adsabs/AstroCLIMB huggingface dataset:
Paper: Very Extended Ionized Gas Discovered around NGC 1068 with the Circumgalactic Hα Spectrograph
Authors: Nicole Melso, David Schiminovich, Meghna Sitaram, Ignacio Cevallos-Aleman, Bárbara Cruvinel Santiago, Brian Smiley, Hwei Ru Ong
Figure caption: CHαS spectral fitting for the ribbon. All panels have been rotated (∼15°) to align the hexagonally packed spectra along the Cartesian y-axis. The transformed coordinates can be compared directly with Figure 1. Left: relative velocity with respect to the systemic velocity of NGC 1068 (V sys = 1137 km s−1) from a Gaussian fit of each lenslet spectrum. Middle: velocity dispersion from the Gaussian fit to each lenslet spectrum. Right: spectra analyzed have a SNR ≥ 5 in a rectangular aperture (w, h) = (5, 3) pixels. This aperture sizing corresponds to emission with a velocity width of ∼100 km s−1.
Paper: Tidal Disruption of a Star on a Nearly Circular Orbit
Authors: Itai Linial, Eliot Quataert
Figure caption: Band-dependent lightcurves (ν L  ν ) from a Sun-like star undergoing unstable mass transfer to an SMBH of mass M • = 106 M⊙. Prior to the final disruption of the star, the emission is accretion-dominated, peaking at X-rays, while toward the final disruption of the star at time t  f , super-Eddington outflow develops, temporarily producing cooler and brighter emission. Following the star’s final disruption and the decay in viscously limited accretion, the disk’s emission dominates at late times. Top panel: linear horizontal time axis, around time t = t  f . Bottom panel: Same as the top panel, but with a double logarithmic horizontal axis, with negative values indicating time prior to the final disruption of the star, and vice versa. Black dashed vertical line marks one viscous time (Equation (25)) following the star’s disruption.
Paper: Tidal Disruption of a Star on a Nearly Circular Orbit
Authors: Itai Linial, Eliot Quataert
Figure caption: Temporal evolution of an unstable mass transfer from a Sun-like main-sequence star onto an SMBH of mass M • = 106 M ⊙. Dashed blue curve is the mass-loss rate ﹩{\dot{m}}_{\star }﹩ in units of ﹩{\dot{M}}_{\mathrm{Edd}}﹩ as a function of time t since the onset of mass transfer. Red solid curve is ﹩{\dot{m}}_{\bullet }﹩, the feeding rate onto the SMBH, which mostly follows ﹩{\dot{m}}_{\star }﹩, almost up to the final disruption of the star at time t  f  ≈ 3100 yr. The remnants of the star then accrete onto the SMBH through viscous spreading, decaying at times t > t  f . Horizontal black dashed line is roughly the steady-state accretion rate through stable mass transfer (Equation (6)), and the two horizontal orange dashed lines represent Eddington ratios of 0.01 and 1, for which a radiatively efficient disk forms. The thin purple curve shows the increase in ﹩{\dot{m}}_{\star }﹩ during the initial phase after the onset of mass transfer, when RLOF is driven by the GW inspiral of the star (Equation (19)), appropriate at times earlier than t runaway (Equation (21)).
Paper: Tidal Disruption of a Star on a Nearly Circular Orbit
Authors: Itai Linial, Eliot Quataert
Figure caption: Top panel: The maximum value of ν L  ν  in different observational bands, as a function of t visc, the (somewhat uncertain) viscous time at r MT (Equation (25)). Bottom panel: The full width at half maximum (FWHM) as a function of t visc. For ν = 500 eV band, we plot the FWHM of both the pre- and post-disruption flares (see Figure 4) in dotted and solid purple lines, respectively. The fiducial value used throughout the paper is marked by the vertical black dashed line.
Paper: Tidal Disruption of a Star on a Nearly Circular Orbit
Authors: Itai Linial, Eliot Quataert
Figure caption: Circum-nuclear density produced by super-Eddington outflow from a circular TDE, for m ⋆ = 1 M ⊙ and M • = 106 M ⊙. Different colors correspond to different epochs relative to the complete disruption of the star. Stars indicate the distance at which nr 3 is maximized, corresponding to where most of the ejected mass is concentrated.
Paper: Tidal Disruption of a Star on a Nearly Circular Orbit
Authors: Itai Linial, Eliot Quataert
Figure caption: A schematic sketch indicating the different stages of evolution. Mass transfer from the star to the SMBH ensues once r = r MT ≈ few × r t. At low accretion rates (﹩{\dot{m}}_{\star }\lesssim {\dot{M}}_{\mathrm{Edd}}﹩), matter leaving the star from the inner Lagrange point produces a thin accretion disk, emitting X-rays (alongside a circumbinary ring fed by the outer Lagrange point). Mass transfer continues to accelerate to super-Eddington rates, producing quasi-spherical, optically thick outflows. The extended photosphere produces super-Eddington emission peaking at optical/UV frequencies. The star is eventually fully disrupted, with its remnants feeding the SMBH through viscous evolution, eventually emitting X-rays from a radiatively efficient thin disk.
Paper: Tidal Disruption of a Star on a Nearly Circular Orbit
Authors: Itai Linial, Eliot Quataert
Figure caption: Bolometric luminosity and characteristic blackbody temperature as a function of time for a Sun-like star orbiting a 106 M ⊙ SMBH. Time is measured relative to the star’s final disruption, t  f . Horizontal black dashed line is the SMBH’s Eddington luminosity.
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: Top: the amount of mass stripped, ΔM, as a function of the number of pericenter passages, N, for a 1M ⊙ ZAMS star with β = 0.6 for each encounter. The absence of a centrally concentrated core-like structure leads to a progressive increase in the amount of mass stripped with the number of pericenter passages. Bottom: fallback rates for the first five encounters between the 1M ⊙ ZAMS star and a 106 M ⊙ SMBH, at β = 0.6, with a resolution of 106 particles. The peak of the fallback rate increases gradually as the amount of mass stripped increases, and the peak timescale shifts to earlier times.
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: Comparison of fallback rates at different resolutions for the 3M ⊙ TAMS star. The solid curves have a higher resolution of 107 particles, and the dashed curves represent the lower-resolution simulations with 106 particles. The curves for corresponding encounters are in good agreement with each other, barring slight differences in the early time fallback, which is sensitive to the resolution.
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: Fallback rates onto a 106 M ⊙ SMBH from the partial disruption of the 3M ⊙ TAMS star on its first six pericenter passages, with (pink) and without shock heating (purple). With the inclusion of shock heating, the outer layers of the star puff-up, leading to an increased amount of mass loss as compared to the case without shock heating. The fallback rates for the second and third encounters show the maximum deviation from the ones for which shock heating is excluded. Once the outer layers of the star are removed, subsequent pericenter passages lead to a comparable amount of mass being lost from the surviving core, and almost indistinguishable fallback rates with and without heating.
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: The timescale on which the fallback rates reach their peak, as a function of the imparted angular velocity Ω. The peak timescale declines as a function of ﹩\left(1+\sqrt{2}{\rm{\Omega }}/\sqrt{{{GM}}_{\bullet }/{r}_{{\rm{p}}}^{3}}\right)﹩, with a power-law index of −0.8.
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: Fallback rates for the disruption of the 1M ⊙ ZAMS star at β = 1.5. The first encounter leads to a partial disruption, but strips of a significant fraction of the mass of the star. The second encounter results in the complete disruption of the star, giving rise to a fallback rate exhibiting a smaller peak magnitude, that scales as ∝t −5/3 at late-times.
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: The column density profile of the 3M ⊙ TAMS star at ∼1 day past pericenter passage, with (right) and without (left) shock heating, at a resolution of 10M particles. The top panel shows a comparison of the density profile in x–y coordinates, and the bottom panel shows the density profile in x–z coordinates. The outer layers of the star are inflated in the simulation including shock heating, but structure of the core is largely unaffected, thus preventing the star from being completely disrupted in a few orbits.
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: Fallback rates for the first seven encounters between a 1.3M ⊙ TAMS star and a 106 M ⊙ SMBH, with an impact parameter β = 1. We used a resolution of 106 particles for these simulations. The evolution of the fallback rates over multiple encounters follows a similar trend to the 3M ⊙ TAMS star.
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: The fallback rates for the first pericenter passage of the 3M ⊙ TAMS star, with and without shock heating. The solid curves are for a higher resolution of 10M particles, whereas the dashed curves are for a resolution of 1M particles.
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: Fallback rates for the disruption of the 1M ⊙ ZAMS star at β = 1. The second encounter yields a brighter peak relative to the first one, as the amount of mass stripped is roughly doubled.
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 best-fitting SED model. The total obscured (observed) SED is shown in blue, and the inferred unobscured (intrinsic) continuum in red. The model components are shown using non-solid lines. The X-ray continuum is modeled as a cutoff power law (green dotted–dashed). We model the soft excess as a phenomenological blackbody spectrum (blue dotted). The accretion disk is modeled as a multitemperature disk blackbody (orange dashed). The X-ray reflection (iron Kα and Compton hump emission) is shown as a pink dotted line.
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: Flux density multiplied by E 2 for the four XMM-Newton+NuSTAR epochs from the prime AGN STORM 2 X-ray campaign. For comparison, we show the archival XMM-Newton observation from 2009 December (Winter et al. 2011) in gray. There is significant variability in the soft X-rays (due to the ionized obscurer) as well as changes in the hard X-ray emission indicative of intrinsic variability in the corona. The 2021 April observation, in blue, is the focus of this paper.
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 AGN STORM 2 Swift XRT and UVW2 light curves from 2020 December to 2022 February (Cackett et al. 2023). Vertical lines indicate when the XMM-Newton and NuSTAR observations were conducted. The green horizontal line indicates the anticipated count rate based on the mean flux of an archival Swift campaign (Morales et al. 2019). During the AGN STORM 2 campaign, the source was largely obscured, with a mean Swift/XRT count rate below 0.2 counts s−1, except for a high-flux state in 2021 April. Our second XMM-Newton and NuSTAR observation serendipitously took place during 2021 April.
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 stacked RGS spectra from the four epochs. The 2021 April high-flux observation (blue) shows clear absorption troughs and is the subject of this paper. All the observations are binned used optimal binning (Kaastra & Bleeker 2016). The 2020 December, 2021 July, and 2021 October RGS spectra are shown in light blue, purple, and orange, respectively. These epochs are lower flux and show clear emission lines (F. Zaidouni et al. 2024, in preparation). These three observations are further binned by a factor of 3 for visualization purposes.
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 XMM-Newton EPIC-pn soft band (0.3–2 keV; top panel) and hard band (2–10 keV; middle panel) light curves in 100 s bins along with the corresponding hardness ratio (hard/soft) for the 2021 April observation. The spectrum hardens significantly at ∼60 ks, and the dotted black line delineates the division into two segments for the time-resolved analysis.
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 region around the Fe-K alpha emission line from the EPIC-pn instrument data. We overlay the best-fit model in red. There are no strong absorption features in this energy band, but we find that the data prefer a mildly ionized reflection model over a neutral reflection model (blue), particularly in Segment 2 when the spectrum is harder (see Table 2 for the parameter values).
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 O VIII Lyα from Segment 1 (t < 60 ks, red points) and Segment 2 (t > 60 ks, blue points) with the best-fitting models. This is an example of the enhanced red wing present in Segment 1 and not Segment 2.
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 evolution of key obscurer parameters between the first and second half of the observation. The top panel shows the intrinsic luminosity (absorption corrected) between 0.3 and 10 keV. The rest of the panels show the best-fitting values of the column density, ionization, and outflow velocity for each segment (values from Table 2).
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 time-averaged RGS spectrum with the best-fitting model overlaid in red. A subset of the absorption lines are labeled at their blueshifted wavelengths. The residuals are calculated as “(data-model)/error.”
Paper: Multistructured Accretion Flow of Sgr A*. II. Signatures of a Cool Accretion Disk in Hydrodynamic Simulations of Stellar Winds
Authors: Mayura Balakrishnan, Christopher M. P. Russell, Lia Corrales, Diego Calderón, Jorge Cuadra, Daryl Haggard, Sera Markoff, Joey Neilsen, Michael Nowak, Q. Daniel Wang, Frederick Baganoff
Figure caption: The top and bottom rows show the results of the disk (runtime of 3500 yr) and no-disk (runtime of 1100 yr) scenarios, respectively, for gas emitting at 6.7 keV. The plots span the central 12″ × 12″ surrounding Sgr A*, with north at the top and East to the left. Left: column density map of the region, with the cool disk of gas seen clearly in the top left panel. Middle: 6.7 keV X-ray intensity with the dark blue highlighting high levels of Fe Kα emission. Right: illustration of the velocity structure in this complex plasma, with color denoting the line-of-sight velocity corresponding to the line profile’s maximum X-ray brightness for each pixel. The grayscale overlay reflects X-ray emission intensity, i.e., dimmer regions indicate X-ray-dim gas.