adsabs/AstroCLIMB huggingface dataset:
Paper: SN 2023zaw: The Low-energy Explosion of an Ultrastripped Star
Authors: T. Moore, J. H. Gillanders, M. Nicholl, M. E. Huber, S. J. Smartt, S. Srivastav, H. F. Stevance, T.-W. Chen, K. C. Chambers, J. P. Anderson, M. D. Fulton, S. R. Oates, C. Angus, G. Pignata, N. Erasmus, H. Gao, J. Herman, C.-C. Lin, T. Lowe, E. A. Magnier, P. Minguez, C.-C. Ngeow, X. Sheng, S. A. Sim, K. W. Smith, R. Wainscoat, S. Yang, D. R. Young, K.-J. Zeng
Figure caption: Optical spectroscopy of SN 2023zaw. The phase in days relative to maximum light is indicated. These spectra have been telluric and Galactic line-of-sight extinction corrected and corrected for host galaxy recessional velocity. The inset shows the blended Na I D lines in the +4.2- and +8.2-day spectra. We also include spectra from SN 2019wxt (I. Agudo et al. 2023), SN 2007C (M. Modjaz et al. 2014), and SN 2019bkc (P. Chen et al. 2020; S. J. Prentice et al. 2020) and include the approximate phase of each observation.
Paper: SN 2023zaw: The Low-energy Explosion of an Ultrastripped Star
Authors: T. Moore, J. H. Gillanders, M. Nicholl, M. E. Huber, S. J. Smartt, S. Srivastav, H. F. Stevance, T.-W. Chen, K. C. Chambers, J. P. Anderson, M. D. Fulton, S. R. Oates, C. Angus, G. Pignata, N. Erasmus, H. Gao, J. Herman, C.-C. Lin, T. Lowe, E. A. Magnier, P. Minguez, C.-C. Ngeow, X. Sheng, S. A. Sim, K. W. Smith, R. Wainscoat, S. Yang, D. R. Young, K.-J. Zeng
Figure caption: Light curves of SN 2023zaw  in the griz bands compared to the fast SNe SN 2019bkc (P. Chen et al. 2020; S. J. Prentice et al. 2020) and SN 2019dge (Y. Yao et al. 2020) and the representative Type Ib SNe SN 2007Y (M. Stritzinger et al. 2009) and SN 2007C (M. R. Drout et al. 2011; M. D. Stritzinger et al. 2018). Each light curve is in the rest frame and has been corrected for Milky Way and host galaxy extinctions (M. R. Drout et al. 2011). These SNe were chosen to represent the population of ultrastripped SNe and typical Type Ib SNe.
Paper: The Influence of Stellar Chromospheres and Coronae on Exoplanet Transmission Spectroscopy
Authors: Volker Perdelwitz, Adam Chaikin-Lifshitz, Aviv Ofir, Oded Aharonson
Figure caption: SDO (W. D. Pesnell et al. 2012) measurements of the Sun’s brightness distribution, azimuthally averaged. The data were acquired at 17.1 nm. As highlighted in the enlarged panel, exterior to the solar disk, an exponentially decaying emission law integrated along the line of sight of the observer (dashed line) is consistent with the 2020 SDO observations.
Paper: The Influence of Stellar Chromospheres and Coronae on Exoplanet Transmission Spectroscopy
Authors: Volker Perdelwitz, Adam Chaikin-Lifshitz, Aviv Ofir, Oded Aharonson
Figure caption: Example corner plot of a light-curve fit for a wavelength bin where H and Br are well constrained (λ = 0.7516 μm).
Paper: The MUSE Ultra Deep Field: A 5 Mpc Stretch of the z ≈ 4 Cosmic Web Revealed in Emission
Authors: Davide Tornotti, Michele Fumagalli, Matteo Fossati, Fabrizio Arrigoni Battaia, Alejandro Benitez-Llambay, Pratika Dayal, Rajeshwari Dutta, Celine Peroux, Marc Rafelski, Mitchell Revalski
Figure caption: Left: extracted Lyα image of a cosmic web filament connecting an overdensity (δ ≈ 25) of 19 LAEs at redshift z ≈ 4.008 obtained from the continuum-subtracted datacube. North is up and east to the left. The black contour is the detection limit at S/N = 2. The purple and red contours are at 1 × 10−19 and 5 × 10−19 erg s−1 cm−2 arcsec−2. The blue crosses indicate the LAEs identified at this redshift. L5 and L19 exhibit only compact emission unconnected to the extended signal and are not shown on this map. The background is a MUSE white-light image of the MUDF with continuum-detected sources visible in black and the dashed green contours defining the exposure time map of the field according to the labeled values. The black rectangles (A–F) are the extraction apertures of the spectra on the right panel. Right: spectra of the Lyα emission detected in the extraction windows, as marked on the left panel. These boxes focus on the spectral emission in regions of low S/N and surface brightness, which are associated with the main filamentary structure. The horizontal dashed blue lines represent the 1σ uncertainty calculated from the region outside ≈±500 km s−1 of the emission line centroid.
Paper: The MUSE Ultra Deep Field: A 5 Mpc Stretch of the z ≈ 4 Cosmic Web Revealed in Emission
Authors: Davide Tornotti, Michele Fumagalli, Matteo Fossati, Fabrizio Arrigoni Battaia, Alejandro Benitez-Llambay, Pratika Dayal, Rajeshwari Dutta, Celine Peroux, Marc Rafelski, Mitchell Revalski
Figure caption: Median SB profile of LAEs extracted along slits aligned with the filament emission (black), randomly oriented slits (blue), and annuli (red). The vertical arrow marks the inflection point we identified at ≈20 kpc. Profiles from large samples of LAEs from the literature are also shown with black, gray, and orange dashed lines.
Paper: The MUSE Ultra Deep Field: A 5 Mpc Stretch of the z ≈ 4 Cosmic Web Revealed in Emission
Authors: Davide Tornotti, Michele Fumagalli, Matteo Fossati, Fabrizio Arrigoni Battaia, Alejandro Benitez-Llambay, Pratika Dayal, Rajeshwari Dutta, Celine Peroux, Marc Rafelski, Mitchell Revalski
Figure caption: The signal-to-noise distribution of the voxels in the datacube used for signal extraction at the redshift of the z ≈ 4.008 LAE group. The purple line defines the distribution of the background. The gray region indicates the voxels associated with the emission from LAEs, while the blue region corresponds to the diffuse emission from the filaments (i.e., not overlapping in projection with SB levels of 4 × 10−19 erg s−1 cm−2 arcsec−2). The black dashed vertical line is the median of the background distribution (≈0) and the red dotted vertical line indicates the S/N = 2 threshold.
Paper: The MUSE Ultra Deep Field: A 5 Mpc Stretch of the z ≈ 4 Cosmic Web Revealed in Emission
Authors: Davide Tornotti, Michele Fumagalli, Matteo Fossati, Fabrizio Arrigoni Battaia, Alejandro Benitez-Llambay, Pratika Dayal, Rajeshwari Dutta, Celine Peroux, Marc Rafelski, Mitchell Revalski
Figure caption: Comparison of the Lyα luminosity of galaxies in the z ≈ 4.008 filament (red diamonds) and in a control sample, which we divide in galaxies in groups (125, yellow stars) or more isolated systems (34, green circles). The solid black line and the associated gray region represent the smoothed median, 25th, and 75th log-luminosity percentile regression curves for the control sample as a function of redshift, obtained with a B-splines (COBS) smoothing algorithm (P. Ng & M. Maechler 2007, 2024). The luminosity distributions, marginalized in redshift, are shown as histograms in the right panel. The top panel shows the redshift distribution of the sample, with the red solid line marking the filament redshift.
Paper: SN 2023zaw: The Low-energy Explosion of an Ultrastripped Star
Authors: T. Moore, J. H. Gillanders, M. Nicholl, M. E. Huber, S. J. Smartt, S. Srivastav, H. F. Stevance, T.-W. Chen, K. C. Chambers, J. P. Anderson, M. D. Fulton, S. R. Oates, C. Angus, G. Pignata, N. Erasmus, H. Gao, J. Herman, C.-C. Lin, T. Lowe, E. A. Magnier, P. Minguez, C.-C. Ngeow, X. Sheng, S. A. Sim, K. W. Smith, R. Wainscoat, S. Yang, D. R. Young, K.-J. Zeng
Figure caption: Best-fitting TARDIS models (red), compared to the +4.2- and +8.2-day observed spectra of SN 2023zaw (black). The +4.2-day observed spectrum and associated model spectra have been vertically offset for clarity (by 6 × 10−17erg s−1 cm−2 Å−1). Also plotted are two model spectra from a helium shell detonation simulation (blue) presented by S. A. Sim et al. (2012). These models have phases comparable to those of the observed spectra (Δt < 0.13 days) and have been rescaled and arbitrarily offset to roughly match the continua of the observed spectra.
Paper: The MUSE Ultra Deep Field: A 5 Mpc Stretch of the z ≈ 4 Cosmic Web Revealed in Emission
Authors: Davide Tornotti, Michele Fumagalli, Matteo Fossati, Fabrizio Arrigoni Battaia, Alejandro Benitez-Llambay, Pratika Dayal, Rajeshwari Dutta, Celine Peroux, Marc Rafelski, Mitchell Revalski
Figure caption: Mean spectral stack for the 19 LAEs associated with the analyzed group. From the left, the three panels show the spectral region associated with the Lyα, C IV, and He II lines. The dashed blue vertical lines represent the expected zero velocity in each line, while the red dashed line is the zero flux reference. The gray-shaded region represents the 1σ noise estimated near each line (±3000 km s−1). Sharp peaks in the C IV region are associated with residual skylines in the cube.
Paper: The MUSE Ultra Deep Field: A 5 Mpc Stretch of the z ≈ 4 Cosmic Web Revealed in Emission
Authors: Davide Tornotti, Michele Fumagalli, Matteo Fossati, Fabrizio Arrigoni Battaia, Alejandro Benitez-Llambay, Pratika Dayal, Rajeshwari Dutta, Celine Peroux, Marc Rafelski, Mitchell Revalski
Figure caption: Spectra of the 19 LAEs associated with the analyzed group. The sources are sorted by redshift as labeled in Figure 1. The flux is rescaled to the rest frame according to individual redshifts, determined as described in the main text. The dashed blue vertical lines represent the zero velocity in each line, while the red dashed line is the zero flux reference. The gray shading represents the 1σ uncertainties in the flux values.
Paper: SN 2023zaw: The Low-energy Explosion of an Ultrastripped Star
Authors: T. Moore, J. H. Gillanders, M. Nicholl, M. E. Huber, S. J. Smartt, S. Srivastav, H. F. Stevance, T.-W. Chen, K. C. Chambers, J. P. Anderson, M. D. Fulton, S. R. Oates, C. Angus, G. Pignata, N. Erasmus, H. Gao, J. Herman, C.-C. Lin, T. Lowe, E. A. Magnier, P. Minguez, C.-C. Ngeow, X. Sheng, S. A. Sim, K. W. Smith, R. Wainscoat, S. Yang, D. R. Young, K.-J. Zeng
Figure caption: Physical parameter posterior distribution of the circumstellar material + nickel model. The important physical parameters are nickel fraction (fNi), kinetic energy (Ek), CSM mass (Mcsm), ejecta mass (Mej), CSM radius (R0) in units of AU, CSM density (ρ), and ﹩{t}_{{\rm{\exp }}}﹩ relative to the first photometric detection (MJD 60285.23) of SN 2023zaw.
Paper: Three Worlds in One: Venus as a Natural Laboratory for the Effect of Rotation Period on Atmospheric Circulation
Authors: Maureen Cohen, James Holmes, Stephen Lewis, Manish Patel, Sébastien Lebonnois
Figure caption: Tropical and extratropical meridional Rossby wavenumber as a function of altitude for the VPCM simulation and the Pioneer Venus Day, Night, and North entry probes. The dotted line indicates where the Rossby radius of deformation equals the planetary radius.
Paper: Three Worlds in One: Venus as a Natural Laboratory for the Effect of Rotation Period on Atmospheric Circulation
Authors: Maureen Cohen, James Holmes, Stephen Lewis, Manish Patel, Sébastien Lebonnois
Figure caption: Top row: (a) Brunt–Väisälä frequency calculated as ﹩N=\sqrt{\frac{g}{\theta (z)}\frac{d\theta }{dz}}﹩ and (b) Brunt–Väisälä frequency with values below 40 km replaced by the mean for this region (approximately 0.0025 s−1). Values above 40 km are the same as in (a). Bottom row: tropical and extratropical meridional Rossby wavenumbers calculated according to Equations (1) and (2) using each of the Brunt–Väisälä frequency profiles shown in the row above. Subfigure (d) is used in the main text to diagnose the circulation regimes.
Paper: Three Worlds in One: Venus as a Natural Laboratory for the Effect of Rotation Period on Atmospheric Circulation
Authors: Maureen Cohen, James Holmes, Stephen Lewis, Manish Patel, Sébastien Lebonnois
Figure caption: Left: vertical profiles of the zonal wind from the Venus PCM and three Pioneer Venus entry probes (Day, Night, and North). The Day and Night probes measured the wind profiles near 30∘S, while the North probe entered near 60∘N. The VPCM profiles are the zonal means at 30∘S and 60∘N. Right: the effective rotation period in Earth days of the atmosphere as a function of altitude for the VPCM simulation and the Day, Night, and North probes, calculated from the zonal wind profiles.
Paper: Three Worlds in One: Venus as a Natural Laboratory for the Effect of Rotation Period on Atmospheric Circulation
Authors: Maureen Cohen, James Holmes, Stephen Lewis, Manish Patel, Sébastien Lebonnois
Figure caption: Tropical and extratropical meridional Rossby wavenumbers calculated according to Equations (1) and (2) using wind profiles from a range of latitudes, as well as the area-weighted global mean.
Paper: Extremely Dense Gas around Little Red Dots and High-redshift Active Galactic Nuclei: A Nonstellar Origin of the Balmer Break and Absorption Features
Authors: Kohei Inayoshi, Roberto Maiolino
Figure caption: Left: AGN SEDs attenuated through a gas slab with a visual extinction of AV = 3 mag with Z = 0.1 Z⊙. Each curve represents the case with different density (107 ≤ nH/cm−3 ≤ 1011) and thickness. With high densities of nH ≃ 109−11 cm−3, the SEDs show a deep Balmer break at ﹩{\lambda }_{{\rm{B,lim}}}=3646\,\,\unicode{x0212B}\,﹩. Two vertical lines indicate the wavelengths (λB,blue = 3600 Å and λB,red = 4000 Å) used to quantify the Balmer break strength. Right: total AGN SEDs, including the nebular emission with a covering fraction of C = 0.5. For the cases with nH = 109−11 cm−3, the nebular components are shown separately (dashed). The Balmer jump feature of the nebular spectrum weakens the Balmer break strength in the total SED when dense absorbers with nH ≳ 1011 cm−3 surround the AGN with a high covering fraction (C ≳ 0.5).
Paper: Extremely Dense Gas around Little Red Dots and High-redshift Active Galactic Nuclei: A Nonstellar Origin of the Balmer Break and Absorption Features
Authors: Kohei Inayoshi, Roberto Maiolino
Figure caption: The Balmer break strength defined by Fλ(λB,red)/Fλ(λB,blue) for NH = 5.4 × 1022 (dashed) and 1.7 × 1023 cm−2 (solid). Two covering fractions are considered: C = 0.5 (black) and C = 1 (gray). For the fiducial case (black and dashed curve), the Balmer break strength reaches values of ≥2 in the density range of 109 ≲ nH/cm−3 ≲ 2 × 1010. With increasing column density, the Balmer break becomes more prominent due to the enhanced column density of atomic hydrogen in the n = 2 state. These depths are consistent with those of six broad-line LRDs that show a Balmer break in the PRISM spectrum (L. J. Furtak et al. 2024; B. Wang et al. 2024b; V. Kokorev et al. 2024b; I. Labbe et al. 2024; see the text).
Paper: Extremely Dense Gas around Little Red Dots and High-redshift Active Galactic Nuclei: A Nonstellar Origin of the Balmer Break and Absorption Features
Authors: Kohei Inayoshi, Roberto Maiolino
Figure caption: The Hα line profiles with FWHMbroad = 3000 km s−1, FWHMnarrow = 400 km s−1, and r = 0.3. We explore two cases: b = 150 km s−1, Δv = −200 km s−1, and C = 0.5 (left panel) and b = 10 km s−1, Δv = +50 km s−1, and C = 0.8 (right panel). The solid and dashed curves show the total Hα line profile and the broad component with absorption by dense gas clumps with a column density of n = 2 atomic hydrogen, NH,n= 2 = 1016 cm−2. The total line profile with a finite spectral resolution (R ≡ Δλ/λ0 = 1500 and 500) is overlaid, where the source redshift is set to z = 5.
Paper: Extremely Dense Gas around Little Red Dots and High-redshift Active Galactic Nuclei: A Nonstellar Origin of the Balmer Break and Absorption Features
Authors: Kohei Inayoshi, Roberto Maiolino
Figure caption: Profiles of the hydrogen level populations in the n = 2 (solid) and n = 3 (dashed) states as a function of slab thickness normalized by the total value Δs for each density case; nH = 107 − 1011 cm−3. The values are normalized by the total density of hydrogen nuclei (nH), including both neutral and ionized states. As the density increases, the hydrogen is excited to the higher-energy states. The ratio of n = 2 states reaches n2/nH ≃ 10−6, which is the equilibrium value with T ≃ 8000 K through particle collisions.
Paper: Extremely Dense Gas around Little Red Dots and High-redshift Active Galactic Nuclei: A Nonstellar Origin of the Balmer Break and Absorption Features
Authors: Kohei Inayoshi, Roberto Maiolino
Figure caption: Same as in Figure 4 but illustrating how the line shape changes with the width of the absorption feature, varying b from 50 to 400 km s−1. The other parameters are identical to those used in Figure 4.
Paper: Simultaneous Evolutionary Fits for Jupiter and Saturn Incorporating Fuzzy Cores
Authors: Ankan Sur, Roberto Tejada Arevalo, Yubo Su, Adam Burrows
Figure caption: A very slightly improved evolutionary model for Jupiter (see R. Tejada Arevalo et al. 2024b) with an initial fuzzy core that matches within observational uncertainties the current values of the effective temperature, equatorial radius, atmospheric helium abundance, outer envelope metallicity, and J2 and J4 gravitational moments. The initial outer entropy is 8.2 kB baryon−1, while the interior entropy is 7.5 kB baryon−1. (Top left) The evolution of the temperature profile; (top middle) the evolution of the helium mass fraction (Y) profile; (top right) effective temperature and equatorial radius; (bottom left) evolution of the entropy profile; (bottom middle) evolution of the Z profile; and (bottom right) evolution of the gravitational moments J2 and J4. This Jupiter model contains 42.5 M⊕of heavy elements, including a compact core of 3 M⊕ (Z = 1). As shown in the bottom-middle panel, the initial Z profile becomes convectively mixed from the outer layers inward, with the most significant changes occurring early in the evolution. The outer metallicity starts at 1.9 Z⊙ and increases to 3.6 Z⊙. Helium rain begins at 4 Gyr, based on the LHR0911miscibility curves with a +410 K temperature shift, resulting in outer helium depletion to Y = 0.236, consistent with Galileo entry probe measurements (U. von Zahn et al. 1998). The black dashed line in the top-left panel indicates the demixing temperature curve encountered by the cooling temperature profile, and the small vertical blue shaded region highlights the helium rain zone. The time stamps are indicated in different colors on the bottom-middle panel.
Paper: Simultaneous Evolutionary Fits for Jupiter and Saturn Incorporating Fuzzy Cores
Authors: Ankan Sur, Roberto Tejada Arevalo, Yubo Su, Adam Burrows
Figure caption: The best-fit evolutionary model for Saturn with an initial fuzzy core that matches its current values of the effective temperature, equatorial radius, atmospheric helium abundance, outer envelope metallicity, Brunt–Väisälä frequency, and gravitational moments within observational uncertainties. The initial outer entropy is 7.9 kB baryon−1, while the interior entropy ​​​​​​∼​​​​​​6.2 kB baryon−1. The panels are the same as in Figure 3: (top left) evolution of the temperature profile; (top middle) evolution of the helium mass fraction (Y) profile; (top right) evolution of the effective temperature and equatorial radius; (bottom left) evolution of the entropy profile; (bottom middle) evolution of the Z profile; and (bottom right) evolution of the gravitational moments J2 and J4. This model contains 25 M⊕ of heavy elements, including a compact core of 4 M⊕. The outer metallicity starts at 2.0 Z⊙ and increases to 4.57 Z⊙. Helium rain begins at 0.92 Gyr, based on the LHR0911miscibility curve with a +410 K temperature shift that also fits our Jupiter model, resulting in outer helium depletion to Yatm ∼ 0.205, consistent with B. J. Conrath & D. Gautier (2000) and T. T. Koskinen & S. Guerlet (2018; shown by the pink shaded region in top middle panel). The top-left panel shows the miscibility curve and helium rain region. The Brunt–Väisälä ratio of approximately 1.7 at 4.56 Gyr, closely aligning with the value of 2 predicted by C. R. Mankovich & J. Fuller (2021), is shown in the bottom-left panel. Similar to C. R. Mankovich & J. Fuller (2021), whose stably stratified region extends to 0.6 Saturn radii, in order to match Saturn’s current observables best our model finds that the stable region extends to 0.5 RSat.
Paper: Simultaneous Evolutionary Fits for Jupiter and Saturn Incorporating Fuzzy Cores
Authors: Ankan Sur, Roberto Tejada Arevalo, Yubo Su, Adam Burrows
Figure caption: Reproduction of the S. Howard et al. (2024) results using APPLE with the SR18 (blue) and LHR0911(red) miscibility curves, with their suggested temperature shifts (+350 and −1250 K, respectively). Our comparison models, represented by solid lines, include a core of mass 30 M⊕ for Jupiter and 20 M⊕ for Saturn. The CMS19+HG23 EOS is used for the H–He envelope, and the models are evolved with the J. J. Fortney et al. (2011) boundary conditions (as did they). The left panels depict the helium mass fraction profile in the H–He envelope at 4.56 Gyr. We see the formation of a helium ocean at pressures above 7–8 Mbar. The dashed line shows the Galileo Yatm constraint (U. von Zahn et al. 1998). The middle panels depict the evolution of effective and internal temperatures with age, with the dashed line indicating the constraints on Teff from L. Li et al. (2010, 2012) for both planets. The right panels show the evolution of radius with age.
Paper: Simultaneous Evolutionary Fits for Jupiter and Saturn Incorporating Fuzzy Cores
Authors: Ankan Sur, Roberto Tejada Arevalo, Yubo Su, Adam Burrows
Figure caption: Reproduction of the C. R. Mankovich & J. J. Fortney (2020, MF2020) results for Jupiter and Saturn using APPLE. The left panels depict the helium abundance in the H–He envelope of the planet, with the color scale indicating the age in Gyr. The dashed line in the top-left panel represents the Galileo constraint Yatm = 0.238 × (1 − Zatm) = 0.234 (U. von Zahn et al. 1998), while the dashed line in the bottom-left panel shows the total helium mass fraction Yatm = 0.066 corresponding to Yatm/(1 − Z) = 0.07, as obtained by MF2020. The right panels display the evolution of effective and internal temperatures with age, with the dashed line indicating the constraints from L. Li et al. (2010, 2012) for both planets.
Paper: Dynamic Imprints of Colliding-wind Dust Formation from WR 140
Authors: Emma P. Lieb, Ryan M. Lau, Jennifer L. Hoffman, Michael F. Corcoran, Macarena Garcia Marin, Theodore R. Gull, Kenji Hamaguchi, Yinuo Han, Matthew J. Hankins, Olivia C. Jones, Thomas I. Madura, Sergey V. Marchenko, Hideo Matsuhara, Florentin Millour, Anthony F. J. Moffat, Mark R. Morris, Patrick W. Morris, Takashi Onaka, Marshall D. Perrin, Armin Rest, Noel Richardson, Christopher M. P. Russell, Joel Sanchez-Bermudez, Anthony Soulain, Peter Tuthill, Gerd Weigelt, Peredur M. Williams
Figure caption: Substructure persisting in WR 140. Left: 7.7 μm PSF-subtracted Cycle 2 image with red lines indicating the 10 radial flux profiles per dust structure (E, C0, and C1) that we used to calculate the proper motions (Section 4.1). The three colored boxes correspond to the zoomed-in regions shown on the right (yellow for E, blue for C1, and green for C0). Top right: zoomed-in 7.7 μm images for Cycle 1 (left) and Cycle 2 (right) at the E dust structure, with clumps highlighted by arrows. Middle right: as above, but for the C1 dust structure. Bottom right: as above, but for the C0 dust structure. The approximate position angles of these dust features are 220°, 150°, and 115° east of north for C1, C0, and E, respectively.