adsabs/AstroCLIMB huggingface dataset:
Paper: Calculation and Uncertainty of Fast Radio Burst Structure Based on Smoothed Data
Authors: Adrian T. Sutinjo, Danica R. Scott, Clancy W. James, Marcin Glowacki, Keith W. Bannister, Hyerin Cho, 혜린 조, Cherie K. Day, Adam T. Deller, Timothy P. Perrett, Ryan M. Shannon
Figure caption: Example noisy pulse (top) and the corresponding spectrum in discrete cosine (bottom). The underlying pulse consists of two unity amplitude Gaussians shown as the red dashed line in the top panel. The offset seen in the black curve is due to additive noise in the simulated noisy data. The solid black curve in the top plot represents the recovered intensity with filter parameters O = 3 and  k  c  = 15.
Paper: Calculation and Uncertainty of Fast Radio Burst Structure Based on Smoothed Data
Authors: Adrian T. Sutinjo, Danica R. Scott, Clancy W. James, Marcin Glowacki, Keith W. Bannister, Hyerin Cho, 혜린 조, Cherie K. Day, Adam T. Deller, Timothy P. Perrett, Ryan M. Shannon
Figure caption: The top left panel shows the mean intensity over frequency of FRB 20181112A at ΔDM = 0 vs. time. The middle left panel is the dynamic spectrum of FRB 20181112A at ΔDM = 0 at 1 μs resolution. The bottom left panel shows intensities vs. time and ΔDM of FRB 20181112A at 1 μs resolution data before filtering. The top right panel shows the DCT spectrum of FRB 20181112A. The middle right panel reports the structure parameters of the recovered signal. The bottom right panel shows the difference between the right- and left-hand sides of Equation (11); the error bounds are inferred from the zero crossings.
Paper: Calculation and Uncertainty of Fast Radio Burst Structure Based on Smoothed Data
Authors: Adrian T. Sutinjo, Danica R. Scott, Clancy W. James, Marcin Glowacki, Keith W. Bannister, Hyerin Cho, 혜린 조, Cherie K. Day, Adam T. Deller, Timothy P. Perrett, Ryan M. Shannon
Figure caption: The top left panel shows the mean intensity over frequency of FRB 20210117A at ΔDM = 0 vs. time. The middle left panel is the dynamic spectrum of FRB 20210117A at ΔDM = 0 at 50 μs resolution. The bottom left panel shows intensities vs. time and ΔDM of FRB 20210117A data at 1 μs resolution before filtering. The top right panel shows the DCT spectrum of FRB 20210117A. The middle right panel reports the structure parameters of the recovered signal. The bottom right panel shows the difference between the right- and left-hand sides of Equation (11); the error bounds are inferred from the zero crossings.
Paper: FAST Drift Scan Survey for HI Intensity Mapping: I. Preliminary Data Analysis
Authors: Yichao Li, Yougang Wang, Furen Deng, Wenxiu Yang, Wenkai Hu, Diyang Liu, Xinyang Zhao, Shifan Zuo, Shuanghao Shu, Jixia Li, Peter Timbie, Réza Ansari, Olivier Perdereau, Albert Stebbins, Laura Wolz, Fengquan Wu, Xin Zhang, Xuelei Chen
Figure caption: The positions of the feeds in the FAST L-band 19-feed array. The feed array without rotation is shown in the left-hand panel and the feed array rotated by ﹩23\mathop{.}\limits^{\circ }4﹩ is shown in the right-hand panel. The circles represent the ﹩3^{\prime} ﹩ beam size at a frequency of 1420 MHz. The central, inner-circle, and outer-circle feeds are shown in red, blue, and green, respectively.
Paper: Calculation and Uncertainty of Fast Radio Burst Structure Based on Smoothed Data
Authors: Adrian T. Sutinjo, Danica R. Scott, Clancy W. James, Marcin Glowacki, Keith W. Bannister, Hyerin Cho, 혜린 조, Cherie K. Day, Adam T. Deller, Timothy P. Perrett, Ryan M. Shannon
Figure caption: Structure-maximizing ΔDM (solid) and 68% error bounds (dashed) for FRB 20210117A as a function of filter cutoff k  c  (O = 3).
Paper: Calculation and Uncertainty of Fast Radio Burst Structure Based on Smoothed Data
Authors: Adrian T. Sutinjo, Danica R. Scott, Clancy W. James, Marcin Glowacki, Keith W. Bannister, Hyerin Cho, 혜린 조, Cherie K. Day, Adam T. Deller, Timothy P. Perrett, Ryan M. Shannon
Figure caption: Recovered structure parameter (top) and uncertainty (bottom) of the structure parameter for k  c  swept from 3 to 300 and filter order 2, 3, and 4 in Equation (16).
Paper: ALMA 0.5 kpc Resolution Spatially Resolved Investigations of Nuclear Dense Molecular Gas Properties in Nearby Ultraluminous Infrared Galaxies Based on HCN and HCO+ Three Transition Line Data
Authors: Masatoshi Imanishi, 昌俊 今西, Shunsuke Baba, 俊介 馬場, Kouichiro Nakanishi, 康一郎 中西, Takuma Izumi, 拓磨 泉
Figure caption: Fitting results for the high-J to low-J flux ratios of HCN and HCO+ for the central ≲0.5 kpc regions of (U)LIRGs. (Left panel): Comparison of the observed and RADEX-calculated emission line flux ratios. The filled light blue circles show the observed flux ratios listed in Table 13. The open green squares indicate the flux ratios of the best-fit model, whose gas density and temperature are denoted as the plus sign in the right panel. Other fixed parameters (column density, abundance ratio, and line width) are noted at the top of the figure. We adopt the second fitting results (flux scaling adjustment allowed; see Section 5.3) for IRAS 00188−0856, IRAS 00456−2904, IRAS 22491−1808, and NGC 1614, for which the observed flux ratios after scaling adjustment are displayed in the half-filled dark blue circles. The scaling factors for each observation are listed below the legend. The reduced χ 2 value of the best-fit model is also noted. (Right panel): Confidence contours for the gas density and temperature quoted at 68%, 90%, and 99% levels (Δχ 2 = 2.28, 4.61, 9.21). The result for IRAS 16090−0139 is displayed separately in Figure 11(a).
Paper: ALMA 0.5 kpc Resolution Spatially Resolved Investigations of Nuclear Dense Molecular Gas Properties in Nearby Ultraluminous Infrared Galaxies Based on HCN and HCO+ Three Transition Line Data
Authors: Masatoshi Imanishi, 昌俊 今西, Shunsuke Baba, 俊介 馬場, Kouichiro Nakanishi, 康一郎 中西, Takuma Izumi, 拓磨 泉
Figure caption:  J = 4–3 (blue circle) or J = 3–2 (red square) to J = 2–1 flux ratio of HCN (filled symbol) and HCO+ (open symbol) measured in the ≲0.5 kpc, ≲1 kpc, 0.5–1 kpc, ≲2 kpc, and 1–2 kpc spectra. Only the Gaussian fit statistical uncertainty is considered, and only ratios with ≳2.5σ are plotted. The vertical axis range of the single LIRG NGC 1614 is much narrower than that of the ULIRGs.
Paper: ALMA 0.5 kpc Resolution Spatially Resolved Investigations of Nuclear Dense Molecular Gas Properties in Nearby Ultraluminous Infrared Galaxies Based on HCN and HCO+ Three Transition Line Data
Authors: Masatoshi Imanishi, 昌俊 今西, Shunsuke Baba, 俊介 馬場, Kouichiro Nakanishi, 康一郎 中西, Takuma Izumi, 拓磨 泉
Figure caption: Comparison of the HCN-to-HCO+ flux ratios measured in the 0.5 kpc beam-sized spectra and those calculated with RADEX. (Left panel): 3D plot of the flux ratios at J = 2–1, J = 3–2, and J = 4–3. The red points represent the observed values. The RADEX-calculated flux ratios are computed for log ﹩{n}_{{{\rm{H}}}_{2}}﹩/cm−3=3–8 in steps of 0.1 (density) and log (T kin/K) =1–3 in steps of 0.05 (temperature). The ratios are shown as a blue mesh consisting of isodensity curves at log ﹩{n}_{{{\rm{H}}}_{2}}\,﹩ = 3, 4, ⋯, 8 (solid), and isotemperature curves at log T kin  = 1.0, 1.5, ⋯, 3.0 (dotted). The molecular line width and HCO+ column density are fixed at Δv = 500 km s−1 and N HCO+  = 1 × 1016 cm−2, respectively. The results of the HCN-to-HCO+ abundance ratio of [HCN]/[HCO+] = 1 and 3 are drawn in dark and light colors, respectively. (Right panels): Projections of the 3D plot along the J = 3–2 (upper) and J = 4–3 (lower) directions.
Paper: ALMA 0.5 kpc Resolution Spatially Resolved Investigations of Nuclear Dense Molecular Gas Properties in Nearby Ultraluminous Infrared Galaxies Based on HCN and HCO+ Three Transition Line Data
Authors: Masatoshi Imanishi, 昌俊 今西, Shunsuke Baba, 俊介 馬場, Kouichiro Nakanishi, 康一郎 中西, Takuma Izumi, 拓磨 泉
Figure caption: Fitting results for the high-J to low-J flux ratios of HCN and HCO+ for various regions of IRAS 16090−0139. (a) Central ≲0.5 kpc region. (b) 0.5–1 kpc annular region. (c) 1–2 kpc annular region. (d) Central ≲1 kpc region. (e) Central ≲2 kpc region. We adopt the second fitting result (flux scaling adjustment allowed) for all regions. The content of each panel and the symbols are the same as Figure 10.
Paper: ALMA 0.5 kpc Resolution Spatially Resolved Investigations of Nuclear Dense Molecular Gas Properties in Nearby Ultraluminous Infrared Galaxies Based on HCN and HCO+ Three Transition Line Data
Authors: Masatoshi Imanishi, 昌俊 今西, Shunsuke Baba, 俊介 馬場, Kouichiro Nakanishi, 康一郎 中西, Takuma Izumi, 拓磨 泉
Figure caption: Example result of the MCMC parameter estimation using the HCN-to-HCO+ and HCO+ multiple J-transition line flux ratios. (a) Central ≲0.5 kpc region of IRAS 16090−0139. (b) Central ≲0.5 kpc region of IRAS 22491−1808. (c) Central ≲1 kpc region of NGC 1614. The corner plot on the left shows 1D and 2D projections of the posterior distribution for any parameter and parameter pairs, respectively. The median and 68% credible bounds of each parameter are given in the label above each column and are denoted by the dashed and dotted lines, respectively, in the 1D posterior. The panel on the upper right shows a comparison of the observed and modeled emission line flux ratios. The model flux ratios (open green squares) are calculated at the medians of log ﹩{n}_{{{\rm{H}}}_{2}}﹩, log T kin, log ﹩{N}_{{\mathrm{HCO}}^{+}}﹩, and [HCN]/[HCO+]. The observed flux ratios (filled light blue circles) are quoted from Tables 12 and 13 and then scaled with the medians of the J21, J32, and J43 scaling factors (half-filled dark blue circles).
Paper: ALMA 0.5 kpc Resolution Spatially Resolved Investigations of Nuclear Dense Molecular Gas Properties in Nearby Ultraluminous Infrared Galaxies Based on HCN and HCO+ Three Transition Line Data
Authors: Masatoshi Imanishi, 昌俊 今西, Shunsuke Baba, 俊介 馬場, Kouichiro Nakanishi, 康一郎 中西, Takuma Izumi, 拓磨 泉
Figure caption: HCN-to-HCO+ flux ratio measured in the ≲0.5 kpc, ≲1 kpc, 0.5–1 kpc, ≲2 kpc, and 1–2 kpc spectra. Open red circle: J = 2–1. Open green star: J = 3–2. Filled blue square: J = 4–3. Only ratios with ≳2.5σ are plotted. Note that the vertical axis range of the single LIRG NGC 1614 is much narrower than that of the ULIRGs.
Paper: ALMA 0.5 kpc Resolution Spatially Resolved Investigations of Nuclear Dense Molecular Gas Properties in Nearby Ultraluminous Infrared Galaxies Based on HCN and HCO+ Three Transition Line Data
Authors: Masatoshi Imanishi, 昌俊 今西, Shunsuke Baba, 俊介 馬場, Kouichiro Nakanishi, 康一郎 中西, Takuma Izumi, 拓磨 泉
Figure caption: HCN J = 4–3 to HCO+ J = 4–3 flux ratio (abscissa) and HCN J = 4–3 to CS J = 7–6 flux ratio (ordinate) derived from the 0.5 kpc beam-sized spectra. The flux ratio is calculated in units of Jy km s−1. Izumi et al. (2016) proposed that starburst-dominated galaxies are distributed in the lower left region, separated by the dashed straight lines, while AGN-important galaxies are distributed in the remaining upper right region.
Paper: ALMA 0.5 kpc Resolution Spatially Resolved Investigations of Nuclear Dense Molecular Gas Properties in Nearby Ultraluminous Infrared Galaxies Based on HCN and HCO+ Three Transition Line Data
Authors: Masatoshi Imanishi, 昌俊 今西, Shunsuke Baba, 俊介 馬場, Kouichiro Nakanishi, 康一郎 中西, Takuma Izumi, 拓磨 泉
Figure caption: Original beam-sized map of the observed HCN-to-HCO+ flux ratio calculated in units of Jy km s−1. An appropriate cutoff (>2–3σ depending on each ULIRG) is applied for the HCO+ flux (i.e., denominator), so that the resulting map is not dominated by noise. The plus mark denotes the continuum peak position, which is regarded as the nucleus of each ULIRG. The length of the vertical solid black bar in the first image of each object corresponds to 1 kpc.
Paper: Photo-zSNthesis: Converting Type Ia Supernova Lightcurves to Redshift Estimates via Deep Learning
Authors: Helen Qu, Masao Sako
Figure caption: The model architecture developed for this work, described in the text in Section 3.3. A layer shown in the figure as “h × d conv, n filters” is a 2D convolutional layer with a kernel size of h × d and n filters filters. Similarly, “h × d, n filters resid block” defines a residual block containing two h × d conv, n  f  convolutional layers. “fc n nodes” denotes a fully connected layer with n nodes nodes. The pooling layers apply max pooling, downsampling both the height and width by 2. The output softmax layer has N  z  nodes, N  z  = 50 for SDSS and N  z  = 150 for LSST.
Paper: Fizzy Super-Earths: Impacts of Magma Composition on the Bulk Density and Structure of Lava Worlds
Authors: Kiersten M. Boley, Wendy R. Panero, Cayman T. Unterborn, Joseph G. Schulze, Romy Rodríguez Martínez, Ji Wang, 吉 王
Figure caption: The percent difference between the bulk density of each magma ocean planet and the solid planet with the corresponding core (i.e., light alloy core or pure iron core) at surface temperatures of (A) 1600 K and (B) 2000 K. The top axis shows radius values for Model (2). The dashed lines represent models with light-element alloys in the core, whereas solid lines show models with pure iron cores. Model (2), the anhydrous magma, is shown in purple. Model (3), the hydrous magma, is shown in teal and has the greatest decrease in density. Model (4), the carbonated magma, is shown in magenta.
Paper: Fizzy Super-Earths: Impacts of Magma Composition on the Bulk Density and Structure of Lava Worlds
Authors: Kiersten M. Boley, Wendy R. Panero, Cayman T. Unterborn, Joseph G. Schulze, Romy Rodríguez Martínez, Ji Wang, 吉 王
Figure caption: Density–Radius plot for each model that is equivalent to a planet with a surface temperature of 2000 K. We include likely lava worlds selected using criteria described in Section 3. The planets are colored by their equilibrium temperatures. Planets distinguished with white circles and planet names are discussed in detail in Sections 4.2 and 4.3. Model (4), the hydrous magma, is limited to a radius of 1.7 R ⊕, because the density of the magma becomes greater than the density of the solid in the surface magma ocean, making it dynamically unstable.
Paper: Photo-zSNthesis: Converting Type Ia Supernova Lightcurves to Redshift Estimates via Deep Learning
Authors: Helen Qu, Masao Sako
Figure caption: Examples of a low (left), medium (middle), and high (right) redshift simulated PLAsTiCC SN. (Top panel) The multi-band lightcurves are shown in colored points, with Gaussian process predictions and uncertainties for this lightcurve shown in colored lines and shaded regions, respectively. (Bottom panel) The flux matrix created from the lightcurve in the top panel (see Section 2.2.1 for details). Large flux values are colored in yellow while lower flux values are in dark blue. The physical effects of redshifting, including longer wavelengths and longer transient durations, are observed in the flux matrices in the downward (toward higher wavelengths) shift of the yellow high flux region and the increased width of the yellow region with increasing redshift.
Paper: Photo-zSNthesis: Converting Type Ia Supernova Lightcurves to Redshift Estimates via Deep Learning
Authors: Helen Qu, Masao Sako
Figure caption: True redshift distribution of the 135,521 simulated SNe Ia in the SDSS training data set (left) and the 5274 simulated SNe Ia and 489 observed photometrically confirmed SNe Ia in the SDSS test sets (right).
Paper: Photo-zSNthesis: Converting Type Ia Supernova Lightcurves to Redshift Estimates via Deep Learning
Authors: Helen Qu, Masao Sako
Figure caption: Examples of a high accuracy (Δz < 0.005, top), medium accuracy (0.01 ≤ Δz ≤ 0.05, middle), and outlier (Δz > 0.05, bottom) lightcurve and GP fit from the SDSS spectroscopic sample and their predicted PDFs. The true (spectroscopic) redshift is shown in the black dotted line, while the predicted redshift (mean(PDF)) is shown in orange. The medium and poor accuracy lightcurves have larger errors and scatter than the high accuracy lightcurve, and the low accuracy lightcurve appears to have much fewer points.
Paper: Photo-zSNthesis: Converting Type Ia Supernova Lightcurves to Redshift Estimates via Deep Learning
Authors: Helen Qu, Masao Sako
Figure caption: True redshift distribution of the 73,620 simulated SNe Ia in the LSST (PLAsTiCC) training data set (left) and 4057 simulated SNe Ia in the test data set (right).
Paper: Photo-zSNthesis: Converting Type Ia Supernova Lightcurves to Redshift Estimates via Deep Learning
Authors: Helen Qu, Masao Sako
Figure caption: Reliability diagram showing PLAsTiCC model calibration before and after temperature scaling.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Contour maps of the best-fitted perturbations obtained from the MIR flux ratios, HST positions of galaxies, VLBA positions of four jet components p, q, r, and s, and smoothing parameters that were used to fit the ALMA data. For the fitting, a Type A smooth model was used, and an additional 22 intermediate-frequency modes were adjusted with smoothing constraints. The plotted maps show the potential perturbation δ ψ, convergence perturbation δ κ, and shear perturbation δ γ reconstructed with L = 3.″6. The gray curves denote the boundaries of regions in which signals are larger than 3σ. The red “X” symbols denote the positions of lensed jet component q. The centers of the square region are (−0.4, 0.3). The coordinates are J2000 centered at the centroid of the primary lensing galaxy G.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: The best-fitted VLBA positions of four jet components in the lens plane using the MIR flux ratios, HST positions of galaxies, and smoothing parameters that were used to fit the ALMA data. For the fitting, a Type A smooth model was used, and an additional 22 intermediate-frequency modes were adjusted with smoothing constraints ﹩{R}_{s}^{2}﹩. The red symbols represent the VLBA positions of p, q, r, and s observed at 5  GHz as in Figure 14, and circles indicate their 1σ errors. The black “X” symbols represent the best-fitted positions in a model with L = 3.″6. The coordinates are J2000 centered at the centroid of the primary lensing galaxy G.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Comparison of results of visibility fitting. The left and right figures show the reduced χ 2 for models with object Y and the difference in the reduced χ 2 between models with and without object Y (Δχ 2 ≡ χ 2(with Y) − χ 2(without Y)), respectively. In each figure, the blue dashed and red lines correspond to the results fitted to the line-free and full-band visibility data, respectively.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: A pre-fitted pixelized model image (left), the rearranged model image (center), and the FFTed image before rearrangement (right). The image size and the pixel size in the sky are ﹩6\prime\prime\prime \times 6^{\prime\prime} ﹩ and 0.″005, respectively. The model images with point- and extended-source components are shown only for illustrative purposes. In our analysis, pixelized images were used only for computing visibilities of extended source components, and zero-padding around the image was used to improve the accuracy of visibilities on large angular scales.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: ALMA images of object Y. The plotted black curves are contours of intensity with 3.5σ for line subtracted images with robust = 0 (left), robust = 0.5 (middle), and a full-band image with robust = 0 (right) overlaid with the best-fit convergence perturbation δ κ obtained from the MIR flux ratios, HST positions of galaxies, VLBA positions of four jet components p, q, r, and s. The reconstruction was conducted with L = 3.″6 and the smoothing parameters that were used to fit the ALMA data.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: The amplitudes (top column) and phases (bottom column) of visibilities in the (u, v) plane for the pre-fitted model shown in Figure 23. The visibilities (right row) are given by the sum of those of the extended source components (left row) and those of the point-source components (center row).