adsabs/AstroCLIMB huggingface dataset:
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: Physical properties of individual clouds in the default model located at 22.2, 133.5, 311.5, and 608.2 pc, respectively, as a function of the depth from the illuminated surface. Upper left: the fraction of the H+ ion; Upper right: electron and hydrogen density; Lower left: electron temperature; Lower right: ionization parameter. The outer edge of the cloud is determined by the stop column density, which is 1020 cm−2 in the default model.
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: The fraction of N and O ion species of individual clouds located at 22.2, 133.5, 311.5, and 608.2 pc in the default model as a function of cloud depth. Left: neutral oxygen (lines with crossed points), O+ (solid lines), and O++ (dotted lines) fraction. Right: N+ (solid lines) and N++ (dotted lines) fraction. The outer edge of the cloud is determined by the stop column density, which is 1020 cm−2 in the default model.
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: Similar to Figure 10, but comparing models with various SP properties, as described in the text. model A with a default bulge SP (age = 8 Gyr, metallicity Z = 1.5 Z ⊙) is shown as a solid red line. Model D with a younger, 2 Gyr old SP is shown as a dashed–dotted blue line. Model E with an SP with an age of 8 Gyr, a solar-metallicity SP is represented by a dotted cyan line. The same AGN SED is adopted in these three models.
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: The radial distribution of the observed line intensities and the simulated line intensities from the CLOUDY models of the major emission lines: Hα, Hβ, [N II], [O III], [O II], and [O I]. The data points in black are the same as in Figure 8. The data points in green show the observed line intensity distribution without deprojection, that is, assuming an inclination angle of zero. The solid red lines represent the default model A, the dotted blue line represents model C with a 10 times brighter AGN, and the dashed blue line represents model F with a density profile of n H ∝ r −1.5. The latter two models have a better chance of alleviating the discrepancy between the observed flat trend of [O III]/Hβ ratio and the prediction of the default model.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Top row: The spectra extraction regions for the ER spectra plotted on band A in each channel. The total ER spectrum was extracted from the white elliptical annulus, with the east and west ER extracted from the segments on the left- and right-hand sides. Bottom row: Same as top but for the cardinal point and ejecta spectra. In both rows, the location of the outer rings is shown by the two faded ellipses, the channels 1–3 background inner boundaries are shown by the dashed cyan circles, and the channel 4 background region is shown by the dashed cyan polygon. The “entire” SN 1987A system spectrum was extracted from a region slightly smaller than the inner boundary of the background regions and excluding Star 3. North is up, east is left.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Sample slices from our 12 MRS sub-band cubes, with the band labels shown in the top left-hand corner. The white lines in each pane represent 1.″0 to highlight the increasing size of the FOV, as well as the decreasing spatial resolution from channels 1–4. “Star 3” is visible to the lower left-hand side of the ER in bands 1A–2A. North is up, east is left.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: The total MIRI MRS background-subtracted spectrum of SN 1987A 12,927 days (35.4 yr) after the explosion. The mid-IR spectrum at this epoch is dominated by dust emission from amorphous silicates in the inner ER. The line emission is from a combination of the ionized ER and the central ejecta (with a broad emission profile, e.g., [Fe II] at 26  μm). The most significant lines are highlighted.
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: The radial distribution of [O III]/[O II] (left) and [O III]/[O I] (right) ratios. Symbols are the same as in Figure 15.
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: Left: similar to Figure 10, but comparing models with different cloud column densities. The default model A with a column density N H = 1020 cm−2 is shown with a solid red line. Model J with N H = 1021 cm−2 is shown with a dotted magenta line, while model K with N H = 1022 cm−2 is shown with a dashed–dotted orange line. Model L with a solar-metallicity gas is shown with a dashed cyan line.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Illustration of the different spatial distributions of the line emission and continuum. The left-hand panel shows an integrated image of the H I 7.460 μm line after subtraction of the continuum, the middle panel shows an image of the continuum on each side of the line, and the right-hand panel shows the two images together. The black contours in the left-hand and middle panels show the hotspots in a HST/F657N image obtained on 2022 September 6 (dominated by Hα emission, S. Rosu et al. 2023, in preparation). Note the good agreement between the H I 7.460 μm line and the HST image, while the continuum is more spatially extended.
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: The χ 2 distribution of different models, for the line intensities (left) and line ratios (right).
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Fits to the MRS and NIRspec data using the two-temperature dust compositions of astrodust (Hensley & Draine 2023) in the top panel, carbon and silicates (Draine & Lee 1984) in the middle panel, and silicates (Draine & Lee 1984) and iron dust in the bottom panel. The synchrotron emission (orange line) has been extrapolated from ALMA observations based on the models described in Cendes et al. (2018) and Cigan et al. (2019) (see text for details). The emission from the H and He continuum and lines (purple line) is described in Larsson et al. (2023). The best-fit parameters for the dust components are summarized in Table 4.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Moment maps for a selection of species prominent in the ring ordered row-by-row. The left-hand panes show the integrated line intensity. The middle panes show the radial velocity of the line emission, corrected for the systemic barycentric velocity of SN 1987A of +287 km s−1 (Gröningsson et al. 2008). The right-hand panes show the line FWHMs. The gray circles overlaid on the images are the locations of the outer rings derived determined from the [Ne II] 12.8135 μm morphology, with the gray contours showing the ER continuum morphology determined from an “off” position adjacent to the line.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Best fit temperatures (left-hand panel) and dust masses (right-hand panel) using a two-temperature dust model for each spectrum shown in Figure 11. The spectra were fitted over the 5–30 μm spectral range using the astrodust (Hensley & Draine 2023) grain composition. The error bars represent the 3σ uncertainties from the fit. The data are summarized in Table 5.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Continuum subtracted emission line images for those species with emission from outside the ER. The gray circles overlaid on the images are the locations of the outer rings determined from the [Ne II] 12.8135 μm morphology, with the light-gray contours showing the ER continuum morphology determined from an “off” position adjacent to the line. The color bars are in units of MJy sr−1.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Left-hand panel: Temporal evolution of the ER’s mid-IR spectra observed by Spitzer IRS (days 6805–7955; year 18.6–21.8) and JWST’s MRS instrument (day 12927; year 35.4). Right-hand panel: Spectra from the left-hand panel normalized to the day 6805 (year 18.6) flux density in the 20–21 μm range.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Same as Figure 6 but for a selection of Ar and Ne lines that reveal material in the outer rings and outside the ER.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Left-hand panel: A comparison of the ER spectra extracted from the East and West regions shown in Figure 2. Right-hand panel: A comparison of the East and West spectra that have been normalized to the integrated 20–21 μm flux density of the West spectrum. The blueward shift of the broad 20 μm feature suggests that the dust temperature is higher in the West.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Same as Figure 6 but for a selection of H I lines.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Dust mass absorption coefficients for some of the common grain species. The astrodust from Hensley & Draine (2023) is shown in blue, silicates from Draine & Lee (1984) in orange, LMC carbonaceous-silicates from Weingartner & Draine (2001) in green, carbon in red (Draine & Lee 1984), and iron grains in purple.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Left-hand panel: Comparison of the [Fe II] 25.99 μm line profiles from the inner ejecta and the total line profile including the ring. The spike at -1150 km s−1 is the narrow [O IV] 25.91 μm line from the ER. Middle panel: Comparison of the line profiles of the [Fe II] 5.340 μm and [Fe II] 25.99 μm lines. Note the lack of emission between±1500 km s−1 in the 5.34 μm profile. Right-hand panel: The same for the [Ne II] 12.81 μm line.
Paper: Probing the Interplay between Jets, Winds, and Multi-phase Gas in 11 Radio-quiet PG Quasars: A uGMRT-VLA Study
Authors: Silpa S., P. Kharb, Luis C. Ho, C. M. Harrison
Figure caption: VLA 5 GHz total intensity contour image with in-band (∼4–6 GHz) spectral index image in color for PG 0923+129 (left panel). The color scale ranges from −2 to 2. The red ticks in the right panel denote the electric polarization vectors, whose lengths are proportional to fractional polarization. 1″ length of the vector corresponds to 12.5% fractional polarization. The peak contour surface brightness is 3.0 mJy beam−1 and the contour levels are 0.034×(−1, 1, 2, 4, 8, 16, 32, 64) mJy beam−1.
Paper: Probing the Interplay between Jets, Winds, and Multi-phase Gas in 11 Radio-quiet PG Quasars: A uGMRT-VLA Study
Authors: Silpa S., P. Kharb, Luis C. Ho, C. M. Harrison
Figure caption: VLA 5 GHz total intensity contour image with in-band (∼4–6 GHz) spectral index image in color for PG 0003+199 (left) and PG 0049+171 (right). The peak contour flux density is 3.3 mJy beam−1 for PG 0003+199 and 1.8 mJy beam−1 for PG 0049+171. The contour levels are 0.026 ×(−1, 1, 2, 4, 8, 16, 32, 64) mJy beam−1 for PG 0003+199, and 0.026 ×(−1, 1, 2, 4, 8, 16) mJy beam−1 for PG 0049+171. The color scale ranges from −1 to 1 for PG 0003+199 and −1.5 to 1.5 for PG 0049+171.
Paper: Probing the Interplay between Jets, Winds, and Multi-phase Gas in 11 Radio-quiet PG Quasars: A uGMRT-VLA Study
Authors: Silpa S., P. Kharb, Luis C. Ho, C. M. Harrison
Figure caption: VLA 5 GHz total intensity contour image with in-band (∼4–6 GHz) spectral index image in color for PG 1011-040 (left), PG 1119+120 (right), and PG 1211+143 (bottom). The peak contour surface brightness is is 0.6 mJy beam−1 for PG 1011-040, 0.2 mJy beam−1 for PG 1119+120, and 85.5 mJy beam−1 for PG 1211+143. The contour levels are 0.031×(−1, 1, 2, 4) mJy beam−1 for PG 1011−040, 0.025×(−1, 1, 2, 4, 8) mJy beam−1 for PG 1119+120, and 0.040×(−1, 1, 2, 4, 8, 16) mJy beam−1 for PG 1211+143. The color scale ranges from −2.5 to 2.5 for both PG 1011−040 and PG 1119+120, and −1 to 1 for PG 1211+143.
Paper: Probing the Interplay between Jets, Winds, and Multi-phase Gas in 11 Radio-quiet PG Quasars: A uGMRT-VLA Study
Authors: Silpa S., P. Kharb, Luis C. Ho, C. M. Harrison
Figure caption: VLA 5 GHz total intensity contour image with in-band (∼4–6 GHz) spectral index image in color for PG 0050+124 (left panel). The color scale ranges from −2.6 to 2.6. The red ticks in the right panel denote the electric polarization vectors, whose lengths are proportional to fractional polarization. 1″ length of the vector corresponds to 2.5% fractional polarization. The peak contour surface brightness is 2.0 mJy beam−1 and the contour levels are 0.026 ×(−1, 1, 2, 4, 8, 16, 32, 64) mJy beam−1.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Same as Figure 6 but for high-velocity line components and without the FWHM maps.
Paper: Probing the Interplay between Jets, Winds, and Multi-phase Gas in 11 Radio-quiet PG Quasars: A uGMRT-VLA Study
Authors: Silpa S., P. Kharb, Luis C. Ho, C. M. Harrison
Figure caption: VLA 5 GHz total intensity contour image with in-band (∼4–6 GHz) spectral index image in color for PG 0934+013 (left panel). The color scale ranges from −2.5 to 2.5. The red ticks in the right panel denote the electric polarization vectors, whose lengths are proportional to fractional polarization. 1″ length of the vector corresponds to 12.5% fractional polarization. The peak contour surface brightness is 0.4 mJy beam−1 and the contour levels are 0.026×(−1, 1, 2, 4, 8) mJy beam−1.
Paper: Ejecta, Rings, and Dust in SN 1987A with JWST MIRI/MRS
Authors: O. C. Jones, P. J. Kavanagh, M. J. Barlow, T. Temim, C. Fransson, J. Larsson, J. A. D. L. Blommaert, M. Meixner, R. M. Lau, B. Sargent, P. Bouchet, J. Hjorth, G. S. Wright, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Jaspers, O. Krause, L. Lenkić, O. Nayak, A. Rest, T. Tikkanen, R. Wesson, L. Colina, E. F. van Dishoeck, M. Güdel, Th. Henning, P.-O. Lagage, G. Östlin, T. P. Ray, B. Vandenbussche
Figure caption: Comparison of the continuum-subtracted line profiles of the [Fe II] 25.99 μm line with [Fe I] 1.44 μm and [Fe II] 1.53 μm lines from the inner ejecta.
Paper: Probing the Interplay between Jets, Winds, and Multi-phase Gas in 11 Radio-quiet PG Quasars: A uGMRT-VLA Study
Authors: Silpa S., P. Kharb, Luis C. Ho, C. M. Harrison
Figure caption: VLA 5 GHz total intensity contour image with in-band (∼4–6 GHz) spectral index image in color for PG 1244+026 (left panel) and PG 1426+015 (right panel). The peak contour surface brightness is 2.0 mJy beam−1 for PG 1244+026 and 0.9 mJy beam−1 for PG 1426+015. The contour levels are 0.030×(−1, 1, 2, 4, 8, 16) mJy beam−1 for PG 1244+026, and 0.055×(−1, 1, 2, 4, 8) mJy beam−1 for PG 1426+015. The color scale ranges from −3 to 2.5 for PG 1244+026 and −1.5 to 1.5 for PG 1426+015.
Paper: Probing the Interplay between Jets, Winds, and Multi-phase Gas in 11 Radio-quiet PG Quasars: A uGMRT-VLA Study
Authors: Silpa S., P. Kharb, Luis C. Ho, C. M. Harrison
Figure caption: VLA 5 GHz total intensity contour image for PG 1229+204 with in-band (∼4–6 GHz) spectral index image in color (left panel). The color scale ranges from −3 to 2.5. The peak contour surface brightness is 3.8 mJy beam−1 and the contour levels are 0.019×(−1, 1, 2, 4, 8, 16) mJy beam−1 for the top panels. The red ticks in the right panel denote the electric polarization vectors, whose lengths are proportional to fractional polarization. 1″ length of the vector corresponds to 8.3% fractional polarization. The bottom panel shows VLA 5 GHz total intensity in color and white contours overlaid on the uGMRT 685 MHz total intensity contours in red (from Silpa et al. 2020) for PG 1229+204. The contour levels are x×(1, 2, 4, 8, 16) mJy beam−1 where x is 0.080 for the uGMRT image and 0.019 for the VLA image. The color scale of the VLA image ranges from −5.28 × 10−5 to 3.32 × 10−4 Jy beam−1. Both uGMRT and VLA images detect extended emission in the same direction.
Paper: Probing the Interplay between Jets, Winds, and Multi-phase Gas in 11 Radio-quiet PG Quasars: A uGMRT-VLA Study
Authors: Silpa S., P. Kharb, Luis C. Ho, C. M. Harrison
Figure caption: uGMRT 685 MHz luminosity vs. (left) host galaxy stellar mass, and (right) BH mass, for the uGMRT-observed PG sample.
Paper: Probing the Interplay between Jets, Winds, and Multi-phase Gas in 11 Radio-quiet PG Quasars: A uGMRT-VLA Study
Authors: Silpa S., P. Kharb, Luis C. Ho, C. M. Harrison
Figure caption: Plot of 685 MHz radio core size vs. [O III]λ5007 luminosity for the uGMRT-observed PG sample