adsabs/AstroCLIMB huggingface dataset:
Paper: A Photometric and Astrometric Study of the Open Clusters NGC 1664 and NGC 6939
Authors: Seliz Koç, Talar Yontan, Selçuk Bilir, Remziye Canbay, Tansel Ak, Timothy Banks, Serap Ak, and Ernst Paunzen
Figure caption: Two-color diagrams of the most probable member main-sequence stars in the regions of NGC 1664 (a) and NGC 6939 (b). Red dashed and green solid curves represent the reddened ZAMS given by Sung et al. (2013) and ±1σ standard deviations, respectively.
Paper: A Photometric and Astrometric Study of the Open Clusters NGC 1664 and NGC 6939
Authors: Seliz Koç, Talar Yontan, Selçuk Bilir, Remziye Canbay, Tansel Ak, Timothy Banks, Serap Ak, and Ernst Paunzen
Figure caption: (U − B)0 × (B − V)0 diagrams (upper panels) and the distributions of normalized δ0.6 (lower panels) for NGC 1664 (a) and NGC 6939 (b). The solid blue lines in the upper and lower panels represent the main sequence of Hyades and the Gaussian models that were fitted to the histograms, respectively.
Paper: A Photometric and Astrometric Study of the Open Clusters NGC 1664 and NGC 6939
Authors: Seliz Koç, Talar Yontan, Selçuk Bilir, Remziye Canbay, Tansel Ak, Timothy Banks, Serap Ak, and Ernst Paunzen
Figure caption: CMDs for the NGC 1664 (panels a, b, and c) and NGC 6939 (panels d, e, and f). The differently colored dots represent the membership probabilities according to the color scales shown on the right side of the diagrams. Gray colored dots identify the field stars. The blue lines show the PARSEC isochrones, while the purple shaded areas surrounding these lines are their associated errors. The best-fitting isochrone for NGC 1664 corresponds to a 675 Myr age for the cluster, while that for NGC 6939 is 1.5 Gyr.
Paper: A Photometric and Astrometric Study of the Open Clusters NGC 1664 and NGC 6939
Authors: Seliz Koç, Talar Yontan, Selçuk Bilir, Remziye Canbay, Tansel Ak, Timothy Banks, Serap Ak, and Ernst Paunzen
Figure caption: The distance histograms of NGC 1664 (a) and NGC 6939 (b). The red and black dashed lines show the best Gaussian fits to the distances of the Bayesian approach method (Bailer-Jones et al. 2021) and are calculated from parallaxes (Gaia Collaboration et al. 2021).
Paper: A Photometric and Astrometric Study of the Open Clusters NGC 1664 and NGC 6939
Authors: Seliz Koç, Talar Yontan, Selçuk Bilir, Remziye Canbay, Tansel Ak, Timothy Banks, Serap Ak, and Ernst Paunzen
Figure caption: The galactic orbits and birth radii of NGC 1664 (a,b) and NGC 6939 (c,d) in the Z × RGC and RGC × t planes. The filled yellow circles and triangles show the present-day and birth positions, respectively. Red arrows are the motion vectors of the OCs.
Paper: A Photometric and Astrometric Study of the Open Clusters NGC 1664 and NGC 6939
Authors: Seliz Koç, Talar Yontan, Selçuk Bilir, Remziye Canbay, Tansel Ak, Timothy Banks, Serap Ak, and Ernst Paunzen
Figure caption: The luminosity functions of NGC 1664 (a) and NGC 6939 (b). The gray color shows all of the sample while green represents most probable single main-sequence stars.
Paper: A Photometric and Astrometric Study of the Open Clusters NGC 1664 and NGC 6939
Authors: Seliz Koç, Talar Yontan, Selçuk Bilir, Remziye Canbay, Tansel Ak, Timothy Banks, Serap Ak, and Ernst Paunzen
Figure caption: Present-day mass functions of NGC 1664 (a) and NGC 6939 (b) derived from all sample (red circle) and the probable single-star sample (green circle) groups. The mass functions of the OCs are shown with the blue lines.
Paper: A Photometric and Astrometric Study of the Open Clusters NGC 1664 and NGC 6939
Authors: Seliz Koç, Talar Yontan, Selçuk Bilir, Remziye Canbay, Tansel Ak, Timothy Banks, Serap Ak, and Ernst Paunzen
Figure caption: The cumulative radial distribution of stars in different mass ranges for NGC 1664 (a) and NGC 6939 (b).
Paper: The Hubble PanCET Program: Emission Spectrum of Hot Jupiter HAT-P-41b
Authors: Guangwei Fu, David K. Sing, Drake Deming, Kyle Sheppard, H. R. Wakeford, Thomas Mikal-Evans, Munazza K. Alam, Leonardo A. Dos Santos, and Mercedes López-Morales
Figure caption: HST WFC3 G141 spectral bin transit lightcurves after ramp-effect correction using RECTE (left) and corresponding residuals (right) with their relative ratios to the photon-limit noise (σ/σγ) levels.
Paper: The Hubble PanCET Program: Emission Spectrum of Hot Jupiter HAT-P-41b
Authors: Guangwei Fu, David K. Sing, Drake Deming, Kyle Sheppard, H. R. Wakeford, Thomas Mikal-Evans, Munazza K. Alam, Leonardo A. Dos Santos, and Mercedes López-Morales
Figure caption: The WFC3/G141 emission spectrum is in excellent agreement with that in Mansfield et al. (2021).
Paper: The Hubble PanCET Program: Emission Spectrum of Hot Jupiter HAT-P-41b
Authors: Guangwei Fu, David K. Sing, Drake Deming, Kyle Sheppard, H. R. Wakeford, Thomas Mikal-Evans, Munazza K. Alam, Leonardo A. Dos Santos, and Mercedes López-Morales
Figure caption: ATMO retrieval of the HAT-P-41b emission spectrum. The featureless black-like spectrum (left) is best fitted with an isothermal TP profile (right).
Paper: The Hubble PanCET Program: Emission Spectrum of Hot Jupiter HAT-P-41b
Authors: Guangwei Fu, David K. Sing, Drake Deming, Kyle Sheppard, H. R. Wakeford, Thomas Mikal-Evans, Munazza K. Alam, Leonardo A. Dos Santos, and Mercedes López-Morales
Figure caption: Posterior distribution of the ATMO retrieval. The metallicity is mostly unconstrained due to a lack of features within the emission spectrum.
Paper: The Hubble PanCET Program: Emission Spectrum of Hot Jupiter HAT-P-41b
Authors: Guangwei Fu, David K. Sing, Drake Deming, Kyle Sheppard, H. R. Wakeford, Thomas Mikal-Evans, Munazza K. Alam, Leonardo A. Dos Santos, and Mercedes López-Morales
Figure caption: HAT-P-41b WFC3/G141 emission spectrum compared with other hot Jupiters. The water feature strength index (﹩{{\rm{S}}}_{{{\rm{H}}}_{2}{\rm{O}}}﹩; Mansfield et al. 2021) measures the 1.4 μm water band feature size relative to the blackbody model based on the out-of-band spectrum. Centered at zero, with zero being the blackbody-like featureless spectrum. Increasing negative values (redder color) represent stronger emission features and increasing positive values (bluer color) represent stronger absorption features. The circle size scales with the host star temperature (Teff). The gray vertical dash lines are condensation lines for various metals at 100 mbar assuming solar metallicity. We see mostly featureless spectra at higher dayside temperatures (>2700 K) where H− continuum opacity expects to dominate (Parmentier et al. 2018). At the lower temperature side, we see mostly water absorption features where the atmosphere is too cool for gaseous heavy metal absorbers such as TiO to form and drive thermal inversion. HAT-P-41b sits at this in between transitional region where planets can have absorption, emission, or featureless spectra. Further observations of HAT-P-41b in the longer wavelength with the James Webb Space Telescope (JWST) will help us to precisely determine its thermal structure and understand what causes thermal inversion in hot-Jupiters atmospheres.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: Flowchart of the SCR method in this work for a given PS1 passband.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: Distribution of stars in the Teff-﹩\mathrm{log}g﹩ plane for the g band. Calibration sample stars are distributed in the green-background region. The two vertical dotted lines mark Teff = 6500 K and 4500 K. The blue dotted line marks the boundary between the main-sequence and giant stars. A color bar is overplotted at the upper-left corner indicating the normalized stellar densities.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: Spatial distribution of the calibration sample stars for the gband. A color bar is overplotted to the right indicating the stellar number densities. The gray dotted line indicates the Galactic plane.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: Spatial distributions of the control sample stars for the grizy bands. The band and the star number are labeled in each panel.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: Two-dimensional second-order polynomial fitting (with six free parameters) of intrinsic colors as functions of Teff and [Fe/H] for the control stars. From top to bottom are for the GBP − g, GRP − r, GRP − i, GRP − z, and GRP − y colors, respectively. The left column shows the fitting results after 3σ clipping, and the outliers are indicated by gray pluses. The red and blue curves represent results for [Fe/H] = 0 and −1, respectively, and the fitting residuals are labeled. The second, third, and fourth columns plot residuals against Teff, [Fe/H], and magnitude, respectively.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: Linear regression of reddening coefficients of the GBP − g, GRP − r, GRP − i, GRP − z, and GRP − y colors with respect to E(GBP − GRP) for the calibration samples. To avoid crowdness, only one in fifty stars are plotted. Colors indicate different temperatures. For the middle and bottom panels where reddening coefficients show weak dependence on temperature, the red pluses are the median values after 3σ clipping and the outliers are indicated by gray pluses; the red lines are linear fits to the red pluses; the slopes, offsets, and fitting residuals are all labeled. For the two top panels where reddening coefficients show moderate temperature dependence, the fitted reddening coefficients for four temperature ranges are shown.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: Spatial variations of magnitude offsets after a ﹩20^{\prime} \times 20^{\prime} ﹩ binning in the g, r, i, z, and ybands. The black dotted line indicates the Galactic plane in each panel. Color bars are overplotted to the right. The small region marked with a red box in the i band is replotted in Figure 8.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: A zoom in plot for the small region in Figure 7 (red box) in the i band with the same color bar. The spacing of the gray grids is 3.°3.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: The correlation plots between the magnitude offsets with a restriction of the star numbers of box is more than five for each two bands. For each panel, the correlation coefficient are marked. The color in each panel indicates number density of stars.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: Same as Figure 7 but after smoothing.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: Magnitude offsets as a function of star numbers in ﹩20^{\prime} \times 20^{\prime} ﹩ region before and after correction. Form top to bottom are for the g, r, i, z, and y bands, respectively. The green (orange) pluses are the initial (corrected) magnitude offsets, and their standard deviations are indicated by red (blue) dots. The convergence value of the scatter is marked in each panel.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: The variations of magnitude offset as a function of magnitude (left) and GBP − GRP (right) in g, r, i, z, and y bands. The red pluses are the median values. The black and gray dotted lines in each panel denote magnitude offsets of 0 and ±5 mmag, respectively.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: An example showing the variations of r magnitude offset as a function of r magnitude obtained by comparing with the SDSS stripe 82 data. The blue pluses are the median values. The color represents the number density of stars.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: The variations of magnitude offset as a function of magnitude in the five bands. The black and blue circles denote results from the SDSS Stripe 82 and DES DR1, respectively. The green dots denote results of comparison with the aperture-based magnitudes of PS1. The red lines denote results from Gaia.
Paper: Validation and Improvement of the Pan-STARRS Photometric Calibration with the Stellar Color Regression Method
Authors: Kai Xiao, and Haibo Yuan
Figure caption: The difference between the aperture-based and PSF magnitudes as a function of PSF magnitude in the five bands. The black points in each panel are the median values. The linear fitting results to these dots are overplotted in red lines and marked.
Paper: Five Decades of Chromospheric Activity in 59 Sun-like Stars and New Maunder Minimum Candidate HD 166620
Authors: Anna C. Baum, Jason T. Wright, Jacob K. Luhn, and Howard Isaacson
Figure caption: Initial plots of HD 10145 showed large, consistent offsets in S-value between pre- and post-2004 CPS data. We present data with adjusted median S-values.
Paper: Five Decades of Chromospheric Activity in 59 Sun-like Stars and New Maunder Minimum Candidate HD 166620
Authors: Anna C. Baum, Jason T. Wright, Jacob K. Luhn, and Howard Isaacson
Figure caption: Cycling in HD 4628 has a phase inconsistent with our sinusoidal model. Cycling in HD 146233 follows a highly variable trend.
Paper: Five Decades of Chromospheric Activity in 59 Sun-like Stars and New Maunder Minimum Candidate HD 166620
Authors: Anna C. Baum, Jason T. Wright, Jacob K. Luhn, and Howard Isaacson
Figure caption: HD 166620 appears to have entered a Maunder minimum between its final observations with HIRES-1 and first observations with HIRES-2. HD 101501 experienced 10 yr of lower activity, a much lower amplitude cycle than the rest of its cycle.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: Spectrum of HD 34415 in the 6430 Å region, which shows the composite profiles of the lines. Component A has the stronger broad lines. The sharp and much weaker lines of component B sit near the center of the broader features.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: Spectrum of HD 182735 in the 6430 Å region, which shows the composite profiles of the lines. Component A is the broad-lined star. Component B is the narrow-lined star that is positioned near the center of the broad-lined component.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: A plot of the HD 34415 radial velocities compared with the computed velocity curves (solid lines). Each CfA velocity is represented by a cross. The squares correspond to KPNO velocities and the circles to those of Fairborn Observatory, with open symbols representing the primary and solid symbols the secondary. Phase zero is a time of periastron passage. This preliminary orbit for HD 34415 has an orbital period of 6400 days and a moderate eccentricity of 0.43.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: A plot of the HD 144839 radial velocities (Solid circles = Fairborn Observatory and open circles = KPNO) compared with the computed velocity curve (solid line). Phase zero is a time of periastron passage. The binary has an orbital period of 995 days and a modest eccentricity of 0.16.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: A plot of the radial velocities of the double-lined binary HD 182735 (Open symbols = primary and solid symbols = secondary) compared with the computed velocity curves (solid lines). Squares = KPNO and circles = Fairborn Observatory. Phase zero is a time of periastron passage. The binary has an orbital period of 1052.4 days and a high eccentricity of 0.728.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: Least-squares frequency spectra of the HD 6260 Johnson B data set, showing the results of progressively fixing the two detected frequencies. The arrows indicate the two frequencies at 1.38803 day−1 (top) and 1.46205 day−1 (middle). The bottom panel shows the frequency spectrum with these two frequencies fixed. Both frequencies were confirmed in the Johnson V data set.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: The Johnson B photometric data for HD 6260, phased with the two frequencies and times of minimum from Table 11. The two frequencies are 1.38803 day−1 (top) and 1.46205 day−1 (bottom). For each panel, the data set has been prewhitened to remove the other known frequency.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: Radial velocities of HD 6260 phased with a period of 0.89477 day. The time of maximum velocity is HJD 2456933.72 ± 0.03 and the amplitude of the sine curve fit is 2.8 ± 0.3 km s−1.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: Least-squares frequency spectra of HD 19649 in Johnson B, showing the results of progressively fixing the three detected frequencies. The arrows indicate the three frequencies (top to bottom): 0.94354, 0.89775, and 1.04214 day−1. All three frequencies were confirmed in the Johnson V data set.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: The Johnson B photometric data for HD 19649, phased with the three frequencies and times of minimum from Table 11. The three frequencies are (top to bottom) 0.94354, 0.89775, and 1.04214 day−1. For each panel, the data set has been prewhitened to remove the other known frequencies.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: Least-squares frequency spectra of the HD 28819 Johnson B data set. The arrow in the top panel indicates the single detected frequency of 3.51010 day−1. The bottom panel is the frequency spectrum resulting when the 3.51010 day−1 frequency is fixed. The same frequency was found in the Johnson V data set.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: The Johnson B photometric data for HD 28819, phased with the 3.51010 day−1 frequency and time of minimum from Table 11.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: Least-squares frequency spectra of the HD 34415 Johnson B data set, showing the results of progressively fixing the four detected frequencies. The arrows indicate the four frequencies (top to bottom) 0.94532, 0.97627, 0.88817, and 0.91529 day−1. All four frequencies were confirmed in the Johnson V data set.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: The Johnson B photometric data for HD 34415, phased with the four frequencies and times of minimum from Table 11. The four frequencies are (top to bottom) 0.94532, 0.97627, 0.88817, and 0.91529 day−1. For each panel, the data set has been prewhitened to remove the other known frequencies.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: Least-squares frequency spectra of the HD 58431 Johnson B data set, showing the results of progressively fixing the two detected frequencies. The arrows indicate the two frequencies at 2.33709 day−1 (top) and 1.64711 day−1 (middle). Both frequencies were confirmed in the Johnson V data set.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: The Johnson B photometric data for HD 58431, phased with the two frequencies and times of minimum from Table 11. The two frequencies are 2.33709 day−1 (top) and 1.64711 day−1 (bottom). For each panel, the data set has been prewhitened to remove the other frequency.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: Least-squares frequency spectra of the HD 122928 Johnson B data set, showing the results of progressively fixing the two detected frequencies. The arrows indicate the two frequencies at 2.57058 day−1 (top) and 2.36802 day−1 (middle). Both frequencies were confirmed in the Johnson V data set.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: The Johnson B photometric data for HD 122928, phased with the two frequencies and times of minimum from Table 11. The two frequencies are 2.57058 day−1 (top) and 2.36802 day−1 (bottom). For each panel, the data set has been prewhitened to remove the other frequency.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: Least-squares frequency spectra of the HD 144839 Johnson B data set. The arrow in the top panel indicates the single detected frequency of 2.20767 day−1. The bottom panel is the frequency spectrum resulting when the 2.20767 day−1 frequency is fixed. The same frequency was found in the Johnson V data set.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: The Johnson B photometric data for HD 144839, phased with the 2.20767 day−1 frequency and time of minimum from Table 11.
Paper: Nine Bright γ Doradus Variables Discovered with Ground-based Photometry
Authors: Gregory W. Henry, Francis C. Fekel, and Michael H. Williamson
Figure caption: Least-squares frequency spectra of the HD 182735 Johnson B data set. The arrow in the top panel indicates the single detected frequency of 2.07866 day−1. The bottom panel is the frequency spectrum resulting when the 2.07866 day−1 frequency is fixed. The same frequency was found in the Johnson V data set.