adsabs/AstroCLIMB huggingface dataset:
Paper: SCUBA-2 High Redshift Bright Quasar Survey. II. The Environment of z ∼ 6 Quasars at Submillimeter Band
Authors: Qiong Li, Ran Wang, Xiaohui Fan, Xue-Bing Wu, Linhua Jiang, Eduardo Bañados, Bram Venemans, Yali Shao, Jianan Li, Jeff Wagg, Roberto Decarli, Chiara Mazzucchelli, Alain Omont, Frank Bertoldi, Sean Johnson, Christopher J. Conselice, Chengpeng Zhang
Figure caption: Cumulative number counts of SMGs, in fields centered on (i) luminous high-redshift AGNs: z ∼ 5 optically selected quasars (gray diamonds; Priddey et al. 2008); z ∼ 4 radio galaxies (gray squares; Stevens et al. 2003); (ii) z ∼ 2 protoclusters (gray triangles; Cooke et al. 2019; Zhang et al. 2022); (iii) z ∼ 1 clusters (gray circles; Best 2002; Webb et al. 2005); and (iv) z ∼ 6 optically selected quasars (this paper; black circles and red/blue diamonds). The black line shows the blank-field number counts of SMGs in the previous survey, i.e., the SCUBA-2 survey for the S2CLS field in Geach et al. (2017). The blue line is calculated from our survey’s combined areas of all 54 quasars (∼620 arcmin2); the red line is from the combined areas of 13 overdense fields around the quasars (∼150 arcmin2). The black filled circles indicate the three most overdense fields selected from our sample at z ∼ 6. Points in this work have been corrected for flux boosting and incompleteness.
Paper: SCUBA-2 High Redshift Bright Quasar Survey. II. The Environment of z ∼ 6 Quasars at Submillimeter Band
Authors: Qiong Li, Ran Wang, Xiaohui Fan, Xue-Bing Wu, Linhua Jiang, Eduardo Bañados, Bram Venemans, Yali Shao, Jianan Li, Jeff Wagg, Roberto Decarli, Chiara Mazzucchelli, Alain Omont, Frank Bertoldi, Sean Johnson, Christopher J. Conselice, Chengpeng Zhang
Figure caption: The combined differential and cumulative number counts at 850 μm from all of our source fields. The filled black circles and black lines indicate our data and Schechter fitting, respectively. The gray line shows the blank-field number counts of SMGs in the S2CLS field in Geach et al. (2017). For clarity, we only show the error bars of S2CLS and our data from Poissonian statistics (Gehrels 1986). Points in this work have been corrected for flux boosting and incompleteness (see Figure 5).
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: Normalized PDF of the plume frequency f pl for the midMS model. The vertical, black dotted–dashed line represents the peak frequency, located at f pl ≈ 6 μHz; the magenta straight lines, possessing slopes of −1/β 1 and −1/β 2, represent exponential fits to the data.
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: Normalized PDFs of the plume overshooting length in units of the pressure scale height (panel (a)) and latitudinal distribution of plumes (panel (b)) for each stellar age (z: ZAMS, purple; m: midMS, cyan; and T: TAMS, orange).
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: Radial profiles for the viscosity ν (full lines) and thermal diffusivity κ (dashed lines) for our simulations. The color-coded vertical lines indicate the size of the respective convective zones.
Paper: Three-dimensional Simulations of Massive Stars. II. Age Dependence
Authors: R. Vanon, P. V. F. Edelmann, R. P. Ratnasingam, A. Varghese, T. M. Rogers
Figure caption: Temporal evolution of the v rms averaged over the entirety of the convective zone for each model.
Paper: Optimizing the Resolution of Hydrodynamic Simulations for MCRaT Radiative Transfer Calculations
Authors: Jose Arita-Escalante, Tyler Parsotan, S. Bradley Cenko
Figure caption: HD properties at different refinement levels for the PLUTO 16TI simulation as functions of refinement level at the first moment of photon injection and final frame of the simulation. We took the initial frame measurements of a shell located at radius r = 1.3 × 1012 cm and time ﹩{t}_{\mathrm{sim}}=\tfrac{\mathrm{frame}}{\mathrm{fps}}=50\,{\rm{s}}﹩. We took the final frame measurements of a shell located at radius r = 1.5 × 1013 cm and time ﹩{t}_{\mathrm{sim}}=\tfrac{\mathrm{frame}}{\mathrm{fps}}=527.6\,{\rm{s}}﹩. Panel (a) shows the average HD cell radius size (Δr) in cm. Panel (b) shows the average density in g cm−3. Panel (c) shows the average temperature in K. Panel (d) shows the average bulk Lorentz factor. The early-time conditions are shown by red triangle markers and the final conditions are shown by blue circle markers. Throughout our analysis, we focus on the five highest spatial refinement levels in a given HD simulation frame. Thus, the final frame quantities for refinement level 5 shown in this figure correspond to the black grid representing level 7 shown in 1(c).
Paper: Optimizing the Resolution of Hydrodynamic Simulations for MCRaT Radiative Transfer Calculations
Authors: Jose Arita-Escalante, Tyler Parsotan, S. Bradley Cenko
Figure caption: Spectra of a 16TI HD-simulated GRB at different refinement levels. The solid purple line is a blackbody spectrum that peaks at each spectrum set’s highest refinement level. Panel (a) shows the spectra of a simulated GRB using the same PLUTO 16TI simulation, but at different spatial refinement levels, maintaining the highest temporal resolution constant. Panel (b) shows the spectra generated with the same 16TI simulation at different temporal resolutions, maintaining the highest spatial resolution constant. Panel (c) shows the spectra of a simulated GRB with matching temporal and spatial resolution levels.
Paper: Optimizing the Resolution of Hydrodynamic Simulations for MCRaT Radiative Transfer Calculations
Authors: Jose Arita-Escalante, Tyler Parsotan, S. Bradley Cenko
Figure caption: Frame properties at the end of the PLUTO 16TI simulation. These quantities are read at the time given by ﹩{t}_{\mathrm{sim}}=\tfrac{\mathrm{frame}}{\mathrm{fps}}=527.6\,{\rm{s}}﹩. Panel (a) shows the Lorentz factor profile at this time. Panel (b) shows the mass density profile at this time. Panel (c) shows the AMR grid shape and levels at this time. In this last panel, we can see the computational efforts are dedicated to the higher-refinement area of the frame, where the jet is located. We note that even though Panel (c) shows seven levels of refinement, in our analysis we highlight the five highest levels of spatial refinement in any HD frame.
Paper: Optimizing the Resolution of Hydrodynamic Simulations for MCRaT Radiative Transfer Calculations
Authors: Jose Arita-Escalante, Tyler Parsotan, S. Bradley Cenko
Figure caption: Matrices containing ζ Prop for different EM properties of the 16TI-simulated GRBs. Panel (a) shows the deviation ﹩{\zeta }_{{L}_{\mathrm{iso}}}﹩ for all spatial and temporal refinement levels. Panel (b) shows the deviation ﹩{\zeta }_{{E}_{\mathrm{pk}}}﹩. Panel (c) shows the deviation ζ  α . Panel (d) shows the deviation ζ  β .
Paper: Optimizing the Resolution of Hydrodynamic Simulations for MCRaT Radiative Transfer Calculations
Authors: Jose Arita-Escalante, Tyler Parsotan, S. Bradley Cenko
Figure caption: Spectral peak energies of a spherical outflow for different refinement levels. Panel (a) shows the E pk of the same spherical outflow simulation, but at different spatial refinement levels, maintaining the highest temporal resolution constant. Panel (b) shows the E pk generated with the same analytic outflow simulation at different temporal resolutions, maintaining the highest spatial resolution constant. Panel (c) shows the E pk with matching temporal and spatial resolution levels. The error bars in panels (a), (b), and (c) are present, but are encompassed within the markers.
Paper: Optimizing the Resolution of Hydrodynamic Simulations for MCRaT Radiative Transfer Calculations
Authors: Jose Arita-Escalante, Tyler Parsotan, S. Bradley Cenko
Figure caption: Spectra of a spherical outflow for different refinement levels. The solid purple line is a blackbody spectrum that peaks at each spectrum set’s highest refinement level. Panel (a) shows the spectra of a spherical outflow profile, but at different spatial refinement levels, maintaining the highest temporal resolution constant. Panel (b) shows the spectra generated with analytic outflow at different temporal resolutions, maintaining the highest spatial resolution constant. Panel (c) shows the spectra with matching temporal and spatial resolution levels.
Paper: Optimizing the Resolution of Hydrodynamic Simulations for MCRaT Radiative Transfer Calculations
Authors: Jose Arita-Escalante, Tyler Parsotan, S. Bradley Cenko
Figure caption: Lightcurves of the 16TI HD-simulated GRB for different refinement levels. Only the first ∼10 s of the simulations are shown to better visualize the qualitative effects of reducing the spatial and/or temporal resolutions. Panel (a) shows the lightcurves of a simulated GRB using the same PLUTO 16TI simulation, but at different spatial refinement levels, maintaining the highest temporal resolution constant. Panel (b) shows the lightcurves generated with the same 16TI simulation at different temporal resolutions, maintaining the highest spatial resolution constant. Panel (c) shows the lightcurves of a simulated GRB with matching temporal and spatial resolution levels.
Paper: Optimizing the Resolution of Hydrodynamic Simulations for MCRaT Radiative Transfer Calculations
Authors: Jose Arita-Escalante, Tyler Parsotan, S. Bradley Cenko
Figure caption: Lightcurves of simulated spherical outflow for different refinement levels. Panel (a) shows the lightcurves using the same analytic outflow simulation, but at different spatial refinement levels, maintaining the highest temporal resolution constant. Panel (b) shows the lightcurves generated with the same spherical outflow simulation at different temporal resolutions, maintaining the highest spatial resolution constant. Panel (c) shows the lightcurves with matching temporal and spatial resolution levels.
Paper: Optimizing the Resolution of Hydrodynamic Simulations for MCRaT Radiative Transfer Calculations
Authors: Jose Arita-Escalante, Tyler Parsotan, S. Bradley Cenko
Figure caption: Spectral luminosities of a spherical outflow for different refinement levels. Panel (a) shows the luminosities using the same analytic outflow simulation, but at different spatial refinement levels, maintaining the highest temporal resolution constant. Panel (b) shows the luminosities generated with the same spherical outflow simulation at different temporal resolutions while holding the highest spatial resolution constant. Panel (c) shows the luminosities with matching temporal and spatial resolution levels. The error bars in panels (a), (b), and (c) are present, but are encompassed within the markers.
Paper: Seismic Signatures of the 12C(α, γ)16O Reaction Rate in White Dwarf Models with Overshooting
Authors: Morgan T. Chidester, F. X. Timmes, Ebraheem Farag
Figure caption: Top two: NOV set’s signature adiabatic pulsation modes shown at T eff = 11,500 K (bright green), and T eff = 10,000 K (blue), respectively. The first panel shows the signal from the g 2 mode; the second shows the signal from the g 6 trapped mode. Bottom: the kinetic energy diagrams for all σ  i  at T eff = 11,500 K (left) and T eff = 10,000 K (right), respectively. The green dots/lines represent E kin for σ  i  > 0, gray for σ  i  < 0, black for σ = 0. The shading of color gets fainter the further away from σ = 0.
Paper: Seismic Signatures of the 12C(α, γ)16O Reaction Rate in White Dwarf Models with Overshooting
Authors: Morgan T. Chidester, F. X. Timmes, Ebraheem Farag
Figure caption: Composition profiles after the NOV (top) and OV (bottom) models cool to T eff = 10,000 K. Region boundaries are indicated by vertical blue lines, and the σ  i  colors are the same as in Figure 1.
Paper: Seismic Signatures of the 12C(α, γ)16O Reaction Rate in White Dwarf Models with Overshooting
Authors: Morgan T. Chidester, F. X. Timmes, Ebraheem Farag
Figure caption: Integer multiples of the local radial wavelengths q · λ  r  for g 2 and g 6 as a function of the star’s radius R. Mode resonance occurs when q · λ  r  closely matches the width of a certain region(s) in the star. The left panel is the NOV set’s mode resonance and the right panel is the OV set’s mode resonance. In both panels, the black horizontal lines mark the respective region widths. Blue curves show q · λ  r  for g 2, and maroon curves show q · λ  r  for g 6. The q values are stated in the legend.
Paper: Seismic Signatures of the 12C(α, γ)16O Reaction Rate in White Dwarf Models with Overshooting
Authors: Morgan T. Chidester, F. X. Timmes, Ebraheem Farag
Figure caption: Mass fraction profiles at the completion of CHeB for a 30-isotope (solid) and 23-isotope nuclear reaction network (dotted). Shown are the five most abundant isotopes for both networks.
Paper: Seismic Signatures of the 12C(α, γ)16O Reaction Rate in White Dwarf Models with Overshooting
Authors: Morgan T. Chidester, F. X. Timmes, Ebraheem Farag
Figure caption: Pulsation periods as function of T eff for the NOV (black) and OV (gray) model sets.
Paper: Seismic Signatures of the 12C(α, γ)16O Reaction Rate in White Dwarf Models with Overshooting
Authors: Morgan T. Chidester, F. X. Timmes, Ebraheem Farag
Figure caption: Left: evolution of central mass fractions during CHeB until ﹩\mathrm{log}({\text{}}L/{L}_{\odot })﹩ = 3.0 at three resolutions. Middle: mass fraction profiles at ﹩\mathrm{log}({\text{}}L/{L}_{\odot })﹩ = 3.0 for the three resolutions. Right: middle figure zoom in to show differences.
Paper: Seismic Signatures of the 12C(α, γ)16O Reaction Rate in White Dwarf Models with Overshooting
Authors: Morgan T. Chidester, F. X. Timmes, Ebraheem Farag
Figure caption: Adiabatic g 2 (left) and g 6 (right) mode signatures for the NOV and OV sets, at T eff = 11,500 K (bright green) and T eff = 10,000 K (blue), respectively.
Paper: The Temperature, Electron, and Pressure Characteristics of Switchbacks: Parker Solar Probe Observations
Authors: Jia Huang, Justin C. Kasper, Davin E. Larson, Michael D. McManus, Phyllis Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, Mingzhe Liu, Lan K. Jian, Jaye L. Verniero, Marco Velli, Samuel T. Badman, Yeimy J. Rivera, Tatiana Niembro, Kristoff Paulson, Michael Stevens, Anthony W. Case, Trevor A. Bowen, Marc Pulupa, Stuart D. Bale, Jasper S. Halekas
Figure caption: Switchback event observed on 2021 January 18. From top to bottom, the panels show the magnetic field components in RTN coordinates, the variations of the radial magnetic field component to the total magnetic field strength (B  R /∣B∣), the normalized pitch-angle distributions of suprathermal electrons (E-PADs), the anisotropy of E-PADs (A  E ) at the energy of 346.5 eV, the integrated intensity of suprathermal electrons (F  E ) at the energy of 346.5 eV (unit is cm−2 s−1 sr−1), the normalized pressure components (thermal pressure P  k , magnetic pressure P  B , total pressure P total), the proton temperature components (T ⊥p  in red and T ∥p  in blue), and the alpha-to-proton temperature ratio (T  α /T  p ). From left to right, the shaded regions represent the leading quiet period (LQP), spike, and trailing quiet period (TQP), respectively, and the leading transition region (LTR) and trailing transition region (TTR) locate between the shaded regions.
Paper: The Temperature, Electron, and Pressure Characteristics of Switchbacks: Parker Solar Probe Observations
Authors: Jia Huang, Justin C. Kasper, Davin E. Larson, Michael D. McManus, Phyllis Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, Mingzhe Liu, Lan K. Jian, Jaye L. Verniero, Marco Velli, Samuel T. Badman, Yeimy J. Rivera, Tatiana Niembro, Kristoff Paulson, Michael Stevens, Anthony W. Case, Trevor A. Bowen, Marc Pulupa, Stuart D. Bale, Jasper S. Halekas
Figure caption: Proton temperature anisotropy in different regions of switchbacks. Panels (a)–(c) present the proton temperature anisotropy (T ⊥p /T ∥p ) vs. parallel proton plasma beta (β ∥p ) in spike, transition region, and quiet period, respectively, with the color bar indicating the normalized counts. Panel (d) shows the histogram distributions of T ⊥p /T ∥p  in the three regions as shown by the legend. In panels (a)–(c), the contours indicate 50% measurements, the dashed lines are colored to indicate different instabilities with thresholds from Hellinger et al. (2006), and the solid line indicates the anticorrelations derived by Marsch et al. (2004).
Paper: The Temperature, Electron, and Pressure Characteristics of Switchbacks: Parker Solar Probe Observations
Authors: Jia Huang, Justin C. Kasper, Davin E. Larson, Michael D. McManus, Phyllis Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, Mingzhe Liu, Lan K. Jian, Jaye L. Verniero, Marco Velli, Samuel T. Badman, Yeimy J. Rivera, Tatiana Niembro, Kristoff Paulson, Michael Stevens, Anthony W. Case, Trevor A. Bowen, Marc Pulupa, Stuart D. Bale, Jasper S. Halekas
Figure caption: The comparisons of E-PADs in different regions of switchbacks. Panels (a) and (b) compare the E-PADs’ anisotropy (A  E ) between different regions of switchbacks, whereas panels (c) and (d) compare the E-PADs’ intensity (F  E ) difference. In panels (a) and (c), the mean values are used to calculate the regional ratios. In panels (b) and (d), the median values are used. The histograms and dashed vertical line in each panel have the same meaning as that in Figure 3.
Paper: The Temperature, Electron, and Pressure Characteristics of Switchbacks: Parker Solar Probe Observations
Authors: Jia Huang, Justin C. Kasper, Davin E. Larson, Michael D. McManus, Phyllis Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, Mingzhe Liu, Lan K. Jian, Jaye L. Verniero, Marco Velli, Samuel T. Badman, Yeimy J. Rivera, Tatiana Niembro, Kristoff Paulson, Michael Stevens, Anthony W. Case, Trevor A. Bowen, Marc Pulupa, Stuart D. Bale, Jasper S. Halekas
Figure caption: The comparisons of proton temperature components in different regions of switchbacks. Panels (a)–(c) show the occurrence rates of the ratios for total temperature T  p , parallel temperature T ∥p , and perpendicular temperature T ⊥p  in the transition region and quiet period as compared with that in spike. In each panel, the black (red) histogram shows the comparison between the TR (QP) and the spike, and the dashed vertical line marks where the ratio equals 1.
Paper: The Temperature, Electron, and Pressure Characteristics of Switchbacks: Parker Solar Probe Observations
Authors: Jia Huang, Justin C. Kasper, Davin E. Larson, Michael D. McManus, Phyllis Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, Mingzhe Liu, Lan K. Jian, Jaye L. Verniero, Marco Velli, Samuel T. Badman, Yeimy J. Rivera, Tatiana Niembro, Kristoff Paulson, Michael Stevens, Anthony W. Case, Trevor A. Bowen, Marc Pulupa, Stuart D. Bale, Jasper S. Halekas
Figure caption: The comparisons of pressures in different regions of switchbacks. Panels (a)–(c) compare the thermal pressure (P  K ), magnetic pressure (P  B ), and total pressure (P total) between different regions of switchbacks, respectively. The mean values are used to calculate the ratios, whereas the median values are used in panels (d)–(f). The histograms and dashed vertical line in each panel have the same meaning as those in Figure 3.
Paper: The Temperature, Electron, and Pressure Characteristics of Switchbacks: Parker Solar Probe Observations
Authors: Jia Huang, Justin C. Kasper, Davin E. Larson, Michael D. McManus, Phyllis Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, Mingzhe Liu, Lan K. Jian, Jaye L. Verniero, Marco Velli, Samuel T. Badman, Yeimy J. Rivera, Tatiana Niembro, Kristoff Paulson, Michael Stevens, Anthony W. Case, Trevor A. Bowen, Marc Pulupa, Stuart D. Bale, Jasper S. Halekas
Figure caption: The comparisons of alpha-to-proton temperature components in different regions of switchbacks. The histograms in each panel are similar to that in Figure 3, but this figure presents the variations of T  α /T  p , T ∥α /T ∥p , and T ⊥α /T ⊥p , respectively.
Paper: The Temperature, Electron, and Pressure Characteristics of Switchbacks: Parker Solar Probe Observations
Authors: Jia Huang, Justin C. Kasper, Davin E. Larson, Michael D. McManus, Phyllis Whittlesey, Roberto Livi, Ali Rahmati, Orlando Romeo, Mingzhe Liu, Lan K. Jian, Jaye L. Verniero, Marco Velli, Samuel T. Badman, Yeimy J. Rivera, Tatiana Niembro, Kristoff Paulson, Michael Stevens, Anthony W. Case, Trevor A. Bowen, Marc Pulupa, Stuart D. Bale, Jasper S. Halekas
Figure caption: Panel (a) shows the occurrence rate of T  α /T  p  in different regions of switchbacks, with the black, red, and blue histograms representing the distributions in spike, transition region, and quiet period, respectively. Panel (b) presents the cumulative distribution function (CDF) of T  α /T  p  in the same regions as shown in panel (a).
Paper: Sudden Extreme Obscuration of a Sun-like Main-sequence Star: Evolution of the Circumstellar Dust around ASASSN-21qj
Authors: Jonathan P. Marshall, Steve Ertel, Francisca Kemper, Carlos del Burgo, Gilles P. P. L. Otten, Peter Scicluna, Sascha T. Zeegers, Álvaro Ribas, Oscar Morata
Figure caption: Top: optical photometry comprising ASAS-SN V and ﹩g^{\prime} ﹩ measurements (dark green squares; V values were transposed to ﹩g^{\prime} ﹩ before plotting) and LCOGT ﹩g^{\prime} ﹩ (light green circles). The horizontal dashed line represents the unocculted ﹩g^{\prime} ﹩ magnitude of the star. An inset panel spans MJD 58,000–58,300, highlighting the region in between the two NEOWISE epochs shown in the lower two panels where the near-infrared excess appears. Upper middle: ATLAS “cyan” (λ = 653 nm) filter band photometry. The dashed line denotes the mean magnitude of the star in measurements prior to MJD 58,500, while the shaded region denotes 3 times the mean uncertainty of those measurements. Lower middle: NEOWISE W1 (3.4 μm) measurements. Individual data points are translucent with the mean for each epoch presented as a solid data point. The shaded region denotes the ±3σ  region around the AllWISE catalog measurement, denoted by a dashed line. Bottom: NEOWISE W2 (4.6 μm) measurements, presented as per the lower middle panel.
Paper: Sudden Extreme Obscuration of a Sun-like Main-sequence Star: Evolution of the Circumstellar Dust around ASASSN-21qj
Authors: Jonathan P. Marshall, Steve Ertel, Francisca Kemper, Carlos del Burgo, Gilles P. P. L. Otten, Peter Scicluna, Sascha T. Zeegers, Álvaro Ribas, Oscar Morata
Figure caption: ASAS-SN and LCOGT ﹩g^{\prime} ﹩ photometry of ASASSN-21qj between MJD 59,300 and 59,900. The observations are denoted by green data points with 1σ uncertainties. Overplotted on the observations is a two-component model of the obscuration. A broad, asymmetric, and shallow component is centered at MJD 59,450. Narrow, deeper events are superimposed upon that (35 in total), with the location of narrow dimming events in the time series denoted by the upward-pointing green triangles. These events were identified by searching for observations that were 3σ fainter than the preceding and subsequent data point in the time series, taking into account the underlying broad, shallow obscuration component. This model does not capture, and does not seek to capture, the full complex behavior of the dimming event, where it is clear that intermediate-duration dimming events lasting several days to tens of days occurred. Rather, it is illustrative of the extremes of the timescales involved within the overall dimming event for ASASSN-21qj.