adsabs/AstroCLIMB huggingface dataset:
Paper: Onset of Particle Acceleration during the Prompt Phase in Gamma-Ray Bursts as Revealed by Synchrotron Emission in GRB 160821A
Authors: Felix Ryde, Shabnam Iyyani, Björn Ahlgren, Asaf Pe'er, Vidushi Sharma, Christoffer Lundman, Magnus Axelsson
Figure caption: The posterior distribution of the fitted power-law index of the accelerated electron distribution in interval 2. The injected power-law slope p is steepened by unity due to the cooling. The shaded area is the 95% credible region. The fitted value of p = 2.3 ± 0.2 is in line with the robust expectations for particle acceleration in weakly magnetized flows (Sironi et al. 2015).
Paper: Consistency of the Parkes Pulsar Timing Array Signal with a Nanohertz Gravitational-wave Background
Authors: Boris Goncharov, Eric Thrane, Ryan M. Shannon, Jan Harms, N. D. Ramesh Bhat, George Hobbs, Matthew Kerr, Richard N. Manchester, Daniel J. Reardon, Christopher J. Russell, Xing-Jiang Zhu, Andrew Zic
Figure caption: Comparison of common-spectrum and quasi-common-spectrum processes in the PPTA DR2. Left: marginalized posterior for ﹩{\sigma }_{{\mathrm{log}}_{10}A}﹩. The value is consistent with zero, which means that the common-spectrum hypothesis holds for the PPTA data. The vertical dashed line is the upper limit on ﹩{\sigma }_{{\mathrm{log}}_{10}A}﹩ at 95% credibility. Right: full posterior for ﹩{\mu }_{{\mathrm{log}}_{10}A}﹩ and ﹩{\sigma }_{{\mathrm{log}}_{10}A}﹩. The vertical dashed line corresponds to the measurement of ﹩{\mathrm{log}}_{10}A﹩ of the common-spectrum process in PPTA DR2 (Goncharov et al. 2021a). Our inference of the common-spectrum-process amplitude is consistent with the previous measurement considering the generalization of the model and the use of likelihood reweighting. Three closed lines correspond to the standard 1σ, 2σ, and 3σ levels. In both panels, the dashed–dotted lines show the measurements performed without three PSRs with special noise properties discussed in Section 3: J0437−4715, J0711−6830, and J1643−1224. Removing these pulsars from the analysis increases uncertainty levels, as expected.
Paper: Consistency of the Parkes Pulsar Timing Array Signal with a Nanohertz Gravitational-wave Background
Authors: Boris Goncharov, Eric Thrane, Ryan M. Shannon, Jan Harms, N. D. Ramesh Bhat, George Hobbs, Matthew Kerr, Richard N. Manchester, Daniel J. Reardon, Christopher J. Russell, Xing-Jiang Zhu, Andrew Zic
Figure caption: Searches for a quasi-common-spectrum process in a simulated data set. Left: marginalized posterior for ﹩{\sigma }_{{\mathrm{log}}_{10}A}﹩. The value is inconsistent with zero, which means that the signal that would have been interpreted as the common-spectrum process with the standard methods is only a quasi-common-spectrum process. Based on this result, the gravitational-wave origin of the signal can be ruled out. The simulated value is represented by the vertical dotted line and cumulative 1σ credible levels are represented by a shaded region. Right: full posterior on ﹩{\mu }_{{\mathrm{log}}_{10}A}﹩ and ﹩{\sigma }_{{\mathrm{log}}_{10}A}﹩. The vertical and the horizontal lines correspond to the simulated values. Three closed lines correspond to the standard 1σ, 2σ, and 3σ levels.
Paper: Optical Light Curve of 4FGL J0935.3+0901: A Flaring Black Widow Candidate
Authors: Jules P. Halpern
Figure caption: Time-series photometry of 4FGL J0935.3+0901 on the MDM 1.3 m, and a Lomb–Scargle periodogram of the combined data. The best-fitted period corresponds to the highest peak at 9.85 cycles day−1 (arrow). Points in red were excluded from the periodogram and the mean folded light curve.
Paper: Optical Light Curve of 4FGL J0935.3+0901: A Flaring Black Widow Candidate
Authors: Jules P. Halpern
Figure caption: High-cadence observations by ZTF on two consecutive nights in 2019. Note the overall change of ≈0.4 mag between nights, as well as apparent flaring up to r = 19.16 on the second night (red points). The bottom panel shows the Lomb–Scargle periodogram of the combined nights’ data, excluding points having r < 20.0.
Paper: Optical Light Curve of 4FGL J0935.3+0901: A Flaring Black Widow Candidate
Authors: Jules P. Halpern
Figure caption: Bottom panel: a periodogram of the entire ZTF r-band data set, but excluding points with r < 20.0 (red, top), identifies the strongest peak as 9.85 cycles day−1. The corresponding ephemeris is listed in line 3 of Table 2. Top panel: folded light curve with phase defined such that maximum light occurs at ϕ = 0.75, the presumed superior conjunction of the companion star.
Paper: No Evolution in the Half-mass Radius of Milky Way–type Galaxies over the Last 10 Gyr
Authors: Maryam Hasheminia, Moein Mosleh, Sandro Tacchella, S. Zahra Hosseini-ShahiSavandi, Minjung Park, Rohan P. Naidu
Figure caption: Comparison of the redshift evolution of r 50 (panel (a)), Sérsic index (panel (b)), and stellar mass (panel (c)) of MW progenitors with recent observational and theoretical studies. Lines and symbols follow Figures 1 and 2. The gray rectangle represents the MW’s r 50 derived from the McMillan (2017) profile and corrected with the typical r mass/r light from Mosleh et al. (2017). Overall, a consistent picture for the MW galaxy arises: While the stellar mass has increased by >1 order of magnitude over the past 10 Gyr, the half-mass size has roughly stayed constant. Over the same time span, the Sérsic index increased from disk like (close to 1) to 2–4 at lower redshift, consistent with the formation of a thick disk or bulge.
Paper: No Evolution in the Half-mass Radius of Milky Way–type Galaxies over the Last 10 Gyr
Authors: Maryam Hasheminia, Moein Mosleh, Sandro Tacchella, S. Zahra Hosseini-ShahiSavandi, Minjung Park, Rohan P. Naidu
Figure caption: (a) Comparing the median stellar-mass density profiles of MW-type progenitors, along with the profiles of the MW from the best-fit parameters estimated by McMillan (2017). (b) The total stellar-mass growth within different apertures. The stellar mass in the core has more rapidly increased than that in the other regions from z = 1.1 to z = 0.7, consistent with the decrease in r 20 and increase in Σ1 over the same epoch (Figure 2).
Paper: No Evolution in the Half-mass Radius of Milky Way–type Galaxies over the Last 10 Gyr
Authors: Maryam Hasheminia, Moein Mosleh, Sandro Tacchella, S. Zahra Hosseini-ShahiSavandi, Minjung Park, Rohan P. Naidu
Figure caption: Evolution of the size (panel (a)), Sérsic index (panel (b)), central stellar-mass density Σ1 (panel (c)), and axis ratio (panel (d)) with redshift for MW progenitors. The yellow circles and cyan squares are for the MW-type and MW progenitors, respectively, and the solid red and blue lines are the corresponding best fits. The green solid lines show the evolution of the TNG50 MW-like galaxies. In panel (a), dashed (small symbols), solid (large symbols), and dotted (small symbols) lines indicate the median evolution of the radii that enclose 20% (r 20), 50% (r 50), and 80% (r 80) of the stellar mass, respectively. In panel (c), the red and blue hex-histograms show the Σ1 distribution of quiescent galaxies and SFGs of a stellar-mass-complete sample. A considerable decrease in r 20 and an increase in the Sérsic index and Σ1 are observed with cosmic time, whereas r 50 and r 80 remain approximately constant. In contrast, the TNG50 MW-like galaxies show a significant increase in r 20, r 50, and r 80 with cosmic time.