We present our mass estimate of the central black hole in the isolated spiral galaxy NGC 4414. Using natural guide star adaptive optics assisted observations with the Gemini Near-Infrared Integral ...Field Spectrometer (NIFS) and the natural seeing Gemini Multi-Object Spectrographs-North (GMOS), we derived two-dimensional stellar kinematic maps of NGC 4414 covering the central 1.5 arcsec and 10 arcsec, respectively, at a NIFS spatial resolution of 0.13 arcsec. The kinematic maps reveal a regular rotation pattern and a central velocity dispersion dip down to around 105 km s-1. We constructed dynamical models using two different methods: Jeans anisotropic dynamical modeling and axisymmetric Schwarzschild modeling. Both modeling methods give consistent results, but we cannot constrain the lower mass limit and only measure an upper limit for the black hole mass of MBH = 1.56 × 106M⊙ (at 3σ level) which is at least 1σ below the recent MBH−σe relations. Further tests with dark matter, mass-to-light ratio variation and different light models confirm that our results are not dominated by uncertainties. The derived upper limit mass is not only below the MBH−σe relation, but is also five times lower than the lower limit black hole mass anticipated from the resolution limit of the sphere of influence. This proves that via high quality integral field data we are now able to push black hole measurements down to at least five times less than the resolution limit.
Star formation rates (SFRs), gas-phase metallicities, and stellar masses are crucial for studying galaxy evolution. The different relations resulting from these properties give insights into the ...complex interplay of gas inside galaxies and their evolutionary trajectory and current characteristics. We aim to characterize these relations at $z 0.3$, corresponding to a 3-4 Gyr lookback time, to gather insight into the galaxies' redshift evolution. We utilized optical integral field spectroscopy data from 65 emission-line galaxies from the MUSE large program MAGPI at a redshift of $0.28<z<0.35$ (average redshift of $z 0.3$) and spanning a total stellar mass range of $8.2< /M_ odot ) < 11.4$. We measured emission line fluxes and stellar masses, allowing us to determine spatially resolved SFRs, gas-phase metallicities, and stellar mass surface densities. We derived the resolved star formation main sequence (rSFMS), resolved mass metallicity relation (rMZR), and resolved fundamental metallicity relation (rFMR) at $z 0.3$, and compared them to results for the local Universe. We find a relatively shallow rSFMS slope of $ 0.014$ compared to the expected slope at this redshift for an ordinary least square (OLS) fitting routine. For an orthogonal distance regression (ODR) routine, a much steeper slope of $ 0.022$ is measured. We confirm the existence of an rMZR at $z 0.3$ with an average metallicity located $ 0.03$ dex above the local Universe's metallicity. Via partial correlation coefficients, evidence is found that the local metallicity is predominantly determined by the stellar mass surface density and has a weak secondary (inverse) dependence on the SFR surface density $ SFR $. Additionally, a significant dependence of the local metallicity on the total stellar mass $M_ $ is found. Furthermore, we find that the stellar mass surface density $ $ and $M_ $ have a significant influence in determining the strength with which $ SFR $ correlates with the local metallicity. We observe that at lower stellar masses, there is a tighter correlation between $ SFR $ and the gas-phase metallicity, resulting in a more pronounced rFMR.
ABSTRACT Studies of the internal mass structure of galaxies have observed a ‘conspiracy’ between the dark matter and stellar components, with total (stars$+$dark) density profiles showing remarkable ...regularity and low intrinsic scatter across various samples of galaxies at different redshifts. Such homogeneity suggests the dark and stellar components must somehow compensate for each other in order to produce such regular mass structures. We test the conspiracy using a sample of 22 galaxies from the ‘Middle Ages Galaxy Properties with Integral field spectroscopy’ Survey that targets massive galaxies at $z \sim 0.3$. We use resolved, 2D stellar kinematics with the Schwarzschild orbit-based modelling technique to recover intrinsic mass structures, shapes, and dark matter fractions. This work is the first implementation of the Schwarzschild modelling method on a sample of galaxies at a cosmologically significant redshift. We find that the variability of structure for combined mass (baryonic and dark) density profiles is greater than that of the stellar components alone. Furthermore, we find no significant correlation between enclosed dark matter fractions at the half-light radius and the stellar mass density structure. Rather, the total density profile slope, $\gamma _{\mathrm{tot}}$, strongly correlates with the dark matter fraction within the half-light radius, as $\gamma _{\mathrm{tot}} = (1.3 \pm 0.2) f_{\mathrm{DM}} - (2.44 \pm 0.04)$. Our results refute the bulge–halo conspiracy and suggest that stochastic processes dominate in the assembly of structure for massive galaxies.
Studies of the internal mass structure of galaxies have observed a `conspiracy' between the dark matter and stellar components, with total (stars \(+\) dark) density profiles showing remarkable ...regularity and low intrinsic scatter across various samples of galaxies at different redshifts. Such homogeneity suggests the dark and stellar components must somehow compensate for each other in order to produce such regular mass structures. We test the conspiracy using a sample of 22 galaxies from the `Middle Ages Galaxy Properties with Integral field spectroscopy' (MAGPI) Survey that targets massive galaxies at \( z \sim 0.3\). We use resolved, 2D stellar kinematics with the Schwarzschild orbit-based modelling technique to recover intrinsic mass structures, shapes, and dark matter fractions. This work is the first implementation of the Schwarzschild modelling method on a sample of galaxies at a cosmologically significant redshift. We find that the variability of structure for combined mass (baryonic and dark) density profiles is greater than that of the stellar components alone. Furthermore, we find no significant correlation between enclosed dark matter fractions at the half-light radius and the stellar mass density structure. Rather, the total density profile slope, \(\gamma_{\mathrm{tot}}\), strongly correlates with the dark matter fraction within the half-light radius, as \(\gamma_{\mathrm{tot}} = (1.3 \pm 0.2) f_{\mathrm{DM}} - (2.44 \pm 0.04)\). Our results refute the bulge-halo conspiracy and suggest that stochastic processes dominate in the assembly of structure for massive galaxies.
Star formation rates (SFRs), gas-phase metallicities, and stellar masses are crucial for studying galaxy evolution. The different relations resulting from these properties give insights into the ...complex interplay of gas inside galaxies and their evolutionary trajectory and current characteristics. We aim to characterize these relations at \(z\sim 0.3\), corresponding to a 3-4 Gyr lookback time. We utilized optical integral field spectroscopy of 65 emission-line galaxies from the MAGPI survey at a redshift of \(0.28<z<0.35\) and spanning a total stellar mass range of \(8.2<\log(M_{*}/M_{\odot}) < 11.4\). We derived the resolved star formation main sequence (rSFMS), resolved mass metallicity relation (rMZR), and resolved fundamental metallicity relation (rFMR) at \(z\sim 0.3\). We find a relatively shallow rSFMS slope of \(\sim 0.425 \pm 0.014\) compared to the expected slope at this redshift for an ordinary least square (OLS) fitting routine. For an orthogonal distance regression (ODR) routine, a much steeper slope of \(\sim 1.162 \pm 0.022\) is measured. We confirm the existence of an rMZR at \(z\sim 0.3\) with an average metallicity located \(\sim 0.03\) dex above the local Universe's metallicity. Via partial correlation coefficients, evidence is found that the local metallicity is predominantly determined by the stellar mass surface density and has a weak secondary (inverse) dependence on the SFR surface density \(\Sigma_{SFR}\). Additionally, a significant dependence of the local metallicity on the total stellar mass \(M_{*}\) is found. Furthermore, we find that the stellar mass surface density \(\Sigma_{*}\) and \(M_{*}\) have a significant influence in determining the strength with which \(\Sigma_{SFR}\) correlates with the local metallicity. We observe that at lower stellar masses, there is a tighter correlation between \(\Sigma_{SFR}\) and the gas-phase metallicity, resulting in a more pronounced rFMR.
Galaxy gas kinematics are sensitive to the physical processes that contribute
to a galaxy's evolution. It is expected that external processes will cause more
significant kinematic disturbances in the ...outer regions, while internal
processes will cause more disturbances for the inner regions. Using a subsample
of 47 galaxies ($0.27<z<0.36$) from the Middle Ages Galaxy Properties with
Integral Field Spectroscopy (MAGPI) survey, we conduct a study into the source
of kinematic disturbances by measuring the asymmetry present in the ionised gas
line-of-sight velocity maps at the $0.5R_e$ (inner regions) and $1.5R_e$ (outer
regions) elliptical annuli. By comparing the inner and outer kinematic
asymmetries, we aim to better understand what physical processes are driving
the asymmetries in galaxies. We find the local environment plays a role in
kinematic disturbance, in agreement with other integral field spectroscopy
studies of the local universe, with most asymmetric systems being in close
proximity to a more massive neighbour. We do not find evidence suggesting that
hosting an Active Galactic Nucleus (AGN) contributes to asymmetry within the
inner regions, with some caveats due to emission line modelling. In contrast to
previous studies, we do not find evidence that processes leading to asymmetry
also enhance star formation in MAGPI galaxies. Finally, we find a weak
anti-correlation between stellar mass and asymmetry (ie. high stellar mass
galaxies are less asymmetric). We conclude by discussing possible sources
driving the asymmetry in the ionised gas, such as disturbances being present in
the colder gas phase (either molecular or atomic) prior to the gas being
ionised, and non-axisymmetric features (e.g., a bar) being present in the
galactic disk. Our results highlight the complex interplay between ionised gas
kinematic disturbances and physical processes involved in galaxy evolution.
Galaxy gas kinematics are sensitive to the physical processes that contribute to a galaxy's evolution. It is expected that external processes will cause more significant kinematic disturbances in the ...outer regions, while internal processes will cause more disturbances for the inner regions. Using a subsample of 47 galaxies (\(0.27<z<0.36\)) from the Middle Ages Galaxy Properties with Integral Field Spectroscopy (MAGPI) survey, we conduct a study into the source of kinematic disturbances by measuring the asymmetry present in the ionised gas line-of-sight velocity maps at the \(0.5R_e\) (inner regions) and \(1.5R_e\) (outer regions) elliptical annuli. By comparing the inner and outer kinematic asymmetries, we aim to better understand what physical processes are driving the asymmetries in galaxies. We find the local environment plays a role in kinematic disturbance, in agreement with other integral field spectroscopy studies of the local universe, with most asymmetric systems being in close proximity to a more massive neighbour. We do not find evidence suggesting that hosting an Active Galactic Nucleus (AGN) contributes to asymmetry within the inner regions, with some caveats due to emission line modelling. In contrast to previous studies, we do not find evidence that processes leading to asymmetry also enhance star formation in MAGPI galaxies. Finally, we find a weak anti-correlation between stellar mass and asymmetry (ie. high stellar mass galaxies are less asymmetric). We conclude by discussing possible sources driving the asymmetry in the ionised gas, such as disturbances being present in the colder gas phase (either molecular or atomic) prior to the gas being ionised, and non-axisymmetric features (e.g., a bar) being present in the galactic disk. Our results highlight the complex interplay between ionised gas kinematic disturbances and physical processes involved in galaxy evolution.
Humans use rich natural language to describe and communicate visual perceptions. In order to provide natural language descriptions for visual content, this paper combines two important ingredients. ...First, we generate a rich semantic representation of the visual content including e.g. object and activity labels. To predict the semantic representation we learn a CRF to model the relationships between different components of the visual input. And second, we propose to formulate the generation of natural language as a machine translation problem using the semantic representation as source language and the generated sentences as target language. For this we exploit the power of a parallel corpus of videos and textual descriptions and adapt statistical machine translation to translate between our two languages. We evaluate our video descriptions on the TACoS dataset, which contains video snippets aligned with sentence descriptions. Using automatic evaluation and human judgments we show significant improvements over several baseline approaches, motivated by prior work. Our translation approach also shows improvements over related work on an image description task.
Different massive black hole mass – host galaxy scaling relations suggest that the growth of massive black holes is entangled with the evolution of their host galaxies. The number of measured black ...hole masses is still limited and additional measurements are necessary to understand the underlying physics of this apparent coevolution. We add six new black hole mass (MBH) measurements of nearby fast rotating early-type galaxies to the known black hole mass sample, namely NGC 584, NGC 2784, NGC 3640, NGC 4570, NGC 4281, and NGC 7049. Our target galaxies have effective velocity dispersions (σe) between 170 and 245 km s−1, and thus this work provides additional insight into the black hole properties of intermediate-mass early-type galaxies. We combined high-resolution adaptive-optics SINFONI data with large-scale MUSE, VIMOS and SAURON data from ATLAS3D to derive two-dimensional stellar kinematics maps. We then built both Jeans Anisotropic Models and axisymmetric Schwarzschild models to measure the central black hole masses. Our Schwarzschild models provide black hole masses of (1.3 ± 0.5) × 108 M⊙ for NGC 584, (1.0 ± 0.6) × 108 M⊙ for NGC 2784, (7.7 ± 5) × 107 M⊙ for NGC 3640, (5.4 ± 0.8) × 108 M⊙ for NGC 4281, (6.8 ± 2.0) × 107 M⊙ for NGC 4570, and (3.2 ± 0.8) × 108 M⊙ for NGC 7049 at 3σ confidence level, which are consistent with recent MBH−σe scaling relations. NGC 3640 has a velocity dispersion dip and NGC 7049 a constant velocity dispersion in the center, but we can clearly constrain their lower black hole mass limit. We conclude our analysis with a test on NGC 4570 taking into account a variable mass-to-light ratio (M/L) when constructing dynamical models. When considering M/L variations linked mostly to radial changes in the stellar metallicity, we find that the dynamically determined black hole mass from NGC 4570 decreases by 30%. Further investigations are needed in the future to account for the impact of radial M/L gradients on dynamical modeling.
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