adsabs/AstroCLIMB huggingface dataset:
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: Dispersion of the polarization angle corrected by the measurement errors as a function of the scale length in field C2 (left), C16 (middle), and C37 (right). The red solid line is the best fit to the scales at which we see a linear increase in dispersion. The insets show a log-scale histogram depicting the number of sampled star pairs per angular scale bin.
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: Mass density (left column) and scaled turbulent velocity dispersion (right column) 2D maps of fields C2 (top row), C16 (middle row), and C37 (bottom row). The black (left) and white (right) pseudo-vectors represent the IPS-GI optical polarization measurements for comparison.
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: Distribution of the median polarization angle (left column) and the standard error (right column) in the field of view of C2 (top row), C16 (middle row), and C37 (bottom row).
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: Optical polarization vectors map (left column) and polarization angle as a function of distance (right column) of fields C2 (top row), C16 (middle row), and C37 (bottom row). The red vectors represent unreliable polarization angle measurements above 3σ  from the mean distribution and are excluded from the calculation of the ADF.
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: Gas column density of the LVC model obtained from ROHSA decomposition in field C2 (left), C16 (middle), and C37 (right). The white pseudo-vectors represent the IPS-GI optical polarization measurements for comparison.
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: The He transmission spectrum for K2-100b (top), HD 63433b (middle), V1298 Tau c (bottom) centered on the helium triplet (dashed gray lines). The dark and light shaded colored regions correspond to the 1σ and 3σ uncertainties, respectively. Telluric regions are shown in the shaded gray regions, as in Figures 2, 3, and 4.
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: Phase-resolved signal-to-noise map of absorption for the partial transit (no pre-ingress baseline) of HD 63433b centered on the helium triplet in the stellar rest frame, compared to fourth contact (solid white line) and the planet’s orbital motion (dashed white lines).
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: Examples of pre- (black) and post-telluric-corrected spectra for K2-100b (green), HD 63433b (purple), and V1298 Tau c (orange). The best-fitting molecfit H2O models are shown in light blue. The telluric OH emission occurs in the shaded gray region; however, this feature is successfully removed by the A–B nod pair subtraction. The dashed gray lines indicate the location of the He triplet, which is different in each observer frame, due to the combination of the barycentric and systemic velocities.
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: In-transit (green) and out-of-transit (black) stellar spectra of K2-100b for all individual spectral frames (top) and the mean spectra (middle), as well as the excess absorption (bottom) centered on the helium triplet (dashed black lines). The OH emission (light gray) and H2O absorption (dark gray) telluric regions are also indicated.
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: In-transit (orange) and out-of-transit (black) stellar spectra of V1298 Tau c for all spectral frames (top) and the mean spectra (middle), as well as the excess absorption (bottom) centered on the helium triplet (dashed black lines). The OH emission (light gray) and H2O absorption (dark gray) telluric regions are also indicated.
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: In-transit (purple) and out-of-transit (black) stellar spectra of HD 63433b for all spectral frames (top) and the mean spectra (middle), as well as the excess absorption (bottom) centered on the helium triplet (dashed black lines). The OH emission (light gray) and H2O absorption (dark gray) telluric regions are also indicated.
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: Phase-resolved signal-to-noise map for the partial transit of V1298 Tau c centered on the helium triplet in the stellar rest frame, compared to the first contact point (solid white lines) and the planet’s orbital motion (dashed white lines).
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: Phase-resolved signal-to-noise map for K2-100b centered on the helium triplet in the stellar rest frame, compared to the first and fourth contact points (solid white lines) and the planet’s orbital motion (dashed white lines).
Paper: Nondetections of Helium in the Young Sub-Jovian Planets K2-100b, HD 63433b, and V1298 Tau c
Authors: Munazza K. Alam, James Kirk, Leonardo A. Dos Santos, Patrick McCreery, Andrew P. Allan, James E. Owen, Aline A. Vidotto, Romain Allart, Vincent Bourrier, Néstor Espinoza, George W. King, Mercedes López-Morales, Julia V. Seidel
Figure caption: Best-fit results for simultaneously modeling the instrumental systematics and atmospheric escape signal.
Paper: Accurate and Model-independent Radius Determination of Single FGK and M Dwarfs Using Gaia DR3 Data
Authors: Rocio Kiman, Timothy D. Brandt, Jacqueline K. Faherty, Mark Popinchalk
Figure caption: Mass–radius relation for the sample from Kiman et al. (2019). Inactive stars according to Hα are shown in gray and active stars are color-coded by fractional Hα luminosity. We only include the typical uncertainly (median) of the sample. Active stars show larger radii than inactive stars, indicating that radius inflation is correlated with magnetic activity.
Paper: Accurate and Model-independent Radius Determination of Single FGK and M Dwarfs Using Gaia DR3 Data
Authors: Rocio Kiman, Timothy D. Brandt, Jacqueline K. Faherty, Mark Popinchalk
Figure caption: Same data as in Figure 8 divided into two bins of metallicity: 0.73 ≤ ζ TiO/CaH < 0.94 (left panel), which corresponds roughly to −0.5 ≤ [Fe/H] < −0.15 dex, and a solar-metallicity bin of 0.97 ≤ ζ TiO/CaH < 1.09 (right panel), which is approximately −0.1 ≤ [Fe/H] < 0.1 dex. We include in the lower panels the fractional radius difference between the radii of the active stars and the fit to the inactive stars for the same mass. In dark blue we show the median and standard deviation for four bins in mass. When we separate the stars by metallicity, the overlap between active and inactive stars seen in Figure 8 decreases.
Paper: Accurate and Model-independent Radius Determination of Single FGK and M Dwarfs Using Gaia DR3 Data
Authors: Rocio Kiman, Timothy D. Brandt, Jacqueline K. Faherty, Mark Popinchalk
Figure caption: Estimated radii for the Kiman et al. (2019) sample of M dwarfs as a function of Hα EW, divided in four mass bins: 0.5 < M[M ⊙] ≤ 0.6, 0.4 < M[M ⊙] ≤ 0.5, 0.3 < M[M ⊙] ≤ 0.4, and 0.2 < M[M ⊙] ≤ 0.3. We estimated Kendall’s τ coefficient and the p-value to test the hypothesis of no correlation in the data. The results are shown in the legend of each panel.
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 (dedispersed) MFS differenced image from Category B—average of XX and YY polarizations. Color bar scale is in 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 waterfall plot showing narrowband RFI (Observation 1160580872). (177.5 MHz is a common DTV broadcast frequency in WA). Color bar scale is in 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: Calculated upper bound event rates at lowest and highest DM values.
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: Calculated upper bound event rates (DM = 170 pc cm−3).
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 of screening for repeat nondispersed signals. Single 7σ detections (circled) were retained, others discarded.
Paper: Asteroid Period Solutions from Combined Dense and Sparse Photometry
Authors: Michael Gowanlock, David E. Trilling, Andrew McNeill, Daniel Kramer, Maria Chernyavskaya
Figure caption: Comparison of rotation period distributions as scatterplots for SS1 and TESSC1 as a function of SS1∩TESSC1, plotted in the left and right panels, respectively. The SS1∩TESSC1 rotation periods and color-coded amplitudes are from the n = 1623 sample that has all optimizations applied and low-confidence solutions removed. In contrast to prior figures, such as Figure 12, the plot is shown on a log scale such that the entire period range can be shown. Consistent periods between the two data sets appear on the diagonal line.
Paper: Asteroid Period Solutions from Combined Dense and Sparse Photometry
Authors: Michael Gowanlock, David E. Trilling, Andrew McNeill, Daniel Kramer, Maria Chernyavskaya
Figure caption: Light curves of object 363. Panels from top to bottom are as follows: SS1∩TESSC1 (p = 16.811 hr), TESSC1 (p = 16.801 hr), SS1 (p = 23.963 hr), and the unphased data for SS1∩TESSC1. The LCDB rotation period is reported as 8.401 hr, which is a factor 0.5 of the TESSC1 derived rotation period solution of 16.801 hr (middle panel). This light curve is also remarkable because it has extra structure at the peaks instead of simply having a sinusoidal shape.
Paper: Asteroid Period Solutions from Combined Dense and Sparse Photometry
Authors: Michael Gowanlock, David E. Trilling, Andrew McNeill, Daniel Kramer, Maria Chernyavskaya
Figure caption: Light curves of object 3176. Panels from top to bottom are as follows: SS1∩TESSC1 (p = 20.457 hr), TESSC1 (p = 20.433 hr), SS1 (p = 10.224 hr), and the unphased data for SS1∩TESSC1.
Paper: Asteroid Period Solutions from Combined Dense and Sparse Photometry
Authors: Michael Gowanlock, David E. Trilling, Andrew McNeill, Daniel Kramer, Maria Chernyavskaya
Figure caption: Light curves of object 339. Panels from top to bottom are as follows: SS1∩TESSC1 (p = 2349.795 hr), TESSC1 (p = 5.967 hr), SS1 (p = 47.957 hr), and the unphased data for SS1∩TESSC1. Orange and black markers refer to observations from TESSC1 and SS1, respectively. The bottom panel shows photometric errors that are plotted using magenta bars, and the markers are plotted on top of the error bars to prevent them from being obfuscated.
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 same as Figure 12, but where low-confidence solutions have been removed.
Paper: Asteroid Period Solutions from Combined Dense and Sparse Photometry
Authors: Michael Gowanlock, David E. Trilling, Andrew McNeill, Daniel Kramer, Maria Chernyavskaya
Figure caption: Light curves of object 18975. Panels from top to bottom are as follows: SS1∩TESSC1 (p = 404.538 hr), TESSC1 (p = 413.212 hr), SS1 (p = 404.608 hr), and the unphased data for SS1∩TESSC1.
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 same as Figure 12, but where we only show those classified as correct with the conservative binary classifier described in Section 4.3. The thresholds are as follows: an amplitude of 0.125 mag, 120 observations, and an LSP power of 0.5.
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 amplitudes of the n = 1623 sample of objects in SS1∩TESSC1 that have all optimizations applied and low-confidence solutions removed. The top horizontal axis shows the ﹩\tfrac{b}{a}﹩ ratio, which is calculated directly from the amplitude (Δmag) where Δmag = ﹩-2.5\mathrm{log}\tfrac{b}{a}﹩.
Paper: Asteroid Period Solutions from Combined Dense and Sparse Photometry
Authors: Michael Gowanlock, David E. Trilling, Andrew McNeill, Daniel Kramer, Maria Chernyavskaya
Figure caption: Light curves of object 14376. Panels from top to bottom are as follows: SS1∩TESSC1 (p = 5.849 hr), TESSC1 (p = 5.848 hr), SS1 (p = 5.849 hr), and the unphased data for SS1∩TESSC1.
Paper: The Nonsingular Estimator for Exoplanet Orbits: An Unscented Batch Estimation Method for Direct Imaging Measurements
Authors: Zvonimir Stojanovski, Dmitry Savransky
Figure caption: Orbital parameter estimates for β Pictoris b. For NEXO, we show the means and 95% credible intervals, and for MCMC, we show the medians and 95% confidence intervals reported by Nielsen et al. (2014) using the fixed-mass method. We shift Ω and ω in the MCMC fit by 180° for consistency. The central estimates using the two methods are quite close for all of the elements except ω. Furthermore, the central estimates for NEXO and MCMC are always within the intersection of the intervals for the two methods.
Paper: The Nonsingular Estimator for Exoplanet Orbits: An Unscented Batch Estimation Method for Direct Imaging Measurements
Authors: Zvonimir Stojanovski, Dmitry Savransky
Figure caption: Orbital parameter estimates for GJ 504 b. For NEXO, we show the means and 95% credible intervals, and for OFTI, we show the medians and 95% confidence intervals reported by Blunt et al. (2017). NEXO and OFTI give nearly equal central estimates for all elements except Ω and ω; the larger differences in those two elements may be due to the long period of the orbit.
Paper: The Nonsingular Estimator for Exoplanet Orbits: An Unscented Batch Estimation Method for Direct Imaging Measurements
Authors: Zvonimir Stojanovski, Dmitry Savransky
Figure caption: Credible intervals for the semimajor axis. All three methods give accurate central estimates. However, the credible intervals for NEXO are much narrower than for MCMC or OFTI.
Paper: The Nonsingular Estimator for Exoplanet Orbits: An Unscented Batch Estimation Method for Direct Imaging Measurements
Authors: Zvonimir Stojanovski, Dmitry Savransky
Figure caption: Astrometric measurements and orbit fits for GJ 504 b. We see good agreement between the orbit fit and the true measurements. However, the measurements appear to cover a smaller fraction of the orbit than for β Pictoris b, making this a more challenging fit.
Paper: The Nonsingular Estimator for Exoplanet Orbits: An Unscented Batch Estimation Method for Direct Imaging Measurements
Authors: Zvonimir Stojanovski, Dmitry Savransky
Figure caption: Astrometric measurements and orbit fits for β Pictoris b. The fit follows the true measurements very closely, despite the apparent “jumps” in both ρ and θ.
Paper: The Nonsingular Estimator for Exoplanet Orbits: An Unscented Batch Estimation Method for Direct Imaging Measurements
Authors: Zvonimir Stojanovski, Dmitry Savransky
Figure caption: Accuracy metrics for NEXO with various prior scaling factors.
Paper: The Nonsingular Estimator for Exoplanet Orbits: An Unscented Batch Estimation Method for Direct Imaging Measurements
Authors: Zvonimir Stojanovski, Dmitry Savransky
Figure caption: Accuracy metrics for NEXO with various numbers of mixture components.
Paper: The Nonsingular Estimator for Exoplanet Orbits: An Unscented Batch Estimation Method for Direct Imaging Measurements
Authors: Zvonimir Stojanovski, Dmitry Savransky
Figure caption: Convergence of Newton–Raphson iteration for φ with M 0 = 120°.
Paper: The Nonsingular Estimator for Exoplanet Orbits: An Unscented Batch Estimation Method for Direct Imaging Measurements
Authors: Zvonimir Stojanovski, Dmitry Savransky
Figure caption: Convergence of Newton–Raphson iteration for φ with ΔM = 120°.
Paper: Investigating Asymmetry Development from SiO to H2O Maser Regions in VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Youngjoo Yun, Haneul Yang, Jaeheon Kim
Figure caption: Optical light curve of VX Sgr from AAVSO (top) and integrated antenna temperature (single-dish) and recovered flux (VLBI) according to the pulsation phases (bottom). The vertical dotted line denotes the optical maximum. In the top figure, the red and blue triangles correspond to the VLBI and single-dish observation dates, respectively. In the bottom figure, the black diamonds and red circles indicate single-dish and VLBI flux variations, respectively. The single-dish data were referenced from Figure 5(b) in Yoon et al. (2023).
Paper: Investigating Asymmetry Development from SiO to H2O Maser Regions in VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Youngjoo Yun, Haneul Yang, Jaeheon Kim
Figure caption: Moment-zero maps of each 43.1 GHz SiO maser transition line. The contour levels are adopted at 10 12 15 20 25 30 50... for multiples of each rms value.
Paper: Investigating Asymmetry Development from SiO to H2O Maser Regions in VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Youngjoo Yun, Haneul Yang, Jaeheon Kim
Figure caption: Moment-zero maps of each 86.2 GHz SiO maser transition line. The contour levels are adopted at 10 12 15 20 25 30 50... for multiples of each rms value.
Paper: Investigating Asymmetry Development from SiO to H2O Maser Regions in VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Youngjoo Yun, Haneul Yang, Jaeheon Kim
Figure caption: Moment-zero maps of each 42.8 GHz SiO maser transition line. The contour levels are adopted at 10 12 15 20 25 30 50... for multiples of each rms value.
Paper: Searching for Protoplanets around MWC 758 and MWC 480 in Br-γ Using Kernel Phase and SCExAO/CHARIS
Authors: Alexander Chaushev, Steph Sallum, Julien Lozi, Jeffrey Chilcote, Tyler Groff, Olivier Guyon, N. Jeremy Kasdin, Barnaby Norris, Andy Skemer
Figure caption: Estimated achieved contrast (contours) for band 7/2163 nm of the high-resolution K-band data for MWC 758 (left) and MWC 480 (right). These contours were calculated using the “per-pointing” SDI calibration and estimated by using the χ 2 interval method as discussed in Chaushev et al. (2023). The equivalent sensitivity of the RDI calibration (pink dashed line) is also shown. SDI improves on the RDI sensitivity by up to ∼2 mag depending on the separation. An example typical inner working angle for a CHARIS Lyot corongraph would range anywhere from 1 to 3 λ/D. An accretion rate of 10−6  M jup. yr−1 would form a 5 M jup planet on the typical disk-lifetime scale of ∼5 Myr. Therefore, assuming a planet mass of 10 M jup, we would be sensitive to accretion rates as low as 10−7  M jup. yr−1 at larger separations and 10−6  M jup. yr−1 down to around 50 mas. This sensitivity allows us to place limits on rapidly accreting massive planets around MWC 480 and MWC 758. For 1 M jup planets, we would only be able to detect the planet during the runaway accretion phase or shortly thereafter, when accretion rates are exceptionally high (Ginzburg & Chiang 2019).