adsabs/AstroCLIMB huggingface dataset:
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Same as Figure 5 but for the UVIS2 detector (amp C).
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Same as Figure 1 but for the F814W filter. In this case, photometry for the CALSPEC G-type standard P330E (right-pointing triangles) is also included.
Paper: Gas Dynamics and Star Formation in NGC 6822
Authors: Hye-Jin Park, Se-Heon Oh, Jing Wang, Yun Zheng, Hong-Xin Zhang, W. J. G. De Blok
Figure caption: Nine arbitrarily chosen velocity profiles (black solid lines). From top to bottom, the optimal number of Gaussians describing the individual line profile is 1, 2, and 3. The left, middle, and right columns present velocity profiles whose peak S/N estimated from SGfit is larger than 15, between 15 and 10, and between 10 and 5, respectively. The red dashed-dotted and blue dashed lines present the SGfit and OptGfit results, respectively. The central velocity measured by MOMENTS (green solid), SGfit (red dashed-dotted), and OptGfit (blue dashed) is indicated as vertical lines on the top of each panel. The flux densities derived from SGfit and OptGfit are also shown as horizontal lines on the right of each panel. The estimated peak S/N value of the SGfit result is shown in the top left corner of each panel.
Paper: Gas Dynamics and Star Formation in NGC 6822
Authors: Hye-Jin Park, Se-Heon Oh, Jing Wang, Yun Zheng, Hong-Xin Zhang, W. J. G. De Blok
Figure caption: Two example profiles (black solid lines) showing the S/N cut adopted in this work. The dashed lines in the left panels show the OptGfit results, and their integrated (“i”) and peak (“p”) S/N values are noted in each panel. The central velocities and flux density values are indicated by the vertical and horizontal lines on the top and right sides of each panel, respectively. The resulting Gaussian components obtained after filtering out the ones with low S/N are shown in the right panels.
Paper: Gas Dynamics and Star Formation in NGC 6822
Authors: Hye-Jin Park, Se-Heon Oh, Jing Wang, Yun Zheng, Hong-Xin Zhang, W. J. G. De Blok
Figure caption: The top left panel shows a multiwavelength color-composite image of NGC 6822 using the integrated flux density map from ATCA H I 21 cm (gray), GALEX FUV (blue), and WISE 22 μm (yellow) data. The top right, bottom left, and bottom right panels show moment maps derived using beam sizes of 48.″0 × 48.″0. This beam is shown in the bottom right corner (magenta) of the top right panel.
Paper: Gas Dynamics and Star Formation in NGC 6822
Authors: Hye-Jin Park, Se-Heon Oh, Jing Wang, Yun Zheng, Hong-Xin Zhang, W. J. G. De Blok
Figure caption: The GALEX FUV (a) and WISE-W4 band (b) images of NGC 6822 degraded to 48.0″ × 48.0″. The contour presents H I gas distribution where its column density is higher than 3.6 × 1019 cm−2.
Paper: Gas Dynamics and Star Formation in NGC 6822
Authors: Hye-Jin Park, Se-Heon Oh, Jing Wang, Yun Zheng, Hong-Xin Zhang, W. J. G. De Blok
Figure caption: Map of the number of optimally decomposed Gaussians. Purple, green, and yellow points indicate where the optimal number of Gaussians is one, two, and three, respectively.
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: Pseudo-local subtraction of sky lines in MaNGA. The “images” in the upper panels are stacks of reduced and wavelength-rectified fiber spectra, where each row displays the 1D spectrum from a different fiber. The result in two red wavelength regions (left and right columns) for the standard pipeline output is shown in the upper panels. Systematic residuals near bright sky lines are apparent. A pseudo-local approach (second row of images) where the nonlocal sky sampling is increased to 50% of available fibers shows significant improvement. The mean sky flux and mean residual flux among this set of nearly 300 fibers is shown in the bottom panels.
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: Wavelength-averaged mean differences between subsequent fiber-flat spectra for all MaNGA fibers as observed in a sequence of exposures compiled across many different pluggings and observed on different nights. Each exposure pair is represented by a different color. This is the maximum variation that would be expected. Note the order-of-magnitude larger scale on the y-axis. Instead of tenths of a percent, the throughput normalization is seen to vary at the several percent level.
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: Relative throughput for two arbitrary MaNGA fibers from a sequence of flat-field exposures in which the fibers are plugged in different cartridges with very different stress states. An overall normalization term (illustrated in Figure 11) has been divided out. The stochastic wavelength-dependent response likely results from variations in the far-field illumination output by the fiber.
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: Automated MaNGA pipeline sky subtraction residual errors relative to Poisson expectations. Errors are determined from the measured variance in a set of blank, sky-subtracted fiber spectra taken for the all-sky Plate 8069. The worst sky lines are associated with residual systematic errors of 20%–25% above theoretical predictions. Figure adapted from Law et al. (2016).
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: Standard deviation in the wavelength-dependent difference spectrum between pairs of fiber flats observed with fibers plugged into different plates and under different stress states and conditions. Each exposure pair is represented by a different color. Compared to the stationary instrument test (Figure 5), a greater degree of scatter is observed.
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: Comparison of the clear rotator angle dependence of the rms scatter in fiber flux offsets among IFUs in the experiment where the telescope is fixed and the instrument rotated (left panel) and the one meant to simulate an observing track (right panel).
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: Final Coma intercluster light spectrum (target “ICL1”) obtained using 13.5 on-source hours of MaNGA data and combining 127 fibers. The observations are described and presented in Gu et al. (2020). Here, we also show data redward of 5700 Å, which were not analyzed in Gu et al. (2020).
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: Example FLAMES sky spectrum indicating wavelength regions used for the analysis of sky -subtraction residuals. The top panel indicates “continuum” regions in red, while the bottom panel indicates “sky-line” regions in blue.
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: Final 19 fiber spectrum of Coma Cluster UDG DF7 obtained using 13.5 on-source hours of MaNGA data by Gu et al. (2018). Here, we also show data redward of 5700 Å, which were not analyzed in Gu et al. (2018).
Paper: TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf
Authors: Charles Cadieux, René Doyon, Mykhaylo Plotnykov, Guillaume Hébrard, Farbod Jahandar, Étienne Artigau, Diana Valencia, Neil J. Cook, Eder Martioli, Thomas Vandal, Jean-François Donati, Ryan Cloutier, Norio Narita, Akihiko Fukui, Teruyuki Hirano, François Bouchy, Nicolas B. Cowan, Erica J. Gonzales, David R. Ciardi, Keivan G. Stassun, Luc Arnold, Björn Benneke, Isabelle Boisse, Xavier Bonfils, Andrés Carmona, Pía Cortés-Zuleta, Xavier Delfosse, Thierry Forveille, Pascal Fouqué, João Gomes da Silva, Jon M. Jenkins, Flavien Kiefer, Ágnes Kóspál, David Lafrenière, Jorge H. C. Martins, Claire Moutou, J.-D. do Nascimento, Merwan Ould-Elhkim, Stefan Pelletier, Joseph D. Twicken, Luke G. Bouma, Scott Cartwright, Antoine Darveau-Bernier, Konstantin Grankin, Masahiro Ikoma, Taiki Kagetani, Kiyoe Kawauchi, Takanori Kodama, Takayuki Kotani, David W. Latham, Kristen Menou, George Ricker, Sara Seager, Motohide Tamura, Roland Vanderspek, Noriharu Watanabe
Figure caption: Left panels: Normalized PDCSAP light curve of TOI-1452 from sectors 14 and 21, featuring transits (blue data points), a ∼5% stellar flare event (zoomed in subpanel), and outliers (red data points) either rejected by sigma clipping (3.5σ clip) or manually (sector 21). A quasiperiodic Gaussian process model is depicted with the green curve (details in Section 4.2). The remaining sectors are presented in Figure A1. Right panel: TESS phase-folded corrected transits (32) from sectors 14–26, 40–41, and 47. Binned photometry (8 minute phase bin) is represented with black points. The blue curve shows the best-fit transit model (described in Section 4.3), with the 68% confidence interval envelope in light blue. The residuals of this fit are shown below.
Paper: TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf
Authors: Charles Cadieux, René Doyon, Mykhaylo Plotnykov, Guillaume Hébrard, Farbod Jahandar, Étienne Artigau, Diana Valencia, Neil J. Cook, Eder Martioli, Thomas Vandal, Jean-François Donati, Ryan Cloutier, Norio Narita, Akihiko Fukui, Teruyuki Hirano, François Bouchy, Nicolas B. Cowan, Erica J. Gonzales, David R. Ciardi, Keivan G. Stassun, Luc Arnold, Björn Benneke, Isabelle Boisse, Xavier Bonfils, Andrés Carmona, Pía Cortés-Zuleta, Xavier Delfosse, Thierry Forveille, Pascal Fouqué, João Gomes da Silva, Jon M. Jenkins, Flavien Kiefer, Ágnes Kóspál, David Lafrenière, Jorge H. C. Martins, Claire Moutou, J.-D. do Nascimento, Merwan Ould-Elhkim, Stefan Pelletier, Joseph D. Twicken, Luke G. Bouma, Scott Cartwright, Antoine Darveau-Bernier, Konstantin Grankin, Masahiro Ikoma, Taiki Kagetani, Kiyoe Kawauchi, Takanori Kodama, Takayuki Kotani, David W. Latham, Kristen Menou, George Ricker, Sara Seager, Motohide Tamura, Roland Vanderspek, Noriharu Watanabe
Figure caption: Upper panel: TESS target pixel file of TOI-1452 from sector 14 (11 × 11 pixels subregion). The optimal aperture to extract the PDCSAP photometry is delimited by a black line. Nearby Gaia EDR3 sources are represented with blue circles. TOI-1452 and its 3.″2 companion (TIC 420112587) are shown with a red and a cyan circle, respectively. Lower panel: Same region of the sky observed with OMM-PESTO 1.6 m on 2020 February 22 (see Section 2.2). The visual binary was partially resolved.
Paper: TOI-1452 b: SPIRou and TESS Reveal a Super-Earth in a Temperate Orbit Transiting an M4 Dwarf
Authors: Charles Cadieux, René Doyon, Mykhaylo Plotnykov, Guillaume Hébrard, Farbod Jahandar, Étienne Artigau, Diana Valencia, Neil J. Cook, Eder Martioli, Thomas Vandal, Jean-François Donati, Ryan Cloutier, Norio Narita, Akihiko Fukui, Teruyuki Hirano, François Bouchy, Nicolas B. Cowan, Erica J. Gonzales, David R. Ciardi, Keivan G. Stassun, Luc Arnold, Björn Benneke, Isabelle Boisse, Xavier Bonfils, Andrés Carmona, Pía Cortés-Zuleta, Xavier Delfosse, Thierry Forveille, Pascal Fouqué, João Gomes da Silva, Jon M. Jenkins, Flavien Kiefer, Ágnes Kóspál, David Lafrenière, Jorge H. C. Martins, Claire Moutou, J.-D. do Nascimento, Merwan Ould-Elhkim, Stefan Pelletier, Joseph D. Twicken, Luke G. Bouma, Scott Cartwright, Antoine Darveau-Bernier, Konstantin Grankin, Masahiro Ikoma, Taiki Kagetani, Kiyoe Kawauchi, Takanori Kodama, Takayuki Kotani, David W. Latham, Kristen Menou, George Ricker, Sara Seager, Motohide Tamura, Roland Vanderspek, Noriharu Watanabe
Figure caption: Ground-based transit monitoring of TOI-1452.01 with the PESTO camera installed at OMM. Left panels: Individual transit observations in the i′ band on 2020 February 22 UT and 2021 March 4 UT. Right panel: Transits from the left panels folded in phase, with black points representing the binned photometry (8 minute phase bin). The red curve shows the best-fit transit model (described in Section 4.3), with the 68% confidence interval envelope in transparent red. The residuals are shown below the phase-folded transit.
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: Hot Neptune Desert in R  p –P and M  p –P parameter space, where Neptune-like is defined as M  p  < 100 M ⊕ and R  p  = 2.0–6.0 R ⊕. Data drawn from the NASA Exoplanet Archive (Akeson et al. 2013; NASA Exoplanet Archive 2022). TOI-1272 b and c are depicted as a green point (both panels) and a blue point (left panel), respectively. Relations dictating the upper and lower boundaries of the Hot Neptune Desert from Mazeh et al. (2016) are shown as black dashed lines. Left: mass–period distribution of all planets, with Neptune-like planets shown in red. Right: radius–period distribution of all planets, with Neptune-like planets shown in red and the R  p  = 2 R ⊕ limit shown as a black dotted line.
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: Eccentricity distribution of planets with eccentricity uncertainties of σ  e  < 0.1, comparing shorter-period planets (blue) against longer-period planets (orange). The lines show kernel density estimation fits to the data of the corresponding color. Top: Jupiter-like planets (>6 R ⊕). Bottom: Neptune-like planets (2–6 R ⊕), including TOI-1272b (dashed gray line).
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: Distribution of initialized e  b  –e  c  values for all rebound simulations of the TOI-1272 system. Green–blue contours show regions with the highest density of stable configurations (simulations lasting 106 orbits of the inner planet).
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: Eccentricity distribution of planets with σ  e  < 0.1 (Neptune-like in red, other known planets in gray) as a function of orbital separation, showing TOI-1272 b and c in green and blue, respectively. A periastron distance of 0.03 au is shown as an empirical threshold for rapid tidal eccentricity decay. Three eccentric Neptunes are labeled for reference (Kepler-1656b; TOI-269b, Cointepas et al. 2021; GJ 436b).
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: (a) Best-fit radial velocity model (blue) for Keck/HIRES RV measurements (black) using Radvel (Fulton et al. 2018) in a joint RV–photometry model via juliet (Espinoza et al. 2018), with corresponding residuals shown below. (b), (c) Phase-folded views of the best-fit RV model for TOI-1272 b and c, with binned points shown in red.
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: Same as Figure 21, but for the comparison of different values of the global PAH abundance within 5 au, as described in Section 5.2.6. First row: UV flux in ISM units; second row: gas temperature; third row: CO gas abundance.
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: Same as Figure 21, but for the comparison of different values of the stellar accretion rate within 30 au, as described in Section 5.2.5. First row: dust temperature within; second row: gas temperature; third row: CO gas abundance; fourth row: UV flux in ISM units.
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: Same as Figure 21, but for the comparison of different values of δ gas1 and δ gas2, as described in Section 5.2.3. First row: gas temperature within 30 au; second row: CO gas abundance within 30 au; third row: gas temperature within 5 au; fourth row: CO gas abundance within 5 au.
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: Same as Figure 21, but for comparison of the effect on the dust temperature for different values of r inner within 5 au (right column), as described in Section 5.2.2.
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: Same as Figure 21, but for the comparison of the effect on the CO gas abundance of different values of δ gas2 within 5 au, as described in Section 5.2.3.