adsabs/AstroCLIMB huggingface dataset:
Paper: PHANGS–JWST First Results: Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628
Authors: Ashley. T. Barnes, Elizabeth J. Watkins, Sharon E. Meidt, Kathryn Kreckel, Mattia C. Sormani, Robin G. Treß, Simon C. O. Glover, Frank Bigiel, Rupali Chandar, Eric Emsellem, Janice C. Lee, Adam K. Leroy, Karin M. Sandstrom, Eva Schinnerer, Erik Rosolowsky, Francesco Belfiore, Guillermo A. Blanc, Médéric Boquien, Jakob den Brok, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Cosima Eibensteiner, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Sarah Jeffreson, María J. Jiménez-Donaire, Benjamin W. Keller, Ralf S. Klessen, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Jing Li, Daizhong Liu, Laura A. Lopez, Eric J. Murphy, Lukas Neumann, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Florent Renaud, Toshiki Saito, Sumit K. Sarbadhicary, Amy Sardone, Rowan J. Smith, Sophia K. Stuber, Jiayi Sun, David A. Thilker, Antonio Usero, Bradley C. Whitmore, Thomas G. Williams
Figure caption: The prominent bubble structures across the Phantom Galaxy (Messier 74 or NGC 628). In all panels, we show an image produced from the 770W (blue), 1000W (green), and 1130W (red) band filters from the JWST (Lee et al. 2023), and overlaid in orange is the continuum-subtracted HST Hα. The faded circles and ellipses show the positions of the bubbles from Watkins et al. (2023).
Paper: PHANGS–JWST First Results: The 21 μm Compact Source Population
Authors: Hamid Hassani, Erik Rosolowsky, Adam K. Leroy, Médéric Boquien, Janice C. Lee, Ashley T. Barnes, Francesco Belfiore, F. Bigiel, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Eric Emsellem, Christopher M. Faesi, Kathryn Grasha, Jaeyeon Kim, Ralf S. Klessen, Kathryn Kreckel, J. M. Diederik Kruijssen, Kirsten L. Larson, Sharon E. Meidt, Karin M. Sandstrom, Eva Schinnerer, David A. Thilker, Elizabeth J. Watkins, Bradley C. Whitmore, Thomas G. Williams
Figure caption: The SEDs of ISM sources (left) and eye-confirmed background galaxies and stars (HZ and STAR; right). We only consider the sources that have >5σ detections in all (JWST+HST) bands: 384 ISM sources and 30 HZ or STAR sources. The gray lines represent the SED of each object, and the solid colored lines show the mean of all SEDs for each individual galaxy.
Paper: PHANGS–JWST First Results: Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628
Authors: Ashley. T. Barnes, Elizabeth J. Watkins, Sharon E. Meidt, Kathryn Kreckel, Mattia C. Sormani, Robin G. Treß, Simon C. O. Glover, Frank Bigiel, Rupali Chandar, Eric Emsellem, Janice C. Lee, Adam K. Leroy, Karin M. Sandstrom, Eva Schinnerer, Erik Rosolowsky, Francesco Belfiore, Guillermo A. Blanc, Médéric Boquien, Jakob den Brok, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Cosima Eibensteiner, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Sarah Jeffreson, María J. Jiménez-Donaire, Benjamin W. Keller, Ralf S. Klessen, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Jing Li, Daizhong Liu, Laura A. Lopez, Eric J. Murphy, Lukas Neumann, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Florent Renaud, Toshiki Saito, Sumit K. Sarbadhicary, Amy Sardone, Rowan J. Smith, Sophia K. Stuber, Jiayi Sun, David A. Thilker, Antonio Usero, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Distribution of intensity and stellar population in the Phantom Void (see Figure 2). The upper panel shows the intensity distribution of the JWST 7.7 μm, continuum-subtracted Hα emission, HST NUV, ALMA CO, and VLA H I emission, as measured radially from the center of the bubble (see Figure 2). We show the 99th percentile of the intensity in each radial bin, normalized to the value of the maximum bin (this percentile is chosen instead, e.g., the mean value to better highlight where the emission distributions peak). The bottom panel shows the radial age distribution of the stellar association catalog. The size of the points indicate the mass of the stellar associations. In both panels we highlight the position of the the Precursor Phantom Void. We find evidence that younger and more higher mass clusters are preferentially located within the shell, with respect to inside the bubble.
Paper: PHANGS–JWST First Results: Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628
Authors: Ashley. T. Barnes, Elizabeth J. Watkins, Sharon E. Meidt, Kathryn Kreckel, Mattia C. Sormani, Robin G. Treß, Simon C. O. Glover, Frank Bigiel, Rupali Chandar, Eric Emsellem, Janice C. Lee, Adam K. Leroy, Karin M. Sandstrom, Eva Schinnerer, Erik Rosolowsky, Francesco Belfiore, Guillermo A. Blanc, Médéric Boquien, Jakob den Brok, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Cosima Eibensteiner, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Sarah Jeffreson, María J. Jiménez-Donaire, Benjamin W. Keller, Ralf S. Klessen, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Jing Li, Daizhong Liu, Laura A. Lopez, Eric J. Murphy, Lukas Neumann, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Florent Renaud, Toshiki Saito, Sumit K. Sarbadhicary, Amy Sardone, Rowan J. Smith, Sophia K. Stuber, Jiayi Sun, David A. Thilker, Antonio Usero, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Phantom voids in both observations and simulations. Shown in the upper panel is the JWST 7.7 μm emission map. The middle panel shows the isolated galaxy simulation from Tress et al. (2020; the same simulation shown in the bottom panels of their Figure 14). In color scale is the total column density, which we expect (away from regions of active star formation) to correspond well to the 7.7 μm emission (Leroy et al. 2023; Sandstrom et al. 2023). The bottom panel shows the isolated galaxy simulation tuned for NGC 628 from E. Emsellem et al. (2022, in prepararion). We have optimized the color scales such that both maps have a similar qualitative appearance and the physical scales of all panels are matched. We see that large-scale (∼1 kpc-sized) voids are also common within the simulations, several of which are highlighted by the faded white ellipses.
Paper: PHANGS–JWST First Results: Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628
Authors: Ashley. T. Barnes, Elizabeth J. Watkins, Sharon E. Meidt, Kathryn Kreckel, Mattia C. Sormani, Robin G. Treß, Simon C. O. Glover, Frank Bigiel, Rupali Chandar, Eric Emsellem, Janice C. Lee, Adam K. Leroy, Karin M. Sandstrom, Eva Schinnerer, Erik Rosolowsky, Francesco Belfiore, Guillermo A. Blanc, Médéric Boquien, Jakob den Brok, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Cosima Eibensteiner, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Sarah Jeffreson, María J. Jiménez-Donaire, Benjamin W. Keller, Ralf S. Klessen, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Jing Li, Daizhong Liu, Laura A. Lopez, Eric J. Murphy, Lukas Neumann, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Florent Renaud, Toshiki Saito, Sumit K. Sarbadhicary, Amy Sardone, Rowan J. Smith, Sophia K. Stuber, Jiayi Sun, David A. Thilker, Antonio Usero, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Evidence of stellar feedback in the ionized gas tracers toward the voids. From left to right, we show the emission-weighted velocity FWHM maps from the Hα and the [S II]6716 lines, and the emission line ratio [O I]6300/Hα. Overlaid as black contours on each panel is the 7.7 μm emission (see Figure 2). We see elevated line widths distributed throughout the center of the bubble (albeit at low signal-to-noise), which we attribute to turbulence and out-of-plane expansion. Moreover, as highlighted on each panel, we see elevated line widths (>100 km s−1) and line ratios toward the shell, which could be indicative of young SN remnants (J. Li et al. 2022, in preparation).
Paper: PHANGS–JWST First Results: Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628
Authors: Ashley. T. Barnes, Elizabeth J. Watkins, Sharon E. Meidt, Kathryn Kreckel, Mattia C. Sormani, Robin G. Treß, Simon C. O. Glover, Frank Bigiel, Rupali Chandar, Eric Emsellem, Janice C. Lee, Adam K. Leroy, Karin M. Sandstrom, Eva Schinnerer, Erik Rosolowsky, Francesco Belfiore, Guillermo A. Blanc, Médéric Boquien, Jakob den Brok, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Cosima Eibensteiner, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Sarah Jeffreson, María J. Jiménez-Donaire, Benjamin W. Keller, Ralf S. Klessen, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Jing Li, Daizhong Liu, Laura A. Lopez, Eric J. Murphy, Lukas Neumann, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Florent Renaud, Toshiki Saito, Sumit K. Sarbadhicary, Amy Sardone, Rowan J. Smith, Sophia K. Stuber, Jiayi Sun, David A. Thilker, Antonio Usero, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Spectra taken inside of the Phantom Void bubble (see Figure 2). In the left and right panels, we present the average CO (2–1) spectrum obtained from the cube that has had the local velocity field subtracted (including rotational and nonrotational components) and the average H I spectrum, respectively. Gaussian fits to the data are overlaid as gray curves. Residuals are plotted as open points. Below each curve, we show a bar and text showing the measured FWHM (corrected for the instrument spectral resolution).
Paper: PHANGS–JWST First Results: Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628
Authors: Ashley. T. Barnes, Elizabeth J. Watkins, Sharon E. Meidt, Kathryn Kreckel, Mattia C. Sormani, Robin G. Treß, Simon C. O. Glover, Frank Bigiel, Rupali Chandar, Eric Emsellem, Janice C. Lee, Adam K. Leroy, Karin M. Sandstrom, Eva Schinnerer, Erik Rosolowsky, Francesco Belfiore, Guillermo A. Blanc, Médéric Boquien, Jakob den Brok, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Cosima Eibensteiner, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Sarah Jeffreson, María J. Jiménez-Donaire, Benjamin W. Keller, Ralf S. Klessen, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Jing Li, Daizhong Liu, Laura A. Lopez, Eric J. Murphy, Lukas Neumann, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Florent Renaud, Toshiki Saito, Sumit K. Sarbadhicary, Amy Sardone, Rowan J. Smith, Sophia K. Stuber, Jiayi Sun, David A. Thilker, Antonio Usero, Bradley C. Whitmore, Thomas G. Williams
Figure caption: The expansion velocity required for Phantom Void–sized shells to retain a high degree of circularity as they expand in the presence of differential rotation at different locations in the inner disk of NGC 628. Curves show the v exp required for different observed axis ratios q = 0.8 to 0.95 (in steps of 0.05). Here a bubble radius R b = 500 pc is adopted and NGC 628's rotation curve is modeled with a two-parameter fit to the measured rotation curve (Lang et al. 2020). Highlighted are the results corresponding to the approximate galactocentric radius of the Phantom Void.
Paper: PHANGS–JWST First Results: Multiwavelength View of Feedback-driven Bubbles (the Phantom Voids) across NGC 628
Authors: Ashley. T. Barnes, Elizabeth J. Watkins, Sharon E. Meidt, Kathryn Kreckel, Mattia C. Sormani, Robin G. Treß, Simon C. O. Glover, Frank Bigiel, Rupali Chandar, Eric Emsellem, Janice C. Lee, Adam K. Leroy, Karin M. Sandstrom, Eva Schinnerer, Erik Rosolowsky, Francesco Belfiore, Guillermo A. Blanc, Médéric Boquien, Jakob den Brok, Yixian Cao, Mélanie Chevance, Daniel A. Dale, Oleg V. Egorov, Cosima Eibensteiner, Kathryn Grasha, Brent Groves, Hamid Hassani, Jonathan D. Henshaw, Sarah Jeffreson, María J. Jiménez-Donaire, Benjamin W. Keller, Ralf S. Klessen, Eric W. Koch, J. M. Diederik Kruijssen, Kirsten L. Larson, Jing Li, Daizhong Liu, Laura A. Lopez, Eric J. Murphy, Lukas Neumann, Jérôme Pety, Francesca Pinna, Miguel Querejeta, Florent Renaud, Toshiki Saito, Sumit K. Sarbadhicary, Amy Sardone, Rowan J. Smith, Sophia K. Stuber, Jiayi Sun, David A. Thilker, Antonio Usero, Bradley C. Whitmore, Thomas G. Williams
Figure caption: Residual CO velocity toward the voids. Here we show the local, nonrotational flows at the location of the phantom void, constructed from the intensity-weighed centroid velocity map after subtracting the projected rotational velocity (measured by Lang et al. 2020) from each pixel. Overlaid as black contours on each panel is the 7.7 μm emission (see Figure 2).
Paper: Magnetic Field Spectral Evolution in the Inner Heliosphere
Authors: Nikos Sioulas, Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Anna Tenerani, Trevor A. Bowen, Stuart D. Bale, Jia Huang, Loukas Vlahos, L. D. Woodham, T. S. Horbury, Thierry Dudok de Wit, Davin Larson, Justin Kasper, Christopher J. Owen, Michael L. Stevens, Anthony Case, Marc Pulupa, David M. Malaspina, J. W. Bonnell, Roberto Livi, Keith Goetz, Peter R. Harvey, Robert J. MacDowall, Milan Maksimović, P. Louarn, A. Fedorov
Figure caption: Magnetic field spectral index a  B  as a function of V sw and (a) heliocentric distance, (b) advection time τ adv, as well as, a function of distance and (c) normalized cross helicity (σ  c ), (d) normalized residual energy (σ  r ).
Paper: Magnetic Field Spectral Evolution in the Inner Heliosphere
Authors: Nikos Sioulas, Zesen Huang, 泽森 黄, Chen Shi, 辰 时, Marco Velli, Anna Tenerani, Trevor A. Bowen, Stuart D. Bale, Jia Huang, Loukas Vlahos, L. D. Woodham, T. S. Horbury, Thierry Dudok de Wit, Davin Larson, Justin Kasper, Christopher J. Owen, Michael L. Stevens, Anthony Case, Marc Pulupa, David M. Malaspina, J. W. Bonnell, Roberto Livi, Keith Goetz, Peter R. Harvey, Robert J. MacDowall, Milan Maksimović, P. Louarn, A. Fedorov
Figure caption: The radial evolution of (a) the ion inertial length d  i , (b) the ion gyroradius ρ  i , (c) ion plasma β.
Paper: Redder than Red: Discovery of an Exceptionally Red L/T Transition Dwarf
Authors: Adam C. Schneider, Adam J. Burgasser, Justice Bruursema, Jeffrey A. Munn, Frederick J. Vrba, Dan Caselden, Martin Kabatnik, Austin Rothermich, Arttu Sainio, Thomas P. Bickle, Scott E. Dahm, Aaron M. Meisner, J. Davy Kirkpatrick, Genaro Suárez, Jonathan Gagné, Jacqueline K. Faherty, Johanna M. Vos, Marc J. Kuchner, Stephen J. Williams, Daniella Bardalez Gagliuffi, Christian Aganze, Chih-Chun Hsu, Christopher Theissen, Michael C. Cushing, Federico Marocco, Sarah Casewell
Figure caption: MCMC forward-model fit of the normalized 2.26–2.38 μm spectrum of CWISE J0506+0738 for RV measurement. The panels along the upper left to lower right diagonal show the posterior distributions for our four fitting parameters: the barycentric RV of the star (RV⊕ in km  s−1), the strength of the telluric absorption (α), the instrumental Gaussian broadening profile width (σ broad in km  s−1), and the wavelength offset from the nominal SpeXtool solution (Δλ in Å). The six lower left panels illustrate correlations between parameters; only the RV and Δλ parameters show a modest inverse correlation, effectively expanding the uncertainty on the RV measurement. The upper right panel shows the NIRES spectrum of CWISE J0506+0738 prior to telluric correction (black line) and the best-fit model spectrum (magenta line) composed of stellar model and telluric absorption components (offset lines above fit). Residuals (data minus model; blue line) are consistent with measurement uncertainties (gray band).
Paper: Redder than Red: Discovery of an Exceptionally Red L/T Transition Dwarf
Authors: Adam C. Schneider, Adam J. Burgasser, Justice Bruursema, Jeffrey A. Munn, Frederick J. Vrba, Dan Caselden, Martin Kabatnik, Austin Rothermich, Arttu Sainio, Thomas P. Bickle, Scott E. Dahm, Aaron M. Meisner, J. Davy Kirkpatrick, Genaro Suárez, Jonathan Gagné, Jacqueline K. Faherty, Johanna M. Vos, Marc J. Kuchner, Stephen J. Williams, Daniella Bardalez Gagliuffi, Christian Aganze, Chih-Chun Hsu, Christopher Theissen, Michael C. Cushing, Federico Marocco, Sarah Casewell
Figure caption: Images of CWISE J0506+0738 from 2MASS (upper left and center), UHS (bottom left and center), Pan-STARRS (upper right; three-color image with g/i/y bands), and AllWISE (WISE Team 2020d) (lower right; three-color image with W1/W2/W3 bands). The position of CWISE J0506+0738 as determined in the UHS K-band images is denoted by a red circle. Note that CWISE J0506+0738 is undetected at 2MASS J and in the Pan-STARRS three-color image but clearly detected in the 2MASS K-band, UHS, and WISE images. The greenish hue of CWISE J0506+0738 in the WISE images shows that this object is significantly brighter at WISE channel W2 (4.6 μm) than at WISE channel W1 (3.4 μm) or W3 (12 μm), typical of brown dwarfs with late-L or later spectral types.
Paper: Redder than Red: Discovery of an Exceptionally Red L/T Transition Dwarf
Authors: Adam C. Schneider, Adam J. Burgasser, Justice Bruursema, Jeffrey A. Munn, Frederick J. Vrba, Dan Caselden, Martin Kabatnik, Austin Rothermich, Arttu Sainio, Thomas P. Bickle, Scott E. Dahm, Aaron M. Meisner, J. Davy Kirkpatrick, Genaro Suárez, Jonathan Gagné, Jacqueline K. Faherty, Johanna M. Vos, Marc J. Kuchner, Stephen J. Williams, Daniella Bardalez Gagliuffi, Christian Aganze, Chih-Chun Hsu, Christopher Theissen, Michael C. Cushing, Federico Marocco, Sarah Casewell
Figure caption: Color–color diagrams showing known brown dwarfs recovered in the UHS (A. Schneider et al. 2023, in preparation), supplemented with known red L dwarfs from Table 2. CWISE J0506+0738 is a clear outlier, being significantly redder than other known L dwarfs both in J − K and J − W2 colors.
Paper: Redder than Red: Discovery of an Exceptionally Red L/T Transition Dwarf
Authors: Adam C. Schneider, Adam J. Burgasser, Justice Bruursema, Jeffrey A. Munn, Frederick J. Vrba, Dan Caselden, Martin Kabatnik, Austin Rothermich, Arttu Sainio, Thomas P. Bickle, Scott E. Dahm, Aaron M. Meisner, J. Davy Kirkpatrick, Genaro Suárez, Jonathan Gagné, Jacqueline K. Faherty, Johanna M. Vos, Marc J. Kuchner, Stephen J. Williams, Daniella Bardalez Gagliuffi, Christian Aganze, Chih-Chun Hsu, Christopher Theissen, Michael C. Cushing, Federico Marocco, Sarah Casewell
Figure caption: The Keck/NIRES spectrum of CWISE J0506+0738, shown in the original resolution (gray lines) and smoothed to a resolution of λ/Δλ ≈100 (black lines). CWISE J0506+0738 is compared to the L7 spectral standard 2MASSI J0825196+211552 (Kirkpatrick et al. 2000; Cruz et al. 2018) in the upper panel and to the young L7 VL-G dwarf PSO J318.5338−22.8603 (Liu et al. 2013a) in the lower panel. Both comparisons highlight the extremely red nature of CWISE J0506+0738. All spectra are normalized between 1.27 and 1.29 μm, and prominent absorption features have been labeled.(The data used to create this figure are available.)
Paper: Redder than Red: Discovery of an Exceptionally Red L/T Transition Dwarf
Authors: Adam C. Schneider, Adam J. Burgasser, Justice Bruursema, Jeffrey A. Munn, Frederick J. Vrba, Dan Caselden, Martin Kabatnik, Austin Rothermich, Arttu Sainio, Thomas P. Bickle, Scott E. Dahm, Aaron M. Meisner, J. Davy Kirkpatrick, Genaro Suárez, Jonathan Gagné, Jacqueline K. Faherty, Johanna M. Vos, Marc J. Kuchner, Stephen J. Williams, Daniella Bardalez Gagliuffi, Christian Aganze, Chih-Chun Hsu, Christopher Theissen, Michael C. Cushing, Federico Marocco, Sarah Casewell
Figure caption:  H-band slope index vs. spectral type for field late-L and T dwarfs (colored circles) based on data from the SPLAT archive (Burgasser 2017), with colors corresponding to spectral type. Young L and T dwarfs are represented by purple squares. CWISE J0506+0738 (blue diamond) is an outlier among field-age late-Ls, similar to the young, late-type L dwarf population. Small offsets have been added to spectral type values for differentiation purposes.
Paper: Redder than Red: Discovery of an Exceptionally Red L/T Transition Dwarf
Authors: Adam C. Schneider, Adam J. Burgasser, Justice Bruursema, Jeffrey A. Munn, Frederick J. Vrba, Dan Caselden, Martin Kabatnik, Austin Rothermich, Arttu Sainio, Thomas P. Bickle, Scott E. Dahm, Aaron M. Meisner, J. Davy Kirkpatrick, Genaro Suárez, Jonathan Gagné, Jacqueline K. Faherty, Johanna M. Vos, Marc J. Kuchner, Stephen J. Williams, Daniella Bardalez Gagliuffi, Christian Aganze, Chih-Chun Hsu, Christopher Theissen, Michael C. Cushing, Federico Marocco, Sarah Casewell
Figure caption: Standard deviation (σ) vs. average magnitude over all single-exposure WISE/NEOWISE W1 (left panel) and W2 (right panel) detections of known brown dwarfs. Color contours indicate 16%–84% and 5%–95% confidence intervals in 0.5 mag bins. The insets in each panel show the difference between measured σ values and polynomial fits to the magnitude trend. 2MASS J2139+0220 (dark green square), PSO J318.5338−22.8603 (light green circle), 2MASSW J0310599+164816 (light purple hexagon), CWISE J0506+0738 (cyan diamond), and WISE J052857.68+090104.4 (dark purple pentagon) are all highlighted as clear deviants from these trends.
Paper: Redder than Red: Discovery of an Exceptionally Red L/T Transition Dwarf
Authors: Adam C. Schneider, Adam J. Burgasser, Justice Bruursema, Jeffrey A. Munn, Frederick J. Vrba, Dan Caselden, Martin Kabatnik, Austin Rothermich, Arttu Sainio, Thomas P. Bickle, Scott E. Dahm, Aaron M. Meisner, J. Davy Kirkpatrick, Genaro Suárez, Jonathan Gagné, Jacqueline K. Faherty, Johanna M. Vos, Marc J. Kuchner, Stephen J. Williams, Daniella Bardalez Gagliuffi, Christian Aganze, Chih-Chun Hsu, Christopher Theissen, Michael C. Cushing, Federico Marocco, Sarah Casewell
Figure caption: Model spectra from Marley et al. (2021) with varying effective temperatures and surface gravity fixed at log(g) = 3.5. The gray bands highlight the approximate regions of the absorption features seen in the spectrum of CWISE J0506+0738.
Paper: Redder than Red: Discovery of an Exceptionally Red L/T Transition Dwarf
Authors: Adam C. Schneider, Adam J. Burgasser, Justice Bruursema, Jeffrey A. Munn, Frederick J. Vrba, Dan Caselden, Martin Kabatnik, Austin Rothermich, Arttu Sainio, Thomas P. Bickle, Scott E. Dahm, Aaron M. Meisner, J. Davy Kirkpatrick, Genaro Suárez, Jonathan Gagné, Jacqueline K. Faherty, Johanna M. Vos, Marc J. Kuchner, Stephen J. Williams, Daniella Bardalez Gagliuffi, Christian Aganze, Chih-Chun Hsu, Christopher Theissen, Michael C. Cushing, Federico Marocco, Sarah Casewell
Figure caption: A comparison of photometric and parallactic distances for free-floating objects from Table 2 with measured parallaxes. Objects are labeled on the x-axis. Dashed lines show average differences between photometric and parallactic distances for each band, with colors corresponding to those given in the legend.
Paper: Photochemical Hazes Can Trace the C/O Ratio in Exoplanet Atmospheres
Authors: Lía Corrales, Lisseth Gavilan, D. J. Teal, Eliza M.-R. Kempton
Figure caption: The transmission spectrum of GJ 1214 b, with light gray squares (Bean et al. 2010, 2011; Désert et al. 2011) and dark gray circles (Fraine et al. 2013; Kreidberg et al. 2014), overlaid with the three ExoTransmit models utilizing the new optical constants derived from the laboratory measurements of G18. Each ExoTransmit model has been renormalized to match the mean 1–2 μm transit depth so that the shape of the spectral features can be compared. The more precise 1–2 μm data are consistent with C/O ratios of solar and 1 assuming significant solar H/He abundances (bottom panel), but the Spitzer data points are more consistent with the Z = 1000 model.
Paper: Polar Circumtriple Planets and Disks Can Only Form Close to a Triple Star
Authors: Stephen Lepp, Rebecca G. Martin, Stephen H. Lubow
Figure caption: The minimum initial inclination (﹩{i}_{\min }﹩, magenta), maximum initial inclination (﹩{i}_{\max }﹩, blue) for librating orbits, and the stationary polar inclination (green) for varying e  A , e  AB , a  AB , or i  A  (in degrees) from our standard model. The analytic curve for the stationary state is from Equation (8), with α = 2. The key in upper left panel applies to all nine panels.