adsabs/AstroCLIMB huggingface dataset:
Paper: Estimators of Bolometric Luminosity and Black Hole Mass with Mid-infrared Continuum Luminosities for Dust-obscured Quasars: Prevalence of Dust-obscured SDSS Quasars
Authors: Dohyeong Kim, Myungshin Im, Minjin Kim, Yongjung Kim, Suhyun Shin, Hyunjin Shim, Hyunmi Song
Figure caption: (a) Comparison between L bol/L 3.4 and redshift. The red-dashed line denotes the best-fit relationship when α and β in Equation (5) are set as free parameters. The gray dashed–dotted and dashed–dot–dotted lines represent the best-fit correlations derived with the AGN templates of Richards et al. (2006) and Assef et al. (2010), respectively, where all parameters are treated as free parameters. (b) L5100/L 3.4 vs. redshift. The meanings of the lines are identical to those in the left panel.
Paper: Estimators of Bolometric Luminosity and Black Hole Mass with Mid-infrared Continuum Luminosities for Dust-obscured Quasars: Prevalence of Dust-obscured SDSS Quasars
Authors: Dohyeong Kim, Myungshin Im, Minjin Kim, Yongjung Kim, Suhyun Shin, Hyunjin Shim, Hyunmi Song
Figure caption: Photometric data of four randomly selected SDSS quasars with their best-fit SED models in the rest frame. Blue triangles, green squares, and red circles indicate photometric data points from SDSS, 2MASS PSC, and WISE (W1, W2, and W3), respectively. The red-dashed, blue-dotted, green-dashed–dotted, and purple-dashed–dot–dot–dotted lines indicate the reddened AGN, elliptical galaxy, spiral galaxy, and irregular galaxy spectra, respectively. The black solid lines show the sums of the best-fit spectra. The name of the sample and the measured E(B − V) value are presented on the top left and right side of each panel, respectively.
Paper: Estimators of Bolometric Luminosity and Black Hole Mass with Mid-infrared Continuum Luminosities for Dust-obscured Quasars: Prevalence of Dust-obscured SDSS Quasars
Authors: Dohyeong Kim, Myungshin Im, Minjin Kim, Yongjung Kim, Suhyun Shin, Hyunjin Shim, Hyunmi Song
Figure caption: Host galaxy contamination at 1.2, 1.7, 2.2, 3.4, 4.6, and 12 μm in the rest frame. Green squares denote the measured host contamination at 1.2, 1.7, and 2.2 μm, and red circles those at 3.4, 4.6, and 12 μm.
Paper: Estimators of Bolometric Luminosity and Black Hole Mass with Mid-infrared Continuum Luminosities for Dust-obscured Quasars: Prevalence of Dust-obscured SDSS Quasars
Authors: Dohyeong Kim, Myungshin Im, Minjin Kim, Yongjung Kim, Suhyun Shin, Hyunjin Shim, Hyunmi Song
Figure caption: Redshift vs. BH mass for our sample. The BH masses are measured based on the L5100 and FWHMHβ  values (Vestergaard & Peterson 2006).
Paper: The Evolution of Ion Charge States in Coronal Mass Ejections
Authors: J. Martin Laming, Elena Provornikova, Yuan-Kuen Ko
Figure caption: Contours of the electron velocity distribution function power-law index γ = 2κ in the σ − a space, for conductivity σ and turbulent spectrum ﹩{k}_{| | }^{-a}﹩. A Lundquist number of S ∼ 104 is assumed on the left, S ∼ 108 on the right, and L σ ∼ S × 1012 cm s−1.
Paper: The Evolution of Ion Charge States in Coronal Mass Ejections
Authors: J. Martin Laming, Elena Provornikova, Yuan-Kuen Ko
Figure caption: Variation in the ionization balance with the heliocentric distance for, from top to bottom C, O, Mg, Si, and Fe, with the electron temperature and density profiles given at the bottom, for the 2010 April 03 CME ejecta epoch 16 (from Table 3). The left panels give the case for Maxwellian electron distributions. The right panels are the same but for κ = 2.6 electron distributions. The broader charge state distributions are the clearest for Si and Fe. The CME expansion velocity is superimposed on the top panel, to be read on the right-hand axis. Selected charge states are labeled. Others can be inferred by comparison with Figure 5.
Paper: The Evolution of Ion Charge States in Coronal Mass Ejections
Authors: J. Martin Laming, Elena Provornikova, Yuan-Kuen Ko
Figure caption: Left: final charge state distributions for C, O, Mg, Si, and Fe, at 1 au in epoch 16 in ICME ejecta from the 2010 April 03 CME event assuming Maxwellian electron distributions. The model is shown as a histogram, and the data are shown as filled black circles, with 2σ uncertainties from the level 2 ACE data given by the radius. Right: the same but for κ = 2.6 electron distributions. The difference in the modeled charge state distributions between the two cases is most clearly seen for Fe and Si.
Paper: The Evolution of Ion Charge States in Coronal Mass Ejections
Authors: J. Martin Laming, Elena Provornikova, Yuan-Kuen Ko
Figure caption: Schematic diagram of a reconnection current sheet with characteristic external scale length L  e , and interior length of diffusion region (shown in gray) of L  i . The exterior and interior flow velocities are v  e  and v  i , respectively. Magnetic islands form either side of the diffusion regions, and are the sites of electron heating as they evolve and merge.
Paper: The Evolution of Ion Charge States in Coronal Mass Ejections
Authors: J. Martin Laming, Elena Provornikova, Yuan-Kuen Ko
Figure caption: Plots of the Fe charge state distribution for Day of Year (DOY) 95.08–97.00 during the 2010 April 3 ICME, observed at ACE during 2010 April 5–7. During DOY 95.83–96.42, the dominant Fe charge state is 16+, indicating extra heating and ionization beyond the typical solar wind value of 8+ to 9+.
Paper: The Evolution of Ion Charge States in Coronal Mass Ejections
Authors: J. Martin Laming, Elena Provornikova, Yuan-Kuen Ko
Figure caption: Left: variation in ionization balance with the heliocentric distance for C, O, Mg, Si, and Fe, and the electron temperature and density, for the 2011 February 15 CME ejecta epoch 25, assuming κ = 106 electron distributions. Right: the same but for κ = 3.5 electron distributions. The CME expansion velocity is superimposed on the top panel, to be read on the right-hand axis. The selected charge states are labeled. Others can be inferred by comparison with Figure 7.
Paper: The Evolution of Ion Charge States in Coronal Mass Ejections
Authors: J. Martin Laming, Elena Provornikova, Yuan-Kuen Ko
Figure caption: Left: final charge state distributions for C, O, Mg, Si, and Fe for the 2011 February 15 CME ejecta epoch 25, assuming κ = 106 electron distributions. The model is shown as a histogram, and the data are shown as filled black circles, with 2σ uncertainties from the level 2 ACE data given by the radius. Right: the same but for κ = 3.5 electron distributions.
Paper: The Evolution of Ion Charge States in Coronal Mass Ejections
Authors: J. Martin Laming, Elena Provornikova, Yuan-Kuen Ko
Figure caption: Examples of the full κ distribution (thick solid), the underlying Maxwellian distribution (thick dashed), and the approximate κ function expressed as a sum of Maxwellians (thin solid) for κ = 30 (top), 10 (middle), and 3 (bottom) as a function of x = v/v  t .
Paper: The Evolution of Ion Charge States in Coronal Mass Ejections
Authors: J. Martin Laming, Elena Provornikova, Yuan-Kuen Ko
Figure caption: GAMERA MHD simulation of magnetic reconnection in Harris current sheet representing post-CME current sheet in the solar corona. Panels (a)–(h) show the out-of-plane current J  z  in the simulation domain. Panels (i)–(k) show the out-of-plane current J  z  when two big islands form a secondary current sheet where reconnection with formation of smaller islands occurs (blue box from panel (h)), panels (l)–(n) show the V  y  velocity component indicating reconnection outflow between merging and reconnecting islands. J  z  and V  y  are shown in normalized units. Time is normalized to the Alfvén time.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: The Black Hole Mass–Stellar Mass Relations at 0.2 ≲ z ≲ 0.8
Authors: Jennifer I-Hsiu Li, Yue Shen, Luis C. Ho, W. N. Brandt, Catherine J. Grier, Patrick B. Hall, Y. Homayouni, Anton M. Koekemoer, Donald P. Schneider, Jonathan R. Trump
Figure caption: Comparison with literature samples. Our sample is shown with black circles (bulge dominated) and gray squares (disk dominated), and the open gray square is the CIGALE stellar mass of RM265. The blue circles are the local RM sample from Bentz & Manne-Nicholas (2018). The triangles show the high-redshift samples with HST imaging (orange: Bennert et al. 2011, median redshift z med = 1.2; green: Jahnke et al. 2009, z med = 1.3; red: Ding et al. 2020, z med = 1.5), and the circles indicate the high-redshift samples with SED fitting (purple: Ding et al. 2021, z med = 1.7; brown: Dong & Wu 2016, z med = 1.1; pink: Suh et al. 2020, z med = 1.6). The solid lines show the best-fit relations of the local quiescent galaxy (red; Kormendy & Ho 2013), active galaxy (orange; Bennert et al.2021), and RM AGN (blue; Bentz & Manne-Nicholas 2018).
Paper: Near-Sun In Situ and Remote-sensing Observations of a Coronal Mass Ejection and its Effect on the Heliospheric Current Sheet
Authors: O. M. Romeo, C. R. Braga, S. T. Badman, D. E. Larson, M. L. Stevens, J. Huang, T. Phan, A. Rahmati, R. Livi, S. T. Alnussirat, P. L. Whittlesey, A. Szabo, K. G. Klein, T. Niembro-Hernandez, K. Paulson, J. L. Verniero, D. Lario, N. E. Raouafi, T. Ervin, J. Kasper, M. Pulupa, S. D. Bale, M. G. Linton
Figure caption: Heuristic functions h(x) for a given normalized parameter x. The frequency heuristic function h  F  (purple) is a function of the normalized frequency bin difference ΔF. The convolution heuristic function h  c  (red) is a function of the normalized convolution value of the resulting spectra.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: The Black Hole Mass–Stellar Mass Relations at 0.2 ≲ z ≲ 0.8
Authors: Jennifer I-Hsiu Li, Yue Shen, Luis C. Ho, W. N. Brandt, Catherine J. Grier, Patrick B. Hall, Y. Homayouni, Anton M. Koekemoer, Donald P. Schneider, Jonathan R. Trump
Figure caption: BH mass as functions of bulge stellar mass (left) and total stellar mass (right) of our sample (black circles for bulge-dominated sources, gray squares for disk-dominated sources, and the open gray square for the CIGALE stellar mass of RM265). The blue dashed lines (and the gray shaded areas) are the best-fit relation (1σ range) of our sample. The red solid lines are the Kormendy & Ho (2013) local M BH–M *, bulge relation. The Pearson r coefficient, p-value, and intrinsic scatter of the relations are labeled in the upper left corner of each panel.
Paper: Near-Sun In Situ and Remote-sensing Observations of a Coronal Mass Ejection and its Effect on the Heliospheric Current Sheet
Authors: O. M. Romeo, C. R. Braga, S. T. Badman, D. E. Larson, M. L. Stevens, J. Huang, T. Phan, A. Rahmati, R. Livi, S. T. Alnussirat, P. L. Whittlesey, A. Szabo, K. G. Klein, T. Niembro-Hernandez, K. Paulson, J. L. Verniero, D. Lario, N. E. Raouafi, T. Ervin, J. Kasper, M. Pulupa, S. D. Bale, M. G. Linton
Figure caption: 2D Histogram of scaled proton temperature T  p  by R  a  as a function of the SW velocity v  p  for PSP encounters 1 through 10. The proton temperature is scaled by R 0.79 in the slow solar wind and R 1.10 in the fast wind. The fitted curves for the slow and fast solar winds are shown in black and cyan, respectively.
Paper: Near-Sun In Situ and Remote-sensing Observations of a Coronal Mass Ejection and its Effect on the Heliospheric Current Sheet
Authors: O. M. Romeo, C. R. Braga, S. T. Badman, D. E. Larson, M. L. Stevens, J. Huang, T. Phan, A. Rahmati, R. Livi, S. T. Alnussirat, P. L. Whittlesey, A. Szabo, K. G. Klein, T. Niembro-Hernandez, K. Paulson, J. L. Verniero, D. Lario, N. E. Raouafi, T. Ervin, J. Kasper, M. Pulupa, S. D. Bale, M. G. Linton
Figure caption: Normalized convolution spectra computed from RFS LFR data on 2021 August 9, targeted on the plasma line. The plasma frequencies selected from the inward and outward searches are designated by the white and black lines, respectively. Within the interval between times t  a  and t  b  (denoted by vertical lines), the two search algorithms do not follow the same path.
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: The Black Hole Mass–Stellar Mass Relations at 0.2 ≲ z ≲ 0.8
Authors: Jennifer I-Hsiu Li, Yue Shen, Luis C. Ho, W. N. Brandt, Catherine J. Grier, Patrick B. Hall, Y. Homayouni, Anton M. Koekemoer, Donald P. Schneider, Jonathan R. Trump
Figure caption: Projected physical offset between the quasar position and host centroid in the IR images as a function of the host effective radius. The uncertainties are estimated from GALFIT (quasar position and effective radius) and the quasar-subtracted host images (centroid position of the host). The error bars are inflated by a factor of 10 for clarity, as the GALFIT uncertainties are small and likely underestimated (median uncertainties are ∼0.02 kpc for the quasar/host separation and ∼0.005 kpc for the effective radius).
Paper: The Sloan Digital Sky Survey Reverberation Mapping Project: The Black Hole Mass–Stellar Mass Relations at 0.2 ≲ z ≲ 0.8
Authors: Jennifer I-Hsiu Li, Yue Shen, Luis C. Ho, W. N. Brandt, Catherine J. Grier, Patrick B. Hall, Y. Homayouni, Anton M. Koekemoer, Donald P. Schneider, Jonathan R. Trump
Figure caption: Quasar luminosity and redshift distribution of our sample (open orange circles), and a representative subset of the local RM sample (from Bentz et al. 2013; gray squares). The parent SDSS-RM sample (black circles) and those with measured lags (blue circles) from Grier et al. (2017b) are also labeled for reference.
Paper: Flare Duty Cycle of Gamma-Ray Blazars and Implications for High-energy Neutrino Emission
Authors: Kenji Yoshida, Maria Petropoulou, Kohta Murase, Foteini Oikonomou
Figure caption: The gamma-ray flux distributions of TXS 0506+056, PKS 0426-380, OJ 287, and PKS 0235+164 in 0.1–316 GeV fitted with a power-law function convolved with a Poisson distribution including the background photons. See text for details.
Paper: Flare Duty Cycle of Gamma-Ray Blazars and Implications for High-energy Neutrino Emission
Authors: Kenji Yoshida, Maria Petropoulou, Kohta Murase, Foteini Oikonomou
Figure caption: Estimated muon neutrino flare fluxes of 136 blazars (101 FSRQs, 28 BL Lac objects, and 7 BCUs) from the gamma-ray photon fluxes for a 1 week bin (a) and a 10 yr bin (b) of scenario (1) with A  γ  = 1.0, and γ = 1.5 as a function of ﹩\sin (\delta )﹩. The 90% IceCube sensitivities are the same as in Figure 8.
Paper: Flare Duty Cycle of Gamma-Ray Blazars and Implications for High-energy Neutrino Emission
Authors: Kenji Yoshida, Maria Petropoulou, Kohta Murase, Foteini Oikonomou
Figure caption: Examples of the 1.0 keV quiescent fluxes (dashed cyan lines) of PKS 0208-512 and PKS 1510-089 X-ray light curves (black points) with the Bayesian block representations (orange solid lines).
Paper: Stream Fanning and Bifurcations: Observable Signatures of Resonances in Stellar Stream Morphology
Authors: Tomer D. Yavetz, Kathryn V. Johnston, Sarah Pearson, Adrian M. Price-Whelan, Chris Hamilton
Figure caption: Left: SoS plot for the potential described in Section 2.1, with energy E = −(342.5 km s−1)2 and angular momentum L  z  = 1598 kpc  ×  km s−1. These values represent the total energy and 70% of the total angular momentum of a particle on a circular orbit at R = 10 kpc orbiting in the MW’s disk plane. The SoS is generated by plotting the consequents of 16 orbits, i.e., the values of R and v  R  every time z = 0 and v  z  > 0. The gray contours represent untrapped orbits and cover the full range of possible orbits given the values of E and L  z  chosen for this SoS, from an orbit in the plane of the disk with maximal radial action and zero vertical action (represented by the outermost gray contour) to a shell orbit with zero radial action and maximal vertical action (represented by the gray dot at the very center). The orange contours represent orbits within this range that are trapped at the Ω z : Ω R  = 1: 1 resonance. The parent orbits of the resonance are marked by black crosses. The separatrix, marking the transition between resonant and nonresonant orbits, is plotted with purple dashed lines. Upper right: frequency ratio of 256 equally spaced orbits between the two black triangles in the left panel (the initial conditions of the orbits are equally spaced in v  R , with fixed values of E, L  z , R = 7.4 kpc, and z = 0 kpc). The orientation of the two black triangles is preserved across all three panels to assist in identifying the orbits. The flat segment with Ω z /Ω R  = 1 corresponds to the resonantly trapped region in the left panel (i.e., the orange contours), and the vertical purple lines mark the separatrix. The frequencies were calculated as described in Section 2.2 over integration windows of 25 Gyr (long integration times are necessary to smooth over the resonant librations). Lower right: libration period T  ℓ  (=2π/ω  ℓ ) for each of the orbits in the upper panel, calculated using the SoS data as described in Section 3.2. Note how the libration period diverges (the libration frequency goes to zero) at the vertical purple lines representing the separatrices. Note also that while we refer to this as a plot of libration periods, only the points between the separatrices belong to librating orbits, whereas those on either side of the separatrix belong to circulating orbits.
Paper: Stream Fanning and Bifurcations: Observable Signatures of Resonances in Stellar Stream Morphology
Authors: Tomer D. Yavetz, Kathryn V. Johnston, Sarah Pearson, Adrian M. Price-Whelan, Chris Hamilton
Figure caption: Left column: two-dimensional histograms depicting the distribution of stellar streams in E − L  z  space for progenitor masses of 105 (top row), 107 (middle row), and 109 (bottom row) M ⊙. The black plus signs in the center mark the energy and angular momentum of the progenitor orbit (which is the same in all three rows), and the two clusters in each figure represent the leading and trailing arms. Each stream is generated as described in Section 2.3 and initialized close to the separatrix. A representative bin in (E, L  z ) from the leading (trailing) arm is chosen and marked with a red (blue) plus sign. Middle column: SoS for the chosen representative bin from the leading arm, marked by the red plus sign in the left panel. The locations of the outer SoS orbit, the resonant parent orbit, and the separatrix are plotted using the same line styles, markers, and colors as Figure 1, and the equivalent orbits from the progenitor’s SoS (i.e., the exact contours from Figure 1) are shown in light gray for reference. The median orbit in the selected (E, L  z ) bin is plotted with a solid red line, and its spread in the SoS is shown with the error bars, which correspond to δ v sos as defined in Section 3.3. Right column: same as the middle column for the trailing arm, with the median orbit and error bars plotted in blue.
Paper: Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353
Authors: Zixuan Peng, 子轩 彭, Crystal L. Martin, Pierre Thibodeaux, Jichen Zhang, 及晨 张, Weida Hu, Yuan Li, 远 李
Figure caption: Left: the gas-phase metallicity map with metallicities measured from the direct method. The bins are obtained via our adaptive binning algorithm with a target S/N = 5 for the [O III] λ4363 line. This map is divided into four regions (by two black dashed lines) with different position angles so we can find out how the metallicity gradients change with position angles (shown in Figure 8). The crossing of these two black dashed lines is the stellar-mass-weighted center (marked by the cyan circular point). Each bin is color coded by its own metallicity in terms of 12 + log(O/H). Right: distribution of the gas-phase metallicity of each bin obtained by the direct method. The median, mean, and standard deviation of the metallicity distribution are shown in the upper right corner. 45 out of 48 bins have metallicities within two standard deviations (σ Z = 0.05) of the median value. Two of the other three bins have metallicities of 7.31, and one has a metallicity of 7.60.
Paper: Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353
Authors: Zixuan Peng, 子轩 彭, Crystal L. Martin, Pierre Thibodeaux, Jichen Zhang, 及晨 张, Weida Hu, Yuan Li, 远 李
Figure caption: Analytical evolution of metallicity with gas fraction from Erb (2008) compared to the observed values of the SB and the PSB regions. Left: homogeneous wind models such that Z W = Z. Evolution curves are shown at fixed outflow rates (f o =  0 or 30), color coded by the inflow rate f i ranging from 0 to 28. Inflow-only models (i.e., the solid lines) can explain the position of the SB region (μ SB ≳ 0.98), which is consistent with Figure 5 in that v  p  is low around this region. The property of the PSB region (0.70 ≲ μ PSB ≲ 0.85) can only be reproduced by a high-f i high-f o model (e.g., f i = 28 and f o = 30), which is unrealistic. Right: non-homogeneous wind models such that Z W is defined in Equation (3). Evolution curves are shown at fixed outflow rates (f o =  0 or 10), color coded by the inflow rate f i ranging from 0 to 10. Compared to the homogeneous model, a reasonable range of f i (i.e., 2 ≲ f i ≲ 8) at a physical outflow rate of f o = 10 can explain the position of the PSB region. In each panel, the horizontal black (or gray) dashed line denotes the gas-phase metallicity for the SB (or PSB) region.
Paper: Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353
Authors: Zixuan Peng, 子轩 彭, Crystal L. Martin, Pierre Thibodeaux, Jichen Zhang, 及晨 张, Weida Hu, Yuan Li, 远 李
Figure caption: Left: the direct-based MZRs. The solid lines in various colors depict MZRs with direct-based metallicity measurements from multiple sources (Lee et al. 2006; Berg et al. 2012; Andrews & Martini 2013; Ly et al. 2016; Yates et al. 2020). The yellow dashed line illustrates the MZR extrapolation from AM13 to the low-mass regime of J1044+0353. The total stellar mass of J1044+0353 is represented by a blue circle and extracted from B22, with the median metallicity value and 1σ uncertainty (σ = 0.05) from Figure 7. Right: total SFR vs. total stellar mass (SFMR). J1044+0353's position is indicated by a blue circle based on values from B22, while the overall CLASSY sample trend is represented by a blue solid line (B22). The z ∼ 0.5–2.5 SFMR trends from Whitaker et al. (2014; orange lines) and z ∼ 0 trends from Chang et al. (2015; SDSS; cyan dashed line) and Berg et al. (2012; LMLVL; green solid line) are included for comparison.
Paper: Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353
Authors: Zixuan Peng, 子轩 彭, Crystal L. Martin, Pierre Thibodeaux, Jichen Zhang, 及晨 张, Weida Hu, Yuan Li, 远 李
Figure caption: Metallicity gradients in different position angles. The galaxy is divided into four regions with corresponding position angles (shown in the title of each panel; see Figure 7). For each panel, the black solid line is the best-fitting linear function. The RSS of each best-fitting linear model is presented in each panel. The green and orange areas respectively represent the 68% and the 95% confidence bands of the best-fitting line. The gradients in the South and West regions could potentially be positive; however, their error bars are comparable to their respective values. The North and East regions, centered around the PSB region, show slightly larger scatter compared to the other two regions. Overall, all regions exhibit relatively flat metallicity gradients considering the error bars, indicating minor azimuthal metallicity variations.
Paper: Stream Fanning and Bifurcations: Observable Signatures of Resonances in Stellar Stream Morphology
Authors: Tomer D. Yavetz, Kathryn V. Johnston, Sarah Pearson, Adrian M. Price-Whelan, Chris Hamilton
Figure caption: Another SoS plot for the same potential used to produce Figure 1, this time with E = −(235.5 km s−1)2 and L  z  = 141.3 kpc × km s−1. The relative value of the angular momentum is much smaller than in Figure 1 and equivalent to only 10% of the value of L  z  for a circular orbit in the xy-plane with the same total energy. As a result, these orbits probe a much larger extent of the potential, and several other resonant orbit families appear in the SoS, in addition to the 1:1 resonance at the top and bottom of the plot. As in Figure 1, the parent orbits of each resonant orbit family are shown by black crosses.