X-RAY ASTRONOMY 2019 Report of Contributions https://indico.ict.inaf.it/e/XRAY2019 X-RAY ASTRON … / Report of Contributions Dissecting black hole-galaxy co- … Contribution ID: 2 Type: Contributed Dissecting black hole-galaxy co-evolution from de-biased scaling relations Thursday, 12 September 2019 09:15 (15 minutes) It has been claimed for decades that almost all galaxies in the local Universe host at their centre a super-massive black hole (SMBH) the mass of which appears to be tightly correlated with the stellar mass and the random motion (”velocity dispersion”, sigma) of the stars of the host galaxy. In this talk I will first highlight that significant biases affect local black hole-galaxy correlations. Iwill specifically show that the majority of quiescent early-type galaxies with central black holemass estimates have significantly higher velocity dispersions than local unbiased galaxies of similar stellar mass. Through aimed Monte-Carlo simulations, residual analysis, and the comparison with latest AGN clustering measurements, I will then illustrate that present data sets of active and quiescent galaxies strongly favour on average lower SMBH masses than previously thought, and point to velocity dispersion as more “fundamental” than galaxy stellar mass, galaxy size or Sersic index. I will then move on discussing the main implications of these findings, in particular: 1) The implied black hole radiative efficiencies and obscured fractions; 2) the consequences on feedback from active black holes and SMBH binary gravitational waves; 3) the connection to cosmological models that rely on velocity dispersion, rather than stellar mass, as main driver of black hole growth. Topic Active Galactic Nuclei: accretion physics and evolution across cosmic time Affiliation University of Southampton Primary author: Dr SHANKAR, Francesco (Southampton) Presenter: Dr SHANKAR, Francesco (Southampton) Session Classification: ACTIVE GALACTIC NUCLEI October 1, 2021 Page 1 X-RAY ASTRON … / Report of Contributions AstroSat observation of GX 5-1: S … Contribution ID: 3 Type: Poster AstroSat observation of GX 5-1: Spectral and timing evolution We report on the first analysis of AstroSat observation of the Z-source GX5- 1 on February 26-27, 2017. The hardness-intensity plot reveals that the source traced out the Horizontal and Normal branches. The 0.8-20 keV spectra from simultaneous SXT and LAXPC data at different locations of the hardness-intensity plot can be well described bya disk emission and a thermal Comptonized component. The ratio of the disk flux to the total i.e. the disk flux ratio increases monotonically along the horizontal to the Normal one.Thus, the difference between the Normal and Horizontal branches is that in the normal branch, the disk dominates the flux while in the horizontal one it is the Comptonized component which dominates. The disk flux scales with the inner disk temperature as T^5.5 andnotasT^4 , suggesting that either the inner radii changes dramatically or that the disk is irradiated by the thermal component changing its hardness factor. The power spectra reveal a Quasi Periodic Oscillation whose frequency changes from ∼ 30 Hz to 50 Hz. The frequency is found to correlate well with the disk flux ratio. In the 3-20 keV LAXPC band the r.m.s ofthe QPO increases with energy (r.m.s ∝ E^0.8 ), while the harder X-ray seems to lag the soft ones with a time-delay of a milliseconds. The results suggest that both the temporal and spectral properties of the source are determined by the geometry of the system which is characterized by the disk flux ratio and that the QPO has its origin in the corona producing the thermal Comptonized component. Topic Affiliation Pacific Academy of Higher Education and Research University, Udaipur Primary author: BHULLA, Yashpal (Pacific Academy of Higher Education and Research University, Udaipur) Presenter: BHULLA, Yashpal (Pacific Academy of Higher Education and Research University, Udaipur) Session Classification: POSTER SESSION October 1, 2021 Page 2 X-RAY ASTRON … / Report of Contributions XMM-Newton mission operations … Contribution ID: 4 Type: Poster XMM-Newton mission operations - preparing for the third decade Friday, 13 September 2019 20:10 (2 minutes) ESA’s X-ray flagship the XMM-Newton space observatory is soon entering it’s third decade ofop- erations. Both the spacecraft and the payload are operating without major degradation and scientific demand is continuously very high. Changing the on board Attitude and Orbit Control System Soft- ware in 2013 we managed to reduce the fuel consumption by a factor of two, additionally reducing stress on the reaction wheels. Currently the Flight Control team is preparing a new thermal oper- ations strategy of the tank system to ensure that the saved fuel is available for continuous usage. We will describe the status of implementation of the so called “fuel migration and replenishment” activities and make predictions how to operate the spacecraft with this concept potentially upto 2030+. Furthermore we describe the overall health status of the mission, the need for evolution of the ground segment and concepts on streamlining mission operations with continued high safety re- quirements using automation tools to keep the science return at the highest possible levels. Topic Affiliation ESA/ESOC Primary author: KIRSCH, Marcus (ESA/ESOC) Co-authors: Dr FINN, Timothy (Telespazio Vega); Mr V. KRUSENSTIERN, Nikolai (Telespazio Vega); Mr MAGUNIA, Arnfried (Terma); Mr MARTIN, Jim (ESA/ESOC); Mr PFEIL, Norbert (Terma); Mr SALT, David (Telespazio Vega); Mr WEBERT, Detlef (Telespazio Vega); Mr WEISSMANN, Uwe (Telespazio Vega); Mr TOMA, Liviu (Telespazio Vega); Mr BENSON, Ian (Serco) Presenter: KIRSCH, Marcus (ESA/ESOC) Session Classification: POSTER SESSION October 1, 2021 Page 3 X-RAY ASTRON … / Report of Contributions 20 Years XMM-Newton: Scientific … Contribution ID: 6 Type: Invited 20 Years XMM-Newton: Scientific Achievements and Perspectives Thursday, 12 September 2019 16:25 (25 minutes) With about 350 refereed papers published each year, XMM-Newton is one of the most successful scientific missions of ESA ever. The talk summarizes the status of the mission and introducesthe main performance indicators, which characterize the scientific impact of the mission. The talk gives then an overview of recent research highlights, which are indicative of the main develop- ments of current X-ray astronomy.Finally, the talk outlines possible research and observational challenges for XMM-Newton in the next decade. Topic Affiliation ESA / XMM-Newton Primary author: SCHARTEL, Norbert (ESA - ESAC) Presenter: SCHARTEL, Norbert (ESA - ESAC) Session Classification: FUTURE MISSIONS October 1, 2021 Page 4 X-RAY ASTRON … / Report of Contributions X-ray emissions from magnetic po … Contribution ID: 7 Type: Poster X-ray emissions from magnetic polar regions of neutron stars Friday, 13 September 2019 15:04 (2 minutes) Structures of X-ray emitting magnetic polar regions on neutron stars in X-ray pulsars are studied. It is shown that a thin, optically thick, radiation energy dominated, X-ray emitting polar cone appears in each of the polar regions. The height of the polar cone from the neutron star surface to a standing shock at the top has a large dependence on the accretion rate. When M_ ' 1016 g s−1, the height is a tenth as low as the neutron star radius. When M_ ' 1018 g s−1, the height is, however, about 10 times as large as the neutron star radius. Histories of the radiation energy carried with the matter flowing in the polar cone also largely varies with the accretion rate.When M_ is as low as 1016 g s−1, the energy is mostly radiated away behind the shock. However, when M_ is as large as 1018 g s−1 or larger, the energy gain due to the gravity of the neutron star exceeds the energy loss due to photon diffusion in the azimuthal direction of the cone, and a significant amount of energy is advected to the neutron star surface. Then, the radiation energy carried with theflow should accumulate there, and the radiation pressure should overcome the magnetic pressure which has been holding the flow within the cone. As a result, the matter should expand in the tangential direction along the neutron star surface, dragging the magnetic lines of force, and form a mound- like structure. The advected energy to the bottom of the cone should finally be radiated fromthe surface of the polar mound and the matter should be settled on the stellar surface there. Fromsuch configurations, we can expect an X-ray spectrum composed of a multi-color black-body spectrum from the polar cone region and a quasi-single black-body spectrum from the polar mound region. This spectral property agrees with observations. A fairly sharp pencil beam is expected together with a broad fan beam from the polar cone region, while a broad pencil beam from the polar mound region. With these X-ray beam properties, basic patterns in X-ray pulse profiles of X-ray pulsars can be explained too. Topic Affiliation ISAS, JAXA Primary author: Dr INOUE, Hajime (ISAS, JAXA) Presenter: Dr INOUE, Hajime (ISAS, JAXA) Session Classification: POSTER SESSION October 1, 2021 Page 5 X-RAY ASTRON … / Report of Contributions The X-ray view of the repeat … Contribution ID: 8 Type: Poster The X-ray view of the repeat changing-look AGN NGC 1566 Friday, 13 September 2019 18:26 (2 minutes) NGC 1566 is one of only a handful of AGN that have undergone more than one changing-look event, having changed from Sy 1.9 to Seyfert 1.2 and at least five times. The most recent event was in 2018, where the source increased in X-ray flux by a factor of ~70 and nearly three magnitudes in the UV in under 9 months, coinciding with the reappearance of strong broad lines in the optical spectra.