adsabs/AstroCLIMB huggingface dataset:
Paper: A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): Impact of Galaxies on the Circumgalactic Medium Metal Enrichment at z > 6 Using the JWST and VLT
Authors: Siwei Zou, Zheng Cai, Feige Wang, Xiaohui Fan, Jaclyn B. Champagne, Joseph F. Hennawi, Jan-Torge Schindler, Emanuele Paolo Farina, Jinyi Yang, Kohei Inayoshi, Eduardo Bañados, Sarah E. I. Bosman, Zihao Li, Xiaojing Lin, Yunjing Wu, Fengwu Sun, Ziyi Guo, Girish Kulkuarni, Mélanie Habouzit, Stephane Charlot, Jacopo Chevallard, Thomas Connor, Anna-Christina Eilers, Linhua Jiang, Xiangyu Jin, Koki Kakiichi, Mingyu Li, Romain A. Meyer, Fabian Walter, Huanian Zhang
Figure caption: We include the absorbing systems at z > 6.0 in Davies et al. (2023a) along the quasar sight lines J0226+0302, J0923+0402, and J0224–4711. The galaxies detected within 350 kpc and 1000 km s−1 of the absorbing gas are presented in the zoom-in red, green, and blue imaging boxes.
Paper: A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): Impact of Galaxies on the Circumgalactic Medium Metal Enrichment at z > 6 Using the JWST and VLT
Authors: Siwei Zou, Zheng Cai, Feige Wang, Xiaohui Fan, Jaclyn B. Champagne, Joseph F. Hennawi, Jan-Torge Schindler, Emanuele Paolo Farina, Jinyi Yang, Kohei Inayoshi, Eduardo Bañados, Sarah E. I. Bosman, Zihao Li, Xiaojing Lin, Yunjing Wu, Fengwu Sun, Ziyi Guo, Girish Kulkuarni, Mélanie Habouzit, Stephane Charlot, Jacopo Chevallard, Thomas Connor, Anna-Christina Eilers, Linhua Jiang, Xiangyu Jin, Koki Kakiichi, Mingyu Li, Romain A. Meyer, Fabian Walter, Huanian Zhang
Figure caption: SED fitting of all detected absorbing gas associated with galaxy candidates. The uncertainty is derived from the BEAGLE fitting results, taking into account the uncertainty when compared with the JAGUAR mock catalog (Williams et al. 2018).
Paper: A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): Impact of Galaxies on the Circumgalactic Medium Metal Enrichment at z > 6 Using the JWST and VLT
Authors: Siwei Zou, Zheng Cai, Feige Wang, Xiaohui Fan, Jaclyn B. Champagne, Joseph F. Hennawi, Jan-Torge Schindler, Emanuele Paolo Farina, Jinyi Yang, Kohei Inayoshi, Eduardo Bañados, Sarah E. I. Bosman, Zihao Li, Xiaojing Lin, Yunjing Wu, Fengwu Sun, Ziyi Guo, Girish Kulkuarni, Mélanie Habouzit, Stephane Charlot, Jacopo Chevallard, Thomas Connor, Anna-Christina Eilers, Linhua Jiang, Xiangyu Jin, Koki Kakiichi, Mingyu Li, Romain A. Meyer, Fabian Walter, Huanian Zhang
Figure caption: The fitting of the metal lines with a Voigt profile in the absorbing system z = 6.30443 toward quasar J0224–4711. Weak Mg II, C II, and Mg II (λ1260) lines are detected. The letters U and L represent the upper and lower limits on the column density measurement of the lines.
Paper: A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): Impact of Galaxies on the Circumgalactic Medium Metal Enrichment at z > 6 Using the JWST and VLT
Authors: Siwei Zou, Zheng Cai, Feige Wang, Xiaohui Fan, Jaclyn B. Champagne, Joseph F. Hennawi, Jan-Torge Schindler, Emanuele Paolo Farina, Jinyi Yang, Kohei Inayoshi, Eduardo Bañados, Sarah E. I. Bosman, Zihao Li, Xiaojing Lin, Yunjing Wu, Fengwu Sun, Ziyi Guo, Girish Kulkuarni, Mélanie Habouzit, Stephane Charlot, Jacopo Chevallard, Thomas Connor, Anna-Christina Eilers, Linhua Jiang, Xiangyu Jin, Koki Kakiichi, Mingyu Li, Romain A. Meyer, Fabian Walter, Huanian Zhang
Figure caption: All the absorbing related [O III]-emitting galaxy candidates.
Paper: JWST Observations Reject Unrecognized Crowding of Cepheid Photometry as an Explanation for the Hubble Tension at 8σ Confidence
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Color–magnitude diagrams (CMD) for the modules covering Cepheids. Each star is plotted using a small black point, while Cepheids are indicated by cyan symbols. A color cut in this space is included for NGC 1559, 0.3 < F090W−F150W < 1.15, corresponding to a broad range around the instability strip (0.5 < V−I < 1.7). For NGC 5643, which has large foreground extinction (E(V − I) = 0.21) the color range is shifted redward. The magnitudes and colors of non-Cepheids are based on the first visit. If a Cepheid is observed in only the first or in both visits, its location on the CMD is based on the first visit. Otherwise, it is based on the second visit.
Paper: JWST Observations Reject Unrecognized Crowding of Cepheid Photometry as an Explanation for the Hubble Tension at 8σ Confidence
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Example HST and JWST image stamps around Cepheids with P ∼ 40 days in all hosts. The top row shows the location of each Cepheid. HST filters are labeled in black while the JWST filters are in magenta.
Paper: JWST Observations Reject Unrecognized Crowding of Cepheid Photometry as an Explanation for the Hubble Tension at 8σ Confidence
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: JWST wave front sensing data during the interval of these observations, 2023 June–August. The wave front sensing, drifts, rectifications, and wave front errors are shown in the top three rows of panels. The bottom panel shows the change to encircled energy in the core of the PSF in the three filters used for this program. The dates of our observations are indicated as vertical dashed lines and a star symbol.
Paper: JWST Observations Reject Unrecognized Crowding of Cepheid Photometry as an Explanation for the Hubble Tension at 8σ Confidence
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: NIRCam fields superimposed on Digitized Sky Survey color images for four hosts (top) and NIRCam RGB images (F090W/F150W/F277W) showing positions of Cepheids (cyan circles) (bottom). North is up and east is to the left.
Paper: Passing Stars as an Important Driver of Paleoclimate and the Solar System’s Orbital Evolution
Authors: Nathan A. Kaib, Sean N. Raymond
Figure caption: (A) The standard deviation of Earth’s orbital eccentricity is plotted against time for 100 back-integrations of solar system clones. Three batches of solar system simulations include the Sun, its eight planets, Pluto, Ceres, Vesta, Pallas, Iris, and Bamberga. One batch includes no stellar perturbations (orange). Another also includes a passage of HD 7977 at t = −2.8 Myr at its median impact parameter of 13,200 au, as indicated by Gaia uncertainties (solid blue; Bailer-Jones 2022). The final batch includes a passage of HD 7977 at t = −2.8 Myr at 3900 au, the 5th percentile of possible impact parameters according to Gaia uncertainties (dashed blue; Bailer-Jones 2022). (B) The difference between the 98th and 2nd percentile of Earth’s orbital eccentricity vs. time among 100 back-integrations of solar system clones. The three batches of clones are the same as in the top panel.
Paper: Passing Stars as an Important Driver of Paleoclimate and the Solar System’s Orbital Evolution
Authors: Nathan A. Kaib, Sean N. Raymond
Figure caption: (A) The distribution of (s 4 − s 3)/(g 4 − g 3) is calculated for our isolated back-integrated systems (blue) and our back-integrated systems perturbed by a 3900 au flyby of HD 7977 at t = −2.8 Myr (orange). These ratios are calculated at t = −50 Myr (solid) and t = −60 Myr (dashed). (B) The distribution of maximum eccentricity values Earth attains between −55 Myr and −56 Myr is plotted for our isolated solar system realizations (blue) and our systems perturbed by a 3900 au flyby of HD 7977 at t = −2.8 Myr (orange).
Paper: Calcium Bright Knots and the Formation of Chromospheric Anemone Jets on the Sun
Authors: Kunwar Alkendra Pratap Singh, Keisuke Nishida, Kazunari Shibata
Figure caption: (a) The height–time plot, derived from calcium IIH filtergram images a selected region near the calcium bright knot. The rectangular box is the same as the one used for Figure 1(e). Velocities are shown with white ticks in the height–time plot. The observed height–time plot can be utilized for comparisons with MHD simulations. The very fast velocities indicated by dashed white lines are not real but apparent motion due to transversal motion of jets on the slit; (b) a simulated height–time plot, derived from 3D MHD modeling, of the jet using the density distribution; (c) a simulated height–time plot of the jet using the velocity distribution. The contours in the velocity distribution shows the velocities in units of kilometers per second. Both (b) and (c) correspond to x = 0.58 Mm, y = −0.47 Mm.
Paper: Calcium Bright Knots and the Formation of Chromospheric Anemone Jets on the Sun
Authors: Kunwar Alkendra Pratap Singh, Keisuke Nishida, Kazunari Shibata
Figure caption: The initial magnetic flux rope configuration along with the uniform, ambient magnetic field utilized in 3D MHD simulation. As time goes on, the initial magnetic flux rope configuration evolves dynamically during the upward rising and at some point in time the jets are formed.
Paper: Measuring Tracers of Planet Formation in the Atmosphere of WASP-77A b: Substellar O/H and C/H Ratios, with a Stellar C/O Ratio and a Potentially Superstellar Ti/H Ratio
Authors: Billy Edwards, Quentin Changeat
Figure caption: The deviation from stellar C/O ratio for each atmospheric study of WASP-77 A b when considering different stellar abundances. While it is no longer applicable in this case, we also show the comparison to solar abundances as these are the reference values if no stellar measurements have been made. Most studies prefer a substellar (blue squares) or stellar (whiter squares) C/O ratio. The exception is the CHIMERA retrievals from Line et al. (2021) although we note that they are consistent with all of the stellar values to 1σ due to the large uncertainties on the planetary C/O ratio.
Paper: Measuring Tracers of Planet Formation in the Atmosphere of WASP-77A b: Substellar O/H and C/H Ratios, with a Stellar C/O Ratio and a Potentially Superstellar Ti/H Ratio
Authors: Billy Edwards, Quentin Changeat
Figure caption: Comparison between the molecular abundances and elemental ratios found here for WASP-77A b and those found by literature works. No work has previously tried to constrain the Ti/H ratio, so it is not plotted here. We note that M/H refers to (C+O)/H for Line et al. (2021), M/H for August et al. (2023), and (C+O+Ti)/H for the atmospheric constraints from this work as well as the measurements of the enrichment of the host star, WASP-77A.
Paper: Measuring Tracers of Planet Formation in the Atmosphere of WASP-77A b: Substellar O/H and C/H Ratios, with a Stellar C/O Ratio and a Potentially Superstellar Ti/H Ratio
Authors: Billy Edwards, Quentin Changeat
Figure caption: Example extraction apertures when splitting the WFC3 data by the nondestructive reads from the reverse (top) and forward (bottom) scans. The extraction is clearly still contaminated by the fainter secondary star. When the light curve from this extraction is fitted, the spectrum closely matches that from Mansfield et al. (2022; see Figure 7), suggesting that their spectrum is still suffering from contamination.
Paper: Measuring Tracers of Planet Formation in the Atmosphere of WASP-77A b: Substellar O/H and C/H Ratios, with a Stellar C/O Ratio and a Potentially Superstellar Ti/H Ratio
Authors: Billy Edwards, Quentin Changeat
Figure caption: Comparison between different HST WFC3 G141 reductions. The contaminated fit from the extraction shown in Figure 6 matches the spectrum from Mansfield et al. (2022). The spectrum from Changeat et al. (2022), which used Wayne to model the contamination, has similar features but a different slope, being significantly deeper at longer wavelengths. Left: absolute eclipse depth. Right: relative eclipse depth having subtracted the mean depth.
Paper: Measuring Tracers of Planet Formation in the Atmosphere of WASP-77A b: Substellar O/H and C/H Ratios, with a Stellar C/O Ratio and a Potentially Superstellar Ti/H Ratio
Authors: Billy Edwards, Quentin Changeat
Figure caption: Comparison of the chemical equilibrium retrieval results when we allow the Ti/O ratio to vary (purple) and when we fix it to solar (yellow). The latter does not provide a good fit to the two highlighted regions, and our retrievals suggest the features in these regions are due to TiO.
Paper: Measuring Tracers of Planet Formation in the Atmosphere of WASP-77A b: Substellar O/H and C/H Ratios, with a Stellar C/O Ratio and a Potentially Superstellar Ti/H Ratio
Authors: Billy Edwards, Quentin Changeat
Figure caption: Best-fit model when jointly fitting the JWST NIRSpec data and HST WFC3 data from Mansfield et al. (2022). The residuals show a clear correlation, indicating a poor fit, which is likely due to the contamination present in the spectrum.
Paper: Tracing the Origins of Mass Segregation in M35: Evidence for Primordially Segregated Binaries
Authors: Erin Motherway, Aaron M. Geller, Anna C. Childs, Claire Zwicker, Ted von Hippel
Figure caption: Cumulative distribution functions of the (left) binary and single star population, (middle) different mass ranges of the single star sample, and (right) different mass ranges of the binary star sample. (For binaries, we use the primary mass of the system.) We also show a p-value in the left panel resulting from a K-S test between the binary and single star samples. Resulting p-values from K-S tests between the highest and lowest mass ranges for the middle and right panel are 7.79 × 10−3 and 3.44 × 10−5, respectively.
Paper: Tracing the Origins of Mass Segregation in M35: Evidence for Primordially Segregated Binaries
Authors: Erin Motherway, Aaron M. Geller, Anna C. Childs, Claire Zwicker, Ted von Hippel
Figure caption: Gaussian fits for M35 for stars within a 0.°5 radius from the cluster center. These fits for the RV (top), distance (middle), and PM (bottom) distributions are shown in pink, where vertical dotted lines represent the mean of the Gaussian fit. Dashed purple lines indicate the Gaussian fit to the field RV data (top) and a sixth-order polynomial fit to the field star distances (middle). Combined fits are represented by gray curves in the top and middle plots.
Paper: Tracing the Origins of Mass Segregation in M35: Evidence for Primordially Segregated Binaries
Authors: Erin Motherway, Aaron M. Geller, Anna C. Childs, Claire Zwicker, Ted von Hippel
Figure caption: Binary fraction with respect to distance from the cluster center. We plot the binary fraction for five equal-sized bins within 1.°75 from the cluster center. The binary fraction is calculated using all binaries and single stars in our sample, but is not corrected for incompleteness.
Paper: Tracing the Origins of Mass Segregation in M35: Evidence for Primordially Segregated Binaries
Authors: Erin Motherway, Aaron M. Geller, Anna C. Childs, Claire Zwicker, Ted von Hippel
Figure caption: Color–magnitude diagram of M35, including the entire sample we downloaded from the Gaia archive (light gray), BASE-9 identified cluster members (overplotted in black), and identified binaries (overplotted in colored symbols, indicating the mass ratio). With the red line, we show a PARSEC isochrone defined by the median cluster parameters found by BASE-9.
Paper: Tracing the Origins of Mass Segregation in M35: Evidence for Primordially Segregated Binaries
Authors: Erin Motherway, Aaron M. Geller, Anna C. Childs, Claire Zwicker, Ted von Hippel
Figure caption: Cumulative distribution functions of the binary and single star population of M35 for stars with t seg > 200  Myr. The p-value from a K-S test comparing both populations is also shown.
Paper: JWST Observations Reject Unrecognized Crowding of Cepheid Photometry as an Explanation for the Hubble Tension at 8σ Confidence
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Comparison of distances to the five SN Ia hosts measured with HST and JWST anchored by the same geometric distance reference, NGC 4258. The lower plot shows the differences in the measurements from the two telescopes. Black shows the comparison for the baseline system used to measure H 0, ﹩{W}_{V,I}^{H}﹩ and is the only system plotted on the top panel. Green and red shows comparisons with two JWST-only magnitude systems. The bottom plot shows a hypothetical, linear model of unrecognized crowding tuned to match the Hubble tension, 5log(73/67.5) = 0.17 mag at the mean distance of the SH0ES sample, μ = 31.7, a trend of 0.07 mag per magnitude of distance modulus beyond NGC 4258. This model is ruled out at 8.2σ.
Paper: JWST Observations Reject Unrecognized Crowding of Cepheid Photometry as an Explanation for the Hubble Tension at 8σ Confidence
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Comparison of Cepheid photometry in NGC 7250 in F115W. Gray shows photometry from HST F160W from Hoffmann et al. (2016) and R22, transformed to F115W using a synthetic relation, F160W = F115W+ 0.41 ± 0.05 + 0.49(F555W−F814W −1). Points in red are from our measurements of images from JWST Program 1995 (PI Freedman). The P–L relations are broadly consistent (JWST brighter than HST by 1.1σ). The JWST dispersion is a factor of 2 smaller than HST.
Paper: JWST Observations Reject Unrecognized Crowding of Cepheid Photometry as an Explanation for the Hubble Tension at 8σ Confidence
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Comparison between the standard (SH0ES: R22) dereddened magnitude m  H   W  period–magnitude relation used to measure distances to SN Ia hosts. The red points use JWST F150W (λ eff = 1.50 μm) and the gray points are from HST F160W (λ eff = 1.53 μm), including a small transformation F150W–F160W = 0.033 + 0.036[(V − I) − 1.0] to account for the differences in these passbands.
Paper: JWST Observations Reject Unrecognized Crowding of Cepheid Photometry as an Explanation for the Hubble Tension at 8σ Confidence
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Magnitude differences of two epochs for Cepheids in NGC 5643 in F090W (red points, left) and simulated (gray left and indicating phase, right). Gray density shows expected frequency of sampling based on random phase and template light curves. Red points are measurements from JWST and the errors do not include the crowding error which effectively cancels in the difference. The asymmetry of Cepheid light curves in F090W produces structure in this diagram that can be used to constrain the phase. The log of the time interval between epochs produces a negligible difference at a value of ﹩\mathrm{log}P\,=﹩ 1.34.
Paper: JWST Observations Reject Unrecognized Crowding of Cepheid Photometry as an Explanation for the Hubble Tension at 8σ Confidence
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption:  P–L relations for four new SN Ia hosts—NGC 1448 (top left), NGC 1559 (top center), NGC 5468 (bottom left), and NGC 5643 (bottom right)—and for the two galaxies presented in R23—NGC 4258 (bottom right) and NGC 5584 (bottom center). Relations are plotted from bluest (bottom) to least reddened (top). The bottom two relations in each panel are from HST while the others are from JWST. The top relation in each panel, plotted in black, is a dereddened or Wesenheit magnitude, F150W −0.72(F090W–F150W). Magnitude offsets are applied as indicated for ease of view and the dispersion for each P–L is given.
Paper: JWST Observations Reject Unrecognized Crowding of Cepheid Photometry as an Explanation for the Hubble Tension at 8σ Confidence
Authors: Adam G. Riess, Gagandeep S. Anand, Wenlong Yuan, Stefano Casertano, Andrew Dolphin, Lucas M. Macri, Louise Breuval, Dan Scolnic, Marshall Perrin, Richard I. Anderson
Figure caption: Relation between the F150W P–L fit residuals and crowding, as measured in JWST F150W frames as the difference between artificial star input and extraction. We find no dependence between these quantities. Red points and errors shown the mean results if dividing the sample in half. The mean level of crowding in NGC 4258 and the SN hosts are indicated by vertical lines. The scatter is evenly split as coming from phase uncertainty, crowding (at JWST resolution) with smaller contributions from the width of the instability strip.
Paper: Passing Stars as an Important Driver of Paleoclimate and the Solar System’s Orbital Evolution
Authors: Nathan A. Kaib, Sean N. Raymond
Figure caption: (A) The absolute difference in Earth’s orbital eccentricity between pairs of solar system clone integrations is plotted against time. One pair is integrated in complete isolation (blue line). In the other pairs (orange and black), one pair member includes the 25 km s−1 passage of a 1.4 M ⊙ star within 7200 au of the Sun at t = 10 Myr, but the other does not include this passage. One pair (black) also excludes the giant planets. (B) For the clone pairs including the giant planets, the absolute pair difference in the proper secular eccentricity precession frequency for each giant planet (g  j  in Equations (1) and (2)) is shown vs. time. Planets from the isolated clone pair (smaller, lighter symbols) and the stellar-perturbed pair (larger, darker symbols) are shown. (C) For the clone pairs including the giant planets, the absolute pair difference in the amplitude of the proper secular eccentricity precession frequency for each giant planet is shown vs. time. Planets from the isolated clone pair (smaller, lighter symbols) and the stellar-perturbed pair (larger, darker symbols) are shown. (D) For the clone pairs including the giant planets, the absolute pair difference in the phase of the proper secular eccentricity precession frequency for each giant planet is shown vs. time. Planets from the isolated clone pair (smaller, lighter symbols) and the stellar-perturbed pair (larger, darker symbols) are shown.
Paper: Passing Stars as an Important Driver of Paleoclimate and the Solar System’s Orbital Evolution
Authors: Nathan A. Kaib, Sean N. Raymond
Figure caption: The standard deviation of Earth’s orbital eccentricity is plotted against time for 100 back-integrations of solar system clones. Four batches of solar system simulations are run. Two only consider the Sun, its eight planets, and Pluto (blue lines), and the other two (orange lines) also include five large asteroids: Ceres, Vesta, Pallas, Iris, and Bamberga. Half of our batches also perturb the solar system with passing field stars (dashed lines), while the others do not include this perturbation (solid lines).
Paper: Passing Stars as an Important Driver of Paleoclimate and the Solar System’s Orbital Evolution
Authors: Nathan A. Kaib, Sean N. Raymond
Figure caption: (A) The absolute difference between the observed amplitude of Neptune’s proper secular eccentricity precession frequency and that measured in 100 integrations of solar system clones is plotted against the impulse gradient of the stellar encounter to which each clone is exposed. (B) The absolute difference between the Earth’s eccentricity in 100 solar system clone integrations and the median eccentricity is plotted against the impulse gradient of the stellar encounter to which each clone is exposed. Filled blue data points are for clones that contain all eight planets, while open red data points do not contain the giant planets. Earth eccentricities are measured ∼1 Myr after the stellar encounter in each integration.