adsabs/AstroCLIMB huggingface dataset:
Paper: A JWST Survey of the Supernova Remnant Cassiopeia A
Authors: Dan Milisavljevic, Tea Temim, Ilse De Looze, Danielle Dickinson, J. Martin Laming, Robert Fesen, John C. Raymond, Richard G. Arendt, Jacco Vink, Bettina Posselt, George G. Pavlov, Ori D. Fox, Ethan Pinarski, Bhagya Subrayan, Judy Schmidt, William P. Blair, Armin Rest, Daniel Patnaude, Bon-Chul Koo, Jeonghee Rho, Salvatore Orlando, Hans-Thomas Janka, Moira Andrews, Michael J. Barlow, Adam Burrows, Roger Chevalier, Geoffrey Clayton, Claes Fransson, Christopher Fryer, Haley L. Gomez, Florian Kirchschlager, Jae-Joon Lee, Mikako Matsuura, Maria Niculescu-Duvaz, Justin D. R. Pierel, Paul P. Plucinsky, Felix D. Priestley, Aravind P. Ravi, Nina S. Sartorio, Franziska Schmidt, Melissa Shahbandeh, Patrick Slane, Nathan Smith, Niharika Sravan, Kathryn Weil, Roger Wesson, J. Craig Wheeler
Figure caption: MIRI/MRS spectra obtained as part of the survey. P1 and P3 were selected to sample two shocked ejecta knots of different compositions. P4 represents a “core sample” of unshocked ejecta through the interior of the remnant, and P2 was selected to help diagnose the emission arising in the Green Monster (see Section 3.2). All spaxels of the overlapping FOVs across all four channels have been integrated. Positions with respect to Cas A are shown and labeled in Figure 3. Dominant emission lines from the ejecta are labeled. Bandpasses of the MIRI filters are overlaid with throughputs normalized to arbitrary units. Many of the same emission lines are seen at all four positions, but offsets due to velocity are evident. Dust emission features (listed in Table 1) are seen at all positions with varying intensities and described in more detail in Section 4.1. Note the large dynamic range on the vertical axis.
Paper: A JWST Survey of the Supernova Remnant Cassiopeia A
Authors: Dan Milisavljevic, Tea Temim, Ilse De Looze, Danielle Dickinson, J. Martin Laming, Robert Fesen, John C. Raymond, Richard G. Arendt, Jacco Vink, Bettina Posselt, George G. Pavlov, Ori D. Fox, Ethan Pinarski, Bhagya Subrayan, Judy Schmidt, William P. Blair, Armin Rest, Daniel Patnaude, Bon-Chul Koo, Jeonghee Rho, Salvatore Orlando, Hans-Thomas Janka, Moira Andrews, Michael J. Barlow, Adam Burrows, Roger Chevalier, Geoffrey Clayton, Claes Fransson, Christopher Fryer, Haley L. Gomez, Florian Kirchschlager, Jae-Joon Lee, Mikako Matsuura, Maria Niculescu-Duvaz, Justin D. R. Pierel, Paul P. Plucinsky, Felix D. Priestley, Aravind P. Ravi, Nina S. Sartorio, Franziska Schmidt, Melissa Shahbandeh, Patrick Slane, Nathan Smith, Niharika Sravan, Kathryn Weil, Roger Wesson, J. Craig Wheeler
Figure caption: Top: the NIRCam F356W image compared to a VLA S-band image from 2012 (courtesy of T. DeLaney). Bottom: the left panel shows a composite image made using the NuSTAR 44Ti map (Grefenstette et al. 2014), the Chandra 1 Ms X-ray image of Cas A (Hwang et al. 2004), and our MIRI F1280W image. The location of the NS (Fesen et al. 2006b) is marked with a black circle. The right panel shows a composite image combining our unshocked ejecta map (see Section 4.2) with the NuSTAR 44Ti map and a Chandra Fe-K map (energy ∼6.7 keV). The locations of the center of expansion (COE; Thorstensen et al. 2001) and the NS are marked with white and black circles, respectively.
Paper: A JWST Survey of the Supernova Remnant Cassiopeia A
Authors: Dan Milisavljevic, Tea Temim, Ilse De Looze, Danielle Dickinson, J. Martin Laming, Robert Fesen, John C. Raymond, Richard G. Arendt, Jacco Vink, Bettina Posselt, George G. Pavlov, Ori D. Fox, Ethan Pinarski, Bhagya Subrayan, Judy Schmidt, William P. Blair, Armin Rest, Daniel Patnaude, Bon-Chul Koo, Jeonghee Rho, Salvatore Orlando, Hans-Thomas Janka, Moira Andrews, Michael J. Barlow, Adam Burrows, Roger Chevalier, Geoffrey Clayton, Claes Fransson, Christopher Fryer, Haley L. Gomez, Florian Kirchschlager, Jae-Joon Lee, Mikako Matsuura, Maria Niculescu-Duvaz, Justin D. R. Pierel, Paul P. Plucinsky, Felix D. Priestley, Aravind P. Ravi, Nina S. Sartorio, Franziska Schmidt, Melissa Shahbandeh, Patrick Slane, Nathan Smith, Niharika Sravan, Kathryn Weil, Roger Wesson, J. Craig Wheeler
Figure caption: Mapping unshocked ejecta of Cas A. Top: image resulting after subtraction of a scaled version of the F2100W filter from F2550W and masking main shell emission (which appears as black). The emission inside the main shell is mostly due to [O IV] 25.89 μm from unshocked oxygen material, with potential minor contributions from cold dust, line emission from filaments of shocked oxygen ejecta, and line emission from other shocked/unshocked material including iron. The dashed box indicates the region enlarged in the right panel, and the labeled boxes identify MIRI/MRS IFU regions. Bottom: a 3D reconstruction of the MIRI/MRS [O IV] 25.89 μm emission from P2 and P4 as a function of velocity showing the wide spread of the ejecta in velocity space. Emission >3σ above the continuum level is represented.
Paper: A JWST Survey of the Supernova Remnant Cassiopeia A
Authors: Dan Milisavljevic, Tea Temim, Ilse De Looze, Danielle Dickinson, J. Martin Laming, Robert Fesen, John C. Raymond, Richard G. Arendt, Jacco Vink, Bettina Posselt, George G. Pavlov, Ori D. Fox, Ethan Pinarski, Bhagya Subrayan, Judy Schmidt, William P. Blair, Armin Rest, Daniel Patnaude, Bon-Chul Koo, Jeonghee Rho, Salvatore Orlando, Hans-Thomas Janka, Moira Andrews, Michael J. Barlow, Adam Burrows, Roger Chevalier, Geoffrey Clayton, Claes Fransson, Christopher Fryer, Haley L. Gomez, Florian Kirchschlager, Jae-Joon Lee, Mikako Matsuura, Maria Niculescu-Duvaz, Justin D. R. Pierel, Paul P. Plucinsky, Felix D. Priestley, Aravind P. Ravi, Nina S. Sartorio, Franziska Schmidt, Melissa Shahbandeh, Patrick Slane, Nathan Smith, Niharika Sravan, Kathryn Weil, Roger Wesson, J. Craig Wheeler
Figure caption: Examples of light echoes around Cas A. The top panel shows an enlarged section of the largest IR echo identified in the middle panels as E1. Comparison of our NIRCam F356W image with archival Spitzer IRAC observations (center) shows that the emission was not present in the past. The boxed region E2 highlights an area where multiple epochs of MIRI observations are available and the time variability of the light echoes can be tracked; this region is enlarged in the bottom two panels. In the bottom right panel, sources with negligible proper motion between the 109 days separating the MIRI F770W observations appear white, whereas light echoes appear as red and teal between the first and second observation. The astrometric shift observed in the emission between the two epochs is associated with apparent velocities between 0.3c and 0.6c, which are too large to be motion of SN ejecta.
Paper: A JWST Survey of the Supernova Remnant Cassiopeia A
Authors: Dan Milisavljevic, Tea Temim, Ilse De Looze, Danielle Dickinson, J. Martin Laming, Robert Fesen, John C. Raymond, Richard G. Arendt, Jacco Vink, Bettina Posselt, George G. Pavlov, Ori D. Fox, Ethan Pinarski, Bhagya Subrayan, Judy Schmidt, William P. Blair, Armin Rest, Daniel Patnaude, Bon-Chul Koo, Jeonghee Rho, Salvatore Orlando, Hans-Thomas Janka, Moira Andrews, Michael J. Barlow, Adam Burrows, Roger Chevalier, Geoffrey Clayton, Claes Fransson, Christopher Fryer, Haley L. Gomez, Florian Kirchschlager, Jae-Joon Lee, Mikako Matsuura, Maria Niculescu-Duvaz, Justin D. R. Pierel, Paul P. Plucinsky, Felix D. Priestley, Aravind P. Ravi, Nina S. Sartorio, Franziska Schmidt, Melissa Shahbandeh, Patrick Slane, Nathan Smith, Niharika Sravan, Kathryn Weil, Roger Wesson, J. Craig Wheeler
Figure caption: Composite images of our NIRCam (top) and MIRI (bottom) mosaics obtained as part of our JWST survey of Cas A. FOVs have been subtly cropped, and minor corrections have been made to compensate for gaps in coverage. Corners not imaged by JWST have been filled in with archival Spitzer data at comparable wavelengths. Mosaics of all individual filters showing the entire FOVs are shown in the Appendix.
Paper: A JWST Survey of the Supernova Remnant Cassiopeia A
Authors: Dan Milisavljevic, Tea Temim, Ilse De Looze, Danielle Dickinson, J. Martin Laming, Robert Fesen, John C. Raymond, Richard G. Arendt, Jacco Vink, Bettina Posselt, George G. Pavlov, Ori D. Fox, Ethan Pinarski, Bhagya Subrayan, Judy Schmidt, William P. Blair, Armin Rest, Daniel Patnaude, Bon-Chul Koo, Jeonghee Rho, Salvatore Orlando, Hans-Thomas Janka, Moira Andrews, Michael J. Barlow, Adam Burrows, Roger Chevalier, Geoffrey Clayton, Claes Fransson, Christopher Fryer, Haley L. Gomez, Florian Kirchschlager, Jae-Joon Lee, Mikako Matsuura, Maria Niculescu-Duvaz, Justin D. R. Pierel, Paul P. Plucinsky, Felix D. Priestley, Aravind P. Ravi, Nina S. Sartorio, Franziska Schmidt, Melissa Shahbandeh, Patrick Slane, Nathan Smith, Niharika Sravan, Kathryn Weil, Roger Wesson, J. Craig Wheeler
Figure caption: The JWST 3σ upper limits in the NIR (NIRCam F162M, F356W, F444W) at the location of the Cas A CCO and the CCO’s X-ray spectrum detected with Chandra ACIS. Power-law spectra consistent with JWST upper limits and an example blackbody spectrum with a temperature of 900 K are plotted for an extinction of A  V  = 8, using the extinction curve by Gordon et al. (2023). The Chandra ACIS X-ray data are from Posselt & Pavlov (2018), the HST optical and NIR limits are from Fesen et al. (2006b), and the Spitzer limits are from Wang et al. (2007).
Paper: A JWST Survey of the Supernova Remnant Cassiopeia A
Authors: Dan Milisavljevic, Tea Temim, Ilse De Looze, Danielle Dickinson, J. Martin Laming, Robert Fesen, John C. Raymond, Richard G. Arendt, Jacco Vink, Bettina Posselt, George G. Pavlov, Ori D. Fox, Ethan Pinarski, Bhagya Subrayan, Judy Schmidt, William P. Blair, Armin Rest, Daniel Patnaude, Bon-Chul Koo, Jeonghee Rho, Salvatore Orlando, Hans-Thomas Janka, Moira Andrews, Michael J. Barlow, Adam Burrows, Roger Chevalier, Geoffrey Clayton, Claes Fransson, Christopher Fryer, Haley L. Gomez, Florian Kirchschlager, Jae-Joon Lee, Mikako Matsuura, Maria Niculescu-Duvaz, Justin D. R. Pierel, Paul P. Plucinsky, Felix D. Priestley, Aravind P. Ravi, Nina S. Sartorio, Franziska Schmidt, Melissa Shahbandeh, Patrick Slane, Nathan Smith, Niharika Sravan, Kathryn Weil, Roger Wesson, J. Craig Wheeler
Figure caption: Three NIRCam imaging mosaics obtained as part of our Cas A survey. The F162M filter was used as the SW channel for both the F356W and F444W observations, so the exposure time is twice as long. Gaps are seen in the F162M mosaic because of the dithering three-point pattern that prioritized the LW filters and introduced gaps in the SW channel detectors. The images have the same angular scale and orientation, and the intensity scale is in units of MJy sr−1. In the color version at lower right, the blue, green, and red show the images in increasing wavelength, respectively. The approximate footprint of the MIRI mosaics is shown.
Paper: A JWST Survey of the Supernova Remnant Cassiopeia A
Authors: Dan Milisavljevic, Tea Temim, Ilse De Looze, Danielle Dickinson, J. Martin Laming, Robert Fesen, John C. Raymond, Richard G. Arendt, Jacco Vink, Bettina Posselt, George G. Pavlov, Ori D. Fox, Ethan Pinarski, Bhagya Subrayan, Judy Schmidt, William P. Blair, Armin Rest, Daniel Patnaude, Bon-Chul Koo, Jeonghee Rho, Salvatore Orlando, Hans-Thomas Janka, Moira Andrews, Michael J. Barlow, Adam Burrows, Roger Chevalier, Geoffrey Clayton, Claes Fransson, Christopher Fryer, Haley L. Gomez, Florian Kirchschlager, Jae-Joon Lee, Mikako Matsuura, Maria Niculescu-Duvaz, Justin D. R. Pierel, Paul P. Plucinsky, Felix D. Priestley, Aravind P. Ravi, Nina S. Sartorio, Franziska Schmidt, Melissa Shahbandeh, Patrick Slane, Nathan Smith, Niharika Sravan, Kathryn Weil, Roger Wesson, J. Craig Wheeler
Figure caption: The four shorter-wavelength MIRI imaging mosaics obtained as part of the survey. The full spatial coverage (including the Lyot coronagraph) is shown. The common angular scale and orientation are shown in the upper left panel. Color bars depict the intensity scale that has units of MJy sr−1.
Paper: A JWST Survey of the Supernova Remnant Cassiopeia A
Authors: Dan Milisavljevic, Tea Temim, Ilse De Looze, Danielle Dickinson, J. Martin Laming, Robert Fesen, John C. Raymond, Richard G. Arendt, Jacco Vink, Bettina Posselt, George G. Pavlov, Ori D. Fox, Ethan Pinarski, Bhagya Subrayan, Judy Schmidt, William P. Blair, Armin Rest, Daniel Patnaude, Bon-Chul Koo, Jeonghee Rho, Salvatore Orlando, Hans-Thomas Janka, Moira Andrews, Michael J. Barlow, Adam Burrows, Roger Chevalier, Geoffrey Clayton, Claes Fransson, Christopher Fryer, Haley L. Gomez, Florian Kirchschlager, Jae-Joon Lee, Mikako Matsuura, Maria Niculescu-Duvaz, Justin D. R. Pierel, Paul P. Plucinsky, Felix D. Priestley, Aravind P. Ravi, Nina S. Sartorio, Franziska Schmidt, Melissa Shahbandeh, Patrick Slane, Nathan Smith, Niharika Sravan, Kathryn Weil, Roger Wesson, J. Craig Wheeler
Figure caption: Same as Figure A2 except showing the four longer-wavelength MIRI imaging mosaics.
Paper: Discovery of Merging Twin Quasars at z = 6.05
Authors: Yoshiki Matsuoka, Takuma Izumi, Masafusa Onoue, Michael A. Strauss, Kazushi Iwasawa, Nobunari Kashikawa, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Masatoshi Imanishi, Rikako Ishimoto, Toshihiro Kawaguchi, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, John D. Silverman, Yoshiki Toba
Figure caption: FOCAS z-band (left) and y-band (right) images around the two quasars, obtained under seeing conditions of 0.″4–0.″6. North is up and east to the left. The scale bars represent 1″. The boxes represent the regions used to calculate the S/N of the bridging emission (signal in the “bridge” box and noise in the “blank” boxes).
Paper: Discovery of Merging Twin Quasars at z = 6.05
Authors: Yoshiki Matsuoka, Takuma Izumi, Masafusa Onoue, Michael A. Strauss, Kazushi Iwasawa, Nobunari Kashikawa, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Masatoshi Imanishi, Rikako Ishimoto, Toshihiro Kawaguchi, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, John D. Silverman, Yoshiki Toba
Figure caption: Upper panels: FOCAS spectra of C1 (top) and C2 (middle) created by stacking all available data, along with a sky spectrum as a guide to the expected noise (bottom). The dotted lines represent the expected positions of Lyα and N V λ1240 emission lines, as well as interstellar absorption lines of Si II λ1260, Si II λ1304, and C II λ1335, given the redshift of z Lyα  = 6.053. An unidentified line at λ obs = 9082 Å in C1 (see the main text) is marked by an arrow. Lower panels: continuum subtracted spectra of C1 (left) and C2 (right) around Lyα. The thick red lines represent the best-fit models, while the thin red lines (only in C1) represent their broad and narrow components. The spectral window used for the fitting (λ obs = 8576–8615 Å) is shown by the vertical dashed lines. The gray shaded area marks the wavelength range affected by strong sky emission. The spectra in both upper and lower panels were smoothed using inverse-variance-weighted means over 3 pixels, for display purposes.
Paper: Discovery of Merging Twin Quasars at z = 6.05
Authors: Yoshiki Matsuoka, Takuma Izumi, Masafusa Onoue, Michael A. Strauss, Kazushi Iwasawa, Nobunari Kashikawa, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Masatoshi Imanishi, Rikako Ishimoto, Toshihiro Kawaguchi, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, John D. Silverman, Yoshiki Toba
Figure caption: Top: three-color (HSC r-, i-, and z-band) composite image around C1 and C2, the two reddest sources at the center. North is up and east to the left, and the image size is approximately 90″ × 25″. The limiting magnitude for point sources is ∼26. The inset shows an expanded view of C1 and C2, with the thin dotted lines representing a 1.″0 slitlet used for FOCAS spectroscopy. Bottom: two-dimensional FOCAS spectrum of C1 (upper trace of light) and C2 (lower trace), created by stacking all available data.
Paper: Discovery of Merging Twin Quasars at z = 6.05
Authors: Yoshiki Matsuoka, Takuma Izumi, Masafusa Onoue, Michael A. Strauss, Kazushi Iwasawa, Nobunari Kashikawa, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Masatoshi Imanishi, Rikako Ishimoto, Toshihiro Kawaguchi, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, John D. Silverman, Yoshiki Toba
Figure caption: Close-up view of the two-dimensional Lyα spectra of C1 (upper trace, at ∼22 kpc) and C2 (lower trace, at ∼10 kpc). The left panel displays the stacked data of all available exposures, totaling 370 minutes (i.e., an enlarged view of Figure 1). The white boxes represent the regions used to calculate the S/N of the bridging emission (signal in the “bridge” box and noise in the “blank” boxes). The right panel displays a single 20 minute exposure taken under the best-seeing condition (∼0″4), which reveals a spatially resolved Lyα profile in C2. The angular distance of 1″ corresponds to 5.7 kpc at the source redshift.
Paper: Discovery of Merging Twin Quasars at z = 6.05
Authors: Yoshiki Matsuoka, Takuma Izumi, Masafusa Onoue, Michael A. Strauss, Kazushi Iwasawa, Nobunari Kashikawa, Masayuki Akiyama, Kentaro Aoki, Junya Arita, Masatoshi Imanishi, Rikako Ishimoto, Toshihiro Kawaguchi, Kotaro Kohno, Chien-Hsiu Lee, Tohru Nagao, John D. Silverman, Yoshiki Toba
Figure caption: GNIRS spectra of C1 (top) and C2 (middle) created by stacking all available data, along with the error spectrum dominated by the sky background (bottom). The vertical lines represent the expected positions of Lyα, N V λ1240, C IV λ1549, C III] λ1906, and Mg II λ2800, given the redshift of z Lyα  = 6.053. The spectra were smoothed using inverse-variance-weighted means over 9 pixels, for display purposes.
Paper: Discovery of Thionylimide, HNSO, in Space: The first N-, S-, and O-bearing Interstellar Molecule
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Holger S. P. Müller, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Belén Tercero, Pablo de Vicente, David San Andrés, Sergio Martín, Miguel A. Requena-Torres
Figure caption: Transitions of HNSO identified toward the GC molecular cloud G + 0.6930.027 (listed in Table 1) sorted by decreasing peak intensity. The result of the best LTE fit of HNSO is plotted with a red line, and the blue line depicts the emission from all the molecules identified to date in our survey, including HNSO (observed spectra shown as gray histograms). The structure of HNSO is also shown (nitrogen atom in blue; oxygen atom in red, sulfur atom in yellow, and hydrogen atom in white).
Paper: Discovery of Thionylimide, HNSO, in Space: The first N-, S-, and O-bearing Interstellar Molecule
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Holger S. P. Müller, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Belén Tercero, Pablo de Vicente, David San Andrés, Sergio Martín, Miguel A. Requena-Torres
Figure caption: Suggested chemical routes for the formation of HNSO in the ISM. We show in blue molecules that have been identified toward G + 0.693 and in yellow molecules that have not been searched for toward G + 0.693 because spectroscopy is not available (NSO). Surface reactions are shown in black solid lines, while gas-phase reactions are depicted with dashed arrows.
Paper: Discovery of Thionylimide, HNSO, in Space: The first N-, S-, and O-bearing Interstellar Molecule
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Holger S. P. Müller, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Belén Tercero, Pablo de Vicente, David San Andrés, Sergio Martín, Miguel A. Requena-Torres
Figure caption: Unblended or slightly blended transitions of SO2 detected toward G + 0.693 molecular cloud (listed in Table C1). The result of the best LTE fit is shown with a red solid line, while the blue line shows the expected molecular emission from all the molecular species identified to date in our survey. The observed spectra are plotted as gray histograms.
Paper: Discovery of Thionylimide, HNSO, in Space: The first N-, S-, and O-bearing Interstellar Molecule
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Holger S. P. Müller, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Belén Tercero, Pablo de Vicente, David San Andrés, Sergio Martín, Miguel A. Requena-Torres
Figure caption: Unblended or slightly blended transitions of NS detected toward G + 0.693 molecular cloud (listed in Table C1). The result of the best LTE fit is shown with a red solid line, while the blue line shows the expected molecular emission from all the molecular species identified to date in our survey. The observed spectra are plotted as gray histograms.
Paper: Discovery of Thionylimide, HNSO, in Space: The first N-, S-, and O-bearing Interstellar Molecule
Authors: Miguel Sanz-Novo, Víctor M. Rivilla, Holger S. P. Müller, Izaskun Jiménez-Serra, Jesús Martín-Pintado, Laura Colzi, Shaoshan Zeng, Andrés Megías, Álvaro López-Gallifa, Antonio Martínez-Henares, Belén Tercero, Pablo de Vicente, David San Andrés, Sergio Martín, Miguel A. Requena-Torres
Figure caption: Rotational diagram of HNSO toward G + 0.693 (blue dots, including 1σ errors). The best linear fit to the data points is depicted using a gray dotted line. The derived values for the molecular column density, N, and the excitation temperature, T ex, are shown in blue.
Paper: Simulating X-Ray Reverberation in the Ultraviolet-emitting Regions of Active Galactic Nuclei Accretion Disks with Three-dimensional Multifrequency Radiation Magnetohydrodynamic Simulations
Authors: Amy Secunda, Yan-Fei Jiang, 燕飞 姜, Jenny E. Greene
Figure caption: Top panels compare the intrinsic and reprocessed UV light curves that come from the one- and two-frequency runs, respectively. Middle and bottom panels compare the reprocessed UV light curves and injected X-rays from the two-frequency runs. τ damp = 30 days for the injected X-ray light curve in the left panels (Run A) and τ damp = 0.1 day for the injected X-ray light curve in the right panels (Run B). In the bottom right panel, the X-ray light curve has been window averaged over 2 days for easier comparison. To make each UV light curve, we sum the total outgoing flux from the low-frequency group over every cell at the top and bottom of the simulation box. For easier comparison, we scale the flux, F, by the standard deviation of the flux, σ(F), and then subtract off the minimum flux for each light curve. Time zero corresponds to when we start injecting the X-rays. Note that because X-rays are injected directly into the simulation, there will be no lag between the X-ray and UV light curves from the light-travel time.
Paper: Simulating X-Ray Reverberation in the Ultraviolet-emitting Regions of Active Galactic Nuclei Accretion Disks with Three-dimensional Multifrequency Radiation Magnetohydrodynamic Simulations
Authors: Amy Secunda, Yan-Fei Jiang, 燕飞 姜, Jenny E. Greene
Figure caption: Top-right panel: schematic of our simulation and spacetime diagram of the gas temperature in the one- and two-frequency simulations in the regions left and right of the gray line, respectively. The red arrows represent the time-varying X-ray radiation we inject in the upper and lower boundaries in our two-frequency simualtions. Middle right panel: spacetime diagram of the gas density in the one- and two-frequency simulations in the regions left and right of the gray line, respectively. Bottom right panel: same as middle panel but for the radiation energy. We show the UV radiation energy above the midplane and the X-ray radiation energy below the midplane. In all panels, the solid white line is z(τ UV = 1) ≈ z(τ XR = 1), and the dashed white line is z(τ  a,UV = 1). τ  a,XR < 1 throughout our simulation. Left panels: horizontally and time-averaged vertical profiles of gas temperature, density, and turbulent velocity in the top, middle, and bottom panels, respectively, for our two-frequency simulation. All figures are for Run A.