adsabs/AstroCLIMB huggingface dataset:
Paper: Bright in the Black: Searching for Electromagnetic Counterparts to Gravitational-wave Candidates in LIGO-Virgo-KAGRA Observation Runs with AstroSat-CZTI
Authors: Gaurav Waratkar, Varun Bhalerao, Dipankar Bhattacharya
Figure caption: We show the isotropic equivalent luminosity L iso erg s−1 (1 keV – 10 MeV) upper limits from AstroSat-CZTI searches as a function of calculated luminosities derived from GRB 150914-GBM for the neutrino model for the case of GW151226. As described in Section 4, we can rule out the luminosities below the diagonal, mainly using our 10 s weighted sensitivity.
Paper: The Oscillation in Evolution of Changing-look Blazar OQ 334
Authors: S. S. Ren, R. X. Zhou, Y. G. Zheng, S. J. Kang
Figure caption: Schematic of the changing-look blazar (CLB) long-term evolution. Green shading indicates the BL Lac state, while purple represents the FSRQ state. The vertical axis represents states, and the horizontal axis denotes the logarithmic values of the timescales for the epochs F and B. Data for the F 1, B 1, F 2, and B 2 are from S. S. Ren et al. (2024).
Paper: Holographic Beam Measurements of the Canadian Hydrogen Intensity Mapping Experiment (CHIME)
Authors: Mandana Amiri, Arnab Chakraborty, Simon Foreman, Mark Halpern, Alex S Hill, Gary Hinshaw, T. L. Landecker, Joshua MacEachern, Kiyoshi W. Masui, Juan Mena-Parra, Nikola Milutinovic, Laura Newburgh, Anna Ordog, Ue-Li Pen, Tristan Pinsonneault-Marotte, Alex Reda, Seth R. Siegel, Saurabh Singh, Haochen Wang, Dallas Wulf
Figure caption: The beam centroids for all feeds along the four cylinders (columns, centroids plotted against the lower x-axis), and for all six sources (rows, in descending order from the highest-decl. source at the top, Cas A, to the lowest, Hya A, at the bottom). Both polarizations are overplotted, and we take a median average over the band. The patterns of variation within a cylinder are consistent between polarizations. The centroid wander is mostly within ±0.15°, corresponding to offsets of the feeds from the cylinder axis ∼1 cm. The solid blue lines indicate measurements of the actual physical displacements (plotted against the upper x-axis) of the CHIME feeds obtained through photogrammetry of the focal lines; these measurements can only determine the displacements up to an overall misalignment of the focal line and so are always centered about 0. The centroid variation is, as expected, correlated with the pattern of feed misalignments, up to the missing overall offset per cylinder. This overall offset noticeably scales with decl. for Cylinder B.
Paper: Holographic Beam Measurements of the Canadian Hydrogen Intensity Mapping Experiment (CHIME)
Authors: Mandana Amiri, Arnab Chakraborty, Simon Foreman, Mark Halpern, Alex S Hill, Gary Hinshaw, T. L. Landecker, Joshua MacEachern, Kiyoshi W. Masui, Juan Mena-Parra, Nikola Milutinovic, Laura Newburgh, Anna Ordog, Ue-Li Pen, Tristan Pinsonneault-Marotte, Alex Reda, Seth R. Siegel, Saurabh Singh, Haochen Wang, Dallas Wulf
Figure caption: The CHIME X-polarized beam response at 717 MHz from the holographic measurements of a Cyg A transit, taken on 2018 September 28. Each panel shows the median response taken over all feeds within a cylinder, normalized such that the copolar response is 1 + 0j at transit. Upper left: the median copolar amplitude of all feeds per cylinder, normalized by the Gaussian-fit peak height, over the full extent of the observation, converted to degrees on-sky, HA ﹩\cdot \cos \left({\delta }_{\mathrm{CygA}}\right);﹩ Upper right: the median cross-polar amplitude from the product of a CHIME feed with the opposite polarization on the Galt receiver. The data have been scaled by the same factor as applied to the copolar response, so the curves give an indication of the level of cross-polarization in the beam. Middle left: same as the upper-left panel, but zoomed to a smaller hour angle (HA) range and plotted on a linear scale. Middle right: same as the upper-right panel, but zoomed to a smaller HA range and plotted on a linear scale. Lower left: the median copolar phase as a function of scaled HA, taken over all feeds in a cylinder (the median was evaluated for the real and imaginary parts separately before evaluating the phase). Lower right: same as the lower-left panel for the cross-polar phase. The phase difference between cylinders, after accounting for phase wrap, is only large near the first zero-crossing of the field. The gray bands in the amplitude plots indicate the standard deviation over all the Cyg A holography tracks of Cylinder A’s median feed response (Cylinder A is representative).
Paper: Holographic Beam Measurements of the Canadian Hydrogen Intensity Mapping Experiment (CHIME)
Authors: Mandana Amiri, Arnab Chakraborty, Simon Foreman, Mark Halpern, Alex S Hill, Gary Hinshaw, T. L. Landecker, Joshua MacEachern, Kiyoshi W. Masui, Juan Mena-Parra, Nikola Milutinovic, Laura Newburgh, Anna Ordog, Ue-Li Pen, Tristan Pinsonneault-Marotte, Alex Reda, Seth R. Siegel, Saurabh Singh, Haochen Wang, Dallas Wulf
Figure caption: FWHM of the holographic beam response as a function of frequency and median-averaged over cylinder A (representative of all cylinders) for all six sources presented in this work. Both polarizations are shown: the X-polarized response is wider in east–west than the Y-polarized response, while the 30 MHz ripple (a purely geometric effect) in the beamwidth is apparent in both polarizations and dominates the modulation of the beamwidth in frequency. After adjusting for the decl. dependence of the on-sky angular distance subtended in 1° of HA, the magnitude of the beamwidth is consistent between sources, but the locations of the peaks of the 30 MHz ripple are seen to shift with declination.
Paper: Holographic Beam Measurements of the Canadian Hydrogen Intensity Mapping Experiment (CHIME)
Authors: Mandana Amiri, Arnab Chakraborty, Simon Foreman, Mark Halpern, Alex S Hill, Gary Hinshaw, T. L. Landecker, Joshua MacEachern, Kiyoshi W. Masui, Juan Mena-Parra, Nikola Milutinovic, Laura Newburgh, Anna Ordog, Ue-Li Pen, Tristan Pinsonneault-Marotte, Alex Reda, Seth R. Siegel, Saurabh Singh, Haochen Wang, Dallas Wulf
Figure caption: Top: all feeds on Cylinder B, at 717 MHz, overplotted in colors with the median along Cylinder B in black. Bottom: residuals between the median profile of Cylinder B and all feeds on Cylinder B. The shaded bands around 0 represent 5% and 10% deviations from the median, relative to the peak. CHIME is a highly redundant array geometrically; here, we observe variations in the per-feed beam response off-axis which are comparable to the overall sidelobe level. The larger residuals near transit are primarily due to centroid wander along feeds; see Figure 8.
Paper: Holographic Beam Measurements of the Canadian Hydrogen Intensity Mapping Experiment (CHIME)
Authors: Mandana Amiri, Arnab Chakraborty, Simon Foreman, Mark Halpern, Alex S Hill, Gary Hinshaw, T. L. Landecker, Joshua MacEachern, Kiyoshi W. Masui, Juan Mena-Parra, Nikola Milutinovic, Laura Newburgh, Anna Ordog, Ue-Li Pen, Tristan Pinsonneault-Marotte, Alex Reda, Seth R. Siegel, Saurabh Singh, Haochen Wang, Dallas Wulf
Figure caption: Waterfall plots (in feed index vs. sky degrees) of the stacked Cyg A data. For each cylinder data are taken from 717 MHz. The top two rows show copolar data while the bottom two rows show cross-polar. The one-dimensional slices above each image panel show the median along the respective cylinders. At a fixed frequency, the width of the main beam is stable along feeds, although the beams in X polarization are wider than those in Y polarization. The beam centroids vary along the cylinders due to small misalignments of the feeds from the cylinder axis. There are also asymmetries in the first sidelobes. The cross-polar response exhibits a strong enhancement off-axis at the locations of the focal-line support legs.
Paper: Holographic Beam Measurements of the Canadian Hydrogen Intensity Mapping Experiment (CHIME)
Authors: Mandana Amiri, Arnab Chakraborty, Simon Foreman, Mark Halpern, Alex S Hill, Gary Hinshaw, T. L. Landecker, Joshua MacEachern, Kiyoshi W. Masui, Juan Mena-Parra, Nikola Milutinovic, Laura Newburgh, Anna Ordog, Ue-Li Pen, Tristan Pinsonneault-Marotte, Alex Reda, Seth R. Siegel, Saurabh Singh, Haochen Wang, Dallas Wulf
Figure caption: Waterfall plots (in frequency vs. sky degrees) of the stacked Cyg A data. For each cylinder, we take a median over all feeds of a given polarization. Zeroed-out bands or points in the data are due to flagged RFI. In this projection of the data the 30 MHz breathing of the beamwidth (see Figure 5) creates a “vertebrae” pattern along the main lobe and first null in the frequency axis. This structure arises from multipath effects in the cavity between the cylinder vertices and the focal line. The X and Y dipoles of the CHIME clover-leaf feeds do not illuminate the telescope equally; note the change in beamwidth and sidelobe patterns between polarizations, as well as an enhanced response in XY relative to YX.
Paper: Holographic Beam Measurements of the Canadian Hydrogen Intensity Mapping Experiment (CHIME)
Authors: Mandana Amiri, Arnab Chakraborty, Simon Foreman, Mark Halpern, Alex S Hill, Gary Hinshaw, T. L. Landecker, Joshua MacEachern, Kiyoshi W. Masui, Juan Mena-Parra, Nikola Milutinovic, Laura Newburgh, Anna Ordog, Ue-Li Pen, Tristan Pinsonneault-Marotte, Alex Reda, Seth R. Siegel, Saurabh Singh, Haochen Wang, Dallas Wulf
Figure caption: The tracks of all holography observations taken to date, shown in orthographic projection on the sky to illustrate the maximum sky coverage of the data set. The red circle of radius 1 in these coordinates represents CHIME’s horizon, i.e., the inner area of the circle represents the extent of CHIME’s observable sky. Various marker shapes denote the centers of tracks that correspond to the brightest sources presented in this work. We note that earlier observations (which tended to be more focused on brighter sources) would track source transits for longer periods of time, corresponding to long tracks on the sky. More recent observations have preferentially (but not exclusively) targeted dimmer sources and in shorter tracks.
Paper: Holographic Beam Measurements of the Canadian Hydrogen Intensity Mapping Experiment (CHIME)
Authors: Mandana Amiri, Arnab Chakraborty, Simon Foreman, Mark Halpern, Alex S Hill, Gary Hinshaw, T. L. Landecker, Joshua MacEachern, Kiyoshi W. Masui, Juan Mena-Parra, Nikola Milutinovic, Laura Newburgh, Anna Ordog, Ue-Li Pen, Tristan Pinsonneault-Marotte, Alex Reda, Seth R. Siegel, Saurabh Singh, Haochen Wang, Dallas Wulf
Figure caption: The range of holography observations used in this paper. In each panel the span of the transit in hour angle (HA) on a particular day is indicated by the length of the vertical line. Most observations are within ±60°. The number of observations of each source used in this paper is indicated in the panel titles.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: Illustration of our favored physical model for Godzilla and its nebula. Due to highly efficient radiative cooling, massive star ejecta from winds and CCSNe has accumulated at the center of a massive, compact young star cluster, forming self-shielded neutral warm gas in a state of supersonic turbulence driven by energy injection from CCSNe. Situated in an extreme radiation environment, this gravitationally retained gas likely has little to no dust. As a result, it is optically thick to ionizing photons but is transparent to UV and optical photons. O stars embedded inside it drive individual wind-blown hot bubbles in which the observed nebula emission lines are excited. In the outskirts of the cluster, stars likely drive a hot, low-density cluster wind that may accelerate warm cloudlets resulting in a secondary broad nebular emission component.
Paper: Multispectral Sirens: Gravitational-wave Cosmology with (Multi-) Subpopulations of Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Yuan-Zhu Wang, 远瞩 王, Yi-Zhong Fan, 一中 范
Figure caption: Hubble constant (left) and expansion rate (middle) inferred with events in GWTC-3 selected by SNR > 10 and the results combined with GW170817 (B. P. Abbott et al. 2017c; right). In the left and right panels, the pink and green bands represent the Hubble constant measured from CMB (Planck Collaboration et al. 2016) and that measured in the local universe (A. G. Riess et al. 2019), respectively. The dotted line represent the prior distribution. In the middle panel, the shaded regions and solid lines are for 90% credible intervals and median values, respectively.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: HST false-color image of the Sunburst Arc with the lone image of Godzilla and four images of the LyC cluster marked. Godzilla appears similarly bright to the multiple images of the LyC cluster, so naively, multiple counterimages of Godzilla would be detectable in a typical strong-lensing configuration. However, the nondetection of counterimages and time variability favors the hypothesis that Godzilla is millilensed and highly magnified.
Paper: Multispectral Sirens: Gravitational-wave Cosmology with (Multi-) Subpopulations of Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Yuan-Zhu Wang, 远瞩 王, Yi-Zhong Fan, 一中 范
Figure caption: Distributions of the parameters for the cosmology model and the PP population model (without spin distribution) using the events with SNR > 11 in GWTC-3. The dashed lines in the marginal distribution represent the median and 68.3% credible intervals.
Paper: Multispectral Sirens: Gravitational-wave Cosmology with (Multi-) Subpopulations of Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Yuan-Zhu Wang, 远瞩 王, Yi-Zhong Fan, 一中 范
Figure caption: Distributions of the Hubble constant, the maximum mass of the first subpopulation, and the masses of the 99.5% and 99% percentiles. The dashed lines in the marginal distribution represent the median and 90% credible intervals.
Paper: Multispectral Sirens: Gravitational-wave Cosmology with (Multi-) Subpopulations of Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Yuan-Zhu Wang, 远瞩 王, Yi-Zhong Fan, 一中 范
Figure caption: Posterior distributions of the hyperparameters inferred with the TwoSpin model and events in GWTC-3 selected by SNR > 11. The dashed lines in the marginal distribution represent the median and 68.3% credible intervals.
Paper: Multispectral Sirens: Gravitational-wave Cosmology with (Multi-) Subpopulations of Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Yuan-Zhu Wang, 远瞩 王, Yi-Zhong Fan, 一中 范
Figure caption: Component-mass and spin-magnitude distributions in the multispectral sirens, inferred with the TwoSpin model and 42 BBHs with SNRs > 11 in GWTC-3. The solid lines and dashed regions are for the median and 90% C.Ls.
Paper: Multispectral Sirens: Gravitational-wave Cosmology with (Multi-) Subpopulations of Binary Black Holes
Authors: Yin-Jie Li, 银杰 李, Shao-Peng Tang, 少鹏 唐, Yuan-Zhu Wang, 远瞩 王, Yi-Zhong Fan, 一中 范
Figure caption: Component-mass and spin-magnitude distributions of the subpopulations in the multispectral sirens, inferred using the TwoSpin model with 50 mock detections in O3. The solid lines and dashed regions are for the median and 90% C.Ls.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: Fractional flux changes with respect to the mean for Godzilla (black) and image 8 of the LyC cluster (purple) sampled across eight visits of HST WFC3/IR F140W. These eight visits make up four distinct epochs relative to the timescales for microlensing fluctuations (≳few days), with the first visit occurring on 2019 June 24. We observe that image 8 of LyC, which is not expected to showcase significant microlensing-induced variability, fluctuates at the ∼2% level, while Godzilla fluctuates marginally more at the ∼3% level and shows the largest fractional change between any two visits of ∼13%. We note that the visit with the greatest fractional change of ∼8% at 14 months is accompanied by three other visits with comparatively smaller fractional changes. These four visits take place over the span of 2 days, a timescale that is likely too short for microlensing to induce significant variability.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: Same as Figure 11 but with abundances plotted relative to oxygen and normalized to the solar value. For reference, we also plot for cumulative ejecta with CCSNe yields of Ne and Si excluded (black dashed lines). We find that the MT12 predictions agree with the inferred abundances of Godzilla at ∼4–6  Myr, with the exception of Ne/O, which only shows agreement if the CCSN Ne yield is significantly reduced (black dashed line).
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: Probability distribution for the maximal observed flux variation expected for a single lensed star, derived from simulating the cadence pattern of the four actual distinct imaging epochs in F140W (solid curves). We set a local macroconvergence κ B = 0.7, κ ⋆ = 0.001 and assume an unresolved macroimage pair of μ B = ±3500. The black vertical line marks the maximal fractional flux change of 13% between two epochs measured through aperture photometry. The results depend on the unknown effective velocity of the source v  t , which, in Planck 2015 cosmology, has a standard deviation of 600 km s−1 for the Sunburst system. The single lensed star scenario is compatible with the data only if the effective velocity is unusually small, e.g., v  t  = 50 km s−1, and would be tightly constrained with another measurement in 2024 or later (dashed curves).
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: ICL surface brightness profile in HST WFC3/IR F160W measured via elliptical isophotes (purple) centered at the BCG. The surface brightness profile begins to flatten at a semimajor axis of ∼25″, which may indicate that the ICL is approaching the diffuse sky background. To conservatively estimate the ICL contribution at the location of Godzilla (∼30″), we fit a Sérsic profile to isophotes with semimajor axis a ≤ 25″ and extrapolate to the location of Godzilla. We find an ICL surface brightness of ﹩\sim 25.5\,\mathrm{mag}\,{\mathrm{arcsec}}^{-2}﹩, corresponding to an average convergence κ ⋆ ≳ 0.001 from intracluster stars. We note that the surface brightness profile shows a peak at the location of the Sunburst Arc due to the diffuse arc background not being well masked by SExtractor, where the arc generally makes up a large fraction of the isophote at that semimajor axis.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: Probability distributions of ﹩1+\delta =\mu /\bar{\mu }﹩ for any individual source star, derived separately for a pair of macroimages with macromagnification factors ﹩\bar{\mu }=\pm 500﹩ (blue) and ﹩\bar{\mu }=\pm 1000﹩ (red). The value of ﹩\sqrt{\langle {\delta }^{2}\rangle }﹩ for each macroimage is quoted in the legend text. We set a local macroconvergence κ B = 0.7, κ ⋆ = 0.001 and use a relatively large average value for the stellar photosphere radius R ⋆ = 160 R ⊙ in order to be conservative in estimating ﹩\sqrt{\langle {\delta }^{2}\rangle }﹩.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: HST false-color image of Godzilla, the “P knots,” and the candidate counterimages identified by J. M. Diego et al. (2022) and K. Sharon et al. (2022); the labeling reflects the naming scheme of both papers. Godzilla is significantly brighter than its counterimages, implying that it is highly magnified by comparison. The color of the counterimages may more closely match the color of the P knots, which may indicate that Godzilla is intrinsically fainter than the P knots and is blended with and dominated by them in the counterimages. This figure is modeled after K. Sharon et al.'s (2022) Figure 2 and S. Choe et al.'s (2024) Figure 1, which both show color images using different HST or JWST filters and provide useful further reference for the relative colors of Godzilla, the P knots, and the candidate counterimages.
Paper: Stellar Bars Form Dark Matter Counterparts in TNG50
Authors: Neil Ash, Monica Valluri, Yingtian Chen, Eric F. Bell
Figure caption: Contributions to the potential from stellar (left columns), DM (center columns), and gas (right columns) particles for TNG50 subhaloID 574286. Top row: rotated l, m = 2 quadrupolar coefficients for the “coarse” time resolution main TNG50 box (left-hand side of each column) next to the high time resolution Subbox-0 snapshots between 0.2 ≤ t  lb  ≤ 1.2 Gyr (right-hand side of each column, tick intervals are 250 Myr) for the same halo. The locations of the “coarse” time resolution snapshots are shown here as dashed horizontal lines. Bottom row: contours for the BFE density model of each particle type overplotted on the midplane mass density at z ∼ 0. Each of the plots are taken in primed coordinates rotated such that the bar major axis lies along ﹩x^{\prime} ﹩ and the minor axis along ﹩z^{\prime} ﹩ (out of the page).
Paper: Stellar Bars Form Dark Matter Counterparts in TNG50
Authors: Neil Ash, Monica Valluri, Yingtian Chen, Eric F. Bell
Figure caption: Bar metrics applied to the RG22 disk galaxy catalog for DM (left) and stellar (right) particle distributions. Top row: A 2(r), with the median (dashed line) and interquartile ranges (shaded region) shown for both the barred (red) and unbarred (blue) populations The median A 2(r) curves show that the DM in barred galaxies is typically elongated within ∼2 kpc more strongly than in unbarred galaxies. Middle row: histograms for ﹩{A}_{2,\max }﹩. Medians (dashed lines) and the interquartile region (dotted lines) of the distributions are shown. Bottom row: cumulative histogram of the difference in phase angles φ(r) between the stellar and DM mass distributions, measured where the bar amplitudes are typically highest. Typical measurement uncertainty is indicated by the black line.
Paper: Stellar Bars Form Dark Matter Counterparts in TNG50
Authors: Neil Ash, Monica Valluri, Yingtian Chen, Eric F. Bell
Figure caption: Normalized BFE quadrupole power C 2/C 0 of the density. The presence of the bar in both DM and stars is demonstrated by the relatively large amplitude at small radii, which falls to some minimum value around ∼3 kpc before rising again due to the disk/halo component. The minimum of A 2(r) measured by RG22 is shown by the cyan squares at t  lb  = 0, 5.2, and 7.9 Gyr and does not share a common minimum with C 2/C 0. The corotation radius of the bars is overplotted as the pink dotted line and demonstrates that the stellar bar is always a fast bar (r bar ≤ r corot ≤ 1.4 · r bar; shaded cyan region shows 1–1.4 · r bar).
Paper: Stellar Bars Form Dark Matter Counterparts in TNG50
Authors: Neil Ash, Monica Valluri, Yingtian Chen, Eric F. Bell
Figure caption: Evolution of the bar rotation axis. Rather than remaining stationary, the rotation axis undergoes both precession and nutation over the 8 Gyr time course. The precession frequency varies over the time course, at times rising suddenly (see, e.g., the blow-up of a loop structure on the right). Nutations are visible as the higher-frequency arcs that occur repeatedly throughout the loop structure and continuously during the time course. Pericenter passages of massive satellites are marked as magenta stars. The rotation axis precession is shown in an arbitrary inertial reference frame in which ϕ″ and θ″ refer to the azimuthal and polar angles, respectively.