adsabs/AstroCLIMB huggingface dataset:
Paper: Early Planet Formation in Embedded Disks (eDisk). XVII. A Compact but Structured Keplerian Disk and Large-scale Streamers Revealed in the Class I Protostellar System IRAS 04169+2702
Authors: Ilseung Han, Woojin Kwon, Yusuke Aso, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Leslie W. Looney, Yuri Aikawa, Christian Flores, Itziar de Gregorio-Monsalvo, Patrick M. Koch, Chang Won Lee, Jeong-Eun Lee, Zhi-Yun Li, Zhe-Yu Daniel Lin, Jinshi Sai, Travis J. Thieme, Jonathan P. Williams, Sacha Gavino, Miyu Kido, Shih-Ping Lai, Nguyen Thi Phuong, Alejandro Santamaría-Miranda, Hsi-Wei Yen
Figure caption: Velocity dispersion (moment 2) maps for the 12CO (2–1) (from the left), 13CO (2–1), and C18O (2–1) emission of the SBLB data. Each panel has an identical spatial scale of 10″ × 10″, allowing direct comparison of the velocity dispersions between the CO isotopologues. The contours represent the integrated intensities (moment 0) of the line emission, which are the same as the contours shown in the middle column of Figure 4. The two orthogonal gray lines indicate the directions of the disk’s major (PA = 140°) and minor (PA = 50°) axes of the LB-only dust continuum image (Figure 1(c)). The black ellipses in the lower left denote the synthesized beams of the emission: 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩182 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩152 in 12CO, 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩189 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩151 in 13CO, and 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩188 × 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩149 in C18O (see also Table 3).
Paper: Balmer Absorption in Iron Low-ionization Broad Absorption Line Quasars
Authors: Karen M. Leighly, Sarah C. Gallagher, Hyunseop Choi, 현섭 최, Donald M. Terndrup, Julianna R. Voelker, Gordon T. Richards, Leah K. Morabito
Figure caption: Left panel: an example of one of the anticorrelations between measurements of dN/dv and LBol or Eddington ratio. The log of the significance for this correlation is given at the top of the plot. The circular marker color indicates the absorption line FWHM, which is weakly correlated with LBol, while the circular marker size indicates the log of the true column density, which is weakly anticorrelated with LBol. The errors on the parameters are shown in pink and cyan for the two objects that lack Hα observations. Right panel: the 12 Hα absorption profiles labeled by their object RAs in inverse order of outflow speed. There is a general trend for higher-velocity lines to be shallower and possibly broader.
Paper: Balmer Absorption in Iron Low-ionization Broad Absorption Line Quasars
Authors: Karen M. Leighly, Sarah C. Gallagher, Hyunseop Choi, 현섭 최, Donald M. Terndrup, Julianna R. Voelker, Gordon T. Richards, Leah K. Morabito
Figure caption: The anticorrelation between Eddington ratio and velocity offset. The red points mark objects that have Hα in the bandpass; the velocity offset is measured from Hβ for the two objects with blue points. The p-values included above the plot were computed for the 12-member sample that includes Hα in the spectrum (p12) and the full sample (p14). The anticorrelation is common among BAL quasars but is weak in this sample, most likely because most of the targets belong to the loitering outflow class (above the green dashed line). First identified by H. Choi et al. (2022b), loitering outflow quasars are identified by their low outflow speeds and compact outflows.
Paper: Balmer Absorption in Iron Low-ionization Broad Absorption Line Quasars
Authors: Karen M. Leighly, Sarah C. Gallagher, Hyunseop Choi, 현섭 최, Donald M. Terndrup, Julianna R. Voelker, Gordon T. Richards, Leah K. Morabito
Figure caption: Relationship between the absorption line width and αoi, the point-to-point slope between 5100 Å and 3 μm. The red points mark objects that have Hα in the bandpass; the velocity offset is measured from Hβ for the two objects with blue points. The horizontal line marks the αoi value from the C. M. Krawczyk et al. (2013) composite spectrum. Objects with values near or below this line have no reddening and weak torus emission. The object with the large value of αoi is SDSS 1621+0819, and the value is large due to a large flux in WISE W3, with SNR = 13.9.
Paper: Nitrogen-bearing Species on Trans-Neptunian Objects Revealed by JWST/DiSCo-TNOs
Authors: S. Cryan, R. Brunetto, A. Guilbert-Lepoutre, N. Pinilla-Alonso, E. Hénault, B. J. Holler, Y. Pendleton, D. Cruikshank, J. Stansberry, J. P. Emery, L. T. McClure, J. Licandro, V. Lorenzi, T. G. Müller, N. Peixinho, B. Harvison, C. Schambeau, M. T. Bannister, A. C. de Souza-Feliciano, M. N. de Prá
Figure caption: (A) The 4.62 µm band area relative to the 4.5 µm band area. Double-Dip-TNOs with detection <2σ in both the 4.5 µm and 4.62 µm features are not included in the plot. TNOs Huya (ID 3) and 2004 PG115 (ID 20) are plotted in gray data points. The Pearson correlation coefficient (r), and its associated p-value and error (D. G. Bonett & T. A. Wright 2000), appears in the bottom right. (B) The Cliff2-TNOs 1999 OX3 (ID 104) and Lempo (ID 6) compared to OCN− produced in the laboratory from the thermal processing of a HNCO:CO (1:1) ice (J. H. Novozamsky et al. 2001, via the Leiden Ice Database for Astrochemistry), as well as the energetic processing of a N2:CH4:H2O (1:1:1) ice using 200 keV H+ (M. Accolla et al. 2018) and a H2O:NH3:HNCO (140:8:1) ice using UV photons (F. A. van Broekhuizen et al. 2004). (C) A selection of TNOs from our sample compared to the dense molecular cloud NIR38 (M. K. McClure et al. 2023) and the massive protostar W 33 A (ISO-SWS data archive; G. C. Sloan et al. 2003) in the 3.7–5.1 µm spectral region. In panels (B) and (C), vertical lines mark notable spectral features. Spectra are shifted in the y direction for clarity.
Paper: The Gamma-Ray Emission from Radio Galaxies and Their Contribution to the Isotropic Gamma-Ray Background
Authors: Antonio Circiello, Alex McDaniel, Mattia Di Mauro, Christopher Karwin, Nikita S. Khatiya, Marco Ajello, Fiorenza Donato, Dieter Hartmann, Andrew W. Strong
Figure caption: Integrated γ-ray emission from RGs. The green band is the predicted contribution from the detected RG population, with its 1σ uncertainty. The gray band is the predicted contribution from the subthreshold RG population with its 1σ uncertainty. The red band is the contribution obtained combining the results of both samples of RGs, with its 1σ uncertainty. The dashed blue, orange, and purple lines are the contributions from M. Di Mauro et al. (2014a), D. Hooper et al. (2016), and F. W. Stecker et al. (2019), respectively. The black dotted–dashed line is the contribution from Y. Fukazawa et al. (2022). The black data points are the LAT evaluation of the IGRB (see M. Ackermann et al. 2015).
Paper: Nitrogen-bearing Species on Trans-Neptunian Objects Revealed by JWST/DiSCo-TNOs
Authors: S. Cryan, R. Brunetto, A. Guilbert-Lepoutre, N. Pinilla-Alonso, E. Hénault, B. J. Holler, Y. Pendleton, D. Cruikshank, J. Stansberry, J. P. Emery, L. T. McClure, J. Licandro, V. Lorenzi, T. G. Müller, N. Peixinho, B. Harvison, C. Schambeau, M. T. Bannister, A. C. de Souza-Feliciano, M. N. de Prá
Figure caption: (A) A selection of Cliff2-TNOs and the centaur 2002 KY14 (ID 38) compared to spectra with a similar 4.5 µm feature: (bottom to top) the N-rich UCAMM DC06-05-65 (E. Dartois et al. 2013), a tholin produced from a spark discharge in a mixture of equimolar CH4 and NH3 gas and 2.5% H2O vapor (C. Sagan & B. N. Khare 1979), irradiation residues from N2:CH4:CO (1:1:1) ice using 200 keV H+ (M. Accolla et al. 2018) and HCN ice using 0.8 MeV H+ (P. A. Gerakines et al. 2004), and a Hapke model of a CH3OH and amorphous carbon mixture. (B) TNO spectra compared to a spectrum of carbon chain oxides produced from the 200 keV H+ irradiation of CO ice (M. E. Palumbo et al. 2004) and HNCO produced from the 200 keV H+ irradiation of N2:CH4:H2O (1:1:1) ice (M. Accolla et al. 2018). In both panels, a gray shaded region marks the broad 4.5 µm feature.
Paper: Nitrogen-bearing Species on Trans-Neptunian Objects Revealed by JWST/DiSCo-TNOs
Authors: S. Cryan, R. Brunetto, A. Guilbert-Lepoutre, N. Pinilla-Alonso, E. Hénault, B. J. Holler, Y. Pendleton, D. Cruikshank, J. Stansberry, J. P. Emery, L. T. McClure, J. Licandro, V. Lorenzi, T. G. Müller, N. Peixinho, B. Harvison, C. Schambeau, M. T. Bannister, A. C. de Souza-Feliciano, M. N. de Prá
Figure caption: (A) The 4.5 µm band area relative to its center, with vertical line marking the 4.46 µm and 4.52 µm spectral signatures due to CH3OH and a CN-bearing refractory on the N-rich UCAMM, DC06-05-65, respectively. (B–D) The 4.5 µm band area plotted against band areas corresponding to C–H stretching between 3.36 and 3.56 µm (B), O–H and N–H groups about 3 µm (C), and the 2.27 µm feature (D). In all panels only the Double-Dip-TNOs with detection >2σ in the 4.5 µm feature are shown and TNOs Huya (ID 3) and 2004 PG115 (ID 20) are plotted in gray data points. Pearson correlation coefficients (r), and their associated p values and errors (D. G. Bonett & T. A. Wright 2000), appear in the bottom right of panels (B), (C) and (D).
Paper: The Gamma-Ray Emission from Radio Galaxies and Their Contribution to the Isotropic Gamma-Ray Background
Authors: Antonio Circiello, Alex McDaniel, Mattia Di Mauro, Christopher Karwin, Nikita S. Khatiya, Marco Ajello, Fiorenza Donato, Dieter Hartmann, Andrew W. Strong
Figure caption: Correlation between the 1 and 800 GeV γ-ray luminosity and the luminosity of the radio core at 5 GHz for the RGs analyzed in this paper. The green points are the individually detected RGs. The values for the γ-ray luminosity are obtained through their individual TS profiles obtained in this analysis, while the core luminosities come from N. S. Khatiya et al. (2024). The green band is the Lγ–LC,5GHz correlation for the detected RGs with its 1σ uncertainty. The gray band is the 1σ band on the Lγ–LC,5GHz correlation derived from the analysis of the subthreshold sample. The red band represents the Lγ–LC,5GHz correlation from the combination of the detected and undetected samples, with its 1σ uncertainty. We also include results from M. Di Mauro et al. (2014a) and F. W. Stecker et al. (2019), as shown in the dashed blue and yellow lines, respectively, with their 1σ uncertainties.
Paper: The Gamma-Ray Emission from Radio Galaxies and Their Contribution to the Isotropic Gamma-Ray Background
Authors: Antonio Circiello, Alex McDaniel, Mattia Di Mauro, Christopher Karwin, Nikita S. Khatiya, Marco Ajello, Fiorenza Donato, Dieter Hartmann, Andrew W. Strong
Figure caption: 5 GHz core luminosity vs. redshift for the sample of detected RGs at γ-rays (green circles) and for the sample of subthreshold RGs (gray circles) presented in Section 2.
Paper: The Gamma-Ray Emission from Radio Galaxies and Their Contribution to the Isotropic Gamma-Ray Background
Authors: Antonio Circiello, Alex McDaniel, Mattia Di Mauro, Christopher Karwin, Nikita S. Khatiya, Marco Ajello, Fiorenza Donato, Dieter Hartmann, Andrew W. Strong
Figure caption: Core dominance (see Equation (3)) vs. redshift for the sample of detected RGs at γ-rays (green circles) and for the sample of subthreshold RGs (gray circles). The subsample of undetected RGs chosen to have R > 0.15 is highlighted with red contours. The green, gray, and red lines represent the average R of the detected RGs, the undetected RGs, and the subsample of undetected RGs, respectively.
Paper: The Gamma-Ray Emission from Radio Galaxies and Their Contribution to the Isotropic Gamma-Ray Background
Authors: Antonio Circiello, Alex McDaniel, Mattia Di Mauro, Christopher Karwin, Nikita S. Khatiya, Marco Ajello, Fiorenza Donato, Dieter Hartmann, Andrew W. Strong
Figure caption: Stacked TS profile for the subthreshold RG sample. The coordinates of the black cross indicate the best estimates for the average integrated flux and photon index of the population. The green contours are the uncertainties at the 1σ, 2σ, and 3σ levels, respectively.
Paper: Role of Sunspot Latitude versus Tilt in Determining the Polar Field and Amplitude of the Next Cycle: Cause of the Weak Solar Cycle 20
Authors: Bidisha Dey, Anu Sreedevi, Bidya Binay Karak
Figure caption: (a) Polar field strength (A(t) index) at the solar minimum plotted against the total sunspot area (strength) of the same solar cycle for Cycles 15–22. (b) Same as (a), but the amplitude of the next solar cycle as measured by the total sunspot area for Cycles 12–23. The cycle numbers are labeled to correspond to the value of n (horizontal axis). The red dotted line shows a polynomial fit, while the blue dashed–dotted line represents a linear fit excluding the data point for Cycle 19.
Paper: Role of Sunspot Latitude versus Tilt in Determining the Polar Field and Amplitude of the Next Cycle: Cause of the Weak Solar Cycle 20
Authors: Bidisha Dey, Anu Sreedevi, Bidya Binay Karak
Figure caption: Solid black line represents the daily calibrated group area as a function of time from S. Mandal et al. (2020). The dashed blue line represents the monthly total sunspot number (International Sunspot Number V2) from World Data Center (WDC)-SILSO, Royal Observatory of Belgium, Brussels. The cycle numbers are marked on the plot.
Paper: Role of Sunspot Latitude versus Tilt in Determining the Polar Field and Amplitude of the Next Cycle: Cause of the Weak Solar Cycle 20
Authors: Bidisha Dey, Anu Sreedevi, Bidya Binay Karak
Figure caption: (a) Strength of cycle n + 1 vs. the strength of cycle n as obtained from the total sunspot area . Note, the sunspot area data is available only from Cycle 12 onward. For earlier times, sunspot number data (V2) have been rescaled to match the sunspot area scale, and these points are shown in gray. (b) The same as (a), but for the reconstructed sunspot number from C14 data of I. G. Usoskin et al. (2021), and it is for the cycle average number and not the total number. Here we have 85 cycles, and we follow the same convention for numbering the cycles as given in I. G. Usoskin et al. (2021). The oval highlights the data points for which the cycle strength of n + 1 is significantly lower than that of cycle n.
Paper: Role of Sunspot Latitude versus Tilt in Determining the Polar Field and Amplitude of the Next Cycle: Cause of the Weak Solar Cycle 20
Authors: Bidisha Dey, Anu Sreedevi, Bidya Binay Karak
Figure caption: Polar field strength (A(t) index) at the solar minimum vs. the (a) total area divided by the mean latitude of sunspots, (b) total area times the mean tilt angle of sunspots, and (c) total area times the mean tilt angle of sunspots divided by the mean latitude of sunspots of a cycle.
Paper: A Search for Be Stars in Multiple Systems within the Solar Neighborhood
Authors: V. M. Kalari, R. Salinas, C. Sáez-Carvajal, R. D. Oudmaijer, S. Howell, S. Caballero-Nieves, K. Kamp, R. Matson, N. Scott, T. Cao, Z. Hartman, H. Kim
Figure caption: The image, power spectrum, model fit (accounting for the point source standard), and residual are shown from the reduction steps for HD 56039 in the blue filter (top). The bottom panel shows the slice across the image (along the blue line in the top panel). The power spectrum fringe indicates the close-in companion.
Paper: Slab Turbulence in the Very Local Interstellar Medium and the IBEX Ribbon
Authors: E. J. Zirnstein, D. J. McComas, J. Giacalone, G. P. Zank, F. Guo, J. Heerikhuisen, H. Li, D. B. Reisenfeld
Figure caption: Comparison of nine cross sections across the ribbon between the models (colored curves) and the data (black curve and dark/light gray contours).
Paper: Slab Turbulence in the Very Local Interstellar Medium and the IBEX Ribbon
Authors: E. J. Zirnstein, D. J. McComas, J. Giacalone, G. P. Zank, F. Guo, J. Heerikhuisen, H. Li, D. B. Reisenfeld
Figure caption: Partial sky map of the modeled ribbon case for slab-50%/2D-50% with nine great circles drawn across the ribbon starting from the ribbon center (RC). We take cross sections of the ribbon along these great circles to compare the intensities and peak locations between the models and data.
Paper: Slab Turbulence in the Very Local Interstellar Medium and the IBEX Ribbon
Authors: E. J. Zirnstein, D. J. McComas, J. Giacalone, G. P. Zank, F. Guo, J. Heerikhuisen, H. Li, D. B. Reisenfeld
Figure caption: Partial sky maps of the modeled ribbon, with five ratios of slab turbulence: slab-90%/2D-10%, slab-70%/2D-30%, slab-50%/2D-50%, slab-30%/2D-70%, and slab-10%/2D-90% turbulence. Note the color scale is different than Figure 1.
Paper: Slab Turbulence in the Very Local Interstellar Medium and the IBEX Ribbon
Authors: E. J. Zirnstein, D. J. McComas, J. Giacalone, G. P. Zank, F. Guo, J. Heerikhuisen, H. Li, D. B. Reisenfeld
Figure caption: IBEX ribbon-only maps measured at ESA 3 (central energy 1.11 keV). The data are Compton–Getting and survival-probability corrected yearly maps weight averaged over 2009–2011.
Paper: Vanishing Refractories: Tracing Dust Evolution in the BP Tau Protoplanetary Disk
Authors: Marbely Micolta, Justin Svarc, Nuria Calvet, Ezequiel Manzo-Martínez, Thanawuth Thanathibodee, Gladis Magris C., Avalon Littwiller
Figure caption: SED of BP Tau. In black, observational data include photometry and Spitzer/IRS spectra (references in text), corrected for reddening. The emission from the inner disk wall (blue), the optically thin region (red), the outer disk wall (green), and the outer disk (purple) is also shown. The photosphere is shown as a dotted line. An inset of the region of the silicate features is shown in the upper right corner.
Paper: Vanishing Refractories: Tracing Dust Evolution in the BP Tau Protoplanetary Disk
Authors: Marbely Micolta, Justin Svarc, Nuria Calvet, Ezequiel Manzo-Martínez, Thanawuth Thanathibodee, Gladis Magris C., Avalon Littwiller
Figure caption: Schematic view of BP Tau. The composition of the gas in the accretion flows (proxy for the innermost gas disk) is obtained from the emission-line profile modeling (see Section 5.2). Dust composition for each disk region and their location is obtained from the SED modeling (see Section 5.3). We find a clear change in the Mg content of the crystalline olivine with radius, discussed in Section 6.3.
Paper: Vanishing Refractories: Tracing Dust Evolution in the BP Tau Protoplanetary Disk
Authors: Marbely Micolta, Justin Svarc, Nuria Calvet, Ezequiel Manzo-Martínez, Thanawuth Thanathibodee, Gladis Magris C., Avalon Littwiller
Figure caption: Left: comparison of the best-fit model and the observations for Mg II k. Gray regions are excluded from the fitting. Right: parameter distribution for the top-25 best-fitting models. The solid line is the median value for each parameter; dashed lines represent the 25th and 75th percentiles.
Paper: Vanishing Refractories: Tracing Dust Evolution in the BP Tau Protoplanetary Disk
Authors: Marbely Micolta, Justin Svarc, Nuria Calvet, Ezequiel Manzo-Martínez, Thanawuth Thanathibodee, Gladis Magris C., Avalon Littwiller
Figure caption: Total opacity per gram of dust for crystalline material: enstatite (green), Mg-rich crystalline olivine (forsterite, blue), Fe-rich crystalline olivine (fayalite, red). The maximum size of the grains is a﹩{}_{{\rm{\max }}}=0.25\,\mu ﹩m.
Paper: Vanishing Refractories: Tracing Dust Evolution in the BP Tau Protoplanetary Disk
Authors: Marbely Micolta, Justin Svarc, Nuria Calvet, Ezequiel Manzo-Martínez, Thanawuth Thanathibodee, Gladis Magris C., Avalon Littwiller
Figure caption: Parameter distribution for the top-150 best-fitting models for the optically thin region structural parameters and dust properties. The solid line is the median value for each parameter; dashed lines represent the 25th and 75th percentiles.
Paper: Vanishing Refractories: Tracing Dust Evolution in the BP Tau Protoplanetary Disk
Authors: Marbely Micolta, Justin Svarc, Nuria Calvet, Ezequiel Manzo-Martínez, Thanawuth Thanathibodee, Gladis Magris C., Avalon Littwiller
Figure caption: Left: comparison of the best-fit model and the observations for Ca II K. Gray regions are excluded from the fitting. Right: parameter distribution for the top-25 best-fitting models. The solid line is the median value for each parameter; dashed lines represent the 25th and 75th percentiles.
Paper: Vanishing Refractories: Tracing Dust Evolution in the BP Tau Protoplanetary Disk
Authors: Marbely Micolta, Justin Svarc, Nuria Calvet, Ezequiel Manzo-Martínez, Thanawuth Thanathibodee, Gladis Magris C., Avalon Littwiller
Figure caption: Parameter distribution for the top-150 best-fitting models for the outer wall structural parameters and dust properties. The solid line is the median value for each parameter; dashed lines represent the 25th and 75th percentiles.
Paper: Vanishing Refractories: Tracing Dust Evolution in the BP Tau Protoplanetary Disk
Authors: Marbely Micolta, Justin Svarc, Nuria Calvet, Ezequiel Manzo-Martínez, Thanawuth Thanathibodee, Gladis Magris C., Avalon Littwiller
Figure caption: Left: comparison of the best-fit model and the observations for Hα. Right: parameter distribution for the top-25 best-fitting models. The solid line is the median value for each parameter; dashed lines represent the 25th and 75th percentiles.
Paper: Vanishing Refractories: Tracing Dust Evolution in the BP Tau Protoplanetary Disk
Authors: Marbely Micolta, Justin Svarc, Nuria Calvet, Ezequiel Manzo-Martínez, Thanawuth Thanathibodee, Gladis Magris C., Avalon Littwiller
Figure caption: Parameter distribution for the top-150 best-fitting models for the inner wall structural parameters and dust properties. The solid line is the median value for each parameter; dashed lines represent the 25th and 75th percentiles.
Paper: Mapping Atmospheric Features of the Planetary-mass Brown Dwarf SIMP 0136 with JWST NIRISS
Authors: Roman Akhmetshyn, Étienne Artigau, Nicolas B. Cowan, Michael K. Plummer, Fei Wang, Ben Burningham, Björn Benneke, René Doyon, Ray Jayawardhana, David Lafrenière, Stanimir A. Metchev, Jason F. Rowe
Figure caption: (a) 1.6–1.8 μm band lightcurve (black dots) fitted with different mapping models. Green dashed line: four-mode sinusoidal fit excluding the third mode; blue dashed line: four-mode sinusoids with the odd mode; solid red line: spherical harmonic mapping. Plot below shows residuals of each method; the sinusoidal odd mode fit and spherical harmonics overlap due to identical performance. (b) Power of four Fourier modes from decomposition of all lightcurves. The nonzero third mode confirms the object’s inclination and implies there is a north–south asymmetry in the atmosphere of SIMP 0136. (c.1) Best-fit spherical harmonics map inferred from the 1.0 to 1.31 μm band lightcurve with the uniform prior on Ylm coefficients. This map demonstrates north–south asymmetry but is physically implausible. (c.2) A spherical harmonics map of the same lightcurve with Ylm priors of an arbitrary spot position. The first map fits the observed lightcurve with χ2 = 210; the second fits with χ2 = 209.8. The fact that both maps look different yet produce indistinguishable lightcurves is a testament to the degeneracy of mapping without enough external constraints.
Paper: Mapping Atmospheric Features of the Planetary-mass Brown Dwarf SIMP 0136 with JWST NIRISS
Authors: Roman Akhmetshyn, Étienne Artigau, Nicolas B. Cowan, Michael K. Plummer, Fei Wang, Ben Burningham, Björn Benneke, René Doyon, Ray Jayawardhana, David Lafrenière, Stanimir A. Metchev, Jason F. Rowe
Figure caption: NIRISS time-averaged spectrum over an entire rotation (black line) compared to various Diamondback grid models and their combinations. A single Diamondback model cannot accurately reproduce data. The interpolation of parameters allows the achievement of higher accuracy, with the green line showing a closer match with data. However, only a linear combination of grid models can substantially explain data. The red line shows such a combination of three spectra of different physical properties, and the blue line is an admixture of six models, which is favored by BIC. We allowed gravitational acceleration to vary because the consensus is that it is between 100 and 316 cm s−2. The lower part of the figure shows residuals normalized to data error. The error was scaled up by 7.8 to efficiently utilize BIC.