adsabs/AstroCLIMB huggingface dataset:
Paper: The Effect of Offsets from True Orbital Parameters on Exoplanet High-resolution Transmission Spectra
Authors: Yasmine J. Meziani, Laura Flagg, Jake D. Turner, Emily K. Deibert, Ray Jayawardhana, Adam B. Langeveld, Ernst J. W. de Mooij
Figure caption: The results of cross-correlating the transmission spectrum—generated after injecting a CrH spectral signature into the data—with a model of WASP-85Ab’s spectral signal using different offsets in transit midpoint are shown. The top plot displays the 2D Kp-vsys map (also known as the CCF matrix) for an ephemeris offset of −16 minutes, while the bottom plot shows the same for an offset of 16 minutes. We observe that larger transit midpoint offsets correspond to higher systemic velocities, indicating a positive correlation.
Paper: The Effect of Offsets from True Orbital Parameters on Exoplanet High-resolution Transmission Spectra
Authors: Yasmine J. Meziani, Laura Flagg, Jake D. Turner, Emily K. Deibert, Ray Jayawardhana, Adam B. Langeveld, Ernst J. W. de Mooij
Figure caption: Cross-correlation results showing the effects of eccentricity offsets. (a) We cross-correlated the transmission spectrum—generated by injecting a CrH spectral signature into the data—with a model of WASP-85Ab’s spectral signal, using eccentricity offsets of −0.05 and 0.08 relative to the true value of 0.05. (b) The same as Figure 4(a), but for a true eccentricity of 0.12 with offsets of −0.12 and 0.08.
Paper: The Effect of Offsets from True Orbital Parameters on Exoplanet High-resolution Transmission Spectra
Authors: Yasmine J. Meziani, Laura Flagg, Jake D. Turner, Emily K. Deibert, Ray Jayawardhana, Adam B. Langeveld, Ernst J. W. de Mooij
Figure caption: Contour plots to approximate vshift for different offsets in ephemeris. The top three panels of the figure use fixed Kp values of 100 km s−1, 150 km s−1, and 200 km s−1, while varying the period and ephemeris offset. The bottom three panels use fixed period values of 1 day, 2 days, and 5 days, while varying the Kp and ephemeris offset.
Paper: Asteroseismology of the Red Giant Companions to Gaia BH2 and BH3
Authors: Daniel Hey, Yaguang Li, 亚光 李, J. M. Joel Ong, 加冕 王
Figure caption: Top panel: TESS target pixel file cutouts of the three sectors of Gaia BH2, with the selected aperture overlaid in red. Note the presence of potential nearby contaminants. Within two pixels of the selected aperture, there are no contaminants brighter than 13th Gaia magnitude besides BH2* itself. Bottom panel: light curves from each sector obtained through regression correction. All the light curves have been binned to a uniform 30 minute cadence, and outliers have been removed.
Paper: Asteroseismology of the Red Giant Companions to Gaia BH2 and BH3
Authors: Daniel Hey, Yaguang Li, 亚光 李, J. M. Joel Ong, 加冕 王
Figure caption: The photometric rotational period of BH2* is unlikely to have arisen without tidal forcing. Here we show the rotational evolution of MESA stellar models initialized at various fractions of the zero-age main-sequence breakup rotational frequency, indicated by the color map. Magnetic braking (calculated here using the prescription of J. L. van Saders & M. H. Pinsonneault 2013) causes stellar rotation to slow over evolutionary timescales, shown here using ﹩{\nu }_{{\rm{\max }}}﹩ as an age proxy. No other sources of angular momentum loss (such as mass loss) are accounted for in this simulation. Even under this extremely permissive scenario, our putative photometric rotation period (horizontal line) at the present day (vertical line) is faster than permitted by if BH2*’s rotation were to be attributed entirely to its primordial angular momentum.
Paper: Asteroseismology of the Red Giant Companions to Gaia BH2 and BH3
Authors: Daniel Hey, Yaguang Li, 亚光 李, J. M. Joel Ong, 加冕 王
Figure caption: Top panel: ASAS-SN (blue circle) and ATLAS (orange diamond) light curves of BH2*. The ASAS-SN light curve is the combination of several different cameras in the network, each of which has its own offset, which has been median-divided out. Bottom panel: the power spectra of the ASAS-SN (blue) and ATLAS (orange) light curves. The dashed black lines indicate measured periods at 397, 495, and 1513 days. The inset on the bottom panel shows the window function (in frequency, day−1), with a signal at Earth’s orbital frequency (1/365) day−1. There are no peaks in the ASAS-SN window function associated with our measured periods (black dashed lines).
Paper: Asteroseismology of the Red Giant Companions to Gaia BH2 and BH3
Authors: Daniel Hey, Yaguang Li, 亚光 李, J. M. Joel Ong, 加冕 王
Figure caption: (a) Power spectral density of BH2*, with the power excess around 60 μHz. The red line is the power spectrum convolved with a Gaussian kernel of width 0.2  μHz, highlighting the individual modes. (b) The echelle diagram of the PSD at the measured Δν  (dashed line). (c) The echelle diagram for a Kepler twin (see the main text), with similar stellar properties. (d) The collapsed echelle diagram of BH2* (black) and the Kepler twin (blue), highlighting the radial, dipole, and quadrupole modes.
Paper: Asteroseismology of the Red Giant Companions to Gaia BH2 and BH3
Authors: Daniel Hey, Yaguang Li, 亚光 李, J. M. Joel Ong, 加冕 王
Figure caption: Posteriors of stellar properties of BH3* sampled from the stellar models, with temperature, luminosity, and metallicity priors (orange), and with an additional age prior (blue).
Paper: Asteroseismology of the Red Giant Companions to Gaia BH2 and BH3
Authors: Daniel Hey, Yaguang Li, 亚光 李, J. M. Joel Ong, 加冕 王
Figure caption: Power spectrum of BH3*. The red line is the power spectrum convolved with a Gaussian kernel of width 0.2 μHz, to highlight the absence of any significant signal. The blue vertical and horizontal lines correspond to the predicted power excess and power of the asteroseismic signal.
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: Recovered sample from our ETV simulations (small orange markers, shaded by circumbinary mass) overlaid on the known circumbinary planet population. The gray shading shows the full simulated population. Green triangles mark the Lomb–Scargle search ranges for our ETV survey of 152 targets. The black lines indicate circumbinary period constraints, with orbits below 4 × Pbinary considered dynamically unstable. In comparison, periods up to 10 × Pbinary were excluded from our recovery methodology owing to susceptibility to Nyquist aliases and dynamical ETVs rather than LiTE. Several circumbinary planets (e.g., Kepler-1660 b, Kepler-1647 b, Kepler-34 b, Kepler-47 c/d) that broadly overlap with our simulations are labeled for reference, along with our candidate TIC 142979644 (TIC 1429).
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: Distributions of the simulated binary and circumbinary parameters. The subscripts bin, 1, 2, 3, PL, and BD correspond to parameters related to the binary system, primary star, secondary star, circumbinary object, planet mass, and brown dwarf mass, respectively. Note that all vertical axes are logarithmic, while some horizontal axes are also logarithmic. The full set of 4 × 106 samples is represented in light color, while the eclipsing binary sample (287,472 systems, or 7.2%) is shown in dark color. The ETV amplitude (AETV) values were calculated only after a binary eclipse condition was satisfied; therefore, this parameter is displayed exclusively in dark colors. Other binary and circumbinary parameters were sampled from uniform distributions and are not shown here. See Sections 2.6.1 and 2.6.2 for further details.
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: Ratios of detected to true ETV amplitudes (top) and periods (bottom) in the CBD simulations, plotted against the number of observed TESS sectors. Point sizes are proportional to the phase coverage, with the scale shown in the upper right corner in units of circumbinary periods, and colors indicate the FAP of the detected signal. Numbers below each bin indicate the number of systems in that bin. Large deviations from unity are common for short baselines, but both amplitudes and periods converge toward the true values as the baseline increases, with minimal scatter beyond ∼20 sectors.
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: Similar to Figure 7, but for the CBD group after applying the SNR, FAP, and detected-to-binary period ratio thresholds, zoomed to the 0.1–10 ratio range on both axes. The color scale represents true periods, with darker points indicating longer periods. Gray markers are for true periods longer than 3000 days. Point sizes are proportional to SNR. The inset in the lower right corner represents the data within the 1/n–n ratio range on both axes. There are 2317 data points within the 1/2–2 ratio range and 3022 points within the 1/3–3 ratio range, including true periods longer than 3000 days (gray).
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: The distribution of the simulated binary sample in the equatorial coordinates, with color-coding based on the number of TESS sectors. Warmer colors represent areas with higher observational coverage. The TESS CVZs appear as the red regions near the ecliptic poles.
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: TESS magnitude vs. ETV uncertainty (σETV) for the entire sample of eclipsing binaries (black points) and the recovered sample (orange circles). Point colors indicate the inferred circumbinary companion masses, and the dashed contours highlight density variations in the entire sample. The recovered systems are concentrated in regions with lower timing uncertainties, while the overall distribution shows increasing uncertainty with decreasing brightness.
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: Correlation between detected-to-true period ratio and amplitude ratio across data points for the CBD group. The color scale represents the FAP, with darker points indicating lower FAP values. Markers with turquoise edges are for true periods longer than 3000 days. Point sizes are proportional to SNR.
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: The distributions of parameters for the CBD group. The light colors are for all the samples where the binary is eclipsing, while the dark colors are for the sample where circumbinary objects are detected in the 1/3–3 range for amplitude and period ratios. Note that both axes for all distributions are on a logarithmic scale.
Paper: Eclipse Timing Variations of Circumbinary Substellar Objects in TESS Data
Authors: Ekrem M. Esmer, Tansu Daylan
Figure caption: Similar to Figure 8, but for the UBD group.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: Scaling relations for NGVS galaxies with ﹩\mathrm{log}{M}_{\star }\,\leqslant \,10﹩. Panels: (a) size–magnitude (﹩\mathrm{log}{r}_{e,g}﹩ vs. Mg), (b) effective surface brightness (μe,g vs. Mg), (c) mean surface brightness within one effective radius (〈μ〉e,g vs. Mg), and (d) color–magnitude (u − i vs. Mg). Black curves show polynomial fits to the NGVS population; long-dashed black lines mark the ±2.5σ envelopes. UDG candidates (blue) and compact galaxies (red) are highlighted. Marker shape encodes how many relations the object is an outlier in: circles = 1, triangles = 2, squares = 3. Outliers are defined as points lying outside the ±2.5σ envelope of the corresponding fit.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: Cumulative distribution functions of the local surface density for 3675 NGVS galaxies with measured surface density (out of the 3689 total in the sample). The left panel shows the distribution by structural code, while the right panel presents the distribution by star formation code. Dotted lines indicate the median density for each classification.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: Surface density profiles for Virgo cluster galaxies. Profiles are measured in circular annuli centered on M87. The left and right panels show profiles found for subsets of the galaxy population after dividing by structural code and star formation code, respectively. The vertical dashed lines show the radii at which the total (i.e., full sample) surface density profile falls to one-half (r50) and one-tenth (r10) of its peak value.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: (Left panel) Distribution in the sky of 3689 confirmed or probable Virgo cluster members from the NGVS. Symbol colors indicate different morphological structural codes, as indicated in the legend. For reference, the large red circles indicate the virial radii of Virgo’s two major subclusters, centered on M87 (A) and M49 (B). The footprint of the NGVS is shown in light gray. (Right panel) Same as the previous panel, except now with symbols showing different star formation codes.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: (Left panel) CMDs for 3689 members of the Virgo cluster from the NGVS. The distribution of galaxies in the g–(u-i) plane is shown with symbols color coded according to the NGVS structural code, as indicated in the legend. Note that power-law fits for the SI and I structural codes are not shown due to the sparsity of data. (Right panel) Same as the previous panel, except with color coding based on the NGVS star formation code.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: A mosaic of the 30 compact galaxies listed in Table 4. The sample includes both M32-like objects, BCD galaxies, as well as intermediate systems. Each panel measures 1﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩5 × 1﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩5 with north at the top and east to the left. The sample includes both M32-like objects (e.g., NGVS50 and NGVS400) and BCD galaxies (e.g., NGVS1515 and NGVS231).
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: Secondary morphologies from the EVCC compared to our structural and star formation codes (left and right panels, respectively). The symbol size is proportional to the number of galaxies at each point on this grid, with the number of galaxies labeled in each case. Note that most of the 661 galaxies in this comparison have either RA or BE morphologies in the EVCC.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: Same as Figure 5 for comparing the primary morphological classifications in the EVCC with NGVS structural codes.
Paper: The Next Generation Virgo Cluster Survey (NGVS). XL. The Morphological Classification of Virgo Cluster Galaxies
Authors: Max M. Kurzner, Patrick Côté, Laura Ferrarese, Kaixiang Wang, Eric W. Peng, Scott Wilkinson, Joel C. Roediger, Chelsea Spengler, Toby Brown, Chengze Liu, Sungsoon Lim, Rubén Sánchez-Janssen, Elisa Toloba, Puragra Guhathakurta, John P. Blakeslee, Patrick R. Durrell, Ariane Lançon, J. Christopher Mihos, Matthew A. Taylor, Tyrone E. Woods, Solveig Thompson, Lauren A. MacArthur
Figure caption: A mosaic of 66 candidate merger or postmerger galaxies from the NGVS. Each panel measures 3′ × 3′ with north at the top and east to the left.
Paper: A Comprehensive Reanalysis of K2-18 b’s JWST NIRISS+NIRSpec Transmission Spectrum
Authors: Stephen P. Schmidt, Ryan J. MacDonald, Shang-Min Tsai, Michael Radica, Le-Chris Wang, Eva-Maria Ahrer, Taylor J. Bell, Chloe Fisher, Daniel P. Thorngren, Nicholas Wogan, Erin M. May, Piero Ferrari, Katherine A. Bennett, Zafar Rustamkulov, Mercedes López-Morales, David K. Sing
Figure caption: Detection significances of CH4, CO2, and DMS from POSEIDON retrievals of K2-18 b’s JWST NIRISS SOSS + NIRSpec G395H transmission spectrum. Each grid cell represents a Bayesian model comparison between two retrievals, one with and one without a molecule, for a specific NIRISS SOSS and NIRSpec G395H data variant pair. The data variants are ordered with increasing spectral resolution to the right (for NIRSpec) and down (for NIRISS). The cells are colored and annotated according to the detection significance equivalent to the calculated Bayes factor (e.g., R. Trotta 2008; B. Benneke & S. Seager 2013). Bayes factors <3 (equivalent to <2.1σ), corresponding to no evidence on the Jeffreys’ scale, are donated by “—.” Our retrievals demonstrate strong evidence for CH4, but find no reliable statistical evidence for CO2 or DMS in K2-18 b’s atmosphere.
Paper: A Comprehensive Reanalysis of K2-18 b’s JWST NIRISS+NIRSpec Transmission Spectrum
Authors: Stephen P. Schmidt, Ryan J. MacDonald, Shang-Min Tsai, Michael Radica, Le-Chris Wang, Eva-Maria Ahrer, Taylor J. Bell, Chloe Fisher, Daniel P. Thorngren, Nicholas Wogan, Erin M. May, Piero Ferrari, Katherine A. Bennett, Zafar Rustamkulov, Mercedes López-Morales, David K. Sing
Figure caption: Sensitivity of K2-18 b’s atmospheric composition to different data treatments and retrieval configurations. Top: comparison between POSEIDON retrievals of data reduced by the FIREFLy and exoTEDRF pipelines. Middle: comparison between POSEIDON retrievals of low-resolution (NIRISS SOSS, R ≈ 25; NIRSpec G395H, R ≈ 100) and high-resolution (pixel-level) exoTEDRF data. Bottom: comparison between the retrieval codes POSEIDON and BeAR on FIREFLy data. The retrieved model transmission spectra, plotted at R ≈ 100 for clarity, show the median (solid lines) and ± 1σ and ± 2σ credible regions (contours) corresponding to the data set(s) shown in each panel. The median retrieved offsets have been applied to the NIRSpec G395H NRS1 and NRS2 data sets. Right: the retrieved CH4, CO2, and DMS abundances corresponding to each retrieval. Our retrievals find broadly consistent CH4 abundances, indicating a robust detection (the median and ±1σ abundance constraints are represented by solid and dashed lines, respectively). However, any suggestions of CO2 and DMS depend on the specific data reduction and data resolution, indicating unreliable inferences (hence the 95% upper limits, represented by arrows).
Paper: A Comprehensive Reanalysis of K2-18 b’s JWST NIRISS+NIRSpec Transmission Spectrum
Authors: Stephen P. Schmidt, Ryan J. MacDonald, Shang-Min Tsai, Michael Radica, Le-Chris Wang, Eva-Maria Ahrer, Taylor J. Bell, Chloe Fisher, Daniel P. Thorngren, Nicholas Wogan, Erin M. May, Piero Ferrari, Katherine A. Bennett, Zafar Rustamkulov, Mercedes López-Morales, David K. Sing
Figure caption: Comparison between our transmission spectra and the reduction from N. Madhusudhan et al. (2023). Three of our reductions, which were performed at the pixel-level and then binned to R ≈ 55, are shown: exoTEDRF (green squares), FIREFLy (blue diamonds), and the NIRSpec-only Eureka! reduction B (gray downward-pointing triangles). We show only Eureka! reduction B, since reduction A was performed at R = 100. We compare these binned pixel-level data to the low-resolution data from N. Madhusudhan et al. (2023), which were obtained using the JExoRES pipeline (black error bars; M. Holmberg & N. Madhusudhan 2023). The N. Madhusudhan et al. (2023) data were binned directly from their pixel-level data, so we bin our pixel-level data using the same binning approach. These R ≈ 55 data sets are purely for visual comparison with N. Madhusudhan et al. (2023), and are not used for retrievals later in our study. Wavelength locations of CH4, CO2, and DMS absorption features are annotated.