adsabs/AstroCLIMB huggingface dataset:
Paper: The Simons Observatory: Design, Integration, and Testing of the Small Aperture Telescopes
Authors: Nicholas Galitzki, Tran Tsan, Jake Spisak, Michael Randall, Max Silva-Feaver, Joseph Seibert, Jacob Lashner, Shunsuke Adachi, Sean M. Adkins, Thomas Alford, Kam Arnold, Peter C. Ashton, Jason E. Austermann, Carlo Baccigalupi, Andrew Bazarko, James A. Beall, Sanah Bhimani, Bryce Bixler, Gabriele Coppi, Lance Corbett, Kevin D. Crowley, Kevin T. Crowley, Samuel Day-Weiss, Mark J. Devlin, Simon Dicker, Brooke DiGia, Peter N. Dow, Cody J. Duell, Shannon M. Duff, Remington G. Gerras, John C. Groh, Jon E. Gudmundsson, Kathleen Harrington, Masaya Hasegawa, Erin Healy, Shawn W. Henderson, Johannes Hubmayr, Jeffrey Iuliano, Bradley R. Johnson, Brian Keating, Ben Keller, Kenji Kiuchi, Anna M. Kofman, Brian J. Koopman, Akito Kusaka, Adrian T. Lee, Richard A. Lew, Lawrence T. Lin, Michael J. Link, Tammy J. Lucas, Marius Lungu, Aashrita Mangu, Jeffrey J McMahon, Amber D. Miller, Jenna E. Moore, Magdy Morshed, Hironobu Nakata, Federico Nati, Laura B. Newburgh, David V. Nguyen, Michael D. Niemack, Lyman A. Page, Kana Sakaguri, Yuki Sakurai, Mayuri Sathyanarayana Rao, Lauren J. Saunders, Jordan E. Shroyer, Junna Sugiyama, Osamu Tajima, Atsuto Takeuchi, Refilwe Tanah Bua, Grant Teply, Tomoki Terasaki, Joel N. Ullom, Jeffrey L. Van Lanen, Eve M. Vavagiakis, Michael R Vissers, Liam Walters, Yuhan Wang, Zhilei Xu, Kyohei Yamada, Kaiwen Zheng
Figure caption: Component level diagram for the Buttkicker setup used to conduct vibrational testing on SAT-MF1.
Paper: Equations of State, Thermodynamics, and Miscibility Curves for Jovian Planet and Giant Exoplanet Evolutionary Models
Authors: Roberto Tejada Arevalo, Yubo Su, Ankan Sur, Adam Burrows
Figure caption: Top: miscibility curves from W. Lorenzen et al. (2009, 2011), M. A. Morales et al. (2013), M. Schöttler & R. Redmer (2018), and the parameterization of Pfaffenzeller. et al (1995) done by J. J. Fortney & W. B. Hubbard (2003) at constant helium abundance (Y = 0.272). The dashed lines denote the temperature shifts predicted by various authors as indicated in the plot: N. Nettelmann et al. (2015) and C. R. Mankovich & J. J. Fortney (2020). The demixing temperatures of all the simulations differ from the experimental results of S. Brygoo et al. (2021), C. Mankovich et al. (2016), and R. Pustow et al. (2016) by more than 1σ. Included is also the (minus) 1σ error line for the S. Brygoo et al. (2021) data in dashed red. The experiments of S. Brygoo et al. (2021) were performed at Y = 0.33. A simpler, though similar, version of this plot is presented in Figure 3 of A. Sur et al. (2024). Bottom: the SR18 curve remains at Y = 0.272, and EOS adiabats are plotted for a range of entropy values in units of k  b  baryon−1. Once the profiles intercept the miscibility curve, the pressure regions highlighted in red will experience H–He phase separation. As entropy decreases, the miscibility gap expands to cover a wider pressure region. The SCvH95 EOS trails the CMS19+HG23 EOS and reaches the immiscibility curve at significantly colder temperatures.
Paper: Equations of State, Thermodynamics, and Miscibility Curves for Jovian Planet and Giant Exoplanet Evolutionary Models
Authors: Roberto Tejada Arevalo, Yubo Su, Ankan Sur, Adam Burrows
Figure caption: Comparison of the H–He EOSs discussed in this study. Top: variant of Figure 2 of A. Sur et al. (2024), originally inspired by Figure 4 of S. Howard & T. Guillot (2023) with corresponding labels for Y = 0.245 and S = 6.21 k  b  baryon−1 and with a comparison to profiles at two epochs of an evolutionary model. Solid lines indicate EOSs calculated with nonideal interaction terms. The dotted blue line highlights the classical SCvH95 EOS, and the green dashed line highlights the original EOS of CMS19, which relies on idealized mixing. Here we include an adiabatic 1M J model with only H–He in the envelope, containing 10 M ⊕ in a compact core. This model was calculated using APPLE (A. Sur et al. 2024) and is shown at different ages, 0.5 and 5 Gyr, for reference. These profiles were calculated using the CD21 H–He EOS (red line). Bottom: adiabatic profiles at different entropy values in k  b  baryon−1 units. We replicate the behavior shown in Figure 10 of B. Militzer & W. B. Hubbard (2013); at modest pressures of ∼1 Mbar, the nonideal effects cause the EOSs to deviate from SCvH95. The region where the SCvH95 deviates significantly is the same region where hydrogen and helium are expected to demix. The H–He 1M J profiles shown in the top panel are also marked in the bottom panel for reference.
Paper: Equations of State, Thermodynamics, and Miscibility Curves for Jovian Planet and Giant Exoplanet Evolutionary Models
Authors: Roberto Tejada Arevalo, Yubo Su, Ankan Sur, Adam Burrows
Figure caption: H–He miscibility curves for various helium fractions with SCvH95 and CMS19+HG23 adiabats at S = 6.1 k  b  baryon−1 and at a constant Y = 0.272. The profiles would experience H–He demixing when they intercept the Y = 0.272 curve, which is highlighted as the dashed green line. The top panel shows curves of constant helium abundance for the L0911 data, and the bottom panels shows those for the SR18 data. The SR18                      Y = 0.272 curve is too cold for any of the adiabats to cross it. The L0911 Y = 0.272 is hot enough to allow each adiabat a miscibility region. We note both that L0911 calculated the demixing temperatures down to 1 Mbar and that SR18 calculated their demixing temperatures down to 0.5 Mbar. As such, the demixing temperatures below these limits shown here are extrapolations for demonstration purposes. Low-pressure (<1.0 Mbar for L0911 and <0.5 Mbar for SR18) demixing temperature extrapolations should not be applied to evolutionary calculations.
Paper: Equations of State, Thermodynamics, and Miscibility Curves for Jovian Planet and Giant Exoplanet Evolutionary Models
Authors: Roberto Tejada Arevalo, Yubo Su, Ankan Sur, Adam Burrows
Figure caption: Pressures that enclose the miscibility gap for the L0911 (left column) and SR18 (right column) H–He immiscibility diagrams with the SCvH95 (top row) and CMS19+HG23 (bottom row) EOSs. This figure shows the low and high pressures, marked by solid lines and dashed lines, respectively, where the gap between solid and dashed lines represents the miscibility gaps as a function of entropy and helium mass fraction. These high and low pressures are the inner and outer ends of the red lines under the miscibility curve shown in the bottom panel of Figure 4. The low-pressure values are weak functions of helium mass fraction, a behavior also shown in Figure 3. Lower entropies are needed to initiate the immiscibility of H–He at higher helium fractions. Differences in the entropy range are due to the L0911 miscibility curves being hotter than the SR18 curves, allowing immiscibility at higher entropies.
Paper: Equations of State, Thermodynamics, and Miscibility Curves for Jovian Planet and Giant Exoplanet Evolutionary Models
Authors: Roberto Tejada Arevalo, Yubo Su, Ankan Sur, Adam Burrows
Figure caption: Differences in demixing temperature calculations as a function of helium abundance. Left: SR18, using van der Waals exchange-correlation functional including nonideal effects on the entropy. Right: L0911, using the PBE exchange-correlation functional and the linear mixing rule. Using the van der Waals functional and including the nonideal effects for the entropy leads to colder demixing temperatures, particularly at low pressures. The regions under each curve are immiscibility regions of hydrogen and helium. These authors calculated such curves for constant pressures, all of which are highlighted by color here, in Mbar.
Paper: An Imaging and Spectroscopic Exploration of the Dusty Compact Obscured Nucleus Galaxy Zw 049.057 
Authors: J. S. Gallagher, R. Kotulla, L. Laufman, E. Geist, S. Aalto, N. Falstad, S. König, J. Krause, G. C. Privon, C. Wethers, A. Evans, M. Gorski
Figure caption: Upper panel: our approach in analyzing the properties of Zw 049.057. The images from left to right are from NOIRlab Legacy Survey’s Sky Viewer (www.legacysurvey.org), our HST optical images, and a high-pass smoothed version of our F125W HST J-band image. The arrows in the left panel point to the southeasterly locations of the Zw 049.057 low-luminosity companions. Dust Pillars-1 and -2 make up the distinctive dust “V.” The central image also shows the polar dust ring band crossing to the north of the central region. Our approach in this paper is to work from larger to smaller spatial scales, starting with the environment and global properties of Zw 049.057 and ending with characteristics of the nuclear region. The location of the CON is denoted by the red circle. Lower panel: the images in three filters illustrate effects of the decrease in optical depth with increasing wavelength. Diffuse dust complexes obscure much of the center of the galaxy in the HST F336W U HST filter but are largely transparent in the F814W I HST filter.
Paper: An Imaging and Spectroscopic Exploration of the Dusty Compact Obscured Nucleus Galaxy Zw 049.057 
Authors: J. S. Gallagher, R. Kotulla, L. Laufman, E. Geist, S. Aalto, N. Falstad, S. König, J. Krause, G. C. Privon, C. Wethers, A. Evans, M. Gorski
Figure caption: Top panel: large-scale dust absorption structures in Zw 049.057 are shown in our HST WFC3/UVIS F555W and smoothed, background subtracted (σ) images in the F125W filter. Major features are marked; see the text for details. The pair of dust pillars that make up the Zw 0049.057 dust “V” are present in our HST F125W image and at longer wavelengths, as shown by Scoville et al. (2000). Pillar-1 stands out in the F125W image, which is consistent with its inferred high optical depth. Pillar-2 to the south is narrower and less pronounced. The asymmetric “blue streak” arm is labeled. Bottom-left panel: the distribution of the observed color (V − I)STMAG = m(F555W)ST − m(814W)ST shows the central reddening due to the polar ring and extraplanar interstellar matter. Deeper inner dust obscuration is associated with the pillars and outflows on the west side of the galaxy. The outer contour defines the “central region” in Section 4.3 where we measured the average diffuse dust absorption. The inner contour outlines the more heavily obscured region that was replaced by the surroundings for the diffuse region opacity measurement. The color map is at the original pixel scale smoothed by a. σ = 1 pixel Gaussian. The circle shows an example of a disk region color measurement of (V − I)STMAG = −0.16 ± 0.07, while the deepest absorption around the nucleus has a color of (V − I)STMAG =  0.9. Bottom-right panel: the ratio of the F555W to F125W images in the observed e−1 s−1 matched to the point-spread function of the F125W data and smoothed with a σ = 1 pixel Gaussian to show regions with a range in optical dust optical depths. Major feature are labeled. The arrow has a length of 3.″5 in both images. A background galaxy is located below the arrow.
Paper: An Imaging and Spectroscopic Exploration of the Dusty Compact Obscured Nucleus Galaxy Zw 049.057 
Authors: J. S. Gallagher, R. Kotulla, L. Laufman, E. Geist, S. Aalto, N. Falstad, S. König, J. Krause, G. C. Privon, C. Wethers, A. Evans, M. Gorski
Figure caption: Upper-left panel: the Zw 049.057 F555W image divided by its mirror image along the major axis to distinguish the discreet dust absorption features. Upper-right panel: map of the regions of interest. Pillar-1 is the top grouping, Pillar-2 is in the middle, and Cloud-3 is at the bottom of the image. The boxes labeled with letters define the regions where photometric results are listed in Table 3. Lower-center panel: schematic model of an idealized pillar embedded in a galaxy with constant stellar volume emissivity. Here, f denotes the fraction of the normalized length of the “galaxy” (i.e., f = 1 refers to the entire column through the galaxy) to where the uniform opacity cloud is located. This basic embedded cloud model assumes that the width of the dust cloud is small compared to the length of the stellar region. A dark cloud at the surface would be at f = 0, and the diagram shows a dark cloud at f = 1/2.
Paper: An Imaging and Spectroscopic Exploration of the Dusty Compact Obscured Nucleus Galaxy Zw 049.057 
Authors: J. S. Gallagher, R. Kotulla, L. Laufman, E. Geist, S. Aalto, N. Falstad, S. König, J. Krause, G. C. Privon, C. Wethers, A. Evans, M. Gorski
Figure caption: Results are shown from our isophotal analysis. Left panel: radial intensity plots are shown from ellipse fits to the HST images. The less-obscured outer disk regions show an exponential profile with a scale length of 2.″2 640 pc). The effects of dust obscuration result in all of the profiles overshooting the observed intensities within R ≲ 2 kpc. The flatter intensity gradient at 6 kpc occurs in the region where the round outer light distribution begins to appear (see Section 3.2). Right: our WFC3 F125W image scaled to show the inclines inner disk of Zw 049.057 with a major axis position angle of 200° and nearly circular outer structure. The outermost isophotes are at μ F125W,AB ≃19 mag arcsec−2. We suggest that this feature is due to the presence of a warped outer disk associated with the interaction that produced the northern polar dust lane. The inner isophotes display the observed b/a = 0.4 axis ratio that we used to derive the inclination.
Paper: An Imaging and Spectroscopic Exploration of the Dusty Compact Obscured Nucleus Galaxy Zw 049.057 
Authors: J. S. Gallagher, R. Kotulla, L. Laufman, E. Geist, S. Aalto, N. Falstad, S. König, J. Krause, G. C. Privon, C. Wethers, A. Evans, M. Gorski
Figure caption: The central region of Zw 049.057 is shown in a full-resolution (V − I)STMAG image with north and east to the left. The location of Pillar-1 is marked by a cyan rectangle. Only the north edge of Pillar-1 is delimited by reddening, while the clumpy Pillar-2 can be traced by its red colors. The color at the location of the Pillar-1 spine is close to that of the surroundings, indicating a high optical depth that limits the transmission of reddened light. The “blue streak” arm is also evident, with the bright northern knot at its head. The 0.″15 circle shows the location of the CON as determined by radio continuum observations.
Paper: An Imaging and Spectroscopic Exploration of the Dusty Compact Obscured Nucleus Galaxy Zw 049.057 
Authors: J. S. Gallagher, R. Kotulla, L. Laufman, E. Geist, S. Aalto, N. Falstad, S. König, J. Krause, G. C. Privon, C. Wethers, A. Evans, M. Gorski
Figure caption: The location of the nucleus is shown with a circle with a radius of 0.″1 on the F814W image of Zw0 49.057. Dust Pillar-1 shows the high-opacity dust spine on its southern edge. Pillar-1 is perpendicular to the bright arc that appears to be in front of the nucleus. This luminous arc is titled with respect to the disk plane of Zw 049.057. Dust Pillars-1 and -2 would be projected to meet ≈1″ east–southeast of the nucleus.The central disk contains a long, spiral arm–like feature (the blue streak in color maps) that extends from the nucleus in the north to the south–southwest. Knots along the arm are star-forming sites, some of which are visible in our F336W image. The compass arms have lengths of 1” each.
Paper: An Imaging and Spectroscopic Exploration of the Dusty Compact Obscured Nucleus Galaxy Zw 049.057 
Authors: J. S. Gallagher, R. Kotulla, L. Laufman, E. Geist, S. Aalto, N. Falstad, S. König, J. Krause, G. C. Privon, C. Wethers, A. Evans, M. Gorski
Figure caption: Illustrations of major axis spectra obtained with RSS on SALT. The upper panel shows the linear Na D absorption lines and weak He I λ 5876 Å emission that is inclined due to rotation. Faint stellar absorption lines showing pronounced rotation can be seen blueward of the Na D lines. The spectrum covers a 35″ region along the slit. We plan a full study of the stellar kinematics of Zw 049.057 using integral field spectra from MUSE (C. Wethers et al. 2024, in preparation). The lower panel shows the strong nebular lines from [N II], Hα, and [S II]. These features show rotation in the same sense as stellar absorption Hα lines in the outer disk. Diffuse [N II] emission is visible beyond the central star-forming disk. The spatial width of the lower spectrum also is 35″.
Paper: An Imaging and Spectroscopic Exploration of the Dusty Compact Obscured Nucleus Galaxy Zw 049.057 
Authors: J. S. Gallagher, R. Kotulla, L. Laufman, E. Geist, S. Aalto, N. Falstad, S. König, J. Krause, G. C. Privon, C. Wethers, A. Evans, M. Gorski
Figure caption: The SALT/RSS spectrum along the major axis of Zw 049.057 shows the presence of three main components of the system: the inner high-SFR disk, Hα absorption from the main disk, and diffuse emission at R ≳ 3″ from gas near the systemic velocity. Red and blue wings of the [N II] λ 6583 Å line at locations away from the center are due to the superposition of extended faint emission located at the systemic velocity of Zw 049.057. The CON is located within the obscured nuclear region at a scale well below the angular resolution of the spectra.
Paper: CMBFSCNN: Cosmic Microwave Background Polarization Foreground Subtraction with a Convolutional Neural Network
Authors: Ye-Peng Yan, Si-Yu Li, Guo-Jian Wang, Zirui Zhang, Jun-Qing Xia
Figure caption: Recovered EE and lensing B-model power spectra for the partial-sky observation data with the performance of CMB-S4 experiment. The two upper panels present the EE and BB power spectra from the recovered noisy CMB maps. The two lower panels show the final EE and BB power spectra, after the denoising procedure. Additionally, the deviations between the recovered power spectra and the input fiducial power spectra are also illustrated. The length of each ℓ bin is set to be 5 for the EE power spectrum and 20 for the BB power spectrum here. We choose the logarithm scales for ℓ within the angle scale range of ℓ ≤ 250, and the linear scales within the angle scale range of ℓ > 250.
Paper: CMBFSCNN: Cosmic Microwave Background Polarization Foreground Subtraction with a Convolutional Neural Network
Authors: Ye-Peng Yan, Si-Yu Li, Guo-Jian Wang, Zirui Zhang, Jun-Qing Xia
Figure caption: The recovered noisy CMB polarization maps for the partial-sky observation data with the performance of the CMB-S4 experiment. The upper panels depict the recovery of the Q map, while the lower panels display the recovery of the U map. The simulated maps utilized in this analysis comprise the beam-convolved CMB map, plus a noise map at a frequency of 220 GHz. The recovered maps correspond to the noisy CMB maps reconstructed using the CMBFSCNN algorithm.
Paper: CMBFSCNN: Cosmic Microwave Background Polarization Foreground Subtraction with a Convolutional Neural Network
Authors: Ye-Peng Yan, Si-Yu Li, Guo-Jian Wang, Zirui Zhang, Jun-Qing Xia
Figure caption: The recovery of EE and lensing B-model power spectra for full-sky observation data with the performance of the LiteBIRD experiment. The two upper panels show the CMB EE and lensing BB power spectra of the recovered noisy CMB maps. The two lower panels show the final EE and BB power spectra, after the denoising step. Additionally, the deviations between the recovered power spectra and the input fiducial power spectra are also presented.
Paper: CMBFSCNN: Cosmic Microwave Background Polarization Foreground Subtraction with a Convolutional Neural Network
Authors: Ye-Peng Yan, Si-Yu Li, Guo-Jian Wang, Zirui Zhang, Jun-Qing Xia
Figure caption: The recovered noisy CMB polarization maps for full-sky observation data with the performance of the LiteBIRD experiment. The upper panels depict the recovery of the Q map, while the lower panels display the recovery of the U map. The simulated CMB maps utilized in this analysis comprise the beam-convolved CMB map plus an ILC noise map. The recovered CMB maps correspond to the noisy CMB maps reconstructed using the CMBFSCNN algorithm. Additionally, the corresponding residual maps are also represented.
Paper: CMBFSCNN: Cosmic Microwave Background Polarization Foreground Subtraction with a Convolutional Neural Network
Authors: Ye-Peng Yan, Si-Yu Li, Guo-Jian Wang, Zirui Zhang, Jun-Qing Xia
Figure caption: The angular power spectra of simulated thermal dust and synchrotron maps for cases 1, 2, 3, 4, and 5 outlined in Table 2. The black lines refer to the power spectra of the template. For the cases 2–5, corresponding shaded areas show the ±2σ ranges of simulated power spectra determined from 200 different random realization.
Paper: CMBFSCNN: Cosmic Microwave Background Polarization Foreground Subtraction with a Convolutional Neural Network
Authors: Ye-Peng Yan, Si-Yu Li, Guo-Jian Wang, Zirui Zhang, Jun-Qing Xia
Figure caption: Lensed and unlensed CMB Q maps and their residual map.