adsabs/AstroCLIMB huggingface dataset:
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Same as Figure 7 but for the 1.0 < z < 1.2 intermediate-redshift samples. For comparison, the median results from the low-redshift samples (Figure 7) are shown as blue dashed lines.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: The star formation main sequence with different parameter estimates. Solid lines and shaded regions show the median and 1σ bounds of each relation binned by redshift, respectively. Left: COSMOS2020 estimates of star formation rate and stellar mass are positively correlated. Middle: this relation becomes shallower when DESI stellar mass estimates are instead used. Right: further using DESI [O II] luminosity as a proxy for star formation rate yields a flat ﹩{\mathrm{log}}\,{L}_{[{\rm{OII}}]}-\,{\mathrm{log}}\,{M}_{* }﹩ distribution.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Same as Figure 8 but for the 1.2 < z < 1.6 high-redshift samples.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Constraints on all model parameters, for the low-redshift (0.8 < z < 1.0) fitting. In each corner plot, shaded boxes show the binned density of the model posterior. Solid contours enclose the central 68% and 95% of the 2D distributions. In each histogram, dashed vertical lines mark the median and central 68% interval.
Paper: Exploration of the Outer Envelope of the K-giant Star Beta Cet 
Authors: Krister E. Nielsen, Gioia Rau, Kenneth G. Carpenter
Figure caption: Chromospheric wind lines (left) observed in the ultraviolet spectrum of β Cet compared with the transition region Si IV and C IV doublets (right). The wind lines are narrower and broadened by thermal motion, while the transition region lines have a significant nonthermal contribution. The strong depression in Si IIλ1527 is predominantly interstellar absorption (S. Redfield & J. L. Linsky 2004), but the non-Gaussian line profiles of O Iλλ1304, 1306, and the absorption in Si IIλ1533 indicate additional absorption in the stellar wind.
Paper: Exploration of the Outer Envelope of the K-giant Star Beta Cet 
Authors: Krister E. Nielsen, Gioia Rau, Kenneth G. Carpenter
Figure caption: The position of β Cet and other giant/supergiants in the H-R diagram. The Linsky–Haisch line (dotted) separates the cool noncoronal objects with spectra dominated by their wind and fluorescent circumstellar lines in the upper right corner from objects with high ionization transition region lines and X-ray signatures. The hybrid stars exhibit spectral characteristics observed in both the coronal and noncoronal objects.
Paper: Exploration of the Outer Envelope of the K-giant Star Beta Cet 
Authors: Krister E. Nielsen, Gioia Rau, Kenneth G. Carpenter
Figure caption: SEI fits of the O Iλ1304 (top) and O Iλ1302 (bottom). The solid lines are modeled with v∞ = 68 km s−1, vt = 7 km s−1 and a wind acceleration β = 0.3. The dashed lines represent a variation of ±8 km s−1 in v∞. The strong interstellar absorption in the O Iλ1302 resonance line complicates the modeling of this line.
Paper: Exploration of the Outer Envelope of the K-giant Star Beta Cet 
Authors: Krister E. Nielsen, Gioia Rau, Kenneth G. Carpenter
Figure caption: Evolution of the spectrum from noncoronal to hybrid and coronal stars. The ultraviolet spectral region is dominated by narrow singly ionized atomic and molecular emission in the noncoronal γ Cru (bottom) compared with a transition region spectrum with broad emission from Si IV and O IV for the hybrid and coronal stars (top). All spectra are obtained with HST/STIS.
Paper: Exploration of the Outer Envelope of the K-giant Star Beta Cet 
Authors: Krister E. Nielsen, Gioia Rau, Kenneth G. Carpenter
Figure caption: Nonthermal broadening (ξ, ◇) and sound speed (vs, ▵) as a function of formation temperature. The dashed lines are polynomial fits for the two data sets and are included as guides for the trends of the broadening. The core components of the double Gaussian fits are included in the fit, while the tail components (∘) are excluded.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Same as Figure 16 but for the 1.2 < z < 1.6 high-redshift fitting.
Paper: DESI Emission-line Galaxies: Clustering Dependence on Stellar Mass and [O II] Luminosity
Authors: T. Hagen, K. S. Dawson, Z. Zheng, J. Aguilar, S. Ahlen, S. BenZvi, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, P. Doel, S. Ferraro, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, V. Gonzalez-Perez, G. Gutierrez, C. Hahn, K. Honscheid, M. Ishak, S. Juneau, R. Kehoe, T. Kisner, A. Kremin, C. Lamman, M. Landriau, L. Le Guillou, A. Leauthaud, M. E. Levi, M. Manera, A. Meisner, R. Miquel, J. Moustakas, S. Nadathur, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, A. J. Ross, G. Rossi, S. Saito, E. Sanchez, D. Schlegel, M. Schubnell, J. Silber, D. Sprayberry, G. Tarlé, B. A. Weaver, R. Zhou, H. Zou
Figure caption: Same as Figure 16 but for the 1.0 < z < 1.2 intermediate-redshift fitting.
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: Top panels: GALFA-H I narrow-channel emission maps centered on the radio source 3C 409 and on the radial velocities of absorption components with existing Zeeman measurements. Each map has a dimension of 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 × 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 and a channel width of 1.7 km s−1. Bottom panel: Gaussian components detected in absorption toward 3C 409 according to the HT03 fit. The upper plot shows the expected H I emission TB,CNM due to each color-coded CNM component. The shaded regions represent the velocity ranges of the GALFA-H I emission maps shown in the top panels. Emission from WNM is not shown (see Section 5.1).
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: Twenty-eight Millennium lines of sight with Zeeman measurements plotted over a velocity-integrated map of CO emission intensity from T. M. Dame & P. Thaddeus (2022) centered at (l, b) = (120°, 0°). Circles indicate CO emission-line detections (yellow) and nondetections (pink), while dark-blue stars and squares mark detections and nondetections, respectively, of OH absorption lines at any velocity along the line of sight, as reported by D. Li et al. (2018a). Crosses represent lines of sight without OH emission spectra, while dark-blue empty circles represent the lack of CO absorption spectra in D. Li et al. (2018a).
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: Sixty-six Zeeman measurements from the Millennium Survey plotted over the GALFA-H I column density map obtained for velocity range ∣v∣ ≤ 90 km s−1. Locations of the background radio sources are marked with stars, white for Arecibo measurements and green for targets where new data was collected with FAST. Zeeman measurements represented by squares are color-coded by BLOS inferred by HT04 and stacked in increasing radial velocity order above each radio source. Positive values of BLOS correspond to the magnetic field pointing away from the observer. Hollow squares indicate low signal-to-noise ratio (S/N) measurements (S/N < 2). Densely dotted and sparsely dotted lines mark Galactic latitudes ∣b∣ = 10° and ∣b∣ = 30°, respectively.
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: On–Off Stokes V =  IEEE RCP - IEEE LCP spectra from FAST toward sources 3C 409, 3C 98, and 3C 207 with the Zeeman splitting fit in purple. For comparison, the Zeeman splitting fit to Millennium Survey data from the Arecibo Observatory obtained by HT04 is plotted in orange. For visual clarity, the leakage of Stokes I into Stokes V has been subtracted, and the spectra are binned by four spectral channels using the unweighted mean (each original FAST channel has a 0.1 km s−1 width, and all fits to the data are performed at the original resolution).
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: Top row panels: examples of two 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 × 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 GALFA-H I emission maps with 1.7 kms−1 channel width, representative of high (Var(θHI) = 0.82, left) and low (Var(θHI) = 0.15, right) variance of θHI angles constructed using the rolling Hough transform. Middle row panels: corresponding RHT intensity maps R(x, y) quantifying the degree of linearity in every pixel of the map. Bottom row panels: deviation of the RHT angle θHI from the mean orientation angle in the image ΔθHI = θHI − 〈θHI〉.
Paper: Exploration of the Outer Envelope of the K-giant Star Beta Cet 
Authors: Krister E. Nielsen, Gioia Rau, Kenneth G. Carpenter
Figure caption: Surface fluxes for the transition region lines observed in β Cet are compared with corresponding lines in the K5 III star γ Dra. Diamonds represent the individual line measurements, while the filled diamonds represent the average values for each formation temperature, ﹩{\mathrm{log}}\,T﹩.
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: Difference between BLOS from FAST and Millennium Survey for absorption components with Millennium uncertainties <10 μG. The error bars represent 1σ uncertainties computed as ﹩{(\sigma {({B}_{\,{\rm{LOS,FAST}}\,})}^{2}+\sigma {({B}_{\,{\rm{LOS,Arecibo}}\,})}^{2})}^{1/2}﹩. The Zeeman measurements from FAST and Arecibo agree within 2σ in all absorption components.
Paper: Exploration of the Outer Envelope of the K-giant Star Beta Cet 
Authors: Krister E. Nielsen, Gioia Rau, Kenneth G. Carpenter
Figure caption: Double Gaussian fits of the N Vλλ1239,1243 that are formed at ﹩{\mathrm{log}}\,T﹩ = 5.30 K. The two lines are simultaneously fit with the average FWHM for the two lines.
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: Inverse-variance-weighted mean ∣BLOS∣ along the line of sight plotted against integrated density tracers: dust visual extinction AV (left) and the total H I column density (right). In the top row panels, points are color-coded by the integrated column density of CO; the bottom row panels show the same but for OH, derived based on the 1667 Hz line. For each molecular tracer, teal squares mark nondetections while gray diamonds mark targets with no molecular line spectrum in D. Li et al. (2018a).
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: Zeeman measurements plotted against the circular variance of H I filament orientations Var(θRHT) computed in a dPOS < 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 region around each radio source. Top panel: we plot the mean and 1σ errors of a normal distribution centered at ∣BLOS∣ with uncertainties of the directional BLOS. Gray points represent measurements we classified as blended in Section 5.1. Bottom panel: orange points represent the mode of a folded-normal distribution of ∣BLOS∣. The error bars represent the 16th and 84th percentiles of the folded-normal PDF.
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: Spearman correlation between ∣BLOS∣ and Var(θHI) as a function of the plane-of-sky diameter dPOS of the region where Var(θHI) is computed and as a function of RHT parameters: the window length DW and the smoothing radius θFWHM, at a fixed RHT threshold ZRHT = 0.75. We find that the result is not strongly sensitive to the choice of RHT parameters. The correlation is not present at scales smaller than the RHT window length, but persists to large angular scales.
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: Zeeman measurements toward background sources with the smallest angular separations in the survey. Each panel shows Zeeman measurements toward two sight lines, and panels are ordered by the angular separation of the background sources. We find a general agreement, both in strength and direction, between BLOS at similar velocities. The first >3σ disagreement between cospectral (∣vi − vj∣ < 3 km s−1) components is observed toward targets separated by 7﹩\mathop{.}\limits^{\unicode{x000b0}}﹩9 (3C 133 and 3C 144 (Tau A)). Each plot spans 20 km s−1, but the central velocity varies.
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: For each component pair i, j in the Millennium sample, we plot the statistical significance of the Zeeman measurement difference, ∣BLOS,i − BLOS,j∣/σi,j, as a function of their radial velocity separation. We show pairs that lie along the same line of sight in blue squares, different lines of sight with a large angular separation (>7﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5) in gray stars, or different lines of sight with a small (≤7﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5) angular separation in orange circles.
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: Dust extinction per parsec toward Millennium Zeeman targets extracted from G. Edenhofer et al. (2024) 3D dust maps. The dust profiles have been averaged over the 12 posterior samples. In dotted orange, we marked the boundaries of the Local Bubble from the model of T. J. O’Neill et al. (2024). The sight lines are sorted in the increasing order of 〈∣BLOS∣〉, the inverse-variance-weighted mean of ∣BLOS∣.
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: The number of dust peaks in G. Edenhofer et al. (2024) extinction profiles against the number of Gaussian components in the H I optical depth spectrum. The purple histogram includes all 80 Millennium sight lines, while the 28 Millennium sight lines with Zeeman measurements are plotted in orange circles scaled by the sight line count, which ranges from 1–6.
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: Zeeman field strength measured in H I absorption as a function of velocity offset between H I absorption component and the nearest OH 1667 Hz absorption component, for sight lines where OH is detected.
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: Spatially averaged RHT output R(θ) centered around the mean orientation and stacked in quartiles of Zeeman field strength. H I emission maps corresponding to lower Zeeman field strengths show more sharply peaked distributions of filament orientations (dark blue), and vice versa.
Paper: Magnetic Fields in the Eos Cloud: Dynamically Important Fields in the Interface between Atomic and Molecular Gas
Authors: Janik Karoly, Kate Pattle, Blakesley Burkhart, Thavisha E. Dharmawardena, B-G Andersson, Thomas J. Haworth
Figure caption: Upper left: Optical polarization angle vs. submillimeter Planck magnetic field angle (polarization angle rotated by 90°). A one-to-one dashed line is plotted. Most of the position angles agree well. Upper center: Polarization efficiency (p/A0) vs. A0 for the optical polarization vectors. A power-law fit gives an index of −0.61, indicating good grain alignment (B-G Andersson et al. 2015). Upper right: Nondebiased polarization percentage (see Equation (2)) vs. Stokes I. A power-law fit gives an index of −0.51, again indicating good grain alignment. Lower left: A plot of the polarization structure function ﹩{ \mathcal S }﹩ evaluated with a lag of 5﹩^{\prime} \rm{}\,\rm{}\,﹩ vs. nondebiased polarization fraction (pfrac). A simple linear fit of log(S) vs. log(pfrac) (see Planck Collaboration et al. 2015a, 2015b; V. J. M. Le Gouellec et al. 2020) is shown as a black dashed line. More details are given in the text. Lower right: A plot of S × pfrac vs. normalized intensity which is used as a proxy for column density. A slight decreasing trend can be seen. The mean S × pfrac value is plotted as a gray dashed line with a shaded area representing the 25% and 75% quartiles.
Paper: Joint Analysis of H I Absorption Zeeman Measurements and the Morphology of Filamentary H I Emission
Authors: Marta Nowotka, Susan E. Clark, Blakesley Burkhart, Laura Fissel, Tao-Chung Ching, Timothy Robishaw, Carl Heiles
Figure caption: As in Figure 7, we plot Zeeman measurements ∣BLOS∣ against the circular variance of H I filament orientations Var(θRHT) computed in a dPOS = 2﹩\mathop{.}\limits^{\unicode{x000b0}}﹩5 region around each radio source. We use colors and symbols to split the sample by AV and Galactic latitude b, and observe that either split results in subsamples that largely occupy different regions of the plot. This suggests that systematic variations in magnetic field inclination or total field strength with Av or b could drive the correlation between ∣BLOS∣ and Var(θRHT).
Paper: Magnetic Fields in the Eos Cloud: Dynamically Important Fields in the Interface between Atomic and Molecular Gas
Authors: Janik Karoly, Kate Pattle, Blakesley Burkhart, Thavisha E. Dharmawardena, B-G Andersson, Thomas J. Haworth
Figure caption: Magnetic fields in the Eos cloud. This image shows Stokes I dust emission observed by Planck at 353 GHz, with overlaid texture showing a line integral convolution (B. Cabral & L. C. Leedom 2023) visualization of the magnetic field observed by Planck. Optical vectors are overlaid as white lines. The gray contour marks the bounds of the Eos cloud as defined using FUV H2 observations (B. Burkhart et al. 2025). The white contours are Planck CO (1–0) observations which show the location of MBM 40 and the star shows the central coordinates of MBM 40 from T. M. Dame & P. Thaddeus (2022).
Paper: Magnetic Fields in the Eos Cloud: Dynamically Important Fields in the Interface between Atomic and Molecular Gas
Authors: Janik Karoly, Kate Pattle, Blakesley Burkhart, Thavisha E. Dharmawardena, B-G Andersson, Thomas J. Haworth
Figure caption: The Eos cloud. Left: FIMS/SPEAR FUV H2 fluorescence emission map, in log line units (LU: photons cm−2 sr−1 s−1), first presented by Y.-S. Jo et al. (2017). Right: Map of the ratio of H2 intensity to total FUV intensity, in percentage points (%). The location of the Eos cloud is outlined and appears as a bright fluorescent feature. The on-sky boundary for the Eos cloud is based on the magenta contours, which outline the 10% ratio of H2 intensity.