adsabs/AstroCLIMB huggingface dataset:
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Observed population of all planets from Kepler as a function of the planet radius (R ⊕) and orbital period (days; A. Dattilo et al. 2023). Transiting planets with an age under 700 Myr are depicted as circles, with colors corresponding to their age derived from their host cluster or stellar association. HIP 67522 b is outlined as a star and lands well within the mature hot Jupiter part of parameter space. Planet properties from the NASA Exoplanet Science Institute (2020).
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Broadband light curve of HIP 67522 b observed with JWST/NIRSpec, which combines data from both NRS1 and NRS2. The top panel shows the raw normalized data (gray data points) overlaid with the systematic model (red line), as described in Section 5.2. During transit, there are two spot crossings, which are highlighted. In the middle panel, the best-fit model from our MCMC fit is overplotted with the systematic-corrected data. The bottom panel shows the residuals. Green data points in each panel represent the binned data at ∼1.5 minute intervals. The egress was missed due to an unknown TTV.
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Left: TESS Sector 64 light curve (blue points) binned to 1.5 minutes intervals and compared to a Gaussian process for the stellar variability (black). The transit times for HIP 67522 b are shaded in gray. Right: phase-folded light curve of HIP 67522 b after the best-fit stellar variability model has been removed. Data is binned to 1 minute intervals with the best-fit transit model shown in black.
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Posteriors from the MCMC fit of the JWST broadband light curve using Pipeline 1 for the parameters, center of transit time (T 0), ratio of the semimajor axis-to-stellar radius (a/R*), and inclination (inc). In the histogram, the dashed lines indicate the 16th and 84th percentiles. Figure was made with corner.py (D. Foreman-Mackey 2016).
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: The spectral energy distribution (SED) for HIP 67522 (black). We label each component of the SED based on how it was derived, as described in Section 4. For our photochemical model, we used a mix of empirical templates and PHOENIX models longward of 5690 Å, but show the pure model version here (and note that the differences were small).
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Transit photometry of HIP 67522 b taken with SOAR using the Sloan ﹩g^{\prime} ﹩ filter compared to 100 random draws from the fit posteriors (black). Photometric uncertainties are larger for the last ≃30 minutes due to the rotator failure.
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Left: radius evolution of HIP 67522 b for masses of 8 M ⊕ (red), 15 M ⊕ (blue), and 30 M ⊕ (green) assuming standard hot Jupiter interior heating. The dotted blue line shows the 15 M ⊕ case without interior heating. Posterior predictive errors on the radius are shown only for the 15 M ⊕ cases, but those of the other cases are similar in magnitude. Right: corner plot of the heated 15 M ⊕ posteriors, showing the bulk metallicity as a mass fraction (Z  p ), the intrinsic temperature of the planet (T int), and the system age, which is in agreement with the age inferred from observations.
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Atmospheric models for each scenario with various masses, metallicity ([M/H]), and C/O. In clear models, variations in mass influence the intensity of the C/O feature. Cloud models exhibit changes in cloud deck strength with varying masses. Photochemical models show additional features with high [M/H] and a weakened C/O feature with low [M/H]. Spot models highlight significant differences in the optical band.
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Transmission spectrum of HIP 67522 b with the best (lowest σ) atmospheric models for each scenario: for the clear-atmosphere model, M = M15⊕, C/O = 0.25, [M/H] = 1.5 (purple); for the cloudy model, M = M8⊕, C/O = 0.25, [M/H] = 1.5 (pink); for the photochemical model, M = M15⊕, C/O = 0.50, [M/H] = 1.0 (red). Models are binned to a spectral resolution of R = 600, and data points are binned to a bin size of 4. The plot on the right highlights the presence of SO2 in the atmosphere of the planet.
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Clear atmospheric models for a mass of 15⊕ across various C/O and [M/H] ratios: C/O = 0.25 and [M/H] = 1.5 (purple), C/O = 0.25; [M/H] = 0.0 (blue); C/O = 2.0 and [M/H] = 1.5 (pink). Models are binned to a spectral resolution of R = 600. The observational data points are shown in black and have been binned to enhance clarity, with a bin size of 4. The C/O = 0.25;[M/H] = 1.5 model (purple) demonstrates the closest fit to the observational data. As the C/O ratio increases (as show in pink), a methane feature is introduced (3.4 μm) that is not present in the data; while there is a decrease in [M/H] (as shown in blue), the CO2 feature decreases.
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Sigma (σ) values for the clear atmosphere PICASO models’ fits to the JWST transmission spectrum, encompassing masses from 8–50 M ⊕, C/O ratios spanning from 0.25 to 2 × solar, and [M/H] ranging from 0–2. Most of the parameter space is ruled out to a confidence level >5σ (pink), while the most favorable fit models (green) are 15–20 M ⊕, a high metallicity, and a C/O ≤1.5 × solar.
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: The transmission spectrum of HIP 67522 b from Pipeline 1 (blue data points; Section 5.2), Pipeline 2 (orange data points; Section 5.3), and Pipeline 3 (pink data points; Section 5.4). All reduction pipelines are consistent with each other.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Sigma for the VULCAN photochemical model grid, which considered a subset of the parameter values from the clear and cloudy model grids. The “X” in the lower-right corner, situated on the solar metallicity, 1.5 × solar C/O model grid, indicates that that particular VULCAN model did not converge despite our best efforts, and thus its σ value may not be correct.
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Same as Figure 9, but for the cloudy models.
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: SO2 mixing ratio profiles for selected cases in the VULCAN photochemistry grid, showing the variation in the SO2 abundance with metallicity and C/O.
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Left: mass–radius plot of planets with reliable mass measurements and relative uncertainties <25% for mass, <8% for radius, and orbital periods P < 20 days. Data points are colored by their equilibrium temperature. Square and circular data points represent mass determination from TTVs and RVs, respectively. Composition lines (dashed) indicate iron (red), rocky (orange), water (blue), and cold H2/He (turquoise; L. Zeng et al. 2019).The masses obtained from PICASO and the retrievals are displayed here, with the former offset for clarity. Right: mass–density plot of these same planets, distinguishing between the rocky and volatile-rich planets separated by the composition of water. The data points are colored by the insolation flux. Both of these plots highlight that HIP 67522 b occupies a distinctive position within the M–R diagram, establishing itself as one of the planets with the lowest density ever discovered. Planet properties from NASA Exoplanet Science Institute (2020).
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Same as Figure 9 but including the impact of inhomogeneities on the stellar surface for the clear-atmosphere models. The effect is largely negligible, with improvements to the fits isolated to the high-metallicity and/or high-C/O cases due to better agreement around the H2O band.
Paper: The Featherweight Giant: Unraveling the Atmosphere of a 17 Myr Planet with JWST
Authors: Pa Chia Thao, Andrew W. Mann, Adina D. Feinstein, Peter Gao, Daniel Thorngren, Yoav Rotman, Luis Welbanks, Alexander Brown, Girish M. Duvvuri, Kevin France, Isabella Longo, Angeli Sandoval, P. Christian Schneider, David J. Wilson, Allison Youngblood, Andrew Vanderburg, Madyson G. Barber, Mackenna L. Wood, Natasha E. Batalha, Adam L. Kraus, Catriona Anne Murray, Elisabeth R. Newton, Aaron Rizzuto, Benjamin M. Tofflemire, Shang-Min Tsai, Jacob L. Bean, Zachory K. Berta-Thompson, Thomas M. Evans-Soma, Cynthia S. Froning, Eliza M.-R. Kempton, Yamila Miguel, J. Sebastian Pineda
Figure caption: Atmospheric retrieval results. The retrieved median model is shown in red while the 1σ and 2σ envelopes are shown by pink shaded regions. The NIRSpec G395H observations are shown using blue error bars. The retrieved posterior distributions for the chemical species of interest (e.g., H2O, CO, CO2, SO2, and H2S) are shown alongside the retrieved posterior probability density for the planetary mass.
Paper: A Close Binary Lens Revealed by the Microlensing Event Gaia20bof
Authors: E. Bachelet, P. Rota, V. Bozza, P. Zieliński, Y. Tsapras, M. Hundertmark, J. Wambsganss, Ł. Wyrzykowski, P. J. Mikołajczyk, R. A. Street, R. Figuera Jaimes, A. Cassan, M. Dominik, D. A. H. Buckley, S. Awiphan, N. Nakhaharutai, S. Zola, K. A. Rybicki, M. Gromadzki, K. Howil, N. Ihanec, M. Jabłońska, K. Kruszyńska, K. Kruszyńska, U. Pylypenko, M. Ratajczak, M. Sitek, M. Rabus
Figure caption: Lightcurves of the event observed from the ground and Gaia. The Wide+ model is presented (blue solid line; the dashed line represents the model seen by Gaia) but all models produce almost identical lightcurves. The parallax signal between Gaia and Earth is almost not visible. All data sets have been artificially shifted to Gaia magnitudes for presentation purposes. The presented uncertainties take into account the rescaling parameters derived during the posterior exploration; see the main text for more details.
Paper: Discovery of RR Lyrae in the Ultra-faint-dwarf Galaxy Virgo III
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: The color–magnitude diagram for stars located within the 4 × r  h  ellipse of Virgo III, including the three detected RR Lyrae, which have been corrected for extinction. For the three RR Lyrae, we have also applied approximate color corrections to bring the single-epoch SDSS photometry close to the mean values. We assumed such corrections carry an error of ∼0.1 mag. The mean r-band magnitudes for them were taken from Table 3. The green curves are three evolutionary tracks for horizontal-branch (HB) models with mass (M) of 0.58, 0.64, and 0.70 M ⊙, taken from the BaSTI library. These HB models are α-enhanced (as found in many UFD; for a review, see Simon 2019), with [Fe/H] = −1.9 dex, and vertically shifted to the absolute magnitudes using the distance modulus derived in our work.
Paper: Discovery of RR Lyrae in the Ultra-faint-dwarf Galaxy Virgo III
Authors: Chow-Choong Ngeow, Anupam Bhardwaj
Figure caption: Number of RR Lyrae (N RRL) as a function of M  V  for the 94 galaxies listed in Table 4. To deal with the ”log of zero” problem on the y-axis (in log-scale), we added +1 to the N RRL. The green solid curve represents the empirical relation derived in Martínez-Vázquez et al. (2019). The dashed curve are for the different selected values of specific RR Lyrae frequency S RR. Several "outliers" are also marked in this plot. The inset figure is the zoomed-in version for UFD galaxies with N RRL < 7, where Virgo III is marked as a magenta star. For clarity, error bars and the curves for S RR < 1 are omitted in the inset figure. Note that the y-axis is in linear scale in the inset figure.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: SFR distribution of four types of galaxies.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Distribution of the relationship between SFR and color indices for the four types of galaxy pairs.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Some visual galaxy pairs that have not been confirmed as physical pairs.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Distribution of the stellar mass ratio of two galaxies in a pair.
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Relationship between the stellar mass and SFR of galaxies in pairs.