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H D> F MD @ > F@ FIP 1 DH DM>> @MDIH CD MI f / M@ M DH
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99 GA+42 84

22 89 GG9&

Resolved Stellar Population in MW
Complex (sub-)structures beside disk

Pan-STARS(Slater+2014)

Inner/ outer halos
Over-densiBes, streams in halo
Numbers of ultra faint dwarf satellites
Bootes I dSph, Subaru/S-CamSlone Digital Sky Survey
UMa I

Her

Boo II(Okamoto+2012)(e.g. Belokurov+2007)

Kop1

Boo I

Pal5Suriittagareas stg
Leo TSeg1mLeo VVirgo
over-density Leo IVeros rin

ComaMonoc

CVn IIOrp

CVn I

ha nWil1stream

UMa IIResolved Stellar Population in LG and beyond(Martin+2013)

Extended stellar halos
Over-densiBes, streams
Numbers of satellites
PISCeS Survey / Centaurs A(11deg2, 80pointings,175h, Magellan/Megacam)(Crnojevic+2016)

PAndAS Survey / M31 & M33(300deg2, 400poinNngs,220h,CFHT/Megacam)angular momentum

Astrometry + Spectroscopy
cross-match between GAIA + APOGEE (Helmi+2018)

Energyr< 5kpc
13 GCs associated?

A merger with GAIA-Enceladus(M*=6*106MSUN when fell in at 10Gyr)
led the formaNon of thick disk
and the inner-halo?

High Mg pop

thick disk

Low Mg pop
thin disk
Fornax dSph

accreted stars in MW halo
APOGEEHigh Mg pop in halo: net Galactic rotation
similar to thick disk pop, in-situ
Low Mg pop in halo: little-no net rotation
likely an accreted population
LAMOST survey -> Subaru/HDS

α-elementfrom massive stars
LMC

neutron-capture(r-process)element
merger of binary
neutron stars?
Sgr dSph
APOGEE (Hayes+2018)

LAMOST+Subaru/HDS (Xing+2019)

HI map (Yun et al. 1994)

Galactic Archaeology beyond LG with HSC[Fe/H]=-2.3-0.75

NGC4631 @ 7Mpc

(1.8deg2, 1pointing, 18h, Subaru/HSC)

R25

Tanaka+2017

Okamoto+2015, 2019

M81 @ 3.6Mpc(6deg2, 7poinBngs, Subaru/HSC)

Subaru Near-Field Cosmology Survey
S19A-S20B
PI: S. Okamoto (Subaru)
N. Arimoto (NAOJ), A. Ferguson (Edinburgh), M. Irwin (Cambridge)
M. Chiba (Tohoku), K. Komiyama (NAOJ), M. Tanaka (Hosei)
M. Tanaka (NAOJ), J. Koda (Stony Brook), M. Rich (UCLA)
M.G. Lee (Seoul), I.S. Jang (AIP), J. Kang (Seoul),
J. W. Lee (Seoul), R. Zemaitis (Edinburgh)

NGC247

NGC253
NGC4244

NGC5236(M83)

NGC7793

NGC4736(M94)
12NGC4236

S404RsPr~uAccretion history of MW
HSC-SSP: sub-structures, satellites-> PFS-SSP: velocity, [Fe/H], [α/Fe]-> TMT/WFOS,HROS : heavy elements& proper motions
Takada san’s talkLG galaxies
HSC (PI-based) -> PFS-SSP -> TMT/WFOS
Milky Way bulge, outer disk
ULTIMATE, small-JASMINE, GaiaNIR?

taken from Chiba-san’s slide at PFS 10th all-hand meeBng

taken from Subaru+TMT Science book(Purcell+2011 changed by M. Ishigaki)

3

While these early studies suﬀered from limitations,the prominent one being the inconsistency whether to
use the brightest cluster magnitude, the average magnitude of a sample of globular clusters, or to derive thepeak magnitude in the distribution, they have alreadyin 1960-ies demonstrated that globular clusters may be
useful distance indicators. Some more modern determinations of the Hubble constant using the GCLF are
discussed in Section 6.
In 1970 Racine remarked that the brightest clusters
in M87 and in the Local Group galaxies, the MW and
M31, may be diﬀerent (Racine 1970), and shortly thereafter the brightest clusters were not used any more as
standard candles. Instead the GCLF maximum value
was established as the standard candle (Hanes 1977a)
and this method is described in the next section.
Given that the brightest clusters are not a standard
candle, I do not discuss them further here. It is worth
mentioning, however, that they are well worth a study
on their own, because they contain important clues forthe GCLF formation and overall shape (see the discussions by McLaughlin 1994; Richtler 2003, 2006), and because they represent a link between the star clusters andthe so-called Ultra Compact Galaxies or Dwarf-Galaxy
Transition Objects (Hilker et al. 1999; Haşegan et al.
2005; Rejkuba et al. 2007; Mieske et al. 2002, 2008).

MWGCLF (Rejkuba+2012)

すばるとTMTで開く銀河考古学
Resolved stellar photometry beyond LG:

HSC: stellar halo profile, populations, sub-structures, satellites,-> PFS: velocity, metallicity of bright sources (BSG, RSG, GCs)-> TMT/WFOS,HROS: more detailed abundances, faint sources
Subaru-ULTIMATE
TMT/IRIS

3 The GCLF distance determination method

4m limit
PFS limit

The main premise of the GCLF method is that theold globular clusters magnitude distribution exhibits auniversal shape that is characterised by some numberthat can be used as the standard candle to measure
the distances. The distance determination method isthen conceptually very simple and observationally relatively inexpensive, as it does not require time-series
imaging: it is only necessary to measure luminositiesof all globular clusters in a given target galaxy reaching a suﬃciently deep limiting magnitude to recover thecharacteristic magnitude, build its magnitude distribution, and compare it with the known magnitude distribution of globular clusters in the MW for which theGCLF standard candle is calibrated based on accurate
individual cluster distances from well understood andwell calibrated primary distance indicators. Of course,
the real measurement has additional complications, andseveral corrections and sources of error are discussed
below and in Section 7.
Figure 2 shows the modern version of the GCLF forthe MW globular clusters based on the 2010 compilation of the Harris McMaster Milky Way Globular Cluster catalogue (Harris 1996). The black histogram shows

Okamoto+2015, 2019

PFS limit
for GCsat M81
4m limit

Fig. 2 The Milky Way GCLF based on the 2010 version of the Harris (1996) catalogue for 129 clusters withE(B − V) < 1.0 is shown with black histogram. The subsetof these clusters that have [Fe/H] < −1 dex is plotted ashatched blue histogram

the distribution of 129 clusters with E(B − V) < 1.0,
while a subset of these that are more metal-poor than
[Fe/H] < −1 dex is shown as hatched histogram. Overplotted to both is a Gaussian fit for the distributions.
As was already mentioned by other authors (e.g. Harris2001; Richtler 2003) the name Globular Cluster Luminosity Function is a misnomer due to the fact that it
refers to the magnitude and not luminosity distribution
25of globular clusters in a galaxy.
The most commonly adopted way to derive the characteristic magnitude is to fit the GCLF with a Gaussianfunction, as introduced by Hanes (1977b):R(MV −MV,0 )21dN
2σ2∝ √ exp−dMV
σ 2π(1)The distribution is then characterized by only two parameters: the dispersion (sigma) and the peak (orturnover, TO) magnitude. The latter is the standard
candle and the distance measurement is done relative
to the MW or to the M31 GCLF TO value. The GCLF
is a secondary distance indicator, since the absolute distances to the MW and M31 globular clusters must beknown. These are based primarily on the RR Lyrae
luminosity scale for the MW globular clusters, or alternatively on the Cepheid distance to M31 (Section 5).
It has to be emphasised that the fitting of the globular cluster magnitude distribution with a Gaussian

M81 young/old stars @ 3.6Mpc

S404RsPr~uSimulated
Nuclear Star Cluster
at 2Mpc
for 3 h exposures

Resolved stellar photometry beyond LG:(Gullieuszik+2014)

HSC -> PFS-> TMT/WFOS,HROS

J=28
point-sources

E-ELT/MICADO

Subaru-ULTIMATE: more resolved stellar photometry atM. Gullieuszik
et al.: Probing the nuclear star cluster of galaxies with ELTs
outer disk, dense/dusty
SF regions
TMT/IRIS

TMT/IRIS :stellar CMDsof Virgo clustergalaxies?

JWST/NIR-cam

4.6magfor 16.5Mpc

S404RsPr~u,:H
:H M
MC@ M
MI @>IH M >M MC@ M@FF >IHM@HM IA MC@ DFE
H H@ =F D@ A I MC@ @M DF@ J IJ@ MD@ IA @ IF @ M@FF JIJ F MDIH DH MC@ @M@Accretion history of MW : substructure, satellites, extremely metal-poor stars
HSC-SSP -> PFS-SSP -> TMT/WFOS,HROS& proper motions
Milky Way bulge, outer disk
ULTIMATE, small-JASMINE, GaiaNIR?
LG galaxies
HSC (PI-based) -> PFS-SSP -> TMT/WFOSResolved stellar photometry beyond LG: halo profile, populations, sub-structures
HSC -> PFS -> TMT/WFOS,HROS
Subaru-ULTIMATE
TMT/IRIS