adsabs/AstroCLIMB huggingface dataset:
Paper: JWST-TST High Contrast: Asymmetries, Dust Populations, and Hints of a Collision in the β Pictoris Disk with NIRCam and MIRI
Authors: Isabel Rebollido, Christopher C. Stark, Jens Kammerer, Marshall D. Perrin, Kellen Lawson, Laurent Pueyo, Christine Chen, Dean Hines, Julien H. Girard, Kadin Worthen, Carl Ingerbretsen, Sarah Betti, Mark Clampin, David Golimowski, Kielan Hoch, Nikole K. Lewis, Cicero X. Lu, Roeland P. van der Marel, Emily Rickman, Sara Seager, Rémi Soummer, Jeff A. Valenti, Kimberly Ward-Duong, C. Matt Mountain
Figure caption: Contrast SED for thermal and scattered light on both sides of the disk. The data points have been obtained as explained in Section 4.1. Different colors and symbols refer to different positions on the disk, as labeled. The data below 2 μm, corresponding with NIRCam data, show a decrease in the scattered light contrast; while at 15.5 and 23 μm, corresponding with MIRI data, they show how the thermal emission picks up as the brightness from the star decreases.
Paper: A 3D Parametric Venusian Bow Shock Model with the Effects of Mach Number and Interplanetary Magnetic Field
Authors: Ming Wang, Qi Xu, Lianghai Xie, Lei Li, Xiaojun Xu
Figure caption: The dependence of the bow shock parameters x 0 (squares in panel (a)), e 0 (circles in panel (b)), e 1 (up triangles, panel (c)), e 2 (down triangles, panel (c)), e 3 (right triangles in panel (c)), and ω (diamonds in panel (d)) on the magnetosonic Mach number M MS (panel (1)), IMF intensity (panel (2)), IMF cone angle μ  XY  (panel (3)), and IMF clock angle λ (panel (4)). The magnetosonic Mach number effects are plotted from Case 1 to 40 in the supplementary document, the IMF intensity effect shows Case 41–64 (In Case 41–48 B  t  varies with B  X  and B  Y  when B  Z  = 0, in Case 49–56 B  X  changes when B  Y  = B  Z  = 0, and B  Y  varies in Case 57–64 when B  X  = B  Z  = 0), the IMF cone angle effect displays Case 65–74, the IMF clock angle effect is from Case 75–86. Symbols show the results of MHD simulations and the lines are the potential fits.
Paper: A 3D Parametric Venusian Bow Shock Model with the Effects of Mach Number and Interplanetary Magnetic Field
Authors: Ming Wang, Qi Xu, Lianghai Xie, Lei Li, Xiaojun Xu
Figure caption: Model results of the solar wind magnetosonic Mach number M MS, IMF component B  X , B  Y  and IMF clock angle λ on the shape and size of the Venusian bow shock. (a1)–(c1) M MS varies from 3.0 to 8.6 with the IMF condition of B  X  = 3.6 nT, B  Y  = −5.4 nT, and B  Z  = 0 nT. (a2)–(c2) B  X  varies from 3 to 11 with B  Y  = −7 nT, B  Z  = 0 nT. (a3)–(c3) B  Y  varies from −2.5 to −20 with B  X  = 5 nT, B  Z  = 0 nT. (a4)–(c4) B  Y  varies from −15° to −75° with B  X  = 0 nT. The n = 9 cm−3 and v = −400 km s−1 is unchanged for (a2)–(c4).
Paper: A 3D Parametric Venusian Bow Shock Model with the Effects of Mach Number and Interplanetary Magnetic Field
Authors: Ming Wang, Qi Xu, Lianghai Xie, Lei Li, Xiaojun Xu
Figure caption: Comparison of our parametric Venusian bow shock model with existing empirical models for solar maximum and solar minimum conditions (a) and (b). The solar wind conditions is set to be n = 17.0 cm−3, U  X  = −400.0 km s−1 and B = 12.1 nT at solar maximum (Xu et al. 2022), and n = 6.9 cm−3, U  X  = −384.0 km s−1 and B = 6.5 nT at solar minimum (Xu et al. 2023). The IMF Parker spiral angle is considered as 42° near Venus (Chang et al. 2019). Black solid lines and red dashed lines represent our parametric model results on the X–Y and X–Z planes. The results of Slavin et al. (1980), Russell et al. (1988), Zhang et al. (1990), Zhang et al. (2008a), Martinecz et al. (2009), Chai et al. (2014), Shan et al. (2015), and Signoles et al. (2023) are shown, respectively.
Paper: A 3D Parametric Venusian Bow Shock Model with the Effects of Mach Number and Interplanetary Magnetic Field
Authors: Ming Wang, Qi Xu, Lianghai Xie, Lei Li, Xiaojun Xu
Figure caption: Example of identified locations of the Venusian bow shock from simulation data on 3D (panel (a)), Y–Z plane (panel (b)), X–Y plane (panel (c)), and X–Z plane (panel (d)) in the VSO coordinate system. The solar wind conditions for this example are n = 6.0 cm−3, U  X  = −400.0 km s−1, B  X  = 3.6 nT, B  Y  = −5.4 nT, and B  Z  = 0 nT. The color code is the solar wind density (cm−3) in Figure (b), (c), and (d).
Paper: A 3D Parametric Venusian Bow Shock Model with the Effects of Mach Number and Interplanetary Magnetic Field
Authors: Ming Wang, Qi Xu, Lianghai Xie, Lei Li, Xiaojun Xu
Figure caption:  R 2 model (a) and RMSE (b) associated with the identified locations of bow shock from simulations and the final model functions (Equations (3)–(10) and Table 2) for all the 110 cases. The black dashed lines represent the average values.
Paper: A 3D Parametric Venusian Bow Shock Model with the Effects of Mach Number and Interplanetary Magnetic Field
Authors: Ming Wang, Qi Xu, Lianghai Xie, Lei Li, Xiaojun Xu
Figure caption: Solar activity effect on the geometry of the bow shock. Parameter x 0-solarmax is the subsolar standoff distance under the solar maximum condition in Case 87–110, and x 0-solarmin is the subsolar standoff distance under the same solar wind condition as that of Case 87–110 but for solar minimum condition. Parameters e 0-solarmin and e 0-solarmax are the flaring degree under the corresponding conditions.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: The Allan variance plot from the white light-curve fits to each pipeline’s reduction and for all three visits. The amplitude of the residuals from Tiberius (blue), Eureka! (orange), and Tswift (green) are shown as a function of bin size in minutes. In the absence of red noise, the residuals would follow the dashed black line.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: Light-curve residual rms (upper panel) and transit depth uncertainties (lower panel) for each reduction (color lines). The expected noise (photon + read noise + dark current) calculated from the data is shown in the upper panel (black line), and the median rms relative to the expected noise is listed in the legend for each reduction. The predicted noise from PandExo (Batalha et al. 2017) is shown in the lower panel (black line).
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: The improvement in residual red noise in the white light curves by adding an additional mnemonic/telemetry time series to the systematics model. The blue, orange, and green lines indicate the residuals from the white light curves of visits 1, 2, and 3. The fiducial model is a linear-in-time polynomial. Each x-tick label indicates an additional mnemonic is added. The dashed gray line indicates the white-noise level that the residual noise would achieve if no red noise is present.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: The light curves and best-fit models resulting from the Eureka! pipeline. The columns show, from left to right: transit 1, transit 2, and transit 3. The rows show, from top to bottom: (1) the white light curve and residuals, (2) the spectroscopic light curves, (3) the best-fit models to the spectroscopic light curves, (4) the residuals from the spectroscopic light-curve fitting.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: GJ 341b’s transmission spectrum as measured by Tiberius (blue), Eureka! (orange), and Tswift (green). These spectra are the the weighted means of the three visits’ spectra. The Eureka! spectrum has been offset by −15 ppm to make the median transit depths equal to Tiberius and Tswift between 4.0 and 4.8 μm.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: A comparison between our measured flux-calibrated spectra (black) and superpositions of PHOENIX stellar atmosphere models: photosphere with no active region contribution (purple), photosphere with contribution from spots (orange), and photosphere with contributions from spots and faculae (green). Given the poor ﹩{\chi }_{\nu }^{2}﹩, and lack of contamination evident in our transmission spectra, we do interpret these model results as evidence for stellar contamination in our data.
Paper: JWST/NIRCam Transmission Spectroscopy of the Nearby Sub-Earth GJ 341b
Authors: James Kirk, Kevin B. Stevenson, Guangwei Fu, Jacob Lustig-Yaeger, Sarah E. Moran, Sarah Peacock, Munazza K. Alam, Natasha E. Batalha, Katherine A. Bennett, Junellie Gonzalez-Quiles, Mercedes López-Morales, Joshua D. Lothringer, Ryan J. MacDonald, E. M. May, L. C. Mayorga, Zafar Rustamkulov, David K. Sing, Kristin S. Sotzen, Jeff A. Valenti, Hannah R. Wakeford
Figure caption: The short-wavelength photometric light curves for each visit, revealing significant pre-transit noise (visit 2) and in-transit noise (visit 3). These have been smoothed with a running median calculated over a sliding box with a width of 51 integrations. The dashed vertical lines indicate the first and fourth contact points of the transit.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XI. An Earth-sized Planet Orbiting a Nearby, Solar-like Host in the 400 Myr Ursa Major Moving Group
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Alyssa Jankowski, Andrew W. Mann, Gabrielle Ross, Gregor Srdoc, Natalie R. Hinkel, Juliette Becker, Christian Magliano, Mary Anne Limbach, Alexander P. Stephan, Andrew C. Nine, Benjamin M. Tofflemire, Adam L. Kraus, Steven Giacalone, Joshua N. Winn, Allyson Bieryla, Luke G. Bouma, David R. Ciardi, Karen A. Collins, Giovanni Covone, Zoë L. de Beurs, Chelsea X. Huang, Jon M. Jenkins, Laura Kreidberg, David W. Latham, Samuel N. Quinn, Sara Seager, Avi Shporer, Joseph D. Twicken, Bill Wohler, Roland K. Vanderspek, Ricardo Yarza, Carl Ziegler
Figure caption: The color–rotation sequence for catalog members of the UMa moving group, as compared to the 120 Myr Pleiades (Rebull et al. 2016) cluster and the 670 Myr Praesepe cluster (Douglas et al. 2017). Circles indicate UMa sources with RUWE <1.2, while squares indicate those with RUWE ≥1.2. Our target HD 63433 is shown as a gold star. Light blue circles/squares denote UMa sources featured in Mann et al. (2020)—those shown with an “x” symbol overplotted lack Gaia DR3 reddening values required for absolute calibration. We identify the spectral types investigated, adding shaded panels that correspond to the hexadecimal color codes for a given spectral type (luminosity class V, subclass 5), as reported by Harre & Heller (2021).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XI. An Earth-sized Planet Orbiting a Nearby, Solar-like Host in the 400 Myr Ursa Major Moving Group
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Alyssa Jankowski, Andrew W. Mann, Gabrielle Ross, Gregor Srdoc, Natalie R. Hinkel, Juliette Becker, Christian Magliano, Mary Anne Limbach, Alexander P. Stephan, Andrew C. Nine, Benjamin M. Tofflemire, Adam L. Kraus, Steven Giacalone, Joshua N. Winn, Allyson Bieryla, Luke G. Bouma, David R. Ciardi, Karen A. Collins, Giovanni Covone, Zoë L. de Beurs, Chelsea X. Huang, Jon M. Jenkins, Laura Kreidberg, David W. Latham, Samuel N. Quinn, Sara Seager, Avi Shporer, Joseph D. Twicken, Bill Wohler, Roland K. Vanderspek, Ricardo Yarza, Carl Ziegler
Figure caption: Color–A(Li) sequence of our cataloged UMa members (crimson circles/squares) with HD 63433 depicted as a gold star. Same legend definitions as Figure 2. Twelve sources in our catalog had published A(Li) abundances. The solar system meteoritic abundance level of 3.3 dex is depicted as a horizontal dashed line (Asplund et al. 2009). To indicate the range in stellar types, we illustrate the hexadecimal color codes reported by Harre & Heller (2021; luminosity class V, subclass 5). The color–A(Li) relation for the 120 Myr Pleiades cluster (Bouvier et al. 2018) and the 670 Myr Praesepe cluster (Cummings et al. 2017) are shown as a comparison. A/F-type stars in all three systems show evidence of the well-known lithium dip feature (Boesgaard & Tripicco 1986).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XI. An Earth-sized Planet Orbiting a Nearby, Solar-like Host in the 400 Myr Ursa Major Moving Group
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Alyssa Jankowski, Andrew W. Mann, Gabrielle Ross, Gregor Srdoc, Natalie R. Hinkel, Juliette Becker, Christian Magliano, Mary Anne Limbach, Alexander P. Stephan, Andrew C. Nine, Benjamin M. Tofflemire, Adam L. Kraus, Steven Giacalone, Joshua N. Winn, Allyson Bieryla, Luke G. Bouma, David R. Ciardi, Karen A. Collins, Giovanni Covone, Zoë L. de Beurs, Chelsea X. Huang, Jon M. Jenkins, Laura Kreidberg, David W. Latham, Samuel N. Quinn, Sara Seager, Avi Shporer, Joseph D. Twicken, Bill Wohler, Roland K. Vanderspek, Ricardo Yarza, Carl Ziegler
Figure caption: Color–magnitude diagram of HD 63433 (gold star) and our catalog of UMa comoving members (crimson circles/squares). Same legend definitions as Figure 2. In black, we illustrate a PAdova and TRieste Stellar Evolution Code (PARSEC) isochrone (version 1.2S) for a 400 Myr system with [M/H] = 0.02 dex (Bressan et al. 2012). We identify the spectral types investigated, adding shaded panels that correspond to the hexadecimal color codes for a given spectral type (luminosity class V, subclass 5), as reported by Harre & Heller (2021).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XI. An Earth-sized Planet Orbiting a Nearby, Solar-like Host in the 400 Myr Ursa Major Moving Group
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Alyssa Jankowski, Andrew W. Mann, Gabrielle Ross, Gregor Srdoc, Natalie R. Hinkel, Juliette Becker, Christian Magliano, Mary Anne Limbach, Alexander P. Stephan, Andrew C. Nine, Benjamin M. Tofflemire, Adam L. Kraus, Steven Giacalone, Joshua N. Winn, Allyson Bieryla, Luke G. Bouma, David R. Ciardi, Karen A. Collins, Giovanni Covone, Zoë L. de Beurs, Chelsea X. Huang, Jon M. Jenkins, Laura Kreidberg, David W. Latham, Samuel N. Quinn, Sara Seager, Avi Shporer, Joseph D. Twicken, Bill Wohler, Roland K. Vanderspek, Ricardo Yarza, Carl Ziegler
Figure caption: The top panel shows the unflattened TESS light curve of HD 63433. The middle panel shows the flattened light curve with our three best-fit transit models for planets b, c, and d, as determined by our edmcmc outputs. The colors of these models correspond to each of the three planets as shown in the bottom panels, which depict the phase-folded light curves for each HD 63433 planet with binned data (red points) plotted over our best-fit models.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XI. An Earth-sized Planet Orbiting a Nearby, Solar-like Host in the 400 Myr Ursa Major Moving Group
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Alyssa Jankowski, Andrew W. Mann, Gabrielle Ross, Gregor Srdoc, Natalie R. Hinkel, Juliette Becker, Christian Magliano, Mary Anne Limbach, Alexander P. Stephan, Andrew C. Nine, Benjamin M. Tofflemire, Adam L. Kraus, Steven Giacalone, Joshua N. Winn, Allyson Bieryla, Luke G. Bouma, David R. Ciardi, Karen A. Collins, Giovanni Covone, Zoë L. de Beurs, Chelsea X. Huang, Jon M. Jenkins, Laura Kreidberg, David W. Latham, Samuel N. Quinn, Sara Seager, Avi Shporer, Joseph D. Twicken, Bill Wohler, Roland K. Vanderspek, Ricardo Yarza, Carl Ziegler
Figure caption: Planet radius vs. orbital period for confirmed exoplanets (gray circles), confirmed exoplanets with reliable age estimates that are <500 Myr (blue pentagons), and the three HD 63433 planets (b, red star; c, orange star; and d, yellow star). Note that there are few detections of young, Earth-sized planets. Those detected are in short-period orbits about their stellar hosts. For enhanced readability of the figure, we omit exoplanets detected via the direct imaging method, as their orbital separations are much larger.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XI. An Earth-sized Planet Orbiting a Nearby, Solar-like Host in the 400 Myr Ursa Major Moving Group
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Alyssa Jankowski, Andrew W. Mann, Gabrielle Ross, Gregor Srdoc, Natalie R. Hinkel, Juliette Becker, Christian Magliano, Mary Anne Limbach, Alexander P. Stephan, Andrew C. Nine, Benjamin M. Tofflemire, Adam L. Kraus, Steven Giacalone, Joshua N. Winn, Allyson Bieryla, Luke G. Bouma, David R. Ciardi, Karen A. Collins, Giovanni Covone, Zoë L. de Beurs, Chelsea X. Huang, Jon M. Jenkins, Laura Kreidberg, David W. Latham, Samuel N. Quinn, Sara Seager, Avi Shporer, Joseph D. Twicken, Bill Wohler, Roland K. Vanderspek, Ricardo Yarza, Carl Ziegler
Figure caption: Contrast curves obtained from Keck/NIRC2 high-contrast observations (black line; Br-γ filter) and VLT observations (red line; K filter). The 5σ contrast limits for secondary sources are plotted against angular separation.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). XI. An Earth-sized Planet Orbiting a Nearby, Solar-like Host in the 400 Myr Ursa Major Moving Group
Authors: Benjamin K. Capistrant, Melinda Soares-Furtado, Andrew Vanderburg, Alyssa Jankowski, Andrew W. Mann, Gabrielle Ross, Gregor Srdoc, Natalie R. Hinkel, Juliette Becker, Christian Magliano, Mary Anne Limbach, Alexander P. Stephan, Andrew C. Nine, Benjamin M. Tofflemire, Adam L. Kraus, Steven Giacalone, Joshua N. Winn, Allyson Bieryla, Luke G. Bouma, David R. Ciardi, Karen A. Collins, Giovanni Covone, Zoë L. de Beurs, Chelsea X. Huang, Jon M. Jenkins, Laura Kreidberg, David W. Latham, Samuel N. Quinn, Sara Seager, Avi Shporer, Joseph D. Twicken, Bill Wohler, Roland K. Vanderspek, Ricardo Yarza, Carl Ziegler
Figure caption: Distance from Earth vs. planet radius for confirmed exoplanets (gray circles), confirmed exoplanets with reliable age estimates that are <500 Myr (blue pentagons), and the three HD 63433 planets (b, red star; c, orange star; and d, yellow star). Note that HD 63433 d is the nearest, young, Earth-sized exoplanet discovered to date.
Paper: Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316
Authors: Saurabh Sharma, Aayushi Verma, Kshitiz Mallick, Lokesh K. Dewangan, Harmeen Kaur, Ram Kesh Yadav, Neelam Panwar, Devendra K. Ojha, Tarak Chand, Mamta Agarwal
Figure caption: Panel (a): WISE 12  μm MIR image for an area of  ∼ 20 × 20 arcmin2 around the NGC 2316 cluster. The black square represents the FOV of the present observations using an optical imager on 3.6 m DOT for the NGC 2316 cluster. The red contours are the isodensity contours generated using the nearest neighbor method from the near-infrared photometric data (see Section 3.1). Panels (b), (c): Color-composite images obtained by using the J (blue), H (green), and K (red) images taken from UKIDSS (top panel), and the V (blue), R (green), and I (red) images taken from the present optical observations (bottom panel). The red polygon is the convex hull representing the cluster area generated on the outermost stellar isodensity contour (see Section 3.1).
Paper: Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316
Authors: Saurabh Sharma, Aayushi Verma, Kshitiz Mallick, Lokesh K. Dewangan, Harmeen Kaur, Ram Kesh Yadav, Neelam Panwar, Devendra K. Ojha, Tarak Chand, Mamta Agarwal
Figure caption: Left panel: (U − B) vs. (B − V) TCD for the sources in the NGC 2316 cluster region (stars within the convex hull, black dots). The solid blue and dotted red curves represent the intrinsic ZAMS for Z = 0.02 given by Pecaut & Mamajek (2013) which shifted along the reddening vector for E(B − V)  = 0.5 mag and E(B − V)  = 1.3 mag, respectively. Right panel: V vs. (V − I  c ) CMD for the stars inside the NGC 2316 cluster region (black dots). The blue solid curve represents the ZAMS corrected for the distance 1.3 kpc and reddening E(B − V)  =  0.5 mag. The candidate massive stars, young stellar objects (Class II), and Gaia DR3 members are shown in both panels by blue circles, red triangles, and square boxes, respectively.
Paper: Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316
Authors: Saurabh Sharma, Aayushi Verma, Kshitiz Mallick, Lokesh K. Dewangan, Harmeen Kaur, Ram Kesh Yadav, Neelam Panwar, Devendra K. Ojha, Tarak Chand, Mamta Agarwal
Figure caption: Panel (a): Stellar density map derived from the NIR catalog. Panel (b): NIR color-composite image (Red: Spitzer 4.5 μm; Green: Spitzer 3.6 μm; Blue: 2MASS K 2.17 μm). Panel (c): FIR color-composite image (Red: Hershel 500 μm; Green: Hershel 350 μm; Blue: Hershel 250 μm) overlaid with the locations of Class I (cyan circles asterisk) and Class II (green circles) YSOs. Panel (d): YSOs density map. The shown FOV is ﹩{21}^{{\prime} }\,\times \,{21}^{{\prime} }﹩ of the NGC 2316 region, and all panels are overlaid with the NGC 2316 cluster region, i.e., Convex hull (red polygon).
Paper: Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316
Authors: Saurabh Sharma, Aayushi Verma, Kshitiz Mallick, Lokesh K. Dewangan, Harmeen Kaur, Ram Kesh Yadav, Neelam Panwar, Devendra K. Ojha, Tarak Chand, Mamta Agarwal
Figure caption:  J vs. (J − H) TCD for the sources in the NGC 2316 cluster region (stars within the convex hull). The blue curve represents the intrinsic ZAMS for Z = 0.02 given by Pecaut & Mamajek (2013) scaled for E(B − V) = 0.5 mag and distance of 1.3 kpc. Symbols are the same as in Figure 3. Asterisks are Class I YSOs.
Paper: Cluster Formation in a Filamentary Cloud: The Case of the Stellar Cluster NGC 2316
Authors: Saurabh Sharma, Aayushi Verma, Kshitiz Mallick, Lokesh K. Dewangan, Harmeen Kaur, Ram Kesh Yadav, Neelam Panwar, Devendra K. Ojha, Tarak Chand, Mamta Agarwal
Figure caption: Photometric error vs. magnitude plots in V, and I  c  filters.