adsabs/AstroCLIMB huggingface dataset:
Paper: On Type 1 Active Galactic Nuclei with Double-peaked [O III]. I. Data Sample and Basic Results
Authors: Qi Zheng, Yansong Ma, Xueguang Zhang, Qirong Yuan, Weihao Bian
Figure caption: An example of the best-fitting results of the emission lines around [O III]. In the top panel, the solid dark green line shows the line spectrum after subtracting starlight determined from the host galaxy with Plate-Mjd-Fiberid shown in the top-left corner. The solid red line represents the best-fitting results with two narrow Gaussian functions describing each core component of the [O III] doublet and the corresponding ﹩{\chi }_{1}^{2}/{{\rm{dof}}}_{1}﹩ is shown in the top-left corner. The ﹩{\chi }_{2}^{2}/{{\rm{dof}}}_{2}﹩ determined by one narrow Gaussian function for each core component of the [O III] doublet is shown in the top-left corner. The dashed cyan line represents continuum emission, the solid purple lines represent Fe II emission lines, the solid green lines represent the broad Hβ emission line, the solid cyan lines represent the extended component of [O III], and the dashed blue and red lines represent the blueshifted and the redshifted components of [O III], respectively. In the bottom panel, the solid blue line represents the residuals calculated by the line spectrum minus the best-fitting results and then divided by the uncertainties of the SDSS spectrum. The horizontal solid and dashed green lines show residuals = 0, ±1, respectively.
Paper: On Type 1 Active Galactic Nuclei with Double-peaked [O III]. I. Data Sample and Basic Results
Authors: Qi Zheng, Yansong Ma, Xueguang Zhang, Qirong Yuan, Weihao Bian
Figure caption: Four examples of the best-fitting results of the Fe II emission lines. In the top of each panel, the solid dark green line shows the line spectrum after subtracting starlight (if present) determined from host galaxy with Plate-Mjd-Fiberid shown in the top-left corner, the solid red line represents the best-fitting results with χ2/dof shown in the top-left corner, the solid blue line represents He II emission line (if present), the solid purple lines represent Fe II emission lines, and the dashed cyan line represents continuum emission, the solid green lines represent broad Hβ emission line, the dashed green line represents narrow Hβ emission line, the solid cyan lines represent extended components of [O III], and the dashed blue and red lines represent the blueshifted and redshifted components of [O III], respectively. In the bottom of each panel, the solid blue line represents the residuals calculated by the line spectrum minus the best-fitting results and then divided by uncertainties of SDSS spectrum, the horizontal solid and dashed green lines show residuals = 0,  ±1, respectively.
Paper: On Type 1 Active Galactic Nuclei with Double-peaked [O III]. I. Data Sample and Basic Results
Authors: Qi Zheng, Yansong Ma, Xueguang Zhang, Qirong Yuan, Weihao Bian
Figure caption: An example of the best-fitting results of the emission lines around Hα. In the top panel, the solid dark green line shows the line spectrum after subtracting starlight from host galaxy with Plate-Mjd-Fiberid shown in the top-left corner, the solid red line represents the best-fitting results with χ2/dof shown in the top-left corner, the dashed cyan line represents continuum emission, the solid green lines represent the determined components of broad Hα emission line, the dashed green line represents narrow Hα emission line, the solid blue lines represent [O I] emission lines, and the dashed purple lines represent the [N II] and [S II] doublets. In the bottom panel, the solid blue line represents the residuals calculated by the line spectrum minus the best-fitting results and then divided by uncertainties of SDSS spectrum, the horizontal solid and dashed green lines show residuals = 0,  ±1, respectively.
Paper: On Type 1 Active Galactic Nuclei with Double-peaked [O III]. I. Data Sample and Basic Results
Authors: Qi Zheng, Yansong Ma, Xueguang Zhang, Qirong Yuan, Weihao Bian
Figure caption: An example of SDSS spectrum in the final sample. The solid dark green line represents the spectrum with Plate-Mjd-Fiberid shown in the top-left corner, the solid red line shows the best-fitting results with χ2/dof shown in the top-left corner, the solid blue line shows starlight, the solid green line represents the AGN continuum emission, and the solid black line represents the line spectrum calculated by the SDSS spectrum minus the best-fitting results.
Paper: On Type 1 Active Galactic Nuclei with Double-peaked [O III]. I. Data Sample and Basic Results
Authors: Qi Zheng, Yansong Ma, Xueguang Zhang, Qirong Yuan, Weihao Bian
Figure caption: The flowchart in this work.
Paper: Toward Higher-order Accuracy in Self-gravitating Hydrodynamics
Authors: Tomoyuki Hanawa, Patrick D. Mullen
Figure caption: Error in the moving slab problem. The abscissa denotes the cell number in the x-direction, while the ordinates denote the L1 norm of the error in the conserved quantities (black) and the density (blue) at t = 2π/k · v0.
Paper: Toward Higher-order Accuracy in Self-gravitating Hydrodynamics
Authors: Tomoyuki Hanawa, Patrick D. Mullen
Figure caption: The error in the total energy as a function of time t for the moving slab problem. When ﹩\left({N}_{x},{N}_{y},{N}_{z}\right)=(64,32,32)﹩, the error is a factor of 256 smaller than that for a twice-coarsened grid and only a factor of 10 larger than the numerical round-off error.
Paper: Toward Higher-order Accuracy in Self-gravitating Hydrodynamics
Authors: Tomoyuki Hanawa, Patrick D. Mullen
Figure caption: Convergence of ﹩{\nu }^{-1}d{s}_{{\rm{\max }}}/dt﹩ and σs for the standing-wave test. This figure was previously included in HM25.
Paper: Toward Higher-order Accuracy in Self-gravitating Hydrodynamics
Authors: Tomoyuki Hanawa, Patrick D. Mullen
Figure caption: Convergence test for the n = 5 polytrope model. The abscissa denotes the cell number in the x-direction, while the ordinates denote the L1 norm of the error in ﹩{\mathrm{ln}}\,\rho ﹩, ﹩{\mathrm{ln}},﹩, and vx at t = 1.0 (dashed) and 10.0 (solid).
Paper: Toward Higher-order Accuracy in Self-gravitating Hydrodynamics
Authors: Tomoyuki Hanawa, Patrick D. Mullen
Figure caption: L1 error convergence for self-gravity modified, small-amplitude linear waves.
Paper: Toward Higher-order Accuracy in Self-gravitating Hydrodynamics
Authors: Tomoyuki Hanawa, Patrick D. Mullen
Figure caption: Conservation of specific entropy in the standing-wave problem. This figure was previously included in HM25.
Paper: Galactic-scale Emission-line Outflow from the Radio-loud Quasar 3C 191
Authors: Qinyuan Zhao, Luming Sun, Lu Shen, Guilin Liu, Junfeng Wang, Mayank Sharma, Nahum Arav, Yulong Gao, Chris Benn
Figure caption: Line fitting of the VLT/SINFONI (left) and VLT/X-shooter (right) data, for the purpose of the redshift determination. Left panel: the black solid line represents the observed [O III] spectrum from VLT/SINFONI, summed within a 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩25 aperture centered on the quasar location, with the continuum and Fe II emission subtracted. The orange solid line shows the total fit, while the individual components are represented by orange dashed lines. The vertical blue line indicates the center wavelength of the narrowest component, which is used to determine the systematic redshift. Right panel: the black solid line represents the observed [O II] spectrum from VLT/X-shooter. The systematic redshift is determined by fitting the [O II] λλ3727, 3729 doublet, with the orange solid line showing the total fit and the orange dashed lines showing the individual components.
Paper: Galactic-scale Emission-line Outflow from the Radio-loud Quasar 3C 191
Authors: Qinyuan Zhao, Luming Sun, Lu Shen, Guilin Liu, Junfeng Wang, Mayank Sharma, Nahum Arav, Yulong Gao, Chris Benn
Figure caption: The maps of the ionized gas for 3C 191. The three columns from left to right, and the three rows from top to bottom, are [O III] λ5007 flux intensity (erg s−1 cm−2 arcsec−2), median velocity (km s−1), and velocity dispersion map (W80, km s−1) of blueshifted, unshifted, and redshifted components of ionized gas with a cutoff at an SNR of 3, respectively. PSF is depicted by the open circle on each map. The red/black cross marks the QSO position. The red contours trace the morphology of the [O III] ionized gas from Figure 5.
Paper: Galactic-scale Emission-line Outflow from the Radio-loud Quasar 3C 191
Authors: Qinyuan Zhao, Luming Sun, Lu Shen, Guilin Liu, Junfeng Wang, Mayank Sharma, Nahum Arav, Yulong Gao, Chris Benn
Figure caption: Nonparametric measurement of [O III] ionized gas around 3C 191. From left to right are flux intensity of [O III] (erg s−1 cm−2 arcsec−2), median velocity (km s−1), and line width (W80, km s−1). Only spaxels where the peak of the [O III] λ5007 line is detected with an SNR > 3 are plotted. PSF is depicted by the open circle on each map. The red/black cross marks the QSO position. The red contours trace the morphology of [O III] ionized gas. We use a dashed line to represent the axes of the outflow by eye.
Paper: Galactic-scale Emission-line Outflow from the Radio-loud Quasar 3C 191
Authors: Qinyuan Zhao, Luming Sun, Lu Shen, Guilin Liu, Junfeng Wang, Mayank Sharma, Nahum Arav, Yulong Gao, Chris Benn
Figure caption: Integrated flux intensity of [O III] (erg s−1 cm−2 arcsec−2) from collapsing the IFS data cube directly after subtracting continuum and the [O III] map after subtracting the PSF. PSF is depicted by the open circle on each map. The red cross marks the QSO position, which is the peak flux location of the PSF for 3C 191. These [O III] maps reach a sensitivity of ∼2 × 10−19 erg s−1​​​​​​ cm−2 arcsec−2 on the background.
Paper: Galactic-scale Emission-line Outflow from the Radio-loud Quasar 3C 191
Authors: Qinyuan Zhao, Luming Sun, Lu Shen, Guilin Liu, Junfeng Wang, Mayank Sharma, Nahum Arav, Yulong Gao, Chris Benn
Figure caption: Spatial distribution of [O III] lines at different velocity. PSF is depicted by the open circle on each map. The red/black cross marks the QSO position.
Paper: Galactic-scale Emission-line Outflow from the Radio-loud Quasar 3C 191
Authors: Qinyuan Zhao, Luming Sun, Lu Shen, Guilin Liu, Junfeng Wang, Mayank Sharma, Nahum Arav, Yulong Gao, Chris Benn
Figure caption: We select four spatial positions to present the [O III] velocity profile therein, including central (“B”), redshifted (“C,” “D”), and blueshifted (“A”) regions. Locations of these regions are labeled by their IDs in Figure 5. The fitted line is in orange, and the central narrow unshifted component and the blue-/redshifted components are in cyan, blue, and red, respectively. The median and zero velocity are marked by green dotted and gray dashed lines, respectively. The integrated intensity of the [O III] emission line, Vmed, and W80 with their uncertainties for the individual regions are shown.
Paper: Galactic-scale Emission-line Outflow from the Radio-loud Quasar 3C 191
Authors: Qinyuan Zhao, Luming Sun, Lu Shen, Guilin Liu, Junfeng Wang, Mayank Sharma, Nahum Arav, Yulong Gao, Chris Benn
Figure caption: The PSF model is integrated over the rest-frame wavelength range of 5030–5800 Å. The black open circle depicts the FWHM of the PSF (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩24).
Paper: Galactic-scale Emission-line Outflow from the Radio-loud Quasar 3C 191
Authors: Qinyuan Zhao, Luming Sun, Lu Shen, Guilin Liu, Junfeng Wang, Mayank Sharma, Nahum Arav, Yulong Gao, Chris Benn
Figure caption: Left: outflow rates as a function of the AGN bolometric luminosity. The filled red pentagon denotes the result from this work. The filled circles mark the outflow rates of ionized gas from different studies: black for C. M. Harrison et al. (2014), cyan for D. Kakkad et al. (2020), orange for F. Fiore et al. (2017), blue for S. Carniani et al. (2015), green for M. Bischetti et al. (2017), and brown for A. Travascio et al. (2024). Right: kinetic power as a function of the AGN bolometric luminosity. Symbols and colors are the same as shown in the left panel. The dashed lines correspond to Pk = 5%, 0.5% LAGN, respectively.
Paper: Galactic-scale Emission-line Outflow from the Radio-loud Quasar 3C 191
Authors: Qinyuan Zhao, Luming Sun, Lu Shen, Guilin Liu, Junfeng Wang, Mayank Sharma, Nahum Arav, Yulong Gao, Chris Benn
Figure caption: The gray contours are Chandra ACIS-S observations of the radio jets of 3C 191 in the 0.5–8 keV energy range (R. M. Sambruna et al. 2004; M. C. Erlund et al. 2006), red contours are VLA observations from the quasar jet and lobes (P. P. Kronberg et al. 1990), while the blue contours representing surface brightness of the integrated [O III] with VLT/SINFONI observations in our data. The green and cyan solid lines represent the axes of the jet and outflow, respectively.
Paper: Galactic-scale Emission-line Outflow from the Radio-loud Quasar 3C 191
Authors: Qinyuan Zhao, Luming Sun, Lu Shen, Guilin Liu, Junfeng Wang, Mayank Sharma, Nahum Arav, Yulong Gao, Chris Benn
Figure caption: The initial spectrum of the 3C 191 extracted from the FOV of 2″ × 2″ (40 × 40 pixel) observed by VLT/SINFONI. The observed spectrum (black) and the best-fitted spectrum (red) are shown. The different components of the best-fitted model are shown as different colored lines: the power-law component in gray, the Fe II component in cyan, and the [O III] component in orange. The zero velocity is marked by blue dashed lines.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Depth maps of the JWST/NIRCam imaging in the GOODS-N field. Shown are the local, aperture-corrected 5σ point-source depths measured in circular apertures with radii r = 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩15. The F090W, F115W, F150W, F200W, F277W, F335M, F356W, and F410M images use data from the JADES program. The F182M and F210M data were acquired by the FRESCO survey (P. A. Oesch et al. 2023a). The deep F444W data are from the JADES program, and the shallow/wide F444W tier is from FRESCO. The aperture correction is performed using the model point-spread functions from Z. Ji et al. (2024). The color bar indicates the local depth in each filter, as measured in units of nJy. For reference, the outline of the HDF (R. E. Williams et al. 1996) is shown in white on the F090W depth map.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Mosaic of JADES JWST/NIRCam data covering the HDF region. Shown are the F444W, F200W, and F090W mosaics as the red–green–blue channels of this multicolor image, respectively. The iconic HDF (R. E. Williams et al. 1996) footprint is shown as a silver line. We note the linear diffuse green feature in the center of the image results from local noise in the F200W image and is not an astrophysical object.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Mosaic of JADES JWST/NIRCam data in the GOODS-N field acquired in 2023 February. The F444W, F200W, and F090W mosaics are shown as the red, green, and blue channels, respectively, in this multicolor image. The scale bar indicates 1′.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: A subset of the observed spectra with multiple emission lines, sorted from bottom to top by increasing redshift. A number of continuum and line features is apparent, illustrating the simultaneous coverage of the rest-frame UV and optical ranges before cosmic noon.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Comparison of the emission-line fluxes measured from the prism and from the medium-resolution gratings, as a function of prism flux (left column) and redshift (right column). The central insets between the columns are the median and standard deviation for each emission-line complex (also displayed as green horizontal lines and shaded regions), while the bottom right corner of each panel reports the Spearman rank correlation coefficient and associated p-value. [O II] λλ3726, 3729 (panels (a) and (d)) shows the regime where the gratings-to-prism flux ratio frat is dominated by systematics in the continuum model; [O III] λλ4959, 5007 (panels (b) and (e)) illustrates with high significance the strong correlation between frat and redshift, which indicates the flux-calibration mismatch between the prism and gratings is most severe in G395M. The dotted vertical lines in panels (e) and (f) show the redshift where [O III] λ5007 and Hα are observed at 2.9 μm—the bluest wavelength captured by the G395M/F290LP disperser–filter combination. Finally, Hα + [N II] λλ6548, 6583 shows that the total fluxes measured by the prism (where we do not separate Hα from [N II] λλ6548, 6583) match the fluxes measured by the gratings well (where the emission-line complex is well resolved); the trends with flux and redshift are consistent with what we see for [O III] λλ4959, 5007.
Paper: JADES Data Release 3: NIRSpec/Microshutter Assembly Spectroscopy for 4000 Galaxies in the GOODS Fields
Authors: Francesco D'Eugenio, Alex J. Cameron, Jan Scholtz, Stefano Carniani, Chris J. Willott, Emma Curtis-Lake, Andrew J. Bunker, Eleonora Parlanti, Roberto Maiolino, Christopher N. A. Willmer, Peter Jakobsen, Brant E. Robertson, Benjamin D. Johnson, Sandro Tacchella, Phillip A. Cargile, Tim Rawle, Santiago Arribas, Jacopo Chevallard, Mirko Curti, Eiichi Egami, Daniel J. Eisenstein, Nimisha Kumari, Tobias J. Looser, Marcia J. Rieke, Bruno Rodríguez Del Pino, Aayush Saxena, Hannah Übler, Giacomo Venturi, Joris Witstok, William M. Baker, Rachana Bhatawdekar, Nina Bonaventura, Kristan Boyett, Stephane Charlot, A. Lola Danhaive, Kevin N. Hainline, Ryan Hausen, Jakob M. Helton, Xihan Ji, Zhiyuan Ji, Gareth C. Jones, Ignas Juodžbalis, Michael V. Maseda, Pablo G. Pérez-González, Michele Perna, Dávid Puskás, Irene Shivaei, Maddie S. Silcock, Charlotte Simmonds, Renske Smit, Fengwu Sun, Natalia C. Villanueva, Christina C. Williams, Yongda Zhu
Figure caption: Target ID 199773 from PID 3215, illustrating remaining calibration problems. Panel (a) shows the prism and grating data (in black and blue, with G140M to the left and G395M to the right), and the grating data after rebinning to the prism grid (yellow) and after matching the nominal resolution of the prism and then rebinning (red; vertical gray areas highlight spectral regions where we interpolated over missing grating data, due to bad pixels or the detector gap; the red line is clipped at the edges of the wavelength range due to the size of the convolution kernel). Panel (b) shows the ratio between the rebinned and smoothed-then-rebinned grating spectrum and the prism spectrum (same line colors as in panel (a)). The flux-calibration mismatch between the prism and gratings is wavelength dependent, and is most severe in G395M. The galaxy image is shown in panel (c), with the MSA shutters overlaid. From Z. Ji et al. (2025, in preparation).