Trakhtenbrot+11 (z~4.8)
Greene & Ho 07 (z<0.35)
Liu+18 (z<0.3)
Shen+11 (z~1-2)
Liu+19 (z<0.35)
47
log Lbol [erg s-1]
For CEERS 3210, if we use the observed H↵ luminosity
ithout an extinction correction, then the BH powering this
CEERS 1670
GN may be comparably low-mass as CEERS 1670. How-z = 5.242
ver, if we assume heavy dust attenuation (AV = 4), it beomes a BH accreting at a rate above the Eddington limit.
Figure 6, we show our results assuming both no extincon for the H↵ luminosity and AV = 4 with the bolometric
minosity converted from L5100 estimated from the H↵ luinosity. Adopting a more moderate level of dust extinction
ferred from the observed Balmer decrement in the NIRpec spectrum (H↵/H = 5.3; AV = 1.9), brings the boloetric luminosity of the source closer to the Eddington value.
hus, CEERS 3210 is likely in its most active mode of accreCEERS 3210
z = 5.624
on and on the way to expelling the material that currently
bscures it. Fujimoto et al. (2022) report a dust-reddened
GN at z = 7.19, the BH mass of which is estimated to be
8
BH . 10 M based on the upper limit of its X-ray lumiosity. Although not confirmed, their AGN and CEERS 3210
ay be drawn from the same population of high-redshift
ust-reddened AGN. We discuss this scenario in greater deil in Section 6.3 below.
46
45
=1
λ Ed
44
d
=0
λ
43
.1
d
Ed
λ Ed
=0
d
.0
1
CEERS 1670
CEERS 3210
CEERS 3210 (AV =4)
42
5
6
7
8
log MBH [M!]
9
10
et -al.
(2023), Kocevski
al. (2023)
Figure 6. The Onoue
BH mass
bolometric
luminosityetplane.
Quasar
samples at z 5 are shown as blue and green symbols and conFigure 2. NIRSpec spectra of sources CEERS 1670 and CEERS 3210 taken in the G395M grating with R ⇠ 1000. The 2D spectra are showntours, while low redshift AGN are shown in black. CEERS 1670 and
Many AGNs with JWST…
JWST/NIRSpec Faint AGNs at z = 4
7
5
6
Harikane et al.
6
Broad-line
AGNs; Harikane et al. (2023)
KOCEVSKI ET AL .
Onoue et al. (2023), Kocevski et al. (2023)
10
1
a
NIRCam
NIRCam
NIRSpec Prism
NIRSpec Prism
QSO (scaled), SDSS composite
1
Galaxy (M = 6 10 9M )
0.1
b
CEERS 3210 (z = 5.624)
Flux density [μJy]
Flux density [μJy]
CEERS 1670 (z = 5.242)
Dust Obscured QSO
0.1
Dusty Galaxy (M = 6 10 10 M )
Type 1 QSO + Dusty Galaxy
0.01
A&A proofs: manuscript no. Infant_BHs
0.01
0.5
0.7
1
2
3
4
5
Wavelength [μm]
Figure 1. NIRSpec spectra of CEERS 01244, GLASS 160133, GLASS 150029, and CEERS 00746. For each object, the left
and middle panels show spectra around H +[Oiii] 4959,5007 and H↵+[Nii] 6548,6584, respectively. The 2D and 1D spectra
are shown in the top and bottom panels, respectively. The red dashed line with the shaded region shows the best-fit broad-line
component (FWHM > 1000 km s 1 ) and other red dashed lines show the best-fit narrow components (FWHM < 500 km s 1 ).
For GLASS 160133 and GLASS 150029, we also show the outflow components with FWHM . 500 km s 1 . The right panels
show the spectra around H↵+[Nii] 6548,6584 with the logarithmic scale. The broad-line components only seen in H↵, which
are detected with a higher signal-to-noise ratio than [Oiii] 5007, indicates that these objects are type-1 AGNs.
0.001
0.5
0.7
2
1
3
4
5
Wavelength [μm]
4
Matthee et al.
Figure 3. The SEDs of the two low-luminosity AGN (CEERS 1670 and CEERS 3210) obtained with the JSWT NIRSpec and NIRCam. Left
panel (a): the continuum spectral shape is explained by the composite quasar spectrum of VB01 scaled to match the photometry of CEERS 1670
(blue), and is fitted well with a single power law with an index of αλ = −1.14 (dashed). The galaxy SED model with M! ! 6.0 × 109 M! is
overlaid (red), where the stellar continuum in the F356W filter becomes comparable to the observed F356W flux density. This gives a robust
upper bound of the underlying stellar population. Right panel (b): the source has a blue continuum spectrum with a UV slope of αλ < −3.0 at
Figure 2. Same as Figure 1 but for CEERS 01665, CEERS 00672, CEERS 02782, and CEERS 00397.
λobs ! 1 − 2 µm and a very steep continuum spectrum (αλ ! 2.0). The redder part can be explained either by a heavily obscured quasar (cyan)
or a dusty starburst galaxy (red). As a possible explanation of the blue excess in the spectrum, the unobscured broad-line AGN contribution is
added to the dusty starburst galaxy (blue). In the dusty galaxy model, the stellar mass is set to M! ! 6 × 1010 M! (see the text in Section 6.3).
Hα, Hβ, and [O III] λλ4960, 5008 emission, and
CEERS 3210 also features a He I λ5877.25 line. Both
sources exhibit a weak line near the expected wavelength of the [Fe X] λ6376 coronal emission line. The
G235M/F170LP spectrum of both sources includes the
Maiolino et al.
(2023)
[Ne III] λ3870.86 line, while CEERS 3210 also exhibits
the Hγ λ4341.69 and auroral [O III] λ4364.44 lines.
We measure line fluxes and uncertainties with a
Levenberg-Marquardt least-squares method implemented by
fit that included an additional broad (σ > 350 km s−1 ) Hβ
component but found that this component is only marginally
(<1σ) detected and including it increases the χ20 of the fit.
We report 1σ upper limits for putative broad Hβ emission
that assume the same width as the broad Hα component applied to the local noise of the Hβ region.
Little red dots; Matthee et al. (2023)
Finally, we fit single narrow Gaussians for the
[O II] λ3728.48 (the 3727+3729 doublet is blended
in the R ! 1000 medium-resolution NIRSpec grating),
anuary 1
Many AGNs with JWST…
Li et al.
Onoue et al.
some z  6
opulations
dsley et al.
dditionally
age down
find that a
Z = 0.004,
he smallest
his model
zetti’s law
el of dust
1011.3 Le,
assuming a
Onoue, KI, Ding+. (2023)
noue et al.
See also Kocevski+ (2023)
ced by the
unless a
and their
Li et al. (2023a,b)
e observed
Figure 4. The z ∼ 5 UV luminosity function of AGNs. Our constraint from
Low-luminosity
AGNs
detected
with
are >10 times
CEERS-AGN-z5-1
is shown
in red.
TheJWST
quasar luminosity
function abundant
data
obtained from different surveys are shown: the rest-UV-selected quasars
more
than extrapolation of the QLFs based on SDSS/HSC/others
combining Subaru HSC and SDSS (Niida et al. 2020, cross) and CFHTLS
(McGreer et al. 2018, dot) in blue. The abundance of AGNs at M
= −19.5
Early BH-galaxy coevolution
14
Li et al.
Black Hole mass
Co-evolution diagram
?
Li et al. (2023b)
Detection of stellar light from QSO hosts
seed BHs
Galaxy mass
?
Ding, Onoue & Silverman et al.+KI (2023);
HSC+JWST (PI: Onoue), Nature
Figure 8. The predicted evolution of the BH-stellar mass relation, M• – M? , for quasars at high redshifts of 4 < z < 11, for
Our team members
Wenxiu Li
Haojie Hu
Zhengrong
Li
Kejian
Chen
Jingsong
Guo
Hanpu Liu
Masafusa
Onoue
・Formation of stars, galaxies and BHs at high-z
・BH accretion & AGN feedback processes
・Gravitational waves from binary BHs
Group meeting; Friday 14:00-16:00 @KIAA 1st floor
See also our website
Thank you!