adsabs/AstroCLIMB huggingface dataset:
Paper: An Algorithm to Calibrate and Correct the Response to Unpolarized Radiation of the X-Ray Polarimeter Onboard IXPE
Authors: John Rankin, Fabio Muleri, Allyn F. Tennant, Matteo Bachetti, Enrico Costa, Alessandro Di Marco, Sergio Fabiani, Fabio La Monaca, Paolo Soffitta, Antonino Tobia, Alessio Trois, Fei Xie, Luca Baldini, Niccolò Di Lalla, Alberto Manfreda, Stephen L. O'Dell, Matteo Perri, Simonetta Puccetti, Brian D. Ramsey, Carmelo Sgrò, Martin C. Weisskopf
Figure caption: Schematic of the GPD. See the text for details. Image credit: Weisskopf et al. (2016)
Paper: Accurate Ground-based Astrometry of Naked-eye Stars: The United States Naval Observatory Bright-star Astrometric Database
Authors: Jeffrey A. Munn, John P. Subasavage, Hugh C. Harris, Trudy M. Tilleman
Figure caption: Differences between Gaia and UBAD catalog positions (Gaia − UBAD, R.A. in the top panel and decl. in the bottom panel), normalized by the expected error in the differences, plotted against the formal UBAD position error. The black points are the differences for individual stars. The blue and orange points are the mean and rms differences, respectively, in equal-sized bins. If the error estimates are correct, the rms values should be near one (indicated by the dotted cyan line). The dashed cyan line is a reference line at zero normalized error.
Paper: Accurate Ground-based Astrometry of Naked-eye Stars: The United States Naval Observatory Bright-star Astrometric Database
Authors: Jeffrey A. Munn, John P. Subasavage, Hugh C. Harris, Trudy M. Tilleman
Figure caption: Distributions of differences in the catalog positions between Gaia and UBAD in R.A. (top panel) and decl. (bottom panel).
Paper: Accurate Ground-based Astrometry of Naked-eye Stars: The United States Naval Observatory Bright-star Astrometric Database
Authors: Jeffrey A. Munn, John P. Subasavage, Hugh C. Harris, Trudy M. Tilleman
Figure caption: Stacked histograms of catalog stars in Hipparcos-2 H  p  magnitude. The hatched blue and unhatched orange histograms are for stars with and without an entry in Gaia EDR3, respectively.
Paper: Accurate Ground-based Astrometry of Naked-eye Stars: The United States Naval Observatory Bright-star Astrometric Database
Authors: Jeffrey A. Munn, John P. Subasavage, Hugh C. Harris, Trudy M. Tilleman
Figure caption: Same as Figure 18, except that the UBAD position errors used to normalize the differences now include a floor error of 1.5 mas added in quadrature with the formal error. The x-axis remains the formal error, without the addition of the floor error.
Paper: Accurate Ground-based Astrometry of Naked-eye Stars: The United States Naval Observatory Bright-star Astrometric Database
Authors: Jeffrey A. Munn, John P. Subasavage, Hugh C. Harris, Trudy M. Tilleman
Figure caption: Distribution of the differences between Hipparcos-2 and UBAD proper motions for a clean sample of stars. There are an additional nine and six stars outside the histogram limits in R.A. and decl., respectively.
Paper: Accurate Ground-based Astrometry of Naked-eye Stars: The United States Naval Observatory Bright-star Astrometric Database
Authors: Jeffrey A. Munn, John P. Subasavage, Hugh C. Harris, Trudy M. Tilleman
Figure caption: Same as Figure 20, but comparing UBAD and Gaia proper motions. There are an additional six and one stars outside the histogram limits in R.A. and decl., respectively.
Paper: Accurate Ground-based Astrometry of Naked-eye Stars: The United States Naval Observatory Bright-star Astrometric Database
Authors: Jeffrey A. Munn, John P. Subasavage, Hugh C. Harris, Trudy M. Tilleman
Figure caption: Distribution of the number of UBAD observations used in the astrometry fits.
Paper: Accurate Ground-based Astrometry of Naked-eye Stars: The United States Naval Observatory Bright-star Astrometric Database
Authors: Jeffrey A. Munn, John P. Subasavage, Hugh C. Harris, Trudy M. Tilleman
Figure caption: The ﹩{\chi }_{\nu }^{2}﹩ distributions for the position and proper-motion fits in R.A. (top panel) and decl. (bottom panel). There are an additional six and 10 unplotted stars with ﹩{\chi }_{\nu }^{2}\gt 3﹩ in R.A. and decl., respectively.
Paper: Comparison of Composite and Star-forming Early-type Galaxies
Authors: Yu-Zhong Wu
Figure caption: Comparison of MZ relations (left-hand panel) for star-forming and composite ETGs. Comparison of relations of 12+log(O/H) and log(N/O) (right-hand panel) for star-forming and composite ETGs. The black dashed line and solid curves are the secondary and primary+secondary relations in nitrogen production. The blue and red dots are the same as in Figure 1.
Paper: Comparison of Composite and Star-forming Early-type Galaxies
Authors: Yu-Zhong Wu
Figure caption: Comparison of the stellar mass and SFR relations for star-forming ETGs and composite ETGs. The black dashed line represents the best fit of Renzini & Peng (2015). The magenta long-dashed line shows the polynomial fit of all star-forming and composite galaxies (93,089 SFGs and 29,643 composite galaxies). Our result (the magenta line) is consistent with the finding of McPartland et al. (2019). The blue solid and red dotted–dashed lines are the fits for star-forming and composite ETGs, respectively (see the text).
Paper: Comparison of Composite and Star-forming Early-type Galaxies
Authors: Yu-Zhong Wu
Figure caption: Comparison of relations of 12+log(O/H) and log(N/O) for star-forming ETGs (left-hand panel) and composite ETGs (right-hand panel) using the color bar of D  n 4000. The black dashed line and solid curves are the same as in Figure 8.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: Central pointing view of M33 galaxy (U band; from Massey et al. 2006) showing 154 of the 163 star clusters from Sarajedini & Mancone (2007) analyzed in this work. The remaining nine clusters are located in the Northern and Southern pointings, and are not shown here. A scale of ﹩{6}^{{\prime} }﹩ correspond to ∼1.5 kpc at the distance of this galaxy. Cyan circles mark clusters for which SED fits were performed, while red circles mark clusters excluded from the fits, and for which only photometry is provided. See text for more details.
Paper: Comparison of Composite and Star-forming Early-type Galaxies
Authors: Yu-Zhong Wu
Figure caption: WHAN diagram. The boundary between AGNs and SFGs on the BPT diagram (Stasińska et al. 2006) is displayed by the vertical magenta dashed line at log [N II]/Hα = −0.10 (Belfiore et al. 2015). The division between sAGNs and wAGNs is shown with the horizontal magenta dashed line at EWHα  = 6Å (Cid Fernandes et al. 2011). RGs lie below the horizontal magenta dashed line at EWHα  < 3Å. The blue and red dots are the same as in Figure 1.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: Five example SEDs of star clusters with <10 Myr. Beginning at the top plot, the clusters shown are 42, 70, 77, 79, and 111. The best-fit extinction, age, mass of each cluster are listed at the top of each panel, with the age and masses in logarithmic scale. Units are: mag for E(B–V), yr for ages and M ⊙ for masses.
Paper: Comparison of Composite and Star-forming Early-type Galaxies
Authors: Yu-Zhong Wu
Figure caption: Comparison of sSFR and 12+log(O/H) relations for star-forming and composite ETGs. The blue and red dots are the same as in Figure 1.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: Five example SEDs of star clusters in the age range 10–100 Myr. Beginning at the top plot, the clusters shown are 22, 33, 52, 61, and 134. See caption of Figure 2 for more details.
Paper: Thermal Phase Curves of XO-3b: An Eccentric Hot Jupiter at the Deuterium Burning Limit
Authors: Lisa Dang, Taylor J. Bell, Nicolas B. Cowan, Daniel Thorngren, Tiffany Kataria, Heather A. Knutson, Nikole K. Lewis, Keivan G. Stassun, Jonathan J. Fortney, Eric Agol, Gregory P. Laughlin, Adam Burrows, Karen A. Collins, Drake Deming, Diana Jovmir, Jonathan Langton, Sara Rastegar, Adam P. Showman
Figure caption: Theoretical planet radius vs. age for XO-3b with typical heating (blue) and with additional heating (red) compared to XO-3b’s observed radius. The shaded swaths represent model uncertainties, dominated by the compositional uncertainties.
Paper: Assessing the Transiting Exoplanet Survey Satellite’s Yield of Rocky Planets Around Nearby M Dwarfs
Authors: Madison T. Brady, Jacob L. Bean
Figure caption: The distribution of rocky planets around M dwarfs as a function of stellar radius. The histogram plots the observed planets from the TESS Prime Mission (Guerrero et al. 2021) in black, and the gold points are the results from the provided Barclay et al. (2018) simulation. The plotted sample only includes planets around M dwarfs within 30 pc, R  p  < 2R ⊕, and P < 13.5 days (which corresponds to the length of half a single TESS sector).
Paper: Assessing the Transiting Exoplanet Survey Satellite’s Yield of Rocky Planets Around Nearby M Dwarfs
Authors: Madison T. Brady, Jacob L. Bean
Figure caption: Additional noise, σ  A , as a function of stellar radius. σ  A  is calculated by comparing the 1 hr CDPP noise determined directly from light curves using lightkurve to the noise calculated with ticgen. The best-fit power-law model is included in gold. A step model with a cutoff at 0.36 R ⊙ (corresponding to where we expect M dwarfs to transition into a fully convective regime) is included in blue.
Paper: Assessing the Transiting Exoplanet Survey Satellite’s Yield of Rocky Planets Around Nearby M Dwarfs
Authors: Madison T. Brady, Jacob L. Bean
Figure caption: Top: the three forms (uniform, power law, Gaussian) of the occurrence model, λ, as a function of stellar radius when σ  A  = 0. Bottom: the number of simulated planetary detections (with errors) around nearby M dwarfs with the three different planet occurrence models, colored to reflect the models shown in the top portion of the figure. The power-law model was tuned by-eye to match the observed number of planets around large M dwarfs, and the Gaussian model was tuned to roughly match the center, width, and height of the observed distribution. A histogram of the observed planets from sectors 1–43 is included for comparison.
Paper: Assessing the Transiting Exoplanet Survey Satellite’s Yield of Rocky Planets Around Nearby M Dwarfs
Authors: Madison T. Brady, Jacob L. Bean
Figure caption: Top: the three forms (uniform, step, and power law) of the additional noise term, σ  A , as a function of stellar radius. Bottom: the number of simulated planetary detections (with errors) around nearby M dwarfs with the given noise models, colored to reflect the models shown in the top panel of the figure. The step and power-law noise models are informed by fits to σ  A , described in Section 2.2.3. A histogram of the observed TESS planets from sectors 1–43 is included for comparison.
Paper: Confirmation of Water Absorption in the Thermal Emission Spectrum of the Hot Jupiter WASP-77Ab with HST/WFC3
Authors: Megan Mansfield, Lindsey Wiser, Kevin B. Stevenson, Peter Smith, Michael R. Line, Jacob L. Bean, Jonathan J. Fortney, Vivien Parmentier, Eliza M.-R. Kempton, Jacob Arcangeli, Jean-Michel Désert, Brian Kilpatrick, Laura Kreidberg, Matej Malik
Figure caption: Left: emission spectrum fits using the 1D free retrieval described in Section 3.1, and the Sc-CHIMERA 1D model grid described in Section 3.2. Dark lines represent the median fit, and dark and light shading show 1 and 2σ regions, respectively. Black points show the observations. The inset shows a zoomed in view of the WFC3 segment of the spectrum. The models generally fit the data well, with the best-fit models having reduced chi squared of ﹩{\chi }_{\nu }^{2}=1.12﹩ for the free retrieval and 1.24 for the grid fit. Right: corresponding pressure-temperature profiles. Grid profiles within 1 and 2σ are shown by dark and light purple lines, respectively. 1 and 2σ regions for the free retrieval are shaded in dark and light yellow, respectively. Contribution functions are also plotted for each Spitzer point, and for in (1.35–1.48 μm) and out (1.55–1.7 μm) of the water feature in the WFC3 wavelength range.
Paper: Confirmation of Water Absorption in the Thermal Emission Spectrum of the Hot Jupiter WASP-77Ab with HST/WFC3
Authors: Megan Mansfield, Lindsey Wiser, Kevin B. Stevenson, Peter Smith, Michael R. Line, Jacob L. Bean, Jonathan J. Fortney, Vivien Parmentier, Eliza M.-R. Kempton, Jacob Arcangeli, Jean-Michel Désert, Brian Kilpatrick, Laura Kreidberg, Matej Malik
Figure caption: Posterior distributions of free parameters in the 1D Sc-CHIMERA model grid fit for the fit to the full data set (blue) and the fit to the data with the bluest 4 points removed (red). For the full data set, 2D histograms for pairs of parameters are shown in off-diagonal plots with 1, 2, and 3σ regions shaded in light, medium, and dark blue, respectively. Histograms on the diagonal show 1D posterior probability distributions for each individual parameter.
Paper: Confirmation of Water Absorption in the Thermal Emission Spectrum of the Hot Jupiter WASP-77Ab with HST/WFC3
Authors: Megan Mansfield, Lindsey Wiser, Kevin B. Stevenson, Peter Smith, Michael R. Line, Jacob L. Bean, Jonathan J. Fortney, Vivien Parmentier, Eliza M.-R. Kempton, Jacob Arcangeli, Jean-Michel Désert, Brian Kilpatrick, Laura Kreidberg, Matej Malik
Figure caption: Posterior distributions of all parameters in the free retrieval (Section 3.1). Off-diagonal plots show 2D posterior probabilities for pairs of parameters, with 1, 2, and 3σ intervals indicated in dark, medium, and light blue. Panels on the diagonal show 1D posterior probability distributions for each parameter. The free parameters include volume mixing ratios of H2O and CO, 6 parameters for the analytic T–P profile, and a scale factor.
Paper: Confirmation of Water Absorption in the Thermal Emission Spectrum of the Hot Jupiter WASP-77Ab with HST/WFC3
Authors: Megan Mansfield, Lindsey Wiser, Kevin B. Stevenson, Peter Smith, Michael R. Line, Jacob L. Bean, Jonathan J. Fortney, Vivien Parmentier, Eliza M.-R. Kempton, Jacob Arcangeli, Jean-Michel Désert, Brian Kilpatrick, Laura Kreidberg, Matej Malik
Figure caption: Example stellar spectrum extracted from one spatially scanned exposure taken by HST/WFC3. Black and red lines indicate the extracted flux before and after correcting for the flux of the companion star, WASP-77B, respectively. The spectrum of WASP-77B appears redder in wavelength than that of WASP-77A because its spectral trace was slightly offset in the spectral direction on the detector. Vertical gray lines indicate the extent of the bins for the spectroscopic light curve.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: The flux ratio 24 μm/FUV plotted against flux density ratio FUV–NUV. The y axis is the logarithm of the ratio of the two fluxes at 24 μm and FUV, expressed as F = λ f(λ) in units of erg cm−2 s−1. The x axis is the logarithm of the ratio of the flux densities in the FUV and NUV, in units of erg/cm2/Å. The 24 μm/FUV ratio gives a measure of the dust extinction affecting the FUV emission (Meurer et al. 1999). This correlation has been previously observed for galaxies and H II regions, and is extended here to clusters. The model line, in red, is from Calzetti et al. (2005). Most of the clusters in M33 are consistent with low-to-negligible dust attenuation. The large scatter in the FUV–NUV colors at constant 24 μm/FUV value are due to the age differences in the stellar populations of the clusters, with redder colors for older populations.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: Cluster 58 is an examples of a <10 Myr cluster. Its best-fit values are: age = 2 Myr, mass = 890 M ⊙, and E(B–V) = 0.32 mag. The eight-band photometry with the best-fit SED model (as a blue line) are shown in the left panel. The four small panels to the right show for the cluster, beginning at the top left and moving clockwise: the Hα emission, the continuum-subtracted Hα emission, an RGB color composite (red = R band, green = Hα band, and blue = U band), and the stellar-subtracted 24 μm emission. The magenta circle shows the size of the aperture used for the photometric measurements. The scale bar below the aperture represents 3”. The flux scale of the images is linear; however, the upper and lower limits differ between bands.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: The masses (left panel) and color excesses E(B–V) (right panel) as a function age for the 137 star clusters in M33 derived via our SED fits. The red line in the left panel shows the luminosity limit of the sample.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: Five example SEDs of star clusters with >100 Myr age. Beginning at the top plot, the clusters shown are 24, 48, 80, 105, and 137. See caption of Figure 2 for more details.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: Cluster 103 is an example of a <10 Myr cluster with a large Hα envelope, which extends outside of the photometric aperture. Some of the Hα emission is missed in the photometric measurements because of this, which explains some of the weakness of the Hα emission in the SED. This cluster has best-fit age = 8 Myr, mass = 2600 M ⊙ and E(B–V) = 0.0 mag. The panels, symbols, lines, and flux scales are the same as in Figure 5.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: Cluster 124 is an example of a >100 Myr cluster. Its best-fit values are: age = 300 Myr, mass = 11,000 M ⊙, and E(B–V) = 0.1 mag. The panels, symbols, lines, and flux scales are the same as in Figure 5.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: Comparison of our SED-fit masses with those of the SM2007 catalog. The one-to-one line is shown in red.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: Comparison of our SED-fit ages with those of the SM2007 catalog.
Paper: Ages and Masses of Star Clusters in M33: a Multiwavelength Study
Authors: Caitlin Moeller, Daniela Calzetti
Figure caption: Cluster 118 is an example of a cluster with age between 10 and 100 Myr. Its best-fit values are: age = 40 Myr, mass = 11,000 M ⊙, and E(B–V) = 0.02 mag. The panels, symbols, lines, and flux scales are the same as in Figure 5.
Paper: The Shellless Supernova Remnant B0532–67.5 in the Large Magellanic Cloud
Authors: Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Chen-Yu Chuang, 鎮宇 莊, Guan-Hong Li, 冠宏 李
Figure caption: Hα image of SNR B0532−67.5 showing the star field. A small dashed circle with a radius of 1.′5 (or 22.5 pc) is drawn around the OB association LH75. A large dashed circle with a radius of 3′ (or 45 pc) is drawn around the SNR and encompasses the star field analyzed. The center of the SNR is marked by “+.” Within this field stars with V < 17 mag are marked with blue circles and used to construct the CMDs. Candidates for the most massive stars are marked with red circles and labeled from A to R. The numbers in parentheses above the labels are their estimated masses in units of M ⊙. Stars that are multiple or confused have larger uncertainties in their masses, and they are marked with double parentheses.
Paper: The Shellless Supernova Remnant B0532–67.5 in the Large Magellanic Cloud
Authors: Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Chen-Yu Chuang, 鎮宇 莊, Guan-Hong Li, 冠宏 李
Figure caption: Multiwavelength images of SNR B0532−67.5. The origin of each image is marked in the upper right corner. The top row presents ASKAP 888 MHz continuum images, and the second row XMM-Newton X-ray images in the full energy band (0.1–15 keV). The bottom four images are CTIO 4 m MOSAIC Hα, MCELS Hα, [O III], and [N II] images. To facilitate comparisons, the contours of the ASKAP 888 MHz radio continuum image (left panel of the top row) are overplotted on the XMM unsmoothed X-ray image and the MCELS Hα image, and the contours of the XMM smoothed X-ray image are overplotted on the ASKAP 888 MHz image (right panel of the top row).
Paper: The Shellless Supernova Remnant B0532–67.5 in the Large Magellanic Cloud
Authors: Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Chen-Yu Chuang, 鎮宇 莊, Guan-Hong Li, 冠宏 李
Figure caption: Left: V vs. BV CMD of stars with V < 17 mag projected in and around SNR B0532−67.5. The MCPS photometric data (Zaritsky et al. 2004) are used. The evolutionary tracks of stars for Z = 0.008 from Lejeune & Schaerer (2001) are reddened by E(B − V) = 0.08 and plotted. The most massive star candidates are marked from A to R both in the CMDs and in the image in Figure 2. Right: close-up V vs. BV CMD near the main sequence of the evolutionary tracks.
Paper: The Shellless Supernova Remnant B0532–67.5 in the Large Magellanic Cloud
Authors: Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Chen-Yu Chuang, 鎮宇 莊, Guan-Hong Li, 冠宏 李
Figure caption: (a) ASKAP radio 888 MHz continuum image of B0532−67.5 with contours at levels of 0.40, 1.55, 2.70, 3.85, and 5.00 mJy beam−1. Three additional contour levels of 6.00, 17.0, and 28.0 mJy beam−1 are plotted for the bright compact source. The unit of the color bar is mJy beam−1. (b) A close-up of Figure 5(a) centered at SNR B0532−67.5. A log scale is used in this image, and the unit of the color bar is Jy beam−1 km s−1. The radio contours are the same as those in panel (a).
Paper: The Shellless Supernova Remnant B0532–67.5 in the Large Magellanic Cloud
Authors: Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Chen-Yu Chuang, 鎮宇 莊, Guan-Hong Li, 冠宏 李
Figure caption: (a) ATCA/Parkes H I moment 0 map (color) integrated over a velocity range of V LSR = 243–348 km s−1, superposed with contours extracted from the ASKAP 888 MHz radio continuum image (AS033) at levels of 0.40, 1.55, 2.70, 3.85, and 5.00 mJy beam−1. The unit of the color bar is Jy beam−1 km s−1. (b) H I position–velocity diagram along the red line marked in (a). A log scale is used in the image, and the unit of the color bar is Jy beam−1. The red dots denote the peak positions of each Gaussian component in the multicomponent Gaussian fitting.
Paper: The Shellless Supernova Remnant B0532–67.5 in the Large Magellanic Cloud
Authors: Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Chen-Yu Chuang, 鎮宇 莊, Guan-Hong Li, 冠宏 李
Figure caption: (a) The 4 m MOSAIC Hα image of B0532−67.5 marked with the CTIO echelle slit position. (b) Hα and [N II] echellograms of the slit position marked in (a). The slit orientation is marked in the upper left corner. Note that the lack of signal at the top and bottom ends of the slit is caused by vignetting in the optics of the echelle spectrograph.
Paper: The Shellless Supernova Remnant B0532–67.5 in the Large Magellanic Cloud
Authors: Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Chen-Yu Chuang, 鎮宇 莊, Guan-Hong Li, 冠宏 李
Figure caption: (a) ASKAP 888 MHz continuum degree of polarization (color), polarized emission (green contour), and polarized vector (black vector). The contour levels are 1.5σ, 2.5σ, and 3.5σ, where 1σ corresponds to 0.14 mJy beam−1. The vector length denotes the degree of polarization and the blue filled ellipse at the bottom left corner denotes the beam size, 35″ × 35″. (b) ASKAP 888 MHz continuum Stoke I emission (color), polarized emission (green contour), and polarized vector rotated by 90° (black vector). The contour levels, vector length, and the beam size are the same as those in panel (a).