adsabs/AstroCLIMB huggingface dataset:
Paper: Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
Authors: Thomas Pfeil, Tilman Birnstiel, Hubert Klahr
Figure caption: Row a: RADMC-3D intensity maps of our VSI simulation with v fr = 100 cm s−1 and α = 10−3, seen edge-on. Rows b, c, and d show intensity maps calculated from analytic dust distribution that assume different diffusivities δ. The grain sizes are identical in all simulations. We convolve the images with a typical ALMA beam with FWHM of 35 mas for a distance of 100 pc shown as a gray circle. Hatched areas mark regions that have optical depth τ ≥ 1. Horizontal hatches correspond to areas for which the τ = 1 surface lies on the far side of the disk. Diagonally hatched regions mark τ = 1 surfaces that lie on the observer’s side of the disk. The right panels show minor-axis cuts through the images along the vertical lines in the intensity maps. Purple lines in all plots are the minor-axis cuts from the VSI simulation (panel (a)).
Paper: Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
Authors: Thomas Pfeil, Tilman Birnstiel, Hubert Klahr
Figure caption: Radial dependency of the turbulent Mach numbers in a polar and time Favre average over 200 orbits in our VSI simulations. VSI simulations based on DustPy models with larger particles have lower levels of turbulence. For our model with the largest particles v fr = 400 cm s−1 and α = 10−3, the outer disk, beyond 80 au, is completely quiescent. The three dashed horizontal lines show the Mach numbers corresponding to the three α values that we assumed for our coagulation models (see Equation (10)). Note that such a conversion assumes a perfect Kolmogorov turbulence spectrum (see discussion in Section 6).
Paper: Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
Authors: Thomas Pfeil, Tilman Birnstiel, Hubert Klahr
Figure caption: Origin of the double-peaked intensity profiles in Figures 9 and 10. The τ = 1 surfaces for the layers above the midplane lie closer to the central star owing to the lower densities. The respectively higher temperatures lead to higher intensities above the midplane. Here shown are the τ = 1 surfaces for row c in Figure 9.
Paper: Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
Authors: Thomas Pfeil, Tilman Birnstiel, Hubert Klahr
Figure caption: Cooling time maps in our five VSI PLUTO simulations on the left-hand side, the residuals between the fit used in our simulations, and the actual cooling time distributions derived from DustPy simulations.
Paper: Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
Authors: Thomas Pfeil, Tilman Birnstiel, Hubert Klahr
Figure caption: Total dust-to-gas ratios in VSI simulations restarted after 425 orbits with four passive dust fluids. Each simulation is started with a dust distribution similar to the one derived from the respective DustPy simulations. Snapshots are taken after 150 orbits of evolution. White contours mark the position at which the critical cooling time for the VSI is reached (Equation (3)), i.e., VSI is theoretically possible within the white lobes.
Paper: Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
Authors: Thomas Pfeil, Tilman Birnstiel, Hubert Klahr
Figure caption: Radially and time-averaged dust-to-gas ratios in the inner and outer parts of our simulations. The inner regions are VSI active, forming plateau-like dust distributions in all simulations with a cutoff at the edges of the VSI-active zones. The outer disk regions appear much more settled in the cases of v fr = 200 cm s−1 and v fr = 400 cm s−1, in which the outer regions are quiescent.
Paper: New Resonance Scattering Model in AtomDB: Application to Line Suppression in Galaxy Clusters and Elliptical Galaxies
Authors: Priyanka Chakraborty, Adam Foster, Randall Smith, Nancy Brickhouse, John Raymond
Figure caption: Top: X-ray spectrum of the elliptical galaxy NGC 4636 observed by RGS/XMM-Newton within the energy range 0.33–2.5 keV using m1(=tbabs∗bapec, blue line) and m2 (=tbabs∗rsapec, red line) Bottom: The same spectrum fitted with m1 and m2 within a narrower energy range (0.8–0.85 keV) around the optically thick Fe XVII line.
Paper: New Resonance Scattering Model in AtomDB: Application to Line Suppression in Galaxy Clusters and Elliptical Galaxies
Authors: Priyanka Chakraborty, Adam Foster, Randall Smith, Nancy Brickhouse, John Raymond
Figure caption: Left: X-ray spectrum of the Perseus cluster core (outer region) fitted with m1(=tbabs∗bapec, blue line) and m2 (=tbabs∗rsapec, red line) within the energy range 6.0–7.0 keV. Right: The same spectrum fitted with m1 and m2 within a narrower energy range (6.5–6.6 keV) around the Fe Kα complex.
Paper: Structure of a Quasi-parallel Shock Front
Authors: Michael A. Balikhin, Michael Gedalin, Simon N. Walker, Oleksiy V. Agapitov, Tielong Zhang
Figure caption: The total normalized magnetic field b = ∣ B ∣/B  u  (black line) and the two perpendicular components, b  z  = B  z /B  u  (red) and b  y  = B  y /B  u  (blue). Top left: θ  Bn  = 60°, M = 2.13. Top right: θ  Bn  = 45°, M = 2.09. Bottom left: θ  Bn  = 30°, M = 2.05. Bottom right: θ  Bn  = 15°, M = 2.01. Other parameters: β = 0.2, M  F  = 2.
Paper: Structure of a Quasi-parallel Shock Front
Authors: Michael A. Balikhin, Michael Gedalin, Simon N. Walker, Oleksiy V. Agapitov, Tielong Zhang
Figure caption: Three-dimensional plot of the evolution of the magnetic field component orthogonal to the shock normal  B  ⊥ = B  l   l   a  + B  m   m   a , as observed during the first Venusian bow shock crossing on 2011 December 15.
Paper: Structure of a Quasi-parallel Shock Front
Authors: Michael A. Balikhin, Michael Gedalin, Simon N. Walker, Oleksiy V. Agapitov, Tielong Zhang
Figure caption: Three-dimensional plot of the evolution of the magnetic field component orthogonal to the shock normal  B  ⊥ = B  l   l   a  + B  m   m   a , as observed during the third Venusian bow shock crossing on 2011 December 15.
Paper: Structure of a Quasi-parallel Shock Front
Authors: Michael A. Balikhin, Michael Gedalin, Simon N. Walker, Oleksiy V. Agapitov, Tielong Zhang
Figure caption: Three-dimensional plot of the evolution of the magnetic field component orthogonal to the shock normal, for the analytical solution with θ  Bn  = 15° and M = 2.01.
Paper: Structure of a Quasi-parallel Shock Front
Authors: Michael A. Balikhin, Michael Gedalin, Simon N. Walker, Oleksiy V. Agapitov, Tielong Zhang
Figure caption: Three-dimensional plot of the evolution of the magnetic field component orthogonal to the shock normal  B  ⊥ = B  l   l   a  + B  m   m   a , as observed during the second Venusian bow shock crossing on 2011 December 15.
Paper: Enthalpy of the N+ + H2 → NH+ + H Reaction—Experimental Study of the Reverse Process
Authors: Štěpán Roučka, Serhiy Rednyk, Thuy Dung Tran, Artem Kovalenko, Dmytro Mulin, Sunil S. Kumar, Petr Dohnal, Radek Plašil, Juraj Glosík
Figure caption: Energy levels of the NH2 + system. The energies of the reactants as a function of the N+ fine-structure state (j  a ) and H2 rotational state (﹩{J}_{{{\rm{H}}}_{2}}﹩) are indicated on the left. The energies of the products as a function of the NH+ rotational state are shown for the two lowest electronic states of NH+. The rotational states of NH+ are labeled by the rotational angular momentum quantum number ﹩{N}_{{\mathrm{NH}}^{+}}﹩. See the text for details of the internal structure calculations. The present value of ΔE 0 = 17.6 meV is indicated in the figure.
Paper: Structure of a Quasi-parallel Shock Front
Authors: Michael A. Balikhin, Michael Gedalin, Simon N. Walker, Oleksiy V. Agapitov, Tielong Zhang
Figure caption: Three components and the magnitude of the magnetic field in the shock coordinate system, based on  n  MV as observed during the third Venusian bow shock crossing on 2011 December 15.
Paper: Structure of a Quasi-parallel Shock Front
Authors: Michael A. Balikhin, Michael Gedalin, Simon N. Walker, Oleksiy V. Agapitov, Tielong Zhang
Figure caption: Three components and the magnitude of the magnetic field in the shock coordinate system, based on  n  MV as observed during the second Venusian bow shock crossing on 2011 December 15.
Paper: Bridging the Gap between Cosmic Dawn and Reionization Favors Models Dominated by Faint Galaxies
Authors: Ankita Bera, Sultan Hassan, Aaron Smith, Renyue Cen, Enrico Garaldi, Rahul Kannan, Mark Vogelsberger
Figure caption: Posterior distributions for the escape fraction of ionizing photons f esc and power-law index C as constrained by the ionizing emissivity (﹩{\dot{N}}_{\mathrm{ion}};﹩ left), IGM neutral fraction (x H I;  middle), and Thomson optical depth (τ; right). The orange line in each plot denotes the value of parameter C obtained in Table 1 for z ∼ 5–20 for reference. The emissivity and optical depth do not provide tight constraints on our parameters because of the large uncertainties. The IGM neutral fraction measurements provide tighter constraints on our parameters and favor models with low f esc and positive C values, suggesting that reionization is driven by massive (bright) galaxies.
Paper: Bridging the Gap between Cosmic Dawn and Reionization Favors Models Dominated by Faint Galaxies
Authors: Ankita Bera, Sultan Hassan, Aaron Smith, Renyue Cen, Enrico Garaldi, Rahul Kannan, Mark Vogelsberger
Figure caption: Top: Redshift evolution of the ionizing emissivity, ﹩{\dot{N}}_{\mathrm{ion}}﹩, as predicted by our models, EoR (solid blue) and CD+EoR (solid red), along with the observational constraint by Becker & Bolton (2013). The dotted blue and red curves show the THESAN-HIGH and THESAN-LOW simulations, respectively. Middle: The neutral hydrogen fraction, x H I, as compared to the data listed in Section 4.2. Bottom: The Thomson optical depth, τ, as compared to the Planck Collaboration et al. (2020) measurement (black line) with 1σ uncertainty (gray shaded region). Massive galaxy-dominated models (blue) favor a gradually increasing emissivity, which in turn produces a later onset of reionization, a more sudden and shorter duration, and a lower optical depth. Faint galaxy-dominated models (red) favor a nearly flat emissivity evolution with the opposite characteristics.
Paper: Bridging the Gap between Cosmic Dawn and Reionization Favors Models Dominated by Faint Galaxies
Authors: Ankita Bera, Sultan Hassan, Aaron Smith, Renyue Cen, Enrico Garaldi, Rahul Kannan, Mark Vogelsberger
Figure caption: Left panel: The ionization rates for different C values at z ∼ 17 (solid) and z ∼ 6 (dashed) while fixing other parameters to values of ﹩A={10}^{40}\,{M}_{\odot }^{-1}{{\rm{s}}}^{-1}﹩, B = 108 M ⊙, and D = 2.28 as derived from radiative transfer simulations (Hassan et al. 2016). This shows that positive and negative C correspond to higher ionization rate efficiencies from massive and low-mass halos, respectively. Right panel: The ionization rates multiplied by the Sheth–Tormen halo mass function for different values of B while keeping the other parameters fixed at ﹩A={10}^{40}\,{M}_{\odot }^{-1}{{\rm{s}}}^{-1}﹩, C = −0.5, and D = 2.28. Parameter B represents the minimum halo mass (﹩{M}_{h,\min }﹩) considered in the model.
Paper: Bridging the Gap between Cosmic Dawn and Reionization Favors Models Dominated by Faint Galaxies
Authors: Ankita Bera, Sultan Hassan, Aaron Smith, Renyue Cen, Enrico Garaldi, Rahul Kannan, Mark Vogelsberger
Figure caption: Left panel: Several posterior distributions derived using the UV luminosity density (Madau 2018), including constraints for three different redshift ranges, namely z > 16 (representing cosmic dawn only, green), z < 10 (during reionization only, red), and z ∼ 5–20 (cosmic dawn and reionization, by combining the full redshift range, blue). Right panel: Comparison between several UV luminosity densities calculated from R ion with the inferred parameter values using MCMC. This figure indicates that fitting to z > 16 favors more negative C values, which implies stronger contributions from low-mass (faint) galaxies.
Paper: Bridging the Gap between Cosmic Dawn and Reionization Favors Models Dominated by Faint Galaxies
Authors: Ankita Bera, Sultan Hassan, Aaron Smith, Renyue Cen, Enrico Garaldi, Rahul Kannan, Mark Vogelsberger
Figure caption: Comparison between the combined constraints from reioniztion, EoR (﹩{\dot{N}}_{\mathrm{ion}},{x}_{{\rm{H}}\,{\rm\small{I}}}﹩, τ) in blue, and by adding cosmic dawn to reionization, CD (ρ UV from EDGES) + EoR (﹩{\dot{N}}_{\mathrm{ion}},{x}_{{\rm{H}}\,{\rm\small{I}}}﹩, τ) in red. The dark and light shaded contours correspond to the 1σand 2σ levels, respectively. This demonstrates that adding cosmic dawn constraints shifts the contours toward higher f esc and negative C parameters. This suggests that low-mass (faint) galaxies play a major role in bridging the gap between cosmic dawn and reionization.
Paper: Bridging the Gap between Cosmic Dawn and Reionization Favors Models Dominated by Faint Galaxies
Authors: Ankita Bera, Sultan Hassan, Aaron Smith, Renyue Cen, Enrico Garaldi, Rahul Kannan, Mark Vogelsberger
Figure caption: The SFR functions at z = 7 obtained for the EoR model and for the CD+EoR model are plotted as solid blue and green curves, respectively. The dashed lines represent the same evaluated at z = 6. The SFRFs from Smit et al. (2012; at z ∼ 6, 7) and Bouwens et al. (2015; at z ∼ 8) are plotted for comparison.
Paper: Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae
Authors: Michael A. Pajkos, Steven J. VanCamp, Kuo-Chuan Pan, David Vartanyan, Nils Deppe, Sean M. Couch
Figure caption: The real value of the decomposition of h + − ih × into spin weighted spherical harmonics −2 a 2m . These coefficients are then squared and normalized by their sum, or ﹩{}_{-2}{\tilde{P}}_{2| m| }={\left({}_{-2}{a}_{2\pm m}\right)}^{2}/{\sum }_{i}{\left({}_{-2}{a}_{2\pm {m}_{i}}\right)}^{2}﹩. For convenience, we introduce, ﹩{\tilde{P}}_{\mathrm{Po}}{=}_{-2}{\tilde{P}}_{2| 2| }﹩, favoring emission along the poles; ﹩{\tilde{P}}_{\mathrm{Mid}}{=}_{-2}{\tilde{P}}_{2| 1| }﹩, favoring emission along the midlatitudes; and ﹩{\tilde{P}}_{\mathrm{Eq}}{=}_{-2}{\tilde{P}}_{20}﹩, favoring emission along the equator. Different rows correspond to different magnitudes of m. Listed in Table 2 are the expressions for spin weighted spherical harmonics, −2 Y 2m . Physically, the more points there are closer to a value of 1, for a given m, the more similar the GW distribution resembles −2 Y 2m . (a) By eye, model s40o0 shows relatively equal contributions (i.e., similar density of points) from ﹩{\tilde{P}}_{\mathrm{Po}}﹩ , ﹩{\tilde{P}}_{\mathrm{Mid}}﹩, and ﹩{\tilde{P}}_{\mathrm{Eq}};﹩ physically, contributions from all three modes correspond to more isotropic emission. (b) Compared to the top panel of Figure 13(a), ﹩{\tilde{P}}_{\mathrm{Po}}﹩ for model s40o1 shows a larger contribution to the overall GW signal emitted. These increased m = ± 2 modes indicate increased GW amplitudes closer to the axis of rotation.
Paper: Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae
Authors: Michael A. Pajkos, Steven J. VanCamp, Kuo-Chuan Pan, David Vartanyan, Nils Deppe, Sean M. Couch
Figure caption: Similar to Figures 9 and 10, but for the nonrotating models v[9BW, 11, 12, 12.25, 23]. Top: Compared to the mesa models, this suite has similar GW amplitudes during the accretion phase, t pb ≲ 300 ms. After, the extreme matter asymmetries dominate the GW signal, by contributing to direct offset GW memory effects. Bottom: During the accretion phase, the preferred direction oscillates about ﹩\langle {\cos }^{2}\theta {\rangle }_{10\,\mathrm{ms}}\sim 0.5﹩. As the matter asymmetries become more drastic, different morphologies and orientations affect directionality to settle at different values of ﹩\langle {\cos }^{2}\theta {\rangle }_{10\,\mathrm{ms}}﹩. We note the only nonexploding model of this set, v12.25, retains its stochastic, nonsecular behavior.
Paper: Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae
Authors: Michael A. Pajkos, Steven J. VanCamp, Kuo-Chuan Pan, David Vartanyan, Nils Deppe, Sean M. Couch
Figure caption: Integrated values of ﹩{}_{-2}{\tilde{P}}_{2| m| }﹩—the time series data seen in Figures 13 and 14(a) for all models in this study, normalized by the total integrated power over all m values. Physically, this value corresponds to what fraction of time the GW strain surface resembles a given spin weighted spherical harmonic. Our data sets are split into thirds by the two vertical dashed lines. The left section indicates results from the mesa suite of models. These nonrotating models act as control cases, displaying equal contributions among m = 0, m = ± 1, and m = ± 2 modes. Between both dashed lines are the rotating models, listed in order of initial rotation rate. As rotation increases, there is a transition of GW amplitudes away from ∣m∣ = 1 modes (lower values of squares), toward ∣m∣ = 2 modes (increasing values of triangles). The right section contains the models that show varying degrees of asymmetry of the supernova ejecta. In particular, v9BW displays GW amplitudes resembling −2 Y 2±1, whereas v11 GW distributions more strongly resemble −2 Y 2±2, due to unique explosion geometries. While the remaining models show varying degrees of asymmetry, they show different contributions due to not only different morphologies but also different relative orientations. In summary, two main factors that influence the directionality of GW emission from CCSNe are the degree of rotation, along with explosion morphology and explosion orientation.
Paper: Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae
Authors: Michael A. Pajkos, Steven J. VanCamp, Kuo-Chuan Pan, David Vartanyan, Nils Deppe, Sean M. Couch
Figure caption: Top: Average ﹩{h}_{+}^{\max }﹩ amplitude for a 10 ms window from t pb to t pb + 10 ms. Larger amplitudes correspond to greater time averages of GW amplitudes. Bottom: Average ﹩| {h}_{+}^{\max }| ﹩ weighted by ﹩{\cos }^{2}\theta ﹩ and normalized by ﹩\langle | {h}_{+}^{\max }| {\rangle }_{10\mathrm{ms}}﹩. Denoted in the black dashed line, for a spherical distribution on the unit sphere, ﹩\langle {\cos }^{2}\theta {\rangle }_{10\,\mathrm{ms}}=1/2﹩. Values above this line indicate an ﹩\langle | {h}_{+}^{\max }| {\rangle }_{10\mathrm{ms}}﹩ distribution that is more prolate; values below this line indicate a distribution that is more oblate. Seen in the rotating models (darker hues), as rotation rate increases, the preferred GW directions favor the axis of rotation, or ﹩{\cos }^{2}\theta =1﹩.
Paper: Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae
Authors: Michael A. Pajkos, Steven J. VanCamp, Kuo-Chuan Pan, David Vartanyan, Nils Deppe, Sean M. Couch
Figure caption: Similar to Figure 9, but for the mesa models from O’Connor & Couch (2018b). Top: compared to the rotating 40 M ⊙ models, the mesa suite has GW amplitudes nearly an order of magnitude lower. Bottom: all GW distributions remain nearly isotropic.
Paper: Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae
Authors: Michael A. Pajkos, Steven J. VanCamp, Kuo-Chuan Pan, David Vartanyan, Nils Deppe, Sean M. Couch
Figure caption: Left: TDWF for model s40o1 when viewed along the equator of the CCSN. Light green color is for a source distance of 10 kpc, and dark blue is for a source distance of 80 kpc. The vertical line marks t pb = − 0.623 ms, when the strain for the 10 kpc source reaches 10−21. Right: Since the bounce creates an axisymmetric GW distribution, we show a slice through a strain surface plot—the x–z plane. The distance from the origin to any point in this plane is the GW strain along that viewing angle. The gray dashed circle shows a contour for ﹩| h| =\sqrt{{h}_{+}^{2}+{h}_{\times }^{2}}={10}^{-22}﹩. The light green, solid, curved line is the strain surface at t pb = − 0.623 ms for the 10 kpc source distance. The dark blue line is for the 80 kpc source distance. Shaded areas show the viewing angles where ∣h∣ > 10−22 for the two source distances. As the CCSN source distance increases, the opening angle for detectable GW strains decreases; the darker blue detectable region traces a smaller angle (∼53°) than the lighter green detectable region (∼143°).
Paper: Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae
Authors: Michael A. Pajkos, Steven J. VanCamp, Kuo-Chuan Pan, David Vartanyan, Nils Deppe, Sean M. Couch
Figure caption: Same as Figure 13, however for model v23. (a) While the PNS oscillations provide the stochasticity in the signal, after t pb ∼ 1.5 s, the asymmetry of the explosion ejecta dominates the GW signal; this secular drift of material provides slow changes in ﹩{\tilde{P}}_{\mathrm{Eq}}﹩ and ﹩{\tilde{P}}_{\mathrm{Mid}}﹩, compared to the models in Figure 13. (b) Similar to the left panel, however, after passing the signal through a 10 Hz high-pass filter. As expected, the power is evenly distributed among ﹩{\tilde{P}}_{\mathrm{Eq}}﹩, ﹩{\tilde{P}}_{\mathrm{Mid}}﹩, and ﹩{\tilde{P}}_{\mathrm{Po}}﹩ modes, similar to model s40o0 in Figure 13(a).
Paper: Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae
Authors: Michael A. Pajkos, Steven J. VanCamp, Kuo-Chuan Pan, David Vartanyan, Nils Deppe, Sean M. Couch
Figure caption: The real value of the decomposition of h + − ih ×, scaled by the distance 10 kpc, into spin weighted spherical harmonics −2 a 2m . Different rows correspond to different m numbers. Listed in Table 2 are the expressions for spin weighted spherical harmonics. At early times, −2 a 20 shows dominant contributions to the GW surfaces. Because of the ﹩{\sin }^{2}\theta ﹩ behavior, as noted in Table 2, this behavior indicates dominant GW emission along the equator of the supernova—characteristic of the axisymmetric bounce signal. Beyond 150 ms pb, the m = ± 2 mode shows dominant contributions along the poles.
Paper: Characterizing the Directionality of Gravitational Wave Emission from Matter Motions within Core-collapse Supernovae
Authors: Michael A. Pajkos, Steven J. VanCamp, Kuo-Chuan Pan, David Vartanyan, Nils Deppe, Sean M. Couch
Figure caption: Nonuniformities in the angular velocity profiles for model s40o1 during the ringdown phase (left) and accretion phase (right). Slice plots show the equatorial plane. White lines indicate the rest mass density contour for 1011 g cm−3.
Paper: The Impact of Patchy Reionization on Ultrafaint Dwarf Galaxies
Authors: Jaeeun Kim, Myoungwon Jeon, Yumi Choi, Hannah Richstein, Elena Sacchi, Nitya Kallivayalil
Figure caption: Cumulative fractional SFHs of the simulated UFD analogs, alongside those of observed MW UFD satellites, represented by different colors. The PR runs are distinguished by colored lines if they exhibit extended SFHs, while gray is used for PR runs without extended SFHs. Here, we focus on the cumulative SFHs of Magellanic UFDs, which are believed to have recently entered the MW environment and are, therefore, suitable samples for studying the effects of patchy reionization. Compared to our simulations, the observed UFDs tend to have formed a majority of their stars (∼90%) prior to reionization, but they also exhibit extended star formation that continues for at least 3 Gyr longer than what is found in our simulated halos.