Department of Astronomy, University of Padova Department of Physics, University of Padova INAF-Astronomical Observatory of Padova Paola Mucciarelli In.

Slides:



Advertisements
Similar presentations
Proton Cyclotron Lines in Thermal Magnetar Spectra S. Zane, R. Turolla, L. Stella and A. Treves Mullard Space Science Laboratory UCL, University of Padova,
Advertisements

Ultraluminous X-ray sources (ULXs) are promising candidates for intermediate-mass black holes. Here we report about the Suzaku observation of two ULXs,
A Large Catalogue of Ultraluminous X-ray Source Candidates in Nearby Galaxies Madrid: 2010 DOM WALTON IoA, Cambridge, UK In collaboration with Jeanette.
Supernova Remnants and ULX bubbles Manfred Pakull, Fabien Grisé, C. Motch, R. Soria 0bservatoire Astronomique de Strasbourg SNR & PWN in the Chandra Era,
Deriving direct mass measurements of black holes in ULXs Jeanette Gladstone, T. Roberts, C. Copperwheat, A. Goulding, C. Heinke, A Swinbank, T. Cartwright,
Ultraluminous X-ray sources. Thurs 14th October 2010Tim Roberts - ULXs2 Ultraluminous X-ray sources (ULXs)  EINSTEIN (early `80s) - some galaxies dominated.
Ultraluminous X-ray sources: a mystery for modern X-ray astronomy Tim Roberts.
The Sharpest Spatial View of a Black Hole Accretion Flow from the Chandra X-ray Visionary Project Observation of the NGC 3115 Bondi Region Jimmy Irwin.
Chandra Observations of the Norma Region Bodaghee et al Search for new HMXBs and study hard X-ray populations Twenty-seven 20 ks pointings Red:
Sean Farrell XMM-Newton Survey Science Centre University of Leicester, UK In collaboration with… N. Webb, D. Barret, O. Godet & B. Plazolles – CESR, France.
Tidal Disruptions of Stars by Supermassive Black Holes Suvi Gezari (Caltech) Chris Martin & GALEX Team Bruno Milliard (GALEX) Stephane Basa (SNLS)
Supernova Remnants in the ChASeM33 X-ray Observations of M33 Knox Long, Bill Blair, Frank Winkler, Terry Gaetz, David Helfand, Jack Hughes, Kip Kuntz,
The Transient Universe: AY 250 Spring 2007 Existing Transient Surveys: High Energy II: X-ray Binaries Geoff Bower.
PX269 Galaxies Part 4: Galactic nuclei 4.1 Active galaxies.
The line-of-sight towards GRB at z = 2.66: Probing matter at stellar, galactic and intergalactic scales Palli Jakobsson Astronomical Observatory.
NASA's Chandra Sees Brightest Supernova Ever N. Smith et al. 2007, astro-ph/ v2.
Early Results from SWIFT's BAT AGN Survey: XMM Follow-up Observations for 22 BAT AGNs Lisa Winter Lisa Winter (Grad Student at UMD) Richard Mushotzky (GSFC),
The Ultra-luminous X-Ray Sources Near the Center of M82 NTHU 10/18/2007 Yi-Jung Yang.
Gemma Anderson ChIcAGO Chasing the Identification of ASCA Galactic Objects.
X-ray Binaries in Nearby Galaxies Vicky Kalogera Northwestern University Super Star Clusters Starburst galaxies Ultra-Luminous X-Ray Sources Elliptical.
Black holes: do they exist?
RXJ a soft X-ray excess in a low luminosity accreting pulsar La Palombara & Mereghetti astro-ph/
SSS in young stellar populations: progenitors of the “prompt” Sne Ia? Thomas Nelson NASA Goddard Space Flight Center University of Maryland – Baltimore.
X-ray Surveys with Space Observatory Khyung Hee University Kim MinBae Park Jisook.
BLACK HOLES: FROM STARS TO GALAXIES – ACROSS THE RANGE OF MASSES Felix Mirabel European Southern Observatory. Chile (on leave from CEA. France) In last.
Sean Farrell XMM-Newton Survey Science Centre University of Leicester, UK (soon to be University of Sydney, Australia) In collaboration with… D. Barret,
Probing AGN Outflows with Variability Smita Mathur Ohio State Collaborators: Yair Krongold, Fabrizio Nicastro, Anjali Gupta Nancy Brickhouse, Martin Elvis.
An X-ray view of the Nature of LINERs Omaira González-Martín Instituto de Astrofísica de Andalucía Cols: J. Masegosa (IAA, SPAIN) I. Márquez (IAA, SPAIN)
Hot gas in galaxy pairs Olga Melnyk. It is known that the dark matter is concentrated in individual haloes of galaxies and is located in the volume of.
A Neutron Star with a Massive Progenitor in the Star Cluster Westerlund 1 Michael Muno (UCLA/Hubble Fellow) J. S. Clark (Open U)R. de Grijs (U Sheffield)
Introduction - Aims 1948 X-ray sources XMM-Newton EPIC observations of the largest Local Group spiral galaxy M 31, taken between June 2006 and February.
ASTR 113 – 003 Spring 2006 Lecture 11 April 12, 2006 Review (Ch4-5): the Foundation Galaxy (Ch 25-27) Cosmology (Ch28-29) Introduction To Modern Astronomy.
A New Magnetar Candidate Located Outside the Galactic Plane? Joe Callingham | Sean Farrell | Bryan Gaensler | Geraint Lewis Sydney Institute for Astronomy.
Gamma-Ray Bursts observed by XMM-Newton Paul O’Brien X-ray and Observational Astronomy Group, University of Leicester Collaborators:- James Reeves, Darach.
Chandra Observation of the Failed Cluster Candidate K. Hayashida, H. Katayama (Osaka University), K. Mori (Penn State University), T.T. Takeuchi.
Growing black holes: from the first seeds to AGN Mar Mezcua Harvard-Smithsonian Center for Astrophysics T. Miyaji, F. Civano, G. Fabbiano, M. Karouzos,
Ultraluminous X-ray Sources Andrew King, University of Leicester ² L x (apparent) > erg s -1 = L Edd (10 M ¯ ) ² do ULXs contain intermediate—mass.
Quasars and Active Galactic Nuclei
Nebulae Associated with Ultraluminous X-ray Sources P. Abolmasov, Special Astrophysical Observatory.
Deep Chandra image in the Boötes Field Junxian Wang Johns Hopkins University.
Observations of Obscured Black Holes
Progenitor stars of supernovae Poonam Chandra Royal Military College of Canada.
X-ray study of a nearby nuclear X-ray study of a nearby nuclear starburst and a nearby AGN starburst and a nearby AGN Roberto Soria (UCL) Mat Page, Kinwah.
An XMM-Newton View of the Luminous X-ray Source Population of M101 Leigh Jenkins Tim Roberts, Robert Warwick, Roy Kilgard*, Martin Ward University of Leicester,
Observational Evidence for Quasi-soft X-Ray Sources in Nearby Galaxies and the link to Intermediate-mass Black Holes Albert Kong and Rosanne Di Stefano.
The relation between the galaxy stellar mass distribution and the mass of its hosting halo BENEDETTA VULCANI KAVLI IPMU What Regulates Galaxy Evolution?
Optical counterparts to Ultraluminous X-ray sources Jeanette Gladstone - University of Alberta T. P. Roberts (U of Durham), A. D. Goulding (CfA) T. Cartwright.
Metal abundance evolution in distant galaxy clusters observed by XMM-Newton Alessandro Baldi Astronomy Dept. - University of Bologna INAF - OABO In collaboration.
The dependence on redshift of quasar black hole masses from the SLOAN survey R. Decarli Università dell’Insubria, Como, Italy A. Treves Università dell’Insubria,
Finding Black Hole Systems in Nearby Galaxies With Simbol-X Paul Gorenstein Harvard-Smithsonian Center for Astrophysics.
The X-ray source population studies in nearby galaxies Wolfgang Pietsch Max Planck Institut für extraterrestrische Physik.
BH Astrophys. Ch4 Intermediate Mass Black Holes. Outline 1. The definition Possible candidates: 2. ULXs (Ultra-luminous X-ray sources) in star-forming.
Accretion #3 When is the thin disk model valid? Reynolds number, viscosity Time scales in disk BH spectra Using X-ray spectra to determine BH mass and.
goals  Observe distorted galaxies using advanced techmaun telescopes  Determine possible galaxy type  Determine possible causes for the distortions.
J. Miguel Mas Hesse Elena Jiménez Bailón María de Santos Luis Colina Rosa González-Delgado When UV meets IR. Moriond 2005.
Ultra-luminous X-ray sources Roberto Soria (University College London) M. Cropper, C. Motch, R. Mushotzky, M. Pakull, K. Wu.
eXTP Workshop Timing Ultraluminous X-ray Sources with eXTP
Quasars: old black holes with young stars (?)
Evidence for an Intermediate Mass Black Hole in NGC 5408 X-1
Dynamical constraints on the mass of the black hole in a ULX
Quasars, Active Galaxies, and super-massive black holes
XMM-NEWTON reveals a dipping black-hole X-ray binary in NGC 55
Paola Rodriguez Hidalgo High Energy Astrophysics
Analysis of Off-Nuclear X-Ray Sources in Galaxy NGC 4945
Supersoft X-ray sources in M31
Suzaku discovery of a transient ultra-luminous X-ray source,
Uncloaking globular clusters of the inner Galaxy
The X-ray Morphology and Spectra of Galactic Disks
Suzaku Observation of Two Ultraluminous X-Ray Sources in NGC1313
Constraining IMBH masses with VLBI
Presentation transcript:

Department of Astronomy, University of Padova Department of Physics, University of Padova INAF-Astronomical Observatory of Padova Paola Mucciarelli In collaboration with: Zampieri, Turolla, Treves, Falomo, Chieregato, Kaaret & di Stefano. The UltraLuminous X-ray source NGC 1313 X-2

NGC1313 X-2: X-ray properties  NGC1313 is a nearby spiral galaxy hosting two ULXs, NGC1313 X-1 and X-2, and the interacting supernova 1978K.  NGC1313 X-2 is a well known ULX, variable on a timescale of months.  Assuming that at maximum the source radiates at the Eddington limit, a mass of 50 M  is derived for the compact remnant. NGC1313 X-2 NGC1313 X-1 MODEST-6, August 29-31, 2005 ♣The XMM spectrum shows statistical evidence for a MCD component with kT=0.2 keV (Miller et al. 2003,Zampieri et al. 2004) M BH ~ 90f 4 M 

NGC1313 X-2: optical counterpart NGC 1313 X-2 optical counterpart was identified in an ESO 3.6m R band image, using the Chandra position with an uncertainty of 0.7  (Zampieri et al., 2004). In archive ESO VLT (BVR) band images the counterpart is resolved in two distinct point-like sources, C1 and C2, separated by 0.7”(Mucciarelli et al., in prep.). Taking into account Galactic absorption: C1: R=23.5, (B-V) 0 =-0.2 (V-R) 0 =-0.2 C2: R=23.4, (B-V) 0 >1.0 (V-R) 0 =0.4 (R-I) 0 =0.2 (from Liu et al. 2005) MODEST-6, August 29-31, 2005 Both object are nor an AGN (absence of redshifted emission lines and very high f X /f R ) neither foreground stars. C1: BO-O9 main sequence star of 20M  in NGC 1313 C2: G supergiant of about 10M  in NGC 1313

Conclusions MODEST-6, August 29-31, 2005 Two optical counterparts are detected (on VLT images) inside the Chandra error box of the ULX NGC 1313 X-2. Irrespectively of wich of the two objects is the actual counterpart, NGC 1313 X-2 appears to be a high mass X-ray binary with a massive donor star. At the present stage, there seems to be no compelling argument to rule out any of the two object C1 and C2 as possible counterpart. Follow up optical spectroscopy under optimal seeing conditions and with the slit along the line of conjunction C1-C2 is crucial to disentangle the emission from the two objects. Theoretical modelling may also help to distinguish the counterpart (Patruno & Zampieri, in prep.)