adsabs/AstroCLIMB huggingface dataset:
Paper: The Hubble Space Telescope Survey of M31 Satellite Galaxies. II. The Star Formation Histories of Ultrafaint Dwarf Galaxies
Authors: Alessandro Savino, Daniel R. Weisz, Evan D. Skillman, Andrew Dolphin, Andrew A. Cole, Nitya Kallivayalil, Andrew Wetzel, Jay Anderson, Gurtina Besla, Michael Boylan-Kolchin, Thomas M. Brown, James S. Bullock, Michelle L. M. Collins, M. C. Cooper, Alis J. Deason, Aaron L. Dotter, Mark Fardal, Annette M. N. Ferguson, Tobias K. Fritz, Marla C. Geha, Karoline M. Gilbert, Puragra Guhathakurta, Rodrigo Ibata, Michael J. Irwin, Myoungwon Jeon, Evan N. Kirby, Geraint F. Lewis, Dougal Mackey, Steven R. Majewski, Nicolas Martin, Alan McConnachie, Ekta Patel, R. Michael Rich, Joshua D. Simon, Sangmo Tony Sohn, Erik J. Tollerud, Roeland P. van der Marel
Figure caption: HST/ACS F606W vs. (F606W-F814W) CMDs for the six UFDs analyzed in this paper. CMDs are for the central 2 half-light radii. The red dashed line marks the 50% completeness level as determined from artificial star tests. Select BaSTI isochrones of different ages and metallicities are overplotted for reference. Note the diversity of horizontal branch morphologies, which suggest a diversity of stellar populations, as previously found by Martin et al. (2017). We do not include the HBs in our SFH determinations and instead use them as a sanity check on our results.
Paper: On the Effectiveness of the Planetary Infrared Excess (PIE) Technique to Retrieve the Parameters of Multiplanet Systems around M Dwarfs: A Case Study on the TRAPPIST-1 System
Authors: L. C. Mayorga, J. Lustig-Yaeger, K. B. Stevenson
Figure caption: The 1D posteriors and priors (from Gillon et al. 2017) for the three noise renditions with simulated JWST data (left: 5 ppm, middle: 10 ppm, right: 100 ppm). The posteriors for each planet (top row: planet b) are given in different colors. Each column is a different fit parameter with the post-processed equilibrium temperature shown on the rightmost column of each noise rendition. The priors are shown in gray with the “true” value (from Agol et al. 2021) shown as a black solid line and the median of the posterior shown as a colored dashed line.
Paper: On the Effectiveness of the Planetary Infrared Excess (PIE) Technique to Retrieve the Parameters of Multiplanet Systems around M Dwarfs: A Case Study on the TRAPPIST-1 System
Authors: L. C. Mayorga, J. Lustig-Yaeger, K. B. Stevenson
Figure caption: The planetary fluxes of the true system in the noisy JWST/MIRI-LRS scenarios (left: 5 ppm, middle: 10 ppm, right: 100 ppm). Top: the flux from the planets. Bottom: the residuals when fitting a star-only model compared to the corresponding noise floor (orange shaded region) for each scenario.
Paper: On the Effectiveness of the Planetary Infrared Excess (PIE) Technique to Retrieve the Parameters of Multiplanet Systems around M Dwarfs: A Case Study on the TRAPPIST-1 System
Authors: L. C. Mayorga, J. Lustig-Yaeger, K. B. Stevenson
Figure caption: Same as Figure 6 but for the radii of the included planets for the best-fit models throughout our historical analysis. Unlike the prior reliant semimajor axes, radius can shift from the priors to compensate for A and a.
Paper: On the Effectiveness of the Planetary Infrared Excess (PIE) Technique to Retrieve the Parameters of Multiplanet Systems around M Dwarfs: A Case Study on the TRAPPIST-1 System
Authors: L. C. Mayorga, J. Lustig-Yaeger, K. B. Stevenson
Figure caption: Same as Figure 3 but with 5 ppm noise (left), 10 ppm noise (middle), and 100 ppm noise (right) with JWST/MIRI-LRS observations. Since we do not allow for semimajor axes beyond our 0.041 au upper limit, planets g and h are not represented in any of our best-fit solutions.
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: Left: f F444W/f F150W vs. f F444W for the JWST NIRCam sources that lie in the area covered by the ALMA data (black dots). The red lines delineate our red galaxy selection region (f F444W >1 μJy and f F444W/f F150W > 3.5). All nine >4.5σ ALMA sources satisfy these criteria (red squares). Right: f F444W/f F150W vs. f F444W/f F115W for sources with f F444W >1 μJy that lie in the area covered by the ALMA data (black dots). The nine >4.5σ ALMA sources are again shown with red squares. The red vertical line shows our f F444W/f F150W > 3.5 selection, while the red horizontal line shows an alternate f F444W/f F115W > 6 selection. The solid portions of the lines delineate a selection region that uses both criteria, but the improvement is marginal.
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 nine >4.5σ ALMA sources in the A2744 field. The thumbnails are 12″ on a side, or ∼100 kpc at z = 2. The ALMA continuum emission is shown with white contours. The redshifts (discussed in Section 2) are marked as either spectroscopic (specz) or photometric (photz).
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 SCUBA-2 850 μm sources (white contours: 1, 2, and 4 mJy per beam; diamonds: local peaks) and their assigned counterparts. Top: a red galaxy with an ALMA counterpart (ALMA3; large red square) lying between two SCUBA-2 sources that are well separated; this source has been assigned as the counterpart to both SCUBA-2 sources. Bottom: a red galaxy with no ALMA counterpart. The underlying images are three-color JWST NIRCam (blue = F115W, green = F150W, and red = F444W), centered on the assigned red galaxy counterpart (green squares). The redshifts are marked as either spectroscopic (specz) or photometric (photz). The pixels are 0.″03, and the fields are 12″ 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: SCUBA-2 850 μm image of the massive lensing cluster field A2744 from Cowie et al. (2022). The footprints of the JWST NIRCam F444W image released by Paris et al. (2023; red) and the combined ALMA mosaics from AFFS and ALCS (green) are overlaid. The imaging and catalog from Weaver et al. (2023) do not cover a small portion of the lower-left corner of the NIRCAM footprint shown.
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 >5σ SCUBA-2 sources with accurate NIRCam positions. The five SCUBA-2 sources with already known accurate positions from ALMA (see Figure 2 and Table 2) are not shown. The thumbnails are 12″ on a side, or roughly 100 kpc at z = 2. The thumbnails are labeled with the photometric redshifts from Weaver et al. (2023).
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 with uncertainties (16th and 84th percentiles of the posterior) vs. either spectroscopic redshift (five sources; orange circles) or photometric redshift (15 sources; red diamonds).
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: Distribution of the measured 850 μm flux for the 156 red galaxy priors (black histogram) and for the full F444W >0.05 μJy sample (red dashed histogram. The latter excludes the priors and is renormalized to match the peak of the priors histogram.
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: Left: deep portion of the SCUBA-2 850 μm image in the JWST NIRCam footprint. Right: SCUBA-2 850 μm image after removing the 850 μm fluxes corresponding to the red galaxy priors.
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 spatial distribution of all the RACS sources that have an ATNF pulsar within 10″. The sky positions (in Mollweide projection) of all the ATNF pulsars are shown as gray dots, the RACS Stokes I pulsar detections are shown as orange diamonds, and the simultaneous RACS Stokes I and Stokes V detections are shown as blue stars. The black dashed line shows the decl. limit, +41°, for RACS DR1. The Galactic plane within ∣b∣ < 5° is shown by the green shaded region.
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 the spatial offset between the ATNF catalog positions and the RACS positions for the pulsar crossmatches. The blue histogram shows the distribution for the RACS Stokes I crossmatches and the black histogram shows the same for the RACS Stokes V sources.
Paper: Regulation of Proton–α Differential Flow by Compressive Fluctuations and Ion-scale Instabilities in the Solar Wind
Authors: Xingyu Zhu, Daniel Verscharen, Jiansen He, Bennett A. Maruca, Christopher J. Owen
Figure caption: Illustration of the fluctuating-beam effect. We assume the velocity distribution functions of protons (red half-circles) and α-particles (blue half-circles) are initially Maxwellian with the same thermal speed. The initial and instantaneous bulk velocities of each component are represented by black dots. We work in the reference frame of the proton bulk velocity but note that this is not an inertial frame when a slow-mode-like compression is present. (a) Case without slow-mode-like compressions (δ B ∥ = 0). Both U pα  and U th remain constant, i.e., U pα  = U pα0 and U th = U th0. (b) Case with slow-mode-like compressions with an amplitude 0 < δ B ∥ < δ B ∥,crit. This configuration is still stable throughout all phases of the large-scale compression since U pα  < U th at all times. (c) Case with slow-mode-like compressions with an amplitude δ B ∥ > δ B ∥,crit. In this case, U pα  crosses the instability threshold U th at least one time during the evolution of the large-scale compression. ΔU pα , ΔU th, ΔP p, and ΔP  α  represent the variations of the corresponding quantities, where P  j  indicates the scalar pressure of species j.
Paper: The Role of Mass and Environment on Satellite Distributions around Milky Way Analogs in the ROMULUS25 Simulation
Authors: Jordan Van Nest, Ferah Munshi, Charlotte Christensen, Alyson M. Brooks, Michael Tremmel, Thomas R. Quinn
Figure caption: Normalized histograms of (a) hosts in K-band magnitude and (b) satellites in V-band magnitude for our M * with simulated R vir sample. We make direct comparisons to SAGA II (Mao et al. 2021) and ELVES (Carlsten et al. 2022) data, with the Milky Way and M31 values taken from the latter. The ELVES satellites are weighted according to their likelihood measurements. For a fair comparison, the satellite distributions in (b) are all normalized to the samples’ number of satellites brighter than M  V  = −14, the approximate completeness limit for ROMULUS25.
Paper: The Role of Mass and Environment on Satellite Distributions around Milky Way Analogs in the ROMULUS25 Simulation
Authors: Jordan Van Nest, Ferah Munshi, Charlotte Christensen, Alyson M. Brooks, Michael Tremmel, Thomas R. Quinn
Figure caption: The average number of satellites hosted by Milky Way analogs as a function of stellar mass and environment (distance to a Milky Way–sized or larger halo). The text in each box indicates the number of Milky Way analogs in that parameter space, as well as the standard deviation among the number of satellites. The left plot shows the M vir with simulated R vir sample, while the right plot shows the sample most analogous to the SAGA Survey. In both cases, the number of satellites appears to increase as stellar mass increases.
Paper: The Role of Mass and Environment on Satellite Distributions around Milky Way Analogs in the ROMULUS25 Simulation
Authors: Jordan Van Nest, Ferah Munshi, Charlotte Christensen, Alyson M. Brooks, Michael Tremmel, Thomas R. Quinn
Figure caption: The V-band satellite luminosity function for our Milky Way analog sample under the M * with simulated R vir criteria. The black line and dark gray region represent the mean and single standard deviation of our sample, respectively, while the outer light gray region encompasses our entire sample. We compare to the Milky Way and M31 (Geha et al. 2017), M94 (Smercina et al. 2018), M101 (Bennet et al. 2019), and NGC 4258 and NGC 4631 (Carlsten et al. 2021b). The dotted vertical line marks the approximate completeness limit for ROMULUS25. Our sample is in good agreement with these observations.
Paper: The Role of Mass and Environment on Satellite Distributions around Milky Way Analogs in the ROMULUS25 Simulation
Authors: Jordan Van Nest, Ferah Munshi, Charlotte Christensen, Alyson M. Brooks, Michael Tremmel, Thomas R. Quinn
Figure caption: Virial and stellar masses plotted against K-band magnitudes for three of our Milky Way analog samples. The dotted lines denote the mass and magnitude cuts used in our samples. The samples diverge at the different boundaries, and even within the boundaries there are analogs that exist in some definitions but not others.
Paper: Can Cosmologically Coupled Mass Growth of Black Holes Solve the Mass Gap Problem?
Authors: Shi-Jie Gao, Xiang-Dong Li
Figure caption: Similar to Figure 3 but the donor mass–orbital period (M 2–P orb) distributions.
Paper: Constraining Nuclear Parameters Using Gravitational Waves from f-mode Oscillations in Neutron Stars
Authors: Bikram Keshari Pradhan, Dhruv Pathak, Debarati Chatterjee
Figure caption: We plot 90% symmetric SCI of (a) the pressure as a function of energy density, (b) the radius as a function of mass, (c) the squared speed of sound as a function of density, and (d) pressure as a function of density, reconstructed using the posteriors of nuclear parameters corresponding to the single f-mode event displayed in Figure 3. To avoid clutter, we show both the 68% (bounded by dashed lines) and 90% (bounded by solid lines) SCIs only for M–R relations.
Paper: Constraining Nuclear Parameters Using Gravitational Waves from f-mode Oscillations in Neutron Stars
Authors: Bikram Keshari Pradhan, Dhruv Pathak, Debarati Chatterjee
Figure caption: Similar to Figure 4 but with consideration of ten random events with S/N ≥ 8 in A+ (blue band) and ET (red band) corresponding to glitches of Vela pulsar. We have also displayed the uncertainties resulting from ten random events in ET, excluding the glitches from Vela pulsar (cyan band).
Paper: Constraining Nuclear Parameters Using Gravitational Waves from f-mode Oscillations in Neutron Stars
Authors: Bikram Keshari Pradhan, Dhruv Pathak, Debarati Chatterjee
Figure caption: (a) The posterior distribution of ﹩{R}_{1.4{M}_{\odot }}﹩, ﹩{f}_{1.4{M}_{\odot }}﹩, and ﹩{\tau }_{1.4{M}_{\odot }}﹩ resulting from the detection of a single event in A+ (blue) and ET (red). (b) Similar to Figure 5(a) but with consideration of 10 random events resulting from Vela with S/N ≥ 8 in A+ (blue) and ET (red) and the posterior resulting from consideration of 10 random events in ET with pulsars other than Vela.
Paper: Constraining Nuclear Parameters Using Gravitational Waves from f-mode Oscillations in Neutron Stars
Authors: Bikram Keshari Pradhan, Dhruv Pathak, Debarati Chatterjee
Figure caption: Similar to Figure 3 but with consideration of ten random events with S/N ≥ 8 in A+ (blue line) and ET (red lines) corresponding to f-mode events from Vela pulsar. We have also shown the distributions of nuclear parameters resulting from considering ten random events in ET, excluding the Vela (cyan color).
Paper: Constraining Nuclear Parameters Using Gravitational Waves from f-mode Oscillations in Neutron Stars
Authors: Bikram Keshari Pradhan, Dhruv Pathak, Debarati Chatterjee
Figure caption: Similar to Figure 3, but the posteriors are resulting from considering existing astrophysical observations (cyan color), combining existing astrophysical events with one f-mode event corresponding to the strongest Vela glitch in A+ (blue color), and ET (red color).
Paper: Constraining Nuclear Parameters Using Gravitational Waves from f-mode Oscillations in Neutron Stars
Authors: Bikram Keshari Pradhan, Dhruv Pathak, Debarati Chatterjee
Figure caption: Shows 90% SCIs for (a) the pressure as a function of energy density and (b) the radius as a function of mass reconstructed from different posteriors of nuclear parameters presented in Figure 8.
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: Emission from various points along the trajectory of a relativistic particle. Panel (a) γ ψ ≫ 1: the emission from some parts (bold portions) of the trajectory is observable. Panel (b) γ ψ ≪ 1: the emission from the entire trajectory is observable.
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: The spectra of multiple radiating bunches with a periodic or quasiperiodic distribution in the time domain. The top panel corresponds to a strictly periodic distribution with δ ϕ  j  = 0. The bottom panel corresponds to a quasiperiodic distribution with δ ϕ  j  uniformly distributed in [−0.5, 0.5]. A curvature-radiation-like spectrum for a single point-source bunch, ﹩| {E}_{0}(\omega ){| }^{2}\propto {\omega }^{2/3}\exp (-\omega /{\omega }_{c})﹩, is taken as an example in this figure. We take ω  m  = ω  c  and N = 103. The peak frequency is at 2n π ω  m  with ﹩n\in {{\mathbb{Z}}}^{+}﹩.
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: The evolution of electric field component of a pulse of electromagnetic wave with a rectangular power spectrum given by Equation (8). The top and bottom panels correspond to the scenarios with a narrow spectrum of Δω  k /ω 0,k  = 0.1 and with a wide spectrum of Δω  k /ω 0,k  = 1, respectively. The phase argument is taken as ϕ  k  = 0 here.
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: The amplification of the gravitational lensing as a function of frequency. The top panel takes the lens mass as M = 10−5 M ⊙. The black, red, and blue lines correspond to r s/r E = 0.5, 1.0, and 1.5, respectively. The bottom panel takes the source projected position as r s/r E = 1.0. The black, red, and blue lines correspond to lens masses of M = 10−6 M ⊙, 10−5 M ⊙, and 10−4 M ⊙, respectively. The distances from the lens to the FRB source, from the observer to the lens, and from the observer to the FRB source are taken as d ls = 1 kpc, d ol = 1 Gpc, and d os = 1 Gpc, respectively.
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: The simulated distribution of the observed spectral bandwidth of radio bursts from an FRB repeater. The purple, yellow, and blue bars correspond to the different relative spectral bandwidths with Δν/ν 0 = 0.1, 0.5, and 1, respectively. We take ν 0,t  = 1.25 GHz and Δν  t  = 0.5 GHz for the telescope’s parameters. The intrinsic peak frequencies ν 0 of the radio bursts are assumed to be uniformly distributed near the telescope’s bandwidths, i.e., ﹩f({\nu }_{0})=\mathrm{const}﹩.
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: The amplification of the synchrotron maser mechanism as a function of frequency. The black, red, and blue lines correspond to electron distribution index p = 2.5, 3, and 3.5, respectively. The optical depth at ﹩{\nu }_{\min }﹩ is assumed to be τ  ν,0 = 10 here. The frequency is dimensionless with ﹩{\nu }_{\min }={\gamma }_{\min }^{2}{\nu }_{B}﹩. Notice that the amplification becomes zero for ﹩\nu \lt {\nu }_{\min }﹩ in this figure; see the text for the discussion.
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: The schematic pyramid illustrates the physical processes affecting the observed spectral features.
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: Two radiation mechanisms with γ ψ ≫ 1 and γ ψ ≪ 1 in the magnetized shocked medium. Panel (a) corresponds to traditional synchrotron radiation. Panel (b) corresponds to the small-pitch-angle synchrotron radiation, in which the emission region has a magnetic field almost parallel to the line of sight, and the direction of the particles’ injection is almost parallel to the field lines.
Paper: Implications of Narrow Spectra of Fast Radio Bursts
Authors: Yuan-Pei Yang
Figure caption: Two radiation mechanisms with γ ψ ≫ 1 and γ ψ ≪ 1 in the magnetosphere of a neutron star. In the inner region with a relatively strong magnetic field, the radiation mechanism is the curvature radiation. In the outer region with a relatively weak magnetic field, the radiation mechanism is the small-pitch-angle synchrotron radiation.
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: Connectivity maps that are produced for four extended periods of 3He, with each map being constructed at the beginning of its respective time period. Panel (a) displays the map for 2022 January 13, panel (b) for 2022 February 05, panel (c) for 2022 July 19, and panel (d) for the time period of 2021 July 23. Each map shows the projected location of the heliospheric current sheet (white line), as well as the open (red and green lines) and closed (black) field lines from the PFSS model. Furthermore, the location of Solar Orbiter is indicated by the blue circle. From that location, the Parker spiral is displayed with a dashed blue line, and the footpoint location of the Parker spiral to the source surface is depicted with a blue cross. From that point, the field lines are traced below the source surface using the PFSS model, and they are depicted with blue lines. The locations of the footpoints of the field lines connecting to the spacecraft during subsequent times and within the 3He time periods are displayed using colored circles. The color coding of these points is given by the color bar on the inner left of each panel. Green (red) footpoints are used to represent times near the beginnings (ends) of the periods.
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: Histograms of the characterization and analysis of 3He-rich event magnetic connectivity. Panel (a) displays the resulting histogram from the classification of the magnetic connectivity to four different classes (“stable,” “stable+,” “dynamic,” and “complex”). Panel (b) displays the histogram resulting from the analysis of the regions of connectivity. The histogram located on the left illustrates the number of instances in which the magnetic connectivity is observed either on the visible disk (VD) or on the far side (FS & FS*; see text for details). On the right-hand side, the histogram exhibits the cases in which the connectivity is located in an active region or a coronal hole. Panel (c) displays the histogram from the analysis of the connectivity changes at the boundaries. The histogram on the left shows connectivity changes at the beginnings of the periods, and that on the right shows changes at the ends of the periods.