adsabs/AstroCLIMB huggingface dataset:
Paper: K2-18b Does Not Meet the Standards of Evidence for Life
Authors: Kevin B. Stevenson, Jacob Lustig-Yaeger, E. M. May, Ravi K. Kopparapu, Thomas J. Fauchez, Jacob Haqq-Misra, Mary Anne Limbach, Edward W. Schwieterman, Kristin S. Sotzen, Shang-Min Tsai
Figure caption: 1D marginalized posterior distributions for a subset of retrieval parameters on the full NIRISS/SOSS, NIRSpec/G395H, and MIRI/LRS spectrum for different choices of MIRI pixel shifts. Despite MIRI/LRS pixel shifts resulting in different preferred gases when analyzed individually, these differences are insignificant when combined with NIR data.
Paper: The NEID Earth Twin Survey. III. Survey Performance after Three Years on Sky
Authors: Arvind F. Gupta, Evan Fitzmaurice, Suvrath Mahadevan, Paul Robertson, Jacob K. Luhn, Jason T. Wright, Sarah E. Logsdon, Daniel M. Krolikowski, Leonardo A. Paredes, Chad F. Bender, Mark R. Giovinazzi, Andrea S.J. Lin, Cullen H. Blake, Caleb I. Cañas, Eric B. Ford, Samuel Halverson, Shubham Kanodia, Michael W. McElwain, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: Top panels: representative seasonal observing schedule for NEID Earth Twin Survey target stars. We schedule sets of time-sensitive observations (red; P0) to bracket the observing season, high-cadence observations (blue; P1) in the middle of each season to sample rotationally modulated stellar signals, and long-baseline observations (yellow; P2) to improve phase coverage. Bottom panels: enacted schedules for each of the first 3 yr of the survey. In gray, we show standard star observations and supplemental NETS observations, including P3 and P4, that do not strictly follow our seasonal and nightly observing schemes.
Paper: The NEID Earth Twin Survey. III. Survey Performance after Three Years on Sky
Authors: Arvind F. Gupta, Evan Fitzmaurice, Suvrath Mahadevan, Paul Robertson, Jacob K. Luhn, Jason T. Wright, Sarah E. Logsdon, Daniel M. Krolikowski, Leonardo A. Paredes, Chad F. Bender, Mark R. Giovinazzi, Andrea S.J. Lin, Cullen H. Blake, Caleb I. Cañas, Eric B. Ford, Samuel Halverson, Shubham Kanodia, Michael W. McElwain, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: Time series of relative FWHM measurements for all NETS stars with multiple nights of data collected prior to 2021 August. We observe a sharp decrease in FWHM in 2021 August for all solar-type stars, and we interpret this as a break in the RV time series necessitating the definition of a new NEID RV era prior to this date. A sharp FWHM change is also observed for HD 95735, an M dwarf, but this change does not follow that of the other stars, suggesting a chromatic dependence. Though the ΔFWHM time series for HD 170657 and HD 201091 stand out from the other solar-type stars, these variations reflect changing stellar activity levels rather than an instrumental effect.
Paper: The NEID Earth Twin Survey. III. Survey Performance after Three Years on Sky
Authors: Arvind F. Gupta, Evan Fitzmaurice, Suvrath Mahadevan, Paul Robertson, Jacob K. Luhn, Jason T. Wright, Sarah E. Logsdon, Daniel M. Krolikowski, Leonardo A. Paredes, Chad F. Bender, Mark R. Giovinazzi, Andrea S.J. Lin, Cullen H. Blake, Caleb I. Cañas, Eric B. Ford, Samuel Halverson, Shubham Kanodia, Michael W. McElwain, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: Same as Figure 5 but for the RV break between Run 1 and Run 2. Significant order-to-order variations are present for orders with wavelength solutions anchored by the ThAr calibration lamp, while all LFC orders have a zero-point change consistent with zero.
Paper: The NEID Earth Twin Survey. III. Survey Performance after Three Years on Sky
Authors: Arvind F. Gupta, Evan Fitzmaurice, Suvrath Mahadevan, Paul Robertson, Jacob K. Luhn, Jason T. Wright, Sarah E. Logsdon, Daniel M. Krolikowski, Leonardo A. Paredes, Chad F. Bender, Mark R. Giovinazzi, Andrea S.J. Lin, Cullen H. Blake, Caleb I. Cañas, Eric B. Ford, Samuel Halverson, Shubham Kanodia, Michael W. McElwain, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: NEID RV zero-point change between Run 0.5 and Run 1. We show the zero-point change as a function of spectral echelle order (a) and as a function of stellar temperature (b). No significant chromatic trends emerge.
Paper: The NEID Earth Twin Survey. III. Survey Performance after Three Years on Sky
Authors: Arvind F. Gupta, Evan Fitzmaurice, Suvrath Mahadevan, Paul Robertson, Jacob K. Luhn, Jason T. Wright, Sarah E. Logsdon, Daniel M. Krolikowski, Leonardo A. Paredes, Chad F. Bender, Mark R. Giovinazzi, Andrea S.J. Lin, Cullen H. Blake, Caleb I. Cañas, Eric B. Ford, Samuel Halverson, Shubham Kanodia, Michael W. McElwain, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: Residual CCFs for HD 185144. The average CCF profile exhibits two sharp transitions. The latter of these corresponds to the thermal cycling of NEID following the Contreras fire, but the earlier transition in summer 2021 remains unexplained. The more gradual decrease in the depth of the CCF core during Run 2 is the result of a matching decrease in the stellar activity level over that time period.
Paper: The NEID Earth Twin Survey. III. Survey Performance after Three Years on Sky
Authors: Arvind F. Gupta, Evan Fitzmaurice, Suvrath Mahadevan, Paul Robertson, Jacob K. Luhn, Jason T. Wright, Sarah E. Logsdon, Daniel M. Krolikowski, Leonardo A. Paredes, Chad F. Bender, Mark R. Giovinazzi, Andrea S.J. Lin, Cullen H. Blake, Caleb I. Cañas, Eric B. Ford, Samuel Halverson, Shubham Kanodia, Michael W. McElwain, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: Run 1 (blue) and Run 2 (red) rms RV for all NETS target stars after removing RV signals from known companions. We use ⋆ to indicate systems for which we subtracted signals from known stellar companions and • to indicate those for which we subtracted signals from known planetary companions. The majority of the stars have rms RV between 1 and 2 m s−1. We also indicate the median single-measurement precision as a black dashed line alongside the histograms for Run 1 and Run 2.
Paper: The NEID Earth Twin Survey. III. Survey Performance after Three Years on Sky
Authors: Arvind F. Gupta, Evan Fitzmaurice, Suvrath Mahadevan, Paul Robertson, Jacob K. Luhn, Jason T. Wright, Sarah E. Logsdon, Daniel M. Krolikowski, Leonardo A. Paredes, Chad F. Bender, Mark R. Giovinazzi, Andrea S.J. Lin, Cullen H. Blake, Caleb I. Cañas, Eric B. Ford, Samuel Halverson, Shubham Kanodia, Michael W. McElwain, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Ryan C. Terrien
Figure caption: Orbital periods and semiamplitudes for all known exoplanets discovered via the RV method. Planetary companions to FGK host stars are shown as green circles, and companions to M dwarfs are shown as gray squares. Planets orbiting NETS target stars that are successfully detected are highlighted with blue triangles (all with P < τ/2), and planets that we fail to independently recover are marked with orange triangles (P < τ/2) and orange circles (P > τ/2). HD 143761 d and HD 115617 d are the only planets with P < τ/2 that we fail to detect. These results suggest that the present survey sensitivity is limited by the observing baseline, not by the achieved RV precision.
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: The hydrogen line and continuum emission from a model with Te = 8000 K toward the Cygnus X region are presented. This model consists of two ionized components with electron densities of 7 cm−3 (EM2 = 1324 pc cm−6) and 500 cm−3 (EM1 = 883/η1 pc cm−6; η1 is set to 1 for the plots). Top left: the model continuum emission as a function of frequency, compared with observed data. Observed values at 408 and 1420 MHz are indicated with ±2.5σ, where the rms values (σ) are provided in Table D1. The continuum emission (TC) is modeled as the net contribution from thermal emission (Tth), nonthermal emission (Tnth), and a cosmic microwave background + extragalactic contribution of 2.8 K (see Appendix D). The thermal contributions from the individual components are shown separately. Top right: the integrated hydrogen line intensity vs. frequency, with observed data points included. The solid red line shows the total emission from the two ionized components, while dashed–dotted lines represent the emissions from the individual components. Bottom left: similar to the top right panel, but with line amplitude vs. frequency. Bottom right: the width of the Voigt line profile vs. frequency for the two components of the model.
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: Left panels: images of the integrated hydrogen line intensity at 342, 800, and 5800 MHz (from top to bottom), after masking the emission above specific cutoff values. The angular resolutions of these images are 45′, 20﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩6, and 2﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩9 at the respective frequencies. The cutoff values applied are 19, 8, and 3 K km s−1 for the three frequencies. Middle panels: histograms of the integrated intensities at 342, 800, and 5800 MHz (from top to bottom), along with the solid red line marking the cutoff values. Right panels: average spectra derived from the unmasked data at 342, 800, and 5800 MHz (from top to bottom). Gaussian models for the hydrogen, carbon, and helium lines are represented by orange, blue, and black dashed lines, respectively. A helium line is detected in the 800 MHz average spectrum, and a tentative detection of a helium line is observed in the 5800 MHz average spectrum.
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: The estimated helium-to-hydrogen ion ratio (﹩{n}_{{\rm{H}}{\rm{e}}}^{+}/{n}_{{\rm{H}}}^{+}﹩) for different observed frequencies and masking schemes. The legend indicates the symbols corresponding to each frequency. The estimated values or upper limits for ﹩{n}_{{\rm{H}}{\rm{e}}}^{+}/{n}_{{\rm{H}}}^{+}﹩, derived from both the H II region and integrated intensity masking (see Appendix B), are plotted alongside similar results obtained from the 45′ angular resolution data set. We also included the derived ﹩{n}_{{\rm{H}}{\rm{e}}}^{+}/{n}_{{\rm{H}}}^{+}﹩ values from the masked region (labeled as “From masked 45”) for comparison. The mask applied in this case is the H II region mask, and the data set used has a 45′ angular resolution. The median value of all helium line detections from the unmasked data is marked by the black dotted line, with the error bar associated with the black circle representing the IQR. For comparison, the corresponding value and its IQR toward H II regions from P. A. Shaver et al. (1983) are shown in magenta. The dashed line represents the upper limit on ﹩{n}_{{\rm{H}}{\rm{e}}}^{+}/{n}_{{\rm{H}}}^{+}﹩ from C. Heiles et al. (1996) toward the inner Galaxy DIG, while the dashed−dotted line shows the upper limit from R. J. Reynolds & S. L. Tufte (1995) toward the WIM.
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: Left: images of the integrated hydrogen line intensity at 342, 800, and 5800 MHz, after convolving and regridding the images at all three frequencies to a resolution of 45′, which matches the resolution of the 342 MHz image. Emission from H II regions is masked out in these images, with the same masking applied to all three. Right: the averaged spectra, derived from the unmasked pixels, correspond to the images shown on the left. Orange, blue, and black dashed lines represent the Gaussian models of hydrogen, carbon, and helium lines, respectively. We identified a helium line based on its velocity shift of −122 km s−1 relative to hydrogen in the averaged spectrum at 800 MHz.
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: Histogram of the difference in LSR velocities (ΔVLSR) of the hydrogen lines in the unmasked pixels. The LSR velocity differences were calculated between the observed line central velocities at pairs of frequencies, as indicated in the figure. The ΔVLSR between the 342 and 800 MHz lines is centered at 0.59 km s−1 (median value), while the differences between the 342 and 5800 MHz lines and between the 800 and 5800 MHz lines are both centered at approximately −3.0 km s−1. This shift in ΔVLSR suggests the presence of two distinct gas components: the 342 and 800 MHz emissions are dominated by one component, while the 5800 MHz emission originates from the other.
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: Left panels: images of integrated hydrogen line intensity at 342, 800, and 5800 MHz (from top to bottom) with their native angular resolution. The emissions from H II regions are masked out in these images. The angular resolutions of these images are 45′, 20﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩6, and 2﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩9 at the respective frequencies. Right panels: averaged spectra at 342, 800, and 5800 MHz (from top to bottom) derived from the unmasked pixels. Orange, blue, and black dashed lines represent the Gaussian models of hydrogen, carbon, and helium lines, respectively. The H II masking method successfully identified a helium line in the averaged spectrum at 800 MHz.
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: Similar to Figure B2, the same integrated intensity masking is applied after convolving and regridding the images at all three frequencies to a resolution of 45′, matching that of the 342 MHz image. The mask is derived from the 5800 MHz data, using a cutoff value of 0.9 K km s−1, which is indicated by the red line in the bottom middle panel.
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: Estimated ﹩{n}_{{\rm{H}}{\rm{e}}}^{+}/{n}_{{\rm{H}}}^{+}﹩ values for different polynomial baseline orders subtracted from the 800 MHz average spectrum obtained after applying H II region masking to the 45′ resolution data set.
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: The region of the sky observed toward Cygnus X in our RRL survey, overlaid on the CGPS 1420 MHz continuum image (A. R. Taylor et al. 2003). The circles represent the size of H II regions identified in the WISE survey (L. D. Anderson et al. 2014).
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: Results from two-component ionized gas models for the line emission toward the Cygnus X region. Results from the model with the same physical properties for the two gas components, referred to as the homogenous model, were also included. Left: the integrated line intensity as a function of frequency, with observed data points shown. For the homogenous model (dotted line), the electron temperature is 5000 K, the density is 20 cm−3, and the EM is 1153 pc cm−6. For the two-component model, the electron densities of the two gas components at Te = 8000 K are 7 cm−3 (EM = 1323 pc cm−6) and 1500 cm−3 (EM = 883/η1 pc cm−6). For Te = 5000 K, the densities are 7 cm−3 (EM = 692 pc cm−6) and 1500 cm−3 (EM = 461/η1 pc cm−6). The solid red line represents the total emission from the two ionized components, while the dashed–dotted lines indicate the emissions from the individual components. Right: the width of the Voigt line profile as a function of frequency for different models.
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: Results from modeling the line and continuum emission toward the Cygnus X region. The model consists of two ionized components. Left: the model continuum emission as a function of frequency, compared with observed data (see Table D1). Results for two models with electron temperatures (Te) of 8000 and 5000 K are shown. Right: the continuum, LTE line, and absolute value of the non-LTE line optical depths for the two components with Te = 8000 K as a function of frequency are shown. The two components have electron densities of 7 cm−3 (EM = 1324 pc cm−6) and 1500 cm−3 (EM = 883/η1 pc cm−6). The range of values satisfies the optically thin condition.
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: Results from a two-component ionized gas model with Te1 = 8000 K and Te2 = 5000 K for the line emission toward the Cygnus X region. Left: the model continuum emission as a function of frequency, compared with observed data. Right: the integrated line intensity as a function of frequency, with observed data points shown. The electron densities derived for the two components are ne1 = 1000 cm−3 (EM1 = 1064/η1 pc cm−6) and ne2 = 7 cm−3 (EM2 = 639 pc cm−6).
Paper: Discovery of a Nearby Habitable Zone Super-Earth Candidate Amenable to Direct Imaging
Authors: Corey Beard, Paul Robertson, Jack Lubin, Eric B. Ford, Suvrath Mahadevan, Gudmundur Stefansson, Jason T. Wright, Eric Wolf, Vincent Kofman, Vidya Venkatesan, Ravi Kopparapu, Roan Arendtsz, Rae Holcomb, Raquel A. Martinez, Stephanie Sallum, Jacob K. Luhn, Chad F. Bender, Cullen H. Blake, William D. Cochran, Megan Delamer, Scott A. Diddams, Michael Endl, Samuel Halverson, Shubham Kanodia, Daniel M. Krolikowski, Andrea S. J. Lin, Sarah E. Logsdon, Michael W. McElwain, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: GLS periodograms of GJ 251 RV data. Top: The entire data set that was used in the analysis of the system, with instrumental offsets applied (taken from Table 4). Bottom: Periodograms on the data from individual instruments. Pre-/postsplits for HIRES, HPF, and NEID have been combined after offset correction. Instruments are ordered from bluest to reddest. NEID and all-data periodograms include a red line, indicating the result when red NEID RVs are utilized. Signals of interest highlighted are at 14, 54, 68, 73, 120, and 130 days.
Paper: Discovery of a Nearby Habitable Zone Super-Earth Candidate Amenable to Direct Imaging
Authors: Corey Beard, Paul Robertson, Jack Lubin, Eric B. Ford, Suvrath Mahadevan, Gudmundur Stefansson, Jason T. Wright, Eric Wolf, Vincent Kofman, Vidya Venkatesan, Ravi Kopparapu, Roan Arendtsz, Rae Holcomb, Raquel A. Martinez, Stephanie Sallum, Jacob K. Luhn, Chad F. Bender, Cullen H. Blake, William D. Cochran, Megan Delamer, Scott A. Diddams, Michael Endl, Samuel Halverson, Shubham Kanodia, Daniel M. Krolikowski, Andrea S. J. Lin, Sarah E. Logsdon, Michael W. McElwain, Andrew Monson, Joe P. Ninan, Jayadev Rajagopal, Arpita Roy, Christian Schwab, Ryan C. Terrien
Figure caption: Science fiber flux as a function of wavelength for the GJ 251 NEID spectra taken on 2021 October 11. Each order of flux is centered around a different peak wavelength. The NEID spectrograph has 174 orders, though the instrument response is primarily meaningful for orders 52 through 174. Notable is the low S/N for the bluer orders. As an early M dwarf, GJ 251 contains most of its flux at longer wavelengths. The section highlighted in red corresponds to a peak order wavelength greater than 8000 Å. These red orders are used in our creation of “red” NEID RVs for GJ 251.
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: A plot of the reduced χ2 for the model assuming identical properties of the two gas components over the electron temperature vs. density space. The χ2 = 15 contour is shown in white.
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: A possible geometry of the two-component ionized gas (not to scale).
Paper: Detection of Helium Recombination Lines in the Cygnus X Diffuse Ionized Gas: Implications for Galactic Interstellar Medium Studies
Authors: D. Anish Roshi, J. Poojapriyatharsheni, Mayumi Sato, Kimberly L. Emig, Pedro Salas, L. D. Anderson, R. Nimma Elizabeth
Figure caption: Averaged spectra, obtained after applying H II region masking to the 45′ resolution data set, along with the Voigt profiles from the ionized gas components of the model. The temperature and density of each component are indicated in the figure.