adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of X-Ray Polarized Emission and Accretion-disk Winds with IXPE and NICER in the Black Hole X-Ray Binary 4U 1630−47
Authors: Divya Rawat, Akash Garg, Mariano Méndez
Figure caption: The polarization degree, PD, polarization angle, PA, and normalized stokes parameter, Q/I and U/I, of 4U 1630−47 measured with the three detectors, DU1, DU2, DU3, on board IXPE. The measurements were obtained using the PCUBE tool in the 2–8 keV band. The contours are at 68.27%, 95.45%, and 99.73% confidence levels for both Stokes parameters.
Paper: The Universe is at Most 88% Neutral at z = 10.6
Authors: Sean Bruton, Yu-Heng Lin, Claudia Scarlata, Matthew J. Hayes
Figure caption: Left: the posterior distribution of x H I. Right: the reionization history. The dash and solid black lines are constant f esc models with Schechter LF (Bouwens et al. 2021) and double power-law LF (Harikane et al. 2023). The red and blue lines are the models where bright and faint galaxies have higher escape fraction, respectively. The observational constraints are shown in white markers, and the constraint in constraint inferred by GN-z11 is marked as yellow star.
Paper: The Universe is at Most 88% Neutral at z = 10.6
Authors: Sean Bruton, Yu-Heng Lin, Claudia Scarlata, Matthew J. Hayes
Figure caption: The probability of EW(Lyα) for varying values of x H I, given that the galaxy has Lyα emission (i.e., excluding nonemitters). The solid lines are empirically taken from the simulation after IGM attenuation—the dashed lines are an attempt to fit the first term of Equation (1) to the distribution. The fit fails when the universe is partially neutral because there is excess probability of having high EWLyα  compared to an exponential cutoff.
Paper: The Universe is at Most 88% Neutral at z = 10.6
Authors: Sean Bruton, Yu-Heng Lin, Claudia Scarlata, Matthew J. Hayes
Figure caption: EW(Lyα) as a function of M UV. The red squares, green stars, and blue pentagons are the measurements from the MUSE HUDF survey at redshift z = 3.6, 4.9, and 6.0, respectively. The magenta triangles are the median measurements from De Barros et al. (2017). The black circles are the results from our model, after matching the MUSE HUDF survey flux limit.
Paper: The Spin–Orbit Misalignment of TOI-1842b: The First Measurement of the Rossiter–McLaughlin Effect for a Warm Sub-Saturn around a Massive Star
Authors: Kyle Hixenbaugh, Xian-Yu Wang, Malena Rice, Songhu Wang
Figure caption: Stellar mass vs. planet mass for systems obtained from Albrecht et al. (2022) and the TEPCat catalog (Southworth 2011). Unfilled circles denote aligned planets, while triangles denote misaligned planets. TOI-1842 is plotted in red. The trend toward alignment that is confined to Jupiter-mass planets orbiting cool, low-mass stars with all other mass combinations showing mixed alignment. Misaligned systems all fall below the red dashed line representing the 1σ upper error to a linear fit performed on the misaligned systems.
Paper: The Earliest Stage of Galactic Star Formation
Authors: Charles L. Steinhardt, Vadim Rusakov, Thomas H. Clark, Andrei Diaconu, John Forbes, Conor McPartland, Albert Sneppen, John Weaver
Figure caption: Density plots showing the best-fit Sérsic profile properties made with Hubble Wide-Field Camera 3 (WFC3) observations in the F814W filter for galaxies at 0.8 < z < 0.9 (i.e., ∼0.44 μm in the rest frame). The panels show median quantities in each T SF-sSFR bin (left to right): the best-fit Sérsic index; the calculated aperture radius containing 20% of light, R 20, using definitions from Miller et al. (2019); the best-fit effective radius, R 50; and the calculated aperture radius containing 80% of light, R 80. The plot indicates the following behaviors: (1) most high-sSFR systems are dominated by a disk+bulge structure or an irregular one (e.g., due to mergers), while the quiescent ones have a compact luminous bulge; (2) the change of physical sizes from R 20 to R 50 and to R 80 shows that the high-T SF objects have the smallest overall profiles, in contrast to large quiescent galaxies. This suggests an interpretation in which the core-forming galaxies are the smallest main-sequence galaxies that grow their stellar bulge and disk over time. Then the supposed transition to elliptical galaxies is associated with the gradual compaction of their bulge and dissipation of the disk by some instability, such as due to mergers. Bins with fewer than five data points are shown as dots.
Paper: The Earliest Stage of Galactic Star Formation
Authors: Charles L. Steinhardt, Vadim Rusakov, Thomas H. Clark, Andrei Diaconu, John Forbes, Conor McPartland, Albert Sneppen, John Weaver
Figure caption: Gas (T SF; top) and dust (bottom) temperatures for COSMOS galaxies as a function of stellar mass M ⋆ and SFR in four redshift windows. The T SF are adapted from Steinhardt et al. (2022c). The dust temperature measurements are based on the analysis of the far-infrared and submillimeter stacked observations made with the Herschel Space Observatory and are reproduced (B. Magnelli 2023, private communication) from Magnelli et al. (2014). For ease of comparison, all panels use the Galactic IMF-derived COSMOS2015 stellar masses and SFR even though a modified IMF will also modify both SFRs and stellar mass. The dashed lines show the best-fit main-sequence ridge lines with the shaded region showing one standard deviation uncertainty from Speagle et al. (2014). Both gas and dust temperatures exhibit a similar gradient, increasing toward lower stellar masses and higher SFR at all redshifts. The two measurements are farther in approximate quantitative agreement, despite the two methods each having significant but independent sources of uncertainty. This is consistent with an equilibrium between cool molecular gas and dust temperatures, as well as the interpretation that T SF is indeed a proxy for temperature.
Paper: The Earliest Stage of Galactic Star Formation
Authors: Charles L. Steinhardt, Vadim Rusakov, Thomas H. Clark, Andrei Diaconu, John Forbes, Conor McPartland, Albert Sneppen, John Weaver
Figure caption: The T SF-sSFR diagram, analogous to a H–R diagram for galaxies, for COSMOS2015 galaxies at 0.7 < z < 1.8 showing bins with at least ten data points. Panels are colored by the median (left) redshift; (top right) stellar mass; and (bottom right) age of the stellar population. Moving from top right to bottom left, galaxies become more massive with older stellar populations and are more commonly observed at later times. Although no morphological information was used to produce the diagram, this is also a morphological sequence (see also Figure 4). The diagram is therefore interpreted as an evolutionary track followed by typical galaxies, with core-forming galaxies identified as the initial stage of star formation. The dashed region in the left panel indicates that the IMF cannot be recovered at T SF ≲ 25 K (Sneppen et al. 2022) although observational evidence (see Section 3.2) indicates that the IMF may be even bottom heavier than T SF ∼ 25 K.
Paper: The Spin–Orbit Misalignment of TOI-1842b: The First Measurement of the Rossiter–McLaughlin Effect for a Warm Sub-Saturn around a Massive Star
Authors: Kyle Hixenbaugh, Xian-Yu Wang, Malena Rice, Songhu Wang
Figure caption: The measured Rossiter–McLaughlin effect for TOI-1842 b suggests a significant misaligned orbit with a sky-projected obliquity of ﹩\lambda =-68\buildrel{\circ}\over{.} {1}_{-14.7}^{+21.2}﹩. The blue points with black error bars represent the measured in-transit radial velocities and their errors. The median model of the R-M effect is shown in red, with the corresponding 1σ uncertainty shown in lighter red. This model was obtained from a global fit of all available radial-velocity and transit data.
Paper: The Earliest Stage of Galactic Star Formation
Authors: Charles L. Steinhardt, Vadim Rusakov, Thomas H. Clark, Andrei Diaconu, John Forbes, Conor McPartland, Albert Sneppen, John Weaver
Figure caption: Hubble WFC3 observations in the F814W and F160W filters for core-forming (top), typical star-forming (middle), and quiescent (bottom) galaxies randomly selected from the highest signal-to-noise ratio objects from the COSMOS2015 survey at z ∼ 0.8. The T SF-sSFR diagram (Figure 2) is interpreted to indicate an evolutionary sequence from top to bottom. The core-forming galaxies are significantly more compact, and the blue color indicates a young stellar population throughout these galaxies. Typical star-forming galaxies have blue colors and young stellar populations when unresolved but also exhibit older populations in their centers than at larger radii. Quiescent galaxies have old stellar populations throughout. This morphology supports the interpretation of the T SF-sSFR diagram track as an evolutionary sequence, running from core formation to typical star formation, and finally to quiescence.
Paper: The Decoupling of Binaries from Their Circumbinary Disks
Authors: Alexander J. Dittmann, Geoffrey Ryan, M. Coleman Miller
Figure caption: The accretion rates, normalized by ﹩{\dot{M}}_{0}=3\pi \nu {{\rm{\Sigma }}}_{0}﹩, for our ν 0 = 0.03 and ν 0 = 0.003 simulations. The leftmost panels display the accretion rates over the course of the entire simulations, after the initial burn-in stage. The other panels in each row focus on narrower windows, displaying shorter-term variation in the binary accretion rate. Vertical dashed lines indicate the time at which each binary reaches a  b =a  d . We note that because the initial binary orbital period Ω0 = 10−3 c 3 G −1 M −1, ﹩2\pi {{\rm{\Omega }}}_{0}^{-1}\approx 8.6(M/{10}^{6}\,{M}_{\odot })﹩ hours. While the accretion rate in the high-viscosity case remains significant until very late in the inspiral, sharply declining accretion rates in systems that decouple at larger separations should identify such systems.
Paper: The Decoupling of Binaries from Their Circumbinary Disks
Authors: Alexander J. Dittmann, Geoffrey Ryan, M. Coleman Miller
Figure caption: Lomb–Scargle periodograms of the accretion rate time series from our ν 0 = 0.01 and ν 0 = 0.001 simulations during three epochs: blue lines plot the periodograms over the first ﹩50\pi {{\rm{\Omega }}}_{0}^{-1}﹩ after burn-in, orange lines plot the periodograms over a period of ﹩50\pi {{\rm{\Omega }}}_{0}^{-1}﹩ centered on the time of decoupling, and red lines plot the periodogram over the final ﹩50\pi {{\rm{\Omega }}}_{0}^{-1}﹩ of each simulation before merger. The left column plots periodograms in the lab frame of the binary. Because the binary orbital frequency changes rapidly at late times, we also plot in the right column periodograms of a rescaled accretion rate time series, in terms of the instantaneous binary frequency and orbital phase. All periodogram amplitudes are renormalized to peak at 1. Accretion rate periodicity continues until late in the inspiral in systems that decouple at later times, whereas in lower-viscosity disks virtually no significant periodicity persists.
Paper: The Decoupling of Binaries from Their Circumbinary Disks
Authors: Alexander J. Dittmann, Geoffrey Ryan, M. Coleman Miller
Figure caption: The top panel displays the measurements of the cavity semimajor axis as a function of binary semimajor axis from each of our simulations. The bottom panel displays our inferences of the characteristic binary semimajor axis at decoupling compared with timescale-based predictions (Equation (5), a solid green line) and velocity-based predictions (Equation (6), a dashed orange line). Although decoupling is a gradual process, the characteristic binary semimajor axis at which it occurs is described well by Equation (6).
Paper: The Decoupling of Binaries from Their Circumbinary Disks
Authors: Alexander J. Dittmann, Geoffrey Ryan, M. Coleman Miller
Figure caption: Surface density profiles from our ν 0 = 0.03 and ν 0 = 0.003 simulations over the course of their inspirals, during which decoupling occurs around a  b  ∼ 14 R  g  and a  b  ∼ 56 R  g  respectively. Each panel is 800 R  g  long in each dimension. The flow of gas around the binary near merger is qualitatively different when the system decouples at earlier times.
Paper: The Decoupling of Binaries from Their Circumbinary Disks
Authors: Alexander J. Dittmann, Geoffrey Ryan, M. Coleman Miller
Figure caption: The evolution of black hole binaries in the LISA band at z = 2 over the final 3 yr prior to merger. Purple, green, and blue dots mark the points where each binary reaches a  d , given by Equation (7), for ν 0 = {0.1, 0.01, 0.001} respectively. The dashed markings along each line mark 1 yr, 1 month, 1 day, and 1 hr before merger. Depending on the system mass and disk viscosity, many binaries might decouple from their disks while emitting in the LISA band. This could identify the host galaxy of the merger, facilitating multimessenger observations.
Paper: Negligible Effects of Baryons on the Angular Momentum Scaling Relations of Galactic Dark Matter Halos
Authors: S. Michael Fall, Vicente Rodriguez-Gomez
Figure caption: Ratios of mass M h (top panel), specific angular momentum j h (middle panel), and spin parameter ﹩{\lambda }^{{\prime} }﹩ (bottom panel) for halos in the FP run to the same quantities for the individually matched halos in the DMO run plotted against mass M h,DMO for TNG100 at z = 0. The color scale indicates the number of halos in each 2D bin. The red horizontal lines indicate equality, while the black lines represent the running median relations and 16th–84th percentile ranges. This diagram shows directly the effects of baryons on the halo properties M h, j h, and ﹩{\lambda }^{{\prime} }﹩. Note the relatively small and nearly constant median offset of ﹩{\lambda }_{\mathrm{FP}}^{{\prime} }﹩ from ﹩{\lambda }_{\mathrm{DMO}}^{{\prime} }﹩, indicating that the halo relation ﹩{j}_{{\rm{h}}}\propto {M}_{{\rm{h}}}^{\alpha }﹩ with α ≈ 2/3 is preserved by baryonic processes.
Paper: Negligible Effects of Baryons on the Angular Momentum Scaling Relations of Galactic Dark Matter Halos
Authors: S. Michael Fall, Vicente Rodriguez-Gomez
Figure caption: Specific angular momentum j h plotted against mass M h for halos in the TNG50 DMO and FP runs at z = 0 (upper left and upper right panels, respectively) and the FP run at z = 0 with selection criteria based on the stellar masses and morphologies of galaxies: M * ≥ 109 M ⊙ (lower left panel) and M * ≥ 109 M ⊙ and κ rot ≥ 0.5 (lower right panel). The last of these replicates the selection criteria adopted by Du et al. (2022). The color scale indicates the number of halos in each 2D bin. The red lines represent the best-fit linear relations, while the black lines represent the running median relations and 16th–84th percentile ranges. Note the close similarity of the halo j–M relations in the DMO and FP runs and the steeper fitted slopes in the samples selected by stellar properties.
Paper: JWST NIRSpec Observations of Supernova 1987A—From the Inner Ejecta to the Reverse Shock
Authors: J. Larsson, C. Fransson, B. Sargent, O. C. Jones, M. J. Barlow, P. Bouchet, M. Meixner, J. A. D. L. Blommaert, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Hjorth, J. Jaspers, P. J. Kavanagh, O. Krause, R. M. Lau, L. Lenkić, O. Nayak, A. Rest, T. Temim, T. Tikkanen, R. Wesson, G. S. Wright
Figure caption: Median flux of the He I 1.083 μm emission from the RS at different positions along the ER. This quantifies the geometry of the emission region and shows the variations between different positions. The fluxes are shown as a function of the velocity in the plane of the ER (x-axis) and velocity perpendicular to this plane (y-axis), implying that the ER is viewed edge on. The y-axis is defined such that positive velocities are directed north and away from the observer, while negative ones are directed south and toward the observer. Each “image” was produced from a 20° interval along the ER, centered at the position angles given in the legends, where 0° is directly toward the observer. The sketches in the lower right corners show the positions of the segments in the observer frame. Positive (negative) angles are in the western (eastern) parts of the ER. The ER segments included in the top (bottom) rows are on the near (far) side of the ER with respect to the observer. The white circle shows the radius of the ER determined from HST data. The region covering V ER plane ≲ 4000 km s−1 and V ER normal ≲ ±6000 km s−1 is contaminated by emission from the inner ejecta, dominated by the Paγ 1.094 μm and [Si I] 1.099 μm lines. There are also residual artifacts in the “images” at 0 and 180°.
Paper: JWST NIRSpec Observations of Supernova 1987A—From the Inner Ejecta to the Reverse Shock
Authors: J. Larsson, C. Fransson, B. Sargent, O. C. Jones, M. J. Barlow, P. Bouchet, M. Meixner, J. A. D. L. Blommaert, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Hjorth, J. Jaspers, P. J. Kavanagh, O. Krause, R. M. Lau, L. Lenkić, O. Nayak, A. Rest, T. Temim, T. Tikkanen, R. Wesson, G. S. Wright
Figure caption: Upper panel: comparison between the NIRSpec ejecta spectrum (blue) and a spectral model (red, see text for details), including H I, H2, He I, Si I, Fe I, and Fe II. The gray line shows the continuum, including synchrotron emission, as well as free–free, bound–free, and two-photon continua from H I, He I, and He II. Lower panel: contributions of the different ions to the spectrum in the upper panel. Note the large number of H2 lines from the PDR model Qm3o from Draine & Bertoldi (1996). Note also that we have not included any line emission from the RS, which is most clearly seen in the very broad wings of the He I 1.083 μm and Paα lines. Scattered emission from the ER adds narrow components in some lines, which are especially strong for H I and He I. The lines at ∼1.035 μm may be a blend of S I and Fe I, while the feature at ∼3.88 μm coincides with lines of the same atoms. These lines come from high levels, not included in our model atoms.
Paper: JWST NIRSpec Observations of Supernova 1987A—From the Inner Ejecta to the Reverse Shock
Authors: J. Larsson, C. Fransson, B. Sargent, O. C. Jones, M. J. Barlow, P. Bouchet, M. Meixner, J. A. D. L. Blommaert, A. Coulais, O. D. Fox, R. Gastaud, A. Glasse, N. Habel, A. S. Hirschauer, J. Hjorth, J. Jaspers, P. J. Kavanagh, O. Krause, R. M. Lau, L. Lenkić, O. Nayak, A. Rest, T. Temim, T. Tikkanen, R. Wesson, G. S. Wright
Figure caption: Spectrum extracted from a 0.13 arcsec2 region in the SW part of the ER with the detected coronal lines marked. We also show the full series of detected lines from the Brackett, Pfund, and Humphreys series in blue. All coronal line identifications are included in Table 2. The uncertainties in the laboratory wavelengths are shown as horizontal error bars. To show the faint emission lines, we limit the range of the y-axis compared to Figure 2. The flux scale is here linear while that in Figure 2 is logarithmic.
Paper: The Population of the Galactic Center Filaments: Position Angle Distribution Reveals a Degree-scale Collimated Outflow from Sgr A* along the Galactic Plane
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood
Figure caption:  Top panel: a mosaic MeerKAT image of the GC at 20 cm with a 4″ resolution (Heywood et al. 2022). Bottom Panel: similar to top but filtered image with a 6.″4 resolution (Yusef-Zadeh et al. 2022a). The units are reported in Jy beam−1, where the beam area is that of the original 4″ beam. The filtering process reduces the numerical value of the brightness in filament pixels by a factor of ∼0.13, with large variations due to the effect of the background removal. This factor is not applied to the filtered image intensities. Supernova remnants and H II regions identified as red circles in both top and bottom panels are excluded in the analysis.
Paper: The Population of the Galactic Center Filaments: Position Angle Distribution Reveals a Degree-scale Collimated Outflow from Sgr A* along the Galactic Plane
Authors: F. Yusef-Zadeh, R. G. Arendt, M. Wardle, I. Heywood
Figure caption: (a) Color-coded position angles for all identified short and long filaments in the mosaic image (Figure 1) are displayed (east of Galactic north is positive). (b) Similar to (a) except that the color table is restricted, indicating a preferred direction of short filaments L < 66″. The filament PAs run between 60° and 120°. Bottom panel: similar to (b) except that the color table is restricted, selecting only long filaments L > 66″ with PAs between −60° and 60°.
Paper: CEERS Key Paper. V. Galaxies at 4 < z < 9 Are Bluer than They Appear–Characterizing Galaxy Stellar Populations from Rest-frame ∼1 μm Imaging
Authors: Casey Papovich, Justin W. Cole, Guang Yang, Steven L. Finkelstein, Guillermo Barro, Véronique Buat, Denis Burgarella, Pablo G. Pérez-González, Paola Santini, Lise-Marie Seillé, Lu Shen, Pablo Arrabal Haro, Micaela B. Bagley, Eric F. Bell, Laura Bisigello, Antonello Calabrò, Caitlin M. Casey, Marco Castellano, Katherine Chworowsky, Nikko J. Cleri, Luca Costantin, M. C. Cooper, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Benne W. Holwerda, Taylor A. Hutchison, Jeyhan S. Kartaltepe, Lisa J. Kewley, Allison Kirkpatrick, Dale D. Kocevski, Anton M. Koekemoer, Rebecca L. Larson, Arianna S. Long, Ray A. Lucas, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephanie M. Urbano Stawinski, Benjamin J. Weiner, Stephen M. Wilkins, L. Y. Aaron Yung, Jorge A. Zavala
Figure caption: Comparison of stellar masses and SFRs derived from the SED modeling for galaxies including the MIRI F560W and F770W data and those without the MIRI data. The top set of panels show the comparison for the stellar mass. The bottom set of panels show the comparison for the SFR. In each row, the left panel shows the direct comparison, where the dashed line shows the one-to-one relation. The right panel shows the logarithmic difference, defined as ﹩{\rm{\Delta }}\mathrm{log}{M}_{* }^{\mathrm{with}\,\mathrm{MIRI}}-\mathrm{log}{M}_{* }^{\mathrm{without}\,\mathrm{MIRI}}﹩ (and similarly for the SFR). The symbols are color-coded by redshift (using the right panel). In the right panel, the large rectangular boxes and error bars show the median value (and scatter) in two bins of redshift (4 < z < 6 and 6 < z < 10). The values for these are given in Table 6. Adding the MIRI data generally lowers the SFRs and stellar masses of these galaxies, though the scatter is significant. The median offset is larger for galaxies at higher redshifts.