adsabs/AstroCLIMB huggingface dataset:
Paper: Wide Separation Planets in Time (WISPIT): Discovery of a Gap Hα Protoplanet WISPIT 2b with MagAO-X
Authors: Laird M. Close, Richelle F. van Capelleveen, Gabriel Weible, Kevin Wagner, Sebastiaan Y. Haffert, Jared R. Males, Ilya Ilyin, Matthew A. Kenworthy, Jialin Li, Joseph D. Long, Steve Ertel, Christian Ginski, Alycia J. Weinberger, Kate Follette, Joshua Liberman, Katie Twitchell, Parker Johnson, Jay Kueny, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Avalon McLeod, Eden McEwen, Logan Pearce, Lauren Schatz, Alexander D. Hedglen, Ya-Lin Wu, Jacob Isbell, Jenny Power, Jared Carlson, Emmeline Close, Elena Tonucci, Matthijs Mars
Figure caption: Here, we zoom in on the inner 1162 × 694 mas to examine the position of the close companion (CC1) at different wavelengths. The z′ image is same as in Figure 1, but shown here is with movement = 0. The cADI Ks image is from SPHERE/IRDIS; see Letter 1 for details. The L′ image is the same as in Figure 2, but with increased smoothing. This very red (z′–L′ ∼ 4.6 mag) CC 1 source has an SNR = 4.3 in the z′ image and SNR = 12.1 in the L′ image. There is little difference between the z′ – L′ positions (Δsep = −3 ± 14 mas and ΔPA = 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩1 ± 3﹩\mathop{.}\limits^{\unicode{x000b0}}﹩0), so they are consistent with being cospatial. The Ks source is partially blocked by the diffracted edge of the SPHERE r = 93 mas coronagraph (dark circle), yet is spatially consistent with the z′ and L′ sources within errors. CC1 is a point source at L′ but appears slightly extended at z′ and Ks. CC1 is not significantly detected in the Hα image (SNR < 2). The CC1 green ellipse is in the same location (110 mas; 192o) in each image. The ellipses trace r = 41 mas (5 au) circles with i = 44o (same as main disk). There is an r = 83 mas semitransparent circle centered exactly on the star. It is unclear if CC1 is a warm inner protoplanet (mass ∼9 Mjup) or an unusually red compact dust clump. If it is a planet, it could appear modesty extended due to its dusty CPD’s edge scattering starlight (no z′ scattering occurs at 2b due to the shadow cast by ring #3). Scaling from the observed size (∼1 Hill sphere) of the PDS 70 b and c CPDs of L. M. Close et al. (2025), we predict CC1’s CPD would appear elongated by r ∼ 2.7 au. The observed size of CC1 at z′ is the PSF convolved with the CPD, yielding a CPD radius of ∼24 mas at z′. Hence, CC1’s CPD’s edge should trace ∼60% inside of the green CC1 ellipse, roughly consistent with the elongation observed in z′.
Paper: Wide Separation Planets in Time (WISPIT): Discovery of a Gap Hα Protoplanet WISPIT 2b with MagAO-X
Authors: Laird M. Close, Richelle F. van Capelleveen, Gabriel Weible, Kevin Wagner, Sebastiaan Y. Haffert, Jared R. Males, Ilya Ilyin, Matthew A. Kenworthy, Jialin Li, Joseph D. Long, Steve Ertel, Christian Ginski, Alycia J. Weinberger, Kate Follette, Joshua Liberman, Katie Twitchell, Parker Johnson, Jay Kueny, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Avalon McLeod, Eden McEwen, Logan Pearce, Lauren Schatz, Alexander D. Hedglen, Ya-Lin Wu, Jacob Isbell, Jenny Power, Jared Carlson, Emmeline Close, Elena Tonucci, Matthijs Mars
Figure caption: Here, we plot predicted planet locations for all 33 known ALMA disks that have an inner cavity or a wide gap >30 au. We use the MAG model (L. M. Close 2020) to predict the average time integrated projected separation of the massive planets that could be responsible for clearing the large gaps in all 33 of these systems. The small blue dots are the predicted locations of the outer (a2) planet from the size of the cavity (Rcav) of each ALMA disk. The small blue “+” symbols are the predicted locations of the inner planets (a1) in 2:1 MMR with the outer planet in the cavity (L. M. Close 2020). The large blue dots are the predicted positions of the annular gap clearing planets. WISPIT 2b is the first and only known accreting Hα annular gap planet; however, the plot also shows the inclinations of the many other ring gaps (large blue dots). Note how there are, to date, only Hα planets (red diamonds) found in the zone: 37≤i≤52o. Despite the abundance of excellent targets (any blue symbol above the green dashed line at 115 mas is considered a “detectable” Hα planet, but only those with red diamonds are actually detected), there are no Hα planets detected with inclinations <37° (pole-on systems). Nor are any found with inclinations >55°. All known protoplanets are plotted as light dots with vertical lines (these vertical error bars denote the estimated angle between the time averaged positions of the MAG model and a pole-on orbit). The red light dots are all of the known Hα protoplanets, and the blue ones are known NIR planets that seem to have no direct Hα emission.
Paper: Wide Separation Planets in Time (WISPIT): Discovery of a Gap Hα Protoplanet WISPIT 2b with MagAO-X
Authors: Laird M. Close, Richelle F. van Capelleveen, Gabriel Weible, Kevin Wagner, Sebastiaan Y. Haffert, Jared R. Males, Ilya Ilyin, Matthew A. Kenworthy, Jialin Li, Joseph D. Long, Steve Ertel, Christian Ginski, Alycia J. Weinberger, Kate Follette, Joshua Liberman, Katie Twitchell, Parker Johnson, Jay Kueny, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Avalon McLeod, Eden McEwen, Logan Pearce, Lauren Schatz, Alexander D. Hedglen, Ya-Lin Wu, Jacob Isbell, Jenny Power, Jared Carlson, Emmeline Close, Elena Tonucci, Matthijs Mars
Figure caption: The calculated Hα line fluxes of all known Hα protoplanets, assuming no extinction (AR = Ap = 0 mag). They have been normalized to 113 pc (the distance to PDS 70). This covers 8 yr of observations and covers all known Hα observations from the literature. We include rotated and scaled thumbnail insets in scattered light of each of the systems with well-known Hα protoplanets. The green circles each represent the location of the Hα planet in that system. While the sample to date is very small, notice how all of these systems have similar inclinations. Note how the full day side of these protoplanets is never seen. Inset disk images: MaXProtoPlanetS 1’s disk in polarized scattered light from C. Ginski et al. (2025); PDS 70’s disk in polarized light from Z. Wahhaj et al. (2024); and WISPIT 2’s disk in z′ from this work. Inclinations fit to the Atacama Large Millimeter/submillimeter Array (ALMA) continuum disk images are called out in yellow text on insets.
Paper: Wide Separation Planets in Time (WISPIT): Discovery of a Gap Hα Protoplanet WISPIT 2b with MagAO-X
Authors: Laird M. Close, Richelle F. van Capelleveen, Gabriel Weible, Kevin Wagner, Sebastiaan Y. Haffert, Jared R. Males, Ilya Ilyin, Matthew A. Kenworthy, Jialin Li, Joseph D. Long, Steve Ertel, Christian Ginski, Alycia J. Weinberger, Kate Follette, Joshua Liberman, Katie Twitchell, Parker Johnson, Jay Kueny, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Avalon McLeod, Eden McEwen, Logan Pearce, Lauren Schatz, Alexander D. Hedglen, Ya-Lin Wu, Jacob Isbell, Jenny Power, Jared Carlson, Emmeline Close, Elena Tonucci, Matthijs Mars
Figure caption: The KLIP reduced L′ image from the LBT telescope with the LBTI LMIRcam instrument. The location of WISPIT 2b and the inner #3 and outer #2 dust rings are clear (despite the significant self-subtraction from KLIP). WISPIT 2b is located nearly in the center of the dust-free gap between the rings. The image is 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩43 × 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩43; see Appendix B for details about the L′ reduction.
Paper: Wide Separation Planets in Time (WISPIT): Discovery of a Gap Hα Protoplanet WISPIT 2b with MagAO-X
Authors: Laird M. Close, Richelle F. van Capelleveen, Gabriel Weible, Kevin Wagner, Sebastiaan Y. Haffert, Jared R. Males, Ilya Ilyin, Matthew A. Kenworthy, Jialin Li, Joseph D. Long, Steve Ertel, Christian Ginski, Alycia J. Weinberger, Kate Follette, Joshua Liberman, Katie Twitchell, Parker Johnson, Jay Kueny, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Avalon McLeod, Eden McEwen, Logan Pearce, Lauren Schatz, Alexander D. Hedglen, Ya-Lin Wu, Jacob Isbell, Jenny Power, Jared Carlson, Emmeline Close, Elena Tonucci, Matthijs Mars
Figure caption: A simple cartoon to show how the Hα line formation zone from magnetospheric accretion could be best viewed by looking straight down the magnetic field lines (G.-D. Marleau et al. 2022). In other words, an observer would have the most direct line of sight to the Hα line formation zone if the ALMA disk and its coplanar planet were both inclined at the line of latitude of where the magnetic field lines (drawn here fixed at 45o). Here, we show a toy model where the heating in the Zel’dovich shock temperature spike (ΔTshock) would reasonably drive strong convection in the dusty atmosphere of the planet. The buoyancy from such a ΔTshock would not be dissimilar to that of the Shoemaker–Levy 9 impactors on Jupiter and lead to the quasi-static ∼5% Rp dusty cloud deck heights shown here.
Paper: Wide Separation Planets in Time (WISPIT): Discovery of a Gap Hα Protoplanet WISPIT 2b with MagAO-X
Authors: Laird M. Close, Richelle F. van Capelleveen, Gabriel Weible, Kevin Wagner, Sebastiaan Y. Haffert, Jared R. Males, Ilya Ilyin, Matthew A. Kenworthy, Jialin Li, Joseph D. Long, Steve Ertel, Christian Ginski, Alycia J. Weinberger, Kate Follette, Joshua Liberman, Katie Twitchell, Parker Johnson, Jay Kueny, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Avalon McLeod, Eden McEwen, Logan Pearce, Lauren Schatz, Alexander D. Hedglen, Ya-Lin Wu, Jacob Isbell, Jenny Power, Jared Carlson, Emmeline Close, Elena Tonucci, Matthijs Mars
Figure caption: Similar to Figure 3 except now we plot the estimated mass accretion rates onto these planets (assuming no extinction). As can be seen, these are all currently accreting weakly (<4 × 10−12 MSun yr−1 or <0.004 Mjup Myr−1). This, in turn, suggests that the Hα self-absorption by the infalling gas should be weak, and so our assumption of there being no absorption/extinction of the Hα is reasonable according to the models of G.-D. Marleau et al. (2022). We see that WISPIT 2b has a similar mass accretion rate to all of the other protoplanets. For clarity, some of the data points have been slightly shifted in time.
Paper: Hidden Activity Revealed: Photospheric Energetics and Dynamics with High-resolution Magnetographic Data
Authors: Manolis K. Georgoulis, Qin Li, Jeongwoo Lee, Haimin Wang, Nour E. Raouafi
Figure caption: Magnetic flux per polarity (top row) and potential magnetic energy of the entire FOV (middle row) and its variations (bottom row) for the GST/NIRIS magnetograms (column (a)) and SDO/HMI magnetograms (column (b)) over the interval of interest. The straight line in the NIRIS data between approximately 95 and 115 minutes is due to the 19 minute data gap mentioned in Section 3. In the middle and bottom rows, all values of energy and energy variations, respectively, include applicable uncertainties (red error bars calculated as in the Appendix). Error bars in the potential energy variations (bottom row) are calculated by propagating nearest-neighbor potential energy uncertainties from the middle row.
Paper: Hidden Activity Revealed: Photospheric Energetics and Dynamics with High-resolution Magnetographic Data
Authors: Manolis K. Georgoulis, Qin Li, Jeongwoo Lee, Haimin Wang, Nour E. Raouafi
Figure caption: The target of our analysis, in full-disk observations ((a) and (b)) and in local LOS magnetogram observations from (c) GST/NIRIS and (d) SDO/HMI. Full-disk observations show (a) the LOS HMI magnetogram and (b) an AIA image at the 171 Å EUV channel. Both NIRIS and HMI images are taken around 2018 July 29T16:49. Full-disk images further include the potential field source surface magnetic field lines to show that our target location (enclosed by a small rectangle and indicated by arrows in both images) corresponds to a small coronal hole (source: HelioViewer). The coaligned NIRIS and HMI magnetogram images are saturated at ±200 G.
Paper: Wide Separation Planets in Time (WISPIT): Discovery of a Gap Hα Protoplanet WISPIT 2b with MagAO-X
Authors: Laird M. Close, Richelle F. van Capelleveen, Gabriel Weible, Kevin Wagner, Sebastiaan Y. Haffert, Jared R. Males, Ilya Ilyin, Matthew A. Kenworthy, Jialin Li, Joseph D. Long, Steve Ertel, Christian Ginski, Alycia J. Weinberger, Kate Follette, Joshua Liberman, Katie Twitchell, Parker Johnson, Jay Kueny, Daniel Apai, Rene Doyon, Warren Foster, Victor Gasho, Kyle Van Gorkom, Olivier Guyon, Maggie Y. Kautz, Avalon McLeod, Eden McEwen, Logan Pearce, Lauren Schatz, Alexander D. Hedglen, Ya-Lin Wu, Jacob Isbell, Jenny Power, Jared Carlson, Emmeline Close, Elena Tonucci, Matthijs Mars
Figure caption: The discovery images of WISPIT 2b. These are both the 2025 April MagAO-X Hα pyKLIP pipeline reduced data sets. The thick central green circles (r = 103 mas) are centered on the star. The lighter-green circles (r = 89 mas) all have identical centers at WISPIT 2b (star–planet separation = 309.43 mas, PA = 242﹩\mathop{.}\limits^{\unicode{x000b0}}﹩2). In the discovery image, WISPIT 2b is detected in the ASDI image at a signal-to-noise ratio (SNR) = 5.5 (top right), on April 16 it was recovered at SNR = 12.5 (bottom right). The dashed yellow line in the Hα image traces the second-brightest ring (visible at z′; called ring #2; the brightest inner ring is ring #3; see Letter 1 for ring images and names). All images have the first 5 principal component (PC) modes removed by pyKLIP with movement set to zero. Images are 1518 × 1388 mas, smoothed by an FWHM = 17 mas Gaussian (except the z′ image, which has a 29 mas smoothing and pyKLIP movement = 5, and a deeper stretch). North is up, and east is left in these, and all following, images.
Paper: The Kinematic Age of 3I/ATLAS and Its Implications for Early Planet Formation
Authors: Aster G. Taylor, Darryl Z. Seligman
Figure caption: Interstellar Object Metallicity. The PDF p([Fe/H]) for the interstellar objects as a function of the metallicity. The median is shown as a dashed line, and the 68% confidence region is shaded.
Paper: The Kinematic Age of 3I/ATLAS and Its Implications for Early Planet Formation
Authors: Aster G. Taylor, Darryl Z. Seligman
Figure caption: Interstellar Object Age. The posterior probability distribution function p(τ∣{v}i) for the three known interstellar objects, where {v} represents the set of measured interstellar object velocities. We show the age distribution as well as the median (dashed line) and the 68% confidence region (shaded).
Paper: Unveiling a Population of Strong Galaxy–Galaxy Lensed, Faint Dusty Star-forming Galaxies
Authors: Ting-Kai Yang, Chian-Chou Chen, Zhen-Kai Gao, Bovornpratch Vijarnwannaluk, Adarsh Ranjan, Wei-Hao Wang, Caitlin M. Casey, Tomotsugu Goto, Jeyhan S. Kartaltepe, Chayan Mondal, James Pearson, Chris Sedgwick, Stephen Serjeant
Figure caption: Galaxy cumulative number counts at 450–500 μm. The orange curve represents the unlensed model obtained from Z.-Y. Cai et al. (2013). The lensed model from M. Negrello et al. (2017) and C. Sedgwick et al. (2025) are shown in the blue solid and dashed–dotted lines, respectively. The blue filled data points represent the results of this work. The STUDIES sample results, derived from the effective area and corrected for spurious detections and completeness, are shown as blue triangles. For the flux- and color-selected DSFGs, we derived the stacked submillimeter flux and present the results as a lower limit due to the likely incompleteness, shown as a blue filled circle. The strongly lensed DSFGs identified in J. L. Wardlow et al. (2013), M. Negrello et al. (2017), B. A. Ward et al. (2022), and T. J. L. C. Bakx et al. (2024) are shown as blue diamonds. Red data points show the number density of unlensed DSFGs from C. M. Casey et al. (2013), C.-C. Chen et al. (2013), J. A. Zavala et al. (2017), Z.-K. Gao et al. (2024), and Q.-N. Hsu et al. (2024).
Paper: Unveiling a Population of Strong Galaxy–Galaxy Lensed, Faint Dusty Star-forming Galaxies
Authors: Ting-Kai Yang, Chian-Chou Chen, Zhen-Kai Gao, Bovornpratch Vijarnwannaluk, Adarsh Ranjan, Wei-Hao Wang, Caitlin M. Casey, Tomotsugu Goto, Jeyhan S. Kartaltepe, Chayan Mondal, James Pearson, Chris Sedgwick, Stephen Serjeant
Figure caption: Cutout images and the photo-z analysis for all 18 candidates, following the style of Figure 2. For STUDIES sources, the solid contours are either ALMA or VLA, with contour levels starting from 3 with steps of 2σ. The dashed contours are MIPS emissions, linearly spaced from 80% to 100% of the peak flux.
Paper: Unveiling a Population of Strong Galaxy–Galaxy Lensed, Faint Dusty Star-forming Galaxies
Authors: Ting-Kai Yang, Chian-Chou Chen, Zhen-Kai Gao, Bovornpratch Vijarnwannaluk, Adarsh Ranjan, Wei-Hao Wang, Caitlin M. Casey, Tomotsugu Goto, Jeyhan S. Kartaltepe, Chayan Mondal, James Pearson, Chris Sedgwick, Stephen Serjeant
Figure caption: Cutout images and the photo-z analysis for all 18 candidates, following the style of Figure 2.
Paper: Unveiling a Population of Strong Galaxy–Galaxy Lensed, Faint Dusty Star-forming Galaxies
Authors: Ting-Kai Yang, Chian-Chou Chen, Zhen-Kai Gao, Bovornpratch Vijarnwannaluk, Adarsh Ranjan, Wei-Hao Wang, Caitlin M. Casey, Tomotsugu Goto, Jeyhan S. Kartaltepe, Chayan Mondal, James Pearson, Chris Sedgwick, Stephen Serjeant
Figure caption: Results of the lensing modeling for all 18 candidates, following the style of Figure 3.
Paper: The Fraction of Distilled White Dwarfs with Long-lived Habitable Zones
Authors: Manuel Barrientos, Mukremin Kilic, Simon Blouin, Michael R. Hayden, Sanjib Sharma, Matthew J. Green
Figure caption: Top: predicted 22Ne mass fraction as a function of metallicity for the WD remnants of stars in the Hypatia Catalog (N. R. Hinkel et al. 2014). The colors represent [N/H] for the same stars. Middle and bottom: C and N abundances of the same stars from the Hypatia Catalog. The color bars represent the predicted neon mass fraction, X(22Ne), in their remnants. Two chemically peculiar low-metallicity objects, BD+80 245 and HD 19445, are labeled and marked as stars.
Paper: The Fraction of Distilled White Dwarfs with Long-lived Habitable Zones
Authors: Manuel Barrientos, Mukremin Kilic, Simon Blouin, Michael R. Hayden, Sanjib Sharma, Matthew J. Green
Figure caption: Predicted number of distilled stars (normalized by the total number of stars in our models) as a function of metallicity for various Galactocentric distances. The blue and green bars show the results for stars of all ages and for those stars older than 2 Gyr, respectively. Each panel is labeled by the Galactocentric distance and the distilled fractions for stars of all ages (f1) and older than 2 Gyr (f2).
Paper: The Fraction of Distilled White Dwarfs with Long-lived Habitable Zones
Authors: Manuel Barrientos, Mukremin Kilic, Simon Blouin, Michael R. Hayden, Sanjib Sharma, Matthew J. Green
Figure caption: Age–metallicity relationship for the stars in the Galactic stellar population model of S. Sharma et al. (2021a) for the different radial bins. The points indicate the average [Fe/H] for every 1 Gyr bin. The average metallicity value is relatively flat for ages younger than 8 Gyr in the outer disk (green, red, and purple lines), but it is slightly steeper in the inner Milky Way (blue and orange lines).
Paper: The Fraction of Distilled White Dwarfs with Long-lived Habitable Zones
Authors: Manuel Barrientos, Mukremin Kilic, Simon Blouin, Michael R. Hayden, Sanjib Sharma, Matthew J. Green
Figure caption: Predicted fraction of distilled stars (Nd/Nt) as a function of metallicity for the WD descendants of stars in the Hypatia Catalog (N. R. Hinkel et al. 2014). The metallicity axis is binned by 0.1 dex, and the error bars are calculated using a binomial distribution function. At the highest metallicities observed, up to ∼50% of stars may leave behind a distilled WD.
Paper: X-Ray Investigation of Possible Super-Eddington Accretion in a Radio-loud Quasar at z = 6.13
Authors: Luca Ighina, Alessandro Caccianiga, Thomas Connor, Alberto Moretti, Fabio Pacucci, Cormac Reynolds, José Afonso, Bruno Arsioli, Silvia Belladitta, Jess W. Broderick, Daniele Dallacasa, Roberto Della Ceca, Francesco Haardt, Erini Lambrides, James K. Leung, Alessandro Lupi, Israel Matute, Fabio Rigamonti, Paola Severgnini, Nick Seymour, Fabrizio Tavecchio, Cristian Vignali
Figure caption: Left panel: X-ray luminosity in the 2–10 keV energy band (rest frame) as a function of redshift for the z > 5.5 quasars with X-ray observations from either Chandra or XMM-Newton available in the literature. We highlight the following objects: RACS J0320−35 (red square; this work), HSC J092120.56+000722.9 (pink diamond; J. Wolf et al. 2023), CFHQS J142952+544717 (yellow triangles; G. Migliori et al. 2023; L. Marcotulli et al. 2025), and PSO J030947+271757 (blue pentagons; A. Moretti et al. 2021). Since these last two sources present variable/flaring emission, we show two data points representing the quiescent and the flaring state, respectively. All the other quasars are reported with different colors based on whether they are also detected in the radio band (purple) or not (green). Right panel: rest-frame, multiwavelength SED of RACS J0320−35. The X-ray-weak super-Eddington SED from F. Pacucci & R. Narayan (2024) is shown in magenta. The solid black line is a quasar template (M. Polletta et al. 2007) matched to the optical–UV data points. The dashed black line is the X-ray emission expected from the UV–X-ray relation derived by E. Lusso & G. Risaliti (2016) and assuming ΓX = 2.0. The gray regions show the 1σ and 2σ dispersion of the relation. The vertical yellow region indicates frequencies heavily affected by the absorption of the intergalactic medium.
Paper: X-Ray Investigation of Possible Super-Eddington Accretion in a Radio-loud Quasar at z = 6.13
Authors: Luca Ighina, Alessandro Caccianiga, Thomas Connor, Alberto Moretti, Fabio Pacucci, Cormac Reynolds, José Afonso, Bruno Arsioli, Silvia Belladitta, Jess W. Broderick, Daniele Dallacasa, Roberto Della Ceca, Francesco Haardt, Erini Lambrides, James K. Leung, Alessandro Lupi, Israel Matute, Fabio Rigamonti, Paola Severgnini, Nick Seymour, Fabrizio Tavecchio, Cristian Vignali
Figure caption: Left: radio spectrum of RACS J0320−35 obtained from dedicated observations (uGMRT+ATCA; light red squares and circles) as well as data available from public surveys (dark red pentagons), as described in the text. Measurements from the VAST survey are shown as a single data point at the median value (3.2 mJy beam−1) and the standard deviation (0.5 mJy beam−1) as uncertainty. The best-fit power law is shown as a black dashed line. We also show the measurement and upper limit from the VLBI-LBA observations (yellow diamond); as these observations are of significantly higher angular resolution, they were not used during the fit. Right: X-ray spectra of RACS J0320−35 obtained with Chandra. The best-fit power law with Galactic absorption is shown as a black solid line, while the best-fit power law (ΓX = 1.9, fixed) with an exponential cutoff and Galactic absorption is shown as a gray dashed line. Photon counts have been rebinned to 5σ for plotting purposes only.
Paper: X-Ray Investigation of Possible Super-Eddington Accretion in a Radio-loud Quasar at z = 6.13
Authors: Luca Ighina, Alessandro Caccianiga, Thomas Connor, Alberto Moretti, Fabio Pacucci, Cormac Reynolds, José Afonso, Bruno Arsioli, Silvia Belladitta, Jess W. Broderick, Daniele Dallacasa, Roberto Della Ceca, Francesco Haardt, Erini Lambrides, James K. Leung, Alessandro Lupi, Israel Matute, Fabio Rigamonti, Paola Severgnini, Nick Seymour, Fabrizio Tavecchio, Cristian Vignali
Figure caption: MWA (200 MHz), uGMRT (400 and 650 MHz), and ATCA (2.1, 5.5, and 9 GHz) images centered on the optical position of RACS J0320−35. Contours start at ±3× rms and increase by factors of ﹩\sqrt{2}﹩.