adsabs/AstroCLIMB huggingface dataset:
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: Different methods to obtain the orientation angle. (a) Comparison of the fit results from three fitting methods. Red dots are the hypothetical data. The black line is the fit line with OLS to the data, and the blue line is also the fit line with OLS, but x and y are inverted. The green line is the fit line with PCA. (b) OLS fitting with vertical offsets. (c) x and y inverted OLS fitting with horizontal offsets. (d) PCA fitting with perpendicular offsets.
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: Convex hull, concave hull, and aspect ratio. In panel (a), red dots and gray segments show one of our filaments F7. The black polygon enclosing it is the convex hull, and the blue polygon is the concave hull. Panel (b) illustrates how we derive the aspect ratio. The aspect ratio of a filament is the ratio of the area between the circle enclosing the vertices and the concave hull.
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: Differences of filaments in arms or outside them. (a) Galactic longitude. (b) Galactic latitude. (c) Distance from the Sun. (d) Height above the Galactic midplane. (e) Mean radial velocity of each filament. (f) Nonthermal velocity dispersion of the clumps in each filament. (g) Mean velocity gradient of the edges in each filament. (h) Mean temperature. (i) Mean separation of the clumps in each filament. (j) Line mass. (k) Volume density. (l) Angle between the major axes and the Galactic midplane in the projected sky. (m) Linearity. (n) Galactocentric radius. (o) Linearity-weighted length. (p) Column density. (q) Mass.
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: Two-color view of filaments. The color-coded circles denote clumps in filaments with various velocities. For backgrounds, cyan represents intermediate-infrared 24 μm emission on a logarithmic scale from MIPSGAL (Carey et al. 2009), and red shows submillimeter 870 μm emission on a linear scale from an APEX + Planck combined image (Csengeri et al. 2016). 1 of 12 images
Paper: A Census of 163 Large-scale (≥10 pc), Velocity-coherent Filaments in the Inner Galactic Plane: Physical Properties, Dense-gas Fraction, and Association with Spiral Arms
Authors: Yifei Ge, and Ke Wang
Figure caption: Filaments overlaid on column-density maps from PPMAP (Marsh et al. 2017).  1 of 8 images
Paper: The Second Catalog of Interplanetary Network Localizations of Konus Short-duration Gamma-Ray Bursts
Authors: D. S. Svinkin, K. Hurley, A. V. Ridnaia, A. L. Lysenko, D. D. Frederiks, S. V. Golenetskii, A. E. Tsvetkova, M. V. Ulanov, A. Kokomov, T. L. Cline, I. Mitrofanov, D. Golovin, A. Kozyrev, M. Litvak, A. Sanin, A. Goldstein, M. S. Briggs, C. Wilson-Hodge, E. Burns, A. von Kienlin, X.-L. Zhang, A. Rau, V. Savchenko, E. Bozzo, C. Ferrigno, S. Barthelmy, J. Cummings, H. Krimm, D. M. Palmer, A. Tohuvavohu, K. Yamaoka, M. Ohno, Y. Fukazawa, Y. Hanabata, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, K. Makishima, W. Boynton, C. W. Fellows, K. P. Harshman, H. Enos, R. Starr, J. Goldsten, R. Gold, A. Ursi, M. Tavani, A. Bulgarelli, C. Casentini, E. Del Monte, Y. Evangelista, M. Galli, F. Longo, M. Marisaldi, N. Parmiggiani, C. Pittori, M. Romani, F. Verrecchia, D. M. Smith, W. Hajdas, S. Xiao, C. Cai, Q. B. Yi, Y. Q. Zhang, S. L. Xiong, X. B. Li, Y. Huang, C. K. Li, S. N. Zhang, L. M. Song, C. Z. Liu, X. Q. Li, W. X. Peng, and I. Martinez-Castellanos
Figure caption: Distributions of uncertainties in time delay d(δT) = (d+(δT) + ∣d−(δT)∣)/2 (left) and 3σ half widths (HWs, right) of the 438 triangulation annuli. Blue dotted lines: 115 annuli involving at least one distant s/c; red dashed lines: 323 annuli not involving any distant s/c. For annuli obtained using the KW and near-Earth (or INTEGRAL) s/c data, the smallest d(δT) is 1.2 ms, the largest is 600 ms, the mean is 29 ms, and the geometric mean is 16 ms; the smallest HW is 0.°021 (1.′3), the largest is 36.°7, the mean is 1.°6, and the geometric mean is 0.°45. For annuli involving distant s/c, the smallest d(δT) is 361 ms, the largest is 1168 ms, the mean is 596 ms, and the geometric mean is 544 ms; the smallest HW is 0.°016 (0.′9), the largest is 2.°1, the mean is 1.°12, and the geometric mean is 0.°72.
Paper: The Second Catalog of Interplanetary Network Localizations of Konus Short-duration Gamma-Ray Bursts
Authors: D. S. Svinkin, K. Hurley, A. V. Ridnaia, A. L. Lysenko, D. D. Frederiks, S. V. Golenetskii, A. E. Tsvetkova, M. V. Ulanov, A. Kokomov, T. L. Cline, I. Mitrofanov, D. Golovin, A. Kozyrev, M. Litvak, A. Sanin, A. Goldstein, M. S. Briggs, C. Wilson-Hodge, E. Burns, A. von Kienlin, X.-L. Zhang, A. Rau, V. Savchenko, E. Bozzo, C. Ferrigno, S. Barthelmy, J. Cummings, H. Krimm, D. M. Palmer, A. Tohuvavohu, K. Yamaoka, M. Ohno, Y. Fukazawa, Y. Hanabata, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, K. Makishima, W. Boynton, C. W. Fellows, K. P. Harshman, H. Enos, R. Starr, J. Goldsten, R. Gold, A. Ursi, M. Tavani, A. Bulgarelli, C. Casentini, E. Del Monte, Y. Evangelista, M. Galli, F. Longo, M. Marisaldi, N. Parmiggiani, C. Pittori, M. Romani, F. Verrecchia, D. M. Smith, W. Hajdas, S. Xiao, C. Cai, Q. B. Yi, Y. Q. Zhang, S. L. Xiong, X. B. Li, Y. Huang, C. K. Li, S. N. Zhang, L. M. Song, C. Z. Liu, X. Q. Li, W. X. Peng, and I. Martinez-Castellanos
Figure caption: Distributions of relative offsets (in σ) of the 27 precise GRB positions from the center lines of the IPN annuli. Red dashed line: 43 KW–near-Earth s/c (including 20 KW–INTEGRAL) annuli; blue dotted line: 16 KW (or Fermi)–distant s/c annuli.
Paper: The Second Catalog of Interplanetary Network Localizations of Konus Short-duration Gamma-Ray Bursts
Authors: D. S. Svinkin, K. Hurley, A. V. Ridnaia, A. L. Lysenko, D. D. Frederiks, S. V. Golenetskii, A. E. Tsvetkova, M. V. Ulanov, A. Kokomov, T. L. Cline, I. Mitrofanov, D. Golovin, A. Kozyrev, M. Litvak, A. Sanin, A. Goldstein, M. S. Briggs, C. Wilson-Hodge, E. Burns, A. von Kienlin, X.-L. Zhang, A. Rau, V. Savchenko, E. Bozzo, C. Ferrigno, S. Barthelmy, J. Cummings, H. Krimm, D. M. Palmer, A. Tohuvavohu, K. Yamaoka, M. Ohno, Y. Fukazawa, Y. Hanabata, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, K. Makishima, W. Boynton, C. W. Fellows, K. P. Harshman, H. Enos, R. Starr, J. Goldsten, R. Gold, A. Ursi, M. Tavani, A. Bulgarelli, C. Casentini, E. Del Monte, Y. Evangelista, M. Galli, F. Longo, M. Marisaldi, N. Parmiggiani, C. Pittori, M. Romani, F. Verrecchia, D. M. Smith, W. Hajdas, S. Xiao, C. Cai, Q. B. Yi, Y. Q. Zhang, S. L. Xiong, X. B. Li, Y. Huang, C. K. Li, S. N. Zhang, L. M. Song, C. Z. Liu, X. Q. Li, W. X. Peng, and I. Martinez-Castellanos
Figure caption: IPN localizations. The three panels present typical cases of IPN localization: GRB detected by four well-separated s/c (top panel); GRB detected by three s/c with an additional constraint used to select the final localization (middle panel); GRB detected by two s/c, the localization is formed by a single annulus and GBM localization (bottom panel). The left plot in each panel shows the whole sky with triangulation annuli and other constraints along with the ecliptic plane (dashed line) and Sun position at the GRB time; the Galactic plane (dashed–dotted line) and the Galactic center. The right plots are magnification insets showing the 3σ localization confidence region (blue solid line). The GRB name and the KW trigger time are given in the figure title.
Paper: The Second Catalog of Interplanetary Network Localizations of Konus Short-duration Gamma-Ray Bursts
Authors: D. S. Svinkin, K. Hurley, A. V. Ridnaia, A. L. Lysenko, D. D. Frederiks, S. V. Golenetskii, A. E. Tsvetkova, M. V. Ulanov, A. Kokomov, T. L. Cline, I. Mitrofanov, D. Golovin, A. Kozyrev, M. Litvak, A. Sanin, A. Goldstein, M. S. Briggs, C. Wilson-Hodge, E. Burns, A. von Kienlin, X.-L. Zhang, A. Rau, V. Savchenko, E. Bozzo, C. Ferrigno, S. Barthelmy, J. Cummings, H. Krimm, D. M. Palmer, A. Tohuvavohu, K. Yamaoka, M. Ohno, Y. Fukazawa, Y. Hanabata, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, K. Makishima, W. Boynton, C. W. Fellows, K. P. Harshman, H. Enos, R. Starr, J. Goldsten, R. Gold, A. Ursi, M. Tavani, A. Bulgarelli, C. Casentini, E. Del Monte, Y. Evangelista, M. Galli, F. Longo, M. Marisaldi, N. Parmiggiani, C. Pittori, M. Romani, F. Verrecchia, D. M. Smith, W. Hajdas, S. Xiao, C. Cai, Q. B. Yi, Y. Q. Zhang, S. L. Xiong, X. B. Li, Y. Huang, C. K. Li, S. N. Zhang, L. M. Song, C. Z. Liu, X. Q. Li, W. X. Peng, and I. Martinez-Castellanos
Figure caption: Distributions of minimum sizes (left) and areas (right) of the IPN localizations. Blue dotted lines: 94 Konus short bursts observed by at least one distant s/c; red dashed lines: 105 bursts not observed by any distant s/c. The minimum region dimensions range from 0.°033 (2.′0) to 3.°32 with a mean of 0.°17, and a geometric mean of 0.°11 (for bursts observed by distant s/c) and from 0.°043 (2.′6) to 36.°5 with a mean of 1.°5, and a geometric mean of 0.°6 (for bursts without distant s/c detections). The areas range from 0.005 deg2 (18 arcmin2) to 14.4 deg2 with a mean of 0.70 deg2, and a geometric mean of 0.12 deg2 (for bursts observed by distant s/c) and from 0.156 deg2 to 3163 deg2 with a mean of 103 deg2, and a geometric mean of 11.0 deg2 (for bursts without distant s/c detections).
Paper: The TESS Faint-star Search: 1617 TOIs from the TESS Primary Mission
Authors: Michelle Kunimoto, Tansu Daylan, Natalia Guerrero, William Fong, Steve Bryson, George R. Ricker, Michael Fausnaugh, Chelsea X. Huang, Lizhou Sha, Avi Shporer, Andrew Vanderburg, Roland K. Vanderspek, and Liang Yu
Figure caption: The vetting page for the 10.4 days planet candidate orbiting TIC-394346647 (now TOI-2620), containing data across Sectors 1, 12, and 13. Top row: raw lightcurve, with odd and even transits marked in blue and orange, respectively. Second row, first panel: detrended lightcurve with the transit model in red. Second row, second panel: odd and even transit phase diagrams. Third row, first panel: full phase diagram. Third row, second panel: phase diagram zoomed into the most significant secondary event from model-shift. Fourth row, first panel: phase diagram close-up to a transit event with the transit model in red. Fourth row, second panel: phase diagram close-up to phase 0.5. Fifth row: phase diagram close-up to a transit event in three different apertures. Second-last column: Full 20 × 20 pixel view of difference and direct images for Sector 13, followed by a close-up of the central 5 × 5 pixels. The target star is marked by a pink star. Nearby stars down to 4 mag fainter are plotted with circles. Last column: fitted and derived parameters from the transit model, BLS, and TIC, and the stellar catalog, with an indication of any matches to known TOIs.
Paper: The TESS Faint-star Search: 1617 TOIs from the TESS Primary Mission
Authors: Michelle Kunimoto, Tansu Daylan, Natalia Guerrero, William Fong, Steve Bryson, George R. Ricker, Michael Fausnaugh, Chelsea X. Huang, Lizhou Sha, Avi Shporer, Andrew Vanderburg, Roland K. Vanderspek, and Liang Yu
Figure caption: A comparison of TOI properties from the TOI catalog, with the faint-star TOIs in orange and other TOIs from the Primary Mission (Guerrero et al. 2021) in blue. Top: TOIs plotted in period–radius space. TOIs larger than 30 R⊕ are not shown as they are highly unlikely to be planetary. Middle: histograms of planet radii. Bottom: histograms of orbital periods. The faint-star TOIs are predominantly giant candidates (Rp > 10 R⊕) and those with short orbital periods (P < 10 days).
Paper: The TESS Faint-star Search: 1617 TOIs from the TESS Primary Mission
Authors: Michelle Kunimoto, Tansu Daylan, Natalia Guerrero, William Fong, Steve Bryson, George R. Ricker, Michael Fausnaugh, Chelsea X. Huang, Lizhou Sha, Avi Shporer, Andrew Vanderburg, Roland K. Vanderspek, and Liang Yu
Figure caption: A comparison of the TESS magnitudes of TOI hosts, with the faint-star TOIs in orange and other TOIs from the Primary Mission in blue. On average, faint-star TOIs orbit stars 2.4 mag fainter than other Primary Mission TOIs.
Paper: Pitfalls of Periodograms: The Nonstationarity Bias in the Analysis of Quasiperiodic Oscillations
Authors: Moritz Hübner, Daniela Huppenkothen, Paul D. Lasky, and Andrew R. Inglis
Figure caption: Effects of extending a time series with zeros. In the top panel, we show a stationary time series between −10 s and 10 s that we multiply with a Hann window to ensure a smooth turn-on from zero. We extended this time series with zeros on either end up to a total duration of 200  s. The upper x-axis shows how the extension factor x maps onto the time axis. Taking only the stationary data from −10 s to 10 s corresponds to x = 1, i.e., no extension has been applied. The extension factor in this case implies that we select data from − 10x s to 10x s. In the bottom panel, we show the periodogram given different extension factors, with the blue curve representing the stationary data (x = 1). The other colors (orange, green, red) show the effect of extending the time series with zeros on either end. In these curves, neighboring bins are not statistically independent, which manifests itself in the emerging smooth structure of the periodogram. The bins are also decreasing inversely proportional to x since we do not apply a normalization.
Paper: Pitfalls of Periodograms: The Nonstationarity Bias in the Analysis of Quasiperiodic Oscillations
Authors: Moritz Hübner, Daniela Huppenkothen, Paul D. Lasky, and Andrew R. Inglis
Figure caption: S/N (blue) and ﹩\mathrm{lnBF}﹩ (orange) vs. the extension factor for a simulated QPO plus white-noise signal that is extended with white noise (top) or zeros (bottom). The solid blue line displays the S/N of the maximum likelihood point, and the shaded blue region displays the S/N’s 90% credible interval. In the top panel both S/N and ﹩\mathrm{lnBF}﹩ decrease with increasing x, which corresponds to the QPO vanishing in noise. In the bottom panel the ﹩\mathrm{lnBF}﹩ increases almost perfectly linearly owing to the increased number of frequency bins that make up the QPO, whereas the S/N increases roughly with the square root.
Paper: Pitfalls of Periodograms: The Nonstationarity Bias in the Analysis of Quasiperiodic Oscillations
Authors: Moritz Hübner, Daniela Huppenkothen, Paul D. Lasky, and Andrew R. Inglis
Figure caption: Simulated data of a nonstationary QPO in a deterministic transient flare shape in the presence of white noise. The time series (top) shows the dominant transient and the QPO that is present for 20 s on the tail of the flare (inset). We remove the deterministic trend of the flare in the inset to make the QPO easily visible. The periodogram (bottom) shows a visible QPO at 1 Hz and displays a low-frequency continuum that arises as a result of the transient flare shape. The periodogram corresponds only to the segment of the light curve that contains the QPO. Note that there is much less variability than we would expect from the ﹩{\chi }_{2}^{2}﹩-distribution for the bins at low frequencies since the noise continuum is due not to a stationary stochastic process but to a deterministic process.
Paper: Pitfalls of Periodograms: The Nonstationarity Bias in the Analysis of Quasiperiodic Oscillations
Authors: Moritz Hübner, Daniela Huppenkothen, Paul D. Lasky, and Andrew R. Inglis
Figure caption: S/N (blue) and ﹩\mathrm{ln}{\rm{BF}}﹩ (orange) vs. the extension factor for the QPO shown in Figure 3. The solid blue line displays the S/N of the maximum likelihood point, and the shaded blue region displays the S/N’s 90% credible interval. Both the ﹩\mathrm{ln}{\rm{BF}}﹩ and the upper edge of the S/N’s credible interval peak at x = 3 (black dashed vertical line), which corresponds to the point where the selected data segment exceeds past the peak of the flare. The strong differences in ﹩\mathrm{ln}{\rm{BF}}﹩ and S/N across extension factors shows that differences in data selection can greatly influence the results.
Paper: Pitfalls of Periodograms: The Nonstationarity Bias in the Analysis of Quasiperiodic Oscillations
Authors: Moritz Hübner, Daniela Huppenkothen, Paul D. Lasky, and Andrew R. Inglis
Figure caption: Simulated data of a nonstationary QPO and red noise in surrounding stationary white noise. In the time series (top) we show how a QPO and red noise are transitioning smoothly into the surrounding part of the time series that is pure white noise (∣t∣ > 10 s) owing to the Hann window that we have applied. In the periodogram (bottom) for ∣t∣ ≤ 10 s the QPO is clearly visible by eye. The Hann window also produces an additional broad feature at ≈ 0.3 Hz in the periodogram.
Paper: Pitfalls of Periodograms: The Nonstationarity Bias in the Analysis of Quasiperiodic Oscillations
Authors: Moritz Hübner, Daniela Huppenkothen, Paul D. Lasky, and Andrew R. Inglis
Figure caption: S/N (blue) and ﹩\mathrm{ln}{\rm{BF}}﹩ (orange) vs. the extension factor for simulated data of a nonstationary QPO and red noise with white noise as described in Section 4.4 for extension with white noise (top) and zeros (bottom). The solid blue line displays the S/N of the maximum likelihood point, and the shaded blue region displays the S/N’s 90% credible interval.
Paper: Pitfalls of Periodograms: The Nonstationarity Bias in the Analysis of Quasiperiodic Oscillations
Authors: Moritz Hübner, Daniela Huppenkothen, Paul D. Lasky, and Andrew R. Inglis
Figure caption: Nita et al. (2014) χ2-tests in the case of a QPO and white noise extended with zeros as described in Section 4.2 (top), and the case of QPO, red noise, and white noise extended with white noise as described in Section 4.4 (bottom). We see in the top panel that the overall fit (blue) and the fit for frequencies above the QPO frequency (green) have χ2 ≈ 1, indicating a good fit. The local χ2-test around the QPO frequency f0 indicates a good fit only for x = 1 and falls much below that for x > 1, indicating overfitting. This implies that the local χ2-test can detect nonstationarity bias in this instance. In the bottom panel, we display some of the limitations of the local χ2-test when we deal with narrow QPOs. For x ≲ 6 the local χ2-test (orange) around f0 swings widely, as we have too few frequency bins within the range. Above x ≈ 6, enough frequency bins accumulate within the range, and we detect the overfitting. We also note that the χ2-test for the entire PSD (blue) and frequencies above the QPO frequency (green) indicate an overall good fit despite us overfitting the QPO.
Paper: Pitfalls of Periodograms: The Nonstationarity Bias in the Analysis of Quasiperiodic Oscillations
Authors: Moritz Hübner, Daniela Huppenkothen, Paul D. Lasky, and Andrew R. Inglis
Figure caption: Solar flare X-ray light curve as observed with GOES in the 1–8 Å band. The figure shows the time selected as done with AFINO. The inset zooms in on the tail of the light curve, where the QPO is clearly visible. The left and right edges of the small inset box demarcate the three segments noted in Table 1.
Paper: Pitfalls of Periodograms: The Nonstationarity Bias in the Analysis of Quasiperiodic Oscillations
Authors: Moritz Hübner, Daniela Huppenkothen, Paul D. Lasky, and Andrew R. Inglis
Figure caption: Maximum likelihood fit of the periodogram just for the second segment of the GOES light curve. The QPO is clearly visible and highly significant. We draw the 2σ and 3σ detection limits based on the Bonferroni-corrected frequentist statistics. We note that the QPO is located in the red-noise-dominated part of the PSD.
Paper: Pitfalls of Periodograms: The Nonstationarity Bias in the Analysis of Quasiperiodic Oscillations
Authors: Moritz Hübner, Daniela Huppenkothen, Paul D. Lasky, and Andrew R. Inglis
Figure caption: Simulated data of a nonstationary QPO in a deterministic transient flare shape in the presence of white photon-counting noise. The time series (top) shows the dominant transient and the QPO that is present for 20 s on the top of the flare (inset). The periodogram for the entire 400 s time series (bottom) has a relatively wide (σ = 0.1) QPO at 5 Hz (barely visible). For our analysis, we cut off all frequencies below 0.5 Hz to avoid any effects arising from the power in low frequencies due to the flare shape.
Paper: Pitfalls of Periodograms: The Nonstationarity Bias in the Analysis of Quasiperiodic Oscillations
Authors: Moritz Hübner, Daniela Huppenkothen, Paul D. Lasky, and Andrew R. Inglis
Figure caption: S/N and Bayes factor for the presence of a QPO in a transient flare for different extension factors, with x = 1 corresponding to the 20 s inset from the top of Figure 10. While we already start with very strong evidence of a QPO at x = 1, the Bayes factors continue to increase as we extend the time series to include more of the transient.
Paper: Pitfalls of Periodograms: The Nonstationarity Bias in the Analysis of Quasiperiodic Oscillations
Authors: Moritz Hübner, Daniela Huppenkothen, Paul D. Lasky, and Andrew R. Inglis
Figure caption: Spectrograms of the solar flare light curve using 200 s (top) and 2760 s nonoverlapping segments (bottom), corresponding to the segment durations in Section 5. We highlight the central location of the QPO in the time–frequency plot with the red plus sign. The color bar shows the log of the power in each time–frequency bin. The QPO is hardly identifiable in the top panel, as it only appears for 1–2 time bins. Meanwhile, the QPO is strongly pronounced in the bottom panel owing to the nonstationarity bias.
Paper: A New Catalog of Head–Tail Radio Galaxies from the VLA FIRST Survey
Authors: Tapan K. Sasmal, Soumen Bera, Sabyasachi Pal, and Soumen Mondal
Figure caption: FIRST image of a sample of 12 narrow-angle tail (NAT) radio sources (contours) overlaid on the DSS2 red image (gray scale).
Paper: A New Catalog of Head–Tail Radio Galaxies from the VLA FIRST Survey
Authors: Tapan K. Sasmal, Soumen Bera, Sabyasachi Pal, and Soumen Mondal
Figure caption: FIRST image of a sample of 12 wide-angle tail (WAT) radio sources (contours) overlaid on the DSS2 red image (gray scale).
Paper: A New Catalog of Head–Tail Radio Galaxies from the VLA FIRST Survey
Authors: Tapan K. Sasmal, Soumen Bera, Sabyasachi Pal, and Soumen Mondal
Figure caption: Histogram showing the angle distribution of narrow-angle tail (NAT) and wide-angle tail (WAT) sources. Left panel is for NAT sources (green color) and right panel is for WAT sources (violet color).
Paper: A New Catalog of Head–Tail Radio Galaxies from the VLA FIRST Survey
Authors: Tapan K. Sasmal, Soumen Bera, Sabyasachi Pal, and Soumen Mondal
Figure caption: Histogram showing spectral index (﹩{\alpha }_{150}^{1400}﹩) distribution of NAT candidates.
Paper: A New Catalog of Head–Tail Radio Galaxies from the VLA FIRST Survey
Authors: Tapan K. Sasmal, Soumen Bera, Sabyasachi Pal, and Soumen Mondal
Figure caption: Histogram showing spectral index (﹩{\alpha }_{150}^{1400}﹩) distribution of WAT candidates.
Paper: A New Catalog of Head–Tail Radio Galaxies from the VLA FIRST Survey
Authors: Tapan K. Sasmal, Soumen Bera, Sabyasachi Pal, and Soumen Mondal
Figure caption: Plot showing the radio luminosity (Lrad) distribution of WAT and NAT sources with redshifts (z).
Paper: 2021 Census of Interstellar, Circumstellar, Extragalactic, Protoplanetary Disk, and Exoplanetary Molecules
Authors: Brett A. McGuire
Figure caption: Cumulative number of known interstellar molecules over time. After the birth of molecular radio astronomy in the 1960s, there have been on average 3.9 new detections per year. The commissioning dates of several major contributing facilities are noted with arrows.