adsabs/AstroCLIMB huggingface dataset:
Paper: Unveiling Central Ortho-H2D+ Depletion at Sub-kau Scales in Prestellar Core G205.46-14.56 M3: The First Interferometric Evidence and Implications for Deuterium Chemistry
Authors: Sheng-Jun Lin, Sheng-Yaun Liu, Dipen Sahu, Laurent Pagani, Tien-Hao Hsieh, Naomi Hirano, Shih-Ping Lai, Tie Liu, Shih-Ying Hsu, Shanghuo Li, Kee-Tae Kim
Figure caption: Comparison of fast and slow-contraction chemodynamical models. (a) H2 number density, ﹩{n}_{{{\rm{H}}}_{2}}﹩. (b) Gas kinetic temperature, Tk (solid), and dust temperature, Td (dashed). (c) Deuteration ratio, x(N2D+)/x(N2H+). (d) Ortho-to-para ratio of H2, OPR(H2). (e) Ortho-to-para ratio of H2D+, OPR(H2D+). Orange and blue curves correspond to snapshots at t = 0.42 Ma (fast) and t = 5.1 Ma (slow), respectively, chosen when both reach a central density of ﹩{n}_{{{\rm{H}}}_{2}}(0)=1.1\times 1{0}^{7}﹩ cm−3. The initial uniform density 5 × 103 cm−3, a 10 K singular isothermal sphere (SIS) reference, the initial Tk = Td = 10 K, and the initial OPR(H2) = 3 are indicated. Boltzmann OPR(H2) and OPR(H2D+) corresponding to the Tk profile are noted. The dotted vertical line marks the outer boundary used in the non-LTE radiative-transfer modeling (7.63 kau).
Paper: Unveiling Central Ortho-H2D+ Depletion at Sub-kau Scales in Prestellar Core G205.46-14.56 M3: The First Interferometric Evidence and Implications for Deuterium Chemistry
Authors: Sheng-Jun Lin, Sheng-Yaun Liu, Dipen Sahu, Laurent Pagani, Tien-Hao Hsieh, Naomi Hirano, Shih-Ping Lai, Tie Liu, Shih-Ying Hsu, Shanghuo Li, Kee-Tae Kim
Figure caption: Spectral observations along the southwest cut compared with the best-fit radiative transfer model. Blue spectra represent observational data, while red spectra show the models. Green dashed lines mark the 3σ noise level. Each row corresponds to a molecular line, with the N2H+ (1–0) line split into three rows for F1-hyperfine groups. Columns represent different offsets from the center of G205 M3 B1, marked by color-coded asterisks in Figure 1. Spectra at gray offsets are excluded from modeling due to nondetections or deviations from spherical geometry. Normalized HFS patterns are shown in red beneath each central spectrum. Black dashed lines indicate the systemic velocity of 10.151 km s−1. For N2H+ (1–0), additional black dashed lines highlight the F1, F = (0, 1–1, 2) and (1, 2–1, 2) components.
Paper: Unveiling Central Ortho-H2D+ Depletion at Sub-kau Scales in Prestellar Core G205.46-14.56 M3: The First Interferometric Evidence and Implications for Deuterium Chemistry
Authors: Sheng-Jun Lin, Sheng-Yaun Liu, Dipen Sahu, Laurent Pagani, Tien-Hao Hsieh, Naomi Hirano, Shih-Ping Lai, Tie Liu, Shih-Ying Hsu, Shanghuo Li, Kee-Tae Kim
Figure caption: Comparison of the ALMA 7 m+12 m combined map and the 7 m-only map of o-H2D+ (110–111). (a) 7 m+12 m combined integrated-intensity map, identical to Figure 1(c). The dashed cyan circle marks the circularized Band 7 beam (0﹩\mathop{.}\limits^{^{\prime\prime} }﹩79) and approximates the FWHD of the depletion zone, while the cyan “×” marks the intensity minimum. (b) 7 m-only integrated-intensity map over the same velocity range as (a), with synthesized beam of ﹩4\mathop{.}\limits^{^{\prime\prime} }30\times 2\mathop{.}\limits^{^{\prime\prime} }72﹩ (P.A. ﹩=81\mathop{.}\limits^{^\circ }7﹩), and the 1σ rms of 27 mJy beam−1 km s−1. To maximize contrast with the color scale, the 3σ o-H2D+ contour is drawn in white, while higher contours are black. Beam sizes, contour levels, and crosses marking B1 and B2 are indicated in each panel. Color images are primary-beam-corrected, whereas contours are drawn from primary-beam-uncorrected images to preserve uniform noise.
Paper: Power Transmission of Whistlers in the Lunar Ionosphere
Authors: Kaiti Wang, Zhan-Rong Hsu, Jacob Bortnik, Ya-Hui Yang
Figure caption: (a) The input altitude profiles of densities for electrons and the 4 ion species (CO2, H2O+, OH+, and H3O+) at a temperature T of 150 K. The surface density of electrons is 250 cm−3. (b) The input altitude profiles of densities for CO2, H2O, and OH molecules at a T of 150 K. (c) The derived altitudinal profiles of effective electron collision frequency and the four ion species are labeled at a T of 150 K. (d) to (f) is the same as (a) to (c), but for temperature T equals 400 K. The surface density of the electron is 80 cm−3.
Paper: Power Transmission of Whistlers in the Lunar Ionosphere
Authors: Kaiti Wang, Zhan-Rong Hsu, Jacob Bortnik, Ya-Hui Yang
Figure caption: Computed transmitted power ratio Pr,0(dB) of whistlers propagating from the surface to 100 km high at different frequencies f0 (denoted in the legends) for different B0 (1 nT, 10 nT, and 100 nT) and different θB-sur at temperature T = 150 K.
Paper: Power Transmission of Whistlers in the Lunar Ionosphere
Authors: Kaiti Wang, Zhan-Rong Hsu, Jacob Bortnik, Ya-Hui Yang
Figure caption: Computed transmitted power ratio Pr,0 (dB) of whistlers from the surface to 100 km high at different frequencies f0 (denoted in the legends) for different B0 (1 nT, 10 nT, and 100 nT) and different θB-sur at temperature T = 400 K.
Paper: Unveiling Central Ortho-H2D+ Depletion at Sub-kau Scales in Prestellar Core G205.46-14.56 M3: The First Interferometric Evidence and Implications for Deuterium Chemistry
Authors: Sheng-Jun Lin, Sheng-Yaun Liu, Dipen Sahu, Laurent Pagani, Tien-Hao Hsieh, Naomi Hirano, Shih-Ping Lai, Tie Liu, Shih-Ying Hsu, Shanghuo Li, Kee-Tae Kim
Figure caption: Mass derivation of G205.46−14.56 M3 substructures B1 and B2 from our 820 μm data. (a) N(H2) map and contours from Figure 2(c) overlaid with 2D Gaussian models, where ellipses indicate the FWHMs of the major and minor axes. (b) Residuals between the observed data and the fitted models, with N(H2) contour levels at −1σ, 1σ, and 2σ, where σ = 2.8 × 1022 cm−2. Blue and red crosses mark the fitted Gaussian centers, while black/white crosses denote the 2D Gaussian centers derived from 1.3 mm data (Table 1 from D. Sahu et al. 2021).
Paper: Power Transmission of Whistlers in the Lunar Ionosphere
Authors: Kaiti Wang, Zhan-Rong Hsu, Jacob Bortnik, Ya-Hui Yang
Figure caption: The stratified slabs of the ionosphere set in the computation. R denotes the R-mode wave, and L denotes the L-mode wave. The transmitted wave at the top (100 km, m = 104) is composed of only the R-mode wave.
Paper: Power Transmission of Whistlers in the Lunar Ionosphere
Authors: Kaiti Wang, Zhan-Rong Hsu, Jacob Bortnik, Ya-Hui Yang
Figure caption: Selenographic distributions of the calculated power ratio Pr,0 at 100 km greater than −3 dB for different f0. Only grids with f0 smaller than the local fupper at the surface are plotted. (a) 1 Hz, (b) 5 Hz, and(c) 10 Hz, assuming T = 150 K, (d) 1 Hz, (e) 5 Hz, and (f) 10 Hz, assuming T = 400 K.
Paper: Power Transmission of Whistlers in the Lunar Ionosphere
Authors: Kaiti Wang, Zhan-Rong Hsu, Jacob Bortnik, Ya-Hui Yang
Figure caption: Selenographic distributions of the Doppler-shifted frequency fobs for different f0 at the surface with Pr,0 at 100 km greater than −3 dB and f0 less than fupper when Vsw is 300 km s−1. (a) 1 Hz at T = 150 K (b) 5 Hz at T = 150 K (c) 10 Hz at T = 150 K (d) 1 Hz at T = 400 K (e) 5 Hz at T = 400 K (f) 10 Hz at T = 400 K.
Paper: Power Transmission of Whistlers in the Lunar Ionosphere
Authors: Kaiti Wang, Zhan-Rong Hsu, Jacob Bortnik, Ya-Hui Yang
Figure caption: Selenographic distributions of the Doppler-shifted frequency fobs for waves of f0 to be 1 Hz at the surface for the region with Pr,0 at 100 km greater than −3 dB and f0 less than fupper when Vsw is from 400 to 600 km s−1. (a) Vsw = 400 km s−1 at T = 150 K (b) Vsw = 500 km s−1 at T = 150 K (c) Vsw = 600 km s−1 at T = 150 K (d) Vsw = 400 km s−1 at T = 400 K (e) Vsw = 500 km s−1 at T = 400 K (f) Vsw = 600 km s−1 at T = 400 K.
Paper: Power Transmission of Whistlers in the Lunar Ionosphere
Authors: Kaiti Wang, Zhan-Rong Hsu, Jacob Bortnik, Ya-Hui Yang
Figure caption: The computed Pr,0 at 100 km for 1, 5, and 10 Hz waves with varying surface electron densities for different ambient field strengths B0 at temperatures of 150 K and 400 K. The θB-sur is specified as 30°. (a) T = 150 K, B0 = 1 nT (b) T = 150 K, B0 = 10 nT (c) T = 150 K, B0 = 100 nT (d) T = 400 K, B0 = 1 nT (e) T = 400 K, B0 = 10 nT (f) T = 400 K, B0 = 100 nT. The horizontal dotted line denotes the value of −3 dB.
Paper: Power Transmission of Whistlers in the Lunar Ionosphere
Authors: Kaiti Wang, Zhan-Rong Hsu, Jacob Bortnik, Ya-Hui Yang
Figure caption: (a) Selenographic distribution of lunar surface magnetic field strength B0 (nT) (b) Distributions of the zenith angle of the surface magnetic field vector θZB. (c) Distributions of the angle between the surface field vector and the surface θB-sur.
Paper: Power Transmission of Whistlers in the Lunar Ionosphere
Authors: Kaiti Wang, Zhan-Rong Hsu, Jacob Bortnik, Ya-Hui Yang
Figure caption: fobs versus f0 at 0.1 Hz, 1 Hz, 5 Hz, and 10 Hz for the acute angle between solar wind and k of the wave (θks) is from 0° to 90°, when B0 is 20 nT using the ionospheric parameters at surface shown in Figures 1(a)–(c) at 150 K. Results for wave angles at ψ = 0°, 30°, and 60° for each frequency are shown as denoted in the legend.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: We show the SFR–mass relation for the subpopulations of the 461 AGN in our analysis within each panel. In the background is a 2D histogram of ∼640,000 galaxies within the GALEX–SDSS–WISE Legacy Catalog. We compare using our Bayesian estimates of average SFR over 100 Myr. The median uncertainty is σlog SFR = 0.09 [M⊙ yr−1].
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: Percentile of the distribution versus offset from median for each cluster within the t-SNE analysis for LAGN. Similar plots for the other host galaxy parameters are given in Appendix B in Figures 17, 18, 19, and 20.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: Magnitude–color space of absolute magnitude in the r band for each subsample, calculated from the cModelMag versus the cModelMag u − r color. Gray contours and mean error bars are the same as in Figure 8.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: SDSS u − g versus g − r diagram for the subsamples of AGN-selected population shown on each panel. The gray contours show the 10th, 50th, and 90th percentiles of the database not selected by the corresponding method for that panel (i.e., the remainder of the database). The mean error of these color measurements for the full sample is shown in black in the last panel.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: Histogram of the fractional contribution of the AGN template to the IR luminosity, fAGN, for each AGN selection method subsample. The color-matched horizontal lines give the mean Bayesian estimate for the uncertainty for the values in each histogram, with the mean error being 0.03.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: The histogram of SFR for the IR-selected subsample of those selected by many methods (top) and those identified by their IR emissions alone (bottom). The vertical dashed lines give the median values of each distribution.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: Distribution of host galaxy parameters for cluster 6 from the t-SNE dimensionality reduction. Similar plots for the remaining clusters are given in Appendix A in Figures 14, 15, and 16.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: LAGN distribution of the broad-line-selected subsample (top) and [O I] (middle) and [S II] (bottom) Seyferts compared to the remaining galaxies in the database.
Paper: Active Dwarf Galaxy Database. II. Connections between Host Galaxy Properties and Black Hole Accretion Signatures
Authors: Erik J. Wasleske, Vivienne F. Baldassare, Christopher M. Carroll
Figure caption: Distribution of host galaxy parameters for clusters 1, 2, and 3 from the t-SNE dimensionality reduction.
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Top panels: 78 spectra (gray) of the 4450–4545 Å (upper plot), 4815–4890 Å (middle plot), and 6520–6690 Å regions (lower plot), overlaid with an averaged spectrum (blue). Bottom panels: phase-resolved spectra of the same regions. The blue dashed line demonstrates the motion of the companion, and the red dashed line—the motion of the Be star.
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Surface density map for a Be binary model with a 50 day orbital period, q = 0.16, and disk viscosity parameter α = 1.0. The white lines trace the Roche equipotential contours, with the two large black circles representing the Be star (in x, y = 0.0) and the companion (x = 25.6 Req, y = 0.0 Req). The small black dots trace the two spiral arms formed in the Be disk due to the presence of the companion. More details about the simulation can be found in A. C. Rubio et al. (2025).
Paper: Dynamical Masses and Radiative Transfer Modeling of HD 698: A Be Binary in Evolutionary Transition
Authors: Ilfa A. Gabitova, Alex C. Carciofi, Tajan H. de Amorim, Mark Suffak, Anatoly S. Miroshnichenko, Sergey V. Zharikov, Amanda C. Rubio, Steve Danford, Alicia N. Aarnio, Peter Prendergast, Richard J. Rudy, Richard C. Puetter, R. Brad Perry, Aldiyar T. Agishev, Nadezhda L. Vaidman, Serik A. Khokhlov
Figure caption: Phase-folded RV curves: companion’s RVs (circles), Be star’s RVs (triangles), with fits overlaid (solid blue line for the companion and solid red line for the Be star). The average error of the companion’s RV measurements is 1.67 km s−1, of the Be star’s—2.07 km s−1.
Paper: Comparing Inside-out and Outside-in Quenching Modes in MaNGA Observation and MaNGIA Simulation
Authors: Hung-Yu Jian, Lihwai Lin, Connor Bottrell, Bau-Ching Hsieh, Carlos López-Cobá, Zi-Hua Ho, Shuai Feng, Shiyin Shen
Figure caption: Analogous to Figure 6, this figure illustrates the inside-out and outside-in quenching fractions within 1.5 effective radii, derived through an alternative scheme utilizing the averaged radial component of the gradient of the sSFR surface density. This method was implemented to overcome the classification limitations of the Fq–Cq approach for fully quenched galaxies. For the MaNGA sample, the derived fractions and their trends with stellar mass and halo mass exhibit agreement with the results obtained using the Fq–Cq method shown in Figure 6. In sharp contrast, the MaNGIA sample displays notable deviations in its quenching fractions relative to Figure 6, with the most prominent discrepancy being a pronounced dependence of the inside-out quenching fraction on host halo mass (Mh) when determined by the sSFR gradient.
Paper: Comparing Inside-out and Outside-in Quenching Modes in MaNGA Observation and MaNGIA Simulation
Authors: Hung-Yu Jian, Lihwai Lin, Connor Bottrell, Bau-Ching Hsieh, Carlos López-Cobá, Zi-Hua Ho, Shuai Feng, Shiyin Shen
Figure caption: Analogous to Figure 8, this figure presents the fractions of galaxies classified by their quenching mode, based on the sum of the averaged gradients of sSFR surface density calculated within two specific annuli (inner: 0–0.5 Re, outer: 1.0–1.5 Re). The results demonstrate broad agreement between the MaNGA and MaNGIA samples, and also consistency with the trends shown in Figure 8. A key discrepancy emerges for satellite galaxies, where MaNGA galaxies exhibit a weak dependence on stellar mass (M*), contrasting with MaNGIA galaxies, which appear largely independent of mass.
Paper: Comparing Inside-out and Outside-in Quenching Modes in MaNGA Observation and MaNGIA Simulation
Authors: Hung-Yu Jian, Lihwai Lin, Connor Bottrell, Bau-Ching Hsieh, Carlos López-Cobá, Zi-Hua Ho, Shuai Feng, Shiyin Shen
Figure caption: This figure presents quenching classifications based on the mean of ∇rΣsSFR for spaxels out to 2.5 Re. MaNGA galaxies are visibly dominated by outside-in quenching in this analysis. Despite this reversal in the dominant mode, MaNGA’s trends in inside-out and outside-in fractions with Mh and M* remain consistent with Figure 8; however, differing absolute values alter the overall dominant quenching mode. For MaNGIA, a significant deviation is apparent for massive central and satellite galaxies in the middle Mh bin when comparing this figure to Figure 8, indicating a transition from inside-out to outside-in quenching.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: The average density of the PDS 70 disk as a function of radius for 22 kyr (top panels), 0.22 Myr (middle panels), and 2.2 Myr (bottom panels) integration times. The Hill radius extension of the two planets is shown as the light blue and light pink shaded regions. The disk profile dissipation at different rates is represented in different colors: blue (κ = 0), red (κ = ﹩\frac{1}{10}﹩), orange (κ = 1), and green (κ = 10).
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Evolution of the planets’ b (blue) and c (pink) orbits under different photoevaporation rates κ for the protoplanetary disk. Here, Mc is set to 4 MJup. We plot the semimajor axis, eccentricity, period ratio, and resonant angle θc:b. The vertical dotted lines in each panel correspond to timescales for the disk’s full dissipation around the planets’ location. For examples of these surface densities around these timescales, please refer to Figure 2.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Comparison of the input photoevaporation prescription presented in G. Picogna et al. 2019 (adjusted for PDS 70’s average X-ray luminosity value) and the output obtained in Dusty-FARGO after implementation. This step serves as a verification that the PDS 70 disk is losing mass according to the prescription. Initial locations of PDS 70 b and c are marked in blue and pink, respectively.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Same as Figure 3, but with Mc set to 7 MJup.
Paper: On the Orbital Evolution of Multiple Wide Super-Jupiters: How Disk Migration and Dispersal Shape the Stability of the PDS 70 System
Authors: Clarissa R. Do Ó, Jaehan Bae, Quinn M. Konopacky, Jayke S. Nguyen, Patrick Diamond, Krzysztof Goździewski, Dawid Jankowski
Figure caption: Same as Figure 3, but with Mc set to 10 MJup.
Paper: Radio Observations Point to a Moderately Relativistic Outflow in the Fast X-Ray Transient EP241021a
Authors: Muskan Yadav, Eleonora Troja, Roberto Ricci, Yu-Han Yang, Mark H. Wieringa, Brendan O'Connor, Yacheng Kang, Rosa L. Becerra, Geoffrey Ryan, Malte Busmann
Figure caption: Observed gamma-ray flux (10–1000 keV) versus X-ray flux (0.5–4 keV) for EP-discovered FXRTs. EP-GRBs are shown by orange circles, and gamma-ray dark FXRTs by upward gray triangles (which mark 3σ upper limits to the gamma-ray emission, based on 8.192 s time-averaged fluxes from Fermi-GBM; see Section 2). The X-ray fluxes represent the time-averaged, unabsorbed 0.5–4 keV fluxes derived from WXT observations; uncertainties are shown at the 90% confidence level. EP241021a is indicated by the downward red triangle. Dashed lines represent power-law spectra with photon indices Γ = 0.5, 1.0, and 1.5.
Paper: Radio Observations Point to a Moderately Relativistic Outflow in the Fast X-Ray Transient EP241021a
Authors: Muskan Yadav, Eleonora Troja, Roberto Ricci, Yu-Han Yang, Mark H. Wieringa, Brendan O'Connor, Yacheng Kang, Rosa L. Becerra, Geoffrey Ryan, Malte Busmann
Figure caption: e-MERLIN image of EP241021a. The transient is co-located with the 90% confidence level from the Fraunhofer Telescope Wendelstein (orange circle; M. Busmann et al. 2025) at coordinates R.A. (J2000): 1h55m23﹩\mathop{.}\limits^{{\rm{s}}}﹩430, decl. (J2000): 5°56′17.86″ with an uncertainty of 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩15. It is also consistent with the 90% C.L. Chandra X-ray localization (yellow circle; see Section 3.4). The e-MERLIN radio data (see Section 3.2) provide an even tighter positional constraint at 1σ confidence, with milliarcsecond-level precision.
Paper: Radio Observations Point to a Moderately Relativistic Outflow in the Fast X-Ray Transient EP241021a
Authors: Muskan Yadav, Eleonora Troja, Roberto Ricci, Yu-Han Yang, Mark H. Wieringa, Brendan O'Connor, Yacheng Kang, Rosa L. Becerra, Geoffrey Ryan, Malte Busmann
Figure caption: ATCA and e-MERLIN radio observations of EP241021a. Flux densities are listed in Tables 1 and 2. The inset panel displays the intra-observation light curve from the first epoch at 5.5 GHz, segmented into 40 minute intervals to highlight short-term variability.