adsabs/AstroCLIMB huggingface dataset:
Paper: The Effect of Stellar Magnetic Activity on Measurements of Morning and Evening Asymmetry of Planetary Terminator
Authors: N. Kostogryz, A. I. Shapiro, L. Carone, L. Gizon, Ch. Helling, S. Kiefer, S. Mercier, S. Seager, S. K. Solanki, Y. Unruh, J. de Wit, V. Witzke
Figure caption: Sketch of a planet transiting a star with a spatially inhomogeneous distribution of magnetic field. The central panel shows a planet (black filled circles) transiting a star with an active eastern hemisphere (left side of the star) and a quiet western hemisphere (right side). The effect of the magnetic field on the stellar surface is especially pronounced at the near-limb stellar regions. We illustrate this by showing quiet (SSD, left panel) and active (300 G case, right panel) MURaM snapshots that are computed with the MPS-ATLAS code at 600 nm for the near-limb viewing angle. The star, planet, and MURaM snapshots are not in scale.
Paper: The Effect of Stellar Magnetic Activity on Measurements of Morning and Evening Asymmetry of Planetary Terminator
Authors: N. Kostogryz, A. I. Shapiro, L. Carone, L. Gizon, Ch. Helling, S. Kiefer, S. Mercier, S. Seager, S. K. Solanki, Y. Unruh, J. de Wit, V. Witzke
Figure caption: Planet vs. stellar asymmetry for the illustrative case of WASP-39. Plotted are the differences between transit depths of ingress and egress, as in Figure 3. The blue line is the stellar magnetically induced asymmetry for 300 G. The orange and blue lines show planetary asymmetry following scenarios from the IWF Graz 3D hierarchical cloud model. The wavelength dependencies of planetary and stellar signals differ significantly, providing a key to disentangle them.
Paper: The Effect of Stellar Magnetic Activity on Measurements of Morning and Evening Asymmetry of Planetary Terminator
Authors: N. Kostogryz, A. I. Shapiro, L. Carone, L. Gizon, Ch. Helling, S. Kiefer, S. Mercier, S. Seager, S. K. Solanki, Y. Unruh, J. de Wit, V. Witzke
Figure caption: Magnetically induced asymmetry of the transit light curve as a function of wavelength. Plotted are the differences between transit depths of ingress and of egress at different wavelength ranges, i.e., from 0.35 to 1.5 μm in panel (a) and from 1.5 to 10 μm in panel (b). The gray arrows demonstrate the passbandwidth of different instruments: Kepler, PLATO, TESS, and CHEOPS. The light-curve asymmetry is strongly wavelength-dependent, decreasing toward infrared wavelengths.
Paper: Solar Disk Gamma-Ray Emission via Synthetic Magnetic Field from Photosphere to Low Corona
Authors: Eleonora Puzzoni, Federico Fraschetti, József Kóta, Joe Giacalone
Figure caption: Left panel: angular components θ and ϕ of the velocity vector of the GCRs at tint for Ep = 100 GeV with σ2 = 10 and injection at z = zdown. Right panel: same as left panel for Ep = 10 TeV.
Paper: CAPERS-LRD-z9: A Gas-enshrouded Little Red Dot Hosting a Broad-line Active Galactic Nucleus at z = 9.288
Authors: Anthony J. Taylor, Vasily Kokorev, Dale D. Kocevski, Hollis B. Akins, Fergus Cullen, Mark Dickinson, Steven L. Finkelstein, Pablo Arrabal Haro, Volker Bromm, Mauro Giavalisco, Kohei Inayoshi, Stéphanie Juneau, Gene C. K. Leung, Pablo G. Pérez-González, Rachel S. Somerville, Jonathan R. Trump, Ricardo O. Amorín, Guillermo Barro, Denis Burgarella, Madisyn Brooks, Adam C. Carnall, Caitlin M. Casey, Yingjie Cheng, John Chisholm, Katherine Chworowsky, Kelcey Davis, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Vital Fernández, Seiji Fujimoto, Norman A. Grogin, Ansh R. Gupta, Nimish P. Hathi, Intae Jung, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Rebecca L. Larson, Ho-Hin Leung, Mario Llerena, Ray A. Lucas, Derek J. McLeod, Ross McLure, Lorenzo Napolitano, Casey Papovich, Thomas M. Stanton, Roberta Tripodi, Xin Wang, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Top: 5″ × 5″ NIRCam and MIRI cutouts of CAPERS-LRD-z9 in the PRIMER-COSMOS NIRCam and COSMOS-3D MIRI images. We also show RGB images generated for both the short-wavelength and long-wavelength NIRCam detectors. We overplot the NIRSpec MSA slitlet. Bottom: we plot the 2D and 1D photometrically calibrated spectra of CAPERS-LRD-z9 in fλ. We mark strongly detected emission features with red dashed lines and overplot the NIRCam photometry with blue squares. Despite being near the corner of the central shutter in the slitlet, CAPERS-LRD-z9 exhibits a detectable Lyα break, a strong Balmer break, and clear rest-optical emission line detections, including broadened Hβ and Hγ and narrow [O III] λλ4959, 5007. The combination of narrow forbidden lines and a broad Hβ clearly indicates that CAPERS-LRD-z9 is a BLAGN at z = 9.288.
Paper: CAPERS-LRD-z9: A Gas-enshrouded Little Red Dot Hosting a Broad-line Active Galactic Nucleus at z = 9.288
Authors: Anthony J. Taylor, Vasily Kokorev, Dale D. Kocevski, Hollis B. Akins, Fergus Cullen, Mark Dickinson, Steven L. Finkelstein, Pablo Arrabal Haro, Volker Bromm, Mauro Giavalisco, Kohei Inayoshi, Stéphanie Juneau, Gene C. K. Leung, Pablo G. Pérez-González, Rachel S. Somerville, Jonathan R. Trump, Ricardo O. Amorín, Guillermo Barro, Denis Burgarella, Madisyn Brooks, Adam C. Carnall, Caitlin M. Casey, Yingjie Cheng, John Chisholm, Katherine Chworowsky, Kelcey Davis, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Vital Fernández, Seiji Fujimoto, Norman A. Grogin, Ansh R. Gupta, Nimish P. Hathi, Intae Jung, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Rebecca L. Larson, Ho-Hin Leung, Mario Llerena, Ray A. Lucas, Derek J. McLeod, Ross McLure, Lorenzo Napolitano, Casey Papovich, Thomas M. Stanton, Roberta Tripodi, Xin Wang, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: The observed NIRSpec/PRISM spectrum of CAPERS-LRD-z9 is shown as the fine black curve with uncertainties in gray. Left: line fits and 1σ uncertainties on Hγ (blue curves and shaded regions), [O III] λ4363 (orange curve and shaded region), and the combined fit (thick black curve and shaded region). We deblend these lines using the high-confidence line widths and redshift solution measured from Hβ + [O III] λλ4959, 5007. We show the region of masked spurious pixels with gray shading. Right: line fits to Hβ + [O III] λλ4959, 5007. A broad (FWHM = 3521 ± 502 km s−1; blue curve) component is clearly necessary to reproduce the Hβ. We also fit narrow emission (light blue) and absorption (dashed red) components to Hβ to better model the double-peak structure of the line, though their fluxes are degenerate at PRISM resolution. The [O III] λλ4959, 5007 doublet is also detected at S/N ∼ 4. The combination of narrow [O III] λλ4959, 5007 and broad Hβ is a clear indicator of a BLAGN.
Paper: CAPERS-LRD-z9: A Gas-enshrouded Little Red Dot Hosting a Broad-line Active Galactic Nucleus at z = 9.288
Authors: Anthony J. Taylor, Vasily Kokorev, Dale D. Kocevski, Hollis B. Akins, Fergus Cullen, Mark Dickinson, Steven L. Finkelstein, Pablo Arrabal Haro, Volker Bromm, Mauro Giavalisco, Kohei Inayoshi, Stéphanie Juneau, Gene C. K. Leung, Pablo G. Pérez-González, Rachel S. Somerville, Jonathan R. Trump, Ricardo O. Amorín, Guillermo Barro, Denis Burgarella, Madisyn Brooks, Adam C. Carnall, Caitlin M. Casey, Yingjie Cheng, John Chisholm, Katherine Chworowsky, Kelcey Davis, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Vital Fernández, Seiji Fujimoto, Norman A. Grogin, Ansh R. Gupta, Nimish P. Hathi, Intae Jung, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Rebecca L. Larson, Ho-Hin Leung, Mario Llerena, Ray A. Lucas, Derek J. McLeod, Ross McLure, Lorenzo Napolitano, Casey Papovich, Thomas M. Stanton, Roberta Tripodi, Xin Wang, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Black hole mass to stellar mass ratio ﹩{\mathrm{log}}\,\left({M}_{{\rm{BH}}}/{M}_{* }\right)﹩ as a function of redshift for CAPERS-LRD-z9 (red star) and a collection of literature JWST-detected AGN (Y. Harikane et al. 2023; D. D. Kocevski et al. 2023, 2025; V. Kokorev et al. 2023, 2024a; R. L. Larson et al. 2023; Á. Bogdán et al. 2024; L. J. Furtak et al. 2024; I. Labbe et al. 2024; R. Maiolino et al. 2024; L. Napolitano et al. 2024; R. Tripodi et al. 2024; H. Übler et al. 2024; B. Wang et al. 2025; M. Yue et al. 2024b; H. B. Akins et al. 2025a; I. Juodžbalis et al. 2025), showing the published errors, typically exclusive of systematic uncertainties. We divide the literature-selected samples into those selected based on a broad Hα line (purple points), a broad Hβ line (pink points), and based on UV line or X-ray detections (yellow points). We plot the statistical errors on CAPERS-LRD-z9 as the black error bars, and we include a larger systematic range on ﹩{\mathrm{log}}\,\left({M}_{{\rm{BH}}}/{M}_{* }\right)﹩ based on the systematic limits on the black hole mass of CAPERS-LRD-z9 as a gray dashed line and upward-pointing arrows. We stress that as our M* measurement is an upper limit, all of our measurements of MBH/M* are lower limits. We plot the MBH/M* = 0.1% value for local galaxies as a black dashed line. For comparison, we overlay the predicted evolution of MBH/M* ratios from early black hole populations formed via two distinct seeding channels: heavy seeds (red shaded region) and light seeds (blue shaded region), based on the semianalytical model presented in H. Hu et al. (2025). The population of JWST-detected AGN exhibits an apparent overmassiveness in this ratio compared to the local relation.
Paper: CAPERS-LRD-z9: A Gas-enshrouded Little Red Dot Hosting a Broad-line Active Galactic Nucleus at z = 9.288
Authors: Anthony J. Taylor, Vasily Kokorev, Dale D. Kocevski, Hollis B. Akins, Fergus Cullen, Mark Dickinson, Steven L. Finkelstein, Pablo Arrabal Haro, Volker Bromm, Mauro Giavalisco, Kohei Inayoshi, Stéphanie Juneau, Gene C. K. Leung, Pablo G. Pérez-González, Rachel S. Somerville, Jonathan R. Trump, Ricardo O. Amorín, Guillermo Barro, Denis Burgarella, Madisyn Brooks, Adam C. Carnall, Caitlin M. Casey, Yingjie Cheng, John Chisholm, Katherine Chworowsky, Kelcey Davis, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Vital Fernández, Seiji Fujimoto, Norman A. Grogin, Ansh R. Gupta, Nimish P. Hathi, Intae Jung, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Rebecca L. Larson, Ho-Hin Leung, Mario Llerena, Ray A. Lucas, Derek J. McLeod, Ross McLure, Lorenzo Napolitano, Casey Papovich, Thomas M. Stanton, Roberta Tripodi, Xin Wang, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: The NIRSpec MSA/PRISM spectra of CAPERS-LRD-z9, MoM-BH*-1 at z = 7.76 (R. P. Naidu et al. 2025), RUBIES-UDS-154183 at z = 3.55 (A. de Graaff et al. 2025), UNCOVER-45924 at z = 4.47 (I. Labbe et al. 2024), and A2744-QSO1 at z = 7.04 (L. J. Furtak et al. 2024; X. Ji et al. 2025) normalized to the spectrum of CAPERS-LRD-z9 at rest-frame 0.51 μm. We apply a 1–2 pixel Gaussian smoothing (smoothing lower-z objects less, as they are already relatively smoothed by PRISM’s lower spectral resolution at bluer observed wavelengths) to all five spectra to increase visual clarity. For comparison, we plot the median and 10th–90th percentile of DESI spectra of 232 quasars (z < 0.95) selected to have similar values of Hβbroad FWHM, L([O III] λ5007), and [O III] λ5007/Hβ flux ratio (gray shading and gray dashed curve) and the stack of the reddest 20 DESI quasars (gray solid curve). While the rest-optical emission from CAPERS-LRD-z9 strongly resembles that of the other NIRSpec sources, these sources are all starkly different from quasars identified in DESI, where even the reddest DESI quasars fail to approach the reddening or Balmer break exhibited in the NIRSpec LRDs.
Paper: CAPERS-LRD-z9: A Gas-enshrouded Little Red Dot Hosting a Broad-line Active Galactic Nucleus at z = 9.288
Authors: Anthony J. Taylor, Vasily Kokorev, Dale D. Kocevski, Hollis B. Akins, Fergus Cullen, Mark Dickinson, Steven L. Finkelstein, Pablo Arrabal Haro, Volker Bromm, Mauro Giavalisco, Kohei Inayoshi, Stéphanie Juneau, Gene C. K. Leung, Pablo G. Pérez-González, Rachel S. Somerville, Jonathan R. Trump, Ricardo O. Amorín, Guillermo Barro, Denis Burgarella, Madisyn Brooks, Adam C. Carnall, Caitlin M. Casey, Yingjie Cheng, John Chisholm, Katherine Chworowsky, Kelcey Davis, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Vital Fernández, Seiji Fujimoto, Norman A. Grogin, Ansh R. Gupta, Nimish P. Hathi, Intae Jung, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Rebecca L. Larson, Ho-Hin Leung, Mario Llerena, Ray A. Lucas, Derek J. McLeod, Ross McLure, Lorenzo Napolitano, Casey Papovich, Thomas M. Stanton, Roberta Tripodi, Xin Wang, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Redshifts and black hole masses of CAPERS-LRD-z9 (red star; canonical errors are shown in black, systematic upper and lower limits are shown in gray), populations of z ≳ 6 quasars (small blue points; K. Inayoshi et al. 2020; X. Fan et al. 2023; R. Maiolino et al. 2024), notable massive z > 6 spectroscopically confirmed BLAGN (filled symbols; V. Kokorev et al. 2023; R. L. Larson et al. 2023; L. J. Furtak et al. 2024; R. Tripodi et al. 2024; H. B. Akins et al. 2025a; X. Lin et al. 2025; R. P. Naidu et al. 2025), and the highest-redshift AGN detected through X-ray emission and high-ionization UV emission lines, respectively (open symbols; A. J. Bunker et al. 2023; A. D. Goulding et al. 2023; O. E. Kovács et al. 2024; L. Napolitano et al. 2024). We also show the growth of 102 M⊙ (blue shading) and 104 M⊙ (red shading) black hole seeds growing at the Eddington limit. We also show the growth track of a 102 M⊙ stellar remnant formed at z = 30 that starts accreting at 1.85× the Eddington limit 100 Myr after formation (dark blue dashed curve). CAPERS-LRD-z9’s black hole is too massive to be the result of an Eddington-limited stellar seed; thus, a stellar remnant light seed undergoing periods of super-Eddington accretion or a heavy seed are necessary to produce CAPERS-LRD-z9’s black hole by z = 9.288.
Paper: CAPERS-LRD-z9: A Gas-enshrouded Little Red Dot Hosting a Broad-line Active Galactic Nucleus at z = 9.288
Authors: Anthony J. Taylor, Vasily Kokorev, Dale D. Kocevski, Hollis B. Akins, Fergus Cullen, Mark Dickinson, Steven L. Finkelstein, Pablo Arrabal Haro, Volker Bromm, Mauro Giavalisco, Kohei Inayoshi, Stéphanie Juneau, Gene C. K. Leung, Pablo G. Pérez-González, Rachel S. Somerville, Jonathan R. Trump, Ricardo O. Amorín, Guillermo Barro, Denis Burgarella, Madisyn Brooks, Adam C. Carnall, Caitlin M. Casey, Yingjie Cheng, John Chisholm, Katherine Chworowsky, Kelcey Davis, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Vital Fernández, Seiji Fujimoto, Norman A. Grogin, Ansh R. Gupta, Nimish P. Hathi, Intae Jung, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Rebecca L. Larson, Ho-Hin Leung, Mario Llerena, Ray A. Lucas, Derek J. McLeod, Ross McLure, Lorenzo Napolitano, Casey Papovich, Thomas M. Stanton, Roberta Tripodi, Xin Wang, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Spectrum and 1σ errors of CAPERS-LRD-z9 (gray curve, light gray shading), the best-fit host galaxy component (solid and dashed blue curves), the best-fit dense-gas-enshrouded AGN component (solid and dashed red curves), combined host+AGN fit (solid and dashed black curves), photometry data (dark blue squares and upper limits), best-fit model photometry (black points) in the upper panel, and masked regions (light orange shading). The lower panel shows the χ residuals of the fit for the spectrum (gray curve) and photometry (dark blue squares). Note that neither the bagpipes stellar model nor the Cloudy AGN model can match the strong [O III] λ4363 emission.
Paper: CAPERS-LRD-z9: A Gas-enshrouded Little Red Dot Hosting a Broad-line Active Galactic Nucleus at z = 9.288
Authors: Anthony J. Taylor, Vasily Kokorev, Dale D. Kocevski, Hollis B. Akins, Fergus Cullen, Mark Dickinson, Steven L. Finkelstein, Pablo Arrabal Haro, Volker Bromm, Mauro Giavalisco, Kohei Inayoshi, Stéphanie Juneau, Gene C. K. Leung, Pablo G. Pérez-González, Rachel S. Somerville, Jonathan R. Trump, Ricardo O. Amorín, Guillermo Barro, Denis Burgarella, Madisyn Brooks, Adam C. Carnall, Caitlin M. Casey, Yingjie Cheng, John Chisholm, Katherine Chworowsky, Kelcey Davis, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Vital Fernández, Seiji Fujimoto, Norman A. Grogin, Ansh R. Gupta, Nimish P. Hathi, Intae Jung, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Rebecca L. Larson, Ho-Hin Leung, Mario Llerena, Ray A. Lucas, Derek J. McLeod, Ross McLure, Lorenzo Napolitano, Casey Papovich, Thomas M. Stanton, Roberta Tripodi, Xin Wang, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Spectrum and 1σ errors of CAPERS-LRD-z9 (gray curve, light gray shading), the best-fit host galaxy component (solid and dashed blue curves), the best-fit dense-gas-enshrouded AGN component (solid and dashed red curves), combined host+AGN fit (solid and dashed black curves), fiducial SMC dust law fit (solid and dashed purple curves), photometry data (dark blue squares and upper limits), best-fit model photometry (black points) in the upper panel, and masked regions (gold shading). The lower panel shows the χ residuals of the fit for the spectrum (gray curve) and photometry (dark blue squares). Note that the flexible (yet unphysically steep) AGN dust law allows for strong agreement with the MIRI F1000W flux that cannot be reproduced by an SMC law.
Paper: CAPERS-LRD-z9: A Gas-enshrouded Little Red Dot Hosting a Broad-line Active Galactic Nucleus at z = 9.288
Authors: Anthony J. Taylor, Vasily Kokorev, Dale D. Kocevski, Hollis B. Akins, Fergus Cullen, Mark Dickinson, Steven L. Finkelstein, Pablo Arrabal Haro, Volker Bromm, Mauro Giavalisco, Kohei Inayoshi, Stéphanie Juneau, Gene C. K. Leung, Pablo G. Pérez-González, Rachel S. Somerville, Jonathan R. Trump, Ricardo O. Amorín, Guillermo Barro, Denis Burgarella, Madisyn Brooks, Adam C. Carnall, Caitlin M. Casey, Yingjie Cheng, John Chisholm, Katherine Chworowsky, Kelcey Davis, Callum T. Donnan, James S. Dunlop, Richard S. Ellis, Vital Fernández, Seiji Fujimoto, Norman A. Grogin, Ansh R. Gupta, Nimish P. Hathi, Intae Jung, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Rebecca L. Larson, Ho-Hin Leung, Mario Llerena, Ray A. Lucas, Derek J. McLeod, Ross McLure, Lorenzo Napolitano, Casey Papovich, Thomas M. Stanton, Roberta Tripodi, Xin Wang, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Results of 2D surface brightness profile fitting. We show 2″ × 2″ cutouts in F200W and F444W around CAPERS-LRD-z9 in the left column. Our best-fit point-source models in each band are shown in the middle column, while the residuals (data-model) are shown in the rightmost column. CAPERS-LRD-z9 is unresolved in all bands, with ﹩{r}_{h}\lt 0\mathop{.}\limits^{^{\prime\prime} }04﹩ and ﹩0\mathop{.}\limits^{^{\prime\prime} }08﹩ in F200W and F444W, respectively, corresponding to respective physical sizes of ≲175 pc and ≲350 pc.
Paper: The Physical Nature of the Off-center Extended Emission Associated with the Little Red Dots
Authors: Chang-Hao Chen, 昌 灏 陈, Luis C. Ho, Ruancun Li, 阮 存 李, Kohei Inayoshi
Figure caption: Best-fit stellar SED models from GalfitS for the off-center emission. The measured flux densities for solid detections are presented by filled green dots with error bars, and upper limits are marked as green triangles. Blue lines and circles represent the best-fit model assuming the photometric redshift from EAzY, while red lines and circles denote the model that uses the spectroscopic redshift of the LRD. The redshift, total fitting χ2, and best-fit stellar mass for each model are labeled in each panel. The best-fit star formation history (averaged in 10 Myr bins) for the model at the LRD redshift is plotted in the inset panel.
Paper: The Physical Nature of the Off-center Extended Emission Associated with the Little Red Dots
Authors: Chang-Hao Chen, 昌 灏 陈, Luis C. Ho, Ruancun Li, 阮 存 李, Kohei Inayoshi
Figure caption: Simultaneous multiband image fitting results for MSA10686 at z = 5.05. Each row shows the result for one NIRCam band. In the leftmost column, the upper portion of each panel shows the radial surface brightness (open circles with error bars), the PSF model (blue dotted line), as well as the median profile of the best-fit model (blue solid line) and its standard deviation (blue shaded region), derived by randomly inserting the model into empty sky regions within the field of view. We present the best-fit point source + Sérsic model for bands where the off-center blobs are detected and a single point-source model for bands where the blobs are not detected. The χ2 for each band is given in the lower left corner of each panel. The lower portion of each panel gives the residuals between the data and the best-fit model (data − model). The imaging columns, from left to right, display the original data, best-fit model, data minus the nucleus component, and residuals normalized by the errors (data − model/error), which are stretched linearly from −5 to 5.
Paper: The Physical Nature of the Off-center Extended Emission Associated with the Little Red Dots
Authors: Chang-Hao Chen, 昌 灏 陈, Luis C. Ho, Ruancun Li, 阮 存 李, Kohei Inayoshi
Figure caption: The variation with stellar mass (M*) of (a) star formation rate and (b) stellar mass effective radius (Re) for the off-center blobs (red dots) and high-redshift EELGs (blue dots) from M. Llerena et al. (2024). The black dashed line in panel (a) represents the star formation main sequence at z = 4.5 from M. P. Koprowski et al. (2024), and in panel (b), it shows the mass–size relation at z = 5 from the evolution model of T. Morishita et al. (2024). The gray shaded region gives the 1σ scatter for the star formation main sequence in panel (a) and the 3σ scatter for the mass–size relation in panel (b). We chose a 3σ confidence region for the mass–size relation in order to be consistent with the comparison made in M. Llerena et al. (2024).
Paper: The Physical Nature of the Off-center Extended Emission Associated with the Little Red Dots
Authors: Chang-Hao Chen, 昌 灏 陈, Luis C. Ho, Ruancun Li, 阮 存 李, Kohei Inayoshi
Figure caption: Overlapping probability as a function of redshift for the off-center emission.
Paper: Uniform Reanalysis of JWST MIRI 15 μm Exoplanet Eclipse Observations Using Frame-normalized Principal Component Analysis
Authors: Nicholas J. Connors, Christopher Monaghan, Björn Benneke, Lisa Dang
Figure caption: FN-PCA detrending fit for TRAPPIST-1 b visit 1 using the Erebus pipeline. The panels on the left, from top to bottom, show the raw lightcurve produced by our pipeline, the detrended lightcurve using the FN-PCA systematic model, a breakdown of the linear and PCA components of the systematic model, and a plot comparing the rms of residuals depending on bin size showing the goodness of fit compared to the ideal case (dotted line). The panels on the right show the raw lightcurve and PSF (first row), and the eigenvalue and eigenimages for the top five principal components explaining most of the variance (rows 2–6). The dashed line on the eigenvalue plots shows where the value is 0. As the dimmest star analyzed, we see the detector-settling component (Section 3.1) is the most prominent principal component (PC1), followed by the positive-diagonal centroiding component (PC2; Section 3.2). The negative-diagonal centroiding component is not present, and the remaining principal components are pixel-dominated (PC3; Section 3.3) or random (PC 4 and 5; Section 3.4). The predicted eclipse is shown as the red area centered around 0.5 phase.
Paper: Uniform Reanalysis of JWST MIRI 15 μm Exoplanet Eclipse Observations Using Frame-normalized Principal Component Analysis
Authors: Nicholas J. Connors, Christopher Monaghan, Björn Benneke, Lisa Dang
Figure caption: Eclipse depths from our reanalysis using the Erebus pipeline with FN-PCA and exponential fit detrending, compared to literature values. The joint fit FN-PCA result is shown by the blue dashed line with a 1σ confidence interval. Exact values used to make this plot are shown in Table 2. The FN-PCA analysis of TRAPPIST-1 c visit 4 (dashed error bar) uses a second-degree polynomial to model the stellar variation during the visit.