adsabs/AstroCLIMB huggingface dataset:
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for the He 584.33 Å line and (b) the solar spectrum utilized in the region of the line. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). For the He 584 Å line, we used the theoretical line-shape profile of Golding et al. (2017; their Figure 10) and scaled the irradiance to the TIMED SEE solar spectral irradiance Level 3A for 2009 March 1. The spectral data were downloaded from the LASP LISIRD site.(The data used to create this figure are available.)
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for the combined H Lyα lines at 1215.668 and 1215.67 Å and (b) the solar spectrum utilized in the region of the lines. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). For the H Lyα line, we used the line profile observed by SUMER/SOHO (Lemaire et al. 2015; their Figure 5(b)) for 2009 April 16. The spectral data were downloaded from the CDS website provided in the referenced paper.(The data used to create this figure are available.)
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for the Al line at 3945.12 Å and (b) the solar spectrum utilized in the region of the lines. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). The TSIS-1 reference spectrum was used for Al.(The data used to create this figure are available.)
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for the Al line at 3962.64 Å and (b) the solar spectrum utilized in the region of the lines. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). The TSIS-1 reference spectrum was used for Al.(The data used to create this figure are available.)
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for K 4045.24 Å and 4048.36 Å and (b) the solar spectrum in the region of the lines. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). The TSIS-1 reference spectrum was used for K at these wavelengths.(The data used to create this figure are available.)
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for the visible K (D1) line at 7701.08 Å and K (D2) at 7667.01 Å and (b) the solar spectrum in the region of the lines. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). The TSIS-1 reference spectrum was used for K at these wavelengths.(The data used to create this figure are available.)
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for Ca+ at 3934.78 Å lines and (b) the solar spectrum utilized in the region of the line. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). The TSIS-1 reference spectrum was used for Ca+.(The data used to create this figure are available.)
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for Ca+ at 3969.59 Å lines and (b) the solar spectrum utilized in the region of the line. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). The TSIS-1 reference spectrum was used for Ca+.(The data used to create this figure are available.)
Paper: Updated Photon Scattering Coefficients (g_values) for Mercury’s Exospheric Species
Authors: Rosemary M. Killen, Ronald J. Vervack Jr., Matthew H. Burger
Figure caption: (a) Updated g_values for the Mn lines at 4031.21 Å, 4034.21 Å, and 4035.63 Å and (b) the solar spectrum utilized in the region of the lines. The dashed lines in (b) indicate the range of wavelengths corresponding to the g_values shown in (a). The TSIS-1 reference spectrum was used for Mn. This region of the spectrum is crowded with solar features that complicate the g_values.(The data used to create this figure are available.)
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Radial velocity contours of the steady dipole case for two simulation cases with low and large electric fields. For better legibility, units are in kilometers per second.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Demonstration of the types of spurious  E -field developing within the computational domain: one due to the initial state of the simulation (left; taken at iteration zero) and one caused by the inner BC (right; generated after 100 iterations).
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Demonstration of the high-velocity patches near the edge of the domain in the case of a flow field where the  V  and  B  distributions are well aligned (left) and a flow field with a large misalignment (right).
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Contours of E  φ  before and after rotation of the mesh, demonstrating that this  E -field component is unrelated to the mesh but produced through other mechanisms. We show them in a vertical cut (as the dipole does not have longitudinal dependency) with contours set between −0.55 and 0.0.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Contours of E  θ  before and after mesh rotation, showing that these structures are mostly mesh related. We show them in a vertical cut (as the dipole does not have longitudinal dependency) with contours set between −0.002 and 0.002.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Temperature distribution (here expressed simply as a ratio of pressure and density) of the steady dipole as resolved in the “low  E ” (left) and “large  E ” (right) cases.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: The mesh used for most simulations in this paper is based on prisms and has 300,000 elements. We show a 3D rendering of the outer spherical slice at 21 R ⊙ in the left panel and a 2D vertical cut to focus on the stretched radial structure in the right panel.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Radial velocity contours near the solar surface, with the color bar adjusted to demonstrate the enhancement in the sharpness of the streamers for the “low  E ” simulation (left). For better legibility, units are in kilometers per second.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Contours of the E  φ  field with the color bar adjusted such that the features show in both cases.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Differences B  r,diff = B  r,2 − B  r,3 (left) and B  θ,diff = B  θ,2 − B  θ,3 (right) between cases 2 and 3 as a result of using different B  r  extrapolations.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Comparison of logarithms of different distance functions (inverse cubic in red, inverse square in green, and inverse 2.5 power-law profile in blue) with the behavior of the logarithm of the nondimensional density vs. the distance from the Sun (in solar radii). The profiles were designed to intersect at 21.5 R ⊙ to allow for slope analysis.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: The projection of V  r  in meters per second on the outer surface of the domain before (left) and during (right) the unstable current sheet residual oscillation shows that once the unstable oscillation is activated, the current sheet stops being continuous and forms mass lumps that are ejected outward.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Relative difference in V  r  (in the absolute sense) between cases 1 and 9 with the ordinary (left) and new (right) mesh. Before, the differences in the formulation of the BC between cases 1 and 9 led to relatively large differences in the velocity profile. With the improved mesh with smaller extrapolation effects, this is no longer the case.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Comparison of the convergence in the V  x  component between the two eclipse cases computed with and without an  E -field generating boundary.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Comparison of the shape of the “ballooning” current sheet of cases 2 and 3 as a result of a different B  r  formulation. For easier comparison, the red line following a case 2  B -field line (left) is projected onto the case 3 flow field (right), where the same line (starting and ending at the same point on the boundary) is followed in blue.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: The amount of ∇ ·  B  in the numerical solution, depending on the selection of the divergence cleaning constant (1 on the left, 0.4 on the right), is shown in terms of the logarithm of the absolute value of ∇ ·  B  (nondimensional).
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: The BC-independent mesh developed for coupling with other codes. The ghost cell is very small; thus, the outer BC extrapolation errors are limited. In addition, the boundary is shifted further away from the 21.5 R ⊙ from which the results are extracted, such that the solution at this coupling location is not affected by the BC formulation.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Logarithmic density profiles of the “low  E ” (left) and “large  E ” (right) simulations.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: The B  r  slope (logarithmic; right) along a streamer from the 2008 eclipse simulation on the BC-independent, extended grid (shown as a black line in the left panel), showing a steeper grid than the expected 1/r 2 scaling.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Comparison of the results of the 2008 simulation with “low  E ” (right) and “large  E ” (left) setups with the observations using the framework by Wagner et al. (2022).
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Comparison between the  B -field lines (with the absolute value of B  θ  in the background) for the old and new BC-independent grid, with both simulations extrapolating B  r  through the inverse square power. The results for the old grid with excessive divergence are shown on the left, while the results with the adjusted grid with small ghost cells are on the right.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Comparison of the nondimensional temperature profiles between the 2008 eclipse cases computed with (right) and without (left) an  E -field generating boundary.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Demonstration of how the new grid design (right) with a small ghost cell can help prevent excessive opening of the streamers observed with the original grid (left) with the same outer BCs.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: Magnetic field configuration, B  r  and B  θ  from PFSS, of the 2008 eclipse.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: The V  r  contours for the “low  E ” and “large  E ” 2008 eclipse cases.
Paper: To  E  or Not to  E : Numerical Nuances of Global Coronal Models
Authors: Michaela Brchnelova, Błażej Kuźma, Barbara Perri, Andrea Lani, Stefaan Poedts
Figure caption: The E  φ  component for the two eclipse cases computed with and without the  E -field generating boundary.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: Comparison of synthetic photometry of our standard-star spectra. Left: V-band residuals vs. V-band magnitude. Here synthetic magnitudes have been subtracted from filter photometry magnitudes. Stars are color coded by whether they are in the primary (blue) or secondary (magenta) samples. Note that some stars have several independent sources of filter photometry from the literature; hence those stars can overlap in their V-band magnitudes on the scale of this plot. The stars deviating the most from the mean are labeled with their name and source of photometry. These outliers have photometry from our most heterogeneous literature sources (often reporting on only a single star in our sample), so are not a serious concern. The results show that our standard-star network is linear (relative to filter photometry) over a span of 12 mag. Right: V-band residuals vs. B − V; this shows that for blue stars our primary and secondary standards agree well. For intermediate colors, there is enhanced scatter for both the primary and secondary standards. For redder colors, there appears to be ∼9 mmag offset between most of the primary standards and secondary standards. This offset appears to be the primary driver of the small V-band offset we measure for our standard-star network, and is more apparent because we have added a large number of red stars, e.g., in comparison to Bohlin & Landolt (2015).
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: The left column shows the mean atmosphere model (k 0 l  from Equation (6)), middle column shows the night-to-night dispersion (σ(k) l  from Equation (6)), and the right panel shows the uncertainty in k 0 l  (rounded to 0.1 mmag). Upper panels show the measured values with their physical decompositions, while the bottom panels show the residuals after the model is subtracted from the measurements. In the left residual panel, a pair of small discrepancies at the peaks of the ozone Chappuis band is apparent; these are not apparent in the dispersion, suggesting a small error in the Serdyuchenko et al. (2014) ozone template. The residual panels show evidence of a slight convolved-template mismatch at the O 2 A band, but this seems to be static (a glitch visible in the mean, but not in the dispersion). At all other wavelengths, the physical decomposition matches our measured atmosphere to better than a few millimagnitude per airmass.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: Photometry of BD+17°4708. Left: photometry vs. Julian date from the SNfactory (filled green circles), Hipparcos (Perryman et al. 1997), converted from Hp magnitudes to V using the formula of Bessell (2000; open red circles), and from Bohlin & Landolt (2015; open blue pentagons). The brightening trend in the Bohlin & Landolt (2015) photometry is readily apparent. It is difficult to definitively ascertain whether that brightening is supported by the Hipparcos data or not. But our new data show that such a brightening did not continue. Right: the same photometry vs. the orbital phase determined by Latham et al. (2002). The phase zero-point is arbitrary. For both figures, for the SNfactory data, we show the binned medians and then shade the range of the robust error on the median. For the left figure, we also show the binned medians and robust error on the median for the Hipparcos data.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: The mean offset between synthetic photometry and literature filter photometry for six different groupings of our standard stars. We plot the residuals for each of B − V, V, V − R, V − I, in which the filter photometry was originally analyzed and reported. The shaded bands, when evaluated at the discrete photometric indices, give the error on the means. We see generally good agreement—within a few millimagnitudes—between our flux-calibrated spectra and filter photometry. The agreement in V − R is especially impressive. The means of the different subsets agree within their uncertainties, except for V − I, where the primary and secondary calibrators are in tension by 2.8σ.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: Median residuals vs. seeing in equal-percentile bins for spectra extracted with both PSFs, separated by long and short exposures. The ﹩{{ \mathcal P }}_{{ \mathcal M }{ \mathcal G }}﹩ PSF (left panel) shows large systematic residuals for both very good and very bad seeing, and these trends are different between long and short exposures. Encouragingly, the ﹩{{ \mathcal P }}_{{\mathfrak{F}}}﹩ PSF does better on all fronts, having much smaller residuals (even for very bad seeing), and having similar behavior for both long and short exposures. On the basis of results like this, we chose the ﹩{{ \mathcal P }}_{{\mathfrak{F}}}﹩ PSF for our primary results. We note that, for long-exposure standard stars, the two PSFs give consistent calibration to within millimagnitudes, as discussed in the text.
Paper: Uniform Recalibration of Common Spectrophotometry Standard Stars onto the CALSPEC System Using the SuperNova Integral Field Spectrograph
Authors: David Rubin, G. Aldering, P. Antilogus, C. Aragon, S. Bailey, C. Baltay, S. Bongard, K. Boone, C. Buton, Y. Copin, S. Dixon, D. Fouchez, E. Gangler, R. Gupta, B. Hayden, W. Hillebrandt, A. G. Kim, M. Kowalski, D. Küsters, P.-F. Léget, F. Mondon, J. Nordin, R. Pain, E. Pecontal, R. Pereira, S. Perlmutter, K. A. Ponder, D. Rabinowitz, M. Rigault, K. Runge, C. Saunders, G. Smadja, N. Suzuki, C. Tao, S. Taubenberger, R. C. Thomas, M. Vincenzi
Figure caption: Our spectra of space-based CALSPEC stars that were used as primary calibrators and had observations on more than one night. Fluxes are linear in F(λ)λ 2 in order to balance the range of spectral slopes across the ensemble of standard stars, and the flux labeling is suppressed for clarity.