adsabs/AstroCLIMB huggingface dataset:
Paper: Parkes Radio and NuSTAR X-Ray Observations of the Composite Supernova Remnant B0453–685 in the Large Magellanic Cloud
Authors: Jordan Eagle, Jeremy Hare, Elizabeth Hays, Daniel Castro, Joseph Gelfand, Jwaher Alnaqbi, Matthew Kerr, Shi Dai, Jean Ballet, Fabio Acero, Patrick Slane, Marco Ajello
Figure caption: Left: time-independent model for B0453–685 in the X-ray band. X-ray data of the PWN (cyan) are from J. Eagle et al. (2023) and the orange and green X-ray data are from Section 3.3. Right: the time-dependent (evolutionary) model from J. Eagle et al. (2023) in the X-ray band. The data are the same as in the left panel.
Paper: Parkes Radio and NuSTAR X-Ray Observations of the Composite Supernova Remnant B0453–685 in the Large Magellanic Cloud
Authors: Jordan Eagle, Jeremy Hare, Elizabeth Hays, Daniel Castro, Joseph Gelfand, Jwaher Alnaqbi, Matthew Kerr, Shi Dai, Jean Ballet, Fabio Acero, Patrick Slane, Marco Ajello
Figure caption: Tricolor Chandra X-ray flux map of B0453–685. Red is 0.5–1.2 keV, green is 1.2–2 keV, and blue is 2–8 keV. Src2 is marked in green.
Paper: Parkes Radio and NuSTAR X-Ray Observations of the Composite Supernova Remnant B0453–685 in the Large Magellanic Cloud
Authors: Jordan Eagle, Jeremy Hare, Elizabeth Hays, Daniel Castro, Joseph Gelfand, Jwaher Alnaqbi, Matthew Kerr, Shi Dai, Jean Ballet, Fabio Acero, Patrick Slane, Marco Ajello
Figure caption:                    ﹩{g}^{{\prime} }﹩ light curve of Src2 folded on periods calculated using ﹩{g}^{{\prime} }﹩ data (25.61 and 29.13 days). The folding period used is labeled in each plot. Each fitted lightcurve (FLC) is fitted with a ﹩\sin +\cos ﹩ model using nterms = 2.
Paper: Parkes Radio and NuSTAR X-Ray Observations of the Composite Supernova Remnant B0453–685 in the Large Magellanic Cloud
Authors: Jordan Eagle, Jeremy Hare, Elizabeth Hays, Daniel Castro, Joseph Gelfand, Jwaher Alnaqbi, Matthew Kerr, Shi Dai, Jean Ballet, Fabio Acero, Patrick Slane, Marco Ajello
Figure caption: Upper and middle panels: optical light curves of Src2 in ﹩{g}^{{\prime} }﹩ and ﹩{r}^{{\prime} }﹩ filters between MJD 60352 and 60388 (2023 December 2 to 2024 March 19). Lower panel: g′ − r′ color evolution over the same duration.
Paper: Resonant Friction on Disks in Galactic Nuclei
Authors: Yuri Levin
Figure caption: Evolution of the stellar disk. The background cluster is initially rotating along the z-axis with the dimensionless rotation rate ﹩\tilde{\gamma }﹩ defined in the text and specified at the top of each subfigure. The counterrotating disk is injected at t = 0. The figure shows some randomly chosen examples of the time evolution of n  z , where ﹩{\boldsymbol{n}}﹩ is the unit vector directed along the star’s angular momentum, for all the stars in the disk. The 52 red lines are marking the inner half of the disk’s stars and the 53 green lines are marking those of the outer half. As the rotation rate increases, we observe the disruption of the outer parts of the disk and a tendency for the inner disk to align with the cluster. At high rotation rate, the disk gets warped or broken into transient rings. These effects are very important at 5 Myr, the likely age of the young stellar population in the Galactic center.
Paper: Resonant Friction on Disks in Galactic Nuclei
Authors: Yuri Levin
Figure caption: Pictorial description of the scenario described here. An infalling cloud of gas is tidally disrupted and its material forms an accretion disk around the SMBH. The initial orientation of the disk is random, but the resonant dynamical friction drives the disk’s angular momentum ﹩{{\boldsymbol{L}}}_{}﹩ into alignment with that of the cluster ﹩{{\boldsymbol{L}}}_{\mathrm{cluster}}﹩.
Paper: Identifying Jittering Jet-shaped Ejecta in the Cygnus Loop Supernova Remnant
Authors: Dmitry Shishkin, Roy Kaye, Noam Soker
Figure caption: The Cygnus Loop SNR in several wavelengths. (a) Planck 30 GHz I (Planck Collaboration et al. 2020; linear scale, truncated at 1.1 mK); (b) GALEX UV (P. Morrissey et al. 2007; 175–280 nm; image credit: NASA/JPL-Caltech); ((c), (e)) ROSAT X-ray count image (B. Aschenbach 1993; soft band: 0.1–0.4 keV; 0.1–50 counts range) in log (panel (c)) and linear (panel (e)) scale; (d) sulfur-hydrogen-oxygen (SHO, visible) image (J. C. Raymond et al. 2023); (f) AKARI IR (140 and 90 μm, MJy sr−1). We identify the morphological features used to identify the point-symmetric morphology (Section 4). The short dashed white line in panels (b) and (d) marks a segment of the pipe, which extends from the north spout to the south spout and connects them. The cavity is the dark area in the visible band that the dashed white ellipse marks on panel (d). The dashed curved lines in panel (f) depict the arc seen in panel (d) (left) and the curved edge of the dust cloud to the north of the Cygnus Loop (right). Contour lines in panel (a) are of a kernel-smoothed image, at ∼40% and ∼50% levels. Marking locations are consistent between different panels.
Paper: Identifying Jittering Jet-shaped Ejecta in the Cygnus Loop Supernova Remnant
Authors: Dmitry Shishkin, Roy Kaye, Noam Soker
Figure caption: Four annotated panels pointing out the point-symmetrical structure we identify in the Cygnus Loop. (a) Red depicts the visible image (panel (d) of Figure 1 and panel (d) here) and green depicts log scale X-ray images (panel (e) in Figure 1 and panel (c) here); (b) magenta represents visible (panel (d) of Figure 1 and panel (d) here), green represents log scale X-ray (panel (c) in Figure 1 and panel (c) here), and teal represents the AKARI 90 μm image (panel (d) in Figure 2); (c) log-scale X-ray; (d) visible as panel (d) in Figure 1. The pipe and the two spouts (see Figure 1) form the “hose,” i.e., the long and narrow faint zone extending north–south. The structure of the hose with the two clumps (dashed yellow ellipses) has a 180° symmetry around its center (marked by a blue star at its center). The two other lines connect two opposite structures, as indicated, with a blue star marking the center of each line. The three symmetry lines form the point-symmetric wind rose of the Cygnus Loop. We attribute this shaping to at least three pairs of opposite jets. A red circle in panel (b) denotes the average location of the three centers (in the plane of the sky). We also denote a possible northern blowout with two curved lines in panel (b), bounded by the visible arc (panel (d) of Figure 1) and the curved edge of the dust cloud also seen in Figure 2. In panel (b) we also mark a circle with a radius matching the eastern edge of the remnant whose center is the average of the wind rose (red circle).
Paper: Identifying Jittering Jet-shaped Ejecta in the Cygnus Loop Supernova Remnant
Authors: Dmitry Shishkin, Roy Kaye, Noam Soker
Figure caption: Four panels at different IR emission wavelengths covering the same area of the panels in Figure 1. These images highlight the dust cloud surrounding the Cygnus Loop remnant. Panels (a) and (b) are Planck images 143 GHz I (K) and 857 GHz I (MJy sr−1), respectively. Panels (c) and (d) are AKARI images at 140 and 90 μm (MJy sr−1), respectively. On panel (d), we mark the curved edge of the dust cloud to the north of the Cygnus Loop and the arc location from Figure 1. We also denote the location of the cavity from panel (d) of Figure 1 with a dashed ellipse for reference.
Paper: Synchrotron Polarization of a Hybrid Distribution of Relativistic Thermal and Nonthermal Electrons in Gamma-Ray Burst Prompt Emission
Authors: Cheng Kangfa, Jirong Mao, Zhao Xiaohong, Liu Hongbang, Merlin Kole, Nicolas Produit, Chen Zhifu
Figure caption: The PD and spectral data of GRBs compared with our numerical results. The black, red, and green lines are compared with GRBs 110301A, 180914B, and 170114A, respectively. For the detailed model parameters of these lines, see Table 2. The spectral parameters (α  E , β  E , and E  p ) with subscripts of 1, 2, and 3 correspond to GRBs 110301A, 180914B, and 170114A, respectively. The observed peak energies are ﹩{E}_{{\rm{p}}1}={106.80}_{+1.85}^{-1.75}﹩ keV, ﹩{E}_{{\rm{p}}2}={453}_{-24}^{+26}﹩ keV, and ﹩{E}_{{\rm{p}}3}={211}_{-25}^{+31}﹩ keV, respectively. The top left panel shows the flux density spectra and the bottom left panel displays the corresponding spectral index. The top right panel shows the PD with different conjunctive LFs. The bottom right panel displays the polarization spectra.
Paper: Identifying Jittering Jet-shaped Ejecta in the Cygnus Loop Supernova Remnant
Authors: Dmitry Shishkin, Roy Kaye, Noam Soker
Figure caption: (a) A radio image of SNR G309.2–00.6 and marks as presented by B. M. Gaensler et al. (1998), who already argued that jets shaped this CCSN. (b) The main CCSNR shell with labels from N. Soker (2024e) of the two arcs (“crescents”), the symmetry axis, and the rim–nozzle structure. We added the labeling of the blowout (panel (a)) and the filaments (panel (b)).
Paper: Identifying Jittering Jet-shaped Ejecta in the Cygnus Loop Supernova Remnant
Authors: Dmitry Shishkin, Roy Kaye, Noam Soker
Figure caption: A small area of the full MeerKAT (radio emission) total-intensity galactic center mosaic (I. Heywood et al. 2022). We added the labels and white dashed line on the image of the SNR G1.0-0.1: the blowout, the ear, and what we suggest to be the main jet axis. We argue this CCSNR was also shaped by pairs of jets, the last jets of the many that exploded this CCSNR in the frame of the JJEM. Grid lines are in dotted white lines and labels denoted at the top right.
Paper: Measuring the 34S and 33S Isotopic Ratios of Volatile Sulfur during Planet Formation
Authors: Alice S. Booth, Maria N. Drozdovskaya, Milou Temmink, Hideko Nomura, Ewine F. van Dishoeck, Luke Keyte, Charles J. Law, Margot Leemker, Nienke van der Marel, Shota Notsu, Karin Öberg, Catherine Walsh
Figure caption: Inferred isotopic ratios of S and O in SO and SO2 for the Oph-IRS 48 disk calculated for a range of excitation temperatures. Note the 34S ratio from SO2 and the 18O ratio from SO are lower limits. The vertical dashed lines highlight our fiducial temperature of 60 K, which is the rotational temperature of SO2 (Temmink et al. 2024, in preparation). The horizontal dashed lines denote the V-CDT standard isotopic ratios for 32S/34S, 32S/33S, 34S/33S, and 16O/18O (R. A. Werner & W. A. Brand 2001; T. Ding et al. 2001).
Paper: Measuring the 34S and 33S Isotopic Ratios of Volatile Sulfur during Planet Formation
Authors: Alice S. Booth, Maria N. Drozdovskaya, Milou Temmink, Hideko Nomura, Ewine F. van Dishoeck, Luke Keyte, Charles J. Law, Margot Leemker, Nienke van der Marel, Shota Notsu, Karin Öberg, Catherine Walsh
Figure caption: Bar plots showing the percentage of observed gas-phase sulfur in different atoms/molecules for the protostar IRAS 16293-2442 B, Class II disk Oph-IRS 48, comet 67P/C-G, and shocked region L1157-B1. Values are taken from U. Calmonte et al. (2016), M. N. Drozdovskaya et al. (2018), J. Holdship et al. (2019), T. Kushwahaa et al. (2023), and A. Booth et al. (2024). Where the percentage is less than 0.5%, a note is added. We note that this comparison naively assumes that 100% of the volatile S can be accounted for in the currently detected molecules in these systems.
Paper: Measuring the 34S and 33S Isotopic Ratios of Volatile Sulfur during Planet Formation
Authors: Alice S. Booth, Maria N. Drozdovskaya, Milou Temmink, Hideko Nomura, Ewine F. van Dishoeck, Luke Keyte, Charles J. Law, Margot Leemker, Nienke van der Marel, Shota Notsu, Karin Öberg, Catherine Walsh
Figure caption: Channel maps of the S18O J = 99 − 88 transition where the black solid contours mark the [3, 4] × σ level and black dashed contours mark [−4, −3] × σ level. The gray solid contour marks the 5σ level of the 34SO J = 98 − 87 transition to show the expected position–velocity pattern of the disk emission.
Paper: Measuring the 34S and 33S Isotopic Ratios of Volatile Sulfur during Planet Formation
Authors: Alice S. Booth, Maria N. Drozdovskaya, Milou Temmink, Hideko Nomura, Ewine F. van Dishoeck, Luke Keyte, Charles J. Law, Margot Leemker, Nienke van der Marel, Shota Notsu, Karin Öberg, Catherine Walsh
Figure caption: Inferred isotopic ratios of S and O in different volatile sulfur species detected toward comets and protoplanetary disks. The results for Oph-IRS 48 are highlighted by the star or arrow markers at temperatures of 30, 60, and 100 K. Note the 34S ratio from SO2 and the 18O ratio from SO are lower limits. The dashed lines denote the V-CDT standard isotopic ratios for 32S/34S, 32S/33S, and 16O/18O (R. A. Werner & W. A. Brand 2001; T. Ding et al. 2001). The vertical bars mark the ±1σ errors. The other disk values are taken from R. Le Gal et al. (2019), N. T. Phuong et al. (2021), and A. Booth et al. (2024). Cometary values are taken from D. C. Jewitt et al. (1997), J. A. Paquette et al. (2018), and K. Altwegg et al. (2020), as well as J. Crovisier et al. (2004), N. Biver et al. (2016), J. A. Paquette et al. (2017), and U. Calmonte et al. (2017). We exclude the S2 isotope ratio reported in U. M. Calmonte (2015) and subsequently in J. A. Paquette et al. (2017) for 67P/C-G from our comparison due to the low signal to noise of the S2 peak in the mass spectra and the significant contamination from other overlapping species (M. Rubin 2024, private communication).
Paper: Measuring the 34S and 33S Isotopic Ratios of Volatile Sulfur during Planet Formation
Authors: Alice S. Booth, Maria N. Drozdovskaya, Milou Temmink, Hideko Nomura, Ewine F. van Dishoeck, Luke Keyte, Charles J. Law, Margot Leemker, Nienke van der Marel, Shota Notsu, Karin Öberg, Catherine Walsh
Figure caption: Integrated intensity maps of the 0.9 mm dust continuum emission and the sulfur isotopologues in the Oph-IRS 48 disk. The units of the color bar are mJy beam−1 km s−1 for the molecular lines and mJy beam−1 for the continuum. The black contours on the S18O map highlight 3× the rms noise level.
Paper: JWST View of Four Infant Galaxies at z = 8.31–8.49 in the MACS J0416.1−2403 Field and Implications for Reionization
Authors: Zhiyuan Ma, Bangzheng Sun, Cheng Cheng, Haojing Yan, Chenxiaoji Ling, Fengwu Sun, Nicholas Foo, Eiichi Egami, José M. Diego, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Rogier A. Windhorst, Jordan C. J. D'Silva, Anton M. Koekemoer, Dan Coe, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Rafael Ortiz, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Nathan J. Adams, Nimish P. Hathi, Hervé Dole, S. P. Willner, Daniel Espada, Lukas J. Furtak, Tiger Yu-Yang Hsiao, Qiong Li, Wenlei Chen, Jean-Baptiste Jolly, Chian-Chou Chen
Figure caption: Extracted 2D and 1D spectra from the NIRCam WFSS observations. For each object, the top panel shows the 2D spectrum with the background and continuum subtracted, and the bottom panel shows the resultant 1D spectrum with the bandpass filter and grism orientation labeled. Identified emission lines are marked. The 2D spectra of JD and JD-N are displayed after smoothing with a Gaussian kernel with σ = 1, while those of Y1 are not smoothed in order to show the separation of the two components. The gray shading in the 1D spectra indicates the 1σ uncertainty band. With only a few exposures in each setup, stacking has limited ability to remove outlying pixels, leaving some narrow spikes in the 1D spectra. Fortunately, the emission lines of interest are not contaminated by such spikes.
Paper: JWST View of Four Infant Galaxies at z = 8.31–8.49 in the MACS J0416.1−2403 Field and Implications for Reionization
Authors: Zhiyuan Ma, Bangzheng Sun, Cheng Cheng, Haojing Yan, Chenxiaoji Ling, Fengwu Sun, Nicholas Foo, Eiichi Egami, José M. Diego, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Rogier A. Windhorst, Jordan C. J. D'Silva, Anton M. Koekemoer, Dan Coe, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Rafael Ortiz, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Nathan J. Adams, Nimish P. Hathi, Hervé Dole, S. P. Willner, Daniel Espada, Lukas J. Furtak, Tiger Yu-Yang Hsiao, Qiong Li, Wenlei Chen, Jean-Baptiste Jolly, Chian-Chou Chen
Figure caption: Color images of the three fields. Image sizes are 1″ square for Y1 and 2″ square for the other two fields. The color scheme is F090W + F115W + F150W as blue, F200W + F277W as green, and F356W + F410M + F444W as red. In each image, the red arrows show the NIRCam grism WFSS dispersion direction in the PID 3538 observation in GC and GR, respectively; the yellow arrows in the other two images show the dispersion direction of GC utilized by the MAGNIF observations.
Paper: JWST View of Four Infant Galaxies at z = 8.31–8.49 in the MACS J0416.1−2403 Field and Implications for Reionization
Authors: Zhiyuan Ma, Bangzheng Sun, Cheng Cheng, Haojing Yan, Chenxiaoji Ling, Fengwu Sun, Nicholas Foo, Eiichi Egami, José M. Diego, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Rogier A. Windhorst, Jordan C. J. D'Silva, Anton M. Koekemoer, Dan Coe, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Rafael Ortiz, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Nathan J. Adams, Nimish P. Hathi, Hervé Dole, S. P. Willner, Daniel Espada, Lukas J. Furtak, Tiger Yu-Yang Hsiao, Qiong Li, Wenlei Chen, Jean-Baptiste Jolly, Chian-Chou Chen
Figure caption: Cutouts of Y1 (top), JD (middle), and f090d_018 (bottom) in the eight NIRCam bands using the 30 mas images. North is up and east is left. The size of the Y1 images is 1″ × 1″, while the others are 2″ × 2″. The three resolved Y1 components (Y1-E, Y1-C, and Y1-W) are labeled in the F200W image. JD has a close companion, JD-N, whose colors also meet the requirements of a J-band dropout. Both objects are labeled in the F200W image.
Paper: JWST View of Four Infant Galaxies at z = 8.31–8.49 in the MACS J0416.1−2403 Field and Implications for Reionization
Authors: Zhiyuan Ma, Bangzheng Sun, Cheng Cheng, Haojing Yan, Chenxiaoji Ling, Fengwu Sun, Nicholas Foo, Eiichi Egami, José M. Diego, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Rogier A. Windhorst, Jordan C. J. D'Silva, Anton M. Koekemoer, Dan Coe, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Rafael Ortiz, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Nathan J. Adams, Nimish P. Hathi, Hervé Dole, S. P. Willner, Daniel Espada, Lukas J. Furtak, Tiger Yu-Yang Hsiao, Qiong Li, Wenlei Chen, Jean-Baptiste Jolly, Chian-Chou Chen
Figure caption: Corner plots showing the posterior distributions of the fitted parameters corresponding to the SED fitting illustrated in Figure 5. The inset in the upper right corner in each panel shows the SFH, where the shaded region corresponds to the 16th to 84th percentile range, and the black curve is the median value.
Paper: JWST View of Four Infant Galaxies at z = 8.31–8.49 in the MACS J0416.1−2403 Field and Implications for Reionization
Authors: Zhiyuan Ma, Bangzheng Sun, Cheng Cheng, Haojing Yan, Chenxiaoji Ling, Fengwu Sun, Nicholas Foo, Eiichi Egami, José M. Diego, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Rogier A. Windhorst, Jordan C. J. D'Silva, Anton M. Koekemoer, Dan Coe, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Rafael Ortiz, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Nathan J. Adams, Nimish P. Hathi, Hervé Dole, S. P. Willner, Daniel Espada, Lukas J. Furtak, Tiger Yu-Yang Hsiao, Qiong Li, Wenlei Chen, Jean-Baptiste Jolly, Chian-Chou Chen
Figure caption: Demonstration of the decomposition of Y1's three components in the seven NIRCam images as labeled. Each panel displays the original image (left), the model constructed by GALFIT using the Sérsic profiles (middle), and the residual image by subtracting the model from the original image (right). The images are all 1.″2 × 1.″2 in size.
Paper: JWST View of Four Infant Galaxies at z = 8.31–8.49 in the MACS J0416.1−2403 Field and Implications for Reionization
Authors: Zhiyuan Ma, Bangzheng Sun, Cheng Cheng, Haojing Yan, Chenxiaoji Ling, Fengwu Sun, Nicholas Foo, Eiichi Egami, José M. Diego, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Rogier A. Windhorst, Jordan C. J. D'Silva, Anton M. Koekemoer, Dan Coe, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Rafael Ortiz, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Nathan J. Adams, Nimish P. Hathi, Hervé Dole, S. P. Willner, Daniel Espada, Lukas J. Furtak, Tiger Yu-Yang Hsiao, Qiong Li, Wenlei Chen, Jean-Baptiste Jolly, Chian-Chou Chen
Figure caption: Illustration of the SED fitting with BAGPIPES for each entry in Table 1. The blue points with error bars show the observed flux densities, and the orange points show the synthesized magnitudes from the 50th percentile fit. The posterior spectra corresponding to the 16th to 84th percentile range are shown in yellow in each panel.
Paper: JWST View of Four Infant Galaxies at z = 8.31–8.49 in the MACS J0416.1−2403 Field and Implications for Reionization
Authors: Zhiyuan Ma, Bangzheng Sun, Cheng Cheng, Haojing Yan, Chenxiaoji Ling, Fengwu Sun, Nicholas Foo, Eiichi Egami, José M. Diego, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Rogier A. Windhorst, Jordan C. J. D'Silva, Anton M. Koekemoer, Dan Coe, Christopher J. Conselice, Simon P. Driver, Brenda Frye, Norman A. Grogin, Madeline A. Marshall, Mario Nonino, Rafael Ortiz, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Nathan J. Adams, Nimish P. Hathi, Hervé Dole, S. P. Willner, Daniel Espada, Lukas J. Furtak, Tiger Yu-Yang Hsiao, Qiong Li, Wenlei Chen, Jean-Baptiste Jolly, Chian-Chou Chen
Figure caption: SED fitting results for f090d_018 with redshift as a free parameter to derive z ph. The plots are similar to those in Figures 5 and 6.
Paper: Determining the Extents, Geometries, and Kinematics of Narrow-line Region Outflows in Nearby Seyfert Galaxies
Authors: Garrett E. Polack, Mitchell Revalski, D. Michael Crenshaw, Travis C. Fischer, Henrique R. Schmitt, Steven B. Kraemer, Beena Meena, Marc Rafelski
Figure caption: The HST WFC3 F547M (left), FQ508N or F502N (center), and continuum-subtracted [O III] images (right) for the 12 AGN with new [O III] images. The location of the continuum peak from the F547M image is shown by a green cross. The archival HST STIS long-slit position angles are denoted by white shaded lines overlaid on the [O III] images. All panels show the inner 10″ × 10″ for each galaxy, with north up and east to the left.
Paper: Determining the Extents, Geometries, and Kinematics of Narrow-line Region Outflows in Nearby Seyfert Galaxies
Authors: Garrett E. Polack, Mitchell Revalski, D. Michael Crenshaw, Travis C. Fischer, Henrique R. Schmitt, Steven B. Kraemer, Beena Meena, Marc Rafelski
Figure caption: A 3.″6 × 3.″4 [O III] image of NGC 7682 with three green contour lines surrounding the ionized gas structure. The middle contour is the measured background 3σ value of 2.3 × 10−18 erg s−1 cm−2 arcsec−2 and the two additional contours on either side represent offsets of 1σ in continuum brightness. The cross indicates the brightness centroid used as the zero-point for radial measurements, and the green circle denotes the radial extent of the middle contour. The recorded extent of the emission is an average of all three contour extents measured this way, with the luminosity being an average of the value contained within each circle.
Paper: Determining the Extents, Geometries, and Kinematics of Narrow-line Region Outflows in Nearby Seyfert Galaxies
Authors: Garrett E. Polack, Mitchell Revalski, D. Michael Crenshaw, Travis C. Fischer, Henrique R. Schmitt, Steven B. Kraemer, Beena Meena, Marc Rafelski
Figure caption: Elliptical modeling of the ground-based image of NGC 7682 on a false color scale to highlight detailed structure. The left panel shows the ground-based imaging, the center panel shows the reconstructed model of the galaxy using the isophotal ellipses fit to the image, and the third panel shows the residual from the model subtraction. Each image shows a 100″ × 100″ field of view with the axes given in pixels.