adsabs/AstroCLIMB huggingface dataset:
Paper: Understanding the Magnetic Field and Plasma-β along Umbral Fan Loops Traced Using 3 Minute Slow Waves
Authors: Ananya Rawat, Girjesh Gupta, Tom Van Doorsselaere, S. Krishna Prasad, Robertus Erdélyi
Figure caption: Image of the fan loop system belonging to AR 12553 obtained from AIA 171 Å passband studied in A. Rawat & G. Gupta (2023). The yellow solid lines represent the manual tracing of coronal Loops 3, 5, and 6 as labeled, and asterisk symbols (*) represent their coronal footpoints. Small open circles represent the identified photospheric footpoints of the corresponding loops. The yellow dashed lines represent the background regions for those loops. The maroon contour indicates the umbra–penumbra boundary as obtained from the HMI continuum image.
Paper: Indication for a Compact Object Next to a LIGO–Virgo Binary Black Hole Merger
Authors: Shu-Cheng Yang, Wen-Biao Han, Hiromichi Tagawa, Song Li, Chen Zhang
Figure caption: BBH forms around a compact object and later coalesces.
Paper: JWST Coronagraphic Images of 14 Her c: A Cold Giant Planet in a Dynamically Hot Multiplanet System
Authors: Daniella C. Bardalez Gagliuffi, William O. Balmer, Laurent Pueyo, Timothy D. Brandt, Mark R. Giovinazzi, Sarah Millholland, Brennen Black, Tiger Lu, Malena Rice, James Mang, Caroline Morley, Brianna Lacy, Julien H. Girard, Elisabeth C. Matthews, Aarynn L. Carter, Brendan P. Bowler, Jacqueline K. Faherty, Clemence Fontanive, Emily Rickman
Figure caption: First direct image of 14 Her c. JWST/NIRCam coronagraphic imaging of the 14 Her system with the MASKA335R coronagraph (transmission indicated by gray shaded circles). N is up, E is left. Left: prediction for the location of 14 Her c from a reproduction of the orbits presented in G. F. Benedict et al. (2023) at the epoch of observation (MJD = 60449) and the location of the point source detected in the F444W filter. Middle: a starlight-subtracted image taken with the F200W filter (1.755–​​​​​2.227 μm), showing extended emission from a background galaxy about 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩5 SE from the host star. No other statistically significant point sources are apparent, as intended, given the cold temperature of the planet 14 Her c. Right: a starlight-subtracted image taken with the F444W filter (3.881–4.982 μm), showing extended emission from the same background galaxy and a point source at 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩1 to the SW with a contrast of 1 × 10−6. The location of the point source, detected with a contrast of 9.6 × 10−7, agrees within 1σ with the predicted location for the planet, so we conclude that we have detected 14 Her c.
Paper: JWST Coronagraphic Images of 14 Her c: A Cold Giant Planet in a Dynamically Hot Multiplanet System
Authors: Daniella C. Bardalez Gagliuffi, William O. Balmer, Laurent Pueyo, Timothy D. Brandt, Mark R. Giovinazzi, Sarah Millholland, Brennen Black, Tiger Lu, Malena Rice, James Mang, Caroline Morley, Brianna Lacy, Julien H. Girard, Elisabeth C. Matthews, Aarynn L. Carter, Brendan P. Bowler, Jacqueline K. Faherty, Clemence Fontanive, Emily Rickman
Figure caption: Sky projection of the architecture of the 14 Her system. The visual orbits for both planets are colored according to the time after the reference epoch 2020.0, MJD = 58849.0. The new NIRCam relative astrometry of 14 Her c strongly constrains the relative orientation of the two planets’ possible orbital planes.
Paper: JWST Coronagraphic Images of 14 Her c: A Cold Giant Planet in a Dynamically Hot Multiplanet System
Authors: Daniella C. Bardalez Gagliuffi, William O. Balmer, Laurent Pueyo, Timothy D. Brandt, Mark R. Giovinazzi, Sarah Millholland, Brennen Black, Tiger Lu, Malena Rice, James Mang, Caroline Morley, Brianna Lacy, Julien H. Girard, Elisabeth C. Matthews, Aarynn L. Carter, Brendan P. Bowler, Jacqueline K. Faherty, Clemence Fontanive, Emily Rickman
Figure caption: Contrast curve for the NIRCam observations of 14 Her using the 335R coronagraph. The F444W and F200W 5σ contrast curves are shown as solid and dashed lines, respectively. The likely detection of 14 Her c at ﹩\sim 1\mathop{.}\limits^{^{\prime\prime} }1﹩ is plotted as a black circle and error bar. The nominal 335R IWA, where the coronagraph transmission reaches 50%, is indicated by a vertical dashed line. Takeaway: our detection of 14 Her c is statistically significant.
Paper: Indication for a Compact Object Next to a LIGO–Virgo Binary Black Hole Merger
Authors: Shu-Cheng Yang, Wen-Biao Han, Hiromichi Tagawa, Song Li, Chen Zhang
Figure caption: Posterior distributions for intrinsic parameters (the two BH masses m1,2, their dimensionless spin magnitudes a1,2, the tilt angle between their spins and the orbital angular momentum θ1,2, the two spin vectors describing the azimuthal angle separating the spin vectors Δϕ, and the cone of precession about the system’s angular momentum ϕJL) for GW190814. The contours show the 50% and 90% credible intervals, and the vertical dashed lines mark the 90% credible intervals. Notice that the BH masses are given in the rest frame of the source. The waveform template is based on IMRPhenomXPHM.
Paper: Indication for a Compact Object Next to a LIGO–Virgo Binary Black Hole Merger
Authors: Shu-Cheng Yang, Wen-Biao Han, Hiromichi Tagawa, Song Li, Chen Zhang
Figure caption: Posterior distributions for the primary and secondary masses, luminosity distance, and LSA for GW190814. The contours show the 50% and 90% credible intervals, and the vertical dashed lines mark the median and 90% credible intervals. Notice that the BH masses are given in the rest frame of the source. The waveform template is based on IMRPhenomXPHM.
Paper: Indication for a Compact Object Next to a LIGO–Virgo Binary Black Hole Merger
Authors: Shu-Cheng Yang, Wen-Biao Han, Hiromichi Tagawa, Song Li, Chen Zhang
Figure caption: Posterior distributions for network signal-to-noise ratio of GW190814 for the isolated BBH model and the LSA model. The posterior distributions for the isolated BBH and the LSA models are shown in blue and orange, respectively. “Without HM” or “With HM” means if the waveform includes the higher multipole.
Paper: Indication for a Compact Object Next to a LIGO–Virgo Binary Black Hole Merger
Authors: Shu-Cheng Yang, Wen-Biao Han, Hiromichi Tagawa, Song Li, Chen Zhang
Figure caption: Posterior distributions for extrinsic parameters (the luminosity distance dL, the R.A., the Decl., the inclination angle between the observer line of sight and the orbital angular momentum ι, the polarization angle ψ, the phase at coalescence ϕ, the time of coalescence tc, and the LSA aL) for GW190814. The contours show the 50% and 90% credible intervals, and the vertical dashed lines mark the 90% credible intervals. The waveform template is based on IMRPhenomXPHM.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: XRISM observation of NGC 4151 on December 2 (Obs. 1). The best-fit model is shown as the red curve in both the main panel and zoom-in panel (upper right). Solid vertical lines marked the absorption/emission features for corresponding Fe states at lab values. In the zoom-in panel, the components for multiple layers of WAs and VFOs are displayed. From the furthest from to the closest to the source, the layers are labeled as pion#1 (green), pion#2 with reemission (orchid), pion#3 (blue), pion#4 (orange), and pion#6 (purple). Note that the VFO absorption features are not fully captured in the zoom-in panel; the blueshifted Fe XXVI at around 7.2 keV is visible in the main panel. The UFO component is shown in the main panel. Refer to Table 2 for parameter values.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: XRISM observation of NGC 4151 on June 22 (Obs. 5) with the best-fit model shown as red curves. From the furthest from to the closest to the source, the layers are labeled as pion#1 (green), pion#2 with reemission (orchid), pion#3 (blue), pion#4 (orange), pion#5 (navy), and pion#6 (purple). The blueshifted emission feature is shown as a cyan curve.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: XRISM observation of NGC 4151 on June 15 (Obs. 4) with the best-fit model shown as red curves. From the furthest from to the closest to the source, the layers are labeled as pion#1 (green), pion#2 with reemission (orchid), pion#3 (blue), pion#4 (orange), pion#5 (navy), and pion#6 (purple). The blueshifted emission feature is shown as a cyan curve.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: XRISM observation of NGC 4151 on December 26 (Obs. 2) with the best-fit model shown as red curves. From the furthest from to the closest to the source, the layers are labeled as pion#1 (green), pion#2 (orchid), pion#3 (blue), pion#4 (orange), and pion#6 (purple). Compared to Obs. 1, the reemission component was excluded due to a zero column density result in the fitting.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: Upper panel: five XRISM observations of NGC 4151 on December 2, December 26, May 18, June 15, and June 22, along with their respective best-fit models (colored curves) as detailed in Table 2, fitted separately in the 2.4–17.4 keV range. For better visualization, the flux of each observation is offset. The data are binned with a factor of 45 in the main panel and a factor of 15 in the zoomed panel (upper right) below 7.4 keV. Lower panel: four simultaneous NuSTAR observations in the 2–50 keV range refitted with the best model for XRISM observations with the power-law index, normalization free (colored curves). The best-fit power-law indices are within ΔΓ ≤ 0.1 and exhibit no significant deviations from the XRISM spectra.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: XRISM observation of NGC 4151 on May 18 (Obs. 3) with the best-fit model shown as red curves. From the furthest from to the closest to the source, the layers are labeled as pion#1 (green), pion#2 with reemission (orchid), pion#3 (blue), pion#4 (orange), pion#5 (navy), and pion#6 (purple).
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: The transmission profile of individual “pion” components across all five observations, calculated by dividing the full best-fit model by the model with the specified component removed. Each panel corresponds to a different “pion” component, ordered from top to bottom as pion#1, pion#2 + pionemis#2, pion#3, pion#4, pion#5, pion#6, and pionblue−emis, following the labeling in Table 2.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: Schematic representation of the multilayer outflow model for five XRISM/Resolve observations of NGC 4151. The model consists of absorbers and emitters that create complex combinations of absorption and emission features. The absorbers are composed of up to four layers of WAs or VFOs, along with two UFO layers. Color-coded solid and dashed boxes indicate the presence of specific outflow components with strong (σ >= 3) and weak (σ < 3) DS in different observations. Emitters include reemission from WA component #2 and a blueshifted emission feature.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: SED models for the five NGC 4151 observations, each including a low- and high-energy cutoff power law and a blackbody component.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: Left panel: comparison of the estimated minimum launching radius (﹩{r}_{{\rm{\min }}}﹩ in Equation (5), derived from the escape velocity condition) and the maximum launching radius (﹩{r}_{{\rm{\max }}}﹩ in Equation (4), constrained by the ionization parameter) for each outflow layer. The dashed line represents the equality line (﹩{r}_{{\rm{\min }}}={r}_{{\rm{\max }}}﹩). Right panel: minimum volume filling factor ﹩{f}_{{v}_{{\rm{\min }}}}﹩ as a function of ﹩{r}_{{\rm{\min }}}﹩. The shaded region represents the estimated radius for the inner wall of the torus from XRISM Collaboration et al. (2024). The red circles represent WAs, blue triangles correspond to VFOs, and green stars indicate UFOs. The transparent red circles show corrected WA values, incorporating the minimum required inclination angle to bring fv below unity. The corresponding minimum angles are plotted on the secondary y-axis in the right panel. The gray data points represent outflows with low DS σ < 3.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: Upper left panel: mass outflow rate per volume filling factor (﹩\dot{M}﹩) as a function of radial velocity (vz) along the line of sight. Because of the large uncertainty in the volume filling factor compared with the propagated statistical uncertainties from the outflow parameters, we do not include the error bar. The solid horizontal line represents the Eddington accretion rate (﹩{\dot{M}}_{\mathrm{Edd}}﹩). The dotted lines in the shaded region represent the mass accretion rate (﹩{\dot{M}}_{\mathrm{acc}}﹩) for five observations. The red circles, blue triangles, and green stars correspond to WAs, VFOs, and UFOs, respectively. The transparent markers represent values accounting for the minimum volume filling factor for VFOs and UFOs estimated in the right panel of Figure 14. The gray data points represent outflows with low DS σ < 3. Lower left panel: kinetic power (﹩{\dot{E}}_{k}﹩) as a function of radial velocity. The solid, dashed, and dashed–dotted horizontal lines mark the Eddington luminosity (LEdd) and 5% and 0.5% of the Eddington luminosity, respectively. The dotted lines in the shaded region represent the bolometric luminosities (Lbol). Most UFOs and VFOs exceed the 0.5% threshold of LEdd.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: Heat maps show the variability of four outflow parameters across five observations for up to six outflow components normalized differently by the mean values for each outflow type. The four panels display column densities NH (upper left), ionization parameters ﹩{\mathrm{log}}\,\xi ﹩ (upper right), turbulence velocities σv (lower left), and velocities along our line of sight vz (lower right). The markers in the center represent different types: circles for WAs, triangles for VFOs, and stars for UFOs. The open markers indicate components with low DS σ < 3.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: The values of four outflow parameters and ionization luminosities as a function of time (MJD) for different outflow types (red circles for WAs, blue triangles for VFOs, green stars for UFOs). Open data points indicate components with low DS (σ < 3). The black squares in the top and bottom panels represent the sum of the column densities NH and the total ionizing luminosity for each observation. The ionization luminosity seen by each component is calculated by multiplying the lixi output from pion by its corresponding value of ξ.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: The relation between column density NH and ionization parameter ξ, giving the AMD of the outflow components. The best-fit lines for different types of outflows (red dots for WAs, blue triangles for VFOs, and green stars for UFOs) are shown, with shaded regions indicating the 1σ confidence level. The best-fit slope m and the corresponding density profile index α with their 1σ uncertainties are presented in the legend. The right panel presents results excluding outflows with DS below 3σ.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: The measured wind velocity along the line of sight (vz) as a function of ionization parameters (ξ) for different wind types (WAs, VFOs, UFOs). The best-fit lines and their slopes m for different types of outflows are shown, with shaded regions indicating the 1σ confidence levels. The right panel excludes the outflows with DS below 3σ.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: The values of column densities (upper panel) and ionization parameters (lower panel) as a function of ionization luminosity seen by each component for different outflow types (circles for WAs, triangles for VFOs, stars for UFOs). Open data points indicate components with low DS (σ < 3).
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: XRISM observation of NGC 4151 on June 15 (Obs. 4) fitted with two different xillver models with ξ = 0 (green curve) and ξ = 200 (blue curve) with a broadband view of 2.4–17.4 keV (left) and a zoom-in view of 5.4–10.4 keV (right). For comparison, the best-fit model with UFO components is shown as a red curve. The lower panels show the residuals ((data – model)/model) for different models. Both xillver models left strong residuals near 8 keV.
Paper: XRISM Spectroscopy of Accretion-driven Wind Feedback in NGC 4151
Authors: Xin Xiang, Jon M. Miller, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Margaret Buhariwalla, Doyee Byun, Chris Done, Luigi Gallo, Dimitra Gerolymatou, Scott Hagen, Jelle Kaastra, Stephane Paltani, Frederick S. Porter, Richard Mushotzky, Hirofumi Noda, Missagh Mehdipour, Takeo Minezaki, Makoto Tashiro, Abderahmen Zoghbi
Figure caption: Comparison of the outflow momentum rate (﹩{\dot{p}}_{\mathrm{out}}﹩) and the momentum flux of the radiation field (﹩{\dot{p}}_{\mathrm{rad}}﹩). The solid and dashed lines show the ratio of the two being 1 and 10, respectively. The transparent markers represent values multiplied by the lower limit of the volume filling factor.