adsabs/AstroCLIMB huggingface dataset:
Paper: Dynamical Evolution of Four Old Galactic Open Clusters Traced by Their Constituent Stars with Gaia DR3
Authors: Shanmugha Balan, Khushboo K. Rao, Kaushar Vaidya, Manan Agarwal, Souradeep Bhattacharya
Figure caption: Differential Reddening correction for Berkeley 39, NGC 6819 and NGC 7789 (from top to bottom) with the reddening map, observed CMD and the reddening corrected CMD for each cluster (from left to right).
Paper: Dynamical Evolution of Four Old Galactic Open Clusters Traced by Their Constituent Stars with Gaia DR3
Authors: Shanmugha Balan, Khushboo K. Rao, Kaushar Vaidya, Manan Agarwal, Souradeep Bhattacharya
Figure caption: The reddening map (left panel), observed CMD (middle panel), and differential reddening corrected CMD (right panel) for Collinder 261 OC.
Paper: Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star
Authors: Xu Ding, KaiFan Ji, ZhiMing Song, NianPing Liu, JianPing Xiong, Qiyuan Cheng, ChuanJun Wang, JinLiang Wang, DeQing Wang, ShouSheng He
Figure caption: Each sector's observed light curves revealed notable flare events.
Paper: All Puffed Up: Exploring Ultra-diffuse Galaxy Origins Through Galaxy Interactions
Authors: Catherine Fielder, Michael G. Jones, David J. Sand, Paul Bennet, Denija Crnojević, Ananthan Karunakaran, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: VLA H I contours overlaid on CFHTLS imaging for KUG 0203-Dw1 (left column) and KDG 013 (right column). The top row is centered on the UDG, while the bottom row shows a wider view of the respective galaxy group. Upper left: a high-contrast CFHT g-band image of KUG 0203-Dw1 with integrated VLA C+D array H I emission contours overlaid. The minimum contour is 1.3 × 1019 cm−2 (3σ) in column density (over 10 km s −1). Each contour is double the previous. The synthesized beam is shown as a semitransparent ellipse in the lower-left corner, which corresponds to a beam size of 27.0 × 22.0 arcsec2. Lower left: same as upper left, but showing the full system with KUG 0203-100. A small overdensity to the north of KUG 0203-100 (black contout) is a real detection and not noise. Upper right: similar to the left panels, for KDG 013. The H I emission is derived from the VLA D array only. Here the minimum contour is 8.4 × 1018 cm−2 (3σ) in column density (over 20 km s −1). The synthesized beam size corresponds to 73.5 × 59.6 arcsec2. Lower right: same as upper right, but showing a majority of the NGC 830 group.
Paper: All Puffed Up: Exploring Ultra-diffuse Galaxy Origins Through Galaxy Interactions
Authors: Catherine Fielder, Michael G. Jones, David J. Sand, Paul Bennet, Denija Crnojević, Ananthan Karunakaran, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: HST ACS/WFC F555W/F814W composite color images of KUG 0203-Dw1 (left column) and KDG 013 (right column). The upper row is centered on the UDG, while the lower row shows the full HST frame. Upper left: HST ACS/WFC F555W/F814W composite color image of KUG 0203-Dw1. The inner, white dotted circular aperture marks r 1/2 (11.″8), and the dashed circular aperture marks 2 × r 1/2 (23.″6), which we select as the outer edge of the UDG. Small cyan apertures enclose all globular cluster candidates (GCCs) within the image, with a total of five within the aperture of the UDG. Lower left: the full HST image of KUG 0203-Dw1, which includes its host galaxy KUG 0203-100. Upper right: same as the left panel, but for KDG 013. Here the apertures correspond to 12.″5 and 25,” with a total of four GCCs. GCCs of either UDG are selected from within the 2 × r 1/2 UDG boundary. Lower right: the full HST image of KDG 013. The edge of Mrk 1019 is visible to the northeast of KDG 013.
Paper: All Puffed Up: Exploring Ultra-diffuse Galaxy Origins Through Galaxy Interactions
Authors: Catherine Fielder, Michael G. Jones, David J. Sand, Paul Bennet, Denija Crnojević, Ananthan Karunakaran, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: Left: size–luminosity relation for the sample of five UDGs with tidal features compared to Coma cluster UDGs (P. G. van Dokkum et al. 2015; blue triquetra), group UDGs (J. J. Somalwar et al. 2020; pink pentagons), and H I-rich UDGs (L. Leisman et al. 2017; purple points). All of our UDGs are consistent with the Coma sample, aside from UGC 9050-Dw1, which is unusually large for its brightness. The dashed vertical line marks the defined UDG lower limit on size used in this work. Right: central surface brightness as a function of half-light radius for the same sample. Here UGC 9050-Dw1 is more consistent with the H I sample while NGC 5631-Dw1 has a very faint central surface brightness. We note that the comparative samples are surface brightness limited so there may be other sources currently undetected at lower central surface brightness. The dashed horizontal line is analogous to that in the left panel. The dashed vertical line indicates the maximum central surface brightness for a UDG as defined in this work (please note that the H I UDGs adhere to a distinct definition, hence why some are brighter).
Paper: All Puffed Up: Exploring Ultra-diffuse Galaxy Origins Through Galaxy Interactions
Authors: Catherine Fielder, Michael G. Jones, David J. Sand, Paul Bennet, Denija Crnojević, Ananthan Karunakaran, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: Counts of GCs (N GC) plotted against the V-band absolute magnitude (M  V ). To provide context, we compare our findings to several data sets found in the literature, including a general galaxy data set (gray ×’s from W. E. Harris et al. 2013), cluster UDGs (various blue points), group UDGs (various pink points), and other distinct GC-rich UDGs from various environments. The solid, dashed, and dotted black lines represent specific frequency (S  N ) values of 1, 10, and 100, respectively. Our full sample of five UDGs with tidal features is shown by orange points: KUG 0203-Dw1 (star), KDG 013 (half-filled star), UGC 9050-Dw1 (diamond), NGC 2708-Dw1 (square), and NGC 5631-Dw1 (half-filled square). KUG 0203-Dw1 and KDG 013 are slightly more GC-rich than the two UV-bereft UDGs in our sample (NGC 2708-Dw1 and NGC 5631-Dw1; J21).
Paper: All Puffed Up: Exploring Ultra-diffuse Galaxy Origins Through Galaxy Interactions
Authors: Catherine Fielder, Michael G. Jones, David J. Sand, Paul Bennet, Denija Crnojević, Ananthan Karunakaran, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: CFHTLS r-band imaging for KUG 0203-Dw1 (left) and KDG 013 (right), masked and scaled to emphasize low-surface-brightness features. There is a faint stellar stream between KUG 0203-Dw1 and KUG 0203-100. Additionally, KUG 0203-Dw1 has a tidal plume that extends toward the southwest of its main body, and extended stellar material northwest and south along the direction of the host. KDG 013 contains similar features compared to KUG 0203-Dw1, but with a smaller tidal plume. The extended stellar material associated with KDG 013 falls along the direction of the majority of mass in the group (NGC 830, NGC 829, and Mrk 1019).
Paper: All Puffed Up: Exploring Ultra-diffuse Galaxy Origins Through Galaxy Interactions
Authors: Catherine Fielder, Michael G. Jones, David J. Sand, Paul Bennet, Denija Crnojević, Ananthan Karunakaran, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: (V − I) color distribution of the five UDGs with associated tidal features. The sample is split for readability. The left histogram shows the UDGs with GCs exhibiting a narrow spread in color, and the right histogram shows the other three UDGs. We also include samples of dwarf galaxies for comparison (from M. E. Sharina et al. 2005 and I. Y. Georgiev et al. 2009). Each histogram is normalized so that it has an integrated area of 1 such that the histograms can be compared on similar axes (hence noninteger GC abundances). The vertical dashed lines correspond to the color cut employed for GC selection: 0.5 < (V − I) < 1.5. KUG 0203-Dw1 exhibits a blue GC population, similar to UGC 9050-Dw1. The GC candidates of NGC 2708-Dw1, NGC 5631-Dw, and KDG 013 generally span the full color space.
Paper: All Puffed Up: Exploring Ultra-diffuse Galaxy Origins Through Galaxy Interactions
Authors: Catherine Fielder, Michael G. Jones, David J. Sand, Paul Bennet, Denija Crnojević, Ananthan Karunakaran, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: Left: composite GALEX FUV and NUV image of KUG 0203-Dw1. Three background galaxies fall very close to the UDG, so we apply a mask setting values above the threshold of 0.008 to 0. The positions of these objects are marked by gray circles. Right: GALEX NUV image of KDG 013. Circular apertures are the same as those shown in Figure 3. No threshold was applied to this image as it was not necessary. Both images have the same scaling.
Paper: All Puffed Up: Exploring Ultra-diffuse Galaxy Origins Through Galaxy Interactions
Authors: Catherine Fielder, Michael G. Jones, David J. Sand, Paul Bennet, Denija Crnojević, Ananthan Karunakaran, Burçin Mutlu-Pakdil, Kristine Spekkens
Figure caption: Left: color–magnitude diagrams (CMDs) of sources within the KUG 0203-Dw1 HST/ACS frame, presented in two panels: sources within the GC search radius of the UDG (r < 2 × r 1/2) at left and sources outside of the search radius at right. Note that in the right panel we have excluded GC candidates that fall inside of the host galaxy KUG 0203-100 as they are unlikely contaminants. DOLPHOT-identified sources classified as “stars” that meet the criteria for S/N, sharpness, roundness, and uncertainty described in Section 5.1 are represented by blue circles. Orange squares depict sources that successfully pass the subsequent concentration cut used to select GC candidates. The CMD space includes a gray outlined box representing the color and magnitude cuts for GCCs. A horizontal black dashed line indicates the 90% completeness limit. Right: same as left, but for KDG 013.
Paper: Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star
Authors: Xu Ding, KaiFan Ji, ZhiMing Song, NianPing Liu, JianPing Xiong, Qiyuan Cheng, ChuanJun Wang, JinLiang Wang, DeQing Wang, ShouSheng He
Figure caption: SED fitting using SPEEDYFIT. The upper panels display the observations and spectral energy distributions of the visible star. The residuals of the fit are presented in the lower panel.
Paper: Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star
Authors: Xu Ding, KaiFan Ji, ZhiMing Song, NianPing Liu, JianPing Xiong, Qiyuan Cheng, ChuanJun Wang, JinLiang Wang, DeQing Wang, ShouSheng He
Figure caption: Left: the radial velocities of M-type dwarfs were only obtained from the blue arm. Right: the red and blue points represent the radial velocity curves calculated using Hα. The green points mirror those in the left panel.
Paper: Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star
Authors: Xu Ding, KaiFan Ji, ZhiMing Song, NianPing Liu, JianPing Xiong, Qiyuan Cheng, ChuanJun Wang, JinLiang Wang, DeQing Wang, ShouSheng He
Figure caption: The Hα spectra of TIC 157365951 are shown alongside a dashed line marking the position of the Hα line.
Paper: Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star
Authors: Xu Ding, KaiFan Ji, ZhiMing Song, NianPing Liu, JianPing Xiong, Qiyuan Cheng, ChuanJun Wang, JinLiang Wang, DeQing Wang, ShouSheng He
Figure caption: The distributions of parameters from SED fitting.
Paper: Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star
Authors: Xu Ding, KaiFan Ji, ZhiMing Song, NianPing Liu, JianPing Xiong, Qiyuan Cheng, ChuanJun Wang, JinLiang Wang, DeQing Wang, ShouSheng He
Figure caption: Parameter distributions derived from the fitting results of light curve (lc) and radial velocity (RV) curve using Phoebe with a detached binary system.
Paper: Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star
Authors: Xu Ding, KaiFan Ji, ZhiMing Song, NianPing Liu, JianPing Xiong, Qiyuan Cheng, ChuanJun Wang, JinLiang Wang, DeQing Wang, ShouSheng He
Figure caption: The folded light curve with phase flux is shown.
Paper: Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star
Authors: Xu Ding, KaiFan Ji, ZhiMing Song, NianPing Liu, JianPing Xiong, Qiyuan Cheng, ChuanJun Wang, JinLiang Wang, DeQing Wang, ShouSheng He
Figure caption: The fitting results of light curves and RV curve using Phoebe with a detached binary system.
Paper: Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star
Authors: Xu Ding, KaiFan Ji, ZhiMing Song, NianPing Liu, JianPing Xiong, Qiyuan Cheng, ChuanJun Wang, JinLiang Wang, DeQing Wang, ShouSheng He
Figure caption: Parameter distributions derived from the fitting results of light curve and RV curve using Phoebe with a semidetached binary system.
Paper: Fundamental Parameters of a Binary System Consisting of a Red Dwarf and a Compact Star
Authors: Xu Ding, KaiFan Ji, ZhiMing Song, NianPing Liu, JianPing Xiong, Qiyuan Cheng, ChuanJun Wang, JinLiang Wang, DeQing Wang, ShouSheng He
Figure caption: The fitting results of light curves and RV curve using Phoebe with a semidetached binary system.
Paper: HIP 65426 is a High-frequency Delta Scuti Pulsator in Plausible Spin–Orbit Alignment with its Directly Imaged Exoplanet
Authors: Aldo G. Sepulveda, Daniel Huber, Timothy R. Bedding, Daniel R. Hey, Simon J. Murphy, Zhoujian Zhang, Michael C. Liu
Figure caption: Orbital inclination compared to stellar inclination for a sample of six directly imaged exoplanet systems (comprising 11 total planets) assuming prograde orbits with respect to the host star. The solid black line denotes the 1:1 relation, and the light cyan region bordered by dashed black lines encapsulates an inclination difference ±10° of the black line. References for the inclination angles are given in Section 4.3.
Paper: HIP 65426 is a High-frequency Delta Scuti Pulsator in Plausible Spin–Orbit Alignment with its Directly Imaged Exoplanet
Authors: Aldo G. Sepulveda, Daniel Huber, Timothy R. Bedding, Daniel R. Hey, Simon J. Murphy, Zhoujian Zhang, Michael C. Liu
Figure caption: (a) Gaia color–magnitude diagram for a sample of Kepler stars generated following Sepulveda et al. (2022). HIP 65426 is overplotted as a large cyan star. The orange diamonds are the δ Scuti stars, blue squares are the γ Dor stars, and the small, gray, semitransparent dots are the general population of Kepler stars. (b): échelle diagram for HIP 65426 generated using our suggested large-frequency separation of Δν = 7.23 cycles day−1. This plot uses an amplitude spectrum calculated from the concatenated TESS time series.
Paper: HIP 65426 is a High-frequency Delta Scuti Pulsator in Plausible Spin–Orbit Alignment with its Directly Imaged Exoplanet
Authors: Aldo G. Sepulveda, Daniel Huber, Timothy R. Bedding, Daniel R. Hey, Simon J. Murphy, Zhoujian Zhang, Michael C. Liu
Figure caption: TESS amplitude spectra of HIP 65426, zoomed in on a region of low frequencies. Vertical dashed lines denote the locations of f  r,1, f  r,2 as described in Section 3.2, as well as the locations of 2 × f  r,1 and 2 × f  r,2.
Paper: HIP 65426 is a High-frequency Delta Scuti Pulsator in Plausible Spin–Orbit Alignment with its Directly Imaged Exoplanet
Authors: Aldo G. Sepulveda, Daniel Huber, Timothy R. Bedding, Daniel R. Hey, Simon J. Murphy, Zhoujian Zhang, Michael C. Liu
Figure caption: The left panel displays a sample of 100 sky-projected posterior orbits resulting from our fit of HIP 65426 b. The cyan star represents the position of HIP 65426 and the orange dots represent the relative astrometry of HIP 65426 b (with no error bars on this panel). The right panels compare the model orbit separation and position angles from the same 100 posterior orbits to the input astrometric data.
Paper: HIP 65426 is a High-frequency Delta Scuti Pulsator in Plausible Spin–Orbit Alignment with its Directly Imaged Exoplanet
Authors: Aldo G. Sepulveda, Daniel Huber, Timothy R. Bedding, Daniel R. Hey, Simon J. Murphy, Zhoujian Zhang, Michael C. Liu
Figure caption: Normalized inclination posteriors for the HIP 65426 system, where ﹩P({i}_{\star }| {P}_{\mathrm{rot}},{R}_{\star },v\sin i)﹩ represents the host star rotational inclination and i HIP 65426 b represents the orbital inclination of HIP 65426 b. Median and 68% credible intervals are written in the figure.
Paper: HIP 65426 is a High-frequency Delta Scuti Pulsator in Plausible Spin–Orbit Alignment with its Directly Imaged Exoplanet
Authors: Aldo G. Sepulveda, Daniel Huber, Timothy R. Bedding, Daniel R. Hey, Simon J. Murphy, Zhoujian Zhang, Michael C. Liu
Figure caption:                       ﹩v\sin i﹩ compared to photometric rotation frequency for the sample of hot (8300–12,000 K) stars presented in Balona (2017). Pink stars for HIP 65426 (8840 ± 200 K, Chauvin et al. 2017) are overplotted to represent both f  r,1 and f  r,2.
Paper: HIP 65426 is a High-frequency Delta Scuti Pulsator in Plausible Spin–Orbit Alignment with its Directly Imaged Exoplanet
Authors: Aldo G. Sepulveda, Daniel Huber, Timothy R. Bedding, Daniel R. Hey, Simon J. Murphy, Zhoujian Zhang, Michael C. Liu
Figure caption: Relative astrometry of HIP 65426 b used in our orbit fit (Section 3.4) compared to our best-fitting linear models used to evaluate the astrometric uncertainties. Even with the inclusion of high-precision measurements from GRAVITY, the uncertainties overall appear reasonable.
Paper: HIP 65426 is a High-frequency Delta Scuti Pulsator in Plausible Spin–Orbit Alignment with its Directly Imaged Exoplanet
Authors: Aldo G. Sepulveda, Daniel Huber, Timothy R. Bedding, Daniel R. Hey, Simon J. Murphy, Zhoujian Zhang, Michael C. Liu
Figure caption: 1D posterior probability densities from our orbit fit of HIP 65426 b.
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: Detection significance contours for a typical target star. For each simulated survey, we show the K/σ  K  = 10σ, 3σ, and 1σ contours as solid, dotted, solid, and dashed lines, respectively. Certain features are more prominent for some survey strategies, such as the strong 2 yr alias peak for the Centered strategy and the lower sensitivity of the Uniform strategy to short-period planets. But at each significance level, it is clear that the local slope within the D ⊕ Earth-analog region (gray) does not change from strategy to strategy.
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: First 2 yr of simulated observations for the Double Burst internight observing strategy as applied to the 40-star target sample with practical constraints on target observability. Stars are shown in order of increasing R.A. from top to bottom. Orange markers represent nights during which each target was observed, gray markers show observations that were scheduled and then dropped owing to simulated weather losses and telescope closures, and gray lines indicate the nights on which these losses occurred. For most stars, we are able to achieve a reasonable approximation of the idealized version of this strategy shown in Figure 4 in spite of these practical constraints.
Paper: Investigating Asymmetry Development from SiO to H2O Maser Regions in VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Youngjoo Yun, Haneul Yang, Jaeheon Kim
Figure caption: Moment-zero maps of each 22.2 GHz H2O maser transition line. The contour levels are adopted at 10 12 15 20 25 30 50... for multiples of each rms value.
Paper: Investigating Asymmetry Development from SiO to H2O Maser Regions in VX Sagittarii
Authors: Dong-Hwan Yoon, Se-Hyung Cho, Youngjoo Yun, Haneul Yang, Jaeheon Kim
Figure caption: Position–velocity spot maps of the 43.1 GHz SiO maser transition line. The spot color indicates the velocity and the spot size represents the logarithmic scale of the intensity.
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: Position–velocity spot maps of the 86.2 GHz SiO maser transition line. The spot color indicates the velocity and the spot size represents the logarithmic scale of the intensity.
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: Position–velocity spot maps of the 22.2 GHz H2O maser transition line. The spot color indicates the velocity and the spot size represents the logarithmic scale of the intensity.
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: Position–velocity spot maps of the 42.8 GHz SiO maser transition line. The spot color indicates the velocity and the spot size represents the logarithmic scale of the intensity.
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 Rossby Number, R 0, and flare rate for young GKM stars. For the younger sample (top row; t age = 4.5–50 Myr), we find no correlations between flare rate and R 0. For the slightly older sample (bottom row; t age = 50–250 Myr), we find no change in the average flare rate for M stars. For K and G stars, we start to see some evolution in this relationship. For K and G stars, we see that as R 0 increases, the average flare rate decreases. This could indicate that as stars spin down, their flare activity also begins to decline. We find that for the full GKM sample of stars (bottom row, rightmost column), the relationship between R 0 and flare rate is best fit by a broken power law, with a turnover at R 0 = 0.136. For the younger full sample (top row, rightmost column), we find this relationship is best fit by a single power law. The histograms are colored by number of stars in each bin. ✎
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: Measured flare frequency distribution slopes, α, as a function of the stellar effective temperature, T eff, and age. We measured these FFDs with respect to flare energy. We find that the FFD slopes as a function of the energy are consistent with α = −0.6 to −0.2 for stars <300 Myr in TESS observations. A shallower FFD slope is indicative of more high-energy flares. We present all measured FFDs in the Appendix and all measured slopes and errors in Table A1. We find the shallowest slopes for stars T eff = 3400–4440 K, with a range from α = −0.44 to −0.22. We do not include the results for stars T eff = 3850–4440 K and t age = 20–40 Myr as this bin contained only six stars with detected flares. We present the average results of measured FFD slopes for the Hyades, Pleiades, and Praesepe clusters from Ilin et al. (2021) as black squares. We present the results of measured FFD slopes for all TESS primary mission targets in white circles (Feinstein et al. 2022b) as “field-age.” We discuss what drives the difference between our sample and Ilin et al. (2021) in Section 3.1. ✎
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: Top: distribution of the selected sample across the sky and colored by the adopted age of the association (see Table 1). The all-sky coverage by TESS has unlocked new populations of stars to observe. We take advantage of this observing strategy to measure flare rates across 26 different nearby young moving groups, clusters, and associations. Bottom: distribution of adopted effective temperatures, T eff [K] for stars in our sample. We include all stars with T eff ≤ 6000 K. ✎