adsabs/AstroCLIMB huggingface dataset:
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: (a) The contours show the E-mode (i.e., M ap) maps constructed from the galaxy sample in the range z = 0.4–2.0 overlaid on the light density map of galaxies in the range z = 0.15–0.55. We fixed ﹩{\sigma }_{{M}_{{\rm{ap}}}}=3.5\times {10}^{-4}\pm 1.75\times {10}^{-5}﹩. Contours are drawn at levels of 0.012, 0.024, 0.036, and 0.048. The background is a light density map that was smoothed with a Gaussian width of ﹩0\buildrel{\,\prime}\over{.} 73﹩. Four major filamentary structures connecting the galaxy cluster are visible and are shown in green arrows: one to the north, one to the west (right), and one toward the southwest (down right); another structure to the southeast is also visible. The filaments seen from the contours broadly agrees with the filaments seen in the light density maps. The location clusters obtained from NED are shown as symbols. The squares are obtained from X-ray studies while the stars are obtained from optical data. Cross symbols show cluster locations obtained using the SZ effect on Planck data. Each symbol and the corresponding literature is discussed in detail in Section 6. (b) Contours of κ(θ) overlaid on the light density maps smoothed with a Gaussian of ﹩0\buildrel{\,\prime}\over{.} 73﹩ of galaxies in the range z = 0.15–0.55. Contours have been drawn at levels of 0.1, 0.2, and 0.3. The κ(θ) map has been smoothed with a Gaussian of width 16.″5. The bimodal mass distribution of the central region of A2390 can be clearly seen at R.A. = 21h:53m:36.ˢ8 and decl. = 17°: ﹩41^{\prime} ﹩: 43″. The other peaks are consistent with the mass concentrations shown by E-mode maps. We find also increased noise at the edges of the κ(θ) map.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: (a) The contours of the E-mode (i.e., M ap) maps shown in blue are overlaid on the galaxy light density map. Contours are drawn at 0.012, 0.024, 0.036, and 0.048. The light density maps are made by adding light from galaxies in the range z = 0.15–0.55 weighted by a Gaussian of width ﹩0\buildrel{\,\prime}\over{.} 73﹩. The main peak matches up perfectly. The smaller peak on the lower left is distinctly separate from the E-mode peak. The two peaks of the E-mode map are shown as yellow circles. (b) Same as before except the contours are from the convergence map. Contours are drawn at 0.1, 0.15, 0.25, and 0.3. The two peaks of the convergence map are shown as yellow circles. (c) In color shown is the X-ray image from Chandra with the convergence map contours overlaid. A slight swirl pattern in the X-ray can be seen matching the swirl pattern of the convergence contours. (d) The convergence map is shown as background. Contours show the compact-component-subtracted radio images from LOFAR obtained after careful reanalysis of DR2 data by M. Cianfaglione et al. (2024, in preparation). Contours are drawn at 0.0014, 0.0021, 0.0028, and 0.0035 Jy beam−1, which corresponds to 2, 3, 4, and 5σ significance, respectively.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: These plots show the ability of our pipeline to accurately recover shear at various levels in the weak lensing regime. To make these plots, we give the PhoSim simulations an input shear of γ 1 = 0.1 in the first case and γ 2 = 0.05 for the second case. It is clear both coadd and individual frame measurements accurately recover shear to within 0.005 of the true shear. In the second case, there is a slight bias of approximately 0.005. The error bars shown are just the Poisson component. Clearly, single frames have smaller error bars as expected. However, the error bars fall short because of non-Poisson sources of error. Hence, we elect to use error bars of 0.005 for shear measured using individual image measurements, which is approximately 10 times the Poisson component.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: Enclosed mass as a function of radius from the center of the galaxy cluster. The center is located on the BCG at R.A. = 21h:53m:36.ˢ8 and decl. = 17°:41′: 43″. We used Poisson error bars and multiplied them with a factor of 10, as found in PhoSim simulations, to take into account systematic/non-Poisson errors. We find our data match extremely well with G. Squires et al. (1996) up to a radius of 700 kpc. The mismatch beyond that is likely due to the mass-sheet degeneracy and can be remedied using a small additive constant.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: The contours show the E-mode (i.e., M ap) maps constructed from the galaxy sample in the range z = 0.4–2.0 overlaid on the light density map from galaxies in the redshift range 0.35–0.75. Contours are drawn at levels of 0.012, 0.024, 0.036, and 0.048. We fixed ﹩{\sigma }_{{M}_{{\rm{ap}}}}=3.5\times {10}^{-4}\pm 1.75\times {10}^{-5}﹩. The background is a light density map that was smoothed with a Gaussian width of ﹩0\buildrel{\,\prime}\over{.} 73﹩.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: (a) Histograms for the difference in shape when sources are measured from the i + r coadd vs. when they are measured in individual images of i- and r-band images. The individual image measurements are combined using inverse error as weight. The reduction in size by weighting individual frames optimally is clear from this plot. This leads to enhanced shear signal and hence shear recovery. (b) Histograms for the difference in shape when sources are measured from the weighted i + r coadd vs. when they are measured in individual simulated images of i- and r-band images produced using PhoSim for the first case, i.e., γ 1 = 0.1. The individual image measurements are combined using inverse error as weight. The reduction in size by weighting individual frames optimally is clear from this plot. This leads to enhanced shear signal and hence shear recovery.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: (a) The adaptive E-mode contours from the foreground slice (z = 0.01–0.6) overlaid on an image showing the light density of galaxies in the redshift range z = 0.15–0.55 smoothed with a Gaussian of width ﹩0\buildrel{\,\prime}\over{.} 73﹩. (b) The contours depicted are from the adaptive E-mode maps of the background slice (z = 0.5–2) overlaid on an image showing the light density of galaxies in the redshift range z = 0.35–0.75 similarly smoothed. In both cases contours are placed at levels of 0.02, 0.07, and 0.12. There is significant noise in our maps. The signal from A2390 appears only in the foreground slice as expected.
Paper: Weak Lensing Analysis of A2390 Using Short Exposures
Authors: A. Dutta, J. R. Peterson, T. Rose, M. Cianfaglione, A. Bonafede, G. Li, G. Sembroski
Figure caption: A composite image of A2390. The X-ray obtained using Chandra (S. Allen et al. 2001) is shown in red and our mass map (convergence) in blue. It is overlaid on the RGB color image of A2390 created using a g-band coadd for blue, r-band coadd for green, and i-band coadd for red. Optical images have been obtained using WIYN-ODI. At the center of the image, the bright elliptical galaxy is the BCG. The X-ray shows a swirl-like pattern in the same direction as the DM.
Paper: Origins of Very Low Helium Abundance Streams Detected in the Solar Wind Plasma
Authors: Yogesh, N. Gopalswamy, D. Chakrabarty, Parisa Mostafavi, Seiji Yashiro, Nandita Srivastava, Leon Ofman
Figure caption: A low helium abundance event observed by Wind spacecraft in 2019 December. The red vertical lines show the start and time of the event. The variations of the magnetic field components, speed (proton and alpha), number density (proton and alpha), helium abundance, proton and alpha temperature (T  p , T  a ), and differential speed, are shown in panels (a)–(f). The blue and red horizontal lines in panel (c) represent the average number density of protons and alpha particles over two solar cycles (SCs). Panel (c) shows that the proton density (N  p ) is higher than the average value of Np (6.29) over the two SCs. In panel (c), the scale for proton density is on the left side and alpha density is on the right side. On the contrary, alpha particle densities are lower than the two SC averaged values. There is significantly less speed difference between the alphas and protons (see panel (f)).
Paper: Origins of Very Low Helium Abundance Streams Detected in the Solar Wind Plasma
Authors: Yogesh, N. Gopalswamy, D. Chakrabarty, Parisa Mostafavi, Seiji Yashiro, Nandita Srivastava, Leon Ofman
Figure caption: The low helium abundance event observed by PSP in 2020 January. Similar to Figure 1, the variations in the solar wind parameters are shown in panels (a)–(f). The event time is selected based on the presence of alphas and protons in the field of view of the SPAN-I instrument on board PSP. The vertical lines indicate the duration of the event during which the helium and hydrogen cores were within the field of view of the SPAN-I instrument and A He remained below 1%. The dashed horizontal lines in panels (a), (d), and (f) are B = 0, A He = 1%, and zero differential speed, respectively.
Paper: Origins of Very Low Helium Abundance Streams Detected in the Solar Wind Plasma
Authors: Yogesh, N. Gopalswamy, D. Chakrabarty, Parisa Mostafavi, Seiji Yashiro, Nandita Srivastava, Leon Ofman
Figure caption: ADAPT-WSA model output for CR 2225. The model run is for the Wind (or ACE) event (corresponding to Figure 1). The white (top panel) and red (middle and bottom panels) tick marks or vertical lines represent the back projection of the Wind satellite at 5 R ⊙. The top panel shows a WSA-derived open field at 1 R ⊙ with model-derived solar wind speed in color scale. Black lines indicate the magnetic connectivity between the projection of the observing satellite location at 5 R ⊙ and the solar wind source region at 1 R ⊙. The field polarity at the photosphere is indicated by the light/dark (positive/negative) gray contours in the same top panel. The photospheric field can be seen in the middle panel. This panel’s black lines again show the connectivity between ACE and the photosphere. The bottom panel shows the WSA-derived coronal field at 5 R ⊙. The yellow contour marks the model-derived heliospheric current sheet, where the overall coronal field changes sign.
Paper: Origins of Very Low Helium Abundance Streams Detected in the Solar Wind Plasma
Authors: Yogesh, N. Gopalswamy, D. Chakrabarty, Parisa Mostafavi, Seiji Yashiro, Nandita Srivastava, Leon Ofman
Figure caption: Similar to Figure 3, ADAPT-WSA model output for CR 2226. The model run is for the PSP event (corresponding to Figure 2). The white (top panel) and red (middle and bottom panels) tick marks or vertical lines represent the back projection of the PSP satellite at 5 R ⊙. The top panel shows a WSA-derived open field at 1 R ⊙ with model-derived solar wind speed in color scale. Black lines indicate the magnetic connectivity between the projection of the observing satellite location at 5 R ⊙ and the solar wind source region at 1 R ⊙. The field polarity at the photosphere is indicated by the light/dark (positive/negative) gray contours in the same top panel. The photospheric field can be seen in the middle panel. This panel’s black lines again show the connectivity between the PSP and the photosphere. The bottom panel shows the WSA-derived coronal field at 5 R ⊙. The yellow contour marks the model-derived heliospheric current sheet, where the overall coronal field changes sign.
Paper: Origins of Very Low Helium Abundance Streams Detected in the Solar Wind Plasma
Authors: Yogesh, N. Gopalswamy, D. Chakrabarty, Parisa Mostafavi, Seiji Yashiro, Nandita Srivastava, Leon Ofman
Figure caption: The FFT with Fisher’s false-alarm test (F-level, left panel) and Lomb–Scargle periodogram analysis with red noise and chi-95% significance level (right panel) for the event shown in Figure 1. It can be seen in both panels that the frequency of 0.44 mHz (period  2270 s) shows the highest power.
Paper: Origins of Very Low Helium Abundance Streams Detected in the Solar Wind Plasma
Authors: Yogesh, N. Gopalswamy, D. Chakrabarty, Parisa Mostafavi, Seiji Yashiro, Nandita Srivastava, Leon Ofman
Figure caption: Helium abundance variation with heliographic latitudes. The dashed red circle shows A He = 1%. The black dot shows the start time and the orbit progresses clockwise. The Ulysses first (1992–1998), second (1999–2004), and third (2005–2009) orbit observations are shown. The first and third orbits show low helium abundance events near the equatorial plane, whereas the second orbit shows the events spread over all the heliographic latitudes.
Paper: Origins of Very Low Helium Abundance Streams Detected in the Solar Wind Plasma
Authors: Yogesh, N. Gopalswamy, D. Chakrabarty, Parisa Mostafavi, Seiji Yashiro, Nandita Srivastava, Leon Ofman
Figure caption: The Fe/O vs. A He density distributions from ACE SWICS data in fast wind (>600 km s−1, left) and slow wind (<450 km s−1, right). The red patches show our events’ average A He and Fe/O values.
Paper: Origins of Very Low Helium Abundance Streams Detected in the Solar Wind Plasma
Authors: Yogesh, N. Gopalswamy, D. Chakrabarty, Parisa Mostafavi, Seiji Yashiro, Nandita Srivastava, Leon Ofman
Figure caption: The schematic structure of the streamers. The (ideal) gravitationally settled helium abundance profile is shown. The reduction in helium abundance in the solar wind is attributed to the release of plasma from higher altitudes, e.g., the solar wind coming from h4 will have less A He as compared to wind from h1. The zoomed version is rotated by 90°.
Paper: The Nature of a Recently Discovered Wolf–Rayet Binary: Archetype of Stripping? 
Authors: Philip Massey, Kathryn F. Neugent, Nidia I. Morrell, Desmond John Hillier, Laura R. Penny
Figure caption: Phased photometry. (a) The OGLE I-band photometry is phased with the OGLE ephemeris of T0 = 2457001.142 and P = 2.1590747. Although the data are noisy, they clearly reveal both a primary and secondary eclipse. (b) Phasing the Swope data with the OGLE ephemeris reveals a small phase shift, as evidenced by the eclipses not quite lining up with phases of 0 and 0.5. (c) The data (Swope, black; OGLE, red) have now been phased using our final adopted ephemeris T0 = 2457001.0906 and P = 2.159044 days. The OGLE I-band data have been shifted by −0.205 mag in order to overlay on the Swope V-band data.
Paper: The Nature of a Recently Discovered Wolf–Rayet Binary: Archetype of Stripping? 
Authors: Philip Massey, Kathryn F. Neugent, Nidia I. Morrell, Desmond John Hillier, Laura R. Penny
Figure caption: Spectral energy distribution (SED). The SED of the model is shown in red; the data are shown in blue. The model flux has been reddened using a combination of a Galactic J. A. Cardelli et al. (1989) reddening law with E(B − V) = 0.08 and a I. D. Howarth (1983) LMC reddening law with E(B − V) = 0.055. The data have been corrected to vacuum wavelengths and to the rest frame assuming a 250 km s−1 radial velocity determined by fitting our optical spectral lines. (This radial velocity value is consistent with the LMC’s systemic radial velocity of 262 km s−1; R. P. van der Marel et al. 2002; see also K. F. Neugent et al. 2012.) The top panel shows the excellent match with the UV spectrum. The middle two panels show that the optical spectra display additional flux contribution from the companion star(s). In the bottom panel the model has been scaled by a factor of 1.22 to produce good agreement with the optical. Note that the optical flux below 3600 Å suffers from calibration issues.
Paper: The Nature of a Recently Discovered Wolf–Rayet Binary: Archetype of Stripping? 
Authors: Philip Massey, Kathryn F. Neugent, Nidia I. Morrell, Desmond John Hillier, Laura R. Penny
Figure caption: Comparison between LMCe055-1 and the WN3/O3 star LMC170-2. Note the presence of N IV emission, the distinctive P Cygni profiles of N V λ λ4603, 19, and the presence of weak He I λ4471 absorption in LMCe055-1. Also note that the even-N Pickering lines of He II, coincident with the Balmer hydrogen lines, are stronger with respect to the odd-N Pickering lines in LMCe055-1, implying a smaller He/H ratio than found in the WN3/O3s.
Paper: The Nature of a Recently Discovered Wolf–Rayet Binary: Archetype of Stripping? 
Authors: Philip Massey, Kathryn F. Neugent, Nidia I. Morrell, Desmond John Hillier, Laura R. Penny
Figure caption: Model fit in the UV. The best-fitting CMFGEN model is shown in red, and the G140L/800 COS observation in blue. The lines used in the fitting are labeled. The model spectrum has been convolved to a spectral resolution of 0.55 Å in order to match the data, and further broadened by a rotation component of 100 km s−1.
Paper: The Nature of a Recently Discovered Wolf–Rayet Binary: Archetype of Stripping? 
Authors: Philip Massey, Kathryn F. Neugent, Nidia I. Morrell, Desmond John Hillier, Laura R. Penny
Figure caption: Phase coverage for each of the five imaging runs. Note that primary eclipse occurs at a phase of 0 and secondary eclipse at a phase of 0.5. In each case the eclipse extends roughly ±0.05 in phase, as shown by the red lines. For clarity, the coverage near primary eclipse is shown at a phase of both 0 and 1. Despite the large amount of data and the relatively short period, there is still a small gap in phase coverage around a phase of 0.4.
Paper: The Nature of a Recently Discovered Wolf–Rayet Binary: Archetype of Stripping? 
Authors: Philip Massey, Kathryn F. Neugent, Nidia I. Morrell, Desmond John Hillier, Laura R. Penny
Figure caption: The radial velocities of the He I λ4471 component. The radial velocities of the He I λ4471 component (averaged of the two methods given in Table 5) are shown as a function of the eclipse phase, with phase 0 being the primary eclipse. If the system consisted of the WR star as the primary and the He I λ4471 component as the secondary, then we would expect the latter to have the largest velocities at a phase of 0.25 as it moved away from us after passing in front of the hotter WR star. Instead, the opposite is seen, suggesting that He I λ4471 arises in the hotter primary of the 2.2 days pair, with an otherwise undetected third component. The error bars have been set to ±30 km s−1, a rough estimate of our measuring uncertainty. The solid black line shows the best-fit radial velocity curve with γ fixed to 250 km s−1, our preferred solution.
Paper: Confirming the Tidal Tails of the Young Open Cluster Blanco 1 with TESS Rotation Periods
Authors: Lizhou Sha, Andrew M. Vanderburg, Luke G. Bouma, Chelsea X. Huang
Figure caption: A table summarizing the degree to which eight literature references are in agreement over Blanco 1 candidates. Each row and column represent one of eight references that contain membership lists for Blanco 1 compiled using Gaia DR2 or (E)DR3 data. The number in each cell is the number of candidates shared by that row’s and column’s references. The color in each cell indicate the fraction of common candidates with respect to the total number identified by each column’s reference. References: G18: Gaia Collaboration et al. (2018a); CG18: T. Cantat-Gaudin et al. (2018); Z20: Y. Zhang et al. (2020); M21: S. Meingast et al. (2021); P21: X. Pang et al. (2021); T22: Y. Tarricq et al. (2022); H22: Z. He et al. (2022); and A23: J. Alfonso & A. García-Varela (2023).
Paper: The Nature of a Recently Discovered Wolf–Rayet Binary: Archetype of Stripping? 
Authors: Philip Massey, Kathryn F. Neugent, Nidia I. Morrell, Desmond John Hillier, Laura R. Penny
Figure caption: Model fit in the optical for selected spectral lines. The normalized best-fitting CMFGEN model is shown in red, and the normalized MagE spectrum is shown in blue. The solid blue line represents the spectrum after the contribution of the B star has been removed; the dashed blue line shows the MagE data before this correction. The model spectrum has been convolved to a resolving power of 4100 and broadened by a rotation component of 100 km s−1.
Paper: The Nature of a Recently Discovered Wolf–Rayet Binary: Archetype of Stripping? 
Authors: Philip Massey, Kathryn F. Neugent, Nidia I. Morrell, Desmond John Hillier, Laura R. Penny
Figure caption: Masses for the secondary in the 35 days WR binary. Using the mass function from Solution A (Table 8), we have plotted the mass M  c  of the companion of the WR star as a function of the WR star’s mass and orbital inclination. The two solid vertical lines denote our expected masses for the WR star. Thus, for the companion to match the masses of the 2.2 days pair, 5.8–7.7 M ⊙, would require an orbital inclination of <20°.
Paper: The Nature of a Recently Discovered Wolf–Rayet Binary: Archetype of Stripping? 
Authors: Philip Massey, Kathryn F. Neugent, Nidia I. Morrell, Desmond John Hillier, Laura R. Penny
Figure caption: Masses for the undetected secondary in the 2.2 days binary. The mass (M  s ) of the secondary is shown as a function of the mass (M  p ) of the primary, the star that is showing He I λ4471. Given the spectral type of the primary is ≈B7 V, we expect its mass to be 3–4 M ⊙. Thus, the mass of the secondary is likely to be 1.7–2 M ⊙, which corresponds to a mid-A through early F-type dwarf.
Paper: The Nature of a Recently Discovered Wolf–Rayet Binary: Archetype of Stripping? 
Authors: Philip Massey, Kathryn F. Neugent, Nidia I. Morrell, Desmond John Hillier, Laura R. Penny
Figure caption: Composite He I λ4471 line. By shifting the spectra by the radial velocities to a rest frame, and combining them with a sigma-clipping algorithm, we recover the weak He I λ4471 line. Even the neighboring Mg II λ4481 is seen. Its strength, relative to the He I lines, leads to a B7 V classification.
Paper: The Nature of a Recently Discovered Wolf–Rayet Binary: Archetype of Stripping? 
Authors: Philip Massey, Kathryn F. Neugent, Nidia I. Morrell, Desmond John Hillier, Laura R. Penny
Figure caption: Corrected light curve of the 2.2 days period binary. Here we show the light curve after subtracting off the expected flux contribution of the WR component, along with our best-fit GENSYN model (red).
Paper: The Nature of a Recently Discovered Wolf–Rayet Binary: Archetype of Stripping? 
Authors: Philip Massey, Kathryn F. Neugent, Nidia I. Morrell, Desmond John Hillier, Laura R. Penny
Figure caption: Two possible orbit solutions for the WR component. The parameters are given in Table 8.
Paper: Confirming the Tidal Tails of the Young Open Cluster Blanco 1 with TESS Rotation Periods
Authors: Lizhou Sha, Andrew M. Vanderburg, Luke G. Bouma, Chelsea X. Huang
Figure caption: Left: proper motion of Blanco 1 member candidates, converted into physical units using the corrected distances by X. Pang et al. (2021). The circular orange marks are the stars in the cluster core, and the square magenta marks are those in the tidal tails. Right: exclusion in proper motion space for the comparison sample. The orange marks are Blanco 1 candidates, and the gray marks are field stars satisfying the first three criteria outlined in Section 2.4 (i.e., before the exclusion in proper motion space). The triangular purple marks are stars in the selected comparison sample. A box of ±2.5 mas yr −1 in μ  α  and ±5 mas yr −1 in μ  δ  (shown in dashed gray lines) centered at (μ  α , μ  δ ) ≈ (18.71, 2.61) mas (indicated by solid thin gray lines) is drawn to exclude potentially unidentified members of the Blanco 1 cluster from contaminating the sample.