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Archetype-based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey

Abhijeet AnandLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]J. GuyLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]S. BaileyLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]John MoustakasDepartment of Physics and Astronomy, Siena College, 515 Loudon Road, Loudonville, NY 12211, USAJ. AguilarLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]S. AhlenPhysics Dept., Boston University, 590 Commonwealth Avenue, Boston, MA 02215, USAA. BoltonNSF NOIRLab, 950 N. Cherry Avenue, Tucson, AZ 85719, USAA. BrodzellerDepartment of Physics and Astronomy, The University of Utah, 115 South 1400 East, Salt Lake City, UT 84112, USADavid BrooksDepartment of Physics & Astronomy, University College London, Gower Street, London, WC1E 6BT, UKT. ClaybaughLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]Shaun ColeInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, UKAxel de la MacorraInstituto de Física, Universidad Nacional Autónoma de México, Cd. de México C.P. 04510, MéxicoBiprateep DeyDepartment of Physics & Astronomy and Pittsburgh Particle Physics, Astrophysics, and Cosmology Center (PITT PACC), University of Pittsburgh, 3941 O’Hara Street, Pittsburgh, PA 15260, USAK. FanningKavli Institute for Particle Astrophysics and Cosmology, Stanford University, Menlo Park, CA 94305, USAJ. E. Forero-RomeroDepartamento de Física, Universidad de los Andes, Cra. 1 No. 18A-10, Edificio Ip, CP 111711, Bogotá, ColombiaE. GaztañagaInstitut d’Estudis Espacials de Catalunya (IEEC), 08034 Barcelona, SpainSatya Gontcho A GontchoLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]G. GutiérrezFermi National Accelerator Laboratory, PO Box 500, Batavia, IL 60510, USAK. HonscheidCenter for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, OH 43210, USACullan HowlettSchool of Mathematics and Physics, University of Queensland, 4072, AustraliaS. JuneauNSF NOIRLab, 950 N. Cherry Avenue, Tucson, AZ 85719, USAD. KirkbyDepartment of Physics and Astronomy, University of California, Irvine, 92697, USATheodore KisnerLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]Anthony KreminLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]Andrew LambertLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]Martin LandriauLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]L. Le GuillouSorbonne Université, CNRS/IN2P3, Laboratoire de Physique Nucléaire et de Hautes Energies (LPNHE), FR-75005 Paris, FranceMarc ManeraDepartament de Física, Serra Húnter, Universitat Autònoma de Barcelona, 08193 Bellaterra (Barcelona), SpainAaron MeisnerNSF NOIRLab, 950 N. Cherry Avenue, Tucson, AZ 85719, USAR. MiquelInstitució Catalana de Recerca i Estudis Avançats, Passeig de Lluís Companys, 23, 08010 Barcelona, SpainEva-Maria MuellerDepartment of Physics and Astronomy, University of Sussex, Brighton BN1 9QH, UKGustavo NizDepartamento de Física, Universidad de Guanajuato—DCI, C.P. 37150, Leon, Guanajuato, MéxicoN. Palanque‐DelabrouilleIRFU, CEA, Université Paris-Saclay, F-91191 Gif-sur-Yvette, FranceWill J. PercivalDepartment of Physics and Astronomy, University of Waterloo, 200 University Avenue W, Waterloo, ON N2L 3G1, CanadaClaire PoppettLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]Francisco PradaInstituto de Astrofísica de Andalucía (CSIC), Glorieta de la Astronomía, s/n, E-18008 Granada, SpainAnand RaichoorLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]Mehdi RezaieDepartment of Physics, Kansas State University, 116 Cardwell Hall, Manhattan, KS 66506, USAGraziano RossiDepartment of Physics and Astronomy, Sejong University, Seoul, 143-747, Republic of KoreaE. SánchezCIEMAT, Avenida Complutense 40, E-28040 Madrid, SpainEdward F. SchlaflySpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USADavid J. SchlegelLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]M. SchubnellDepartment of Physics, University of Michigan, Ann Arbor, MI 48109, USADavid SprayberryNSF NOIRLab, 950 N. Cherry Avenue, Tucson, AZ 85719, USAG. TarléUniversity of Michigan, Ann Arbor, MI 48109, USAC. WarnerDepartment of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USAB. A. WeaverNSF NOIRLab, 950 N. Cherry Avenue, Tucson, AZ 85719, USARongpu ZhouLawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA; [email protected]H. ZouNational Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, Chaoyang District, Beijing, 100012, People's Republic of China

2024en

ABI

Аннотация

Abstract We present a computationally efficient galaxy archetype-based redshift estimation and spectral classification method for the Dark Energy Survey Instrument (DESI) survey. The DESI survey currently relies on a redshift fitter and spectral classifier using a linear combination of principal component analysis–derived templates, which is very efficient in processing large volumes of DESI spectra within a short time frame. However, this method occasionally yields unphysical model fits for galaxies and fails to adequately absorb calibration errors that may still be occasionally visible in the reduced spectra. Our proposed approach improves upon this existing method by refitting the spectra with carefully generated physical galaxy archetypes combined with additional terms designed to absorb data reduction defects and provide more physical models to the DESI spectra. We test our method on an extensive data set derived from the survey validation (SV) and Year 1 (Y1) data of DESI. Our findings indicate that the new method delivers marginally better redshift success for SV tiles while reducing catastrophic redshift failure by 10%–30%. At the same time, results from millions of targets from the main survey show that our model has relatively higher redshift success and purity rates (0.5%–0.8% higher) for galaxy targets while having similar success for QSOs. These improvements also demonstrate that the main DESI redshift pipeline is generally robust. Additionally, it reduces the false-positive redshift estimation by 5%−40% for sky fibers. We also discuss the generic nature of our method and how it can be extended to other large spectroscopic surveys, along with possible future improvements.

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DOI: 10.3847/1538-3881/ad60c2

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