adsabs/AstroCLIMB huggingface dataset:
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: Relation between dust mass and stellar mass. The red-filled diamonds represent Himiko and CR7, whose total stellar and dust masses are estimated in this study. The red-open symbols show the UV bright (MUV ≲ −21.5) and clumpy galaxies in the literature: UVISTA-238225 (R. A. A. Bowler et al. 2018), XMM1-Z-1664 (R. J. Bouwens et al. 2022; H. Inami et al. 2022), COS-2987030247 (H. Inami et al. 2022; Y. Harikane et al. 2025), COS-3018555981 (H. Inami et al. 2022; J. Witstok et al. 2022; Y. Harikane et al. 2025), as indicated in the legend. The upper limits are 3σ levels. The black symbols show the other high-redshift merger galaxies HZ10 (P. L. Capak et al. 2015; V. Villanueva et al. 2024), DC818760 (G. C. Jones et al. 2020), A1689-zD1 (D. Watson et al. 2015; K. K. Knudsen et al. 2017), and B14-65666 (T. Hashimoto et al. 2019). The magenta-filled symbols show high-redshift (z = 6–7) clumpy SMGs (SPT0311-58E, D. P. Marrone et al. 2018; SPT0311-58W, D. P. Marrone et al. 2018; HFLS3, D. A. Riechers et al. 2013). The magenta-open symbols show large SMG samples (ALESS, E. da Cunha et al. 2015; HUDF, J. S. Dunlop et al. 2017). The gray-shaded region shows local galaxy samples from the Herschel-ATLAS/GAMA survey (N. Bourne et al. 2012). The black-open circles show the JWST CEERS samples at 4 < z < 11 (D. Burgarella et al. 2024). The black-dashed line shows the S850μm = 1 mJy at z = 4, which corresponds to SCUBA’s deepest detection limit (W. S. Holland et al. 1999). This threshold remains largely unchanged with redshift due to the negative-k correction (e.g., A. W. Blain & M. S. Longair 1993; A. W. Blain et al. 2002). The gray-dashed lines correspond to the dust-to-stellar mass ratio from 10−4 to 10−1 from bottom to top. The ticks at the top represent metallicities, derived from stellar mass, using the mass–metallicity relation at z = 4–10 as presented in K. Nakajima et al. (2023).
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: Projected phase-space diagrams for Himiko (top) and CR7 (bottom). The horizontal axis shows the projected distance from Himiko-B (CR7-B) normalized to r200. The vertical axis is the absolute line-of-sight velocity from the fiducial clump (Himiko-B, CR7-C) normalized by the velocity dispersion of the halo. The red diamonds show the clumps of Himiko or CR7 with clump IDs. The black-dashed line shows the escape velocity in the NFW potential of ﹩{\mathrm{log}}({M}_{200}/{M}_{\odot })=11.3﹩ (11.4) for Himiko (CR7). The gray region is below the escape velocity (infalling region). The blue region shows the virialized region. The solid black line and the dashed–dotted line show the simulated tracks of merging galaxies from FOREVER22 (PCR0-ID32) and FirstLight (FL956), respectively (see Sections 5.1 and 5.4). The redshift of each point is indicated by the labels.
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: FirstLight simulation (D. Ceverino et al. 2017; Y. Nakazato et al. 2024) results for a galaxy sample FL956. Panels (a) and (b) show the time evolution of gas density distribution and SFR surface density from z = 6.69 to z = 6.14, respectively. Each panel shows a region of 10 × 10 kpc, corresponding to ﹩1\mathop{.}\limits{^{\prime\prime} }8\times 1\mathop{.}\limits{^{\prime\prime} }8﹩ at z = 6.6. Panel (c) shows the star formation history (blue) and stellar mass evolution (black) from z = 9.0 to z = 5.3. In panel (c), z = 6.69, z = 6.52, and z = 6.14 are indicated by gray-dashed lines, which correspond to panels (a) and (b).
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: FOREVER22 simulation (H. Yajima et al. 2022; H. Yajima et al. 2023) results for a galaxy sample, PCR0-ID32, at z = 6.8. Each panel represents a physical scale of 40 × 40 kpc. Left: stellar distribution. The simulated map is smoothed to match the spatial resolution of NIRCam F444W (﹩0\mathop{.}\limits{^{\prime\prime} }16﹩). The contours show the Lyα surface brightness levels of 10−20, 10−19, and 10−18 erg s−1 cm−2 arcsec−2 in the dust-free model. The scale bar shows the 1″. The circles at the bottom right show the PSF FWHM of JWST/NIRCam F444W (﹩{\rm{PSF}}\,{\rm{FWHM}}\sim 0\mathop{.}\limits{^{\prime\prime} }16﹩, right) and Subaru NB921 (﹩0\mathop{.}\limits{^{\prime\prime} }75﹩, left). Middle (right): Lyα surface brightness with dust-free (dust) model. The simulated map is smoothed to match the spatial resolution of Subaru NB921 (﹩{\rm{PSF}}\,{\rm{FWHM}}\sim 0\mathop{.}\limits{^{\prime\prime} }75﹩). The area brighter than the Subaru surface brightness limit (∼10−18 erg s−1 cm−2 arcsec−2) is indicated by the colorbar, while regions approximately fainter than the limit are shown in black. The scalebar and circles are the same as in the left panel.
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: Relation between [C II]-IR luminosity ratio and IR luminosity. The red-filled diamond and square show Himiko and CR7 (total [C II] and IR luminosity), respectively. The red-open symbols show the UV bright (MUV ≲ −21.5) and clumpy galaxies in the literature: COS-298703024 (R. Smit et al. 2018) and COS-3018555981 (J. Witstok et al. 2022), as indicated in the legend. The black symbols show the high-redshift dusty merger galaxies: HZ10 (P. L. Capak et al. 2015), A1689-zD1 (Y. H. V. Wong et al. 2022), and B14-65666 (T. Hashimoto et al. 2019). The magenta-filled symbols show the clumpy submillimeter galaxies at z = 6–7 (SPT0311-58E, D. P. Marrone et al. 2018; SPT0311-58W, D. P. Marrone et al. 2018; HFLS3, D. A. Riechers et al. 2013). The open-magenta and filled-gray plots show the submillimeter galaxies at 2 < z < 6 (South Pole Telescope (SPT) samples, B. Gullberg et al. 2015) and the local galaxies from GOALS (T. Díaz-Santos et al. 2013), respectively. From the literature, we convert the IR luminosity LIR by multiplying the factor of 1.7 for L42.5−122.5 μm, and 1.3 for L42−500 μm.
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: Relation between the black hole mass and the stellar mass. The red-filled diamond shows the Himiko clump B. The red-open squares and circles show AGN samples found with JWST/NIRSpec utilizing broad emission lines at z = 4.0–6.9 (Y. Harikane et al. 2023) and z = 4.4–6.7 (R. Maiolino et al. 2024), respectively. The red-dashed line shows the fitting result of AGN samples discovered with JWST presented in F. Pacucci et al. (2023). The gray dots show the AGNs at z ∼ 0 presented in A. E. Reines & M. Volonteri (2015). The solid black line and gray shade show the fitting result and its error of AGNs at z ∼ 0 (A. E. Reines & M. Volonteri 2015). The gray-dashed lines show the black hole mass to stellar mass ratio of 0.1, 0.01, and 0.001. In the top right, the gray error bar shows the systematic uncertainty of the black hole mass measurement (±0.5 dex; A. E. Reines & M. Volonteri 2015).
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: Line ratio maps of Hα/Hβ, E(B − V) derived from Hα/Hβ, R3, and metallicity derived from R3. The top (bottom) four panels show Himiko (CR7). The metallicity is estimated using the relation from M. Hirschmann et al. (2023) and is broadly consistent with the direct method applied to the spatially integrated spectra of individual clumps (see Figure 13). The gray circle in the upper left corner indicates the PSF FWHM size, and the scale bar shows 2 kpc at z = 6.6.
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: Relation between the bolometric luminosity and the black hole mass. The red-filled diamond shows the Himiko clump B. The red-open squares and circles show AGNs found with JWST/NIRSpec utilizing broad emission lines at z = 4.0–6.9 (Y. Harikane et al. 2023) and z = 4.4–6.7 (R. Maiolino et al. 2024), respectively. The blue plots show the high-z quasars (circle, B. Trakhtenbrot et al. 2011; triangle, Y. Shen et al. 2019). The gray and blue contours show the distribution of broad-line AGNs at z < 0.35 (H.-Y. Liu et al. 2019) and SDSS DR7 quasars at z = 1–3 (Y. Shen et al. 2011), respectively. The gray-dashed lines show 100%, 10%, and 1% Eddington luminosity.
Paper: Comprehensive JWST+ALMA Study on the Extended Lyα Emitters, Himiko, and CR7 at z ∼ 7: Blue Major Merger Systems in Stark Contrast to Submillimeter Galaxies
Authors: Tomokazu Kiyota, Masami Ouchi, Yi Xu, Yurina Nakazato, Kenta Soga, Hidenobu Yajima, Seiji Fujimoto, Yuichi Harikane, Kimihiko Nakajima, Yoshiaki Ono, Dongsheng Sun, Haruka Kusakabe, Daniel Ceverino, Bunyo Hatsukade, Daisuke Iono, Kotaro Kohno, Kouichiro Nakanishi
Figure caption: Relation between DTG (DTM) and metallicity shown in left (right). The red diamond and square show Himiko and CR7, respectively. The blue, magenta, and gray plots show the DLA (C. Péroux & J. C. Howk 2020), SMGs at z ∼ 2 (A. E. Shapley et al. 2020), and local galaxies (DustPedia; P. De Vis et al. 2019; V. Casasola et al. 2020), respectively.
Paper: How Invisible Stellar Halos Bias Our Understanding of Ultrafaint Galaxies
Authors: Coral Wheeler, Jorge Moreno, M. Katy Rodriguez Wimberly, Francisco J. Mercado, James S. Bullock, Michael Boylan-Kolchin, Pratik J. Gandhi, Sarah R. Loebman, Philip F. Hopkins
Figure caption: Left: line-of-sight velocity dispersion versus stellar mass within the galaxy “edge” for the R15% (open symbols) and RSB cut (solid symbols), color coded by dark matter halo mass. Marker shapes indicate centrals (stars) and satellites (triangles). Vertical lines descending from each simulated data point, but visible only at the lowest masses, show conservative lower-bound estimates for σlos if impacted by nonphysical secular evolution. See Section 4.2 for more details on the possibility of spurious numerical heating. Data are from a compilation by A. B. Pace (2024), and are limited to M⋆ < 105 M⊙. The RSB cut moves the predicted σlos toward lower values and closer to observations. We also plot predictions from other high-resolution simulations as various colored symbols, where we have assumed an M/L of 1 to convert to stellar mass where needed (M. Jeon et al. 2017, 2021; E. Applebaum et al. 2021; M. Go et al. 2024). Right: line-of-sight velocity dispersion versus dark matter halo mass, color coded by surface brightness. Using the RSB cut, a weak trend exists between halo mass and surface brightness for galaxies with similar σlos, such that lower-mass halos are more difficult to see. However, the opposite trend exists for the R15% cut.
Paper: How Invisible Stellar Halos Bias Our Understanding of Ultrafaint Galaxies
Authors: Coral Wheeler, Jorge Moreno, M. Katy Rodriguez Wimberly, Francisco J. Mercado, James S. Bullock, Michael Boylan-Kolchin, Pratik J. Gandhi, Sarah R. Loebman, Philip F. Hopkins
Figure caption: Left: ratio of estimated total mass enclosed within R1/2 from J. Wolf et al. (2010), ﹩{M}_{1/2}^{{\rm{est}}}﹩, to the true total mass enclosed within the same radius, ﹩{M}_{1/2}^{{\rm{true}}}﹩, for the R15% (open points) and surface brightness limit (RSB; closed points) as a function of R1/2. Marker shapes and transparency indicate centrals (stars; darker) and satellites (triangles; dimmer). The dashed line shows a ratio of 1, and the arrows point from the R15% cut to the RSB cut for each galaxy. With just a few notable exceptions, removing the stellar halo from these galaxies (RSB cut) leads to smaller R1/2 values and ﹩{M}_{1/2}^{{\rm{est}}}/{M}_{1/2}^{{\rm{true}}}﹩ farther from 1 (i.e., the mass estimate gets worse along the arrow). This is a result of the relatively larger decrease in the true mass enclosed within R1/2 compared to the decrease in ﹩{M}_{1/2}^{{\rm{est}}}﹩, rather than an increase in the J. Wolf et al. (2010) estimate. Right: same as the left panel, but as a function of mean effective surface brightness, μV, within R1/2. With the same counter examples as in the left panel, removing the stellar halo from these galaxies (RSB cut) leads to lower μV values (higher surface brightness) and higher ﹩{M}_{1/2}^{{\rm{est}}}/{M}_{1/2}^{{\rm{true}}}﹩ values along the arrow.
Paper: How Invisible Stellar Halos Bias Our Understanding of Ultrafaint Galaxies
Authors: Coral Wheeler, Jorge Moreno, M. Katy Rodriguez Wimberly, Francisco J. Mercado, James S. Bullock, Michael Boylan-Kolchin, Pratik J. Gandhi, Sarah R. Loebman, Philip F. Hopkins
Figure caption: Stellar mass (M⋆) versus metallicity ([Fe/H]) in our simulated galaxies using a galaxy edge defined as 15% rvir (R15%; open symbols) and using a surface brightness cut at ﹩{\mu }_{V}=32.5\,{\rm{mag}}\,{{\rm{arcsec}}}^{-2}﹩ (RSB; closed symbols). As in C. Wheeler et al. (2019), the UFDs at [Fe/H] ∼ –4 are at the baseline initial metallicity of the simulation. The two most massive UFDs show slightly improved agreement with the updated data from A. B. Pace (2024), shown as points with error bars for both methods of determining galaxy edge, but the surface brightness cut moves the simulated points even closer. Data from other high-resolution simulations are also shown, where we have assumed an M/L of 1 to convert to stellar mass where needed (M. Jeon et al. 2017, 2021; E. Applebaum et al. 2021; M. Prgomet et al. 2022; M. Go et al. 2024; M. P. Rey et al. 2025).
Paper: How Invisible Stellar Halos Bias Our Understanding of Ultrafaint Galaxies
Authors: Coral Wheeler, Jorge Moreno, M. Katy Rodriguez Wimberly, Francisco J. Mercado, James S. Bullock, Michael Boylan-Kolchin, Pratik J. Gandhi, Sarah R. Loebman, Philip F. Hopkins
Figure caption: Left: metallicity distribution function (MDF) for our most massive ultrafaint galaxy, m10v30 B, for the R15% (solid black line) and surface brightness limit (RSB; dashed blue line). We also show all stars within the virial radius of the galaxy’s host halo as a thin dashed black line. MDFs for Bootes 1 (Eridanus 2) are also shown as red (cyan) shaded histograms (M. K. Rodriguez Wimberly 2025, in preparation). Many of the stars remain at the metallicity floor of the simulation, and those stars are preferentially removed from the outer edge of the galaxy when performing the RSB cut, shifting the mean [Fe/H] upward. Right: same but for the second most massive galaxy, m0930.
Paper: How Invisible Stellar Halos Bias Our Understanding of Ultrafaint Galaxies
Authors: Coral Wheeler, Jorge Moreno, M. Katy Rodriguez Wimberly, Francisco J. Mercado, James S. Bullock, Michael Boylan-Kolchin, Pratik J. Gandhi, Sarah R. Loebman, Philip F. Hopkins
Figure caption: 2D (projected) half-stellar-mass radii (R1/2) versus M⋆ for all simulated galaxies in the sample. Galaxies are color coded by their z = 0 dark matter halo mass. Open symbols show values calculated assuming the galaxy edge is R15%, while solid symbols use the RSB cut described in Section 2.1. Marker shapes indicate centrals (stars) and satellites (triangles). Observed MW UFDs are compiled from A. B. Pace (2024). The solid line is a typical surface brightness limit of these surveys, ﹩30\,{\rm{mag}}\,{{\rm{arcsec}}}^{-2}﹩ for M/L ≈ 1 M⊙/L⊙. The dashed line shows a surface brightness limit of ﹩32.5\,{\rm{mag}}\,{{\rm{arcsec}}}^{-2}﹩, more comparable to future surveys such as LSST. We also plot predictions from other high-resolution simulations as various colored symbols, where we have assumed an M/L of 1 if needed to convert to stellar mass (M. Jeon et al. 2017, 2021; E. Applebaum et al. 2021; M. Prgomet et al. 2022; M. Go et al. 2024; E. P. Andersson et al. 2025; M. P. Rey et al. 2025).
Paper: How Invisible Stellar Halos Bias Our Understanding of Ultrafaint Galaxies
Authors: Coral Wheeler, Jorge Moreno, M. Katy Rodriguez Wimberly, Francisco J. Mercado, James S. Bullock, Michael Boylan-Kolchin, Pratik J. Gandhi, Sarah R. Loebman, Philip F. Hopkins
Figure caption: Projected surface brightness profiles (assuming M/L = 1M⊙/L⊙) out to 15% of the halo virial radius for all ultrafaint (M⋆ < 105 M⊙) galaxies in our sample, color coded by dark matter halo mass. We select the radius at which each profile crosses the horizontal line shown at ﹩32.5\,{\rm{mag}}\,{{\rm{arcsec}}}^{-2}﹩ as the new galaxy edge (open circles). In every case, this decreases the defined galaxy “edge” of our simulated sample. We restrict our sample to all galaxies that maintain at least 10 star particles using both definitions for galaxy edge, and that have well-defined and measurable surface brightness profiles above the detection threshold.
Paper: How Invisible Stellar Halos Bias Our Understanding of Ultrafaint Galaxies
Authors: Coral Wheeler, Jorge Moreno, M. Katy Rodriguez Wimberly, Francisco J. Mercado, James S. Bullock, Michael Boylan-Kolchin, Pratik J. Gandhi, Sarah R. Loebman, Philip F. Hopkins
Figure caption: Left: estimated mass within R1/2 from the J. Wolf et al. (2010) formula, ﹩{M}_{1/2}^{{\rm{est}}}﹩, versus 3D deprojected half-light radius for simulated FIRE-2 UFDs using the R15% cut. Marker shapes indicate centrals (stars) and satellites (triangles). Point color indicates the true dark matter mass, Mhalo, as measured by the halo finder. The lines represent the enclosed mass for NFW halo mass profiles of varying masses, color coded the same as the points. Right: same as in the left panel, but for the RSB cut. We assume a halo concentration of c = 24, as predicted by extrapolating the A. F. Neto et al. (2007) halo concentration relation down to UFD masses.
Paper: How Invisible Stellar Halos Bias Our Understanding of Ultrafaint Galaxies
Authors: Coral Wheeler, Jorge Moreno, M. Katy Rodriguez Wimberly, Francisco J. Mercado, James S. Bullock, Michael Boylan-Kolchin, Pratik J. Gandhi, Sarah R. Loebman, Philip F. Hopkins
Figure caption: Left: circular velocity profiles for galaxies in the m10v30 simulation. Solid lines show the total circular velocity profile computed from the total dark matter, gas, and stellar mass enclosed within the 3D radius. Color-matched markers denote the J. Wolf et al. (2010) dynamical mass estimator as in the left panel. Right: J. Wolf et al. (2010) dynamical mass estimator evaluated at the 3D deprojected half-light radius using the R15% cut (open symbols) and the RSB cut (closed symbols) for the same galaxy. Marker shapes indicate centrals (stars) and satellites (triangles). Thin lines connect matched pairs for each halo. Data from A. B. Pace (2024) is shown as points with error bars.
Paper: Rest-frame Optical Spectroscopy of z ∼ 2 Quasars with Steep Hard X-Ray Spectral Shapes: X-Ray Selection of Super-Eddington Accretion and Verification
Authors: Y. Chen, B. Luo, J. Huang
Figure caption: Rest-frame optical spectra for our nine targets with their best-fit models. The positions of major emission lines are marked for reference. In the left panel, the broadband spectra are represented by the black curves, smoothed using box convolutions varying from 5 to 10 pixels. Light gray shaded areas represent the spectral error bars (i.e., the uncertainty range of the spectral data); the best-fit models generally fall within these error regions. The blue curves illustrate the best-fit continua + emission-line models. The orange curves depict the best-fit continua, and cyan curves represent the Fe II pseudocontinua. The light blue shaded regions mark the portions of the spectra that are strongly affected by telluric absorption (observed-frame 13550–15300 Å and 17800–21000 Å). The right panel shows zoomed-in views of the spectra in the Hβ region after subtraction of the continuum and the Fe II pseudocontinuum. The Hβ and [O III] emission lines are fitted with broad (red curves) and/or narrow (green curves) Gaussian components.
Paper: Rest-frame Optical Spectroscopy of z ∼ 2 Quasars with Steep Hard X-Ray Spectral Shapes: X-Ray Selection of Super-Eddington Accretion and Verification
Authors: Y. Chen, B. Luo, J. Huang
Figure caption: Chandra spectrum for J0806 overlaid with the best-fit simple power-law model. The bottom panel displays the residuals between the spectral data and the best-fit model, normalized by the errors.
Paper: Rest-frame Optical Spectroscopy of z ∼ 2 Quasars with Steep Hard X-Ray Spectral Shapes: X-Ray Selection of Super-Eddington Accretion and Verification
Authors: Y. Chen, B. Luo, J. Huang
Figure caption: Absolute i-band magnitude vs. redshift for our nine targets, represented by the red stars. The blue and green triangles represent the super-Eddington and sub-Eddington comparison samples drawn from B. M. Matthews et al. (2023). Our targets are, on average, less luminous than the GNIRS quasars.
Paper: Is Dark Energy Changing? Probing the Universe’s Expansion with Present and Future Astronomical Probes
Authors: Mehdi Rezaei, Supriya Pan, Weiqiang Yang, David F. Mota
Figure caption: One-dimensional marginalized posterior distributions and two-dimensional joint contours at 1σ and 2σ considering some of the model parameters are shown for flat Padé-II using the combined data sets SN+BAO+BBN+H(z), SN+BAO+BBN+H(z)+GW, SN+BAO+BBN+H(z)+CMB, and SN+BAO+BBN+H(z)+CMB+GW. The solid lines through w1 = 0 and w2 = 0 correspond to the ΛCDM cosmology, which is also considered as the fiducial model for generating the GW mock data set.