adsabs/AstroCLIMB huggingface dataset:
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: (a) Left: HST J-band (1.1  μm) image of G28.20-0.05. Cyan contours show the ALMA 1.3 mm continuum image (same contour levels as in Figure 10). (b) Right: as (a), but now showing the HST H-band (1.6  μm) image.
Paper: Isolated Massive Star Formation in G28.20-0.05
Authors: Chi-Yan Law, Jonathan C. Tan, Prasanta Gorai, Yichen Zhang, Rubén Fedriani, Daniel Tafoya, Kei E. I. Tanaka, Giuliana Cosentino, Yao-Lun Yang, Diego Mardones, Maria T. Beltrán, Guido Garay
Figure caption: CO(2–1) and SiO(5-4) averaged spectra extracted from a circular aperture of radius 10″.
Paper: SALT3-NIR: Taking the Open-source Type Ia Supernova Model to Longer Wavelengths for Next-generation Cosmological Measurements
Authors: J. D. R. Pierel, D. O. Jones, W. D. Kenworthy, M. Dai, R. Kessler, C. Ashall, A. Do, E. R. Peterson, B. J. Shappee, M. R. Siebert, T. Barna, T. G. Brink, J. Burke, A. Calamida, Y. Camacho-Neves, T. de Jaeger, A. V. Filippenko, R. J. Foley, L. Galbany, O. D. Fox, S. Gomez, D. Hiramatsu, R. Hounsell, D. A. Howell, S. W. Jha, L. A. Kwok, I. Pérez-Fournon, F. Poidevin, A. Rest, D. Rubin, D. M. Scolnic, R. Shirley, L. G. Strolger, S. Tinyanont, Q. Wang
Figure caption: The primary components that make up the existing SALT3 model at peak (p = 0) brightness (black solid). The M 0 component (red dotted) defines a “baseline” SN Ia spectrum, the M 1 component (green dashed) controls the stretch of a given SN, and the color law (blue dashed–dotted) is equivalently A  λ –A  B . The terms x 0, x 1, and c are free fitting parameters.
Paper: SALT3-NIR: Taking the Open-source Type Ia Supernova Model to Longer Wavelengths for Next-generation Cosmological Measurements
Authors: J. D. R. Pierel, D. O. Jones, W. D. Kenworthy, M. Dai, R. Kessler, C. Ashall, A. Do, E. R. Peterson, B. J. Shappee, M. R. Siebert, T. Barna, T. G. Brink, J. Burke, A. Calamida, Y. Camacho-Neves, T. de Jaeger, A. V. Filippenko, R. J. Foley, L. Galbany, O. D. Fox, S. Gomez, D. Hiramatsu, R. Hounsell, D. A. Howell, S. W. Jha, L. A. Kwok, I. Pérez-Fournon, F. Poidevin, A. Rest, D. Rubin, D. M. Scolnic, R. Shirley, L. G. Strolger, S. Tinyanont, Q. Wang
Figure caption: The density of photometric (filter effective wavelength; top) and spectroscopic (bottom) data in the K21 sample, as a function of rest-frame wavelength and days relative to peak brightness (phase).
Paper: SALT3-NIR: Taking the Open-source Type Ia Supernova Model to Longer Wavelengths for Next-generation Cosmological Measurements
Authors: J. D. R. Pierel, D. O. Jones, W. D. Kenworthy, M. Dai, R. Kessler, C. Ashall, A. Do, E. R. Peterson, B. J. Shappee, M. R. Siebert, T. Barna, T. G. Brink, J. Burke, A. Calamida, Y. Camacho-Neves, T. de Jaeger, A. V. Filippenko, R. J. Foley, L. Galbany, O. D. Fox, S. Gomez, D. Hiramatsu, R. Hounsell, D. A. Howell, S. W. Jha, L. A. Kwok, I. Pérez-Fournon, F. Poidevin, A. Rest, D. Rubin, D. M. Scolnic, R. Shirley, L. G. Strolger, S. Tinyanont, Q. Wang
Figure caption: Additional YJH data from the SIRAH, RAISIN, and DEHVILS surveys described in Sections 3.2.2–3.2.4. These light curves are combined with the legacy public NIR data listed in Table 1 to create the full SALT3-NIR training sample.
Paper: SALT3-NIR: Taking the Open-source Type Ia Supernova Model to Longer Wavelengths for Next-generation Cosmological Measurements
Authors: J. D. R. Pierel, D. O. Jones, W. D. Kenworthy, M. Dai, R. Kessler, C. Ashall, A. Do, E. R. Peterson, B. J. Shappee, M. R. Siebert, T. Barna, T. G. Brink, J. Burke, A. Calamida, Y. Camacho-Neves, T. de Jaeger, A. V. Filippenko, R. J. Foley, L. Galbany, O. D. Fox, S. Gomez, D. Hiramatsu, R. Hounsell, D. A. Howell, S. W. Jha, L. A. Kwok, I. Pérez-Fournon, F. Poidevin, A. Rest, D. Rubin, D. M. Scolnic, R. Shirley, L. G. Strolger, S. Tinyanont, Q. Wang
Figure caption: The density of photometric (filter effective wavelength; top) and spectroscopic (bottom) data in the K21+NIR training sample, as a function of rest-frame wavelength and days relative to peak brightness (phase).
Paper: SALT3-NIR: Taking the Open-source Type Ia Supernova Model to Longer Wavelengths for Next-generation Cosmological Measurements
Authors: J. D. R. Pierel, D. O. Jones, W. D. Kenworthy, M. Dai, R. Kessler, C. Ashall, A. Do, E. R. Peterson, B. J. Shappee, M. R. Siebert, T. Barna, T. G. Brink, J. Burke, A. Calamida, Y. Camacho-Neves, T. de Jaeger, A. V. Filippenko, R. J. Foley, L. Galbany, O. D. Fox, S. Gomez, D. Hiramatsu, R. Hounsell, D. A. Howell, S. W. Jha, L. A. Kwok, I. Pérez-Fournon, F. Poidevin, A. Rest, D. Rubin, D. M. Scolnic, R. Shirley, L. G. Strolger, S. Tinyanont, Q. Wang
Figure caption: Distributions of SALT3 c (top) and x 1 (bottom) for the K21 sample (red dashed line) and the added NIR sample (black).
Paper: SALT3-NIR: Taking the Open-source Type Ia Supernova Model to Longer Wavelengths for Next-generation Cosmological Measurements
Authors: J. D. R. Pierel, D. O. Jones, W. D. Kenworthy, M. Dai, R. Kessler, C. Ashall, A. Do, E. R. Peterson, B. J. Shappee, M. R. Siebert, T. Barna, T. G. Brink, J. Burke, A. Calamida, Y. Camacho-Neves, T. de Jaeger, A. V. Filippenko, R. J. Foley, L. Galbany, O. D. Fox, S. Gomez, D. Hiramatsu, R. Hounsell, D. A. Howell, S. W. Jha, L. A. Kwok, I. Pérez-Fournon, F. Poidevin, A. Rest, D. Rubin, D. M. Scolnic, R. Shirley, L. G. Strolger, S. Tinyanont, Q. Wang
Figure caption: Correlations (black points with error bars) between SALT3 and SALT3-NIR measured values of c (left), x 1 (middle), and μ–μ ΛCDM (right) for YJH (top row) and Optical + YJH (bottom row) fitting scenarios. The SALT3 fits are for the same SNe Ia fit by SALT3-NIR, but using only optical data. Best-fit linear regressions are shown as blue dotted lines, and a slope of 1 (red solid line) is given for comparison.
Paper: SALT3-NIR: Taking the Open-source Type Ia Supernova Model to Longer Wavelengths for Next-generation Cosmological Measurements
Authors: J. D. R. Pierel, D. O. Jones, W. D. Kenworthy, M. Dai, R. Kessler, C. Ashall, A. Do, E. R. Peterson, B. J. Shappee, M. R. Siebert, T. Barna, T. G. Brink, J. Burke, A. Calamida, Y. Camacho-Neves, T. de Jaeger, A. V. Filippenko, R. J. Foley, L. Galbany, O. D. Fox, S. Gomez, D. Hiramatsu, R. Hounsell, D. A. Howell, S. W. Jha, L. A. Kwok, I. Pérez-Fournon, F. Poidevin, A. Rest, D. Rubin, D. M. Scolnic, R. Shirley, L. G. Strolger, S. Tinyanont, Q. Wang
Figure caption: The fraction of all Roman HLTDS observations that SALT2 (black dashed–dotted), SALT3 (blue dashed), and SALT3-NIR (red solid) are capable of fitting (i.e., the wavelength range fully encompasses the respective filter) as a function of redshift. The difference is most significant at low redshifts, where Roman filters probe the rest-frame NIR.
Paper: Improved Measurements of Galaxy Star Formation Stochasticity from the Intrinsic Scatter of Burst Indicators
Authors: Adam Broussard, Eric Gawiser, Kartheik Iyer
Figure caption: Balmer decrement (F Hα,uncorr/F Hβ,uncorr) and corresponding ﹩{Q}_{{sg}}^{-1}(\mathrm{assuming}\,E{\left(B-V\right)}_{\mathrm{stars}}=0.1)﹩ vs. Hβ star formation rate (SFR) signal-to-noise ratio (S/N) for MOSDEF galaxies with simultaneous Hα and Hβ detections. Here, we label the right axis with ﹩{Q}_{{sg}}^{-1}﹩ rather than the inverse because this quantity approaches 0 at a Balmer decrement of 2.86 rather than tending toward positive and negative infinity. ﹩{Q}_{{sg}}^{-1}﹩ is also useful in calculating the intrinsic variance in η, which we describe in Section 5. The red horizontal line indicates Q  sg  = 0.44, the value used for low-redshift galaxies by Calzetti et al. (2000), while the black dashed line indicates a Balmer decrement of 2.86, which is expected in the absence of dust. The green shaded region indicates SFRHβ  S/N > 5, which we use to select the MOSDEF Gold sample used to measure the distribution of Q  sg .
Paper: Improved Measurements of Galaxy Star Formation Stochasticity from the Intrinsic Scatter of Burst Indicators
Authors: Adam Broussard, Eric Gawiser, Kartheik Iyer
Figure caption: Plots showing the 3D-HST (top major row), FMOS-COSMOS (middle major row), and MOSDEF (bottom major row) mock catalogs generated from the Santa Cruz SAM (top minor rows) and MUFASA (bottom minor rows). The detailed descriptions of each step involved in creating the mock catalog are described in Section 4. The final step “SFR Noise Added” represents the addition of a small amount of scatter at the end of the mock catalog generation process to match the total observed scatter in SFRNUV and SFRHα  for each survey.
Paper: Improved Measurements of Galaxy Star Formation Stochasticity from the Intrinsic Scatter of Burst Indicators
Authors: Adam Broussard, Eric Gawiser, Kartheik Iyer
Figure caption: Scatter plot of ﹩E{\left(B-V\right)}_{\mathrm{gas}}﹩ vs. ﹩E{\left(B-V\right)}_{\mathrm{stars}}﹩ for MOSDEF galaxies assuming a Calzetti et al. (2000) dust law. Dashed lines indicate various values of ﹩{Q}_{{sg}}=E{\left(B-V\right)}_{{\rm{stars}}}/E{\left(B-V\right)}_{{\rm{gas}}}﹩. Many objects have ﹩E{\left(B-V\right)}_{\mathrm{gas}}\lt 0﹩, caused by emission line ratios with F Hα /F Hβ  < 2.86. This indicates an unphysical inversion of the typical Balmer decrement dust correction.
Paper: Improved Measurements of Galaxy Star Formation Stochasticity from the Intrinsic Scatter of Burst Indicators
Authors: Adam Broussard, Eric Gawiser, Kartheik Iyer
Figure caption: Distributions of η for the MUFASA mocks (red), Semi-Analytic Model mocks (blue), and observed galaxies (yellow). We see good agreement between distribution shapes and widths for the 3D-HST mock and observed samples, but the FMOS-COSMOS and MOSDEF mocks underestimate the median value and scatter in η.
Paper: Bridging the Gap between Intermediate and Massive Stars. I. Validation of MESA against the State-of-the-Art Monash Stellar Evolution Program for a 2M ⊙ AGB Star
Authors: Giulia C. Cinquegrana, Meridith Joyce, Amanda I. Karakas
Figure caption: Evolutionary tracks of the two 2 M ⊙, Z = 0.03 models.
Paper: Bridging the Gap between Intermediate and Massive Stars. I. Validation of MESA against the State-of-the-Art Monash Stellar Evolution Program for a 2M ⊙ AGB Star
Authors: Giulia C. Cinquegrana, Meridith Joyce, Amanda I. Karakas
Figure caption: A comparison of the surface properties of the two models. We show luminosity (top panel), effective temperature (center panel), and radius (bottom panel) as functions of time on the thermally pulsing AGB. All show excellent agreement between the models.
Paper: Bridging the Gap between Intermediate and Massive Stars. I. Validation of MESA against the State-of-the-Art Monash Stellar Evolution Program for a 2M ⊙ AGB Star
Authors: Giulia C. Cinquegrana, Meridith Joyce, Amanda I. Karakas
Figure caption: A pair of 2 M ⊙, Z = 0.03 models both run with the Monash code. The cyan blue (dashed line) model is run using the mass-loss approximation of Blöcker (1995), and the magenta (solid line) model with Vassiliadis & Wood (1993) mass loss.
Paper: Light Bridge and Magnetic Field in a Solar Active Region
Authors: Huaning Wang, Changhui Rao, Naiting Gu, Libo Zhong, Xin Huang
Figure caption: AIA193 image and extrapolated field lines. (a) Intensity image in logarithmic scale; (b) extrapolated field lines and AIA193 image. The extrapolated field lines are uniformly distributed at grid points with a spatial solution of 5.″9 × 5.″9. Some field lines from grid points within 12″ close to the map limb are not plotted because of the boundary effect. The field lines from the hole (weak EUV emission area) in the dominant spot are not plotted because they are open.
Paper: Light Bridge and Magnetic Field in a Solar Active Region
Authors: Huaning Wang, Changhui Rao, Naiting Gu, Libo Zhong, Xin Huang
Figure caption: Maps of hmi. sharp − 720s from the dominant spot in NOAA 12529 (a) magnetic field strength (grayscale range: [86.4, 3293.1]G; average in the umbra: 2573.6G; WFL: weak field lane; AF: abnormal feature); (b) continuum intensity (FWFL: feature similar to WFL); (c) Doppler velocity (grayscale range: [−2.40, 2.43]km s−1).
Paper: Light Bridge and Magnetic Field in a Solar Active Region
Authors: Huaning Wang, Changhui Rao, Naiting Gu, Libo Zhong, Xin Huang
Figure caption: WFLs and QSLs in the dominant spot. (a) WFLs and QSL intersections (closed white lanes with Q values over 0.6Qmax) in the xy plane; (b) field lines from QSL intersections. The map of magnetic strength is taken as background images in (a) and (b); Q values are computed in the white box.
Paper: Light Bridge and Magnetic Field in a Solar Active Region
Authors: Huaning Wang, Changhui Rao, Naiting Gu, Libo Zhong, Xin Huang
Figure caption: Maps of hmi. sharp − 720s from NOAA 12529 (a) continuum intensity; (b) magnetic flux (grayscale range: [−1971.0, 1310.3]G; white: N polarity; black: S polarity).
Paper: Light Bridge and Magnetic Field in a Solar Active Region
Authors: Huaning Wang, Changhui Rao, Naiting Gu, Libo Zhong, Xin Huang
Figure caption: Field lines in the dominant spot. (a) Closed field lines; (b) open field lines. The map of magnetic strength is taken as background images in (a) and (b); Q values are computed in the white box; the closed white lanes with Q values over 0.6Qmax indicate QSL intersections.
Paper: Light Bridge and Magnetic Field in a Solar Active Region
Authors: Huaning Wang, Changhui Rao, Naiting Gu, Libo Zhong, Xin Huang
Figure caption: TiO 7057 Å image. The dashed lines indicate locations of weak field lanes in the dominant spot; SLB: strong light bridge; FLB: faint light bridge; AF: abnormal feature.
Paper: Deep-learning Reconstruction of Sunspot Vector Magnetic Fields for Forecasting Solar Storms
Authors: Dattaraj B. Dhuri, Shamik Bhattacharjee, Shravan M. Hanasoge, Sashi Kiran Mahapatra
Figure caption: Additional examples of IG attribution maps (Figure 8).
Paper: Informed Systematic Method to Identify Variable Mid- and Late-T Dwarfs
Authors: Natalia Oliveros-Gomez, Elena Manjavacas, Afra Ashraf, Daniella C. Bardalez-Gagliuffi, Johanna M. Vos, Jacqueline K. Faherty, Theodora Karalidi, Daniel Apai
Figure caption: Index–index plots comparing the designed spectral indices to find mid- and late-T brown dwarf variables. The blue points correspond to the spectra that show the lowest variability amplitude (close to the 1.0 of the light curve in Figure 1), and the red correspond to the most variable spectra (close to the 1.007 or 0.992 of the light curve in Figure 1). The black star in the center corresponds to the indices calculated for the template spectrum with no variability. We show the provisional variable regions (in yellow) using the indices calculated only with observed spectra.
Paper: Analysis of Thermal Emissions of Exoplanets with Axially Symmetric Temperature Gradients
Authors: Jennifer L. Carter
Figure caption: Shown is the corner plot for the posterior distributions of select parameters for a B + E+TNVary6, C model with planetary mass held fixed applied to B + E+TN6, C synthetic data with a large temperature gradient. These are the distributions for the photometric variations shown in Figure 11(A). Note that the cooler zones, T 4 through T 6, are less constrained. We also see a peaked ridge structure for said zones vs. T 3, which is located on the star side of the terminator. Finally, we see that the star-side zones, T 1 through T 3, display multimodal and sharply curved banana-like structures.
Paper: Informed Systematic Method to Identify Variable Mid- and Late-T Dwarfs
Authors: Natalia Oliveros-Gomez, Elena Manjavacas, Afra Ashraf, Daniella C. Bardalez-Gagliuffi, Johanna M. Vos, Jacqueline K. Faherty, Theodora Karalidi, Daniel Apai
Figure caption: Ranges of wavelengths used to calculate spectral indices on a sample brown dwarf spectrum. Red corresponds to the numerator and blue to the denominator in Equation (1).
Paper: Informed Systematic Method to Identify Variable Mid- and Late-T Dwarfs
Authors: Natalia Oliveros-Gomez, Elena Manjavacas, Afra Ashraf, Daniella C. Bardalez-Gagliuffi, Johanna M. Vos, Jacqueline K. Faherty, Theodora Karalidi, Daniel Apai
Figure caption: 2M2228 near-infrared light curve to identify the regions of variability based on visual inspection. The least variable spectra are those corresponding to the center of the light curve (flux ∼1, black line). The most variable spectra are those corresponding to the peaks for the light curve (dashed orange lines).
Paper: Informed Systematic Method to Identify Variable Mid- and Late-T Dwarfs
Authors: Natalia Oliveros-Gomez, Elena Manjavacas, Afra Ashraf, Daniella C. Bardalez-Gagliuffi, Johanna M. Vos, Jacqueline K. Faherty, Theodora Karalidi, Daniel Apai
Figure caption: Top: template for 2M2228 after median-combining the 40 HST/WFC3 spectra (black), and example of one variable spectrum for 2M2228. Bottom: residuals after subtracting the variable spectrum of 2M2228 from the 2M2228 template. We highlight in red the most variable region (the peaks of the J band and H band), and in blue the least variable regions of the spectrum according to the residuals.
Paper: Analysis of Thermal Emissions of Exoplanets with Axially Symmetric Temperature Gradients
Authors: Jennifer L. Carter
Figure caption: The above plots (A)–(D) show the thermal flux normalized to the blackbody flux of the host star Φ for N = 4, 6, 8, and 10 zones, respectively, for Kepler-91 b. In the plots, the temperature values decrease monotonically from T sub = 2442 K to T min = 2348 K, corresponding to the dayside and nightside temperature estimates in Placek et al. (2015), respectively. The full phase of the exoplanet occurs at 0 and 1 fractional period, and the new phase at 0.5 fractional period. In each, the dark blue line indicates the total normalized thermal flux due to all N zones. In addition, the contribution from each zone is plotted.
Paper: Analysis of Thermal Emissions of Exoplanets with Axially Symmetric Temperature Gradients
Authors: Jennifer L. Carter
Figure caption: Shown are the results for the analysis of Kepler-41b and Kepler-412b using the highest-likelihood parameters of the highest-evidence models listed in Table 7. (A) and (B) are the light-curve and thermal variations for Kepler-41b, respectively, and (C) and (D) those of Kepler-412b. In (A) and (C), the gray dots are the normalized, detrended, cleaned, and phase-folded data points. The solid black line is the best-fit model to the data. In (B) and (D), the thermal variations generated by the estimated zone temperatures are shown, in addition to the total thermal light.
Paper: Informed Systematic Method to Identify Variable Mid- and Late-T Dwarfs
Authors: Natalia Oliveros-Gomez, Elena Manjavacas, Afra Ashraf, Daniella C. Bardalez-Gagliuffi, Johanna M. Vos, Jacqueline K. Faherty, Theodora Karalidi, Daniel Apai
Figure caption: Index–index plot as in Figure 4 including the value of the indices calculated for the synthetic spectra created using the most variable spectra of 2M2228 (purple stars) and the least variable ones (green stars). We show the updated new variable regions (in gray) using the synthetic spectra.
Paper: Recombination of Hot Ionized Nebulae: The Old Planetary Nebula around V4334 Sgr (Sakurai’s Star) 
Authors: Martin Reichel, Stefan Kimeswenger, Peter A. M. van Hoof, Albert A. Zijlstra, Daniela Barría, Marcin Hajduk, Griet C. Van de Steene, Daniel Tafoya
Figure caption: The distribution of the C  k  parameter (solid line) and of the constant solution (dashed line) were derived using the MC runs for the [O III] line at 5007 Å. The shaded area gives the parameter A for the determination of x in Equation (5). The fit and the region of the standard error derived from a normal regression program are shown for reference with the dashed–dotted and dotted lines, respectively.
Paper: Recombination of Hot Ionized Nebulae: The Old Planetary Nebula around V4334 Sgr (Sakurai’s Star) 
Authors: Martin Reichel, Stefan Kimeswenger, Peter A. M. van Hoof, Albert A. Zijlstra, Daniela Barría, Marcin Hajduk, Griet C. Van de Steene, Daniel Tafoya
Figure caption: Frequency distribution of the (a) airmass, (b) seeing, (c) slit efficiency calculated from the seeing, and (d) measured transparency losses. The arrows indicate the rejection limits applied for the sample (see the text).
Paper: Recombination of Hot Ionized Nebulae: The Old Planetary Nebula around V4334 Sgr (Sakurai’s Star) 
Authors: Martin Reichel, Stefan Kimeswenger, Peter A. M. van Hoof, Albert A. Zijlstra, Daniela Barría, Marcin Hajduk, Griet C. Van de Steene, Daniel Tafoya
Figure caption: The selection of calibration stars. The upper panel shows a direct image taken through the slit (expanded in the y-direction to enhance the visibility of the centering) before adding the GRISM. Only well-centered stars were selected for calibration purposes. The lower panel shows a fraction of the red end of the spectrum taken directly thereafter. The selected calibration stars are marked with the red bars connecting their image in the slit preview with their appearance in the spectrum. The night sky line identifications are taken from Osterbrock et al. (1996).
Paper: Recombination of Hot Ionized Nebulae: The Old Planetary Nebula around V4334 Sgr (Sakurai’s Star) 
Authors: Martin Reichel, Stefan Kimeswenger, Peter A. M. van Hoof, Albert A. Zijlstra, Daniela Barría, Marcin Hajduk, Griet C. Van de Steene, Daniel Tafoya
Figure caption: The overlapping region of the 600V (upper), 300V (middle), and 300I (lower) GRISMs from 6250 Å to 6950 Å after sky emission line removal showing the effects of the different resolutions as well as contamination by field stars and the clumpy emission of the central object V4334 Sgr itself.
Paper: Recombination of Hot Ionized Nebulae: The Old Planetary Nebula around V4334 Sgr (Sakurai’s Star) 
Authors: Martin Reichel, Stefan Kimeswenger, Peter A. M. van Hoof, Albert A. Zijlstra, Daniela Barría, Marcin Hajduk, Griet C. Van de Steene, Daniel Tafoya
Figure caption: The old PN around V4334 Sgr. Left: a single 300 s frame taken with the [O III] filter. Right: after star removal and averaging the two available frames (see the text). The black lines indicate the position of our slit. The old PN is 44″ across.
Paper: Recombination of Hot Ionized Nebulae: The Old Planetary Nebula around V4334 Sgr (Sakurai’s Star) 
Authors: Martin Reichel, Stefan Kimeswenger, Peter A. M. van Hoof, Albert A. Zijlstra, Daniela Barría, Marcin Hajduk, Griet C. Van de Steene, Daniel Tafoya
Figure caption: The slit loss calibration. A cut through the stellar image (black), the slit boundaries (red), and the resulting remaining flux reaching the instrument (green). The insert shows the full 2D representation on a linear color scale.
Paper: Recombination of Hot Ionized Nebulae: The Old Planetary Nebula around V4334 Sgr (Sakurai’s Star) 
Authors: Martin Reichel, Stefan Kimeswenger, Peter A. M. van Hoof, Albert A. Zijlstra, Daniela Barría, Marcin Hajduk, Griet C. Van de Steene, Daniel Tafoya
Figure caption: The 16 measurements (thin lines) and the derived mean (thick line) of the [N II] 6584 Å line taken in 2010 with the visual band GRISMs V300 and V600. The shaded areas are the applied rejection masks The data value d  i  is derived as the mean of the integrals from the unmasked regions.
Paper: Recombination of Hot Ionized Nebulae: The Old Planetary Nebula around V4334 Sgr (Sakurai’s Star) 
Authors: Martin Reichel, Stefan Kimeswenger, Peter A. M. van Hoof, Albert A. Zijlstra, Daniela Barría, Marcin Hajduk, Griet C. Van de Steene, Daniel Tafoya
Figure caption: The time evolution of various permitted lines of H I, He I, and He II and the forbidden line transitions of [O III], [N II], [S II], [S III], and [Ar III]. The best linear fits are indicated. The dashed lines indicate the constant solution.