adsabs/AstroCLIMB huggingface dataset:
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Top panel: logarithmic intrinsic AGN luminosity vs. logarithmic physical size of the dominant IR emission from polar dust, estimated from the sublimation radius and polar dust temperature. The dashed red line and pink shaded region show the best-fitting linear relation and its 1σ dispersion among the AGNs, respectively. The green circles illustrate the physical size of ionized outflows measured with optical IFU observations, and the light-blue circles mark the size of molecular outflows measured with submillimeter observations in the subsample of our U/LIRGs (Fluetsch et al. 2019, 2021). The gray diamonds and small circles denote the sizes of extended mid-IR emission for U/LIRGs and non-U/LIRG sources respectively (Asmus 2019). For the sizes of the molecular outflows and extended mid-IR region, the bolometric AGN luminosities of U/LIRGs are adopted to the estimates in this study, while those of non-U/LIRGs are calculated as the X-ray luminosity (Asmus 2019) times 20 (e.g., Vasudevan & Fabian 2007). The other symbols are the same as in Figure 8. Bottom panel: schematic picture of the AGN structure (polar dust, NLR, torus, failed winds, accretion disk, and SMBH) in U/LIRGs.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Top left panel: histogram of the line-of-sight extinction in the V band by the torus ﹩{A}_{V,\mathrm{torus}}^{(\mathrm{LOS})}﹩ (top). These are divided by the X-ray AGN classification (unobscured, Compton-thin, and CT AGNs; Yamada et al. 2021). Bottom left panel: the same for the polar dust extinction, ﹩{A}_{V,\mathrm{polar}}^{(\mathrm{LOS})}﹩ (bottom). The seven sources showing 90° − i > σ (i.e., ﹩{A}_{V,\mathrm{polar}}^{(\mathrm{LOS})}=0﹩) are excluded. Top right panel: histogram of the torus (top) luminosity in the UV-to-IR band. Bottom right panel: the same for polar dust luminosity. The number of AGNs whose best-fit SED models do not include a polar dust component is shown on the left side.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Logarithmic Eddington ratio vs. α OX computed using extinction-corrected 2500 Å and unabsorbed 2 keV luminosities. The black solid curve represents the best-fit relation among local and high-z AGNs (Lusso et al. 2010). The gray shaded area shows its 1σ uncertainty. The upper limit of a ULIRG at z = 7.2 (GNz7q; Fujimoto et al. 2022) is shown as a red dashed line since its SMBH mass and Eddington ratios are not constrained. The yellow circles mark the WISSH quasars in z ∼ 2–4 (Zappacosta et al. 2020). The other symbols are the same as in Figure 8.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Line-of-sight hydrogen column density ﹩{N}_{{\rm{H}}}^{(\mathrm{LOS})}﹩ derived from X-ray spectra vs. ﹩{A}_{V,\mathrm{torus}}^{(\mathrm{LOS})}﹩, and polar dust, ﹩{A}_{V,\mathrm{polar}}^{(\mathrm{LOS})}﹩ (if 90° − i > σ, ﹩{A}_{V,\mathrm{polar}}^{(\mathrm{LOS})}=0﹩). The solid line shows the Galactic gas-to-dust ratio (N H/A  V  = 1.87 × 1021 cm−2 mag−1; Draine 2003). The large orange circles mark the AGNs showing ﹩{A}_{V,\mathrm{polar}}^{(\mathrm{LOS})}\gt {A}_{V,\mathrm{torus}}^{(\mathrm{LOS})}﹩. The other symbols are the same as in Figure 8.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Polar-dust luminosity as a function of molecular outflow velocity (left) and logarithmic mass transfer rate of said molecular outflows (right) referred from Yamada et al. (2021). The red dashed line and pink shaded area mark the best-fitting relation and its 1σ dispersion, respectively. The symbols are the same as in Figure 8.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Left panel: logarithmic Eddington ratio vs. the ratio of the torus and intrinsic AGN luminosities. Two AGNs whose luminosity ratios are above 1 are plotted as L torus/L AGN,int = 1. Right panel: logarithmic Eddington ratio vs. the ratio of polar dust and intrinsic AGN luminosities. The symbols are the same as in Figure 8.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Differences in the polar-dust temperature with merger stage, described in logarithmic scale. The diamonds and uncertainties represent the averaged value and 1σ dispersions, respectively.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Left panel: logarithmic torus luminosity vs. logarithmic polar-dust luminosity in the UV-to-IR bands. Right panel: logarithmic Eddington ratio vs. logarithmic polar-dust luminosity. The symbols are the same as in Figure 8.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Logarithmic polar-dust luminosity vs. polar-dust temperature. The symbols are the same as in Figure 8.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Logarithmic stellar mass vs. logarithmic SMBH mass referred from Yamada et al. (2021) for the AGNs in stage C (orange diamond) and stage D (red star) U/LIRGs. The solid arrows represent the expected masses of the galaxy and SMBH if they evolve with constant growth rates (SFR and ﹩{\dot{M}}_{\mathrm{BH}}﹩) for 30 Myr. For the three dual AGN systems in stage A mergers, the merged masses of the two sources including the mass increase for 30 Myr are marked as empty blue stars with dotted lines. The black solid line denotes the local bulge mass (M bulge) and SMBH mass (M BH) relation for classical bulges and elliptical galaxies (Kormendy & Ho 2013). The dashed line shows the scaled relation that has bulge masses scaled down by 0.33 dex to consider the difference in the adopted mass-to-light ratios, and the blue dotted line presents the typical M *–M BH relation for classical bulges and ellipticals (Reines & Volonteri 2015).
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Logarithmic SFR vs. intrinsic AGN luminosity. The black dotted line denotes the typical relation among low-z Seyfert 2 s, QUEST QSOs, and high-z QSOs (Trakhtenbrot & Netzer 2010). The red dashed line and pink shaded area mark the best-fitting relation and its 1σ dispersion, respectively, for the AGNs in U/LIRGs, excluding nonmergers and AGNs with logSFR < 0. The black solid line is the galaxy–SMBH “simultaneous evolution” line for A = 200 (see also Ueda et al. 2018). The large symbols are the same as in Figure 8. The small crosses mark starburst-dominant and hard X-ray–nondetected sources, whose L AGN,int values are derived from their [O IV] luminosities (Yamada et al. 2021).
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Left panel: comparison of L AGN,int estimated by Yamada et al. (2021) and this work. Right panel: comparison with the AGN (torus and polar-dust components) 12 μm luminosity from the UV-to-IR SED analysis (L 12 μm,AGN) and the nuclear 12 μm luminosity (L 12 μm,nuc;  Asmus et al. 2015).
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Left panel: comparison of the intrinsic (bolometric) AGN luminosities derived with the CLUMPY model and SKIRTOR model. Right panel: comparison of the polar-dust luminosities derived with the CLUMPY model and SKIRTOR model. The symbols are the same as in Figure 8.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: SFR and intrinsic AGN luminosity as a function of projected separation between two galaxies in units of kiloparsecs. Single nuclei in merging (stage D) and nonmerging (stage N) sources are plotted on the left (negative value) and right sides, respectively. The large symbols are the same as in Figure 8, while the small crosses illustrate the starburst-dominant and hard X-ray–nondetected sources.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Left panel: comparison of M * estimated by Shangguan et al. (2019) and this work. Right panel: comparison of M * estimated by Paspaliaris et al. (2021) and this work. The former values are converted from a Salpeter (1955) IMF to a Chabrier (2003) IMF with 0.24 dex. The symbols are the same as in Figure 8.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Schematic picture of merger-driven coevolution of galaxies and SMBHs. The middle panels are compiled from Pan-STARRS DR2 and SDSS DR16 images (Section 3.3), whose sources are merging U/LIRGs (NGC 833/NGC 835, NGC 3690, and Mrk 231) and post-merger candidates (a quasar H1821+643; e.g., Jadhav et al. 2021; and an elliptical galaxy M87; e.g., Longobardi et al. 2015).
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Left panel: comparison of the SFRs estimated by Shangguan et al. (2019) and this work. Right panel: comparison of SFRs estimated by Paspaliaris et al. (2021) and this work. The former values are converted from a Salpeter (1955) IMF to a Chabrier (2003) IMF with 0.15 dex. The symbols are the same as in Figure 8.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Comparison of the best-fit parameters and those derived from the mock analysis for M * (top left), SFR (top right), AGN fraction (middle left), intrinsic AGN luminosity (middle right), polar dust luminosity (bottom left), and polar dust temperature (bottom right). The symbols are the same as in Figure 8.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: The hard X-ray-to-radio SEDs and the best-fitting models in units of luminosity for the sample with ID = 1–10. The bottom panels show the residuals in the UV-to-radio bands. The individual curves are the same as in Figure 1. The purple and red circles represent the observed and model flux densities, respectively. The red crosses in the X-ray band denote the NuSTAR spectra (or, Swift/BAT for NGC235 and XMM-Newton/MOS for IC5283 and MCG+01-59-081). The red arrows and green triangles mark 5σ upper limits.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: Left panel: comparison of the polar dust temperatures derived with the CLUMPY model and SKIRTOR model. Right panel: logarithmic polar-dust luminosity vs. polar-dust temperature when the SKIRTOR model is adopted. The symbols are the same as in Figure 8.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: The same as in Figure E2 but for the sample with ID = 51–60.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: The same as in Figure E2 but for the sample with ID = 21–30.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: The same as in Figure E2 but for the sample with ID = 41–50.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: The same as in Figure E2 but for the sample with ID = 31–40.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: The same as in Figure E2 but for the sample with ID = 11–20.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: The same as in Figure E2 but for the sample with ID = 61–70.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: The same as in Figure E2 but for the sample with ID = 81–85.
Paper: Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component
Authors: Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci
Figure caption: The same as in Figure E2 but for the sample with ID = 71–80.
Paper: Updated Void Catalogs of the SDSS DR7 Main Sample
Authors: Kelly A. Douglass, Dahlia Veyrat, Segev BenZvi
Figure caption: A 10 h −1 Mpc thick slice of SDSS DR7 centered at a decl. of 25° assuming Planck 2018 cosmology. The locations of the galaxies that fall within a void are shown in red, while those that do not are shown in black. The intersection of all voids with the center of this slice are shown in the shaded blue (orange for boundary voids) regions, for VoidFinder (top), V2/VIDE (middle), and V2/REVOLVER (bottom).
Paper: Updated Void Catalogs of the SDSS DR7 Main Sample
Authors: Kelly A. Douglass, Dahlia Veyrat, Segev BenZvi
Figure caption: Distribution of voids’ effective radii for the VoidFinder (left), V2/VIDE (center), and V2/REVOLVER (right) SDSS DR7 void catalogs (solid lines) generated assuming WMAP5 cosmology. The shaded uncertainties were computed using 64 DR7 mock catalogs produced from the Horizon Run 4 simulation (Kim et al. 2015). VoidFinder voids are more numerous and generally smaller due to how V2 aggregates disconnected voids (see Section 4.3 for discussion). We extend the V2/REVOLVER distribution down to 10 h −1 Mpc so that it is consistent with both VoidFinder and V2/VIDE.
Paper: Updated Void Catalogs of the SDSS DR7 Main Sample
Authors: Kelly A. Douglass, Dahlia Veyrat, Segev BenZvi
Figure caption: Same region of the SDSS DR7 survey, showing the intersection of the voids published by Pan et al. (2012; left) and our VoidFinder catalog (right) generated assuming a Planck 2018 cosmology. The excess void regions identified by Pan et al. (2012) are easily seen along the boundaries of the survey. Within the footprint, we also see that the void catalog published by Pan et al. (2012) has significant overlap between identified voids.
Paper: Updated Void Catalogs of the SDSS DR7 Main Sample
Authors: Kelly A. Douglass, Dahlia Veyrat, Segev BenZvi
Figure caption: Stacked normalized radial void density profiles assuming WMAP5 cosmology, measured in concentric spherical shells around void centers. We estimate the profiles using the average density of all galaxies, measured from the centers of voids. The radii of the spherical shells are normalized to each void’s effective radius, R eff. 1 + δ = 1 corresponds to the mean survey density, while 1 + δ = 0 corresponds to a density of 0.
Paper: Updated Void Catalogs of the SDSS DR7 Main Sample
Authors: Kelly A. Douglass, Dahlia Veyrat, Segev BenZvi
Figure caption: Distribution of the ratio of the surface area of V2 voids shared with boundary cells (A edge) to the total surface area of each void (A total), for all voids with A edge > 0.
Paper: Updated Void Catalogs of the SDSS DR7 Main Sample
Authors: Kelly A. Douglass, Dahlia Veyrat, Segev BenZvi
Figure caption: Stacked radial void density profiles, measured in concentric spherical shells around void centers generated assuming the WMAP5 cosmology. We estimate the profiles using the average density of all galaxies, measured from the centers of voids. 1 + δ = 1 corresponds to the mean survey density, while 1 + δ = 0 corresponds to a density of 0.
Paper: Updated Void Catalogs of the SDSS DR7 Main Sample
Authors: Kelly A. Douglass, Dahlia Veyrat, Segev BenZvi
Figure caption: Example volume overlap between two void catalogs: VoidFinder (blue) and V2 (red). Within the survey volume, we calculate the fraction of the space that both catalogs classify as a void (purple).
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: A series of histograms of various coronal-line luminosity ratios, in logarithmic units. The solid black histograms show the luminosity ratios with [O III] λ5007, while the red dashed histograms show Hα. Each panel displays a different coronal line, labeled on the horizontal axes, with the exception of the first (top-left) panel, which shows a concatenation of all the coronal lines together. The horizontal and vertical scales of each plot are identical, again with the exception of the top-left panel.
Paper: CLASS Survey Description: Coronal-line Needles in the SDSS Haystack
Authors: Michael Reefe, Remington O. Sexton, Sara M. Doan, Shobita Satyapal, Nathan J. Secrest, Jenna M. Cann
Figure caption: A 2D correlation plot between each pair of lines. The color of each box represents the number of spectra in which both lines from the horizontal and vertical labels are found together. Along the diagonal, the color instead represents the pure number of detections of that single line. The color bar is logarithmic, corresponding to ﹩{\mathrm{log}}_{10}(N+1)﹩ where N is the number of detections.