adsabs/AstroCLIMB huggingface dataset:
Paper: 3D MC. II. X-Ray Echoes Reveal a Clumpy Molecular Cloud in the CMZ
Authors: Danya Alboslani, Cara Battersby, Samantha W. Brunker, Maïca Clavel, Dani Lipman, Daniel L. Walker
Figure caption: We investigate possible X-ray smoothing kernels and contour levels in order to select the ones that best represented the overall structure seen in X-rays. This figure shows X-ray data of the Stone (left) MCs collected in 2010. Shown from top to bottom are increasing numbers of kernels used for smoothing. From left to right, increasing flux levels of contours are drawn. In this work we use the middle right and bottom left panels (Contours A and B, respectively) to show the overall structure and the densest parts of the Stone MC.
Paper: 3D MC. II. X-Ray Echoes Reveal a Clumpy Molecular Cloud in the CMZ
Authors: Danya Alboslani, Cara Battersby, Samantha W. Brunker, Maïca Clavel, Dani Lipman, Daniel L. Walker
Figure caption: X-ray data collected from 2008 to 2017 show the most significant 6.4 keV emission in the vicinity of the cloud. The X-ray emission is plotted in gray scale, smoothed with a Gaussian kernel of 4, with rms values for each year in the lower left corner. Overplotted are Contours A in thick lines and Contours B in thin lines.
Paper: 3D MC. II. X-Ray Echoes Reveal a Clumpy Molecular Cloud in the CMZ
Authors: Danya Alboslani, Cara Battersby, Samantha W. Brunker, Maïca Clavel, Dani Lipman, Daniel L. Walker
Figure caption: Assuming that the peak in X-ray emission correlates linearly with the peak of submillimeter continuum data from C. Battersby et al. (2020), we produce localized densities for each slice of the Stone MC. Contours are drawn at 3 × 10−9 ﹩{\mathrm{photons}\,\mathrm{cm}}^{-2}\,{{\rm{s}}}^{-1}\,{\mathrm{arcsec}}^{-2}﹩ from data smoothed with a kernel of 4.
Paper: 3D MC. II. X-Ray Echoes Reveal a Clumpy Molecular Cloud in the CMZ
Authors: Danya Alboslani, Cara Battersby, Samantha W. Brunker, Maïca Clavel, Dani Lipman, Daniel L. Walker
Figure caption: Using Equation (1) and assuming an X-ray flare event ∼140.6 yr ago (See Section 3.1) where dlos = 17 pc, we are able to create a 3D model of the Stone MC with Contours A. Structures that were less than 15″ wide were omitted from the plot to omit background fluctuations.
Paper: 3D MC. II. X-Ray Echoes Reveal a Clumpy Molecular Cloud in the CMZ
Authors: Danya Alboslani, Cara Battersby, Samantha W. Brunker, Maïca Clavel, Dani Lipman, Daniel L. Walker
Figure caption: Spectral lines integrated reveal the 2D shape of the Stone MC from our line of sight. The spectral lines used were H2CO 3(0,3)–2(0,2), H2CO 3(2,2)–2(2,1), and SiO (5–4), plotted in blue, green, and red, respectively.
Paper: Multiple Populations of the Large Magellanic Cloud Globular Cluster NGC 2257: No Major Environmental Effect on the Formation of Multiple Populations of Old Globular Clusters in the Large Magellanic Cloud
Authors: Jae-Woo Lee, Tae-Hyeong Kim, Hak-Sub Kim, Hyun-Il Sung, Hwihyun Kim, Francesco Di Mille
Figure caption: CMDs of NGC 2257 for the clean stars. The red error bars indicate the measurement uncertainties at a given V magnitude.
Paper: Multiple Populations of the Large Magellanic Cloud Globular Cluster NGC 2257: No Major Environmental Effect on the Formation of Multiple Populations of Old Globular Clusters in the Large Magellanic Cloud
Authors: Jae-Woo Lee, Tae-Hyeong Kim, Hak-Sub Kim, Hyun-Il Sung, Hwihyun Kim, Francesco Di Mille
Figure caption: (a) Comparison of M55 and the model isochrone for [Fe/H] = −1.8 dex and 13.0 Gyr. The distance modulus of (m − M) = 13.80 mag and the interstellar reddening value of E(B − V) = 0.12 mag are used. (b) Comparison of NGC 2257 and the model isochrone for [Fe/H] =  −1.8 dex and 11.8 Gyr. The distance modulus of (m − M)0  = 18.38 mag and the interstellar reddening value of E(B − V) = 0.04 mag are used.
Paper: Multiple Populations of the Large Magellanic Cloud Globular Cluster NGC 2257: No Major Environmental Effect on the Formation of Multiple Populations of Old Globular Clusters in the Large Magellanic Cloud
Authors: Jae-Woo Lee, Tae-Hyeong Kim, Hak-Sub Kim, Hyun-Il Sung, Hwihyun Kim, Francesco Di Mille
Figure caption: CMDs of NGC 2257 with −2.0 mag ≤V − VHB ≤ 1.5 mag. The blue and red squares denote the FG and SG RGB stars, respectively, returned from our EM estimator discussed below.
Paper: Multiple Populations of the Large Magellanic Cloud Globular Cluster NGC 2257: No Major Environmental Effect on the Formation of Multiple Populations of Old Globular Clusters in the Large Magellanic Cloud
Authors: Jae-Woo Lee, Tae-Hyeong Kim, Hak-Sub Kim, Hyun-Il Sung, Hwihyun Kim, Francesco Di Mille
Figure caption: Comparison of NGC 2257 (black squares) and M55 (orange squares). The V magnitude and (b − y) color of individual M55 stars are increased by ΔV  = 4.524 and Δ(b − y) = 0.066 mag, respectively.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Architectures of multiplanet systems (including two-planet systems) that have planet pairs with strongly inverted mass ratios, ordered by the period of the innermost planet in each class. We define these systems as warm-Jupiter systems with a non-Jupiter exterior to a Jupiter (top) or peas-in-a-pod systems with a pair of adjacent planets with an outer–inner mass ratio of <1/7 (bottom). All such planets under our definition are inner planets, because no non-Jovian outer planets appear in our data set.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Architectures of planetary systems (of any multiplicity) that contain super-puffs (circled), ordered by period of the innermost planet. We define super-puffs as <0.3 g cm−3 and <30M⊕. All super-puffs are classified as “Neptunes” in our analysis, regardless of other properties.
Paper: Architecture Classification for Extrasolar Planetary Systems
Authors: Alex R. Howe, Juliette C. Becker, Christopher C. Stark, Fred C. Adams
Figure caption: Architectures of N ≥ 3 systems with one or more detected Jupiter (of any period), ordered by period of the first Jupiter in the system and colored by discovery method. RV discoveries (orange) and transit discoveries (purple) are distinguished from all other detection methods (green). Planets in the same system may or may not have the same discovery method.
Paper: Beam Measurements of Full Stokes Parameters for the FAST L-band 19-beam Receiver
Authors: Xunzhou Chen, Tao-Chung Ching, Di Li, Carl Heiles, Timothy Robishaw, Xuan Du, Marko Krco, Peng Jiang, Qingliang Yang, Jiguang Lu
Figure caption: Left: Combined response of the FAST 19-beam receiver for Stokes Q toward J1407+2827. Black contours represent Q/Ipeak at 2%, 4%, and 6%, respectively, while red dashed contours represent Q/Ipeak at −2%, −4%, and −6%, respectively. Right: Simulated Stokes Q patterns for the combined beam. The cross marks represent the 19 beam centers.
Paper: Beam Measurements of Full Stokes Parameters for the FAST L-band 19-beam Receiver
Authors: Xunzhou Chen, Tao-Chung Ching, Di Li, Carl Heiles, Timothy Robishaw, Xuan Du, Marko Krco, Peng Jiang, Qingliang Yang, Jiguang Lu
Figure caption: Similar to Figure 18, but for Stokes U. Black contours represent U/Ipeak at 0.2%, 0.4%, and 0.6%, respectively, while red dashed contours represent U/Ipeak at −0.2%, −0.4%, and −0.6%, respectively.