adsabs/AstroCLIMB huggingface dataset:
Paper: Ryugu’s Anhydrous Ingredients and Their Spectral Link to Primitive Dust from the Outer Solar System
Authors: R. Brunetto, C. Lantz, Y. Fukuda, A. Aléon-Toppani, T. Nakamura, Z. Dionnet, D. Baklouti, F. Borondics, Z. Djouadi, S. Rubino, K. Amano, M. Matsumoto, Y. Fujioka, T. Morita, M. Kukuiri, E. Kagawa, M. Matsuoka, R. Milliken, H. Yurimoto, T. Noguchi, R. Okazaki, H. Yabuta, H. Naraoka, K. Sakamoto, S. Tachibana, T. Yada, M. Nishimura, A. Nakato, A. Miyazaki, K. Yogata, M. Abe, T. Okada, T. Usui, M. Yoshikawa, T. Saiki, S. Tanaka, F. Terui, S. Nakazawa, S. Watanabe, Y. Tsuda
Figure caption: IR maps for four ROIs containing clasts 1–5 in C0002 (see their locations in Figure 1). The four chosen ROIs are piled up for a quick visualization, and also for treating them as a unique and consistent data set. First column (left): zoomed BSE images. Second: the reflectance at 1120 cm−1 (R), 910 cm−1 (G), and 880 cm−1 (B), chosen to highlight the differences between typical anhydrous and hydrated phases (see Figure 1 for a complete map). Third: results of a PCA (R = PC1, G = PC2, and B = PC3) of the spectra around the 10 μm feature. Fourth: map of the peak position of the main Reststrahlen feature (the strongest band in each spectrum). Blue pixels are grains dominated by anhydrous phases, while yellow grains are mainly carbonates. Fifth: a selection of pixels of the anhydrous grains, whose average spectra are reported in the sixth column (right). One of them is highlighted as an amorphous-rich grain. The anhydrous grains represent less than 5% of the chosen ROIs, which means they are even less abundant with respect to the total volume of C0002.
Paper: Millimeter Observations of the Type II SN 2023ixf: Constraints on the Proximate Circumstellar Medium
Authors: Edo Berger, Garrett K. Keating, Raffaella Margutti, Keiichi Maeda, Kate D. Alexander, Yvette Cendes, Tarraneh Eftekhari, Mark Gurwell, Daichi Hiramatsu, Anna Y. Q. Ho, Tanmoy Laskar, Ramprasad Rao, Peter K. G. Williams
Figure caption: The phase space of progenitor mass-loss rate vs. ejecta velocity that is excluded by our most constraining SMA limits at 2.7, 7.7, and 18.6 days. The models (Chevalier 1998) assume v  w  = 115 km s−1 (Smith et al. 2023) and are shown for two sets of equipartition parameters (ϵ  e  and ϵ  B ), an electron power-law distribution with ﹩{N}_{e}({\gamma }_{e})\propto {\gamma }_{e}^{-p}﹩ with p = 3, a volume filling factor of 0.5, and two values for the electron temperature (T  e ). The vertical gray shaded region indicates an ejecta velocity range of v ej = (1 − 2) × 104 km s−1. The blue dot marks the value of ﹩\dot{M}﹩ inferred from X-ray observations acquired at ≲11 days (Grefenstette et al. 2023), while the horizontal blue dotted–dashed line marks the value of ﹩\dot{M}﹩ inferred from optical spectra at ≲14 days (Jacobson-Galan et al. 2023). Both values have been updated to v  w  = 115 km s−1.
Paper: Ryugu’s Anhydrous Ingredients and Their Spectral Link to Primitive Dust from the Outer Solar System
Authors: R. Brunetto, C. Lantz, Y. Fukuda, A. Aléon-Toppani, T. Nakamura, Z. Dionnet, D. Baklouti, F. Borondics, Z. Djouadi, S. Rubino, K. Amano, M. Matsumoto, Y. Fujioka, T. Morita, M. Kukuiri, E. Kagawa, M. Matsuoka, R. Milliken, H. Yurimoto, T. Noguchi, R. Okazaki, H. Yabuta, H. Naraoka, K. Sakamoto, S. Tachibana, T. Yada, M. Nishimura, A. Nakato, A. Miyazaki, K. Yogata, M. Abe, T. Okada, T. Usui, M. Yoshikawa, T. Saiki, S. Tanaka, F. Terui, S. Nakazawa, S. Watanabe, Y. Tsuda
Figure caption: Top: optical image of a pFIB section of A0026. Bottom: IR map (pixel size 3.3 μm, 3 × 2 tiles with an imperfect joining of the upper and lower tiles) using the same color code and the scale of reflectance as C0002 in Figure 1. The major lithology (the matrix rich in phyllosilicates is shown in green, plus abundant carbonates in blue and iron sulfides and magnetite in red and pink, respectively) dominates A0026, but different from C0002 there is no detection of clasts rich in anhydrous phases.
Paper: Millimeter Observations of the Type II SN 2023ixf: Constraints on the Proximate Circumstellar Medium
Authors: Edo Berger, Garrett K. Keating, Raffaella Margutti, Keiichi Maeda, Kate D. Alexander, Yvette Cendes, Tarraneh Eftekhari, Mark Gurwell, Daichi Hiramatsu, Anna Y. Q. Ho, Tanmoy Laskar, Ramprasad Rao, Peter K. G. Williams
Figure caption: Model light curves at 230 GHz (lines) using the formalism of Maeda et al. (2021) and Maeda et al. (2023) for several choices of the mass-loss rate and for two sets of equipartition parameters: ϵ  e  = ϵ  B  = 0.1 (left) and ϵ e = 0.04 and ϵ B = 0.02 (right; calibrated with models for SN 2020oi: Maeda et al. 2023). The triangles are the upper limits for SN 2023ixf.
Paper: Millimeter Observations of the Type II SN 2023ixf: Constraints on the Proximate Circumstellar Medium
Authors: Edo Berger, Garrett K. Keating, Raffaella Margutti, Keiichi Maeda, Kate D. Alexander, Yvette Cendes, Tarraneh Eftekhari, Mark Gurwell, Daichi Hiramatsu, Anna Y. Q. Ho, Tanmoy Laskar, Ramprasad Rao, Peter K. G. Williams
Figure caption: SMA 230 GHz upper limits for SN 2023ixf (black triangles; 3σ) compared to the existing sample of CCSNe with early millimeter-band detections (squares: Type II; circles: Type Ib/c; Weiler et al. 2007; Soderberg et al. 2008; Gorosabel et al. 2010; Chakraborti et al. 2013; Horesh et al. 2013a, 2013b; Zauderer et al. 2013b, 2014; Maeda et al. 2021), or upper limits (triangles; Carpenter 2010; Horesh et al. 2012b, 2012a; Zauderer et al. 2013a); we particularly highlight the nondetection of the Type IIP SN 2012A.
Paper: Millimeter Observations of the Type II SN 2023ixf: Constraints on the Proximate Circumstellar Medium
Authors: Edo Berger, Garrett K. Keating, Raffaella Margutti, Keiichi Maeda, Kate D. Alexander, Yvette Cendes, Tarraneh Eftekhari, Mark Gurwell, Daichi Hiramatsu, Anna Y. Q. Ho, Tanmoy Laskar, Ramprasad Rao, Peter K. G. Williams
Figure caption: Map from the aggregate SMA data from all six epochs of observations, of the region around SN 2023ixf (white cross) overlaid on a false-color Hubble Space Telescope image, with the synthesized beam shown in the lower left (white ellipse). We show contours of the 230 GHz (1.3 mm) continuum emission in red, and the CO(2–1) line emission in cyan. Continuum contours correspond to 0.6, 0.9, 1.2, and 1.5 mJy; CO(2–1) contours correspond to 2, 4, and 8 Jy  km  s−1 (uncorrected for primary beam effects). No continuum emission is detected at the position of SN 2023ixf, which is located near NGC 5461, an H II region at the southeastern edge of M101 (white box in inset).
Paper: Life beyond 30: Probing the −20 < M UV < −17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey
Authors: Pablo G. Pérez-González, Luca Costantin, Danial Langeroodi, Pierluigi Rinaldi, Marianna Annunziatella, Olivier Ilbert, Luis Colina, Hans Ulrik Nørgaard-Nielsen, Thomas R. Greve, Göran Östlin, Gillian Wright, Almudena Alonso-Herrero, Javier Álvarez-Márquez, Karina I. Caputi, Andreas Eckart, Olivier Le Fèvre, Álvaro Labiano, Macarena García-Marín, Jens Hjorth, Sarah Kendrew, John P. Pye, Tuomo Tikkanen, Paul van der Werf, Fabian Walter, Martin Ward, Arjan Bik, Leindert Boogaard, Sarah E. I. Bosman, Alejandro Crespo Gómez, Steven Gillman, Edoardo Iani, Iris Jermann, Jens Melinder, Romain A. Meyer, Thibaud Moutard, Ewine van Dishoek, Thomas Henning, Pierre-Olivier Lagage, Manuel Guedel, Florian Peissker, Tom Ray, Bart Vandenbussche, Ángela García-Argumánez, Rosa María Mérida
Figure caption: Evolution of the UV luminosity density, transformed into SFR density on the right vertical axis (assuming a Chabrier 2003 IMF). Our results are plotted with a red shaded region. Estimates from the literature are plotted with gray symbols (Oesch et al. 2018; Bouwens et al. 2023a, 2023b; Donnan et al. 2023; Harikane et al. 2023). The densities at z > 16 are shown in light gray since they were mostly based on a z ∼ 5 redshift interloper (Arrabal Haro et al. 2023a; Harikane et al. 2023). We also plot predictions from several galaxy formation simulations, listed in the following lines. The Illustris-1, TNG50, TNG100, TNG300 results are plotted with blue continuous, dashed, dotted, and dashed–dotted lines, respectively, all referring to SFRs measured in 0.″5 diameter apertures for M ⋆ > 107 M ⊙ galaxies, except for TNG300, cut at M ⋆ > 108 M ⊙. The thick dotted line refers to TNG100 results using whole-galaxy measurements (Vogelsberger et al. 2014; Nelson et al. 2015; Naiman et al. 2018; Marinacci et al. 2018; Nelson et al. 2018; Pillepich et al. 2018, 2019; Springel et al. 2018; Nelson et al. 2019). The EAGLE simulations (Schaye et al. 2015; Crain et al. 2015) are plotted in green for galaxy samples cut in stellar masses M ⋆ > 106,7,8 M ⊙ in continuous, dotted, dashed lines. The SIMBA predictions are shown with a brown continuous line for all galaxies, dashed line for F277W < 31 mag sources (Davé et al. 2019). The THESAN-1 and THESAN-SDAO-2 simulations (Kannan et al. 2022) are shown in magenta with continuous and dotted lines, respectively (see text for differences). The FLARES predictions are shown in cyan (Lovell et al. 2021; Vijayan et al. 2021). The UniverseMachine semiempirical model (Behroozi et al. 2020) is shown in orange with the same mass cuts and line styles mentioned for EAGLE. Finally, the models in Maio & Viel (2023) are shown in yellow, and the predictions from the Santa Cruz semianalytic models (Yung et al. 2019, 2020) are depicted in orchid.
Paper: Life beyond 30: Probing the −20 < M UV < −17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey
Authors: Pablo G. Pérez-González, Luca Costantin, Danial Langeroodi, Pierluigi Rinaldi, Marianna Annunziatella, Olivier Ilbert, Luis Colina, Hans Ulrik Nørgaard-Nielsen, Thomas R. Greve, Göran Östlin, Gillian Wright, Almudena Alonso-Herrero, Javier Álvarez-Márquez, Karina I. Caputi, Andreas Eckart, Olivier Le Fèvre, Álvaro Labiano, Macarena García-Marín, Jens Hjorth, Sarah Kendrew, John P. Pye, Tuomo Tikkanen, Paul van der Werf, Fabian Walter, Martin Ward, Arjan Bik, Leindert Boogaard, Sarah E. I. Bosman, Alejandro Crespo Gómez, Steven Gillman, Edoardo Iani, Iris Jermann, Jens Melinder, Romain A. Meyer, Thibaud Moutard, Ewine van Dishoek, Thomas Henning, Pierre-Olivier Lagage, Manuel Guedel, Florian Peissker, Tom Ray, Bart Vandenbussche, Ángela García-Argumánez, Rosa María Mérida
Figure caption: Magnitude in the NIRCam F277W filter vs. photometric redshift for z > 8 galaxies. General galaxy samples extracted from the catalogs released by G. Brammer for the SMACS0723, GLASS, and CEERS data sets gathered in 2022 are plotted with blue small dots to illustrate the magnitude limits of the surveys and the number of high-redshift galaxies in unsupervised and unvetted photometric catalogs. Our parent galaxy sample is plotted with red small dots, and the final sample of z > 8 galaxy candidates with red hexagons. We depict 1σ uncertainties plotted in both axes and the data point referring to the zPDF peak redshift. We also plot the photometric high-redshift galaxy candidates of Bouwens et al. (2023a), Naidu et al. (2022a), Harikane et al. (2023), Donnan et al. (2023), and Finkelstein et al. (2023) with large black circles (we do not remove repeated sources with different measurements), as well as spectroscopically confirmed galaxies from JADES (Curtis-Lake et al. 2023; Robertson et al. 2023), lensing clusters (Langeroodi et al. 2022; Roberts-Borsani et al. 2023; Williams et al. 2023; Carnall et al. 2023, not corrected for magnification), and CEERS sources (Arrabal Haro et al. 2023a, 2023b), all in green. The top panel shows the histogram of redshifts for these samples of high-redshift galaxy candidates. The right panel shows the magnitude distribution of the different data sets mentioned before, with the three 2022 surveys plotted with transparency. Our deeper data (peaking around 2 mag fainter than previous surveys) probe the 29–31 mag regime, providing candidates at the previously unexplored faint-end of the luminosity functions.
Paper: Life beyond 30: Probing the −20 < M UV < −17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey
Authors: Pablo G. Pérez-González, Luca Costantin, Danial Langeroodi, Pierluigi Rinaldi, Marianna Annunziatella, Olivier Ilbert, Luis Colina, Hans Ulrik Nørgaard-Nielsen, Thomas R. Greve, Göran Östlin, Gillian Wright, Almudena Alonso-Herrero, Javier Álvarez-Márquez, Karina I. Caputi, Andreas Eckart, Olivier Le Fèvre, Álvaro Labiano, Macarena García-Marín, Jens Hjorth, Sarah Kendrew, John P. Pye, Tuomo Tikkanen, Paul van der Werf, Fabian Walter, Martin Ward, Arjan Bik, Leindert Boogaard, Sarah E. I. Bosman, Alejandro Crespo Gómez, Steven Gillman, Edoardo Iani, Iris Jermann, Jens Melinder, Romain A. Meyer, Thibaud Moutard, Ewine van Dishoek, Thomas Henning, Pierre-Olivier Lagage, Manuel Guedel, Florian Peissker, Tom Ray, Bart Vandenbussche, Ángela García-Argumánez, Rosa María Mérida
Figure caption: From left to right, UV luminosity functions at z ∼ 9, z ∼ 11 and z ∼ 12. We plot our results with red hexagons (uncertainties smaller than data points in some cases, see Table 3), and compare with literature estimations from Bouwens et al. (2023a), Naidu et al. (2022a), Donnan et al. (2023), Finkelstein et al. (2023), Harikane et al. (2023), and Castellano et al. (2023). We fit all points (ours and those in the literature) to a Schechter (1976) function, which is plotted with red continuous lines in each panel, with the fits for other redshifts shown with dashed lines.
Paper: Life beyond 30: Probing the −20 < M UV < −17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey
Authors: Pablo G. Pérez-González, Luca Costantin, Danial Langeroodi, Pierluigi Rinaldi, Marianna Annunziatella, Olivier Ilbert, Luis Colina, Hans Ulrik Nørgaard-Nielsen, Thomas R. Greve, Göran Östlin, Gillian Wright, Almudena Alonso-Herrero, Javier Álvarez-Márquez, Karina I. Caputi, Andreas Eckart, Olivier Le Fèvre, Álvaro Labiano, Macarena García-Marín, Jens Hjorth, Sarah Kendrew, John P. Pye, Tuomo Tikkanen, Paul van der Werf, Fabian Walter, Martin Ward, Arjan Bik, Leindert Boogaard, Sarah E. I. Bosman, Alejandro Crespo Gómez, Steven Gillman, Edoardo Iani, Iris Jermann, Jens Melinder, Romain A. Meyer, Thibaud Moutard, Ewine van Dishoek, Thomas Henning, Pierre-Olivier Lagage, Manuel Guedel, Florian Peissker, Tom Ray, Bart Vandenbussche, Ángela García-Argumánez, Rosa María Mérida
Figure caption: Examples of F115W and F150W dropout galaxies in our sample. For each source, in the top left, we show the SED (for the 0.″3 diameter aperture; filled dots) and template fits to low- and high-redshift solutions. Arrows indicate 1σ upper limits. The top right panel shows the photometric redshift probability distribution function for the different codes used in this work and the derived redshift and uncertainties. The bottom of the figure for each source presents 1.″5 × 1.″5 postage stamps in ACS, WFC3, and NIRCam bands, with the source marked with a 0.″15 radius red circle.
Paper: Life beyond 30: Probing the −20 < M UV < −17 Luminosity Function at 8 < z < 13 with the NIRCam Parallel Field of the MIRI Deep Survey
Authors: Pablo G. Pérez-González, Luca Costantin, Danial Langeroodi, Pierluigi Rinaldi, Marianna Annunziatella, Olivier Ilbert, Luis Colina, Hans Ulrik Nørgaard-Nielsen, Thomas R. Greve, Göran Östlin, Gillian Wright, Almudena Alonso-Herrero, Javier Álvarez-Márquez, Karina I. Caputi, Andreas Eckart, Olivier Le Fèvre, Álvaro Labiano, Macarena García-Marín, Jens Hjorth, Sarah Kendrew, John P. Pye, Tuomo Tikkanen, Paul van der Werf, Fabian Walter, Martin Ward, Arjan Bik, Leindert Boogaard, Sarah E. I. Bosman, Alejandro Crespo Gómez, Steven Gillman, Edoardo Iani, Iris Jermann, Jens Melinder, Romain A. Meyer, Thibaud Moutard, Ewine van Dishoek, Thomas Henning, Pierre-Olivier Lagage, Manuel Guedel, Florian Peissker, Tom Ray, Bart Vandenbussche, Ángela García-Argumánez, Rosa María Mérida
Figure caption: Examples of F115W and F150W dropout galaxies in our sample; in this case, for sources fainter than F277W = 30 mag (distinctively probed by our data set). Same information as in Figure 1 given.
Paper: A SPectroscopic Survey of Biased Halos in the Reionization Era (ASPIRE): A First Look at the Rest-frame Optical Spectra of z > 6.5 Quasars Using JWST
Authors: Jinyi Yang, Feige Wang, Xiaohui Fan, Joseph F. Hennawi, Aaron J. Barth, Eduardo Bañados, Fengwu Sun, Weizhe Liu, Zheng Cai, Linhua Jiang, Zihao Li, Masafusa Onoue, Jan-Torge Schindler, Yue Shen, Yunjing Wu, Aklant K. Bhowmick, Rebekka Bieri, Laura Blecha, Sarah Bosman, Jaclyn B. Champagne, Luis Colina, Thomas Connor, Tiago Costa, Frederick B. Davies, Roberto Decarli, Gisella De Rosa, Alyssa B. Drake, Eiichi Egami, Anna-Christina Eilers, Analis E. Evans, Emanuele Paolo Farina, Melanie Habouzit, Zoltan Haiman, Xiangyu Jin, Hyunsung D. Jun, Koki Kakiichi, Yana Khusanova, Girish Kulkarni, Federica Loiacono, Alessandro Lupi, Chiara Mazzucchelli, Zhiwei Pan, Sofía Rojas-Ruiz, Michael A. Strauss, Wei Leong Tee, Benny Trakhtenbrot, Maxime Trebitsch, Bram Venemans, Marianne Vestergaard, Marta Volonteri, Fabian Walter, Zhang-Liang Xie, Minghao Yue, Haowen Zhang, Huanian Zhang, Siwei Zou
Figure caption: The JWST NIRCam WFSS F356W spectra of eight ASPIRE quasars (black line) with spectral uncertainty (gray), ordered by R.A. The red solid lines denote the best total fits. The best fits of different spectral components are shown with dashed and dotted lines. For each object, the left panel presents the entire spectrum with total fit, power-law continuum, and pseudocontinuum (i.e., power-law plus Fe II emission). The right panel shows the zoomed-in region of Hβ and [O III] lines. The systemic redshifts of the quasars are based on their [C II] line measurements from ALMA observations. The blue squares with error bars are the photometric data in the WISE W1 3.4 μm band. The panels below the spectra present the residuals (data model) of each best-fit model.
Paper: A SPectroscopic Survey of Biased Halos in the Reionization Era (ASPIRE): A First Look at the Rest-frame Optical Spectra of z > 6.5 Quasars Using JWST
Authors: Jinyi Yang, Feige Wang, Xiaohui Fan, Joseph F. Hennawi, Aaron J. Barth, Eduardo Bañados, Fengwu Sun, Weizhe Liu, Zheng Cai, Linhua Jiang, Zihao Li, Masafusa Onoue, Jan-Torge Schindler, Yue Shen, Yunjing Wu, Aklant K. Bhowmick, Rebekka Bieri, Laura Blecha, Sarah Bosman, Jaclyn B. Champagne, Luis Colina, Thomas Connor, Tiago Costa, Frederick B. Davies, Roberto Decarli, Gisella De Rosa, Alyssa B. Drake, Eiichi Egami, Anna-Christina Eilers, Analis E. Evans, Emanuele Paolo Farina, Melanie Habouzit, Zoltan Haiman, Xiangyu Jin, Hyunsung D. Jun, Koki Kakiichi, Yana Khusanova, Girish Kulkarni, Federica Loiacono, Alessandro Lupi, Chiara Mazzucchelli, Zhiwei Pan, Sofía Rojas-Ruiz, Michael A. Strauss, Wei Leong Tee, Benny Trakhtenbrot, Maxime Trebitsch, Bram Venemans, Marianne Vestergaard, Marta Volonteri, Fabian Walter, Zhang-Liang Xie, Minghao Yue, Haowen Zhang, Huanian Zhang, Siwei Zou
Figure caption: The [O III] 5008 lines with strong broad and blueshifted components have been observed in two quasars, J0218+0007 (top) and J0224–4711 (bottom). The blue solid lines denote the median velocity (v 50), and the dashed lines mark the part containing 80% of the line power (w 80). J0218+0007 has a v 50 of ∼−610 km s−1 and a w 80 of 1590 km s−1; quasar J0224–4711 has a more remarkable [O III], with a v 50 of ∼−1430 km s−1 and a w 80 of 4140 km s−1. These blueshifted broad lines, in particular in J0224–4711, are comparable to the most extreme cases observed at lower redshift (e.g., Zakamska et al. 2016; Bischetti et al. 2017).
Paper: A SPectroscopic Survey of Biased Halos in the Reionization Era (ASPIRE): A First Look at the Rest-frame Optical Spectra of z > 6.5 Quasars Using JWST
Authors: Jinyi Yang, Feige Wang, Xiaohui Fan, Joseph F. Hennawi, Aaron J. Barth, Eduardo Bañados, Fengwu Sun, Weizhe Liu, Zheng Cai, Linhua Jiang, Zihao Li, Masafusa Onoue, Jan-Torge Schindler, Yue Shen, Yunjing Wu, Aklant K. Bhowmick, Rebekka Bieri, Laura Blecha, Sarah Bosman, Jaclyn B. Champagne, Luis Colina, Thomas Connor, Tiago Costa, Frederick B. Davies, Roberto Decarli, Gisella De Rosa, Alyssa B. Drake, Eiichi Egami, Anna-Christina Eilers, Analis E. Evans, Emanuele Paolo Farina, Melanie Habouzit, Zoltan Haiman, Xiangyu Jin, Hyunsung D. Jun, Koki Kakiichi, Yana Khusanova, Girish Kulkarni, Federica Loiacono, Alessandro Lupi, Chiara Mazzucchelli, Zhiwei Pan, Sofía Rojas-Ruiz, Michael A. Strauss, Wei Leong Tee, Benny Trakhtenbrot, Maxime Trebitsch, Bram Venemans, Marianne Vestergaard, Marta Volonteri, Fabian Walter, Zhang-Liang Xie, Minghao Yue, Haowen Zhang, Huanian Zhang, Siwei Zou
Figure caption: The BH masses of eight ASPIRE quasars (red squares), measured from the Hβ lines in JWST/NIRCam WFSS spectra and the Mg II lines in their NIR spectra. These are compared with the measurements of low-z quasars from the SDSS Data Release 7 (DR7) sample (Shen et al. 2011) using the same Mg II and Hβ BH mass estimators (gray small squares and blue contours). The differences between M BH,Hβ  and M BH,Mg II  of these high-redshift quasars are comparable to the scatter shown in the low-redshift quasar sample. The mean value of M BH,Hβ –M BH,Mg II  is −0.13 dex, while the sample size is too small to identify a systematic offset.
Paper: A SPectroscopic Survey of Biased Halos in the Reionization Era (ASPIRE): A First Look at the Rest-frame Optical Spectra of z > 6.5 Quasars Using JWST
Authors: Jinyi Yang, Feige Wang, Xiaohui Fan, Joseph F. Hennawi, Aaron J. Barth, Eduardo Bañados, Fengwu Sun, Weizhe Liu, Zheng Cai, Linhua Jiang, Zihao Li, Masafusa Onoue, Jan-Torge Schindler, Yue Shen, Yunjing Wu, Aklant K. Bhowmick, Rebekka Bieri, Laura Blecha, Sarah Bosman, Jaclyn B. Champagne, Luis Colina, Thomas Connor, Tiago Costa, Frederick B. Davies, Roberto Decarli, Gisella De Rosa, Alyssa B. Drake, Eiichi Egami, Anna-Christina Eilers, Analis E. Evans, Emanuele Paolo Farina, Melanie Habouzit, Zoltan Haiman, Xiangyu Jin, Hyunsung D. Jun, Koki Kakiichi, Yana Khusanova, Girish Kulkarni, Federica Loiacono, Alessandro Lupi, Chiara Mazzucchelli, Zhiwei Pan, Sofía Rojas-Ruiz, Michael A. Strauss, Wei Leong Tee, Benny Trakhtenbrot, Maxime Trebitsch, Bram Venemans, Marianne Vestergaard, Marta Volonteri, Fabian Walter, Zhang-Liang Xie, Minghao Yue, Haowen Zhang, Huanian Zhang, Siwei Zou
Figure caption: EV1 relations using our eight high-redshift quasars (red squares), compared with luminous quasars at intermediate redshift (Shen 2016; open diamonds) and SDSS low-z quasars (Shen et al. 2011; gray dots). The black filled circles and the dashed lines denote the median, 16th, and 84th percentiles of the SDSS low-z quasars at each redshift bin. These reionization-era quasars generally follow the trends observed in lower-redshift quasars.