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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: This figure is similar to Figure 5, but it specifically illustrates the hydrogen photoionization rate (left) and photoheating rate (right) produced by galaxies within a large box, spanning a linear size of 30 comoving Mpc. In this region, three massive galaxies (with M vir ≳ 1013 M ⊙ at z = 0) predominantly (≳80%) influence the simulated UFD analog, HALO 4. Despite the substantial mass of these halos and their significant contribution of UV photons to HALO 4, it is noteworthy that during the reionization epoch, these three halos were, on average, five times farther from HALO 4 compared to the distance between HALO 4 and the MW-like halo. Consequently, the total level of reionization by all galaxies within the simulation box is elevated by a factor of 5–10 in comparison to what the Milky Way–mass halo imposes on the target UFDs. However, it remains lower by a factor of 20–50 compared to the intensity of GR.
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: The relationship between the stellar mass and the mean [Fe/H] of the simulated UFD analogs, in comparison with observations (Kirby et al. 2013; Sacchi et al. 2021) and other theoretical studies (Jeon et al. 2017; Wheeler et al. 2019; Agertz et al. 2020). The PR runs show that the metallicities of our simulated UFDs tend to agree well with those of observed MW satellites in the stellar mass range of 104 M ⊙ ≲ M * ≲ 105 M ⊙. However, reproducing the metallicity plateau in the lowest-mass galaxy regime (M * < 104 M ⊙), where −3 ≲ [Fe/H] ≲ −2 remains challenging for our simulations. While patchy reionization can contribute to increasing stellar metallicities, it also pushes them to the higher stellar mass regime (M * ≳ 104 M ⊙).)
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: The MDF of our simulated UFDs (shown in blue) in the PR runs adopting z t = 5.5 is compared with that of Reticulum II (gray), one of the Magellanic UFD satellites, and Canes Venatici I (brown), in the form of a normalized histogram. Despite Reticulum II having a stellar mass lower by 1–2 orders of magnitude than the simulated galaxies (with 〈M *〉 = 7.6 × 104 M ⊙), its mean stellar metallicity (〈[Fe/H]〉 = −2.46) is similar to that of the simulated galaxies (〈[Fe/H]〉 = −2.32). On the other hand, Canes Venatici I, which is about twice as massive as the simulated galaxy (blue), likely exhibits a wide range of metallicities, including stars with relatively high metallicity at [Fe/H] = −1. Achieving such high-metallicity stars is a challenging aspect of our study.
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: The direct orbits of the Magellanic UFD satellites and the LMC from the center of the MW, reconstructed using Gaia’s proper-motion measurements (Patel et al. 2020). For comparison, the red pentagon represents the average distance of the simulated UFD analogs from the host halo at z = 7, while the blue pentagon represents the average distance at z = 6. Due to the lack of orbital histories of the Magellanic UFDs prior to 6 Gyr ago, it is difficult to determine the location of the observed UFDs during reionization. However, if the Magellanic UFDs were distant from the MW (d > 400 kpc) at the end of reionization, they may have been exposed to a weaker local UV field from the MW progenitor, which could have allowed for star formation to continue after reionization.
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: The normalized MDF of stars from HALO4-PR is shown to compare the effect of transition time, with the cyan-filled MDF corresponding to z t = 5.8, and the blue MDF representing the run adopting z t = 5.5. As the transition time is moved to lower redshift, the fraction of late star formation in HALO4-PR increases from 65% to 80%. This contributes to the shift toward higher metallicity in the MDF, as previously discussed in Figure 8. For HALO4-PR, we have found that delaying the transition time from z t = 5.8 to z t = 5.5 results in a mean stellar metallicity increase of 0.2 dex.
Paper: The Formation of Blue Large-amplitude Pulsators from White-dwarf Main-sequence Star Mergers
Authors: Xianfei Zhang, C. Simon Jeffery, Jie Su, Shaolan Bi
Figure caption: Location of BLAPs and evolutionary tracks of HeWD+MS merger models in the H-R diagram. The MS evolutionary tracks for 1–10 M ⊙ are shown as gray lines for metallicity Z = 0.02 (mass fraction). The black line indicates the evolutionary track of a 0.250+0.650 M ⊙ HeWD+MS merger remnant. The star indicates the first helium shell flash (He-flash). The square regions show the locations of BLAPs and different types of pulsating hot subdwarfs, including short-period p-mode sdB stars (sdBVr: purple), long-period g-mode sdBs (sdBVs: pink), and the hotter sdO variables (sdOV: gray).
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: The SFHs of HALO 4 by employing different escape fractions. When the escape fraction decreases from 100% (dotted line) to 30% (dashed line), the duration of the SFH extends by approximately 70 Myr, indicating that more extended SFHs can be attained with a lower escape fraction. We find that the stellar masses are similar between the two cases, but the run with f esc = 1.0 has 40% less gas mass compared to the run adopting f esc = 0.3.
Paper: Multiwavelength Study of Dark Globule DC 314.8–5.1: Point-source Identification and Diffuse Emission Characterization
Authors: E. Kosmaczewski, Ł Stawarz, C. C. Cheung, A. Bamba, A. Karska, W. R. M. Rocha
Figure caption: Top left: Spitzer MIPS 24 μm image of the DC 314.8–5.1 region. The color bar spans from a minimum of 23.5 to 100 MJy sr−1 on a log scale. White contours in the following panels represent MIPS emission, with levels set at 24.1, 25.05, and 26 MJy sr−1. Top right: ROSAT full-band 0.1–2.4 keV image of the same region, with Spitzer MIPS contours superimposed. The color bar shows a range of 0.6–2.5 smoothed counts on a square-root scale with a Gaussian smoothing, see Appendix B. Bottom: Swift-XRT hard-band 2–10 keV and soft-band 0.3–2.0 keV images of the same region (left and right, respectively), smoothed with a boxcar kernel, see Appendix B. Spitzer MIPS contours are superimposed in white for reference. The color bar shows a range of 0–0.05 smoothed counts on a linear scale.
Paper: Multiwavelength Study of Dark Globule DC 314.8–5.1: Point-source Identification and Diffuse Emission Characterization
Authors: E. Kosmaczewski, Ł Stawarz, C. C. Cheung, A. Bamba, A. Karska, W. R. M. Rocha
Figure caption: IRAC color–color diagram with selection cuts from Gutermuth et al. (2009). Top left: a total of 1319 sources from the SEIP query of ﹩{5}^{{\prime} }﹩ radius from the optical center of DC 314.8–5.1. It is overlaid with the first selection cut, red dashed lines showing the removal of star-forming galaxies (SFG). Top right: second SFG selection cut; removed sources are marked as red diamonds. Bottom left: AGN selection cut with AGN-like sources marked in blue. Bottom right: selection cut in order to remove Galactic-scale unresolved shocks and unresolved sources of PAH emission; sources of PAH emission are marked with green pentagons; no unresolved shock sources were selected.
Paper: Multiwavelength Study of Dark Globule DC 314.8–5.1: Point-source Identification and Diffuse Emission Characterization
Authors: E. Kosmaczewski, Ł Stawarz, C. C. Cheung, A. Bamba, A. Karska, W. R. M. Rocha
Figure caption: IRAC color–color diagram with YSO selection criteria from Gutermuth et al. (2009). The black marked regions display the final selection cuts identifying YSO Class I and II sources. Sources outside the delineated regions are undefined in this selection.
Paper: Particle-in-Cell Simulations of Sunward and Anti-sunward Whistler Waves in the Solar Wind
Authors: Ilya V. Kuzichev, Ivan Y. Vasko, Anton V. Artemyev, Stuart D. Bale, Forrest S. Mozer
Figure caption: Panel (a) presents the relative spectral widths Δω/ω of parallel (anti-sunward) and antiparallel (sunward) whistler waves observed over the saturation stage in the simulations performed at various background plasma parameters (Table 1). The spectral widths Δω and central frequencies ω were computed using Gaussian fittings of the spectra. Panel (b) presents the ratio between the left and right sides of Equation (3), computed separately for sunward and anti-sunward whistler waves and plotted vs. their initial linear growth rates. The fact that this ratio is larger than 1 implies the nonlinear evolution and saturation of the whistler waves can described within quasi-linear theory.
Paper: Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx
Authors: Yuan Qi Ni, Dae-Sik Moon, Maria R. Drout, Christopher D. Matzner, Kelvin C. C. Leong, Sang Chul Kim, Hong Soo Park, Youngdae Lee
Figure caption: The observed evolution of the Si II PVF and HVF velocity in SN 2021aefx is compared to those of SNe 2009ig (cyan hexagons; Silverman et al. 2015), 2018aoz (orange squares; Ni et al. 2022), and 2011fe (green triangles; Pereira et al. 2013) as well as the predictions of two models: (1) homologous expansion of the 1.34 M ⊙ SN ejecta and a low-mass secondary distribution of high-velocity material (red and blue lines); and (2) reverse-shocked SN ejecta (pink shaded region). SNe 2018aoz and 2011fe are typical Type Ia SNe with normal Si II photospheric velocities, while the Si II features of SN 2009ig also exhibit prominent HVF and PVF components (Marion et al. 2013) resembling those of SN 2021aefx. The light gray diagonal lines are t −2/9 power laws fitted to each SN. The red vertical dashed and horizonal dotted lines represent the epoch of B-band maximum of SN 2021aefx (﹩{t}_{\max }﹩ = 17.26 days since explosion) and the estimated transition velocity of its ejecta (v  t  = 0.93v ej ∼  11,520 km s−1; see Section 6.1), respectively, while the blue ones represent the epoch when the HVF of SN 2021aefx begins to plateau (﹩{t}_{\max }^{{\prime} }﹩ = 3.6 days) and the observed plateau velocity (﹩{v}_{t}^{{\prime} }﹩ = 21,860 ± 20 km s−1), respectively. These HVF properties match the homologous expansion of ﹩{v}_{\mathrm{ej}}^{{\prime} }﹩ = 23,500 km s−1 material embedded in the outermost ∼16% of the ejecta along the line of sight. The magenta dotted line represents the velocity at the inner boundary of the reverse-shocked region for the case of CSM with an s = 2 density profile.
Paper: Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx
Authors: Yuan Qi Ni, Dae-Sik Moon, Maria R. Drout, Christopher D. Matzner, Kelvin C. C. Leong, Sang Chul Kim, Hong Soo Park, Youngdae Lee
Figure caption: Top: the KSP BVI-band transmission curves used for BVi-band photometry. Bottom: The spectrum (orange solid curve) and SED (orange symbols) of SN 2021aefx from −16.7 rest-frame days since B-band maximum, near the peak epoch of the early excess emission (−16.2 days; Section 3.1), is compared to the blackbody (orange dashed curve) predicted by the best-fit surface 56Ni heating model (Section 5.1) from the same post-explosion phase (0.6 day in rest frame). The SED consists of interpolated photometry from KSP, LCO, Swift, and DLT40. The spectrum is flux-calibrated to the KSP BVi-band photometry (orange stars). The wavelengths of key absorption features in Type Ia SNe are labeled at the top of the panel. The spectrum from −14.9 days (brown), near the epoch of the reddest early B − V color (−15.2 days; Section 3), is also shown compared to the modeled blackbody for that phase (2.4 days post-explosion; brown dashed curve). Both spectrum and SED are normalized to the same KSP BVi-band observations (orange stars) for better comparison to the observations from the prior phase. The model explains the observed redward color evolution in SN 2021aefx (Figure 3) with a shift in continuum temperature between the two epochs.
Paper: Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx
Authors: Yuan Qi Ni, Dae-Sik Moon, Maria R. Drout, Christopher D. Matzner, Kelvin C. C. Leong, Sang Chul Kim, Hong Soo Park, Youngdae Lee
Figure caption: Top: UVOIR bolometric light curve of SN 2021aefx (black crosses) are compared to those of three events with super-Chandrasekhar inferred ejecta masses (Scalzo et al. 2019) and two models (1) Arnett model (Arnett 1982) matched to the rise time and peak luminosity of the bolometric light curve (red dotted curve); and (2) Arnett model fitted to the bolometric light curve near the peak (green dotted–dashed curve). The bounds of the pumpkin colored region correspond to the larger of two uncertainties: (1) the 1σ uncertainty level of the bolometric light curve; and (2) the potential uncertainty from using the best-fit SNooPy template to complete the UVOIR waverange where observations are absent. Middle and bottom: the observed (nondereddened) UV–optical colors of SN 2021aefx (black open circles) are compared to those of the 03fg/09dc-like events SNe 2012dn and 2011aa (green and magenta circles, respectively; Brown et al. 2014), and the expectations for the NUV-red and blue groups of normal Type Ia SNe (red and blue colored shaded areas, respectively; Milne et al. 2013).
Paper: Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx
Authors: Yuan Qi Ni, Dae-Sik Moon, Maria R. Drout, Christopher D. Matzner, Kelvin C. C. Leong, Sang Chul Kim, Hong Soo Park, Youngdae Lee
Figure caption: Left: The dereddened early BVi (from top to bottom) light curves of SN 2021aefx in rest frame are compared to what is expected from power-law + three models of early excess emission in Type Ia SNe (1) surface 56Ni shell (blue solid curves); (2) ejecta interaction with the companion (green solid curves); and (3) ejecta interaction with CSM (magenta solid curves). The transparent curves show the early excess emission (dashed) and underlying power-law (dotted) components, respectively, of each correspondingly colored model, while the inverted arrows with dotted lines mark the onsets of the power-law components. The black dashed vertical line and shaded region represent the epoch of explosion and its 1σ uncertainty. The orange and brown vertical lines mark the epochs of the correspondingly colored spectra in Figure 11 from near the excess emission peak (see Figure 4) and the reddest B − V color (see top right), respectively. Right: the dereddened B − V (top) and V − i (bottom) colors of SN 2021aefx are compared with those predicted by the same models from the left panels.
Paper: Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx
Authors: Yuan Qi Ni, Dae-Sik Moon, Maria R. Drout, Christopher D. Matzner, Kelvin C. C. Leong, Sang Chul Kim, Hong Soo Park, Youngdae Lee
Figure caption: Same as Figure 6, but showing multicomponent Gaussian fits of the Ca NIR triplet with PVF (cyan curves) and HVF (blue curves) components. The solid curve in each component represents the Ca II λ8498 Å line of the triplet, while the dashed curves represent the other two lines at 8542 and 8662 Å. Rows (1)–(2) are during the early Si II PVF and HVF decline, (3)–(5) span the Si II HVF plateau (see Figure 7), (6) near B-band maximum is the last phase when the Ca II NIR triplet HVF is detected, and (7) is from after B-band maximum. The x-axes of the right panels represent velocity in the rest frame of the fitted minima of the Ca II λ8498 Å PVF at each phase (blue vertical dotted line). The cyan vertical dotted line with shaded region represents the mean and 1σ velocity of the fitted minima of the Ca II λ8498 Å HVF in this frame.
Paper: Origin of High-velocity Ejecta, Excess Emission, and Redward Color Evolution in the Infant Type Ia Supernova 2021aefx
Authors: Yuan Qi Ni, Dae-Sik Moon, Maria R. Drout, Christopher D. Matzner, Kelvin C. C. Leong, Sang Chul Kim, Hong Soo Park, Youngdae Lee
Figure caption: The dereddened nebular-phase spectrum of SN 2021aefx from ∼300 days since B-band maximum in rest frame obtained by GMOS with B600 and R400 filters (indigo and magenta curves, respectively). The observed emission lines of Fe III, Co III, and the Fe II + Ni II complex are labeled near the top with vertical shaded regions representing the wavelengths used for flux integration. The expected positions of nondetected Hα, He I, and [O I] emission lines are represented with vertical dotted lines near the bottom.
Paper: Hubble Constant Measurement from Three Large-separation Quasars Strongly Lensed by Galaxy Clusters
Authors: Kate Napier, Keren Sharon, Håkon Dahle, Matthew Bayliss, Michael D. Gladders, Guillaume Mahler, Jane R. Rigby, Michael Florian
Figure caption: HST imaging of the three cluster-lensed quasars used to derive H 0. We computed the lens models for SDSS J1004+4112 and SDSS J1029+2623. SDSS J2222+2745 is reproduced from Sharon et al. (2017). The positions of the quasar images are denoted with the cyan letters. The critical curves, the loci of maximum magnification at a specified source redshift, are generated at the quasar redshifts—z = 1.734, z = 2.1992, and z = 2.805, for SDSS J1004+4112, SDSS J1029+2623, and SDSS J2222+2745, respectively, and are plotted in red.
Paper: Hubble Constant Measurement from Three Large-separation Quasars Strongly Lensed by Galaxy Clusters
Authors: Kate Napier, Keren Sharon, Håkon Dahle, Matthew Bayliss, Michael D. Gladders, Guillaume Mahler, Jane R. Rigby, Michael Florian
Figure caption: Constraints on H 0 from three cluster-lensed quasars, SDSS J1004+4112, SDSS J1029+2623, and SDSS J2222+2745. The histograms are created from 500 random models sampled from the MCMC. Overplotted are Gaussian fits to the distributions. Whereas individual time-delay measurements produce H 0 values with an average of 41% error, the error is decreased to 11% when the systems are analyzed together. The inverse-variance weighted mean of H 0 is 74.1 km s−1 Mpc−1 (solid gray line) and the standard error of the weighted mean is 8.0 km s−1 Mpc−1.
Paper: Uncovering Hidden Massive Black Hole Companions with Tidal Disruption Events
Authors: Brenna Mockler, Denyz Melchor, Smadar Naoz, Enrico Ramirez-Ruiz
Figure caption: TDE rates calculated for the EKL mechanism compared to rates calculated for two-body relaxation and to observed rates. The two-body relaxation rates (from Stone & Metzger 2016) plotted for “cuspy” galaxies (dashed lines) correspond to galaxies with an inner 2D surface brightness profile exponent of γ > 0.5 (I(R) ∝ R −γ ), while the rates plotted for “core” galaxies (dotted lines) correspond to γ < 0.3 (Lauer et al. 2007; the cuspy galaxies approximately correspond to density profile exponents α between 1 and 2; however note that these profiles are estimated observationally from radii >r  h , and therefore are not a direct comparison to the profiles used in simulations in this paper for radii interior to r  h ). The observed rate for all TDEs (shaded gray) is from van Velzen et al. (2020), and the observed rate in post-starburst galaxies (hatched region) is from French et al. (2020).
Paper: Uncovering Hidden Massive Black Hole Companions with Tidal Disruption Events
Authors: Brenna Mockler, Denyz Melchor, Smadar Naoz, Enrico Ramirez-Ruiz
Figure caption: Analytical exploration of the parameter space showing the number of stars susceptible to the EKL mechanism. The white stars represent the parameter combinations chosen for numerical simulation runs. This is calculated by determining the range of semimajor axes for each parameter combination where the EKL timescale is the shortest dynamical timescale. All of our systems have e bin = 0.5 and a bin = 0.5r  h,disrupting. While we compare against a variety of dynamical timescales (including those for two-body relaxation, vector resonant relaxation, GR precession, and binary hardening through gravitational wave emission; see Appendix), the two competing timescales are t GR,1 and t NT. These are the timescales for GR precession due to the disrupting black hole and Newtonian precession due to the stellar potential, respectively.
Paper: Uncovering Hidden Massive Black Hole Companions with Tidal Disruption Events
Authors: Brenna Mockler, Denyz Melchor, Smadar Naoz, Enrico Ramirez-Ruiz
Figure caption: The final distributions of the stars’ semimajor axes (a 1) and maximum eccentricities (﹩{e}_{\max }﹩, plotted as ﹩1-{e}_{\max }﹩) for three runs with varying inner black hole mass (m 1 = 105, 106, 107 M ⊙). The critical radius for disruption used here is R  p  ≤ 2R  T  (allowing for both partial and full disruptions), denoted by dashed lines in the plot. Disruptions are plotted with a star-shaped marker, and plunges (disruptions that occur with R  T  < R  S ) are shaded gray. The maximum semimajor axis included for stars in a given run is defined by the hierarchical condition (Equation (1)).
Paper: Uncovering Hidden Massive Black Hole Companions with Tidal Disruption Events
Authors: Brenna Mockler, Denyz Melchor, Smadar Naoz, Enrico Ramirez-Ruiz
Figure caption: Example run showing EKL cycles as a function of time. The dashed horizontal line denotes our critical radius for partial disruption (β = 0.5), and the dotted vertical lines denote t quad given the initial orbital conditions. As you can see, t quad is of the order of the period of one eccentricity oscillation, as expected. This simulation is part of the set of runs with m 1 = 106 M ⊙, m 2 = 107 M ⊙, and α = 2.
Paper: Uncovering Hidden Massive Black Hole Companions with Tidal Disruption Events
Authors: Brenna Mockler, Denyz Melchor, Smadar Naoz, Enrico Ramirez-Ruiz
Figure caption: The fraction of stars that are disrupted as TDEs as a function of the semimajor axis (scaled by the hierarchical radius). Each panel varies one simulation parameter. Top: α = 1.5, q = 10. Middle: m 1 = 106 M ⊙, q = 10. Bottom: m 1 = 106 M ⊙, α = 1.5.
Paper: Uncovering Hidden Massive Black Hole Companions with Tidal Disruption Events
Authors: Brenna Mockler, Denyz Melchor, Smadar Naoz, Enrico Ramirez-Ruiz
Figure caption: Cartoon of simulation setup (not to scale). We study stars orbiting the smaller of the two SMBHs, and focus on the region within the hierarchical radius (defined in Equation (2)), as orbits in this region are less likely to be chaotically scattered by the second black hole.
Paper: Probing the Low-mass End of Core-collapse Supernovae Using a Sample of Strongly-stripped Calcium-rich Type IIb Supernovae from the Zwicky Transient Facility
Authors: Kaustav K. Das, Mansi M. Kasliwal, Christoffer Fremling, Sheng Yang, Steve Schulze, Jesper Sollerman, Tawny Sit, Kishalay De, Anastasios Tzanidakis, Daniel A. Perley, Shreya Anand, Igor Andreoni, C. Barbarino, K. Brudge, Andrew Drake, Avishay Gal-Yam, Russ R. Laher, Viraj Karambelkar, S. R. Kulkarni, Frank J. Masci, Michael S. Medford, Abigail Polin, Harrison Reedy, Reed Riddle, Yashvi Sharma, Roger Smith, Lin Yan, Yi Yang, Yuhan Yao
Figure caption: Radioactive (Arnett et al. 1989) fits to bolometric luminosity data excluding the data points fit by shock cooling.