adsabs/AstroCLIMB huggingface dataset:
Paper: The Target-selection Pipeline for the Dark Energy Spectroscopic Instrument
Authors: Adam D. Myers, John Moustakas, Stephen Bailey, Benjamin A. Weaver, Andrew P. Cooper, Jaime E. Forero-Romero, Bela Abolfathi, David M. Alexander, David Brooks, Edmond Chaussidon, Chia-Hsun Chuang, Kyle Dawson, Arjun Dey, Biprateep Dey, Govinda Dhungana, Peter Doel, Kevin Fanning, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma X. Gonzalez-Morales, ChangHoon Hahn, Hiram K. Herrera-Alcantar, Klaus Honscheid, Mustapha Ishak, Tanveer Karim, David Kirkby, Theodore Kisner, Sergey E. Koposov, Anthony Kremin, Ting-Wen Lan, Martin Landriau, Dustin Lang, Michael E. Levi, Christophe Magneville, Lucas Napolitano, Paul Martini, Aaron Meisner, Jeffrey A. Newman, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Edward F. Schlafly, David Schlegel, Michael Schubnell, Ting Tan, Gregory Tarle, Michael J. Wilson, Christophe Yèche, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Example blank-sky locations. Crosses depict supplemental sky locations (SUPP_SKY; see Section 4.4.2). Large blue circles represent masks around bright stars, and red diamonds depict “safe” locations generated when a SUPP_SKY falls in a mask (BAD_SKY; see Section 4.4.4). SUPP_SKY locations in masks are not discarded, but have the IN_BRIGHT_OBJECT bit set (green circles). The masks in the top-right corner demonstrate how safe locations that have both BAD_SKY and IN_BRIGHT_OBJECT set are discarded: safe (BAD_SKY) locations were generated around the left-hand star mask based on a SUPP_SKY in that mask, but half fell in the right-hand star mask and so were discarded.
Paper: The Target-selection Pipeline for the Dark Energy Spectroscopic Instrument
Authors: Adam D. Myers, John Moustakas, Stephen Bailey, Benjamin A. Weaver, Andrew P. Cooper, Jaime E. Forero-Romero, Bela Abolfathi, David M. Alexander, David Brooks, Edmond Chaussidon, Chia-Hsun Chuang, Kyle Dawson, Arjun Dey, Biprateep Dey, Govinda Dhungana, Peter Doel, Kevin Fanning, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma X. Gonzalez-Morales, ChangHoon Hahn, Hiram K. Herrera-Alcantar, Klaus Honscheid, Mustapha Ishak, Tanveer Karim, David Kirkby, Theodore Kisner, Sergey E. Koposov, Anthony Kremin, Ting-Wen Lan, Martin Landriau, Dustin Lang, Michael E. Levi, Christophe Magneville, Lucas Napolitano, Paul Martini, Aaron Meisner, Jeffrey A. Newman, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Edward F. Schlafly, David Schlegel, Michael Schubnell, Ting Tan, Gregory Tarle, Michael J. Wilson, Christophe Yèche, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: An example use of the desitarget “allsky” random catalogs. Colors distinguish different numbers of g-band observations in DR9 of the Legacy Surveys. For instance, areas colored green (pink) were covered by two (≥5) observations. Areas that have zero observations because they are outside of the Legacy Surveys are immediately obvious, as is the lower coverage near the edge of the footprint. The division between BASS and MzLS at a decl. of ∼32.°375 is also apparent (see also Section 4.1.3). It is trivial to use these random catalogs to characterize how much area in the Legacy Surveys match specified observational criteria.
Paper: The Target-selection Pipeline for the Dark Energy Spectroscopic Instrument
Authors: Adam D. Myers, John Moustakas, Stephen Bailey, Benjamin A. Weaver, Andrew P. Cooper, Jaime E. Forero-Romero, Bela Abolfathi, David M. Alexander, David Brooks, Edmond Chaussidon, Chia-Hsun Chuang, Kyle Dawson, Arjun Dey, Biprateep Dey, Govinda Dhungana, Peter Doel, Kevin Fanning, Enrique Gaztañaga, Satya Gontcho A Gontcho, Alma X. Gonzalez-Morales, ChangHoon Hahn, Hiram K. Herrera-Alcantar, Klaus Honscheid, Mustapha Ishak, Tanveer Karim, David Kirkby, Theodore Kisner, Sergey E. Koposov, Anthony Kremin, Ting-Wen Lan, Martin Landriau, Dustin Lang, Michael E. Levi, Christophe Magneville, Lucas Napolitano, Paul Martini, Aaron Meisner, Jeffrey A. Newman, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Edward F. Schlafly, David Schlegel, Michael Schubnell, Ting Tan, Gregory Tarle, Michael J. Wilson, Christophe Yèche, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Example quality assurance diagnostic plots derived from running the desitarget code base on DR9 of the Legacy Surveys. Left panel: number density contours for DESI Main Survey LRG (dark-time) targets in an optical color (r − z) compared to the 3.4 and 4.6 μm bands (W1 − W2) from the WISE survey. Right panel: density of all SV3 BGS targets in equatorial coordinates. The solid black line depicts the plane of our Galaxy and the red dotted line depicts the ecliptic.
Paper: KIC 7284688: A Solar-type Eclipsing Binary with Rapidly Varying O’Connell Effect
Authors: Yang Pan, Xiaobin Zhang
Figure caption: Left panel: top panel: the phased Kepler light curve and the best-fit WD model. Second panel: the residuals after fitting the Kepler light curve. Third panel: the phased RVs of the primary (blue points), the secondary (green points), the third component (red triangles), and the best-fit WD model (red solid lines). The systemic velocities of the binary are indicated by black dashed line. Bottom panel: the residuals after fitting the primary and the secondary RVs. Right panel: top panel: the phased TESS light curves from Sector 15 (black points), 40 (black squares), 41 (black diamonds), 54 (black stars), 55 (black pluses), and the best-fit WD models (red solid lines). For better visualization, the normalized light curves are shifted up and down by 0.1 for sectors 15, 55, and by 0.05 for sectors 40, 54, respectively. Second panel: the corresponding residuals after fitting the TESS light curves. Third panel: the phased RVs of the primary (blue points), the secondary (green points), the third component (red triangles), and the best-fit WD model (red solid lines). The systemic velocities of the binary are indicated by black dashed line. Bottom panel: the residuals after fitting the primary and the secondary RVs.
Paper: KIC 7284688: A Solar-type Eclipsing Binary with Rapidly Varying O’Connell Effect
Authors: Yang Pan, Xiaobin Zhang
Figure caption: Left panel: a 12 day segment of the normalized light curve of KIC 7284688 from Q2. The times corresponding to orbital phase at 0.25 and 0.75 are marked by the red and blue dashed lines, respectively. Right panel: the phased Kepler light curve of KIC 7284688 evolving with time represented by the color in the color bar.
Paper: KIC 7284688: A Solar-type Eclipsing Binary with Rapidly Varying O’Connell Effect
Authors: Yang Pan, Xiaobin Zhang
Figure caption: The normalized and phased TESS light curves from Sector 15 (black points), Sector 40 (green squares), Sector 41 (blue diamonds), Sector 54 (red points), Sector 55 (yellow points).
Paper: KIC 7284688: A Solar-type Eclipsing Binary with Rapidly Varying O’Connell Effect
Authors: Yang Pan, Xiaobin Zhang
Figure caption: Left panel: the LS periodogram of the out-of-eclipse residuals for Kepler data (upper panel) and a zoom-in of the LS periodogram around the orbital frequency of the binary (lower panel). Right panel: the LS periodograms of the out-of-eclipse residuals for TESS Sector 15, Sector 40, 41 and Sector 54, 55 (upper panel), and a zoom-in of the LS periodograms around the orbital frequency of the binary (lower panel). The red dashed lines represent the orbital frequency of the binary and orbital harmonics.
Paper: KIC 7284688: A Solar-type Eclipsing Binary with Rapidly Varying O’Connell Effect
Authors: Yang Pan, Xiaobin Zhang
Figure caption: The BF (black points) and the Gaussian fits (red lines). The abscissa is is radial velocity on the heliocentric frame. The vertical axis is arbitrary amplitude of the BF. The orbital phase, and the peaks due to the primary (p), the secondary (s), and the third component (T) are indicated.
Paper: KIC 7284688: A Solar-type Eclipsing Binary with Rapidly Varying O’Connell Effect
Authors: Yang Pan, Xiaobin Zhang
Figure caption: Left panel: the O−C diagram for the primary and secondary eclipses given by KEBC (top panel), the LS periodogram of the primary O−C (middle panel), and the LS periodogram of the secondary O−C (bottom panel). Right panel: the O−C diagram for the primary and secondary eclipses obtained from TESS data.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: Comparison of differences in the H I line profile parameters of the galaxies in our two samples that were detected by us with more than one telescope. Plotted as a function of their average central H I velocity, V H I , are the differences in (a) central H I velocity, ΔV H I  in kilometers per second, (b) in W 50 line width, ΔW 50 in kilometers per second, and (c) in integrated H I line flux, ΔF H I  in Jansky kilometers per second. As indicated in the legend, colors indicate which telescopes’ results are compared: Green Bank (GBT) vs. Nançay (NRT) in black, Arecibo (AO) vs. NRT in blue, AO vs. GBT in red, and NRT (HyperLeda sample) vs. NRT (UGC sample) in green. Different symbols indicate the probability of a detection being confused by another galaxy within a telescope beam: large filled dots for uncontaminated, crosses for possibly contaminated, and small open dots for clearly contaminated. Outliers in all plots are described in Section 4.3 and the Appendix.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: Optical images of target galaxies that were not detected by us in H I. Images are 2 × 2 arcmin in size, unless otherwise indicated in the lower right corner. False color (i, r, and g filter) images are from SDSS DR16 (Ahumada et al. 2020) and black and white images are from DSS2 blue plates (Abazajian et al. 2004), used when DR16 images are not available. Objects are arranged in alphabetical order.
Paper: Searching in H I for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: K. O'Neil, Stephen E. Schneider, W. van Driel, G. Liu, T. Joseph, A. C. Schwortz, Z. Butcher
Figure caption: Distributions of the total H I mass M H I , in solar masses, for all detected galaxies in our survey: (a) comparison between the UGC sample (red) and the HyperLeda sample (gray), and (b) as a function of the telescope(s) which detected the galaxy.
Paper: The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation
Authors: ChangHoon Hahn, Michael J. Wilson, Omar Ruiz-Macias, Shaun Cole, David H. Weinberg, John Moustakas, Anthony Kremin, Jeremy L. Tinker, Alex Smith, Risa H. Wechsler, Steven Ahlen, Shadab Alam, Stephen Bailey, David Brooks, Andrew P. Cooper, Tamara M. Davis, Kyle Dawson, Arjun Dey, Biprateep Dey, Sarah Eftekharzadeh, Daniel J. Eisenstein, Kevin Fanning, Jaime E. Forero-Romero, Carlos S. Frenk, Enrique Gaztañaga, Satya Gontcho A Gontcho, Julien Guy, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Ting-Wen Lan, Martin Landriau, Laurent Le Guillou, Michael E. Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Adam D. Myers, Jundan Nie, Peder Norberg, Nathalie Palanque-Delabrouille, Will J. Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Sasha Gaines, Christoph Saulder, Eddie Schlafly, David Schlegel, David Sierra-Porta, Gregory Tarle, Benjamin A. Weaver, Christophe Yèche, Pauline Zarrouk, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Targets for the BGS Bright sample are chosen based on the selection cuts described in Section 3.1 and an r < 19.5 magnitude cut. In the left panel, we show these cuts (based on fiber magnitude) and the r < 19.5 cut (black dashed) on the distribution of r vs. r fiber magnitude for LS objects that pass our star–galaxy selection (gray). The contours mark the 11.7, 39.3, 67.5, and 86.4 percentiles of the distribution (dotted). We also include the r and r fiber cuts for the BGS Faint sample (dotted–dashed). We impose selection cuts on BGS targets in order to minimize the number of spurious objects and mitigate any systematic effects that can affect galaxy clustering analyses. In the right panel, we present the target density of the BGS Bright targets (color map). In total, we have 864 targets deg–2 for the BGS Bright sample.
Paper: The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation
Authors: ChangHoon Hahn, Michael J. Wilson, Omar Ruiz-Macias, Shaun Cole, David H. Weinberg, John Moustakas, Anthony Kremin, Jeremy L. Tinker, Alex Smith, Risa H. Wechsler, Steven Ahlen, Shadab Alam, Stephen Bailey, David Brooks, Andrew P. Cooper, Tamara M. Davis, Kyle Dawson, Arjun Dey, Biprateep Dey, Sarah Eftekharzadeh, Daniel J. Eisenstein, Kevin Fanning, Jaime E. Forero-Romero, Carlos S. Frenk, Enrique Gaztañaga, Satya Gontcho A Gontcho, Julien Guy, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Ting-Wen Lan, Martin Landriau, Laurent Le Guillou, Michael E. Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Adam D. Myers, Jundan Nie, Peder Norberg, Nathalie Palanque-Delabrouille, Will J. Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Sasha Gaines, Christoph Saulder, Eddie Schlafly, David Schlegel, David Sierra-Porta, Gregory Tarle, Benjamin A. Weaver, Christophe Yèche, Pauline Zarrouk, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Star–galaxy separation in BGS is performed using a G Gaia − r raw cut. This criterion exploits the fact that the Gaia magnitude is measured from space with a diffraction-limited PSF while the LS r magnitude captures the light from the entire source. LS objects (gray) with G Gaia − r raw > 0.6 (black dashed) or objects not in Gaia are classified as galaxies. G Gaia is the G-band magnitude from Gaia DR2; r raw is the LS r-band magnitude without Galactic extinction correction. In the middle and right panels, we present in the color maps the stellar contamination fraction for SV1 and the One-Percent Survey, respectively. The contamination fraction is estimated based on REDROCK spectral type classification and a minimum redshift cut, z > 300 km s−1. We only include hexbins with at least 10 BGS targets. Stellar contamination is negligible (<1%) above our star–galaxy separation threshold.
Paper: The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation
Authors: ChangHoon Hahn, Michael J. Wilson, Omar Ruiz-Macias, Shaun Cole, David H. Weinberg, John Moustakas, Anthony Kremin, Jeremy L. Tinker, Alex Smith, Risa H. Wechsler, Steven Ahlen, Shadab Alam, Stephen Bailey, David Brooks, Andrew P. Cooper, Tamara M. Davis, Kyle Dawson, Arjun Dey, Biprateep Dey, Sarah Eftekharzadeh, Daniel J. Eisenstein, Kevin Fanning, Jaime E. Forero-Romero, Carlos S. Frenk, Enrique Gaztañaga, Satya Gontcho A Gontcho, Julien Guy, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Ting-Wen Lan, Martin Landriau, Laurent Le Guillou, Michael E. Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Adam D. Myers, Jundan Nie, Peder Norberg, Nathalie Palanque-Delabrouille, Will J. Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Sasha Gaines, Christoph Saulder, Eddie Schlafly, David Schlegel, David Sierra-Porta, Gregory Tarle, Benjamin A. Weaver, Christophe Yèche, Pauline Zarrouk, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: The dependence of BGS Bright (blue) and Faint (orange) target densities on different imaging properties: stellar density, galactic extinction, PSF size (in g, r, and z bands), and photometric depth (in g, r, z, W1, and W2 bands). The target densities, η, are divided by the average target density of the samples over the 14,000 deg2 DESI footprint (﹩\bar{\eta };﹩ included in the legend) to highlight variations. The error bars represent the uncertainties on the mean. The histogram in each panel represents the normalized distribution of each imaging property. We find the consistency of Bright and Faint target densities especially encouraging because we use more complex cuts in the latter. Overall, we find <5% variation in the target densities of BGS Bright and Faint samples and no strong systematic dependence on imaging properties.
Paper: The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation
Authors: ChangHoon Hahn, Michael J. Wilson, Omar Ruiz-Macias, Shaun Cole, David H. Weinberg, John Moustakas, Anthony Kremin, Jeremy L. Tinker, Alex Smith, Risa H. Wechsler, Steven Ahlen, Shadab Alam, Stephen Bailey, David Brooks, Andrew P. Cooper, Tamara M. Davis, Kyle Dawson, Arjun Dey, Biprateep Dey, Sarah Eftekharzadeh, Daniel J. Eisenstein, Kevin Fanning, Jaime E. Forero-Romero, Carlos S. Frenk, Enrique Gaztañaga, Satya Gontcho A Gontcho, Julien Guy, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Ting-Wen Lan, Martin Landriau, Laurent Le Guillou, Michael E. Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Adam D. Myers, Jundan Nie, Peder Norberg, Nathalie Palanque-Delabrouille, Will J. Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Sasha Gaines, Christoph Saulder, Eddie Schlafly, David Schlegel, David Sierra-Porta, Gregory Tarle, Benjamin A. Weaver, Christophe Yèche, Pauline Zarrouk, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: BGS Faint targets include objects fainter than BGS Bright, 19.5 mag < r < 20.175 mag, that are within custom r fiber−color selection cuts (Equation (7)). In the left panel, we show the r fiber−color cut (black dashed) on the r fiber vs. (z − W1) − 1.2(g − r) + 1.2 distribution of LS objects that pass our star–galaxy separation (gray). The contours mark the 11.7, 39.3, 67.5, and 86.4 percentiles of the distribution (dotted). Here (z − W1) − 1.2(g − r) + 1.2 is a proxy for the strength of Hα and Hβ, so BGS Faint targets either have bright fiber magnitudes or strong emission lines. We impose the r fiber−color cut in order to maintain high redshift efficiency for BGS Faint. In the right panel, we present the target density of the BGS Faint targets (color map). In total, we have 533 targets deg–2 for the BGS Faint sample.
Paper: The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation
Authors: ChangHoon Hahn, Michael J. Wilson, Omar Ruiz-Macias, Shaun Cole, David H. Weinberg, John Moustakas, Anthony Kremin, Jeremy L. Tinker, Alex Smith, Risa H. Wechsler, Steven Ahlen, Shadab Alam, Stephen Bailey, David Brooks, Andrew P. Cooper, Tamara M. Davis, Kyle Dawson, Arjun Dey, Biprateep Dey, Sarah Eftekharzadeh, Daniel J. Eisenstein, Kevin Fanning, Jaime E. Forero-Romero, Carlos S. Frenk, Enrique Gaztañaga, Satya Gontcho A Gontcho, Julien Guy, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Ting-Wen Lan, Martin Landriau, Laurent Le Guillou, Michael E. Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Adam D. Myers, Jundan Nie, Peder Norberg, Nathalie Palanque-Delabrouille, Will J. Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Sasha Gaines, Christoph Saulder, Eddie Schlafly, David Schlegel, David Sierra-Porta, Gregory Tarle, Benjamin A. Weaver, Christophe Yèche, Pauline Zarrouk, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption:  REDROCK Δχ 2 as a function of best-fit redshift, z Redrock, for BGS Bright (top) and Faint (bottom) galaxies from the SV1 (left) and One-Percent Survey. Δχ 2 and z Redrock are measured using spectra from single BGS-like exposures. We highlight the spectra that have catastrophic redshift discrepancies with the redshift measured from corresponding deep exposures, ∣Δz∣/(1 + z) > 0.0033, in red. Our Δχ 2 > 40 criterion for redshift success (black dashed) excludes the majority of catastrophic redshift failures. Conversely, below the Δχ 2 threshold, ∼30% and ∼15% of BGS Bright and Faint galaxies, respectively, have catastrophic redshift failures.
Paper: The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation
Authors: ChangHoon Hahn, Michael J. Wilson, Omar Ruiz-Macias, Shaun Cole, David H. Weinberg, John Moustakas, Anthony Kremin, Jeremy L. Tinker, Alex Smith, Risa H. Wechsler, Steven Ahlen, Shadab Alam, Stephen Bailey, David Brooks, Andrew P. Cooper, Tamara M. Davis, Kyle Dawson, Arjun Dey, Biprateep Dey, Sarah Eftekharzadeh, Daniel J. Eisenstein, Kevin Fanning, Jaime E. Forero-Romero, Carlos S. Frenk, Enrique Gaztañaga, Satya Gontcho A Gontcho, Julien Guy, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Ting-Wen Lan, Martin Landriau, Laurent Le Guillou, Michael E. Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Adam D. Myers, Jundan Nie, Peder Norberg, Nathalie Palanque-Delabrouille, Will J. Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Sasha Gaines, Christoph Saulder, Eddie Schlafly, David Schlegel, David Sierra-Porta, Gregory Tarle, Benjamin A. Weaver, Christophe Yèche, Pauline Zarrouk, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: The 14,000 deg2 footprint for the DESI BGC (color map). Imaging from the Legacy Surveys DR9 allows the selection of BGS targets over a larger area, approximately 20,000 deg2 (gray). The color map represents the density of BGS Bright targets (Section 3.1). During the SV phases of operations, DESI observed SV1 and the One-Percent Survey to optimize and validate the BGS target selection and survey performance. We mark the tiles observed during SV1 and the One-Percent Survey in red and orange, respectively.
Paper: The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation
Authors: ChangHoon Hahn, Michael J. Wilson, Omar Ruiz-Macias, Shaun Cole, David H. Weinberg, John Moustakas, Anthony Kremin, Jeremy L. Tinker, Alex Smith, Risa H. Wechsler, Steven Ahlen, Shadab Alam, Stephen Bailey, David Brooks, Andrew P. Cooper, Tamara M. Davis, Kyle Dawson, Arjun Dey, Biprateep Dey, Sarah Eftekharzadeh, Daniel J. Eisenstein, Kevin Fanning, Jaime E. Forero-Romero, Carlos S. Frenk, Enrique Gaztañaga, Satya Gontcho A Gontcho, Julien Guy, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Ting-Wen Lan, Martin Landriau, Laurent Le Guillou, Michael E. Levi, Christophe Magneville, Paul Martini, Aaron Meisner, Adam D. Myers, Jundan Nie, Peder Norberg, Nathalie Palanque-Delabrouille, Will J. Percival, Claire Poppett, Francisco Prada, Anand Raichoor, Ashley J. Ross, Sasha Gaines, Christoph Saulder, Eddie Schlafly, David Schlegel, David Sierra-Porta, Gregory Tarle, Benjamin A. Weaver, Christophe Yèche, Pauline Zarrouk, Rongpu Zhou, Zhimin Zhou, Hu Zou
Figure caption: Redshift success rate of spectral simulations run using a nominal exposure time of t nom = 180 s (blue) as a function of r-band magnitude. We include z success rates for spectral simulations run using t nom = 160 (orange dashed) and 240 s (green dashed) for comparison. The overall z success rates of all r < 19.5 galaxies are presented in the legend. These simulations assume spectra based on realistic continuum templates derived from AGES, matched to g, r, z LS photometry, and GAMA emission-line fluxes. They incorporate realistic noise and throughput for BGS observations. With t nom = 180 s, we predict that the BGS Bright sample can achieve an overall redshift success rate of 95%.