Author: "Font P" - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Font P"' showing total 6,633 results

Start Over Author "Font P"

6,633 results on '"Font P"'

151. Bound by the Bounty: Collaboratively Shaping Evaluation Processes for Queer AI Harms

Author: QueerInAI, Organizers of, Dennler, Nathan, Ovalle, Anaelia, Singh, Ashwin, Soldaini, Luca, Subramonian, Arjun, Tu, Huy, Agnew, William, Ghosh, Avijit, Yee, Kyra, Peradejordi, Irene Font, Talat, Zeerak, Russo, Mayra, and Pinhal, Jess de Jesus de Pinho
Subjects: Computer Science - Computers and Society, Computer Science - Artificial Intelligence
Abstract: Bias evaluation benchmarks and dataset and model documentation have emerged as central processes for assessing the biases and harms of artificial intelligence (AI) systems. However, these auditing processes have been criticized for their failure to integrate the knowledge of marginalized communities and consider the power dynamics between auditors and the communities. Consequently, modes of bias evaluation have been proposed that engage impacted communities in identifying and assessing the harms of AI systems (e.g., bias bounties). Even so, asking what marginalized communities want from such auditing processes has been neglected. In this paper, we ask queer communities for their positions on, and desires from, auditing processes. To this end, we organized a participatory workshop to critique and redesign bias bounties from queer perspectives. We found that when given space, the scope of feedback from workshop participants goes far beyond what bias bounties afford, with participants questioning the ownership, incentives, and efficacy of bounties. We conclude by advocating for community ownership of bounties and complementing bounties with participatory processes (e.g., co-creation)., Comment: To appear at AIES 2023
Published: 2023

152. Astrometric Calibration and Performance of the Dark Energy Spectroscopic Instrument Focal Plane

Author: Kent, S., Neilsen, E., Honscheid, K., Rabinowitz, D., Schlafly, E. F., Guy, J., Schlegel, D., Garcia-Bellido, J., Li, T. S., Sanchez, E., Silber, Joseph Harry, Aguilar, J., Ahlen, S., Brooks, D., Claybaugh, T., de la Macorra, A., Doel, P., Eisenstein, D. J., Fanning, K., Font-Ribera, A., Forero-Romero, J. E., Gontcho, S. Gontcho A, Jimenez, J., Kirkby, D., Kisner, T., Kremin, Anthony, Landriau, M., Guillou, L. Le, Levi, Michael E., Magneville, C., Manera, M., Martini, Paul, Meisner, Aaron M., Miquel, R., Moustakas, J., Nie, J., Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Rezaie, M., Ross, A. J., Rossi, G., Schubnell, M., Seo, H., Tarle, Gregory, Weaver, B. A., Zhou, Rongpu, Zhou, Zhimin, and Zou, H.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Dark Energy Spectroscopic Instrument, consisting of 5020 robotic fiber positioners and associated systems on the Mayall telescope at Kitt Peak, Arizona, is carrying out a survey to measure the spectra of 40 million galaxies and quasars and produce the largest 3D map of the universe to date. The primary science goal is to use baryon acoustic oscillations to measure the expansion history of the universe and the time evolution of dark energy. A key function of the online control system is to position each fiber on a particular target in the focal plane with an accuracy of 11$\mu$m rms 2-D. This paper describes the set of software programs used to perform this function along with the methods used to validate their performance., Comment: 27 pages, 16 figures
Published: 2023
Full Text: View/download PDF

153. Local primordial non-Gaussianity from the large-scale clustering of photometric DESI luminous red galaxies

Author: Rezaie, Mehdi, Ross, Ashley J., Seo, Hee-Jong, Kong, Hui, Porredon, Anna, Samushia, Lado, Chaussidon, Edmond, Krolewski, Alex, de Mattia, Arnaud, Beutler, Florian, Aguilar, Jessica Nicole, Ahlen, Steven, Alam, Shadab, Avila, Santiago, Bahr-Kalus, Benedict, Bermejo-Climent, Jose, Brooks, David, Claybaugh, Todd, Cole, Shaun, Dawson, Kyle, de la Macorra, Axel, Doel, Peter, Font-Ribera, Andreu, Forero-Romero, Jaime E., Gontcho, Satya Gontcho A, Guy, Julien, Honscheid, Klaus, Huterer, Dragan, Kisner, Theodore, Landriau, Martin, Levi, Michael, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Mueller, Eva-Maria, Myers, Adam, Newman, Jeffrey A., Nie, Jundan, Palanque-Delabrouille, Nathalie, Percival, Will, Poppett, Claire, Rossi, Graziano, Sanchez, Eusebio, Schubnell, Michael, Tarlé, Gregory, Weaver, Benjamin Alan, Yèche, Christophe, Zhou, Zhimin, and Zou, Hu
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Computer Science - Machine Learning, Physics - Computational Physics, Physics - Data Analysis, Statistics and Probability
Abstract: We use angular clustering of luminous red galaxies from the Dark Energy Spectroscopic Instrument (DESI) imaging surveys to constrain the local primordial non-Gaussianity parameter $\fnl$. Our sample comprises over 12 million targets, covering 14,000 square degrees of the sky, with redshifts in the range $0.2< z < 1.35$. We identify Galactic extinction, survey depth, and astronomical seeing as the primary sources of systematic error, and employ linear regression and artificial neural networks to alleviate non-cosmological excess clustering on large scales. Our methods are tested against simulations with and without $\fnl$ and systematics, showing superior performance of the neural network treatment. The neural network with a set of nine imaging property maps passes our systematic null test criteria, and is chosen as the fiducial treatment. Assuming the universality relation, we find $\fnl = 34^{+24(+50)}_{-44(-73)}$ at 68\%(95\%) confidence. We apply a series of robustness tests (e.g., cuts on imaging, declination, or scales used) that show consistency in the obtained constraints. We study how the regression method biases the measured angular power-spectrum and degrades the $\fnl$ constraining power. The use of the nine maps more than doubles the uncertainty compared to using only the three primary maps in the regression. Our results thus motivate the development of more efficient methods that avoid over-correction, protect large-scale clustering information, and preserve constraining power. Additionally, our results encourage further studies of $\fnl$ with DESI spectroscopic samples, where the inclusion of 3D clustering modes should help separate imaging systematics and lessen the degradation in the $\fnl$ uncertainty., Comment: 21 pages, 17 figures, 7 tables (Appendix excluded). Published in MNRAS
Published: 2023
Full Text: View/download PDF

154. The 2-point correlation function covariance with fewer mocks

Author: Trusov, Svyatoslav, Zarrouk, Pauline, Cole, Shaun, Norberg, Peder, Zhao, Cheng, Aguilar, Jessica Nicole, Ahlen, Steven, Brooks, David, de la Macorra, Axel, Doel, Peder, Font-Ribera, Andreu, Honscheid, Klaus, Kisner, Theodore, Landriau, Martin, Magneville, Christophe, Miquel, Ramon, Nie, Jundan, Poppett, Claire, Schubnell, Michael, Tarlé, Gregory, and Zhou, Zhimin
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present an approach for accurate estimation of the covariance of 2-point correlation functions that requires fewer mocks than the standard mock-based covariance. This can be achieved by dividing a set of mocks into jackknife regions and fitting the correction term first introduced in Mohammad & Percival (2022), such that the mean of the jackknife covariances corresponds to the one from the mocks. This extends the model beyond the shot-noise limited regime, allowing it to be used for denser samples of galaxies. We test the performance of our fitted jackknife approach, both in terms of accuracy and precision, using lognormal mocks with varying densities and approximate EZmocks mimicking the DESI LRG and ELG samples in the redshift range of z = [0.8, 1.2]. We find that the Mohammad-Percival correction produces a bias in the 2-point correlation function covariance matrix that grows with number density and that our fitted jackknife approach does not. We also study the effect of the covariance on the uncertainty of cosmological parameters by performing a full-shape analysis. We find that our fitted jackknife approach based on 25 mocks is able to recover unbiased and as precise cosmological parameters as the ones obtained from a covariance matrix based on 1000 or 1500 mocks, while the Mohammad-Percival correction produces uncertainties that are twice as large. The number of mocks required to obtain an accurate estimation of the covariance for 2-point correlation function is therefore reduced by a factor of 40-60., Comment: 13 pages, 14 figures, accepted to MNRAS
Published: 2023
Full Text: View/download PDF

155. Validation of semi-analytical, semi-empirical covariance matrices for two-point correlation function for Early DESI data

Author: Rashkovetskyi, Michael, Eisenstein, Daniel J., Aguilar, Jessica Nicole, Brooks, David, Claybaugh, Todd, Cole, Shaun, Dawson, Kyle, de la Macorra, Axel, Doel, Peter, Fanning, Kevin, Font-Ribera, Andreu, Forero-Romero, Jaime E., Gontcho, Satya Gontcho A, Hahn, ChangHoon, Honscheid, Klaus, Kehoe, Robert, Kisner, Theodore, Landriau, Martin, Levi, Michael, Manera, Marc, Miquel, Ramon, Moon, Jeongin, Nadathur, Seshadri, Nie, Jundan, Poppett, Claire, Ross, Ashley J., Rossi, Graziano, Sanchez, Eusebio, Saulder, Christoph, Schubnell, Michael, Seo, Hee-Jong, Tarle, Gregory, Valcin, David, Weaver, Benjamin Alan, Zhao, Cheng, Zhou, Zhimin, and Zou, Hu
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Mathematics - Statistics Theory, Physics - Data Analysis, Statistics and Probability
Abstract: We present an extended validation of semi-analytical, semi-empirical covariance matrices for the two-point correlation function (2PCF) on simulated catalogs representative of Luminous Red Galaxies (LRG) data collected during the initial two months of operations of the Stage-IV ground-based Dark Energy Spectroscopic Instrument (DESI). We run the pipeline on multiple effective Zel'dovich (EZ) mock galaxy catalogs with the corresponding cuts applied and compare the results with the mock sample covariance to assess the accuracy and its fluctuations. We propose an extension of the previously developed formalism for catalogs processed with standard reconstruction algorithms. We consider methods for comparing covariance matrices in detail, highlighting their interpretation and statistical properties caused by sample variance, in particular, nontrivial expectation values of certain metrics even when the external covariance estimate is perfect. With improved mocks and validation techniques, we confirm a good agreement between our predictions and sample covariance. This allows one to generate covariance matrices for comparable datasets without the need to create numerous mock galaxy catalogs with matching clustering, only requiring 2PCF measurements from the data itself. The code used in this paper is publicly available at https://github.com/oliverphilcox/RascalC., Comment: 19 pages, 1 figure. Published in MNRAS. Code available at https://github.com/oliverphilcox/RascalC, table and figure data available at https://dx.doi.org/10.5281/zenodo.7750637
Published: 2023
Full Text: View/download PDF

156. PROVABGS: The Probabilistic Stellar Mass Function of the BGS One-Percent Survey

Author: Hahn, ChangHoon, Aguilar, Jessica Nicole, Alam, Shadab, Ahlen, Steven, Brooks, David, Cole, Shaun, de la Macorra, Axel, Doel, Peter, Font-Ribera, Andreu A., Forero-Romero, Jaime E., Gontcho, Satya Gontcho A, Honscheid, Klaus, Huang, Song, Kisner, Theodore, Kremin, Anthony, Landriau, Martin, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Nie, Jundan, Poppett, Claire, Rossi, Graziano, Saintonge, Amélie, Sanchez, Eusebio, Saulder, Christoph, Schubnell, Michael, Seo, Hee-Jong, Siudek, Małgorzata, Speranza, Federico, Tarlé, Gregory, Weaver, Benjamin A., Wechsler, Risa H., Yuan, Sihan, Zhou, Zhimin, and Zou, Hu
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the probabilistic stellar mass function (pSMF) of galaxies in the DESI Bright Galaxy Survey (BGS), observed during the One-Percent Survey. The One-Percent Survey was one of DESI's survey validation programs conducted from April to May 2021, before the start of the main survey. It used the same target selection and similar observing strategy as the main survey and successfully observed the spectra and redshifts of 143,017 galaxies in the $r < 19.5$ magnitude-limited BGS Bright sample and 95,499 galaxies in the fainter surface brightness and color selected BGS Faint sample over $z < 0.6$. We derive pSMFs from posteriors of stellar mass, $M_*$, inferred from DESI photometry and spectroscopy using the Hahn et al. (2022a; arXiv:2202.01809) PRObabilistic Value-Added BGS (PROVABGS) Bayesian SED modeling framework. We use a hierarchical population inference framework that statistically and rigorously propagates the $M_*$ uncertainties. Furthermore, we include correction weights that account for the selection effects and incompleteness of the BGS observations. We present the redshift evolution of the pSMF in BGS as well as the pSMFs of star-forming and quiescent galaxies classified using average specific star formation rates from PROVABGS. Overall, the pSMFs show good agreement with previous stellar mass function measurements in the literature. Our pSMFs showcase the potential and statistical power of BGS, which in its main survey will observe >100$\times$ more galaxies. Moreover, we present the statistical framework for subsequent population statistics measurements using BGS, which will characterize the global galaxy population and scaling relations at low redshifts with unprecedented precision., Comment: 25 pages, 12 figures; data used to generate figures is available at https://doi.org/10.5281/zenodo.8018936; submitted to ApJ
Published: 2023

157. Optimal 1D Ly$\alpha$ Forest Power Spectrum Estimation -- III. DESI early data

Author: Karaçaylı, Naim Göksel, Martini, Paul, Guy, Julien, Ravoux, Corentin, Karim, Marie Lynn Abdul, Armengaud, Eric, Walther, Michael, Aguilar, J., Ahlen, S., Bailey, S., Bautista, J., Beltran, S. F., Brooks, D., Cabayol-Garcia, L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Dawson, K., de la Cruz, R., de la Macorra, A., Doel, P., Font-Ribera, A., Forero-Romero, J. E., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gordon, C., Herrera-Alcantar, H. K, Honscheid, K., Iršič, V., Ishak, M., Kehoe, R., Kisner, T., Kremin, A., Landriau, M., Guillou, L. Le, Levi, M. E., Lukić, Z., Meisner, A., Miquel, R., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Napolitano, L., Nie, J., Niz, G., Palanque-Delabrouille, N., Percival, W. J., Pieri, M., Poppett, C., Prada, F., Pérez-Ràfols, I., Ramírez-Pérez, C., Rossi, G., Sanchez, E., Seo, H., Sinigaglia, F., Tan, T., Tarlé, G., Wang, B., Weaver, B. A., Yèche, C., and Zhou, Z.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The one-dimensional power spectrum $P_{\mathrm{1D}}$ of the Ly$\alpha$ forest provides important information about cosmological and astrophysical parameters, including constraints on warm dark matter models, the sum of the masses of the three neutrino species, and the thermal state of the intergalactic medium. We present the first measurement of $P_{\mathrm{1D}}$ with the quadratic maximum likelihood estimator (QMLE) from the Dark Energy Spectroscopic Instrument (DESI) survey early data sample. This early sample of $54~600$ quasars is already comparable in size to the largest previous studies, and we conduct a thorough investigation of numerous instrumental and analysis systematic errors to evaluate their impact on DESI data with QMLE. We demonstrate the excellent performance of the spectroscopic pipeline noise estimation and the impressive accuracy of the spectrograph resolution matrix with two-dimensional image simulations of raw DESI images that we processed with the DESI spectroscopic pipeline. We also study metal line contamination and noise calibration systematics with quasar spectra on the red side of the Ly$\alpha$ emission line. In a companion paper, we present a similar analysis based on the Fast Fourier Transform estimate of the power spectrum. We conclude with a comparison of these two approaches and implications for the upcoming DESI Year 1 analysis., Comment: 23 pages, 20 figures. To be published in MNRAS
Published: 2023

158. The DESI One-Percent Survey: Exploring A Generalized SHAM for Multiple Tracers with the UNIT Simulation

Author: Yu, Jiaxi, Zhao, Cheng, Gonzalez-Perez, Violeta, Chuang, Chia-Hsun, Brodzeller, Allyson, de Mattia, Arnaud, Kneib, Jean-Paul, Krolewski, Alex, Rocher, Antoine, Ross, Ashley, Wang, Yunchong, Yuan, Sihan, Zhang, Hanyu, Zhou, Rongpu, Aguilar, Jessica Nicole, Ahlen, Steven, Brooks, David, Dawson, Kyle, de la Macorra, Alex, Doel, Peter, Fanning, Kevin, Font-Ribera, Andreu, Forero-Romero, Jaime, Gontcho, Satya Gontcho A, Honscheid, Klaus, Kehoe, Robert, Kisner, Theodore, Kremin, Anthony, Landriau, Martin, Manera, Marc, Martini, Paul, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Nie, Jundan, Percival, Will, Poppett, Claire, Raichoor, Anand, Rossi, Graziano, Seo, Hee-Jong, Tarlé, Gregory, Zhou, Zhimin, and Zou, Hu
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We perform SubHalo Abundance Matching (SHAM) studies on UNIT simulations with \{$\sigma, V_{\rm ceil}, v_{\rm smear}$\}-SHAM and \{$\sigma, V_{\rm ceil},f_{\rm sat}$\}-SHAM. They are designed to reproduce the clustering on 5--30$\,\hmpc$ of Luminous Red Galaxies (LRGs), Emission Line Galaxies (ELGs) and Quasi-Stellar Objects (QSOs) at $0.4
Published: 2023

159. The Lyman-$\alpha$ forest catalog from the Dark Energy Spectroscopic Instrument Early Data Release

Author: Ramírez-Pérez, César, Pérez-Ràfols, Ignasi, Font-Ribera, Andreu, Karim, M. Abdul, Armengaud, E., Bautista, J., Beltran, S. F., Cabayol-Garcia, L., Cai, Z., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Cuceu, A., de la Cruz, R., García-Bellido, J., Gonzalez-Morales, A. X., Gordon, C., Herrera-Alcantar, H. K., Iršič, V., Ishak, M., Karaçaylı, N. G., Lukić, Zarija, Manser, C. J., Montero-Camacho, P., Napolitano, L., Niz, G., Pieri, M., Ravoux, C., Sinigaglia, F., Tan, T., Walther, M., Wang, B., Aguilar, J., Ahlen, S., Bailey, S., Brooks, D., Claybaugh, T., Dawson, K., de la Macorra, A., Dhungana, G., Doel, P., Fanning, K., Forero-Romero, J. E., Gontcho, S. Gontcho A, Guy, J., Honscheid, K., Kehoe, R., Kisner, T., Landriau, M., Guillou, L. Le, Levi, M. E., Magneville, C., Martini, P., Meisner, A., Miquel, R., Moustakas, J., Mueller, E., Muñoz-Gutiérrez, A., Nie, J., Palanque-Delabrouille, N., Percival, W. J., Rossi, G., Sanchez, E., Schlafly, E. F., Schlegel, D., Seo, H., Tarlé, G., Weaver, B. A., Yèche, C., and Zhou, Z.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present and validate the catalog of Lyman-$\alpha$ forest fluctuations for 3D analyses using the Early Data Release (EDR) from the Dark Energy Spectroscopic Instrument (DESI) survey. We used 88,511 quasars collected from DESI Survey Validation (SV) data and the first two months of the main survey (M2). We present several improvements to the method used to extract the Lyman-$\alpha$ absorption fluctuations performed in previous analyses from the Sloan Digital Sky Survey (SDSS). In particular, we modify the weighting scheme and show that it can improve the precision of the correlation function measurement by more than 20%. This catalog can be downloaded from https://data.desi.lbl.gov/public/edr/vac/edr/lya/fuji/v0.3 and it will be used in the near future for the first DESI measurements of the 3D correlations in the Lyman-$\alpha$ forest.
Published: 2023

160. The Dark Energy Spectroscopic Instrument: One-dimensional power spectrum from first Lyman-$\alpha$ forest samples with Fast Fourier Transform

Author: Ravoux, Corentin, Karim, Marie Lynn Abdul, Armengaud, Eric, Walther, Michael, Karaçaylı, Naim Göksel, Martini, Paul, Guy, Julien, Aguilar, Jessica Nicole, Ahlen, Steven, Bailey, Stephen, Bautista, Julian, Beltran, Sergio Felipe, Brooks, David, Cabayol-Garcia, Laura, Chabanier, Solène, Chaussidon, Edmond, Chaves-Montero, Jonás, Dawson, Kyle, de la Cruz, Rodrigo, de la Macorra, Axel, Doel, Peter, Fanning, Kevin, Font-Ribera, Andreu, Forero-Romero, Jaime, Gontcho, Satya Gontcho A, Gonzalez-Morales, Alma, Gordon, Calum, Herrera-Alcantar, Hiram, Honscheid, Klaus, Iršič, Vid, Ishak, Mustapha, Kehoe, Robert, Kisner, Theodore, Kremin, Anthony, Landriau, Martin, Guillou, Laurent Le, Levi, Michael, Lukić, Zarija, Magneville, Christophe, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Mueller, Eva-Maria, Muñoz-Gutiérrez, Andrea, Napolitano, Lucas, Nie, Jundan, Niz, Gustavo, Palanque-Delabrouille, Nathalie, Percival, Will, Pérez-Ràfols, Ignasi, Pieri, Matthew, Poppett, Claire, Prada, Francisco, Pérez, César Ramírez, Rossi, Graziano, Sanchez, Eusebio, Schlegel, David, Schubnell, Michael, Seo, Hee-Jong, Sinigaglia, Francesco, Tan, Ting, Tarlé, Gregory, Wang, Ben, Weaver, Benjamin, Yèche, Christophe, and Zhou, Zhimin
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the one-dimensional Lyman-$\alpha$ forest power spectrum measurement using the first data provided by the Dark Energy Spectroscopic Instrument (DESI). The data sample comprises $26,330$ quasar spectra, at redshift $z > 2.1$, contained in the DESI Early Data Release and the first two months of the main survey. We employ a Fast Fourier Transform (FFT) estimator and compare the resulting power spectrum to an alternative likelihood-based method in a companion paper. We investigate methodological and instrumental contaminants associated to the new DESI instrument, applying techniques similar to previous Sloan Digital Sky Survey (SDSS) measurements. We use synthetic data based on log-normal approximation to validate and correct our measurement. We compare our resulting power spectrum with previous SDSS and high-resolution measurements. With relatively small number statistics, we successfully perform the FFT measurement, which is already competitive in terms of the scale range. At the end of the DESI survey, we expect a five times larger Lyman-$\alpha$ forest sample than SDSS, providing an unprecedented precise one-dimensional power spectrum measurement., Comment: 23 pages, 23 figures, Journal version
Published: 2023
Full Text: View/download PDF

161. The Early Data Release of the Dark Energy Spectroscopic Instrument

Author: DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Aldering, G., Alexander, D. M., Alfarsy, R., Prieto, C. Allende, Alvarez, M., Alves, O., Anand, A., Andrade-Oliveira, F., Armengaud, E., Asorey, J., Avila, S., Aviles, A., Bailey, S., Balaguera-Antolínez, A., Ballester, O., Baltay, C., Bault, A., Bautista, J., Behera, J., Beltran, S. F., BenZvi, S., Silva, L. Beraldo e, Bermejo-Climent, J. R., Berti, A., Besuner, R., Beutler, F., Bianchi, D., Blake, C., Blum, R., Bolton, A. S., Brieden, S., Brodzeller, A., Brooks, D., Brown, Z., Buckley-Geer, E., Burtin, E., Cabayol-Garcia, L., Cai, Z., Canning, R., Cardiel-Sas, L., Rosell, A. Carnero, Castander, F. J., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chen, X., Chuang, C., Claybaugh, T., Cole, S., Cooper, A. P., Cuceu, A., Davis, T. M., Dawson, K., de Belsunce, R., de la Cruz, R., de la Macorra, A., Della Costa, J., de Mattia, A., Demina, R., Demirbozan, U., DeRose, J., Dey, A., Dey, B., Dhungana, G., Ding, J., Ding, Z., Doel, P., Doshi, R., Douglass, K., Edge, A., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Escoffier, S., Fagrelius, P., Fan, X., Fanning, K., Fawcett, V. A., Ferraro, S., Ereza, J., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Frenk, C. S., Gänsicke, B. T., García, L. Á., García-Bellido, J., Garcia-Quintero, C., Garrison, L. H., Gil-Marín, H., Golden-Marx, J., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Graur, O., Green, D., Gruen, D., Guy, J., Hadzhiyska, B., Hahn, C., Han, J. J., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Hou, J., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Jacques, A., Jana, A., Jiang, L., Jimenez, J., Jing, Y. P., Joudaki, S., Jullo, E., Juneau, S., Kizhuprakkat, N., Karaçaylı, N. G., Karim, T., Kehoe, R., Kent, S., Khederlarian, A., Kim, S., Kirkby, D., Kisner, T., Kitaura, F., Kneib, J., Koposov, S. E., Kovács, A., Kremin, A., Krolewski, A., L'Huillier, B., Lahav, O., Lambert, A., Lamman, C., Lan, T. -W., Landriau, M., Lang, D., Lange, J. U., Lasker, J., Leauthaud, A., Guillou, L. Le, Levi, M. E., Li, T. S., Linder, E., Lyons, A., Magneville, C., Manera, M., Manser, C. J., Margala, D., Martini, P., McDonald, P., Medina, G. E., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Meneses-Rizo, J., Mezcua, M., Miquel, R., Montero-Camacho, P., Moon, J., Moore, S., Moustakas, J., Mueller, E., Mundet, J., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nie, J., Nikutta, R., Niz, G., Norberg, P., Noriega, H. E., Paillas, E., Palanque-Delabrouille, N., Palmese, A., Zhiwei, P., Parkinson, D., Penmetsa, S., Percival, W. J., Pérez-Fernández, A., Pérez-Ràfols, I., Pieri, M., Poppett, C., Porredon, A., Pothier, S., Prada, F., Pucha, R., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Ravoux, C., Rocher, A., Rockosi, C., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Sabiu, C. G., Said, K., Saintonge, A., Samushia, L., Sanchez, E., Saulder, C., Schaan, E., Schlafly, E. F., Schlegel, D., Scholte, D., Schubnell, M., Seo, H., Shafieloo, A., Sharples, R., Sheu, W., Silber, J., Sinigaglia, F., Siudek, M., Slepian, Z., Smith, A., Soumagnac, M. T., Sprayberry, D., Stephey, L., Suárez-Pérez, J., Sun, Z., Tan, T., Tarlé, G., Tojeiro, R., Ureña-López, L. A., Vaisakh, R., Valcin, D., Valdes, F., Valluri, M., Vargas-Magaña, M., Variu, A., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., White, M., Xie, Y., Yang, J., Yèche, C., Yu, J., Yuan, S., Zhang, H., Zhang, Z., Zhao, C., Zheng, Z., Zhou, R., Zhou, Z., Zou, H., Zou, S., and Zu, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) completed its five-month Survey Validation in May 2021. Spectra of stellar and extragalactic targets from Survey Validation constitute the first major data sample from the DESI survey. This paper describes the public release of those spectra, the catalogs of derived properties, and the intermediate data products. In total, the public release includes good-quality spectral information from 466,447 objects targeted as part of the Milky Way Survey, 428,758 as part of the Bright Galaxy Survey, 227,318 as part of the Luminous Red Galaxy sample, 437,664 as part of the Emission Line Galaxy sample, and 76,079 as part of the Quasar sample. In addition, the release includes spectral information from 137,148 objects that expand the scope beyond the primary samples as part of a series of secondary programs. Here, we describe the spectral data, data quality, data products, Large-Scale Structure science catalogs, access to the data, and references that provide relevant background to using these spectra., Comment: 43 pages, 7 figures, 17 tables, accepted for publication in the Astronomical Journal
Published: 2023
Full Text: View/download PDF

162. The Optical Corrector for the Dark Energy Spectroscopic Instrument

Author: Miller, Timothy N., Doel, Peter, Gutierrez, Gaston, Besuner, Robert, Brooks, David, Gallo, Giuseppe, Heetderks, Henry, Jelinsky, Patrick, Kent, Stephen M., Lampton, Michael, Levi, Michael, Liang, Ming, Meisner, Aaron, Sholl, Michael J., Silber, Joseph Harry, Sprayberry, David, Aguilar, Jessica Nicole, de la Macorra, Axel, Eisenstein, Daniel, Fanning, Kevin, Font-Ribera, Andreu, Gaztanaga, Enrique, Gontcho, Satya Gontcho A, Honscheid, Klaus, Jimenez, Jorge, Joyce, Dick, Kehoe, Robert, Kisner, Theodore, Kremin, Anthony, Landriau, Martin, Guillou, Laurent Le, Magneville, Christophe, Martini, Paul, Miquel, Ramon, Moustakas, John, Nie, Jundan, Percival, Will, Poppett, Claire, Prada, Francisco, Rossi, Graziano, Schlegel, David, Schubnell, Michael, Seo, Hee-Jong, Sharples, Ray, Tarle, Gregory, Vargas-Magana, Mariana, and Zhou, Zhimin
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) is currently measuring the spectra of 40\,million galaxies and quasars, the largest such survey ever made to probe the nature of cosmological dark energy. The 4-meter Mayall telescope at Kitt Peak National Observatory has been adapted for DESI, including the construction of a 3.2-degree diameter prime focus corrector that focuses astronomical light onto a 0.8-meter diameter focal surface with excellent image quality over the DESI bandpass of 360-980nm. The wide-field corrector includes six lenses, as large as 1.1-meters in diameter and as heavy as 237\,kilograms, including two counter-rotating wedged lenses that correct for atmospheric dispersion over Zenith angles from 0 to 60 degrees. The lenses, cells, and barrel assembly all meet precise alignment tolerances on the order of tens of microns. The barrel alignment is maintained throughout a range of observing angles and temperature excursions in the Mayall dome by use of a hexapod, which is itself supported by a new cage, ring, and truss structure. In this paper we describe the design, fabrication, and performance of the new corrector and associated structure, focusing on how they meet DESI requirements. In particular we describe the prescription and specifications of the lenses, design choices and error budgeting of the barrel assembly, stray light mitigations, and integration and test at the Mayall telescope. We conclude with some validation highlights that demonstrate the successful corrector on-sky performance, and list some lessons learned during the multi-year fabrication phase., Comment: 68 pages, 56 figures, 22 tables. Submitted to the Astronomical Journal
Published: 2023

163. Survey Operations for the Dark Energy Spectroscopic Instrument

Author: Schlafly, E. F., Kirkby, D., Schlegel, D. J., Myers, A. D., Raichoor, A., Dawson, K., Aguilar, J., Prieto, C. Allende, Bailey, S., BenZvi, S., Bermejo-Climent, J., Brooks, D., de la Macorra, A., Dey, Arjun, Doel, P., Fanning, K., Font-Ribera, A., Forero-Romero, J. E., García-Bellido, J., Gontcho, S. Gontcho A, Guy, J., Hahn, C., Honscheid, K., Ishak, M., Juneau, S., Kehoe, R., Kisner, T., Kremin, A., Landriau, M., Lang, D. A., Lasker, J., Levi, M. E., Magneville, C., Manser, C. J., Martini, P., Meisner, A. M., Miquel, R., Moustakas, J., Newman, J. A., Nie, Jundan, Palanque-Delabrouille, N., Percival, W. J., Poppett, C., Rockosi, C., Ross, A. J., Rossi, G., Tarlé, G., Weaver, B. A., Yèche, C., and Zhou, R.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) survey is a spectroscopic survey of tens of millions of galaxies at $0 < z < 3.5$ covering 14,000 square degrees of the sky. In its first 1.1 years of survey operations, it has observed more than 14 million galaxies and 4 million stars. We describe the processes that govern DESI's observations of the 15,000 fields composing the survey. This includes the planning of each night's observations in the afternoon; automatic selection of fields to observe during the night; real-time assessment of field completeness on the basis of observing conditions during each exposure; reduction, redshifting, and quality assurance of each field of targets in the morning following observation; and updates to the list of future targets to observe on the basis of these results. We also compare the performance of the survey with historical expectations and find good agreement. Simulations of the weather and of DESI observations using the real field-selection algorithm show good agreement with the actual observations. After accounting for major unplanned shutdowns, the dark time survey is progressing about 7% faster than forecast, which is good agreement given approximations made in the simulations., Comment: 30 pages, 12 figures; updated following referee report
Published: 2023

164. Validation of the Scientific Program for the Dark Energy Spectroscopic Instrument

Author: DESI Collaboration, Adame, A. G., Aguilar, J., Ahlen, S., Alam, S., Aldering, G., Alexander, D. M., Alfarsy, R., Prieto, C. Allende, Alvarez, M., Alves, O., Anand, A., Andrade-Oliveira, F., Armengaud, E., Asorey, J., Avila, S., Aviles, A., Bailey, S., Balaguera-Antolínez, A., Ballester, O., Baltay, C., Bault, A., Bautista, J., Behera, J., Beltran, S. F., BenZvi, S., Silva, L. Beraldo e, Bermejo-Climent, J. R., Berti, A., Besuner, R., Beutler, F., Bianchi, D., Blake, C., Blum, R., Bolton, A. S., Brieden, S., Brodzeller, A., Brooks, D., Brown, Z., Buckley-Geer, E., Burtin, E., Cabayol-Garcia, L., Cai, Z., Canning, R., Cardiel-Sas, L., Rosell, A. Carnero, Castander, F. J., Cervantes-Cota, J. L., Chabanier, S., Chaussidon, E., Chaves-Montero, J., Chen, S., Chuang, C., Claybaugh, T., Cole, S., Cooper, A. P., Cuceu, A., Davis, T. M., Dawson, K., de Belsunce, R., de la Cruz, R., de la Macorra, A., de Mattia, A., Demina, R., Demirbozan, U., DeRose, J., Dey, A., Dey, B., Dhungana, G., Ding, J., Ding, Z., Doel, P., Doshi, R., Douglass, K., Edge, A., Eftekharzadeh, S., Eisenstein, D. J., Elliott, A., Escoffier, S., Fagrelius, P., Fan, X., Fanning, K., Fawcett, V. A., Ferraro, S., Ereza, J., Flaugher, B., Font-Ribera, A., Forero-Sánchez, D., Forero-Romero, J. E., Frenk, C. S., Gänsicke, B. T., García, L. Á., García-Bellido, J., Garcia-Quintero, C., Garrison, L. H., Gil-Marín, H., Golden-Marx, J., Gontcho, S. Gontcho A, Gonzalez-Morales, A. X., Gonzalez-Perez, V., Gordon, C., Graur, O., Green, D., Gruen, D., Guy, J., Hadzhiyska, B., Hahn, C., Han, J. J., Hanif, M. M. S, Herrera-Alcantar, H. K., Honscheid, K., Hou, J., Howlett, C., Huterer, D., Iršič, V., Ishak, M., Jana, A., Jiang, L., Jimenez, J., Jing, Y. P., Joudaki, S., Joyce, R., Jullo, E., Juneau, S., Kizhuprakkat, N., Karaçaylı, N. G., Karim, T., Kehoe, R., Kent, S., Khederlarian, A., Kim, S., Kirkby, D., Kisner, T., Kitaura, F., Kneib, J., Koposov, S. E., Kovács, A., Kremin, A., Krolewski, A., L'Huillier, B., Lahav, O., Lambert, A., Lamman, C., Lan, T. -W., Landriau, M., Lang, D., Lange, J. U., Lasker, J., Guillou, L. Le, Leauthaud, A., Levi, M. E., Li, T. S., Linder, E., Lyons, A., Magneville, C., Manera, M., Manser, C. J., Margala, D., Martini, P., McDonald, P., Medina, G. E., Medina-Varela, L., Meisner, A., Mena-Fernández, J., Meneses-Rizo, J., Mezcua, M., Miquel, R., Montero-Camacho, P., Moon, J., Moore, S., Moustakas, J., Mueller, E., Mundet, J., Muñoz-Gutiérrez, A., Myers, A. D., Nadathur, S., Napolitano, L., Neveux, R., Newman, J. A., Nie, J., Niz, G., Norberg, P., Noriega, H. E., Paillas, E., Palanque-Delabrouille, N., Palmese, A., Zhiwei, P., Parkinson, D., Penmetsa, S., Percival, W. J., Pérez-Fernández, A., Pérez-Ràfols, I., Pieri, M., Poppett, C., Porredon, A., Prada, F., Pucha, R., Raichoor, A., Ramírez-Pérez, C., Ramirez-Solano, S., Rashkovetskyi, M., Ravoux, C., Rocher, A., Rockosi, C., Ross, A. J., Rossi, G., Ruggeri, R., Ruhlmann-Kleider, V., Sabiu, C. G., Said, K., Saintonge, A., Samushia, L., Sanchez, E., Saulder, C., Schaan, E., Schlafly, E. F., Schlegel, D., Scholte, D., Schubnell, M., Seo, H., Shafieloo, A., Sharples, R., Sheu, W., Silber, J., Sinigaglia, F., Siudek, M., Slepian, Z., Smith, A., Sprayberry, D., Stephey, L., Suárez-Pérez, J., Sun, Z., Tan, T., Tarlé, G., Tojeiro, R., Ureña-López, L. A., Vaisakh, R., Valcin, D., Valdes, F., Valluri, M., Vargas-Magaña, M., Variu, A., Verde, L., Walther, M., Wang, B., Wang, M. S., Weaver, B. A., Weaverdyck, N., Wechsler, R. H., White, M., Xie, Y., Yang, J., Yèche, C., Yu, J., Yuan, S., Zhang, H., Zhang, Z., Zhao, C., Zheng, Z., Zhou, R., Zhou, Z., Zou, H., Zou, S., and Zu, Y.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The Dark Energy Spectroscopic Instrument (DESI) was designed to conduct a survey covering 14,000 deg$^2$ over five years to constrain the cosmic expansion history through precise measurements of Baryon Acoustic Oscillations (BAO). The scientific program for DESI was evaluated during a five month Survey Validation (SV) campaign before beginning full operations. This program produced deep spectra of tens of thousands of objects from each of the stellar (MWS), bright galaxy (BGS), luminous red galaxy (LRG), emission line galaxy (ELG), and quasar target classes. These SV spectra were used to optimize redshift distributions, characterize exposure times, determine calibration procedures, and assess observational overheads for the five-year program. In this paper, we present the final target selection algorithms, redshift distributions, and projected cosmology constraints resulting from those studies. We also present a `One-Percent survey' conducted at the conclusion of Survey Validation covering 140 deg$^2$ using the final target selection algorithms with exposures of a depth typical of the main survey. The Survey Validation indicates that DESI will be able to complete the full 14,000 deg$^2$ program with spectroscopically-confirmed targets from the MWS, BGS, LRG, ELG, and quasar programs with total sample sizes of 7.2, 13.8, 7.46, 15.7, and 2.87 million, respectively. These samples will allow exploration of the Milky Way halo, clustering on all scales, and BAO measurements with a statistical precision of 0.28% over the redshift interval $z<1.1$, 0.39% over the redshift interval $1.1
Published: 2023
Full Text: View/download PDF

165. GHOST Commissioning Science Results: Identifying a new chemically peculiar star in Reticulum II

Author: Hayes, Christian R., Venn, Kim A., Waller, Fletcher, Jensen, Jaclyn, McConnachie, Alan W., Pazder, John, Sestito, Federico, Anthony, Andre, Baker, Gabriella, Bassett, John, Bento, Joao, Burley, Gregory, Brzeski, Jurek, Case, Scott, Chapin, Edward, Chin, Timothy, Chisholm, Eric, Churilov, Vladimir, Densmore, Adam, Diaz, Ruben, Dunn, Jennifer, Edgar, Michael, Farrell, Tony, Firpo, Veronica, Fitzsimmons, Joeleff, Font-Serra, Juan, Fuentes, Javier, Ganton, Colin, Gomez-Jimenez, Manuel, Hardy, Tim, Henderson, David, Hill, Alexis, Hoff, Brian, Ireland, Michael, Kalari, Venu, Kelly, Neal, Klauser, Urs, Kondrat, Yuriy, Labrie, Kathleen, Lambert, Sam, Luvaul, Lance, Lawrence, Jon, Lothrop, Jordan, Macdonald, G. Scott, Mali, Slavko, Margheim, Steve, McDermid, Richard, McGregor, Helen, Miller, Bryan, Miranda, Felipe, Muller, Rolf, Nielsen, Jon, Norbury, Ryan, Oberdorf, Oliver, Pai, Naveen, Perez, Gabriel, Prado, Pablo, Price, Ian, Quiroz, Carlos, Reshetov, Vladimir, Robertson, Gordon, Ruiz-Carmona, Roque, Salinas, Ricardo, Sebo, Kim M., Sheinis, Andrew, Shetrone, Matthew, Shortridge, Keith, Silversides, Katherine, Silva, Karleyne, Simpson, Chris, Smith, Greg, Szeto, Kei, Tims, Julia, Toro, Eduardo, Urrutia, Cristian, Venkatesan, Sudharshan, Waller, Lewis, Wevers, Ivan, Wierzbicki, Ramunas, White, Marc, Young, Peter, and Zhelem, Ross
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: The Gemini High-resolution Optical SpecTrograph (GHOST) is the newest high resolution spectrograph to be developed for a large aperture telescope, recently deployed and commissioned at the Gemini-South telescope. In this paper, we present the first science results from the GHOST spectrograph taking during its commissioning runs. We have observed the bright metal-poor benchmark star HD 122563, along with two stars in the ultra faint dwarf galaxy, Ret II, one of which was previously identified as a candidate member, but did not have a previous detailed chemical abundance analysis. This star (GDR3 0928) is found to be a bona fide member of Ret II, and from a spectral synthesis analysis, it is also revealed to be a CEMP-r star, with significant enhancements in the several light elements (C, N, O, Na, Mg, and Si), in addition to featuring an r-process enhancement like many other Ret II stars. The light-element enhancements in this star resemble the abundance patterns seen in the CEMP-no stars of other ultra faint dwarf galaxies, and are thought to have been produced by an independent source from the r-process. These unusual abundance patterns are thought to be produced by faint supernovae, which may be produced by some of the earliest generations of stars., Comment: 23 pages, 9 figures, 7 tables, submitted to the AAS Journals
Published: 2023

166. First detection of the BAO signal from early DESI data

Author: Moon, Jeongin, Valcin, David, Rashkovetskyi, Michael, Saulder, Christoph, Aguilar, Jessica Nicole, Ahlen, Steven, Alam, Shadab, Bailey, Stephen, Baltay, Charles, Blum, Robert, Brooks, David, Burtin, Etienne, Chaussidon, Edmond, Dawson, Kyle, de la Macorra, Axel, de M attia, Arnaud, Dhungana, Govinda, Eisenstein, Daniel, Flaugher, Brenna, Font-Ribera, Andreu, Forero-Romero, Jaime E, Garcia-Quintero, Cristhian, Gontcho, Satya Gontcho A, Guy, Julien, Hanif, Malik Muhammad Sikandar, Honscheid, Klaus, Ishak, Mustapha, Kehoe, Robert, Kim, Sumi, Kisner, Theodore, Kremin, Anthony, Landriau, Martin, Le Guillou, Laurent, Levi, Michael, Manera, Marc, Martini, Paul, McDonald, Patrick, Meisner, Aaron, Miquel, Ramon, Moustakas, John, Myers, Adam, Nadathur, Seshadri, Neveux, Richard, Newman, Jeffrey A, Nie, Jundan, Padmanabhan, Nikhil, Palanque-Delabrouille, Nathalie, Percival, Will, Fernández, Alejandro Pérez, Poppett, Claire, Prada, Francisco, Raichoor, Anand, Ross, Ashley J, Rossi, Graziano, Samushia, Lado, Schlegel, David, Seo, Hee-Jong, Tarlé, Gregory, Magana, Mariana Vargas, Variu, Andrei, Weaver, Benjamin Alan, White, Martin J, Yèche, Christophe, Yuan, Sihan, Zhao, Cheng, Zhou, Rongpu, Zhou, Zhimin, and Zou, Hu
Subjects: Space Sciences, Particle and High Energy Physics, Astronomical Sciences, Physical Sciences, galaxies: statistics, cosmology: large-scale structure of Universe, observations, dark energy, methods: data analysis, statistical, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: We present the first detection of the baryon acoustic oscillations (BAOs) signal obtained using unblinded data collected during the initial 2 months of operations of the Stage-IV ground-based Dark Energy Spectroscopic Instrument (DESI). From a selected sample of 261 291 luminous red galaxies spanning the redshift interval 0.4 < z < 1.1 and covering 1651 square degrees with a 57.9 per cent completeness level, we report a ∼5σ level BAO detection and the measurement of the BAO location at a precision of 1.7 per cent. Using a bright galaxy sample of 109 523 galaxies in the redshift range 0.1 < z < 0.5, over 3677 square degrees with a 50.0 per cent completeness, we also detect the BAO feature at ∼3σ significance with a 2.6 per cent precision. These first BAO measurements represent an important milestone, acting as a quality control on the optimal performance of the complex robotically actuated, fibre-fed DESI spectrograph, as well as an early validation of the DESI spectroscopic pipeline and data management system. Based on these first promising results, we forecast that DESI is on target to achieve a high-significance BAO detection at sub-per cent precision with the completed 5-yr survey data, meeting the top-level science requirements on BAO measurements. This exquisite level of precision will set new standards in cosmology and confirm DESI as the most competitive BAO experiment for the remainder of this decade.
Published: 2023

167. A striking relationship between dust extinction and radio detection in DESI QSOs: evidence for a dusty blow-out phase in red QSOs

Author: Fawcett, VA, Alexander, DM, Brodzeller, A, Edge, AC, Rosario, DJ, Myers, AD, Aguilar, J, Ahlen, S, Alfarsy, R, Brooks, D, Canning, R, Circosta, C, Dawson, K, de la Macorra, A, Doel, P, Fanning, K, Font-Ribera, A, Forero-Romero, JE, Gontcho, S Gontcho A, Guy, J, Harrison, CM, Honscheid, K, Juneau, S, Kehoe, R, Kisner, T, Kremin, A, Landriau, M, Manera, M, Meisner, AM, Miquel, R, Moustakas, J, Nie, J, Percival, WJ, Poppett, C, Pucha, R, Rossi, G, Schlegel, D, Siudek, M, Tarlé, G, Weaver, BA, Zhou, Z, and Zou, H
Subjects: Space Sciences, Physical Sciences, galaxies: active, galaxies: evolution, quasars: general, quasars: supermassive black holes, radio continuum: galaxies, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: We present the first eight months of data from our secondary target programme within the ongoing Dark Energy Spectroscopic Instrument (DESI) survey. Our programme uses a mid-infrared and optical colour selection to preferentially target dust-reddened quasi-stellar objects (QSOs) that would have otherwise been missed by the nominal DESI QSO selection. So far, we have obtained optical spectra for 3038 candidates, of which ∼70 per cent of the high-quality objects (those with robust redshifts) are visually confirmed to be Type 1 QSOs, consistent with the expected fraction from the main DESI QSO survey. By fitting a dust-reddened blue QSO composite to the QSO spectra, we find they are well-fitted by a normal QSO with up to AV ∼4 mag of line-of-sight dust extinction. Utilizing radio data from the LOFAR Two-metre Sky Survey (LoTSS) DR2, we identify a striking positive relationship between the amount of line-of-sight dust extinction towards a QSO and the radio detection fraction, that is not driven by radio-loud systems, redshift and/or luminosity effects. This demonstrates an intrinsic connection between dust reddening and the production of radio emission in QSOs, whereby the radio emission is most likely due to low-powered jets or winds/outflows causing shocks in a dusty environment. On the basis of this evidence, we suggest that red QSOs may represent a transitional 'blow-out' phase in the evolution of QSOs, where winds and outflows evacuate the dust and gas to reveal an unobscured blue QSO.
Published: 2023

168. Detecting and Characterizing Mg ii Absorption in DESI Survey Validation Quasar Spectra

Author: Napolitano, Lucas, Pandey, Agnesh, Myers, Adam D, Lan, Ting-Wen, Anand, Abhijeet, Aguilar, Jessica, Ahlen, Steven, Alexander, David M, Brooks, David, Canning, Rebecca, Circosta, Chiara, De La Macorra, Axel, Doel, Peter, Eftekharzadeh, Sarah, Fawcett, Victoria A, Font-Ribera, Andreu, Garcia-Bellido, Juan, Gontcho, Satya Gontcho A, Le Guillou, L, Guy, Julien, Honscheid, Klaus, Juneau, Stephanie, Kisner, T, Landriau, Martin, Meisner, Aaron M, Miquel, Ramon, Moustakas, J, Percival, Will J, Prochaska, J Xavier, Schubnell, Michael, Tarlé, Gregory, Weaver, BA, Weiner, Benjamin, Zhou, Zhimin, Zou, Hu, and Zou, Siwei
Subjects: Astronomical Sciences, Physical Sciences, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics
Abstract: We present findings of the detection of Magnesium II (Mg ii, λ = 2796, 2803 Å) absorbers from the early data release of the Dark Energy Spectroscopic Instrument (DESI). DESI is projected to obtain spectroscopy of approximately 3 million quasars (QSOs), of which over 99% are anticipated to be at redshifts greater than z > 0.3, such that DESI would be able to observe an associated or intervening Mg ii absorber illuminated by the background QSO. We have developed an autonomous supplementary spectral pipeline that detects these systems through an initial line-fitting process and then confirms the line properties using a Markov Chain Monte Carlo sampler. Based upon a visual inspection of the resulting systems, we estimate that this sample has a purity greater than 99%. We have also investigated the completeness of our sample in regard to both the signal-to-noise properties of the input spectra and the rest-frame equivalent width (W 0) of the absorber systems. From a parent catalog containing 83,207 quasars, we detect a total of 23,921 Mg ii absorption systems following a series of quality cuts. Extrapolating from this occurrence rate of 28.8% implies a catalog at the completion of the five-year DESI survey that will contain over eight hundred thousand Mg ii absorbers. The cataloging of these systems will enable significant further research because they carry information regarding circumgalactic medium environments, the distribution of intervening galaxies, and the growth of metallicity across the redshift range 0.3 ≤ z < 2.5.
Published: 2023

169. Semiautomatic Quantitative Assessment of DIEP Flap Volume and Thickness for Breast Reconstruction using CTA Data and Implications in Postoperative Complications

Author: María A. Cerón Hurtado, Sergi Barrantes, Antonio Sánchez Egea, Farners Armengol Siñol, Hernán González Rojas, Anna Padullés-Escarré, Jose A Jerez-Gonzalez, Anna López Ojeda, and Joan Fontdevila Font
Subjects: DIEP flap, Image processing algorithm, Computed tomography angiography, Perforator flap planning, 3D planning, Surgery, RD1-811
Abstract: Summary: Accurately assessing flap volume and thickness is a crucial aspect of breast reconstruction using the deep inferior epigastric perforator (DIEP) flap, especially in challenging cases such as thin or large-breasted women or bilateral reconstruction. To address this, we present an innovative image processing tool utilizing computed tomography angiography (CTA) to measure DIEP flap volume and thickness. Our approach incorporates an elliptical equation validated on DIEP reconstruction patients. Preoperative abdominal CTA images were obtained from 70 patients who underwent DIEP flap breast reconstruction at Hospital Universitari de Bellvitge from 2017 to 2021. The image processing tool was employed for preoperative quantification, utilizing elliptical approximations, to determine the volume to be harvested and assess the central thickness of the flap. Subsequently, a non-parametric statistical retrospective analysis was conducted to examine these parameters in relation to immediate complications. The mean maximum recruitable volume (MRV) was 1017.15 ± 325.51 cm³, with a mean thickness of 3.65 ± 1.14 cm. No significant correlation was found between postoperative complications and MRV or thickness values. The processing tool offers a reliable solution for accurately measuring the volume and thickness of the DIEP flap from CTA images, aiding surgeons in breast reconstruction decision-making. This innovative approach enhances surgical planning by addressing quantitative values of thickness and volume of the DIEP flap, which is critical for accurate flap assessment.
Published: 2024
Full Text: View/download PDF

170. Towards clinical translation of urinary vitronectin for non-invasive detection and monitoring of renal fibrosis in kidney transplant patients

Author: Clos-Sansalvador, Marta, Taco, Omar, Rodríguez-Martínez, Paula, Garcia, Sergio G., Font-Morón, Miriam, Bover, Jordi, Vila-Santandreu, Anna, Franquesa, Marcella, Juega, Javier, and Borràs, Francesc E.
Published: 2024
Full Text: View/download PDF

171. Author Correction: Location and function of TDP-43 in platelets, alterations in neurodegenerative diseases and arising considerations for current plasma biobank protocols

Author: Luthi-Carter, Ruth, Cappelli, Sara, Le Roux-Bourdieu, Morgan, Tentillier, Noemie, Quinn, James P., Petrozziello, Tiziana, Gopalakrishnan, Lathika, Sethi, Purva, Choudhary, Himanshi, Bartolini, Giorgia, Gebara, Elias, Stuani, Cristiana, Font, Laure, An, Jiyan, Ortega, Vanessa, Sage, Jessica, Kosa, Edina, Trombetta, Bianca A., Simeone, Roberto, Seredenina, Tamara, Afroz, Tariq, Berry, James D., Arnold, Steven E., Carlyle, Becky C., Adolfsson, Oskar, Sadri-Vakili, Ghazaleh, Buratti, Emanuele, Bowser, Robert, and Agbas, Abdulbaki
Published: 2024
Full Text: View/download PDF

172. Immersive virtual reality for learning exoskeleton-like virtual walking: a feasibility study

Author: Rodríguez-Fernández, Antonio, den Berg, Alex van, Cucinella, Salvatore Luca, Lobo-Prat, Joan, Font-Llagunes, Josep M., and Marchal-Crespo, Laura
Published: 2024
Full Text: View/download PDF

173. Correction to: Evolving Real-time Stereo Odometry for AUV Navigation in Challenging Marine Environments

Author: Nordfeldt-Fiol, Bo Miquel, Bonin-Font, Francisco, and Oliver, Gabriel
Published: 2024
Full Text: View/download PDF

174. Heterochromatin dynamics during the initial stages of sexual development in Plasmodium falciparum

Author: Nhim, Sandra, Tintó-Font, Elisabet, Casas-Vila, Núria, Michel-Todó, Lucas, and Cortés, Alfred
Published: 2024
Full Text: View/download PDF

175. Aerobic exercise and cognitive function in chronic severe traumatic brain injury survivors: a within-subject A-B-A intervention study

Author: López, Lidia Pérez, Coll-Andreu, Margalida, Torras-Garcia, Meritxell, Font-Farré, Manel, Oviedo, Guillermo R., Capdevila, Lluis, Guerra-Balic, Myriam, Portell-Cortés, Isabel, Costa-Miserachs, David, and Morris, Timothy P.
Published: 2024
Full Text: View/download PDF

176. Location and function of TDP-43 in platelets, alterations in neurodegenerative diseases and arising considerations for current plasma biobank protocols

Author: Luthi-Carter, Ruth, Cappelli, Sara, Le Roux-Bourdieu, Morgan, Tentillier, Noemie, Quinn, James P., Petrozziello, Tiziana, Gopalakrishnan, Lathika, Sethi, Purva, Choudhary, Himanshi, Bartolini, Giorgia, Gebara, Elias, Stuani, Cristiana, Font, Laure, An, Jiyan, Ortega, Vanessa, Sage, Jessica, Kosa, Edina, Trombetta, Bianca A., Simeone, Roberto, Seredenina, Tamara, Afroz, Tariq, Berry, James D., Arnold, Steven E., Carlyle, Becky C., Adolfsson, Oskar, Sadri-Vakili, Ghazaleh, Buratti, Emanuele, Bowser, Robert, and Agbas, Abdulbaki
Published: 2024
Full Text: View/download PDF

177. A summer course in cancer for high school students-an update on lessons taught and lessons learned

Author: Solone, Xzaviar K., Chitre, Siddhi, Font, Laura Falceto, Pereira, Kimberly N. Espinoza, Stofer, Kathryn, and Siemann, Dietmar W.
Published: 2024
Full Text: View/download PDF

178. Sewage sludge fertilization affects microbial community structure and its resistome in agricultural soils

Author: Serwecińska, Liliana, Font-Nájera, Arnoldo, Strapagiel, Dominik, Lach, Jakub, Tołoczko, Wojciech, Bołdak, Małgorzata, and Urbaniak, Magdalena
Published: 2024
Full Text: View/download PDF

179. A new modular neuroprosthesis suitable for hybrid FES-robot applications and tailored assistance

Author: Gil-Castillo, Javier, Herrera-Valenzuela, Diana, Torricelli, Diego, Gil-Agudo, Ángel, Opisso, Eloy, Vidal, Joan, Font-Llagunes, Josep M., del-Ama, Antonio J., and Moreno, Juan C.
Published: 2024
Full Text: View/download PDF

180. Language and the use of law are predictive of judge gender and seniority

Author: Font-Pomarol, Lluc, Piga, Angelo, Nasarre-Aznar, Sergio, Sales-Pardo, Marta, and Guimerà, Roger
Published: 2024
Full Text: View/download PDF

181. Endogenous LXR signaling controls pulmonary surfactant homeostasis and prevents lung inflammation

Author: Hernández-Hernández, Irene, De La Rosa, Juan V., Martín-Rodríguez, Patricia, Díaz-Sarmiento, Mercedes, Recio, Carlota, Guerra, Borja, Fernández-Pérez, Leandro, León, Theresa E., Torres, Rosa, Font-Díaz, Joan, Roig, Angela, de Mora, Fernando, Boscá, Lisardo, Díaz, Mario, Valledor, Annabel F., Castrillo, Antonio, and Tabraue, Carlos
Published: 2024
Full Text: View/download PDF

182. Discovery of active mouse, plant and fungal cytochrome P450s in endogenous proteomes and upon expression in planta

Author: Font-Farre, Maria, Brown, Daniel, Toth, Reka, Mahadevan, Chidambareswaren, Brazier-Hicks, Melissa, Morimoto, Kyoko, Kaschani, Farnusch, Sinclair, John, Dale, Richard, Hall, Samantha, Morris, Melloney, Kaiser, Markus, Wright, Aaron T., Burton, Jonathan, and van der Hoorn, Renier A. L.
Published: 2024
Full Text: View/download PDF

183. Microenvironmental reorganization in brain tumors following radiotherapy and recurrence revealed by hyperplexed immunofluorescence imaging

Author: Watson, Spencer S., Duc, Benoit, Kang, Ziqi, de Tonnac, Axel, Eling, Nils, Font, Laure, Whitmarsh, Tristan, Massara, Matteo, Bodenmiller, Bernd, Hausser, Jean, and Joyce, Johanna A.
Published: 2024
Full Text: View/download PDF

184. Soluble CD27 is an intrathecal biomarker of T-cell-mediated lesion activity in multiple sclerosis

Author: Cencioni, Maria T., Magliozzi, Roberta, Palmisano, Ilaria, Suwan, Keittisak, Mensi, Antonella, Fuentes-Font, Laura, Villar, Luisa M., Fernández-Velasco, José I., Migallón, Noelia Villarrubia, Costa-Frossard, Lucienne, Monreal, Enric, Ali, Rehiana, Romozzi, Marina, Mazarakis, Nicholas, Reynolds, Richard, Nicholas, Richard, and Muraro, Paolo A.
Published: 2024
Full Text: View/download PDF

185. A progesterone derivative linked to a stable phospholipid activates breast cancer cell response without leaving the cell membrane

Author: Font-Mateu, Jofre, Sanllehí, Pol, Sot, Jesús, Abad, Beatriz, Mateos, Nicolas, Torreno-Pina, Juan Andres, Ferrari, Roberto, Wright, Roni H. G., Garcia-Parajo, Maria F., Joglar, Jesús, Goñi, Félix M., and Beato, Miguel
Published: 2024
Full Text: View/download PDF

186. Correction: ERK mediates interferon gamma-induced melanoma cell death

Author: Champhekar, Ameya, Heymans, Rachel, Saco, Justin, Font, Guillem Turon, Gonzalez, Cynthia, Gao, Anne, Pham, John, Lee, June, Maryoung, Ryan, Medina, Egmidio, Campbell, Katie M., Karin, Daniel, Austin, David, Damioseaux, Robert, and Ribas, Antoni
Published: 2024
Full Text: View/download PDF

187. Governance, Mobility, and Pastureland Ecology. An Eco-Anthropological Study of Three Pastoral Commons in Northeastern Andalusia

Author: Godoy-Sepúlveda, Francisco, Sanosa-Cols, Pau, Parra, Santiago A., Peña-Enguix, Adrià, Pérez-Luque, Antonio J., Ramos-Font, María Eugenia, Robles, Ana Belén, Tognetti, Mauro J., González-Robles, Ana, Ravera, Federica, Ventura, Montserrat, and Dominguez, Pablo
Published: 2024
Full Text: View/download PDF

188. Understanding and Promoting Child Wellbeing After Child Welfare System Involvement: Progress Made and Challenges Ahead

Author: Font, Sarah A. and Fluke, John D.
Published: 2024
Full Text: View/download PDF

189. A neural network emulator for the Lyman-$\alpha$ 1D flux power spectrum

Author: Cabayol-Garcia, Laura, Chaves-Montero, Jonás, Font-Ribera, Andreu, and Pedersen, Christian
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: The Lyman-$\alpha$ forest offers a unique avenue for studying the distribution of matter in the high redshift universe and extracting precise constraints on the nature of dark matter, neutrino masses, and other $\Lambda$CDM extensions. However, interpreting this observable requires accurate modelling of the thermal and ionisation state of the intergalactic medium, and therefore resorting to computationally expensive hydrodynamical simulations. In this work, we build a neural network that serves as a surrogate model for rapid predictions of the one-dimensional \lya flux power spectrum ($P_{\rm 1D}$), thereby making Bayesian inference feasible for this observable. Our emulation technique is based on modelling $P_{\rm 1D}$ as a function of the slope and amplitude of the linear matter power spectrum rather than as a function of cosmological parameters. We show that our emulator achieves sub-percent precision across the full range of scales ($k_{\parallel }=0.1$ to 4Mpc$^{-1}$) and redshifts ($z=2$ to 4.5) considered, and also for three $\Lambda$CDM extensions not included in the training set: massive neutrinos, running of the spectral index, and curvature. Furthermore, we show that it performs at the 1% level for ionisation and thermal histories not present in the training set and performs at the percent level when emulating down to $k_{\parallel}$=8Mpc$^{-1}$. These results affirm the efficacy of our emulation strategy in providing accurate predictions even for cosmologies and reionisation histories that were not explicitly incorporated during the training phase, and we expect it to play a critical role in the cosmological analysis of the DESI survey., Comment: 15 pages, 17 figures
Published: 2023
Full Text: View/download PDF

190. An Optically Targeted Search for Gravitational Waves emitted by Core-Collapse Supernovae during the Third Observing Run of Advanced LIGO and Advanced Virgo

Author: Szczepańczyk, Marek J., Zheng, Yanyan, Antelis, Javier M., Benjamin, Michael, Bizouard, Marie-Anne, Casallas-Lagos, Alejandro, Cerdá-Durán, Pablo, Davis, Derek, Gondek-Rosińska, Dorota, Klimenko, Sergey, Moreno, Claudia, Obergaulinger, Martin, Powell, Jade, Ramirez, Dymetris, Ratto, Brad, Richarson, Colter, Rijal, Abhinav, Stuver, Amber L., Szewczyk, Paweł, Vedovato, Gabriele, Zanolin, Michele, Bartos, Imre, Bhaumik, Shubhagata, Bulik, Tomasz, Drago, Marco, Font, José A., De Colle, Fabio, García-Bellido, Juan, Gayathri, V., Hughey, Brennan, Mitselmakher, Guenakh, Mishra, Tanmaya, Mukherjee, Soma, Nguyen, Quynh Lan, Chan, Man Leong, Di Palma, Irene, Piotrzkowski, Brandon J., and Singh, Neha
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: We present the results from a search for gravitational-wave transients associated with core-collapse supernovae observed optically within 30 Mpc during the third observing run of Advanced LIGO and Advanced Virgo. No gravitational wave associated with a core-collapse supernova has been identified. We then report the detection efficiency for a variety of possible gravitational-wave emissions. For neutrino-driven explosions, the distance at which we reach 50% detection efficiency is up to 8.9 kpc, while more energetic magnetorotationally-driven explosions are detectable at larger distances. The distance reaches for selected models of the black hole formation, and quantum chromodynamics phase transition are also provided. We then constrain the core-collapse supernova engine across a wide frequency range from 50 Hz to 2 kHz. The upper limits on gravitational-wave energy and luminosity emission are at low frequencies down to $10^{-4}\,M_\odot c^2$ and $6 \times 10^{-4}\,M_\odot c^2$/s, respectively. The upper limits on the proto-neutron star ellipticity are down to 3 at high frequencies. Finally, by combining the results obtained with the data from the first and second observing runs of LIGO and Virgo, we improve the constraints of the parameter spaces of the extreme emission models. Specifically, the proto-neutron star ellipticities for the long-lasting bar mode model are down to 1 for long emission (1 s) at high frequency., Comment: 20 pages, 11 figures; https://dcc.ligo.org/LIGO-P2200361
Published: 2023

191. Performance of the Quasar Spectral Templates for the Dark Energy Spectroscopic Instrument

Author: Brodzeller, Allyson, Dawson, Kyle, Bailey, Stephen, Yu, Jiaxi, Ross, A. J., Bault, A., Filbert, S., Aguilar, J., Ahlen, S., Alexander, David M., Armengaud, E., Berti, A., Brooks, D., Chaussidon, E., de la Macorra, A., Doel, P., Fanning, K., Fawcett, V. A., Font-Ribera, A., Gontcho, S. Gontcho A, Guy, J., Honscheid, K., Juneau, S., Kehoe, R., Kisner, T., Kremin, Anthony, Lan, Ting-Wen, Landriau, M., Levi, Michael E., Magneville, C., Martini, Paul, Meisner, Aaron M., Miquel, R., Moustakas, J., Palanque-Delabrouille, N., Percival, W. J., Prada, F., Ravoux, C., Rossi, Graziano, Saulder, C., Siudek, M., Tarlé, Gregory, Weaver, B. A., Youles, S., Zheng, Zheng, Zhou, Rongpu, and Zhou, Zhimin
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Millions of quasar spectra will be collected by the Dark Energy Spectroscopic Instrument (DESI), leading to a four-fold increase in the number of known quasars. High accuracy quasar classification is essential to tighten constraints on cosmological parameters measured at the highest redshifts DESI observes ($z>2.0$). We present the spectral templates for identification and redshift estimation of quasars in the DESI Year 1 data release. The quasar templates are comprised of two quasar eigenspectra sets, trained on spectra from the Sloan Digital Sky Survey. The sets are specialized to reconstruct quasar spectral variation observed over separate yet overlapping redshift ranges and, together, are capable of identifying DESI quasars from $0.05 < z <7.0$. The new quasar templates show significant improvement over the previous DESI quasar templates regarding catastrophic failure rates, redshift precision and accuracy, quasar completeness, and the contamination fraction in the final quasar sample., Comment: to be published in Astronomical Journal; 21 pages, 8 figures
Published: 2023
Full Text: View/download PDF

192. SP(k) -- A hydrodynamical simulation-based model for the impact of baryon physics on the non-linear matter power spectrum

Author: Salcido, Jaime, McCarthy, Ian G., Kwan, Juliana, Upadhye, Amol, and Font, Andreea S.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract: Upcoming large-scale structure surveys will measure the matter power spectrum to approximately percent level accuracy with the aim of searching for evidence for new physics beyond the standard model of cosmology. In order to avoid biasing our conclusions, the theoretical predictions need to be at least as accurate as the measurements for a given choice of cosmological parameters. However, recent theoretical work has shown that complex physical processes associated with galaxy formation (particularly energetic feedback processes associated with stars and especially supermassive black holes) can alter the predictions by many times larger than the required accuracy. Here we present $\texttt{SP(k)}$, a model for the effects of baryon physics on the non-linear matter power spectrum based on a new large suite of hydrodynamical simulations. Specifically, the ANTILLES suite consists of 400 simulations spanning a very wide range of the "feedback landscape" and show that the effects of baryons on the matter power spectrum can be understood at approaching the percent level in terms of the mean baryon fraction of haloes, at scales of up to $k \lesssim 10 \, h \, $Mpc$^{-1}$ and redshifts up to $z=3$. For the range of scales and redshifts that will be probed by forthcoming cosmic shear measurements, most of the effects are driven by galaxy group-mass haloes ($M \sim 10^{13-14}$ M$_\odot$). We present a simple Python implementation of our model, available at $\href{https://github.com/jemme07/pyspk}{\mathrm{https{:}//github.com/jemme07/pyspk}}$, which can be used to incorporate baryon effects in standard gravity-only predictions, allowing for marginalisation over baryon physics within cosmological pipelines., Comment: Refereed version accepted for publication in Monthly Notices of the Royal Astronomical Society (MNRAS). 16 pages, 11 figures
Published: 2023
Full Text: View/download PDF

193. Planting a Lyman alpha forest on AbacusSummit

Author: Hadzhiyska, Boryana, Font-Ribera, Andreu, Cuceu, Andrei, Chabanier, Solène, Aguilar, Jessica Nicole, Brooks, David, de la Macorra, Axel, Doel, Peter, Eisenstein, Daniel J., Forero-Romero, Jaime E., Gontcho, Satya Gontcho A, Honscheid, Klaus, Kehoe, Robert, Landriau, Martin, Manera, Marc, Miquel, Ramon, Nie, Jundan, Percival, Will, Rossi, Graziano, Schubnell, Michael, Tarlé, Gregory, and Zhou, Zhimin
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The full-shape correlations of the Lyman alpha (Ly$\alpha$) forest contain a wealth of cosmological information through the Alcock-Paczy\'{n}ski effect. However, these measurements are challenging to model without robustly testing and verifying the theoretical framework used for analyzing them. Here, we leverage the accuracy and volume of the $N$-body simulation suite \textsc{AbacusSummit} to generate high-resolution Ly$\alpha$ skewers and quasi-stellar object (QSO) catalogs. One of the main goals of our mocks is to aid in the full-shape Ly$\alpha$ analysis planned by the Dark Energy Spectroscopic Instrument (DESI) team. We provide optical depth skewers for six of the fiducial cosmology base-resolution simulations ($L_{\rm box} = 2\,h^{-1}{\rm Gpc}$, $N = 6912^3$) at $z = 2.5$. We adopt a simple recipe based on the Fluctuating Gunn-Peterson Approximation (FGPA) for constructing these skewers from the matter density in an $N$-body simulation and calibrate it against the 1D and 3D Ly$\alpha$ power spectra extracted from the hydrodynamical simulation IllustrisTNG (TNG; $L_{\rm box} = 205\,h^{-1}{\rm Mpc}$, $N = 2500^3$). As an important application, we study the non-linear broadening of the baryon acoustic oscillation (BAO) peak and show the cross-correlation between DESI-like QSOs and our Ly$\alpha$ forest skewers. We find differences on small scales between the Kaiser approximation prediction and our mock measurements of the Ly$\alpha$$\times$QSO cross-correlation, which would be important to account for in upcoming analyses. The \textsc{AbacusSummit} Ly$\alpha$ forest mocks open up the possibility for improved modelling of cross correlations between Ly$\alpha$ and cosmic microwave background (CMB) lensing and Ly$\alpha$ and QSOs, and for forecasts of the 3-point Ly$\alpha$ correlation function. Our catalogues and skewers are publicly available on Globus., Comment: 17 pages, 8 figures, Globus link: https://app.globus.org/file-manager?origin_id=9ce29982-eed1-11ed-9bb4-c9bb788c490e&path=%2F
Published: 2023
Full Text: View/download PDF

194. Gradient-Annihilated PINNs for Solving Riemann Problems: Application to Relativistic Hydrodynamics

Author: Ferrer-Sánchez, Antonio, Martín-Guerrero, José D., de Austri, Roberto Ruiz, Torres-Forné, Alejandro, and Font, José A.
Subjects: Physics - Computational Physics, Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: We present a novel methodology based on Physics-Informed Neural Networks (PINNs) for solving systems of partial differential equations admitting discontinuous solutions. Our method, called Gradient-Annihilated PINNs (GA-PINNs), introduces a modified loss function that requires the model to partially ignore high-gradients in the physical variables, achieved by introducing a suitable weighting function. The method relies on a set of hyperparameters that control how gradients are treated in the physical loss and how the activation functions of the neural model are dynamically accounted for. The performance of our GA-PINN model is demonstrated by solving Riemann problems in special relativistic hydrodynamics, extending earlier studies with PINNs in the context of the classical Euler equations. The solutions obtained with our GA-PINN model correctly describe the propagation speeds of discontinuities and sharply capture the associated jumps. We use the relative $l^{2}$ error to compare our results with the exact solution of special relativistic Riemann problems, used as the reference ``ground truth'', and with the error obtained with a second-order, central, shock-capturing scheme. In all problems investigated, the accuracy reached by our GA-PINN model is comparable to that obtained with a shock-capturing scheme and significantly higher than that achieved by a baseline PINN algorithm. An additional benefit worth stressing is that our PINN-based approach sidesteps the costly recovery of the primitive variables from the state vector of conserved ones, a well-known drawback of grid-based solutions of the relativistic hydrodynamics equations. Due to its inherent generality and its ability to handle steep gradients, the GA-PINN method discussed could be a valuable tool to model relativistic flows in astrophysics and particle physics, characterized by the prevalence of discontinuous solutions., Comment: 25 pages, 16 figures
Published: 2023

195. Constraining primordial non-Gaussianity from DESI quasar targets and Planck CMB lensing

Author: Krolewski, Alex, Percival, Will J., Ferraro, Simone, Chaussidon, Edmond, Rezaie, Mehdi, Aguilar, Jessica Nicole, Ahlen, Steven, Brooks, David, Dawson, Kyle, de la Macorra, Axel, Doel, Peter, Fanning, Kevin, Font-Ribera, Andreu, Gontcho, Satya Gontcho A, Guy, Julien, Honscheid, Klaus, Kehoe, Robert, Kisner, Theodore, Kremin, Anthony, Landriau, Martin, Levi, Michael E., Martini, Paul, Meisner, Aaron M., Miquel, Ramon, Nie, Jundan, Poppett, Claire, Ross, Ashley J., Rossi, Graziano, Schubnell, Michael, Seo, Hee-Jong, Tarle, Gregory, Vargas-Magana, Mariana, Weaver, Benjamin Alan, Yeche, Christophe, Zhou, Rongpu, and Zhou, Zhimin
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We detect the cross-correlation between 2.7 million DESI quasar targets across 14,700 deg$^2$ (180 quasars deg$^{-2}$) and Planck 2018 CMB lensing at $\sim$30$\sigma$. We use the cross-correlation on very large scales to constrain local primordial non-Gaussianity via the scale dependence of quasar bias. The DESI quasar targets lie at an effective redshift of 1.51 and are separated into four imaging regions of varying depth and image quality. We select quasar targets from Legacy Survey DR9 imaging, apply additional flux and photometric redshift cuts to improve the purity and reduce the fraction of unclassified redshifts, and use early DESI spectroscopy of 194,000 quasar targets to determine their redshift distribution and stellar contamination fraction (2.6%). Due to significant excess large-scale power in the quasar autocorrelation, we apply weights to mitigate contamination from imaging systematics such as depth, extinction, and stellar density. We use realistic contaminated mocks to determine the greatest number of systematic modes that we can fit, before we are biased by overfitting and spuriously remove real power. We find that linear regression with one to seven imaging templates removed per region accurately recovers the input cross-power, $f_{\textrm{NL}}$ and linear bias. As in previous analyses, our $f_{\textrm{NL}}$ constraint depends on the linear primordial non-Gaussianity bias parameter, $b_{\phi} = 2(b - p)\delta_c$ assuming universality of the halo mass function. We measure $f_{\textrm{NL}} = -26^{+45}_{-40}$ with $p=1.6$ $(f_{\textrm{NL}} = -18^{+29}_{-27}$ with $p=1.0$), and find that this result is robust under several systematics tests. Future spectroscopic quasar cross-correlations with Planck lensing lensing can tighten the $f_{\textrm{NL}}$ constraints by a factor of 2 if they can remove the excess power on large scales in the quasar auto power spectrum., Comment: 57 pages, 25 figures, updated to match accepted version
Published: 2023
Full Text: View/download PDF

196. Birth of baby universes from gravitational collapse in a modified-gravity scenario

Author: Masó-Ferrando, Andreu, Sanchis-Gual, Nicolas, Font, José A., and Olmo, Gonzalo J.
Subjects: General Relativity and Quantum Cosmology
Abstract: We consider equilibrium models of spherical boson stars in Palatini $f(\mathcal{R})=\mathcal{R}+\xi \mathcal{R}^2$ gravity and study their collapse when perturbed. The Einstein-Klein-Gordon system is solved using a recently established correspondence in an Einstein frame representation. We find that, in that frame, the endpoint is a nonrotating black hole surrounded by a quasi-stationary cloud of scalar field. However, the dynamics in the $f(\mathcal{R})$ frame is dramatically different. The innermost region of the collapsing object exhibits the formation of a finite-size, exponentially-expanding $\textit{ baby universe}$ connected with the outer (parent) universe via a minimal area surface (a throat or umbilical cord). Our simulations indicate that this surface is at all times hidden inside a horizon, causally disconnecting the baby universe from observers above the horizon. The implications of our findings in other areas of gravitational physics are also discussed.
Published: 2023
Full Text: View/download PDF

197. Search for gravitational-lensing signatures in the full third observing run of the LIGO-Virgo network

Author: The LIGO Scientific Collaboration, the Virgo Collaboration, the KAGRA Collaboration, Abbott, R., Abe, H., Acernese, F., Ackley, K., Adhicary, S., Adhikari, N., Adhikari, R. X., Adkins, V. K., Adya, V. B., Affeldt, C., Agarwal, D., Agathos, M., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Akutsu, T., Albanesi, S., Alfaidi, R. A., Alléné, C., Allocca, A., Altin, P. A., Amato, A., Anand, S., Ananyeva, A., Anderson, S. B., Anderson, W. G., Ando, M., Andrade, T., Andres, N., Andrés-Carcasona, M., Andrić, T., Ansoldi, S., Antelis, J. M., Antier, S., Apostolatos, T., Appavuravther, E. Z., Appert, S., Apple, S. K., Arai, K., Araya, A., Araya, M. C., Areeda, J. S., Arène, M., Aritomi, N., Arnaud, N., Arogeti, M., Aronson, S. M., Asada, H., Ashton, G., Aso, Y., Assiduo, M., Melo, S. Assis de Souza, Aston, S. M., Astone, P., Aubin, F., AultONeal, K., Babak, S., Badaracco, F., Badger, C., Bae, S., Bae, Y., Bagnasco, S., Bai, Y., Baier, J. G., Baird, J., Bajpai, R., Baka, T., Ball, M., Ballardin, G., Ballmer, S. W., Baltus, G., Banagiri, S., Banerjee, B., Bankar, D., Barayoga, J. C., Barish, B. C., Barker, D., Barneo, P., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Barton, M. A., Bartos, I., Basak, S., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Bedakihale, V. M., Beirnaert, F., Bejger, M., Belahcene, I., Bell, A. S., Benedetto, V., Beniwal, D., Benoit, W., Bentley, J. D., BenYaala, M., Bera, S., Berbel, M., Bergamin, F., Berger, B. K., Bernuzzi, S., Beroiz, M., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Beveridge, D., Bhandare, R., Bhandari, A. V., Bhardwaj, U., Bhatt, R., Bhattacharjee, D., Bhaumik, S., Bianchi, A., Bilenko, I. A., Bilicki, M., Billingsley, G., Bini, S., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Biswas, B., Bitossi, M., Bizouard, M. -A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bobba, F., Bode, N., Boër, M., Bogaert, G., Boldrini, M., Bolingbroke, G. N., Bonavena, L. D., Bondarescu, R., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Bork, R., Boschi, V., Bose, N., Bose, S., Bossilkov, V., Boudart, V., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branch, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., Bruno, G., Bruntz, R., Bryant, J., Bucci, F., Buchanan, J., Bulik, T., Bulten, H. J., Buonanno, A., Burtnyk, K., Buscicchio, R., Buskulic, D., Buy, C., Byer, R. L., Davies, G. S. Cabourn, Cabras, G., Cabrita, R., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderón, Callaghan, J. D., Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Caneva, G., Cannavacciuolo, M., Cannon, K. C., Cao, H., Cao, Z., Capistran, L. A., Capocasa, E., Capote, E., Carapella, G., Carbognani, F., Carlassara, M., Carlin, J. B., Carpinelli, M., Carrillo, G., Carter, J. J., Carullo, G., Diaz, J. Casanueva, Casentini, C., Castaldi, G., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cerdá-Durán, P., Cesarini, E., Chaibi, W., Chakalis, W., Subrahmanya, S. Chalathadka, Champion, E., Chan, C. -H., Chan, C., Chan, C. L., Chan, K., Chan, M., Chandra, K., Chang, I. P., Chang, W., Chanial, P., Chao, S., Chapman-Bird, C., Charlton, P., Chassande-Mottin, E., Chatterjee, C., Chatterjee, Debarati, Chatterjee, Deep, Chaturvedi, M., Chaty, S., Chatziioannou, K., Chen, C., Chen, D., Chen, H. Y., Chen, J., Chen, K., Chen, X., Chen, Y. -B., Chen, Y. -R., Chen, Y., Cheng, H., Chessa, P., Cheung, H. Y., Chia, H. Y., Chiadini, F., Chiang, C-Y., Chiarini, G., Chierici, R., Chincarini, A., Chiofalo, M. L., Chiummo, A., Choudhary, R. K., Choudhary, S., Christensen, N., Chu, Q., Chu, Y-K., Chua, S. S. Y., Chung, K. W., Ciani, G., Ciecielag, P., Cieślar, M., Cifaldi, M., Ciobanu, A. A., Ciolfi, R., Clara, F., Clark, J. A., Clarke, T. A., Clearwater, P., Clesse, S., Cleva, F., Coccia, E., Codazzo, E., Cohadon, P. -F., Cohen, D. E., Colleoni, M., Collette, C. G., Colombo, A., Colpi, M., Compton, C. M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corezzi, S., Cornish, N. J., Corsi, A., Cortese, S., Coschizza, A. C., Cotesta, R., Cottingham, R., Coughlin, M. W., Coulon, J. -P., Countryman, S. T., Cousins, B., Couvares, P., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Creighton, T. D., Criswell, A. W., Croquette, M., Crowder, S. G., Cudell, J. R., Cullen, T. J., Cumming, A., Cummings, R., Cuoco, E., Curyło, M., Dabadie, P., Canton, T. Dal, Dall'Osso, S., Dálya, G., Dana, A., D'Angelo, B., Danilishin, S., D'Antonio, S., Danzmann, K., Darsow-Fromm, C., Dasgupta, A., Datrier, L. E. H., Datta, Sayak, Datta, Sayantani, Dattilo, V., Dave, I., Davier, M., Davis, D., Davis, M. C., Daw, E. J., Dax, M., DeBra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deléglise, S., Del Favero, V., De Lillo, F., De Lillo, N., Dell'Aquila, D., Del Pozzo, W., De Matteis, F., D'Emilio, V., Demos, N., Dent, T., Depasse, A., De Pietri, R., De Rosa, R., De Rossi, C., DeSalvo, R., De Simone, R., Dhurandhar, S., Diab, R., Díaz, M. C., Didio, N. A., Dietrich, T., Di Fiore, L., Di Fronzo, C., Di Giorgio, C., Di Giovanni, F., Di Giovanni, M., Di Girolamo, T., Diksha, D., Di Lieto, A., Di Michele, A., Di Pace, S., Di Palma, I., Di Renzo, F., Divakarla, A. K., Dmitriev, A., Doctor, Z., Doleva, P. P., Donahue, L., D'Onofrio, L., Donovan, F., Dooley, K. L., Dooney, T., Doravari, S., Dorosh, O., Drago, M., Driggers, J. C., Drori, Y., Ducoin, J. -G., Dunn, L., Dupletsa, U., Durante, O., D'Urso, D., Duverne, P. -A., Dwyer, S. E., Eassa, C., Easter, P. J., Ebersold, M., Eckhardt, T., Eddolls, G., Edelman, B., Edo, T. B., Edy, O., Effler, A., Eguchi, S., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Ejlli, A., Engelby, E., Enomoto, Y., Errico, L., Essick, R. C., Estellés, H., Estevez, D., Etzel, T., Evans, M., Evans, T. M., Evstafyeva, T., Ewing, B. E., Ezquiaga, J. M., Fabrizi, F., Faedi, F., Fafone, V., Fair, H., Fairhurst, S., Fan, P. C., Farah, A. M., Farr, B., Farr, W. M., Favaro, G., Favata, M., Fays, M., Fazio, M., Feicht, J., Fejer, M. M., Fenyvesi, E., Ferguson, D. L., Fernandez-Galiana, A., Ferrante, I., Ferreira, T. A., Fidecaro, F., Figura, P., Fiori, A., Fiori, I., Fishbach, M., Fisher, R. P., Fittipaldi, R., Fiumara, V., Flaminio, R., Floden, E., Fong, H. K., Font, J. A., Fornal, B., Forsyth, P. W. F., Franke, A., Frasca, S., Frasconi, F., Freed, J. P., Frei, Z., Freise, A., Freitas, O., Frey, R., Fritschel, P., Frolov, V. V., Fronzé, G. G., Fujii, Y., Fujikawa, Y., Fujimoto, Y., Fulda, P., Fyffe, M., Gabbard, H. A., Gabella, W. E., Gadre, B. U., Gair, J. R., Gais, J., Galaudage, S., Gamba, R., Ganapathy, D., Ganguly, A., Gao, D. -F., Gao, D., Gaonkar, S. G., Garaventa, B., García-Núñez, C., García-Quirós, C., Gardner, K. A., Gargiulo, J., Garufi, F., Gasbarra, C., Gateley, B., Gayathri, V., Ge, G. -G., Gemme, G., Gennai, A., George, J., Gerberding, O., Gergely, L., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, Shaon, Ghosh, Shrobana, Ghosh, Tathagata, Giacoppo, L., Giaime, J. A., Giardina, K. D., Gibson, D. R., Gier, C., Giri, P., Gissi, F., Gkaitatzis, S., Glanzer, J., Gleckl, A. E., Godoy, F. G., Godwin, P., Goetz, E., Goetz, R., Golomb, J., Goncharov, B., González, G., Gosselin, M., Gouaty, R., Gould, D. W., Goyal, S., Grace, B., Grado, A., Graham, V., Granata, M., Granata, V., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, A. M., Gretarsson, E. M., Griffith, D., Griffiths, W. L., Griggs, H. L., Grignani, G., Grimaldi, A., Grimm, S. J., Grote, H., Grunewald, S., Gruson, A. S., Guerra, D., Guidi, G. M., Guimaraes, A. R., Gulati, H. K., Gulminelli, F., Gunny, A. M., Guo, H. -K., Guo, Y., Gupta, Anchal, Gupta, Anuradha, Gupta, P., Gupta, S. K., Gurs, J., Gustafson, R., Gutierrez, N., Guzman, F., Ha, S., Hadiputrawan, I. P. W., Haegel, L., Haino, S., Halim, O., Hall, E. D., Hamilton, E. Z., Hammond, G., Han, W. -B., Haney, M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O., Hansen, H., Hanson, J., Harada, R., Harder, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hartwig, D., Hasegawa, K., Haskell, B., Haster, C. -J., Hathaway, J. S., Hattori, K., Haughian, K., Hayakawa, H., Hayama, K., Hayes, F. J., Healy, J., Heidmann, A., Heidt, A., Heintze, M. C., Heinze, J., Heinzel, J., Heitmann, H., Hellman, F., Hello, P., Helmling-Cornell, A. F., Hemming, G., Hendry, M., Heng, I. S., Hennes, E., Hennig, J. -S., Hennig, M., Henshaw, C., Hernandez, A. G., Vivanco, F. Hernandez, Heurs, M., Hewitt, A. L., Higginbotham, S., Hild, S., Hill, P., Himemoto, Y., Hines, A. S., Hirata, N., Hirose, C., Ho, T-C., Hochheim, S., Hofman, D., Hohmann, J. N., Holcomb, D. G., Holland, N. A., Hollows, I. J., Holmes, Z. J., Holt, K., Holz, D. E., Hong, Q., Hough, J., Hourihane, S., Howell, D., Howell, E. J., Hoy, C. G., Hoyland, D., Hreibi, A., Hsieh, B-H., Hsieh, H-F., Hsiung, C., Huang, H-Y., Huang, P., Huang, Y-C., Huang, Y. -J., Huang, Y., Hübner, M. T., Huddart, A. D., Hughey, B., Hui, D. C. Y., Hui, V., Husa, S., Huttner, S. H., Huxford, R., Huynh-Dinh, T., Hyland, J., Iandolo, G. A., Ide, S., Idzkowski, B., Iess, A., Inayoshi, K., Inoue, Y., Iosif, P., Irwin, J., Gupta, Ish, Isi, M., Ito, K., Itoh, Y., Iyer, B. R., JaberianHamedan, V., Jacqmin, T., Jacquet, P. -E., Jadhav, S. J., Jadhav, S. P., Jain, T., James, A. L., Jan, A. Z., Jani, K., Janquart, J., Janssens, K., Janthalur, N. N., Jaranowski, P., Jariwala, D., Jarov, S., Jaume, R., Jenkins, A. C., Jenner, K., Jeon, C., Jia, W., Jiang, J., Jin, H. -B., Johns, G. R., Johnston, R., Johny, N., Jones, A. W., Jones, D. I., Jones, P., Jones, R., Joshi, P., Ju, L., Jung, K., Jung, P., Junker, J., Juste, V., Kaihotsu, K., Kajita, T., Kakizaki, M., Kalaghatgi, C., Kalogera, V., Kamai, B., Kamiizumi, M., Kanda, N., Kandhasamy, S., Kang, G., Kanner, J. B., Kao, Y., Kapadia, S. J., Kapasi, D. P., Karat, S., Karathanasis, C., Karki, S., Kashyap, R., Kasprzack, M., Kastaun, W., Kato, T., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaur, T., Kawabe, K., Kawaguchi, K., Kéfélian, F., Keitel, D., Key, J. S., Khadka, S., Khalili, F. Y., Khan, S., Khanam, T., Khazanov, E. A., Khetan, N., Khursheed, M., Kijbunchoo, N., Kim, C., Kim, J. C., Kim, J., Kim, K., Kim, P., Kim, W. S., Kim, Y. -M., Kimball, C., Kimura, N., King, B., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Klimenko, S., Klinger, T., Knee, A. M., Knust, N., Kobayashi, Y., Koch, P., Koehlenbeck, S. M., Koekoek, G., Kohri, K., Kokeyama, K., Koley, S., Kolitsidou, P., Kolstein, M., Kondrashov, V., Kong, A. K. H., Kontos, A., Korobko, M., Kossak, R. V., Kovalam, M., Koyama, N., Kozak, D. B., Kozakai, C., Kranzhoff, L., Kringel, V., Krishnendu, N. V., Królak, A., Kuehn, G., Kuijer, P., Kulkarni, S., Kumar, A., Kumar, Praveen, Kumar, Prayush, Kumar, Rahul, Kumar, Rakesh, Kume, J., Kuns, K., Kuromiya, Y., Kuroyanagi, S., Kuwahara, S., Kwak, K., Lacaille, G., Lagabbe, P., Laghi, D., Lalande, E., Lalleman, M., Lamberts, A., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., La Rosa, I., Lartaux-Vollard, A., Lasky, P. D., Lawrence, J., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., LeBohec, S., Lecoeuche, Y. K., Lee, E., Lee, H. M., Lee, K., Lee, R., Legred, I. N., Lehmann, J., Lemaître, A., Lenti, M., Leonardi, M., Leonova, E., Leroy, N., Letendre, N., Levesque, C., Levin, Y., Leviton, J. N., Leyde, K., Li, A. K. Y., Li, B., Li, K. L., Li, P., Li, T. G. F., Li, X., Lin, C-Y., Lin, E. T., Lin, F-K., Lin, F-L., Lin, H. L., Lin, L. C. -C., Linde, F., Linker, S. D., Littenberg, T. B., Liu, G. C., Liu, J., Liu, X., Llamas, F., Lo, R. K. L., Lo, T., London, L. T., Longo, A., Lopez, D., Portilla, M. Lopez, Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lott, T. P., Lough, J. D., Lousto, C. O., Lovelace, G., Lowry, M. J., Lucaccioni, J. F., Lück, H., Lumaca, D., Lundgren, A. P., Lung, Y., Luo, L. -W., Lussier, A. W., Lynam, J. E., Ma'arif, M., Macas, R., MacInnis, M., Macleod, D. M., MacMillan, I. A. O., Macquet, A., Hernandez, I. Magaña, Magazzù, C., Magee, R. M., Maggiore, R., Magnozzi, M., Mahesh, S., Majorana, E., Makarem, C. N., Maksimovic, I., Maliakal, S., Malik, A., Man, N., Mandic, V., Mangano, V., Mannix, B. R., Mansell, G. L., Mansingh, G., Manske, M., Mantovani, M., Mapelli, M., Marchesoni, F., Pina, D. Marín, Marion, F., Mark, Z., Márka, S., Márka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martinez, M., Martinez, V. A., Martinez, V., Martinovic, K., Martynov, D. V., Marx, E. J., Masalehdan, H., Mason, K., Masserot, A., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Mateu-Lucena, M., Matiushechkina, M., Mavalvala, N., McCann, J. J., McCarthy, R., McClelland, D. E., McClincy, P. K., McCormick, S., McCuller, L., McGhee, G. I., McGinn, J., McGuire, S. C., McIsaac, C., McIver, J., McLeod, A., McRae, T., McWilliams, S. T., Meacher, D., Mehmet, M., Mehta, A. K., Meijer, Q., Melatos, A., Mendell, G., Menendez-Vazquez, A., Menoni, C. S., Mercer, R. A., Mereni, L., Merfeld, K., Merilh, E. L., Merritt, J. D., Merzougui, M., Messenger, C., Messick, C., Meyers, P. M., Meylahn, F., Mhaske, A., Miani, A., Miao, H., Michaloliakos, I., Michel, C., Michimura, Y., Middleton, H., Mihaylov, D. P., Miller, A., Miller, A. L., Miller, B., Millhouse, M., Mills, J. C., Milotti, E., Minenkov, Y., Mio, N., Mir, Ll. M., Miravet-Tenés, M., Mishkin, A., Mishra, C., Mishra, T., Mistry, T., Mitchell, A. L., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Miyo, K., Miyoki, S., Mo, Geoffrey, Modafferi, L. M., Moguel, E., Mogushi, K., Mohapatra, S. R. P., Mohite, S. R., Molina-Ruiz, M., Mondal, C., Mondin, M., Montani, M., Moore, C. J., Moragues, J., Moraru, D., Morawski, F., More, A., More, S., Moreno, C., Moreno, G., Mori, Y., Morisaki, S., Morisue, N., Moriwaki, Y., Mours, B., Mow-Lowry, C. M., Mozzon, S., Muciaccia, F., Mukherjee, D., Mukherjee, Soma, Mukherjee, Subroto, Mukherjee, Suvodip, Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Murray, P. G., Muusse, S., Nadji, S. L., Nagano, K., Nagar, A., Nagar, T., Nakamura, K., Nakano, H., Nakano, M., Nakayama, Y., Napolano, V., Nardecchia, I., Narola, H., Naticchioni, L., Nayak, R. K., Neil, B. F., Neilson, J., Nelson, A., Nelson, T. J. N., Nery, M., Neubauer, P., Neunzert, A., Ng, K. Y., Ng, S. W. S., Nguyen, C., Nguyen, P., Nguyen, T., Quynh, L. Nguyen, Ni, J., Ni, W. -T., Nichols, S. A., Nieradka, G., Nishimoto, T., Nishizawa, A., Nissanke, S., Nitoglia, E., Niu, W., Nocera, F., Norman, M., North, C., Notte, J., Novak, J., Nozaki, S., Nurbek, G., Nuttall, L. K., Obayashi, Y., Oberling, J., O'Brien, B. D., O'Dell, J., Oelker, E., Oertel, M., Ogaki, W., Oganesyan, G., Oh, J. J., Oh, K., Oh, S. H., O'Hanlon, T., Ohashi, M., Ohashi, T., Ohkawa, M., Ohme, F., Ohta, H., Okutani, Y., Oliveri, R., Olivetto, C., Oohara, K., Oram, R., O'Reilly, B., Ormiston, R. G., Ormsby, N. D., Orselli, M., O'Shaughnessy, R., O'Shea, E., Oshino, S., Ossokine, S., Osthelder, C., Otabe, S., Ottaway, D. J., Overmier, H., Pace, A. E., Pagano, G., Pagano, R., Pagliaroli, G., Pai, A., Pai, S. A., Pal, S., Palamos, J. R., Palashov, O., Palomba, C., Pan, K. -C., Panda, P. K., Pang, P. T. H., Pannarale, F., Pant, B. C., Panther, F. H., Paoletti, F., Paoli, A., Paolone, A., Pappas, G., Parisi, A., Park, J., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, M., Patel, N. R., Pathak, M., Patricelli, B., Patron, A. S., Paul, S., Payne, E., Pedraza, M., Pedurand, R., Pegna, R., Pegoraro, M., Pele, A., Arellano, F. E. Peña, Penano, S., Penn, S., Perego, A., Pereira, A., Pereira, T., Perez, C. J., Périgois, C., Perkins, C. C., Perreca, A., Perriès, S., Perry, J. W., Pesios, D., Petermann, J., Pfeiffer, H. P., Pham, H., Pham, K. A., Phukon, K. S., Phurailatpam, H., Piccinni, O. J., Pichot, M., Piendibene, M., Piergiovanni, F., Pierini, L., Pierra, G., Pierro, V., Pillant, G., Pillas, M., Pilo, F., Pinard, L., Pineda-Bosque, C., Pinto, I. M., Pinto, M., Piotrzkowski, B. J., Piotrzkowski, K., Pirello, M., Pitkin, M. D., Placidi, A., Placidi, E., Planas, M. L., Plastino, W., Poggiani, R., Polini, E., Pong, D. Y. T., Ponrathnam, S., Porter, E. K., Posnansky, C., Poulton, R., Powell, J., Pracchia, M., Pradier, T., Prajapati, A. K., Prasai, K., Prasanna, R., Pratten, G., Principe, M., Prodi, G. A., Prokhorov, L., Prosposito, P., Prudenzi, L., Puecher, A., Punturo, M., Puosi, F., Puppo, P., Pürrer, M., Qi, H., Quartey, N., Quetschke, V., Quinonez, P. J., Quitzow-James, R., Raab, F. J., Raaijmakers, G., Radkins, H., Radulesco, N., Raffai, P., Rail, S. X., Raja, S., Rajan, C., Ramirez, K. E., Ramirez, T. D., Ramos-Buades, A., Rana, D., Rana, J., Rangnekar, P. R., Rapagnani, P., Ray, A., Raymond, V., Raza, N., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reid, S. W., Reinhard, M., Reitze, D. H., Relton, P., Renzini, A., Rettegno, P., Revenu, B., Reyes, J., Reza, A., Rezac, M., Rezaei, A. S., Ricci, F., Richards, D., Richardson, J. W., Richardson, L., Riles, K., Rinaldi, S., Robertson, C., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rodriguez, S., Rolland, L., Rollins, J. G., Romanelli, M., Romano, R., Romel, C. L., Romero, A., Romero-Shaw, I. M., Romie, J. H., Ronchini, S., Roocke, T. J., Rosa, L., Rose, C. A., Rosińska, D., Ross, M. P., Rossello, M., Rowan, S., Rowlinson, S. J., Roy, Santosh, Roy, Soumen, Royzman, A., Rozza, D., Ruggi, P., Ruiz-Rocha, K., Ryan, K., Sachdev, S., Sadecki, T., Sadiq, J., Saffarieh, P., Saha, S., Saito, Y., Sakai, K., Sakellariadou, M., Sakon, S., Salces-Carcoba, F., Salconi, L., Saleem, M., Salemi, F., Sallé, M., Samajdar, A., Sanchez, E. J., Sanchez, J. H., Sanchez, L. E., Sanchis-Gual, N., Sanders, J. R., Sanuy, A., Saravanan, T. R., Sarin, N., Sasli, A., Sassolas, B., Satari, H., Sathyaprakash, B. S., Sauter, O., Savage, R. L., Savant, V., Sawada, T., Sawant, H. L., Sayah, S., Schaetzl, D., Scheel, M., Scheuer, J., Schiworski, M. G., Schmidt, P., Schmidt, S., Schnabel, R., Schneewind, M., Schofield, R. M. S., Schönbeck, A., Schulte, B. W., Schutz, B. F., Schwartz, E., Scott, J., Scott, S. M., Seglar-Arroyo, M., Sekiguchi, Y., Sellers, D., Sengupta, A. S., Sentenac, D., Seo, E. G., Sequino, V., Sergeev, A., Servignat, G., Setyawati, Y., Shaffer, T., Shahriar, M. S., Shaikh, M. A., Shams, B., Shao, L., Sharma, A., Sharma, P., Shawhan, P., Shcheblanov, N. S., Sheela, A., Sheridan, E., Shikano, Y., Shikauchi, M., Shimizu, H., Shimode, K., Shinkai, H., Shishido, T., Shoda, A., Shoemaker, D. H., Shoemaker, D. M., ShyamSundar, S., Sieniawska, M., Sigg, D., Silenzi, L., Singer, L. P., Singh, D., Singh, M. K., Singh, N., Singha, A., Sintes, A. M., Sipala, V., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smetana, J., Smith, J. R., Smith, L., Smith, R. J. E., Soldateschi, J., Somala, S. N., Somiya, K., Song, I., Soni, K., Soni, S., Sordini, V., Sorrentino, F., Sorrentino, N., Soulard, R., Souradeep, T., Spagnuolo, V., Spencer, A. P., Spera, M., Spinicelli, P., Srivastava, A. K., Srivastava, V., Stachie, C., Stachurski, F., Steer, D. A., Steinlechner, J., Steinlechner, S., Stergioulas, N., Stops, D. J., Strain, K. A., Strang, L. C., Stratta, G., Strong, M. D., Strunk, A., Sturani, R., Stuver, A. L., Suchenek, M., Sudhagar, S., Sugimoto, R., Suh, H. G., Sullivan, A. G., Summerscales, T. Z., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Suzuki, Takamasa, Suzuki, Takanori, Suzuki, Toshikazu, Swinkels, B. L., Syx, A., Szczepańczyk, M. J., Szewczyk, P., Tacca, M., Tagoshi, H., Tait, S. C., Takahashi, H., Takahashi, R., Takano, S., Takeda, H., Takeda, M., Talbot, C. J., Talbot, C., Tamanini, N., Tanaka, K., Tanaka, Taiki, Tanaka, Takahiro, Tanasijczuk, A. J., Tanioka, S., Tanner, D. B., Tao, D., Tao, L., Tapia, R. D., Martín, E. N. Tapia San, Taranto, C., Taruya, A., Tasson, J. D., Tenorio, R., Terhune, J. E. S., Terkowski, L., Themann, H., Thirugnanasambandam, M. P., Thomas, M., Thomas, P., Thomas, S., Thompson, D., Thompson, E. E., Thompson, J. E., Thondapu, S. R., Thorne, K. A., Thrane, E., Tiwari, Shubhanshu, Tiwari, Srishti, Tiwari, V., Toivonen, A. M., Tolley, A. E., Tomaru, T., Tomura, T., Tonelli, M., Torres-Forné, A., Torrie, C. I., Melo, I. Tosta e, Tournefier, E., Töyrä, D., Trapananti, A., Travasso, F., Traylor, G., Trenado, J., Trevor, M., Tringali, M. C., Tripathee, A., Troiano, L., Trovato, A., Trozzo, L., Trudeau, R. J., Tsai, D., Tsang, K. W., Tsang, T., Tsao, J-S., Tse, M., Tso, R., Tsuchida, S., Tsukada, L., Tsuna, D., Tsutsui, T., Turbang, K., Turconi, M., Turski, C., Tuyenbayev, D., Ubach, H., Ubhi, A. S., Uchiyama, T., Udall, R. P., Ueda, A., Uehara, T., Ueno, K., Ueshima, G., Unnikrishnan, C. S., Urban, A. L., Ushiba, T., Utina, A., Vahlbruch, H., Vaidya, N., Vajente, G., Vajpeyi, A., Valdes, G., Valentini, M., Vallero, S., Valsan, V., van Bakel, N., van Beuzekom, M., van Dael, M., Brand, J. F. J. van den, Broeck, C. Van Den, Vander-Hyde, D. C., Van de Walle, A., van Dongen, J., van Haevermaet, H., van Heijningen, J. V., Vanosky, J., van Putten, M. H. P. M., van Ranst, Z., van Remortel, N., Vardaro, M., Vargas, A. F., Varma, V., Vasúth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venneberg, J., Venugopalan, G., Verdier, P., Verkindt, D., Verma, P., Verma, Y., Vermeulen, S. M., Veske, D., Vetrano, F., Viceré, A., Vidyant, S., Viets, A. D., Vijaykumar, A., Villa-Ortega, V., Vinet, J. -Y., Virtuoso, A., Vitale, S., Vocca, H., von Reis, E. R. G., von Wrangel, J. S. A., Vorvick, C., Vyatchanin, S. P., Wade, L. E., Wade, M., Wagner, K. J., Walet, R. C., Walker, M., Wallace, G. S., Wallace, L., Wang, J., Wang, J. Z., Wang, W. H., Ward, R. L., Warner, J., Was, M., Washimi, T., Washington, N. Y., Watada, K., Watarai, D., Watchi, J., Wayt, K. E., Weaver, B., Weaving, C. R., Webster, S. A., Weinert, M., Weinstein, A. J., Weiss, R., Weller, C. M., Weller, R. A., Wellmann, F., Wen, L., Weßels, P., Wette, K., Whelan, J. T., White, D. D., Whiting, B. F., Whittle, C., Wilk, O. S., Wilken, D., Williams, C. E., Williams, D., Williams, M. J., Williamson, A. R., Willis, J. L., Willke, B., Wipf, C. C., Woan, G., Woehler, J., Wofford, J. K., Wojtowicz, I. A., Wong, D., Wong, I. C. F., Wright, M., Wu, C., Wu, D. S., Wu, H., Wysocki, D. M., Xiao, L., Yadav, N., Yamada, T., Yamamoto, H., Yamamoto, K., Yamamoto, T., Yamashita, K., Yamazaki, R., Yang, F. W., Yang, K. Z., Yang, L., Yang, Y. -C., Yang, Y., Yang, Yang, Yap, M. J., Yeeles, D. W., Yeh, S. -W., Yelikar, A. B., Yokoyama, J., Yokozawa, T., Yoo, J., Yoshioka, T., Yu, Hang, Yu, Haocun, Yuzurihara, H., Zadrożny, A., Zanolin, M., Zeidler, S., Zelenova, T., Zendri, J. -P., Zevin, M., Zhan, M., Zhang, H., Zhang, J., Zhang, L., Zhang, R., Zhang, T., Zhang, Y., Zhao, C., Zhao, G., Zhao, Y., Zhao, Yue, Zheng, Y., Zhou, R., Zhu, X. J., Zhu, Z. -H., Zimmerman, A. B., Zucker, M. E., and Zweizig, J.
Subjects: General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Gravitational lensing by massive objects along the line of sight to the source causes distortions of gravitational wave-signals; such distortions may reveal information about fundamental physics, cosmology and astrophysics. In this work, we have extended the search for lensing signatures to all binary black hole events from the third observing run of the LIGO--Virgo network. We search for repeated signals from strong lensing by 1) performing targeted searches for subthreshold signals, 2) calculating the degree of overlap amongst the intrinsic parameters and sky location of pairs of signals, 3) comparing the similarities of the spectrograms amongst pairs of signals, and 4) performing dual-signal Bayesian analysis that takes into account selection effects and astrophysical knowledge. We also search for distortions to the gravitational waveform caused by 1) frequency-independent phase shifts in strongly lensed images, and 2) frequency-dependent modulation of the amplitude and phase due to point masses. None of these searches yields significant evidence for lensing. Finally, we use the non-detection of gravitational-wave lensing to constrain the lensing rate based on the latest merger-rate estimates and the fraction of dark matter composed of compact objects., Comment: 28 pages, 11 figures
Published: 2023

198. WaterLily.jl: A differentiable fluid simulator in Julia with fast heterogeneous execution

Author: Weymouth, Gabriel D. and Font, Bernat
Subjects: Physics - Fluid Dynamics, Physics - Computational Physics
Abstract: Integrating computational fluid dynamics (CFD) software into optimization and machine-learning frameworks is hampered by the rigidity of classic computational languages and the slow performance of more flexible high-level languages. WaterLily.jl is an open-source incompressible viscous flow solver written in the Julia language. The small code base is multi-dimensional, multi-platform and backend-agnostic (serial CPU, multi-threaded, & GPU execution). The simulator is differentiable and uses automatic-differentiation internally to immerse solid geometries and optimize the pressure solver. The computational time per time step scales linearly with the number of degrees of freedom on CPUs, and we see up to a 182x speed-up using CUDA kernels. This leads to comparable performance with Fortran solvers on many research-scale problems opening up exciting possible future applications on the cutting edge of machine-learning research.
Published: 2023

199. Analysis of the impact of broad absorption lines on quasar redshift measurements with synthetic observations

Author: García, Luz Ángela, Martini, Paul, Gonzalez-Morales, Alma X., Font-Ribera, Andreu, Herrera-Alcantar, Hiram K., Aguilar, Jessica Nicole, Ahlen, Steve, Brooks, David, de la Macorra, Axel, Doel, Peter, Forero-Romero, Jaime E., Guy, Julien, Kisner, Theodore, Landriau, Martin, Miquel, Ramon, Moustakas, John, Nie, Jundan, Poppett, Claire, Tarlé, Gregory, and Zhou, Zhimin
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology
Abstract: Accurate quasar classifications and redshift measurements are increasingly important to precision cosmology experiments. Broad absorption line (BAL) features are present in 15-20\% of all quasars, and these features can introduce systematic redshift errors, and in extreme cases produce misclassifications. We quantitatively investigate the impact of BAL features on quasar classifications and redshift measurements with synthetic spectra that were designed to match observations by the Dark Energy Spectroscopic Instrument (DESI) survey. Over the course of five years, DESI aims to measure spectra for 40 million galaxies and quasars, including nearly three million quasars. Our synthetic quasar spectra match the signal-to-noise ratio and redshift distributions of the first year of DESI observations, and include the same synthetic quasar spectra both with and without BAL features. We demonstrate that masking the locations of the BAL features decreases the redshift errors by about 1\% and reduces the number of catastrophic redshift errors by about 80\%. We conclude that identifying and masking BAL troughs should be a standard part of the redshift determination step for DESI and other large-scale spectroscopic surveys of quasars., Comment: 12 pages, 9 figures, submitted to MNRAS
Published: 2023

200. Magnetized tori with magnetic polarization around Kerr black holes: Variable angular momentum discs

Author: Gimeno-Soler, Sergio, Pimentel, Oscar. M., Lora-Clavijo, Fabio D., Cruz-Osorio, Alejandro, and Font, José A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology, 83C57, 76W05, 85A30, 83C55
Abstract: Analytical models of magnetized, geometrically thick disks are relevant to understand the physical conditions of plasma around compact objects and to explore its emitting properties. This has become increasingly important in recent years in the light of the Event Horizon Telescope observations of Sgr A$^*$ and M87. Models of thick disks around black holes usually consider constant angular momentum distributions and do not take into account the magnetic response of the fluid to applied magnetic fields. We present a generalization of our previous work on stationary models of magnetized accretion disks with magnetic polarization (Pimentel et al. 2018). This extension is achieved by accounting for non-constant specific angular momentum profiles, done through a two-parameter ansatz for those distributions. We build a large number of new equilibrium solutions of thick disks with magnetic polarization around Kerr black holes, selecting suitable parameter values within the intrinsically substantial parameter space of the models. We study the morphology and the physical properties of those solutions, finding qualitative changes with respect to the constant angular momentum tori solutions (Pimentel et al. 2018). However, the dependences found on the angular momentum distribution or on the black hole spin do not seem to be strong. Some of the new solutions, however, exhibit a local maximum of the magnetization function, absent in standard magnetized tori. Due to the enhanced development of the magneto-rotational instability as a result of magnetic susceptibility, those models might be particularly well-suited to investigate jet formation through general-relativistic MHD simulations. The new equilibrium solutions reported here can be used as initial data in numerical codes to assess the impact of magnetic susceptibility in the dynamics and observational properties of black hole-thick disk systems., Comment: 19 pages, 10 figures. Accepted for publication in Physical Review D
Published: 2023

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Language

Publication Type

Journal

Region

Database

Publisher

6,633 results on '"Font P"'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources