adsabs/AstroCLIMB huggingface dataset:
Paper:  MEDEA: A New Model for Emulating Radio Antenna Beam Patterns for 21 cm Cosmology and Antenna Design Studies
Authors: Joshua J. Hibbard, Bang D. Nhan, David Rapetti, Jack O. Burns
Figure caption: Relative errors between the mean and each of the patch antenna's ∣S 11∣2 values generated by CST. Note that the differences are up to ±10−4 − 10−2, depending on the frequency.
Paper: An X-Ray Significantly Variable, Luminous, Type 2 Quasar at z = 2.99 with a Massive Host Galaxy
Authors: Xiurui Zhao, Stefano Marchesi, Marco Ajello, Francesca Civano, Roberto Gilli, Giorgio Lanzuisi, Iván E. López, Peter G. Boorman, Ross Silver, Nuria Torres-Albà, Andrealuna Pizzetti
Figure caption: Rest-frame 6 μm AGN luminosity as a function of the 2–10 keV intrinsic luminosity of J1714+6027 (red square) compared with the mid-IR-to-X-ray relation obtained by D. Lutz et al. (2004; blue dotted line), F. Fiore et al. (2009; green short-dashed line), P. Gandhi et al. (2009; purple long-dashed line), G. Lanzuisi et al. (2009; orange dashed–dotted line), and D. Stern (2015; black solid line). The extrapolations of each work to higher luminosities are plotted with dotted lines. Hot DOGs from C. Ricci et al. (2017a), R. J. Assef et al. (2016), F. Vito et al. (2018), and L. Zappacosta et al. (2018b) are plotted as gray circles.
Paper: An X-Ray Significantly Variable, Luminous, Type 2 Quasar at z = 2.99 with a Massive Host Galaxy
Authors: Xiurui Zhao, Stefano Marchesi, Marco Ajello, Francesca Civano, Roberto Gilli, Giorgio Lanzuisi, Iván E. López, Peter G. Boorman, Ross Silver, Nuria Torres-Albà, Andrealuna Pizzetti
Figure caption: SFR as a function of stellar mass of J1714+6027 (red square) and z ≥ 3.5 AGN (median redshift of 3.7) measured in E. Pouliasis et al. (2022). The dashed and dotted lines represent the SFR and stellar mass correlations of z = 3 and z = 3.7 MS star-forming galaxies derived in C. Schreiber et al. (2015), respectively.
Paper: An X-Ray Significantly Variable, Luminous, Type 2 Quasar at z = 2.99 with a Massive Host Galaxy
Authors: Xiurui Zhao, Stefano Marchesi, Marco Ajello, Francesca Civano, Roberto Gilli, Giorgio Lanzuisi, Iván E. López, Peter G. Boorman, Ross Silver, Nuria Torres-Albà, Andrealuna Pizzetti
Figure caption: Rest-frame 12 μm AGN luminosity as a function of 2–10 keV intrinsic luminosity of J1714+6027 (red square) and D. Asmus et al. (2015) measurement using a sample of obscured (22 < log(N H) < 23) AGN in the local Universe and its extrapolation to high luminosities (blue dotted line).
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: (a)–(b) 10 minute averages of near-relativistic electron intensities observed by EPD/EPT on board SolO (blue), by SEPT on board STA (red), and by Wind/3DP (green) at two different energies. (c) 10 minute averages of the relativistic electron intensities measured by EPD/HET on board SolO (blue), and COSTEP/EPHIN on board SOHO (green), together with 15 minute averages of the 2.8–4.0 MeV electron intensities measured by the HET telescope on board STA (red). The three solid green circles in panel (c) indicate three relativistic electron enhancements observed by SOHO at energies above ∼2 MeV with solar origin associated with CMEs. There are two additional relativistic electron enhancements at SOHO in mid-November 11 and early November 12 for which no CMEs were observed in association with their solar origin (indicated by open green circles). An additional small relativistic electron event at SOHO can be perceived early on November 11 (see Section 5 for details). Panel (a) includes 10 minute averages of the 15–25 keV X-ray intensities observed by STIX on board SolO (thin teal trace); see Section 3.1.
Paper: A Rapid Sequence of Solar Energetic Particle Events Associated with a Series of Extreme-ultraviolet Jets: Solar Orbiter, STEREO-A, and Near-Earth Spacecraft Observations
Authors: D. Lario, L. A. Balmaceda, R. Gómez-Herrero, G. M. Mason, V. Krupar, C. Mac Cormack, A. Kouloumvakos, I. Cernuda, H. Collier, I. G. Richardson, P. Kumar, S. Krucker, F. Carcaboso, N. Wijsen, R. D. Strauss, N. Dresing, A. Warmuth, J. Rodríguez-Pacheco, L. Rodríguez-García, I. C. Jebaraj, G. C. Ho, R. Buĉík, D. Pacheco, F. Espinosa Lara, A. Hutchinson, T. S. Horbury, L. Rodríguez, N. P. Janitzek, A. N. Zhukov, A. Aran, N. V. Nitta
Figure caption: Schematic representation of the nominal interplanetary magnetic field configuration in the solar equatorial plane as seen from the north, showing field lines connecting the Sun to the locations of Earth (green circle), Solar Orbiter (SolO; blue circle), STEREO-A (STA; red circle), and Parker Solar Probe (PSP; gray circle) on 2022 November 10 at 04:00 UT. Nominal Parker spiral magnetic field lines have been plotted using the solar wind speed indicated next to the HEEQ coordinates of each spacecraft; R being the heliocentric radial distance, Φ the HEEQ longitude and Λ the latitude. The light blue region indicates an SIR successively observed from east to west.
Paper: Statistics of Solar White-light Flares. I. Optimization and Application of Identification Methods
Authors: Yingjie Cai, Yijun Hou, Ting Li, Jifeng Liu
Figure caption: Percentage of WLFs among different GOES energy levels and two flare types (eruptive and confined). (a): Percentage of WLFs among C-class, M-class, and X-class flares, respectively. The purple histograms mark the flares that are NWLFs, and the cyan histograms mark the WLFs. (b): Percentage of WLFs among confined and eruptive C-class, M-class, and X-class flares, respectively.
Paper: Statistics of Solar White-light Flares. I. Optimization and Application of Identification Methods
Authors: Yingjie Cai, Yijun Hou, Ting Li, Jifeng Liu
Figure caption: Performance comparison between methods 1 and 5 when applied to a M1.5-class WLF. (a1): Spatial distribution of the pixels with WL emission enhancement identified by Method 1 (with a constant threshold of 5%) during the M1.5-class WLF. The appearance time of the enhancement is marked by different colors. The red contour encompasses the flare ribbon region based on the AIA 1600 Å images. (a2): Calculated WL light curve profile during the flare. The red vertical lines in panels (a2) and (b2) denote the start, peak, and end times of GOES SXR 1–8 Å. (b1)–(b2): Similar to (a1)–(a2), but for Method 5 (with a intrinsic threshold of ﹩1.5\times {\delta }_{\max 2}﹩). The blue vertical line in panel (b2) denotes the peak time of calculated WL light curve.
Paper: Statistics of Solar White-light Flares. I. Optimization and Application of Identification Methods
Authors: Yingjie Cai, Yijun Hou, Ting Li, Jifeng Liu
Figure caption: Performance comparison between methods 1 and 5 when applied to an X1.6-class WLF. (a1): Spatial distribution of the pixels with WL emission enhancement identified by Method 1 (with a constant threshold of 5%) during the X1.6-class WLF. The appearance time of the enhancement is marked by different colors. The red contour encompasses the flare ribbon region based on the AIA 1600 Å images. (a2): Calculated WL light curve profile during the flare. The red vertical lines in panels (a2) and (b2) denote the start, peak, and end times of GOES SXR 1–8 Å. (b1)–(b2): Similar to (a1)–(a2), but for Method 5 (with a intrinsic threshold of ﹩2\times {\delta }_{\max 2}﹩). The blue vertical line in panel (b2) denotes the peak time of calculated WL light curve.
Paper: Statistics of Solar White-light Flares. I. Optimization and Application of Identification Methods
Authors: Yingjie Cai, Yijun Hou, Ting Li, Jifeng Liu
Figure caption: Performance comparison between methods 1 and 5 when applied to a C5.6-class WLF. (a1): Spatial distribution of the pixels with WL emission enhancement identified by Method 1 (with a constant threshold of 5%) during the C5.6-class WLF. The appearance time of the enhancement is marked by different colors. The red contour encompasses the flare ribbon region based on the AIA 1600 Å images. (a2): Calculated WL light curve profile during the flare. The red vertical lines in panels (a2) and (b2) denote the start, peak, and end times of GOES SXR 1–8 Å. (b1)–(b2): Similar to (a1)–(a2), but for Method 5 (with a intrinsic threshold of ﹩1.5\times {\delta }_{\max 2}﹩). The blue vertical line in panel (b2) denotes the peak time of calculated WL light curve.
Paper: Statistics of Solar White-light Flares. I. Optimization and Application of Identification Methods
Authors: Yingjie Cai, Yijun Hou, Ting Li, Jifeng Liu
Figure caption: Comparison between WLF energy and duration. Points of different colors represent WLFs with different GOES energy levels, while the red and black dashed lines, respectively, show the fitting results for all WLFs and for M-class and X-class WLFs using a linear regression method.
Paper: Topological Approach to Void Finding Applied to the SDSS Galaxy Map
Authors: Manu Aggarwal, Motonari Tonegawa, Stephen Appleby, Changbom Park, Vipul Periwal
Figure caption: (A) Top panel shows two cycles a and b on the surface of a sphere. Both can be continuously deformed along the surface of the sphere to the same point. Any cycle on the surface of a sphere can contract to a point. The bottom panel shows three cycles on the surface of a 2-torus. Cycle c contracts to a point. Cycles a and b are noncontractible and cannot be deformed to each other. Any noncontractible cycle on the surface of the torus can deform to either a or b. (B) A hole dies when its triangulation gets filled in. The hole in simplicial complex K 1 dies when edge {a, c} and triangles {a, b, c} and {a, d, c} are added to it to give a new complex K 2. (C) (from M. Aggarwal et al. 2023) Vietoris–Rips filtration on a discrete set of points. The simplicial complex at a given value of τ is a collection of all simplices with diameter at most τ. Number of holes is initially 0. One hole is born at a spatial scale of τ = 2.5 when edge {a, d} is added. Another is born when {a, c} is added at τ = 2.75. Both holes get filled in, or die, at τ = 2.75 when triangles (2-simplices) are added to the simplicial complex. The first hole has persistence 2.75 − 2.5 = 0.25. The second hole dies at the same spatial scale it is born on, and so has persistence 0.
Paper: Topological Approach to Void Finding Applied to the SDSS Galaxy Map
Authors: Manu Aggarwal, Motonari Tonegawa, Stephen Appleby, Changbom Park, Vipul Periwal
Figure caption: SDSS and the 360 mocks exhibit similar morphology. (A) Cumulative probability density function (CPDF) of R eff for SDSS (red) and all mocks (turquoise). (B) p-values from Mann–Whitney U and KS significance tests comparing the distribution of R eff of voids in SDSS to the distributions of R eff of voids in the mocks. The majority are greater than 0.05 (red dashed line). (C) Minimums, medians, and maximums of distributions of effective radii of voids computed for mocks (turquoise) and SDSS (red). (D) Radial distribution functions of each void that is computed for SDSS. The average of radial distributions over all voids is shown in a bold red line plot. (E) Averages of radial distribution functions of voids computed for mocks follow a similar pattern to the average of the voids in SDSS. (F) p-values from Mann–Whitney U and KS significance tests show that the sphericities of voids is less than 1 but greater than 0.6. (G) p-values from comparing distributions of sphericities of voids in mocks to that in SDSS.
Paper: Topological Approach to Void Finding Applied to the SDSS Galaxy Map
Authors: Manu Aggarwal, Motonari Tonegawa, Stephen Appleby, Changbom Park, Vipul Periwal
Figure caption: Topology of the mocks agrees with SDSS. (A) H2 PD for SDSS DR7 computed until a threshold of 30 h −1 Mpc. Significant features are defined as those above the orange dashed line (persistence threshold of 7.5 h −1 Mpc) and to the left of the black dashed line (birth threshold of 22.5 h −1 Mpc). (B) kernel density estimation plot of significant features over all mocks. Significant features in SDSS are shown by white x markers. (C) The number of significant H2 features. (D) Distribution of numbers of computed tight H2 representatives in mocks. (E) Three views of computed tight H2 representatives in SDSS. One of the voids is highlighted in blue color.
Paper: Topological Approach to Void Finding Applied to the SDSS Galaxy Map
Authors: Manu Aggarwal, Motonari Tonegawa, Stephen Appleby, Changbom Park, Vipul Periwal
Figure caption: Characteristic distances between nearest void centers. (A) All cubic voxels that are inside voids computed for SDSS. (B) An example of cubic voxels inside one of the computed voids in SDSS. The color scheme is scaled based on the distance of voxels from the centroid of the void it is in. (C) The two-point correlation function of the void central positions. The red line represents the SDSS data, while the blue line and area indicate the mean and standard deviation from mocks. (D) Distribution of distances of the nearest void center to all void centers. The KDE of the distribution is shown in red. (E) KDE of the distributions of distances of the nearest void center to all void centers for the mocks (turquoise). The median of the KDEs for mocks is shown in blue.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: The dispersion of the orbital poles computed using subhalos with masses ≥107  M ⊙ and within 150 kpc in the five remaining Latte halos not included in the main text. The properties of the host halos and the massive satellites are summarized in Table 1. The gray-shaded regions show the distribution of the dispersion of the orbital poles of DM subhalos after downsampling to the same number of satellite galaxies. Blue vertical lines illustrate the first pericenter passage of the massive satellites. As also seen in the MW–LMC analog (m12b) in some cases the dispersion of the orbital poles in the host decreases close to the pericentric passage of the satellite.
Paper: Topological Approach to Void Finding Applied to the SDSS Galaxy Map
Authors: Manu Aggarwal, Motonari Tonegawa, Stephen Appleby, Changbom Park, Vipul Periwal
Figure caption: Comparing PH and V 2 voids. (A) PH voids in white and V 2 voids in blue. PH finds a void not found by V 2. (B) Distributions of R eff of V 2 and PH voids, categorized on the basis of whether their representative boundaries contain topologically significant features. The majority of V 2 voids do not contain topologically significant features. (C) g(r) of PH and V 2 for SDSS and mocks.
Paper: Topological Approach to Void Finding Applied to the SDSS Galaxy Map
Authors: Manu Aggarwal, Motonari Tonegawa, Stephen Appleby, Changbom Park, Vipul Periwal
Figure caption: The SDSS galaxy point distribution as a function of angular coordinates on the sky (left panel). The number density ﹩\bar{n}﹩ of the SDSS volume-limited sample as a function of comoving distance is presented in the middle panel (solid black line), along with the mean and rms values of the mocks (blue points/error bars). In the right panel, we present the fraction of the SDSS footprint as a function of its angular completeness. approximately 90% of the footprint has completeness greater than 0.95.
Paper: On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Nicolás Garavito-Camargo, Adrian M. Price-Whelan, Jenna Samuel, Emily C. Cunningham, Ekta Patel, Andrew Wetzel, Kathryn V. Johnston, Arpit Arora, Robyn E. Sanderson, Lehman Garrison, Danny Horta
Figure caption: Temporal evolution of the spherical standard distance Δsph of the k closest orbital poles of the top 11 massive satellites in the remaining halos of the Latte simulations. Smaller values of Δsph correspond to more clustered orbital poles. Dashed lines show Δsph at the pericenter passages. In halos that undergo mergers with massive satellites spread in Δsph is observed, being m12r and m12w the clearest cases. While in m12m the evolution of Δsph is minimal.
Paper: Coordinated JWST Imaging of Three Distance Indicators in a Supernova Host Galaxy and an Estimate of the Tip of the Red Giant Branch Color Dependence
Authors: Taylor J. Hoyt, In Sung Jang, Wendy L. Freedman, Barry F. Madore, Abigail J. Lee, Kayla A. Owens
Figure caption: Identification of TRGB stars in NGC 4536 from the overlap of the optical ACS/WFC and IR NIRCam fields of view. Left: optical CMD. The quadratic F814W band color dependence from I. S. Jang & M. G. Lee (2017) was adopted (red dashed curve) to rectify, or flatten, against color the TRGB feature contained within the selection of RGB stars (blue slanting lines). Overplotted are 10 Gyr BaSTI isochrones arbitrarily scaled along the vertical axis and colored (light yellow to dark purple) according to their metallicity Z = {0.002, 0.004, 0.008, Z ⊙}. Middle: the EDR (red curve) function is is computed as the Poisson-weighted first derivative of the rectified LF (gray and black curve). Tip stars are identified within a ±0.08 mag window centered on the location of the TRGB peak in the EDR. Right: the F814W-identified TRGB stars are highlighted in the JWST/NIRCAM CMD. Overplotted again are 10 Gyr BaSTI isochrones, this time as predicted for the JWST NIR filters in this study. A set of representative error bars for the TRGB stars is plotted (orange cross with caps). A single random offset between −0.2 and 0.2 mag has been applied to both of the F115W and F444W magnitudes.
Paper: Coordinated JWST Imaging of Three Distance Indicators in a Supernova Host Galaxy and an Estimate of the Tip of the Red Giant Branch Color Dependence
Authors: Taylor J. Hoyt, In Sung Jang, Wendy L. Freedman, Barry F. Madore, Abigail J. Lee, Kayla A. Owens
Figure caption: Fits to the TRGB’s magnitude–color relation in the F115W and F444W bandpasses. Left: F115W magnitudes vs. (F115W – F444W) colors for tip stars (blue circles) previously shown as orange circles in Figure 6, now plotted with their photometric errors (blue lines). Note that most of the scatter about the trend lines is due to color uncertainties from the F444W magnitudes. Right: same as left panel, with four equal-number bins (sorted by color) representing the TRGB magnitudes and colors (black dots). The error bars represent the standard deviation of each quantity’s distribution within each bin. Two of the fitted lines are plotted along with their 90% confidence interval (CI) bands determined via bootstrapping: the result from ordinary least squares (blue dotted–dashed–dotted line and band) and ODR (red solid line and band). The fits were performed on the unbinned data points (left), not the binned points (right). In both panels, BaSTI 10 Gyr isochrones are again plotted on a viridis color map, this time over a metallicity range expanded to include more metal-poor isochrones, Z = {0.0002, 0.0004, 0.0008, 0.0014, 0.0039, 0.008, 0.017} or [Fe/H] = {–1.90, –1.55, –1.30, –1.05, –0.60, –0.30, +0.06}.
Paper: Coordinated JWST Imaging of Three Distance Indicators in a Supernova Host Galaxy and an Estimate of the Tip of the Red Giant Branch Color Dependence
Authors: Taylor J. Hoyt, In Sung Jang, Wendy L. Freedman, Barry F. Madore, Abigail J. Lee, Kayla A. Owens
Figure caption: Demonstration of TRGB rectification in the full JWST halo data set and subsequent sharpened measurement of the IR TRGB in JWST filters. Left: F115W vs. F444W CMD. The color–magnitude selection used to select along the RGB is shown (blue lines) with RGB sources (solid black points) plotted along with non-RGB sources (transparent black points). The locations of two equally likely peaks in the resulting EDR (red dashed curves in the right-most panel) are marked (transparent, horizontal dashed lines). Middle: T 115 vs. F444W CMD, wherein the stars that fall inside the unrectified RGB selection (solid black if RGB, transparent gray if not) are rotated via a separate derivation of the TRGB’s color slope (adopted here as −0.99 mag mag−1), such as that determined in the previous section. The resulting EDR is singly peaked, demonstrating the success of the TRGB slope in improving the clarity of the TRGB. The location of the peak magnitude is marked on the rectified CMD (horizontal black line). Right: unrectified RGB LF are computed for bins of size 0.01 mag (gray curve) and smoothed with Gaussian kernel of width 0.08 mag (black curve). Plotted also are the EDRs derived from both the unrectified (red, transparent, dashed curve) and the rectified (solid red curve) RGB magnitudes. Both EDRs have been normalized to the same peak value and scaled to the maximum value of the RGB LF. The locations of the two strong peaks in the unrectified EDR are marked (red, horizontal, dashed lines) along with the single dominant peak in the rectified EDR (red, horizontal, solid line).
Paper: Coordinated JWST Imaging of Three Distance Indicators in a Supernova Host Galaxy and an Estimate of the Tip of the Red Giant Branch Color Dependence
Authors: Taylor J. Hoyt, In Sung Jang, Wendy L. Freedman, Barry F. Madore, Abigail J. Lee, Kayla A. Owens
Figure caption: EDR curves computed from RGB LFs that were derived from rectified T magnitudes over a range of TRGB slopes used for the rectification. Seven representative EDRs are shown to demonstrate the behavior of vertical edge features in the rotated and color-marginalized CMD as a function of the slope used to perform said rotation. Plotted are the left and right edges of the uncorrected (slope = 0) TRGB peak as well as those belonging to the peak resulting from the ODR slope determined in the previous section (vertical dashed lines, colored to match the associated EDR curve and slope value). The threshold adopted for defining the edges of peak features is also plotted (horizontal black dashed line). For reference, the kernel used to smooth the RGB LF is shown with arbitrary height (black curve, top right).
Paper: Coordinated JWST Imaging of Three Distance Indicators in a Supernova Host Galaxy and an Estimate of the Tip of the Red Giant Branch Color Dependence
Authors: Taylor J. Hoyt, In Sung Jang, Wendy L. Freedman, Barry F. Madore, Abigail J. Lee, Kayla A. Owens
Figure caption: Delta in TRGB distance as a function of adopted TRGB slope for four fiducial calibrations. The thick, black curve represents rotation of the CMD about the mean color of the observed TRGB. The thinner, colored curves represent different pivot colors. The distance shifts Δμ are computed relative to the median of the black curve within the “good slope range” (vertical lines), determined from the top panel. The red, boxed region encloses the suite of curves contained by the standard error interval of the ODR results from the optical–IR trace method.
Paper: Coordinated JWST Imaging of Three Distance Indicators in a Supernova Host Galaxy and an Estimate of the Tip of the Red Giant Branch Color Dependence
Authors: Taylor J. Hoyt, In Sung Jang, Wendy L. Freedman, Barry F. Madore, Abigail J. Lee, Kayla A. Owens
Figure caption: 68% width of the TRGB peak feature as a function of the slope that was used to flatten the TRGB feature on the CMD (rectification). One hundred linearly spaced steps in TRGB slope values ranging from −2.2 to 0.0 were considered. The width of the smoothing kernel is plotted for reference (horizontal black dashed line). Note both the x-axis and the color map are aligned to the TRGB slope axis. The redundancy is meant to aid in comparison with the representative EDRs plotted in Figure 9.