adsabs/AstroCLIMB huggingface dataset:
Paper: A Potential Dynamical Origin of the Galactic Disk Warp: The Gaia–Sausage–Enceladus Major Merger
Authors: Mingji Deng, Cuihua Du, Yanbin Yang, Jiwei Liao, Dashuang Ye
Figure caption: Distribution of simulated stars and gas in Galactocentric cylindrical coordinates at the present time (9.05 Gyr since the simulation started). Negative/positive R indicates the southern/northern warp. The top panel depicts the warp of the stellar disk, with a color bar indicating stellar ages. The bottom panel shows the gas warp in a density projection map with a contour profile. Here, the green lines represent a height of ∣Z∣ = 2.5 kpc, indicating the northern warp is stronger than the southern part. Comparative data are sourced from X. Chen et al. (2019), Lemasle (2022), and E. S. Levine et al. (2006).
Paper: Discovering Subsolar Metallicity Brown Dwarf Candidates in the Small Magellanic Cloud
Authors: Peter Zeidler, Elena Sabbi, Antonella Nota, Elena Manjavacas, Olivia C. Jones, Camilla Pacifici
Figure caption: The spatial distribution of the PMS stars and cBDs (upper panel) and the cYSOs (lower panel). The PMS stars and the cBDs follow the same spatial distribution, while the cYSOs are mainly located on the gas and dust ridges. The blue circle marks the CF used to estimate the contamination from the SMC field stars and the background galaxies. The black circle marks the equally sized cluster region. The underlying image is the F277W filter. North is up, and east is to the left.
Paper: A Potential Dynamical Origin of the Galactic Disk Warp: The Gaia–Sausage–Enceladus Major Merger
Authors: Mingji Deng, Cuihua Du, Yanbin Yang, Jiwei Liao, Dashuang Ye
Figure caption: Top panel: illustrating the evolution of the DM halo’s tilt angle with respect to the disk. Middle panel: DM triaxiality variations with time, with values predominantly less than 0.3, indicating an oblate shape. Bottom panel: net angular momentum about the Z-axis L  Z  of the DM halo as a function of time. A negative value indicates a retrograde halo.
Paper: Discovering Subsolar Metallicity Brown Dwarf Candidates in the Small Magellanic Cloud
Authors: Peter Zeidler, Elena Sabbi, Antonella Nota, Elena Manjavacas, Olivia C. Jones, Camilla Pacifici
Figure caption: The normalized cumulative radial distribution of the PMS stars (red), cYSOs (green), and cBDs (yellow) within the inner 60″ from the cluster center. The PMS stars and BDs are similarly distributed, confirmed by the KS test. The cYSOs are less concentrated in the cluster center.
Paper: A Potential Dynamical Origin of the Galactic Disk Warp: The Gaia–Sausage–Enceladus Major Merger
Authors: Mingji Deng, Cuihua Du, Yanbin Yang, Jiwei Liao, Dashuang Ye
Figure caption: Comparison between the obtained values of warp precession rate varying with Galactocentric radius R in our simulation (purple circle), together with other values from the literature.
Paper: Scylla. III. The Outside-in Radial Age Gradient in the Small Magellanic Cloud and the Star Formation Histories of the Main Body, Wing, and Outer Regions
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Caroline Bot, Andrew E. Dolphin, Karoline M. Gilbert, Steven Goldman, Alec S. Hirschauer, Karin M. Sandstrom, O. Grace Telford
Figure caption: Left: the seven input line-of-sight distance distributions applied to our synthetic CMDs before SFH recovery. Middle: the two input SFHs we used in our simulations, one based on the results of P. Massana et al. (2022) representing the main body of the SMC and another representing our outer SMC fields, which show a drop-off in star formation in the past ∼3 Gyr (Section 4.1). Top right: the three values used in our simulations for the number of observed stars per field, overplotted on the cumulative distribution of the number of stars per field across our sample. Bottom right: cumulative distributions of the 80% completeness limit across our Scylla fields, shown for the F475W filter in cyan and the F814W filter in magenta. Using vertical lines, we overplot the 80% completeness limits in the “deep” (SMC_23; dotted lines) and “shallow” (SMC_35; dashed lines) fields from which we draw our observational noise model based on artificial star tests. The input values we use in our simulations essentially bracket the range of values across our sample of observed fields.
Paper: Scylla. III. The Outside-in Radial Age Gradient in the Small Magellanic Cloud and the Star Formation Histories of the Main Body, Wing, and Outer Regions
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Caroline Bot, Andrew E. Dolphin, Karoline M. Gilbert, Steven Goldman, Alec S. Hirschauer, Karin M. Sandstrom, O. Grace Telford
Figure caption: Top row: example synthetic CMDs generated assuming the different line-of-sight stellar distance distributions we sample, color coded and labeled as in the left panel of Figure 13. To allow a direct visual comparison, all synthetic CMDs were generated assuming the same PARSEC evolutionary models, input SFH, observational noise model, and number of observed stars. Bottom row: the recovered SFH for each CMD (assuming PARSEC evolutionary models also for SFH fitting) is overplotted on the input SFH, which is the same “main body” SFH (middle panel of Figure 13) in all cases. While results vary slightly beyond 1σ uncertainties in some cases at early look-back times ≳6 Gyr, input values of τ 50, τ 75, and τ 90 (sampling more recent look-back times) are recovered to within 1σ uncertainties for all stellar distance distributions.
Paper: Scylla. III. The Outside-in Radial Age Gradient in the Small Magellanic Cloud and the Star Formation Histories of the Main Body, Wing, and Outer Regions
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Caroline Bot, Andrew E. Dolphin, Karoline M. Gilbert, Steven Goldman, Alec S. Hirschauer, Karin M. Sandstrom, O. Grace Telford
Figure caption: Left: difference between recovered and input values of τ 75 for input stellar populations with different line-of-sight distance distributions, labeled along the horizontal axis and color coded as in Figures 13 and 14. Synthetic CMDs were generated using PARSEC stellar evolutionary models and then recovered assuming three different assumed stellar evolutionary libraries (one per row), identically to our observational sample. The leftmost column shows the difference between recovered and input values of τ 75 in Gyr (with the 10th and 90th percentiles over all simulation runs indicated by dashed gray lines), and the second column from the left shows these differences normalized by their 1σ uncertainties (with ±1σ deviations indicated by dotted gray lines). Right columns: same as the left columns, but for τ 90.
Paper: Scylla. III. The Outside-in Radial Age Gradient in the Small Magellanic Cloud and the Star Formation Histories of the Main Body, Wing, and Outer Regions
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Caroline Bot, Andrew E. Dolphin, Karoline M. Gilbert, Steven Goldman, Alec S. Hirschauer, Karin M. Sandstrom, O. Grace Telford
Figure caption: An example of our removal of known clusters from our fields and its impact on the resulting CSFH. This example corresponds to the most pessimistic case, in which the cluster (Bruck 100) occupies the largest projected area (1.54 arcmin2, or 21% of the field of view) in any of our target fields. In the left four panels, stars removed from our catalog are color coded by distance from the center of the cluster R SMA listed by E. Bica et al. (2020), and stars beyond R SMA, retained in our catalog, are shown in gray. In the right column, we compare the CSFH obtained after removing sources with R < R SMA (orange) to the CSFH obtained without removing any sources over the entire field of view (blue). The values of τ 50, τ 75, and τ 90 are not impacted beyond their uncertainties even if no effort is made to remove the cluster from our photometric catalog.
Paper: Scylla. III. The Outside-in Radial Age Gradient in the Small Magellanic Cloud and the Star Formation Histories of the Main Body, Wing, and Outer Regions
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Caroline Bot, Andrew E. Dolphin, Karoline M. Gilbert, Steven Goldman, Alec S. Hirschauer, Karin M. Sandstrom, O. Grace Telford
Figure caption: Comparison of R 90, the radius enclosing 90% of the cluster light from A. Hill & D. Zaritsky (2006), against R SMA, the cluster semimajor axis from the E. Bica et al. (2020) catalog inside which we remove all stars from our catalogs before fitting SFHs. Among the 15 clusters in common, all but one have R SMA ≥ R 90 to within uncertainties.
Paper: Scylla. III. The Outside-in Radial Age Gradient in the Small Magellanic Cloud and the Star Formation Histories of the Main Body, Wing, and Outer Regions
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Caroline Bot, Andrew E. Dolphin, Karoline M. Gilbert, Steven Goldman, Alec S. Hirschauer, Karin M. Sandstrom, O. Grace Telford
Figure caption: CSFHs for different SMC regions as in the left panel of Figure 5, but now with our combined CSFH for the LMC (Cohen et al. 2024) overplotted as a black dotted line.
Paper: Scylla. III. The Outside-in Radial Age Gradient in the Small Magellanic Cloud and the Star Formation Histories of the Main Body, Wing, and Outer Regions
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Caroline Bot, Andrew E. Dolphin, Karoline M. Gilbert, Steven Goldman, Alec S. Hirschauer, Karin M. Sandstrom, O. Grace Telford
Figure caption: Comparison between CSFHs for two cospatial fields observed with different instrument and filter combinations: SMC_5 was observed with WFC3/UVIS F475W and F814W filters, and SMC_A16 was observed with ACS/WFC F606W and F814W filters. Each panel presents a comparison assuming a different stellar evolutionary library for SFH fitting. The best-fit CSFHs are in excellent agreement, showing no evidence of observational systematics.
Paper: Scylla. III. The Outside-in Radial Age Gradient in the Small Magellanic Cloud and the Star Formation Histories of the Main Body, Wing, and Outer Regions
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Caroline Bot, Andrew E. Dolphin, Karoline M. Gilbert, Steven Goldman, Alec S. Hirschauer, Karin M. Sandstrom, O. Grace Telford
Figure caption: Per-field comparison between our CSFHs from MATCH (black) and those of M. Cignoni et al. (2012, 2013), who used both the Cole (red) and Bologna (blue) SFH fitting codes and then-recent Padova evolutionary models (G. Bertelli et al. 2008, 2009). Each row shows results for all six fields assuming a different set of evolutionary models for our SFH fitting. Each column is labeled with the corresponding field name used here, as well as the field name used by M. Cignoni et al. (2013).
Paper: Scylla. III. The Outside-in Radial Age Gradient in the Small Magellanic Cloud and the Star Formation Histories of the Main Body, Wing, and Outer Regions
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Caroline Bot, Andrew E. Dolphin, Karoline M. Gilbert, Steven Goldman, Alec S. Hirschauer, Karin M. Sandstrom, O. Grace Telford
Figure caption: Comparison of our best-fit values for τ 50 (top row), τ 75 (middle row), and τ 90 (bottom row) assuming different stellar evolutionary models for SFH fitting. Results are in agreement across different evolutionary models in nearly all (>97%) cases.
Paper: Lensing Point-spread Function of Coherent Astrophysical Sources and Nontrivial Wave Effects
Authors: Xun Shi
Figure caption: Frequency dependence of the LPSF—the smoothed flux density distribution I s for 1D rational lenses. We show both the x−ν distribution of I s (the upper panels in each subplot) and the corresponding I s(x) curves (lower panels) for various frequencies. The four subplots represent four lensing configurations, namely lenses with amplitudes κ = ±10, with a plus sign for diverging lenses and a minus sign for converging lenses, placed at two different source locations, β = 5 and β = 2, respectively. The flux density distribution is smoothed with a Gaussian kernel of width 0.1 along the x-axis. We label the locations of the images in the geometric limit with the orange vertical lines and distinguish between real images with positive parity (dashed line), real images with negative parity (dashed–dotted line), and effective imaginary images (dotted line). The four subplots illustrate four different situations: (a) three real images and one observable imaginary image; (b) three real images and one indistinguishable imaginary image; (c) one real image and two imaginary images; and (d) three real images and no imaginary image. In the I s(x) plots, the dashed curves show the unlensed LPSFs given by Equation (A3).
Paper: Lensing Point-spread Function of Coherent Astrophysical Sources and Nontrivial Wave Effects
Authors: Xun Shi
Figure caption: 2D LPSFs at different frequencies ν = 0.3, 1, 3, and 10 are shown in the upper panels for a converging point-mass lens ﹩\psi =-\mathrm{ln}(\sqrt{{x}^{2}+{y}^{2}})﹩ with κ = −1 at β = 2 displaced in the x-direction. For this lensing configuration, there exist two real images at y = 0, x = 2.4 and −0.4, respectively. The unit of the coordinates is the characteristic width of the lens, and the smoothing kernel is a 2D Gaussian of size r s = 0.1. The envelope of the diffuse brightness distribution can be well fitted by the 2D generalization of Equation (A3): ﹩{I}_{{\rm{s}}}\propto \exp \left(-{\nu }^{2}{r}_{{\rm{s}}}^{2}\left({\left(x-\beta \right)}^{2}+{y}^{2}\right)\right)﹩, irrespective of the κ value. The corresponding phase function structures are shown in the lower panels. Note the different scales of the axes for the four columns.
Paper: Impacts of Black-hole-forming Supernova Explosions on the Diffuse Neutrino Background
Authors: Ken'ichiro Nakazato, Ryuichiro Akaho, Yosuke Ashida, Takuji Tsujimoto
Figure caption: Integrated ﹩{\bar{\nu }}_{e}﹩ flux with E  ν  > 17.3 MeV estimated by our DSNB models in comparison with the best-fit values and their ±1σ uncertainties shown in gray solid lines and shaded regions, respectively, and the 90% observed upper limits shown in red dashed–dotted lines from SK with pure water (K. Abe et al. 2021b). Note that these experimental constraints are associated with the spectral models in K. Nakazato et al. (2015) while they are insensitive to the adopted spectrum models. Models with different mass hierarchies are shown in each panel: (a) NH and (b) IH. Solid and dashed lines represent the spectra for the models with MD14 SFR and HB06 SFR, respectively. Orange and blue lines correspond to the (i) fallback-induced and (ii) prompt BH-formation cases, respectively, in Table 1.
Paper: Impacts of Black-hole-forming Supernova Explosions on the Diffuse Neutrino Background
Authors: Ken'ichiro Nakazato, Ryuichiro Akaho, Yosuke Ashida, Takuji Tsujimoto
Figure caption: Spectra of cosmic background ﹩{\bar{\nu }}_{e}﹩ flux from this study compared with the 90% confidence level upper bounds from SK with pure (K. Abe et al. 2021b) and gadolinium-loaded (M. Harada et al. 2023b) water, and KamLAND (S. Abe et al. 2022). Models with different mass hierarchies and SFRs are shown in each panel: (a) NH and MD14, (b) NH and HB06, (C) IH and MD14, and (d) IH and HB06. Solid, dashed, and dashed–dotted lines show the spectra estimated with ﹩{f}_{\mathrm{BHSN}}=0.5﹩, 0.1, and 0, respectively, where ﹩{f}_{\mathrm{BHSN}}﹩ is the fraction of successful SN explosions that form a BH. Orange and blue lines correspond to the (i) fallback-induced and (ii) prompt BH-formation cases, respectively, in Table 1.
Paper: Impacts of Black-hole-forming Supernova Explosions on the Diffuse Neutrino Background
Authors: Ken'ichiro Nakazato, Ryuichiro Akaho, Yosuke Ashida, Takuji Tsujimoto
Figure caption: Time-integrated spectra of (a) ν  e , (b) ﹩{\bar{\nu }}_{e}﹩, and (c) ν  x , where ﹩{\nu }_{x}={\nu }_{\mu }={\bar{\nu }}_{\mu }={\nu }_{\tau }={\bar{\nu }}_{\tau }﹩, for the fallback-induced BH-formation model. Orange, blue, and green histograms correspond to the components of the early dynamical phase, the PNS cooling, and the fallback mass accretion, respectively.
Paper: Impacts of Black-hole-forming Supernova Explosions on the Diffuse Neutrino Background
Authors: Ken'ichiro Nakazato, Ryuichiro Akaho, Yosuke Ashida, Takuji Tsujimoto
Figure caption: Predicted DSNB event rate spectra at SK (a water volume of 22.5 kt) per year with different choices of the BH-forming SNe model and ﹩{f}_{\mathrm{BHSN}}﹩ for NH (top) and IH (bottom) and MD14 SFR. The notation of lines is the same as in Figure 2.
Paper: Impacts of Black-hole-forming Supernova Explosions on the Diffuse Neutrino Background
Authors: Ken'ichiro Nakazato, Ryuichiro Akaho, Yosuke Ashida, Takuji Tsujimoto
Figure caption: Operation time required to detect the DSNB at HK as a function of the fraction of BH-forming SNe, ﹩{f}_{\mathrm{BHSN}}﹩, based on our models with different mass hierarchy at different C.L.: (a) NH and 2σ, (b) IH and 2σ, (c) NH and 3σ, and (d) IH and 3σ. The notation of lines is the same as in Figure 3.
Paper: To High Redshift and Low Mass: Exploring the Emergence of Quenched Galaxies and Their Environments at 3 < z < 6 in the Ultra-deep JADES MIRI F770W Parallel
Authors: Stacey Alberts, Christina C. Williams, Jakob M. Helton, Katherine A. Suess, Zhiyuan Ji, Irene Shivaei, Jianwei Lyu, George Rieke, William M. Baker, Nina Bonaventura, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Emma Curtis-Lake, Francesco D'Eugenio, Daniel J. Eisenstein, Anna de Graaff, Kevin N. Hainline, Ryan Hausen, Benjamin D. Johnson, Roberto Maiolino, Eleonora Parlanti, Marcia J. Rieke, Brant E. Robertson, Yang Sun, Sandro Tacchella, Christopher N. A. Willmer, Chris J. Willott
Figure caption: The rest-frame UVJ colors of log M ⋆/M ⊙ ≥ 8.5 galaxies in the JADES MIRI parallel footprint at z = 3–4 (left) and z = 4–6 (right). The stars, pluses, and circles indicate QG candidates, PSB candidates, and SFGs, respectively. Closed symbols colored by stellar mass are colors derived from SED modeling including the F770W data point. Open gray symbols are colors derived from fits excluding F770W. The connecting lines show where sources move in UVJ space when MIRI is added. The red open star is the close companion source to JADES 172799 (172799b; Section 5.3). The purple solid (dashed) line shows the main (expanded) UVJ selection region for QGs from Antwi-Danso et al. (2023b). The gray dotted line is the selection from B19, which extends past the standard U − V boundary. The inset histogram shows that the color shifts are consistent within the measurement uncertainties (gray hatched region) for log M ⋆/M ⊙ = 8.5–9.5 (blue), but show a small systematic shift redward at higher masses (orange).
Paper: To High Redshift and Low Mass: Exploring the Emergence of Quenched Galaxies and Their Environments at 3 < z < 6 in the Ultra-deep JADES MIRI F770W Parallel
Authors: Stacey Alberts, Christina C. Williams, Jakob M. Helton, Katherine A. Suess, Zhiyuan Ji, Irene Shivaei, Jianwei Lyu, George Rieke, William M. Baker, Nina Bonaventura, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Emma Curtis-Lake, Francesco D'Eugenio, Daniel J. Eisenstein, Anna de Graaff, Kevin N. Hainline, Ryan Hausen, Benjamin D. Johnson, Roberto Maiolino, Eleonora Parlanti, Marcia J. Rieke, Brant E. Robertson, Yang Sun, Sandro Tacchella, Christopher N. A. Willmer, Chris J. Willott
Figure caption: Our mass-limited parent sample relative to the MS from Popesso et al. (2023) as a function of redshift. Red stars (orange pluses) are our QG (PSB) candidates. The red open star is the close companion source to JADES 172799 (172799b; Section 5.3). Solid plus signs indicate our primary PSB sample, while open symbols are the secondary sample. Only one PSB is a contaminant on the MS. White circles are galaxies in our parent sample not selected as QG or PSB. Purple x’s are galaxies selected by the Long et al. (2023) NIRCam color selection (Section 4.2.1) that are not in our sample.
Paper: To High Redshift and Low Mass: Exploring the Emergence of Quenched Galaxies and Their Environments at 3 < z < 6 in the Ultra-deep JADES MIRI F770W Parallel
Authors: Stacey Alberts, Christina C. Williams, Jakob M. Helton, Katherine A. Suess, Zhiyuan Ji, Irene Shivaei, Jianwei Lyu, George Rieke, William M. Baker, Nina Bonaventura, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Emma Curtis-Lake, Francesco D'Eugenio, Daniel J. Eisenstein, Anna de Graaff, Kevin N. Hainline, Ryan Hausen, Benjamin D. Johnson, Roberto Maiolino, Eleonora Parlanti, Marcia J. Rieke, Brant E. Robertson, Yang Sun, Sandro Tacchella, Christopher N. A. Willmer, Chris J. Willott
Figure caption: Properties of the UVJ-selected quiescent galaxies. Top row for each source: F606W, F090W, F200W, F444W, F770W cutouts, 1.″2 on a side. Bottom row for each source: the SEDs (left), SSFR posterior distributions (middle), and SFHs (right). Robust candidates are highlighted with tan backgrounds.
Paper: To High Redshift and Low Mass: Exploring the Emergence of Quenched Galaxies and Their Environments at 3 < z < 6 in the Ultra-deep JADES MIRI F770W Parallel
Authors: Stacey Alberts, Christina C. Williams, Jakob M. Helton, Katherine A. Suess, Zhiyuan Ji, Irene Shivaei, Jianwei Lyu, George Rieke, William M. Baker, Nina Bonaventura, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Emma Curtis-Lake, Francesco D'Eugenio, Daniel J. Eisenstein, Anna de Graaff, Kevin N. Hainline, Ryan Hausen, Benjamin D. Johnson, Roberto Maiolino, Eleonora Parlanti, Marcia J. Rieke, Brant E. Robertson, Yang Sun, Sandro Tacchella, Christopher N. A. Willmer, Chris J. Willott
Figure caption: (a) Overdensities of galaxies at 3.55 < z < 3.85 in the JADES NIRCam (black outline) and MIRI parallel (red outline) field of views. Contours increment by 1σ, with the purple contour outlining 4σ peaks. The yellow star indicates the Cosmic Rose. The green pluses show low-mass PSBs with redshifts consistent with z = 3.7. The inset histogram shows the redshift distribution of galaxies in the overdensity. (b) RGB (F444W, F200W, F090W) image of ∼150 kpc around the Cosmic Rose. (c) Zoom-in of the Cosmic Rose. Quiescent and PSB (SFG) galaxies in the z ∼ 3.7 overdensity are circled with solid (dotted) lines (†172811 is at z = 4.53; its proximity to the Rose is a projection effect). QGs and PSBs are labeled.