Optical counterparts of ULXs. S. Fabrika

Transcription

1 Optical counterparts of ULXs S. Fabrika

2 Examples of ULX counterparts NGC4559 X-7 Soria et al NGC5408 X-1 Grise et al Holmberg IX X-1 Pakull & Grise, 2008 Grise et al Cseh et al. 2012

3 Optical spectra of counterparts NGC5408 X-1 Cseh et al NGC1313 X-2 Roberts et al Highly variable HeII line Holmberg IX X-1 Grise et al. 2011

4 P13 in NGC7793 Motch et al B9Ia donor star Black hole mass is restricted to M BH < 15 M sun Broad emissions are from supercritical disk Highly variable in X-rays, long-scale (years)

5 M101 ULS1 Liu et al WN8 donor at 8.2-day orbit Highly variable in X-rays, short-scale (hours)

6 M81 ULS1 Liu et al.2015 Barionic jets like that in SS433

7 HLX in NGC470 Gutierrez & Moon 2014 Lx > erg/s, L x /L opt ~ 300 HeII line FWHM ~ 400 km/s probable blue cluster, M g ~ -12 HLX-1 Soria et al Hα line FWHM ~ 450 km/s

8 Holmberg II X-1 Holmberg IX X-1 NGC4559 X-7 NGC5204 X-1 Fabrika et al. 2015

9 IR spectra of ULX counterparts Heida et al, 2014, 2015, 2016 (VLT/X-shooter, Magellan/MMIRS, Keck/MOSFIRE) 11 out of 62 counterparts with luminosities of red supergiants ULXs in Holmberg II, NGC925, NGC4136, NGC253 all have absorption spectra with nebular emission lines In visible Holmberg II, NGC925, NGC253 have blue spectra, probably because of accretion disk

10 Optical spectra of counterparts SS433 NGC5408 X-1 NGC5408, NGC1313 NGC4395 X-1 NGC1313 X-2 NGC5204 X-1 NGC4559 X-7 Holmberg IX X-1 NGC4395 X-1 Holmberg II X-1 SS433, NGC5294, NGC4559, Holm IX, Holm II

11 Subaru All studied ULX have broad HeII 4686 A and Hα. That is high ionization wind: EW(HeII)/EW(Hβ) 2

12 Classification diagram for WNL stars (Crowther & Smith, 1997) three LBVs - AG Car, V532, HD5980 with known transitions (Sholukhova et al., 2011) WN11 WN9-10 WN9 Crowther, Walborn, 2011: ζ Pup O2If*, O3If* O2If*/WN5, O2.5If*/WN6, O3If*/WN7 WN6ha, WN7ha

13 All the nearby persistent ULXs (L x > erg/s) ever spectroscopically observed, have the same optical spectra. (Fabrika et al. 2015) The spectra are similar to: - SS Galactic super-accretor with stellar-mass black hole - or LBVs (luminous blue variables) in their hot states - or WNLs (late nitrogen Wolf-Rayet stars) They must constitute a homogeneous class of objects (less that 10% may have another), which most likely have super-eddington disks

14 NGC4395 spectra Vinokurov et al Variable HeII line 63-day period (Swift data) Similar to SS433 Cherepashchuk et al. 2005

15 Super-Eddington or irradiated disk? Black with errors from top to bottom: NGC5204 X-1, Holmberg II X-1, NGC5408 X-1, NGC4559 X-7, Holmberg IX X-1 (Fabrika et al archive data) LBV Romano star (V532) in M33 WR22 (WN7ha), WR24 (WN6ha), WR25 (WN6ha) GX339-4 (Soria et al. 1999; Rahoui et al. 2014) V404 Cyg (Casares et al. 1991; Cottehelf et al.1992) GRO J (Hunstead et al. 1997; Soria et al. 1998) Dense and optically thick winds in LBVs, WNLs, supergiants, SS433, ULXs versus Winds from disks irradiated surface

16 Optical luminosities of studied ULX and SS433 In decreasing luminosity: SS433, NGC6946 ULX-1, NGC7793 P13, NGC4559 X-7, NGC5408 X-1, NGC5204 X-1, NGC4395 X-1, M81 ULS1, Holmberg II X-1, IC342 X-1, Holmberg IX X-1, NGC4559 X-10, NGC1313 X-2, NGC5474 X-1, NGC1313 X-1, M66 X-1, M81 X-6 In super-eddington disks X-ray luminosity logarithmically depends on the accretion rate L L 1 aln( M / M )) LEdd Tao et al., 2012; Vinokurov et al., Eddington luminosity, - Eddington rate UV/optical luminosity strongly 9/ 4 1/ 2 depends on the accretion rate M M, Edd ( Edd L 3/ 4 1/ 2 V M M T ph Formally, the accretion rate in ULXs times less than in SS433, the wind temperature times higher than in SS 433. M Edd X

17 what about this histogram? 1. Selection effect, objects may be missed in galaxies farther than 10 Mpc 2. With decreasing an accretion rate the optical luminosity does decrease. The donor star becomes dominating. Three of six objects with M V > -5.3 have F-G type spectra. (Avdan et al. 2016, Vinokurov et al. 2016) All studied ULXs L X / L opt > 200 (Avdan et al., 2016)

18 HolmbergIX X-1 NGC5408 X-1 HST data corrected for reddening, for 5 Mpc distance NGC1313 X-1 NGC5408 X-1 (x4), α = 3.35 Holmberg IX X-1 (x2), α = 3.58 NGC1313 X-1 (x1), α = 2.81 F λ λ -α For Raileigh-Jeans BB tail α = 4 NGC4559 X-10 NGC5474 X-1 M66 X-1 F-G-type spectra: NGC4559 X-1 (x4) NGC5474 X-1 (x2) M66 X-1 (x1) all have M V > -5.3

19 MF16 nebula around NGC6946 ULX-1 Abolmasov et al BB Candra HeII HeI HI opt MCD F140LB F555W Kaaret et al. 2010: the nebula 3 times brighter in FUV that the source F450W F814W

20 MF16 nebula around NGC6946 ULX-1 Cloudy model by A. Vinokurov red Cloudy model green SCAD model after passing through the nebula blue red + green circles HST date (nebula only) triangles Cloudy model in the filters - Kaaret et al. L140LB point The MF16 nebula cannot be ionized by X-rays, but FUV radiation

21 NGC7331 X-1 cluster and nebula Abolmasov et al Cluster: 1.1 x 10 5 M sun, 4.2 Myr Cloudy model: the cluster + additional shock exitation like that in MF16 NGC4669 ULX-1 The additional source ~5 times more powerful than the cluster s SNe or stellar winds

22 Nebula surrounding Holmberg II X-1 is dynamically disturbed, ~100 km/s at a scale of ~100 pc Lehmann et al IC342 X-1 nebula (Pakull, Mirioni 2002; Abolmasov et al. 2007; Moon et al. 2001; Cseh et al. 2012) The well-studied nebulae have kinetic luminosity ~ erg/s

23 VLT/HST observations of ULX in merging starburst galaxies Antennae and NGC3256 Poutanen et al. 2013

24 Association of the ULXs with extremely young (< 5 Myr) clusters is not occasional, < The coordinate displacements, < pc, is a common property of the HMXBs and ULXs. They need ejection velocity ~80 km/s (if only transportation). Fainter X-ray sources (LMXB) loose a relation with parent clusters: Kaaret et al. (2004), Rangelov et al. (2011). Cluster age = Primary evolution + Secondary evolution (+ Transportation time) The ULX progenitors in Antennae are very massive binary stars, М 1 ~ М 2 ~ 100 Mo or М 1 ~ 2М 2 ~ 100 Mo Ejection of the binaries from clusters at their beginning stages of formation (Moeckel, Bate, 2010; Pflamm-Altenburg, Kroupa, 2010; +++) due to few-body encounters.

25 Thank you