adsabs/AstroCLIMB huggingface dataset:
Paper: A Gradual Decline of Star Formation since Cluster Infall: New Kinematic Insights into Environmental Quenching at 0.3 < z < 1.1
Authors: Keunho J. Kim, Matthew B. Bayliss, Allison G. Noble, Gourav Khullar, Ethan Cronk, Joshua Roberson, Behzad Ansarinejad, Lindsey E. Bleem, Benjamin Floyd, Sebastian Grandis, Guillaume Mahler, Michael A. McDonald, Christian L. Reichardt, Alexandro Saro, Keren Sharon, Taweewat Somboonpanyakul, Veronica Strazzullo
Figure caption: Left: sample cluster mass distribution with redshift. Due to the uniform selection function based on the redshift-independent SZ effect, our sample clusters are nearly mass-limited at all redshifts, forming a relatively narrow mass range with a median (standard deviation) mass of 4.97 (±2.24)  ×  1014 M ⊙ (Section 2.1). Right: i-band luminosity (L  i /L*, relative to the characteristic luminosity) distribution of sample cluster galaxies with redshift. The dark blue points are the sample galaxies used after applying the luminosity cut of L  i /L*  > 0.35, while the light blue points are the ones excluded. The numbers of sample clusters and cluster galaxies considered in this study are marked in the top right corner in the left and right panels, respectively. See also Table 1 and Section 3.1 for details on the sample selection.
Paper: A Gradual Decline of Star Formation since Cluster Infall: New Kinematic Insights into Environmental Quenching at 0.3 < z < 1.1
Authors: Keunho J. Kim, Matthew B. Bayliss, Allison G. Noble, Gourav Khullar, Ethan Cronk, Joshua Roberson, Behzad Ansarinejad, Lindsey E. Bleem, Benjamin Floyd, Sebastian Grandis, Guillaume Mahler, Michael A. McDonald, Christian L. Reichardt, Alexandro Saro, Keren Sharon, Taweewat Somboonpanyakul, Veronica Strazzullo
Figure caption: Diagram showing that the fraction of quiescent galaxies (f Q) increases with infall time proxy. Each panel shows the same relationship but for different redshift ranges, as indicated on the tops of the panels. Quiescent galaxies are defined as Dn4000  > 1.55. The f Q are calculated in bins of 0.25 or 0.5 dex (smaller bin size adopted for crowded infall bins) of infall proxy (﹩\mathrm{log}[({r}_{\mathrm{proj}}/{r}_{500})\,\times \,({\rm{\Delta }}v/{\sigma }_{\mathrm{cl}}﹩)). The error bars indicate 1σ uncertainties based on Poisson statistics. There is an increasing f Q with infall proxy in all panels (i.e., regardless of redshift), although the low-z galaxies (middle panel) show a systematically higher f Q compared to the high-z galaxies (right panel) for any given infall bin (see Section 4.3 for the redshift dependence of environmental quenching trends). The increasing quiescent fraction of galaxies with infall time proxy suggests that galaxies become quiescent due to longer exposure to environmental effects.
Paper: A Gradual Decline of Star Formation since Cluster Infall: New Kinematic Insights into Environmental Quenching at 0.3 < z < 1.1
Authors: Keunho J. Kim, Matthew B. Bayliss, Allison G. Noble, Gourav Khullar, Ethan Cronk, Joshua Roberson, Behzad Ansarinejad, Lindsey E. Bleem, Benjamin Floyd, Sebastian Grandis, Guillaume Mahler, Michael A. McDonald, Christian L. Reichardt, Alexandro Saro, Keren Sharon, Taweewat Somboonpanyakul, Veronica Strazzullo
Figure caption: Schematic diagram showing the orbit of an infalling galaxy into a cluster. This is illustrated in 3D (left) and 2D projected (right) phase space (i.e., peculiar velocity vs. clustercentric radius). Moving from stages 1 to 4, (1) an infalling galaxy plunges into the gravitational potential of the cluster, (2) passes the pericenter, (3) backsplashes, and eventually becomes (4) virialized. This simplified orbit of an infalling galaxy is qualitatively consistent with that of an infalling galaxy traced in cluster simulations (e.g., see Figure 4 of Jaffé et al. 2015). This figure illustrates how a galaxy orbit is statistically traced in a phase space diagram during infall (see also Figure 3 for the projected phase space of our sample galaxies).
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. II. Evolution of a UV-bright Underlying Source 2–4 Yr Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, M. R. Magee
Figure caption: The HST SEDs of the underlying source (dereddened from Galactic extinction) and best-fit power laws (dotted lines) and blackbodies (dashed lines), as well as the 3σ Swift-XRT upper limits (downward triangles), assuming a power law and fiducial photon indices Γ. The shaded regions represent 1σ uncertainties for the best-fit blackbodies. In the zoomed-in plot, the HST SED of AT 2018cow at t ≃ 60.1 days with brightness lowered by a factor of 20 is also shown for comparison. Although the optical emission seems relatively stable, the fading UV emission confirms the transient nature of the underlying source.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. II. Evolution of a UV-bright Underlying Source 2–4 Yr Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, M. R. Magee
Figure caption: Parameter space ﹩\dot{M}﹩ vs. M BH for the disk blackbody model representing an accreting BH scenario. ﹩\dot{M}﹩ values derived from fitting the HST SED at t ≃ 1453 days are shown in blue (with errors shown as shaded regions), while values derived from the Swift-XRT upper limit are shown in black. Three fiducial θ values were considered: 0◦ (solid lines), 40◦ (dashed lines), and 80◦ (dotted lines). The Eddington accretion rates are also shown in orange, considering three fiducial values of the radiative efficiency ϵ: 0.01 (solid lines), 0.1 (dashed lines), and 0.4 (dotted lines). A vertical dashed line is shown to indicate the limiting M BH < 850 M ⊙ derived from the NICER QPO (Pasham et al. 2021).
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. II. Evolution of a UV-bright Underlying Source 2–4 Yr Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, M. R. Magee
Figure caption: Extrapolated disk blackbody models at t ≃ 703 days (dashed lines) and t ≃ 1119 days (dotted lines), based on the best-fit models at t ≃ 1453 days (solid lines). The observed (dereddened) HST SEDs are also shown for reference. The top and bottom panels show models for M BH = 10 M ⊙ and M BH = 106 M ⊙, respectively. The left panels assume θ = 0° for the best-fit models, with θ fixed for the extrapolations. The right panels assume θ = 80° for the best-fit models, with θ being a free parameter for the extrapolations and θ fit being the best-fit value that matches the observed amplitude.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. II. Evolution of a UV-bright Underlying Source 2–4 Yr Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, M. R. Magee
Figure caption: CSM density profile used in our ejecta–CSM interaction model (top panels) and the forward- and reverse-shock properties derived from the model (bottom three panels). See the text for details regarding our model. The three HST epochs are marked with gray dashed lines. We also show ﹩{L}_{\mathrm{UVO},\min }﹩ (triangles), and a key finding here is that ﹩{L}_{\mathrm{UVO},\min }﹩ is orders of magnitude above the L rad.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. II. Evolution of a UV-bright Underlying Source 2–4 Yr Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, M. R. Magee
Figure caption: Left: observed (dereddened) HST SED at t ≃ 1453 days compared with BPASS clusters and selected LEGUS clusters. The BPASS clusters come from the default model, which assumes an initial mass function with a power-law slope of −1.30 between 0.1–0.5 M ⊙ and −2.35 above 0.5 M ⊙, extending to a maximum mass of 300 M ⊙. Right: observed (dereddened) HST SEDs and the difference SED calculated by taking the difference between the HST SEDs observed at t ≃ 703 days and 1453 days. The difference SED corresponds to the transient component at t ≃ 703 days if the HST SED at t ≃ 1453 days is solely from a stellar source.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. II. Evolution of a UV-bright Underlying Source 2–4 Yr Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, M. R. Magee
Figure caption: Magnetar parameter space with the surface magnetic field strength B and the initial spin period P 0. Lines of constant spin-down luminosity L sd are shown for ﹩{L}_{\mathrm{sd}}={L}_{\mathrm{UVO},\min }﹩, ﹩10{L}_{\mathrm{UVO},\min }﹩, and ﹩100{L}_{\mathrm{UVO},\min }﹩ (green, yellow, and blue). The solid and dashed lines indicate ﹩{L}_{\mathrm{UVO},\min }﹩ values derived from t ≃ 703 days and 1453 days, respectively. A purple region is shown for magnetar parameters that could power the optical peak of AT 2018cow (Margutti et al. 2019).
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. II. Evolution of a UV-bright Underlying Source 2–4 Yr Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, M. R. Magee
Figure caption: The HST SEDs of the underlying source at t ≃ 703 days and 1453 days, the best-fit power law (PL) at t ≃ 703 days, and the reddened power law with E B−V ≃ 0.072 assuming the Cardelli extinction law. Extinction can account for the observed fading in the UV.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. II. Evolution of a UV-bright Underlying Source 2–4 Yr Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, M. R. Magee
Figure caption: Disk blackbody fits to the latest HST SED of the underlying source at t ≃ 1453 days. All three (dereddened) HST SEDs are also shown for reference. The order-of-magnitude estimates of the upper limit L  ν  derived from the Swift-XRT nondetection at t ≃ 1360 days are also shown. The horizontal span of the limit represents the range of 0.3 − 10 keV, while the vertical span represents the range of L  ν  derived from the range of M BH.
Paper: Global Electron Thermodynamics in Radiatively Inefficient Accretion Flows
Authors: Kaushik Satapathy, Dimitrios Psaltis, Feryal Özel
Figure caption: The electron heating fraction, Q  e /(Q  i  + Q  e ), as a function of the plasma β, as calculated by Kawazura et al. (2020) for different values of the relative driving power of compressive and Alfvénic waves, P comp/P A. The width of each curve represents the range of heating ratios for different ion-to-electron temperature ratios (1 ≤ T  i /T  e  ≤ 100) and illustrates the weak dependence on this quantity. The cyan curve corresponds to the earlier analytical calculation by Howes (2011), which did not incorporate compressive waves. The typical values of plasma β found in the midplane regions of GRMHD simulations are shown by the shaded region in gray.
Paper: Global Electron Thermodynamics in Radiatively Inefficient Accretion Flows
Authors: Kaushik Satapathy, Dimitrios Psaltis, Feryal Özel
Figure caption: Top: ion (dashed blue) and electron (solid blue) temperatures in units of ion rest mass energy as a function of radial distance, for a mass accretion rate of ﹩\dot{M}={10}^{-4}{\dot{M}}_{{\rm{E}}}﹩, plasma β = 5, n  R  = 1.5, and neglecting radiative cooling effects. The black solid line shows the electron temperature profile if electrons were heated purely through Coulomb collisions with the ions. In the absence of direct heating from turbulence, the electron temperature in the inner accretion flow increases only as a result of adiabatic compressional heating, as shown with the red dashed line. Bottom: the ion-to-electron temperature ratio, T  i /T  e , as a function of radial distance for the same calculation.
Paper: Global Electron Thermodynamics in Radiatively Inefficient Accretion Flows
Authors: Kaushik Satapathy, Dimitrios Psaltis, Feryal Özel
Figure caption: Top: the ion (dashed) and electron (solid) temperatures in units of the ion rest mass energy as a function of radial distance for a flow with accretion rate ﹩\dot{M}\ll {10}^{-7}{\dot{M}}_{{\rm{E}}}﹩, plasma β = 5, and a radial velocity profile index of n  R  = 1.5, in the absence of the radiative cooling of the electrons. The dotted lines indicate approximate analytical solutions for different values of the adiabatic indices γ. In the inner accretion flow, where the electrons become relativistic, their temperature profile shifts toward the relativistic (γ  e  = 4/3) solution. Bottom: the ion-to-electron temperature ratio as a function of radial distance for the same calculation.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. I. Further Constraints on the Fading Prompt Emission and Thermal Properties 50–60 days Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, Kirsty Taggart, Matthew R. Siebert, M. R. Magee
Figure caption: Wind mass-loss rate ﹩{\dot{M}}_{{\rm{w}}}﹩ (top panel), photosphere radius R ph (second panel), wind velocity v w (third panel), and luminosity at equipartition radius L eq (bottom panel) derived using observed properties of AT 2018cow based on the wind-reprocessed transient model from Uno & Maeda (2020). A power-law fit to the wind mass-loss rate after t ∼ 15 days is also shown on the top panel. A shaded region is shown on the third panel to indicate the observed emission-line velocity 3000 km s−1 ≲ v ≲ 6000 km s−1. Observed properties are also plotted for comparisons with R ph and L eq.
Paper: Global Electron Thermodynamics in Radiatively Inefficient Accretion Flows
Authors: Kaushik Satapathy, Dimitrios Psaltis, Feryal Özel
Figure caption: Top: ion (dashed) and electron (solid) temperatures in units of the ion rest mass energy as a function of radial distance, for plasma β = 5 and n  R  = 1.5, at different accretion rates, neglecting the effects of radiative cooling for the electrons. At the higher accretion rates shown, Coulomb collisions cause the ion and electron temperatures to equilibrate at large radii. Bottom: the ion-to-electron temperature ratio, T  i /T  e , as a function of radial distance for the same calculation.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. I. Further Constraints on the Fading Prompt Emission and Thermal Properties 50–60 days Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, Kirsty Taggart, Matthew R. Siebert, M. R. Magee
Figure caption: The observed (dereddened) SEDs of AT 2018cow (black circles) and the best-fit models (solid lines) derived from fitting the BLACKBODY + DUST model. The six chosen epochs all have JHK measurements that provide better constraints on the excess IR emission. Photometry excluded from the fit is shown in gray (see text for reasoning). The dust model generally provides a reasonable fit to the observed excess IR emission. More importantly, the UV–optical continuum is almost exclusively from the hot blackbody and unaffected by the dust model.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. I. Further Constraints on the Fading Prompt Emission and Thermal Properties 50–60 days Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, Kirsty Taggart, Matthew R. Siebert, M. R. Magee
Figure caption: Kast and LRIS spectra of AT 2018cow over t ≃ 2–59 days, showing an initial featureless spectrum with emerging intermediate-width lines at t ≳ 15 days.
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. I. Further Constraints on the Fading Prompt Emission and Thermal Properties 50–60 days Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, Kirsty Taggart, Matthew R. Siebert, M. R. Magee
Figure caption: High-resolution APF and Kast spectra in the velocity space centered at Hα in the rest frame relative to the host redshift.
Paper:  ESCARGOT: Mapping Vertical Phase Spiral Characteristics Throughout the Real and Simulated Milky Way
Authors: Elise Darragh-Ford, Jason A. S. Hunt, Adrian M. Price-Whelan, Kathryn V. Johnston
Figure caption: Left: distribution of interaction times, t 0, recovered from application of ESCARGOT to phase spirals in the idealized simulation. The dark green histogram shows all of the bins, while the blue shows only bins with a well-measured fit (σ  t  < 100 Myr), which approximately corresponds to J  ϕ  > 2000 (km s−1 kpc−1). The dashed lines mark the median of both the full (dark green) and restricted (blue) samples. The magenta dashed line shows the actual time since dwarf disk crossing. Right: distribution of interaction times (t 0) recovered from the simulation as a function of x  act –y  act  (See Equation (4).). The dashed black circle marks 2000 = J  ϕ  (km s−1 kpc−1), within which most of the spirals are poorly resolved. The cutout displays a zoom-in on −2500 < x act, y act < −1500 (kpc km s−1) to show the fine-grained structure.
Paper:  ESCARGOT: Mapping Vertical Phase Spiral Characteristics Throughout the Real and Simulated Milky Way
Authors: Elise Darragh-Ford, Jason A. S. Hunt, Adrian M. Price-Whelan, Kathryn V. Johnston
Figure caption: Steps in ESCARGOT. Top: mode determination using a Fourier transform. Stars are binned in R  z –θ  z  (left). For each bin in R  z , we compute a Fourier transform with respect to θ  z  and measure the strength of the m = 1 and m = 2 modes relative to the background m = 0 mode (right). Middle: ridgeline extraction using a peak-finding algorithm. The peaks are extracted in 1D bins of θ  z  (colored lines, left) with a minimum threshold of 0.05 in residual counts. The lines are colored by the median θ  z  for each bin and range from [0, 2π]. The peaks are plotted as black dots as a function of R  z  (left) and on top of the background-subtracted phase spiral (right). Bottom: a fit to the ridgeline using the Hough transform. We find the best-fit line (red) to the extracted ridgeline (blue points) using a combination of the Hough transform and least-squares error.
Paper:  ESCARGOT: Mapping Vertical Phase Spiral Characteristics Throughout the Real and Simulated Milky Way
Authors: Elise Darragh-Ford, Jason A. S. Hunt, Adrian M. Price-Whelan, Kathryn V. Johnston
Figure caption: Analysis of simulated data (static potential)—center panel: background-subtracted phase spirals as a function of (J  ϕ , −θ  ϕ ). Frame: ridgeline fits to the spirals projected into θ  z −Ω z  for different θ  ϕ  (right panels) and J  ϕ  (bottom panels) bins. The lighter lines represent the fit to the data after bootstrap resampling. The center panel shows the smooth variation in phase spiral morphology as a function of (J  ϕ , −θ  ϕ ). In the bottom (left) panels the subtle shifts in phase spiral slope and phase angle as a function of θ  ϕ  (J  ϕ ) can be seen.
Paper:  ESCARGOT: Mapping Vertical Phase Spiral Characteristics Throughout the Real and Simulated Milky Way
Authors: Elise Darragh-Ford, Jason A. S. Hunt, Adrian M. Price-Whelan, Kathryn V. Johnston
Figure caption: The Gaia phase spiral in stellar number counts (left and center panels) and a Gaussian-smoothed and background-subtracted representation (right panel). The coordinates in the middle panel are computed by transforming to action–angle coordinates (J  z , θ  z ) and defining ﹩{R}_{z}\equiv \sqrt{{J}_{z}}﹩. The color bar in the right panel has units of residual stellar number counts (and is linearly scaled). The phase spiral shown is centered at J  ϕ  = 1800 ± 30 kpc km s−1 and θ  ϕ  = 3.1 ± 0.05 rad.
Paper: Modeling of Transverse Oscillations Driven by p-modes in Short Coronal Loops
Authors: Yuhang Gao, 宇航 高, Mingzhe Guo, Tom Van Doorsselaere, Hui Tian, Samuel J. Skirvin
Figure caption: Similar to Figure 2 but for the transverse velocity perturbation v  x .
Paper: Modeling of Transverse Oscillations Driven by p-modes in Short Coronal Loops
Authors: Yuhang Gao, 宇航 高, Mingzhe Guo, Tom Van Doorsselaere, Hui Tian, Samuel J. Skirvin
Figure caption: (A) Horizontal velocity along the loop axis at several time steps, with solid lines representing v  x  and dashed lines representing v  y  (multiplied by 10 because the value of v  y  is very low). (B) Transverse displacement of the loop obtained from considering the center of mass. (C) and (D) The cross-section profiles of the normalized density at z = 0 (loop apex) at t = 980.9 s and t = 1121.0 s, with the horizontal velocity marked by white arrows.
Paper: Modeling of Transverse Oscillations Driven by p-modes in Short Coronal Loops
Authors: Yuhang Gao, 宇航 高, Mingzhe Guo, Tom Van Doorsselaere, Hui Tian, Samuel J. Skirvin
Figure caption: The top two panels present the profiles of temperature (black) and number density (blue) along the loop axis (z-direction) before (A) and after (B) the 2D relaxation. The horizontal axis “Height” is actually the increase in z with respect to the footpoint. The solid and dashed lines represent the values inside and outside the loop. Panel (C) shows the 3D loop configuration.
Paper: Modeling of Transverse Oscillations Driven by p-modes in Short Coronal Loops
Authors: Yuhang Gao, 宇航 高, Mingzhe Guo, Tom Van Doorsselaere, Hui Tian, Samuel J. Skirvin
Figure caption: (A) Space–time plot for longitudinal velocity perturbation v  z  at the loop axis. (B) Time series of v  z  at the loop apex (z = 0), corresponding to the dashed black line in (A). (C) and (D) Wavelet analysis results of the time series shown in (B). A darker color represents a larger wavelet power. The dashed lines denote a 95% significance level.
Paper: Modeling of Transverse Oscillations Driven by p-modes in Short Coronal Loops
Authors: Yuhang Gao, 宇航 高, Mingzhe Guo, Tom Van Doorsselaere, Hui Tian, Samuel J. Skirvin
Figure caption: (A) The Alfvén speed c A and sound speed c s along the loop axis. (B) and (C) Similar to panel (A) of Figures 2 and 3, but we use blue dotted lines and green dashed lines to show the Alfvén speed and sound speed, respectively.
Paper: Modeling of Transverse Oscillations Driven by p-modes in Short Coronal Loops
Authors: Yuhang Gao, 宇航 高, Mingzhe Guo, Tom Van Doorsselaere, Hui Tian, Samuel J. Skirvin
Figure caption: (A) The global wavelet power derived from time series of v  x  at different positions (z) along the loop axis. (B) The global wavelet power at the period of 54 s along the loop axis. (C)–(E) Similar to Figures 3(B)–(D) but for v  x  at the loop leg (z = 11 Mm) rather than the loop apex.
Paper: Modeling of Transverse Oscillations Driven by p-modes in Short Coronal Loops
Authors: Yuhang Gao, 宇航 高, Mingzhe Guo, Tom Van Doorsselaere, Hui Tian, Samuel J. Skirvin
Figure caption: Global wavelet spectrum for a period range of 0–120 s for cases of different inclination angles (θ). (A) θ = 90°. (B) θ = 15°. A 95% significance level is also indicated in both panels with dashed lines.