adsabs/AstroCLIMB huggingface dataset:
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 11072. The positions of components are shown on the H-R diagram with evolutionary tracks and the 3.981 Gyr isochrone with Z = 0.019.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 4239. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 1.413 Gyr isochrone with Z = 0.019.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 111805. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 3.548 Gyr isochrone with Z = 0.008.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 89234. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 1.413 Gyr isochrone with Z = 0.03.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 17895. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 1.778 Gyr isochrone with Z = 0.019.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 51255. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 7.08 Gyr isochrone with Z = 0.019.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 54611. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 1.259 Gyr isochrone with Z = 0.019.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: The structures of the 17 systems are analyzed here. Green circles denote subsystems designated as primary, secondary, or parent, while orange circles denote individual stars.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 12548. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 5.012 Gyr isochrone with Z = 0.03.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Synthetic SED diagrams for the eight triple systems. The three dotted and dashed lines are the synthetic SEDs from the individual stars, while the black line is the sum of the individual SEDs (composed). The blue points are the calculated flux density using the measured blue Johnson magnitude, and the green points are the calculated flux density using the measured visual Johnson magnitude (from Hipparcos ESA 1997).
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Synthetic SED diagrams for the nine quadruple systems. The four dotted and dashed lines are the SEDs from the individual stars, while the black line is the sum of the individual SEDs (composed). The blue points are the calculated flux density using the measured blue Johnson magnitude, and the green points are the calculated flux density using the measured visual Johnson magnitude (from Hipparcos ESA 1997).
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 19915. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 6.31 Gyr isochrone with Z = 0.008.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 28614. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 0.5012 Gyr isochrone with Z = 0.019.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 78977. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 3.612 Gyr isochrone with Z = 0.019.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Comparison between the dynamical parallax calculated in this work and the Hipparcos 2 (red), Gaia DR2 (blue), Gaia DR3 (green), dynamical (magenta), and Gaia DR1 (yellow) parallaxes (only for HIP 25240). The line represents y = x.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 5588. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 1 Gyr isochrone with Z = 0.019.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Best quadratic curve fitting as the MLR for the whole sample compared to the linear MLRs of Eker et al. (2015).
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 51966. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 7.08 Gyr isochrone with Z = 0.008.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 41171. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 1.259 Gyr isochrone with Z = 0.019.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 22607. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 1.122 Gyr isochrone with Z = 0.019.
Paper: Atmospheric and Fundamental Parameters of the Individual Components of Multiple Stellar Systems
Authors: Enas M. Abu-Alrob, Abdallah M. Hussein, Mashhoor A. Al-Wardat
Figure caption: Analysis for HIP 25240. The positions of the components are shown on the H-R diagram with evolutionary tracks and the 1.259 Gyr isochrone with Z = 0.03.
Paper: High-resolution Observations of H I in the IC 63 Reflection Nebula
Authors: Lars Bonne, B-G Andersson, Robert Minchin, Archana Soam, Joshua Yaldaei, Kristin Kulas, Janik Karoly, Lewis B. G. Knee, Siddharth Kumar, Nirupam Roy
Figure caption: The average H I emission profile of the ring as a function of the offset from the center of the ring with a Gaussian profile fitted to it (red dashed line). The error bars indicate the standard deviation of the emission over the ring at each offset.
Paper: Observing Atmospheric Escape in Sub-Jovian Worlds with JWST
Authors: Leonardo A. Dos Santos, Munazza K. Alam, Néstor Espinoza, Shreyas Vissapragada
Figure caption: Theoretical (red) and observable (black) metastable He transmission spectra of GJ 436 b assuming a substellar escape rate of 108 g s−1 and an outflow temperature of 2700 K.
Paper: High-resolution Observations of H I in the IC 63 Reflection Nebula
Authors: Lars Bonne, B-G Andersson, Robert Minchin, Archana Soam, Joshua Yaldaei, Kristin Kulas, Janik Karoly, Lewis B. G. Knee, Siddharth Kumar, Nirupam Roy
Figure caption: Left: the ring seen in the moment 0 map from the combined cube with contours from 0.1 to 0.225 Jy km s−1 in steps of 0.025 Jy km s−1. Center: the same field in the moment 0 map from the WSRT data with the contours from the combined cube overlaid. Right: the same field in the moment 0 map from the GMRT data with the contours from the combined cube overlaid. These plots show that the ring is seen in both interferometric data sets and so is not an artifact from a single telescope that has propagated into our combined cube. They also reveal that there appears to be some substructure in the ring.
Paper: Observing Atmospheric Escape in Sub-Jovian Worlds with JWST
Authors: Leonardo A. Dos Santos, Munazza K. Alam, Néstor Espinoza, Shreyas Vissapragada
Figure caption: High-energy SED incident on GJ 436 b and GJ 1214 b taken from the MUSCLES database and scaled to the semimajor axis of the planets.
Paper: High-resolution Observations of H I in the IC 63 Reflection Nebula
Authors: Lars Bonne, B-G Andersson, Robert Minchin, Archana Soam, Joshua Yaldaei, Kristin Kulas, Janik Karoly, Lewis B. G. Knee, Siddharth Kumar, Nirupam Roy
Figure caption: Left: the different paths that were defined over the H I ring-like feature on top of the H I integrated intensity map. Right: the H I emission profiles over the ring for the eight individual paths defined on the left.
Paper: Observing Atmospheric Escape in Sub-Jovian Worlds with JWST
Authors: Leonardo A. Dos Santos, Munazza K. Alam, Néstor Espinoza, Shreyas Vissapragada
Figure caption: Upper panels: structure of the upper atmosphere of GJ 436 b (left) and GJ 1214 b (right). The circles represent the sonic point of the outflow. Lower panels: distribution of ionized singlet, and triplet He nuclei in the upper atmosphere of GJ 436 b (left) and GJ 1214 b (right).
Paper: High-resolution Observations of H I in the IC 63 Reflection Nebula
Authors: Lars Bonne, B-G Andersson, Robert Minchin, Archana Soam, Joshua Yaldaei, Kristin Kulas, Janik Karoly, Lewis B. G. Knee, Siddharth Kumar, Nirupam Roy
Figure caption: Left: the moment zero map for IC 63 between −2.5 and 4.5 km s−1 obtained using the MEM reduction technique. Right: the same using the CLEAN reduction technique, showing a similar clumpy morphology.
Paper: High-resolution Observations of H I in the IC 63 Reflection Nebula
Authors: Lars Bonne, B-G Andersson, Robert Minchin, Archana Soam, Joshua Yaldaei, Kristin Kulas, Janik Karoly, Lewis B. G. Knee, Siddharth Kumar, Nirupam Roy
Figure caption: The average H I spectrum obtained from inside the ring at the tip of IC 63. As expected the noise is fairly high, making it challenging to conclude on the presence of self absorption.
Paper: Contamination in TESS Light Curves: The Case of the Fast Yellow Pulsating Supergiants
Authors: May G. Pedersen, Keaton J. Bell
Figure caption: Median TPF flux of TESS sector 34 for the YSG star HD 269953 (TIC 404850274; red star) and positions of three nearby contaminating stars shown in gray, pink, and blue. These points mark the average locations obtained for each signal across 23 sectors, with error bars representing 3 σ std. Bottom panels provide the first half of each extracted light curve (left; corresponding to one spacecraft orbit) and associated periodograms (right) for the five different pixel masks indicated in the top panel. The frequency values of the three independent signals identified by DW20 based on the SPOC PDCSAP light curves (yellow) are shown by vertical dashed lines in the periodograms. See text for further details.
Paper: Contamination in TESS Light Curves: The Case of the Fast Yellow Pulsating Supergiants
Authors: May G. Pedersen, Keaton J. Bell
Figure caption: Position of the 17 FYPS stars in the HR diagram (top) and their dominant frequency f 0 reported by DW22 as a function of effective temperature (bottom). Blue circles indicate LMC stars, whereas orange triangles correspond to SMC stars. Example evolutionary tracks computed with MESA for LMC composition (see Appendix A) are shown by black lines, with the corresponding evolution of the acoustic cutoff frequency shown in the bottom panel. Different line styles correspond to different initial stellar masses as indicated by the legend. The combined predicted excited frequency ranges for a 20 and 25 M ⊙ star from Figure 5 of Saio et al. (2013) at solar metallicity are shown as a function of ﹩\mathrm{log}{T}_{\mathrm{eff}}﹩ for pre-RSG (hatched gray) and post-RSG (light gray) evolution, respectively.
Paper: Contamination in TESS Light Curves: The Case of the Fast Yellow Pulsating Supergiants
Authors: May G. Pedersen, Keaton J. Bell
Figure caption: Median TPF flux of TESS sector 28 for the YSG star HD 268687 (TIC 29984014; red star) and position of a nearby contaminating star indicated by the white cross. Bottom panels show the extracted light curve (left), the phase folded light curves using ﹩\tfrac{1}{6}{f}_{0}=0.460877﹩ day−1 (center), and the periodograms (right) for the three different pixel masks indicated in the top panel. The f 0 value of the the highest-amplitude independent signal identified by DW22 based on the SPOC aperture (yellow) is shown by vertical dashed line in the periodograms.
Paper: Contamination in TESS Light Curves: The Case of the Fast Yellow Pulsating Supergiants
Authors: May G. Pedersen, Keaton J. Bell
Figure caption: Median TPF flux of TESS sector 28 for the YSG star HD 269787 (TIC 276863889, red star) and position of a nearby contaminating star indicated by the white cross. Bottom panels show the extracted light curve (left), the phase folded light curves using f 0 = 0.90868 day−1 (center), and the periodograms (right) for the three different pixel masks indicated in the top panel. The f 0 value of the the highest-amplitude independent signal identified by DW22 based on the SPOC light curves (yellow) is shown by the vertical dashed line in the periodograms.
Paper: Contamination in TESS Light Curves: The Case of the Fast Yellow Pulsating Supergiants
Authors: May G. Pedersen, Keaton J. Bell
Figure caption: Light curves from the left-hand panels of Figure 2 phase folded by one half of the three independent frequencies 1.174 day−1 (left), 1.335 day−1 (center), and 1.593 day−1 (right) identified by DW20 for HD 269953, and corresponding to the three vertical dashed lines in the right-hand panels of Figure 2. The black dotted curves show the average flux calculated in 0.05 phase bins. We note again that DW22 had already found 1.174 day−1 and 1.593 day−1 to originate from nearby contaminants.
Paper: Contamination in TESS Light Curves: The Case of the Fast Yellow Pulsating Supergiants
Authors: May G. Pedersen, Keaton J. Bell
Figure caption: Phase-binned light curves of OGLE LMC-ECL-1544 using the 2 minute cadence TESS data (top panel; aame as bottom center panel of Figure 4), and the OGLE V (middle) and I (bottom) band photometry (Udalski et al. 1997; Szymanski 2005). The light curves were phases folded assuming ﹩{f}_{\mathrm{orb}}=\tfrac{1}{6}{f}_{0}=0.460877﹩ day−1. The black curves show the average flux in 0.01 (top), 0.02 (middle), and 0.01 (bottom) phase bins.
Paper: Observing Atmospheric Escape in Sub-Jovian Worlds with JWST
Authors: Leonardo A. Dos Santos, Munazza K. Alam, Néstor Espinoza, Shreyas Vissapragada
Figure caption: Posterior distributions of substellar mass-loss rate and outflow temperature of GJ 436 b in a mock retrieval with p-winds. The injected truth is shown as the blue cross-hair.
Paper: Observing Atmospheric Escape in Sub-Jovian Worlds with JWST
Authors: Leonardo A. Dos Santos, Munazza K. Alam, Néstor Espinoza, Shreyas Vissapragada
Figure caption: Theoretical (red) and observable (black) metastable He transmission spectra of GJ 1214 b assuming a substellar escape rate of 1.9 × 1010 g s−1 and an outflow temperature of 2700 K based on the self-consistent models of Salz et al. (2016).
Paper: Observing Atmospheric Escape in Sub-Jovian Worlds with JWST
Authors: Leonardo A. Dos Santos, Munazza K. Alam, Néstor Espinoza, Shreyas Vissapragada
Figure caption: Metastable He transmission spectra of GJ 1214 b simulated for NIRSpec/G140H, G140M and NIRISS/SOSS.
Paper: Contamination in TESS Light Curves: The Case of the Fast Yellow Pulsating Supergiants
Authors: May G. Pedersen, Keaton J. Bell
Figure caption: SAP (top panels; gray) and PDCSAP (middle panels; black) light curves of BZ Tuc for the two available 2 minutes cadence sectors. The bottom panels show the periodogram of PDCSAP and SAP light curves with the f 0 signal indicated by the dashed red line. Due to the different amplitude scales of the PDCSAP and SAP periodograms, the SAP amplitudes are shown in gray on the right-hand sides of both bottom subplots in units of ppt.
Paper: Contamination in TESS Light Curves: The Case of the Fast Yellow Pulsating Supergiants
Authors: May G. Pedersen, Keaton J. Bell
Figure caption: TESS localization result for BZ Tuc (TIC 267547804), showing that the f 0 signal identified by DW22 coincides with the position of the YSG on the TPF. Positions of nearby Gaia sources brighter than 17 mag are also shown.
Paper: High-resolution Observations of H I in the IC 63 Reflection Nebula
Authors: Lars Bonne, B-G Andersson, Robert Minchin, Archana Soam, Joshua Yaldaei, Kristin Kulas, Janik Karoly, Lewis B. G. Knee, Siddharth Kumar, Nirupam Roy
Figure caption: Left: the H I intensity map of IC 63 that is obtained from the background-subtracted data cube. The white box outlines the zoomed-in region presented on the right. The red lines indicate the three legs visible in H I that are connected to the tip of IC 63 with their names. Right: a zoom into the brightest region of H I intensity map with the [C II] intensity contours overlaid (starting at 10−4 erg s−1 cm−2 sr−1 with increments of 5×10−5 erg s−1 cm−2 sr−1). The red circle highlights the circular morphology seen in H I toward the tip of IC 63. The white arrow indicates the direction of the incident radiation from γ Cas. The full white circle indicates the 15″ beam size of the H I data.
Paper: High-resolution Observations of H I in the IC 63 Reflection Nebula
Authors: Lars Bonne, B-G Andersson, Robert Minchin, Archana Soam, Joshua Yaldaei, Kristin Kulas, Janik Karoly, Lewis B. G. Knee, Siddharth Kumar, Nirupam Roy
Figure caption: Left: the geometry of a simple model to estimate whether the observed H I ring is the projection of a spherical ring (see Equations (2) and (3)). In this specific schematic presentation, S corresponds to the path length through the center of the shell (S cent). If we assume that all of the H I emission is optically thin, we can compare the geometric ratio of ring size and rim/shell thickness with the ratio of the related brightness temperatures. The observed ring radius is Δ = 25.″2 and the shell thickness (FWHM) yields δ = 22.″1. Right: the observed intensity ratio could be recovered from this model if we assume that the shell is anisotropic, and/or that the center of the region is filled with cold, self-absorbing (HISA) gas.
Paper: High-resolution Observations of H I in the IC 63 Reflection Nebula
Authors: Lars Bonne, B-G Andersson, Robert Minchin, Archana Soam, Joshua Yaldaei, Kristin Kulas, Janik Karoly, Lewis B. G. Knee, Siddharth Kumar, Nirupam Roy
Figure caption: The difference in central velocity of the emission in [C II] (Caputo et al. 2023, submitted) and H I at the locations where both lines are detected. The black contours indicate the integrated [C II] emission starting at 10−4 erg s−1 cm−2 sr−1 with increments of 5 × 10−5 erg s−1 cm−2 sr−1.
Paper: High-resolution Observations of H I in the IC 63 Reflection Nebula
Authors: Lars Bonne, B-G Andersson, Robert Minchin, Archana Soam, Joshua Yaldaei, Kristin Kulas, Janik Karoly, Lewis B. G. Knee, Siddharth Kumar, Nirupam Roy
Figure caption: Left: the H I moment zero map for IC 63 with the colored arrows indicating the cuts that were made to construct position–velocity (PV) diagrams on the right. Right: the H I PV diagrams along the axes/arrows indicated in the figure on the left. The contours indicate the corresponding [C II] PV diagrams starting at 2 K with increments of 2 K. The darkest contours indicate the weakest emission and the white contour indicates the brightest emission.
Paper: High-resolution Observations of H I in the IC 63 Reflection Nebula
Authors: Lars Bonne, B-G Andersson, Robert Minchin, Archana Soam, Joshua Yaldaei, Kristin Kulas, Janik Karoly, Lewis B. G. Knee, Siddharth Kumar, Nirupam Roy
Figure caption: Left: H I integrated intensity map (without background subtraction) of the IC 63 region. The yellow and magenta boxes indicate the regions used to make an average spectrum for background subtraction. The black box indicates the region associated with IC 63. Right: the spectra from the corresponding colored boxes on the left after background subtraction. The emission from IC 63 (black) has a clearly defined profile while the background regions (yellow and magenta) are relatively close to the baseline.
Paper: High-resolution Observations of H I in the IC 63 Reflection Nebula
Authors: Lars Bonne, B-G Andersson, Robert Minchin, Archana Soam, Joshua Yaldaei, Kristin Kulas, Janik Karoly, Lewis B. G. Knee, Siddharth Kumar, Nirupam Roy
Figure caption: Channel maps between –4.3 and 7.7 km s−1 of the IC 63 region in steps of ∼0.8 km s−1.
Paper: High-resolution Observations of H I in the IC 63 Reflection Nebula
Authors: Lars Bonne, B-G Andersson, Robert Minchin, Archana Soam, Joshua Yaldaei, Kristin Kulas, Janik Karoly, Lewis B. G. Knee, Siddharth Kumar, Nirupam Roy
Figure caption: Coverage of the UV plane for the IC 63 observations by the different observatories. Blue is GMRT, red is WSRT, and yellow is CGPS.
Paper: A Measurement of the Kuiper Belt’s Mean Plane From Objects Classified By Machine Learning
Authors: Ian Matheson, Renu Malhotra
Figure caption: Kuiper Belt mean plane and its confidence ellipses in the (q, p) plane, by semimajor axis bin. Semimajor axis bins are (a) 35–40.3 au, (b) 40.3–42 au, (c) 42–43 au, (d) 43–44 au, (e) 44–45 au, (f) 45–48 au, (g) 45–50 au, (h) 50–80 au, and (i) 50–150 au. The best-fit mean plane is the dark green +. The mean planes of 40,000 Monte Carlo samples are in light green, and the 68.2%, 95.4%, and 99.7% covariance ellipses for them are in dark green. The J2000 ecliptic/equinox pole is at the origin. The invariable plane is the black x. The best-fit mean plane from VM17 is the magenta +. The theoretical prediction (from linear secular theory) for the Laplace surface as a function of semimajor axis is plotted in blue. More details are given in the main text. The 68.2%, 95.4%, and 99.7% covariance ellipses from VM17 are plotted in magenta. Each subplot has the same scale, showing that an increased sample size does reduce mean plane uncertainty; in each semimajor axis bin, we have more objects and smaller covariance ellipses than VM17, and the more heavily populated semimajor axis bins on the second row have smaller covariance ellipses than the less heavily populated bins on the first row. The larger covariance ellipses on the third row, above 50 au, reflect the wider model inclination distribution used for those bins.