adsabs/AstroCLIMB huggingface dataset:
Paper: Rotational Characteristics of the Solar Transition Region Using SDO/AIA 304 Å Images
Authors: Qian-Rui Wu, Sheng Zheng, Shu-Guang Zeng, Miao Wan, Xiang-Yun Zeng, Lin-Hua Deng, Yao Huang
Figure caption: The average rotation rates at different latitudes (black scatter points and their corresponding error bars), and the fitted rotation profile (blue solid line) of the entire period from 2011 to 2022.
Paper: Rotational Characteristics of the Solar Transition Region Using SDO/AIA 304 Å Images
Authors: Qian-Rui Wu, Sheng Zheng, Shu-Guang Zeng, Miao Wan, Xiang-Yun Zeng, Lin-Hua Deng, Yao Huang
Figure caption: The yearly average rotation rate of the STR (blue solid line and their corresponding error bars) and annual sunspot numbers (black dotted line) from 2011 to 2022.
Paper: Rotational Characteristics of the Solar Transition Region Using SDO/AIA 304 Å Images
Authors: Qian-Rui Wu, Sheng Zheng, Shu-Guang Zeng, Miao Wan, Xiang-Yun Zeng, Lin-Hua Deng, Yao Huang
Figure caption: Schematic diagram of divided latitudinal rectangular bands on the solar disk of SDO/AIA 304 Å SFD image.
Paper: Giant Impact Events for Protoplanets: Energetics of Atmospheric Erosion by Head-on Collision
Authors: Kenji Kurosaki, Shu-ichiro Inutsuka
Figure caption: The relationship between the input energy and atmosphere loss fraction. The escaping mass fraction for the atmosphere X atm and core X core are shown, which are escape mass fractions normalized by the total atmospheric mass M T,atm + M I,atm and core mass M T,c + M I,c, respectively. Circles are the impact simulations when the impactor has an atmosphere, while squares are the bare-rock impactor. Filled marks reflect that the planet retains a layered structure after the impact, while open marks represent that the planet has a region where the atmosphere and core are mixed. Purple and red symbols represent the atmosphere loss fraction X atm, while green and orange symbols are the core loss mass fraction X core. The black line is the analytic prediction for X atm shown in Equation (40).
Paper: Giant Impact Events for Protoplanets: Energetics of Atmospheric Erosion by Head-on Collision
Authors: Kenji Kurosaki, Shu-ichiro Inutsuka
Figure caption: Snapshots of impact simulations. The top leftmost panel is color-coded diagrams of lost and bound particles. Red indicates lost atmospheric particles. Green indicates bound atmospheric particles. Black indicates escaping rock particles, and blue indicates bound rock particles. For the target mass of 1 M ⊕ with 10% of the atmosphere by mass and the impactor mass of 1 M ⊕ with 10% of the atmosphere (mix (34) A3+A3), simulation results of central cross sections are shown in four panels. Those snapshots show the time when t = 0 × τ ff (panel (1)), t = 1.5 × τ ff (panel (1)), t = 2.5 × τ ff (panel (2)), and t = 30 × τ ff (panel (4)) from left to right, respectively. Run (31) simulation is start from t = −2.5 × τ ff, where τ ff = 2.2  hr. The colors are the same as in Figure 1.
Paper: Giant Impact Events for Protoplanets: Energetics of Atmospheric Erosion by Head-on Collision
Authors: Kenji Kurosaki, Shu-ichiro Inutsuka
Figure caption: The relationship between the sum of the kinetic impact energy and the released energy from the merged core K imp − δΦ c , the kinetic energy of escaping mass K esc, and energy changes δ E atm, δ U  c . δΦ c  is calculated by Equation (29). Plot colors represent the energy changes. Red plots are the kinetic energy of escaping mass (Equation (15)), purple plots are the change of the internal energy of the core (Equation (32)), and the green plots are the change of the energy of the atmosphere (Equation (31)). Blue plots represent the fraction of K esc − δ U  c  − δ E atm to K imp − δΦ c .
Paper: Giant Impact Events for Protoplanets: Energetics of Atmospheric Erosion by Head-on Collision
Authors: Kenji Kurosaki, Shu-ichiro Inutsuka
Figure caption: Left panel: time evolution of the escaping mass fraction after the impact event. The target mass is 1 M ⊕ with 10% of the atmosphere by mass. The impactor is the same as the target. Colored lines are the same as those in the Figure 3. Right panel: the interior structure at t = 50 τ ff. The target mass is 1 M ⊕ with 10% of the atmosphere by mass while the impactor is the same as the target. The bound body radius is normalized by the target radius. Colored lines are the same as those in Figure 4.
Paper: Giant Impact Events for Protoplanets: Energetics of Atmospheric Erosion by Head-on Collision
Authors: Kenji Kurosaki, Shu-ichiro Inutsuka
Figure caption: The relationship between the available energy calculated by Equation (35) and the internal energy change calculated by Equation (32). The black line indicates the relation δ U  c  = 0.68 E av. The left bottom panel shows the fraction δ U  c  to E av. Plot colors are the same as those in Figure 8.
Paper: Giant Impact Events for Protoplanets: Energetics of Atmospheric Erosion by Head-on Collision
Authors: Kenji Kurosaki, Shu-ichiro Inutsuka
Figure caption: The relative error between the numerical results X atm and the predictions ﹩{X}_{\mathrm{atm}}^{\mathrm{pred}}﹩. Purples marks are calculated by Equation (42). Red marks are Equation (1) in Kegerreis et al. (2020a). Green marks are Equation (21) in Denman et al. (2020). Black dashed line is the upper limit line for ﹩{X}_{\mathrm{atm}}^{\mathrm{pred}}=1﹩.
Paper: Giant Impact Events for Protoplanets: Energetics of Atmospheric Erosion by Head-on Collision
Authors: Kenji Kurosaki, Shu-ichiro Inutsuka
Figure caption: The comparison of the energy of bound atmosphere calculated by Equation (33) and numerical results E B,atm. Black line represent the linear regression result ϵ = 0.56. Plot colors are the same as those shown in Figure 8.
Paper: Giant Impact Events for Protoplanets: Energetics of Atmospheric Erosion by Head-on Collision
Authors: Kenji Kurosaki, Shu-ichiro Inutsuka
Figure caption: Upper panel: the velocity distribution for run (31) after the impact. The velocity is normalized by Equation (A1). Red dots are the bound atmosphere particles. Blue dots are the bound core particles. Green particles are escaping atmosphere particles. Black particles are escaping core particles.
Paper: Giant Impact Events for Protoplanets: Energetics of Atmospheric Erosion by Head-on Collision
Authors: Kenji Kurosaki, Shu-ichiro Inutsuka
Figure caption: The relationship between the available energy calculated by Equation (35) and the kinetic energy of escaping particles. The black line indicates the relation K esc = α E av where α = 0.31. Plot colors are the same as those shown in Figure 8.
Paper: Particle Energization at a High Mach Number Perpendicular Shock: 1D Particle-in-cell Simulations
Authors: Yufei Hao, Zhongwei Yang, Fan Guo, Terry Z. Liu, Xiangliang Kong, Lican Shan, Dejin Wu
Figure caption: Trajectories of the typical particle with contour plots of time evolutions of (a) the total magnetic fields; (b)–(c) x- and z-component electric fields; the corresponding (d) electric and magnetic forces in the x-direction; (e) its velocity and three components; and (f) potential difference from the x- and z-directions and their sum. The black dotted line denotes the shock speed V shock = 5.8 in the downstream frame. R 1, R 2, R 11, R 11, and R 20 indicate the subareas of E  x  and E  x  in the foot area. The dotted lines denote the times Ω i  t 1 = 5.8, Ω i  t 2 = 6.02, Ω i  t 3 = 6.2, Ω i  t 4 = 7.1, and Ω i  t 5 = 6.48.
Paper: Particle Energization at a High Mach Number Perpendicular Shock: 1D Particle-in-cell Simulations
Authors: Yufei Hao, Zhongwei Yang, Fan Guo, Terry Z. Liu, Xiangliang Kong, Lican Shan, Dejin Wu
Figure caption: Time evolutions of (a) x- and (b) z-components of the average velocity of particles. The shock foot area is restricted by black solid and dashed lines, which indicate the contour line corresponding to B = 1.3B 0 and the rough positions of the ramp. R V11, R V12, R V22, R V1, and R V2 denote the subareas in the restricted foot area of evolution of V  x  and V  z . For comparison, time evolutions of (c) x- and (d) z-components of the average velocity of particles from a shock with M  A  = 3.6 are also displayed in the same format as the upper panels.
Paper: Particle Energization at a High Mach Number Perpendicular Shock: 1D Particle-in-cell Simulations
Authors: Yufei Hao, Zhongwei Yang, Fan Guo, Terry Z. Liu, Xiangliang Kong, Lican Shan, Dejin Wu
Figure caption: Trajectories of the typical particle with contour plots of time evolutions of (a) the total magnetic fields; (b)–(c) x- and z-component electric fields; the corresponding (d) electric and magnetic forces in the x-direction; (e) its velocity and three components; and (f) potential difference from the x- and z-directions and their sum. The black dotted line denotes the shock speed V shock = 5.8 in the downstream frame.
Paper: Particle Energization at a High Mach Number Perpendicular Shock: 1D Particle-in-cell Simulations
Authors: Yufei Hao, Zhongwei Yang, Fan Guo, Terry Z. Liu, Xiangliang Kong, Lican Shan, Dejin Wu
Figure caption: Trajectories of the typical particle with contour plots of time evolutions of (a) the total magnetic fields; (b)–(c) x- and z-component electric fields; the corresponding (d) electric and magnetic forces in the x-direction; (e) its velocity and three components; and (f) potential difference from the x- and z-directions and their sum. The black dotted line denotes the shock speed V shock = 5.8 in the downstream frame. The dotted lines denote the times Ω i  t 1 = 5.9, Ω i  t 2 = 6.12, Ω i  t 3 = 6.4, and Ω i  t 4 = 7.5.
Paper: Particle Energization at a High Mach Number Perpendicular Shock: 1D Particle-in-cell Simulations
Authors: Yufei Hao, Zhongwei Yang, Fan Guo, Terry Z. Liu, Xiangliang Kong, Lican Shan, Dejin Wu
Figure caption: Scales of shock foot, x-component magnetic force, x-component electric force at time ﹩{t}_{01}={t}_{0}-0.3{{\rm{\Omega }}}_{i}^{-1}﹩, the minimum v  ix  at time t 0, the potential difference φ  x , φ  z , and kinetic energies at time ﹩{t}_{02}={t}_{0}+1.0{{\rm{\Omega }}}_{i}^{-1}﹩ of all the particles denoted by black dots are shown from the top to bottom panel, where t 0 is the time when each particle gets a minimum v  ix  after being reflected.
Paper: Particle Energization at a High Mach Number Perpendicular Shock: 1D Particle-in-cell Simulations
Authors: Yufei Hao, Zhongwei Yang, Fan Guo, Terry Z. Liu, Xiangliang Kong, Lican Shan, Dejin Wu
Figure caption: From the top to bottom panels, profiles of total magnetic fields, three components of average velocity, three components of electric fields, and phase space (x, v  ix,z ) distributions are shown at time Ω i  t = (a) 4.0 and (b) 4.9. Red dotted lines denote the corresponding downstream average values.
Paper: Particle Energization at a High Mach Number Perpendicular Shock: 1D Particle-in-cell Simulations
Authors: Yufei Hao, Zhongwei Yang, Fan Guo, Terry Z. Liu, Xiangliang Kong, Lican Shan, Dejin Wu
Figure caption: From the top to bottom panel: averaged potential differences of all the followed particles φ  ax , φ  az , and their sum denoted by blue dashed, red dashed, and black solid lines; the ratios of the number of particles with ﹩{v}_{\min }\lt -{V}_{\mathrm{inj}}﹩, ﹩{v}_{\min }\lt -1.5{V}_{\mathrm{inj}}﹩, and ﹩{v}_{\min }\lt -2{V}_{\mathrm{inj}}﹩ denoted by black solid, dashed, and dotted lines; scales of shock foot, cyclic time periods, and propagating speed of shock front for M  A  = 17.8, 12.1, 9.1, 6.8, and 3.6.
Paper: Particle Energization at a High Mach Number Perpendicular Shock: 1D Particle-in-cell Simulations
Authors: Yufei Hao, Zhongwei Yang, Fan Guo, Terry Z. Liu, Xiangliang Kong, Lican Shan, Dejin Wu
Figure caption: Potential differences of all of the particles we followed at time Ω i  t = 7.6 from the (a) x- and (b) z-directions. The black dashed lines indicate the kinetic energy corresponding to the injected flow velocity, and the blue solid lines denote their corresponding average values.
Paper: Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809
Authors: Takuya Midooka, Misaki Mizumoto, Ken Ebisawa
Figure caption: (Cont.) Spectral fitting results of all the spectra except spectrum F in the main text.
Paper: Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809
Authors: Takuya Midooka, Misaki Mizumoto, Ken Ebisawa
Figure caption: Spectral fitting results of all the spectra except the spectrum F in the main text.
Paper: Radiatively Driven Clumpy X-Ray Absorbers in the NLS1 Galaxy IRAS 13224-3809
Authors: Takuya Midooka, Misaki Mizumoto, Ken Ebisawa
Figure caption: Corner plots of the MCMC parameter estimation for all the spectral ratios except the spectral ratio F/A, which is in the main text.
Paper: The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors
Authors: Alexa C. Gordon, Wen-fai Fong, Charles D. Kilpatrick, Tarraneh Eftekhari, Joel Leja, J. Xavier Prochaska, Anya E. Nugent, Shivani Bhandari, Peter K. Blanchard, Manisha Caleb, Cherie K. Day, Adam T. Deller, Yuxin Dong, 雨欣 董, Marcin Glowacki, Kelly Gourdji, Alexandra G. Mannings, Elizabeth K. Mahoney, Lachlan Marnoch, Adam A. Miller, Kerry Paterson, Jillian C. Rastinejad, Stuart D. Ryder, Elaine M. Sadler, Danica R. Scott, Huei Sears, Ryan M. Shannon, Sunil Simha, Benjamin W. Stappers, Nicolas Tejos
Figure caption: New spectroscopic observations included in this work from SOAR/Goodman, Keck/DEIMOS, and Keck/LRIS. Major emission and absorption lines are denoted by colored lines: Balmer lines are in green, oxygen lines are in blue, nitrogen lines are in orange, sulfur lines are in purple, and calcium lines are in pink. The spectra are normalized to the photometry in Prospector. The Prospector-derived redshifts are listed in each panel along with the facility/instrument of observation.
Paper: The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors
Authors: Alexa C. Gordon, Wen-fai Fong, Charles D. Kilpatrick, Tarraneh Eftekhari, Joel Leja, J. Xavier Prochaska, Anya E. Nugent, Shivani Bhandari, Peter K. Blanchard, Manisha Caleb, Cherie K. Day, Adam T. Deller, Yuxin Dong, 雨欣 董, Marcin Glowacki, Kelly Gourdji, Alexandra G. Mannings, Elizabeth K. Mahoney, Lachlan Marnoch, Adam A. Miller, Kerry Paterson, Jillian C. Rastinejad, Stuart D. Ryder, Elaine M. Sadler, Danica R. Scott, Huei Sears, Ryan M. Shannon, Sunil Simha, Benjamin W. Stappers, Nicolas Tejos
Figure caption: Posterior distributions of log(SFR0−100 Myr), log(sSFR0−100 Myr), log(M */M ⊙), log(Z */Z ⊙), t m, A V, young, and A V,old for the full sample. We show the repeater (blue) and nonrepeater (pink) populations separately. While the two populations are similar for most properties, repeaters tend to have lower log(M */M ⊙) than nonrepeaters.
Paper: The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors
Authors: Alexa C. Gordon, Wen-fai Fong, Charles D. Kilpatrick, Tarraneh Eftekhari, Joel Leja, J. Xavier Prochaska, Anya E. Nugent, Shivani Bhandari, Peter K. Blanchard, Manisha Caleb, Cherie K. Day, Adam T. Deller, Yuxin Dong, 雨欣 董, Marcin Glowacki, Kelly Gourdji, Alexandra G. Mannings, Elizabeth K. Mahoney, Lachlan Marnoch, Adam A. Miller, Kerry Paterson, Jillian C. Rastinejad, Stuart D. Ryder, Elaine M. Sadler, Danica R. Scott, Huei Sears, Ryan M. Shannon, Sunil Simha, Benjamin W. Stappers, Nicolas Tejos
Figure caption: Example SED for the host of FRB 20211127I. Top panel: the observed spectrum (light blue) and its associated error spectrum (light gray) are modeled jointly with the observed photometry (blue circles). The best-fit Prospector model spectrum (black) and corresponding model photometry (red squares) are also displayed. Bottom panel: zoom-in of the observed and model spectra following the same color scheme as the top panel. As the nebular emission lines are self-consistently modeled, the Prospector model provides excellent agreement to the spectroscopic data. The remaining SEDs are in Appendix B.
Paper: The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors
Authors: Alexa C. Gordon, Wen-fai Fong, Charles D. Kilpatrick, Tarraneh Eftekhari, Joel Leja, J. Xavier Prochaska, Anya E. Nugent, Shivani Bhandari, Peter K. Blanchard, Manisha Caleb, Cherie K. Day, Adam T. Deller, Yuxin Dong, 雨欣 董, Marcin Glowacki, Kelly Gourdji, Alexandra G. Mannings, Elizabeth K. Mahoney, Lachlan Marnoch, Adam A. Miller, Kerry Paterson, Jillian C. Rastinejad, Stuart D. Ryder, Elaine M. Sadler, Danica R. Scott, Huei Sears, Ryan M. Shannon, Sunil Simha, Benjamin W. Stappers, Nicolas Tejos
Figure caption: Imaging gallery of the 23 FRB hosts included in our sample, with images oriented with north up and east to the left. The host galaxies are marked by the purple crosshairs and the 68% confidence interval FRB localizations are denoted in red by an ellipse. For the three FRBs with milliarcsecond-scale localizations (FRB 20121102A; Marcote et al. 2017; FRB 20180916B; Marcote et al. 2020; and FRB 20201124A; Nimmo et al. 2022) and one with ∼0.″1 localization (FRB 20190520B; Niu et al. 2022), the position is indicated by a plus sign. The facility or survey that discovered the FRB is also listed.
Paper: The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors
Authors: Alexa C. Gordon, Wen-fai Fong, Charles D. Kilpatrick, Tarraneh Eftekhari, Joel Leja, J. Xavier Prochaska, Anya E. Nugent, Shivani Bhandari, Peter K. Blanchard, Manisha Caleb, Cherie K. Day, Adam T. Deller, Yuxin Dong, 雨欣 董, Marcin Glowacki, Kelly Gourdji, Alexandra G. Mannings, Elizabeth K. Mahoney, Lachlan Marnoch, Adam A. Miller, Kerry Paterson, Jillian C. Rastinejad, Stuart D. Ryder, Elaine M. Sadler, Danica R. Scott, Huei Sears, Ryan M. Shannon, Sunil Simha, Benjamin W. Stappers, Nicolas Tejos
Figure caption: Boxplots of the full sample of FRB hosts split by repeater and nonrepeaters derived from 1000 representative samples of the hosts’ posterior probability distributions. The box represents the range between the first and third quartiles, with the median denoted by an orange line. The whiskers denote the maxima and minima, and outliers are represented by circles.
Paper: The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors
Authors: Alexa C. Gordon, Wen-fai Fong, Charles D. Kilpatrick, Tarraneh Eftekhari, Joel Leja, J. Xavier Prochaska, Anya E. Nugent, Shivani Bhandari, Peter K. Blanchard, Manisha Caleb, Cherie K. Day, Adam T. Deller, Yuxin Dong, 雨欣 董, Marcin Glowacki, Kelly Gourdji, Alexandra G. Mannings, Elizabeth K. Mahoney, Lachlan Marnoch, Adam A. Miller, Kerry Paterson, Jillian C. Rastinejad, Stuart D. Ryder, Elaine M. Sadler, Danica R. Scott, Huei Sears, Ryan M. Shannon, Sunil Simha, Benjamin W. Stappers, Nicolas Tejos
Figure caption: The recent star formation rate vs. stellar mass for the full host sample plotted against the COSMOS field galaxies, tracing the star-forming main sequence. We split the sample into three redshift bins (individual panels) to account for evolution in the sequence. Repeaters and nonrepeaters are denoted by stars and squares, respectively. The symbols are color-coded by their Tacchella et al. (2022) classification.
Paper: The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors
Authors: Alexa C. Gordon, Wen-fai Fong, Charles D. Kilpatrick, Tarraneh Eftekhari, Joel Leja, J. Xavier Prochaska, Anya E. Nugent, Shivani Bhandari, Peter K. Blanchard, Manisha Caleb, Cherie K. Day, Adam T. Deller, Yuxin Dong, 雨欣 董, Marcin Glowacki, Kelly Gourdji, Alexandra G. Mannings, Elizabeth K. Mahoney, Lachlan Marnoch, Adam A. Miller, Kerry Paterson, Jillian C. Rastinejad, Stuart D. Ryder, Elaine M. Sadler, Danica R. Scott, Huei Sears, Ryan M. Shannon, Sunil Simha, Benjamin W. Stappers, Nicolas Tejos
Figure caption: log(sSFR0−100 Myr) vs. t m of FRB host galaxies compared to COSMOS field galaxies for three redshift bins. The parameter space is divided into star-forming, transitioning, and quiescent following the Tacchella et al. (2022) classification. Repeaters are denoted by stars, and nonrepeaters are denoted by squares. Both are color-coded by their classification type. Error bars correspond to 68% confidence. While FRB 20210807D is on the borderline between transitioning (445 model draws) and quiescent (555 model draws), the mode favors a quiescent classification and is thus classified as such.
Paper: The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors
Authors: Alexa C. Gordon, Wen-fai Fong, Charles D. Kilpatrick, Tarraneh Eftekhari, Joel Leja, J. Xavier Prochaska, Anya E. Nugent, Shivani Bhandari, Peter K. Blanchard, Manisha Caleb, Cherie K. Day, Adam T. Deller, Yuxin Dong, 雨欣 董, Marcin Glowacki, Kelly Gourdji, Alexandra G. Mannings, Elizabeth K. Mahoney, Lachlan Marnoch, Adam A. Miller, Kerry Paterson, Jillian C. Rastinejad, Stuart D. Ryder, Elaine M. Sadler, Danica R. Scott, Huei Sears, Ryan M. Shannon, Sunil Simha, Benjamin W. Stappers, Nicolas Tejos
Figure caption: Star formation histories (SFHs) of all FRB host galaxies in the sample. The x-axis is the lookback time, such that the left-hand side is the age of the Universe at the redshift of the galaxy, and the right-hand side is the present day. The SFHs are color-coded by SFH type: rising (purple), delayed-τ exponentially declining (teal), τ-linear exponentially declining (green), post-starburst (yellow), and rejuvenating (orange). We denote repeating FRBs with an (R) in the titles.
Paper: The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors
Authors: Alexa C. Gordon, Wen-fai Fong, Charles D. Kilpatrick, Tarraneh Eftekhari, Joel Leja, J. Xavier Prochaska, Anya E. Nugent, Shivani Bhandari, Peter K. Blanchard, Manisha Caleb, Cherie K. Day, Adam T. Deller, Yuxin Dong, 雨欣 董, Marcin Glowacki, Kelly Gourdji, Alexandra G. Mannings, Elizabeth K. Mahoney, Lachlan Marnoch, Adam A. Miller, Kerry Paterson, Jillian C. Rastinejad, Stuart D. Ryder, Elaine M. Sadler, Danica R. Scott, Huei Sears, Ryan M. Shannon, Sunil Simha, Benjamin W. Stappers, Nicolas Tejos
Figure caption: Luminosity–redshift distribution for all FRB hosts to date. We denote repeaters by blue stars and nonrepeaters by pink squares. We also include FRB hosts from the literature that did not meet our sample criteria as open symbols.
Paper: The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors
Authors: Alexa C. Gordon, Wen-fai Fong, Charles D. Kilpatrick, Tarraneh Eftekhari, Joel Leja, J. Xavier Prochaska, Anya E. Nugent, Shivani Bhandari, Peter K. Blanchard, Manisha Caleb, Cherie K. Day, Adam T. Deller, Yuxin Dong, 雨欣 董, Marcin Glowacki, Kelly Gourdji, Alexandra G. Mannings, Elizabeth K. Mahoney, Lachlan Marnoch, Adam A. Miller, Kerry Paterson, Jillian C. Rastinejad, Stuart D. Ryder, Elaine M. Sadler, Danica R. Scott, Huei Sears, Ryan M. Shannon, Sunil Simha, Benjamin W. Stappers, Nicolas Tejos
Figure caption: SED of FRB 20121102A.
Paper: The Demographics, Stellar Populations, and Star Formation Histories of Fast Radio Burst Host Galaxies: Implications for the Progenitors
Authors: Alexa C. Gordon, Wen-fai Fong, Charles D. Kilpatrick, Tarraneh Eftekhari, Joel Leja, J. Xavier Prochaska, Anya E. Nugent, Shivani Bhandari, Peter K. Blanchard, Manisha Caleb, Cherie K. Day, Adam T. Deller, Yuxin Dong, 雨欣 董, Marcin Glowacki, Kelly Gourdji, Alexandra G. Mannings, Elizabeth K. Mahoney, Lachlan Marnoch, Adam A. Miller, Kerry Paterson, Jillian C. Rastinejad, Stuart D. Ryder, Elaine M. Sadler, Danica R. Scott, Huei Sears, Ryan M. Shannon, Sunil Simha, Benjamin W. Stappers, Nicolas Tejos
Figure caption: SED of FRB 20180301A.