adsabs/AstroCLIMB huggingface dataset:
Paper: Empirical Stability Criteria for 3D Hierarchical Triple Systems. I. Circumbinary Planets
Authors: Nikolaos Georgakarakos, Siegfried Eggl, Mohamad Ali-Dib, Ian Dobbs-Dixon
Figure caption: Same as Figure 2, but for the planet to binary mass ratio M  p  = m  p /(m 1 + m 2) (top left), a zoomed-in plot of the same (top right), the pericenter (bottom left), and the longitude of the ascending node (bottom right). In the parameter regime we have chosen for this study, the planet’s mass does not substantially affect the stability limits. Aligned pericenters lead to lower instability in a system. The relative position of the nodes does not significantly impact the location of stability limits.
Paper: 3D Morphology and Motions of the Canis Major Region from Gaia DR3
Authors: Yiwei Dong, Ye Xu, Chaojie Hao, Yingjie Li, Dejian Liu, Yan Sun, Zehao Lin
Figure caption: Histograms of ϖ (left), ﹩{\mu }_{{\alpha }^{* }}﹩ (middle), and μ  δ  (right) for the YSO samples in the subregions. From top to bottom: the histograms of subregions A–F, with the same colors as in Figure 3. Vertical dashed lines indicate the average values of the parameters, and dotted lines mark the positions of ±1σ around the average values.
Paper: Empirical Stability Criteria for 3D Hierarchical Triple Systems. I. Circumbinary Planets
Authors: Nikolaos Georgakarakos, Siegfried Eggl, Mohamad Ali-Dib, Ian Dobbs-Dixon
Figure caption: Stability map of the TOI-1338 c planet. The parameters of the system were taken from M. R. Standing et al. (2023). TOI-1338 c is assumed to be the only planet in the system in a coplanar configuration. The integration time was 10,000 planetary periods. Mean motion resonances between the binary and the planet are shown in gray. The green and blue lines with 3σ uncertainty regions correspond to the empirical fits presented in Equation (10).
Paper: Empirical Stability Criteria for 3D Hierarchical Triple Systems. I. Circumbinary Planets
Authors: Nikolaos Georgakarakos, Siegfried Eggl, Mohamad Ali-Dib, Ian Dobbs-Dixon
Figure caption: A schematic representation of a circumbinary orbit.
Paper: 3D Morphology and Motions of the Canis Major Region from Gaia DR3
Authors: Yiwei Dong, Ye Xu, Chaojie Hao, Yingjie Li, Dejian Liu, Yan Sun, Zehao Lin
Figure caption: The distribution of the subregions within ±4.4 Myr, projected onto the x c–y c plane. The markers of the subregions are the same as in Figure 4.
Paper: 3D Morphology and Motions of the Canis Major Region from Gaia DR3
Authors: Yiwei Dong, Ye Xu, Chaojie Hao, Yingjie Li, Dejian Liu, Yan Sun, Zehao Lin
Figure caption: Same as Figure A2, but projected onto the y c–z c plane.
Paper: 3D Morphology and Motions of the Canis Major Region from Gaia DR3
Authors: Yiwei Dong, Ye Xu, Chaojie Hao, Yingjie Li, Dejian Liu, Yan Sun, Zehao Lin
Figure caption: Same as Figure A2, but projected onto the x c−z c plane.
Paper: UVIT Study of the MAgellanic Clouds (U-SMAC). II. A Far-UV Catalog of the Small Magellanic Cloud: Morphology and Kinematics of Young Stellar Population
Authors: Sipra Hota, Annapurni Subramaniam, Prasanta K. Nayak, Smitha Subramanian
Figure caption: The SMC: UVIT observed fields in white circles are displayed over the GALEX background. The background is a two-color combined image of GALEX, where the blue color represents FUV observations, whereas the red color denotes NUV observations (encompassing both GR6 and GR7 data releases). The yellow arrow points in the direction of the LMC (V. Belokurov et al. 2017; M. De Leo et al. 2020).
Paper: UVIT Study of the MAgellanic Clouds (U-SMAC). II. A Far-UV Catalog of the Small Magellanic Cloud: Morphology and Kinematics of Young Stellar Population
Authors: Sipra Hota, Annapurni Subramaniam, Prasanta K. Nayak, Smitha Subramanian
Figure caption: FUV magnitude vs. error in magnitude (PSF fit error) for various fields of the SMC with different exposure times.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: An all-sky map illustrating the DR0 (red), planned DR1 (purple) and planned DR2 (yellow) regions of the MDW Hα Sky Survey. The Northern Galactic Plane covered by the IGAPS survey is shown within the blue lines. Each box represents one field, spanning 3.°6 × 3.°6. The survey will cover a total of 4120 fields, including two special fields for the north and south celestial poles. We do not include field numbers in the map due to space constraints, but the full map can be found in the online version of the journal.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: After calibrating our instrumental magnitudes per Section 3.2, we run source detection on each DR0 image with a detection threshold of 4σ above the image median and apply our calculated zero-point for each field (Section 4.2.2) to convert to calibrated AB magnitudes. Looking at where the frequency of sources drops off in this histogram, we find that the limiting magnitude for point-source objects in DR0 is around 16–17 mag. This value is based on the DR0 mean images and is subject to change in future data releases as we continue to refine our calibration and stacking processes.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: A plot comparing the same region of the sky as imaged in different Hα surveys: mean-combined field 2139 of the MDW Survey (left), field 205 of SHASSA (middle), and Field Ori09 of VTSS (right). While we do not quantify the diffuse emission sensitivity of the MDW Survey, we can visually see the subtle structure revealed in the MDW field compared to the relatively low-resolution SHASSA and VTSS surveys. Note that DR0 and VTSS fields have been reprojected onto SHASSA’s WCS information, using astropy's reproject package.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: An illustration of the specifications of an MDW Survey field, using field 368 of DR0 as an example. The individual exposures are mean combined with sigma rejection so as to increase the signal-to-noise ratio of the stacked field.
Paper: Revisiting the Relationship Between Rocky Exoplanet and Stellar Compositions: Reduced Evidence for a Super-Mercury Population
Authors: Casey L. Brinkman, Alex S. Polanski, Daniel Huber, Lauren M. Weiss, Diana Valencia, Mykhaylo Plotnykov
Figure caption: Radius vs. mass for planets with radii R < 1.8 R ⊕ that have a fractional uncertainty of <30% in mass and radius, from the NASA Exoplanet Archive (queried 2023 June 5; R. L. Akeson et al. 2013). Exoplanets that are consistent with a rocky composition (mixture of iron and rock only; violet shaded region) are shown in color, while those inconsistent with a rocky composition are shown in gray. Planets that are less dense than rock likely have gaseous envelopes, while planets more dense than iron likely have measurement errors, either in mass, radius, or both. Point size scales inversely with the uncertainty in density (larger points have smaller uncertainties), and color indicates host-star metallicity. Planets that orbit stars for which we have detailed homogeneously measured abundances for Mg, Si, and Fe are circled in black.
Paper: Revisiting the Relationship Between Rocky Exoplanet and Stellar Compositions: Reduced Evidence for a Super-Mercury Population
Authors: Casey L. Brinkman, Alex S. Polanski, Daniel Huber, Lauren M. Weiss, Diana Valencia, Mykhaylo Plotnykov
Figure caption: The difference in ﹩v\sin (i)﹩, [Fe/H], [Mg/H], and [Si/H] for a sample of spectra that had their spectral resolutions degraded (top four panels) showing that KeckSpec is insensitive to changes in spectral resolution down to a ﹩v\sin (i)﹩ of around 4 km s−1. The blue shaded region gives the range of uncertainty quoted for the abundance measurements. The bottom two panels show a comparison of relative abundances between the native spectral resolution and a degraded one.
Paper: Revisiting the Relationship Between Rocky Exoplanet and Stellar Compositions: Reduced Evidence for a Super-Mercury Population
Authors: Casey L. Brinkman, Alex S. Polanski, Daniel Huber, Lauren M. Weiss, Diana Valencia, Mykhaylo Plotnykov
Figure caption: Alpha abundances [α/Fe] as a function of [Fe/H] for each host star in our KeckSpec sample (indigo), along with a larger sample of exoplanets from the SPOCS catalog (J. M. Brewer & D. A. Fischer 2018). The black dashed line approximately separates the galactic thin-disk and thick-disk populations (L. M. Weiss et al. 2021). The three stars in our sample that fall above this line and were likely born in the galactic thick disk are labeled.
Paper: Revisiting the Relationship Between Rocky Exoplanet and Stellar Compositions: Reduced Evidence for a Super-Mercury Population
Authors: Casey L. Brinkman, Alex S. Polanski, Daniel Huber, Lauren M. Weiss, Diana Valencia, Mykhaylo Plotnykov
Figure caption: Planet core mass fraction (CMF) of the planet as a function of host-star metallicity. The color corresponds to planet radius. CMF values below zero (green shaded region) mean that the planet density is too low to be composed entirely of rock and iron, and likely has a low-density component such as a gaseous envelope or water layer. The vertical gray line divides host stars below and above the median metallicity in the solar neighborhood ([Fe/H] = –0.1 dex).
Paper: Oxygen Abundance Throughout the Dwarf Starburst Galaxy IC 10
Authors: Maren Cosens, Shelley A. Wright, Karin Sandstrom, Lee Armus, Norman Murray, Jordan N. Runco, Sanchit Sabhlok, James Wiley
Figure caption: KCWI footprint overlaid on a Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) image of the central region of IC 10 taken with the F606W filter. The footprint of the previous high-resolution KCWI observations discussed in Paper I is shown in blue, while the new observations are outlined in orange.
Paper: UVIT Study of the MAgellanic Clouds (U-SMAC). II. A Far-UV Catalog of the Small Magellanic Cloud: Morphology and Kinematics of Young Stellar Population
Authors: Sipra Hota, Annapurni Subramaniam, Prasanta K. Nayak, Smitha Subramanian
Figure caption: (a) BL stars on the optical CMD. Blue and orange polygons denote the BL stars with age ≤150 Myr and >150 Myr, respectively. (b) Gaussian curve fits the PM distribution. (c) and (d) VPDs with PMRA and PMDec distribution at the top and right, respectively. (e) and (f) present the spatial distribution of PMRA of two BL subpopulations (age ≤150 Myr and >150 Myr).
Paper: UVIT Study of the MAgellanic Clouds (U-SMAC). II. A Far-UV Catalog of the Small Magellanic Cloud: Morphology and Kinematics of Young Stellar Population
Authors: Sipra Hota, Annapurni Subramaniam, Prasanta K. Nayak, Smitha Subramanian
Figure caption: UVIT and UIT FUV magnitudes of common sources (for search radii of 2″ and 1″). Different markers represent UVIT-UIT-SIMBAD stars classified as emission-line stars, eclipsing binaries, Be star candidates, high-mass X-ray binaries, and Be stars.
Paper: UVIT Study of the MAgellanic Clouds (U-SMAC). II. A Far-UV Catalog of the Small Magellanic Cloud: Morphology and Kinematics of Young Stellar Population
Authors: Sipra Hota, Annapurni Subramaniam, Prasanta K. Nayak, Smitha Subramanian
Figure caption: Spatial distribution of the SMC FUV stars brighter than 15 mag corresponding to a photometric mass >8M ⊙.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: Above: spatial distribution of separation distances across DR0 images when catalog matching DR0 sources with Pan-STARRS1. Below: the same distribution, using IGAPS instead. Within the bullseye pattern, we see that the separation distances are less than half a pixel, with maximum separation (<1 pix) occurring in the field corners. To further correct these offsets, we may consider refinements to the polynomial order of our astrometric solutions in future data releases; we currently use a tweak order of 3. Note that we set a separation limit of 2.″5 when catalog matching to Pan-STARRS1 and 1.″5 for IGAPS.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: A histogram of the difference between our calibrated Hα magnitudes and the corresponding IGAPS source's Hα AB magnitude, with a log-scale applied to the y-axis, for the region where IGAPS and DR0 overlap. The histogram centers closely around 0, indicating that the MDW magnitudes align well with IGAPS. We do see a left-leaning tail in the histogram, indicating a number of brighter sources with fainter MDW Hα magnitudes compared to IGAPS.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: 2D histogram of (r − MDW Hα) vs. (r − i) for DR0 field 702, before (left) and after (right) applying our second offset. Note that our stellar locus sits in the 0 < (Pan − STARRS1 r  − Pan − STARRS1 i ) < 0.25 range, while the IGAPS stellar locus is located at 0.5 < (Pan − STARRS1 r  − Pan − STARRS1 i ) < 0.75. This may be because IGAPS detects redder sources due to its fainter limiting magnitude (20.5 in Hα), changing the position of their locus.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: Above: distribution of separation distances when catalog matching DR0 sources with the Pan-STARRS1 survey. Below: distribution of separation distances when catalog matching DR0 sources with IGAPS. The red and yellow dotted lines are the mean and median separation distances in arcseconds. We limit our catalog to sources with a Pan-STARRS1 match that is 2.″5 or closer. IGAPS covers the Galactic plane, which may result in more mismatches because the region has a high source density. Hence, we limit matching to IGAPS sources that have a separation of at most 1.″5.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: A plot of boxes corresponding to the width and height of each DR0 field and numbered by field. A brighter-colored box corresponds to a field with a high median local background standard deviation, correlating to high nebulosity areas in the sky. The brightest field, 2253, contains the Orion Nebula (M42). The Rosette Nebula (NGC 2237) sits in the intersection of fields 256, 244, 144, and 143, making up the second-brightest field in the plot.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: Top: the density plot shows our instrumental Hα magnitudes vs. the r magnitude of the corresponding Pan-STARRS1 sources for 5000 sources in DR0 field 22. The red line is the optimized linear model, which we then model over all DR0 fields to get the mean value of the y-intercept, b ≈ −21.5. Bottom: we overlay 5000 apertures (red circles) at the center of field 22, from which we measure the instrumental magnitudes used for deriving the linear model in the top plot. 5000 apertures is sufficient for finding the optimal value of b since it is only an initial calibration.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: The above is a visual of the star removal process for one field. The original image of field 368 is shown on the top left. We create a point-source mask such that each detected source takes on the value of its local background (top right) while the detected sources are masked in the original image (bottom left). The combination of the masked image and the point-source mask yields the final star-removed image (bottom right). This process is repeated for all 238 fields in DR0.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: A comparison of field coverage and density for the Tycho-2 catalog, Pan-STARRS1 catalog, and MDW source detections for DR0 field 144. Note that field 144 sits in the Galactic plane, where source density is particularly high. We see that the Tycho-2 catalog is relatively sparse, indicating Pan-STARRS1 as the preferred choice when creating the DR0 catalog. We also see that the MDW field has a field density that sits in the middle of Tycho and Pan-STARRS1.
Paper: The MDW Hα Sky Survey: Data Release 0
Authors: Noor Aftab, Xunhe (Andrew) Zhang, David R. Mittelman, Dennis di Cicco, Sean Walker, David H. Sliski, Julia Homa, Colin Holm-Hansen, Mary Putman, David Schiminovich, Arne Henden, Gary Walker
Figure caption: A 2D histogram showing the relationship between the local background standard deviation of our DR0 sources in the overlapping IGAPS region and the difference of our calibrated Hα magnitudes with the corresponding IGAPS Hα magnitude.
Paper: A New Statistical Analysis of the Morphology of Spiral Galaxies
Authors: Junye Wei, Ye Xu, Zehao Lin, Chaojie Hao, Yingjie Li, Dejian Liu, Shuaibo Bian
Figure caption: (a) A spiral galaxy with a clear spiral arm structure: SDSS J151201.76+061309.3. Two inner arms can be clearly observed, while a branch of this spiral galaxy can be seen about 5″ southeast of the center (red dot). (b) A spiral galaxy with an ambiguous structure: SDSS J160149.44+173826.0. This spiral galaxy has a spiral arm structure, but the spiral arms are too chaotic for us to be able to conduct any further analysis.
Paper: A New Statistical Analysis of the Morphology of Spiral Galaxies
Authors: Junye Wei, Ye Xu, Zehao Lin, Chaojie Hao, Yingjie Li, Dejian Liu, Shuaibo Bian
Figure caption: NGC 4321. The spiral arm has a clear branch at the position indicated by the arrow. Therefore, it is classified as a multiple-arm galaxy.
Paper: A New Statistical Analysis of the Morphology of Spiral Galaxies
Authors: Junye Wei, Ye Xu, Zehao Lin, Chaojie Hao, Yingjie Li, Dejian Liu, Shuaibo Bian
Figure caption: Fractions of each morphology in different f DeV ranges. Shown are flocculent galaxies (blue), multiple-arm galaxies (red), and grand-design galaxies (black). The errors are presented in the form of error bars.
Paper: A New Statistical Analysis of the Morphology of Spiral Galaxies
Authors: Junye Wei, Ye Xu, Zehao Lin, Chaojie Hao, Yingjie Li, Dejian Liu, Shuaibo Bian
Figure caption: Difference in the position angles of the branching points of each arm (with 180° subtracted) for the multiple-arm galaxies with two inner arms and with both arms branching. Many arms are symmetric to within 20°.
Paper: A New Statistical Analysis of the Morphology of Spiral Galaxies
Authors: Junye Wei, Ye Xu, Zehao Lin, Chaojie Hao, Yingjie Li, Dejian Liu, Shuaibo Bian
Figure caption: (a) Spiral galaxy with one inner arm, SDSS J124701.94+403547.1. (b) Spiral galaxy with two inner arms, SDSS J032139.98-063808.2. (c) Spiral galaxy with three inner arms, SDSS J161533.08+262957.0. (d) Spiral galaxy with four inner arms, SDSS J115853.95+014408.3.
Paper: A New Statistical Analysis of the Morphology of Spiral Galaxies
Authors: Junye Wei, Ye Xu, Zehao Lin, Chaojie Hao, Yingjie Li, Dejian Liu, Shuaibo Bian
Figure caption: Fractions of each morphology in different redshift ranges. Shown are flocculent galaxies (blue), multiple-arm galaxies (red), and grand-design galaxies (black). The errors are presented in the form of error bars.
Paper: A New Statistical Analysis of the Morphology of Spiral Galaxies
Authors: Junye Wei, Ye Xu, Zehao Lin, Chaojie Hao, Yingjie Li, Dejian Liu, Shuaibo Bian
Figure caption: A multiple-arm galaxy with an inner two-arm symmetry: SDSS J113116.03+043908.7. The branching points of its two inner arms (red dots) are symmetric.
Paper: A New Statistical Analysis of the Morphology of Spiral Galaxies
Authors: Junye Wei, Ye Xu, Zehao Lin, Chaojie Hao, Yingjie Li, Dejian Liu, Shuaibo Bian
Figure caption: This galaxy (SDSS J230616.43+135856.3) has two arms in the inner region. However, the arms spread out in the outer region.
Paper: Oxygen Abundance Throughout the Dwarf Starburst Galaxy IC 10
Authors: Maren Cosens, Shelley A. Wright, Karin Sandstrom, Lee Armus, Norman Murray, Jordan N. Runco, Sanchit Sabhlok, James Wiley
Figure caption: (a) Integrated [O III] 5007 Å flux map utilizing the KCWI large slicer and BL grating with a 50 pc scale bar at the bottom right. These observations cover the field shown by the orange contours in Figure 1. (b) Map of oxygen abundance in those 12 H II regions with a sufficient SNR to detect [O III] 4363 Å required for the direct method (SNR[O III] 4363 > 3). These detections are in the integrated region spectra so the color is shown filling the region contour. The remaining H II regions are shown by the unfilled blue contours. The outlier region M16c—discussed further in Section 4—is shown in white in order to increase the contrast of the variations seen between the other 11 regions which span a narrower range of oxygen abundance. These maps cover the exact same field as those in (a), but the axes are converted to parsecs to illustrate the spatial scale and separation of the H II regions. (c) The electron temperature determined from the [O III] 4363 Å line following Equation (2). The locations of spectroscopically confirmed W-R stars are shown with white Xs and unconfirmed with white +s. These maps illustrate the range of oxygen abundance across H II regions on even these small distances within the central region of IC 10.