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2,450 results on '"A. Meisner"'

1. Leveraging mechanochemistry for sustainable polymer degradation

Author: Aydonat, Simay, Hergesell, Adrian H., Seitzinger, Claire L., Lennarz, Regina, Chang, George, Sievers, Carsten, Meisner, Jan, Vollmer, Ina, Göstl, Robert, Aydonat, Simay, Hergesell, Adrian H., Seitzinger, Claire L., Lennarz, Regina, Chang, George, Sievers, Carsten, Meisner, Jan, Vollmer, Ina, and Göstl, Robert
Abstract: Over 8 billion tons of plastic have been produced to date, and a 100% reclamation recycling strategy is not foreseeable. This review summarizes how the mechanochemistry of polymers may contribute to a sustainable polymer future by controlling the degradation not only of de novo developed designer polymers but also of plastics in existing waste streams. The historical development of polymer mechanochemistry is presented while highlighting current examples of mechanochemically induced polymer degradation. Additionally, theoretical and computational frameworks are discussed that may lead to the discovery and better understanding of new mechanochemical reactions in the future. This review takes into account technical and engineering perspectives converging the fields of trituration and polymer mechanochemistry with a particular focus on the fate of commodity polymers and potential technologies to monitor mechanochemical reactions while they occur. Therefore, a unique perspective of multiple communities is presented, highlighting the need for future transdisciplinary research to tackle the high-leverage parameters governing an eventually successful mechanochemical degradation approach for a circular economy.
Published: 2024

2. DESI complete calibration of the colour–redshift relation (DC3R2): results from early DESI data

Author: McCullough, J, McCullough, J, Gruen, D, Amon, A, Roodman, A, Masters, D, Raichoor, A, Schlegel, D, Canning, R, Castander, FJ, DeRose, J, Miquel, R, Myles, J, Newman, JA, Slosar, A, Speagle, J, Wilson, MJ, Aguilar, J, Ahlen, S, Bailey, S, Brooks, D, Claybaugh, T, Cole, S, Dawson, K, de la Macorra, A, Doel, P, Forero-Romero, JE, Gontcho, S Gontcho A, Guy, J, Kehoe, R, Kremin, A, Landriau, M, Le Guillou, L, Levi, M, Manera, M, Martini, P, Meisner, A, Moustakas, J, Nie, J, Percival, WJ, Poppett, C, Prada, F, Rezaie, M, Rossi, G, Sanchez, E, Seo, H, Tarlé, G, Weaver, BA, Zhou, Z, Zou, H, Collaboration, DESI, McCullough, J, McCullough, J, Gruen, D, Amon, A, Roodman, A, Masters, D, Raichoor, A, Schlegel, D, Canning, R, Castander, FJ, DeRose, J, Miquel, R, Myles, J, Newman, JA, Slosar, A, Speagle, J, Wilson, MJ, Aguilar, J, Ahlen, S, Bailey, S, Brooks, D, Claybaugh, T, Cole, S, Dawson, K, de la Macorra, A, Doel, P, Forero-Romero, JE, Gontcho, S Gontcho A, Guy, J, Kehoe, R, Kremin, A, Landriau, M, Le Guillou, L, Levi, M, Manera, M, Martini, P, Meisner, A, Moustakas, J, Nie, J, Percival, WJ, Poppett, C, Prada, F, Rezaie, M, Rossi, G, Sanchez, E, Seo, H, Tarlé, G, Weaver, BA, Zhou, Z, Zou, H, and Collaboration, DESI
Abstract: We present initial results from the Dark Energy Spectroscopic Instrument (DESI) complete calibration of the colour–redshift relation (DC3R2) secondary target survey. Our analysis uses 230 k galaxies that overlap with KiDS-VIKING ugriZYJHKs photometry to calibrate the colour–redshift relation and to inform photometric redshift (photo-z) inference methods of future weak lensing surveys. Together with emission line galaxies (ELGs), luminous red galaxies (LRGs), and the Bright Galaxy Survey (BGS) that provide samples of complementary colour, the DC3R2 targets help DESI to span 56 per cent of the colour space visible to Euclid and LSST with high confidence spectroscopic redshifts. The effects of spectroscopic completeness and quality are explored, as well as systematic uncertainties introduced with the use of common Self-Organizing Maps trained on different photometry than the analysis sample. We further examine the dependence of redshift on magnitude at fixed colour, important for the use of bright galaxy spectra to calibrate redshifts in a fainter photometric galaxy sample. We find that noise in the KiDS-VIKING photometry introduces a dominant, apparent magnitude dependence of redshift at fixed colour, which indicates a need for carefully chosen deep drilling fields, and survey simulation to model this effect for future weak lensing surveys.
Published: 2024

3. Measuring Fiber Positioning Accuracy and Throughput with Fiber Dithering for the Dark Energy Spectroscopic Instrument

Author: Schlafly, EF, Schlafly, EF, Schlegel, D, BenZvi, S, Raichoor, A, Forero-Romero, JE, Aguilar, J, Ahlen, S, Bailey, S, Bault, A, Brooks, D, Claybaugh, T, Dawson, K, de la Macorra, A, Dey, Arjun, Doel, P, Gaztañaga, E, Gontcho, S Gontcho A, Guy, J, Hahn, C, Honscheid, K, Jimenez, J, Kent, S, Kirkby, D, Kisner, T, Kremin, A, Lambert, A, Landriau, M, Levi, ME, Manera, M, Martini, P, Meisner, A, Miquel, R, Moustakas, J, Myers, AD, Nie, J, Palanque-Delabrouille, N, Percival, WJ, Poppett, C, Prada, F, Rabinowitz, D, Rezaie, M, Rossi, G, Sanchez, E, Schubnell, M, Sharples, R, Silber, J, Tarlé, G, Weaver, BA, Zhou, Z, Zou, H, Schlafly, EF, Schlafly, EF, Schlegel, D, BenZvi, S, Raichoor, A, Forero-Romero, JE, Aguilar, J, Ahlen, S, Bailey, S, Bault, A, Brooks, D, Claybaugh, T, Dawson, K, de la Macorra, A, Dey, Arjun, Doel, P, Gaztañaga, E, Gontcho, S Gontcho A, Guy, J, Hahn, C, Honscheid, K, Jimenez, J, Kent, S, Kirkby, D, Kisner, T, Kremin, A, Lambert, A, Landriau, M, Levi, ME, Manera, M, Martini, P, Meisner, A, Miquel, R, Moustakas, J, Myers, AD, Nie, J, Palanque-Delabrouille, N, Percival, WJ, Poppett, C, Prada, F, Rabinowitz, D, Rezaie, M, Rossi, G, Sanchez, E, Schubnell, M, Sharples, R, Silber, J, Tarlé, G, Weaver, BA, Zhou, Z, and Zou, H
Abstract: Highly multiplexed, fiber-fed spectroscopy is enabling surveys of millions of stars and galaxies. The performance of these surveys depends on accurately positioning fibers in the focal plane to capture target light. We describe a technique to measure the positioning accuracy of fibers by dithering fibers slightly around their ideal locations. This approach also enables measurement of the total system throughput and point-spread function delivered to the focal plane. We then apply this technique to observations from the Dark Energy Survey Instrument (DESI), and demonstrate that DESI positions fibers to within 0.″08 of their targets (5% of a fiber diameter) and achieves a system throughput within about 7% of expectations.
Published: 2024

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

Author: Anand, Abhijeet, Anand, Abhijeet, Guy, Julien, Bailey, Stephen, Moustakas, John, Aguilar, J, Ahlen, S, Bolton, AS, Brodzeller, A, Brooks, D, Claybaugh, T, Cole, S, de la Macorra, A, Dey, Biprateep, Fanning, K, Forero-Romero, JE, Gaztañaga, E, Gontcho, S Gontcho A, Gutierrez, G, Honscheid, K, Howlett, C, Juneau, S, Kirkby, D, Kisner, T, Kremin, A, Lambert, A, Landriau, M, Le Guillou, L, Manera, M, Meisner, A, Miquel, R, Mueller, E, Niz, G, Palanque-Delabrouille, N, Percival, WJ, Poppett, C, Prada, F, Raichoor, A, Rezaie, M, Rossi, G, Sanchez, E, Schlafly, EF, Schlegel, D, Schubnell, M, Sprayberry, D, Tarlé, G, Warner, C, Weaver, BA, Zhou, R, Zou, H, Anand, Abhijeet, Anand, Abhijeet, Guy, Julien, Bailey, Stephen, Moustakas, John, Aguilar, J, Ahlen, S, Bolton, AS, Brodzeller, A, Brooks, D, Claybaugh, T, Cole, S, de la Macorra, A, Dey, Biprateep, Fanning, K, Forero-Romero, JE, Gaztañaga, E, Gontcho, S Gontcho A, Gutierrez, G, Honscheid, K, Howlett, C, Juneau, S, Kirkby, D, Kisner, T, Kremin, A, Lambert, A, Landriau, M, Le Guillou, L, Manera, M, Meisner, A, Miquel, R, Mueller, E, Niz, G, Palanque-Delabrouille, N, Percival, WJ, Poppett, C, Prada, F, Raichoor, A, Rezaie, M, Rossi, G, Sanchez, E, Schlafly, EF, Schlegel, D, Schubnell, M, Sprayberry, D, Tarlé, G, Warner, C, Weaver, BA, Zhou, R, and Zou, H
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.
Published: 2024

5. Laser spectroscopy of the ground-state hyperfine structure in H-like and Li-like bismuth

Author: Vollbrecht, J., Andelkovic, Z., Dax, A., Geithner, W., Geppert, C., Gorges, C., Hammen, M., Hannen, V., Kaufmann, S., König, K., Litvinov, Y., Lochmann, M., Maass, B., Meisner, J., Murboeck, T., Nörtershäuser, W., Sánchez, R., Schmidt, S., Schmidt, M., Steck, M., Stöhlker, T., Thompson, R. C., Ullmann, J., Weinheimer, C., Vollbrecht, J., Andelkovic, Z., Dax, A., Geithner, W., Geppert, C., Gorges, C., Hammen, M., Hannen, V., Kaufmann, S., König, K., Litvinov, Y., Lochmann, M., Maass, B., Meisner, J., Murboeck, T., Nörtershäuser, W., Sánchez, R., Schmidt, S., Schmidt, M., Steck, M., Stöhlker, T., Thompson, R. C., Ullmann, J., and Weinheimer, C.
Abstract: The LIBELLE experiment performed at the experimental storage ring (ESR) at the GSI Helmholtz Center in Darmstadt aims for the determination of the ground state hyperfine (HFS) transitions and lifetimes in hydrogen-like (²⁰⁹Bi⁸²⁺) and lithium-like (²⁰⁹Bi⁸⁰⁺) bismuth. The study of HFS transitions in highly charged ions enables precision tests of QED in extreme electric and magnetic fields otherwise not attainable in laboratory experiments. While the HFS transition in H-like bismuth was already observed in earlier experiments at the ESR, the LIBELLE experiment succeeded for the first time to measure the HFS transition in Li-like bismuth in a laser spectroscopy experiment.
Published: 2024

6. Population genomics of the muskox' resilience in the near absence of genetic variation

Author: Pečnerová, Patrícia, Lord, Edana, Garcia-Erill, Genís, Hanghøj, Kristian, Rasmussen, Malthe Sebro, Meisner, Jonas, Liu, Xiaodong, van der Valk, Tom, Santander, Cindy G., Quinn, Liam, Lin, Long, Liu, Shanlin, Carøe, Christian, Dalerum, Fredrik, Götherström, Anders, Måsviken, Johannes, Vartanyan, Sergey, Raundrup, Katrine, Al-Chaer, Amal, Rasmussen, Linett, Hvilsom, Christina, Heide-Jørgensen, Mads Peter, Sinding, Mikkel-Holger S., Aastrup, Peter, Van Coeverden de Groot, Peter J., Schmidt, Niels Martin, Albrechtsen, Anders, Dalén, Love, Heller, Rasmus, Moltke, Ida, Redlef Siegismund, Hans, Pečnerová, Patrícia, Lord, Edana, Garcia-Erill, Genís, Hanghøj, Kristian, Rasmussen, Malthe Sebro, Meisner, Jonas, Liu, Xiaodong, van der Valk, Tom, Santander, Cindy G., Quinn, Liam, Lin, Long, Liu, Shanlin, Carøe, Christian, Dalerum, Fredrik, Götherström, Anders, Måsviken, Johannes, Vartanyan, Sergey, Raundrup, Katrine, Al-Chaer, Amal, Rasmussen, Linett, Hvilsom, Christina, Heide-Jørgensen, Mads Peter, Sinding, Mikkel-Holger S., Aastrup, Peter, Van Coeverden de Groot, Peter J., Schmidt, Niels Martin, Albrechtsen, Anders, Dalén, Love, Heller, Rasmus, Moltke, Ida, and Redlef Siegismund, Hans
Abstract: Genomic studies of species threatened by extinction are providing crucial information about evolutionary mechanisms and genetic consequences of population declines and bottlenecks. However, to understand how species avoid the extinction vortex, insights can be drawn by studying species that thrive despite past declines. Here, we studied the population genomics of the muskox (Ovibos moschatus), an Ice Age relict that was at the brink of extinction for thousands of years at the end of the Pleistocene yet appears to be thriving today. We analysed 108 whole genomes, including present-day individuals representing the current native range of both muskox subspecies, the white-faced and the barren-ground muskox (O. moschatus wardi and O. moschatus moschatus) and a ~21,000-year-old ancient individual from Siberia. We found that the muskox' demographic history was profoundly shaped by past climate changes and post-glacial re-colonizations. In particular, the white-faced muskox has the lowest genome-wide heterozygosity recorded in an ungulate. Yet, there is no evidence of inbreeding depression in native muskox populations. We hypothesize that this can be explained by the effect of long-term gradual population declines that allowed for purging of strongly deleterious mutations. This study provides insights into how species with a history of population bottlenecks, small population sizes and low genetic diversity survive against all odds.
Published: 2024
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7. DESI Survey Validation Data in the COSMOS/Hyper Suprime-Cam Field: Cool Gas Trace Main-sequence Star-forming Galaxies at the Cosmic Noon

Author: Zou, Siwei, Zou, Siwei, Jiang, Linhua, Cai, Zheng, Moustakas, John, Sun, Zechang, Pan, Zhiwei, Ding, Jiani, Forero-Romero, Jaime E, Zou, Hu, Ting, Yuan-sen, Pieri, Matthew, Ahlen, Steven, Alexander, David, Brooks, David, Dey, Arjun, Font-Ribera, Andreu, Gontcho, Satya Gontcho A, Honscheid, Klaus, Landriau, Martin, de la Macorra, Axel, Magana, Mariana Vargas, Meisner, Aaron, Miquel, Ramon, Schubnell, Michael, Tarlé, Gregory, Zhou, Zhimin, Zou, Siwei, Zou, Siwei, Jiang, Linhua, Cai, Zheng, Moustakas, John, Sun, Zechang, Pan, Zhiwei, Ding, Jiani, Forero-Romero, Jaime E, Zou, Hu, Ting, Yuan-sen, Pieri, Matthew, Ahlen, Steven, Alexander, David, Brooks, David, Dey, Arjun, Font-Ribera, Andreu, Gontcho, Satya Gontcho A, Honscheid, Klaus, Landriau, Martin, de la Macorra, Axel, Magana, Mariana Vargas, Meisner, Aaron, Miquel, Ramon, Schubnell, Michael, Tarlé, Gregory, and Zhou, Zhimin
Abstract: We present the first result in exploring the gaseous halo and galaxy correlation using the Dark Energy Spectroscopic Instrument survey validation data in the Cosmic Evolution Survey (COSMOS) and Hyper Suprime-Cam field. We obtain multiphase gaseous halo properties in the circumgalactic medium by using 115 quasar spectra (signal-to-noise ratio > 3). We detect Mg ii absorption at redshift 0.6 < z < 2.5, C iv absorption at 1.6 < z < 3.6, and H i absorption associated with the Mg ii and C iv. By crossmatching the COSMOS2020 catalog, we identify the Mg ii and C iv host galaxies in 10 quasar fields at 0.9< z < 3.1. We find that within the impact parameter of 250 kpc, a tight correlation is seen between the strong Mg ii equivalent width and the host galaxy star formation rate. The covering fraction f c of the strong Mg ii selected galaxies, which is the ratio of the absorbing galaxy in a certain galaxy population, shows significant evolution in the main-sequence galaxies and marginal evolution in all the galaxy populations within 250 kpc at 0.9 < z < 2.2. The f c increase in the main-sequence galaxies likely suggests the coevolution of strong Mg ii absorbing gas and the main-sequence galaxies at the cosmic noon. Furthermore, Mg ii and C iv absorbing gas is detected out of the galaxy virial radius, tentatively indicating the feedback produced by the star formation and/or the environmental effects.
Published: 2024

8. Production of Alternate Realizations of DESI Fiber Assignment for Unbiased Clustering Measurement in Data and Simulations

Author: Lasker, J., Rosell, A. Carnero, Myers, A. D., Ross, A. J., Bianchi, D., Hanif, M. M. S, Kehoe, R., de Mattia, A., Napolitano, L., Percival, W. J., Staten, R., Aguilar, J., Ahlen, S., Bigwood, L., Brooks, D., Claybaugh, T., Cole, S., de la Macorra, A., Ding, Z., Doel, P., Fanning, K., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Honscheid, K., Howlett, C., Juneau, S., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Meisner, A., Miquel, R., Moustakas, J., Mueller, E., Nie, J., Niz, G., Oh, M., Palanque-Delabrouille, N., Poppett, C., Prada, F., Rezaie, M., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Sprayberry, D., Tarlé, G., Vargas-Magaña, M., Weaver, B. A., Wilson, Michael J., Zheng, Y., Lasker, J., Rosell, A. Carnero, Myers, A. D., Ross, A. J., Bianchi, D., Hanif, M. M. S, Kehoe, R., de Mattia, A., Napolitano, L., Percival, W. J., Staten, R., Aguilar, J., Ahlen, S., Bigwood, L., Brooks, D., Claybaugh, T., Cole, S., de la Macorra, A., Ding, Z., Doel, P., Fanning, K., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Honscheid, K., Howlett, C., Juneau, S., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Meisner, A., Miquel, R., Moustakas, J., Mueller, E., Nie, J., Niz, G., Oh, M., Palanque-Delabrouille, N., Poppett, C., Prada, F., Rezaie, M., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Sprayberry, D., Tarlé, G., Vargas-Magaña, M., Weaver, B. A., Wilson, Michael J., and Zheng, Y.
Abstract: A critical requirement of spectroscopic large scale structure analyses is correcting for selection of which galaxies to observe from an isotropic target list. This selection is often limited by the hardware used to perform the survey which will impose angular constraints of simultaneously observable targets, requiring multiple passes to observe all of them. In SDSS this manifested solely as the collision of physical fibers and plugs placed in plates. In DESI, there is the additional constraint of the robotic positioner which controls each fiber being limited to a finite patrol radius. A number of approximate methods have previously been proposed to correct the galaxy clustering statistics for these effects, but these generally fail on small scales. To accurately correct the clustering we need to upweight pairs of galaxies based on the inverse probability that those pairs would be observed (Bianchi \& Percival 2017). This paper details an implementation of that method to correct the Dark Energy Spectroscopic Instrument (DESI) survey for incompleteness. To calculate the required probabilities, we need a set of alternate realizations of DESI where we vary the relative priority of otherwise identical targets. These realizations take the form of alternate Merged Target Ledgers (AMTL), the files that link DESI observations and targets. We present the method used to generate these alternate realizations and how they are tracked forward in time using the real observational record and hardware status, propagating the survey as though the alternate orderings had been adopted. We detail the first applications of this method to the DESI One-Percent Survey (SV3) and the DESI year 1 data. We include evaluations of the pipeline outputs, estimation of survey completeness from this and other methods, and validation of the method using mock galaxy catalogs., Comment: 30 pages, 21 figures
Published: 2024

9. DESI 2024 IV: Baryon Acoustic Oscillations from the Lyman Alpha Forest

Author: DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Alexander, D. M., Alvarez, M., Alves, O., Anand, A., Andrade, U., Armengaud, E., Avila, S., Aviles, A., Awan, H., Bailey, S., Baltay, C., Bault, A., Bautista, J., Behera, J., BenZvi, S., Beutler, F., Bianchi, D., Blake, C., Blum, R., Brieden, S., Brodzeller, A., Brooks, D., Buckley-Geer, E., Burtin, E., Calderon, R., Canning, R., Rosell, A. Carnero, Cereskaite, R., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chen, X., Claybaugh, T., Cole, S., Cuceu, A., Davis, T. M., Dawson, K., de la Cruz, R., de la Macorra, A., de Mattia, A., Deiosso, N., Dey, A., Dey, B., Ding, J., Ding, Z., Doel, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Fagrelius, P., Fanning, K., Ferraro, S., Ereza, J., Findlay, N., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Garcia-Quintero, C., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Green, D., Gruen, D., Gsponer, R., Gutierrez, G., Guy, J., Hadzhiyska, B., Hahn, C., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Juneau, S., Karaçayli, N. G., Kehoe, R., Kent, S., Kirkby, D., Kremin, A., Krolewski, A., Lai, Y., Lan, T. -W., Landriau, M., Lang, D., Lasker, J., Goff, J. M. Le, Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Linder, E., Lodha, K., Magneville, C., Manera, M., Margala, D., Martini, P., Maus, M., McDonald, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moon, J., Moore, S., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nguyen, N. M., Nie, J., Niz, G., Noriega, H. E., Padmanabhan, N., Paillas, E., Palanque-Delabrouille, N., Pan, J., Penmetsa, S., Percival, W. J., Pieri, M. M., Pinon, M., Poppett, C., Porredon, A., Prada, F., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Ravoux, C., Rezaie, M., Rich, J., Rocher, A., Rockosi, C., Roe, N. A., Rosado-Marin, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Samushia, L., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Sharples, R., Silber, J., Sinigaglia, F., Slosar, A., Smith, A., Sprayberry, D., Tan, T., Tarlé, G., Trusov, S., Vaisakh, R., Valcin, D., Valdes, F., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., Weinberg, D. H., White, M., Yu, J., Yu, Y., Yuan, S., Yèche, C., Zaborowski, E. A., Zarrouk, P., Zhang, H., Zhao, C., Zhao, R., Zhou, R., Zou, H., DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Alexander, D. M., Alvarez, M., Alves, O., Anand, A., Andrade, U., Armengaud, E., Avila, S., Aviles, A., Awan, H., Bailey, S., Baltay, C., Bault, A., Bautista, J., Behera, J., BenZvi, S., Beutler, F., Bianchi, D., Blake, C., Blum, R., Brieden, S., Brodzeller, A., Brooks, D., Buckley-Geer, E., Burtin, E., Calderon, R., Canning, R., Rosell, A. Carnero, Cereskaite, R., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chen, X., Claybaugh, T., Cole, S., Cuceu, A., Davis, T. M., Dawson, K., de la Cruz, R., de la Macorra, A., de Mattia, A., Deiosso, N., Dey, A., Dey, B., Ding, J., Ding, Z., Doel, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Fagrelius, P., Fanning, K., Ferraro, S., Ereza, J., Findlay, N., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Garcia-Quintero, C., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Green, D., Gruen, D., Gsponer, R., Gutierrez, G., Guy, J., Hadzhiyska, B., Hahn, C., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Juneau, S., Karaçayli, N. G., Kehoe, R., Kent, S., Kirkby, D., Kremin, A., Krolewski, A., Lai, Y., Lan, T. -W., Landriau, M., Lang, D., Lasker, J., Goff, J. M. Le, Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Linder, E., Lodha, K., Magneville, C., Manera, M., Margala, D., Martini, P., Maus, M., McDonald, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moon, J., Moore, S., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nguyen, N. M., Nie, J., Niz, G., Noriega, H. E., Padmanabhan, N., Paillas, E., Palanque-Delabrouille, N., Pan, J., Penmetsa, S., Percival, W. J., Pieri, M. M., Pinon, M., Poppett, C., Porredon, A., Prada, F., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Ravoux, C., Rezaie, M., Rich, J., Rocher, A., Rockosi, C., Roe, N. A., Rosado-Marin, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Samushia, L., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Sharples, R., Silber, J., Sinigaglia, F., Slosar, A., Smith, A., Sprayberry, D., Tan, T., Tarlé, G., Trusov, S., Vaisakh, R., Valcin, D., Valdes, F., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., Weinberg, D. H., White, M., Yu, J., Yu, Y., Yuan, S., Yèche, C., Zaborowski, E. A., Zarrouk, P., Zhang, H., Zhao, C., Zhao, R., Zhou, R., and Zou, H.
Abstract: We present the measurement of Baryon Acoustic Oscillations (BAO) from the Lyman-$\alpha$ (Ly$\alpha$) forest of high-redshift quasars with the first-year dataset of the Dark Energy Spectroscopic Instrument (DESI). Our analysis uses over $420\,000$ Ly$\alpha$ forest spectra and their correlation with the spatial distribution of more than $700\,000$ quasars. An essential facet of this work is the development of a new analysis methodology on a blinded dataset. We conducted rigorous tests using synthetic data to ensure the reliability of our methodology and findings before unblinding. Additionally, we conducted multiple data splits to assess the consistency of the results and scrutinized various analysis approaches to confirm their robustness. For a given value of the sound horizon ($r_d$), we measure the expansion at $z_{\rm eff}=2.33$ with 2\% precision, $H(z_{\rm eff}) = (239.2 \pm 4.8) (147.09~{\rm Mpc} /r_d)$ km/s/Mpc. Similarly, we present a 2.4\% measurement of the transverse comoving distance to the same redshift, $D_M(z_{\rm eff}) = (5.84 \pm 0.14) (r_d/147.09~{\rm Mpc})$ Gpc. Together with other DESI BAO measurements at lower redshifts, these results are used in a companion paper to constrain cosmological parameters., Comment: This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers)
Published: 2024

10. Optimal Reconstruction of Baryon Acoustic Oscillations for DESI 2024

Author: Paillas, E., Ding, Z., Chen, X., Seo, H., Padmanabhan, N., de Mattia, A., Ross, A. J., Nadathur, S., Howlett, C., Aguilar, J., Ahlen, S., Alves, O., Andrade, U., Brooks, D., Buckley-Geer, E., Burtin, E., Chen, S., Claybaugh, T., Cole, S., Dawson, K., de la Macorra, A., Dey, Arjun, Doel, P., Fanning, K., Ferraro, S., Forero-Romero, J. E., Garcia-Quintero, C., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gutierrez, G., Hahn, C., Hanif, M. M. S, Honscheid, K., Ishak, M., Kehoe, R., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Martini, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Newman, J. A., Nie, J., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Pérez-Fernández, A., Rashkovetskyi, M., Rezaie, M., Rosado-Marin, A., Rossi, G., Ruggeri, R., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Sprayberry, D., Tarlé, G., Valcin, D., Vargas-Magaña, M., Yu, J., Yuan, S., Zhou, R., Zou, H., Paillas, E., Ding, Z., Chen, X., Seo, H., Padmanabhan, N., de Mattia, A., Ross, A. J., Nadathur, S., Howlett, C., Aguilar, J., Ahlen, S., Alves, O., Andrade, U., Brooks, D., Buckley-Geer, E., Burtin, E., Chen, S., Claybaugh, T., Cole, S., Dawson, K., de la Macorra, A., Dey, Arjun, Doel, P., Fanning, K., Ferraro, S., Forero-Romero, J. E., Garcia-Quintero, C., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gutierrez, G., Hahn, C., Hanif, M. M. S, Honscheid, K., Ishak, M., Kehoe, R., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Martini, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Newman, J. A., Nie, J., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Pérez-Fernández, A., Rashkovetskyi, M., Rezaie, M., Rosado-Marin, A., Rossi, G., Ruggeri, R., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Sprayberry, D., Tarlé, G., Valcin, D., Vargas-Magaña, M., Yu, J., Yuan, S., Zhou, R., and Zou, H.
Abstract: Baryon acoustic oscillations (BAO) provide a robust standard ruler to measure the expansion history of the Universe through galaxy clustering. Density-field reconstruction is now a widely adopted procedure for increasing the precision and accuracy of the BAO detection. With the goal of finding the optimal reconstruction settings to be used in the DESI 2024 galaxy BAO analysis, we assess the sensitivity of the post-reconstruction BAO constraints to different choices in our analysis configuration, performing tests on blinded data from the first year of DESI observations (DR1), as well as on mocks that mimic the expected clustering and selection properties of the DESI DR1 target samples. Overall, we find that BAO constraints remain robust against multiple aspects in the reconstruction process, including the choice of smoothing scale, treatment of redshift-space distortions, fiber assignment incompleteness, and parameterizations of the BAO model. We also present a series of tests that DESI followed in order to assess the maturity of the end-to-end galaxy BAO pipeline before the unblinding of the large-scale structure catalogs., Comment: Supporting publication of DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars
Published: 2024

11. Methane Emission From a Cool Brown Dwarf

Author: Faherty, Jacqueline K., Burningham, Ben, Gagné, Jonathan, Suárez, Genaro, Vos, Johanna M., Merchan, Sherelyn Alejandro, Morley, Caroline V., Rowland, Melanie, Lacy, Brianna, Kiman, Rocio, Caselden, Dan, Kirkpatrick, J. Davy, Meisner, Aaron, Schneider, Adam C., Kuchner, Marc Jason, Gagliuffi, Daniella Carolina Bardalez, Beichman, Charles, Eisenhardt, Peter, Gelino, Christopher R., Gharib-Nezhad, Ehsan, Gonzales, Eileen, Marocco, Federico, Rothermich, Austin James, Whiteford, Niall, Faherty, Jacqueline K., Burningham, Ben, Gagné, Jonathan, Suárez, Genaro, Vos, Johanna M., Merchan, Sherelyn Alejandro, Morley, Caroline V., Rowland, Melanie, Lacy, Brianna, Kiman, Rocio, Caselden, Dan, Kirkpatrick, J. Davy, Meisner, Aaron, Schneider, Adam C., Kuchner, Marc Jason, Gagliuffi, Daniella Carolina Bardalez, Beichman, Charles, Eisenhardt, Peter, Gelino, Christopher R., Gharib-Nezhad, Ehsan, Gonzales, Eileen, Marocco, Federico, Rothermich, Austin James, and Whiteford, Niall
Abstract: Beyond our solar system, aurorae have been inferred from radio observations of isolated brown dwarfs (e.g. Hallinan et al. 2006; Kao et al. 2023). Within our solar system, giant planets have auroral emission with signatures across the electromagnetic spectrum including infrared emission of H3+ and methane. Isolated brown dwarfs with auroral signatures in the radio have been searched for corresponding infrared features but have only had null detections (e.g. Gibbs et al. 2022). CWISEP J193518.59-154620.3. (W1935 for short) is an isolated brown dwarf with a temperature of ~482 K. Here we report JWST observations of strong methane emission from W1935 at 3.326 microns. Atmospheric modeling leads us to conclude that a temperature inversion of ~300 K centered at 1-10 millibar replicates the feature. This represents an atmospheric temperature inversion for a Jupiter-like atmosphere without irradiation from a host star. A plausible explanation for the strong inversion is heating by auroral processes, although other internal and/or external dynamical processes cannot be ruled out. The best fit model rules out the contribution of H3+ emission which is prominent in solar system gas giants however this is consistent with rapid destruction of H3+ at the higher pressure where the W1935 emission originates (e.g. Helling et al. 2019)., Comment: Accepted in Nature 9 February 2024
Published: 2024
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12. Validating the Galaxy and Quasar Catalog-Level Blinding Scheme for the DESI 2024 analysis

Author: Andrade, U., Mena-Fernández, J., Awan, H., Ross, A. J., Brieden, S., Pan, J., de Mattia, A., Aguilar, J., Ahlen, S., Alves, O., Brooks, D., Buckley-Geer, E., Chaussidon, E., Claybaugh, T., Cole, S., de la Macorra, A., Dey, Arjun, Doel, P., Fanning, K., Forero-Romero, J. E., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Guy, J., Hahn, C., Hanif, M. M. S, Honscheid, K., Howlett, C., Huterer, D., Juneau, S., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Martini, P., Meisner, A., Miquel, R., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Newman, J. A., Nie, J., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Pinon, M., Poppett, C., Prada, F., Rashkovetskyi, M., Rezaie, M., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Sprayberry, D., Tarlé, G., Vargas-Magaña, M., Verde, L., Weaver, B. A., Andrade, U., Mena-Fernández, J., Awan, H., Ross, A. J., Brieden, S., Pan, J., de Mattia, A., Aguilar, J., Ahlen, S., Alves, O., Brooks, D., Buckley-Geer, E., Chaussidon, E., Claybaugh, T., Cole, S., de la Macorra, A., Dey, Arjun, Doel, P., Fanning, K., Forero-Romero, J. E., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Guy, J., Hahn, C., Hanif, M. M. S, Honscheid, K., Howlett, C., Huterer, D., Juneau, S., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Martini, P., Meisner, A., Miquel, R., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Newman, J. A., Nie, J., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Pinon, M., Poppett, C., Prada, F., Rashkovetskyi, M., Rezaie, M., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Sprayberry, D., Tarlé, G., Vargas-Magaña, M., Verde, L., and Weaver, B. A.
Abstract: In the era of precision cosmology, ensuring the integrity of data analysis through blinding techniques is paramount -- a challenge particularly relevant for the Dark Energy Spectroscopic Instrument (DESI). DESI represents a monumental effort to map the cosmic web, with the goal to measure the redshifts of tens of millions of galaxies and quasars. Given the data volume and the impact of the findings, the potential for confirmation bias poses a significant challenge. To address this, we implement and validate a comprehensive blind analysis strategy for DESI Data Release 1 (DR1), tailored to the specific observables DESI is most sensitive to: Baryonic Acoustic Oscillations (BAO), Redshift-Space Distortion (RSD) and primordial non-Gaussianities (PNG). We carry out the blinding at the catalog level, implementing shifts in the redshifts of the observed galaxies to blind for BAO and RSD signals and weights to blind for PNG through a scale-dependent bias. We validate the blinding technique on mocks, as well as on data by applying a second blinding layer to perform a battery of sanity checks. We find that the blinding strategy alters the data vector in a controlled way such that the BAO and RSD analysis choices do not need any modification before and after unblinding. The successful validation of the blinding strategy paves the way for the unblinded DESI DR1 analysis, alongside future blind analyses with DESI and other surveys., Comment: Supporting publication of "DESI 2024 II: Sample definitions, characteristics, and two-point clustering statistics", "DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars", and "DESI 2024 V: Analysis of the full shape of two-point clustering statistics from galaxies and quasars". (v2 - update DESI references)
Published: 2024

13. Characterization of contaminants in the Lyman-alpha forest auto-correlation with DESI

Author: Guy, J., Gontcho, S. Gontcho A, Armengaud, E., Brodzeller, A., Cuceu, A., Font-Ribera, A., Herrera-Alcantar, H. K., Karaçaylı, N. G., Muñoz-Gutiérrez, A., Pieri, M., Pérez-Ràfols, I., Ramírez-Pérez, C., Ravoux, C., Rich, J., Walther, M., Karim, M. Abdul, Aguilar, J., Ahlen, S., Bault, A., Brooks, D., Claybaugh, T., de la Cruz, R., de la Macorra, A., Doel, P., Fanning, K., Forero-Romero, J. E., Gaztañaga, E., Gonzalez-Morales, A. X., Gutierrez, G., Hahn, C., Honscheid, K., Juneau, S., Kehoe, R., Kirkby, D., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Guillou, L. Le, Manera, M., Martini, P., Meisner, A., Miquel, R., Montero-Camacho, P., Moustakas, J., Mueller, E., Myers, A. D., Nie, J., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Rezaie, M., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Silber, J., Sprayberry, D., Tan, T., Tarlé, G., Vargas-Magaña, M., Zou, H., Guy, J., Gontcho, S. Gontcho A, Armengaud, E., Brodzeller, A., Cuceu, A., Font-Ribera, A., Herrera-Alcantar, H. K., Karaçaylı, N. G., Muñoz-Gutiérrez, A., Pieri, M., Pérez-Ràfols, I., Ramírez-Pérez, C., Ravoux, C., Rich, J., Walther, M., Karim, M. Abdul, Aguilar, J., Ahlen, S., Bault, A., Brooks, D., Claybaugh, T., de la Cruz, R., de la Macorra, A., Doel, P., Fanning, K., Forero-Romero, J. E., Gaztañaga, E., Gonzalez-Morales, A. X., Gutierrez, G., Hahn, C., Honscheid, K., Juneau, S., Kehoe, R., Kirkby, D., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Guillou, L. Le, Manera, M., Martini, P., Meisner, A., Miquel, R., Montero-Camacho, P., Moustakas, J., Mueller, E., Myers, A. D., Nie, J., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Rezaie, M., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Silber, J., Sprayberry, D., Tan, T., Tarlé, G., Vargas-Magaña, M., and Zou, H.
Abstract: Baryon Acoustic Oscillations can be measured with sub-percent precision above redshift two with the Lyman-alpha forest auto-correlation and its cross-correlation with quasar positions. This is one of the key goals of the Dark Energy Spectroscopic Instrument (DESI) which started its main survey in May 2021. We present in this paper a study of the contaminants to the lyman-alpha forest which are mainly caused by correlated signals introduced by the spectroscopic data processing pipeline as well as astrophysical contaminants due to foreground absorption in the intergalactic medium. Notably, an excess signal caused by the sky background subtraction noise is present in the lyman-alpha auto-correlation in the first line-of-sight separation bin. We use synthetic data to isolate this contribution, we also characterize the effect of spectro-photometric calibration noise, and propose a simple model to account for both effects in the analysis of the lyman-alpha forest. We then measure the auto-correlation of the quasar flux transmission fraction of low redshift quasars, where there is no lyman-alpha forest absorption but only its contaminants. We demonstrate that we can interpret the data with a two-component model: data processing noise and triply ionized Silicon and Carbon auto-correlations. This result can be used to improve the modeling of the lyman-alpha auto-correlation function measured with DESI., Comment: 30 pages, 12 figures
Published: 2024

14. DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations

Author: DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Alexander, D. M., Alvarez, M., Alves, O., Anand, A., Andrade, U., Armengaud, E., Avila, S., Aviles, A., Awan, H., Bahr-Kalus, B., Bailey, S., Baltay, C., Bault, A., Behera, J., BenZvi, S., Bera, A., Beutler, F., Bianchi, D., Blake, C., Blum, R., Brieden, S., Brodzeller, A., Brooks, D., Buckley-Geer, E., Burtin, E., Calderon, R., Canning, R., Rosell, A. Carnero, Cereskaite, R., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chen, X., Claybaugh, T., Cole, S., Cuceu, A., Davis, T. M., Dawson, K., de la Macorra, A., de Mattia, A., Deiosso, N., Dey, A., Dey, B., Ding, Z., Doel, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Fagrelius, P., Fanning, K., Ferraro, S., Ereza, J., Findlay, N., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Frenk, C. S., Garcia-Quintero, C., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Green, D., Gruen, D., Gsponer, R., Gutierrez, G., Guy, J., Hadzhiyska, B., Hahn, C., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Juneau, S., Karaçaylı, N. G., Kehoe, R., Kent, S., Kirkby, D., Kremin, A., Krolewski, A., Lai, Y., Lan, T. -W., Landriau, M., Lang, D., Lasker, J., Goff, J. M. Le, Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Linder, E., Lodha, K., Magneville, C., Manera, M., Margala, D., Martini, P., Maus, M., McDonald, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moon, J., Moore, S., Moustakas, J., Mudur, N., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nguyen, N. M., Nie, J., Niz, G., Noriega, H. E., Padmanabhan, N., Paillas, E., Palanque-Delabrouille, N., Pan, J., Penmetsa, S., Percival, W. J., Pieri, M., Pinon, M., Poppett, C., Porredon, A., Prada, F., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Rezaie, M., Rich, J., Rocher, A., Rockosi, C., Roe, N. A., Rosado-Marin, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Samushia, L., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Shafieloo, A., Sharples, R., Silber, J., Slosar, A., Smith, A., Sprayberry, D., Tan, T., Tarlé, G., Taylor, P., Trusov, S., Ureña-López, L. A., Vaisakh, R., Valcin, D., Valdes, F., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., Weinberg, D. H., White, M., Yu, J., Yu, Y., Yuan, S., Yèche, C., Zaborowski, E. A., Zarrouk, P., Zhang, H., Zhao, C., Zhao, R., Zhou, R., Zhuang, T., Zou, H., DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Alexander, D. M., Alvarez, M., Alves, O., Anand, A., Andrade, U., Armengaud, E., Avila, S., Aviles, A., Awan, H., Bahr-Kalus, B., Bailey, S., Baltay, C., Bault, A., Behera, J., BenZvi, S., Bera, A., Beutler, F., Bianchi, D., Blake, C., Blum, R., Brieden, S., Brodzeller, A., Brooks, D., Buckley-Geer, E., Burtin, E., Calderon, R., Canning, R., Rosell, A. Carnero, Cereskaite, R., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chen, X., Claybaugh, T., Cole, S., Cuceu, A., Davis, T. M., Dawson, K., de la Macorra, A., de Mattia, A., Deiosso, N., Dey, A., Dey, B., Ding, Z., Doel, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Fagrelius, P., Fanning, K., Ferraro, S., Ereza, J., Findlay, N., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Frenk, C. S., Garcia-Quintero, C., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Green, D., Gruen, D., Gsponer, R., Gutierrez, G., Guy, J., Hadzhiyska, B., Hahn, C., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Juneau, S., Karaçaylı, N. G., Kehoe, R., Kent, S., Kirkby, D., Kremin, A., Krolewski, A., Lai, Y., Lan, T. -W., Landriau, M., Lang, D., Lasker, J., Goff, J. M. Le, Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Linder, E., Lodha, K., Magneville, C., Manera, M., Margala, D., Martini, P., Maus, M., McDonald, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moon, J., Moore, S., Moustakas, J., Mudur, N., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nguyen, N. M., Nie, J., Niz, G., Noriega, H. E., Padmanabhan, N., Paillas, E., Palanque-Delabrouille, N., Pan, J., Penmetsa, S., Percival, W. J., Pieri, M., Pinon, M., Poppett, C., Porredon, A., Prada, F., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Rezaie, M., Rich, J., Rocher, A., Rockosi, C., Roe, N. A., Rosado-Marin, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Samushia, L., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Shafieloo, A., Sharples, R., Silber, J., Slosar, A., Smith, A., Sprayberry, D., Tan, T., Tarlé, G., Taylor, P., Trusov, S., Ureña-López, L. A., Vaisakh, R., Valcin, D., Valdes, F., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., Weinberg, D. H., White, M., Yu, J., Yu, Y., Yuan, S., Yèche, C., Zaborowski, E. A., Zarrouk, P., Zhang, H., Zhao, C., Zhao, R., Zhou, R., Zhuang, T., and Zou, H.
Abstract: We present cosmological results from the measurement of baryon acoustic oscillations (BAO) in galaxy, quasar and Lyman-$\alpha$ forest tracers from the first year of observations from the Dark Energy Spectroscopic Instrument (DESI), to be released in the DESI Data Release 1. DESI BAO provide robust measurements of the transverse comoving distance and Hubble rate, or their combination, relative to the sound horizon, in seven redshift bins from over 6 million extragalactic objects in the redshift range $0.1-1$ and $w_a<0$. This preference is 2.6$\sigma$ for the DESI+CMB combination, and persists or grows when SN~Ia are added in, giving results discrepant with the $\Lambda$CDM model at the $2.5\sigma$, $3.5\sigma$ or $3.9\sigma$ levels for the addition of Pantheon+, Union3, or DES-SN5YR datasets respectively. For the flat $\Lambda$CDM model with the sum of neutrino mass $\sum m_\nu$ free, combining the DESI and CMB data yields an upper limit $\sum m_\nu < 0.072$ $(0.113)$ eV at 95% confidence for a $\sum m_\nu>0$ $(\sum m_\nu>0.059)$ eV prior. These neutrino-mass constraints are substantially relaxed in models beyond $\Lambda$CDM. [Abridged.], Comment: This DESI Collaboration Key Publication is part of the 2024 publication series using the first year of observations (see https://data.desi.lbl.gov/doc/papers)
Published: 2024

15. Validation of the DESI 2024 Ly$\alpha$ forest BAO analysis using synthetic datasets

Author: Cuceu, Andrei, Herrera-Alcantar, Hiram K., Gordon, Calum, Martini, Paul, Guy, Julien, Font-Ribera, Andreu, Gonzalez-Morales, Alma X., Karim, M. Abdul, Aguilar, J., Ahlen, S., Armengaud, E., Bault, A., Brooks, D., Claybaugh, T., de la Macorra, A., Doel, P., Fanning, K., Ferraro, S., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Honscheid, K., Howlett, C., Karaçaylı, N. G., Kirkby, D., Kremin, A., Landriau, M., Goff, J. M. Le, Guillou, L. Le, Levi, M. E., Manera, M., Meisner, A., Miquel, R., Moustakas, J., Muñoz-Gutiérrez, A., Myers, A. D., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Pérez-Ràfols, I., Ramírez-Pérez, C., Ravoux, C., Rezaie, M., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Sprayberry, D., Tan, T., Tarlé, G., Vargas-Magaña, M., Walther, M., Weaver, B. A., Zhou, R., Zou, H., Cuceu, Andrei, Herrera-Alcantar, Hiram K., Gordon, Calum, Martini, Paul, Guy, Julien, Font-Ribera, Andreu, Gonzalez-Morales, Alma X., Karim, M. Abdul, Aguilar, J., Ahlen, S., Armengaud, E., Bault, A., Brooks, D., Claybaugh, T., de la Macorra, A., Doel, P., Fanning, K., Ferraro, S., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Honscheid, K., Howlett, C., Karaçaylı, N. G., Kirkby, D., Kremin, A., Landriau, M., Goff, J. M. Le, Guillou, L. Le, Levi, M. E., Manera, M., Meisner, A., Miquel, R., Moustakas, J., Muñoz-Gutiérrez, A., Myers, A. D., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Pérez-Ràfols, I., Ramírez-Pérez, C., Ravoux, C., Rezaie, M., Rossi, G., Sanchez, E., Schlegel, D., Schubnell, M., Seo, H., Sprayberry, D., Tan, T., Tarlé, G., Vargas-Magaña, M., Walther, M., Weaver, B. A., Zhou, R., and Zou, H.
Abstract: The first year of data from the Dark Energy Spectroscopic Instrument (DESI) contains the largest set of Lyman-$\alpha$ (Ly$\alpha$) forest spectra ever observed. This data, collected in the DESI Data Release 1 (DR1) sample, has been used to measure the Baryon Acoustic Oscillation (BAO) feature at redshift $z=2.33$. In this work, we use a set of 150 synthetic realizations of DESI DR1 to validate the DESI 2024 Ly$\alpha$ forest BAO measurement. The synthetic data sets are based on Gaussian random fields using the log-normal approximation. We produce realistic synthetic DESI spectra that include all major contaminants affecting the Ly$\alpha$ forest. The synthetic data sets span a redshift range $1.8
Published: 2024

16. HOD-Dependent Systematics for Luminous Red Galaxies in the DESI 2024 BAO Analysis

Author: Mena-Fernández, J., Garcia-Quintero, C., Yuan, S., Hadzhiyska, B., Alves, O., Rashkovetskyi, M., Seo, H., Padmanabhan, N., Nadathur, S., Howlett, C., Alam, S., Rocher, A., Ross, A. J., Sanchez, E., Ishak, M., Aguilar, J., Ahlen, S., Andrade, U., BenZvi, S., Brooks, D., Burtin, E., Chen, S., Chen, X., Claybaugh, T., Cole, S., de la Macorra, A., de Mattia, A., Dey, Arjun, Dey, B., Ding, Z., Doel, P., Fanning, K., Forero-Romero, J. E., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gutierrez, G., Guy, J., Hahn, C., Honscheid, K., Juneau, S., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Martini, P., Medina-Varela, L., Meisner, A., Miquel, R., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Newman, J. A., Nie, J., Niz, G., Paillas, E., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Pérez-Fernández, A., Rosado-Marin, A., Rossi, G., Ruggeri, R., Saulder, C., Schlegel, D., Schubnell, M., Sprayberry, D., Tarlé, G., Vargas-Magaña, M., Weaver, B. A., Yu, J., Zhang, H., Zou, H., Mena-Fernández, J., Garcia-Quintero, C., Yuan, S., Hadzhiyska, B., Alves, O., Rashkovetskyi, M., Seo, H., Padmanabhan, N., Nadathur, S., Howlett, C., Alam, S., Rocher, A., Ross, A. J., Sanchez, E., Ishak, M., Aguilar, J., Ahlen, S., Andrade, U., BenZvi, S., Brooks, D., Burtin, E., Chen, S., Chen, X., Claybaugh, T., Cole, S., de la Macorra, A., de Mattia, A., Dey, Arjun, Dey, B., Ding, Z., Doel, P., Fanning, K., Forero-Romero, J. E., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gutierrez, G., Guy, J., Hahn, C., Honscheid, K., Juneau, S., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Martini, P., Medina-Varela, L., Meisner, A., Miquel, R., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Newman, J. A., Nie, J., Niz, G., Paillas, E., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Pérez-Fernández, A., Rosado-Marin, A., Rossi, G., Ruggeri, R., Saulder, C., Schlegel, D., Schubnell, M., Sprayberry, D., Tarlé, G., Vargas-Magaña, M., Weaver, B. A., Yu, J., Zhang, H., and Zou, H.
Abstract: In this paper, we present the estimation of systematics related to the halo occupation distribution (HOD) modeling in the baryon acoustic oscillations (BAO) distance measurement of the Dark Energy Spectroscopic Instrument (DESI) 2024 analysis. This paper focuses on the study of HOD systematics for luminous red galaxies (LRG). We consider three different HOD models for LRGs, including the base 5-parameter vanilla model and two extensions to it, that we refer to as baseline and extended models. The baseline model is described by the 5 vanilla HOD parameters, an incompleteness factor and a velocity bias parameter, whereas the extended one also includes a galaxy assembly bias and a satellite profile parameter. We utilize the 25 dark matter simulations available in the AbacusSummit simulation suite at $z=$ 0.8 and generate mock catalogs for our different HOD models. To test the impact of the HOD modeling in the position of the BAO peak, we run BAO fits for all these sets of simulations and compare the best-fit BAO-scaling parameters $\alpha_{\rm iso}$ and $\alpha_{\rm AP}$ between every pair of HOD models. We do this for both Fourier and configuration spaces independently, using post-reconstruction measurements. We find a 3.3$\sigma$ detection of HOD systematic for $\alpha_{\rm AP}$ in configuration space with an amplitude of 0.19%. For the other cases, we did not find a 3$\sigma$ detection, and we decided to compute a conservative estimation of the systematic using the ensemble of shifts between all pairs of HOD models. By doing this, we quote a systematic with an amplitude of 0.07% in $\alpha_{\rm iso}$ for both Fourier and configuration spaces; and of 0.09% in $\alpha_{\rm AP}$ for Fourier space., Comment: 36 pages, 9 figures. Supporting publication of DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars
Published: 2024

17. DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars

Author: DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Alexander, D. M., Alvarez, M., Alves, O., Anand, A., Andrade, U., Armengaud, E., Avila, S., Aviles, A., Awan, H., Bailey, S., Baltay, C., Bault, A., Behera, J., BenZvi, S., Beutler, F., Bianchi, D., Blake, C., Blum, R., Brieden, S., Brodzeller, A., Brooks, D., Buckley-Geer, E., Burtin, E., Calderon, R., Canning, R., Rosell, A. Carnero, Cereskaite, R., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chen, X., Claybaugh, T., Cole, S., Cuceu, A., Davis, T. M., Dawson, K., de la Macorra, A., de Mattia, A., Deiosso, N., Dey, A., Dey, B., Ding, Z., Doel, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Fagrelius, P., Fanning, K., Ferraro, S., Ereza, J., Findlay, N., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Garcia-Quintero, C., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Green, D., Gruen, D., Gsponer, R., Gutierrez, G., Guy, J., Hadzhiyska, B., Hahn, C., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Juneau, S., Karaçaylı, N. G., Kehoe, R., Kent, S., Kirkby, D., Kremin, A., Krolewski, A., Lai, Y., Lan, T. -W., Landriau, M., Lang, D., Lasker, J., Goff, J. M. Le, Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Linder, E., Lodha, K., Magneville, C., Manera, M., Margala, D., Martini, P., Maus, M., McDonald, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moon, J., Moore, S., Moustakas, J., Mudur, N., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nguyen, N. M., Nie, J., Niz, G., Noriega, H. E., Padmanabhan, N., Paillas, E., Palanque-Delabrouille, N., Pan, J., Penmetsa, S., Percival, W. J., Pieri, M., Pinon, M., Poppett, C., Porredon, A., Prada, F., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Rezaie, M., Rich, J., Rocher, A., Rockosi, C., Roe, N. A., Rosado-Marin, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Samushia, L., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Sharples, R., Silber, J., Slosar, A., Smith, A., Sprayberry, D., Swanson, J., Tan, T., Tarlé, G., Trusov, S., Vaisakh, R., Valcin, D., Valdes, F., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., Weinberg, D. H., White, M., Yu, J., Yu, Y., Yuan, S., Yèche, C., Zaborowski, E. A., Zarrouk, P., Zhang, H., Zhao, C., Zhao, R., Zhou, R., Zou, H., DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Alexander, D. M., Alvarez, M., Alves, O., Anand, A., Andrade, U., Armengaud, E., Avila, S., Aviles, A., Awan, H., Bailey, S., Baltay, C., Bault, A., Behera, J., BenZvi, S., Beutler, F., Bianchi, D., Blake, C., Blum, R., Brieden, S., Brodzeller, A., Brooks, D., Buckley-Geer, E., Burtin, E., Calderon, R., Canning, R., Rosell, A. Carnero, Cereskaite, R., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chen, X., Claybaugh, T., Cole, S., Cuceu, A., Davis, T. M., Dawson, K., de la Macorra, A., de Mattia, A., Deiosso, N., Dey, A., Dey, B., Ding, Z., Doel, P., Edelstein, J., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Fagrelius, P., Fanning, K., Ferraro, S., Ereza, J., Findlay, N., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Garcia-Quintero, C., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Green, D., Gruen, D., Gsponer, R., Gutierrez, G., Guy, J., Hadzhiyska, B., Hahn, C., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Juneau, S., Karaçaylı, N. G., Kehoe, R., Kent, S., Kirkby, D., Kremin, A., Krolewski, A., Lai, Y., Lan, T. -W., Landriau, M., Lang, D., Lasker, J., Goff, J. M. Le, Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Linder, E., Lodha, K., Magneville, C., Manera, M., Margala, D., Martini, P., Maus, M., McDonald, P., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Miquel, R., Moon, J., Moore, S., Moustakas, J., Mudur, N., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nguyen, N. M., Nie, J., Niz, G., Noriega, H. E., Padmanabhan, N., Paillas, E., Palanque-Delabrouille, N., Pan, J., Penmetsa, S., Percival, W. J., Pieri, M., Pinon, M., Poppett, C., Porredon, A., Prada, F., Pérez-Fernández, A., Pérez-Ràfols, I., Rabinowitz, D., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Rezaie, M., Rich, J., Rocher, A., Rockosi, C., Roe, N. A., Rosado-Marin, A., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Samushia, L., Sanchez, E., Saulder, C., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Sharples, R., Silber, J., Slosar, A., Smith, A., Sprayberry, D., Swanson, J., Tan, T., Tarlé, G., Trusov, S., Vaisakh, R., Valcin, D., Valdes, F., Vargas-Magaña, M., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., Weinberg, D. H., White, M., Yu, J., Yu, Y., Yuan, S., Yèche, C., Zaborowski, E. A., Zarrouk, P., Zhang, H., Zhao, C., Zhao, R., Zhou, R., and Zou, H.
Abstract: We present the DESI 2024 galaxy and quasar baryon acoustic oscillations (BAO) measurements using over 5.7 million unique galaxy and quasar redshifts in the range 0.1
Published: 2024

18. Emission Line Predictions for Mock Galaxy Catalogues: a New Differentiable and Empirical Mapping from DESI

Author: Khederlarian, Ashod, Newman, Jeffrey A., Andrews, Brett H., Dey, Biprateep, Moustakas, John, Hearin, Andrew, Juneau, Stéphanie, Tortorelli, Luca, Gruen, Daniel, Hahn, ChangHoon, Canning, Rebecca E. A., Aguilar, Jessica Nicole, Ahlen, Steven, Brooks, David, Claybaugh, Todd, de la Macorra, Axel, Doel, Peter, Fanning, Kevin, Ferraro, Simone, Forero-Romero, Jaime, Gaztañaga, Enrique, Gontcho, Satya Gontcho A, Kehoe, Robert, Kisner, Theodore, Kremin, Anthony, Lambert, Andrew, Landriau, Martin, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Mueller, Eva-Maria, Muñoz-Gutiérrez, Andrea, Myers, Adam, Nie, Jundan, Poppett, Claire, Prada, Francisco, Rezaie, Mehdi, Rossi, Graziano, Sanchez, Eusebio, Schubnell, Michael, Silber, Joseph Harry, Sprayberry, David, Tarlé, Gregory, Weaver, Benjamin Alan, Zhou, Zhimin, Zou, Hu, Khederlarian, Ashod, Newman, Jeffrey A., Andrews, Brett H., Dey, Biprateep, Moustakas, John, Hearin, Andrew, Juneau, Stéphanie, Tortorelli, Luca, Gruen, Daniel, Hahn, ChangHoon, Canning, Rebecca E. A., Aguilar, Jessica Nicole, Ahlen, Steven, Brooks, David, Claybaugh, Todd, de la Macorra, Axel, Doel, Peter, Fanning, Kevin, Ferraro, Simone, Forero-Romero, Jaime, Gaztañaga, Enrique, Gontcho, Satya Gontcho A, Kehoe, Robert, Kisner, Theodore, Kremin, Anthony, Lambert, Andrew, Landriau, Martin, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Mueller, Eva-Maria, Muñoz-Gutiérrez, Andrea, Myers, Adam, Nie, Jundan, Poppett, Claire, Prada, Francisco, Rezaie, Mehdi, Rossi, Graziano, Sanchez, Eusebio, Schubnell, Michael, Silber, Joseph Harry, Sprayberry, David, Tarlé, Gregory, Weaver, Benjamin Alan, Zhou, Zhimin, and Zou, Hu
Abstract: We present a simple, differentiable method for predicting emission line strengths from rest-frame optical continua using an empirically-determined mapping. Extensive work has been done to develop mock galaxy catalogues that include robust predictions for galaxy photometry, but reliably predicting the strengths of emission lines has remained challenging. Our new mapping is a simple neural network implemented using the JAX Python automatic differentiation library. It is trained on Dark Energy Spectroscopic Instrument Early Release data to predict the equivalent widths (EWs) of the eight brightest optical emission lines (including H$\alpha$, H$\beta$, [O II], and [O III]) from a galaxy's rest-frame optical continuum. The predicted EW distributions are consistent with the observed ones when noise is accounted for, and we find Spearman's rank correlation coefficient $\rho_s > 0.87$ between predictions and observations for most lines. Using a non-linear dimensionality reduction technique (UMAP), we show that this is true for galaxies across the full range of observed spectral energy distributions. In addition, we find that adding measurement uncertainties to the predicted line strengths is essential for reproducing the distribution of observed line-ratios in the BPT diagram. Our trained network can easily be incorporated into a differentiable stellar population synthesis pipeline without hindering differentiability or scalability with GPUs. A synthetic catalogue generated with such a pipeline can be used to characterise and account for biases in the spectroscopic training sets used for training and calibration of photo-$z$'s, improving the modelling of systematic incompleteness for the Rubin Observatory LSST and other surveys., Comment: 17 pages, 8 figures, 1 table. Submitted to MNRAS
Published: 2024

19. HOD-Dependent Systematics in Emission Line Galaxies for the DESI 2024 BAO analysis

Author: Garcia-Quintero, C., Mena-Fernández, J., Rocher, A., Yuan, S., Hadzhiyska, B., Alves, O., Rashkovetskyi, M., Seo, H., Padmanabhan, N., Nadathur, S., Howlett, C., Ishak, M., Medina-Varela, L., McDonald, P., Ross, A. J., Xie, Y., Chen, X., Bera, A., Aguilar, J., Ahlen, S., Andrade, U., BenZvi, S., Brooks, D., Burtin, E., Chen, S., Claybaugh, T., Cole, S., de la Macorra, A., de Mattia, A., Dey, A., Dey, B., Ding, Z., Doel, P., Fanning, K., Forero-Romero, J. E., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gutierrez, G., Guy, J., Hahn, C., Honscheid, K., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Martini, P., Meisner, A., Miquel, R., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Newman, J. A., Nie, J., Niz, G., Paillas, E., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Pérez-Fernández, A., Rosado-Marin, A., Rossi, G., Ruggeri, R., Sanchez, E., Schlegel, D., Schubnell, M., Sprayberry, D., Tarlé, G., Vargas-Magaña, M., Weaver, B. A., Yu, J., Zhang, H., Zhou, R., Zou, H., Garcia-Quintero, C., Mena-Fernández, J., Rocher, A., Yuan, S., Hadzhiyska, B., Alves, O., Rashkovetskyi, M., Seo, H., Padmanabhan, N., Nadathur, S., Howlett, C., Ishak, M., Medina-Varela, L., McDonald, P., Ross, A. J., Xie, Y., Chen, X., Bera, A., Aguilar, J., Ahlen, S., Andrade, U., BenZvi, S., Brooks, D., Burtin, E., Chen, S., Claybaugh, T., Cole, S., de la Macorra, A., de Mattia, A., Dey, A., Dey, B., Ding, Z., Doel, P., Fanning, K., Forero-Romero, J. E., Gaztañaga, E., Gil-Marín, H., Gontcho, S. Gontcho A, Gutierrez, G., Guy, J., Hahn, C., Honscheid, K., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Martini, P., Meisner, A., Miquel, R., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Myers, A. D., Newman, J. A., Nie, J., Niz, G., Paillas, E., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Pérez-Fernández, A., Rosado-Marin, A., Rossi, G., Ruggeri, R., Sanchez, E., Schlegel, D., Schubnell, M., Sprayberry, D., Tarlé, G., Vargas-Magaña, M., Weaver, B. A., Yu, J., Zhang, H., Zhou, R., and Zou, H.
Abstract: The Dark Energy Spectroscopic Instrument (DESI) will provide precise measurements of Baryon Acoustic Oscillations (BAO) to constrain the expansion history of the Universe and set stringent constraints on dark energy. Therefore, precise control of the global error budget due to various systematic effects is required for the DESI 2024 BAO analysis. In this work, we focus on the robustness of the BAO analysis against the Halo Occupation Distribution (HOD) modeling for the Emission Line Galaxy (ELG) tracer. Based on a common dark matter simulation, our analysis relies on HOD mocks tuned to early DESI data, namely the One-Percent survey data. To build the mocks, we use several HOD models for the ELG tracer as well as extensions to the baseline HOD models. Among these extensions, we consider distinct recipes for galactic conformity and assembly bias. We perform two independent analyses in the Fourier space and in the configuration space. We recover the BAO signal from two-point measurements after performing reconstruction on our mocks. Additionally, we also apply the control variates technique to reduce sample variance noise. Our BAO analysis can recover the isotropic BAO parameter $\alpha_\text{iso}$ within 0.1\% and the Alcock Paczynski parameter $\alpha_\text{AP}$ within 0.3\%. Overall, we find that our systematic error due to the HOD dependence is below 0.17\%, with the Fourier space analysis being more robust against the HOD systematics. We conclude that our analysis pipeline is robust enough against the HOD systematics for the ELG tracer in the DESI 2024 BAO analysis., Comment: Supporting publication of DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars
Published: 2024

20. Identifying Quasars from the DESI Bright Galaxy Survey

Author: Juneau, S., Canning, R., Alexander, D. M., Pucha, R., Fawcett, V. A., Myers, A. D., Moustakas, J., Ruiz-Macias, O., Cole, S., Pan, Z., Aguilar, J., Ahlen, S., Alam, S., Bailey, S., Brooks, D., Chaussidon, E., Circosta, C., Claybaugh, T., Dawson, K., de la Macorra, A., Dey, Arjun, Doel, P., Fanning, K., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Hahn, C., Honscheid, K., Kehoe, R., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Guillou, L. Le, Manera, M., Martini, P., Meisner, A., Miquel, R., Muñoz-Gutiérrez, A., Nie, J., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Ravoux, C., Rezaie, M., Rossi, G., Sanchez, E., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Silber, J., Siudek, M., Sprayberry, D., Tarlé, G., Zhou, Z., Zou, H., Juneau, S., Canning, R., Alexander, D. M., Pucha, R., Fawcett, V. A., Myers, A. D., Moustakas, J., Ruiz-Macias, O., Cole, S., Pan, Z., Aguilar, J., Ahlen, S., Alam, S., Bailey, S., Brooks, D., Chaussidon, E., Circosta, C., Claybaugh, T., Dawson, K., de la Macorra, A., Dey, Arjun, Doel, P., Fanning, K., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gutierrez, G., Hahn, C., Honscheid, K., Kehoe, R., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Guillou, L. Le, Manera, M., Martini, P., Meisner, A., Miquel, R., Muñoz-Gutiérrez, A., Nie, J., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Ravoux, C., Rezaie, M., Rossi, G., Sanchez, E., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Silber, J., Siudek, M., Sprayberry, D., Tarlé, G., Zhou, Z., and Zou, H.
Abstract: The Dark Energy Spectroscopic Instrument (DESI) cosmology survey includes a Bright Galaxy Survey (BGS) which will yield spectra for over ten million bright galaxies (r<20.2 AB mag). The resulting sample will be valuable for both cosmological and astrophysical studies. However, the star/galaxy separation criterion implemented in the nominal BGS target selection algorithm excludes quasar host galaxies in addition to bona fide stars. While this excluded population is comparatively rare (~3-4 per square degrees), it may hold interesting clues regarding galaxy and quasar physics. Therefore, we present a target selection strategy that was implemented to recover these missing active galactic nuclei (AGN) from the BGS sample. The design of the selection criteria was both motivated and confirmed using spectroscopy. The resulting BGS-AGN sample is uniformly distributed over the entire DESI footprint. According to DESI survey validation data, the sample comprises 93% quasi-stellar objects (QSOs), 3% narrow-line AGN or blazars with a galaxy contamination rate of 2% and a stellar contamination rate of 2%. Peaking around redshift z=0.5, the BGS-AGN sample is intermediary between quasars from the rest of the BGS and those from the DESI QSO sample in terms of redshifts and AGN luminosities. The stacked spectrum is nearly identical to that of the DESI QSO targets, confirming that the sample is dominated by quasars. We highlight interesting small populations reaching z>2 which are either faint quasars with nearby projected companions or very bright quasars with strong absorption features including the Lyman-apha forest, metal absorbers and/or broad absorption lines., Comment: 41 pages, 31 figures, submitted to the AAS journals. Comments are welcome
Published: 2024

21. High redshift LBGs from deep broadband imaging for future spectroscopic surveys

Author: Ruhlmann-Kleider, Vanina, Yèche, Christophe, Magneville, Christophe, Coquinot, Henri, Armengaud, Eric, Palanque-Delabrouille, Nathalie, Raichoor, Anand, Aguilar, Jessica Nicole, Ahlen, Steven, Arnouts, Stéphane, Brooks, David, Chaussidon, Edmond, Claybaugh, Todd, Dawson, Kyle, de la Macorra, Axel, Dey, Arjun, Dey, Biprateep, Doel, Peter, Fanning, Kevin, Ferraro, Simone, Forero-Romero, Jaime E., Gontcho, Satya Gontcho A, Gutierrez, Gaston, Gwyn, Stephen, Honscheid, Klaus, Juneau, Stephanie, Kehoe, Robert, Kisner, Theodore, Kremin, Anthony, Lambert, Andrew, Landriau, Martin, Guillou, Laurent Le, Levi, Michael E., Manera, Marc, Martini, Paul, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Mueller, Eva-Maria, Muñoz-Gutiérrez, Andrea, Newman, Jeffrey A., Nie, Jundan, Niz, Gustavo, Payerne, Constantin, Picouet, Vincent, Ravoux, Corentin, Rezaie, Mehdi, Rossi, Graziano, Sanchez, Eusebio, Sawicki, Marcin, Schlafly, Edward F., Schlegel, David, Schubnell, Michael, Seo, Hee-Jong, Silber, Joseph, Sprayberry, David, Taran, Julien, Tarlé, Gregory, Weaver, Benjamin A., White, Martin, Wilson, Michael J., Zhou, Zhimin, Zou, Hu, Ruhlmann-Kleider, Vanina, Yèche, Christophe, Magneville, Christophe, Coquinot, Henri, Armengaud, Eric, Palanque-Delabrouille, Nathalie, Raichoor, Anand, Aguilar, Jessica Nicole, Ahlen, Steven, Arnouts, Stéphane, Brooks, David, Chaussidon, Edmond, Claybaugh, Todd, Dawson, Kyle, de la Macorra, Axel, Dey, Arjun, Dey, Biprateep, Doel, Peter, Fanning, Kevin, Ferraro, Simone, Forero-Romero, Jaime E., Gontcho, Satya Gontcho A, Gutierrez, Gaston, Gwyn, Stephen, Honscheid, Klaus, Juneau, Stephanie, Kehoe, Robert, Kisner, Theodore, Kremin, Anthony, Lambert, Andrew, Landriau, Martin, Guillou, Laurent Le, Levi, Michael E., Manera, Marc, Martini, Paul, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Mueller, Eva-Maria, Muñoz-Gutiérrez, Andrea, Newman, Jeffrey A., Nie, Jundan, Niz, Gustavo, Payerne, Constantin, Picouet, Vincent, Ravoux, Corentin, Rezaie, Mehdi, Rossi, Graziano, Sanchez, Eusebio, Sawicki, Marcin, Schlafly, Edward F., Schlegel, David, Schubnell, Michael, Seo, Hee-Jong, Silber, Joseph, Sprayberry, David, Taran, Julien, Tarlé, Gregory, Weaver, Benjamin A., White, Martin, Wilson, Michael J., Zhou, Zhimin, and Zou, Hu
Abstract: Lyman break galaxies (LBGs) are promising probes for clustering measurements at high redshift, $z>2$, a region only covered so far by Lyman-$\alpha$ forest measurements. In this paper, we investigate the feasibility of selecting LBGs by exploiting the existence of a strong deficit of flux shortward of the Lyman limit, due to various absorption processes along the line of sight. The target selection relies on deep imaging data from the HSC and CLAUDS surveys in the $g,r,z$ and $u$ bands, respectively, with median depths reaching 27 AB in all bands. The selections were validated by several dedicated spectroscopic observation campaigns with DESI. Visual inspection of spectra has enabled us to develop an automated spectroscopic typing and redshift estimation algorithm specific to LBGs. Based on these data and tools, we assess the efficiency and purity of target selections optimised for different purposes. Selections providing a wide redshift coverage retain $57\%$ of the observed targets after spectroscopic confirmation with DESI, and provide an efficiency for LBGs of $83\pm3\%$, for a purity of the selected LBG sample of $90\pm2\%$. This would deliver a confirmed LBG density of $\sim 620$ deg$^{-2}$ in the range $2.3
Published: 2024

22. 89 New Ultracool Dwarf Co-Moving Companions Identified With The Backyard Worlds: Planet 9 Citizen Science Project

Author: Rothermich, Austin, Faherty, Jacqueline K., Bardalez-Gagliuffi, Daniella, Schneider, Adam C., Kirkpatrick, J. Davy, Meisner, Aaron M., Burgasser, Adam J., Kuchner, Marc, Allers, Katelyn, Gagné, Jonathan, Caselden, Dan, Calamari, Emily, Popinchalk, Mark, Suárez, Genaro, Gerasimov, Roman, Aganze, Christian, Softich, Emma, Hsu, Chin-Chun, Karpoor, Preethi, Theissen, Christopher A., Rees, Jon, Cecilio-Flores-Elie, Rosario, Cushing, Michael C., Marocco, Federico, Casewell, Sarah, Bickle, Thomas P., Hamlet, Les, Allen, Michaela B., Beaulieu, Paul, Colin, Guillaume, Gantier, Jean Marc, Gramaize, Leopold, Jalowiczor, Peter, Kabatnik, Martin, Kiwy, Frank, Martin, David W., Pendrill, Billy, Pumphrey, Ben, Sainio, Arttu, Schumann, Jorg, Stevnbak, Nikolaj, Sun, Guoyou, Tanner, Christopher, Thakur, Vinod, Thevenot, Melina, Wedracki, Zbigniew, Rothermich, Austin, Faherty, Jacqueline K., Bardalez-Gagliuffi, Daniella, Schneider, Adam C., Kirkpatrick, J. Davy, Meisner, Aaron M., Burgasser, Adam J., Kuchner, Marc, Allers, Katelyn, Gagné, Jonathan, Caselden, Dan, Calamari, Emily, Popinchalk, Mark, Suárez, Genaro, Gerasimov, Roman, Aganze, Christian, Softich, Emma, Hsu, Chin-Chun, Karpoor, Preethi, Theissen, Christopher A., Rees, Jon, Cecilio-Flores-Elie, Rosario, Cushing, Michael C., Marocco, Federico, Casewell, Sarah, Bickle, Thomas P., Hamlet, Les, Allen, Michaela B., Beaulieu, Paul, Colin, Guillaume, Gantier, Jean Marc, Gramaize, Leopold, Jalowiczor, Peter, Kabatnik, Martin, Kiwy, Frank, Martin, David W., Pendrill, Billy, Pumphrey, Ben, Sainio, Arttu, Schumann, Jorg, Stevnbak, Nikolaj, Sun, Guoyou, Tanner, Christopher, Thakur, Vinod, Thevenot, Melina, and Wedracki, Zbigniew
Abstract: We report the identification of 89 new systems containing ultracool dwarf companions to main sequence stars and white dwarfs, using the citizen science project Backyard Worlds: Planet 9 and cross-reference between Gaia and CatWISE2020. Thirty-two of these companions and thirty-three host stars were followed up with spectroscopic observations, with companion spectral types ranging from M7-T9 and host spectral types ranging from G2-M9. These systems exhibit diverse characteristics, from young to old ages, blue to very red spectral morphologies, potential membership to known young moving groups, and evidence of spectral binarity in 9 companions. Twenty of the host stars in our sample show evidence for higher order multiplicity, with an additional 11 host stars being resolved binaries themselves. We compare this sample's characteristics with those of the known stellar binary and exoplanet populations, and find our sample begins to fill in the gap between directly imaged exoplanets and stellary binaries on mass ratio-binding energy plots. With this study, we increase the population of ultracool dwarf companions to FGK stars by $\sim$42\%, and more than triple the known population of ultracool dwarf companions with separations larger than 1,000 au, providing excellent targets for future atmospheric retrievals., Comment: 61 pages, 11 figures, 11 tables. Accepted for publication in AJ
Published: 2024

23. The DESI Early Data Release White Dwarf Catalogue

Author: Manser, Christopher J., Izquierdo, Paula, Gänsicke, Boris T., Swan, Andrew, Koester, Detlev, Robert, Akshay, Xu, Siyi, Inight, Keith, Amroota, Ben, Fusillo, N. P. Gentile, Koposov, Sergey E., Kim, Bokyoung, Dey, Arjun, Prieto, Carlos Allende, Aguilar, J., Ahlen, S., Blum, R., Brooks, D., Claybaugh, T., Cooper, A. P., Dawson, K., de la Macorra, A., Doel, P., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Honscheid, K., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Guillou, L. Le, Levi, Michael E., Li, T. S., Meisner, A., Miquel, R., Moustakas, J., Nie, J., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Rezaie, M., Rossi, G., Sanchez, E., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Silber, J., Tarlé, G., Weaver, B. A., Zhou, Z., Zou, H., Manser, Christopher J., Izquierdo, Paula, Gänsicke, Boris T., Swan, Andrew, Koester, Detlev, Robert, Akshay, Xu, Siyi, Inight, Keith, Amroota, Ben, Fusillo, N. P. Gentile, Koposov, Sergey E., Kim, Bokyoung, Dey, Arjun, Prieto, Carlos Allende, Aguilar, J., Ahlen, S., Blum, R., Brooks, D., Claybaugh, T., Cooper, A. P., Dawson, K., de la Macorra, A., Doel, P., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Honscheid, K., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Guillou, L. Le, Levi, Michael E., Li, T. S., Meisner, A., Miquel, R., Moustakas, J., Nie, J., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Rezaie, M., Rossi, G., Sanchez, E., Schlafly, E. F., Schlegel, D., Schubnell, M., Seo, H., Silber, J., Tarlé, G., Weaver, B. A., Zhou, Z., and Zou, H.
Abstract: The Early Data Release (EDR) of the Dark Energy Spectroscopic Instrument (DESI) comprises spectroscopy obtained from 2020 December 14 to 2021 June 10. White dwarfs were targeted by DESI both as calibration sources and as science targets and were selected based on Gaia photometry and astrometry. Here we present the DESI EDR white dwarf catalogue, which includes 2706 spectroscopically confirmed white dwarfs of which approximately 1630 (roughly 60 per cent) have been spectroscopically observed for the first time, as well as 66 white dwarf binary systems. We provide spectral classifications for all white dwarfs, and discuss their distribution within the Gaia Hertzsprung-Russell diagram. We provide atmospheric parameters derived from spectroscopic and photometric fits for white dwarfs with pure hydrogen or helium photospheres, a mixture of those two, and white dwarfs displaying carbon features in their spectra. We also discuss the less abundant systems in the sample, such as those with magnetic fields, and cataclysmic variables. The DESI EDR white dwarf sample is significantly less biased than the sample observed by the Sloan Digital Sky Survey, which is skewed to bluer and therefore hotter white dwarfs, making DESI more complete and suitable for performing statistical studies of white dwarfs., Comment: 19 pages, 17 figures, not including appendix. Submitting to MNRAS. Comments and suggestions welcome
Published: 2024

24. Redshift evolution and covariances for joint lensing and clustering studies with DESI Y1

Author: Yuan, Sihan, Blake, Chris, Krolewski, Alex, Lange, Johannes, Elvin-Poole, Jack, Leauthaud, Alexie, DeRose, Joseph, Aguilar, Jessica Nicole, Ahlen, Steven, Beltz-Mohrmann, Gillian, Brooks, David, Claybaugh, Todd, de la Macorra, Axel, Doel, Peter, Emas, Ni Putu Audita Placida, Ferraro, Simone, Forero-Romero, Jaime E., Garcia-Quintero, Cristhian, Gaztañaga, Enrique, Gontcho, Satya Gontcho A, Hadzhiyska, Boryana, Heydenreich, Sven, Honscheid, Klaus, Ishak, Mustapha, Joudaki, Shahab, Jullo, Eric, Kisner, Theodore, Kremin, Anthony, Lambert, Andrew, Landriau, Martin, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Nie, Jundan, Palanque-Delabrouille, Nathalie, Poppett, Claire, Porredon, Anna, Rezaie, Mehdi, Ross, Ashley J., Rossi, Graziano, Ruggeri, Rossana, Sanchez, Eusebio, Saulder, Christoph, Seo, Hee-Jong, Silber, Joseph Harry, Tarlé, Gregory, Vargas-Magaña, Mariana, Weaver, Benjamin Alan, Xhakaj, Enia, Zhou, Zhimin, Zou, Hu, Yuan, Sihan, Blake, Chris, Krolewski, Alex, Lange, Johannes, Elvin-Poole, Jack, Leauthaud, Alexie, DeRose, Joseph, Aguilar, Jessica Nicole, Ahlen, Steven, Beltz-Mohrmann, Gillian, Brooks, David, Claybaugh, Todd, de la Macorra, Axel, Doel, Peter, Emas, Ni Putu Audita Placida, Ferraro, Simone, Forero-Romero, Jaime E., Garcia-Quintero, Cristhian, Gaztañaga, Enrique, Gontcho, Satya Gontcho A, Hadzhiyska, Boryana, Heydenreich, Sven, Honscheid, Klaus, Ishak, Mustapha, Joudaki, Shahab, Jullo, Eric, Kisner, Theodore, Kremin, Anthony, Lambert, Andrew, Landriau, Martin, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Nie, Jundan, Palanque-Delabrouille, Nathalie, Poppett, Claire, Porredon, Anna, Rezaie, Mehdi, Ross, Ashley J., Rossi, Graziano, Ruggeri, Rossana, Sanchez, Eusebio, Saulder, Christoph, Seo, Hee-Jong, Silber, Joseph Harry, Tarlé, Gregory, Vargas-Magaña, Mariana, Weaver, Benjamin Alan, Xhakaj, Enia, Zhou, Zhimin, and Zou, Hu
Abstract: Galaxy-galaxy lensing (GGL) and clustering measurements from the Dark Energy Spectroscopic Instrument Year 1 (DESI Y1) dataset promise to yield unprecedented combined-probe tests of cosmology and the galaxy-halo connection. In such analyses, it is essential to identify and characterise all relevant statistical and systematic errors. In this paper, we forecast the covariances of DESI Y1 GGL+clustering measurements and characterise the systematic bias due to redshift evolution in the lens samples. Focusing on the projected clustering and galaxy-galaxy lensing correlations, we compute a Gaussian analytical covariance, using a suite of N-body and log-normal simulations to characterise the effect of the survey footprint. Using the DESI One Percent Survey data, we measure the evolution of galaxy bias parameters for the DESI Luminous Red Galaxy (LRG) and Bright Galaxy Survey (BGS) samples. We find mild evolution in the LRGs in 0.4 < z < 0.8, subdominant compared to the expected statistical errors. For BGS, we find less evolution effects for brighter absolute magnitude cuts, at the cost of reduced sample size. We find that with a fiducial redshift bin width delta z = 0.1, evolution effects on GGL is negligible across all scales, all fiducial selection cuts, all fiducial redshift bins, given DESI Y1 sample size. Galaxy clustering is more sensitive to evolution due to the bias squared scaling. Nevertheless the redshift evolution effect is insignificant for clustering above the 1-halo scale of 0.1Mpc/h. For studies that wish to reliably access smaller scales, additional treatment of redshift evolution is likely needed. This study serves as a reference for GGL and clustering studies using the DESI Y1 sample, Comment: 19 pages, 15 figures, submitted to MNRAS
Published: 2024

25. The frequency of metal-enrichment of cool helium-atmosphere white dwarfs using the DESI Early Data Release

Author: Manser, Christopher J., Gänsicke, Boris T., Izquierdo, Paula, Swan, Andrew, Najita, Joan, Rockosi, C., Carrillo, Andreia, Kim, Bokyoung, Xu, Siyi, Dey, Arjun, Aguilar, J., Ahlen, S., Blum, R., Brooks, D., Claybaugh, T., Dawson, K., de la Macorra, A., Doel, P., Gaztañaga, E., Gontcho, S. Gontcho A, Honscheid, K., Kehoe, R., Kremin, A., Landriau, M., Guillou, L. Le, Levi, Michael E., Li, T. S., Meisner, A., Miquel, R., Nie, J., Rezaie, M., Rossi, G., Sanchez, E., Schubnell, M., Tarlé, G., Weaver, B. A., Zhou, Z., Zou, H., Manser, Christopher J., Gänsicke, Boris T., Izquierdo, Paula, Swan, Andrew, Najita, Joan, Rockosi, C., Carrillo, Andreia, Kim, Bokyoung, Xu, Siyi, Dey, Arjun, Aguilar, J., Ahlen, S., Blum, R., Brooks, D., Claybaugh, T., Dawson, K., de la Macorra, A., Doel, P., Gaztañaga, E., Gontcho, S. Gontcho A, Honscheid, K., Kehoe, R., Kremin, A., Landriau, M., Guillou, L. Le, Levi, Michael E., Li, T. S., Meisner, A., Miquel, R., Nie, J., Rezaie, M., Rossi, G., Sanchez, E., Schubnell, M., Tarlé, G., Weaver, B. A., Zhou, Z., and Zou, H.
Abstract: There is overwhelming evidence that white dwarfs host planetary systems; revealed by the presence, disruption, and accretion of planetary bodies. A lower limit on the frequency of white dwarfs that host planetary material has been estimated to be roughly 25-50 per cent; inferred from the ongoing or recent accretion of metals onto both hydrogen-atmosphere and warm helium-atmosphere white dwarfs. Now with the unbiased sample of white dwarfs observed by the Dark Energy Spectroscopic Instrument (DESI) survey in their Early Data Release (EDR), we have determined the frequency of metal-enrichment around cool-helium atmosphere white dwarfs as 21 $\pm$ 3 per cent using a sample of 234 systems. This value is in good agreement with values determined from previous studies. With the current samples we cannot distinguish whether the frequency of planetary accretion varies with system age or host-star mass, but the DESI data release 1 will contain roughly an order of magnitude more white dwarfs than DESI EDR and will allow these parameters to be investigated., Comment: 6 pages, 1 figure. Submitted to MNRAS. Comments and suggestions welcome
Published: 2024

26. Baryon Acoustic Oscillation Theory and Modelling Systematics for the DESI 2024 results

Author: Chen, Shi-Fan, Howlett, Cullan, White, Martin, McDonald, Patrick, Ross, Ashley J., Seo, Hee-Jong, Padmanabhan, Nikhil, Aguilar, J., Ahlen, S., Alam, S., Alves, O., Blum, R., Brooks, D., Chen, X., Cole, S., Davis, T. M., Dawson, K., de la Macorra, A., Dey, Arjun, Ding, Z., Doel, P., Ferraro, S., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Garcia-Quintero, C., Gaztañaga, E., Gontcho, S. Gontcho A, Hanif, M. M. S, Honscheid, K., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Levi, M. E., Manera, M., Meisner, A., Mena-Fernández, J., Miquel, R., Muñoz-Gutiérrez, A., Paillas, E., Palanque-Delabrouille, N., Percival, W. J., Prada, F., Pérez-Fernández, A., Rashkovetskyi, M., Rezaie, M., Rossi, G., Ruggeri, R., Sanchez, E., Schlegel, D., Silber, J., Tarlé, G., Vargas-Magaña, M., Weaver, B. A., Yuan, S., Zhou, R., Zhou, Z., Chen, Shi-Fan, Howlett, Cullan, White, Martin, McDonald, Patrick, Ross, Ashley J., Seo, Hee-Jong, Padmanabhan, Nikhil, Aguilar, J., Ahlen, S., Alam, S., Alves, O., Blum, R., Brooks, D., Chen, X., Cole, S., Davis, T. M., Dawson, K., de la Macorra, A., Dey, Arjun, Ding, Z., Doel, P., Ferraro, S., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Garcia-Quintero, C., Gaztañaga, E., Gontcho, S. Gontcho A, Hanif, M. M. S, Honscheid, K., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Levi, M. E., Manera, M., Meisner, A., Mena-Fernández, J., Miquel, R., Muñoz-Gutiérrez, A., Paillas, E., Palanque-Delabrouille, N., Percival, W. J., Prada, F., Pérez-Fernández, A., Rashkovetskyi, M., Rezaie, M., Rossi, G., Ruggeri, R., Sanchez, E., Schlegel, D., Silber, J., Tarlé, G., Vargas-Magaña, M., Weaver, B. A., Yuan, S., Zhou, R., and Zhou, Z.
Abstract: This paper provides a comprehensive overview of how fitting of Baryon Acoustic Oscillations (BAO) is carried out within the upcoming Dark Energy Spectroscopic Instrument's (DESI) 2024 results using its DR1 dataset, and the associated systematic error budget from theory and modelling of the BAO. We derive new results showing how non-linearities in the clustering of galaxies can cause potential biases in measurements of the isotropic ($\alpha_{\mathrm{iso}}$) and anisotropic ($\alpha_{\mathrm{ap}}$) BAO distance scales, and how these can be effectively removed with an appropriate choice of reconstruction algorithm. We then demonstrate how theory leads to a clear choice for how to model the BAO and develop, implement and validate a new model for the remaining smooth-broadband (i.e., without BAO) component of the galaxy clustering. Finally, we explore the impact of all remaining modelling choices on the BAO constraints from DESI using a suite of high-precision simulations, arriving at a set of best-practices for DESI BAO fits, and an associated theory and modelling systematic error. Overall, our results demonstrate the remarkable robustness of the BAO to all our modelling choices and motivate a combined theory and modelling systematic error contribution to the post-reconstruction DESI BAO measurements of no more than $0.1\%$ ($0.2\%$) for its isotropic (anisotropic) distance measurements. We expect the theory and best-practices laid out to here to be applicable to other BAO experiments in the era of DESI and beyond., Comment: 29 pages, 18 figures, 1 table, submitted to MNRAS
Published: 2024

27. Measuring Fiber Positioning Accuracy and Throughput with Fiber Dithering for the Dark Energy Spectroscopic Instrument

Author: Schlafly, E. F., Schlegel, D., BenZvi, S., Raichoor, A., Forero-Romero, J. E., Aguilar, J., Ahlen, S., Bailey, S., Bault, A., Brooks, D., Claybaugh, T., Dawson, K., de la Macorra, A., Dey, Arjun, Doel, P., Gaztañaga, E., Gontcho, S. Gontcho A, Guy, J., Hahn, C., Honscheid, K., Jimenez, J., Kent, S., Kirkby, D., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Levi, M. E., Manera, M., Martini, P., Meisner, A., Miquel, R., Moustakas, J., Myers, A. D., Nie, J., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Rabinowitz, D., Rezaie, M., Rossi, G., Sanchez, E., Schubnell, M., Sharples, R., Silber, J., Tarlé, G., Weaver, B. A., Zhou, Z., Zou, H., Schlafly, E. F., Schlegel, D., BenZvi, S., Raichoor, A., Forero-Romero, J. E., Aguilar, J., Ahlen, S., Bailey, S., Bault, A., Brooks, D., Claybaugh, T., Dawson, K., de la Macorra, A., Dey, Arjun, Doel, P., Gaztañaga, E., Gontcho, S. Gontcho A, Guy, J., Hahn, C., Honscheid, K., Jimenez, J., Kent, S., Kirkby, D., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Levi, M. E., Manera, M., Martini, P., Meisner, A., Miquel, R., Moustakas, J., Myers, A. D., Nie, J., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Rabinowitz, D., Rezaie, M., Rossi, G., Sanchez, E., Schubnell, M., Sharples, R., Silber, J., Tarlé, G., Weaver, B. A., Zhou, Z., and Zou, H.
Abstract: Highly multiplexed, fiber-fed spectroscopy is enabling surveys of millions of stars and galaxies. The performance of these surveys depends on accurately positioning fibers in the focal plane to capture target light. We describe a technique to measure the positioning accuracy of fibers by dithering fibers slightly around their ideal locations. This approach also enables measurement of the total system throughput and point spread function delivered to the focal plane. We then apply this technique to observations from the Dark Energy Survey Instrument (DESI), and demonstrate that DESI positions fibers to within 0.08" of their targets (5% of a fiber diameter) and achieves a system throughput within about 5% of expectations., Comment: 17 pages, 9 figures
Published: 2024

28. Impact of Systematic Redshift Errors on the Cross-correlation of the Lyman-$\alpha$ Forest with Quasars at Small Scales Using DESI Early Data

Author: Bault, Abby, Kirkby, David, Guy, Julien, Brodzeller, Allyson, Aguilar, J., Ahlen, S., Bailey, S., Brooks, D., Cabayol-Garcia, L., Chaves-Montero, J., Claybaugh, T., Cuceu, A., Dawson, K., de la Cruz, R., de la Macorra, A., Dey, A., Doel, P., Filbert, S., Font-Ribera, A., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gordon, C., Herrera-Alcantar, H. K., Honscheid, K., Iršič, V., Karaçaylı, N. G., Kehoe, R., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Martini, P., Meisner, A., Miquel, R., Montero-Camacho, P., Moustakas, J., Muñoz-Gutiérrez, A., Nie, J., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Pérez-Ràfols, I., Ramírez-Pérez, C., Ravoux, C., Rezaie, M., Rossi, G., Sanchez, E., Schlafly, E. F., Schlegel, D., Schubnell, M., Silber, J., Tan, T., Tarlé, G., Walther, M., Weaver, B. A., Zhou, Z., Bault, Abby, Kirkby, David, Guy, Julien, Brodzeller, Allyson, Aguilar, J., Ahlen, S., Bailey, S., Brooks, D., Cabayol-Garcia, L., Chaves-Montero, J., Claybaugh, T., Cuceu, A., Dawson, K., de la Cruz, R., de la Macorra, A., Dey, A., Doel, P., Filbert, S., Font-Ribera, A., Forero-Romero, J. E., Gaztañaga, E., Gontcho, S. Gontcho A, Gordon, C., Herrera-Alcantar, H. K., Honscheid, K., Iršič, V., Karaçaylı, N. G., Kehoe, R., Kisner, T., Kremin, A., Lambert, A., Landriau, M., Guillou, L. Le, Levi, M. E., Manera, M., Martini, P., Meisner, A., Miquel, R., Montero-Camacho, P., Moustakas, J., Muñoz-Gutiérrez, A., Nie, J., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Prada, F., Pérez-Ràfols, I., Ramírez-Pérez, C., Ravoux, C., Rezaie, M., Rossi, G., Sanchez, E., Schlafly, E. F., Schlegel, D., Schubnell, M., Silber, J., Tan, T., Tarlé, G., Walther, M., Weaver, B. A., and Zhou, Z.
Abstract: The Dark Energy Spectroscopic Instrument (DESI) will measure millions of quasar spectra by the end of its 5 year survey. Quasar redshift errors impact the shape of the Lyman-$\alpha$ forest correlation functions, which can affect cosmological analyses and therefore cosmological interpretations. Using data from the DESI Early Data Release and the first two months of the main survey, we measure the systematic redshift error from an offset in the cross-correlation of the Lyman-$\alpha$ forest with quasars. We find evidence for a redshift dependent bias causing redshifts to be underestimated with increasing redshift, stemming from improper modeling of the Lyman-$\alpha$ optical depth in the templates used for redshift estimation. New templates were derived for the DESI Year 1 quasar sample at $z > 1.6$ and we found the redshift dependent bias, $\Delta r_\parallel$, increased from $-1.94 \pm 0.15$ $h^{-1}$ Mpc to $-0.08 \pm 0.04$ $h^{-1}$ Mpc ($-205 \pm 15~\text{km s}^{-1}$ to $-9.0 \pm 4.0~\text{km s}^{-1}$). These new templates will be used to provide redshifts for the DESI Year 1 quasar sample., Comment: 29 pages, 9 figures, 5 tables
Published: 2024

29. The rate of extreme coronal line emitting galaxies in the Sloan Digital Sky Survey and their relation to tidal disruption events

Author: Callow, Joseph, Graur, Or, Clark, Peter, Palmese, Antonella, Aguilar, Jessica, Ahlen, Steven, BenZvi, Segev, Brooks, David, Claybaugh, Todd, de la Macorra, Axel, Doel, Peter, Forero-Romero, Jaime E., Gaztañaga, Enrique, Gontcho, Satya Gontcho A, Lambert, Andrew, Landriau, Martin, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Nie, Jundan, Poppett, Claire, Prada, Francisco, Rezaie, Mehdi, Rossi, Graziano, Sanchez, Eusebio, Silber, Joseph H., Tarlé, Gregory, Weaver, Benjamin A., Zhou, Zhimin, Callow, Joseph, Graur, Or, Clark, Peter, Palmese, Antonella, Aguilar, Jessica, Ahlen, Steven, BenZvi, Segev, Brooks, David, Claybaugh, Todd, de la Macorra, Axel, Doel, Peter, Forero-Romero, Jaime E., Gaztañaga, Enrique, Gontcho, Satya Gontcho A, Lambert, Andrew, Landriau, Martin, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Nie, Jundan, Poppett, Claire, Prada, Francisco, Rezaie, Mehdi, Rossi, Graziano, Sanchez, Eusebio, Silber, Joseph H., Tarlé, Gregory, Weaver, Benjamin A., and Zhou, Zhimin
Abstract: Strong high-ionization iron coronal lines (CLs) are a rare phenomenon observed in galaxy and quasi-stellar object spectra that are thought to be created as a result of tidal disruption event (TDE) flares. To test whether these CLs are the result of TDE activity, we search for extreme coronal line emitting galaxies (ECLEs) in the Sloan Digital Sky Survey (SDSS), measure their rate, and compare it to TDE rates from the literature. We detect sufficiently strong CLs in 14 objects, doubling the number previously found in SDSS. Using follow-up spectra from the Dark Energy Spectroscopic Instrument and Gemini Multi-Object Spectrograph, Wide-field Infrared Survey Explorer mid-infrared observations, and Liverpool Telescope optical photometry, we find that of the seven new objects, only one evolves in a manner consistent with that of the five previously discovered variable ECLEs. Using this new sample of six variable ECLEs, we calculate the galaxy-normalised rate of ECLEs in SDSS to be $R_\mathrm{G}=2.2~^{+1.3}_{-0.8}~(\mathrm{statistical})~^{+0.0}_{-1.3}~(\mathrm{systematic})\times10^{-5}~\mathrm{galaxy}^{-1}~\mathrm{year}^{-1}$. The mass-normalised rate is $R_\mathrm{M}=1.9~^{+1.1}_{-0.7}~(\mathrm{statistical})~^{+0.0}_{-1.1}~(\mathrm{systematic})\times10^{-16}~\mathrm{M_\odot^{-1}}~\mathrm{year}^{-1}$ and the volumetric rate is $R_\mathrm{V}=6.9~^{+5.6}_{-2.1}~(\mathrm{statistical})~^{+0.0}_{-3.9}~(\mathrm{systematic})\times10^{-8}~\mathrm{Mpc}^{-3}~\mathrm{year}^{-1}$. Our rates are comparable to TDE rates from the literature, supporting the suggestion that the CLs in variable ECLEs are the product of TDEs., Comment: Submitted to MNRAS. 19 pages, 12 figures
Published: 2024

30. High-Precision Atmospheric Constraints for a Cool T Dwarf from JWST Spectroscopy

Author: Hood, Callie E., Mukherjee, Sagnick, Fortney, Jonathan J., Line, Michael R., Faherty, Jacqueline K., Merchan, Sherelyn Alejandro, Burningham, Ben, Suárez, Genaro, Kiman, Rocio, Gagné, Jonathan, Beichman, Charles A., Vos, Johanna M., Gagliuffi, Daniella Bardalez, Meisner, Aaron M., Gonzales, Eileen C., Hood, Callie E., Mukherjee, Sagnick, Fortney, Jonathan J., Line, Michael R., Faherty, Jacqueline K., Merchan, Sherelyn Alejandro, Burningham, Ben, Suárez, Genaro, Kiman, Rocio, Gagné, Jonathan, Beichman, Charles A., Vos, Johanna M., Gagliuffi, Daniella Bardalez, Meisner, Aaron M., and Gonzales, Eileen C.
Abstract: We present observations of the T8 dwarf 2MASS 0415-0935 with JWST's NIRSpec spectrograph using the G395H grating ($\sim$ 2.87 - 5.14 $\mu$m). We perform the first atmospheric retrieval analysis at the maximum spectral resolution of NIRSpec (R$\sim$2700) and combine the spectrum with previous observations to study the 0.9-20 $\mu$m spectral energy distribution. We obtain precise constraints on chemical abundances ($\sim$0.02 dex) for a number of species which complicate our understanding of disequilibrium chemistry, particularly for CO$_{2}$ and PH$_{3}$. Furthermore, we measure a $^{12}$CO/$^{13}$CO ratio of $\sim 97^{+9}_{-8}$, making 2MASS 0415-0935 the coldest ($\sim 760$ K) substellar object outside of our solar system with a measured $^{12}$CO/$^{13}$CO ratio. This work shows promise for similar observations with JWST to provide precise abundances of major chemical species as well as isotopologues, allowing for new tests of our understanding of the formation and atmospheres of substellar objects., Comment: 28 pages, 10 figures. Submitted to Nature Astronomy on Oct. 5th, 2023
Published: 2024

31. Leveraging mechanochemistry for sustainable polymer degradation

Author: Sub Inorganic Chemistry and Catalysis, Inorganic Chemistry and Catalysis, Aydonat, Simay, Hergesell, Adrian H., Seitzinger, Claire L., Lennarz, Regina, Chang, George, Sievers, Carsten, Meisner, Jan, Vollmer, Ina, Göstl, Robert, Sub Inorganic Chemistry and Catalysis, Inorganic Chemistry and Catalysis, Aydonat, Simay, Hergesell, Adrian H., Seitzinger, Claire L., Lennarz, Regina, Chang, George, Sievers, Carsten, Meisner, Jan, Vollmer, Ina, and Göstl, Robert
Published: 2024

32. A New Population of Mid-Infrared-Selected Tidal Disruption Events: Implications for Tidal Disruption Event Rates and Host Galaxy Properties

Author: Masterson, Megan, De, Kishalay, Panagiotou, Christos, Kara, Erin, Arcavi, Iair, Eilers, Anna-Christina, Frostig, Danielle, Gezari, Suvi, Grotova, Iuliia, Liu, Zhu, Malyali, Adam, Meisner, Aaron M., Merloni, Andrea, Newsome, Megan, Rau, Arne, Simcoe, Robert A., van Velzen, Sjoert, Masterson, Megan, De, Kishalay, Panagiotou, Christos, Kara, Erin, Arcavi, Iair, Eilers, Anna-Christina, Frostig, Danielle, Gezari, Suvi, Grotova, Iuliia, Liu, Zhu, Malyali, Adam, Meisner, Aaron M., Merloni, Andrea, Newsome, Megan, Rau, Arne, Simcoe, Robert A., and van Velzen, Sjoert
Abstract: Most tidal disruption events (TDEs) are currently found in time-domain optical and soft X-ray surveys, both of which are prone to significant obscuration. The infrared (IR), however, is a powerful probe of dust-enshrouded environments, and hence, we recently performed a systematic search of NEOWISE mid-IR data for nearby, obscured TDEs within roughly 200 Mpc. We identified 18 TDE candidates in galactic nuclei, using difference imaging to uncover nuclear variability amongst significant host galaxy emission. These candidates were selected based on the following IR light curve properties: (1) $L_\mathrm{W2}\gtrsim10^{42}$ erg s$^{-1}$ at peak, (2) fast rise, followed by a slow, monotonic decline, (3) no significant prior variability, and (4) no evidence for AGN activity in WISE colors. The majority of these sources showed no variable optical counterpart, suggesting that optical surveys indeed miss numerous obscured TDEs. Using narrow line ionization levels and variability arguments, we identified 6 sources as possible underlying AGN, yielding a total of 12 TDEs in our gold sample. This gold sample yields a lower limit on the IR-selected TDE rate of $2.0\pm0.3\times10^{-5}$ galaxy$^{-1}$ year$^{-1}$ ($1.3\pm0.2\times10^{-7}$ Mpc$^{-3}$ year$^{-1}$), which is comparable to optical and X-ray TDE rates. The IR-selected TDE host galaxies do not show a green valley overdensity nor a preference for quiescent, Balmer strong galaxies, which are both overrepresented in optical and X-ray TDE samples. This IR-selected sample represents a new population of dusty TDEs that have historically been missed by optical and X-ray surveys and helps alleviate tensions between observed and theoretical TDE rates and the so-called missing energy problem., Comment: 28 pages, 13 figures (+ 7 pages, 4 figures in appendix), accepted for publication in ApJ
Published: 2024

33. Giraffe lineages are shaped by major ancient admixture events

Author: Bertola, Laura D., Quinn, Liam, Hanghøj, Kristian, Garcia-Erill, Genís, Rasmussen, Malthe Sebro, Balboa, Renzo F., Meisner, Jonas, Bøggild, Thomas, Wang, Xi, Lin, Long, Nursyifa, Casia, Liu, Xiaodong, Li, Zilong, Chege, Mumbi, Moodley, Yoshan, Brüniche-Olsen, Anna, Kuja, Josiah, Schubert, Mikkel, Agaba, Morris, Santander, Cindy G., Sinding, Mikkel Holger S., Muwanika, Vincent, Masembe, Charles, Siegismund, Hans R., Moltke, Ida, Albrechtsen, Anders, Heller, Rasmus, Bertola, Laura D., Quinn, Liam, Hanghøj, Kristian, Garcia-Erill, Genís, Rasmussen, Malthe Sebro, Balboa, Renzo F., Meisner, Jonas, Bøggild, Thomas, Wang, Xi, Lin, Long, Nursyifa, Casia, Liu, Xiaodong, Li, Zilong, Chege, Mumbi, Moodley, Yoshan, Brüniche-Olsen, Anna, Kuja, Josiah, Schubert, Mikkel, Agaba, Morris, Santander, Cindy G., Sinding, Mikkel Holger S., Muwanika, Vincent, Masembe, Charles, Siegismund, Hans R., Moltke, Ida, Albrechtsen, Anders, and Heller, Rasmus
Abstract: Strong genetic structure has prompted discussion regarding giraffe taxonomy,1,2,3 including a suggestion to split the giraffe into four species: Northern (Giraffa c. camelopardalis), Reticulated (G. c. reticulata), Masai (G. c. tippelskirchi), and Southern giraffes (G. c. giraffa).4,5,6 However, their evolutionary history is not yet fully resolved, as previous studies used a simple bifurcating model and did not explore the presence or extent of gene flow between lineages. We therefore inferred a model that incorporates various evolutionary processes to assess the drivers of contemporary giraffe diversity. We analyzed whole-genome sequencing data from 90 wild giraffes from 29 localities across their current distribution. The most basal divergence was dated to 280 kya. Genetic differentiation, FST, among major lineages ranged between 0.28 and 0.62, and we found significant levels of ancient gene flow between them. In particular, several analyses suggested that the Reticulated lineage evolved through admixture, with almost equal contribution from the Northern lineage and an ancestral lineage related to Masai and Southern giraffes. These new results highlight a scenario of strong differentiation despite gene flow, providing further context for the interpretation of giraffe diversity and the process of speciation in general. They also illustrate that conservation measures need to target various lineages and sublineages and that separate management strategies are needed to conserve giraffe diversity effectively. Given local extinctions and recent dramatic declines in many giraffe populations, this improved understanding of giraffe evolutionary history is relevant for conservation interventions, including reintroductions and reinforcements of existing populations., Strong genetic structure has prompted discussion regarding giraffe taxonomy,1,2,3 including a suggestion to split the giraffe into four species: Northern (Giraffa c. camelopardalis), Reticulated (G. c. reticulata), Masai (G. c. tippelskirchi), and Southern giraffes (G. c. giraffa).4,5,6 However, their evolutionary history is not yet fully resolved, as previous studies used a simple bifurcating model and did not explore the presence or extent of gene flow between lineages. We therefore inferred a model that incorporates various evolutionary processes to assess the drivers of contemporary giraffe diversity. We analyzed whole-genome sequencing data from 90 wild giraffes from 29 localities across their current distribution. The most basal divergence was dated to 280 kya. Genetic differentiation, FST, among major lineages ranged between 0.28 and 0.62, and we found significant levels of ancient gene flow between them. In particular, several analyses suggested that the Reticulated lineage evolved through admixture, with almost equal contribution from the Northern lineage and an ancestral lineage related to Masai and Southern giraffes. These new results highlight a scenario of strong differentiation despite gene flow, providing further context for the interpretation of giraffe diversity and the process of speciation in general. They also illustrate that conservation measures need to target various lineages and sublineages and that separate management strategies are needed to conserve giraffe diversity effectively. Given local extinctions and recent dramatic declines in many giraffe populations, this improved understanding of giraffe evolutionary history is relevant for conservation interventions, including reintroductions and reinforcements of existing populations.
Published: 2024

34. Introgression and disruption of migration routes have shaped the genetic integrity of wildebeest populations

Author: Liu, Xiaodong, Lin, Long, Sinding, Mikkel Holger S., Bertola, Laura D., Hanghøj, Kristian, Quinn, Liam, Garcia-Erill, Genís, Rasmussen, Malthe Sebro, Schubert, Mikkel, Pečnerová, Patrícia, Balboa, Renzo F., Li, Zilong, Heaton, Michael P., Smith, Timothy P.L., Pinto, Rui Resende, Wang, Xi, Kuja, Josiah, Brüniche-Olsen, Anna, Meisner, Jonas, Santander, Cindy G., Ogutu, Joseph O., Masembe, Charles, da Fonseca, Rute R., Muwanika, Vincent, Siegismund, Hans R., Albrechtsen, Anders, Moltke, Ida, Heller, Rasmus, Liu, Xiaodong, Lin, Long, Sinding, Mikkel Holger S., Bertola, Laura D., Hanghøj, Kristian, Quinn, Liam, Garcia-Erill, Genís, Rasmussen, Malthe Sebro, Schubert, Mikkel, Pečnerová, Patrícia, Balboa, Renzo F., Li, Zilong, Heaton, Michael P., Smith, Timothy P.L., Pinto, Rui Resende, Wang, Xi, Kuja, Josiah, Brüniche-Olsen, Anna, Meisner, Jonas, Santander, Cindy G., Ogutu, Joseph O., Masembe, Charles, da Fonseca, Rute R., Muwanika, Vincent, Siegismund, Hans R., Albrechtsen, Anders, Moltke, Ida, and Heller, Rasmus
Abstract: The blue wildebeest (Connochaetes taurinus) is a keystone species in savanna ecosystems from southern to eastern Africa, and is well known for its spectacular migrations and locally extreme abundance. In contrast, the black wildebeest (C. gnou) is endemic to southern Africa, barely escaped extinction in the 1900s and is feared to be in danger of genetic swamping from the blue wildebeest. Despite the ecological importance of the wildebeest, there is a lack of understanding of how its unique migratory ecology has affected its gene flow, genetic structure and phylogeography. Here, we analyze whole genomes from 121 blue and 22 black wildebeest across the genus’ range. We find discrete genetic structure consistent with the morphologically defined subspecies. Unexpectedly, our analyses reveal no signs of recent interspecific admixture, but rather a late Pleistocene introgression of black wildebeest into the southern blue wildebeest populations. Finally, we find that migratory blue wildebeest populations exhibit a combination of long-range panmixia, higher genetic diversity and lower inbreeding levels compared to neighboring populations whose migration has recently been disrupted. These findings provide crucial insights into the evolutionary history of the wildebeest, and tangible genetic evidence for the negative effects of anthropogenic activities on highly migratory ungulates., The blue wildebeest (Connochaetes taurinus) is a keystone species in savanna ecosystems from southern to eastern Africa, and is well known for its spectacular migrations and locally extreme abundance. In contrast, the black wildebeest (C. gnou) is endemic to southern Africa, barely escaped extinction in the 1900s and is feared to be in danger of genetic swamping from the blue wildebeest. Despite the ecological importance of the wildebeest, there is a lack of understanding of how its unique migratory ecology has affected its gene flow, genetic structure and phylogeography. Here, we analyze whole genomes from 121 blue and 22 black wildebeest across the genus’ range. We find discrete genetic structure consistent with the morphologically defined subspecies. Unexpectedly, our analyses reveal no signs of recent interspecific admixture, but rather a late Pleistocene introgression of black wildebeest into the southern blue wildebeest populations. Finally, we find that migratory blue wildebeest populations exhibit a combination of long-range panmixia, higher genetic diversity and lower inbreeding levels compared to neighboring populations whose migration has recently been disrupted. These findings provide crucial insights into the evolutionary history of the wildebeest, and tangible genetic evidence for the negative effects of anthropogenic activities on highly migratory ungulates.
Published: 2024

35. Long-term follow-up observations of extreme coronal line emitting galaxies

Author: Clark, Peter, Graur, Or, Callow, Joseph, Aguilar, Jessica, Ahlen, Steven, Anderson, Joseph P, Berger, Edo, Müller-bravo, Tomás E, Brink, Thomas G, Brooks, David, Chen, Ting-wan, Claybaugh, Todd, De la macorra, Axel, Doel, Peter, Filippenko, Alexei V, Forero-romero, Jamie E, Gomez, Sebastian, Gromadzki, Mariusz, Honscheid, Klaus, Inserra, Cosimo, Kisner, Theodore, Landriau, Martin, Makrygianni, Lydia, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Nicholl, Matt, Nie, Jundan, Onori, Francesca, Palmese, Antonella, Poppett, Claire, Reynolds, Thomas, Rezaie, Mehdi, Rossi, Graziano, Sanchez, Eusebio, Schubnell, Michael, Tarlé, Gregory, Weaver, Benjamin A, Wevers, Thomas, Young, David R, Zheng, Weikang, Zhou, Zhimin, Clark, Peter, Graur, Or, Callow, Joseph, Aguilar, Jessica, Ahlen, Steven, Anderson, Joseph P, Berger, Edo, Müller-bravo, Tomás E, Brink, Thomas G, Brooks, David, Chen, Ting-wan, Claybaugh, Todd, De la macorra, Axel, Doel, Peter, Filippenko, Alexei V, Forero-romero, Jamie E, Gomez, Sebastian, Gromadzki, Mariusz, Honscheid, Klaus, Inserra, Cosimo, Kisner, Theodore, Landriau, Martin, Makrygianni, Lydia, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Nicholl, Matt, Nie, Jundan, Onori, Francesca, Palmese, Antonella, Poppett, Claire, Reynolds, Thomas, Rezaie, Mehdi, Rossi, Graziano, Sanchez, Eusebio, Schubnell, Michael, Tarlé, Gregory, Weaver, Benjamin A, Wevers, Thomas, Young, David R, Zheng, Weikang, and Zhou, Zhimin
Published: 2024

36. Co-occurrence of borderline and schizotypal personality disorders: a scoping review

Author: Meisner, Maria W., Lenzenweger, Mark F., Storebø, Ole J., Petersen, Lea S., Bach, Bo, Simonsen, Erik, Meisner, Maria W., Lenzenweger, Mark F., Storebø, Ole J., Petersen, Lea S., Bach, Bo, and Simonsen, Erik
Abstract: Background The historical concept of borderline conditions refers to the pathology on the border between neurosis and psychosis. In DSM-III the conditions were divided into specific but also somewhat overlapping diagnostic criteria for Borderline Personality Disorder (BPD) and Schizotypal Personality Disorder (SPD). This phenomenological overlap, which results in co-occurrence of the two diagnoses, remains a clinical challenge to this day. Methods To address this issue we examined the co-occurrence of SPD and BPD according to the established DSM-IV/-5 diagnostic criteria. A literature search was conducted including studies that employed a structured interview with defined BPD and SPD criteria. Results Studies from 20 samples were included (i.e. 15 patients, 3 community and 2 forensic samples). For patients diagnosed primarily with BPD, 1–27% also met the criteria for SPD and for patients diagnosed primarily with SPD, 5 – 33% showed co-occurrence with BPD. In the forensic samples, co-occurrence for primary BPD was 10% and 67 – 82% for primary SPD. In the community samples, co-occurrence for primary BPD was 29% and 50% for primary SPD. The pattern of co-occurrence across community samples was particularly heterogeneous. Conclusion The identified co-occurrences for BPD and SPD were considerably sample-dependent, and samples and measurements were generally too heterogeneous for a precise meta-analysis. Forensic and community samples generally showed higher co-occurrences, but these findings were characterized by potential methodological limitations.
Published: 2024

37. The role of Marius Petipa in the creation of Russian ballet

Author: Meisner, Nadine
Subjects: 792.8, Ballet--Russia--History--19th century
Published: 2013
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38. Encounters with exhibits : a study of children’s activity at interactive exhibits in three museums

Author: Meisner, Robin Stephanie
Subjects: 370
Abstract: This thesis develops arguments relevant to learning in informal environments about the nature of the activity, interaction and collaboration that emerge in young children (ages 4-12) at specific interactive exhibits in informal learning institutions. Using video recordings of children's activity at ten different interactive exhibits as principal data, this thesis seeks to unpack the notion that children are merely 'just playing' with, at and around the exhibits - or, put differently, it aims to specify the activity behind 'interactivity'. In so doing, it explores the ways in which the diverse forms of social interaction occurring at the exhibit face contribute to and might enable the emergence of specific forms of activity. A case is made for the use of two distinct analytic methods in order to address, firstly, what behaviours are displayed by young children at the exhibits studied, and then, how and why aspects of those behaviours emerge in the particular manner in which they do. Sources from education, cognitive development and developmental psychology are used in the development of a theoretically and empirically driven coding schema that is applied systematically to the video data to begin to address 'what' behaviours are displayed - the first question. Subsequently, building on an interactional perspective that gives primacy to the pervasive nature of the contributions of others - to social interaction - the 'how' and 'why', or second questions are addressed. To this end, an analysis that draws on ethnomethodology and conversation analysis is used to explore the role of observation and imitation in the children's activity at the exhibit face. The final chapter reflects upon the observations and findings of the whole study to consider their implications for potential learning at and the design of interactive exhibits. It explores the extent to which the design of exhibits might enable particular forms of activity and co-participation, and puts forth design sensitivities for exhibit designers to consider. It offers a critique of the two analytic methods and their potential utility for future research. And, finally, it seeks to show that when children's activity at exhibits is analysed in detail, children who are seen to be 'just playing' are indeed engaged in a range of productive actions and interactions.
Published: 2007

39. The genetics of susceptibility to leprosy

Author: Meisner, Sarah
Subjects: 572.8, Genome screen, Candidate gene studies
Abstract: There is strong evidence that genetic factors play a role in susceptibility to leprosy. Although the major histocompatibility complex is known to play a part, it does not account for the whole picture. Recent advances in genetic technology have made it possible to identify loci involved in complex traits. In this thesis I discuss two contrasting approaches: a genome-wide search for the detection of major genes, and candidate gene association studies capable of detecting smaller genetic effects. 242 affected sibling pairs with leprosy were identified in Tamil Nadu in South India. DNA extracted from their blood was used to perform a two-stage genome wide search. Initially 92 families were screened using 293 polymorphic microsatellite markers. A further 96 families were then used to rescreen the markers that showed lod scores suggestive of linkage. Markers on chromosomes 2, 6, 10, 16 and 17 showed increased sharing which could be consistent with the presence of minor genes. These regions include some interesting candidate genes that warrant further investigation. Association studies were performed on 5 candidate gaies using cases and controls from South India, Bengal, and Mali: Interleukins-4 and -10, tumour necrosis factor (INF), vitamin D receptor, and the natural resistance associated macrophage protein 1 (NRAMP1). An association was found between the NRAMP1 1729+55del4 polymorphism and leprosy type in a population from Mali, mutant homozygotes being susceptible to paucibacillary leprosy whilst heterozygotes were susceptible to multibacillary leprosy (x2 =8.88, p=0.00288 OR=5.79{CI 1.46-24.61}). These findings persisted after logistic regression to allow for region and ethnicity. This association was not observed in the South Indian cases and controls. A borderline association was found between the TNF - 238 polymorphism and susceptibility to leprosy in a South Indian population, cases having an excess of the common allele compared to controls (2x2 x2 = 4.12, p=0.042 OR=1.68{CI 0.98-2.87}).
Published: 1999
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40. The VST ATLAS quasar survey I: Catalogue of photometrically selected quasar candidates

Author: Eltvedt, AM, Shanks, T, Metcalfe, N, Ansarinejad, B, Barrientos, LF, Sharp, R, Malik, U, Murphy, DNA, Irwin, M, Wilson, M, Alexander, DM, Kovacs, A, Garcia-Bellido, J, Ahlen, S, Brooks, D, de la Macorra, A, Font-Ribera, A, Gontcho, SGA, Honscheid, K, Meisner, A, Miquel, R, Nie, J, Tarle, G, Vargas-Magana, M, Zhou, Z, Eltvedt, AM, Shanks, T, Metcalfe, N, Ansarinejad, B, Barrientos, LF, Sharp, R, Malik, U, Murphy, DNA, Irwin, M, Wilson, M, Alexander, DM, Kovacs, A, Garcia-Bellido, J, Ahlen, S, Brooks, D, de la Macorra, A, Font-Ribera, A, Gontcho, SGA, Honscheid, K, Meisner, A, Miquel, R, Nie, J, Tarle, G, Vargas-Magana, M, and Zhou, Z
Abstract: We present the VST ATLAS Quasar Survey, consisting of ∼1229 000 quasar (QSO) candidates with 16 < g < 22.5 over ∼4700 deg2. The catalogue is based on VST ATLAS+NEOWISE imaging surveys and aims to reach a QSO sky density of 130 deg−2 for $z$ < 2.2 and ∼30 deg−2 for $z$ > 2.2. To guide our selection, we use X-ray/UV/optical/MIR data in the extended William Herschel Deep Field (WHDF) where we find a g < 22.5 broad-line QSO density of 269 ± 67 deg−2, roughly consistent with the expected ∼196 deg−2. We find that ∼25 per cent of our QSOs are morphologically classed as optically extended. Overall, we find that in these deep data, MIR, UV, and X-ray selections are ∼70–90 per cent complete while X-ray suffers less contamination than MIR and UV. MIR is however more sensitive than X-ray or UV to $z$ > 2.2 QSOs at g < 22.5 and the $S_X(0.5-10\, {\rm keV})\gt 1\times 10^{-14}$ ergs cm−2 s−1 limit of eROSITA. We adjust the selection criteria from our previous 2QDES pilot survey and prioritize VST ATLAS candidates that show both UV and MIR excess, also selecting candidates initially classified as extended. We test our selections using data from DESI (which will be released in DR1) and 2dF to estimate the efficiency and completeness, and we use ANNz2 to determine photometric redshifts. Applying over the ∼4700 deg2 ATLAS area gives us $\sim 917\,000\, z\lt 2.2$ QSO candidates of which 472 000 are likely to be $z$ < 2.2 QSOs, implying a sky density of ∼100 deg−2, which our WHDF analysis suggests will rise to at least 130 deg−2 when eROSITA X-ray candidates are included. At $z$ > 2.2, we find ∼310() 000 candidates, of which 169 000 are likely to be QSOs for a sky density of ∼36 deg−2.
Published: 2023

41. Konflikt eller inte konflikt, det är frågan... :

Author: Meisner, Sanna, Hagerman, Karolina, Meisner, Sanna, and Hagerman, Karolina
Abstract: Syftet med studien är att undersöka pedagogers syn på konflikter mellan kollegor i förskolan. Genom studien önskar vi belysa konflikter mellan pedagoger i förskolan samt vilken inverkan konflikter kan ha på pedagogers samspel, trivsel och välmående. Vi fann här ett GAP i den forskning som vi hittat inom området konflikt och konflikthantering. Vi använder oss av en kvantitativ metod genom enkäter för att samla in empirisk data. Enkäterna besvarades av 171 pedagoger i 28 skånska kommuner. Den insamlade empirin analyseras genom deskriptiv statistik och tolkas utifrån Jordans (2015) begrepp: robust samarbetskultur och självinsikt, konfliktnivåerna: individnivå, relationsnivå och systemnivå samt Galtungs ABC-modell. Resultatet visar att det i stor utsträckning förekommer konflikter mellan kollegor i förskolan samt att dessa kan komma att inverka på samspel, trivseln och välmåendet om de förblir olösta. Trivsel anses vara högt prioriterat av respondenterna och trots förekomsten av konflikter verkar respondenterna trivas på arbetsplatsen. Utifrån resultatet drar vi slutsatsen att majoriteten av respondenterna uppfattar begreppet konflikt som negativt betingat. En annan slutsats är att det behöver finnas kunskap om konflikter och konflikthantering kollegor emellan för att kunna skapa ett gott sampel samt ökad trivseln och välmåendet hos pedagoger på arbetsplatsen.
Published: 2023

42. Charakterisierung der kurzperiodischen Bewegung des Ekström-Eisschelfs im Bereich der Aufsetzzone mit Hilfe von GNSS-Messungen

Author: Scheinert, Mirko, Fromm, Tanja, Horwath, Martin, Technische Universität Dresden, Heidrich-Meisner, Karl, Scheinert, Mirko, Fromm, Tanja, Horwath, Martin, Technische Universität Dresden, and Heidrich-Meisner, Karl
Abstract: Gezeitenbewegungen auf Eisschelfen werden schon seit den 90er-Jahren mit globalen Navigationssatellitensystemen (GNSS) gemessen. Kürzlich wurden an der Neumayer-Station III auf dem Ekström-Eisschelf mit Seismologie und GNSS unerwartet große drittel- und vierteltägige Gezeitensignale in der horizontalen Bewegung beobachtet. Es wurde die Hypothese aufgestellt, dass diese hochfrequenten Gezeitensignale ihren Ursprung an der Aufsetzzone des Ekström-Eisschelfs haben. Deshalb wurden im Laufe der letzten zwei Jahre weitere seismologische und GNSS-Messungen an der Aufsetzzone durchgeführt. Diese Arbeit verfolgt die Forschungsfragen, mit welcher Genauigkeit epochenweise geschätzte Koordinaten der GNSS-Messungen an der Aufsetzzone bestimmt werden können und welche Gezeitensignale signifikant auf geophysikalische oder glaziologische Prozesse zurückzuführen sind. Dafür wurden sowohl mit den Grundgestein verbundene GNSS-Stationen als auch die GNSS-Stationen an der Aufsetzzone mit der Bernese GNSS Software ausgewertet. Die stationären mit dem Grundgestein verbundenen GNSS-Stationen wurden dabei zur Abschätzung der erreichbaren Genauigkeit genutzt und als Referenzstation für die differentielle GNSS-Auswertung verwendet. Die Koordinatenzeitreihen wurden anschließend im Zeit- sowie Frequenzbereich analysiert. Die Ergebnisse zeigen, dass mit differentiellem GNSS kinematische Koordinaten in Nordrichtung auf 6,0 mm, in Ostrichtung auf 5,4 mm und vertikal auf 17,7 mm genau bestimmt werden können. Dabei handelt es sich aber um eine Genauigkeit zu einem zeitlichen Mittel. Die absolute Position wird eventuell weniger genau bestimmt. Die Signifikanz geophysikalischer und glaziologischer Signale ist abhängig vom Messrauschen in den Zeitreihen. Die dadurch entstehenden Unsicherheiten konnten in dieser Arbeit akkurat abgeschätzt werden. Zusätzlich wird die Signifikanz einzelner Signale stark von Artefakten aus den GNSS-Orbits beeinflusst. Konkret betrifft das Frequenzen, die nahe den ganzzahli
Published: 2023

43. GTC Follow-up Observations of Very Metal-poor Star Candidates from DESI

Author: Prieto, Carlos Allende, Prieto, Carlos Allende, Aguado, David S, Hernández, Jonay I González, Rebolo, Rafael, Najita, Joan, Manser, Christopher J, Rockosi, Constance, Slepian, Zachary, Mezcua, Mar, Valluri, Monica, Ezzeddine, Rana, Koposov, Sergey E, Cooper, Andrew P, Dey, Arjun, Gänsicke, Boris T, Li, Ting S, Cunha, Katia, Zou, Siwei, Aguilar, Jessica Nicole, Ahlen, Steven, Brooks, David, Claybaugh, Todd, Cole, Shaun, Eftekharzadeh, Sarah, Fanning, Kevin, Forero-Romero, Jaime, Gontcho, Satya Gontcho A, Honscheid, Klaus, Jablonka, Pascale, Kehoe, Robert, Kisner, Theodore, Landriau, Martin, de la Macorra, Axel, Meisner, Aaron, Miquel, Ramón, Moustakas, John, Nie, Jundan, Poppett, Claire, Prada, Francisco, Rezaie, Mehdi, Rossi, Graziano, Sánchez, Eusebio, Schubnell, Michael, Sharples, Ray, Siudek, Malgorzata, Smith, Verne V, Tarlé, Gregory, Vincenzo, Fiorenzo, Weaver, Benjamin Alan, Zhou, Zhimin, Zou, Hu, Prieto, Carlos Allende, Prieto, Carlos Allende, Aguado, David S, Hernández, Jonay I González, Rebolo, Rafael, Najita, Joan, Manser, Christopher J, Rockosi, Constance, Slepian, Zachary, Mezcua, Mar, Valluri, Monica, Ezzeddine, Rana, Koposov, Sergey E, Cooper, Andrew P, Dey, Arjun, Gänsicke, Boris T, Li, Ting S, Cunha, Katia, Zou, Siwei, Aguilar, Jessica Nicole, Ahlen, Steven, Brooks, David, Claybaugh, Todd, Cole, Shaun, Eftekharzadeh, Sarah, Fanning, Kevin, Forero-Romero, Jaime, Gontcho, Satya Gontcho A, Honscheid, Klaus, Jablonka, Pascale, Kehoe, Robert, Kisner, Theodore, Landriau, Martin, de la Macorra, Axel, Meisner, Aaron, Miquel, Ramón, Moustakas, John, Nie, Jundan, Poppett, Claire, Prada, Francisco, Rezaie, Mehdi, Rossi, Graziano, Sánchez, Eusebio, Schubnell, Michael, Sharples, Ray, Siudek, Malgorzata, Smith, Verne V, Tarlé, Gregory, Vincenzo, Fiorenzo, Weaver, Benjamin Alan, Zhou, Zhimin, and Zou, Hu
Abstract: The observations from the Dark Energy Spectroscopic Instrument (DESI) will significantly increase the numbers of known extremely metal-poor stars by a factor of ∼10, improving the sample statistics to study the early chemical evolution of the Milky Way and the nature of the first stars. In this paper we report follow-up observations with high signal-to-noise ratio of nine metal-poor stars identified during the DESI commissioning with the Optical System for Imaging and Low-Resolution Integrated Spectroscopy (OSIRIS) instrument on the 10.4 m Gran Telescopio Canarias. The analysis of the data using a well-vetted methodology confirms the quality of the DESI spectra and the performance of the pipelines developed for the data reduction and analysis of DESI data.
Published: 2023

44. Adjuvant Docetaxel in Node-Negative Breast Cancer Patients: A Randomized Trial of AGO-Breast Study Group, German Breast Group, and EORTC-Pathobiology Group.

Author: Thomssen, C., Vetter, M., Kantelhardt, E.J., Meisner, C., Schmidt, M., Martin, P.M., Clatot, F., Augustin, D., Hanf, V., Paepke, D., Meinerz, W., Hoffmann, G., Wiest, W., Sweep, F.C.G.J., Schmitt, M., Jänicke, F., Loibl, S., Minckwitz, G.V., Harbeck, N., Thomssen, C., Vetter, M., Kantelhardt, E.J., Meisner, C., Schmidt, M., Martin, P.M., Clatot, F., Augustin, D., Hanf, V., Paepke, D., Meinerz, W., Hoffmann, G., Wiest, W., Sweep, F.C.G.J., Schmitt, M., Jänicke, F., Loibl, S., Minckwitz, G.V., and Harbeck, N.
Abstract: Item does not contain fulltext, BACKGROUND: In node-negative breast cancer (NNBC), a high risk of recurrence is determined by clinico-pathological or tumor-biological assessment. Taxanes may improve adjuvant chemotherapy. METHODS: NNBC 3-Europe, the first randomized phase-3 trial in node-negative breast cancer (BC) with tumor-biological risk assessment, recruited 4146 node-negative breast cancer patients from 2002 to 2009 in 153 centers. Risk assessment was performed by clinico-pathological factors (43%) or biomarkers (uPA/PAI-1, urokinase-type plasminogen activator/its inhibitor PAI-1). High-risk patients received six courses 5-fluorouracil (500 mg/m(2)), epirubicin (100 mg/m(2)), cyclophosphamide (500 mg/m(2)) (FEC), or three courses FEC followed by three courses docetaxel 100 mg/m(2) (FEC-Doc). Primary endpoint was disease-free survival (DFS). RESULTS: In the intent-to-treat population, 1286 patients had received FEC-Doc, and 1255 received FEC. Median follow-up was 45 months. Tumor characteristics were equally distributed; 90.6% of tested tumors had high uPA/PAI-1-concentrations. Planned courses were given in 84.4% (FEC-Doc) and 91.5% (FEC). Five-year-DFS was 93.2% (95% C.I. 91.1-94.8) with FEC-Doc and 93.7% (91.7-95.3) with FEC. Five-year-overall survival was 97.0% (95.4-98.0) for FEC-Doc and 96.6% % (94.9-97.8) for FEC. CONCLUSIONS: With adequate adjuvant chemotherapy, even high-risk node-negative breast cancer patients have an excellent prognosis. Docetaxel did not further reduce the rate of early recurrences and led to significantly more treatment discontinuations.
Published: 2023

45. Target Selection and Validation of DESI Luminous Red Galaxies

Author: Zhou, R, Zhou, R, Dey, B, Newman, JA, Eisenstein, DJ, Dawson, K, Bailey, S, Berti, A, Guy, J, Lan, TW, Zou, H, Aguilar, J, Ahlen, S, Alam, S, Brooks, D, de la Macorra, A, Dey, A, Dhungana, G, Fanning, K, Font-Ribera, A, Gontcho, SGA, Honscheid, K, Ishak, M, Kisner, T, Kovács, A, Kremin, A, Landriau, M, Levi, ME, Magneville, C, Manera, M, Martini, P, Meisner, AM, Miquel, R, Moustakas, J, Myers, AD, Nie, J, Palanque-Delabrouille, N, Percival, WJ, Poppett, C, Prada, F, Raichoor, A, Ross, AJ, Schlafly, E, Schlegel, D, Schubnell, M, Tarlé, G, Weaver, BA, Wechsler, RH, Yéche, C, Zhou, Z, Zhou, R, Zhou, R, Dey, B, Newman, JA, Eisenstein, DJ, Dawson, K, Bailey, S, Berti, A, Guy, J, Lan, TW, Zou, H, Aguilar, J, Ahlen, S, Alam, S, Brooks, D, de la Macorra, A, Dey, A, Dhungana, G, Fanning, K, Font-Ribera, A, Gontcho, SGA, Honscheid, K, Ishak, M, Kisner, T, Kovács, A, Kremin, A, Landriau, M, Levi, ME, Magneville, C, Manera, M, Martini, P, Meisner, AM, Miquel, R, Moustakas, J, Myers, AD, Nie, J, Palanque-Delabrouille, N, Percival, WJ, Poppett, C, Prada, F, Raichoor, A, Ross, AJ, Schlafly, E, Schlegel, D, Schubnell, M, Tarlé, G, Weaver, BA, Wechsler, RH, Yéche, C, and Zhou, Z
Abstract: The Dark Energy Spectroscopic Instrument (DESI) is carrying out a five-year survey that aims to measure the redshifts of tens of millions of galaxies and quasars, including 8 million luminous red galaxies (LRGs) in the redshift range 0.4 < z ≲ 1.0. Here we present the selection of the DESI LRG sample and assess its spectroscopic performance using data from Survey Validation (SV) and the first two months of the Main Survey. The DESI LRG sample, selected using g, r, z, and W1 photometry from the DESI Legacy Imaging Surveys, is highly robust against imaging systematics. The sample has a target density of 605 deg−2 and a comoving number density of 5 × 10−4 h3 Mpc−3 in 0.4 < z < 0.8; this is a significantly higher density than previous LRG surveys (such as SDSS, BOSS, and eBOSS) while also extending to z ∼ 1. After applying a bright star veto mask developed for the sample, 98.9% of the observed LRG targets yield confident redshifts (with a catastrophic failure rate of 0.2% in the confident redshifts), and only 0.5% of the LRG targets are stellar contamination. The LRG redshift efficiency varies with source brightness and effective exposure time, and we present a simple model that accurately characterizes this dependence. In the appendices, we describe the extended LRG samples observed during SV.
Published: 2023

46. The DESI Bright Galaxy Survey: Final Target Selection, Design, and Validation

Author: ChangHoon Hahn, Wilson, Michael J., Ruiz-Macias, Omar, Cole, Shaun, Weinberg, David H., Moustakas, John, Kremin, Anthony, Tinker, Jeremy L., Smith, Alex, Wechsler, Risa H., Ahlen, Steven, Alam, Shadab, Bailey, Stephen, Brooks, David, Cooper, Andrew P., Davis, Tamara M., Dawson, Kyle, Dey, Arjun, Dey, Biprateep, Eftekharzadeh, Sarah, Eisenstein, Daniel J., Fanning, Kevin, Forero-Romero, Jaime E., Frenk, Carlos S., Gaztañaga, Enrique, Gontcho A Gontcho, Satya, Guy, Julien, Honscheid, Klaus, Ishak, Mustapha, Juneau, Stéphanie, Kehoe, Robert, Kisner, Theodore, Lan, Ting-Wen, Landriau, Martin, Le Guillou, Laurent, Levi, Michael E., Magneville, Christophe, Martini, Paul, Meisner, Aaron, Myers, Adam D., Nie, Jundan, Norberg, Peder, Palanque-Delabrouille, Nathalie, Percival, Will J., Poppett, Claire, Prada, Francisco, Raichoor, Anand, Ross, Ashley J., Safonova, Sasha, Saulder, Christoph, Schlafly, Eddie, Schlegel, David, Sierra-Porta, David, Tarle, Gregory, Weaver, Benjamin A, Yèche, Christophe, Zarrouk, Pauline, Zhou, Rongpu, Zhou, Zhimin, Zou, Hu, ChangHoon Hahn, Wilson, Michael J., Ruiz-Macias, Omar, Cole, Shaun, Weinberg, David H., Moustakas, John, Kremin, Anthony, Tinker, Jeremy L., Smith, Alex, Wechsler, Risa H., Ahlen, Steven, Alam, Shadab, Bailey, Stephen, Brooks, David, Cooper, Andrew P., Davis, Tamara M., Dawson, Kyle, Dey, Arjun, Dey, Biprateep, Eftekharzadeh, Sarah, Eisenstein, Daniel J., Fanning, Kevin, Forero-Romero, Jaime E., Frenk, Carlos S., Gaztañaga, Enrique, Gontcho A Gontcho, Satya, Guy, Julien, Honscheid, Klaus, Ishak, Mustapha, Juneau, Stéphanie, Kehoe, Robert, Kisner, Theodore, Lan, Ting-Wen, Landriau, Martin, Le Guillou, Laurent, Levi, Michael E., Magneville, Christophe, Martini, Paul, Meisner, Aaron, Myers, Adam D., Nie, Jundan, Norberg, Peder, Palanque-Delabrouille, Nathalie, Percival, Will J., Poppett, Claire, Prada, Francisco, Raichoor, Anand, Ross, Ashley J., Safonova, Sasha, Saulder, Christoph, Schlafly, Eddie, Schlegel, David, Sierra-Porta, David, Tarle, Gregory, Weaver, Benjamin A, Yèche, Christophe, Zarrouk, Pauline, Zhou, Rongpu, Zhou, Zhimin, and Zou, Hu
Abstract: Over the next 5 yr, the Dark Energy Spectroscopic Instrument (DESI) will use 10 spectrographs with 5000 fibers on the 4 m Mayall Telescope at Kitt Peak National Observatory to conduct the first Stage IV dark energy galaxy survey. At z < 0.6, the DESI Bright Galaxy Survey (BGS) will produce the most detailed map of the universe during the dark-energy-dominated epoch with redshifts of >10 million galaxies spanning 14,000 deg2 . In this work, we present and validate the final BGS target selection and survey design. From the Legacy Surveys, BGS will target an r < 19.5 mag limited sample (BGS Bright), a fainter 19.5 < r < 20.175 color-selected sample (BGS Faint), and a smaller low-z quasar sample. BGS will observe these targets using exposure times scaled to achieve homogeneous completeness and cover the footprint three times. We use observations from the Survey Validation programs conducted prior to the main survey along with simulations to show that BGS can complete its strategy and make optimal use of “bright” time. BGS targets have stellar contamination <1%, and their densities do not depend strongly on imaging properties. BGS Bright will achieve >80% fiber assignment efficiency. Finally, BGS Bright and BGS Faint will achieve >95% redshift success over any observing condition. BGS meets the requirements for an extensive range of scientific applications. BGS will yield the most precise baryon acoustic oscillation and redshift-space distortion measurements at z < 0.4. It presents opportunities for new methods that require highly complete and dense samples (e.g., N-point statistics, multitracers). BGS further provides a powerful tool to study galaxy populations and the relations between galaxies and dark matter.
Published: 2023

47. Unraveling emission line galaxy conformity at z~1 with DESI early data

Author: Yuan, Sihan, Wechsler, Risa H., Wang, Yunchong, Reyes, Mithi A. C. de los, Myles, Justin, Rocher, Antoine, Hadzhiyska, Boryana, Aguilar, Jessica Nicole, Ahlen, Steven, Brooks, David, Claybaugh, Todd, Cole, Shaun, de la Macorra, Axel, Forero-Romero, Jaime E., Gontcho, Satya Gontcho A, Guy, Julien, Honscheid, Klaus, Kisner, Theodore, Levi, Michael, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Nie, Jundan, Palanque-Delabrouille, Nathalie, Poppett, Claire, Rezaie, Mehdi, Ross, Ashley J., Rossi, Graziano, Sanchez, Eusebio, Schubnel, Michael, Seo, Hee- Jong, Tarlé, Gregory, Weaver, Benjamin Alan, Zhou, Zhimin, Yuan, Sihan, Wechsler, Risa H., Wang, Yunchong, Reyes, Mithi A. C. de los, Myles, Justin, Rocher, Antoine, Hadzhiyska, Boryana, Aguilar, Jessica Nicole, Ahlen, Steven, Brooks, David, Claybaugh, Todd, Cole, Shaun, de la Macorra, Axel, Forero-Romero, Jaime E., Gontcho, Satya Gontcho A, Guy, Julien, Honscheid, Klaus, Kisner, Theodore, Levi, Michael, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Nie, Jundan, Palanque-Delabrouille, Nathalie, Poppett, Claire, Rezaie, Mehdi, Ross, Ashley J., Rossi, Graziano, Sanchez, Eusebio, Schubnel, Michael, Seo, Hee- Jong, Tarlé, Gregory, Weaver, Benjamin Alan, and Zhou, Zhimin
Abstract: Emission line galaxies (ELGs) are now the preeminent tracers of large-scale structure at z>0.8 due to their high density and strong emission lines, which enable accurate redshift measurements. However, relatively little is known about ELG evolution and the ELG-halo connection, exposing us to potential modeling systematics in cosmology inference using these sources. In this paper, we propose a physical picture of ELGs and improve ELG-halo connection modeling using a variety of observations and simulated galaxy models. We investigate DESI-selected ELGs in COSMOS data, and infer that ELGs are rapidly star-forming galaxies with a large fraction exhibiting disturbed morphology, implying that many of them are likely to be merger-driven starbursts. We further postulate that the tidal interactions from mergers lead to correlated star formation in central-satellite ELG pairs, a phenomenon dubbed "conformity." We argue for the need to include conformity in the ELG-halo connection using galaxy models such as IllustrisTNG, and by combining observations such as the DESI ELG auto-correlation, ELG cross-correlation with Luminous Red Galaxies (LRGs), and ELG-cluster cross-correlation. We also explore the origin of conformity using the UniverseMachine model and elucidate the difference between conformity and the well-known galaxy assembly bias effect., Comment: 25 pages, 20 figures, submitted to MNRAS, comments welcome
Published: 2023

48. An Investigation of New Brown Dwarf Spectral Binary Candidates From the Backyard Worlds: Planet 9 Citizen Science Initiative

Author: Bravo, Alexia, Schneider, Adam C., Gagliuffi, Daniella Bardalez, Burgasser, Adam J., Meisner, Aaron M., Kirkpatrick, J. Davy, Faherty, Jacqueline K., Kuchner, Marc J., Caselden, Dan, Sainio, Arttu, Hamlet, Les, Worlds, The Backyard, Collaboration, Planet 9, Bravo, Alexia, Schneider, Adam C., Gagliuffi, Daniella Bardalez, Burgasser, Adam J., Meisner, Aaron M., Kirkpatrick, J. Davy, Faherty, Jacqueline K., Kuchner, Marc J., Caselden, Dan, Sainio, Arttu, Hamlet, Les, Worlds, The Backyard, and Collaboration, Planet 9
Abstract: We present three new brown dwarf spectral binary candidates: CWISE J072708.09$-$360729.2, CWISE J103604.84$-$514424.4, and CWISE J134446.62$-$732053.9, discovered by citizen scientists through the Backyard Worlds: Planet 9 project. Follow-up near-infrared spectroscopy shows that each of these objects is poorly fit by a single near-infrared standard. We constructed binary templates and found significantly better fits, with component types of L7+T4 for CWISE J072708.09$-$360729.2, L7+T4 for CWISE J103604.84$-$514424.4, and L7+T7 for CWISE J134446.62$-$732053.9. However, further investigation of available spectroscopic indices for evidence of binarity and large amplitude variability suggests that CWISE J072708.09$-$360729.2 may instead be a strong variability candidate. Our analysis offers tentative evidence and characterization of these peculiar brown dwarf sources, emphasizing their value as promising targets for future high-resolution imaging or photometric variability studies., Comment: Accepted to the Astronomical Journal
Published: 2023

49. CWISE J105512.11+544328.3: A Nearby Y Dwarf Spectroscopically Confirmed with Keck/NIRES

Author: Robbins, Grady, Meisner, Aaron M., Schneider, Adam C., Burgasser, Adam J., Kirkpatrick, J. Davy, Gagne, Jonathan, Hsu, Chih-Chun, Moranta, Leslie, Casewell, Sarah, Marocco, Federico, Gerasimov, Roman, Faherty, Jacqueline K., Kuchner, Marc J., Caselden, Dan, Cushing, Michael C., Alejandro, Sherelyn, Worlds, The Backyard, Collaboration, Planet 9, Collaboration, Cool Neighbors, Robbins, Grady, Meisner, Aaron M., Schneider, Adam C., Burgasser, Adam J., Kirkpatrick, J. Davy, Gagne, Jonathan, Hsu, Chih-Chun, Moranta, Leslie, Casewell, Sarah, Marocco, Federico, Gerasimov, Roman, Faherty, Jacqueline K., Kuchner, Marc J., Caselden, Dan, Cushing, Michael C., Alejandro, Sherelyn, Worlds, The Backyard, Collaboration, Planet 9, and Collaboration, Cool Neighbors
Abstract: Y dwarfs, the coolest known spectral class of brown dwarfs, overlap in mass and temperature with giant exoplanets, providing unique laboratories for studying low-temperature atmospheres. However, only a fraction of Y dwarf candidates have been spectroscopically confirmed. We present Keck/NIRES near-infrared spectroscopy of the nearby ($d \approx 6-8$ pc) brown dwarf CWISE J105512.11+544328.3. Although its near-infrared spectrum aligns best with the Y0 standard in the $J$-band, no standard matches well across the full $YJHK$ wavelength range. The CWISE J105512.11+544328.3 NH$_3$-$H$ = 0.427 $\pm$ 0.0012 and CH$_4$-$J$ = 0.0385 $\pm$ 0.0007 absorption indices and absolute Spitzer [4.5] magnitude of 15.18 $\pm$ 0.22 are also indicative of an early Y dwarf rather than a late T dwarf. CWISE J105512.11+544328.3 additionally exhibits the bluest Spitzer [3.6]$-$[4.5] color among all spectroscopically confirmed Y dwarfs. Despite this anomalously blue Spitzer color given its low luminosity, CWISE J105512.11+544328.3 does not show other clear kinematic or spectral indications of low metallicity. Atmospheric model comparisons yield a log(g) $\le$ 4.5 and $T_{\rm eff} \approx 500 \pm 150$ K for this source. We classify CWISE J105512.11+544328.3 as a Y0 (pec) dwarf, adding to the remarkable diversity of the Y-type population. JWST spectroscopy would be crucial to understanding the origin of this Y dwarf's unusual preference for low-gravity models and blue 3-5 $\mu$m color., Comment: accepted for publication in The Astrophysical Journal
Published: 2023

50. DESI Complete Calibration of the Color-Redshift Relation (DC3R2): Results from early DESI data

Author: McCullough, J., Gruen, D., Amon, A., Roodman, A., Masters, D., Raichoor, A., Schlegel, D., Canning, R., Castander, F. J., DeRose, J., Miquel, R., Myles, J., Newman, J. A., Slosar, A., Speagle, J., Wilson, M. J., Aguilar, J., Ahlen, S., Bailey, S., Brooks, D., Claybaugh, T., Cole, S., Dawson, K., de la Macorra, A., Doel, P., Forero-Romero, J. E., Gontcho, S. Gontcho A, Guy, J., Kehoe, R., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M., Manera, M., Martini, P., Meisner, A., Moustakas, J., Nie, J., Percival, W. J., Poppett, C., Prada, F., Rezaie, M., Rossi, G., Sanchez, E., Seo, H., Tarlé, G., Weaver, B. A., Zhou, Z., Zou, H., McCullough, J., Gruen, D., Amon, A., Roodman, A., Masters, D., Raichoor, A., Schlegel, D., Canning, R., Castander, F. J., DeRose, J., Miquel, R., Myles, J., Newman, J. A., Slosar, A., Speagle, J., Wilson, M. J., Aguilar, J., Ahlen, S., Bailey, S., Brooks, D., Claybaugh, T., Cole, S., Dawson, K., de la Macorra, A., Doel, P., Forero-Romero, J. E., Gontcho, S. Gontcho A, Guy, J., Kehoe, R., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M., Manera, M., Martini, P., Meisner, A., Moustakas, J., Nie, J., Percival, W. J., Poppett, C., Prada, F., Rezaie, M., Rossi, G., Sanchez, E., Seo, H., Tarlé, G., Weaver, B. A., Zhou, Z., and Zou, H.
Abstract: We present initial results from the Dark Energy Spectroscopic Instrument (DESI) Complete Calibration of the Color-Redshift Relation (DC3R2) secondary target survey. Our analysis uses 230k galaxies that overlap with KiDS-VIKING $ugriZYJHK_s$ photometry to calibrate the color-redshift relation and to inform photometric redshift (photo-z) inference methods of future weak lensing surveys. Together with Emission Line Galaxies (ELGs), Luminous Red Galaxies (LRGs), and the Bright Galaxy Survey (BGS) that provide samples of complementary color, the DC3R2 targets help DESI to span 56% of the color space visible to Euclid and LSST with high confidence spectroscopic redshifts. The effects of spectroscopic completeness and quality are explored, as well as systematic uncertainties introduced with the use of common Self Organizing Maps trained on different photometry than the analysis sample. We further examine the dependence of redshift on magnitude at fixed color, important for the use of bright galaxy spectra to calibrate redshifts in a fainter photometric galaxy sample. We find that noise in the KiDS-VIKING photometry introduces a dominant, apparent magnitude dependence of redshift at fixed color, which indicates a need for carefully chosen deep drilling fields, and survey simulation to model this effect for future weak lensing surveys., Comment: 19 pages, 16 figures, submitted to MNRAS, interactive visualizations at https://jmccull.github.io/DC3R2_Overview
Published: 2023

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