adsabs/AstroCLIMB huggingface dataset:
Paper: Spectropolarimetric Evolution Reveals Dual-axis Ejecta in the Atypical Magnetar-powered SN 2012au
Authors: Sabrina DeSoto, Jennifer L. Hoffman, G. Grant Williams, Christopher Bilinski, Douglas C. Leonard, Peter A. Milne, Christopher Pickens, Manisha Shrestha, Nathan Smith, Paul S. Smith
Figure caption: Day 295 polarization regions in velocity space near the rest wavelengths of major spectral lines (Section 6.4). The flux spectrum for each region is plotted in gray, while the corresponding region of each polarization spectrum is color coded and labeled by species. In each panel, the rest velocity of each line is plotted as a vertical dotted line color coded for that species, and p = 0 is shown as a horizontal dashed black line. The error-weighted mean values for three velocity regions defined in Section 6.4 are shown as black horizontal bars; these values are presented in Table 5. These data have not been continuum subtracted.
Paper: Spectropolarimetric Evolution Reveals Dual-axis Ejecta in the Atypical Magnetar-powered SN 2012au
Authors: Sabrina DeSoto, Jennifer L. Hoffman, G. Grant Williams, Christopher Bilinski, Douglas C. Leonard, Peter A. Milne, Christopher Pickens, Manisha Shrestha, Nathan Smith, Paul S. Smith
Figure caption: Polar plots showing the Fe II (left) and He I (right) line regions after continuum subtraction for days 0–7. For each line region, the PA (+180° for clarity of angle variation) is plotted as a function of blueshifted velocity (on the radial axes). Data are binned to 15 Å and represented by individual blocks; the angular width of each block is either 10° or the uncertainty in PA for that data point (whichever is larger for legibility). The continuum is represented by a gray wedge at the angle of the GCF slope (+180°) spanning the width of the calculated PA uncertainty and stretched over the whole velocity space. The black, dashed semicircle represents the photospheric velocity, measured by the shift of the Fe II flux absorption minimum from rest (Section 3.2).
Paper: Spectropolarimetric Evolution Reveals Dual-axis Ejecta in the Atypical Magnetar-powered SN 2012au
Authors: Sabrina DeSoto, Jennifer L. Hoffman, G. Grant Williams, Christopher Bilinski, Douglas C. Leonard, Peter A. Milne, Christopher Pickens, Manisha Shrestha, Nathan Smith, Paul S. Smith
Figure caption: The same error-weighted mean polarization values shown for the transitional-nebular line regions in Figure 9 and tabulated in Table 5, now displayed in q−u space. Blue, white, and red points represent the blue wing (–15,000 to –5000 km s−1), central region (–5000 to +5000 km s−1), and red wing (+5000 to +15,000 km s−1) values, respectively. The GCF slopes for days 0–7 and day 295 are plotted as gray- and black-dotted lines, respectively; the Serkowski-reddening maximum ISP estimate is displayed as a red circle. These data have not been continuum subtracted.
Paper: Spectropolarimetric Evolution Reveals Dual-axis Ejecta in the Atypical Magnetar-powered SN 2012au
Authors: Sabrina DeSoto, Jennifer L. Hoffman, G. Grant Williams, Christopher Bilinski, Douglas C. Leonard, Peter A. Milne, Christopher Pickens, Manisha Shrestha, Nathan Smith, Paul S. Smith
Figure caption: Comparison of polarization measurements by line species (or continuum) and day post-R-band maximum for all Type Ib SNe SP data published thus far. Values shown are quoted in Table 6 with citations. Each SN is specified by a different color and marker style. In many cases, the level of uncertainty is indistinguishable on the points plotted, so measurements with unknown uncertainties are displayed as lighter colored points.
Paper: Discovery of a Little Red Dot Candidate at z ≳ 10 in COSMOS-web Based on MIRI-NIRCam Selection
Authors: Takumi S. Tanaka, Hollis B. Akins, Yuichi Harikane, John D. Silverman, Caitlin M. Casey, Kohei Inayoshi, Jan-Torge Schindler, Kazuhiro Shimasaku, Dale D. Kocevski, Masafusa Onoue, Andreas L. Faisst, Brant E. Robertson, Vasily Kokorev, Marko Shuntov, Anton M. Koekemoer, Maximilien Franco, Eiichi Egami, Daizhong Liu, Anthony J. Taylor, Jeyhan S. Kartaltepe, Sarah E. I. Bosman, Jaclyn B. Champagne, Koki Kakiichi, Santosh Harish, Zijian Zhang, Sophie L. Newman, Darshan Kakkad, Qinyue Fei, Seiji Fujimoto, Mingyu Li, Steven L. Finkelstein, Zi-Jian Li, Erini Lambrides, Laura Sommovigo, Jorge A. Zavala, Kei Ito, Zhaoxuan Liu, Ezequiel Treister, Manuel Aravena, Ghassem Gozaliasl, Haowen Zhang, Hossein Hatamnia, Hiroya Umeda, Akio K. Inoue, Jinyi Yang, Makoto Ando, Junya Arita, Xuheng Ding, Suin Matsui, Yuki Shibanuma, Georgios Magdis, Mingyang Zhuang, Xiaohui Fan, Zihao Li, Weizhe Liu, Jianwei Lyu, Jason Rhodes, Sune Toft, Feige Wang, Siwei Zou, Rafael C. Arango-Toro, Andrew J. Battisti, Steven Gillman, Ali Ahmad Khostovan, Arianna S. Long, Bahram Mobasher, David B. Sanders
Figure caption: Color–color diagrams based on the LRD model SEDs from H. B. Akins et al. (2024; red lines). The left and right panels show mF115W − mF150W versus mF150W − mF277W and mF277W − mF444W versus mF444W − mF770W, respectively. The red filled region defined by 0 < mF277W − mF444W < 2.25 and 1.5 < mF444W − mF770W can effectively distinguish z ∼ 10 LRDs from other objects. The selected candidate in this study, CW-LRD-z10, is highlighted with a red star with error bars. Note that mF115W − mF150W color for CW-LRD-z10 is a 2σ lower limit. CW-LRD-z10 also passes the color criteria for F115W dropouts (Y. Harikane et al. 2023b) shown by the gray shaded region in the left panel. Model galaxy SEDs generated using FSPS (C. Conroy et al. 2009; C. Conroy & J. E. Gunn 2010) with various star formation histories and dust attenuation values at z = 0–10 are shown in gray solid lines. Of these, we highlight two cases: (1) a stellar-origin Balmer break (with an fν ratio of ∼2) and AV = 0.5 (green), and (2) a dusty star-forming galaxy (SFG) model with AV = 5 (cyan). Seed BH models from K. Inayoshi et al. (2022) at z = 8–14 and LRDs with an extremely strong Balmer break at z = 9–15, assuming the spectrum of The Cliff in A. de Graaff et al. (2025), are shown in black and orange, respectively. For these model SEDs, dots are placed at redshift intervals of Δz = 1. Specifically, z = 10 Balmer break galaxy, z = 10 seed BH, z = 2.5 galaxy with stellar-origin Balmer break, and z = 0.2 dusty SFG are shown in green triangle, black triangle, green hexagon, and cyan hexagon, respectively. Photometrically selected LRDs from H. B. Akins et al. (2024) with a signal-to-noise ratio (S/N) > 3 are shown as orange diamonds; among them are two objects that pass our color selection (red diamonds). Dwarf stars and main-sequence stars from the BT-Settl model (F. Allard et al. 2012) are plotted in magenta crosses and pentagons, respectively.
Paper: Discovery of a Little Red Dot Candidate at z ≳ 10 in COSMOS-web Based on MIRI-NIRCam Selection
Authors: Takumi S. Tanaka, Hollis B. Akins, Yuichi Harikane, John D. Silverman, Caitlin M. Casey, Kohei Inayoshi, Jan-Torge Schindler, Kazuhiro Shimasaku, Dale D. Kocevski, Masafusa Onoue, Andreas L. Faisst, Brant E. Robertson, Vasily Kokorev, Marko Shuntov, Anton M. Koekemoer, Maximilien Franco, Eiichi Egami, Daizhong Liu, Anthony J. Taylor, Jeyhan S. Kartaltepe, Sarah E. I. Bosman, Jaclyn B. Champagne, Koki Kakiichi, Santosh Harish, Zijian Zhang, Sophie L. Newman, Darshan Kakkad, Qinyue Fei, Seiji Fujimoto, Mingyu Li, Steven L. Finkelstein, Zi-Jian Li, Erini Lambrides, Laura Sommovigo, Jorge A. Zavala, Kei Ito, Zhaoxuan Liu, Ezequiel Treister, Manuel Aravena, Ghassem Gozaliasl, Haowen Zhang, Hossein Hatamnia, Hiroya Umeda, Akio K. Inoue, Jinyi Yang, Makoto Ando, Junya Arita, Xuheng Ding, Suin Matsui, Yuki Shibanuma, Georgios Magdis, Mingyang Zhuang, Xiaohui Fan, Zihao Li, Weizhe Liu, Jianwei Lyu, Jason Rhodes, Sune Toft, Feige Wang, Siwei Zou, Rafael C. Arango-Toro, Andrew J. Battisti, Steven Gillman, Ali Ahmad Khostovan, Arianna S. Long, Bahram Mobasher, David B. Sanders
Figure caption: Model spectral energy distribution (SED) of a z = 10 LRD with MUV = −20 (red) and 5σ depth for point sources in COSMOS-Web (F115W, F150W, F277W, F444W, and F770W) from C. M. Casey et al. (2023) and in COSMOS-3D (F115W, F200W, F356W, and F1000W) shown in gray and gold rectangles, respectively. Model SEDs of potential contaminants of the z ∼ 10 LRD photometric selection, a z = 10 galaxy with a stellar-origin Balmer break with AV = 0.5 and M* = 1.5 × 1010 M⊙, are overlaid. The LRD model SED is from H. B. Akins et al. (2024), and the galaxy SED is generated using FSPS (C. Conroy et al. 2009; C. Conroy & J. E. Gunn 2010). The predicted model photometry is shown with diamonds for the LRD and squares for the galaxy. MIRI photometry is essential to distinguish between z ∼ 10 LRDs and z ∼ 10 galaxies with stellar-origin Balmer break.
Paper: Spectropolarimetric Evolution Reveals Dual-axis Ejecta in the Atypical Magnetar-powered SN 2012au
Authors: Sabrina DeSoto, Jennifer L. Hoffman, G. Grant Williams, Christopher Bilinski, Douglas C. Leonard, Peter A. Milne, Christopher Pickens, Manisha Shrestha, Nathan Smith, Paul S. Smith
Figure caption: Serkowski curves for a representative sample of the parameters we explored. Each panel contains a Milky Way curve (blue solid line), a host galaxy curve (orange solid line), a “raw” combined curve (MW + host; black-dotted line), and a “fit” curve constructed from the P﹩{}_{{\rm{\max }}}﹩ and ﹩{\lambda }_{{\rm{\max }}}﹩ values of the raw curve (red-dashed line), as well as the corresponding KS statistic for each set of curves (see Appendix B for details). The peak polarization value for each curve is denoted by a round point in the respective color.
Paper: Discovery of a Little Red Dot Candidate at z ≳ 10 in COSMOS-web Based on MIRI-NIRCam Selection
Authors: Takumi S. Tanaka, Hollis B. Akins, Yuichi Harikane, John D. Silverman, Caitlin M. Casey, Kohei Inayoshi, Jan-Torge Schindler, Kazuhiro Shimasaku, Dale D. Kocevski, Masafusa Onoue, Andreas L. Faisst, Brant E. Robertson, Vasily Kokorev, Marko Shuntov, Anton M. Koekemoer, Maximilien Franco, Eiichi Egami, Daizhong Liu, Anthony J. Taylor, Jeyhan S. Kartaltepe, Sarah E. I. Bosman, Jaclyn B. Champagne, Koki Kakiichi, Santosh Harish, Zijian Zhang, Sophie L. Newman, Darshan Kakkad, Qinyue Fei, Seiji Fujimoto, Mingyu Li, Steven L. Finkelstein, Zi-Jian Li, Erini Lambrides, Laura Sommovigo, Jorge A. Zavala, Kei Ito, Zhaoxuan Liu, Ezequiel Treister, Manuel Aravena, Ghassem Gozaliasl, Haowen Zhang, Hossein Hatamnia, Hiroya Umeda, Akio K. Inoue, Jinyi Yang, Makoto Ando, Junya Arita, Xuheng Ding, Suin Matsui, Yuki Shibanuma, Georgios Magdis, Mingyang Zhuang, Xiaohui Fan, Zihao Li, Weizhe Liu, Jianwei Lyu, Jason Rhodes, Sune Toft, Feige Wang, Siwei Zou, Rafael C. Arango-Toro, Andrew J. Battisti, Steven Gillman, Ali Ahmad Khostovan, Arianna S. Long, Bahram Mobasher, David B. Sanders
Figure caption: Observed photometry and SED fitting results using BAGPIPES. In the left panel, black open circles, small dots, and lines represent the observed photometry, the model photometry, and the model SEDs. The estimated zphoto and corresponding χ2 value for each fit are indicated in the lower-right corner. The right panel shows the χ2 distribution as a function of redshift. Red, cyan, and green lines indicate fits using the LRD model from H. B. Akins et al. (2024) over 0 < z < 15, the galaxy model over 0 < z < 2, and the galaxy model over 2 < z < 15, respectively.
Paper: Discovery of a Little Red Dot Candidate at z ≳ 10 in COSMOS-web Based on MIRI-NIRCam Selection
Authors: Takumi S. Tanaka, Hollis B. Akins, Yuichi Harikane, John D. Silverman, Caitlin M. Casey, Kohei Inayoshi, Jan-Torge Schindler, Kazuhiro Shimasaku, Dale D. Kocevski, Masafusa Onoue, Andreas L. Faisst, Brant E. Robertson, Vasily Kokorev, Marko Shuntov, Anton M. Koekemoer, Maximilien Franco, Eiichi Egami, Daizhong Liu, Anthony J. Taylor, Jeyhan S. Kartaltepe, Sarah E. I. Bosman, Jaclyn B. Champagne, Koki Kakiichi, Santosh Harish, Zijian Zhang, Sophie L. Newman, Darshan Kakkad, Qinyue Fei, Seiji Fujimoto, Mingyu Li, Steven L. Finkelstein, Zi-Jian Li, Erini Lambrides, Laura Sommovigo, Jorge A. Zavala, Kei Ito, Zhaoxuan Liu, Ezequiel Treister, Manuel Aravena, Ghassem Gozaliasl, Haowen Zhang, Hossein Hatamnia, Hiroya Umeda, Akio K. Inoue, Jinyi Yang, Makoto Ando, Junya Arita, Xuheng Ding, Suin Matsui, Yuki Shibanuma, Georgios Magdis, Mingyang Zhuang, Xiaohui Fan, Zihao Li, Weizhe Liu, Jianwei Lyu, Jason Rhodes, Sune Toft, Feige Wang, Siwei Zou, Rafael C. Arango-Toro, Andrew J. Battisti, Steven Gillman, Ali Ahmad Khostovan, Arianna S. Long, Bahram Mobasher, David B. Sanders
Figure caption: Upper panels: HST + JWST 3″ × 3″ cutout images centered on CW-LRD-z10. Each image is scaled by a noise map. If detected, the S/N measured from forced photometry is shown in the top-left corner. Lower panels: observed SED of CW-LRD-z10. For F606W, F814W, F115W, F1000W, and F2100W, we plot the 2σ upper limits. The red line indicates the best-fit LRD model SED from the SED fitting analysis (Section 4.2)
Paper: Spectropolarimetric Evolution Reveals Dual-axis Ejecta in the Atypical Magnetar-powered SN 2012au
Authors: Sabrina DeSoto, Jennifer L. Hoffman, G. Grant Williams, Christopher Bilinski, Douglas C. Leonard, Peter A. Milne, Christopher Pickens, Manisha Shrestha, Nathan Smith, Paul S. Smith
Figure caption: Occurrences of values of the KS statistic for the tested parameter space. Regions corresponding to the “true fit” and “poor fit” categories (based on the KS statistic; Appendix B) are filled with gray dots and hashes, respectively. The categories “good fit” and “questionable fit” both span the middle unfilled region. The average KS statistic is shown as a black vertical line with the value labeled.
Paper: Spectropolarimetric Evolution Reveals Dual-axis Ejecta in the Atypical Magnetar-powered SN 2012au
Authors: Sabrina DeSoto, Jennifer L. Hoffman, G. Grant Williams, Christopher Bilinski, Douglas C. Leonard, Peter A. Milne, Christopher Pickens, Manisha Shrestha, Nathan Smith, Paul S. Smith
Figure caption: KS statistic mapped by the difference in p﹩{}_{{\rm{\max }}}﹩ and ﹩{\lambda }_{{\rm{\max }}}﹩ values between the MW and host galaxy.
Paper: Spectropolarimetric Evolution Reveals Dual-axis Ejecta in the Atypical Magnetar-powered SN 2012au
Authors: Sabrina DeSoto, Jennifer L. Hoffman, G. Grant Williams, Christopher Bilinski, Douglas C. Leonard, Peter A. Milne, Christopher Pickens, Manisha Shrestha, Nathan Smith, Paul S. Smith
Figure caption: KS statistic mapped by the difference in θ and ﹩{\lambda }_{{\rm{\max }}}﹩ values between the MW and host galaxy.
Paper: Discovery of a Little Red Dot Candidate at z ≳ 10 in COSMOS-web Based on MIRI-NIRCam Selection
Authors: Takumi S. Tanaka, Hollis B. Akins, Yuichi Harikane, John D. Silverman, Caitlin M. Casey, Kohei Inayoshi, Jan-Torge Schindler, Kazuhiro Shimasaku, Dale D. Kocevski, Masafusa Onoue, Andreas L. Faisst, Brant E. Robertson, Vasily Kokorev, Marko Shuntov, Anton M. Koekemoer, Maximilien Franco, Eiichi Egami, Daizhong Liu, Anthony J. Taylor, Jeyhan S. Kartaltepe, Sarah E. I. Bosman, Jaclyn B. Champagne, Koki Kakiichi, Santosh Harish, Zijian Zhang, Sophie L. Newman, Darshan Kakkad, Qinyue Fei, Seiji Fujimoto, Mingyu Li, Steven L. Finkelstein, Zi-Jian Li, Erini Lambrides, Laura Sommovigo, Jorge A. Zavala, Kei Ito, Zhaoxuan Liu, Ezequiel Treister, Manuel Aravena, Ghassem Gozaliasl, Haowen Zhang, Hossein Hatamnia, Hiroya Umeda, Akio K. Inoue, Jinyi Yang, Makoto Ando, Junya Arita, Xuheng Ding, Suin Matsui, Yuki Shibanuma, Georgios Magdis, Mingyang Zhuang, Xiaohui Fan, Zihao Li, Weizhe Liu, Jianwei Lyu, Jason Rhodes, Sune Toft, Feige Wang, Siwei Zou, Rafael C. Arango-Toro, Andrew J. Battisti, Steven Gillman, Ali Ahmad Khostovan, Arianna S. Long, Bahram Mobasher, David B. Sanders
Figure caption: Redshift evolution of the LRD fraction relative to the overall galaxy population at MUV =  −20. Symbols for lower-redshift LRDs (V. Kokorev et al. 2024a; J. Matthee et al. 2024; D. D. Kocevski et al. 2025; Y. Ma et al. 2025b; M.-Y. Zhuang et al. 2025) are the same as in Figure 6 (left panel). The red solid line shows the best-fit linear model. The red dashed and dotted lines indicate the modeled fLRD redshift evolution that combines the evolutions of the UV luminosity function of LRDs (the fitted log-normal distribution shown in Figure 7) and galaxies from R. J. Bouwens et al. (2021) and M. Franco et al. (2025b), respectively. For each model, the black line indicates the extrapolation of each luminosity function evolution beyond the range constrained by observational data. The blue dashed line indicates 0.3 times Salpeter time (τSalpeter, with the assumption of ε = 0.1) divided by the age of the Universe (tUniv) at each redshift. The blue dotted line represents the prediction from F. Pacucci & A. Loeb (2025). The gray dashed line and shaded region indicate the fitted peak redshift of the log-normal distribution (z0).
Paper: Discovery of a Little Red Dot Candidate at z ≳ 10 in COSMOS-web Based on MIRI-NIRCam Selection
Authors: Takumi S. Tanaka, Hollis B. Akins, Yuichi Harikane, John D. Silverman, Caitlin M. Casey, Kohei Inayoshi, Jan-Torge Schindler, Kazuhiro Shimasaku, Dale D. Kocevski, Masafusa Onoue, Andreas L. Faisst, Brant E. Robertson, Vasily Kokorev, Marko Shuntov, Anton M. Koekemoer, Maximilien Franco, Eiichi Egami, Daizhong Liu, Anthony J. Taylor, Jeyhan S. Kartaltepe, Sarah E. I. Bosman, Jaclyn B. Champagne, Koki Kakiichi, Santosh Harish, Zijian Zhang, Sophie L. Newman, Darshan Kakkad, Qinyue Fei, Seiji Fujimoto, Mingyu Li, Steven L. Finkelstein, Zi-Jian Li, Erini Lambrides, Laura Sommovigo, Jorge A. Zavala, Kei Ito, Zhaoxuan Liu, Ezequiel Treister, Manuel Aravena, Ghassem Gozaliasl, Haowen Zhang, Hossein Hatamnia, Hiroya Umeda, Akio K. Inoue, Jinyi Yang, Makoto Ando, Junya Arita, Xuheng Ding, Suin Matsui, Yuki Shibanuma, Georgios Magdis, Mingyang Zhuang, Xiaohui Fan, Zihao Li, Weizhe Liu, Jianwei Lyu, Jason Rhodes, Sune Toft, Feige Wang, Siwei Zou, Rafael C. Arango-Toro, Andrew J. Battisti, Steven Gillman, Ali Ahmad Khostovan, Arianna S. Long, Bahram Mobasher, David B. Sanders
Figure caption: Luminosity function of z ∼ 10 LRDs shown by the red star data point. Left panel: comparison with the luminosity functions of LRDs at lower redshifts (1.7 < z < 8.5) from previous studies (V. Kokorev et al. 2024a; J. Matthee et al. 2024; D. D. Kocevski et al. 2025; Y. Ma et al. 2025b). Note that the lower limit at MUV = −18.2 and 9 < z < 12 is based on the assumption that only CAPERS-LRD-z9 (A. J. Taylor et al. 2025b) is a true z ∼ 10 LRD in the selection by D. D. Kocevski et al. (2025), independently identified of the selection in this study. Right panel: comparison of the LRD luminosity function with that of galaxies at z ∼ 10 (R. Bouwens et al. 2023; C. T. Donnan et al. 2023; Y. Harikane et al. 2023b; P. G. Pérez-González et al. 2023; C. M. Casey et al. 2024; M. Franco et al. 2024, 2025b). The best-fit double power-law model from Y. Harikane et al. (2025) is indicated by the black line.
Paper: Discovery of a Little Red Dot Candidate at z ≳ 10 in COSMOS-web Based on MIRI-NIRCam Selection
Authors: Takumi S. Tanaka, Hollis B. Akins, Yuichi Harikane, John D. Silverman, Caitlin M. Casey, Kohei Inayoshi, Jan-Torge Schindler, Kazuhiro Shimasaku, Dale D. Kocevski, Masafusa Onoue, Andreas L. Faisst, Brant E. Robertson, Vasily Kokorev, Marko Shuntov, Anton M. Koekemoer, Maximilien Franco, Eiichi Egami, Daizhong Liu, Anthony J. Taylor, Jeyhan S. Kartaltepe, Sarah E. I. Bosman, Jaclyn B. Champagne, Koki Kakiichi, Santosh Harish, Zijian Zhang, Sophie L. Newman, Darshan Kakkad, Qinyue Fei, Seiji Fujimoto, Mingyu Li, Steven L. Finkelstein, Zi-Jian Li, Erini Lambrides, Laura Sommovigo, Jorge A. Zavala, Kei Ito, Zhaoxuan Liu, Ezequiel Treister, Manuel Aravena, Ghassem Gozaliasl, Haowen Zhang, Hossein Hatamnia, Hiroya Umeda, Akio K. Inoue, Jinyi Yang, Makoto Ando, Junya Arita, Xuheng Ding, Suin Matsui, Yuki Shibanuma, Georgios Magdis, Mingyang Zhuang, Xiaohui Fan, Zihao Li, Weizhe Liu, Jianwei Lyu, Jason Rhodes, Sune Toft, Feige Wang, Siwei Zou, Rafael C. Arango-Toro, Andrew J. Battisti, Steven Gillman, Ali Ahmad Khostovan, Arianna S. Long, Bahram Mobasher, David B. Sanders
Figure caption: Redshift evolution of the luminosity function at MUV =  −20. Symbols for lower-redshift LRDs (V. Kokorev et al. 2024a; J. Matthee et al. 2024; D. D. Kocevski et al. 2025; Y. Ma et al. 2025b; M.-Y. Zhuang et al. 2025) are the same as in Figure 6 (left panel). The red dotted line indicates the best-fit log-normal distribution. The gray dashed line and shaded region indicate the best-fit peak redshift (z0). The blue line and cyan shaded region indicate the AGN luminosity function at MUV =  −20 from the X-rays (Y. Ueda et al. 2014) and model prediction (W. Li et al. 2024). Note that we assume an X-ray-UV luminosity ratio (E. Lusso & G. Risaliti 2016) and a photon index of Γ = 1.9 to convert the X-ray (Y. Ueda et al. 2014) to UV luminosity function.
Paper: Discovery of a Little Red Dot Candidate at z ≳ 10 in COSMOS-web Based on MIRI-NIRCam Selection
Authors: Takumi S. Tanaka, Hollis B. Akins, Yuichi Harikane, John D. Silverman, Caitlin M. Casey, Kohei Inayoshi, Jan-Torge Schindler, Kazuhiro Shimasaku, Dale D. Kocevski, Masafusa Onoue, Andreas L. Faisst, Brant E. Robertson, Vasily Kokorev, Marko Shuntov, Anton M. Koekemoer, Maximilien Franco, Eiichi Egami, Daizhong Liu, Anthony J. Taylor, Jeyhan S. Kartaltepe, Sarah E. I. Bosman, Jaclyn B. Champagne, Koki Kakiichi, Santosh Harish, Zijian Zhang, Sophie L. Newman, Darshan Kakkad, Qinyue Fei, Seiji Fujimoto, Mingyu Li, Steven L. Finkelstein, Zi-Jian Li, Erini Lambrides, Laura Sommovigo, Jorge A. Zavala, Kei Ito, Zhaoxuan Liu, Ezequiel Treister, Manuel Aravena, Ghassem Gozaliasl, Haowen Zhang, Hossein Hatamnia, Hiroya Umeda, Akio K. Inoue, Jinyi Yang, Makoto Ando, Junya Arita, Xuheng Ding, Suin Matsui, Yuki Shibanuma, Georgios Magdis, Mingyang Zhuang, Xiaohui Fan, Zihao Li, Weizhe Liu, Jianwei Lyu, Jason Rhodes, Sune Toft, Feige Wang, Siwei Zou, Rafael C. Arango-Toro, Andrew J. Battisti, Steven Gillman, Ali Ahmad Khostovan, Arianna S. Long, Bahram Mobasher, David B. Sanders
Figure caption: Spectrum of JADES-67592 (zspec = 9.65) downloaded from DJA. The upper and lower panels show the overall four-times binned PRISM spectra (R ∼ 25) and the zoomed-in original (R ∼ 100) spectra around Hβ + [O III]λλ4959, 5007. The wavelengths of Lyα, Balmer limit, Hβ, and [O III]λλ4959, 5007 are shown in red vertical lines.
Paper: Discovery of a Little Red Dot Candidate at z ≳ 10 in COSMOS-web Based on MIRI-NIRCam Selection
Authors: Takumi S. Tanaka, Hollis B. Akins, Yuichi Harikane, John D. Silverman, Caitlin M. Casey, Kohei Inayoshi, Jan-Torge Schindler, Kazuhiro Shimasaku, Dale D. Kocevski, Masafusa Onoue, Andreas L. Faisst, Brant E. Robertson, Vasily Kokorev, Marko Shuntov, Anton M. Koekemoer, Maximilien Franco, Eiichi Egami, Daizhong Liu, Anthony J. Taylor, Jeyhan S. Kartaltepe, Sarah E. I. Bosman, Jaclyn B. Champagne, Koki Kakiichi, Santosh Harish, Zijian Zhang, Sophie L. Newman, Darshan Kakkad, Qinyue Fei, Seiji Fujimoto, Mingyu Li, Steven L. Finkelstein, Zi-Jian Li, Erini Lambrides, Laura Sommovigo, Jorge A. Zavala, Kei Ito, Zhaoxuan Liu, Ezequiel Treister, Manuel Aravena, Ghassem Gozaliasl, Haowen Zhang, Hossein Hatamnia, Hiroya Umeda, Akio K. Inoue, Jinyi Yang, Makoto Ando, Junya Arita, Xuheng Ding, Suin Matsui, Yuki Shibanuma, Georgios Magdis, Mingyang Zhuang, Xiaohui Fan, Zihao Li, Weizhe Liu, Jianwei Lyu, Jason Rhodes, Sune Toft, Feige Wang, Siwei Zou, Rafael C. Arango-Toro, Andrew J. Battisti, Steven Gillman, Ali Ahmad Khostovan, Arianna S. Long, Bahram Mobasher, David B. Sanders
Figure caption: Same as Figure 4 but for the results with EAZY. Red, cyan, and green correspond to fits using the sorted_agn_blue_sfhz_13 template over 0 < z < 15, the tweak_fsps_QSF_12_v3 template over 0 < z < 2, and the tweak_fsps_QSF_12_v3 template over 2 < z < 15, respectively.