adsabs/AstroCLIMB huggingface dataset:
Paper: Fishing for Planets: A Comparative Analysis of EPRV Survey Performance in the Presence of Correlated Noise
Authors: Arvind F. Gupta, Megan Bedell
Figure caption: Comparison of ﹩{[K\,/\,{\sigma }_{K}]}_{\oplus }﹩ for a 10 yr survey with 100 observations per year (vertical axis) and a 5 yr survey with 200 observations per year (horizontal axis). We compute the latter values using the first 5 yr of observations from the 20-star survey simulations. On the left, we show that for the quasi-periodic kernel the longer 10 yr survey delivers a higher detection significance than the higher-cadence 5 yr survey. On the right, we show that the opposite is true for the Matérn-5/2 kernel, which performs better with a higher observing cadence.
Paper: Utilizing Voronoi Tessellations to Determine Radial Density Profiles
Authors: Veronika Dornan, William E. Harris
Figure caption: A boxplot depicting the results of the number of objects in each system returned when the radial density profile obtained from each method is integrated, done across all 30 random object distributions for each system. The dashed line shows where 100% of all objects are returned. The boxes represent the interquartile range (IQR), the black lines within the boxes denote the medians, the diamonds denote the means, and the error bars encompass all nonoutlier data that lie outside the IQR. The colored circles represent outliers, defined as data that lie greater than 1.5 times the IQR past the upper and lower quartiles.
Paper: Utilizing Voronoi Tessellations to Determine Radial Density Profiles
Authors: Veronika Dornan, William E. Harris
Figure caption: The density data for the observed GCSs MASX J13272961-3123237 (top) and ESO 509-G067 (bottom) using the annulus fitting method (red data points) and the Voronoi fitting method (blue data points). Both data sets are fit with a power-law function. The gray-shaded region is unobservable due to high surface brightness.
Paper: Utilizing Voronoi Tessellations to Determine Radial Density Profiles
Authors: Veronika Dornan, William E. Harris
Figure caption: A histogram of the normalized density of Voronoi cells for a Hubble distribution. The red curve is the log-normal fit to the histogram and the red line is the average for the Hubble distribution. The blue curve is the fit to the histogram for a uniform distribution and the blue line is average for the uniform distribution. The black line is the mean normalized number density, where x = n/〈n〉 = 1 when n = 〈n〉 for all distributions.
Paper: Utilizing Voronoi Tessellations to Determine Radial Density Profiles
Authors: Veronika Dornan, William E. Harris
Figure caption: Sample radial profile showing the radial density distributions for one, three, five, and seven objects percell (going from top down). All annulus data and fitting are identical, as they are independent from the Voronoi fitting.
Paper: Utilizing Voronoi Tessellations to Determine Radial Density Profiles
Authors: Veronika Dornan, William E. Harris
Figure caption: The density data for the same system using the annulus fitting method (red data points) and the Voronoi fitting method (blue data points). Both data sets are fit with a power-law function and compared to the “true” Hubble profile (green line).
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: Astrometrically registered velocity-integrated intensity maps of the H2O and SiO maser obtained from the noninteger SFPR method for 2017.12. 8 (ϕ = 2.79). Purple, blue, red, and yellow colors represent the 22.2 GHz H2O, 43.1, 42.8, and 86.2 GHz SiO maser, respectively. The right figure depicts an enlarged view of the SiO maser, and the color index is the same as that on the left. The concentric circles are the ring-fitting range of each SiO maser, including the uncertainty.
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: Schematic of the relationship between near the SiO maser CSE and H2O maser. Black and turquoise green arrow tips indicate the outward and inward motion directions in the SiO maser ring structure, respectively. The multicolored arrows roughly represent the velocity components of the ambient atmosphere affected by stellar pulsations: red denotes the redshifted velocity component, blue denotes the blueshifted velocity component, and the other color represents the near-stellar velocity component. (a) Schematic perpendicular to the line-of-sight direction. (b) and (c) Extrapolation of the atmospheric motion to the H2O maser region located outside the dust layer, showing the red- and blueshifted and near-stellar velocity components.
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: Total, red- and blueshifted, and near-stellar velocity spot map of the H2O maser at about one-year intervals. The first row represents all spots, the second row represents red- and blueshifted velocity spots (v < −4.7, v > 15.3 km s−1), and the third row represents near-stellar velocity spots (−4.7 < v < 15.3 km s−1). The spot color indicates the local-standard-of-rest velocity and the spot size indicates the logarithmic scale of the intensity. The pink star at the center represents the position of the central star obtained by the ring fitting of the SiO maser using noninteger SFPR for alignment.
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: Positions of the four prominent features NE, SW, N, and SE track morphological changes in the 43.1 and 86.2 GHz SiO masers. The bottom graph represents the distance of the NE–SW and N–SE values with the maximum intensity measured by the position–velocity spot maps. Blue and green dots represent distance measurements between the peak velocity spots associated with NE–SW and N–SE pairs. The red dotted line represents the one-dimensional trend line of the measured distances. The figures on the right depict position–velocity spot maps for the same epoch.
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 magnitude variation of VX Sgr from AAVSO (top) and change in SiO maser ring radius according to the optical phase (bottom). In the top figure, the vertical dotted lines and the red triangles denote the optical maximum and observation dates, respectively. In the bottom figure, the blue, red, yellow, and cyan colors signify the 43.1, 42.8, 86.2, and 129.3 GHz SiO maser ring radii, respectively. The ring-fitting uncertainty is indicated by the vertical bar. Fake features due to side lobes are a dominant source of errors in ring fitting from position–velocity spot maps.
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: H2O maser proper motion represented in R.A., decl. direction. The left figure represents the total velocity range, and the middle and right figures indicate the ranges of red- and blueshifted velocity and the near-stellar velocity, respectively.
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: Shape transformation of the SiO maser from the ring-shaped structure to the NE–SW direction from 2017 September to 2018 March.
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: Histogram of the maser spot distribution toward the central star on a similar date. The first row represents the total velocity spots, and the second and third rows depict the red- and blueshifted velocity spots and the near-stellar velocity spots, respectively.
Paper: Evolution of Flare Activity in GKM Stars Younger Than 300 Myr over Five Years of TESS Observations
Authors: Adina D. Feinstein, Darryl Z. Seligman, Kevin France, Jonathan Gagné, Adam Kowalski
Figure caption: Comparison of three flare-driven metrics in searching for evidence of stellar cycles. Each column contains information for the Sun (left), followed by TIC 142015852, 269797536, 270676943, and 278825715. The top row shows trends in the fractional luminosity emitted in flares, ﹩{L}_{\mathrm{fl}}/{L}_{\mathrm{TESS}}\equiv {\xi }_{\mathrm{flare}}/{t}_{\exp }﹩ (Lurie et al. 2015). The second and third rows show the calculated flare rate and cumulative FFD, respectively. For the Sun, we used the RHESSI X-ray flare catalog and binned the flares per year from 2002 February to 2014 February. The Sun shows clear trends in ﹩{\xi }_{\mathrm{flare}}/{t}_{\exp }﹩ and flare rate over the 12 yr solar cycle. The cumulative FFD shows that (i) the overall number of flares decreases, which can be seen in the flare rate as well and (ii) the high-energy flare end of the distribution decreases. A quadratic polynomial is plotted to help guide the eye. It is important to note that these fits do not provide constraints on the length of potential stellar cycles in these stars due to the limited baseline obtained with TESS thus far. We present the measured flare rates and fractional luminosity emitted for each star in Table A2.
Paper: Evolution of Flare Activity in GKM Stars Younger Than 300 Myr over Five Years of TESS Observations
Authors: Adina D. Feinstein, Darryl Z. Seligman, Kevin France, Jonathan Gagné, Adam Kowalski
Figure caption: Comparison of flare rates from young planet host stars with respect to a comparable sample with respect to age [Myr] and T eff [K]. Circles represent the flare rate of the host star (name along the x-axis); vertical bars represent the lower 16th and upper 84th percentiles for the comparable sample. The majority of young planet host stars have comparable flare rates to the lower end of the comparison sample. A handful of hosts have more flares, including HIP 67522, AU Mic, DS Tuc A, and TOI 451. We find no correlation with the spectral type or age which may indicate why these host stars are relatively flare quiet. The measured flare rates are presented in Table 2. ✎
Paper: Evolution of Flare Activity in GKM Stars Younger Than 300 Myr over Five Years of TESS Observations
Authors: Adina D. Feinstein, Darryl Z. Seligman, Kevin France, Jonathan Gagné, Adam Kowalski
Figure caption: Calculated FUV (left) and NUV (right) GALEX flux for stars in our sample normalized by the stellar J-band flux. There is no obvious correlation between the fractional NUV/FUV flux and the measured flare rate or Rossby number. The top row shows GKM stars <50 Myr; the bottom row shows GKM stars ≥50 Myr. M stars are shown as circles, K stars as triangles, and G stars as squares. We note that f NUV traces the photosphere of G, K, and massive M stars, and therefore may not be the best comparison bandpass when looking for trends in magnetic activity. ✎
Paper: Evolution of Flare Activity in GKM Stars Younger Than 300 Myr over Five Years of TESS Observations
Authors: Adina D. Feinstein, Darryl Z. Seligman, Kevin France, Jonathan Gagné, Adam Kowalski
Figure caption: Flare frequency distributions, as a function of the flare amplitude, for stars with R 0 ≤ 0.12 (red) and stars with R 0 > 0.12 (black). We present the best-fit model and the best-fit values of the model slope and normalization factor in the legends. Our sample of R 0 ≤ 0.12 includes 13,132 flares from 800 stars; our sample of R 0 > 0.12 includes 5603 flares from 747 stars. We find the stars with smaller Rossby numbers have shallower slopes, consistent with more, high-energy flares and a more dominant rotational dynamo (Seligman et al. 2022). ✎
Paper: Evolution of Flare Activity in GKM Stars Younger Than 300 Myr over Five Years of TESS Observations
Authors: Adina D. Feinstein, Darryl Z. Seligman, Kevin France, Jonathan Gagné, Adam Kowalski
Figure caption: FFDs for subgroups of stars, clustered by age and effective temperature, T eff. Flares were sorted into 25 bins in log space from 1027 to 1035 erg. We fit the FFD from the turnover in the binned flares, likely a result of low-energy flares missed by the flare-detection algorithm. The bins used to fit the FFD are shown in black, while all bins are shown in gray. We ran an MCMC fit to these distributions with a simple power law; 100 random samples from these fits are overplotted in orange. We fit distributions with >3 bins. The best-fit slopes from these fits are presented in Figure 4.
Paper: JWST-TST DREAMS: Nonuniform Dayside Emission for WASP-17b from MIRI/LRS
Authors: Daniel Valentine, Hannah R. Wakeford, Ryan C. Challener, Natasha E. Batalha, Nikole K. Lewis, David Grant, Elijah Mullens, Lili Alderson, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Néstor Espinoza, Ana Glidden, Amélie Gressier, Jingcheng Huang, Zifan Lin, Douglas Long, Dana R. Louie, Mark Clampin, Marshall Perrin, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Azimuthally-weighted zonal flux slice through the atmosphere, in units of eclipse depth, highlighting the decreasing flux contributions to the map going away from the substellar point and the increased uncertainties. (Middle) Broadband 5–12μm MIRI/LRS eclipse map of WASP-17b, in units of brightness temperature (see Section 4.3 for conversion details). The model shown is the L2N2 model. The cross symbol (and dashed line in the upper panel) marks the substellar point; the star symbol (and dashed–dotted line in the upper panel) marks the hotspot. We omit the longitudes not scanned during the observation (∣ϕ∣ ≳ 110°) because we have no data to validate the model in these regions. (Bottom) Basis eigenmap components, scaled by their fitted weights. Values show the deviations that the maps incur from a spatially uniform map, in units of eclipse depth. The first eigenmap broadly corresponds to a day–night temperature contrast, and the second eigenmap to a hotspot offset.
Paper: JWST-TST DREAMS: Nonuniform Dayside Emission for WASP-17b from MIRI/LRS
Authors: Daniel Valentine, Hannah R. Wakeford, Ryan C. Challener, Natasha E. Batalha, Nikole K. Lewis, David Grant, Elijah Mullens, Lili Alderson, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Néstor Espinoza, Ana Glidden, Amélie Gressier, Jingcheng Huang, Zifan Lin, Douglas Long, Dana R. Louie, Mark Clampin, Marshall Perrin, Roeland P. van der Marel, C. Matt Mountain
Figure caption: (Left) Difference in BIC scores, ΔBIC, between the fit to the data of ThERESA eclipse mapping models with varying maximum degrees, l max, and numbers of basis components, N, vs. that of a uniform spatial emission model. A positive score indicates that the eclipse mapping model scores worse than the uniform model, while a negative score indicates that the eclipse mapping model scores better. (Right) Residuals of the uniform spatial emission model fit to the white light curve (blue data points, at native cadence in the background and 5 minute bins in the foreground). The gray lines are the range of uniform model fits, and the purple lines are the range of L2N2 eclipse mapping model fits post-processed from the posterior distribution, with the best fit shown by the lines outlined in black. Residual deviations to the data in ingress/egress, which the uniform model is unable to adequately fit, comprise the eclipse mapping signal, which the eclipse mapping model fits to in order to produce the map.
Paper: JWST-TST DREAMS: Nonuniform Dayside Emission for WASP-17b from MIRI/LRS
Authors: Daniel Valentine, Hannah R. Wakeford, Ryan C. Challener, Natasha E. Batalha, Nikole K. Lewis, David Grant, Elijah Mullens, Lili Alderson, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Néstor Espinoza, Ana Glidden, Amélie Gressier, Jingcheng Huang, Zifan Lin, Douglas Long, Dana R. Louie, Mark Clampin, Marshall Perrin, Roeland P. van der Marel, C. Matt Mountain
Figure caption: The 5–12 μm emission spectrum generated using ExoTiC-MIRI (0.25 μm bins in light blue circles, 0.50 μm bins in dark blue squares) and Eureka! (0.25 μm bins in pink circles, 0.50 μm bins in purple squares). The black hexagons are previous Spitzer measurements (Anderson et al. 2011). The dashed lines are blackbodies corresponding to temperatures ranging from 1200 to 2200 K, to give a scale of the temperatures probed by this data and to highlight deviations due to spectral features. All data products and models are available at 10.5281/zenodo.12571830.
Paper: JWST-TST DREAMS: Nonuniform Dayside Emission for WASP-17b from MIRI/LRS
Authors: Daniel Valentine, Hannah R. Wakeford, Ryan C. Challener, Natasha E. Batalha, Nikole K. Lewis, David Grant, Elijah Mullens, Lili Alderson, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Néstor Espinoza, Ana Glidden, Amélie Gressier, Jingcheng Huang, Zifan Lin, Douglas Long, Dana R. Louie, Mark Clampin, Marshall Perrin, Roeland P. van der Marel, C. Matt Mountain
Figure caption: PICACO forward-model fits to the 0.25 μm resolution brightness temperature spectra from both reduction pipelines (ExoTiC-MIRI in blue, Eureka! in pink). The shaded regions are the 1σ and 3σ credibility regions. The free parameters in the forward models fits are interior temperature (T int), heat redistribution efficiency (f rd), metallicity (log [M/H] ×  solar), and carbon-to-oxygen ratio (C/O (×solar = 0.458)). We highlight the wavelengths where we observe absorption due to water. We additionally show the median best-fit blackbody to both spectra in gray with shaded 1σ and 3σ credibility regions.
Paper: JWST-TST DREAMS: Nonuniform Dayside Emission for WASP-17b from MIRI/LRS
Authors: Daniel Valentine, Hannah R. Wakeford, Ryan C. Challener, Natasha E. Batalha, Nikole K. Lewis, David Grant, Elijah Mullens, Lili Alderson, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Néstor Espinoza, Ana Glidden, Amélie Gressier, Jingcheng Huang, Zifan Lin, Douglas Long, Dana R. Louie, Mark Clampin, Marshall Perrin, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Cloud condensate effective cross sections in the MIRI/LRS bandpass of plausible cloud species at the dayside temperatures of WASP-17b. The highlighted region indicates the wavelengths where we observe potential astrophysical features in the data, over which many of these species show prominent absorption features of a similar morphology to the features.
Paper: JWST-TST DREAMS: Nonuniform Dayside Emission for WASP-17b from MIRI/LRS
Authors: Daniel Valentine, Hannah R. Wakeford, Ryan C. Challener, Natasha E. Batalha, Nikole K. Lewis, David Grant, Elijah Mullens, Lili Alderson, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Néstor Espinoza, Ana Glidden, Amélie Gressier, Jingcheng Huang, Zifan Lin, Douglas Long, Dana R. Louie, Mark Clampin, Marshall Perrin, Roeland P. van der Marel, C. Matt Mountain
Figure caption:  ExoTiC-MIRI and Eureka! 0.50 μm binned spectroscopic light curves, excluding any trimmed or masked integrations (see text for details), with best-fit models overlaid. The histograms along the right-hand y-axis show the residuals between the data and model fits.
Paper: JWST-TST DREAMS: Nonuniform Dayside Emission for WASP-17b from MIRI/LRS
Authors: Daniel Valentine, Hannah R. Wakeford, Ryan C. Challener, Natasha E. Batalha, Nikole K. Lewis, David Grant, Elijah Mullens, Lili Alderson, Jayesh Goyal, Ryan J. MacDonald, Erin M. May, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Natalie H. Allen, Néstor Espinoza, Ana Glidden, Amélie Gressier, Jingcheng Huang, Zifan Lin, Douglas Long, Dana R. Louie, Mark Clampin, Marshall Perrin, Roeland P. van der Marel, C. Matt Mountain
Figure caption: Timings of central eclipse found in the BATMAN fits to the 0.25 μm bin spectroscopic light curves (ExoTiC-MIRI reduction). Overlaid is the white light curve value, showing the broadband average.
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: Top: influence radii for all sample galaxies plotted against MBH mass and color-coded by the galaxy stellar mass. Star symbols indicate galaxies with dynamical MBH mass measurements, while bullets and crosses indicate MBH mass estimates from scaling relations. The diagonal lines show the range of r infl possible given uncertainties in these mass estimates (either dynamical or from scaling relations). The galaxies plotted as crosses have distributions of r infl spanning ≳2 orders of magnitude, so they are plotted without a line to avoid clutter. NGC 4733 is plotted as an upper limit due to the use of a constant-density extrapolation. The solid and dashed green lines provide the two power-law fits to the data points. Bottom: identical to the top panel but displays the fraction of the influence radius that is observationally resolved, with the black dashed line indicating the threshold for influence radius resolution.
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: Top: color–mass diagram of our sample, which highlights the mass coverage and morphological diversity of the sample. The colors in this panel indicate the galaxy type, while closed symbols indicate NSC hosts. Nuclear g − i colors were used for the four galaxies indicated with star symbols due to a lack of existing galaxy color measurements. The shaded contours give the distributions of all galaxies in 50MGC. Bottom: distance distribution of our galaxies with colors indicating the parent sample. Similar to the top panel, nucleation is indicated by closed symbols.
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: Top: the MGE fit (magenta) to SB data for NGC 4365 (black points) compared to the prior Nuker-law fit (cyan) from Lauer et al. (2005) highlights the ability of an MGE to capture the excess nuclear luminosity resulting from the NSC. Bottom: maximum residual within a radius of 10 pc for Nuker-law fits plotted against galaxy stellar mass. The black dashed line represents the y = 0 line. This demonstrates the effect of NSCs on the Nuker-law fit quality at projected radii <10 pc, where nucleated galaxies show the largest fit residuals. The corresponding MGE fits for these galaxies produce residuals <0.09 mag arcsec−2 in all cases.
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: This figure shows the nucleation fraction of early-type galaxies in our sample (dotted–dashed line) compared with existing measurements from Hoyer et al. (2021) and Neumayer et al. (2020; solid and dotted, respectively). The distribution of early-type galaxies in our sample is shown by the histogram, and the black horizontal lines indicate the mass ranges used for the nucleated low-mass sample (Group 1) and the high-mass sample with mixed nucleation (Group 2). Over the mass range covered by Group 2, our sample follows a similar nucleation fraction to past observations.