adsabs/AstroCLIMB huggingface dataset:
Paper: Gaia22dkvLb: A Microlensing Planet Potentially Accessible to Radial-velocity Characterization
Authors: Zexuan Wu, Subo Dong, Tuan Yi, Zhuokai Liu, Kareem El-Badry, Andrew Gould, L. Wyrzykowski, K. A. Rybicki, Etienne Bachelet, Grant W. Christie, L. de Almeida, L. A. G. Monard, J. McCormick, Tim Natusch, P. Zieliński, Huiling Chen, Yang Huang, Chang Liu, A. Mérand, Przemek Mróz, Jinyi Shangguan, Andrzej Udalski, J. Woillez, Huawei Zhang, Franz-Josef Hambsch, P. J. Mikołajczyk, M. Gromadzki, M. Ratajczak, Katarzyna Kruszyńska, N. Ihanec, Uliana Pylypenko, M. Sitek, K. Howil, Staszek Zola, Olga Michniewicz, Michal Zejmo, Fraser Lewis, Mateusz Bronikowski, Stephen Potter, Jan Andrzejewski, Jaroslav Merc, Rachel Street, Akihiko Fukui, R. Figuera Jaimes, V. Bozza, P. Rota, A. Cassan, M. Dominik, Y. Tsapras, M. Hundertmark, J. Wambsganss, K. Bąkowska, A. Słowikowska
Figure caption: Posteriors of astrometric lensing model parameters from MCMC sampling. The red, yellow, green, and blue areas represent Δχ 2 within 1, 4, 9, and 16 of the best fit. The model parameters with light-curve priors, i.e., (t 0, u 0, t E, f B/f S), are not shown.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: IR pseudocolor images of possible outflow or jet components within Cloud 1b main cluster (top) and Cloud 2S main cluster (bottom). The left panels are the images from previous observations (top: WISE with w2, w3, and w4 bands; bottom: Spitzer with IRAC ch1, ch2, and ch4 bands). The right panels are the new JWST images (top: F770W, F1280W, and F2100W filters; bottom: F356W, F444W, and F770 filters). The displayed area of Cloud 1b and Cloud 2S corresponds to the white dashed square labeled (b) in Figure 4 and (a) in Figure 6, respectively. The white arrows indicate the positions of the possible outflow or jet components. The white dotted rectangles mark the areas shown in Figures 12 (Cloud 1b) and 13 (Cloud 2N).
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: CM diagrams for all detected sources. Red triangles, yellow triangles, magenta squares, and orange squares indicate the cluster members within Cloud 1a, Cloud 1b, Cloud 2N, and Cloud 2S, respectively. These cluster members were identified in Subaru data (Yasui et al. 2009; Izumi et al. 2014). The black dots indicate all sources. The black arrows in panels (a), (b), and (c) show the redding vectors of A V = 5 mag (Wang & Chen 2019). The blue solid and dashed lines represent models for pre-main-sequence stars (isochrone model) by Baraffe et al. (2015) at ages of 0.5 Myr and 1.0 Myr, respectively, with a distance of 12 kpc. Similarly, the green solid and dashed lines depict models for pre-main-sequence stars (isochrone model) by Baraffe et al. (2015) at ages of 0.5 Myr and 1.0 Myr, respectively, but with a distance of 16 kpc. The blue stars indicate the very young source candidates. The black dotted lines indicate the threshold between cluster members and other sources in longer-wavelength colors with the criteria: F356W – F770W = 1.0 (d), F444W – F1280W = 1.5 (e), and F444W – F2100W = 2.0 (f).
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: Top: overall IR (2.00, 3.56, and 4.44 μm) pseudocolor image of Digel Cloud 1a from NIRCam. Bottom: overall IR (7.7, 12.8, and 21.0 μm) pseudocolor image of Digel Cloud 1a from MIRI. The white dotted squares indicate the notable structures: (a) main cluster and (b), (c) isolated reddened single sources. The physical scale (∼0.78 pc) at the scale bars in both panels is calculated assuming that the distance to Digel Cloud 1 is 16 kpc.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: Top: overall IR (2.00, 3.56, and 4.44 μm) pseudocolor image of Digel Cloud 2N from NIRCam. Bottom: overall IR (7.7, 12.8, and 21.0 μm) pseudocolor image of Digel Cloud 2N from MIRI. The white dotted squares indicate the notable structures: (a) main cluster and (b) subcluster. The physical scale (∼0.58 pc) at the scale bars in both panels is calculated assuming that the distance to Digel Cloud 2 is 12 kpc.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: Top: overall IR (2.00, 3.56, and 4.44 μm) pseudocolor image of Digel Cloud 2S from NIRCam. Bottom: overall IR (7.7, 12.8, and 21.0 μm) pseudocolor image of Digel Cloud 2S from MIRI. The white dotted squares indicate the notable structures: (a) main cluster and (b) subcluster. The physical scale (∼0.58 pc) at the scale bars in both panels is calculated assuming that the distance to Digel Cloud 2 is 12 kpc.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: Overall IR (7.7, 12.8, and 21.0 μm) pseudocolor image of Digel Cloud 1b from MIRI. The white dotted squares indicate the notable structures: (a) main cluster and (b) candidates of outflow/jet components. The physical scale (∼0.78 pc) at the scale bars in both panels is calculated assuming that the distance to Digel Cloud 1 is 16 kpc.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: Color–color diagrams for all detected sources. Red triangles, magenta squares, and orange squares indicate the cluster members within Cloud 1a, Cloud 2N, and Cloud 2S, respectively. These cluster members were identified in Subaru data (Yasui et al. 2009; Izumi et al. 2014). The black dots indicate all sources. The cyan crosses are the jet/outflow structures. The blue stars are the very young source candidates. The black dotted lines indicate the WISE color criteria for class 0 protostars from Fischer et al. (2016).
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: IR pseudocolor image of clusters ((a): Cloud 1a, (b): Cloud 2N, (c): Cloud 2S) detected by Subaru (left: J, H, and K bands) and JWST (right: F115W, F150W, and F200W filters). The displayed area of Cloud 1a and Cloud 2N corresponds to the white dashed square labeled (a) in Figures 3 and 5, respectively. The displayed area of cloud 2S is within the area of the white dashed square labeled (a) in Figure 6.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: NIRCam and MIRI images of candidates of very young sources in Cloud 1a (top) and Cloud 2N (bottom). Black arrows indicate the positions of the candidates. The displayed area of Cloud 1a and Cloud 2N corresponds to the white dashed square labeled (c) in Figures 3 and 5, respectively.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: All MIRI monochromatic images of DC 2S.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: IR pseudocolor images of nebular structures in Cloud 2N (top) and 2S (bottom). The left panels are the images from previous Spitzer observations (IRAC ch1, ch2, and ch4 bands). The right panels are the new JWST images (F356W, F444W, and F770 filters). The cyan dashed contours show the integrated 12CO(1–0) map of Digel Cloud 2 from our NRO 45 m data (V LSR = −106.1–99.1 km s−1; Izumi et al. 2017), with contour levels at 3σ, 5σ, 7σ, 9σ, and 11σ, where 1σ = 1.35 K km s−1 (same as in the bottom-right panel in Figure 2). The color bar located in the top right indicates the contour level. The white circle at the lower left corner in the top-right panel shows the beam size of the NRO 45 m (∼17″).
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: NIRCam and MIRI images with F200W (a), F356W (b), F444W (c), F770W (d), and F1280W (e) for two representative possible outflow or jet components within the Cloud 2S main cluster (white dotted rectangle in the bottom-right panel of Figure 11). Panel (f) shows the comparison between F444W (white contours) and F1280W (background) filters. The contours indicate 3σ, 9σ, and 15σ where 1σ is 0.025 MJy sr−1. The width of the contours increases with the contour level.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: MIRI images with F770W (a) and F1280W (b) filters for possible outflow or jet components within the Cloud 1b main cluster (white dotted rectangle in the top-right panel of Figure 11). The panel (c) shows the comparison between F770W (white contours) and F1280W (background) filters. The contours indicate 3σ, 5σ, and 7σ where 1σ is 0.15 MJy sr−1. The width of the contours increases with the contour level.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: All NIRCam monochromatic images of DC 1a.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: All NIRCam monochromatic images of DC 2N.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: All MIRI monochromatic images of DC 1a.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: All MIRI monochromatic images of DC 2N.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: All NIRCam monochromatic images of DC 2S.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: All MIRI monochromatic images of DC 1b.
Paper: LIGHTS. Survey Overview and a Search for Low Surface Brightness Satellite Galaxies
Authors: Dennis Zaritsky, Giulia Golini, Richard Donnerstein, Ignacio Trujillo, Mohammad Akhlaghi, Nushkia Chamba, Mauro D'Onofrio, Sepideh Eskandarlou, S. Zahra Hosseini-ShahiSavandi, Raúl Infante-Sainz, Garreth Martin, Mireia Montes, Javier Román, Nafise Sedighi, Zahra Sharbaf
Figure caption: Comparison of properties of LIGHTS LSB satellites, open red circles, and a combination of data from the literature in filled gray circles. In the left panels, the literature sample consists of data from ELVES (S.G. Carlsten et al. 2022) and KMTNet (H. S. Park et al. 2017, 2019), while in the right panels, the literature data come from MATLAS (M. Poulain et al. 2021).
Paper: LIGHTS. Survey Overview and a Search for Low Surface Brightness Satellite Galaxies
Authors: Dennis Zaritsky, Giulia Golini, Richard Donnerstein, Ignacio Trujillo, Mohammad Akhlaghi, Nushkia Chamba, Mauro D'Onofrio, Sepideh Eskandarlou, S. Zahra Hosseini-ShahiSavandi, Raúl Infante-Sainz, Garreth Martin, Mireia Montes, Javier Román, Nafise Sedighi, Zahra Sharbaf
Figure caption: The distribution of target galaxies as a function of low surface brightness satellite count (not corrected for completeness). Solid line is a Poisson distribution with mean 54/25 that integrates to 25 systems. The error bars represent ﹩\sqrt{N}﹩ uncertainties only. The dotted line revisits the Poisson fit if we exclude systems with >5 satellites. The mean in this case is 1.4 LSB identified satellite candidates per host.
Paper: LIGHTS. Survey Overview and a Search for Low Surface Brightness Satellite Galaxies
Authors: Dennis Zaritsky, Giulia Golini, Richard Donnerstein, Ignacio Trujillo, Mohammad Akhlaghi, Nushkia Chamba, Mauro D'Onofrio, Sepideh Eskandarlou, S. Zahra Hosseini-ShahiSavandi, Raúl Infante-Sainz, Garreth Martin, Mireia Montes, Javier Román, Nafise Sedighi, Zahra Sharbaf
Figure caption: Distribution in satellite properties. Those galaxies also in the SMUDGes catalog (D. Zaritsky et al. 2023) are highlighted with larger, light red circles. Vertical lines in the first column of panels mark the SMUDGes minimum angular size criterion. The vertical lines in the middle panels mark the minimum physical size that defines the UDG category.
Paper: LIGHTS. Survey Overview and a Search for Low Surface Brightness Satellite Galaxies
Authors: Dennis Zaritsky, Giulia Golini, Richard Donnerstein, Ignacio Trujillo, Mohammad Akhlaghi, Nushkia Chamba, Mauro D'Onofrio, Sepideh Eskandarlou, S. Zahra Hosseini-ShahiSavandi, Raúl Infante-Sainz, Garreth Martin, Mireia Montes, Javier Román, Nafise Sedighi, Zahra Sharbaf
Figure caption: The 12 satellites galaxies identified visually to have nuclear star clusters. Square black regions indicate regions masked from the LIGHTS final images because they contain corrupted data. The images are ∼70″ on a side, and north is up.
Paper: LIGHTS. Survey Overview and a Search for Low Surface Brightness Satellite Galaxies
Authors: Dennis Zaritsky, Giulia Golini, Richard Donnerstein, Ignacio Trujillo, Mohammad Akhlaghi, Nushkia Chamba, Mauro D'Onofrio, Sepideh Eskandarlou, S. Zahra Hosseini-ShahiSavandi, Raúl Infante-Sainz, Garreth Martin, Mireia Montes, Javier Román, Nafise Sedighi, Zahra Sharbaf
Figure caption: Basic properties of the satellite sample. Histograms represent objects in our catalog. Light/narrower bars represent completeness-corrected values.
Paper: Unveiling MOA-2007-BLG-192: An M Dwarf Hosting a Likely Super-Earth
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Euan Hamdorf, Aparna Bhattacharya, Viveka Chaudhry, Andrew A. Cole, Naoki Koshimoto, Jay Anderson, Etienne Bachelet, Joshua W. Blackman, Ian A. Bond, Jessica R. Lu, Jean Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Kailash Sahu, Aikaterini Vandorou
Figure caption: The observed color–magnitude diagram (CMD) for the MB07192 field. The OGLE-III stars within 90″ of MB07192 are shown in black, with the HST CMD of all detected sources from the 2014 epoch shown in green. The red point indicates the location of the red clump centroid, and the purple and orange points show the source and lens colors and magnitudes from the 2014 HST observations. The blue point indicates the source star magnitude and color given by the original light-curve modeling.
Paper: Unveiling MOA-2007-BLG-192: An M Dwarf Hosting a Likely Super-Earth
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Euan Hamdorf, Aparna Bhattacharya, Viveka Chaudhry, Andrew A. Cole, Naoki Koshimoto, Jay Anderson, Etienne Bachelet, Joshua W. Blackman, Ian A. Bond, Jessica R. Lu, Jean Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Kailash Sahu, Aikaterini Vandorou
Figure caption: The probability distribution for the north and east components of lens–source relative proper motion (μ rel) using the Galactic model from Koshimoto et al. (2021) and genulens (Koshimoto & Ranc 2021). The possible lens positions (north and south) are plotted in black and given by the relative motion of the two stars detected in the HST and Keck data. Importantly, this distribution uses t E values that are close to the measured t E value from the light-curve modeling (t E ∼ 99.5 days). This implies that the “North star” is >2× more likely to be the lens than the “South star.”
Paper: Unveiling MOA-2007-BLG-192: An M Dwarf Hosting a Likely Super-Earth
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Euan Hamdorf, Aparna Bhattacharya, Viveka Chaudhry, Andrew A. Cole, Naoki Koshimoto, Jay Anderson, Etienne Bachelet, Joshua W. Blackman, Ian A. Bond, Jessica R. Lu, Jean Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Kailash Sahu, Aikaterini Vandorou
Figure caption: Top left: the coadded sum of 15 Keck-NIRC2 narrow-camera images, each with an exposure time of 60 s. The target is indicated with a square outline. Top right: zoomed image of the MB07192 blended source and lens stars. The magnitude of the separation in this epoch is 29.3 ± 1.1 mas. Bottom left: the residual image from a single-star PSF fit with DAOPHOT. A clear signal is seen due to the blended stellar profiles. Bottom right: the residual image for a simultaneous two-star PSF fit, showing a significantly improved subtraction. The color bar represents the pixel intensity (or counts) in the bottom panel residual images.
Paper: Unveiling MOA-2007-BLG-192: An M Dwarf Hosting a Likely Super-Earth
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Euan Hamdorf, Aparna Bhattacharya, Viveka Chaudhry, Andrew A. Cole, Naoki Koshimoto, Jay Anderson, Etienne Bachelet, Joshua W. Blackman, Ian A. Bond, Jessica R. Lu, Jean Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Kailash Sahu, Aikaterini Vandorou
Figure caption: Best-fit light curve with constraints from the high-resolution follow-up data as described in Section 3. The 2L1S model shown is from the second column of Table 6 with u 0 < 0 and s < 1. The y-axis is given in flux units which are normalized to the I  S  = 21.8 source star (e.g., “magnification”) from the modeling.
Paper: Unveiling MOA-2007-BLG-192: An M Dwarf Hosting a Likely Super-Earth
Authors: Sean K. Terry, Jean-Philippe Beaulieu, David P. Bennett, Euan Hamdorf, Aparna Bhattacharya, Viveka Chaudhry, Andrew A. Cole, Naoki Koshimoto, Jay Anderson, Etienne Bachelet, Joshua W. Blackman, Ian A. Bond, Jessica R. Lu, Jean Baptiste Marquette, Clément Ranc, Natalia E. Rektsini, Kailash Sahu, Aikaterini Vandorou
Figure caption: Similar to Figure 2, but for the 2014 HST data (eight exposures). The zoomed inset and residual image panels show 100 × 100 supersampled pixels where the observed dither offsets are accurate to 0.01 pixels. The color bar represents the pixel intensity (counts) seen in the top-right and lower-left/lower-right panels.
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: Ground-based time-series photometry observations of the transits of TOI-6029 b and TOI-4379 b. The light-green symbols show the unbinned data. The larger dark-green symbols show the data binned in 10-minute bins. The solid green line is the best-fit transit model. (a) Partial transit of TOI-6029 b observed by LCOGT on 2023 August 3. (b) Transit of TOI-4379 b observed by LCOGT on 2022 May 15. (c) Transit of TOI-4379 b observed by PEST on 2023 May 27.
Paper: TESS Giants Transiting Giants. VI. Newly Discovered Hot Jupiters Provide Evidence for Efficient Obliquity Damping after the Main Sequence
Authors: Nicholas Saunders, Samuel K. Grunblatt, Ashley Chontos, Fei Dai, Daniel Huber, Jingwen Zhang, 婧雯 张, Guđmundur Stefánsson, Jennifer L. van Saders, Joshua N. Winn, Daniel Hey, Andrew W. Howard, Benjamin Fulton, Howard Isaacson, Corey Beard, Steven Giacalone, Judah Van Zandt, Joseph M. Akana Murphey, Malena Rice, Sarah Blunt, Emma Turtelboom, Paul A. Dalba, Jack Lubin, Casey Brinkman, Emma M. Louden, Emma Page, Cristilyn N. Watkins, Karen A. Collins, Chris Stockdale, Thiam-Guan Tan, Richard P. Schwarz, Bob Massey, Steve B. Howell, Andrew Vanderburg, George R. Ricker, Jon M. Jenkins, Sara Seager, Jessie L. Christiansen, Tansu Daylan, Ben Falk, Max Brodheim, Steven R. Gibson, Grant M. Hill, Bradford Holden, Aaron Householder, Stephen Kaye, Russ R. Laher, Kyle Lanclos, Erik A. Petigura, Arpita Roy, Ryan A. Rubenzahl, Christian Schwab, Abby P. Shaum, Martin M. Sirk, Christopher L. Smith, Josh Walawender, Sherry Yeh
Figure caption: High-contrast image of TOI-6029 taken with the Keck/NIRC2 near-infrared imager in the Kp bandpass. The image has been corrected and derotated. The color bar indicates the measured flux.
Paper: Clusters, Clumps, Dust, and Gas (CCDG) in NGC 1614: Benchmarking Cluster Demographics in Extreme Systems
Authors: Miranda Caputo, Rupali Chandar, Angus Mok, Sean Linden, Paul Goudfrooij, Bradley C. Whitmore
Figure caption: HST image of NGC 1614, with B, V, and Hα represented by blue, green, and red, respectively. A variety of environments within this galaxy are highlighted, with the western UV-bright arm, eastern star-forming arm, and central region enlarged as shown. The yellow circle represents an aperture with a 2-pixel radius. The white circles show the 7- and 9-pixel radii used to determine the background level. The locations of the five most massive clusters younger than 400 Myr are shown as the magenta crosses in the two right panels.
Paper: Clusters, Clumps, Dust, and Gas (CCDG) in NGC 1614: Benchmarking Cluster Demographics in Extreme Systems
Authors: Miranda Caputo, Rupali Chandar, Angus Mok, Sean Linden, Paul Goudfrooij, Bradley C. Whitmore
Figure caption: Left: U-, I-, and H-band HST color image of NGC 1614, with new sources visible in the NIR (H band) but not in the optical (V band) circled in lime green. These were identified by eye. Right: B, V, I HST color image with optically detected clusters circled in cyan and new NIR-only clusters circled in lime green.