HLX-1: unsolved puzzles
|
|
|
- Justin Wells
- 5 years ago
- Views:
Transcription
1 HLX-1: unsolved puzzles Roberto Soria Many thanks to: Sean Farrell Francesca Annibali Jeanette Gladstone Pasi Hakala George Hau Paul Kuin Michela Mapelli Manfred Pakull Luca Zampieri Brindisi 2013
2 Outline What we know about HLX-1 Outstanding problems for the nature of this BH Formation scenarios and relation with ESO Where to look for similar systems? 1 Brindisi 2013
3 IC1633 (cd galaxy) Abell 2877 (Swift kev) d ~ 95 Mpc 2 Brindisi 2013
4 IC1633 (cd galaxy) Abell 2877 (Swift kev) d ~ 95 Mpc 3 Brindisi 2013
5 IC1633 IC1633 (cd galaxy) (cd galaxy) Abell 2877 (Swift kev) d ~ 95 Mpc 4 Brindisi 2013
6 IC1633 (cd galaxy) Abell 2877 (Swift kev) d ~ 95 Mpc 5 Brindisi 2013
7 X-ray source corresponds to optical point-like source (V ~ 24 mag) projected ~4 kpc from galaxy nucleus HLX1 ESO (F555W band) 6 Brindisi 2013
8 HST/WFC3 (U,V,I) 7 Brindisi 2013
9 X-ray outbursts every ~370 days 8 Brindisi 2013
10 Transient radio emission during outbursts similar to state transitions in Galactic BHs? (Webb et al 2012) 9 Brindisi 2013
11 X-ray spectra over (XMM-Newton/EPIC) (Servillat et al 2011) (Dominant) soft disk-blackbody + (weak) power-law 10 Brindisi 2013
12 X-ray spectrum in the 2010 outburst (Chandra/ACIS) Multicolour blackbody T ~ 0.2 kev R ~ (4 6) x 10 4 km (Servillat et al 2011) 11 Brindisi 2013
13 X-ray spectrum in the 2010 outburst (Swift/XRT) Multicolour blackbody T ~ 0.2 kev R ~ (4 6) x 10 4 km Power-law photon index ~ 2 (Soria et al 2012) 12 Brindisi 2013
14 X-ray temperature-luminosity relation consistent with disk emission Modelled as standard disk Modelled as slim disk BH mass ~ a few 10 3 a few 10 4 M sun (Davis et al 2011 Godet et al 2012) 13 Brindisi 2013
15 The case for an IMBH (M ~ 10 4 M sun ) Peak luminosity ~ 1E42 erg/s ~ L Edd of a 10,000 M sun BH Size of the thermal emitter ~ 50,000 km ~ expected inner-disk radius around a 10,000 M sun BH Typical Galactic BHs have M ~ 10 M sun, L ~ 1E39 erg/s, R ~ 50 km 14 Brindisi 2013
16 Outstanding problems 1 Outburst timescale and BH mass 15 Brindisi 2013
17 4 outbursts of HLX-1 ( ) 16 Brindisi 2013
18 HLX-1 M ~ 10,000 M sun? Exponential + linear decay (King & Ritter 1998) (Soria 2013) GRO J M ~ 7 M sun (Powell et al 2007) Viscous timescale of HLX-1 only 3 or 4 times longer than in typical Galactic BHs 17 Brindisi 2013
19 Very small outer-disk size? τ e R 2 (3n) n αc s H R 12 τ e 60 d 4 5 α M m3 1 5 For T ~ 10 4 K, c s cm/s, H/R ~ 0.1 R out ατ e ~ cm Compared with the large semimajor axis a = m q 1 3 P yr 2 3 cm ~ few cm 18 Brindisi 2013
20 Roche Lobe geometry for a circular orbit a = semimajor axis a = m q 1 3 P yr 2 3 cm R T Disk size: R out R T 0.60a 1+q 19 Brindisi 2013
21 Roche Lobe geometry for a circular orbit a = semimajor axis a = m q 1 3 P yr 2 3 cm R cir Disk size: R out R cir 20 Brindisi 2013
22 e ~ ! Mismatch between disk size (very small) and orbital size (very large) suggests an eccentric orbit (Lasota et al 2011, Soria 2013) 1 + e a Donor star fills its Roche Lobe only at periastron 1 e a X-ray outbursts shortly after periastron 21 Brindisi 2013
23 Why is the outer disk radius so small? (= why outburst timescale so short) Very eccentric orbit? Have we overestimated the BH mass? Very low-angular-momentum accretion flow? (wind rather than Lagrangian point overflow) Higher viscosity than in Galactic BHs? 22 Brindisi 2013
24 Outstanding problems 2 What is the optical/uv emission? 23 Brindisi 2013
25 What is the optical/uv emission: young star cluster or BH accretion disk? Three ways to find out: Is the optical/uv variable? Is it point-like or extended? Broad-band spectral fit? 24 Brindisi 2013
26 What is the optical/uv emission: young star cluster or BH accretion disk? Three ways to find out: Is the optical/uv variable? HST (Sep 2010): U ~ V ~ I ~ Vegamag VLT (Nov 2010): U ~ 23.9 V ~ 24.8 R ~ 24.7 Gemini (Sep-Oct 2012): R ~ 24.5 Still no definitive answer (Farrell et al 2012 Soria et al 2013 Farrell et al 2013 submitted) 25 Brindisi 2013
27 Is the optical/uv point-like or extended? HST/ACS 1500 Ang Point-like in optical (size < 40 pc) Point-like core with possibly extended wings in the far-uv (1500 Ang) (Mapelli et al 2013a,b) 26 Brindisi 2013
28 Broad-band spectral fit: disk and star cluster both contribute to optical/uv (Farrell et al 2013 subm) 27 Brindisi 2013
29 Outstanding problems 3 Where is the star-forming gas from? 28 Brindisi 2013
30 M ~ (a few E4-1E5) M sun of young stars (age <~ 20 Myr) Requires ~1E6 M sun of gas around the BH BH too small to keep so much gas in its sphere of influence No other young clusters/super-star-clusters near HLX-1 ESO is an old galaxy, not much gas Gas and young star cluster likely to come from outside 29 Brindisi 2013
31 Outstanding problems 4 Relation between HLX-1 and nearby host galaxy ESO243-49? 30 Brindisi 2013
32 VLT/FORS2 long-slit spectrum (Soria, Hau & Pakull 2013; Wiersema et al 2010) 31 Brindisi 2013
33 32 Brindisi 2013
34 Nebular(?) Ha emission FWHM ~ 400 km/s L(Ha) ~ few E37 erg/s Higher recession velocity than stars in ESO Brindisi 2013
35 HLX-1 would cross ESO in ~ 20 Myr (Soria et al 2013) +210 km/s HLX km/s -210 km/s 34 Brindisi 2013
36 Extended far-uv emission near HLX-1 (Mapelli, Annibali, Zampieri & Soria 2013) 35 Brindisi 2013
37 Extended far-uv emission near HLX-1 (Mapelli, Annibali, Zampieri & Soria 2013) 36 Brindisi 2013
38 37 Brindisi 2013
39 Smoking gun of minor merger, or unrelated background? 38 Brindisi 2013
40 N-body SPH simulations of a minor merger (Mapelli et al 2012, 2013a,b) Bulgeless gas-rich satellite, mass ratio ~ 1/20 Gas carried by satellite star formation Can reproduce optical/uv light profile of HLX-1 39 Brindisi 2013
41 Galaxy-satellite distance, SFR in satellite & host galaxy (Mapelli et al 2013a) 40 Brindisi 2013
42 HLX-1 spends >~ 80% of its orbit (if bound!) well outside the D25 of the nearby galaxy VLT/FORS2 image by Hau & Soria 41 Brindisi 2013
43 IMBH only active when inside the D25 of a host galaxy? X-ray source spotted as IMBH candidate because it was seen inside a host galaxy Would we recognize similar IMBHs located ~100 kpc from any nearby big galaxies? Challenge for erosita s all sky X-ray survey 42 Brindisi 2013
44 Soft X-ray spectrum with X/O ~ 100 may be a clue (eg Brandt et al, Mainieri et al, Comastri et al ) 43 Brindisi 2013
45 Conclusions HLX-1 is disk-dominated during outbursts disk models can give a good estimate of BH mass X-ray lightcurve suggests single donor star on eccentric orbit Short rise & decline timescales: very small outer disk radius? Still unclear how much optical/uv from outer disk & how much from a young star cluster Extended far-uv emission around HLX-1: unrelated background or proof of recent minor merger? Recession velocity shows HLX-1 did not form inside ESO Brindisi 2013
Optical studies of an ultraluminous X-ray source: NGC1313 X-2
Optical studies of an ultraluminous X-ray source: NGC1313 X-2 Jifeng Liu Harvard-Smithsonian Center for Astrophysics in collaboration with Joel Bregman, Jon Miller, Philip Kaaret outline background: ultraluminous
Ultraluminous X-ray Sources: The most extreme X-ray binaries
Ultraluminous X-ray Sources: The most extreme X-ray binaries Luca Zampieri INAF-Astronomical Observatory of Padova 1 Outline Recent advancements on ULXs Present understanding of ULXs Conclusions 2 ULXs
Investigating Ultraluminous X-ray Sources through multi-wavelength variability, broadband spectra, and theoretical modelling
Investigating Ultraluminous X-ray Sources through multi-wavelength variability, broadband spectra, and theoretical modelling Luca Zampieri INAF-Astronomical Observatory of Padova In collaboration with:
A confirmed stellar-mass ULX with recurrent X-ray occultations from its precessing disk
A confirmed stellar-mass ULX with recurrent X-ray occultations from its precessing disk C. Motch, R. Soria and M. Pakull Thanks to F. Grisé and J. Greiner P13 in NGC 7793 : a key ULX D = 3.7 Mpc In Sculptor
Ultraluminous X-ray Sources forming in low metallicity natal environments
Ultraluminous X-ray Sources forming in low metallicity natal environments Luca Zampieri INAF-Astronomical Observatory of Padova M. Colpi, M. Mapelli, A. Patruno, T. P. Roberts Outline Intermediate or stellar
X-ray data analysis. Andrea Marinucci. Università degli Studi Roma Tre
X-ray data analysis Andrea Marinucci Università degli Studi Roma Tre marinucci@fis.uniroma3.it Goal of these lectures X-ray data analysis why? what? how? Why? Active Galactic Nuclei (AGN) Physics in a
A new catalogue of ultraluminous X-ray sources (and more!)
A new catalogue of ultraluminous X-ray sources (and more!) Tim Roberts Presented by Dom Walton (Cambridge) Hannah Earnshaw (Durham) Matt Middleton (Southampton) Silvia Mateos (IFCA) Ultraluminous X-ray
The fundamental INTEGRAL contributions to advance the millisecond X-ray pulsars research field
The fundamental INTEGRAL contributions to advance the millisecond X-ray pulsars research field M A U R I Z I O F A L A N G A Collaborators: L. Kuipers, W. Hermsen, J. Poutanen, A. Goldwurm, L. Stella June
Optical counterparts of ULXs. S. Fabrika
Optical counterparts of ULXs S. Fabrika Examples of ULX counterparts NGC4559 X-7 Soria et al. 2005 NGC5408 X-1 Grise et al. 2012 Holmberg IX X-1 Pakull & Grise, 2008 Grise et al. 2006 Cseh et al. 2012
Observing the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics
Observing the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics with: Tim Heckman (JHU) GALEX Science Team (PI: Chris Martin), Lee Armus,
Simulations of the tidal interaction and mass transfer of a star in an eccentric orbit around an intermediate-mass black hole: the case of HLX-1
doi:10.1093/mnras/stv2318 Simulations of the tidal interaction and mass transfer of a star in an eccentric orbit around an intermediate-mass black hole: the case of HLX-1 Edwin van der Helm, 1 Simon Portegies
The Black Hole in the Galactic Center. Eliot Quataert (UC Berkeley)
The Black Hole in the Galactic Center Eliot Quataert (UC Berkeley) Why focus on the Galactic Center? The Best Evidence for a BH: M 3.6 10 6 M (M = mass of sun) It s s close! only ~ 10 55 Planck Lengths
Pulsars as probes for the existence of IMBHs
Universidad de Valencia 15 November 2010 Pulsars as probes for the existence of IMBHs ANDREA POSSENTI Layout Known Black Hole classes Formation scenarios for the IMBHs IMBH candidates IMBH candidates (?)
Modelling multiwavelength emission of ULXs
Modelling multiwavelength emission of ULXs Elena Ambrosi University of Padova Luca Zampieri, Michela Mapelli INAF-Astronomical Observatory of Padova ULXs and Their Environments-Workshop 13-16 June 2016
The Milky Way Galaxy
1/5/011 The Milky Way Galaxy Distribution of Globular Clusters around a Point in Sagittarius About 00 globular clusters are distributed in random directions around the center of our galaxy. 1 1/5/011 Structure
Tidal disruption events from the first XMM-Newton Slew Survey
Tidal disruption events from the first XMM-Newton Slew Survey Pilar Esquej Centro de Astrobiologia (INTA-CSIC) Richard Saxton, Stefanie Komossa, Andy Read, M. Sanchez-Portal et al. Tidal disruption events
Roberto Soria (UCAS) Jets and outflows from super-eddington sources
Jets and outflows from super-eddington sources Roberto Soria (UCAS) Also thanks to: Ryan Urquhart (ICRAR PhD student) James Miller-Jones (ICRAR-Curtin) Manfred Pakull (Strasbourg Observatory) Christian
The parsec scale of. ac-ve galac-c nuclei. Mar Mezcua. International Max Planck Research School for Astronomy and Astrophysics
The parsec scale of ESO ac-ve galac-c nuclei International Max Planck Research School for Astronomy and Astrophysics COST Ac(on MP0905 - Black Holes in a Violent Universe In collaboration with A. Prieto,
A galaxy without its SMBH: implications for feedback
A galaxy without its SMBH: implications for feedback Francesca Civano (SAO) M. Elvis, G. Lanzuisi,, L. Blecha, A. Loeb, T. Aldcroft, M. Trichas A. Bongiorno, M. Brusa, A. Comastri, M. Salvato, A. Fruscione,
FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS
FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS Main Categories of Compact Systems Formation of Compact Objects Mass and Angular Momentum Loss Evolutionary Links to Classes of Binary Systems Future Work
X-ray binaries. Marat Gilfanov MPA, Garching
X-ray binaries Marat Gilfanov MPA, Garching Outline observational appearance populations in galaxies relation to star-formation history numbers, luminosity distributions, IMF Hans-Jakob Grimm (CfA) Igor
Based on a study by L.Yungelson, J.-P.Lasota, G.Dubus, G. Nelemans, E. van den Heuvel, S. Portegies Zwart, J. Dewi
EVOLUTION OF LOW-MASS CLOSE BINARIES WITH BLACK-HOLE COMPONENTS Based on a study by L.Yungelson, J.-P.Lasota, G.Dubus, G. Nelemans, E. van den Heuvel, S. Portegies Zwart, J. Dewi Out of 20 confirmed bh-candidate
7. BINARY STARS (ZG: 12; CO: 7, 17)
7. BINARY STARS (ZG: 12; CO: 7, 17) most stars are members of binary systems or multiple systems (triples, quadruples, quintuplets,...) orbital period distribution: P orb = 11 min to 10 6 yr the majority
A new mechanism for the formation of PRGs
A new mechanism for the formation of PRGs Spavone Marilena (INAF-OAC) Iodice Enrica (INAF-OAC), Arnaboldi Magda (ESO-Garching), Longo Giuseppe (Università Federico II ), Gerhard Ortwin (MPE-Garching).
X-ray observations of X-ray binaries and AGN
X-ray observations of X-ray binaries and AGN Tomaso M. Be!oni (INAF - Osservatorio Astronomico di Brera) (Visiting Professor, Univ. of Southampton) OUTLINE Lecture I: Accretion onto compact objects, X-ray
Decretion Disk Dynamics in Binary Be Stars
Decretion Disk Dynamics in Binary Be Stars Atsuo Okazaki (Hokkai- Gakuen Univ, Japan) In collaboration with S. Stefl (ESO), Th. Rivinius (ESO), D. Baade (ESO), K. Hayasaki (Hokkaido Univ, Japan) 1 Talk
Synchrotron Radiation II Cyclotron v Search for X-ray Transients with MAXI
Search for X-ray Transients with MAXI Nobuyuki Kawai (Tokyo Tech) M. Serino (RIKEN), H. Negoro (Nihon U.) on behalf of the MAXI Team MAXI Instrumentation and operation Observations for GW 150914 and results
Quasars ASTR 2120 Sarazin. Quintuple Gravitational Lens Quasar
Quasars ASTR 2120 Sarazin Quintuple Gravitational Lens Quasar Quasars Quasar = Quasi-stellar (radio) source Optical: faint, blue, star-like objects Radio: point radio sources, faint blue star-like optical
Ultra Luminous X-ray sources ~one of the most curious objects in the universe~
Ultra Luminous X-ray sources ~one of the most curious objects in the universe~ Shogo B. Kobayashi the University of Tokyo ULX workshop@isas 1 The discovery of the enigmatic sources pfabbiano & Trincheri
Basics, types Evolution. Novae. Spectra (days after eruption) Nova shells (months to years after eruption) Abundances
Basics, types Evolution Novae Spectra (days after eruption) Nova shells (months to years after eruption) Abundances 1 Cataclysmic Variables (CVs) M.S. dwarf or subgiant overflows Roche lobe and transfers
Crustal cooling in accretion heated neutron stars
Crustal cooling in accretion heated neutron stars Ed Cackett ecackett@umich.edu University of Michigan Collaborators: Rudy Wijnands, Jon Miller, Jeroen Homan, Walter Lewin, Manuel Linares Outline X-ray
v Characteristics v Possible Interpretations L X = erg s -1
Ultra Luminous X-ray sources v Characteristics L X = 39-41 erg s -1 >> M black hole(bh) L Edd = 39 erg s -1. Usually seen in star forming regions. On arms of spiral galaxies (right). In starburst or irregular
Observational Evidence of Black Holes Kolkata (India), Feb 2008
Observational Evidence of Black Holes Kolkata (India), Feb 2008 S Chakrabarti L Titarchuk R Kerr F Mirabel T Belloni S Zhang E Koerding T Alexander G Bisnovatyi-Kogan M DellaValle Z Paragi T Alexander
High Redshift Universe
High Redshift Universe Finding high z galaxies Lyman break galaxies (LBGs) Photometric redshifts Deep fields Starburst galaxies Extremely red objects (EROs) Sub-mm galaxies Lyman α systems Finding high
The Classification of Galaxies
Admin. 11/9/17 1. Class website http://www.astro.ufl.edu/~jt/teaching/ast1002/ 2. Optional Discussion sections: Tue. ~11.30am (period 5), Bryant 3; Thur. ~12.30pm (end of period 5 and period 6), start
Active Galactic Nuclei - Zoology
Active Galactic Nuclei - Zoology Normal galaxy Radio galaxy Seyfert galaxy Quasar Blazar Example Milky Way M87, Cygnus A NGC 4151 3C273 BL Lac, 3C279 Galaxy Type spiral elliptical, lenticular spiral irregular
Accretion in Binaries
Accretion in Binaries Two paths for accretion Roche-lobe overflow Wind-fed accretion Classes of X-ray binaries Low-mass (BH and NS) High-mass (BH and NS) X-ray pulsars (NS) Be/X-ray binaries (NS) Roche
Multi-wavelength Surveys for AGN & AGN Variability. Vicki Sarajedini University of Florida
Multi-wavelength Surveys for AGN & AGN Variability Vicki Sarajedini University of Florida What are Active Galactic Nuclei (AGN)? Galaxies with a source of non-stellar emission arising in the nucleus (excessive
GW from GRBs Gravitational Radiation from Gamma-Ray Bursts
GW from GRBs Gravitational Radiation from Gamma-Ray Bursts Tsvi Piran Racah Inst. of Jerusalem, Israel Dafne Guetta,, Ehud Nakar, Reem Sari Once or twice a day we see a burst of low energy gamma-rays from
Accretion onto the Massive Black Hole in the Galactic Center. Eliot Quataert (UC Berkeley)
Accretion onto the Massive Black Hole in the Galactic Center Eliot Quataert (UC Berkeley) Why focus on the Galactic Center? GR! Best evidence for a BH (stellar orbits) M 4x10 6 M Largest BH on the sky
Astr 2320 Thurs. April 27, 2017 Today s Topics. Chapter 21: Active Galaxies and Quasars
Astr 2320 Thurs. April 27, 2017 Today s Topics Chapter 21: Active Galaxies and Quasars Emission Mechanisms Synchrotron Radiation Starburst Galaxies Active Galactic Nuclei Seyfert Galaxies BL Lac Galaxies
Ultraluminous X-ray Sources in Nearby Galaxies
Ultraluminous X-ray Sources in Nearby Galaxies Doug Swartz NASA/Marshall Space Flight Center Ultraluminous X-ray Sources in the Universe Doug Swartz NASA/Marshall Space Flight Center Pre-Einstein X-ray
Formation and evolution of supergiant High Mass X-ray Binaries
Formation and evolution of supergiant High Mass X-ray Binaries, F. Fortin, W. Massonneau CEA, Université Paris Diderot Institut Universitaire de France The Impact of Binaries on Stellar Evolution ESO Worshop,
Demographics of radio galaxies nearby and at z~0.55. Are radio galaxies signposts to black-hole mergers?
Elaine M. Sadler Black holes in massive galaxies Demographics of radio galaxies nearby and at z~0.55 Are radio galaxies signposts to black-hole mergers? Work done with Russell Cannon, Scott Croom, Helen
Active Galactic Nuclei-I. The paradigm
Active Galactic Nuclei-I The paradigm An accretion disk around a supermassive black hole M. Almudena Prieto, July 2007, Unv. Nacional de Bogota Centers of galaxies Centers of galaxies are the most powerful
AG Draconis. A high density plasma laboratory. Dr Peter Young Collaborators A.K. Dupree S.J. Kenyon B. Espey T.B.
AG Draconis A high density plasma laboratory Collaborators A.K. Dupree S.J. Kenyon B. Espey T.B. Ake p.r.young@rl.ac.uk Overview CHIANTI database Symbiotic Stars AG Draconis FUSE FUSE observations of AG
Clustering studies of ROSAT/SDSS AGN through cross-correlation functions with SDSS Galaxies
Clustering studies of ROSAT/SDSS AGN through cross-correlation functions with SDSS Galaxies Mirko Krumpe (ESO, UCSD) mkrumpe@eso.org Collaborators: Takamitsu Miyaji (UNAM-E, UCSD), Alison L. Coil (UCSD),
Fermi 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
A Shock Model for the the Outburst from the Supermassive Black Hole in M87 Bill Forman - SAO/CfA
M87 A Shock Model for the the Outburst from the Supermassive Black Hole in M87 Bill Forman - SAO/CfA interactions galore; stripping at work, M87 outburst Low Eddington ratio accretion (like other normal
High Energy Astrophysics
High Energy Astrophysics Gamma-ray Bursts Giampaolo Pisano Jodrell Bank Centre for Astrophysics - University of Manchester giampaolo.pisano@manchester.ac.uk May 2011 Gamma-ray Bursts - Observations - Long-duration
Formation 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
Non-Blazar Gamma-ray Active Galactic Nuclei seen by Fermi-LAT. C.C. Teddy Cheung Naval Research Lab/NRC on behalf of the Fermi-LAT Collaboration
Non-Blazar Gamma-ray Active Galactic Nuclei seen by Fermi-LAT C.C. Teddy Cheung Naval Research Lab/NRC on behalf of the Fermi-LAT Collaboration 1 st LAT AGN Catalog (1LAC) Summary FmJ 2010 Entire 1LAC:
Astronomy 422! Lecture 7: The Milky Way Galaxy III!
Astronomy 422 Lecture 7: The Milky Way Galaxy III Key concepts: The supermassive black hole at the center of the Milky Way Radio and X-ray sources Announcements: Test next Tuesday, February 16 Chapters
Star formation in XMMU J : a massive galaxy cluster at z=1.4
Star formation in XMMU J2235.3-2557: a massive galaxy cluster at z=1.4 Ruth Grutzbauch University of Nottingham Amanda E. Bauer, University of Nottingham Marcel Bergmann, Gemini Observatory South Inger
XRBs in Star-forming Galaxies X-ray Luminosity Functions Ultra-Luminous X-ray Sources
XRBs in Star-forming Galaxies X-ray Luminosity Functions Ultra-Luminous X-ray Sources G. Fabbiano Harvard-Smithsonian CfA XRB Populations in Nearby Galaxies External galaxies provide `cleaner samples Distances
Active Galactic Nuclei
Active Galactic Nuclei Optical spectra, distance, line width Varieties of AGN and unified scheme Variability and lifetime Black hole mass and growth Geometry: disk, BLR, NLR Reverberation mapping Jets
GRB history. Discovered 1967 Vela satellites. classified! Published 1973! Ruderman 1974 Texas: More theories than bursts!
Discovered 1967 Vela satellites classified! Published 1973! GRB history Ruderman 1974 Texas: More theories than bursts! Burst diversity E peak ~ 300 kev Non-thermal spectrum In some thermal contrib. Short
LECTURE 1: Introduction to Galaxies. The Milky Way on a clear night
LECTURE 1: Introduction to Galaxies The Milky Way on a clear night VISIBLE COMPONENTS OF THE MILKY WAY Our Sun is located 28,000 light years (8.58 kiloparsecs from the center of our Galaxy) in the Orion
Scientific cases for Simbol-X of interest of the Italian community
Scientific cases for Simbol-X of interest of the Italian community Based on the High Energy Astrophysics study: Fields of interest and perspective for the national community ASI 2003-2004 Fabrizio Fiore
Dr G. I. Ogilvie Lent Term 2005 INTRODUCTION
Accretion Discs Mathematical Tripos, Part III Dr G. I. Ogilvie Lent Term 2005 INTRODUCTION 0.1. Accretion If a particle of mass m falls from infinity and comes to rest on the surface of a star of mass
High Energy Astrophysics
High Energy Astrophysics Accretion Giampaolo Pisano Jodrell Bank Centre for Astrophysics - University of Manchester giampaolo.pisano@manchester.ac.uk April 01 Accretion - Accretion efficiency - Eddington
Number of Stars: 100 billion (10 11 ) Mass : 5 x Solar masses. Size of Disk: 100,000 Light Years (30 kpc)
THE MILKY WAY GALAXY Type: Spiral galaxy composed of a highly flattened disk and a central elliptical bulge. The disk is about 100,000 light years (30kpc) in diameter. The term spiral arises from the external
Unstable Mass Transfer
Unstable Mass Transfer When the mass ratios are large, or when the donor star has a deep convective layer (so R M-1/3), mass loss will occur on a dynamical timescale. The result will be common envelope
The bolometric output of AGN in the XMM-COSMOS survey
The bolometric output of AGN in the XMM-COSMOS survey Elisabeta Lusso Dipartimento di Astronomia Università di Bologna-INAF/OABO A. Comastri, C. Vignali, G. Zamorani, M. Brusa, E. Treister, R. Gilli, M.
4U E. Bozzo. M. Falanga, A. Papitto, L. Stella, R. Perna, D. Lazzati G. Israel, S. Campana, V. Mangano, T. Di Salvo, L.
X-Ray Eclipse Time Delays in 4U2129+47 E. Bozzo M. Falanga, A. Papitto, L. Stella, R. Perna, D. Lazzati G. Israel, S. Campana, V. Mangano, T. Di Salvo, L. Burderi Università di Roma Tor Vergata, Italy
Globular Clusters and Low-Mass X-Ray Binaries in M87
Globular Clusters and Low-Mass X-Ray Binaries in M87 Daniel-Jens Kusterer, Amelia Bayo, Sinan Alis, Genoveva Micheva Tutor: Andrés Jordán ESO NEON Summer School NEON 2006-08.09.2006 Outline 1 Introduction
Quasars and Active Galactic Nuclei (AGN)
Quasars and Active Galactic Nuclei (AGN) Astronomy Summer School in Mongolia National University of Mongolia, Ulaanbaatar July 21-26, 2008 Kaz Sekiguchi Hubble Classification M94-Sa M81-Sb M101-Sc M87-E0
MASSIVE 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
AST 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
THE LAST SURVEY OF THE OLD WSRT: TOOLS AND RESULTS FOR THE FUTURE HI ABSORPTION SURVEYS
F. Maccagni; R. Morganti; T. Oosterloo; K. Geréb; N. Maddox, J. Allison THE LAST SURVEY OF THE OLD WSRT: TOOLS AND RESULTS FOR THE FUTURE HI ABSORPTION SURVEYS A SURVEY BEFORE THE BLIND SURVEYS During
In a dense region all roads lead to a black Hole (Rees 1984 ARAA) Deriving the Mass of SuperMassive Black Holes
In a dense region all roads lead to a black Hole (Rees 1984 ARAA) Deriving the Mass of SuperMassive Black Holes Stellar velocity fields MW Distant galaxies Gas motions gas disks around nearby black holes
Radio Detections During Two State Transitions of the Intermediate Mass Black Hole HLX-1
Radio Detections During Two State Transitions of the Intermediate Mass Black Hole HLX-1 Natalie Webb, 1,2 David Cseh, 3 Emil Lenc, 4,5 Olivier Godet, 1,2 Didier Barret, 1,2 Stephane Corbel, 3 Sean Farrell,
Old pre-main-sequence stars
Old pre-main-sequence stars and a second chance for planet formation Peter Scicluna Uni Kiel & ESO, Garching 9th September 2014 Giovanni Rosotti (MPE, USM, IoA) Leonardo Testi (ESO, INAF) Jim Dale (Excellence
Measuring Black Hole Masses in Nearby Galaxies with Laser Guide Star Adaptive Optics
Measuring Black Hole Masses in Nearby Galaxies with Laser Guide Star Adaptive Optics Claire Max Anne Medling Mark Ammons UC Santa Cruz Ric Davies Hauke Engel MPE-Garching Image of NGC 6240: Bush et al.
Vivienne Wild. Timing the starburst AGN connection
Vivienne Wild Timing the starburst AGN connection There are many theories successful in explaining the observed correlations between black holes and their host galaxies. In turn, these theories play a
Galaxies. Galaxy Diversity. Galaxies, AGN and Quasars. Physics 113 Goderya
Galaxies, AGN and Quasars Physics 113 Goderya Chapter(s): 16 and 17 Learning Outcomes: Galaxies Star systems like our Milky Way Contain a few thousand to tens of billions of stars. Large variety of shapes
Galaxies and the Universe. Our Galaxy - The Milky Way The Interstellar Medium
Galaxies and the Universe Our Galaxy - The Milky Way The Interstellar Medium Our view of the Milky Way The Radio Sky COBE Image of our Galaxy The Milky Way Galaxy - The Galaxy By Visual Observation
Active Galactic Nuclei
Active Galactic Nuclei Prof. Jeff Kenney Class 18 June 20, 2018 the first quasar discovered 3C273 (1963) very bright point source (the quasar ) jet the first quasar discovered 3C273 (1963) very bright
Halo Gas Velocities Using Multi-slit Spectroscopy
Halo Gas Velocities Using Multi-slit Spectroscopy Cat Wu Thesis Proposal, Fall 2009 Astronomy Department New Mexico State University Outline Diffuse ionized gas; galaxy halos Origin of halo galactic fountain
LeMMINGs the emerlin radio legacy survey of nearby galaxies Ranieri D. Baldi
LeMMINGs the emerlin radio legacy survey of nearby galaxies Ranieri D. Baldi in collaboration with I. McHardy, D. Williams, R. Beswick and many others The radio-loud / radio-quiet dichotomy Among the many
arxiv: v1 [astro-ph.he] 3 Sep 2016
![arxiv: v1 [astro-ph.he] 3 Sep 2016](/thumbs/91/105032374.jpg "arxiv: v1 [astro-ph.he] 3 Sep 2016")
Accepted for publication in Astronomy & Astrophysics, on August 29, 2016 arxiv:1609.00780v1 [astro-ph.he] 3 Sep 2016 ESO 243-49 HLX-1: scaling of X-ray spectral properties and black hole mass determination
Three Major Components
The Milky Way Three Major Components Bulge young and old stars Disk young stars located in spiral arms Halo oldest stars and globular clusters Components are chemically, kinematically, and spatially distinct
V2487 Oph 1998: a puzzling recurrent nova observed with XMM-Newton
V2487 Oph 1998: a puzzling recurrent nova observed with XMM-Newton Margarita Hernanz Institute of Space Sciences (CSIC-IEEC) - Barcelona (Spain) Gloria Sala (UPC-IEEC), Nataly Ospina (CSIC-IEEC) V2487
Extreme optical outbursts from a magnetar-like transient source: SWIFT J
Extreme optical outbursts from a magnetar-like transient source: SWIFT J1955+26 Gottfried Kanbach 1 Alexander Stefanescu 1,2 Agnieszka Słowikowska 3 Jochen Greiner 1 Sheila McBreen 4 Glòria Sala 5 1 Max-Planck-Institut
Gas 1: Molecular clouds
Gas 1: Molecular clouds > 4000 known with masses ~ 10 3 to 10 5 M T ~ 10 to 25 K (cold!); number density n > 10 9 gas particles m 3 Emission bands in IR, mm, radio regions from molecules comprising H,
Black Holes in Hibernation
Black Holes in Hibernation Black Holes in Hibernation Only about 1 in 100 galaxies contains an active nucleus. This however does not mean that most galaxies do no have SMBHs since activity also requires
The History of Active Galaxies A.Barger, P. Capak, L. Cowie, RFM, A. Steffen, and Y. Yang
The History of Active Galaxies A.Barger, P. Capak, L. Cowie, RFM, A. Steffen, and Y. Yang Active Galaxies (AKA quasars, Seyfert galaxies etc) are radiating massive black holes with L~10 8-10 14 L sun The
Active galactic nuclei (AGN)
Active galactic nuclei (AGN) General characteristics and types Supermassive blackholes (SMBHs) Accretion disks around SMBHs X-ray emission processes Jets and their interaction with ambient medium Radio
Part 2. Hot gas halos and SMBHs in optically faint ellipticals. Part 3. After Chandra?
Hot gas and AGN Feedback in Nearby Groups and Galaxies Part 1. Cool cores and outbursts from supermassive black holes in clusters, groups and normal galaxies Part 2. Hot gas halos and SMBHs in optically
Millisecond X-ray pulsars: 10 years of progress. Maurizio Falanga
Millisecond X-ray pulsars: 10 years of progress Maurizio Falanga History I Radio Astronomy in the 30 s-60 s Karl Jansky 1933 3C273 Discovery (1961-63) Quasi-Stellar Radio Sources as the most energetic
Accretion Disks. 1. Accretion Efficiency. 2. Eddington Luminosity. 3. Bondi-Hoyle Accretion. 4. Temperature profile and spectrum of accretion disk
Accretion Disks Accretion Disks 1. Accretion Efficiency 2. Eddington Luminosity 3. Bondi-Hoyle Accretion 4. Temperature profile and spectrum of accretion disk 5. Spectra of AGN 5.1 Continuum 5.2 Line Emission
(Anomalous) X-Ray Pulsars. Vicky Kaspi. Montreal, Canada. Stanford December 16, 2004
(Anomalous) X-Ray Pulsars Vicky Kaspi Montreal, Canada Texas @ Stanford December 16, 2004 Summary Introduction to AXPs Evidence that AXPs are magnetars Open Issues and Recent Results: IR emission Transient
The structure and evolution of stars. Learning Outcomes
The structure and evolution of stars Lecture14: Type Ia Supernovae The Extravagant Universe By R. Kirshner 1 Learning Outcomes In these final two lectures the student will learn about the following issues:
Probing 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
The impact of metallicity on the demographics of ULXs
1,2,3 Michela Mapelli 1 INAF, Padova Observatory MERAC prize 3 2012 FIRB fellow 2 2015 The impact of metallicity on the demographics of ULXs Collaborators: Mario Spera, Nicola Giacobbo, Elena Ambrosi,
Stellar Populations: Resolved vs. unresolved
Outline Stellar Populations: Resolved vs. unresolved Individual stars can be analyzed Applicable for Milky Way star clusters and the most nearby galaxies Integrated spectroscopy / photometry only The most
Gamma- ray emission from Microquasars
Gamma- ray emission from Microquasars S. Saba5ni (G. Piano) on behalf of the AGILE Team AGILE (in orbit since April 23, 2007) all sky map GRS 1915+105 Galactic Centre GRO 1655-40 Cyg X-3 Cyg X-1 SS 433
Dual and Binary MBHs and AGN: Connecting Dynamics and Accretion
Dual and Binary MBHs and AGN: Connecting Dynamics and Accretion Sandor Van Wassenhove Marta Volonteri Lucio Mayer Jillian Bellovary Massimo Dotti Simone Callegari BH-Galaxy Coevolution Black holes found
AGN 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;