adsabs/AstroCLIMB huggingface dataset:
Paper: JWST-TST DREAMS: The Nightside Emission and Chemistry of WASP-17b
Authors: Jacob Lustig-Yaeger, Kristin S. Sotzen, Kevin B. Stevenson, Shang-Min Tsai, Ryan C. Challener, Jayesh Goyal, Nikole K. Lewis, Dana R. Louie, L. C. Mayorga, Daniel Valentine, Hannah R. Wakeford, Lili Alderson, Natalie H. Allen, Thomas J. Fauchez, Ana Glidden, Amélie Gressier, Sarah M. Hörst, Jingcheng Huang, Zifan Lin, Avi M. Mandell, Elijah Mullens, Sarah Peacock, Edward W. Schwieterman, Jeff A. Valenti, C. Matt Mountain, Marshall Perrin, Roeland P. van der Marel
Figure caption: The dayside and nightside abundances of H2O as a function of metallicity and C/O ratio computed from our two-column VULCAN grids, assuming Kzz = 10 cm2 s−1 and no day–night transport. The abundances are averaged between 0.1 bar and 10−4 bar, guided by the contribution function shown in Figure 4. The dashed lines and solid lines show the upper and lower bounds of the 1σ, 2σ, and 3σ uncertainty intervals, respectively. Bounds outside of the modeled abundance ranges are not shown (e.g., only the 1σ upper limit of H2O is visible for the nightside).
Paper: JWST-TST DREAMS: The Nightside Emission and Chemistry of WASP-17b
Authors: Jacob Lustig-Yaeger, Kristin S. Sotzen, Kevin B. Stevenson, Shang-Min Tsai, Ryan C. Challener, Jayesh Goyal, Nikole K. Lewis, Dana R. Louie, L. C. Mayorga, Daniel Valentine, Hannah R. Wakeford, Lili Alderson, Natalie H. Allen, Thomas J. Fauchez, Ana Glidden, Amélie Gressier, Sarah M. Hörst, Jingcheng Huang, Zifan Lin, Avi M. Mandell, Elijah Mullens, Sarah Peacock, Edward W. Schwieterman, Jeff A. Valenti, C. Matt Mountain, Marshall Perrin, Roeland P. van der Marel
Figure caption: Pressure contribution functions from the retrieved dayside (top) and nightside (bottom) emission spectra for the primary gaseous species in the retrieval models (colors). The left panels show the pressure contributions as a function of wavelength, while the right panels show the same contributions integrated over the NIRSpec G395H bandpass. The vertical error bars show the range of pressures where 95.5% (2σ) of the flux that is sensitive to each gas probes.
Paper: JWST-TST DREAMS: The Nightside Emission and Chemistry of WASP-17b
Authors: Jacob Lustig-Yaeger, Kristin S. Sotzen, Kevin B. Stevenson, Shang-Min Tsai, Ryan C. Challener, Jayesh Goyal, Nikole K. Lewis, Dana R. Louie, L. C. Mayorga, Daniel Valentine, Hannah R. Wakeford, Lili Alderson, Natalie H. Allen, Thomas J. Fauchez, Ana Glidden, Amélie Gressier, Sarah M. Hörst, Jingcheng Huang, Zifan Lin, Avi M. Mandell, Elijah Mullens, Sarah Peacock, Edward W. Schwieterman, Jeff A. Valenti, C. Matt Mountain, Marshall Perrin, Roeland P. van der Marel
Figure caption: Similar to the retrieval results shown in Figure 3 but without error inflation. The ﹩{\chi }_{\nu }^{2}﹩ for the best-fitting spectral model is 1.9 and 8.3 for the dayside and nightside spectra, respectively.
Paper: JWST-TST DREAMS: The Nightside Emission and Chemistry of WASP-17b
Authors: Jacob Lustig-Yaeger, Kristin S. Sotzen, Kevin B. Stevenson, Shang-Min Tsai, Ryan C. Challener, Jayesh Goyal, Nikole K. Lewis, Dana R. Louie, L. C. Mayorga, Daniel Valentine, Hannah R. Wakeford, Lili Alderson, Natalie H. Allen, Thomas J. Fauchez, Ana Glidden, Amélie Gressier, Sarah M. Hörst, Jingcheng Huang, Zifan Lin, Avi M. Mandell, Elijah Mullens, Sarah Peacock, Edward W. Schwieterman, Jeff A. Valenti, C. Matt Mountain, Marshall Perrin, Roeland P. van der Marel
Figure caption: The same as Figure 6 but for CH4. While the uncertainty on the retrieved CH4 VMRs is large, the nightside containing more CH4 is consistent with our predictions, particularly for all the strong-vertical-mixing cases or weak vertical mixing with zonal wind ≲3000 m s−1.
Paper: A Deep Dive down the Broad-line Region: Permitted O I, Ca II, and Fe II Emission in an Active Galactic Nucleus Little Red Dot at z = 5.3
Authors: Roberta Tripodi, Maruša Bradač, Francesco D'Eugenio, Nicholas Martis, Gregor Rihtaršič, Chris Willott, Laura Pentericci, Bianca Moreschini, Maxim Markevitch, Yoshihisa Asada, Antonello Calabró, Guillaume Desprez, Giordano Felicioni, Gaia Gaspar, Anthony H. Gonzalez, Anishya Harshan, Xihan Ji, Jon Judež, Brian C. Lemaux, Alessandro Marconi, Vladan Markov, Rosa M. Merida, Lorenzo Napolitano, Gaël Noirot, Massimiliano Parente, Annika H. G. Peter, Luke Robbins, Andrew Robertson, Ghassan T. E. Sarrouh, Marcin Sawicki
Figure caption: HST/ACS and NIRCam photometry and NIRSpec spectra of Bz5.3. Top panels: 2D and 1D NIRSpec spectra. Fluxes are not corrected for magnification. Lines of interest for this work are highlighted by colored vertical bars. Other detected emission lines are marked with dashed gray vertical lines. The y-axis scale of the 1D spectrum is logarithmic. For comparison, the spectrum of A2744–45924 at z = 4.47 is shown in light orange. Bottom panels: NIRCam cutout photometry in different filters, specified at the top left corner of each panel, and an RGB image made combining the F444W, F356W, and F277W filters for red; F150W and F200W filters for green; and F090W and F115W filters for blue. Cutout images are 2″ × 2″ in size. In each panel, there is an inset zoom-in on the center region to show the flux centroid of the filter (red plus sign) compared to the flux centroid in F444W (black plus sign). The PSF size of each NIRCam filter is shown as a gray circle in the bottom right corner of each panel (or zoom-in inset).
Paper: Detection of Compton Scattering in the Jet of 3C 84
Authors: Ioannis Liodakis, Sudip Chakraborty, Frédéric Marin, Steven R. Ehlert, Thibault Barnouin, Pouya M. Kouch, Kari Nilsson, Elina Lindfors, Tapio Pursimo, Georgios F. Paraschos, Riccardo Middei, Anna Trindade Falcão, Svetlana Jorstad, Iván Agudo, Yuri Y. Kovalev, Jacob J. Casey, Laura Di Gesu, Philip Kaaret, Dawoon E. Kim, Fabian Kislat, Ajay Ratheesh, M. Lynne Saade, Francesco Tombesi, Alan Marscher, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Gabriel Emery, Juan Escudero Pedrosa, Daniel Morcuende, Jorge Otero-Santos, Alfredo Sota, Vilppu Piirola, Rumen Bachev, Anton Strigachev, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Chanwoo Song, Shan Li, Myeong-Seok Nam, Diego Álvarez-Ortega, Carolina Casadio, Emmanouil Angelakis, Alexander Kraus, Jenni Jormanainen, Vandad Fallah Ramazani, Chien-Ting Chen, Enrico Costa, Eugene Churazov, Riccardo Ferrazzoli, Giorgio Galanti, Ildar Khabibullin, Stephen L. O'Dell, Luigi Pacciani, Marco Roncadelli, Oliver J. Roberts, Paolo Soffitta, Douglas A. Swartz, Fabrizio Tavecchio, Martin C. Weisskopf, Irina Zhuravleva
Figure caption: Left: IXPE counts image of the Perseus Cluster overlaid with surface brightness contours from Chandra, showing that many of the substructures clearly apparent in the higher angular resolution Chandra data are also visible at lower resolution in IXPE. The black cross corresponds to the position of 3C 84. Right: cleaned 15 GHz StokesIVLBA image of the parsec-scale jet of 3C 84, observed as part of the MOJAVE program on 2025 February 21, in units of Jy beam−1. Notice that the angular scale of this radio image is approximately three orders of magnitude smaller than the IXPE image. Overlaid in green is the X-ray polarization vector with the 1σ confidence interval of the polarization angle denoted by the two dashed lines. The polarization vector’s direction is fully consistent with the direction of the radio jet.
Paper: A Deep Dive down the Broad-line Region: Permitted O I, Ca II, and Fe II Emission in an Active Galactic Nucleus Little Red Dot at z = 5.3
Authors: Roberta Tripodi, Maruša Bradač, Francesco D'Eugenio, Nicholas Martis, Gregor Rihtaršič, Chris Willott, Laura Pentericci, Bianca Moreschini, Maxim Markevitch, Yoshihisa Asada, Antonello Calabró, Guillaume Desprez, Giordano Felicioni, Gaia Gaspar, Anthony H. Gonzalez, Anishya Harshan, Xihan Ji, Jon Judež, Brian C. Lemaux, Alessandro Marconi, Vladan Markov, Rosa M. Merida, Lorenzo Napolitano, Gaël Noirot, Massimiliano Parente, Annika H. G. Peter, Luke Robbins, Andrew Robertson, Ghassan T. E. Sarrouh, Marcin Sawicki
Figure caption: Zoom-in of the 2D and 1D spectra of Bz5.3. The observed spectrum is shown in black, while the best-fitting model is shown in blue. Residuals are shown at the bottom of each panel, where the shaded dark gray area represents the 1σ noise level. Top panel: zoom-in on the Fe II emission in the optical. The vertical lines are at the laboratory rest wavelength of the reported emission line. Bottom panel: zoom-in on the Fe II complex in the UV and Mg II emission line. The 2σ and 3σ noise levels are reported in the residual as shaded light gray areas.
Paper: A Deep Dive down the Broad-line Region: Permitted O I, Ca II, and Fe II Emission in an Active Galactic Nucleus Little Red Dot at z = 5.3
Authors: Roberta Tripodi, Maruša Bradač, Francesco D'Eugenio, Nicholas Martis, Gregor Rihtaršič, Chris Willott, Laura Pentericci, Bianca Moreschini, Maxim Markevitch, Yoshihisa Asada, Antonello Calabró, Guillaume Desprez, Giordano Felicioni, Gaia Gaspar, Anthony H. Gonzalez, Anishya Harshan, Xihan Ji, Jon Judež, Brian C. Lemaux, Alessandro Marconi, Vladan Markov, Rosa M. Merida, Lorenzo Napolitano, Gaël Noirot, Massimiliano Parente, Annika H. G. Peter, Luke Robbins, Andrew Robertson, Ghassan T. E. Sarrouh, Marcin Sawicki
Figure caption: Zoom-in of the 2D and 1D spectra of Bz5.3. The observed spectrum is shown in black, and the best-fitting model is shown in red. Residuals are shown at the bottom of each panel, where the shaded gray area represents the 1σ noise level. Left panel: zoom-in on the λ1304 bump. The vertical pink line is at the laboratory rest wavelength of the O Iλ1304 emission line. The vertical dashed black line marks the Lyα line. Right panel: zoom-in on the O I λ8446 emission line and the Ca II λ8498, 8542, 8662 triplet. Vertical lines are set at laboratory rest wavelength for these emission lines. The scale of the y-axis is linear.
Paper: A Deep Dive down the Broad-line Region: Permitted O I, Ca II, and Fe II Emission in an Active Galactic Nucleus Little Red Dot at z = 5.3
Authors: Roberta Tripodi, Maruša Bradač, Francesco D'Eugenio, Nicholas Martis, Gregor Rihtaršič, Chris Willott, Laura Pentericci, Bianca Moreschini, Maxim Markevitch, Yoshihisa Asada, Antonello Calabró, Guillaume Desprez, Giordano Felicioni, Gaia Gaspar, Anthony H. Gonzalez, Anishya Harshan, Xihan Ji, Jon Judež, Brian C. Lemaux, Alessandro Marconi, Vladan Markov, Rosa M. Merida, Lorenzo Napolitano, Gaël Noirot, Massimiliano Parente, Annika H. G. Peter, Luke Robbins, Andrew Robertson, Ghassan T. E. Sarrouh, Marcin Sawicki
Figure caption: Same as Figure 5 but for the HOMERUN template (shown in yellow).
Paper: A Deep Dive down the Broad-line Region: Permitted O I, Ca II, and Fe II Emission in an Active Galactic Nucleus Little Red Dot at z = 5.3
Authors: Roberta Tripodi, Maruša Bradač, Francesco D'Eugenio, Nicholas Martis, Gregor Rihtaršič, Chris Willott, Laura Pentericci, Bianca Moreschini, Maxim Markevitch, Yoshihisa Asada, Antonello Calabró, Guillaume Desprez, Giordano Felicioni, Gaia Gaspar, Anthony H. Gonzalez, Anishya Harshan, Xihan Ji, Jon Judež, Brian C. Lemaux, Alessandro Marconi, Vladan Markov, Rosa M. Merida, Lorenzo Napolitano, Gaël Noirot, Massimiliano Parente, Annika H. G. Peter, Luke Robbins, Andrew Robertson, Ghassan T. E. Sarrouh, Marcin Sawicki
Figure caption: Zoom-in of the 2D and 1D spectra of Bz5.3 on the Fe II complex in the UV and Mg II emission line. The observed spectrum is shown in black, while the best-fitting model is shown in blue. Residuals are shown at the bottom of each panel, where the shaded dark gray area represents the 1σ noise level. The 2σ and 3σ noise levels are reported in the residual as shaded light gray areas.
Paper: A Deep Dive down the Broad-line Region: Permitted O I, Ca II, and Fe II Emission in an Active Galactic Nucleus Little Red Dot at z = 5.3
Authors: Roberta Tripodi, Maruša Bradač, Francesco D'Eugenio, Nicholas Martis, Gregor Rihtaršič, Chris Willott, Laura Pentericci, Bianca Moreschini, Maxim Markevitch, Yoshihisa Asada, Antonello Calabró, Guillaume Desprez, Giordano Felicioni, Gaia Gaspar, Anthony H. Gonzalez, Anishya Harshan, Xihan Ji, Jon Judež, Brian C. Lemaux, Alessandro Marconi, Vladan Markov, Rosa M. Merida, Lorenzo Napolitano, Gaël Noirot, Massimiliano Parente, Annika H. G. Peter, Luke Robbins, Andrew Robertson, Ghassan T. E. Sarrouh, Marcin Sawicki
Figure caption: Results of modeling Bz5.3 with Galfit. Left panels: data and results assuming a single point source as a model for each filter. The white cross indicates the centroid of the model. Right panels: data and results assuming as a model a combination of a point source and a Sérsic profile for each filter with λ < 4 μm, with a single point source otherwise.
Paper: A Deep Dive down the Broad-line Region: Permitted O I, Ca II, and Fe II Emission in an Active Galactic Nucleus Little Red Dot at z = 5.3
Authors: Roberta Tripodi, Maruša Bradač, Francesco D'Eugenio, Nicholas Martis, Gregor Rihtaršič, Chris Willott, Laura Pentericci, Bianca Moreschini, Maxim Markevitch, Yoshihisa Asada, Antonello Calabró, Guillaume Desprez, Giordano Felicioni, Gaia Gaspar, Anthony H. Gonzalez, Anishya Harshan, Xihan Ji, Jon Judež, Brian C. Lemaux, Alessandro Marconi, Vladan Markov, Rosa M. Merida, Lorenzo Napolitano, Gaël Noirot, Massimiliano Parente, Annika H. G. Peter, Luke Robbins, Andrew Robertson, Ghassan T. E. Sarrouh, Marcin Sawicki
Figure caption: Same as Figure 5 but for Tsuzuki’s template (shown in yellow).
Paper: Detection of Compton Scattering in the Jet of 3C 84
Authors: Ioannis Liodakis, Sudip Chakraborty, Frédéric Marin, Steven R. Ehlert, Thibault Barnouin, Pouya M. Kouch, Kari Nilsson, Elina Lindfors, Tapio Pursimo, Georgios F. Paraschos, Riccardo Middei, Anna Trindade Falcão, Svetlana Jorstad, Iván Agudo, Yuri Y. Kovalev, Jacob J. Casey, Laura Di Gesu, Philip Kaaret, Dawoon E. Kim, Fabian Kislat, Ajay Ratheesh, M. Lynne Saade, Francesco Tombesi, Alan Marscher, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Gabriel Emery, Juan Escudero Pedrosa, Daniel Morcuende, Jorge Otero-Santos, Alfredo Sota, Vilppu Piirola, Rumen Bachev, Anton Strigachev, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Chanwoo Song, Shan Li, Myeong-Seok Nam, Diego Álvarez-Ortega, Carolina Casadio, Emmanouil Angelakis, Alexander Kraus, Jenni Jormanainen, Vandad Fallah Ramazani, Chien-Ting Chen, Enrico Costa, Eugene Churazov, Riccardo Ferrazzoli, Giorgio Galanti, Ildar Khabibullin, Stephen L. O'Dell, Luigi Pacciani, Marco Roncadelli, Oliver J. Roberts, Paolo Soffitta, Douglas A. Swartz, Fabrizio Tavecchio, Martin C. Weisskopf, Irina Zhuravleva
Figure caption: Archival optical and γ-ray polarization observations. The top panel shows the host-corrected polarization degree (%, R band), the middle panel the polarization angle (degrees, R band), and the bottom panel the 3-day binned Fermi photon flux light curve in the 0.1–100 GeV band. The horizontal red shaded area marks the projected direction of the jet. The error bars correspond to the 68% (1σ) confidence interval.
Paper: Detection of Compton Scattering in the Jet of 3C 84
Authors: Ioannis Liodakis, Sudip Chakraborty, Frédéric Marin, Steven R. Ehlert, Thibault Barnouin, Pouya M. Kouch, Kari Nilsson, Elina Lindfors, Tapio Pursimo, Georgios F. Paraschos, Riccardo Middei, Anna Trindade Falcão, Svetlana Jorstad, Iván Agudo, Yuri Y. Kovalev, Jacob J. Casey, Laura Di Gesu, Philip Kaaret, Dawoon E. Kim, Fabian Kislat, Ajay Ratheesh, M. Lynne Saade, Francesco Tombesi, Alan Marscher, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Gabriel Emery, Juan Escudero Pedrosa, Daniel Morcuende, Jorge Otero-Santos, Alfredo Sota, Vilppu Piirola, Rumen Bachev, Anton Strigachev, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Chanwoo Song, Shan Li, Myeong-Seok Nam, Diego Álvarez-Ortega, Carolina Casadio, Emmanouil Angelakis, Alexander Kraus, Jenni Jormanainen, Vandad Fallah Ramazani, Chien-Ting Chen, Enrico Costa, Eugene Churazov, Riccardo Ferrazzoli, Giorgio Galanti, Ildar Khabibullin, Stephen L. O'Dell, Luigi Pacciani, Marco Roncadelli, Oliver J. Roberts, Paolo Soffitta, Douglas A. Swartz, Fabrizio Tavecchio, Martin C. Weisskopf, Irina Zhuravleva
Figure caption: Radio flux density and polarization measurements during the IXPE observations. The top panel shows the flux density in jansky, the middle panel the polarization degree (%), and the bottom panel the polarization angle (degrees). The gray shaded areas mark the IXPE exposures over the entire observation. The different radio frequencies are marked with different symbols and colors as shown in the legend. The horizontal red shaded area marks the projected direction of the jet. The error bars correspond to the 68% (1σ) confidence interval.
Paper: Detection of Compton Scattering in the Jet of 3C 84
Authors: Ioannis Liodakis, Sudip Chakraborty, Frédéric Marin, Steven R. Ehlert, Thibault Barnouin, Pouya M. Kouch, Kari Nilsson, Elina Lindfors, Tapio Pursimo, Georgios F. Paraschos, Riccardo Middei, Anna Trindade Falcão, Svetlana Jorstad, Iván Agudo, Yuri Y. Kovalev, Jacob J. Casey, Laura Di Gesu, Philip Kaaret, Dawoon E. Kim, Fabian Kislat, Ajay Ratheesh, M. Lynne Saade, Francesco Tombesi, Alan Marscher, Francisco José Aceituno, Giacomo Bonnoli, Víctor Casanova, Gabriel Emery, Juan Escudero Pedrosa, Daniel Morcuende, Jorge Otero-Santos, Alfredo Sota, Vilppu Piirola, Rumen Bachev, Anton Strigachev, George A. Borman, Tatiana S. Grishina, Vladimir A. Hagen-Thorn, Evgenia N. Kopatskaya, Elena G. Larionova, Daria A. Morozova, Sergey S. Savchenko, Ekaterina V. Shishkina, Ivan S. Troitskiy, Yulia V. Troitskaya, Andrey A. Vasilyev, Alexey V. Zhovtan, Ioannis Myserlis, Mark Gurwell, Garrett Keating, Ramprasad Rao, Sincheol Kang, Sang-Sung Lee, Sanghyun Kim, Whee Yeon Cheong, Hyeon-Woo Jeong, Chanwoo Song, Shan Li, Myeong-Seok Nam, Diego Álvarez-Ortega, Carolina Casadio, Emmanouil Angelakis, Alexander Kraus, Jenni Jormanainen, Vandad Fallah Ramazani, Chien-Ting Chen, Enrico Costa, Eugene Churazov, Riccardo Ferrazzoli, Giorgio Galanti, Ildar Khabibullin, Stephen L. O'Dell, Luigi Pacciani, Marco Roncadelli, Oliver J. Roberts, Paolo Soffitta, Douglas A. Swartz, Fabrizio Tavecchio, Martin C. Weisskopf, Irina Zhuravleva
Figure caption: DCF between optical and the 3-day binned γ-ray light curves. The top panel shows the DCF considering all the available observations, and the bottom panel shows the DCF for the 2025 flare that coincided with the IXPE observations. In both panels the vertical magenta line marks a time lag of zero.
Paper: 1000–10,000 M⊙ Primordial Stars Created the Nitrogen Excess in GS 3073 at z = 5.55
Authors: Devesh Nandal, Daniel J. Whalen, Muhammad A. Latif, Alexander Heger
Figure caption: N/O, C/O, and Ne/O number ratios for five select models in the mass range of 1000–10,000 M⊙ Pop III stars. Top: 10% mass loss. Center: 50% mass loss. Bottom: loss of all the mass above the CO core. The green, yellow, and brown stars indicate ratios for GS 3073, CEERS 1019, and GN-z11, respectively. The dilution factor is the mass of the gas contaminated by outflows from the star divided by the mass of the outflow. Outliers appear only in the “CO core” case (bottom panel), where the mass cut can intersect the narrow N-rich/O-poor layer immediately outside the core; the 10% and 50% fixed fraction cases average over this gradient and exhibit much smaller scatter.
Paper: 1000–10,000 M⊙ Primordial Stars Created the Nitrogen Excess in GS 3073 at z = 5.55
Authors: Devesh Nandal, Daniel J. Whalen, Muhammad A. Latif, Alexander Heger
Figure caption: Abundance ratios of five SMSs with contributions by the galactic stars for the case of 10% mass loss. The green, yellow, and brown stars indicate ratios for GS 3073, CEERS 1019, and GN-z11, respectively. If the chemically mature stellar population contributes C, N, O, and Ne mass fractions χC = 2.8 × 10−4, χN = 8 × 10−5, χO = 1.2 × 10−3, and χNe = 9.4 × 10−4 then all 10 models can reproduce the observed near-vertical transition in the N/O ratio while also explaining the C/O ratios (X. Ji et al. 2024).
Paper: The Near-ultraviolet Spectra of FU Orionis Accretion Disks
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Gregory J. Herczeg, Kevin France
Figure caption: The G230L and G430L spectra for each of our objects (dark blue), along with the disk (green) and disk + UV excess (light blue) models for each of the FUOrs in the survey. The shaded regions show the range of the 16th and 84th percentile models from the Markov Chain Monte Carlo samples. The blackbody component in each panel (maroon) matches the flux level of the binned continuum points (salmon) blueward of 2300 Å. The flux upper limits for V1057 Cyg, HBC 722, and BBW 76 are shown as empty triangles.
Paper: The Near-ultraviolet Spectra of FU Orionis Accretion Disks
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Gregory J. Herczeg, Kevin France
Figure caption: Upper panel: the ratio of the observed binned STIS spectra used to fit the blackbody excess model and the disk models binned to the same wavelength sampling. Notice that for all the FUOrs in the sample, the NUV flux is at least 2× as bright as the disk model predicts at 2200 Å and for many, the flux ratio is > 10 (for HBC 722 and V1057 Cyg, this is true at 2400 Å, despite the lack of data at 2200 Å). Lower panel: the Lexcess measurements for each of the FUOrs compared with their disk-model-derived Lacc. The error bars on each point are given by the 1σ ranges of their posterior distributions. The mean and standard deviation on the UV excess luminosities (excluding BBW 76) are marked by the purple line and shading, respectively.
Paper: 1000–10,000 M⊙ Primordial Stars Created the Nitrogen Excess in GS 3073 at z = 5.55
Authors: Devesh Nandal, Daniel J. Whalen, Muhammad A. Latif, Alexander Heger
Figure caption: BH growth rates. Birth redshifts are z = 10 and 20, and we consider mass losses of 10% and 50%. The AGN and its error bars in mass are marked by the solid black circle. Green is the 9000 M⊙ BH growing at 0.5 LEdd, blue is the 500 M⊙ BH growing at LEdd, cyan is the 500 M⊙ BH growing at 0.5 LEdd, magenta is the 2700 M⊙ BH growing at LEdd, and red is the 1500 M⊙ BH growing at LEdd. Observational constraints on the accretion rate of the AGN at z = 5.55 are 0.1–1.6 LEdd (X. Ji et al. 2024).
Paper: 1000–10,000 M⊙ Primordial Stars Created the Nitrogen Excess in GS 3073 at z = 5.55
Authors: Devesh Nandal, Daniel J. Whalen, Muhammad A. Latif, Alexander Heger
Figure caption: Top: N/O ratios for rotating and nonrotating 5000 M⊙ SMSs. Bottom: He/H abundance ratios. Panels (a), (b) and (c) are for mass losses of 10%, 50%, and the CO core, respectively.
Paper: 1000–10,000 M⊙ Primordial Stars Created the Nitrogen Excess in GS 3073 at z = 5.55
Authors: Devesh Nandal, Daniel J. Whalen, Muhammad A. Latif, Alexander Heger
Figure caption: Left: evolution of central densities versus central temperatures. The gray shaded zone is the PI regime. A few models such as the 6000, 7000, and 8000 M⊙ stars were evolved past the PI into core Si burning. Right: collapse of the 8000 M⊙ star to a BH.