adsabs/AstroCLIMB huggingface dataset:
Paper: The XRISM/Resolve View of the Fe K Region of Cyg X-3
Authors: Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, María Díaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Ryota Tomaru, Tasuku Hayashi, Tomohiro Hakamata, Daiki Miura, Karri Koljonen, Mike McCollough
Figure caption: The 2–10 keV XRISM/Resolve spectrum of Cyg X-3, modeled with an absorbed disk blackbody and several Gaussian emission and absorption lines. Black labels are lines that are included in the model and listed in Table 1.
Paper: The XRISM/Resolve View of the Fe K Region of Cyg X-3
Authors: Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, María Díaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Ryota Tomaru, Tasuku Hayashi, Tomohiro Hakamata, Daiki Miura, Karri Koljonen, Mike McCollough
Figure caption: Top: orbital-phase-resolved XRISM/Resolve spectra of Cyg X-3. The gray line shows the respective best-fit model that has the same components as the phase-averaged model described in Section 3.2. Bottom: χ residuals of the individual phase-resolved spectra.
Paper: Be Careful in Multimessenger Inference of the Hubble Constant: A Path Forward for Robust Inference
Authors: Michael Müller, Suvodip Mukherjee, Geoffrey Ryan
Figure caption: This figure shows the median and standard deviation (with error bars) for the (marginal) H 0 posteriors, considering all available ﹩{\theta }_{{\rm{m}}}^{(\mathrm{true})}\ne 0﹩ data sets at ﹩{\theta }_{\mathrm{vi}}^{(\mathrm{true})}=30^\circ ﹩. The leftmost set shows the behavior for standard inference with H 0 and assuming ﹩{\theta }_{{\rm{m}}}^{(\mathrm{true})}=0﹩ and complements Figures 3 and 4. The set in the middle refers to the co-inference of (θ m, H 0), as discussed in Section 3.3, with a ﹩{ \mathcal U }\left(-60^\circ ,60^\circ \right)﹩ prior for θ m (complementing Figures 5 and B1). The set on the right also considers the co-inference of (θ m, H 0) but with a narrower prior of ﹩{ \mathcal U }\left(-10^\circ ,10^\circ \right)﹩ for θ m, which complements Figure B4.
Paper: Be Careful in Multimessenger Inference of the Hubble Constant: A Path Forward for Robust Inference
Authors: Michael Müller, Suvodip Mukherjee, Geoffrey Ryan
Figure caption: 2D posteriors for the (θ m, H 0) inference of the ﹩{\theta }_{\mathrm{vi}}^{(\mathrm{true})}=30^\circ ﹩ event, with ﹩{\theta }_{{\rm{m}}}^{(\mathrm{true})}\in \{-15.^\circ 7﹩, −10°, −4.°2, 0°, 4.°4, 15.°7} from left to right. The heat map represents the GW+GJ+z posterior, while the magenta and red contours indicate the 1σ (dashed) and 2σ (solid) highest posterior density regions for the GW+GJ+z and GW+GJc+z posteriors, respectively. The truths are marked with white stars. We also indicate the 1σ (dashed) and 2σ (solid) regions of the GW+z posteriors with cyan lines.
Paper: Be Careful in Multimessenger Inference of the Hubble Constant: A Path Forward for Robust Inference
Authors: Michael Müller, Suvodip Mukherjee, Geoffrey Ryan
Figure caption: 95% highest posterior density credible regions (2σ) for the Hubble posteriors of all four GW+EM inference scenarios (different scenarios are indicated by red/magenta colored regions for the GJ(c) model and blue/cyan for the PLJ(c) model), with ﹩{\theta }_{\mathrm{vi}}^{(\mathrm{true})}=20^\circ ,30^\circ ,40^\circ ﹩ and ﹩{\theta }_{\mathrm{JN}}^{(\mathrm{true})}={\theta }_{\mathrm{vi}}^{(\mathrm{true})}+{\theta }_{{\rm{m}}}﹩ and θ m varying systematically. The truth is indicated with a dashed line. (Data tabulated in Tables B3 and B4.)
Paper: Be Careful in Multimessenger Inference of the Hubble Constant: A Path Forward for Robust Inference
Authors: Michael Müller, Suvodip Mukherjee, Geoffrey Ryan
Figure caption: Progression of joint GW+GJ(c)+z Hubble posteriors for ﹩{\theta }_{\mathrm{JN}}^{({\rm{true}})}={\theta }_{\mathrm{vi}}^{({\rm{true}})}+{\theta }_{{\rm{m}}}﹩, with θ m varying systematically from −16° to 14°. We show the posteriors for ﹩{\theta }_{\mathrm{vi}}^{({\rm{true}})}=30^\circ ﹩ (white contours) and ﹩{\theta }_{\mathrm{vi}}^{({\rm{true}})}=40^\circ ﹩ (magenta contours). The posteriors on the left and right represent the results from the inference with the GJ and GJc scenario, respectively.
Paper: Be Careful in Multimessenger Inference of the Hubble Constant: A Path Forward for Robust Inference
Authors: Michael Müller, Suvodip Mukherjee, Geoffrey Ryan
Figure caption: Sketch for the definition of the system inclination θ JN during the inspiral/merger on the left and for the definition of the jet viewing angle θ vi and misalignment angle θ m for the postmerger remnant. The line of sight for the observer is indicated with the vector ﹩\hat{n}﹩.
Paper: Be Careful in Multimessenger Inference of the Hubble Constant: A Path Forward for Robust Inference
Authors: Michael Müller, Suvodip Mukherjee, Geoffrey Ryan
Figure caption: This figure shows the marginal posterior probability density functions (PDFs) for H 0 from the ﹩{\theta }_{{\rm{m}}}^{(\mathrm{true})}\ne 0﹩ data sets at ﹩{\theta }_{\mathrm{vi}}^{(\mathrm{true})}=30^\circ ﹩ in the case of the co-inference of (θ m, H 0), as discussed in Section 3.3. We present the same angles as in Figure 5, and the median and 2.5th–97.5th percentiles of the marginal posterior are shown with a dashed line and colored regions (using the same color as for the PDF), respectively.
Paper: Be Careful in Multimessenger Inference of the Hubble Constant: A Path Forward for Robust Inference
Authors: Michael Müller, Suvodip Mukherjee, Geoffrey Ryan
Figure caption: The GW (heat map and black contours) and EM (red contours) posteriors in the d  L –θ vi plane for injected/true parameters θ JN = 30° and d  L  = 21.56 Mpc (marked in white). The dashed and solid contours indicate the 1σ and 2σ highest posterior density credible regions. The yellow and magenta contours show two EM posteriors with a positive or negative angular shift of 5.°7 between the jet angle and system inclination (the injected/true θ vi is indicated with stars).
Paper: Be Careful in Multimessenger Inference of the Hubble Constant: A Path Forward for Robust Inference
Authors: Michael Müller, Suvodip Mukherjee, Geoffrey Ryan
Figure caption: This figure shows the median and standard deviation (with error bars) for the (marginal) H 0 posteriors, considering all available ﹩{\theta }_{{\rm{m}}}^{(\mathrm{true})}=﹩ data sets. The left column shows the behavior for standard inference with H 0, which assumes ﹩{\theta }_{{\rm{m}}}^{(\mathrm{true})}=0﹩. The right column refers to the co-inference of (θ m, H 0), as discussed in Section 3.3, with a ﹩{ \mathcal U }\left(-60^\circ ,60^\circ \right)﹩ prior for θ m.
Paper: Be Careful in Multimessenger Inference of the Hubble Constant: A Path Forward for Robust Inference
Authors: Michael Müller, Suvodip Mukherjee, Geoffrey Ryan
Figure caption: We show the light-curve data for the used EM counterparts, generated with a GJ. The different frequency bands are color coded (red: radio; blue: optical; violet: X-ray), and measurements are plotted with an error bar, while upper limits are denoted with an upside-down triangle.
Paper: Be Careful in Multimessenger Inference of the Hubble Constant: A Path Forward for Robust Inference
Authors: Michael Müller, Suvodip Mukherjee, Geoffrey Ryan
Figure caption: This figure shows the marginal posterior PDFs for H 0 from the ﹩{\theta }_{{\rm{m}}}^{(\mathrm{true})}\ne 0﹩ data sets at ﹩{\theta }_{\mathrm{vi}}^{(\mathrm{true})}=30^\circ ﹩ in the case of the co-inference of (θ m, H 0) using the narrower prior ﹩{ \mathcal U }\left(-10^\circ ,10^\circ \right)﹩ for θ m, as discussed in Section 3.3. We present the data for ﹩{\theta }_{{\rm{m}}}^{(\mathrm{true})}\in \{-10^\circ ﹩, −6.°5, −4.°2, 0°, 4.°2, 6.°7}, and the median and 2.5th–97.5th percentiles of the marginal posterior are shown with a dashed line and colored regions (using the same color as for the PDF), respectively.
Paper: Detection of Gas Inflow during the Onset of a Starburst in a Low-mass Galaxy at z = 2.45
Authors: Erin Coleman, Keerthi Vasan G.C., Yuguang Chen, 昱光 陈, Tucker Jones, Sunny Rhoades, Richard Ellis, Dan Stark, Nicha Leethochawalit, Ryan Sanders, Kris Mortensen, Karl Glazebrook, Glenn G. Kacprzak
Figure caption: Top: rest-frame spectrum of System 10, obtained by summing the three multiple images. Solid red lines indicate strong features at the redshift of System 10, including ISM absorption, which shows signatures of gas inflow. Dashed blue lines indicate intervening absorption features at the redshift z = 2.225 of the brighter arc, arising from its circumgalactic medium. Spectral regions affected by intervening absorption are not used in this work. Bottom left: the summed spectrum zoomed in around the Lyα feature. The red side of Lyα is affected by intervening O I λ1302 and Si II λ1304 absorption from the foreground arc, such that we cannot reliably determine the Lyα emission properties. However, there is clearly a component of blueshifted Lyα emission, indicative of low H I column density or inflowing gas. Bottom center: the summed spectrum zoomed in around the Si II* λλ1264, 1533 fine structure emission lines. The Si II* λ1309 line is not used in this work because it is affected by intervening absorption. Bottom right: average velocity profile of several strong ISM absorption lines with respect to the systemic redshift of the galaxy. The red line shows a best-fit Gaussian profile. The absorption is clearly redshifted, indicating inflowing gas, while the absorption at negative (blueshifted) velocities is nearly zero. Shaded regions in all panels show the 1σ uncertainty.
Paper: Detection of Gas Inflow during the Onset of a Starburst in a Low-mass Galaxy at z = 2.45
Authors: Erin Coleman, Keerthi Vasan G.C., Yuguang Chen, 昱光 陈, Tucker Jones, Sunny Rhoades, Richard Ellis, Dan Stark, Nicha Leethochawalit, Ryan Sanders, Kris Mortensen, Karl Glazebrook, Glenn G. Kacprzak
Figure caption: Images of the CSWA 128 lens system. Both panels are oriented with north up and east to the left. Three magnified images of System 10 are marked in each panel. Left panel: optical false-color image obtained by averaging the KCWI datacube used in this work over three wavelength ranges (blue: λ = 3500–4100 Å; green: λ = 4200–4800 Å; red: λ = 4900–5500 Å). White outlines show the regions used to extract spectra for each image of System 10, and red outlines indicate the regions used to correct sky subtraction residuals around each image. Right panel: Keck NIRC2 near-IR adaptive optics image (see S. Sharma et al. 2018 for details). Images of System 10 (z = 2.45) are circled in red and images of the z = 2.225 foreground galaxy are circled in blue. The target galaxy images are spatially compact despite the lensing magnification.
Paper: Detection of Gas Inflow during the Onset of a Starburst in a Low-mass Galaxy at z = 2.45
Authors: Erin Coleman, Keerthi Vasan G.C., Yuguang Chen, 昱光 陈, Tucker Jones, Sunny Rhoades, Richard Ellis, Dan Stark, Nicha Leethochawalit, Ryan Sanders, Kris Mortensen, Karl Glazebrook, Glenn G. Kacprzak
Figure caption: Top left: stellar continuum models for a simple stellar population showing the effect of varying metallicity (Z) at fixed age. The weak P-Cygni stellar wind absorption component clearly favors a low metallicity (Z ≲ 0.001, or  ≲ 10% solar, for an age of 4 Myr). Regions of the spectrum affected by strong nonstellar features are masked in gray. Top right: similar to the center panel, showing the effect of varying the age. For a metallicity Z = 0.001, the stellar wind absorption indicates ages  ≲5 Myr. While ages  ≳15 Myr can also provide a reasonable fit to the C IV stellar wind, they cannot explain the strong nebular component which requires very massive (thus young) stars. Bottom: spectrum of System 10 in the region of C IV. Nebular emission is prominent, with interstellar absorption redshifted relative to the emission features, clearly indicative of inflows. The best-fit model of the C IV feature is shown in red. This model includes the stellar component, nebular emission, and interstellar absorption.
Paper: Detection of Gas Inflow during the Onset of a Starburst in a Low-mass Galaxy at z = 2.45
Authors: Erin Coleman, Keerthi Vasan G.C., Yuguang Chen, 昱光 陈, Tucker Jones, Sunny Rhoades, Richard Ellis, Dan Stark, Nicha Leethochawalit, Ryan Sanders, Kris Mortensen, Karl Glazebrook, Glenn G. Kacprzak
Figure caption: Comparison of the ISM absorption velocity centroid in System 10 with the sample of z ∼ 2 galaxies studied in C. C. Steidel et al. (2010) and D. K. Erb et al. (2006), shown as the blue histogram. Three LRIS-Inflow galaxies studied in A. Weldon et al. (2023) out of a parent sample of 134 are shown as the red histogram. System 10 is an outlier, with clear inflow indicated by the + 250 km s−1 velocity (black line, with gray shading showing the 1σ uncertainty). In contrast, the blue and red histograms show  <200 km s​​​​​−1 in all cases, with the vast majority having blueshifted (negative) ISM velocities corresponding to outflows. We note that System 10 has a considerably lower dynamical mass as indicated by its small velocity dispersion and radius, relative to the other samples shown here. We posit that the inflow seen in System 10 is associated with accretion-driven bursty star formation, predicted to occur only in such low-mass galaxies.
Paper: Fermi-LAT Detection of the Low-luminosity Radio Galaxy NGC 4278 during the LHAASO Campaign
Authors: Ettore Bronzini, Paola Grandi, Eleonora Torresi, Sara Buson
Figure caption: Multiwavelength and multiepoch SED of nuclear emission in NGC 4278. Archival data are shown in gray, and data are collected from S. Antón et al. (2004), M. Giroletti et al. (2005), A. Cardullo et al. (2009), G. Younes et al. (2010), S. Pellegrini et al. (2012), and J. W. Isbell et al. (2021). Swift-XRT, Fermi-LAT, and LHAASO simultaneous data are shown in blue and are from Z. Cao et al. (2024b) and this work.
Paper: Fermi-LAT Detection of the Low-luminosity Radio Galaxy NGC 4278 during the LHAASO Campaign
Authors: Ettore Bronzini, Paola Grandi, Eleonora Torresi, Sara Buson
Figure caption: TS map of NGC 4278. The position of the 4FGL-DR4 sources (J. Ballet et al. 2023) are shown as white crosses. In the zoomed-in map, the orange star marks the radio position of NGC 4278 (C. Ly et al. 2004), while the violet and white stars are the LHAASO (Z. Cao et al. 2024a, 2024b) and Fermi-LAT best-fit positions, respectively. The LHAASO and Fermi-LAT 95% localization uncertainty regions are shown as dashed circular regions using the same color code.
Paper: 131 and 304 Å Emission Variability Increases Hours Prior to Solar Flare Onset
Authors: Kara L. Kniezewski, E. I. Mason, Vadim M. Uritsky, Seth H. Garland
Figure caption: (a) Example normalized integrated emission plot for the 6 hr prior to a M2.3 flare on 2012-10-08T11:05:00 showing a general increase in all channels; of particular note is the significant spike in the 131 emission several hours before the flare onset, which is not seen in the other 3 wavelengths. (b) An analogous plot for a C-class flare, showing a general decrease in all channels. (c) An analogous plot for a different C-class flare, showing poor correlation between the channels. (d) An analogous plot for a nonflaring time period, showing significantly less variation in the emission levels during a 6 hr period.
Paper: 131 and 304 Å Emission Variability Increases Hours Prior to Solar Flare Onset
Authors: Kara L. Kniezewski, E. I. Mason, Vadim M. Uritsky, Seth H. Garland
Figure caption: (a) Cumulative hourly standard deviation ratios by GOES flare class and cumulative number of hours before flare onset. The y-axis for all three plots is 1 to 5, and the zero-point on the x-axis corresponds to the timestamp of flare onset. The maximum value is labeled with its respective value for each channel. (b) Box and whisker plot showing the distribution of normalized standard deviations, by GOES class and AIA channel. The median value for each data set is represented by a cyan line, and outliers are shown as black circles.
Paper: 131 and 304 Å Emission Variability Increases Hours Prior to Solar Flare Onset
Authors: Kara L. Kniezewski, E. I. Mason, Vadim M. Uritsky, Seth H. Garland
Figure caption: This figure graphs the percentage of flares whose integrated emission standard deviations exceed those of the nonflaring cases for the cumulative 6 hr time range studied here. The exceptionally small event pool for X-class flares causes the poor data quality in the graph on the far right and is included only for completeness.
Paper: 131 and 304 Å Emission Variability Increases Hours Prior to Solar Flare Onset
Authors: Kara L. Kniezewski, E. I. Mason, Vadim M. Uritsky, Seth H. Garland
Figure caption: SF analysis of the flaring (red) and nonflaring (blue) time series for each AIA channel (columns) and GOES flare class (rows). Note that computations were done for normalized data in each channel.
Paper: 131 and 304 Å Emission Variability Increases Hours Prior to Solar Flare Onset
Authors: Kara L. Kniezewski, E. I. Mason, Vadim M. Uritsky, Seth H. Garland
Figure caption: DFA of the flaring (red) and nonflaring (blue) time series for each AIA channel (columns) and GOES flare class (rows). Note that computations were done for normalized data in each channel.
Paper: 131 and 304 Å Emission Variability Increases Hours Prior to Solar Flare Onset
Authors: Kara L. Kniezewski, E. I. Mason, Vadim M. Uritsky, Seth H. Garland
Figure caption: Stacked histogram plots, one for each SDO AIA channel investigated. The bins cover the full available range of values in the normalized integrated emission plots, and the different shades and patterns denote C flares, M flares, X flares, and nonflaring cases.
Paper: Atmospheric Abundances and Bulk Properties of the Binary Brown Dwarf Gliese 229Bab from JWST/MIRI Spectroscopy
Authors: Jerry W. Xuan, Marshall D. Perrin, Dimitri Mawet, Heather A. Knutson, Sagnick Mukherjee, Yapeng Zhang, Kielan K. W. Hoch, Jason J. Wang, Julie Inglis, Nicole L. Wallack, Jean-Baptiste Ruffio
Figure caption: Target acquisition confirmation exposure and forward modeling. Left panel: the observed TA confirmation image, showing the LRS slit with the companion positioned for the first of two nod positions. Second panel: the best-fit PSF model for the science target. Third panel: the best-fit model for the wings of the host star PSF plus the diffuse flat sky background seen through the LRS slit. The host star Gliese 229 itself is out of view, ~4﹩\mathop{.}\limits^{{\rm{^{\prime\prime} }}}﹩5 up and to the left from B. For scale, the LRS slit itself is 4﹩\mathop{.}\limits^{{\rm{^{\prime} }}{\rm{^{\prime} }}}﹩7 in length. Fourth panel: the combined forward model summing the previous two panels. Right panel: residuals of the data minus the model. The goodness-of-fit metric χ2 is noted, evaluated over the optimization region indicated by the white contour. This is a reasonably good, though imperfect, fit to this complex scene. The geometric parameters refined in this fit were then used for modeling the LRS-dispersed version of this scene.
Paper: Atmospheric Abundances and Bulk Properties of the Binary Brown Dwarf Gliese 229Bab from JWST/MIRI Spectroscopy
Authors: Jerry W. Xuan, Marshall D. Perrin, Dimitri Mawet, Heather A. Knutson, Sagnick Mukherjee, Yapeng Zhang, Kielan K. W. Hoch, Jason J. Wang, Julie Inglis, Nicole L. Wallack, Jean-Baptiste Ruffio
Figure caption: Top panel: the best-fit combined (red dashed) and component models (light purple and teal) from the binary brown dwarf fit. The models are Gaussian-convolved using a constant spectral resolution of 200 for illustration purposes. The shaded gray area indicates the wavelength range covered by the MIRI LRS data. Bottom panel: the computed flux ratio (Bb/Ba) from the best-fit models above. In general, the flux ratio in the near-infrared is lower and shows more structure between the two components.