adsabs/AstroCLIMB huggingface dataset:
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Contrast curves for HATS-76 (TOI 555) derived from high-resolution images at 562 and 832 nm obtained with Zorro/Gemini8 m. The 832 nm image is also shown in the inset.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Contrast curves for HATS-77 (TOI 730) derived from high-resolution images at 562 and 832 nm obtained with Zorro/Gemini8 m. The 832 nm image is also shown in the inset.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Planetary radius vs. stellar effective temperature Teff for confirmed transiting exoplanets. The dotted vertical lines indicate the Teff values that roughly separate the host star spectral types as indicated on top, while the horizontal line at R = 0.6RJ indicates the separation between giant and smaller planets. Different symbols are used to plot known giants around M dwarfs and the discoveries presented in this work as indicated in the legend. Data were downloaded from the NASA Exoplanet Archive on 2021 May 13.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Mass–Radius diagram for the population of exoplanets with measured mass and radii. The points corresponding to the discoveries presented in this work are indicated with diamonds. The color represents the equilibrium temperature of the planet. The dashed gray lines correspond to isodensity curves for 0.3, 3, and 30 g cm−3 , respectively. The solid line corresponds to the predicted radius using the models of Fortney et al. (2007) for a planet with a 10 M⊕ central core.
Paper: HATS-74Ab, HATS-75b, HATS-76b, and HATS-77b: Four Transiting Giant Planets Around K and M Dwarfs  
Authors: Andrés Jordán, J. D. Hartman, D. Bayliss, G. Á. Bakos, R. Brahm, E. M. Bryant, Z. Csubry, Th. Henning, M. Hobson, L. Mancini, K. Penev, M. Rabus, V. Suc, M. de Val-Borro, J. Wallace, K. Barkaoui, David R. Ciardi, K. A. Collins, E. Esparza-Borges, E. Furlan, T. Gan, Z. Benkhaldoun, M. Ghachoui, M. Gillon, S. Howell, E. Jehin, A. Fukui, K. Kawauchi, J. H. Livingston, R. Luque, R. Matson, E. C. Matthews, H. P. Osborn, F. Murgas, Norio Narita, E. Palle, H. Parvianen, and W. C. Waalkes
Figure caption: Mass vs. effective temperature Teff for confirmed transiting exoplanets. The dotted vertical lines indicate the Teff values that roughly separate the spectral types as indicated on top, while the horizontal line at M = 0.2M⊙ indicates the adopted boundary between giant and smaller planets. Different symbols are used to plot known giants around M dwarfs and the discoveries presented in this work as indicated in the legend. Data were downloaded from the NASA Exoplanet Archive on 2021 May 13.
Paper: Online Database of Multiwavelength Water Masers in Galactic Star-forming Regions
Authors: Dmitry A. Ladeyschikov, Andrey M. Sobolev, Olga S. Bayandina, and Nadezhda N. Shakhvorostova
Figure caption: Number of known methanol and water maser sources as a function of the year of publication. The total number of water masers is shown in blue, and the number of water masers related to star formation regions is shown in orange.
Paper: Online Database of Multiwavelength Water Masers in Galactic Star-forming Regions
Authors: Dmitry A. Ladeyschikov, Andrey M. Sobolev, Olga S. Bayandina, and Nadezhda N. Shakhvorostova
Figure caption: The objects’ page of the database’s web interface.
Paper: Online Database of Multiwavelength Water Masers in Galactic Star-forming Regions
Authors: Dmitry A. Ladeyschikov, Andrey M. Sobolev, Olga S. Bayandina, and Nadezhda N. Shakhvorostova
Figure caption: Distribution of H2O masers in the Galaxy. Background CO images are taken from Dame et al. (2001). Green and red dots in the top and bottom panels are detections and nondetections, respectively.
Paper: Online Database of Multiwavelength Water Masers in Galactic Star-forming Regions
Authors: Dmitry A. Ladeyschikov, Andrey M. Sobolev, Olga S. Bayandina, and Nadezhda N. Shakhvorostova
Figure caption: Entity–relation diagram for the database of water masers. In each panel, the name, data type, and short description of each column are shown. Dashed arrows indicate foreign keys that link tables
Paper: The Effects of Stellar Gravity Darkening on High-resolution Transmission Spectra
Authors: P. Wilson Cauley, and John P. Ahlers
Figure caption: TESS photometry and best-fit results for KELT-9 and HAT-P-70. Both transits are visibly asymmetric due to stellar gravity darkening. The gravity-darkened model (blue) yields an improved fit to both data sets vs. the spherical star model (red).
Paper: The Effects of Stellar Gravity Darkening on High-resolution Transmission Spectra
Authors: P. Wilson Cauley, and John P. Ahlers
Figure caption: Colatitude vs. temperature for HAT-P-70 (top) and KELT-9 (bottom). HAT-P-70's polar temperature is almost 850 K greater than its equatorial temperature. For KELT-9 the difference is approximately 700 K.
Paper: The Effects of Stellar Gravity Darkening on High-resolution Transmission Spectra
Authors: P. Wilson Cauley, and John P. Ahlers
Figure caption: Comparison of disk-center (μ = 1.0) synthetic spectra for the approximate polar and equatorial temperatures for KELT-9 (upper panels) and HAT-P-70 (lower panels). The intensity differences are a result of the drastically different temperatures. The bottom panels show the normalized ratio between the polar (hotter) and equatorial (cooler) spectra: differences of ≈10%–30% are apparent in the line cores of Fe II 5169 Å and Na I D2 for both stars.
Paper: The Effects of Stellar Gravity Darkening on High-resolution Transmission Spectra
Authors: P. Wilson Cauley, and John P. Ahlers
Figure caption: Surface temperature maps and transit chords (red lines) for KELT-9 (left) and HAT-P-70 (right). Higher temperatures are indicated by lighter colors. The sky-projected polar and equatorial radii are to-scale relative to each star's equatorial radius. The stellar poles are marked by vertical black arrows, where the circular arrow shows the direction of stellar rotation.
Paper: The Effects of Stellar Gravity Darkening on High-resolution Transmission Spectra
Authors: P. Wilson Cauley, and John P. Ahlers
Figure caption: Simulated transmission spectra (Sin/Sout; first and third rows) and the absolute difference between the gravity-darkened and uniform temperature cases (∣ST − Sgd∣; second and fourth rows). The KELT-9 b spectra are in the top two rows and those for HAT-P-70 b are in the bottom two rows. The uniform stellar temperature case is displayed in red and the gravity-darkened case in blue. Note the different y-axis scaling. In all cases the magnitude of the difference in the transmission spectra is less than a part per thousand.
Paper: The Effects of Stellar Gravity Darkening on High-resolution Transmission Spectra
Authors: P. Wilson Cauley, and John P. Ahlers
Figure caption: Spectroscopic light curves for each atomic transition for a gravity-darkened stellar surface (blue lines) and uniform temperature surface (red lines). The shaded gray regions indicate the ingress and egress portions of the white light transit. The second and fourth rows show the difference in the light curves from the first and third rows, respectively. The light curve differences are larger for HAT-P-70 b, reflecting the fact that the planet transits a cooler chord of the star relative to the single-temperature Teff values. Note that the transit duration is slightly longer than the white light transit duration due to early and trailing occultation of the star by the planet's extended atmosphere.
Paper: Efficiently Imaging Accreting Protoplanets from Space: Reference Star Differential Imaging of the PDS 70 Planetary System Using the HST/WFC3 Archival PSF Library
Authors: Aniket Sanghi, Yifan Zhou, and Brendan P. Bowler
Figure caption: 1σ contrast at the separation of PDS 70 b as a function of resolution element radius. For small radii, significant variation in intensity among the resolution elements increases the 1σ contrast level. While we get the lowest contrast level (absolute minimum) at a radius of ∼3.8 pixels, the number of resolution elements is too small to enable accurate computation. Balancing the two factors, we select the local minimum at 2.36 pixels and adopt this as the radius of our circular apertures for contrast curve determinations.
Paper: Efficiently Imaging Accreting Protoplanets from Space: Reference Star Differential Imaging of the PDS 70 Planetary System Using the HST/WFC3 Archival PSF Library
Authors: Aniket Sanghi, Yifan Zhou, and Brendan P. Bowler
Figure caption: Left: the distribution of 5σ contrast curves obtained for an assortment of reference libraries consisting of 31 randomly selected reference stars, each presented as a dashed gray curve. The solid red curve is the 5σ contrast curve, and the dashed red curve is the 3σ contrast curve for our final postprocessed image shown in Figure 4. The contrast of PDS 70 b based on our measurement of its flux is marked as a red star with the corresponding uncertainties. Our detection of PDS 70 b has an S/N of 5.3. The 5σ contrast curve and corresponding PDS 70 b contrast from Zhou et al. (2021) using ADI are plotted as a yellow solid line and yellow star, respectively, for comparison. Three contrast curves are selected from the distribution as examples (see below). They are colored dark blue, light blue, and cyan from the top to bottom respectively. Right: postprocessed images corresponding to selected contrast curves in the left panel. Image (a) corresponds to the dark blue (top) contrast curve, image (b) corresponds to the light blue (center) contrast curve, image (c) corresponds to the cyan (bottom) contrast curve, and image (d) corresponds to the solid red (5σ) contrast curve. The residuals progressively decrease from images (a) to (d) at the separation of PDS 70 b and thus correspond to an improvement in detection limits.
Paper: Efficiently Imaging Accreting Protoplanets from Space: Reference Star Differential Imaging of the PDS 70 Planetary System Using the HST/WFC3 Archival PSF Library
Authors: Aniket Sanghi, Yifan Zhou, and Brendan P. Bowler
Figure caption: Assessment of the optimal size of the WFC3 reference star library for RDI reduction. Top left: mean of the fifty 5σ contrast curves generated for each library size depicted in the legend at the right. Brighter colors correspond to larger reference libraries. Top right: similar to the top-left panel but presenting the best of the fifty 5σ contrast curves generated for each library size depicted in the legend. The green shaded area represents the 1σ separation interval for our detection of PDS 70 b. 1σ limits are illustrated by dashed gray lines and the solid line marks the center of the separation interval. Bottom left: example distributions of the fifty 5σ contrast curves generated for libraries of size 25 and 35. The solid lines represent the mean contrast curve, and the dashed lines represent the best and the worst contrast curves for the given library size. Shaded regions highlight the spread in the contrast curve distribution from the mean. Bottom right: separation-averaged 5σ contrast requirement in the shaded green region for each library size, derived using the curves in the top-right panel. No correlation is found between library size and the separation-averaged 5σ contrast requirement.
Paper: Efficiently Imaging Accreting Protoplanets from Space: Reference Star Differential Imaging of the PDS 70 Planetary System Using the HST/WFC3 Archival PSF Library
Authors: Aniket Sanghi, Yifan Zhou, and Brendan P. Bowler
Figure caption: The morphology-significance criteria applied to the 162 ADI PSFs (orange circles). The pink and the gray regions represent the selection cuts using the morphology and significance criteria, respectively. The intersection of the two regions is the final adopted selection region. All of the ADI PSFs are in the selection region. The yellow circles show the location of our reference stars. The ADI PSFs have a peak-to-background ratio that is nearly two orders of magnitude greater than that of the reference PSFs. This highlights the significant difference in quality between the archival PSFs and the ADI PSFs.
Paper: Efficiently Imaging Accreting Protoplanets from Space: Reference Star Differential Imaging of the PDS 70 Planetary System Using the HST/WFC3 Archival PSF Library
Authors: Aniket Sanghi, Yifan Zhou, and Brendan P. Bowler
Figure caption: Calibrating astrometry and photometry of our detection of PDS 70 b with forward modeling. Top panel: RSS electron count flux as a function of position angle and separation based on a quadratic LSQ fit to our measurements. Subpanels show the fit residuals as a percentage of the RSS electron count flux for each measurement. A P.A. of 144° with respect to north and a separation of 184 mas from the host star minimizes the residuals. Bottom panel: RSS electron count flux as a function of injected electron count flux. The subpanel shows the fit residuals as a percentage of the RSS electron count flux for each measurement. A total absolute electron count flux of 111.3 electron counts or, equivalently, 1.6 × 10−15 erg s−1 cm−2, minimizes the residuals based on a quadratic LSQ fit to the measurements.
Paper: Efficiently Imaging Accreting Protoplanets from Space: Reference Star Differential Imaging of the PDS 70 Planetary System Using the HST/WFC3 Archival PSF Library
Authors: Aniket Sanghi, Yifan Zhou, and Brendan P. Bowler
Figure caption: Error estimated by injection-recovery tests. The mean ADI template PSF is injected with the same positive flux as that obtained for PDS 70 b from forward modeling. Left: 1σ uncertainty in separation as a function of injection separation from PDS 70. Center: 1σ uncertainty in P.A. as a function of injection separation from PDS 70. Right: mean flux change percentage as a function of injection separation from PDS 70. The astrometric uncertainty and mean flux change percentage at the separation of PDS 70 b (red stars) are calculated as the mean value of adjacent measurements.
Paper: Efficiently Imaging Accreting Protoplanets from Space: Reference Star Differential Imaging of the PDS 70 Planetary System Using the HST/WFC3 Archival PSF Library
Authors: Aniket Sanghi, Yifan Zhou, and Brendan P. Bowler
Figure caption: Example PSFs from the archival WFC3 PSF Library categorized in columns as true positives, false positives, true negatives, and false negatives based on the comparison between the visually assigned quality flag and the automated results of the morphology-significance criteria. This mosaic also provides representative examples for each quality-flag category, which is represented as a number on the top left of each image frame: 1 represents good-quality PSFs, 2 represents intermediate-quality PSFs, and 3 represents bad-quality PSFs.
Paper: Efficiently Imaging Accreting Protoplanets from Space: Reference Star Differential Imaging of the PDS 70 Planetary System Using the HST/WFC3 Archival PSF Library
Authors: Aniket Sanghi, Yifan Zhou, and Brendan P. Bowler
Figure caption: Classification of the reference PSFs based on the results obtained from the morphology-significance criteria, defined by the PSF’s quality flag and whether it was selected or rejected by the criteria. TP stands for true positive, TN for true negative, FP for false positive, and FN for false negative. These classifications provide a way to characterize the success and failure rates of the selection criteria. Green cells highlight the expected result combinations (TP, TN), and red cells highlight the anomalous result combinations (FP, FN).
Paper: Efficiently Imaging Accreting Protoplanets from Space: Reference Star Differential Imaging of the PDS 70 Planetary System Using the HST/WFC3 Archival PSF Library
Authors: Aniket Sanghi, Yifan Zhou, and Brendan P. Bowler
Figure caption: PSF selection using the morphology-significance criteria and STScI’s QFIT parameter. Green triangles represent Quality 1 PSFs, yellow circles represent Quality 2 PSFs, and red diamonds represent Quality 3 PSFs. The gray and pink regions are the selection cuts for the y- and x-axis parameters, respectively, across all panels. The intersection of the gray and pink regions is the final selection region. Top left: selection using the morphology-significance criteria. Top right: selection using the combination of the morphology-significance criteria and the QFIT parameter. All PSFs with QFIT ≥0.1 have been excluded from the plot and calculated TP and FP percentages are shown. Bottom: these panels show the results of selecting PSFs using a combination of the QFIT parameter and one of the morphology-significance criteria. The calculated TP and FP percentages are shown for the combined application as well as for the sole application of the QFIT parameter (FP-QFIT, TP-QFIT).
Paper: Efficiently Imaging Accreting Protoplanets from Space: Reference Star Differential Imaging of the PDS 70 Planetary System Using the HST/WFC3 Archival PSF Library
Authors: Aniket Sanghi, Yifan Zhou, and Brendan P. Bowler
Figure caption: Left: final primary-subtracted image depicting our detection of PDS 70 b after performing RDI KLIP subtraction on 162 Hα images. The above images are resampled by a factor of 2 using 2D cubic spline interpolation. To reduce high-frequency noise, we smooth these images with a Gaussian kernel with an FWHM of 2 pixels (∼60% of the PSF FWHM). North is up, and east is to the left. Astrometric measurements from literature are plotted for comparison. Right: a demonstration of how the S/N is calculated based on the methodology in Mawet et al. (2014), using an aperture size of 2.36 pixels (∼1.4 FWHM).
Paper: Efficiently Imaging Accreting Protoplanets from Space: Reference Star Differential Imaging of the PDS 70 Planetary System Using the HST/WFC3 Archival PSF Library
Authors: Aniket Sanghi, Yifan Zhou, and Brendan P. Bowler
Figure caption: Calibrating astrometry and photometry of our detection of PDS 70 b with forward modeling. Top panel: RSS electron count flux as a function of position angle and separation based on a quadratic least-squares (LSQ) fit to our measurements. Subpanels show the fit residuals as a percentage of the RSS electron count flux for each measurement. A P.A. of 142° with respect to north and a separation of 186 mas from the host star minimizes the residuals. Bottom panel: RSS electron count flux as a function of injected electron count flux. The subpanel shows the fit residuals as a percentage of the RSS electron count flux for each measurement. A total absolute electron count flux of 119.3 electron counts or, equivalently, 1.7 × 10−15 erg s−1 cm−2, minimizes the residuals based on a quadratic least-squares (LSQ) fit to the measurements. These values are adopted as our final astrometry and photometry for PDS 70 b.
Paper: Efficiently Imaging Accreting Protoplanets from Space: Reference Star Differential Imaging of the PDS 70 Planetary System Using the HST/WFC3 Archival PSF Library
Authors: Aniket Sanghi, Yifan Zhou, and Brendan P. Bowler
Figure caption: Error estimated by injection-recovery tests. The synthetic PSF is injected with the same positive flux as that obtained for PDS 70 b from forward modeling. Left: 1σ uncertainty in separation as a function of injection separation from PDS 70. Center: 1σ uncertainty in P.A. as a function of injection separation from PDS 70. Right: mean flux change percentage as a function of injection separation from PDS 70. The astrometric uncertainty and mean flux change percentage at the separation of PDS 70 b (red stars) are calculated as the mean value of adjacent measurements.
Paper: Orbital Elements and Individual Component Masses from Joint Spectroscopic and Astrometric Data of Double-line Spectroscopic Binaries  
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Rubén M. Clavería, and Edgardo Costa
Figure caption: Comparison of Hipparcos V- (top panel) and I-band magnitudes (bottom panel) with other photometric data presented in Tables 1 and 2. The dotted vertical lines in the top panel show the reliably bright limits of the APASS (V = 7) and ASAS (V = 8) surveys. In the whole magnitude range covered by these figures, all ASAS-SN photometry is unreliable (note the large declared error bars), but it was included for completeness. In both panels, the diagonal solid line depicts a one-to-one relationship. In the bottom panel, the diagonal dotted–dashed line shows the 0.38 mag offset between I and ﹩i^{\prime} ﹩ from APASS found by Mendez et al. (2021, their Figure 1). The highly discrepant point for Bag25Aa,Ab from ASAS-SN in the top panel is probably due to a misidentification of the target. See text for details.
Paper: Orbital Elements and Individual Component Masses from Joint Spectroscopic and Astrometric Data of Double-line Spectroscopic Binaries  
Authors: Jennifer Anguita-Aguero, Rene A. Mendez, Rubén M. Clavería, and Edgardo Costa
Figure caption: The ML orbits from simultaneous fits to the astrometric and RV curves for three representative cases. From top to bottom: A2801 (WDS 04107–0452), A2983 (WDS 14492+1013), and Bag25Aa,Ab (WDS 15282–0921). The left panels show the data points and astrometric orbit. The size and color of the dots indicate the weight (uncertainty) of each observation; large, light dots indicate larger errors, and the opposite is true for small, dark dots. Smaller dots are from more recent interferometric measurements, including—but not limited to—our own. The green line indicates the line of nodes, while the black line indicates the direction to apoastron. The right panels show the RV curves of both components. The horizontal dashed line indicates the inferred (fitted) systemic velocity reported in Table 3.