adsabs/AstroCLIMB huggingface dataset:
Paper: Limits on the Auroral Generation of H3 + in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph
Authors: Aidan Gibbs, Michael P. Fitzgerald
Figure caption: H3 + brown dwarf emission upper limits. Blue lines represent the sensitivity limits placed in this work for brown dwarfs. The red/black line is the observed luminosity of optical Balmer emission for the brown dwarf 2MASSI J183537+32594 (Hallinan et al. 2015) for which total H3 + emission is thought to have similar or higher luminosity depending on auroral mechanisms (Bhardwaj & Gladstone 2000). The green arrow is our estimated Q(3,0) emission luminosity from 2MASSI J1835379+325954 based on its relative cyclotron maser emission intensity compared to Jupiter and assuming the same auroral electron energy distributions as Jupiter. We estimate that JWST/NIRSPEC can reach this 1016 W sensitivity limit to lines around 4 μm for a 2000 K brown dwarf with ∼1 hr of exposure time.
Paper: Limits on the Auroral Generation of H3 + in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph
Authors: Aidan Gibbs, Michael P. Fitzgerald
Figure caption: H3 + planetary emission sensitivities vs. theoretical predictions. Blue/gray dots represent the sensitivity limits placed in this work for extrasolar giant planets. Square points represent the sensitivity limits placed by other works. X points represent the theoretical predictions for extrasolar giant planets. Note that one observed system can contain multiple giant planets. The green line represents the predicted sensitivity by Lenz et al. (2016) of the E-ELT in 6.5 hr of exposure time using an instrument similar to CRIRES (currently on the VLT) to observe the GJ 86 system. Recent models (Chadney et al. 2016) predict that the gray shaded region is the distance from a host star where a planet will reach a maximum H3 + luminosity for a Sun-like or smaller stellar host.
Paper: Limits on the Auroral Generation of H3 + in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph
Authors: Aidan Gibbs, Michael P. Fitzgerald
Figure caption: Spectrum of the M dwarf GJ 876. This star hosts two giant planets, GJ 876 c, which is closer to the star, and GJ 876 b. Each panel is zoomed into the expected position of one or more H3 + emission lines. The top portion of each panel shows the continuum normalized science and telluric model produced by molecfit together, while the bottom portion shows only the science spectrum after the telluric model has been divided out. The expected H3 + line positions are shown separately for each planet. The upper limits for H3 + emission for GJ 876 c from the Q(1,0) and Q(3,0) lines are 2.2 × 1017 W and 6.8 × 1017 W, respectively. The corresponding upper limits for GJ 876 b are 4.7 × 1017 W and 5.2 × 1017 W.
Paper: Limits on the Auroral Generation of H3 + in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph
Authors: Aidan Gibbs, Michael P. Fitzgerald
Figure caption: Spectrum of the free-floating brown dwarf 2MASSI J1835379+325954. Each panel is zoomed into the expected position of one or more H3 + emission lines. The top portion of each panel shows the continuum normalized science and telluric model produced by molecfit together, while the bottom portion shows only the science spectrum after the telluric model has been divided out. Expected H3 + line positions are marked by a red vertical dashed line. The upper limits for H3 + emission from the Q(1,0) and Q(3,0) lines are 6.3 × 1016 W and 6.7 × 1016 W, respectively.
Paper: Limits on the Auroral Generation of H3 + in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph
Authors: Aidan Gibbs, Michael P. Fitzgerald
Figure caption: Estimated EUV flux received by planetary targets. Giant planets observed in this work are shown by black squares. Orange diamonds mark previously observed giant planets by Shkolnik et al. (2006), Laughlin et al. (2008), Lenz et al. (2016), which based on models are likely to have thermospheres too hot to host observable H3 + emission. EUV data are taken from Sanz-Forcada et al. (2011) and are from observations or coronal modeling. HD 192263 was also observed in this work, but EUV estimates are not available.
Paper: Limits on the Auroral Generation of H3 + in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph
Authors: Aidan Gibbs, Michael P. Fitzgerald
Figure caption: Spectrum of the free-floating brown dwarf SIMP J013656.5+093347.3. Each panel is zoomed into the expected position of one or more H3 + emission lines. The top portion of each panel shows the continuum normalized science and telluric model produced by molecfit together, while the bottom portion shows only the science spectrum after the telluric model has been divided out. Expected H3 + line positions are marked by a red vertical dashed line. The upper limits for H3 + emission from the Q(1,0) and Q(3,0) lines are 2.7 × 1016 W and 2.9 × 1016 W, respectively.
Paper: Limits on the Auroral Generation of H3 + in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph
Authors: Aidan Gibbs, Michael P. Fitzgerald
Figure caption: Spectrum of the free-floating brown dwarf LSPM J0036+1821. Each panel is zoomed into the expected position of one or more H3 + emission lines. The top portion of each panel shows the continuum normalized science and telluric model produced by molecfit together, while the bottom portion shows only the science spectrum after the telluric model has been divided out. Expected H3 + line positions are marked by a red vertical dashed line. The upper limits for H3 + emission from the Q(1,0) and Q(3,0) lines are 6.7 × 1016 W and 1.1 × 1017 W, respectively.
Paper: Measuring Elemental Abundances of JWST Target Stars for Exoplanet Characterization. I. FGK Stars
Authors: Jared R. Kolecki, Ji Wang, 吉 王
Figure caption: Surface gravity plotted against the magnitude of NLTE corrections for the O I triplet calculated by Amarsi et al. (2019). The dashed lines represent an application of our extrapolation method used for sulfur corrections to those of oxygen. The linear extrapolation from log(g) = 4.0 to 5.5 at each temperature is represented by the dashed line, in which the corrections at 5.5 are assumed to be equal to zero. The deviation of the true corrections from our approximation is minimal, ≲0.03 dex in the relevant parameter space.
Paper: Measuring Elemental Abundances of JWST Target Stars for Exoplanet Characterization. I. FGK Stars
Authors: Jared R. Kolecki, Ji Wang, 吉 王
Figure caption: An excerpt from the spectrum of HD 209458 in the range of the red edge of the telluric O2 A band (seen here as repeating doublets across the spectrum decreasing in depth from left to right). Highlighted in red are three lines of Si, Mg, and K (from left to right), which were used in our analysis. While the left end of the Mg line (center) overlaps with one of the telluric features, this blending is easily ignored by measuring the equivalent width of a model line profile.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VI. Galactic Chemical Gradient Analysis from APOGEE DR17
Authors: Natalie Myers, John Donor, Taylor Spoo, Peter M. Frinchaboy, Katia Cunha, Adrian M. Price-Whelan, Steven R. Majewski, Rachael L. Beaton, Gail Zasowski, Julia O'Connell, Amy E. Ray, Dmitry Bizyaev, Cristina Chiappini, D. A. García-Hernández, Doug Geisler, Henrik Jönsson, Richard R. Lane, Penélope Longa-Peña, Ivan Minchev, Dante Minniti, Christian Nitschelm, A. Roman-Lopes
Figure caption: The open cluster sample from this study (red dots) overlaid on the models of Chiappini (2009; the blue line) and Minchev et al. (2013, 2014; blue dots). The plots are split into the same age bins used in Figure 9.
Paper: Measuring Elemental Abundances of JWST Target Stars for Exoplanet Characterization. I. FGK Stars
Authors: Jared R. Kolecki, Ji Wang, 吉 王
Figure caption: A comparison of abundance values measured by this work (with 1σ uncertainties) and by Brewer et al. (2016) and Petigura & Marcy (2011). We found that >80% of our measurements fall within 0.1 dex of the literature, which implies good agreement with previously published values, as outlined in Section 5.2.
Paper: Measuring Elemental Abundances of JWST Target Stars for Exoplanet Characterization. I. FGK Stars
Authors: Jared R. Kolecki, Ji Wang, 吉 王
Figure caption: Distribution of Mg/Si ratios of the target stars in LTE and NLTE.
Paper: Implicit Biases in Transit Models Using Stellar Pseudo Density
Authors: Gregory J. Gilbert, Mason G. MacDougall, Erik A. Petigura
Figure caption: Posterior distributions of impact parameter for a random selection of KOIs, organized in logarithmic bins on a P − r grid. Data shown are the posterior MCMC chains from Kepler Data Release 25 (Thompson et al. 2018), described in detail in Rowe et al. (2014) and downloaded from the NASA Exoplanet Archive (Akeson et al. 2013). Each posterior distribution is plotted with 20% opacity so that dark regions indicate where many distributions overlap; colors correspond to the median b value for a given KOI. For visual clarity, a maximum of twelve KOIs are plotted per panel. The horizontal axis of each panel ranges over b = (0, 1.2); the vertical range of each row is different, but the dashed line indicates the same distribution height. The median S/N in each 2D bin is printed in the upper right-hand corner of the grid squares. It is clear from inspection that most of the objects (excluding the largest, highest-S/N objects) show qualitatively similar posterior distributions of b. The similarity is particularly striking for small (low-S/N) objects.
Paper: Implicit Biases in Transit Models Using Stellar Pseudo Density
Authors: Gregory J. Gilbert, Mason G. MacDougall, Erik A. Petigura
Figure caption: Results of the numerical sampling experiment described in Section 3. Each row corresponds to the prior, likelihood, and posterior for a given model parameterization. For visual clarity, the height of the T 14 posterior has been reduced by a factor of 3 on all plots. The difference in the prior distribution on b for rows 1 & 3 compared to rows 2 & 4 stems from the use of r vs. ﹩\mathrm{log}r﹩, respectively. Sampling with a uniform prior on ﹩\tilde{\rho }﹩ (top row) produces a nonuniform prior on T 14 and a biased posterior for b. In contrast, sampling in any of the other parameter bases produces a posterior estimate of b, which matches the prior, except in cases where constraints on r would produce a nontransiting orbit.
Paper: The Stability of Fiber Spectrographs in the Faint-source Regime
Authors: Kevin Bundy, David Law, Nick MacDonald, Kyle B. Westfall, T. Sivarani, Devika Divakar, Matthew Bershady, Meng Gu, Renbin Yan, Namrata Roy, Claire Poppett, Niv Drory
Figure caption: Residuals for each of three fiber pairs after applying cross-beam switching to a set of three AB exposure sequences. The amplitude of residuals is reduced compared to single stare sky subtraction results in Figure 19. Continuum and sky-line regions indicate accuracy biases of ∼1%, while the rms is approximately 9% for both the continuum and sky lines. These numbers reflect both instrument systematics and Poisson statistics.
Paper: Implicit Biases in Transit Models Using Stellar Pseudo Density
Authors: Gregory J. Gilbert, Mason G. MacDougall, Erik A. Petigura
Figure caption: Simulated photometry for a mini-Neptune on a circular 15 day orbit around a Sun-like star, transiting at b = 0.5. The orange line indicates the ground-truth transit model. Gray points show simulated observations at a one minute observing cadence; black circles are binned to 30 minutes. The white noise level was set to S/N = 16, close to the Kepler median. See Table 1 for ground-truth simulation parameters.
Paper: Implicit Biases in Transit Models Using Stellar Pseudo Density
Authors: Gregory J. Gilbert, Mason G. MacDougall, Erik A. Petigura
Figure caption: Posterior corner plots when sampling in the ﹩\tilde{\rho }﹩ basis (orange) vs. the logT 14 basis (purple). The bias on impact parameter, b, is apparent when sampling with ﹩\tilde{\rho }﹩ but is resolved when sampling in T 14.
Paper: The Stability of Fiber Spectrographs in the Faint-source Regime
Authors: Kevin Bundy, David Law, Nick MacDonald, Kyle B. Westfall, T. Sivarani, Devika Divakar, Matthew Bershady, Meng Gu, Renbin Yan, Namrata Roy, Claire Poppett, Niv Drory
Figure caption: Average fractional residuals using “single stare subtraction” of fiber pairs observed in the A position. The total exposure time represented by this plot is 30 minutes.
Paper: Implicit Biases in Transit Models Using Stellar Pseudo Density
Authors: Gregory J. Gilbert, Mason G. MacDougall, Erik A. Petigura
Figure caption: Posterior samples of b from the simulated transit fit (orange histogram, Section 2) and the numerical experiment (purple histogram, Section 3) are nearly perfectly matched by the expected bias from the analytically derived Jacobian (gray shaded region, Section 4).
Paper: The Stability of Fiber Spectrographs in the Faint-source Regime
Authors: Kevin Bundy, David Law, Nick MacDonald, Kyle B. Westfall, T. Sivarani, Devika Divakar, Matthew Bershady, Meng Gu, Renbin Yan, Namrata Roy, Claire Poppett, Niv Drory
Figure caption: Average fractional residuals using “single stare subtraction” of fiber pairs observed in the B position. The total exposure time represented by this plot is 30 minutes.
Paper: The TESS–Keck Survey. XIII. An Eccentric Hot Neptune with a Similar-mass Outer Companion around TOI-1272
Authors: Mason G. MacDougall, Erik A. Petigura, Tara Fetherolf, Corey Beard, Jack Lubin, Isabel Angelo, Natalie M. Batalha, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Emma Esparza-Borges, Akihiko Fukui, Keisuke Isogai, Kiyoe Kawauchi, Mayuko Mori, Felipe Murgas, Norio Narita, Taku Nishiumi, Enric Palle, Hannu Parviainen, Noriharu Watanabe, Jon M. Jenkins, David W. Latham, George R. Ricker, S. Seager, Roland K. Vanderspek, Joshua N. Winn, Allyson Bieryla, Douglas A. Caldwell, Diana Dragomir, M. M. Fausnaugh, Ismael Mireles, David R. Rodriguez
Figure caption: Top: TESS light curve of TOI-1272 from sectors 15, 16, and 22. The gray points show the original TESS SAP light curve and the black points show the TESS-SIP corrected light curve that is used to extract the variability period. The vertical dashed lines mark the gaps between TESS sectors. Bottom left: Lomb–Scargle periodogram of the TESS-SIP corrected light curve. The orbital period and transit depth from the TOI catalog are listed at the top of the panel. Bottom right: phase-folded light curve based on the most significant period detected from the periodogram. The gray points show the TESS-SIP corrected photometry, the black points show the binned data, and the red curve is a sinusoidal fit to the phase-folded light curve. The period, amplitude, and their associated uncertainties from the best-fit sinusoidal function are listed at the top of the panel.
Paper: The TESS–Keck Survey. XIII. An Eccentric Hot Neptune with a Similar-mass Outer Companion around TOI-1272
Authors: Mason G. MacDougall, Erik A. Petigura, Tara Fetherolf, Corey Beard, Jack Lubin, Isabel Angelo, Natalie M. Batalha, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Emma Esparza-Borges, Akihiko Fukui, Keisuke Isogai, Kiyoe Kawauchi, Mayuko Mori, Felipe Murgas, Norio Narita, Taku Nishiumi, Enric Palle, Hannu Parviainen, Noriharu Watanabe, Jon M. Jenkins, David W. Latham, George R. Ricker, S. Seager, Roland K. Vanderspek, Joshua N. Winn, Allyson Bieryla, Douglas A. Caldwell, Diana Dragomir, M. M. Fausnaugh, Ismael Mireles, David R. Rodriguez
Figure caption: Corner plot of exoplanet model posteriors for TOI-1272b, showing the effects of e–ω– b degeneracy on our transit fit. The best-fit value for eccentricity is given by ﹩e={0.40}_{-0.22}^{+0.20}﹩. The argument of periastron ω remained loosely constrained about 90°, suggesting a transit near periastron.
Paper: The TESS–Keck Survey. XIII. An Eccentric Hot Neptune with a Similar-mass Outer Companion around TOI-1272
Authors: Mason G. MacDougall, Erik A. Petigura, Tara Fetherolf, Corey Beard, Jack Lubin, Isabel Angelo, Natalie M. Batalha, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Emma Esparza-Borges, Akihiko Fukui, Keisuke Isogai, Kiyoe Kawauchi, Mayuko Mori, Felipe Murgas, Norio Narita, Taku Nishiumi, Enric Palle, Hannu Parviainen, Noriharu Watanabe, Jon M. Jenkins, David W. Latham, George R. Ricker, S. Seager, Roland K. Vanderspek, Joshua N. Winn, Allyson Bieryla, Douglas A. Caldwell, Diana Dragomir, M. M. Fausnaugh, Ismael Mireles, David R. Rodriguez
Figure caption: Iterative Keplerian periodogram search of TOI-1272 RV data using RVSearch. We confirmed the 3.3 day transiting planet (top panel) and identified a significant 8.7 day period with no corresponding transits (middle panel). ΔBIC was used to discriminate between models with additional Keplerians over a grid of periods (Bayesian information criterion; Schwarz 1978), corresponding to a significance threshold of FAP = 0.001 at the yellow dashed horizontal line. The bottom panel shows a sub-significant signal at a 14.1 day period, likely corresponding to P rot/2.
Paper: The TESS–Keck Survey. XIII. An Eccentric Hot Neptune with a Similar-mass Outer Companion around TOI-1272
Authors: Mason G. MacDougall, Erik A. Petigura, Tara Fetherolf, Corey Beard, Jack Lubin, Isabel Angelo, Natalie M. Batalha, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Emma Esparza-Borges, Akihiko Fukui, Keisuke Isogai, Kiyoe Kawauchi, Mayuko Mori, Felipe Murgas, Norio Narita, Taku Nishiumi, Enric Palle, Hannu Parviainen, Noriharu Watanabe, Jon M. Jenkins, David W. Latham, George R. Ricker, S. Seager, Roland K. Vanderspek, Joshua N. Winn, Allyson Bieryla, Douglas A. Caldwell, Diana Dragomir, M. M. Fausnaugh, Ismael Mireles, David R. Rodriguez
Figure caption: Transit photometry for two independent single transits measured by the MuSCAT2 and MuSCAT instruments, plotted with 10 minute binning and photometric fits by the corresponding instrument pipeline. Horizontal dashed lines indicate the expected transit depth. Top: combined photometry from MuSCAT2 g, r, i, and z  s  bands, observed on UT 2020 February 28. Bottom: photometry from MuSCAT g, r, and z bands, observed on UT 2021 April 8.
Paper: The TESS–Keck Survey. XIII. An Eccentric Hot Neptune with a Similar-mass Outer Companion around TOI-1272
Authors: Mason G. MacDougall, Erik A. Petigura, Tara Fetherolf, Corey Beard, Jack Lubin, Isabel Angelo, Natalie M. Batalha, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Emma Esparza-Borges, Akihiko Fukui, Keisuke Isogai, Kiyoe Kawauchi, Mayuko Mori, Felipe Murgas, Norio Narita, Taku Nishiumi, Enric Palle, Hannu Parviainen, Noriharu Watanabe, Jon M. Jenkins, David W. Latham, George R. Ricker, S. Seager, Roland K. Vanderspek, Joshua N. Winn, Allyson Bieryla, Douglas A. Caldwell, Diana Dragomir, M. M. Fausnaugh, Ismael Mireles, David R. Rodriguez
Figure caption: Top: transit models drawn from parameter posterior distributions (orange; 50 samples) for phase-folded TESS photometry of TOI-1272b. Expected transit shape for a circular orbit is shown in blue, modeled using median posterior distribution values for all other model parameters. Details regarding fitting procedure are discussed in Section 2.2. Bottom: residuals to our maximum a posteriori model.
Paper: The TESS–Keck Survey. XIII. An Eccentric Hot Neptune with a Similar-mass Outer Companion around TOI-1272
Authors: Mason G. MacDougall, Erik A. Petigura, Tara Fetherolf, Corey Beard, Jack Lubin, Isabel Angelo, Natalie M. Batalha, Aida Behmard, Sarah Blunt, Casey Brinkman, Ashley Chontos, Ian J. M. Crossfield, Fei Dai, Paul A. Dalba, Courtney Dressing, Benjamin Fulton, Steven Giacalone, Michelle L. Hill, Andrew W. Howard, Daniel Huber, Howard Isaacson, Stephen R. Kane, Molly Kosiarek, Andrew Mayo, Teo Močnik, Joseph M. Akana Murphy, Daria Pidhorodetska, Alex Polanski, Malena Rice, Paul Robertson, Lee J. Rosenthal, Arpita Roy, Ryan A. Rubenzahl, Nicholas Scarsdale, Emma V. Turtelboom, Dakotah Tyler, Judah Van Zandt, Lauren M. Weiss, Emma Esparza-Borges, Akihiko Fukui, Keisuke Isogai, Kiyoe Kawauchi, Mayuko Mori, Felipe Murgas, Norio Narita, Taku Nishiumi, Enric Palle, Hannu Parviainen, Noriharu Watanabe, Jon M. Jenkins, David W. Latham, George R. Ricker, S. Seager, Roland K. Vanderspek, Joshua N. Winn, Allyson Bieryla, Douglas A. Caldwell, Diana Dragomir, M. M. Fausnaugh, Ismael Mireles, David R. Rodriguez
Figure caption: Lomb–Scargle periodogram search of TOI-1272 S HK data, identifying a significant 28.5 day variability signal consistent with the suspected stellar rotation period.
Paper: Gap Opening and Inner Disk Structure in the Strongly Accreting Transition Disk of DM Tau
Authors: Logan Francis, Nienke van der Marel, Doug Johnstone, Eiji Akiyama, Simon Bruderer, Ruobing Dong, Jun Hashimoto, Hauyu Baobab Liu, Takayuki Muto, Yi Yang
Figure caption: Top panels: 1.3 mm dust continuum images of DM Tau and zoom in on the 21 au dust cavity. Lower-left panels: moment 0 maps of each observed CO line. Lower-right panels: flux of each CO line integrated over the disk vs. the velocity. The beams for the continuum and moment 0 images are shown in the bottom left of each panel as white ellipses.
Paper: Gap Opening and Inner Disk Structure in the Strongly Accreting Transition Disk of DM Tau
Authors: Logan Francis, Nienke van der Marel, Doug Johnstone, Eiji Akiyama, Simon Bruderer, Ruobing Dong, Jun Hashimoto, Hauyu Baobab Liu, Takayuki Muto, Yi Yang
Figure caption: Deprojected and azimuthally averaged intensity profiles of the 1.3 mm dust continuum and moment 0 maps for each observed CO line. The FWHM of the beam is shown by the scalebar.