adsabs/AstroCLIMB huggingface dataset:
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: Targeting accuracy for DESI fiber robots over a 2.5 week period of survey operations, during which the Focal Plane System acquired more than 1.2 million targets. During this period, we operated with code that corrects some of the dome turbulence effects in the FVC measurement. This reduced the positioning error to 6 μm rms (prior performance was 9 μm rms, as shown in Figure 4).
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: Best-fit errors for a calibration measurement of 4252 positioner robots, performed in 2020 December. For each positioner, transformation parameters between (θ, ϕ) and (x, y) coordinates were calculated so as to minimize the error between measured and predicted fiber locations. The minimization in this case was done on a data set of 62 points per robot. The left plot shows the distribution of the transformation’s overall fit error for each unit (6.5 μm rms). The middle and right plots show errors on the six key kinematic parameters independently. “R1” and “R2” are respectively the kinematic arm lengths between central (θ) and eccentric (ϕ) axes, and between the eccentric axis and fiber. “Xo” and “Yo” are the location of the central axis on the focal plane. “To” and “Po” are angular zero-points for the θ and ϕ axes, respectively. The Xo and Yo fit errors are effectively a measure of FVC measurement precision.
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: Left: we selected the pattern of guider versus wave front cameras (indicated by “G” and “W”) to maximize spacing of the wave front measurements, since they must control the tip/tilt degrees of freedom of the hexapod. Middle and right: at the interfaces between software systems—such as move scheduling (Section 3.3) and PlateMaker (Section 3.5)—we use a modified polar coordinate system (Q, S), where “S” is the distance along the aspheric focal surface within a plane that intersects the optical axis and is at angle “Q” with respect to the cartesian coordinates of the focal plane (X5, Y5, Z5). By matching the natural geometry of the focal surface, the coordinate system removed several possible sources of ambiguity between developers.
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: Fiber positioner robots are shown packed together on the focal plate. In addition to the fiber ferrule, each ϕ arm has a light-trap hole with a dark dye. The original concept for these light traps was to be able to selectively extinguish bright stars in the field; in practice, they have been most useful for identifying ϕ angles during hardware debugging. A projecting tab feature on each ferrule holder provides a simple but effective hard limit against clockwise overextension.
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: This diagram shows the location of the focal plane system components as installed on the Mayall telescope. The focal plate assembly, which contains all robotic fiber positioners, guide and focus cameras, and fiducial sources, is mounted to the prime focus corrector. The FVC is mounted behind the primary mirror and measures the positions of the backlit fibers, as well as the fixed fiducials interspersed throughout the array.
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 DESI fiber positioner robot is designed for a minimum 10.4 mm pitch between neighboring units. It has two rotational axes, driven by independent ø 4 mm 337:1 gearmotors. Drive electronics are integrated into a board mounted to the aft end. The assembly consists of 22 parts and 10 fasteners. The design was developed at LBNL and SSL, and mass-produced by UM and EPFL.
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: Layout of the focal plate. Left: the envelopes were iteratively squeezed together, with three key constraints: fiber tips stay on the asphere, the central axis matches the chief ray, and the pattern along one edge of the 36° petal is a straight line (see Section 2.2). Right: an axisymmetric tolerance envelope was defined by five conical sections.
Paper: Close Trans-Neptunian Object Passages as a Driver of the Origin and Evolution of Ultrawide Kuiper Belt Binaries
Authors: Hunter M. Campbell, Lukas R. Stone, Nathan A. Kaib
Figure caption: Separation (R  H  percentage) vs. time (millions of years) of a simulated binary. This is an example of a binary starting with a separation under 5% R  H  but is eventually widened to beyond that of 2001 QW322. For comparison are the current separations (in relative Hill radii) of the binaries 2001 QW322 (22% H  R ), 2000 CF105 (17% H  R ), and 2006 JZ81 (9% H  R ). This wide separation does not last as the binary is lost at around 3.8 Gyr.
Paper: Close Trans-Neptunian Object Passages as a Driver of the Origin and Evolution of Ultrawide Kuiper Belt Binaries
Authors: Hunter M. Campbell, Lukas R. Stone, Nathan A. Kaib
Figure caption: The three zones around a binary system. Bodies with an encounter separation between 4 and 8 R  H  must have a greater mass than 1.1 × 1020 kg. Bodies with an encounter separation between 4 and 1 R  H  must have a greater mass than 2.6 × 1017 kg. Bodies of any mass can pass closer than 1 R  H .
Paper: Close Trans-Neptunian Object Passages as a Driver of the Origin and Evolution of Ultrawide Kuiper Belt Binaries
Authors: Hunter M. Campbell, Lukas R. Stone, Nathan A. Kaib
Figure caption: The dark gray curves are the percentage of surviving binaries over time whose initial separation is that of 2000 CF105, starting at 100. The blue dotted line represents a fit exponential decay curve. Each panel represents the different Kuiper Belt parameters simulated and includes a box showing the average binary lifetime in that SFD. B  r  is the break radius of the dynamically hot populations and α is the albedo of the CCB.
Paper: Close Trans-Neptunian Object Passages as a Driver of the Origin and Evolution of Ultrawide Kuiper Belt Binaries
Authors: Hunter M. Campbell, Lukas R. Stone, Nathan A. Kaib
Figure caption: A cumulative distribution of the separations of each sampled binary. A line is drawn at 7% Hill radius as this marks where a binary becomes ultrawide. Each panel represents a Kuiper Belt SFD we have modeled; in none of them does the fraction of ultrawide binaries rise over 2%.
Paper: Close Trans-Neptunian Object Passages as a Driver of the Origin and Evolution of Ultrawide Kuiper Belt Binaries
Authors: Hunter M. Campbell, Lukas R. Stone, Nathan A. Kaib
Figure caption: The combined probability density of encounter speeds for a CCB binary from each TNO population. Also plotted are the individual component population speeds with the resonant populations merged into one.
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 magnitude of the centroiding variance when the turbulence is high (left) and low (right). The highest turbulence occurs when the DESI focal plane is imaged with the dome closed, mirror cooling fans running, and the dome air temperature very different from the mirror temperature. The lowest turbulence occurs with the dome open, cooling fans off, and the mirror temperature matching the air temperature. The small dots in these maps show the location of each measured source in the FVC image (∼5500 sources). The brightness of each dot scales with the variance of the respective source position, determined from 10 repeated observations over a short time interval. Only the variance in the horizontal direction is represented, but the variance in the vertical direction is similar. The high turbulence map shows regions in the image where the variance is as high as 50 millipixels (∼160 μm pixel−1 at the focal surface), depending on the location in the field. The median is 30 millipixels. When the turbulence is low, the peak and median variance fall to 30 and 18 millipixels, respectively.
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: A sample guide camera image of a region with high stellar density and dust. White squares highlight the stars automatically selected for real-time monitoring of the atmospheric transparency and fiber acceptance fraction. The data was captured with a 10 s exposure on 2019 November 3.