adsabs/AstroCLIMB huggingface dataset:
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: A 100 × 100 pixel region of an image from a red camera. The upper panels show the pixel values with the pixels identified as cosmic ray masked out. The bottom panels show the masked pixels at each step of the cosmic-ray identification procedure.
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: Seven 11 × 11 pixel binary structuring elements used to merge disconnected particle tracks with binary closure during the final step of cosmic-ray identification.
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: Relative transmission of a subsample of 10 fibers from the spectrograph SM2 obtained with one exposure of 2 min on the dome screen with LED lamps in the blue, red, and NIR cameras. Each colored curve corresponds to a fiber. The measurement appears noisy, but 12 such exposures are combined to determine the final correction. The spectral features in the blue camera at 3800 and 4400 Å are due to a dip in the reflectivity of the spectrograph collimator mirror at these wavelength, with a profile that varies with the location in the mirror and with the light incidence angle. The variations around 5750 Å and 7500 Å in the red and NIR camera spectra are due to the change of transmission and reflection of the dichroics again with the light incidence angle that varies with the fiber location in the pseudoslit. Spectral regions affected by cosmic-ray hits have been masked and are interpolated over in the figures.
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: Extraction bias from using overlapping subregions for fibers 25 and 29 of the r1 CCD. The top plot shows the subregion extracted flux (solid colored) overlayed with the full extraction (dotted black). Bottom shows the difference normalized by the statistical error of the extractions. Although there is systematic ringing at the subregion boundaries, it is below 5% of the statistical error.
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: Measurement bias if fitting a model directly to data without using the resolution matrix. The upper plot shows a 200 Å region of a raw extracted sky spectrum. The bottom plot blue line shows the resolution matrix R normalization vs. wavelength. Orange and green lines show the normalization convolved with an input [O III]-like Lorentzian or a [O II]-like double Gaussian.
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: Focal plane view of the median flux in fibers from a twilight observation (exposure No. 00055559 from 2020 March 15) after applying the nightly averaged fiber flat correction (see Section 4.6.2) and a normalization factor per camera (blue, red, and NIR cameras from left to right). The color scales have been saturated to enhance the residual gradient. This figure highlights the agreement between cameras, demonstrating this twilight flat is very nearly achromatic.
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: illumination pattern on the focal plane for one calibration lamp. Right: illumination pattern obtained with four calibration lamps divided by the illumination from the sky. The nonhomogeneity of the illumination ratio is purely radial, with a variation of about 1% from the center to the edge of the focal plane.
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: Illustration of a subregion of 2D extractions. See text for details.
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: Variance and correlation of 2D extractions of 10,000 noise realizations of CCD images of a spectrum. The upper plot shows that the wavelengths bins have uncorrelated noise, while the lower 3 plots show the excellent agreement with the reported variance. The second from the bottom plot shows the statistical uncertainty of the variance of 10,000 simulations in thin gray lines.
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: Transmission of a subsample of fibers from spectrograph SM2 normalized to the average transmission of all the fibers from the 10 spectrographs. These curves are the result of the combination of 12 individual fiber flats as shown in Figure 24, but with a different normalization (average of 10 spectrographs instead of one).
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: 2D flux extractions compared to resolution-convolved input for 10,000 noise realizations of simulated CCD images.
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: Dispersion of the spectral residuals in sky fibers as a function of wavelength. The value at each wavelength is the rms of the residuals in all the sky fibers from all spectrographs, and for several exposures of 1000 ± 10 s. The gray band is the expected noise rms from Equation (16), in the ideal case with ϵ  λ  = 0 (but accounting for the flat field and sky model statistical uncertainties). The colored curves are the measured rms, the colors indicating when the variance exceeds the expected noise. The top panel is the full spectral range of the NIR camera, whereas the lower panels focus on some narrower wavelength ranges. There is naturally a larger rms on the lines because of the Poisson noise, but the measurements also exhibit deviations due to systematic errors in the flat field, wavelength calibration, or PSF shape.
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: Flat-fielded night sky background variation in the r-camera as a function of the distance from the focal plane center. This figure has been obtained by averaging the sky spectra of all sky fibers from 4 nights of observations. The rms of 1%–1.5% comprises the measurement statistical errors, the residual contamination for stars, and systematic errors in the spectroscopic measurements. The radial variation is due to a difference in the vignetting between the sky and the calibrations with the dome screen.
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: Top: zoom on a few NIR lines of the sky model spectrum derived from a 900 s science exposure with 80 sky fibers. The blue curve is the deconvolved spectrum (S), and the orange the reconvolved spectrum ﹩\tilde{S}={RS}﹩. Bottom: correlation coefficients (﹩\equiv {C}_{i,i+{\rm{\Delta }}}/\sqrt{{C}_{i,i}{C}_{i+{\rm{\Delta }},i+{\rm{\Delta }}}}﹩ with C the covariance matrix) of neighboring flux values in the same spectrum. The neighboring fluxes (Δ = 1) on the deconvolved spectrum are highly anticorrelated with a coefficient of about −0.8, whereas the correlations in the reconvolved spectrum never exceed a few percent.
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: A typical standard star spectrum from an exposure of 900 s (colored curves) along with the best-fit model (black curve). The upper panel shows the full spectrum while the lower panels present zooms in various wavelength range. For these, the model has been renormalized to better fit the data and highlight the agreement on the absorption lines.
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: Flat field variation of the central fiber of the SM10 blue camera as a function of the humidity in the spectrographs’ enclosure. Left: wavelength shift of the feature. Right: fiber flat as a function of wavelength (normalized to the average of the 500 fibers for this camera).
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: Histogram of the multiplicative correction term applied in the sky subtraction per camera for a 900 s sky exposure. There is one entry per fiber. Measurements with statistical uncertainties (σ in the legend) larger than 0.03 were discarded.
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: Projections of the 3D stellar parameter grid as a function of effective temperature (T eff), surface gravity (﹩{\mathrm{log}}_{10}g﹩), and iron abundance ([Fe/H]). Models satisfying the color selection cuts for the DESI standard stars are marked as orange dots while the others are in blue.