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STELLAR BLACK HOLES AT THE DAWN OF THE UNIVERSE

STELLAR BLACK HOLES AT THE DAWN OF THE UNIVERSE. Félix Mirabel CEA-Saclay-France & CONICET -Argentina. A subject at the crossroads of massive stellar evolution, High Energy & black hole Astrophysics, & Cosmology. HOW WAS THE IGM RE-IONIZED?.

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STELLAR BLACK HOLES AT THE DAWN OF THE UNIVERSE

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  1. STELLAR BLACK HOLES AT THE DAWN OF THE UNIVERSE Félix Mirabel CEA-Saclay-France & CONICET-Argentina A subject at the crossroads of massive stellar evolution, High Energy & black hole Astrophysics, & Cosmology

  2. HOW WAS THE IGMRE-IONIZED? THE « SWISS CHEESE » MODEL for the re-ionization of the IGM: Gunn-Peterson effect • The IGM was fully ionized by the UV from the first stars (Pop III & II)  HII regions expanding at < 100 Km/s. Dark age • WHAT COULD HAVE BEEN THE ROLE OF mQSOs, HMXBs? • Based on recent results from Stellar evolution and high energy astrophysics: • I propose that in galaxies at z>10 a large fraction of Pop III-II stars end as Stellar BHs in HMXBs X-rays & jets • X-rays & jets overtake the HIIregions produced by UVs, heat and partially ionize the IGM over large volumes of space.

  3. ASTROPHYSICAL GROUNDS FOR THE STELLAR BLACK HOLE HYPOTHESIS THEORETICAL GROUNDS • MOST POP III & II STARS WERE FORMED AS MULTIPLE SYSTEMS Turk+Science 2009; Krumholz+ Science 2009;Clark+ Science 2011; Stacy+…etc. • STARS OF LOW Z WITH M > 20 MEND AS BHsDIRECTLYFryer,1999;Heger+2003;Georgy+2009;Woosley+2008;Nomoto+2010; Linden,Kalogera+2011 • NO ENERGETIC SNe STELLAR BHs REMAIN BOUND TO DONORSMirabel & Rodrigues, Science 2003; Mirabel+ Nature 2008 OBSERVATIONAL GROUNDS • MOST ULXs & LGRBsARE HOSTED IN LOW Z-HIGH-SSFRGALAXIES Feng & Soria,2011;LeFloc’h,Duc,Mirabel;2003;Fruchter+ Nature, 2006; Perley+ 2014 • Lx/SFR EVOLUTION WITH z IS DRIVEN BY Z EVOLUTION IN HMXBsFragos+2012; Basu-Zych+2012 • IN LOW Z GALAXIES Lx/SFR IS LARGER THAN IN MAIN-S GALAXIES Thuan+ 2004; Kaaret+ 2014; Douna, Pellizza, Mirabel, 2014 (in progress)

  4. EVOLUTION OF MASSIVE STARSPOP III & II STARS WERE FORMED IN MULTIPLE SYSTEMS Stacy, Greif & Bromm (ApJ2010) Fragmentation: Clark+ (Science 2011) Turk, Abel & O’Shea (Science 2009) Krumholz et al. (Science 2009) • THEORY • Pop III stars were multiple systems dominated by binaries with 10-100 M • OBSERVATIONS • In the MW >70% of OB type stars are binaries (Chini+2011;Sana+ 2012-14) DID A LARGE FRACTION OF Pop III & II STARS END AS BH-HMXBs ?

  5. STARS OF LOW Z & M>20 MEND AS BHs DIRECTLY with no rotation (Heger+ 2003) with rotation (Georgy+ 2009) Z solar metallicity Mass of progenitor star • Low metal progenitors form BHs by IMPLOSION(e.g. Fryer, 1999, Heger+2003…)

  6. THE FORMATION OF HMXBs IS STRONGLY METALLICITY DEPENDENT (Linden, Kalogera+ 2011) Number of HMXBs per starburst of 106 M • AT LOW Z • the number of HMXBsincreases • the orbital perioddecreases • progenitorsof > 20 M end asBHs What observations could test these theoretical predictions?

  7. If the mass lost in lowmetallicityprogenitorsisrelativellysmall, the collapsingcoresshouldbe more massive, leading to more massive compact remnants THE MASSES OF BHs IN HMXBs ARE LARGER IN HOSTS OF LOW METALLICITY BH masses determined dynamically(Crowtheret al. 2010) BH-HMXBs The stellar BHs in the low metallicity galaxies M33 X-7, NGC300 X-1, IC10 X-1 have MBH>15 Mwhereasin the Galaxy and M31 all known stellar BHs have MBH<14 M

  8. EVIDENCE FOR BH FORMATION WITH NO KICKS APPROACHBASED ON KINEMATICS(Mirabel & Irapuan Rodrigues 2001-2009) STEADY JETS TRANSIENTJETS Credit S&T Mirabel-Rodríguez 1994 Mirabel+ 1992 • With VLBIget sub-miliarcsec precision. • Proper motions withVLBI of compact jets and/or optical images withHST VLA COMPACT JETS Dhawan, Mirabel, Rodríguez (2007) In low hard state compact jets have Sizes ~ 100 AU & Same PA as large scale jets. l3.6 cm l3.6 cm

  9. RESULTS FOR FIVE BH-XRBs Mirabelet al. (Nature 2001) GALACTOCENTRIC ORBIT (230 Myrs) Yellow: Sun White: binary BH XTE J1118+480;GRO J1655-40 WITH BHs OF < 8 M areRUNAWAY BLACK HOLES Mirabel & Rodrigues (Science, 2003) Cygnus X-1: Vp< 9+/-2 km/s < 1 M ejected in a SN also GRS 1915+105 & V404 Cygsuggest that BHs WITH > 10 M FORM IN THE DARK

  10. THE OCCURRENCE RATE OF ULXs PER UNIT GALAXY MASS INCREASES WITH THE SFR AND 1/Ze.g.Zampieri & Roberts (2009) X-ray (Chandra) ULTRALUMINOUS X-RAY SOURCES (ULXs) Fabbiano et al. Antennae

  11. ULXs IN LOW METALLICITY REGIONS OF GALAXIES The integrated ULXs luminosity of ~1042erg s-1 rivals that of AGN (Gao+ 2003)

  12. BH-HMXBs ARE MOSTLY FOUND IN STAR-FORMING GALAXIES OF LOW METALLICITY& ARE POWERFUL ENERGY SOURCES Dwarf galaxies of small Z are the best local templates of primeval galaxies Review by Feng & Soria, 2011 Shape of X-ray spectra are critical shock & photo-ionized bubbles of >100 pc in size Ha images Massive outflows BH-HMXB E > 1053 erg

  13. THE HOSTS OF LGRBs WITH OPTICAL AFTERGLOWS ARE SMALL IRREGULAR GALAXIES OF LOW Z Le Floc´h,Duc,Mirabelwith VLT (2003); Fruchter+ with HST (Nature 2006); Vergani+ (2014) Graham& Fruchter, (2012) Levesque et al. (2010) From 53000 SDD galaxies From 940 line emission galaxies However, dark LGRBs may pose some caveats & controversy

  14. FROM STUDIES OF HMXBs IN LOCAL UNIVERSE IT IS INFERRED THE COSMIC EVOLUTION OF METALLICITYA COSMIC EVOLUTION OF BH-HMXBs • . At low metallicities (Z<Z-5) thereshould be an increase of: • The mass of stellar BHs because the progenitor cores are more massive • The number of BH-HMXBs since massive stars form BHs by direct collapse • The X-ray luminosity of BH-HMXBs…an issue being investigated… • Mirabel. Invited Review. Proceedingsof IAUSymp. 275 (2011) (arXiV:1012.4944v1 [astro-ph.CO] 22 Dec 2010)

  15. Ionizing power of mQSOs versus ionizing power of massive stars Mirabel, Dijkstra, Laurent, Loeb, Pritchard (A&A 2011) N&V in Nature (2011) Counting photons fedd = fraction of Eddington luminosity for a time tacc Nphot = number of ionizing photons emitted per atom of H nucleus <E>g= mean photon energy emitted by the accreting BH fesc,* (fesq,BH) = fraction of ionizing photons that escape For fiducially values of the model parameters: AN ACCRETING STELLAR BLACK HOLE EMITS A NUMBER OF X-RAY PHOTONS COMPARABLE TO THE UV PHOTONS FROM ITS PROGENITOR STAR • But in a fully neutral medium Nsec* = 25 (Eg/1 keV), where Eg is the photon energy • However, not all stars will be massive and lead to the formation of BH-HMXBs…

  16. HMXBs & HI TOMOGRAPHY DURING THE EoR fxat z > 6 must increaseas Z < 10-5 Z Gas Temperature Mirabel+ (2011) l21cm line Mirabel+ (2011) BH-HMXBs HEATED THE IGM TO ~104 K OVER LARGE VOLUMES At z=8.9 the IGM was already heated and ionized (Paciga+ 2014) CONCLUSION X-RAYS HAVE LONGER MEAN FREE PATH THAN UVs.THEY HEAT THE GAS FAR FROM THE GALAXIES AND PARTIALLY IONIZE THE BULK OF THE IGM. l21cm line X-ray hard spectrum Fialkov+Nature, 2014

  17. BH-HMXBs LIMITED THE MASS OF DWARF GALAXIES • Mmin~ 109 (r/100rc)-1/2 (m/0.6)-3/2 [T(K)/104]3/2 [(1+z)/10]-3/2 M • rc = critical mass density for a flat universe, r = mass density in the galaxy m= mean molecular weight, z = redshift, T = temperature of the IGM • THE THERMAL HISTORY OF THE IGM DETERMINED BY STELLAR BLACK HOLES LIMITED THE MASS & NUMBER OF DWARF GALAXIES PREDICED BY THE lCDM

  18. OPEN QUESTIONS • I) Will l21cm tomography of HI with LOFAR, SKAshow a smoother end to the dark ages? • II) Could the X-rays from BH-HMXBs contribute to the 10-20% unresolved hard X-ray background? • III) Do mQSO jets penetrate deeper in the IGM? (in progress) • IV) Will BH-BHstellar binariesmay be frequently detected as sources of gravitational waves? (Belczynski+2011;Ziosi+2014) • V) Does feedback from stellar BHs reduce the lCDMpredicted number of dwarf galaxies? • VI) Are there naked dark matter haloes with M < 109M? • VII) Are HMXBsat z>6 be the source of the intriguing radio background discovered with ARCADE 2? (Fixsen+2011; Seiffer+ 2011; Condon+ 2013)

  19. OBSERVATIONS RELATED TO HIGH z HMXBs? • COSMIC RADIO BACKGROUND WITH ARCADE 2 • He II IONIZATION AT z > 3.5 (Worseck+; Compostella+ 2014) Absorption spectroscopy of the He II La line lrest=303.78°A Aradiation field with photons hn> 54.4 eV that can not be provided by luminous QSQs Excess emission ARCADE2 (Fixsen+; Seiffer+ 2011) discrete sources VLAfollow up by Condon+ (2012): The ARCADE 2 excess is smooth  A new unexpected discrete-source population too numerous to be associated with bright galaxies 2.725 K blackbody ARE THE RADIO BACKGROUND & PHOTONS WITH hn>54.4 eV FROM A POPULATION OF HMXBs AT z>6 OR FROM SUPERMASSIVE BHs? (Biermann+2014)

  20. CONCLUSION I) l21cm tomography of HI with LOFAR, SKA, etc., may reveal a smoother end to the dark ages X-rays=0 large fluctuations. X-rays=50%  lower fluctuations but at shorter ls (Visbal & Loeb, 2011; Fialkov+ Nature 2014) X-ray spectra of galaxies UVs vs UVs+X-rays. HMXBs with hard spectra Slice of 170×170×0.66 Mpc3 Fialkov+ Nature 2014 Hard X-ray spectra Pacucci et al., 20014) Softer X-ray spectra HMXBs + soft X-rays  Larger fluctuations Slice 1.5 Mpcat zpeak = 16 hard (right) and soft (left ) X-ray SED

  21. Prestwich+2013 using Nustar Basu-Zych Figure 2. NULX(SFR) for individual SINGS galaxies, intermediate metallicity galaxies and the combined metal poor and XMPG. This plot uses the PT05 metallicity calibration. . (Prestwich+2013) NULX(SFR) for individual SINGS galaxies, NGC 922 and the Cartwheel. This plot uses the KK04metallicity calibration. (Prestwich+2013)

  22. NO ENERGETIC NATAL SNestBHs REMAIN BOUND STELLAR BHsARE OBSERVED IN BINARIES Credit: S&T CORE COLLAPSE MODELS: Massive stellar black holes (M>10 M) should form with no energetic kicks (Fryer & Kalogera; Woosley & Heger; Nomoto et al.) THIS HYPOTHESIS IS BEEN TESTED USING THE KINEMATICS OF mQSOs Mirabel et al. in Nature, Science & A&A (2001-2012 ) e.g. Mirabel & Rodrigues (Science, 2003) Cygnus X-1 was form in the Dark With no energetic kick Now confirmed by Gou, McClintock+ (2011) & Reid+ (2012)

  23. PROPER MOTIONS USING COMPACT JETS Mirabel & Rodríguez 1994 Mirabel, Rodriguez+ 1992 TRANSIENT JETS STEADY JETS VLA Dhawan, Mirabel, Rodríguez (2007) COMPACT JETS In low hard state. Size ~ 100 AU. Same PA USED TO DETERMINE PROPER MOTIONS (with VLBI to get sub-miliarc sec precision) l3.6 cm l3.6 cm

  24. Boera+ 2014 Panucci Panucci

  25. OPEN QUESTIONS • LIFE TIME OF BLACK HOLE HMXBs • INCORPORATION OF NEUTRON STAR HMXBs • ACCRETION RATE-FEEDBACK AS A FUNCTION OF METALLICITY • PHYSICAL MECHANISMS OF COOLING, IONIZATION & HEATING • X-RAYS FROM SNeBY COMPARISON WITH X-RAYS FROM HMXBs • INCLUSION OF RELATIVISTIC JETS OF PARTICLES • BINARY stBHs THE FIRST SOURCES OF GRAVIATIONAL WAVES TO DETECT? • WILL THE l21cm SIGNALS FROM HI AT HIGH z (LOWFAR, SKA, EDGES), AS PREDICTED INCLUDING HMXBs, HAVE LOWER AMPLITUDES, BE MORE UNIFORM RATHER THAN HII REGION DOMINATED WITH PATCHY “SWISS CHESS TOPOLOGY , AND THE REIONIZATION HAVE TAKEN LONGER TIME, SHIFTING THE SIGNALS TO HIGHER FREQUENCIES? l21cm tomography (Visbal & Loeb, 2011) X-rays=50%  lower fluctuations due to more uniform heating Signals up to lower z’s X-rays = 0  large fluctuations

  26. Gunn-Peterson effect • EVIDENCE FOR THE DARK AGES • No light (continuum radiation) is observed at wavelengths less than La because it is fully absorbed by atomic hydrogen. • The Gunn–Peterson trough is a feature of the spectra of quasars due to the presence of neutral • hydrogen in the IGM. The trough is characterized by suppression of • electromagnetic emission from the quasar at wavelengths less than that of the Laline at the redshift of the emitted light. This effect was originally predicted in 1965 by James E. Gunn and Bruce Peterson

  27. STELLAR EVOLUTION & HIGH ENERGY ASTROPHYSICS: STELLAR BHsARE OBSERVED IN BINARIES CORE COLLAPSE MODELS: Massive stellar black holes (M>10 M) should form with no energetic kicks (Fryer & Kalogera; Woosley & Heger; Nomoto et al.) THIS HYPOTESIS IS BEEN TESTED USING THE KINEMATICS OF mQSOs Mirabel et al. in Nature, Science & A&A (2001-2012 ) e.g. Mirabel & Rodrigues (Science, 2003) Cygnus X-1 was form in the Dark With no energetic kick Now confirmed by Gou, McClintock+ (2011) & Reid+ (2012)

  28. DO StBHs RECEIVE NATAL SN KICKS? FORM WITH OR WITHOUT ENERGETIC NATAL SNe? • CORE COLLAPSE MODELS: • Massive stellar black holes (M>10 M) should form with no energetic kicks (Fryer & Kalogera; Woosley & Heger; Nomoto et al.) • IS THERE ANY EVIDENCE OF StBH FORMATION BY DIRECT COLLAPSE? • IS THERE A RELATION BETWEEN KICK VELOCITIES AND BH MASS? THE CORE COLLAPSE MODELS CAN BE TESTED USING THE KINEMATICS OF BHmQSOs Mirabel et al. (2001-2009 )

  29. RESULTS FOR FIVE BH-XRBs Mirabel & Rodrigues (Science, 2003) Cygnus X-1 Vp< 9+/-2 km/s < 1 M ejected in a SN together with GRS 1915+105 & V404 Cygsuggest that BHs WITH >10 M MAY FORM IN THE DARK Mirabelet al.(Nature 2001) XTE J1118+480;GRO J1655-40 BHs OF < 8M RUNAWAY BLACK HOLES GALACTOCENTRIC ORBIT (230 Myrs) Yellow: Sun White: binary BH BLACK HOLES WITH > 10 M FORM BY IMPLOSION STELLAR BLACK HOLES REMAIN BOUND TO DONORS

  30. BHs OF >10 MFORM BY DIRECT COLLAPSE APPROACH BASED ON THE KINEMATICS (Mirabel & Irapuan Rodrigues 2001-2009) THE BH IN Cyg X-1 WAS FORMED IN THE DARKMirabel & Rodrigues (Science, 2003) Gou, McClintock et al. (2012) confirmed this result Cyg X-1 remained in its birth place Vp< 9 +/- 2 km/s < 1 Min SN Other BHs with >10 Mform by direct collapse: GRS 1915:W=7+/-3 km/s (Dhawan,Mirabel,Rodríguez,01) V404 Cyg:W=0.2+/-3 km/s (Miller-Jones et al. 2009) The BHs remain bound to donors Sky & Telescope

  31. DO LOCAL TEMPLATES OF HIGH z GALAXIES HAVE ENHANCED Lx/SFR? Douna, Pellizza, Mirabel (2014, in progress) • Lx/SFR EVOLUTION WITH z IS DRIVEN BY Z EVOLUTION IN HMXBsBased on large surveys: Fragos+2012; Basu-Zych+2012 • IN LOW Z GALAXIES Lx/SFR IS LARGER THAN IN MAIN-S GALAXIES • Thuan+ 2004; Kaaret+ 2014; Douna, Pellizza, Mirabel(2014, in progress)

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