adsabs/AstroCLIMB huggingface dataset:
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: CHIME visibilities (XX-polarization) as a function of baseline separation at a frequency of 612.5 MHz for a single 10 s time integration acquired on 2019 October 24. At this time, the visibilities are dominated by the signal from Cyg A, which is in the main lobe of the primary beam at an HA of 1◦. The visibilities have been fringe-stopped to the location of Cyg A and normalized so that they are equal to 1 at the transit of Cyg A. Each column corresponds to a different east–west baseline distance, with the x-axis denoting the north–south baseline distance. The redundant copies of each baseline have been averaged. The data are shown in black, the best-fit, simple model given by Equation (15) is shown in blue, and the best-fit, holography-based model given by Equation (16) is shown in red. The visibilities exhibit ∼10% variations across baselines, which are not captured by a simple point-source model but are well described by a model consisting of a point source modulated by the feed-dependent primary beam pattern inferred from holographic observations of this source. The fine structure present in the visibilities as a function of north–south baseline distance is due to fainter sources within the CHIME FOV that are not being modeled during the fit.
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: Comparison of the solar beam measurement at the decl. of Tau A with the beam profile as measured by holography of Tau A, at 786 MHz. Top: in YY-polarization, the measurements are comparable to one another. Middle: in XX-polarization, CHIME’s beam sees an excess on either side of the meridian, due to polarization leakage from CHIME Y to CHIME X. The holographic measurement here, constructed purely from the copolarized data, does not include that leakage and appears with an ordinary Gaussian main lobe. Bottom: after including cross-polarized holography in the reconstruction, the “double bump” feature is successfully captured.
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: amplitude of the full stack of Her A transits for a single frequency and feed. All input transits are overplotted in gray. The individual transits are dominated by the noise bias at the level of −10 dB, while beam features outside the main lobe and at lower amplitudes start to be discerned in the stack. Middle panel: the real part of the residuals between the stack and the individual transits, where the blue shaded region indicates the span of two standard errors about the mean σ obs, and centered about 0. Bottom: the standard error on the stack (in blue) compared to the fast-cadence estimate of the radiometric noise (in black), indicating that the noise observed in the stack for this frequency and feed follows the behavior of the expected thermal noise.
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: Right: the common-mode primary beam profiles computed from the stacks of six holography sources, in YY-polarization at 759 MHz, presented in order of descending decl. from top to bottom. Left: the solar measurement is plotted in orthographic projection with amplitude mapped to color; holography tracks are overplotted with colored lines outlining the tracks (colored outlines in the left panel correspond to the source with the same color in the one-dimensional panels). Tau A, Vir A, Her A, and Hya A overlap the solar measurement; slices of the solar data are overplotted in black in the right panels for these overlapping sources.
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 row of corner plots: jack-knives for two different partitions of the Cyg A data set. The three image panels for each case show the real part of the fractional residuals (i.e., normalized by the value of the beam as measured by the final stack in that pixel) in the three different spaces of the data: feed (for cylinder A) vs. frequency (taking a median over HA), HA vs. frequency (taking a median over feeds on cylinder A), and HA vs. feed (taking a median over frequency). Bottom row of corner plots: noise realizations of the jack-knives, i.e., what we would have expected to see from the differencing procedure had the stacks of each partition been identical with the exception of their noise realizations. In both cases only the real part is plotted. The residuals indicate systematic differences between partitions of the data at the subpercent level between disjoint subsets of the data. However, from the comparison of the two jack-knives it is not evident that these systematics are correlated with temperature.
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 best-fit peak amplitudes in YY-polarization of several different transits overplotted for each of Cas A, Cyg A, and Tau A. The four cylinders are plotted in different colors to highlight the discrete jumps in amplitude between cylinders. One expects the response of an interferometer to be independent of baseline for a true point source, however the discrete jumps in amplitude between cylinders indicate that these sources are resolved to an extent by the holographic (∼300 m) baselines. There is an additional overall linear trend in the amplitudes as a function of feed along the cylinders.
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: Map of the sky at 612.5 MHz in the region around Tau A before point-source subtraction (top), after subtracting a simple model for Tau A given by Equation (15) (middle), and after subtracting a model for Tau A based on the holography measurements and given by Equation (16) (bottom). The map was constructed from the XX-polarization CHIME visibilities acquired on 2019 October 24. The color scale spans [−0.5%, 1.0%] of the spectral flux density of Tau A.
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 (amplitude of the) aperture illumination inferred from holography of Cyg A, as a function of x (in meters relative to the focal line at x = 0 m) and feed, for both copolarizations and at 717 MHz. The black dashed lines indicate the extent of the focal-line ground plane, and the solid black lines indicate the physical edges of the cylinders. The pattern is consistent between different feeds; the medians over cylinders are shown in the panels above each image. In YY-polarization especially there is an apparent coupling between neighboring cylinders given the absence of power beyond −10(+10) m for Cylinder A (D), where there is no other neighboring cylinder.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: Left: nitrogen abundances for Godzilla, the LyC cluster of Sunburst (M. Pascale et al. 2023), GN-z11 (P. Senchyna et al. 2024), the z ∼ 8 galaxy CEERS-1019 (R. Marques-Chaves et al. 2024), stars of local globular clusters (NGC 6752; E. Carretta et al. 2005), local star-forming galaxies (CLASSY; D. A. Berg et al. 2022; M. G. Stephenson et al. 2023), and local H II regions in SDSS galaxies (L. S. Pilyugin et al. 2012). Middle: neon abundance of Godzilla compared to local star-forming galaxies from CLASSY and D. A. Berg et al. (2019), star-forming regions of M33 from CHAOS (N. S. J. Rogers et al. 2022), the z ∼ 7 galaxies of K. Z. Arellano-Córdova et al. (2022), and the solar value ﹩\mathrm{log}(\mathrm{Ne}/{\rm{O}})=0.63\pm 0.05﹩ (M. Asplund et al. 2021). Right: carbon abundance of Godzilla compared to local star-forming galaxies (Á. López-Sánchez et al. 2007; D. A. Berg et al. 2016, 2019; P. Senchyna et al. 2017), galactic H II regions (K. Z. Arellano-Córdova et al. 2020), a sample of z ∼ 2 galaxies from the literature (M. Pettini et al. 2000; R. A. E. Fosbury et al. 2003; D. K. Erb et al. 2010; L. Christensen et al. 2012; M. B. Bayliss et al. 2014; B. L. James et al. 2014; D. P. Stark et al. 2014; C. C. Steidel et al. 2016; E. Vanzella et al. 2016; R. Amorín et al. 2017; D. A. Berg et al. 2018; J. R. Rigby et al. 2018) and the empirical relation derived by D. C. Nicholls et al. (2017). Figures are recreated following P. Senchyna et al. (2024), D. A. Berg et al. (2019), and K. Z. Arellano-Córdova et al. (2022), and error bars are omitted for visual clarity.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: Evolution of the abundances of accumulated wind and CCSN ejecta. Model predictions from MT12 (black solid lines) are compared to abundances inferred for Godzilla with the chemically anomalous model (red dashed lines and red swaths represent the median and 68% confidence interval, respectively). The relative contributions of winds and SNe to the total ejecta are plotted in purple and green, respectively. We note that these represent the contribution to the abundance of the cumulative ejecta and not the abundances of the winds or SNe themselves. We find that the cluster age of ∼4–6 Myr (blue box) inferred from the chemically anomalous model is in good agreement with the MT12 predictions, such that Godzilla’s nebula may be an order-unity condensation of wind and CCSN ejecta.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: Posterior distributions for the physical parameters describing the nebula for the chemically anomalous model (black) and the base model (purple). Contours levels and histogram confidence intervals follow Figure 7. The 68% confidence intervals of the parameters are tabulated in Table 4.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: MUSE IFU spectrum in the rest-frame wavelength range 1410–2670 Å (observed flux density ﹩{F}_{{\lambda }_{\mathrm{obs}}}﹩ in units of 10−17 erg s−1 cm−2 Å−1). We compare specific fluxes extracted from three circular apertures of radius 0.″5, centered on Godzilla (red), the LyC star cluster (E. Vanzella et al. 2020a; blue), and another unremarkable region on the Sunburst Arc (black). We mark narrow nebular emission lines (black dotted), ISM absorption lines (yellow dotted), and additional unusual emission lines related to H Lyman pumping (magenta dotted).
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: Example of surface brightness modeling of Godzilla and the host arc in F814W. Godzilla is modeled as a Sérsic profile convolved with the PSF, and its neighboring knots are modeled as simple PSFs. The underlying arc background is approximated as a line convolved with a 2D Gaussian, for which the line slope and intercept, as well as the Gaussian width, are free parameters. We find that, even in the highest-resolution filters, the best-fit Sérsic for Godzilla has an effective radius r eff < 1 pixel, consistent with an unresolved FUV source. For a fiducial tangential magnification value μ  t  = 500, this implies a physical size for the OB star component R FUV < 1 pc given the measured F814W PSF FWHM of 0.″13.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: Best-fit SED (gray) from Cloudy modeling with the chemically anomalous model (Section 4.2). Coplotted is the 68% confidence interval range of the model-predicted filter magnitude (open boxes) and the observed magnitude (circles with error bars). Two of the bluest filters, F390W and F410M (open circles and green boxes), are excluded from the fit since the fluxes might have been significantly affected by Lyα line transfer and damping wing effects. The narrowband F164N filter, significantly enhanced by Hβ, is not used due to potential flux calibration issues; however, its measured flux is consistent with the model prediction.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: Posterior distributions for the star cluster parameters in the chemically anomalous model (black) and the base model (purple). 1D histograms representing the posterior distributions are marked with the mean and 68% confidence intervals for the chemically anomalous model (dashed lines). 2D contours enclose 50% and 90% of the posterior samples. Refer to Table 4 for the 68% confidence intervals of the parameters.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: 68% confidence interval for model-predicted line fluxes (blue boxes) in the chemically anomalous model (Section 4.2) and observed line fluxes from the MUSE and X-Shooter data (circles with error bars). For nondetections, upper limits are plotted as downward arrows, which are implemented in fitting as strict upper limits.
Paper: A Young Super Star Cluster Powering a Nebula of Retained Massive Star Ejecta
Authors: Massimo Pascale, Liang Dai
Figure caption: Posterior distributions for the gas-phase abundances of C, N, Ne, and Si relative to O for the chemically anomalous model (black) and the base model (purple). The 68% confidence intervals of the parameters are tabulated in Table 4.
Paper: The SPT-Chandra BCG Spectroscopic Survey. I. Evolution of the Entropy Threshold for ICM Cooling and AGN Feedback in Galaxy Clusters over the Last 10 Gyr
Authors: Michael S. Calzadilla, Michael McDonald, Bradford A. Benson, Lindsey E. Bleem, Judith H. Croston, Megan Donahue, Alastair C. Edge, Benjamin Floyd, Gordon P. Garmire, Julie Hlavacek-Larrondo, Minh T. Huynh, Gourav Khullar, Ralph P. Kraft, Brian R. McNamara, Allison G. Noble, Charles E. Romero, Florian Ruppin, Taweewat Somboonpanyakul, G. Mark Voit
Figure caption: Same as in Figure 8, but separated into redshift bins and compared to ACCEPT clusters with M 500 ≳ 2 × 1014 M ⊙ as before in Figure 6. Error bars are omitted for clarity. Just as before, there is no apparent correlation between a central entropy threshold and radio AGN activity. In the low-z ACCEPT clusters, the demarcation between radio detection and nondetection is clear at K 10 kpc = 60 keV cm2 in the lowest redshift bin. A higher proportion of radio detections is above the threshold in the 0.15 < z < 0.295 redshift bin, but it is clear that the entropy distribution is still bimodal. In our SZ-based sample, the correlation vanishes abruptly. One possible source of bias is contamination of the SZ signal by the radio source, potentially making our sample deficient in high-power radio sources. In the three right panels, a horizontal dashed line shows the level at which radio emission from a 4.2 × 1014 M ⊙ cluster at each median redshift (shown in the upper left of each panel) would suppress 100% of the SZ signal. The varying strength of this effect is explored in more detail in Section 4.2 and Figure 10.
Paper: The SPT-Chandra BCG Spectroscopic Survey. I. Evolution of the Entropy Threshold for ICM Cooling and AGN Feedback in Galaxy Clusters over the Last 10 Gyr
Authors: Michael S. Calzadilla, Michael McDonald, Bradford A. Benson, Lindsey E. Bleem, Judith H. Croston, Megan Donahue, Alastair C. Edge, Benjamin Floyd, Gordon P. Garmire, Julie Hlavacek-Larrondo, Minh T. Huynh, Gourav Khullar, Ralph P. Kraft, Brian R. McNamara, Allison G. Noble, Charles E. Romero, Florian Ruppin, Taweewat Somboonpanyakul, G. Mark Voit
Figure caption: Central entropy (K 10 kpc) vs. Hα or [O II] emission line luminosity (indicators of star formation). For low-z clusters from the ACCEPT sample (left two panels), we show Hα luminosities that are more readily available at low-z, while for high-z clusters from this work (next three panels) we show [O II] luminosities which are available for our higher-z sample. Uncertainties are omitted for clarity. The two samples are split into various redshift bins to look for evolutionary trends in the central entropy threshold originally observed at low-z (vertical dashed line). The median redshift in each bin is noted in the top left of each panel. We see that the entropy threshold of K 10 kpc ≈ 60 keV cm2 (vertical dashed line) persists out to our highest redshift bin. At the bottom left, we compute the binomial probability that all of the detections lie below the median entropy among both detections and nondetections (purple vertical dotted line).
Paper: The SPT-Chandra BCG Spectroscopic Survey. I. Evolution of the Entropy Threshold for ICM Cooling and AGN Feedback in Galaxy Clusters over the Last 10 Gyr
Authors: Michael S. Calzadilla, Michael McDonald, Bradford A. Benson, Lindsey E. Bleem, Judith H. Croston, Megan Donahue, Alastair C. Edge, Benjamin Floyd, Gordon P. Garmire, Julie Hlavacek-Larrondo, Minh T. Huynh, Gourav Khullar, Ralph P. Kraft, Brian R. McNamara, Allison G. Noble, Charles E. Romero, Florian Ruppin, Taweewat Somboonpanyakul, G. Mark Voit
Figure caption: Central entropy of the ICM measured at a radius of 10 kpc (K 10 kpc) vs. 1.4 GHz rest luminosity of the central radio source (ν L  ν ) whenever one was associated with the BCG (i.e., a detection, in blue) or of the radio map rms noise (i.e., upper limits, shown in red). In contrast to low-z systems, or like the case for star formation (Figure 5), in our sample, we do not see a correlation between a cluster’s central entropy and AGN activity. This could be due to an actual evolution in the entropy threshold, due to a less tight feedback-cooling cycle or higher mergers at high-z competing with CFs to drive more gas toward the AGN, for instance, or an artificial evolution due to some biases we discuss in Section 4.2.
Paper: The SPT-Chandra BCG Spectroscopic Survey. I. Evolution of the Entropy Threshold for ICM Cooling and AGN Feedback in Galaxy Clusters over the Last 10 Gyr
Authors: Michael S. Calzadilla, Michael McDonald, Bradford A. Benson, Lindsey E. Bleem, Judith H. Croston, Megan Donahue, Alastair C. Edge, Benjamin Floyd, Gordon P. Garmire, Julie Hlavacek-Larrondo, Minh T. Huynh, Gourav Khullar, Ralph P. Kraft, Brian R. McNamara, Allison G. Noble, Charles E. Romero, Florian Ruppin, Taweewat Somboonpanyakul, G. Mark Voit
Figure caption: 1.4 GHz radio luminosity vs. redshift. Lines of constant flux are overlaid, depicting the amount of bias (δ ζ/ζ) by which the radio flux suppresses the SZ signal by 1%, 10%, and 100% (H. W. Lin et al. 2015). We see that our sample contains no clusters for which the SZ signal in a M 500 = 4.2 × 1014 M ⊙ cluster would be biased by >30%, which could be indicating a significant source of selection bias for SZ-based surveys.
Paper: The SPT-Chandra BCG Spectroscopic Survey. I. Evolution of the Entropy Threshold for ICM Cooling and AGN Feedback in Galaxy Clusters over the Last 10 Gyr
Authors: Michael S. Calzadilla, Michael McDonald, Bradford A. Benson, Lindsey E. Bleem, Judith H. Croston, Megan Donahue, Alastair C. Edge, Benjamin Floyd, Gordon P. Garmire, Julie Hlavacek-Larrondo, Minh T. Huynh, Gourav Khullar, Ralph P. Kraft, Brian R. McNamara, Allison G. Noble, Charles E. Romero, Florian Ruppin, Taweewat Somboonpanyakul, G. Mark Voit
Figure caption: Bootstrapped threshold values of entropy that separate detections of Hα (first two bins) or [O II] (next three bins) from nondetections in each redshift bin. For each bootstrap iteration, we use a support vector classifier to find the threshold value that maximizes the margin between the two classes. We see that, while there is a slight increase in the measured threshold value with redshift, there is no strong statistical evidence for evolution.
Paper: Luminosity Function of Collapsar Gamma-Ray Bursts: The Progenitor of Long Gamma-Ray Bursts Is Not Singular
Authors: Yan-Kun Qu, 艳坤 屈, Zhong-Xiao Man, Shuang-Xi Yi, 双喜 仪, Yu-Peng Yang, 玉鹏 杨
Figure caption: The redshift distribution. Three curves representing the redshift distributions of collapsar GRBs calculated by three different models. The shaded areas indicate the 1σ confidence intervals. The green data points represent the observed redshift distribution of 301 long GRBs with P ≥ 1 photons cm−2 s−1.
Paper: Luminosity Function of Collapsar Gamma-Ray Bursts: The Progenitor of Long Gamma-Ray Bursts Is Not Singular
Authors: Yan-Kun Qu, 艳坤 屈, Zhong-Xiao Man, Shuang-Xi Yi, 双喜 仪, Yu-Peng Yang, 玉鹏 杨
Figure caption: The L iso distribution of GRBs, where gray represents all 423 Swift long GRBs, purple represents 206 bursts with z ≥ 2, and yellow represents bursts with z ≥ 2 and 1 s peak flux P ≥ 1 photons cm−2 s−1, totaling 134 bursts.
Paper: Luminosity Function of Collapsar Gamma-Ray Bursts: The Progenitor of Long Gamma-Ray Bursts Is Not Singular
Authors: Yan-Kun Qu, 艳坤 屈, Zhong-Xiao Man, Shuang-Xi Yi, 双喜 仪, Yu-Peng Yang, 玉鹏 杨
Figure caption: The distribution of redshifts for all 423 Swift long GRBs, with the red dashed line representing the location of z = 2, and there are a total of 206 samples with z ≥ 2.