De canon "Vijftig jaar Nederlands ruimteonderzoek" is opgesteld in 2012.

On this page, the PDF versions of the slides presented at the conference are published. Click on the link to open the file. The presentations are sorted in the order in which they have been presented. The third column indicates Invited reviews (I), Sollicited talks (S), or Contributed talks (C).

History

Frank Verbunt The Netherlands I History of X-ray spectroscopy in Utrecht

 

 

 

 

Present and future instrumentation

Frits Paerels USA I X-ray gratings
Jan-Willem den Herder The Netherlands I Calorimeters
Takaya Ohashi Japan I Future X-ray missions
Michael Shull USA I The Cosmic Origins Spectrograph: first results

 

 

 

 

Abundances in X-ray plasmas

Paola Testa USA I Abundances in stars
Carles Badenes USA I Abundances in supernova remnants
Norbert Werner USA I Abundances in clusters of galaxies
Yan Grange The Netherlands C Metal abundances of NGC 5044, NGC 5813 and Abell 2052
Stefano Ettori Italy C The ICM metallicity from z=0 to z=1.3: the observations & a model
Richard Mushotzky USA I Abundances in galaxies
Ciro Pinto The Netherlands S High-resolution X-ray spectroscopy of the interstellar medium

 

 

 

 

Atom-atom interactions as seen through X-rays

Konrad Dennerl Germany I Charge transfer reactions
Graziella Branduardi-Raymont UK S X-ray views of Jupiter
S. Gwynne Crowder USA C A High Resolution Spectrum of the Diffuse Soft X-ray Background from 0.1 to 1 keV
Cor de Vries The Netherlands S Observing the structure of solid interstellar particles in the line of sight towards Sco-X1
Julia Lee USA I X-ray spectroscopy of dust

 

 

 

 

He-like triplet diagnostics

Delphine Porquet France I He-like triplet diagnostics
Matteo Guainazzi Spain S AGN/starburst connection in action: the half million second RGS spectrum of NGC 1365
Hans Moritz Guenther Germany C When does accretion cease?
Piero Ranalli Italy C X-ray gaseous emission in star forming galaxies
Anna Lia Longinotti USA C Warm absorber and warm emitter in AGNs: clues from X-ray spectroscopy

 

 

 

 

Laboratory plasmas and models

Randall Smith USA I Plasma emission codes and atomic data
Peter Beiersdorfer USA I Laboratory experiments
Jose Crespo Lopez-Urrutia Germany S Photoionization measurements of Fe and Ar highly charged ions in the keV regime
Stefan Schippers Germany C Laboratory measurements of rate coefficients for dielectronic recombination and electron-impact ionization of highly charged atomic ions

 

 

 

 

X-ray spectroscopy and gravity fields

Jon Miller USA I Strong gravity: relativistic oxygen and iron lines in AGN & binaries
Oliwia Madej The Netherlands C Search for reflection features in the high-resolution spectra of ultra-compact X-ray binaries
Maria Diaz Trigo Spain C A systematic analysis of the broad Fe K alpha line in neutron star LMXBs with XMM-Newton
Manabu Ishida Japan I Non-relativistic strong gravity: accreting white dwarfs

 

 

 

 

Plasmas with finite optical depth

Wolfgang Pietsch Germany C High time and spectral resolution observations of the supersoft X-ray emission of the optical nova LMC 2009
Jan-Uwe Ness Spain C Expanding X-ray Atmospheres
Andy Fabian UK I Reflection and fluorescence on cold material
Alexander Blustin UK S Disc reflection at high resolution: the X-ray broad-line region
Jose Miguel Torrejon Spain C A Chandra Survey of fluorescence Fe lines in X-ray Binaries at high resolution
Tim Kallman USA I Photoionised plasmas
Eleonora Torresi Italy C Warm absorbers in AGN with powerful jets
Eugene Churazov Russia I X-ray resonance scattering in cosmic plasmas
David Cohen USA S Line Shapes in Hot Stars
Maurice Leutenegger USA C X-ray radiative transfer in massive star winds

 

 

 

 

Kinematics and shock diagnostics

Manuel Guedel Switzerland I Kinematics of hot and cool stars
Jacco Vink The Netherlands I Plasma equilibration and shocks
Dan Dewey USA I Kinematics of supernova remnants
Hiroya Yamaguchi Japan C Discovery of recombining plasmas in mixed-morphology SNRs: recent Suzaku spectroscopy and future prospects
Frank Haberl Germany C Spectral evolution of SN 1987A as seen with XMM-Newton
Ehud Behar Israel I Kinematics of AGN outflows
Shai Kaspi Israel C Massive outflows in AGN's X-ray spectra

 

 

 

 

The UV- X-ray connection

Elisa Costantini The Netherlands I The UV-X-ray connection in AGN outflows
Nahum Arav USA S High-resolution X-ray spectroscopy and the study of AGN Warm absorbers
Rob Detmers The Netherlands C Unravelling the inner region of an AGN: The 600 ks RGS spectrum of Mrk 509
Gerard Kriss USA C Coordinated HST/COS and X-ray Observations of Mrk 509
Joel Bregman USA I The UV-X-ray connection in the ISM and WHIM
Q. Daniel Wang USA S X-raying the Hot Interstellar and Circum-galactic Media

Below, we list all the posters presented at the conference. Click on the link to find the PDF or JPG version of the poster.

Session 1. Present and future instrumentation

1.01 Yoh Takei Japan The X-ray microcalorimeter SXS on board Astro-H
1.02 Herman Marshall USA Adapting an IXO Grating Spectrometer for Polarimetry
1.03 Randall McEntaffer USA Soft X-ray spectroscopy simulations for the IXO OP-XGS
1.04 Norbert Schartel Spain A completely different view of RGS observations: A trial to estimate the intrinsic discovery space
1.05 Ton Raassen The Netherlands Investigation of the line spread function (LSF) of RGS
1.06 Aitor Ibarra Spain SAS methods for stacking RGS spectra
1.07 Daniel Dewey USA High-resolution Soft X-ray Spectroscopy on IXO using a Critical-Angle Transmission Grating

Session 2. Abundances in X-ray plasmas

2.01 Lorenzo Lovisari Austria Metallicity maps: X-ray observations versus simulations
2.03 Marina Orio Italy & USA The surprising X-ray spectra of classical and recurrent novae in outburst
2.04 Jan Robrade Germany Neon and oxygen in low activity stars: towards a coronal unification with the Sun

Session 3. Atom-atom interactions as seen through X-rays

3.01 Hiroshi Yoshitake Japan Long-term variations of Solar Wind Charge Exchange induced X-ray emission with Suzaku
3.02 P.C. Schneider Germany X-raying the AU Microscopii debris disk

Session 4. He-like triplet diagnostics

4.01 Dimitra Koutroumpa USA Thermal Emission or Charge Exchange from the North Polar Spur?
4.02 O. Gonzalez-Martin Greece Diagnosis on the soft X-ray emission of LINER nuclei using RGS/XMM-Newton spectra
4.03 Joy Nichols USA Chandra HETG Analysis of Theta 2 Ori A

Session 5. Laboratory plasmas and models

5.01 Jaan Lepson USA Laboratory measurements of density-sensitive lines of Fe XXII
5.02 Daniel Wolf Savin USA Collisional Ionization Equilibrium for Optically Thin Plasmas
5.03 L. Natarajan India Radiative de-excitation of 2s2p configuration of He-like ions
5.04 Sripathi Punchithaya India K-Shell Fluorescence Yields of Low, Medium and High Z Elements
5.05 Manuel Bautista USA Photoionization and photoabsorption of neutral iron
5.06 Patrick Palmeri Belgium Atomic Decay Data for Modeling the Al K Lines
5.07 Michael Witthoeft USA K-shell photoionization calculations using R-matrix
5.08 Claudio Mendoza Venezuela XSTAR: application deployment in the global cyber-infrastructure
5.09 Li Ji USA Implementation of the Non-equilibrium Ionization Code in ISIS
5.10 Giulio Del Zanna UK Atomic data for X-ray plasma modeling - recent advances

Session 6. X-ray spectroscopy and gravity fields

6.04 Takehiro Miyakawa Japan X-ray emission and absorption environments in Seyfert 1 galaxy MCG-6-30-15
6.05 Jiri Svoboda Czech Republic Warm absorber and truncated accretion disc in IRAS 05078+1626
6.07 G. B. Zhang The Netherlands Using the quiescent spectrum to constrain the distance to the low-mass X-ray binary EXO 0748-676
6.08 Osamu Nagae Japan Detection of redshifted X-ray emission lines in the neutron star X-ray binary 4U 1700+24
6.09 Ivica Miskovicova Germany Spectroscopy of the stellar wind in the Cyg X-1 system
6.10 Iris Traulsen Germany Accretion flows onto highly magnetic white dwarfs - Diagnostic potential of high-resolution X-ray spectroscopy

Session 7. Plasmas with finite optical depth

7.01 Jacobo Ebrero The Netherlands A close look into the warm absorber in Mrk 509: a 180 ks Chandra LETGS observation
7.02 Javier Garcia USA New Models for Disk Reflection and Reprocessing Spectra
7.03 Missagh Mehdipour UK The warm absorber and X-ray variability of NGC 3516
7.04 Stefano Bianchi Italy The soft X-ray emission in obscured AGN: more than a pure photoionised plasma?
7.05 Tomer Holczer Israel X-Ray Spectroscopy of AGN Outflows: The Absorption Measure Distribution
7.07 Irina Zhuravleva Germany Polarization of X-ray lines from galaxy clusters - a way to measure tangential gas motions
7.08 Hirokazu Odaka Japan Monte Carlo simulations of X-ray reflection nebulae in the Galactic Center region for future high-resolution imaging spectroscopy
7.09 Agata Rozanska Poland Photoionization modeling with TITAN code

Session 8. Kinematics and shock diagnostics

8.01 Midori Ozawa Japan Suzaku discovery of strong recombination structures from the SNR
8.02 Daria Kosenko The Netherlands X-ray spectroscopy of supernova remnants in LMC
8.03 Asami Hayato Japan Doppler broadened X-ray Emission Lines in Tycho's Supernova Remnant
8.04 Jose Ramirez Germany Chandra LETGS observation of the variable NLS1 galaxy Ark 564 I.
8.05 Andrew Lobban UK Deep High-Resolution Chandra HETG Spectroscopy of the Outflow in NGC 4051
8.06 Rob Detmers The Netherlands Probing the Seyfert 1 X-ray narrow line region geometry with variability: Ionized outflows in emission?
8.07 Katrien Steenbrugge UK Cygnus A: a case for spatially resolved high resolution X-ray spectroscopy
8.08 Anthony Herve Belgium Comparison of two models of wind fragmentation and consequences on the emergent X-ray spectra
8.09 Gregor Rauw Belgium A close look at the RGS spectra of the O4Ief star zeta Pup

Session 9. The UV- X-ray connection

9.01 Jacobo Ebrero The Netherlands A global view of the absorption/emission processes in a Seyfert 1 galaxy: the case of Mrk 279
9.03 Missagh Mehdipour UK Mrk 509 as seen by the XMM-Newton Optical Monitor

 

If your presentation is larger than 10 MB, then please use the upload facility below to send us your file.

Important:

Please change the name of the file to something we can recognize and is unique to you, e.g. your name. For example: jdeplaa.pdf 

Please send us an email that you uploaded the file and indicate what we should check (mail to: This email address is being protected from spambots. You need JavaScript enabled to view it.).

 

The invited reviews presented at this conference are planned to be published by Springer as a 'topical volume' of Space Science Reviews. There will also be a spin-off hardcover book. The papers will be refereed. Editors are Jelle Kaastra and Frits Paerels.

Instructions for authors

  • The expected number of pages per paper is about 20. There is no strict min/max number of pages, but we aim for a balanced review of the field.
  • Color images/graphs are allowed for 2 pages per paper (because of costs).
  • Please see "For authors and editors" at Space Science Reviews. You can find there the LaTeX macro package to be used and additional info on formatting your paper.
  • The submission site is here. If you are a new author for Space Sciecnce Reviews, please click the 'Register' button, otherwise the 'Login' button. After login select 'Submit New Manuscript' and select 'Vol xxx: X-ray Spectroscopy' from the list of article types.
  • When your paper has been accepted for publication, you (and the editors) will receive proofs within a few weeks. Once the proofs are accepted, your paper will be made publicly available with a doi number on SpringerLink under 'Online First'.
  • Submission deadline is

    July 1st 2010

    .

Since the program is full, we will instruct the chairs of the sessions to be strictly controlling the speaking time. Please keep in mind the following times for your talk:

Invited talk (30 min) = 25 min talk + 5 min discussion
Invited talk (20 min) = 17 min talk + 3 min discussion
Sollicited talk (15 min) = 12 min talk + 3 min discussion
Contributed talk (15 min) = 12 min talk + 3 min discussion

Please note that your effective speaking time is less than the total time mentioned in the program. If you take more time, this time will be subtracted from the time for questions and discussion. The total time of your talk (talk + discussion) should not take longer than the time listed in the program.

Technical instructions (IMPORTANT)

At the conference, one laptop will be available for the oral presentations. It is a Macbook with the following presentation software:

  • Adobe Acrobat Reader (PDF)
  • iWorks keynote '09
  • MS Powerpoint 2008
  • OpenOffice.org 3.2
The presentations will be published on the conference web site after the meeting. Therefore, we prefer that you convert your presentation to PDF beforehand. We strongly recommend that you use the conference laptop for your presentation.

Testing presentations

Upload and test your presentation in the break before the session starts or upload your talk before the conference starts so that we can test your talk beforehand. The login details for the upload facility on the conference web site will be sent to you by email.

If you have special requests, like showing movies, then please notify us before March 8th, well in advance through This email address is being protected from spambots. You need JavaScript enabled to view it.. We will test your movie on the hardware available at the conference location and make sure it will work. Please note that the sound of the movie cannot be put on the speakers.

Own laptop

The use of your own laptop for your presentation is strongly discouraged. The projection system consists of a beamer and several TV screens, which may cause problems when used with your own laptop. Time lost due to switching laptops and subsequent technical problems with your own hardware will not be compensated.

Contrast

The lecture hall is a very impressive historic location, but unfortunately there are also large windows which make it impossible to make the room dark. The beamer setup consists of a large projection screen near the speaker and several television screens at both sides of the room. The contrast of the television screens is very good. However, if the weather is sunny, then the contrast on the big screen may diminish. Please make sure that your slides have sufficient contrast! Use contrasting colours for your text on the slides and make sure the line width of your plots is sufficiently large to make the information visible for everyone.



SCROLL TO TOP