adsabs/AstroCLIMB huggingface dataset:
Paper: A Deep Search for Ethylene Glycol and Glycolonitrile in the V883 Ori Protoplanetary Disk
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Tushar Suhasaria, Jenny K. Calahan, Jane Huang, Merel L. R. van 't Hoff
Figure caption: The top and lower left panels show the integrated intensity map and the intensity-weighted velocity for EG. The top and lower right panels show the same for GN. We only included that data above 0.005 Jy beam−1 in the moment maps. Gray contours in the intensity-weighted velocity maps represent 1σ, 3σ, 5σ, and 7σ, where σ = 0.005 Jy beam−1 channel−1, integrated over 10 channels. The beam size is shown in the lower left of each panel. The moment 0 maps for EG and GN were generated by summing the following transitions (EG: 350.70, 351.02, 351.30, and 351.81 GHz; GN: 348.19 and 362.22 GHz). The moment 1 maps were generated by averaging the same transitions used for moment 0 maps. The HNC detection at 362.63 GHz is shown for comparison.
Paper: A Deep Search for Ethylene Glycol and Glycolonitrile in the V883 Ori Protoplanetary Disk
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Tushar Suhasaria, Jenny K. Calahan, Jane Huang, Merel L. R. van 't Hoff
Figure caption: The best-fit model of the detected transitions of ﹩{{\rm{g}}}^{{\prime} }{\rm{Gg}}-{({{\rm{CH}}}_{2}{\rm{OH}})}_{2}﹩ is shown in green, and ﹩{{\rm{HOCH}}}_{2}{\rm{CN}}﹩ is shown in orange. These are plotted on top of the data, which is shown in black, along with the summed spectra of the other detected molecules by A. M. A. Fadul et al. (2025), shown in blue. The dotted and dashed gray line indicates the noise level in the data (corresponding to 1σ and 3σ).
Paper: CAPERS Observations of Two UV-bright Galaxies at z > 10. More Evidence for Bursting Star Formation in the Early Universe
Authors: Vasily Kokorev, Óscar A. Chávez Ortiz, Anthony J. Taylor, Steven L. Finkelstein, Pablo Arrabal Haro, Mark Dickinson, John Chisholm, Seiji Fujimoto, Julian B. Mu noz, Ryan Endsley, Weida Hu, Lorenzo Napolitano, Stephen M. Wilkins, Hollis B. Akins, Ricardo Amoriín, Caitlin M. Casey, Yingjie Cheng, Nikko J. Cleri, Justin Cole, Fergus Cullen, Emanuele Daddi, Kelcey Davis, Callum T. Donnan, James S. Dunlop, Vital Fernández, Mauro Giavalisco, Norman A. Grogin, Nimish Hathi, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Ho-Hin Leung, Ray A. Lucas, Derek McLeod, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Rachel S. Somerville, Xin Wang, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Bursting star formation of bright z > 10 galaxies. The ratio between SFR10 and SFR100 as a function of the age of the Universe is shown. Alongside the CAPERS (red) galaxies, we show all the literature results for MUV < −20 high-z galaxies, which report on the recent SFR (A. J. Bunker et al. 2023; T. Y.-Y. Hsiao et al. 2024a, 2024b; J. Álvarez-Márquez et al. 2025; S. Carniani et al. 2024; S. Fujimoto et al. 2024; L. Napolitano et al. 2025). The CEERS high-z galaxies presented in P. Arrabal Haro et al. (2023a, 2023b), and bright z ∼ 10 galaxies presented in L. Napolitano et al. (2025) and S. Fujimoto et al. (2024) do not have a reported SFR10, and were thus fit with the same BAGPIPES setup as discussed in Section 3.4. In the right panel we show the median and scatter of burstiness derived from bootstrapping, accounting for the uncertainty of each measurement for all the available data. We additionally show results from the power-spectrum distribution (PSD) toy model (maroon) and hydrodynamical simulations (FLARES; C. C. Lovell et al. 2021; S. M. Wilkins et al. 2023a, 2023b, in green) of burstiness at high z, where the median and scatter are shown with solid and dashed lines, respectively. Finally, in the subpanel on the left we show medians (solid lines) and 68% confidence intervals (shaded regions) of observational constraints on burstiness of bright z ∼ 6 galaxies from R. Endsley et al. (2024b) and J. W. Cole et al. (2025).
Paper: CAPERS Observations of Two UV-bright Galaxies at z > 10. More Evidence for Bursting Star Formation in the Early Universe
Authors: Vasily Kokorev, Óscar A. Chávez Ortiz, Anthony J. Taylor, Steven L. Finkelstein, Pablo Arrabal Haro, Mark Dickinson, John Chisholm, Seiji Fujimoto, Julian B. Mu noz, Ryan Endsley, Weida Hu, Lorenzo Napolitano, Stephen M. Wilkins, Hollis B. Akins, Ricardo Amoriín, Caitlin M. Casey, Yingjie Cheng, Nikko J. Cleri, Justin Cole, Fergus Cullen, Emanuele Daddi, Kelcey Davis, Callum T. Donnan, James S. Dunlop, Vital Fernández, Mauro Giavalisco, Norman A. Grogin, Nimish Hathi, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Ho-Hin Leung, Ray A. Lucas, Derek McLeod, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Rachel S. Somerville, Xin Wang, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: CAPERS high-z sources. Top: JWST/NIRCam and MIRI F770W 2﹩\mathop{.}\limits^{^{\prime\prime} }﹩0 image stamps and red–green–blue (RGB) long-wavelength color images comprised of the F277W, F356W, and F444W bands, respectively. The MSA slitlet layout (white) is overlaid on the RGB composite (F277W + F356W + F444W) image. Each panel shows the total magnitude as presented in the photometric catalog. The spectrum of CAPERS_UDS_z11 was processed with an alternative nodding pattern (see end of Section 2.3), to remove the impact of the companion source on the final spectrum. Middle: 2D MSA PRISM spectrum. Bottom: 1D spectra of CAPERS galaxies in the observed frame. We show the spectroscopic data in black, while the 1σ uncertainty on the spectrum is in dashed red. Best-fit BAGPIPES model is shown in solid blue, with its uncertainty highlighted by a shaded region. NIRCam photometry is shown with square symbols. Further, we show the positions and label the prominent emission lines with significant (>3σ) detections as solid vertical lines. Emission lines for which we only obtain an upper limit are shown with dashed lines.
Paper: CAPERS Observations of Two UV-bright Galaxies at z > 10. More Evidence for Bursting Star Formation in the Early Universe
Authors: Vasily Kokorev, Óscar A. Chávez Ortiz, Anthony J. Taylor, Steven L. Finkelstein, Pablo Arrabal Haro, Mark Dickinson, John Chisholm, Seiji Fujimoto, Julian B. Mu noz, Ryan Endsley, Weida Hu, Lorenzo Napolitano, Stephen M. Wilkins, Hollis B. Akins, Ricardo Amoriín, Caitlin M. Casey, Yingjie Cheng, Nikko J. Cleri, Justin Cole, Fergus Cullen, Emanuele Daddi, Kelcey Davis, Callum T. Donnan, James S. Dunlop, Vital Fernández, Mauro Giavalisco, Norman A. Grogin, Nimish Hathi, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Ho-Hin Leung, Ray A. Lucas, Derek McLeod, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Rachel S. Somerville, Xin Wang, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: BAGPIPES posteriors and SFH for CAPERS_UDS_z10. Left: posterior probability distributions obtained with BAGPIPES for the nonparametric SFH fit. The columns (left to right) show the M*, SFR100, burstiness (defined as log10SFR10/SFR100), UV slope β, dust extinction AV, ionization parameter log10U, and the mass-weighted age. We plot the 1D posterior distributions of each parameter along the diagonal. In the 2D scatterplot we show the joint posterior distributions with contours representing the 1σ, 2σ, and 3σ intervals. Right: the best-fit nonparametric SFH. The shaded region shows the ±1σ uncertainty on the fit.
Paper: A Deep Search for Ethylene Glycol and Glycolonitrile in the V883 Ori Protoplanetary Disk
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Tushar Suhasaria, Jenny K. Calahan, Jane Huang, Merel L. R. van 't Hoff
Figure caption: The cumulative model for all species reported by A. M. A. Fadul et al. (2025) in blue, and the same cumulative model includes EG and GN in green. The black represents the observed spectra, and the gray dotted horizontal line represents the noise level, which corresponds to 1σ.
Paper: A Deep Search for Ethylene Glycol and Glycolonitrile in the V883 Ori Protoplanetary Disk
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Tushar Suhasaria, Jenny K. Calahan, Jane Huang, Merel L. R. van 't Hoff
Figure caption: Shows ethylene glycol spectra in steel blue overlaid on the observed spectra from ALMA Band 6 in black (J.-H. Jeong et al. 2025).
Paper: A Deep Search for Ethylene Glycol and Glycolonitrile in the V883 Ori Protoplanetary Disk
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Tushar Suhasaria, Jenny K. Calahan, Jane Huang, Merel L. R. van 't Hoff
Figure caption: Continuation of Figure 7.
Paper: CAPERS Observations of Two UV-bright Galaxies at z > 10. More Evidence for Bursting Star Formation in the Early Universe
Authors: Vasily Kokorev, Óscar A. Chávez Ortiz, Anthony J. Taylor, Steven L. Finkelstein, Pablo Arrabal Haro, Mark Dickinson, John Chisholm, Seiji Fujimoto, Julian B. Mu noz, Ryan Endsley, Weida Hu, Lorenzo Napolitano, Stephen M. Wilkins, Hollis B. Akins, Ricardo Amoriín, Caitlin M. Casey, Yingjie Cheng, Nikko J. Cleri, Justin Cole, Fergus Cullen, Emanuele Daddi, Kelcey Davis, Callum T. Donnan, James S. Dunlop, Vital Fernández, Mauro Giavalisco, Norman A. Grogin, Nimish Hathi, Michaela Hirschmann, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Ho-Hin Leung, Ray A. Lucas, Derek McLeod, Casey Papovich, Laura Pentericci, Pablo G. Pérez-González, Rachel S. Somerville, Xin Wang, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: BAGPIPES posteriors and SFH for CAPERS_UDS_z11. Same as Figure 2.
Paper: A Deep Search for Ethylene Glycol and Glycolonitrile in the V883 Ori Protoplanetary Disk
Authors: Abubakar M. A. Fadul, Kamber R. Schwarz, Tushar Suhasaria, Jenny K. Calahan, Jane Huang, Merel L. R. van 't Hoff
Figure caption: Glycolonitrile ﹩{{\rm{HOCH}}}_{2}{\rm{CN}}﹩.
Paper: Formation of Supersonic Turbulence in the Primordial Star-forming Cloud
Authors: Ke-Jung Chen, Meng-Yuan Ho, Pei-Cheng Tung
Figure caption: Physical properties of a primordial halo. From top to bottom, left to right, panels show the gas density, dark matter distribution, gas temperature, and ﹩{ \mathcal M }﹩ at the end of the simulation. The dashed circle marks the inner region of the halo with a radius of 100 pc. The gas density morphology closely traces the underlying dark matter structure, with dense gas regions coinciding with concentrations of dark matter. The central high-density gas exhibits lower temperatures, primarily due to efficient cooling by molecular hydrogen.
Paper: Formation of Supersonic Turbulence in the Primordial Star-forming Cloud
Authors: Ke-Jung Chen, Meng-Yuan Ho, Pei-Cheng Tung
Figure caption: Density evolution during the assembly of a minihalo. Panels from left to right show snapshots at different stages of the evolution. The streamlines illustrate the direction of gas flow. The initially diffuse and featureless gas distribution rapidly evolves into a concentrated gas cloud as the minihalo forms. Filamentary and clumpy structures emerge within the cloud, likely driven by anisotropic accretion flows of primordial gas.
Paper: Formation of Supersonic Turbulence in the Primordial Star-forming Cloud
Authors: Ke-Jung Chen, Meng-Yuan Ho, Pei-Cheng Tung
Figure caption: Morphology of a primordial minihalo at z = 18.78. The series of panels shows successive zoom-ins of the gas density from a scale of 40 kpc down to the inner 4 pc of the targeted halo. Clumpy structures become increasingly prominent at smaller scales. In the 4 pc panel, the central region exhibits an elongated dense clump surrounded by a tail of circularly streaming gas, highlighting the complex, anisotropic dynamics within the collapsing core.
Paper: Formation of Supersonic Turbulence in the Primordial Star-forming Cloud
Authors: Ke-Jung Chen, Meng-Yuan Ho, Pei-Cheng Tung
Figure caption: Kinetic energy power spectrum of gas in the halo. The energy spectrum has a turning point at k ≈ k1, corresponding to a physical scale of 1063 pc—approximately 3 times the halo’s virial radius. When k > k1, the spectrum follows the Kolmogorov power-law scaling of k−5/3, indicative of a turbulent inertial cascade, down to k ≈ 50, which corresponds to a physical scale of about 2 pc.
Paper: Formation of Supersonic Turbulence in the Primordial Star-forming Cloud
Authors: Ke-Jung Chen, Meng-Yuan Ho, Pei-Cheng Tung
Figure caption: Gas temperature-density phase diagram at the end of the simulations. The gas density spans from 10−5 to 106 cm−3, corresponding to temperatures ranging from 10 to 104 K. For 10−5 < n < 10−2 cm−3, the temperature increases with density following adiabatic compression due to gas clustering via gravity. In contrast, for n > 10−2 cm−3, the temperature decreases as density increases, owing to efficient cooling by H2 and HD. The warm gas with T ∼ 104 K originates from shock-heated diffuse gas in the outer regions of the halo.
Paper: Formation of Supersonic Turbulence in the Primordial Star-forming Cloud
Authors: Ke-Jung Chen, Meng-Yuan Ho, Pei-Cheng Tung
Figure caption: 3D volume rendering of dense clumps at the center of the halo. Several dense clumps appear as yellow-red nuggets. At this stage, one of the clumps has surpassed the Jeans instability threshold and begun to collapse into a Population III star with a mass of approximately 8.07 M⊙.
Paper: Formation of Supersonic Turbulence in the Primordial Star-forming Cloud
Authors: Ke-Jung Chen, Meng-Yuan Ho, Pei-Cheng Tung
Figure caption: The gas mass fraction as a function of ﹩{ \mathcal M }﹩. It shows a peak at ﹩{ \mathcal M }﹩ ∼5.2, with a broad distribution spanning ﹩{ \mathcal M }﹩ ∼0.5 to 28.
Paper: Central Concentration and Escape of Ionizing Photons in Galaxies at the Epoch of Reionization
Authors: Cheqiu Lyu, Enci Wang, Junxian Wang, Cheng Jia, Jie Song, Yangyao Chen, Zeyu Chen, Haoran Yu, Chengyu Ma, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Photometric measurements and spectral energy distribution fitting for a representative galaxy (ID 45776) at zphot = 6.908 in the JADES GOODS-S field. Panel (a): multiband cutouts convolved to match the F444W PSF, with red circles marking the photometric annuli. Panel (b): RGB color composite image constructed from the F444W (R), F410M (G), and F356W (B) filters. The pixel resolution and cutout scale is 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩04 and 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩2, corresponding to ∼0.21 and ∼6.3 kpc at the target redshift, respectively. Panels (c) and (d): SED and 500 fitting model spectra generated with BAGPIPES, along with the corresponding star formation history. Panels (e)–(h): spatially resolved SEDs and fitted spectra for concentric annuli at pixel radii [0–1], [2–3], [4–5], and [6–7], respectively. Panels (i)–(l): star formation histories associated with the annuli shown in panels (e)–(h).
Paper: Central Concentration and Escape of Ionizing Photons in Galaxies at the Epoch of Reionization
Authors: Cheqiu Lyu, Enci Wang, Junxian Wang, Cheng Jia, Jie Song, Yangyao Chen, Zeyu Chen, Haoran Yu, Chengyu Ma, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Data selection and classification. Left: signal-to-noise ratio (S/N) distributions in the F356W, F410M, and F444W filters for all galaxies with [O III]λ5007 emission covered by the F410M filter. The black dashed line marks the adopted S/N threshold. Right: color–magnitude diagram color-coded by photometric redshift (zphot). Green-edged points indicate sources that meet the S/N selection criterion.
Paper: Central Concentration and Escape of Ionizing Photons in Galaxies at the Epoch of Reionization
Authors: Cheqiu Lyu, Enci Wang, Junxian Wang, Cheng Jia, Jie Song, Yangyao Chen, Zeyu Chen, Haoran Yu, Chengyu Ma, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Radial profiles of stellar mass projected surface density (Σ*, top left), SFR projected surface density (ΣSFR, top right), sSFR (bottom left), and mass-weighted age (bottom right). The light-green, green, and dark-green curves represent the median profiles of galaxies in three stellar mass bins. Shaded regions represent the 1σ uncertainties, calculated as ﹩1.253\times \sigma /\sqrt{n}﹩, where σ is the standard deviation of the valid data points within each radial bin, and n is the number of valid data points in that bin, also indicated at the bottom of the bottom-left panel. The gray shaded area indicates the range of the F444W PSF FWHM across the redshift range of our sample.
Paper: Central Concentration and Escape of Ionizing Photons in Galaxies at the Epoch of Reionization
Authors: Cheqiu Lyu, Enci Wang, Junxian Wang, Cheng Jia, Jie Song, Yangyao Chen, Zeyu Chen, Haoran Yu, Chengyu Ma, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Radial profiles of [O III]+Hβ equivalent width and corresponding ionized photon production efficiency (left), and UV continuum slope and corresponding ionized photon escape fraction (right) of our galaxy sample. The color scheme, line styles, and shaded regions follow those in Figure 5.
Paper: Central Concentration and Escape of Ionizing Photons in Galaxies at the Epoch of Reionization
Authors: Cheqiu Lyu, Enci Wang, Junxian Wang, Cheng Jia, Jie Song, Yangyao Chen, Zeyu Chen, Haoran Yu, Chengyu Ma, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Left: total UV continuum slope (β) as a function of stellar mass for our galaxy samples. Short lines denote the 16th and 84th percentile ranges for each galaxy. The side panel presents the β distribution along with kernel density estimation (KDE) curves. The blue dashed line marks the median value for galaxies at 5 < z < 7 from S. Mascia et al. (2025, Mascia+25). Yellow and magenta curves show KDE distributions from the JADES/GOODS-S and PRIMER samples in R. Begley et al. (2025, B+25). Right: rest-frame [O III]+Hβ equivalent width as a function of stellar mass. The black dashed line represents the linear fit of our sample. The symbol coding and histogram format follow those of the left panel. The magenta KDE curve represents the PRIMER+JADES sample from R. Begley et al. (2025, B+25).
Paper: Central Concentration and Escape of Ionizing Photons in Galaxies at the Epoch of Reionization
Authors: Cheqiu Lyu, Enci Wang, Junxian Wang, Cheng Jia, Jie Song, Yangyao Chen, Zeyu Chen, Haoran Yu, Chengyu Ma, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Left twelve panels: stacked JWST NIRCam imaging cutouts of the galaxy sample of three stellar mass bins. From left to right, the panels show the F356W, F410M, and F444W bands, followed by an RGB composite image. The physical resolution of the cutouts is 0.2 kpc pixel−1. Rightmost panels: radial surface brightness profiles (top) and flux ratio profiles (bottom) of stacked galaxies. The profiles for the F356W, F410M, and F444W bands are shown in blue, green, and red, respectively. The surface brightness has been calculated by assuming the average kiloparsec to arcsec scale at 〈z〉 ∼ 7.1166 of our sample. The gray shaded area indicates the range of the F444W PSF FWHM across the redshift range of our sample.
Paper: Central Concentration and Escape of Ionizing Photons in Galaxies at the Epoch of Reionization
Authors: Cheqiu Lyu, Enci Wang, Junxian Wang, Cheng Jia, Jie Song, Yangyao Chen, Zeyu Chen, Haoran Yu, Chengyu Ma, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Normalized nonparametric “continuity” star formation histories for each sample (left), and for each annulus across the entire sample (right). In both panels, the SFR and the SFR surface density (i.e., resolved SFR) are normalized to their values at the most recent time bin (0–3 Myr). Resolved SFHs for each sample in individual stellar mass bins are presented in Figure C1 in the Appendix.
Paper: Central Concentration and Escape of Ionizing Photons in Galaxies at the Epoch of Reionization
Authors: Cheqiu Lyu, Enci Wang, Junxian Wang, Cheng Jia, Jie Song, Yangyao Chen, Zeyu Chen, Haoran Yu, Chengyu Ma, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Stellar mass–SFR relation for our sample. Each point is color-coded by the galaxy’s photometric redshift (zphot). Short gray lines indicate the 16th and 84th percentile ranges. The solid black line shows the best-fit linear relation for our sample. For comparison, the gray dotted and dashed lines represent empirical main sequences of star-forming galaxies at 6 < z < 7 from L. Clarke et al. (2024) and at z ∼ 7 from P. Popesso et al. (2023), respectively.
Paper: Central Concentration and Escape of Ionizing Photons in Galaxies at the Epoch of Reionization
Authors: Cheqiu Lyu, Enci Wang, Junxian Wang, Cheng Jia, Jie Song, Yangyao Chen, Zeyu Chen, Haoran Yu, Chengyu Ma, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Similar to the right panel of Figure 7 but shown separately for three distinct samples of different stellar mass, as indicated in the bottom-left corner of each panel.
Paper: Central Concentration and Escape of Ionizing Photons in Galaxies at the Epoch of Reionization
Authors: Cheqiu Lyu, Enci Wang, Junxian Wang, Cheng Jia, Jie Song, Yangyao Chen, Zeyu Chen, Haoran Yu, Chengyu Ma, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Similar to Figure 6 but normalized by effective radius in the x-axis.
Paper: Central Concentration and Escape of Ionizing Photons in Galaxies at the Epoch of Reionization
Authors: Cheqiu Lyu, Enci Wang, Junxian Wang, Cheng Jia, Jie Song, Yangyao Chen, Zeyu Chen, Haoran Yu, Chengyu Ma, Jinyang Wang, Yifan Wang, Xu Kong
Figure caption: Similar to Figure 5 but normalized by effective radius in the x-axis.
Paper: On the Universality of the Split Monopole Black Hole Magnetosphere
Authors: S. Selvi, O. Porth, B. Ripperda, L. Sironi
Figure caption: Two-dimensional snapshots showing the evolution in each row for the dipole, offset dipole, quadrudipole, and octuquadrupole initial magnetic field configurations. The four leftmost panels in each row show the plasma magnetization σ. The BHs are shown by black circles and magnetic field lines by black arrows. The rightmost panels show the normalized radial magnetic field over the event horizon as a function of the cumulative surface coordinate at matching times.
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: Impact of MIRI on photometric redshift estimates. The data points indicate the relative difference between the derived photo-z values for the galaxies excluding MIRI (znoMIRI) and when including MIRI (zMIRI, Δz = (znoMIRI − zMIRI)/(1 + zMIRI)) as a function of znoMIRI. The rms values and outlier fractions are indicated in the top-left corner. Galaxies with spec-z values are further color-coded by the relative differences between spec-z values and znoMIRI, Δzspec = (znoMIRI − zspec)/(1 + zspec)). The red filled circles and open squares show LRDs, with the open squares indicating sources with spec-z values. The violin plots denote the median and 1σ confidence interval of Δz at each redshift bin.
Paper: JWST/MIRI Reveals the True Number Density of Massive Galaxies in the Early Universe
Authors: Tao Wang, Hanwen Sun, Luwenjia Zhou, Ke Xu, Cheng Cheng, Zhaozhou Li, Yangyao Chen, H. J. Mo, Avishai Dekel, Tiancheng Yang, Yijun Wang, Longyue Chen, Xianzhong Zheng, Zheng Cai, David Elbaz, Y.-S. Dai, J.-S. Huang
Figure caption: Comparison of our JWST/NIRCam F150W (aperture photometry using APHOT) and VISTA/H photometry (deblended photometry with TPHOT) with previous measurements by other teams. The color maps indicate the local density of data points. The HST/FI60W photometry is obtained from the CANDELS survey (H. Nayyeri et al. 2017), while the VISTA/H band photometry is obtained from the COSMOS2020 catalog (J. R. Weaver et al. 2022). The red dashed lines denote the median values of the magnitude differences, which are close to zero across a wide magnitude range.