adsabs/AstroCLIMB huggingface dataset:
Paper: Resolved SPLASH Chemodynamics in Andromeda’s PHAT Stellar Halo and Disk: On the Nature of the Inner Halo along the Major Axis
Authors: Ivanna Escala, Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, J. Leigh Wojno, Lara Cullinane, Benjamin F. Williams, Julianne Dalcanton
Figure caption: The ratio between the BICs for the three-component and two-component velocity models for the line-of-sight velocity distribution of each subregion (Appendix E). The blue, magenta, and black lines correspond to the radial regions R1, R2, and R3, respectively (Section 3.2.1). The dashed horizontal line is unity. For all subregions, M31's disk is well described by a single thickened component (BIC2 < BIC3). Regardless, the similarity between the BIC values indicates that a simpler two-component model (halo, thick disk) is preferred.
Paper: Resolved SPLASH Chemodynamics in Andromeda’s PHAT Stellar Halo and Disk: On the Nature of the Inner Halo along the Major Axis
Authors: Ivanna Escala, Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, J. Leigh Wojno, Lara Cullinane, Benjamin F. Williams, Julianne Dalcanton
Figure caption: The same as Figure 4, except for region R2.
Paper: Resolved SPLASH Chemodynamics in Andromeda’s PHAT Stellar Halo and Disk: On the Nature of the Inner Halo along the Major Axis
Authors: Ivanna Escala, Amanda C. N. Quirk, Puragra Guhathakurta, Karoline M. Gilbert, J. Leigh Wojno, Lara Cullinane, Benjamin F. Williams, Julianne Dalcanton
Figure caption: The same as Figure 4, except for region R1.
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption: CMDs of (a, b) Berkeley 68 and (c, d) Stock 20 based on (a, c) UBV and (b, d) Gaia DR3 photometry. The blue dashed lines show the ZAMS (Sung et al. 2013) including the binary-star contamination. The membership probabilities of stars are shown with different colors; these member stars are located within ﹩{r}_{\mathrm{lim}}=8^{\prime} ﹩ and ﹩{r}_{\mathrm{lim}}=7\buildrel{\prime\prime}\over{.} 5﹩ of the cluster centers calculated for Berkeley 68 and Stock 20, respectively. The stars with the low membership probabilities are indicated with gray circles.
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption: VPDs of (a) Berkeley 68 and (b) Stock 20 based on Gaia DR3 astrometry. The membership probabilities of the stars are identified with the color scale shown on the right. The zoomed-in insets in panels (a) and (b) show the region of condensation for each cluster in the VPDs. The intersection of the dashed blue lines is the point of mean proper-motion values.
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption: Identification chart of stars located in regions of (a) Berkeley 68 and (b) Stock 20. The field of view of the charts is 21.″5 × 21.″5. North and east correspond to the up and left directions, respectively
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption: TCDs of the most probable member main-sequence stars in the regions of clusters (a) Berkeley 68 and (b) Stock 20. Red dashed and green solid curves represent the reddened ZAMS given by Sung et al. (2013) and ±1σ standard deviations, respectively. In the inner panels χ 2 vs. reddening vector values are shown. Dashed blue lines represent the best reddening vector corresponding to ﹩{\chi }_{\min }^{2}﹩.
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption: Gaia DR3-based trigonometric parallax histograms for (a) Berkeley 68 and (b) Stock 20. The red histograms are based on stars selected without limiting the relative parallax error and applied Gaussian fit, whereas the distribution of stars within the 0.2 relative parallax error and applied Gaussian fit are shown in black.
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption: Distribution for the membership probabilities of the stars in the (a) Berkeley 68 and (b) Stock 20 regions. The white shading presents the stars that are detected in the cluster areas, while the green shading denotes the stars that lie within the main-sequence band and cluster ﹩{r}_{\mathrm{lim}}﹩ radii.
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption: Histograms of (a, b) Berkeley 68 and (c, d) Stock 20 per magnitude bin in V and G filters. The red arrows indicate the adopted faint limiting apparent magnitudes in V and G filters. Black lines are the star counts based on V-band photometry, while blue lines are counts based on Gaia DR3 data for the same cluster regions.
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption: The stellar density distribution for (a) Berkeley 68 and (b) Stock 20. The fitted black curve represents the King (1962) profile, while the horizontal gray band shows background stellar density. The 1σ King fit uncertainty is shown by the red shaded domain.
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption: (U − B)0 × (B − V)0 TCDs (top panels) and histograms for the normalized δ 0.6 (bottom panels) for 17 (Berkeley 68; panel (a)) and 6 (Stock 20; panel (b)) most probable F- and G-type main-sequence stars. The solid blue lines in the TCDs represent the main sequence of Hyades and Gaussian fits, respectively.
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption:  U BV and Gaia-based CMDs for (a−c) Berkeley 68 and (d−f) Stock 20. Membership probabilities of most probable cluster stars are represented with different color scales that are shown on the color bars to the right, whereas field stars are shown with gray circles. The best-fitting PARSEC isochrones and their errors are presented as the blue lines with the surrounding purple shaded areas. Superimposed isochrone ages match to 2.4 Gyr for Berkeley 68 and 50 Myr for Stock 20.
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption: The orbit of Berkeley 68 in the Z × R GC and R GC × t planes. The filled yellow circles and triangle are the present-day and birth positions, respectively. The red arrow shows the motion vector of the cluster. The pink and green dotted lines show the orbit when errors in input parameters are considered, while the pink and green filled triangles represent the birth locations of the cluster based on the upper and lower error estimates, respectively.
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption: The LFs based on selected stars for (a) Berkeley 68 and (b) Stock 20.
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption: PDMFs of (a) Berkeley 68 and (b) Stock 20. Blue lines indicate the computed MFs of the OCs, while green lines are the ±1σ standard deviations.
Paper: An Investigation of Open Clusters Berkeley 68 and Stock 20 Using CCD UBV and Gaia DR3 Data
Authors: Talar Yontan
Figure caption: The cumulative radial distribution of stars in different mass ranges for (a) Berkeley 68 and (b) Stock 20.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Summary of the free-retrieval results for the constrained species, H2O, CO, and OH. Top row: marginalized gas mixing ratio histograms (95% CI shown as shaded region) under the “Fiducial” scenario described in Section 4.1 compared to a series of variable-composition self-consistent 1D-RCTE model abundance profiles (see footnotes 24–26). The retrieved abundances are consistent with a wide range of metallicities, but their combination can rule out self-consistent combinations of gases at high C/O. Bottom row: summarizes the impact of the free-retrieval assumptions on the marginalized gas mixing ratio histograms (see Sections 4.2 and 4.3). These assumptions appear to have a minimal quantitative impact on the gas volume mixing ratios.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Components of the spectrum that contribute to the observed signal. The template spectrum is a result of a 1× solar composition atmosphere in the 1D-RCTE, assuming a redistribution factor of 2.35 (based upon the trend of Parmentier et al. 2021). The dominant absorbers are H2O, OH, and CO. Starting with H2O (on top of an H-bound–free/free–free continuum), the other gases are sequentially added to illustrate their contribution to the total spectrum. The right panel shows the atmospheric structure (gas volume mixing ratio profiles for H2O, OH, CO, and O as dashed lines and the temperature–pressure profile in solid red) from the 1D-RCTE model. The atomic oxygen (O) profile is also shown to illustrate its role in the total elemental oxygen inventory. Also shown is the τ = 2/3 surface (in gray) used to identify the pressure levels sensed by the observations—between 1 and 0.01 bar. This suggests that the observations are sensitive to the region where the mixing ratio profiles change rapidly due to thermal dissociation as a result of the rapidly increasing temperature with altitude.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Summary of the Roasting Marshmallows dayside thermal emission HRCCS survey with IGRINS on GS. The key goals are to identify trends in composition and thermal structure over a wide range of stellar irradiation (equilibrium temperature) and planetary mass (gravity). The red circles are the proposed targets and blue is WASP-18, the focus of this work. The symbol size is proportional to the relative emission S/N for each target (e.g., Kempton et al. 2017), scaled to WASP-77 Ab (Line et al. 2021). Qualitative temperature–gravity locations of key atmospheric transitions (onset of the major inversion-causing species TiO/VO and the molecular thermal dissociation transition) are shown as dashed lines (based upon Parmentier et al. 2018). Broad questions are also indicated in the appropriate regions of parameter space. W = WASP, M = MASCARA.
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Top row: cross-correlation maps of the species detected in the atmosphere of WASP-18 b using the model spectra shown in Figure 3. The S/Ns are computed by dividing the peak value by the standard deviation away from the peak (Section 3.1). The literature solution for the planet velocity is indicated with white dashed lines. Bottom row: CIs for the same models as the top row, obtained via the likelihood framework and a three-parameter Markov Chain Monte Carlo model as described in Section 3.2. Each species is detected above the 3σ level. Visual comparison of the offset contours to the literature solution (red cross) indicates the potential atmospheric dynamics as a function of species (Section 5.3).
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Detection of the thermal emission spectrum of WASP-18 b when cross-correlating with the 1D-RCTE model described in Section 3.1. The planet is detected at an S/N of 5.9, and at a position in velocity space consistent with the literature solution for the orbit and the velocity of the system (white dotted lines).
Paper: The Roasting Marshmallows Program with IGRINS on Gemini South I: Composition and Climate of the Ultrahot Jupiter WASP-18 b
Authors: Matteo Brogi, Vanessa Emeka-Okafor, Michael R. Line, Siddharth Gandhi, Lorenzo Pino, Eliza M.-R. Kempton, Emily Rauscher, Vivien Parmentier, Jacob L. Bean, Gregory N. Mace, Nicolas B. Cowan, Evgenya Shkolnik, Joost P. Wardenier, Megan Mansfield, Luis Welbanks, Peter Smith, Jonathan J. Fortney, Jayne L. Birkby, Joseph A. Zalesky, Lisa Dang, Jennifer Patience, Jean-Michel Désert
Figure caption: Measured shifts (in pixels) vs. time of the IGRINS spectral sequence for orders in the H band (blue, one dot per order) and in the K band (red dots).
Paper: The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)
Authors: Joseph Harry Silber, Parker Fagrelius, Kevin Fanning, Michael Schubnell, Jessica Nicole Aguilar, Steven Ahlen, Jon Ameel, Otger Ballester, Charles Baltay, Chris Bebek, Dominic Benton Beard, Robert Besuner, Laia Cardiel-Sas, Ricard Casas, Francisco Javier Castander, Todd Claybaugh, Carl Dobson, Yutong Duan, Patrick Dunlop, Jerry Edelstein, William T. Emmet, Ann Elliott, Matthew Evatt, Irena Gershkovich, Julien Guy, Stu Harris, Henry Heetderks, Ian Heetderks, Klaus Honscheid, Jose Maria Illa, Patrick Jelinsky, Sharon R. Jelinsky, Jorge Jimenez, Armin Karcher, Stephen Kent, David Kirkby, Jean-Paul Kneib, Andrew Lambert, Mike Lampton, Daniela Leitner, Michael Levi, Jeremy McCauley, Aaron Meisner, Timothy N. Miller, Ramon Miquel, Juliá Mundet, Claire Poppett, David Rabinowitz, Kevin Reil, David Roman, David Schlegel, Santiago Serrano, William Van Shourt, David Sprayberry, Gregory Tarlé, Suk Sien Tie, Curtis Weaverdyck, Kai Zhang, Marco Azzaro, Stephen Bailey, Santiago Becerril, Tami Blackwell, Mohamed Bouri, David Brooks, Elizabeth Buckley-Geer, Jose Peñate Castro, Mark Derwent, Arjun Dey, Govinda Dhungana, Peter Doel, Daniel J. Eisenstein, Nasib Fahim, Juan Garcia-Bellido, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Philipp Hörler, Robert Kehoe, Theodore Kisner, Anthony Kremin, Luzius Kronig, Martin Landriau, Laurent Le Guillou, Paul Martini, John Moustakas, Nathalie Palanque-Delabrouille, Xiyan Peng, Will Percival, Francisco Prada, Carlos Allende Prieto, Guillermo Gonzalez de Rivera, Eusebio Sanchez, Justo Sanchez, Ray Sharples, Marcelle Soares-Santos, Edward Schlafly, Benjamin Alan Weaver, Zhimin Zhou, Yaling Zhu, Hu Zou
Figure caption: Each as-built petal was robotically surveyed and aligned such that fiber tips, fiducials, and cameras, when installed, would land in focus on DESI's nominal aspheric focal surface. The upper-left and lower-right photos show the FPR and petals being surveyed in a CMM at LBNL. The two photos at the lower left show the GFA camera mount plate on a petal, which is adjusted by shimming at its three mount screws. At the upper right, a stack of two gauge blocks and an aluminum retention/contact pad are seen at the corner of a petal. Each petal has two of these, which contact the FPR, and give us both stiff mounting and fine tilt adjustment. Not shown in these photos are two additional adjustment features of the petals: these are captive shim stacks at (1) the outer radius, to set the focal position, and (2) at the inner radius Figure 11, to equalize the petals with respect to each other at their tips. Over the set of all 12 petals (10 installed plus two spares), we achieved 12 μm rms, 33 μm max error in our alignment.
Paper: The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)
Authors: Joseph Harry Silber, Parker Fagrelius, Kevin Fanning, Michael Schubnell, Jessica Nicole Aguilar, Steven Ahlen, Jon Ameel, Otger Ballester, Charles Baltay, Chris Bebek, Dominic Benton Beard, Robert Besuner, Laia Cardiel-Sas, Ricard Casas, Francisco Javier Castander, Todd Claybaugh, Carl Dobson, Yutong Duan, Patrick Dunlop, Jerry Edelstein, William T. Emmet, Ann Elliott, Matthew Evatt, Irena Gershkovich, Julien Guy, Stu Harris, Henry Heetderks, Ian Heetderks, Klaus Honscheid, Jose Maria Illa, Patrick Jelinsky, Sharon R. Jelinsky, Jorge Jimenez, Armin Karcher, Stephen Kent, David Kirkby, Jean-Paul Kneib, Andrew Lambert, Mike Lampton, Daniela Leitner, Michael Levi, Jeremy McCauley, Aaron Meisner, Timothy N. Miller, Ramon Miquel, Juliá Mundet, Claire Poppett, David Rabinowitz, Kevin Reil, David Roman, David Schlegel, Santiago Serrano, William Van Shourt, David Sprayberry, Gregory Tarlé, Suk Sien Tie, Curtis Weaverdyck, Kai Zhang, Marco Azzaro, Stephen Bailey, Santiago Becerril, Tami Blackwell, Mohamed Bouri, David Brooks, Elizabeth Buckley-Geer, Jose Peñate Castro, Mark Derwent, Arjun Dey, Govinda Dhungana, Peter Doel, Daniel J. Eisenstein, Nasib Fahim, Juan Garcia-Bellido, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Philipp Hörler, Robert Kehoe, Theodore Kisner, Anthony Kremin, Luzius Kronig, Martin Landriau, Laurent Le Guillou, Paul Martini, John Moustakas, Nathalie Palanque-Delabrouille, Xiyan Peng, Will Percival, Francisco Prada, Carlos Allende Prieto, Guillermo Gonzalez de Rivera, Eusebio Sanchez, Justo Sanchez, Ray Sharples, Marcelle Soares-Santos, Edward Schlafly, Benjamin Alan Weaver, Zhimin Zhou, Yaling Zhu, Hu Zou
Figure caption: The 10 petals mount into a large integration ring (FPR), about 1/4 of which can be seen in the left photo. At the upper right, a petal is shown from the side, illustrating the curved front surface. We made the back surface flat to facilitate machining, metrology, and mounting of hardware. At the lower right, two petals are placed adjacent to each other at their separation distance (0.6 mm) when installed in the ring. Individual robot/fiducial mounting holes can be seen, each with a precision spotface and M8.7 × 0.35 mounting thread. Also visible (in the upper of these two petals) are accessory mounting holes, which we located in the natural gaps which occur along the irregular edge of each 36° petal.
Paper: The Robotic Multiobject Focal Plane System of the Dark Energy Spectroscopic Instrument (DESI)
Authors: Joseph Harry Silber, Parker Fagrelius, Kevin Fanning, Michael Schubnell, Jessica Nicole Aguilar, Steven Ahlen, Jon Ameel, Otger Ballester, Charles Baltay, Chris Bebek, Dominic Benton Beard, Robert Besuner, Laia Cardiel-Sas, Ricard Casas, Francisco Javier Castander, Todd Claybaugh, Carl Dobson, Yutong Duan, Patrick Dunlop, Jerry Edelstein, William T. Emmet, Ann Elliott, Matthew Evatt, Irena Gershkovich, Julien Guy, Stu Harris, Henry Heetderks, Ian Heetderks, Klaus Honscheid, Jose Maria Illa, Patrick Jelinsky, Sharon R. Jelinsky, Jorge Jimenez, Armin Karcher, Stephen Kent, David Kirkby, Jean-Paul Kneib, Andrew Lambert, Mike Lampton, Daniela Leitner, Michael Levi, Jeremy McCauley, Aaron Meisner, Timothy N. Miller, Ramon Miquel, Juliá Mundet, Claire Poppett, David Rabinowitz, Kevin Reil, David Roman, David Schlegel, Santiago Serrano, William Van Shourt, David Sprayberry, Gregory Tarlé, Suk Sien Tie, Curtis Weaverdyck, Kai Zhang, Marco Azzaro, Stephen Bailey, Santiago Becerril, Tami Blackwell, Mohamed Bouri, David Brooks, Elizabeth Buckley-Geer, Jose Peñate Castro, Mark Derwent, Arjun Dey, Govinda Dhungana, Peter Doel, Daniel J. Eisenstein, Nasib Fahim, Juan Garcia-Bellido, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Philipp Hörler, Robert Kehoe, Theodore Kisner, Anthony Kremin, Luzius Kronig, Martin Landriau, Laurent Le Guillou, Paul Martini, John Moustakas, Nathalie Palanque-Delabrouille, Xiyan Peng, Will Percival, Francisco Prada, Carlos Allende Prieto, Guillermo Gonzalez de Rivera, Eusebio Sanchez, Justo Sanchez, Ray Sharples, Marcelle Soares-Santos, Edward Schlafly, Benjamin Alan Weaver, Zhimin Zhou, Yaling Zhu, Hu Zou
Figure caption: The robots and the fiducials screw into the petal like a spark plug. This photo shows a prototype robot, placed in a cross-sectioned aluminum test block. The test block was fabricated by milling two faces flat, clamping them together, and then drilling, reaming, and tapping the custom threads.