Subaru PFS Cosmology

Tomomi Sunayama (U. Arizona): On behalf of PFS Cosmology WGTimeline of spectroscopic galaxy surveys
Stage-III Dark Energy Experiments (BOSS, eBOSS) are nishedand now DESI and Subaru PFS will start taking data…

arXiv:2212.09094
Credit: SDSS, NOIRLab, NAOJ, ESA/C. Carreau, NASAfi❖

Galaxy Map: Spectroscopic Survey DesignHigherPFS
Redshift
Roman

Wider
Area

DESI
EuclidThe growing PFS Collaboration

PI: Hitoshi Murayama (Kavli IPMU/UC Berkeley)❖Project Of ce: Kavli IPMU, Kashiwa, Japan❖

Technical work: Princeton, JHU, ASIAA (Taiwan), Caltech, LNA (Brazil), LAM (France), Nat’l Astronomical
Observatories of Japan (NAOJ)fi❖

❖

8.2m diameter telescope onMaunakea, Hawaii (medianseeing 0.6 arcsec)❖

Fiber-fed spectrograph fed bySubaru wide- eld corrector❖

2400 bers over 1.25 sq deg
FOV at prime focus❖

Optical-NIR coverage from380nm-1260nm❖

Facility instrument for Subaru
Telescope (anyone with
Subaru access can apply)❖~4x greater spectroscopic
ef ciency than DESI (N ber x
Mirror Area / D ber2)

fififiSubaru Prime Focus Spectrograph (PFS)Focus Spectrograph (PFS) on Subaru

Subaru Prime Focus Spectrograph (PFS)

ary of the current status of the PFS project❖ 8.2m diameter telescope onSpectrograph(PFS) is a highly multiplexed fiber spectrograph for the Subaru
Maunakea, Hawaii (medians uniqueseeing
in severalways
GTC0.6 arcsec)
u is one of the largest telescopes❖ Fiber-fed spectrograph fed by
HETwith unparalleledfieldofview
Subaru wide- eld corrector
e of the best sites for an excellent❖2400 bers over 1.2 sq deg
FOV at prime focus

KeckSALT
Subarufififi

overs the wavelengths 380–
❖ Optical-NIR coverage fromm that allow for galaxy survey
380nm-1260nm
o gap in redshift range❖ Facility instrument for Subarue (Subaru
Measurements ofTelescope (anyone withVLT
s and Redshifts)
combines
Subaru accesscan apply)HSCng) and PFS (spectroscopy) using❖ ~4x greater spectroscopic
Geminime telescope
andthesame
fieldsef ciency than DESI (N ber x
scope ofscience
MirrorArea / Dwithber2) three, cosmology, galaxy evolution, and galactic archaeology

LBTtelescopes ≥8m

8.2m diameter telescope on
Maunakea, Hawaii (medianseeing 0.6 arcsec)❖Fiber-fed spectrograph fed bySubaru wide- eld corrector❖

2400 bers over 1.25 sq deg FOV
at prime focus❖

Optical-NIR coverage from380nm-1260nm: NIR=940-1260nm❖Facility instrument for Subaru
Telescope (anyone with Subaru
access can apply)❖~4x greater spectroscopic
ef ciency than DESI (N ber xMirror Area / D ber2)

fi❖fifi

Subaru Prime Focus Spectrograph (PFS)Complementarity with DESI-II/Spec-S5❖

DESI is observing ELGs at z<1.6 and DESI-II is planning toobserve LBGs at z>2.5

Complementarity with DESI-II/Spec-S5❖

PFS can bridge the gap between DESI and DESI-II withcomparable constraining power!

nimiler
PyraScientific Themes of PFS Survey
Cosmology

GalaxyArcheology

GalaxyEvolution

Scientific Themes of PFS Survey• Nature of Dark Energy• Sum of Neutrino Mass

Cosmology

Nature ofDark Matter•

GalaxyArcheology•Test Theory of Gravity• Assembly History

Galaxy of GalaxiesEvolution

Scientific Themes of PFS

From PFS-SSP proposalSurvey Design of PFS Cosmology Program❖

Accurate and robust cosmological constraints using the single tracer (4 million[OII] emission line galaxies) to map evolution of the large-scale structure of
the Universe in a wide range of redshifts, 0.6 < z < 2.4, over 1200deg2❖

Other galaxy surveys only go to z=1.6 (DESI) and z=2 (Euclid), meaning
2<z<2.4 is a unique territory of PFS

Discovery Space: galaxy surveys are trying to explore…
❖Why do we spend time and money for these large galaxy surveys?

By Kyle Dawson

Discovery Space: galaxy surveys are trying to explore…
❖Why do we spend time and money for these large galaxy surveys?

By Kyle Dawson

Overview❖❖

What is Subaru Prime Focus Spectrograph (PFS) Survey?
❖PFS Instrument/Collaboration❖The strength and uniqueness of PFS❖

Scienti c Goals from three programs

What are we trying to do in the cosmology program?
❖Constraining sum of neutrino mass❖

Measuring Dark Energy❖

Testing theory of gravity

Where can we do to constrain DM models?

fi❖

Overview❖❖

What is Subaru Prime Focus Spectrograph (PFS) Survey?
❖PFS Instrument/Collaboration❖The strength and uniqueness of PFS❖

Scienti c Goals from three programs

What are we trying to do in the cosmology program?
❖Constraining sum of neutrino mass → High number density of ELGs❖

Measuring Dark Energy → Wide redshift range❖

Testing theory of gravity → Synergy with Subaru HSC survey

Where can we do to constrain DM models?

fi❖

Correlation Functions: Statistical tool to quantify galaxy distribution❖Galaxy correlation functions measure an excess probability(relative to Poisson) of galaxy pairs separated by distance r.

dP = n2 (1 + ⇠(r))dV1 dV2Zd3 kik·r⇠(r) =P(k)e(2⇡)3<latexit sha1_base64="gfSG8PrBq3n8YEiKAAxdk0temh8=">AAACAnicbZDLSgMxFIbP1Futt1FX4iZYhBahzBRBN0LRjcsK9gLtOGQyaRuayQxJRiyluPFV3LhQxK1P4c63Mb0stPVAwsf/n0Ny/iDhTGnH+bYyS8srq2vZ9dzG5tb2jr27V1dxKgmtkZjHshlgRTkTtKaZ5rSZSIqjgNNG0L8a+417KhWLxa0eJNSLcFewDiNYG8m3D8LqhbgrF9yT9gMryGIxrPsuMlfZt/NOyZkUWgR3BnmYVdW3v9phTNKICk04VqrlOon2hlhqRjgd5dqpogkmfdylLYMCR1R5w8kKI3RslBB1YmmO0Gii/p4Y4kipQRSYzgjrnpr3xuJ/XivVnXNvyESSairI9KFOypGO0TgPFDJJieYDA5hIZv6KSA9LTLRJLWdCcOdXXoR6ueQavjnNVy5ncWThEI6gAC6cQQWuoQo1IPAIz/AKb9aT9WK9Wx/T1ow1m9mHP2V9/gCRkJT2</latexit>“Correlation
Function”<latexit sha1_base64="6HtEWRgAN5F4iu7HFAwuqgEqmms=">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</latexit>

If the density eld is a random Gaussian, it can be fully
characterized by the correlation functions.
fi❖“Power Spectrum”

PFS Cosmology program will explore…
❖How well can we measure the sum of neutrino mass?

Neutrino Mass HierarchyΣmν = 0.06eVΣmν = 0.1eV∑mν = 0.1eV is a key to test the hierarchy❖

Deciding the mass
hierarchy sets a
concrete target for theneutrino-less double
beta decay
experiments❖

Can test whether
neutrinos are Dirac orMajorana

What does neutrino do on large scale structure?
❖Neutrinos decoupled when they were still relativistic,
hence they wiped out structure on small scales
Without Neutrinos

With Neutrinos

Agarwal&Feldman 2010

What does neutrino do on clustering of galaxies?
❖Neutrinos suppress power spectrum (clustering of galaxies)❖PFS can achieve σ(Σmν) = 0.02eV!

Abazajian+2013

High-number density=can push to smaller scales❖

PFS Cosmology program keep the high-number density at 0.6<z<2.4, which enables us
to use small scale clustering.

❖Going to smaller scales (k=0.5h/Mpc) can improve the neutrino mass constraint by 30%

Implication on Ultra-light DM❖

Ultra-light DM also suppresses power spectra on small scales
due to the macroscopic de Broglie wavelengths of ultra-light DM

Ferreira+2020

Current constraints on axions❖Constraints are from Planck and BOSS for various axion
massesRogers+2023

PFS Cosmology program will explore…
❖What can we learn about Dark Energy?

PFS can measure Dark Energy…
❖ΩDE(z) to about 7% accuracy in each redshift bin❖

We can test the evolution of the Universe with a single tracer!

PFS
UniqueTerritory

Discovery Potential: Time Evolving Dark Energy
There is a signi cant theoretical motivation for darkenergy potentials with periodic modulations.

fi❖Where are we now? Concordance Cosmology?
❖Improvements in statistical precision reveal tensions in cosmology
Clumpiness of the density uctuation

Evidence for suppression ofstructure growth?

Minh+,2023

flValentino+,2020

Constraints on growth of structure from PFS❖

We can constrain S8 comparable to ACT CMB lensing
measurement and growth rate of structure much more
precisely than any existed measurements.

Ultra-light axions and the S8 tension❖❖

Axions can be anexplanation to the S8tension?

Ωa and S8 aredegenerate

Rogers+2023

Testing theory of gravity: synergy with HSC❖Combining galaxy lensing from HSC and clustering from PFS ca be a powerful probe to testtheory of gravity❖

Recently, the review paper (2212.09094) is published (led by Dr. Arai, Prof. Yokoyama andProf. Miyatake at Nagoya University/KMI)

Shankaranarayanan&Johnson2022

Summary❖

Subaru PFS Cosmology program is unique to have a wide
redshift range, high number density of ELGs, and having asynergy with Subaru HSC survey.

❖PFS Cosmology program will measure the sum of neutrinomass with σ(Σmν) = 0.02ev, which will enable us todistinguish the mass hierarchy of neutrino.

❖High number density of ELGs enables us to measure powerspectra on small scales.

❖Observing ELGs at z=2-2.4 is a unique strength of PFS
cosmology program and enables us to trace the redshift
evolution of growth of structure and dark energy density

PFS is supported by …
❖

Prof. Naoyuki
Tamura(Kavli IPMU)

Without all these people, Subaru PFS will not
happen and each person greatly contributes
and push the project moving forward!

Prof. Yuki
Moritani(U. Hawaii)

Dr. KiyotoYabe(Kavli IPMU)