Please click on any talk listed below to read the full abstracts. The posters can be found under the poster session of Monday, June 12th.

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Sunday, June 11th

17:30 - Reception

Monday, June 12th

  • Session 1 - X-ray Winds

    Time Name Title
    9:00 Dominguez Introduction and Welcome
    Chair: Mike Crenshaw
    9:10 Kriss Space Telescope and Optical Reverberation Mapping Project 2: X-ray, UV, and Optical Monitoring of Mrk 817 The STORM 2 Collaboration is in the midst of a multi-wavelength reverberation-mapping campaign on the Seyfert 1 galaxy Mrk 817. Using HST/COS, Swift, NICER, XMM, and numerous ground-based facilities we have uncovered strong, highly variable absorption that obscures the X-rays and produces broad, blue-shifted UV absorption troughs. While the obscuration makes the X-rays faint, occasional bright flares reveal X-ray spectral features kinematically related to the UV absorption features. Despite the faintness of the X-rays, the UV and optical continuum is at historically bright levels. Although there is significant absorption, the UV/optical continuum remains highly variable, but that variability is uncorrelated with the observed X-ray flux. The variability within the UV and optical, however, is well correlated, and show reverberation lags with the longer wavelengths lagging the UV by several days. The UV emission lines also reverberate strongly, and show lags ranging from 2-15 days. However, response times vary significantly throughout the campaign, changing on roughly 60-day timescales. The shortest time lags occur during periods with diminishing obscuration, whereas the longest lags occur during periods with rising obscuration. Photoionization modeling of the UV absorption shows that the gas lies near the inner edge of the broad-line region, and is illuminated by an ionizing continuum filtered by the gas obscuring the X-ray emission. We propose that the obscuring outflow shields the BLR from the ionizing continuum, and the changing spectral energy distribution of the ionizing continuum is responsible for the changes in emission-line response. The broad UV absorption and the X-ray obscuration may be related to variations in the accretion flow resulting in an outflowing wind driven off the accretion disk. Proposed integral field observations with JWST/NIRSpec may reveal how the outflow interacts with the host galaxy.
    9:30 Laha The feeding and feedback in active galactic nuclei as explored through X-ray spectroscopy. Outflows from active galactic Nuclei (AGN) are one of the fundamental mechanisms by which the central supermassive black hole interacts with its host galaxy. Detected in >50% of nearby AGNs, these outflows have been found to carry kinetic energy that is a large fraction of the AGN power, and thereby give ‘negative’ feedback to their host galaxies. However, the outflows do not work in isolation, they work in tandem with inflows. The inflow of gas onto the SMBH is notoriously hard to detect. Changing obscuration in X-rays offer an interesting glimpse of the cold (clumpy) matter in near vicinity of the central engine, which are also believed to play a role in supplying gas to the SMBH. Here we present our work on outflows (warm absorbers, Laha et al. 2014, 2016, 2021) and also on X-ray obscuration variability in samples of nearby AGN (Laha et al. 2020, 2021, 2023 in prep) to unveil the interesting aspects of outflows and possible `inflows' of matter in AGN. We also discuss how the AGN central engine impacts the large scale molecular outflows and drives them (MOX sample, Laha et al. 2018).
    9:50 Mehdipour Multifarious landscape of winds in AGN: joint X-ray+UV views Winds link the supermassive black holes at the heart of active galactic nuclei (AGN) to their environment. Combined high-resolution UV and X-ray spectroscopy is a crucial tool to advance our understanding of the origin and role of these outflows in AGN. I present results from recent studies investigating the physical connection between different forms of outflows that have been found in AGN. By understanding their relations, and mapping their ionization and kinematic structure, new insights can be gained on the formation and driving of AGN outflows. To this end, I discuss the UV perspective of (1) X-ray warm absorbers, (2) transient X-ray obscuring winds, and (3) X-ray ultra-fast outflows (UFOs) using spectroscopy with the Hubble Space Telescope. This includes Seyfert-1 galaxies NGC 5548 and IRAS 17020+4544, and a sample of QSOs called the Supermassive Black Hole Winds in X-rays (SUBWAYS). The combined UV and X-ray spectroscopy suggests that in cases of objects with multiple UFO components, a powerful primary UFO entrains and shocks the ambient medium. This results in the formation of weaker secondary UFO components that may be seen in the UV band. Finally, I discuss the future prospects for AGN wind studies with the upcoming XRISM and the proposed Arcus mission.
    10:10 Ogorzalek A deep, multi-epoch Chandra HETG study of the ionized outflow from NGC 4051 Active Galactic Nuclei (AGN) significantly impact the evolution of their host galaxies by expelling large fractions of gas with wide-angle outflows. The X-ray band is key to understanding how these winds affect their environment, because they are heated to high, X-ray temperatures. In this talk, I will introduce our Bayesian framework for characterizing AGN outflows, which provides substantial improvements in our ability to explore parameter space and perform robust model selection. We applied this framework to the new and archival deep Chandra HETG observation of the Seyfert galaxy NGC 4051. We detected six components, spanning velocities from 100s to 10,000s km/s, and mapped their evolution across an eight year period. The most significant wind component is collisionally, rather than photo-, ionized and remains remarkably stable between the two epochs. This is the first detection in absorption of such an AGN outflow, which, critically, was enabled by using a Bayesian approach. Furthermore, for one of the fast components, we obtain one of the tightest wind density measurements to date, log n/[cm^-3]=13.0+/-0.015, and determine that it is located at ~240 gravitational radii. We will demonstrate how, within a Bayesian framework, such precise density measurements are possible by properly accounting for free-free heating and infrared radiation. The potential of our method will be fully realized with the next generation of X-ray gratings and microcalorimeters, such as XRISM, Athena, LEM, and Arcus.
    10:30 Coffee
    11:00 Hagen Using Spectral Timing to Uncover AGN Winds: The Contribution from an Outflow to the Reverberation Signal in Fairall 9 Continuum reverberation mapping of AGN can provide new insights into the nature and geometry of the accretion flow. X-rays illuminate the outer disc, and so any variations in the observed X-ray luminosity will echo in the UV and Optical. However, by modelling this response directly and comparing to data from the recent multiwavelength campaign in Fairall 9, we showed that the simple disc re-processing picture is insufficient to explain the observed variability (Hagen & Done, 2023). Instead, the data suggest a picture where the majority of the re-processed variability occurs in a vertically extended structure about 3 light-days from the central source, i.e. a wind on the inner edge of the BLR. Here we present ongoing work in detailed modelling of the wind response to changes in illumination from both the disc and central X-ray corona, and how spectral timing can place constraints on disc wind extent, structure and location.
    11:20 Matzeu Understanding Ultra Fast Winds with XRISM and XRADE Ultra-fast outflows (UFOs) are routinely detected in the X-ray spectra of 30-40% of local-, intermediate- and high-redshift AGNs. UFOs manifest themselves as absorption troughs associated with Fe XXV Hea and Fe XXVI Lya transitions blueshifted at energies above 7 keV. The degree of blueshift translates into the range of extreme outflow velocities observed between up to ~0.4c. Measuring the intrinsic physical properties of these UFOs can provide important insights into the mechanism through which they are driven (launched, accelerated). There are currently three known physical mechanisms responsible for driving accretion UFOs: gas pressure, radiation pressure, and magnetic fields. While gas pressure (thermal driving) is unable to explain the large velocities observed in UFOs in AGN, the two other mechanisms are in principle able to do so. The launch of XRISM expected in May 2023 will allow us to detect a wealth of high-ionization absorption and emission phases that so far escaped detection and as a result, it is expected to revolutionize our understanding of the most energetic UFOs thanks to its unprecedented spectral resolution. However, a problem arising from such technological advances is that all the current models available in fitting software packages, e.g., XSPEC, are based on a CCD resolution framework and their transition to microcalorimeter resolution is hugely CPU demanding. In this talk, I present a new state-of-the-art X-Ray Accretion Disk-wind Emulator (XRADE) based on the Monte Carlo multi-dimensional (3D) radiative transfer DISK-WIND code. XRADE is produced through a process that combines X-ray tracing with supervised machine learning. As a result, we develop a novel emulation technique consisting of training, validating, and testing the simulated synthetic DISK-WIND spectra into a purposely built artificial neural network (ANN). This method will provide a unique solution to the above-mentioned CPU problem by speeding up the computational processes by an outstanding 5 orders of magnitudes. Moreover, our emulator does not suffer issues with multi-dimensional spaces that are typically faced by traditional interpolation methods which particularly affect physically motivated models. By performing a range of XRISM/Resolve simulations with XRADE of the prototypical UFO hosted in PDS 456, I will demonstrate that the characterization of its driving/launching mechanism is very promising.
    11:40 Reeves The X-ray view of the accretion disk wind in the mini BAL QSO, PG 1126-041 Accretion disk winds are observed in many AGN and likely manifest themselves via BAL like profiles in the UV and via ultrafast outflows in X-rays. PG 1126-041 is a nearby (z=0.062) mini BAL QSO based on its CIV and NV profiles, while at soft X-rays it is strongly absorbed. Archival XMM-Newton data show the soft X-ray obscurer is variable in column, which may be connected with the highest velocity components of the CIV absorber through recent monitoring. Co-ordinated XMM-Newton and NuSTAR observations were performed in December 2022, in order to study the highest velocity component of the wind at Fe K. These reveal a very deep (300 eV equivalent width) broad absorption line profile, which extends up to 40000 km/s in blueshift. This ultra fast outflow can be modeled adopting an equatorial line of sight (about 70 degrees) to a geometrically thick accretion disk wind, covering a range of terminal velocities from 0.06 to 0.15c. Thus in X-rays, PG 1126-041 exhibits the properties of the UV BAL QSOs. Future XRISM observations will provide the first high resolution views of the ultra fast winds, starting with the prototype example in PDS 456.
    12:00 Braito The remarkable disk wind in IZw 1 IZw 1 is the prototype narrow line Seyfert 1 galaxy; with a bolometric luminosity of 3x10^45 erg/s and an estimated black hole mass of 3x10^7 Msun, it implies that IZw 1 accretes at close to the Eddington limit. Such high accretion rate AGN are prime candidates for driving a fast disk wind. Indeed past XMM-Newton observations of IZw 1 revealed the presence of a broad, blueshifted P-Cygni profile with a broadened emission from ionized iron near 7 keV and a blue-shifted absorption at 9 keV likely originating from a wide angle wind outflowing at v~0.25c. I will present the results of the new simultaneous XMM & NuSTAR observations of IZw 1 that were performed in 2020. These new observations confirm the presence of the powerful wind with a kinetic power on average of ~10% of the Eddington luminosity. A multi-epoch modelling of the past X-ray observations of IZw 1 with the latest state of the art disk wind model will be presented. Despite the variability of the primary emission the disk wind in IZw 1 appears to be less variable than other disk winds.
    12:30 Lunch
    Chair: James Reeves
    13:40 Chartas Multiphase Powerful Outflows Detected in High-z Quasars We present results from a comprehensive study of ultrafast outflows (UFOs) detected in a sample of fourteen quasars near the peak of the AGN and star formation activity. Our study adds six new detections (~99% confidence) of UFOs at z ~ 1.4, almost doubling the current number of cases. Based on our survey, the coexistence of intrinsic UV NALs and UFOs is found to be significant in ~83% of quasars, suggesting a link between multiphase AGN feedback properties of the meso- and micro-scale. The kinematic luminosities of the UFOs of our high-z sample are large compared to their bolometric luminosities (median of LK/LBol ~50%). This suggests they provide efficient feedback to influence the evolution of their host galaxies and that magnetic driving may be a significant contributor to their acceleration. Our spatial analysis of Chandra observations of several lensed quasars of our sample show partial X-ray Einstein rings. These Einstein rings are signatures of extended X-ray emission likely arising from the interaction of the UFOs with the interstellar medium.
    14:00 Trindade Falcao Discovery of Extended Fe Ka; Complex X-ray Emission in NGC 5728 We report the discovery of kpc-scale Fe Ka Complex emission in the CT AGN NGC 5728. We identify spectrally and spatially resolved features redward and blueward of the neutral Fe Ka 6.4 keV line, in the extended bicone. These features have 6.5sigma and 5.3sigma significance, and equivalent widths much higher than in the nuclear spectrum. If due to redshifted and blueshifted neutral Fe Ka, these energies imply line-of-sight velocities of ~19,000-42,000 km/s and ~28,000 km/s, respectively. These velocities are more than 50% greater than velocities found for outflows observed in optical spectroscopy and could potentially provide the necessary kinetic power to disrupt the host ISM, generating efficient AGN feedback.
    14:20 Fiore BH "noisy" feedback Black hole (BH) feedback can be be both radiative and kinetic, carried out by jets, winds and shocks. 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. At the same time, nuclear winds and outflows can provide the feedback which regulates BH growth and AGN emission. We study the statistical properties of nuclear winds (the so called Ultra Fast Outflows). 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, We study the links between $\bar \omega$, $\lambda_w$ and the Eddington ratio $\lambda=\frac{L_{bol}}{L_{Edd}}$. We find that the distribution functions of $\bar \omega$, $\lambda_w$, and $\lambda$ can be described by power laws above some threshold, suggesting that there may be several/many relatively small wind episodes for each major wind event in each AGN activity cycle, that is many relatively long phases of low activity and fewer shorter phases of high activity. We study the impact of such “noisy” feedback on both BH and galaxy growth.

  • Session 2, Part 1 - BLR and BAL Winds

    Time Name Title
    14:40 Hall BAL quasar surveys and science with the SDSS The Sloan Digital Sky Survey (SDSS) has wrapped up its SDSS-IV phase and embarked on its SDSS-V phase. SDSS-V continues to obtain spectra of quasars, including broad absorption line (BAL) quasars, to establish an unprecedented time-domain variability survey of quasar winds seen in absorption. I review some work on BAL quasars from SDSS-IV and outline the SDSS-V projects continuing to obtain quasar spectra. Byun, Arav, Hall (2022, ApJ) reported on continuing observations of SDSS J0242+0049, found to have acceleration in a trough outflowing at 18,000 km/s by Hall et al. (2007). The later spectra of Byun et al. confirm a continued velocity shift, although trough broadening with time may complicate the interpretation. I present more recent SDSS spectra which show continued evolution with time in the properties of this trough. Continued evolution is also occurring in SDSS J0230+0059, originally studied by Rogerson et al. (2016). Hemler et al. (2019) presented an investigation of short-timescale C IV broad absorption line variability in quasars from the SDSS Reveberation Mapping Project (SDSS-RM). About half of the sample of 27 quasars exhibits significant C IV BAL equivalent width variability on timescales less than 10 rest-frame days. Ionization variability is a preferred explanation in many cases. However, in some cases the presence of accompanying P V absorption indicates the C IV absorption is mostly saturated; C IV equivalent width changes in such cases may be due to covering factor changes.
    15:00 Coffee and Poster Viewing - CLICK HERE TO ACCESS POSTER PDFs

    (1) Boissay-Malaquin
    • Title: Investigation on the Narrow Line Seyfert 1 Mrk 335 in an intermediate state, with Chandra/HETGS, NuSTAR and NICER
    • Abstract: The Narrow Line Seyfert 1 Mrk 335 has been observed in X-rays since 2000 and has shown to be highly and rapidly variable in flux and spectral shape, due to changes in the structure of the hot corona responsible for the primary X-ray emission via Comptonization. Its complex X-ray spectrum presents interesting features that need to be investigated in different states. While several studies have already been performed in low-flux states and during flares, we focus here on the intermediate-flux state, where previously detected warm absorbers are expected to be more easily detectable. After spending two years in a historically long low-flux state, the source finally became brighter in June-July 2020. On this occasion, we performed simultaneous observations of Mrk 335 with NuSTAR, NICER, and first the first time, Chandra/HETG. We present here our preliminary results regarding the use of NuSTAR observations to constrain the continuum, reflection properties and the broadened Fe-K line, the need for the high-resolution of HETGS to get information on the absorbers structures, and the value of NICER to study the strong soft excess.


    (2) Hoffman
    • Title: A Deep Chandra HETG study of MCG-6-30-15 Ionized Outflows: Developing a Robust Bayesian Framework
    • Abstract: Ionized outflows from Active Galactic Nuclei (AGN) have strong potential to explain the underlying mechanisms of galaxy-AGN co-evolution. Studying these outflows requires careful statistical analysis of absorption lines in the X-ray band to capture winds at their origin. Typical investigations of these high-resolution X-ray spectra are not yet optimized to extract the full potential of the data. Therefore new approaches to analyzing archival or future observations from instruments like Chandra's High Energy Transmission Grating (HETG) and the X-ray Imaging and Spectroscopy Mission (XRISM’s) microcalorimeter Resolve can yield crucial progress. In this poster, I will present a new implementation of a significantly updated Bayesian analysis framework on archival, deep HETG MCG-6-30-15 data from 2000 (130 ks) and 2004 (520 ks). By utilizing Bayesian statistics and high-performance computing, this approach reduces bias in measurements of outflow properties by exploring the whole parameter space, performing agnostic model selection, and avoiding computing-related simplifications. Combined with a new generation of models, my results will yield the most robust constraints on properties and variability of outflows in MCG-6-30-15 to date. This will significantly improve our understanding of AGN winds and their role in galaxy evolution. The full potential of this approach will be enabled with the data from future X-ray missions such as XRISM (launch in 2023), Athena, and the Line Emission Mapper (LEM) X-ray Probe.


    (3) Li
    • Title: Density diagnostics of NGC 3783 warm absorbers using a time-dependent photoionization model
    • Abstract: Outflows in active galactic nuclei (AGNs) are thought to carry kinetic energy away from the central engine as a kind of feedback channel, impacting on their host galaxies. However, the distance of the outflowing wind is poorly constrained due to lack of direct imaging observations, which limits our understanding of their kinetic power and therefore makes the impact on the local galactic environment unclear. But once the density of the outflow is known, the distance can be derived from the ionization parameter measured based on the ionization states. We perform theoretical tpho calculations using a realistic spectral energy distribution (SED) with variability information and investigate the delayed state of the ionized plasma, which enable us to derive the density-dependent lag timescale and compare to the previous observations. We also compare tpho-delay method with metastable density method as well as the more accuracy UV observation to further constrain the density range of 10 X-ray WAs of NGC 3783.


    (4) Byun
    • Title: HST/STIS Observation of the Extreme UV Outflow of QSO B0254-3327B
    • Abstract: We have identified a broad absorption line (BAL) outflow in the HST/STIS spectrum of the quasar QSO B0254-3327B at velocity 𝑣 = −3200 km s−1. We identified ionic absorption lines such as Ne viii, Na ix, Si xii, and Ne v. Via measurement of the ionic column densities, photoionization analysis, and determination of the electron number density of the outflow, we found the kinetic luminosity of the outflow system to be ∼ 0.8% of the quasar’s Eddington luminosity, or ∼ 2.14% of the bolometric luminosity, leaving its ability to contribute to AGN feedback dependent on the theoretical model. We also examined the physical properties of the outflow of Q0254-334 along with previously studied extreme UV outflows, with a total sample of 29 outflow systems, finding a weak negative correlation between outflow velocity and distance from the central source.


    (5) Harrington
    • Title: Identifying UFOs in the COS FUV spectra of PDS 456
    • Abstract: We conduct a study of the quasar PDS 456 using COS FUV spectra from the Hubble Space Telescope. We explore the absorption troughs in 7 spectra over 4 different epochs and find two troughs that are potentially due to intrinsic Ly α absorption at 0.09c and 0.006c. These lines are clearly detected in the earliest epoch but are not detected in subsequent observations, which suggests that the presence of these troughs are intrinsic to the AGN due to their variability.


    (6) Patrick
    • Title: Exploring the Physical Properties of the Outflows of the Quasars 2MASSJ14025120 and PG1425+267
    • Abstract: We have determined the column densities and covering fractions for the observed outflows in each of the low-z quasars 2MASSJ14025120 and PG1425+267. For both objects, we find multiple kinematic components as detected by multiple blueshifted absorption troughs in either the C IV doublet (ll 1548, 1550) or the O VI doublet (ll 1031, 1037), which suggest multiple outflows. We use photoionization models based on the measured ionic column densities to determine the physical states of these outflows.


    (7) Terndrup
    • Title: Temporal variability in the high-velocity broad absorption lines of Markarian 231
    • Abstract: We present time-series optical and infrared spectra of the He I*, Na I and Ca II broad absorption lines (BALs) of Markarian 231, taken at intervals of 1-2 years over a decade. We see considerable variation some but not all velocity components, including the appearance and disappearance of some lines and approximately steady changes in the mean velocity of others. We use the temporal variations to test the conclusions in our earlier paper (Leighly et al. 2014, ApJ, 788, 123) about the characteristic size scales of absorbers in different regions of the outflowing gas.


    (8) Voelker
    • Title: Analysis of a Sample of High Redshift, High Luminosity FeLoBAL Quasars
    • Abstract: Quasars are particularly luminous Active Galactic Nuclei (AGNs). The light from the central engine is absorbed by gas in our line of sight, producing absorption lines in the spectra. By modeling these spectra, we can derive the physical parameters of the absorbing gas as well as the velocities of quasar outflows, which tell us how powerful the outflow is. FeLoBAL quasars contain high ionization and low ionization broad absorption lines as well as iron lines. Though FeLoBAL quasars comprise less than 2% of the quasar population, they can contain the most powerful outflows, which provide information about galaxy evolution and feedback.
      Our group models FeLoBAL quasars using the novel spectral synthesis code SimBAL, which uses Markov Chain Monte Carlo methods to fit a model to the spectra and derive the physical parameters of the absorbing gas from that model. Previously, our group has analyzed a selection of low redshift (0.5 < z < 1.5) quasars with a luminosity range of 45 < logLbol < 47.5 (Choi et al. 2022) and a selection of intermediate redshift (1.1 < z < 1.9) quasars (Voelker et al. 2022). Here, we expand our study to include a sample of high redshift (2.1 < z < 2.6), high luminosity (46.5 < logLbol < 47.5) quasars. As higher luminosity quasars are associated with faster outflows and higher redshifts allow us access to shorter wavelengths in the observed-frame optical spectra, we can obtain more information about quasar outflows and physical gas properties, including exploring the relationship between high ionization and low ionization lines in our spectra. Using SimBAL, we modeled our objects and extracted their physical parameters, including ionization and density, which we then compared along with the bolometric luminosity logLbol with the outflow velocity. We found that of the objects we currently have analyzed, high redshift objects have a greater percentage of powerful outflows (~77.3%) than the low and intermediate redshift objects (~36.6% and 50%, respectively). Additionally, we calculated the distance of each quasar’s outflow from its central supermassive black hole (logR). Preliminary results show that the high redshift objects appear to have powerful outflows distributed amongst a broad range of logR values (0.81 pc < logR < 4.21 pc), compared to the low redshift objects which occupy two main groups – high (logR > 2.90 pc) and low (logR < 1.09 pc) logR. There is additionally tentative evidence that the high-redshift sample may have a different distribution of ionization parameters and densities than the low and intermediate redshift samples.


    (9) Armah
    • Title: Oxygen abundance in the NLR of Seyfert galaxy and the metallicity-luminosity relation
    • Abstract: Gas-phase and stellar metallicities are observed to scale primarily with galaxy stellar mass and, as a result, with other integrated properties that scale with mass, such as luminosity in bands where old stellar population predominates. The mass–metallicity relation (MZR) has been found to exist for both gas-phase and stellar metallicities. Despite decades of research, which has undoubtedly established the MZR in H II regions and star-forming galaxies (SFGs), clear direct links between gas-phase metallicity (Z) and active galactic nuclei (AGNs) properties such as luminosity and accretion rate remain unclear. I will present the recent results obtained from the BASS survey from a large survey of 561 hard X-ray selected AGNs, measuring direct emission from the AGN which is unaffected by dust or contamination from SFGs, and is much less sensitive to obscuration in the line-of-sight as compared to soft X-ray or optical wavelengths, allowing a selection based on only the supermassive black hole (SMBH) properties.


    (10) Ferree
    • Title: Gas Outflow Kinematics in NGC 3516
    • Abstract: Previous analysis of the narrow line region of the Seyfert 1 galaxy NGC 3516 has found ambiguous evidence for outflows driven by the active galactic nucleus (AGN). While the extended ionized gas kinematics were found to be inconsistent with purely rotational motion, they were not positively identified as outflows. We present long slit spectroscopy from the Hubble Space Telescope’s Space Telescope Imaging Spectrograph (STIS) to further analyze the narrow line region in this galaxy. In particular, we fit the H𝛼, Hβ, and [OIII] narrow emission lines with multiple Gaussian components using the Bayesian Evidence Analysis Tool (BEAT). Our objective is to use this spectral analysis to separate AGN driven outflows from rotation in order to determine the extent of the outflows, ultimately creating a template to understand other active galaxies with ambiguous kinematics.


    (11) Gatto
    • Title: Ionized gas outflows vs. “maintenance mode" feedback in MaNGA AGN
    • Abstract: We present a study of the ionized gas kinematics of 297 Active Galactic Nuclei (AGN) host galaxies as compared to that of 537 control galaxies observed in the MaNGA-SDSS survey using measurements of the [O III]λ5007Å emission line profiles, fitted with one narrow and one broad component – found in 45% of the AGN. We present flux, velocity and W80 maps, comparing them between AGN hosts and controls. We identify ""kinematically disturbed regions"" (KDRs) within the Extended Narrow Line Region (ENLR) of the AGN, with W80 ≥ W80,cut = 315 km s^−1 the mean value for the controls plus its standard deviation. The median difference in the W80 values between AGN and controls is 238 km s^−1. We find a positive correlation between 〈W80〉 and L[OIII] for the AGN, but, inexpectedly, also for the control sample, that we attribute to a possible presence of faint AGN in the control galaxy sample. The extent of the KDR RKDR ranges from 1 to 10 kpc, with a mean ratio to that of the ENLR RENLR of 55%. We estimate the ionized gas mass in outflow (Mout) and the corresponding kinetic powers (Eout) assuming that the KDR is due to an AGN outflow. Using two methods to obtain the outflow velocity – one based on W80 and the other using the velocity of the broad component, we find mean values Mout,W80=1.87 ±0.98 ×10^−3 M yr^−1 and Mout,b=3.54 ±0.14 ×10^−3 M yr^−1 , and Eout,W80=1.70 ±0.71 ×10^38 erg s^−1 and Eout,b=4.51 ±0.13 ×10^38 erg s^−1. These values correlate with the AGN luminosity Lbol, populating the low luminosity region of this known relation and correspond to a coupling efficiency between the outflow power and AGN luminosity of 0.01% and lower. But the large extent of the KDR, in spite of this low coupling efficiency, show that even low-luminosity AGN can impact the host galaxy in a low, “maintenance mode"" feedback.


    (12) Kudoh
    • Title: Sub-parsec scale nature of AGN outflows in the radiation-hydrodynamic simulations
    • Abstract: The multi-phase gas outflows observed in active galactic nuclei (AGN) are important for understanding the supply onto the central supermassive black hole (SMBH). The driving mechanisms can be explained by the radiation force from the AGN luminous sources according to the simulation studies: (i) continuum for the dusty outflow (e.g., Wada 2012, 2015) and (ii) the lines for the ultrafast outflow (UFO; e.g., Nomura et al. 2020, Mizumoto et al. 2021). They successfully reproduced the velocity structure of the observed lines, but they focused on different scales and physical processes of the UFO launched from accretion disk (100 Rs) and the dusty wind formed in torus (1 pc ~ 10^6 Rs), respectively. Therefore, the questions are where do dusty wind come from and how do UFO propagate on a sub-pc scale? Our simulations for the dusty wind and UFO in AGN have been carried out with the computational domain with a dynamic range of 4 orders of magnitude (i.e. 10^2 -10^6 Rs). We have performed the axisymmetric 2D hydrodynamic simulations using the CANS+ code taking into account dust and radiation. The Eddington ratio expected from the gas entering a boundary radius varies with time. We adopted the radiation field and UFO dependent on the Eddington ratio inside this boundary. We found that outflow and inflow measured outside of the central boundary condition alternately increase and decrease on a yearly time scale. UFO is dominant above the angle of 40 degrees, measured from the equatorial plane, while the dusty outflow is around the disk surface. UFO contributes significantly to the variability of the column density. These outflows are expected to build the AGN gas structure and explain the absorbers and time-varying phenomena observed in X-rays.


    (13) Sadaula
    • Title: Modeling of Warm Absorbers in Active Galactic Nuclei.
    • Abstract: The nature of the extreme variability of the central ionizing source in active galactic nuclei (AGN) suggests that the outflowing gas may deviate from the commonly approached equilibrium approximation. Hence, we need to consider a time-dependent calculation to accurately describe the ionization states and the transmitted spectra. To see the effects of the source variability quantitatively, we carried out a time-dependent photoionization simulation by solving a time-dependent balance equation for level population, internal energy, and radiative transfer simultaneously and self-consistently and developed a time-dependent photoionization modeling code (TDP code). The outflows, which are responsible for the absorption of the X-rays, known as warm absorbers, are investigated using this newly developed TDP code for various sets of input parameters such as density, the shape of the incident light curve, SED, etc. We simulated the outflow for step and flare incident light curves and will present the results. In addition, we analyzed the high-resolution transmitted model spectra to understand how the ionization structure of the outflow changes over time. The study of the time-resolved spectra could be used in constraining the warm absorber properties such as density and, in turn, the location. This will help to understand the AGN feedback by estimating the kinetic power of the outflow.


    (14) Smith
    • Title: Position dependent radiation fields near accretion disks
    • Abstract: In the line driven disk wind model for active galactic nuclei (AGN) outflows, the high energy radiation poses a significant problem wherein the gas becomes overionized. The exact spectral energy distribution of an AGN is difficult to constrain through observations, because of variate uncertainties. But what is certain, is that the spectrum seen by a distant observer differs from the spectrum observed by a fluid element near the accretion disk which is the source of the radiation. In particular, the amount of ionizing radiation can strongly depend on the fluid element's position above the disk, so the problem of overionization could be less extreme than one would expect from observed spectra. We have developed a code to quantify this position dependence. Specifically, we compute energy distributions of the mean intensity and flux as well as energy integrated quantities such as mean photon energy. We find that the shapes of spectra vary significantly with position, and that the mean intensity spectrum is significantly softer than the radial radiation flux for certain positions near the disk. This result implies that the overionization problem is indeed less severe because the mean intensity controls ionization while the radial flux is the quantity closest aligned with the observed flux. The radiation flux is the source of the momentum needed for line driving, and we use the results of our calculations to compute the radiation force felt by a fluid element when given a velocity field and distribution of spectral lines. We explore the geometric effects of the disk on the radiation force in a vertical velocity field and find that, in opposition to a common assumption, the direction of the radiation force is not parallel with the flux. This misalignment of the force and flux is due to an additional geometric and frequency weighting of different parts of the disk imposed by the velocity field.



    (15) Souza de Oliveira
    • Title: Spatially resolved observations of outflows in the radio loud AGN of UGC 8782
    • Abstract: We use optical Integral Field Spectroscopy (IFU) to study the gas emission structure and kinematics in the inner 3.4×4.9 kpc^2 region of the galaxy UGC 8782, host of a radio loud Active Galactic Nucleus (AGN). The observations were performed with the GMOS-IFU on the Gemini North telescope, resulting in a spatial resolution of ∼ 725 pc at the distance of the galaxy (z = 0.045). While the stars present ordered rotation following the orientation of the large scale disc, the gas shows a disturbed kinematics. The emission-line profiles present two kinematic components: a narrow component (σ ≲ 200 km/s), associated with the gas in the disc of the galaxy and a broad component (σ ≳ 200 km/s), produced by gas outflows. Emission-line ratio diagrams indicate that the gas in the disc is excited by the AGN radiation field, while the emission of the outflow includes additional contribution of shock excitation due to the interaction of the radio jet with the environment gas. Deviations from pure rotation, of up to 30 km/s, are observed in the disc component and likely produced by a previous merger event. The broad component is blueshifted by ∼ 150 − 500 km/s relative to the systemic velocity of the galaxy in all locations. We construct radial profiles of the mass rate and kinetic power of the ionized gas outflows, which have the maximum values at ∼ 1 kpc from the nucleus with peak values of 0.5 ± 0.1 solar masses per year and (6.8 ± 1.1)×10^41 erg/s, respectively. The kinetic coupling efficiency of these outflows are in the range of 1–6 per cent, indicating that they could be powerful enough to affect the star formation in the host galaxy as predicted by theoretical simulations. This galaxy will be observed with JWST as part of a cycle 1 program (proposal ID 1928), together with NGC 3884 e CGCG-012-070. We also will present preliminary results on the gas kinematics of NGC 3884 e CGCG-012-070, that have been already observed with GMOS-IFU, in preparation for the observations. As our JWST observations are scheduled to be carried out from April onwards, we will possibly be able to show preliminary results based on data obtained with the NIRSpec and MIRI MRS instruments. We will be aiming at the characterization of the molecular gas distribution and kinematics in these galaxies, providing a complete census of their multi-phase gas outflows.


    (16) Frankel
    • Title: Molecular Inflows and Outflows of Gravitationally Lensed Quasar HS 0810+2554
    • Abstract: We present the Atacama Large Millimeter/submillimeter Array (ALMA) observations on the gravitationally lensed quasar HS 0810+2554, located at a redshift of z = 1.51. We analyzed the data from ALMA observations targeting three carbon monoxide transitions: CO(2→1), CO(3→2), and CO(5→4) using the Common Astronomy Software Applications (CASA) software and Python codes. A number of significant galactic molecular inflows and outflows were found in each transition. In total, 62 significant CO clumps were observed across the three transitions with velocities ranging from -2000 km/s to +3000 km/s. Based on the ALMA observations, the mass, mass outflow rate, radius, significance, and momentum of the outflows and inflows were calculated. Additionally, based on the location of clumps around the quasar, it can be concluded that they are not randomly distributed but rather trace some underlying structure within the galaxy. By mapping the molecular inflows and outflows of HS 0810+2554 and continuing with this research project, we hope to gain a better understanding of how active galactic nuclei (AGN) outflows influence galaxy evolution and to find a link between large-scale molecular outflows and small-scale relativistic outflows.



    (17) Kim
    • Title: GMOS-IFU survey of AGN-driven outflows: A lack of global/instantaneous AGN feedback based on outflow size and SFR
    • Abstract: Energetic gas outflow driven by AGN has been suggested as an effective mechanism of AGN feedback by sweeping up or heating the interstellar medium (ISM) in its host galaxy. However, direct evidence of star formation quenching is still missing. Therefore, it is essential to investigate kinematics, physical size, energetics of outflow, and more importantly, their connection with star formation. In this talk, we present the main results of our Gemini Multi-Object Spectrograph IFU (GMOS-IFU) survey of AGN-driven outflows and provide constraints on AGN feedback scenarios. We have observed 31 local AGNs (z < 0.3) with various outflow strengths and analyzed their spatially resolved emission line properties. Furthermore, we performed the spectral energy distribution fitting and determined the star formation rates (SFRs) based on the dust luminosity. We find that (i) [OIII] λ5007 line is blue-shifted at the central region, which can be interpreted as the approaching cone in the biconical outflow, while H𝛼 emission line follows host galaxy rotation; (ii) AGN photoionization is dominant at the central region, and it is often surrounded by LINER, composite or star formation in BPT map; (iii) Outflow size determined by kinematics correlates with the [OIII] luminosity, yet in general, it is not large enough (~ several kpc) to affect the ISM across the host galaxy; (iv) AGN hosts with strong outflows are still actively forming as many stars as normal star forming galaxies. Our results suggest that AGN feedback by ionized outflow is neither global nor instantaneous.



    (18) Marconcini
    • Title: MOKA3D: Innovative approach to 3D AGN outflow kinematic modelling: accurate determination of outflow physical properties
    • Abstract: The determination of outflow physical properties is important to assess the possible effects of Active Galactic Nuclei feedback on host galaxies and to compare observed outflow properties with model predictions. However, current estimates are based on simplified assumptions and do not take into account many observational aspects like projection effects and spatial resolution. I present MOKA3D , a novel method to model the kinematics and orientation of outflows, which is particularly successful in recovering the three-dimensional structure, even in the presence of observed clumpy emission and irregular kinematics. At variance with previous works, this model does not assume a distribution of the observed gas emission flux but uses a novel procedure to derive it directly from observations, reproducing a 3D distribution of the emitting clouds and providing accurate estimates of the outflows physical properties, e.g. the outflow and energy rate as a function of distance from the galaxy nucleus. I have successfully tested the performance of the method with both nearby Seyfert-II galaxies observed with the Multi Unit Spectroscopic Explorer at VLT and high redshift sources observed by JWST, showing that the very complex kinematical features observed can be ascribed to the clouds clumpiness in a very simple radial velocity field, accounted by a suitable geometry.



    (19) Vazquez
    • Title: A New Sample of Sub-kpc Dual AGN with Direct Keck AO Imaging
    • Abstract: Dual accreting supermassive black holes (SMBH) represent a very important yet elusive stage of galaxy evolution. These systems are very rare: of the few observed, the majority have spatial pair separations > 1 kpc, with only a handful observed with separations less than 1 kpc. These closely separated systems represent the most dynamically important stage of a galaxy merger. To assess the frequency and constrain the properties of these closely separated systems it is essential to build up a larger sample of sub-kpc dual candidates with direct high-resolution (sub-arcsecond) imaging. To address this challenge, we have developed a systematic pre-selection strategy that exploits both the Wide-field Infrared Survey Explorer (WISE) and the Sloan Digital Sky Survey (SDSS) and successfully recovers all known close dual AGN systems. Here I present resolved Keck AO imaging of (~0.2“ resolution) of sources selected by this method with nuclear separations less than 1 kpc. These closely separated duals span a largely unexplored region of parameter space and as such, they provide an excellent opportunity to constrain how often AGN are triggered in galaxy mergers, as well as the timescale over which the AGN activity is sustained. I will discuss new evidence for AGN feedback in this unique sample of sub-kpc duals based on multi-wavelength data and its potential impact on galaxy evolution.



    (20) Weiss
    • Title: Modelling Quasar Outflow Bubbles and Searching for Deceleration
    • Abstract: Quasar accretion disks often produce outflowing winds that are supersonic in the ambient interstellar medium (ISM). This may give rise to an expanding shockwave “bubble” structure of wind, shocked wind, and shocked ISM. This phenomenon could in turn play a role in AGN feedback and/or regulating accretion rates. Existing bubble models predict, for some reasonable parameter choices, that both the expansion and gas within decelerate as more ISM is swept up. We combine past models of spherically symmetric bubbles and discuss the limitations of the model given our assumptions. We then use new observations of SDSS J030000.56+004828.0 (J0300) to search for decelerating low-velocity Ca II absorption in the outermost region of the bubble. We place an upper limit of 1 km/s per rest-frame-year on any bulk acceleration or deceleration, translating to a (parameter-dependent) lower limit on the age of the outflow. Finally, we discuss the structure of the Ca II outflow in light of our results, the outflow's relatively low velocity, a recent analysis of J0300 placing the absorbing gas at a distance of ~12 pc (Choi et al. 2022), and the fact that the Ca II must be shielded from ionising radiation.



    (21) Seaton
    • SDSS/BHM-RM: BAL Quasar Catalog
    15:40 Richards Reanalysis of CIV Emission in HST Quasar Spectra We reanalyze the UV spectra of over 200 archival HST spectra of luminous quasars. The spectra are reconstructed using the Mean-Field Independent Component Analysis templates of Rankine et al. (2021). By using this suite of templates, we are able to determine robust and uniformly measured properties of the CIV emission line, including equivalent width and blueshift. These measurements are combined into a non-linear metric, the CIV "distance" (Rivera et al. 2022; Richards et al. 2021), which we show to be a robust indicator of L/LEdd and of the presence of accretion disk winds. Using this CIV-based diagnostic tool, we find that high optical/UV luminosity is a necessary, but insufficient condition for accretion disk winds.
    16:00 Dunn An Investigation into the Relationship Between the Global Covering Fraction and Luminosity of AGN We conduct a study of 18,000 BAL quasars observed by the Sloan Digital Sky Survey to explore the relationship between global covering fractions for several ions and the luminosity of AGN. The quasars have redshifts between 2.00 and 2.30, which provides spectral coverage of the N V, Si IV, C IV and Mg II doublets. We find that 3000 of the objects showed absorption troughs with FWHM velocities ⪆1000 km/s. We compare detection fractions for each ion as a function of the λ Lλ of the AGN. We find a cutoff luminosity of approximately 7x10^45 ergs/s, where objects less than this cutoff show a significantly lower detection rate of outflows. We observe a scalable increase in global covering fraction for all 4 ions across a similar range of luminosity and a plateau that agrees with canonical global covering fraction for each ion that begins at approximately 1x10^46 ergs/s.
    16:20 Marziani Mildly ionized outflows along the quasar main sequence Gas outflows appear to be a phenomenon shared by the vast majority of type-1 active galactic nuclei. Optical and UV observations indicate that there is wide range in outflow prominence. In this paper we review how the 4D eigenvector 1 scheme/main sequence helps to organize observed properties and to lead to meaningful constraints on the outflow physical and dynamical processes. Blueshifts are interpreted as due to Doppler effect and selective obscuration, and indicate outflows occurring over a wide range of spatial scales. We found evidence in favor of the nuclear origin of the outflows diagnosed by [OIII] λ 4959,5007. The outflow phenomenology reaches its peak in the most luminous quasars that show a high prevalence of large blueshifts in the CIV 1549 λ 1549 and [OIII] λλ 4959,5007 emission line profiles. The ionized gas mass, kinetic power, and mechanical thrust of the outflows are extremely high, and suggest widespread feedback effects on the host galaxies of very luminous quasars, at cosmic epochs between 2 and 6 Gyr from the Big Bang.
    16:40 Temple Confronting AGN outflow and accretion models with SDSS quasar demographics One commonly-invoked launching mechanism for AGN outflows is radiation line driving. This mechanism depends closely on the SED of the ionizing continuum, and so is inherently linked to the structure of the accretion flow. Theories of radiation line-driven winds therefore provide testable predictions as a function of black hole (BH) mass and accretion rate. In the first part of my talk I will confront these predictions using the ultraviolet emission line properties of 190,000 quasars from SDSS DR17. We quantify how the shape of CIV 1549A and the equivalent width (EW) of HeII 1640A depend on the BH mass and Eddington ratio inferred from MgII 2800A. The blueshift of the CIV emission line is commonly interpreted as a tracer of quasar outflows, while the HeII EW traces the strength of the 10-100eV continuum which photo-ionizes the ultraviolet emission line regions. Above L/LEdd>0.2, there is a strong mass dependence in both CIV blueshift and HeII EW. Large CIV blueshifts are observed only in regions with both high BH mass and high accretion rate, consistent with predictions for radiation line driven winds. The observed trends in HeII and 2 keV X-ray strength are broadly consistent with theoretical models of AGN SEDs, where the ionizing SED depends on the accretion disc temperature and the strength of the soft excess. At L/LEdd < 0.2, we find a dramatic switch in behaviour: the ultraviolet emission properties show much weaker trends, and no longer agree with SED models, hinting at changes in the structure of the broad line region. Overall the observed emission line properties are generally consistent with the radiation line driving scenario, where quasar winds are governed by the SED, which itself results from the accretion flow and hence depends on both the SMBH mass and accretion rate. Finally, in the last part of my talk I will present new infrared spectra from Magellan FIRE which measure the [OIII] 5008A emission in a sample of high-velocity BAL quasars. I will discuss how the NLR outflows traced by [OIII] correlate with the properties of the BAL outflows seen in the UV, and compare the [OIII] kinematics seen in the BAL and non-BAL quasar populations.
    17:00 Petley Does the radio enhancement of broad absorption line quasars have a distinct origin? AGN powered winds have now been observed in many different forms and phases but knowledge of their importance in a galaxy’s history has not advanced nearly as quickly as the understanding of the accretion that powers them. For example, Broad Absorption Line Quasars (BALQSOs) are easily identifiable ionised outflows in a substantial fraction (10-20%) of the most powerful AGN sources we observe, yet even in these most luminous sources there has been little success in tracing the effect of the winds through to the galaxy itself. Curiously, BALQSOs have been observed to have a higher radio-detection fraction than the general quasar population despite their otherwise similar features. Although radio studies of these sources have been undertaken over the past two decades, large surveys have not been able to disentangle different sources of emission, namely radio jets, wind shocks and star formation, while high resolution work has been limited by small numbers and biases to the most radio luminous sources. In my previous work on BALQSOs I showed that the presence and shape of their absorption profiles has a correlation with their radio-detection fraction at low frequencies using LOFAR. This is not definitively a direct observation of wind shocks as the BAL wind meets the intra-galactic medium, but clearly couples the radio emission with wind properties. To determine whether this is an observation of the BAL wind or is actually connected with accretion properties or dust content of the BALQSOs, other features that are known to correlate with radio-detection fraction, my most recent study analyses the radio properties of the quasar population as a function of their CIV properties (accretion rate), their colour (dust) and the presence of BAL winds. In this talk I will present these new results which find that BALQSOs have an enhanced radio-detection fraction across the CIV space and for all colours despite having a lower average radio luminosity. This is a strong indicator that there is a different or additional radio emission mechanism at work in the BALQSO population. I will discuss interpretations of these findings for the whole quasar population along with attempts to model the population using wind shocks.
Tuesday, June 13th

  • Session 2, Part 2 - BLR and BAL Winds

    Time Name Title
    Chair: George Chartas
    9:00 Choi Characterizing the outflow properties of FeLoBAL winds with SimBAL Broad absorption line (BAL) features reveal unambiguous evidence for the presence of powerful winds from the central supermassive black holes in luminous quasars. These energetic outflows are considered one of the primary channels the central black holes inject energy and mass into their host galaxies. Thus, BAL quasars are attractive targets for investigating the potential mechanisms of quasar feedback on galaxies. Many spectroscopic surveys have observed hundreds of thousands of BAL quasars, enabling the statistical study of empirical wind properties. However, detailed physical properties of BAL outflows and their relation to quasar properties and role in feedback remain elusive because detailed spectral analysis of BAL quasar spectra using conventional methods is extremely challenging. We used the novel spectral synthesis software SimBAL to analyze complex BAL quasar spectra and to constrain the physical properties of the absorbing gas. SimBAL forward models BAL quasar spectra by creating synthetic spectra in terms of the physical conditions in the outflow and thereby constrains the location and the energetics of the outflows. The forward modeling technique and sophisticated spectral models SimBAL uses allow us to analyze even the most heavily absorbed BAL quasar spectrum and to investigate the physics of BAL quasar outflows in unprecedented detail. We performed the first systematic study of BAL outflows in a sample of 50 low-redshift iron low-ionization BAL (FeLoBAL) quasars observed by the SDSS. We used SimBAL to analyze the BAL features observed in the near-UV and measured the physical properties, distances from the central engine, and energetics of the outflowing gas. We found a large range of ionization parameters and densities in the outflow gas as well as a wide range of distances from the central supermassive black holes, ranging from torus scales (~pc) to host galaxy scales (~kpc). We found that more energetic BAL winds were found in more luminous or redder quasars. A new class of FeLoBAL winds, the ‘loitering outflows’ characterized by near-zero velocity compact outflows, were identified from our sample. Subsequent emission line analysis showed that they represent a distinct population of BAL quasars with low Eddington ratios. We extended our project to include FeLoBAL quasars at higher redshifts with higher black hole masses and luminosities. This new sample will allow us to investigate the FeLoBAL outflow gas properties as a function of luminosity and to test whether the results from the low-redshift sample are replicated in high-redshift quasars. The preliminary results suggest that the luminous FeLoBAL quasars have faster and more energetic outflows.
    9:20 Leighly A Link Between Feeding and Feedback in FeLoBAL Quasars Whether or not BAL outflows occur in all quasars is important for understanding the astrophysics of the outflows, as well as their possible role in galaxy evolution. We report the results of an analysis of the Hβ emission line region of a sample of 30 low-redshift (z < 1) iron low-ionization broad absorption line quasars (FeLoBALQs). A matched sample of 132 unabsorbed quasars was analyzed in parallel. The emission lines showed the well-known anticorrelation between the [O III] and Fe II emission. Using a summary statistic called E1 to quantify this anticorrelation, we found that while the distribution of E1 for the unabsorbed quasars has a single peak, the FeLoBALQs have a bimodal shape in this parameter. The two populations of FeLoBALQs are characterized by low and high bolometric luminosities and Eddington ratios. Some previous studies have suggested that BALQs are high accretion rate objects and therefore the discovery of the low accretion rate branch of FeLoBAL quasars was unexpected. The implications of this result and further research will be presented.
    9:40 Green Investigating the Cause of Variability in UV Broad Absorption Lines using SimBAL Broad Absorption Line Quasars (BALQs) are quasars that have strong outflows characterized by broad absorption lines in their rest-UV spectra. We present the first detailed variability study into the changing physical conditions for a few select BALQs. Around one-third of BALQ spectra show variability in depth or equivalent width of their absorption lines over scales of years. Variability studies provide constraints on the distance and geometry of the outflow, which have proven to be critical constraints for outflow models. To date, variability studies have been limited to empirical studies of a limited number of lines due to line-blending. Often this leads to making a simplifying assumption about the cause of variability and the underlying change in physical conditions of the gas. What is missing from the picture are detailed photoionization studies of variable sources. We use a new approach with forward modeling and spectral synthesis code SimBAL to fit multiple lines (and epochs) simultaneously. The first source studied, WPVS 007, has shown dramatic variability in both X-ray emission and the UV BALs. We find that the cause of the variability is a change in covering fraction, contrary to previous studies that support a change in ionization state. In addition, we present other variability work with SimBAL including a study of a variable FeLoBALQ and our work to characterize variability using SimBAL. These detailed case studies illustrate that variability can reveal the physical conditions of the outflowing gas, and that simple explanations (such as the equivalent width of key lines like C IV) may be insufficient for explaining the complexity of variability for the population as a whole.
    10:00 Arav Extremely energetic quasar outflows: HST/COS observations in the rest-frame EUV 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).
    10:20 Walker High Mass Flow Rate in a BAL Outflow of Quasar SDSS J1130+0411 We present the analysis of the absorption troughs of six outflows observed in quasar SDSS J1130+0411 (z ≈ 3.98) with radial velocities ranging from -2400 to -15,400 km s-1. These spectra were taken with the Very Large Telescope/Ultraviolet and Visual Echelle Spectrograph over the rest frame wavelength range of 1135-1890 Å. In the main outflow system (v ≈ -3200 km s-1), we identify Fe II and several Fe II* absorption troughs as well as Si II and Si II* troughs, which we use to determine the electron number density log ne = 2.6-0.7+0.8 cm-3. Using the column densities of these and other ions, we determine a photoionization solution with hydrogen column density log NH = 21.44-0.33+0.24 cm-2 and ionization parameter log UH = -1.75-0.45+0.28. From these values we derive the distance R = 16-11+23 kpc, an average mass flow rate of 4100-2400+6600 solar masses per year, and a kinetic luminosity of 46.13-0.37+0.41 erg s-1. This kinetic luminosity is 1.4-0.8+2.2 % of the quasar's Eddington luminosity, and therefore contributes significantly to AGN feedback.
    10:40 Coffee
    11:10 Rodriguez-Hidalgo Exciting prospects in the studies of Extremely High Velocity Outflows Outflows launched from the vicinity of supermassive black holes are among the most promising candidates for linking the small and the large scale phenomena in Active Galactic Nuclei. A recently discovered class of outflows, extremely high velocity outflows (EHVOs), may be key to understanding feedback processes, as it is likely the most powerful in terms of mass energy. These EHVOs have been observed at a large range of redshifts, including several cases among the few observations of quasars at z>7. In two recent projects we have identified almost 140 new cases, enlarging the previously number of known cases by 20. This is allowing us to carry out several investigations not accessible before. I will discuss how extremely high velocity outflows seem to appear predominantly in quasars where their CIV emission line shows larger blueshifts, the first indication that quasars with EHVOs also show outflows in emission. I will also show how they seem to appear in quasars with distinct properties, such as bolometric luminosity and Eddington ratio, relative to their lower-speeds counterparts - the already well-studied population of BALQSOs. Finally, I will discuss the latest results on the studies of their variability. Understanding how EHVOs evolve in time and through the story of the universe, especially now that they are being found at very large redshifts, might be crucial to put together the puzzle of galaxy evolution.
    11:30 Vietri Extremely high-velocity UV outflows in the most luminous QSOs at Cosmic noon: discovery, implications & perspectives I will report on an investigation of extremely high-velocity (∼0.1-0.3c) ionized outflows (EHVOs) imprinting their signatures in the UV band of most luminous QSOs shining at Cosmic noon, finding them in ~1 out of 10 quasars. Such large velocities imply large kinetic energy rate (∝v^3), therefore EHVOs are believed to play a major role in communicating the huge SMBH accretion luminosity to the gas reservoir in the host. Broad absorption lines (BALs) probe quasar outflows originating from the inner regions around the black hole, providing us unparalleled insight in the structure of quasar central engines. Studying the variability of these BALs can help us to understand their structure, temporal evolution, and key physical properties. After an overview of the main results from this on-going program, I will focus on a recently-discovered multi-component EHVO CIV BAL in an hyper-luminous quasar at z~3.6, exhibiting complex variability in each component at five different epochs, spanning 17 yr in the observed frame. I will discuss the possible mechanisms responsible for the variability, which allow us to derive the location and kinematics of the outflow, and the role of these powerful EHVO UV outflows as a promising mechanism for feedback in luminous quasars. Finally, I will present the recent discovery of a CIV EHVO in the most luminous quasar (z = 4.6) found to date and, briefly, an overview of future perspectives in this blooming research field.

  • Section 3 - Ionized and NLR scale outflows

    Time Name Title
    11:50 Marconi A new approach to photoionization modelling and the physical properties of AGN outflows I will start by summarising the results from MAGNUM, a survey to study outflows in nearby AGN with VLT/MUSE integral field spectroscopy. I will argue that the complex observed structures in kinematics and physical properties cannot be reliably interpreted with the simple approaches adopted so far. In particular, crucial outflow physical properties like mass or energy rates depend on the ionization status and density of the outflowing material. The latter value is usually assumed, as it is very difficult to estimate it from the [SII] 6730,6716 doublet. I will then present a new approach to photoionization modelling based on multiple components of photoionized gas which, at variance with previous works, are combined in a way which is set by observations. I will show how our new method is able to reproduce all observable emission lines from wide ranges of excitation with very high accuracy (i.e. to within an unprecedented 10%) and therefore allows high accuracy estimates of gas metallicity, average density and ionization parameters. While this approach is general and valid for any photoionized gas clouds, here I will focus on the gas in the NLR of AGN and show how it can be used to estimate accurate outflow physical properties, including gas density and metallicity.
    12:10 Binette The temperature problem of NLR models Different studies have reported the so-called temperature problem of the narrow line region in active galactic nuclei. The temperature of the NLR in Seyfert 2's is generally inferred from the observed [O III] λ4363Å/λ5007Å line ratio. However, for the spatially unresolved NLR, this ratio can be affected by collisional deexcitation when the plasma densities involved are high, in which case the inferred temperatures become unreliable unless the densities can be evaluated or constrained. In the case of high excitation plasma, we propose that the [ArIV] λ4711Å/λ4740Å doublet ratio could be considered a reliable density diagnostics. Using the Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7), we dispose of 28 Seyfert 2's, 22 of which present a reliable measurement of the [ArIV] ratio. It turns out that 18 objects appear to share a similar [O III] ratio corresponding to 13,350K (+/-1250K) if we adopt the same density as derived from [ArIV]. Since accessing this temperature is problematic with photoionization calculations, this would confirm the existence of a temperature problem. Since 3 of the 4 outliers show a weak polarised BLR, it might suggest that the AGN unified model geometry may apply to some degree to Seyfert 2's as suggested by Nagao et al. (2001), Bennert et al. (2006), Meléndez et al. (2008) where it is proposed that an inner dusty torus cover the densest NLR components which are observed in Seyfert I.
    12:30 Lunch
    Chair: Karen Leighly
    13:40 Revalski The Effects of Different Density Profiles on Spatially Resolved Outflow Energetics We have precisely quantified the energetics of narrow-line region (NLR) outflows in six low-redshift active galaxies. We utilized Hubble Space Telescope observations and Cloudy photoionization models to constrain the ionized gas masses, velocities, and radial extents of the outflows, and to calculate spatially resolved mass outflow rates. The outflows contain total ionized gas masses of log(M) = 5.5 – 7.5 solar masses and reach peak velocities of 800 – 2000 km/s. The outflows exhibit maximum mass outflow rates of = 3 – 12 solar masses per year, and carry kinetic energies of log(E) = 54 – 56 erg, with the gas masses, energetics, and radial extents correlating with AGN luminosity. The photoionization models reveal that the ionized gas spans more than six orders of magnitude in density, which decreases with distance from the central AGN. While these models tightly constrain the outflow energetics, they require measuring many emission lines over a large wavelength range. With the goal of streamlining this technique, we have compared these gas masses with those derived from techniques often used in the literature, including using the recombination equation and single-component models. We explored a range of radial density profiles, including those derived from assuming constant densities, using the [S II] doublet, and power-law profiles. We find that these techniques can overestimate the gas masses and outflow rates by 1-3 orders of magnitude, but single-component photoionization models based on a few key emission line ratios typically provide reasonable density constraints that are required to derive accurate outflow energetics.
    14:00 Feuillet Classifying High Redshift Galaxies in SDSS: an Alternative Diagnostic Diagram We select a sample of 815 AGN from the catalog of SDSS galaxy properties from the Portsmouth group by detection of the high-ionization [Ne V] 3426 A emission line. Our sample extends from 10^40 to 10^42.5 erg s^−1 in [Ne V] luminosity in a redshift range z = 0.17 to 0.57. We compare the luminosities of [Ne III] 3869 A, [O III] 5007 A, [O II] 3726 A, and [O I] 6300 A to that of [Ne V]. All four lines show a strong linear correlation with [Ne V], although lines with lower ionization potentials have a lower correlation coefficient. We then investigate the use of two alternative diagnostic diagrams that do not rely on Hα in order to classify high redshift galaxies, which use the [Ne III]/[O II] line ratio plotted against [O III]/[O I] and [O III]/[O II] respectively. We use photoionization modeling to characterize the behavior of the narrow-line region (NLR) in AGN and star-forming regions and test the validity of our diagnostic diagrams. We also use a luminosity cutoff of log L[O III] = 42 to limit the contamination of the AGN region to 9%. This method also allows us to isolate Green Pea and Purple Grape galaxies from the star-forming sample. Using or new diagnostic diagram, we are able to reliably classify AGNs up to a redshift of z = 1.06, and add more than 400 new AGN to the [Ne V]-selected AGN sample.
    14:20 Bianchin Multiphase gas kinematics as a tracer of AGN-driven outflows across different wavelengths 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 z<0.2 and Lbol>1045erg/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 deaccelerating 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.
    14:40 Circosta 5000 eyes on AGN feedback: Exploring [OIII] outflows with the Dark Energy Spectroscopic Instrument Feedback from active galactic nuclei (AGN) is thought to be key in shaping the life-cycle of galaxies. AGN inject a significant amount of energy into the surrounding interstellar medium and launch gaseous winds. They are therefore able to potentially suppress or inhibit future star formation in their hosts. AGN feedback is a necessary ingredient of theoretical models of galaxy evolution, although proving its role observationally remains a challenge. The Dark Energy Spectroscopic Instrument (DESI) survey is collecting 5000 spectra at a time over a large area of the sky, therefore providing an unprecedented sample of thousands of targets to investigate widespread ionized outflow diagnostics such as [OIII] up to redshift ~1. DESI offers an ideal avenue to build a statistical understanding of AGN feedback across the galaxy population. In this talk I will present recent work aimed at characterizing ionized outflows through multi-component line fitting. This dataset enables studies of the occurrence of outflows in AGN as a function of redshift and AGN/host galaxy properties (e.g., AGN luminosity, black hole mass, stellar mass, star-formation rate) and scaling relations between outflow and AGN physical parameters, for a cosmic epoch overall unexplored so far with such large statistics.
    15:00 Coffee and Poster Viewing

    (1) Boissay-Malaquin
    • Title: Investigation on the Narrow Line Seyfert 1 Mrk 335 in an intermediate state, with Chandra/HETGS, NuSTAR and NICER
    • Abstract: The Narrow Line Seyfert 1 Mrk 335 has been observed in X-rays since 2000 and has shown to be highly and rapidly variable in flux and spectral shape, due to changes in the structure of the hot corona responsible for the primary X-ray emission via Comptonization. Its complex X-ray spectrum presents interesting features that need to be investigated in different states. While several studies have already been performed in low-flux states and during flares, we focus here on the intermediate-flux state, where previously detected warm absorbers are expected to be more easily detectable. After spending two years in a historically long low-flux state, the source finally became brighter in June-July 2020. On this occasion, we performed simultaneous observations of Mrk 335 with NuSTAR, NICER, and first the first time, Chandra/HETG. We present here our preliminary results regarding the use of NuSTAR observations to constrain the continuum, reflection properties and the broadened Fe-K line, the need for the high-resolution of HETGS to get information on the absorbers structures, and the value of NICER to study the strong soft excess.


    (2) Hoffman
    • Title: A Deep Chandra HETG study of MCG-6-30-15 Ionized Outflows: Developing a Robust Bayesian Framework
    • Abstract: Ionized outflows from Active Galactic Nuclei (AGN) have strong potential to explain the underlying mechanisms of galaxy-AGN co-evolution. Studying these outflows requires careful statistical analysis of absorption lines in the X-ray band to capture winds at their origin. Typical investigations of these high-resolution X-ray spectra are not yet optimized to extract the full potential of the data. Therefore new approaches to analyzing archival or future observations from instruments like Chandra's High Energy Transmission Grating (HETG) and the X-ray Imaging and Spectroscopy Mission (XRISM’s) microcalorimeter Resolve can yield crucial progress. In this poster, I will present a new implementation of a significantly updated Bayesian analysis framework on archival, deep HETG MCG-6-30-15 data from 2000 (130 ks) and 2004 (520 ks). By utilizing Bayesian statistics and high-performance computing, this approach reduces bias in measurements of outflow properties by exploring the whole parameter space, performing agnostic model selection, and avoiding computing-related simplifications. Combined with a new generation of models, my results will yield the most robust constraints on properties and variability of outflows in MCG-6-30-15 to date. This will significantly improve our understanding of AGN winds and their role in galaxy evolution. The full potential of this approach will be enabled with the data from future X-ray missions such as XRISM (launch in 2023), Athena, and the Line Emission Mapper (LEM) X-ray Probe.


    (3) Li
    • Title: Density diagnostics of NGC 3783 warm absorbers using a time-dependent photoionization model
    • Abstract: Outflows in active galactic nuclei (AGNs) are thought to carry kinetic energy away from the central engine as a kind of feedback channel, impacting on their host galaxies. However, the distance of the outflowing wind is poorly constrained due to lack of direct imaging observations, which limits our understanding of their kinetic power and therefore makes the impact on the local galactic environment unclear. But once the density of the outflow is known, the distance can be derived from the ionization parameter measured based on the ionization states. We perform theoretical tpho calculations using a realistic spectral energy distribution (SED) with variability information and investigate the delayed state of the ionized plasma, which enable us to derive the density-dependent lag timescale and compare to the previous observations. We also compare tpho-delay method with metastable density method as well as the more accuracy UV observation to further constrain the density range of 10 X-ray WAs of NGC 3783.


    (4) Byun
    • Title: HST/STIS Observation of the Extreme UV Outflow of QSO B0254-3327B
    • Abstract: We have identified a broad absorption line (BAL) outflow in the HST/STIS spectrum of the quasar QSO B0254-3327B at velocity 𝑣 = −3200 km s−1. We identified ionic absorption lines such as Ne viii, Na ix, Si xii, and Ne v. Via measurement of the ionic column densities, photoionization analysis, and determination of the electron number density of the outflow, we found the kinetic luminosity of the outflow system to be ∼ 0.8% of the quasar’s Eddington luminosity, or ∼ 2.14% of the bolometric luminosity, leaving its ability to contribute to AGN feedback dependent on the theoretical model. We also examined the physical properties of the outflow of Q0254-334 along with previously studied extreme UV outflows, with a total sample of 29 outflow systems, finding a weak negative correlation between outflow velocity and distance from the central source.


    (5) Harrington
    • Title: Identifying UFOs in the COS FUV spectra of PDS 456
    • Abstract: We conduct a study of the quasar PDS 456 using COS FUV spectra from the Hubble Space Telescope. We explore the absorption troughs in 7 spectra over 4 different epochs and find two troughs that are potentially due to intrinsic Ly α absorption at 0.09c and 0.006c. These lines are clearly detected in the earliest epoch but are not detected in subsequent observations, which suggests that the presence of these troughs are intrinsic to the AGN due to their variability.


    (6) Patrick
    • Title: Exploring the Physical Properties of the Outflows of the Quasars 2MASSJ14025120 and PG1425+267
    • Abstract: We have determined the column densities and covering fractions for the observed outflows in each of the low-z quasars 2MASSJ14025120 and PG1425+267. For both objects, we find multiple kinematic components as detected by multiple blueshifted absorption troughs in either the C IV doublet (ll 1548, 1550) or the O VI doublet (ll 1031, 1037), which suggest multiple outflows. We use photoionization models based on the measured ionic column densities to determine the physical states of these outflows.


    (7) Terndrup
    • Title: Temporal variability in the high-velocity broad absorption lines of Markarian 231
    • Abstract: We present time-series optical and infrared spectra of the He I*, Na I and Ca II broad absorption lines (BALs) of Markarian 231, taken at intervals of 1-2 years over a decade. We see considerable variation some but not all velocity components, including the appearance and disappearance of some lines and approximately steady changes in the mean velocity of others. We use the temporal variations to test the conclusions in our earlier paper (Leighly et al. 2014, ApJ, 788, 123) about the characteristic size scales of absorbers in different regions of the outflowing gas.


    (8) Voelker
    • Title: Analysis of a Sample of High Redshift, High Luminosity FeLoBAL Quasars
    • Abstract: Quasars are particularly luminous Active Galactic Nuclei (AGNs). The light from the central engine is absorbed by gas in our line of sight, producing absorption lines in the spectra. By modeling these spectra, we can derive the physical parameters of the absorbing gas as well as the velocities of quasar outflows, which tell us how powerful the outflow is. FeLoBAL quasars contain high ionization and low ionization broad absorption lines as well as iron lines. Though FeLoBAL quasars comprise less than 2% of the quasar population, they can contain the most powerful outflows, which provide information about galaxy evolution and feedback.
      Our group models FeLoBAL quasars using the novel spectral synthesis code SimBAL, which uses Markov Chain Monte Carlo methods to fit a model to the spectra and derive the physical parameters of the absorbing gas from that model. Previously, our group has analyzed a selection of low redshift (0.5 < z < 1.5) quasars with a luminosity range of 45 < logLbol < 47.5 (Choi et al. 2022) and a selection of intermediate redshift (1.1 < z < 1.9) quasars (Voelker et al. 2022). Here, we expand our study to include a sample of high redshift (2.1 < z < 2.6), high luminosity (46.5 < logLbol < 47.5) quasars. As higher luminosity quasars are associated with faster outflows and higher redshifts allow us access to shorter wavelengths in the observed-frame optical spectra, we can obtain more information about quasar outflows and physical gas properties, including exploring the relationship between high ionization and low ionization lines in our spectra. Using SimBAL, we modeled our objects and extracted their physical parameters, including ionization and density, which we then compared along with the bolometric luminosity logLbol with the outflow velocity. We found that of the objects we currently have analyzed, high redshift objects have a greater percentage of powerful outflows (~77.3%) than the low and intermediate redshift objects (~36.6% and 50%, respectively). Additionally, we calculated the distance of each quasar’s outflow from its central supermassive black hole (logR). Preliminary results show that the high redshift objects appear to have powerful outflows distributed amongst a broad range of logR values (0.81 pc < logR < 4.21 pc), compared to the low redshift objects which occupy two main groups – high (logR > 2.90 pc) and low (logR < 1.09 pc) logR. There is additionally tentative evidence that the high-redshift sample may have a different distribution of ionization parameters and densities than the low and intermediate redshift samples.


    (9) Armah
    • Title: Oxygen abundance in the NLR of Seyfert galaxy and the metallicity-luminosity relation
    • Abstract: Gas-phase and stellar metallicities are observed to scale primarily with galaxy stellar mass and, as a result, with other integrated properties that scale with mass, such as luminosity in bands where old stellar population predominates. The mass–metallicity relation (MZR) has been found to exist for both gas-phase and stellar metallicities. Despite decades of research, which has undoubtedly established the MZR in H II regions and star-forming galaxies (SFGs), clear direct links between gas-phase metallicity (Z) and active galactic nuclei (AGNs) properties such as luminosity and accretion rate remain unclear. I will present the recent results obtained from the BASS survey from a large survey of 561 hard X-ray selected AGNs, measuring direct emission from the AGN which is unaffected by dust or contamination from SFGs, and is much less sensitive to obscuration in the line-of-sight as compared to soft X-ray or optical wavelengths, allowing a selection based on only the supermassive black hole (SMBH) properties.


    (10)Ferree
    • Title: Gas Outflow Kinematics in NGC 3516
    • Abstract: Previous analysis of the narrow line region of the Seyfert 1 galaxy NGC 3516 has found ambiguous evidence for outflows driven by the active galactic nucleus (AGN). While the extended ionized gas kinematics were found to be inconsistent with purely rotational motion, they were not positively identified as outflows. We present long slit spectroscopy from the Hubble Space Telescope’s Space Telescope Imaging Spectrograph (STIS) to further analyze the narrow line region in this galaxy. In particular, we fit the H𝛼, Hβ, and [OIII] narrow emission lines with multiple Gaussian components using the Bayesian Evidence Analysis Tool (BEAT). Our objective is to use this spectral analysis to separate AGN driven outflows from rotation in order to determine the extent of the outflows, ultimately creating a template to understand other active galaxies with ambiguous kinematics.


    (11) Gatto
    • Title: Ionized gas outflows vs. “maintenance mode" feedback in MaNGA AGN
    • Abstract: We present a study of the ionized gas kinematics of 297 Active Galactic Nuclei (AGN) host galaxies as compared to that of 537 control galaxies observed in the MaNGA-SDSS survey using measurements of the [O III]λ5007Å emission line profiles, fitted with one narrow and one broad component – found in 45% of the AGN. We present flux, velocity and W80 maps, comparing them between AGN hosts and controls. We identify ""kinematically disturbed regions"" (KDRs) within the Extended Narrow Line Region (ENLR) of the AGN, with W80 ≥ W80,cut = 315 km s^−1 the mean value for the controls plus its standard deviation. The median difference in the W80 values between AGN and controls is 238 km s^−1. We find a positive correlation between 〈W80〉 and L[OIII] for the AGN, but, inexpectedly, also for the control sample, that we attribute to a possible presence of faint AGN in the control galaxy sample. The extent of the KDR RKDR ranges from 1 to 10 kpc, with a mean ratio to that of the ENLR RENLR of 55%. We estimate the ionized gas mass in outflow (Mout) and the corresponding kinetic powers (Eout) assuming that the KDR is due to an AGN outflow. Using two methods to obtain the outflow velocity – one based on W80 and the other using the velocity of the broad component, we find mean values Mout,W80=1.87 ±0.98 ×10^−3 M yr^−1 and Mout,b=3.54 ±0.14 ×10^−3 M yr^−1 , and Eout,W80=1.70 ±0.71 ×10^38 erg s^−1 and Eout,b=4.51 ±0.13 ×10^38 erg s^−1. These values correlate with the AGN luminosity Lbol, populating the low luminosity region of this known relation and correspond to a coupling efficiency between the outflow power and AGN luminosity of 0.01% and lower. But the large extent of the KDR, in spite of this low coupling efficiency, show that even low-luminosity AGN can impact the host galaxy in a low, “maintenance mode"" feedback.


    (12) Kudoh
    • Title: Sub-parsec scale nature of AGN outflows in the radiation-hydrodynamic simulations
    • Abstract: The multi-phase gas outflows observed in active galactic nuclei (AGN) are important for understanding the supply onto the central supermassive black hole (SMBH). The driving mechanisms can be explained by the radiation force from the AGN luminous sources according to the simulation studies: (i) continuum for the dusty outflow (e.g., Wada 2012, 2015) and (ii) the lines for the ultrafast outflow (UFO; e.g., Nomura et al. 2020, Mizumoto et al. 2021). They successfully reproduced the velocity structure of the observed lines, but they focused on different scales and physical processes of the UFO launched from accretion disk (100 Rs) and the dusty wind formed in torus (1 pc ~ 10^6 Rs), respectively. Therefore, the questions are where do dusty wind come from and how do UFO propagate on a sub-pc scale? Our simulations for the dusty wind and UFO in AGN have been carried out with the computational domain with a dynamic range of 4 orders of magnitude (i.e. 10^2 -10^6 Rs). We have performed the axisymmetric 2D hydrodynamic simulations using the CANS+ code taking into account dust and radiation. The Eddington ratio expected from the gas entering a boundary radius varies with time. We adopted the radiation field and UFO dependent on the Eddington ratio inside this boundary. We found that outflow and inflow measured outside of the central boundary condition alternately increase and decrease on a yearly time scale. UFO is dominant above the angle of 40 degrees, measured from the equatorial plane, while the dusty outflow is around the disk surface. UFO contributes significantly to the variability of the column density. These outflows are expected to build the AGN gas structure and explain the absorbers and time-varying phenomena observed in X-rays.


    (13) Sadaula
    • Title: Modeling of Warm Absorbers in Active Galactic Nuclei.
    • Abstract: The nature of the extreme variability of the central ionizing source in active galactic nuclei (AGN) suggests that the outflowing gas may deviate from the commonly approached equilibrium approximation. Hence, we need to consider a time-dependent calculation to accurately describe the ionization states and the transmitted spectra. To see the effects of the source variability quantitatively, we carried out a time-dependent photoionization simulation by solving a time-dependent balance equation for level population, internal energy, and radiative transfer simultaneously and self-consistently and developed a time-dependent photoionization modeling code (TDP code). The outflows, which are responsible for the absorption of the X-rays, known as warm absorbers, are investigated using this newly developed TDP code for various sets of input parameters such as density, the shape of the incident light curve, SED, etc. We simulated the outflow for step and flare incident light curves and will present the results. In addition, we analyzed the high-resolution transmitted model spectra to understand how the ionization structure of the outflow changes over time. The study of the time-resolved spectra could be used in constraining the warm absorber properties such as density and, in turn, the location. This will help to understand the AGN feedback by estimating the kinetic power of the outflow.


    (14) Smith
    • Title: Position dependent radiation fields near accretion disks
    • Abstract: In the line driven disk wind model for active galactic nuclei (AGN) outflows, the high energy radiation poses a significant problem wherein the gas becomes overionized. The exact spectral energy distribution of an AGN is difficult to constrain through observations, because of variate uncertainties. But what is certain, is that the spectrum seen by a distant observer differs from the spectrum observed by a fluid element near the accretion disk which is the source of the radiation. In particular, the amount of ionizing radiation can strongly depend on the fluid element's position above the disk, so the problem of overionization could be less extreme than one would expect from observed spectra. We have developed a code to quantify this position dependence. Specifically, we compute energy distributions of the mean intensity and flux as well as energy integrated quantities such as mean photon energy. We find that the shapes of spectra vary significantly with position, and that the mean intensity spectrum is significantly softer than the radial radiation flux for certain positions near the disk. This result implies that the overionization problem is indeed less severe because the mean intensity controls ionization while the radial flux is the quantity closest aligned with the observed flux. The radiation flux is the source of the momentum needed for line driving, and we use the results of our calculations to compute the radiation force felt by a fluid element when given a velocity field and distribution of spectral lines. We explore the geometric effects of the disk on the radiation force in a vertical velocity field and find that, in opposition to a common assumption, the direction of the radiation force is not parallel with the flux. This misalignment of the force and flux is due to an additional geometric and frequency weighting of different parts of the disk imposed by the velocity field.


    (15) Souza de Oliveira
    • Title: Spatially resolved observations of outflows in the radio loud AGN of UGC 8782
    • Abstract: We use optical Integral Field Spectroscopy (IFU) to study the gas emission structure and kinematics in the inner 3.4×4.9 kpc^2 region of the galaxy UGC 8782, host of a radio loud Active Galactic Nucleus (AGN). The observations were performed with the GMOS-IFU on the Gemini North telescope, resulting in a spatial resolution of ∼ 725 pc at the distance of the galaxy (z = 0.045). While the stars present ordered rotation following the orientation of the large scale disc, the gas shows a disturbed kinematics. The emission-line profiles present two kinematic components: a narrow component (σ ≲ 200 km/s), associated with the gas in the disc of the galaxy and a broad component (σ ≳ 200 km/s), produced by gas outflows. Emission-line ratio diagrams indicate that the gas in the disc is excited by the AGN radiation field, while the emission of the outflow includes additional contribution of shock excitation due to the interaction of the radio jet with the environment gas. Deviations from pure rotation, of up to 30 km/s, are observed in the disc component and likely produced by a previous merger event. The broad component is blueshifted by ∼ 150 − 500 km/s relative to the systemic velocity of the galaxy in all locations. We construct radial profiles of the mass rate and kinetic power of the ionized gas outflows, which have the maximum values at ∼ 1 kpc from the nucleus with peak values of 0.5 ± 0.1 solar masses per year and (6.8 ± 1.1)×10^41 erg/s, respectively. The kinetic coupling efficiency of these outflows are in the range of 1–6 per cent, indicating that they could be powerful enough to affect the star formation in the host galaxy as predicted by theoretical simulations. This galaxy will be observed with JWST as part of a cycle 1 program (proposal ID 1928), together with NGC 3884 e CGCG-012-070. We also will present preliminary results on the gas kinematics of NGC 3884 e CGCG-012-070, that have been already observed with GMOS-IFU, in preparation for the observations. As our JWST observations are scheduled to be carried out from April onwards, we will possibly be able to show preliminary results based on data obtained with the NIRSpec and MIRI MRS instruments. We will be aiming at the characterization of the molecular gas distribution and kinematics in these galaxies, providing a complete census of their multi-phase gas outflows.


    (16) Frankel
    • Title: Molecular Inflows and Outflows of Gravitationally Lensed Quasar HS 0810+2554
    • Abstract: We present the Atacama Large Millimeter/submillimeter Array (ALMA) observations on the gravitationally lensed quasar HS 0810+2554, located at a redshift of z = 1.51. We analyzed the data from ALMA observations targeting three carbon monoxide transitions: CO(2→1), CO(3→2), and CO(5→4) using the Common Astronomy Software Applications (CASA) software and Python codes. A number of significant galactic molecular inflows and outflows were found in each transition. In total, 62 significant CO clumps were observed across the three transitions with velocities ranging from -2000 km/s to +3000 km/s. Based on the ALMA observations, the mass, mass outflow rate, radius, significance, and momentum of the outflows and inflows were calculated. Additionally, based on the location of clumps around the quasar, it can be concluded that they are not randomly distributed but rather trace some underlying structure within the galaxy. By mapping the molecular inflows and outflows of HS 0810+2554 and continuing with this research project, we hope to gain a better understanding of how active galactic nuclei (AGN) outflows influence galaxy evolution and to find a link between large-scale molecular outflows and small-scale relativistic outflows.


    (17) Kim
    • Title: GMOS-IFU survey of AGN-driven outflows: A lack of global/instantaneous AGN feedback based on outflow size and SFR
    • Abstract: Energetic gas outflow driven by AGN has been suggested as an effective mechanism of AGN feedback by sweeping up or heating the interstellar medium (ISM) in its host galaxy. However, direct evidence of star formation quenching is still missing. Therefore, it is essential to investigate kinematics, physical size, energetics of outflow, and more importantly, their connection with star formation. In this talk, we present the main results of our Gemini Multi-Object Spectrograph IFU (GMOS-IFU) survey of AGN-driven outflows and provide constraints on AGN feedback scenarios. We have observed 31 local AGNs (z < 0.3) with various outflow strengths and analyzed their spatially resolved emission line properties. Furthermore, we performed the spectral energy distribution fitting and determined the star formation rates (SFRs) based on the dust luminosity. We find that (i) [OIII] λ5007 line is blue-shifted at the central region, which can be interpreted as the approaching cone in the biconical outflow, while H𝛼 emission line follows host galaxy rotation; (ii) AGN photoionization is dominant at the central region, and it is often surrounded by LINER, composite or star formation in BPT map; (iii) Outflow size determined by kinematics correlates with the [OIII] luminosity, yet in general, it is not large enough (~ several kpc) to affect the ISM across the host galaxy; (iv) AGN hosts with strong outflows are still actively forming as many stars as normal star forming galaxies. Our results suggest that AGN feedback by ionized outflow is neither global nor instantaneous.


    (18) Marconcini
    • Title: MOKA3D: Innovative approach to 3D AGN outflow kinematic modelling: accurate determination of outflow physical properties
    • Abstract: The determination of outflow physical properties is important to assess the possible effects of Active Galactic Nuclei feedback on host galaxies and to compare observed outflow properties with model predictions. However, current estimates are based on simplified assumptions and do not take into account many observational aspects like projection effects and spatial resolution. I present MOKA3D , a novel method to model the kinematics and orientation of outflows, which is particularly successful in recovering the three-dimensional structure, even in the presence of observed clumpy emission and irregular kinematics. At variance with previous works, this model does not assume a distribution of the observed gas emission flux but uses a novel procedure to derive it directly from observations, reproducing a 3D distribution of the emitting clouds and providing accurate estimates of the outflows physical properties, e.g. the outflow and energy rate as a function of distance from the galaxy nucleus. I have successfully tested the performance of the method with both nearby Seyfert-II galaxies observed with the Multi Unit Spectroscopic Explorer at VLT and high redshift sources observed by JWST, showing that the very complex kinematical features observed can be ascribed to the clouds clumpiness in a very simple radial velocity field, accounted by a suitable geometry.


    (19) Vazquez
    • Title: A New Sample of Sub-kpc Dual AGN with Direct Keck AO Imaging
    • Abstract: Dual accreting supermassive black holes (SMBH) represent a very important yet elusive stage of galaxy evolution. These systems are very rare: of the few observed, the majority have spatial pair separations > 1 kpc, with only a handful observed with separations less than 1 kpc. These closely separated systems represent the most dynamically important stage of a galaxy merger. To assess the frequency and constrain the properties of these closely separated systems it is essential to build up a larger sample of sub-kpc dual candidates with direct high-resolution (sub-arcsecond) imaging. To address this challenge, we have developed a systematic pre-selection strategy that exploits both the Wide-field Infrared Survey Explorer (WISE) and the Sloan Digital Sky Survey (SDSS) and successfully recovers all known close dual AGN systems. Here I present resolved Keck AO imaging of (~0.2“ resolution) of sources selected by this method with nuclear separations less than 1 kpc. These closely separated duals span a largely unexplored region of parameter space and as such, they provide an excellent opportunity to constrain how often AGN are triggered in galaxy mergers, as well as the timescale over which the AGN activity is sustained. I will discuss new evidence for AGN feedback in this unique sample of sub-kpc duals based on multi-wavelength data and its potential impact on galaxy evolution.


    (20) Weiss
    • Title: Modelling Quasar Outflow Bubbles and Searching for Deceleration
    • Abstract: Quasar accretion disks often produce outflowing winds that are supersonic in the ambient interstellar medium (ISM). This may give rise to an expanding shockwave “bubble” structure of wind, shocked wind, and shocked ISM. This phenomenon could in turn play a role in AGN feedback and/or regulating accretion rates. Existing bubble models predict, for some reasonable parameter choices, that both the expansion and gas within decelerate as more ISM is swept up. We combine past models of spherically symmetric bubbles and discuss the limitations of the model given our assumptions. We then use new observations of SDSS J030000.56+004828.0 (J0300) to search for decelerating low-velocity Ca II absorption in the outermost region of the bubble. We place an upper limit of 1 km/s per rest-frame-year on any bulk acceleration or deceleration, translating to a (parameter-dependent) lower limit on the age of the outflow. Finally, we discuss the structure of the Ca II outflow in light of our results, the outflow's relatively low velocity, a recent analysis of J0300 placing the absorbing gas at a distance of ~12 pc (Choi et al. 2022), and the fact that the Ca II must be shielded from ionising radiation.
    15:40 Falcone Disentangling the Ionized Gas Kinematics in the Seyfert 1 Galaxy NGC 3227 NGC 3227 is a nearby (z ~ 0.004) star-forming Seyfert 1 active galaxy that is tidally interacting with its neighboring galaxy NGC 3226. Our ongoing work focuses on the connection and interplay between AGN and star formation-driven feeding and feedback in this system, and the role that NGC 3226 has in these processes. We present a spatially resolved study of the kinematics and physical conditions of the ionized gas in NGC 3227 using observations from the Hubble Space Telescope’s Space Telescope Imaging Spectrograph (STIS), Apache Point Observatory’s (APO) Dual Imaging Spectrograph (DIS), APO’s Kitt Peak Ohio State Multi-Object Spectrograph (KOSMOS), and the Gemini-North Near-Infrared Integral Field Spectrometer (NIFS). Using the Bayesian Evidence Analysis Tool (BEAT), we fit multiple Gaussian profiles to the spatially resolved optical and NIR emission lines. Using the APO and NIFS observations, we map the circumnuclear and large-scale rotation of the host galaxy, which allows us to separate the contributions of the rotational and outflow components of the ionized gas and accurately determine the extent of AGN driven outflows. By utilizing multiwavelength datasets, we aim to create a comprehensive model of the feeding and feedback processes in NGC 3227.
    16:00 Meena The Origins and Driving Mechanism of Narrow Line Region Outflows Investigating the dynamics of Narrow Line Regions (NLRs) in active galaxies is crucial for understanding the effects of AGN feedback on their host galaxies and constructing realistic simulations of supermassive black hole (SMBH)-galaxy formation and co-evolution. In this work, we identify the physical processes that govern the origins and acceleration of NLR outflows. Using the spectroscopic and imaging capabilities of the Hubble Space Telescope and Apache Point Observatory's 3.5m Telescope, we perform an in-depth analysis of outflow dynamics in a sample of five nearby active galaxies. We employ spatially-resolved spectroscopic observations of nuclear and circumnuclear regions to map the radial velocity gradients of the ionized gas and outflows in the NLRs. Independent of the observed kinematics, we develop an analytical model based on radiative driving by the AGN, as well as gravitational deceleration from both the SMBH and the enclosed mass of the galaxy, to derive velocity profiles of the NLR outflows. Our models successfully reproduce the distinct velocity and mass outflow rate profiles observed in spatially resolved measurements, particularly the turnover distance where gravity from the host galaxy starts to overwhelm radiation pressure. This consistency between observed and model kinematics confirms that AGN radiation pressure is the primary driving mechanism responsible for the observed NLR outflows in our sample. Additionally, using our radiation-gravity models, we determine the launch distances of the observed outflows, which may correspond to the star-forming gas reservoir sites in these active galaxies. We find that the maximum distances from which the outflows originate increase with AGN luminosity, indicating that more luminous AGN may have the potential to provide negative feedback required for bulge quenching. These results will provide significant constraints on the outflows in high redshift active galaxies, which may dominate feedback in the early universe, and for which spatially resolved information can be obtained with upcoming JWST observations.
    16:20 Polack Determining the extents and Kinematics of Ionized Winds in Nearby AGN Outflowing radiation from supermassive black holes in the centers of active galaxies is postulated as a major contributor to galactic evolution. In an effort to explore the interaction between active galactic nuclei (AGN) and their host galaxies, we gather Hubble Space Telescope (HST) spectra and images of nearby (z < 0.1) active galaxies to quantify the extents and kinematics of their narrow-line region outflows. We present results for nine AGN that were recently observed with HST to obtain continuum and [O III] imaging that match existing long-slit spectra from HST's Space Telescope Imaging Spectrograph (STIS). We measure the spatially-resolved outflow velocities and build kinematic models to determine the deprojected distances and velocities of the outflowing gas. Our kinematic analysis will be used to accurately measure the outflow properties, including mass outflow rates and kinetic luminosities, as a function of distance from the nucleus. For each galaxy, these parameters will provide the locations and amounts of energy deposited into the gas. It will also provide direct measurements of the depletion of stellar gas reservoirs, establishing a possible connection between AGN activity and galaxy evolution.
    16:40 Rodriguez-Ardila Using the Optical/NIR Coronal Lines to Measure the Kinematics of the Extended X-ray Emission The fundamental nature and extent of the coronal line region (CLR) in Active Galactic Nuclei (AGN) are open questions despite decades of research. In this work, we discuss recent results on this matter. In particular, we study the CLR in a sample of seven radio-weak bona-fide active galactic nuclei by means of IFU MUSE and SINFONI spectroscopy. We found that the [FeVII] 6087 Ang line (IP 99 eV), one of the brightest coronal line (CL) observed, extends to distances of up to 2 kpc from the central source. Higher ionization CLs such as [SiVI] 1.963 microns (167 eV), [FeX] 6374 Ang (262 eV), and [ArX] 5538 Ang (422 eV) are detected as far as 0.5 kpc from the central engine. These results allow us to set new limits to the size of the coronal line region in AGN. We found in all cases that the high-ionization gas is strongly aligned to the radio-jet and is kinematically perturbed, with splitted line profiles suggesting gas in expansion, decoupled from galaxy rotation. Blue- and red-shifted gas with velocities reaching ~400 km/s in excess of the systemic are measured, indicating that this gas is likely outflowing. Moreover, the coronal gas morphology and extension coincides with that of the extended X-ray emission. Models combining photoinization by the central source and shocks confirm that the extended coronal emission gas is mostly shock-driven. We derive pre-shock gas densities in the range 100 - 300 cm-3, gas temperatures of up to Te ~ 30000K and shock velocities of ~400 km/s, in agreement to the values derived from the observations.This last result is particularly relevant, as very recently Trindade Falcao et al. (2022) showed that CLs from ions with ionization potential greater than or equal to that of O VII, i.e. 138 eV, trace the footprint of X-ray gas. Therefore, CLs can be used to measure the kinematics of the extended X-ray emitting gas at the spectral resolution dictated by optical/NIR spectrographs. In this respect, coronal lines allow us to study the highest-excitation component of the AGN, at spectral and spatial resolutions not yet possible using X-ray observations.
    17:00 Shea Kinematic Maps of the Ionized Gas in Stephan’s Quintet and its Active Galaxy NGC 7319 Compact galaxy groups are the ideal laboratory for studying the effects of AGN gas outflows on multiple galaxies and the circum-galactic medium (CGM). Recent JWST observations of the nearby compact group known as Stephan’s Quintet highlight tidal flows between the interacting galaxies, particularly in the vicinity of the active galaxy NGC 7319. We present a spatially resolved kinematic analysis of the ionized gas in the extended narrow line region (NLR) of NGC 7319 and its surrounding tidal structures. We obtained spatially resolved spectra from Apache Point Observatory‚Äôs Kitt Peak Ohio State Multi-Object Spectrograph (KOSMOS) at multiple slit position angles, including the major and minor axes of the galaxy. We fit multiple Gaussian components to the [O III] 5007 and H-alpha emission lines to measure the velocity centroid, full width at half maximum (FWHM), and integrated flux of each kinematic component as a function of position along each long slit. Our goal is to disentangle the kinematics of outflows, rotation, tidal flows, and inflows in order to better understand the feeding and feedback processes in nearby compact groups.
Wednesday, June 14th

  • Session 4 - Driving Mechanisms

    Time Name Title
    Chair: Mitchell Revalski
    9:00 Elvis AGN Feedback Mechanisms Imaged by Chandra: Winds, Jets, and Radiation AGN feedback requires coupling of the power output of the accreting SMBH with the host galaxy ISM, to unbind it from the galaxy or at least to disrupt the molecular clouds in which star formation will occur. Three forms of coupling are possible: direct radiation, impact of relativistic jets, or impact of a wider-angle wind. Direct high resolution imaging of the inner kpc of AGN host galaxies in X-rays with Chandra now encompasses over 2 dozen cases (Fabbiano and Elvis 2023, arXiv:2202.13803). In about half the objects, deep exposures provide detailed mapping. As a result, we see all three possible mechanisms for feedback on the host ISM at work. We will describe some particularly clear cases. MRK 78 illustrates wind deposition of energy, but not radiating where it was expected (Fornasini et al., 2022, arXiv:2204.13140). NGC 1167 (Fabbiano et al., 2022 arXiv:2209.02549) for a radio jet impacting molecular clouds, and IC5063 (Travascio et al, 2021, arXiv:2107.12403) for radio jet material heating and pushing ISM out of the galaxy disk plane. For radiation, ESO 428-G014 (Fabbiano et al., 2017, arXiv:1705.10680, 2018, arXiv:1811.06436) shows nuclear irradiation of molecular clouds in the most. We will discuss the relative importance of these and other cases where feedback is seen directly.
    9:20 Dannen On the Efficiency of Driving Winds Due to Gas, Radiation, or both Observations of ionized AGN outflows have provided compelling evidence that the radiation field transfers both momentum and energy to the plasma. At parsec scale distances in AGN, energy transfer can dominate, in which case the only force needed to launch an outflow is due to gas pressure. Much closer to the black hole, gravity dominates thermal energy due to insufficient heating by the radiation and the gas is in the so-called 'cold wind solution' regime. Only magnetic or radiation forces can lead to outflow, but it is unclear how these forces depend on the spectral energy distribution (SED) and the gas ionization state. To accurately compute the radiation force, it is still necessary to know the gas temperature. To better understand how SED affects the efficiency of line driving, we survey the parameter space of radiation forces due to spectral lines resulting from blackbody SEDs with temperatures ranging from $2\times 10^4$~K to $10^6$~K, while also self-consistently computing the heating and cooling balance to estimate the temperature. Our main finding is a quantification of how the wind properties depend on the assumed SED and the key parameters characterizing the wind base. Our findings also show that for some SEDs, as this ratio increases the wind weakens but still reaches a steady state, but for other SEDs, namely our high temperature black body SEDs, the wind can become variable as that ratio becomes comparatively large. We discuss the physics behind this qualitative change in the wind’s behavior.
    9:40 Proga Physics of clumpy ionized winds in AGN Large-scale mass outflows from AGN provide a natural link between a galaxy and its central black hole. This link is likely a very efficient mode of the so-called AGN feedback. However, quantifying AGN feedback is very challenging because one has to account for multi-dimensional fluid dynamics, energy dissipation, radiative processes, effects of dust, magnetic processes etc. In other words, studies of AGN feedback require incorporation of processes and their interplay that are typically considered separately in specialized areas of astrophysics. For example, the mechanism of thermal driving for launching accretion disk winds is interconnected with classical thermal instability (TI). We recently demonstrated that as a result of this interconnectedness, radial wind solutions of X-ray heated flows are prone to becoming clumpy. However, in over two decades of numerical work, only smooth thermally driven disk wind solutions that approach a steady state have been found. Although smooth solutions are easier to model and analyze they are likely more difficult to test against the observations. In this talk, I will summarize the main results from Dannen et al. (2019) and Waters et al. (2021, 2022), where we investigated the stability of thermally driven disk winds. In particular, I will discuss the following three issues: (i) The physical conditions under which TI should accompany thermal driving, resulting in clumpy disk wind solutions; (ii) The reasons for why in disk winds, TI seeds the formation of hot spots in the disk atmosphere that consequently produces large scale vortices and results in the continual production of characteristic cold phase structures that we refer to as irradiated atmospheric fragments (IAFs). (iii) Observational consequences of IAFs. Specifically, I will show that X-ray absorption lines can reveal this complicated dynamics through spectral signatures such as a less sudden desaturation of O VIII Lyα and multiple absorption troughs in Fe XXV Kα.
    10:00 Dyda Time Dependent Line Driven Disc Winds - X-ray Irradiation Line driving is a promising explanation for AGN winds as it provides both a launching mechanism and an explanation for the absorption and emission lines in spectra. As the community moves towards multi-wavelength and multi-epoch observations, our modeling of AGN systems must likewise follow suit to leverage these new capabilities. For line driving to be a viable acceleration mechanism two conditions must exist in the wind 1) The gas must be sufficiently, though not overly ionized by soft X-rays, so that the gas can interact with the UV 2) The UV flux incident on the gas must be high enough to transfer sufficient momentum to overcome gravity. We present novel simulations of AGN disc winds using time-dependent, multi-frequency radiation hydrodynamics focusing on the problem of gas ionization, where we model both the X-ray and UV radiation fields. We consider a suit of models for gas/X-ray interactions and identify the conditions on scattering and absorption opacities where wind self-shielding can operate and allows line driving to launch and robustly accelerate winds.
    10:20 Coffee
    10:40 Fukumura Emission Features Characterized by AGN Disk Winds AGN winds originating from accretion disks have been manifested in the form of characteristic absorption features in UV/X-ray band. While its launching mechanisms are yet to be observationally constrained, the same disk wind can also imprint a unique signature in the continuum and emission components from the disk through significant scattering depending on the wind's physical condition and geometry at large scale. We propose a scenario in which the disk wind of parameterized characteristics reprocesses X-ray photons (e.g. Fe K lines and soft excess). We show in our proof-of-concept calculations that Comptonization within a wide-open wind over extended distances such as magnetically-driven winds can potentially distort locally emitted features by reddening. Such Comptonization could be a necessary consequence by the presence of powerful disk winds in AGNs.
    11:00 Soliman Dust in the AGN Wind The dusty AGN torus represents one of several natural locations where radiation pressure from bright AGN should drive strong outflows. Most theoretical work on this topic assumes that the dynamics of the dust within the torus are perfectly coupled to that of the surrounding gas. However, in this environment, the dust and gas experience different forces which could act to decouple their dynamics. Further, it has been shown that when different forces act on the dust versus the gas, the fluid is generically unstable to a class of fast-growing resonant drag instabilities (RDIs). Idealized simulations have shown that RDIs drive clustering in the dust and gas and could induce dust-gas separation, generating low opacity regions. Therefore, the presence of RDIs could influence whether outflows launch from the torus, contribute to torus clumpiness, and help explain some cases of AGN time variability. To address these questions, I will present the first set of numerical simulations of radiation driven outflows that explicitly evolve dust dynamics in conditions resembling AGN winds. We find that the RDIs develop rapidly giving rise to filamentary structures within the outflow on box-size scales (~ a few parsecs) with strong dust clumping and super-alfvenic velocity dispersions on micro-scales. In turn, this drives 10-20% fluctuations in dust opacity and gas column density, integrated along mock observed lines-of-sight to the quasar accretion disk, over year to decade timescales with a red-noise power spectrum as commonly observed for AGN. Additionally, our simulations show that the radiation is sufficiently coupled to the dust-gas mixture launching highly super-sonic winds with less than a factor of ~ 3 photon momentum loss relative to the ideal case. Therefore, the RDIs could play an important role in generating the clumpy nature of AGN torii and driving AGN variability consistent with observations.

  • Session 5, Part 1 - Radio Mode Outflows

    Time Name Title
    11:20 Daly New Black Hole Spin Values for Sgr A* Spin energy is a key parameter describing astrophysical black holes since it contributes in part to the total (dynamical) black hole mass and can be extracted, thereby impacting the black hole environment. A new method to empirically determine the spin mass-energy characteristics of black holes will be presented. The method will be applied to a sample of 100 supermassive black holes associated with classical double radio sources with redshifts between about zero and two and includes four different types of AGN as defined by their nuclear spectroscopic properties. An analysis indicates that about two-thirds of the supermassive black holes are maximally spinning, while one-third have a broad distribution of spin values. The new method will be applied to obtain both the spin mass-energy contribution to the total black hole mass and the mass-energy that is available for extraction from each black hole. The total energy output in the form of jets per outflow event will be compared with the spin energy available and with the dynamical black hole mass, and the rather surprising results will be discussed. The new method has broad applications for astrophysical black holes.
    11:40 Borkar Feeding AGN in the presence of strong Feedback: The Case Study of Centaurus A AGN feedback plays a crucial role in the growth of supermassive black holes. By injecting a vast amount of energy in the form of intense radiation, jets, and outflows, the surrounding gas is heated and pushed away from the vicinity of the black hole. So how can the SMBH continue to feed and grow in the presence of strong feedback? To investigate this, I will present our multi-wavelength analysis of the closest radio-loud AGN with a prominent radio and X-ray jet, Centaurus A. We combine high-resolution ALMA and Chandra observations to study the circum-nuclear region of the source, focusing on the inner ∼200 parsec. The observations confirm the presence of hot and cold gas phases in the form of a hot X-ray emitting plasma surrounded by a cold CO-emitting molecular disc. To understand the interaction between the incident radiation and the surrounding circum-nuclear medium, we used the spectral synthesis code Cloudy to perform photoionization calculations of the transfer of radiation through the matter for a wide range of temperature, density and irradiating spectral shapes. We show that the thermal instability arising from the interaction between the high-energy radiation from the nucleus and the ambient gas and dust naturally explains the observed multi-phase medium. Efficient cooling of the gas allows clouds of cooler gas to co-exist within the hot plasma, which eventually fall towards the center, feeding the AGN. Colder dusty molecular clouds have to exist away from the hot region to survive, correctly reproducing the ALMA and Chandra observations. Our work highlights the importance of thermal instabilities within the framework of black hole growth in the presence of strong feedback.
    14:00 Excursions
Thursday, June 15th

  • Session 5, Part 2 - Radio Mode Outflows

    Time Name Title
    Chair: Anna Trindade Falcao
    9:00 Ulivi Outflows and feedback in jetted AGN Powerful and extended radio jets are believed to play a fundamental role in AGN feedback but recent works suggest that also low-power (<10^45 erg/s) jets may have a significant impact on their host galaxies. We aim to investigate the relationship between radio jets and host galaxies in order to identify a new potential mechanism of AGN feedback. We extended the seminal work by Venturi et al., 2021 that found a turbulent, high velocity dispersion gas in the direction perpendicular to low-radio jet emission, at higher jet luminosities. We selected four luminous type-II AGN with a moderate powerful radio jet (10^44 erg/s) observed with the Multi Unit Spectroscopic Explorer (MUSE) at the VLT, to analyze the properties of the extended ionized gas in these systems, employing the high spatial resolution of new generation integral field data. We detected ionized outflows extended over kiloparsec scales aligned with the direction of the jet. We also detected a strong enhancement in line-emission velocity dispersion perpendicular to the radio jets and found a correlation between the mass and the energetics of the high velocity dispersion gas and the power of the radio jet, supporting that jets may be responsible for the enhancement of turbulence and could represent a significant mechanism of AGN feedback in luminous sources. This phenomenon, being observed in a growing number of objects, could potentially represent an important additional channel of AGN feedback to be taken into account.
    9:20 Chen Radio probes of AGN winds in radio-quiet AGN The AGN wind interaction with the host interstellar medium likely produces radio synchrotron emission through shocks and particle acceleration, and it may dominate the observed radio emission in radio-quiet (RQ) AGN. High-resolution radio observations can be used to probe the AGN wind down to mas scales. We present new VLBA observations at 1 and 5 GHz for a representative sample of 18 nearby (z < 0.5) RQ AGN, which is drawn from the Palomar-Green sample and covers a wide range of luminosity and black hole mass. In most objects (12/18) we detect a compact optically thick (flat spectrum) radio core, which can reach a high brightness temperature (> 10^7 K), is consistent with the Gaia position, and likely resides at the physical center of the AGN. Seven objects show extended emission, which is generally optically thin (steep spectrum), displaces from the AGN center, and has a low brightness temperature (< 10^7 K). The extended emission may be associated with an AGN driven wind. Since the extended emission dominates in high Eddington ratio objects, it may be associated with a radiation pressure driven wind. Our additional VLBI, e-MERLIN, and GMRT observations, and future VLA, NOEMA, and ALMA observations of the extended emission may provide additional evidence for the interaction between the AGN wind and the ambient medium, and possibly show the AGN feedback in action.
    9:40 Hlavacek-Larrondo Novel observations of the multiphase gas in the Perseus cluster of galaxies The Perseus cluster of galaxies is the archetype of radio-mode black hole feedback. It is the most extensively studied galaxy cluster in the literature and has been observed at all wavelengths, providing the best laboratory to understand the complex interactions between an AGN and the hot X-ray emitting IntraCluster Medium (ICM). Its central dominant galaxy, NGC 1275, is surrounded by a giant multiphase nebula that spans the inner 100 kpc. The fractal tendrils of this nebula are made of soft X-ray emission, cold and warm molecular gas, as well as ionized optical gas. Such nebulae have been interpreted as a telltale sign of atmospheric cooling, connecting the large scale ICM to the micro-physics occurring near the black hole, as these nebulae condense and clouds rain back down onto the black hole, re-igniting the feedback cycle. Here, we present state-of-the-art optical imaging Fourier transform spectroscopic observations of the Perseus cluster from SITELLE/CFHT that cover the entire 100 kpc nebula at high-spectral resolution (R=7000). These data reveal in entirety the kinematical structure of the multiphase gas at optical wavelengths. Crucially, they show for the first time that radio jets can lead to the multiphase nature of the ICM. They also reveal the presence of a widely-spread component of the multiphase gas that is remarkably quiescent with a low and uniform velocity dispersion. The uniformity of the velocity dispersion is puzzling given that NGC 1275 hosts multiple epochs of radio jets, shock fronts and star formation. These phenomena are thought to impact strongly the surrounding gas, and thus the ICM, yet here, the ICM retains a uniformly low velocity dispersion out to large radii. We also compare the SITELLE maps to recent Hitomi measurements of the X-ray gas (and eventually XRISM), enabling us to better understand the heating and cooling mechanisms of the hot ICM.
    10:00 Jimenez-Gallardo A Chandra-MUSE view of feedback in powerful radio galaxies Interactions between radio galaxies and their large-scale environments are key factors in the feedback processes responsible for triggering and fueling AGN activity. To improve our understanding of such interactions, we carried out a multi-frequency analysis based on the comparison of Chandra and VLT/MUSE observations of radio galaxies in the Third Cambridge Catalog. I will focus on the results on 3CR 196.1, the potential first detection of an ionized gas bubble filling an X-ray cavity. I will discuss the implications of such a bubble and the different feeding/feedback features found surrounding 3CR 196.1, which make it a prime example of the interplay between the multiphase gas haloes surrounding radio sources and their radio jets. Lastly, I will present our preliminary results on the optical-to-X-ray comparison of a sample of 3CR radio galaxies. Apart from showcasing the morphological link between their extended X-ray and optical emission, sources with the same ionization status also display approximately constant X-ray to optical flux ratios. This result points to a different origin of the ionized gas surrounding radio galaxies as a function of their excitation status and supports the scenario in which the excitation status of radio sources is determined by their accretion material.
    10:20 Deconto-Machado Outflows and winds in high-luminosity and high-redshift radio-loud quasars Outflows and winds seem to be a ubiquitous feature in Active Galactic Nuclei (AGN). Especially at high and intermediate redshift, many sources seem to harbor a powerful central mechanism that allows for strong jets in radio and/or winds observed in the optical and UV ranges of their spectra. Through the decomposition of the broad emission line profiles, we can find some hint of the relevance of winds for the structure and dynamics of the broad line emitting regions. Feedback contributions can be estimated through the decomposition of the broad emission line profiles from quasar spectra and high-ionization lines such as CIV λ1549 and [OIII] λ4959,5007. High-ionization lines usually present a significant asymmetry towards the blue especially in radio-quiet sources that is strong evidence of outflow motions. At variance, radio-loud quasars tend to present modest blueshifted components. The strongest radio emitters are also found with more symmetric emission line profiles in both UV and optical ranges. In this work, we present a remarkable sample of 32 high-luminosity and high-redshift quasars (z = 1.5 – 3.7) observed with ESO-VLT. We present a dedicated analysis of the radio-loud sources in this sample. Measurements are shown and contextualized taking advantage of a set of correlations associated with the quasar Main Sequence (MS), which consists of a parameter space that allows to connect observed UV, optical, and X-ray properties to the relative relevance of radiative and gravitational forces. We discuss the main differences found in accretion and feedback properties and highlight the effects of the radio-loudness on the emission line properties.
    10:40 Coffee
    11:10 Fischer Let's talk about jets: Origins of radio emission in NGC 1068 We present multi-epoch VLBA interferometry and multi-wavelength HST imaging to study the characteristics of the extranuclear radio emission in prototypical Seyfert 2 NGC 1068. From our recent studies, we have noted that radio structures in previous analyses of radio-quiet AGN align and intertwine with their optical Narrow-Line Regions (NLRs), which represent the intersection between AGN ionization and host galaxy disk material. We hypothesize that radiatively-driven winds, launched from small radii, impact dense gas lanes at larger distances and produce shocks, with relativistic particles accelerated in the shocks in turn producing localized synchrotron radio emission similar to processes in supernova remnants. In this scenario, the observed radio emission is then a byproduct that occurs only at locations where winds are producing shocks in the radio-quiet AGN host galaxy. As this hypothesis lies in tension with the standard paradigm of radio structures in AGN, we present further testing on the radio structures observed in NGC 1068 to provide evidence for this scenario on how AGN produce feedback and interact with the interstellar medium in their host galaxies.

  • Session 6 - Large Scale Winds and Feedback

    Time Name Title
    11:30 Ramos-Almeida Investigating the impact of quasar feedback on the central kiloparsecs of galaxies. Different modes of AGN feedback, which can be broadly divided into radiative/quasar and kinetic/radio, are now considered key processes in the evolution of massive galaxies by regulating black hole and galaxy growth. Indeed, a wealth of observational evidence demonstrates that feedback from supermassive black holes impacts the galaxies and the haloes they inhabit on a wide range of scales: from the central parsecs to hundreds of kpc. What we are still far from understanding is how AGN feedback couples with the host galaxy, which is what ultimately determines its efficiency. The aim of the Quasar Feedback (QSOFEED) project is to answer this question by quantifying the impact of multi-phase quasar-driven outflows on the nuclear regions of galaxies, which have the same dynamical timescales as AGN activity and the outflows that it drives. In this talk I will present recent results from the project based on high angular resolution data from cutting-edge telescopes including Keck, Gemini, and ALMA. We do not find evidence for a significant impact of quasar-driven winds on the total molecular gas reservoirs and star formation rates, but they are undoubtedly modifying the distribution of cold molecular gas and young stellar populations (ages < 100 Myr) in the central kiloparsec of the galaxies.
    11:50 Fujita AGN winds as the origin of the Fermi bubbles The Fermi bubbles are large gamma-ray-emitting structures. They are symmetric about the Galactic Center (GC), and their creation is therefore attributed to intensive energy injection at the GC. In this talk, I indicate that the Fermi bubbles are a nearby example of AGN winds. I focus on the non-equilibrium X-ray gas structures associated with the bubbles. I find that a combination of the density, temperature, and shock age profiles of the X-ray gas can be used to distinguish the energy-injection mechanisms. By comparing the results of numerical simulations with observations, I show that the bubbles were created by a fast wind from the GC because it generates a strong reverse shock and reproduces the observed temperature peak there. On the other hand, instantaneous energy injection at the GC cannot reproduce the temperature profile. The wind had a speed of ~1000 km s^-1, and blew for ~10^7 yr. Because the mass flux of the wind is large, the entrainment of interstellar gas by wide-angle outflows from the black hole is required. Thus, the wind appears to be the same as AGN winds often observed in other galaxies.
    12:10 Dall’Agnol de Oliveira Cold molecular gas outflow encasing the ionized one in the Seyfert galaxy NGC 3281 We present ALMA CO(2-1) observations of the Seyfert 2 galaxy NGC 3281 at ~100 pc spatial resolution. This galaxy was previously known to present a bi-conical ionised gas outflow extending to 2 kpc from the nucleus. The analysis of the CO moment and channel maps, as well as kinematic modelling reveals two main components in the molecular gas: one rotating in the galaxy plane and another outflowing and extending up to ~1.8--2.6 kpc from the nucleus, partially encasing the ionised component. The mass of the outflowing molecular gas component is M_{out,mol} = (2.5 ± 1.6)x10^6 Msun, representing ~1.7--2 % of the total molecular gas seen in emission within the inner 2.3 kpc. The corresponding mass outflow rate and power are Ṁ_{out,mol} = 0.12--0.72 Msun/yr and Ė_{out,mol} = (0.045--1.6) x 10^{40} erg/s, which translates to a kinetic coupling efficiency of only 0.0001--0.02 %. This value reaches up to 0.1 % when including both the feedback in the ionised and molecular gas, as well as considering that only part of the energy couples kinetically with the gas. Some of the non-rotating CO emission can also be attributed to inflow in the galaxy plane towards the nucleus. The similarity of the CO outflow -- encasing the ionised gas one and the X-ray emission -- to those seen in other sources, suggests that this may be a common property of galactic outflows.
    12:30 Lunch
    Chair: Travis Fischer
    13:40 Kakkad Ionized gas winds from X-ray AGN and their impact on molecular gas and star formation AGN play a crucial role in regulating star formation in their host galaxies, primarily through accretion-driven outflows or energy injection from radio jets. Integral Field Spectroscopy (IFS) has been instrumental in characterising outflows in the ionised and warm molecular gas phase, and assessing whether they trigger or suppress star formation. In this talk, I will present the results from recent VLT/MUSE and VLT/SINFONI IFS surveys of X-ray AGN host galaxies at low and high redshift. I will begin by demonstrating how radio jets contribute to driving outflows from regions near the AGN, using recent parsec-scale MUSE observations of the Circinus galaxy. Additionally, I will describe how we characterise the conditions within an outflow, such as electron density, to obtain accurate estimates of the outflow's kinetic power for a large sample of galaxies at both low (z~0.1) and high (z=2.4) redshift. These outflow properties exhibit a strong correlation with the AGN bolometric luminosity at all redshifts, with the strongest coupling observed in regions close to the AGN. In conclusion, I will discuss recent findings from ALMA that indicate a lower molecular gas content in AGN host galaxies compared to mass-matched normal star-forming galaxies, suggesting a negative feedback mechanism at work. Moreover, I will demonstrate how outflows in some galaxies suppress star formation, as traced using H-alpha emission. However, such negative feedback scenarios are not widespread in most galaxies. Overall, AGN play a crucial role in regulating star formation in their host galaxies, and multi-wavelength techniques provide a powerful tool to better understand their mechanisms and effects.
    14:00 Rojas Lilayu The relation between ionised outflows and molecular gas content in nearby X-ray AGN using MUSE and ALMA An open question in extragalactic astronomy is what is the extent to which the Active Galactic Nuclei (AGN) affect the evolution of their host galaxies. Proper characterization of the AGN influence becomes necessary for cosmological hydrodynamical simulations that invoke feedback from these AGN to realistically simulate galaxy growth and evolution. AGN-driven outflows are frequently detected in low-redshift and high-redshift galaxies across a wide range in luminosity and multiple gas phases. However, most of the samples considered by these studies are incomplete as often only bright AGN are considered and the samples are biased against absorption in the optical/soft X-ray band. Therefore, it has been difficult to place the outflow signatures of galaxy populations in the context of both obscured and unobscured AGN. In this study, we present recent MUSE and ALMA CO (2-1) observations of nearby hard X-ray selected AGN, derived from the BASS survey. The AGN sample covers a large range in bolometric luminosity, black hole mass and Eddington ratio and therefore, allows us to perform an unbiased statistical study of outflows and their impact on host galaxies, namely star formation rate and the molecular gas content. We find kpc-scale ionized outflow signals in all galaxies and substantial amounts of molecular gas in their central regions distributed in a compact disk or ring-like structure. We will show if the presence of AGN results in a negative or positive feedback by investigating a systematic difference in the star formation efficiencies between the regions close to the AGN and regions further out in the disk. We will conclude by presenting relations between the AGN luminosity, outflow power with molecular gas content and star formation rate of the host galaxy determined using ancillary multi-wavelength data and advanced SED models.
    14:20 Glikman Dusty AGN-Driven Winds as a Mode of Feedback in Red Quasars Quasar activity plays an important role in regulating how galaxies and their nuclear supermassive black holes grow and co-evolve. The population of highly luminous dust-reddened quasars may be the key to understanding this co-evolution. Luminous quasars are thought to be ignited by major mergers between gas-rich galaxies and red quasars are among the most intrinsically-luminous quasars in the Universe representing a short-lived phase in the lifetime of a quasar, during which their energy output (feedback) irrevocably impacts their host galaxies. Broad absorption line features in the spectra of red quasars are extremely common and recent evidence has also shown that red quasars have enhanced radio emission, which may be explained by dusty, radiation-driven winds. Red quasars are thus ideal laboratories for addressing fundamental questions on the co-evolution of black holes and their host galaxies as well as the physics of feedback. I will present findings from several surveys that are exploring this elusive population to investigate dusty winds as a form of feedback and a source of radio emission.
    14:40 Haidar Dust in the Wind: A JWST/MIRI survey of polar outflows in nearby Seyfert galaxies A surprising result from mid-infrared (MIR) interferometry of nearby active galactic nuclei (AGN) is that a major fraction of the pc-scale dust emission is elongated in the polar direction perpendicular to the accretion plane. This has spurred a new paradigm for the nuclear structure, where a dusty conical wind, launched from the inner edge of classical torus, carries a substantial outflow of material into the interstellar medium. I will report on a Cycle 1 JWST/MIRI imaging programme undertaking a detailed multi-band study of a carefully-selected sample of nearby Seyfert AGN that have prior evidence for extended dust emission from ground-based observations. Thanks to our international team, the Galaxy Activity, Torus and Activity Survey (GATOS), these Seyferts have a wealth of high-resolution multi-wavelength ancillary data offering a wide range of gaseous and stellar tracers. Our team is also undertaking advanced PSF modelling for JWST observations, a crucial component in the quest to unveil the polar dust structure at the smallest-resolvable scales. I will discuss key results from two AGN that have been studied in detail: ESO 428-G14 and NGC 5728. These demonstrate the first solid evidence for AGN-driven polar dust emission. The superb resolution, sensitivity and PSF stability of JWST allows us to measure the size and shape of this polar dust, explore its composition, and directly trace its interaction with neighboring gas, zooming in on the sites of feedback in action. Our study is providing new insights on the properties of these outflows, their effect on the circumnuclear ISM, and on the detailed astrophysics underlying AGN feedback from cool winds.
    15:00 Coffee and Poster Viewing

    (1) Boissay-Malaquin
    • Title: Investigation on the Narrow Line Seyfert 1 Mrk 335 in an intermediate state, with Chandra/HETGS, NuSTAR and NICER
    • Abstract: The Narrow Line Seyfert 1 Mrk 335 has been observed in X-rays since 2000 and has shown to be highly and rapidly variable in flux and spectral shape, due to changes in the structure of the hot corona responsible for the primary X-ray emission via Comptonization. Its complex X-ray spectrum presents interesting features that need to be investigated in different states. While several studies have already been performed in low-flux states and during flares, we focus here on the intermediate-flux state, where previously detected warm absorbers are expected to be more easily detectable. After spending two years in a historically long low-flux state, the source finally became brighter in June-July 2020. On this occasion, we performed simultaneous observations of Mrk 335 with NuSTAR, NICER, and first the first time, Chandra/HETG. We present here our preliminary results regarding the use of NuSTAR observations to constrain the continuum, reflection properties and the broadened Fe-K line, the need for the high-resolution of HETGS to get information on the absorbers structures, and the value of NICER to study the strong soft excess.


    (2) Hoffman
    • Title: A Deep Chandra HETG study of MCG-6-30-15 Ionized Outflows: Developing a Robust Bayesian Framework
    • Abstract: Ionized outflows from Active Galactic Nuclei (AGN) have strong potential to explain the underlying mechanisms of galaxy-AGN co-evolution. Studying these outflows requires careful statistical analysis of absorption lines in the X-ray band to capture winds at their origin. Typical investigations of these high-resolution X-ray spectra are not yet optimized to extract the full potential of the data. Therefore new approaches to analyzing archival or future observations from instruments like Chandra's High Energy Transmission Grating (HETG) and the X-ray Imaging and Spectroscopy Mission (XRISM’s) microcalorimeter Resolve can yield crucial progress. In this poster, I will present a new implementation of a significantly updated Bayesian analysis framework on archival, deep HETG MCG-6-30-15 data from 2000 (130 ks) and 2004 (520 ks). By utilizing Bayesian statistics and high-performance computing, this approach reduces bias in measurements of outflow properties by exploring the whole parameter space, performing agnostic model selection, and avoiding computing-related simplifications. Combined with a new generation of models, my results will yield the most robust constraints on properties and variability of outflows in MCG-6-30-15 to date. This will significantly improve our understanding of AGN winds and their role in galaxy evolution. The full potential of this approach will be enabled with the data from future X-ray missions such as XRISM (launch in 2023), Athena, and the Line Emission Mapper (LEM) X-ray Probe.


    (3) Li
    • Title: Density diagnostics of NGC 3783 warm absorbers using a time-dependent photoionization model
    • Abstract: Outflows in active galactic nuclei (AGNs) are thought to carry kinetic energy away from the central engine as a kind of feedback channel, impacting on their host galaxies. However, the distance of the outflowing wind is poorly constrained due to lack of direct imaging observations, which limits our understanding of their kinetic power and therefore makes the impact on the local galactic environment unclear. But once the density of the outflow is known, the distance can be derived from the ionization parameter measured based on the ionization states. We perform theoretical tpho calculations using a realistic spectral energy distribution (SED) with variability information and investigate the delayed state of the ionized plasma, which enable us to derive the density-dependent lag timescale and compare to the previous observations. We also compare tpho-delay method with metastable density method as well as the more accuracy UV observation to further constrain the density range of 10 X-ray WAs of NGC 3783.


    (4) Byun
    • Title: HST/STIS Observation of the Extreme UV Outflow of QSO B0254-3327B
    • Abstract: We have identified a broad absorption line (BAL) outflow in the HST/STIS spectrum of the quasar QSO B0254-3327B at velocity 𝑣 = −3200 km s−1. We identified ionic absorption lines such as Ne viii, Na ix, Si xii, and Ne v. Via measurement of the ionic column densities, photoionization analysis, and determination of the electron number density of the outflow, we found the kinetic luminosity of the outflow system to be ∼ 0.8% of the quasar’s Eddington luminosity, or ∼ 2.14% of the bolometric luminosity, leaving its ability to contribute to AGN feedback dependent on the theoretical model. We also examined the physical properties of the outflow of Q0254-334 along with previously studied extreme UV outflows, with a total sample of 29 outflow systems, finding a weak negative correlation between outflow velocity and distance from the central source.


    (5) Harrington
    • Title: Identifying UFOs in the COS FUV spectra of PDS 456
    • Abstract: We conduct a study of the quasar PDS 456 using COS FUV spectra from the Hubble Space Telescope. We explore the absorption troughs in 7 spectra over 4 different epochs and find two troughs that are potentially due to intrinsic Ly α absorption at 0.09c and 0.006c. These lines are clearly detected in the earliest epoch but are not detected in subsequent observations, which suggests that the presence of these troughs are intrinsic to the AGN due to their variability.


    (6) Patrick
    • Title: Exploring the Physical Properties of the Outflows of the Quasars 2MASSJ14025120 and PG1425+267
    • Abstract: We have determined the column densities and covering fractions for the observed outflows in each of the low-z quasars 2MASSJ14025120 and PG1425+267. For both objects, we find multiple kinematic components as detected by multiple blueshifted absorption troughs in either the C IV doublet (ll 1548, 1550) or the O VI doublet (ll 1031, 1037), which suggest multiple outflows. We use photoionization models based on the measured ionic column densities to determine the physical states of these outflows.


    (7) Terndrup
    • Title: Temporal variability in the high-velocity broad absorption lines of Markarian 231
    • Abstract: We present time-series optical and infrared spectra of the He I*, Na I and Ca II broad absorption lines (BALs) of Markarian 231, taken at intervals of 1-2 years over a decade. We see considerable variation some but not all velocity components, including the appearance and disappearance of some lines and approximately steady changes in the mean velocity of others. We use the temporal variations to test the conclusions in our earlier paper (Leighly et al. 2014, ApJ, 788, 123) about the characteristic size scales of absorbers in different regions of the outflowing gas.


    (8) Voelker
    • Title: Analysis of a Sample of High Redshift, High Luminosity FeLoBAL Quasars
    • Abstract: Quasars are particularly luminous Active Galactic Nuclei (AGNs). The light from the central engine is absorbed by gas in our line of sight, producing absorption lines in the spectra. By modeling these spectra, we can derive the physical parameters of the absorbing gas as well as the velocities of quasar outflows, which tell us how powerful the outflow is. FeLoBAL quasars contain high ionization and low ionization broad absorption lines as well as iron lines. Though FeLoBAL quasars comprise less than 2% of the quasar population, they can contain the most powerful outflows, which provide information about galaxy evolution and feedback.
      Our group models FeLoBAL quasars using the novel spectral synthesis code SimBAL, which uses Markov Chain Monte Carlo methods to fit a model to the spectra and derive the physical parameters of the absorbing gas from that model. Previously, our group has analyzed a selection of low redshift (0.5 < z < 1.5) quasars with a luminosity range of 45 < logLbol < 47.5 (Choi et al. 2022) and a selection of intermediate redshift (1.1 < z < 1.9) quasars (Voelker et al. 2022). Here, we expand our study to include a sample of high redshift (2.1 < z < 2.6), high luminosity (46.5 < logLbol < 47.5) quasars. As higher luminosity quasars are associated with faster outflows and higher redshifts allow us access to shorter wavelengths in the observed-frame optical spectra, we can obtain more information about quasar outflows and physical gas properties, including exploring the relationship between high ionization and low ionization lines in our spectra. Using SimBAL, we modeled our objects and extracted their physical parameters, including ionization and density, which we then compared along with the bolometric luminosity logLbol with the outflow velocity. We found that of the objects we currently have analyzed, high redshift objects have a greater percentage of powerful outflows (~77.3%) than the low and intermediate redshift objects (~36.6% and 50%, respectively). Additionally, we calculated the distance of each quasar’s outflow from its central supermassive black hole (logR). Preliminary results show that the high redshift objects appear to have powerful outflows distributed amongst a broad range of logR values (0.81 pc < logR < 4.21 pc), compared to the low redshift objects which occupy two main groups – high (logR > 2.90 pc) and low (logR < 1.09 pc) logR. There is additionally tentative evidence that the high-redshift sample may have a different distribution of ionization parameters and densities than the low and intermediate redshift samples.


    (9) Armah
    • Title: Oxygen abundance in the NLR of Seyfert galaxy and the metallicity-luminosity relation
    • Abstract: Gas-phase and stellar metallicities are observed to scale primarily with galaxy stellar mass and, as a result, with other integrated properties that scale with mass, such as luminosity in bands where old stellar population predominates. The mass–metallicity relation (MZR) has been found to exist for both gas-phase and stellar metallicities. Despite decades of research, which has undoubtedly established the MZR in H II regions and star-forming galaxies (SFGs), clear direct links between gas-phase metallicity (Z) and active galactic nuclei (AGNs) properties such as luminosity and accretion rate remain unclear. I will present the recent results obtained from the BASS survey from a large survey of 561 hard X-ray selected AGNs, measuring direct emission from the AGN which is unaffected by dust or contamination from SFGs, and is much less sensitive to obscuration in the line-of-sight as compared to soft X-ray or optical wavelengths, allowing a selection based on only the supermassive black hole (SMBH) properties.


    (10)Ferree
    • Title: Gas Outflow Kinematics in NGC 3516
    • Abstract: Previous analysis of the narrow line region of the Seyfert 1 galaxy NGC 3516 has found ambiguous evidence for outflows driven by the active galactic nucleus (AGN). While the extended ionized gas kinematics were found to be inconsistent with purely rotational motion, they were not positively identified as outflows. We present long slit spectroscopy from the Hubble Space Telescope’s Space Telescope Imaging Spectrograph (STIS) to further analyze the narrow line region in this galaxy. In particular, we fit the H𝛼, Hβ, and [OIII] narrow emission lines with multiple Gaussian components using the Bayesian Evidence Analysis Tool (BEAT). Our objective is to use this spectral analysis to separate AGN driven outflows from rotation in order to determine the extent of the outflows, ultimately creating a template to understand other active galaxies with ambiguous kinematics.


    (11) Gatto
    • Title: Ionized gas outflows vs. “maintenance mode" feedback in MaNGA AGN
    • Abstract: We present a study of the ionized gas kinematics of 297 Active Galactic Nuclei (AGN) host galaxies as compared to that of 537 control galaxies observed in the MaNGA-SDSS survey using measurements of the [O III]λ5007Å emission line profiles, fitted with one narrow and one broad component – found in 45% of the AGN. We present flux, velocity and W80 maps, comparing them between AGN hosts and controls. We identify ""kinematically disturbed regions"" (KDRs) within the Extended Narrow Line Region (ENLR) of the AGN, with W80 ≥ W80,cut = 315 km s^−1 the mean value for the controls plus its standard deviation. The median difference in the W80 values between AGN and controls is 238 km s^−1. We find a positive correlation between 〈W80〉 and L[OIII] for the AGN, but, inexpectedly, also for the control sample, that we attribute to a possible presence of faint AGN in the control galaxy sample. The extent of the KDR RKDR ranges from 1 to 10 kpc, with a mean ratio to that of the ENLR RENLR of 55%. We estimate the ionized gas mass in outflow (Mout) and the corresponding kinetic powers (Eout) assuming that the KDR is due to an AGN outflow. Using two methods to obtain the outflow velocity – one based on W80 and the other using the velocity of the broad component, we find mean values Mout,W80=1.87 ±0.98 ×10^−3 M yr^−1 and Mout,b=3.54 ±0.14 ×10^−3 M yr^−1 , and Eout,W80=1.70 ±0.71 ×10^38 erg s^−1 and Eout,b=4.51 ±0.13 ×10^38 erg s^−1. These values correlate with the AGN luminosity Lbol, populating the low luminosity region of this known relation and correspond to a coupling efficiency between the outflow power and AGN luminosity of 0.01% and lower. But the large extent of the KDR, in spite of this low coupling efficiency, show that even low-luminosity AGN can impact the host galaxy in a low, “maintenance mode"" feedback.


    (12) Kudoh
    • Title: Sub-parsec scale nature of AGN outflows in the radiation-hydrodynamic simulations
    • Abstract: The multi-phase gas outflows observed in active galactic nuclei (AGN) are important for understanding the supply onto the central supermassive black hole (SMBH). The driving mechanisms can be explained by the radiation force from the AGN luminous sources according to the simulation studies: (i) continuum for the dusty outflow (e.g., Wada 2012, 2015) and (ii) the lines for the ultrafast outflow (UFO; e.g., Nomura et al. 2020, Mizumoto et al. 2021). They successfully reproduced the velocity structure of the observed lines, but they focused on different scales and physical processes of the UFO launched from accretion disk (100 Rs) and the dusty wind formed in torus (1 pc ~ 10^6 Rs), respectively. Therefore, the questions are where do dusty wind come from and how do UFO propagate on a sub-pc scale? Our simulations for the dusty wind and UFO in AGN have been carried out with the computational domain with a dynamic range of 4 orders of magnitude (i.e. 10^2 -10^6 Rs). We have performed the axisymmetric 2D hydrodynamic simulations using the CANS+ code taking into account dust and radiation. The Eddington ratio expected from the gas entering a boundary radius varies with time. We adopted the radiation field and UFO dependent on the Eddington ratio inside this boundary. We found that outflow and inflow measured outside of the central boundary condition alternately increase and decrease on a yearly time scale. UFO is dominant above the angle of 40 degrees, measured from the equatorial plane, while the dusty outflow is around the disk surface. UFO contributes significantly to the variability of the column density. These outflows are expected to build the AGN gas structure and explain the absorbers and time-varying phenomena observed in X-rays.


    (13) Sadaula
    • Title: Modeling of Warm Absorbers in Active Galactic Nuclei.
    • Abstract: The nature of the extreme variability of the central ionizing source in active galactic nuclei (AGN) suggests that the outflowing gas may deviate from the commonly approached equilibrium approximation. Hence, we need to consider a time-dependent calculation to accurately describe the ionization states and the transmitted spectra. To see the effects of the source variability quantitatively, we carried out a time-dependent photoionization simulation by solving a time-dependent balance equation for level population, internal energy, and radiative transfer simultaneously and self-consistently and developed a time-dependent photoionization modeling code (TDP code). The outflows, which are responsible for the absorption of the X-rays, known as warm absorbers, are investigated using this newly developed TDP code for various sets of input parameters such as density, the shape of the incident light curve, SED, etc. We simulated the outflow for step and flare incident light curves and will present the results. In addition, we analyzed the high-resolution transmitted model spectra to understand how the ionization structure of the outflow changes over time. The study of the time-resolved spectra could be used in constraining the warm absorber properties such as density and, in turn, the location. This will help to understand the AGN feedback by estimating the kinetic power of the outflow.


    (14) Smith
    • Title: Position dependent radiation fields near accretion disks
    • Abstract: In the line driven disk wind model for active galactic nuclei (AGN) outflows, the high energy radiation poses a significant problem wherein the gas becomes overionized. The exact spectral energy distribution of an AGN is difficult to constrain through observations, because of variate uncertainties. But what is certain, is that the spectrum seen by a distant observer differs from the spectrum observed by a fluid element near the accretion disk which is the source of the radiation. In particular, the amount of ionizing radiation can strongly depend on the fluid element's position above the disk, so the problem of overionization could be less extreme than one would expect from observed spectra. We have developed a code to quantify this position dependence. Specifically, we compute energy distributions of the mean intensity and flux as well as energy integrated quantities such as mean photon energy. We find that the shapes of spectra vary significantly with position, and that the mean intensity spectrum is significantly softer than the radial radiation flux for certain positions near the disk. This result implies that the overionization problem is indeed less severe because the mean intensity controls ionization while the radial flux is the quantity closest aligned with the observed flux. The radiation flux is the source of the momentum needed for line driving, and we use the results of our calculations to compute the radiation force felt by a fluid element when given a velocity field and distribution of spectral lines. We explore the geometric effects of the disk on the radiation force in a vertical velocity field and find that, in opposition to a common assumption, the direction of the radiation force is not parallel with the flux. This misalignment of the force and flux is due to an additional geometric and frequency weighting of different parts of the disk imposed by the velocity field.


    (15) Souza de Oliveira
    • Title: Spatially resolved observations of outflows in the radio loud AGN of UGC 8782
    • Abstract: We use optical Integral Field Spectroscopy (IFU) to study the gas emission structure and kinematics in the inner 3.4×4.9 kpc^2 region of the galaxy UGC 8782, host of a radio loud Active Galactic Nucleus (AGN). The observations were performed with the GMOS-IFU on the Gemini North telescope, resulting in a spatial resolution of ∼ 725 pc at the distance of the galaxy (z = 0.045). While the stars present ordered rotation following the orientation of the large scale disc, the gas shows a disturbed kinematics. The emission-line profiles present two kinematic components: a narrow component (σ ≲ 200 km/s), associated with the gas in the disc of the galaxy and a broad component (σ ≳ 200 km/s), produced by gas outflows. Emission-line ratio diagrams indicate that the gas in the disc is excited by the AGN radiation field, while the emission of the outflow includes additional contribution of shock excitation due to the interaction of the radio jet with the environment gas. Deviations from pure rotation, of up to 30 km/s, are observed in the disc component and likely produced by a previous merger event. The broad component is blueshifted by ∼ 150 − 500 km/s relative to the systemic velocity of the galaxy in all locations. We construct radial profiles of the mass rate and kinetic power of the ionized gas outflows, which have the maximum values at ∼ 1 kpc from the nucleus with peak values of 0.5 ± 0.1 solar masses per year and (6.8 ± 1.1)×10^41 erg/s, respectively. The kinetic coupling efficiency of these outflows are in the range of 1–6 per cent, indicating that they could be powerful enough to affect the star formation in the host galaxy as predicted by theoretical simulations. This galaxy will be observed with JWST as part of a cycle 1 program (proposal ID 1928), together with NGC 3884 e CGCG-012-070. We also will present preliminary results on the gas kinematics of NGC 3884 e CGCG-012-070, that have been already observed with GMOS-IFU, in preparation for the observations. As our JWST observations are scheduled to be carried out from April onwards, we will possibly be able to show preliminary results based on data obtained with the NIRSpec and MIRI MRS instruments. We will be aiming at the characterization of the molecular gas distribution and kinematics in these galaxies, providing a complete census of their multi-phase gas outflows.


    (16) Frankel
    • Title: Molecular Inflows and Outflows of Gravitationally Lensed Quasar HS 0810+2554
    • Abstract: We present the Atacama Large Millimeter/submillimeter Array (ALMA) observations on the gravitationally lensed quasar HS 0810+2554, located at a redshift of z = 1.51. We analyzed the data from ALMA observations targeting three carbon monoxide transitions: CO(2→1), CO(3→2), and CO(5→4) using the Common Astronomy Software Applications (CASA) software and Python codes. A number of significant galactic molecular inflows and outflows were found in each transition. In total, 62 significant CO clumps were observed across the three transitions with velocities ranging from -2000 km/s to +3000 km/s. Based on the ALMA observations, the mass, mass outflow rate, radius, significance, and momentum of the outflows and inflows were calculated. Additionally, based on the location of clumps around the quasar, it can be concluded that they are not randomly distributed but rather trace some underlying structure within the galaxy. By mapping the molecular inflows and outflows of HS 0810+2554 and continuing with this research project, we hope to gain a better understanding of how active galactic nuclei (AGN) outflows influence galaxy evolution and to find a link between large-scale molecular outflows and small-scale relativistic outflows.


    (17) Kim
    • Title: GMOS-IFU survey of AGN-driven outflows: A lack of global/instantaneous AGN feedback based on outflow size and SFR
    • Abstract: Energetic gas outflow driven by AGN has been suggested as an effective mechanism of AGN feedback by sweeping up or heating the interstellar medium (ISM) in its host galaxy. However, direct evidence of star formation quenching is still missing. Therefore, it is essential to investigate kinematics, physical size, energetics of outflow, and more importantly, their connection with star formation. In this talk, we present the main results of our Gemini Multi-Object Spectrograph IFU (GMOS-IFU) survey of AGN-driven outflows and provide constraints on AGN feedback scenarios. We have observed 31 local AGNs (z < 0.3) with various outflow strengths and analyzed their spatially resolved emission line properties. Furthermore, we performed the spectral energy distribution fitting and determined the star formation rates (SFRs) based on the dust luminosity. We find that (i) [OIII] λ5007 line is blue-shifted at the central region, which can be interpreted as the approaching cone in the biconical outflow, while H𝛼 emission line follows host galaxy rotation; (ii) AGN photoionization is dominant at the central region, and it is often surrounded by LINER, composite or star formation in BPT map; (iii) Outflow size determined by kinematics correlates with the [OIII] luminosity, yet in general, it is not large enough (~ several kpc) to affect the ISM across the host galaxy; (iv) AGN hosts with strong outflows are still actively forming as many stars as normal star forming galaxies. Our results suggest that AGN feedback by ionized outflow is neither global nor instantaneous.


    (18) Marconcini
    • Title: MOKA3D: Innovative approach to 3D AGN outflow kinematic modelling: accurate determination of outflow physical properties
    • Abstract: The determination of outflow physical properties is important to assess the possible effects of Active Galactic Nuclei feedback on host galaxies and to compare observed outflow properties with model predictions. However, current estimates are based on simplified assumptions and do not take into account many observational aspects like projection effects and spatial resolution. I present MOKA3D , a novel method to model the kinematics and orientation of outflows, which is particularly successful in recovering the three-dimensional structure, even in the presence of observed clumpy emission and irregular kinematics. At variance with previous works, this model does not assume a distribution of the observed gas emission flux but uses a novel procedure to derive it directly from observations, reproducing a 3D distribution of the emitting clouds and providing accurate estimates of the outflows physical properties, e.g. the outflow and energy rate as a function of distance from the galaxy nucleus. I have successfully tested the performance of the method with both nearby Seyfert-II galaxies observed with the Multi Unit Spectroscopic Explorer at VLT and high redshift sources observed by JWST, showing that the very complex kinematical features observed can be ascribed to the clouds clumpiness in a very simple radial velocity field, accounted by a suitable geometry.


    (19) Vazquez
    • Title: A New Sample of Sub-kpc Dual AGN with Direct Keck AO Imaging
    • Abstract: Dual accreting supermassive black holes (SMBH) represent a very important yet elusive stage of galaxy evolution. These systems are very rare: of the few observed, the majority have spatial pair separations > 1 kpc, with only a handful observed with separations less than 1 kpc. These closely separated systems represent the most dynamically important stage of a galaxy merger. To assess the frequency and constrain the properties of these closely separated systems it is essential to build up a larger sample of sub-kpc dual candidates with direct high-resolution (sub-arcsecond) imaging. To address this challenge, we have developed a systematic pre-selection strategy that exploits both the Wide-field Infrared Survey Explorer (WISE) and the Sloan Digital Sky Survey (SDSS) and successfully recovers all known close dual AGN systems. Here I present resolved Keck AO imaging of (~0.2“ resolution) of sources selected by this method with nuclear separations less than 1 kpc. These closely separated duals span a largely unexplored region of parameter space and as such, they provide an excellent opportunity to constrain how often AGN are triggered in galaxy mergers, as well as the timescale over which the AGN activity is sustained. I will discuss new evidence for AGN feedback in this unique sample of sub-kpc duals based on multi-wavelength data and its potential impact on galaxy evolution.


    (20) Weiss
    • Title: Modelling Quasar Outflow Bubbles and Searching for Deceleration
    • Abstract: Quasar accretion disks often produce outflowing winds that are supersonic in the ambient interstellar medium (ISM). This may give rise to an expanding shockwave “bubble” structure of wind, shocked wind, and shocked ISM. This phenomenon could in turn play a role in AGN feedback and/or regulating accretion rates. Existing bubble models predict, for some reasonable parameter choices, that both the expansion and gas within decelerate as more ISM is swept up. We combine past models of spherically symmetric bubbles and discuss the limitations of the model given our assumptions. We then use new observations of SDSS J030000.56+004828.0 (J0300) to search for decelerating low-velocity Ca II absorption in the outermost region of the bubble. We place an upper limit of 1 km/s per rest-frame-year on any bulk acceleration or deceleration, translating to a (parameter-dependent) lower limit on the age of the outflow. Finally, we discuss the structure of the Ca II outflow in light of our results, the outflow's relatively low velocity, a recent analysis of J0300 placing the absorbing gas at a distance of ~12 pc (Choi et al. 2022), and the fact that the Ca II must be shielded from ionising radiation.
    15:40 Tozzi Galaxy-scale winds and their nuclear powering engine Outflows driven by active galactic nuclei (AGN) are widely accepted to play a key role in shaping the evolution of host galaxies, but their real impact on the host as well as their acceleration mechanism on galaxy scales are still debated topics. To shed light on this, it is crucial to carry out observations both locally, where the higher spatial resolution allows us a more detailed description of AGN winds, and at higher redshifts, with primary focus on the Cosmic Noon (z~2), where AGN feedback and outflows are expected to be more effective. With the aim of addressing these questions, I will describe the main properties and energetics of ionised outflows at z~2, also as a function of host galaxy properties (e.g. stellar mass, star formation rate), by presenting latest results from SUPER (a VLT/SINFONI Survey for Unveiling the Physics and Effect of Radiative feedback). Then, I will focus on the acceleration mechanism of AGN winds, particularly on X-ray ultra-fast outflows as the main nuclear engine powering winds on larger scales. I will indeed present results on galaxy-scale ionised winds detected in two nearby and two z~1.5 quasars (observed with VLT/MUSE and SINFONI, respectively), and show that our findings, along with observational results from the literature, overall support the existence of a strict connection between nuclear and large-scale AGN outflows.
    16:00 Winkel Tracing the onset of the AGN feeding-feedback cycle The host galaxy processes in many nearby, low-accretion active galactic nuclei (AGN) have been resolved down to pc scales. However, building up supermassive black holes (SMBHs) requires high accretion rates, a phenomenon for which the host galaxy conditions and associated timescales are largely unconstrained. Narrow-line Seyfert 1 (NLS1) galaxies are hypothesized to be archetypes of AGN at early stages of their evolution. In Winkel et al. (2022), we present VLT MUSE narrow field mode (NFM) observations of Mrk 1044, a nearby (80 Mpc) NLS1 that accretes at a super-Eddington rate. The unprecedented resolution of 80 mas (17 pc) allows us to trace the host galaxy ISM conditions and to resolve the circumnuclear star formation from 10 kpc galaxy scales down to the very central 30 pc. According to the Baldwin-Phillips-Terlevich (BPT) classification, star formation is the dominant ionization mechanism, even in Mrk 1044's nucleus. We detect a pc-scale, high density outflow that is present in [O III] emission and Ly-α absorption (Winkel et al. 2023). I will discuss the outflow origin, geometry and its potential future impact on the host galaxy star formation. The ISM structure on pc scales turns out to be complex, and established diagnostics such as the BPT diagram may not be applicable. Our single-case study demonstrates that resolving the AGN-host interaction on different spatial, time and density scales is crucial to understand black hole fueling and feedback in its complexity. In particular, the spatial scales to resolve compact AGN signatures are inaccessible at cosmic noon where the cosmic BH accretion rate peaked; young, powerful AGN may be blended with host galaxy star formation, potentially hiding the sites of SMBH growth.
    16:20 Raimundo Fuelling supermassive black holes with galaxy interactions Identifying black hole gas fuelling mechanisms is important to understand how supermassive black holes grow and what physical conditions favour the onset of black hole activity. However, it is challenging to find clear observational signatures of black hole fuelling. In this presentation I will show that galaxy interactions, such as major mergers, minor mergers or galaxy flybys, provide the necessary conditions to fuel black hole activity and growth. I will present a new method that uses kinematically misaligned gas to observationally identify galaxies that went through an interaction. With this method we have recently shown that galaxies that have misaligned gas have a higher observed fraction of AGN. This is the first time that an observational connection is seen between the process of formation and/or presence of misaligned structures and the fuelling of active supermassive black holes.
    16:40 Cresci Bubbles and outflows: the novel JWST/NIRSpec view of the z=1.59 quasar XID2028 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.
    17:00 Kazanas AGN MHD Accretion Disk Winds and their Relation to GBHB Phenomenology 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
    17:20 CONFERENCE PICTURE
    18:30 BANQUET (Crystal Ballroom)
Friday, June 16th

  • Session 7 - High Redshift Outflows

    Time Name Title
    Chair: Paola Rodriguez Hidalgo
    8:30 Feruglio Super massive black hole / host galaxy growth and the onset of strong feedback at z=6 - 7.5 The first quasars at the 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 present recent results, using ALMA, NOEMA and VLT observations, and synergy with JWST, 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~6-7.5.
    8:50 Bischetti Tracing black hole feedback at Reionization via broad absorption line quasar winds Luminous quasars are ideal targets to investigate the early growth phases of supermassive black-holes (BHs) and to understand when and how BH feedback started influencing the growth of the host-galaxies. I will discuss the cosmic evolution of the occurrence and kinematics of BH-driven winds, as traced by broad absorption line (BAL) features. I will exploit a sample of ~1900 luminous quasars at z=2.1-6.6, drawn from the X-shooter legacy survey of Quasars at Reionisation (XQR-30, based on a 250 hours ESO large program) and from SDSS. We find a BAL quasar fraction close to 20% at z~2-4, while it increases to almost 50% at z~6 (Bischetti et al. 2022, Nature, 605,244). The velocity and width of the BAL features also increase at z>~4.5. I will show evidence for a genuine redshift evolution of the BAL properties that cannot be ascribed to differences in terms of quasar luminosity and accretion rate. These results indicate efficient BH feedback occurring in the 1 Gyr old Universe, likely affecting the growth of BHs and, possibly, of their host galaxies. I will also show that BAL quasars are ideal targets for spatially-resolved studies of galaxy-scale winds with JWST/NIRSpec IFU.
    9:10 Byrne Multi-channel AGN Feedback in FIRE Cosmological Zoom-Ins: Impact on Star Formation and Galaxy Evolution AGN feedback is believed to play a significant role in the formation and evolution of massive galaxies. In particular, it is thought that AGN feedback is the primary driver of the observed quenching of star formation and color bimodality for galaxies above Milky Way mass. In recent years, various forms of AGN feedback have been implemented as sub-grid models in galaxy formation simulations, but many questions remain as to how to most realistically model the impact of this feedback. In this talk, I will discuss the effects of multi-channel AGN feedback in cosmological zoom-in simulations from the FIRE project, ranging from Milky Way-mass galaxies to galaxies massive enough to host luminous quasars. I consider two models of AGN physics: one which includes AGN mechanical winds and radiation, and one which includes cosmic rays in addition to winds and radiation. Comparing these models to each other and to simulations without AGN, I assess how well each model can produce populations of galaxies that match observational scaling relations and color bimodality. I will discuss the implications for our understanding of how AGN feedback, and winds in particular, can shape the evolution of galaxies throughout their lifetimes.
    9:30 Mercedes-Feliz Investigating Positive and Negative AGN Feedback in the FIRE cosmological simulations Active Galactic Nuclei (AGN) feedback is regarded as a key ingredient in suppressing star formation and quenching massive galaxies. However, several models and observations have suggested that AGN feedback may have a positive effect, triggering star formation by compressing interstellar medium gas to higher densities. We investigate the dual role of AGN feedback using cosmological simulations of a massive, star-forming galaxy at z~2 from the Feedback In Realistic Environments (FIRE) project, including a novel implementation of hyper-refined accretion-driven winds. We find that strong quasar winds drive the formation of a central gas cavity dramatically reducing the amount of star formation across the galaxy disk. Despite the global negative impact of quasar winds, we also identify several possible signatures of local positive feedback across different simulation suites, including: (1) spatial anti-correlation of wind-dominated regions and star-forming clumps, (2) higher local star formation efficiency in compressed gas near the edge of the cavity, (3) increased local contribution of outflowing material to star formation, and (4) the formation of massive stellar clumps in high-pressure dominated clouds under the presence of very strong quasar winds. Our results suggest that positive and negative AGN feedback can coexist in galaxies, but local positive feedback plays a minor role in global galaxy growth.
    9:50 Coffee
    10:20 Vayner Extremely Red Quasars at Cosmic Noon with JWST. Theoretical work proposes that winds driven by quasars into the surrounding interstellar medium (ISM) play a key role in shaping the properties of massive galaxies. This coupling between quasar-driven winds and the ISM is expected to be strongest in the environments of powerful, heavily obscured active galactic nuclei (AGN) at the peak epoch of galaxy and supermassive black hole (SMBH) growth in the early Universe. Extremely red quasars (ERQs) are a recently discovered AGN class showcasing the fastest moving outflows of any AGN sample to date, with velocities reaching several thousand km/s. I will present early-release science (ERS) JWST NIRSpec integral field unit (IFU) observations of a highly obscured, intrinsically luminous, extremely red quasar at z=2.94. I will present our discovery of a powerful wide-angle galaxy-scale outflow that reaches parts of the galaxy that are not directly illuminated by the quasar, driving shocks that heat up the gas and cause turbulence in the ISM. I will discuss the source of ionization across the quasar host galaxy and in the immediate group environment showcasing a discovery of an extreme star-forming region inside the quasar host galaxy with a recent burst of star formation. I will highlight our discovery of one of the densest galaxy groups at z~3, with at least four galaxies discovered in the narrow 3x3 arcseconds NIRSpec IFU field of view. Finally, I will briefly highlight our Q3Dfit software developed part of the ERS program capable of performing point-spread-function subtraction to remove the quasar emission and model the spatially resolved quasar host galaxy by fitting the continuum and emission lines from 1 - 28 μm simultaneously, and I will highlight more observations of ERQs as part of my GO Cycle 1 program.
    10:40 Veilleux Q-3D: A JWST Early Release Science Program to Study Quasar Feedback around Cosmic Noon JWST ERS program Q-3D ("Quasars in 3D") takes advantage of the outstanding integral field spectroscopic (IFS) capabilities of JWST to study quasar feedback and the interaction of quasars with their hosts in unprecedented detail. The strategy is (1) to use IFS observations, where within the velocity range of individual spectral features the contrast between the host galaxy and the central source is more favorable, and (2) to utilize a highly optimized PSF decomposition software package, q3dfit, which takes advantage of all available spatial and spectral information. All NIRSpec and MIRI data cubes on the three quasars of the sample have now been acquired. These quasars were selected to cover a range of redshifts centered on the epoch of peak SMBH accretion around cosmic noon (z ~ 0.5 - 3.0). This talk will summarize the results obtained so far on J1652 and XID 2028, two luminous, extremely red, quasars at redshifts ~ 3 and ~ 1.6, respectively. The results include the detection and characterization of warm-ionized gas outflows on scales of 10-30 kpc in both systems, and the serendipitous discovery around J1652 of a giant complex of warm-ionized gas that has been tidally stripped from several interacting companion galaxies, likely representing the core of a forming cluster of galaxies.
    Chair: Steve Kraemer
    11:00 Discussion
    12:00 Meeting Ends