adsabs/AstroCLIMB huggingface dataset:
Paper: The CHILES Continuum and Polarization Survey. II. Radio Continuum Source Catalog and Radio Properties
Authors: Hansung B. Gim, Min S. Yun, Nicholas M. Luber, Emmanuel Momjian, D. J. Pisano, Kelley M. Hess, Julia Blue Bird, Lucas Hunt
Figure caption: The radio spectral index distribution of the CHILES Con Pol radio continuum sources. The peak of the histogram is placed on α = −0.725, implying that the majority of microjansky radio sources are dominated by star formation. Panels (B)–(G) display histograms of the spectral index for different S/N cuts, e.g., 7, 10, 15, 20, 25, and 30.
Paper: The CHILES Continuum and Polarization Survey. II. Radio Continuum Source Catalog and Radio Properties
Authors: Hansung B. Gim, Min S. Yun, Nicholas M. Luber, Emmanuel Momjian, D. J. Pisano, Kelley M. Hess, Julia Blue Bird, Lucas Hunt
Figure caption: The histogram of redshifts is presented with a bin size of 0.1, where zspec is shown with the blue line and zphot is shown with the green filled histogram. The majority (51.0%) are located within z < 1.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Results of our most preferred retrieval setup, QEQ-1 (see Tables 3–4 and discussions in Section 7.1), which has the lowest BIC value. The top panel compares the observed JWST/NIRSpec spectrum of 2MASS 1207 b (black circles) with the best-fit spectrum from QEQ-1 (orange). The emergent spectra from each atmospheric column are plotted in purple and green, with fluxes scaled by their corresponding coverage fractions. The blue error bars (σ) represent the total error budget, where ﹩\sigma =\sqrt{{\sigma }_{{\rm{obs}}}^{2}+{b}_{{\rm{chunk}}}^{2}}﹩, with σobs as the observed flux uncertainty and bchunk as the fitted hyperparameter (explained in Section 5.5). The second panel from the top shows the residual spectrum between the observed and best-fit spectra, scaled by σ. The middle-left panel presents the confidence intervals for the retrieved T–P profiles. The remaining panels present the posteriors of key parameters, with median values and confidence intervals summarized in Table 3.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Top panel: the left panel shows T–P profiles from the Sonroa Diamondback models with varying effective temperatures: Teff = 1700 K (red), 1500 K (orange), 1300 K (blue), and 1100 K (purple). All models have ﹩\mathrm{log}(g)=4.5﹩ dex, [M/H] = 0 dex, and fsed = 2. The 3–4 μm photosphere of each model is highlighted with a thick line. The CO−CH4 transition curve (see Figure 10) is shown as a dashed line. The right panel presents the corresponding spectra, with CH4 absorption features (R, Q, and P branches) labeled. Bottom panel: these two panels follow the same format as the top panels but present the T–P profiles and spectra for models with different [M/H] values: + 0.5 dex (red), 0 dex (orange), and −0.5 dex (blue). All models have Teff = 1400 K, ﹩\mathrm{log}(g)=4.5﹩ dex, and fsed = 2.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Top-left panel: retrieved T–P profiles from the QEQ-1 setup, with 1σ/2σ/3σ confidence intervals shown in orange. The solid black line represents the best-fit T–P profile. Condensation curves of Mg2SiO4 and Fe, calculated using the maximum-likelihood [M/H] and C/O values, are shown by dashed and dotted lines, respectively. The best-fit cloud mass fraction profiles for the first column (thin-cloud patches covering about 9% of 2MASS 1207 b’s atmosphere) are plotted in purple, with values indicated on the upper x-axis. Top-right panel: maximum-likelihood contribution function of the thin-cloud patches. Bottom panel: these two panels show the best-fit cloud content and contribution function for the second column (thick-cloud regions covering about 91% of the atmosphere), following the same format as the top two panels.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Retrieved T–P profiles from the QEQ-1 setup, with 1σ, 2σ, and 3σ confidence intervals shown in orange. The best-fit T–P profile is indicated by the solid black line, with the 3–4 μm photosphere of thin-cloud patches highlighted by a thicker line. The CO−CH4 transition curve for solar metallicity, from J. J. Fortney et al. (2020), is overlaid as a dashed blue line; along this line, the CO and CH4 have equal volume mixing ratios. A thermal structure with hotter temperatures and/or lower pressures than this transition curve would have a decreased CH4 abundance, while a cooler and/or higher-pressure thermal structure would have a decreased CO abundance.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: The atmospheric metallicity (top), carbon-to-oxygen ratio (middle), and ξthin (bottom) inferred from all QEQ retrieval setups. The parameter ξthin is only defined in inhomogeneous atmospheric models. For schemes with patchy clouds or a combination of patchy clouds and hot spots, ξthin represents the fraction of thin-cloud patches; for the hot-spot scheme, it describes the fraction of the column with a hotter thermal structure (i.e., hot spots; Section 5.4). Retrievals with evolution-based priors for surface gravity, radius, and mass are shown in orange, while those with broad parameter priors are shown in blue.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: The top two panels present T–P profiles and corresponding spectra from the Sonroa Diamondback models with varying fsed values of 1 (red), 2 (orange), 3 (blue), and 8 (purple). All models have Teff = 1400 K, ﹩\mathrm{log}(g)=4.5﹩ dex, and [M/H] = 0 dex. The bottom two panels show models with varying ﹩\mathrm{log}(g)﹩ of 3.5 dex (red), 4.0 dex (orange), 4.5 dex (blue), and 5.5 dex, all with Teff = 1200 K, [M/H] = 0 dex, and fsed = 1. These panels follow the same format as Figure 11.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: The top three spectra show the observed JWST/NIRSpec data of 2MASS 1207 b (black), as well as the best-fit retrieval model spectra emerging from the thick-cloud regions (green) and thin-cloud patches (purple) based on the QEQ-1 setup. The JWST/NIRSpec spectrum of VHS 1256 b (B. E. Miles et al. 2023) is shown at the bottom. All spectra are plotted at a spectral resolution of R = 1000. Key molecular absorption features are labeled.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: The variability amplitude as a function of wavelength predicted by our preferred retrieval setup, QEQ-1. The solid red line represents the variability amplitude when the fraction of thin-cloud patches changes by Δξcol1 = 0.16% (solid red line) from the maximum-likelihood value. The red-shaded region indicates the range of variability amplitudes when Δξcol1 = 0.11%–0.21%. Black and gray circles with error bars represent the measured variability amplitudes from Y. Zhou et al. (2016), with gray circles corresponding to measurements from Y. Zhou et al. (2019), which are affected by systematics.
Paper: ELemental Abundances of Planets and Brown Dwarfs Imaged around Stars (ELPIS). II. The Jupiter-like Inhomogeneous Atmosphere of the First Directly Imaged Planetary-mass Companion 2MASS 1207 b
Authors: Zhoujian Zhang, 周健 张, Paul Mollière, Jonathan J. Fortney, Mark S. Marley
Figure caption: Corner plot for the inferred parameters of 2MASS 1207 b based on the most preferred retrieval setup, QEQ-1. The 1σ and 2σ confidence intervals are highlighted for each parameter.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: Radius vs. mass for all transiting companions from 7 to 150  MJ. The black dashed lines depict the canonical 13 and 80 MJ BD boundaries. The solid purple line at 42 MJ shows the proposed B. Ma & J. Ge (2014) boundary between planet- and star-like BDs. Note, systems where the primary object is a white dwarf or brown dwarf are not shown. References: B. A. Henderson et al. (2024b) and references therein as well as G. Á. Bakos et al. (2010), L. A. Buchhave et al. (2011), B. Tingley et al. (2011), H. Parviainen et al. (2014), A. S. Bonomo et al. (2015), L. J. Esteves et al. (2015), K. G. Stassun et al. (2017), J. Bento et al. (2018), C. I. Cañas et al. (2018), B. F. Cooke et al. (2020), P. Cortés-Zuleta et al. (2020), K. El-Badry et al. (2023), M. Lambert et al. (2023), S. P. Schmidt et al. (2023), P. A. Dalba et al. (2024), Y. T. Davis et al. (2024), J. Eberhardt et al. (2023), B. A. Henderson et al. (2024a), M. I. Swayne et al. (2024), and J.-Q. Wang et al. (2024).
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: Left: eccentricity vs. mass for transiting BDs with a dotted line at the proposed B. Ma & J. Ge (2014) boundary between planet- and star-like BDs. Right: all transiting companions ranging from 7 to 150 MJ in eccentricity vs. mass ratio with a dashed line at the same 42 MJ location assuming a 1.0 M⊙ host star. As discussed in Section 4.1, the eccentricity dichotomy between low- and high-mass BDs does not hold up when plotted against mass ratio, suggesting that this feature may not represent the boundary between planet-like and star-like BDs.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: The solid-lined histogram depicts the metallicity distribution of transiting companions ranging from 7 to 42 MJ, while the dotted-lined histogram depicts the metallicity distribution of transiting companions from 42 to 150 MJ. Both histograms are normalized such that their areas are equal to 1. There appears to be a slight trend toward higher metallicities for host stars with lower-mass companions. Note, the metallicities shown here are the values cited by their original discovery papers, and hence represent a heterogeneous sample with a variety of different measurement techniques.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: Same as Figure 4 except for TOI-5882.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: Same as Figure 2 except for TOI-5467.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: Same as Figure 2 except for TOI-5240.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: Same as Figure 4 except for TOI-4759.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: Same as Figure 2 except for TOI-4737.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: Same as Figure 2 except for TOI-4635.
Paper: Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS
Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn
Figure caption: The coadded spectra of TOI-5882 zoomed in to the Li absorption line at 6708 Å. The measurement region used to determine the equivalent width is shaded in purple, with the dashed line at the center indicating the rest wavelength of the Li doublet, 6707.844 Å.
Paper: Multiparameter Constraints on Empirical Infrasound Period-Yield Relations for Bolides and Implications for Planetary Defense
Authors: Elizabeth A. Silber, Josep M. Trigo-Rodríguez, Iyare Oseghae, Eloy Peña-Asensio, Mark Boslough, Rodney Whitaker, Christoph Pilger, Philip Lubin, Vedant Sawal, Claus Hetzer, Randy Longenbaugh, Peter Jenniskens, Brin Bailey, Esther Mas Sanz, Patrick Hupe, Alexander N. Cohen, Thom R. Edwards, Sasha Egan, Reynold E. Silber, Summer C. Czarnowski, Miro Ronac Giannone
Figure caption: Idealized diagram, not drawn to scale and intended only as a rough conceptual representation, illustrates how a bolide’s fragmentation behavior affects the resulting light curve. The left column shows four conceptual light curves, from a single-peaked airburst to continuous multipoint fragmentation, while the right panels depict how different geometry scenarios might look for steep vs. shallow entries.
Paper: Multiparameter Constraints on Empirical Infrasound Period-Yield Relations for Bolides and Implications for Planetary Defense
Authors: Elizabeth A. Silber, Josep M. Trigo-Rodríguez, Iyare Oseghae, Eloy Peña-Asensio, Mark Boslough, Rodney Whitaker, Christoph Pilger, Philip Lubin, Vedant Sawal, Claus Hetzer, Randy Longenbaugh, Peter Jenniskens, Brin Bailey, Esther Mas Sanz, Patrick Hupe, Alexander N. Cohen, Thom R. Edwards, Sasha Egan, Reynold E. Silber, Summer C. Czarnowski, Miro Ronac Giannone
Figure caption: Representative examples of different classes of light curves, plotted as a function of the USG-provided time (left) and calculated altitude assuming no deceleration (right). Panels (a) and (b) show LC class 1, depicting a single dominant fragmentation event, where a single abrupt peak unfolds within 2 s and spans only about 4 km in altitude (37–33 km). This single fragmentation event is consistent with a classic “airburst” in which the entire object is abruptly vaporized due to the fragmentation. Panels (c) and (d) show LC class 2. This is a multifragmentation event, with multiple bursts across 4 s and an altitude range from 48 km down to 35 km, indicative of energy deposition over 13 km.
Paper: Multiparameter Constraints on Empirical Infrasound Period-Yield Relations for Bolides and Implications for Planetary Defense
Authors: Elizabeth A. Silber, Josep M. Trigo-Rodríguez, Iyare Oseghae, Eloy Peña-Asensio, Mark Boslough, Rodney Whitaker, Christoph Pilger, Philip Lubin, Vedant Sawal, Claus Hetzer, Randy Longenbaugh, Peter Jenniskens, Brin Bailey, Esther Mas Sanz, Patrick Hupe, Alexander N. Cohen, Thom R. Edwards, Sasha Egan, Reynold E. Silber, Summer C. Czarnowski, Miro Ronac Giannone
Figure caption: Log–log plot of energy vs. signal period comparing published period–energy relations. Each line represents a different empirical fit: D. O. Revelle (1997), R. Whitaker & J. Mutschlecner (2006), R. W. Whitaker (2023), and bolide-based relations from T. A. Ens et al. (2012) and N. Gi & P. Brown (2017), the latter two of which include both single-station and multistation (averaged) data. T. A. Ens et al. (2012) and N. Gi & P. Brown (2017) calibrated the bolide energy relations against the USG sensor data, while the other relations stem from calibration against nuclear-explosion data.