adsabs/AstroCLIMB huggingface dataset:
Paper: Photo-dynamical Analysis of Circumbinary Multi-planet System TOI-1338: A Fully Coplanar Configuration with a Puffy Planet
Authors: Mu-Tian Wang, 牧天 王, Hui-Gen Liu, 慧根 刘
Figure caption: Top: optimized Δχ 2 map of the transit light curve of TOI-1338 b and RV data fitting as a function of the mutual inclination between TOI-1338 c and binary orbit ΔI  c . The red vertical dashed line denotes the stability limit (∼40°) derived from S23, beyond which the system would be unstable. Bottom: the isolines of the optimized Δχ 2 map of the transit light curve and RV data fitting assuming different orbital inclination i  c  and node angles Ω c  of TOI-1338 c. The isolines of mutual inclinations of 5°, 10°, 20°, and 40° are also plotted with gray dashed lines.
Paper: Photo-dynamical Analysis of Circumbinary Multi-planet System TOI-1338: A Fully Coplanar Configuration with a Puffy Planet
Authors: Mu-Tian Wang, 牧天 王, Hui-Gen Liu, 慧根 刘
Figure caption: Left to right: the best-fit RV signals of TOI-1338 b from joint, esp-only, and harps-only analyses. The RV data from HARPS and ESPRESSO prior to and after 2019 are shown in blue, orange, and green, respectively. Two periods of TOI-1338 b are shown in the phase-folded figure. Black symbols with error bars are RVs binned in 11 evenly spaced intervals within one period. The simulated RV signals of TOI-1338 b in each analysis at the observation epoch are also plotted with red circles.
Paper: Photo-dynamical Analysis of Circumbinary Multi-planet System TOI-1338: A Fully Coplanar Configuration with a Puffy Planet
Authors: Mu-Tian Wang, 牧天 王, Hui-Gen Liu, 慧根 刘
Figure caption: The O−C diagram of the midtimes of primary and secondary eclipses, fitted to the common period. The periods fitted from primary and secondary eclipses are (14.6085574 ± 9) × 10−7 days and (14.6085774 ± 1.58) × 10−5 days, respectively. Neither the divergence of primary and secondary ephemerides (0.8 minutes) nor the dynamical delay of the primary eclipse due to the short-term perturbations (0.03 minutes) predicted from the best-fit model is observable given the large uncertainties in midtimes of primary and secondary eclipses (0.36 and 5 minutes, respectively).
Paper: Photo-dynamical Analysis of Circumbinary Multi-planet System TOI-1338: A Fully Coplanar Configuration with a Puffy Planet
Authors: Mu-Tian Wang, 牧天 王, Hui-Gen Liu, 慧根 刘
Figure caption: Left: the periodogram of HARPS, ESPRESSO, and all RV observations after subtracting the binary and TOI-1338 c MAP signal from the Keplerian orbit fit; the dotted, dotted–dashed, and dashed lines represent false-alarm probabilities of 0.1%, 1%, and 10%, respectively. Right: the phase-folded plot of HARPS ESPRESSO, and all RV residuals at the binary period. We show two periods of folded residuals to display the modulation. The binary’s Keplerian RV signal is also plotted with red lines to compare with the residual phases.
Paper: Photo-dynamical Analysis of Circumbinary Multi-planet System TOI-1338: A Fully Coplanar Configuration with a Puffy Planet
Authors: Mu-Tian Wang, 牧天 王, Hui-Gen Liu, 慧根 刘
Figure caption: The difference between the measured transit midtimes and durations of TOI-1338 and those derived from best-fit solution (black circles). The error bars are the measured uncertainties from the observation (listed in Table 1). We also show how the transit midtimes/durations of TOI-1338 b would change if we tweaked TOI-1338 c’s planetary mass to be zero (blue) and inclination to be 110° (green); the deviations shown by the tweaked models indicate that TOI-1338 b is gravitationally interacting with TOI-1338 c.
Paper: Photo-dynamical Analysis of Circumbinary Multi-planet System TOI-1338: A Fully Coplanar Configuration with a Puffy Planet
Authors: Mu-Tian Wang, 牧天 王, Hui-Gen Liu, 慧根 刘
Figure caption: The nine primary eclipse light curves used in the photodynamical modeling. Gray error bars are TESS 2-minute light curves, and red lines are synthetic light curves from the best-fit models. Residuals are plotted below each panel.
Paper: Photo-dynamical Analysis of Circumbinary Multi-planet System TOI-1338: A Fully Coplanar Configuration with a Puffy Planet
Authors: Mu-Tian Wang, 牧天 王, Hui-Gen Liu, 慧根 刘
Figure caption: The nine secondary eclipse light curves used in the photodynamical modeling. Labels are the same as in Figure 12.
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: Model and residual images for two SDSS galaxies. In the top row, we show a set of images corresponding to the first galaxy in our sample (sorted by SDSS “SpecObjID”), for which the S1 + N1,PSF model is statistically preferred. In the bottom row, we show the corresponding set of images for the very first galaxy in our SDSS catalog that is classified as double Sérsic. In each row, the images are from left to right: the original r-band image, the best-fit single-Sérsic model, the difference between the r-band image and best-fit single-Sérsic model, the best-fit two-component model (Sérsic + PSF model for the top row, double Sérsic for the bottom row), and the difference between the r-band image and best-fit two-component model. The display scale of the images in the third and fifth columns is stretched by a factor of 2 to highlight the residuals. The NSC in the top row is evident in the residuals from the single-component fit and well modeled by the two-component one. The central structure is somewhat ambiguous for the second galaxy, but there is no clear evidence for an NSC.
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: NSC detection limits in the r band as a function of r-band central surface brightness, μ 0,r , for three different sets of simulations. The analysis involves the placement and attempted recovery of a central point source in a set of single-Sérsic SMUDGes galaxies (blue) and versions of those galaxy images where the flux is increased by a factor of 16 (green) and 100 (red). Points represent the most luminous simulated point source that we failed to identify as an NSC in each galaxy. The horizontal lines mark the 50% completeness magnitude for the three samples, ranging from 23.4 mag for the red points to 24.1 mag for the blue points.
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: The absolute magnitude of NSCs in SMUDGes (blue) and SDSS (red) galaxies across redshift. The plotted curve represents the 50% completeness threshold for the SMUDGes sample, which corresponds to the blue horizontal line illustrated in Figure 2. For reference, we denote the redshifts corresponding to the Virgo and Coma Clusters.
Paper: Study of Double-mode RR Lyrae Stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, Chow-Choong Ngeow
Figure caption: SDSS 3478713: analysis of amplitude (A 1) and phase (ϕ 1) variation on a season-to-season basis in the r band. Points until 2007 are from SDSS data, while the latter ones are from ZTF data.
Paper: Study of Double-mode RR Lyrae Stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, Chow-Choong Ngeow
Figure caption: Blazhko side peak in SDSS 850835: the top panel shows the spectra around f 1 observed for the g-band LC. The bottom panel shows the Blazhko side peak f 1 + f  m  in the vicinity of f 1.
Paper: Study of Double-mode RR Lyrae Stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, Chow-Choong Ngeow
Figure caption: SDSS 850835: analysis of amplitude (A 1) and phase (ϕ 1) variation on a season-to-season basis. The left and right panels show the analysis in the g and i bands, respectively.
Paper: Study of Double-mode RR Lyrae Stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, Chow-Choong Ngeow
Figure caption: SDSS 3214909: analysis of amplitude (A 1) and phase (ϕ 1) variation on a season-to-season basis in the g band.
Paper: Study of Double-mode RR Lyrae Stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, Chow-Choong Ngeow
Figure caption: Blazhko side peak in SDSS 3214909: the panels are similar to Figure 6.
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: Cutout images of 18 bare PSF (PSF only) targets in our SDSS sample sorted by increasing g − r. The field of view of each image is 52.″4. The SDSS spectroscopic classification is provided at the bottom of each panel. We also indicate whether the target is located within 10° of the Virgo Cluster center. These images are drawn from the Legacy Survey's online viewer (https://www.legacysurvey.org/viewer).
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: Color–magnitude relation for SMUDGes (blue) and SDSS (red) galaxies. Galaxies with NSCs are highlighted using circles (SMUDGes) and triangles (SDSS) and are almost exclusively found along the red sequence. The black line represents the fitted red sequence. Galaxies whose color difference from the red sequence is less than 0.1 mag are considered to be red sequence galaxies (shaded region). All data points have error bars representing the uncertainty measured from GALFIT.
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: NSC stellar mass vs. host galaxy stellar mass for SMUDGes (circles) and SDSS galaxies (triangles). The stellar mass distributions of the SMUDGes (solid line) and SDSS (dotted line) galaxies are in the top panel. In the bottom panel, the solid line and shaded region represent the best-fit line and its 1σ uncertainty, respectively. For comparison, we also present the relationship from Neumayer et al. (2020; dashed line) and lines of proportionality for three different fractional levels (dotted lines). We find ﹩{M}_{\mathrm{NSC}}/{M}_{\odot }={10}^{6.02\pm 0.03}{({M}_{* ,\mathrm{gal}}/{10}^{8}{M}_{\odot })}^{0.77\pm 0.04}﹩ with 0.27 dex scatter.
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: The dependence of NSC occupation fraction, f NSC, on stellar and halo mass for the red sequence SMUDGes sample. The dashed black line shows the mean M *,gal–M  h,gal relation from Zaritsky & Behroozi (2023) for reference. Each pixel with a plotted occupation fraction must contain at least four galaxies. Galaxies above the mean stellar mass–halo mass relation have higher f NSC than those below the line.
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: Cutout images of galaxies exemplifying cases where no satisfactory model was identified (referred to as the “failed fitting” category). We display the first 12 such galaxies as sorted by SDSS “SpecObjID.” There is a range of morphology, although blue and highly inclined systems are overrepresented in the category. The field of view of each image is 52.″4. These images are drawn from the Legacy Survey's online viewer (https://www.legacysurvey.org/viewer).
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: The dependence of NSC occupation fraction, f NSC, on stellar mass fraction, surface brightness, axis ratio, and D 10 for the red sequence SMUDGes (blue) and SDSS (red) samples. The error bars are calculated using the binomial distribution for the appropriate number of objects in each bin and represent the 1σ uncertainties. The two samples show the same trends in f NSC where they overlap, although the normalizations may differ for reasons described in the text.
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: The dependence of the NSC occupation fraction, f NSC, on central surface brightness and axis ratio for the red sequence SMUDGes sample. There is a decline in occupation fraction with fainter central surface brightness and with a smaller axis ratio.
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: Stellar and estimated halo masses of SMUDGes (blue) and SDSS (red) galaxies. Galaxies with NSCs are highlighted using circles (SMUDGes) and triangles (SDSS) and are, in general, biased upward from the parent galaxy population.
Paper: Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies
Authors: Donghyeon J. Khim, Dennis Zaritsky, Mika Lambert, Richard Donnerstein
Figure caption: The dependence of NSC occupation fraction, f NSC, on host stellar mass and the environmental measure D 10 for the red sequence SMUDGes sample. A dependence on both variables is evident.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: Left: histogram distributions of ﹩\mathrm{log}q﹩ for the 2016–2019 KMTNet AnomalyFinder-discovery (magenta) and AnomalyFinder-recovery (blue) planets, and the planets detected before KMTNet’s regular survey (black). Right: cumulative distributions of ﹩\mathrm{log}q﹩ for the pre-KMTNet planets and the 2016–2019 KMTNet AnomalyFinder planets, which are the sum of the AnomalyFinder-discovery and AnomalyFinder-recovery planets shown in the left panel. The dark turquoise region indicates the “sub-Saturn desert” (﹩\mathrm{log}q=\left[-3.6,-3.0\right]﹩) in the KMTNet sample.
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: HST ACS image centered on the Perseus central giant NGC 1275. The field shown is 200″ across, equivalent to 75 kpc at the distance of Perseus. The maroon dots mark the positions of star cluster candidates (F814W < 25.5, F475W − F814W < 2.4; see also the CMD in Figure 3).
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption:  Left panel:  DOLPHOT values of sharp plotted vs. magnitude, for each of the two filters. All detected objects are plotted here before any culling. Nonstellar, extended objects scatter downward to lower sharp values. The red lines denote the culling boundaries. Right panel:  DOLPHOT values of chi vs. magnitude. Normally χ − values near 1 indicate objects that ideally match the point-spread function, while higher χ − values indicate objects that are poorly fit by the PSF.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: Bayesian posterior distributions (PDF) of the mass of the host star, M host, the planetary mass, M planet, the lens distance, D L, the projected planet–host separation, r ⊥, and the lens–source relative proper motion in the heliocentric frame, μ hel,rel. In each panel, the solid black line and the two dashed black lines represent the median value and the 15.9% and 84.1% percentiles of the distribution. The solid black histogram shows the total distribution, and the bulge and disk lens distributions are shown in red and blue, respectively.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: CMD for the four unambiguous planetary events. The CMDs of KMT-2017-BLG-0849, KMT-2017-BLG-1057, and KMT-2017-BLG-2331 are constructed using the KMTC field stars, and the CMD of OGLE-2017-BLG-0364 is built using the OGLE-III star catalog (Szymański et al. 2011). For each panel, the red asterisk and the blue dot represent the centroid of the red-giant clump and the source star, respectively. The green dots represent the HST CMD of Holtzman et al. (1998), whose centroid of the red-giant clump (V − I, I)cl,HST = (1.62, 15.15) (Bennett et al. 2008) is matched to that of KMTC or OGLE-III.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: Observed data together with three 2L1S models and the 1L2S model for KMT-2017-BLG-0958. All models can fit the data well and thus this is only a candidate planetary event.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: Caustic geometries of the candidate planetary event, KMT-2017-BLG-0958.
Paper: Systematic KMTNet Planetary Anomaly Search. XII. Complete Sample of 2017 Subprime Field Planets
Authors: Yuqian Gui, Weicheng Zang, Ruocheng Zhai, Yoon-Hyun Ryu, Andrzej Udalski, Hongjing Yang, Cheongho Han, Shude Mao, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radosław Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Jiyuan Zhang, Renkun Kuang, Qiyue Qian, Wei Zhu
Figure caption: Observed data and the 2L1S model for KMT-2017-BLG-2331.
Paper: Photometric Completeness Modelled with Neural Networks
Authors: William E. Harris, Joshua S. Speagle, 佳士 沈
Figure caption: Similar to Figure 15, but now highlighting the behavior of the four NN models labeled in Figure 20 and with the magnitude distribution of the training (rather than testing) data shown. The 50% recovery limit in the testing set from the prediction and the data are also plotted as red and black vertical lines, respectively. These results help to illustrate how the NN is able to learn from increasing numbers of ASTs, and how many ASTs might be needed for various tasks.
Paper: Forced Measurement of Astronomical Sources at Low Signal-to-noise
Authors: A. Dutta, J. R. Peterson, G. Sembroski
Figure caption: This plot shows the intrinsic errors in flux, centroid, size, and ellipticity. A wide range of sizes, counts, and ellipticity has been used to make this plot. The background was set to 0. To produce each point, 106 samples were drawn, and the error in measurement was recorded. Forced indicates only a single iteration was performed with the true values as guess. The black lines from the top are 2/N, 1/N, 1/2N, 1/4N, and 1/8N, respectively. The black circle that denotes ﹩{\epsilon }_{\mathrm{flux}}^{2}/{N}^{2}﹩ closely follows the 1/N line. Light green circles that denote ﹩{\epsilon }_{\mathrm{size}}^{2}/{S}^{4}﹩ closely follow the 1/2N line. In the case of the centroid, ﹩{\epsilon }_{{\mu }_{x}}^{2}/{S}^{2}﹩ is shown in light blue circles and seems to follow the 1/N line. For ellipticity, ﹩{\epsilon }_{{e}_{1}}^{2}﹩ is shown in red circles, and ﹩{\epsilon }_{{e}_{2}}^{2}﹩ is shown in red triangles. Both follow the 1/N line. It is clear from the plot that the errors in all components except flux are approximately twice as large when convergence is allowed. The large deviation in fractional flux error when the number of counts is extremely low is likely due to the breakdown of the Gaussian approximation.
Paper: Forced Measurement of Astronomical Sources at Low Signal-to-noise
Authors: A. Dutta, J. R. Peterson, G. Sembroski
Figure caption: The figure on the left shows how the flux overestimation function f 1 is related to other image parameters. On the right, we show how the σ 2 overestimation function g 1 is related to other image parameters. The points in blue show the 4512 different cases we simulated to find the correction. The red curve is the piecewise linear interpolation. The black line shows the approximate analytical function in Equations (31) and (32).
Paper: Forced Measurement of Astronomical Sources at Low Signal-to-noise
Authors: A. Dutta, J. R. Peterson, G. Sembroski
Figure caption: Error adjustment factor for flux, i.e., p  N , is shown. This is the factor by which the error in flux presented in Section 2.1 needs to be adjusted. The adjustment factor is needed because the initial guess is the truth, and a single iteration is performed when using forced measurement. The red curve is the piecewise linear interpolation. The approximate logistic function is shown in Equation (36).