adsabs/AstroCLIMB huggingface dataset:
Paper: The Hot Circumgalactic Medium in Stacked X-Rays: Observations versus Simulations
Authors: Skylar Grayson, Evan Scannapieco, Johan Comparat, John A. ZuHone, Yi Zhang, Soumya Shreeram, Marcus Brüggen, Esra Bulbul
Figure caption: Stacked synthetic observations of hot CGM emission for galaxies with 11 < log(M*/M⊙) < 11.25 for (left to right) EAGLE, EAGLE-AGNdT9, EAGLE-NoAGN, SIMBA, and SIMBA-NoAGN. Each box is 22﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩5 across (≈2.5 Mpc at z = 0.1).
Paper: The Hot Circumgalactic Medium in Stacked X-Rays: Observations versus Simulations
Authors: Skylar Grayson, Evan Scannapieco, Johan Comparat, John A. ZuHone, Yi Zhang, Soumya Shreeram, Marcus Brüggen, Esra Bulbul
Figure caption: Halo mass–stellar mass relationship for the five simulations used in this work. Here we show the average central stellar mass for each 0.1 dex halo mass bin. Shaded regions represent the 1σ spread in each halo mass bin.
Paper: The Hot Circumgalactic Medium in Stacked X-Rays: Observations versus Simulations
Authors: Skylar Grayson, Evan Scannapieco, Johan Comparat, John A. ZuHone, Yi Zhang, Soumya Shreeram, Marcus Brüggen, Esra Bulbul
Figure caption: Stacked synthetic observations of XRB emission for galaxies with 11 < log(M*/M⊙) < 11.25 in EAGLE (top) and SIMBA (bottom). Each box is 22﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩5 across (≈2.5 Mpc at z = 0.1).
Paper: Confirming Near- to Mid-infrared Photometrically Identified Obscured AGNs in the JWST Era
Authors: George H. Rieke, Yang Sun, Jianwei Lyu, Christopher N. A. Willmer, Yongda Zhu, Pierluigi Rinaldi, Meredith A. Stone, Kevin N. Hainline, Pablo G. Pérez-González
Figure caption: Comparison of Haro 11 mid-infrared spectra with those of heavily obscured AGN examples. The figure also shows the WISE photometry of low-metallicity galaxies picked as possible AGN mimics. All data are normalized at ∼5 μm.
Paper: Confirming Near- to Mid-infrared Photometrically Identified Obscured AGNs in the JWST Era
Authors: George H. Rieke, Yang Sun, Jianwei Lyu, Christopher N. A. Willmer, Yongda Zhu, Pierluigi Rinaldi, Meredith A. Stone, Kevin N. Hainline, Pablo G. Pérez-González
Figure caption: Spectra of six of the sources discussed in this paper. The Hα lines have been indicated for quick orientation.
Paper: Interpreting Cosmological Information from Neural Networks in the Hydrodynamic Universe
Authors: Arnab Lahiry, Adrian E. Bayer, Francisco Villaescusa-Navarro
Figure caption: Underdensity cut inference. The R2 scores (left) and average variance ﹩\bar{{\sigma }^{2}}﹩ (right) of the predicted cosmological parameters Ωm (circles in blue) and σ8 (squares in red) as a function of ﹩{\rho }_{{\rm{\min }}}﹩. The solid lines represent the maps from the hydrodynamic simulations, the dashed lines represent the maps from the N-body simulations, and the dotted line represents the case where an equal number of pixels to the corresponding ﹩{\rho }_{{\rm{\min }}}﹩ case is randomly augmented for each N-body map.
Paper: Interpreting Cosmological Information from Neural Networks in the Hydrodynamic Universe
Authors: Arnab Lahiry, Adrian E. Bayer, Francisco Villaescusa-Navarro
Figure caption: Random density cut Integrated Gradients. Illustration of the random cutting procedure where, for each underdensity threshold value ﹩{\rho }_{{\rm{\min }}}=﹩ 1011, 2 × 1011, 4 × 1011, 6 × 1011, 8 × 1011, 1012,   and 2 × 1012  (M⊙/h)/(Mpc/h)2, an equal number of pixels are randomly selected and replaced with values uniformly sampled from the global minimum and maximum across all maps. These randomly augmented maps (left column) are used to examine whether the cosmological inference is sensitive to the spatial structure of the removed pixels. The right column shows the corresponding Integrated Gradients attribution maps for Ωm, with Integrated Gradients values normalized between 0 and 1 (the black-and-white scale is chosen for optimal visualization of patterns).
Paper: Interpreting Cosmological Information from Neural Networks in the Hydrodynamic Universe
Authors: Arnab Lahiry, Adrian E. Bayer, Francisco Villaescusa-Navarro
Figure caption: Overdensity cut Integrated Gradients. Illustration of the overdensity cutting procedure applied to density maps. For each threshold value ﹩{\rho }_{{\rm{\max }}}=1{0}^{12}﹩, 5 × 1011, 2 × 1011, 1011, and 5 × 1010  (M⊙/h)/(Mpc/h)2, pixel values above ﹩{\rho }_{{\rm{\max }}}﹩ are replaced with random values uniformly sampled from the global minimum and maximum density values across all maps. These augmented maps (left column) are used to train the neural network to assess the impact of overdensity cutting on cosmological parameter inference. The right column shows the corresponding Integrated Gradients attribution maps for Ωm, with Integrated Gradients values normalized between 0 and 1 (the black-and-white scale is chosen for optimal visualization of patterns).
Paper: Interpreting Cosmological Information from Neural Networks in the Hydrodynamic Universe
Authors: Arnab Lahiry, Adrian E. Bayer, Francisco Villaescusa-Navarro
Figure caption: Underdensity cut Integrated Gradients. Illustration of the underdensity cutting procedure applied to density maps. For each ﹩{\rho }_{{\rm{\min }}}=﹩ 1011, 2 × 1011, 4 × 1011, 6 × 1011, 8 × 1011, 1012, and 2 × 1012  (M⊙/h)/(Mpc/h)2, pixel values below ﹩{\rho }_{{\rm{\min }}}﹩ are replaced with random values uniformly sampled from the global minimum and maximum density values across all maps. These augmented maps (left columns) are used to train the neural network to assess the impact of underdensity cutting on cosmological parameter inference. The right column shows the corresponding Integrated Gradients attribution maps for Ωm, with Integrated Gradients values normalized between 0 and 1 (the black-and-white scale is chosen for optimal visualization of patterns).
Paper: Interpreting Cosmological Information from Neural Networks in the Hydrodynamic Universe
Authors: Arnab Lahiry, Adrian E. Bayer, Francisco Villaescusa-Navarro
Figure caption: Histogram of the matter density pixel values. The dashed lines (triangles) represent the upper-limit density cuts (﹩{\rho }_{{\rm{\max }}}﹩), and the solid lines (circles) represent the lower-limit density cuts (﹩{\rho }_{{\rm{\min }}}﹩). The top axis shows the values of ρ in various multiples of the average density ﹩\bar{\rho }=4.29\times 1{0}^{11}﹩  (M⊙/h)/(Mpc/h)2 at z = 0.
Paper: Interpreting Cosmological Information from Neural Networks in the Hydrodynamic Universe
Authors: Arnab Lahiry, Adrian E. Bayer, Francisco Villaescusa-Navarro
Figure caption: Fourier scale cut inference. The R2 scores (left) and average variance ﹩\bar{{\sigma }^{2}}﹩ (right) of the predicted cosmological parameters Ωm (circles in blue) and σ8 (squares in red) as a function of ﹩{k}_{{\rm{\max }}}﹩ for the hydrodynamic maps. Note that the Nyquist frequency is ∼32 h/Mpc. At low ﹩{k}_{{\rm{\max }}}﹩ there is a sharp increase in the R2 and a decrease in variance up to around ﹩{k}_{{\rm{\max }}}\sim 20\,{h}/{\rm{Mpc}}﹩, with only a slight improvement when including smaller scales.
Paper: Interpreting Cosmological Information from Neural Networks in the Hydrodynamic Universe
Authors: Arnab Lahiry, Adrian E. Bayer, Francisco Villaescusa-Navarro
Figure caption: Schematic of the CNN architecture employed in parameter estimation. There are sets of multiple convolution layers with a kernel size = 4, stride = 2, and padding = 1, coupled with 2D batch normalization and LeakyReLU activation functions. The 256 × 256 × 1 image is convolved and flattened into a 1D array and is then connected to an output array of size 12 (posterior mean and variance for the six inferred parameters) using fully connected layers.
Paper: Interpreting Cosmological Information from Neural Networks in the Hydrodynamic Universe
Authors: Arnab Lahiry, Adrian E. Bayer, Francisco Villaescusa-Navarro
Figure caption: Interpretability maps. Saliency Map, Integrated Gradients, and GradientSHAP interpretability methods for Ωm (top right) and σ8 (bottom right) for an example image of the cosmic web (left). The cosmic web map is scaled logarithmically. Black color in the attribution plots refers to features that are important to the neural network, while white implies low importance.
Paper: Interpreting Cosmological Information from Neural Networks in the Hydrodynamic Universe
Authors: Arnab Lahiry, Adrian E. Bayer, Francisco Villaescusa-Navarro
Figure caption: Fourier scale cuts. An example of applying a top-hat filter in k-space to a total matter density map for ﹩{k}_{{\rm{\max }}}=50,30,20,10,5﹩, and 1  h/Mpc.
Paper: Millimeter-wave Spectrum Analysis and Searches for 2-aminopropenenitrile (﹩{{\rm{H}}}_{2}{\rm{C}}\rm{=}{\rm{C}}({\mathrm{NH}}_{2})\mathrm{CN}﹩) toward the Galactic Center Sources Sgr B2(N1) and G+0.693–0.027
Authors: Kateřina Luková, Lucie Kolesniková, Jean-Claude Guillemin, Tereza Uhlíková, Jan Koucký, František Horák, Lukáš Hrubčík, Karel Vávra, Patrik Kania, Štěpán Urban, Arnaud Belloche, Izaskun Jiménez-Serra, Víctor M. Rivilla
Figure caption: Section of the millimeter-wave spectrum of 2-APN. Two representative lines corresponding to the overlapped a-type R-branch Ka = 0, 1 (J =26 ← 25) and 1, 2 (J =25 ← 24) transitions are shown for the vibrational ground state (G.S., 0+ and 0− pair) and vibrational satellites (S1–S9). S1 and S2 correspond to the 0+ and 0− states in the v21 = 1 excited vibrational state, respectively, while S7 and S9 correspond to the 0+ and 0− states in the v21 = 2 state, respectively.
Paper: On the Origin of Neutron-capture Elements in r-I and r-II Stars: A Differential-abundance Analysis
Authors: Pallavi Saraf, Thirupathi Sivarani, Timothy C. Beers, Yutaka Hirai, Masaomi Tanaka, Carlos Allende Prieto, Drisya Karinkuzhi
Figure caption: The evolution of [Sr/Eu], as a function of [Eu/Fe]. The gray, yellow, cyan, and magenta colors represent non-RPE stars, limited-r stars, r-I stars, and r-II stars, respectively. The black-solid lines are linear fits to the data, and the gray-shaded regions are the 1σ dispersions. The gray-dashed horizontal lines represent solar values. The predictions for mixing NSM ejecta in the ISM with metallicity of [Fe/H] = −3.5, −3.0, −2.5, −2.0, −1.5 are shown using blue, orange, green, red, and purple color curves, respectively. See text for details on mixing simulated NSM ejecta into the ISM.
Paper: Millimeter-wave Spectrum Analysis and Searches for 2-aminopropenenitrile (﹩{{\rm{H}}}_{2}{\rm{C}}\rm{=}{\rm{C}}({\mathrm{NH}}_{2})\mathrm{CN}﹩) toward the Galactic Center Sources Sgr B2(N1) and G+0.693–0.027
Authors: Kateřina Luková, Lucie Kolesniková, Jean-Claude Guillemin, Tereza Uhlíková, Jan Koucký, František Horák, Lukáš Hrubčík, Karel Vávra, Patrik Kania, Štěpán Urban, Arnaud Belloche, Izaskun Jiménez-Serra, Víctor M. Rivilla
Figure caption: Potential energy scan for the –NH2 inversion and rotation about the C1–N3 bond. The relative energies are in cm−1. The barrier heights hindering the inversion and rotation motions are displayed in white.
Paper: Millimeter-wave Spectrum Analysis and Searches for 2-aminopropenenitrile (﹩{{\rm{H}}}_{2}{\rm{C}}\rm{=}{\rm{C}}({\mathrm{NH}}_{2})\mathrm{CN}﹩) toward the Galactic Center Sources Sgr B2(N1) and G+0.693–0.027
Authors: Kateřina Luková, Lucie Kolesniková, Jean-Claude Guillemin, Tereza Uhlíková, Jan Koucký, František Horák, Lukáš Hrubčík, Karel Vávra, Patrik Kania, Štěpán Urban, Arnaud Belloche, Izaskun Jiménez-Serra, Víctor M. Rivilla
Figure caption: Equilibrium geometry of 2-APN with indication of the angles used for the calculation of the potential energy scan from Figure 2. Labels l and k denote two perpendicular planes.
Paper: On the Origin of Neutron-capture Elements in r-I and r-II Stars: A Differential-abundance Analysis
Authors: Pallavi Saraf, Thirupathi Sivarani, Timothy C. Beers, Yutaka Hirai, Masaomi Tanaka, Carlos Allende Prieto, Drisya Karinkuzhi
Figure caption: The evolution of first-peak r-process abundance ratios ([Sr/Ba], [Y/Ba], and [Zr/Ba]), as a function of [Ba/Fe]. The gray, yellow, cyan, and magenta colors represent non-RPE stars, limited-r stars, r-I stars, and r-II stars, respectively. The black-solid lines are linear fits to the data, and the gray-shaded regions are the 1σ dispersions. The fitted equations are shown on the top of respective panels. The gray-dashed horizontal lines represent solar values. For reference, see P. Saraf et al. (2023) and P. Saraf & T. Sivarani (2024).
Paper: On the Origin of Neutron-capture Elements in r-I and r-II Stars: A Differential-abundance Analysis
Authors: Pallavi Saraf, Thirupathi Sivarani, Timothy C. Beers, Yutaka Hirai, Masaomi Tanaka, Carlos Allende Prieto, Drisya Karinkuzhi
Figure caption: Comparison overplots of different regions corresponding to the listed non neutron-capture elements of CS 31082-001 (black-dotted curves) and HD 107752 (magenta-solid curves)
Paper: Millimeter-wave Spectrum Analysis and Searches for 2-aminopropenenitrile (﹩{{\rm{H}}}_{2}{\rm{C}}\rm{=}{\rm{C}}({\mathrm{NH}}_{2})\mathrm{CN}﹩) toward the Galactic Center Sources Sgr B2(N1) and G+0.693–0.027
Authors: Kateřina Luková, Lucie Kolesniková, Jean-Claude Guillemin, Tereza Uhlíková, Jan Koucký, František Horák, Lukáš Hrubčík, Karel Vávra, Patrik Kania, Štěpán Urban, Arnaud Belloche, Izaskun Jiménez-Serra, Víctor M. Rivilla
Figure caption: (a) Section of the recorded THz spectrum where a signal possibly attributable to 2-APN is labeled with a gray star. (b) Prediction of the cQ-transitions of 2-APN based on the spectroscopic constants from Table 1 and ΔE =  49.685 cm−1. (c) Deterioration of the plausible 2-APN signal with time.
Paper: On the Origin of Neutron-capture Elements in r-I and r-II Stars: A Differential-abundance Analysis
Authors: Pallavi Saraf, Thirupathi Sivarani, Timothy C. Beers, Yutaka Hirai, Masaomi Tanaka, Carlos Allende Prieto, Drisya Karinkuzhi
Figure caption: Comparison overplot of different regions corresponding to the listed neutron-capture elements of CS 31082-001 (black-dotted curves) and HD 107752 (magenta-solid curves).
Paper: Creating Pileups of Eccentric Planet Pairs Wide of Mean Motion Resonances through Divergent Migration
Authors: Jingyun Lin, 靖云 林, Ivan Dudiak, Samuel Hadden, Daniel Tamayo
Figure caption: Evolution across the 3:2 MMR for two ≈1.5M⊕ planets, varying the migration timescale relative to ﹩{\tau }_{a}^{{\rm{crit}}}﹩ (Equation (7)). In the adiabatic limit where ﹩{\tau }_{a}\gg {\tau }_{a}^{{\rm{crit}}}﹩ (blue), we recover the full magnitude of the jumps obtained above. For migration timescales comparable to (orange) or shorter (green) than ﹩{\tau }_{a}^{{\rm{crit}}}﹩, the size of the jump is suppressed. This could help explain the low eccentricities in Figure 5 for observed TTV systems.
Paper: Creating Pileups of Eccentric Planet Pairs Wide of Mean Motion Resonances through Divergent Migration
Authors: Jingyun Lin, 靖云 林, Ivan Dudiak, Samuel Hadden, Daniel Tamayo
Figure caption: N-body integration crossing the 3:2 MMR with an eccentricity damping timescale τe = τa/100.
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Power spectra of fluctuations in the X-ray (left) and radio (right) images of the Tycho SNR calculated as FFT amplitudes of the autocorrelation functions and averaged over the azimuthal angle. The spectra are obtained after applying a correction for a geometrical factor for each pixel in the image. Different assumptions about the geometrical factor η are considered. The shaded regions display 1σ statistical uncertainties. To prevent overlapping, consecutive spectra were shifted by a factor of 1/100. The red dashed lines correspond to the best-fit power laws; see the text for their spectral indices.
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Two-dimensional discrete Fourier transform of the autocorrelation function from the image before background noise cancellation, for the X-ray image of the Tycho SNR (left column) and its radio image (right column). The color scale corresponds to the decimal logarithm of the Fourier amplitudes. The red circle marks the 1/3″ wavenumber. The same distributions after background noise cancellation are shown in Figure 3.
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Average power spectra for a number of sectors calculated from CFTs of the individual radial profiles of X-ray brightness within the sector. The red dashed lines indicate the Kolmogorov-type 5/3 power law; the amplitude is the same on all plots. Spatial scales are normalized to the average radius ﹩R={4}^{{\prime} }﹩. Vertical lines mark the 1/R, 1/3″, and Nyquist wavenumbers. Spectra start at different k because the radius of each sector is different.
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: The same power spectra as shown by the solid lines in Figure 9, for X-ray (left) and radio (right) images. Different assumptions about the geometrical factor η are considered. Red dashed lines correspond to k−5/3.
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Radial autocorrelation functions from the radial profiles extracted from the X-ray image of the Tycho SNR. They are calculated for each of the individual profiles within a 15° sector and then averaged across the sector. The numbers in the legend correspond to the angle where a given sector begins. The errors shown are at the 1σ level. The red dashed line corresponds to a correlation of 0.1.
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Radial profiles extracted from the X-ray image of the Tycho SNR. Profiles are calculated as an average within 15° sectors, which begin at the angle written in the legend of each plot. Dotted horizontal lines mark the profile’s average value. The errors shown are at the 1σ level.
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Same as in Figure 18 but for the radio data.
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Same as in Figure 14 but for the radio image of the Tycho SNR.
Paper: On the Properties of Turbulence in the Remnant of the Tycho Supernova
Authors: Oleh Petruk, Taras Kuzyo
Figure caption: Same as in Figure 16 but for the radio image.
Paper: The Role of Spiral Arms in Galaxies. II. Similarities amid Diversity
Authors: Bingqing Sun, Daniela Calzetti, Andrew J. Battisti
Figure caption: Similar to Figure 11, but for SFR10Myr.
Paper: The Role of Spiral Arms in Galaxies. II. Similarities amid Diversity
Authors: Bingqing Sun, Daniela Calzetti, Andrew J. Battisti
Figure caption: SFE vs. sSFR for each galaxy.
Paper: The AURORA Survey: Tracing Galactic Outflows at z ≳ 2.5 with JWST/NIRSpec Near-ultraviolet Absorption Lines
Authors: Emily Kehoe, Alice E. Shapley, Ryan L. Sanders, Naveen A. Reddy, Michael W. Topping, Natalie Lam, Leonardo Clarke, Fergus Cullen, Richard S. Ellis, N. M. Förster Schreiber, Tucker Jones, Ali Ahmad Khostovan, Derek J. McLeod, Ross J. McLure, Desika Narayanan, Pascal Oesch, Anthony J. Pahl
Figure caption: Outflow velocity vs. various galaxy properties. Blue filled circles are velocities measured from Fe II centroids. Red filled squares are velocities from the Mg II doublet measured from MCMC. Large blue open circles are velocities from the Fe II stacks. Large red open squares are velocities from the Mg II stacks. Large red filled squares are ﹩{v}_{{\rm{\max }}}﹩ measured from the Mg II stacks. We were unable to robustly determine ﹩{v}_{{\rm{\max }}}﹩ for the high-sSFR composite owing to its complex profile shape. Large blue circles are ﹩{v}_{{\rm{\max }}}﹩ measured from the Fe II stacks. The dashed gray line indicates the separation between the low and high bins for each property. The individual measurements and composite spectra show no correlation between outflow velocity and galaxy property. The ﹩{v}_{{\rm{\max }}}﹩ measured from Mg II suggests that the amplitude of the outflow maximum velocity increases with M*, SFR, β, E(B − V), and AV.
Paper: The AURORA Survey: Tracing Galactic Outflows at z ≳ 2.5 with JWST/NIRSpec Near-ultraviolet Absorption Lines
Authors: Emily Kehoe, Alice E. Shapley, Ryan L. Sanders, Naveen A. Reddy, Michael W. Topping, Natalie Lam, Leonardo Clarke, Fergus Cullen, Richard S. Ellis, N. M. Förster Schreiber, Tucker Jones, Ali Ahmad Khostovan, Derek J. McLeod, Ross J. McLure, Desika Narayanan, Pascal Oesch, Anthony J. Pahl
Figure caption: Comparisons of galaxies with detected outflows (Δv < 0 and the magnitude of Δv greater than its uncertainty) from Fe II lines (blue) or Mg II (red) and galaxies where no outflow was detected (black) for the various galaxy properties. Average property values are printed in the upper right corner. The average M* is significantly higher for galaxies with outflows detected from either Fe II or Mg II, compared with galaxies in which no outflow is detected.
Paper: The AURORA Survey: Tracing Galactic Outflows at z ≳ 2.5 with JWST/NIRSpec Near-ultraviolet Absorption Lines
Authors: Emily Kehoe, Alice E. Shapley, Ryan L. Sanders, Naveen A. Reddy, Michael W. Topping, Natalie Lam, Leonardo Clarke, Fergus Cullen, Richard S. Ellis, N. M. Förster Schreiber, Tucker Jones, Ali Ahmad Khostovan, Derek J. McLeod, Ross J. McLure, Desika Narayanan, Pascal Oesch, Anthony J. Pahl
Figure caption: Comparisons of the low (blue for the Fe II composite and red for the Mg II) and high (black) bins for the different stacks. The left portions of each panel are the Fe II stacks, and the right portions are the Mg II stacks. The dashed vertical lines mark the rest wavelengths for Fe II λ2587, Fe II λ2600, Mg II λ2796, and Mg II λ2803. The Mg II stacks for M*, β, and AV exhibit the strongest evidence of Mg II emission in the low bins.
Paper: The AURORA Survey: Tracing Galactic Outflows at z ≳ 2.5 with JWST/NIRSpec Near-ultraviolet Absorption Lines
Authors: Emily Kehoe, Alice E. Shapley, Ryan L. Sanders, Naveen A. Reddy, Michael W. Topping, Natalie Lam, Leonardo Clarke, Fergus Cullen, Richard S. Ellis, N. M. Förster Schreiber, Tucker Jones, Ali Ahmad Khostovan, Derek J. McLeod, Ross J. McLure, Desika Narayanan, Pascal Oesch, Anthony J. Pahl
Figure caption: Histograms showing the distributions of various galaxy properties for the Mg II nonemitter (blue) and Mg II emitter (red) samples. The dashed blue and red lines show the property averages for nonemitters and emitters, respectively. On average, Mg II emitters have lower stellar mass, higher sSFR, lower β, and lower AV than Mg II nonemitters.
Paper: The AURORA Survey: Tracing Galactic Outflows at z ≳ 2.5 with JWST/NIRSpec Near-ultraviolet Absorption Lines
Authors: Emily Kehoe, Alice E. Shapley, Ryan L. Sanders, Naveen A. Reddy, Michael W. Topping, Natalie Lam, Leonardo Clarke, Fergus Cullen, Richard S. Ellis, N. M. Förster Schreiber, Tucker Jones, Ali Ahmad Khostovan, Derek J. McLeod, Ross J. McLure, Desika Narayanan, Pascal Oesch, Anthony J. Pahl
Figure caption: Properties of galaxies from the AURORA survey. Left: redshift distribution of the full survey (black histogram), of galaxies with measured Fe II centroids (blue histogram), and of galaxies with measured Mg II centroids (red histogram). Right: the SFR and stellar masses for the full survey (open black circles), galaxies with measured Fe II centroids (blue circles), and galaxies with measured Mg II centroids (red squares). The dashed line represents the SFR main sequence from J. S. Speagle et al. (2014) at z ∼ 3. Our Fe II and Mg II samples scatter well around the star-forming main sequence.