adsabs/AstroCLIMB huggingface dataset:
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: (A) Temperature profiles at a dayside surface temperature of 250 K. (B) Mixing ratios of gaseous and condensed phases. (C) Cloud coverage profile with a cloud cover fraction set to 60%.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: (A) Temperature profiles at a dayside surface temperature of 650 K. (B) Mixing ratios of gaseous and condensed phases. (C) Cloud coverage profile with a cloud cover fraction set to 60%. The horizontal red line is the lifted condensation level.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: WTG parameter Λ as a function of the characteristic temperature of different atmospheres. If Λ is smaller than unity, it indicates an atmosphere that can support significant horizontal temperature gradients away from the equator. The further above unity Λ is, the deeper the atmosphere is in a WTG regime.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: Spectral flux contributions over the range [1, 25] μm for a surface temperature of (Top) 250 K and (Bottom) 650 K. The white lines delineate the areas where the ﹩{ \mathcal C }{{ \mathcal F }}_{{\rm{F}}}﹩ per spectral band is higher than unity. The spectral range of LIFE and the vertical extent of the cloud are overplotted.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: Upward photon top-of-atmosphere fluxes as a function of wavelength at a surface temperature of 300 K, for a range of cloud cover fractions. The black dashed curve is the Planck emission of a surface of 300 K and zero albedo.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: Relative humidity profiles for a dayside surface temperature of (top) 250 K and (bottom) 650 K.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: (A, B) Dayside and (C) nightside flux profiles with a dayside surface temperature of 250 K and a cloud fraction of (A) 60% and (B) 0%.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: LIFESIM simulation of an observation of Teegarden’s Star b with a resolution of 50 and an integration time of 24 hr. (Top) Upward photon top-of-atmosphere fluxes as a function of wavelength at a surface temperature of 300 K, for a range of cloud cover fractions. The shaded areas represent the 1σ confidence level. (Bottom) Statistical significance of the detected difference between the clear-sky scenario and the cloudy scenarios.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: (Top) Top-of-atmosphere fluxes as a function of surface temperature. The solid curves from yellow to brown are the dayside outgoing planetary fluxes varying the cloud cover fraction. The green dotted curve is the nightside clear-sky outgoing planetary flux. The dashed–dotted curves in shades of blue are the absorbed stellar fluxes varying the cloud cover fraction. (Bottom) Planetary albedo as a function of surface temperature for a range of cloud cover fractions.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: The same LIFESIM synthetic observation with an integration time increased to 168 hr and the addition of 40 Pa of CO2 in the atmosphere.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: The same LIFESIM synthetic observation with an integration time increased to 168 hr.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: Venus-like atmosphere with 3.3 bars of N2 and 89.7 bars of CO2, added to a 7 bar water ocean, which is evaporated into the atmosphere. The surface temperature is 740 K. The resolution is 50, and the integration time is 168 hr.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: Upward radiant fluxes as a function of wavenumber at a surface temperature of 300 K, a cloud cover fraction of 60%, and at four pressure levels spanning the vertical extent of the column. The surface blackbody curve is plotted as a reference.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: LIFESIM synthetic phase curves sweeping over five partial pressures of N2, with a resolution of 50 and an integration time of 24 hr.
Paper: The Impact of Water Clouds on the Prospective Emission Spectrum of Teegarden’s Star b as Observed by LIFE
Authors: Ryan Boukrouche, Rodrigo Caballero, Markus Janson
Figure caption: Flux contribution function profiles for a surface temperature of (top) 250 K and (bottom) 650 K. Solid lines are the sum over the range [1, 30,000] cm−1 and the dashed lines are the sum over the spectral range of LIFE [540.54, 2500] cm−1.
Paper: Reverse Shock Emission from Misaligned Structured Jets in Gamma-Ray Bursts
Authors: Sen-Lin Pang, Zi-Gao Dai
Figure caption: The coordinate system used to calculate afterglow emission from the observer direction. The jet direction is along the z direction, while LOS is along the ﹩\tilde{z}﹩ direction. The yellow ring is an arbitrary segment of structured jet.
Paper: Realistic Outcomes of Moon–Moon Collisions in Lunar Formation Theory
Authors: Uri Malamud, Hagai B. Perets
Figure caption: Close Earth approach of the massive moonlet (m 1) from scenario 20_2 in Table 7. The Earth is a single gravitating SPH particle, rendered as a sphere and scaled to the Earth’s size. The orbital pericenter q is left of the Earth. The first (q = 0.88R Roche_f—(a), (c)) and second (q = 1.12R Roche_f—(e)) close approaches occur 6.94 and 30.56 hr after the initial collision (not shown), respectively. Panels show (a) first close approach including internal strength; (b) q remains unaffected several hours later; (c) first close approach with pure hydrodynamics indicating tidal elongation; (d) tidal stripping is observed several hours later, after which the pericenter q increases by 25%; (e) second close approach with pure hydrodynamics indicating tidal elongation; (f) tidal stripping is observed a second time, after which the pericenter q increases by additional 10%. The color scheme for the SPH particles denotes temperature, as shown in the color bar of panel (a).
Paper: Realistic Outcomes of Moon–Moon Collisions in Lunar Formation Theory
Authors: Uri Malamud, Hagai B. Perets
Figure caption: The four-stage collision evolution of scenario 20_166. Each two panels show the respective start and end state of each stage: (a)–(b) first hydrodynamic; (c)–(d) first N-body; (e)–(f) second hydrodynamic; (g)–(h) second N-body. In the hydrodynamic simulations, the Earth is a single gravitating SPH particle. For visual clarity, it is rendered as a sphere and scaled to the Earth’s size. In the N-body simulations, all particles are rendered as spheres and scaled to their respective physical size, which the code is modified to inform. The color scheme for the SPH particles denotes temperature, as shown in the color bar of panel (a).
Paper: Realistic Outcomes of Moon–Moon Collisions in Lunar Formation Theory
Authors: Uri Malamud, Hagai B. Perets
Figure caption: The mass fraction of the two largest fragments (or one fragment in the case of a perfect merger) to the total mass, compared between simulations with internal strength (solid) vs. pure hydrodynamics (dotted). The simulation label names are color coded to the impact velocity (color bar), indicating a general correlation with fragmentation.
Paper: Realistic Outcomes of Moon–Moon Collisions in Lunar Formation Theory
Authors: Uri Malamud, Hagai B. Perets
Figure caption: The rotation period of moonlets emerging in hydrodynamic impacts from Table 1, as a function of the impact angle of the original colliding moonlets. The data points are color coded to the impact velocity (color bar) and size coded to the mass ratio of the original moonlets (smallest/largest circles representing a 1:1/2.5:1 mass ratio, respectively).
Paper: Effects of Background Solar Wind and Drag Force on the Propagation of Coronal-mass-ejection-driven Shocks
Authors: Chin-Chun Wu, Kan Liou, Brian E. Wood, Lynn Hutting
Figure caption: The panels from top to bottom show the time profile of the simulated magnetic field intensity (B), the solar wind density (N  p ), the temperature (T  P ), the radial speed (V  r ), the MHD wave-mode speeds (C  s : slow mode; C A: Alfvén mode; and C  f : fast mode), the shock speed in the inertial frame (V  s ), the shock speed in the solar wind frame (V S@SW), the fast-mode Mach number (M  f ), and the radial distance from the Sun’s center (r) at regions immediately upstream of the shock. The left panels ((a)–(i)) are for CME03 and the right panels ((j)–(r)) are for CME12.
Paper: Effects of Background Solar Wind and Drag Force on the Propagation of Coronal-mass-ejection-driven Shocks
Authors: Chin-Chun Wu, Kan Liou, Brian E. Wood, Lynn Hutting
Figure caption: Selected solar wind radial velocity maps on the surface where the Earth is located. The surface is defined by θ = 97.°5 for the CME03 event (top panels) and by θ = 82.°5 for the CME12 event (bottom panels). The Sun is marked as a red dot in the center. The black circle marks r = 1 au and the blue contours are the heliospheric current sheet or HCS (B  ϕ  = 0). The HCS is marked as the HCS that has been interacting with the CME. The noses of the CME-driven shocks are marked with “Nose,” with an arrow pointing to the leading edge. The locations of the spacecraft are marked by a “+” sign and “E” for Wind, “A” for STEREO-A, and “B” for STEREO-B, respectively. The color bar is listed to the right. The black solid circle indicates the location of 1 au. The black dashed circle indicates the front boundary of the nose of the CME-driven shock.
Paper: Effects of Background Solar Wind and Drag Force on the Propagation of Coronal-mass-ejection-driven Shocks
Authors: Chin-Chun Wu, Kan Liou, Brian E. Wood, Lynn Hutting
Figure caption: Wind-observed in situ solar wind parameters and geomagnetic activity index (Dst) during 2010 April 05–06 (left panels) and 2012 July 13–17 (right panels). From top to bottom: (a) proton plasma beta; (b) Dst; (c)–(d) longitude [ϕ B] and latitude [θ B], in geocentric solar ecliptic (GSE) coordinates; (e) Bz of the field in GSE coordinates; (f) magnetic field [B] in terms of magnitude; (g) thermal velocity [V th] or proton temperature [T]; (h) bulk speed [V ]; and (i) number density [Np]. The blue horizontal line in (c) represents the scheme’s identification of the extent of this MC candidate (Lepping et al. 1990). The vertical solid line, dotted line, and dashed line represent the IP shock, the front boundary, and the end boundary of the MC.
Paper: Effects of Background Solar Wind and Drag Force on the Propagation of Coronal-mass-ejection-driven Shocks
Authors: Chin-Chun Wu, Kan Liou, Brian E. Wood, Lynn Hutting
Figure caption: Comparison of the solar wind parameters (from the top to bottom panels: V  r : radial speed; N  p : proton density; T  p : proton temperature; and B: magnetic intensity) between the G3DMHD results (black traces) and the Wind in situ measurements (red dotted curves) for the CME03 (left panels) and CME12 (right panels) event periods. The SAT is marked as a vertical dotted line in each panel.
Paper: Effects of Background Solar Wind and Drag Force on the Propagation of Coronal-mass-ejection-driven Shocks
Authors: Chin-Chun Wu, Kan Liou, Brian E. Wood, Lynn Hutting
Figure caption: Selected coronagraph images recorded by STEREO/SECCHI for CME03 on 2010 April 3–4 (top panels) and for CME12 on 2012 July 12–14 (bottom panels; see the text for details). The FOVs of Cor1 and Cor2 cover 1.5–4 R ⊙ and 2–15  R ⊙ from the limb, respectively (Howard et al. 2008).
Paper: Effects of Background Solar Wind and Drag Force on the Propagation of Coronal-mass-ejection-driven Shocks
Authors: Chin-Chun Wu, Kan Liou, Brian E. Wood, Lynn Hutting
Figure caption: Least-squares regression line representing the average propagation speed of CME03 (top panels) and CME12 (bottom panels) in the FOVs of Cor1a (panels (a) and (e)), Cor1b (panels (b) and (f)), Cor2a (panels (c) and (g)), and Cor2b (panels (d) and (h)).
Paper: The Hubble Constant Anchor Galaxy NGC 4258: Metallicity and Distance from Blue Supergiants
Authors: Rolf-Peter Kudritzki, Miguel A. Urbaneja, Fabio Bresolin, Lucas M. Macri, Wenlong Yuan, Siyang Li, Gagandeep S. Anand, Adam G. Riess
Figure caption: Blue supergiant metallicity [Z] (red circles) as a function of deprojected galactocentric distance r/r 25. The linear regression is plotted in red. H II region oxygen abundances (in units of the solar value) by W. Yuan et al. (2022) obtained from the strong line ratio R 23 with the M. Pettini & B. E. J. Pagel (2004) (upper plot) and D. Zaritsky et al. (1994) (lower plot) metallicity calibrations are shown in gray together with the corresponding regressions (dashed). The horizontal line in the upper plot indicates the Cepheid metallicity adopted by A. G. Riess et al. (2022). The blue symbols correspond to H II region oxygen abundances obtained by the direct method using auroral lines (F. Bresolin 2011).
Paper: The Hubble Constant Anchor Galaxy NGC 4258: Metallicity and Distance from Blue Supergiants
Authors: Rolf-Peter Kudritzki, Miguel A. Urbaneja, Fabio Bresolin, Lucas M. Macri, Wenlong Yuan, Siyang Li, Gagandeep S. Anand, Adam G. Riess
Figure caption: The mass–metallicity relationship of star-forming galaxies obtained from absorption line studies of the young stellar population. The pink star represents NGC 4258 as the result of this work. Blue circles refer to the spectroscopy of blue supergiant (BSG) stars carried out in previous work as mentioned in the main text. Red circles report metallicities determined by the analysis of near-infrared spectra of red supergiants (RSG) or superstar clusters (SSC). The yellow circle is the result of the spatially resolved stellar population synthesis study by E. Sextl et al. (2024), while the yellow squares refer to the analysis of integrated galaxy spectra of 250,000 star-forming Sloan Digital Sky Survey galaxies again using a population synthesis technique (E. Sextl et al. 2023). Predictions from the galaxy evolution look-back models by R.-P. Kudritzki et al. (2021a, 2021b) are shown as the green line.
Paper: The Hubble Constant Anchor Galaxy NGC 4258: Metallicity and Distance from Blue Supergiants
Authors: Rolf-Peter Kudritzki, Miguel A. Urbaneja, Fabio Bresolin, Lucas M. Macri, Wenlong Yuan, Siyang Li, Gagandeep S. Anand, Adam G. Riess
Figure caption: Difference between blue supergiant and H II region metallicities. For the latter, the direct method using collisionally excited auroral lines has been used. The H II region nebular metallicities have been increased by 0.1 dex to account for oxygen depletion onto dust grains. The data are from F. Bresolin et al. (2016, 2022), M. A. Urbaneja et al. (2023), and this work.
Paper: The Hubble Constant Anchor Galaxy NGC 4258: Metallicity and Distance from Blue Supergiants
Authors: Rolf-Peter Kudritzki, Miguel A. Urbaneja, Fabio Bresolin, Lucas M. Macri, Wenlong Yuan, Siyang Li, Gagandeep S. Anand, Adam G. Riess
Figure caption: The observed FGLR in NGC 4258. The fiducial relationships of Equations (1) and (2) shifted by the fitted distance modulus are shown in green. A distance modulus of m − M = 29.38 ± 0.12 is obtained from the fit.
Paper: The Hubble Constant Anchor Galaxy NGC 4258: Metallicity and Distance from Blue Supergiants
Authors: Rolf-Peter Kudritzki, Miguel A. Urbaneja, Fabio Bresolin, Lucas M. Macri, Wenlong Yuan, Siyang Li, Gagandeep S. Anand, Adam G. Riess
Figure caption: The observed distribution of R F555W values as a function of E F435W−F555W in NGC 4258, plotted using filled symbols. For reference, the values derived in the LMC by M. A. Urbaneja et al. (2017) are plotted using smaller open symbols.
Paper: The Radio Spectra of High-luminosity Compact Symmetric Objects: Implications for Studies of Compact Jetted Active Galactic Nuclei
Authors: P. V. de la Parra, A. C. S Readhead, T. Herbig, S. Kiehlmann, M. L. Lister, V. Pavlidou, R. A. Reeves, A. Siemiginowska, A. G. Sullivan, T. Surti, A. Synani, K. Tassis, G. B. Taylor, P. N. Wilkinson, M. F. Aller, R. D. Blandford, N. Globus, C. R. Lawrence, B. Molina, S. O'Neill, T. J. Pearson
Figure caption: Hazards of using spectral filters in selecting samples of jetted AGN for statistically rigorous studies. Maps of the 18 CSO-2s in the PR, CJ1, and PW complete samples arranged in order of increasing size, as in Figure 1, and with B1333+589, which has no spectroscopic redshift, plotted last. The objects with red contours have steep spectra, so they would be excluded in flat-spectrum samples (see text). VLBI observations of the steep-spectrum counterpart of VIPS, corresponding to the red sources, are needed for a definitive proof/disproof the sharp cutoff in CSO-2 sizes at ∼500 pc (see text). The objects in large black boxes do not have peaked spectra in the observed range, so they would be excluded in peaked-spectrum samples (see text). The map references are as follows: (1) M. L. Lister et al. (2018), (2) H. L. Maness et al. (2004), (3) G. B. Taylor et al. (1996), (4) M. Orienti & D. Dallacasa (2014), (5) W. Tschager et al. (1999), (6) M. Giroletti et al. (2003), (7) A. G. Polatidis et al. (1995), (8) C. Stanghellini et al. (1997), (9) G. B. Taylor et al. (2000), (10) G. B. Taylor et al. (2000), (11) J. M. Marr et al. (2014), (12) G. B. Taylor et al. (1996), (13) S. E. Tremblay et al. (2016), (14) M. L. Lister et al. (2018), (15) G. B. Taylor et al. (1996), (16) W. Xu et al. (1995), (17) M. Orienti et al. (2004), (18) C. Stanghellini et al. (2009).
Paper: The Radio Spectra of High-luminosity Compact Symmetric Objects: Implications for Studies of Compact Jetted Active Galactic Nuclei
Authors: P. V. de la Parra, A. C. S Readhead, T. Herbig, S. Kiehlmann, M. L. Lister, V. Pavlidou, R. A. Reeves, A. Siemiginowska, A. G. Sullivan, T. Surti, A. Synani, K. Tassis, G. B. Taylor, P. N. Wilkinson, M. F. Aller, R. D. Blandford, N. Globus, C. R. Lawrence, B. Molina, S. O'Neill, T. J. Pearson
Figure caption: The 5–8 GHz spectral indices of the PR, CJ1, and PW CSOs plotted against their size. The pink squares are the CSO-2.0s, the green circles are the CSO-2.1s, and the brown diamonds are the CSO-2.2s. The dotted line indicates spectral index α = 0, and the dashed line indicates α = −0.5. The solid line is the linear least-squares fit to the data.
Paper: The Radio Spectra of High-luminosity Compact Symmetric Objects: Implications for Studies of Compact Jetted Active Galactic Nuclei
Authors: P. V. de la Parra, A. C. S Readhead, T. Herbig, S. Kiehlmann, M. L. Lister, V. Pavlidou, R. A. Reeves, A. Siemiginowska, A. G. Sullivan, T. Surti, A. Synani, K. Tassis, G. B. Taylor, P. N. Wilkinson, M. F. Aller, R. D. Blandford, N. Globus, C. R. Lawrence, B. Molina, S. O'Neill, T. J. Pearson
Figure caption: Radio spectra of the 17 CSO-2s with spectroscopic redshifts in the PR, CJ1, and PW complete samples arranged in order of increasing largest physical size from left to right in successive rows. The dotted lines show spline fits to the data. The CSO-2 B1333+589 is plotted last, since it does not have a spectroscopic redshift, so we do not know its size. These spectra are taken from T. Herbig & A. C. S. Readhead (1992), A. C. S. Readhead et al. (1996), and the CATS database (O. V. Verkhodanov et al. 2005).
Paper: Fast Radio Bursts and Interstellar Objects
Authors: Dang Pham, Matthew J. Hopkins, Chris Lintott, Michele T. Bannister, Hanno Rein
Figure caption: The CHIME Catalog 1 distribution of FRB boxcar pulse width. On the top axis, we show the equivalent planetesimal size, R, assuming tensile strength s = 500 Pa and density ρ 0 = 3 g cm−3. Dashed vertical lines show the estimated sizes of two observed ISOs, 1I/‘Oumuamua and 2I/Borisov. The apparent sudden cutoff in FRB pulse duration at 100 ms is due to CHIME’s time resolution (0.983 ms; CHIME/FRB Collaboration et al. 2021).
Paper: GRB 211024B: An Ultra-long GRB Powered by Magnetar
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, Daniele B. Malesani, David Alexander Kann, Páll Jakobsson, Johan P. U. Fynbo, Elisabetta Maiorano, Andrea Rossi, Diego Paris, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Xing Gao, Jian-Yan Wei
Figure caption: Cut-outs of VLT/X-shooter two-dimensional spectrum of the host galaxy. The emission line at 10582 Å is [O III] (top right-hand panel), we can derive redshift of z = 1.113, which is supported by the weak signals of [O II] seen at 7875 Å (top left-hand panel) and H β  at 10271 Å (top middle panel). However, if we assume that the emission line at 10582 Å is H α  (bottom right-hand panel), implying a corresponding redshift of z = 0.612, we should expect to see [O III] at 8073 Å (bottom middle panel) and possibly H β  at 7836 Å (bottom left-hand panel), but no evidence of emission lines could be found in the expected region of the two-dimensional spectrum.
Paper: GRB 211024B: An Ultra-long GRB Powered by Magnetar
Authors: Shao-Yu Fu, Dong Xu, Wei-Hua Lei, Antonio de Ugarte Postigo, Daniele B. Malesani, David Alexander Kann, Páll Jakobsson, Johan P. U. Fynbo, Elisabetta Maiorano, Andrea Rossi, Diego Paris, Xing Liu, Shuai-Qing Jiang, Tian-Hua Lu, Jie An, Zi-Pei Zhu, Xing Gao, Jian-Yan Wei
Figure caption: Multiband prompt emission and afterglow light curve of GRB 211024B in logarithmic timescale. The inset shows the Swift/BAT light curve in linear timescale. Inverted triangles represent 3σ upper limits. Dashed lines depict the best-fit smoothly broken power-law models to the light curves. Note that the data have been subtracted for the host galaxy flux contribution and no Galactic extinction correction has been made.