Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey:
Cosmology & Galaxy/AGN
Evolution
Kiyoto Yabe
(PFS project of ce, Kavli IPMU)

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey:• Subaru Strategic Program (SSP): 〜300 nights over 〜5 years‣ HSC SSP has been started since 2014 and continues until 〜2020?
‣ PFS SSP is going to start after the HSC SSP is nished✓ Expected to start from early 2022
✓ A proposal is currently in preparation✓ A survey program with three big science topics

Cosmology

Galactic
Archaeology

Galaxy/AGN
Evolution"Comprehensive Challenge on Standard Model of the Universe and Beyond"

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey:
Hitoshi Murayama[PI of PFS project]
Survey integration
team
Masahiro Takada[Kavli IPMU]

Richard Ellis[UCL]

Science working group co-chairs
Cosmology

Eiichiro Komatsu(MPA/IPMU)

Galaxy/AGN
evolution

Jenny Greene (Princeton)

Galactic
Archaeology

Masashi Chiba(Tohoku U.)

Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey: Cosmology• Scienti c goals:‣ Precise measurement of cosmological parameters‣ Constraint on the neutrino mass hierarchy• Front loading survey because of other competitors?
• Neutrino science and the higher redshift would be uniqueby Masahiro
Grey: DESI[One of the] Expected Main Plotin the Cosmology Paper! by R. Makiya

PFS and DESI arecomparable at z>1.2

Measurements of cosmologicalparameter as a function of redshift

Constraint on Σmν from measurementsof power spectrum with high precision

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey: Cosmology• Target elds:‣ 〜1400 deg2 of HSC-wide elds
‣ cf. eBOSS=〜6000 deg2, DESI=〜14000 deg2

• Targets:‣ Emission line ([OII] emitters) galaxies at 0.6 < z < 2.4‣ Various AGNs (BL AGNs at z>4, MIR/radio AGNs, time variable
AGNs, QSO absorption, and so on...) are also included
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Wide-field imaging with Hyper Suprime-Cam

HSC-D

PFS Cosmology

R.A.

PFS Cosmology
HSC-W

HSC-D/UDDEC
Galactic Extinction E(B-V)

Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey: Cosmology• Target selection for emission line galaxies‣ Basically, color selected sample‣ Improvement of the color selection is on-going•

66, No. 14M emission line galaxies will be
R1-7 detected in total• Survey strategy
Downloaded from http://pasj.o‣ 2 visits for the same eld‣ 15 min. (450 sec. × 2) ineach visit‣ Strategy of the tiling of FoVs
is currently under discussion
Takada et al. 2014
the color–magnitude diagram. Right: The fraction of objects in each cell that6

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)

Too shallow for galaxy science?
• Probably, NO• We (at least I) have experience of Fastsound (FMOS SSP)
‣ On-source exp. time is 〜30 min.
‣ We wrote (and will) science papers on galaxy science• Much larger galaxy sample is obtained in the PFS survey
gray dots: individual data points
composite
spectrum of all~4000 sample

close-upYabe et al. 2015

metallicity

SDSS

GTO sample

Yabe et al. in prep.
Yabe et al. 2015

Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)

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D RAFT VERSION J UNE 1, 2017

PFS
SSP
survey:Galaxy/AGN
EvolutionA
Preprint typeset using L TEX style emulateapj v. 26/01/00• Scienti c goals:‣ Charting mass assembly within the cosmic web (from z〜7 to z〜1)

• Targets:‣ 〜Magnitude limit sample at 0.7<z<2
for IGM tomography‣ Galaxies at z=2-2.5
PFS GALAXYEVOLUTION: CHARTING MASS AS‣ Galaxies at z>3 and LAEs@z=2.2, 5.7, 6.6
UTION: CHARTING MASSASSEMBLY
WITHINTHE
COSMICWEB‣ All in 〜15 deg2 of HSC-D with U-band and NIR/Spitzer
Draftcoverage
version June 1
Draft version June 1, 2017

ABSTRACTHα[OIII][OII] MgII
Lyα
ABSTRACTWe describe an ambitious 60 night survey to chart the evoluti
nightStar
surveyto chart the evolution
formation
Ionizationof typical galaxies during the epoch (0.7 < z <
2)
at
which
half
of
the
stellarmassingalaxies
isassembled.
The
Winds
Reionization
rates
Metallicity
ass in galaxies is assembled. The survey will cover 11 PFS pointings (⇠ 14.5 deg2 )in ⇠23.0
the HSC
Deep
fields.
Galaxies
to JAB⇠23.0
or yAB ⇠2
es down to JAB
or yAB⇠22.5
will beselecteddown
accordingto theirphotometricredshifts.
The
spectrawillages,
haveandsufficient
S/N torates
measuree sufficient S/N
to measurestellarmasses,star formation
as wellstellaasWith
300,000
galaxies,
volumeequivalent
the SDes, a volume redshifts.
equivalent to
the SDSS
legacysurvey aandhigh sampling,
thistosurveyrepresents
a theuniqueopportunity
to investigate
the rolejust
ofafterthe cy to investigate
the role ofcosmicweb in shaping
galaxy properties
mation activity
duringthe major
build-upof the quiescentpopulation.
Wethe
willm
theandpeakof thecosmicstar formation
activityand during
alaxies with theanisotropic
environments
tracedby the cosmic
web,
to disentangle
linkthephysicalproperties
ofgalaxieswiththeanisotropic
envi
from slides by J. Greene

k hole feedback, merging, halo masses and other environmental factors on galaxy

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey: Galaxy/AGN Evolution• Scienti c goals:‣ Charting mass assembly within the cosmic web (from z〜7 to z〜1)

• Targets:‣ 〜Magnitude limit sample at 0.7<z<2‣ Galaxies at z=2-2.5 for IGM tomography‣ Galaxies at z>3 and LAEs@z=2.2, 5.7, 6.6‣ All in 〜15 deg2 of HSC-D with U-band and NIR/Spitzer coverage
As of Aug. 2018

XMM-LSS

DEEP2-3

COSMOS

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey: Galaxy/AGN Evolution"Current" plan of target sample
sampleredshiftmag / flux limit exp. time

Total area: 14.5 deg2

numberdescription(hours)low-z (main)

0.7<z<2J~23

2~230,000main compoent

low-z (deep)

0.7<z<2

J~22.5

12~14,000

deep component

high-z (IGM)

2.1<z<3.5

g~25, y~24

6-12

~44,000

IGM tomography

very high-z

3.5<z<7.0

y~24.5

6~22,000

very high-zLAE

z=2.2, 5.7, 6.6

L(Lya) ~ 3-5×1042

3-12~15,000

LAEs

AGN

variousvariousvarious~10,000

AGN• The total observing time is 70 nights (including weather factor)• A single pointing is observed in 40-50 hours

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey: Galaxy/AGN Evolution“ISM properties"

Metallicity

Ionization diagnostics

Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey: Galaxy/AGN Evolution
Build-up of “red sequence"
Velocity dispersion

Number density of poststar burst galaxies

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey: Galaxy/AGN Evolution
Out ow velocity as a function of SFR
SFR vs. Environment

All these properties as afunction of “environment"Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey: Galaxy/AGN Evolution

Tomographic reconstruction of 3D gas distribution using
Lyα forest (Lee et al. 2014)

HI 21 cm crosscorrelation to LAEs at z>6

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey: Galaxy/AGN Evolution

AGN science2

PFS-AGN TeamTABLE 1
Target selection and observing strategy in the GE survey fieldTarget(1)
BL/X-ray AGNs
0.5 < z < 2.0
2.0 ≤ z < 4.0
4.0 ≤ z < 6.0
6.0 ≤ zSMGs
Radio AGNs
XMP AGNs
IMBHs
RM project
Total

Selection(2)
CLAUDS/HSC/UKIRT/X-rayiAB < 22.5
22.5 < iAB < 23.3
23.3 < iAB < 24.0
iAB < 22.5
22.5 < iAB < 23.3
23.3 < iAB < 24.0
iAB < 24.0
zAB < 25.0
HSC/SCUBA-2 f850µm > 8 mJy
HSC/FIRST detection
HSC NB excess
HSC variability
COSMOS/VVDS variability

total
NAGN
(3)

NAGN
(4)

Nfiber
(5)

Texp
(6)

2,000
1,000
1,000
600
500
600
400
10
100
2,000
···
30
···

500
500
500
600
500
600
400
10
100
200
a few
30
300

1,000 (0.5)
1,000 (0.5)
1,000 (0.5)
1,200 (0.5)
1,000 (0.5)
1,200 (0.5)
800 (0.5)
100 (0.1)500 (0.2)
250 (0.9)
1,000 (0.001)
300 (0.1)
300 (1.0)

1
2
4
1
2
4
4
5
4
3
2
2
0.5×30Nfiber Texp
(7)
7,000
8,000
3,200
500
2,000
750
2,000
600
4,500
28,550Note. — Columns (1) target; (2) selection method; (3) total number of AGNs expected in 15 deg2 ; (4) number of AGNs we aim
to observe; (5) number of requested fibers (the number in parenthesis represents the expected success rate of AGN identification, i.e.,
NAGN /Nfiber ); (6) exposure time (hr); (7) fiber hours.

The wide wavelength coverage of PFS will enable a consistent and uniform MBH estimation with the Mg II line
over the range 0.5 < z < 3.5, and will provide a unique

AGNs with very high frequency (e.g., Alexander et al.
2005). Such AGNs may represent the most active phaseof SMBH growth after galaxy major mergers, hidden be-Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS SSP survey: Galaxy/AGN Evolution• The current plan does not necessarily include everything...
‣ Low-mass emission line galaxies such as Hα/[OIII] emitters at
low redshift‣ Clusters are not target so much (cf. we expect >30
clusters@z=1-2 with Mhalo > 1014 Msun)‣ Time domain science• We are welcome to include additional sample if it makes the
proposal stronger

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS survey planning and simulations
orange: Cosmology
blue: Galactic Archaeology
red: Galaxy/AGN Evolution

As of Aug. 2018

Fiber hour:number of targets
× exposure time

Cosmology

For simplicity, the Cosmology
sub regions

The total

Archaeology

eld is divided into 11

ber hours per program is 1.1M FHs

Evolution* Cosmology and Evolution include AGN
targets

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS survey planning and simulations• For an ideal case of night

Distribution ofobserving nights

allocation, we simulates theactual observing nights‣ Sep. 2021 - Sep. 2026
‣ 1 PFS run = 10 dark/gray nights‣ 30 runs in total (=300 nights)‣ Weather factor = 0.7

twilight ends

twilight startsnight• 1-hour obs. blocks• An observable target
eld assigned to eachobserving block is
selected by "score":‣ Remaining ber
hours‣ Visibility‣ WG progress

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS survey planning and simulations
Running 20 simulations
by changing nights lost
due to bad weather
The average resultof 20 simulations

shaded region: ±1σ

We can achieve>90%
completeness foreach science WG

Low completeness in apart of "CO fall elds","GA M31", "GE XMMLSS and DEEP23"
because they are incrowded R.A.

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)

o
Ev

l

io
ut

n

io
r
p

r

ed
z
i
it

• Using a set of weights [wCO,

wGA, wGE] for the score, theprogress of a speci c science
program can be controlled• Strategy will be discussed in

c
Ar

o
ol
e
ha

gy

io
pr

r

d
e
z
iti

the collaboration with being
led by "survey integrationteam"• We want to maximize thescienti c outputs from thesurvey, but how to evaluate/
quantify the output?

ol
m
s
Co

io
r
yp
g
o

r

d
e
z
iti

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS survey planning and simulations
PFS survey procedure

SPT?

User
interface

Targetselection

ETS
Fiber
assignment

QA
Database
Data archive

both on-siteand off-site?

HSC DB

Data reduction(2D + 1D)

DRP

Observation

ICS

Repeating the observing cycle
to eachother Software
ETSconnecting= Exposure
Targeting
ICS = Instrument Control Software
DRP = Data Reduction Pipeline

Repeating the observing cycle with connecting toeach component

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)• Targets‣ Galaxy/AGN evolution survey‣ 12 different sample components‣ COSMOS galaxy catalog‣ 〜40 hour-visits per pointing

Completeness map• The number of galaxies assigned tobers per visit decreases slightly in theend of the survey• The ( ber-hour-base) completenessreaches 〜80%

The number of targets
assigned to bers

4 pointings (~5 deg2)
simulation

Growth curve for completeness~80%

400 skybers

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)• Different prioritization leads to different results• How do we optimize the prioritization?
‣ Maximize the total survey completeness?
‣ Minimize the target-to-target variation?
case1

case2

~80%

~65%

case4

case3

~70%

case5
~75%

~75%

Further tests anddiscussion are now
on-going

Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)

How to be involved with the collaboration?
• We discuss how to get involve this project later• New science cases to make the survey stronger are welcome• Detailed process to call for additional targets is currently
under discussion‣ Is the science case interesting?
‣ Is the science case feasible?
‣ Does it t with the story of the proposal?
‣ Does it t with the current survey plan?

• If you have some thoughts, please let us (PFS people) know
• We have prepared some tools for your idea

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)ETC and spectral simulator• The project of ce presents information on the baseline of performance‣ summarizing the instrument throughput and the expected sensitivity
and presenting them on our of cial website (https://pfs.ipmu.jp)‣ providing a package of exposure time calculator (ETC) and spectral
simulator on GitHub

https://github.com/Subaru-PFS/spt_ExposureTimeCalculator

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS performancePFS Expected Performance
Summary
5σsensitivity for 1-hour exposure

Spectral arm

Blue

Low res.
Red
Mid. res.

NIR

Wavelength range[nm]

Throughput[%]

380 - 450
450 - 550
550 - 650
630 - 750
750 - 850
850 - 970
710 - 775
775 - 825
825 - 885
940 - 1050
1050 - 1150
1150 - 1260

14.9
24.5
23.9
29.1
30.1
27.8
26.4
28.4
27.3
17.9
19.5
17.1

13

Continuum sensitivity[AB mag]mean representative

Line sensitivity[10 17 erg/s/cm2 ]mean representative

22.0
22.4
22.1
22.2
22.0
21.6
21.6
21.6
21.5
20.9
21.0
20.9

2.9
1.5
1.5
1.2
1.1
1.2
1.3
1.1
1.2
2.0
1.6
1.5

22.1
22.5
22.2
22.5
22.4
22.1
21.8
21.8
21.7
21.5
21.4
21.3

2.8
1.4
1.3
1.0
0.9
0.9
1.1
1.0
1.0
1.3
1.2
1.2

Table 7: The limiting magnitude for a continuum and the limiting flux of an emission line. A point source
is assumed.
*1 Here a point source is assumed

Sensitivity:
Spectral arm

Wavelength range
Continuum 〜22 AB[nm]*2 For continuum, 3-pix binning along spec. direction is applied*3 The representative value at the wavelength free from OH line

Throughput Continuum sensitivity
Line sensitivity*4 The average value in the wavelength window
17
2
[%]
[AB
mag]
[10
erg/s/cm]*5 Seeing FWHM of 0.8 arcsec. is assumed
mean representative mean representative
Line 〜10-17 erg/s/cm2
380 - 450

14.9 https://pfs.ipmu.jp/research/performance.html
21.7
21.8
3.8
3.7

Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS survey simulator• The simulator is open
for the collaboration• Python + Jupyter
notebook running ona remote server

https://pfs.ipmu.jp/jupyterspt/notebooks/example/
example_end-toend_simulation.ipynb

PFS account is required
If you are interested, please
let us know

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS survey simulator• The simulator is open
for the collaboration• Python + Jupyter
notebook running ona remote server

https://pfs.ipmu.jp/jupyterspt/notebooks/example/
example_end-toend_simulation.ipynb

PFS account is required
If you are interested, please
let us know

import module

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS survey simulator• The simulator is open
for the collaboration• Python + Jupyter
notebook running ona remote server

Set parameters

https://pfs.ipmu.jp/jupyterspt/notebooks/example/
example_end-toend_simulation.ipynb

PFS account is required
If you are interested, please
let us know

Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)PFS survey simulator• The simulator is open
for the collaboration• Python + Jupyter
notebook running ona remote server

https://pfs.ipmu.jp/jupyterspt/notebooks/example/
example_end-toend_simulation.ipynb

PFS account is required
If you are interested, please
let us know

Run!

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Galaxy Evolution Workshop 2019 (Kiyoto Yabe, Kavli IPMU)

Summary• PFS SSP survey‣ Cosmology survey✓ 〜1400 deg2 of the HSC-wide elds
✓ Precise measurement of cosmological parameters andconstraint on the neutrino mass hierarchy✓ Competitiveness to other large surveys‣ Galaxy/AGN Evolution survey✓ 〜15 deg2 of the HSC-deep elds
✓ Understand how galaxies form and evolve along the cosmic
large scale structure✓ Many science cases have been discussed so far• Survey planning and simulation are on-going• Some tools have been provided for your own science31