adsabs/AstroCLIMB huggingface dataset:
Paper: The Space Weather Context of the First Extreme Event of Solar Cycle 25, on 2022 September 5
Authors: Evangelos Paouris, Angelos Vourlidas, Athanasios Kouloumvakos, Athanasios Papaioannou, Vamsee Krishna Jagarlamudi, Timothy Horbury
Figure caption: The SEP events with E > 300 MeV (blue crosses) and non-SEP events (black diamonds) as a function of the maximum magnitude of the SXR flux (x-axis) and the POS CME speed (y-axis). We apply an ML model (second-order polynomial logistic regression) to distinguish the SEP productive events from the non-SEP cases. The decision boundary level (red line) is 30%. We overplot the 2022 September 5 and 2012 July 23 events with their corresponding probabilities (99% and 95%, respectively) that could produce an SEP event with E > 300 MeV. The metrics of accuracy, MSE, and R 2 are denoted in the top left corner. In this version of our model, the metrics indicate a perfect performance, which is not a surprise, as the decision boundary perfectly separates the black from the blue points.
Paper: The Space Weather Context of the First Extreme Event of Solar Cycle 25, on 2022 September 5
Authors: Evangelos Paouris, Angelos Vourlidas, Athanasios Kouloumvakos, Athanasios Papaioannou, Vamsee Krishna Jagarlamudi, Timothy Horbury
Figure caption: The PSP position (red star) at the time of the eruption around 16:00 UT in the Earth ecliptic (HEE) coordinate system. The propagation direction of the CME is indicated with the blue dashed lines. The directions of the other spacecraft (Solar Orbiter, ST-A, and SOHO) are indicated with the solid (black, magenta, and green) lines. The perihelion of the PSP orbit (orange line) is depicted with the orange diamond. The FOV of WISPR is represented by the light gray shaded region bordered with red solid lines for WISPR-I and red dashed–dotted lines for WISPR-O telescopes. The region where the electron scattering efficiency is around maximum, i.e., the Thomson sphere, is shown by the gray circle.
Paper: The Space Weather Context of the First Extreme Event of Solar Cycle 25, on 2022 September 5
Authors: Evangelos Paouris, Angelos Vourlidas, Athanasios Kouloumvakos, Athanasios Papaioannou, Vamsee Krishna Jagarlamudi, Timothy Horbury
Figure caption: Effective connected magnetic field strength (B eff) as a function of time for AR 13088. The onset times of the C- and M-class solar flares associated with this AR are indicated at the top of the figure with blue and green triangles. The HARP that gave the maximum B eff of ∼2420 G is overplotted. Above the top x-axis in dark blue is presented the Stonyhurst longitude of the flux-weighted center of active pixels of the HARP.
Paper: The Space Weather Context of the First Extreme Event of Solar Cycle 25, on 2022 September 5
Authors: Evangelos Paouris, Angelos Vourlidas, Athanasios Kouloumvakos, Athanasios Papaioannou, Vamsee Krishna Jagarlamudi, Timothy Horbury
Figure caption: Histograms of mass (top) and kinetic energy (bottom) for a sample of 19,210 CMEs observed in the period 1996 January 22–2022 July 1. The mean and median values are indicated with the solid and dashed lines, respectively. For better visual comparison, we also indicate the 2022 September 5 and 2012 July 23 CMEs with the vertical red and blue solid lines, respectively. Both cases are placed in the rare and extreme cases of the sample.
Paper: The Space Weather Context of the First Extreme Event of Solar Cycle 25, on 2022 September 5
Authors: Evangelos Paouris, Angelos Vourlidas, Athanasios Kouloumvakos, Athanasios Papaioannou, Vamsee Krishna Jagarlamudi, Timothy Horbury
Figure caption: Magnetic fields (magnitude and RTN components), solar wind speed, density, and temperature in situ data obtained from PSP on 2022 September 5 for the time interval 17:00–19:20 UT. The arrival of the shock at the PSP position at 17:27 (orange vertical dashed line) is obvious in all parameters. The blue horizontal dashed line in the solar wind speed panel indicates the maximum observed speed of approximately 1360 km s−1 at 17:38 UT, which is in agreement with our kinematic analysis using COR2 data.
Paper: The Space Weather Context of the First Extreme Event of Solar Cycle 25, on 2022 September 5
Authors: Evangelos Paouris, Angelos Vourlidas, Athanasios Kouloumvakos, Athanasios Papaioannou, Vamsee Krishna Jagarlamudi, Timothy Horbury
Figure caption: Radial distances with error bars as a function of time utilizing the harmonic mean geometric technique on the time-elongation profile. On the available (black) data points, we apply a second-order polynomial fit (orange curve) to calculate the deceleration of the tracking point at the direction of PA270. The distances of Solar Orbiter and 1 au are represented with yellow and red horizontal lines. Beyond a distance of ∼130 R ☉, we assume a coasting movement (solid and dashed green lines). The ToA of the CME’s shock at Solar Orbiter is estimated with the HeRPA algorithm on September 6 at 09:55, approximately 5 minutes earlier than the in situ observations. The arrival at 1 au (blue triangle) is estimated almost 8 hr later, indicating a transit time of almost 25.5 hr and a transit speed of ∼1560 km s−1.
Paper: The Space Weather Context of the First Extreme Event of Solar Cycle 25, on 2022 September 5
Authors: Evangelos Paouris, Angelos Vourlidas, Athanasios Kouloumvakos, Athanasios Papaioannou, Vamsee Krishna Jagarlamudi, Timothy Horbury
Figure caption: In situ 1 minute average data (from top to bottom) of proton density, solar wind speed, and magnetic field components in the RTN coordinate system from the MAG and SWA instruments on the Solar Orbiter mission. The last panel depicts the calculated Dst index values utilizing the Burton et al. (1975) and O’Brien & McPherron (2000) models. The dashed lines represent the extrapolated values at 1 au.
Paper: The Atacama Cosmology Telescope: Systematic Transient Search of 3 Day Maps
Authors: Yaqiong Li, Emily Biermann, Sigurd Naess, Simone Aiola, Rui An, Nicholas Battaglia, Tanay Bhandarkar, Erminia Calabrese, Steve K. Choi, Kevin T. Crowley, Mark Devlin, Cody J. Duell, Shannon M. Duff, Jo Dunkley, Rolando Dünner, Patricio A. Gallardo, Yilun Guan, Carlos Hervías-Caimapo, Adam D. Hincks, Johannes Hubmayr, Kevin M. Huffenberger, John P. Hughes, Arthur Kosowsky, Thibaut Louis, Maya Mallaby-Kay, Jeff McMahon, Federico Nati, Michael D. Niemack, John Orlowski-Scherer, Lyman Page, Maria Salatino, Cristóbal Sifón, Suzanne T. Staggs, Cristian Vargas, Eve M. Vavagiakis, Yuhan Wang, Edward J. Wollack
Figure caption: Combined ACT data from 2007–2019 overlayed with the transient positions. Images from DSS at each location, indicated by a + sign in the center of each image, are also shown with a 1′ contour plotted for scale. The majority of the transient events have bright stellar counterparts seen in the optical.
Paper: An Anisotropic Density Turbulence Model from the Sun to 1 au Derived from Radio Observations
Authors: Eduard P. Kontar, A. Gordon Emslie, Daniel L. Clarkson, Xingyao Chen, Nicolina Chrysaphi, Francesco Azzollini, Natasha L. S. Jeffrey, Mykola Gordovskyy
Figure caption: Left: spectrum of density fluctuations showing the q 2 S(q) ∼ q −γ  spectrum at large scales ﹩\gt {q}_{o}^{-1}﹩, the (Kolmogorov) inertial range q 2 S(q) ∼ q −5/3 between the outer scale ﹩{q}_{o}^{-1}﹩ and the inner scale ﹩{q}_{i}^{-1}﹩, and the dissipation range q 2 S(q) ∼ q −δ  (with δ > 2) at small scales ﹩\lt {q}_{i}^{-1}﹩. Right: the ﹩\mathrm{ln}q﹩ space integrand required to compute the mean wavenumber ﹩\overline{q\,{\epsilon }^{2}}\propto \int q\,S(q)\,{q}^{2}\,{dq}=\int {q}^{4}\,S(q)\,d\mathrm{ln}q﹩, highlighting the peak near the inner scale ﹩{q}_{i}^{-1}﹩. All axes are on logarithmic scales.
Paper: The Ultraviolet to Mid-infrared Extinction Law of the Taurus Molecular Cloud Based on the Gaia DR3, GALEX, APASS, Pan-STARRS1, 2MASS, and WISE Surveys
Authors: Ling Li, Shu Wang, Xiaodian Chen, QingQuan Jiang
Figure caption: Comparison of our E(G BP − G RP) with Gaia E(G BP − G RP), colored by the number density of stars. The x-axis is the E(G BP − G RP) derived in this work, the y-axis is the E(G BP − G RP) from Gaia DR3, and the black solid line is y = x. The bottom panel is the distribution of CE residuals Δ = ﹩E{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{\mathrm{our}}-E{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{\mathrm{Gaia}}﹩, and the black dashed line is y = 0.
Paper: The Ultraviolet to Mid-infrared Extinction Law of the Taurus Molecular Cloud Based on the Gaia DR3, GALEX, APASS, Pan-STARRS1, 2MASS, and WISE Surveys
Authors: Ling Li, Shu Wang, Xiaodian Chen, QingQuan Jiang
Figure caption: The UV to mid-IR average extinction curve of the Taurus molecular cloud (red filled circles with error bars). The color bars in J, H, K S, W1, and W2 bands represent the RMSE of the relative extinction values for the different types of stars. For comparison, the extinction curves of (Cardelli et al. 1989, pink dashed line), (Wang & Chen 2019, blue solid line), (Fitzpatrick et al. 2019, orange solid line), (Hensley & Draine 2020, green dotted–dashed line), and (Gordon et al. 2023, purple dotted line) are also shown.
Paper: The Ultraviolet to Mid-infrared Extinction Law of the Taurus Molecular Cloud Based on the Gaia DR3, GALEX, APASS, Pan-STARRS1, 2MASS, and WISE Surveys
Authors: Ling Li, Shu Wang, Xiaodian Chen, QingQuan Jiang
Figure caption: CE–CE diagrams E(G BP − G RP) vs. E(λ − G RP) or E(λ − G BP) of the Taurus dwarfs with −0.5 ≤ [M/H] < 0, where λ is B and V bands from APASS; r, i, and z bands from PS1; J, H and K S bands from 2MASS; and W1 band from WISE, respectively, from the top left to the bottom right. The black lines are the best linear-fit lines, and the results are listed in the upper left corner of each subfigure.
Paper: The Ultraviolet to Mid-infrared Extinction Law of the Taurus Molecular Cloud Based on the Gaia DR3, GALEX, APASS, Pan-STARRS1, 2MASS, and WISE Surveys
Authors: Ling Li, Shu Wang, Xiaodian Chen, QingQuan Jiang
Figure caption: Top: extinction map of the Taurus molecular cloud region colored by the CE E(G BP − G RP). Bottom: variation of extinction law in the Taurus molecular cloud region characterized by R V. The entire Taurus region is divided into subregions with a grid of l × b = 2° × 1°. There is no correlation between the regions with large deviations in R V and the amount of the CE E(G BP − G RP) or any structure of the Taurus cloud.
Paper: The Ultraviolet to Mid-infrared Extinction Law of the Taurus Molecular Cloud Based on the Gaia DR3, GALEX, APASS, Pan-STARRS1, 2MASS, and WISE Surveys
Authors: Ling Li, Shu Wang, Xiaodian Chen, QingQuan Jiang
Figure caption: CE–CE diagrams E(G BP − G RP) vs. E(λ − G RP) of the Taurus giants, where λ is the G band from Gaia; B and V bands from APASS; J, H, and K S bands from 2MASS; and W1, W2, and W3 bands from WISE, respectively, from the top left to the bottom right. The black lines are the best linear-fit lines, and the results are listed in the upper left corner of each subfigure.
Paper: The Ultraviolet to Mid-infrared Extinction Law of the Taurus Molecular Cloud Based on the Gaia DR3, GALEX, APASS, Pan-STARRS1, 2MASS, and WISE Surveys
Authors: Ling Li, Shu Wang, Xiaodian Chen, QingQuan Jiang
Figure caption: Distribution of R V for each subregion of the Taurus molecular cloud. This distribution is fitted by a Gaussian function with a mean value of μ = 3.13 and a width of σ = 0.32. The dotted lines show the 16th, 50th, and 84th percentiles of the R V distribution.
Paper: The Ultraviolet to Mid-infrared Extinction Law of the Taurus Molecular Cloud Based on the Gaia DR3, GALEX, APASS, Pan-STARRS1, 2MASS, and WISE Surveys
Authors: Ling Li, Shu Wang, Xiaodian Chen, QingQuan Jiang
Figure caption: UV to mid-IR multiband extinction A  λ  relative to A V (red circles with error bars) for different types of stars. The blue lines are the R V = 3.1 extinction curve of Wang & Chen (2019).
Paper: The Ultraviolet to Mid-infrared Extinction Law of the Taurus Molecular Cloud Based on the Gaia DR3, GALEX, APASS, Pan-STARRS1, 2MASS, and WISE Surveys
Authors: Ling Li, Shu Wang, Xiaodian Chen, QingQuan Jiang
Figure caption: Determination of intrinsic color indices based on the blue-edge method. Gray dots are dwarf stars with −0.5 ≤ [M/H] < 0 in the diffuse region (235° ≤ l ≤ 245°, −5° ≤ b ≤ 5°) in the T eff vs. observed color diagrams. Magenta asterisks are the zero-reddening stars selected according to the T eff vs. (G BP − G RP) and (J − K S) diagrams. These zero-reddening stars are fitted by a cubic polynomial, and the blue dashed line is the best-fitting lines representing the T eff–intrinsic color relations.
Paper: The Ultraviolet to Mid-infrared Extinction Law of the Taurus Molecular Cloud Based on the Gaia DR3, GALEX, APASS, Pan-STARRS1, 2MASS, and WISE Surveys
Authors: Ling Li, Shu Wang, Xiaodian Chen, QingQuan Jiang
Figure caption: The E(G BP − G RP) vs. E(G − G RP) diagrams of the dwarfs with −0.5 ≤ [M/H] < 0 before (a) and after (b) the curvature correction. Different colors represent dwarf stars in different T eff intervals. The results of the linear fitting of dwarfs in different T eff intervals are listed in the upper left corner of (b).
Paper: The Ultraviolet to Mid-infrared Extinction Law of the Taurus Molecular Cloud Based on the Gaia DR3, GALEX, APASS, Pan-STARRS1, 2MASS, and WISE Surveys
Authors: Ling Li, Shu Wang, Xiaodian Chen, QingQuan Jiang
Figure caption: Left: differences in effective temperature ﹩{\rm{\Delta }}{T}_{\mathrm{eff}}={({T}_{\mathrm{eff}})}_{\mathrm{Gaia}}-{({T}_{\mathrm{eff}})}_{\mathrm{APOGEE}}﹩ as function of estimated extinction A 0. The red dots and blue dots are giants and dwarfs, respectively. The gray dashed line is y = 0. Right: histogram of ΔT eff for giants (red) and dwarfs (blue). N is the normalized number.
Paper: The Ultraviolet to Mid-infrared Extinction Law of the Taurus Molecular Cloud Based on the Gaia DR3, GALEX, APASS, Pan-STARRS1, 2MASS, and WISE Surveys
Authors: Ling Li, Shu Wang, Xiaodian Chen, QingQuan Jiang
Figure caption:  T eff vs. observed color (G BP − G RP) diagram for the dwarfs with −0.5 ≤ [M/H] < 0 in the Taurus region. The red solid line represents the T eff–﹩{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{0}﹩ relation, while colors denote the reddening E(G BP − G RP) of stars.
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: Histograms showing the intensity distributions of the pulsar emission and the background noise for PSR J2210+5712. The dotted and solid histograms show the OFF and ON intensity distributions, respectively. The presence of excess samples in the ON distribution at the level consistent with background noise is evidence for nulling. The blue line shows the Gaussian fit to the OFF histogram. The fit to the ON histogram, shown by the dashed magenta line, is the sum of the “emission” and “null” components. The emission component (orange line) is a Gaussian centered above the background noise. The null component (green line) is a scaled-down version of the Gaussian noise; this scale factor gives the NF, which we measure to be 38.8% ± 2.2% for this pulsar.
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: Timing residuals for PSR J1327+3423 that compare LWA1 TOAs to our AO/GBT timing solution are shown, plotted against radio frequency. The dashed gray line shows δ t = 0. The curved dashed line shows our fit to the residuals assuming a ν −2 dependence, corresponding to a DM 0.000912(9) pc cm−3 higher than the fiducial DM used in our timing model (modulo a constant offset). The dotted–dashed line shows a fit that does not make that assumption. The dependence is consistent with a dispersive delay.
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: Upper limits on T eff for PSR J1239+3239’s ∼0.2 M ☉ companion, over a range of typical WD radii. The solid and dashed lines show the limits assuming DA and DB atmospheres, respectively. The gray points show WD radii and effective temperatures from WDs within 100 pc in the Sloan Digital Sky Survey footprint (Brown et al. 2022), and the blue points show values from the ELM Survey (Kilic et al. 2020).
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: PS1 r-band images, centered at the positions of PSR J0032+6946 (left) and PSR J1239+3239 (right). The red ellipses represent 1000× the uncertainties in the pulsar timing positions. No optical counterparts were found. There is a marginally detected star near the position of PSR J1239+3239 that also appears in the i-band image, but the distance between it and the pulsar is much larger than the frame-time uncertainty (∼0.″1).
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: Intensity of pulsar signal vs. time and rotational phase for typical 820 MHz observations of PSRs J0957−0619, J2145+2158, and J2210+5712, with greater intensity plotted as brighter and lower intensity plotted as darker. The nulling behavior of each pulsar is readily apparent, with the pulsar signal sometimes disappearing for well over a minute.
Paper: Mirror Acceleration of Cosmic Rays in a High-β Medium
Authors: Alex Lazarian, Siyao Xu
Figure caption: Illustration for mirror diffusion. The perpendicular super-diffusion of turbulent magnetic field lines originally identified in Lazarian & Vishniac (1999), induces the parallel diffusion of particles that stochastically interact with different magnetic mirrors. Black lines are magnetic field lines. Blue and red lines are trajectories of two particles with a small initial separation. From LX21.
Paper: Mirror Acceleration of Cosmic Rays in a High-β Medium
Authors: Alex Lazarian, Siyao Xu
Figure caption: The slow-mode eddy is elongated along the local magnetic field direction, with a CR particle spiraling about the magnetic field and the electric field induced by the compression/expansion of the magnetic field. Modified from Cho & Lazarian (2006).
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: Timing residuals for the five pulsars in binary systems are plotted vs. orbital phase (see Equation (5), but one orbit = 1.0 instead of 2π radians). The gray dashed vertical line at ϕ = 0.25 denotes superior conjunction, and the horizontal dashed lines correspond to a residual of zero. The second set of residuals from the bottom are the residuals for PSR J1816+4510 that contributed to our timing solution. The bottommost set of residuals comprises all of our residuals for PSR J1816+4510, including those that exhibit additional timing delays before and after eclipse. In the latter set, TOAs from the full-orbit observations of PSR J1816+4510 were created with shorter subintegrations so that the behavior near eclipse can be seen more easily. The 350, 820, 1500, and 2000 MHz residuals from GBT observations are plotted in red, blue, purple, and yellow, respectively. Error bars are the 1σ uncertainties at each TOA.
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: DMX time series for PSRs J0636+5128, J1327+3423, and J1816+4510, showing the offset from a fiducial DM value at each epoch. The dashed gray line in each plot corresponds to an offset of zero. The plot for PSR J1327+3423 shows DMX in red, corresponding to LWA1 observations; the points in black are from the GBT (before MJD 58000) and AO (after MJD 58000). Epochs for which we were unable to fit for DMX (described in Section 4.2) are not shown. Error bars correspond to the 1σ uncertainty in DMX reported by TEMPO2.
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: Histograms showing the distribution of pulsar spectral indices (α) for pulsars in the ATNF catalog (dashed line) and those in this work (solid line). We calculated spectral indices for pulsars in the ATNF catalog using flux density measurements at 400 and 1400 MHz. Visually, there appears to be an excess of flatter-spectrum pulsars with −1 ≲ α ≲ 0 in this work, but a Kolmogorov–Smirnov test does not indicate that the two samples are drawn from different underlying distributions.
Paper: The Green Bank North Celestial Cap Survey. VIII. 21 New Pulsar Timing Solutions
Authors: W. Fiore, L. Levin, M. A. McLaughlin, A. Anumarlapudi, D. L. Kaplan, J. K. Swiggum, G. Y. Agazie, R. Bavisotto, P. Chawla, M. E. DeCesar, T. Dolch, E. Fonseca, V. M. Kaspi, Z. Komassa, V. I. Kondratiev, J. van Leeuwen, E. F. Lewis, R. S. Lynch, A. E. McEwen, R. Mundorf, H. Al Noori, E. Parent, Z. Pleunis, S. M. Ransom, X. Siemens, R. Spiewak, I. H. Stairs, M. Surnis, T. J. Tobin
Figure caption: The pulsars presented in this work are plotted as red stars (or as dots surrounded by circles, if in binary systems) on this P–﹩\dot{P}﹩ diagram, with values for the rest taken from the ATNF pulsar catalog. Lines of constant minimum surface magnetic field B surf (in Gauss; dashed lines) and characteristic age τ c (dotted–dashed lines) are also shown.