adsabs/AstroCLIMB huggingface dataset:
Paper: Near-infrared Spectroscopy of a Massive Young Stellar Object in the Direction toward the Galactic Center: XCN and Aromatic C–D Features
Authors: Takashi Onaka, Itsuki Sakon, Takashi Shimonishi
Figure caption: Location of the Nh slit of the IRC on the IRAC three-color image of the target position (blue, IRAC band 1; green, IRAC band 2; and red, IRAC band 3). The IRAC images are taken from IRSA (2022). The Nh slit of a 30.″66 × 3″ area is depicted by the solid yellow rectangle. The numbers along the yellow rectangle indicate the position number of the extracted spectrum (see the text), increasing from −3 at the east end to +3 at the west end with an interval of 4.″38. The boundaries of the spectrum extraction windows are indicated by the yellow dashed lines. The slit center (position 0) is located at (R.A., decl. (J2000.0)) = (17:47:04.39, −28:33:21.8). The green × marks the position of IRAS 17438-2832, while the blue × and the red + indicate the positions of the Spitzer/IRAC source of SSTGC 0753438 (Ramírez et al. 2008) and 2MASS J17470424-2833204, respectively. The while + shows the position of the Hi-GAL source HIGALPB000.4901-0.0744 (Molinari et al. 2016).
Paper: Near-infrared Spectroscopy of a Massive Young Stellar Object in the Direction toward the Galactic Center: XCN and Aromatic C–D Features
Authors: Takashi Onaka, Itsuki Sakon, Takashi Shimonishi
Figure caption: Correlations of the XCN column density with (a) the Brα intensity corrected for the extinction, (b) the extinction at Brα, (c) the column density of H2O ice, (d) the column density of CO2 ice, (e) the column density of CO ice, and (f) the column density of the red-wing component. Note that the column density of the red-wing component is only relative since the band strength is not known.
Paper: Near-infrared Spectroscopy of a Massive Young Stellar Object in the Direction toward the Galactic Center: XCN and Aromatic C–D Features
Authors: Takashi Onaka, Itsuki Sakon, Takashi Shimonishi
Figure caption: The 3–4 μm spectra of two extreme cases of the column density of XCN. The black and blue lines show the observed spectrum and assumed continuum at position +2, where the column density of XCN is the largest, while the red and orange lines indicate those at position −3, where XCN is not detected with a significant level.
Paper: Near-infrared Spectroscopy of a Massive Young Stellar Object in the Direction toward the Galactic Center: XCN and Aromatic C–D Features
Authors: Takashi Onaka, Itsuki Sakon, Takashi Shimonishi
Figure caption: Column densities of XCN, CO ice, and CO ice along the slit for three cases of the Pfβ intensity estimate. The estimates of the column densities of (a) XCN, (b) CO ice, and (c) CO gas are plotted against the slit position. The standard cases are shown by the red circles, while the results of no extinction correction (minimum Pfβ) are indicated by the green diamonds. The maximum Pfβ cases (addition of 3σ uncertainty) are indicated by the blue triangles. The results of the three cases are slightly shifted horizontally to avoid overlapping.
Paper: Near-infrared Spectroscopy of a Massive Young Stellar Object in the Direction toward the Galactic Center: XCN and Aromatic C–D Features
Authors: Takashi Onaka, Itsuki Sakon, Takashi Shimonishi
Figure caption: Observed Pfγ intensity at 3.74 μm against the predicted intensity from the observed Brα intensity and the estimated extinction. The predicted intensity takes account of the foreground extinction as well as the extinction due to the red-wing component of H2O ice. The dashed line shows a line with a slope of unity. Only upper limits are given for the observed intensity at some positions.
Paper: Near-infrared Spectroscopy of a Massive Young Stellar Object in the Direction toward the Galactic Center: XCN and Aromatic C–D Features
Authors: Takashi Onaka, Itsuki Sakon, Takashi Shimonishi
Figure caption: Enlarged portion of the 4.4 μm region spectra to show the 4.4 μm excess after subtracting a linear baseline between 4.37 and 4.45 μm. At position 0, the excess is not detected with a significant level.
Paper: X-Ray Spectral Analysis of the Jet Termination Shock in Pictor A on Subarcsecond Scales with Chandra
Authors: R. Thimmappa, Ł. Stawarz, J. Neilsen, M. Ostrowski, B. Reville
Figure caption: Left panel: HR map of the W hot spot in Pictor A, corresponding to the combined deconvolved Chandra images with 0.5 px resolution (combined ObsIDs 3090 and 4369); white contours denote the total Chandra intensity, based similarly on deconvolved images with 0.5 px resolution. Right panel: the corresponding standard deviation (σ) of the HR value, again with the total intensity contours superimposed.
Paper: X-Ray Spectral Analysis of the Jet Termination Shock in Pictor A on Subarcsecond Scales with Chandra
Authors: R. Thimmappa, Ł. Stawarz, J. Neilsen, M. Ostrowski, B. Reville
Figure caption: Left panel: black solid curves denote the values of the photon index Γ, corresponding to different values of the 0.5–7.0 keV HR, assuming Galactic column density N H,Gal = 3.6 × 1020 cm−2. Dark-gray and gray regions in between the dashed and dotted curves denote, respectively, the ±0.1 and ±0.2 statistical uncertainty in HR. The canonical shock-type index Γ = 1.5, corresponds to the HR value of ≃ − 0.56 (thin solid lines in the panel). Right panel: the resulting 0.5–7.0 keV photon index map corresponding to the 0.5 px resolution HR map presented in the left panel of Figure 5, obtained assuming Galactic column density N H,Gal = 3.6 × 1020 cm−2.
Paper: X-Ray Spectral Analysis of the Jet Termination Shock in Pictor A on Subarcsecond Scales with Chandra
Authors: R. Thimmappa, Ł. Stawarz, J. Neilsen, M. Ostrowski, B. Reville
Figure caption: Deconvolved images of the W hot spot in Pictor A, in the soft 0.5–2.5 keV and hard 2.5–7.0 keV bands (left and right panels, respectively), for ObsID 3090 and ObsID 4369 (top and bottom panels, respectively). Each image corresponds to the average over 50 PSF simulations with 0.5 px resolution.
Paper: X-Ray Spectral Analysis of the Jet Termination Shock in Pictor A on Subarcsecond Scales with Chandra
Authors: R. Thimmappa, Ł. Stawarz, J. Neilsen, M. Ostrowski, B. Reville
Figure caption: Examples of simulated PSF images for ObsID 3090 in the soft and hard bands (left and right panels, respectively), with 0.5 px resolution.
Paper: X-Ray Spectral Analysis of the Jet Termination Shock in Pictor A on Subarcsecond Scales with Chandra
Authors: R. Thimmappa, Ł. Stawarz, J. Neilsen, M. Ostrowski, B. Reville
Figure caption: The 0.5–2.0 keV and 2.5–7.0 keV spectra of the entire (20 px radius) W hot spot of Pictor A, for ID 3090 (top) and 4369 (bottom), fitted with a single power-law model modified by the Galactic absorption (solid curves), along with the residuals.
Paper: X-Ray Spectral Analysis of the Jet Termination Shock in Pictor A on Subarcsecond Scales with Chandra
Authors: R. Thimmappa, Ł. Stawarz, J. Neilsen, M. Ostrowski, B. Reville
Figure caption: ECF as a function of the aperture radius for all 50 of the simulated PSFs in the soft and hard bands (left and right panels), ObsID 3090. The horizontal green, blue, and red lines correspond to 1σ, 2σ, and 3σ ECFs, respectively.
Paper: X-Ray Spectral Analysis of the Jet Termination Shock in Pictor A on Subarcsecond Scales with Chandra
Authors: R. Thimmappa, Ł. Stawarz, J. Neilsen, M. Ostrowski, B. Reville
Figure caption: Low-energy (0.5–2.0 keV) deconvolved intensity contours (at 0.5 px resolution) of the quasar B2251+134, superimposed on the event file (top left), the deconvolved soft image (top right), the deconvolved hard image (bottom left), and the averaged HR map (bottom right).
Paper: X-Ray Spectral Analysis of the Jet Termination Shock in Pictor A on Subarcsecond Scales with Chandra
Authors: R. Thimmappa, Ł. Stawarz, J. Neilsen, M. Ostrowski, B. Reville
Figure caption: Low-energy (0.5–2.0 keV) deconvolved intensity contours (at 0.5 px resolution) of the blazar AO 0235+16, superimposed on the event file (top left), the deconvolved soft image (top right), the deconvolved hard image (bottom left), and the averaged HR map (bottom right).
Paper: First Detection of the Molecular Cloud Population in the Extended Ultraviolet Disk of M83
Authors: Jin Koda, Linda Watson, Françoise Combes, Monica Rubio, Samuel Boissier, Masafumi Yagi, David Thilker, Amanda M Lee, Yutaka Komiyama, Kana Morokuma-Matsui, Celia Verdugo
Figure caption: (a) GALEX FUV and NUV-band color composite image. The inner (green) and outer (cyan) contours are the edge of the optical disk and the extent of H I gas at an H I surface density of 1.5 × 1020 cm−2 (see Koda et al. 2012b). The red box is the 1.′5 × 3′ (2.0 × 3.9 kpc2) field from the ALMA CO(J = 2–1) observations (Bicalho et al. 2019). The three panels on the right are zoom-ins to the CO(2−1) field: (b) the GALEX color composite, as in panel (a), (c) the continuum-subtracted Hα image from the Subaru telescope, and (d) the H I 21 cm emission image from Walter et al. (2008). The area of our CO(3−2) observations is indicated by the inner magenta box of ∼0.′75 × 0.′85 (∼0.98 × 1.11 kpc2). The bottom two panels are zoom-ins to the CO(3−2) field: (e) the Hα image with visually identified H II regions (circles); (f) the same as (e), but on the GALEX color composite. Panels (e), (f), and Figures 2, 3, and 7 show the same region, and their coordinates are written explicitly in Figures 2 and 3.
Paper: First Detection of the Molecular Cloud Population in the Extended Ultraviolet Disk of M83
Authors: Jin Koda, Linda Watson, Françoise Combes, Monica Rubio, Samuel Boissier, Masafumi Yagi, David Thilker, Amanda M Lee, Yutaka Komiyama, Kana Morokuma-Matsui, Celia Verdugo
Figure caption: (a) CO(3−2) integrated intensity map. (b) CO(3−2) peak intensity map. (c) Band 7 (349 GHz) continuum map. (d) Molecular clouds on the CO(3−2) peak intensity map. Cloud IDs are indicated and correspond to the ones in Table 3. Each circle has a diameter of 2″. The beam size of 0.″96 × 0.″82 (PA = −84.°7) is shown in the bottom left corner, corresponding to 21 × 18 pc2 at 4.5 Mpc.
Paper: First Detection of the Molecular Cloud Population in the Extended Ultraviolet Disk of M83
Authors: Jin Koda, Linda Watson, Françoise Combes, Monica Rubio, Samuel Boissier, Masafumi Yagi, David Thilker, Amanda M Lee, Yutaka Komiyama, Kana Morokuma-Matsui, Celia Verdugo
Figure caption: Schematic illustrations of the physical and chemical structures of a molecular cloud (a) in a high-metallicity environment and (b) in a low-metallicity environment. The physical structures (i.e., mass distribution and SF activity) are common between (a) and (b), but their chemical structures (i.e., CO abundances) are different. The ambient radiation penetrates into the cloud, dissociates CO molecules in the cloud’s outer layers, and makes them CO-deficient and CO-dark, while more abundant H2 molecules can self-shield themselves and remain (gray). These CO-dark layers thicken at low metallicity, since a lower dust abundance results in less efficient extinction and allows the radiation to penetrate deeper into the cloud (e.g., Maloney & Black 1988; van Dishoeck & Black 1988). Still, the CO molecules can remain near the cloud center (orange). We hypothesize that the dense clumps (brown), often associated with SF (yellow), are located at the heart of the cloud and likely remain intact with abundant CO molecules. The CO(3−2) emission originates from the dense clump region.
Paper: First Detection of the Molecular Cloud Population in the Extended Ultraviolet Disk of M83
Authors: Jin Koda, Linda Watson, Françoise Combes, Monica Rubio, Samuel Boissier, Masafumi Yagi, David Thilker, Amanda M Lee, Yutaka Komiyama, Kana Morokuma-Matsui, Celia Verdugo
Figure caption: (a) Subaru Hα image at a resolution of about 1″. (b) GALEX FUV and NUV-band color composite image at a resolution of about 5″ (Gil de Paz et al. 2007a). (c) VLA + GBT H I 21 cm image (grayscale) with contours—from the brightest—at 0.30, 0.25, 0.20, 0.15, 0.10, and 0.05 Jy beam−1  km s−1 with the 15″ beam. The brightest contour corresponds to the H I surface density of ∼12 M ⊙  pc−2 (and 16 M ⊙  pc−2 for H I + He). Magenta circles denote the H II regions identified by eye with the labels “A,” “B,” “C,” .... The Hα luminosities ﹩{L}_{{\rm{H}}\alpha }﹩ enclosed within each circle are listed in Table 2. Blue or yellow circles are molecular clouds and are the same as the ones in Figure 2(d) with the labels “1,” “2,” “3,” ....
Paper: First Detection of the Molecular Cloud Population in the Extended Ultraviolet Disk of M83
Authors: Jin Koda, Linda Watson, Françoise Combes, Monica Rubio, Samuel Boissier, Masafumi Yagi, David Thilker, Amanda M Lee, Yutaka Komiyama, Kana Morokuma-Matsui, Celia Verdugo
Figure caption: Postage stamp images of individual clouds. Only the pixels with >3σ emission in the data cube are used for these images. The peaks at the center of each image are the clouds of interest. Surrounding clouds, when they exist, are also in the images. Top: integrated intensity maps in units of Jy beam−1  km s−1. Bottom: peak intensity maps in units of Jy beam−1. The hatched ellipses in the bottom left corners indicate the beam size.
Paper: First Detection of the Molecular Cloud Population in the Extended Ultraviolet Disk of M83
Authors: Jin Koda, Linda Watson, Françoise Combes, Monica Rubio, Samuel Boissier, Masafumi Yagi, David Thilker, Amanda M Lee, Yutaka Komiyama, Kana Morokuma-Matsui, Celia Verdugo
Figure caption: CO(3−2) spectra of the clouds produced with the 1 km s−1 cube. The spatial pixels and volume that each cloud occupies in the (R.A., decl., velocity) space are determined with the 2.54 km s−1 cube. The gray spectra show the sum over all the spatial pixels including noises in each 1 km s−1 channel. The red spectra include only the pixels with >3σ emission in the cloud volume.
Paper: First Detection of the Molecular Cloud Population in the Extended Ultraviolet Disk of M83
Authors: Jin Koda, Linda Watson, Françoise Combes, Monica Rubio, Samuel Boissier, Masafumi Yagi, David Thilker, Amanda M Lee, Yutaka Komiyama, Kana Morokuma-Matsui, Celia Verdugo
Figure caption: Plot of cloud radius vs. velocity dispersion. M83 XUV clouds are blue (and the blue arrows are the upper limits in radius, while they are resolved in velocity). Reference points in the background are for the MW’s inner disk (Solomon et al. 1987), outer disk (r gal ∼ 12–14 kpc; Sun et al. 2017), and far outer disk (∼14–22 kpc; Sun et al. 2015), and for the Large and Small Magellanic Clouds (Bolatto et al. 2008; Wong et al. 2011) and the galaxy WLM (Rubio et al. 2015). The solid line is a fit to the inner disk clouds (Solomon et al. 1987).
Paper: First Detection of the Molecular Cloud Population in the Extended Ultraviolet Disk of M83
Authors: Jin Koda, Linda Watson, Françoise Combes, Monica Rubio, Samuel Boissier, Masafumi Yagi, David Thilker, Amanda M Lee, Yutaka Komiyama, Kana Morokuma-Matsui, Celia Verdugo
Figure caption: CO(3−2) channel maps with the field of view of the ALMA observations outlined. Channel velocities are shown in the bottom left corner. The rms noise is 0.96 mJy beam−1 in the 2.54  km s−1 channel, and the contours are at 3σ, 5σ, 8σ, 12σ, and 17σ significance.
Paper: Observations of Quiescent Solar Wind Regions with Near-f ce Wave Activity
Authors: Benjamin Short, David M. Malaspina, Jasper Halekas, Orlando Romeo, J. L. Verniero, Adam J. Finley, Justin C. Kasper, Ali Rahmati, Stuart D. Bale, John W. Bonnell, Anthony W. Case, Thierry Dudok de Wit, Keith Goetz, Katherine Goodrich, Peter R. Harvey, Kelly E. Korreck, Davin Larson, Roberto Livi, Robert J. MacDowall, Marc Pulupa, Michael L. Stevens, Phyllis Whittlesey
Figure caption: 2D histograms of magnetic field unit vectors and deflection angle from a nominal Parker spiral. Figure 3(a) shows the R component of the magnetic field unit vector in RTN coordinates. 3(b) shows the T component. 3(c) shows the N component. Figure 3(d) shows the angle that the magnetic field unit vector makes with respect to a theoretical Parker spiral. Counts are given in log scale to highlight changes in variance. SPC velocity values are used to calculate the Parker spiral for Encounter 1.
Paper: Observations of Quiescent Solar Wind Regions with Near-f ce Wave Activity
Authors: Benjamin Short, David M. Malaspina, Jasper Halekas, Orlando Romeo, J. L. Verniero, Adam J. Finley, Justin C. Kasper, Ali Rahmati, Stuart D. Bale, John W. Bonnell, Anthony W. Case, Thierry Dudok de Wit, Keith Goetz, Katherine Goodrich, Peter R. Harvey, Kelly E. Korreck, Davin Larson, Roberto Livi, Robert J. MacDowall, Marc Pulupa, Michael L. Stevens, Phyllis Whittlesey
Figure caption: Demonstration of the wave-finding algorithm. Figure 2(a) shows the V12 AC spectrogram from 2020-01-29/10:00:00 to 2020-01-29/11:00:00 UTC. At roughly 10:40:00, there is significant wave power near f ce. This set of wave power is an ideal example of the spectra we are looking for. Generally, there are two or more frequency bands that occur at the same time, roughly at 0.7 and 1 f ce. Figure 2(b) shows the output of the island-locating routine. Figure 2(c) shows the island output after a 7 s time filter is applied. Figure 2(d) shows the island output after the frequency threshold of ≥0.5 f ce is applied. These limitations of wave frequency are discussed in Malaspina et al. (2020).
Paper: Observations of Quiescent Solar Wind Regions with Near-f ce Wave Activity
Authors: Benjamin Short, David M. Malaspina, Jasper Halekas, Orlando Romeo, J. L. Verniero, Adam J. Finley, Justin C. Kasper, Ali Rahmati, Stuart D. Bale, John W. Bonnell, Anthony W. Case, Thierry Dudok de Wit, Keith Goetz, Katherine Goodrich, Peter R. Harvey, Kelly E. Korreck, Davin Larson, Roberto Livi, Robert J. MacDowall, Marc Pulupa, Michael L. Stevens, Phyllis Whittlesey
Figure caption: 1D Histograms constructed by integrating along the time axis of Figure 3. Figure 5(a) is the ﹩\hat{R}﹩ component of the unit vector. Figure 5(b) is the ﹩\hat{T}﹩ component. Figure 5(c) is the ﹩\hat{N}﹩ component. Figure 5(d) is the Parker deflection angle. SPC velocity values are used to calculate the Parker spiral for Encounter 1.
Paper: Observations of Quiescent Solar Wind Regions with Near-f ce Wave Activity
Authors: Benjamin Short, David M. Malaspina, Jasper Halekas, Orlando Romeo, J. L. Verniero, Adam J. Finley, Justin C. Kasper, Ali Rahmati, Stuart D. Bale, John W. Bonnell, Anthony W. Case, Thierry Dudok de Wit, Keith Goetz, Katherine Goodrich, Peter R. Harvey, Kelly E. Korreck, Davin Larson, Roberto Livi, Robert J. MacDowall, Marc Pulupa, Michael L. Stevens, Phyllis Whittlesey
Figure caption: This figure is identical to Figure 5, with the exception that only Encounter 1 is included. Figure 6(a) is the ﹩\hat{R}﹩ component of the unit vector. Figure 6(b) is the ﹩\hat{T}﹩ component. Figure 6(c) is the ﹩\hat{N}﹩ component. Figure 6(d) is the deflection angle. SPC velocity values are used to calculate the Parker spiral for Encounter 1.
Paper: Observations of Quiescent Solar Wind Regions with Near-f ce Wave Activity
Authors: Benjamin Short, David M. Malaspina, Jasper Halekas, Orlando Romeo, J. L. Verniero, Adam J. Finley, Justin C. Kasper, Ali Rahmati, Stuart D. Bale, John W. Bonnell, Anthony W. Case, Thierry Dudok de Wit, Keith Goetz, Katherine Goodrich, Peter R. Harvey, Kelly E. Korreck, Davin Larson, Roberto Livi, Robert J. MacDowall, Marc Pulupa, Michael L. Stevens, Phyllis Whittlesey
Figure caption: Example of a wave-active quiescent region. Figure 1(a) contains the V12 AC Spectrum of a wave-active quiescent region. Figure 1(b) is a plot of the magnetic field vector ﹩\vec{{\boldsymbol{B}}}﹩. It is observed that, during the interval with wave power, the magnetic field appears to take on particular characteristics. It has been shown that these intervals are associated with times of near-radial magnetic field with low levels of magnetic turbulence. It is these characteristics and their limits that this study seeks to explore.
Paper: Observations of Quiescent Solar Wind Regions with Near-f ce Wave Activity
Authors: Benjamin Short, David M. Malaspina, Jasper Halekas, Orlando Romeo, J. L. Verniero, Adam J. Finley, Justin C. Kasper, Ali Rahmati, Stuart D. Bale, John W. Bonnell, Anthony W. Case, Thierry Dudok de Wit, Keith Goetz, Katherine Goodrich, Peter R. Harvey, Kelly E. Korreck, Davin Larson, Roberto Livi, Robert J. MacDowall, Marc Pulupa, Michael L. Stevens, Phyllis Whittlesey
Figure caption: Cartoon depicting magnetic field angles relative to ﹩\hat{{\boldsymbol{R}}}﹩ unit vector. ﹩{\hat{{\boldsymbol{B}}}}_{{arbitrary}}﹩ and θ arb are arbitrary vectors and angles drawn to demonstrate angles in this coordinate system.
Paper: Self-ionizing Galactic Winds
Authors: Kartick C. Sarkar, Amiel Sternberg, Orly Gnat
Figure caption: Observable emission spectra at different impact parameters, b = 0 (left panel) and 1 kpc (right panel). The spectra are considered to be absorbed by the Galactic ISM at temperature 8000 K with column density 2 × 1021 cm2. Nonequilibrium/self-radiation signatures are clearly observable for several lines, such as O VII, O VIII, Fe XVII etc. and corresponding free–bound continuum.
Paper: Self-ionizing Galactic Winds
Authors: Kartick C. Sarkar, Amiel Sternberg, Orly Gnat
Figure caption: Oxygen ion fractions for different runs at 28 Myr, when the wind has reached a steady state. The left panel shows ion fractions for O III and O VIII, whereas the right panel shows results for O IV and O VI. Different line styles show the results for the PIE (dotted), PIE-SR (dashed–dotted), NEI (dashed), and NEI-SR (solid) runs. As a general mnemonic, included physics increases going from dotted to solid curves.
Paper: Self-ionizing Galactic Winds
Authors: Kartick C. Sarkar, Amiel Sternberg, Orly Gnat
Figure caption: Left: Ratio of line intensities of two oxygen lines, O VIII (18.97 Å) and O VII (22.1012 Å + 21.6020 Å + 21.8070 Å). Different line styles represent different simulations. The gray part of each line represents the region where the O VII (22.1012 Å + 21.6020 Å + 21.8070 Å) intensity falls below 10−5 of the central (b  =  0) value. This low-intensity region is not expected to be observed. Right: “Observable density” ratio (Equation (21)) of PIE-SR, NEI, and NEI-SR with respect to the PIE case. The gray parts of the lines represent the region when the “observable density” in PIE case is lower than 10−5 × its central value.
Paper: Self-ionizing Galactic Winds
Authors: Kartick C. Sarkar, Amiel Sternberg, Orly Gnat
Figure caption: Radiation spectra inside the wind (same as Figure 3 but with ISM absorption). Top panel: evolution of the spectrum. The solid red line represents the unabsorbed spectra at t  =  28 Myr. The predicted ISM spectra (24) are shown in gray solid line. The reduction of the radiation field is due to absorption from ISM (corresponding to N H = 2 × 1021 cm−2, T = 8000 K) uniformly distributed within the star-forming region. Bottom panel: total number of photons with energy > E. The solid gray lines show the final spectra (at t  =  28 Myr) for the unabsorbed case.
Paper: Self-ionizing Galactic Winds
Authors: Kartick C. Sarkar, Amiel Sternberg, Orly Gnat
Figure caption: Ionization parameter for O VI (ionization potential = 138 eV) at steady state for PIE (dotted line) and for PIE-SR runs (dashed–dotted line). The sharp rise in ionization parameter in PIE case happens due to the sharp decrease of the overall density. The ionization parameter remains roughly constant for the PIE-SR case as both the density and radiation field decreases as ∼ 1/r 2.
Paper: Self-ionizing Galactic Winds
Authors: Kartick C. Sarkar, Amiel Sternberg, Orly Gnat
Figure caption: Column density for oxygen ions at t = 28 Myr as a function of the impact parameter (b) from the center of the star formation injection region. Different line styles represent different simulations: PIE (dotted), PIE-SR (dashed–dotted), NEI (dashed), and NEI-SR (solid).
Paper: Self-ionizing Galactic Winds
Authors: Kartick C. Sarkar, Amiel Sternberg, Orly Gnat
Figure caption: Ion fractions of O III and O VIII in the wind (same as Figure 4) but shows results for simulations containing ISM absorption (thick solid lines). Different line styles represent different simulations—dotted: PIE, dashed: NEI, dashed–dotted: PIE-SR, and solid: NEI-SR.