adsabs/AstroCLIMB huggingface dataset:
Paper: The Ultraviolet/Optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with Swift: Further Evidence for the Outer Component
Authors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen
Figure caption: Top left panel: The relationship between the ICCF-Cut lags and Hβ lags. Top right panel: The relationship between the Javelin lags and Hβ lags. Bottom left panel: The relationship between the ICCF-Cut lags and luminosity at 5100 Å. Bottom right panel: The relationship between the Javelin lags and luminosity at 5100 Å. In each panel, the relationships are analyzed using a log–log regression. The fitting results are shown in black solid lines. The specific formulas and scatters are displayed in the upper-left corner of each panel. The red dot on the bottom right panel represents NGC 4151, obtained from Y. Jiang et al. (2024). It was removed from the fitting due to the significant deviation.
Paper: The Ultraviolet/Optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with Swift: Further Evidence for the Outer Component
Authors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen
Figure caption: Comparison of the U- and V-band results. Top left panel: Mean SNRs. Top middle panel: Fractional variability amplitudes. Top right panel: Distributions of diffuse continuum ratios (U: orange, V: blue). Bottom left panel: Lags measured by the ICCF-Cut method. Bottom right panel: Maximum correlation coefficients measured by the ICCF-Cut method. The dashed line indicates the one-to-one relation.
Paper: The Ultraviolet/Optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with Swift: Further Evidence for the Outer Component
Authors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen
Figure caption: The same as Figure 8, but for the second part light curves of Fairall 9.
Paper: The Ultraviolet/Optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with Swift: Further Evidence for the Outer Component
Authors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen
Figure caption: Left panel: Search for quasiperiodic variability in the whole light curves of Fairall 9. The top subpanel shows the UW2 band light curve, and the left bottom subpanel shows the 2D color contour of the WWZ power spectrum for the light curve. In the right bottom subpanel, the blue line represents the time-averaged WWZ power. The orange, green, and red lines represent the 1σ, 2σ, and 3σ confidence levels, respectively. Right panel: The same as the left panel, but for the first segment light curves of Mrk 817.
Paper: The Ultraviolet/Optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with Swift: Further Evidence for the Outer Component
Authors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen
Figure caption: ICCF-Cut results derived from the V-band light curves. Each panel shows the CCF (black solid line) and the CCCD (gray shaded region) between the UVW2 band and cut light curves. The maximum of the CCF and the corresponding lag estimation are indicated in the upper-left corner of each panel.
Paper: The Ultraviolet/Optical Continuum Reverberation Mapping of Eight Active Galactic Nuclei with Swift: Further Evidence for the Outer Component
Authors: Chi-Zhuo Wang, Xue-Bing Wu, Yuanzhe Jiang, Qinchun Ma, Huapeng Gu, Yuhan Wen
Figure caption: The same as Figure 8, but for the first part detrended light curves of Fairall 9.
Paper: Why Do Solar Wind Models Get It Wrong? Understanding the Capabilities of Time-dependent Solar Wind Simulations
Authors: Evangelia Samara, Elena Provornikova, C. Nick Arge, Andrew J. McCubbin, Viacheslav G. Merkin
Figure caption: Comparison of in situ solar wind observations (black) with predictions from WSA (orange dots) and WSA-GAMERA, at STEREO-A. The red color is indicative of the SS WSA-GAMERA simulations performed with the first realization of the GONG ADAPT magnetogram on 2021 September 11. The blue color shows the TD WSA-GAMERA simulations as we update the input GONG ADAPT magnetograms daily. Left panel: SS and TD predictions with WSA-GAMERA based on the default WSA velocity formula (Equation (1)). Right panel: SS and TD predictions with WSA-GAMERA based on the optimized WSA velocity formula (Equation (2)).
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Comparison between the fiducial simulation (vfrag = 400 cm s−1, α = 10−3, Mp = 0.4 MJup ≈ 6.4 Mth) with dust coagulation and fragmentation and a simulation with fixed particle sizes and no mass exchange between the two dust fluids after 45,000 planetary orbits. Panel (a) shows the gas densities, and panels (b) and (c) depict the total dust densities and the two components, respectively. We show the mass-averaged particle sizes for the coagulation simulation (black) and the constant particle sizes from the comparison run in panel (d).
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Zoomed-in snapshot of our simulation with Mp = 0.6 MJup, α = 10−3, and vfrag = 400 cm s−1.
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Characteristic particle sizes of the TriPoD size distribution and power-law exponent of the distribution at the end of our fiducial simulation. From left to right: maximum particle size, mass-averaged particle size of the small population, mass-averaged particle size of the large population, and power-law exponent.
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Global evolution of the grain size distributions (azimuthally averaged) for our simulations with four different α parameters. Thin dashed lines indicate the boundaries of the radial damping zones. The thick dashed line indicates the location of the planet.
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Global evolution of the grain size distributions (azimuthally averaged) for our simulations with four different fragmentations. Thin dashed lines indicate the boundaries of the radial damping zones. The thick dashed line indicates the location of the planet.
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Comparison between the fiducial simulation (without dust accretion, solid lines) and a simulation with dust accretion (dashed lines).
Paper: Fragmentation-limited Dust Filtration in 2D Simulations of Planet–Disk Systems with Dust Coagulation: Parameter Study and Implications for the Inner Disk’s Dust Mass Budget and Composition
Authors: Thomas Pfeil, Philip J. Armitage, Yan-Fei Jiang, 燕飞 姜
Figure caption: Comparison between the streamlines in the circumplanetary region of our fiducial simulation and the simulation with dust accretion.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Evolution of the half-mass radius (r1/2, left panel), the size of the star-forming disk (rSFR, middle panel), and the concentration (C82, right panel) as functions of stellar mass of the target galaxy in each code. The thick black dashed line in the left panel represents the evolution of galaxies undergoing wet compaction in the VELA3 simulations (S. Lapiner et al. 2023). In both r1/2 and rSFR, ENZO, RAMSES, and GEAR exhibit a steady increase in size with stellar mass, while the other five codes show a contraction phase followed by an expansion phase. Differences in C82 between these two code groups become apparent at M⋆ ≳ 109.5 M⊙. The dashed portion in each line indicates the period that is heavily influenced by the major merger at z ∼ 4.5 (denoted by a circle marker). For more information, see Section 3.2.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Evolution of disk properties of the target galaxy in each code. The panels display the disk-to-total ratio (D/T), the half-mass radius (r1/2), the stellar surface density within a 1 kpc radius (Σ⋆,1 kpc), and the concentration (C82; see Section 2.4). The gray-shaded regions indicate mergers at z ∼ 4.5 and z ∼ 2.2, during which D/T may not be well defined. The D/T of the target galaxies exceeds 0.5 before the merger event at z ∼ 2.2, roughly coinciding with the increases in Σ⋆,1 kpc and C82, and the decrease in r1/2. For more information, see Section 3.1.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Face-on and edge-on views of stellar surface density at redshift z = 2.8. From top to bottom, each set of rows represents the total, thin disk, thick disk, and spheroid stellar component. The mass fractions of each component are shown in the upper-right corner of each panel, and the circularity threshold between the thin and thick disk, ϵthre, is displayed below the mass fraction of the thin disk component. The black dashed circles in the top panels represent 3 × r1/2. The results at z = 1 are presented in Appendix A. For more information, see Section 2.2.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Radial velocity dispersion (σr, green) and tangential velocity (Vϕ, orange) of the stellar and gas components as a function of cosmic time. The gray-shaded regions indicate mergers at z ∼ 4.5 and z ∼ 2.2. A rapid transition from Vϕ/σr < 1 to Vϕ/σr ≳ 2 is highlighted for some codes, primarily induced by the major merger at z ∼ 4.5. For more details, see Section 3.2.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Mock JWST NIRCam RGB images (R: F356W, G: F200W, B: F115W) at z = 2.8. Upper panels and lower panels represent the face-on and edge-on views, the same viewing angles with Figure 1. For more information, see Section 2.3.
Paper: The AGORA High-resolution Galaxy Simulations Comparison Project. VIII. Disk Formation and Evolution of Simulated Milky Way Mass Galaxy Progenitors at 1 < z < 5
Authors: Minyong Jung, Ji-hoon Kim, Thịnh Hũ'u Nguyễn, Ramón Rodríguez-Cardoso, Santi Roca-Fàbrega, Joel R. Primack, Kirk S. S. Barrow, Anna Genina, Pablo Granizo, Hyeonyong Kim, Kentaro Nagamine, Yuri Oku, Johnny W. Powell, Yves Revaz, Héctor Velázquez, Alessandro Lupi, Ikkoh Shimizu, Tom Abel, Oscar Agertz, Renyue Cen, Daniel Ceverino, Avishai Dekel, Chaerin Jeong, Lucio Mayer, Boon Kiat Oh, Thomas R. Quinn, Hyunmi Song
Figure caption: Same as Figure 2 but with different broadband filters (R: F200W, G: F115W, B: F070W) at z = 1. Note that six out of eight codes seen in Figure 2 reach redshift z = 1, while RAMSES and GIZMO end their simulations at z = 2 (see Sections 2.1 and 2.3).
Paper: Constraints on the Progenitor and Explosion of SN 2024ggi in Harmony with Preexplosion Detection and Hydrodynamic Simulations
Authors: Amar Aryan, Erin Higgins, Matt Nicholl, Ting-Wan Chen, Yu-Hsuan Liu
Figure caption: Effect of varying explosion energy and nickel mass on the 11 M⊙ model with accelerated-wind CSM (for comparison, the steady-wind CSM model is also shown). The variations help us to constrain the range of plausible explosion energy and the amount of nickel mass.
Paper: Constraints on the Progenitor and Explosion of SN 2024ggi in Harmony with Preexplosion Detection and Hydrodynamic Simulations
Authors: Amar Aryan, Erin Higgins, Matt Nicholl, Ting-Wan Chen, Yu-Hsuan Liu
Figure caption: Left: the density distribution as a function of radius for the two different CSM models assumed in the study. Right: corresponding wind velocity distribution.
Paper: The End of the Road for Far-infrared Reddening Maps? Evidence for Reddening Errors Driven by Changes in Polycyclic Aromatic Hydrocarbon Abundance
Authors: Dennis Lee, Brandon S. Hensley, Tzu-Ching Chang, Olivier Doré
Figure caption: The ratio of 3.3 μm emission to emission at WISE W3, ﹩{I}_{\nu }^{3.3}/{I}_{\nu }^{{\rm{W3}}}﹩, as a function of the increase in PAH mass. The solid line indicates the accretion growth model shown in Figure 4. The dashed line indicates a model of PAH growth where small PAH grains are not lost. The gray band indicates the RV range where the Ursa Major region sees increased PAH grain growth. Depending on the behavior of the PAH dust grain distribution as the total PAH mass increases, the predicted ﹩{I}_{\nu }^{3.3}﹩ may track ﹩{I}_{\nu }^{{\rm{W3}}}﹩ closely or diverge due to the changes in grain size distribution. SPHEREx will be able to distinguish between these two possible models of PAH abundance variations.
Paper: The End of the Road for Far-infrared Reddening Maps? Evidence for Reddening Errors Driven by Changes in Polycyclic Aromatic Hydrocarbon Abundance
Authors: Dennis Lee, Brandon S. Hensley, Tzu-Ching Chang, Olivier Doré
Figure caption: Top: galaxy density per deg2 of the DESI ELG_LOP galaxy sample selected using the extinction map constructed from both mid-infrared and far-infrared emission using the model from Section 6. Compared with Figure 2, the analysis for this reddening map qualitatively exhibits less spatial variation associated with Ursa Major cloud as well as the lowest value for the galaxy density MAD (28 galaxies per deg2). Bottom: median-subtracted ELG_LOP galaxy sample density vs. qPAH for the model reddening map. The Pearson correlation coefficient r is also shown. Compared with Figure 3, this reddening map exhibits the weakest correlation of spatial variations with PAH abundance.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: Region files (purple) with the three fields observed (red squares) with MOSFIRE, showing the positions of the objects plotted over the ONC HST/WFC3 image from M. Robberto et al. (2020). The objects in black indicate our science targets, and the objects in red are stars used for aligning the MOSFIRE masks.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: Region file for the first field observed, on 2021 October 27, in the ONC. The objects in black indicate our science targets, and the objects in red are stars used for aligning the MOSFIRE mask.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: Region file for the second field observed, on 2021 October 28, in the ONC. The objects in black indicate our science targets, and the objects in red are stars used for aligning the MOSFIRE mask.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: Region file for the thrid field, observed on 2021 November 12, in the ONC. The objects in black indicate our science targets, and the objects in red are stars used for aligning the MOSFIRE mask.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: J-band spectra of the high-mass brown dwarfs with masses between 41 and 76 MJup. See the main text for discussion of the significance of the identified lines.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: Pseudo-equivalent-widths (left) and spectral indices (right) calculated for our targets (red stars), following the methodology presented in K. N. Allers & M. C. Liu (2013). We include the same indices calculated for brown dwarfs and low-mass stars that are members of YMGs, γ-dwarfs and β-dwarfs (K. N. Allers et al. 2007; M. Bonnefoy et al. 2014), young companions (K. N. Allers et al. 2007), α Persei (90 Myr), Upper Scorpius (5–10 Myr), Taurus (2 Myr), and ρ Ophiuchus (0.3 Myr) from E. C. Martín et al. (2017) and for field brown dwarfs from I. S. McLean et al. (2003) and M. C. Cushing et al. (2005).
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: H-band spectra of the intermediate-mass brown dwarfs with masses between 14 and 40 MJup.See the main text for discussion of the significance of the identified lines.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: H-band spectra of the planetary mass brown dwarfs with masses between 7 and 13 MJup. See the main text for discussion of the significance of the identified lines.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: H-band spectra of the high-mass brown dwarfs with masses between 41 and 76 MJup. See the main text for discussion of the significance of the identified lines.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: J-band spectra of the intermediate-mass brown dwarfs with masses between 14 and 40 MJup. See the main text for discussion of the significance of the identified lines.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: J-band spectra of the planetary mass brown dwarfs with masses between 7 and 13 MJup. See the main text for discussion of the significance of the identified lines.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: K-band spectra of the intermediate-mass brown dwarfs with masses between 14 and 40 MJup. See the main text for discussion of the significance of the identified lines.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: K-band spectra of the planetary mass brown dwarfs with masses between 7 and 13 MJup. See the main text for discussion of the significance of the identified lines.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: K-band spectra of the high-mass brown dwarfs with masses between 41 and 76 MJup. See the main text for discussion of the significance of the identified lines.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: J-band spectra of the L3–T8 planetary mass objects with masses between 7 and 10 MJup. In red is the spectrum of target 473 of our sample (1–3 Myr old). In orange is the JWST/NIRSpec spectrum of the L6 spectral type planet, 2M1207b (∼10 Myr old). In purple, we show the VLT/X-shooter spectrum of the L8 free-floating brown dwarf PSO 318–22 (∼23 Myr). In blue, we show the VLT/X-shooter spectrum of GU Psc b (T3.0, ∼100 Myr), and in dark blue, we show the JWST/NIRSpec spectrum of Ross 458 c (T8.0, ∼200 Myr).