adsabs/AstroCLIMB huggingface dataset:
Paper: On the Scarcity of Dense Cores (n > 105 cm−3) in High-latitude Planck Galactic Cold Clumps
Authors: Fengwei Xu, Ke Wang, Tie Liu, David Eden, Xunchuan Liu, Mika Juvela, Jinhua He, Doug Johnstone, Paul Goldsmith, Guido Garay, Yuefang Wu, Archana Soam, Alessio Traficante, Isabelle Ristorcelli, Edith Falgarone, Huei-Ru Vivien Chen, Naomi Hirano, Yasuo Doi, Woojin Kwon, Glenn J. White, Anthony Whitworth, Patricio Sanhueza, Mark G. Rawlings, Dana Alina, Zhiyuan Ren, Chang Won Lee, Ken'ichi Tatematsu, Chuan-Peng Zhang, Jianjun Zhou, Shih-Ping Lai, Derek Ward-Thompson, Sheng-Yuan Liu, Qilao Gu, Eswaraiah Chakali, Lei Zhu, Diego Mardones, L. Viktor Tóth
Figure caption: The gray histogram shows the distribution of 13,188 PGCCs. The blue histogram is for 793 high-latitude PGCCs, while the orange histogram is for the 70 HLPCs used in this work. A subpanel zooms in the H2 column density range of 1020.8–1022.2 cm−2.
Paper: Progenitors of Low-redshift Gamma-Ray Bursts
Authors: Vahé Petrosian, Maria G. Dainotti
Figure caption: Left: cosmic SFR from most comprehensive compilation by Madau & Dickinson (2014) and two examples of delayed SFR with power-law distribution of delay times, ﹩{\rm{\Phi }}{({\tau }_{d})\propto ({\tau }_{d}/{\tau }_{0})}^{-n}﹩, with indexes n = 1.0 and 3.0; from Paul (2018). Right: results of five independent determinations of LGRB FR of somewhat different samples, in the redshift range ∼1.5 < z < 4, using the EP-L method, all normalized at the peak value of the observed SFR (black solid line with selected error bars): from the top, (a) magenta, Lloyd-Ronning et al. (2019); (b) cyan, Yu et al. (2015); (c) green, Tsvetkova et al. (2017); (d) red, Petrosian et al. (2015); and (e) blue, Pescalli et al. (2016). With different degrees, all are showing higher LGRB FR than the SFR at low redshift (see the text for more detailed comparison of these works).
Paper: Progenitors of Low-redshift Gamma-Ray Bursts
Authors: Vahé Petrosian, Maria G. Dainotti
Figure caption: Left: same as Figure 1 left but showing the average value of five independent estimates plus Petrosian et al. (2015) results in red. The blue lines show the two low-redshift components obtained by subtracting the cosmic SFR from the observed ones. The magenta is the FR of SGRBs described in the right panel. Right: FR of SGRBs using most recent Swift sample of SGRBs with known redshift, using the procedures described in Dainotti et al. (2021c). Here σ(Z) is the cumulative (>Z) redshift distribution corrected for observational selection effects (blue dots), with arbitrary normalization. The blue curve is a smoothly broken power-law fit (with indicated form and parameters of the fit), from which we obtain the FR, ﹩\dot{\rho }(Z)﹩ analytically as described in the text.
Paper: Progenitors of Low-redshift Gamma-Ray Bursts
Authors: Vahé Petrosian, Maria G. Dainotti
Figure caption: The pie chart showing the LGRBs in purple, SGRBs in blue (with intrinsically short (IS) in yellow) adopted from Petrosian et al. (2015) and Dainotti et al. (2021d), respectively. The red shows fraction of all LGRBs for which the associated Type Ib/c supernovae have been observed.
Paper: On the Scarcity of Dense Cores (n > 105 cm−3) in High-latitude Planck Galactic Cold Clumps
Authors: Fengwei Xu, Ke Wang, Tie Liu, David Eden, Xunchuan Liu, Mika Juvela, Jinhua He, Doug Johnstone, Paul Goldsmith, Guido Garay, Yuefang Wu, Archana Soam, Alessio Traficante, Isabelle Ristorcelli, Edith Falgarone, Huei-Ru Vivien Chen, Naomi Hirano, Yasuo Doi, Woojin Kwon, Glenn J. White, Anthony Whitworth, Patricio Sanhueza, Mark G. Rawlings, Dana Alina, Zhiyuan Ren, Chang Won Lee, Ken'ichi Tatematsu, Chuan-Peng Zhang, Jianjun Zhou, Shih-Ping Lai, Derek Ward-Thompson, Sheng-Yuan Liu, Qilao Gu, Eswaraiah Chakali, Lei Zhu, Diego Mardones, L. Viktor Tóth
Figure caption: The peak intensity ﹩{\widetilde{I}}_{\nu }^{\mathrm{peak}}﹩ observed by SCUBA-2 across parameter space defined by the flat radius R flat ∈ [103, 104.5] au and the central density n  c  ∈ [103.5, 106] cm−3. The white curves mark 1σ, 3σ, and 9σ levels, while the black curves trace the same loci of synthetic model (no large-scale flux filtered out). The green dashed lines delineate the flat inner radius limits R flat ∈ [2500, 20000]. The shaded gray region indicates the permissible parameter interval of undetected prestellar cores should they exist. Blue and red stars show the L183 prestellar cores and other previously detected prestellar cores (Ward-Thompson et al. 1994, 1999; Kirk et al. 2005). The orange rectangles show two weakly detected cores in our fields. The green triangles show cores detected by Herschel in several HLPCs (Montillaud et al. 2015), but undetected by SCUBA-2.
Paper: Advancing Solar Magnetic Field Extrapolations through Multiheight Magnetic Field Measurements
Authors: Robert Jarolim, Benoit Tremblay, Matthias Rempel, Momchil Molnar, Astrid M. Veronig, Julia K. Thalmann, Tatiana Podladchikova
Figure caption: Evaluation of  B  ext as a function of geometrical height. The dotted horizontal lines indicate the average height of the τ surfaces. (a) Comparison to  B  ref for the baseline single-height extrapolations (potential, extrapolation, and extrapolation—PF) and the multiheight extrapolations (fixed height, mapped heights). (b) Same comparison as in (a) but for the realistic configurations (realistic vector, realistic split, and realistic LOS). The best value of all performance metrics is 1. (c) Evaluation of the force-freeness (σ  J ) and divergence-freeness (﹩{L}_{n,\mathrm{div}}﹩) of the extrapolated and reference magnetic fields as function of geometrical height. The best value of both metrics is 0. We compare the reference magnetic field (MURaM) and our single-height (extrapolation and extrapolation—PF) and multiheight extrapolations (fixed height, mapped heights, realistic vector, realistic split, and realistic LOS). Note that the value range in all plots is adjusted to enhance the visibility of differences among the extrapolation methods.
Paper: Advancing Solar Magnetic Field Extrapolations through Multiheight Magnetic Field Measurements
Authors: Robert Jarolim, Benoit Tremblay, Matthias Rempel, Momchil Molnar, Astrid M. Veronig, Julia K. Thalmann, Tatiana Podladchikova
Figure caption: Comparison between the height surfaces at which magnetograms are formed at constant optical depths τ in the MURaM simulation z ref(x, y, τ) and the height surfaces at which they are inferred by our model ﹩z^{\prime} (x,y,z)﹩. The columns show B ref,z (τ), the ground-truth z ref(x, y, τ), the results of the height model ﹩z^{\prime} (x,y,z)﹩, and a 2D histogram of ground-truth and mapped heights. The red lines in the 2D histograms indicate the ideal one-to-one correlation. From top to bottom, the rows show decreasing optical depths τ (i.e., increasing geometrical heights).
Paper: Advancing Solar Magnetic Field Extrapolations through Multiheight Magnetic Field Measurements
Authors: Robert Jarolim, Benoit Tremblay, Matthias Rempel, Momchil Molnar, Astrid M. Veronig, Julia K. Thalmann, Tatiana Podladchikova
Figure caption: Application of our multiheight magnetic field extrapolation to observations from 2011 March 9 16:34. (a) Reference EUV (left) and Hα (middle) observation together with the estimated height from our height-mapping model ﹩z^{\prime} ﹩ (right) in the coordinate frame of the SHARP region (NOAA AR 11166; SHARP 401). The vertical magnetic field strength is overlaid as contours at −1000 and 1000 G in blue and red, respectively. (b) Comparison of magnetic field lines modeled with a single-height (photospheric HMI) extrapolation (left) and an extrapolation that also includes SOLIS/VSM chromospheric magnetic field information (right). The region corresponds to the white rectangle in panel (a). The pink arrows indicate the position where we extract magnetic field lines. The blue arrow indicates the position where additional field lines were extracted for the single-height extrapolation. (c) Squashing factor and twist number of the single-height (left) and multiheight (right) extrapolated magnetic field. The orange dashed line in panel (a) indicates the position where the slices are extracted.
Paper: Advancing Solar Magnetic Field Extrapolations through Multiheight Magnetic Field Measurements
Authors: Robert Jarolim, Benoit Tremblay, Matthias Rempel, Momchil Molnar, Astrid M. Veronig, Julia K. Thalmann, Tatiana Podladchikova
Figure caption: Overview of our proposed method. We extend the method presented in Jarolim et al. (2023) by including a height-mapping model. The height-mapping model takes coordinate points (x, y, z) and adjusts the vertical component to ﹩z^{\prime} ﹩. From the corrugated surface, we sample both boundary values and random coordinates for our model training. The PINN and the height-mapping model are updated simultaneously by optimizing for the force-free condition and matching the boundary condition of the observed magnetograms.
Paper: Discovery of Magnetically Guided Metal Accretion onto a Polluted White Dwarf
Authors: Stefano Bagnulo, Jay Farihi, John D. Landstreet, Colin P. Folsom
Figure caption: The photospheric mass ratios Z/Mg for WD 0816–310, plotted as filled red circles with error bars, ordered by atomic mass, and compared to models. The ratios are the linear average of the two sets of elemental abundances determined from atmospheric model fitting (Table 3 in Kawka et al. 2021), where conservative errors of 0.1 dex have been adopted based on the internal consistency of the published values. The data are plotted relative to CI chondrites, which are frequently identified as a good match for the parent bodies of white dwarf pollution (see the main text). There are four models shown for comparison, with varying degrees of agreement, all based on the accretion of chondritic material. Model 1 (open black stars) is simply chondritic Z/Mg, such as might be directly observed in the star during an increasing abundance phase. Model 2 (open pink circles) is similar, but where these ratios are modified by steady-state accretion. Model 3 (open blue squares) assumes a decreasing phase of 0.76 Myr follows an increasing phase, and model 4 (filled blue squares) represents a decreasing phase of 0.31 Myr after a steady state.
Paper: Discovery of Magnetically Guided Metal Accretion onto a Polluted White Dwarf
Authors: Stefano Bagnulo, Jay Farihi, John D. Landstreet, Colin P. Folsom
Figure caption: Time-reversed, post-accretion evolution of the mass ratios Fe/Ca, Ca/Mg, and Fe/Mg for the accreted source material in WD 0816–310, normalized to the values of chondritic meteorites (Lodders 2003). Time on the x-axis corresponds to t − t 0 in Equation (C4), increases toward earlier epochs, and is normalized by the Mg sinking time. Two cases are plotted, where the photospheric mass ratios at t 0 are the result of (1) an increasing phase, shown by dashed lines, or (2) steady-state accretion, plotted as solid lines. All three ratios exhibit an underabundance of the heavier element at the current epoch, but as time moves into the past, these approach and eventually broadly match those of the primitive inner solar system. Comparing the two plotted models, the solid lines span a narrower range of times when crossing over with the chondritic model, thus supporting a steady state of accretion prior to its cessation. An additional figure and details are provided in Appendix C.
Paper: Discovery of Magnetically Guided Metal Accretion onto a Polluted White Dwarf
Authors: Stefano Bagnulo, Jay Farihi, John D. Landstreet, Colin P. Folsom
Figure caption: Panel (a): the best-fit sinusoidal model to the 〈B  z 〉 data of Table 1, having adopted a rotation period of 10.89426 days. The zero-point of the rotational phase is set arbitrarily at JD = 2460000.0. Other values of the rotational period in the range between 2 and 16 days lead to equally satisfactory fits with longitudinal curves of similar amplitude. Panel (b): the equivalent width of the lines in the region between 4357 and 4425 Å phased to the same rotation period and ephemeris as 〈B  z 〉.
Paper: Discovery of Magnetically Guided Metal Accretion onto a Polluted White Dwarf
Authors: Stefano Bagnulo, Jay Farihi, John D. Landstreet, Colin P. Folsom
Figure caption: Stokes spectra of WD 0816–310, with flux normalized to the continuum shown in panel (a) and V/I plotted in panel (b). The unsaturated lines are stronger when the longitudinal field is near maximum, and weaker when the field is close to zero. The presence of a field is revealed by the nonzero Stokes V profile, as detailed in Appendix A. For visual clarity, in panel (b) only the V/I profiles obtained on 2023 February 23 and March 26 are shown, and their uncertainties are plotted in cyan, offset by −7.5%. Line identification from Kawka et al. (2021).
Paper: Discovery of Magnetically Guided Metal Accretion onto a Polluted White Dwarf
Authors: Stefano Bagnulo, Jay Farihi, John D. Landstreet, Colin P. Folsom
Figure caption: All Very Large Telescope flux spectra of WD 0816–310 analyzed in this paper, normalized to the continuum, in a wavelength range dominated by Ca I and Fe I lines. Note that two spectra obtained on 2023 February 25, nearly overlapping, are plotted using the same color.
Paper: Discovery of Magnetically Guided Metal Accretion onto a Polluted White Dwarf
Authors: Stefano Bagnulo, Jay Farihi, John D. Landstreet, Colin P. Folsom
Figure caption: Equation (A1) correlations for the observing dates and spectral ranges as given in the figure panel labels. The slopes of the fitted lines are proportional to the mean longitudinal magnetic field.
Paper: NGDEEP Epoch 1: Spatially Resolved Hα Observations of Disk and Bulge Growth in Star-forming Galaxies at z ∼ 0.6–2.2 from JWST NIRISS Slitless Spectroscopy
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Bren E. Backhaus, Micaela B. Bagley, Yingjie Cheng, Nikko J. Cleri, Steven L. Finkelstein, Marc Huertas-Company, Mauro Giavalisco, Norman A. Grogin, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Michael V. Maseda, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Sandro Tacchella, Christina C. Williams, L. Y. Aaron Yung
Figure caption: Relation between spatially resolved sSFR and EW(Hα) (left) and between spatially resolved age and EW(Hα) (right). The 2D histograms include all pixels in the spatially resolved images for galaxies in our sample. In each panel, the orange symbols show the medians of the values and errors derived from the individual pixels. The red crosses show values derived from the integrated photometry. The median error of individual, spatially resolved pixels is indicated by the blue error bar in each panel. For comparison, the dashed lines show the relations derived from MOSDEF galaxies at z = 1.4–3.8 (Reddy et al. 2018; median and 1σ scatter). The median values of our spatially resolved measurements broadly agree with the results from the integrated emission of our galaxies. However, these are offset slightly to lower EW(Hα) compared to the relation from MOSDEF.
Paper: NGDEEP Epoch 1: Spatially Resolved Hα Observations of Disk and Bulge Growth in Star-forming Galaxies at z ∼ 0.6–2.2 from JWST NIRISS Slitless Spectroscopy
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Bren E. Backhaus, Micaela B. Bagley, Yingjie Cheng, Nikko J. Cleri, Steven L. Finkelstein, Marc Huertas-Company, Mauro Giavalisco, Norman A. Grogin, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Michael V. Maseda, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Sandro Tacchella, Christina C. Williams, L. Y. Aaron Yung
Figure caption: The stellar mass vs. the SED-derived SFR of our final sample. Galaxies are colored by their redshift. The two galaxies with X-ray-detected AGNs are marked by red diamonds, and the two with AGNs implied by their near-/mid-IR excess are marked with orange squares. For comparison, the SFMSs for galaxies at 1.0 < z < 1.5 and 1.5 < z < 2.0 from Whitaker et al. (2014) are shown in blue and orange, respectively, as labeled.
Paper: NGDEEP Epoch 1: Spatially Resolved Hα Observations of Disk and Bulge Growth in Star-forming Galaxies at z ∼ 0.6–2.2 from JWST NIRISS Slitless Spectroscopy
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Bren E. Backhaus, Micaela B. Bagley, Yingjie Cheng, Nikko J. Cleri, Steven L. Finkelstein, Marc Huertas-Company, Mauro Giavalisco, Norman A. Grogin, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Michael V. Maseda, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Sandro Tacchella, Christina C. Williams, L. Y. Aaron Yung
Figure caption: Left and middle: comparison between the stellar mass and SFR derived by summing the values from the bins in the spatially resolved “map(s)” with the same aperture as used for integrated photometry and the “integrated” values derived from integrated photometry. Right: comparison between the Hα EW average from the EW(Hα) “map(s)” and the “integrated” EW(Hα) measured by GRIZLI from the total 1D spectra. Note that statistical errors on the EW(Hα) values from the maps and from GRIZLI are smaller than the data points.
Paper: NGDEEP Epoch 1: Spatially Resolved Hα Observations of Disk and Bulge Growth in Star-forming Galaxies at z ∼ 0.6–2.2 from JWST NIRISS Slitless Spectroscopy
Authors: Lu Shen, Casey Papovich, Jasleen Matharu, Nor Pirzkal, Weida Hu, Bren E. Backhaus, Micaela B. Bagley, Yingjie Cheng, Nikko J. Cleri, Steven L. Finkelstein, Marc Huertas-Company, Mauro Giavalisco, Norman A. Grogin, Intae Jung, Jeyhan S. Kartaltepe, Anton M. Koekemoer, Jennifer M. Lotz, Michael V. Maseda, Pablo G. Pérez-González, Barry Rothberg, Raymond C. Simons, Sandro Tacchella, Christina C. Williams, L. Y. Aaron Yung
Figure caption: False-color images and Hα maps for the galaxies in our galaxy sample. For each galaxy, we show the RGB images using HST/ACS F814W, JWST/NIRISS F150W, and JWST/NIRCam F444W (left) and the Hα emission-line map constructed from the NIRISS slitless spectroscopy (right). The sample is ordered by increasing redshift. Each image is 2″ × 2″, corresponding to 13.4 × 13.4 kpc2 and 16.6 × 16.6 kpc2 at z = 0.6 and z = 2.2, respectively. The text inset lists the galaxy ID, redshift, and whether galaxies are identified with an AGN.
Paper: The Strength and Shapes of Contact Binary Objects
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: Plots showing the minimum normalized cohesion as a function of (a) the prolateness of the secondary lobe at different size ratios; (b) the oblateness of the secondary lobe at different size ratios; (c) the size ratio for prolate secondary lobes; and (d) the size ratio for prolate secondary lobes. Our contact binaries are plotted as data points, with asteroids shown as diamonds, comets as stars, and KBOs as squares.
Paper: The Strength and Shapes of Contact Binary Objects
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: The minimum friction angle as a function of normalized cohesion for the case of two equal-sized spheres. We show results for various density ratios, and the solution for the cohesionless equal-mass case is plotted as a dashed line.
Paper: The Strength and Shapes of Contact Binary Objects
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: The minimum normalized cohesion as a function of (a) prolateness and (b) oblateness of the secondary lobe for different values of the density ratio. The curves assume a size ratio of D 2/D 1 = 0.7.
Paper: The Strength and Shapes of Contact Binary Objects
Authors: Alex J. Meyer, Daniel J. Scheeres
Figure caption: The friction angle as a function of cohesion for our 11 contact binaries. These curves represent the critical combinations of friction angle and bulk cohesion that result in structural failure of the secondary lobe of the contact binary.
Paper: The Very Early Soft X-Ray Plateau of GRB 230307A: Signature of an Evolving Radiative Efficiency in Magnetar Wind Dissipation?
Authors: Shu-Qing Zhong, Long Li, Di Xiao, Hui Sun, Bin-Bin Zhang, Zi-Gao Dai
Figure caption: The spectral evolution of LEIA X-ray data plotted from the extended data table 1 of Sun et al. (2023).
Paper: The Very Early Soft X-Ray Plateau of GRB 230307A: Signature of an Evolving Radiative Efficiency in Magnetar Wind Dissipation?
Authors: Shu-Qing Zhong, Long Li, Di Xiao, Hui Sun, Bin-Bin Zhang, Zi-Gao Dai
Figure caption: The corner plot for the X-ray plateau of GRB 230307A.
Paper: The Very Early Soft X-Ray Plateau of GRB 230307A: Signature of an Evolving Radiative Efficiency in Magnetar Wind Dissipation?
Authors: Shu-Qing Zhong, Long Li, Di Xiao, Hui Sun, Bin-Bin Zhang, Zi-Gao Dai
Figure caption: The best joint fitting for the multiwavelength afterglow and kilonova light curves of GRB 230307A by combining the standard external forward-shock model and the kilonova model. The early X-ray (1keV) data before 300 s is scaled from the LEIA data and the late is scaled from the Swift XRT, XMM-Newton, and Chandra data. The early X-ray data as a plateau is fitted by the MIGMAD model (black dashed–dotted line), the same as the left panel of Figure 3. The data points denoted by an inverted triangle are upper limits. The GRB afterglow (AG) components are denoted by dashed lines.
Paper: The Very Early Soft X-Ray Plateau of GRB 230307A: Signature of an Evolving Radiative Efficiency in Magnetar Wind Dissipation?
Authors: Shu-Qing Zhong, Long Li, Di Xiao, Hui Sun, Bin-Bin Zhang, Zi-Gao Dai
Figure caption: Left panel: the best-fit results with an evolving radiative efficiency via the MIGMAD model (black solid line) and with a constant efficiency (orange dashed line). Right panel: the corresponding evolving and constant efficiencies. The time-averaged value ﹩\langle {\mathrm{log}}_{10}({\eta }_{X})\rangle =-2.06﹩ of the evolving efficiency is plotted with a black dashed line.
Paper: Evidence for Evolved Stellar Binary Mergers in Observed B-type Blue Supergiants
Authors: Athira Menon, Andrea Ercolino, Miguel A. Urbaneja, Daniel J. Lennon, Artemio Herrero, Ryosuke Hirai, Norbert Langer, Abel Schootemeijer, Emmanouil Chatzopoulos, Juhan Frank, Sagiv Shiber
Figure caption: HRD showing the evolutionary tracks of merger-born (a) and born-alone (b) stellar models during their BSG phase (log T eff ⪆ 4.0), along with the observed data sample (symbols as described in Figure 2). The observed HRD position of Sk-69°202 (Woosley et al. 1988) is also added. Errors of the MS sample are about 0.1 dex for both log L/L⊙ and log T eff. Tick marks on the evolutionary tracks indicate intervals of 0.1 Myr in time in the post-MS BSG phase. (a): The tracks of a selection of our merger models from Table 2 including the core He-burning BSG phase (light blue shading), core C-depletion location and their corresponding mass (rounded off M C-dep values). Pre-supernova BSGs are indicated as blue stars, where those with log T eff ⪅ 4.3 are connected to their corresponding core He-burning phase via blue dotted lines. Pre-supernova RSGs (log T eff < 4.0) are not indicated and are only connected by red dotted lines to their core He-burning phase. (b): Born-alone stellar tracks indicating the classical (yellow lines) and high-luminosity (light brown lines) blue-loop phase (blue dotted lines), along with their mass range in this phase. For reference, the ZAMS and TAMS curves and evolutionary tracks (light gray lines) of rotating single-star models with v i,rot ≈ 220 km s−1 from Brott et al. (2011) are also added.