adsabs/AstroCLIMB huggingface dataset:
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: Left panel: E  p,i –E iso diagram of GRB 200613A (yellow star). Blue and red points represent LGRBs and SGRBs, respectively. Right panel: E  p –T 90 diagram of GRB 200613A (yellow star). The color indicates the probability of being SGRB, with red being 100% SGRB and blue being 100% LGRB.
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: Multiband afterglow light curve of GRB 200613A spanning a temporal range of 0.5–16.25 days post-burst. Solid (hollow) green data points represent R(r) band observations. The inverted triangle denotes the limiting magnitude. For convenience, we added offsets in fluxes as shown in the legend. Note that the data are not corrected for the Galactic extinctions and the host galaxy contribution.
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: Left panel: CCF vs. time delay between the (100–150)/(1 + z) keV and (200–250)/(1 + z) keV channels for the main pulse. The error in each bin of the CCF is determined by running the Monte Carlo simulation 1000 times. The blue solid line shows a Gaussian fit. The time delay corresponding to the peak of the Gaussian fit determines the spectral lag. Right panel: histogram of 1000 simulated spectral lag values for the main pulse between (100–150)/(1 + z) keV and (200–250)/(1 + z) keV. The standard deviation of this simulated spectral lag distribution is considered as its associated uncertainty. The derived spectral lag of the main pulse is 607.6 ± 57.8 ms.
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: BZ power ﹩{\dot{E}}_{{\rm{B}}}﹩ (blue lines) and neutrino annihilation power ﹩{\dot{E}}_{\nu \bar{\nu }}﹩ (red lines) as a function of the accretion rate ﹩\dot{m}﹩ for different BH spins a • = 0.01 (thick solid lines) and 0.9 (dashed lines). We adopt a BH mass of m • = 3. The same results can also be found in Lei et al. (2017).
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: SED of the host galaxy of GRB 200613A. The best-fit model SED is shown in the red line, and the slit-corrected observed GTC spectrum is shown in the blue line. The model photometry results are marked as squares, and the sky-survey results are represented by black data points. The g-, r-, and z-band magnitudes were adopted from the LS rather than SDSS due to higher S/N. All the data are corrected for the Galactic extinctions.
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: Best-fit PyFRS afterglow model light curve of GRB 200613A (solid lines). All optical data plots in this figure are subtracted by the host galaxy flux, with u- and i-band estimates from SDSS and g- and r-band estimates from LS (Table 4). For convenience, we added offsets in fluxes as shown in the legend.
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: Posterior probability distributions of the host galaxy parameters of GRB 200613A.
Paper: Unveiling the Multifaceted GRB 200613A: Prompt Emission Dynamics, Afterglow Evolution, and the Host Galaxy’s Properties
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, D. Alexander Kann, Christina C. Thöne, José Feliciano Agüí Fernández, Yi Shuang-Xi, Wei Xie, Yuan-Chuan Zou, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Jie Zheng, Qing-Wen Tang, Peng-Wei Zhao, Li-Ping Xin, Jian-Yan Wei
Figure caption: Posterior probability distributions of the afterglow parameters of GRB 200613A.
Paper: Molecular Distribution in the Central Region of M87
Authors: Mahitosh Ray, Chorng-Yuan Hwang
Figure caption: Top left: continuum-subtracted absorption spectrum of the CO(1–0) toward the center of M87, standard deviation (σ) = 0.0012 Jy, fitted with Lorentzian. Dashed line at the center shows the systemic velocity (sys. vel.) of the galaxy. Top right: continuum-subtracted absorption spectrum of the CO(2–1) toward the center of M87, σ = 0.0015 Jy, fitted with Lorentzian. Bottom: CO(2–1) overlapped with the CO(1–0) showing the position of the absorption feature; the subplot inside the figure provides a magnified view of the absorption feature.
Paper: Molecular Distribution in the Central Region of M87
Authors: Mahitosh Ray, Chorng-Yuan Hwang
Figure caption: Left: CO(1–0) integrated intensity map with 3σ cutoff showing the distribution of the gas toward the nucleus with a maximum integrated intensity = 3.02 Jy beam−1 km s−1 and σ = 0.18 Jy beam−1 km s−1. The green dashed lines indicates continuum contours at relative contour levels of 0.2, 0.4, 0.6, and 0.8 on the CO(1–0) map. Right: CO(1–0) velocity map with intensity greater than 5σ showing the velocity distribution of the gas toward the nucleus. The black contours indicate CO(1–0) position at relative contour levels of 0.2, 0.4, 0.6, and 0.8 of the peak.
Paper: Molecular Distribution in the Central Region of M87
Authors: Mahitosh Ray, Chorng-Yuan Hwang
Figure caption: Left: CO(1–0) channel maps at different velocities. The rms of the pixel values in the images is 0.0007 Jy beam−1. Right: CO(2–1) channel maps at different velocities. The rms of the pixel values in the images is 0.002 Jy beam−1.
Paper: Molecular Distribution in the Central Region of M87
Authors: Mahitosh Ray, Chorng-Yuan Hwang
Figure caption: Continuum image at 114.79 GHz of nucleus and jet of M87.
Paper: Where Have All the Sulfur Atoms Gone? Polycyclic Aromatic Hydrocarbon as a Possible Sink for the Missing Sulfur in the Interstellar Medium. I. The C–S Band Strengths
Authors: X. J. Yang, Lijun Hua, Aigen Li
Figure caption: Calculated spectra of BT (left panel) and BT+ (right panel). The origins of the main features are labeled, including C–H, C–C, and C–S bonds. The frequencies of the calculated spectra are scaled with a factor 0.9688, and an FWHM of 16 cm−1 is assigned.
Paper: Where Have All the Sulfur Atoms Gone? Polycyclic Aromatic Hydrocarbon as a Possible Sink for the Missing Sulfur in the Interstellar Medium. I. The C–S Band Strengths
Authors: X. J. Yang, Lijun Hua, Aigen Li
Figure caption: Calculated spectra of all the target molecules (left panel; see Figure 2) and their cations (right panel). The wavelength ranges for the main vibrational bands are marked on top.
Paper: Where Have All the Sulfur Atoms Gone? Polycyclic Aromatic Hydrocarbon as a Possible Sink for the Missing Sulfur in the Interstellar Medium. I. The C–S Band Strengths
Authors: X. J. Yang, Lijun Hua, Aigen Li
Figure caption: Comparison of the experimental (black solid lines) and calculational (red solid lines) spectra for BT (upper panel), DBT (middle), and TT (bottom). The experimental spectra are taken from the NIST webbook. The frequencies of the calculated spectra are scaled with a factor of 0.9688, and an FWHM of 16 cm−1 is assigned. For comparison, both the experimental and calculated spectra are normalized to their maxima due to the lack of experimental information on the intensities of these molecules.
Paper: Where Have All the Sulfur Atoms Gone? Polycyclic Aromatic Hydrocarbon as a Possible Sink for the Missing Sulfur in the Interstellar Medium. I. The C–S Band Strengths
Authors: X. J. Yang, Lijun Hua, Aigen Li
Figure caption: Structures of all the target molecules considered in this work.
Paper: Using the Cartwheel CME to Predict Off-limb Observations of CMEs for New and Upcoming UV and EUV Spectrometers
Authors: E. M. Wraback, E. Landi, W. B. Manchester
Figure caption: Graphical representation of the potential temperature diagnostics for EUVST vs. the maximum temperature of line formation, for comparison to Figure 2. The black line represents T max = T ratio.
Paper: Using the Cartwheel CME to Predict Off-limb Observations of CMEs for New and Upcoming UV and EUV Spectrometers
Authors: E. M. Wraback, E. Landi, W. B. Manchester
Figure caption: Potential use of the SPICE (top) and EUVST (bottom) observations for studying the FIP effect.
Paper: Using the Cartwheel CME to Predict Off-limb Observations of CMEs for New and Upcoming UV and EUV Spectrometers
Authors: E. M. Wraback, E. Landi, W. B. Manchester
Figure caption: Graphical representation of the potential density diagnostics for SPICE (left) and EUVST’s (right) vs. the effective electron temperature.
Paper: Where Have All the Sulfur Atoms Gone? Polycyclic Aromatic Hydrocarbon as a Possible Sink for the Missing Sulfur in the Interstellar Medium. I. The C–S Band Strengths
Authors: X. J. Yang, Lijun Hua, Aigen Li
Figure caption: Structures of PASH molecules identified in meteorites.
Paper: Spectropolarimetry of Fraunhofer Lines in Local Upper Solar Atmosphere
Authors: Z. Q. Qu, L. Chang, G. T. Dun, X. M. Cheng, C. Fang, Z. Xu, D. Yuan, L. H. Deng, X. Y. Zhang
Figure caption: Approximate locations of FOVs of the IFU, directional indicator, and alignment configuration of the microlens-coupled fiber array as the head of the IFU of the prototype FASOT. Top two and bottom-left panels: bright sickles are solar crescents formed by lunar occultation in the process of the eclipse. Artificial white squares superposed in these monitoring images represent the IFU FOVs of sample data, locating at approximately estimated positions. Their spatial coverage array is 5 × 5 pixels or spatial volumes, and each pixel covers 2″ × 2″ in the sky plane. Their sizes are exaggerated relative to the crescent. The codes of the array are assigned in the bottom-right square icon, corresponding to the numbers written on the rightmost columns of Figures 2–6 outlining the IFU end slits. The monitoring images of SE196-2 and SE196-4 are combined on the top-left panel, the SE204-3 image is plotted in the top-right panel, and the SE205-1 image is in the bottom-left panel. The location of SE196-2 is a little higher than SE196-4 above their nearest solar limb. Bottom-right panel: the directional indicator is placed on the left, and on the right is the alignment configuration of 5 × 5 spatial volumes of the IFU FOVs, corresponding to the IFU head microlens and fiber array.
Paper: Spectropolarimetry of Fraunhofer Lines in Local Upper Solar Atmosphere
Authors: Z. Q. Qu, L. Chang, G. T. Dun, X. M. Cheng, C. Fang, Z. Xu, D. Yuan, L. H. Deng, X. Y. Zhang
Figure caption: Sample polarimetric results acquired at the disk center before the eclipse to show the binning effect. The demodulated intensity and fractional linear polarization profiles without and with binning performances are plotted below the raw spectral image to show the enhancement of the polarimetric accuracy after the spatial binning. The symbols above the top image indicate the line producers with their ionization state, and the numbers attached with letters “a” and “b” in the rightmost column reflect ordinary and extraordinary light beams originated from the incident volume array described in the bottom-right panel of Figure 1. The intensity I is obtained by adding the dual beams with the same numbers, and the fractional linear polarization Q/I is demodulated also from the dual beams via a technique called reduced polarimetric optical switching, and hereafter in the figures.
Paper: Spectropolarimetry of Fraunhofer Lines in Local Upper Solar Atmosphere
Authors: Z. Q. Qu, L. Chang, G. T. Dun, X. M. Cheng, C. Fang, Z. Xu, D. Yuan, L. H. Deng, X. Y. Zhang
Figure caption: SE196-2. Top panel: the raw spectral image. Lower panels: the intensity I and fractional linear polarization Q/I profiles obtained from polarization demodulation after spatial binning over P1–P15 (see bottom panel of Figure 1), P16–P25, and the whole (P1–P25) of the FOV respectively.
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 angular velocity of the dumbbell relative to ﹩{{\rm{\Omega }}}_{{\rm{p}}}=\sqrt{{{GM}}_{\bullet }\left(1+e\right)}/{r}_{{\rm{p}}}^{3/2}﹩ as a function of time in units of the Keplerian orbital period, T. The different curves correspond to the initial phase of the dumbbell with respect to the argument of pericenter. This figure demonstrates that the dumbbell is originally spun up to an angular velocity that is comparable to Ωp, and on each successive pericenter passage, the dumbbell receives a pseudorandom kick to its angular velocity, resulting in a scatter about the mean value of 1.
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: Results of the SPH simulation for the 3M ⊙ TAMS star. The top panel shows the angular velocity Ω imparted to the core, with the primary y-axis normalized by the breakup angular velocity of the core, ﹩\sqrt{{{GM}}_{{\rm{c}}}}/{R}_{{\rm{c}}}^{3/2}﹩, and the secondary y-axis normalized by the angular velocity of the COM at pericenter. The bottom panel shows its linear component, v  φ  = sΩ in units of ﹩\sqrt{{{GM}}_{{\rm{c}}}/{R}_{{\rm{c}}}}﹩, as a function of cylindrical distance s from the center.
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 from a simulation of the repeated partial disruption of a 3M ⊙ TAMS star by a 106 M ⊙ SMBH, with a resolution of 106 particles for the disrupted star. Each encounter is labeled by a different color, as indicated by the number in the legend. The impact parameter for each encounter was β = 1. Roughly the same amount of mass is stripped off from the star during each subsequent pericenter passage, thus giving rise to a comparable peak luminosity between pericenter passages. The late-time evolution of the fallback rates scales as t −9/4, consistent with the expected scaling for partial disruptions.
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: Left: the relative difference of the time between pericenter passages N and N − 1 to the Keplerian orbital period, e.g., the value appropriate to N = 2 represents the time between the first and second pericenter passage, minus and subsequently divided by the Keplerian orbital period T. Right: the relative difference between the pericenter distance on the Nth pericenter passage to the Keplerian pericenter distance r p. The values in these figures are consistent with the analytical expressions derived here; see Equation (2). These data are appropriate to the orange curve in Figure 1, from which it is apparent that the largest changes in the rotational velocity of the dumbbell correspond to the largest changes in both the orbital period and the pericenter, which is expected.
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: A particle plot showing the density of the disrupted 3M ⊙ TAMS star as a function of radial distance from the black hole, at ∼2 days after the COM of the star reaches pericenter. The density profile shows a distinct division between particles belonging to the core (densities ≳10−2 g cm−3) and those belonging to the tidally disrupted debris stream (densities ≲10−6 g cm−3). In this case, the subset of particles having densities greater than 0.001 g cm−3 is defined as the core.
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 amount of mass stripped ΔM, as a function of number of pericenter passages N, for the 3M ⊙ TAMS star on an orbit having an impact parameter β = 1.
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 density of the core in the orbital plane, represented as a function of its COM subtracted position coordinates. The vectors overlaid on the figure represent the velocity of the core particles in the COM frame, with their length indicating the norm of the vectors. The velocity structure shows the spin imparted to the stellar core through tidal interactions.
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: Left: the fractional change in the angular velocity imparted to the core between the Nth and (N − 1)th pericenter passages. The downward trend indicates that the increment in angular velocity between consecutive pericenter passages decreases with an increase in the number of pericenter passages, N. Right: the angular velocity imparted to the core, in units of its breakup spin ﹩\sqrt{{{GM}}_{{\rm{c}}}/{R}_{{\rm{c}}}^{3}}﹩, as a function of the number of pericenter passages.
Paper: Blowing Star Formation Away in Active Galactic Nuclei Hosts. I. Observation of Warm Molecular Outflows with JWST MIRI
Authors: J. H. Costa-Souza, Rogemar A. Riffel, Gabriel L. Souza-Oliveira, Nadia L. Zakamska, Marina Bianchin, Thaisa Storchi-Bergmann, Rogério Riffel
Figure caption: Sloan Digital Sky Survey red, green, and blue (RGB) composition of UGC 8782. The white contours trace the radio jet at 1.4 GHz, obtained from the Very Large Array archive (R. H. Becker et al. 1995). The zoomed-in panel displays the JWST MIRI 7.0 μm continuum image. The white contours are from an L-Band (1.65 GHz) image from the e-Merlin archive. The position of the MIR emission peak is indicated by a + sign, while the × shows the position of the optical nucleus. The plots show examples of fits of the emission lines for four positions, along with the residuals of the fits divided by the standard deviation of the nearby continuum. The bottom panel shows an integrated spectrum within a circular aperture of 1″ around the nucleus.
Paper: Blowing Star Formation Away in Active Galactic Nuclei Hosts. I. Observation of Warm Molecular Outflows with JWST MIRI
Authors: J. H. Costa-Souza, Rogemar A. Riffel, Gabriel L. Souza-Oliveira, Nadia L. Zakamska, Marina Bianchin, Thaisa Storchi-Bergmann, Rogério Riffel
Figure caption: The top panels show the flux distribution in ﹩{\mathrm{log}}_{10}(\mathrm{erg}\,{{\rm{s}}}^{-1}{\mathrm{cm}}^{-2}﹩) (left), velocity field (center), and velocity dispersion map (right) for the narrow (disk) component of the H2 S(1) (top) and [Ar II] 6.99 μm (bottom) emission lines. The + and × symbols mark the position of the MIR and optical continuum peaks, respectively. The gray regions correspond to locations where the emission lines are not detected with at least 3σ above the continuum noise. The green contours are from the L-Band (1.65 GHz) image from the e-Merlin archive. The middle panels show the results for the outflow component with the same nomenclature used for the disk component, while the bottom panels show the results for the fast outflow seen in [Ar II] 6.99 μm.
Paper: Blowing Star Formation Away in Active Galactic Nuclei Hosts. I. Observation of Warm Molecular Outflows with JWST MIRI
Authors: J. H. Costa-Souza, Rogemar A. Riffel, Gabriel L. Souza-Oliveira, Nadia L. Zakamska, Marina Bianchin, Thaisa Storchi-Bergmann, Rogério Riffel
Figure caption: Excitation diagrams for the outflow and disk components. The y-axis shows the population number of the J state divided by the degeneracy of the state and normalized by the J = 3 state, while the x-axis shows the upper-level energy. The red line describes the power-law model fitted at the outflow component, while the blue line represents the disk.
Paper: Blowing Star Formation Away in Active Galactic Nuclei Hosts. I. Observation of Warm Molecular Outflows with JWST MIRI
Authors: J. H. Costa-Souza, Rogemar A. Riffel, Gabriel L. Souza-Oliveira, Nadia L. Zakamska, Marina Bianchin, Thaisa Storchi-Bergmann, Rogério Riffel
Figure caption: Radial plots for the mass-outflow rate (top panel) and kinetic power of the outflows (bottom panel). The dark blue points represent the ionized outflows, warm H2 is shown in light blue and the hot H2 is shown as orange squares. The arrows in the first radial bin show the minimum values of the outflow properties, after correcting for the PSF scatter if an unresolved outflow is present. For bins further from the nucleus, the PSF contribution is negligible (≲2%), so the arrows are not shown.
Paper: Blowing Star Formation Away in Active Galactic Nuclei Hosts. I. Observation of Warm Molecular Outflows with JWST MIRI
Authors: J. H. Costa-Souza, Rogemar A. Riffel, Gabriel L. Souza-Oliveira, Nadia L. Zakamska, Marina Bianchin, Thaisa Storchi-Bergmann, Rogério Riffel
Figure caption: The maps show the models for the velocity (left) and the emission-line flux distribution (right) before (top) and after (bottom) the convolution with PSF. Examples of line profiles before (in blue) and after (orange) the convolution with the PSF are shown at the bottom plots, for the positions indicated in the model flux map.