adsabs/AstroCLIMB huggingface dataset:
Paper: The Effect of Age and Stellar Model Choice on Globular Cluster Color-to-metallicity Conversions
Authors: Kate Hartman, William E. Harris
Figure caption: MDFs for the sample from Hartman et al. (2023), transformed from color distribution functions using each of the five stellar models.
Paper: The Effect of Age and Stellar Model Choice on Globular Cluster Color-to-metallicity Conversions
Authors: Kate Hartman, William E. Harris
Figure caption: Fitted exponential metallicity–color relations for the five models and the five GC age groups.
Paper: The Effect of Age and Stellar Model Choice on Globular Cluster Color-to-metallicity Conversions
Authors: Kate Hartman, William E. Harris
Figure caption: GC age corrections for the fitted CMRs. The corrected relations are slightly flatter than the CMRs for specific GC ages in the PARSEC and MIST models, and slightly more curved in the BaSTI models. In all cases, the difference between fitted relations for individual ages and the age-corrected relation is very small.
Paper: The Effect of Age and Stellar Model Choice on Globular Cluster Color-to-metallicity Conversions
Authors: Kate Hartman, William E. Harris
Figure caption: Age vs. metallicity for Milky Way GCs. Data are from Forbes & Bridges (2010), VandenBerg et al. (2013), and Dotter et al. (2010); the black line shows Equation (4), a fitted linear age–metallicity relation based on all three data sets.
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: Constraints on the mass and radius of TOI-2015 b. M-dwarf TTV planets are denoted with black points and non-TTV M-dwarf planets are shown with faint gray points. Blue squares show solar system planets. TOI-2015 b (red point) is similar to TTV planets AU Mic b and K2-146 b/c, which have potential composition models consistent with a rocky core and low-mass H/He atmosphere. The red curve shows the two-layer composition model of Lopez & Fortney (2014) with a rocky core shrouded by a H/He envelope, suggesting that TOI-2015 b has a H/He mass fraction of 6%. The other solid lines show composition models from Zeng et al. (2019). The shaded gray region shows where the expected planetary iron content would exceed the maximum value predicted from models of collisional stripping from Marcus et al. (2010).
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: The Neptune desert plotted in radius–period and radius–insolation parameter spaces. Colored points are M-dwarf planets, and translucent gray points are planets with FGK hosts. TOI-2015 b is circled in green. (A) Planet radius vs. orbital period plane. Points are colored by Log10 insolation. The dashed line represents the boundary of the Neptune desert in the radius–period plane as defined by Mazeh et al. (2016). (B) Planet radius vs. insolation plane. Points are colored by stellar effective temperature. The black dashed line represents the Neptune desert boundary as defined by Mazeh et al. (2016), assuming a solar-type star (M * = 1 M ⊙, L * = 1 L ⊙). The gray dotted–dashed line is a redefined boundary assuming a M4-type star (M * = 0.35 M ⊙, L * = 0.01 L ⊙). While TOI-2015 b falls within the Mazeh et al. (2016) Neptune desert boundary in radius–period space, its host star is a faint red mid-type M dwarf, so the planet receives too little flux to place it inside the Neptune desert.
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: TTVs of TOI-2015 b as a function of time (filled circles). Twenty models corresponding to stable posterior samples from each of the 2:1, 3:2, and 4:3 joint TTV-RV solutions are shown with thin blue, orange, and green lines, respectively. The residuals in the bottom panel are shown with respect to the maximum-likelihood 2:1 solution. Here the TTVs are shown with respect to the ephemeris of t 0(BJD) = 2458956.0238 and P = 3.3489393 days obtained by linear fitting of the observed transit times. The linear trend seen in the posterior TTV models in this figure indicates that the mean orbital period inferred from the dynamical modeling differs from the value estimated from the available transit times. TESS will observe TOI-2015 again from 2024 April 23 to 2024 May 21 in Sector 78, denoted by the gray region in the figure.
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: Generalized Lomb–Scargle periodograms of the HPF RVs and HPF activity indicators. (A) HPF RVs. (B) HPF differential line width (dLW) indicator. (C) Chromatic activity index (CRX). (D)–(F) Ca II infrared triplet (IRT) line indicators. (G) Window function (WF) of the observations. The known planet period and the stellar rotation period are denoted with the vertical blue and red dashed lines, respectively. False-alarm probabilities (FAPs) of 1% and 0.1% calculated using a bootstrap method are denoted with the gray solid and gray dashed lines, respectively. Although we see a hint of a peak near the known planet period, it is not significant (FAP > 1%). For the activity indicators, we see no significant peaks at the known planet or stellar rotation periods. Periodograms (A)–(F) are normalized using the formalism in Zechmeister & Kürster (2009), while the WF in panel (G) is normalized such that the highest peak has a power of 1.
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: (A) The maximum-likelihood 2:1 solution from the joint TTV and RV fit (blue solid line) compared with the HPF data (white circles with error bars). (B)–(C) The contribution of each planet to the RV signal in the above solution is shown as a function of the orbital phase. Here the signal due to each planet is computed by setting the mass of the other planet to be zero in the N-body model. In the right panel, the RV signal due to the inner planet is subtracted from the data. Note that the stellar RVs are computed via direct N-body integration in our joint TTV and RV fit, rather than by adding two independent Keplerian signals; thus the RV signals do not have fixed periods in reality.
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: TOI-2015 phased photometry from juliet joint TTV fit. Data points are plotted in blue. The best-fit transit models are plotted with solid black lines. The vertical black lines represent the expected linear midpoint predictions, and the vertical red lines are the true TTV midpoints. The transit number (first TESS transit is #0) is labeled in the bottom-left corner of each ground-based transit. (A) Phase-folded photometry of 12 TESS transits. White points are N Bin = 15 binned data. (B) LCOGT partial-transit photometry. (C) WIRO full-transit photometry. (D) RBO full-transit photometry. (E) ARC 2023 April full-transit photometry. (F) ARC 2023 May full-transit photometry.
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: Transit least-squares signal detection efficiency (TLS SDE) power spectra as a function of orbital period for TESS Sectors 24 and 51. The solid blue bands indicate the maximum peak of each power spectrum. The blue dotted lines in panels (A) and (B) are the integer harmonics of the 3.3490 days orbital period of TOI-2015 b in red. The gray dashed lines represent 0.1% false-alarm probability (FAP). We do not detect signals of an additional transiting companion in the TESS data.
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: HPF RV measurements. RVs (blue points) are plotted with respect to the baseline (horizontal dashed line) and the best-fit model (bold black line). (A) RVs as a function of time. (B) RVs phase-folded at the period of TOI-2015 b. Residuals are displayed in the corresponding lower panels. The RV data are listed in Table 6 in Appendix B. TOI-2015 b is evident in the RVs, but there are no additional planetary signals.
Paper: TOI-2015 b: A Warm Neptune with Transit Timing Variations Orbiting an Active Mid-type M Dwarf
Authors: Sinclaire E. Jones, Guđmundur Stefánsson, Kento Masuda, Jessica E. Libby-Roberts, Cristilyn N. Gardner, Rae Holcomb, Corey Beard, Paul Robertson, Caleb I. Cañas, Suvrath Mahadevan, Shubham Kanodia, Andrea S. J. Lin, Henry A. Kobulnicky, Brock A. Parker, Chad F. Bender, William D. Cochran, Scott A. Diddams, Rachel B. Fernandes, Arvind F. Gupta, Samuel Halverson, Suzanne L. Hawley, Fred R. Hearty, Leslie Hebb, Adam Kowalski, Jack Lubin, Andrew Monson, Joe P. Ninan, Lawrence Ramsey, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski
Figure caption: Individual TESS transits detrended photometry with juliet TTV fit model. The vertical black lines represent the expected linear predictions, and the vertical red lines are the true TTV midpoints. Transit number is labeled in the bottom-right corner of each transit.
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 acquisition and guiding software maps the AG exposures into the focal plane, creating a large MF covering both sensors and the IFU. The transformations derived from the laboratory focal plane metrology, coupled with an astrometry.net solve of the MF, yields the pointing direction and field rotation. In the figure, the AG camera frames are from the instrument, while the background image of the same field is a DSS2 red exposure centered near the bright star β Corvi.
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 preintegration facility on the north side of the MPIA campus. Note that, for these tests, we used an undersized prototype siderostat mirror assembly. Heidelberg is not an ideal observatory site: a thick PVC-coated polyester cover and a portable tent protected the instrument from the elements when not in use. Note also the dehumidifier under the optical table—it ran continuously when the instrument was covered.
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 delivered FWHM in arcseconds for the LVM telescopes on MJD 60355. The green triangle shows the measured rms value and the vertical line indicates the 3.″5 rms 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: Scanning the surface of the custom reflecting target to align the PSM perpendicular to the focal plane. Note that this photo depicts an early lab measurement using prototype prism mirrors. The final prisms and mounts are blackened to minimize scattered light.
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 diamond-turned reflecting target with a precise central mark assists with alignment (left). When bolted to the objective lens barrel, for example (right), the target provides clear centering, pitch, and yaw information to the AA.
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 measured best-focus position as a function of ambient temperature for the four LVM telescopes.
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: LVM telescope first light image of M42 on 2023 February 16. This an unguided, 2 minute exposure using the color on-axis CMOS test camera.
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: One of the mounted siderostat mirrors undergoing full-aperture interferometric testing. Photo courtesy of Precision Optical (Costa Mesa, CA, USA).
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: (Left) Craning of the first optical table onto the telescope platform at the beginning of 2023 February. (Right) the completed telescope array at the end of 2023 February.
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 elevation (left) and azimuth (right) for the sky above Las Campanas Observatory. North is up and east to the left. The colors indicate the elevation and azimuth angles for all locations above the horizon, with white traces showing every 10°. The LVM survey operates above 30° elevation (outer dashed circles). The solid black contours are constant decl., and objects track from left to right along these lines. For objects with decl. near −29°, the latitude of the observatory, the target rapidly traverses a large range of azimuth angles near transit.
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 K-mirror rotation rate. Again, the separation of the white contours is 0.°001 s−1. Note that the K-mirror tracking rate is always negative.
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: Angular tracking rates for the two siderostat axes. Note that in these plots, the spacing of the white contours is 0.°001 s−1.
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 S1 and S2 siderostat angles for all sky locations.
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: Incidence angles for the LVM K-mirror. See text for details.