adsabs/AstroCLIMB huggingface dataset:
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: Spectra of an example model with T eff = 4000 K, ﹩\mathrm{log}g=0.00﹩ and M = 5 M ⊙, [M/H] = -0.50, τ 9.7 = 0.2. The gray spectrum is the MARCS stellar spectrum. The blue and red spectrum are the input and output spectra of 2-DUST, respectively. The black vertical lines above the spectra represent the output wavelength grid.
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: The 2MASS Color–magnitude diagram including background about 30,000 AGB stars and final 4714 RSGs (red).
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: Histogram of numbers of data points for the RSG sample.
Paper: High-resolution Imaging of a TESS Control Sample: Verifying a Deficit of Close-in Stellar Companions to Exoplanet Host Stars
Authors: Colin Littlefield, Steve B. Howell, David R. Ciardi, Kathryn V. Lester, Mark E. Everett, Elise Furlan, Rachel A. Matson, Sergio B. Fajardo-Acosta, Crystal L. Gnilka
Figure caption: Two-dimensional histograms of the contrast curves used in this study, separated by instrument and bandpass. Detected companions within ρ < 1.″2 are marked with green crosses. Companions detected at wider separations (six at 832 nm and two at 562 nm) are not shown. Many of the companions detected at 832 nm were undetected at 562 nm. The color scale represents the fraction of contrast curves in which a companion could have been detected at a given combination of ρ and Δmag. Note that the range of Δmag varies between the panels because the contrast curves vary from from instrument to instrument.
Paper: High-resolution Imaging of a TESS Control Sample: Verifying a Deficit of Close-in Stellar Companions to Exoplanet Host Stars
Authors: Colin Littlefield, Steve B. Howell, David R. Ciardi, Kathryn V. Lester, Mark E. Everett, Elise Furlan, Rachel A. Matson, Sergio B. Fajardo-Acosta, Crystal L. Gnilka
Figure caption: Left: color–magnitude diagram of the control-star sample compared to that of all TOIs (white circles), showing the absolute TESS magnitude as a function of effective temperature. The color of each control-star marker indicates the 832 nm speckle fraction, defined as the fraction of possible companions that could be detected in that bandpass based on our contrast limits, the instrument field of view, and the Raghavan et al. (2010) binary parameters. Right: histograms of the speckle fraction for each bandpass.
Paper: High-resolution Imaging of a TESS Control Sample: Verifying a Deficit of Close-in Stellar Companions to Exoplanet Host Stars
Authors: Colin Littlefield, Steve B. Howell, David R. Ciardi, Kathryn V. Lester, Mark E. Everett, Elise Furlan, Rachel A. Matson, Sergio B. Fajardo-Acosta, Crystal L. Gnilka
Figure caption: Comparison of effective temperature, stellar radius, and distance between each observed control star and its corresponding TOI. The abscissa in each panel is the fractional difference between a control star’s property and that of the TOI.
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: Mass–radius diagrams of known exoplanets taken from the NASA Exoplanet Archive on 2023 October 25 in gray, with the planets in TOI-1136 highlighted. We include only exoplanets with better than 2σ mass precision. We include composition profiles taken from Zeng et al. (2019) for rock, water, and iron compositions, indicated by a solid line in the figure, and a (Z) in the legend. We include H2 envelopes of different percentages taken from Lopez & Fortney (2014), as the Zeng et al. (2019) profiles may not be as accurate in the regime of large gaseous envelopes (Rogers et al. 2023). These are indicated by dashed lines, and are notated with a (LF) in the plot legend. A wide variety of compositions might explain the bulk density of the planets in TOI-1136, and planet b in particular might have either a small volatile envelope or could be consistent with a “water world”. We place TOI-1136 (h) at its 3σ upper limit, and use a downard arrow to indicate our uncertainty in its mass.
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: We include comparisons of the ﹩\sqrt{e}\cos \omega ﹩ and ﹩\sqrt{e}\sin \omega ﹩ posteriors for each planet in the system. Batygin & Morbidelli (2013) predict that the argument of periastrons of neighboring planets should be anti-aligned when in resonance. Planets in the TOI-1136 system seem to generally follow this principle, a strong indicator that the system experienced Type I migration.
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: Histogram of the difference between the scaled log-likelihood of the training data sets described in Section 5.3 and the scaled test data sets. As a model becomes overfit to data, the training likelihood should become much higher than the test likelihood. Positive values indicate overfitting, and negative values indicate underfitting. A histogram of our grid search results is shown in blue, and a histogram of the 100 samples using our six-planet TTV+RV posterior are shown in red hatches. Our model likelihood differences skew slightly into overfitting, but they are much more highly concentrated around 0 than our grid search.
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: TSM vs. planetary radius of known exoplanets, taken from the Exoplanet Archive on 2023 October 25. We also highlight TRAPPIST-1, Kepler-90, Kepler-11, and V1298 Tau, the systems we discussed as most relevant for comparison with TOI-1136. None of these other systems have TSM values as high as TOI-1136. While several planets in TOI-1136 have only average TSM values, planets c and d are very good for follow-up. We emphasize that the probable existence of an atmosphere on all planets in the TOI-1136 system inflates the system’s TSM values, and the system would be less useful for a study focused on terrestrial planets.
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: Left: a comparison of the rms of the training and test residuals during our cross-validation. The test data sets exhibit higher scatter, but their GP uncertainty is also high, indicating that the model has trouble predicting the held-out, test data set. Right: a histogram of the residuals/uncertainty of the training and test data sets. Despite the large rms of the test data set, its associated uncertainty is also high. Consequently, the predictions are not unreliable, though imprecise. This again indicates slight overfitting, though it is less than in Blunt et al. (2023).
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: A comparison of the posterior samples for mass and eccentricity of a TTV-only six-planet fit to our TTV+RV+GP six-planet fit. The TTV-only posteriors are more precise in most cases, indicating that improved posterior estimates in our model are not necessarily due to inclusion of RVs, but may also be sampler dependent.
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: We highlight the disparate architectures of the highest-known-multiplicity planetary systems, as well as a few systems similar to TOI-1136. We highlight that the candidate seventh planet in TOI-1136 does not have a confidently detected orbital distance. Planet and stellar radii are scaled for comparison to other systems, though we emphasize that the planet–star size is not to scale. None of the systems exhibits a clear analog to any of the others, and all have the potential for very interesting future study.
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: Here we present an amusing rendition of the TOI-1136 system if each body in the system were a duck or duckling, created by coauthor R.H. We encourage any future promotions of work associated with TOI-1136 to use this graphic at their leisure.
Paper: The TESS-Keck Survey. XVII. Precise Mass Measurements in a Young, High-multiplicity Transiting Planet System Using Radial Velocities and Transit Timing Variations
Authors: Corey Beard, Paul Robertson, Fei Dai, Rae Holcomb, Jack Lubin, Joseph M. Akana Murphy, Natalie M. Batalha, Sarah Blunt, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Andrew W. Howard, Dan Huber, Howard Isaacson, Stephen R. Kane, Grzegorz Nowak, Erik A Petigura, Arpita Roy, Ryan A. Rubenzahl, Lauren M. Weiss, Rafael Barrena, Aida Behmard, Casey L. Brinkman, Ilaria Carleo, Ashley Chontos, Paul A. Dalba, Tara Fetherolf, Steven Giacalone, Michelle L. Hill, Kiyoe Kawauchi, Judith Korth, Rafael Luque, Mason G. MacDougall, Andrew W. Mayo, Teo Močnik, Giuseppe Morello, Felipe Murgas, Jaume Orell-Miquel, Enric Palle, Alex S. Polanski, Malena Rice, Nicholas Scarsdale, Dakotah Tyler, Judah Van Zandt
Figure caption: Corner plot highlighting the mass fits to each planet in our adopted model. Blue lines indicate the value reported in D23.
Paper: Free-floating or Wide-orbit? Keck Adaptive-optics Observations of Free-floating Planet Candidates Detected with Gravitational Microlensing
Authors: Przemek Mróz, Makiko Ban, Pierlou Marty, Radosław Poleski
Figure caption: Same as Figure A1, but for event OGLE-2015-BLG-1200.
Paper: Free-floating or Wide-orbit? Keck Adaptive-optics Observations of Free-floating Planet Candidates Detected with Gravitational Microlensing
Authors: Przemek Mróz, Makiko Ban, Pierlou Marty, Radosław Poleski
Figure caption: Images for OGLE-2011-BLG-0284. Left-hand panel: 30″ × 30″ OGLE I-band image, right-hand panel: 30″ × 30″ Keck NIRC2 wide camera H-band image. No NIRC2 narrow-camera images of the target were obtained because of a malfunction of the adaptive-optics system.
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: Luminosity-MLR diagram. The left panel shows the luminosity obtained by integrating the observed SED (L obs), and the right panel shows the luminosity obtained by integrating the best-fit model ﹩{L}_{\mathrm{mod}}﹩. The excluded and retained stars are marked by gray and black, respectively. The red curves represent the best-fitted relations, which are labeled in the diagrams.
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: Comparisons of our luminosity-MLR relations with those from previous works. The left panel show the luminosity obtained by integrating the observation SED (L obs), and the right panel shows the luminosity obtained by integrating the best-fit model ﹩{L}_{\mathrm{mod}}﹩. The retained stars are marked by black. Different curves are the relations from our work and the literature, which are labeled in the diagrams (see Section 5.3).
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: Comparison between our DPR and luminosity and the results of R + 12 (left, middle), and the panel on the right is the comparison between the luminosity obtained by integrating the observed SED and the luminosity obtained by integrating the best-fit model SED.
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: Examples of IRS spectra with high DPR and their classification in our sample. The red line represents the IRS spectral data, and other marks are the same as Figure 5.
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: Histograms of the resultant χ 2. The red, blue, and gray bars represent those of the C-rich, O-rich, and optically thin stars, respectively. The vertical lines show the 95th percentile χ 2 values of the corresponding samples.
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: Histograms of the best-fit values of optical depth (left), effective temperature (middle) and luminosity (right). Red, blue, and gray bars represent those of the C-rich, O-rich, and optically thin RSGs, respectively.
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: Histograms of the best-fit values of DPR ﹩(\dot{{M}_{{\rm{d}}}}﹩; left) and MLR ﹩(\dot{M}﹩; right). Red, blue, and gray bars represent those of the C-rich, O-rich, and optically thin RSGs, respectively.
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: Stellar colors vs. DPR diagrams for the optically thin (gray dots), O-rich (blue dots) and C-rich (red dots) RSG sample.
Paper: Evolved Massive Stars at Low Metallicity. VI. Mass-loss Rate of Red Supergiant Stars in the Large Magellanic Cloud
Authors: Jing Wen, 静 文, Jian Gao, 健 高, Ming Yang, 明 杨, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Tianding Wang, 天丁 王, Biwei Jiang, 碧沩 姜
Figure caption: [3.6]–[8.0] color vs. MLR diagram; we depicted the color—DPR relation obtained from previous work (black) too.
Paper: A Phenomenon Resembling Early Superhumps in a New SU UMa-type Dwarf Nova with a 2 hr Orbital Period
Authors: Rebecca S. Boyle, Colin Littlefield, Peter Garnavich, Ryan Ridden-Harper, Paula Szkody, Patricia Boyd, Krista Lynne Smith
Figure caption: The full Kepler/K2 light curve shown in magnitudes relative to the quiescent magnitude (top panel) and time-resolved power spectrum of K2BS5 (bottom panel). The light curve shows a long-period of quiescence before the steep rise at the beginning of the superoutburst. A decrease in magnitude near the end of the superoutburst precedes an rebrightening event before the system resumes its original state of quiescence. The time-resolved power spectrum shows that periodic variability is present only during the superoutburst.
Paper: A Phenomenon Resembling Early Superhumps in a New SU UMa-type Dwarf Nova with a 2 hr Orbital Period
Authors: Rebecca S. Boyle, Colin Littlefield, Peter Garnavich, Ryan Ridden-Harper, Paula Szkody, Patricia Boyd, Krista Lynne Smith
Figure caption: The ASAS-SN, Gaia, CRTS, and ATLAS extended light curves from February 2005 to April 2022.The more sparse sampling shows evidence of few notable events apart from one superoutburst occurring in September 2019. There are no normal outbursts beyond superoutbursts, a hallmark of WZ Sge systems. The superoutburst observed by Kepler, whose observation time is highlighted in red, is not visible because the system was near solar conjunction at the time.
Paper: A Phenomenon Resembling Early Superhumps in a New SU UMa-type Dwarf Nova with a 2 hr Orbital Period
Authors: Rebecca S. Boyle, Colin Littlefield, Peter Garnavich, Ryan Ridden-Harper, Paula Szkody, Patricia Boyd, Krista Lynne Smith
Figure caption: A distribution of the estimated mass ratio (q) vs. binary orbital period of known WZ Sge stars. The dashed blue line shows the standard CV evolutionary track from Knigge et al. (2011), while the solid blue line represents their optimal binary track. The dashed red line marks the short-period edge of the orbital period gap (Knigge 2006). Confirmed WZ Sge stars from Kato (2015) and Kato (2022b) are labeled in red alongside short-period CV stars from Kato (2022c) in gray. K2BS5 is shown in gold, while the long-period WZ Sge systems RZ Leo and ASASSN-16eg (Wakamatsu et al. 2017) are plotted as blue diamonds.