adsabs/AstroCLIMB huggingface dataset:
Paper: OTI on FIRE: Testing the Efficacy of Orbital Torus Imaging to Recover the Galactic Potential
Authors: Micah Oeur, Sarah R. Loebman, Adrian M. Price-Whelan, Arpit Arora, Lina Necib, Danny Horta
Figure caption: This table summarizes key local disk properties across solar volumes, including asymmetry, vertical metallicity gradient slope, total density at z = 1.1 kpc, median age, scale height, and normalized χ2. We color code each cell by relative score: red (worst), yellow (intermediate), and green (best); worse scores are those we find correlate with a decrease in OTI accuracy for the az estimates. Total density, age, and scale height show the strongest correlation with normalized χ2, suggesting greater importance for OTI accuracy than asymmetry or vertical metallicity gradient slope (see Section 6 and Figure 9 for further discussion). Volumes with high χ2 (e.g., V14, V13, V3) tend to have low Σ⊙, large scale heights, and older populations, while those with low χ2 (e.g., V6, V7, V9) show the opposite trend.
Paper: OTI on FIRE: Testing the Efficacy of Orbital Torus Imaging to Recover the Galactic Potential
Authors: Micah Oeur, Sarah R. Loebman, Adrian M. Price-Whelan, Arpit Arora, Lina Necib, Danny Horta
Figure caption: Vertical acceleration gradient (﹩\frac{d{a}_{z}}{dz}﹩) for all 16 solar-analog volumes, similar to Figure 3 from A. Arora et al. (2024b), for m12i assuming a ΛCDM cosmology. For the majority of volumes, OTI (black dashed line) recovers the true FIRE (solid black line) ﹩\frac{d{a}_{z}}{dz}﹩ profile within the 3σ limit. For reference, the MW’s best-fit ﹩\frac{d{a}_{z}}{dz}﹩ at z = 0 kpc is −3200 ± 2560 Gyr−2 (T. Donlon et al. 2024), which lies within the range of values we probe with OTI. As discussed in Section 6.1, the volume-to-volume variation is on the same scale as the variation expected between SIDM and CDM, suggesting caution regarding its use in differentiating between dark matter models. See Section 6.1 for further discussion.
Paper: OTI on FIRE: Testing the Efficacy of Orbital Torus Imaging to Recover the Galactic Potential
Authors: Micah Oeur, Sarah R. Loebman, Adrian M. Price-Whelan, Arpit Arora, Lina Necib, Danny Horta
Figure caption: Age histograms (colored lines) for each solar volume with the mean histogram (gray line) across all volumes. Vertical lines indicate the predisk, early disk, and late disk definitions following F. McCluskey et al. (2024), denoting three different epochs of star formation. We find a moderately strong correlation (Pearson’s r = 0.56) between the fraction of intermediate-to-old (>4 Gyr) stars, fold, and χ2 (Equation (10)): volumes with a high (>0.5) fraction of old stars correlate with a loss in OTI model accuracy (i.e., high χ2) for the az estimates. See Section 6 for further discussion.
Paper: Feature Intensity Mapping: Polycyclic Aromatic Hydrocarbon Emission from All Galaxies Across Cosmic Time
Authors: Yun-Ting Cheng, 昀庭 鄭, Brandon S. Hensley, Thomas S.-Y. Lai, 劭愉 賴
Figure caption: Normalized observed spectral profiles (νIν) as a function of observed wavelength for various spectral features considered in this work. The relative luminosity and spectral shape of each feature are described in Section 4.1. The left, middle, and right columns show the cases for SPHEREx, PHI, and FIRESS, respectively, with three example redshifts in each row (z = 0, 0.2, and 0.5 for SPHEREx; z = 1, 3, and 5 for PHI and FIRESS). Solid lines represent the intrinsic spectral shapes of the features, and dots indicate the intensities that will be observed by the spectral channels of the respective survey. The central wavelength of each feature is marked with a dashed vertical line for visual clarity. The inset panels show a zoomed-in view of the same spectrum on a log scale to better visualize the faint features.
Paper: Feature Intensity Mapping: Polycyclic Aromatic Hydrocarbon Emission from All Galaxies Across Cosmic Time
Authors: Yun-Ting Cheng, 昀庭 鄭, Brandon S. Hensley, Thomas S.-Y. Lai, 劭愉 賴
Figure caption: Top: SPHEREx spectral resolution of each channel. Bottom: SPHEREx surface brightness sensitivity per spectral channel in a 6﹩\mathop{.}\limits^{\unicode{x02033}}﹩2 sky pixel. The brown and gray points represent the SPHEREx all-sky and deep-field sensitivity, respectively.
Paper: Asymptotic Giant Branch Mass-loss Rates and Metal Yields from Scaled Mixing-length and Mass-loss Parameters
Authors: Ezra Huscher, Kristian Finlator, Jason Jackiewicz
Figure caption: More ejected isotope yields as a function of initial stellar mass for three initial metallicities: nearly metal free (0.0001), solar (0.015), and supersolar (0.03). For comparison, yields from A. I. Karakas (2010; 13C at Z = 0.0001) and U. Battino et al. (2022; Z = 0.01 and Z = 0.03 at 2 M⊙ and 3 M⊙) are included where available.
Paper: Learning to Estimate Photospheric Vector Fields from Line-of-sight Magnetograms
Authors: David Fouhey, KD Leka
Figure caption: Distributions produced by SSLOS . We show two examples (both 75″ × 75″): a simple active region near disk center (NOAA 12418 2015 September 17, 12:36TAI) and a more complex region on the limb (NOAA 12488; 2016 January 28, 18:24 TAI). Top panels: we show the inferred three components as well as the inferred distribution over angles at four locations per sample. We visualize the angular distribution on a Mollweide projection with a power law applied to the color map (min  max probability) to enhance contrast. At the low-polarization region (A), SSLOS is uncertain about direction and produces the great circle corresponding to the Milne-Eddington plus disambiguation method. Within the region (B,C,D), it is more confident. At another low-polarization area (E), SSLOS is again uncertain, but produces a different distribution (with BR near zero). At (F), it is confident. Near the polarity inversion line (G), the results are very uncertain, and at (H), there is considerable spread. Bottom panels: line plots through the samples of each component. We plot SSLOS in red solid lines (along with shaded confidence intervals) and HMIP in blue dashed lines. Color map: −2000  2000 Mx cm−2 . Mollweide coordinate system: BR = 0 along the vertical center; Bϕ = 0 along the horizontal center line; Bθ = 0 along center ring.
Paper: Learning to Estimate Photospheric Vector Fields from Line-of-sight Magnetograms
Authors: David Fouhey, KD Leka
Figure caption: Overview. The radial component of the magnetic field BR is the preferred quantity of interest, but many instruments only provide the magnetic field projected on the line of sight, Blos. Blos is often heuristically corrected to BR by accounting for viewing angle μ and assuming that the field is radial. We show 130″ × 100″ cutouts from NOAA AR 13664 close to the limb, 2024 May 10, 22:48 TAI, 2 hr before an X5.8 flare. The μ-corrected Blos has false polarity inversion lines and several other incorrect polarities (all indicated with arrows →). Our learned correction improves over the μ-correction for BR and also estimates a rough (albeit not insufficiently sheared) Bϕ and Bθ. Color map: −3000  3000 Mx cm−2 with μ isocountours in dotted lines (every 0.1 here, and throughout the paper unless otherwise specified). Please note that this and all subsequent figures, are best viewed in color on a screen. This figure, and all purple-orange colormapped results are plotted with the y-axis inverted compared to many other visualizations due to a difference in Python and IDL conventions.
Paper: Learning to Estimate Photospheric Vector Fields from Line-of-sight Magnetograms
Authors: David Fouhey, KD Leka
Figure caption: Bivariate log-histograms of BR in active regions and plage using SDO/HMI and NSO/GONG Blos data. We compare results from μ-corrected Blos and SSLOS . We plot a y = x line and y = 0 and x = 0 lines in red. Content in the top-left or bottom-right quadrants comprises polarity errors. The proposed method improves over the standard μ-correction as seen by the tighter alignment with the axis and substantial reduction in polarity confusions. In plage with SDO/HMI Blos , the proposed method shows slight concentration at the y = −x diagonal. These errors are on pixels with low field strength; the μ-correction has a similar amount of polarity confusion, but it is spread out over more values since the μ-correction does not get the magnitude right. Color map: empty bins are colored white; non-empty bins follow lowest  highest density. Color maps are logarithmically colored, and normalized identically per-condition (e.g., GONG AR, HMI Plage) in this and the Bϕ/Bθ plots in Figure 8.
Paper: Learning to Estimate Photospheric Vector Fields from Line-of-sight Magnetograms
Authors: David Fouhey, KD Leka
Figure caption: Comparison of SSLOS with ablations (variants of the method with modules/steps removed). Without logit dither, there are large regions with the same orientation in low-polarization regions. Without smoothing, there are regions of uncertainty and “flip-flopping” near polarity inversions. Smoothing helps mitigate the artifact. While the HMIP BR appears to have smaller values in parts of the region as compared to SSLOS, this is due to a disagreement in orientation: SSLOS and HMIP agree on the total length, as seen in Figure 5. Data: NOAA AR 1570 captured 2016 August 7, 13:12 TAI. Color map: −2000  2000 Mx cm−2.
Paper: Learning to Estimate Photospheric Vector Fields from Line-of-sight Magnetograms
Authors: David Fouhey, KD Leka
Figure caption: Comparison of BR and ∣∣B∣∣, using the same data (NOAA AR 12570) as Figure 3. We show the reference HMIP data, Blos/mu, the per-component ℓ1 regression, and SSLOS . Per-component ℓ1 regression and Blos/μ systematically underestimate the total magnetic flux density. Blos/μ assumes that Bϕ and Bθ are zero, and so is an underestimate and has false zero-flux density lines through sunspots. Per-component ℓ1 regression does well in active regions, but zeros-out the flux density in regions with low-polarization signal. This is because the per-component ℓ1 minimizing solution for these pixels is, in fact zero. SSLOS faithfully handles both the active regions as well as the low-polarization regime.
Paper: Learning to Estimate Photospheric Vector Fields from Line-of-sight Magnetograms
Authors: David Fouhey, KD Leka
Figure caption: A schematic illustrating why Blos cannot be easily converted to physically meaningful data, where the paper is the ecliptic plane. Many applications need BR, the radial component of the magnetic field B, but many important instruments only provide the projection of the field onto the line of sight Blos. When the field is inclined away from radial, Blos cannot be straightforwardly related to BR: in this example, Blos has the wrong sign. Similarly, if the field were flipped around the BR angle and pointed at the viewer, it would be a substantial overestimate. Diagram following K. Leka et al. (2017).
Paper: Learning to Estimate Photospheric Vector Fields from Line-of-sight Magnetograms
Authors: David Fouhey, KD Leka
Figure caption: Selected results for BR for NSO/GONG . We show both a simple sunspot in the left panels (NOAA AR 12553), and a more complex region in the right panels (NOAA AR 12595). In both cases, we point to false polarity inversion lines with arrows in the Blos/μ results. While more easily seen on the limbs, these false inversion lines appear closer to disk center. Color map: BR color map: −2000  2000 Mx cm−2.
Paper: A Search for Minute-timescale Flares from the Transient AT 2024wpp
Authors: Eran O. Ofek, Lior Ozer, Ruslan Konno, Nimrod Strasman, Ping Chen, Sagi Ben-Ami, David Polishook, Alexander Krassilchtchikov, Simone Garrappa, Erez A. Zimmermann, Enrico Segre, Asaf Horowicz, Avishay Gal-Yam, Yarin M. Shani, Stanislav Fainer, Michael Engel, Yahel Sofer-Rimalt, Anna Y. Q. Ho, Yossi Shvartzvald, Ofer Yaron, Kris Rybicki, Arie Blumenzweig, Sarah Spitzer, Ron Arad
Figure caption: The cumulative independent observing time of AT 2024wpp, as a function of the absolute magnitude corresponding to the 5σ detection limit. The upper x-axis indicates the approximate luminosity, in erg s−1, corresponding to the absolute magnitude.
Paper: Consistent Gas-phase C/O Abundances from UV and Optical Emission Lines: A Robust Scale for Chemical Evolution across Cosmic Time
Authors: Paige M. Kelly, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Danielle A. Berg, Peter Senchyna, Fabio Bresolin, Daniel Stark
Figure caption: C2+/O﹩{}_{\mathrm{CELs}}^{2+}﹩ vs. C2+/O﹩{}_{\mathrm{RLs}}^{2+}﹩ for the four cases outlined in Section 4.2 and summarized in each panel. t2, Te([O III]), C2+/O﹩{}_{\mathrm{RLs}}^{2+}﹩, and Te([S III]) are from the literature (see Table 1). The black points represent the four H II regions presented, and the open points are from the literature. A 1:1 relationship is indicated in purple, with all cases showing good agreement. The average offset between the ionic abundances obtained from RLs and CELs is displayed in the bottom right of each panel. The teal line is shifted by the average ADF(O2+) of our H II regions, showing the trend we would expect if carbon did not exhibit an ADF.
Paper: Consistent Gas-phase C/O Abundances from UV and Optical Emission Lines: A Robust Scale for Chemical Evolution across Cosmic Time
Authors: Paige M. Kelly, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Danielle A. Berg, Peter Senchyna, Fabio Bresolin, Daniel Stark
Figure caption: log(C2+/O2+) derived from RLs (from C. Esteban et al. 2009; C. Esteban et al. 2014, and L. Toribio San Cipriano et al. 2017) vs. the equivalent UV CEL-based measurements described in Section 3.3. For the UV CEL-based abundances, we used Te([O III]) for both C2+ and O2+. The UV CEL and optical RL values are in good agreement, all falling near the 1:1 line shown in black. The square symbols represent sources from the literature (Mrk 71 and N88A), which are included in our analysis. We note that N66A and N81 overlap due to their nearly identical values.
Paper: Consistent Gas-phase C/O Abundances from UV and Optical Emission Lines: A Robust Scale for Chemical Evolution across Cosmic Time
Authors: Paige M. Kelly, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Danielle A. Berg, Peter Senchyna, Fabio Bresolin, Daniel Stark
Figure caption: C2+/O2+ abundance derived for N66A at varying extraction widths of the G185M spectrum, which covers the C III] emission. The star indicates the chosen BOXCAR pixel height of 95 pixels. This was chosen based on the spatial profile of emission seen in the 2D spectra, as described in the main text. Uncertainty due to the extraction width was determined using C2+/O2+ at heights from 57 to 95. This corresponds to an uncertainty of  ±0.01 dex, which is small compared to the statistical uncertainty (pink shaded region). In all targets, we find that uncertainty due to the extraction aperture is small compared to other sources of uncertainty.
Paper: Consistent Gas-phase C/O Abundances from UV and Optical Emission Lines: A Robust Scale for Chemical Evolution across Cosmic Time
Authors: Paige M. Kelly, Tucker Jones, Yuguang Chen, Ryan L. Sanders, Danielle A. Berg, Peter Senchyna, Fabio Bresolin, Daniel Stark
Figure caption: The ADF(O2+) vs. ADF(C2+) for the nearby H II regions in our sample (teal squares) and three objects from L. Toribio San Cipriano et al. (2017; gray squares). Values for the ADF(O2+) originate from C. Esteban et al. (2014) and L. Toribio San Cipriano et al. (2017). In all cases, the ADF(C2+) and ADF(O2+) are consistent, illustrated by the 1:1 line in black.
Paper: JWST/NIRCam Imaging of the Bipolar Planetary Nebula NGC 6537: The (Infra)red Spider, Revealed
Authors: Joel H. Kastner, Paula Moraga Baez, Bruce Balick, Rodolfo Montez, Caroline Gieser, Mikako Matsuura, Jason Nordhaus, Miguel Santander-Garcia
Figure caption: Top: overlay of 4.05 μm Brα (green), 2.12 μm H2 (blue), and 1.64 μm [Fe II] (red) images of NGC 6537, rotated through 47° in PA (such that the polar axis is horizontal in the image). The inset shows a zoom into the core region, which is saturated in the wide-field rendering. Bottom: schematic of the main structural components of NGC 6537: (1) H2-bounded polar lobes; (2) point-symmetric, [Fe II]-emitting regions along opposing lobe walls; (3) slowly expanding equatorial molecular torus with ionized interior; and (4) bubble-like dust structure detected in PAH emission. The line of sight toward the system (indicated at the upper right of the diagram) is such that both the polar axis and the equatorial torus are viewed at intermediate inclination. See text (Section 4.1).
Paper: JWST/NIRCam Imaging of the Bipolar Planetary Nebula NGC 6537: The (Infra)red Spider, Revealed
Authors: Joel H. Kastner, Paula Moraga Baez, Bruce Balick, Rodolfo Montez, Caroline Gieser, Mikako Matsuura, Jason Nordhaus, Miguel Santander-Garcia
Figure caption: Top and middle panels: wide-field (∼80″ × 40″) and zoomed-in (∼20″ × 10″) color overlays of 4.05 μm Brα (red), 1.64 μm [Fe II] (green), and 2.12 μm H2 (blue) images of NGC 6537. Bottom: the same (∼20″ × 10″) FOV as the middle panel, with the 3.56 μm PAH image replacing Brα in the red channel. Images are displayed in log scale, with min and max intensities as in Figure 1, with further enhancements to highlight emission outside the core regions.
Paper: JWST/NIRCam Imaging of the Bipolar Planetary Nebula NGC 6537: The (Infra)red Spider, Revealed
Authors: Joel H. Kastner, Paula Moraga Baez, Bruce Balick, Rodolfo Montez, Caroline Gieser, Mikako Matsuura, Jason Nordhaus, Miguel Santander-Garcia
Figure caption: Left: overlay of a velocity-integrated ALMA 13CO(1–0) emission-line map (green linear intensity scale, with green contours) on JWST/NIRCam 3.56 μm PAH imaging (logarithmic gray scale). The contours are set to levels of 0.25, 0.5, 1.0, 1.5, 2.0, and 2.5 Jy beam−1 km s−1. Right: intensity-weighted velocity map of ALMA 13CO(1–0) emission, showing blueshifted and redshifted emission (see color bar) on JWST/NIRCam 3.56 μm PAH imaging (gray scale), with contours of velocity-integrated blueshifted (0–9 km s−1) and redshifted (11–20 km s−1) 13CO(1–0) emission overlaid; the contours are set to levels of 0.25, 0.5, 0.75, 1.0, 1.25, and 1.5 Jy beam−1 km s−1.
Paper: JWST/NIRCam Imaging of the Bipolar Planetary Nebula NGC 6537: The (Infra)red Spider, Revealed
Authors: Joel H. Kastner, Paula Moraga Baez, Bruce Balick, Rodolfo Montez, Caroline Gieser, Mikako Matsuura, Jason Nordhaus, Miguel Santander-Garcia
Figure caption: JWST/NIRCam images of NGC 6537, full 150″ × 150″ field of view (FOV). The four image frames are arranged, from left to right and top to bottom, in the order F164N, F212N, F356W, and F405N. The rearward-facing NE and forward-facing SW polar lobes are indicated in the H2 (F212N, upper right) image.
Paper: JWST/NIRCam Imaging of the Bipolar Planetary Nebula NGC 6537: The (Infra)red Spider, Revealed
Authors: Joel H. Kastner, Paula Moraga Baez, Bruce Balick, Rodolfo Montez, Caroline Gieser, Mikako Matsuura, Jason Nordhaus, Miguel Santander-Garcia
Figure caption: Overlay of ALMA 3 mm continuum emission map (red), JWST/NIRCam 4.05 μm Brα image (green), and HST/WFPC2 Hα image (blue) of NGC 6537. The ALMA continuum image is also presented in the black and white inset of the top panel. The annotations in the bottom panel denote features that are especially bright in Hα, Brα, or 3 mm continuum. Features that are bright in Hα or Brα and are likely directed toward and away from the observer, respectively, while the millimeter-wave continuum likely traces ionized material confined to the PN’s equatorial plane region (see Section 3.3.1).
Paper: JWST/NIRCam Imaging of the Bipolar Planetary Nebula NGC 6537: The (Infra)red Spider, Revealed
Authors: Joel H. Kastner, Paula Moraga Baez, Bruce Balick, Rodolfo Montez, Caroline Gieser, Mikako Matsuura, Jason Nordhaus, Miguel Santander-Garcia
Figure caption: JWST/NIRCam images of NGC 6537 arranged as in Figure 1; zoomed-in views, 30″ × 30″ FOV. The position of the central star is indicated in the PAH (F356W, lower left) image.
Paper: JWST/NIRCam Imaging of the Bipolar Planetary Nebula NGC 6537: The (Infra)red Spider, Revealed
Authors: Joel H. Kastner, Paula Moraga Baez, Bruce Balick, Rodolfo Montez, Caroline Gieser, Mikako Matsuura, Jason Nordhaus, Miguel Santander-Garcia
Figure caption: Overlay of 4.05 μm Brα (green), 2.12 μm H2 (blue), and 1.64 μm [Fe II] (red) images of half of the NE-directed polar lobe of NGC 6537, with the lobe “half” flipped along its polar axis (leftmost panel), compared with images illustrating various aspects of the simulation described in Section 4.2.
Paper: Mapping the Spatial Distribution of Fast Radio Bursts within their Host Galaxies
Authors: Alexa C. Gordon, Wen-fai Fong, Adam T. Deller, Lachlan Marnoch, Sungsoon Lim, Eric W. Peng, Keith W. Bannister, Apurba Bera, N. D. R. Bhat, Tyson Dial, Yuxin Dong, 雨欣 董, Tarraneh Eftekhari, Marcin Glowacki, Kelly Gourdji, Vivek Gupta, Joscha N. Jahns-Schindler, Akhil Jaini, Charles D. Kilpatrick, Chang Liu, J. Xavier Prochaska, Stuart D. Ryder, Ryan M. Shannon, Sunil Simha, Nicolas Tejos, Yuanming Wang, Ziteng Wang
Figure caption: Compilation of residual images for our sample of FRB hosts, derived via Galfit surface-brightness profile modeling (Section 4.1), along with the FRB localizations (1σ total uncertainty; magenta ellipses). For clarity, FRBs with milliarcsecond-scale localizations are denoted by magenta stars as the localization is much smaller than the size of the symbol. The images have been scaled to highlight features of interest but span a range of sizes (≈10″−0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩75 across). The images are oriented with north up and east to left, unless otherwise noted. There is broad diversity in the observed morphology of FRB hosts, with all at z ≲ 0.1 showing clear spiral structure.
Paper: Mapping the Spatial Distribution of Fast Radio Bursts within their Host Galaxies
Authors: Alexa C. Gordon, Wen-fai Fong, Adam T. Deller, Lachlan Marnoch, Sungsoon Lim, Eric W. Peng, Keith W. Bannister, Apurba Bera, N. D. R. Bhat, Tyson Dial, Yuxin Dong, 雨欣 董, Tarraneh Eftekhari, Marcin Glowacki, Kelly Gourdji, Vivek Gupta, Joscha N. Jahns-Schindler, Akhil Jaini, Charles D. Kilpatrick, Chang Liu, J. Xavier Prochaska, Stuart D. Ryder, Ryan M. Shannon, Sunil Simha, Nicolas Tejos, Yuanming Wang, Ziteng Wang
Figure caption: The redshift distribution of the FRB host galaxies in our sample, which extends to z ≈ 0.64. We denote the subsample of 20 hosts with clear spiral arms as solid light blue bars. There is a clear drop-off in the detection of spiral structure at z ≳ 0.15, which is likely an effect of the limit of our survey as opposed to an intrinsic effect.
Paper: JWST/NIRCam Imaging of the Bipolar Planetary Nebula NGC 6537: The (Infra)red Spider, Revealed
Authors: Joel H. Kastner, Paula Moraga Baez, Bruce Balick, Rodolfo Montez, Caroline Gieser, Mikako Matsuura, Jason Nordhaus, Miguel Santander-Garcia
Figure caption: JWST/NIRCam images of NGC 6537 arranged as in Figure 1; zoomed-in views, 75″ × 75″ FOV.
Paper: TESS Subgiant and Lower-red-giant Asteroseismology in the Continuous Viewing Zones
Authors: Sophia Grusnis, Jamie Tayar, Diego Godoy-Rivera
Figure caption: [α/M] plotted against [M/H]. Our data is circled in black and color coded by age. We show for comparison (gray) the full sample from the APOGEE DR17 spectroscopic survey in this temperature and metallicity regime. Average error bars are shown in the top-right corner.