List of Abstracts

It is increasingly clear that feedback from star formation and AGNs is fundamental to regulating the evolution of galaxies in the nearby Universe as well as at earlier epochs.
Mechanical feedback occurs in the form of winds, turbulence, superbubbles, AGN jets and backflows. There is mounting evidence that massive amount of cold molecular gas is being ejected from galaxy nuclei by the feedback processes. With the advent of ALMA and the NOEMA telescopes we can now study the extent, morphology, velocity structure, physical conditions and even chemistry of these cold flows at unprecedented sensitivity and resolution.

I will present recent ALMA molecular and continuum images of the molecular feedback structures of extremely dust embedded galaxy nuclei. We have imaged nearby Compact Obscured Nuclei (CONs) at spatial resolutions of only a few pc, revealing fast, collimated and complex outflows. We propose an evolutionary path for these extremely thick nuclear tori that is directly driven by these cool outflows, and that links them to more “normal” AGN obscuring structures. Possible scenarios for what is powering these thick and cool outflows will be discussed.

Ram pressure stripping is a process known to remove gas from satellite galaxies, and thus quench star formation. However, observational studies have recently found an increased ratio of active galactic nuclei (AGN) among the population of ram-pressure stripped galaxies compared to regular galaxies in the field and clusters. To test whether ram pressure (RP) can trigger an AGN, we perform a suite of hydrodynamical wind-tunnel simulations of a massive (Mstar = 10^11 Msun) galaxy, with inclusion of star formation, stellar feedback and high resolution up to 39 pc. We detect increased radial inflows to the galaxy centre under RP which are caused by growing torque (mainly from the local pressure gradients) and by mixing of non-rotating intracluster media with the interstellar media. We estimate black hole accretion with Bondi-Hoyle and torque models and with mass flux to the centremost 140 pc sphere. All three estimators give dramatically different results, and we argue that the commonly used models are incomplete and in order to correctly estimate accretion under RP a new model is required to include the missing physics. We also estimate pressure of outflows from our accretion rates to make a first prediction about the effect of AGN outflows on the process of stripping.

Determining the distance of quasar absorption outflows from the
central source and their kinetic luminosity are crucial for
understanding their contribution to AGN feedback. Here we summarize
the results for a sample of nine luminous quasars that were observed
with the Hubble Space Telescope. We find that the outflows in more
than half of the objects are powerful enough to be the main agents for
AGN feedback. The sample is representative of the quasar absorption
outflow population as a whole and is unbiased towards specific
distance ranges or kinetic luminosity value. Therefore, the analysis
results can be extended to the majority of such objects, including
broad absorption line quasars (BALQSO).

Active supermassive black holes can influence the fate of their host galaxies. Gas outflows, frequently triggered by the radiation pressure from the accretion disk, can disturb the kinematics of the gas at different scales, from a few tens to tens of thousands of parsecs. In recent years, AGN-driven outflows have been studied across different wavelength domains. From the optical to the mid-infrared, integral field spectroscopy observations have provided insights into the extent and kinematics of the multiphase outflowing gas, including the classical optical hydrogen recombination and atomic transitions, warm (~700 K) and hot (~2000 K) molecular hydrogen, and high ionization coronal lines. Optically selected QSOs (at z10^45erg/s) show kinematics of the [OIII]5007A line consistent with the presence of gas outflows at distances up to tens of kiloparsecs. The kinetic power of such outflows decreases to the outer parts of the galaxies, indicating decelerating motions. In a sample of hard X-ray-selected nearby Seyfert galaxies, gas motions consistent with outflow, are observed in 55% and 79% of the sample when analyzing the hot molecular and ionized gas species, respectively. However, the observations cover only the central kiloparsec of these objects. At similar scales, the JWST MIRI observation of nearby galaxies is becoming a key tool to disentangle the kinematics of active galaxies. In NGC 7469, an outflow traced by coronal gas has been identified with a mass loss rate up to 100 times larger than the accretion rate. The interaction of the high ionization and high-velocity gas with the ISM creates shocks observed in the hot molecular gas. In summary, AGN-driven outflows are ubiquitous among active galaxies, and are intrinsically multiphase, multiscale phenomena requiring multi-wavelength and spatially resolved observations to fully characterize them.

The WISSH quasars project aims at studying the nuclear and host galaxy properties of the most luminous quasars (L_bol>10^47 erg s−1, 1.8<z<4.6), with special emphasis on the occurrence and physical parameters of winds at different scales. In AGN, nuclear winds are manifested as UV-broad (≥2000 km s−1) absorption lines (BAL) in about 15% of quasars. In our recent work, we studied the incidence and properties of such winds in the WISSH sample, to investigate possible differences to active galactic nucleus regimes with lower luminosity. We found a higher observed fraction of CIV BAL quasars in the WISSH sample (24%) than in previous catalogues (10−15%). These WISSH BAL quasars are also characterised by a higher average BI (∼4000 km s−1) and maximum velocity (∼17000 km s−1). Moreover, for two objects we discovered BAL features bluewards of the SiIV peak, which can be associated with CIV absorption with a velocity of 0.15c. These results suggest that the higher luminosity regime of the WISSH quasars likely favours the acceleration of BAL outflows, and that their most likely driving mechanism is radiation pressure. As a whole, BAL winds shows intermediate properties compared to molecular or ionised winds and ultra-fast outflows. We will also show preliminary results from our radio survey of the WISSH sample, investigating the relations between the presence of a jet and the BAL wind.

Understanding the complex interplay between the different gas phases involved in galactic winds, can provide key information about active galactic nuclei (AGN) feedback mechanism. Theoretical models and hydrodynamical simulations of AGN feedback predict that outflows developing in the host galaxies of AGN have a multiphase and multiscale nature and that some physical mechanisms must link the inner regions where the SMBH gravitational field dominates, to the larger scales, where its direct influence is negligible.
This paradigm has been unambiguously confirmed by a plethora of multiwavelength observations in the past years (and decades). I will review the observational progresses obtained both on single objects studied at the greatest details, and from studies based on relatively large, statistical samples which tried to connect the different winds phase. I will focus particularly on state-of-the-art results for winds detected in the warm and hot gas phases, and on the excellent perspectives offered by new generation ground-based and space observatories.

Feedback and outflows associated with a quasar phase are expected to be critical in quenching the most massive galaxies at high-z. Observations targeting the cool molecular and atomic phases, which dominate the mass and momentum budget of massive galaxy outflows and which remove the direct fuel for star formation are, however, severely limited in high-z quasar hosts. I will present two ALMA programs: one targeting the molecular outflowing gas in 3 z~6 QSO hosts using the OH 119 µm absorption (Butler et al. 2022) and another targeting the diffuse, predominantly atomic gas in the halos surrounding 5 QSO host between z~2-4 using OH+(1_1-1_0) absorption (Butler in prep.). Outflows are successfully detected in both samples and compared with outflows driven by high-z star-forming galaxies observed in the same lines. Conclusions from both samples indicate that observing QSOs during the blow-out phase is crucial for studying the impact of the active nucleus on the ejection of gas from the host galaxy whilst gas in the halo may continue to be driven by mechanisms associated with the quasar phase in the halo in the unobscured phase. We further show evidence from the wide/narrow CO(9-8) emission observed simultaneously with the OH+ line in obscured/unobscured QSOs, supporting this scenario.

Accreting supermassive black holes (SMBHs) are essential in galaxy evolution models to regulate the assembly of galaxies, and consequently of matter, in the Universe. The regulation mechanisms, known as feedback, are traditionally classified into two fundamental modes: a radiative mode, associated with ionised outflows and winds in quasars, and a mechanical mode associated with radio jets, considered relevant only for a small fraction of the overall galaxy population. Crucially, this two-fold paradigm is becoming obsolete as new-generation radio interferometers, pathfinders and precursors of SKA, are providing increasing evidence of the ubiquitous low-level radio emission in most quasars, linked to black hole accretion and winds. In this talk, I will present observations supporting this paradigm-shift in black hole feedback studies, focusing on the characterisation of quasar feedback using deep and wide-field LOFAR surveys (LoTSS). Our results capitalise on synergies between the deepest LOFAR images, SDSS, and radio-to-X-ray multiwavelength surveys to unveil the physical mechanisms driving feedback and its impact on galaxy evolution. We infer physical properties from panchromatic SED-fitting, and explore the relations between accretion, outflow/wind properties from SDSS spectra, and radio emission. We investigate how feedback modes interact and how they evolve as a function of physical properties such as black hole accretion and quasar reddening. These results represent key stepping stones for future black hole wind studies using surveys in the SKA era.

Disk reflection and disk wind are two seemingly disconnected phenomena in the X-ray spectra of Black Hole X-ray binaries, providing independent probes to constrain important physical parameters associated with the accretion disks (e.g., inclination and density). A synergy between reflection and absorption spectroscopy, therefore, can provide an unprecedented insight into the physical conditions of the disk. In this work, we demonstrate this union using broadband spectral analysis of all the six hard, intermediate and soft state \textit{NuSTAR} observations of the low-mass black hole X-ray binary MAXI J1348-630 during its first outburst in 2019. Using high-density disc reflection models, we find the disk density and inclination to be $10^{20.3-21.4} \rm cm^{-3}$ and $\sim 30^\circ-50^\circ$, respectively. We also find evidence of a high-velocity wind in the form of blue-shifted Fe K (at $\sim$7.3 keV) absorption lines. We then carry out the first direct MHD modelling of non-equatorial fast outflows in an X-ray binary, with MAXI J1348-630. We find that an MHD wind of density at the base of the wind $\rm \sim 10^{19-21} \ cm^{-3}$ and an inclination of $30-40^{\circ}$ can account for the absorption line throughout all of its spectral states. This broad consistency between the best-fit parameters of the two mutually exclusive methods provides credence to our novel approach.

Line locking (LL) of absorption-line systems is a clear signature of the dynamical importance of radiation pressure force in driving astrophysical flows, with recent findings suggesting that it may be common in quasars exhibiting multiple intrinsic narrow absorption-line (NAL) systems. We find that a small volume of the phase-phase admits LL, suggesting a high-degree of fine-tuning between the physical properties of locked systems. We demonstrate that LL poses significant challenges to current theories for the formation of non-intervening NAL systems, and speculate that it may be a manifestation of outflowing and expanding circumstellar shells in the quasar-host bulge.

AGN winds may produce radio synchrotron emission through shocks and particle acceleration, and may underlie the radio emission observed in radio-quiet quasars (RQQ). Our earlier VLBA study of eight RQQ suggests that the radio emission in flat spectra objects is produced on sub-pc scales, possibly associated with the accretion disk corona, while in steep spectra objects it is produced on tens of pc scales, possibly by AGN winds. We will report on new VLBA observations of 10 more RQQ, which together cover a wide range of luminosity and black hole mass. We found that most of the RQQ have an optically thick compact core, which is still unresolved at mas scales, has a high surface brightness, and is close to the Gaia position. This core emission is consistent with self-absorbed synchrotron of coronal origin. The high Eddington ratio RQQ generally also show optically thin extended emission, which has a low surface brightness and is about 10-100 pc away from the radio core. This component may be produced by a radiation pressure driven outflow, which interacts with the local ambient medium.

Broad absorption line (BAL) quasars reveal unambiguous evidence of powerful quasar-driven outflows in their spectra. Iron low-ionization BAL (FeLoBAL) quasars are a subtype of BAL quasars that are expected to have massive and energetic winds, making them excellent targets to study quasar outflows and how black hole winds affect their environment and host galaxy. Because BAL quasar spectra are challenging to analyze with conventional methods, detailed physical properties of FeLoBAL winds, their relationship to quasar properties, and their role in feedback remain elusive. Our group has developed the novel spectral synthesis software SimBAL that can be used to model complex BAL quasar spectra and provide measurements of the physical properties of the absorbing gas in unprecedented detail. SimBAL allowed us to discover the most energetic BAL outflow ever analyzed and to perform the first systematic study of a large sample of BAL quasar spectra.
We used SimBAL to analyze the spectra of a sample of 50 low-redshift FeLoBAL quasars observed by the Sloan Digital Sky Survey. We measured the physical properties of the outflowing gas and constrained their distances from the central engine and their energetics. We found a large range of ionization parameters and densities as well as a wide range of distances from the central supermassive black holes, spanning more than four orders of magnitude (0 < log R < 4.4 [pc]). We analyzed the rest-optical emission lines for a subset of 30 z < 1.0 objects and found that FeLoBAL quasars are characterized by either high or low accretion rates, and intermediate accretion rates are avoided. We found that the outflow properties (e.g., velocity, volume filling factor) are different for the two different types. We suggest that different formation, acceleration, and confinement mechanisms may be responsible for the FeLoBAL winds.

Thanks to its existing extensive multi-wavelength coverage and to the massive and extended outflow detected both in the ionised and molecular components, XID2028 at z=1.6 represents a unique test case to study QSO feedback in action at the peak epoch of AGN-galaxy coevolution. This target was thus selected to be observed with the NIRSpec and MIRI IFU on board of JWST during the Cycle 0 Early Release Science (ERS) campaign.
In this talk I will focus on the NIRSpec integral field dataset, which is revealing a wealth of details hidden in the previous, seeing limited ground-based data thanks to the unprecedented sensitivity and resolution of JWST instrumentation. In particular, we found evidence of interaction between the QSO-driven radio jet, outflow and the ISM of the galaxy, which is producing an expanding hot bubble from which the fast and extended wind detected in previous observations is emerging. The new observations confirm the complex interplay between the AGN wind and the ISM of the host galaxy, resulting in a showcase of the new window opened by NIRSpec and JWST on the detailed study of feedback at high redshift.

When an accretion disk wind impacts the ISM of the host galaxy, the shocked wind inflates a bubble of hot gas. The wind bubble expands in the galaxy, sweeping up ambient gas. I will review the theory of wind bubbles driven by AGN. Key concepts include the energy- vs. momentum-driven limits and expansion along paths of least resistance. I will also review the multiphase structure expected in wind bubbles, including the formation of molecular gas, and different emission processes that can be used to observationally probe AGN-driven galactic winds.

The first quasars near Reionisation epoch, z~6-7.5, probe the early stages of super massive black holes and host galaxy assembly. ALMA high frequency, band 9 and 8, observations are able to constrain the gas and dust properties, and star formation rates in these luminous quasar host galaxies with unprecedented accuracy. I will discuss recent results, using ALMA, NOEMA and VLT observations, that allow us to constrain the host galaxy growth, the super massive black hole growth and the onset of strong SMBH feedback in the highest redshift quasars, z~7.5.

Powerful winds emerging from galaxy nuclei of have been observed in the past twenty years in many AGN, the so called Ultra-Fast Outflows (UFOs). Outflows are intimately related to mass accretion due to the conservation of angular momentum, and therefore are a key ingredient of most accretion disk models around black holes (BH). At the same time, nuclear winds and outflows can provide the feedback which regulates both BH and galaxy growth. We reconsider UFO observations in the framework in the framework of the Magneto-Hydrodynamic Disk Wind (MHDW) scenario. We collect from the literature UFOs observations We study the statistical properties of UFOs and derive the distribution functions of the ratio $\bar \omega$ between the mass outflow rate and mass inflow rate, and the ratio $\lambda_w$ between the mass outflow rate and the Eddington rate, key parameters in MHDW systems. We study the links between $\bar \omega$ and $\lambda_w$ and the Eddington ratio $\lambda=\frac{L_{bol}}{L_{Edd}}$. We find that the distribution functions of $\bar \omega$ and $\lambda_w$, can be described as power laws above some thresholds, suggesting that there may be several/many relatively small wind events for each major wind event in each AGN activity cycle, that is a fractal behaviour.. We then introduce a simple cellular automaton to investigate how the dynamical properties of an idealized disk-wind system change following the introduction of simple feedback rules. We find that without feedback the system is over-critical. Conversely, if feedback is present, the system can be driven toward a self organized critical state.

The immense luminosity of quasars strongly suggests they significantly impact their host galaxies. In the 10% of quasars which are "radio-loud," this is the result of the powerful jets generated by the accretion on material onto the supermassive black hole. However, the 90% of quasars with are "radio-quiet" (but not, necessarily, "radio-silent") can impact their host galaxies through a variety of physical mechanisms, including weaker versions of the jets observed from their "radio loud" counterparts, winds emanating from the accretion disk, as well as ionizing gas and/or triggering star formation in their immediate surroundings. Understanding how radio quiet quasars affect their host galaxies requires identifying the physical properties which determines the dominant mechanism for a particular radio quiet quasar. This is best achieved by identifying the dominant mechanism in a sample of radio quiet quasars, best done by measuring the properties of their parsec and kiloparsec radio emission, and determining its dependence on the quasar properties. In this talk, will present the result of such a study on a sample of radio quiet quasars, which indicates the mechanism depends on their Eddington ratio, and compare our initial findings with similar studies of other classes of active galactic nuclei.

Mergers of black holes (BHs) with cores of giant stars are a topic of ongoing research. The transient event powered by the jets that the black hole launches as it mergers with the core of the giant star is termed common envelope jets supernova (CEJSN). In the CEJSN event, the BH is engulfed by a giant star and spirals-in inside its envelope accreting mass through an accretion disk in the process. The accretion disk launches opposite jets that propagate perpendicular to the equatorial plane and expel mass from the envelope. Eventually, the BH reaches the much denser core and launches more energetic jets powered by accretion of the destroyed core matter. We study the interaction between the relativistic jets that the BH launches on the envelope of the giant star during the common envelope evolution phase and the emission of very energetic (∼PeV) neutrinos formed in the jets using a semi-analytical model and the stellar evolution code MESA. We estimate the event rate of BH-core mergers using the binary population synthesis code COMPAS and find its implications to the diffuse neutrino spectrum expected on earth due to the contribution of BH-core mergers.

Without significant energy injection from active galactic nuclei (AGN) into their host galaxy's interstellar medium (ISM) and the wider-scale environment, cosmological simulations fail to reproduce realistic looking galaxy populations. This had led to a plethora of observational work searching for evidence that rapidly growing AGN have an impact on their host galaxy's ISM and star formation properties. However, most observational papers find that AGN typically, live in gas rich, star-forming galaxies. Consequently, many papers claim little evidence for this so-called "AGN feedback". I will dissect this apparent conflict between observations and simulations. Using three cosmological simulations (IllustrisTNG, EAGLE and SIMBA), I will show what their predictions are for the type of experiments being conducted by observers. I will move on to discuss how spatially resolved studies of individual targets can be used to catch AGN "in the act" of influencing the ISM and host galaxy evolution and our how Quasar Feedback Survey reveals a, perhaps surprising, important role of radio jets in so-called 'radio quiet' sources.

Radio observations of tidal disruption events can provide key information that can help to identify and unlock the answers to what are the physical process responsible for launching fast outflows and/or relativistic jets. Since super-massive black holes (SMBH) play a major role in these events, understanding outflow ejection can also help in unveiling key information about SMBH accretion physics and provide additional information on the quiescent SMBH population. A key measurement, for example, that can currently, be solely obtained in those events, is the circumnuclear matter distribution around SMBHs in faraway galaxies. Recently, our group has unveiled a new phenomenon in TDEs, namely, delayed radio flares. While these delayed flares can be a manifestation of an off-axis jet in some cases, in others, they may be a result of a delayed outflow ejection (possibly related to a transition in accretion state). In my talk I will review both the diagnostics that radio observation provide and will also review several cases of this newly discovered phenomenon.

One of the X-ray spectroscopy discoveries by ASCA, Chandra and XMM has been the ubiquitous presence of outflows in the X-ray spectra of AGN and also Galactic Black Holes (BH). These have been named Warm Absorbers (WA) or Ultra Fast Outflows (UFO) depending on the observed outflow velocities, with the higher velocities associated generally with the higher ionization ions, reaching v > 10,000 km/s for Fexxv or Fexxvi with lower velocities for the lower ionization ions, implying the presence of different ionization and different outflow velocities along the observers' LoS. The novel insight that provided a unifying scheme of these facts has been a global modeling of these wide ionization states (and ionization parameter ξ) observations by a single function that relates their Hydrogen equivalent column to ξ by Behar and collaborators. At the same time it was realized that such a dependence is naturally associated with MHD winds launched across the entire domain of the associated accretion disks, spanning a range of a million gravitational radii. In this talk I will summarize the observations and models of these winds and will touch upon the possible underlying physics and corresponding AGN phenomenology. At the end I will make contact with their relation to the corresponding Galactic BH winds that will be covered in greater detail by PO Petrucci.

X-ray binaries (XRBs) have been studied for many years, but there remain open questions regarding different stages in their evolution, and the role of accretion and outflow states. Since XRBs show dramatic changes over short time periods, there are only a handful of high-resolution outflow observations, especially in the X-ray band. One exceptional outflow was observed in the transient stellar black hole GRO J1655-40 during its 2005 outburst. Its launch mechanism remains in dispute. The spectrum features deep absorption lines from many elements, including rare ones. We find that the relative element abundances, and the Absorption Measure Distribution (AMD) are closely entangled. By using the equivalent width measurement and theoretical curve of growth we infer an ionic column density from each resolved line. Some H-like ions include Lyman series lines of α, β, γ, and δ, which tightly constrains the ionic column densities. From these, we construct an AMD, and the density profile of the wind, which provides insights into the physical wind launching mechanism. The elemental abundances are also surprising, and hint to the precursor of the black hole in this XRB.

Spatially resolved spectroscopic studies provide the most direct means to test the effects of AGN outflows (or "winds") on their host galaxies and quantify the efficiency of AGN feedback. I will present the results of recent studies of optically-detected mass outflows in low-redshift AGN based on HST/STIS and ground-based spectroscopy and HST/ACS [O III] images. The results suggest that for the most part the [O III] emitting gas lacks the power for efficient feedback. However, there is evidence for interaction between the [O III] gas and more highly ionized, soft X-ray emitting winds. In fact, the X-ray winds may be the dominant component of mass outflow in radio quiet AGN. I will discuss this possibility and present a novel method for mapping the kinematics of the X-ray emission-line gas.

Feedback from radio AGN has been seen in the observed in the form of jet driven gas outflows. Although radio AGN are also known to have a life-cycle of activity, it is still not well understood whether the effect of feedback evolves with the AGN life-cycle. In the first part of my talk, I will discuss our results from a study to investigate this with a sample of uniformly selected 129 radio AGN with L(1.4 GHz) ~ 1e23-1e26 W/Hz. We used the radio spectral shape as proxy for the evolutionary stage of the AGN , and [OIII] emission line spectra to trace the warm ionised gas kinematics. We found that outflows in young sources (peaked radio spectrum) are more extreme than outflows in more evolved (non-peaked) sources. This is true even if we include the [OIII] non-detections and use a stacking analysis, which shows that this trend is true on average for the population of radio AGN. Sources with a peak in their radio spectra, on average, drive a broad outflow (FWHM=1330 km/s) with a velocity v=240 km/s. However, we detect no outflow in the stacked [OIII] profile of sources without a peak in their radio spectrum. We conclude that radio jets are most effective at driving gas outflows when young, and the outflow is typically short lived. This shows impact of feedback on ionised gas evolves with the radio AGN life-cycle. Using highly sensitive low frequency (150 MHz) LOFAR images, we find on average, no significant dependence of ionised gas kinematics on the radio morphology. We also find that 1.4 GHz luminosity, optical luminosity, ionisation state and Eddington ratio of these sources do not play a definitive role in driving feedback in our sample. We also identify candidate restarted AGN in our sample, whose [OIII] profiles suggest that they have more disturbed gas kinematics than their evolved counterparts, although the evidence for this is tentative.
In the second part, I will discuss new results from an expansion of this study to ~3000 sources, covering a larger range in redshift (up to z=0.8) and radio luminosity (up to L(1.4 GHz) = 1e28 W/Hz). Our findings support the picture from hydrodynamical simulations where the impact of AGN feedback changes as the radio jets grow, interact with the ambient medium, clearing a channel of gas as they expand.

Contrary to the standard picture for black-hole X-ray binaries (BHXRBs), which invokes an accretion flow (hot inner flow and outer accretion disk) and a jet, it is important to stress the importance of the outflow in BHXRBs. Assuming that the outflow is the “corona”, where Compton up-scattering of soft photons from the accretion disk occurs, we have been able to explain over the years a number of observations and correlations, some of which have not been explained in any other way. In particular, the model explains quantitatively 1) the power-law spectral index Gamma of the hard X-ray spectrum, 2) the time lag of the hard X-ray photons with respect to the softer ones, 3) the correlation between time lag and Fourier frequency in Cyg X-1 and GX 339-4, 4) the correlation between the time lag and the spectral index Gamma in GX 339-4 and other sources, 5) the fact that this correlation depends on the inclination of the source, 6) the phase-lag – cutoff-energy correlation observed in GX 339-4, 7) the narrowing of the auto-correlation function with increasing photon energy seen in Cyg X-1, 8) the correlation between the Lorentzian frequencies in the power spectrum and the spectral index Gamma in Cyg X-1 and GX 339-4, 9) the B-type QPOs in GX 339-4, and 10) the radio – X-ray correlation in GX 339-4 (unpublished work). All the above observations and correlations are explained with only two parameters: the radius at the base of the parabolic outflow and the Thomson optical depth along the axis of the outflow. For all the observations and correlations, these two parameters vary in the same narrow ranges: 10 ~< R/R_g ~< 1000 and 1 ~< tau ~< 10, where R_g is the gravitational radius.