Resumen:

We present a study the ionized gas kinematics of 298 Active Galactic Nuclei (AGN) host galaxies as compared to that of 485 control galaxies from the MaNGA-SDSS survey using measurements of the [O\,{\sc III}]$\lambda$5007\AA\, emission line profiles, fitted with one narrow Gaussian component and, for 45\%\ of the sources with one additional broad component. We present flux, velocity and W$_{80}$ maps, comparing them between AGN hosts and controls. The median difference in the $W_{80}$ values between AGN and controls is 238\,km\,s$^{-1}$. We identify "kinematically disturbed regions" (KDRs) within the Extended Narrow Line Region (ENLR) of the AGN, characterized by W$_{80} \ge W_{80,cut}=315$\,km\,s$^{-1}$ -- the mean value for the controls plus its standard deviation. The extent of the KDR R$_{KDR}$ ranges from 1 to 10\,kpc, with a mean ratio to that of the ENLR R$_{ENLR}$ of 55\%. We find a positive correlation between $\langle$W$_{80}\rangle$ and L[O{\sc III}] for the AGN, but, unexpectedly, also for the control sample, suggesting the possible presence of faint AGN in the control galaxies. We estimate the ionized gas mass outflow rate ($\dot{M}_{out}$) and the corresponding kinetic powers ($\dot{E}_{out}$) assuming that the KDR is due to an AGN outflow. Using two methods to obtain the outflow velocity --- one based on W$_{80}$ and the other using the velocity of the broad component, we find kinetic powers for the outflows that correlate with the AGN luminosity $L_{bol}$, populating the low luminosity region of this known correlation. This correlation corresponds 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, shows that even low-luminosity AGN, as those of our sample, can impact the host galaxy in a low, ``maintenance mode" feedback.

Resumen:

Double-peaked profiles observed in active galactic nuclei (AGNs) are signs of the presence of a disk-like geometry for the broad line region (BLR). These profiles are generally identified in the optical region in the Balmer lines, and in the ultraviolet (UV) in the Mg\,{\sc ii}\,$\lambda$2798. These spectral features allow us to obtain valuable insights into the geometry of the BLR since the region is not yet spatially resolved. In this work, we detected for the first time a double-peaked emission line in the O\,{\sc i}~$\lambda$11297 profile, in the near-infrared (NIR) spectrum of the local Seyfert 1 galaxy, III~Zw~002. This finding expands our understanding of double-peaked profiles beyond traditional optical and UV lines. In addition to O\,{\sc i} we observe a double-peaked emission in the Pa~$\alpha$ line simultaneously. This is the first case of detecting multiple broad double-peaked NIR emission lines together in an AGN. To investigate the properties of the emitting region, we employ a disk model and an additional Gaussian component attributed to non-disk clouds, namely the classical BLR, to adjust the line profiles. From this procedure, we obtained important parameters, such as the inclination and geometry of the disk, allowing us to estimate the mass of the supermassive black hole in this source. Based on our findings, we suggest that the O\,{\sc i} emission for III~Zw~002 comes from a flattened, low-ionization line-emitting region, providing insight into the complex BLR geometry within the challenging context of active galaxies.

Resumen:

\begin{abstract} Using the modelling code X-CIGALE, we reproduced the SEDs of 1,359 SDSS QSOs within the redshift range $0 < z < 4$, for which we have NIR/MIR fluxes with the highest quality and spectral data characterizing their SMBHs. Consistent with a rapid formation of the host galaxies, the star formation histories (SFHs) have small e-folding, at most 750 Myrs using an SFH function for Spiral or 1000 Myrs using one for Elliptical. Above $z \sim 1.6$, the two solutions are degenerate, the SEDs being dominated by the AGN continuum and high star formation rates (SFRs), typical of starburst galaxies, while at lower redshifts the starburst nature of the host, independent from its morphology, is better reproduced by an Spiral SFH. In general, the SFR increases with the redshift, the mass of the bulge, the AGN luminosity and Eddington ratio, suggesting there is no evidence of AGN quenching of star formation. Comparing the specific BHAR with specific SFR, all the QSOs at any redshift trace a linear sequence below the Eddington luminosity, in parallel and above the one-to-one relation, implying that QSOs are in a special phase of evolution during which the growth in mass of their SMBH is more rapid than the growth in mass of their galaxy hosts. This particular phase is consistent with a scenario where the galaxy hosts of QSOs in the past grew in mass more rapidly than their SMBHs, suggesting that a high star formation efficiency during their formation was responsible in limiting their masses. \end{abstract}

Resumen:

The abundance of UV-bright galaxies at redshift $z > 8$, or within the first $\sim$600 Myrs, can provide key constraints on galaxy evolution models and the epoch of reionization, as the predicted abundance varies greatly when different physical prescriptions for gas cooling and star formation are implemented. The Hubble Space Telescope (HST) has been used to find such bright galaxies in deep surveys but in a focused patch of the sky, making the known galaxy population highly affected by cosmic variance effects. Pure parallel programs -- where random field pointings result in completely independent, uncorrelated observations -- provide an excellent opportunity to observe a population of rare bright sources that may not be fully sampled by deep surveys covering the same area in contiguous fields. Galaxy candidates from the HST surveys of superBoRG, BoRG, HIPPIES, and WISP comprise the largest pure-parallel sample including some of the brightest candidates at these redshifts, potentially representing some of the most massive galaxies to form at $< 600$ Myr. We are leading JWST/NIRSpec observations from Cycle 1 programs GO 1747 and GO 2426 to spectroscopically confirm these galaxy candidates. We have 9 out of 21 targets already observed with low-resolution Prism spectroscopy. Here, we will present the so far four galaxy confirmations via the detection of the Lyman break, and their ionizing power through the characterization of the [OIII]/[OII] line ratio (see e.g. Fig 1). We expect to present more results as observations arrive by the time of the conference meeting. The resulting observed density of UV-bright galaxies from our study will provide important constraints on models of star formation efficiency to some of the earliest-probed redshifts ($z > 10$), as well as chemical and ionizing characterization of galaxies deep into the epoch of reionization.

Resumen:

Dusty star-forming galaxies (DSFGs) are commonly used as tracers of galaxy protoclusters, with many spectacular examples identified with telescopes such as the South Pole Telescope, Planck, and Herschel. However, to date, there has been relatively little 'first principles' theoretical work that models the connection between DSFGs and protoclusters. To address this gap, we have incorporated scaling relations (derived in previous work by performing radiative transfer calculations on hydro simulations) to predict far-IR/submm flux densities into the L-Galaxies semi-analytic model. I will present a few results from this new model. Specifically, I will show that protocluster cores exhibit an excess of DSFGs relative to protocluster 'outskirts' and the field. However, contrary to some claims in the literature, this is not due to the dense environment 'triggering' starbursts. Rather, the DSFGs typically lie near the star formation main sequence. The reason for the excess is that protocluster cores have an excess of massive galaxies relative to less-overdense regions. Moreover, the model predicts that the brightest DSFGs are predominantly located in protocluster cores.

Resumen:

We continue to explore the relationship between globular cluster total number, $N_{\rm GC}$, and central black hole mass, $M_\bullet$, in spiral galaxies. We present here results for the Sab galaxies NGC\,3368, NGC\,4736 (M\,94) and NGC\,4826 (M\,64), and the Sm galaxy NGC\,4395. The globular cluster (GC) candidate selection is based on the (u* - i') versus (i' - Ks) color-color diagram, and i'-band shape parameters. We determine the $M_\bullet$ versus $N_{\rm GC}$ correlation for these spirals, plus NGC\,4258, NGC\,253, M\,104, M\,81, M\,31, and the Milky Way (i.e., we have doubled the previously existing sample of spirals with both $M_\bullet$ and $N_{\rm GC}$ measurements). We also redetermine the correlation for the elliptical sample in Harris et al. (2014), with updated galaxy types from Sahu et al. (2019). Additionally, we derive total stellar galaxy mass, $M_\ast$, from its two-slope correlation with $N_{\rm GC}$ (Hudson et al. 2014), and fit $M_\bullet$ versus $M_\ast$ for both spirals and ellipticals. We obtain log$M_\bullet \propto$ (1.01 $\pm$ 0.13) log $N_{\rm GC}$ for ellipticals, and log $M_\bullet \propto$ (1.64 $\pm$ 0.24) log $N_{\rm GC}$ for late type galaxies (LTG). The linear $M_\bullet$ versus $N_{\rm GC}$ correlation in ellipticals could be due to statistical convergence through mergers, but not the much steeper correlation for LTG. However, in the $M_\bullet$ versus total stellar mass ($M_\ast$) parameter space, {\it with $M_\ast$ derived from its correlation with $N_{\rm GC}$}, log $M_\bullet \propto$ (1.48 $\pm$ 0.18) log $M_\ast$ for ellipticals, and log $M_\bullet \propto$ (1.21 $\pm$ 0.16) log $M_\ast$ for LTG. The observed agreement between ellipticals and LTG in this parameter space may imply that black holes and galaxies co-evolve through ``calm” accretion, AGN feedback, and other secular processes.