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1. Overview of the Instrumentation for the Dark Energy Spectroscopic Instrument

Author

DESI Collaboration, Abareshi, B., Aguilar, J., Ahlen, S., Alam, Shadab, Alexander, David M., Alfarsy, R., Allen, L., Prieto, C. Allende, Alves, O., Ameel, J., Armengaud, E., Asorey, J., Aviles, Alejandro, Bailey, S., Balaguera-Antolínez, A., Ballester, O., Baltay, C., Bault, A., Beltran, S. F., Benavides, B., BenZvi, S., Berti, A., Besuner, R., Beutler, Florian, Bianchi, D., Blake, C., Blanc, P., Blum, R., Bolton, A., Bose, S., Bramall, D., Brieden, S., Brodzeller, A., Brooks, D., Brownewell, C., Buckley-Geer, E., Cahn, R. N., Cai, Z., Canning, R., Capasso, R., Rosell, A. Carnero, Carton, P., Casas, R., Castander, F. J., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chuang, C., Circosta, C., Cole, S., Cooper, A. P., Costa, L. Da, Cousinou, M.-C., Cuceu, A., Davis, T. M., Dawson, K., Cruz-Noriega, R. De La, Macorra, A. De La, Mattia, A. De, Costa, J. Della, Demmer, P., Derwent, M., Dey, A., Dey, B., Dhungana, G., Ding, Z., Dobson, C., Doel, P., Donald-McCann, J., Donaldson, J., Douglass, K., Duan, Y., Dunlop, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Enriquez-Vargas, M., Escoffier, S., Evatt, M., Fagrelius, P., Fan, X., Fanning, K., Fawcett, V. A., Ferraro, S., Ereza, J., Flaugher, B., Font-Ribera, A., Forero-Romero, J. E., Frenk, C. S., Fromenteau, S., Gänsicke, B. T., Garcia-Quintero, C., Garrison, L., Gaztañaga, E., Gerardi, F., Gil-Marín, H., A Gontcho, S. Gontcho, Gonzalez-Morales, Alma X., Gonzalez-De-Rivera, G., Gonzalez-Perez, V., Gordon, C., Graur, O., Green, D., Grove, C., Gruen, D., Gutierrez, G., Guy, J., Hahn, C., Harris, S., Herrera, D., Herrera-Alcantar, Hiram K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Jelinsky, P., Jiang, L., Jimenez, J., Jing, Y. P., Joyce, R., Jullo, E., Juneau, S., Karaçaylı, N. G., Karamanis, M., Karcher, A., Karim, T., Kehoe, R., Kent, S., Kirkby, D., Kisner, T., Kitaura, F., Koposov, S. E., Kovács, A., Kremin, A., Krolewski, Alex, L’Huillier, B., Lahav, O., Lambert, A., Lamman, C., Lan, Ting-Wen, Landriau, M., Lane, S., Lang, D., Lange, J. U., Lasker, J., Guillou, L. Le, Leauthaud, A., Van Suu, A. Le, Levi, Michael E., Li, T. S., Magneville, C., Manera, M., Manser, Christopher J., Marshall, B., Martini, Paul, McCollam, W., McDonald, P., Meisner, Aaron M., Mena-Fernández, J., Meneses-Rizo, J., Mezcua, M., Miller, T., Miquel, R., Montero-Camacho, P., Moon, J., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, Andrea, Myers, Adam D., Nadathur, S., Najita, J., Napolitano, L., Neilsen, E., Newman, Jeffrey A., Nie, J. D., Ning, Y., Niz, G., Norberg, P., Noriega, Hernán E., O’Brien, T., Obuljen, A., Palanque-Delabrouille, N., Palmese, A., Zhiwei, P., Pappalardo, D., PENG, X., Percival, W. J., Perruchot, S., Pogge, R., Poppett, C., Porredon, A., Prada, F., Prochaska, J., Pucha, R., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramirez-Solano, S., Ramírez-Pérez, César, Ravoux, C., Reil, K., Rezaie, M., Rocher, A., Rockosi, C., Roe, N. A., Roodman, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Sabiu, C. G., Safonova, S., Said, K., Saintonge, A., Catonga, Javier Salas, Samushia, L., Sanchez, E., Saulder, C., Schaan, E., Schlafly, E., Schlegel, D., Schmoll, J., Scholte, D., Schubnell, M., Secroun, A., Seo, H., Serrano, S., Sharples, Ray M., Sholl, Michael J., Silber, Joseph Harry, Silva, D. R., Sirk, M., Siudek, M., Smith, A., Sprayberry, D., Staten, R., Stupak, B., Tan, T., Tarlé, Gregory, Tie, Suk Sien, Tojeiro, R., Ureña-López, L. A., Valdes, F., Valenzuela, O., Valluri, M., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, C., Wechsler, R., Wilson, Michael J., Yang, J., Yu, Y., Yuan, S., Yèche, Christophe, Zhang, H., Zhang, K., Zhao, Cheng, Zhou, Rongpu, Zhou, Zhimin, Zou, H., Zou, J., Zou, S., Zu, Y., Aguilar, J. [0000-0003-0822-452X], Ahlen, S. [0000-0001-6098-7247], Alam, Shadab [0000-0002-3757-6359], Alexander, David M. [0000-0002-5896-6313], Allen, L. [0000-0002-7789-5119], Prieto, C. Allende [0000-0002-0084-572X], Ameel, J. [0000-0003-3638-2584], Asorey, J. [0000-0002-6211-499X], Bailey, S. [0000-0003-4162-6619], Balaguera-Antolínez, A. [0000-0001-5028-3035], Ballester, O. [0000-0002-7126-5300], Bault, A. [0000-0002-9964-1005], Beltran, S. F. [0000-0001-6324-4019], Berti, A. [0000-0003-3582-6649], Beutler, Florian [0000-0003-0467-5438], Bose, S. [0000-0002-0974-5266], Brieden, S. [0000-0003-3896-9215], Brodzeller, A. [0000-0002-8934-0954], Brooks, D. [0000-0002-8458-5047], Cahn, R. N. [0000-0003-2748-0641], Cai, Z. [0000-0001-8467-6478], Capasso, R. [0000-0002-3083-6840], Rosell, A. Carnero [0000-0003-3044-5150], Castander, F. J. [0000-0001-7316-4573], Cervantes-Cota, J. L. [0000-0002-3057-6786], Chabanier, S. [0000-0002-5692-5243], Chaussidon, E. [0000-0001-8996-4874], Chuang, C. [0000-0002-3882-078X], Cole, S. [0000-0002-5954-7903], Cooper, A. P. [0000-0001-8274-158X], Cuceu, A. [0000-0002-2169-0595], Davis, T. M. [0000-0002-4213-8783], Dawson, K. [0000-0002-0553-3805], Costa, J. Della [0000-0003-0928-2000], Dey, A. [0000-0002-4928-4003], Dey, B. [0000-0002-5665-7912], Dhungana, G. [0000-0002-5402-1216], Ding, Z. [0000-0002-3369-3718], Douglass, K. [0000-0002-9540-546X], Duan, Y. [0000-0002-2611-0895], Eisenstein, D. J. [0000-0002-2929-3121], Escoffier, S. [0000-0002-2847-7498], Fan, X. [0000-0003-3310-0131], Fawcett, V. A. [0000-0003-1251-532X], Ereza, J. [0000-0002-0194-4017], Frenk, C. S. [0000-0002-2338-716X], Gänsicke, B. T. [0000-0002-2761-3005], Garrison, L. [0000-0002-9853-5673], Gaztañaga, E. [0000-0001-9632-0815], Gonzalez-Morales, Alma X. [0000-0003-4089-6924], Gonzalez-de-Rivera, G. [0000-0003-4452-743X], Gonzalez-Perez, V. [0000-0001-9938-2755], Graur, O. [0000-0002-4391-6137], Green, D. [0000-0002-0676-3661], Gruen, D. [0000-0003-3270-7644], Hahn, C. [0000-0003-1197-0902], Herrera, D. [0000-0003-2092-6727], Herrera-Alcantar, Hiram K. [0000-0002-9136-9609], Huterer, D. [0000-0001-6558-0112], Iršič, V. [0000-0002-5445-461X], Ishak, M. [0000-0002-6024-466X], Jiang, L. [0000-0003-4176-6486], Jing, Y. P. [0000-0002-4534-3125], Joyce, R. [0000-0003-0201-5241], Jullo, E. [0000-0002-9253-053X], Juneau, S. [0000-0002-0000-2394], Karaçaylı, N. G. [0000-0001-7336-8912], Karamanis, M. [0000-0001-9489-4612], Karim, T. [0000-0002-5652-8870], Kehoe, R. [0000-0002-7101-697X], Kent, S. [0000-0003-4207-7420], Kirkby, D. [0000-0002-8828-5463], Kisner, T. [0000-0003-3510-7134], Koposov, S. E. [0000-0003-2644-135X], Kovács, A. [0000-0002-5825-579X], Kremin, A. [0000-0001-6356-7424], L’Huillier, B. [0000-0003-2934-6243], Landriau, M. [0000-0003-1838-8528], Lang, D. [0000-0002-1172-0754], Lasker, J. [0000-0003-2999-4873], Guillou, L. Le [0000-0001-7178-8868], Leauthaud, A. [0000-0002-3677-3617], Van Suu, A. Le [0000-0001-5488-783X], Levi, Michael E. [0000-0003-1887-1018], Li, T. S. [0000-0002-9110-6163], Manser, Christopher J. [0000-0003-1543-5405], Martini, Paul [0000-0002-0194-4017], McDonald, P. [0000-0001-8346-8394], Meisner, Aaron M. [0000-0002-1125-7384], Mena-Fernández, J. [0000-0001-9497-7266], Meneses-Rizo, J. [0000-0003-3201-9788], Miquel, R. [0000-0002-6610-4836], Moustakas, J. [0000-0002-2733-4559], Nadathur, S. [0000-0001-9070-3102], Neilsen, E. [0000-0002-7357-0317], Newman, Jeffrey A. [0000-0001-8684-2222], Nie, J. D. [0000-0001-6590-8122], Ning, Y. [0000-0001-9442-1217], Niz, G. [0000-0002-1544-8946], Norberg, P. [0000-0002-5875-0440], Noriega, Hernán E. [0000-0002-3397-3998], Obuljen, A. [0000-0002-9012-6621], Palanque-Delabrouille, N. [0000-0003-3188-784], PENG, X. [0000-0002-3784-830X], Percival, W. J. [0000-0002-0644-5727], Pogge, R. [0000-0003-1435-3053], Porredon, A. [0000-0002-2762-2024], Prada, F. [0000-0001-7145-8674], Prochaska, J. [0000-0002-7738-6875], Pucha, R. [0000-0002-4940-3009], Pérez-Ràfols, I. [0000-0001-6979-0125], Rabinowitz, D. [0000-0003-4961-7653], Raichoor, A. [0000-0001-5999-7923], Rezaie, M. [0000-0001-5589-7116], Rockosi, C. [0000-0002-6667-7028], Roodman, A. [0000-0001-5326-3486], Sabiu, C. G. [0000-0002-5513-5303], Safonova, S. [0000-0002-2240-7421], Said, K. [0000-0002-1809-6325], Saintonge, A. [0000-0003-4357-3450], Samushia, L. [0000-0002-1609-5687], Sanchez, E. [0000-0002-9646-8198], Saulder, C. [0000-0002-0408-5633], Schaan, E. [0000-0002-4619-8927], Schlegel, D. [0000-0002-5042-5088], Secroun, A. [0000-0003-0505-3710], Seo, H. [0000-0002-6588-3508], Sharples, Ray M. [0000-0003-3449-8583], Silber, Joseph Harry [0000-0002-3461-0320], Silva, D. R. [0000-0002-7678-2155], Sprayberry, D. [0000-0001-7583-6441], Tarlé, Gregory [0000-0003-1704-0781], Tie, Suk Sien [0000-0002-5249-1353], Valdes, F. [0000-0001-5567-1301], Valenzuela, O. [0000-0002-0523-5509], Valluri, M. [0000-0002-6257-2341], Verde, L. [0000-0003-2601-8770], Walther, M. [0000-0002-1748-3745], Wang, B. [0000-0003-4877-1659], Wang, M. S. [0000-0002-2652-4043], Wechsler, R. [0000-0003-2229-011X], Yang, J. [0000-0001-5287-4242], Yu, Y. [0000-0002-9359-7170], Yuan, S. [0000-0002-5992-7586], Yèche, Christophe [0000-0001-5146-8533], Zhang, H. [0000-0001-6847-5254], Zhang, K. [0000-0002-9808-3646], Zhao, Cheng [0000-0002-1991-7295], Zhou, Rongpu [0000-0001-5381-4372], Zhou, Zhimin [0000-0002-4135-0977], Zou, H. [0000-0002-6684-3997], Zou, J. [0000-0001-9189-0368], Zou, S. [0000-0002-3983-6484], Zu, Y. [0000-0001-6966-6925], Apollo - University of Cambridge Repository, University of St Andrews. School of Physics and Astronomy, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DESI, HEP, INSPIRE, and Ministerio de Ciencia e Innovación (España)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, redshift 0.6, Settore FIS/05 - Astronomia e Astrofisica, QB Astronomy, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), QC, QB, MCC, Astronomy and Astrophysics, DAS, space, distortions, peak, Laboratory Astrophysics, Instrumentation, Software, and Data, QC Physics, Space and Planetary Science, [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], astro-ph.CO, galaxy sample, power-spectrum, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], growth-rate, Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract

Full list of authors: Abareshi, B.; Aguilar, J.; Ahlen, S.; Alam, Shadab; Alexander, David M.; Alfarsy, R.; Allen, L.; Allende Prieto, C.; Alves, O.; Ameel, J.; Armengaud, E.; Asorey, J.; Aviles, Alejandro; Bailey, S.; Balaguera-Antolinez, A.; Ballester, O.; Baltay, C.; Bault, A.; Beltran, S. F.; Benavides, B.; BenZvi, S.; Berti, A.; Besuner, R.; Beutler, Florian; Bianchi, D.; Blake, C.; Blanc, P.; Blum, R.; Bolton, A.; Bose, S.; Bramall, D.; Brieden, S.; Brodzeller, A.; Brooks, D.; Brownewell, C.; Buckley-Geer, E.; Cahn, R. N.; Cai, Z.; Canning, R.; Capasso, R.; Carnero Rosell, A.; Carton, P.; Casas, R.; Castander, F. J.; Cervantes-Cota, J. L.; Chabanier, S.; Chaussidon, E.; Chuang, C.; Circosta, C.; Cole, S.; Cooper, A. P.; da Costa, L.; Cousinou, M-C; Cuceu, A.; Davis, T. M.; Dawson, K.; De la Cruz-Noriega, R.; de la Macorra, A.; de Mattia, A.; Della Costa, J.; Demmer, P.; Derwent, M.; Dey, A.; Dey, B.; Dhungana, G.; Ding, Z.; Dobson, C.; Doel, P.; Donald-McCann, J.; Donaldson, J.; Douglass, K.; Duan, Y.; Dunlop, P.; Edelstein, J.; Eftekharzadeh, S.; Eisenstein, D. J.; Enriquez-Vargas, M.; Escoffier, S.; Evatt, M.; Fagrelius, P.; Fan, X.; Fanning, K.; Fawcett, V. A.; Ferraro, S.; Ereza, J.; Flaugher, B.; Font-Ribera, A.; Forero-Romero, J. E.; Frenk, C. S.; Fromenteau, S.; Gansicke, B. T.; Garcia-Quintero, C.; Garrison, L.; Gaztanaga, E.; Gerardi, F.; Gil-Marin, H.; Gontcho, S. Gontcho A.; Gonzalez-Morales, Alma X.; Gonzalez-de-Rivera, G.; Gonzalez-Perez, V; Gordon, C.; Graur, O.; Green, D.; Grove, C.; Gruen, D.; Gutierrez, G.; Guy, J.; Hahn, C.; Harris, S.; Herrera, D.; Herrera-Alcantar, Hiram K.; Honscheid, K.; Howlett, C.; Huterer, D.; Irsic, V; Ishak, M.; Jelinsky, P.; Jiang, L.; Jimenez, J.; Jing, Y. P.; Joyce, R.; Jullo, E.; Juneau, S.; Karacayli, N. G.; Karamanis, M.; Karcher, A.; Karim, T.; Kehoe, R.; Kent, S.; Kirkby, D.; Kisner, T.; Kitaura, F.; Koposov, S. E.; Kovacs, A.; Kremin, A.; Krolewski, Alex; L'Huillier, B.; Lahav, O.; Lambert, A.; Lamman, C.; Lan, Ting-Wen; Landriau, M.; Lane, S.; Lang, D.; Lange, J. U.; Lasker, J.; Le Guillou, L.; Leauthaud, A.; Suu, A. Le Van; Levi, Michael E.; Li, T. S.; Magneville, C.; Manera, M.; Manser, Christopher J.; Marshall, B.; Martini, Paul; McCollam, W.; McDonald, P.; Meisner, Aaron M.; Mena-Fernandez, J.; Meneses-Rizo, J.; Mezcua, M.; Miller, T.; Miquel, R.; Montero-Camacho, P.; Moon, J.; Moustakas, J.; Mueller, E.; Munoz-Gutierrez, Andrea; Myers, Adam D.; Nadathur, S.; Najita, J.; Napolitano, L.; Neilsen, E.; Newman, Jeffrey A.; Nie, J. D.; Ning, Y.; Niz, G.; Norberg, P.; Noriega, Hernan E.; O'Brien, T.; Obuljen, A.; Palanque-Delabrouille, N.; Palmese, A.; Zhiwei, P.; Pappalardo, D.; Peng, X.; Percival, W. J.; Perruchot, S.; Pogge, R.; Poppett, C.; Porredon, A.; Prada, F.; Prochaska, J.; Pucha, R.; Perez-Fernandez, A.; Perez-Rafols, I; Rabinowitz, D.; Raichoor, A.; Ramirez-Solano, S.; Ramirez-Perez, Cesar; Ravoux, C.; Reil, K.; Rezaie, M.; Rocher, A.; Rockosi, C.; Roe, N. A.; Roodman, A.; Ross, A. J.; Rossi, G.; Ruggeri, R.; Ruhlmann-Kleider, V; Sabiu, C. G.; Safonova, S.; Said, K.; Saintonge, A.; Catonga, Javier Salas; Samushia, L.; Sanchez, E.; Saulder, C.; Schaan, E.; Schlafly, E.; Schlegel, D.; Schmoll, J.; Scholte, D.; Schubnell, M.; Secroun, A.; Seo, H.; Serrano, S.; Sharples, Ray M.; Sholl, Michael J.; Silber, Joseph Harry; Silva, D. R.; Sirk, M.; Siudek, M.; Smith, A.; Sprayberry, D.; Staten, R.; Stupak, B.; Tan, T.; Tarle, Gregory; Tie, Suk Sien; Tojeiro, R.; Urena-Lopez, L. A.; Valdes, F.; Valenzuela, O.; Valluri, M.; Vargas-Magana, M.; Verde, L.; Walther, M.; Wang, B.; Wang, M. S.; Weaver, B. A.; Weaverdyck, C.; Wechsler, R.; Wilson, Michael J.; Yang, J.; Yu, Y.; Yuan, S.; Yeche, Christophe; Zhang, H.; Zhang, K.; Zhao, Cheng; Zhou, Rongpu; Zhou, Zhimin; Zou, H.; Zou, J.; Zou, S.; Zu, Y.; DESI Collaboration.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., The Dark Energy Spectroscopic Instrument (DESI) embarked on an ambitious 5 yr survey in 2021 May to explore the nature of dark energy with spectroscopic measurements of 40 million galaxies and quasars. DESI will determine precise redshifts and employ the baryon acoustic oscillation method to measure distances from the nearby universe to beyond redshift z > 3.5, and employ redshift space distortions to measure the growth of structure and probe potential modifications to general relativity. We describe the significant instrumentation we developed to conduct the DESI survey. This includes: a wide-field, 3fdg2 diameter prime-focus corrector; a focal plane system with 5020 fiber positioners on the 0.812 m diameter, aspheric focal surface; 10 continuous, high-efficiency fiber cable bundles that connect the focal plane to the spectrographs; and 10 identical spectrographs. Each spectrograph employs a pair of dichroics to split the light into three channels that together record the light from 360–980 nm with a spectral resolution that ranges from 2000–5000. We describe the science requirements, their connection to the technical requirements, the management of the project, and interfaces between subsystems. DESI was installed at the 4 m Mayall Telescope at Kitt Peak National Observatory and has achieved all of its performance goals. Some performance highlights include an rms positioner accuracy of better than 0farcs1 and a median signal-to-noise ratio of 7 of the [O ii] doublet at 8 × 10−17 erg s−1 cm−2 in 1000 s for galaxies at z = 1.4–1.6. We conclude with additional highlights from the on-sky validation and commissioning, key successes, and lessons learned. © 2022. The Author(s). Published by the American Astronomical Society., This research is supported by the Director, Office of Science, Office of High Energy Physics of the U.S. Department of Energy under contract No. DE-AC02-05CH11231, and by the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility under the same contract. Additional support for DESI is provided by the U.S. National Science Foundation, Division of Astronomical Sciences under contract No. AST-0950945 to the NSF's National Optical-Infrared Astronomy Research Laboratory; the Science and Technologies Facilities Council of the United Kingdom; the Gordon and Betty Moore Foundation; the Heising–Simons Foundation; the French Alternative Energies and Atomic Energy Commission (CEA); the National Council of Science and Technology of Mexico (CONACYT); the Ministry of Science and Innovation of Spain, and by the DESI Member Institutions: Aix-Marseille University; Argonne National Laboratory; Barcelona-Madrid Regional Participation Group; Brookhaven National Laboratory; Boston University; Brazil Regional Participation Group; Carnegie Mellon University; CEA-IRFU, Saclay; China Participation Group; Cornell University; Durham University; École Polytechnique Fédérale de Lausanne; Eidgenössische Technische Hochschule, Zürich; Fermi National Accelerator Laboratory; Granada-Madrid-Tenerife Regional Participation Group; Harvard University; Kansas State University; Korea Astronomy and Space Science Institute; Korea Institute for Advanced Study; Lawrence Berkeley National Laboratory; Laboratoire de Physique Nucléaire et de Hautes Energies; Ludwig Maximilians University; Max Planck Institute; Mexico Regional Participation Group; New York University; NSF's National Optical-Infrared Astronomy Research Laboratory; Ohio University; Perimeter Institute; Shanghai Jiao Tong University; Siena College; SLAC National Accelerator Laboratory; Southern Methodist University; Swinburne University; The Ohio State University; Universidad de los Andes; University of Arizona; University of Barcelona; University of California, Berkeley; University of California, Irvine; University of California, Santa Cruz; University College London; University of Florida; University of Michigan at Ann Arbor; University of Pennsylvania; University of Pittsburgh; University of Portsmouth; University of Queensland; University of Rochester; University of Toronto; University of Utah; University of Waterloo; University of Wyoming; University of Zurich; UK Regional Participation Group; and Yale University. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

Published
2022
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2. H I constraints from the cross-correlation of eBOSS galaxies and Green Bank Telescope intensity maps

Author

Wolz, Laura, Pourtsidou, Alkistis, Masui, Kiyoshi W., Chang, Tzu-Ching, Bautista, Julian E., Mueller, Eva-Maria, Avila, Santiago, Bacon, David, Percival, Will J., Cunnington, Steven, Anderson, Chris, Chen, Xuelei, Kneib, Jean-Paul, Li, Yi-Chao, Liao, Yu-Wei, Pen, Ue-Li, Peterson, Jeffrey B., Rossi, Graziano, Schneider, Donald P., Yadav, Jaswant, and Zhao, Gong-Bo

Subjects
large-scale structure of universe, radio lines: galaxies, methods: statistical, 1/f noise, spectroscopic survey measurement, power spectrum, redshift 0.6, large-scale structure, mass function, cosmology: observations, cosmic neutral hydrogen, galaxies: evolution, multipole expansion, growth-rate, dark energy survey
Abstract

We present the joint analysis of Neutral Hydrogen (H I) Intensity Mapping observations with three galaxy samples: the Luminous Red Galaxy (LRG) and Emission Line Galaxy (ELG) samples from the eBOSS survey, and the WiggleZ Dark Energy Survey sample. The H I intensity maps are Green Bank Telescope observations of the redshifted 21cm emission on 100 deg(2) covering the redshift range 0.6 < z < 1.0. We process the data by separating and removing the foregrounds present in the radio frequencies with FAsTI ICA. We verify the quality of the foreground separation with mock realizations, and construct a transfer function to correct for the effects of foreground removal on the H I signal. We cross-correlate the cleaned H I data with the galaxy samples and study the overall amplitude as well as the scale dependence of the power spectrum. We also qualitatively compare our findings with the predictions by a semianalytical galaxy evolution simulation. The cross-correlations constrain the quantity Omega(H I)b(H I)r(H I,opt) at an effective scale k(eff), where Omega(H I) is the H I density fraction, b(H I )is the H I bias, and r(H I,opt) the galaxy-hydrogen correlation coefficient, which is dependent on the H I content of the optical galaxy sample. At k(eff) = 0.31 h Mpc(-1) we find Omega(H I)b(H I)r(H I,wig) = [0.58 +/- 0.09 (stat) +/- 0.05 (sys)] x 10(-3) for GBT-WiggleZ, Omega(H I)b(H I)r(H I,ELG) = [0.40 +/- 0.09 (stat) +/- 0.04 (sys)] x 10(-3) for GBT-ELG, and Omega(H I)b(H I)r(H I,LRG) = [0.35 +/- 0.08 (stat) +/- 0.03 (sys)] x 10(-3) for GBT-LRG, at z similar or equal to 0.8. We also report results at k(eff) = 0.24 and k(eff) = 0.48 h Mpc(-1). With little information on H I parameters beyond our local Universe, these are amongst the most precise constraints on neutral hydrogen density fluctuations in an underexplored redshift range.

3. Hydrogen Intensity and Real-Time Analysis Experiment: 256-element array status and overview

Author

Devin Crichton, Moumita Aich, Adam Amara, Kevin Bandura, Bruce A. Bassett, Carlos Bengaly, Pascale Berner, Shruti Bhatporia, Martin Bucher, Tzu-Ching Chang, H. Cynthia Chiang, Jean-Francois Cliche, Carolyn Crichton, Romeel Dave, Dirk I. L. De Villiers, Matt Dobbs, Aaron M. Ewall-Wice, Scott Eyono, Christopher Finlay, Sindhu Gaddam, Ken Ganga, Kevin G. Gayley, Kit Gerodias, Tim B. Gibbon, Austine Gumba, Neeraj Gupta, Maile Harris, Heiko Heilgendorff, Matt Hilton, Adam D. Hincks, Pascal Hitz, Mona Jalilvand, Roufurd P. M. Julie, Zahra Kader, Joseph Kania, Dionysios Karagiannis, Aris Karastergiou, Kabelo Kesebonye, Piyanat Kittiwisit, Jean-Paul Kneib, Kenda Knowles, Emily R. Kuhn, Martin Kunz, Roy Maartens, Vincent MacKay, Stuart MacPherson, Christian Monstein, Kavilan Moodley, V. Mugundhan, Warren Naidoo, Arun Naidu, Laura B. Newburgh, Viraj Nistane, Amanda Di Nitto, Deniz Ölçek, Xinyu Pan, Sourabh Paul, Jeffrey B. Peterson, Elizabeth Pieters, Carla Pieterse, Aritha Pillay, Anna R. Polish, Liantsoa Randrianjanahary, Alexandre Refregier, Andre Renard, Edwin Retana-Montenegro, Ian H. Rout, Cyndie Russeeawon, Alireza Vafaei Sadr, Benjamin R. B. Saliwanchik, Ajith Sampath, Pranav Sanghavi, Mario G. Santos, Onkabetse Sengate, J. Richard Shaw, Jonathan L. Sievers, Oleg M. Smirnov, Kendrick M. Smith, Ulrich Armel Mbou Sob, Raghunathan Srianand, Pieter Stronkhorst, Dhaneshwar D. Sunder, Simon Tartakovsky, Russ Taylor, Peter Timbie, Emma E. Tolley, Junaid Townsend, Will Tyndall, Cornelius Ungerer, Jacques van Dyk, Gary van Vuuren, Keith Vanderlinde, Thierry Viant, Anthony Walters, Jingying Wang, Amanda Weltman, Patrick Woudt, Dallas Wulf, Anatoly Zavyalov, Zheng Zhang, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Astrophysique, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)

Subjects
Signal processing, Cosmology and Nongalactic Astrophysics (astro-ph.CO), anisotropic power spectrum, bao, Observatories, spectroscopic survey measurement, 21 cm, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Receivers, redshift 0.6, 010309 optics, scale, project, interferometers, 0103 physical sciences, radio transients, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Radio astronomy, dark energy, 010303 astronomy & astrophysics, Instrumentation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Pulsars, Baryon acoustic oscillations, Mechanical Engineering, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Electronic, Optical and Magnetic Materials, Space and Planetary Science, Control and Systems Engineering, intensity mapping, galaxy sample, Visibility, astropy, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmology, growth-rate, Astrophysics - Cosmology and Nongalactic Astrophysics, Hydrogen, Telescopes
Abstract

The Hydrogen Intensity and Real-time Analysis eXperiment (HIRAX) is a radio interferometer array currently in development, with an initial 256-element array to be deployed at the South African Radio Astronomy Observatory (SARAO) Square Kilometer Array (SKA) site in South Africa. Each of the 6m, $f/0.23$ dishes will be instrumented with dual-polarisation feeds operating over a frequency range of 400-800 MHz. Through intensity mapping of the 21 cm emission line of neutral hydrogen, HIRAX will provide a cosmological survey of the distribution of large-scale structure over the redshift range of $0.775 < z < 2.55$ over $\sim$15,000 square degrees of the southern sky. The statistical power of such a survey is sufficient to produce $\sim$7 percent constraints on the dark energy equation of state parameter when combined with measurements from the Planck satellite. Additionally, HIRAX will provide a highly competitive platform for radio transient and HI absorber science while enabling a multitude of cross-correlation studies. In this paper, we describe the science goals of the experiment, overview of the design and status of the sub-components of the telescope system, and describe the expected performance of the initial 256-element array as well as the planned future expansion to the final, 1024-element array., 24 pages, 6 figures. Updated to match published version

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