adsabs/AstroCLIMB huggingface dataset:
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Model and observed spectra of V883 Ori in the H and K band, along with eight selected lines. The H-band model spectrum is shifted down by 0.075.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Flowchart showing the process of the FUor fits. The parameters summarized in Table 1 are in green rounded rectangles, and the spectrophotometric input data in blue boxes. Only the photometry is quantitatively used for the χ 2 fitting. Equations and models relevant to each step are annotated in bold. Blue arrows indicate processes, and orange ones on the right are collections of best-fit parameters. The stellar distance d * is only adopted from previous studies but not examined here, hence shown in gray.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Components of M * = 0.3 M ⊙ model spectra across different accretion rates. High accretion rates (e.g., 10−5 M ⊙ yr−1) crush the magnetosphere and eliminate magnetospheric accretion, while low accretion rates (e.g., 10−8 M ⊙ yr−1) fail to heat up the disk viscously. The dust disk component mainly contributes to the continuum in the near-IR. The magnetospheric accretion, when existent, affords optical excess to the SED. Line features vary from predominantly disk-sourced (high ﹩\dot{M}﹩) to photosphere-sourced (low ﹩\dot{M}﹩).
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Observed data and best-fit models of the SEDs of three FUors: FU Ori (upper left), HBC 722 (bottom left), and V883 Ori (R  V  = 3.1, upper-right and R  V  = 4.3, lower-right; see the text in Section 4.2).
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Model and observed spectra of FU Ori in the H and K band, along with eight selected lines.
Paper: Diagnosing FU Ori-like Sources: The Parameter Space of Viscously Heated Disks in the Optical and Near-infrared
Authors: Hanpu Liu, Gregory J. Herczeg, Doug Johnstone, Carlos Contreras-Peña, Jeong-Eun Lee, Haifeng Yang, Xingyu Zhou, Sung-Yong Yoon, Ho-Gyu Lee, Masanobu Kunitomo, Jessy Jose
Figure caption: Model spectra of different T 0. For visualization, the spectra are convolved to lower resolution. Higher T 0 helps to raise the SED, especially in the redder zones in the K band, and veils the CO bandhead lines (enlarged on the lower-right). Other parameters are held constant at M * = 0.3 M ⊙, ﹩\dot{M}=1\,\times \,{10}^{-7}{M}_{\odot }﹩ yr−1, i = 45°, and A  V  = 10 mag.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Left: Integrated (total) colors of candidate star-forming regions in each cloud (top: [3.4]–[4.6], middle: [4.6]–[12], bottom: [4.6]–[22]) plotted against Galactocentric radius (R G). Red circles and yellow squares show clouds with candidates with respective contamination rates of their parental clouds of <30% (reliable) and ≥30% (less reliable). The sizes of these markers indicate the respective masses of their parental molecular clouds (small: M ⊙ ≤ M CO <103 M ⊙, middle: 103 M ⊙ ≤ M CO <104 M ⊙, large: 104 M ⊙ ≤ M CO). The gray lines show our identification criteria for candidates with WISE data: [3.4]–[4.6] ≥ 0.5 and [4.6]–[12] = 0.5–2.0 (Paper I). The number ratios of the reddened candidates (top: [3.4]–[4.6] > 1.5, middle: [4.6]–[12] > 4.0, bottom: [4.6]–[22] > 7.0) per total star-forming regions are presented at the bottom of each color distributions (magenta: all candidates, red: only candidates with contamination rate of <30%). The error bars represent Poisson errors (1σ). The gray dotted lines show the threshold for the reddened candidates. The gray areas indicate the concentrated areas considered to be spiral arms. Right: Individual colors of candidate star-forming regions plotted against cloud mass. Notations are the same as in the left panels.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Top: Galactocentric radius variation of fraction of molecular clouds with candidate star-forming regions (N SF/N all) for clouds with M CO ≥ 183.6 M ⊙. The magenta squares and red circles show all the clouds with candidates and only clouds with reliable candidates, respectively. The error bars represent Poisson errors (1σ). The magenta and red dotted lines show the results of least-squares fittings: N SF/N all = 5.8(±2.5)R G –52.3(±36.5) (magenta: all clouds with candidates) and N SF/N all = 6.2(±2.1)R G –64.0(±31.0) (red: only clouds with reliable candidates), respectively. Bottom: Galactocentric radius variation of the number clouds with and without candidates. The red and orange bars show the respective numbers of clouds with candidates with contamination rates of <30% (reliable) and ≥30% (less reliable). The white bars show the numbers of clouds without candidates. Only clouds with M CO ≥ 183.6 M ⊙ are plotted. The gray areas indicate the concentrated areas considered to be spiral arms.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Top: Relation between virial mass (M vir) and mass derived from CO intensity (M CO). Red circles and yellow squares show clouds with associated candidate star-forming regions with a contamination rate of their parental clouds of <30% (reliable) and ≥30% (less reliable), respectively. Black open circles show clouds without associated star-forming regions. The gray dotted line shows the M vir = M CO relation. The vertical gray dotted–dashed line indicates the mass threshold (183.6 M ⊙). The arrows indicate the upper limit (using dv = 0.98 km s−1) for 277 clouds for which the linewidths are not derived in the BKP catalog. Bottom: Relation between completeness of M vir (number of clouds whose linewidth is derived / total number of clouds) and M CO. The error bars represent Poisson errors (1σ).
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Left: Integrated (total) monochromatic luminosity of candidate star-forming regions in each cloud plotted against cloud mass. Red circles and yellow squares show clouds with candidates with respective contamination rates of their parental clouds of <30% (reliable) and ≥30% (less reliable). The cyan and blue lines show the flux densities for A0 and B0 stars in the main sequence (Cox 2000). Note that we used intrinsic V − L colors (V band: 0.5555  μm;  L band: 3.547 μm) and the absolute V-band magnitudes of A0 and B0 stars for calculating the apparent magnitudes of those stars for any of the four bands, since infrared colors, such as [3.4]–[22], are negligible for those early-type stars. The blue dashed line shows the 22 μm flux density for an H II region ionized by a B0 star (Anderson et al. 2014). The gray dashed lines show the completeness limit of cloud detection (183.6 M ⊙). Right: Individual monochromatic luminosity of candidate star-forming regions plotted against cloud mass. Notations are the same as in the left panels.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Size–linewidth relation of all BKP clouds in the outer Galaxy. Black open circles show clouds without associated star-forming regions. Red circles and yellow squares show clouds with associated candidate star-forming regions with respective contamination rates of their parental clouds of <30% (reliable) and ≥30% (less reliable). The arrows indicate the upper limit (dv = 0.98 km s−1) for 277 clouds for which the linewidths are not derived in the BKP catalog. The gray solid and black dashed lines show the respective results of the least-squares fitting through the outer Galaxy data (R G ≳16 kpc), dv = (0.94 ± 0.08)r 0.53±0.03, and through the inner Galaxy data, dv = (1.75 ± 0.24)r 0.48±0.04, from Brand & Wouterloot (1995). The blue dotted line shows the result of the least-squares fitting through data of dwarf galaxies including the SMC, LMC, and Wolf–Lundmark–Melotte (WLM): dv = (0.94 ± 0.07)r 0.52±0.03 from Rubio et al. (2015).
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Distribution of BKP clouds beyond R G of 13.5 kpc. Red circles and yellow squares show clouds with associated candidate star-forming regions with respective contamination rates of their parental clouds of <30% (reliable) and ≥30% (less reliable). Black open circles show clouds without associated candidates. The sizes of these markers indicate the cloud masses (larger sizes correspond to larger masses). The black dotted–dashed lines indicate the area of the FCRAO survey (102°.49 ≤ l ≤ 141°.54). The gray dotted curves indicate the R G of 8.5, 13.5, 16.0, and 18.0 kpc. Note that the two molecular clouds with kinematic distances of more than 20 kpc (R G  > 27 kpc) are known to be actually located at a distance of 12 kpc (R G = 19 kpc) based on high-resolution optical spectra (e.g., Smartt et al. 1996; Kobayashi et al. 2008).
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: (a): Relation between cloud mass derived from CO intensity (M CO) and cloud size (radius; r) of BKP clouds in the outer Galaxy. Red circles and yellow squares show clouds with associated candidate star-forming regions with a respective contamination rates of their parental clouds of <30% (reliable) and ≥30% (less reliable). Black open circles show clouds without associated candidates. The gray dashed line shows the mass threshold (183.6 M ⊙) for comparison of cloud properties at various distances up to R G = 20.0 kpc. (b): Number distribution of cloud size (r). (c): Number distribution of cloud mass (M CO). The black histograms show the number distribution of clouds without candidates. The magenta and red histograms are the respective number distributions of clouds with all associated candidates and those with only reliable associated candidates.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Left: WISE colors of 121 integrated (total) candidate star-forming regions in each parental cloud (top: [3.4]–[4.6], middle: [4.6]–[12], bottom: [4.6]–[22]) plotted against cloud mass. Red circles and yellow squares show clouds with associated star-forming regions with respective contamination rates of their parental clouds of <30% (reliable) and ≥30% (less reliable). The gray lines show our identification criteria for star-forming regions with WISE data: [3.4]–[4.6] ≥ 0.5 and [4.6]–[12] = 0.5–2.0 (Paper I). The gray dashed lines show the completeness limit of cloud detection (183.6 M ⊙). Correlation coefficients (CC) are noted in the top left corners. Right: WISE colors of 288 individual candidate star-forming regions plotted against cloud mass. Notations are the same as in the left panels.
Paper: Star Formation Activity beyond the Outer Arm. II. Distribution and Properties of Star Formation
Authors: Natsuko Izumi, Naoto Kobayashi, Chikako Yasui, Masao Saito, Satoshi Hamano, Patrick M. Koch
Figure caption: Number distributions of cloud mass (M CO). The blue and green histograms show the respective number distributions of clouds in the ranges R G = 13.5–14.5 kpc (arm-1) and 15.5–17.0 kpc (arm-2). The black histogram shows the number distribution of clouds in the other area (interarm area). The gray dashed line shows the mass threshold (183.6 M ⊙) for comparison of cloud properties at various distances up to R G = 20.0 kpc.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption:  Pα for various models, in which only the stellar Lyα source is considered. (a) H/He = 92/8, F XUV = F 0, β  m  = 0.22; (b) H/He = 92/8, F XUV = 8F 0, β  m  = 0.22; (c) H/He = 92/8, F XUV = F 0, β  m  = 0.5; (d) H/He = 99.5/0.5, F XUV = F 0, β  m  = 0.22. Note that in panels (b)–(d) the value of Pα is slightly larger than 30 in the gray region near the edge.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: Atmosphere structures for models with various F XUV when H/He = 92/8, β  m  = 0.22. Here r denotes the altitude (the radial distance from the planet center) and r obs is the projected distance onto a plane perpendicular to the z-axis.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: The radial profiles of the source (solid lines) and sink (dashed lines) terms for H(2p) in the model of H/He = 92/8, F XUV = F 0, and β  m  = 0.22. The black dotted line represents the absolute value of the advection term ﹩\tfrac{1}{{r}^{2}}\tfrac{\partial }{\partial r}({r}^{2}{n}_{2p}v)﹩. From top to bottom, the figure shows the cases of the dayside where r cyl = 0, the terminator where z = 0, and the nightside where r cyl = 0, respectively. In each panel, the three-body recombination term ﹩{\beta }_{2p}{n}_{e}^{2}{n}_{{{\rm{H}}}^{+}}﹩ is so small that the line representing this term does not appear in the plot.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: Heating and cooling rates for the model of H/He = 92/8, F XUV = F 0, and β  m  = 0.22. The total cooling rate plotted with the blue dotted line is the sum of the cooling rate by Lyα, H3 +, recombination radiation, and free–free emission.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: Schematic of Hα and He 10830 radiative transfer. In the bottom panel, the radial velocity is decomposed of two orthogonal components V  x  and V  y , where V  x  causes the Doppler shift along the line of sight.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption:  Pα for various models, in which only the planetary Lyα source is considered. (a) H/He = 92/8, F XUV = F 0, β  m  = 0.22; (b) H/He = 92/8, F XUV = 8F 0, β  m  = 0.22; (c) H/He = 92/8, F XUV = F 0, β  m  = 0.5; (d) H/He = 99.5/0.5, F XUV = F 0, β  m  = 0.22.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: Atmosphere structures for models with various β  m  when H/He = 92/8, F XUV = F 0.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: Variation of the atmosphere structures with H/He ratio when F XUV = F 0 and β  m  = 0.22.
Paper: Modeling the Hα and He 10830 Transmission Spectrum of WASP-52b
Authors: Dongdong Yan, Kwang-il Seon, Jianheng Guo, Guo Chen, Lifang Li
Figure caption: Same as Figure 15, but for H(2s).
Paper: An EUV Jet Driven by a Series of Transition Region Microjets
Authors: Hengyuan Wei, Zhenghua Huang, Hui Fu, Ming Xiong, Lidong Xia, Chao Zhang, Kaiwen Deng, Haiyi Li
Figure caption: A closer look at the region marked with a black dotted square in Figure 1(a) taken with IRIS 1400 Å, AIA 1600 Å, and the HMI line-of-sight magnetogram. The green lines are contours at a level of 8000 DN of the IRIS 1400 Å image. The HMI magnetogram is scaled from −250 to 250 G. In panel (a), the dashed lines roughly enclose the region of the dome of the large jet. In panel (c), the associated polarities of the brightening in the IRIS 1400 Å image are denoted by the arrows with notes of “P1,” “P2,” “P3,” and “N1,” “N2,” “N3,” which have magnetic strengths around the sensitive limit of the instrument and are mostly determined from the connectivities of the microloops as described in the main text. The associated polarities of the base of the EUV jet are marked as “P5,” “P6,” and “N5” and “N4” mark the footpoint of an “open” field as determined from the first microjet (see the main text for detail).
Paper: An EUV Jet Driven by a Series of Transition Region Microjets
Authors: Hengyuan Wei, Zhenghua Huang, Hui Fu, Ming Xiong, Lidong Xia, Chao Zhang, Kaiwen Deng, Haiyi Li
Figure caption: Panels (a)–(d): IRIS slit images in the wavelengths around 1400 Å including the O IV line pair of 1399.8 Å and 1401.2 Å at the location marked by the white dashed line in Figure 1(a) at four different times. Panels (e)–(g): O IV spectral profiles averaged across the EUV jet (the region between the two horizontal dotted lines in panels (a)–(d)) at the times shown in panels (b), (c), (d), in which the black lines are the observations and the red lines are the results from single or double Gaussian fits. Panel (h): theoretical profile showing how the line ratio between the O IV 1399.8 Å and O IV 1401.2 Å varies with the electron densities given by CHIANTI, and the line ratios from the cases in panel (e)–(g) are marked by red crosses and the derived electron densities are marked in panels (e)–(g).
Paper: An EUV Jet Driven by a Series of Transition Region Microjets
Authors: Hengyuan Wei, Zhenghua Huang, Hui Fu, Ming Xiong, Lidong Xia, Chao Zhang, Kaiwen Deng, Haiyi Li
Figure caption: Evolution of IRIS slit images of Si IV 1402.8 Å (first column), C II 1335.7 Å (second column), and Mg II 2796.3 Å (third column) taken from the spatial range marked in Figure 1(a).
Paper: An EUV Jet Driven by a Series of Transition Region Microjets
Authors: Hengyuan Wei, Zhenghua Huang, Hui Fu, Ming Xiong, Lidong Xia, Chao Zhang, Kaiwen Deng, Haiyi Li
Figure caption: A magnetic reconnection scenario interpreting the full set of the events. (See the main text for details.)
Paper: An EUV Jet Driven by a Series of Transition Region Microjets
Authors: Hengyuan Wei, Zhenghua Huang, Hui Fu, Ming Xiong, Lidong Xia, Chao Zhang, Kaiwen Deng, Haiyi Li
Figure caption: Evolution of the footpoint region of the large jet. The green dashed line in panel (b) marks the rising twisted flux ropes as shown in Figure 8. The green dotted lines in panel (g) mark a few brightening threads in the base of the jet. The black crosses in panel (g)–(h) mark the compact brightening that occurs at the start of the large jet.
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: Log scale plot comparing the warm component EM to that of the hot component. Northern CGM fields are marked with black error bars, while the southern CGM fields are marked with magenta error bars. NPS and Eridanus Enhancement fields are marked with cyan center points, while other fields are marked in orange. The gray line is a regression line for the data based on the Bayesian method from Kelly (2007), which utilizes the error on both components. The shaded gray region is the 90% confidence region for the regression. The regression line does not include the NPS or Eridanus Enhancement, and also does not use the four additional outlying fields in the upper right (which are near the Galactic bulge). The linear regression has a slope of 0.092 ± 0.017 and an intercept of 0.00026 ± 0.00022 (90% confidence interval), calculated using the linmix python module from https://github.com/jmeyers314/linmix. The slope being close to 0.1 reflects the typical tenfold difference between the two component’s EMs.
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: Stacked spectra of consistent fields in the northern CGM. Each detector is a different color, following Figure 7. The model for the CGM is a VAPEC with freed neon abundance, marked with a solid black line. Background and foreground components are marked in dashed lines. Model components that are identical between each detector are only shown once. This overall fit is worse than the fit presented in Figure 6. There are significant residuals around 0.5–0.7 keV and a poorly fit section of the high-temperature bump from 0.8 to 0.9 keV. This is the region that corresponds to the neon emission. The additional high-temperature APEC fit in Figure 6 fits to this feature much better than the neon enhancement shown here does.
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: Polar plots for the northern and southern EM. Northern CGM figures mark the fields used in the stacked spectra with black rings. The NPS and Eridanus Enhancement are marked with cyan rings. The median EM from Figure 4 is marked on each color bar, with an uncertainty that is equivalent to the average uncertainty (90% confidence interval).
Paper: Widespread Detection of Two Components in the Hot Circumgalactic Medium of the Milky Way
Authors: Jesse Bluem, Philip Kaaret, K. D. Kuntz, Keith M. Jahoda, Dimitra Koutroumpa, Edmund J. Hodges-Kluck, Chase A. Fuller, Daniel M. LaRocca, Anna Zajczyk
Figure caption: X-ray spectra of Cas A. Data are shown for all three DPUs: 14 = red, 54 = green, and 38 = red. The fitted instrumental background for each DPU is shown as a dotted curve with the same color as the data. The dotted cyan curve is the cosmic X-ray background. The dotted magenta curve is the power law from Cas A. The dotted black curves are the Gaussian emission lines.