adsabs/AstroCLIMB huggingface dataset:
Paper: The SDSS-V Local Volume Mapper Telescope System
Authors: T. M. Herbst, Peter Bizenberger, Guillermo A. Blanc, Florian Briegel, Niv Drory, Cynthia S. Froning, Wolfgang Gaessler, Maximilian Häberle, Nicholas P. Konidaris, Markus Kuhlberg, Alicia Lanz, Richard Mathar, Lars Mohr, Solange Ramirez, Christopher Ritz, Ralf-Rainer Rohloff, José Sánchez-Gallego, Stefanie Wachter, Hojae Ahn, Felipe Besser, Scott Case, Tobias Feger, Anthony Hebert, Juna A. Kollmeier, Soojong Pak, Hans-Walter Rix, David Robertson, Paula Stępień, Ross Zhelem
Figure caption: Distribution of the cumulative open-loop tracking error of the spec telescope during a single reference star pointing.
Paper: The SDSS-V Local Volume Mapper Telescope System
Authors: T. M. Herbst, Peter Bizenberger, Guillermo A. Blanc, Florian Briegel, Niv Drory, Cynthia S. Froning, Wolfgang Gaessler, Maximilian Häberle, Nicholas P. Konidaris, Markus Kuhlberg, Alicia Lanz, Richard Mathar, Lars Mohr, Solange Ramirez, Christopher Ritz, Ralf-Rainer Rohloff, José Sánchez-Gallego, Stefanie Wachter, Hojae Ahn, Felipe Besser, Scott Case, Tobias Feger, Anthony Hebert, Juna A. Kollmeier, Soojong Pak, Hans-Walter Rix, David Robertson, Paula Stępień, Ross Zhelem
Figure caption: Guide errors over 6 hr and 4000+ AG frames on MJD 60355. As before, the green triangle indicates the measured rms value and the vertical line, the requirement.
Paper: The SDSS-V Local Volume Mapper Telescope System
Authors: T. M. Herbst, Peter Bizenberger, Guillermo A. Blanc, Florian Briegel, Niv Drory, Cynthia S. Froning, Wolfgang Gaessler, Maximilian Häberle, Nicholas P. Konidaris, Markus Kuhlberg, Alicia Lanz, Richard Mathar, Lars Mohr, Solange Ramirez, Christopher Ritz, Ralf-Rainer Rohloff, José Sánchez-Gallego, Stefanie Wachter, Hojae Ahn, Felipe Besser, Scott Case, Tobias Feger, Anthony Hebert, Juna A. Kollmeier, Soojong Pak, Hans-Walter Rix, David Robertson, Paula Stępień, Ross Zhelem
Figure caption: Blind pointing error for the four LVM telescopes. See text for details.
Paper: The SDSS-V Local Volume Mapper (LVM): Scientific Motivation and Project Overview
Authors: Niv Drory, Guillermo A. Blanc, Kathryn Kreckel, Sebastián F. Sánchez, Alfredo Mejía-Narváez, Evelyn J. Johnston, Amy M. Jones, Eric W. Pellegrini, Nicholas P. Konidaris, Tom Herbst, José Sánchez-Gallego, Juna A. Kollmeier, Florence de Almeida, Jorge K. Barrera-Ballesteros, Dmitry Bizyaev, Joel R. Brownstein, Mar Canal i Saguer, Brian Cherinka, Maria-Rosa L. Cioni, Enrico Congiu, Maren Cosens, Bruno Dias, John Donor, Oleg Egorov, Evgeniia Egorova, Cynthia S. Froning, Pablo García, Simon C. O. Glover, Hannah Greve, Maximilian Häberle, Kevin Hoy, Hector Ibarra, Jing Li, Ralf S. Klessen, Dhanesh Krishnarao, Nimisha Kumari, Knox S. Long, José Eduardo Méndez-Delgado, Silvia Anastasia Popa, Solange Ramirez, Hans-Walter Rix, Aurora Mata Sánchez, Ravi Sankrit, Natascha Sattler, Conor Sayres, Amrita Singh, Guy Stringfellow, Stefanie Wachter, Elizabeth Jayne Watkins, Tony Wong, Aida Wofford
Figure caption: Example of the fitting procedure performed by the pDAP. The top panel shows the integrated spectrum within the central pointing of the Rosette Nebula (back line), together with the best-fit stellar template (red line), the residual after subtracting this model (cyan line), the multi-Gaussian model of the ionized gas emission lines (blue line), and the total residual (the result of subtracting the stellar and emission line models from the original spectrum). The small orange vertical lines indicate the emission lines the pDAP is attempting to extract (flux, velocity, velocity dispersion, and equivalent width) using a weighted-moment analysis, as described in the text. We adopt a square-root scaling in the top panel to compress the large dynamic range of the data. The panels in the middle row show zoom-ins around the strongest emission lines, now in linear scaling: [O II]3726,28 , Hδ, Hγ, Hβ, [O III]5007, Hα+[N II]6548,83, [S II]3717,31, [S III]9069, and [S III]9531, from left to right. Finally, the bottom row shows a zoom-in around stellar absorption features to illustrate the quality of the template fit: 3800-4100 Å and 4800-5100 Å. The remaining four panels show the detections of weak emission lines, including (i) HeI4471 and HeI6678, two lines used to determine the He abundance (e.g., M. Valerdi et al. 2021), (ii) [O II]7318, a line tracing the presence of SNR (e.g., R. Cid Fernandes et al. 2021), and (iii) two auroral lines frequently adopted to determine the electron temperature, [N II]5755 and [S III]6312 (e.g., R. A. Marino et al. 2013).
Paper: The SDSS-V Local Volume Mapper (LVM): Scientific Motivation and Project Overview
Authors: Niv Drory, Guillermo A. Blanc, Kathryn Kreckel, Sebastián F. Sánchez, Alfredo Mejía-Narváez, Evelyn J. Johnston, Amy M. Jones, Eric W. Pellegrini, Nicholas P. Konidaris, Tom Herbst, José Sánchez-Gallego, Juna A. Kollmeier, Florence de Almeida, Jorge K. Barrera-Ballesteros, Dmitry Bizyaev, Joel R. Brownstein, Mar Canal i Saguer, Brian Cherinka, Maria-Rosa L. Cioni, Enrico Congiu, Maren Cosens, Bruno Dias, John Donor, Oleg Egorov, Evgeniia Egorova, Cynthia S. Froning, Pablo García, Simon C. O. Glover, Hannah Greve, Maximilian Häberle, Kevin Hoy, Hector Ibarra, Jing Li, Ralf S. Klessen, Dhanesh Krishnarao, Nimisha Kumari, Knox S. Long, José Eduardo Méndez-Delgado, Silvia Anastasia Popa, Solange Ramirez, Hans-Walter Rix, Aurora Mata Sánchez, Ravi Sankrit, Natascha Sattler, Conor Sayres, Amrita Singh, Guy Stringfellow, Stefanie Wachter, Elizabeth Jayne Watkins, Tony Wong, Aida Wofford
Figure caption: Spatial distribution of different parameters derived from the weighted-moments analysis included in the LVM pDAP for the Rosette Nebulae data shown in Figure 11. From top left to bottom right, we show (i) the Hα velocity, (ii) the Hα velocity dispersion, (iii) the Hα to Hβ flux intensity ratio, (iv) the [O III] to Hβ flux intensity ratio, (v) the [N II] to Hα flux intensity ratio, and (vi) the [S II]6717 to [S II]6731 flux intensity ratio.
Paper: The SDSS-V Local Volume Mapper (LVM): Scientific Motivation and Project Overview
Authors: Niv Drory, Guillermo A. Blanc, Kathryn Kreckel, Sebastián F. Sánchez, Alfredo Mejía-Narváez, Evelyn J. Johnston, Amy M. Jones, Eric W. Pellegrini, Nicholas P. Konidaris, Tom Herbst, José Sánchez-Gallego, Juna A. Kollmeier, Florence de Almeida, Jorge K. Barrera-Ballesteros, Dmitry Bizyaev, Joel R. Brownstein, Mar Canal i Saguer, Brian Cherinka, Maria-Rosa L. Cioni, Enrico Congiu, Maren Cosens, Bruno Dias, John Donor, Oleg Egorov, Evgeniia Egorova, Cynthia S. Froning, Pablo García, Simon C. O. Glover, Hannah Greve, Maximilian Häberle, Kevin Hoy, Hector Ibarra, Jing Li, Ralf S. Klessen, Dhanesh Krishnarao, Nimisha Kumari, Knox S. Long, José Eduardo Méndez-Delgado, Silvia Anastasia Popa, Solange Ramirez, Hans-Walter Rix, Aurora Mata Sánchez, Ravi Sankrit, Natascha Sattler, Conor Sayres, Amrita Singh, Guy Stringfellow, Stefanie Wachter, Elizabeth Jayne Watkins, Tony Wong, Aida Wofford
Figure caption: Flux intensity maps in units of 10−16 erg s−1 cm−2 of a set of emission lines derived using the weighted-moments analysis included in the LVM pDAP for the Rosette Nebulae. Each panel comprises a mosaic of seven different hexagonal pointings, covering an area with a diameter of ∼1°. The flux extracted for each of the ∼1800 fibers (per pointing) is shown as an individual color-coded circles (i.e., no interpolation is performed). The intensity range has been adjusted for each emission line, covering between the mean value minus 10% and the mean value plus 3σ.
Paper: The SDSS-V Local Volume Mapper (LVM): Scientific Motivation and Project Overview
Authors: Niv Drory, Guillermo A. Blanc, Kathryn Kreckel, Sebastián F. Sánchez, Alfredo Mejía-Narváez, Evelyn J. Johnston, Amy M. Jones, Eric W. Pellegrini, Nicholas P. Konidaris, Tom Herbst, José Sánchez-Gallego, Juna A. Kollmeier, Florence de Almeida, Jorge K. Barrera-Ballesteros, Dmitry Bizyaev, Joel R. Brownstein, Mar Canal i Saguer, Brian Cherinka, Maria-Rosa L. Cioni, Enrico Congiu, Maren Cosens, Bruno Dias, John Donor, Oleg Egorov, Evgeniia Egorova, Cynthia S. Froning, Pablo García, Simon C. O. Glover, Hannah Greve, Maximilian Häberle, Kevin Hoy, Hector Ibarra, Jing Li, Ralf S. Klessen, Dhanesh Krishnarao, Nimisha Kumari, Knox S. Long, José Eduardo Méndez-Delgado, Silvia Anastasia Popa, Solange Ramirez, Hans-Walter Rix, Aurora Mata Sánchez, Ravi Sankrit, Natascha Sattler, Conor Sayres, Amrita Singh, Guy Stringfellow, Stefanie Wachter, Elizabeth Jayne Watkins, Tony Wong, Aida Wofford
Figure caption: 58 LVM survey tiles reveal filamentary diffuse structures and bright ionized nebulae in our continuum subtracted Hα map, covering ∼3 kpc of the LMC. These maps resolve structures on scales of 10 pc, building toward a panoptic view of this galaxy.
Paper: The SDSS-V Local Volume Mapper Telescope System
Authors: T. M. Herbst, Peter Bizenberger, Guillermo A. Blanc, Florian Briegel, Niv Drory, Cynthia S. Froning, Wolfgang Gaessler, Maximilian Häberle, Nicholas P. Konidaris, Markus Kuhlberg, Alicia Lanz, Richard Mathar, Lars Mohr, Solange Ramirez, Christopher Ritz, Ralf-Rainer Rohloff, José Sánchez-Gallego, Stefanie Wachter, Hojae Ahn, Felipe Besser, Scott Case, Tobias Feger, Anthony Hebert, Juna A. Kollmeier, Soojong Pak, Hans-Walter Rix, David Robertson, Paula Stępień, Ross Zhelem
Figure caption: Orientation of the LVM telescopes, with the siderostats mounted on a concrete platform south of the optical tables and feeding the light to the north. Note also our internal right-handed coordinate system with X to the east, Y to the north, and Z pointing to zenith. This is the spectrophotometric telescope, which has no K-mirror derotator. Instead, a fiber selector mechanism exposes individual IFU lenslets to the current reference star. Both the spectrophotometric and science/sky telescopes use multiple internal baffles to suppress scattered light (five for the sci/sky telescopes and three for the spec telescope as shown). A 3D-printed “snout” mounted to the dust cover encloses the siderostat housing, preventing light and dust ingress while allowing free rotation.
Paper: The SDSS-V Local Volume Mapper Telescope System
Authors: T. M. Herbst, Peter Bizenberger, Guillermo A. Blanc, Florian Briegel, Niv Drory, Cynthia S. Froning, Wolfgang Gaessler, Maximilian Häberle, Nicholas P. Konidaris, Markus Kuhlberg, Alicia Lanz, Richard Mathar, Lars Mohr, Solange Ramirez, Christopher Ritz, Ralf-Rainer Rohloff, José Sánchez-Gallego, Stefanie Wachter, Hojae Ahn, Felipe Besser, Scott Case, Tobias Feger, Anthony Hebert, Juna A. Kollmeier, Soojong Pak, Hans-Walter Rix, David Robertson, Paula Stępień, Ross Zhelem
Figure caption: Timeline and a portion of a notional spectrograph exposure illustrating the LVM telescope operating principle of interspersing Science, Sky, and Spectrophotometric observations. Note that the roughly 1 minute “Setup” phase includes readout of the CCDs from the previous exposure and setup on the new target.
Paper: The SDSS-V Local Volume Mapper Telescope System
Authors: T. M. Herbst, Peter Bizenberger, Guillermo A. Blanc, Florian Briegel, Niv Drory, Cynthia S. Froning, Wolfgang Gaessler, Maximilian Häberle, Nicholas P. Konidaris, Markus Kuhlberg, Alicia Lanz, Richard Mathar, Lars Mohr, Solange Ramirez, Christopher Ritz, Ralf-Rainer Rohloff, José Sánchez-Gallego, Stefanie Wachter, Hojae Ahn, Felipe Besser, Scott Case, Tobias Feger, Anthony Hebert, Juna A. Kollmeier, Soojong Pak, Hans-Walter Rix, David Robertson, Paula Stępień, Ross Zhelem
Figure caption: Mirror names, axis definitions, and angles for the siderostats. We define siderostat angles S1 = S2 = 0 when looking at zenith, and the angles increase as shown, since this is a right-hand system.
Paper: The SDSS-V Local Volume Mapper Telescope System
Authors: T. M. Herbst, Peter Bizenberger, Guillermo A. Blanc, Florian Briegel, Niv Drory, Cynthia S. Froning, Wolfgang Gaessler, Maximilian Häberle, Nicholas P. Konidaris, Markus Kuhlberg, Alicia Lanz, Richard Mathar, Lars Mohr, Solange Ramirez, Christopher Ritz, Ralf-Rainer Rohloff, José Sánchez-Gallego, Stefanie Wachter, Hojae Ahn, Felipe Besser, Scott Case, Tobias Feger, Anthony Hebert, Juna A. Kollmeier, Soojong Pak, Hans-Walter Rix, David Robertson, Paula Stępień, Ross Zhelem
Figure caption: Hardware components of the LVM telescopes. Note that this layout corresponds to the Science and Sky telescopes. Figure 5 portrays the Spectrophotometric breadboard and illustrates the internal baffling scheme present on all four optical tables.
Paper: The SDSS-V Local Volume Mapper Telescope System
Authors: T. M. Herbst, Peter Bizenberger, Guillermo A. Blanc, Florian Briegel, Niv Drory, Cynthia S. Froning, Wolfgang Gaessler, Maximilian Häberle, Nicholas P. Konidaris, Markus Kuhlberg, Alicia Lanz, Richard Mathar, Lars Mohr, Solange Ramirez, Christopher Ritz, Ralf-Rainer Rohloff, José Sánchez-Gallego, Stefanie Wachter, Hojae Ahn, Felipe Besser, Scott Case, Tobias Feger, Anthony Hebert, Juna A. Kollmeier, Soojong Pak, Hans-Walter Rix, David Robertson, Paula Stępień, Ross Zhelem
Figure caption: The LVM-I. Each of the four LVM telescopes uses a siderostat in altitude–altitude configuration feeding fixed components on an optical table. Fiber bundles convey the light to an environmentally controlled spectrograph chamber containing a sorting box to distribute the fibers to three identical spectrographs. The roll-off roof protects the instrument during daytime and inclement weather.
Paper: The SDSS-V Local Volume Mapper Telescope System
Authors: T. M. Herbst, Peter Bizenberger, Guillermo A. Blanc, Florian Briegel, Niv Drory, Cynthia S. Froning, Wolfgang Gaessler, Maximilian Häberle, Nicholas P. Konidaris, Markus Kuhlberg, Alicia Lanz, Richard Mathar, Lars Mohr, Solange Ramirez, Christopher Ritz, Ralf-Rainer Rohloff, José Sánchez-Gallego, Stefanie Wachter, Hojae Ahn, Felipe Besser, Scott Case, Tobias Feger, Anthony Hebert, Juna A. Kollmeier, Soojong Pak, Hans-Walter Rix, David Robertson, Paula Stępień, Ross Zhelem
Figure caption: Lenslet geometry. The individual IFU lenslets are 330 μm or 37″ center to center (left). An opaque chromium mask restricts the aperture to 315 μm or 35.″3 diameter, to prevent aberrations and cross talk at the lenslet boundaries. The microlenses themselves compress the field and deliver a slightly undersized, f/3.7 image to the fiber cores (right).
Paper: The SDSS-V Local Volume Mapper Telescope System
Authors: T. M. Herbst, Peter Bizenberger, Guillermo A. Blanc, Florian Briegel, Niv Drory, Cynthia S. Froning, Wolfgang Gaessler, Maximilian Häberle, Nicholas P. Konidaris, Markus Kuhlberg, Alicia Lanz, Richard Mathar, Lars Mohr, Solange Ramirez, Christopher Ritz, Ralf-Rainer Rohloff, José Sánchez-Gallego, Stefanie Wachter, Hojae Ahn, Felipe Besser, Scott Case, Tobias Feger, Anthony Hebert, Juna A. Kollmeier, Soojong Pak, Hans-Walter Rix, David Robertson, Paula Stępień, Ross Zhelem
Figure caption: A custom triskelion flexure plate accommodates in-plane mirror motion and differential thermal expansion (left). The conical cups in the flexure plate mate with hemispherical pucks bonded to the rear of the Zerodur mirror (right).
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Schematic diagram of the two observation modes.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Power spectra corresponding to the two observation modes (in black: the spectrum of the reference gravity field).
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Power spectra corresponding to the orbital inclinations.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Power spectra corresponding to the different observation times.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Inter-satellite distance change and orbital altitude difference of the two satellites.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Range-rate data in the two observation modes.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Orbital altitude difference between two satellites with different orbital inclinations.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Orbital chart of the two satellites.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Power spectra corresponding to the initial satellite distances.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: The subsatellite point coverage for 10 days (left) and 35 days (right) observation times. The sidereal period of Callisto is about 16.69 days.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Power spectra corresponding to the orbital altitudes.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Admittances for ice shell thickness = 200 km, ice shell density = 1200 kg m−3.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Admittances for ice shell thickness = 200 km, elastic thickness = 100 km.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Power spectra corresponding to the 2W+SST and only SST observation modes.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Position and velocity difference for d/o 40 and d/o 80, d/o60 and d/o80.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Normalized correlation coefficients between the gravity-field coefficients for orbital inclinations of 70° and 90°.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Normalized correlation coefficients between the gravity-field coefficients for the orbital inclination of 90°.
Paper: Assessment of Callisto Gravity-field Determination Using the Inter-satellite Range-rate Link
Authors: Shangbiao Sun, Jianguo Yan, Wutong Gao, Bo Wang, Dominic Dirkx, Zhen Wang, Yongzhang Yang, Jean-Pierre Barriot
Figure caption: Normalized correlation coefficients between the gravity-field coefficients for orbital inclinations of 80° and 90°.
Paper: Host-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways
Authors: Bihan Banerjee, Mayank Narang, P. Manoj, Thomas Henning, Himanshu Tyagi, Arun Surya, Prasanta K. Nayak, Mihir Tripathi
Figure caption: [Fe/H] distributions for HJs, WJs, and CJs. (a) Colored histograms and KDEs, which show HJs are relatively metal rich compared to WJs and CJs. Any difference between WJs and CJs in terms of host-star metallicity is not apparent. The black vertical lines denote the median [Fe/H]. (b) Violin plots showing the distribution of [Fe/H] for HJ, WJ, and CJ hosts (c) Cumulative distributions of [Fe/H] for HJ, WJ, and CJ hosts. The plots clearly show HJ hosts are distinctly metal rich.
Paper: Host-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways
Authors: Bihan Banerjee, Mayank Narang, P. Manoj, Thomas Henning, Himanshu Tyagi, Arun Surya, Prasanta K. Nayak, Mihir Tripathi
Figure caption: Gaia DR3 color–magnitude diagram of planet-hosting stars in the solar neighborhood. All stars within 250 pc with detected planets are shown as blue points. Red points indicate main-sequence stars. The black solid line represents Equation (1), and the dashed lines represent ±1.5 mag of the expected M  G  value for a given G BP − G RP.
Paper: Host-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways
Authors: Bihan Banerjee, Mayank Narang, P. Manoj, Thomas Henning, Himanshu Tyagi, Arun Surya, Prasanta K. Nayak, Mihir Tripathi
Figure caption: Monte Carlo Analysis 2: can random sampling from an underlying uniform distribution of host-star [Fe/H] produce the observed results? (a) The underlying distribution is a KDE of the [Fe/H] distribution of Jupiter hosts in our sample. We draw random samples from this distribution repeatedly of the exact sizes of our observed sample and compute the median difference. The blue histograms are the distributions of median differences for (b) HJs and CJs, (c) HJs and CCJs, and (d) CEJs and CCJs. The vertical black solid lines in all these figures represent the observed median differences. The region right to this black solid line is colored yellow, where where the median difference is greater than the observed median difference. The probability of the median difference ≥ the observed median difference is the area under the histogram in the yellow shaded region divided by the total number of counts.