adsabs/AstroCLIMB huggingface dataset:
Paper: Constraining the Fluctuating Gunn–Peterson Approximation using Lyα Forest Tomography at z = 2
Authors: Robin Kooistra, Khee-Gan Lee, Benjamin Horowitz
Figure caption: Example realization of the Lyα transmission–DM density distribution of all simulations including CLAMATO-like noise. As before, the contours denote the 2%, 20%, and 80% levels of the PDF of the distribution, respectively. In each panel the hydrodynamical skewer distribution is compared to the respective FGPA-based distribution. The dotted lines show the fits to the distribution on the high-density side with the slopes α written in the bottom left corner of every panel, where the thick lines denote the hydrodynamical simulation slopes and the thin lines the FGPA slopes. The difference between the FGPA and hydrodynamical distributions can still clearly be recovered in all cases.
Paper: Constraining the Fluctuating Gunn–Peterson Approximation using Lyα Forest Tomography at z = 2
Authors: Robin Kooistra, Khee-Gan Lee, Benjamin Horowitz
Figure caption: Lyα transmission–DM density distribution of all simulations compared to their respective FGPA-based distributions. The contours denote the 2%, 20%, and 80% levels of the PDF of the distribution, respectively. The thick dotted line denotes the fit to the slope of the distribution based on the hydrodynamical skewers and the thin dotted line shows the same for the FGPA skewers. The values of the slopes α are written in the bottom left corner of every panel.
Paper: Constraining the Fluctuating Gunn–Peterson Approximation using Lyα Forest Tomography at z = 2
Authors: Robin Kooistra, Khee-Gan Lee, Benjamin Horowitz
Figure caption: Example realization of the Lyα transmission–DM density distribution of all simulations including ELT-like noise. The contours denote the 2%, 20%, and 80% levels of the PDF of the distribution, respectively. In each panel the hydrodynamical skewer distribution is compared to the respective FGPA-based distribution. The dotted lines show the fits to the distribution on the high-density side with the slopes α written in the bottom left corner of every panel, where the thick lines denote the hydrodynamical simulation slopes and the thin lines the FGPA slopes. The difference between the FGPA and hydrodynamical distributions can be recovered for all simulations and the contours are less noisy than was the case for CLAMATO-like realizations in Figure 4.
Paper: Constraining the Fluctuating Gunn–Peterson Approximation using Lyα Forest Tomography at z = 2
Authors: Robin Kooistra, Khee-Gan Lee, Benjamin Horowitz
Figure caption: PDFs normalized to unity of the slopes of the Lyα transmission–DM density distribution of all simulations including ELT-like noise. 100 realizations were used for EAGLE and 50 realizations for the other simulations. The panel on the left shows the distribution for full hydrodynamical skewers, whereas the right panel shows the same for skewers based on the FGPA. The mean of each distribution can be found in Table 2.
Paper: Constraining the Fluctuating Gunn–Peterson Approximation using Lyα Forest Tomography at z = 2
Authors: Robin Kooistra, Khee-Gan Lee, Benjamin Horowitz
Figure caption: PDFs normalized to unity of the slopes of 1000 realizations of the Lyα transmission–DM density distribution of all simulations including CLAMATO-like noise. The panel on the left shows the distribution for full hydrodynamical skewers, whereas the right panel shows the same for skewers based on the FGPA. The mean of each distribution can be found in Table 2.
Paper: Constraining the Fluctuating Gunn–Peterson Approximation using Lyα Forest Tomography at z = 2
Authors: Robin Kooistra, Khee-Gan Lee, Benjamin Horowitz
Figure caption: Properties of a single skewer through the center of the Nyx simulation. The top panel shows the Lyα transmission of the hydrodynamical skewer, as well as the same sightline from the FGPA skewers. The second panel displays the density along the sightline. The third panel shows the velocity along the skewer. We note that the Nyx output does not contain DM velocities. The final panel gives the gas temperature along the skewer.
Paper: Constraining the Fluctuating Gunn–Peterson Approximation using Lyα Forest Tomography at z = 2
Authors: Robin Kooistra, Khee-Gan Lee, Benjamin Horowitz
Figure caption: Lyα transmission–DM density distribution for all simulations (thick-lined contours) compared to the FGPA-based distribution from TNG100-1 (thin, solid-lined magenta contours). The contours denote the 2% and 80% levels of the PDF of the distribution, respectively. This clearly shows the deviation of the FGPA from the dynamical simulations.
Paper: Constraining the Fluctuating Gunn–Peterson Approximation using Lyα Forest Tomography at z = 2
Authors: Robin Kooistra, Khee-Gan Lee, Benjamin Horowitz
Figure caption: Examples of Lyα forest skewers through each of the simulations. The solid colored lines denote the hydrodynamical skewers, whereas the magenta dashed lines show the FGPA-based skewers generated along the same sightlines.
Paper: Constraining the Fluctuating Gunn–Peterson Approximation using Lyα Forest Tomography at z = 2
Authors: Robin Kooistra, Khee-Gan Lee, Benjamin Horowitz
Figure caption: Lyα transmission–DM density distribution for all simulations compared to the FGPA-based distribution with the best-fit β slope. The contours again denote the 2%, 20%, and 80% levels of the PDF of the distribution, respectively. The best-fit FGPA slope values are given in the legends of each respective panel.
Paper: The Relative Importance of Thermal Gas, Radiation, and Magnetic Pressures around Star-forming Regions in Normal Galaxies and Dusty Starbursts
Authors: Eric J. Murphy
Figure caption: Logarithmic thermal gas-to-radiation pressure ratios plotted as a function of SFR surface density. Subsets of the sample are identified using different plotting symbols. The dashed line indicates a ratio of unity. The thin solid line illustrates the expected trend given the correlated nature of the axes, as they both rely on the photometric aperture diameters. The two sources having thermal gas-to-radiation pressure ratios ≳5 are labeled: the nucleus of NGC 4594 hosts an AGN (Moustakas et al. 2010); NGC 2403 Enuc. 1a is likely an optically faint SNR (Turner & Ho 1994; Schlegel & Pannuti 2003). A least-squares fit to the data is shown by a dotted–dashed line (along with 1σ uncertainties by the dotted lines), indicating that the decrease in thermal gas-to-radiation pressure ratios with increasing values of ΣSFR is only marginally steeper than what is expected given the correlated nature of the axes.
Paper: The Relative Importance of Thermal Gas, Radiation, and Magnetic Pressures around Star-forming Regions in Normal Galaxies and Dusty Starbursts
Authors: Eric J. Murphy
Figure caption: Left: radiation pressure distribution for all sources, along with the distributions for nuclear and extranuclear regions. Similar to the minimum-energy magnetic field strength distribution, the radiation pressure estimates for the extranuclear regions are, on average, smaller and more narrowly distributed than those for the nuclear regions. Right: radiation pressure distributions for regions within the SFRS and GOALS galaxies. The radiation pressures for regions within the SFRS galaxies are, on average, smaller than those within the GOALS sources. The vertical lines in both figures indicate the minimum and maximum radiation pressure estimates averaged over a sample of HII regions measured on ∼50–100 pc scales by Barnes et al. (2021), indicating that our measurements largely fall between their extreme average values.
Paper: The Relative Importance of Thermal Gas, Radiation, and Magnetic Pressures around Star-forming Regions in Normal Galaxies and Dusty Starbursts
Authors: Eric J. Murphy
Figure caption: Left: thermal gas pressure distribution for all sources, along with the distributions for nuclear and extranuclear regions. Unlike what is seen for the radiation pressure distributions, the thermal gas pressure estimates for the nuclear and extranculear regions are, on average, quite similar. Right: thermal gas pressure distributions for regions within the SFRS and GOALS galaxies. The thermal gas pressure distributions for regions within the SFRS and GOALS galaxies are quite similar. The vertical lines in both figures indicate the minimum and maximum thermal gas pressure estimates averaged over a sample of HII regions measured on ∼50–100 pc scales by Barnes et al. (2021), indicating that our measurements largely fall between their extreme average values.
Paper: The Relative Importance of Thermal Gas, Radiation, and Magnetic Pressures around Star-forming Regions in Normal Galaxies and Dusty Starbursts
Authors: Eric J. Murphy
Figure caption: Logarithmic thermal gas-to-radiation pressure ratio plotted as a function of aperture diameter in physical units. Subsets of the sample are identified using different plotting symbols: SFRS nuclear regions (open diamonds); SFRS extranuclear regions (filled circles); GOALS nuclear regions (open triangles); and GOALS extranuclear regions (open squares). Running medians for all regions, as well as all nuclear and extranuclear regions, are shown by solid lines using large filled circles, triangles, and squares, respectively. The thermal gas-to-radiation pressure ratios appear to decrease with increasing physical size of each region, indicating that the thermal pressure (i.e., free–free emission) is more centrally peaked on individual star-forming regions than the radiation pressure (i.e., infrared emission).
Paper: The Relative Importance of Thermal Gas, Radiation, and Magnetic Pressures around Star-forming Regions in Normal Galaxies and Dusty Starbursts
Authors: Eric J. Murphy
Figure caption: Left: minimum-energy magnetic field strength distribution for all sources, along with the distributions for nuclear and extranuclear regions. The field strengths for the extranuclear regions are, on average, smaller and more narrowly distributed than those for the nuclear regions. Right: minimum-energy magnetic field strength distributions for regions within the SFRS and GOALS galaxies. The field strengths of regions within the SFRS galaxies are, on average, smaller and more narrowly distributed than those within the GOALS sources.
Paper: The Relative Importance of Thermal Gas, Radiation, and Magnetic Pressures around Star-forming Regions in Normal Galaxies and Dusty Starbursts
Authors: Eric J. Murphy
Figure caption: Logarithmic magnetic-to-radiation pressure ratios plotted as a function of SFR surface density. Subsets of the sample are identified using different plotting symbols. The dashed line indicates a ratio of unity. The two sources having magnetic-to-radiation pressure ratios ≳5 are labeled: the nucleus of NGC 5866 hosts a known AGN (Moustakas et al. 2010); NGC 5194 Enuc. 11c may be an optically faint SNR (Maddox et al. 2007). The distribution of magnetic-to-radiation pressure ratios appears relatively flat as a function of SFR surface density.
Paper: The Relative Importance of Thermal Gas, Radiation, and Magnetic Pressures around Star-forming Regions in Normal Galaxies and Dusty Starbursts
Authors: Eric J. Murphy
Figure caption: Logarithmic magnetic-to-radiation pressure ratio plotted as a function of aperture diameter in physical units. Subsets of the sample are identified using different plotting symbols: SFRS nuclear regions (open diamonds); SFRS extranuclear regions (filled circles); GOALS nuclear regions (open triangles); and GOALS extranuclear regions (open squares). Running medians for all regions, as well as all nuclear and extranuclear regions, are shown by solid lines using large filled circles, triangles, and squares, respectively. The red dashed lines and open symbols indicate how the magnetic pressure estimates change by letting the path length of the synchrotron emitting medium scale with the physical diameter of the photometric apertures for extranuclear regions resolved on scales <1 kpc after subtracting a local background. The magnetic-to-radiation pressure ratios appear to be sensitive to the physical size of each region, showing a steady increase with increasing physical size of the aperture.
Paper: The Relative Importance of Thermal Gas, Radiation, and Magnetic Pressures around Star-forming Regions in Normal Galaxies and Dusty Starbursts
Authors: Eric J. Murphy
Figure caption: Logarithmic ratios of the total internal-to-dynamical equilibrium pressures plotted as a function of aperture diameter in physical units. The dynamical equilibrium pressures are estimated via a linear interpolation using the measured SFR surface densities and the correlation between ΣSFR and P DE found by Sun et al. (2020). Subsets of the sample are identified using different plotting symbols. The dashed line indicates a ratio of unity, while the solid line illustrates the median ratio. Neglecting any additional pressure term associated with turbulent motions of the gas, only ≈5% of the star-forming regions appear to be overpressurized relative to the dynamical equilibrium pressure, each of which are measured on ≲1 kpc scales.
Paper: The Relative Importance of Thermal Gas, Radiation, and Magnetic Pressures around Star-forming Regions in Normal Galaxies and Dusty Starbursts
Authors: Eric J. Murphy
Figure caption: A box and whiskers plot illustrating the minimum, lower quartile, median, upper quartile, and maximum values for the logarithmic ratio of magnetic-to-radiation pressures for the SFRS and GOALS nuclear and extranuclear regions. The median ratios are quite similar for the nuclear regions in both the SFRS and GOALS galaxies, however the ratio for the extranuclear regions in the GOALS galaxies is a factor of ∼2 larger than that for the SFRS extranuclear regions.
Paper: The Absolute Magnitudes of 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Christopher R. Burns, Carlos Contreras, L. Galbany, P. Hoeflich, E. Y. Hsiao, Nidia Morrell, Peter Nugent, Syed A. Uddin, E. Baron, Wendy L. Freedman, Chelsea E. Harris, Kevin Krisciunas, S. Kumar, J. Lu, S. E. Persson, Anthony L. Piro, Abigail Polin, Shahbandeh M., Maximilian Stritzinger, Nicholas B. Suntzeff
Figure caption: (a) Branch diagram for SNe Ia observed by the CfA Supernova Group and the first phase of the Carnegie Supernova Project (CSP-I). The dashed lines approximate the boundaries between the different subtypes adopted by Branch et al. (2009) (see Figure 10 of Silverman et al. 2012b), while the different colors correspond to the boundaries assumed by Folatelli et al. (2013), which are similar to those used by Blondin et al. (2012); (b) light curve decline rate parameter, Δm 15(B), plotted vs. the pseudo-equivalent width of the Si II λ6355 absorption for the Branch shallow-silicon (SS; turquoise triangles) and core-normal (CN; black circles) subtypes in the CfA Supernova Group and the CSP-I samples. In this paper, we refer to CN events lying below the red horizontal line (Δm 15(B)  < 1.1) as the “slow-declining Branch CN” SNe (see Section 4).
Paper: The Absolute Magnitudes of 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Christopher R. Burns, Carlos Contreras, L. Galbany, P. Hoeflich, E. Y. Hsiao, Nidia Morrell, Peter Nugent, Syed A. Uddin, E. Baron, Wendy L. Freedman, Chelsea E. Harris, Kevin Krisciunas, S. Kumar, J. Lu, S. E. Persson, Anthony L. Piro, Abigail Polin, Shahbandeh M., Maximilian Stritzinger, Nicholas B. Suntzeff
Figure caption: Hubble diagram distance modulus residuals, Δ(m − M), for 91T-like, 99aa-like, and slow-declining Branch CN SNe observed by the CSP-II. The sample of slow-declining Branch CN SNe is defined as those events with Δm 15(B) < 1.10. The larger symbols are SNe whose values of Δm 15(B) were measured directly; the smaller symbols correspond to those where SNooPy template fits were used to measure the decline rate. The samples were limited to those with redshifts z ≥ 0.02 to minimize uncertainties due to peculiar velocities. Note that negative values of Δ(m − M) correspond to over-luminous events.
Paper: BASS XXXVII: The Role of Radiative Feedback in the Growth and Obscuration Properties of Nearby Supermassive Black Holes
Authors: C. Ricci, T. T. Ananna, M. J. Temple, C. M. Urry, M. J. Koss, B. Trakhtenbrot, Y. Ueda, D. Stern, F. E. Bauer, E. Treister, G. C. Privon, K. Oh, S. Paltani, M. Stalevski, L. C. Ho, A. C. Fabian, R. Mushotzky, C. S. Chang, F. Ricci, D. Kakkad, L. Sartori, R. Baer, T. Caglar, M. Powell, F. Harrison
Figure caption: Top panel: fraction of sources with column densities in a given range vs. the Eddington ratio for AGNs in two different bins of intrinsic 14–150 keV luminosity (in units of erg s−1). The red dashed lines show the expected Eddington limit for dusty gas with ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\simeq 22﹩ (bottom-left panel; Fabian et al. 2006, 2008, 2009) and ﹩\mathrm{log}({N}_{{\rm{H}}}/{\mathrm{cm}}^{-2})\simeq 23﹩ (bottom-right panel; Ishibashi et al. 2018; Venanzi et al. 2020). The latter value of the effective Eddington limit includes the contribution from IR radiation trapping. Bottom panel: same as top panel, but with AGNs divided into two different ranges of black hole mass (in units of solar mass).
Paper: The Absolute Magnitudes of 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Christopher R. Burns, Carlos Contreras, L. Galbany, P. Hoeflich, E. Y. Hsiao, Nidia Morrell, Peter Nugent, Syed A. Uddin, E. Baron, Wendy L. Freedman, Chelsea E. Harris, Kevin Krisciunas, S. Kumar, J. Lu, S. E. Persson, Anthony L. Piro, Abigail Polin, Shahbandeh M., Maximilian Stritzinger, Nicholas B. Suntzeff
Figure caption: Optical spectra of the 10 91T-like SNe in the CSP-II sample obtained −8 to +7 days with respect to the time of maximum light in the B-band. Spectra of SN1991T at three phases covering this range are plotted in black for comparison. Where necessary, the spectra have been multiplied by a low-order polynomial to match the photometry. They have also been corrected for Galactic reddening using the Schlafly & Finkbeiner (2011) recalibration of the Schlegel et al. (1998) IR-based dust map and assuming R  V  = 3.1. Unremoved telluric absorption features are marked with an ⊕ symbol.
Paper: The Absolute Magnitudes of 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Christopher R. Burns, Carlos Contreras, L. Galbany, P. Hoeflich, E. Y. Hsiao, Nidia Morrell, Peter Nugent, Syed A. Uddin, E. Baron, Wendy L. Freedman, Chelsea E. Harris, Kevin Krisciunas, S. Kumar, J. Lu, S. E. Persson, Anthony L. Piro, Abigail Polin, Shahbandeh M., Maximilian Stritzinger, Nicholas B. Suntzeff
Figure caption:  B-band Hubble diagram residuals in magnitudes plotted vs. the residuals in V, r, Y, and H for 91T-like, 99aa-like, and CN SNe observed by the CSP-II. The solid black line in each plot indicates the expected correlation in the residuals for R  V  = 3 and a systematic error between ±0.5 mag in E(B − V); the dashed black line shows the same for R  V  = 2.
Paper: The Absolute Magnitudes of 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Christopher R. Burns, Carlos Contreras, L. Galbany, P. Hoeflich, E. Y. Hsiao, Nidia Morrell, Peter Nugent, Syed A. Uddin, E. Baron, Wendy L. Freedman, Chelsea E. Harris, Kevin Krisciunas, S. Kumar, J. Lu, S. E. Persson, Anthony L. Piro, Abigail Polin, Shahbandeh M., Maximilian Stritzinger, Nicholas B. Suntzeff
Figure caption: (Upper) Hubble diagram residuals in magnitudes plotted vs. the pEW of the Si II λ6355 absorption at maximum light for 91T-like, 99aa-like, and CN SNe observed by the CSP-II. (Lower) E(B − V)host values derived using SNooPy for the same SNe.
Paper: Suzaku Observations of the Cluster Outskirts and Intercluster Filament in the Triple Merger Cluster A98
Authors: Gabriella E. Alvarez, Scott W. Randall, Yuanyuan Su, Arnab Sarkar, Stephen Walker, Nicholas P. Lee, Craig L. Sarazin, Elizabeth Blanton
Figure caption: The entropy profile from north to south across the bridge between A98N and A98S. The blue line is the expected universal entropy profile for A98N. The black line is the expected universal entropy profile for A98S. The pink points show the inferred entropy for a filament orientation in the POS. The green triangles are for a filament orientation along the LOS. A filament orientation closer to the LOS is preferred, as the LOS entropy values are ∼2 times higher than what is expected in the outskirts of both subclusters.
Paper: Suzaku Observations of the Cluster Outskirts and Intercluster Filament in the Triple Merger Cluster A98
Authors: Gabriella E. Alvarez, Scott W. Randall, Yuanyuan Su, Arnab Sarkar, Stephen Walker, Nicholas P. Lee, Craig L. Sarazin, Elizabeth Blanton
Figure caption: The surface brightness profile with XIS3 in the 0.5–2.0 keV range, where the 1σ errors of the filamentary region shown in Figure 6 are shown as black points, using the y-axis scale on the left. The corresponding combined rectangular annuli shown in Figure 6 for A98N and A98S are shown for comparison with the blue points. The filament excesses, are shown in red, using the y-axis scale on the right. The zero point on the x-axis is the midpoint of the tentative bridge connecting A98N to A98S.
Paper: Suzaku Observations of the Cluster Outskirts and Intercluster Filament in the Triple Merger Cluster A98
Authors: Gabriella E. Alvarez, Scott W. Randall, Yuanyuan Su, Arnab Sarkar, Stephen Walker, Nicholas P. Lee, Craig L. Sarazin, Elizabeth Blanton
Figure caption: Same as Figure 1 (Left). The rectangular annuli to the north of A98N and to the south of A98S are used to compare the combined surface brightness of the two clusters to the box regions in the bridge region (see Figure 7).
Paper: Suzaku Observations of the Cluster Outskirts and Intercluster Filament in the Triple Merger Cluster A98
Authors: Gabriella E. Alvarez, Scott W. Randall, Yuanyuan Su, Arnab Sarkar, Stephen Walker, Nicholas P. Lee, Craig L. Sarazin, Elizabeth Blanton
Figure caption: The blue line is the entropy profile expected from pure gravitational collapse (Voit et al. 2005) for A98N. The black points are for the sector regions to the north of A98N and the pink points are for the sector regions to the west of A98N shown in Figure 1.
Paper: Suzaku Observations of the Cluster Outskirts and Intercluster Filament in the Triple Merger Cluster A98
Authors: Gabriella E. Alvarez, Scott W. Randall, Yuanyuan Su, Arnab Sarkar, Stephen Walker, Nicholas P. Lee, Craig L. Sarazin, Elizabeth Blanton
Figure caption: The temperature profile of the box regions across the A98 system shown in Figure 1. The profile starts from the north on the left of the plot. The purple, pink, and green dashed lines mark the center of A98N, A98S, and A98SS, respectively.
Paper: Suzaku Observations of the Cluster Outskirts and Intercluster Filament in the Triple Merger Cluster A98
Authors: Gabriella E. Alvarez, Scott W. Randall, Yuanyuan Su, Arnab Sarkar, Stephen Walker, Nicholas P. Lee, Craig L. Sarazin, Elizabeth Blanton
Figure caption: Inferred electron density profile across the A98 system. The profile starts from the north on the left of the plot. The purple, pink, and green dashed lines mark the center of A98N, A98S, and A98SS, respectively.
Paper: Suzaku Observations of the Cluster Outskirts and Intercluster Filament in the Triple Merger Cluster A98
Authors: Gabriella E. Alvarez, Scott W. Randall, Yuanyuan Su, Arnab Sarkar, Stephen Walker, Nicholas P. Lee, Craig L. Sarazin, Elizabeth Blanton
Figure caption: The metallicity profile across the A98 bridge. The profile starts from the north on the left of the plot. The purple, pink, and green dashed lines mark the center of A98N, A98S, and A98SS, respectively.
Paper: Suzaku Observations of the Cluster Outskirts and Intercluster Filament in the Triple Merger Cluster A98
Authors: Gabriella E. Alvarez, Scott W. Randall, Yuanyuan Su, Arnab Sarkar, Stephen Walker, Nicholas P. Lee, Craig L. Sarazin, Elizabeth Blanton
Figure caption: The electron density profiles of the annuli to the north and west of A98N (see, e.g., Figure 1 (Left)).