adsabs/AstroCLIMB huggingface dataset:
Paper: Preparing to Discover the Unknown with Rubin LSST: Time Domain
Authors: Xiaolong Li, Fabio Ragosta, William I. Clarkson, and Federica B. Bianco
Figure caption: The figure of merit FoMEG (a) and FoMGal (b) for all OpSim runs (for the WFD survey, selected as proposalId=1 in the SQL query; see Section 2) based on footprint coverage and star count with image pairs in the same filter (measuring light-curve shape) as described in Section 5 (Equation (5)). Colors and symbols denote filter combinations using the same conventions as in Figure 5. The two FoMs go hand in hand, with small differences in the ranking.
Paper: Preparing to Discover the Unknown with Rubin LSST: Time Domain
Authors: Xiaolong Li, Fabio Ragosta, William I. Clarkson, and Federica B. Bianco
Figure caption: The same as Figure 9 but for image pairs in different filters (measuring color) as described in Section 5 (Equation (5)). Colors and symbols denote filter combinations using the same conventions as in Figure 5.
Paper: Preparing to Discover the Unknown with Rubin LSST: Time Domain
Authors: Xiaolong Li, Fabio Ragosta, William I. Clarkson, and Federica B. Bianco
Figure caption: Bar plot showing the performance for our final five-fold FoM ranked by family’s top-performing OpSim: (a) for WFD observations selected by setting proposalId=1, and (b) all observations not identified with DDF. Arrows point to the OpSims that are also shown in the radar plots in Figure 12. This plot is discussed in Section 6.
Paper: Preparing to Discover the Unknown with Rubin LSST: Time Domain
Authors: Xiaolong Li, Fabio Ragosta, William I. Clarkson, and Federica B. Bianco
Figure caption: Radar plots showing the highest-performing OpSim in each of the top four OpSim families, plus short_exp_2ns_1exp (in purple: this is the most well-balanced of the OpSims for WFD), for (a) the WFD survey (proposalId=1), and (b) for all regions excluding the DDFs. An interactive version of this plot is available at https://xiaolng.github.io/widgets/radar.html (see Appendix B). These present the metrics as the vertices of a polygon with the metric value mapped to the distance from the center of the polygon. With multiple OpSims plotted in the same radar plot, we can compare the tensions between FoM components, while the total area inside of the polygon is a measure of the overall quality of the OpSim. For our FoM, which is the simple sum of five components, this visualization is well suited to provide a synoptic view. This plot is discussed in Section 6.1.
Paper: Preparing to Discover the Unknown with Rubin LSST: Time Domain
Authors: Xiaolong Li, Fabio Ragosta, William I. Clarkson, and Federica B. Bianco
Figure caption: The footprint of the GP and Magellanic Clouds. The definition of these spatial regions and the selection of the corresponding footprint are described in Section 6.2. We select 254 fields for the GP, 12 fields for the LMC, and five fields for the SMC. The color shows the number of visits in baseline_v1.5 in six bands in each field.
Paper: Preparing to Discover the Unknown with Rubin LSST: Time Domain
Authors: Xiaolong Li, Fabio Ragosta, William I. Clarkson, and Federica B. Bianco
Figure caption: Bar plot, as Figure 11, showing OpSims ranked by family, but this time for three selected spatial regions: (a) the GP, (b) the LMC, and (c) the SMC. Only visits allocated to the WFD (labeled as proposalId=1) are counted. Arrows point to the OpSims that are also shown in the radar plots in Figure 12. The twilight and short families of OpSims perform best on the GP, as they did over the entire WFD footprint, while wfd_depth, formerly ranked third, is now ranked the seventh. But in reality, the top-performing OpSims in most families all perform similarly. The main differences are generally driven by FoMtGaps in the same filter. Only eight OpSims cover the SMC, and only five cover both the LMC and SMC with WFD-identified observations. See Section 6.2.
Paper: Preparing to Discover the Unknown with Rubin LSST: Time Domain
Authors: Xiaolong Li, Fabio Ragosta, William I. Clarkson, and Federica B. Bianco
Figure caption: The same as Figure 14 but with all visits excluding DDFs being counted for the mini-survey spatial regions: (a) GP, (b) LMC, and (c) SMC. Arrows point to the OpSims that are also shown in the radar plots in Figure 12. While the footprint family has the best-performing OpSim overall for the GP (footprint_gp_smooth), it also has the worst-performing OpSims, showing the largest dynamical range due to the combined effects of both the footprint and time-gap metrics. Meanwhile, all filterdist OpSims perform well. However, the LMC and SMC are now covered with most OpSims, with the exception of the filtdist family. See Section 6.2.
Paper: Preparing to Discover the Unknown with Rubin LSST: Time Domain
Authors: Xiaolong Li, Fabio Ragosta, William I. Clarkson, and Federica B. Bianco
Figure caption: Bar plot showing the ranking of OpSims based on our five-fold FoM for WFD visits (selected as proposalId=1). All simulations from OpSim v1.5, OpSim v1.7, and OpSim v1.7.1 are included. Panel (a) shows the result of our FoM while (b) shows the result after scaling down the number of visits in OpSim v1.5 by 9% to isolate the impact of small differences in survey efficiency associated with the single-visit collection strategy (1 × 30 s vs. 2 × 15 s). The contribution of each component of our FoM is shown in the same order as in Figures 11, 14, and 15: flux change, color, depth, footprint, and star count from left to right. This plot is discussed in Section 6.3.
Paper: Preparing to Discover the Unknown with Rubin LSST: Time Domain
Authors: Xiaolong Li, Fabio Ragosta, William I. Clarkson, and Federica B. Bianco
Figure caption: The same as Figure 16 but for all regions of the sky that do not correspond to DDFs. This plot is discussed in Section 6.3.
Paper: Preparing to Discover the Unknown with Rubin LSST: Time Domain
Authors: Xiaolong Li, Fabio Ragosta, William I. Clarkson, and Federica B. Bianco
Figure caption: Parallel coordinate plots showing the change in rank for the top 15 OpSims when using a different “ideal” distribution for time gaps between observations in different filters (leading to color measurements). The OpSims are color-coded by family, as indicated in the legend. This figure is described in Appendix A.
Paper: Preparing to Discover the Unknown with Rubin LSST: Time Domain
Authors: Xiaolong Li, Fabio Ragosta, William I. Clarkson, and Federica B. Bianco
Figure caption: Rank changes after modifying the maximum time gap from two days to 1.5 hr in the FoMEG (see Section 5). OpSims that changed rank quartile are marked in red. This figure is described in Appendix A.
Paper: Preparing to Discover the Unknown with Rubin LSST: Time Domain
Authors: Xiaolong Li, Fabio Ragosta, William I. Clarkson, and Federica B. Bianco
Figure caption: Snapshots of the interactive versions of two kinds of summary plots: a parallel coordinate plot (a) and a radar plot (b). These interactive visualizations are made available to the reader to explore our metrics or load their own. See Appendix B.
Paper: Preparing to Discover the Unknown with Rubin LSST: Time Domain
Authors: Xiaolong Li, Fabio Ragosta, William I. Clarkson, and Federica B. Bianco
Figure caption: Healpixel-based selection of sky areas performed with our widget: convex, concave, and hollow regions can be selected on multiple spatial projections (Mollweide shown). See Appendix B.
Paper: A 12.2 GHz Methanol Maser Survey toward the 6.7 GHz Counterparts Associated with/without UC H II Regions
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, Bin Li, Kai Yang, Xujia Ouyang, Andrej M. Sobolev, Zhang Zhao, Xiao-Qiong Li, and Fan Cai
Figure caption: The spectra of the newly detected 12.2 GHz methanol masers from our survey.
Paper: A 12.2 GHz Methanol Maser Survey toward the 6.7 GHz Counterparts Associated with/without UC H II Regions
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, Bin Li, Kai Yang, Xujia Ouyang, Andrej M. Sobolev, Zhang Zhao, Xiao-Qiong Li, and Fan Cai
Figure caption: Left panel: WISE image (red, 22 μm; green, 4.6 μm; blue, 3.4 μm) of the newly detected 13.4 GHz OH maser sources G6.880+0.093 and G69.539-0.097. Right panel: the 13.4 GHz OH maser spectra of the two sources. As comparisons, the 6.7 GHz methanol maser spectra of G6.880+0.093 and G69.539-0.097 extracted from Caswell et al. (2010) and Yang et al. (2019), respectively, are given.
Paper: A 12.2 GHz Methanol Maser Survey toward the 6.7 GHz Counterparts Associated with/without UC H II Regions
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, Bin Li, Kai Yang, Xujia Ouyang, Andrej M. Sobolev, Zhang Zhao, Xiao-Qiong Li, and Fan Cai
Figure caption: The l − b and l − v distributions and detection rates along the Galactic longitude of the methanol masers in our surveyed sample. The upper panel shows the overall Galactic l − b distributions of our sample sources. The middle panel gives the velocity distributions of the sample sources along the Galactic longitude. In the two panels, the sources with the 12.2 GHz maser detected are marked with red points; other sources are marked with blue points. The lower panel shows the detection rate distributions along the Galactic longitude. Notably, different bin intervals are adopted for sources at different Galactic longitude regions to generate the data points shown in this panel.
Paper: A 12.2 GHz Methanol Maser Survey toward the 6.7 GHz Counterparts Associated with/without UC H II Regions
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, Bin Li, Kai Yang, Xujia Ouyang, Andrej M. Sobolev, Zhang Zhao, Xiao-Qiong Li, and Fan Cai
Figure caption: Left panel: the Galactic plane distributions of the 6.7 and 12.2 GHz methanol masers in our surveyed sample. The red points represent the sources associated with both the 6.7 and 12.2 GHz masers, and the blue points denote the sources associated with only 6.7 GHz methanol masers (the Milky Way background is credited to the Xing-Wu Zheng & Mark Reid BeSSeL/NJU/CFA). Upper right panel: the detection rates of the 12.2 GHz masers for the four main spiral arms and the Local arm. Lower right panel: the detection rate distributions of the 12.2 GHz masers along the Galactocentric distances.
Paper: A 12.2 GHz Methanol Maser Survey toward the 6.7 GHz Counterparts Associated with/without UC H II Regions
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, Bin Li, Kai Yang, Xujia Ouyang, Andrej M. Sobolev, Zhang Zhao, Xiao-Qiong Li, and Fan Cai
Figure caption: The relationships of the integrated luminosity (left panel) and peak luminosity (right panel) between the 12.2 and 6.7 GHz methanol masers. The solid line represents the best fit for their luminosity relationships and the dashed line represents the same luminosities between the 6.7 and 12.2 GHz masers.
Paper: A 12.2 GHz Methanol Maser Survey toward the 6.7 GHz Counterparts Associated with/without UC H II Regions
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, Bin Li, Kai Yang, Xujia Ouyang, Andrej M. Sobolev, Zhang Zhao, Xiao-Qiong Li, and Fan Cai
Figure caption: Histograms of the peak luminosities of the 6.7 GHz methanol masers toward sources with and without 12.2 GHz maser detections. The 6.7 GHz maser sources with 12.2 GHz detections are shown with red bars; the mean of the log peak luminosity is 2.77. The 6.7 GHz methanol maser sources without 12.2 GHz detections are shown with blue bars; the mean of the log peak luminosity is 2.23.
Paper: A 12.2 GHz Methanol Maser Survey toward the 6.7 GHz Counterparts Associated with/without UC H II Regions
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, Bin Li, Kai Yang, Xujia Ouyang, Andrej M. Sobolev, Zhang Zhao, Xiao-Qiong Li, and Fan Cai
Figure caption: Histograms of the spatial sizes of H II regions associated with and without the 12.2 GHz methanol masers. The blue bars represent sources with only the 6.7 GHz methanol masers, and the red bars represent sources with both the 6.7 and 12.2 GHz masers. Obviously, sources with the 6.7 GHz methanol masers have a wider range of spatial sizes of the associated H II regions. For small sized H II regions, there are many more sources without 12.2 GHz masers.
Paper: A 12.2 GHz Methanol Maser Survey toward the 6.7 GHz Counterparts Associated with/without UC H II Regions
Authors: Shi-Min Song, Xi Chen, Zhi-Qiang Shen, Bin Li, Kai Yang, Xujia Ouyang, Andrej M. Sobolev, Zhang Zhao, Xiao-Qiong Li, and Fan Cai
Figure caption: The distributions of the peak luminosities of the methanol masers along the spatial sizes of their associated UC H II regions. In the upper panel, the blue and red dots represent the 12.2 and 6.7 GHz masers, respectively. In the lower panel, the data points in the upper panel are divided into 6 groups to get the average; all groups have 20 points with an exception that the last group has 14 data points. The averaged points with error bars are linked by dashed lines.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: Map of TESS EBs observed in sectors 1–26 in the Galactic reference frame. Depicted in green are all vetted and validated EBs observed with the 2 minute cadence. Depicted in cyan are the simulated EBs brighter than T = 12 (Wells & Prša 2021). The dearth of systems in the region north of the ecliptic plane is due to the change in boresight in sectors 14–16 and 24–26, where the satellite was pointed at +85° instead of the nominal +54° to mitigate excessive contamination by stray Earth light and moonlight in cameras 1 and 2.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: A showcase of interesting objects observed by TESS. The panels on the left display time series and the panels on the right depict phase plots. The objects are, top to bottom: (a) wide eclipsing binary TIC 24935204, (b) benchmark-grade eclipsing binary TIC 33419790, (c) totally eclipsing contact binary TIC 5674169, (d) high-reflection subdwarf binary TIC 31690845, (e) eccentric ellipsoidal binary TIC 11046410, (f) flaring M-dwarf pair TIC 436869712, (g) eclipsing binary with a pulsating component TIC 10891640, (h) multiple signal eclipsing binary TIC 375422201, and (i) quadruple star system TIC 424508303.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: Demonstration of a successful (top panels) and unsuccessful (bottom panels) fit with the two models. The top panels show a system with asymmetric variability outside of eclipse, which cannot be modeled by the two-Gaussian model. However, this does not prevent the model from fitting the eclipses correctly. Polyfit, due to its higher degree of freedom, manages to capture both the eclipses and variability outside of eclipse. The bottom panels show the deficiencies of the two models that cause it to not correctly fit the shallow secondary eclipse: the two-Gaussian model considers it part of the asymmetric variability outside of eclipse that it is unable to model, while polyfit fits the variability as an eclipse instead.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: Combined period distribution for a two-Gaussian and polyfit with comparable ﹩{\chi }_{r}^{2}﹩ (left) and one where polyfit is significantly better (right).
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: The relationship between morphology parameter, logarithm of the period, and primary eclipse widths, as determined from the two-Gaussian model.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: A light curve extracted for each pixel around the target star, where the red line indicates the aperture used to extract the 2 minute cadence SPOC light curve. Left: example of an EB that is on target (TIC 255700967). The overall EB score for this target is 0.87. Right: example of a signal that is not on target (TIC 230530979). The overall EB score for this target is 0.42.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: Histogram showing the distribution of the individual test scores (dashed outlines), which combined, give the overall likelihood of the candidate being a real EB (solid black outlines).
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: The distribution of orbital periods for 4584 EBs observed in sectors 1 through 26. Shades correspond to the number of sectors in which the target was observed.
Paper: TESS Eclipsing Binary Stars. I. Short-cadence Observations of 4584 Eclipsing Binaries in Sectors 1–26
Authors: Andrej Prša, Angela Kochoska, Kyle E. Conroy, Nora Eisner, Daniel R. Hey, Luc IJspeert, Ethan Kruse, Scott W. Fleming, Cole Johnston, Martti H. Kristiansen, Daryll LaCourse, Danielle Mortensen, Joshua Pepper, Keivan G. Stassun, Guillermo Torres, Michael Abdul-Masih, Joheen Chakraborty, Robert Gagliano, Zhao Guo, Kelly Hambleton, Kyeongsoo Hong, Thomas Jacobs, David Jones, Veselin Kostov, Jae Woo Lee, Mark Omohundro, Jerome A. Orosz, Emma J. Page, Brian P. Powell, Saul Rappaport, Phill Reed, Jeremy Schnittman, Hans Martin Schwengeler, Avi Shporer, Ivan A. Terentev, Andrew Vanderburg, William F. Welsh, Douglas A. Caldwell, John P. Doty, Jon M. Jenkins, David W. Latham, George R. Ricker, Sara Seager, Joshua E. Schlieder, Bernie Shiao, Roland Vanderspek, and Joshua N. Winn
Figure caption: The distributions of primary and secondary eclipse depths and their ratios, derived from the polyfit and two-Gaussian models. Note the log scale of the y-axis. Eclipse depth ratios serve as rough proxies for the surface brightness ratios.