adsabs/AstroCLIMB huggingface dataset:
Paper: The Candidate Progenitor Companion Star of the Type Ib/c SN 2013ge
Authors: Ori D. Fox, Schuyler D. Van Dyk, Benjamin F. Williams, Maria Drout, Emmanouil Zapartas, Nathan Smith, Dan Milisavljevic, Jennifer E. Andrews, K. Azalee Bostroem, Alexei V. Filippenko, Sebastian Gomez, Patrick L. Kelly, S. E. de Mink, Justin Pierel, Armin Rest, Stuart Ryder, Niharika Sravan, Lou Strolger, Qinan Wang, Kathryn E. Weil
Figure caption: Photometry of SN 2013ge obtained in 2020 (red circle; Table 1). For comparison, overplotted are several different stellar models scaled to roughly the observed F275W value with an applied extinction E(B − V) = 0.067 mag and R  V  = 3.1. Also shown are the synthetic photometry for the B5 I model (black circle). Specific stellar model properties are as follows (temperature, log Z metallicity, and log g gravity): B5 I (14,000, −0.3, 2.44), A0 I (9730, −0.3, 2.14), B0 I (19,000, −0.3, 3.0), B0 III (29,000, −0.3, 3.5), and B5 III (15,000, −0.3, 3.5). The left and right ordinate axes are not directly aligned owing to the fact that any flux corresponds to a different Vega magnitude in each filter. The overplotted models should only be used for qualitative comparisons. While no model from the catalog matches perfectly to the observations, we find the SED is most consistent with a B5 I (supergiant) or III (giant).
Paper: The Candidate Progenitor Companion Star of the Type Ib/c SN 2013ge
Authors: Ori D. Fox, Schuyler D. Van Dyk, Benjamin F. Williams, Maria Drout, Emmanouil Zapartas, Nathan Smith, Dan Milisavljevic, Jennifer E. Andrews, K. Azalee Bostroem, Alexei V. Filippenko, Sebastian Gomez, Patrick L. Kelly, S. E. de Mink, Justin Pierel, Armin Rest, Stuart Ryder, Niharika Sravan, Lou Strolger, Qinan Wang, Kathryn E. Weil
Figure caption: Single-star evolutionary tracks of 10 and 12 M ⊙ stars in MIST for different HST/WFC3 filters, plotted in both (left) temperature and (right) color space. Overplotted are values for SN 2013ge (solid circles), in addition to the calculated limiting magnitudes of our designed observations (dashed horizontal lines). The source detected at the position of SN 2013ge is redward of the MS and consistent with a ∼12 M ⊙ B5 I star crossing the Hertzsprung gap (HG) toward becoming a giant, with an absolute magnitude F275W = −6.5 (Vega).
Paper: A Model of Homologous Confined and Ejective Eruptions Involving Kink Instability and Flux Cancellation
Authors: Alshaimaa Hassanin, Bernhard Kliem, Norbert Seehafer, Tibor Török
Figure caption: Ejective eruption. (a)–(f) Magnetogram, B  z (x, y, 0, t  i ), and field lines of the re-formed flux rope (green/brown; drawn from each of the original rope’s footprints) and of the reconnecting flux that forms a new rope (rainbow colors; a subset is shown in Figure 2). The displayed volume is 73 (a)–(d), 103 (e), and 203 (f). (g)–(i) Vertical cuts, centered at the z-axis and rotated by ϕ (in degrees), of the force-free parameter, α = J ∥/B, and normal (out-of-plane) current-density component, J n. Overlaid are in-plane velocity vectors, u  sz , and field vectors, B  sz .
Paper: A Model of Homologous Confined and Ejective Eruptions Involving Kink Instability and Flux Cancellation
Authors: Alshaimaa Hassanin, Bernhard Kliem, Norbert Seehafer, Tibor Török
Figure caption: (a)–(c) Rise profiles of the fluid elements at the apex points of the re-formed (black) and new (blue) flux ropes after imposing converging photospheric flows (deceleration shown dotted). The latter fluid element is formed at the z-axis due to the inflows and reconnection and, therefore, cannot be traced from t = 0. (d) Magnetic flux, (e) magnetic, and (f) kinetic energies in the box. Vertical dashed (dotted) lines mark the onset of instability (“flare” reconnection at the z-axis).
Paper: A Model of Homologous Confined and Ejective Eruptions Involving Kink Instability and Flux Cancellation
Authors: Alshaimaa Hassanin, Bernhard Kliem, Norbert Seehafer, Tibor Török
Figure caption: Confined eruption. (a) Rise profile of the fluid element at the apex of the initial flux rope’s magnetic axis. (b)–(e) Main features of the confined eruption.
Paper: A Model of Homologous Confined and Ejective Eruptions Involving Kink Instability and Flux Cancellation
Authors: Alshaimaa Hassanin, Bernhard Kliem, Norbert Seehafer, Tibor Török
Figure caption: Profiles of u  z (0, 0, z, t i). (a) Snapshots before, at peak of, and after “tether-cutting” reconnection. (b) Before and immediately after the onset of “flare” reconnection flows at the z-axis. (c) Rapid rise of flare reconnection. Black and blue symbols mark the flux rope apex positions plotted in Figure 4(a).
Paper: A Model of Homologous Confined and Ejective Eruptions Involving Kink Instability and Flux Cancellation
Authors: Alshaimaa Hassanin, Bernhard Kliem, Norbert Seehafer, Tibor Török
Figure caption: Transformation of sheared into twisted coronal flux by converging motions and flux cancellation at the photosphere.
Paper: A Tale of Two Circularization Periods
Authors: J. J. Zanazzi
Figure caption: Eccentricity data from Kepler (purple points) and TESS (white triangles), with contours denoting smoothed kernel density estimates of the eccentricity measurements. The dashed orange line denotes typical errors in ﹩| e\cos \omega | ﹩ measurements in the Kepler/TESS data set, while light-brown points denote removed binaries with morph > 0.5 (see text for discussion). White solid and dotted lines denote fits for the circularization (P circ) and envelope (P env) periods. We take N  s  = 3000, with the other parameter fits being ﹩{\alpha }_{\mathrm{circ}}={0.21}_{-0.06}^{+0.79}﹩, ﹩{\beta }_{\mathrm{circ}}={0.8}_{-0.7}^{+1.2}﹩, ﹩{\alpha }_{\mathrm{env}}={0.39}_{-0.05}^{+0.06}﹩, and ﹩{\beta }_{\mathrm{env}}={1.5}_{-0.6}^{+1.0}﹩. See text for discussion of the “eccentricity envelope” and “cold core” labels.
Paper: A Tale of Two Circularization Periods
Authors: J. J. Zanazzi
Figure caption: Top panel: young (<1 Gyr, orange) and old (>3 Gyr, blue) binaries from the Meibom & Mathieu (2005) data set (with updates in M35, Leiner et al. 2015, and M67, Geller et al. 2021). Vertical gray dashed lines delineate orbital periods of 3–20 days. Bottom panel: cumulative eccentricity distribution for the young (orange) and evolved (blue) binaries between 3 and 20 days, for no eccentricity cutoff (solid) and an eccentricity cutoff of e > 0.05 (dashed). The legend gives results from a two-sample KS test between the young and old binaries, showing the “eccentricity envelope” (e > 0.05) is consistent with no evolution with age (p > 0.05).
Paper: A Tale of Two Circularization Periods
Authors: J. J. Zanazzi
Figure caption: Circularization P circ (blue) and envelope P env (orange) periods for the Kepler/TESS EBs, varying the number of binaries N  b  drawn from the data set, with triangles and lines denoting the median and 1σ uncertainty values (also displayed above/below lines). Young (<1 Gyr; dark blue) and old (>3 Gyr; dark red) Meibom & Mathieu (2005) circularization period measurements are shown for comparison, with N  b  denoting the number of cluster measurements with orbital periods less than 100 days.
Paper: A Tale of Two Circularization Periods
Authors: J. J. Zanazzi
Figure caption: Circularization P circ (blue) and envelope P env (orange) periods for the synthetically observed binaries, varying the number of binaries N  b  drawn from the tidally circularized population, for the values of η (Equation (3)) indicated. Triangles and lines denote the median and 1σ uncertainty values (also displayed above/below lines). See Appendix B for details.
Paper: A Tale of Two Circularization Periods
Authors: J. J. Zanazzi
Figure caption: Calculated longitude of pericenter ω over orbital periods P orb, using the EB data from Windemuth et al. (2019) and Justesen & Albrecht (2021). The clustering around ω ≈ ±π/2 is not real but indicates a bias due to large ﹩e\sin \omega ﹩ measurement errors, which tend to produce measurements with ﹩| e\sin \omega | \gg | e\cos \omega | ﹩. We discard ﹩e\sin \omega ﹩ measurements in this work.
Paper: A Tale of Two Circularization Periods
Authors: J. J. Zanazzi
Figure caption: Comparing P circ, P env constraints using the projected (triangles) and full (squares) eccentricity measurements, drawing N  b  binaries from the tidally circularized population, for the η values indicated. Lines denote 1σ errors, slightly displaced from their y-axis N  b  value for clarity. There is no notable difference between P circ, P env constraints using the projected versus full eccentricity measurements.
Paper: A Tale of Two Circularization Periods
Authors: J. J. Zanazzi
Figure caption: Synthetic observations of N  b  = 524 tidally circularized binaries, for the η values indicated. Salmon diamonds denote projected eccentricity measurements, contours denote smoothed kernel density estimates of the projected eccentricities, while solid (dotted) lines denote P circ (P env) fits to 1000 observations of the circularized population. The P circ, P env parameter fits are displayed in the legends.
Paper: A Tale of Two Circularization Periods
Authors: J. J. Zanazzi
Figure caption: Initial (blue) and final (red) population of binaries after tidal circularization, for η = 4.5. Black dotted line displays the periastron distance of r p = 1.5 R ⊙. See text for details.
Paper: Twin Extreme Ultraviolet Waves in the Solar Corona
Authors: Ruisheng Zheng, Bing Wang, Liang Zhang, Yao Chen, Robertus Erdélyi
Figure caption: The filament eruption in the HMI magnetogram, AIA 304, 193, and 94 Å, and EUVI-B 304 and 195 Å. The white arrows indicate the filament, and P1, N1, and N2 represent associated magnetic polarities. The red arrows indicate the erupting filament, and the green arrow points out the flare loops. The yellow and orange arrows indicate coronal loops L3 and the cusp structure, respectively. The dotted boxes represent the FOV of panels (b) and (c), respectively. The yellow and blue contours superposed on panel (b) represent the positive and negative magnetic polarities with levels of 200, 400, and 600 G. The dotted line (S6) starting at a diamond is used to derive the filament speed that is shown in the time–distance plot of Figure 7.
Paper: Twin Extreme Ultraviolet Waves in the Solar Corona
Authors: Ruisheng Zheng, Bing Wang, Liang Zhang, Yao Chen, Robertus Erdélyi
Figure caption: The extrapolated PFSS field lines superimposed on the intensity-normalized images in AIA 211 Å and EUVI-A 195 Å (top panels) and the difference images in AIA 193 Å and EUVI-B 195 Å (bottom panels). The blue and pink lines represent the coronal closed loops and open field lines, respectively. The yellow, green, cyan, and orange lines are the vital loops (L1–L4) for the generation of TEWs. The yellow and red arrows show the fraternal TEWs, and the white and purple arrows show the coronal dimmings associated with identical TEWs.
Paper: Twin Extreme Ultraviolet Waves in the Solar Corona
Authors: Ruisheng Zheng, Bing Wang, Liang Zhang, Yao Chen, Robertus Erdélyi
Figure caption: Sketch of the fraternal (top panels) and identical (bottom panels) TEWs based on the PFSS extrapolated field lines and HMI magnetograms. The yellow, green, cyan, and orange lines are the vital loops for the generation of twin waves, and the cyan, blue, yellow, and green shades represent the wave fronts of W1–W4. The yellow star indicates the magnetic reconnection between two small filaments (brown and pink lines), and the red dashed arrow represents the trajectory of the jet. The thick lines show the erupting filaments or jets. The black arrows indicate the moving direction of the erupting jet and filament.
Paper: Twin Extreme Ultraviolet Waves in the Solar Corona
Authors: Ruisheng Zheng, Bing Wang, Liang Zhang, Yao Chen, Robertus Erdélyi
Figure caption: Graphical abstract of the fraternal twin EUV waves. Two waves are shown clearly in the running-difference images in EUVI-A 195 Å (middle panels), and the FOV of the middle panels is indicated by the rectangles in the EUVI-A 195 Å image of the right panel. The source region is represented by the dashed panel in the composite image of AIA 304 and 94 Å (the left background panel) and is magnified to display the jet, filament, and flux rope in the left foreground panels. The wide blue and green arrows point out the temporal evolution of waves.
Paper: Twin Extreme Ultraviolet Waves in the Solar Corona
Authors: Ruisheng Zheng, Bing Wang, Liang Zhang, Yao Chen, Robertus Erdélyi
Figure caption: The eruption of the newly formed long filament in the Hα negative filtergram and AIA 304, 171, 131, and 94 Å. The green arrows indicate the newly formed filament, and the black arrows indicate the current sheet. The cyan arrows indicate postflare arcades, and the white arrows indicate the hot channel. The dotted box in panel (g) represents the FOV of panels (a)–(f).
Paper: Twin Extreme Ultraviolet Waves in the Solar Corona
Authors: Ruisheng Zheng, Bing Wang, Liang Zhang, Yao Chen, Robertus Erdélyi
Figure caption: Graphical abstract of the identical twin EUV waves. Two waves are shown clearly in the running-difference images in AIA 193 Å (bottom panels), and the associated filament and the eruption are shown in images in AIA 304 and 94 Å (top panels). Their FOVs are indicated by the rectangles in the background image in AIA 304 Å. The wide blue arrows point out the temporal evolution of waves.
Paper: First Census of Gas-phase Metallicity Gradients of Star-forming Galaxies in Overdense Environments at Cosmic Noon
Authors: Zihao Li, Xin Wang, Zheng Cai, Dong Dong Shi, Xiaohui Fan, Xian Zhong Zheng, Matthew A. Malkan, Harry I. Teplitz, Alaina L. Henry, Fuyan Bian, James Colbert
Figure caption: The metallicity gradients as a function of stellar mass for high-z star-forming galaxies in blank fields and overdense environments. The red diamonds are from our BOSS 1244 field, and the hollow one marks the galaxy categorized as an AGN. The orange circles are observed in F18. The blue diamonds come from the combined sample in W17 and W20, and the ones with left-pointing arrows represent dwarf galaxies (﹩\mathrm{log}({M}_{* }/{M}_{\odot })\lt 8.5﹩). These upper limits are omitted from our comparison for being far from our sample mass range. The red and orange contours denote the 50th, 68th, and 95th percentiles of the distribution estimated with Gaussian KDE. The dashed green line is the population stack of five mass bins from FIRE simulations (Ma et al. 2017). The magenta dashed line is the population stack of four mass bins from TNG50 simulations (Hemler et al. 2021). The histograms on the top and right of the main figure show the number distribution of observed stellar masses and metallicity gradients, respectively. From the histogram, our sample has the largest number of galaxies in the mass range ﹩\mathrm{log}({M}_{* }/{M}_{\odot })=[10,10.5]﹩ and has a notable number and fraction of inverted metallicity gradients.
Paper: First Census of Gas-phase Metallicity Gradients of Star-forming Galaxies in Overdense Environments at Cosmic Noon
Authors: Zihao Li, Xin Wang, Zheng Cai, Dong Dong Shi, Xiaohui Fan, Xian Zhong Zheng, Matthew A. Malkan, Harry I. Teplitz, Alaina L. Henry, Fuyan Bian, James Colbert
Figure caption: Left: relation between metallicity gradients and global metallicity of our galaxies. The red dashed lines show the linear fitting of the data using the LINMIX software with the 1σ error of both metallicity and metallicity gradient taken into account. The data points are color-coded by their environment overdensity δ  g  . The diamond with an orange error bar marks the galaxy classified as an AGN, which is excluded in the linear fitting in both left and right panels. Right: the metallicity gradients as a function of overdensity δ  g  of our samples. The data points are color-coded in SFR. The blue dashed line is also the linear fitting using LINMIX, taking into account the 1σ errors of the metallicity gradients. The data points are color-coded in SFR.
Paper: First Census of Gas-phase Metallicity Gradients of Star-forming Galaxies in Overdense Environments at Cosmic Noon
Authors: Zihao Li, Xin Wang, Zheng Cai, Dong Dong Shi, Xiaohui Fan, Xian Zhong Zheng, Matthew A. Malkan, Harry I. Teplitz, Alaina L. Henry, Fuyan Bian, James Colbert
Figure caption: The mass–metallicity relation (MZR) for our galaxy sample compared with the MZR measured in the field by the MOSDEF survey at z ∼ 2.3 (Sanders et al. 2021). The diamonds with pink bars represent individual galaxies, color-coded in overdensity δ  g . The red and blue lines correspond to the stacks of galaxies in our BOSS 1244 protocluster and the MOSDEF fields. The gray dotted line shows the reference MZR derived using the Sanders et al. (2021) FMR assuming the SFR and M * of our sample galaxies. We see that our galaxies residing in overdense environments show significant metallicity deficiency, compared with their coeval field counterparts, particularly in the high-mass regime. Here we not only show the 20 galaxies in this work, but also the other 16 galaxies in W22, to illustrate the relation in our protocluster environment with stronger statistical significance.
Paper: First Census of Gas-phase Metallicity Gradients of Star-forming Galaxies in Overdense Environments at Cosmic Noon
Authors: Zihao Li, Xin Wang, Zheng Cai, Dong Dong Shi, Xiaohui Fan, Xian Zhong Zheng, Matthew A. Malkan, Harry I. Teplitz, Alaina L. Henry, Fuyan Bian, James Colbert
Figure caption: The galaxy ID 03495 as an example of the analysis procedures applied to our entire sample. Top, from left to right: the F160W image of this galaxy, its metallicity map, and radial gradient. The black solid contours mark the deprojected galactocentric radii with a 1 kpc interval. The black dashed–dotted ellipses mark the half-light radii fitted by Galfit. Bottom: The smoothed 2D emission-line maps ([O III], [O II], Hβ, and Hγ) are used to infer the metallicity map. In all maps, north is up and east is to the left.
Paper: First Census of Gas-phase Metallicity Gradients of Star-forming Galaxies in Overdense Environments at Cosmic Noon
Authors: Zihao Li, Xin Wang, Zheng Cai, Dong Dong Shi, Xiaohui Fan, Xian Zhong Zheng, Matthew A. Malkan, Harry I. Teplitz, Alaina L. Henry, Fuyan Bian, James Colbert
Figure caption: The histogram of the fitted metallicity gradients (top), and the metallicity gradients divided by their uncertainties (bottom). From left to right: the results for five different mocks with true gradients [0,0.02, 0.04, −0.02, −0.04] dex kpc−1. The black dotted line denotes the true gradient value. The solid red line represents the median value in the 100 reconstructions, and the red dashed lines show the 1σ interval.
Paper: First Census of Gas-phase Metallicity Gradients of Star-forming Galaxies in Overdense Environments at Cosmic Noon
Authors: Zihao Li, Xin Wang, Zheng Cai, Dong Dong Shi, Xiaohui Fan, Xian Zhong Zheng, Matthew A. Malkan, Harry I. Teplitz, Alaina L. Henry, Fuyan Bian, James Colbert
Figure caption: Metallicity radial gradients measured in our sample. The same as Figure 1.
Paper: Using the Hills Mechanism to Generate Repeating Partial Tidal Disruption Events and ASASSN-14ko
Authors: M. Cufari, Eric R. Coughlin, C. J. Nixon
Figure caption: The probability distribution function (PDF) of the semimajor axis of the captured star, a • (top left), the orbital period of the captured star, P • (top right), the eccentricity of the captured star orbit, e • (bottom left), and the period decay rate due to the emission of gravitational waves, ﹩{\dot{P}}_{\bullet }﹩ (bottom right), for an initial binary semimajor axis of a ⋆ = 0.005 au and SMBH mass of M • = 107  M ⊙. Vertical dashed lines on these plots give the estimates that result from the calculations in Section 2; the predicted eccentricity for β = 0.5 is e • ≃ 0.981 and was excluded from the bottom left panel to retain the clarity of the figure. We similarly excluded the vertical dashed line for β = 0.5 (﹩{\dot{P}}_{\bullet }=-1.15\times {10}^{-7}﹩) in the bottom right panel. The different colors correspond to the β shown in the legend, where β is the ratio of the tidal radius of the binary to the point of closest approach of the binary. The vertical blue line in the top right corresponds to the period of ASASSN-14ko, which is 114 days, and the vertical blue line in the bottom right panel is the observed ﹩{\dot{P}}_{\bullet }﹩ of ASASSN-14ko, that is, ﹩\dot{P}=-0.002﹩.
Paper: Chaotic and Clumpy Galaxy Formation in an Extremely Massive Reionization-era Halo
Authors: Justin S. Spilker, Christopher C. Hayward, Daniel P. Marrone, Manuel Aravena, Matthieu Béthermin, James Burgoyne, Scott C. Chapman, Thomas R. Greve, Gayathri Gururajan, Yashar D. Hezaveh, Ryley Hill, Katrina C. Litke, Christopher C. Lovell, Matthew A. Malkan, Eric J. Murphy, Desika Narayanan, Kedar A. Phadke, Cassie Reuter, Antony A. Stark, Nikolaus Sulzenauer, Joaquin D. Vieira, David Vizgan, Axel Weiß
Figure caption: Summary of SPT 0311–58 clump properties in comparison to cloud-scale structures identified in nearby galaxies and two high-redshift lensed objects. Although more massive and larger in scale, the internal properties of the SPT 0311–58 clumps are remarkably similar to the lower-redshift structures: They have similar gas surface densities as the z ∼ 1 and 3 clouds in the lensed objects (left), are approximately consistent with being virialized (center), and (assuming virialization) show a distribution of clump freefall times similar to the lower-redshift clouds (right). In the left panel, the gray shaded regions show the approximate limits of our data in size and line width for both highly magnified and unlensed regions of the source plane. Section 3.3 details the derivation of the dotted lines in the left and center panels. All the clump properties used in this work are available as data behind the figure (See Figure 4).
Paper: Chaotic and Clumpy Galaxy Formation in an Extremely Massive Reionization-era Halo
Authors: Justin S. Spilker, Christopher C. Hayward, Daniel P. Marrone, Manuel Aravena, Matthieu Béthermin, James Burgoyne, Scott C. Chapman, Thomas R. Greve, Gayathri Gururajan, Yashar D. Hezaveh, Ryley Hill, Katrina C. Litke, Christopher C. Lovell, Matthew A. Malkan, Eric J. Murphy, Desika Narayanan, Kedar A. Phadke, Cassie Reuter, Antony A. Stark, Nikolaus Sulzenauer, Joaquin D. Vieira, David Vizgan, Axel Weiß
Figure caption: Observed (image-plane) and reconstructed (source-plane) maps of the dust and integrated [C II] emission in SPT 0311–58. The 12 clumps we identify in the source-plane reconstructions are labeled; clumps E1 and W7 are identified only in the [C II] data cube and are marked with dotted circles. Because of the relatively simple lensing geometry, each of the source-plane clumps maps nearly one to one with the clumps visible by eye in the image plane (clumps W2–W4 together create the southeastern arc/counterimage). Contours in the [C II] maps are of the dust continuum. The ≈0.″07 synthesized beam is shown in the lower left of the observed images, and the lensing caustics are shown in the source-plane maps in white.
Paper: Chaotic and Clumpy Galaxy Formation in an Extremely Massive Reionization-era Halo
Authors: Justin S. Spilker, Christopher C. Hayward, Daniel P. Marrone, Manuel Aravena, Matthieu Béthermin, James Burgoyne, Scott C. Chapman, Thomas R. Greve, Gayathri Gururajan, Yashar D. Hezaveh, Ryley Hill, Katrina C. Litke, Christopher C. Lovell, Matthew A. Malkan, Eric J. Murphy, Desika Narayanan, Kedar A. Phadke, Cassie Reuter, Antony A. Stark, Nikolaus Sulzenauer, Joaquin D. Vieira, David Vizgan, Axel Weiß
Figure caption: The individual clumps identified in SPT 0311–58 are similar in mass to “typical” coeval massive galaxies, but show SFRs elevated by ≈3–5×. However they formed, the clumps can be thought of as similar in scale to known reionization-era galaxies. All comparison objects also have spatially-resolved ALMA [C II] observations; see Section 3.2. All the clump properties used in this work are available as data behind the figure.(The data used to create this figure are available.)