KOOLS-IFUによるブラックホール形成環境の解明
Yoshiyuki Inoue (RIKEN) + Kiyoto Yabe (Kavli IPMU)
Shinya Nakashima, Naoki Isobe, Yoshihiro Ueda,
Kazuya Matsubayashi

Seimei Users Meeting @ Kyoto, 2019-08-07

Less Metal,Heavier Remnant Black Holesl Letters, 818:L22 (15pp), 2016 February 20

Abbott et al.

Spera+’15; Abbott+’16

maximum BH mass on metallicity Z, with Z : = 0.02 for the old (strong) and new (weak) massive-star winds (Figure 3 from Belczynski
emnant mass as a function of zero-age main-sequence (ZAMS; i.e., initial) progenitor mass for a set of different (absolute) metallicity
t al. 2015). The masses for GW150914 are indicated by the horizontal bands.

• Less mass loss at lower metallicity (e.g., Spera+’15).

Quantitatively, Belczynski et al. (2010a)
It is, in principle, possible that “heavy” BHs are formed
through indirect
pathssuchthat dorequire a low metallicity,013) and Spera et al. (2015)
showed X-ray
thatLuminous
binaries(XRBs)
asnotultra-luminous
X-raybut
sources (ULXs) may
we consider this very unlikely. For example, the formation ofprescriptions(Vink 2008) signiﬁcantly
favor
lower
metallicity
environment(Belczynski+’10)“heavy”
BHs through the
dynamical mergers of lower-mass
at core collapse and thus the maximum
BHs with massive stars in young clusters has been considered.
from single stars, although the exact
However, these models adopt the optimistic assumption that inmass and ﬁnal BH mass depends on theX-1 mergers,
has 50%offor
oxygensolaris value (Mizuno+’07)
evengrazing abundancecollisions, all ofthan
the mass
ription (see Figure 1).A ULX NGC 1313 suchretained, leading to signiﬁcant BH mass growth(Mapelli &ad to angular momentum transport and➡
•

level slightly below 2σ , while it is roughly consistent with theratio of the expected numbers of massive BHs below and above
Z ∼ 0.2 Z⊙ (see Fig. 1). This might be a further indication that
the SFR is not the only ingredient of the correlation between N BH
and N ULX and that the second ingredient might actually be themetallicity, as proposed in our model.

licity in equation (1). We know from equation (1) thbetween N BH /SFR and Z is not a power law. Howecompare it with equation (8), we can approximate it"!
M⊙ yr−1= 10κ2 (Z/Z⊙ )ι2 ,NBH
SFR

Environment of X-ray Binaries

Mapelli+’10

Rolleston+’00

Figure 5. From left to right: N ULX /SFR versus Z, N BH /SFR versus Z for P98, N BH /SFR versus Z for B10. Filled black circles: entire sam
power-law fit. The error bars on both the x- and the y-axis are 1σ errors. Central and right-handpanels: the error bars on N BH /SFR account fosun (Mapelli+’10)
on the metallicity (see Section 2.3 for details).

• ULXs are hosted by galaxies with Z< 0.5 Z• BUT, galaxies are not chemically homogeneous (Rolleston+’00)⃝C 2010 The Authors. Journal compilation ⃝C 2010 RAS, MNRAS 408, 234–253
ownloaded from https://academic.oup.com/mnras/article-abstract/408/1/234/1055884
y guestn 22 January 2018

➡Let’s see local environment

very effectively ejected from the clusters by few-body encountersat the initial stages of the cluster formation (Poveda, Ruiz & Allen
1967; Heggie 1975; Mikkola 1983; Moeckel & Bate 2010; PflammAltenburg & Kroupa 2010; Mapelli et al. 2011). Also the supernova(SN) explosions can eject massive binaries (Zwicky 1957; Blaauw
1961; Shklovskii 1976; Woosley 1987; Cordes & Chernoff 1998;
van den Heuvel et al. 2000), but probably with lower velocities andat a later stage of cluster evolution, when the massive stars had timeto evolve.
Thus, the distribution of the X-ray sources around stellar clusters
as well as the cluster age can give us a clue on the nature of ULXs
and on the ejection mechanism. Kaaret et al. (2004) have found thatbright X-ray sources (1036 < LX < 1039 erg s−1 ) in three starburst
galaxies are preferentially located near the star clusters, but notwithin them. In a search for optical counterparts of 44 ULXs in
26 nearby galaxies, Ptak et al. (2006) have found that 28 of them
have potential optical counterparts within 2σ error circles and 10 of
those have multiple counterparts. Their astrometric accuracy variedin the range 0.3–1.7 arcsec depending on the object and the method(the best accuracy was achieved for half of the galaxies which havean active nuclei in the centre).
The colliding star-forming Antennae galaxies constitute an obvious target for a detailed study of the separation between the X-ray
sources and clusters, because they contain a couple of dozens bright
X-ray sources (Zezas et al. 2006) and a thousand catalogued clusters(Whitmore & Schweizer 1995). Zezas et al. (2002b) have noticed
that most of the brightest X-ray sources are displaced from theneighbouring star clusters. However, their absolute astrometry hasan ∼1.5 arcsec error (∼160 pc); therefore, they could not possibly
measure displacements smaller than that and prove unambiguously

an association between the X-ray sources and clusters. Thus, thequestion about the association of the X-ray sources and clusters
remains open.
The aim of this paper is to determine the distances between
the brightest X-ray sources and the stellar clusters in the Antennae galaxies using an accurate astrometric solution (with error <0.3 arcsec). We find significant displacement between the ULXs
and the clusters as well as a highly significant association between
them. We also estimate the ages of the stellar clusters. This allows
us to determine the minimum masses of the ULX progenitors.

XRBs are associated with stellar clusters

Ultraluminous X-ray sources in the Antennae galaxie• Correlation between XRBs and stellarclusters (Kaaret+14)

2 O B S E RVAT I O N S A N D DATA R E D U C T I O N
2.1 X-ray source sample• Mostly showing strong emission lines• ULXs are associated with young (<10 Myr)stellar clusters (Poutanen+13)

Downloaded from http://mnras.oxfordjournals.org/ at Uchu Kagaku Kenkyujo on March 1, 2016

The X-ray sources in the Antennae galaxies, NGC 4038/NGC 4039
(see Fig. 1), were surveyed by Zezas et al. (2002a, 2006) and Swartz
et al. (2004). From the catalogue of Zezas et al. (2002a), we haveselected sources situated in the main bodies of the galaxies to reduce the chance that they are background or foreground sources. We
restrict the sample to those having more than 45 counts, which guaranties high accuracy of the coordinates. We then further down selectthe sources, which have average absorption corrected 0.1–10 keVluminosities in excess of 2.75 × 1038 erg s−1 as estimated by Zezas
et al. (2006) assuming a power-law spectrum with photon index" = 1.7 and the Galactic line-of-sight hydrogen column density
NH = 3.4 × 1020 cm−2 (Stark et al. 1992). These luminosities wererecomputed for the distance to the Antennae galaxies of 22 Mpc asrecommended by Schweizer et al. (2008). This distance gives thescale of 107 pc arcsec−1 and the distance modulus −31.71.

512

Figure A6. Same
Fig. A2, but for the source X-42.
J. Poutanen
etasal.

see Figs 2 and A5, Table 1) is situated 0.83 arcsec to the SSW
from X-35 at the edge of a strong dust line. The cluster is notably
reddened (AV ∼ 3.5) and its spectrum is noisy. We find about thesame nebular spectrum as that in X-16 with the [O III] λ5007 line
being brighter that Hβ. However, in the red spectral region He I
nebular lines and [Ar III] are strong and broadened. Interestingly,
there are [Fe III] emission lines in the spectrum like those we observein N5 and N6 clusters close to X-32. The [Fe II] emission lines are
marginally detected.
A5 X-42
This X-ray source is located close (at 0.8 arcsec) to a bright clustercomplex with total (dereddened) V = 17.2 (see Figs 2 and A6,Poutanen+’13

Figure 1. The rgb image of Antennae produced from HST/ACS images taken in FR656N (Hα, red), F435W (blue) and F550M (green) bands. NE bar length
corresponds to 5 arcsec (107 pc/1 arcsec). The VIMOS frames of the studied ULX regions together with Chandra positions (1.0 arcsec radius) are indicated inTables 1 and 3). The set of nebular lines is the same(Leitherclusters. However, this complex includes starsof difinstanta
there is a notable amount of A-type stars, because
thebroad absorption wings. There are many stellar
absorpfunction
the spectrum indicating the B/A populations, metallic
numerou
C II lines as well as the Mg II and Si II lines. He I linewith theemission in the red part of the spectrum.

only doclusters
from sometallic
their stuThis paper has been typeset from a TEX/LATEX file preparedbyto X-44of AV w
tracks toTheerror cothe clus
are extr
For theobtaine
the theo(for a cM51 (NGC5194/5195)

+02

KOOLS-IFU Observation• 1 ULX + 3 XRBs (2019/04/10-11)• 600 s x ~5 for each
No Detection

Detection

2CXO J133001.0+471343

2CXO J132955.9+471228

6.5e+02

log LX = 39.4
V=18.5 mag
6.9e+02

7.4e+0231

7.8e+02796

8.2e+02862

411

8.6e+02928

log LX = 36.5
V=17.6 mag

9e+02

993

9.4e1059

1125

Detection

632

1191

Detection

2CXO J132952.1+471245

853

1257

1077

1298

15211742

1963

log LX = 36.2
V=17.7 mag
1322

1377734

2186

791

2CXO J132943.3+471134

2407

2628

849

log LX = 37.0
V=18.0 mag
906

964

1021

1079

113

2CXO J132952.1+471245

14800

4850

4900
4950
Wavelength [Å]

5000

5050

[S ii] 6716
[S ii] 6731

2

[N ii] 6583

3
[N ii] 6548

Flux [erg/cm2/s/Å]2[O iii] 5007

[O iii] 4959

3

⇥10 15H↵4H

Flux [erg/cm2/s/Å]4⇥10 15

16550

6600

• Very preliminary…
• [O III] is not detected… Need further checks.

6650
6700
Wavelength [Å]6750

A New X-ray Binary Catalog

Chandra Source Catalog• Chandra X-ray sources + Nearby
galaxy catalog (LVG & IRAS)• 5243 XRBs (281 ULXs)
YI, Yabe,+ in prep.

Requests• 天体の位置を一定に保ってほしい。
• 解析ツールの更新情報は逐次展開してほしい。
• IFU として意味のある観測ができるようにしてほしい。
• 安定運用後は三鷹リモートができるようにしてほしい。

Summary• Theoretically, lower metallicity hosts heavier black holes.
• We would like to observationally investigate this hypothesis w/Seimei/KOOLS-IFU.

• We observed 1 ULX + 3 XRBs w/ KOOLS-IFU.
• 3 XRBs are detected.
• Spectral analysis is on-going.