adsabs/AstroCLIMB huggingface dataset:
Paper: A Strong He II λ1640 Emitter with an Extremely Blue UV Spectral Slope at z = 8.16: Presence of Population III Stars?
Authors: Xin Wang, Cheng Cheng, Junqiang Ge, Xiao-Lei Meng, Emanuele Daddi, Haojing Yan, Zhiyuan Ji, Yifei Jin, Tucker Jones, Matthew A. Malkan, Pablo Arrabal Haro, Gabriel Brammer, Masamune Oguri, Meicun Hou, Shiwu Zhang
Figure caption: Corner plot showing the 1D/2D posterior constraints of the fitting parameters, i.e., gas-phase metallicity (﹩12+\mathrm{log}({\rm{O}}/{\rm{H}})﹩), nebular dust content (﹩{A}_{{\rm{V}}}^{{\rm{N}}}﹩), and instantaneous SFR already corrected for lensing magnification (μ = 2.26 ± 0.14) of RX J2129–z8He II, obtained from our Bayesian forward-modeling emission line diagnostic method. On top of each 1D posterior panel is shown the resulting median with 1σ uncertainties for each parameter. Yet notice that we can only draw a 1σ upper limit on ﹩{A}_{{\rm{V}}}^{{\rm{N}}}﹩ as presented in Table 1. The panel in the upper right shows the −χ 2/2 values for all 80,000 parameter sampling iterations. They clearly reach a global minimum of χ 2, implying a good convergence of our Bayesian inference.
Paper: A Strong He II λ1640 Emitter with an Extremely Blue UV Spectral Slope at z = 8.16: Presence of Population III Stars?
Authors: Xin Wang, Cheng Cheng, Junqiang Ge, Xiao-Lei Meng, Emanuele Daddi, Haojing Yan, Zhiyuan Ji, Yifei Jin, Tucker Jones, Matthew A. Malkan, Pablo Arrabal Haro, Gabriel Brammer, Masamune Oguri, Meicun Hou, Shiwu Zhang
Figure caption: UV spectral slope (β) as a function of absolute UV magnitude (M UV). The color-coded circles represent the spectroscopically confirmed galaxies at z spec > 7 with β measurements (Watson et al. 2015; Zitrin et al. 2015; Hashimoto et al. 2018; Williams et al. 2023; Morishita et al. 2023; Schaerer et al. 2022; Curtis-Lake et al. 2023; Bunker et al. 2023). Among this cohort, RX J2129–z8He II (indicated as the star) has the steepest slopes. The gray diamonds show the galaxy candidates with z phot ≳ 8 (Tacchella et al. 2022; Castellano et al. 2022; Naidu et al. 2022; Finkelstein et al. 2022; Topping et al. 2022; Cullen et al. 2023). The dotted and dashed lines denote the population-averaged correlation of M UV and β at z ∼ 7 (Bouwens et al. 2010, 2014) and z ∼ 8 (Bhatawdekar & Conselice 2021), respectively. The shaded regions correspond to the parameter space where the escape fraction of the ionizing radiation (﹩{f}_{\mathrm{esc}}^{\mathrm{LyC}}﹩) is above 5%, 10%, and 20%, respectively, derived by Chisholm et al. (2022) from the LzLCS data set. This strongly suggests that RX J2129–z8He II is hitherto the most promising spectroscopically confirmed galaxy that enables significant LyC leakage into the IGM to contribute to the cosmic reionization.
Paper: On the Heating of the Slow Solar Wind by Imbalanced Alfvén-wave Turbulence from 0.06 to 1 au: Parker Solar Probe and Solar Orbiter Observations
Authors: Sofiane Bourouaine, Jean C. Perez, Benjamin D. G. Chandran, Vamsee K. Jagarlamudi, Nour E. Raouafi, Jasper S. Halekas
Figure caption: Top left panel: the normalized cross helicity ∣σ  c ∣. Top right panel: the magnetic compressibility C  B . Bottom left panel: the plasma compressibility C  n . Bottom right panel: the quantity B 0r (r/au)2 in nT unit that is proportional to the magnetic-field flux. The orange (blue) scatter points are the slow-wind PSP (SO) intervals with more than 70% of either Sun-outward or -inward magnetic-field polarity. The black dots correspond to the selected ASW intervals used for our analysis, i.e., intervals that satisfy C  B  < 0.25, C  n  < 0.25, and ∣σ  c ∣ > 0.65 and where B 0r (r/1 au)2 ranges between 2 and 4 nT.
Paper: On the Heating of the Slow Solar Wind by Imbalanced Alfvén-wave Turbulence from 0.06 to 1 au: Parker Solar Probe and Solar Orbiter Observations
Authors: Sofiane Bourouaine, Jean C. Perez, Benjamin D. G. Chandran, Vamsee K. Jagarlamudi, Nour E. Raouafi, Jasper S. Halekas
Figure caption: Top panels from left to right: the plasma density n and the proton temperature T  p . Middle panels from left to right: The strength of the average magnetic field B 0 and the energy densities of the antisunward E out sunward E in AWs. Bottom panels from left to right: the kinetic energy density E  V  and the magnetic energy density E  b  in velocity unit. All are plotted as a function of the radial distance r.
Paper: On the Heating of the Slow Solar Wind by Imbalanced Alfvén-wave Turbulence from 0.06 to 1 au: Parker Solar Probe and Solar Orbiter Observations
Authors: Sofiane Bourouaine, Jean C. Perez, Benjamin D. G. Chandran, Vamsee K. Jagarlamudi, Nour E. Raouafi, Jasper S. Halekas
Figure caption: Top panel: black dots are the estimated turbulent dissipation rate Q  W  from Equation (10) for ASW intervals for r < 0.3 au (r > 0.3 au) using PSP (SO). Red dots represent the proton heating rate Q  p  for ASW. Solid green line represents the estimated electron heating rate Q  e  when α  H  = 0.9. Bottom panel: proton-to-total-heating ratio vs. heliocentric distance when α  H  = 0.9, α  H  = 0.75, and α  H  = 0.5, and the solid lines are the same ratio obtained from the power-law fits of Q  p  and Q  e .
Paper: On the Heating of the Slow Solar Wind by Imbalanced Alfvén-wave Turbulence from 0.06 to 1 au: Parker Solar Probe and Solar Orbiter Observations
Authors: Sofiane Bourouaine, Jean C. Perez, Benjamin D. G. Chandran, Vamsee K. Jagarlamudi, Nour E. Raouafi, Jasper S. Halekas
Figure caption: The estimated turbulent dissipation rate, Q CH09, from the turbulence reflection model of Chandran & Hollweg (2009; blue dots) from Equation (11) compared to the turbulent dissipation rate Q  W  obtained from Equation (10) (black dots). All were measured using PSP for r < 0.3 au and SO at r > 0.3 au.
Paper: On the Heating of the Slow Solar Wind by Imbalanced Alfvén-wave Turbulence from 0.06 to 1 au: Parker Solar Probe and Solar Orbiter Observations
Authors: Sofiane Bourouaine, Jean C. Perez, Benjamin D. G. Chandran, Vamsee K. Jagarlamudi, Nour E. Raouafi, Jasper S. Halekas
Figure caption: Red dots: measured proton heating rate Q  p  for ASW at r < 0.3 au (r > 0.3 au) using PSP (SO). Green lines: the estimated electron heating rate Q  e  for ASW at r < 0.3 au (r > 0.3 au) using T  e  = 1.4 · 105(r/1 au)−0.5 (K) for α  H  = 0.9 (solid), α  H  = 0.75 (dashed), and α  H  = 0.5 (dotted).
Paper: Ultra-high-energy Cosmic-Ray Sources Can Be Gamma-Ray Dim
Authors: Angelina Sherman, Ke Fang, Rafael Alves Batista, Rogerio Menezes de Almeida
Figure caption: Sky map of the 4FGL-DR4 catalog after Galactic sources and unassociated sources within ∣b∣ < 10° are removed. The color bar indicates the gamma-ray energy flux in erg cm−2 s−1. The dimmest source in the catalog has energy flux 3.09 × 10−13 erg cm−2 s−1.
Paper: Ultra-high-energy Cosmic-Ray Sources Can Be Gamma-Ray Dim
Authors: Angelina Sherman, Ke Fang, Rafael Alves Batista, Rogerio Menezes de Almeida
Figure caption: Spectrum at Earth of simulated UHECRs from Fermi-LAT sources in the case of gamma-ray flux weighting. Because the signal is dominated by one source, there is some discrepancy between the simulated spectrum and Auger data at high energies; however, the disagreement in the spectra is not sufficient to explain the order of magnitude in difference between the simulated and observed dipole amplitude.
Paper: Ultra-high-energy Cosmic-Ray Sources Can Be Gamma-Ray Dim
Authors: Angelina Sherman, Ke Fang, Rafael Alves Batista, Rogerio Menezes de Almeida
Figure caption: Redshift distribution of sources in 4FGL-DR4 after removing Galactic sources and low-latitude unassociated sources. Sources with known redshifts are indicated by the blue shaded region. Sources without distance information are assigned random redshifts following an SFR distribution (Yüksel et al. 2008) as indicated by the black dotted curve. The sum of the two are shown as the red solid curve.
Paper: Ultra-high-energy Cosmic-Ray Sources Can Be Gamma-Ray Dim
Authors: Angelina Sherman, Ke Fang, Rafael Alves Batista, Rogerio Menezes de Almeida
Figure caption: Flux map corresponding to the case of gamma-ray flux weighting. The flux map is obtained by taking the ratio of the smoothed count density and exposure map following Aab et al. (2017). The sky map is smoothed with a 45° top-hat function using the healpy.sphtfnc.beam2bl function.
Paper: Ultra-high-energy Cosmic-Ray Sources Can Be Gamma-Ray Dim
Authors: Angelina Sherman, Ke Fang, Rafael Alves Batista, Rogerio Menezes de Almeida
Figure caption: Flux map corresponding to the case of uniform source weighting. The flux map is obtained by taking the ratio of the smoothed count density and exposure map following Aab et al. (2017). The sky map is smoothed with a 45° top-hat function using the healpy.sphtfnc.beam2bl function.
Paper: Ultra-high-energy Cosmic-Ray Sources Can Be Gamma-Ray Dim
Authors: Angelina Sherman, Ke Fang, Rafael Alves Batista, Rogerio Menezes de Almeida
Figure caption: Spectrum at Earth of simulated UHECRs from Fermi-LAT sources. The energy range below 8 EeV is shaded in gray as only events with energy greater than 8 EeV are used in evaluating the dipole as in Aab et al. (2017).
Paper: Deneb Is a Large-amplitude Polarimetric Variable
Authors: Daniel V. Cotton, Jeremy Bailey, Jean Perkins, Derek L. Buzasi, Ievgeniia Boiko
Figure caption: Observational data. (a) Time-series data from Sector 55 and 56 TESS photometry (top panel) and ﹩{g}^{{\prime} }﹩-band polarimetry (bottom four panels; HIPPI-2/36-inch/OOS—circles, PICSARR/C14/WSO—squares, PICSARR/CDK-14/OOS—diamonds). The time series are divided into a number of segments, which we denote S[n]; these are all 72.4 days in length corresponding to the semiregular cycle for the “resumption” events. The beginning of the first segment is 2459810 BJD, which is the last resumption event identified by Abt et al. (2023). Deneb’s 11.7 days pulsation cycle can be seen in the TESS data; the gray grid lines are placed every 11.7 days offset to +6.1 days to correspond with the first photometric maximum. Green lines are the medians in q (1418.5 ppm) and u (3612.5 ppm). A gray line guides the eye in q after the extreme event. The red lines correspond to the BJD dates when BACHES spectra (S/N=150–200) were taken; these are shown in (b) centered on H α /H β  (left/right); the strongest additional absorption features are seen at +10, +361, and +362 days. (c) (Semi)amplitude spectrum derived from TESS Sectors 41, 55, and 56 in parts per thousand (ppt =1000 × ppm); prominent peaks correspond to periods of ∼38 days, 11–12 days, and 18–20 days. Note that the frequency resolution is low due to the short length of the time series.
Paper: Deneb Is a Large-amplitude Polarimetric Variable
Authors: Daniel V. Cotton, Jeremy Bailey, Jean Perkins, Derek L. Buzasi, Ievgeniia Boiko
Figure caption: Following Watson (1983)'s analytical model, the ratio of the polarimetric to photometric pulsation amplitudes is equal to z  ℓ /b  ℓ  × G  ℓ mi . In the upper panels is the ratio of the photometric scaling factor, b  ℓ , at 800 nm (∼TESS λ eff) and the polarimetric scaling factor, z  ℓ λ , for mode degree, ℓ = 2 (left), 3 (center), and 4 (right) for both Deneb (T eff =  8500 K and ﹩\mathrm{log}g\,=﹩ 1.100 dex) and β Cru. In the lower panels are histograms showing the distribution of values of the geometric factor, G  ℓ mi , in which q and u amplitudes are combined as the root sum of the squares. One model instance, N, is calculated for each inclination, i, between 1° and 89° in 1° increments, and each m = − ℓ, …, 0, …, + ℓ for ℓ = 2 (left), 3 (center), and 4 (right). The vertical blue line indicates G 3,−3,46°—corresponding to the largest polarimetric amplitude detected for β Cru.
Paper: Mechanisms of Fundamental Electromagnetic Wave Radiation in the Solar Wind
Authors: C. Krafft, P. Savoini, F. J. Polanco-Rodríguez
Figure caption: Low-frequency energy spectra in the plane (k  x  λ D, k  y  λ D), in logarithmic scales, at ω  p  t = 5500, 6500, 7500, 8500, 10,500, and 13,500, for the box with size L  x  × L  y  = 1448λ D × 1448λ D. Labels in panel (f) indicate ion-acoustic waves excited: ﹩{{ \mathcal S }}^{{\prime} }﹩ (﹩{ \mathcal L }\to {{ \mathcal S }}^{{\prime} }+{{ \mathcal L }}^{{\prime} }﹩), ﹩{{ \mathcal S }}^{{\prime\prime} }﹩ (﹩{{ \mathcal L }}^{{\prime} }\to {{ \mathcal S }}^{{\prime\prime} }+{{ \mathcal L }}^{{\prime\prime} }﹩), ﹩{{ \mathcal S }}_{b}﹩ (﹩{{ \mathcal L }}^{{\prime} }\to { \mathcal F }+{{ \mathcal S }}_{b}﹩), ﹩{{ \mathcal S }}_{f}﹩ (﹩{ \mathcal L }\to { \mathcal F }+{{ \mathcal S }}_{f}﹩, ﹩{{ \mathcal L }}^{{\prime\prime} }\to { \mathcal F }+{{ \mathcal S }}_{f}﹩). Note that panels (a)–(f) are the continuation from ω  p  t ≃ 5500 to ω  p  t ≃ 13,500 of the left panels of Figure 2 in Krafft & Savoini (2024). All variables are normalized.
Paper: Mechanisms of Fundamental Electromagnetic Wave Radiation in the Solar Wind
Authors: C. Krafft, P. Savoini, F. J. Polanco-Rodríguez
Figure caption: (a–f) Dispersion curves in the plane (ω/ω  p , k  x  λ D), corresponding to spectra of Figure 1, in logarithmic scales, for the box ﹩{L}_{x}\times {L}_{y}=1448\times 1448{\lambda }_{{\rm{D}}}^{2}﹩. Dashed black lines represent the theoretical dispersion law of ion-acoustic waves. (g–i) Magnetic energy spectra of ﹩{ \mathcal F }﹩ waves, filtered around ω  p , in the plane (k  x  λ D, k  y  λ D), at ω  p  t ≃ 4000, 5500, and 7500, in logarithmic scales, for the large box ﹩{L}_{x}\times {L}_{y}=5792\times 2896{\lambda }_{{\rm{D}}}^{2}﹩. All variables are normalized.
Paper: Mechanisms of Fundamental Electromagnetic Wave Radiation in the Solar Wind
Authors: C. Krafft, P. Savoini, F. J. Polanco-Rodríguez
Figure caption: Variations with time of wave energy (integrated on the 2D simulation box and normalized by the initial beam energy W  b ) of (a) Langmuir waves ﹩{ \mathcal L }﹩, ﹩{{ \mathcal L }}^{{\prime} }﹩, and ﹩{{ \mathcal L }}^{{\prime\prime} }﹩ involved in the two ESD cascades ﹩{ \mathcal L }\to {{ \mathcal S }}^{{\prime} }+{{ \mathcal L }}^{{\prime} }﹩ and ﹩{{ \mathcal L }}^{{\prime} }\to {{ \mathcal S }}^{{\prime\prime} }+{{ \mathcal L }}^{{\prime\prime} }﹩, electromagnetic waves ﹩{ \mathcal F }﹩, and (b) backward- and forward-propagating ion-acoustic waves ﹩{{ \mathcal S }}_{b}﹩ and ﹩{{ \mathcal S }}_{f}﹩. (a–b) The energies of waves radiated directly or indirectly by the beam are several orders of magnitude above the noise, as shown by the analysis of a “thermal” simulation with no beam injection. (c) Cross-bicoherence b  c (k  x1, k  x2) at ω  p  t ≃ 8000; k  x1 and k  x2 represent the parallel wavenumbers of waves ﹩{{ \mathcal L }}^{{\prime} }﹩ and ﹩{{ \mathcal S }}_{b};﹩ the maximum is b  c  = 0.9, for ﹩({k}_{x1},{k}_{x2})=(-0.117,-0.121){\lambda }_{{\rm{D}}}^{-1}﹩. (d) Cross-bicoherence b  c (ω 1, ω 2) at ω  p  t ≃ 8000, where ω 1 and ω 2 represent the frequencies of waves ﹩{ \mathcal F }﹩ and ﹩{{ \mathcal S }}_{b};﹩ the maximum is b  c  = 0.85, for (ω 1, ω 2) = (1.020, 0.0042)ω  p . (e) Time variations of energies ﹩{W}_{{ \mathcal F }}﹩ (blue) and ﹩{W}_{{{ \mathcal S }}_{b}}﹩ (red) and of energy products ﹩{W}_{{{ \mathcal S }}_{b}}{W}_{{{ \mathcal L }}^{{\prime} }}﹩ (dotted light blue, ﹩{{ \mathcal S }}_{b}\ast {{ \mathcal L }}^{{\prime} }﹩) and ﹩{W}_{{ \mathcal F }}{W}_{{{ \mathcal L }}^{{\prime} }}﹩ (dotted green, ﹩{ \mathcal F }\ast {{ \mathcal L }}^{{\prime} }﹩). (f) Time variations of energies ﹩{W}_{{{ \mathcal L }}^{{\prime\prime} }}﹩ (black), ﹩{W}_{{ \mathcal F }}﹩ (blue), and ﹩{W}_{{{ \mathcal S }}_{f}}﹩ (red) and energy products ﹩{{ \mathcal S }}_{b}^{{qm}}﹩ (dotted light blue, ﹩{{ \mathcal S }}_{f}\ast {{ \mathcal L }}^{{\prime\prime} }﹩) , ﹩{W}_{{ \mathcal F }}{W}_{{{ \mathcal L }}^{{\prime\prime} }}﹩ (dotted green, ﹩{ \mathcal F }\ast {{ \mathcal L }}^{{\prime\prime} }﹩), and ﹩{W}_{{ \mathcal F }}{W}_{{{ \mathcal S }}_{f}}﹩ (dotted orange, ﹩{ \mathcal F }\ast {{ \mathcal S }}_{f}﹩). (g) Time variations of energies ﹩{W}_{{ \mathcal F }}﹩ (blue) and ﹩{W}_{{{ \mathcal S }}_{f}}﹩ (red) and of energy products ﹩{W}_{{{ \mathcal S }}_{f}}{W}_{{ \mathcal L }}﹩ (dotted light blue, ﹩{{ \mathcal S }}_{f}\ast { \mathcal L }﹩) and ﹩{W}_{{ \mathcal F }}{W}_{{ \mathcal L }}﹩ (dotted green, ﹩{ \mathcal F }\ast { \mathcal L }﹩). Panels (a)–(b) and (e)–(g) are in logarithmic scales. All variables are dimensionless. Note that, as the plasma is homogeneous (ΔN = 0), the energy of electromagnetic waves should be considered as an upper limit of the actual energy radiated in an optically thin region of the solar wind, due to the periodic boundary conditions used, which do not allow electromagnetic waves to escape from the simulated system.
Paper: Mechanisms of Fundamental Electromagnetic Wave Radiation in the Solar Wind
Authors: C. Krafft, P. Savoini, F. J. Polanco-Rodríguez
Figure caption: (a–d) Ion-acoustic energy spectra in the plane (k  x  λ D, k  y  λ D), at ω  p  t = 4500, 7500, 9500, and 12,500, for ΔN = 0 and T  e /T  i  = 1 ; the ion-acoustic quasi-modes are indicated on each panel. (e) Corresponding dispersion (ω/ω  p , k  x  λ D) at ω  p  t = 12,500. (f) Time variations of ﹩{W}_{{ \mathcal F }}﹩ (integrated on the 2D simulation box and normalized by the initial beam energy) for T  e /T  i  = 1 (dashed) and T  e /T  i  = 10 (solid), for ΔN = 0 (black) and ΔN = 0.05 (blue), in logarithmic scales. Inset shows the time variation of energies ﹩{W}_{{ \mathcal S }}﹩ of quasi-modes ﹩{{ \mathcal S }}_{b}^{{qm}}﹩ and ﹩{{ \mathcal S }}_{f}^{{qm}}﹩ (red), for ΔN = 0, in logarithmic scales. (g) Low-frequency energy spectrum at ω  p  t = 3500, where the quasi-modes ﹩{{ \mathcal S }}_{{qm}}^{{\prime} }﹩, ﹩{{ \mathcal S }}_{{qm}}^{{\prime\prime} },﹩                      ﹩{{ \mathcal S }}_{f}^{{qm}}﹩, and ﹩{{ \mathcal S }}_{b}^{{qm}}﹩ are visible, for T  e /T  i  = 1 and ΔN = 0.05, in logarithmic scale. (h) Spatial distribution of δ n  i (x, y)/n 0 filtered around ﹩{k}_{x{ \mathcal L }},﹩ at ω  p  t = 3500, showing enhanced ion-acoustic quasi-modes’ structures corresponding to ﹩\left|{k}_{x{{ \mathcal S }}_{b}^{{qm}}}\right|\sim \left|{k}_{x{{ \mathcal S }}_{f}^{{qm}}}\right|\sim {k}_{x{ \mathcal L }}\sim 0.1{\lambda }_{{\rm{D}}}^{-1}﹩.
Paper: Mechanisms of Fundamental Electromagnetic Wave Radiation in the Solar Wind
Authors: C. Krafft, P. Savoini, F. J. Polanco-Rodríguez
Figure caption: Inhomogeneous plasma with random density fluctuations δ n. Variations of energies (a) ﹩{W}_{{ \mathcal F }}﹩ and (b) ﹩{W}_{{ \mathcal L }}﹩, integrated on the 2D simulation box and normalized by the initial beam energy, in logarithmic scales, for ΔN = 0.05 (blue), ΔN = 0.025 (red), and ΔN = 0 (black). (c) Spatial distribution of δ n  i (x, y)/n 0, at ω  p  t = 1700, filtered around ﹩{k}_{{ \mathcal L }}\sim 0.1{\lambda }_{{\rm{D}}}^{-1}﹩, on which density fluctuations’ isocontours δ n(x, y) = 0 (red) are superimposed. Intense propagation structures appear where δ n ≤ 0. (d–e) Profiles along x (at fixed y) of δ n  i /n 0 (applied density fluctuations δ n have been subtracted by filtering), at ω  p  t = 4700 (panel (d)) and ω  p  t = 13,400 (panel (e)), for ΔN = 0.05; waves with wavelengths ﹩2\pi /{k}_{x{ \mathcal S }}\simeq 2\pi /{k}_{x{ \mathcal L }}\sim 60{\lambda }_{{\rm{D}}}﹩ are visible around 180 ≲ x/λ D ≲ 300 (panel (d)) and 300 ≲ x/λ D ≲ 600 (panel (e)). (f) Dispersion curves of ion-acoustic waves in the plane (ω/ω  p , k  x  λ D) at ω  p  t = 5000, for ΔN = 0.05;                       ﹩{{ \mathcal S }}_{b}﹩ waves are visible near ﹩{k}_{x{{ \mathcal S }}_{b}}\simeq -0.1{\lambda }_{{\rm{D}}}^{-1}﹩. All variables are normalized.
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 (a) displays the eROSITA X-ray RGB image (Predehl et al. 2020), in which the white circle marks the LPC and the four white boxes are the image frames of Figure 2 (G308+21), Figure 3 (NPS root), and Figure 4 (northwestern border and southwestern bright rim). The red crosses and blue squares are manually selected marks of the X-ray bubble border (Section 3.1). Panel (b) display the dust extinction map in the 400–1000 pc distance range of the Ve22 dust cube plotted in Hammer–Aitoff projection. Panel (c) displays the extinction map of the pixels with Galactic latitude >15° in the Ve22 cube viewed from the north Galactic pole. In panel (c), the Sun is at (0, 0), the direction of GC is to the top, and the dotted lines correspond to Galactic longitudes 33°, 19°, and 308°. The three isolated clouds G19+18, G33+25, and G308+21 are marked on the three maps with red circles.
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 (a), (b), and (c) display the eROSITA X-ray RGB image (R: 0.2–0.5 keV; G: 0.5–1 keV; B: 1–2 keV), the total N H map, and the Le22 dust extinction map in the distance range 520–650 pc (with the patch border marked with black lines), respectively. Both the extinction and N H maps use a rainbow color map, where purple indicates large values. The contour of the total N H map is overplotted on the X-ray image and the extinction map. Thirteen positions are marked in the lower panels with 40′-diameter circles. Panel (d) displays the Le22 and Ve22 distance profiles of extinction at these positions, separating the positions into two groups for the sake of 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: Panel (c) displays the 3D skewed cup model (purple), created by cutting off the high-Z part (gray) of the skewed ellipsoid model. The blue and green points indicate the centers of the ellipsoids before and after shifting. The red and black points indicate the locations of the Sun and the GC. The LOS tangent of the 3D surface is marked in orange and green, and green indicates the l > 180°, 35° < b < 65° section, where the border is determined by the radio arcs shown in Figure 4. Panels (a) and (b) display the view of the 3D model from two aspects facing east (l = 90°) and the GC, respectively. Panel (d) displays the Hammer–Aitoff projection of the skewed cup model. The red crosses and blue squares are manually selected marks of the border position (see also Figure 1). Only the red points were used to constrain the 3D model, whose border is displayed by the cyan dashed lines. The HI column density map along the Galactic tangent circle presented by Sofue (2017) is overplotted on the 2D map.
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: Chemical abundances predicted for environments uniquely enriched by PISNe (red), by other Pop III SNe (faint SNe: green; core-collapse SNe: blue; hypernovae: purple), and by normal Pop II SNe (gray shaded areas). Each environment is enriched by a single Pop III SN with different mass and explosion energy. The contours with decreasing color intensity identify 30%, 60%, and 90% probability densities, corresponding to the fraction of environments predicting those abundances for each SN type. Points with error bars are the measured abundances of absorbers in the literature (Section 3; labels). The values reported by Christensen et al. (2023; red empty) are connected with the new measurements obtained using higher-resolution spectra (star). The absorber in the sight line to J1018+0548 (Saccardi et al. 2023; z = 3.39) is highlighted with a black cross (see Section 4.2). The arrows show in which direction dust depletion would modify the predicted abundances.