adsabs/AstroCLIMB huggingface dataset:
Paper: Localizing Sources of Variability in Crowded TESS Photometry
Authors: Michael E. Higgins, Keaton J. Bell
Figure caption: Same as Figure 6, but for the four frequencies that are shared between the two stars.
Paper: Localizing Sources of Variability in Crowded TESS Photometry
Authors: Michael E. Higgins, Keaton J. Bell
Figure caption: Fraction of source star fits with significant detections at the S/N levels presented in Figure 2. Fits with relative amplitude errors less than 20% are considered significant.
Paper: Localizing Sources of Variability in Crowded TESS Photometry
Authors: Michael E. Higgins, Keaton J. Bell
Figure caption: Average distance between the fitted location and the true location of two stars as a function of their simulated separation (in pixels) for the four frequencies unique to star 1. The result is consistently fit to the correct location of star 1.
Paper: Localizing Sources of Variability in Crowded TESS Photometry
Authors: Michael E. Higgins, Keaton J. Bell
Figure caption: Same as Figure 2, but as a function of the distance of the variable star from the edge of the TPF.
Paper: Localizing Sources of Variability in Crowded TESS Photometry
Authors: Michael E. Higgins, Keaton J. Bell
Figure caption: Same as Figure 2 for both the X- and Y-directions as a function of the separation between the source star and the non-source star.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: PSF stability measurement. Each dot on the figures is the variation of a property of the PSF from exposure to exposure (i.e., current value minus average overexposures) for a given exposure, fiber, and wavelength. The properties are, from top to bottom, the variation of the PSF center along X (fiber direction) or Y (wavelength direction), the relative change of PSF width along X and Y, and finally the variation of emission line flux bias (Equation (4)). The fibers and wavelength were chosen to cover evenly the active region of the CCD, excluding regions at short and long wavelength for each camera where the statistical noise is too large. Fibers 10, 100, 200, 300, 400, 490 are shown, and the wavelength are respectively in the range 3860–5650 Å, 5900–7500 Å, and 7700–9500 Å, for the blue, red, and NIR cameras. The PSF model of the spectrograph SM10 are shown. The calibration exposures are from the nights of 2020 March 13, 14, and 15. Note that the fiber positioners were moved during the nights, so the variations from night to night are a test of the stability with positioner moves. Also, the dome was moved between the calibration observations of March 13, so the stability of the PSF during this sequence is a test of the stability with the change of telescope pointing (because the calibration screen the telescope is pointing to is attached to the dome).
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Radial velocity offsets of stars with respect to the measurements in the SoS catalog (Tsantaki et al. 2022) computed separately for each arm of the instrument. The left panel shows the histogram of radial velocity offsets in DESI Survey Validation data. The B (blue), R (red), and Z (for NIR) median offsets are of 0.97, 2.13, and 2.88 km s−1 respectively, and the median absolute deviations are of 4.2, 3.7, and 3.5 km s−1. The right panel shows the radial velocity offsets on the y-axis, in kilometers per second, as a function of the MJD of observation.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Left: a 150 × 150 pixel region showing the inverse variance derived from the individual pixel values for a 1200 s dark-time exposure in a red camera CCD. Right: same pixel area with the inverse variance model used for the data processing. Spectral traces appear dark as the Poisson noise is larger, and so the inverse of the variance smaller. Note the model has much lower noise. The residual spatial noise is coming from the pixel flat field. Note also that the inverse variance on cosmic rays and bright fibers is preserved.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Spectra from arc-lamp exposures in the blue, red, and NIR camera CCDs, from top to bottom. The y-axis gives the average number of electron per pixel, for each row of a vertical band covering fibers 250–274. The blue curve is the data, and the orange dashed curve the best-fit model from the PSF fit. The full wavelength range accessible for each camera is shown.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Cross-dispersion profile from arc-lamp exposures in the blue, red, and NIR camera CCDs, from top to bottom. The y-axis gives the average number of electron per pixel, for each column of a narrow band centered on the brightest emission line in the central region of the CCD. The blue curve is the data, and the orange dashed curve the best-fit model from the PSF fit. Both linear and log-scale graphs are shown to highlight the agreement of the PSF model with data in the core and tails of the PSF.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Left: a 300 × 300 pixel region showing the average of a series of images obtained with the flat field slit for the red camera of spectrograph SM8. Right: the pixel flat field correction derived from the image. The range of scales is ±20% in the left panel and only ±5% in the right panel. A lighter gray corresponds to a higher efficiency. The vertical strips on the left panel are caused by small variations in the slit width. The gradient from top to bottom is due to spectral variations in the illumination.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Variations of the spectral traces’ coordinates with time for the three cameras of spectrograph SM2. Variation along X (direction of fiber number, left panels) for the blue cameras are the largest with peak to peak variations of ±0.7 pixel and an r.m.s of 0.3 pixel. The variations are smaller in the red and NIR cameras (0.15 and 0.03 pixels rms for X, respectively). The rms variation along the y-axis (direction of wavelength dispersion, right panels) is about 0.05 pixel rms for all cameras. This would represent a wavelength calibration error of about 0.03 Å if not corrected.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Example PSF of a central fiber (No. 260) at 7034.3 Å in a red camera CCD. From top left to bottom right: 2D PSF model, PSF model integrated in pixels, arc-lamp image where PSF from neighboring fibers is visible, and cross-dispersion profile of the PSF.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Spectrograph PSF FWHM in the blue, red, and NIR cameras, in units of CCD pixel (the pixel size is 15 μm). This is the width of a slice of the PSF along the dispersion axis, and it is not convolved with the pixel size, so this is different from the line-spread function FWHM. This PSF width as to be compared with the diameter the fiber tip image of 3.4 pixel. The solid curves are the average PSF widths, and the dotted curves the minimum and maximum PSF widths.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Templates ﹩\sqrt{\left\langle {\left(\delta F\right)}^{2}\right\rangle }﹩ used to compute the TSNR values for LRG, ELG, QSO, Lyα, and BGS targets (see Table 2 for the redshift ranges).
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: The average residuals (black) to WD spectra observed by the three spectroscopic arms of DESI and fitted by the WD pipeline (Cooper et al. 2022). The gray shaded region indicates the wavelength range over which each model was scaled to the WD b-arm spectrum. Orange tabs denote the wavelengths of the Balmer and Paschen lines, in particular highlighting the Balmer jump around where the largest discrepancy in the residuals is observed.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: White dwarf spectra observed by DESI showing the individual b- (blue), r- (orange), and z- (red) arm spectra and best-fitted models from the WD pipeline (Cooper et al. 2022) shown in gray, which have been scaled by a constant factor by normalizing to the region shaded in gray.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Ratio of spectroscopic to imaging r-band flux for the targets from several main survey dark-time tiles. The top panels compare the total flux, which is only valid for point sources for DESI. The lower panels compare the fiber fluxes, which are consistent between spectroscopy and imaging for both point sources (in orange) and extended sources (in blue). The x-axis is the imaging fiber magnitude on the left panels and the fraction of light in the fiber aperture on the right panels.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Comparison of the LRG TSNR2 per exposure and the corresponding Δχ 2 from Redrock. Each dot corresponds to one exposure; both the TSNR2 and Δχ 2 values are the median over the LRG target spectra observed during that exposure. The vertical dashed line indicates the TSNR2 value, which corresponds to an effective time of 1000 s.
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: Measured cross talk between fibers N and N + 1 (top) or N + 2 (bottom) for all 30 CCD cameras, as a function of wavelength, for a central fiber (N ∼ 250).
Paper: The Spectroscopic Data Processing Pipeline for the Dark Energy Spectroscopic Instrument
Authors: J. Guy, S. Bailey, A. Kremin, Shadab Alam, D. M. Alexander, C. Allende Prieto, S. BenZvi, A. S. Bolton, D. Brooks, E. Chaussidon, A. P. Cooper, K. Dawson, A. de la Macorra, A. Dey, Biprateep Dey, G. Dhungana, D. J. Eisenstein, A. Font-Ribera, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, D. Green, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, Sergey E. Koposov, Ting-Wen Lan, M. Landriau, L. Le Guillou, Michael E. Levi, C. Magneville, Christopher J. Manser, P. Martini, Aaron M. Meisner, R. Miquel, J. Moustakas, Adam D. Myers, Jeffrey A. Newman, Jundan Nie, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, C. Ravoux, A. J. Ross, E. F. Schlafly, D. Schlegel, M. Schubnell, Ray M. Sharples, Gregory Tarlé, B. A. Weaver, Christophe Yéche, Rongpu Zhou, Zhimin Zhou, H. Zou
Figure caption: For left to right, average ratio of the spectroscopic to imaging flux of standard stars in the blue (4500–5500 Å), red (6000–7300 Å), and NIR (8500–9800 Å) as a function of focal plane coordinates.