Current Paradigm of Direct Collapse BH formation
|
|
- James Garrison
- 5 years ago
- Views:
Transcription
1 Guillermo Haro Workshop, 2015 Current Paradigm of Direct Collapse BH formation Bhaskar Agarwal Yale University (prev: PhD at Max Planck for Extraterrestrial Physics)
2 What is the Problem? SDSS Quasars at z > 6 highest redshift: z = (770 Myr) (Momjian et al. 2013) most massive: z = 6.30 (900 Myr), M = 1.3x10 12 (Wu et al. 2015) First Stars form at z = 20 Latest Planck results push the z lower! How do we grow the Quasars to supermassive scales? time scale is t(z 6 ) - t(z first_star ) ~ 700 Myr* *Take this time with a pinch of salt
3 Solving the problem z t 200 Myr 550 Myr 1 Gyr seed' a BH grow the seed make it a SMBH - For a given BH growth scenario: Bondi-Hoyle, Eddington etc. - sensitive to two parameters M seed t grow
4 The Possible Paths pristine gas in minihalo withstand SF Pop III/II cluster Pop III star: BH: 100 M-sun halo grows: T vir = 10 4 K critical LW radiation NO fragmentation: SMS/QS Merge before 100 M sun go SN BH: 1000 M sun super-edd. BH growth BH: M sun sub-edd. BH growth Quasar BH: 10 9 M sun
5 PopIII stellar BH seeds Heger et al. 2003
6 PopIII stellar BH seeds Volonteri et al. Bromm et al. Yoshida et al. Assuming z f edd = 1 rad. eff = 0.1 M seed = 100 M sun M BH [M sun ] t grow : t 1 {z(20-6)} = 700 Myr t 2 {z(9-6)} = 200 Myr z t age [Myr] 6 t 200 Myr 1 Gyr seed' a BH make it a SMBH
7 Hirano et al PopIII stellar BH seeds: IMF PopIII : IMF Highest mass: 1000 M sun Mstar > 100 M sun desirable seed mass! Doesn t have to be too' common
8 PopIII stellar BH seeds: where? DM Mass ? BH + II* SMBH + II* BH + II* III* PopIII : first sources of light! Minihaloes: M = M sun (DM) Effect on neighbouring haloes: -Moderate LW feedback can kill SF -X-rays feedback -SN 'blow out'
9 PopIII stellar BH seeds: problems highly optimistic scenario! ignores feedback Assuming f edd = 1 rad. eff = 0.1 where is the gas? constant availability of gas form in mini-haloes! merger scenario unclear merger b/w 2 mini-haloes - time-scale - BH present in both M seed = 100 M sun t grow : t 1 {z(20-6)} = 700 Myr t 2 {z(9-6)} = 200 Myr need to be super-edd! all the time!
10 Direct Collapse BH seeds Eisenstein & Loeb Oh & Haiman Bromm & Loeb Koushiappas et al. Bullock & Dekel Lodato & Natarajan z Assuming f edd < 1 rad. eff = 0.1 M seed = M sun M BH [M sun ] t grow : t 1 {z(20-6)} = 700 Myr t 2 {z(9-6)} = 200 Myr t age [Myr] z t 200 Myr 550 Myr 1 Gyr seed' a BH make it a SMBH
11 DCBH seeds: how LW photons: ev Enough LW Radiation H2 + {LW} H2 Delay Pop III Star formation H2 H + H Tvir < 10,000 K
12 DCBH seeds: how LW photons: ev Critical (high) LW Radiation H H H2 Stop Pop III Star formation H + H H Tvir > 10,000 K Pop III n = 10 5 cm 3 T = 200 K 8000 DCBH n = 10 5 cm 3 T = 8000 K M BE ~ 100 M sun M BE ~ 10 5 M sun
13 DCBH seeds: problems Assuming f edd < 1 rad. eff = 0.1 M seed = M sun What is the critical LW flux? HOW does the gas collapse proceed? Feedback from the DCBH once it forms t grow : t 1 {z(20-6)} = 700 Myr t 2 {z(9-6)} = 200 Myr Subsequent merger: with the LW producing galaxy z t 200 Myr 550 Myr 1 Gyr seed' a BH make it a SMBH
14 Do you like movies? Films, cinema. NOT simulation movies My guilty pleasure: BOLLYWOOD! 1. Introduce the audience to your plot 2. Everything is OK, songs/dance 3. Something bad happens! 4. Oh No! 5. There is hope
15 DCBH seeds: where Close to a LW source: Pop II galaxy M = 10 7 M sun (DM) DCBH Continued exposure to LW radiation LW LWcrit Mhot Mhot tdyn tdyn Mcold Mcold tdyn tdyn Metal Free Pop III Polluted Pop II Mhot Outflows Mhot Outflows
16 DCBH seeds: The Hunt SAM Agarwal et al FiBY Dalla Vecchia et al. Agarwal et al Cosmological Volume Yes Yes Minihaloes resolved Yes Yes Halo histories Yes Yes Outflows Yes Yes Pop III + Pop II Yes Yes LW radiation: Spatial + Global Yes Yes Gas No Yes IGM Metal Dispersion No Yes
17 DCBH seeds: The Hunt (SAM) SAM Halo history: Merger Trees Subfind output: LCDM simulation Min halo mass required : at least 10 6 M solar Box Size Cosmology N particles Min. Halo Mass z final 4.86 Mpc WMAP M solar 6
18 DCBH seeds: The Hunt (SAM) DCBH LW LWcrit Mhot Mhot tdyn tdyn Mcold Mcold tdyn tdyn Mhot Mhot Outflows Outflows
19 DCBH seeds: The Hunt (SAM) Reionisation feedback: 13.6 ev : photoionisation / heating of gas in haloes gas needs a larger potential well to re-collapse Vc = 20 km/s (Dijkstra 08) LW Escape Fractions: more photons = more feedback (Ahn et al. 09, Kitayama 04) Stars: Pop II stars (Starburst 99) sfe: 1 % Pop III stars (Schaerer et al.) Range of SAM models Each explores a different parameter set Most vs. Least optimistic scenarios
20 DCBH seeds: The Hunt (SAM) Agarwal et al. 2012
21 DCBH seeds: The Hunt (SAM) PopII J max PopII J bg PopII J crit PopIII J max PopIII J bg PopIII J crit J bg 10 2 J LW z Agarwal et al. 2012
22 DCBH seeds: The Hunt (SAM) 2.0 esc log(dn/dz) [Mpc 3 ] esc esc esc0.5hsfe esc0.5reion z DC sites: Few (<10) at z>6 in a ~100 cmpc 3 box Quasars: few / Gpc 3 at z>6 Discrepancy: 10 7 objects too many! (?) Agarwal et al. 2012
23 DCBH seeds: The Hunt (SAM) z= , , Steeper Two point correlation ξ Halo(DC) / ξ Halo(NoDC) , , z= z= DC sites prefer a more clustered neighbourhood Need to be close to a larger galaxy giving out critical LW flux , , log(d phy ) [pc] Agarwal et al. 2012
24 DCBH seeds: The Hunt (FiBY)
25 DCBH seeds: The Hunt (FiBY) Y [phy. kpc] Y [phy. kpc] X [phy. kpc] Z [phy. kpc] Z [phy. kpc] Y [phy. kpc] X [phy. kpc] Y [phy. kpc] Z [phy. kpc] Log J LW,II Log Z sun Agarwal et al. 2014a X [phy. kpc] Y [phy. kpc] X [phy. kpc] -8.00
26 DCBH seeds: The Hunt (FiBY) J LW DC3 ON08 J LW,II J LW,III J LW,Total 10-1 DC 10 (sites) seems to be more probable than previously thought redshift T vir =10000 K redshift first prog. next prog. DC0 at z= (Agarwal et al. 12 vs. Dijkstra et al. 08) Discrepancy broken if a higher J crit used 7.50 Log(M DM ) [M sun ] (Dijkstra et al 2015) Agarwal et al. 2014a M DM [M sun ] 10 6 T vir =2000 K redshift
27 DCBH seeds: The Evolution DCBH Merger In Situ Pop III Star Pop II Cluster Empty halo Growth of BH ± Stars
28 DCBH seeds: The Evolution Metal Free Pop III Polluted Pop II DCBH Outflows Mhot LW Mhot Mhot LWcrit tdyn Mcold DCBH tdyn tdyn Mcold tdyn Mcold tdyn OBG Phase Mhot flim Mhot Outflows Mcold + Mhot Outflows
29 DCBH seeds: The Evolution O1, z g =6.18 O2, z g =8.93 O3, z g =7.34 O4, z g =6.55 M BH [M O ] f lim = 1.5 f lim = 0.75 f lim = 0.1 f edd = M * [M O ] Agarwal et al. 2013
30 DCBH seeds: Observations Rest wavelength [Å] O1 O2 O3 O4 f lim = 1.5 f lim = 0.75 f lim = m AB Observed wavelength [Å] Agarwal et al. 2014
31 DCBH seeds: Revised Theory? L hv - Rates depend on the shape of incident spectrum of external galaxy - In literature the J crit values have been derived by assuming Pop III source: black body at 10 5 K 1000 Pop II source : black body at 10 4 K (Omukai et al. 01, Shang et al. 10, Wolcott-Green et al. 12, Sugimura et al. 14, Dijkstra et al. 14, Agarwal et al. '15)
32 DCBH seeds: Revised Theory? Rates depend on the shape of the incident spectrum from the external galaxy: relative ratios of 1eV to 12.4 ev photons Agarwal et al. 2014b
33 DCBH seeds: THE J crit Agarwal et al Parameter space reaction rates: kh -, kh2 DC Input the rates directly into the Enzo framework with S.Glover 15 chem. PopIII Find the rate parameter space where you find DC Compare it to rate parameter space from realistic SEDs: Starburst 99
34 DCBH seeds: THE J crit from Starburst99 Agarwal et al ST99: galaxy is placed 5 kpc from the atomic cooling halo de: photo-detachment of H - di: photo-dissociation of H 2
35 DCBH seeds: THE J crit ST99: ISF, Z = IMF: Salpeter [1-100] No unique" value of J crit : depends on the age, SFH of the galaxy Agarwal et al. 2015
36 DCBH seed: Found? Observed by: Sobral et al Claimed as DCBH: Pallotini et al. 2015
37 DCBH seed: found? asterisks: B+C diamonds: A A: BH B+C: stellar Agarwal et al. 2015b in prep
38 DCBH seeds: Recently Latif et al. NO fragmentation Aykutalp et al. X-ray feedback Glover et al. relevant chemistry Scahuer et al. fesc of LW Sugimura et al. Jcrit
39 DCBH: Take Away Message DCBH works maybe too well still << frequent as Pop III seeds Local LW flux essential for z>6 galaxy formation models DCBH form in satellites of LW producing galaxies DCBH prefer clustered environments DCBH can merge with the galaxies later on: OBG Need to account for realistic SEDs : BB not enough QUESTIONS QUESTI All DCBH are not 'future' SMBH
40 Stellar cluster BH seeds Zwart et al. Volonteri et al. Katz et al. Cluster M = M sun Merge within few Myr M BH = M sun Assuming f edd < 1 rad. eff = z M seed = 1000 M sun t grow : t 1 {z(20-6)} = 700 Myr t 2 {z(9-6)} = 200 Myr M BH [M sun ] t age [Myr] z t 200 Myr 550 Myr 1 Gyr seed' a BH make it a SMBH
41 Stellar cluster BH seeds: where? DM Mass ? MBH + II* SMBH + II* MBH + II* II*/III* cluster A proto-galaxy type stellar cluster Metals M = M sun (DM) III* Pre-enrichment : VERY early on
42 Stellar cluster BH seeds: problems Cluster M = M sun Merge within few Myr M BH = M sun Assuming f edd < 1 rad. eff = 0.1 M seed = 1000 M sun t grow : t 1 {z(20-6)} = 700 Myr t 2 {z(9-6)} = 200 Myr formation epoch: Pop II cluster- VERY early on N-body problem mergers: all stars must merge timescale < 3 Myr z t 200 Myr 550 Myr 1 Gyr seed' a BH make it a SMBH
DIRECT COLLAPSE BLACK HOLES AS SEEDS OF QUASARS AT REDSHIFT > 6. Bhaskar Agarwal TMoX Group Max Planck for Extraterrestrial Physics!!
DIRECT COLLAPSE BLACK HOLES AS SEEDS OF QUASARS AT REDSHIFT > 6 Bhaskar Agarwal TMoX Group Max Planck for Extraterrestrial Physics!! OPINAS Seminar, 30 April 2014 PROBLEM Explain supermassive black holes
More informationThe Impact of Radiation on the Formation and Growth of Seed Black Holes
The Impact of Radiation on the Formation and Growth of Seed Black Holes Jarrett Johnson Los Alamos National Laboratory with Joe Smidt (LANL) Aycin Aykutalp (LANL) Daniel Whalen (Portsmouth) Hui Li (LANL)
More informationThe First Black Holes and. their Host Galaxies. John Wise
The First Black Holes and John Wise Chao Shi (GT), Pengfei Chen (UCSD), Ayçin Aykutalp (GT), Tom Abel (Stanford), Peter Johansson (Helsinki), Michael Norman (UCSD), Brian O Shea (MSU), John Regan (Helsinki),
More informationMassive black hole formation in cosmological simulations
Institut d Astrophysique de Paris IAP - France Massive black hole formation in cosmological simulations Mélanie HABOUZIT Marta Volonteri In collaboration with Yohan Dubois Muhammed Latif Outline Project:
More informationThe Supermassive Seeds of Supermassive Black Holes
The Supermassive Seeds of Supermassive Black Holes Jarrett Johnson (LANL) with Hui Li, Joe Smidt, Dan Whalen, Wes Even, Chris Fryer (LANL) Bhaskar Agarwal, Claudio Dalla Vecchia, Eyal Neistein (MPE) Ken
More informationThe Growth and Radiative Signatures of High Redshift Black Holes
The Growth and Radiative Signatures of High Redshift Black Holes Jarrett Johnson (LANL) with Bhaskar Agarwal (Yale) Joe Smidt (LANL) Brandon Wiggins (LANL, BYU) Dan Whalen (Heidelberg, Portsmouth) Erik
More informationThe First Billion Years project: birthplaces of direct collapse black holes
doi:10.1093/mnras/stu1112 The First Billion Years project: birthplaces of direct collapse black holes Bhaskar Agarwal, 1 Claudio Dalla Vecchia, 1,2,3 Jarrett L. Johnson, 1,4 Sadegh Khochfar 1,5 and Jan-Pieter
More informationarxiv: v1 [astro-ph.ga] 28 Jan 2016
Mon. Not. R. Astron. Soc. 000,?? 16 (2016) Printed 1 February 2016 (MN LATEX style file v2.2) From the first stars to the first black holes Rosa Valiante 1, Raffaella Schneider 1, Marta Volonteri 2, Kazuyuki
More informationThe Interplay Between Galaxies and Black Holes A Theoretical Overview. Massimo Ricotti (U of Maryland)
The Interplay Between Galaxies and Black Holes A Theoretical Overview Massimo Ricotti (U of Maryland) ..a tale of many sleepless nights Maya and Noemi Ricotti Cosmological Context Outline Formation of
More informationThe Origin of Supermassive Black Holes. Daniel Whalen. McWilliams Fellow Carnegie Mellon
The Origin of Supermassive Black Holes Daniel Whalen McWilliams Fellow Carnegie Mellon Mergers Accretion The SMBH Conundrum SDSS quasars of ~ 10 9 Msun have been found at z ~ 6, a Gyr after the Big Bang
More informationThe Pop III/II Transition
The First Stars and Galaxies: Challenges for the Next Decade March 8-11, 2010 Austin, Texas The Pop III/II Transition Raffaella Schneider INAF/Osservatorio Astrofisico di Arcetri What are the minimal conditions
More informationThe first black holes
The first black holes Marta Volonteri Institut d Astrophysique de Paris M. Habouzit, Y. Dubois, M. Latif (IAP) A. Reines (NOAO) M. Tremmel (University of Washington) F. Pacucci (SNS) High-redshift quasars
More informationFeedback, AGN and galaxy formation. Debora Sijacki
Feedback, AGN and galaxy formation Debora Sijacki Formation of black hole seeds: the big picture Planck data, 2013 (new results 2015) Formation of black hole seeds: the big picture CMB black body spectrum
More informationSupermassive black hole formation at high redshift
Supermassive black hole formation at high redshift Muhammad Latif Institut d'astrophysique de Paris, France Marta Volonteri, Dominik Schleicher, Melanie Habouzit,Tilman Hartwig, Kazu Omukai, Jens Niemeyer,
More informationDetecting direct collapse black holes: making the case for CR7
Advance Access publication 2016 May 19 doi:10.1093/mnras/stw1173 Detecting direct collapse black holes: making the case for CR7 Bhaskar Agarwal, 1 Jarrett L. Johnson, 2 Erik Zackrisson, 3 Ivo Labbe, 4
More informationarxiv: v3 [astro-ph.ga] 8 Aug 2016
Mon. Not. R. Astron. Soc. 000, 1 21 (2016) Printed 10 August 2016 (MN LATEX style file v2.2) Exploring the nature of the Lyman-α emitter CR7 arxiv:1512.01111v3 [astro-ph.ga] 8 Aug 2016 Tilman Hartwig 1,2,
More informationFormation and cosmic evolution of supermassive black holes. Debora Sijacki
Formation and cosmic evolution of supermassive black holes Debora Sijacki Summer school: Black Holes at all scales Ioannina, Greece, Sept 16-19, 2013 Lecture 1: - formation of black hole seeds - low mass
More informationBlack hole formation and growth with non-gaussian primordial density perturbations
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed November 5, 2018 (MN LATEX style file v2.2) Black hole formation and growth with non-gaussian primordial density perturbations Primordial perturbations
More informationGrowing and merging massive black holes
Growing and merging massive black holes Marta Volonteri Institut d Astrophysique de Paris S. Cielo (IAP) R. Bieri (MPA) Y. Dubois (IAP) M. Habouzit (Flatiron Institute) T. Hartwig (IAP) H. Pfister (IAP)
More informationForma&on of supermassive black holes
Forma&on of supermassive black holes Mélanie Habouzit Marta Volonteri Muhammad La&f Yohan Dubois Collaborators: Joe Silk, Gary Mamon, Sébas&en Peirani, Takahiro Nishimichi Two main scenarios to form supermassive
More informationFORMATION OF SUPERMASSIVE BLACK HOLES Nestor M. Lasso Cabrera
FORMATION OF SUPERMASSIVE BLACK HOLES Nestor M. Lasso Cabrera In this presentation the different theories that can explain the formation of Supermassive Black Holes (SMBH) are presented. Before focus on
More informationThe First Galaxies. Erik Zackrisson. Department of Astronomy Stockholm University
The First Galaxies Erik Zackrisson Department of Astronomy Stockholm University Outline The first galaxies what, when, why? What s so special about them? Why are they important for cosmology? How can we
More informationThe first stars and primordial IMBHs
The first stars and primordial IMBHs Ab initio predictions of black hole merger rates by the time LISA flies? Tom Abel Penn State Initial Conditions Time Evolution z=100 z=24 z=20.4 10 comoving kpc Cosmological
More informationarxiv: v2 [astro-ph.ga] 24 Apr 2017
Mon. Not. R. Astron. Soc. 000, 1 6 (0000) Printed 21 October 2018 (MN LATEX style file v2.2) Effects of binary stellar populations on direct collapse black hole formation arxiv:1609.08605v2 [astro-ph.ga]
More informationarxiv: v1 [astro-ph.ga] 26 May 2014
Mon. Not. R. Astron. Soc. 000, 1 12 (2012) Printed 18 June 2018 (MN LATEX style file v2.2) arxiv:1405.6743v1 [astro-ph.ga] 26 May 2014 Feedback-regulated Super Massive Black Hole Seed Formation Mark Dijkstra
More informationFormation of z~6 Quasars from Hierarchical Galaxy Mergers
Formation of z~6 Quasars from Hierarchical Galaxy Mergers Yuexing Li et al Presentation by: William Gray Definitions and Jargon QUASAR stands for QUASI-stellAR radio source Extremely bright and active
More informationGrowing massive black holes via super-critical accretion on to stellar-mass seeds
Growing massive black holes via super-critical accretion on to stellar-mass seeds Alessandro Lupi IAP (Paris) DARK ERC-2010 AdG_20100224 in collaboration with: F. Haardt, M. Dotti, M. Colpi, D. Fiacconi,
More informationSupermassive Black Holes in Galactic Nuclei and their Models of Formation
Supermassive Black Holes in Galactic Nuclei and their Models of Formation Clemence Yun Chan Lee Abstract Supermassive black holes (SMBHs) are black holes with masses larger than 10 5 solar mass, and they
More informationLyman-Werner escape fractions from the first galaxies
Lyman-Werner escape fractions from the first galaxies Schauer+17, ArXiv 1701.07031 (MNRAS accepted) Anna T. P. Schauer with Ralf Klessen, Simon Glover, Dan Whalen and Muhammad Latif, Bhaskar Agarwal, Lluis
More informationThe Pop III IMF: A Progress Report. Michael L. Norman University of California, San Diego & San Diego Supercomputer Center
The Pop III IMF: A Progress Report Michael L. Norman University of California, San Diego & San Diego Supercomputer Center Disclaimer Notion of Pop III IMF is not well-defined We don t observe Pop III stars
More informationFORMATION OF PRIMORDIAL STARS
Talk@INT, UW, July 5, 2006 FORMATION OF PRIMORDIAL STARS Naoki Yoshida Department of Physics Nagoya University Outline Thermal evolution of a primordial gas - Physics at high densities (cooling, chem.
More informationThe formation of the first supermassive black holes
The formation of the first supermassive black holes Zoltán Haiman Columbia University Collaborators: Eli Visbal (Columbia) Kohei Inayoshi (Columbia) Taka Tanaka (Stony Brook/NYU) Jemma Wolcott-Green (Columbia)
More informationMichael Shull (University of Colorado)
Early Galaxies, Stars, Metals, and the Epoch of Reionization Michael Shull (University of Colorado) Far-IR Workshop (Pasadena, CA) May 29, 2008 Submillimeter Galaxies: only the brightest? How long? [dust
More informationarxiv: v5 [astro-ph.co] 14 Sep 2015
Formation of the First Galaxies: Theory and Simulations Jarrett L. Johnson arxiv:1105.5701v5 [astro-ph.co] 14 Sep 2015 Abstract The properties of the first galaxies are shaped in large part by the first
More informationFeedback and Galaxy Formation
Heating and Cooling in Galaxies and Clusters Garching August 2006 Feedback and Galaxy Formation Simon White Max Planck Institute for Astrophysics Cluster assembly in ΛCDM Gao et al 2004 'Concordance'
More informationQuasi-stars and the Cosmic Evolution of Massive Black Holes
Quasi-stars and the Cosmic Evolution of Massive Black Holes Marta Volonteri and Mitchell C. Begelman 2010 MNRAS 409:1022 David Riethmiller January 26, 2011 Outline Two different methods for MBH formation:
More informationMotivation Q: WHY IS STAR FORMATION SO INEFFICIENT? Ṁ M gas / dyn. Log SFR. Kennicutt Log. gas / dyn
Motivation Q: WHY IS STAR FORMATION SO INEFFICIENT? Ṁ 0.017 M gas / dyn Log SFR Kennicutt 1998 Log gas / dyn Motivation Q: WHY IS STAR FORMATION SO INEFFICIENT? Moster 2009 No Feedback 10% of baryons Log(
More informationThe improvement of START
The improvement of START Kenji Hasegawa (U. Tsukuba, CCS Kobe branch) Takashi Okamoto (U. Tsukuba, CCS Kobe branch) Cosmological Radiative Transfer Comparison Project Workshop IV @ Austin, Texas, Dec 11-14,
More informationTHE ROLE OF RADIATION PRESSURE IN HIGH-Z DWARF GALAXIES
THE ROLE OF RADIATION PRESSURE IN HIGH-Z DWARF GALAXIES John Wise (Georgia Tech) Tom Abel (Stanford), Michael Norman (UC San Diego), Britton Smith (Michigan State), Matthew Turk (Columbia) 14 Dec 2012
More informationThe chemistry and thermodynamics of Pop III star formation
The chemistry and thermodynamics of Pop III star formation Where do the first stars form Form in dark matter minihalos with mass Mhalo 5 10 5 M Redshift z = 16-20 Tvir ~ 1000 K Gas density is around 1
More informationProbing the End of Dark Ages with High-redshift Quasars. Xiaohui Fan University of Arizona Dec 14, 2004
Probing the End of Dark Ages with High-redshift Quasars Xiaohui Fan University of Arizona Dec 14, 2004 High-redshift Quasars and the End of Cosmic Dark Ages Existence of SBHs at the end of Dark Ages BH
More informationarxiv: v2 [astro-ph.ga] 15 Dec 2016
Mon. Not. R. Astron. Soc. 000, 1 5 00 Printed 16 December 016 MN LATEX style file v. Upper limits on the mass and luminosity of Population III-dominated galaxies arxiv:1610.044v [astro-ph.ga] 15 Dec 016
More informationSurveys for high-redshift (z>6) AGN with AXIS (cf. Athena) James Aird. University of Cambridge (-> University of Leicester)
Surveys for high-redshift (z>6) AGN with AXIS (cf. Athena) James Aird University of Cambridge (-> University of Leicester) SMBH seed formation mechanisms Pop III star remnants MBH ~ 100 M z~20-30 Direct
More informationFormation and growth of galaxies in the young Universe: progress & challenges
Obergurgl. April 2014 Formation and growth of galaxies in the young Universe: progress & challenges Simon White Max Planck Institute for Astrophysics Ly α forest spectra and small-scale initial structure
More informationHigh-redshift formation and evolution of central massive objects II. The census of BH seeds
Mon. Not. R. Astron. Soc. 421, 1465 1475 (2012) doi:10.1111/j.1365-2966.2012.20406.x High-redshift formation and evolution of central massive objects II. The census of BH seeds B. Devecchi, 1 M. Volonteri,
More informationOutline: Part II. The end of the dark ages. Structure formation. Merging cold dark matter halos. First stars z t Univ Myr.
Outline: Part I Outline: Part II The end of the dark ages Dark ages First stars z 20 30 t Univ 100 200 Myr First galaxies z 10 15 t Univ 300 500 Myr Current observational limit: HST and 8 10 m telescopes
More informationMethodology. Friday, August 17, 12
Methodology Conditions for the formation of massive seed black holes 1. Major merger (1:3) of gas-rich late-type galaxies (B/T < 0.2) 2. Host halo Mh > 10 11 MSun 3. No a pre-existing black hole of MBH
More informationSearch for the FIRST GALAXIES
Search for the FIRST GALAXIES R. Pelló IRAP - Institut de Recherche en Astrophysique et Planétologie 1 XIème Ecole de Cosmologie : 17-22 Sep 2012 (Cargèse) Outline 1. Looking for the first galaxies a)
More informationThe Monster Roars: AGN Feedback & Co-Evolution with Galaxies
The Monster Roars: AGN Feedback & Co-Evolution with Galaxies Philip Hopkins Ø (Nearly?) Every massive galaxy hosts a supermassive black hole Ø Mass accreted in ~couple bright quasar phase(s) (Soltan, Salucci+,
More informationarxiv: v1 [astro-ph.ga] 5 Jun 2014
The formation of massive primordial stars in the presence of moderate UV backgrounds arxiv:1406.1465v1 [astro-ph.ga] 5 Jun 2014 M. A. Latif 1, D. R. G. Schleicher 1, S. Bovino 1, T. Grassi 2,3, M. Spaans
More informationRADIATION HYDRODYNAMICAL SIMULATIONS OF THE FIRST QUASARS
Draft version September 25, 2018 Preprint typeset using L A TEX style emulateapj v. 12/16/11 RADIATION HYDRODYNAMICAL SIMULATIONS OF THE FIRST QUASARS Joseph Smidt 1, Daniel J. Whalen 2, Jarrett L. Johnson
More informationMpc scale effects on the inner pcs of galaxies
Mpc scale effects on the inner pcs of galaxies Nelson Padilla PUC-Chile Collaborators: Sofía Cora (U. N. La Plata), Andrés Ruiz, Dante Paz (U. N. Córdoba), Claudia Lagos (Durham U.), Federico Stasyszyn
More informationSMBH growth parameters in the early Universe of Millennium and Millennium-II simulations
doi:10.1093/mnras/stv1065 SMBH growth parameters in the early Universe of Millennium and Millennium-II simulations Majda Smole, Miroslav Micic and Nemanja Martinović Astronomical Observatory, Volgina 7,
More informationThe formation of direct collapse black holes under the influence of streaming velocities
Mon. Not. R. Astron. Soc., 1 8 (22) Printed 12 January 218 (MN LATEX style file v2.2) The formation of direct collapse black holes under the influence of streaming velocities Anna T. P. Schauer 1, John
More informationarxiv: v2 [astro-ph.ga] 31 Jul 2018
Mon. Not. R. Astron. Soc. 000, 1 12 (2016) Printed 2 August 2018 (MN LATEX style file v2.2) The Growth of Black Holes from Population III Remnants in the Renaissance Simulations arxiv:1804.06477v2 [astro-ph.ga]
More informationSTELLAR BLACK HOLES & HMXBs AT THE DAWN OF THE UNIVERSE
STELLAR BLACK HOLES & HMXBs AT THE DAWN OF THE UNIVERSE Félix Mirabel CEA-Saclay (France) & CONICET (Argentina) At the crossroads of Stellar Evolution, High Energy Astrophysics & Cosmology FEEDBACK FROM
More informationstelle e galassie primordiali
stelle e galassie primordiali Raffaella Schneider INAF/Osservatorio Astronomico di Roma Matteo de Bennassuti, PhD INAF/OAR Stefania Marassi, Pdoc INAF/OAR Luca Graziani, Pdoc INAF/OAR Rosa Valiante, Pdoc
More informationFirst Light And Reionization. Nick Gnedin
First Light And Reionization Nick Gnedin Reionization and 5-Year Plans Sovier leaders would love reionization it is a field where every 5 years something interesting happens. SDSS Quasars ~ 2005 z=5.7
More informationSimulations of First Star Formation
Simulations of First Star Formation Michael L. Norman (UCSD) Brian O Shea (LANL) 1 Formation of the first stars: current paradigm (Abel et al. 2002, Bromm et al. 2002,Yoshida et al. 2006) DM halos of M~10
More informationOutline. Walls, Filaments, Voids. Cosmic epochs. Jeans length I. Jeans length II. Cosmology AS7009, 2008 Lecture 10. λ =
Cosmology AS7009, 2008 Lecture 10 Outline Structure formation Jeans length, Jeans mass Structure formation with and without dark matter Cold versus hot dark matter Dissipation The matter power spectrum
More informationThe Iguaçu Lectures. Nonlinear Structure Formation: The growth of galaxies and larger scale structures
April 2006 The Iguaçu Lectures Nonlinear Structure Formation: The growth of galaxies and larger scale structures Simon White Max Planck Institute for Astrophysics z = 0 Dark Matter ROT EVOL Cluster structure
More informationarxiv: v1 [astro-ph.co] 27 Mar 2012
The Formation of the First Massive Black Holes Zoltán Haiman arxiv:1203.6075v1 [astro-ph.co] 27 Mar 2012 Abstract Supermassive black holes (SMBHs) are common in local galactic nuclei, and SMBHs as massive
More informationWFIRST and JWST synergies in the study of First Light. M. Stiavelli STScI, Baltimore
WFIRST and JWST synergies in the study of First Light M. Stiavelli STScI, Baltimore 1 WFIRST and JWST synergies in the study of First Light Plan: - Detecting the First Stars WFIRST-AFTA as an object finder
More informationAGN in hierarchical galaxy formation models
AGN in hierarchical galaxy formation models Nikos Fanidakis and C.M. Baugh, R.G. Bower, S. Cole, C. Done, C. S. Frenk Physics of Galactic Nuclei, Ringberg Castle, June 18, 2009 Outline Brief introduction
More informationProbing the Origin of Supermassive Black Hole Seeds with Nearby Dwarf Galaxies. Amy Reines Einstein Fellow NRAO Charlottesville
Probing the Origin of Supermassive Black Hole Seeds with Nearby Dwarf Galaxies Amy Reines Einstein Fellow NRAO Charlottesville Motivation: The origin of supermassive BH seeds Motivation: The origin of
More informationOn the inside-out reionization of the MW satellite system
On the inside-out reionization of the MW satellite system Reionization at galaxy-scale P. Ocvirk, D. Aubert Observatoire astronomique de Strasbourg Impact of radiation field structure on the Galaxy RT
More informationarxiv: v1 [astro-ph.co] 18 Jan 2012
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 19 January 2012 (MN LATEX style file v2.2) High-redshift formation and evolution of central massive objects II: The census of BH seeds arxiv:1201.3761v1
More informationOrianne ROOS CEA-Saclay Collaborators : F. Bournaud, J. Gabor, S. Juneau
Orianne ROOS CEA-Saclay Collaborators : F. Bournaud, J. Gabor, S. Juneau Bachelor of Physics, Master of Astrophysics Université de Strasbourg PhD, Université Paris-Diderot Observatoire de Strasbourg Les
More informationStar Formation at the End of the Dark Ages
Star Formation at the End of the Dark Ages...or when (rest-frame) UV becomes (observed) IR Piero Madau University of California Santa Cruz Distant Star Formation: what who came first? neanderthal Outline
More informationCompact Starbursts: Extreme Star Formation and Feedback at High Density Aleks Diamond-Stanic Grainger Fellow, University of Wisconsin
Compact Starbursts: Extreme Star Formation and Feedback at High Density Aleks Diamond-Stanic Grainger Fellow, University of Wisconsin Arp 220 (talks by N. Scoville, D. Elbaz) 12 galaxies from our sample
More informationFermi Bubbles: echoes of the last quasar outburst?
Fermi Bubbles: echoes of the last quasar outburst? Sergei Nayakshin, University of Leicester Kastytis Zubovas, Andrew King (Leicester) Chris Power (U of Western Australia, Perth) The Fermi Bubbles in the
More informationarxiv:astro-ph/ v1 29 Mar 2007
DRAFT VERSION SEPTEMBER 16, 2018 Preprint typeset using LATEX style emulateapj v. 6/22/04 HOW RAPIDLY DO SUPERMASSIVE BLACK HOLE SEEDS GROW AT EARLY TIMES? FEDERICO I. PELUPESSY 1, TIZIANA DI MATTEO 1,
More informationObservations of First Light
Image from Space Telescope Science Institute Observations of First Light Betsy Barton (UC Irvine) Member, TMT SAC Project Scientist, IRIS on TMT Microwave Background What reionized the universe? The End
More informationCo-Evolution of Central Black Holes and Nuclear Star Clusters
Co-Evolution of Central Black Holes and Nuclear Star Clusters Oleg Gnedin (University of Michigan) Globular clusters in the Galaxy median distance from the center is 5 kpc Resolved star cluster highest
More informationGALAXIES 626. The Milky Way II. Chemical evolution:
GALAXIES 626 The Milky Way II. Chemical evolution: Chemical evolution Observation of spiral and irregular galaxies show that the fraction of heavy elements varies with the fraction of the total mass which
More informationin the Milky NOW Way AND and THEN dwarf galaxies Stefania Salvadori
CARBON-ENHANCED DWARF GALAXIES: METAL-POOR STARS in the Milky NOW Way AND and THEN dwarf galaxies Stefania Salvadori University of Groningen Kapteyn Astronomical Institute Netherlands Organization for
More informationCosmological simulations of galaxy formation
Cosmological simulations of galaxy formation Modern galaxy formation simulations Mock gri SDSS composite image with dust absorption based on Draine opacity model. NGC4622 as seen from HST Outline - Impact
More informationMASSIVE BLACK HOLES AMY REINES IN NEARBY DWARF GALAXIES HUBBLE FELLOW NATIONAL OPTICAL ASTRONOMY OBSERVATROY
MASSIVE BLACK HOLES IN NEARBY DWARF GALAXIES AMY REINES HUBBLE FELLOW NATIONAL OPTICAL ASTRONOMY OBSERVATROY Motivation: The origin of massive black holes (BHs) Massive BHs are fundamental components of
More informationAST Cosmology and extragalactic astronomy. Lecture 20. Black Holes Part II
AST4320 - Cosmology and extragalactic astronomy Lecture 20 Black Holes Part II 1 AST4320 - Cosmology and extragalactic astronomy Outline: Black Holes Part II Gas accretion disks around black holes, and
More informationAGN Feedback In an Isolated Elliptical Galaxy
AGN Feedback In an Isolated Elliptical Galaxy Feng Yuan Shanghai Astronomical Observatory, CAS Collaborators: Zhaoming Gan (SHAO) Jerry Ostriker (Princeton) Luca Ciotti (Bologna) Greg Novak (Paris) 2014.9.10;
More informationOrigin of Bi-modality
Origin of Bi-modality and Downsizing Avishai Dekel HU Jerusalem Galaxies and Structures Through Cosmic Times Venice, March 2006 Summary Q: z
More informationFormation Processes of IMBHs
Formation Processes of IMBHs Melvyn B. Davies Department of Astronomy and Theoretical Physics Lund University www.astro.lu.se Stellar mass Intermediate mass SMBH (A) (B) Runaway collisions... Runaway mergers
More informationM. Dijkstra (UiO) Aspen, Mark Dijkstra. with: Shiv Sethi (RRI), Abraham Loeb (CfA), Max Gronke (UiO) & David Sobral (Lancaster)
Mark Dijkstra with: Shiv Sethi (RRI), Abraham Loeb (CfA), Max Gronke (UiO) & David Sobral (Lancaster) arxiv:1601.04712 (ApJ accepted), Dijkstra, Sethi & Loeb arxiv:1602.07695 (resubmitted to ApJ), Dijkstra,
More informationDiffuse Extragalactic Background Radiation and Gamma-Ray Attenuation
Diffuse Extragalactic Background Radiation and Gamma-Ray Attenuation Joel Primack, Rudy Gilmore, Piero Madau & Rachel Somerville UCSC & STScI The EBL is very difficult to observe directly because of foregrounds,
More informationAstronomy. Astrophysics. Effects of turbulence and rotation on protostar formation as a precursor of massive black holes
DOI: 10.1051/0004-6361/201424658 c ESO 2014 Astronomy & Astrophysics Effects of turbulence and rotation on protostar formation as a precursor of massive black holes C. Van Borm 1,2, S. Bovino 1, M. A.
More informationBlack Hole Formation in the Early Universe
1 Black Hole Formation in the Early Universe Luo Yang (Osaka University) XC30 2 1. Introduction Observations of high-redshift quasars reveal that some supermassive black holes (SMBH) with masses exceeding
More informationLocal photo-ionization radiation, Circum-galactic gas cooling and galaxy formation
Local photo-ionization radiation, Circum-galactic gas cooling and galaxy formation or A critical Star-Formation-Rate divides hot-mode from cold-mode accretion Sebastiano Cantalupo IMPS Fellow, UCSC Chandra
More informationBridging the near and the far: constraints on first star formation from stellar archaeology. Raffaella Schneider Sapienza University of Rome
Bridging the near and the far: constraints on first star formation from stellar archaeology Raffaella Schneider Sapienza University of Rome Kyoto,First Stars IV 2012 Kyoto,First Stars IV 2012 "As we extend
More informationThe First Stars and their Impact on Cosmology
The First Stars and their Impact on Cosmology V. Bromm University of Texas, Austin, TX 78712, USA Within variants of the cold dark matter model of cosmological structure formation, the first sources of
More informationGalaxy Formation, Reionization, the First Stars and Quasars
Ay 127 Galaxy Formation, Reionization, the First Stars and Quasars Coral Wheeler Galaxy Formation The early stages of galaxy evolution no clear-cut boundary has two principal aspects: assembly of the mass,
More informationHunting for Infrared Signatures of Supermassive Black Hole Activity in Dwarf Galaxies
Hunting for Infrared Signatures of Supermassive Black Hole Activity in Dwarf Galaxies Kevin Hainline University of Arizona, Steward Observatory Amy Reines, NOAO Jenny Greene, Princeton University Daniel
More informationGravitational Radiation from Coalescing SMBH Binaries in a Hierarchical Galaxy Formation Model
Gravitational Radiation from Coalescing SMBH Binaries in a Hierarchical Galaxy Formation Model Motohiro ENOKI (National Astronomical Observatory of Japan) Kaiki Taro INOUE (Kinki University) Masahiro NAGASHIMA
More informationResearch Collection. How will we determine the reionization history of the universe?: introduction to session 2. Other Conference Item.
Research Collection Other Conference Item How will we determine the reionization history of the universe?: introduction to session 2 Author(s): Haiman, Zoltàn Publication Date: 2003 Permanent Link: https://doi.org/10.3929/ethz-a-004584667
More informationn [Mpc -3 ] [erg] E bind
Submitted to ApJ on April 26, 2007 Preprint typeset using L A TEX style emulateapj v. 10/09/06 SLAC-PUB-12666 astro-ph/0707.2059 August 2007 SUPPRESSION OF H 2 COOLING IN THE ULTRAVIOLET BACKGROUND John
More informationSupermassive Black Hole Formation in Galactic Nuclei
Supermassive Black Hole Formation in Galactic Nuclei Melvyn B. Davies Department of Astronomy and Theoretical Physics Lund University Ross Church (Lund), Cole Miller (Maryland), Serge Nzoke (Lund), Jillian
More informationReview of stellar evolution and color-magnitude diagrams
Review of stellar evolution and color-magnitude diagrams The evolution of stars can be used to study the properties of galaxies Very characteristic features pinpoint at the age (chemistry) of the stars
More informationHeating and Cooling in Clusters & Galaxies
Physics 463, Spring 07 Lecture 12 Heating and Cooling in Clusters & Galaxies review of the white & rees model hydrodynamical simulations hot and cold flows multi-phase cooling feedback: photoionization,
More informationThe First Cosmic Billion Years. Andrea Ferrara Scuola Normale Superiore, Pisa, Italy
The First Cosmic Billion Years Andrea Ferrara Scuola Normale Superiore, Pisa, Italy DAVID The Dark Ages VIrtual Department http://www.arcetri.astro.it/twiki/bin/view/david/webhome S. Bianchi INAF/Arcetri
More informationFormation of primordial supermassive stars by burst accretion
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 15 October 2018 (MN LATEX style file v2.2) Formation of primordial supermassive stars by burst accretion An alternative model which circumvents these
More informationWhat do we need to know about galaxy formation?
What do we need to know about galaxy formation? rachel somerville University of Michigan Hubble Science Legacy Workshop April 2002 what s next? test the CDM paradigm constrain the nature of the dark matter
More information