adsabs/AstroCLIMB huggingface dataset:
Paper: Determining the Timescale over Which Stellar Feedback Drives Turbulence in the Interstellar Medium: A Study of Four Nearby Dwarf Irregular Galaxies
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Ray Garner, and Andrew E. Dolphin
Figure caption: UGC 9128 maps from observations with the SparsePak IFU on the WIYN 3.5 m telescope, with Hα line measurements from PAN. Left: Hα on a log scale in units of 10−17 erg s−1 cm−1. Center: Hα line centers map. Right: Hα velocity dispersion (σHα) map. Each filled circle corresponds to a fiber’s size and position on the sky. For reference to where the Sparsepak fibers fall on the galaxy compared with the H I and optical distributions, see Figure 12.
Paper: Determining the Timescale over Which Stellar Feedback Drives Turbulence in the Interstellar Medium: A Study of Four Nearby Dwarf Irregular Galaxies
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Ray Garner, and Andrew E. Dolphin
Figure caption: NGC 4068. Left: two-color image from HST F814W (red) and F606W (blue) observations with ACS. Center: H I dispersion map from VLA observations with isovelocity contours in 2.25 km s−1 step size. Right: σHα map from the SparsePak IFU on the WIYN 3.5 m telescope, with each filled circle corresponding to a fiber’s size and position on the sky. Overlaid on all three panels are the outlines of the regions used for the analysis.
Paper: Determining the Timescale over Which Stellar Feedback Drives Turbulence in the Interstellar Medium: A Study of Four Nearby Dwarf Irregular Galaxies
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Ray Garner, and Andrew E. Dolphin
Figure caption: NGC 4163. Left: two-color image from HST F814W (red) and F606W (blue) observations with ACS. Center: H I dispersion map from VLA observations with isovelocity contours in 2 km s−1 step size. Right: σHα map from the SparsePak IFU on the WIYN 3.5 m telescope, with each filled circle corresponding to a fiber’s size and position on the sky. Overlaid on all three panels are the outlines of the regions used for the analysis.
Paper: Determining the Timescale over Which Stellar Feedback Drives Turbulence in the Interstellar Medium: A Study of Four Nearby Dwarf Irregular Galaxies
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Ray Garner, and Andrew E. Dolphin
Figure caption: NGC 6789. Left: two-color image from HST F814W (red) and F555W (blue observations with WFPC2). Center: H I dispersion map from VLA observations with isovelocity contours in 2 km s−1 step size. Right: σHα map from the SparsePak IFU on the WIYN 3.5 m telescope, with each filled circle corresponding to a fiber’s size and position on the sky. Overlaid on all three panels are the outlines of the regions used for the analysis.
Paper: Determining the Timescale over Which Stellar Feedback Drives Turbulence in the Interstellar Medium: A Study of Four Nearby Dwarf Irregular Galaxies
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Ray Garner, and Andrew E. Dolphin
Figure caption: UGC 9128. Left: two-color image from HST F814W (red) and F606W (blue) observations with ACS. Center: H I dispersion map from VLA observations with isovelocity contours in 2 km s−1 step size. Right: σHα map from the SparsePak IFU on the WIYN 3.5 m telescope, with each filled circle corresponding to a fiber’s size and position on the sky. Overlaid on all three panels are the outlines of the regions used for the analysis.
Paper: Determining the Timescale over Which Stellar Feedback Drives Turbulence in the Interstellar Medium: A Study of Four Nearby Dwarf Irregular Galaxies
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Ray Garner, and Andrew E. Dolphin
Figure caption: Example CMDs and SFHs for 400 × 400 pc2 regions in UGC 9128 and NGC 4163 WFPC2 and ACS data. For both regions, the main sequence (blue), blue He-burning stars (HeB; green), and red HeB (red) sequence are traced. The SFHs have a ≤25 Myr time resolution in the two most recent time bins with Δlog(t) = 0.3 time steps and cover the 500 Myr baseline necessary for our science goals. The gray shading is the combined systematic and random uncertainties on the SFR. The green shading represents the random uncertainties. In regions where no green shading is shown these uncertainties are too small to be seen on the scale of the figure. The CMD derived SFHs are compared with regional measurements of the H I and Hα turbulence to determine the time over which stellar feedback impacts multiple phases of the ISM.
Paper: Determining the Timescale over Which Stellar Feedback Drives Turbulence in the Interstellar Medium: A Study of Four Nearby Dwarf Irregular Galaxies
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Ray Garner, and Andrew E. Dolphin
Figure caption: The superprofile of a selected region in NGC 4163. The black line is the bulk motion corrected H I flux from the region and the red line is the Gaussian fit for the data. The shaded gray region is the error on the data, while the shaded red region is the wings of the H I flux. The wings are the high-velocity, low-density gas that is poorly fit by a single Gaussian.
Paper: Determining the Timescale over Which Stellar Feedback Drives Turbulence in the Interstellar Medium: A Study of Four Nearby Dwarf Irregular Galaxies
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Ray Garner, and Andrew E. Dolphin
Figure caption: The Spearman ρ coefficient versus log time, which demonstrates how correlated the SFR of a given time bin is with the σHα. The light blue shaded region represents the 1σ bootstrapping error and under each point is the relevant P value. ForσHα, we do not find a strong correlation between the velocity dispersion and the SFR in any of the time bins.
Paper: Determining the Timescale over Which Stellar Feedback Drives Turbulence in the Interstellar Medium: A Study of Four Nearby Dwarf Irregular Galaxies
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Ray Garner, and Andrew E. Dolphin
Figure caption: The Spearman ρ coefficient and corresponding P value plotted against log time showing how correlated the SFR of a given time bin is with the H I turbulence measures. The light blue shaded region represents the 1σ bootstrapping error. Panels (a) and (b) are the correlation of the SFH with the velocity dispersion and energy surface density of the Gaussian superprofiles, panels (c) and (d) are the correlation of the SFH with the velocity dispersion and energy surface density of the wings of the superprofiles, and panels (e) and (f) are the correlation of the SFH with the velocity dispersion and energy surface density measured from the second moment maps. For all H I turbulence measures there is at least a modest correlation with the SFR at about 100–200 Myr (8–8.3 log(age)), which is highlighted by the gray shaded region.
Paper: Determining the Timescale over Which Stellar Feedback Drives Turbulence in the Interstellar Medium: A Study of Four Nearby Dwarf Irregular Galaxies
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Ray Garner, and Andrew E. Dolphin
Figure caption: The Hα velocity dispersion vs. the SFR 10–25 Myr ago. The error bars represent the 68% confidence interval of the measurements.
Paper: Determining the Timescale over Which Stellar Feedback Drives Turbulence in the Interstellar Medium: A Study of Four Nearby Dwarf Irregular Galaxies
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Ray Garner, and Andrew E. Dolphin
Figure caption: The H I energy surface density (ΣH I) of the Gaussian superprofile fit vs. the SFR 100–200 Myr ago. The error bars on the SFRs represent the 68% confidence interval of the measurements. A slight trend of higher ΣH I with higher SFR can be seen.
Paper: Determining the Timescale over Which Stellar Feedback Drives Turbulence in the Interstellar Medium: A Study of Four Nearby Dwarf Irregular Galaxies
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Ray Garner, and Andrew E. Dolphin
Figure caption: The Spearman ρ coefficient and corresponding P value plotted against log time showing how correlated the SFR of a given time bin is with the velocity dispersion and energy surface density of the Gaussian superprofiles. The light blue shaded region represents the 1σ bootstrapping error. Panels (a) and (b) are the correlations for regions within NGC 4068 and panels (c) and (d) are the correlation for the regions within NGC 4163, NGC 6789, and UGC 9128. For all H I turbulence measures, there is a peak in the correlation at about 100–200 Myr.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The R.A. and decl. of stars in the APOGEE-KOI sample. The grayscale points show the density of stars in the Kepler stellar properties table at a particular sky coordinate, while the points show the DR24 KOIs observed (blue), and not observed (red) by the APOGEE-KOI program in a temperature range with reliable abundance ratio measurements (see Figure 2). The name of each field is listed at the top left of the field.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The trends between abundance ratio and Teff for dwarfs in the solar neighborhood observed by APOGEE, for each element considered in this study. The color of the points in each figure corresponds to the metallicity of the star. The white points show the median abundance ratio in Teff bins of 100 K, the dashed vertical lines show our adopted Teff range for this study (4800 K < Teff < 6200 K), and the horizontal lines denote the abundance range of ±0.05 dex of the median abundance within the adopted temperature range. The median uncertainty for each abundance is shown as an error bar in the bottom of each panel.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The relative errors of the stellar radius (top) and mass (bottom) in the APOGEE-KOI sample derived with isofit. The mean and median stellar radius uncertainties are 2.7% and 2.3%, respectively. The mean and median uncertainties on the stellar mass are 4.5% and 4.7%, respectively.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: Comparison of the fundamental stellar properties derived in this work vs. the stellar properties derived by Berger et al. (2020b) for the same stars (B20). The dashed blue lines in each case represent the one-to-one agreement between the two samples. Left: comparisons of the stellar radii derived in this work. Overall there is excellent agreement, with a scatter in the ratio of radii of 3.4%, and an average offset of <1%. Right: comparisons of the stellar masses derived in this work and in Berger et al. (2020b). They agree overall within the scatter, but have an offset of ≈6%, in that the APOGEE sample has a lower mass on average.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: Comparison of the fundamental stellar properties derived in this work vs. the stellar properties derived by Martinez et al. (2019) for the same stars (M19). In each panel, the dashed black line denotes agreement. Left: comparison of the stellar radii. We find relative agreement, with an average offset and scatter of 1.1% ± 1.3% in the ratio of the radii. Right: comparison of the effective temperatures derived by ASPCAP and the effective temperatures from M19. There is a mean offset and scatter of 108 ± 171 K between the two samples. The systematically lower Teff in ASPCAP is the likely reason for the systematic offset in stellar radii.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The three samples considered in this study. The effective temperature and radii of the stars in each sample are shown along the top row, and the metallicity distribution function for each sample is shown along the bottom row. The metallicity distributions are scaled to arbitrary units. Left: Kepler field stars with parameters derived in Berger et al. (2020b). The stars cut from ﹩{ \mathcal S }﹩ are shown in gray, and those included in ﹩{ \mathcal S }﹩ are shown in green. The metallicities for the stars in ﹩{ \mathcal S }﹩ are heterogeneous, or assumed to be solar, and thus are not as reliable for this study. Center: the stars in the Control sample (gray), and the subset of these stars included in ﹩{ \mathcal C }﹩ (tan). Right: all of the stars in the APOGEE-KOI program (gray) and the stars included in ﹩{ \mathcal P }﹩ (purple).
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The planets in ﹩{ \mathcal P }﹩, plotted with all of the DR24 planet candidates that have a host in ﹩{ \mathcal S }﹩. Top: the planet radius and orbital period of all planets in ﹩{ \mathcal P }﹩. The gray points show all of the planets from the DR24 KOI catalog with a host star in ﹩{ \mathcal S }﹩ that are not included in ﹩{ \mathcal P }﹩. Bottom: the radius distribution of the planets in ﹩{ \mathcal P }﹩. The gray histogram shows the radii of all of the planets in DR24 with a host in ﹩{ \mathcal S }﹩, while those in ﹩{ \mathcal P }﹩ are displayed in blue. The primary reasons for exclusion in ﹩{ \mathcal P }﹩ are RV variability, a poor solution from ASPCAP, or pre-DR24 target selection.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: Chemical abundances for the planet host (purple) and control (tan) samples. The chemical abundance displayed is shown in the upper left corner of each panel. The median error (±1σ) for each abundance is shown by the black error bar in the top right corner of each panel, and the dashed lines indicate the median abundances for the planet host sample (purple) and the control sample (tan).
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: Left: the average metallicity for host stars of planets in given orbital period bins. The circular points show the average metallicity, while the horizontal lines show the 68% confidence interval on the metallicity distribution. We recover the same planet period–stellar metallicity anticorrelation reported in previous literature (e.g., Mulders et al. 2016; Wilson et al. 2018). Right: the average host star metallicity as a function of planet radius, binned for planets of given size classes, sub-Earths, super-Earths, sub-Neptunes, sub-Saturns, and Jupiters. The sub-Earth, super-Earth, and sub-Neptune classes are split into two radius bins each. We find similar relations as in the literature: that there is a notable increase in the average host metallicity for planets with larger radii. In particular, there are very few planets with Rp > 4 R⊕ and 〈[Fe/H]〉 < −0.2.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: Top: trends with planet radius for abundance ratios to iron. Just as in Figure 9, the points represent the means of each bin, with error bars representing the error on the mean [X/Fe] from bootstrapping. The horizontal lines show the 16th and 84th percentiles of the distribution in each bin to display the variance. We detect significant positive correlations for [Mn/Fe] and [S/Fe] vs. Rp. Bottom: the distribution of host star abundance ratios to iron as a function of planet period. We detect a statistically significant positive correlation between [S/Fe] and P. Such a correlation cannot be explained with well-known trends in [Fe/H].
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The mean completeness model, ﹩\eta ={p}_{\mathrm{tra}}\times \ {p}_{\det }\times \ {p}_{\mathrm{apo}}\times \ (1-{p}_{\mathrm{fail}})﹩, for each APOGEE field in ﹩{ \mathcal S }﹩, and the combined model from all fields. The blue filled contours give the survey efficiency in the P–Rp plane, representing the probability that a given planet orbiting a star in ﹩{ \mathcal S }﹩ is in ﹩{ \mathcal P }﹩. The lightest shade shows where η > 0.1, while the darkest shade represents survey efficiencies of η < 10−4. The gray dashed lines are the corresponding contours for the Kepler DR24 pipeline efficiency and are shown for comparison to highlight the effects of the APOGEE-KOI program selection function. The panels representing the APOGEE fields are organized from least to most divergent from the DR24 pipeline efficiency with the combined survey efficiency on the far right.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The planet occurrence rate in the P–Rp plane. We divide the plane into bins of size ﹩{\rm{\Delta }}\mathrm{log}P\times \ {\rm{\Delta }}\mathrm{log}{R}_{p}=0.25\times \ 0.15﹩ dex. The color shows the measured occurrence rate in the bin of interest on a logarithmic scale. The gray bins do not have any detected planets. The numbers in each cell shows the occurrence rate in units of number of planets per 100 stars. The uncertainty shown is taken to be half of the 68% confidence interval range on the occurrence rate. Bins without detected planets have the upper limit displayed. Bins with no detected planets and no upper limit listed are areas of low completeness where an upper limit is not constraining.
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The planet occurrence rate in the P–Rp plane. For each row of figures, the left panel shows the planets in ﹩{ \mathcal P }﹩ as white points, and the filled contours show the derived occurrence rate, with darker shades representing higher occurrence rates. The top row displays the occurrence rates on a linear scale, and the bottom row displays occurrence rates on a log scale, where darker shades of red indicate a higher occurrence and lighter shades of yellow indicate a lower occurrence. A box in the upper left corner of each panel shows the FWHM of the Gaussian kernel used to calculate the contours for this figure. The gray region denotes areas of low survey completeness. The dashed black line shows the location and slope of the radius gap measured by Martinez et al. (2019).
Paper: The Influence of 10 Unique Chemical Elements in Shaping the Distribution of Kepler Planets
Authors: Robert F. Wilson, Caleb I. Cañas, Steven R. Majewski, Katia Cunha, Verne V. Smith, Chad F. Bender, Suvrath Mahadevan, Scott W. Fleming, Johanna Teske, Luan Ghezzi, Henrik Jönsson, Rachael L. Beaton, Sten Hasselquist, Keivan Stassun, Christian Nitschelm, D. A. García-Hernández, Christian R. Hayes, and Jamie Tayar
Figure caption: The number of planets per star (multiplied by 100) for a given orbital period bin and planet size class. The colors denote the planet size class. The circular points denote the occurrence rates while the triangular points denote upper limits. We fit the sub-Neptune and super-Earth occurrence rates with a function of the form, ﹩{f}_{P}\propto {P}^{\alpha }(1-{e}^{-{(P/P0)}^{\gamma }})﹩. The lines show the adopted best-fit solution, and the shaded regions denote the 1σ confidence interval of credible models. The occurrence rates shown in this figure are displayed over substantially larger bin sizes than those used to fit the model but are displayed here to guide the eye.