AGN observations Reviews - Masafusa Onoue (MPIA - KIAA / Kavli IPMU) - GALAXY!IGM WORKSHOP, AUG 18, 2021, ONLINE
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GALAXY-IGM WORKSHOP, AUG 18, 2021, ONLINE
AGN observations Reviews
Masafusa Onoue (MPIA -> KIAA / Kavli IPMU)
1
‣ SMBH formation paths (Inayoshi+19)
Why do we observe
AGNs/quasars?
‣ Cosmic evolution of Type-I quasar LF ‣ Quasar-LAE clustering at z=4
(Niida+20) (Garcia-Vergara+19) ‣ Formation and Evolution of supermassive
black holes (SMBHs; MBH~105-10 Msun)
- How did they form at high redshift?
- How did they accrete billion solar mass?
(cf. Inayoshi-san’s review)
- In what local/large-scale environments is
the AGN activity triggered?
2
‣ Schmatic picture of SMBH-galaxy co-evolution (Volonteri12)
Why do we observe
AGNs/quasars?
‣ z=0.4 dual SMBH (Silverman+20) ‣ Redshift evolution of MBH / M* (Ding+20) ‣ Co-evolutionary growth of SMBHs and host
galaxies
- Do SMBHs grow in lock step with the host
galaxies over the cosmic time?
- How does the AGN-driven feedback
regulate host star-formation activity?
- How do gas-rich galaxy mergers affect
SMBH growth?
3
‣ z evolution of Lyα optical depth (Bosman+21)
τeff
Why do we observe
AGNs/quasars?
‣ Jackpot nebula (Hennawi+15) ‣ A z=6.8 metal absorber in a z=7.5 quasar
(Simcoe+20)
‣ High-z Quasars as bright light sources
- Reionization history
- Extended Lyα blobs irradiated by QSOs
- Metal abundance and ionization of metal
absorbers imprinted on quasar spectra
4
GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Highest-redshift quasar studies
5
GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
‣ Known z>5.8 quasars (as of July 2021) Discovery
J1342+0928
Lbol~1047erg/s (Bañados+18)
J1007+2115 • ~300 known at z>6 (-24)
(Yang+20)
- Need >1000 deg2 coverage rather than depth
- SDSS/PS1/HSC/DES/UKIDSS/VIKING/WISE, etc.
J0303-1806
(Wang+21) • Frontier: z~7.5 (Bañados+18; Yang+20; Wang+21)
- 8 at z>7, 50 at z>6.5
- The low-luminosity regime dominated by the HSC
sample (Matsuoka+16-19)
• z=8-10 discoveries expected in 2020s with Euclid,
Roman, and Rubin
6
GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
‣ Known z>5.8 quasars (as of July 2021) Discovery
SDSS
Lbol~1047erg/s
PS1 J1342+0928
(Bañados+18)
DES J1007+2115 • ~300 known at z>6 (-24)
(Yang+20)
- Need >1000 deg2 coverage rather than depth
- SDSS/PS1/HSC/DES/UKIDSS/VIKING/WISE, etc.
J0303-1806
(Wang+21) • Frontier: z~7.5 (Bañados+18; Yang+20; Wang+21)
- 8 at z>7, 50 at z>6.5
- The low-luminosity regime dominated by the HSC
sample (Matsuoka+16-19)
• z=8-10 discoveries expected in 2020s with Euclid,
Roman, and Rubin
7
GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
‣ Known z>5.8 quasars (as of July 2021) Discovery
SDSS
PS1 UKIDSS J1342+0928
Lbol~1047erg/s
DES VIKING (Bañados+18)
UHS/VHS J1007+2115 • ~300 known at z>6 (-24)
(Yang+20)
- Need >1000 deg2 coverage rather than depth
- SDSS/PS1/HSC/DES/UKIDSS/VIKING/WISE, etc.
J0303-1806
(Wang+21) • Frontier: z~7.5 (Bañados+18; Yang+20; Wang+21)
- 8 at z>7, 50 at z>6.5
- The low-luminosity regime dominated by the HSC
sample (Matsuoka+16-19)
• z=8-10 discoveries expected in 2020s with Euclid,
Roman, and Rubin
8
GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
‣ Known z>5.8 quasars (as of July 2021) Discovery
SDSS
PS1 UKIDSS J1342+0928
Lbol~1047erg/s
DES VIKING (Bañados+18)
UHS/VHS J1007+2115 • ~300 known at z>6 (-24)
(Yang+20)
- Need >1000 deg2 coverage rather than depth
- SDSS/PS1/HSC/DES/UKIDSS/VIKING/WISE, etc.
J0303-1806
(Wang+21) • Frontier: z~7.5 (Bañados+18; Yang+20; Wang+21)
- 8 at z>7, 50 at z>6.5
HSC - The low-luminosity regime dominated by the HSC
CFHQS sample (Matsuoka+16-19)
~1/3 from HSC
• z=8-10 discoveries expected in 2020s with Euclid,
Roman, and Rubin
9
GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
‣ Known z>5.8 quasars (as of July 2021) Discovery
SDSS
PS1 UKIDSS J1342+0928
Lbol~1047erg/s
DES VIKING (Bañados+18)
UHS/VHS J1007+2115 • ~300 known at z>6 (-24)
(Yang+20)
Most extreme - Need >1000 deg2 coverage rather than depth
(luminous/massive)
SMBHs - SDSS/PS1/HSC/DES/UKIDSS/VIKING/WISE, etc.
J0303-1806
(Wang+21) • Frontier: z~7.5 (Bañados+18; Yang+20; Wang+21)
More general
(growing /
- 8 at z>7, 50 at z>6.5
matured)
SMBHs HSC - The low-luminosity regime dominated by the HSC
CFHQS sample (Matsuoka+16-19)
~1/3 from HSC
• z=8-10 discoveries expected in 2020s with Euclid,
Roman, and Rubin
10GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
‣ Known z>5.8 quasars (as of July 2021)
Toward mid 2020s Euclid: launch in Fall 2022!
‣ Expected number of z>6 quasars from Rubin/Euclid/Roman (Fan+, Astro2020)
SDSS UKIDSS
Lbol~1047erg/s
PS1 VIKING
DES UHS/VHS
(N>100)
Rubin (N~10)
HSC Euclid
CFHQS Roman (N~1)
11GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
ULAS J1342+0928 at z=7.54
‣ ALMA dust (top) and [CII] 158 μm (bottom); Bañados+19
‣ NIR spectrum (FIRE 3.5 hr + GNIRS 4.7hr; Bañados+18)
J=20.3, H=20.2, Ks=20.1 mag
~0.3” beam
✦ SMBH: MBH=8×108 Msun, Lbol/LEdd=1.5 (Bañados+18; Onoue+20)
✦ Host: SFR=150Msun/yr, Dust mass: 4×107 Msun (Venemans+17, Novak+19), Merger? (Bañados+19)
12GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Billion-solar-mass SMBHs at z>7
‣ Growth history of known z>7 SMBHs (Wang+21)
• The z~7.5 SMBHs all have MBH~109Msun
Edd. Limit accretion
(tuni~0.7Gyr)
rad. efficiency=0.1
Duty cycle=1 • BH mass reaches only down to ~104-5 Msun if
constant Edd. Limit accretion is assumed
- still too massive for stellar remnant seeds
(GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Blueshifts of High-ionization Lines
‣ Normalized BLR line profiles of J1342+0928 (Onoue+20) ‣ BLR blueshifts (wrt [CII] 158μm) vs ionization potential
Blue wrt [CII] redshift Red
✦ Large BLR blueshift at z=7.5 in high ionization lines -> nuclear-scale outflow
✦ Higher-ionization gas traces the gas that is closer to SMBHs?
14GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Rapid Fe enrichment in BLR clouds
tuniv time delay of Fe enrichment expected at z>6
✦ No FeII/MgII break found up to tuniv=0.7Gyr: prompt SNIa / PISNe, or nucleosynthesis in accretion disk?
15GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Two New z~7.5 Quasars
‣ J1007+2115 at z=7.515 (“Pōniuā’ena”; Yang+20) ‣ J0313-1806 at z=7.642 (Wang+21)
ALMA [CII]158μm
MgII
• Selection: J & WISE detection + color cuts • Selection: J & WISE detection + color cuts
• JAB=20.20, MUV=-26.66 • JAB=20.92, MUV=-26.13
• MBH =1.5 x 109 Msun, Lbol/LEdd=1.06 • MBH =1.6 x 109 Msun, Lbol/LEdd=0.67
• Strong BAL feature in CIV & SiIV (+ MgII?)
16GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Statistical Properties of z>6 SMBHs and
Host Galaxies
17GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Quasar LF
‣ z=4-6 QLF (Matsuoka+18) ‣ QLF evolution at z=0-6 (Niida+20)
β=-1.3 (Akiyama+18)
(McGreer+18)
β=-1.2 ×10-0.47
β=-1.2 ×10-0.95
(Matsuoka+18)
Flat faint-end slopes revealed by HSC-SSP
Willott+10 (z=6) Brighter QSOs have peaks at earlier epoch
photon budget during EoR:GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Galaxy/AGN Transition in UV LF
‣ z=4 UV LF (Harikane+21)
‣ HSC J1609+5328 (z=6.923, MUV=-22.7)
Broad Lyα
Transition
regime
‣ COSY (z=7.149, MUV=-21.8; Laporte+17)
Lyα NV 1240
Stellar light contamination is non-negligible at the faint end (i.e., bright galaxies or faint AGNs)
19GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Biases in Morphology-based QSO Selection
‣ The effects of different AGN selection on z=4 UV LF (Bowler+21): ‣ AGN fraction (left) and spectra of MUV~-22.5
QSO selection = point source + color cut sources (right)
HST-based Stacked HST images
SF Galaxy
HSC
fAGN
AGN: α=-1.19 α=-1.83
MUV [mag]
See also Laporte+17; Sobral+18; Grazian+20;
Boutsia+21; Zhang+21; Calhau+21
The observed flat faint-end slopes seem partly owing to the morphology-based selection cut
➡ Spectroscopic or Xray studies are required (e.g., PFS, JWST, Lynx)
20GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Velocity Shifts of BLR High-Ionization Lines
‣ Redshift evolution of CIV blueshifts at z=6-7 (Schindler+20) ‣ Δv(CIV-MgII) vs EW(CIV)
low-z
(SDSS)
z>6
See also Mazzucchelli+17; Shen+19
Larger CIV velocity shifts at z>6; stronger BLR-scale outflow (distinct changes in the BLR properties?)
21GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
High-velocity Nuclear outflow:
Broad Absorption Line (BAL) quasars at z>7
‣ Normalized spectrum of J0313-1806 at z=7.6 (Wang+21) ‣ Normalized spectrum of J0038-1527 at z=7.0 (Wang+18)
‣ AGN disk wind simulation (Proga+00)
Observer
disk
BH
See also Matsuoka+19; Xu+20; Bischetti+ in prep.
2/8 z>7 quasars have >0.1c outflow (0.6% at z=2-5; Rodriguez Hidalgo+20)
Quasar-driven fast outflow more common at z>6?
22GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Quasar-Driven [CII] Outflow:
Individual Detection at z>6
‣ J1148+5152 (z=6.42; Cicone+15) ‣ J1243+0100 at z=7.07 (Izumi+21b) Wing
PdBI [CII]
ALMA [CII]
[CII]
Extended
component
~30kpc
1.3” 0.7”
See also Maiolino+12; Izumi+21a
Large-scale outflow just starting to regulate host star formation:
Propagation of nuclear-scale wind, or radiation pressure-driven dusty wind?
23Table 2
Emission Line Measurements
Matsuoka et al. Lyα + N V λ1240 C IV λ1549 C III] λ1
GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Redshift L L L
Quasar Driven [CII] Outflow:
Velocity Offset (km s−1) L −2400±500 −800±
Flux (erg s−1 cm−2) (9.6±0.4) × 10−17 (2.1±0.4) × 10−16 (1.6±0.5)
Rest-frame Equivalent Widths (Å) 16±1 39 48±10 51±
The Highest-z Low-luminosity Quasar (z = 7) FWHM (km s−1) L 5500±1300 4600±
Individual Detection at z>6
MBH (Me) L L L
λEdd L L L
Note. The velocity offsets were measured relative to Mg II λ2800. The FWHMs were corrected for the instrumental veloc
Lbol=1.4×1046 erg s-1, MBH =3.3×108 M sun (Matsuoka+19)
Matsuoka et al. 2019
‣ J1148+5152 (z=6.42; Cicone+15) ‣ J1243+0100 at z=7.07 (Izumi+21b) Wing
an order of magnitude lowe
quasars at z>7. The es
MBH=(3.3±2.0)×108 Me
PdBI [CII] λEdd=0.34±0.20. As such
ALMA [CII] first example of an ordinary q
blueshift of the C IV emission
suggest the presence of a fast
[CII] nucleus.
Extended The discovery of J1243+010
component HSC-SSP survey to explore SM
Three-color (HSC i-, z-, and y-band) composite image around J1243
arked with the cross-hair. The image size is 1 arcmin on a side. North
of lower-z quasars. The quasar
east is to the left. the survey (including substantia
~30kpc and we are in the course of
Table 1
a
SiIV and CIV BAL remaining candidates. We expe
Coordinates and Brightness
1.3” z>7 by the completion of the
12h43m53 93 0.7” 1400 deg2 in the wide layer.
+01°00′38 5
quasars discovered by other43
Early Bulge Formation at z ~ 7??
8 T. Izumi et al. Courtesy of T.Izumi
(preliminary!)
ALMA observations of the z = 7.07 LLQSO J1243+0100 15
Izumi et al. 2021b, to be submitted
Observed
J1243: [CII] velocity map
Bulge?
M = 3.3 × 1010 Msun
Vrot/σdisp=3-5
0.2” resolution follow-up
Figure 10. (a) Modeled mean velocityscheduled in ALMA C8!
field (moment-1)
(PI: T.Izumi)
of J1243+0100. The contours indicate relative velocities to
the systemic, in steps of ±20 km s−1 . (b) Residual velocity
0.7” (1.8kpc)
component after subtracting the model from the observed
moment-1 map (Figure 4). The residual amplitude is mostly
ALMAofobservations
< 20 km s−1 , indicating a good quality our fit. of the z = 7.07 LLQSO J1243+0100 15
velocity to the systemic redshift, ranging from −60 to +60 km s −1• We experimentally extracted a [CII] rotation
Figure 4. (a) Intensity-weighted mean velocity map of the central 3!! region of J1243+0100. The contours indicate the relative
Figure 11. Radial
−1 profiles of rotation velocity (Vrot ;
in steps of 20 km s . (b) Intensity-weighted velocity
Model
red curve by decomposing (modeling) the
circle) and velocity dispersion (σ ; bluewith
diamonds) of
can be varied in each Residual
dispersion map of the same region. Here the contours indicate 25, 50, 75, and 100 km s−1
. These maps dispmade
were a
883 (PA), all of which ring. For a bet-
884 observed velocity field.
J1243+0100.
conservative 5σ clipping. In each panel, the bottom-left ellipse corresponds
ter convergence, we fixed the dynamical center to the
to our We also plot
synthesized a theoretical
beam. The centralrotation curve made
black plus
with a Plummer potential (red dashed line), which predicts a
denotes the FIR continuum peak position.
•
−1
885 quasar position and Vsys to 0 km s . bulge-scale mass of (3.3 ± 0.2) × 1010 M" with a scale length
886 We first made a series of models having initial guesses
z of
We
! 0.36
found
0.03 kpc,
4 − 6±galaxies
a gradual
respectively.
(Fujimoto
rise in V rot
3
et al. 2019, 2020) . The
toward the
galaxy size→
467
887 of i = 29◦ .5 and PA = 90◦ (see § 3.2.3 and 3.2.5). Al- 468 hostcenter Indication
becomes of a which
slightly smaller, nuclear
is nowbulge??
888 lowing variations of these angles within ±10◦ resulted in consistent with the imfit result within 1σ uncertainty.
•
469
a good convergence at i = 25◦ and PA = 87◦ . Thus, we
889
890 re-modeled the dynamics with fixing the angles to these
470
471 weak
Would
However,
potential be
(< 2σ),model
consistent
the significance
whichofprohibits
a spherical
us from
with
of the halo component
system simulations.
is very
(Plummer
further investi- 1911), See also Smit+17;
25
values. Figure 10. (a) Modeled
A conservative meanwas
5σ clipping velocity field (moment-1)
applied to avoid 472 gating it with the current data. Much deeper [C II] RIzzo+20; Neeleman+20
891
GMGALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
[CII] Outflow of z>6 Quasar Hosts:
Stacking Analysis
‣ Compilation of 48 sources at z>6 (Bischetti+19): ‣ 1kpc-resolution ALMA sample (N=27; Novak+20):
[CII] stacking in the velocity space [CII] stacking of velocity-normalized spectra
Extended
component may
~0.8” beam ~0.2” beam be resolved out?
1σ~0.06 mJy FWHM=1700 km s-1 1σ~0.06 mJy
Velocity / σline
Velocity [km/s]
✴The broad wing in the stacked spectra may be the contribution of
QSOs with relatively wide [CII] (FWHMGALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
QSO Companion Galaxies at z>6
‣ 10-100 kpc-scale companion galaxies at z>6 (Decarli+17) ‣ 6
27GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Short summary 1
Properties
No evolution Maximum MBH, BLR metallicity, host dust/gas enrichment
Evolution QLF, BLR velocity shift, BAL fraction, merger/companion rate
A large sample of z>6 quasars have recently enabled statistical analyses
z>6 SMBHs seem to be matured, whereas some properties do manifest redshift evolution
➡ Hints of rapid assembly of SMBHs and host galaxies?
28GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Missing AGN Populations at z>6
29GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Quasar Evolutionary Sequence
z=0.95
Urrutia+09
SMBH obscured
Gemini Observatory
e.g., Hopkins+08
rest-UV surveys
Current z>6 AGN sample mostly consists of luminous unobscured quasars
30GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Host Environments of z>7 SMBHs
‣ BLUETIDES simulation of z=7 SMBHs (Ni+20)
High-column density gas and dust in
the innermost region can significantly
contribute to the total NH, which
highly depends on the observers’ LoS
The most active growth is
‣ BH4’s angular variation of NH, τ1450, rad. velocity ‣ Time evolution associated with high NH gas!
MBH Lbol Edd ratio NH, ave σ(NH, ave)
obscured
Unobscured
Obscured phase is the key to rapid SMBH growth and SMBH demographics?
31GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Dust-Reddened Quasar at z=6.7
‣ XShooter spectrum of J1205-0000 (Texp=7hr)
Flat continuum at blue side with
strong BAL feature (Nv, SiIV, CIV)
‣ SED fitting with HSC/VIKING/WISE (Kato+20)
Dereddened
E(B-V)=0.12
Lbol,corr=8×1046 erg s-1
Gemini Observatory Observed
A modestly dust-obscured quasar found from the
HSC’s low-luminosity quasar sample at z>6
32The Most Distant “Red” Quasar J1205-0000 GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
38
6 T. Izumi et al.
Dust-Reddened Quasar at z=6.7
4 T. Izumi et al.
J1205-0000 Izumi et al. 2021
(a) Single Gaussian
‣ XShooter spectrum of J1205-0000 (Texp=7hr) χ2/d.o.f. = 37.6/22
The Most Distant “Red” Quasar A
×
B
Flat×continuum at blue side with
strong BAL feature (Nv, SiIV, CIV)
6 × C
T. Izumi et al.
4 T. Izumi et al.
J1205-0000
‣ ALMA dust+[CII] followup (Izumi+21a) Izumi et al. 2021
(a) Single Gau
[CII]: L[CII]=2×109Lsun FIR cont: LFIR=3×1012Lsun
(b) Double Gaussian χ2/d.o.f. = 37.6
χ2/d.o.f. = 21.1/19 Dereddened
Figure 2. Velocity channel maps of [C II] line emission E(B-V)=0.12
of J1205−0000. Each channel is labelled with its central B Lbol,corr=8×1046 erg s-1
× Close companion/merger
velocity in km s−1 . The plus signs indicate the FIR contin- A
× or [CII] outflow?
uum peak position. The three representative Geminioff-center
Observatory posi- Observed
tions (Figure 1) are also marked at the 98 km s−1 channel.
The synthesized beam is plotted in the bottom-left corner. × C
Figure 1. (Top-left) Integrated [C IIContours are drawn at −3, −2 (dashed
−1
km sline),
−1
unit).2,We
3,integrated
4, 5, 7,over a
0.8” ] 158 µm intensity map of J1205−0000 (Jy beam
A modestly
velocity range of ±500 km s−1 relative10, dust-obscured
12,
to the and redshift
systemic 15σ levels (solid
(z[CII] = quasar
6.7224),line;
which1σ found
was = 0.13
determinedmJy
fromfrom
beam
a double the
−1
).
Gaussian
• HSC’s beam low-luminosity
Extended emission quasar black plus sample at positions
z>6
−1 −1
fit to the area-integrated spectrum (Figure 3b). Contours start at ±3σ (1σ = 0.045 Jy beam km s ) and increase in powers
We found a spatially extended [CII] distribution, bright
exists at several off-center
Figure 3.FIR
over
continuum [C II] (3E12 Lsun; of
√
of 2. The synthesized is shown in the corner. The central denotes the continuum peak position. Three
severalspectrum
representative positions to extract off-center contiguous channels.
are marked as A, B, and C. (Top-middle) Spatial distribution of the
Area-integrated 158 µm spectrum
of 2. The 575 Msun /yr),
(A–C) as well as aSubaru
peculiar
HSC y-band map[CII] line spectrum.
−1 −1
rest-FIR continuum emission (mJy beam unit). Contours again start at ±3σ (1σ = 17.6 µJy beam ) and increase in powers J1205−0000 measured over a region of [C II] integrated-
√ 33
same off-center positions are marked. (Top-right) of the same region (arbitrary ""
intensity > 3σ ∩ r < 1 .5. The channel-based sensitivityGALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
A Candidate Obscured Quasar at z>6
‣ J1423-0018 at z=6.13 (Matsuoka+18) ‣ MOSFIRE Y-band (2hr; Onoue+20)
zLyα=6.13
Nv1239
Nv1243
Lyα
Extraction
aperture
(2.2”)
CIV 1548
CIV 1550
FWHMGALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
A QSO-Galaxy Merger at z=6.2
‣ PJ308-21 (Decarli+19)
HST
HST - PSF
Satellite galaxy is tidally
stripped by interaction
with the central quasar
[CII]
ALMA [CII]
20kpc
✦JWST Cy1 GO: NIRSpec IFU (Hβ+[OIII], Hα+[NII], etc.)
- Kinematics of ionized gas
- Host M*, metallicity, etc.
See also: Pensabene+21; Matsuoka+ in prep.
35GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Dual AGN Search with HSC-SSP
‣ SDSS J1416+0033, z=0.43, iAB=18.2 Host Model
SDSS HSC-i
A MgII [NeV]+[OII]
Hβ+[OIII]
+[NeIII]
B
0.”7 (3.9kpc)
Silverman+20; Tang+21
HSC images of SDSS quasars revealing dual SMBHs at zGALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Origin of SMBHs - Host Co-evolution
37GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Redshift Evolution of MBH/M* Ratio
‣ Host stellar mass measurements at z~1.5 (Ding+20)
data ‣ Prediction from six cosmological simulations (Habouzit+ in prep.):
QSO
1.HST 2.PFS model Host (=1-2) Residual Completely different predictions due to different modeling of AGN feedback
Host
Radial profile
*y-axis calibrated with the local
relation of each simulation
×2.7 from z=0: BH-dominant growth?
(but consistent with no evolution when
selection effect taken into account)
M*: HST image
MBH: Hα
38GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
42
Early SMBH-galaxy co-evolution at z ~ 7
ALMA Views of Co-evolution at z>6
Figure 15. Simulated face-on images of the median currently observable quasar in the JWST NIRCam
The host galaxy emission is shown in the top panels, the emission from the quasar in the middle panels, w
in the bottom panels. All images include dust extinction of both the quasar and the host galaxy. These
(preliminary!)
detection sensitivities as predicted by STSci (2017). The field of view is 12 × 12 kpc, or 2."" 23 × 2."" 23. N
scale.
z>6 Met
Izumi dyn vs MBH relation (Izumi+21b)
al. 2021b, to be submitted ‣ BLUETIDES prediction (Marshall+20b)
Marshall et al. 2020
Overmassive SMBHs
Local relation
~ Mbulge
✦Co-evolution relation established already atFigure 16. The relation between black hole mass and stellar mass (left) and black hole mass and bulge m
• J1243+0100 shows a well consistent MBH/Mbulge
✦Less-biased low-luminosity quasars essential
z=6-7?
2018; to
to relations
best-fitting the local
trace
Pensabene et the
galaxies
as given
general
al. 2020),
(assume
in equations (5)
assumingSMBH
and (6). We M
trend
that their stellar
plotdyn = See
a range
mass is equal
of observations of 5 ! z ! 7 quas
also Wang+15; Izumi+18;
to their measured dynamical ma
Mbulge). → Co-evolution relation has been established already at z = 7 !? Pensabene+20;
relation at z = 0 (Kormendy & Ho 2013). This relation is also shownNeeleman+21
Marshall+20ab;
in the left (stellar mass) panel for c
✦Consistent with a recent hydrodynamical model prediction
•
galaxies with M∗ = Mbulge .
Importance of probing lower-luminosity (less-biased lower mass) objects to depict a
39
true picture of the early co-evolution. will be able to detect the majority of companions, with less than We find that 90GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
42
Early SMBH-galaxy co-evolution at z ~ 7
ALMA Views of Co-evolution at z>6
Figure 15. Simulated face-on images of the median currently observable quasar in the JWST NIRCam
The host galaxy emission is shown in the top panels, the emission from the quasar in the middle panels, w
in the bottom panels. All images include dust extinction of both the quasar and the host galaxy. These
(preliminary!)
detection sensitivities as predicted by STSci (2017). The field of view is 12 × 12 kpc, or 2."" 23 × 2."" 23. N
scale.
z>6 Met
Izumi dyn vs MBH relation (Izumi+21b)
al. 2021b, to be submitted ‣ BLUETIDES prediction (Marshall+20b)
Marshall et al. 2020
Overmassive SMBHs
Is Mdyn really a good estimator of Mbulge? (gas,DM,disk inclination, etc.)
Local relation
~ Mbulge
✦Co-evolution relation established already atFigure 16. The relation between black hole mass and stellar mass (left) and black hole mass and bulge m
• J1243+0100 shows a well consistent MBH/Mbulge
✦Less-biased low-luminosity quasars essential
z=6-7?
2018; to
to relations
best-fitting the local
trace
Pensabene et the
galaxies
as given
general
al. 2020),
(assume
in equations (5)
assumingSMBH
and (6). We M
trend
that their stellar
plotdyn = See
a range
mass is equal
of observations of 5 ! z ! 7 quas
also Wang+15; Izumi+18;
to their measured dynamical ma
Mbulge). → Co-evolution relation has been established already at z = 7 !? Pensabene+20;
relation at z = 0 (Kormendy & Ho 2013). This relation is also shownNeeleman+21
Marshall+20ab;
in the left (stellar mass) panel for c
✦Consistent with a recent hydrodynamical model prediction
•
galaxies with M∗ = Mbulge .
Importance of probing lower-luminosity (less-biased lower mass) objects to depict a
40
true picture of the early co-evolution. will be able to detect the majority of companions, with less than We find that 90GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Stellar Mass vs BH Mass at z=6
• JWST Cy1 GO medium ``A Complete Census of SMBHs and Host Galaxies at z=6”
(PI:MO, co-PI: Y.Matsuoka, T.Izumi, X.Ding, J.Silverman)
- NIRSpec G395M Fixed-Slit spectroscopy + NIRCam F150W+F356W imaging
Ground-based MgII-based MBH
Bright
Low-mass
Image decomposition of host stellar and SDSS
near-Eddington
quasar emission with JWST!
Ground-based
←ALMA
M BH=10(Fig.4)
J0859 7.6M
sun
HSC 3σ from this proposal Faint
JWST targets
This Proposal
z~2 High-mass
quiescent
Characterization of SMBH-galaxy co-evolution with 12 lowest-luminosity HSC quasars at z=6:
Hβ-based MBH and host M* (+age) measurements (+ many ancillary science)
41Cy1 GO programs (High-z QSO only)
Prime/
ID program PI instrument science targets Notes
Parallel Time
NIRSpec IFU G395H Satellite galaxy with
Nebular line diagnostics in a merger -> M*, SFR, ionized gas tidal-stripping
1554 at cosmic dawn
Dr. R. Decarli 7.8
kinematics, metallicity,
z=6.2 merger in Decarli+19 PJ308-21
signature seen in HST
ionization parameter + ALMA
First Accreting BH candidates” IR-
NIRSpec FS G395H + MIRI Spec confirmation of IR-dropout X-ray 7 IRAC sources in DCBHs or heavily
1760 dropout heavily obscured X-ray Dr. H. Suh 23.6
LRS sources COSMOS obscured AGNs?
AGNs
A Comprehensive JWST View of the Prof. X. Fan
NIRCam + MIRI imaging/
1764 Most Distant QSOs Deep into the Dr. J. Yang 65.5/8.6
MRS + NIRSpec FS/IFU
Everything on highest-qsos Three z=7.5 QSOs
EoR Dr. E. Bañados
Unveiling Stellar Light from Host NIRCam F150W, F200W, J2054 HST+ALMA presented
1813 Galaxies at z=6 QSOs
Dr. M. Marshall 15.9
F277W, F356W, F444W
Host (SED, M*), companions
J0129 (both SDSS) in Marshall+20
The Role of Radio AGN Feedback in Prof. R. Overzier Ionized gas kinematics and metallicity, TN J1338-1942 Most distant radio
1964 Massive Galaxies at z=4-6 Dr. A. Saxena
23.8 NIRSpec IFU
host stellar population, morphology TGSS J1530+1049 galaxies
Dr. M. Onoue
A Complete Census of SMBHs and Prof. Y. Matsuoka
1967 Host Galaxies at z=6 Prof. J. Silverman
49.5 NIRCam + NIRSpec Host M* + MBH, BHMF, etc. 12 lowest-L QSOs
Dr. T.Izumi, Dr. X.Ding
Mapping a Distant Protocluster
Dr. F. Wang PC member confirmation (target sfrom Protocluster identified
2028 Anchored by a Luminous QSO in
Dr. J. Yang
16.3/5.8 NIRSpec MSA+IFU
HST imaging) + quasar characterization
z=6.63 QSO field
with HSC+JCMT+ALMA
the EoR
Monster in the Early Universe:
Unveiling the Nature of a Dust Dr. J. Yang
2249 Reddened QSO Hosting a 1010 Dr. F. Wang
5.5 NIRSpec IFU + MIRI Imaging Constraining dust extinction, MBH, J0038-0653 Unpublished dusty qso?
Msun BH at z=7.1
Dr. F. Wang 350 galaxies at 5.3GALAXY-IGM WS, AUG 18, 2021, MASAFUSA ONOUE
Summary
✦ Wide-field optical and NIR surveys have revealed ~300 EoR quasars up to z=7.5. More to come with next-
generation survey telescopes coming in mid-to-late 2020s.
✦ Billion-solar-mass SMBHs within the first billion years of the universe have put a stringent constraint on the
early SMBH growth
✦ The most luminous quasars are powered by already matured SMBHs and host galaxies, whereas there are
some possible signatures of BLR that are in the rapid process of formation
✦ AGNs in the early stages of merger-induced quasar activity (early mergers, modestly/heavily-obscured
quasars) have started to be identified from the HSC-SSP
✦ ALMA dynamical mass measurements have shown that the SMBH-galaxy co-evolution may have already been
establishes at z>6; JWST’s direct stellar mass measurements at z>6 will provide more robust evidence
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