14.02.2022

Dr. Karina Voggel

Relic Nuclear Star Clusters and their hidden Super-Massive Black Holes.

I will summarize the current state of the field of surviving nuclear star clusters and what the future holds for these objects with the advent of large surveys such as Euclid. These former Nuclear Star Clusters (NSCs) end up in the halos of massive galaxies when they are stripped of their surrounding stars by tidal forces. Many of these former nuclei contain "hidden" SMBHs, a signpost of their past in the centers of a large galaxy. I will show how can can identify surviving nuclei and use them to trace galaxy and SMBH formation. I will in particular show NGC7727, a system that has two potential nuclear star clusters, one in the photometric center of the galaxy and one offset by only 500pc. Using high-resolution MUSE data, we detect a SMBH in each Nucleus, confirming that the offset nucleus is the relic of a galaxy that has merged with NGC7727. This is the first dynamically confirmed dual SMBH system at a separation of less than a kpc. The orbital parameters of the SMBHs show that it is in an advanced state of merging and it will constitute a ~1:25 mass ratio SMBH merger and produce a gravitational wave event. The discovery of this offset SMBH is another confirmation that many SMBHs exist outside the centers of galaxies that have not been discovered yet but are a crucial element for our understanding of black holes as well as galaxy assembly.

21.03.2022

Emily Moravec

Do Radio Active Galactic Nuclei Reflect X-ray Binary Spectral States?

Over recent years there has been mounting evidence that accreting supermassive black holes in active galactic nuclei (AGNs) and stellar mass black holes have similar observational signatures. Further, there have been investigations into whether or not AGNs have spectral states similar to those of X-ray binaries (XRBs) and what parallels can be drawn between the two using a hardness-intensity diagram (HID). To address whether AGN jets might be related to accretion states as in XRBs, I will present the results of recently published work where we explore whether populations of radio AGNs classified according to their (a) radio jet morphology, Fanaroff-Riley classes I and II, (b) excitation class, high- and low- excitation radio galaxies, and (c) radio jet linear extent, compact to giant, occupy different and distinct regions of the AGN HID.

04.04.2022

Samuel Barnier

A spectral model of accretion ejection: the JED-SAD model applied to X-ray binaries and AGN

I will present the JED-SAD model, a spectral model stemming from self-similar magnetized accretion ejection solutions around black holes. In the JED-SAD model, the inner region is an inner Jet Emitting Disk (JED, Ferreira 1997), playing the role of the hot corona, and the outer region is a Standard Accretion Disk (SAD, Shakura & Sunyaev 1973). The JED-SAD can explain both the spectral evolution of the disk and dynamical evolution from the jet observed during X-ray binaries outbursts. I built spectral tables of the JED-SAD model and will present their application to both X-ray binaries observations and the non-linear correlation between the UV and Xray observed in AGN samples.

11.04.2022

Adam Ingram

Measuring black hole mass and the expansion rate of the Universe with X-ray reverberation mapping

Stellar-mass black holes accreting gas from a binary partner (X-ray binaries) and supermassive black holes accreting gas from their host galaxy (active galactic nuclei, AGN) can emit a huge X-ray flux from the vicinity of the black hole event horizon. This can be exploited to probe the strong field regime of General Relativity and measure the properties of the black hole: its mass and angular momentum. For all but two objects in the Universe, the vicinity of the accreting BH is far too small to directly image, necessitating the use of mapping techniques that exploit rapid X-ray variability. I will talk about X-ray reverberation mapping, which utilises the relativistically broadened iron emission line that results from centrally emitted X-rays reflecting from the disk. Modelling the light-crossing delay between reflected and directly observed X-rays returns a black hole mass measurement. I will summarise our efforts to measure the mass of stellar and supermassive black holes with our X-ray reverberation mapping code RELTRANS, including our first proof-of-principle constraint on Cygnus X-1. I will then describe how we can use RELTRANS for an even more ambitious goal: measuring the Hubble constant, H0. This is possible because the shape of the reflection spectrum depends on the intensity of illuminating flux, meaning that modelling with RELTRANS can effectively turn bright nearby AGN into standard candles. New, independent methods to measure H0 are currently highly desirable because modelling of the cosmic microwave background returns an H0 value in >4 sigma tension with the value derived from the traditional distance ladder. I will show that the statistical precision required to prefer one of these two discrepant values is achievable with a sample of ~25 AGN. I will discuss the improvements to our model that are required to achieve such a measurement in reality.

12.05.2022

Vladimír Karas (ASU), Michael Prouza (FZU), Miroslav Hrabovský (UP) a kol.

Demonstration of two newly installed Cherenkov telescopes at the observatory in Ondřejov

This is the first and in a way unique installation of Cherenkov high-energy gamma imaging telescopes in the Czech Republic. Two instruments are among the largest telescopes in our country. They are characterized, among other things, by the ability of a simultaneous stereoscopic observation mode. The primary goal is the technical verification. Further, the science program will address a range of fundamental questions about the Universe: how do the most powerful cosmic accelerators work? What is the essence of cosmic rays and dark energy? What is the role of black holes? The meeting will take place at the observatory in Ondřejov on Thursday, 12 May 2022 from 10:00am.

19.05.2022

Maitrayee Gupta

Comparing radio-loud Swift/BAT AGN with their radio-quiet counterparts

Some AGN are known to be efficient producers of strong, relativistic jets that power extended radio sources. Most spectacular with respect to power and size are the radio sources associated with AGN hosted by giant elliptical galaxies. However, even among them, the production of powerful jets is a very rare phenomenon and the question of why it is so remains unanswered. Since relativistic jets are most likely powered by rotating BHs via the Blandford-Znajek mechanism, one might expect that the parameters key to determining efficient jet production would be BH spins and magnetic fluxes. If their values are large, then the innermost portions of accretion flow should be affected by the jet production, and this should be imprinted in their radiative properties. In order to verify whether this is the case, we compare the radiative properties of radio-loud (RL) and radio-quiet (RQ) AGN selected from the Swift/BAT catalog with similar BH masses and Eddington ratios. As we have found, the only significant difference concerns the hard X-ray luminosities, which are about two times larger in RL AGN than in RQ AGN. One might speculate that this difference comes from RL AGN having X-ray contributions not only from the innermost, hot portions of the accretion flow but also from a jet. However, this interpretation is challenged by our following findings: (1) hard X-ray spectra of RL AGN have similar slopes and high-energy breaks to those of RQ AGN; (2) hard X-ray radiation is quasi-isotropic in both RQ and RL AGN. Hence, we argue that the production of hard X-rays in the RL AGN is like that in the RQ AGN: dominated by hot, central portions of accretion flows, while larger X-ray production efficiencies in RL AGN can be associated with larger magnetic fields and faster rotating BHs in these objects.

31.05.2022

Roberto Taverna on behalf of the IXPE team and its Magnetars Topical Working Group

Detection of polarized X-ray emission from the magnetar 4U 0142+61

Soft gamma repeaters and anomalous X-ray pulsars are believed to host a magnetar, an ultra-magnetized neutron star with surface magnetic field B ~ 10^14-10^15 G. We report on the first detection of linearly polarized X-ray emission from a magnetar with the Imaging X-ray Polarimetry Explorer (IXPE). The IXPE observation of the anomalous X-ray pulsar 4U 0142+61 reveals a linear polarization degree of (12±1)% throughout the instrumental working energy band 2-8 keV at 15σ confidence level. The IXPE measurement demonstrates the power of X-ray polarimetry, giving us completely new information about the properties of the neutron star surface and magnetosphere and lending further support for the presence of the quantum mechanical effect of vacuum birefringence.

09.06.2022

Victoria Grinberg

X-raying the winds of massive stars using high mass X-ray binaries

We are made of stardust—or, at least in significant parts, of material processed in stars. Hot, massive giant stars can drive the chemical evolution of galaxies and trigger and quench star formation through their strong winds and their final demise as supernovae. Yet optical and X-ray measurements of the wind mass loss strongly disagree and can only be reconciled if the winds are highly structured, with colder, dense clumps embedded in a tenuous hot gas. In (quasi-)single stars, however, wind properties are inferred for the whole wind ensemble only; no measurements of individual clumps or clump groups are possible, limiting our understanding of wind properties. Luckily, nature provides us with perfect laboratories to study clumpy winds: high mass X-ray binaries. The radiation from close to the compact object is quasi-point like and effectively X-rays the wind, in particular the clumps crossing our line of sight. In this talk, I will show how we can use a variety of observations of some of the brightest X-ray binaries to constrain wind properties. Low resolution, high cadence observations combined with simulations reveal the dynamics of clump movements and the large-scale wind structure. Time- and absorption-resolved high resolution X-ray spectroscopy reveals the composition of the multicomponent wind plasma, the layered temperature profile and comet-like structure of clumps. Future X-ray telescopes such as XRISM and Athena will revolutionise the field, allowing us to observe individual clumps in bright sources and, for the first time, make faint sources accessible for high resolution spectroscopy. This will provide us with a sample of HMXBs that will allow us to compare wind properties in massive stars of different stellar (sub-)types and at different radii, thereby directly testing theories of clumpy wind formation and evolution.

10.06.2022

Sumanta Chakraborty

Probing gravity and matter through gravitational waves

In this talk, I will discuss how theories beyond general relativity, as well as exotic matter contents, provide testable predictions for the gravitational waves. How tidal effects in the inspiral regime, and the quasi-normal modes during ringdown, are affected by such non-trivial modifications will be presented. The consequences of putative quantum effects near the horizon will also be discussed.

13.06.2022

Teo Muñoz-Darias

Accretion and outflows in stellar-mass black holes

Black-hole (BH) transients are a type of X-ray binary in which a stellar-mass BH accretes material from a low-mass star via an accretion disc. They spend most part of their lives in a dim, quiescent state, but display powerful outbursts when their luminosity increases by up to seven orders of magnitude in all wavelengths. X-ray and radio observations performed during the last couple of decades have provided a rich data base on BH transients. A strong coupling between the properties of the accretion flow and the presence of outflows, such as radio-jets and hot X-ray winds, has been found to be a fundamental characteristic of these systems, and, to a great extend, of X-ray binaries in general. In addition to this, and particularly since the spectacular case of the 2015 outburst of the BH transient V404 Cygni, cold (optical/infrared) accretion disc winds have been discovered in several systems, with observables indicating that they also have a significant impact on the entire BH accretion process. I will review the state-of-the-art of this field, with emphasis on the studies that we are currently carrying out on these novel cold winds with a suite of the largest telescopes.

16.06.2022

Juan Antonio Fernández-Ontiveros

X-ray binary accretion states in AGN? Sensing the accretion disc of supermassive black holes with mid-IR nebular lines

Accretion states, which are universally observed in stellar-mass black holes in X-ray binaries, are also anticipated in active galactic nuclei (AGN). This is the case at low luminosities, when the jet-corona coupling dominates the energy output in both populations. Previous attempts to extend this framework to a wider AGN population have been extremely challenging due to heavy hydrogen absorption of the accretion disc continuum and starlight contamination from the host galaxies. The luminosity-excitation diagram (LED), based on the [OIV]25.9µm and [NeII]12.8µm mid-IR nebular line fluxes, enables to probe the accretion disc contribution to the ionising continuum. When applied to a sample of 167 nearby AGN, the LED recovers the characteristic q-shaped morphology outlined by individual X-ray binaries during a typical accretion episode, allowing us to tentatively identify the main accretion states in supermassive black holes. The soft state would include broad-line Seyferts and about half of the Seyfert 2 population, showing highly excited gas and radio-quiet cores consistent with disc-dominated nuclei. The hard state mostly includes low-luminosity AGN (<10^-3 Ledd) characterised by low-excitation radio-loud nuclei and a negligible disc contribution. The remaining half of Seyfert 2 nuclei and the bright LINERs show low excitation at high accretion luminosities, and could be identified with the bright-hard and intermediate states. The hosts of hard-state AGN are mostly passive galaxies, whereas intermediate-state AGN exhibit substantial star formation activity in their central kiloparsecs. I will discuss the above scenario, its potential links with the galaxy evolution picture, and the possible presence of accretion state transitions in AGN, as suggested by the growing population of changing-look quasars.

03.08.2022

Konstantinos Kouroumpatzakis

Star-formation rates in galaxies and their correlation with X-ray emission

The star-formation rate (SFR) is a fundamental characteristic of galaxies which is strongly linked with their evolution and current state. Therefore, acquiring accurate measurements of the SFR is essential for galaxy studies. I will present a study of different SFR indicators, focusing on Hα emission, and its comparison with other SFR tracers based on ultraviolet, infrared (IR), radio emission, and spectral energy distribution (SED) fits. I will present Hα photometry and provide calibrations of Hα-based SFRs for the Star-Formation Reference Survey (SFRS), a representative sample of star-forming galaxies in the local Universe. This study also explores the effect of extinction corrections based on the Balmer decrement, infrared excess (IRX), and SEDs fits, as well as, corrections for the contribution of the adjacent-to-Hα [N II] emission lines. Moreover, for a subset of the SFRS sample with good quality X-ray data, the connection between SFR and X-ray luminosity (LX) originating from X-ray binaries (XRBs) is explored in sub-galactic scales. There is good agreement with established LX-–SFR relations down to SFR = 0.01 Msol/yr, below which an excess in X-ray luminosity emerges which likely arises from low-mass X-ray binaries. The SFR derived from Hα shows the tightest correlation with X-ray luminosity because Hα emission probes stellar populations with ages similar to HMXB formation timescales. In order to explore the effect of metallicity on the LX--SFR relation, I present a systematic study of the metallicity variations within the collisional ring galaxy NGC 922, based on long-slit spectroscopic, X-ray, and IR observations. NGC 922 shows a strong metallicity difference between star-forming regions in the bulge and the ring, with metallicities ranging from almost solar to significantly sub-solar ([12 + log(O/H)]=8.2). Additional, it is shown for the first time within a single galaxy, that there is an anti-correlation between the X-ray luminosity and metallicity of the sub-galactic regions of NGC 922.The different regions have similar stellar population ages leaving metallicity as the main driver of the anti-correlation.

08.08.2022

Guillermo Tenorio Tagle

The Formation of Globular Clusters

Globular Clusters are among the most astonishing manifestations of star formation in galaxies. The Milky Way has around 200 of these compact (a few parsecs across) and massive (up to several million stars) orbiting the galaxy. During the last 25 years they have evolved from being one of the most boring Astronomical subjects to become the most astonishing and more brains demanding field in stellar Astrophysics. All of this just because instead of making possible to study them as simple stellar populations, the discovery has been that each globular cluster present several stellar generations. Furthermore, the multiple generations have being found to be self-polluted, with the youngest populations carrying in their atmospheres traces of elements processed by former or older generations. So the main questions now are: how can stars form in places already occupied by a massive and compact stellar generation? How is it possible to reach star formation again despite the mechanical feedback from the older generation? I shall review some of the main ideas that have been postulated as possible solutions and what is that we find wrong with them. I shall also go through the possibility of star formation at very high densities, indicating the limits posed by theory and by the observations, on the power of the strong winds from massive stars. I shall look for models that care in particular about the resultant metallicity, which can only be enhanced by trapping supernovae and finally I will show that our results are in excellent agreement with the observations.

09.08.2022

Sergio Martínez González

Dusty Supernovae within Superbubbles

I will present our hydrodynamical modelling of the injection and survival of the dust grains produced by sequential supernovae. Our goal has been to investigate whether supernovae are net producers or destroyers of interstellar dust. We have found that they indeed lead to massively enhance the amount of dust within low-metallicity star-forming molecular clouds, in accordance with the large dust masses present in galaxies soon after the onset of cosmic reionization.

25.08.2022

Andrzej Zdziarski

The jet in Cyg X-1

I will discuss a number of results related to the jet in Cyg X-1. Recently, we have found that the jet is misaligned with respect to the binary axis by about 20 degrees and its azimuth with respect to the line of sight is about 80 degrees. The binary rotates clockwise. This allows us to fully determine the geometry of the binary, including the jet viewing angle and the position angle of the binary axis on the sky. We have also studied constraints on the electron-positron pair content of the jet and found it consistent with being pair-dominated. I will also discuss the contributions of the jet to the broad-band spectrum, from radio to high-energy gamma rays, of the system.

30.08.2022

Nikita Kosogorov

Parsec-scale evolution of the bizarre gigahertz-peaked spectrum quasar 0858-279

We performed multi-epoch multi-frequency parsec-scale studies on the gigahertz-peaked spectrum quasar 0858−279. Initially, the analysis of the parsec-scale properties with the VLBA during 2005-11-26 demonstrated that this source has a weak core with an inverted spectrum and a bent jet with a pronounced bright feature in its Stokes I emission. The polarization and spectral properties enabled us to suggest that a shock wave was formed in the feature through an interaction with a dense region in the ambient medium. We showed that VLBI-Gaia astrometry confirms the identification of the core. We also analysed six additional epochs 2007-02-09, 2007-05-23, 2007-08-03, 2017-05-27, 2018-04-08 and 2018-07-21 of VLBA observations to study the evolution of this quasar. The source presented no significant changes in its general structure. Flux density changes in the brightest feature and the core region imply that new plasma is ejected into the jet. RATAN-600 observations of the source allowed us to study the integrated spectra and hinted at the possibility of a non-linear interaction of standing and travelling shock waves in 2005. Multi-epoch polarization studies demonstrated that rotation measure values decreased from 6000 rad/m^2 to 1000 rad/m^2 in one year because the external interstellar cloud magnetic field and density decreased. This can arise due to a shock in the cloud triggered by the interaction with the jet and causing its expansion. Apart from that, the magnetic field direction in the jet also drastically changed from being perpendicular to the propagation of the jet after its observed bend to becoming perpendicular to the propagation of the jet before the bend. This is likely to be caused by the aforementioned interaction of shock waves.