adsabs/AstroCLIMB huggingface dataset:
Paper: The Close AGN Reference Survey (CARS): An Interplay between Radio Jets and AGN Radiation in the Radio-quiet AGN HE0040-1105
Authors: M. Singha, N. Winkel, S. Vaddi, M. Perez Torres, M. Gaspari, I. Smirnova-Pinchukova, C. P. O'Dea, F. Combes, Osase Omoruyi, T. Rose, R. McElroy, B. Husemann, T. A. Davis, S. A. Baum, C. Lawlor-Forsyth, J. Neumann, G. R. Tremblay
Figure caption: Flowchart showing the method by which we constrain the location and morphology of the ionized gas cloud C1. Panel (a) shows the flux map retrieved from the two-component model fitted to the original MUSE data cube. In panel (b), we show an example slice of the flux profile at fixed decl., together with the model of the PSF. This slice has been taken from the slice at the decl. with the brightest C1 emission, where the 1D PSF fit follows the 1D flux profile closely. We map the location of the one-dimensional surface profiles in panel (c), which line up to a shell that extends in the north–south direction. The blue line represents the centroids of C1. Panel (d) shows the deconvolved image of C1, where the width of the underlying structure is achieved by fitting with the flux profile at a fixed decl. with the brightest C1 emission with a 1D PSF convolved with a 1D Gaussian. The standard deviation of the Gaussian provides us with the width of the structure (shaded in gray).
Paper: Strong Resemblance between Surface and Deep Zonal Winds inside Jupiter Revealed by High-degree Gravity Moments
Authors: Hao Cao, Jeremy Bloxham, Ryan S. Park, Burkhard Militzer, Rakesh K. Yadav, Laura Kulowski, David J. Stevenson, Scott J. Bolton
Figure caption: Angular velocity of the reconstructed deep zonal winds with a truncation depth of 2500 km (red trace) compared to the observed surface zonal winds (blue trace) as a function of surface planetocentric latitude. Also shown are the uncertainties associated with the reconstruction (dashed lines), computed from the full covariance matrix of the gravity solution. The strong resemblance between the observed surface zonal winds and reconstructed deep zonal winds, in both pattern and amplitude, is visible.
Paper: Strong Resemblance between Surface and Deep Zonal Winds inside Jupiter Revealed by High-degree Gravity Moments
Authors: Hao Cao, Jeremy Bloxham, Ryan S. Park, Burkhard Militzer, Rakesh K. Yadav, Laura Kulowski, David J. Stevenson, Scott J. Bolton
Figure caption: Meridional structure of single mode deep zonal winds and the vertical truncation function. Panel (a) shows an equatorially symmetric (even) mode with l = 20; panel (b) shows an equatorially antisymmetric (odd) mode with l = 21. For both the even and the odd modes, a vertical truncation function (Equation (4)) with H = 2500 km, and ΔH = 75 km has been applied (panel (c)). In addition, an equatorial smoothing function (Equation (5)) with Δz = 0.075 R  J  has been applied to the odd mode (see Figure 4).
Paper: Strong Resemblance between Surface and Deep Zonal Winds inside Jupiter Revealed by High-degree Gravity Moments
Authors: Hao Cao, Jeremy Bloxham, Ryan S. Park, Burkhard Militzer, Rakesh K. Yadav, Laura Kulowski, David J. Stevenson, Scott J. Bolton
Figure caption: Example of an equatorial smoothing function with Δz = 0.075 R  J . An equatorial smoothing function (Equation (5)) is applied to the equatorial antisymmetric (odd) mode to ensure a smooth transition between the nearly z-invariant winds in each hemisphere.
Paper: Strong Resemblance between Surface and Deep Zonal Winds inside Jupiter Revealed by High-degree Gravity Moments
Authors: Hao Cao, Jeremy Bloxham, Ryan S. Park, Burkhard Militzer, Rakesh K. Yadav, Laura Kulowski, David J. Stevenson, Scott J. Bolton
Figure caption: Pattern and amplitude of the reconstructed deep zonal flows at a few different truncation depths. The observed surface zonal winds are also shown for comparison. It can be seen that the pattern of the reconstructed deep zonal flows remains broadly similar, while the amplitude increases rapidly as the truncation depth decreases.
Paper: An Optically Thin View of the Solar Chromosphere from Observations of the O I 1355 Å Spectral Line
Authors: Mats Carlsson, Bart De Pontieu
Figure caption: IRIS spectroheliograms of NOAA AR 12920 on 2015 September 24. The left column shows the O I 1355 Å intensity, while the right column row shows the line-of-sight magnetic field as deduced from HMI magnetograms stitched together to replicate the IRIS raster timings and locations. The red circles indicate locations with neutral lines between opposite polarities and increased O I 1355 Å intensities, as described in the text.
Paper: Little Ado about Everything: ηCDM, a Cosmological Model with Fluctuation-driven Acceleration at Late Times
Authors: Andrea Lapi, Lumen Boco, Marcos M. Cueli, Balakrishna S. Haridasu, Tommaso Ronconi, Carlo Baccigalupi, Luigi Danese
Figure caption: Top panels: snapshots at z ≈ 0 extracted from an N-body simulation in the ΛCDM cosmology with a box of 2 h −1 Gpc and 10243 particles, which shows the amplitude ﹩\mathrm{log}(1+\delta )﹩ of the overdensity field (color-coded) smoothed via a top-hat window function on scales of R ≈ 5 (left), 50 (middle), and 500  (right) h −1 Mpc. Bottom panels: average and dispersion of the lognormal distribution followed by the density contrast field in the simulation when smoothed on different scales R at redshifts z ≈ 0 (red), 0.5 (magenta), 1 (green), and 3 (blue). The red circles highlight the smoothing scales used in the snapshots shown in the top panels.
Paper: Little Ado about Everything: ηCDM, a Cosmological Model with Fluctuation-driven Acceleration at Late Times
Authors: Andrea Lapi, Lumen Boco, Marcos M. Cueli, Balakrishna S. Haridasu, Tommaso Ronconi, Carlo Baccigalupi, Luigi Danese
Figure caption: Average evolution in the ηCDM model. Top panel: Hubble parameter as a function of redshift; the inset zooms in on the late-time evolution. Middle panel: energy density parameters of matter (blue), dark energy (red), radiation (orange), and curvature (green) as a function of redshift. The inset refers to the equation of state for the dominant energy density component at late times. Bottom panel: age of the Universe (cyan) and look-back time (magenta) as a function of redshift. The inset shows the late-time evolution of the deceleration parameter q (green) and jerk parameter j (brown). In all panels, solid lines are from ηCDM with best-fit parameters (h, Ω m,0, ζ, α) from the joint analysis of Section 4, dashed lines are for a flat ΛCDM with the same parameters (h, Ω m,0), and dotted lines are for an open CDM model with the same parameters (h, Ω m,0). In the middle panel, the green shaded area on the ηCDM curvature parameter illustrates the typical 2σ uncertainty on the plotted quantities.
Paper: Little Ado about Everything: ηCDM, a Cosmological Model with Fluctuation-driven Acceleration at Late Times
Authors: Andrea Lapi, Lumen Boco, Marcos M. Cueli, Balakrishna S. Haridasu, Tommaso Ronconi, Carlo Baccigalupi, Luigi Danese
Figure caption: Cosmic evolution and probability distribution of the Hubble (top panels), matter density (middle panel), and radiation density (bottom panel) parameters in the ηCDM model. The left panels illustrate the average evolution (colored solid line), the 1σ–2σ variance of the different quantities as originated by the noise (colored shaded areas), and some examples of the random component depurated by the average (gray lines); the insets zoom in on the late-time evolution, with that for h(z) also reporting data from CCs. The right panels illustrate the corresponding probability distributions (histograms and kernel density estimators as solid lines) at different representative redshifts in the late Universe (see legend); the dotted vertical line shows the present value (see Section 4).
Paper: ALMA Millimeter/Submillimeter Sources among Spitzer SMUVS Galaxies at z > 2 in the COSMOS Field
Authors: Tomoko L. Suzuki, Sophie E. van Mierlo, Karina I. Caputi
Figure caption: Comparison of the physical quantities between the ALMA-detected and nondetected SMUVS sources at z = 2.0–3.0 (left) and z = 3.0–5.5 (right). Here, the nondetected SMUVS sources are weighted according to their stellar masses, as done in Figure 4. The ALMA-detected sources tend to be dustier and more active in star formation than the nondetected sources.
Paper: Little Ado about Everything: ηCDM, a Cosmological Model with Fluctuation-driven Acceleration at Late Times
Authors: Andrea Lapi, Lumen Boco, Marcos M. Cueli, Balakrishna S. Haridasu, Tommaso Ronconi, Carlo Baccigalupi, Luigi Danese
Figure caption: MCMC posterior distributions in the ηCDM model for the normalized Hubble constant h 0, the matter density parameter Ω m,0, and the parameters regulating the noise strength ζ and time dependence α. Colored contours/lines refer to different observables: blue for SN+Cepheid, orange for CC+transverse BAO⊥, green for BAO+CMB first peak angular position, and black for joint analysis. The contours show 1σ–2σ–3σ confidence intervals, white crosses mark the maximum-likelihood estimates of the joint analysis, and the marginalized distributions of the joint analysis are reported in the diagonal panels in arbitrary units (normalized to 1 at their maximum value).
Paper: ALMA Millimeter/Submillimeter Sources among Spitzer SMUVS Galaxies at z > 2 in the COSMOS Field
Authors: Tomoko L. Suzuki, Sophie E. van Mierlo, Karina I. Caputi
Figure caption: Stellar mass vs. SFR diagram of the SMUVS sources at z = 2.0–3.0 (left) and z = 3.0–5.5 (right). The stacking results with detection greater than 3σ  (Section 3.1) are also shown. The solid line in each panel represents the star-forming main sequence at z = 2–3 (left) and at z = 3–4 (right) from Santini et al. (2017). The dotted line shows the lower envelope of starburst galaxies defined by Caputi et al. (2021). The ALMA-detected SMUVS sources are located on and above the star-forming main sequence at the epoch.
Paper: Little Ado about Everything: ηCDM, a Cosmological Model with Fluctuation-driven Acceleration at Late Times
Authors: Andrea Lapi, Lumen Boco, Marcos M. Cueli, Balakrishna S. Haridasu, Tommaso Ronconi, Carlo Baccigalupi, Luigi Danese
Figure caption: Fits to SN+Cepheid (top panel), CC+BAO⊥ (middle panel), and BAO+CMB θ ⋆ (bottom panel) in the ηCDM model. In each panel, solid lines and shaded areas illustrate the median and 2σ credible interval from sampling the posterior distribution of the joint analysis, while the dashed line is the median from the posterior distribution of the analysis to the individual data set. Data and references for each observable are described in Section 4.
Paper: ALMA Millimeter/Submillimeter Sources among Spitzer SMUVS Galaxies at z > 2 in the COSMOS Field
Authors: Tomoko L. Suzuki, Sophie E. van Mierlo, Karina I. Caputi
Figure caption: Comparison of E(B − V) (left) and M FUV (right) between the ALMA-detected and nondetected galaxies after dividing the samples into two groups, namely main-sequence galaxies (top) and starburst galaxies (bottom). The nondetected sources are weighted according to their stellar masses. The passive galaxies among the nondetected SMUVS sources are excluded based on the criteria in Deshmukh et al. (2018).
Paper: ALMA Millimeter/Submillimeter Sources among Spitzer SMUVS Galaxies at z > 2 in the COSMOS Field
Authors: Tomoko L. Suzuki, Sophie E. van Mierlo, Karina I. Caputi
Figure caption: Continuum flux (upper limit) at ∼1.2 mm (top) and ∼870 μm (bottom) as a function of stellar mass of the SMUVS sources in the two redshift bins, namely z = 2.0–3.0 (left) and z = 3.0–5.5 (right), analyzed in this study. As for the nondetected SMUVS sources, we show 4.2σ upper limits after correcting for the primary beam attenuation (Liu et al. 2019). The nondetected SMUVS sources have reasonable upper limits on their continuum fluxes as compared to the individually detected SMUVS sources. The results of the stacking analysis for the nondetected sources are also shown with star symbols and arrows (Section 3.1).
Paper: ALMA Millimeter/Submillimeter Sources among Spitzer SMUVS Galaxies at z > 2 in the COSMOS Field
Authors: Tomoko L. Suzuki, Sophie E. van Mierlo, Karina I. Caputi
Figure caption: Comparison of Ks-band magnitude, 4.5 μm magnitude, and Ks–[4.5] color between the ALMA-detected and nondetected SMUVS sources at z = 2.0–5.5. The histograms of the nondetected SMUVS sources are weighted according to the stellar masses so that the stellar-mass distribution becomes the same between the ALMA-detected and nondetected sources. The ALMA-detected sources at z ≥ 2 tend to be brighter at 4.5 μm and have systematically redder Ks–[4.5] colors than the nondetected sources, even when considering the difference of the stellar-mass distributions.
Paper: ALMA Millimeter/Submillimeter Sources among Spitzer SMUVS Galaxies at z > 2 in the COSMOS Field
Authors: Tomoko L. Suzuki, Sophie E. van Mierlo, Karina I. Caputi
Figure caption: Stellar mass of the ALMA-detected and nondetected SMUVS sources analyzed in this study as a function of redshift. The stellar masses and redshifts of both the ALMA-detected and nondetected sources are from the best-fit SEDs obtained from LEPHARE with the 28 band photometry from u band to 4.5 μm (van Mierlo et al. 2022). ALMA-detected sources are at the high-mass end of the mass distribution of the nondetected SMUVS sources, whereas there is no clear difference between the redshift distributions of the two samples.
Paper: ALMA Millimeter/Submillimeter Sources among Spitzer SMUVS Galaxies at z > 2 in the COSMOS Field
Authors: Tomoko L. Suzuki, Sophie E. van Mierlo, Karina I. Caputi
Figure caption: Comparison of the stellar masses obtained from LEPHARE and MAGPHYS for the ALMA-detected SMUVS sources at z = 2.0–5.5. The solid line represents the identity line. The dashed line represents the case when the stellar mass from MAGPHYS is 0.25 dex larger than that from LEPHARE. The stellar masses from MAGPHYS are systematically larger than those from LEPHARE.
Paper: Mode Changing in PSR B0844-35 and PSR B1758-29 with Enhanced Emission at the Profile Centers
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: Longitude resolved fluctuation spectra (LRFS) to estimate the drifting behavior in the two modes of PSR B0844-35. The left panel shows the LRFS for a pulse sequence of 180 periods in mode A and the right panel shows the LRFS of mode B for 102 pulses. A peak frequency due to subpulse drifting with periodicity ∼2P is seen during mode A, while mode B does not show any clear periodic behavior.
Paper: Mode Changing in PSR B0844-35 and PSR B1758-29 with Enhanced Emission at the Profile Centers
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: The left panel shows the single pulse sequence corresponding to mode A of PSR B0844-35, observed on 2018 January 27, and represents the pulse range between 625 and 725 from the start of the observing session averaged over the 300–500 MHz frequency band. The right panel shows the 300–500 MHz frequency averaged pulse sequence also observed on 2018 January 27, between pulses 280 and 360, belonging to mode B.
Paper: Mode Changing in PSR B0844-35 and PSR B1758-29 with Enhanced Emission at the Profile Centers
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: The average profiles of PSR B0844-35 during mode A (left panel) and mode B (right panel). The profiles at two separated frequencies are shown in each panel to highlight the frequency evolution of the modes.
Paper: Mode Changing in PSR B0844-35 and PSR B1758-29 with Enhanced Emission at the Profile Centers
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: The average profile from selected pulses where there is flaring in the core emission.
Paper: Strong Resemblance between Surface and Deep Zonal Winds inside Jupiter Revealed by High-degree Gravity Moments
Authors: Hao Cao, Jeremy Bloxham, Ryan S. Park, Burkhard Militzer, Rakesh K. Yadav, Laura Kulowski, David J. Stevenson, Scott J. Bolton
Figure caption: The zonal harmonics of the latest gravity solution for Jupiter (black circles), the derived uncertainties (dashed lines; Kaspi et al. 2023), the solid-body rotation contribution (red circles) according to one of the latest interior models of Jupiter (Militzer et al. 2022), and the differences between the two (blue circles). For the J  n s, filled (open) circles represent positive (negative) values. Twice the derived uncertainties are about 3 times the formal uncertainty.
Paper: Strong Resemblance between Surface and Deep Zonal Winds inside Jupiter Revealed by High-degree Gravity Moments
Authors: Hao Cao, Jeremy Bloxham, Ryan S. Park, Burkhard Militzer, Rakesh K. Yadav, Laura Kulowski, David J. Stevenson, Scott J. Bolton
Figure caption: Angular velocity of Jupiter’s surface zonal winds in real space (Tollefson et al. 2017) as a function of planetocentric latitude (a) and in spherical harmonic space (b). Here we show the ratio of the zonal winds angular velocity in the System III rotating frame, ω, and the angular velocity of the background rotation Ω0. In panel (b), filled circles represent positive values while open circles represent negative values. It can be seen that the peak zonal wind speed is ∼1% of the background rotation and the dominant latitudinal length scale in the surface zonal wind corresponds to spherical harmonic degree ∼24.
Paper: Little Ado about Everything: ηCDM, a Cosmological Model with Fluctuation-driven Acceleration at Late Times
Authors: Andrea Lapi, Lumen Boco, Marcos M. Cueli, Balakrishna S. Haridasu, Tommaso Ronconi, Carlo Baccigalupi, Luigi Danese
Figure caption: Schematics that illustrate the mathematical meaning of a stochastic differential equation ﹩\dot{x}=f(x)+g(x)\eta (t)﹩. Each realization of the noise η(t) yields a different random walk (e.g., with reference to the main text, the walkers in red, blue, and green correspond to the evolution of the density in three regions at different spatial locations). At a given time t = T, sampling the value of the variable x from the ensemble of walkers (e.g., from the different patches in the Universe) would yield a nontrivial probability distribution P(x, T) of the variable x, which is the solution to the stochastic differential equation. The average ﹩\bar{x}﹩ of this distribution will evolve in time as prescribed by Equation (A5).
Paper: Little Ado about Everything: ηCDM, a Cosmological Model with Fluctuation-driven Acceleration at Late Times
Authors: Andrea Lapi, Lumen Boco, Marcos M. Cueli, Balakrishna S. Haridasu, Tommaso Ronconi, Carlo Baccigalupi, Luigi Danese
Figure caption: MCMC posterior distributions in the (curvature-free) ΛCDM model for the normalized Hubble constant h 0, matter density parameter Ω m,0, and dark energy density parameter ΩΛ,0. Colored contours/lines refer to different observables: blue for SN+Cepheid, orange for CC+transverse BAOs, green for isotropic BAO+CMB first peak angular position, and black for joint. The contours show 1σ–2σ–3σ confidence intervals, crosses mark the maximum-likelihood estimates of the joint analysis, and the marginalized distributions of the joint analysis are reported on the diagonal panels in arbitrary units (normalized to 1 at their maximum value).
Paper: Mode Changing in PSR B0844-35 and PSR B1758-29 with Enhanced Emission at the Profile Centers
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: The PPA distribution of the single pulse time samples of PSR B0844-35. The top windows (a) and (b) show the behavior of mode A and B, respectively, at the 300–500 MHz frequency range. The bottom windows (c) and (d) show the PPA of the two modes averaged between 550 and 750 MHz. The top panel in each window shows the average profile (black) and the average linear (red) and circular polarization (blue) properties of the radio emission. In the bottom window, the distribution of the single pulse PPA is shown as a color scale, representing the number of points in each location, as well as the average PPA behavior across the window (red error bars). The RVM fit to the PPA is also shown in the figure (pink dashed line), along with the steepest gradient point of the RVM fit (black error bar).
Paper: Mode Changing in PSR B0844-35 and PSR B1758-29 with Enhanced Emission at the Profile Centers
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: The left panel shows the single pulse sequence corresponding to the B mode of PSR B1758-29, observed on 2019 March 18, and represents the pulse range between 260 and 460 from the start of the observing session. The right panel shows the pulse sequence between pulses 870 and 1070, belonging to the Q mode.
Paper: Mode Changing in PSR B0844-35 and PSR B1758-29 with Enhanced Emission at the Profile Centers
Authors: Rahul Basu, Dipanjan Mitra, George I. Melikidze
Figure caption: The LRFS across the single pulse sequences of PSR B1758-29 during the observations on 2019 March 18, showing the different periodic behavior. (a) The pulse sequence between 1700 and 1850 in mode B showing the low-frequency periodic modulation seen in this mode. The phase variations corresponding to the periodic modulation feature (top window) are flat with close to zero slope across the profile. This highlights that the emission across the entire window changes simultaneously during periodic modulations. (b) The average LRFS estimated in mode Q showing the subpulse drifting behavior with P 3 = 2.4P. (c) The pulse between 15 and 185, in mode Q, showing the presence of both subpulse drifting as well as periodic modulation. The phase behavior corresponding to subpulse drifting in this pulsar is also flat but limited primarily to the leading component.
Paper: Cosmological Tensions and the Transitional Planck Mass Model
Authors: Joshua A. Kable, Giampaolo Benevento, Graeme E. Addison, Charles L. Bennett
Figure caption: Posterior parameter distributions showing the effect of including or excluding the H 0 prior from local measurements. The TPM fit to SPT+Base (green) does not prefer the same shift in the Planck mass as the case where the H 0 prior is included (gray); however, the posterior distribution has a non-Gaussian tail that allows for larger amplitude transitions. When Planck TT650TEEE is included, the allowed parameter space for Ω0 is restricted for both the case where the H 0 prior is included (blue) or excluded (red). Without the H 0 prior, the c 0 shifts upward (less negative). This corroborates the assertion that the shift in c 0 for the TPM fit to SPT+Planck TT650TEEE+Base+H  0  is driven by the prior on H 0 and the limitation of the Ω0 parameter to increase H 0 when the SPT and Planck data are combined. We cut the parameter values for Ω0 > 0.0035 for visualization purposes.
Paper: Cosmological Tensions and the Transitional Planck Mass Model
Authors: Joshua A. Kable, Giampaolo Benevento, Graeme E. Addison, Charles L. Bennett
Figure caption: Posterior distribution functions for the TPM and TPM f(R) model fits to SPT+Base+H  0  and SPT+Planck TT650TEEE+Base+H  0 . The TPM f(R) model is the subset of the TPM model where c 0 is fixed to 0, which isolates the phenomenology of the transition of the Planck mass. The c 0 parameter acts as a equation of state parameter for the scalar field in the late Universe. For the fits to SPT+Base+H  0 , there is little difference between the TPM (green) and TPM f(R) (gray) models because the data allow for large shifts in the Planck mass. When the Planck TT650TEEE data are added, this model freedom is removed and the full TPM model (red) shifts c 0 to be more negative to increase H 0. The TPM f(R) model (blue) can still achieve higher H 0 values, but the fit to the data is worse. We cut the parameter values for Ω0 > 0.0035 for visualization purposes.