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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: LVM survey footprint overlaid on the D. P. Finkbeiner (2003) Hα  map of the full sky. We show different target classes in different colors for clarity. The Milky Way survey consists of an 8° band in the midplane of the disk spanning 30° longitude through the Galactic center to 175° (blue). A lower-priority 18° band spans 30° longitude to 240° (green). These bands around the midplane are augmented by coverage of the two nearby H II regions: Orion (purple) and Gum (dark blue). We supplement disk plane survey with a sparse grid (green) tracking large scale diffuse ionized gas above the Milky Way plane. LVM furthermore covers the LMC and SMC to their optical radius (∼R 25; light purple). The simple geometric selection function of the MW midplane survey facilitates easy comparison with simulations. Zooming into the Orion region (lower right), we show ionized emission sampled at the LVM spaxel size of 0.07 pc. At larger distances in the Milky Way of ∼3 kpc, we still recover filamentary emission features (lower left) at 0.6 pc resolution. Within the LMC (center bottom), we show a continuum and ionized emission in the 30 Doradus star-forming region, sampled at the 10 pc spaxel size LVM will deliver in the Magellanic System.
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: Candidate sky fields (left) and spectrophotometric calibration stars (right). Areas of the sky not observable by LVM at LCO are shaded in blue. Left: Gray dots form an all-sky grid of sky fields. Red dots are the WHAM darkest regions with Hα flux below 0.5 R; blue dots are the IRDC fields (see text for explanation of the selection). Right: The location of bright, isolated F-type stars (gray dots) are selected from Gaia DR3. We can find ensembles of 12 calibration stars within 5°–8° of any science field.
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: The LVM-I integral-field units feeding the spectrographs. The science IFU consists of 1801 fibers arranged in 25 hexagonal rings (including the central fiber), and three segments feeding one spectrograph each. The two sky telescopes have 59 and 60 fibers respectively and are also divided into three segments each feeding the three spectrographs. Each block of fibers along the slit is flanked by two sky fibers on each side, one from each sky telescope. Finally, the spectrophotometric telescopes has 24 fibers covered by a rotary shutter allowing us to expose one fiber at a time. Eight fibers go to each spectrograph.
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: LVM baseline 4 yr survey footprint and target definition. We divide the MW midplane survey into a high-priority 8° wide band (pink), surrounded by a lower-priority 18° wide band (brown). We highlight the region observed by THOR near the MW center (gray). In addition, we target a densely sampled region around the Orion Nebula (near R.A. 6 h, just south of the plane; red), surrounded by a wider, more sparsely sampled region to cover the entire ionized nebula and its interface to the surrounding ISM. We extend the midplane survey around R.A. of 8 h to cover a wider area in the Gum Nebula (cyan, green). We augment the MW disk coverage with a sparse all-sky grid of pointings to sample the out-of-plane targeted when no other target is observable (gray). Finally, we target the LMC (blue) and SMC (orange).
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: Initial 101 LVM survey tiles covering the H II region IC 434 within Orion. Continuum subtracted line emission ([S III]9532 in magenta, [S II]6717+6731 in blue, and Hα in orange, tracing high- and low-ionization zones and average nebula emission, respectively) reveals beautiful ionized gas structures. This map provides <0.1 pc scale views, capable of tracing changes in both gas physical conditions (density, temperature, abundances) and kinematics.
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: An LVM-I telescope and its components. For scale, the optical bench is 210 × 75 cm in size
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: LVM Survey area with tile outlines in the LMC (left panel) and the SMC (right panel) overlaid on top of Hα imaging SHASSA (J. E. Gaustad et al. 2001).
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: The LVM-I instrument and its major subsystems.
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 SkyE dust cover integrated in the lab prior to shipment. The latches and handles provide easy access, while the white weatherproofing seals at the edges of the panels prevent dust ingress. This is the southeast corner of the cover, and it is truncated to permit full sky coverage when the siderostat looks to the northeast (M1 is low and the counterweight high in the east—see Figure 6). The snout coupling to the siderostat mounts at the location of the circular aperture at lower left.
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 spectrophotometric FPA (left panel). This is the view looking toward the IFU from the siderostat (i.e., looking north—see Figure 5). The Newport rotary stage on the left (west) side drives the two-hole mask (inset), while a reflecting prism on the right (east) side feeds light to a single acquisition camera. The rotary mask exposes one of the 24 spectrophotometric fiber locations at a time (right panel).
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 focal plane layout for the four LVM telescopes. Unless marked otherwise, all dimensions are in arcminutes on the sky. See text for details.
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: We used a custom rig to bond the lenses (left). The oversized silicone bonding pads led to web-like voids in the SYLGARD elastomer (right). Reducing the bond size and mounting to one of the N-BAK2 lenses eliminated these features.
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 optical tables consist of an optical breadboard mounted to a welded steel support structure (left). A combination of push bolt mechanisms and Airloc Wedgmount height adjusters enable adjustment in X–Y–Z location as well as pitch and yaw. See text for details.
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 derotators combine three, high-performance flat mirrors with a precision commercial rotary stage to cancel the field rotation induced by the combination of a moving telescope with a fixed focal plane. Note that this image shows the derotator with aluminum dummy mirrors used for preliminary assembly and functionality tests.
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 objective lens focuser mechanism permits adjustment in X–Y–Z location, as well as pitch and yaw.
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 components of the FPA for the one science and two sky telescopes. Figure 14 shows the layout of the spectrophotometric FPA.
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: Broadband reflectivity of the first and third K-mirror mirrors (left) and the second mirror (right). The multilayer coating designs are optimized for 60° and 30° incidence, respectively. The green region shows the operating wavelength range of LVM.
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: Spherical triangle to derive the siderostat angles S1 and S2 from the elevation–azimuth coordinates of a target. The inset shows the LVM coordinate system (see also Figures 5 and 6).
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) Directing the light off the mount in the elevation–azimuth configuration is unworkable, since the 20 cm beam must penetrate the azimuth drive or head straight up into the sky. (Right) In altitude–altitude configuration, we can send the light along the M2 axis away from the motorized base.
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: An object transiting near zenith imposes no unusual demands on an altitude–altitude mount (top panel). For an elevation–azimuth mount, however, the azimuth tracking rates can become extreme (bottom panel). See text for details.
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: Histogram of slew times to the LVM survey fields. As before, the green marker indicates the measured rms value and the vertical line shows 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: rms scatter around the mean PA during individual spectrograph exposures on MJD 60355. The vertical line indicates the 1.′4 requirement on PA stability, while the green triangle shows the measured rms value.
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 FWHM (blue) and the ambient temperature (red) during 5 hr of observing on the night of MJD 60355. See text for details.