adsabs/AstroCLIMB huggingface dataset:
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Asteroseismic constraints on δ ν * and i * for KIC 5773345 (Group Aa).
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Asteroseismic constraints on δ ν * and i * for Kepler-128 (Group Ba).
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Asteroseismic constraints on δ ν * and i * for Kepler-409 (Group Ab).
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Asteroseismic constraints on δ ν * and i * for Kepler-93 (Group Ba).
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Asteroseismic constraints on δ ν * and i * for Kepler-25 (Group Ba).
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The LS periodograms of Kepler-25 (Group Ba) for different quarters.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The LS periodograms of Kepler-128 (Group Ba) for different quarters.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The LS periodograms of Kepler-409 (Group Ab) for different quarters.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The LS periodograms of Kepler-93 (Group Ba) for different quarters.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The LS periodograms of KOI-268 (Group Ab) for different quarters.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Asteroseismic constraints on δ ν * and i * for KIC 7970740 (Group Ab).
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Asteroseismic constraints on δ ν * and i * for KIC 9965715 (Group Ba).
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Asteroseismic constraints on δ ν * and i * for KIC 6225718 (Group Ba).
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Asteroseismic constraints on δ ν * and i * for KOI-268 (Group Ab).
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The LS periodograms of KIC 6225718 (Group Ba) for different quarters.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The LS periodograms of KIC 9965715 (Group Ba) for different quarters.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The LS periodograms of KIC 7970740 (Group Ab) for different quarters.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The LS periodograms of Kepler-2 for different quarters.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Asteroseismic constraints on δ ν * and i * for KOI-288.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Asteroseismic constraints on δ ν * and i * for Kepler-410.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Asteroseismic constraints on δ ν * and i * for Kepler-2.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The LS periodograms of Kepler-410 for different quarters.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The LS periodograms of KOI-288 for different quarters.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Rotation periods for seven KOI stars classified in Group Aa. We plot the values of P LS,q  for different quarters in gray crosses, with the orange vertical lines indicating their median value 〈P LS,q 〉 for each target. For comparison, we show the other three photometric rotation periods, P LS, P ACF, and P WA, in red, green, and blue dots with error bars (corresponding to their half-widths at half-maximum, HWHMs), respectively. Black dots indicate the asteroseismic results P astero with quoted errors representing the 16th and 84th percentiles. For reference, we plot the orbital periods of transiting planets in each system as cyan dots.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The light curve of Kepler-100 for Q9. The left and right panels show the light curves with no padding and Gaussian noise-padding. This system hosts three planet candidates of orbital period P orb = 6.9, 12.8, and 35.3 days. We use vertical bars to indicate the padded epochs of transits and occultations corresponding to P orb = 12.9 days, similar to the detected rotation period ∼12.92 days. We also mark the padded locations of transits and occultations for the remaining two planet candidates using triangles of different colors.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Same as Figure 7 but for 16 non-KOI stars classified in Group Ba.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: 〈P LS,q 〉 vs. ΔLS (left) and P astero vs. ΔP astero/P astero (right). The green, blue, magenta, and gray symbols correspond to Groups Aa, Ba, Ab, and Bb, respectively.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Same as Figure 7 but for six KOI stars classified in Group Ab.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Same as Figure 7 but for five non-KOI stars classified in Group Ab.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Same as Figure 7 but for three KOI stars classified in Group Ba.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Same as Figure 7 but for seven non-KOI stars classified in Group Aa.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Same as Figure 7 but for 10 KOI stars classified in Group Bb.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Wavelet power spectrum (WPS; lower panel) and global wavelet power spectrum (GWPS; upper panel) of Kepler-1655 (KIC 4141376, KOI-280). The brighter color in the WPS indicates a larger power. The cross-hatched region near the bottom edge of the WPS is the cone of influence within which power is less reliable. The dotted line in the right panel marks the maxima of the GWPS, which corresponds to the measured period. The removed quarters are indicated in magenta. The shaded region in the upper panel covers the HWHM in both sides of the peak.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: An example of the LS periodogram for Kepler-1655 (KIC 4141376, KOI-280). Left: LS periodogram computed from the entire light curve. Right: periodogram computed from Q9. The thick black line indicates the boxcar-smoothed result (over 0.1 μHz) of the original LS periodogram (thin gray curves). The vertical blue dashed line indicates the location of P LS, and the associated blue shaded area corresponds to the HWHM on both sides.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Posterior probability density (PPD) on the stellar inclination i * and rotation frequency δ ν * for Kepler-1655 (KIC 4141376, KOI-280) marginalized over all other parameters. The top-left, bottom-left, and bottom-right panels plot one-dimensional marginalized densities of δ ν *, ﹩\delta {\nu }_{* }\sin {i}_{* }﹩, and i *, respectively. The solid and dashed lines in those panels indicate the median and 16%–84% intervals for those parameters derived from asteroseismology alone.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Same as Figure 23 but for non-KOI stars. Spectroscopic ﹩v\sin i﹩ values for deriving ﹩\sin {i}_{* ,{spec}}﹩ are adopted from Lund et al. (2017), Molenda-Żakowicz et al. (2013), Bruntt et al. (2012), and Brewer et al. (2016). For some targets, there are more than one available ﹩v\sin i﹩ value. In the second panel, we adopt Bruntt et al. (2012) if there is both ﹩v\sin i﹩ from Bruntt et al. (2012) and from other literature. In the third panel, we use ﹩v\sin i﹩ from Molenda-Żakowicz et al. (2013) if multiple values are available.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Comparison of the rotation periods for 44 stars overlapped in the previous literature and our sample. The left panel shows the comparison based on the same photometric method, while the right panel plots their rotation periods against our P LS. Different colors indicate four groups that we introduced in the previous section, while different symbols indicate different papers: P LS from Nielsen et al. (2013) and Karoff et al. (2013), P ACF from McQuillan et al. (2013) and McQuillan et al. (2014), and P WA from Ceillier et al. (2016) and García et al. (2014).
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Examples of ACF analysis for KIC 4141376 (KOI-280, Kepler-1655). The top, middle, and bottom panels show the ACF, smoothed ACF, and LS periodogram of the smoothed ACF. In the middle panel, P 0 is the period associated with the first maximum and P max is that associated with the highest maximum.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The LS periodograms of Kepler-100 (Group Aa) for different quarters.
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: Asteroseismic constraints on δ ν * and i * for Kepler-100 (Group Aa).
Paper: Meta-analysis of Photometric and Asteroseismic Measurements of Stellar Rotation Periods: The Lomb–Scargle Periodogram, Autocorrelation Function, and Wavelet and Rotational Splitting Analysis for 92 Kepler Asteroseismic Targets
Authors: Yuting Lu, 鈺婷 卢, Othman Benomar, Shoya Kamiaka, 翔也 上赤, Yasushi Suto
Figure caption: The LS periodograms of KIC 5773345 (Group Aa) for different quarters.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: Left: a comparison between the stellar masses of the galaxies in this work (x-axis) and their catalog NSA stellar masses. The dashed line and shaded regions show the median, and range between the 16th and 84th percentiles of the deviation ﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })-{\mathrm{log}}_{10}({M}_{\star ,{NSA}}/{M}_{\odot })﹩. Middle: the same, but for SED fitting-derived SFRs and FUV-only SFRs as computed from the catalog GALEX measurements using the SFR(FUV) prescription of Kennicutt (1998). Right: a comparison between SFRs derived from the Hα fluxes measured from SDSS 3" fiber fibers (x-axis) and the total SFR within the central 3" of our SED fits (y-axis, red). The dashed black line denotes a 1:1 relation. As in the left panel, the dashed purple line and shaded purple regions show the median, and range between the 16th and 84th percentiles. SFRs derived from Hα measure star formation over a shorter timescale (∼10 Myr) than our SED fits (100 Myr), and some physical scatter is expected as a result; we show the standard deviation (in logarithmic space) of the difference between Hα-derived and FUV-derived SFRs for a set of Local Volume dwarfs from Karachentsev et al. (2021) as a visual aid to the reader in gauging the scatter.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: A schematic layout of the fitting technique used in this work. At left, we represent the high-resolution optical data and low-resolution UV data (panels (a) and (c), respectively). Panels (b) and (d) represent the global fit between the optical and UV data; in this step, the apertures are matched between the optical and UV data. Panel (e) shows the spatial division of the optical data into regions in which regional SEDs are measured. Panel (f) shows the clustering of these spatial regions into three representative clusters; these cluster SEDs will be fit jointly with the global UV photometry (panel (d)).
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: A comparison between H I surface density estimates and SFR surface density measurements averaged over 500 pc, 1 kpc, and global scales. In all panels, we only show NSA galaxies that are within the stellar mass range of the UDG sample (i.e., M ⋆ < 3 × 108 M ⊙). For visual clarify, we show a random subset of (at most) 70 points for each sample with individual error bars and colored by sample source; we show the full sample as the underlying gray scatter. Here, we demonstrate that the low SFE(H I) that characterizes the globally averaged properties of UDGs persists down to sub-kiloparsec scales.
Paper: Ultra-diffuse Galaxies as Extreme Star-forming Environments. I. Mapping Star Formation in H I-rich UDGs
Authors: Erin Kado-Fong, Jenny E. Greene, Song Huang, Andy Goulding
Figure caption: A comparison between various measures of galaxy mass and galaxy size; the top row shows size as a function of H I mass, while the bottom row shows size as a function of stellar mass. The left column shows size as measured by the HSC-g band half-light radius, while the right column shows size as measured by the half-stellar mass radius. In each panel, the purple dashed line shows the least squares power-law fit to the NSA galaxies. The red dashed line shows the least squares fit to the UDG sample when the index of the power law is held fixed to that of the NSA dwarf fit. The shaded regions span the 16th–84th percentiles as estimated from bootstrap resampling. As one expects, the UDG sample is large in size for their stellar masses. However, their half-stellar mass radii are unremarkable for their H I masses.