adsabs/AstroCLIMB huggingface dataset:
Paper: Simulated Bars May Be Shorter but Are Not Slower Than Those Observed: TNG50 versus MaNGA
Authors: Neige Frankel, Annalisa Pillepich, Hans-Walter Rix, Vicente Rodriguez-Gomez, Jason Sanders, Jo Bovy, Juna Kollmeier, Norm Murray, Ted Mackereth
Figure caption: Matching the stellar mass–size plane for the simulated galaxies from TNG50 (left) and the observed galaxies from MaNGA (middle). The gray dots represent all disk galaxies (at face value), and the black crosses are the barred galaxies in TNG50 (left). The G19 sample targeted by MaNGA and identified as barred via visual inspection by Guo et al. (2019) is also represented by gray dots and black crosses, respectively (middle). Here, total mass means “all bound stars” in TNG0 and “total stellar mass estimate” from Pace et al. (2019) for MaNGA. The third panel shows contours of the distributions of barred galaxies matched between MaNGA and TNG50 in the plane of stellar mass inside IFU and effective radius, quantities that are used to match the galaxy samples. The TNG50 galaxies that are analogs of the MaNGA ones and are used to construct the TNG50 match sample are indicated as green crosses in the left panel.
Paper: Simulated Bars May Be Shorter but Are Not Slower Than Those Observed: TNG50 versus MaNGA
Authors: Neige Frankel, Annalisa Pillepich, Hans-Walter Rix, Vicente Rodriguez-Gomez, Jason Sanders, Jo Bovy, Juna Kollmeier, Norm Murray, Ted Mackereth
Figure caption: Illustrating the determination of the bar length for an example TNG50 galaxy at z = 0. Top left: surface density map of the galaxy (representing the real stellar mass distribution). Top right: face-on image of the galaxy constructed with SKIRT (Baes et al. 2011; Camps & Baes 2015; Rodriguez-Gomez et al. 2019) with an SDSS r-band PSF of FWHM = 1.″3. The horizontal dashed lines show the bar extent derived from the mass (black) and the PSF-convolved mock image (orange). Bottom: radial profile of the normalized Fourier component (A 2/A 0) for the mass distribution (dashed black) and the mock image with PSF convolution (orange). The vertical lines represent the bar length as measured from the mass and PSF-convolved light profiles respectively.
Paper: Simulated Bars May Be Shorter but Are Not Slower Than Those Observed: TNG50 versus MaNGA
Authors: Neige Frankel, Annalisa Pillepich, Hans-Walter Rix, Vicente Rodriguez-Gomez, Jason Sanders, Jo Bovy, Juna Kollmeier, Norm Murray, Ted Mackereth
Figure caption: Same as Figure 5, with the analysis (including the matching to MaNGA) repeated with a lower-resolution version of the TNG50 simulation: TNG50-2. The pattern speed in the lower-resolution simulation is lower than that in the high-resolution run by a factor ∼2 and compares poorly with the observed pattern speeds, with no high pattern-speed values. The bar sizes in the lower-resolution run match those observed well. This combination of lower pattern speed and comparable bar size leads to large ﹩{ \mathcal R }﹩ values in the simulation, as seen in previous-generation cosmological simulations.
Paper: Simulated Bars May Be Shorter but Are Not Slower Than Those Observed: TNG50 versus MaNGA
Authors: Neige Frankel, Annalisa Pillepich, Hans-Walter Rix, Vicente Rodriguez-Gomez, Jason Sanders, Jo Bovy, Juna Kollmeier, Norm Murray, Ted Mackereth
Figure caption: SDSS r-band image stamps of the TNG50 simulated galaxies that are matched to MaNGA observed galaxies and are used in this analysis. They are seen face on and are annotated by their subhalo IDs and their log stellar mass per M ⊙. In the top left panel, a white horizontal segment gives the scale of 1 kpc.
Paper: Simulated Bars May Be Shorter but Are Not Slower Than Those Observed: TNG50 versus MaNGA
Authors: Neige Frankel, Annalisa Pillepich, Hans-Walter Rix, Vicente Rodriguez-Gomez, Jason Sanders, Jo Bovy, Juna Kollmeier, Norm Murray, Ted Mackereth
Figure caption: Figure 3 continued.
Paper: Inconspicuous Solar Polar Coronal X-Ray Jets as the Source of Conspicuous Hinode/EUV Imaging Spectrometer Doppler Outflows
Authors: Alphonse C. Sterling, Conrad Schwanitz, Louise K. Harra, Nour E. Raouafi, Navdeep K. Panesar, Ronald L. Moore
Figure caption: Magnetic field evolution at the base of event 5. Panel (a) shows positive (red) and negative (green) contours from a Helioseismic and Magnetic Imager (HMI) line-of-sight magnetogram at 17:55:56 UT on 2020 March 2, as contours with levels set at 30 and 50 G. This is overlaid onto a grayscale version of an 304 Å image within seconds of that in Figure 6(e) (the field of view here is more zoomed in than shown in Figure 6(e)), just as the minifilament is erupting. That erupting minifilament plausibly formed and was ejected from the neutral line of the two closest opposite-polarity strong-flux patches. Panels (b)–(d) show the line-of-sight HMI magnetograms of the location evolving over time, with positive and negative polarities represented by white and black, respectively (contours in (a) are within a minute of (d)). These panels show that the two opposite-polarity patches that may have caused the minifilament eruption converged toward each other in the hours prior to that eruption. Such flux convergence (and cancellation) is commonly observed to occur leading up to minifilament eruptions that produce typical coronal jets. The FOV here is slightly smaller than that of the AIA images in Figure 6, in order to center the bipolar flux patches better.
Paper: Study of Complex Absorption and Reflection in a Unique Intermediate Polar Paloma
Authors: Anirban Dutta, Vikram Rana
Figure caption: Folded light curve, based on period 9384 s, from different energy bands, using PN (left) and FPMA (right). The bin size is 188 s. In the bottom panels, HR1 (left) and HR2 (right) are shown. A constant model is fitted to HR2, represented by a black line.
Paper: Study of Complex Absorption and Reflection in a Unique Intermediate Polar Paloma
Authors: Anirban Dutta, Vikram Rana
Figure caption: Power spectra obtained from NuSTAR-FPMA using the Lomb–Scargle algorithm (top) and CLEAN algorithm (bottom). We have identified the two fundamental peaks, Ω and ω, along with the location of a few sidebands and harmonics.
Paper: Study of Complex Absorption and Reflection in a Unique Intermediate Polar Paloma
Authors: Anirban Dutta, Vikram Rana
Figure caption: Power spectra obtained from XMM-Newton PN using the Lomb–Scargle algorithm (top figure) and CLEAN algorithm (bottom figure). The Ω peak is identified, along with the expected (from FPMA power spectra) position of ω. Few sideband frequencies and harmonics are labeled.
Paper: Study of Complex Absorption and Reflection in a Unique Intermediate Polar Paloma
Authors: Anirban Dutta, Vikram Rana
Figure caption: The top and middle panels show the plots of the best-fit model and ratio (data/model) for the broadband spectra using model variant M1. We In the bottom panel we show the ratio plot using the “reflect” version of model M1, i.e., M1-R.
Paper: Study of Complex Absorption and Reflection in a Unique Intermediate Polar Paloma
Authors: Anirban Dutta, Vikram Rana
Figure caption: Fitting the O VII Kα line in RGS spectra. The spectral quality is poor, but the O VII line appears with significant strength and fitted with a Gaussian over an absorbed bremsstrahlung continuum. The spectra and data-to-model ratio are shown in the top and bottom panels, respectively. Expected locations of O VIII and N VII Kα lines are marked.
Paper: Study of Complex Absorption and Reflection in a Unique Intermediate Polar Paloma
Authors: Anirban Dutta, Vikram Rana
Figure caption: Effect of complex absorber and Compton reflection in the spectral modeling. Spectral parameters from model M1-R have been used. The blue curve represents the model spectrum including both reflection and absorption. For the black curve, the absorption is set to zero, but reflection is present. The red curve denotes the spectra when absorption is present but reflection is not.
Paper: Study of Complex Absorption and Reflection in a Unique Intermediate Polar Paloma
Authors: Anirban Dutta, Vikram Rana
Figure caption: Fe Kα lines are fitted with three Gaussian components over an absorbed bremsstrahlung continuum using EPIC data in the 5–8 keV range. We show the spectra and data-to-model ratio in the top and bottom panels, respectively.
Paper: Study of Complex Absorption and Reflection in a Unique Intermediate Polar Paloma
Authors: Anirban Dutta, Vikram Rana
Figure caption: Background-subtracted light curves from XMM-Newton (top) and NuSTAR (middle) and overlapping 3–10 keV light curves from both the observatories for comparison (bottom).
Paper: Stellar Obliquity from Spot Transit Mapping of Kepler-210
Authors: Adriana Valio, Alexandre Araújo
Figure caption: Distribution of all the spots on the stellar surface occulted by planets Kepler-210 b (blue circle) and Kepler-210 c (red circle). Left: the orbits of both planets are assumed to be parallel to the stellar equator; the orbit of Kepler-210 b is shown in blue, whereas that of Kepler-210 c is in red. The dashed line is the 40° meridian, that of maximum observed longitude of occulted spots by Kepler-210 c. Right: now the orbit of Kepler-210 is assumed to be inclined with respect to the stellar equator. The dashed horizontal lines correspond to a maximum latitude of spots of 40°. The sizes of the spots and of the planets are to scale.
Paper: Stellar Obliquity from Spot Transit Mapping of Kepler-210
Authors: Adriana Valio, Alexandre Araújo
Figure caption: Geometry considered in the estimate of the obliquity, λ. The outer solid circle represents the stellar disk, whereas the inner dotted circle has a radius equal to the impact parameter, z, of the orbit of Kepler-210 c (red line). ρ 0 is the distance of the center of the transit to the equator of the star (horizontal dotted line). Point B is the intersection of the transit and the maximum spot latitude, α  m , and A is where the transit intersects the stellar limb.
Paper: Stellar Obliquity from Spot Transit Mapping of Kepler-210
Authors: Adriana Valio, Alexandre Araújo
Figure caption: Light-curve transits of Kepler-210 b (left) and Kepler-210 c (right). The raw SAP_FLUX data are shown as black dots for all the valid transits. The Lee filtered data are shown as orange dots. The average of all smoothed (orange) points is shown as gray circles, whereas the blue curve is the fit to this average transit.
Paper: Stellar Obliquity from Spot Transit Mapping of Kepler-210
Authors: Adriana Valio, Alexandre Araújo
Figure caption: Maps of spot longitude in time for Kepler-210 as seen from an observer on Earth. The top and bottom panels correspond to the spots detected on the transits of Kepler-210 b and Kepler-201 c exoplanets, respectively. The vertical dashed line at 38° highlights that there is a maximum longitude for spots occulted by Kepler-210 c.
Paper: Stellar Obliquity from Spot Transit Mapping of Kepler-210
Authors: Adriana Valio, Alexandre Araújo
Figure caption: Histograms of spot parameters. Top left: radius (in units of 103km). Top right: longitude (degrees). Bottom left: intensity (with respect to surrounding intensity, I  c ). Bottom right: temperature (kelvins). Spot parameters obtained from the transits of Kepler-210 b are shown in magenta, whereas those from Kepler-210 c are shown in orange.
Paper: Stellar Obliquity from Spot Transit Mapping of Kepler-210
Authors: Adriana Valio, Alexandre Araújo
Figure caption: The estimated obliquity of Kepler-210 c’s orbit, considering that the spots are restricted to a maximum latitude, similar to sunspots. The dashed horizontal line represents the obliquity of 34.°8 estimated from the dip in the spots’ longitude at −37° (see Figure 11), which intercepts the pink curve at a maximum latitude value of the spots of 39.°9 (vertical dashed line).
Paper: Stellar Obliquity from Spot Transit Mapping of Kepler-210
Authors: Adriana Valio, Alexandre Araújo
Figure caption: Mean of all 121 transits of Kepler-210 c shown as gray circles. The best fit to this average transit is shown by the pink line. As can be seen, this model does not fit well the mean average transit due to its intrinsic asymmetry. The blue curve represents the model of transits without spots and is adopted as the best one.
Paper: Stellar Obliquity from Spot Transit Mapping of Kepler-210
Authors: Adriana Valio, Alexandre Araújo
Figure caption: Top: light curve of a single transit (194) of planet Kepler-210 b. The yellow curve represents a spotless star model, whereas the red curve is the fit of the planetary transit in front of a star with two spots. Bottom: the residuals after spotless star model subtraction, with the fit of a star with two spots shown in red, also after subtracting the spotless model.
Paper: Stellar Obliquity from Spot Transit Mapping of Kepler-210
Authors: Adriana Valio, Alexandre Araújo
Figure caption: Top: light curve of a single transit (7) of planet Kepler-210 c. The yellow curve represents a spotless star model, whereas the red curve is the fit of the planetary transit in front of a star with two spots. Bottom: the residuals after spotless star model subtraction, with the fit of a star with two spots shown in red, also after subtracting the spotless model.
Paper: A Direct Measurement of Galaxy Major and Minor Merger Rates and Stellar Mass Accretion Histories at Z < 3 Using Galaxy Pairs in the REFINE Survey
Authors: Christopher J. Conselice, Carl J. Mundy, Leonardo Ferreira, Kenneth Duncan
Figure caption: Plots showing the constant number density analysis of the merger history for galaxies selected at n = 1 × 10−4Mpc−3 down to a stellar mass ratio of 1:10. Shown in the three panels are the measured pair fraction, f pair (upper left), galaxy merger rate per galaxy, ﹩{ \mathcal R }(z)﹩ (upper right), and the derived volume-averaged merger rate, Γ(z) (bottom). Measurements are made in the UDS (red circles), UltraVISTA (green triangles), VIDEO (blue squares), and GAMA (gold crosses) survey fields. A power law (black solid line) is fit to the total merger history at this selection. The dashed line is for the major mergers at the same n = 1 × 10−4Mpc−3 selection, and the dotted–dashed blue lines are for the corresponding minor mergers. The red dotted line is the corresponding massive galaxy selection for systems with M * > 1011 M ⊙.
Paper: A Direct Measurement of Galaxy Major and Minor Merger Rates and Stellar Mass Accretion Histories at Z < 3 Using Galaxy Pairs in the REFINE Survey
Authors: Christopher J. Conselice, Carl J. Mundy, Leonardo Ferreira, Kenneth Duncan
Figure caption: The evolution of the stellar mass accretion rate due to major and minor mergers for M * > 1011 M ⊙ selected galaxies. The left-hand side shows the results for the major merger accretion rate due to mergers with mass ratios μ > 0.25, while the right side panel shows this relation for the minor mergers with 0.1 < μ < 0.25. The solid line shows the major merger fit on both plots, and the dashed line is for the minor mergers. The blue line is the prediction for the accretion rate for mass within systems selected at this mass range from the Illustris simulation (see text).
Paper: A Direct Measurement of Galaxy Major and Minor Merger Rates and Stellar Mass Accretion Histories at Z < 3 Using Galaxy Pairs in the REFINE Survey
Authors: Christopher J. Conselice, Carl J. Mundy, Leonardo Ferreira, Kenneth Duncan
Figure caption: Derived total galaxy merger rates, ﹩{ \mathcal R }{(z)}_{\mathrm{tot}}﹩, for galaxies at (M/M ⊙) > 1011 down to stellar mass ratios of 1:10. Estimates are calculated from measured pair fractions in the UDS (red circles), UltraVISTA (green triangles), VIDEO (blue squares), and GAMA (gold crosses) survey fields. The two orange points at higher redshifts are derived from the merger fractions for minor mergers from Bluck et al. (2012), as in Figure 2. A power-law function (black solid line) is fit to the data points. The short-dashed line shows the corresponding merger rate for major mergers at the same redshift range. The minor mergers best line fit is shown by the dotted–dashed cyan line. Also shown are simulated predictions for the total galaxy merger rate mimicking our selection, as taken from the Illustris simulation.
Paper: A Direct Measurement of Galaxy Major and Minor Merger Rates and Stellar Mass Accretion Histories at Z < 3 Using Galaxy Pairs in the REFINE Survey
Authors: Christopher J. Conselice, Carl J. Mundy, Leonardo Ferreira, Kenneth Duncan
Figure caption: The evolution of the stellar mass accretion rate due to major and minor mergers for a constant number density selection at n >10−4 Mpc−3. The left-hand side shows the data for the major merger accretion rate with mergers with mass ratios μ > 0.25, while the right side panel shows this relation for the minor mergers with 0.1 < μ < 0.25. The solid black line shows the major merger fit, and the dashed line is for the minor mergers. The blue line shows the prediction for the accretion rate for stellar mass within systems selected at this number density limit from the Illustris simulation (see text).
Paper: A Direct Measurement of Galaxy Major and Minor Merger Rates and Stellar Mass Accretion Histories at Z < 3 Using Galaxy Pairs in the REFINE Survey
Authors: Christopher J. Conselice, Carl J. Mundy, Leonardo Ferreira, Kenneth Duncan
Figure caption: Derived volume-averaged merger rate, Γ(z) per galaxy, for galaxies at (M/M ⊙) > 1011 down to a stellar mass ratio of 1:10. Estimates are calculated from measured pair fractions in the UDS (red circles), UltraVISTA (green triangles), VIDEO (blue squares), and GAMA (gold crosses) survey fields, as in Figure 2. The orange points at higher redshifts are derived from the measurements from Bluck et al. (2012). A power-law + exponential function (black solid line) is fit to the data points for the overall merger rate per galaxy, while the dashed line shows the major merger rate per galaxy. The best fit for the minor mergers’ merger rate density is shown by the dotted–dashed cyan line.
Paper: Multimessenger Picture of J1048+7143 
Authors: Emma Kun, Ilja Jaroschewski, Armin Ghorbanietemad, Sándor Frey, Julia Becker Tjus, Silke Britzen, Krisztina Éva Gabányi, Vladimir Kiselev, Leander Schlegel, Marcel Schroller, Patrick Reichherzer, Lang Cui, Xin Wang, Yuling Shen
Figure caption: The Fermi-LAT photon flux (168 MeV < E < 800 GeV) of 4FGL J1048.4+7143 as a function of time (black points with error bars).
Paper: A Direct Measurement of Galaxy Major and Minor Merger Rates and Stellar Mass Accretion Histories at Z < 3 Using Galaxy Pairs in the REFINE Survey
Authors: Christopher J. Conselice, Carl J. Mundy, Leonardo Ferreira, Kenneth Duncan
Figure caption: Timescale dependence on redshift and merger mass ratio, μ, based on the best-fit parameters a and b of Equation (27) found by estimating the merging timescale of objects in TNG300-1 with mass ratio μ > 0.1 and with stellar masses M * > 109 M ⊙.
Paper: A Direct Measurement of Galaxy Major and Minor Merger Rates and Stellar Mass Accretion Histories at Z < 3 Using Galaxy Pairs in the REFINE Survey
Authors: Christopher J. Conselice, Carl J. Mundy, Leonardo Ferreira, Kenneth Duncan
Figure caption: The relation between the fits for the equation for the merger time as a function of the mass ratio μ given in Equation (28). The values of a and b are used in Equation (27), where a shows an inverse dependence on μ, while b is found to be independent of μ. Error bars show ±1σ from the mean values.
Paper: Formation and Reconnection of Electron Scale Current Layers in the Turbulent Outflows of a Primary Reconnection Site
Authors: Giovanni Lapenta, Martin Goldman, David L. Newman, Stefan Eriksson
Figure caption: Virtual probe sweeping through the domain along x at y = 8.27 and z = 3.1. From top to bottom reported are: magnetic field B/B 0, electric field e  E /m  i  c ω  pi , parallel electric field eE ∣∣/m  i  c ω  pi , electron speed  V   e , ion speed  V   i , agyrotropy, electron and ion density (n/4π n 0), and dissipation  J  ·  E . To facilitate comparison with observational data we have betrayed a theoretician’s best instinct and used physical units instead of normalized dimensionless units.
Paper: Formation and Reconnection of Electron Scale Current Layers in the Turbulent Outflows of a Primary Reconnection Site
Authors: Giovanni Lapenta, Martin Goldman, David L. Newman, Stefan Eriksson
Figure caption: Scatter plot of the identified current layers. Each layer is characterized with an ellipsoid with three axes: σ 1, σ 2, σ 3, ordered in decreasing size. The plot shows the major axis (length of the current layer) on the abscissa and the aspect ratio of the smallest to the largest axis of each current cluster (modeled as an ellipsoid) in the ordinate. From top to bottom: (a) parallel electric field, (b) agyrotropy, (c) dissipation in the electron comoving frame, all averaged over the cells comprising the current layer.
Paper: Formation and Reconnection of Electron Scale Current Layers in the Turbulent Outflows of a Primary Reconnection Site
Authors: Giovanni Lapenta, Martin Goldman, David L. Newman, Stefan Eriksson
Figure caption: Orthogonal views of the current layers identified by the DBSCAN clustering algorithm for the bottom (panels (a) and (b)) and top (panel (c)) of the system. Each cluster is shown with a different color. The big central laminar current sheet at x = L  x /2 is not shown to avoid overcrowding the figure. Each pixel shown is one cell of the computational domain flagged as carrying a significant electron current.
Paper: Formation and Reconnection of Electron Scale Current Layers in the Turbulent Outflows of a Primary Reconnection Site
Authors: Giovanni Lapenta, Martin Goldman, David L. Newman, Stefan Eriksson
Figure caption: Magnitude of the electron current. Panel (a) shows a 3D visualization with two different cuts with a color scale that highlights the local turbulent variations of the current. Panel (b) is a 2D cut at z = L  z /2 using a different color scale.
Paper: Formation and Reconnection of Electron Scale Current Layers in the Turbulent Outflows of a Primary Reconnection Site
Authors: Giovanni Lapenta, Martin Goldman, David L. Newman, Stefan Eriksson
Figure caption: Scatter plot of the identified current layers based on their average agyrotropy and average parallel electric field. The dot size is proportional to the number of cells forming the current and their color is proportional to the measured Lorentz reconnection indicator, in logarithmic scale, ﹩{\mathrm{log}}_{10}({v}_{L}/c)﹩ (Lapenta 2021).
Paper: Formation and Reconnection of Electron Scale Current Layers in the Turbulent Outflows of a Primary Reconnection Site
Authors: Giovanni Lapenta, Martin Goldman, David L. Newman, Stefan Eriksson
Figure caption: Cross section of the domain at the same time used in the previous analysis (cycle 18,000) at y = 8.27. The path of the virtual probe used in Figure 6 is shown as a white arrow. False color representation of the magnetic field intensity in nT (panel (a)) and of agyrotropy (panel (b)).
Paper: Formation and Reconnection of Electron Scale Current Layers in the Turbulent Outflows of a Primary Reconnection Site
Authors: Giovanni Lapenta, Martin Goldman, David L. Newman, Stefan Eriksson
Figure caption: Scatter plot of the identified current layers based on their average ion and electron current. The size of each dot is proportional to the volume of the current layer and their color represents the average agyrotropy as shown in the colorbar.