adsabs/AstroCLIMB huggingface dataset:
Paper: Catalog of Integrated-light Star Cluster Light Curves in TESS
Authors: Tobin M. Wainer, Gail Zasowski, Joshua Pepper, Tom Wagg, Christina L. Hedges, Vijith Jacob Poovelil, Tara Fetherolf, James R. A. Davenport, P. Marios Christodoulou, Jack T. Dinsmore, Avi Patel, Kameron Goold, Benjamin J. Gibson
Figure caption: LSPs for thee MW clusters with Cepheid variable stars inside the cluster radius (Medina et al. 2021). The blue line represents the LSP power for each cluster, and the gray region is the frequency range of the LSP to which our light-curve correction methodology is not sensitive. The dashed gold lines correspond to the literature frequencies for the Cepheids.
Paper: Catalog of Integrated-light Star Cluster Light Curves in TESS
Authors: Tobin M. Wainer, Gail Zasowski, Joshua Pepper, Tom Wagg, Christina L. Hedges, Vijith Jacob Poovelil, Tara Fetherolf, James R. A. Davenport, P. Marios Christodoulou, Jack T. Dinsmore, Avi Patel, Kameron Goold, Benjamin J. Gibson
Figure caption: Properties of the clusters in this paper’s catalog. The top row shows the distribution of the MW clusters (Section 2.1.1) in Galactocentric radius and height above the plane ∣Z GC∣ and of the SMC and LMC clusters (Sections 2.1.3–2.1.2) in R.A. and decl., colored by their ages. The bottom panels show the distributions of cluster angular radius (left), median TESS magnitude of the integrated light (middle), and log(age) of the clusters (right). Background (g-band) images of the LMC and SMC are from the SMASH survey (Nidever et al. 2017, 2021).
Paper: Catalog of Integrated-light Star Cluster Light Curves in TESS
Authors: Tobin M. Wainer, Gail Zasowski, Joshua Pepper, Tom Wagg, Christina L. Hedges, Vijith Jacob Poovelil, Tara Fetherolf, James R. A. Davenport, P. Marios Christodoulou, Jack T. Dinsmore, Avi Patel, Kameron Goold, Benjamin J. Gibson
Figure caption: The LSP for each sector of observation for NGC 1261 (Section 5.2). The vertical lines in each panel correspond to literature frequencies of the cluster’s 20 RRL stars and are colored by the G-band amplitude of variation seen in Figure 6. The bottom panel is the LSP for the sector-stitched light curve, sampled more finely owing to the increased baseline of considering multiple sectors.
Paper: Catalog of Integrated-light Star Cluster Light Curves in TESS
Authors: Tobin M. Wainer, Gail Zasowski, Joshua Pepper, Tom Wagg, Christina L. Hedges, Vijith Jacob Poovelil, Tara Fetherolf, James R. A. Davenport, P. Marios Christodoulou, Jack T. Dinsmore, Avi Patel, Kameron Goold, Benjamin J. Gibson
Figure caption: The CMD for NGC 1261 is shown on the left. All of the Gaia stars are shown in gray, and the 20 RRL stars discussed in Section 5.2 are colored according to the amplitude of their G-band photometric variability. The middle panel is the TESS flux map, with points indicating the location of the RRL stars from the left panel. On the right is the HST F606W image, mapped to the sky position of the TESS image. Both images are centered at (α, δ) = (48.060, − 55.225), covering the central ∼3′ of the cluster.
Paper: Catalog of Integrated-light Star Cluster Light Curves in TESS
Authors: Tobin M. Wainer, Gail Zasowski, Joshua Pepper, Tom Wagg, Christina L. Hedges, Vijith Jacob Poovelil, Tara Fetherolf, James R. A. Davenport, P. Marios Christodoulou, Jack T. Dinsmore, Avi Patel, Kameron Goold, Benjamin J. Gibson
Figure caption: The normalized light-curve standard deviation as a function of ﹩\mathrm{log}({\rm{S}}/{\rm{N}})﹩ (Section 4.1). Each point represents a sector observation: black for MW clusters (which have the highest S/N owing to their close proximity), blue for SMC clusters, and red for LMC clusters. The green line represents the theoretical limit for a light curve being dominated by purely Gaussian noise.
Paper: Catalog of Integrated-light Star Cluster Light Curves in TESS
Authors: Tobin M. Wainer, Gail Zasowski, Joshua Pepper, Tom Wagg, Christina L. Hedges, Vijith Jacob Poovelil, Tara Fetherolf, James R. A. Davenport, P. Marios Christodoulou, Jack T. Dinsmore, Avi Patel, Kameron Goold, Benjamin J. Gibson
Figure caption: Distribution of the 1σ uncertainty for LMC cluster range and standard deviation metrics (Section 4.1), demonstrating the consistency in which the flux distribution metrics are consistent across each available sector of observation.
Paper: Terrestrial- and Neptune-mass Free-Floating Planet Candidates from the MOA-II 9 yr Galactic Bulge Survey
Authors: Naoki Koshimoto, Takahiro Sumi, David P. Bennett, Valerio Bozza, Przemek Mróz, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Two- and one-dimensional detection efficiencies including finite-source measurements. The top row shows ϵ(t E, θ E), which is the detection efficiency as a function of the Einstein radius crossing time, t E, and angular Einstein radius θ E. The middle row shows the detection efficiency, ϵ(t E, ρ), as a function of t E and the finite-source parameter ρ, and the bottom row shows the one-dimensional integrated detection efficiencies as a function of t E. The orange solid, blue dashed, and green dotted curves in the bottom panels show ﹩\tilde{\epsilon }({t}_{{\rm{E}}};{\rm{\Gamma }})﹩ with the best-fit Γ(t E, θ E) taken from S23, with Γ(t E, θ E) = const. in the simulated range, and with the PSPL assumption, respectively. The left, middle, and right columns show the detection efficiencies for field gb9, field gb19, and the mean of all 20 fields using criteria CR2. The simulation is limited in 0.8 ≤ μ rel/(mas yr−1) ≤ 20. Note that our selection criteria (Table 2) do not require θ E to be measurable.
Paper: Terrestrial- and Neptune-mass Free-Floating Planet Candidates from the MOA-II 9 yr Galactic Bulge Survey
Authors: Naoki Koshimoto, Takahiro Sumi, David P. Bennett, Valerio Bozza, Przemek Mróz, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Relative probability distributions of event rate, Γ(t E, θ E) (left), Γ(θ E∣t E) (middle), and Γ(t E∣θ E) (right), calculated using the Galactic model of Koshimoto et al. (2021a) but with the modified broken power law given by Equation (10), where α 4 = 0, α 4 = 0.92 (best), and α 4 = 1.5 are used in the top, middle, and bottom panels, respectively. Lower and upper dashed gray lines in each panel indicate μ rel = 0.8 mas yr−1 and μ rel = 20 mas yr−1, respectively. Note that while the distributions in long t E and/or large θ E should be the same across all α 4 values, they appear different because we used Monte Carlo simulations, which generated fewer high-mass lens events with larger α 4 values.
Paper: Terrestrial- and Neptune-mass Free-Floating Planet Candidates from the MOA-II 9 yr Galactic Bulge Survey
Authors: Naoki Koshimoto, Takahiro Sumi, David P. Bennett, Valerio Bozza, Przemek Mróz, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Dependence of integrated detection efficiency on the mass function for three different slopes in the planetary mass range, α 4 = 0, 0.92, and 1.5, for different event selection criteria and different variables, t E and θ E. Panels (a) and (b) show the detection efficiency as a function of t E after integrating over θ E for our original selection criterion CR2, which yields ﹩\tilde{\epsilon }({t}_{{\rm{E}}};{\rm{\Gamma }})﹩ in panel (a), and for our modified criterion, which requires a θ E measurement, yielding ﹩{\tilde{\epsilon }}_{\mathrm{FS}}({t}_{{\rm{E}}};{\rm{\Gamma }})﹩ in panel (b). Panel (c) shows ﹩{\tilde{\epsilon }}_{\mathrm{FS}}({\theta }_{{\rm{E}}};{\rm{\Gamma }})﹩, which is the integrated detection efficiency as a function of θ E using the modified selection criterion that requires a θ E measurement. In each panel, the orange solid, magenta dashed, and cyan dashed curves show integrated detection efficiencies with the event rate Γ(t E, θ E) calculated with the mass functions with α 4 = 0.92 (consistent with the best fit in S23), α 4 = 0, and α 4 = 1.5.
Paper: Terrestrial- and Neptune-mass Free-Floating Planet Candidates from the MOA-II 9 yr Galactic Bulge Survey
Authors: Naoki Koshimoto, Takahiro Sumi, David P. Bennett, Valerio Bozza, Przemek Mróz, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Detection efficiencies for FSPL events as functions of (a) the timescale t E and the angular Einstein radius θ E, (b) t E, and (c) θ E, for the mean of all 20 fields with the criterion CR2. In panels (b) and (c), the orange solid and blue dashed curves show integrated detection efficiencies with the best-fit Γ(t E, θ E) taken from S23 and with Γ(t E, θ E) = const. in the simulated range, respectively. The solid orange histogram indicates the 13 FSPL events detected in our sample, where 10−6 corresponds to one event. The green line in panel (c) shows the relative detection efficiency for the KMTNet giant source sample (Gould et al. 2022).
Paper: Terrestrial- and Neptune-mass Free-Floating Planet Candidates from the MOA-II 9 yr Galactic Bulge Survey
Authors: Naoki Koshimoto, Takahiro Sumi, David P. Bennett, Valerio Bozza, Przemek Mróz, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: The extinction-free CMD of an MOA subfield gb13-5-4, which combines the MOA data (black circles) and the HST data by Holtzman et al. (1998; green circles). The orange curve is the isochrone matched to this subfield. The cyan square is the RCG centroid. The red filled circles with error bars are sources of the 13 FSPL events. The blue filled circles indicate the two FFP candidates.
Paper: Terrestrial- and Neptune-mass Free-Floating Planet Candidates from the MOA-II 9 yr Galactic Bulge Survey
Authors: Naoki Koshimoto, Takahiro Sumi, David P. Bennett, Valerio Bozza, Przemek Mróz, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Posterior mass and distance distributions of the two FFP and one BD candidates by a Bayesian analysis. The blue histograms are for when the slope α 4 is applied down to 10−8  M ⊙ (M lo = 0.0033 M ⊕). The orange histograms are for when the slope α 4 is applied down to 10−6  M ⊙ and ﹩{dN}/d\mathrm{log}M=\mathrm{const}.﹩ is applied for M < 10−6  M ⊙ (M lo = 0.33 M ⊕).
Paper: Terrestrial- and Neptune-mass Free-Floating Planet Candidates from the MOA-II 9 yr Galactic Bulge Survey
Authors: Naoki Koshimoto, Takahiro Sumi, David P. Bennett, Valerio Bozza, Przemek Mróz, Andrzej Udalski, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Light curves of the BD candidate MOA-9y-1944.
Paper: A Hierarchical Bayesian Framework for Inferring the Stellar Obliquity Distribution
Authors: Jiayin Dong, Daniel Foreman-Mackey
Figure caption: A probabilistic graphical model showing the conditional structure of our hierarchical Bayesian framework for inferring the stellar obliquity distribution of exoplanetary systems. The population model is parameterized by hyperparameters  β , and it is constrained by the stellar obliquity ψ  n  of each n th individual system. The stellar obliquity ψ  n , azimuthal angle θ  n , and orbital inclination i orb,n  are constrained by the sky-projected stellar obliquity λ  n  and, if available, the stellar inclination i ⋆,n . Properties of the star other than its inclination, such as its radius and rotation period, are represented by γ ⋆,n , and these can inform the constraint on i ⋆,n , if available. ﹩{\hat{\lambda }}_{n}﹩ comprises the measured sky-projected stellar obliquity and its uncertainty, Obs⋆,n  contains all observed properties of the star with uncertainties, and ﹩{\hat{i}}_{\mathrm{orb},n}﹩ comprises the measured orbital inclination and its uncertainty (✎).
Paper: A Hierarchical Bayesian Framework for Inferring the Stellar Obliquity Distribution
Authors: Jiayin Dong, Daniel Foreman-Mackey
Figure caption: Two coordinate systems that describe the stellar spin axis ﹩{\hat{{\boldsymbol{n}}}}_{\star }﹩ and the planet’s orbital axis ﹩{\hat{{\boldsymbol{n}}}}_{\mathrm{orb}}﹩. The {ψ, θ} coordinate system setup is motivated by the physical properties of a planetary system. The {λ, i ⋆} coordinate system setup is motivated by observables (✎).
Paper: A Hierarchical Bayesian Framework for Inferring the Stellar Obliquity Distribution
Authors: Jiayin Dong, Daniel Foreman-Mackey
Figure caption: Inferred stellar obliquity distribution for the full sample of exoplanetary systems with sky-projected stellar obliquity measurements (left panel) and the subsample of systems with both sky-projected stellar obliquity measurements and stellar inclination measurements (middle and right panels). The subsample inference made purely from measured projected stellar obliquity is shown in the middle panel, and the subsample inference made from both measured projected stellar obliquity and stellar inclination is shown in the right panel. The line and shallow contours represent the median and 1σ and 2σ uncertainties of the inferred distributions. The samples are extracted from Albrecht et al. (2021, 2022) (✎).
Paper: A Hierarchical Bayesian Framework for Inferring the Stellar Obliquity Distribution
Authors: Jiayin Dong, Daniel Foreman-Mackey
Figure caption: Simulated ﹩\cos \psi ﹩ distributions (first column) and the corresponding distributions of sky-projected stellar obliquity λ (second column) and stellar inclination i ⋆ (third column). The gray histograms present the random samplings of λ and i ⋆ from the ﹩\cos \psi ﹩ distributions, and the blue curves present the numerical solutions (✎).
Paper: A Hierarchical Bayesian Framework for Inferring the Stellar Obliquity Distribution
Authors: Jiayin Dong, Daniel Foreman-Mackey
Figure caption: Inferred stellar obliquity distribution for all exoplanetary systems with sky-projected stellar obliquity measurements. This inference is based purely on the observed sky-projected obliquities using a two-component model. The blue line and shallow contours represent the median and 1σ and 2σ uncertainties of the inferred distributions. The medians of the two components are shown as dashed and dotted–dashed lines (✎).
Paper: A Hierarchical Bayesian Framework for Inferring the Stellar Obliquity Distribution
Authors: Jiayin Dong, Daniel Foreman-Mackey
Figure caption: Inferred stellar obliquity distributions from sky-projected stellar obliquities without and with information on the stellar inclination, depicted in blue and orange curves, respectively. Each row presents a set of simulated data with the true distribution of ﹩\cos \psi ﹩ indicated by gray dashed curves. The shallow contours represent the 1σ and 2σ uncertainties of the inferred distribution (✎).
Paper: The Kiloparsec-scale Influence of the AGN in NGC 1068 with SALT RSS Fabry–Pérot Spectroscopy 
Authors: Raphael E. Hviding, Ryan C. Hickox, Petri Väisänen, Rajin Ramphul, Kevin N. Hainline
Figure caption: The reduced data of NGC 1068. In panel (a) we present the reduced 2D spectrum of NGC 1068 taken with the RSS longslit (top) along with the sum along the spatial dimension (bottom). In panel (b) we show the total measured intensity of the FP observations (left) along with the associated signal-to-noise ratio (S/N; right). In addition we provide the spatial scale of the image assuming 10.1 Mpc and 13.97 Mpc distances to NGC 1068 (top right corner), the orientation of the image (bottom right corner), and a circle depicting the final FWHM of our observation. Due to the nature of the stationary primary mirror of SALT, no absolute flux calibration can be performed from the data.
Paper: The Kiloparsec-scale Influence of the AGN in NGC 1068 with SALT RSS Fabry–Pérot Spectroscopy 
Authors: Raphael E. Hviding, Ryan C. Hickox, Petri Väisänen, Rajin Ramphul, Kevin N. Hainline
Figure caption: The final binning of the FP data of NGC 1068 generated from the VorBin routine. Panel (a) depicts the Voronoi tessellation map of NGC 1068. The sizes of the Voronoi bins are chosen to achieve bins of a minimum intensity. Note how the bin size increases with distance from the center, as the intensity from the galaxy falls off. Panels (b) and (c) present the number of pixels and S/N in a given bin, respectively. Finally, panel (d) shows how the total number of bins changes with distance from the center (red), along with the total enclosed intensity at a given radius (blue).
Paper: The Kiloparsec-scale Influence of the AGN in NGC 1068 with SALT RSS Fabry–Pérot Spectroscopy 
Authors: Raphael E. Hviding, Ryan C. Hickox, Petri Väisänen, Rajin Ramphul, Kevin N. Hainline
Figure caption: Velocity maps (left) and their associated standard deviations (right) for the Hα (top) and [N II] (bottom) emission lines. The colorbars for the velocity are centered on the systemic redshift of NGC 1068 corresponding to 1137 km s−1.
Paper: The Kiloparsec-scale Influence of the AGN in NGC 1068 with SALT RSS Fabry–Pérot Spectroscopy 
Authors: Raphael E. Hviding, Ryan C. Hickox, Petri Väisänen, Rajin Ramphul, Kevin N. Hainline
Figure caption: The final binning of the longslit data of NGC 1068 generated from the VorBin routine. Panel (a) depicts the bin map of the longslit data. The sizes of the Voronoi bins are chosen to achieve bins of a minimum intensity. Panels (b) and (c) present the number of pixels and S/N in a given bin, respectively. Finally, panel (d) depicts the total intensity summed along the spectral dimension (red), along with the cumulative number of bins (blue).
Paper: The Kiloparsec-scale Influence of the AGN in NGC 1068 with SALT RSS Fabry–Pérot Spectroscopy 
Authors: Raphael E. Hviding, Ryan C. Hickox, Petri Väisänen, Rajin Ramphul, Kevin N. Hainline
Figure caption: Our model of the kiloparsec-scale ionized region as light echoes from the AGN in NGC 1068. In the top panel we present the model lightcurves with the main model depicted in solid purple. The center left panel shows the derived (Hα)AGN flux in log scale. In the bottom left panel we show the modeled AGN flux following the procedure described in Section 5.4 in log scale. We plot the radial profiles of the derived (Hα)AGN flux (solid) and the model AGN lightcurves (dashed) for the four cardinal directions in the center middle (south), right middle (west), center bottom (north), and right bottom (east) panels.
Paper: The Kiloparsec-scale Influence of the AGN in NGC 1068 with SALT RSS Fabry–Pérot Spectroscopy 
Authors: Raphael E. Hviding, Ryan C. Hickox, Petri Väisänen, Rajin Ramphul, Kevin N. Hainline
Figure caption: In panel (a), we overplot colored longslit positions on the FP log10(Hα/[N II]) diagnostic map. In panel (b) we plot the BPT positions of the colored longslit positions to highlight the transition between the star-forming and AGN regions of NGC 1068 along the longslit spectrum. With the additional [O III] and Hβ information afforded by the longslit spectrum, the source of the kiloparsec-scale ionization features becomes clear as the line ratios are consistent with that of an AGN. In addition, we plot the Kewley et al. (2001a) and Kauffmann et al. (2003b) demarcations as solid and dashed lines, respectively.
Paper: The Kiloparsec-scale Influence of the AGN in NGC 1068 with SALT RSS Fabry–Pérot Spectroscopy 
Authors: Raphael E. Hviding, Ryan C. Hickox, Petri Väisänen, Rajin Ramphul, Kevin N. Hainline
Figure caption: Maps of Hα/[N II] (left) and their associated S/N (right) for the FP (top) and longslit (bottom) data. The longslit observations are plotted over the gray-scale FP Hα/[N II] ratio maps. The longslit observations confirm the accuracy of our FP data reduction and analysis and highlight the kiloparsec-scale ionizing features.
Paper: The Kiloparsec-scale Influence of the AGN in NGC 1068 with SALT RSS Fabry–Pérot Spectroscopy 
Authors: Raphael E. Hviding, Ryan C. Hickox, Petri Väisänen, Rajin Ramphul, Kevin N. Hainline
Figure caption: In panel (a), we overplot the BPT positions of the longslit spectrum bins on the FP log10(Hα/[N II]) diagnostic map. In panel (b), we present the stacked spectra from the highlighted regions in panel (a). The selected regions highlight the transition of the longslit spectrum from star-forming to AGN activity across the FoV. In addition, the spectra reveal the rotational motion of the galaxy with the slight shift of the emission lines relative to the average redshift of the galaxy.
Paper: The Kiloparsec-scale Influence of the AGN in NGC 1068 with SALT RSS Fabry–Pérot Spectroscopy 
Authors: Raphael E. Hviding, Ryan C. Hickox, Petri Väisänen, Rajin Ramphul, Kevin N. Hainline
Figure caption: Emission line flux maps (left) and their associated standard deviations (right) for the Hα (top) and [N II] λ6583 (bottom) lines. While there is no absolute flux calibration due to the nature of the stationary primary mirror of SALT, the relative flux is preserved.
Paper: Refining the Stellar Parameters of τ Ceti: a Pole-on Solar Analog
Authors: Maria Korolik, Rachael M. Roettenbacher, Debra A. Fischer, Stephen R. Kane, Jean M. Perkins, John D. Monnier, Claire L. Davies, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Tyler Gardner, Cyprien Lanthermann, Gail H. Schaefer, Benjamin Setterholm, John M. Brewer, Joe Llama, Lily L. Zhao, Andrew E. Szymkowiak, Gregory W. Henry
Figure caption: Total rotational broadening of 2934 spectra of τ Ceti from three different spectrographs. The Chiron spectra (red) show a bimodal distribution caused by poor characterization of the instrumental profile when using the fiber slicer vs. the slit, which has a higher resolution. The dwarf macroturbulence relation from Brewer et al. (2016; blue line) shows that, for most of the spectra, there is no appreciable rotation beyond that likely due to macroturbulence, resulting in our low estimate of ﹩v\sin i﹩ = 0.1 ± 0.1 km s−1.