adsabs/AstroCLIMB huggingface dataset:
Paper: Counting the Unseen. I. Nuclear Density Scaling Relations for Nucleated Galaxies
Authors: Christian H. Hannah, Anil C. Seth, Nicholas C. Stone, Sjoert van Velzen
Figure caption: New nuclear scaling relations derived in this work. The left two panels display the relations between ρ 5pc (top) and γ (bottom) and galaxy mass for the nucleated galaxy subsamples, where the colors distinguish galaxy type. The right panels are identical to the left but show the relations for the higher-mass early-type galaxies with mixed nucleation.
Paper: Counting the Unseen. I. Nuclear Density Scaling Relations for Nucleated Galaxies
Authors: Christian H. Hannah, Anil C. Seth, Nicholas C. Stone, Sjoert van Velzen
Figure caption: Comparison between nuclear g − i (r < 0.″5) and galaxy-wide g − i with data points colored by the galaxy stellar mass. Early-type galaxies are indicated with bullets, while late-type galaxies are shown as diamonds. Nucleation is indicated with closed symbols.
Paper: An Image-based Blind Search for Fast Radio Bursts in 88 hr of Data from the EoR0 Field, with the Murchison Widefield Array
Authors: Ian Kemp, Steven Tingay, Stuart Midgley, Daniel Mitchell
Figure caption: Example satellite track (obs. id 106672616), showing all pixels >6σ in one 2 minute differenced MFS image set.
Paper: An Image-based Blind Search for Fast Radio Bursts in 88 hr of Data from the EoR0 Field, with the Murchison Widefield Array
Authors: Ian Kemp, Steven Tingay, Stuart Midgley, Daniel Mitchell
Figure caption: Typical (non-de-dispersed) MFS differenced image of a snapshot from Category B, XX polarization. a = full image; b = central portion, showing texture. Scale units are Jy beam−1.
Paper: An Image-based Blind Search for Fast Radio Bursts in 88 hr of Data from the EoR0 Field, with the Murchison Widefield Array
Authors: Ian Kemp, Steven Tingay, Stuart Midgley, Daniel Mitchell
Figure caption: Example Scintillation Mask.
Paper: Testing Cluster Membership of Planetary Nebulae with High-precision Proper Motions. I. HST Observations of JaFu 1 Near the Globular Cluster Palomar 6
Authors: Howard E. Bond, Andrea Bellini, Kailash C. Sahu
Figure caption: (a) Positions of Gaia DR3 stars brighter than G = 19 in the vicinity of the globular cluster Pal 6 (gold circle). The red border outlines the field in which archival HST data overlap with our new 2024 images. The position of the planetary nebula JaFu 1 is marked with a green cross. (b) Color–magnitude diagram for the Gaia stars. Gold points are likely cluster members, having positions and PMs within the gold circles in both panels (a) and (c). Red points are the Gaia stars that lie within the HST field in panel (a). (c) Vector-point PM diagram of Gaia stars shown in panel (a). Red points are Gaia stars lying within the HST field of view. The gold circle highlights likely Pal 6 members according to their PMs. (d) and (e) Absolute PMs in R.A. and decl. for stars measured in the HST field and cataloged in Gaia DR3. Red lines are the loci of equality. There is good consistency within the errors. (f) Vector-point diagram for the absolute PMs we measured in the HST field. The PM of the nucleus of JaFu 1 is marked with a green circle; its uncertainties are smaller than the plotting symbol. The gold circle for the cluster motion is the same as in panel (c). Turquoise arrows show the directions of PMs in Galactic longitude l and latitude b. See text for details of these diagrams.
Paper: Testing Cluster Membership of Planetary Nebulae with High-precision Proper Motions. I. HST Observations of JaFu 1 Near the Globular Cluster Palomar 6
Authors: Howard E. Bond, Andrea Bellini, Kailash C. Sahu
Figure caption: Color image created from PanSTARRS-1 g, r, and i frames, showing the globular cluster Pal 6 (below right) and the location of the planetary nebula JaFu 1 (faintly visible at the center of the white rectangle at upper left). North is at the top, east on the left. Height of frame is 320″.
Paper: The K2 and TESS Synergy. III. Search and Rescue of the Lost Ephemeris for K2's First Planet
Authors: Erica Thygesen, Joseph E. Rodriguez, Zoë L. de Beurs, Andrew Vanderburg, John H. Livingston, Jonathon Irwin, Alexander Venner, Michael Cretignier, Karen A. Collins, Allyson Bieryla, David Charbonneau, Ian J. M. Crossfield, Xavier Dumusque, John Kielkopf, David W. Latham, Michael Werner
Figure caption: Archival HARPS-N radial velocities for K2-2 from Vanderburg et al. (2015) and Bonomo et al. (2023). The left panel shows the phased-folded RVs, and the right panel shows the long-term trend in the unphased RVs.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The K2 and TESS Synergy. III. Search and Rescue of the Lost Ephemeris for K2's First Planet
Authors: Erica Thygesen, Joseph E. Rodriguez, Zoë L. de Beurs, Andrew Vanderburg, John H. Livingston, Jonathon Irwin, Alexander Venner, Michael Cretignier, Karen A. Collins, Allyson Bieryla, David Charbonneau, Ian J. M. Crossfield, Xavier Dumusque, John Kielkopf, David W. Latham, Michael Werner
Figure caption: The discovery and follow-up phase-folded transits of K2-2 b used in the EXOFASTv2 (see Section 3) analysis. The observations from K2 (black), TESS (purple), Spitzer (blue), MEarth (green), and ULMT (yellow) are shown in open colored circles, with the solid colored line representing the EXOFASTv2 model for that data set. The closed colored circles represent 30 minute bins. East transit is offset by a constant for clarity.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The K2 and TESS Synergy. III. Search and Rescue of the Lost Ephemeris for K2's First Planet
Authors: Erica Thygesen, Joseph E. Rodriguez, Zoë L. de Beurs, Andrew Vanderburg, John H. Livingston, Jonathon Irwin, Alexander Venner, Michael Cretignier, Karen A. Collins, Allyson Bieryla, David Charbonneau, Ian J. M. Crossfield, Xavier Dumusque, John Kielkopf, David W. Latham, Michael Werner
Figure caption: Residual CCFs (ΔCCFs) computed from HARPS-N spectra. The residual CCFs are computed by subtracting a median CCF. The CALM-predicted stellar activity signal is indicated by the color (red = redshifted RVs, blue = blueshifted RVs). The five CCF indices used in our stellar activity model are indicated by black lines.
Paper: Testing Cluster Membership of Planetary Nebulae with High-precision Proper Motions. I. HST Observations of JaFu 1 Near the Globular Cluster Palomar 6
Authors: Howard E. Bond, Andrea Bellini, Kailash C. Sahu
Figure caption: Measured positions of the central star of JaFu 1 in our master reference frame vs. observation epoch. Labels indicate the HST cameras used for the images. The X and Y positions are measured in pixels, with X pointing west and Y pointing north, and the pixel scale is 40 mas pixel−1. Positions from broadband filters are plotted with black filled circles, and measurements from narrowband emission-line filters with green filled circles. Points at the same epochs are slightly separated in time for clarity. The red lines show the proper-motion fits, and the shaded red areas their 1σ confidence intervals. See text for further details.
Paper: Testing Cluster Membership of Planetary Nebulae with High-precision Proper Motions. I. HST Observations of JaFu 1 Near the Globular Cluster Palomar 6
Authors: Howard E. Bond, Andrea Bellini, Kailash C. Sahu
Figure caption: False-color HST image of the field centered on the planetary nebula JaFu 1, outlined by the white rectangle in Figure 1. Created from WFC3 frames in Hα (red) and V (blue), and an ACS frame in [O III] 5007 Å (green). North is at the top, east on the left. Height of frame is 50″.
Paper: The Pre-perihelion Evolution of the Activity of Comet C/2017 K2 (Pan-STARRS) during the Water Ice-line Crossover
Authors: Yuna G. Kwon, Stefano Bagnulo, Johannes Markkanen, Ludmilla Kolokolova, Jessica Agarwal, Manuela Lippi, Zuri Gray
Figure caption: Secular evolution of r-band brightness and Afρ parameter of K2 as a function of heliocentric distance r H. The r-band absolute magnitude H r corrected for the heliocentric and geocentric distances and phase effects (Equation (4)) is presented in panel a, while Afρ parameter was calculated from Equation (5) and is shown in panel (b). Panel (c) illustrates the impact of an abrupt change in K2's α during our heliocentric coverage. All points correspond to the photometric parameters measured from the aperture size ρ of 20,000 km from the photocenter. Vertical lines indicate the r H of our VLT observations at three epochs (Table 2). Two inflection points where K2 experienced a change in its r-band brightness are marked with yellow triangles in panel (a).
Paper: The JWST/NIRISS Deep Spectroscopic Survey for Young Brown Dwarfs and Free-floating Planets
Authors: Adam B. Langeveld, Aleks Scholz, Koraljka Mužić, Ray Jayawardhana, Daniel Capela, Loïc Albert, René Doyon, Laura Flagg, Matthew de Furio, Doug Johnstone, David Lafrèniere, Michael Meyer
Figure caption: Results of the spectroscopic survey for object NIRISS-NGC1333-10B (NN10B)—the companion object of the binary NN10 (with NN10A shown in Figure 14). Panels shown are the same as in Figure 5. Similarly to NN10A (Figure 14), there is contamination in the F200W spectrum from a source that overlaps with the spectral trail—the data in this region is unusable and was removed (evident by the gap in the spectrum in the top panel between ∼1.95 and 2.1 μm). The cutouts also display a large white region (where all values are NaNs) to remove the spectrum of the primary object.
Paper: The JWST/NIRISS Deep Spectroscopic Survey for Young Brown Dwarfs and Free-floating Planets
Authors: Adam B. Langeveld, Aleks Scholz, Koraljka Mužić, Ray Jayawardhana, Daniel Capela, Loïc Albert, René Doyon, Laura Flagg, Matthew de Furio, Doug Johnstone, David Lafrèniere, Michael Meyer
Figure caption: Results of the spectroscopic survey for object NIRISS-NGC1333-10A (NN10A)—the primary object of the binary NN10 (with NN10B shown in Figure 15). Panels shown are the same as in Figure 5. The calibrated slope image cutouts show that there is contamination in the F200W spectrum from a source that overlaps with the spectral trail—the data in this region is unusable and was removed (evident by the gap in the spectrum in the top panel between ∼1.95 and 2.1 μm). The cutouts also display a large white region (where all values are NaNs) to remove the spectrum of the companion object.
Paper: The JWST/NIRISS Deep Spectroscopic Survey for Young Brown Dwarfs and Free-floating Planets
Authors: Adam B. Langeveld, Aleks Scholz, Koraljka Mužić, Ray Jayawardhana, Daniel Capela, Loïc Albert, René Doyon, Laura Flagg, Matthew de Furio, Doug Johnstone, David Lafrèniere, Michael Meyer
Figure caption: Results of the spectroscopic survey for object NIRISS-NGC1333-6 (NN6). Panels shown are the same as in Figure 5. The calibrated slope image cutouts show that there is contamination from a nearby source (evident by a small trail in the upper right of both cutouts, overlapping the NN6 spectrum at longer wavelengths). This causes excess flux at ∼1.65 μm and ∼2.2 μm, and the deviation from the model template in the top panel.
Paper: The JWST/NIRISS Deep Spectroscopic Survey for Young Brown Dwarfs and Free-floating Planets
Authors: Adam B. Langeveld, Aleks Scholz, Koraljka Mužić, Ray Jayawardhana, Daniel Capela, Loïc Albert, René Doyon, Laura Flagg, Matthew de Furio, Doug Johnstone, David Lafrèniere, Michael Meyer
Figure caption: Results of the spectroscopic survey for object NIRISS-NGC1333-5 (NN5). Panels shown are the same as in Figure 5. This object has known infrared excess (see Section 4.3), which may explain the excess flux at ∼2.2 μm.
Paper: Asteroid Period Solutions from Combined Dense and Sparse Photometry
Authors: Michael Gowanlock, David E. Trilling, Andrew McNeill, Daniel Kramer, Maria Chernyavskaya
Figure caption: The distribution of correct rotation periods as a function of period for the 222 objects in LCDB∩SS1∩TESSC1 across the four data sets is shown. Each rotation period bin is 1 hr, and the bins are centered on integer period values. The top panel shows the LCDB period distribution, where each object has been assigned an unambiguously correct rotation period. The three lower panels from top to bottom are as follows: SS1∩TESSC1, SS1, and TESSC1, where the (correct) LCDB distribution is plotted behind the period distribution shown for each of these three data sets. Only those objects whose periods exactly match the LCDB period are plotted.
Paper: Asteroid Period Solutions from Combined Dense and Sparse Photometry
Authors: Michael Gowanlock, David E. Trilling, Andrew McNeill, Daniel Kramer, Maria Chernyavskaya
Figure caption: The period distribution for the n = 3168 objects in SS1∩TESSC1. The bottom to top panels show the period distribution using only the observations in TESSC1, the period distribution using only the observations in SS1, and the period distribution when combining the observational records of both data sets, respectively. Although we search for solutions up to 10,000 hr, we only show solutions up to 100 hr because there are so few solutions >100 hr.
Paper: Asteroid Period Solutions from Combined Dense and Sparse Photometry
Authors: Michael Gowanlock, David E. Trilling, Andrew McNeill, Daniel Kramer, Maria Chernyavskaya
Figure caption: The distribution of the number of observations for the objects in the (a) SS1, (b) TESSC1, and (c) SS1∩TESSC1 data sets, limited to the n = 3168 objects appearing in both SS1 and TESSC1. The bin width is 10 observations in each histogram.
Paper: Verification of Astrometrically Accelerating Stars from Hipparcos and Gaia. I. Methodology and Application to HIP 44842
Authors: Valeri V. Makarov, Andrei Tokovinin
Figure caption: Best-fitting mixed distribution of normalized apparent acceleration values χ   μ   for 102,549 Hipparcos–Gaia stars. Left panel: PDF curves of the fitting mixed distribution. Right panel: corresponding histograms of the mixed distribution fit and its two components in the log-log scale simulated by random number generator, which can be compared with Figure 1, left.
Paper: Verification of Astrometrically Accelerating Stars from Hipparcos and Gaia. I. Methodology and Application to HIP 44842
Authors: Valeri V. Makarov, Andrei Tokovinin
Figure caption: Top panel: RV curve fitted to the CHIRON data (green solid line and squares for primary, blue dash and triangles for the secondary). The green dashed line shows the Gaia DR3 spectroastrometric orbit. Bottom panel: the CCF recorded on JD 2459178.85 (line and pluses) fitted by a sum of two Gaussians (dash–dot line).
Paper: Verification of Astrometrically Accelerating Stars from Hipparcos and Gaia. I. Methodology and Application to HIP 44842
Authors: Valeri V. Makarov, Andrei Tokovinin
Figure caption: PARSEC isochrones (Bressan et al. 2012) for 1.5 and 2.5 Gyr ages and solar metallicity in the (V − K, M  V ) color–magnitude diagram. Asterisks mark masses of 1.2, 1.3, and 1.4 M ⊙  on the 2.5 Gyr isochrone.
Paper: Verification of Astrometrically Accelerating Stars from Hipparcos and Gaia. I. Methodology and Application to HIP 44842
Authors: Valeri V. Makarov, Andrei Tokovinin
Figure caption: Average spectrum of HIP 44842 shifted to zero velocity (full line) and the POLLUX synthetic spectrum (Palacios et al. 2010) for T  e  = 4500 K, ﹩\mathrm{log}g=3.0﹩, and solar metallicity (green dash line).
Paper: The Nonsingular Estimator for Exoplanet Orbits: An Unscented Batch Estimation Method for Direct Imaging Measurements
Authors: Zvonimir Stojanovski, Dmitry Savransky
Figure caption: In the direct imaging of exoplanets, we observe the projection ﹩P^{\prime} ﹩ of the exoplanet’s position P with respect to the star S onto the image plane. The basis vectors of the planet’s perifocal frame are denoted by ( p  1,  p  2,  p  3).
Paper: The Nonsingular Estimator for Exoplanet Orbits: An Unscented Batch Estimation Method for Direct Imaging Measurements
Authors: Zvonimir Stojanovski, Dmitry Savransky
Figure caption: The perifocal frame ﹩{ \mathcal P }﹩ and the auxiliary frame ﹩{ \mathcal Q }﹩, with basis vectors ( q  1,  q  2,  q  3).
Paper: The Nonsingular Estimator for Exoplanet Orbits: An Unscented Batch Estimation Method for Direct Imaging Measurements
Authors: Zvonimir Stojanovski, Dmitry Savransky
Figure caption: Prior distribution of the nonsingular elements with M ⋆ = 1M ⊙, ϖ = 1 as, and K = 1500.
Paper: Utilizing Voronoi Tessellations to Determine Radial Density Profiles
Authors: Veronika Dornan, William E. Harris
Figure caption: Left: the 2D spatial distribution of objects with concentric annuli drawn out from the center of the system. These annuli are used to bin the objects and determine densities as a function of radius. Right: the Voronoi tessellation plot for the same 2D distribution of objects, with one object per cell. For both plots, cell color represents comparative density on the same scale.
Paper: Occurrence Rates of Exosatellites Orbiting 3–30 M Jup Hosts from 44 Spitzer Light Curves
Authors: Mary Anne Limbach, Johanna M. Vos, Andrew Vanderburg, Fei Dai
Figure caption: Percentage of retrieved transits as a function of the target’s Spitzer [3.6] band magnitude for injected transits with transit depths ranging between 0.3% and 1.0% and with a duration of 60 minutes. The red stars correspond to the transit fits that had ﹩{\rm{\Delta }}\mathrm{log}z﹩ values of ≥2.4σ significance. The percentage of transits with similar transit depths that are successfully retrieved is labeled on the plot. In all three cases, transits with similar proprieties were retrievable in a substantial (38%–92%) portion of the sample, indicating the data enables the detection of transits with parameters comparable to those detected.
Paper: Occurrence Rates of Exosatellites Orbiting 3–30 M Jup Hosts from 44 Spitzer Light Curves
Authors: Mary Anne Limbach, Johanna M. Vos, Andrew Vanderburg, Fei Dai
Figure caption: Companion vs. host mass for the known exoplanet population (blue and black points) as well as the approximate sensitivity of several past, ongoing, or upcoming exosatellite (or moon) surveys of substellar, FFP, and exoplanet hosts. This study was sensitive to exosatellites down to the size of 0.7 R ⊕ (∼0.25 M ⊕) around 3–30 M Jup hosts. The majority of the targets within this survey, TEMPO and JWST are young (1–1000 Myr) unlike the typical stars that host known exoplanets. References: (a) Limbach et al. (2021), (b) Limbach et al. (2023), (c) Tamburo et al. (2022a, 2022b) and (d) Kipping et al. (2022).
Paper: Occurrence Rates of Exosatellites Orbiting 3–30 M Jup Hosts from 44 Spitzer Light Curves
Authors: Mary Anne Limbach, Johanna M. Vos, Andrew Vanderburg, Fei Dai
Figure caption: Occurrence rate constraints under the assumption that there are no detected transiting exosatellites in this sample. Upper limits on the occurrence rates for sub-Neptunes on 0.3–0.8 day orbits (upper left panel) and 0.8–1.5 day orbits (upper right panel). Upper limits on the occurrence rates for terrestrial (∼0.7–1.6 R ⊕) exosatellites on 0.3–0.8 day orbits (bottom left panel) and 0.8–1.5 day orbits (bottom right panel).
Paper: Occurrence Rates of Exosatellites Orbiting 3–30 M Jup Hosts from 44 Spitzer Light Curves
Authors: Mary Anne Limbach, Johanna M. Vos, Andrew Vanderburg, Fei Dai
Figure caption: Median ﹩{\rm{\Delta }}\mathrm{log}z﹩ (black line, with blue band showing one standard deviation) as a function of the target’s Spitzer [3.6] band magnitude for transits that were successfully injected in retrieved. From top to bottom, the injected transit depths were 0.3%–0.4%, 0.5%–0.6% and 0.8%–1.0%. The red stars (labeled with target name and retrieved transit depth, δ) show the ﹩{\rm{\Delta }}\mathrm{log}z﹩ of the retrieved transits from the real transit search, all of which lie within one standard deviation of the median retrieved value with the exception of the bottom plot (the 2M0642 retrieval), which lies slightly below the typical values.
Paper: Occurrence Rates of Exosatellites Orbiting 3–30 M Jup Hosts from 44 Spitzer Light Curves
Authors: Mary Anne Limbach, Johanna M. Vos, Andrew Vanderburg, Fei Dai
Figure caption: Occurrence rate constraints under the assumption that one or two of the detected outlier transits are real. This distribution is the average of the two distributions derived for one or two outlier detections and constrains the occurrence rate of short-period, terrestrial (∼0.7–1.6 R ⊕) companions to ﹩\eta ={0.61}_{-0.34}^{+0.49}﹩ exosatellites per substellar world.
Paper: Occurrence Rates of Exosatellites Orbiting 3–30 M Jup Hosts from 44 Spitzer Light Curves
Authors: Mary Anne Limbach, Johanna M. Vos, Andrew Vanderburg, Fei Dai
Figure caption: Percentage of recovered transits with a depth of 0.7% as a function of the orbital period for bright targets (blue line) and fainter targets (red line) and the sample as a whole (gray dashed line).
Paper: Interstellar Polarization Survey. IV. Characterizing the Magnetic Field Strength and Turbulent Dispersion Using Optical Starlight Polarization in the Diffuse Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, A. Marchal, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Extinction density as a function of the distance retrieved from Vergely et al. (2022) at 10 pc resolution in units of mag pc−1 (the blue solid line), Leike et al. (2020) at 1 pc resolution in units of e-foldings pc−1 (the orange solid line), and Edenhofer et al. (2023) with resolution between 0.4 and 7 pc in the units of the parameter E from Zhang et al. (2023; the gray solid line) in direction of C2 (top), C16 (middle), and C37 (bottom). The gray dots show the IPS-GI optical polarization as a function of the distance. The vertical black dashed lines show the distance to the dust peaks taken from Zucker et al. (2021). The vertical black solid lines are the total dust depth assumed, l  c .
Paper: Interstellar Polarization Survey. IV. Characterizing the Magnetic Field Strength and Turbulent Dispersion Using Optical Starlight Polarization in the Diffuse Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, A. Marchal, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Volume density as a function of the distance obtained from Leike et al. (2020; the gray and orange dots) and Vergely et al. (2022; the blue dots) 3D dust maps in C2 (top), C16 (middle), and C37 (bottom). The orange solid line is the mean smoothed curve, with kernel 4. The gray bars are the standard deviation. The blue shaded curve is the error from Vergely et al. (2022). The horizontal black line marks the approximated peak volume density. The vertical black dashed line is the distance to the cloud in C2 and C16, which is assumed from Zucker et al. (2021). In the case of C37, the vertical red dashed line is the mean distance of the entire dust distribution.
Paper: Interstellar Polarization Survey. IV. Characterizing the Magnetic Field Strength and Turbulent Dispersion Using Optical Starlight Polarization in the Diffuse Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, A. Marchal, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: H I emission line of GASS (red solid line) compared to ROHSA’s total model (black solid line) and the CNM (blue solid line), LNM (green solid line), and WNM (orange solid line) models in the center of the map. The insets in each panel present the model built with the components of the low-velocity clouds (LVCs, ∣V  lsr ∣ < 20 km s−1) from the ROHSA decomposition.