High mass X-ray binaries and recent star formation in the host

galaxy

P.Shtykovskiy, M.Gilfanov

IKI, Moscow; MPA, Garching

High mass X-ray binaries andrecent star formation

HMXB XLF HMXB XLF

Observations:

Grimm, Gilfanov & Sunyaev, 2003Scaled to one SFR

M1 ,t1 , NHMXB1

M2 ,t2,NHMXB2

M3 ,t3,NHMXB3

NHMXB=Σ NHMXBi =Σ Mi η(ti)

M - Masst - Age

NHMXB – number of HMXBs

of the stellarpopulation

SNII rate

FirstB.H.

Last N.S.

Evolution of HMXBs population

Evolution of HMXBs population: observational constraints

Observed HMXBs:

Small Magellanic Cloud in the IR(100µm) + HMXBs (XMM, Shtykovskiy & Gilfanov 2005)

inverse problem for

X

Star formation history in the Small Magellanic Cloud

CMD of the SMC (MCPS catalogue, Zaritsky et al., 2002)+ Padua isochrones (Girardi et al., 2002)

MS Supergiants10 Myr

40 Myr

• Metallicity

• Extinction, distance

• IMF, binary fraction, binary mass ratio

• An adequacy of stellar evolution models

• Completeness

• Photometric errors

• Foreground stars

Model stellarpopulation

MS +Sg

Supergiants

Model stellar populations:

Star formation history in the SMCSMC in the IR(100µm) + HMXB (XMM)

Evolution of HMXBs population: observational constraints

• Maximum abundance of HMXBs 20-50 Myr after the SF event

• Paucity of young HMXBs

NHMXB(t)

Black holeXRB

Evolution of HMXBs population: observational constraints

• Maximum abundance of HMXBs 20-50 Myr after the SF event

• Paucity of young HMXBs

Popov et al. (1998) (Z=0.02, log(Lmin)=33)

• Maximum abundance of HMXBs 20-50 Myr after the SF event

• Paucity of young HMXBs

Evolution of HMXBs population: observational constraints

Evolution of HMXBs population: observational constraints

SMC:Log(Lmin)=34

Distant galaxies:Log(Lmin)=38-39

Bright HMXBs(expected)

Bright HMXBs: youngWeak HMXBs: older on average

Spiral structure and HMXBs

Density waveМ 51 HST image

Stars and gas

Bright HII regions -Current star formation HMXB-Star formation 10-50 Myr ago

HMXBs in M51

M51 in Hα + Chandra HMXB (Terashima et al., 2004)

Distance to the closest spiral arm

Bright HII regions

HMXB

HMXBs in the Galaxy

HMXB peaks shifted

Lutovinov et al. (2005) -Shift in the HMXB density has been observed with INTEGRAL

40 Myr

Young objects

Conclusions

• Simple linear relation N(HMXB)=A*SFR may break down in some cases.

• Maximum number of HMXBs is reached after 20-50 Myr after the star formation burst.

• Spiral structure in the HMXBs distribution may be shifted relative to the spiral structure in the distribution of young objects.

HMXBs in Magellanic Clouds

XLF of HMXBs in the Small Magellanic Cloud

XMM-Newton

ASCA

HMXBs in Magellanic Clouds

Standart SFR indicators: • FIR• Hα

• UV

X-ray luminosity -Independent SFR indicator

X-ray binaries

● HMXBMopt >5-10 M☼ t~5-100 Myr

N ~ SFR

● LMXBMopt~ M☼ t~ few Gyr

N ~Stellar mass

HMXB in the LMC

Supergiant shell LMC4:Numerous HMXBs, Weak SF, t~10-30 Myr

30 Dor: No HMXBs,Intensive SF, t<10 Myr

LMC4

30 Dor

LMC in Нα

HMXB (Liu, 2005)

Magellanic Clouds

● High SFR/M* N

HMXB>N

LMXB

● D=50-60 kpc Sensitivity(XMM) L

Xmin~1033erg/s

● Low metallicity

30 pointingsXMM-Newton

SMC (IRAS, 100 µm)

LMC (IRAS, 100 µm)

Outline:

• HMXBs and recent star formation history in Magellanic Clouds

• HMXBs and the spiral structure of the host galaxy

High mass X-ray binaries and the spiral structure

of the host galaxy

Spiral structure

Bright HII regions - Current SF

HMXB-Star formation 10-50 Myr ago

Agegradient

d = Расстояние до ближайшей ветви

d

corotation

Young objects

40 Myr

40 Myr

0 Myr

Black hole systems – on spiral armsNeutron star low luminosity systems - shifted

HMXBs in Galaxy

Peaks in density are shifted

Lutovinov et al. (2005) - peaks in HMXB density observed by INTEGRAL are shifted

40 Myr objects

Young objects

HMXBs in the M51

M51 in Hα + Chandra HMXB (Terashima et al.., 2004)

Nature of X-ray souces:

• HMXB ~ SFR

• LMXB ~ Stellar mass

• AGN Uniform distribution

HMXBs in the M51

Evolution of HMXBs populationHMXBs shift - AGE

Galactic dynamicsCorotation radius etc.

Спиральная структура в распределении HMXB

Ω(волна плотности)< Ω(звезд)

М 51 HST image

Вращение звезд

Внутри радиуса коротации:

Яркие области HII -текущее звездообразование

HMXB-звездообразование 10-50 млн.лет назад

возраст

0 млн. лет

40 млн. лет

Волна плотности

HMXBs as a star formation indicator

X-ray luminosity functions

SFR~0.15-7 M☼/yr

Grimm, Gilfanov & Sunyaev, 2003

HMXBs as a star formation indicator

X-ray luminosity functions,

scaled to one SFR

Grimm, Gilfanov & Sunyaev, 2003

HMXBs – SFR indicator