adsabs/AstroCLIMB huggingface dataset:
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Illustration of the aperture (dashed ellipse) for a resolved galaxy in images from FUV to W4, color coded by the flux intensity in each filter. The aperture is twice the size of the isophote of the galaxy at 25 ﹩\mathrm{mag}\,{\mathrm{arcsec}}^{-2}﹩ in the r band. Optical images come from the coaddition of SDSS Stripe 82 data produced by Fliri & Trujillo (2016). The first panel shows the SDSS gri color composite image provided by the SDSS SkyServer.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Multiband model fitting for a galaxy with a close interacting companion. The original data, best-fit model, and model-subtracted residual map are presented from left to right for each of the 10 bands from u to W2.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Ratio of the flux densities between the model and the data, as a function of M *. The median and standard deviation in each mass bin are indicated by circles and error bars, respectively. Different bands are shown in different colors.
Paper: A Data Science Platform to Enable Time-domain Astronomy
Authors: Michael W. Coughlin, Joshua S. Bloom, Guy Nir, Sarah Antier, Theophile Jegou du Laz, Stéfan van der Walt, Arien Crellin-Quick, Thomas Culino, Dmitry A. Duev, Daniel A. Goldstein, Brian F. Healy, Viraj Karambelkar, Jada Lilleboe, Kyung Min Shin, Leo P. Singer, Tomás Ahumada, Shreya Anand, Eric C. Bellm, Richard Dekany, Matthew J. Graham, Mansi M. Kasliwal, Ivona Kostadinova, R. Weizmann Kiendrebeogo, Shrinivas R. Kulkarni, Sydney Jenkins, Natalie LeBaron, Ashish A. Mahabal, James D. Neill, B. Parazin, Julien Peloton, Daniel A. Perley, Reed Riddle, Ben Rusholme, Jakob van Santen, Jesper Sollerman, Robert Stein, D. Turpin, Avery Wold, Carla Amat, Adrien Bonnefon, Adrien Bonnefoy, Manon Flament, Frank Kerkow, Sulekha Kishore, Shloke Jani, Stephen K. Mahanty, Céline Liu, Laura Llinares, Jolyane Makarison, Alix Olliéric, Inès Perez, Lydie Pont, Vyom Sharma
Figure caption: An example of the multiresolution HEALPix sampling scheme for tiling localizations. The left panel shows an example heat map image representing the localization probabilities; darker, deeper colors represent higher probability densities. The middle panel shows the boundaries of the multiresolution HEALPix tiles on which the sky map was sampled. The right panel shows potential telescope field of views covering that sky map with the sky map confidence level contours included.
Paper: A Data Science Platform to Enable Time-domain Astronomy
Authors: Michael W. Coughlin, Joshua S. Bloom, Guy Nir, Sarah Antier, Theophile Jegou du Laz, Stéfan van der Walt, Arien Crellin-Quick, Thomas Culino, Dmitry A. Duev, Daniel A. Goldstein, Brian F. Healy, Viraj Karambelkar, Jada Lilleboe, Kyung Min Shin, Leo P. Singer, Tomás Ahumada, Shreya Anand, Eric C. Bellm, Richard Dekany, Matthew J. Graham, Mansi M. Kasliwal, Ivona Kostadinova, R. Weizmann Kiendrebeogo, Shrinivas R. Kulkarni, Sydney Jenkins, Natalie LeBaron, Ashish A. Mahabal, James D. Neill, B. Parazin, Julien Peloton, Daniel A. Perley, Reed Riddle, Ben Rusholme, Jakob van Santen, Jesper Sollerman, Robert Stein, D. Turpin, Avery Wold, Carla Amat, Adrien Bonnefon, Adrien Bonnefoy, Manon Flament, Frank Kerkow, Sulekha Kishore, Shloke Jani, Stephen K. Mahanty, Céline Liu, Laura Llinares, Jolyane Makarison, Alix Olliéric, Inès Perez, Lydie Pont, Vyom Sharma
Figure caption: Flowchart for the multimessenger, technical ecosystem envisioned in this platform.
Paper: A Data Science Platform to Enable Time-domain Astronomy
Authors: Michael W. Coughlin, Joshua S. Bloom, Guy Nir, Sarah Antier, Theophile Jegou du Laz, Stéfan van der Walt, Arien Crellin-Quick, Thomas Culino, Dmitry A. Duev, Daniel A. Goldstein, Brian F. Healy, Viraj Karambelkar, Jada Lilleboe, Kyung Min Shin, Leo P. Singer, Tomás Ahumada, Shreya Anand, Eric C. Bellm, Richard Dekany, Matthew J. Graham, Mansi M. Kasliwal, Ivona Kostadinova, R. Weizmann Kiendrebeogo, Shrinivas R. Kulkarni, Sydney Jenkins, Natalie LeBaron, Ashish A. Mahabal, James D. Neill, B. Parazin, Julien Peloton, Daniel A. Perley, Reed Riddle, Ben Rusholme, Jakob van Santen, Jesper Sollerman, Robert Stein, D. Turpin, Avery Wold, Carla Amat, Adrien Bonnefon, Adrien Bonnefoy, Manon Flament, Frank Kerkow, Sulekha Kishore, Shloke Jani, Stephen K. Mahanty, Céline Liu, Laura Llinares, Jolyane Makarison, Alix Olliéric, Inès Perez, Lydie Pont, Vyom Sharma
Figure caption: GCN Page—Analysis Section: here, users can visualize the localizations associated with an event, and query the sources, galaxies, instrument tiles (for a given allocation on an instrument), and observations contained in the different localizations, while restraining their searches based on several parameters: cumulative probability, number of detections, distance in megaparsecs, and first and last detection dates. Other features accessible in this section allow the user to query catalogs of candidates from different alert brokers, run simulations with simsurvey, and generate text-based summaries similar to GCN circulars with added version control. It is also possible to submit the executed observations to treasuremap.space (Wyatt et al. 2020). Side panels can be opened that contain the properties of the event and localizations, light curves, GCN notices and circulars, as well as a comment section for users to communicate their results.
Paper: A Data Science Platform to Enable Time-domain Astronomy
Authors: Michael W. Coughlin, Joshua S. Bloom, Guy Nir, Sarah Antier, Theophile Jegou du Laz, Stéfan van der Walt, Arien Crellin-Quick, Thomas Culino, Dmitry A. Duev, Daniel A. Goldstein, Brian F. Healy, Viraj Karambelkar, Jada Lilleboe, Kyung Min Shin, Leo P. Singer, Tomás Ahumada, Shreya Anand, Eric C. Bellm, Richard Dekany, Matthew J. Graham, Mansi M. Kasliwal, Ivona Kostadinova, R. Weizmann Kiendrebeogo, Shrinivas R. Kulkarni, Sydney Jenkins, Natalie LeBaron, Ashish A. Mahabal, James D. Neill, B. Parazin, Julien Peloton, Daniel A. Perley, Reed Riddle, Ben Rusholme, Jakob van Santen, Jesper Sollerman, Robert Stein, D. Turpin, Avery Wold, Carla Amat, Adrien Bonnefon, Adrien Bonnefoy, Manon Flament, Frank Kerkow, Sulekha Kishore, Shloke Jani, Stephen K. Mahanty, Céline Liu, Laura Llinares, Jolyane Makarison, Alix Olliéric, Inès Perez, Lydie Pont, Vyom Sharma
Figure caption: GCN Page–Observation Plans: here, users select an allocation, the fields of the instrument of the allocation that overlap with a localization, as well as pick the parameters to use from the MMA API class of the instrument. Multiple observation plans can be created simultaneously and combined if necessary. Moreover, buttons allow users to download observability and airmass charts, as well as recompute airmass in real time to show which tiles of the sky map are observable. It is also possible to submit the proposed observations to treasuremap.space (Wyatt et al. 2020). Once created, all observation plans will be listed by instrument, where they can be updated, sent, or deleted to/from an instrument queue.
Paper: A Data Science Platform to Enable Time-domain Astronomy
Authors: Michael W. Coughlin, Joshua S. Bloom, Guy Nir, Sarah Antier, Theophile Jegou du Laz, Stéfan van der Walt, Arien Crellin-Quick, Thomas Culino, Dmitry A. Duev, Daniel A. Goldstein, Brian F. Healy, Viraj Karambelkar, Jada Lilleboe, Kyung Min Shin, Leo P. Singer, Tomás Ahumada, Shreya Anand, Eric C. Bellm, Richard Dekany, Matthew J. Graham, Mansi M. Kasliwal, Ivona Kostadinova, R. Weizmann Kiendrebeogo, Shrinivas R. Kulkarni, Sydney Jenkins, Natalie LeBaron, Ashish A. Mahabal, James D. Neill, B. Parazin, Julien Peloton, Daniel A. Perley, Reed Riddle, Ben Rusholme, Jakob van Santen, Jesper Sollerman, Robert Stein, D. Turpin, Avery Wold, Carla Amat, Adrien Bonnefon, Adrien Bonnefoy, Manon Flament, Frank Kerkow, Sulekha Kishore, Shloke Jani, Stephen K. Mahanty, Céline Liu, Laura Llinares, Jolyane Makarison, Alix Olliéric, Inès Perez, Lydie Pont, Vyom Sharma
Figure caption: Shifts Page: users can see the shifts on a calendar and click on them to display more information and interact with them, as well as create new shifts.
Paper: A Data Science Platform to Enable Time-domain Astronomy
Authors: Michael W. Coughlin, Joshua S. Bloom, Guy Nir, Sarah Antier, Theophile Jegou du Laz, Stéfan van der Walt, Arien Crellin-Quick, Thomas Culino, Dmitry A. Duev, Daniel A. Goldstein, Brian F. Healy, Viraj Karambelkar, Jada Lilleboe, Kyung Min Shin, Leo P. Singer, Tomás Ahumada, Shreya Anand, Eric C. Bellm, Richard Dekany, Matthew J. Graham, Mansi M. Kasliwal, Ivona Kostadinova, R. Weizmann Kiendrebeogo, Shrinivas R. Kulkarni, Sydney Jenkins, Natalie LeBaron, Ashish A. Mahabal, James D. Neill, B. Parazin, Julien Peloton, Daniel A. Perley, Reed Riddle, Ben Rusholme, Jakob van Santen, Jesper Sollerman, Robert Stein, D. Turpin, Avery Wold, Carla Amat, Adrien Bonnefon, Adrien Bonnefoy, Manon Flament, Frank Kerkow, Sulekha Kishore, Shloke Jani, Stephen K. Mahanty, Céline Liu, Laura Llinares, Jolyane Makarison, Alix Olliéric, Inès Perez, Lydie Pont, Vyom Sharma
Figure caption: Analysis section from the GCN event page of GRB 221110A. The GBM region is uploaded after correcting for Earth occultation, which produces a cut on the shape of the original map. The sources detected in the region covered by ZTF are shown as red dots, with their names. The Sources menu allows for in-depth scanning of the candidates, showing cutouts of ZTF, and other surveys, as well as the photometry of the candidate. For this event, all the sources were unrelated to the GRB.
Paper: A Data Science Platform to Enable Time-domain Astronomy
Authors: Michael W. Coughlin, Joshua S. Bloom, Guy Nir, Sarah Antier, Theophile Jegou du Laz, Stéfan van der Walt, Arien Crellin-Quick, Thomas Culino, Dmitry A. Duev, Daniel A. Goldstein, Brian F. Healy, Viraj Karambelkar, Jada Lilleboe, Kyung Min Shin, Leo P. Singer, Tomás Ahumada, Shreya Anand, Eric C. Bellm, Richard Dekany, Matthew J. Graham, Mansi M. Kasliwal, Ivona Kostadinova, R. Weizmann Kiendrebeogo, Shrinivas R. Kulkarni, Sydney Jenkins, Natalie LeBaron, Ashish A. Mahabal, James D. Neill, B. Parazin, Julien Peloton, Daniel A. Perley, Reed Riddle, Ben Rusholme, Jakob van Santen, Jesper Sollerman, Robert Stein, D. Turpin, Avery Wold, Carla Amat, Adrien Bonnefon, Adrien Bonnefoy, Manon Flament, Frank Kerkow, Sulekha Kishore, Shloke Jani, Stephen K. Mahanty, Céline Liu, Laura Llinares, Jolyane Makarison, Alix Olliéric, Inès Perez, Lydie Pont, Vyom Sharma
Figure caption: User Profile–Notifications Preferences: users can activate or deactivate notifications, specify parameters on which to notify, as well as choose where to be notified by clicking the bell icon next to each notification type.
Paper: A Data Science Platform to Enable Time-domain Astronomy
Authors: Michael W. Coughlin, Joshua S. Bloom, Guy Nir, Sarah Antier, Theophile Jegou du Laz, Stéfan van der Walt, Arien Crellin-Quick, Thomas Culino, Dmitry A. Duev, Daniel A. Goldstein, Brian F. Healy, Viraj Karambelkar, Jada Lilleboe, Kyung Min Shin, Leo P. Singer, Tomás Ahumada, Shreya Anand, Eric C. Bellm, Richard Dekany, Matthew J. Graham, Mansi M. Kasliwal, Ivona Kostadinova, R. Weizmann Kiendrebeogo, Shrinivas R. Kulkarni, Sydney Jenkins, Natalie LeBaron, Ashish A. Mahabal, James D. Neill, B. Parazin, Julien Peloton, Daniel A. Perley, Reed Riddle, Ben Rusholme, Jakob van Santen, Jesper Sollerman, Robert Stein, D. Turpin, Avery Wold, Carla Amat, Adrien Bonnefon, Adrien Bonnefoy, Manon Flament, Frank Kerkow, Sulekha Kishore, Shloke Jani, Stephen K. Mahanty, Céline Liu, Laura Llinares, Jolyane Makarison, Alix Olliéric, Inès Perez, Lydie Pont, Vyom Sharma
Figure caption: Source page visualization of the AI-generated summary of using the ChatGPT 3.5 completion service on ZTF 21abqhkjd (Yao et al. 2021).
Paper: A Data Science Platform to Enable Time-domain Astronomy
Authors: Michael W. Coughlin, Joshua S. Bloom, Guy Nir, Sarah Antier, Theophile Jegou du Laz, Stéfan van der Walt, Arien Crellin-Quick, Thomas Culino, Dmitry A. Duev, Daniel A. Goldstein, Brian F. Healy, Viraj Karambelkar, Jada Lilleboe, Kyung Min Shin, Leo P. Singer, Tomás Ahumada, Shreya Anand, Eric C. Bellm, Richard Dekany, Matthew J. Graham, Mansi M. Kasliwal, Ivona Kostadinova, R. Weizmann Kiendrebeogo, Shrinivas R. Kulkarni, Sydney Jenkins, Natalie LeBaron, Ashish A. Mahabal, James D. Neill, B. Parazin, Julien Peloton, Daniel A. Perley, Reed Riddle, Ben Rusholme, Jakob van Santen, Jesper Sollerman, Robert Stein, D. Turpin, Avery Wold, Carla Amat, Adrien Bonnefon, Adrien Bonnefoy, Manon Flament, Frank Kerkow, Sulekha Kishore, Shloke Jani, Stephen K. Mahanty, Céline Liu, Laura Llinares, Jolyane Makarison, Alix Olliéric, Inès Perez, Lydie Pont, Vyom Sharma
Figure caption: Analysis posterior for a fit to ZTF 22abykahf with the Type Ia supernova analysis service.
Paper: A Data Science Platform to Enable Time-domain Astronomy
Authors: Michael W. Coughlin, Joshua S. Bloom, Guy Nir, Sarah Antier, Theophile Jegou du Laz, Stéfan van der Walt, Arien Crellin-Quick, Thomas Culino, Dmitry A. Duev, Daniel A. Goldstein, Brian F. Healy, Viraj Karambelkar, Jada Lilleboe, Kyung Min Shin, Leo P. Singer, Tomás Ahumada, Shreya Anand, Eric C. Bellm, Richard Dekany, Matthew J. Graham, Mansi M. Kasliwal, Ivona Kostadinova, R. Weizmann Kiendrebeogo, Shrinivas R. Kulkarni, Sydney Jenkins, Natalie LeBaron, Ashish A. Mahabal, James D. Neill, B. Parazin, Julien Peloton, Daniel A. Perley, Reed Riddle, Ben Rusholme, Jakob van Santen, Jesper Sollerman, Robert Stein, D. Turpin, Avery Wold, Carla Amat, Adrien Bonnefon, Adrien Bonnefoy, Manon Flament, Frank Kerkow, Sulekha Kishore, Shloke Jani, Stephen K. Mahanty, Céline Liu, Laura Llinares, Jolyane Makarison, Alix Olliéric, Inès Perez, Lydie Pont, Vyom Sharma
Figure caption: JSON-based follow-up interface.
Paper: A Data Science Platform to Enable Time-domain Astronomy
Authors: Michael W. Coughlin, Joshua S. Bloom, Guy Nir, Sarah Antier, Theophile Jegou du Laz, Stéfan van der Walt, Arien Crellin-Quick, Thomas Culino, Dmitry A. Duev, Daniel A. Goldstein, Brian F. Healy, Viraj Karambelkar, Jada Lilleboe, Kyung Min Shin, Leo P. Singer, Tomás Ahumada, Shreya Anand, Eric C. Bellm, Richard Dekany, Matthew J. Graham, Mansi M. Kasliwal, Ivona Kostadinova, R. Weizmann Kiendrebeogo, Shrinivas R. Kulkarni, Sydney Jenkins, Natalie LeBaron, Ashish A. Mahabal, James D. Neill, B. Parazin, Julien Peloton, Daniel A. Perley, Reed Riddle, Ben Rusholme, Jakob van Santen, Jesper Sollerman, Robert Stein, D. Turpin, Avery Wold, Carla Amat, Adrien Bonnefon, Adrien Bonnefoy, Manon Flament, Frank Kerkow, Sulekha Kishore, Shloke Jani, Stephen K. Mahanty, Céline Liu, Laura Llinares, Jolyane Makarison, Alix Olliéric, Inès Perez, Lydie Pont, Vyom Sharma
Figure caption: Scatter plot of sky area in square degrees vs. number of candidates (with at least two detections). The colors correspond to probability.
Paper: Modeling and Orbital Parameters of Kepler Heartbeat Stars
Authors: Min-Yu Li, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Qi-Bin Sun
Figure caption: The eccentricity–period (e–P) diagram. Orange stars indicate the 153 Kepler HBSs in this work. Green and blue pluses indicate 43 OGLE HBSs (Wrona et al. 2022a) and 8 TESS HBSs (Kołaczek-Szymański et al. 2021) with orbital periods less than 10 days, respectively. The gray circles represent the positions of the SB9 binaries (Pourbaix et al. 2004). The two black dashed curves mark an e–P relation of ﹩e=\sqrt{1-{({P}_{0}/P)}^{2/3}}﹩, which is the expected functional form assuming the conservation of angular momentum. The two curves use P 0 of 3 and 20 days. The red dashed line represents an empirical equation for the relation between the upper limit of eccentricity and the orbital period ﹩{e}_{\max }=\tfrac{4}{5}\cdot {\rm{l}}{\rm{o}}{\rm{g}}{P}﹩.
Paper: Modeling and Orbital Parameters of Kepler Heartbeat Stars
Authors: Min-Yu Li, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Qi-Bin Sun
Figure caption: Corner plot of the MCMC fit procedure for KIC 4377638. Red vertical lines indicate the median values of the presented histograms for each parameter. Black vertical dashed lines indicate the posterior distributions at the 16% and 84% quantiles. The unit of T 0 is BJD’ = BJD − 2,400,000.
Paper: Modeling and Orbital Parameters of Kepler Heartbeat Stars
Authors: Min-Yu Li, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Qi-Bin Sun
Figure caption: Same as Figure 1 for KIC 10334122. We have added two colored synthetic light curves with e of 0.5 and 0.6, and only adjusted the amplitude scaling factor S to the appropriate value to make the curve highly consistent with the red line.
Paper: Modeling and Orbital Parameters of Kepler Heartbeat Stars
Authors: Min-Yu Li, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Qi-Bin Sun
Figure caption: Comparison of the orbital parameters (P, e, i, ω) between this work (horizontal axis) and previous works (vertical axis) for the overlapping sample of HBSs. In the top-right (e), bottom-left (i), and bottom-right (ω) panels, the two gray dashed lines present deviations of ±1.°5, ±15°, and ±15°, respectively.
Paper: Modeling and Orbital Parameters of Kepler Heartbeat Stars
Authors: Min-Yu Li, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Qi-Bin Sun
Figure caption: Same as Figure 1 for KIC 7672068. We have added three colored synthetic light curves with i of 30°, 40°, 50°, and the other six parameters equal to those of our fitting results.
Paper: Modeling and Orbital Parameters of Kepler Heartbeat Stars
Authors: Min-Yu Li, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Qi-Bin Sun
Figure caption: Same as Figure 1 for KIC 5877364. We have added a blue synthetic light curve with ω of 90°, and the other six parameters equal to those of our fitting results.
Paper: Modeling and Orbital Parameters of Kepler Heartbeat Stars
Authors: Min-Yu Li, Sheng-Bang Qian, Li-Ying Zhu, Wen-Ping Liao, Er-Gang Zhao, Xiang-Dong Shi, Qi-Bin Sun
Figure caption: Same as Figure 1 for KIC 11923629.
Paper: A Multitransition Methanol Survey toward a Large Sample of High-mass Star-forming Regions
Authors: J. Y. Zhao, J. S. Zhang, Y. X. Wang, J. J. Qiu, Y. T. Yan, H. Z. Yu, J. L. Chen, Y. P. Zou
Figure caption:  N(CH3OH) and X(CH3OH) against T dust (upper panels) and against N(H2) (lower panels) for our E-type (squares) and A-type CH3OH sources (empty circles). The solid line is the fit to the E-type CH3OH and the dashed line to the A-type CH3OH.
Paper: A Multitransition Methanol Survey toward a Large Sample of High-mass Star-forming Regions
Authors: J. Y. Zhao, J. S. Zhang, Y. X. Wang, J. J. Qiu, Y. T. Yan, H. Z. Yu, J. L. Chen, Y. P. Zou
Figure caption: The histograms show the distribution of logL bol, T dust, log﹩{N}_{{{\rm{H}}}_{2}}﹩, and log﹩{N}_{{\mathrm{CH}}_{3}\mathrm{OH}}﹩ for sources with detections of less than 10 (solid lines) and more than 10 CH3OH lines (dashed lines).
Paper: A Multitransition Methanol Survey toward a Large Sample of High-mass Star-forming Regions
Authors: J. Y. Zhao, J. S. Zhang, Y. X. Wang, J. J. Qiu, Y. T. Yan, H. Z. Yu, J. L. Chen, Y. P. Zou
Figure caption: The histograms show the distribution of logL bol, T dust, log﹩{N}_{{{\rm{H}}}_{2}}﹩, and log﹩{N}_{{\mathrm{CH}}_{3}\mathrm{OH}}﹩ for sources without (dashed lines) and with detections of 95 GHz CH3OH masers (solid lines).
Paper: A Multitransition Methanol Survey toward a Large Sample of High-mass Star-forming Regions
Authors: J. Y. Zhao, J. S. Zhang, Y. X. Wang, J. J. Qiu, Y. T. Yan, H. Z. Yu, J. L. Chen, Y. P. Zou
Figure caption: (a) Histogram of the column density ratios of E-type and A-type CH3OH and (b) the E/A ratio against the column density of H2 for our sample.
Paper: Statistical Recovery of 21 cm Visibilities and Their Power Spectra with Gaussian-constrained Realizations and Gibbs Sampling
Authors: Fraser Kennedy, Philip Bull, Michael J. Wilensky, Jacob Burba, Samir Choudhuri
Figure caption: An example set of in-painted visibilities using Scheme 2, for a single 14.6 m E–W baseline. Fifteen percent of the band has been flagged, with a combination of a broad region and several randomly flagged channels. The units of the visibilities are given as janskys. Upper left: amplitude (absolute value) of the “observed” visibilities, including flagged regions. Upper right: amplitude of the mean of the EoR plus foreground realizations from the sampler (i.e., the average over all 800 samples). Lower left: difference between the mean of the EoR plus foreground realizations (upper-right panel) and the true (input) EoR plus foreground model used in the simulation. Lower right: standard deviation of the amplitude of the EoR plus foreground realizations from the sampler (calculated over all 800 samples).
Paper: Statistical Recovery of 21 cm Visibilities and Their Power Spectra with Gaussian-constrained Realizations and Gibbs Sampling
Authors: Fraser Kennedy, Philip Bull, Michael J. Wilensky, Jacob Burba, Samir Choudhuri
Figure caption: First eight foreground principal components (covariance eigenmodes) derived from the frequency–frequency covariance matrix measured from simulations of a 14.6 m E–W baseline. The upper and lower panels show the real and imaginary parts, respectively.
Paper: Tuning the Legacy Survey of Space and Time (LSST) Observing Strategy for Solar System Science
Authors: Megan E. Schwamb, R. Lynne Jones, Peter Yoachim, Kathryn Volk, Rosemary C. Dorsey, Cyrielle Opitom, Sarah Greenstreet, Tim Lister, Colin Snodgrass, Bryce T. Bolin, Laura Inno, Michele T. Bannister, Siegfried Eggl, Michael Solontoi, Michael S. P. Kelley, Mario Jurić, Hsing Wen Lin, 省文 林, Darin Ragozzine, Pedro H. Bernardinelli, Steven R. Chesley, Tansu Daylan, Josef Ďurech, Wesley C. Fraser, Mikael Granvik, Matthew M. Knight, Carey M. Lisse, Renu Malhotra, William J. Oldroyd, Audrey Thirouin, Quanzhi Ye, 泉志 叶
Figure caption: ‘Ayló’chaxnim (previously known in the literature as Vatira) population discovery completeness comparisons for cadences that include a possible low-SE solar system twilight microsurvey (v2.2 simulations). The baseline (reference) simulation with the default scheduler configuration for this cadence experiment is the first entry on the left. These metric values have not been normalized to the baseline’s simulation output since the baseline simulation, which does not include the low-SE twilight microsurvey, finds no ‘Ayló’chaxnims with three nightly pairs over 14 days. Top: discovery completeness for three nightly pairs in 14 days (the Rubin SSP discovery criteria). Bottom: discovery completeness for four detections in a single night for twilight simulations that take four visits per pointing. Simulation legend: twi_neo_repeatX_Y_npZ_v2.2_10yrs for a microsurvey with X repeat visits in Y filter(s) per pointing per twilight observed where Z = 1 (on every night), 2 (one night on/one night off), 3 (one night on/two nights off), 4 (one night on/three nights off), 5 (four nights on/four nights off), 6 (three nights on/four nights off), 7 (two nights on/four nights off).