adsabs/AstroCLIMB huggingface dataset:
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Top: east–west polarized power spectra for pure observations over the five pointings present in the data. The array points more westerly toward the right of the figure. The number of observations in each integration is annotated at the bottom of the figure. The depth of integration ranges by about a factor of 2.5. All of these power spectra appear noise dominated in the EoR window (region above the solid black line) in that there is a roughly even speckling of positive and negative data. Bottom: corresponding absolved power spectra, where any RFI type is included so long as the observation has RFI z-scores that lie between 10 and 100. We see a signal-like component in the EoR window. Rather than an even speckling of positive and negative data, we see consistent, smoothly varying positive power up to and occasionally past the first coarse band harmonic. This suggests residual RFI that was uncaught by SSINS. This contamination is generally worse in the later pointings that point more west. There is no clear correlation between integration depth and contamination levels.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Top, middle: cumulative density functions for the absolute value of the inverse-noise weighted spherical power neglecting the foreground wedge and coarse band harmonics. The top row, which shows measurements from absolved observations, appears ordered by pointing from east to west for most of the domain. The pure observations are not as clearly ordered or distinct from one another. Neither data set looks consistent with pure noise, however. Bottom: cumulative density function for the difference between corresponding inverse-noise weighted spherical power of the top two rows (absolved minus pure). The preference of the distributions to lie toward the right of the dotted curve, which reflects a null hypothesis, shows that absolved observations generally produce power spectra that are more positively outlying than their pure counterparts.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Histograms of SSINS amplitudes and z-scores for the entire season, separated by flagged and unflagged data. These z-scores are calculated per fine 40 kHz channel using the time average of 112 s of data as a reference. The horizontal axis is a hybrid linear-logarithmic scale, where the boundary between scales is demarcated by the black vertical lines. The z-scores of the unflagged samples (bottom orange) are highly Gaussian, as expected from the assumptions about the thermal noise. The flagged samples have a highly non-Gaussian z-score distribution. Their brightness distribution has significant overlap with the unflagged brightness distribution, and cannot be separated solely by drawing an amplitude cut.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Top: histogram of flag interarrival times over all nights for the broadcast SSINS flags. The “Poisson Mixture Comparison” (green) is a hyperexponential distribution where each component has consistent mean interarrival time as each night of data (and is weighted according to the amount of data in the corresponding night). The Markov chain histogram is built from Markov chain realizations of each night with consistent transition probabilities as the night of RFI flags they are built from. Interarrival times from the Markov chain realizations are roughly consistent with those from the RFI flag time series, whereas the Poisson mixture model tends to underpredict short and long interarrival times, thereby failing to predict clumps of flags. Bottom: cumulative density for what is shown in the top plot. The data and Markov chain cumulative densities are inconsistent with a Poisson model.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Total occupancy scatter plot after extending flags across frequency, which roughly doubles the total occupancy in the data set. Each marker represents a 2 minute observation, where its horizontal position is its starting sidereal time and its vertical position is its beginning civil time. Clusters of flags are apparent.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Same as Figure 8, but with brightnesses and z-scores calculated by doing the SSINS sub-band sum that is employed in the match filter over the TV7 frequencies. Interestingly, the unflagged and flagged brightness samples appear bimodal. Examination of this plot on a per-pointing basis shows that the mode above 40 Jy belongs to the eastern-most pointing in the data, while the other mode is a combination of all other pointings.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Autocorrelation of RFI flag time series for a particular night (blue) along with the autocorrelation function for a Markov chain realization (transparent orange). Bottom panel: residual of the top panel. The Markov chain realization is clearly missing the peaks at lags between 0 and 50 minutes, meaning that the Markov model does not fully capture the time-like properties of the RFI events, and so a more detailed model is required in future efforts.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Left: raw SSINS of a 112 s observation at various stages of flagging. Right: mean-subtracted SSINS. Top: data with initial flagging mask. Middle: additional flagging mask after match filtering. Bottom: flags after frequency extension.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Histogram of DTV occupancies per observation, before the ionospheric cut. Since observations with more than 60% occupancy are entirely flagged, there is a cutoff in the histogram at 0.6 and a buildup at 1. Only a small fraction of the allocation for TV9 is in the observing band, so the SSINS match filter is less sensitive to it. Data about TV broadcasting stations also suggests this allocation may be used less often.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Flowchart of most salient steps in the analysis of this data set. The top row of nodes shows the major analysis steps. Analysis stages are color coded as follows. Blue: Data Acquisition; Cyan: Pre-processing; Yellow: RFI Analysis; and Green: Calibration, Imaging, and Power Spectrum Estimation. The lower flowchart shows each major analysis step in more detail and how the outputs of each step feed into subsequent steps.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Scatter plot of observations included in the analysis in only the central five pointings (left), and after an ionospheric quality cut (right). Vertical axis shows the date of the observations (blue dots), and horizontal axis is the Local Sidereal Time.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Similar power spectrum jackknife test as Figure 10, except this time comparing only the +2 (most westerly) pointing for RFI of any type in the annotated z-score bins at the top of the figure. This comparison demonstrates two features that were common among our 2D power spectrum jackknife tests. First, excess power is more noticeable for observations in which the identified contaminants had relatively low SSINS z-scores. Since the number of contributing observations ranges from 1–32, there is significant variation in the noise levels of each integration, which makes the significance of excess power from residual RFI harder to discern from this Figure alone. Figure 13 makes this claim more evident. Second, the +2 pointing appears to be the most obviously contaminated pointing, and contamination can sometimes even be seen in the pure observations. For example, the corresponding pure integration for the power spectra whose SSINS z-scores fall between 10 and 100 as well as the one for z-scores between 3 and 5 appear to have moderate excess window contamination, though less than their absolved counterparts.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Cumulative distribution functions in the same style as Figure 11, but this time collated by the z-score of the events found by SSINS. In this case, the absolved observations appear to fall into two classes. The observations with extremely bright events do not appear to produce significantly outlying power spectra, whereas observations with only faint or moderately bright RFI appear to produce more strongly outlying power spectra. The pure power spectra also seem divided in this way, although the distinction is less obvious. Since observations with lower SSINS z-scores are more plentiful, this trend that is present in both the top and middle panels may indicate a systematic that integrates somewhat coherently over the timescales used in these jackknife tests. We again see that absolved power spectra are more often positively outlying than pure ones.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Deep 2D power spectra from three different sets of data, all of which were deemed uncontaminated by SSINS. As with all other 2D power spectra shown in this work, we show the “dirty” power spectrum, i.e., without model subtraction. The wall of shame set shows a clear RFI footprint in the spectrum made from the east–west dipoles, but appears noise-limited in the one from the north–south dipoles. On the other hand, the limit set power spectra appear similarly, regardless of which polarization is used. Specifically both the east–west and north–south power spectra appear systematically dominated below the first coarse band harmonic in the limit set, in contrast to the wall of shame set and the majority of shorter power spectrum integrations we inspected. A key difference between this contamination and the RFI footprint is that it does not extend to large k ⊥. The coherent average of the two performs to expectation in that adding the wall of shame set does not strongly affect the appearance of the power spectrum from the north–south data, and imprints the characteristic RFI footprint in the spectrum made from the east–west data.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: A power spectrum test in which two separate power spectra were made for the same observations, once with flags applied and once without flags applied. In the difference plot, blue bins indicate power is higher without flags. We find that applying the SSINS flags removes power from the window in the exact shape as seen in other absolved power spectra. Additionally, power is removed in the region of the wedge corresponding to the sidelobes, which is where we observe DTV sources in our images. The clean LST-matched observations are shown on the far left as a reference.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: A power spectrum jackknife test for zenith-pointed observations, where spectra are separated by RFI type. These all have RFI events with z-scores between 10 and 100. We find that the region of contamination seems unrelated to the type of RFI. This may be due to multiple RFI types cohabiting these observations.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Spherical power spectra for the limit set, along with 2σ upper limits, a fiducial theory model for the EoR signal whose implementation is described in Barry et al. (2019b). In short, the astrophysical constraints from Park et al. (2019) are used in combination with 21CMMC (Greig & Mesinger 2015) to generate samples from a probability distribution of 21 cm power spectra. The fiducial model and theoretical confidence interval are then calculated from these samples (brown solid and dashed lines, respectively). We notice that the range of wave modes between the coarse band harmonics are almost all noise dominated. This could be a direct consequence of the rigorous RFI cuts we have employed. Compare to limits at the same redshifts in Li et al. (2019).
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: Power spectrum jackknife test for observations classified as containing broadband interference. Excess window power takes a similar shape as RFI events in Figure 14.
Paper: Evidence of Ultrafaint Radio Frequency Interference in Deep 21 cm Epoch of Reionization Power Spectra with the Murchison Wide-field Array
Authors: Michael J. Wilensky, Miguel F. Morales, Bryna J. Hazelton, Pyxie L. Star, Nichole Barry, Ruby Byrne, C. H. Jordan, Daniel C. Jacobs, Jonathan C. Pober, C. M. Trott
Figure caption: All subintegrations that were determined to possess clear indications of ultrafaint RFI contamination in the EoR window (but found to be unoccupied by SSINS) that were subsequently removed from the limit integration.
Paper: Interaction of Inner Heliosheath Ions with Electromagnetic Ion Cyclotron Waves
Authors: Dae-Young Lee, Sung-Jun Noh
Figure caption: Diffusive and advective changes in the pitch angle ((Δα)dif, (Δα)adv in (a) and (b), respectively) and in the kinetic energy ((Δ KE)dif/KE o , (Δ KE)adv/KE o ) in (c) and (d), respectively) for protons shown in the space defined by the initial pitch angle α  o  versus the initial kinetic energy KE o . Note that the pitch-angle changes are in degrees, and the kinetic energy changes are normalized to the corresponding initial kinetic energy. The ellipsoidal contours refer to the main scattering domains to help visual identification.
Paper: Interaction of Inner Heliosheath Ions with Electromagnetic Ion Cyclotron Waves
Authors: Dae-Young Lee, Sung-Jun Noh
Figure caption: Diffusive (upper panels) and advective (lower panels) changes for He+ shown in the same format as Figure 5 but with a different EMIC wave model covering a larger wavenumber regime (Figure 9). Note that the larger ranges of color scales are used for the energy changes in (c) and (d) than those used for protons and He2+ in Figures 10 and 11.
Paper: Interaction of Inner Heliosheath Ions with Electromagnetic Ion Cyclotron Waves
Authors: Dae-Young Lee, Sung-Jun Noh
Figure caption: Diffusive (upper panels) and advective (lower panels) changes for protons shown in the same format as in Figure 5 but with a different EMIC wave model covering a larger wavenumber regime (as shown in Figure 9).
Paper: Interaction of Inner Heliosheath Ions with Electromagnetic Ion Cyclotron Waves
Authors: Dae-Young Lee, Sung-Jun Noh
Figure caption: Schematic demonstration of two cases where the velocity vector v of ions along the line of sight (LOS) toward an ENA observing spacecraft makes different angles with the background magnetic field B  o  at the time when the ions are supposed to charge exchange with neutral atoms. In one case (LOS0), the angle is 90°, and in the other case (LOS1), it is > 90°. The waves (magenta) are superposed, which may scatter ions (see text in Section 3.3 for details).
Paper: Interaction of Inner Heliosheath Ions with Electromagnetic Ion Cyclotron Waves
Authors: Dae-Young Lee, Sung-Jun Noh
Figure caption: Diffusive (upper panels) and advective (lower panels) changes in the pitch angle (left) and energy (right) for He2+ shown in the same format as Figure 5.
Paper: Interaction of Inner Heliosheath Ions with Electromagnetic Ion Cyclotron Waves
Authors: Dae-Young Lee, Sung-Jun Noh
Figure caption: Diffusive (upper panels) and advective (lower panels) changes in the pitch angle (left) and energy (right) for He+ shown in the same format as Figure 5.
Paper: Interaction of Inner Heliosheath Ions with Electromagnetic Ion Cyclotron Waves
Authors: Dae-Young Lee, Sung-Jun Noh
Figure caption: Diffusive (upper panels) and advective (lower panels) changes for He2+ shown in the same format as Figure 5 but with a different EMIC wave model covering a larger wavenumber regime (Figure 9).
Paper: Interaction of Inner Heliosheath Ions with Electromagnetic Ion Cyclotron Waves
Authors: Dae-Young Lee, Sung-Jun Noh
Figure caption: Unstable EMIC wave solution in a larger wavenumber domain and the corresponding minimum resonant energies for interaction with protons and He2+.
Paper: Interaction of Inner Heliosheath Ions with Electromagnetic Ion Cyclotron Waves
Authors: Dae-Young Lee, Sung-Jun Noh
Figure caption: Example of the particle positions in velocity space for a proton launched with (KEo = 5 keV, α o = 135°). The start point is marked by the solid blue circle, the particle positions at numerous selected times are in open black circles, the constant kinetic energy contour is in green, and the single wave characteristics curve is in red. ﹩{V}_{| | \mathrm{Res}}﹩ is the parallel velocity of resonant kinetic energy.
Paper: An Optically Discovered Outburst from XTE J1859+226
Authors: Eric C. Bellm, Yuankun Wang, Jan van Roestel, Rebecca A. Phillipson, Michael W. Coughlin, John A. Tomsick, Steven L. Groom, Brian Healy, Josiah Purdum, Ben Rusholme, Jesper Sollerman, Peter Bealo, Stefano Lora, Eddy Muyllaert, Ivo Peretto, Erik J. Schwendeman
Figure caption: Time evolution of absorbed power-law parameters from spectral fits to Swift (blue) and joint Swift–NuSTAR (orange) data. Top panel: 0.3–10 keV energy flux in erg cm−2 s−1. The best-fit exponential (green), linear (orange), and limited-range linear (gray dashed) models are overplotted. Bottom panel: best-fit spectral index Γ, where F(E) ∝ E −Γ.
Paper: An Optically Discovered Outburst from XTE J1859+226
Authors: Eric C. Bellm, Yuankun Wang, Jan van Roestel, Rebecca A. Phillipson, Michael W. Coughlin, John A. Tomsick, Steven L. Groom, Brian Healy, Josiah Purdum, Ben Rusholme, Jesper Sollerman, Peter Bealo, Stefano Lora, Eddy Muyllaert, Ivo Peretto, Erik J. Schwendeman
Figure caption: Optical spectra (gray: SEDM; blue: LRIS) of XTE J1859+226 in outburst. The full LRIS spectrum is convolved with an 8 pixel boxcar filter for plot clarity. Inset: double Gaussian fit (orange) to the LRIS Hα emission line. The gap in the data corresponds to the pixels excluded due to contamination by a cosmic ray.
Paper: VERTICO. VII. Environmental Quenching Caused by the Suppression of Molecular Gas Content and Star Formation Efficiency in Virgo Cluster Galaxies
Authors: Toby Brown, Ian D. Roberts, Mallory Thorp, Sara L. Ellison, Nikki Zabel, Christine D. Wilson, Yannick M. Bahé, Dhruv Bisaria, Alberto D. Bolatto, Alessandro Boselli, Aeree Chung, Luca Cortese, Barbara Catinella, Timothy A. Davis, María J. Jiménez-Donaire, Claudia D. P. Lagos, Bumhyun Lee, Laura C. Parker, Rory Smith, Kristine Spekkens, Adam R. H. Stevens, Vicente Villanueva, Adam B. Watts
Figure caption: The distribution of ΔΣSFR, Δf mol, and ΔSFE pixel values for galaxies in different evolutionary stages. Field galaxies are drawn from the HERACLES sample, while H I–identified RPS stages and anemic disks are taken from Yoon et al. (2017). Pixel distributions are divided into the inner and outer disk (r < r 90,mol and r ≥ r 90,mol, respectively). We annotate the number and percentages of pixels in the inner and outer disks for each stage in the corresponding color. The gray horizontal bar simply illustrates the distinction between our field and cluster samples. We see the systematic decrease in ΔΣSFR, Δf mol, and ΔSFE during the stripping sequence and also in anemic disks with respect to the field. The reduction in gas content and SFE, and consequently star formation activity, happens preferentially in the outer disks for galaxies undergoing RPS.