Active Nuclei Research Articles

Supermassive black hole feeding and feedback observed on subparsec scales.

Active galaxies contain a supermassive black hole at their center that grows by accreting matter from the surrounding galaxy. The accretion process in about the central 10 parsecs has not been directly resolved in previous observations because of the small apparent angular sizes involved. We observed the active nucleus of the Circinus Galaxy using submillimeter interferometry. A dense inflow of molecular gas was evident on subparsec scales. We calculated that less than 3% of this inflow is accreted by the black hole, with the rest being ejected by multiphase outflows, providing feedback to the host galaxy. Our observations also reveal a dense gas disk surrounding the inflow that is gravitationally unstable, which drives the accretion into about the central 1 parsec.

Cygnus A obscuring torus: ionized, atomic, or molecular?

ABSTRACT The prototypical powerful FR II radio galaxy Cygnus A fits extremely well into the quasar/radio galaxy unified model: high polarization with an angle almost perpendicular to the radio jet and polarized flux showing broad permitted lines. It has been claimed that ionized gas in the torus reveals a very clear torus shape via Bremmstrahlung emission. We rule out the later with an energetic argument, and we constrain the molecular and atomic gas properties with existing observations. The atomic absorption against the core has been shown to match the X-ray column only if the spin temperature is an implausible Ts = 1 × 106 K. This points to a molecular medium for the X-ray column $\log (N_{\rm H} ~[\rm {cm^{-2}}]) \sim 23.5$. Yet not low-J CO absorption is detected to sensitive limits. The non-detection is surprising given that this powerful radio galaxy hosts a luminous, dust-obscured active nucleus and copious warm molecular hydrogen. These conditions suggest a detectable level of emission. Furthermore, the torus X-ray column density suggests detectable absorption. We explore various possibilities to explain the lack of a signature from warm CO (200–250 K). Specifically, that the radiative excitation by the radio core renders low-J CO absorption below current sensitivities, and that high-J levels are well populated and conducive to producing absorption. We test this hypothesis using archival Hershel/SPIRE FTS observations of Cygnus A of high-J CO lines (14 ≥ J ≥ 4 transitions). Still high-J CO lines are not detected. We suggest that ALMA observations near its high frequency limit can be critical to obtain the signature of molecular line of the torus of Cygnus A.

MULTIWAVELENGTH PROPERTIES OF THE LOW-REDSHIFT ISOLATED GALAXIES WITH ACTIVE NUCLEI MODELLED WITH CIGALE

Using the CIGALE software, we present the preliminary results of a multiwavelength analysis of eighteen low-redshift isolated galaxies with active nuclei (isolated AGNs). This sample was formed by cross-matching the 2MIG isolated AGNs sample with the SDSS DR9 catalog. The host galaxies of this sample have not undergone a merger for at least three billion years, making them a unique laboratory for studying interactions between various astrophysical processes without the complicating factors of merging with other galaxies or the effects of a denser environment. In addition, the study of isolated AGNs can provide valuable information about the evolution and activity of galaxies in the broader context of the distribution of large-scale structures of the Universe. First, we seek to understand how the environment affects the physical processes involved in the accretion of matter onto supermassive black holes in these galaxies. Secondly, to what extent do processes of star formation or degeneration of nuclei activity continue the evolution of these galaxies? Third, how does the localization of isolated AGNs in voids or filaments of a large-scale structure determine the properties of this envi- ronment at the low redshifts? Using observable fluxes from UV to the radio ranges from archival databases of space-born and ground-based observatories (GALEX, SDSS, 2MASS, Spitzer, Hershel, IRAS, WISE, VLA), we estimated the contribution from the emission of an active nucleus to the galaxy’s total emission, the stellar mass, and the star formation rate. The mass of the stellar component falls from 1010 MSun and 1011 MSun. The star formation rate for most galaxies (except UGC 10120) does not exceed 3 MSun per year. The best SED fittings (with χ2 values less than 5) are obtained for the galaxies CGCG248-019 (χ2 = 1.6), CGCG179-005 (χ2 = 1.6), CGCG243-024 (χ2 = 2.6), IC0009 (χ2 = 2.8), MCG+09-25-022 (χ2 = 3.1), UGC10244 (χ2 = 4.1)

Complex AGN feedback in the Teacup galaxy

Context. The z ∼ 0.1 type-2 QSO J1430+1339, known as the “Teacup”, is a complex galaxy showing a loop of ionised gas ∼10 kpc in diameter, co-spatial radio bubbles, a compact (∼1 kpc) jet, and outflow activity. Its closeness offers the opportunity to study in detail the intricate interplay between the central supermassive black hole (SMBH) and the material in and around the galaxy, both the interstellar medium (ISM) and circumgalactic medium (CGM). Aims. We characterise the spatially resolved properties and effects of the galactic ionised gas outflow and compare them with those of the radio jet and with theoretical predictions to infer its acceleration mechanism. Methods. We used VLT/MUSE optical integral field spectroscopic observations to obtain flux, kinematic, and excitation maps of the extended (up to ∼100 kpc) ionised gas and to characterise the properties of stellar populations. We built radial profiles of the outflow properties as a function of distance from the active nucleus, from kiloparsec up to tens of kiloparsec scales, at ∼1 kpc resolution. Results. We detect a velocity dispersion enhancement (≳300 km s−1) elongated over several kiloparsecs perpendicular to the radio jet, the active galactic nucleus (AGN) ionisation lobes, and the fast outflow, similar to what is found in other galaxies hosting compact, low-power jets, indicating that the jet strongly perturbs the host ISM during its passage. We observe a decreasing trend with distance from the nucleus for the outflow properties (mass outflow rate, kinetic rate, momentum rate). The mass outflow rate drops from around 100 M⊙ yr−1 in the inner 1–2 kpc to ≲0.1 M⊙ yr−1 at 30 kpc. The mass outflow rate of the ionised outflow is significantly higher (∼1–8 times) than the molecular one, in contrast with what is often quoted in AGN. Based on energetic and morphological arguments, the driver of the multi-phase outflow is likely a combination of AGN radiation and the jet, or AGN radiation pressure on dust alone. The outflow mass-loading factor is ∼5–10 and the molecular gas depletion time due to the multi-phase outflow is ≲108 yr, indicating that the outflow can significantly affect the star formation and the gas reservoir in the galaxy. However, the fraction of the ionised outflow that is able to escape the dark matter halo potential is likely negligible. We detect blue-coloured continuum emission co-spatial with the ionised gas loop. Here, stellar populations are younger (≲100–150 Myr) than in the rest of the galaxy (∼0.5–1 Gyr). This constitutes possible evidence for star formation triggered at the edge of the bubble due to the compressing action of the jet and outflow (“positive feedback”), as predicted by theory. All in all, the Teacup constitutes a rich system in which AGN feedback from outflows and jets, in both its negative and positive flavours, co-exist.

Synthesis of New 2-Pyridinone and 2-Iminochromene Derivatives Bearing Biologically Active Pyrrole Moiety as Expected Antibacterial and Antifungal Agents

In an attempt to discover new antimicrobial drugs, new 2-pyridinone and 2-iminochromene derivatives bearing biologically active pyrrole nucleus were designed and synthesized. The pyridin-2-one derivatives were synthesized via ring closure of 2-cyano-N'-((1-methyl-1H-pyrrol-2-yl)methylene)acetohydrazide by acetylacetone or 2-arylidenemalononitriles. The 2-iminochromene derivatives were obtained in high yields through the cyclocondensation reaction of 2-cyano-N'-((1-methyl-1H-pyrrol-2-yl)methylene)acetohydrazide with o-hydroxy aldehyde derivatives (salicyaldehyde derivatives, 2-hydroxy-1-naphthaldehyde and 7-hydroxy-chromone-6-carboxaldehyde derivative). The antibacterial and antifungal properties of all synthesized compounds were evaluated. All tested compounds displayed weak activities toward the G + ve bacteria (S. aureus) and G –ve bacteria (E. coli and P. vulgaris). The polycyclic benzo[f]chromene derivative 7 showed weak activity toward both G + ve and G –ve bacteria.

A Comprehensive Review on the Benzimidazole Scaffold as a Potential Nucleus for Anticancer Activity

Abstract: It is common knowledge that cancer is the world's biggest cause of mortality. This has led to the ongoing introduction and validation of new cancer therapy outcomes. Benzimidazole derivatives control DNA stability and cell cycle advancement. A heterocyclic nucleus is structurally more favourable for a direct DNA connection and, thus, for the management of the DNA replication process. This review seeks to explore the usefulness of such drugs in the future facets of cancer prognosis and treatment in addition to discussing the role of benzimidazole in cancer therapy. Benzimidazole derivatives have been reported as a pertinent therapeutic strategy to modify cancer progression and malignancy in the data from 2013 to 2022. Here, we emphasize these features in several cancer types and cell lines using in vitro and in vivo methods.

Torus skin outflow in a near-Eddington quasar revealed by spectropolarimetry

ABSTRACT Even when the direct view towards the active nucleus is obscured, nuclear emission propagating along other directions can scatter off surrounding material, become polarized and reach the observer. Spectropolarimetry can thus be an important tool in investigating the circumnuclear geometry and kinematics of quasars on scales that cannot yet be probed via direct observations. Here, we discuss an intriguing class of quasars where the polarization position angle swings by large amounts ($\sim 90\deg$) within an emission line. We investigate a kinematic model in which the scattering dust or electrons are in an axisymmetric outflow. We propagate Stokes parameters in a variety of geometries of emitter, scatterer, and observer. We use these models to predict polarization fraction, line profiles, and polarization position angles and compare them to observations. We demonstrate that the swinging polarization angle can be a result of the geometry of the outflow and the orientation of the observer. Polarization properties of a near-Eddington extremely red quasar SDSS J1652 can be successfully explained by a model in which the quasar is surrounded by a geometrically thick disc, whose ‘skin’ is outflowing at ∼1000 km s−1 and acts as the scatterer on scales of a few tens of pc. The line of sight to the observer in this source is within or close to the skin of the torus, in agreement with multiwavelength data. Spectropolarimetric data and models presented here strongly support the thick-disc geometry of circumnuclear material suggested by recent numerical simulations of high-rate accretion flows on to black holes.

The Interaction between AGN and Starburst Activity in the Circumnuclear Region of NGC 7469 as Viewed with JWST

We combine mid-infrared diagnostics obtained from integral-field-unit observations taken with Mid-Infrared Instrument/Medium Resolution Spectrograph on the James Webb Space Telescope with cold molecular gas information derived from Atacama Large Millimeter/submillimeter Array observations of CO(1–0) emission to investigate the star formation rate and efficiency within the central ∼1.5 kpc × 1.3 kpc region of the Seyfert 1 galaxy NGC 7469 on ∼100 pc scales. The active nucleus leaves a notable imprint on its immediate surroundings by elevating the temperature of the warm molecular gas, driving an ionized gas outflow on subkiloparsec scales, and selectively destroying small dust grains. These effects, nevertheless, have relatively little impact on the cold circumnuclear medium or its ability to form stars. Most of the star formation in NGC 7469 is confined to a clumpy starburst ring, but the star formation efficiency remains quite elevated even for the nuclear region that is most affected by the active nucleus.

A UFO Seen Edge-on? Resolving Ultrafast Outflow Emission on ∼200 pc Scales with Chandra in the Active Nucleus of Mrk 34

We present Chandra ACIS imaging spectroscopy of the nucleus of the Seyfert 2 Galaxy Mrk 34. We identify spatially and spectrally resolved features in the band that includes Fe Kα, Fe xxv, and Fe xxvi. These features suggest high-velocity (≳15,000 km s−1 line-of-sight) material spanning ∼0.″5, within ∼200 pc of the nucleus. This outflow could have deprojected velocities ∼12–28× greater than the [O iii]-emitting outflows, and could potentially dominate the kinetic power in the outflow. This emission may point to the origins of the optical and X-ray winds observed at larger radii, and could indicate a link between ultrafast outflows and AGN feedback on ≳kiloparsec scales.

The ALPINE-ALMA [CII] survey: Double stellar population and active galactic nucleus activity in a galaxy at z ∼ 5.5

Context. GDS J033218.92-275302.7 (here GS-14) is a z ∼ 5.5 galaxy with unusual UV spectral features that have been interpreted as signatures of either a double stellar population or of an active galactic nucleus (AGN). GS-14 was detected in [C II] 158 μm as part of the ALPINE survey and was found to be the galaxy with the lowest molecular gas fraction (fmol = Mmolgas/(Mmolgas + M*)∼0.1) of that sample. Aims. We exploited the multiwavelength coverage of GS-14 to investigate the properties and the origin of its emission. Methods. We fit the UV-to-near-IR spectral energy distribution (SED) with a single and double stellar population and/or AGN component. We analyzed the latest release of the VIMOS spectrum, which shows highly ionized emission lines (O VI1032 Å, N V1240 Å, and N IV] 1483,1486 Å). The line equivalent widths and line ratios were compared with those observed in galaxies and AGN, as well as with the predictions from radiation transfer models for star-forming galaxies, AGN, and shocks. Results. The SED-fitting provides a total stellar mass of M* = (4 ± 1)×1010 M⊙, an age of the main stellar population of ∼ 670 Myr, and a recent (∼ 8 Myr) short burst of star formation (SF) of ∼90 M⊙ yr−1. We do not find a significant contribution from an AGN, although we do not have any coverage in the mid-IR, where the dust emission of the AGN would peak. The N V line has a characteristic P Cygni profile. Fitting it with stellar models suggests a ∼ 3 Myr old population of stars with a mass of ∼5 × 107 M⊙, consistent with a second component of young stars, as found in the SED-fitting analysis. The N V profile also shows evidence for an additional component of nebular emission. The comparison of the line ratios (N IV]/N V and O VI/N V) with theoretical models allows us to associate the emission with SF or AGN, but the strong radiation field required to ionize the O VI is more commonly related to AGN activity. Conclusions. Studying GS-14, we found evidence for an old and already evolved stellar population at z ∼ 5.5, and we show that the galaxy is experiencing a second short burst of SF. In addition, GS-14 carries signatures of obscured AGN activity. The AGN could be responsible for the short depletion time of this galaxy, thus making GS-14 one of the two ALPINE sources with indications of an active nucleus and an interesting target for future follow-ups to understand the connection between SF and AGN activity.

Metabolic labeling of hyaluronan: Biosynthesis and quantitative analysis of 13C,15N-enriched hyaluronan by NMR and MS-based methods

Hyaluronan (HA), a member of the GAG family of glycans, has many diverse biological functions that vary a lot depending on the length of the HA chain and its concentration. A better understanding of the structure of different-sized HA at the atomic level is therefore crucial to decipher these biological functions. NMR is a method of choice for conformational studies of biomolecules, but there are limitations due to the low natural abundance of the NMR active nuclei 13C and 15N. We describe here the metabolic labeling of HA using the bacterium Streptococcus equi subsp. Zooepidemicus and the subsequent analysis by NMR and mass spectrometry. The level of 13C and 15N isotope enrichment at each position was determined quantitatively by NMR spectroscopy and was further confirmed by high-resolution mass spectrometry analysis. This study provides a valid methodological approach that can be applied to the quantitative assessment of isotopically labeled glycans and will help improve detection capabilities and facilitate future structure-function relationship analysis of complex glycans.

A Diverse Population of z ∼ 2 ULIRGs Revealed by JWST Imaging

Four ultraluminous infrared galaxies (ULIRGs) observed with JWST/NIRcam in the Cosmos Evolution Early Release Science program offer an unbiased preview of the z ∼ 2 ULIRG population. The objects were originally selected at 24 μm and have strong polycyclic aromatic hydrocarbon emission features observed with Spitzer/Infrared Spectrometer. The four objects have similar stellar masses of ∼1011 M ⊙ but otherwise are quite diverse. One is an isolated disk galaxy, but it has an active nucleus as shown by X-ray observations and by a bright point-source nucleus. Two others are merging pairs with mass ratios of 6–7:1. One has active nuclei in both components, while the other has only one active nucleus: the one in the less-massive neighbor, not the ULIRG. The fourth object is clumpy and irregular and is probably a merger, but there is no sign of an active nucleus. The intrinsic spectral energy distributions for the four active galactic nuclei in these systems are typical of type-2 QSOs. This study is consistent with the idea that even if internal processes can produce large luminosities at z ∼ 2, galaxy merging may still be necessary for the most luminous objects. The diversity of these four initial examples suggests that large samples will be needed to understand the z ∼ 2 ULIRG population.

Strong gravitational lensing by AGNs as a probe of the quasar–host relations in the distant Universe

The tight correlations found between the mass of supermassive black holes and the luminosities, stellar masses and velocity dispersions of their host galaxies are often interpreted as a sign of their co-evolution. Studying these correlations across redshift provides a powerful insight into the evolutionary path followed by the quasar and its host galaxy. While the mass of the black hole is accessible from single-epoch spectra, measuring the mass of its host galaxy is challenging as the active nucleus largely overshines its host. Here we present a technique to probe quasar–host relations beyond the local Universe with strong gravitational lensing, hence overcoming the use of stellar population models or velocity dispersion measurements, both prone to degeneracies. We study in detail one of the three known cases of strong lensing by a quasar to accurately measure the mass of its host and to infer a total lensing mass within the Einstein radius. The lensing measurement is more precise than any other alternative technique and compatible with the local scaling relation between the mass of the black hole and the stellar mass. The sample of such quasar–galaxy or quasar–quasar lensing systems should reach a few hundred with Euclid and the Rubin-Large Synoptic Survey Telescope, thus enabling the application of such a method with statistically significant sample sizes. A rare case of a quasar acting as a gravitational lens allows a precise determination of the mass of the quasar’s host galaxy and offers a new path to studying the connections between supermassive black holes and their host galaxies.

On the large scale morphology of Hercules A: destabilized hot jets?

ABSTRACT Extragalactic jets are generated as bipolar outflows at the nuclei of active galaxies. Depending on their morphology, they are classified as Fanaroff–Riley type I (FRI) (centre-brightened) and Fanaroff–Riley type II (FRII) (edge-brightened) radio jets. However, this division is not sharp, and observations of these sources at large scales often show intermediate jet morphologies or even hybrid jet morphologies with a FRI type jet on one side and a FRII type jet on the other. A good example of a radio galaxy that is difficult to classify as FRI or FRII is Hercules A. This source shows jets with bright radio lobes (a common feature of FRII type jets) albeit without the hotspots indicative of the violent interaction between the jet and the ambient medium at the impact region, because the jets seem to be disrupted inside the lobes at a distance from the bow shocks surrounding the lobes. In this paper, we explore the jet physics that could trigger this peculiar morphology by means of three-dimensional relativisitic hydrodynamical simulations. Our results show that the large-scale morphological features of Hercules A jets and lobes can be reproduced by the propagation of a relativistically hot plasma outflow that is disrupted by helical instability modes, and generates a hot lobe that expands isotropically against the pressure-decreasing intergalactic medium. We also discuss the implications that this result may have for the host active nucleus in terms of a possible transition from high-excitation to low-excitation galaxy modes.

Application of Machine Learning to Predict the Acoustic Cavitation Threshold of Fluids

The acoustic cavitation of fluids, as well as related physical and chemical phenomena, causes a variety of effects that are highly important in technological processes and medicine. Therefore, it is important to be able to control the conditions that allow cavitation to begin and progress. However, the accurate prediction of acoustic cavitation is dependent on a complex relationship between external influence parameters and fluid characteristics. The multiparameter problem restricts the development of successful theoretical models. As a result, it is critical to identify the most important parameters influencing the onset of the cavitation process. In this paper, the ultrasonic frequency, hydrostatic pressure, temperature, degassing, density, viscosity, volume, and surface tension of a fluid were investigated using machine learning to determine their significance in predicting acoustic cavitation strength. Three machine learning models based on support vector regression (SVR), ridge regression (RR), and random forest (RF) algorithms with different input parameters were trained. The results showed that the SVM algorithm performed better than the other two algorithms. The parameters affecting the active cavitation nuclei, namely hydrostatic pressure, ultrasound frequency, and outgassing degree, were found to be the most important input parameters influencing the prediction of the cavitation threshold. Other parameters have a minor impact when compared to the first three, and their role can be compensated for by alternative variables. The further development of the obtained results provides a new way to optimize and improve existing theoretical models.

Echo pulses for background suppression by optimal control.

Materials used to construct magic-angle-spinning NMR probes can contain NMR active nuclei that produce a significant amount of background signal. Because these materials are located outside the sample coil, the use of spatially selective pulses to remove the background is a popular approach for background suppression. However, previously suggested spatially selective pulses suffer from limited excitation bandwidths, which may make them unsuitable for the acquisition of nuclei with a large chemical shift range. Here, a pulse (OC-BACK) is presented, which has been developed by optimal control, which has a flat profile of ~120 kHz with respect to off-resonance effects and extended pass and suppression bands with respect to the nominal nutation frequency. The presented solution is large enough to be effective for background suppression schemes in 19 F magic-angle-spinning NMR at medium and low magnetic fields.

Effects of magnesium on the structure of aluminoborosilicate glasses: NMR assessment of interatomic potentials models for molecular dynamics

AbstractClassical molecular dynamics simulations have been used to investigate the structural role of Mg and its effect when it is incorporated in sodium aluminoborosilicate glasses. The simulations have been performed using three interatomic potentials; one is based on the rigid ionic model parameterized by Wang et al. (2018) and two slightly different parameterization of the core–shell model provided by Stevensson et al. (2018) and Pedone et al. (2020) The accuracies of these models have been assessed by detailed structural analysis and comparing the simulated nuclear magnetic resonance (NMR) spectra for spin active nuclei (29Si, 27Al, 11B, 17O, 25Mg, and 23Na) with the experimental counterparts collected in a previous work. Our simulations reveal that the core–shell parameterizations provide better structural models. In fact, they better reproduce the NMR spectra of all the investigated nuclei and give better agreement with known experimental data. Magnesium is found to be five coordinated on average with distances with oxygen in between a network modifier (like Na) and an intermediate network formed (like Al). It prefers to lay closer to three‐coordinated B atoms, forming B–NBO bonds, with respect to Si and especially Al. This can explain the formation of AlO5 and AlO6 units in the investigated Na‐free glass, together with a Si clusterization.

GSKIP modulates cell aggregation through EMT/MET signaling rather than differentiation in SH-SY5Y human neuroblastoma cells.

GSK3β interacting protein (GSKIP) is a small A-kinase anchor protein previously reported to mediate the N-cadherin/β-catenin pool for differentiation in SH-SY5Y cells through overexpression of GSKIP to present the neuron outgrowth phenotype. To further investigate how GSKIP functions in neurons, CRISPR/Cas9 technology was utilized to knock out GSKIP (GSKIP-KO) in SH-SY5Y. Several GSKIP-KO clones resulted in an aggregation phenotype and reduced cell growth without retinoic acid (RA) treatment. However, neuron outgrowth was still observed in GSKIP-KO clones treated with RA. The GSKIP-KO clones exhibited an aggregation phenotype through suppression of GSK3β/β-catenin pathways and cell cycle progression rather than cell differentiation. Gene set enrichment analysis indicated that GSKIP-KO was related to epithelial mesenchymal transition/mesenchymal epithelial transition (EMT/MET) and Wnt/β-catenin/cadherin signaling pathways, suppressing cell migration and tumorigenesis through the inhibition of Wnt/β-catenin mediated EMT/MET. Conversely, reintroduction of GSKIP into GSKIP-KO clones restored cell migration and tumorigenesis. Notably, phosphor-β-catenin (S675) and β-catenin (S552) but not phosphor-β-catenin (S33/S37/T41) translocated into the nucleus for further gene activation. Collectively, these results suggested that GSKIP may function as an oncogene to form an aggregation phenotype for cell survival in harsh environments through EMT/MET rather than differentiation in the GSKIP-KO of SH-SY5Y cells. GSKIP Implication in Signaling Pathways with Potential Impact on SHSY-5Y Cell Aggregation.

Exploring the potential application of alternative nuclei in NMR based metabolomics

IntroductionNuclear magnetic resonance (NMR) is widely used in metabolomics but it focusses on 1H over other NMR-active nuclei.ObjectivesTo evaluate the potential of alternative NMR-sensitive nuclei to generate useful metabolomic data.MethodProton, carbon, phosphorus, and nitrogen-based NMR metabolomics was undertaken on extracts from mint and European honey bee tissue.ResultsCarbon NMR provided useful information but required larger sample sizes. Phosphorus produced overlapping peaks in one dimensional (1D) analysis but showed potential in 2D experiments. 15N NMR was found to not be sensitive enough for general metabolomic work.ConclusionsAlternative NMR active nuclei are useful for metabolomics.

Radio Properties of the Low-Redshift Isolated Galaxies with Active Nuclei

Radio Properties of the Low-Redshift Isolated Galaxies with Active Nuclei