adsabs/AstroCLIMB huggingface dataset:
Paper: Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Erica Behrens, Jeffrey G. Mangum, Serena Viti, Jonathan Holdship, Ko-Yun Huang, Mathilde Bouvier, Joshua Butterworth, Cosima Eibensteiner, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Laura Colzi, Christian Henkel, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Posterior distributions for region 1 using UCLCHEM (a) vs. the neural network (b).
Paper: Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Erica Behrens, Jeffrey G. Mangum, Serena Viti, Jonathan Holdship, Ko-Yun Huang, Mathilde Bouvier, Joshua Butterworth, Cosima Eibensteiner, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Laura Colzi, Christian Henkel, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Posterior distributions for regions 19 (a), 69 (b), 78 (c), and 88 (d), which all feature high CRIRs paired with low kinetic temperatures.
Paper: Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Erica Behrens, Jeffrey G. Mangum, Serena Viti, Jonathan Holdship, Ko-Yun Huang, Mathilde Bouvier, Joshua Butterworth, Cosima Eibensteiner, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Laura Colzi, Christian Henkel, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Posterior distributions for regions 26 (top) and 53 (bottom) before (left) and after (right) including a beam-filling factor as a free parameter in our modeling algorithm.
Paper: Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Erica Behrens, Jeffrey G. Mangum, Serena Viti, Jonathan Holdship, Ko-Yun Huang, Mathilde Bouvier, Joshua Butterworth, Cosima Eibensteiner, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Laura Colzi, Christian Henkel, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Posterior distributions for regions 26 (top) and 53 (bottom) using only one phase of chemical modeling (left column) vs. two phases (right column).
Paper: Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Erica Behrens, Jeffrey G. Mangum, Serena Viti, Jonathan Holdship, Ko-Yun Huang, Mathilde Bouvier, Joshua Butterworth, Cosima Eibensteiner, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Laura Colzi, Christian Henkel, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: HCN ((a) and (b)) and HNC ((c) and (d)) integrated intensities (top panel in each pair) and integrated intensity ratios (new rates divided by old rates; bottom panels in each pair) as a function of kinetic temperature. Volume and column density are held constant at the listed values for each comparison.
Paper: Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Erica Behrens, Jeffrey G. Mangum, Serena Viti, Jonathan Holdship, Ko-Yun Huang, Mathilde Bouvier, Joshua Butterworth, Cosima Eibensteiner, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Laura Colzi, Christian Henkel, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Same as in Figures C1 and C2 but plotted as a function of column density, where kinetic temperature and volume density are held constant.
Paper: Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Erica Behrens, Jeffrey G. Mangum, Serena Viti, Jonathan Holdship, Ko-Yun Huang, Mathilde Bouvier, Joshua Butterworth, Cosima Eibensteiner, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Laura Colzi, Christian Henkel, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption: Same as in Figure C1 but plotted as a function of volume density, where kinetic temperature and column density are held constant.
Paper: Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Erica Behrens, Jeffrey G. Mangum, Serena Viti, Jonathan Holdship, Ko-Yun Huang, Mathilde Bouvier, Joshua Butterworth, Cosima Eibensteiner, Nanase Harada, Sergio Martín, Kazushi Sakamoto, Sebastien Muller, Kunihiko Tanaka, Laura Colzi, Christian Henkel, David S. Meier, Víctor M. Rivilla, Paul P. van der Werf
Figure caption:  UltraNest inference results derived from HCN and HNC data for regions 26 (top) and 53 (bottom) using old (left) vs. new (right) HCN and HNC collisional excitation rates.
Paper: KIC 10855535: An Elegant δ Scuti Pulsator with Amplitude and Phase Modulation
Authors: Li-xian Shen, Ali Esamdin, Cheng-long Lv, Hao-zhi Wang, Tao-zhi Yang, Rivkat Karimov, Shuhrat A. Ehgamberdiev, Hu-biao Niu, Jin-zhong Liu
Figure caption: Phase modulation before and after removing the LTE. The upper panel shows the time delay (derived from the phase modulation method) and O − C results of the F0 mode in KIC 10855535 over the Kepler observing span. Each red open circle represents the time delay measured every 15 days. The black dots indicate the O − C results, based on a period of 0.05639 day (P = 1/F0). The lower panel shows the time delays after eliminating binary effects by adjusting the time axis. The red curve represents a parabolic fit. An abrupt error bar exists due to fewer data points in the corresponding segment.
Paper: KIC 10855535: An Elegant δ Scuti Pulsator with Amplitude and Phase Modulation
Authors: Li-xian Shen, Ali Esamdin, Cheng-long Lv, Hao-zhi Wang, Tao-zhi Yang, Rivkat Karimov, Shuhrat A. Ehgamberdiev, Hu-biao Niu, Jin-zhong Liu
Figure caption: An equidistant quintuplet centered on the peak at 17.733260 day−1. The black solid curve represents the amplitude spectrum of KIC 10855535 after prewhitening F0, while the blue one represents the spectrum after removing all other frequencies in the p-mode region (≥5 day−1). All vertical dashed lines mark precise positions of the quintuplet. Note different y-axis scales for the blue and black lines; they have been scaled for easier comparison.
Paper: KIC 10855535: An Elegant δ Scuti Pulsator with Amplitude and Phase Modulation
Authors: Li-xian Shen, Ali Esamdin, Cheng-long Lv, Hao-zhi Wang, Tao-zhi Yang, Rivkat Karimov, Shuhrat A. Ehgamberdiev, Hu-biao Niu, Jin-zhong Liu
Figure caption: Phased time-delay curve derived from Kepler and TESS observations at orbital frequency (0.00243 day−1). Black and blue points represent Kepler and TESS time delays, respectively. The red curve is one of best fit for Kepler time delays. Error bars for TESS data are derived by bootstrap resampling. The Doppler shift and constant differences between two missions have been rectified for a better view. The bottom panel shows corresponding residuals.
Paper: KIC 10855535: An Elegant δ Scuti Pulsator with Amplitude and Phase Modulation
Authors: Li-xian Shen, Ali Esamdin, Cheng-long Lv, Hao-zhi Wang, Tao-zhi Yang, Rivkat Karimov, Shuhrat A. Ehgamberdiev, Hu-biao Niu, Jin-zhong Liu
Figure caption: Amplitude modulation in F0 over 4 yr. Each point in the top panel represents the fitted amplitude derived from a 15 days segment of the light curve. The red line shows a linear fitting to it. The residuals are shown in the bottom panel.
Paper: KIC 10855535: An Elegant δ Scuti Pulsator with Amplitude and Phase Modulation
Authors: Li-xian Shen, Ali Esamdin, Cheng-long Lv, Hao-zhi Wang, Tao-zhi Yang, Rivkat Karimov, Shuhrat A. Ehgamberdiev, Hu-biao Niu, Jin-zhong Liu
Figure caption: Diagram of the phase evolution over a time span of about four years for the residuals of the Kepler LC data. Pixel shades, from blue to purple, indicate the mean flux in each (time, phase) bin from low to high. Each pixel represents 10 days on the time axis and 0.05 on the phase axis. The vertical white gap inside exists due to a gap in data.
Paper: Absolute Dimensions of the Interferometric Binary HD 174881: A Test of Stellar Evolution Models for Evolved Stars
Authors: Guillermo Torres, Andrew F. Boden, John D. Monnier, Gerard T. van Belle
Figure caption: Image reconstruction of HD 174881 from the MIRC data of UT 2007 July 7, using the MACIM algorithm. The location and uniform diameters from the model-fitting procedure are overlaid.
Paper: KIC 10855535: An Elegant δ Scuti Pulsator with Amplitude and Phase Modulation
Authors: Li-xian Shen, Ali Esamdin, Cheng-long Lv, Hao-zhi Wang, Tao-zhi Yang, Rivkat Karimov, Shuhrat A. Ehgamberdiev, Hu-biao Niu, Jin-zhong Liu
Figure caption: Phase diagram of KIC 10855535 from Kepler data, folded by F0. The red line represents the polynomial fit for a sliding average result with phase bin of 0.001 and sliding gap of 0.0001. For better clarity, two periods are plotted.
Paper: KIC 10855535: An Elegant δ Scuti Pulsator with Amplitude and Phase Modulation
Authors: Li-xian Shen, Ali Esamdin, Cheng-long Lv, Hao-zhi Wang, Tao-zhi Yang, Rivkat Karimov, Shuhrat A. Ehgamberdiev, Hu-biao Niu, Jin-zhong Liu
Figure caption: The amplitude spectra and phase-folded light curves of each segment. The phases are binned every 0.002 phase.
Paper: Detection Rate of Galaxy Cluster-lensed Stellar Binary Black Hole Mergers by the Third-generation Gravitational-wave Detectors
Authors: Zhiwei Chen, Yushan Xie, Youjun Lu, Huanyuan Shan, Nan Li, Yuchao Luo, Xiao Guo
Figure caption: The redshift evolution of the cosmic lensing optical depth. The black solid line shows the results obtained by adopting the PSJ profile. The upper and lower bounds of the blue-shaded region are the optical depths estimated by the eNFW+SIS profile obtained by adopting the ﹩{c}_{{\rm{v}}}^{{\rm{o}}}﹩ and ﹩{c}_{{\rm{v}}}^{{\rm{w}}}﹩ relationship, respectively, while the blue dotted–dashed line is the result obtained by adopting the average concentration of both, i.e., ﹩{c}_{{\rm{v}}}^{{\rm{a}}}=({c}_{{\rm{v}}}^{{\rm{o}}}+{c}_{{\rm{v}}}^{{\rm{w}}})/2﹩. The red-dashed line shows the optical depth only considering the BCG in galaxy clusters. The red-dotted line is the optical depth inferred from the cosmoDC2 catalog data extrapolation Equation (18). For comparison, we also plot the optical depth for galaxy lensing from Z. Chen (2023) denoted by the green dotted–dashed line.
Paper: Detection Rate of Galaxy Cluster-lensed Stellar Binary Black Hole Mergers by the Third-generation Gravitational-wave Detectors
Authors: Zhiwei Chen, Yushan Xie, Youjun Lu, Huanyuan Shan, Nan Li, Yuchao Luo, Xiao Guo
Figure caption: The predicted redshift evolution of the merger rate density of sBBHs. The blue-dashed and the red-dotted–dashed lines show the results obtained from the EMBS and dynamical channels, respectively, with the calibration by the local sBBH merger rate density obtained from LIGO-Virgo observations, and the corresponding shaded regions show the errors induced by the uncertainties of local merger rate densities (90% confidence interval) (e.g., C. L. Rodriguez & A. Loeb 2018; R. Abbott et al. 2023a, 2023b). The green-shaded region shows the constraints on the merger rate density evolution obtained by the LVK observations assuming the peak+power-law model (R. Abbott et al. 2023a).
Paper: Detection Rate of Galaxy Cluster-lensed Stellar Binary Black Hole Mergers by the Third-generation Gravitational-wave Detectors
Authors: Zhiwei Chen, Yushan Xie, Youjun Lu, Huanyuan Shan, Nan Li, Yuchao Luo, Xiao Guo
Figure caption: The cumulative distribution of the magnified S/N, i.e., ﹩\sqrt{{\mu }^{{\ell }}}\rho ﹩ of cluster-lensed sBBH mergers produced via the EMBS channel, assuming the eNFW+SIS model. The dashed vertical line represents the typical threshold ρ 0 = 8 for GW detection.
Paper: Detection Rate of Galaxy Cluster-lensed Stellar Binary Black Hole Mergers by the Third-generation Gravitational-wave Detectors
Authors: Zhiwei Chen, Yushan Xie, Youjun Lu, Huanyuan Shan, Nan Li, Yuchao Luo, Xiao Guo
Figure caption: The accumulative (top panel) and differential (bottom panel) source redshift distribution, i.e., ﹩{\dot{N}}^{l}(\lt {z}_{{\rm{s}}})﹩ and ﹩d{\dot{N}}^{l}/{{dz}}_{{\rm{s}}}﹩ of cluster-lensed sBBH mergers produced by the EMBS (solid) and dynamical (dashed) channels.
Paper: Detection Rate of Galaxy Cluster-lensed Stellar Binary Black Hole Mergers by the Third-generation Gravitational-wave Detectors
Authors: Zhiwei Chen, Yushan Xie, Youjun Lu, Huanyuan Shan, Nan Li, Yuchao Luo, Xiao Guo
Figure caption: A cluster example extracted from the cosmoDC2 catalog. Within the galaxy cluster, the positions of member galaxies are indicated as filled blue circles, where the size of the circles is proportional to the galaxy’s absolute luminosity. The critical curves (caustics) for a source at z s = 2 are overplotted as the red (green) lines.
Paper: Expanding the Ultracompacts: Gravitational-wave-driven Mass Transfer in the Shortest-period Binaries with Accretion Disks
Authors: Joheen Chakraborty, Kevin B. Burdge, Saul A. Rappaport, James Munday, Hai-Liang Chen, Pablo Rodríguez-Gil, V. S. Dhillon, Scott A. Hughes, Gijs Nelemans, Erin Kara, Eric C. Bellm, Alex J. Brown, Noel Castro Segura, Tracy X. Chen, Emma Chickles, Martin J. Dyer, Richard Dekany, Andrew J. Drake, James Garbutt, Matthew J. Graham, Matthew J. Green, Dan Jarvis, Mark R. Kennedy, Paul Kerry, S. R. Kulkarni, Stuart P. Littlefair, Ashish A. Mahabal, Frank J. Masci, James McCormac, Steven G. Parsons, Ingrid Pelisoli, Eleanor Pike, Thomas A. Prince, Reed Riddle, Jan van Roestel, Dave Sahman, Avery Wold, Tin Long Sunny Wong
Figure caption: Top panels: O–C diagrams for ZTF J0546+3843 (left) and ZTF J1858–2024 (right). Bottom panels: phase folds with a fixed P 0, with eclipse times and instruments noted for each epoch. The eclipse time drifts by ∼0.1–0.15P over the baseline. We overplot the predicted waveforms from our coherent timing models (blue), as well as the single-epoch fits used to construct the O–C diagrams. The 5–10 s discrepancies are likely dominated by timing jitter due to accretion (see Section 3.3).
Paper: Expanding the Ultracompacts: Gravitational-wave-driven Mass Transfer in the Shortest-period Binaries with Accretion Disks
Authors: Joheen Chakraborty, Kevin B. Burdge, Saul A. Rappaport, James Munday, Hai-Liang Chen, Pablo Rodríguez-Gil, V. S. Dhillon, Scott A. Hughes, Gijs Nelemans, Erin Kara, Eric C. Bellm, Alex J. Brown, Noel Castro Segura, Tracy X. Chen, Emma Chickles, Martin J. Dyer, Richard Dekany, Andrew J. Drake, James Garbutt, Matthew J. Graham, Matthew J. Green, Dan Jarvis, Mark R. Kennedy, Paul Kerry, S. R. Kulkarni, Stuart P. Littlefair, Ashish A. Mahabal, Frank J. Masci, James McCormac, Steven G. Parsons, Ingrid Pelisoli, Eleanor Pike, Thomas A. Prince, Reed Riddle, Jan van Roestel, Dave Sahman, Avery Wold, Tin Long Sunny Wong
Figure caption: Top and bottom panels: trailed spectra (continuum-subtracted) of the He II 4686 and 5411 Å emission lines that might show S-wave variability at the orbital period. The orbital cycle is plotted twice. All spectra were taken with the LRIS instrument on Keck. Middle panels: phase-folded light curves in different filters. The pictured light curves of ZTF J0546+3843 and ZTF J1858–2024 were taken with HiPERCAM (u  s /g  s /r  s /i  s /z  s  filters from top to bottom), while ZTF J0425+3858 was observed with CHIMERA (g/r). Different bands are offset for visual clarity.
Paper: Expanding the Ultracompacts: Gravitational-wave-driven Mass Transfer in the Shortest-period Binaries with Accretion Disks
Authors: Joheen Chakraborty, Kevin B. Burdge, Saul A. Rappaport, James Munday, Hai-Liang Chen, Pablo Rodríguez-Gil, V. S. Dhillon, Scott A. Hughes, Gijs Nelemans, Erin Kara, Eric C. Bellm, Alex J. Brown, Noel Castro Segura, Tracy X. Chen, Emma Chickles, Martin J. Dyer, Richard Dekany, Andrew J. Drake, James Garbutt, Matthew J. Graham, Matthew J. Green, Dan Jarvis, Mark R. Kennedy, Paul Kerry, S. R. Kulkarni, Stuart P. Littlefair, Ashish A. Mahabal, Frank J. Masci, James McCormac, Steven G. Parsons, Ingrid Pelisoli, Eleanor Pike, Thomas A. Prince, Reed Riddle, Jan van Roestel, Dave Sahman, Avery Wold, Tin Long Sunny Wong
Figure caption: Likelihood contours of M 1 and M 2 for our Monte Carlo runs based on the argument outlined in Section 4.3. Solid black lines correspond to 1σ/2σ/3σ contours. These imply chirp masses close to 0.3 M ⊙ in both systems. As expected from the inward vs. outward ﹩\dot{P}﹩, the donor of ZTF J0546+3843 is significantly less degenerate (ξ ad larger) than that of ZTF J1858–2024.
Paper: Expanding the Ultracompacts: Gravitational-wave-driven Mass Transfer in the Shortest-period Binaries with Accretion Disks
Authors: Joheen Chakraborty, Kevin B. Burdge, Saul A. Rappaport, James Munday, Hai-Liang Chen, Pablo Rodríguez-Gil, V. S. Dhillon, Scott A. Hughes, Gijs Nelemans, Erin Kara, Eric C. Bellm, Alex J. Brown, Noel Castro Segura, Tracy X. Chen, Emma Chickles, Martin J. Dyer, Richard Dekany, Andrew J. Drake, James Garbutt, Matthew J. Graham, Matthew J. Green, Dan Jarvis, Mark R. Kennedy, Paul Kerry, S. R. Kulkarni, Stuart P. Littlefair, Ashish A. Mahabal, Frank J. Masci, James McCormac, Steven G. Parsons, Ingrid Pelisoli, Eleanor Pike, Thomas A. Prince, Reed Riddle, Jan van Roestel, Dave Sahman, Avery Wold, Tin Long Sunny Wong
Figure caption: Evolutionary tracks (from MESA binary modeling) of double WDs with different binary parameters. The observed P and ﹩\dot{P}﹩ in ZTF J0546+3843 are compatible with a donor of M 2 ≲ 0.13M ⊙ close to period minimum. The large observed ﹩\dot{P}﹩ in ZTF J1858+2024 is more difficult to reconcile. In all cases, the donors initially have a hydrogen envelope mass of 7 × 10−3 M ⊙.
Paper: Expanding the Ultracompacts: Gravitational-wave-driven Mass Transfer in the Shortest-period Binaries with Accretion Disks
Authors: Joheen Chakraborty, Kevin B. Burdge, Saul A. Rappaport, James Munday, Hai-Liang Chen, Pablo Rodríguez-Gil, V. S. Dhillon, Scott A. Hughes, Gijs Nelemans, Erin Kara, Eric C. Bellm, Alex J. Brown, Noel Castro Segura, Tracy X. Chen, Emma Chickles, Martin J. Dyer, Richard Dekany, Andrew J. Drake, James Garbutt, Matthew J. Graham, Matthew J. Green, Dan Jarvis, Mark R. Kennedy, Paul Kerry, S. R. Kulkarni, Stuart P. Littlefair, Ashish A. Mahabal, Frank J. Masci, James McCormac, Steven G. Parsons, Ingrid Pelisoli, Eleanor Pike, Thomas A. Prince, Reed Riddle, Jan van Roestel, Dave Sahman, Avery Wold, Tin Long Sunny Wong
Figure caption: Minimum mass bounds for disk-accreting systems as a function of orbital period, computed by the argument outlined in Section 4.2. For the relevant orbital periods of 7.95, 8.68, and 13.15 minutes, we obtain minimum donor/accretor masses of 0.084/0.54, 0.076/0.51, and 0.048/0.35 M ⊙, respectively.
Paper: Expanding the Ultracompacts: Gravitational-wave-driven Mass Transfer in the Shortest-period Binaries with Accretion Disks
Authors: Joheen Chakraborty, Kevin B. Burdge, Saul A. Rappaport, James Munday, Hai-Liang Chen, Pablo Rodríguez-Gil, V. S. Dhillon, Scott A. Hughes, Gijs Nelemans, Erin Kara, Eric C. Bellm, Alex J. Brown, Noel Castro Segura, Tracy X. Chen, Emma Chickles, Martin J. Dyer, Richard Dekany, Andrew J. Drake, James Garbutt, Matthew J. Graham, Matthew J. Green, Dan Jarvis, Mark R. Kennedy, Paul Kerry, S. R. Kulkarni, Stuart P. Littlefair, Ashish A. Mahabal, Frank J. Masci, James McCormac, Steven G. Parsons, Ingrid Pelisoli, Eleanor Pike, Thomas A. Prince, Reed Riddle, Jan van Roestel, Dave Sahman, Avery Wold, Tin Long Sunny Wong
Figure caption: A comparison of the UV spectra of ZTF J0546+3843 (HST STIS) and ES Cet (IUE). Both objects exhibit detectable nitrogen and helium features (though the strength of the nitrogen emission lines relative to helium is much larger in ES Cet). The carbon emission line visible in the spectrum of ZTF J0546+3843 is notably absent in the spectrum of ES Cet.
Paper: Expanding the Ultracompacts: Gravitational-wave-driven Mass Transfer in the Shortest-period Binaries with Accretion Disks
Authors: Joheen Chakraborty, Kevin B. Burdge, Saul A. Rappaport, James Munday, Hai-Liang Chen, Pablo Rodríguez-Gil, V. S. Dhillon, Scott A. Hughes, Gijs Nelemans, Erin Kara, Eric C. Bellm, Alex J. Brown, Noel Castro Segura, Tracy X. Chen, Emma Chickles, Martin J. Dyer, Richard Dekany, Andrew J. Drake, James Garbutt, Matthew J. Graham, Matthew J. Green, Dan Jarvis, Mark R. Kennedy, Paul Kerry, S. R. Kulkarni, Stuart P. Littlefair, Ashish A. Mahabal, Frank J. Masci, James McCormac, Steven G. Parsons, Ingrid Pelisoli, Eleanor Pike, Thomas A. Prince, Reed Riddle, Jan van Roestel, Dave Sahman, Avery Wold, Tin Long Sunny Wong
Figure caption: Multiband phase-folded light curves of four illustrative ultracompact binaries (u  s /g  s /r  s /i  s /z  s  filters from top to bottom). Light curves of HM Cnc/V407 Vul are drawn from J. Munday et al. (2023)/J. Munday (2024, in preparation), respectively.
Paper: Expanding the Ultracompacts: Gravitational-wave-driven Mass Transfer in the Shortest-period Binaries with Accretion Disks
Authors: Joheen Chakraborty, Kevin B. Burdge, Saul A. Rappaport, James Munday, Hai-Liang Chen, Pablo Rodríguez-Gil, V. S. Dhillon, Scott A. Hughes, Gijs Nelemans, Erin Kara, Eric C. Bellm, Alex J. Brown, Noel Castro Segura, Tracy X. Chen, Emma Chickles, Martin J. Dyer, Richard Dekany, Andrew J. Drake, James Garbutt, Matthew J. Graham, Matthew J. Green, Dan Jarvis, Mark R. Kennedy, Paul Kerry, S. R. Kulkarni, Stuart P. Littlefair, Ashish A. Mahabal, Frank J. Masci, James McCormac, Steven G. Parsons, Ingrid Pelisoli, Eleanor Pike, Thomas A. Prince, Reed Riddle, Jan van Roestel, Dave Sahman, Avery Wold, Tin Long Sunny Wong
Figure caption: Orbital period vs. ﹩\dot{M}﹩ for AM CVns. G. Ramsay et al. (2018) obtained their values by fitting UV-optical-IR spectral energy distributions. The lower bounds for ZTF J1858–2024 and ZTF J0546+3843 were obtained by using the lowest allowable masses (via the argument in Section 4.2) and Equation (12).
Paper: Expanding the Ultracompacts: Gravitational-wave-driven Mass Transfer in the Shortest-period Binaries with Accretion Disks
Authors: Joheen Chakraborty, Kevin B. Burdge, Saul A. Rappaport, James Munday, Hai-Liang Chen, Pablo Rodríguez-Gil, V. S. Dhillon, Scott A. Hughes, Gijs Nelemans, Erin Kara, Eric C. Bellm, Alex J. Brown, Noel Castro Segura, Tracy X. Chen, Emma Chickles, Martin J. Dyer, Richard Dekany, Andrew J. Drake, James Garbutt, Matthew J. Graham, Matthew J. Green, Dan Jarvis, Mark R. Kennedy, Paul Kerry, S. R. Kulkarni, Stuart P. Littlefair, Ashish A. Mahabal, Frank J. Masci, James McCormac, Steven G. Parsons, Ingrid Pelisoli, Eleanor Pike, Thomas A. Prince, Reed Riddle, Jan van Roestel, Dave Sahman, Avery Wold, Tin Long Sunny Wong
Figure caption: Violin plots of characteristic strains (over 4 yr) of ZTF J0546+3843 and ZTF J1858–2024 using the constraints from Section 4.3. We also plot the strains of several ZTF-discovered ultracompact binaries (K. B. Burdge et al. 2020a, 2020b, 2023) and LISA verification binaries (T. Kupfer et al. 2024) for comparison.