adsabs/AstroCLIMB huggingface dataset:
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 galaxy spectra from the One-Percent Survey (gray). We present spectra of a blue and a red galaxy from the BGS Bright sample and a blue and a red galaxy from the BGS Faint samples (top to bottom panels). In each panel, we also plot the spectrum rebinned to a coarser wavelength grid (black) and the measured uncertainties (orange), and we include the best-fit REDROCK template used to measure the redshift (blue). The redshift measurement, uncertainty, and Δχ 2 from REDROCK are included in the upper right corner, along with the r-band magnitude and fiber magnitude of 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: BGS tiles observed by DESI over its 5 yr of operation according to survey simulations. In each panel, we present BGS tiles that will be observed up to and including that year. BGS will observe a footprint of 14,000 deg2, which will match the footprint of the dark program as closely as possible, with a four-pass strategy. Each point on the footprint will be visited three times on average. For reference, we mark the ecliptic in each panel (black dotted). According to survey simulations, we achieve the 14,000 deg2 footprint with four passes after 4 yr and meet the required 20% operational survey margins.
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 BGS galaxies as a function of r and r fiber magnitudes. We present BGS spectra from SV1 (left) and the One-Percent Survey (right). The color map represents the z success rate; hexbins with >95% redshift success rate are marked with a blue color mapping. For the BGS Bright sample, we find overall >95% redshift success rates. Galaxies with fainter r fiber > 21.5 have lower redshift success rates, as expected. However, even for the small fraction of galaxies with r fiber > 21.5, BGS Bright maintains a ≳90% redshift success rate with the final selection (right). For the BGS Faint sample, the r fiber−color cut in the One-Percent Survey selection excludes galaxies with the lowest redshift success rates in SV1. As a result, the BGS Faint sample has high redshift success rates (>90%) throughout its entire r−r fiber range.
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 as a function of r-band magnitude for galaxies in the One-Percent Survey observations (blue). The z success rates are estimated using the criteria listed in Section 5.3 and only include spectra from exposures that correspond to t nom ∼ 180 s. The error bars represent the Poisson uncertainties for each magnitude bin. We mark the r = 19.5 mag cut that separates the BGS Bright and Faint samples (black dashed). We include the z success rate for SV1 galaxies, excluding the Low Quality class, for reference. BGS galaxies in SV1 are more broadly selected than in the final target selection. We achieve z success rate >95% for the entire BGS sample throughout its full r magnitude range. We achieve overall z success rates of 98.4% and 97.9% for BGS Bright and Faint, respectively, in the One-Percent Survey.
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: Fiber assignment efficiency of BGS Bright (blue) and Faint (orange) as a function of the number of passes. BGS will be observed with four passes; each position in the footprint will be visited on average three times to ensure the required completeness. The BGS Bright targets and 20% of the BGS Faint targets (orange dotted–dashed) are assigned fibers with the highest priority during bright time. The rest of the BGS Faint targets are assigned lower priorities (orange dotted). We assign higher priorities to a fraction of BGS Faint targets to facilitate corrections for fiber assignment incompleteness in future clustering analyses. The fiber assignment efficiencies are estimated for the focal plane condition as of 2021 October, where 4174 of 5000 fiber positioners are available for science targets. Some of the remaining malfunctioning positioners are used to meet the sky fiber budget. Even if the number of functional positioners does not increase in the future, with four passes we achieve the 80% fiber assignment efficiency requirement for BGS Bright.
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 BGS Bright galaxies from SV1 (left) and the One-Percent Survey (right) as a function of g − r and r − z colors. The top panels include galaxies with 0.0 < z < 0.2; the bottom panels include galaxies with 0.2 < z < 0.6. For reference, we mark the 68th and 95th percentiles of the color distribution of One-Percent Survey BGS Bright galaxies (white contours). The color map represents the z success rate, where redshift success rates above >95% are marked with a blue color mapping. We find slightly lower redshift success rates in the bluest galaxies (g − r < 0.4) because they are systematically fainter. Overall, we find a >90% redshift success rate throughout the color space and no strong color dependence for the One-Percent Survey.
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: Comparison of BGS redshifts to GAMA redshifts for BGS galaxies from the SV1 (green), One-Percent Survey (blue), and main survey (orange) that are also in GAMA. In the top panel, we plot GAMA redshift, z GAMA, vs. BGS redshift, z BGS. In the bottom panels, we plot the fractional redshift residual, Δz/(1 + z BGS), as a function of z BGS (left) and the normalized histogram of Δz/(1 + z BGS) (right). The comparison only includes high-quality GAMA redshifts with quality flag NQ > 2. Of the ∼25,000 overlapping BGS galaxies, 99.7% have ∣Δz/(1 + z BGS)∣ < 0.001. The scatter in the redshift difference between BGS and GAMA is small: σ Δz  = 43 km s−1. BGS redshifts show excellent overall agreement with GAMA redshifts.
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 as a function of “survey speed” for all BGS galaxies in the One-Percent Survey (blue) and main survey (orange). We also include the redshift success rate for the BGS Bright sample from SV1 (green dashed). Survey speed is used to determine whether to observe the bright-time, dark-time, or BACKUP program and is estimated by the Exposure Time Calculator. It is derived from seeing, transparency, air mass, and sky brightness of the exposure and serves as a metric for the observing conditions. The BGS survey speed boundaries are currently defined to be ﹩[\tfrac{1}{6},0.4]﹩. BGS achieves a redshift success rate above the required >95% threshold throughout its entire survey speed range.
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 the BGS Faint sample as a function of r fiber and (z − W1) − 1.2(g − r) + 1.2 color from the SV1 (left) and the One-Percent Survey (right) observations. We mark the r fiber−color BGS Faint selection in black dashed and represent the redshift success rate with the color map. The SV1 BGS Faint sample (left) is selected using only a 19.5 mag < r < 20.0 mag cut instead of the r fiber−color selection. The redshift success rate of SV1 galaxies outside the r fiber−color cut illustrates that the BGS Faint selection is effective at excluding objects with low redshift success and produces a sample with high redshift efficiency.
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 distribution of BGS galaxies from SV1 (hashed) and the One-Percent Survey (solid). We present the distributions of the BGS Bright and Faint galaxies in the left and right panels, respectively. The success of BGS targeting delivers galaxies in the desired redshift range, 0.0 < z < 0.6. The Bright and Faint samples have median redshifts of z ∼ 0.2 and 0.3, respectively. During ∼5 months of SV observations, DESI amassed 286,934 BGS Bright and 202,590 Faint BGS redshifts at an average rate of ≃4200 per 20-minute exposure. The BGS Bright sample from SV already exceeds the number of redshifts in GAMA DR4 (dotted–dashed). Over the course of the next 5 yr, BGS will expand to an unprecedented >10 million spectra over a third of the sky.
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 purity (solid) as a function of the REDROCK Δχ 2 threshold for the redshift success definition of the BGS Bright (blue) and Faint (orange) samples. We also present the redshift completeness, the fraction of successful redshifts included for a given Δχ 2 threshold. We assess redshift success according to the criteria listed in Section 5.3 based on redshifts measured from corresponding deep exposures. The Δχ 2 > 40 threshold we impose to determine redshift success results in a BGS Bright sample with >99.5% purity and >99% completeness.
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: Comoving number density distribution, ﹩\bar{n}(z)﹩, of BGS galaxies from the EDR (black; SV1 and the One-Percent Survey). We plot ﹩\bar{n}(z)﹩ for BGS Bright (blue) and Faint (orange). We show external data sets of interest, SDSS (dashed), BOSS (dotted), and GAMA DR4 (dashed–dotted), and DESI LRGs (red) in the overlapping range. BGS will provide the highest-density cosmological galaxy sample to date at low redshifts. It will provide maximum leverage against higher-redshift measurements and CMB constraints for dark energy constraints. Furthermore, its high density and broad galaxy selection will enable a wide range of new approaches to galaxy clustering and galaxy evolution studies.
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:  r fib vs. r distribution of SV1 targets in the “Bright” (blue), “Faint” (orange), “Faint extended” (red), and “Faint extended fiber magnitude” (purple) target classes. We mark the r and r fib limits of the target classes in black dashed. Target selection for SV1 was designed to test the star–galaxy separation, BGS Faint sample selection, and quality cuts. Therefore, the SV1 selection, which we present in Appendix A, is overall a more relaxed version of the final BGS target selection (Section 3).