adsabs/AstroCLIMB huggingface dataset:
Paper: Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate 
Authors: K. B. Webber, T. T. Hansen, J. L. Marshall, J. D. Simon, A. B. Pace, B. Mutlu-Pakdil, A. Drlica-Wagner, C. E. Martínez-Vázquez, M. Aguena, S. S. Allam, O. Alves, E. Bertin, D. Brooks, A. Carnero Rosell, J. Carretero, L. N. da Costa, J. De Vicente, P. Doel, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, R. A. Gruendl, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, E. Sanchez, B. Santiago, J. Allyn Smith, M. Smith, E. Suchyta, G. Tarle, C. To, N. Weaverdyck, B. Yanny
Figure caption: Best-fit SN yield model (Heger & Woosley 2010) for the derived abundances in J0117 (top) and HD 84937 (bottom). The black points are the derived abundances for J0117, the gray points are the derived abundances for HD 84937 (Sneden et al. 2016; Spite et al. 2017), and the red line is the best-fit SN yield model for each star.
Paper: Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate 
Authors: K. B. Webber, T. T. Hansen, J. L. Marshall, J. D. Simon, A. B. Pace, B. Mutlu-Pakdil, A. Drlica-Wagner, C. E. Martínez-Vázquez, M. Aguena, S. S. Allam, O. Alves, E. Bertin, D. Brooks, A. Carnero Rosell, J. Carretero, L. N. da Costa, J. De Vicente, P. Doel, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, R. A. Gruendl, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, E. Sanchez, B. Santiago, J. Allyn Smith, M. Smith, E. Suchyta, G. Tarle, C. To, N. Weaverdyck, B. Yanny
Figure caption: Comparison of the Sc II and Ti II absorption lines in J0117 to the MW halo stars BD+29 2356 and HD 26297 from Roederer et al. (2014). The absorption features for J0117 are weaker than what is seen for BD+29 2356 and HD 26297. The model atmosphere parameters and Sc and Ti abundances for each star are shown in Table 5.
Paper: Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate 
Authors: K. B. Webber, T. T. Hansen, J. L. Marshall, J. D. Simon, A. B. Pace, B. Mutlu-Pakdil, A. Drlica-Wagner, C. E. Martínez-Vázquez, M. Aguena, S. S. Allam, O. Alves, E. Bertin, D. Brooks, A. Carnero Rosell, J. Carretero, L. N. da Costa, J. De Vicente, P. Doel, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, R. A. Gruendl, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, E. Sanchez, B. Santiago, J. Allyn Smith, M. Smith, E. Suchyta, G. Tarle, C. To, N. Weaverdyck, B. Yanny
Figure caption: Color–magnitude diagram for Cetus II. The black dots are stars with a membership probability p > 0.01 (Pace et al. 2022), and the red dot is J0117. The blue line shows a Dartmouth isochrone (Dotter et al. 2008) with [Fe/H] = − 2.3 and age = 12.5 Gyr, transformed to the DES photometric system (Drlica-Wagner et al. 2018) and shifted to the distance of Cetus II (∼30 kpc; Drlica-Wagner et al. 2015).
Paper: Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate 
Authors: K. B. Webber, T. T. Hansen, J. L. Marshall, J. D. Simon, A. B. Pace, B. Mutlu-Pakdil, A. Drlica-Wagner, C. E. Martínez-Vázquez, M. Aguena, S. S. Allam, O. Alves, E. Bertin, D. Brooks, A. Carnero Rosell, J. Carretero, L. N. da Costa, J. De Vicente, P. Doel, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, R. A. Gruendl, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, E. Sanchez, B. Santiago, J. Allyn Smith, M. Smith, E. Suchyta, G. Tarle, C. To, N. Weaverdyck, B. Yanny
Figure caption: Spectral synthesis of the 4077 Å Sr II line (top) and 4554 Å Ba II line (bottom). The black squares show the observed spectrum of J0117. The dotted line shows a synthesis without Sr or Ba, and the blue line shows a synthesis with the [Sr/Fe] ± σ [Sr/Fe] or [Ba/Fe] ± σ [Ba/Fe] value derived for J0117.
Paper: On the Lifetime of Molecular Clouds with the “Tuning-fork” Analysis
Authors: Jin Koda, Jonathan C. Tan
Figure caption: Snapshot of a randomly sampled uniform distribution of clouds at t = 300 Myr. Top: case A—mortal clouds. Bottom: case B—immortal clouds. The input parameters are shown in the right panels (top-right corners). Left: the gas/cloud distributions in blue. They occasionally form star particles (red) with a lifetime of t star at a probability of p SF = Δt/t gas in each Δt = 1 Myr time step. The gas clouds do not move from their birth locations. The star particles stay/overlap with the clouds for t over and then drift away from the clouds and travel for the rest of their lives. Their drift velocity is v drift in a random direction. The black lines connect the start points (clouds) and end points of the stellar trajectories, but are short and often hidden behind the other markers. In case A (top), clouds die/disappear at the end of the overlap period t over, and the same number of clouds are redistributed uniformly over the disk (the total number N gas stays constant). In case B (bottom), clouds live forever and stay at the same locations throughout the simulation. Right: the TF fits. The blue and red dots are from Equation (2) for gas clouds and stars, respectively. The solid lines are fits of Equations (6) and (7). The fit results are also presented (bottom-right corners).
Paper: Rotational Components of the Sun’s Mean Field
Authors: Neil R. Sheeley
Figure caption: Wavelet power in the region of the solar rotation period (middle panel) and its second and third harmonics (top panel), displayed using γ/2π = 20 and γ/2π = 40, respectively. Faint dotted lines indicate periods of T = 27, 28.5, and 30 days near 5.8 on the vertical scale, and for their second harmonics near 4.8. A single dotted line indicates the third harmonic of T = 27 days near 4.2. The arrows indicate features at 4.73 in 1990–1991 and 5.73 during 2002–2004, corresponding to rotation periods ∼26.5 days. Bottom: monthly averaged sunspot number from the Royal Observatory of Belgium (SILSO).
Paper: On the Lifetime of Molecular Clouds with the “Tuning-fork” Analysis
Authors: Jin Koda, Jonathan C. Tan
Figure caption: Schematic presentations of (A) mortal molecular clouds by KL14 and K18, and (B) immortal clouds with infinite lifetime. In case A, t gas is the lifetime of gas cloud, t over is the timescale in which a cloud contains a star particle (SF tracer peak), t star is the lifetime of a star particle, and t tot is the total duration between the birth of a cloud and the death of its star particle. In case B, clouds live forever and repeat an SF cycle. The definitions of the timescales are the same as in case A, except for t gas, which is the timescale of one SF cycle in a gas cloud. In both cases, t tot = t gas + t star − t over. Note, case B involves a relative drift velocity, v drift, between stars and clouds.
Paper: On the Lifetime of Molecular Clouds with the “Tuning-fork” Analysis
Authors: Jin Koda, Jonathan C. Tan
Figure caption: The same as Figure 2, but for the exponential disk plus spiral arm distribution. We set the disk radius R gas = 5 kpc, scale length of the exponential disk h = 3 kpc, spiral arm width parameter w = 0.6 kpc, and pitch angle i = 30°. As in Figure 2, the immortal clouds with occasional SF produce a TF pattern if the stars drift away from the parental clouds (bottom-right panel). In this case the TF fit returns t gas, which is not a cloud lifetime.
Paper: On the Lifetime of Molecular Clouds with the “Tuning-fork” Analysis
Authors: Jin Koda, Jonathan C. Tan
Figure caption: The same as Figure 2 (uniform distribution), except for (left) v drift = 0 km s−1 and (rght) v drift = 5 km s−1. Top: mortal clouds; bottom: immortal clouds. In the case of v drift = 0 km s−1 (no drift), the stars do not drift away from the parental clouds. Hence, there are no stars without overlapping parental clouds when the clouds are immortal. Thus, the top branch (blue) of the TF pattern stays at a value close to unity in panel (c).
Paper: On the Lifetime of Molecular Clouds with the “Tuning-fork” Analysis
Authors: Jin Koda, Jonathan C. Tan
Figure caption: TF plots of immortal clouds. The same as the bottom-right panel (immortal clouds) of Figure 3, but for different values of v drift and t gas: v drift = 10 km s−1 (left) and 30 km s−1 (right); t gas = 30 Myr (top), 40 Myr (middle), and 50 Myr (bottom).
Paper: On the Lifetime of Molecular Clouds with the “Tuning-fork” Analysis
Authors: Jin Koda, Jonathan C. Tan
Figure caption: The same as Figure 2 (uniform distribution), except for p SF = Δt/(b rot t rot), i.e., t gas = b rot t rot with the galactic rotation timescale t rot and the efficiency of (a) b rot = 0.2 and (b) b rot = 0.4.
Paper: Formation of Massive and Wide First-star Binaries in Radiation Hydrodynamic Simulations
Authors: Kazuyuki Sugimura, Tomoaki Matsumoto, Takashi Hosokawa, Shingo Hirano, Kazuyuki Omukai
Figure caption: One-dimensional profile of the circumbinary disk presented in Figure 8. From top to bottom, we plot the angle-averaged column density Σ, temperature T, angular velocity v  ϕ , disk height H disk, and scale height H scale (see the text for definitions), and Toomre’s Q parameter Q. In the third panel, we show the two Kepler velocities considering only the mass of the protostars (green) and considering both the mass of the protostars and the enclosed gas mass (orange). Black-dashed lines indicate the aspect ratio of unity, H/R = 1, in the fourth panel and the marginally stable state, Q = 1, in the last panel. The two sink particles are located around 800 au from the center.
Paper: Formation of Massive and Wide First-star Binaries in Radiation Hydrodynamic Simulations
Authors: Kazuyuki Sugimura, Tomoaki Matsumoto, Takashi Hosokawa, Shingo Hirano, Kazuyuki Omukai
Figure caption: The edge-on slice snapshots for one of the circumstellar disks at Δt = 10,000 yr in the intermediate-﹩\dot{M}﹩ case. From the top to bottom, we plot the density, temperature, H2 fraction, and H+ fraction. In the lower three panels, the bipolar photoionization and photodissociation fronts are demarcated with solid and dashed lines.
Paper: Formation of Massive and Wide First-star Binaries in Radiation Hydrodynamic Simulations
Authors: Kazuyuki Sugimura, Tomoaki Matsumoto, Takashi Hosokawa, Shingo Hirano, Kazuyuki Omukai
Figure caption: Radiative properties of the Population III protostars obtained from the table used in this work. We plot the protostellar radius R *, luminosity L *, effective temperature T eff, EUV emissivity S EUV, and FUV emissivity S FUV from top to bottom. The horizontal axis corresponds to the mass M, and the color indicates the accretion rate ﹩\dot{M}={10}^{-5},{10}^{-4},{10}^{-3},{10}^{-2},\mathrm{and}{10}^{-1}\,{M}_{\odot }{\mathrm{yr}}^{-1}﹩ (see the labels in the top panel). In the second panel, we also show the Eddington luminosity L Edd with a dashed line.
Paper: Formation of Massive and Wide First-star Binaries in Radiation Hydrodynamic Simulations
Authors: Kazuyuki Sugimura, Tomoaki Matsumoto, Takashi Hosokawa, Shingo Hirano, Kazuyuki Omukai
Figure caption: Same as Figure 18 but for the circumstellar disk presented in Figure 19. The sink radius is indicated with the vertical dashed line.
Paper: Formation of Massive and Wide First-star Binaries in Radiation Hydrodynamic Simulations
Authors: Kazuyuki Sugimura, Tomoaki Matsumoto, Takashi Hosokawa, Shingo Hirano, Kazuyuki Omukai
Figure caption: Same as Figure 13 but for the resolution dependence in no-radiation runs. We compare the runs with different sink radii of r sink = 64 (blue), 32 (orange), and 16 au (green).
Paper: Formation of Massive and Wide First-star Binaries in Radiation Hydrodynamic Simulations
Authors: Kazuyuki Sugimura, Tomoaki Matsumoto, Takashi Hosokawa, Shingo Hirano, Kazuyuki Omukai
Figure caption: Same as Figure 13 but for the resolution dependence in full-feedback runs. We compare the runs with different sink radii of r sink = 64 (blue) and 32 au (orange).
Paper: Investigation of Emission States of PSR J1722–3207
Authors: D. Zhao, W. M. Yan, N. Wang, J. P. Yuan
Figure caption: A single-pulse stack of 340 successive pulses (bottom) and corresponding mean pulse profile (top). The three vertical dashed lines in each panel are the boundaries that divide the profiles into two components.
Paper: Investigation of Emission States of PSR J1722–3207
Authors: D. Zhao, W. M. Yan, N. Wang, J. P. Yuan
Figure caption: Fluctuation analysis for PSR J1722−3207. The top panel shows the average profile (solid line) and longitude-resolved modulation index (points with error bars). The LRFS is given below this panel. The 2DFS is shown at the bottom.
Paper: Investigation of Emission States of PSR J1722–3207
Authors: D. Zhao, W. M. Yan, N. Wang, J. P. Yuan
Figure caption: The S/N distributions for the leading (solid histogram) and trailing (dashed histogram) components. In the inset, we zoom in on the high-S/N region (S/N > 10), using the same axis units as the main plot.
Paper: Investigation of Emission States of PSR J1722–3207
Authors: D. Zhao, W. M. Yan, N. Wang, J. P. Yuan
Figure caption: The S/N variations for the leading (upper panel) and the trailing (lower panel) components of a single pulse for the pulse sequence shown in Figure 1.
Paper: Investigation of Emission States of PSR J1722–3207
Authors: D. Zhao, W. M. Yan, N. Wang, J. P. Yuan
Figure caption: The distributions of duration of the strong (solid histogram) and weak (dashed histogram) states for the leading component.
Paper: Investigation of Emission States of PSR J1722–3207
Authors: D. Zhao, W. M. Yan, N. Wang, J. P. Yuan
Figure caption: The 2DFS for the trailing component.
Paper: Investigation of Emission States of PSR J1722–3207
Authors: D. Zhao, W. M. Yan, N. Wang, J. P. Yuan
Figure caption: Pulse energy distributions for the off-pulse region (green dotted histogram), on-pulse (black dotted histogram), leading component (blue solid histogram), and trailing component (red dashed histogram). The energies are normalized by the mean on-pulse energy.
Paper: RZ Piscium Hosts a Compact and Highly Perturbed Debris Disk
Authors: Kate Y. L. Su, Grant M. Kennedy, G. H. Rieke, A. Meredith Hughes, Yu-Chia Lin, Jamar Kittling, Alan P. Jackson, Ramya M. Anche, Hauyu Baobab Liu
Figure caption: SED comparison for three different types of debris disks around solar-like stars: RZ Psc (red; EDD), HIP 61049 (green; typical young debris disk), and HD 69830 (blue; highly stirred warm belt), with the latter two normalized to the distance of RZ Psc. Photometry points are shown as various symbols, mid-infrared spectra as the solid lines, and model disk emission as the dashed lines. The amount of infrared excess emission in EDDs is exceptionally large compared to typical debris disks.
Paper: RZ Piscium Hosts a Compact and Highly Perturbed Debris Disk
Authors: Kate Y. L. Su, Grant M. Kennedy, G. H. Rieke, A. Meredith Hughes, Yu-Chia Lin, Jamar Kittling, Alan P. Jackson, Ramya M. Anche, Hauyu Baobab Liu
Figure caption: Spitzer monitoring data of the RZ Psc system: top for the 3.6 and 4.5 μm excess fluxes, middle for its corresponding color temperature, and bottom for the optical light curves. The arrow-like symbols near the top of the top panel mark the year boundaries of the data. Horizontal dashed lines in the top and middle panels are the median value of the derived quantity. Optical light curves include ASAS-SN V- (orange) and g-band (green) and AAVSO V-band (various colors) data (for details, see Section 2.2).
Paper: RZ Piscium Hosts a Compact and Highly Perturbed Debris Disk
Authors: Kate Y. L. Su, Grant M. Kennedy, G. H. Rieke, A. Meredith Hughes, Yu-Chia Lin, Jamar Kittling, Alan P. Jackson, Ramya M. Anche, Hauyu Baobab Liu
Figure caption: (a) A naturally weighted ALMA image of the 1.3 mm continuum observation centered at RZ Psc (star). Contours are [1, 3, 5] × σ, where σ = the rms noise = 8 μJy beam−1. The synthesized beam dimensions, represented by the red ellipse in the lower left corner, are 0.″06 × 0.″04 with a P.A. of 14.°8. The position of RZ Psc B (Kennedy et al. 2020) is marked by a red plus sign for reference. The middle and right panels are the corresponding residual maps after the subtraction of a Gaussian disk model in panel (b) and the associated uv-data in panel (c) (for details, see Section 3.1).
Paper: RZ Piscium Hosts a Compact and Highly Perturbed Debris Disk
Authors: Kate Y. L. Su, Grant M. Kennedy, G. H. Rieke, A. Meredith Hughes, Yu-Chia Lin, Jamar Kittling, Alan P. Jackson, Ramya M. Anche, Hauyu Baobab Liu
Figure caption: SED models of the RZ Psc system, including the star and a single-component disk (see Section 3.2 for details). Various symbols are publicly available broadband photometry points from Simbad, 2MASS (Cutri et al. 2003), ALLWISE (Cutri et al. 2014), and AKARI (Ishihara et al. 2010), and the yellow dashed line is the N-band grism spectrum from Kennedy et al. (2017).
Paper: RZ Piscium Hosts a Compact and Highly Perturbed Debris Disk
Authors: Kate Y. L. Su, Grant M. Kennedy, G. H. Rieke, A. Meredith Hughes, Yu-Chia Lin, Jamar Kittling, Alan P. Jackson, Ramya M. Anche, Hauyu Baobab Liu
Figure caption: WISE/NEOWISE W1 and W2 data for the RZ Psc system, where the stellar contribution has been subtracted off. The peak infrared flux occurred in mid-2014, prior to the Spitzer monitoring period (shaded region).
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: NIRSpec spectra of CEERS_01244, GLASS_160133, GLASS_150029, and CEERS_00746. For each object, the left and middle panels show spectra around Hβ+[OIII]λ λ 4959,5007 and Hα+[NII]λ λ 6548,6584, respectively. The 2D and 1D spectra are shown in the top and bottom panels, respectively. The red-dashed line with the shaded region shows the best-fit broad-line component (FWHM > 1000 km s−1) and the other red-dashed lines show the best-fit narrow component (FWHM < 500 km s−1). For GLASS_160133 and GLASS_150029, we also show the outflow components with FWHM ≲ 500 km s−1. The right panels show the spectra around Hα+[NII]λ λ 6548,6584 with the logarithmic scale. The broad-line components only seen in Hα, which are detected with a higher S/N than [O III]λ5007, indicate that these objects are type 1 AGNs.
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: 3″ × 3″ images of our faint type 1 AGNs. The HST/ACS F606W, F814W, and the JWST/NIRCam F115W, F150W, F200W, F277W, F356W, and F444W images are shown. For objects whose NIRCam images are not available, we instead show the HST/WFC3 F125W and F160W images. The NIRSpec MSA aperture is shown with the blue rectangle in the longest wavelength band. More than half of the sources show extended morphologies, indicating that the total lights are significantly contributed by their host galaxies.
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: UV magnitude and spectroscopic redshifts of our selected broad-line AGNs (the diamonds). The magenta diamonds denote red AGNs (E(B − V) > 0.5) and the red diamonds denote the other AGNs identified in this study. The gray circles show the star-forming galaxies in Nakajima et al. (2023).
Paper: Accretion Disk Wind of Hercules X-1 during the Short High State
Authors: P. Kosec, E. Kara, A. C. Fabian, C. Pinto, I. Psaradaki, D. Rogantini, R. Staubert, D. J. Walton
Figure caption: Simulated 10 ks XRISM spectrum of Her X-1 in the Short High state, focusing only on the Fe K energy band. XRISM data are in blue and the simulated spectral model (including the ionized absorption component) is in red. The data are binned to oversample the instrumental resolution by a factor of 2.
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: False color stamps of our faint AGNs. We use JWST/NIRCam F115W, F200W, and F356W images, while HST/ACS F814W and HST/WFC3 F125W and F160W are used for the objects whose NIRCam images are not available. Each thumbnail is 2″ × 2″ in size.
Paper: Accretion Disk Wind of Hercules X-1 during the Short High State
Authors: P. Kosec, E. Kara, A. C. Fabian, C. Pinto, I. Psaradaki, D. Rogantini, R. Staubert, D. J. Walton
Figure caption: Wind column density (top panel) and ionization parameter (bottom panel) vs. the equivalent disk precession phase. Main High state observations (taken from Kosec et al. 2023) are shown in black (XMM-Newton) and blue (Chandra), the only Chandra observation during the Short High is in red. The X-axis value of the Short High state data point is the precession phase elapsed since the Rise into the Short High state.
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: Same as Figure 1 but for CEERS_00717 and CEERS_01236.
Paper: A JWST/NIRSpec First Census of Broad-line AGNs at z = 4–7: Detection of 10 Faint AGNs with M BH ∼ 106–108 M ⊙ and Their Host Galaxy Properties
Authors: Yuichi Harikane, Yechi Zhang, Kimihiko Nakajima, Masami Ouchi, Yuki Isobe, Yoshiaki Ono, Shun Hatano, Yi Xu, Hiroya Umeda
Figure caption: Same as Figure 1 but for CEERS_01665, CEERS_00672, CEERS_02782, and CEERS_00397.
Paper: Characterizing the Near-infrared Spectra of Flares from TRAPPIST-1 during JWST Transit Spectroscopy Observations
Authors: Ward S. Howard, Adam F. Kowalski, Laura Flagg, Meredith A. MacGregor, Olivia Lim, Michael Radica, Caroline Piaulet, Pierre-Alexis Roy, David Lafrenière, Björn Benneke, Alexander Brown, Néstor Espinoza, René Doyon, Louis-Philippe Coulombe, Doug Johnstone, Nicolas B. Cowan, Ray Jayawardhana, Jake D. Turner, Lisa Dang
Figure caption: Left: we compare the JWST measured flare rate of TRAPPIST-1 in the TESS-band (0.6–1 μm; blue points) against two previous FFDs of the star reproduced from Seli et al. (2021). The K2 flare rate of TRAPPIST-1 from Vida et al. (2017) is shown in gray and scaled to the TESS bandpass by Seli et al. (2021). The flare rate of TRAPPIST-1 analog stars observed by the TESS mission in its full-frame images is shown in orange and is higher than that predicted from K2. The flare rate measured by JWST agrees with the flare rate measured from the TRAPPIST-1 analogs, suggesting flares are likely to contaminate more transits than suggested by the K2 data. NIRSpec flares are noted with a dagger. Right: cooler flares lead to an underestimated TESS-band energy when scaling from the Kepler band using a 9000 K blackbody. Both 9000 and 5000 K flare spectra emit the same energy in the Kepler band, but the TESS-band energies are higher for the cooler flare by 46%.