adsabs/AstroCLIMB huggingface dataset:
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: (a) Plot of the fractional abundances with respect to CS between the observation with ALMA and the NRO 45 m telescope. Blue open circles and red filled circles represent the abundances in the CND at the 350 pc scale and those in the AGN at the 60 pc scale, respectively. These results represent the abundance correlation between the 350 and 1.2 kpc scales, and between the 60 and 1.2 kpc scales. Plots with the bold dashed line represent the same abundance without dependence on the observational scale. Arrows indicate increasing or decreasing abundance from 350 pc to the 60 pc scale. (b) Fractional abundances with respect to CS normalized by the NRO 45 m telescope traced on a 1.2 kpc scale. The bold dashed line represents an abundance ratio of unity.
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: Fractional abundances relative to CS in (a) the 350 pc scale and (b) the 60 pc scale. Ratios over unity, which is indicated by the bold dashed line, represent the enhancement of molecular abundances relative to CS. White arrows indicate the upper limits of the relative abundances. The order of the molecules is arranged in descending order from left to right based on the difference between the CND and the SBR for (a) and between the AGN and the SBR for (b). Therefore, the molecules on the left side of CS are enhancements in the CND (or AGN) compared with the SBR; in contrast, those on the right side of CS are enhancements in the SBR. Note that C34S, SO, HC15N, and HC18O+ are not detected in both the CND (or AGN) and SBR.
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: Column density ratios of (a) N(HCN)/N(HCO+) and (b) N(H13CN)/N(H13CO+). The values with the IRAM 30 m telescope and the NRO 45 m telescope are taken from Aladro et al. (2015) and Nakajima et al. (2018), respectively. The red and blue columns represent the values in the CND (or AGN) of NGC 1068 and in the SBR of NGC 1068 or starburst galaxies, respectively. The light blue columns in (b) represent the upper limit of both the numerator and denominator of a fraction because both H13CN and H13CO+ are not detected.
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: Obtained spectra with a spatial resolution of 0.″9 (∼60 pc) from 85–114 GHz in the AGN, the E-knot, the W-knot, and the SBR (from top down). The vertical and horizontal axes are the beam-averaged flux density and rest frequency, respectively. The velocity resolution is 20 km s−1, and the primary beam correction is applied. The names of major molecular line carriers are indicated above the spectra.
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: Enlarged spectra with a spatial resolution of 0.″9 (∼60 pc) from 85–95 GHz in four regions (see the caption of Figure 9). The vertical and horizontal axes are the beam-averaged flux density and rest frequency, respectively. The velocity resolution is 20 km s−1, and the primary beam correction is applied. The shaded regions represent the range of the ± 1σ noise level. The names of the molecular line carriers, for which the peak flux is more than 1σ, are indicated above the spectra.
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: Plots of the fractional abundances relative to CS (a) between CND and SBR with a 350 pc scale, (b) between AGN and SBR with a 60 pc scale, (c) between E-knot and SBR with a 60 pc scale, and (d) between W-knot and SBR with a 60 pc scale. These results represent the abundance correlation between the CND and the SBR. Plots above the bold dashed line represent the enhanced molecules and plots below represent deficient ones in the CND (or AGN).
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: Comparison of column densities of each molecule in (a) 350 pc scale and (b) 60 pc scale. The bar graphs in red, blue, green, and black are for the CND (or AGN), the E-knot, the W-knot, and the SBR, respectively. The order of molecules is arranged in descending order from left to right based on the column density toward CND in (a) or AGN in (b). Arrows indicate upper limits.
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: Enlarged spectra with a spatial resolution of 0.″9 (∼60 pc) from 105–114 GHz in four regions (see the caption of Figure 9).
Paper: Molecular Abundance of the Circumnuclear Region Surrounding an Active Galactic Nucleus in NGC 1068 Based on an Imaging Line Survey in the 3 mm Band with ALMA
Authors: Taku Nakajima, Shuro Takano, Tomoka Tosaki, Akio Taniguchi, Nanase Harada, Toshiki Saito, Masatoshi Imanishi, Yuri Nishimura, Takuma Izumi, Yoichi Tamura, Kotaro Kohno, Eric Herbst
Figure caption: Enlarged spectra with a spatial resolution of 0.″9 (∼60 pc) from 95–105 GHz in four regions (see the caption of Figure 9).
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: The angular momentum evolution of the inflowing gas particles since redshift of 0.4 for two individual galaxies: ID-342447 (top panels) and ID-503437 (bottom panels). The inflowing gas particles can later be either outflowing gas particles, stellar particles, or remaining gas particles (see text). We therefore show the cumulative mass of inflowing gas particles, as well as the mass of three different components (the cumulative mass of outflowing particles and the instantaneous masses of stellar and gas particles) in the left column of panels. We can check that the combination of the three components equals the cumulative mass of inflowing gas particles at any epoch, as a consistency check. The middle column of panels show the cumulative angular momentum for the inflowing gas particles, as well as the three different components (the cumulative angular momentum for the outflowing gas particles, and the angular momentum of instantaneous stellar and gas particles). The right column of panels show the evolution of the mean specific angular momentum of the inflowing gas, outflowing gas, remaining gas, and the newly formed stellar particles (defined at the corresponding epochs rather than the cumulative particles).
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: Illustration of the definition of net inflow rate with one individual TNG50 galaxy (ID:342447). Top left panel: the red line shows the cumulative SFR as a function of radius, i.e., SFR(<r). The blue dashed line shows the inflow rate as a function of radius, the cyan dashed line shows the outflow rate as a function of radius, and the blue solid line shows the net inflow rate as a function of radius. The green line shows the change rate of cumulative gas mass as a function of radius. We can check that the net inflow rate within a given r equals the SFR(<r) plus the ﹩{\dot{M}}_{\mathrm{gas}}(\lt r)﹩, which is shown in the red dashed line (net inflow rate minus SFR(<r) and ﹩{\dot{M}}_{\mathrm{gas}}(\lt r)﹩). We note that all these quantities are measured between the two snapshots of z = 0.0 and z = 0.4. The other three panels are the same as the top left panel, but all these quantities are measured between two snapshots of shorter time intervals, as denoted in each panel.
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: Illustration of the radial migration of stellar particles with two TNG50 individual galaxies: ID-342447 (top panels) and ID-503437 (bottom panels). Left panels: The radial distribution of the Σ* at the current epoch (z = 0.0) for those stellar particles that formed prior to a set of different redshifts. Right panels: The evolution of Σ* for the individual galaxies, found by tracing their main progenitors in the merging tree at different snapshots. Therefore, by comparing of left and right panels, one can imagine that the differences are due to the radial migration of stellar particles and mergers.
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: The ratio of net inflow rate to SFR(<r) as a function of radius for the TNG50 galaxies of the four stellar mass bins. In each panel, the red line shows the mean profile of the TNG50 galaxies of the corresponding stellar mass bin. The green horizontal line shows the value of Φ/ SFR expected from the cosmic evolution of SFMS (see text).
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: The mass-weighted distribution of the change of specific angular momentum, Δj (see the detailed definition in text), for individual inflowing gas particles (being either outflowing gas particles, stellar particles, or remaining gas particles). We calculate the Δj for all the sample galaxies of TNG50 by tracing the inflowing particles from z = 0.4 to z = 0.2 (to save computing time). As above, the results are shown for the four stellar mass bins. In each panel, we indicate the mass-weighted average Δj for the three cases with the corresponding colors, and show the mass-weighted average Δj for all of the inflowing particles in the vertical dashed line in each panel.
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: The distribution of ﹩{r}_{\max }﹩ for TNG50 (red histograms) and MaNGA (blue histograms) galaxies. The ﹩{r}_{\max }﹩ roughly corresponds to the radius within which 80% of star formation is enclosed for each galaxy. The red and blue vertical dashed lines indicate the median values of ﹩{r}_{\max }﹩ for TNG50 and MaNGA, respectively. As above, galaxies are separated into four stellar mass bins.
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: The mass-weighted age profiles for TNG50 galaxies (red lines) and MaNGA galaxies (blue lines). The red and blue diamonds show the median age profiles for TNG50 and MaNGA, respectively. As above, we show the result in the four stellar mass bins.
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: The cumulative SFR(<r), net inflow rate, and ﹩{\dot{M}}_{\mathrm{gas}}(\lt r)﹩ as a function of radius for the TNG50 galaxies. As above, galaxies are separated into the four stellar mass bins in showing the result.
Paper: The Formation of Star-forming Disks in the TNG50 Simulation
Authors: Enci Wang, Simon J. Lilly
Figure caption: The stellar surface mass density profiles for TNG50 galaxies. As above, we show the result for the four stellar mass bins, as denoted in each panel.
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: Isothermal, 2563 (circle symbols) and 5123 (diamond symbols, bottom panel only) simulations with streaming and P CR ∼ P  g . The MHD (undamped) version of these simulations give ﹩{{ \mathcal M }}_{{\rm{s}}}={v}_{0}/{c}_{s}\sim ﹩ 0.15 (black), 0.5 (green), and 0.75 (cyan). The top panel shows only the ﹩{{ \mathcal M }}_{{\rm{s}}}\sim 0.15﹩ points and shows the partitioning of turbulent forcing that ends up in CRs (﹩{f}_{\mathrm{CR}}={\dot{E}}_{\mathrm{CR}}/\tilde{\epsilon };﹩ green points and right y-axis), as well as ﹩{f}_{E}=(\rho {v}^{3}/L)/\tilde{\epsilon }﹩ (black points and left y-axis) vs. the steady-state plasma beta β  f . While for diffusion there was a clear correlation between f CR and f  E , now, f CR is small, and f  E  correlates inversely with β, at least in this sub-Alfvénic regime studied. The bottom panel shows the turbulent kinetic energy relative to the undamped case, where ﹩\rho {v}_{0}^{3}/L\sim \tilde{\epsilon }﹩. With CRs, even with streaming-only transport where there is no reacceleration, ﹩{v}^{2}/{v}_{0}^{2}\propto {\beta }^{-1/2}﹩, at least roughly, in this sub-Alfvénic or “fast-transport” regime. There is also a weak trend toward larger overall damping with increasing driving rate (larger ﹩{{ \mathcal M }}_{s}﹩ has smaller ﹩{v}^{2}/{v}_{0}^{2}﹩), at fixed β.
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: Kinetic energy spectra for ﹩{{ \mathcal M }}_{{\rm{s}}}\sim 0.15﹩, 2563 simulations each with P CR/P  g  ∼ 1 but varying CR transport and varying the initial plasma β from 1 (top) to 10 (middle) to 100 (bottom). The magenta-colored lines show the resulting MHD (no CR) spectra as a reference. The left column shows k 2 E(k)dk normalized by the MHD value at k = 3, while, to more clearly show the changes in spectral shape, the right column shows the ratio of each spectrum to the MHD spectrum. For diffusion only, efficient reacceleration damps the kinetic energy spectrum, resulting in less power at small scales compared to the MHD case. However, with streaming included, both reacceleration rates and field-aligned CR pressure gradients depend on β. At low β (low Alfvén Mach number ﹩{{ \mathcal M }}_{{\rm{A}}}=v/{v}_{{\rm{A}}}﹩), streaming negates reacceleration, and the kinetic energy spectra revert to the MHD case. For larger β, however, reacceleration becomes somewhat more efficient, causing damping, and a more significant fraction of turbulent energy is channeled through CRs and lost via streaming energy transfer. This latter effect, most clearly evident in the streaming-only simulations (red curves), decreases the overall kinetic energy in the system but does not appear to induce cutoffs like the diffusion-only runs.
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: Top row: kinetic energy spectra, multiplied by k 2 and normalized to the k = 3 MHD value, decomposed into compressive (solid lines) and solenoidal (dashed lines) components. Each simulation was run on a 5123 grid. The left panel shows β ∼ 10 simulations, where solenoidal power is a significant fraction of the total power and dominates at small scales, leading to a shallower than k −2 spectrum. The right panel shows β ∼ 100 simulations, where compressive modes are dominant at almost all scales in the MHD case. CRs considerably damp the compressive fluctuations, though, which in turn decreases the power in solenoidal motions that are generated by a combination of compressions and magnetic tension. In both the β ∼ 10 and β ∼ 100 cases with streaming, compressive damping leads to an increased ratio of solenoidal to compressive power. However, this “divergence cleaning” is not pronounced in the pure diffusion run, where solenoidal and compressive power decrease by about the same amount. Bottom row: power in velocity fluctuations v  x  along the initial mean magnetic field divided by the power in total velocity fluctuations. This quick measure of anisotropy roughly tracks the compressive vs. solenoidal motions seen above: with CR streaming present, CR damping leads to more anisotropy (higher fraction of v  x  power), consistent with a larger fraction of anisotropic solenoidal modes rather than isotropic compressive modes. The diffusion-only case, which shows a kink at high-k, is an outlier whose analysis we leave for future work.
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: Kinetic energy spectra (left), magnetic energy spectra (middle), and CR energy spectra (right) multiplied by k 2 for 5123, β ∼ 10 simulations with varying κ. Note that the left panel is the same as in Figure 6 and that the y-axis of the right panel extends down to 10−3 rather than 10−2 for the other panels. Overall, magnetic energy spectra follow the same trend as kinetic energy spectra, showing damped small-scale power when the diffusivity is near the sweet spot κ ∼ 0.15L 0 c  s . CR energy spectra instead show an approximately monotonic decrease in small-scale power with increasing diffusivity, as strong diffusion damps small-scale CR perturbations.
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: Kinetic energy spectra for a partial simulation suite run on a 5123 grid instead of a 2563 grid (compare to Figure 8 in Section 4.4). Computer resource limits prohibit us from running the streaming-only (κ ∼ 0 + streaming) simulations of Section 4.4 on a 5123 domain, but all other spectra look qualitatively similar to those on a 2563 grid; namely, diffusion-only transport shows clear differences in spectral slope at both β = 1 and 10. Streaming simulations instead appear to uniformly decrease kinetic energy at all scales as β increases. Note there is some resolution dependence for β = 10, with 5123 showing less damping compared to the 2563, but the difference is mild, especially in comparison to the diffusion-only simulations.
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: Fluctuating density (blue symbols), velocity (black symbols), and CR pressure (green symbols) as a function of P CR/P  g . Open circles denote simulations with nonzero diffusion coefficient κ ∣∣ ∼ 0.15L 0 v ph, and open diamonds denote purely advective CR transport (κ = 0). None of these simulations include additional streaming transport.
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: Comparison of kinetic energy without CRs (MHD) and with CRs but no transport (κ ∣∣ ∼ 0), simulated on grids with 2563 and 5123 cells. Note that 5123 simulation results are divided by a factor of 10 to separate those curves from the 2563 results.
Paper: Cosmic-Ray Drag and Damping of Compressive Turbulence
Authors: Chad Bustard, S. Peng Oh
Figure caption: Time convergence of select spectra, each run on a 2563 grid. The diffusion-only simulations, which show the most damping, converge very early. Note that 5123 simulations (not shown) are similarly converged with respect to time.
Paper: Direct Collapse to Precursors of Supermassive Black Hole Seeds: Radiation-feedback-generated Outflows
Authors: Yang Luo, Isaac Shlosman, Kentaro Nagamine
Figure caption: Evolution of the outflow from the sink particle and the surrounding accretion disk driven by the radiation feedback. The slice snapshots are shown on the scale of 2 × 10−2 pc and 2.0 pc. Top row: the arrows indicate the direction and the value of the outflow velocities. Second row: from left to right, an anisotropic outflow is generated above and below the disk. The long red arrow in the panel at t = 0 points to the position of the sink. At t = 0, the outflow is not yet visible and the accretion dominates. The t = 1000 yr snapshot displays a developing outflow in the upper hemisphere and a growing cavity there. At t = 2000 yr, the outflow is substantially collimated and pushes the gas into an expanding shell, outlining the low-density cavity. The t = 3000 yr snapshot shows the biconical outflow, which has expanded beyond the disk. The upper and lower bubbles are asymmetric. Note the dominance of the outflow and generated bubble below the accretion disk.
Paper: Direct Collapse to Precursors of Supermassive Black Hole Seeds: Radiation-feedback-generated Outflows
Authors: Yang Luo, Isaac Shlosman, Kentaro Nagamine
Figure caption: Growth rate of the sink particle due to accretion (top) and the accretion luminosity from the sink and the surrounding accretion disk (bottom). The time t = 0 corresponds to the time when the sink particle reaches 105 M ⊙ and when the radiation feedback has been initiated. Prior to this, the sink particle grew from 10 to 105 M ⊙ without feedback. Its growth is negligible over the time of the run with radiation feedback, 3 × 103 yr. Red dashed lines show the Eddington accretion rate onto the sink assuming only the electron scattering opacity (top panel) and the Eddington luminosity (bottom panel). The observed noise in the accretion rate is twofold: the natural variation and the radiation feedback. Both lead to episodic accretion. The outflow generated by the feedback does not totally suppress the accretion, and the sink particle can still grow at a high rate.
Paper: Direct Collapse to Precursors of Supermassive Black Hole Seeds: Radiation-feedback-generated Outflows
Authors: Yang Luo, Isaac Shlosman, Kentaro Nagamine
Figure caption: Accretion disk structure around the sink particle forming on a scale of ∼0.1 pc. Shown are (top to bottom) the cylindrical radial profiles of the surface density, Σ(r), temperature, T(r), inflow velocity, v  r , and mass accretion rate in the disk, ﹩{\dot{M}}_{d,\mathrm{acc}}﹩, as a function of the cylindrical radius at different times. Note that accretion proceeds also at other polar angles—this accretion is not included in the disk accretion rate shown here.
Paper: A High-mass, Young Star-forming Core Escaping from Its Parental Filament
Authors: Zhiyuan Ren, 致远 任, Xi Chen, 曦 陈, Tie Liu, 铁 刘, Emma Mannfors, Leonardo Bronfman, Fengwei Xu, 峰玮 许, Siyi Feng, 思轶 冯, Hongli Liu, 洪礼 刘, Fanyi Meng, 繁一 孟, Amelia M. Stutz, Shanghuo Li, 尚活 李, Chang Won Lee, Ke Wang, 科 王, Jianwen Zhou, 建文 周, Di Li, 菂 李, Chen Wang, 晨 王, Chakali Eswaraiah, Anandmayee Tej, Long-Fei Chen, 龙飞 陈, Hui Shi, 惠 石
Figure caption: (a) The HCO+ outflow lobes overlaid on the HCO+ excitation temperature map. The line intensity is converted to T ex using Equation (A3). The contour levels are 15%–90% of the maximum intensity, which is 22.6 and 22.9 K km s−1 for the blue and red lobes, respectively. (b, c) The molecular spectra at selected cores. For each spectrum, the horizontal line represents the zero-level baseline. The vertical dashed line denotes the division between the blueshift gas (M1 core) and main-filament components.