adsabs/AstroCLIMB huggingface dataset:
Paper: Tidal Disruption Event Demographics in Supermassive Black Hole Binaries over Cosmic Times
Authors: Denyz Melchor, Smadar Naoz, Suvi Gezari, Brenna Mockler
Figure caption: Correlation between TDE light curves and black hole mass. Adapted from Y. Yao et al. (2023), this figure depicts the relationship between black hole masses (estimated from host galaxy properties; x-axis) and t1/2, the duration a TDE remains above half its peak luminosity (rise plus decline; y-axis). Green markers denote TDEs in green-valley galaxies, while the pink markers fall outside that category. The orange curve is a best-fit relation with fixed slope ﹩{t}_{1/2}\propto {{\rm{M}}}_{BH}^{1/2}﹩, and the yellow shaded band shows a 1σ scatter. Circle markers use black hole mass estimates from MBH–Mgal; inverted triangles use estimates from the MBH–σ⋆ relation. The shaded area below the lower 1σ bound highlights candidate TDEs that may originate from SMBH-binary systems.
Paper: Tidal Disruption Event Demographics in Supermassive Black Hole Binaries over Cosmic Times
Authors: Denyz Melchor, Smadar Naoz, Suvi Gezari, Brenna Mockler
Figure caption: Number of TDEs from an SMBH binary: uncertainty at z = 1. The x-axis shows η, which represents the confidence in the binary mechanism (EKL + two-body relaxation) producing TDEs, and the y-axis gives the predicted TDE count per redshift at z = 1. The vertical dashed gray line at η = 1 indicates full confidence in binary-driven origins of TDEs. The intersection of the pink curve and the light blue line represents the predicted TDE count under this assumption. As η→0, the pink curve approaches the single-SMBH TDE rate. The light blue provides a linear extrapolation of uncertainty anchored at η = 1. Vertical purple lines mark the observed fraction of PSB galaxies at z ≲ 1 and z ∼ 2; their intersections with the model lines correspond to the expected TDE contribution from binaries in PSB hosts at those redshifts.
Paper: The Perfect Host: JWST Cepheid Observations in a Background-free Type Ia Supernova Host Confirm No Bias in Hubble-constant Measurements
Authors: Adam G. Riess, Siyang Li, Gagandeep S. Anand, Wenlong Yuan, Louise Breuval, Stefano Casertano, Lucas M. Macri, Dan Scolnic, Yukei S. Murakami, Alexei V. Filippenko, Thomas G. Brink
Figure caption: Left: Red, green, blue color image of the NGC 3447 field, generated from HST WFC3/UVIS imaging (F814W + F814W/F555W + F555W). The tidal companion (NGC 3447A; left) and the main body (NGC 3447; right) regions used in this Letter are delineated using dashed ellipses (the region to the lower left of the yellow dashed line in the dwarf region was further excluded to remove a separate dwarf in projection). Right: zoomed-in views that show color JWST/NIRCam (F277W/F150W/F090W) imaging from a region within the dwarf (top) and the main body (bottom). These two cutouts are shown with identical stretch and contrast (drawn from the same parent image) to highlight the lack of crowded stellar background in the dwarf region. Cepheids are identified using yellow circles.
Paper: The Perfect Host: JWST Cepheid Observations in a Background-free Type Ia Supernova Host Confirm No Bias in Hubble-constant Measurements
Authors: Adam G. Riess, Siyang Li, Gagandeep S. Anand, Wenlong Yuan, Louise Breuval, Stefano Casertano, Lucas M. Macri, Dan Scolnic, Yukei S. Murakami, Alexei V. Filippenko, Thomas G. Brink
Figure caption: Top left: CMD of the main spiral body (NGC 3447). Overlaid are example stellar sequences drawn using the ArtPop software package (J. P. Greco & S. Danieli 2022). The main spiral body shows clear signs of a broad age of stellar populations, from young main-sequence stars to old red giants. Top right: CMD of the selected tidal dwarf region. Unlike the main body, the stellar population here is dominated by young main-sequence and intermediate-age blue and red helium-burning stars (∼100 Myr). The few red giants are likely interlopers from the halo of the main spiral and the separate dwarf found in projection to the system. Bottom panels: example color-image cutouts drawn from the main body and the tidal dwarf, showing the clear visible differences in stellar populations—the tidal dwarf region lacks the background, old stellar population that can be seen in the disk of the main galaxy.
Paper: The Perfect Host: JWST Cepheid Observations in a Background-free Type Ia Supernova Host Confirm No Bias in Hubble-constant Measurements
Authors: Adam G. Riess, Siyang Li, Gagandeep S. Anand, Wenlong Yuan, Louise Breuval, Stefano Casertano, Lucas M. Macri, Dan Scolnic, Yukei S. Murakami, Alexei V. Filippenko, Thomas G. Brink
Figure caption: Metallicity map and Hα image (from P. Mazzei et al. 2018). The metallicity measures were obtained using the method described by R22 (see also S. L. Hoffmann et al. 2016) from strong nebular lines in H II regions at the locations indicated using Keck/LRIS.
Paper: The Perfect Host: JWST Cepheid Observations in a Background-free Type Ia Supernova Host Confirm No Bias in Hubble-constant Measurements
Authors: Adam G. Riess, Siyang Li, Gagandeep S. Anand, Wenlong Yuan, Louise Breuval, Stefano Casertano, Lucas M. Macri, Dan Scolnic, Yukei S. Murakami, Alexei V. Filippenko, Thomas G. Brink
Figure caption: Comparison of the mean JWST background due to crowding (as measured from artificial stars) and the crowding noise (measured from the dispersion of artificial stars). The two quantities are closely related as they are both measures of the stellar background. Several regions in NGC 3447 are shown including the tidal host (“perfect host”), which is very similar to the “blank sky” measured from the opposite (host-free) NIRCam module. The inset plots the crowding level vs. the residual of each hosted SN from the distance-ladder fit of R22. We find no correlation between these quantities and thus no evidence for an uncorrected bias in HST photometry with crowding.
Paper: The Perfect Host: JWST Cepheid Observations in a Background-free Type Ia Supernova Host Confirm No Bias in Hubble-constant Measurements
Authors: Adam G. Riess, Siyang Li, Gagandeep S. Anand, Wenlong Yuan, Louise Breuval, Stefano Casertano, Lucas M. Macri, Dan Scolnic, Yukei S. Murakami, Alexei V. Filippenko, Thomas G. Brink
Figure caption: Comparison of distances to 19 hosts of 24 SNe Ia measured with HST and JWST anchored by the same geometric distance reference, NGC 4258. The lower plot shows the differences in the measurements from the two telescopes. Red illustrates the comparison for the baseline system used to measure H0, WHV,I where H = F150W from JWST NIRCam. Light gray shows WJV,I where J = F115W. Green gives the two components of NGC 3447 measured in WH. The bottom plot shows a constant value of ﹩5\,\mathrm{log}(73/67.5)=0.17﹩ mag labeled “Hubble tension” that would resolve the tension (but is strongly ruled out).
Paper: The Perfect Host: JWST Cepheid Observations in a Background-free Type Ia Supernova Host Confirm No Bias in Hubble-constant Measurements
Authors: Adam G. Riess, Siyang Li, Gagandeep S. Anand, Wenlong Yuan, Louise Breuval, Stefano Casertano, Lucas M. Macri, Dan Scolnic, Yukei S. Murakami, Alexei V. Filippenko, Thomas G. Brink
Figure caption: Color-coded identity of stars in the NIRCam field of NGC 3447. Regions follow the definitions in Section 2.1. As shown, the Cepheids in tidal host NGC 3447A (upper right) are free of contamination from common RGB stars with F090W0 > 27.55 mag and 0.7 <  (F090W − F150W)0 < 2.0 mag.
Paper: The Perfect Host: JWST Cepheid Observations in a Background-free Type Ia Supernova Host Confirm No Bias in Hubble-constant Measurements
Authors: Adam G. Riess, Siyang Li, Gagandeep S. Anand, Wenlong Yuan, Louise Breuval, Stefano Casertano, Lucas M. Macri, Dan Scolnic, Yukei S. Murakami, Alexei V. Filippenko, Thomas G. Brink
Figure caption: A larger sample of Cepheids in NGC 3447A, the tidal companion, illustrating the absence of a contaminating background. The general appearance is similar to that of an MW open cluster. As discussed in Section 3.2, the rare superposition of a blue star with a Cepheid would suppress the latter’s amplitude more strongly in the optical (where their light curves are measured) than in the infrared and eliminate such an object from the amplitude selection.
Paper: The Perfect Host: JWST Cepheid Observations in a Background-free Type Ia Supernova Host Confirm No Bias in Hubble-constant Measurements
Authors: Adam G. Riess, Siyang Li, Gagandeep S. Anand, Wenlong Yuan, Louise Breuval, Stefano Casertano, Lucas M. Macri, Dan Scolnic, Yukei S. Murakami, Alexei V. Filippenko, Thomas G. Brink
Figure caption: Reddening-free (Wesenheit) P–L relations for three levels of crowding in NGC 3447. The points in light gray are from HST measurements in F160W as given by R22. In blue are Cepheids observed with JWST F150W in the spiral host, and in red are those observed in the tidal host, NGC 3447A. All three samples yield consistent distance measures but with decreasing levels of P–L noise.
Paper: The Perfect Host: JWST Cepheid Observations in a Background-free Type Ia Supernova Host Confirm No Bias in Hubble-constant Measurements
Authors: Adam G. Riess, Siyang Li, Gagandeep S. Anand, Wenlong Yuan, Louise Breuval, Stefano Casertano, Lucas M. Macri, Dan Scolnic, Yukei S. Murakami, Alexei V. Filippenko, Thomas G. Brink
Figure caption: NIR postage stamps of Cepheids in NGC 3447 that illustrate the three levels of crowding in this study. The left panel shows a Cepheid observed with HST in the spiral component of NGC 3447. In the middle panel, we see the same Cepheid observed with JWST NIRCAM at the same wavelength. In the right-hand panel is a Cepheid of similar period in the tidal host, NGC 3447A, illustrating the lack of a stellar background.
Paper: The Perfect Host: JWST Cepheid Observations in a Background-free Type Ia Supernova Host Confirm No Bias in Hubble-constant Measurements
Authors: Adam G. Riess, Siyang Li, Gagandeep S. Anand, Wenlong Yuan, Louise Breuval, Stefano Casertano, Lucas M. Macri, Dan Scolnic, Yukei S. Murakami, Alexei V. Filippenko, Thomas G. Brink
Figure caption: Wesenheit relations for F150W for Figure 9. Additional hosts and color combination relations may be found in A. G. Riess et al. (2024a). F150W data are from GO programs 1685 and 2875 (PI: A. Riess), with the exception of NGC 4038 and M101, and all F555W − F814 colors are from the HST SH0ES project. All data are phase-corrected using an additional JWST short-wavelength color as described in Section 3.2.1.
Paper: The Perfect Host: JWST Cepheid Observations in a Background-free Type Ia Supernova Host Confirm No Bias in Hubble-constant Measurements
Authors: Adam G. Riess, Siyang Li, Gagandeep S. Anand, Wenlong Yuan, Louise Breuval, Stefano Casertano, Lucas M. Macri, Dan Scolnic, Yukei S. Murakami, Alexei V. Filippenko, Thomas G. Brink
Figure caption: Wesenheit relations for F115W for Figure 9. F115W data are from GO program 1995 (PI: W. Freedman), with the exception of “NGC 4258cyc2” (GO-2875, PI: A. Riess) and M101f2 (PI: Huang), and all F555W − F814 colors are from the HST SH0ES project.
Paper: A Dense Molecular Ringlike Structure in Gaseous CO Depletion Region G34.74−0.12
Authors: Shuting Lin, Siyi Feng, Fengwei Xu, Ke Wang, Patricio Sanhueza, Junzhi Wang, Zhi-Yu Zhang, Yichen Zhang, Kaho Morii, Hauyu Baobab Liu, Sheng-Yuan Liu, Lile Wang, Giovanni Sabatini, Hui Li, Willem Baan, Zhi-Kai Zhu, Shanghuo Li
Figure caption: (a) Integrated intensity map of C18O (2–1) from ALMA 12m+7m+TP data with full UV coverage, integrated over the velocity range 79.9–81.9 km s−1, overlaid on large-scale two-color maps of G34.74−0.12. The red and cyan colors represent the integrated intensities of C18O (2–1) and DCO+ (1–0), respectively, over the velocity range of 72–85 km s−1, obtained from IRAM-30 m observations (S. Feng et al. 2020). White contours represent the dust continuum emission from the combined Planck and APEX 870 μm map of the ATLASGAL survey, shown at contour levels of 4σ, 5σ, 6σ, 7σ, and 8σ, where σ = 0.18 Jy beam−1. The orange contours represent the C18O (2–1) gas ringlike structure with levels starting from 10σ and increase in steps of 3σ (1σ = 0.02 Jy beam−1 km s−1). The relative coordinate center (0, 0) denotes the center of the ring. (b) The grayscale map and black contours represent the integrated intensity of the C18O (2–1) ring (integrated velocity range: 79.9–81.9 km s−1). The contour level are same as (a). The blue and red contours represent the blue- and redshifted components of outflows traced by CO (2–1), respectively (S. Lin et al. 2025). The yellow contours represent the integrated intensity of H2CO (30,3–20,2) within the same integrated velocity range of C18O (2–1), showing a similar ringlike morphology. The contour levels of H2CO start from 4σ and increase in steps of 4σ (1σ = 0.01 Jy beam−1 km s−1). The white contours represent the 1.3 mm dust continuum from ASHES observations. White crosses outlined in black mark the positions of cores 1, 2, 4, and 10, as labeled by K. Morii et al. (2023). (c) C18O (2–1) ring overlaid on the integrated intensity map of HNC (1–0). The black contours represents the C18O (2–1) gas ringlike structure, same as (a). The white contours represents the HNC (1–0) emission with levels starting from 3σ and increasing in steps of 2σ (1σ = 0.012 Jy beam−1 km s−1), integrated over the same integrated velocity range of C18O (2–1). The gray arrows indicate the paths along four different directions, corresponding to a P.A. of 0°, 45°, 90°, and 135°. (d) C18O (2–1) ring overlaid on the integrated intensity map of N2H+ (1–0), derived by stacking its hyperfine components. The black contours represent the C18O (2–1) gas ringlike structure, same as panel (a). The white contours represent the N2H+ (1–0) emission with levels starting from 3σ and increasing in steps of 2σ (1σ = 0.019 Jy beam−1 km s−1), integrated over the same integrated velocity range of C18O (2–1). A, B, and C mark the positions where HNC (1–0), N2H+ (1–0), and C18O (2–1) lines all show emissions S/N > 4. The synthesized beam for each line is shown in the bottom right corner of each panel.
Paper: A Dense Molecular Ringlike Structure in Gaseous CO Depletion Region G34.74−0.12
Authors: Shuting Lin, Siyi Feng, Fengwei Xu, Ke Wang, Patricio Sanhueza, Junzhi Wang, Zhi-Yu Zhang, Yichen Zhang, Kaho Morii, Hauyu Baobab Liu, Sheng-Yuan Liu, Lile Wang, Giovanni Sabatini, Hui Li, Willem Baan, Zhi-Kai Zhu, Shanghuo Li
Figure caption: PV diagrams of HNC (1–0) along four cuts with a P.A. of 0°, 45°, 90°, and 135° (labeled in Figure 1) of the ringlike structure. Contour levels are set at 3σ, 4σ and 5σ, where σ = 0.008 Jy beam−1. The vertical black dashed line marks the center of the ringlike structure, while the horizontal black dashed line indicates the systemic velocity. The gray curve in the PV diagram represents the best-fit result from the spherical expanding shell model.
Paper: A Dense Molecular Ringlike Structure in Gaseous CO Depletion Region G34.74−0.12
Authors: Shuting Lin, Siyi Feng, Fengwei Xu, Ke Wang, Patricio Sanhueza, Junzhi Wang, Zhi-Yu Zhang, Yichen Zhang, Kaho Morii, Hauyu Baobab Liu, Sheng-Yuan Liu, Lile Wang, Giovanni Sabatini, Hui Li, Willem Baan, Zhi-Kai Zhu, Shanghuo Li
Figure caption: Multiwavelength continuum images in the range of 3.6 μm–3 mm. Top row: Spitzer 3.6, 4.5, 5.8, and 8.0 μm images from GLIMPSE (E. Churchwell et al. 2009). Bottom row: Spitzer 24 μm image from MIPSGAL (S. J. Carey et al. 2009), Herschel 70 μm image, ALMA 1.3 mm image from ASHES (K. Morii et al. 2023), and ALMA 3 mm image (this work). White contours indicate the dust continuum from the combined Planck/High Frequency Instrument and APEX/LABOCA map of the ATLASGAL survey, shown at levels of 4σ, 5σ, 6σ, 7σ, and 8σ, where σ = 0.18 Jy beam−1. The angular resolution is shown at the bottom of each panel.
Paper: A Dense Molecular Ringlike Structure in Gaseous CO Depletion Region G34.74−0.12
Authors: Shuting Lin, Siyi Feng, Fengwei Xu, Ke Wang, Patricio Sanhueza, Junzhi Wang, Zhi-Yu Zhang, Yichen Zhang, Kaho Morii, Hauyu Baobab Liu, Sheng-Yuan Liu, Lile Wang, Giovanni Sabatini, Hui Li, Willem Baan, Zhi-Kai Zhu, Shanghuo Li
Figure caption: The line profiles of C18O (2–1), HNC (1–0), and N2H+ (1–0), extracted from synthesized beam-averaged regions centered on core10, positions A, B, and C (as shown in Figure 1). The vertical red dashed line indicates the systemic velocity, and the shaded region shows the integrated velocity range for the ring component.
Paper: A Dense Molecular Ringlike Structure in Gaseous CO Depletion Region G34.74−0.12
Authors: Shuting Lin, Siyi Feng, Fengwei Xu, Ke Wang, Patricio Sanhueza, Junzhi Wang, Zhi-Yu Zhang, Yichen Zhang, Kaho Morii, Hauyu Baobab Liu, Sheng-Yuan Liu, Lile Wang, Giovanni Sabatini, Hui Li, Willem Baan, Zhi-Kai Zhu, Shanghuo Li
Figure caption: HNC (1–0) channel map. The observational velocity resolution is 0.21 km s−1; here, we smooth the data to 0.42 km s−1. The contour levels start from 4σ and increase in steps of 10σ (1σ = 0.008 Jy beam−1). The cyan crosses indicate the position of cores 1, 2, 4, and 10, as labeled in Figure 1. The synthesized beam is given in the bottom right.
Paper: A Dense Molecular Ringlike Structure in Gaseous CO Depletion Region G34.74−0.12
Authors: Shuting Lin, Siyi Feng, Fengwei Xu, Ke Wang, Patricio Sanhueza, Junzhi Wang, Zhi-Yu Zhang, Yichen Zhang, Kaho Morii, Hauyu Baobab Liu, Sheng-Yuan Liu, Lile Wang, Giovanni Sabatini, Hui Li, Willem Baan, Zhi-Kai Zhu, Shanghuo Li
Figure caption: PV diagrams of C18O (2–1) along four cuts with a P.A. of 0°, 45°, 90°, and 135° (labeled in Figure 1) of the ringlike structure. The gray lines indicate the fitting results from HNC (1–0) (Figure 3). Contour levels are set at 10σ, 20σ, 30σ, and 40σ, where σ = 0.007 Jy beam−1.
Paper: A Dense Molecular Ringlike Structure in Gaseous CO Depletion Region G34.74−0.12
Authors: Shuting Lin, Siyi Feng, Fengwei Xu, Ke Wang, Patricio Sanhueza, Junzhi Wang, Zhi-Yu Zhang, Yichen Zhang, Kaho Morii, Hauyu Baobab Liu, Sheng-Yuan Liu, Lile Wang, Giovanni Sabatini, Hui Li, Willem Baan, Zhi-Kai Zhu, Shanghuo Li
Figure caption: C18O (2–1) channel map. The contour levels start from 5σ and increase in steps of 6σ (1σ = 0.007 Jy beam−1). The cyan crosses indicate the position of cores 1, 2, 4, and 10, as labeled in Figure 1. The synthesized beam is given in the bottom right.
Paper: A Dense Molecular Ringlike Structure in Gaseous CO Depletion Region G34.74−0.12
Authors: Shuting Lin, Siyi Feng, Fengwei Xu, Ke Wang, Patricio Sanhueza, Junzhi Wang, Zhi-Yu Zhang, Yichen Zhang, Kaho Morii, Hauyu Baobab Liu, Sheng-Yuan Liu, Lile Wang, Giovanni Sabatini, Hui Li, Willem Baan, Zhi-Kai Zhu, Shanghuo Li
Figure caption: PV diagrams of N2H+ (1–0) along four cuts with a P.A. of 0°, 45°, 90°, and 135° (labeled in Figure 1) of the ringlike structure. Contour levels are set at 3σ, 4σ, and 5σ, where σ = 0.008 Jy beam−1.
Paper: Jet Collimation in a Spiral-hosted Active Galactic Nucleus: A Parabolic Jet Profile in 0313–192
Authors: Seung Yeon Lee, Jae-Young Kim
Figure caption: Example of double-Gaussian fitting to a cross-jet intensity slice profile in order to decompose the jet and lobe emission. Left: an example VLA X-band, (u, v)-tapered CnD configuration image of 0313–192 (see Section 3). The red line shows a slice used to make the intensity profile on the right panel. Right: example of double-Gaussian fitting to the jet slice intensity profile. The data, fitted profiles for the single- and double-Gaussian cases, and the individual jet and lobe components are shown in the upper panel. The corresponding fit residuals are shown in the lower panel.
Paper: Jet Collimation in a Spiral-hosted Active Galactic Nucleus: A Parabolic Jet Profile in 0313–192
Authors: Seung Yeon Lee, Jae-Young Kim
Figure caption: Individual VLBA images of 0313–192 across different observing bands, tapering, and epochs, arranged vertically by observing date (in yymmdd format). From top left to bottom right, panels show the VLBA images at increasing beam sizes: raw-resolution X-band (top left), the raw and (u, v)-tapered S band (top center and top right), and the raw and tapered L-band images (bottom row). Within each panel, the restoring beam sizes (2, 8, 15, 10, and 30 mas, respectively) are shown by magenta circles located at the lower-left corner of each panel. Also, separation between contours of different colors is proportional to the time difference of the observing epochs. In all images, contour levels start at 2.5σ and increase by factors of 2.
Paper: Jet Collimation in a Spiral-hosted Active Galactic Nucleus: A Parabolic Jet Profile in 0313–192
Authors: Seung Yeon Lee, Jae-Young Kim
Figure caption: Jet widths vs. projected distances from the core, shown in logarithmic scale. The black solid line represents a broken power-law fit to the data, using Equation (1), with a fixed smoothness parameter h = 25. The dashed gray line corresponds to a single power-law fit to the data. The width errors include 10% of the measured value as additional systematic uncertainty, and its minimum is set to one-fifth of the beam size.
Paper: Jet Collimation in a Spiral-hosted Active Galactic Nucleus: A Parabolic Jet Profile in 0313–192
Authors: Seung Yeon Lee, Jae-Young Kim
Figure caption: Stacked VLBA and VLA images of 0313–192. Upper panels: images for VLBA X-band (top left), S band (top center), tapered S band (top right), L band (bottom left), and tapered L-band (bottom right). Restoring beam sizes are 2, 8, 15, 10, and 30 mas, respectively. Lower panels: VLA images in X-band A (top left), L-band A (top center), tapered L-band A (top right), X-band CnD (bottom left), tapered X-band CnD (bottom center), and L-band CnD (bottom right) configurations. Restoring beam sizes are 500, 2500, 3500, 5000, 13,000, and 25,000 mas, respectively. Contours in all images start at 2.5σ image noise levels and increase by factors of 2. The color scale indicates total intensity in Jy beam–1.
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: Observations of the nine hyperfine components of the CN N = 1–0 transition from the TW Hya disk used in this Letter. The flux densities are calculated by integrating a circular mask with a radius of 4″. Each spectrum shows ±300 kHz (≈800 m s−1) around the line center. The w value under each line denotes the relative sensitivity of the component to Zeeman broadening. Note the sensitivity of the line to magnetic fields is uncorrelated with the intensity.
Paper: A Radially Resolved Magnetic Field Threading the Disk of TW Hya
Authors: Richard Teague, Boy Lankhaar, Sean M. Andrews, Chunhua Qi, Roger R. Fu, David J. Wilner, John B. Biersteker, Joan R. Najita
Figure caption: How the line strengths and positions of the three magnetic subtransition groups (π0, σ+, σ−) vary when differing the orientation of a 15 mG magnetic field relative to the line of sight described by θ for the most sensitive hyperfine component, N = 1–0   J = 3/1–1/2   F = 3/2–1/2 (left), and the least sensitive component, N = 1–0   J = 3/1–1/2   F = 5/2–3/2 (right). Magnetic subtransition groups are influenced by a magnetic field, broadening the line profile by an amount proportional to the sensitivity of the component to Zeeman broadening. At the 15 mG assumed here, the resulting line profile, the sum of the three components, is still close to a Gaussian profile. The gray annotations in the lower left of each panel show the relative change in line width and optical depth at the line center relative to an unsplit transition. For the most sensitive component, the changing field orientation leads to a different level of broadening and a corresponding change in the peak optical depth, while for the least sensitive component, there is only an imperceptible change with changing field orientation.