Francisco Förster - Universidad de Chile (Chile)[cv]
Francisco Förster
Universidad de Chile
Curriculum Vitae:
Professor at U. of Chile, Data and Artificial Intelligence Initiative. Associate Researcher at the Millenium Institute of Astrophysics, researcher at the Center for Mathematical Modeling, Fondecyt Regular Fellow. Obtained D.Phil. at the University of Oxford in theoretical studies on supernova progenitors. Principal Investigator of the ALeRCE project, an astronomical alert broker for next generation survey telescopes selected as Community Broker for the Vera C. Rubin Observatory; and of the High cadence Transient Survey (HiTS), a real–time search for very young supernova using the Dark Energy Camera.
A new generation of large aperture and large field of view telescopes is allowing the exploration of large volumes of the Universe in an unprecedented fashion. In order to take advantage of these new telescopes, notably the Vera C. Rubin Observatory, a new time domain ecosystem is developing. Among the tools required are fast machine learning aided discovery and classification algorithms, interoperable tools to allow for an effective communication with the community and follow-up telescopes, and new models and tools to extract the most physical knowledge from these observations. In this talk I will review the challenges and progress of building one of these systems: the Automatic Learning for the Rapid Classification of Events (ALeRCE) astronomical alert broker. ALeRCE (http://alerce.science/) is an alert annotation and classification system led by an interdisciplinary and interinstitutional group of scientists from Chile since 2019. ALeRCE is focused around three scientific cases: transients, variable stars and active galactic nuclei. Thanks to its state-of-the-art machine learning models, ALeRCE has become the 3rd group to report most transient candidates to the Transient Name Server, and it is enabling new science with different astrophysical objects, e.g. AGN science. I will discuss some of the challenges associated with the problem of alert classification, including the ingestion of multiple alert streams, annotation, database management, training set building, feature computation and distributed processing, machine learning classification and visualization, or the challenges of working in large interdisciplinary teams. I will also show some results based on the real‐time ingestion and classification using the Zwicky Transient Facility (ZTF) alert stream as input, as well as some of the tools available.
09:50 - 10:20
Plenary Target Talk
Invited Speaker:
Marcio Meléndez - Space Telescope Science Institute (EE.UU.)[cv]
Marcio Meléndez
Space Telescope Science Institute
Curriculum Vitae:
El Dr. Marcio Meléndez obtuvo una Licenciatura en Física en la Universidad Simón Bolívar de Venezuela y después una Maestría en Física en el Instituto Venezolano de Investigaciones Científicas, IVIC. Durante este tiempo su trabajo de investigación se enfocó en realizar cálculos atómicos de plasmas astrofísicos. Posteriormente continuó sus estudios en la Universidad Católica de América, en Washington DC, donde obtuvo una Maestría y Doctorado en Física, realizando en el Centro Goddard de la NASA su trabajo de tesis doctoral sobre agujeros negros super masivos en el centro de galaxias activas. En el 2008 obtuvo una beca de investigación como parte del programa postdoctorante de la NASA (NPP) para trabajar con observaciones de galaxias activas usando el telescopio espacial en el infrarrojo Spitzer. Seguidamente obtuvo posiciones como investigador en el departamento de Física y Astronomía de la Universidad John Hopkins y Departamento de Astronomía de la Universidad de Maryland. En el 2015 se unió al equipo de óptica del módulo integrado de instrumentos científicos del telescopio espacial James Webb donde participó en las pruebas al vacío del telescopio realizadas en los centros de la NASA, Goddard y el centro espacial Johnson en Houston, Texas, EEUU. Actualmente el Dr. Marcio Meléndez es científico principal de óptica astronómica en el Instituto Científico del Telescopio Espacial en Baltimore, Maryland, EEUU. Dr. Meléndez participó en la comisión del elemento óptico del telescopio espacial James Webb, en particular, la alineación de sus espejos hasta lograr imágenes, limitada solamente por la difracción. Los intereses científicos de Dr. Meléndez están relacionados con el estudio de los agujeros negros supermasivos en el centro de galaxias activas y su interacción con la galaxia en la que residen.
Chair: Javier Licandro
#599 |
The James Webb Space Telescope: commissioning and first year of operations
The James Webb Space Telescope (JWST) is a segmented deployable telescope for infrared astronomy, launched on December 25th, 2021 and currently operating at L2. In this talk, I will summarize the details of Webb’s Optical Telescope Element commissioning process that began about 1 month after launch and finished with the release of its first public images. I will describe the wavefront sensing commissioning process that transformed an array of 18 scattered mirror segments into a phased telescope, producing diffraction-limited images. I will share my experience as a member of the wavefront sensing and control group at the Space Telescope Science Institute (STScI) and show the evolution of Webb imaging; from first light to its first year of science operations. I will conclude with a summary of the telescope current optical stability and a list of lessons learned that can be valuable for the future of large segmented cryogenic space telescopes.
10:20 - 11:00
COFFEE BREAK
11:00 - 12:30
J: Galaxies and Cosmology
Early Universe / AGN
Chair: Félix Mirabel
#230 |
XQR-30: Black hole masses and accretion rates for 42 z \textgreater 6 quasars
Luminous, high-redshift ($z>6$) quasars are formidable probes of the universe
in the Epoch of Reionization. They are observed to already host super-massive
black holes (BHs) in their centers, and to reside in the earliest, most
massive galaxies, where they are thought to be surrounded by large galactic
over-densities. How BHs and hosts get this massive in such short amount
of time after the Big Bang is one of the key open questions of current
astrophysics. Here, we present bolometric luminosities, BH masses and
Eddington ratios for 42 luminous quasars at z>6 using, for the first
time, high signal-to-noise ratio VLT/X-Shooter spectra, acquired as part
of the ESO Large Programme XQR-30. We find that quasars at high-redshift
host slightly less massive BHs which accrete slightly more rapidly
than a bolometric luminosity matched quasars sample at $z\sim 1$,
and we explore the repercussion of such results with respect to
BH seeds formation and evolution scenarios.
#015 |
Search for LAE galaxies at z~6 in the Thesan simulations
In this work, we study the number density of Lyman Alpha Emitter (LAE) galaxies, their physical properties, and synthetic spectra at redshift ~ 6 using high-resolution hydrodynamical simulations with radiative transfer from the Thesan project. By recreating the scenario described in Becker et al. 2018, we test the hypothesis that observations to date are missing the vast majority of the high-redshift galaxies' signal since they are extremely faint and, thus, are out of the observational limits of our current telescopes. We also follow the evolution of the neutral Hydrogen fraction, the chemical enrichment of the circum- and intergalactic medium, and specific star formation rate of galaxies in the simulation at the end of Reionization, and evaluate why the detections from HST and the Silverrush project significantly underestimate the number of faint galaxies. Our study indicates an observational bias to massive galaxies in the field. Thus, we forecast the properties of the dwarf galaxies responsible for completing the budget of ionizing photons that concluded the Epoch of Reionization.
#319 |
First detection of a newborn AGN
Patricia Arevalo1
;
Elena López Nava
1
;
Mary Loli Martínez Aldama
2
;
Paula Sánchez-Sáez
3
;
Santiago Bernal
1
;
Lorena Hernández García
1
;
Paulina Lira
4
1 - Universidad de Valparaíso.2 - Universidad de Concepción.3 - ESO.4 - Universidad de Chile.
Observations and models indicate that the fraction of active galaxies in the local Universe is about 10\% . As most large galaxies host a supermassive black hole (SMBH), this can be interpreted as a duty cycle, where 10\% of galaxies are active at any given time. Estimating this activation rate is important to constrain central black hole feeding mechanisms in galaxy evolution models. Black hole ignition events, which involve a galaxy transitioning from a quiescent or star-forming state to a an AGN are, however, exceptionally challenging to detect.
For our work, we took advantage of the very large public photometric monitorings that are currently ongoing together with machine-learning algorithms for selecting interesting objects. Black hole ignition event candidates were selected form a parent sample of spectrally classified non-active galaxies ($>2.300.000$ objects), that currently show optical flux variability indicative of a type I AGN, according to the ALeRCE light curve classifier. In this talk we will present spectral results for the most convincing case of new AGN activity, for a galaxy with a previous star-forming optical classification, where the confirmation spectrum shows the appearance of prominent, broad Balmer lines without significant changes in the narrow line flux ratios. MIR colors have also evolved from typical non active galaxy colors to AGN-like colors.
#144 |
The deepest and sharpest radio continuum map of the sky: the VLA 10GHz Survey of GOODS-N
Eric Jimenez Andrade1
1 - Institute of Radio Astronomy and Astrophysics/UNAM.
Structural analyses of high-redshift galaxies are key to understanding the physical processes that drive galaxy evolution across cosmic time. While high-resolution observations from the HST and JWST open a window into dust-unobscured star formation and stellar mass content of high-redshift galaxies, radio continuum imaging at sub-arcsec resolution is needed to trace dust-obscured star formation that dominates the star formation rate density of the Universe out to $z\approx5$. To address this open issue, we have conducted the first high-resolution (0.2 arcsec), high-frequency observational campaign to fully map an extragalactic deep field at unprecedented sensitivity: ``The VLA 10GHz Survey of GOODS-N’’. Surveying the extragalactic sky at 10GHz has the advantage of yielding higher angular resolution imaging while probing thermal (free-free) radiation of high-redshift galaxies, which is more directly proportional to the rate of massive star formation. The deep 10GHz images of GOODS-N, thereby, provide an extinction-free view for the morphologies of massive star-forming galaxies out to $z\approx3$ on 1.7kpc scales. In this talk, I will review the key science goals of the “VLA 10GHz Survey of GOODS-N”, present the initial results, and describe the plans for the data release. Finally, I will discuss how the ``VLA 10GHz Survey of GOODS-N’’ will serve as a pathfinder for future ngVLA observations to trace the sub-kpc scale distribution of star formation of high-redshift galaxies.
#247 |
On the nature of type 2 quasars
Gabriel Roberto Hauschild-Roier1
;
Thaisa Storchi-Bergmann
1
Quasars and QSOs are the most luminous objects in the Universe, having bolometric luminosities Lbol > 10$^{46}$ erg/s produced by a Supermassive Black Hole (SMBH) with a high accretion rate in the nucleus of their host galaxies. The SMBH is surrounded by an accretion disk and emitting clouds with velocities in excess of 1000 km/s, surrounded by a dusty molecular torus at ~pc scales. In the Unified Model of AGN (Active Galactic Nuclei), this torus blocks the view of the inner region if observed "edge-on", in the so-called type 2 QSOs. Type 1 QSOs, on the other hand, are supposed to be seen face-on and do not show obscuration. However, there has been some evidence suggesting that these two types of objects do not differ only due to orientation. The goal of this work is to investigate this for a QSO sample, comparing the optical spectral properties of QSO 1 with those of QSOs 2 using, in particular, the [O III] emission-line doublet for the quasar sample from SDSS DR 16, named DR16Q, to investigate a QSO 1 and 2 subsample within 0.4 < z < z 0.5. We found that the [O III] kinematic profile, traced by the W80 parameter, shows that the QSO 2 population has a broader profile than those for the QSOs 1. Moreover, the [O III] luminosity is higher for the QSOs 2 than for the QSOs 1. Both results suggest that there is a difference between these two QSO populations that cannot be fully explained by the AGN Unified Model. Our next step is to check if this difference persists up to z = 1 (when the [O III] doublet goes out of the SDSS wavelength range).
12:30 - 14:30
LUNCH
14:30 - 15:20
Plenary Review Talk
Invited Speaker:
Luis A. Núñez - Universidad Industrial de Santander (Colombia)[cv]
Luis A. Núñez
Universidad Industrial de Santander
Curriculum Vitae:
Experimental particle physics and Astrophysics are global endeavours out of necessity. The sheer scale of designing, constructing, and operating immense equipment, along with managing and analysing vast data sets, often demands the collaboration of hundreds or even thousands of individuals, alongside funding from numerous nations. Participation in these endeavours offers individuals, institutions, and countries access to valuable training, cutting-edge technology, and a wealth of knowledge. However, becoming fully integrated into international experimental research efforts is a process that often spans generations.
During this presentation, we will provide an overview of various initiatives underway in Latin America. One is the BELLA initiative, establishing a state-of-the-art transcontinental fibre optic connecting research and education networks of Europe (GÉANT) and Latin America (RedCLARA). This link facilitates collaborative efforts among academic communities, including Scientific Collaboration on Climate Change, Advanced Computing System for Latin America and the Caribbean (SCALAC) and University Telemedicine Network (RUTE-AL)
Additionally, we will delve into the efforts of the Latin American Strategy Forum for Research Infrastructure (LASF4RI), dedicated to formulating a strategic framework for advancing research infrastructures in high-energy physics, Cosmology, and Astroparticle Physics. This initiative led, in November 2021, to the Latin American Association for High Energy Physics, Cosmology and Astroparticle Physics (LAA-HECAP) aimed at consolidating and expanding the momentum in research within these fields.
We will also detail LA-CoNGA physics, an ERASMUS+ initiative focused on modernising university infrastructure and enhancing pedagogical offerings in advanced physics. This exemplifies a collaboration between Europe and Latin America to train the next generation of HECAP physicists through a virtual teaching and research network involving three European universities and eight in Latin America, as well as scientific and industrial partners.
Finally, we will explore strategies for aligning these initiatives with the needs and aspirations of the Astronomy, Astrophysics, and Space Science community in Latin America.
Chair: Carlos Román
#598 |
Empowering Latin American Research: Initiatives in Particle Physics, Astroparticle, and more
Luis A. Núñez1
1 - Escuela de Física, Universidad Industrial de Santander.
Experimental particle physics and Astrophysics are global endeavours out of necessity. The sheer scale of designing, constructing, and operating immense equipment, along with managing and analysing vast data sets, often demands the collaboration of hundreds or even thousands of individuals, alongside funding from numerous nations. Participation in these endeavours offers individuals, institutions, and countries access to valuable training, cutting-edge technology, and a wealth of knowledge. However, becoming fully integrated into international experimental research efforts is a process that often spans generations.
During this presentation, we will provide an overview of various initiatives underway in Latin America. One is the BELLA initiative, establishing a state-of-the-art transcontinental fibre optic connecting research and education networks of Europe (GÉANT) and Latin America (RedCLARA). This link facilitates collaborative efforts among academic communities, including Scientific Collaboration on Climate Change, Advanced Computing System for Latin America and the Caribbean (SCALAC) and University Telemedicine Network (RUTE-AL)
Additionally, we will delve into the efforts of the Latin American Strategy Forum for Research Infrastructure (LASF4RI), dedicated to formulating a strategic framework for advancing research infrastructures in high-energy physics, Cosmology, and Astroparticle Physics. This initiative led, in November 2021, to the Latin American Association for High Energy Physics, Cosmology and Astroparticle Physics (LAA-HECAP) aimed at consolidating and expanding the momentum in research within these fields.
We will also detail LA-CoNGA physics, an ERASMUS+ initiative focused on modernising university infrastructure and enhancing pedagogical offerings in advanced physics. This exemplifies a collaboration between Europe and Latin America to train the next generation of HECAP physicists through a virtual teaching and research network involving three European universities and eight in Latin America, as well as scientific and industrial partners.
Finally, we will explore strategies for aligning these initiatives with the needs and aspirations of the Astronomy, Astrophysics, and Space Science community in Latin America.
15:20 - 16:00
COFFEE BREAK
16:00 - 17:30
J: Galaxies and Cosmology
AGN / Supermassive Black Holes
#283 |
Ionized gas outflows vs. maintenance mod feedback in MaNGA AGN
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.
#466 |
First observation of double-peaked OI emission in the near-infrared spectrum of an active galaxy
Denimara Dias dos Santos1
;
Alberto Rodríguez-Ardila
2
;
Swayamtrupta Panda
2
;
Murilo Marinello
2
1 - Instituto Nacional de Pesquisas Espaciais.2 - Laboratório Nacional de Astrofísica.
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.
#185 |
Probing the rapid formation of black holes and their Galaxy hosts in QSOs
Karla Alejandra Cutiva Alvarez1
;
Roger Coziol
1
;
Juan Pablo Torres Papaqui
1
\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}
#302 |
Unveiling Spectroscopic Confirmation and Characterization of Bright Galaxies at $\gtrsim$ 8 with JWST
1 - University of California, Los Angeles.2 - The University of Texas at Austin.3 - University of Geneva.4 - AURA/NOIRLab.5 - Max Planck Institute for Astronomy.6 - NASA Goddard Space Flight Center.7 - Rochester Institute of Technology.8 - National Astronomical Research Institute of Thailand.9 - University of Copenhagen / DAWN.10 - Caltech/IPAC.11 - Rutgers University/ Flatiron Institute.12 - University of Melbourne.13 - Space Telescope Science Institute.
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.
#462 |
Dusty star-forming galaxies as tracers of protoclusters: A simulated perspective
Pablo Araya Araya1
;
Rachel Cochrane
2
;
Christopher Hayward
2
;
Douglas Rennehan
3
;
Laerte Sodré Jr.
1
;
Robert Yates
4
;
Roderik Overzier
5
;
Marcelo Vicentin
1
1 - Universidade de São Paulo.2 - Flatiron Institute (CCA).3 - Flatiron Institute.4 - University of Hertfordshire.5 - Observatório Nacional.
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.
#028 |
The relation between globular cluster systems and supermassive black holes in spiral galaxies III. The link to the $M_\bullet - M_\ast$ correlation.
Rosa A. Gonzalez Lopez Lira1
;
Luis Lomelí-Núñez
2
;
Yasna Ordenes-Briceño
3
;
Laurent Loinard
1
;
Stephen Gwyn
4
;
Karla Alamo-Martínez
5
;
Gustavo Bruzual
1
;
Ariane Lançon
6
;
Thomas Puzia
3
1 - UNAM.2 - Universidade Federal do Rio de Janeiro.3 - Pontificia Universidad Católica de Chile.4 - Herzberg Institute of Astrophysics.5 - Universidad de Guanajuato.6 - Université de Strasbourg.
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.