adsabs/AstroCLIMB huggingface dataset:
Paper: Extended 3He-rich Time Periods Observed by Solar Orbiter: Magnetic Connectivity and Sources
Authors: A. Kouloumvakos, G. M. Mason, G. C. Ho, R. C. Allen, Robert F. Wimmer-Schweingruber, A. P. Rouillard, J. Rodriguez-Pacheco
Figure caption: Statistical results from the characteristics of the extended 3He time periods. Panel (a) shows the relation between the total duration of the extended 3He-rich time periods with the spacecraft radial distance measured at the beginning of each time period. At the bottom and right axis, we show the distributions of the total duration and the radial distance, respectively, and we note the median values for each case. Panel (b) shows the relation between the total duration of the time periods and the peak flux of the 3He. On the right axis, we show the distribution of the peak flux of 3He and note the median value. Panel (c) shows the distributions of the peak flux of 3He (blue) and the total duration of the time periods (red) for the three injection classes using a box-plot format.
Paper: Can Cosmologically Coupled Mass Growth of Black Holes Solve the Mass Gap Problem?
Authors: Shi-Jie Gao, Xiang-Dong Li
Figure caption: Orbital periods (P orb), BH mass (M BH), and companion mass (M 2) as a function of stellar age (t age) and redshift (z) for tracks a0/a3 (left), b0/b3 (middle), and c0/c3 (right). The red and blue lines correspond to the k = 0 and k = 3 cases, respectively. The solid and dashed lines in the lower panel show the evolution of the BH and the companion, respectively. The circles and crosses indicate the onset and end of RLOF, respectively.
Paper: Can Cosmologically Coupled Mass Growth of Black Holes Solve the Mass Gap Problem?
Authors: Shi-Jie Gao, Xiang-Dong Li
Figure caption: Number distribution of I/LMXBs in the donor mass–BH mass (M 2–M BH) plane. The upper and lower panels correspond k = 0 and k = 3 cases, respectively. The left, middle, and right panels represent the results in the rapid, delayed, and stochastic supernova models, respectively. The number of I/LMXBs in each pixel is represented by different colors. The green crosses with errors show the observed L/IMXBs (see Table 1).
Paper: Can Cosmologically Coupled Mass Growth of Black Holes Solve the Mass Gap Problem?
Authors: Shi-Jie Gao, Xiang-Dong Li
Figure caption: Mass distribution of BHs in I/LMXBs. The left, middle, and right panels show the results of the rapid, delayed, and stochastic supernova models. The red and blue solid histograms correspond to k = 0 and k = 3 cases, respectively. The red and blue dashed lines show the normalized cumulative mass distribution in the range of 2.5–15 M ⊙ in k = 0 and k = 3 cases, respectively. The shaded region indicates the mass gap (2.5–5 M ⊙).
Paper: Mapping the Decline with Redshift of Dusty Star-forming Galaxies Using JWST and SCUBA-2
Authors: A. J. Barger, L. L. Cowie
Figure caption: Three-color JWST NIRCam images (blue = F115W, green = F150W, and red=F444W) for the 44 >3σ SCUBA-2 850 μm detected JWST NIRCam f F444W > 1 μJy and f F444W/f F150W > 3.5 sources in the UNCOVER area (Table 3). The demagnified 850 μm flux is shown in the lower left, together with the photometric (photz) and spectroscopic (specz) redshifts. Sources with a Chandra detection are labeled X-ray in the upper left. Sources with direct >4.5σ ALMA detections (Table 1) or direct >5σ SCUBA-2 detections (Table 2) are labeled with those numbers in the upper right. The thumbnails are 6″ on a side, or roughly 50 kpc at z = 2.
Paper: Mapping the Decline with Redshift of Dusty Star-forming Galaxies Using JWST and SCUBA-2
Authors: A. J. Barger, L. L. Cowie
Figure caption:  f F444W/f F150W vs. f F444W for the full sample in the JWST NIRCam plus SCUBA-2 footprint with f F444W > 0.05 μJy (black dots). Squares show the red galaxies with f F444W/f F150W > 3.5, with those having >3σ 850 μm detections marked in red. For these red galaxies: the small number of objects in the Paris et al. (2023) catalog with multiple parts were combined into single objects; the four stars are shown with star symbols (none are detected at 850 μm); and no source that lies closer than 4″ to a f F444W-brighter red galaxy is shown to avoid multiple-counting in the submillimeter.
Paper: Mapping the Decline with Redshift of Dusty Star-forming Galaxies Using JWST and SCUBA-2
Authors: A. J. Barger, L. L. Cowie
Figure caption:                    ﹩{f}_{850\mu {\rm{m}}}^{d}﹩ vs. ﹩{L}_{\nu }^{d}﹩(5000) for the (a) z < 4 and (b) z > 4 sources in our extended sample. Sources with >3σ 850 μm detections are marked in red. X-ray sources are enclosed in large green squares. The solid diamonds show the mean values in the ﹩{L}_{\nu }^{d}﹩(5000) ranges 1028 to 5 × 1028, 5 × 1028 to 1.5 × 1029, and 1.5 × 1029 to 4 × 1029 erg s−1 Hz−1. The curves correspond to R = 30 (gold) and R = 6 (purple) (see Equation (1)).
Paper: Mapping the Decline with Redshift of Dusty Star-forming Galaxies Using JWST and SCUBA-2
Authors: A. J. Barger, L. L. Cowie
Figure caption: Two examples of faint SCUBA-2 850 μm sources (white contours: 0.6 and 1.2 mJy per beam; diamonds: local peaks; fluxes shown in lower-left corner) found by using the red galaxy priors. Both sources lie in the JWST NIRCam footprint but not in the combined ALMA mosaics from AFFS and ALCS. The underlying images are three-color JWST (blue = F115W, green = F150W, and red = F444W). The priors are shown with green squares. The pixels are 0.″03, and the fields are 30″ on a side.
Paper: Mapping the Decline with Redshift of Dusty Star-forming Galaxies Using JWST and SCUBA-2
Authors: A. J. Barger, L. L. Cowie
Figure caption: Photometric redshift vs. ﹩{L}_{\nu }^{d}﹩(5000) for our extended sample. Sources with >3σ 850 μm detections are marked in red. We show sources whose photometric redshifts are >9 at z = 9 with upward pointing arrows for illustrative purposes only.
Paper: Interstellar Carbonaceous Dust Erosion Induced by X-Ray Irradiation of Water Ice in Star-forming Regions
Authors: K.-J. Chuang, C. Jäger, N.-E. Sie, C.-H. Huang, C.-Y. Lee, Y.-Y. Hsu, Th. Henning, Y.-J. Chen
Figure caption: Left: the IR difference spectra obtained before and after X-ray irradiation of H2O ice on a-13C dust analog at 15 K for 60 minutes. The thickness of a-13C dust is ∼100 nm, and the deposited abundance of H2O is ∼5 ×1017 molecule cm−2. The dashed lines highlight the peak position of 13C-labeled products. The spectra are offset for clarity. Right: abundance evolution of the product 13CO2 (solid) and 13CO (open) obtained from the X-ray irradiation of H2O ice on the same a-13C dust over X-ray photons fluence of (7.6–8.0) ×1018 photon cm−2 (i.e., (7.0–7.4) ×1020 eV cm−2). The dashed lines show the linear fit for the initial formation rate.
Paper: Interstellar Carbonaceous Dust Erosion Induced by X-Ray Irradiation of Water Ice in Star-forming Regions
Authors: K.-J. Chuang, C. Jäger, N.-E. Sie, C.-H. Huang, C.-Y. Lee, Y.-Y. Hsu, Th. Henning, Y.-J. Chen
Figure caption: Left: the IR difference spectra obtained before and after X-ray irradiation of (a) (16)O2 and (b) 18O2 ices on the same a-13C dust analog as well as (c) H2O on a-13C dust analog at 15 K for 60 minutes. Right: the corresponding residual spectra measured at 300 K. The thickness of a-13C dust is ∼100 nm, and the deposited abundances of H2O and (16/18) O2 are ∼5 ×1017 molecule cm−2. The total fluence of X-ray photons is (7.6–7.9) ×1018 photon cm−2. The dashed lines highlight the peak position of 13C-labeled products, and the shadowed area highlights the regions of the carbonyl group feature. The spectra are offset for clarity.
Paper: Interstellar Carbonaceous Dust Erosion Induced by X-Ray Irradiation of Water Ice in Star-forming Regions
Authors: K.-J. Chuang, C. Jäger, N.-E. Sie, C.-H. Huang, C.-Y. Lee, Y.-Y. Hsu, Th. Henning, Y.-J. Chen
Figure caption: Abundance evolution of the product 13CO2 (left) and 13CO (right) obtained from the X-ray irradiation of O2 ice on a-13C dust sample with a thickness of 100 nm over photon fluence of 7.6 ×10−18 photon cm−2 The solid lines show the total fitting results and the dotted and dashed lines represent the fitting curves "[1]" and "[2]", respectively.
Paper: Characterizing Pulsars Detected in the Rapid ASKAP Continuum Survey
Authors: Akash Anumarlapudi, Anna Ehlke, Megan L. Jones, David L. Kaplan, Dougal Dobie, Emil Lenc, James K. Leung, Tara Murphy, Joshua Pritchard, Adam J. Stewart, Rahul Sengar, Craig Anderson, Julie Banfield, George Heald, Aidan W. Hotan, David McConnell, Vanessa A. Moss, Wasim Raja, Matthew T. Whiting
Figure caption: Top: circular polarization fractions for the pulsars in our sample. Shown by the orange diamonds are the polarization fractions for sources detected in both Stokes I and Stokes V. Shown by the blue triangles are the upper limits in the cases of Stokes V nondetections, and shown by the black dashed line is the 1% polarization resulting from leakage into Stokes V (Pritchard et al. 2021). Shown by the vertical red dashed line is the Stokes I completeness limit (see Figure 3), and shown by the blue dashed line is the expected polarization fraction for a Stokes V flux density that is twice the all-sky RMS value in the RACS survey. Bottom: distribution of circular polarization fractions for pulsars detected in the RACS Stokes V survey. The blue shaded histogram shows the distribution for the 61/661 pulsars that are detected in Stokes V images, the black histogram shows the distribution of the polarization fractions from nondetections (using upper limits), and the green shaded region shows the polarization values from the literature (Gould & Lyne 1998; Sobey et al. 2021; Oswald et al. 2023). The distribution is peaked around 10%, with few pulsars having higher polarization fractions. The black dashed line shows the mean polarization fraction (4.6%) using the Kaplan–Meier estimate, and the black dotted line indicates the 1σ spread (8.6%) from the mean of the distribution.
Paper: Characterizing Pulsars Detected in the Rapid ASKAP Continuum Survey
Authors: Akash Anumarlapudi, Anna Ehlke, Megan L. Jones, David L. Kaplan, Dougal Dobie, Emil Lenc, James K. Leung, Tara Murphy, Joshua Pritchard, Adam J. Stewart, Rahul Sengar, Craig Anderson, Julie Banfield, George Heald, Aidan W. Hotan, David McConnell, Vanessa A. Moss, Wasim Raja, Matthew T. Whiting
Figure caption: The residual (observed−predicted in logarithmic space) or the ratio between the observed flux density and the power-law-modeled flux density for the 150 pulsars that exhibit monotonic trends. The individual colored dashed lines show the residuals for each pulsar in our 150-pulsar sample. The color scheme represents the degree of error summed over the three frequencies resulting from a power-law fit, with violet and yellow representing maximal overprediction and underprediction, respectively, by a power-law spectrum. It can be clearly seen that for many pulsars, a simple power-law fit is not adequate where the lower- and higher-frequency deviations are very commonly seen.
Paper: Characterizing Pulsars Detected in the Rapid ASKAP Continuum Survey
Authors: Akash Anumarlapudi, Anna Ehlke, Megan L. Jones, David L. Kaplan, Dougal Dobie, Emil Lenc, James K. Leung, Tara Murphy, Joshua Pritchard, Adam J. Stewart, Rahul Sengar, Craig Anderson, Julie Banfield, George Heald, Aidan W. Hotan, David McConnell, Vanessa A. Moss, Wasim Raja, Matthew T. Whiting
Figure caption: The distribution of the number of pulsars as a function of flux density detected in the Stokes I images (left) vs. the Stokes V images (right) is shown by the red histogram. Shown by the dashed black line is a power-law fit to the number of sources per flux density bin, assuming a two-dimensional (Galactic) distribution of standard candles (β = −1). The vertical black dashed–dotted line shows the flux density limit below which we see large deviations in the observed number of sources, suggesting that the survey is complete above ≈2  mJy.
Paper: Characterizing Pulsars Detected in the Rapid ASKAP Continuum Survey
Authors: Akash Anumarlapudi, Anna Ehlke, Megan L. Jones, David L. Kaplan, Dougal Dobie, Emil Lenc, James K. Leung, Tara Murphy, Joshua Pritchard, Adam J. Stewart, Rahul Sengar, Craig Anderson, Julie Banfield, George Heald, Aidan W. Hotan, David McConnell, Vanessa A. Moss, Wasim Raja, Matthew T. Whiting
Figure caption: The distribution of the Galactic latitudes of the pulsars detected in our sample. The blue histogram shows the Galactic latitudes of the pulsars detected in the RACS survey, and the green histogram shows the overall distribution of the pulsars from the ATNF catalog. We see that there is a deficit in the number of pulsars detected for ∣b∣ < 8° (the vertical dashed line). We then remove all the detected pulsars below 3 mJy, and the resulting distribution (orange histogram) traces the expected population.
Paper: Characterizing Pulsars Detected in the Rapid ASKAP Continuum Survey
Authors: Akash Anumarlapudi, Anna Ehlke, Megan L. Jones, David L. Kaplan, Dougal Dobie, Emil Lenc, James K. Leung, Tara Murphy, Joshua Pritchard, Adam J. Stewart, Rahul Sengar, Craig Anderson, Julie Banfield, George Heald, Aidan W. Hotan, David McConnell, Vanessa A. Moss, Wasim Raja, Matthew T. Whiting
Figure caption: Distribution of spectral indices using the sample of pulsars in RACS that have measured flux densities at both 400 and 1400 MHz. The blue shaded histogram shows the spectral index from a fit using the flux at all three frequencies, while the green histogram shows the best-fit index using the two higher frequencies; the dashed black histogram shows the same, using the two lower frequencies, and the magenta histogram shows the distribution using archival (400 and 1400 MHz) data. The golden shaded region shows the range of spectral values reported in the literature (varying from −1.9 to −1.4) and the black dashed line shows the mean of the distribution using the three frequencies in this work, −1.78.
Paper: Characterizing Pulsars Detected in the Rapid ASKAP Continuum Survey
Authors: Akash Anumarlapudi, Anna Ehlke, Megan L. Jones, David L. Kaplan, Dougal Dobie, Emil Lenc, James K. Leung, Tara Murphy, Joshua Pritchard, Adam J. Stewart, Rahul Sengar, Craig Anderson, Julie Banfield, George Heald, Aidan W. Hotan, David McConnell, Vanessa A. Moss, Wasim Raja, Matthew T. Whiting
Figure caption: The sample of 18 pulsars that deviate significantly from monotonic spectral energy distributions. Each line in the plot shows the spectrum for a single pulsar using the flux density measurements taken at 400, 888, and 1400 MHz. The color scheme represents the extent of the deviation from a flat spectrum (violet/yellow corresponds to maximum deficit/excess) added over the three frequencies. The flux density at 888 MHz is normalized to 1. We excluded such pulsars from the fit when using a simple power law to model the spectrum.
Paper: Characterizing Pulsars Detected in the Rapid ASKAP Continuum Survey
Authors: Akash Anumarlapudi, Anna Ehlke, Megan L. Jones, David L. Kaplan, Dougal Dobie, Emil Lenc, James K. Leung, Tara Murphy, Joshua Pritchard, Adam J. Stewart, Rahul Sengar, Craig Anderson, Julie Banfield, George Heald, Aidan W. Hotan, David McConnell, Vanessa A. Moss, Wasim Raja, Matthew T. Whiting
Figure caption: For pulsars identified in the RACS data, the fractional error in flux density due to diffractive scintillation as a function of the DM is shown as the red dots. We see that only a few pulsars (18 pulsars in the sample—∼2.5% of the sample) are strongly affected (having a fractional error >0.5) by scintillation, and most of them have DM < 10 pc/cm3. We can also see that most of the pulsars that have a fractional error of >0.1 have DM < 40 pc/cm3.
Paper: Characterizing Pulsars Detected in the Rapid ASKAP Continuum Survey
Authors: Akash Anumarlapudi, Anna Ehlke, Megan L. Jones, David L. Kaplan, Dougal Dobie, Emil Lenc, James K. Leung, Tara Murphy, Joshua Pritchard, Adam J. Stewart, Rahul Sengar, Craig Anderson, Julie Banfield, George Heald, Aidan W. Hotan, David McConnell, Vanessa A. Moss, Wasim Raja, Matthew T. Whiting
Figure caption: Residuals between the observed flux densities and the power-law-modeled flux densities at all three different frequencies—400, 888, and 1400 MHz, shown by orange, blue, and green error bars, respectively. The residuals are normalized by the uncertainty in the flux density measurements at the three different frequencies.
Paper: Characterizing Pulsars Detected in the Rapid ASKAP Continuum Survey
Authors: Akash Anumarlapudi, Anna Ehlke, Megan L. Jones, David L. Kaplan, Dougal Dobie, Emil Lenc, James K. Leung, Tara Murphy, Joshua Pritchard, Adam J. Stewart, Rahul Sengar, Craig Anderson, Julie Banfield, George Heald, Aidan W. Hotan, David McConnell, Vanessa A. Moss, Wasim Raja, Matthew T. Whiting
Figure caption: The distribution of spectral indices as a function of the pulsar’s period. We see two clear populations representing the normal pulsars and the recycled pulsars. There is no clear evidence for steep spectral indices in the recycled pulsars compared to normal pulsars.
Paper: Standardized Luminosity of the Tip of the Red Giant Branch Utilizing Multiple Fields in NGC 4258 and the CATs Algorithm
Authors: Siyang Li, Adam G. Riess, Daniel Scolnic, Gagandeep S. Anand, Jiaxi Wu, Stefano Casertano, Wenlong Yuan, Rachael Beaton, Richard I. Anderson
Figure caption: CMDs and LFs for simulated stellar populations of [Fe/H] = −2.0, −1.7, −1.3, and −1.0 and ages of 13, 10, 6, and 3 Gyr, respectively, from clockwise order from the top left. Blue diagonal lines in the left subpanels are the color bands used. Red and blue lines in both subpanels correspond to smoothing values of s = 0.05 and s = 0.15, respectively. Solid, dashed, and dotted–dashed lines correspond to the measured tip, smoothed LF, and Sobel response, respectively. We shade the extra space representing extra stars underneath the smoothed LF created by applying a higher smoothing parameter in red.
Paper: Constraining Nuclear Parameters Using Gravitational Waves from f-mode Oscillations in Neutron Stars
Authors: Bikram Keshari Pradhan, Dhruv Pathak, Debarati Chatterjee
Figure caption: Joint distribution of the posteriors of the nuclear parameters recovered from the posterior of (f, τ) (see Figure 2) for the considered event in A+ (blue line) and ET (red lines). The black lines show the injected values. The median and 90% SCIs are also shown in the respective marginalized one-dimensional posterior histograms. The considered priors are also shown in green color.
Paper: Standardized Luminosity of the Tip of the Red Giant Branch Utilizing Multiple Fields in NGC 4258 and the CATs Algorithm
Authors: Siyang Li, Adam G. Riess, Daniel Scolnic, Gagandeep S. Anand, Jiaxi Wu, Stefano Casertano, Wenlong Yuan, Rachael Beaton, Richard I. Anderson
Figure caption: Sobel responses with four smoothings (s = 0.01 (top left), 0.05 (top right), 0.1 (bottom left), and 0.15 (bottom right)) and three different weightings (CATs (orange; Equation (B1)), inverse variance (green; Equation (B2)), and none (blue)) on the same LF simulated with 1,000,000 samples using von Neumann rejection sampling, a TRGB at −4 mag, and shape parameters of α = β = γ = 0.3 for the broken-power-law model described in Méndez et al. (2002), Makarov et al. (2006), and Li et al. (2022). The vertical red lines mark the location of the TRGB in each subplot.
Paper: Constraining Nuclear Parameters Using Gravitational Waves from f-mode Oscillations in Neutron Stars
Authors: Bikram Keshari Pradhan, Dhruv Pathak, Debarati Chatterjee
Figure caption: Distribution of glitches in the d and ﹩\tfrac{{\rm{\Delta }}\nu }{\nu }﹩ plane having S/N ≥ 8 in (a) A + configuration and (b) ET configuration. In both (a) and (b), the frequency histogram of the glitches and distances with network S/N ≥ 8 are also plotted in the top  and right panels, respectively. In (a), all glitches shown are from Vela, which is also reflected as a single bar in the histogram of (a) corresponding to distance.
Paper: Constraining Nuclear Parameters Using Gravitational Waves from f-mode Oscillations in Neutron Stars
Authors: Bikram Keshari Pradhan, Dhruv Pathak, Debarati Chatterjee
Figure caption: The joint corner and marginalized posterior distribution of the recovered (f, τ) for an injected event corresponding to one of the Vela glitches with ﹩\tfrac{{\rm{\Delta }}\nu }{\nu }=3.1\times {10}^{-6}﹩ in A+ (blue in color) and ET (red) GW detector configurations. The black lines display the injected values. The 90% SCIs are also shown with dashed lines. The errors shown on top correspond to the 90% SCI.
Paper: Standardized Luminosity of the Tip of the Red Giant Branch Utilizing Multiple Fields in NGC 4258 and the CATs Algorithm
Authors: Siyang Li, Adam G. Riess, Daniel Scolnic, Gagandeep S. Anand, Jiaxi Wu, Stefano Casertano, Wenlong Yuan, Rachael Beaton, Richard I. Anderson
Figure caption: 90% bootstrap widths for the SN Ia host galaxies from Scolnic et al. (2023). We indicate the limit of 0.025 mag used by Hoyt (2023) to select LMC fields such that all bootstrap widths greater than 0.025 mag would be rejected. We find that none of the SN Ia host galaxies would pass the cuts made by Hoyt (2023) for the LMC.
Paper: Standardized Luminosity of the Tip of the Red Giant Branch Utilizing Multiple Fields in NGC 4258 and the CATs Algorithm
Authors: Siyang Li, Adam G. Riess, Daniel Scolnic, Gagandeep S. Anand, Jiaxi Wu, Stefano Casertano, Wenlong Yuan, Rachael Beaton, Richard I. Anderson
Figure caption: Tips from Hoyt (2023) as a function of their contrast ratio.
Paper: Standardized Luminosity of the Tip of the Red Giant Branch Utilizing Multiple Fields in NGC 4258 and the CATs Algorithm
Authors: Siyang Li, Adam G. Riess, Daniel Scolnic, Gagandeep S. Anand, Jiaxi Wu, Stefano Casertano, Wenlong Yuan, Rachael Beaton, Richard I. Anderson
Figure caption: Grouping of the three G fields for Field 4. We remove the fields colored in black and green; Field 4 comprises only the fields colored in blue and red. In our analysis we measure the tip separately for G1 and G2.
Paper: Collapse of Rotating Massive Stars Leading to Black Hole Formation and Energetic Supernovae
Authors: Sho Fujibayashi, Yuichiro Sekiguchi, Masaru Shibata, Shinya Wanajo
Figure caption: Top panel: mass-infall rate across the surface of r = r in (solid curves) and mass accretion rate onto the black hole (dashed curves). Circles on each curve denote the time at which the viscosity is turned on. Middle panel: total neutrino luminosity (solid curves) and total viscous heating rate (dashed curves) inside the shock wave. Bottom panel: neutrino cooling efficiency defined by the total neutrino luminosity divided by the mass accretion rate onto the black hole. For model BHdisk, t pb = 0 corresponds to the beginning of the simulation.
Paper: Collapse of Rotating Massive Stars Leading to Black Hole Formation and Energetic Supernovae
Authors: Sho Fujibayashi, Yuichiro Sekiguchi, Masaru Shibata, Shinya Wanajo
Figure caption: Bolometric light-curve models. The time origin is chosen to be the peak time for each curve. The solid curves denote the light curves with ejecta mass and explosion energy extracted for r ext = 2 × 109 cm (see Table 2 for the values). The dashed curves denote those with the assumption that a half of the mass and binding energy outside the extraction radius contribute to the ejecta properties. The point shows the time at which the ejecta becomes optically thin, τ = κ ρ R = 1, to thermal photons for each model. The shaded regions denote the templates of the bolometric light curves with standard deviations for type Ib, Ic, and Ic-BL supernovae taken from Lyman et al. (2016).
Paper: Collapse of Rotating Massive Stars Leading to Black Hole Formation and Energetic Supernovae
Authors: Sho Fujibayashi, Yuichiro Sekiguchi, Masaru Shibata, Shinya Wanajo
Figure caption: The same as Figure 2 but for models AD09x1 (top panels) and AD20x2 (bottom panels). For each model, the panels from left to right show the snapshots at the formation of a geometrically thick disk, after the onset of the outflow, and the final snapshots, respectively.