adsabs/AstroCLIMB huggingface dataset:
Paper: NuSTAR Observations of a Varying-flux Quasar in the Epoch of Reionization
Authors: Lea Marcotulli, Thomas Connor, Eduardo Bañados, Peter G. Boorman, Giulia Migliori, Brian W. Grefenstette, Emmanuel Momjian, Aneta Siemiginowska, Daniel Stern, Silvia Belladitta, C. C. Cheung, Andrew Fabian, Yana Khusanova, Chiara Mazzucchelli, Sofía Rojas-Ruiz, C. Megan Urry
Figure caption: Left: histogram of the difference between the Chandra and NuSTAR 3–7 keV posterior flux distribution obtained by simultaneously fitting all three Chandra data sets and the NuSTAR coadded FPMA. The mean (dashed vertical line) and 90% confidence limit (solid vertical lines) of the distributions obtained by a Gaussian fit (solid line) are shown. This histogram highlights that J1429+5447 varied in flux between the Chandra and NuSTAR epoch of observation at a >90% confidence limit. The mean of the distribution indicates that the NuSTAR flux is ∼2.6 times higher than the Chandra one. Moreover, only 0.26% of the distribution has a value of ≤0, in support of the fact that it is highly unlikely that the source did not vary between the two epochs. Right: 90% distribution of flux offsets observed for J1429+5447 (dark blue-green) relative to flux offsets observed for lower-redshift (z = [1, 2]) AGN in a broadly similar regime of black hole masses (MBH > 108) and Eddington ratios (λEdd > 0.01) by A. Georgakakis et al. (2024; from dark to light pink). Most of the probability distribution of the observed brightening occupies the region where fewer than 5% of the comparison flux variations reside. The rapidity of such a significant flux offset is thus unusual for an AGN.
Paper: The Blue Lurker WOCS 14020: A Long-period Post-common-envelope Binary in M67 Originating from a Merger in a Triple System
Authors: Emily M. Leiner, Natalie M. Gosnell, Aaron M. Geller, Meng Sun, Robert D. Mathieu, Alison Sills
Figure caption: (top) COSMIC model grid showing the initial primary mass and initial orbital period of our postmerger binary. Colors indicates the mass of the C/O WD that emerges after the final CE and emphasize final WD masses that fall within our mass confidence interval (0.68–0.78 M⊙). (bottom) The progenitor masses and orbital periods of the binary system after evolution through mass transfer or a CE. On the left, we show models using α = 1.0, and on the right, we show models using α = 0.8. The 359 day orbital period of WOCS 14020 is indicated with the vertical dashed line.
Paper: NuSTAR Observations of a Varying-flux Quasar in the Epoch of Reionization
Authors: Lea Marcotulli, Thomas Connor, Eduardo Bañados, Peter G. Boorman, Giulia Migliori, Brian W. Grefenstette, Emmanuel Momjian, Aneta Siemiginowska, Daniel Stern, Silvia Belladitta, C. C. Cheung, Andrew Fabian, Yana Khusanova, Chiara Mazzucchelli, Sofía Rojas-Ruiz, C. Megan Urry
Figure caption: Background-subtracted counts spectra for all three Chandra sources (J1429+5447, light blue plus signs; I-NE, navy squares; I-SW, green diamonds) and the NuSTAR data (fuchsia points) after binning each spectrum to have a minimum significance of three per bin for visual clarity. Source counts are not unfolded through the model but are instead normalized by the average effective area in each bin. In both panels, we show the model predictions for the fits to the Chandra data of J1429+5447 (light blue dashed–dotted lines), I-NE (navy dashed line), and I-SW (green shading and dotted line). The shaded bands in the plot represent the 68th percentile range regions of model predictions, as calculated from our posteriors. The top panel shows the Chandra-only fits extrapolated (and summed) into the NuSTAR passband (gray shading and solid line), which is representative of the scenario in which none of the sources are variable; the bottom panel instead shows the result of our fit in which J1429+5447 was allowed to vary in its normalization and photon index between the NuSTAR and Chandra epochs (fuchsia shading and solid line) under the assumption that I-NE and I-SW did not vary in the four months (observed frame; <two months rest frame assuming their photometric redshifts in Table 2) between the two observations. The results indicate that the J1429+5447 X-ray flux varied by a factor of 2.6 at >90% confidence limit (see also Figure 3).
Paper: NuSTAR Observations of a Varying-flux Quasar in the Epoch of Reionization
Authors: Lea Marcotulli, Thomas Connor, Eduardo Bañados, Peter G. Boorman, Giulia Migliori, Brian W. Grefenstette, Emmanuel Momjian, Aneta Siemiginowska, Daniel Stern, Silvia Belladitta, C. C. Cheung, Andrew Fabian, Yana Khusanova, Chiara Mazzucchelli, Sofía Rojas-Ruiz, C. Megan Urry
Figure caption: The 3–78 keV spectrum of J1429+5447 using a more complex spectral model. Left: redshifted power law with high-energy cutoff. The shaded bands in the plot represent the 68th percentile range regions of model predictions as calculated considering all posteriors for which Ecut,rest-frame < 169 keV (orange backward-slashed shaded region) and Ecut,rest-frame > 169 keV (blue forward-slashed shaded region; i.e., akin to the simple power-law model). Right: redshifted broken power law. The shaded bands in the plot represent the 68th percentile range regions of model predictions as calculated considering all posteriors for which Eb,rest-frame ≤ 100 keV (green backward-slashed shaded region; i.e., region of the posterior that includes values of Eb at 68% HDI level from the mode of the distribution) and Eb,rest-frame > 100 keV (purple forward-slashed shaded region; i.e., akin to the simple power-law model). These plots show that, within the uncertainties, we cannot determine whether a complex modeling of the source is favored. Therefore, the best-fit representation of the data at hand is the simplest one.
Paper: NuSTAR Observations of a Varying-flux Quasar in the Epoch of Reionization
Authors: Lea Marcotulli, Thomas Connor, Eduardo Bañados, Peter G. Boorman, Giulia Migliori, Brian W. Grefenstette, Emmanuel Momjian, Aneta Siemiginowska, Daniel Stern, Silvia Belladitta, C. C. Cheung, Andrew Fabian, Yana Khusanova, Chiara Mazzucchelli, Sofía Rojas-Ruiz, C. Megan Urry
Figure caption: The 3–7 keV light curve of J1429+5447; the errors are the 90% HDI levels. The eROSITA flux points (black diamond and green triangle) are derived by extrapolating the spectrum to the 3–7 keV range using Γ = 2.5 and the eROSITA 0.2–6 keV fluxes reported in P. Medvedev et al. (2021). The XMM-Newton flux point (cyan star) was derived using the best-fit power-law model of P. Medvedev et al. (2021). The Chandra (red dot) and NuSTAR (yellow square) data points are the ones obtained in this work. To guide the eye, the red dashed line at the level of the Chandra flux is plotted. This plot highlights that there was no evidence of variability for J1429+5447 before the NuSTAR observation, when the source flux brightened by 0.4 dex.
Paper: The Blue Lurker WOCS 14020: A Long-period Post-common-envelope Binary in M67 Originating from a Merger in a Triple System
Authors: Emily M. Leiner, Natalie M. Gosnell, Aaron M. Geller, Meng Sun, Robert D. Mathieu, Alison Sills
Figure caption: (a) Binned COS spectrum for WOCS 14020, overlaid with 100 random draws from the posterior distribution from the WD atmosphere fits. The light blue data points correspond to Earth-shine emission and are not included in the fitting routine. (b) Posterior probability distributions for the WD atmosphere fits to the COS spectrum, with the median, 16%–84% (approximating 1σ), and 2.5%–97.5% (approximating 2σ) percentile values marked as indicated in the legend. The ﹩\mathrm{log}g﹩ and Teff values are fit directly, and the corresponding WD mass and age are calculated using CO-core mass–radius relationships and cooling times.
Paper: Dust-extinction-curve Variation in the Translucent Interstellar Medium Is Driven by Polycyclic Aromatic Hydrocarbon Growth
Authors: Xiangyu Zhang, Brandon S. Hensley, Gregory M. Green
Figure caption: Comparison of 2D distribution of A(V), R(V), and qPAH for dust clouds. For A(V) and R(V) maps, we select high-quality stars from ZG24 and remove lines of sight where only partial extinction is covered by XP. For the qPAH map, we remove lines of sight where the qPAH map is of low quality (χ2/DOF > 3 or qPAH/σ(qPAH) < 3) or cross multiple clouds (Equation (1)). The binning method and selection of stars in the 2D maps are described in Appendix A. Despite different baselines and finer structures in different maps, all clouds tend to have lower R(V) at high-qPAH regions, as indicated quantitatively on the per-star basis in Figure 3.
Paper: Dust-extinction-curve Variation in the Translucent Interstellar Medium Is Driven by Polycyclic Aromatic Hydrocarbon Growth
Authors: Xiangyu Zhang, Brandon S. Hensley, Gregory M. Green
Figure caption: R(V) variation as a function of the mass accreted onto astrodust or PAHs relative to initial mass, holding the other component (PAHs or astrodust) fixed. For R(V) to decrease from 3.1 to 2.5, the astrodust mass must grow by a factor of ~291. This greatly exceeds the available mass budget of Mg, Fe, and Si (the major components of astrodust) in the gas. However, PAHs only have to grow by 91% in mass, or 54 ppm of C, which is a viable amount given the mass budget of carbon in the gas phase (E. B. Jenkins 2009; B. S. Hensley & B. T. Draine 2021).
Paper: Dust-extinction-curve Variation in the Translucent Interstellar Medium Is Driven by Polycyclic Aromatic Hydrocarbon Growth
Authors: Xiangyu Zhang, Brandon S. Hensley, Gregory M. Green
Figure caption: Correlation between R(V) and qPAH using stars that pass all the cuts in Figure 1. The 16th, 50th, and 84th percentiles are shown as cyan lines. We also label R(V) = 3.1, the Milky Way average value, in red dotted lines. Although different clouds have different baselines of R(V) due to different initial distribution of dust grain size, all dust clouds show anticorrelation between R(V) and qPAH.
Paper: Dust-extinction-curve Variation in the Translucent Interstellar Medium Is Driven by Polycyclic Aromatic Hydrocarbon Growth
Authors: Xiangyu Zhang, Brandon S. Hensley, Gregory M. Green
Figure caption: R(V) distribution of LMC and SMC is shown in the top panels. We select stars by distance and proper motion and remove foreground extinction, described in Appendix B. We label a few dense dust clouds in magenta circles indicated by H II signal from L. A. Lopez et al. (2014), which tend to have higher R(V) than their neighborhood. We also show the qPAH map from J. Chastenet et al. (2019) in the bottom panels. The H II regions generally have lower qPAH. The quantitative comparison on the per-star basis is shown in Figure 5.
Paper: NuSTAR Observations of a Varying-flux Quasar in the Epoch of Reionization
Authors: Lea Marcotulli, Thomas Connor, Eduardo Bañados, Peter G. Boorman, Giulia Migliori, Brian W. Grefenstette, Emmanuel Momjian, Aneta Siemiginowska, Daniel Stern, Silvia Belladitta, C. C. Cheung, Andrew Fabian, Yana Khusanova, Chiara Mazzucchelli, Sofía Rojas-Ruiz, C. Megan Urry
Figure caption: The 3–7 keV posterior flux distribution vs. the full-band photon index posterior distribution for J1429+5447 (Chandra epoch: solid lines; NuSTAR epoch: dashed lines), I-NE (dotted lines), and I-SW (dashed–dotted lines) obtained with the simultaneous fit of the three Chandra sources and the coadded FPMAs (details in Section 4.3). The 1σ and 90% contour levels are reported in the plot. This is an extension of Figure 3 to show how subdominant I-NE and I-SW are in the 3–7 keV band compared to J1429+5447.
Paper: Dust-extinction-curve Variation in the Translucent Interstellar Medium Is Driven by Polycyclic Aromatic Hydrocarbon Growth
Authors: Xiangyu Zhang, Brandon S. Hensley, Gregory M. Green
Figure caption: Quantitative comparison on the per-star basis between R(V) and qPAH in LMC (left panel) and SMC (right panel). The median value of R(V) decreases by 0.4 as qPAH increases from 1% to 6% in the LMC. In the SMC, the trend is not clear because of small variation range of qPAH.
Paper: Dust-extinction-curve Variation in the Translucent Interstellar Medium Is Driven by Polycyclic Aromatic Hydrocarbon Growth
Authors: Xiangyu Zhang, Brandon S. Hensley, Gregory M. Green
Figure caption: Continuation of Figure 1.
Paper: A Possible Formation Scenario of the Gaia ID 3425577610762832384: Inner Binary Merger inside a Triple Common Envelope
Authors: Zhuowen Li, Xizhen Lu, Guoliang Lü, Chunhua Zhu, Helei Liu, Jinlong Yu
Figure caption: The key evolutionary stage diagram of the initial triple leading to the formation of G3425, where the light-red shaded area represents the duration of the observed G3425 phase.
Paper: A Possible Formation Scenario of the Gaia ID 3425577610762832384: Inner Binary Merger inside a Triple Common Envelope
Authors: Zhuowen Li, Xizhen Lu, Guoliang Lü, Chunhua Zhu, Helei Liu, Jinlong Yu
Figure caption: The distribution of the initial reduced mass of the inner binary (﹩\frac{{m}_{{\rm{1,ini}}}{m}_{{\rm{2,ini}}}}{{m}_{{\rm{1,ini}}}+{m}_{{\rm{2,ini}}}}﹩), the initial mass of the tertiary, the initial inner and outer orbital periods, and the orbital period of the PTBs (PPTB,orb) under the assumption that αCE,in = αCE,out = 1. Different colors represent the orbital periods of the PTBs, with the blue stars indicating the initial parameters selected in Figures 1 and 2.
Paper: A Possible Formation Scenario of the Gaia ID 3425577610762832384: Inner Binary Merger inside a Triple Common Envelope
Authors: Zhuowen Li, Xizhen Lu, Guoliang Lü, Chunhua Zhu, Helei Liu, Jinlong Yu
Figure caption: The probability distribution of the orbital period and eccentricity for the surviving BH binary of the PTB after undergoing an SNe event. The darker the color, the higher the probability. The red and green markers represent the locations of the PTB before the SNe and the observed location of G3425, respectively. The left and right panels show the Maxwellian distributions for σk values of 50 and 10 km s−1, respectively.
Paper: A Possible Formation Scenario of the Gaia ID 3425577610762832384: Inner Binary Merger inside a Triple Common Envelope
Authors: Zhuowen Li, Xizhen Lu, Guoliang Lü, Chunhua Zhu, Helei Liu, Jinlong Yu
Figure caption: The time functions of orbital period (Porb), eccentricity (e), mass, and radius for the selected triple.
Paper: The Blue Lurker WOCS 14020: A Long-period Post-common-envelope Binary in M67 Originating from a Merger in a Triple System
Authors: Emily M. Leiner, Natalie M. Gosnell, Aaron M. Geller, Meng Sun, Robert D. Mathieu, Alison Sills
Figure caption: CMD of M67 highlighting Gaia DR3 proper-motion members (gray); blue stragglers (blue); BLs (orange); and our target, the BL WOCS 14020 (red square). Memberships are determined as described in E. M. Leiner & A. Geller (2021).
Paper: Persistent GeV Counterpart to the Microquasar GRS 1915+105
Authors: Guillem Martí-Devesa, Laura Olivera-Nieto
Figure caption: TS map zoomed in to the position of PS J1915.5+1056 with the location of possible counterparts. A plus sign and dashed line represent the best-fit position and 99% containment of PS J1915.5+1056 using the standard IEM. The position of GRS 1915+105 is represented with a white star. The position of the binary IGR J19149+1036 is shown with a red square. The white contours show radio emission from GLEAM (N. Hurley-Walker et al. 2019), outlining the shape of a nearby SNR, indicated with a pink circle. The closest pulsar and stellar cluster are represented with a green rhombus and a white diamond, respectively. The only source besides GRS 1915+105 that falls within the 99% containment radius is a faint unassociated X-ray source, indicated with a blue cross. Finally, the three possible sites of jet interaction with the ISM are indicated with yellow triangles.
Paper: Persistent GeV Counterpart to the Microquasar GRS 1915+105
Authors: Guillem Martí-Devesa, Laura Olivera-Nieto
Figure caption: (a) Best-fit spectral model and flux points for PS J1915.5+1056. The teal circles show the flux points calculated with the standard IEM, and the gray squares correspond to the alternative IEM. Uncertainties are statistical only. The machine-readable values for the flux points shown can be found in Table 2. (b) Residual p-value statistic map showing no significant excesses. For reference, PS = 6.24 is equivalent to 5σ. (c) Distribution of the residual p-value statistic. The expected distribution is shown with a dotted line, and the fitted distribution is shown with a solid line.
Paper: Persistent GeV Counterpart to the Microquasar GRS 1915+105
Authors: Guillem Martí-Devesa, Laura Olivera-Nieto
Figure caption: Temporal analysis of PS J1915.5+1056. Top: periodogram for PS J1915.5+1056, derived using photon weights. The orbital periods of GRS 1915+105 and IGR J19149+1036 are marked (with the uncertainty represented with a shaded area), as well as Fermi’s orbital precession period. Globally, no signal is found above 3σ for any frequency evaluated. Bottom: light curve for PS J1915.5+1056 employing a daily and weekly binning. Flux values are displayed relative to that obtained in Section 3. We report detections for bins with TS > 4; otherwise, upper limits are reported at 95% confidence level. The results are consistent with a constant flux.
Paper: Persistent GeV Counterpart to the Microquasar GRS 1915+105
Authors: Guillem Martí-Devesa, Laura Olivera-Nieto
Figure caption: TS residual map (excluding PS J1915.5+1056) of the ROI zoomed in to the position of GRS 1915+105, which is marked with a star. The best-fit position and 99% statistical containment region of PS J1915.5+1056 are shown with a plus sign and dashed black line for the standard IEM and with a cross and dotted green line for the alternative IEM. The other two pointlike excesses, which fall below the detection threshold when using the alternative IEM, are indicated with white circles. The direction of the jet axis (e.g., M. J. Reid et al. 2014) is indicated with a straight dashed blue line.
Paper: Persistent GeV Counterpart to the Microquasar GRS 1915+105
Authors: Guillem Martí-Devesa, Laura Olivera-Nieto
Figure caption: Molecular gas emission around GRS 1915+105. (a) FUGIN 12CO (J = 1–0) spectrum of molecular gas toward GRS 1915+105. (b) Integrated 12CO emission map in the velocity interval shaded green in panel (a). The white circles represent the extraction regions of 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩1 radius used to derive the number density. The plus sign and dashed black ellipse show the position and 99% position uncertainty of PS J1915.5+1056, respectively. The white star represents the nominal position of GRS 1915+105.
Paper: Persistent GeV Counterpart to the Microquasar GRS 1915+105
Authors: Guillem Martí-Devesa, Laura Olivera-Nieto
Figure caption: The first two panels show TS residual maps after considering all the model components except those associated with PS J1915.5+1056 and SNR G045.7-00.4, centered at the catalog position of 4FGL J1916.3+1108. Comparison between the 1–100 GeV (left) and 5–500 GeV (middle) energy ranges reveals energy dependence of the overall morphology of the gamma-ray signal of the region. The solid line represents the best-fit extension of 4FGL J1916.3+1108, while the dashed line represents the 99% position uncertainty of PS J1915.5+1056 as obtained in the analysis above 1 GeV (Section 3). The white star represents the nominal position of GRS 1915+105. The right panel shows the best-fit spectral model and flux points for the 4FGL J1916.3+1108 power-law (solid line) and log-parabola (dashed line) models. The SED of PS J1915.5+1056 (standard IEM case) is also shown for easy comparison.
Paper: The Massive and Quiescent Elliptical Host Galaxy of the Repeating Fast Radio Burst FRB 20240209A
Authors: T. Eftekhari, Y. Dong, 雨欣 董, W. Fong, V. Shah, S. Simha, B. C. Andersen, S. Andrew, M. Bhardwaj, T. Cassanelli, S. Chatterjee, D. A. Coulter, E. Fonseca, B. M. Gaensler, A. C. Gordon, J. W. T. Hessels, A. L. Ibik, R. C. Joseph, L. A. Kahinga, V. Kaspi, B. Kharel, C. D. Kilpatrick, A. E. Lanman, M. Lazda, C. Leung, C. Liu, L. Mas-Ribas, K. W. Masui, R. Mckinven, J. Mena-Parra, A. A. Miller, K. Nimmo, A. Pandhi, S. S. Patil, A. B. Pearlman, Z. Pleunis, J. X. Prochaska, M. Rafiei-Ravandi, M. Sammons, P. Scholz, K. Shin, K. Smith, I. Stairs
Figure caption: sSFR as a function of the mass-weighted age for the host of FRB 20240209A and for a sample of FRB hosts at z < 0.3 from the literature. We denote FRBs with sSFRs and mass-weighted ages derived in a similar manner as for FRB 20240209A from A. C. Gordon et al. (2023) and K. Sharma et al. (2024) as closed symbols. Also shown are the values for the hosts of Type I and Type II CCSNe (S. Schulze et al. 2021), Type Ia SNe (J. D. Neill et al. 2009), and short GRBs (P. K. Blanchard et al. 2017; A. E. Nugent et al. 2022). Open symbols for FRBs and values for SNe are not necessarily derived using the same formalism. Ages for the Type Ia SNe sample are weighted by the host galaxy luminosity and hence represent an underestimate of the mass-weighted age. For comparison, we include the distribution of field galaxies from the COSMOS sample at z < 0.3 in grayscale. Horizontal lines mark the divisions between star-forming, transitioning, and quiescent galaxies based on the mass-doubling number ﹩{ \mathcal D }(z)﹩ at a redshift z = 0.3.
Paper: The Massive and Quiescent Elliptical Host Galaxy of the Repeating Fast Radio Burst FRB 20240209A
Authors: T. Eftekhari, Y. Dong, 雨欣 董, W. Fong, V. Shah, S. Simha, B. C. Andersen, S. Andrew, M. Bhardwaj, T. Cassanelli, S. Chatterjee, D. A. Coulter, E. Fonseca, B. M. Gaensler, A. C. Gordon, J. W. T. Hessels, A. L. Ibik, R. C. Joseph, L. A. Kahinga, V. Kaspi, B. Kharel, C. D. Kilpatrick, A. E. Lanman, M. Lazda, C. Leung, C. Liu, L. Mas-Ribas, K. W. Masui, R. Mckinven, J. Mena-Parra, A. A. Miller, K. Nimmo, A. Pandhi, S. S. Patil, A. B. Pearlman, Z. Pleunis, J. X. Prochaska, M. Rafiei-Ravandi, M. Sammons, P. Scholz, K. Shin, K. Smith, I. Stairs
Figure caption: SFRs and stellar masses for FRB host galaxies, including FRB 20240209A, at z < 0.3 plotted against field galaxies from the COSMOS sample. For comparison, we also include the host galaxies of Type I and Type II CCSNe (S. Schulze et al. 2021), Type Ia SNe (H. Lampeitl et al. 2010), short GRBs (P. K. Blanchard et al. 2017; A. E. Nugent et al. 2022; M. Jeong & M. Im 2024), and ULXs (K. Kovlakas et al. 2020). Type Ia hosts classified as "passive" galaxies in H. Lampeitl et al. (2010) owing to a lack of recent star formation activity are arbitrarily plotted at log(SFR/M⊙yr−1) = −4.75. All other values plotted represent solid SFR measurements.
Paper: The Massive and Quiescent Elliptical Host Galaxy of the Repeating Fast Radio Burst FRB 20240209A
Authors: T. Eftekhari, Y. Dong, 雨欣 董, W. Fong, V. Shah, S. Simha, B. C. Andersen, S. Andrew, M. Bhardwaj, T. Cassanelli, S. Chatterjee, D. A. Coulter, E. Fonseca, B. M. Gaensler, A. C. Gordon, J. W. T. Hessels, A. L. Ibik, R. C. Joseph, L. A. Kahinga, V. Kaspi, B. Kharel, C. D. Kilpatrick, A. E. Lanman, M. Lazda, C. Leung, C. Liu, L. Mas-Ribas, K. W. Masui, R. Mckinven, J. Mena-Parra, A. A. Miller, K. Nimmo, A. Pandhi, S. S. Patil, A. B. Pearlman, Z. Pleunis, J. X. Prochaska, M. Rafiei-Ravandi, M. Sammons, P. Scholz, K. Shin, K. Smith, I. Stairs
Figure caption: Results of our GALFIT modeling of the host of FRB 20240209A, where we subtract a single-component Sérsic profile (middle panel) from a Gemini/GMOS r-band image (left panel; originally presented by V. Shah et al. 2024) to derive a residual image (right panel). The circular region with radius re illustrates the best-fit effective radius re = 7.78 ± 0.03 kpc. Each image is oriented north up and east to the left. At the Galactic latitude of the source (+26.58118), dust extinction is not a significant issue in our modeling.