adsabs/AstroCLIMB huggingface dataset:
Paper: Unresolved z ∼ 8 Point Sources and Their Impact on the Bright End of the Galaxy Luminosity Function
Authors: Yuzo Ishikawa, Takahiro Morishita, Massimo Stiavelli, Nicha Leethochawalit, Harry Ferguson, Roberto Gilli, Charlotte Mason, Michele Trenti, Tommaso Treu, Colin Norman
Figure caption: The derived number density of the 3D-HST point sources in red, of the SuperBoRG point sources (Morishita et al. 2020) in blue, and of galaxies at z ∼ 7–8 (Bouwens et al. 2021) in black. The z ∼ 7 number density from Harikane et al. (2022) is in green. Open symbols indicate observed data, and filled symbols indicate upper limits, which are estimated from the completeness simulation. Our number density values are listed in Table 6.
Paper: Unresolved z ∼ 8 Point Sources and Their Impact on the Bright End of the Galaxy Luminosity Function
Authors: Yuzo Ishikawa, Takahiro Morishita, Massimo Stiavelli, Nicha Leethochawalit, Harry Ferguson, Roberto Gilli, Charlotte Mason, Michele Trenti, Tommaso Treu, Colin Norman
Figure caption: Low-redshift template (blue), z ∼ 6 SDSS composite (gray), and full composite quasar spectrum (red).
Paper: Relationship between Total Solar Irradiance and Magnetic Flux during Solar Minima
Authors: Sergey V. Marchenko, Judith L. Lean, Matthew T. DeLand
Figure caption: Shown in (a) are the time series of the total magnetic flux (red line, the integral of the red histograms in Figure 9(a)) and of the total flux within the histograms’ Gaussian cores (black line, the integral of the black histograms in Figure 9). Shown in (b) by the blue line is the difference between the total magnetic flux of the entire Sun and the total flux within the Gaussian core for 2008 and 2009. The blue symbols indicate days without sunspots and with minimal faculae. Also shown for comparison is the TSI (green line) where the gray symbols identify days without sunspots and with minimal faculae.
Paper: Relationship between Total Solar Irradiance and Magnetic Flux during Solar Minima
Authors: Sergey V. Marchenko, Judith L. Lean, Matthew T. DeLand
Figure caption: Shown in (a) by the red curves are histograms of the MDI full-disk images of magnetic flux, once per day from 1996 to 2010 (inclusive), and by the green curves, for just days during the 2008 and 2009 extended activity minimum epoch. Shown in (b) by the green curves are the histograms of days during 2008 and 2009 (as in (a)). The blue curves are histograms of the MDI magnetic flux for days when there were no sunspots on the disk, and the pink curves are histograms for days when there were no sunspots and minimal faculae, defined by the Bremen Mg II index in the range 0.1500 to 0.1507 (for comparison, the solar-cycle range of the Mg II index is 0.150–0.174). The black lines in both (a) and (b) are Gaussian fits to the individual histograms.
Paper: Relationship between Total Solar Irradiance and Magnetic Flux during Solar Minima
Authors: Sergey V. Marchenko, Judith L. Lean, Matthew T. DeLand
Figure caption: Shown is the scatter plot of the total flux within the histograms’ Gaussian cores (B core, black line in Figure 10(a)) vs. the total magnetic flux (B tot, red line in Figure 10(a)) determined using MDI magnetograms from 1996 to 2011. The red line is a linear fit to the scatter plot, and the value of r is the linear correlation coefficient. The green line is a fit based on local regression smoothing (LOWESS) with width 5 G.
Paper: Relationship between Total Solar Irradiance and Magnetic Flux during Solar Minima
Authors: Sergey V. Marchenko, Judith L. Lean, Matthew T. DeLand
Figure caption: Shown as colored lines are time series of (a) the total number of pixels in the Gaussian cores of the histograms (black lines in Figure 9), (b) the number of pixels at the histogram peak intensity, (c) the FWHM of the Gaussian fits to the histograms, and (d) the pixel location of the histogram maximum intensity. The underlying black symbols in each panel are the corresponding values for Gaussian fits to 11 different histograms of only quiet-Sun pixels.
Paper: Relationship between Total Solar Irradiance and Magnetic Flux during Solar Minima
Authors: Sergey V. Marchenko, Judith L. Lean, Matthew T. DeLand
Figure caption: Black lines: the individual 40 minute averages of the magnetic field strengths of short-living (t ≤ 15 minutes) sources with ∣B∣ ≥ 40 G. Pink line: the average dependence for all selected sources on 2008 July 3.
Paper: Relationship between Total Solar Irradiance and Magnetic Flux during Solar Minima
Authors: Sergey V. Marchenko, Judith L. Lean, Matthew T. DeLand
Figure caption: Surface fraction pdfs for the “low” and “high” TSI cases with corresponding ±σ uncertainties.
Paper: A Rosetta Stone for Eccentric Gravitational Waveform Models
Authors: Alan M. Knee, Isobel M. Romero-Shaw, Paul D. Lasky, Jess McIver, Eric Thrane
Figure caption: Left panel: mismatch between TEOBResumS waveforms and a fiducial SEOBNRE waveform for an equal-mass non-spinning BBH with total mass 200 M ⊙ in the detector frame, assuming a white noise PSD. The TEOBResumS waveforms are distributed over a grid in waveform eccentricity and (Keplerian) reference frequency. The SEOBNRE waveform has ﹩{e}_{0}^{\mathrm{SEOB}}=0.1﹩ at 10 Hz. The color scale shows the log-scaled mismatch between the waveforms at each grid point, where darker shading indicates a smaller mismatch. The regions of lower mismatch coincide with successive alignments of the arguments of periastron. The red cross marks the grid point with the lowest mismatch, which sits at the center of a bounding box that is used as the search range for the optimization algorithm. The true minimum found by the optimizer is given by the cyan star, which is at a mismatch of ﹩1-{ \mathcal O }=0.0071﹩. For reference, the mismatch found when supplying identical parameters to both waveforms is 0.1567. The cyan curve shows the eccentricity evolution track calculated with Peters’ equations, which is used to forward-evolve the eccentricity to 10 Hz. Right panels: comparison of the fiducial SEOBNRE waveform (as observed in a detector; red curve) with two TEOBResumS waveforms, in which we supply either identical parameters as SEOBNRE (blue curve) or the optimal parameters (dashed black curve) from the parameter search that give the minimum mismatch. The top panel shows the time-domain strain, and the bottom panel shows the frequency evolution. The plotted waveforms are each aligned in coalescence phase and time. The small vertical feature in the red curve of the bottom panel, at around t ≈ −0.05 s, reflects a slight discontinuity inherent to the waveform model.
Paper: A Rosetta Stone for Eccentric Gravitational Waveform Models
Authors: Alan M. Knee, Isobel M. Romero-Shaw, Paul D. Lasky, Jess McIver, Eric Thrane
Figure caption: Mismatch between the eccentric and quasi-circular versions of TEOBResumS and SEOBNRE (50 M ⊙ + 50 M ⊙, non-spinning), plotted as a function of waveform eccentricity at 10 Hz. As the eccentricity of SEOBNRE decreases, there is a corresponding decrease in mismatch with its quasi-circular counterpart. In contrast, the mismatch between the eccentric model TEOBResumS-DALI and the quasi-circular model TEOBResumS-GIOTTO levels off at a minimum value, reflecting a discontinuity between the behaviors of the two models. As in Figure 2, the mismatches are shown for white noise (solid curves) and LVK sensitivity (dashed curves), and we use the same frequency adjustment for TEOBResumS.
Paper: A Rosetta Stone for Eccentric Gravitational Waveform Models
Authors: Alan M. Knee, Isobel M. Romero-Shaw, Paul D. Lasky, Jess McIver, Eric Thrane
Figure caption: Mismatch between TEOBResumS and SEOBNRE as a function of waveform eccentricity at 10 Hz, showing how the mismatch increases with higher eccentricity. Curves are shown for equal-mass systems with different total masses as indicated. The reference frequencies supplied to TEOBResumS are adjusted so that the waveform starts with a Keplerian frequency of 10 Hz, ensuring consistency with the way SEOBNRE defines the reference frequency. We show mismatches calculated for both white noise (solid curves) and LVK sensitivity (dashed curves).
Paper: Dropouts of Fully Stripped Ions in the Solar Wind: A Diagnostic for Wave Heating versus Reconnection
Authors: John C. Raymond, M. Asgari-Targhi, Maurice L. Wilson, Yeimy J. Rivera, Susan T. Lepri, Chengcai Shen
Figure caption: Flow parameters along a particular streamline in a pseudostreamer computed with the MAS model, as presented in Shen et al. (2017) (solid lines). The dashed lines show a clumpy AWT model similar to that of Asgari-Targhi et al. (2021), but for the magnetic field expansion of Shen et al. (2017) and fractional density inhomogeneities similar to those computed by Asgari-Targhi et al. (2021) (dashed lines).
Paper: A Rosetta Stone for Eccentric Gravitational Waveform Models
Authors: Alan M. Knee, Isobel M. Romero-Shaw, Paul D. Lasky, Jess McIver, Eric Thrane
Figure caption: Comparison of the two waveform models, TEOBResumS and SEOBNRE, for an equal-mass, non-spinning BBH with a total mass of ﹩{M}_{\det }=100\,{M}_{\odot }﹩ in the detector frame, showing the (ℓ = 2, ∣m∣ = 2) waveform frequency as a function of time. The waveforms are given identical input parameters, with waveform eccentricity e 0 = 0.1 at a reference frequency of 10 Hz (indicated by a horizontal line). For the same input value of eccentricity, the frequency oscillations in TEOBResumS are noticeably larger, implying a higher simulated eccentricity. TEOBResumS also interprets the reference frequency differently (described in Section 2.2), causing it to start at a lower frequency than SEOBNRE. Lastly, the waveforms start from different points in the orbit: TEOBResumS starts from apastron (a trough), and SEOBNRE starts from periastron (a peak).
Paper: Dropouts of Fully Stripped Ions in the Solar Wind: A Diagnostic for Wave Heating versus Reconnection
Authors: John C. Raymond, M. Asgari-Targhi, Maurice L. Wilson, Yeimy J. Rivera, Susan T. Lepri, Chengcai Shen
Figure caption: Heating rate along the streamline shown in Figure 1 for the clumpy AWT model. Excursions above and below the average by an order of magnitude occur on small scales, especially below 5 R ☉.
Paper: Dropouts of Fully Stripped Ions in the Solar Wind: A Diagnostic for Wave Heating versus Reconnection
Authors: John C. Raymond, M. Asgari-Targhi, Maurice L. Wilson, Yeimy J. Rivera, Susan T. Lepri, Chengcai Shen
Figure caption: Timescales computed for the models shown in Figure 1. For each model, the flow time (taken to be 0.3 R/V; solid line), ionization timescale for C5+ (1./(density × ionization rate); dashed line), Coulomb energy loss timescale (dashed–dotted), and heating timescale (dotted) are given. The smooth flow magnetohydrodynamics on a sphere (MAS) model (Shen et al. 2017) is shown in the left panel, and the clumpy AWT model in the right panel.
Paper: Dropouts of Fully Stripped Ions in the Solar Wind: A Diagnostic for Wave Heating versus Reconnection
Authors: John C. Raymond, M. Asgari-Targhi, Maurice L. Wilson, Yeimy J. Rivera, Susan T. Lepri, Chengcai Shen
Figure caption: C6+ over C5+ ionization fractions for one streamline of the MAS model (solid line) and the MAS model with the temperature from the clumpy AWT model (dashed line). The figure emphasizes the large range of possible ionization states, but shows that for this streamline, the C6+ ionization fraction freezes in below 3 R ☉.
Paper: The Molecular Composition of Shadowed Proto-solar Disk Midplanes Beyond the Water Snowline
Authors: Shota Notsu, Kazumasa Ohno, Takahiro Ueda, Catherine Walsh, Christian Eistrup, Hideko Nomura
Figure caption: The radial profiles of C/H ratios at t =106 yr. The dashed and solid lines show the profiles for gaseous and icy molecules, respectively. The black, red, blue, and green lines show the profiles for different values of the parameter f (=1.0, 0.3, 0.03, and 0.003), respectively. The top panels show the results when assuming molecular initial abundances (the “inheritance” scenario), whereas the bottom panels show those when assuming atomic initial abundances (“reset” scenario). The left panels show the results for ξ CR(r) =1.0 × 10−17 [s−1], whereas right panels show the results for ξ CR(r) =1.0 × 10−18 [s−1]. The initial elemental C/H ratio is 1.40 × 10−4.
Paper: The Molecular Composition of Shadowed Proto-solar Disk Midplanes Beyond the Water Snowline
Authors: Shota Notsu, Kazumasa Ohno, Takahiro Ueda, Catherine Walsh, Christian Eistrup, Hideko Nomura
Figure caption: Same as Figure 20, but for the radial profiles of O/H ratios at t =106 yr. The initial elemental O/H ratio is 3.20 × 10−4.
Paper: The Molecular Composition of Shadowed Proto-solar Disk Midplanes Beyond the Water Snowline
Authors: Shota Notsu, Kazumasa Ohno, Takahiro Ueda, Catherine Walsh, Christian Eistrup, Hideko Nomura
Figure caption: Same as Figure 20, but for the radial profiles of N/H ratios at t =106 yr. The initial elemental N/H ratio is 7.50 × 10−5.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Metallicities of the SLFSs (﹩14.5\lt \mathrm{log}{N}_{{\rm{H}}\,{\rm\small{I}}}\lt 16.2﹩), pLLSs (﹩16.2\,\leqslant \mathrm{log}{N}_{{\rm{H}}\,{\rm\small{I}}}\lt 17.2﹩), LLSs (﹩17.2\leqslant \mathrm{log}{N}_{{\rm{H}}\,{\rm\small{I}}}\lt 19﹩), SLLSs (﹩19\,\leqslant \mathrm{log}{N}_{{\rm{H}}\,{\rm\small{I}}}\lt 20.3﹩), and DLAs (﹩\mathrm{log}{N}_{{\rm{H}}\,{\rm\small{I}}}\geqslant 20.3﹩) at 2.2. ≲ z ≲ 3.6 as a function of N H I . The blue data are from the KODIAQ-Z survey (this paper). The orange data are from the HD-LLS survey (Fumagalli et al. 2016b), but we reestimated the metallicities of these absorbers following the same EUVB and methodology as in KODIAQ-Z. The purple data (DLAs) are from Rafelski et al. (2012).
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: The metallicity of different absorbers as a function of the redshift. For the HD-LLS and KODIAQ-Z surveys, lighter symbols are upper limits on the metallicity. For CCC, lighter symbols are upper limits if [X/H] ≤ − 1 and lower limits if [X/H] > − 1. Median metallicities are plotted for the CCC, KODIAQ-Z, and HD-LLS surveys, but we treat upper and lower limits as in Figure 19, i.e., the lower and upper values represent the 10th and 90th percentiles, respectively.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: The metallicity as a function of N H I  at low z (CCC) and high z (KODIAQ-Z, HD-LLS, R12-DLA). For the z < 1 absorbers, we subtract the metallicity of each absorber by 0.9 dex (see text for more details). For the black circles, lighter symbols are upper limits on the metallicity. For the blue plus signs, lighter symbols are upper limits if [X/H] ≤ − 1 and lower limits if [X/H] > − 1. For clarity, we did not plot the error bars (which are available in Figure 19 and Figure 9 of CCCIII for the low-redshift sample). Median metallicities are plotted, but we treat upper and lower limits as in Figure 19, i.e., the lower and upper values represent the 10th and 90th percentiles, respectively.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Left: scatter plot of the difference between the higher and lower median metallicities for the paired absorbers as a function of their absolute velocity difference. For the lower limits (blue triangles), we use the lower bound of the 80% CI to be the most conservative. Right: distribution of the metallicity differences between paired absorbers.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: The metallicities of closely redshift-separated KODIAQ-Z absorbers (aka paired absorbers) as a function of their absolute velocity difference. For the upper limits (blue triangles), we use the upper bound of the 80% CI to be the most conservative. Each paired absorber is connected with a dotted line.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Comparison of the metallicity CDFs of the absorbers in KODIAQ-Z and HD-LLS with ﹩14.5\leqslant \mathrm{log}{N}_{{\rm{H}}\,{\rm\small{I}}}\lt 19﹩ above and below a given redshift threshold, z th = 2.8, 2.9, and 3.0. The numbers between parentheses indicate the number of absorbers in each redshift interval.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Comparison of the posterior metallicity pdf’s of the absorbers with ﹩15\leqslant \mathrm{log}{N}_{{\rm{H}}\,{\rm\small{I}}}\lt 19﹩ at high and low redshifts. The light-colored region indicates the contribution from the upper limits. For CCC, the light-colored histogram indicates the contributions from upper and lower limits.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Cumulative probabilities of the SLFS, pLLS, LLS, SLLS, and DLA metallicity pdf’s. The SLFSs and pLLSs are from KODIAQ-Z, the LLSs and SLLSs from KODIAQ-Z and HD-LLS, and the DLAs from R12-DLA.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Posterior metallicity pdf of the absorbers with ﹩14.5\lesssim \mathrm{log}{N}_{{\rm{H}}\,{\rm\small{I}}}\lt 19﹩ in the combined sample of KODIAQ-Z and HD-LLS. The light-colored region indicates the contribution from the upper limits.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: The neutral fraction of H I vs. N H I  using the KODIAQ-Z and HD-LLS surveys. The median values of the posterior pdf’s are adopted with 68% CI. Light-blue data were estimated using a Gaussian prior on ﹩\mathrm{log}U﹩, while the other data have a flat prior on ﹩\mathrm{log}U﹩. The black curve is a GP-derived model to the entire N H I  range shown in the figure (the dark area corresponds to the dispersion derived from the GP model). The dashed red line is a linear fit to the data with ﹩14.6\leqslant \mathrm{log}{N}_{{\rm{H}}\,{\rm\small{I}}}\lt 19﹩ (i.e., the SLFSs, pLLSs, and LLSs). The dashed–dotted magenta line is a linear fit to the data with ﹩17.2\lt \mathrm{log}{N}_{{\rm{H}}\,{\rm\small{I}}}\leqslant 20﹩ (i.e., the LLSs and SLLSs). For all the models, we consider only data with a flat prior on ﹩\mathrm{log}U﹩ (although the results are similar if the entire data set was considered instead). The orange curve is a GP-derived model to the entire N H I  range but considering the neutral fraction derived using the HM12 EUVB instead of HM05.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Metallicities of the FOGGIE H I absorbers vs. their distance from the central galaxy, colored by the distance to their closest galaxy. Possible “closest galaxies” include the central satellite and all satellites with more than 1% of the central’s stellar mass. High-metallicity absorbers far from the central galaxy tend to be close to a satellite galaxy. Dashed and dotted lines are the same as in Figure 19.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Metallicities of the H I absorbers extracted from the FOGGIE cosmological zoom-in simulations (Peeples et al. 2019; Simons et al. 2020). On the left, all H I absorbers (cyan) are compared to the KODIAQ-Z, HD-LLS, and R12-DLA surveys (where we limit these surveys to 2 ≤ z ≤ 3 to match the FOGGIE redshift range). Contours have been added where the density of cyan scatter plot points is highest. In the middle panel, we only show H I absorbers that have been paired with a C IV (blue filled circles) or Si IV (orange open circles) absorber, analogous to requiring detection of C IV or Si IV with ﹩\mathrm{log}{N}_{{\rm{X}}}\gt 12﹩. Probability densities of both the full FOGGIE H I absorber population (cyan) and the subset with paired metal absorbers (blue and orange) are shown on the right. The dashed and dotted lines are the solar and VMP metallicity levels, respectively.
Paper: KODIAQ-Z: Metals and Baryons in the Cool Intergalactic and Circumgalactic Gas at 2.2 ≲ z ≲ 3.6
Authors: Nicolas Lehner, Claire Kopenhafer, John M. O'Meara, J. Christopher Howk, Michele Fumagalli, J. Xavier Prochaska, Ayan Acharyya, Brian W. O'Shea, Molly S. Peeples, Jason Tumlinson, Cameron B. Hummels
Figure caption: Metallicities of the FOGGIE H I absorbers in Figure 29, split into outflowing (red) and inflowing (blue) based on ﹩| \hat{v}\cdot \hat{r}| \gt 0.5﹩ in the frame of the host central galaxy. Saturation shows the magnitude of the radial velocity. Probability densities are provided as histograms along the side and top. Both metallicity distributions are repeated in the side panels, with the filled histogram corresponding to the adjacent scatter plot. Contours have been added to show where the density of inflowing absorbers is highest.