adsabs/AstroCLIMB huggingface dataset:
Paper: Morphological Evidence for the eROSITA Bubbles Being Giant and Distant Structures
Authors: Teng Liu, 腾 刘, Andrea Merloni, Jeremy Sanders, Gabriele Ponti, Andrew Strong, Michael C. H. Yeung, Nicola Locatelli, Peter Predehl, Xueying Zheng, Manami Sasaki, Michael Freyberg, Konrad Dennerl, Werner Becker, Kirpal Nandra, Martin Mayer, Johannes Buchner
Figure caption: Panel (c) displays the eROSITA X-ray RGB image published in Predehl et al. (2020). Panels (a) and (b) display respectively the total N H map and the high-frequency N H map, which is calculated by subtracting the low-frequency map (white contours) from the total N H map. Panel (d) displays the Ve22 dust extinction map in the distance range 400–1000 pc. The regions of G33+25 and G19+18 are marked with two big white circles. All the extinction and N H maps use a rainbow color map, where purple indicates large values. The contours of the high-frequency N H map are overplotted on the X-ray image and the extinction map in white, and in the former case we removed some small patches of the contours for the clarity of the X-ray image. Panel (e) displays the Le22 (upper) and Ve22 (lower) distance profiles of extinction in the 12 positions that are marked on the N H and extinction maps with 1°-diameter circles, separating the positions into two groups for clarity.
Paper: Morphological Evidence for the eROSITA Bubbles Being Giant and Distant Structures
Authors: Teng Liu, 腾 刘, Andrea Merloni, Jeremy Sanders, Gabriele Ponti, Andrew Strong, Michael C. H. Yeung, Nicola Locatelli, Peter Predehl, Xueying Zheng, Manami Sasaki, Michael Freyberg, Konrad Dennerl, Werner Becker, Kirpal Nandra, Martin Mayer, Johannes Buchner
Figure caption: Panels (N0), (N1), (N2), and (N3) display the northwestern bubble border in terms of the X-ray RGB image (Predehl et al. 2020), the SPASS polarized intensity map, and Stokes U and Q maps. Five sections of the border in this field are marked with white or blue strips (A, B, C, D, and E) with a width of 2°. The LPC is marked by a red circle in panel (N0). Panels (S0) and (S1) display the southwestern bright rim in terms of X-ray RGB image (Predehl et al. 2020) and the SPASS polarized intensity map. The position of the radio rim is marked with a white strip with a width of 2°.
Paper: Chemical Diagnostics to Unveil Environments Enriched by First Stars
Authors: Irene Vanni, Stefania Salvadori, Valentina D'Odorico, George D. Becker, Guido Cupani
Figure caption: The same as Figure 1 but for environments whose metals have been inherited: uniquely by PISNe/other Pop III SNe (red/blue solid line, f PopIII = 1); mainly by PISNe/other Pop III SNe but also by normal Pop II SNe (red/blue dashed lines, f PopIII ≥ 0.6); mainly by normal Pop II SNe but also by PISNe/other Pop III SNe (brown/gray dotted lines, f PopIII ≤ 0.5).
Paper: Chemical Diagnostics to Unveil Environments Enriched by First Stars
Authors: Irene Vanni, Stefania Salvadori, Valentina D'Odorico, George D. Becker, Guido Cupani
Figure caption: The same as Figure 2. The yellow star and shaded area are the abundances of Xing et al.'s (2023) star: the possible pure PISN descendant.
Paper: Chemical Diagnostics to Unveil Environments Enriched by First Stars
Authors: Irene Vanni, Stefania Salvadori, Valentina D'Odorico, George D. Becker, Guido Cupani
Figure caption: Abundance pattern of the absorber J1018+0548 (Saccardi et al. 2023; black crosses) compared with the two best-fitting models predicting an enrichment from: (i) a PISN and a Pop III SN (red); (ii) two Pop III SNe (blue).
Paper: Chemical Diagnostics to Unveil Environments Enriched by First Stars
Authors: Irene Vanni, Stefania Salvadori, Valentina D'Odorico, George D. Becker, Guido Cupani
Figure caption: Transitions detected at z = 6.2897 in the X-Shooter spectrum of UHS J0439+1634. The observed flux is plotted as a gray histogram with 1σ error bars plotted for each pixel; the Voigt profile model is plotted as a blue solid line. This figure can be compared with Figure B.45 in Christensen et al. (2023), noting the different velocity scale.
Paper: Chemical Diagnostics to Unveil Environments Enriched by First Stars
Authors: Irene Vanni, Stefania Salvadori, Valentina D'Odorico, George D. Becker, Guido Cupani
Figure caption: Same as Figure 2, but the chemical abundances are inherited by only PISNe (solid red), only other Pop III SNe (solid blue), and a single PISN but also another Pop III SN in different proportions (≥60% PISN: solid orange; ≤50% PISN: solid green). We show also the chemical abundances predicted for environments enriched mainly by PISNe but also by Pop II SNe (f PopIII ≥ 0.6, dashed red) and mainly by Pop II SNe but also by PISNe (f PopIII ≤ 0.5, dotted gray; see Figures 2–3).
Paper: Chemical Diagnostics to Unveil Environments Enriched by First Stars
Authors: Irene Vanni, Stefania Salvadori, Valentina D'Odorico, George D. Becker, Guido Cupani
Figure caption: Transitions detected at z = 7.368 in the X-Shooter spectrum of ULAS J1342+0928. The lines are the same as in Figure 5. This figure can be compared with Figure B.59 in Christensen et al. (2023), noting the different velocity scale.
Paper: Chemical Diagnostics to Unveil Environments Enriched by First Stars
Authors: Irene Vanni, Stefania Salvadori, Valentina D'Odorico, George D. Becker, Guido Cupani
Figure caption: Transitions detected at z = 7.4434 in the X-Shooter spectrum of ULAS J1342+0928. The lines are the same as in Figure 5. This figure can be compared with Figure B.60 in Christensen et al. (2023), noting the different velocity scale.
Paper: Chemical Diagnostics to Unveil Environments Enriched by First Stars
Authors: Irene Vanni, Stefania Salvadori, Valentina D'Odorico, George D. Becker, Guido Cupani
Figure caption: The same as Figure 3, but with the additional models described in the caption of Figure 8.
Paper: Chemical Diagnostics to Unveil Environments Enriched by First Stars
Authors: Irene Vanni, Stefania Salvadori, Valentina D'Odorico, George D. Becker, Guido Cupani
Figure caption: Minimum relative reduced chi square computed fitting the abundances of J1018+0548 for models with different f PopIII and different initial masses of the SN that explodes first, M PopIII or M 1.
Paper: Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER
Authors: Sam E. Cutler, Katherine E. Whitaker, John R. Weaver, Bingjie Wang, 冰洁 王, Richard Pan, Rachel Bezanson, Lukas J. Furtak, Ivo Labbe, Joel Leja, Sedona H. Price, Yingjie Cheng, Maike Clausen, Fergus Cullen, Pratika Dayal, Anna de Graaff, Mark Dickinson, James S. Dunlop, Robert Feldmann, Marijn Franx, Mauro Giavalisco, Karl Glazebrook, Jenny E. Greene, Norman A. Grogin, Garth Illingworth, Anton M. Koekemoer, Vasily Kokorev, Danilo Marchesini, Michael V. Maseda, Tim B. Miller, Themiya Nanayakkara, Erica J. Nelson, David J. Setton, Heath Shipley, Katherine A. Suess
Figure caption: Center top and middle: the quiescent galaxy size–mass relation changes significantly at low masses. Quiescent size–mass relations in both JWST/NIRCam F150W (top) and F444W (middle) are shown with blue triangles, purple squares, and red circles indicating the individual sizes of 30 < t 50 < 100, 100 < t 50 < 500, and t 50 > 500 Myr quiescent galaxies, respectively. Light gray error bars indicate the 1σ uncertainty on size and mass for galaxies in the sample. Solid gray contours and thick black lines indicate the 1 < z < 3 HST/WFC3 F160W sizes of galaxies from COSMOS-DASH (Cutler et al. 2022), while cyan lines represent the 1.5 < z < 2.0 quiescent size–mass relation from Nedkova et al. (2021). Open pentagons show the median size–mass of local dwarf satellites from Carlsten et al. (2021). Thin black dotted lines show the F160W HWHM and black shading shows the F444W HWHM at z = 2. The 50% mass-completeness detection limits of the combined PRIMER and UNCOVER sample for t 50 > 100 and >500 Myr quiescent galaxies are indicated with dark and light brown shading, respectively. Marginal histograms show the 1D distributions of galaxy mass and size. Center bottom: the ratio of F444W to F150W sizes exhibiting comparable trends to the Suess et al. (2022a) color gradients (thin black line). Left and Right: F444W–F277W–F150W color images for example low-mass (left) and massive (right) galaxies in our sample highlight the morphological differences between these mass regimes. Galaxies are ordered from top-left to bottom-right by increasing F150W size (in kiloparsecs) and the boundaries of the cutouts are highlighted in blue, purple, or red according to the median stellar age of the galaxy (as in Figure 2).
Paper: Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER
Authors: Sam E. Cutler, Katherine E. Whitaker, John R. Weaver, Bingjie Wang, 冰洁 王, Richard Pan, Rachel Bezanson, Lukas J. Furtak, Ivo Labbe, Joel Leja, Sedona H. Price, Yingjie Cheng, Maike Clausen, Fergus Cullen, Pratika Dayal, Anna de Graaff, Mark Dickinson, James S. Dunlop, Robert Feldmann, Marijn Franx, Mauro Giavalisco, Karl Glazebrook, Jenny E. Greene, Norman A. Grogin, Garth Illingworth, Anton M. Koekemoer, Vasily Kokorev, Danilo Marchesini, Michael V. Maseda, Tim B. Miller, Themiya Nanayakkara, Erica J. Nelson, David J. Setton, Heath Shipley, Katherine A. Suess
Figure caption: The rest-frame colors and star formation properties of the 333 quiescent galaxies at 1 < z < 3 with ﹩\mathrm{log}({M}_{\star }/{M}_{\odot })\lt 11﹩, as defined in Section 2. Sources are identified as t 50 > 500 Myr quiescent (circles), 100–500 Myr quiescent (black-outlined squares), or 30–100 Myr quenched galaxies (triangles), respectively, relative to the parent sample at 1 < z < 3 (small gray points). The left panel shows rest-frame UVJ colors from best-fit SPS models, with an inset (center) to show more detail, colored by ΔMS10 (Equation (3)). Solid black and dotted lines show the UVJ selections for general quiescent galaxies and cuts selecting galaxies of varying median age, respectively. The degree of quiescence for the sample is captured by the difference in SFR relative to the average SFMS (dashed line), ΔMS10, colored by the SFR at 10 Myr (right). Galaxies 0.5 dex below the SFMS (dotted line) are considered quenched. Sources marked with black x's are potential contaminants and have been removed from the sample.
Paper: Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER
Authors: Sam E. Cutler, Katherine E. Whitaker, John R. Weaver, Bingjie Wang, 冰洁 王, Richard Pan, Rachel Bezanson, Lukas J. Furtak, Ivo Labbe, Joel Leja, Sedona H. Price, Yingjie Cheng, Maike Clausen, Fergus Cullen, Pratika Dayal, Anna de Graaff, Mark Dickinson, James S. Dunlop, Robert Feldmann, Marijn Franx, Mauro Giavalisco, Karl Glazebrook, Jenny E. Greene, Norman A. Grogin, Garth Illingworth, Anton M. Koekemoer, Vasily Kokorev, Danilo Marchesini, Michael V. Maseda, Tim B. Miller, Themiya Nanayakkara, Erica J. Nelson, David J. Setton, Heath Shipley, Katherine A. Suess
Figure caption: In general, physical parameters differ dramatically between low- and high-mass quiescent galaxies, though R  e  and q alone are not sufficient to separate these samples. Smoothed histograms showing distributions of age, mass, and structural parameters (R  e , n, q) for F150W (top) and F444W (bottom). Individual distributions of 30 < t 50 < 100, 100 < t 50 < 500, and t 50 > 500 Myr quiescent galaxies are shown with blue, purple, and red curves, respectively, while the total distribution is shown with a gray-shaded curve. p-values for total-sample KS tests are shown, with bold values indicating that the parameter distribution is significantly different from a single Gaussian distribution.
Paper: Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER
Authors: Sam E. Cutler, Katherine E. Whitaker, John R. Weaver, Bingjie Wang, 冰洁 王, Richard Pan, Rachel Bezanson, Lukas J. Furtak, Ivo Labbe, Joel Leja, Sedona H. Price, Yingjie Cheng, Maike Clausen, Fergus Cullen, Pratika Dayal, Anna de Graaff, Mark Dickinson, James S. Dunlop, Robert Feldmann, Marijn Franx, Mauro Giavalisco, Karl Glazebrook, Jenny E. Greene, Norman A. Grogin, Garth Illingworth, Anton M. Koekemoer, Vasily Kokorev, Danilo Marchesini, Michael V. Maseda, Tim B. Miller, Themiya Nanayakkara, Erica J. Nelson, David J. Setton, Heath Shipley, Katherine A. Suess
Figure caption: The size–mass relation for galaxies in our sample colored based on the axis ratio (left) and Sérsic index (right) for both F150W (top) and F444W (bottom). Galaxies in the flattened part of the size–mass relation have smaller axis ratios and Sérsic indices. Individual points have the same shape symbols as Figure 3. Large circles indicate the median size–mass for a given stellar mass bin, color-coded by the median axis ratio or Sérsic index. The median axis ratio and Sérsic index are also shown numerically in each point. Typical error bars on the axis ratio are ±0.10 at ﹩\mathrm{log}({M}_{\star }/{M}_{\odot })\lt 10﹩ and ±0.04 at higher masses. For the Sérsic index, error bars are typically ±0.4.
Paper: Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER
Authors: Sam E. Cutler, Katherine E. Whitaker, John R. Weaver, Bingjie Wang, 冰洁 王, Richard Pan, Rachel Bezanson, Lukas J. Furtak, Ivo Labbe, Joel Leja, Sedona H. Price, Yingjie Cheng, Maike Clausen, Fergus Cullen, Pratika Dayal, Anna de Graaff, Mark Dickinson, James S. Dunlop, Robert Feldmann, Marijn Franx, Mauro Giavalisco, Karl Glazebrook, Jenny E. Greene, Norman A. Grogin, Garth Illingworth, Anton M. Koekemoer, Vasily Kokorev, Danilo Marchesini, Michael V. Maseda, Tim B. Miller, Themiya Nanayakkara, Erica J. Nelson, David J. Setton, Heath Shipley, Katherine A. Suess
Figure caption: 30 < t 50 < 100 quenched (blue triangles), 100 < t 50 < 500 quiescent (purple squares), and t 50 > 500 Myr quiescent galaxies (red circles) have fundamentally different spectral shapes. Composite SEDs are shown with large points while individual photometric data is shown with small points. Error bars show the standard error in the mean. Composite SED points are only shown in wavelength bins that contain >1% of the total number of photometric points for a given subsample.
Paper: Two Distinct Classes of Quiescent Galaxies at Cosmic Noon Revealed by JWST PRIMER and UNCOVER
Authors: Sam E. Cutler, Katherine E. Whitaker, John R. Weaver, Bingjie Wang, 冰洁 王, Richard Pan, Rachel Bezanson, Lukas J. Furtak, Ivo Labbe, Joel Leja, Sedona H. Price, Yingjie Cheng, Maike Clausen, Fergus Cullen, Pratika Dayal, Anna de Graaff, Mark Dickinson, James S. Dunlop, Robert Feldmann, Marijn Franx, Mauro Giavalisco, Karl Glazebrook, Jenny E. Greene, Norman A. Grogin, Garth Illingworth, Anton M. Koekemoer, Vasily Kokorev, Danilo Marchesini, Michael V. Maseda, Tim B. Miller, Themiya Nanayakkara, Erica J. Nelson, David J. Setton, Heath Shipley, Katherine A. Suess
Figure caption: Quiescent galaxies at cosmic noon separate into two distinct populations in age–mass space. Median stellar age is computed from the color-estimated t 50 (Equation (2)). Triangles, squares, and circles (along with blue, purple, and red bars on the left) indicate the 30 < t 50 < 100 quenched, 100 < t 50 < 500 quiescent, and t 50 > 500 Myr quiescent galaxy subsamples, respectively. Points are colored according to their F150W effective radii.
Paper: JWST’s First Glimpse of a z > 2 Forming Cluster Reveals a Top-heavy Stellar Mass Function
Authors: Hanwen Sun, Tao Wang, Ke Xu, Emanuele Daddi, Qing Gu, Tadayuki Kodama, Anita Zanella, David Elbaz, Ichi Tanaka, Raphael Gobat, Qi Guo, Jiaxin Han, Shiying Lu, Luwenjia Zhou
Figure caption: Left panel: the projected stellar mass density profile of J1001 compared with the best-fit projected NFW profiles at lower redshifts given by van der Burg et al. (2014, 2015). Following van der Burg et al. (2015), the original results with dimensionless units are converted to have physical units by assuming M 200 = 3 × 1014 M ⊙ at z ∼ 1 and M 200 = 9 × 1014  M ⊙ at z ∼ 0.15. Field level is given by galaxies with 2.483 < z phot < 2.519 from the COSMOS2020 catalog (Weaver et al. 2022). The vertical dotted line shows the R 200 of J1001. Middle panel: similar to the left panel, but the number density profiles are shown. Right panel: the redshift evolution of the concentration of cluster-galaxy number density profiles from observations (filled circles) and of the density profile of massive (M  h  = 1014  M ⊙) dark matter halos (dotted line) based on simulations from Duffy et al. (2008).
Paper: JWST’s First Glimpse of a z > 2 Forming Cluster Reveals a Top-heavy Stellar Mass Function
Authors: Hanwen Sun, Tao Wang, Ke Xu, Emanuele Daddi, Qing Gu, Tadayuki Kodama, Anita Zanella, David Elbaz, Ichi Tanaka, Raphael Gobat, Qi Guo, Jiaxin Han, Shiying Lu, Luwenjia Zhou
Figure caption: Left: the red, green, and blue (RGB) composite color image of J1001. The R, G, and B channels of the image correspond respectively to the NIRCam/F444W, F277W, and F115W bands. The large blue square indicates the region covered by Subaru/MOIRCS narrowband imaging targeting HAEs. All member galaxies are marked with open circles, with massive HAEs, less massive HAEs, non-HAE SF members, and quiescent members denoted in yellow, cyan, green, and red, respectively. Right: JWST/NIRCam RGB and HST/F160W images of the four HST-dark red members (circles) and their companions (crosses).
Paper: JWST’s First Glimpse of a z > 2 Forming Cluster Reveals a Top-heavy Stellar Mass Function
Authors: Hanwen Sun, Tao Wang, Ke Xu, Emanuele Daddi, Qing Gu, Tadayuki Kodama, Anita Zanella, David Elbaz, Ichi Tanaka, Raphael Gobat, Qi Guo, Jiaxin Han, Shiying Lu, Luwenjia Zhou
Figure caption: Upper panel: the relative transmission curve of the NB2300 filter. The redshift range of HAEs is given by the FWHM range of this filter. Lower panel: the color–magnitude diagram used to select HAEs. The red stars, blue circles, and gray points are HAEs, spectroscopically confirmed members and interlopers, respectively. The magenta solid line shows the limitation given by Equation (1) with Σ = 2. The magenta dashed line corresponds to the color cut given by Equation (2).
Paper: JWST’s First Glimpse of a z > 2 Forming Cluster Reveals a Top-heavy Stellar Mass Function
Authors: Hanwen Sun, Tao Wang, Ke Xu, Emanuele Daddi, Qing Gu, Tadayuki Kodama, Anita Zanella, David Elbaz, Ichi Tanaka, Raphael Gobat, Qi Guo, Jiaxin Han, Shiying Lu, Luwenjia Zhou
Figure caption: SMF of cluster J1001 compared with results in other protoclusters at z ∼ 2. The blue and red solid lines show the SMF of SFGs and QGs in cluster J1001 at z=2.506. The blue dashed line is the SMF of HAEs in J1001, which provides fair comparisons with Shimakawa et al. (2018a, 2018b). The purple dashed line is the stacked SMF of SFGs in 14 (proto)clusters between z = 2.0 − 2.5 in the COSMOS field (Edward et al. 2023), the green dotted line is the SMF of HAEs in cluster USS 1558 at z = 2.5 (Shimakawa et al. 2018a), and the brown dashed–dotted line is the SMF of HAEs in cluster PKS 1138 at z = 2.2 (Shimakawa et al. 2018b). All three SMFs of other (proto)clusters have been renormalized to match the normalization of J1001.
Paper: JWST’s First Glimpse of a z > 2 Forming Cluster Reveals a Top-heavy Stellar Mass Function
Authors: Hanwen Sun, Tao Wang, Ke Xu, Emanuele Daddi, Qing Gu, Tadayuki Kodama, Anita Zanella, David Elbaz, Ichi Tanaka, Raphael Gobat, Qi Guo, Jiaxin Han, Shiying Lu, Luwenjia Zhou
Figure caption: Upper panel: the selection completeness. Blue and red points are the simulated selection completeness as a function of narrowband magnitude and stellar mass, respectively. And the blue and red lines are the completeness function fitted by the complementary error function. Lower panel: the narrow band exceeds fluxes as a function of narrowband magnitude. The red solid line is the result of linear fitting, while the dotted lines show the scatter of 0.12 dex.
Paper: JWST’s First Glimpse of a z > 2 Forming Cluster Reveals a Top-heavy Stellar Mass Function
Authors: Hanwen Sun, Tao Wang, Ke Xu, Emanuele Daddi, Qing Gu, Tadayuki Kodama, Anita Zanella, David Elbaz, Ichi Tanaka, Raphael Gobat, Qi Guo, Jiaxin Han, Shiying Lu, Luwenjia Zhou
Figure caption: Left panel: similar to Figure 4, while all the massive central galaxies within 50 kpc are merged into a quiescent BCG. The green dotted line is a copy of the blue line in Figure 4. The dashed line is the SMF of clusters at z ∼ 1.2 (van der Burg et al. 2020) within 1 Mpc of their center (comparable with the size of our survey). Right panel: the SF and quiescent SMF of cluster J1001 with all galaxies to be quenched within 0.5 Gyr considered as QGs. The blue and red dashed lines show the SF and quiescent SMF of cluster galaxies at z ∼ 1.2, respectively.
Paper: JWST’s First Glimpse of a z > 2 Forming Cluster Reveals a Top-heavy Stellar Mass Function
Authors: Hanwen Sun, Tao Wang, Ke Xu, Emanuele Daddi, Qing Gu, Tadayuki Kodama, Anita Zanella, David Elbaz, Ichi Tanaka, Raphael Gobat, Qi Guo, Jiaxin Han, Shiying Lu, Luwenjia Zhou
Figure caption: The comparison of the K s-band fluxes measured with T-PHOT and the Kron method. The blue and red points show the unblended and blended sources, respectively.
Paper: JWST’s First Glimpse of a z > 2 Forming Cluster Reveals a Top-heavy Stellar Mass Function
Authors: Hanwen Sun, Tao Wang, Ke Xu, Emanuele Daddi, Qing Gu, Tadayuki Kodama, Anita Zanella, David Elbaz, Ichi Tanaka, Raphael Gobat, Qi Guo, Jiaxin Han, Shiying Lu, Luwenjia Zhou
Figure caption: Left panels: examples of the best-fit SED of two member galaxies from Bagpipes. Right panels: the probability density distribution functions of the photometric redshift from EAZY and stellar mass from Bagpipes.