adsabs/AstroCLIMB huggingface dataset:
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: Sun in the center, positions of Mercury, Venus, Earth, and Mars on 2023 August 28 and trajectory of Mercury, Venus, Earth, and Mars from 2020 January 1 to 2030 January 1 viewed from an angle of ϕ ≈ 0.9 π/2 rad from the orbit plane of Earth. Circles represent the resolution of a traditional telescope with diameter d = bim. The small one (gray) is for λ = 4 μm, the medium one (black) is for λ = 10 μm, and the large one (dashed gray) is for λ = 18.5 μm. The imaging baseline changes with the star system distance to have optimal sensitivity for planets in the HZ. This representation of the spatial resolution is valid for distances from 6.59 pc (60 m telescope Eq.) up to 65.9 pc (600 m telescope equivalent). Recall that this representation is not an accurate model to decide if photobombing occurs for LIFE.
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: Top: inner solar system seen from a near edge-on angle ϕ ≈ 0.9π/2 rad = 81°. At each point, p = (δx, δy) is the maximum of the target confusion map between Earth at p and another planet. The red line is ﹩{ \mathcal D }=0﹩. Earth is inside a region where ﹩{ \mathcal D }\gt 0﹩; i.e., Earth is photobombed. In this case, Earth is photobombed by Venus. The white dot represents the planet detected in that case. Bottom: flux of Earth, Venus, and the photobombed Earth. Photobombing depends on the flux of both Earth’s and Venus’s flux. The photobombed Earth’s flux is the best point source that generates a signal similar to that of Earth and Venus together.
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: The detection probability of TRAPPIST-1 e. The detection probability is the probability that the integrated S/N of TRAPPIST-1 e is above the threshold of 7 after an observation of 100 hr. TRAPPIST-1 e becomes undetectable for a distance above ≈6.5 pc under that criterion.
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: The contamination probability of TRAPPIST-1 e. The contamination probability is the probability that a given detected planet is contaminated. The contamination probability increases with distance and inclination angle.
Paper: Thermal Variability in the Martian Upper Atmosphere within the Crustal Magnetic Field Region Induced by Gravity Wave Dissipation Due to Ion-drag Effect
Authors: Xing Wang, Xiaojun Xu, Jun Cui, Siqi Yi, Hao Gu, Zilu Zhou, Hengyan Man, Lei Luo, Peishan He, Pu Yang
Figure caption: The wave (a) heating/cooling rates and (b) energy fluxes. Hni is the neutral-ion frictional heating rate; Hsen refers to the sensible heat flux divergence; Hpress and HEuler are the works done per unit time by wave-induced pressure gradients and Eulerian drifts; and Htot denotes the sum of these heating/cooling rates. Fni, Fsen, Fpress, FEuler, and Ftot are the respective heating/cooling energy fluxes. Q = Htot/cpρ0 represents the wave heating/cooling rate in unit of Kelvin per sol (K sol−1). Input parameters of the selected wave mode are τ = 55.19 minutes, λx = 60 km, kz0 = −0.50 km−1, and cp = 18.12 m s−1.
Paper: Thermal Variability in the Martian Upper Atmosphere within the Crustal Magnetic Field Region Induced by Gravity Wave Dissipation Due to Ion-drag Effect
Authors: Xing Wang, Xiaojun Xu, Jun Cui, Siqi Yi, Hao Gu, Zilu Zhou, Hengyan Man, Lei Luo, Peishan He, Pu Yang
Figure caption: Vertical profiles of the wave damping rate driven by the ion-drag effect (﹩{k}_{{zi}}^{{\rm{ion}}}﹩) and molecular diffusion and thermal conduction (﹩{k}_{{zi}}^{{\rm{mol}}}﹩). The input parameters of the selected wave mode are τ = 55.19 minutes, λx = 60 km, kz0 = −0.50 km−1, and cp = 18.12 m s−1.
Paper: Thermal Variability in the Martian Upper Atmosphere within the Crustal Magnetic Field Region Induced by Gravity Wave Dissipation Due to Ion-drag Effect
Authors: Xing Wang, Xiaojun Xu, Jun Cui, Siqi Yi, Hao Gu, Zilu Zhou, Hengyan Man, Lei Luo, Peishan He, Pu Yang
Figure caption: The difference of wave-driven temperatures between the strong magnetic field region and the NCF region of the two selected wave sets. The vertical wave numbers of the two selected wave sets are (a) −0.19 km−1 and (b) −0.50 km−1. Horizontal wavelengths of the selected wave sets range from 60 to 210 km in intervals of 30 km.
Paper: Thermal Variability in the Martian Upper Atmosphere within the Crustal Magnetic Field Region Induced by Gravity Wave Dissipation Due to Ion-drag Effect
Authors: Xing Wang, Xiaojun Xu, Jun Cui, Siqi Yi, Hao Gu, Zilu Zhou, Hengyan Man, Lei Luo, Peishan He, Pu Yang
Figure caption: Vertical profiles of (a) wave-driven pressure ratio (p1/p0) and temperature ratio (T1/T0) and (b) horizontal (u1) and vertical (w1) perturbed velocity. Input parameters of the selected wave mode are τ = 55.19 minutes, λx = 60 km, kz0 = −0.50 km−1, and cp =  18.12 m s−1.
Paper: Thermal Variability in the Martian Upper Atmosphere within the Crustal Magnetic Field Region Induced by Gravity Wave Dissipation Due to Ion-drag Effect
Authors: Xing Wang, Xiaojun Xu, Jun Cui, Siqi Yi, Hao Gu, Zilu Zhou, Hengyan Man, Lei Luo, Peishan He, Pu Yang
Figure caption: Vertical profiles of the wave heating/cooling rates in unit of K sol−1 driven by the two selected wave sets, with vertical wave numbers of (a) −0.19 km−1 and (b) −0.50 km−1. Horizontal wavelengths of the selected wave sets range from 60 to 210 km in intervals of 30 km.
Paper: Photometric Determination of Unresolved Main-sequence Binaries in the Pleiades: Binary Fraction and Mass-ratio Distribution
Authors: Rongrong Liu, Zhengyi Shao, Lu Li
Figure caption: Distributions of stars in the Pleiades region on CMDs of (a) Gaia, (b) 2MASS, and (c) combined optical and NIR bands. The crosses denote stars with kinematic membership probability Pk < 0.5. The gray points show stars with Pk ≥ 0.5. The star symbols mark the stars with neighbors in 5″. The error bars represent original observational errors. The black solid and dashed lines represent isochrones for q = 0 and 1, respectively, from the PARSEC 1.2s model of [Fe/H] = 0.1, ﹩\mathrm{log}(\mathrm{Age})/\mathrm{yr}=8.026﹩, and AV = 0.135 mag. The dotted–dashed lines represent isochrons for triples with equal masses. The horizontal line marks G = 16 mag. Note that three stars have been excluded from the plot due to invalid errors.
Paper: Photometric Determination of Unresolved Main-sequence Binaries in the Pleiades: Binary Fraction and Mass-ratio Distribution
Authors: Rongrong Liu, Zhengyi Shao, Lu Li
Figure caption:  ﹩\delta m\mbox{--}{{ \mathcal M }}_{{\rm{s}}}﹩ planes and ridgelines of six photometric bands for the Pleiades. ﹩{{ \mathcal M }}_{{\rm{s}}}﹩ represents the mass derived from the single-star multiband fitting. δm represents the magnitude difference between the observational data and the best-fit model in each band. Each error bar corresponds to an individual star, with the length indicating the observational error. The solid black line shows the ridgeline that represents the ﹩{{ \mathcal M }}_{{\rm{s}}}\mbox{--}{\rm{\Delta }}m﹩ relation. The dashed black line marks the position where the magnitude difference equals zero.
Paper: Eighteen Exoplanet Host Stars from the NPOI Data Archive
Authors: Ellyn K. Baines, Jeremy Jones, James H. Clark, Henrique R. Schmitt, Jordan M. Stone
Figure caption: Comparing the stellar mass from EPE and those based on NPOI measurements. All the stars are shown in the left panel, while a zoomed-in version is shown in the right panel so there is not as much crowding. The dotted line is the 1:1 ratio, the dashed lines in the left panel show which section of the plot is magnified in the right panel, and the solid red line is the linear fit of f(x) = 0.788x − 0.624.
Paper: Photometric Determination of Unresolved Main-sequence Binaries in the Pleiades: Binary Fraction and Mass-ratio Distribution
Authors: Rongrong Liu, Zhengyi Shao, Lu Li
Figure caption: Probability density functions (PDFs) of three members. The contour plots in panels (a), (b), and (c) illustrate the PDFs of stars with different binary probabilities: Pb = 0, 0.6, 1, respectively. The Source IDs of Gaia DR3 are marked in each panel. Each contour corresponds to the 1σ, 2σ, and 3σ (39.3%, 86.5%, and 98.9%) confidence levels. The blue lines denote the lower limit of detectable mass ratios.
Paper: Photometric Determination of Unresolved Main-sequence Binaries in the Pleiades: Binary Fraction and Mass-ratio Distribution
Authors: Rongrong Liu, Zhengyi Shao, Lu Li
Figure caption: Distributions of (a) equatorial coordinates, (b) proper motions, and (c) parallaxes for stars in the Pleiades region. The crosses denote field stars with kinematic membership probability Pk < 0.5. The gray points represent kinematic member stars with Pk ≥ 0.5. The black circle in panel (a) shows the half-number radius R50 = 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩37 of the kinematic members.
Paper: Photometric Determination of Unresolved Main-sequence Binaries in the Pleiades: Binary Fraction and Mass-ratio Distribution
Authors: Rongrong Liu, Zhengyi Shao, Lu Li
Figure caption: Lower limit of the detectable mass ratio (﹩{q}_{{\rm{lim}}}﹩) varying with primary mass. The blue line denotes the threshold where the secondary mass is 0.09﹩{{ \mathcal M }}_{\odot }﹩. Stars with mass ratios above this line are binary stars, and those below are considered “single stars.”
Paper: Eighteen Exoplanet Host Stars from the NPOI Data Archive
Authors: Ellyn K. Baines, Jeremy Jones, James H. Clark, Henrique R. Schmitt, Jordan M. Stone
Figure caption: Comparing ﹩m\sin i﹩ from EPE and ﹩m\sin i﹩ based on NPOI measurements. The dotted line is the 1:1 ratio, and the solid red line is the linear fit of f(x) = 1.124x − 0.335.
Paper: Kinematics of Cataclysmic Variables in the Solar Neighborhood in the Gaia Era
Authors: Remziye Canbay, Tansel AK, Selçuk Bilir, Faruk Soydugan, Zeki Eker
Figure caption: The spatial distribution of 385 CVs in the sample with respect to the Sun. X, Y, and Z are Sun-centered rectangular Galactic coordinates. P and IP denote polars and intermediate polars, respectively.
Paper: Kinematics of Cataclysmic Variables in the Solar Neighborhood in the Gaia Era
Authors: Remziye Canbay, Tansel AK, Selçuk Bilir, Faruk Soydugan, Zeki Eker
Figure caption: Comparison of the cumulative number of CVs estimated for 100 pc intervals. The numbers were estimated using the space densities and scale heights given by A. F. Pala et al. (2020) and R. Canbay et al. (2023). Red circles represent the data sample in this study.
Paper: Kinematics of Cataclysmic Variables in the Solar Neighborhood in the Gaia Era
Authors: Remziye Canbay, Tansel AK, Selçuk Bilir, Faruk Soydugan, Zeki Eker
Figure caption: Histogram of orbital periods of the final CV sample, including 385 CVs. The shaded area represents the orbital period gap. The vertical axis is given on a logarithmic scale since the numbers of polars (P) and intermediate polars (IP) are small compared to nonmagnetic systems.
Paper: Kinematics of Cataclysmic Variables in the Solar Neighborhood in the Gaia Era
Authors: Remziye Canbay, Tansel AK, Selçuk Bilir, Faruk Soydugan, Zeki Eker
Figure caption: Toomre diagram of the final CV sample of 385 objects. Systems are colored according to their population types described in the text.
Paper: Kinematics of Cataclysmic Variables in the Solar Neighborhood in the Gaia Era
Authors: Remziye Canbay, Tansel AK, Selçuk Bilir, Faruk Soydugan, Zeki Eker
Figure caption: Comparison of age–velocity dispersion relations of CVs and single white dwarfs. Blue circles represent the relation obtained from S. Cheng et al. (2019), while red circles show the values found for thin-disk CVs in this study.
Paper: Kinematics of Cataclysmic Variables in the Solar Neighborhood in the Gaia Era
Authors: Remziye Canbay, Tansel AK, Selçuk Bilir, Faruk Soydugan, Zeki Eker
Figure caption: Distribution of 385 CVs in the sample according to their equatorial (a) and Galactic (b) coordinates. In the upper panel, the red curve indicates the Galactic plane, and the green star symbol indicates the Galactic center.
Paper: Kinematics of Cataclysmic Variables in the Solar Neighborhood in the Gaia Era
Authors: Remziye Canbay, Tansel AK, Selçuk Bilir, Faruk Soydugan, Zeki Eker
Figure caption: Comparison of orbital period histograms of the samples used in A. C. Rodriguez et al. (2024) (a), A. F. Pala et al. (2020) (b), and this study (c). The orbital period histogram of the catalog of H. Ritter & U. Kolb (2003) is shown in the bottom panel. The shaded area represents the orbital period gap.
Paper: Kinematics of Cataclysmic Variables in the Solar Neighborhood in the Gaia Era
Authors: Remziye Canbay, Tansel AK, Selçuk Bilir, Faruk Soydugan, Zeki Eker
Figure caption: Orbital period–kinematic age relations found for all CVs (a) and nonmagnetic CVs (b) located in the thin-disk component of the Galaxy. Red solid lines represent the linear fits.
Paper: Kinematics of Cataclysmic Variables in the Solar Neighborhood in the Gaia Era
Authors: Remziye Canbay, Tansel AK, Selçuk Bilir, Faruk Soydugan, Zeki Eker
Figure caption: Histogram of orbital periods of the final CV sample. Systems are colored according to their population types described in the text.
Paper: Mon R2: A Hub–Filament System with an Infrared Bubble at the Hub Center
Authors: L. K. Dewangan, N. K. Bhadari, A. K. Maity, O. R. Jadhav, Saurabh Sharma, A. Haj Ismail
Figure caption: (a) The UKIDSS K-band image overlaid with the NVAS radio continuum emission contours at 4.8 GHz. The radio contours are shown at levels of 5, 15, 20, 24, 50, and 85 mJy beam−1. The inset at the bottom right exhibits the area containing the NVAS 4.8 GHz continuum emission. The thick curves (in pale green) show the arclike features. The solid box highlights the area covered by the ALMA band-6 observations, while the dotted–dashed box shows the area covered by HST/NICMOS2. (b) The HST/NICMOS2 F207M band image overlaid with embedded pointlike sources with H − K ≥ 2.3 mag (see open circles). The inset at the bottom right shows a zoomed-in view in the same band. (c) The SHARC-II 350 μm emission map, which is overlaid with the 350 μm continuum sources (see open squares and also Table A1). The peru contour at 0.34 Jy beam−1 and the light coral contour at 6 Jy beam−1 are the SHARC-II 350 μm emission (see text for details). (d) A zoomed-in view using the SHARC-II 350 μm emission map (see the solid box in Figure 1(c)) overlaid with the column density (N(H2)) contour (in red) at 1.2 × 1020 cm−2. The area highlighted by the solid box is presented in Figures 8(a)–(e). In each panel, the scale bar is computed at a distance of 830 pc, and the positions of five IR sources (i.e., IRS 1, IRS 2, IRS 3, IRS 4, and IRS 5) are highlighted by diamonds. The SHARC-II continuum map was smoothed using a boxcar averaging method with a width of 2 pixels.
Paper: Mon R2: A Hub–Filament System with an Infrared Bubble at the Hub Center
Authors: L. K. Dewangan, N. K. Bhadari, A. K. Maity, O. R. Jadhav, Saurabh Sharma, A. Haj Ismail
Figure caption: (a) ALMA 1.14 mm dust continuum map (see the solid box in Figure 1(a)). (b) A two-color composite map produced using the ALMA 1.14 mm dust continuum map (in red) and the HST/NICMOS2 F207M band image (in cyan). (c) A clumpfind decomposition of the ALMA 1.14 mm dust continuum emission, highlighting the spatial extent of several continuum sources (i.e., t1–t4, r1–r5, c1–c5, and u1–u5; see Table A2). In each panel, the scale bar is drawn at a distance of 830 pc and diamonds are the same as in Figure 1(a).
Paper: Mon R2: A Hub–Filament System with an Infrared Bubble at the Hub Center
Authors: L. K. Dewangan, N. K. Bhadari, A. K. Maity, O. R. Jadhav, Saurabh Sharma, A. Haj Ismail
Figure caption: (a) A three-color composite map produced using the ALMA 1.14 mm dust continuum map (in red), the HNC(3–2) moment-0 map (in green), and the UKIDSS K-band image (in blue). The dotted–dashed curve shows the location of the IR ring traced in the HST/NICMOS2 F207M band image. (b) A two-color composite map made using the ALMA 1.14 mm dust continuum map (in red) and the HST/NICMOS2 F207M band image (in cyan; see the solid box in Figure 7(a)). (c) A two-color composite map produced using the H13CN(3–2) moment-0 map (in red) and the HST/NICMOS2 F207M band image (in cyan). (d) The ALMA HNC(3–2) filled contour map at 10.68 km s−1 (in green) overlaid with contours of HNC(3–2) emission maps at 12.16 km s−1 (in red) and 9.94 km s−1 (in blue). (e) Average HNC(3–2) emission profile in the direction of the area highlighted by the rectangle (in cyan) in Figure 7(d). Contours of the HNC(3–2) map at 12.16 km s−1 are plotted with levels of 0.58 × [0.12, 0.21, 0.3, 0.5, 0.7, 0.8, 0.9] Jy beam−1, while the HNC(3–2) emission contours at 9.94 km s−1 are shown with levels of 0.49 × [0.12, 0.21, 0.3, 0.4, 0.5, 0.6, 0.7, 0.8, 0.9] Jy beam−1. In each panel, diamonds are the same as in Figure 1(a) and the scale bar is produced at a distance of 830 pc.
Paper: Mon R2: A Hub–Filament System with an Infrared Bubble at the Hub Center
Authors: L. K. Dewangan, N. K. Bhadari, A. K. Maity, O. R. Jadhav, Saurabh Sharma, A. Haj Ismail
Figure caption: (a) Clumpfind decomposition of the ALMA 1.14 mm dust continuum emission (see the dotted–dashed box in Figure 4(b)), displaying the spatial extent of at least five continuum sources (i.e., r1, r2, r3, r4, and r5; see Figure 4(c) and also Table A2). (b) Two-color composite map produced using the NVAS 4.8 GHz continuum map (in red) and the HST/NICMOS2 F207M band image (in cyan; see the dotted–dashed box in Figure 4(b)). (c) Clumpfind decomposition of the ALMA 1.14 mm dust continuum emission in the direction of continuum source r2 (see the dotted–dashed box in Figure 4(c) and also Figure 5(a)), which is also overlaid with the 1.14 mm continuum emission contours. The contours are plotted at levels of 1.32, 4.24, 6.5, 9.85, 13.25, 15.0, 19.0, and 24.31 mJy beam−1. The spatial extent of five compact continuum sources (i.e., c1, c2, c3, c4, and c5; see Figure 4(c) and also Table A2) is indicated by the five different colors. (d) Overlay of the 1.14 mm continuum emission contours on the NVAS 4.8 GHz continuum map; the contours are the same as in Figure 5(c). Beam sizes of the 1.14 mm dust continuum map (open ellipse) and the NVAS map (filled ellipse) are shown in the bottom left corner. In each panel, the scale bar is drawn at a distance of 830 pc and diamonds are the same as in Figure 1(a).
Paper: Mon R2: A Hub–Filament System with an Infrared Bubble at the Hub Center
Authors: L. K. Dewangan, N. K. Bhadari, A. K. Maity, O. R. Jadhav, Saurabh Sharma, A. Haj Ismail
Figure caption: (a) The ALMA CS(2–1) moment-0 map at [5, 14] km s−1. The molecular ring morphology, visible in the ALMA C18O(1–0) and CS(2–1) moment-0 maps, is outlined by a magenta curve based on visual inspection. The dashed curve highlights the connection between molecular filaments and molecular ring. (b) The ALMA CS(2–1) moment-1 map. The lower panels show PV diagrams of the (c) ALMA C18O(1–0) and (d) ALMA CS(2–1) emission along the curve indicated in panel (a). In panel (c), an almost inverted V feature is indicated by the dashed curve. In panels (a) and (b), the scale bar is computed at a distance of 830 pc, and diamonds are the same as in Figure 1(a).
Paper: Mon R2: A Hub–Filament System with an Infrared Bubble at the Hub Center
Authors: L. K. Dewangan, N. K. Bhadari, A. K. Maity, O. R. Jadhav, Saurabh Sharma, A. Haj Ismail
Figure caption: (a) The ALMA C18O(1–0) moment-0 map at [8, 13] km s−1. (b) The N(H2) map derived using the ALMA C18O(1–0) emission, with the N(H2) contour level of 1.2 × 1020 cm−2. (c) The ALMA C18O(1–0) moment-1 map. (d) The zoomed-in ALMA C18O(1–0) moment-1 map (see the solid box in Figure 2(c)). The map is also overlaid with contours (in orange) of the HST/NICMOS2 F207M band image and the positions of embedded pointlike sources with H − K ≥ 2.3 mag (see open circles and also Figure 1(b)). In each panel, the scale bar is computed at a distance of 830 pc, and diamonds are the same as in Figure 1(a).
Paper: Mon R2: A Hub–Filament System with an Infrared Bubble at the Hub Center
Authors: L. K. Dewangan, N. K. Bhadari, A. K. Maity, O. R. Jadhav, Saurabh Sharma, A. Haj Ismail
Figure caption: (a)–(d) Moment-0 maps and (e)–(h) moment-1 maps of ALMA HNC(3–2), H13CN(3–2), CCH(3–2), and CCH(4–3) emission, respectively. In each panel, diamonds are the same as in Figure 1(a).
Paper: Accurate and Robust Stellar Rotation Periods Catalog for 82771 Kepler Stars Using Deep Learning
Authors: Ilay Kamai, Hagai B. Perets
Figure caption: Three potential wrong predictions of our model. For each sample, the left panel shows the full light curve, and the right panel shows a zoomed-in slice of 180 days. The gray color represents the raw light curve. The orange color represents an averaged light curve over a window of 1 day. The titles show the Kepler KIC, lightPred period, and McQ14 period from A. McQuillan et al. (2014).
Paper: Structural Parameters of the Thin Disk Population from Evolved Stars in the Solar Neighborhood
Authors: Sedanur İyisan, Selçuk Bilir, Özgecan Önal Taş, Olcay Plevne
Figure caption: Space densities (left-hand panels) and scale heights (right-hand panels) estimated for different five absolute magnitude intervals of star fields within the Galactic latitude intervals in the 36-star fields. Green and red solid lines represent star fields in the north and south Galactic hemispheres, respectively.
Paper: Structural Parameters of the Thin Disk Population from Evolved Stars in the Solar Neighborhood
Authors: Sedanur İyisan, Selçuk Bilir, Özgecan Önal Taş, Olcay Plevne
Figure caption:  ﹩{M}_{{\rm{G}}}\times {({G}_{{\rm{BP}}}-{G}_{{\rm{RP}}})}_{0}﹩ CMD of a sample of 39,099,903 stars within the solar neighborhood. Main-sequence and evolved stars occupy the black dashed and blue dashed regions, respectively. The star clump at the lower left-hand part of the diagram is the white dwarf region. Spectral types concerning the dereddened color index are shown in the bottom part of the diagram.
Paper: Structural Parameters of the Thin Disk Population from Evolved Stars in the Solar Neighborhood
Authors: Sedanur İyisan, Selçuk Bilir, Özgecan Önal Taş, Olcay Plevne
Figure caption: Stellar density profiles for five absolute magnitude intervals in star field #01 (upper panels) and variations of model parameters with χ2 values (lower panels). The red lines in the upper panels show the Galaxy model fitted to the star density points, and the intersections of the red dashed lines represent the Galaxy model parameters with the minimum ﹩{\chi }_{{\rm{\min }}}^{2}﹩ value. The numerical values between the two panels are the central coordinates of the star field in the Galactic coordinate system, the absolute magnitude interval, the estimated space density, and the scale height.
Paper: Structural Parameters of the Thin Disk Population from Evolved Stars in the Solar Neighborhood
Authors: Sedanur İyisan, Selçuk Bilir, Özgecan Önal Taş, Olcay Plevne
Figure caption: MG × d diagram of evolved stars with σϖ/ϖ ≤ 0.02. White vertical lines are bright G-apparent magnitude limits for different MG absolute magnitude intervals, and solid and dash curves also represent G-apparent magnitudes.