adsabs/AstroCLIMB huggingface dataset:
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Integrated intensity (l–b; top) and Galactic longitude–velocity (l–v; bottom) maps of MCs in the G50 Perseus–Outer inter-arm spurs, with the intensity of all identified MCs shown in grayscale. The l–b and l–v maps are of the same field. The selected inter-arm MCs are the same as those indicated by the red crosses in the right panel of Figure 8, of which the masks are overlaid in random colors. The color scheme is the same in the top and bottom panels. Background intensities are in linear scale, with the maximum values of 73.5 K km s−1 and 872.3  K in the l–b and l–v maps, respectively. Intensities greater than the maxima are truncated for better visibility.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Same as Figure 12, but for the Outer and OSC arm segments. Due to insufficient samples in the OSC–G50 segment, the center and deviation of its Gaussian function are determined as the mean and deviation of zgal, respectively, weighted by the logarithm of mass.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Thickness (FWHM) as a function of height from the Galactic plane for different segments of the Galactic disk in regions G50 (diamonds) and G120 (crosses). The FWHMs and heights of each Galactic disk segment are obtained by fitting the MC height distribution shown in Figures 12 and 13. The segments around the Local arm (i.e., the Local–G120 and Local–G50 segments) are excluded because their thicknesses are not well determined. A linear fit is performed for all segments except the OSC–G50 segment, which has insufficient MC samples to determine height and thickness through Gaussian fitting. The fitting result is shown by a black solid line, and the corresponding linear function is indicated in the lower-right corner.
Paper: Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°
Authors: Xin Zhou, Ji Yang, Yan Sun, Qing-Zeng Yan, Lixia Yuan, Yang Su, Xuepeng Chen, Shaobo Zhang
Figure caption: Plan view of MC locations in the G120 and G50 regions from the northern Galactic pole. MC distances are estimated using the Galactic rotation curve and the full distance–probability density function method only for MCs with positive systemic velocity in the G50 region. The red dots mark the same selected MCs as those indicated by the red crosses in Figure 8. The Galactic center and the Sun are marked by black and blue stars, respectively. A blue dashed circle indicates the solar circle. The approximate positions of the spiral arms are shown.
Paper: The DELVE Quadruple Quasar Search. I. A Lensed Low-luminosity Active Galactic Nucleus
Authors: Paul L. Schechter, Dominique Sluse, Erik A. Zaborowski, Alex Drlica-Wagner, Cameron Lemon, Frederic Dux, Frederic Courbin, Angela Hempel, Martin Millon, Tommaso Treu, Raul Teixeira, Monika Adamów, Clecio R. Bom, Julio A. Carballo-Bello, Peter S. Ferguson, Robert A. Gruendl, David J. James, Clara E. Martínez-Vázquez, Pol Massana, Sidney Mau, Burçin Mutlu-Pakdil, Noëlia E. D. Noël, Andrew B. Pace, Joanna D. Sakowska, Guy S. Stringfellow, Erik J. Tollerud, A. Katherina Vivas, Alfredo Zenteno
Figure caption: NOT spectrum of the brightest quasar component A, extending from 3800 to 9000 Å. The high ionization lines of N V, C IV, and He II seen at z = 2.225 are narrow, with widths ranging from 1300 to 2000 km s−1, suggesting a type 2 AGN rather than a quasar.
Paper: The DELVE Quadruple Quasar Search. I. A Lensed Low-luminosity Active Galactic Nucleus
Authors: Paul L. Schechter, Dominique Sluse, Erik A. Zaborowski, Alex Drlica-Wagner, Cameron Lemon, Frederic Dux, Frederic Courbin, Angela Hempel, Martin Millon, Tommaso Treu, Raul Teixeira, Monika Adamów, Clecio R. Bom, Julio A. Carballo-Bello, Peter S. Ferguson, Robert A. Gruendl, David J. James, Clara E. Martínez-Vázquez, Pol Massana, Sidney Mau, Burçin Mutlu-Pakdil, Noëlia E. D. Noël, Andrew B. Pace, Joanna D. Sakowska, Guy S. Stringfellow, Erik J. Tollerud, A. Katherina Vivas, Alfredo Zenteno
Figure caption: A color composite representation of DELQQ 1258–0319 taken with DECam on the Blanco Telescope, using DES r, i, and z exposures (for blue, green, and red) taken as part of the DELVE survey. The approximate positions of four images subsequently labeled A, B, C, and D are shown in red with the symbols ∘, +, ∼, and ∣, respectively.
Paper: Identification of Outer Galaxy Cluster Members Using Gaia DR3 and Multidimensional Simulation
Authors: Vishwas Patel, Joseph L. Hora, Matthew L. N. Ashby, Sarita Vig
Figure caption: Interpreting complementary cumulative plot (plotting number of retained YSOs on increasing ﹩{ \mathcal M }{{ \mathcal C }}_{\mathrm{thr}}﹩), henceforth referred to as the Monte Carlo spectrum, for the field and member YSOs of the W4/W5 complex (Cluster 257). The kinematic distance estimate for this cluster is 2000 pc. The green curve illustrates the decrease in observed total cluster members with increasing threshold. The black curve represents the identified total cluster members for the simulated cluster. The blue dashed–dotted line and red curve depict the decline in simulated true members and false positives, respectively, with increasing threshold. The difference between identified total cluster members for the observed and simulated clusters is shown by the black dashed–dotted line in the residual plot. The faded gray lines represent the total identified cluster members for simulated clusters generated using an alternative set of parameters, with mean squared deviation (MSD) within three times the MSD of the best-fit black curve from the green plot. The yellow vertical dashed–dotted line represents the final determined Monte Carlo threshold (﹩{ \mathcal M }{{ \mathcal C }}_{\mathrm{thr}}=29,000﹩ for this cluster), where the simulated true members comprise 95% of the initial count.
Paper: TESS Photometry and LAMOST Spectroscopy of 10 Detached Eclipsing Binaries
Authors: Mengxin Wang, Hailong Yuan, Zhongrui Bai, Yiqiao Dong, Ming Zhou, Mingkuan Yang, Yuji He, Shuguo Ma, Xiaobin Zhang, Haotong Zhang
Figure caption: Panel (a) shows the 2 minute short cadence TESS observations from Sector 56 for TIC 369605666, along with the modeled quasi-sinusoidal signals obtained by using a GP approach. The red curve in the left-hand panel represents the modeled quasi-sinusoidal signal, and the black curve in the right-hand panel displays the phase-folded LCs after the GP method process. The abscissa of the left-hand panel is the epoch and the abscissa of the right-hand panel is the phase. Panel (b) presents a comparable scenario to panel (a), but it pertains to the 10 minute cadence TESS observations from Sectors 43, 44, and 45 for TIC 54759992.
Paper: Scaling K2. VIII. Short-period Sub-Neptune Occurrence Rates Peak Around Early-type M Dwarfs
Authors: Kevin K. Hardegree-Ullman, Galen J. Bergsten, Jessie L. Christiansen, Jon K. Zink, Sakhee Bhure, Kiersten M. Boley, Rachel B. Fernandes, Steven Giacalone, Preethi R. Karpoor
Figure caption: Planet occurrence rates as a function of stellar temperature for short-period (P = 1–40 days) super-Earths (green squares) and sub-Neptunes (blue circles). A power law was fit to the super-Earths, and a double broken power law was fit to the sub-Neptunes, showing two breaks: ﹩{T}_{{\rm{Br}},{\rm{1}}}=375{0}_{-97}^{+153}﹩ K and ﹩{T}_{{\rm{Br}},{\rm{2}}}=575{8}_{-145}^{+94}﹩ K. The short-period sub-Neptunes peak around a host type of M0.5 V, then decrease in planet occurrence toward cooler M dwarfs. G- and K-type stars have comparable rates of short-period super-Earths and sub-Neptunes. Another noticeable decrease in sub-Neptunes happens for host stars hotter than the Sun. Short-period super-Earths increase in occurrence toward cooler stars, with no discernible peak in the host-star temperatures for which we have data from Kepler and K2.
Paper: Scaling K2. VIII. Short-period Sub-Neptune Occurrence Rates Peak Around Early-type M Dwarfs
Authors: Kevin K. Hardegree-Ullman, Galen J. Bergsten, Jessie L. Christiansen, Jon K. Zink, Sakhee Bhure, Kiersten M. Boley, Rachel B. Fernandes, Steven Giacalone, Preethi R. Karpoor
Figure caption: Comparison of Kepler+K2 planet occurrence rates to formation model planet occurrence rates from (top panel) G. D. Mulders et al. (2021), (middle panel) R. Burn et al. (2021), and (lower panel) M. Pan et al. (2025). Kepler+K2 occurrence rates were calculated at either the same, or as close as possible to the limits specified by each model. A scaling factor of 7 and 4.5 were applied to the models from G. D. Mulders et al. (2021) and M. Pan et al. (2025), respectively, in order to roughly match the peak of the models to the peak in the K2+Kepler occurrence rates. The models were also originally in terms of host-star mass and were converted to a host-star effective temperature using an updated version of Table 5 from M. J. Pecaut & E. E. Mamajek (2013). Qualitatively, the models loosely follow the trends seen from observations. Our new planet occurrence rates can help guide further planet-formation modeling efforts to more accurately reflect the observed population.
Paper: Scaling K2. VIII. Short-period Sub-Neptune Occurrence Rates Peak Around Early-type M Dwarfs
Authors: Kevin K. Hardegree-Ullman, Galen J. Bergsten, Jessie L. Christiansen, Jon K. Zink, Sakhee Bhure, Kiersten M. Boley, Rachel B. Fernandes, Steven Giacalone, Preethi R. Karpoor
Figure caption: (Left) Period and radius diagram and (right) incident flux and radius diagram of the combined Kepler (no outline) and K2 planet candidates (black outlined points) orbiting FGKM stars used for our analysis. The dotted lines are the fit to the partition between super-Earths and sub-Neptunes from a KDE fit to the radius valley (Equation (1)), with the shaded region highlighting the uncertainties from a 1000 bootstrap resampling of the planet population. Super-Earths are shown as green squares below the lines, and sub-Neptunes are shown as blue circles above the lines. The dark shaded regions behind the points highlight the density of exoplanets in the respective phase space. We note that we have not corrected for detection completeness in these plots. The corresponding parameters of the planet sample are provided in Tables 6 and 7.
Paper: TESS Photometry and LAMOST Spectroscopy of 10 Detached Eclipsing Binaries
Authors: Mengxin Wang, Hailong Yuan, Zhongrui Bai, Yiqiao Dong, Ming Zhou, Mingkuan Yang, Yuji He, Shuguo Ma, Xiaobin Zhang, Haotong Zhang
Figure caption: Spectral fitting of TIC 189069314 was performed using LAMOST-MRS spectra. The blue-end spectral fitting is shown in the upper panel, and the red-end one is in the lower panel. The magenta line indicates the observed spectrum, and the black line is the synthetic template. The green and blue dashed lines highlight, respectively, the positions of the Mg b triplet and Hα absorption lines at various RVs within the synthetic templates. For better clarity, the upper panel covers a wavelength range from 5150 to 5220 Å. The local modified Julian minutes (LMJMs) of each exposure recorded by LAMOST and the corresponding orbital phase are marked in the lower right corner of each figure frame.
Paper: TESS Photometry and LAMOST Spectroscopy of 10 Detached Eclipsing Binaries
Authors: Mengxin Wang, Hailong Yuan, Zhongrui Bai, Yiqiao Dong, Ming Zhou, Mingkuan Yang, Yuji He, Shuguo Ma, Xiaobin Zhang, Haotong Zhang
Figure caption: LCs and spectroscopic orbit models are provided for objects TIC 189069314 and 54759992. Each panel is presented in three parts: from top to bottom, the phase-folded RVs for the primary and secondary components (depicted by filled circles) are displayed with the best-fitting spectroscopic orbit model for both components (illustrated by solid and dashed lines, respectively). The middle part highlights the phase-folded LC (represented by blue dots) together with the optimal LC model (denoted by the black line). The bottom part illustrates the LC fitting residuals.
Paper: Scaling K2. VIII. Short-period Sub-Neptune Occurrence Rates Peak Around Early-type M Dwarfs
Authors: Kevin K. Hardegree-Ullman, Galen J. Bergsten, Jessie L. Christiansen, Jon K. Zink, Sakhee Bhure, Kiersten M. Boley, Rachel B. Fernandes, Steven Giacalone, Preethi R. Karpoor
Figure caption: Hertzsprung–Russell diagrams of the Kepler (left), K2 (middle), and combined Kepler and K2 stellar populations (right) from T. A. Berger et al. (2020a) and K. K. Hardegree-Ullman et al. (2020; top) and our new uniform stellar classification (bottom). Stars in orange are M dwarfs based on temperature and absolute magnitude. The top panels highlight the original stellar parameter differences due to different methodologies and target populations. Most of the original K2 M dwarfs from K. K. Hardegree-Ullman et al. (2020) have temperatures near 3700 K due to the input training set limitations, which is mitigated with the new temperature derivation. It is clear that the Kepler mission was focused on Sun-like main-sequence stars, but the guest-driven K2 mission more broadly sampled a wider population of F, G, K, and M stars. K2 notably observed nine times more M dwarfs than Kepler.
Paper: Scaling K2. VIII. Short-period Sub-Neptune Occurrence Rates Peak Around Early-type M Dwarfs
Authors: Kevin K. Hardegree-Ullman, Galen J. Bergsten, Jessie L. Christiansen, Jon K. Zink, Sakhee Bhure, Kiersten M. Boley, Rachel B. Fernandes, Steven Giacalone, Preethi R. Karpoor
Figure caption: Histograms of Kepler (orange) and K2 (blue) super-Earth and sub-Neptune host-star effective temperatures used in this study. While comparable total numbers of super-Earth and sub-Neptune candidates were found orbiting M dwarfs (Teff ≲ 4000 K) in both Kepler and K2, it is worth noting that for Teff < 3700 K, there are 3.5 times more K2 candidates than Kepler candidates (see inset plot).
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: This flowchart illustrates the process of identifying extinction-jump points in a D–A diagram using the CU-JADE method. The process is demonstrated through a simple example with two jump points. Initialization: Begin with a set of simulated stellar samples exhibiting two jump points on the D–A diagram (subplot (a)). These jump points are indicated by blue lines. CUSUM Statistic Calculation: Compute the CUSUM statistic S to locate the first jump point (Step 1). Subplot b shows the CUSUM curve, where black points represent binned stellar samples at intervals of 20 pc, and the red curve represents the calculated CUSUM values using Equation (3). The position with the maximum S value, marked by a red star, identifies the first jump point. Validity check: Determine if the first jump point is valid (Step 2). This involves calculating the Sdiff value and comparing it to the Sdiff background (see Section 3.2 for details). Subplots (c) and (d) illustrate this comparison using percentile, similar to a confidence level, with a parameter C for adjustment. Splitting and recalculation: If the first jump point is confirmed, split the D–A data at this position (Step 3, see subplots (b) and (e)). Recalculate the separate data sets and repeat the process, as indicated by the dashed arrow. This begins the traversal of all extinction-jump points (suggested by bulges on the CUSUM curve). Final jump point identification: Since only two jump points were initially set, the next round of calculations locates the last jump point (Step 4, subplot (f)). The process enables us to return all detected jump point positions (Step 5). Validation: Compare and check the detected jump point positions against the preset positions (Step 6, subplots (g) and (a)).
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: A 2D histogram illustrating ΔAV weighted extinction jumps is presented in polar coordinates. The map has been smoothed using a uniform filter in Scipy with a kernel size of 3. The blue sector represents Cepheus, and the orange sector is Cygnus. Yellow squares with error bars represent masers, the data for which is sourced from M. J. Reid et al. (2019). Red circles with error bars denote YOCs from E. L. Hunt & S. Reffert (2023). The light yellow belts delineate the kpc-scale linear structures (e.g., the Split, the Radcliffe Wave, and the Cepheus spur in R. Lallement et al. 2019; J. Alves et al. 2020; M. Pantaleoni González et al. 2021), while the red (the Mon-Gem superbubble and Carina superbubble) and green (J. L. Vergely et al. 2022) ellipses show large-scale cavities where dust is scarce. For more top-down views along different latitude slices, please refer to the Table 2 catalog or at doi:10.57760/sciencedb.24650.
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: CfA 12CO and extinction map toward the Cepheus region. Panel (a) depicts the extinction between 200 and 500 pc using a colormap, while contours show the smoothed integrated intensity of 12CO emission within the LSR velocity range of −6 to 15 km s−1. Panel (b) is similar to panel (a) but focuses on the distance range in (500, 1500) pc and LSR velocities in (−20, −6) km s−1. Panel (c) is similar to panel (a) but presents data for distances in (1500, 3000) pc and LSR velocity in (−45, −20) km s−1. Red circles indicate regions where extinction jumps were detected in right panels (d), (e), and (f). Vertical lines represent the distances of detected extinction jumps with uncertainties in D–A plots. Gray dots are raw stellar data points, binned every 50 pc with black lines. Blue text and horizontal lines denote the mean extinction value after accounting for extinction jumps. Orange curves are binned radial velocities of stars from the Gaia DR3.
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: The sky map displays the distances corresponding to the largest ΔAV component along the LoS in a Mollweide view. Some well-studied regions are indicated on the map. It should be noted that the values are likely to represent the MCs’ distances, but they could also correspond to other components superimposed on them. For the slices (every 200 pc) and integrated extinctions map for 0–4 kpc, please check the catalog in Table 2 or at doi:10.57760/sciencedb.24650.
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: For the case far from the Cygnus Rift, we show four examples with good matches between extinction and the integrated intensity of MWISP 12CO, and continuous distances for their structures. The colormap represents the distance of the strongest extinction component within a given distance interval along the LoS, and the colorbar shows the interval for distance measurement. Thin black contours ([0.5, 0.6, 0.7, 0.8, 0.9, 1.0] mag labeled in line) indicate the cumulative value of the extinction within this interval, outlining the structures with strong extinction in this region. Thick yellow contours represent the 12CO emission ([5, 15, 25, 35, 45] K km s−1), with the integrated velocity range and the determined distance at the top of the figure.
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: Face-on maps from different star catalogs/techniques. Panels (a) and (b) present Polar coordinate dust maps of ZGR23. Panel (a) is produced by our method, and panel (b) is generated using a simple spatial binning technique as outlined by X. Zhang et al. (2023). Panel (c) is reproduced in Cartesian coordinates from the map in Section 5.1.1. Panel (d) is from J. L. Vergely et al. (2022), using a hierarchical-inversion technique and two merged star catalogs.
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: Overlay of the identified MWISP 13CO cloud structures (white contours) within 1.1 kpc (clouds in the Cygnus Rift from S. Zhang et al. 2024) based on the extinction jumps detected within 1.1 kpc. The colormap shows the distance of the largest extinction in the distance interval, and the thick black contours delineate the integrated extinction in [1, 2] mag. The dashed ellipse denotes the “800 pc loop” identified in S. Zhang et al. (2024). The rectangles indicate areas for further distance measurements in the following.
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: An illustration of our multi-extinction-jump model (here in Mode I, C = 3 for the left column, C = 1 for the middle and right columns) applied to the mock data. Different rows set the jump points number from 1 to 6, with distances at ﹩\left[300,700,1200,1800,2500,3300\right]\,{\mathrm{pc}}﹩, respectively. The three columns mirror different LoS extinction properties (see the text). Gray dots are the produced mock data and black dots are binned values every 20 pc.
Paper: CU-JADE: A Method for Traversing Extinction Jumps Along the Line of Sight
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Fujun Du, Shaobo Zhang, Qing-Zeng Yan, Xin Liu, Miaomiao Zhang, Yan Sun, Ji Yang
Figure caption: The distance correspondence between parallaxes from masers and those derived from our multi-extinction-jump model. Orange triangles highlight masers in the Cygnus region, while blue triangles represent those outside the Cygnus region.
Paper: OGLE-2014-BLG-1760: A Jupiter–Sun Analogue Residing in the Galactic Bulge
Authors: Natalia E. Rektsini, Clément Ranc, Naoki Koshimoto, Jean-Philippe Beaulieu, David P. Bennett, Andrew A. Cole, Sean K. Terry, Aparna Bhattacharya, Étienne Bachelet, Ian A. Bond, Andrzej Udalski, Joshua W. Blackman, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: Left panel: Jackknife stack of 20 science frames of the 2020 August Keck OSIRIS Kp band follow-up observation. Upper right panel: Close-up (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩38 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩38) frame of the source (star 1), the lens (star 2), and the third star (star 3), which is unrelated to the event. Lower right panel: Close-up (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩38 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩38) of the three-star PSF fit residual using DAOPHOT.