adsabs/AstroCLIMB huggingface dataset:
Paper: To High Redshift and Low Mass: Exploring the Emergence of Quenched Galaxies and Their Environments at 3 < z < 6 in the Ultra-deep JADES MIRI F770W Parallel
Authors: Stacey Alberts, Christina C. Williams, Jakob M. Helton, Katherine A. Suess, Zhiyuan Ji, Irene Shivaei, Jianwei Lyu, George Rieke, William M. Baker, Nina Bonaventura, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Emma Curtis-Lake, Francesco D'Eugenio, Daniel J. Eisenstein, Anna de Graaff, Kevin N. Hainline, Ryan Hausen, Benjamin D. Johnson, Roberto Maiolino, Eleonora Parlanti, Marcia J. Rieke, Brant E. Robertson, Yang Sun, Sandro Tacchella, Christopher N. A. Willmer, Chris J. Willott
Figure caption: Properties of the tentative poststarburst galaxies selected via B19. Top rows for each source: F606W, F090W, F200W, F444W, F770W cutouts, 1.″2 on a side. Bottom rows for each source: the SEDs (left), SSFR posterior distributions (middle), and SFHs (right).
Paper: To High Redshift and Low Mass: Exploring the Emergence of Quenched Galaxies and Their Environments at 3 < z < 6 in the Ultra-deep JADES MIRI F770W Parallel
Authors: Stacey Alberts, Christina C. Williams, Jakob M. Helton, Katherine A. Suess, Zhiyuan Ji, Irene Shivaei, Jianwei Lyu, George Rieke, William M. Baker, Nina Bonaventura, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Emma Curtis-Lake, Francesco D'Eugenio, Daniel J. Eisenstein, Anna de Graaff, Kevin N. Hainline, Ryan Hausen, Benjamin D. Johnson, Roberto Maiolino, Eleonora Parlanti, Marcia J. Rieke, Brant E. Robertson, Yang Sun, Sandro Tacchella, Christopher N. A. Willmer, Chris J. Willott
Figure caption: Overdensities of galaxies at 3.25 < z < 3.55 in the JADES NIRCam (black outline) and MIRI parallel (red outline) field of views. Contours increment by 1σ, with the purple contour outlining 4σ peaks. The yellow pluses show low-mass PSBs that are part of the z ∼ 3.4 overdensity.
Paper: Reconstructing the Genealogy of LIGO-Virgo Black Holes
Authors: Parthapratim Mahapatra, Debatri Chattopadhyay, Anuradha Gupta, Fabio Antonini, Marc Favata, B. S. Sathyaprakash, K. G. Arun
Figure caption: A schematic depiction of the possible merger history of GW190521 as inferred by our method. The middle of the figure depicts the binary components of GW190521, indicating the masses (in units of solar masses, M ⊙) as well as the effective dimensionless spin parameters (χ eff, χ  p ) as inferred from the LVK Collaboration analysis. The lower part of the figure shows the analogous parameters (m 1,p, m 2,p, χ eff, p, χ  p,p) for the parents of the primary component of GW190521. Those values are inferred via the method described in Section 2 and are among the main results of this paper. The numbers shown here quote the median parameter values, as well as the upper and lower limits of the 90% credibility interval of the inferred posteriors. We also show the redshift and merger rate (in units of Gpc-3 yr-1) for GW190521, as well as the kick magnitude for the primary (in km s-1).
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: CO(1-0) spectra at two locations (with and without a sink) in Figure 11. The spectral cube is from the RT in Section 3.4. (a): CO(1-0) spectrum within a 10″ beam centered at no sink 1. (b): CO(1-0) spectrum within a 10″ beam centered at sink 31.
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: Time-dependent molecular gas mass comparison between MRCOLA_CNM (left) and MRCOLA_CNM4 (right). The black curve shows the H2 mass, while the blue curve shows the CO-dominated gas mass. The two plots have the same x-range and y-range.
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: Same format as Figure 3 but for model MRCOLA_CNM_noB.
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: Same format as Figure 7 but for model MRCOLA_CNM4 (see Section 4.2).
Paper: Filamentary Molecular Cloud Formation via Collision-induced Magnetic Reconnection in a Cold Neutral Medium
Authors: Shuo Kong (孔朔), Rowan J. Smith, David Whitworth, Erika T. Hamden
Figure caption: CO-dominated gas temperature histogram in K. The CO domination is defined as CO abundance greater than half the initial elemental abundance of carbon.
Paper: Modeling ALMA Observations of the Warped Molecular Gas Disk in the Red Nugget Relic Galaxy NGC 384
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: The M BH−σ ⋆ (left), M BH−L bul (middle), and M BH−M bul (right) relationships (J. Kormendy & L. C. Ho 2013; N. J. McConnell & C.-P. Ma 2013; R. Läsker et al. 2014; R. P. Saglia et al. 2016; G. A. D. Savorgnan et al. 2016; R. C. E. van den Bosch 2016), with shaded regions indicating their intrinsic scatter. The local compact relic galaxies with ALMA-based molecular gas-dynamical M BH determinations (J. H. Cohn et al. 2021, 2023), including NGC 384 (this work), are shown with blue diamonds. Red-filled squares indicate stellar-dynamical M BH measurements from adaptive optics-assisted integral field spectroscopy (J. L. Walsh et al. 2015, 2016, 2017). The relic galaxies are plotted with their total luminosities and masses on the M BH−L bul and M BH−M bul relations, making them upper limits on bulge values. PGC 11179, Mrk 1216, NGC 1271, and NGC 1277 are positive outliers from M BH−L bul and M BH−M bul, but NGC 384 and UGC 2698 are consistent within the intrinsic scatter of all three relations.
Paper: Modeling ALMA Observations of the Warped Molecular Gas Disk in the Red Nugget Relic Galaxy NGC 384
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: Zeroth (top row), first (middle row), and second (bottom row) moment maps of NGC 384 built from the ALMA data (left column) and best-fit fiducial model (middle column) within the fiducial elliptical fitting region. The uncertainty in the first moment map (upper right) and first moment map residual (data−model) normalized by the uncertainty (lower right) are also displayed. The moment maps are constructed on the original ALMA pixel scale of 0.″04 pixel−1 and linearly mapped to their respective scale bars, with each moment’s data and model using the same scale. These maps are not used in the fit, as models are fit directly to the data cube (Section 3). The first moment map shows that the CO disk displays a kinematic twist in the inner ∼0.″5.
Paper: Modeling ALMA Observations of the Warped Molecular Gas Disk in the Red Nugget Relic Galaxy NGC 384
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: Inclination (i; left) and position angle (Γ; right) profiles for the best-fit fiducial warped disk (blue solid line), tilted ring (red dashed line), linear twist (green dashed–dotted line), and flat disk (black dotted line) models, plotted as a function of the input radius r over the extent of the disk. Shaded regions correspond to 1σ confidence intervals. The i(r) for the fiducial warped disk model is consistent with the i(r) profiles of the tilted ring and the linear twist models, while Γ(r) for the fiducial warped disk model shows a significant, well-constrained twist at the center. At radii ≳200 pc (≳0.″75, outside of the central twist), the fiducial warped disk Γ(r) agrees with the flat disk model.
Paper: Poynting Flux of MHD Modes in Magnetic Solar Vortex Tubes
Authors: Samuel J. Skirvin, Viktor Fedun, Marcel Goossens, Suzana S. A. Silva, Gary Verth
Figure caption: The dispersion diagram for a rotating photospheric flux tube with v 0,φ  = 0.1r, indicating the wave solutions obtained with SESAME. Red curves denote the sausage m = 0 mode, blue curves highlight the m = ±1 kink mode, and green curves denote fluting m = ±2 modes. The dashed blue and green curves indicate the flow-modified slow continuum for the m = 1 kink mode and m = 2 fluting mode, respectively. The dashed gray curve indicates the flow-modified Alfvén continuum for the m = −1 kink mode.
Paper: Modeling ALMA Observations of the Warped Molecular Gas Disk in the Red Nugget Relic Galaxy NGC 384
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: Central surface brightness profiles as a function of projected radius along the minor axis. Profiles are shown for the H-band image (black circles), original MGE (blue triangles), and fiducial dust-masked MGE (pink pluses). As shown in Figure 1, the dust is located to the southwest of the nucleus along the minor axis. The impact of the dust is visible as the difference between the surface brightness profiles in this figure at radii of ∼0.″6−1″.
Paper: Modeling ALMA Observations of the Warped Molecular Gas Disk in the Red Nugget Relic Galaxy NGC 384
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: PVDs extracted from the observed data cube (top) and best-fit fiducial model cube (bottom) for NGC 384. The best-fit systemic velocity (see Table 2) has been subtracted from the line-of-sight velocities displayed here. The extraction path for the PVDs is along the disk major axis (PA = 132.°8 east of north, based on the flat disk model in Section 4.2), with a width set by the geometric mean of the synthesized beam (0.″22). Both panels are linearly mapped according to the color bar. As a result of the kinematic twist, the central region of the PVD highlights features of the minor kinematic axis. Our dynamical models are fit directly to the data cube, so these PVDs are not used in the fit.
Paper: Modeling ALMA Observations of the Warped Molecular Gas Disk in the Red Nugget Relic Galaxy NGC 384
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: One-dimensional (1D; top edge) and 2D posteriors of fiducial model parameters for NGC 384. The 2D panels display 1σ, 2σ, and 3σ contours. In the 1D panels, black lines correspond to the posterior median and blue dashed lines to 3σ confidence intervals. Parameter median and 3σ values are also labeled above each 1D panel. The BH mass is M BH                      ﹩=({7.26}_{-0.48}^{+0.43}[1\sigma {]}_{-1.74}^{+1.36}[3\sigma ])\times {10}^{8}\ {M}_{\odot }﹩. Our best-fit fiducial model is built with the posterior medians and produces a reduced ﹩{\chi }_{\nu }^{2}=1.159﹩.
Paper: Modeling ALMA Observations of the Warped Molecular Gas Disk in the Red Nugget Relic Galaxy NGC 384
Authors: Jonathan H. Cohn, Maeve Curliss, Jonelle L. Walsh, Kyle M. Kabasares, Benjamin D. Boizelle, Aaron J. Barth, Karl Gebhardt, Kayhan Gültekin, David A. Buote, Jeremy Darling, Andrew J. Baker, Luis C. Ho
Figure caption: Observed (black) and best-fit fiducial model (blue) line profiles in the fitting ellipse, on the downsampled pixel scale, with noise per channel shown in gray. The BH location is shown with a black star. The x-axis is labeled with the velocity channel ranges for each panel, and the y-axis is labeled with the minimum and maximum flux shown in each panel. The physical extent of the fitting region is also indicated at the corners of the x and y axes. This figure indicates the model is a good fit to the observations across the gas disk.
Paper: Impact of Systematic Modeling Uncertainties on Kilonova Property Estimation
Authors: D. Brethauer, D. Kasen, R. Margutti, R. Chornock
Figure caption: Comparing the fiducial model of M = 10−2 M ⊙, v = 0.1c, ﹩{\mathrm{log}}_{10}({X}_{\mathrm{lan}})﹩ = −2 across the LSST r and y filters, the JWST F115W, F277W, F560W filters, and bolometric luminosity curve with atomic data sets HULLAC, ATOMIC, and Autostructure in orange, blue, and green, respectively, at a distance of 40.7 Mpc. Models using the local thermalization prescription are solid lines, while the global thermalization prescription is represented by the dotted line. The choice of atomic data for light r-process elements (31 ≤ Z ≤ 50) has a dramatic impact on optical emission as seen by the differences between atomic data sets HULLAC and ATOMIC against Autostructure. Differences in lanthanide atomic data result in a ≳3 mag difference at NIR and MIR wavelengths by δ t ∼ 2 weeks that only continues to grow. The global thermalization prescription tends to increase emission across filters by 0.5–1 mag, especially at bluer filters and at early times while the ejecta is optically thick. Notably, we would expect NLTE effects to become important at δ t ∼ 13 days as per Equation (3).
Paper: Binary Disruption and Ejected Stars from Hierarchical Star Cluster Assembly
Authors: Claude Cournoyer-Cloutier, Jeremy Karam, Alison Sills, Simon Portegies Zwart, Maite J. C. Wilhelm
Figure caption: Gas surface density for the merger inherited from the TORCH simulation (left) and for the merger of two isolated Plummer spheres (right). The maximum surface density in the Plummer sphere simulation is about one order of magnitude higher than in the merger from the TORCH simulation.
Paper: Binary Disruption and Ejected Stars from Hierarchical Star Cluster Assembly
Authors: Claude Cournoyer-Cloutier, Jeremy Karam, Alison Sills, Simon Portegies Zwart, Maite J. C. Wilhelm
Figure caption: Projected direction of motion in the x-y plane of all unbound stars in simulations with TORCH initial conditions, at the end of the merger. The length of the arrow is proportional to the projected velocity, and the origin of the arrow corresponds to the location of the star. Runaway stars are color-coded by simulation, while stars with v  r  < 30 km s−1 are shown in light gray.
Paper: Binary Disruption and Ejected Stars from Hierarchical Star Cluster Assembly
Authors: Claude Cournoyer-Cloutier, Jeremy Karam, Alison Sills, Simon Portegies Zwart, Maite J. C. Wilhelm
Figure caption: Mass fraction of unbound stars as a function of time, for all simulations.
Paper: Binary Disruption and Ejected Stars from Hierarchical Star Cluster Assembly
Authors: Claude Cournoyer-Cloutier, Jeremy Karam, Alison Sills, Simon Portegies Zwart, Maite J. C. Wilhelm
Figure caption: Semimajor axes of binary systems disrupted in IB1, PB, and PM during the first 0.41 Myr of the simulation, which corresponds to the time required for the merger to complete in IB1. The three simulations have the same initial population of binaries.
Paper: Binary Disruption and Ejected Stars from Hierarchical Star Cluster Assembly
Authors: Claude Cournoyer-Cloutier, Jeremy Karam, Alison Sills, Simon Portegies Zwart, Maite J. C. Wilhelm
Figure caption: Mollweide projection of the direction of motion of all unbound stars in simulations with TORCH initial conditions, at the end of the merger.
Paper: Binary Disruption and Ejected Stars from Hierarchical Star Cluster Assembly
Authors: Claude Cournoyer-Cloutier, Jeremy Karam, Alison Sills, Simon Portegies Zwart, Maite J. C. Wilhelm
Figure caption: Binary fraction as defined in Equation (3) as a function of time for runs with primordial binaries. In merger runs with TORCH initial conditions, about half of the total decrease in binary fraction takes place during the merger, which ends at 0.41 Myr.
Paper: Binary Disruption and Ejected Stars from Hierarchical Star Cluster Assembly
Authors: Claude Cournoyer-Cloutier, Jeremy Karam, Alison Sills, Simon Portegies Zwart, Maite J. C. Wilhelm
Figure caption: Cumulative number of disrupted systems for IB1, PB, and PM. The three simulations have the same initial population of binaries.
Paper: Quiescent Solar Wind Regions in the Near-Sun Environment: Properties and Radial Evolution
Authors: Benjamin Short, David M. Malaspina, Alexandros Chasapis, Jaye L. Verniero
Figure caption: Proton ﹩{ \mathcal R }﹩ vs. β ∥p  for quiescent and nonquiescent solar wind at different radial distances. Panel (a) is a scatter plot of the proton data that satisfies the SPAN-I requirements in Section 2.3. The y-axes of each subplot are the proton temperature anisotropies, and the x-axes of the subplots are the plasma betas parallel to the background magnetic field. The columns of panel (a) represent distributions for quiescent plots on the left and nonquiescent plots on the right. The rows represent radial bins, with the topmost row being the innermost altitudes that PSP reaches and the lower rows representing higher altitudes. The contours in each plot represent the density of data points at each location in the plot. The color scale is normalized to the number N max, which is the maximum value for each contour in the panel. In panel (b), the peaks of each subplot in panel (a) are tracked through altitudes and plot relative to one another. Solid lines are various instability thresholds past which solar wind would become likely to grow waves. The black line is the ion cyclotron instability, the blue line is the mirror mode instability, and the green line is the parallel firehose instability (P. Hellinger et al. 2006). These peaks are based on 2D histograms of the data, and the error bars are the full width of the distributions at half-maximum. The encounter 13 ICME wake is plotted in purple. This event is discussed in more detail in Section 4.2.
Paper: Quiescent Solar Wind Regions in the Near-Sun Environment: Properties and Radial Evolution
Authors: Benjamin Short, David M. Malaspina, Alexandros Chasapis, Jaye L. Verniero
Figure caption: Normalized histograms of various solar wind properties. The rows of histograms represent radial distances, with the top row being the innermost radial bin with data ranging from 11.4 R ⊙ to 15 R ⊙. The following two rows are in 10 R ⊙ increments, the center row being from 15 to 25 R ⊙ and the bottom row from 25 to 35 R ⊙. The columns are each property at those radial distances. Column (a) is the number of protons cm–3, column (b) is the proton core temperature in eV, column (c) is the bulk velocity magnitude in km s−1, and column (d) is the magnetic field magnitude in nT. Median values are pictured as vertical lines for both quiescent (orange) and nonquiescent (blue) distributions.
Paper: Quiescent Solar Wind Regions in the Near-Sun Environment: Properties and Radial Evolution
Authors: Benjamin Short, David M. Malaspina, Alexandros Chasapis, Jaye L. Verniero
Figure caption: Nonnormalized histograms of δ B/〈∣B∣〉 for each quiescent region across all radial distances. The orange histogram is for quiescent regions, and the blue is for nonquiescent solar wind of the same scale.
Paper: Joint Observations of Late Universe Probes: Cosmological Parameter Constraints from Gravitational Wave and Type Ia Supernova Data
Authors: Jie Zheng, Xiao-Hui Liu, Jing-Zhao Qi
Figure caption: In each panel, the posterior probability density is depicted for the wCDM model within three phenomenological population mass models. The solid lines delineate the 68% and 95% confidence level contours, respectively. The gray lines represent the constraints from GW data, the red lines represent the SNe Ia data, and the blue lines represent the combination of SNe Ia and GW.
Paper: Quiescent Solar Wind Regions in the Near-Sun Environment: Properties and Radial Evolution
Authors: Benjamin Short, David M. Malaspina, Alexandros Chasapis, Jaye L. Verniero
Figure caption: Radial evolution of quiescent region occurrence. The vertical axis represents the percentage of solar wind plasma that has been labeled as quiescent out of the total plasma that PSP has flown through. The percentages presented are ratios of the quiescent meters of plasma flown through over the total meters of plasma flown through at that altitude. The fit exponential falls off with a scale of ∼36.5 R ⊙ indicating a rapid decay of quiescent plasma with solar wind distance.
Paper: Joint Observations of Late Universe Probes: Cosmological Parameter Constraints from Gravitational Wave and Type Ia Supernova Data
Authors: Jie Zheng, Xiao-Hui Liu, Jing-Zhao Qi
Figure caption: In each panel, the posterior probability density is depicted for the ΛCDM model within three phenomenological population mass models. The solid lines delineate the 68% and 95% confidence level contours, respectively. The gray lines represent the constraints from GW data, the red lines represent the SNe Ia data, and the blue lines represent the combination of SNe Ia and GW.
Paper: Joint Observations of Late Universe Probes: Cosmological Parameter Constraints from Gravitational Wave and Type Ia Supernova Data
Authors: Jie Zheng, Xiao-Hui Liu, Jing-Zhao Qi
Figure caption: Posterior distributions for H 0 and Ω m  obtained from the 42 BBH events (dotted lines) and combined with the bright standard siren GW170817 (solid lines).
Paper: JWST Imaging of Edge-on Protoplanetary Disks. III. Drastic Morphological Transformation Across the Mid-infrared in Oph163131
Authors: Marion Villenave, Karl R. Stapelfeldt, Gaspard Duchêne, François Ménard, Marshall D. Perrin, Christophe Pinte, Schuyler G. Wolff, Ryo Tazaki, Deborah L. Padgett
Figure caption: JWST/MIRI images of Oph163131. While the orientation is the same as in Figure 1, the field of view is twice as large. On the leftmost panel, the white contours correspond to 15 and 100 MJy sr−1 levels in the 2.0 μm NIRCam image (same as in Figure 1), and the dark cross shows the location of the brightest pixel at 7.7 μm. The resolution of the observations is shown as white ellipses in the bottom left corner.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. III. Drastic Morphological Transformation Across the Mid-infrared in Oph163131
Authors: Marion Villenave, Karl R. Stapelfeldt, Gaspard Duchêne, François Ménard, Marshall D. Perrin, Christophe Pinte, Schuyler G. Wolff, Ryo Tazaki, Deborah L. Padgett
Figure caption: HST/ACS (0.6, 0.8 μm) and JWST/NIRCam (2.0, 4.44 μm) images of Oph163131, rotated so that the brighter southeast nebula is up. The white ellipse in the bottom left of each panel represents the resolution of the observations. On the third panel, the faint white contours correspond to 15 and 100 MJy sr−1 levels in the 2.0 μm NIRCam image.
Paper: JWST Imaging of Edge-on Protoplanetary Disks. III. Drastic Morphological Transformation Across the Mid-infrared in Oph163131
Authors: Marion Villenave, Karl R. Stapelfeldt, Gaspard Duchêne, François Ménard, Marshall D. Perrin, Christophe Pinte, Schuyler G. Wolff, Ryo Tazaki, Deborah L. Padgett
Figure caption: Overlay MIRI 7.7 μm image, using the same color scale as in Figure 2, and ALMA 1.3 mm dust continuum (green contours, with levels 10σ cont and 20σ cont) and 12CO observations (white contours, with levels 5σ CO and 20σ CO), illustrating that the fluffy emission is located at higher altitude and larger radii than the gas emission. The ALMA data were published in M. Villenave et al. (2022). A 1″ scale is represented by a horizontal line in the bottom left corner of the figure.