adsabs/AstroCLIMB huggingface dataset:
Paper: Enough Sulfur and Iron for Potential Life Make Enceladus’s Ocean Fully Habitable
Authors: Weiming Xu, Can Liu, Ao Zhang, Maggie Lau, H. James Cleaves, Fang Huang, Christopher R. Glein, Jihua Hao
Figure caption: Comparisons of the elemental stoichiometry in intracellular fluid and ocean water. Panel (a) shows the elemental stoichiometry in the intracellular fluid of phytoplankton and Earth seawater. The filled boxes mark the range of the carbon-normalized elemental ratio of marine phytoplankton to the carbon-normalized elemental ratio dissolved in seawater. Panel (b) shows the elemental stoichiometry in intracellular fluid and the Enceladus ocean. Boxes of dashed lines represent our predictions for Fe and S, whereas filled boxes are the results from analyses of Cassini data. Elements to the upper left of the gray dashed line are in excess in ocean water, while elements to the lower right of the gray dashed line may be limiting for life. The full data set and reference list are shown in Table B1.
Paper: Enough Sulfur and Iron for Potential Life Make Enceladus’s Ocean Fully Habitable
Authors: Weiming Xu, Can Liu, Ao Zhang, Maggie Lau, H. James Cleaves, Fang Huang, Christopher R. Glein, Jihua Hao
Figure caption: Equilibrium speciation diagrams of aqueous Fe and S. Speciation of dissolved (a) Fe and (b) S as a function of pH and activity (∼molality) of dissolved H2 at 0°C and 70 bar (1 bar for reference shown in dashed lines). These diagrams are for the Fe–O–H and S–O–H systems. Blue shaded areas correspond to estimated ranges of pH and H2,aq activity in the Enceladus ocean (C. R. Glein et al. 2018). Note the different vertical scales in panels (a) and (b).
Paper: Strong Rest-UV Emission Lines in a “Little Red Dot” Active Galactic Nucleus at z = 7: Early Supermassive Black Hole Growth alongside Compact Massive Star Formation?
Authors: Hollis B. Akins, Caitlin M. Casey, Danielle A. Berg, John Chisholm, Aidan P. Cloonan, Maximilien Franco, Steven L. Finkelstein, Seiji Fujimoto, Anton M. Koekemoer, Vasily Kokorev, Erini Lambrides, Brant E. Robertson, Anthony J. Taylor, David A. Coulter, Ori Fox, Mitchell Karmen
Figure caption: Line ratio diagnostics in the UV and optical. In both panels, model grids for AGN and star-forming galaxies from A. Feltre et al. (2016) and J. Gutkin et al. (2016) are shown in red and blue, respectively. Left: the C III]/C IV vs. C III]/He II UV line ratio diagnostic diagram. We plot the classification regions from J. Scholtz et al. (2023) with dashed lines, and we additionally include PopIII and DCBH models from K. Nakajima & R. Maiolino (2022) and observed low-z type I AGN from J. K. Kuraszkiewicz et al. (2004). COS-66964 is shown in red, where we adopt the 95th percentile of the He II flux as a 2σ upper limit. Several high-redshift sources are also shown, including GN-z11 (A. J. Bunker et al. 2023), GHZ2 (M. Castellano et al. 2024), GS-z12 (F. D’Eugenio et al. 2023), RXCJ2248-ID (M. W. Topping et al. 2024), and GS-NDG-9422 (A. J. Cameron et al. 2024). Based on the nondetection of He II λ1640, the UV emission from COS-66964 lies in the composite region and is consistent with ionization from massive/low-metallicity stars. Right: the He II λ4687/Hβ vs. [N II]/Hα diagram. Model grids are the same as in the left panel, and we additionally plot extreme He II-emitting SFGs from SDSS (M. Shirazi & J. Brinchmann 2012). Based on the He II λ4687/Hβ ratio, the rest-optical emission from COS-66964 is inconsistent with star formation—even in the most extreme He II-emitting WR galaxies—and is better fit by ionization from the AGN.
Paper: Strong Rest-UV Emission Lines in a “Little Red Dot” Active Galactic Nucleus at z = 7: Early Supermassive Black Hole Growth alongside Compact Massive Star Formation?
Authors: Hollis B. Akins, Caitlin M. Casey, Danielle A. Berg, John Chisholm, Aidan P. Cloonan, Maximilien Franco, Steven L. Finkelstein, Seiji Fujimoto, Anton M. Koekemoer, Vasily Kokorev, Erini Lambrides, Brant E. Robertson, Anthony J. Taylor, David A. Coulter, Ori Fox, Mitchell Karmen
Figure caption: COS-66964 in context among high-z AGN. Left: BH mass vs. redshift. COS-66964 is shown in red. Filled points indicate JWST-selected AGN (A. D. Goulding et al. 2023; Y. Harikane et al. 2023; D. D. Kocevski et al. 2023; V. Kokorev et al. 2023, 2024b; R. L. Larson et al. 2023; R. Maiolino et al. 2024b; Á. Bogdán et al. 2024; L. J. Furtak et al. 2024; I. Juodžbalis et al. 2024; R. Maiolino et al. 2024c; B. Wang et al. 2024). Open points indicate classical QSOs selected from ground-based surveys, from the compilation of X. Fan et al. (2023, gray) and objects with individual host galaxy measurements via 2D decomposition (X. Ding et al. 2023; M. A. Stone et al. 2024; M. Yue et al. 2024b). We show the range of evolutionary pathways for AGN, starting from stellar mass seeds (blue, M ∼ 10–300 M⊙, z ∼ 15–30) and DCBH seeds (purple, M ∼ 103−5 M⊙, z ∼ 10–20) and accreting at the Eddington limit. Right: BH mass vs. stellar mass. Points are the same as in the left panel. The blue line and shaded region shows the local relation from A. E. Reines & M. Volonteri (2015). Based on our SED decomposition, COS-66964 has a MBH/M⋆ ratio ∼0.1, consistent with other JWST-selected AGN at z ≳ 4.
Paper: Strong Rest-UV Emission Lines in a “Little Red Dot” Active Galactic Nucleus at z = 7: Early Supermassive Black Hole Growth alongside Compact Massive Star Formation?
Authors: Hollis B. Akins, Caitlin M. Casey, Danielle A. Berg, John Chisholm, Aidan P. Cloonan, Maximilien Franco, Steven L. Finkelstein, Seiji Fujimoto, Anton M. Koekemoer, Vasily Kokorev, Erini Lambrides, Brant E. Robertson, Anthony J. Taylor, David A. Coulter, Ori Fox, Mitchell Karmen
Figure caption: JWST/NIRCam photometry and the NIRSpec PRISM spectrum for COS-66964. Top: cutouts in the eight NIRCam bands available from PRIMER, as well as an RGB image. We also highlight the position of the NIRSpec shutters over the RGB image. Bottom: the 2D and optimally extracted 1D spectrum. The 1σ uncertainty on the spectrum is indicated with the gray shaded region. Several notable emission lines are marked, including Lyα, C IV, C III], Hβ, [O III], and Hα. Emission lines labeled in gray are not significantly detected (see Section 3.2). The continuum is detected across the full wavelength range and exhibits a turnover from blue to red around 3 μm (rest frame 3800 Å).
Paper: Strong Rest-UV Emission Lines in a “Little Red Dot” Active Galactic Nucleus at z = 7: Early Supermassive Black Hole Growth alongside Compact Massive Star Formation?
Authors: Hollis B. Akins, Caitlin M. Casey, Danielle A. Berg, John Chisholm, Aidan P. Cloonan, Maximilien Franco, Steven L. Finkelstein, Seiji Fujimoto, Anton M. Koekemoer, Vasily Kokorev, Erini Lambrides, Brant E. Robertson, Anthony J. Taylor, David A. Coulter, Ori Fox, Mitchell Karmen
Figure caption: Zoom-in around several emission lines of interest in the NIRSpec/PRISM spectrum of COS-66964. In all panels, the spectrum has been continuum-subtracted using the best-fit model. Blue lines and shaded regions show the posterior model spectrum and include the uncertainty on the subtracted continuum. For Hβ, He I λ5876, and Hα, we show the narrow+broad line decomposition in orange and red, respectively. We derive narrow/broad FWHMs of ﹩20{0}_{-50}^{+50}.﹩ and ﹩201{0}_{-120}^{+130}﹩ km s−1, respectively. The blended lines Hγ+[O III] λ4363 and Si II+[Fe X] are fit with multiple Gaussians, which are plotted separately in purple/green dashed lines. For Mg II, we overplot the SDSS QSO composite (D. E. Vanden Berk et al. 2001), scaled to match the observed continuum and convolved to the PRISM resolution.
Paper: Strong Rest-UV Emission Lines in a “Little Red Dot” Active Galactic Nucleus at z = 7: Early Supermassive Black Hole Growth alongside Compact Massive Star Formation?
Authors: Hollis B. Akins, Caitlin M. Casey, Danielle A. Berg, John Chisholm, Aidan P. Cloonan, Maximilien Franco, Steven L. Finkelstein, Seiji Fujimoto, Anton M. Koekemoer, Vasily Kokorev, Erini Lambrides, Brant E. Robertson, Anthony J. Taylor, David A. Coulter, Ori Fox, Mitchell Karmen
Figure caption: Rest-frame UV C III]/C IV vs. C III]/[O III], highlighting the potentially elevated C/O ratio in COS-66964. We plot model grids for star-forming galaxies from J. Gutkin et al. (2016) at five metallicities between 0% and 20% solar (metallicities >20% solar are inconsistent with the measured C III]/C IV ratio). We outline the parameter space spanned by the grids at Z/Z⊙ ∼ 0.7% with colored lines indicating the varying ionization parameter ﹩\mathrm{log}\,U﹩ and carbon-to-oxygen abundance ratio (C/O). The nondetection of [O III] λλ1660, 1666 in COS-66964 implies a supersolar C/O, which may indicate a bursty star formation history or exotic stellar populations, such as supermassive stars.
Paper: Strong Rest-UV Emission Lines in a “Little Red Dot” Active Galactic Nucleus at z = 7: Early Supermassive Black Hole Growth alongside Compact Massive Star Formation?
Authors: Hollis B. Akins, Caitlin M. Casey, Danielle A. Berg, John Chisholm, Aidan P. Cloonan, Maximilien Franco, Steven L. Finkelstein, Seiji Fujimoto, Anton M. Koekemoer, Vasily Kokorev, Erini Lambrides, Brant E. Robertson, Anthony J. Taylor, David A. Coulter, Ori Fox, Mitchell Karmen
Figure caption: Results from multicomponent SED fitting to COS-66964. The NIRSpec/PRISM spectrum is shown in light gray in the background. We show the stellar+nebular continuum model in blue, which dominates in the rest-frame UV, and the AGN continuum model in red, which dominates in the optical. In both cases we show the posterior 16th–84th percentiles with the shaded region. The total model, which includes both continuum components and the fitted nebular lines, is shown in black and matches the observed spectrum and photometry well.
Paper: Detectability of Solar Rotation Period across Various Wavelengths
Authors: Valeriy Vasilyev, Timo Reinhold, Alexander I. Shapiro, Theodosios Chatzistergos, Natalie Krivova, Sami K. Solanki
Figure caption: Recovery of the solar rotation period at various wavelengths (a). Shown are probabilities of detecting the true solar rotation period using the autocovariance technique in the original SSI data (black) and its facular (red) and spot (blue) components at a random phase of the activity cycle. For illustrative purposes we also show disk-integrated facular (b) and spot (c) contrasts and the spot-to-facular contrast ratio (d).
Paper: Detectability of Solar Rotation Period across Various Wavelengths
Authors: Valeriy Vasilyev, Timo Reinhold, Alexander I. Shapiro, Theodosios Chatzistergos, Natalie Krivova, Sami K. Solanki
Figure caption: Recovery of the solar rotation period as a function of time (abscissa) and wavelength (ordinate). (a) Measured LPHs. (b) Measured rotation periods. (c) White patches indicate wavelengths and times where the true rotation period is recoverable, while gray patches represent the wavelengths and times where it is not. (d) The TSI time series covering the same time interval for comparison.
Paper: Detectability of Solar Rotation Period across Various Wavelengths
Authors: Valeriy Vasilyev, Timo Reinhold, Alexander I. Shapiro, Theodosios Chatzistergos, Natalie Krivova, Sami K. Solanki
Figure caption: Determination of solar rotation period using the ACF. Top panels: 180 day-long time series of SSI averaged over a 441–442 nm spectral interval (left) as well as the facular (middle) and spot (right) contributions to this time series. The long-term trends from these three time series were removed by subtracting the 81 day running mean. Bottom panels: ACFs computed for the time series shown in the respective top panels. Red markers indicate the highest peaks for each case (at a nonzero time lag).
Paper: Detectability of Solar Rotation Period across Various Wavelengths
Authors: Valeriy Vasilyev, Timo Reinhold, Alexander I. Shapiro, Theodosios Chatzistergos, Natalie Krivova, Sami K. Solanki
Figure caption: Detectability of the solar rotation in photometric observations with a rectangular filter. The probability is shown as a function of the central wavelength and width of the filter.
Paper: Exploring the Complex Heliotail Boundary by an Extended Level Set Approach
Authors: C. Onubogu, M. Opher, M. Kornbleuth, G. Tóth, V. Florinski
Figure caption: The HP defined by the level set isosurface, fHP = 0. (a) The isosurface results in a long, connected heliotail. (b) A cut through the heliotail at X = 490 au downwind of the Sun as seen in the inset. The yellow contour of the level set, fHP = 0, shows the collimated lobes connected thinly across the heliotail. (c, d) Side views of the fHP = 0 isosurface with green interstellar magnetic field lines, gray solar magnetic field lines, and purple interstellar velocity field lines shown. ISM plasma flows through the heliotail as seen by the trajectories of both the interstellar magnetic and velocity field lines. The field-line behavior is not fully consistent with this level set characterization for the HP.
Paper: Exploring the Complex Heliotail Boundary by an Extended Level Set Approach
Authors: C. Onubogu, M. Opher, M. Kornbleuth, G. Tóth, V. Florinski
Figure caption: Contours of the (a) plasma density, (b) speed, and (c) magnetic field strength in the MFP cut. The green-yellow color contours in plasma density show the mixed region of solar wind and ISM plasma. This mixed region is turbulent, inferred by the disordered flow field seen in the plasma speed and reconnection regions (regions where magnetic intensity dissipates) in the low-latitude heliotail. Various level set contours of fHP =  0.99, 0.75, 0.5, and 0 are shown in panels (d)–(g), in the same view as the top row of panels. The heliotail extends with decreasing values of fHP.
Paper: Exploring the Complex Heliotail Boundary by an Extended Level Set Approach
Authors: C. Onubogu, M. Opher, M. Kornbleuth, G. Tóth, V. Florinski
Figure caption: The HP defined by the level set isosurface, fHP = 0.99. (a) This isosurface results in a short and separated heliotail. (b) A cut through the heliotail at X = 490 au shows that the lobe structures remain intact but are no longer connected as in the fHP = 0 case. (c, d) Side views of the fHP = 0.99 isosurface with the interstellar field lines show good agreement of the field-line arrangement with the HP.
Paper: Exploring the Complex Heliotail Boundary by an Extended Level Set Approach
Authors: C. Onubogu, M. Opher, M. Kornbleuth, G. Tóth, V. Florinski
Figure caption: (a) Contours of the mass flux in a cut through the heliotail at X = 400 au. The two peaks in mass flux inside the heliosphere show where the heliosheath plasma is collimated. Projections of the MFP in white and the BV plane in black are overlaid on the cut to show how the MFP is more suitable to display the heliosheath plasma solution. (b) Nose and (c) tail views of the MFP, which optimally cut through the heliosphere.
Paper: SIRIUS: Identifying Metal-poor Stars Enriched by a Single Supernova in a Dwarf Galaxy Cosmological Zoom-in Simulation Resolving Individual Massive Stars
Authors: Yutaka Hirai, Takayuki R. Saitoh, Michiko S. Fujii, Katsuhiro Kaneko, Timothy C. Beers
Figure caption: [C/Fe], as a function of [Fe/H], at z = 6.5. The color bar to the right encodes the mass fraction of stars contained in each metallicity bin, with a size of 0.02  ×  0.004 dex2. Orange dots show the mono-enriched stars.
Paper: SIRIUS: Identifying Metal-poor Stars Enriched by a Single Supernova in a Dwarf Galaxy Cosmological Zoom-in Simulation Resolving Individual Massive Stars
Authors: Yutaka Hirai, Takayuki R. Saitoh, Michiko S. Fujii, Katsuhiro Kaneko, Timothy C. Beers
Figure caption: The number fraction of mono-enriched stars, as a function of [Fe/H].
Paper: Exploring the Complex Heliotail Boundary by an Extended Level Set Approach
Authors: C. Onubogu, M. Opher, M. Kornbleuth, G. Tóth, V. Florinski
Figure caption: Diagram illustrating the regions tracked by the level set function. Inflowing ISM material from the outer boundary (blue arrows) is assigned a value of fHP = −1. Outflowing solar wind material from the inner boundary (red arrows) around the Sun is assigned a value of fHP = 1. The zero level set, fHP = 0, is used as the standard surface to capture the locations where solar wind and ISM meet, denoted by where the magenta and cyan contours meet, respectively (S. N. Borovikov et al. 2011; V. Florinski et al. 2013; E. Provornikova et al. 2014; N. V. Pogorelov et al. 2015; F. Fraternale et al. 2023).
Paper: SIRIUS: Identifying Metal-poor Stars Enriched by a Single Supernova in a Dwarf Galaxy Cosmological Zoom-in Simulation Resolving Individual Massive Stars
Authors: Yutaka Hirai, Takayuki R. Saitoh, Michiko S. Fujii, Katsuhiro Kaneko, Timothy C. Beers
Figure caption: The density profiles of multienriched (blue dashed line) and mono-enriched (orange solid line) stars at z = 6.5. The density profile of multienriched stars is multiplied by 0.017 to be scaled to that of mono-enriched stars.
Paper: SIRIUS: Identifying Metal-poor Stars Enriched by a Single Supernova in a Dwarf Galaxy Cosmological Zoom-in Simulation Resolving Individual Massive Stars
Authors: Yutaka Hirai, Takayuki R. Saitoh, Michiko S. Fujii, Katsuhiro Kaneko, Timothy C. Beers
Figure caption: The formation times of multienriched (blue dashed line) and mono-enriched (orange solid line) stars.
Paper: SIRIUS: Identifying Metal-poor Stars Enriched by a Single Supernova in a Dwarf Galaxy Cosmological Zoom-in Simulation Resolving Individual Massive Stars
Authors: Yutaka Hirai, Takayuki R. Saitoh, Michiko S. Fujii, Katsuhiro Kaneko, Timothy C. Beers
Figure caption: The metallicity distribution functions of multienriched (blue dashed line) and mono-enriched (orange solid line) stars at z = 6.5.
Paper: Looking at Infrared Background Radiation Anisotropies with Spitzer: Large-scale Anisotropies and Their Implications
Authors: A. Kashlinsky, Richard G. Arendt, M. L. N. Ashby, J. Kruk, N. Odegard
Figure caption: Open circles with error bars show the diffuse light fluctuations in the final maps. Black circles show the signal at the final model subtraction adopted here, and the green circles show results without model subtraction when the subtraction was performed (NEP Ch1, CDFS Ch2); the subtraction was performed to achieve close levels of the effective shot noise between the two fields. The differences are negligibly small above arcminute scales, which are the subject of the study here. Red error bars show the noise power estimates from the (A − B)/2 maps. The vertical blue dashes show the estimated range of the zodi contributions to the white noise per R. G. Arendt et al. (2016); the contribution is small at angular scales outside the beam.
Paper: Looking at Infrared Background Radiation Anisotropies with Spitzer: Large-scale Anisotropies and Their Implications
Authors: A. Kashlinsky, Richard G. Arendt, M. L. N. Ashby, J. Kruk, N. Odegard
Figure caption: NEP (left) and CDFS (right) fields after masking and source subtraction as described. The 3.6 μm images (top row) are scaled [−4.2, 2.5] nW m−2 sr−1. The 4.5 μm images (bottom row) are scaled [−3.3, 2.0] nW m−2 sr−1. For display purposes these images have been resampled to ﹩4\mathop{.}\limits^{^{\prime\prime} }8﹩ pixel sizes. The truncation of an extended bright region by the top edge of the CDFS 4.5 μm image causes the unusually high power at ∼2000″ in Figures 1 and 2. Bottom left: exposure times for the selected for CIB analysis regions. Red/blue are 3.6/4.5 μm; solid/dotted are CDFS/NEP fields. Bottom middle: flux histograms at 3.6 (left) and 4.5 (right) μm; solid/dotted are CDFS/NEP fields. Bottom right: The number of independent Fourier elements, Nq, to compute power at each q with the division of the Fourier space here per A. Kashlinsky et al. (2012). Open triangles/filled circles correspond to NEP/CDFS fields.
Paper: Looking at Infrared Background Radiation Anisotropies with Spitzer: Large-scale Anisotropies and Their Implications
Authors: A. Kashlinsky, Richard G. Arendt, M. L. N. Ashby, J. Kruk, N. Odegard
Figure caption: Source-subtracted CIB fluctuations after the noise is subtracted with errors propagated. The dotted line is the shot noise fitted to small-scale data; ﹩{P}_{{\rm{SN}}}﹩ is marked in nJy · nW m−2 sr−1. Green lines are the K. Helgason et al. (2012) reconstruction with shot noise, as fitted plus 1H and 2H terms, all convolved with the beam; solid is the default reconstruction, and dotted lines are the allowed span.
Paper: Looking at Infrared Background Radiation Anisotropies with Spitzer: Large-scale Anisotropies and Their Implications
Authors: A. Kashlinsky, Richard G. Arendt, M. L. N. Ashby, J. Kruk, N. Odegard
Figure caption: Source-subtracted CIB anisotropies from the analysis here (blue and red) from Figure 9 of A. Kashlinsky et al. (2012; black) and from Figure 1 of A. Kashlinsky et al. (2007a; green and brown). The powers here and at A. Kashlinsky et al. (2012) are evaluated at the same q grid, but black symbols are slightly shifted for clarity. The brown/green data for the q-grid from A. Kashlinsky et al. (2007a, 2007c) were slightly shifted for clearer display, with the leftmost green corresponding to the original q. The lines correspond to single-z templates of the CIB at z = 10, 15, 20, 25, 30.
Paper: Looking at Infrared Background Radiation Anisotropies with Spitzer: Large-scale Anisotropies and Their Implications
Authors: A. Kashlinsky, Richard G. Arendt, M. L. N. Ashby, J. Kruk, N. Odegard
Figure caption: (a) ﹩{P}_{{\rm{SN}}}﹩ from known galaxies with AB magnitude >m0 from JWST counts (solid lines; R. A. Windhorst et al. 2023) and Spitzer (dashed lines; M. L. N. Ashby et al. 2013, 2015). The shot-noise levels remaining in the fields are shown with horizontal lines: blue, red at 3.6, 4.5 μm. The adopted magnitude of source clipping is shown with vertical lines, mAB = 24.8, 24.5 at 3.6, 4.5 μm, which are slightly shifted for clearer display. Vertical and horizontal lines correspond to NEP (dotted) and CDFS (solid). (b) Flux remaining from known galaxies of m > m0 vs. the shot-noise contributed by them. Vertical blue/red lines show ﹩{P}_{{\rm{SN}}}﹩ at 3.6/4.5 μm from Table 1 of A. Kashlinsky et al. (2007a), marking also the F(>m0) due to these galaxies.
Paper: Looking at Infrared Background Radiation Anisotropies with Spitzer: Large-scale Anisotropies and Their Implications
Authors: A. Kashlinsky, Richard G. Arendt, M. L. N. Ashby, J. Kruk, N. Odegard
Figure caption: The dimensionless cross power between the IRAS 100 μm cirrus data and the Spitzer IR maps for each of the two fields under study. Filled and open circles represent use of either the ISSA or IRIS reductions of the IRAS survey. Solid and dashed lines indicate the ranges of ﹩1/{N}_{q}^{0.5}﹩ and ﹩2/{N}_{q}^{0.5}﹩ that would be expected from uncorrelated data to reflect 1σ and 2σ at small ﹩{ \mathcal R }﹩. (Note that this does not strictly reflect the appropriate confidence levels and as ﹩{ \mathcal R }﹩ approaches unity the latter must be evaluated from the Fisher transformation as discussed in A. Kashlinsky et al. 2018). The amplitude of the cross power demonstrates the negligible contribution of cirrus to the power displayed in Figure 2.
Paper: Looking at Infrared Background Radiation Anisotropies with Spitzer: Large-scale Anisotropies and Their Implications
Authors: A. Kashlinsky, Richard G. Arendt, M. L. N. Ashby, J. Kruk, N. Odegard
Figure caption: Noise properties for the A–B maps: the top shows the scatter plot between the two wavelengths illustrating a completely random, uncorrelated components between the two wavelengths for each of the fields. The bottom shows the cross powers between the two wavelengths in each of the fields, demonstrating randomness between the two wavelengths.