adsabs/AstroCLIMB huggingface dataset:
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: The TCF periodograms and best period phase-folded light curves for the stars in Figure 3. The red curve is the LOESS fit to trends in the median of the periodogram. The blue cross indicates the peak with the highest S/N over a window around that peak. The lower left panel shows the original light curve phase-folded on the best TCF period. The lower right panel shows the residuals after the best-fit ARIMA model has been subtracted from the light curve phase-folded on the parameters from the best TCF periodogram peak. It should be noted that the ordinate scales of the two folded light curves differ.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Feature importance for the final Random Forest classifier ordered by importance. Descriptions of the 37 features appear in Table 1.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Scatter plots of the transit parameters of the 949 confirmed Kepler planets from the NASA Exoplanet Archive (NASA Exoplanet Science Institute 2022), accessed 2021 March 14, plotted in olive green in the left column. The distribution of the synthetically created exoplanet transit parameters created using Adaptive Neighbor SMOTE (ANS) on the 949 Kepler planets are plotted in teal in the right column. Smoothed contours have been included to better illustrate the distributions.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Distribution of p-values from the Ljung–Box test for the light curves extracted from the DIAmante data set (on the left) and for the ARIMA residuals (on the right). The first bin in the histogram of Ljung–Box test p-values in the DIAmante data (left) has a frequency of 318,227.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Confusion matrix for the final RF classifier with threshold P RF = 0.300. Values are based on the validation set and OOB predictions for the training set.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: The steps for injecting a synthetic transit signal into a random DIAmante light curve. The top panel shows the original DIAmante light curve. The middle panel shows the transit mask created for a planetary injection. The bottom panel shows the final injected light curve.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: The estimates of the deconvolved half width at half maximum, HWHMeff (left), and position angle relative to the continuum (right) of the [Ne II] 12.81 μm emission in our models without (fiducial, red), and with a 15 au dust cavity (cyan) as a function of the model’s inner radius, estimated from 2D Gaussian fits. For the left-hand panel, the right-hand axis gives the corresponding deprojected size at the distance of T Cha. The horizontal dotted lines indicate the observational value derived using the standard star HD37962 as the PSF model, while the dotted–dashed lines are the equivalent derived using HD167060 as an alternative standard star. The error bars on the simulation data (or equivalently, the shaded gray regions for the observations) are the uncertainties obtained by propagating the uncertainty on the position angle of the fit; these are typically smaller or similar in size to the systematic difference due to the uncertainty in the PSF model.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: Cross sections of the inner 13 au (1 r  G ) of the wind. The first panel shows a streamline from the self-similar model (gray dashed line) superposed on the temperatures calculated by MOCASSIN, with various significant angles indicated. The second and third panels show the neutral hydrogen density (at this level of ionization, essentially equal to the gas density) and electron densities, respectively; the dashed contours show where the critical densities with neutral H/electrons are reached for each transition and are labeled by the corresponding ion. The fourth panel shows the ionization fraction with the contours indicating where neutral H and electrons should contribute equally to the excitation of the transitions. The bottom row shows, from left to right, the emissivities of the [Ne II], [Ne III], [Ar II], and [Ar III] lines; in each case, the contour encloses the brightest region where 50% of the total luminosity is emitted.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: A comparison between the moment 0 maps of the integrated line flux across all wavelengths for the unconvolved model for the line emission (left), the continuum-subtracted synthetic image of each line (center), and the observed line emission (Bajaj et al. 2024, right). Superposed as green dashed lines on the central and right-hand panels are the 2D Gaussian fits, while the left-hand panels instead show the estimated deconvolved fit. The gray ellipses on the central and right-hand panels indicate the size of the synthetic PSF and HD37962 PSF models, respectively.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: Examples of the integrated emission maps of [Ne II] (left) and [Ar II] (right) for different mass-loss rates and inner radii for models using the hiLX_TCha_sUV spectrum. These are provided as inputs to MIRISIM for the synthetic imaging. Each of the left-hand panels shows the full field of view in Channel 3 (which contains the [Ne II] line). The right-hand panels show the same field of view for ease of comparison between the two lines with the field of view of Channel 1 (which contains the [Ar II] line) shown by the dashed box.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: Comparison of the ratio of the [Ar III] 8.99 μm and [Ar II] 6.98 μm lines to the ratio of the [Ne III] 15.55 μm and [Ne II] 12.81 μm. Each set of points of a given color represents a particular one of the five spectra considered in this work; increasing point sizes indicate the sequence of inner radii from smallest to largest. Results are shown for different ﹩\dot{M}﹩ on each panel. JWST measurements for T Cha are shown as the gray cross in the lower left—the error bar includes the 5% absolute flux error added to the 1σ error in quadrature (Bajaj et al. 2024) but is generally too small to be visible except in relation to the [Ar III] flux. The shaded regions indicate values that would be consistent with CS Cha (pink) or TW Hya (brown), while the hashed vertical lines indicate the regions excluded by the upper limits on [Ne III] emission for V4046 Sgr (purple) and RX J1615.3-3255 (cyan). The diagonal dotted gray line indicates equal ratios.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: Comparison of the fluxes of the [Ne III] 15.55 μm and [Ne II] 12.81 μm lines. The models are plotted the same as in Figure 5, focusing on higher-density normalizations (mass-loss rates). The JWST measurements for T Cha are included for comparison (gray cross) along with literature estimates for other sources (Table 6). The blue squares are predictions from Ercolano & Owen (2010; borderless: full disk, black border: gas cavity) using the same spectrum as our Ercolano_RSCVn models.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: Observable mass-loss rates inferred from our hiLX_TCha_sUV models. The models were constructed with nominal mass-loss normalizations of 10−10 M ☉ yr−1 (blue), 10−9 M ☉ yr−1 (orange), 10−8 M ☉ yr−1 (green), and 10−7 M ☉ yr−1 (red). The observable rates were determined by taking the outer radius of the wind to be the radius containing 95% (dotted–dashed) and 97% (dashed) of the [Ne II] 12.81 μm emission. The black dotted line indicates T Cha’s observed accretion rate (Cahill et al. 2019) for comparison.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: The photoionization cross sections (per hydrogen atom) σ H used in this work. The black dotted–dashed line shows the total cross section of a neutral gas while the blue and orange lines indicate that of Ne I and Ar I, respectively, with major thresholds corresponding to ionization from different electron shells labeled. The typical energy ranges described as EUV (13.6–100 eV) or X-ray (>100 eV) are indicated by the shaded zones.
Paper: Modeling JWST MIRI-MRS Observations of T Cha: Mid-IR Noble Gas Emission Tracing a Dense Disk Wind
Authors: Andrew D. Sellek, Naman S. Bajaj, Ilaria Pascucci, Cathie J. Clarke, Richard Alexander, Chengyan Xie, Giulia Ballabio, Dingshan Deng, Uma Gorti, Andras Gaspar, Jane Morrison
Figure caption: As with Figure 6 but comparing the ratio of the [Ar II] 6.98 μm and [Ne II] 12.81 μm lines.
Paper: Stellar Variability and Distance Indicators in the Near-infrared in Nearby Galaxies. I. RR Lyrae and Anomalous Cepheids in Draco Dwarf Spheroidal
Authors: Anupam Bhardwaj, Marina Rejkuba, Chow-Choong Ngeow, Marcella Marconi, Vincenzo Ripepi, Abhinna Sundar Samantaray, Harinder P. Singh
Figure caption: Optical and NIR color–magnitude diagrams for the proper-motion cleaned members of Draco dSph. Left: V − I, I color–magnitude diagram. Right: J − K  s , J color–magnitude diagram. The overplotted open circles represent red giants used to determine average color, J − K  s  = 0.74 ± 0.03 mag, for TRGB measurement. The dashed lines represent the location of TRGB in Draco dSph in the optical and NIR and the shaded regions display their ±1σ uncertainties. The dotted lines show BaSTI stellar isochrones (Pietrinferni et al. 2021) with 10 Gyr age and metallicity of Draco dSph. The open and filled arrows display the expected location of TRGB corresponding to the distance modulus of 19.35 and 19.85 mag, respectively. These are the upper and lower limit of the distance moduli for Draco in the recent literature studies (see text).
Paper: Stellar Variability and Distance Indicators in the Near-infrared in Nearby Galaxies. I. RR Lyrae and Anomalous Cepheids in Draco Dwarf Spheroidal
Authors: Anupam Bhardwaj, Marina Rejkuba, Chow-Choong Ngeow, Marcella Marconi, Vincenzo Ripepi, Abhinna Sundar Samantaray, Harinder P. Singh
Figure caption: Near-infrared period–luminosity relations for ACEP (triangles) in J (top), H (middle), and K  s  (bottom). In the bottom panel, open circles and squares represent fundamental and first-overtone mode ACEP in the LMC, respectively, and the shaded regions represent their PL relations with ±1σ scatter (Ripepi et al. 2014). The dashed lines represent best-fitting PL relation to four ACEP pulsating in the fundamental mode while the dotted lines display ±2.5σ offsets from the best-fitting relation. The first-overtone mode ACEP is marked with overplotted open triangle.
Paper: Stellar Variability and Distance Indicators in the Near-infrared in Nearby Galaxies. I. RR Lyrae and Anomalous Cepheids in Draco Dwarf Spheroidal
Authors: Anupam Bhardwaj, Marina Rejkuba, Chow-Choong Ngeow, Marcella Marconi, Vincenzo Ripepi, Abhinna Sundar Samantaray, Harinder P. Singh
Figure caption: NIR color–magnitude diagram for Draco dSph in (J − K  s ), K  s  (small gray dots). The larger symbols represent likely Draco members based on their proper motions in Gaia DR3. Variable stars studied in this work are also overplotted with their mean magnitudes and colors. The theoretically predicted instability strip boundaries—fundamental red edge (solid red line) and first-overtone blue edge (dashed blue line) are taken from Marconi et al. (2015). On the right the representative ±3σ error bars are shown as a function of magnitude and color.
Paper: Stellar Variability and Distance Indicators in the Near-infrared in Nearby Galaxies. I. RR Lyrae and Anomalous Cepheids in Draco Dwarf Spheroidal
Authors: Anupam Bhardwaj, Marina Rejkuba, Chow-Choong Ngeow, Marcella Marconi, Vincenzo Ripepi, Abhinna Sundar Samantaray, Harinder P. Singh
Figure caption: Near-infrared period–luminosity relations for RRab and RRc stars (left) and all RRL stars (right) in J (top), H (middle), and K  s  (bottom). In the right panels, the periods for the RRc stars have been shifted to their corresponding fundamental-mode periods, as explained in the text. The gray symbols represent outliers removed iteratively during the fitting procedure. The dashed lines represent best-fitting linear regressions over the period range under consideration, while the dotted lines display ±2.5σ offsets from the best-fitting PLRs.
Paper: Stellar Variability and Distance Indicators in the Near-infrared in Nearby Galaxies. I. RR Lyrae and Anomalous Cepheids in Draco Dwarf Spheroidal
Authors: Anupam Bhardwaj, Marina Rejkuba, Chow-Choong Ngeow, Marcella Marconi, Vincenzo Ripepi, Abhinna Sundar Samantaray, Harinder P. Singh
Figure caption: Example phased light curves of RR Lyrae stars in NIR bands covering the entire range of periods in our sample. Left: RRab stars. Right: RRc/RRd stars. The J-band (blue) and K  s -band (red) light curves are offset for clarity by +0.2 mag and −0.3 mag, respectively. The dashed lines represent the best-fitting templates to the data in each band. The Gaia DR3 star ID, variable subtype, and the pulsation period are included at the top of each panel.
Paper: Stellar Variability and Distance Indicators in the Near-infrared in Nearby Galaxies. I. RR Lyrae and Anomalous Cepheids in Draco Dwarf Spheroidal
Authors: Anupam Bhardwaj, Marina Rejkuba, Chow-Choong Ngeow, Marcella Marconi, Vincenzo Ripepi, Abhinna Sundar Samantaray, Harinder P. Singh
Figure caption: Same as Figure 1 but for ACEP stars. The J-band (blue) and K  s -band (red) light curves are offset for clarity by +0.1 mag and −0.2 mag, respectively.
Paper: Stellar Variability and Distance Indicators in the Near-infrared in Nearby Galaxies. I. RR Lyrae and Anomalous Cepheids in Draco Dwarf Spheroidal
Authors: Anupam Bhardwaj, Marina Rejkuba, Chow-Choong Ngeow, Marcella Marconi, Vincenzo Ripepi, Abhinna Sundar Samantaray, Harinder P. Singh
Figure caption: Same as Figure 4, but for ﹩{W}_{J,{K}_{s}}﹩ period–Wesenheit relation for RRab and RRc stars (top) and all RRL stars (bottom).
Paper: Stellar Variability and Distance Indicators in the Near-infrared in Nearby Galaxies. I. RR Lyrae and Anomalous Cepheids in Draco Dwarf Spheroidal
Authors: Anupam Bhardwaj, Marina Rejkuba, Chow-Choong Ngeow, Marcella Marconi, Vincenzo Ripepi, Abhinna Sundar Samantaray, Harinder P. Singh
Figure caption: Same as Figure 6, but for ﹩{W}_{J,{K}_{s}}﹩ period–Wesenheit relation for ACEP stars.
Paper: The Digitization of Photographic Spectra in the Dominion Astrophysical Observatory Plate Collection with Commercial Scanners: A Pilot Study
Authors: T. J. Davidge
Figure caption: Moderately weak absorption lines in the CCD and 1963 spectra. The scanned photographic spectrum contains weak features that match those in the CCD spectrum.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: RM grids of polarized components in the median-filtered EL, EM, EC, and GL observations. The markers indicate the presence of a polarized component at that location in the observation. Positive RMs are red and negative RMs are blue, while the depth of the color indicates the magnitude of the RM. Circle and star markers denote Faraday simple and complex components, respectively. Plus signs indicate Faraday simple components where the RM is consistent with 0 within the uncertainty. The color scale of the background total intensity image is the same as in Figure 1.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: (a) Plot of distance to the NNN vs. NN for the polarized components in the EC RM catalog. The points are colored according to whether only the NN is polarized (green filled circles), only the NNN is polarized (green open circles), both the NN and NNN are polarized (black filled circles), or neither the NN nor NNN are polarized (black open circles). Dashed lines are plotted at 70″ and 100″ to highlight different populations of sources described in the text. (b) Absolute difference in RM of polarized components in the EC RM catalog and their NN vs. distance. The dashed line at 70″ separates small- and large-separation pairs. The data are colored by polarized fraction, with low polarized fraction components (p < 0.03) in orange and high polarized fraction components (p ≥ 0.03) in green, and the solid colored lines indicate the median value of the two populations of pairs.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Comparison of the σ add and m 2 complexity metrics for polarized components in the median-filtered GL observation. The points are colored by log10(S/Npol), and the thresholds for complexity for both metrics are shown by dashed lines: σ add = 1 (blue vertical) and m 2 = 0.5 (red horizontal). Note that the σ add axis is on a log scale, while the m 2 axis is on a linear scale.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Distribution of the difference between the EM and EC RMs in units of δRM. We overplot a Gaussian fit to the data, shown by the dashed red line. There are three points beyond ±3σ and no points beyond the bounds of the graph. The distribution has μ ∼ 0 and σ ∼ 1, suggesting that the large spread in RMs in Figure 10 is due to the large RM uncertainties in the EM and is not an issue with data quality.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Left: EC RMs vs. EL RMs. Right: EC RMs vs. EM RMs. The dashed red line in both panels is the one-to-one line.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Polarized intensity vs. total intensity for components in the four median-filtered polarized component catalogs. Lines of constant polarized fraction are plotted at 0.1%, 1%, and 10%, and the solid blue line indicates the typical estimated residual off-axis leakage level in the observation.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Scatter in RM as measured by the IQR vs. S/Npol for both low (p < 0.03) and high (p ≥ 0.03) polarized fraction components.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Top panel: total intensity image of a region of the EL observation. Polarized component RMs are indicated with circles with color corresponding to the sign and magnitude of the RM as described in Figure 13(c). Bottom panel: same as for the top panel but in peak polarized intensity.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Comparison of EL and EM POSSUM RMs to RMs from the QUOCKA survey. POSSUM EL RMs are plotted as orange circles, and POSSUM EM RMs are plotted as blue triangles.