adsabs/AstroCLIMB huggingface dataset:
Paper: Ultraviolet Radiation Fields in Star-forming Disk Galaxies: Numerical Simulations with TIGRESS-NCR
Authors: Nora B. Linzer, Jeong-Gyu Kim, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Same as in Figure 10 but for model LGR4-2pc over time range 250–350 Myr. The red dashed line represents the best fit of Equation (7) to the mode of the distribution. The black dashed line represents the value of Equation (7) using the value of τ FUV,eff fit from the R8-4pc model (Equation (8)).
Paper: Ultraviolet Radiation Fields in Star-forming Disk Galaxies: Numerical Simulations with TIGRESS-NCR
Authors: Nora B. Linzer, Jeong-Gyu Kim, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Vertical profiles of contribution to the mean density 〈n H〉 and volume filling factor f  V  for each of four ISM phases, as well as density ﹩{\bar{n}}_{{\rm{H}}}﹩, mass weighted electron abundance x  e  = 〈n  e 〉/〈n H〉, and LyC and FUV radiation density ﹩{\bar{{\boldsymbol{ \mathcal E }}}}_{\mathrm{LyC}}﹩ and ﹩{\bar{{\boldsymbol{ \mathcal E }}}}_{\mathrm{FUV}}﹩ within defined gas phases. Profiles are based on ∼200 simulation snapshots between 250 and 450 Myr for the R8-4pc model. The lines represent the median value, and the shaded regions indicate 25th–75th percentiles. See text for details.
Paper: Ultraviolet Radiation Fields in Star-forming Disk Galaxies: Numerical Simulations with TIGRESS-NCR
Authors: Nora B. Linzer, Jeong-Gyu Kim, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Same as Figure 3 but for the LGR4-2pc model at t = 298 Myr. The black contour in each panel represents a classical H II region, which contains a star cluster source of mass 1.2 × 103 M ⊙.
Paper: Ultraviolet Radiation Fields in Star-forming Disk Galaxies: Numerical Simulations with TIGRESS-NCR
Authors: Nora B. Linzer, Jeong-Gyu Kim, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Physical quantities along a one-dimensional, horizontal ray through z = 0, y = −134 pc of the R8-4pc model at t = 430 Myr. From top to bottom, the panels represent x  e , T, n H, ﹩{{\boldsymbol{ \mathcal E }}}_{\mathrm{FUV}}﹩, and ﹩{{\boldsymbol{ \mathcal E }}}_{\mathrm{LyC}}﹩. The gas phase is represented by the background color. Sharp photoionization fronts are clearly seen in the ﹩{{\boldsymbol{ \mathcal E }}}_{\mathrm{LyC}}﹩ and x  e  and T panels, which separate WIM from C+U gas. These represent the boundary of the H II region visible in Figure 3 at x = −200 pc.
Paper: Ultraviolet Radiation Fields in Star-forming Disk Galaxies: Numerical Simulations with TIGRESS-NCR
Authors: Nora B. Linzer, Jeong-Gyu Kim, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Same as Figure 6 but for the LGR4-2pc model between times 250 and 350 Myr.
Paper: Ultraviolet Radiation Fields in Star-forming Disk Galaxies: Numerical Simulations with TIGRESS-NCR
Authors: Nora B. Linzer, Jeong-Gyu Kim, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Same as Figure 8, but for the LGR4-2pc model.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: Upper panel: redshift distributions of different subsets—the entire cluster sample (black histogram), consistent BCG spectroscopic redshift (red histogram), DESI confirmation (green histogram), member galaxy DEmP photometric redshift check (blue histogram), and clusters with confident redshift (magenta histogram). The total cluster count for each subset is shown in the legend. Lower panel: fraction of cluster photometric redshift without any confirmation as a function of redshift.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: The comoving number density as a function of the redshift of the CAMIRA S21A cluster sample (red curves) and mock catalogs made from our simulation and halo light cone from R. Takahashi et al. (2017; blue points and magenta curves; described later in Section 3.2). The curves in dashed style and the upper blue points correspond to a richness cut N cut = 10.0. The curves in the dotted style and the lower blue points correspond to a richness cut N cut = 15.0. The black solid curves are the halo number density obtained by integrating the halo mass function in J. Tinker et al. (2008) from 6.5 × 1013 h −1   M ⊙ and 1.0 × 1014 h −1   M ⊙, respectively. The error bands and error bars are calculated assuming Poisson errors. We do not show the errors of the mock catalog made by R. Takahashi et al. (2017) for clarity of the figure.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: Left: the workflow of linking length calibration. We start by applying the richness cut N cut to the ROCKSTAR catalogs to construct mock catalogs (Section 3.2). The optimized linking length l opt (Section 3.3) is obtained by iteratively comparing the results of the FoF algorithm with ground-truth superclusters (referred to as SCs in the figure). Right: the workflow of the supercluster finding algorithm. First, we apply different richness cuts and divide the CAMIRA clusters into different redshift bins. We then apply the calibrated linking length to each redshift bin and obtain supercluster candidates. The last step involves merging supercluster candidates from different redshift bins and the richness cuts into the final supercluster catalog.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: Demonstration of comparing CAMIRA cluster photometric redshift with  DEmP  photometric redshift of member galaxies. The blue curve shows the normalized CDF of member galaxies’ photo-z estimated by DEmP. The black vertical curve indicates the cluster photo-z. The gray dashed line and the gray dotted line indicate the value of CDF at the lower and upper bound of the redshift interval [z  l , z  u ] (two vertical gray lines) considered, respectively. According to the criteria described in Section 2.3, the cluster photo-z is inconsistent with member galaxies’ photo-z in the top and middle panels, while the bottom panel demonstrates a consistent case.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: The stellar mass of BCGs as a function of cluster richness. The blue and red points represent Iso-Cls and SC-Cls, respectively. The upper and right side panels show the distributions of richness and stellar mass. The corresponding redshift bin and sample set are indicated in each panel. The black dashed line indicates the power-law fit of all data points in a given redshift bin and sample set. The richness distributions and stellar mass distributions in the side panels all suggest that clusters and BCGs in the supercluster environment tend to be more massive (see Figures 18 and 19 for more details).
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption:  CAMIRA supercluster candidates and Iso-Cls in the KGSC field overlaid by HSC PDR3 density map in two different redshift slices. The orange open circles represent the positions of CAMIRA clusters that are not associated with any supercluster candidates. Red crosses and red triangles indicate the positions of supercluster candidates with multiplicity 2 (m = 2) and 3(m = 3), respectively (here, the positions are the mean positions of member clusters). The number labeled under each supercluster candidate is the mean redshift of member clusters. If all members of a given supercluster have confident redshift (see Section 2.4), then the redshift number is colored in green; otherwise redshift number is colored in yellow. Under the definition that superclusters will eventually experience gravitational collapse, our results suggest that KGSC might be fragmented into numerous supercluster candidates.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: The normalized distributions of stellar mass residual ﹩{\delta }_{\mathrm{log}({M}_{* ,\mathrm{BCG}})}﹩ for SC-Cls (red) and Iso-Cls (blue). The vertical dashed and the dotted lines show the median values of the residual distributions of SC-Cls and Iso-Cls, respectively. The width of the vertical band indicates the median uncertainty calculated by ﹩\sigma \sqrt{\pi /(2N)}﹩ where N and σ are the sample size and the standard deviation. The corresponding redshift bin, sample set, and KS test p-value of each panel are shown in the upper left corner. Given the offset of the median in the supercluster environments and the median uncertainty, all panels suggest BCG stellar mass has a marginal dependence on the supercluster environments.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: Left: halo mass M 200m  crossmatch between  ROCKSTAR  halo catalogs of low-resolution (N = 5123) and high-resolution (N = 10243) runs using a maximum separation 0.2 h −1 cMpc at redshift z = 1.0. The matched halo fraction, bias, and scatter are shown in the lower right corner. The color map indicates the halo count in each 2D histogram bin. Right: in both panels, the crossmatch between halo catalogs of different softening lengths is indicated by the red curves. The crossmatch between halo catalogs of different mass resolutions is indicated by the blue curves. Upper panel: the matched fraction as a function of redshift. Lower panel: bias (filled squares) and scatter (filled circles) as a function of redshift.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: The normalized distributions of rest-frame color M g − M r for SC-Cls (red) and Iso-Cls (blue). The vertical dashed and the dotted lines show the median values of the distributions of SC-Cls and Iso-Cls, respectively. The width of the vertical band indicates the median uncertainty. The values of medians and median uncertainties are listed in Table 5. The corresponding redshift bin, sample set, and KS test p-value of each panel are shown in the upper left corner. For demonstration purposes, we only show the color range that encompasses 98% of the sample.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: CAMIRA supercluster candidates and Iso-Cls in the CL 1604 field overlaid by the HSC PDR3 density map in two different redshift slices. The blue open circles represent the positions of CAMIRA clusters that are not associated with any supercluster candidates. The red open circles are CAMIRA clusters associated with supercluster candidates. The number labeled under each cluster is the redshift of the cluster. If we are confident (see Section 2.4) in the redshift of the clusters, then the redshift number is colored in green; otherwise redshift number is colored in yellow. We note that we invert the color map here compared to Figure 15 for display purposes.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: Stellar mass residual ﹩{\delta }_{\mathrm{log}({M}_{* ,\mathrm{BCG}})}﹩ as a function of richness for each redshift bin and each sample. The vertical gray lines show the edges of the richness bin. The red circles (blue-filled squares) and error bars are the medians and median uncertainties of ﹩{\delta }_{\mathrm{log}({M}_{* ,\mathrm{BCG}})}﹩ calculated within each richness bin for SC-Cls (Iso-Cls). The number in each richness bin shows the sample size.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: Supercluster total mass M tot distribution of unperturbed mock catalog (left) and perturbed mock catalog (right). Histograms of different colors correspond to different multiplicity bins indicated by the legend in the upper right corner.
Paper: A Systematic Search of Distant Superclusters with the Subaru Hyper Suprime-Cam Survey
Authors: Tsung-Chi Chen, Yen-Ting Lin, Hsi-Yu Schive, Masamune Oguri, Kai-Feng Chen, Nobuhiro Okabe, Sadman Ali, Connor Bottrell, Roohi Dalal, Yusei Koyama, Rogério Monteiro-Oliveira, Rhythm Shimakawa, Tomotsugu Goto, Bau-Ching Hsieh, Tadayuki Kodama, Atsushi J. Nishizawa
Figure caption: Same as Figure 20, but for SFR. For demonstration purposes, the range of SFR is chosen to encompass ≳99% of the samples.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: The top panel illustrates the fact that the total mass in all the protostars is likely to increase at a comparatively higher rate for the denser cloud in the initial stage of evolution. However, this trend reverses at around t ≈ 3–4 kyr, once the radiation pressure becomes significant and starts impacting the mass accretion rate. We observe a similar characteristic in the second panel that shows the effects of gas rotation (v gas) on the mass evolution. This is represented by the three rotation parameters g rot ≈ 0.0, 0.2, 0.4. Since the mass accretion rate is inversely proportional to the relative velocity between the gas and the protostars, a fast-rotating cloud results in the formation of comparatively low-mass stars. Once again, feedback changes the scenario in the later stages. The third panel shows the impact of the core size on the total mass evolution, which follows a similar trend until the epoch when radiative feedback becomes significant. Finally, the bottom panel demonstrates the effects of varying the suppressed accretion rate ﹩{\dot{M}}_{\sup }﹩ on the time evolution of the total mass in the protostars. We do not find the total mass to change dramatically as we vary the suppressed accretion rate.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: Combined scatter distribution of the mass and radial distance of the protostars from all five random realizations is demonstrated in the left-hand panel, whereas the right-hand panel depicts their individual distributions. Both the trends hold for all three values of f ≈ 1, 0.5, 0.1.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: The likelihood of finding at least one protostar (ψ cut) whose Bondi–Hoyle accretion rate exceeds the maximum accretion rate cutoff is lower when the radiation factor f is high. In such a scenario, fewer mergers lead to more protostars in the system. This introduces increased dynamical interactions that induce rapid fluctuations in their velocities. Thereby, the Bondi–Hoyle accretion rate drops below the cutoff, resulting in a more sustained accretion.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: The left-hand panel demonstrates the cumulative number of mergers with time taking all five random realizations into account for three values of f ≈ 0.1, 0.5, 1. As expected, a lower value of f leads to a higher number of mergers that kick in earlier as a result of dynamical friction. On the other hand, we do not see such a distinct trend in the cumulative number of mergers with the radial distance in the right-hand panel.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: The trajectories of the two particles, i.e., P1 (in red) and P2 (in orange), which merge together, are demonstrated in the x − y plane (left-hand panel). It is to be noted that both the particles are coming from the opposite direction with the same speed, and the particle P2 merges into the particle P1. Hence, the x-component of the velocity of the merged P1 becomes 0, whereas the y-component remains unchanged.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: The well-established Figure-8 solution for the three-body problem has been numerically reproduced, ensuring the correctness of our N-body solver. The trajectories of all three particles P1, P2, and P3 exhibit a similar profile resembling the shape of the number “8.”
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: The ICs, i.e., distribution of initial mass, velocity, and radial distance of the 10 protostars in the four random realizations, namely r1, r2, r3, and r4 follow the same distribution as the fiducial model. This IC corresponds to physical systems explored in previous studies, the details of which are mentioned in Section 2.8.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: The time evolution of the radial distance (the top panel), accretion rate (the middle panel), and mass (the bottom panel) of the evolving protostar show similar trends in all five realizations. Every realization shows previously observed phenomena, such as close encounters, mergers, and the escape phenomenon.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: The numerical test is performed for a one-particle system in order to verify the correctness of the dynamics. The time evolution of the radial distance (denoted in black) is similar to the previous study by J. Dutta et al. (2020)
Paper: Common Envelopes, Gamma Rays, and Sudden Spectral Changes of Novae
Authors: Robert Williams, Russell Ryan, Richard Rudy
Figure caption: ARAS spectra of V5855 Sgr shortly after outburst. Except for Hα, the P Cygni profiles present in the initial October 20 spectrum have disappeared by October 23. The spectrum suddenly emerging on October 26 shows emission lines prominent, with the large majority of absorption lines present on October 25 having disappeared within 24 hr.
Paper: Common Envelopes, Gamma Rays, and Sudden Spectral Changes of Novae
Authors: Robert Williams, Russell Ryan, Richard Rudy
Figure caption: Nova V1405 Cas displayed classic Fe II-phase spectra in these ARAS spectra with narrow Fe II P Cygni profiles having prominent absorption components until their disappearance on May 16. Non-Balmer emission components weakened significantly between May 3 and 8, as narrow absorption features appeared and strengthened, especially below 4700 Å, until their disappearance.
Paper: Common Envelopes, Gamma Rays, and Sudden Spectral Changes of Novae
Authors: Robert Williams, Russell Ryan, Richard Rudy
Figure caption: Light curves for the five novae whose spectra are presented in Figures 1–5, taken from AAVSO observations. Visible measurements are displayed in green, with r-band brightness denoted by red squares. Vertical lines mark the dates on which the ARAS spectra were obtained that are shown in Figures 1–5. Purple horizontal brackets denote the time interval when γ-ray emission was detected by the Fermi LAT.
Paper: Common Envelopes, Gamma Rays, and Sudden Spectral Changes of Novae
Authors: Robert Williams, Russell Ryan, Richard Rudy
Figure caption: ARAS spectra for V613 Sct show this nova’s spectrum to have transformed significantly within a 20 hr period on July 1 from very prominent, narrow absorption lines to an emission spectrum. During the July 1 transformation interval, the visible brightness may have decreased by an amount on the order of 0.5 mag, as shown in Figure 6.
Paper: Common Envelopes, Gamma Rays, and Sudden Spectral Changes of Novae
Authors: Robert Williams, Russell Ryan, Richard Rudy
Figure caption: After an initial Fe II-phase emission spectrum, between October 28 and 30 the V5856 Sgr spectrum changed from emission to a dominant absorption spectrum. The absorption lines strengthened and persisted until November 12, when emission components reappeared in the form of P Cygni profiles. By November 18, the spectrum had reverted to its initial Fe II emission structure.
Paper: Common Envelopes, Gamma Rays, and Sudden Spectral Changes of Novae
Authors: Robert Williams, Russell Ryan, Richard Rudy
Figure caption: V1674 Her displayed a He/N-phase spectrum during its rapid decline in brightness. Strong, broad absorption lines initially present in these ARAS spectra disappeared rapidly on June 13 as the spectrum became dominated by strong emission features.
Paper: Studying the Effect of Radiation Pressure on Evolution of a Population III Stellar Cluster
Authors: Sukalpa Kundu, Jayanta Dutta
Figure caption: Each realization leads to the formation of binary pairs. Two selected pairs from each realization are illustrated above.