adsabs/AstroCLIMB huggingface dataset:
Paper: OGLE-2017-BLG-0448Lb: A Low Mass–Ratio Wide-orbit Microlensing Planet?
Authors: Ruocheng Zhai, Radosław Poleski, Weicheng Zang, Youn Kil Jung, Andrzej Udalski, Renkun Kuang, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Jan Skowron, Michał K. Szymański, Igor Soszyński, Krzysztof Ulaczyk, Paweł Pietrukowicz, Szymon Kozłowski, Przemek Mróz, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Shude Mao, Jiyuan Zhang, Qiyue Qian, Wei Zhu
Figure caption: Caustic geometries of the four static 2L1S solutions. The locations of the host star and planet are indicated by cyan and blue arrows, respectively. The magenta lines show the caustic structures, and the red lines with an arrow indicate the source trajectory and the direction of the source motion. The radii of the green dots represent the best-fit normalized source radius, ρ, of each solution.
Paper: OGLE-2017-BLG-0448Lb: A Low Mass–Ratio Wide-orbit Microlensing Planet?
Authors: Ruocheng Zhai, Radosław Poleski, Weicheng Zang, Youn Kil Jung, Andrzej Udalski, Renkun Kuang, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Jan Skowron, Michał K. Szymański, Igor Soszyński, Krzysztof Ulaczyk, Paweł Pietrukowicz, Szymon Kozłowski, Przemek Mróz, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Shude Mao, Jiyuan Zhang, Qiyue Qian, Wei Zhu
Figure caption: Observed data together with the four static 2L1S solutions. Data shown in the top two panels are daily binned. All four solutions can fit the anomaly well (the lower five panels), but there are long-term residuals before ﹩{\mathrm{HJD}}^{{\prime} }=7900﹩, so we include high-order effects.
Paper: OGLE-2017-BLG-0448Lb: A Low Mass–Ratio Wide-orbit Microlensing Planet?
Authors: Ruocheng Zhai, Radosław Poleski, Weicheng Zang, Youn Kil Jung, Andrzej Udalski, Renkun Kuang, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Jan Skowron, Michał K. Szymański, Igor Soszyński, Krzysztof Ulaczyk, Paweł Pietrukowicz, Szymon Kozłowski, Przemek Mróz, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona, Mariusz Gromadzki, Hanyue Wang, Shude Mao, Jiyuan Zhang, Qiyue Qian, Wei Zhu
Figure caption: Observed light curve of the microlensing event, OGLE-2017-BLG-0448. Different colors represent the observed data from different data sets. The upper panel shows all of the data taken in 2017, and the lower panel displays a close-up of the planetary signal.
Paper: CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Thøger Emil Rivera-Thorsen, Alessandra Aloisi, Arjan Bik, Daniela Calzetti, John Chisholm, Andrew J. Fox, Michele Fumagalli, Kathryn Grasha, Svea Hernandez, Matteo Messa, Shannon Osborne, Göran Östlin, Elena Sabbi, Eva Schinnerer, Linda J. Smith, Christopher Usher, Aida Wofford
Figure caption: N V  P Cygni line of the target M95-YSC1 (black line). Shown in blue is the best-fit model as reported in Paper I. Shown in orange is the improved model found by fitting only between 1230 and 1250 Å, rather than the whole available spectrum. The red dashed vertical lines mark the wavelengths where the N V  ISM absorption is expected owing to the gas in the target galaxy, whereas the black dashed lines mark the Milky Way gas absorption.
Paper: CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Thøger Emil Rivera-Thorsen, Alessandra Aloisi, Arjan Bik, Daniela Calzetti, John Chisholm, Andrew J. Fox, Michele Fumagalli, Kathryn Grasha, Svea Hernandez, Matteo Messa, Shannon Osborne, Göran Östlin, Elena Sabbi, Eva Schinnerer, Linda J. Smith, Christopher Usher, Aida Wofford
Figure caption: Full-sky map of Magellanic and Galactic high-velocity clouds, color-coded by the LSR velocity of H I 21 cm emission. The locations of the CLUES target galaxies are marked with red stars. The data for the velocity map are taken from Westmeier (2018).
Paper: CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Thøger Emil Rivera-Thorsen, Alessandra Aloisi, Arjan Bik, Daniela Calzetti, John Chisholm, Andrew J. Fox, Michele Fumagalli, Kathryn Grasha, Svea Hernandez, Matteo Messa, Shannon Osborne, Göran Östlin, Elena Sabbi, Eva Schinnerer, Linda J. Smith, Christopher Usher, Aida Wofford
Figure caption: Observed FUV spectrum of M74-YSC1 in black, best-fit model in blue. The regions masked out of the fit are marked in gray. The detected ISM absorption lines are marked as green dashed lines and labeled. See Table 3 for the full list of detected absorption lines.
Paper: CLusters in the Uv as EngineS (CLUES). II. Subkiloparsec-scale Outflows Driven by Stellar Feedback
Authors: Mattia Sirressi, Angela Adamo, Matthew Hayes, Thøger Emil Rivera-Thorsen, Alessandra Aloisi, Arjan Bik, Daniela Calzetti, John Chisholm, Andrew J. Fox, Michele Fumagalli, Kathryn Grasha, Svea Hernandez, Matteo Messa, Shannon Osborne, Göran Östlin, Elena Sabbi, Eva Schinnerer, Linda J. Smith, Christopher Usher, Aida Wofford
Figure caption: Kinematics of neutral and ionized gas surrounding the CLUES clusters. The Si II  spectrum is shown in blue, and Si IV  (or C IV) is shown in red/orange, including data, model, and model components (dashed lines). Regions of the spectrum with absorption contamination from the Milky Way or Magellanic System gas are marked with gray and pink shaded areas, respectively.
Paper: An ALMA Molecular Inventory of Warm Herbig Ae Disks. I. Molecular Rings, Asymmetries, and Complexity in the HD 100546 Disk
Authors: Alice S. Booth, Margot Leemker, Ewine F. van Dishoeck, Lucy Evans, John D. Ilee, Mihkel Kama, Luke Keyte, Charles J. Law, Nienke van der Marel, Hideko Nomura, Shota Notsu, Karin Öberg, Milou Temmink, Catherine Walsh
Figure caption: Matched filter responses with Keplerian models and strong lines as filters alongside GoFish radial profiles and Keplerian masked integrated intensity maps for the C34S, ﹩{{\rm{H}}}_{2}^{13}\mathrm{CO}﹩, NO, 34SO, and SO2 lines in the HD 100546 disk.
Paper: An ALMA Molecular Inventory of Warm Herbig Ae Disks. I. Molecular Rings, Asymmetries, and Complexity in the HD 100546 Disk
Authors: Alice S. Booth, Margot Leemker, Ewine F. van Dishoeck, Lucy Evans, John D. Ilee, Mihkel Kama, Luke Keyte, Charles J. Law, Nienke van der Marel, Hideko Nomura, Shota Notsu, Karin Öberg, Milou Temmink, Catherine Walsh
Figure caption: Spectra generated using GoFish stacked over a 180–250 au annulus (Teague 2019).
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: McDonald 2.1 m broadband light curves of 1631+69 from 2020 July 24, August 18, September 22, and 2023 May 24 are shown phased with the new orbital ephemeris in the top panels. The sharpest eclipse-like features at cycle 0 (top left) and cycle 15,914 (second row right) were used to establish the orbital ephemeris. The bottom panel shows the photometry folded on the orbital period with the running average superimposed in white.
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: The ZTF g-, r-, and i-band light-curve data in green, red, and purple of 1631+69. The top panel shows the unfolded light curve. The middle panel shows the data folded on the orbital period, with the eclipse at phase 0. The bottom panel shows the Lomb–Scargle power spectrum as calculated from the ZTF high-state data. The orbital frequency and spin frequency are indicated with Ω and ω, the same as in Figure 7.
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: The ZTF g-, r-, and i-band light-curve data in green, red, and purple of 2313+16. The top panel shows the entire light curve. The middle panel shows the data folded on the orbital period. The bottom panel shows the Lomb–Scargle power spectrum showing the orbital (Ω) and possible spin frequencies (ω), including alias frequencies.
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: The ZTF g-, r-, and i-band light-curve data in green, red, and purple of 1626+33. The top panel shows the unfolded light curve. The middle panel shows the light curve folded on the orbital period after first detrending the data, and shows a subtle but significant eclipse at phase 0. The bottom panel shows the box least-squares power spectrum. We identify the strongest frequency as the orbital frequency (Ω), and also indicate the multiples and significant alias frequencies.
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: TESS power spectrum of 1631+69 with frequency identifications expressed as linear combinations of the orbital (Ω), spin (ω), and sampling (f samp) frequencies.
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: Power spectrum of the TESS data for the diskless IP 2011+60 (Romanov V48), showing the strong orbit (Ω), spin (ω), and beat (ω − Ω) frequencies, as well as their various sidebands and harmonics. The identifications of Ω and ω are identical to those from Kato & Romanov (2022).
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: The ZTF g-, r-, and i-band light-curve data in green, red, and purple of 2011+60. The top panel shows the entire light curve. The middle panel shows the data folded on the orbital period. The bottom panel shows the Lomb–Scargle power spectrum showing the orbital (Ω), spin (ω), and combination frequencies.
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: Two-dimensional TESS light curve of 1631+69, showing the dependence of the orbital profile on the spin–orbit beat phase. Deep eclipses are observed only at certain beat phases, thus explaining the extreme cycle-to-cycle variation in the eclipse depth in the McDonald photometry.
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: TESS data of 2011+60 (Romanov V48), folded on the spin and beat periods, showing the large changes in the spin profile during the beat phase. Phase 0 is arbitrary.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Gravity scores from Allers & Liu (2013) obtained for our targets (purple circle = TWA 28, smaller dark blue circle = TWA 27A, and light blue circle = TWA 27B), and for other M3–L7 objects with different ages as a comparison. We show for comparison field objects (McLean et al. 2003; Cushing et al. 2005), young companions (Allers et al. 2007; Bonnefoy et al. 2014), young β, and γ dwarfs. For members of α Persei, Upper Scorpious, Taurus, and ρ Ophiuchi, we include the value of the FeH index (Martín et al. 2017).
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Full 0.97–5.3 μm NIRSpec/IFU flux-calibrated spectra of TWA 28, TWA 27A, and TWA 27B, from top to bottom, respectively, at their original resolution of R ∼ 2700. We show in different colors the approximate wavelength ranges covered by each NIRSpec grating and filter combination. The spectra in this figure are available for download in the online journal.(The data used to create this figure are available.)
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Best matches found for the 0.97–5.3 μm spectra of TWA 28 (purple), TWA 27A (dark blue), and TWA 27B (light blue) using the BT-Settl model and the ATMO models.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Equivalent widths of the K I and Na I alkali lines for our targets (purple circle = TWA 28, smaller dark blue circle = TWA 27A, and light blue circle = TWA 27B) and the same comparison objects mentioned in Figure 4.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Full 0.97–2.0 μm NIRSpec/IFU spectrum of TWA 28 (purple), TWA 27A (dark blue), and TWA 27B (light blue), from top to bottom, respectively, at their original resolution of R ∼ 2700. We indicate the atomic absorption lines, emission lines, and molecular bands we expect for these objects.
Paper: Spectroscopic Follow-up on Potential Magnetic Cataclysmic Variables
Authors: Paula Szkody, Jan van Roestel, Paul A. Mason, Colin Littlefield, R. Michael Rich, Eric C. Bellm, Filipp D. Romanov, Brian F. Healy, Theophile Jegou du Laz, Russ R. Laher, Ben Rusholme
Figure caption: TESS power spectrum and phased light curve of 2313+16. The power spectrum shows no evidence of the 33.3 day−1 signal in the ZTF data, while the phased TESS light curve shows a shallow, well-defined dip. Phase 0 was defined arbitrarily to coincide with this dip, but without a radial velocity curve of the secondary it is unknown whether this dip coincides with the secondary’s inferior conjunction. Because 2313+16 has significant blending, the true amplitude of variation is much larger than it is in TESS.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Full 2.0–5.27 μm NIRSpec/IFU spectrum of TWA 28 (purple), TWA 27A (dark blue), and TWA 27B (light blue), from top to bottom, respectively, at their original resolution of R ∼ 2700. We indicate the atomic absorption lines, emission lines, and molecular bands we expect for these objects.
Paper: Medium-resolution 0.97–5.3 μm Spectra of Very Young Benchmark Brown Dwarfs with NIRSpec on Board the James Webb Space Telescope
Authors: Elena Manjavacas, Pascal Tremblin, Stephan Birkmann, Jeff Valenti, Catarina Alves de Oliveira, Tracy L. Beck, G. Giardino, N. Lützgendorf, B. J. Rauscher, M. Sirianni
Figure caption: Best fit of the ATMO and BT-Settl CIFIST models to the TWA 28 0.97–2.0 μm spectrum. We highlight the main atomic lines and molecular absorptions present in this wavelength range.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: Identification chart of NGC 2345 of size 15 × 15 arcmin2 taken from the DSS and oriented in the northeast direction (north is up and east is left). The inner circle represents the core radius (3.′9), while the outer ring denotes the cluster radius (12.′8).
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: Plot of proper motions and their associated errors vs. G magnitude. The red empty circle symbols represents stars having membership probability ≥70%, and the black circle shows the field stars.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: The V/(B − V) color–magnitude and (U − B)/(B − V) color–color diagrams of the cluster NGC 2345. A total of 426 stars observed in the present analysis are used for these diagrams.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: Photometric errors in different filters against V magnitude.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: This figure shows the initial cluster member separation method using Gaia proper motions for the cluster. The top panel shows the vector point diagram and the bottom panels show the respective Gaia color–magnitude diagrams for the total stars, cluster members, and field stars. In the top panel, we have drawn a circle with a radius of 0.5 mas yr−1 inside the cluster field, representing the member stars.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: A zoomed-in view of the proper-motion distribution of stars within a red circular area with a radius of 0.5 mas yr−1. The plus sign denotes the proper-motion center.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: The radial density profile for the cluster. The best-fit blue curve represents the King (1962) profile, from which we obtained both the core (r  c  ) and the tidal (r  t  ) radius. Their positions are indicated with vertical dashed lines. The horizontal lines represent the stars’ background density and the corresponding errors.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: The Gaia membership probability is plotted as a function of G magnitude, with cluster members indicated by red empty circles with membership probability higher than 70%. The distribution of stars in the CMD is shown in the right panel.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: The (V − λ)/(B − V) diagrams for member stars in the cluster NGC 2345. The continuous lines represent the slope determined through the least-squares linear fit and are mentioned in each panel.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: The blue dots on the graph represent the differences between our photometry and that of Alonso-Santiago et al. against V magnitude. The dotted line indicates zero difference.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: Differences between measurements presented in the APASS catalog and this study for V magnitude and (B − V) colors. The dotted line on the plot represents zero difference.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: The (U − B) vs. (B − V) color–color diagram for NGC 2345. We have used only cluster members with membership probability higher than 70%. The arrow indicates the reddening vector.
Paper: Exploring NGC 2345: A Comprehensive Study of a Young Open Cluster through Photometric and Kinematic Analysis
Authors: Kuldeep Belwal, D. Bisht, Mohit Singh Bisht, Geeta Rangwal, Ashish Raj, Arvind K. Dattatrey, R. K. S. Yadav, B. C. Bhatt
Figure caption: Stellar count profiles across the cluster region have been analyzed using Gaussian fits. The center of symmetry about the peaks of R.A. and decl. is the position of the cluster's center.