adsabs/AstroCLIMB huggingface dataset:
Paper: Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS
Authors: Wei Liu, Shengbang Qian
Figure caption: The two figures correspond to two superoutbursts of V1504 Cyg. The top panels in each figure show the light curves of the superoutbursts, where the red lines show the trend of the superoutbursts. Middle: the detrended light curves. Bottom: O − C curves of the superhumps. The ephemerides of the superhumps for each superoutburst are marked in each figure. The blue dashed lines represent the temporal dividing line among stages A, B, and C. Stage C of the superoutburst in panel (a) was not well observed by TESS.
Paper: Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS
Authors: Wei Liu, Shengbang Qian
Figure caption: The two figures correspond to two superoutbursts of DT Oct. The top panels in each figure show the light curves of the superoutbursts, where the red lines show the trend of the superoutbursts. Middle: the detrended light curves. Bottom: O − C curves of the superhumps. The ephemerides of the superhumps for each superoutburst are marked in each figure. The blue dashed lines represent the temporal dividing line among stages A, B, and C.
Paper: Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS
Authors: Wei Liu, Shengbang Qian
Figure caption: Top: the superoutburst light curves of SS UMi, where the red line presents the trend of the superoutburst. Middle: the detrended light curves. Bottom: O − C diagram of SS UMi during the BJD 2,458,768–2,458,781 superoutburst. The ephemeris of ﹩{T}_{\max }={BJD}2459721.41611+0.070253E﹩ was used for drawing this O − C diagram. The blue dashed lines represent the temporal dividing line among stages A, B, and C.
Paper: Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS
Authors: Wei Liu, Shengbang Qian
Figure caption: The four figures correspond to four superoutbursts of IX Dra. The top panel in each figure is the light curve of the superoutburst, where the red lines show the trend of the superoutburst. Middle: the detrended light curves. Bottom: O − C curves of the superhumps. The ephemerides of the superhumps for each superoutburst are marked in each figure. The blue dashed lines represent the temporal dividing line among stages A, B, and C.
Paper: Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS
Authors: Wei Liu, Shengbang Qian
Figure caption: Top: the superoutburst light curves of TY Psc, where the red line shows the trend of the superoutburst. Middle: the detrended light curves. Bottom: O − C diagram of TY Psc during the BJD 2,458,768–2,458,781 superoutburst. The ephemeris of ﹩{T}_{\max }={BJD}2458769.5520261+0.070756E﹩ was used for drawing this O − C diagram. The blue dashed line represents the temporal dividing line between stage A and B.
Paper: Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS
Authors: Wei Liu, Shengbang Qian
Figure caption: Top: light curves of the superoutburst of V503 Cyg, where the red line shows the trend of the superoutburst. Middle: the detrended light curves. Bottom: O − C diagram of V503 Cyg during the BJD 2,459,069–2,459,086 superoutburst. The ephemeris of ﹩{T}_{\max }={BJD}2458726.9966571+0.081477E﹩ was used to draw this O − C diagram. The two blue dashed lines represent the temporal dividing line among stages A, B, and C.
Paper: Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS
Authors: Wei Liu, Shengbang Qian
Figure caption: The two figures correspond to two superoutbursts of J1730+6247. The top panels in each figure show the light curves of the superoutbursts, where the red lines show the trend of the superoutbursts. Middle: the detrended light curves. Bottom: O − C curves of the superhumps. The ephemerides of the superhumps for each superoutburst are marked in each figure. The blue dashed lines represent the temporal dividing line among stages A, B, and C.
Paper: Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS
Authors: Wei Liu, Shengbang Qian
Figure caption: Mass ratio–orbital period relation of CVs. The blue points are from the literature (Kato 2022). The red dots are obtained by this work. The black dashed line shows the standard model for CV evolution. The red solid line shows the evolution of donor properties along the revised model track (Knigge et al. 2011).
Paper: Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS
Authors: Wei Liu, Shengbang Qian
Figure caption: The distribution of precession periods with orbital periods.
Paper: Beyond BPT: A New Multidimensional Diagnostic Diagram for Classifying Power Sources Tested Using the SAMI Galaxy Survey
Authors: Victor D. Johnston, Anne M. Medling, Brent Groves, Lisa J. Kewley, Luca Cortese, Scott Croom, Ángel R. López-Sánchez, Henry Zovaro, Joss Bland-Hawthorn, Julia Bryant, Jon Lawrence, Matt Owers, Samuel Richards, Jesse van de Sande
Figure caption: Emission-line diagnostics and maps for GAMA 106717. The first row are the BPT/VO87 diagrams colored according to our new diagnostic: black points are spaxels dominated by star formation and colored points are spaxels with shock ionization colored by increasing radius from the center of the galaxy. The middle row contains plots of log([N II]/Hα), log([O III]/Hβ), and effective radius vs. velocity dispersion. The separation between shocked and star-forming gas can be easily seen in the middle and right panels in this row. The last row contains a histogram of the velocity dispersion with a vertical line separating the groups of gas with low and high velocity dispersion, a map of the velocity dispersion, a map of shock fraction, which shows the relative contribution of shocks on a per-spaxel basis, and a three-color image on the right matching the FOV of the SAMI data.
Paper: Beyond BPT: A New Multidimensional Diagnostic Diagram for Classifying Power Sources Tested Using the SAMI Galaxy Survey
Authors: Victor D. Johnston, Anne M. Medling, Brent Groves, Lisa J. Kewley, Luca Cortese, Scott Croom, Ángel R. López-Sánchez, Henry Zovaro, Joss Bland-Hawthorn, Julia Bryant, Jon Lawrence, Matt Owers, Samuel Richards, Jesse van de Sande
Figure caption: Emission-line diagnostics and maps for GAMA 298666, a galaxy containing diffuse ionized gas. Each panel in the first row shows the emission-line diagnostics colored according to where each spaxel falls in its respective diagram: green for star-forming, blue for composite or LINER, and red for AGN. Below each diagnostic is the corresponding spatial map showing where in the galaxy the points in the diagram above are located. The middle row contains plots of log([N II]/Hα), log([O III]/Hβ), and effective radius vs. velocity dispersion. As our method classifies all of the spaxels as being dominated by star formation, all of the points here are labeled black. The last row contains a histogram of the velocity dispersion with a vertical line denoting the two components in velocity dispersion space, a map of the velocity dispersion in the middle, a spatial map showing that there is no ionization contribution from non-star-forming sources, and a three-color image on the right matching the FOV of the SAMI data.
Paper: Beyond BPT: A New Multidimensional Diagnostic Diagram for Classifying Power Sources Tested Using the SAMI Galaxy Survey
Authors: Victor D. Johnston, Anne M. Medling, Brent Groves, Lisa J. Kewley, Luca Cortese, Scott Croom, Ángel R. López-Sánchez, Henry Zovaro, Joss Bland-Hawthorn, Julia Bryant, Jon Lawrence, Matt Owers, Samuel Richards, Jesse van de Sande
Figure caption: Emission-line diagnostics and maps for GAMA 9388000338, a galaxy containing elevated velocity dispersion, low emission-line spaxels. Each figure in the first row shows the emission-line diagnostics colored according to where each spaxel falls in its respective diagram: green for star-forming, blue for composite or LINER, and red for AGN. Below each diagnostic is the corresponding spatial map showing where in the galaxy the points in the diagram above are located. The middle row contains plots of log([N II]/Hα), log([O III]/Hβ), and effective radius vs. velocity dispersion with points being colored black if they lie below the velocity dispersion cutoff, and colored by increasing radius if they lie above it. The last row contains a histogram of the velocity dispersion with a vertical line denoting the two components in velocity dispersion space, a map of the velocity dispersion in the middle, a map of the ionization fraction tracing the elevated velocity dispersion from lowest to highest values, and a three-color image on the right matching the FOV of the SAMI data.
Paper: Beyond BPT: A New Multidimensional Diagnostic Diagram for Classifying Power Sources Tested Using the SAMI Galaxy Survey
Authors: Victor D. Johnston, Anne M. Medling, Brent Groves, Lisa J. Kewley, Luca Cortese, Scott Croom, Ángel R. López-Sánchez, Henry Zovaro, Joss Bland-Hawthorn, Julia Bryant, Jon Lawrence, Matt Owers, Samuel Richards, Jesse van de Sande
Figure caption: Emission-line diagnostics and maps for GAMA 376478. The first row are the BPT/VO87 diagrams colored according to our new diagnostic: black points are spaxels dominated by star formation and colored points are spaxels with AGN ionization colored by increasing radius from the center of the galaxy. The middle row contains plots of log([N II]/Hα), log([O III]/Hβ), and effective radius vs. velocity dispersion. The last row contains a histogram of the velocity dispersion with a vertical line denoting the two components in velocity dispersion space, a map of the velocity dispersion, a map of the AGN fraction, which shows the relative contribution of AGN ionization on a per-spaxel basis, and a three-color image on the right matching the FOV of the SAMI data.
Paper: Beyond BPT: A New Multidimensional Diagnostic Diagram for Classifying Power Sources Tested Using the SAMI Galaxy Survey
Authors: Victor D. Johnston, Anne M. Medling, Brent Groves, Lisa J. Kewley, Luca Cortese, Scott Croom, Ángel R. López-Sánchez, Henry Zovaro, Joss Bland-Hawthorn, Julia Bryant, Jon Lawrence, Matt Owers, Samuel Richards, Jesse van de Sande
Figure caption: GAMA 273514, which contains AGN-like ionization. The top row shows BPT/VO87 emission-line diagrams and the bottom row presents spatial maps colored according to the diagnostic directly above it. There is no clear pattern in any of the spatial maps that suggests true ionization from a central AGN, despite the emission-line diagnostics having a large number of AGN-like spaxels.
Paper: Beyond BPT: A New Multidimensional Diagnostic Diagram for Classifying Power Sources Tested Using the SAMI Galaxy Survey
Authors: Victor D. Johnston, Anne M. Medling, Brent Groves, Lisa J. Kewley, Luca Cortese, Scott Croom, Ángel R. López-Sánchez, Henry Zovaro, Joss Bland-Hawthorn, Julia Bryant, Jon Lawrence, Matt Owers, Samuel Richards, Jesse van de Sande
Figure caption: Emission-line diagnostics and spatial maps for GAMA 376478. Each figure in the first row shows the emission-line diagnostics colored according to where each spaxel falls in its respective diagram: green for star-forming, blue for composite or LINER, and red for AGN. Below each diagnostic is the corresponding spatial map showing where in the galaxy the points in the diagram above are located.
Paper: Beyond BPT: A New Multidimensional Diagnostic Diagram for Classifying Power Sources Tested Using the SAMI Galaxy Survey
Authors: Victor D. Johnston, Anne M. Medling, Brent Groves, Lisa J. Kewley, Luca Cortese, Scott Croom, Ángel R. López-Sánchez, Henry Zovaro, Joss Bland-Hawthorn, Julia Bryant, Jon Lawrence, Matt Owers, Samuel Richards, Jesse van de Sande
Figure caption: A histogram of the distribution of EWHα  for AGN-like spaxels. The red vertical line shows the 3 Å separation used to distinguish between HOLMES and true AGN ionization.
Paper: Beyond BPT: A New Multidimensional Diagnostic Diagram for Classifying Power Sources Tested Using the SAMI Galaxy Survey
Authors: Victor D. Johnston, Anne M. Medling, Brent Groves, Lisa J. Kewley, Luca Cortese, Scott Croom, Ángel R. López-Sánchez, Henry Zovaro, Joss Bland-Hawthorn, Julia Bryant, Jon Lawrence, Matt Owers, Samuel Richards, Jesse van de Sande
Figure caption: Histograms showing the distribution of galaxy mass and morphological type for galaxies identified as hosting AGNs and AGN-like ionization.
Paper: Beyond BPT: A New Multidimensional Diagnostic Diagram for Classifying Power Sources Tested Using the SAMI Galaxy Survey
Authors: Victor D. Johnston, Anne M. Medling, Brent Groves, Lisa J. Kewley, Luca Cortese, Scott Croom, Ángel R. López-Sánchez, Henry Zovaro, Joss Bland-Hawthorn, Julia Bryant, Jon Lawrence, Matt Owers, Samuel Richards, Jesse van de Sande
Figure caption: A comparison of ionization sources detected using just the BPT/VO87 diagrams (left) and our new method using emission-line ratios, kinematics, and spatial information (right). Our 3D classification method is more sensitive at detecting ionization from non-star-forming sources than just emission-line diagnostics alone.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The age–metallicity relation across the Milky Way disk. Panels represent different spatial zones, laid out in the same way as Figure 8, with rows corresponding to Z and columns increasing in R. The number in the top-right corner of each panel is the number of stars in our sample in that spatial bin. The age and metallicity for individual stars are plotted, colored by [Mg/Fe] abundance. The running median trend is plotted in black square points to guide the eye, with the vertical bars indicating the standard deviation in [Fe/H] for bins in log(age). The typical (median) uncertainty for any given point is shown in the top-right corner of each panel.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The metallicity distribution function (MDF) of the Milky Way disk, split into different height bins (panels), from closest to the Galactic plane (top) to the farthest beyond (bottom). Each panel shows the fraction of stars at each metallicity [Fe/H] as a function of Galactocentric radius, further split by color between high-α (red) and low-α (blue) samples. Every third row is annotated with markings for the peak (or mode) of the distribution (white diamond), as well as the 25th, 50th (median), and 75th percentiles (white tick marks) to highlight the shape of the distribution.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The age–α relation across the Milky Way disk. Panels represent different spatial zones, laid out in the same way as Figure 8. The contours represent the density of points on the diagram. The gray background shape outlines the 90% contour for the entire sample, and is the same in all panels for reference. The typical (median) uncertainty for any given point is shown in the top-right corner of each panel.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The MDF and its first three moments, limited to the low-α sample and close to the Galactic plane (∣Z∣ < 0.5 kpc; equivalent to the top panel in Figure 18). Left panel: the MDF at different radii in the Galaxy (colored lines). The right panels show the first three statistical moments for quantifying this distribution as a function of radius. Top right: a characteristic [Fe/H] for each distribution function, measured as a median (blue line), a mean (green line), and the peak (or mode; purple line). Middle right: the width, σ, of the distribution. Bottom right: the skewness of the distribution, where a negative number indicates a left-leaning distribution as shown in the left panel, and a positive number corresponds to a right-leaning distribution. The solar position (R = 8.3 kpc) is marked by a vertical gray line in all right panels.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The radial distribution of the low-α (solid lines) and high-α (dashed lines) populations shown as the contour containing 75% of all points for different bins in stellar age (line color) all at fixed −0.1 ≤ [Fe/H] ≤0.1. The center of each contour is marked as a point. The typical (median) uncertainty [Mg/Fe] is plotted in the bottom-left corner.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The age distribution function (ADF) of the Milky Way disk, split into different height bins (panels), from closest to the Galactic plane (top) to farthest beyond (bottom). Each panel shows the fraction of stars at each age as a function of Galactocentric radius, further split by color between high-α (red) and low-α (blue) samples. Every third row is annotated with markings for the peak (or mode) of the distribution (white diamond), as well as the 25th, 50th (median), and 75th percentiles (white tick marks) to highlight the shape of the distribution.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: Radial median age profile as a function of height above the plane (line color), for the total stellar population (top panel), the low-α disk (middle panel), and the high-α disk (bottom panel).
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: The best-fit slope for each radial age profile in Figure 20 in units of Gyr kpc−1, fit with a single line for stars beyond R > 7 kpc for the total sample (black line), and the low-α (blue line) and high-α (red line) samples independently. The shaded region indicates the ±1σ uncertainty in the slope measurement.
Paper: A Tale of Two Disks: Mapping the Milky Way with the Final Data Release of APOGEE
Authors: Julie Imig, Cathryn Price, Jon A. Holtzman, Alexander Stone-Martinez, Steven R. Majewski, David H. Weinberg, Jennifer A. Johnson, Carlos Allende Prieto, Rachael L. Beaton, Timothy C. Beers, Dmitry Bizyaev, Michael R. Blanton, Joel R. Brownstein, Katia Cunha, José G. Fernández-Trincado, Diane K. Feuillet, Sten Hasselquist, Christian R. Hayes, Henrik Jönsson, Richard R. Lane, Jianhui Lian, Szabolcs Mészáros, David L. Nidever, Annie C. Robin, Matthew Shetrone, Verne Smith, John C. Wilson
Figure caption: Same as Figure 23, but showing the contours of point density in each panel.
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 and middle left panels show the simulated frequency down-drifting data at ΔDM = 0. The top left panel shows the mean intensity over frequency of the noisy data (solid line) and the Gaussian envelope (dashed line) vs. time. The middle left panel is the frequency-time representation (dynamic spectrum) of the simulated data. The bottom left panel shows intensities vs. time and ΔDM of simulated frequency down-drifting data before filtering. The top right panel shows the DCT spectrum of the simulated noisy signal. The middle right panel reports the structure parameters of the recovered signal and the known structure parameter computed by applying time shifting based on the group delay to the envelope of the known 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.