adsabs/AstroCLIMB huggingface dataset:
Paper: Refining the Stellar Parameters of τ Ceti: a Pole-on Solar Analog
Authors: Maria Korolik, Rachael M. Roettenbacher, Debra A. Fischer, Stephen R. Kane, Jean M. Perkins, John D. Monnier, Claire L. Davies, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Tyler Gardner, Cyprien Lanthermann, Gail H. Schaefer, Benjamin Setterholm, John M. Brewer, Joe Llama, Lily L. Zhao, Andrew E. Szymkowiak, Gregory W. Henry
Figure caption: Periodogram created by chromospheric data from the MWO HK Project, photometric data from the Automatic Photoelectric Telescope at the Fairborn Observatory, and RV data from EXPRES. The red line shows the rotation period of the star at 32 days (MWO), 43 days (APT), and 23 days (EXPRES).
Paper: Refining the Stellar Parameters of τ Ceti: a Pole-on Solar Analog
Authors: Maria Korolik, Rachael M. Roettenbacher, Debra A. Fischer, Stephen R. Kane, Jean M. Perkins, John D. Monnier, Claire L. Davies, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Tyler Gardner, Cyprien Lanthermann, Gail H. Schaefer, Benjamin Setterholm, John M. Brewer, Joe Llama, Lily L. Zhao, Andrew E. Szymkowiak, Gregory W. Henry
Figure caption: Plot (top) of normalized visibility amplitude vs. spatial frequency (B ⊥/λ). The data combines all eight nights of observation for a total of 613 data points. Plot (bottom) of closure phases for all eight nights of observation, showing nonzero phases.
Paper: Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c
Authors: Zoë L. de Beurs, Julien de Wit, Alexander Venner, David Berardo, Jared Bryan, Joshua N. Winn, Benjamin J. Fulton, Andrew W. Howard
Figure caption: Comparison of our stable, nonevolving orbital models. From top to bottom, we include the stable one-planet model with no background trends (a), (b); the stable two-planet model with the long-period companion modeled as a Keplerian (c), (d); and the stable two-planet model with the long-period companion modeled as a quadratic trend (e), (f). For more details on these orbital models, see Section 3.1. In each of the left-hand panels (a), (c), (e), we plot the orbital fit of HAT-P-2 b minus a secondary companion (or no companion if this was not included in the model). The data is color-coded by instrument (turquoise = HARPS-N 2013-2015, red = HARPS-N 2015-2017, black = HIRES). The median model is plotted in dark purple and 100 draws from the posteriors are plotted in light purple. In each of the right-hand panels (b), (d), (f), we plot the secondary companion (or no trend/companion if this was not included in the model) minus the median HAT-P-2 b model. We also include the goodness-of-fit metrics corresponding to each orbital model in the yellow box. “Red. ﹩{\chi }_{r}^{2}﹩” is an abbreviation for reduced ﹩{\chi }_{r}^{2}﹩.
Paper: Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c
Authors: Zoë L. de Beurs, Julien de Wit, Alexander Venner, David Berardo, Jared Bryan, Joshua N. Winn, Benjamin J. Fulton, Andrew W. Howard
Figure caption: The orbit of HAT-P-2 c from a joint fit to the RVs (left) and astrometry (right). Colors are as in Figure 1. The astrometry is consistent with zero net acceleration; the limits of this nondetection allow us to place useful constraints on the orbital period and inclination (﹩{P}_{c}={8500}_{-1500}^{+2600}﹩ days, i  c  = 90° ± 16°). The resulting mass of HAT-P-2 c is ﹩{10.7}_{-2.2}^{+5.2}﹩                      M j, establishing it as a substellar-mass object. We indicate the next observing window (2023 April 1–2023 September 28) with green shading. Further RV observations would help to improve constraints on the companion’s orbit.
Paper: Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c
Authors: Zoë L. de Beurs, Julien de Wit, Alexander Venner, David Berardo, Jared Bryan, Joshua N. Winn, Benjamin J. Fulton, Andrew W. Howard
Figure caption: Expected RVs for the first orbit of the current observing window (2023 April 1–2023 April 5). (a) This is a zoomed-in version of Figure A1 and demonstrates the differences in expected RVs more clearly for a singular orbit. (b) The two best-fit models (ii), (vi) are plotted side by side to compare their differences. In green, we indicate the three orbital phases we propose to sample three times to detect the orbital evolution or lack thereof. (c) The residual RVs from subtracting the expected RVs from model (vi) from model (iii).
Paper: Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c
Authors: Zoë L. de Beurs, Julien de Wit, Alexander Venner, David Berardo, Jared Bryan, Joshua N. Winn, Benjamin J. Fulton, Andrew W. Howard
Figure caption: Expected RVs for each orbital model for the current observing window (2022 April 1–2023 September 28). (a) The expected RVs for the six orbital models from Table 1 are plotted for 32 orbits starting on 2022 April 1. (b) The expected RVs minus the long-period companion are plotted. (c) The expected RVs minus HAT-P-2 c are plotted.
Paper: Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c
Authors: Zoë L. de Beurs, Julien de Wit, Alexander Venner, David Berardo, Jared Bryan, Joshua N. Winn, Benjamin J. Fulton, Andrew W. Howard
Figure caption: Variation in orbital shape over time for HAT-P-2 as e and ω increase linearly over time. The long-period companion is modeled as a quadratic trend here. The trends in e and ω were fit using the entire data set, but for visualization the data is split into four equal-sized chunks (∼25 observations per chunk) here. The median model corresponding to that time period is computed using the median e and ω for the corresponding time period.
Paper: Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c
Authors: Zoë L. de Beurs, Julien de Wit, Alexander Venner, David Berardo, Jared Bryan, Joshua N. Winn, Benjamin J. Fulton, Andrew W. Howard
Figure caption: Comparison of our evolving orbital models. From top to bottom, we include the evolving one-planet model with no background trends (a), (b); the evolving two-planet model with the long-period companion modeled as a Keplerian (c), (d); and the evolving two-planet model with the long-period companion modeled as a quadratic trend (e), (f). For more details on these orbital models, see Section 3.1. The color-coding is identical to Figure 1.
Paper: Revisiting Orbital Evolution in HAT-P-2 b and Confirmation of HAT-P-2 c
Authors: Zoë L. de Beurs, Julien de Wit, Alexander Venner, David Berardo, Jared Bryan, Joshua N. Winn, Benjamin J. Fulton, Andrew W. Howard
Figure caption: The orbital period distribution of HAT-P-2 c for our joint RV-astrometry fit (blue) vs. RV-only (black).
Paper: GJ 357 d: Potentially Habitable World or Agent of Chaos?
Authors: Stephen R. Kane, Tara Fetherolf
Figure caption: Dynamical stability results for the system architecture cases that vary the inclination, mass, and eccentricity of planet d. Each panel shows the percentage of the simulation that the injected planet survived as a function of semimajor axis, shown as a solid line. As for Figure 1, the CHZ is shown in light green and the OHZ is shown in dark green. The vertical dashed line indicates the semimajor axis of planet d, and the mass and eccentricity for planet d are labeled near the top of each panel. The maximum eccentricities of the injected planet through the simulations are shown as black dots (see Section 3.3).
Paper: GJ 357 d: Potentially Habitable World or Agent of Chaos?
Authors: Stephen R. Kane, Tara Fetherolf
Figure caption: The architecture and HZ of the GJ 357 system, where the scale of the figure is 0.57 au along each side. The CHZ is shown in light green, the OHZ extensions to the HZ are shown in dark green, and the orbits of the known planets are shown as solid circles.
Paper: GJ 357 d: Potentially Habitable World or Agent of Chaos?
Authors: Stephen R. Kane, Tara Fetherolf
Figure caption: The TESS PDCSAP light curve of GJ 357, which includes photometry obtained during Sectors 8 (top panel), 35 (middle panel), and 62 (bottom panel). Transits of the inner planet, GJ 357 b, can be seen in the light curve every ∼4 days. The vertical dashed lines in the middle and bottom panels indicate the predicted inferior conjunction passage for planet d.
Paper: The Most Sensitive SETI Observations Toward Barnard's Star with FAST
Authors: Zhen-Zhao Tao, Bo-Lun Huang, Xiao-Hang Luan, Jian-Kang Li, Hai-Chen Zhao, Hong-Feng Wang, Tong-Jie Zhang, 同杰 张
Figure caption: Histograms of hits and events for XX as functions of frequency, drift rate and S/N. Frequency bands of cataloged interference sources are displayed on the frequency panel. The blue bars show the distributions of the hits detected by all 19 beams. The orange bars show the distributions of the events detected by Beam 1.
Paper: The Most Sensitive SETI Observations Toward Barnard's Star with FAST
Authors: Zhen-Zhao Tao, Bo-Lun Huang, Xiao-Hang Luan, Jian-Kang Li, Hai-Chen Zhao, Hong-Feng Wang, Tong-Jie Zhang, 同杰 张
Figure caption: Histograms of hits and events for YY as functions of frequency, drift rate and S/N.
Paper: The Most Sensitive SETI Observations Toward Barnard's Star with FAST
Authors: Zhen-Zhao Tao, Bo-Lun Huang, Xiao-Hang Luan, Jian-Kang Li, Hai-Chen Zhao, Hong-Feng Wang, Tong-Jie Zhang, 同杰 张
Figure caption: Schematic diagram of FAST’s 19-beam receiver, the beam filled with green is Beam 1, which tracks the target star during the entire observation; the six outermost beams filled with orange are sufficiently separated from Beam 1 and act as the reference beams.
Paper: The Most Sensitive SETI Observations Toward Barnard's Star with FAST
Authors: Zhen-Zhao Tao, Bo-Lun Huang, Xiao-Hang Luan, Jian-Kang Li, Hai-Chen Zhao, Hong-Feng Wang, Tong-Jie Zhang, 同杰 张
Figure caption: Simulated FAST received signals from radio transmitters of different powers on the surface of Barnard’s Star B (drift rate is 0.2 Hz s−1): top (EIRP ≈109 W), bottom (EIR ≈1013 W).
Paper: The Most Sensitive SETI Observations Toward Barnard's Star with FAST
Authors: Zhen-Zhao Tao, Bo-Lun Huang, Xiao-Hang Luan, Jian-Kang Li, Hai-Chen Zhao, Hong-Feng Wang, Tong-Jie Zhang, 同杰 张
Figure caption: Pseudosinusoidal relative frequency curves of long-term observations for Barnard’s Star b.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: Apparent orbit of BU 1163. The green crosses represent the micrometric observations, the empty blue circles denote observations made with eyepiece interferometer, the red H the Hipparcos observations, the filled blue circles correspond to the speckle observations, and the magenta cross the last observation used in the calculation of the orbit, which provides the current relative position of the components in the apparent orbit.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: Flowchart of the calculation process.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: Different parallaxes for each star. They show a good agreement between them in most cases.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: Apparent orbit of S 634 AaAb. .
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: Apparent orbit of CHR 240.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: HR diagram and isochrones for BU 1163.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: Apparent orbit of HDS 3053.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: HR diagram and isochrones for S 634 AaAb.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: HR diagram and isochrones for HDS 1895.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: HR diagram and isochrones for CHR 240.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: Apparent orbit of BAG 25 AaAb.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: Apparent orbit of HDS 1895.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: Apparent orbit of STF 2173.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: Apparent orbit of HO 276.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: HR diagram and isochrones for HDS 3053.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: HR diagram and isochrones for BAG 25 AaAb.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: HR diagram and isochrones for STF 2173.
Paper: A Study of Eight Visual-spectroscopic Southern Binaries Using Recent SOAR Observations
Authors: José A. Docobo, Pedro P. Campo, Jorge Gómez, René A. Méndez, Edgardo Costa
Figure caption: HR diagram and isochrones for HO 276.
Paper: Radio-optical Reference Catalog, Version 1
Authors: Valeri V. Makarov, Megan C. Johnson, Nathan J. Secrest
Figure caption: Left-hand panel: Histogram of the X-values of the radio-optical position offsets of S/X sources matched in ICRF3 and Gaia DR3. The expected Rayleigh (ν = 1) distribution is shown with the black line. Right-hand panel: Log–log histogram of the phot_bp_rp_excess_factor values for the same sources from Gaia DR3.
Paper: Radio-optical Reference Catalog, Version 1
Authors: Valeri V. Makarov, Megan C. Johnson, Nathan J. Secrest
Figure caption: Graphical presentation of the VSH-fitted Gaia−S/X position offsets on the celestial sphere in the Aitoff equatorial projection. Orange dots at the origin of vectors indicate the actual position of S/X sources. The length and direction of small vectors represent the cumulative VSH fit for the corresponding point. The median length of the arrows is 56  μas. The gray line shows the location of the nominal Galactic equator.
Paper: Radio-optical Reference Catalog, Version 1
Authors: Valeri V. Makarov, Megan C. Johnson, Nathan J. Secrest
Figure caption: Graphical presentation of the VSH-fitted Gaia−K position offsets on the celestial sphere in the Aitoff equatorial projection. Orange dots at the origin of vectors indicate the actual position of K sources. The length and direction of small vectors represent the cumulative VSH fit for the corresponding point. The median length of the arrows is 100  μas. The gray line shows the location of the nominal Galactic equator.
Paper: Radio-optical Reference Catalog, Version 1
Authors: Valeri V. Makarov, Megan C. Johnson, Nathan J. Secrest
Figure caption: Histograms of angular separations of ICRF3 S/X sources from matched Gaia DR3 counterparts in the log–log scale. Left-hand panel: Separations of the primary, i.e., nearest matches. Right-hand panel: Separations of the second-nearest neighbors, if any.
Paper: Confirming Resonance in Three Transiting Systems
Authors: Tyler Quinn, Mariah G. MacDonald
Figure caption: Example evolution of systems like Kepler-254, forming the resonant chain through three formation pathways: eccentricity damping only, short-scale migration, and long-scale migration. The period ratio marked as black dots is the ratio between planets b and c, the period ratio marked as green dots is the ratio between planets c and d, and the vertical red line indicates when we “turn off” the damping effects. Both eccentricity dampening and short-scale migration are lock the planets into both two-body resonances while only short-scale migration results in the libration of the three-body angle 3λ  d  − 4λ  c  − λ  b , which we find to be circulating. Long-scale migration did not lead to enough simulations remaining stable to yield statistically significant results.
Paper: Confirming Resonance in Three Transiting Systems
Authors: Tyler Quinn, Mariah G. MacDonald
Figure caption: Example evolution of systems like Kepler-363, forming the resonant chain through three formation pathways: eccentricity damping only, short-scale migration, and long-scale migration. The period ratio marked as black dots is the ratio between planets b and c, the period ratio marked as green dots is the ratio between planets c and d, and the vertical red line indicates when we “turn off” the damping effects. Although each pathway is able to lock the planets into both two-body resonances, both short-scale migration and long-scale migration result in the libration of the three-body angle 3λ  d  − 4λ  c  − λ  b , which we find to be circulating.
Paper: Confirming Resonance in Three Transiting Systems
Authors: Tyler Quinn, Mariah G. MacDonald
Figure caption: Example evolution of the orbital periods, eccentricities, inclinations, all four two-body resonant angles, and the three-body resonant angle of the three planets of Kepler-363. We find that the two-body angles Θ b,c , Θ c,d , and ﹩{{\rm{\Theta }}}_{c,d}^{{\prime} }﹩, librate in nearly all of our simulations, but the corresponding three-body angle circulates in each one. The initial values for this simulation were drawn from independent, normal distributions, as described in Section 2 and summarized in Table 1. We integrate this simulation beyond 10 Myr for visualization purposes.
Paper: Accurate and Efficient Photoeccentric Transit Modeling
Authors: Mason G. MacDougall, Gregory J. Gilbert, Erik A. Petigura
Figure caption: Diagram showing (bottom middle) our grid of injected e and b values, along with (top) a gallery of phase-folded light curves for all combinations of S/N and injected ω values (at e = 0.2 and b = 0.7, as an example). The four panels to the left and right of the bottom grid show demonstrative examples of phase-folded light curves at the different extremes of our injected parameter grid (e.g., b  =   0.1 or 0.9 and e  =   0.05 or 0.8), all shown with ω = 132° and S/N = 40. Each light curve is shown with the median final transit fits from both the e–ω–ρ (orange) and T 14 + umb (blue) modeling methods, which overlap almost entirely.
Paper: Accurate and Efficient Photoeccentric Transit Modeling
Authors: Mason G. MacDougall, Gregory J. Gilbert, Erik A. Petigura
Figure caption: Comparison of e values measured from the T 14 + umb and e–ω–ρ modeling methods at the 15th, 50th, and 85th percentiles of their distributions, along with the residuals Δe  k  for each comparison (e.g., Δe 50 = e 50,e ω ρ  − e 50,umb). We show Δe  k ={0.05, 0.1, 0.15} in gray, as well as the ideal 1-to-1 line shown in black. These comparisons generally lie close to the 1-to-1 line, implying that the results of the two models are approximately equivalent. We see no trends in the residuals of these comparisons.
Paper: Accurate and Efficient Photoeccentric Transit Modeling
Authors: Mason G. MacDougall, Gregory J. Gilbert, Erik A. Petigura
Figure caption: Diagram demonstrating an overview of our modeling procedure, from an input synthetic light curve to output e and ω constraints via both the e–ω–ρ (orange) and T 14 + umb (blue) modeling methods.
Paper: Performance of the Quasar Spectral Templates for the Dark Energy Spectroscopic Instrument
Authors: Allyson Brodzeller, Kyle Dawson, Stephen Bailey, Jiaxi Yu, A. J. Ross, A. Bault, S. Filbert, J. Aguilar, S. Ahlen, David M. Alexander, E. Armengaud, A. Berti, D. Brooks, E. Chaussidon, A. de la Macorra, P. Doel, K. Fanning, V. A. Fawcett, A. Font-Ribera, S. Gontcho A Gontcho, J. Guy, K. Honscheid, S. Juneau, R. Kehoe, T. Kisner, Anthony Kremin, Ting-Wen Lan, M. Landriau, Michael E. Levi, C. Magneville, Paul Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, W. J. Percival, F. Prada, C. Ravoux, Graziano Rossi, C. Saulder, M. Siudek, Gregory Tarlé, B. A. Weaver, S. Youles, Zheng Zheng, Rongpu Zhou, Zhimin Zhou
Figure caption: The high-redshift templates are shown on the left in black and cover 1.4 < z < 7.0. The low-redshift templates are shown on the right in black and cover 0.05 < z < 1.6. The previous DESI QSO templates are overlaid in red in both figures. The previous templates are trimmed to the wavelength coverage of the new templates and scaled for clarity in comparison. Prominent QSO emission lines are annotated on the mean spectra. The gray shading indicates the wavelength region that is poorly constrained in both eigenspectra sets owing to low QSO numbers and degraded spectrophotometric calibration at the shortest wavelengths of SDSS spectra.
Paper: Performance of the Quasar Spectral Templates for the Dark Energy Spectroscopic Instrument
Authors: Allyson Brodzeller, Kyle Dawson, Stephen Bailey, Jiaxi Yu, A. J. Ross, A. Bault, S. Filbert, J. Aguilar, S. Ahlen, David M. Alexander, E. Armengaud, A. Berti, D. Brooks, E. Chaussidon, A. de la Macorra, P. Doel, K. Fanning, V. A. Fawcett, A. Font-Ribera, S. Gontcho A Gontcho, J. Guy, K. Honscheid, S. Juneau, R. Kehoe, T. Kisner, Anthony Kremin, Ting-Wen Lan, M. Landriau, Michael E. Levi, C. Magneville, Paul Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, W. J. Percival, F. Prada, C. Ravoux, Graziano Rossi, C. Saulder, M. Siudek, Gregory Tarlé, B. A. Weaver, S. Youles, Zheng Zheng, Rongpu Zhou, Zhimin Zhou
Figure caption: Red circles (blue squares) indicate the median redshift correction applied to cluster composite spectra of each low (high) redshift bin, including the z < 0.35 bin. Error bars indicate the 16th and 84th percentiles of each distribution.
Paper: Performance of the Quasar Spectral Templates for the Dark Energy Spectroscopic Instrument
Authors: Allyson Brodzeller, Kyle Dawson, Stephen Bailey, Jiaxi Yu, A. J. Ross, A. Bault, S. Filbert, J. Aguilar, S. Ahlen, David M. Alexander, E. Armengaud, A. Berti, D. Brooks, E. Chaussidon, A. de la Macorra, P. Doel, K. Fanning, V. A. Fawcett, A. Font-Ribera, S. Gontcho A Gontcho, J. Guy, K. Honscheid, S. Juneau, R. Kehoe, T. Kisner, Anthony Kremin, Ting-Wen Lan, M. Landriau, Michael E. Levi, C. Magneville, Paul Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, W. J. Percival, F. Prada, C. Ravoux, Graziano Rossi, C. Saulder, M. Siudek, Gregory Tarlé, B. A. Weaver, S. Youles, Zheng Zheng, Rongpu Zhou, Zhimin Zhou
Figure caption: Flowchart of the template development process.