adsabs/AstroCLIMB huggingface dataset:
Paper: The Potential for Long-lived Intermediate-mass Black Hole Binaries in the Lowest Density Dwarf Galaxies
Authors: Fazeel Mahmood Khan, Fiza Javed, Kelly Holley-Bockelmann, Lucio Mayer, Peter Berczik, Andrea V. Macciò
Figure caption: IMBH pair and binary evolution in our nonnucleated dwarf galaxy models. Top left: IMBH orbit semimajor axis. Top right: IMBH orbit eccentricity evolution. Bottom left: combined semimajor axis evolution from our N-body run and semianalytic estimates for the IMBH binary. Bottom right: combined eccentricity evolution from our N-body run and semianalytic estimates for the IMBH binary.
Paper: The Potential for Long-lived Intermediate-mass Black Hole Binaries in the Lowest Density Dwarf Galaxies
Authors: Fazeel Mahmood Khan, Fiza Javed, Kelly Holley-Bockelmann, Lucio Mayer, Peter Berczik, Andrea V. Macciò
Figure caption: Mass density profile of our dwarf galaxy sample at the end of the simulation run as described in Table 1. Central densities have dropped marginally for low Sérsic index models and substantially for high n and smaller effective radius models. For comparison, we have also plotted the initial profiles (dotted lines).
Paper: The Potential for Long-lived Intermediate-mass Black Hole Binaries in the Lowest Density Dwarf Galaxies
Authors: Fazeel Mahmood Khan, Fiza Javed, Kelly Holley-Bockelmann, Lucio Mayer, Peter Berczik, Andrea V. Macciò
Figure caption: Central stellar density required for an IMBH binary to merge within a Hubble time, if the host is a nonnucleated dwarf galaxy, as a function of eccentricity.
Paper: The Potential for Long-lived Intermediate-mass Black Hole Binaries in the Lowest Density Dwarf Galaxies
Authors: Fazeel Mahmood Khan, Fiza Javed, Kelly Holley-Bockelmann, Lucio Mayer, Peter Berczik, Andrea V. Macciò
Figure caption: IMBH binary hardening rates (model units) vs. density (model units) at the binary influence radius. The straight line shows the linear fit to the data.
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: Number density of massive quiescent galaxies as a function of redshift. The filled green star is the number density of the Blue Jay quiescent galaxies at z ∼ 2. We predict the number densities of massive quiescent galaxies at higher redshifts (z = 4–6) by tracing back the SFHs of our entire representative sample using the continuity prior, shown as empty green stars. We also show the predicted number densities based on the SFHs derived using the bursty prior as magenta arrows, and these estimates are likely the upper bounds. The true number densities at z > 4 would likely fall between the two estimates: n qsc ≈ (1.5–6.0) × 10−5 Mpc−3(z = 4–6), shown as the gray hatched region. The number densities of massive quiescent galaxies directly measured by other recent studies are also shown as different symbols: A. C. Carnall et al. (2023b; orange pentagons), K. M. L. Gould et al. (2023; brown squares), F. Valentino et al. (2023; yellow diamonds), and S. Alberts et al. (2024; gold triangles). We find that our predicted number densities at z > 3 are broadly consistent with the number densities measured at high redshifts.
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: Na I D absorption by neutral gas (left) and Hα and [N II]λ6550, λ6585 emission (right) of the 14 massive quiescent galaxies. The observed data divided by the best-fit stellar model are plotted for Na I D absorption, and for ionized gas emission the observed data subtracted by the best-fit model are shown. The background of each Na I D panel is color-coded by the offset of centroid velocity of the Na I D line (green: same as the galaxy systemic velocity; blue: blueshifted by at least ∼100 km s−1). Three Gaussian components are fitted for the ionized gas emission complex, each accounting for Hα and [N II]λ6550, λ6585 emission. We find that almost all massive quiescent galaxies (except for COSMOS-21477) show neutral gas probed by Na I D absorption. Most of the recently quenched galaxies (Group-2 and Group-3) show neutral gas outflows (blueshifted Na I D absorption) and ionized gas emissions with high [N II]/Hα ratios. This supports the scenario of AGN activities driving multiphase outflows, eventually leading to recent rapid quenching.
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: The formation redshift (z form) shown as a function of the observed redshift (z observed). Galaxies are color-coded by their stellar mass. The dashed curves indicate lookback times of 0.5, 1.0, 1.5, and 2.0 Gyr (or the “age” of a galaxy). The 14 Blue Jay massive quiescent galaxies are shown as circles with their IDs. Massive quiescent galaxies found at z > 3 collected from the literature are also plotted with different symbols.
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: Fraction of quiescent galaxies that are rapidly quenched (left) and PSBs (right) among massive (﹩\mathrm{log}({M}_{\star })/{M}_{\odot })\gt 10﹩) quiescent populations as a function of redshift. The RQs include PSBs. The green and blue circles show the fractions from the Blue Jay quiescent sample. The fractions at different redshifts from the literature are also shown with different symbols (summarized in Table 3). We find that approximately 60% (9/14) of our Blue Jay quiescent galaxies are rapidly quenched, and only 30% (4/14) are rapidly quenched after “major ” starbursts (PSBs). These fractions at z ∼ 2 agree well with the trend where the fraction of young quiescent galaxies increases with redshift.
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: Comparison of (a) the formation redshift (z form), (b) the quenching redshift (z quench), and (c) the light-weighted ages (in Gyr) of the 14 massive quiescent galaxies derived using the continuity and bursty SFH priors. The error bars indicate the 16th to 84th percentiles of the derived parameters. We find that the formation and quenching epochs and the light-weighted ages inferred using the two priors are broadly consistent.
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: Rest-frame UVJ diagram. Galaxies are color-coded by their light-weighted ages derived from Prospector fitting. Most of the 14 massive quiescent galaxies selected by sSFR (1 dex below the SFMS) would also be identified as quiescent by the rest-frame UVJ criterion. Two of the 14 galaxies, COSMOS-8469 and 18668, are outside the UVJ quiescent region but near its border.
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: Best-fit SED fitting to both observed photometry and spectrum. (a) Observed HST and NIRCam photometry in blue and green circles, respectively. The best-fit SED model is shown with the red line. (b) NIRSpec spectrum between 0.37 and 0.67 μm in the rest frame, shown with the sky-blue line. The green shaded region indicates the wavelength range used for fitting, and the spectrum data used for fitting are highlighted as the blue line. Both the observed spectrum and best-fit model are smoothed by 3 pixels. (c) Color-composite image in 5″ × 5″ box.
Paper: Widespread Rapid Quenching at Cosmic Noon Revealed by JWST Deep Spectroscopy
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Benjamin D. Johnson, Rebecca L. Davies, Joel Leja, Sandro Tacchella, J. Trevor Mendel, Chloë Benton, Letizia Bugiani, Razieh Emami, Amir H. Khoram, Yijia Li, Gabriel Maheson, Elijah P. Mathews, Rohan P. Naidu, Erica J. Nelson, Bryan A. Terrazas, Rainer Weinberger
Figure caption: Continued.
Paper: Acoustic Wake in a Singular Isothermal Profile: Dynamical Friction and Gravitational-wave Emission
Authors: Gali Eytan, Vincent Desjacques, Robin Buehler
Figure caption: Tangential (left panel) and radial (right panel) friction coefficients ﹩{I}_{\varphi }({ \mathcal M })﹩ and ﹩{I}_{r}({ \mathcal M })﹩ as a function of the Mach number ﹩{ \mathcal M }﹩ in the steady-state regime for a circularly moving perturber in an infinite homogeneous background. The dashed curves represent the contribution from the inner and outer regions (assuming ﹩{{\ell }}_{\max }=12﹩), whereas the (cyan) dotted and (green) dotted–dashed curves are the contribution from the ℓ = 0 and ℓ ≤ 1 multipoles, respectively. The data is from H. Kim & W.-T. Kim (2007; see text for details).
Paper: Acoustic Wake in a Singular Isothermal Profile: Dynamical Friction and Gravitational-wave Emission
Authors: Gali Eytan, Vincent Desjacques, Robin Buehler
Figure caption: Slice through the density profile of the acoustic wake for a static perturber (﹩{ \mathcal M }=0﹩). The unperturbed density is normalized to ρ 0(a) = 1. For the perturber, we have assumed a Bondi radius ﹩2{GM}/{c}_{s}^{2}=0.2a﹩, within which linear response theory is not reliable. Dotted (blue) lines indicate negative values (of δ ρ).
Paper: Acoustic Wake in a Singular Isothermal Profile: Dynamical Friction and Gravitational-wave Emission
Authors: Gali Eytan, Vincent Desjacques, Robin Buehler
Figure caption: Steady-state acoustic wake overdensity δ ρ/ρ 0 in the orbital plane of a perturber moving circularly with a Mach number of ﹩{ \mathcal M }=0.2﹩ (upper panels) and ﹩{ \mathcal M }=2﹩ (lower panels). The left panels display the dipole contribution, while the right panels show the acoustic wake for ﹩{{\ell }}_{\max }=8﹩. The mass M of the perturber, the sound speed, and the orbital radius a are chosen such that ϵ = 10−4 and 10−5 for ﹩{ \mathcal M }=0.2﹩ and 2, respectively. The perturber’s position is represented as a white symbol, and its circular orbit as a white circle.
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: Comparisons of parameters derived by the Sonora Elf Owl (Figure (a)) and ATMO2020++ (Figure (b)) models with spectra from different instruments vs. combined spectra. The parameters on the x-axis are obtained from the combined spectra (NIRSpec+MIRI), i.e., the values listed in Tables 3, 4, and 6. The y-axis shows the differences between parameters derived from NIRSpec-only and combined spectra (inverted triangles), as well as differences between MIRI-only and combined spectra (crosses). Larger data points indicate a greater number of overlapping objects at that position.
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: The marginalized posterior distribution of eight parameters for the observed spectra of WISEA J2159−48, using the Sonora Elf Owl models. The parameters are, in order, the logarithm of vertical eddy diffusion parameter ﹩\mathrm{log}{K}_{\mathrm{zz}}﹩, effective temperature T eff, surface gravity ﹩\mathrm{log}g﹩, metallicity [M/H], carbon-to-oxygen ratio C/O, wavelength correction parameters A  λ  and C  λ , and scaling factor ﹩\mathrm{log}({R}^{2}/{D}^{2})﹩.
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: The marginalized posterior distribution of six parameters for the observed spectra of WISEA J2159−48, using the ATMO2020++ models. The parameters are, in order, effective temperature T eff, surface gravity ﹩\mathrm{log}g﹩, metallicity [M/H], wavelength correction parameters A  λ  and C  λ , and scaling factor ﹩\mathrm{log}({R}^{2}/{D}^{2})﹩.
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: Comparisons between the original model spectra and the linearly interpolated spectra with the same parameters using the Sonora Elf Owl models. All six samples have ﹩\mathrm{log}{K}_{{zz}}=7﹩ [cm2 s−1], [M/H] = 0, and C/O = 0.458. Other parameters are provided at the top of each subfigure.
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: Surface gravity vs. effective temperature for dwarfs. These points in the gray circle are the objects from The UltracoolSheet. The points in the blue triangle are from our sample with the parameters derived using the ATMO2020++ models, while the red inverted triangles represent those parameters obtained using the Sonora Elf Owl models.
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: Spectral type vs. effective temperature for dwarfs. The data points represented by circles are sourced from The UltracoolSheet. The blue and green data points are our investigated brown dwarfs with physical parameters derived from the ATMO2020++ models. Different colored data points of the same shape represent data points in different ranges of surface gravity as shown in the legend.
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: Similar to Figure B1, but for CWISEP J1446−23 using the Sonora Elf Owl models.
Paper: Physical Parameters and Properties of 20 Cold Brown Dwarfs in JWST
Authors: Zhijun Tu, Shu Wang, Jifeng Liu
Figure caption: Similar to Figure B2, but for CWISEP J1446−23 using the ATMO2020++ models.
Paper: Medium Bands, Mega Science: A JWST/NIRCam Medium-band Imaging Survey of A2744
Authors: Katherine A. Suess, John R. Weaver, Sedona H. Price, Richard Pan, Bingjie Wang, 冰洁 王, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Ivo Labbé, Joel Leja, Christina C. Williams, Katherine E. Whitaker, Hakim Atek, Pratika Dayal, Anna de Graaff, Robert Feldmann, Marijn Franx, Yoshinobu Fudamoto, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Jenny E. Greene, Gourav Khullar, Vasily Kokorev, Mariska Kriek, Brian Lorenz, Danilo Marchesini, Michael V. Maseda, Jorryt Matthee, Tim B. Miller, Ikki Mitsuhashi, Lamiya A. Mowla, Adam Muzzin, Rohan P. Naidu, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, David J. Setton, Heath Shipley, Renske Smit, Justin S. Spilker, Pieter van Dokkum, Adi Zitrin
Figure caption: Example SEDs from UNCOVER (left) vs. MegaScience (center), as well as eazy-py photometric redshift distributions (right). SEDs are shown in f  ν  (in units of 1030 erg s−1 cm−2 Hz−1). Each object is spectroscopically confirmed by UNCOVER (top four objects; S. Price et al. 2024) or ALT (bottom two objects; R. P. Naidu et al. 2024, in preparation). Objects are ordered by increasing redshift; each is chosen to demonstrate one “failure mode” of SED fitting that is solved by the increased photometric coverage of MegaScience. Each example is discussed in additional detail in Section 3.1. HST photometry is plotted where available; IDs 61218 and 34713 lie outside of the HST area.
Paper: Medium Bands, Mega Science: A JWST/NIRCam Medium-band Imaging Survey of A2744
Authors: Katherine A. Suess, John R. Weaver, Sedona H. Price, Richard Pan, Bingjie Wang, 冰洁 王, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Ivo Labbé, Joel Leja, Christina C. Williams, Katherine E. Whitaker, Hakim Atek, Pratika Dayal, Anna de Graaff, Robert Feldmann, Marijn Franx, Yoshinobu Fudamoto, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Jenny E. Greene, Gourav Khullar, Vasily Kokorev, Mariska Kriek, Brian Lorenz, Danilo Marchesini, Michael V. Maseda, Jorryt Matthee, Tim B. Miller, Ikki Mitsuhashi, Lamiya A. Mowla, Adam Muzzin, Rohan P. Naidu, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, David J. Setton, Heath Shipley, Renske Smit, Justin S. Spilker, Pieter van Dokkum, Adi Zitrin
Figure caption: Comparison of photometric redshifts with a sample of ∼300 high-quality spectroscopic redshifts from the UNCOVER survey (S. Price et al. 2024). The top row shows our Prospector redshifts (for details, see B. Wang et al. 2024c), and the bottom row shows eazy-py redshifts based on photometry from the “SUPER” catalog (for details, see J. R. Weaver et al. 2024). The left column shows redshifts from the public DR2 UNCOVER data release, while the right column shows MegaScience redshifts from the DR3 public data products accompanying this paper. MegaScience shows nearly a factor-of-three reduction in σ NMAD, and close to a factor-of-two reduction in catastrophic outliers (as in J. R. Weaver et al. 2024, defined as objects with Δz/(1 + z spec) ≥ 0.15; shown by dotted red lines). Prospector and eazy-py show similar performance.
Paper: Medium Bands, Mega Science: A JWST/NIRCam Medium-band Imaging Survey of A2744
Authors: Katherine A. Suess, John R. Weaver, Sedona H. Price, Richard Pan, Bingjie Wang, 冰洁 王, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Ivo Labbé, Joel Leja, Christina C. Williams, Katherine E. Whitaker, Hakim Atek, Pratika Dayal, Anna de Graaff, Robert Feldmann, Marijn Franx, Yoshinobu Fudamoto, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Jenny E. Greene, Gourav Khullar, Vasily Kokorev, Mariska Kriek, Brian Lorenz, Danilo Marchesini, Michael V. Maseda, Jorryt Matthee, Tim B. Miller, Ikki Mitsuhashi, Lamiya A. Mowla, Adam Muzzin, Rohan P. Naidu, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, David J. Setton, Heath Shipley, Renske Smit, Justin S. Spilker, Pieter van Dokkum, Adi Zitrin
Figure caption: Schematic of the on-sky footprint of MegaScience and UNCOVER (left), other NIRCam and NIRISS imaging programs (center), and NIRCam grism programs (right); these programs are described in additional detail in the main text. The MegaScience footprint is shown in light blue in all three panels. A comparison with footprints of pre-JWST data, including HST and MUSE, is shown in R. Bezanson et al. (2024). For the UNCOVER parallel observations in the southeast of the image, we only show pointings that are included in the reduced mosaics released along with this paper (decl. > –30°28).
Paper: Medium Bands, Mega Science: A JWST/NIRCam Medium-band Imaging Survey of A2744
Authors: Katherine A. Suess, John R. Weaver, Sedona H. Price, Richard Pan, Bingjie Wang, 冰洁 王, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Ivo Labbé, Joel Leja, Christina C. Williams, Katherine E. Whitaker, Hakim Atek, Pratika Dayal, Anna de Graaff, Robert Feldmann, Marijn Franx, Yoshinobu Fudamoto, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Jenny E. Greene, Gourav Khullar, Vasily Kokorev, Mariska Kriek, Brian Lorenz, Danilo Marchesini, Michael V. Maseda, Jorryt Matthee, Tim B. Miller, Ikki Mitsuhashi, Lamiya A. Mowla, Adam Muzzin, Rohan P. Naidu, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, David J. Setton, Heath Shipley, Renske Smit, Justin S. Spilker, Pieter van Dokkum, Adi Zitrin
Figure caption: Examples of four galaxies in the A2744 cluster itself; each object uses the same arcsinh color stretch. While most cluster galaxies have low ongoing SFRs and relatively uniform colors (like the top object), the cluster also hosts several spectacular morphologically disturbed galaxies with strong Paα and 3.3 μm PAH emission. The white scale bar shows 0.″5, and emission lines are labeled with red, green, or blue text depending on which filter they are expected to fall into.
Paper: Medium Bands, Mega Science: A JWST/NIRCam Medium-band Imaging Survey of A2744
Authors: Katherine A. Suess, John R. Weaver, Sedona H. Price, Richard Pan, Bingjie Wang, 冰洁 王, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Ivo Labbé, Joel Leja, Christina C. Williams, Katherine E. Whitaker, Hakim Atek, Pratika Dayal, Anna de Graaff, Robert Feldmann, Marijn Franx, Yoshinobu Fudamoto, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Jenny E. Greene, Gourav Khullar, Vasily Kokorev, Mariska Kriek, Brian Lorenz, Danilo Marchesini, Michael V. Maseda, Jorryt Matthee, Tim B. Miller, Ikki Mitsuhashi, Lamiya A. Mowla, Adam Muzzin, Rohan P. Naidu, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, David J. Setton, Heath Shipley, Renske Smit, Justin S. Spilker, Pieter van Dokkum, Adi Zitrin
Figure caption: PSF growth curves for each filter added to UNCOVER before (top) and after (bottom) matching to F444W. After matching, all filters have deviations below the 1% level at the smallest aperture diameter used (0.″32). Growth curves are shown relative to the F444W growth curve; a value of 1 indicates perfect matching with F444W. Dashed lines indicate the ±1% deviations from exact matching (solid black line). Dotted lines indicate the locations of the 0.″32 and 0.″70 aperture diameters.
Paper: Medium Bands, Mega Science: A JWST/NIRCam Medium-band Imaging Survey of A2744
Authors: Katherine A. Suess, John R. Weaver, Sedona H. Price, Richard Pan, Bingjie Wang, 冰洁 王, Rachel Bezanson, Gabriel Brammer, Sam E. Cutler, Ivo Labbé, Joel Leja, Christina C. Williams, Katherine E. Whitaker, Hakim Atek, Pratika Dayal, Anna de Graaff, Robert Feldmann, Marijn Franx, Yoshinobu Fudamoto, Seiji Fujimoto, Lukas J. Furtak, Andy D. Goulding, Jenny E. Greene, Gourav Khullar, Vasily Kokorev, Mariska Kriek, Brian Lorenz, Danilo Marchesini, Michael V. Maseda, Jorryt Matthee, Tim B. Miller, Ikki Mitsuhashi, Lamiya A. Mowla, Adam Muzzin, Rohan P. Naidu, Themiya Nanayakkara, Erica J. Nelson, Pascal A. Oesch, David J. Setton, Heath Shipley, Renske Smit, Justin S. Spilker, Pieter van Dokkum, Adi Zitrin
Figure caption: Examples of galaxies at cosmic noon, 1 ≲ z ≲ 3. Color images are shown on a linear stretch; the white scale bar shows 0.″5, which corresponds to ∼4 kpc at these redshifts. Emission lines are labeled with red, green, or blue text, depending on which filter they are expected to fall into.