adsabs/AstroCLIMB huggingface dataset:
Paper: Radio Scrutiny of the X-Ray-weak Tail of Low-mass Active Galactic Nuclei: A Novel Signature of High-Eddington Accretion?
Authors: Jeremiah D. Paul, Richard M. Plotkin, W. N. Brandt, Christopher H. Ellis, Elena Gallo, Jenny E. Greene, Luis C. Ho, Amy E. Kimball, Daryl Haggard
Figure caption: (a) Histograms comparing our sample’s distributions of radio-loudness parameters, ﹩{{ \mathcal R }}_{{\rm{O}}}﹩ (top) and ﹩{{ \mathcal R }}_{{\rm{X}}}﹩ (bottom), on matched log scales. Arrows denote limits from nondetections. The dashed–dotted and dashed vertical lines respectively show our adopted ﹩{{ \mathcal R }}_{{\rm{O}}}﹩-quiet and ﹩{{ \mathcal R }}_{{\rm{X}}}﹩-quiet demarcations. Objects to the left of these lines are considered radio-quiet. Our sample is predominantly radio-quiet in ﹩{{ \mathcal R }}_{{\rm{O}}}﹩ but not ﹩{{ \mathcal R }}_{{\rm{X}}}﹩, suggesting that X-rays are preferentially weakened. (b) Comparison of ﹩{{ \mathcal R }}_{{\rm{X}}}﹩ and ﹩{{ \mathcal R }}_{{\rm{O}}}﹩ in log scale. Symbols are as defined for Figure 2(a), except objects in our sample with f weak ≥ 10 are pink-filled and those with f weak < 10 are green-filled. The vertical dashed–dotted lines show the conventional ﹩{{ \mathcal R }}_{{\rm{O}}}﹩-quiet (teal) and ﹩{{ \mathcal R }}_{{\rm{O}}}﹩-loud (orange) demarcations, and the horizontal dashed lines show our adopted ﹩{{ \mathcal R }}_{{\rm{X}}}﹩-quiet (teal) and ﹩{{ \mathcal R }}_{{\rm{X}}}﹩-loud (orange) demarcations (based on empirical boundaries suggested by Terashima & Wilson 2003 and Panessa et al. 2007). The yellow shaded area roughly illustrates the tendency for large, radio-diverse samples of AGNs to experience a tandem increase in radio loudness on both axes (see, e.g., Figure 5 of Zuther et al. 2012). While our sample is largely ﹩{{ \mathcal R }}_{{\rm{O}}}﹩-quiet, the f weak ≥ 10 objects deviate from the trend further into ﹩{{ \mathcal R }}_{{\rm{X}}}﹩-intermediate space, suggesting that X-rays are preferentially weakened. Zuther et al. (2012) note that this behavior is also seen with broad absorption line quasars (which may experience X-ray weakness due to obscuration).
Paper: Radio Scrutiny of the X-Ray-weak Tail of Low-mass Active Galactic Nuclei: A Novel Signature of High-Eddington Accretion?
Authors: Jeremiah D. Paul, Richard M. Plotkin, W. N. Brandt, Christopher H. Ellis, Elena Gallo, Jenny E. Greene, Luis C. Ho, Amy E. Kimball, Daryl Haggard
Figure caption: (a) X-ray weakness (represented by Δα ox; more negative values are X-ray-weaker) vs. 2500 Å monochromatic luminosity. Horizontal dotted lines denote f weak at values of 1, 10, and 100 (see Section 2.1). Note that f weak = 1 (Δα ox = 0) marks the best-fit α ox–l 2500 relationship of Just et al. (2007). Our target sample of 18 G&H07 low-mass AGNs is shown by green diamonds (Δα ox values are from our recalculations; see Section 2.2), while the remainder of the G&H07 catalog is represented by black circles (Δα ox values from Desroches et al. 2009 and R. Dong et al. 2012). Filled and empty symbols denote X-ray detections and nondetections, respectively. Gray squares represent the SDSS quasar samples used by Steffen et al. (2006) and Just et al. (2007) to define Δα ox. Our sample spans the full range of X-ray weaknesses observed in the G&H07 catalog. (b) Histograms showing the M BH (top) and ℓ Edd (bottom) distributions of our sample selection (orange hatched region) compared to the G&H07 parent sample (blue outlined region).
Paper: Radio Scrutiny of the X-Ray-weak Tail of Low-mass Active Galactic Nuclei: A Novel Signature of High-Eddington Accretion?
Authors: Jeremiah D. Paul, Richard M. Plotkin, W. N. Brandt, Christopher H. Ellis, Elena Gallo, Jenny E. Greene, Luis C. Ho, Amy E. Kimball, Daryl Haggard
Figure caption: Radio images for the first nine new observations (object order follows the earlier data tables). North is up and east is left. For each image, GH ID is given in the upper left corner, synthesized beam size is shown in the lower left corner, and estimated projected physical scale at the target’s location is illustrated in the lower right corner. Green contours are applied at −3 (dashed), 3, 4, 6, 8, 16, and 32× the image rms (σ rms). The orange dot indicates coordinates of the galaxy center from SDSS. Purple outlines show unique fit selection regions discussed in the Appendix text. The grayscale tone map indicates flux density in Jy beam−1. Top left: GH 25, σ rms = 0.004 mJy, beam size 1.″28 × 0.″72. Top middle: GH 73, σ rms = 0.007 mJy, beam size 1.″02 × 0.″56. Top right: GH 80, σ rms = 0.004 mJy, beam size 1.″18 × 0.″69. Mid left: GH 104, σ rms = 0.004 mJy, beam size 1.″06 × 0.″59. Center: GH 157, σ rms = 0.006 mJy, beam size 0.″89 × 0.″75. Mid right: GH 160, σ rms = 0.004 mJy, beam size 0.″63 × 0.″61. Bottom left: GH 185, σ rms = 0.005 mJy, beam size 1.″24 × 0.″68. Bottom middle: GH 211, σ rms = 0.008 mJy, beam size 1.″13 × 0.″70. Bottom right: GH 213, σ rms = 0.009 mJy, beam size 0.″96 × 0.″58.
Paper: Radio Scrutiny of the X-Ray-weak Tail of Low-mass Active Galactic Nuclei: A Novel Signature of High-Eddington Accretion?
Authors: Jeremiah D. Paul, Richard M. Plotkin, W. N. Brandt, Christopher H. Ellis, Elena Gallo, Jenny E. Greene, Luis C. Ho, Amy E. Kimball, Daryl Haggard
Figure caption: X-ray photon index, Γ, vs. Δα ox (see Section 4.2). Symbols are as defined for Figure 2(a). Note that objects with X-ray nondetections or low counts lack Γ measurements (see Section 2.2) and are not included. The solid orange line shows a linear regression fit excluding GH 47 (tagged by name), with the 1σ confidence level given by the yellow shaded area. Our sample shows weak hints of a correlation (p null = 0.087). We extend the figure leftward to illustrate how the best-fit regression reaches values of Γ ∼ 1.0 near our X-ray-weakest targets’ upper limits on Δα ox (≲−0.7), consistent with the X-ray stacking analysis performed by Plotkin et al. (2016). The dashed orange line shows an alternative version of the regression including GH 47.
Paper: Radio Scrutiny of the X-Ray-weak Tail of Low-mass Active Galactic Nuclei: A Novel Signature of High-Eddington Accretion?
Authors: Jeremiah D. Paul, Richard M. Plotkin, W. N. Brandt, Christopher H. Ellis, Elena Gallo, Jenny E. Greene, Luis C. Ho, Amy E. Kimball, Daryl Haggard
Figure caption: Radio images for the remaining two new observations and all archival observations (object order follows the earlier data tables). North is up and east is left. For each image, GH ID is given in the upper left corner, synthesized beam size is shown in the lower left corner, and estimated projected physical scale at the target’s location is illustrated in the lower right corner. Green contours are applied at −3 (dashed), 3, 4, 6, 8, 16, 32, and 64× the image rms (σ rms). The orange dot indicates coordinates of the galaxy center from SDSS. The grayscale tone map indicates flux density in Jy beam−1. Top left: GH 214, σ rms = 0.009 mJy, beam size 0.″78 × 0.″59. Top middle: GH 215, σ rms = 0.010 mJy, beam size 0.″86 × 0.″57. Top right: GH 47, σ rms = 0.003 mJy, beam size 0.″29 × 0.″22. Mid left: GH 69, σ rms = 0.004 mJy, beam size 0.″32 × 0.″26. Center: GH 87, σ rms = 0.005 mJy, beam size 0.″32 × 0.″23. Mid right: GH 106, σ rms = 0.003 mJy, beam size 0.″27 × 0.″19. Bottom left: GH 146, σ rms = 0.004 mJy, beam size 0.″32 × 0.″22. Bottom middle: GH 174, σ rms = 0.005 mJy, beam size 0.″29 × 0.″18. Bottom right: GH 203, σ rms = 0.004 mJy, beam size 0.″24 × 0.″2.
Paper: Radio Scrutiny of the X-Ray-weak Tail of Low-mass Active Galactic Nuclei: A Novel Signature of High-Eddington Accretion?
Authors: Jeremiah D. Paul, Richard M. Plotkin, W. N. Brandt, Christopher H. Ellis, Elena Gallo, Jenny E. Greene, Luis C. Ho, Amy E. Kimball, Daryl Haggard
Figure caption: BPT diagram (Baldwin et al. 1981) comparing narrow emission-line ratios (see Section 4.1.2). Objects in our sample with f weak ≳ 10 are pink-filled, and those with f weak < 10 are green-filled. The black dots show the remainder of the G&H07 high-confidence parent sample (excluding objects with limits on one or more of the emission-line strengths). The solid curve shows the empirical demarcation of “pure star formation” from Kauffmann et al. (2003), while the dashed curve shows the theoretical “maximum starburst line” from Kewley et al. (2001); “composite” galaxies fall between the two. The diagonal dotted line divides Seyferts and low-ionization nuclear emission-line regions (LINERs; Schawinski et al. 2007).
Paper: Tidal Disruption of a Star on a Nearly Circular Orbit
Authors: Itai Linial, Eliot Quataert
Figure caption: Band-dependent lightcurve, ν L  ν  for an m ⋆ = 0.5 M ⊙ white dwarf and an M • = 105 M ⊙ IMBH.
Paper: Repeating Nuclear Transients from Repeating Partial Tidal Disruption Events: Reproducing ASASSN-14ko and AT2020vdq
Authors: Ananya Bandopadhyay, Eric R. Coughlin, C. J. Nixon, Dheeraj R. Pasham
Figure caption: Rotational velocity Ω imparted to the core of the 3M ⊙ TAMS star, in units of its breakup spin, as a function of time measured relative to when the COM of the star reaches pericenter. The initially nonrotating star is spun up near pericenter, and continues to rotate with a roughly constant angular velocity beyond ∼2 days past pericenter.
Paper: Searching for the Highest-z Dual Active Galactic Nuclei in the Deepest Chandra Surveys
Authors: Brandon Sandoval, Adi Foord, Steven W. Allen, Marta Volonteri, Nianyi Chen, Tiziana Di Matteo, Aaron Stemo, Kayhan Gültekin, Melanie Habouzit, Clara Puerto-Sánchez, Edmund Hodges-Kluck, Yohan Dubois
Figure caption: Dual-AGN fraction measured from our sample (black arrow) at the 95% confidence level. We overplot predictions of the dual-AGN fraction as a function of the redshift from cosmological simulations: Magneticum (brown; Steinborn et al. 2016), EAGLE (yellow; Rosas-Guevara et al. 2019), Horizon-AGN (blue; Volonteri et al. 2022), and ASTRID (purple; Chen et al. 2023a). All simulations define AGN as SMBHs with bolometric luminosities greater than 1043 erg s−1 (in dashed lines we show Horizon-AGN and ASTRID results where AGN are defined as SMBHS with bolometric luminosities greater than 1044 erg s−1; see Section 5.2). Error bars for Horizon-AGN, ASTRID, and Magneticum are calculated via binomial error analysis and represent the 95% confidence level. Error bars for the EAGLE simulations are taken from Rosas-Guevara et al. 2019 and represent a standard deviation. Albeit an upper limit, our measurement is consistent with predictions from simulations. We show how well future X-ray mission probe concept AXIS could constrain the dual-AGN fraction at this same redshift bin (assuming a dual-AGN fraction of ∼3% and the flux limit of CDF-S; red solid line). In general, future X-ray missions, with small PSFs, large FOVs, and large effective areas will find hundreds of new dual AGN, which will allow for better constraining the population of dual AGN in our Universe. Foord et al. (2024) present more details regarding AXIS’s ability to quantify the fraction of dual AGN as a function of the redshift.
Paper: Searching for the Highest-z Dual Active Galactic Nuclei in the Deepest Chandra Surveys
Authors: Brandon Sandoval, Adi Foord, Steven W. Allen, Marta Volonteri, Nianyi Chen, Tiziana Di Matteo, Aaron Stemo, Kayhan Gültekin, Melanie Habouzit, Clara Puerto-Sánchez, Edmund Hodges-Kluck, Yohan Dubois
Figure caption: Top: duty cycle of AGN from the ASTRID simulations, defined as the fraction of SMBHs in a given bolometric luminosity, over the total number of SMBHs (active and inactive) in each SMBH mass bin. At z = 2, M SMBH > 107 M ⊙, and ﹩43\lt \mathrm{log}{L}_{\mathrm{bol}}\lt 44﹩, we find that the duty cycles predicted by ASTRID agree with those from the Horizon-AGN simulations (Volonteri et al. 2016); the latter have been shown to also agree with observational measurements (Juneau et al. 2013; Schulze et al. 2015). The zoomed inset highlights marginal differences between each mass cut at the low-luminosity and high-duty-cycle region of the parameter space. Bottom: The expected dual-AGN activation fraction in ASTRID simulations (based on the duty cycle and assuming the activation of two SMBHs in the pair is completely independent), compared to the measured dual-AGN activation fraction in ASTRID. We find that the measured value is slightly higher than the baseline value, indicating that the pairing likely enhances the AGN activities. Additionally, analyzing the probability that at least one SMBH in the pair is active, the value remains higher than the expected value from the duty cycle. These results are in agreement with those found in Volonteri et al. (2016), where enhancement of AGN activity in galaxies with companions may be expected and which can lead to enhanced dual-AGN fractions (as seen in Figure 4).
Paper: Searching for the Highest-z Dual Active Galactic Nuclei in the Deepest Chandra Surveys
Authors: Brandon Sandoval, Adi Foord, Steven W. Allen, Marta Volonteri, Nianyi Chen, Tiziana Di Matteo, Aaron Stemo, Kayhan Gültekin, Melanie Habouzit, Clara Puerto-Sánchez, Edmund Hodges-Kluck, Yohan Dubois
Figure caption: Stacked 0.5−8 keV Chandra observations analyzed for each AGN. We analyze the photons in a 20″ × 20″ box on the nominal X-ray coordinate listed in the point-source catalogs, with the exception of AEGISXD214.93+52.77 (7) and XUDS34.52-5.06 (64). These sources contained a second, bright source within the 20″ × 20″ FOV with a redshift measurement inconsistent (> 300 km−2) with the primary AGN being analyzed. For these two sources, we analyzed a smaller FOV that avoids these secondary nearby sources. We denote sources that have ﹩\mathrm{log}{ \mathcal B }{ \mathcal F }﹩ that is greater than zero at the 3σ level with †(see Table 2). False-positive testing shows that these values are consistent with ﹩\mathrm{log}{ \mathcal B }{ \mathcal F }﹩ values expected from a single point source (see Section 4.1).
Paper: Searching for the Highest-z Dual Active Galactic Nuclei in the Deepest Chandra Surveys
Authors: Brandon Sandoval, Adi Foord, Steven W. Allen, Marta Volonteri, Nianyi Chen, Tiziana Di Matteo, Aaron Stemo, Kayhan Gültekin, Melanie Habouzit, Clara Puerto-Sánchez, Edmund Hodges-Kluck, Yohan Dubois
Figure caption: The 90th percentiles of the CDF of the 100 simulated single-point-source ﹩\mathrm{log}{ \mathcal B }{ \mathcal F }﹩ values calculated for each source. In red, we show sources with ﹩\mathrm{log}{ \mathcal B }{ \mathcal F }﹩ values greater than zero at the 3σ level. A line is drawn at 3′, above which we tend to get consistently larger ﹩\mathrm{log}{ \mathcal B }{ \mathcal F }﹩ values. The inset shows the spread of values when restricting our sample to sources with OAA < 3′. For sources with more than one observation, we calculate a weighted OAA average (via the exposure times).
Paper: Searching for the Highest-z Dual Active Galactic Nuclei in the Deepest Chandra Surveys
Authors: Brandon Sandoval, Adi Foord, Steven W. Allen, Marta Volonteri, Nianyi Chen, Tiziana Di Matteo, Aaron Stemo, Kayhan Gültekin, Melanie Habouzit, Clara Puerto-Sánchez, Edmund Hodges-Kluck, Yohan Dubois
Figure caption: Distributions of the redshift (left), OAA (center), and total counts between 0.5 and 8 keV (right) for the 62 X-ray sources composing the sample. Each X-ray source has photometric or spectroscopic redshift data from its respective catalog. For sources with more than one observation, we calculate a weighted OAA average (via the exposure time). The count number is determined by the number of 0.5−8 keV photons in a 20″ × 20″ box centered on the nominal coordinate listed in the source catalog.
Paper: Searching for the Highest-z Dual Active Galactic Nuclei in the Deepest Chandra Surveys
Authors: Brandon Sandoval, Adi Foord, Steven W. Allen, Marta Volonteri, Nianyi Chen, Tiziana Di Matteo, Aaron Stemo, Kayhan Gültekin, Melanie Habouzit, Clara Puerto-Sánchez, Edmund Hodges-Kluck, Yohan Dubois
Figure caption: We show the test statistic distributions for the AD test (above) and the KS test (below) when comparing the distribution of measured Bayes factors to the distribution we would expect from a sample composed entirely of single point sources. On the horizontal axis, we have labeled the critical values corresponding to the 5% and 1% significance levels.
Paper: AGN STORM 2. IX. Studying the Dynamics of the Ionized Obscurer in Mrk 817 with High-resolution X-Ray Spectroscopy
Authors: Fatima Zaidouni, Erin Kara, Peter Kosec, Missagh Mehdipour, Daniele Rogantini, Gerard A. Kriss, Ehud Behar, Jelle Kaastra, Aaron J. Barth, Edward M. Cackett, Gisella De Rosa, Yasaman Homayouni, Keith Horne, Hermine Landt, Nahum Arav, Misty C. Bentz, Michael S. Brotherton, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Jonathan Gelbord, Michael R. Goad, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Collin Lewin, John Montano, Hagai Netzer, Jack M. M. Neustadt, Christos Panagiotou, Ethan R. Partington, Rachel Plesha, Luka Č. Popović, Daniel Proga, Thaisa Storchi-Bergmann, David Sanmartim, Matthew R. Siebert, Matilde Signorini, Marianne Vestergaard, Tim Waters, Ying Zu
Figure caption: The contribution of each of the PION photoionization model components to the overall fit for Segment 1 (t < 60 ks, top panel), and Segment 2 (t > 60 ks, middle panel). The bottom panel shows the scenario where a statistically significant, but redundant PION component is added to the fit of Segment 2. The models are in the form of “(pow × etau × etau + bb + dbb + refl) × pion, ” which we achieve by setting the covering fraction of the other PION components to zero. For both Segments 1 and 2, PION 1 (black) is the lowest ionization component, fitting largely the long wavelength lines and the iron UTA, while PION 2 (blue) is a higher ionization component, modeling largely the shorter wavelength lines. PION 3 (pink) accounts for the asymmetry in the line shapes of Segment 1 (see the text for details).
Paper: AGN STORM 2. IX. Studying the Dynamics of the Ionized Obscurer in Mrk 817 with High-resolution X-Ray Spectroscopy
Authors: Fatima Zaidouni, Erin Kara, Peter Kosec, Missagh Mehdipour, Daniele Rogantini, Gerard A. Kriss, Ehud Behar, Jelle Kaastra, Aaron J. Barth, Edward M. Cackett, Gisella De Rosa, Yasaman Homayouni, Keith Horne, Hermine Landt, Nahum Arav, Misty C. Bentz, Michael S. Brotherton, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Jonathan Gelbord, Michael R. Goad, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Collin Lewin, John Montano, Hagai Netzer, Jack M. M. Neustadt, Christos Panagiotou, Ethan R. Partington, Rachel Plesha, Luka Č. Popović, Daniel Proga, Thaisa Storchi-Bergmann, David Sanmartim, Matthew R. Siebert, Matilde Signorini, Marianne Vestergaard, Tim Waters, Ying Zu
Figure caption: The top panel shows the C IV line profile from an HST COS spectrum taken a day before the X-ray observation (see text for details). The bottom panel shows strong X-ray absorption line profiles from the overall 2021 April RGS spectrum, notably, the transitions: O VII Lyα, O VII (r), N VII Lyα, and C VI Lyα along with the model fit to the overall observation. The velocities are with respect to the rest frame of the source. The y-axis is the normalized flux with respect to the unabsorbed continuum. Both the X-ray and UV data show evidence for an obscurer outflowing at between ∼ −5000 and ∼ −6000 km s−1. The vertical dashed lines show the approximate centers of the absorption troughs.
Paper: AGN STORM 2. IX. Studying the Dynamics of the Ionized Obscurer in Mrk 817 with High-resolution X-Ray Spectroscopy
Authors: Fatima Zaidouni, Erin Kara, Peter Kosec, Missagh Mehdipour, Daniele Rogantini, Gerard A. Kriss, Ehud Behar, Jelle Kaastra, Aaron J. Barth, Edward M. Cackett, Gisella De Rosa, Yasaman Homayouni, Keith Horne, Hermine Landt, Nahum Arav, Misty C. Bentz, Michael S. Brotherton, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Jonathan Gelbord, Michael R. Goad, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Collin Lewin, John Montano, Hagai Netzer, Jack M. M. Neustadt, Christos Panagiotou, Ethan R. Partington, Rachel Plesha, Luka Č. Popović, Daniel Proga, Thaisa Storchi-Bergmann, David Sanmartim, Matthew R. Siebert, Matilde Signorini, Marianne Vestergaard, Tim Waters, Ying Zu
Figure caption: Thermal stability curves (S curves) showing the equilibrium electron temperature of the gas as a function of the ionization parameter (ξ) in the bottom panels and as a function of the pressure form of the ionization parameter (Ξ) in the top panels. The S curves are calculated using the SEDs seen by each of the photoionization components during the first half of the observation (Segment 1, left column) and the second half (Segment 2, right column). The thick strips show the positions of the derived photoionization components (including the fitting uncertainties) from the best-fitting model of the spectra.
Paper: AGN STORM 2. IX. Studying the Dynamics of the Ionized Obscurer in Mrk 817 with High-resolution X-Ray Spectroscopy
Authors: Fatima Zaidouni, Erin Kara, Peter Kosec, Missagh Mehdipour, Daniele Rogantini, Gerard A. Kriss, Ehud Behar, Jelle Kaastra, Aaron J. Barth, Edward M. Cackett, Gisella De Rosa, Yasaman Homayouni, Keith Horne, Hermine Landt, Nahum Arav, Misty C. Bentz, Michael S. Brotherton, Elena Dalla Bontà, Maryam Dehghanian, Gary J. Ferland, Carina Fian, Jonathan Gelbord, Michael R. Goad, Diego H. González Buitrago, Catherine J. Grier, Patrick B. Hall, Chen Hu, Dragana Ilić, Shai Kaspi, Christopher S. Kochanek, Andjelka B. Kovačević, Daniel Kynoch, Collin Lewin, John Montano, Hagai Netzer, Jack M. M. Neustadt, Christos Panagiotou, Ethan R. Partington, Rachel Plesha, Luka Č. Popović, Daniel Proga, Thaisa Storchi-Bergmann, David Sanmartim, Matthew R. Siebert, Matilde Signorini, Marianne Vestergaard, Tim Waters, Ying Zu
Figure caption: The RGS spectra for Segment 1 (top two panels) and Segment 2 (bottom panel) with the best-fitting model overlaid in red. We show the best fitting models using two and three PIONs for Segment 1 to highlight the difference in accounting for the extended red wing of the absorption troughs. The residuals are calculated as (data-model)/error.
Paper: Bayesian Black Hole Photogrammetry
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede, Daniel C. M. Palumbo
Figure caption: Partial corner plot showing the posterior for a subset of the parameter space of a dual-cone fit to itself using EHT 2017 coverage. The shown parameters are the mass-to-distance ratio (θ  g ), the black hole spin (a), the observer inclination (θ o), the jet opening angle (θ  s ), the projected position angle of the spin axis on the observer’s screen (p.a.), and the characteristic radius of the emissivity function (R). The true values of the model used to generate the data are shown with black lines. The posterior features two distinct clusters, depicted in blue and yellow, which we isolate using the k-means clustering algorithm. Figure 16 shows the full corner plot for this fit.