adsabs/AstroCLIMB huggingface dataset:
Paper: Gap Opening and Inner Disk Structure in the Strongly Accreting Transition Disk of DM Tau
Authors: Logan Francis, Nienke van der Marel, Doug Johnstone, Eiji Akiyama, Simon Bruderer, Ruobing Dong, Jun Hashimoto, Hauyu Baobab Liu, Takayuki Muto, Yi Yang
Figure caption: Same as Figure 9, but for the effects of changing the gas surface density enhancement in the inner disk in the DALI model described in Section 5.2.3.
Paper: AU Microscopii in the Far-UV: Observations in Quiescence, during Flares, and Implications for AU Mic b and c
Authors: Adina D. Feinstein, Kevin France, Allison Youngblood, Girish M. Duvvuri, D. J. Teal, P. Wilson Cauley, Darryl Z. Seligman, Eric Gaidos, Eliza M.-R. Kempton, Jacob L. Bean, Hannah Diamond-Lowe, Elisabeth Newton, Sivan Ginzburg, Peter Plavchan, Peter Gao, Hilke Schlichting
Figure caption: Comparison of photoevaporation-driven atmospheric mass loss for AU Mic b. We run our calculations under three different flare evolution scenarios: (top) no flares present; (middle) persistent flares during the first 200 Myr; and (bottom) persistent flares during the first 1000 Myr. The box represents the first quartile (Q 1; 25th percentile), the median (50th percentile), and the third quartile (Q 3; 75th percentile). The whiskers mark the interquartile (IQR  = Q 3–Q 1), where the lower limit is defined as Q 1–1.5 × IQR, and the upper limit is defined as Q3 + 1.5 × IQR. The largest spread is seen in the calculation where we inject flares for the first 1000 Myr. The boxes are colored by the median mass-loss rate in [grams per second]. Super-flares (﹩{L}_{\mathrm{flare}}\gt {10}^{33}﹩ erg s−1) can boost mass loss by up to five orders of magnitude. (https://github.com/afeinstein20/cos_flares/blob/paper-version/notebooks/flare_mass_loss.ipynb)
Paper: AU Microscopii in the Far-UV: Observations in Quiescence, during Flares, and Implications for AU Mic b and c
Authors: Adina D. Feinstein, Kevin France, Allison Youngblood, Girish M. Duvvuri, D. J. Teal, P. Wilson Cauley, Darryl Z. Seligman, Eric Gaidos, Eliza M.-R. Kempton, Jacob L. Bean, Hannah Diamond-Lowe, Elisabeth Newton, Sivan Ginzburg, Peter Plavchan, Peter Gao, Hilke Schlichting
Figure caption: The average quiescent spectrum for AU Mic. We removed time intervals that fall within the highlighted yellow regions in Figure 1. We labeled all known emission lines seen in our spectrum. Emission features marked with pink lines (O I triplet) are partially contaminated by air glow. We present all measured line centers and flux values for these emission features in Table A1. (https://github.com/afeinstein20/cos_flares/blob/paper-version/notebooks/labeled_quiescent_spectrum.ipynb)
Paper: AU Microscopii in the Far-UV: Observations in Quiescence, during Flares, and Implications for AU Mic b and c
Authors: Adina D. Feinstein, Kevin France, Allison Youngblood, Girish M. Duvvuri, D. J. Teal, P. Wilson Cauley, Darryl Z. Seligman, Eric Gaidos, Eliza M.-R. Kempton, Jacob L. Bean, Hannah Diamond-Lowe, Elisabeth Newton, Sivan Ginzburg, Peter Plavchan, Peter Gao, Hilke Schlichting
Figure caption: Photochemical models for AU Mic b and c. Temperature–pressure profiles (black lines) and mixing ratios (colored) for AU Mic b (top left) and AU Mic c (top right). We model the planets in equilibrium (dashed) and disequilibrium (solid). Normalized transmission spectra as observed from 0.6 to 12 μm for AU Mic b (middle row) and AU Mic c (bottom row). Dominant CH4, CO2, CO, and C2H6 are labeled in the normalized transmission spectra. These models follow the methods presented in Teal et al. (2022) and are evaluated with AU Mic in quiescence. (https://github.com/afeinstein20/cos_flares/blob/paper-version/notebooks/tp_profile.ipynb)
Paper: AU Microscopii in the Far-UV: Observations in Quiescence, during Flares, and Implications for AU Mic b and c
Authors: Adina D. Feinstein, Kevin France, Allison Youngblood, Girish M. Duvvuri, D. J. Teal, P. Wilson Cauley, Darryl Z. Seligman, Eric Gaidos, Eliza M.-R. Kempton, Jacob L. Bean, Hannah Diamond-Lowe, Elisabeth Newton, Sivan Ginzburg, Peter Plavchan, Peter Gao, Hilke Schlichting
Figure caption: Light curves of the C III emission line at 1175.95 Å (black) and the Si III emission line at 1294.55 Å (blue) used to identify flares in the data. Flares identified are labeled with vertical orange lines.
Paper: BD+47 378: An Eclipsing Binary Containing a δ Sct Pulsating Star
Authors: Kyeongsoo Hong, Jae Woo Lee, Pakakaew Rittipruk, Jang-Ho Park, Hye-Young Kim, Cheongho Han
Figure caption: The positions for the primary (filled circle) and secondary (open circle) components of BD+47 378 on the H-R diagram. The pink solid lines represent the evolutionary tracks (Z = 0.019; Y = 0.273) for the primary with a mass of 1.69 M ⊙ and the secondary with a mass of 0.80 M ⊙, and the dotted line denotes the isochrones with logarithmic age of log (t) = 8.95 yr (Girardi et al. 2000). The black solid and dashed–dotted lines are the instability strips of δ Sct and γ Dor stars (Dupret et al. 2005), respectively.
Paper: BD+47 378: An Eclipsing Binary Containing a δ Sct Pulsating Star
Authors: Kyeongsoo Hong, Jae Woo Lee, Pakakaew Rittipruk, Jang-Ho Park, Hye-Young Kim, Cheongho Han
Figure caption: The amplitude spectra from the PERIOD04 software. No significant peaks higher than 20 day−1 are found.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: The log of the spiral arm strength vs. log sSFR for field galaxies (top panel) and galaxies in massive clusters (bottom panel). The sSFRs in these plots come from the GSWLC-2. The green and red lines in both plots are the best fits for field and cluster galaxies, respectively, with log sSFR ≥ −12, only including galaxies with 10 ≤ log M* from the NSA < 11. The slope (m), y-intercept (b), and rms of the best-fit lines are printed on the corresponding plot, along with the Spearman (ρ) and Pearson (r) correlation coefficients. The data points are color coded based on concentration (red: C ≥ 4.5; yellow: 4.0 ≤ C < 4.5; green: 3.5 ≤ C < 4.0; blue: C < 3.5). The galaxies marked by open magenta diamonds were classified by Yu & Ho (2020) as either S0-, S0, or SB0.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Histograms of spiral galaxy properties for field galaxies (top panels) and galaxies in massive clusters (bottom panels). (a) arm strength, (b) bar strength, (c) f3, (d) pitch angle ϕ, (e) concentration, and (f) stellar mass. The red histograms give the full sample. Hatched histograms indicate unbarred galaxies. The cyan histograms mark galaxies with pitch angle measurements.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: (a) Concentration vs. log(stellar mass) for all field galaxies (upper left), all galaxies in massive clusters (lower left), unbarred field galaxies (upper right), and unbarred galaxies in massive clusters (lower right). In the left panels, the green and red lines give the best-fit lines for 10 ≤ log M* < 11 for all field and cluster galaxies, respectively. In the right panels, the blue and black lines give the best-fit lines for 10 ≤ log M* < 11 for unbarred field and cluster galaxies, respectively. The best-fit parameters are given in Table 1.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Bar strength vs. concentration (left panels) and bar strength vs. log M* (right panels) for barred galaxies in the field (top row) and in massive clusters (bottom row). In the left panels, the green and red lines are the best-fit linear bar strength vs. C relations for all field and cluster galaxies, respectively, with 10 ≤ log M* < 11. No correlation between bar strength and log M* is found for unbarred field galaxies (upper-right panel). In the lower-right panel, the black line is the best-fit bar strength vs. log M* relation for unbarred cluster galaxies. See Table 1 for more information about the best-fit relations.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Comparison of s vs. C for all field galaxies (upper left), all galaxies in massive clusters (lower left), unbarred field galaxies (upper right), and unbarred galaxies in massive clusters (lower right). The green line in the two left panels and the upper-right panel is the best-fit line for all field galaxies with 10 ≤ log M* < 11. The red line in the two left panels is the best-fit relation for all galaxies with 10 ≤ log M* < 11 in massive clusters. The blue line in the upper-right panel is the best-fit lines for unbarred field galaxies for 10 ≤ log M* < 11. The parameters of the best-fit lines are given in Table 1.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Plots of f3 vs. concentration for all field galaxies (upper left), unbarred field galaxies (upper right), all galaxies in massive clusters (lower left), and unbarred galaxies in massive clusters (lower right). The green and red lines in the two left panels are the best-fit lines for the full set of field and cluster galaxies, respectively, with 10 ≤ log M* < 11. The blue line in the upper-right panel is the best-fit line for 10 ≤ log M* < 11 unbarred field galaxies. No significant correlation is seen for unbarred cluster galaxies. Best-fit parameters are available in Table 1.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Comparison of arm strength s vs. bar strength for field galaxies (top row) and galaxies in massive clusters (bottom row). The left panels include galaxies with 3 ≤ C < 4, while the right panel includes galaxies with 4 ≤ C < 5. In all panels, the sample is limited to galaxies with 10.0 ≤ log M* < 11.0. The green line in the left panels is the best-fit line for field galaxies with 3 ≤ C < 4. The blue and black lines in the right panels are the best-fit lines for field and cluster galaxies, respectively, for 4 ≤ C < 5. Best-fit parameters of these lines are provided in Table 1.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Pitch angle ϕ vs. concentration (left panels) and ϕ vs. log M* (right panels) for all field galaxies (top row) and all galaxies in massive clusters (bottom row). The green and red lines in the left panels are the best-fit lines for ϕ vs. C for all field and cluster galaxies, respectively, with 10 ≤ log M* < 11. The green and red lines in the right panels are the best-fits for ϕ vs. log M* for all field and cluster galaxies, respectively, with 10 ≤ log M* < 11. See Table 1 for the parameters of these fits.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Comparison of s vs. stellar mass for the full set of field galaxies (upper left) and the full set of galaxies in massive clusters (lower left). In the upper right, the data for the unbarred field spirals are shown, and the lower right gives the unbarred galaxies in massive clusters. No correlations are present (see Table 1).
Paper: SOFIA FEEDBACK Survey: PDR Diagnostics of Stellar Feedback in Different Regions of RCW 49
Authors: M. Tiwari, M. Wolfire, M. W. Pound, E. Tarantino, R. Karim, L. Bonne, C. Buchbender, R. Güsten, C. Guevara, S. Kabanovic, Ü. Kavak, M. Mertens, N. Schneider, R. Simon, J. Stutzki, A. G. G. M. Tielens
Figure caption: A red-blue-green (RBG) image of RCW 49 is shown in the top left panel. Red corresponds to the [C II] integrated intensity emission within the velocity range of −30 to 30 km s−1. Green corresponds to the GLIMPSE (Benjamin et al. 2003) 8 μm emission, and blue corresponds to the ATLASGAL (Schuller et al. 2009) 870 μm continuum. Different interesting regions toward which the PDR analysis is done are shown and outlined with white boxes. The [C II] and 12CO emissions toward the northern cloud, ridge, shell, and pillar are shown in the middle and right panels, respectively. The red crosses mark the lines of sight for which the spectra are presented in Figure 3. In the bottom left panel, the 8 μm emission image is overlaid with [C II] emission contours highlighting these regions. The contour colors are the same as the ones in the [C II] maps shown in the middle panels. The Wd2 cluster, the WR20b star, and the O9V star are shown in pink in all panels.
Paper: SOFIA FEEDBACK Survey: PDR Diagnostics of Stellar Feedback in Different Regions of RCW 49
Authors: M. Tiwari, M. Wolfire, M. W. Pound, E. Tarantino, R. Karim, L. Bonne, C. Buchbender, R. Güsten, C. Guevara, S. Kabanovic, Ü. Kavak, M. Mertens, N. Schneider, R. Simon, J. Stutzki, A. G. G. M. Tielens
Figure caption: Representative spectra of [C II], 12CO, 13CO, and [O I] toward the northern cloud (nc), ridge, shell, pillar, p1, p3, and p7. All data were convolved to the same angular resolution of ∼20″, and the spectral resolution of the spectra shown here is 1 km s−1.
Paper: SOFIA FEEDBACK Survey: PDR Diagnostics of Stellar Feedback in Different Regions of RCW 49
Authors: M. Tiwari, M. Wolfire, M. W. Pound, E. Tarantino, R. Karim, L. Bonne, C. Buchbender, R. Güsten, C. Guevara, S. Kabanovic, Ü. Kavak, M. Mertens, N. Schneider, R. Simon, J. Stutzki, A. G. G. M. Tielens
Figure caption: Emission maps of [C II] and 12CO (3–2) toward the regions p1, p3, and p7 (shown in Figure 1). The [C II] maps are overlaid with H2 0–0 S(1) intensity contours, and the 12CO maps are overlaid with H2 0–0 S(2) intensity contours. The contours are colored such that the darkest shade of red corresponds to the highest intensity. The red crosses mark the lines of sight for which the spectra are presented in Figure 3.
Paper: On the Unusual Variability of 2MASS J06195260–2903592: A Long-lived Disk around a Young Ultracool Dwarf
Authors: Michael C. Liu, Eugene A. Magnier, Zhoujian Zhang, Eric Gaidos, Trent J. Dupuy, Pengyu Liu, Beth A. Biller, Johanna M. Vos, Katelyn N. Allers, Jason T. Hinkle, Benjamin J. Shappee, Sage N. L. Constantinou, Mitchell T. Dennis, Kenji S. Emerson
Figure caption: PS1 light curve for 2MASS J0619-2903, showing variability on timescales from subday to 11 yr. Upper limits (5σ) are plotted as open circles with downward-pointing arrows. For reference, the dashed lines indicate the predicted 1σ range of magnitudes assuming no extinction, adopting the PS1 colors of M6 dwarfs from Best et al. (2018), and using the minimum (brightest) y P1 magnitude (which is shown as the solid red line) to compute magnitudes from the colors. Such color information is not available for the w P1 band, so there are no corresponding dashed lines for it. The small panel at the top shows the (J − K)MKO color synthesized from our SpeX spectra, and labels at the very top denote the start of each calendar year.
Paper: On the Unusual Variability of 2MASS J06195260–2903592: A Long-lived Disk around a Young Ultracool Dwarf
Authors: Michael C. Liu, Eugene A. Magnier, Zhoujian Zhang, Eric Gaidos, Trent J. Dupuy, Pengyu Liu, Beth A. Biller, Johanna M. Vos, Katelyn N. Allers, Jason T. Hinkle, Benjamin J. Shappee, Sage N. L. Constantinou, Mitchell T. Dennis, Kenji S. Emerson
Figure caption: Possible short-timescale variability of 2MASS J0619-2903 from PS1 optical photometry, showing the six most variable observing blocks (defined as four or more detections in the same filter within a 1.5 hr window). Different colors indicate different filters, and the titles give the average Modified Julian Date for each block’s detections. The reduced χ 2 value for the photometry compared to each block’s average magnitude is also reported, all of which correspond to p-values of < 10−4. The x- and y-axes ranges are identical in all the plots.
Paper: On the Unusual Variability of 2MASS J06195260–2903592: A Long-lived Disk around a Young Ultracool Dwarf
Authors: Michael C. Liu, Eugene A. Magnier, Zhoujian Zhang, Eric Gaidos, Trent J. Dupuy, Pengyu Liu, Beth A. Biller, Johanna M. Vos, Katelyn N. Allers, Jason T. Hinkle, Benjamin J. Shappee, Sage N. L. Constantinou, Mitchell T. Dennis, Kenji S. Emerson
Figure caption: Comparison of 2MASS J0619-2903 optical spectrum from Cruz et al. (2003) with the solar-metallicity M6 template from PyHammer v2.0 (Roulston et al. 2020), normalized by their fluxes at 8400–8900 Å. The observed spectrum (gray) is significantly redder than the template. After dereddening by A  V  = 4.3 mag, the agreement is much better. (The Cruz et al. spectra plotted here have been smoothed by a 5 pixel boxcar.)
Paper: On the Unusual Variability of 2MASS J06195260–2903592: A Long-lived Disk around a Young Ultracool Dwarf
Authors: Michael C. Liu, Eugene A. Magnier, Zhoujian Zhang, Eric Gaidos, Trent J. Dupuy, Pengyu Liu, Beth A. Biller, Johanna M. Vos, Katelyn N. Allers, Jason T. Hinkle, Benjamin J. Shappee, Sage N. L. Constantinou, Mitchell T. Dennis, Kenji S. Emerson
Figure caption: Near-IR light curves of 2MASS J0619-2903 taken with SOFI in the J  S , H, and K  S  bands. The light curves show variability with an amplitude of ≈1% over the ≈ 4 hr of observing at each night. The median magnitude of each light curve is listed in the legend, as calibrated with 2MASS stars in the field.
Paper: On the Unusual Variability of 2MASS J06195260–2903592: A Long-lived Disk around a Young Ultracool Dwarf
Authors: Michael C. Liu, Eugene A. Magnier, Zhoujian Zhang, Eric Gaidos, Trent J. Dupuy, Pengyu Liu, Beth A. Biller, Johanna M. Vos, Katelyn N. Allers, Jason T. Hinkle, Benjamin J. Shappee, Sage N. L. Constantinou, Mitchell T. Dennis, Kenji S. Emerson
Figure caption: Optical light curves of 2MASS J0619-2903 taken with LCOGT, showing the relative photometry of the source from 2021 December to 2022 February. For each filter, the baseline flux is taken to be the median of the upper 50% of points and subtracted from all the epochs. The different passbands offset by 0.2 days for clarity. No clear evidence for variability is detected over this 1.5 month duration given the measurement uncertainties.
Paper: On the Unusual Variability of 2MASS J06195260–2903592: A Long-lived Disk around a Young Ultracool Dwarf
Authors: Michael C. Liu, Eugene A. Magnier, Zhoujian Zhang, Eric Gaidos, Trent J. Dupuy, Pengyu Liu, Beth A. Biller, Johanna M. Vos, Katelyn N. Allers, Jason T. Hinkle, Benjamin J. Shappee, Sage N. L. Constantinou, Mitchell T. Dennis, Kenji S. Emerson
Figure caption: IRTF/SpeX prism spectra of 2MASS J0619-2903 after dereddening with the best-fit extinction relative to the 2015 spectrum, all normalized to their 2.15–2.25 μm flux. The results are consistent with the scenario that the near-IR variability is due to changes in circumstellar extinction.
Paper: On the Unusual Variability of 2MASS J06195260–2903592: A Long-lived Disk around a Young Ultracool Dwarf
Authors: Michael C. Liu, Eugene A. Magnier, Zhoujian Zhang, Eric Gaidos, Trent J. Dupuy, Pengyu Liu, Beth A. Biller, Johanna M. Vos, Katelyn N. Allers, Jason T. Hinkle, Benjamin J. Shappee, Sage N. L. Constantinou, Mitchell T. Dennis, Kenji S. Emerson
Figure caption: IRTF/SpeX prism spectra of 2MASS J0619-2903, all normalized to their 2.05–2.25 μm flux. The legend with the observing dates is ordered by synthesized J − K color, with the bluest epoch listed at the top.
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: Identification chart of stars in NGC 1664 (left panel) and for NGC 6939 (right panel), taken from Leicester database and archive service (LEDAS).
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: Interval V- and G-band magnitude histograms of NGC 1664 (a, b) and NGC 6939 (c, d). The arrows show the faint limiting apparent magnitudes in the V and G bands. Black lines indicate the star counts based on the stars detected in the study, while red lines are star counts based on the stars taken from Gaia EDR3 for the same cluster regions.
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: Comparisons of observational magnitude and colors with those calculated from Maciejewski & Niedzielski (2007) (a)–(b) and for NGC 6939. The mean differences and their ±1σ dispersions are represented with solid and dashed red lines, 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: The radial density profiles for the NGC 1664 (a) and NGC 6939 (b) clusters. Errors were derived using an equation of ﹩1/\sqrt{N}﹩, where N represents the number of stars used in the density estimation. The fitted red curve represents the King (1962) profile. The horizontal blue dashed line shows background stellar density.
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: VPDs and the radial distribution of proper-motion diagrams for NGC 1664 (panels a and b) and NGC 6939 (panels c and d). The zoomed box in panel (c) shows the region of condensation for NGC 6939 in the VPD. The continuous curves in panels (b) and (d) represent the King (1962) profiles, which are fitted to the data points. Gray horizontal lines represent the field star contamination and dotted lines indicate the radius that was adopted to find the possible cluster members.
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: V × (B − V) and G × (GBP − GRP) CMDs of NGC 1664 (a), (b) and NGC 6939 (c), (d). The blue dotted–dashed lines represent the ZAMS (Sung et al. 2013) including the binary star effect. The membership probabilities of stars that lie within the fitted ZAMS are shown with different colors; these member stars are located within ﹩{r}_{\mathrm{lim}}=8.5﹩ and ﹩{r}_{\mathrm{lim}}=6\buildrel{\,\prime}\over{.} 5﹩ of the cluster centers calculated for NGC 1664 and NGC 6939, respectively. Gray dots indicate the field stars. Letters A and B in panels (c) and (d) indicate possible BSSs of NGC 6939.
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: Histograms of the membership probabilities versus number of stars for NGC 1664 (a) and NGC 6939 (b). The green colored shading denotes the stars that lie within the main-sequence band and effective cluster radii.
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: VPDs of NGC 1664 (a) and NGC 6939 (b). Colored dots identify the membership probabilities of the cluster stars according to the color scale shown on the right. The zoomed box in panel (b) represents the region of condensation for the NGC 6939 cluster in the VPD. Dashed lines are the intersection of the mean proper-motion values. The color scale shows the membership probabilities of the most likely cluster members.