adsabs/AstroCLIMB huggingface dataset:
Paper: Finding the Missing Baryons in the Intergalactic Medium with Localized Fast Radio Bursts
Authors: K. B. Yang, Q. Wu, F. Y. Wang
Figure caption: The DMIGM − z relation for fast radio bursts (FRBs). The scatter star points are 23 localized FRBs. DMIGM values are derived by deducing the DMMW, DMhalo, and DMhost from DMobs. DMMW values are deduced from the NE2001 model, and DMhalo values are estimated to be 65 pc cm−3. We use the median value of DMhost at different redshifts according to Equation (5). The blue line is the result derived from IllustrisTNG 300 cosmological simulation and the green shaded region is the 95% confidence level. The red line represents the theoretical model DMIGM (Equation (2)) assuming f IGM = 0.82, Ω b  = 0.0488 and H 0 = 70 km  s−1 Mpc−1. Due to FRB 210117 (red point) deviating from the 95% confidence region of DMIGM, we exclude it in the following analysis.
Paper: Finding the Missing Baryons in the Intergalactic Medium with Localized Fast Radio Bursts
Authors: K. B. Yang, Q. Wu, F. Y. Wang
Figure caption: The normalized probability density distribution of Ω b  from 22 localized FRBs. The best fit is ﹩{{\rm{\Omega }}}_{b}={0.0490}_{-0.0033}^{+0.0036}﹩ in 1σ confidence level. The red solid line shows the best-fit value, and dotted lines present the 1σ and 2σ confidence levels. The blue shaded region shows the constraint on Ω b  from cosmic microwave background (CMB) with 1σ confidence level, and the yellow shade region represents the constraint from Big Bang nucleosynthesis (BBN) with 1σ confidence level. The green dashed lines correspond to the 1σ uncertainty range of Ω b  derived by Macquart et al. (2020).
Paper: Finding the Missing Baryons in the Intergalactic Medium with Localized Fast Radio Bursts
Authors: K. B. Yang, Q. Wu, F. Y. Wang
Figure caption: Current observational measurements of the low-redshift baryon census. From the DM−z relation of fast radio bursts (FRBs), 83% ± 6% of the cosmic baryons in the diffuse form are derived. The values in collapsed forms, including in galaxies, the circumgalactic medium (CGM), the intercluster medium (ICM), and cold gas, are adjusted from Shull et al. (2012). Collapsed phases (galaxies, CGM, ICM, and cold neutral gas) contribute 17% ± 4% of the total cosmic baryons. From our study, almost 100% cosmic baryons are found in the late-time universe.
Paper: Finding the Missing Baryons in the Intergalactic Medium with Localized Fast Radio Bursts
Authors: K. B. Yang, Q. Wu, F. Y. Wang
Figure caption: The coordinates of 18 localized fast radio bursts (FRBs) in the galactic coordinate system. There is no FRB with both low galactic latitudes and low galactic longitudes.
Paper: Testing the Galaxy-collision-induced Formation Scenario for the Trail of Dark-matter-deficient Galaxies with the Susceptibility of Globular Clusters to the Tidal Force
Authors: Go Ogiya, Frank C. van den Bosch, Andreas Burkert, Xi Kang
Figure caption: (Top) Comparison of mean densities. Orange lines show the mean density of the DMDG measured at the indicated r. The mean density of NGC 1052 is given as a function of the distance from its center, R, and multiplied by a factor of 2.5 (solid black) or 1.5 (dotted black). (Middle) Fraction of GCs stripped from the DMDG when it is at R. (Bottom) Cumulative number fraction of satellite galaxies contained within R. The NFW density profile with parameters explained in the main text and the power-law index of β = 1 are used to compute it. Half of the satellite galaxies are located at R < 150 kpc where the tidal force reduces the number of GCs by a factor of 5–10.
Paper: Testing the Galaxy-collision-induced Formation Scenario for the Trail of Dark-matter-deficient Galaxies with the Susceptibility of Globular Clusters to the Tidal Force
Authors: Go Ogiya, Frank C. van den Bosch, Andreas Burkert, Xi Kang
Figure caption: Orbital evolution of two GCs in the DMDG model (black and orange). Solid and dotted lines represent the prediction by the semianalytic model and the N-body simulation result, respectively. While the simulation employs the forward time integration, the semianalytic model adopts the last snapshot of the GCs in the simulation as the final condition and traces back their orbital evolution with the backward time integration. The semianalytic model reasonably reproduces the simulation with ﹩{b}_{\min }=1﹩ pc.
Paper: Testing the Galaxy-collision-induced Formation Scenario for the Trail of Dark-matter-deficient Galaxies with the Susceptibility of Globular Clusters to the Tidal Force
Authors: Go Ogiya, Frank C. van den Bosch, Andreas Burkert, Xi Kang
Figure caption: Probability distribution of the maximum-r, ﹩{r}_{\max }﹩, at t = [−8, −7.5] Gyr (solid) and at t = [−7.5, −7] Gyr (dotted). GCs should have been on orbits of ﹩{r}_{\max }=5\mbox{--}10\,\mathrm{kpc}﹩ at the formation epoch.
Paper: The Periodic Signals of Nova V1674 Herculis (2021)
Authors: Joseph Patterson, Josie Enenstein, Enrique de Miguel, Marguerite Epstein-Martin, Jonathan Kemp, Richard Sabo, Walt Cooney, Tonny Vanmunster, Pavol Dubovsky, Franz-Josef Hambsch, Gordon Myers, Damien Lemay, Kirill Sokolovsky, Donald Collins, Tut Campbell, George Roberts, Michael Richmond, Stephen Brincat, Joseph Ulowetz, Shawn Dvorak, Tamás Tordai, Sjoerd Dufoer, Andrew Cahaly, Charles Galdies, Bill Goff, Francis P. Wilkin, Matt A. Wood
Figure caption: (a) Light curve on JD 2,459,382 (V = 10) after subtracting the linear decline. The apparent dips seem to correspond to phases near 0.0 and 0.5 in our orbital ephemeris. At a remarkable 7 mag above the 2022 level, the light curve looks basically the same. (b) O  −  C diagram of the times of minimum light in the orbital signal, relative to the test ephemeris HJD 2,459,400.636+0.152921 E. Omitted are timings of “secondary minima,” some of which are included in Table 1. (c) The average orbital waveform after the first 30 days of outburst.
Paper: The Periodic Signals of Nova V1674 Herculis (2021)
Authors: Joseph Patterson, Josie Enenstein, Enrique de Miguel, Marguerite Epstein-Martin, Jonathan Kemp, Richard Sabo, Walt Cooney, Tonny Vanmunster, Pavol Dubovsky, Franz-Josef Hambsch, Gordon Myers, Damien Lemay, Kirill Sokolovsky, Donald Collins, Tut Campbell, George Roberts, Michael Richmond, Stephen Brincat, Joseph Ulowetz, Shawn Dvorak, Tamás Tordai, Sjoerd Dufoer, Andrew Cahaly, Charles Galdies, Bill Goff, Francis P. Wilkin, Matt A. Wood
Figure caption:  O  −  C diagrams for the extrema of the 501 s pulse. The 2021 diagram represents maximum light, relative to the ephemeris HJD 2,459,415.38195+0.00580417 E. The curve indicates a mean period decrease of 182(18) ms yr−1. The 2022 diagram represents minimum light, relative to the test ephemeris HJD 2,459,637.6733+0.00580315 E. The curve indicates a period decrease of 88(15) ms yr−1.
Paper: The Periodic Signals of Nova V1674 Herculis (2021)
Authors: Joseph Patterson, Josie Enenstein, Enrique de Miguel, Marguerite Epstein-Martin, Jonathan Kemp, Richard Sabo, Walt Cooney, Tonny Vanmunster, Pavol Dubovsky, Franz-Josef Hambsch, Gordon Myers, Damien Lemay, Kirill Sokolovsky, Donald Collins, Tut Campbell, George Roberts, Michael Richmond, Stephen Brincat, Joseph Ulowetz, Shawn Dvorak, Tamás Tordai, Sjoerd Dufoer, Andrew Cahaly, Charles Galdies, Bill Goff, Francis P. Wilkin, Matt A. Wood
Figure caption: Power spectrum of a typical 14 day segment of light curve early in the outburst, showing the powerful rotational signal at ω, and orbital sidebands at ω  − Ω and ω  − 2Ω. The sidebands disappeared after ∼60 days.
Paper: The Maximum Isotropic Equivalent Energy of Gamma-Ray Bursts
Authors: Shlomo Dado, Arnon Dar
Figure caption: The best-fit Amati correlation (red line) between recalibrated values of (1 + z)E  p  and E iso of GRBs (black data points), within 1σ and 3σ limits (shaded region) adapted from Amati et al. (2019).
Paper: The Maximum Isotropic Equivalent Energy of Gamma-Ray Bursts
Authors: Shlomo Dado, Arnon Dar
Figure caption: A cutoff power-law fit to the combined CRe flux (multiplied by E 3) measured near Earth with AMS-02 (filled circles: Aguilar et al. 2014) and with H.E.S.S (empty and filled squares: Aharonian et al. 2008, 2009, respectively). The normalization of the H.E.S.S data was adjusted within their estimated systematic error to match the more precise AMS-02 data below TeV.
Paper: The Maximum Isotropic Equivalent Energy of Gamma-Ray Bursts
Authors: Shlomo Dado, Arnon Dar
Figure caption: A broken power-law fit to the CRE spectrum (multiplied by E 3) measured with the Calorimetric Electron Telescope (CALET) on the International Space Station, from 11 GeV to 4.8 TeV.
Paper: The Maximum Isotropic Equivalent Energy of Gamma-Ray Bursts
Authors: Shlomo Dado, Arnon Dar
Figure caption: A broken power-law fit to the CRE spectrum (multiplied by E 3) measured by DAMPE (Chang et al. 2017) between 50 GeV and 5 TeV. A CRE knee is indicated by the wide band around 1 TeV.
Paper: First Results from the JWST Early Release Science Program Q3D: Turbulent Times in the Life of a z ∼ 3 Extremely Red Quasar Revealed by NIRSpec IFU
Authors: Dominika Wylezalek, Andrey Vayner, David S. N. Rupke, Nadia L. Zakamska, Sylvain Veilleux, Yuzo Ishikawa, Caroline Bertemes, Weizhe Liu, Jorge K. Barrera-Ballesteros, Hsiao-Wen Chen, Andy D. Goulding, Jenny E. Greene, Kevin N. Hainline, Fred Hamann, Timothy Heckman, Sean D. Johnson, Dieter Lutz, Nora Lützgendorf, Vincenzo Mainieri, Roberto Maiolino, Nicole P. H. Nesvadba, Patrick Ogle, Eckhard Sturm
Figure caption: Next to the HST ACS & WFC3 wide-field composite we show the four-color image (middle) showcasing the complex [O III] kinematics and morphology around the extremely red quasar J1652 at z = 2.9489 from the JWST data. North is up and East is to the left. The quasar position is at the center of the image. The image is ∼ 26 kpc on the side and is composed of four narrow-band images made from the NIRSpec cube. The narrow-band images, shown individually in the right panels, are centered on the [O III]5007A emission line at velocities of −350, 0, 370, and 700 km s−1 and they are ∼120 km s−1 wide. The four-color image reveals the biconical (blue- and red/orange-shifted emission) quasar-driven outflow in the NE-SW direction as well as a companion galaxy (Companion C1) at ∼ 700 km s−1 in the North-East corner of the NIRSpec cube (red emission). In addition, the NIRSpec cube reveals an extended [O III] component at 600 − 800 km s−1 (red) in the South-Western quadrant of the image. This extended component is associated with continuum stellar emission as revealed by the HST data. Image Credit: ESA/Webb, NASA & CSA, D. Wylezalek, A. Vayner & the Q3D Team, and N. Zakamska.
Paper: First Results from the JWST Early Release Science Program Q3D: Turbulent Times in the Life of a z ∼ 3 Extremely Red Quasar Revealed by NIRSpec IFU
Authors: Dominika Wylezalek, Andrey Vayner, David S. N. Rupke, Nadia L. Zakamska, Sylvain Veilleux, Yuzo Ishikawa, Caroline Bertemes, Weizhe Liu, Jorge K. Barrera-Ballesteros, Hsiao-Wen Chen, Andy D. Goulding, Jenny E. Greene, Kevin N. Hainline, Fred Hamann, Timothy Heckman, Sean D. Johnson, Dieter Lutz, Nora Lützgendorf, Vincenzo Mainieri, Roberto Maiolino, Nicole P. H. Nesvadba, Patrick Ogle, Eckhard Sturm
Figure caption: NIRSpec [O III] color composite (from Figure 1) along with the NIRSpec spectra (in dimensionless F  λ  units) zooming into the [O III] doublet at different positions in the NIRSpec field of view. The spectra reveal spatially well-defined individual kinematic components at velocities ranging between v = −450 and 820 km s−1 and velocity dispersions between σ = 50 and 500 km s−1. The fits are performed by using up to three Gaussian components, and the fit results are presented in Table 1. The companion galaxies C1, C2, and C3 (see Figure 2) are spectroscopically confirmed in apertures A2, A8, and A9, respectively, at velocity offsets of ∼600 km s−1 with respect to the quasar host [O III] emission. We also detect extended [O III] emission associated with the extended stellar feature seen in the HST images (e.g., A4, A5, and A6) at velocities of ∼700–800 km s−1. Additionally, we confirm the blueshifted component of the quasar-driven outflow (e.g., in A0 and A7) and newly identify the likely redshifted counterpart in the north (e.g., detected in A3). The outflow axis well matches previous constraints of the projected quasar illumination direction from polarization measurements of this source (Alexandroff et al. 2018). Image credit of central color composite: ESA/Webb, NASA & CSA, D. Wylezalek, A. Vayner & the Q3D Team.
Paper: First Results from the JWST Early Release Science Program Q3D: Turbulent Times in the Life of a z ∼ 3 Extremely Red Quasar Revealed by NIRSpec IFU
Authors: Dominika Wylezalek, Andrey Vayner, David S. N. Rupke, Nadia L. Zakamska, Sylvain Veilleux, Yuzo Ishikawa, Caroline Bertemes, Weizhe Liu, Jorge K. Barrera-Ballesteros, Hsiao-Wen Chen, Andy D. Goulding, Jenny E. Greene, Kevin N. Hainline, Fred Hamann, Timothy Heckman, Sean D. Johnson, Dieter Lutz, Nora Lützgendorf, Vincenzo Mainieri, Roberto Maiolino, Nicole P. H. Nesvadba, Patrick Ogle, Eckhard Sturm
Figure caption: We show the PSF-subtracted HST WFC3 F160W image adopting a color scheme that highlights faint features showing the negative, zero, and positive values in blue, white, and red, respectively (see also Zakamska et al. 2019). The extended stellar light emission is clearly visible toward the west, and we mark it with the pink ellipse. We also show the NIRSpec contours of the narrowband images Sys and Red2 and the NIRSpec footprint with the black dashed box. The NIRSpec-detected [O III] emission, extending in the same direction as the HST extended emission (marked with the pink ellipse), confirms that the extended emission feature is associated with the J1652 system. With the NIRSpec data, we furthermore confirm that three HST continuum sources are companion sources (C1, C2, and C3). The foreground star in the field is marked by the yellow star, and the position of the quasar J1652 is indicated by the red cross.
Paper: On the Statistics of Elsasser Increments in Solar Wind and Magnetohydrodynamic Turbulence
Authors: Juan C. Palacios, Sofiane Bourouaine, Jean C. Perez
Figure caption: Top panels: continuous lines represent the estimated PDFs ﹩{{\mathscr{P}}}^{+}(u,l)﹩ vs. u/σ  l  for fast wind (left), slow wind (middle), and simulation (right), where ﹩u=\delta {z}_{L}^{+}﹩. Note that for spacecraft data the space lag is l = V  SW  τ via Taylor’s Hypothesis, and σ  l  represents the standard deviation at scale l. Middle and bottom panels: distribution of n th moment ﹩{{\mathscr{I}}}_{n}^{+}(u,l)﹩ normalized to its maximum value (﹩{{\mathscr{I}}}_{n,\max }^{+}﹩) for fast wind (left), slow wind (middle), and simulation (right) for two different lags near the end (middle panel) and beginning (bottom panel) of the inertial range. Dashed lines represent the approximation of the PDF extending the tails assuming an exponential behavior.
Paper: On the Statistics of Elsasser Increments in Solar Wind and Magnetohydrodynamic Turbulence
Authors: Juan C. Palacios, Sofiane Bourouaine, Jean C. Perez
Figure caption: Scaling exponents for ﹩\delta {z}_{L}^{+}﹩ and ﹩\delta {z}_{L}^{-}﹩ increments for fast wind (left), slow wind (middle), and simulation (right) directly calculated with the experimental data (ζ  e ) and using the PDF modeled with exponential tails (ζ  m ). ESS is applied in all cases.
Paper: On the Statistics of Elsasser Increments in Solar Wind and Magnetohydrodynamic Turbulence
Authors: Juan C. Palacios, Sofiane Bourouaine, Jean C. Perez
Figure caption: Exponential decrements of extended tails α  l  for ﹩\delta {z}_{l}^{+}﹩ (black) and ﹩\delta {z}_{l}^{-}﹩ (blue) in the fast solar wind (left), slow solar wind (center), and simulation (right). Here l/L out represents the increment scale normalized with respect to the outer scale L out which corresponds to 700 s for fast wind, 2000 s for slow wind, and 256δ x for simulations. Vertical lines represent the limits of the inertial range.
Paper: On the Statistics of Elsasser Increments in Solar Wind and Magnetohydrodynamic Turbulence
Authors: Juan C. Palacios, Sofiane Bourouaine, Jean C. Perez
Figure caption: Third (top) and tenth (bottom) order structure functions for δ z + of slow wind calculated using the empirical PDF (black marks) and the extrapolated PDF using exponential tails (blue marks) vs. time lags. Green and red lines show power-law fits for the dissipative and injection regions, respectively, while the black vertical lines indicate the lower and upper limits of the inertial range.
Paper: Ultramassive Black Holes Formed by Triple Quasar Mergers at z ∼ 2
Authors: Yueying Ni, Tiziana Di Matteo, Nianyi Chen, Rupert Croft, Simeon Bird
Figure caption: Detailed evolution of each of the three quasars. The blue line represents the BH1, the central black hole in Figure 2. The red (orange) line in the first panel gives the 3D distance between BH2 (BH3) and BH1. The horizontal dashed line marks 2ϵ  g  as the gravitational softening when the black hole merger occurs in the simulation. The two insets zoom into the dashed rectangles to better show the evolution before the SMBH mergers. The second to the fourth panels show the evolution of black hole mass, bolometric luminosity, and the Eddington ratio, respectively. The bottom panel shows the gas column density N H surrounding each black hole. We calculate N H by integrating the neutral hydrogen number density along different lines of sights toward the central BHs and show the median N H among all sight lines. The vertical dashed lines in each panel mark the time of SMBH mergers.
Paper: Ultramassive Black Holes Formed by Triple Quasar Mergers at z ∼ 2
Authors: Yueying Ni, Tiziana Di Matteo, Nianyi Chen, Rupert Croft, Simeon Bird
Figure caption: Relation between the stellar mass of galaxies with (i) mass of the most massive black hole in that galaxy (left panel) and (ii) star formation rate of the galaxy (right panel). The blue background shows the 2D histogram for all the galaxy populations at z = 2 in the ASTRID simulation. The gray dashed line and brown dotted line give the observational fitting of  M BH −  M * from Kormendy & Ho (2013) and Reines & Volonteri (2015) based on z ∼ 0 AGN observations. The orange data points give 2 < z < 4 quasars collected from Kormendy & Ho (2013). The circles mark the evolution of the triple quasar system from z = 2.7 to z = 2.0. Insets in the left panel illustrate the morphology of the BH1 host galaxy (in the face-on direction) at z = 2.5 and z = 2.0 in the 20 h −1 kpc region. Insets in the right panel illustrate the gas density field colored by the star formation rate (with red color indicating high star formation rate) in the 300 h −1 kpc region centered at BH1.
Paper: Ultramassive Black Holes Formed by Triple Quasar Mergers at z ∼ 2
Authors: Yueying Ni, Tiziana Di Matteo, Nianyi Chen, Rupert Croft, Simeon Bird
Figure caption: Illustration of the quasar triplet system and its environment (host galaxies). The background in the lower panels shows the stellar density field in a 600 h −1 kpc region centered at the most massive quasar (BH1). Crosses mark the positions of the three quasars. The red and yellow lines mark the trajectories of the other two quasars (BH2 and BH3) in the reference frame of BH1. The left upper panel shows a cartoon of the quasar triplet system in a field of view with 25″ (500  h −1 kpc at z = 2.7). The image is convolved with a Gaussian point-spread function with FWHM 0.″5. Estimation of quasar UV band magnitude is given in the legend. (Here we do not include dust attenuation.) The right upper panel illustrates the host galaxies for the three quasars at z = 2.7 in 20 h −1 kpc regions, projected in the same direction as the cartoon on the left. Colors show the stellar age, with older stars being redder.
Paper: Ultramassive Black Holes Formed by Triple Quasar Mergers at z ∼ 2
Authors: Yueying Ni, Tiziana Di Matteo, Nianyi Chen, Rupert Croft, Simeon Bird
Figure caption: Cumulative number density of quasars as well as dual and triple quasars as a function of redshift. The gray dashed line shows the observational determination of the quasar number density from Shen et al. (2020), obtained by integrating the quasar luminosity function fit from a collection of all-band quasar observations. The dark blue line shows the number density of quasars with ﹩\mathrm{log}{L}_{\mathrm{bol}}\gt 45.5﹩ within the 250  h −1 Mpc volume of ASTRID. The orange (pink) line shows the time-averaged number density of quasar pairs (triples) where quasars are within 5 h −1 kpc < r < 200 h −1 kpc from each other. The shaded area corresponds to the Poisson noise.
Paper: JWST Imaging of Earendel, the Extremely Magnified Star at Redshift z = 6.2
Authors: Brian Welch, Dan Coe, Erik Zackrisson, S. E. de Mink, Swara Ravindranath, Jay Anderson, Gabriel Brammer, Larry Bradley, Jinmi Yoon, Patrick Kelly, Jose M. Diego, Rogier Windhorst, Adi Zitrin, Paola Dimauro, Yolanda Jiménez-Teja, Abdurro'uf, Mario Nonino, Ana Acebron, Felipe Andrade-Santos, Roberto J. Avila, Matthew B. Bayliss, Alex Benítez, Tom Broadhurst, Rachana Bhatawdekar, Maruša Bradač, Gabriel B. Caminha, Wenlei Chen, Jan Eldridge, Ebraheem Farag, Michael Florian, Brenda Frye, Seiji Fujimoto, Sebastian Gomez, Alaina Henry, Tiger Y.-Y Hsiao, Taylor A. Hutchison, Bethan L. James, Meridith Joyce, Intae Jung, Gourav Khullar, Rebecca L. Larson, Guillaume Mahler, Nir Mandelker, Stephan McCandliss, Takahiro Morishita, Rosa Newshore, Colin Norman, Kyle O'Connor, Pascal A. Oesch, Masamune Oguri, Masami Ouchi, Marc Postman, Jane R. Rigby, Russell E. Ryan Jr, Soniya Sharma, Keren Sharon, Victoria Strait, Louis-Gregory Strolger, F. X. Timmes, Sune Toft, Michele Trenti, Eros Vanzella, Anton Vikaeus
Figure caption: JWST NIRCam image of the z ∼ 6.2 Sunrise Arc, including the lensed star Earendel, marked with an arrow. This 15.″2 × 12.″4 color image combines all eight NIRCam images on a 0.″02 pixel scale.