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373 results on '"Santiago B."'

1. Representación gráfica militar del territorio : El Servicio Geográfico del Ejército español y la Comisión n.º 8 de La Coruña

Author: Franco Taboada, José Antonio, Pernas Alonso, María Inés, Tarrío Carrodeguas, Santiago B. (titor), Fraga López, Francisco Javier, Franco Taboada, José Antonio, Pernas Alonso, María Inés, Tarrío Carrodeguas, Santiago B. (titor), and Fraga López, Francisco Javier
Abstract: [Resumen]: Aun cuando sus orígenes se remontan a 1810 con la fundación del Cuerpo de Estado Mayor (Baldovín 2001), el Servicio Geográfico del Ejército (SGE) español desarrolla su actividad entre 1939-1998, años de su creación-recentralización en el Centro Geográfico del Ejército (CGE). El conocimiento detallado del territorio pasa por distintas fases, en algunas de las cuales el Ejército se convierte en actor principal, tales como: la exploración, la construcción y la representación. Si hay que destacar alguna, sería esta última, debido a la importancia estratégica que supone poder contar con buenos mapas de los posibles teatros de operaciones. A lo largo de su existencia, el SGE ha dedicado la mayor parte de sus esfuerzos a la elaboración de diferente cartografía (Mapa Topográfico Nacional, Mapa militar de España a 1:200.000; nueva serie L a 1:50.000; nueva cartografía normalizada OTAN 1:250.00, 1:500.000 y 1:1.000.000), realizada bien individualmente o bien en colaboración con otras instituciones (Instituto Geográfico). Razones de diferente carácter: político, económico, estratégico o incluso tecnológicas pueden haber influido en la recentralización del SGE en el CGE. El objetivo principal de esta comunicación es el de poner en valor la labor desarrollada por el SGE en relación con la representación del territorio.
Published: 2024

2. Dark Energy Survey: A 2.1% measurement of the angular Baryonic Acoustic Oscillation scale at redshift $z_{\rm eff}$=0.85 from the final dataset

Author: DES Collaboration, Abbott, T. M. C., Adamow, M., Aguena, M., Allam, S., Alves, O., Amon, A., Andrade-Oliveira, F., Asorey, J., Avila, S., Bacon, D., Bechtol, K., Bernstein, G. M., Bertin, E., Blazek, J., Bocquet, S., Brooks, D., Burke, D. L., Camacho, H., Rosell, A. Carnero, Carollo, D., Carretero, J., Castander, F. J., Cawthon, R., Chan, K. C., Chang, C., Conselice, C., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Deiosso, N., Desai, S., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Elvin-Poole, J., Everett, S., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Giannini, G., Gruendl, R. A., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kent, S., Kuehn, K., Lahav, O., Lee, S., Lidman, C., Lin, H., Marshall, J. L., Martini, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Mohr, J. J., Myles, J., Nichol, R. C., Ogando, R. L. C., Palmese, A., Percival, W. J., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Rodríguez-Monroy, M., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sako, M., Samuroff, S., Sánchez, C., Sanchez, E., Cid, D. Sanchez, Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Cipriano, L. Toribio San, Troxel, M. A., Tucker, B. E., Tucker, D. L., Walker, A. R., Weaverdyck, N., Weller, J., Wiseman, P., Yanny, B., DES Collaboration, Abbott, T. M. C., Adamow, M., Aguena, M., Allam, S., Alves, O., Amon, A., Andrade-Oliveira, F., Asorey, J., Avila, S., Bacon, D., Bechtol, K., Bernstein, G. M., Bertin, E., Blazek, J., Bocquet, S., Brooks, D., Burke, D. L., Camacho, H., Rosell, A. Carnero, Carollo, D., Carretero, J., Castander, F. J., Cawthon, R., Chan, K. C., Chang, C., Conselice, C., Costanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Deiosso, N., Desai, S., Diehl, H. T., Dodelson, S., Doux, C., Drlica-Wagner, A., Elvin-Poole, J., Everett, S., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Giannini, G., Gruendl, R. A., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Kent, S., Kuehn, K., Lahav, O., Lee, S., Lidman, C., Lin, H., Marshall, J. L., Martini, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Mohr, J. J., Myles, J., Nichol, R. C., Ogando, R. L. C., Palmese, A., Percival, W. J., Pieres, A., Malagón, A. A. Plazas, Porredon, A., Prat, J., Rodríguez-Monroy, M., Romer, A. K., Roodman, A., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Sako, M., Samuroff, S., Sánchez, C., Sanchez, E., Cid, D. Sanchez, Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Cipriano, L. Toribio San, Troxel, M. A., Tucker, B. E., Tucker, D. L., Walker, A. R., Weaverdyck, N., Weller, J., Wiseman, P., and Yanny, B.
Abstract: We present the angular diameter distance measurement obtained with the Baryonic Acoustic Oscillation feature from galaxy clustering in the completed Dark Energy Survey, consisting of six years (Y6) of observations. We use the Y6 BAO galaxy sample, optimized for BAO science in the redshift range 0.6<$z$<1.2, with an effective redshift at $z_{\rm eff}$=0.85 and split into six tomographic bins. The sample has nearly 16 million galaxies over 4,273 square degrees. Our consensus measurement constrains the ratio of the angular distance to sound horizon scale to $D_M(z_{\rm eff})/r_d$ = 19.51$\pm$0.41 (at 68.3% confidence interval), resulting from comparing the BAO position in our data to that predicted by Planck $\Lambda$CDM via the BAO shift parameter $\alpha=(D_M/r_d)/(D_M/r_d)_{\rm Planck}$. To achieve this, the BAO shift is measured with three different methods, Angular Correlation Function (ACF), Angular Power Spectrum (APS), and Projected Correlation Function (PCF) obtaining $\alpha=$ 0.952$\pm$0.023, 0.962$\pm$0.022, and 0.955$\pm$0.020, respectively, which we combine to $\alpha=$ 0.957$\pm$0.020, including systematic errors. When compared with the $\Lambda$CDM model that best fits Planck data, this measurement is found to be 4.3% and 2.1$\sigma$ below the angular BAO scale predicted. To date, it represents the most precise angular BAO measurement at $z$>0.75 from any survey and the most precise measurement at any redshift from photometric surveys. The analysis was performed blinded to the BAO position and it is shown to be robust against analysis choices, data removal, redshift calibrations and observational systematics., Comment: Submitted to PRD, 39 pages, 12 figures
Published: 2024

3. Dark Energy Survey: Galaxy Sample for the Baryonic Acoustic Oscillation Measurement from the Final Dataset

Author: Mena-Fernández, J., Rodríguez-Monroy, M., Avila, S., Porredon, A., Chan, K. C., Camacho, H., Weaverdyck, N., Sevilla-Noarbe, I., Sanchez, E., Cipriano, L. Toribio San, De Vicente, J., Ferrero, I., Cawthon, R., Rosell, A. Carnero, Elvin-Poole, J., Giannini, G., Adamow, M., Bechtol, K., Drlica-Wagner, A., Gruendl, R. A., Hartley, W. G., Pieres, A., Ross, A. J., Rykoff, E. S., Sheldon, E., Yanny, B., Abbott, T. M. C., Aguena, M., Allam, S., Alves, O., Amon, A., Andrade-Oliveira, F., Annis, J., Bacon, D., Blazek, J., Bocquet, S., Brooks, D., Carretero, J., Castander, F. J., Conselice, C., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Deiosso, N., Desai, S., Diehl, H. T., Dodelson, S., Doux, C., Everett, S., Frieman, J., García-Bellido, J., Gaztanaga, E., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., Kuehn, K., Lahav, O., Lee, S., Lidman, C., Lin, H., Marshall, J. L., Menanteau, F., Miquel, R., Myles, J., Ogando, R. L. C., Palmese, A., Percival, W. J., Malagón, A. A. Plazas, Roodman, A., Rosenfeld, R., Samuroff, S., Cid, D. Sanchez, Santiago, B., Schubnell, M., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Walker, A. R., Weller, J., Wiseman, P., Yamamoto, M., Mena-Fernández, J., Rodríguez-Monroy, M., Avila, S., Porredon, A., Chan, K. C., Camacho, H., Weaverdyck, N., Sevilla-Noarbe, I., Sanchez, E., Cipriano, L. Toribio San, De Vicente, J., Ferrero, I., Cawthon, R., Rosell, A. Carnero, Elvin-Poole, J., Giannini, G., Adamow, M., Bechtol, K., Drlica-Wagner, A., Gruendl, R. A., Hartley, W. G., Pieres, A., Ross, A. J., Rykoff, E. S., Sheldon, E., Yanny, B., Abbott, T. M. C., Aguena, M., Allam, S., Alves, O., Amon, A., Andrade-Oliveira, F., Annis, J., Bacon, D., Blazek, J., Bocquet, S., Brooks, D., Carretero, J., Castander, F. J., Conselice, C., Crocce, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Deiosso, N., Desai, S., Diehl, H. T., Dodelson, S., Doux, C., Everett, S., Frieman, J., García-Bellido, J., Gaztanaga, E., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., Kuehn, K., Lahav, O., Lee, S., Lidman, C., Lin, H., Marshall, J. L., Menanteau, F., Miquel, R., Myles, J., Ogando, R. L. C., Palmese, A., Percival, W. J., Malagón, A. A. Plazas, Roodman, A., Rosenfeld, R., Samuroff, S., Cid, D. Sanchez, Santiago, B., Schubnell, M., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tucker, D. L., Walker, A. R., Weller, J., Wiseman, P., and Yamamoto, M.
Abstract: In this paper we present and validate the galaxy sample used for the analysis of the baryon acoustic oscillation (BAO) signal in the Dark Energy Survey (DES) Y6 data. The definition is based on a color and redshift-dependent magnitude cut optimized to select galaxies at redshifts higher than 0.6, while ensuring a high-quality photo-$z$ determination. The optimization is performed using a Fisher forecast algorithm, finding the optimal $i$-magnitude cut to be given by $i$<19.64+2.894$z_{\rm ph}$. For the optimal sample, we forecast an increase in precision in the BAO measurement of $\sim$25% with respect to the Y3 analysis. Our BAO sample has a total of 15,937,556 galaxies in the redshift range 0.6<$z_{\rm ph}$<1.2, and its angular mask covers 4,273.42 deg${}^2$ to a depth of $i$=22.5. We validate its redshift distributions with three different methods: directional neighborhood fitting algorithm (DNF), which is our primary photo-$z$ estimation; direct calibration with spectroscopic redshifts from VIPERS; and clustering redshift using SDSS galaxies. The fiducial redshift distribution is a combination of these three techniques performed by modifying the mean and width of the DNF distributions to match those of VIPERS and clustering redshift. In this paper we also describe the methodology used to mitigate the effect of observational systematics, which is analogous to the one used in the Y3 analysis. This paper is one of the two dedicated to the analysis of the BAO signal in DES Y6. In its companion paper, we present the angular diameter distance constraints obtained through the fitting to the BAO scale., Comment: 23 pages, 10 figures. Submitted to PRD
Published: 2024

4. Copacabana: A Probabilistic Membership Assignment Method for Galaxy Clusters

Author: Esteves, J. H., Pereira, M. E. S., Soares-Santos, M., Annis, J., Farahi, A., Andrade-Oliveira, F., Barchi, P., Palmese, A., Lin, H., Welch, B., Wu, H. -Y., Aguena, M., Bacon, O. Alves D., Bocquet, S., Brooks, D., Rosell, A. Carnero, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Doel, P., Everett, S., Flaugher, B., Frieman, J., García-Bellido, J., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lidman, C., Lima, M., Marshall, J. L., Mena-Fernández, J., Miquel, R., Myles, J., Ogando, R. L. C., Pieres, A., Malagón, A. A. Plazas, Romer, A. K., Sanchez, E., Cid, D. Sanchez, Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Weaverdyck, N., Wiseman, P., Yamamoto, M., collaboration, DES, Esteves, J. H., Pereira, M. E. S., Soares-Santos, M., Annis, J., Farahi, A., Andrade-Oliveira, F., Barchi, P., Palmese, A., Lin, H., Welch, B., Wu, H. -Y., Aguena, M., Bacon, O. Alves D., Bocquet, S., Brooks, D., Rosell, A. Carnero, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Doel, P., Everett, S., Flaugher, B., Frieman, J., García-Bellido, J., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Lidman, C., Lima, M., Marshall, J. L., Mena-Fernández, J., Miquel, R., Myles, J., Ogando, R. L. C., Pieres, A., Malagón, A. A. Plazas, Romer, A. K., Sanchez, E., Cid, D. Sanchez, Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Weaverdyck, N., Wiseman, P., Yamamoto, M., and collaboration, DES
Abstract: Cosmological analyses using galaxy clusters in optical/NIR photometric surveys require robust characterization of their galaxy content. Precisely determining which galaxies belong to a cluster is crucial. In this paper, we present the COlor Probabilistic Assignment of Clusters And BAyesiaN Analysis (Copacabana) algorithm. Copacabana computes membership probabilities for {\it all} galaxies within an aperture centred on the cluster using photometric redshifts, colours, and projected radial probability density functions. We use simulations to validate Copacabana and we show that it achieves up to 89\% membership accuracy with a mild dependency on photometric redshift uncertainties and choice of aperture size. We find that the precision of the photometric redshifts has the largest impact on the determination of the membership probabilities followed by the choice of the cluster aperture size. We also quantify how much these uncertainties in the membership probabilities affect the stellar mass--cluster mass scaling relation, a relation that directly impacts cosmology. Using the sum of the stellar masses weighted by membership probabilities ($\mu_{\star}$) as the observable, we find that Copacabana can reach an accuracy of 0.06 dex in the measurement of the scaling relation. These results indicate the potential of Copacabana and $\mu_{\star}$ to be used in cosmological analyses of optically selected clusters in the future., Comment: 14 pages, 10 figures, submitted to MNRAS
Published: 2024

5. Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate

Author: Webber, K. B., Hansen, Terese T, Marshall, J. L., Simon, J. D., Pace, A. B., Mutlu-Pakdil, B., Drlica-Wagner, A., Martinez-Vazquez, C. E., Aguena, M., Allam, S. S., Alves, O., Bertin, E., Brooks, D., Carnero Rosell, A., Carretero, J., da Costa, L. N., De Vicente, J., Doel, P., Ferrero, I., Friedel, D., Frieman, J., Garcia-Bellido, J., Giannini, G., Gruen, D., Gruendl, R. A., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuehn, K., Mena-Fernandez, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Pereira, M. E. S., Pieres, A., Plazas Malagon, A. A., Sanchez, E., Santiago, B., Smith, J. Allyn, Smith, M., Suchyta, E., Tarle, G., To, C., Weaverdyck, N., Yanny, B., Webber, K. B., Hansen, Terese T, Marshall, J. L., Simon, J. D., Pace, A. B., Mutlu-Pakdil, B., Drlica-Wagner, A., Martinez-Vazquez, C. E., Aguena, M., Allam, S. S., Alves, O., Bertin, E., Brooks, D., Carnero Rosell, A., Carretero, J., da Costa, L. N., De Vicente, J., Doel, P., Ferrero, I., Friedel, D., Frieman, J., Garcia-Bellido, J., Giannini, G., Gruen, D., Gruendl, R. A., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuehn, K., Mena-Fernandez, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Pereira, M. E. S., Pieres, A., Plazas Malagon, A. A., Sanchez, E., Santiago, B., Smith, J. Allyn, Smith, M., Suchyta, E., Tarle, G., To, C., Weaverdyck, N., and Yanny, B.
Abstract: We present a detailed chemical abundance analysis of the brightest star in the ultrafaint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from carbon to europium are derived. Its chemical abundances generally follow those of other UFD galaxy stars, with a slight enhancement of the alpha-elements (Mg, Si, and Ca) and low neutron-capture element (Sr, Ba, and Eu) abundances supporting the classification of Cetus II as a likely UFD. The star exhibits lower Sc, Ti, and V abundances than Milky Way (MW) halo stars with similar metallicity. This signature is consistent with yields from a supernova originating from a star with a mass of similar to 11.2 M-circle dot. In addition, the star has a potassium abundance of [K/Fe] = 0.81, which is somewhat higher than the K abundances of MW halo stars with similar metallicity, a signature that is also present in a number of UFD galaxies. A comparison including globular clusters and stellar stream stars suggests that high K is a specific characteristic of some UFD galaxy stars and can thus be used to help classify objects as UFD galaxies.
Published: 2023
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6. Adequacy of the 10 mg/kg Daily Dose of Antituberculosis Drug Isoniazid in Infants under 6 Months of Age.

Author: López-Ramos, M.G., Vinent, J., Aarnoutse, R.E., Colbers, A., Velasco-Arnaiz, E., Martorell, L., Falcón-Neyra, L., Neth, O., Prieto, L., Guillén, S., Baquero-Artigao, F., Méndez-Echevarría, A., Gómez-Pastrana, D., Jiménez, A.B., Lahoz, R., Ramos-Amador, J.T., Soriano-Arandes, A., Santiago, B., Farré, R., Fortuny, C., Soy, D., Noguera-Julian, A., López-Ramos, M.G., Vinent, J., Aarnoutse, R.E., Colbers, A., Velasco-Arnaiz, E., Martorell, L., Falcón-Neyra, L., Neth, O., Prieto, L., Guillén, S., Baquero-Artigao, F., Méndez-Echevarría, A., Gómez-Pastrana, D., Jiménez, A.B., Lahoz, R., Ramos-Amador, J.T., Soriano-Arandes, A., Santiago, B., Farré, R., Fortuny, C., Soy, D., and Noguera-Julian, A.
Abstract: Item does not contain fulltext, In 2010, the WHO recommended an increase in the daily doses of first-line anti-tuberculosis medicines in children. We aim to characterize the pharmacokinetics of the once-daily isoniazid (INH) dose at 10 mg/kg of body weight in infants <6 months of age. We performed a multicenter pharmacokinetic study in Spain. The N-acetyltransferase 2 gene was analyzed to determine the acetylation status. Samples were analyzed using a validated UPLC-UV assay. A non-compartmental pharmacokinetic analysis was performed. Twenty-three pharmacokinetic profiles were performed in 20 infants (8 females) at a median (IQR) age of 19.0 (12.6-23.3) weeks. The acetylator statuses were homozygous fast (n = 1), heterozygous intermediate (n = 12), and homozygous slow (n = 7). INH median (IQR) C(max) and AUC(0-24h) values were 4.8 (3.7-6.7) mg/L and 23.5 (13.4-36.7) h*mg/L and the adult targets (>3 mg/L and 11.6-26.3 h*mg/L) were not reached in three and five cases, respectively. The age at assessment or acetylator status had no impact on C(max) values, but a larger INH AUC(0-24h) (p = 0.025) and trends towards a longer half-life (p = 0.055) and slower clearance (p = 0.070) were observed in homozygous slow acetylators. Treatment was well tolerated; mildly elevated alanine aminotransferase levels were observed in three cases. In our series of young infants receiving isoniazid, no major safety concerns were raised, and the target adult levels were reached in most patients.
Published: 2023

7. Adequacy of the 10 mg/kg Daily Dose of Antituberculosis Drug Isoniazid in Infants under 6 Months of Age.

Author: López-Ramos, M.G., Vinent, J., Aarnoutse, R.E., Colbers, A., Velasco-Arnaiz, E., Martorell, L., Falcón-Neyra, L., Neth, O., Prieto, L., Guillén, S., Baquero-Artigao, F., Méndez-Echevarría, A., Gómez-Pastrana, D., Jiménez, A.B., Lahoz, R., Ramos-Amador, J.T., Soriano-Arandes, A., Santiago, B., Farré, R., Fortuny, C., Soy, D., Noguera-Julian, A., López-Ramos, M.G., Vinent, J., Aarnoutse, R.E., Colbers, A., Velasco-Arnaiz, E., Martorell, L., Falcón-Neyra, L., Neth, O., Prieto, L., Guillén, S., Baquero-Artigao, F., Méndez-Echevarría, A., Gómez-Pastrana, D., Jiménez, A.B., Lahoz, R., Ramos-Amador, J.T., Soriano-Arandes, A., Santiago, B., Farré, R., Fortuny, C., Soy, D., and Noguera-Julian, A.
Abstract: Contains fulltext : 290828.pdf (Publisher’s version ) (Open Access), In 2010, the WHO recommended an increase in the daily doses of first-line anti-tuberculosis medicines in children. We aim to characterize the pharmacokinetics of the once-daily isoniazid (INH) dose at 10 mg/kg of body weight in infants <6 months of age. We performed a multicenter pharmacokinetic study in Spain. The N-acetyltransferase 2 gene was analyzed to determine the acetylation status. Samples were analyzed using a validated UPLC-UV assay. A non-compartmental pharmacokinetic analysis was performed. Twenty-three pharmacokinetic profiles were performed in 20 infants (8 females) at a median (IQR) age of 19.0 (12.6-23.3) weeks. The acetylator statuses were homozygous fast (n = 1), heterozygous intermediate (n = 12), and homozygous slow (n = 7). INH median (IQR) C(max) and AUC(0-24h) values were 4.8 (3.7-6.7) mg/L and 23.5 (13.4-36.7) h*mg/L and the adult targets (>3 mg/L and 11.6-26.3 h*mg/L) were not reached in three and five cases, respectively. The age at assessment or acetylator status had no impact on C(max) values, but a larger INH AUC(0-24h) (p = 0.025) and trends towards a longer half-life (p = 0.055) and slower clearance (p = 0.070) were observed in homozygous slow acetylators. Treatment was well tolerated; mildly elevated alanine aminotransferase levels were observed in three cases. In our series of young infants receiving isoniazid, no major safety concerns were raised, and the target adult levels were reached in most patients.
Published: 2023

8. Chemical Analysis of the Brightest Star of the Cetus II Ultra-Faint Dwarf Galaxy Candidate

Author: Webber, K. B., Hansen, T. T., Marshall, J. L., Simon, J. D., Pace, A. B., Mutlu-Pakdil, B., Drlica-Wagner, A., MartÍnez-VÁzquez, C. E., Aguena, M., Allam, S. S., Alves, O., Bertin, E., Brooks, D., Rosell, A. Carnero, Carretero, J., Da Costa, L. N., De Vicente, J., Doel, P., Ferrero, I., Friedel, D., Frieman, J., GarcÍa-Bellido, J., Giannini, G., Gruen, D., Gruendl, R. A., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuehn, K., Mena-FernÁndez, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Pereira, M. E. S., Pieres, A., MalagÓn, A. A. Plazas, Sanchez, E., Santiago, B., Smith, J. Allyn, Smith, M., Suchyta, E., Tarle, G., To, C., Weaverdyck, N., Yanny, B., Webber, K. B., Hansen, T. T., Marshall, J. L., Simon, J. D., Pace, A. B., Mutlu-Pakdil, B., Drlica-Wagner, A., MartÍnez-VÁzquez, C. E., Aguena, M., Allam, S. S., Alves, O., Bertin, E., Brooks, D., Rosell, A. Carnero, Carretero, J., Da Costa, L. N., De Vicente, J., Doel, P., Ferrero, I., Friedel, D., Frieman, J., GarcÍa-Bellido, J., Giannini, G., Gruen, D., Gruendl, R. A., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuehn, K., Mena-FernÁndez, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Pereira, M. E. S., Pieres, A., MalagÓn, A. A. Plazas, Sanchez, E., Santiago, B., Smith, J. Allyn, Smith, M., Suchyta, E., Tarle, G., To, C., Weaverdyck, N., and Yanny, B.
Abstract: We present a detailed chemical abundance analysis of the brightest star in the ultra-faint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from Carbon to Europium are derived. Its chemical abundances generally follow those of other UFD galaxy stars, with a slight enhancement of the alpha-elements (Mg, Si, and Ca) and low neutron-capture element (Sr, Ba, Eu) abundances supporting the classification of Cetus II as a likely UFD. The star exhibits lower Sc, Ti, and V abundances than Milky Way (MW) halo stars with similar metallicity. This signature is consistent with yields from a supernova (SN) originating from a star with a mass of ~11.2 solar masses. In addition, the star has a Potassium abundance of [K/Fe] = 0.81 which is somewhat higher than the K abundances of MW halo stars with similar metallicity, a signature which is also present in a number of UFD galaxies. A comparison including globular clusters (GC) and stellar stream stars suggests that high K is a specific characteristic for some UFD galaxy stars and can thus be used to help classify objects as UFD galaxies., Comment: 15 pages, 7 figures, 5 tables, accepted to ApJ
Published: 2023

9. A search for faint resolved galaxies beyond the Milky Way in DES Year 6: A new faint, diffuse dwarf satellite of NGC 55

Author: McNanna, M., Bechtol, K., Mau, S., Nadler, E. O., Medoff, J., Drlica-Wagner, A., Cerny, W., Crnojevic, D., Mutlu-Pakdil, B., Vivas, A. K., Pace, A. B., Carlin, J. L., Collins, M. L. M., Ferguson, P. S., Martinez-Delgado, D., Martinez-Vazquez, C. E., Noel, N. E. D., Riley, A. H., Sand, D. J., Smercina, A., Tollerud, E., Wechsler, R. H., Abbott, T. M. C., Aguena, M., Alves, O., Bacon, D., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Rosell, A. Carnero, Carretero, J., da Costa, L. N., Davis, T. M., De Vicente, J., Diehl, H. T., Doel, P., Ferrero, I., Frieman, J., Giannini, G., Gruen, D., Gutierrez, G., Gruendl, R. A., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Marshall, J. L., Mena-Fernandez, J., Miquel, R., Pereira, M. E. S., Pieres, A., Malagon, A. A. Plazas, Sakowska, J. D., Sanchez, E., Cid, D. Sanchez, Santiago, B., Sevilla-Noarbe, I., Smith, M., Stringfellow, G. S., Suchyta, E., Swanson, M. E. C., Tarle, G., Weaverdyck, N., Wiseman, P., McNanna, M., Bechtol, K., Mau, S., Nadler, E. O., Medoff, J., Drlica-Wagner, A., Cerny, W., Crnojevic, D., Mutlu-Pakdil, B., Vivas, A. K., Pace, A. B., Carlin, J. L., Collins, M. L. M., Ferguson, P. S., Martinez-Delgado, D., Martinez-Vazquez, C. E., Noel, N. E. D., Riley, A. H., Sand, D. J., Smercina, A., Tollerud, E., Wechsler, R. H., Abbott, T. M. C., Aguena, M., Alves, O., Bacon, D., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Rosell, A. Carnero, Carretero, J., da Costa, L. N., Davis, T. M., De Vicente, J., Diehl, H. T., Doel, P., Ferrero, I., Frieman, J., Giannini, G., Gruen, D., Gutierrez, G., Gruendl, R. A., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Marshall, J. L., Mena-Fernandez, J., Miquel, R., Pereira, M. E. S., Pieres, A., Malagon, A. A. Plazas, Sakowska, J. D., Sanchez, E., Cid, D. Sanchez, Santiago, B., Sevilla-Noarbe, I., Smith, M., Stringfellow, G. S., Suchyta, E., Swanson, M. E. C., Tarle, G., Weaverdyck, N., and Wiseman, P.
Abstract: We report results from a systematic wide-area search for faint dwarf galaxies at heliocentric distances from 0.3 to 2 Mpc using the full six years of data from the Dark Energy Survey (DES). Unlike previous searches over the DES data, this search specifically targeted a field population of faint galaxies located beyond the Milky Way virial radius. We derive our detection efficiency for faint, resolved dwarf galaxies in the Local Volume with a set of synthetic galaxies and expect our search to be complete to $M_V$ ~ $(-7, -10)$ mag for galaxies at $D = (0.3, 2.0)$ Mpc respectively. We find no new field dwarfs in the DES footprint, but we report the discovery of one high-significance candidate dwarf galaxy at a distance of $2.2\substack{+0.05\\-0.12}$ Mpc, a potential satellite of the Local Volume galaxy NGC 55, separated by $47$ arcmin (physical separation as small as 30 kpc). We estimate this dwarf galaxy to have an absolute V-band magnitude of $-8.0\substack{+0.5\\-0.3}$ mag and an azimuthally averaged physical half-light radius of $2.2\substack{+0.5\\-0.4}$ kpc, making this one of the lowest surface brightness galaxies ever found with $\mu = 32.3$ mag ${\rm arcsec}^{-2}$. This is the largest, most diffuse galaxy known at this luminosity, suggesting possible tidal interactions with its host., Comment: 20 pages, 7 figures
Published: 2023

10. The Dark Energy Survey Six-Year Calibration Star Catalog

Author: Rykoff, E. S., Tucker, D. L., Burke, D. L., Allam, S. S., Bechtol, K., Bernstein, G. M., Brout, D., Gruendl, R. A., Lasker, J., Smith, J. A., Wester, W. C., Yanny, B., Abbott, T. M. C., Aguena, M., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Rosell, A. Carnero, Carretero, J., Castander, F. J., Choi, A., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Giannini, G., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kuehn, K., Lahav, O., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Myles, J., Nord, B. D., Ogando, R. L. C., Palmese, A., Pieres, A., Malagón, A. A. Plazas, Raveri, M., Rodgríguez-Monroy, M., Sanchez, E., Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Varga, T. N., Vincenzi, M., Walker, A. R., Weaverdyck, N., Wiseman, P., Rykoff, E. S., Tucker, D. L., Burke, D. L., Allam, S. S., Bechtol, K., Bernstein, G. M., Brout, D., Gruendl, R. A., Lasker, J., Smith, J. A., Wester, W. C., Yanny, B., Abbott, T. M. C., Aguena, M., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Rosell, A. Carnero, Carretero, J., Castander, F. J., Choi, A., da Costa, L. N., Pereira, M. E. S., Davis, T. M., De Vicente, J., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Giannini, G., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kuehn, K., Lahav, O., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Myles, J., Nord, B. D., Ogando, R. L. C., Palmese, A., Pieres, A., Malagón, A. A. Plazas, Raveri, M., Rodgríguez-Monroy, M., Sanchez, E., Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Varga, T. N., Vincenzi, M., Walker, A. R., Weaverdyck, N., and Wiseman, P.
Abstract: This Technical Note presents a catalog of calibrated reference stars that was generated by the Forward Calibration Method (FGCM) pipeline (arXiv:1706.01542) as part of the FGCM photometric calibration of the full Dark Energy Survey (DES) 6-Year data set (Y6). This catalog provides DES grizY magnitudes for 17 million stars with i-band magnitudes mostly in the range 16 < i < 21 spread over the full DES footprint covering 5000 square degrees over the Southern Galactic Cap at galactic latitudes b < -20 degrees (plus a few outlying fields disconnected from the main survey footprint). These stars are calibrated to a uniformity of better than 1.8 milli-mag (0.18%) RMS over the survey area. The absolute calibration of the catalog is computed with reference to the STISNIC.007 spectrum of the Hubble Space Telescope CalSpec standard star C26202; including systematic errors, the absolute flux system is known at the approximately 1% level. As such, these stars provide a useful reference catalog for calibrating grizY-band or grizY-like band photometry in the Southern Hemisphere, particularly for observations within the DES footprint., Comment: 21 pages, 15 figures, Fermilab Technical Note. Official Data Access Site: https://des.ncsa.illinois.edu/releases/other ; Temporary Data Access Site: https://data.darkenergysurvey.org/public_calib/DES_6yr_CalibStarCat/index.html
Published: 2023

11. Ultracool dwarfs candidates based on six years of the Dark Energy Survey data

Author: Ponte, M. dal, Santiago, B., Rosell, A. Carnero, De Paris, L., Pace, A. B., Bechtol, K., Abbott, T. M. C., Aguena, M., Allam, S., Alves, O., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Kind, M. Carrasco, Carretero, J., Conselice, C., Costanzi, M., Desai, S., De Vicente, J., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kuehn, K., Kuropatkin, N., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Malagón, A. A. Plazas, Pieres, A., Raveri, M., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Weaverdyck, N., Ponte, M. dal, Santiago, B., Rosell, A. Carnero, De Paris, L., Pace, A. B., Bechtol, K., Abbott, T. M. C., Aguena, M., Allam, S., Alves, O., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D. L., Kind, M. Carrasco, Carretero, J., Conselice, C., Costanzi, M., Desai, S., De Vicente, J., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Gruendl, R. A., Gruen, D., Gutierrez, G., Hinton, S. R., Hollowood, D. L., James, D. J., Kuehn, K., Kuropatkin, N., Marshall, J. L., Mena-Fernández, J., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Malagón, A. A. Plazas, Pieres, A., Raveri, M., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Weaverdyck, N.
Abstract: We present a sample of 19,583 ultracool dwarf candidates brighter than z $\leq 23$ selected from the Dark Energy Survey DR2 coadd data matched to VHS DR6, VIKING DR5 and AllWISE covering $\sim$ 4,800 $deg^2$. The ultracool candidates were first pre-selected based on their (i-z), (z-Y), and (Y-J) colours. They were further classified using a method that compares their optical, near-infrared and mid-infrared colours against templates of M, L and T dwarfs. 14,099 objects are presented as new L and T candidates and the remaining objects are from the literature, including 5,342 candidates from our previous work. Using this new and deeper sample of ultracool dwarf candidates we also present: 20 new candidate members to nearby young moving groups (YMG) and associations, variable candidate sources and four new wide binary systems composed of two ultracool dwarfs. Finally, we also show the spectra of twelve new ultracool dwarfs discovered by our group and presented here for the first time. These spectroscopically confirmed objects are a sanity check of our selection of ultracool dwarfs and photometric classification method., Comment: 18 pages, 10 figures, 7 tables. Accepted for publication in MNRAS
Published: 2023
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12. Designing an Optimal Kilonova Search using DECam for Gravitational Wave Events

Author: Bom, C. R., Annis, J., Garcia, A., Palmese, A., Sherman, N., Soares-Santos, M., Santana-Silva, L., Morgan, R., Bechtol, K., Davis, T., Diehl, H. T., Allam, S. S., Bachmann, T. G., Fraga, B. M. O., Garcıa-Bellido, J., Gill, M. S. S., Herner, K., Kilpatrick, C. D., Makler, M., E., F. Olivares, Pereira, M. E. S., Pineda, J., Santos, A., Tucker, D. L., Wiesner, M. P., Aguena, M., Alves, O., Bacon, D., Bernardinelli, P. H., Bertin, E., Bocquet, S., Brooks, D., Kind, M. Carrasco, Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Everett, S., Ferrero, I., Frieman, J., Gatti, M., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Melchior, P., Mena-Fernandez, J., Menanteau, F., Pieres, A., Malagon, A. A. Plazas, Raveri, M., Rodriguez-Monroy, M., Sanchez, E., Santiago, B., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Weaverdyck, N., Bom, C. R., Annis, J., Garcia, A., Palmese, A., Sherman, N., Soares-Santos, M., Santana-Silva, L., Morgan, R., Bechtol, K., Davis, T., Diehl, H. T., Allam, S. S., Bachmann, T. G., Fraga, B. M. O., Garcıa-Bellido, J., Gill, M. S. S., Herner, K., Kilpatrick, C. D., Makler, M., E., F. Olivares, Pereira, M. E. S., Pineda, J., Santos, A., Tucker, D. L., Wiesner, M. P., Aguena, M., Alves, O., Bacon, D., Bernardinelli, P. H., Bertin, E., Bocquet, S., Brooks, D., Kind, M. Carrasco, Carretero, J., Conselice, C., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Everett, S., Ferrero, I., Frieman, J., Gatti, M., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Melchior, P., Mena-Fernandez, J., Menanteau, F., Pieres, A., Malagon, A. A. Plazas, Raveri, M., Rodriguez-Monroy, M., Sanchez, E., Santiago, B., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., and Weaverdyck, N.
Abstract: We address the problem of optimally identifying all kilonovae detected via gravitational wave emission in the upcoming LIGO/Virgo/KAGRA Collaboration observing run, O4, which is expected to be sensitive to a factor of $\sim 7$ more Binary Neutron Stars alerts than previously. Electromagnetic follow-up of all but the brightest of these new events will require $>1$ meter telescopes, for which limited time is available. We present an optimized observing strategy for the Dark Energy Camera during O4. We base our study on simulations of gravitational wave events expected for O4 and wide-prior kilonova simulations. We derive the detectabilities of events for realistic observing conditions. We optimize our strategy for confirming a kilonova while minimizing telescope time. For a wide range of kilonova parameters, corresponding to a fainter kilonova compared to GW170817/AT2017gfo we find that, with this optimal strategy, the discovery probability for electromagnetic counterparts with the Dark Energy Camera is $\sim 80\%$ at the nominal binary neutron star gravitational wave detection limit for the next LVK observing run (190 Mpc), which corresponds to a $\sim 30\%$ improvement compared to the strategy adopted during the previous observing run. For more distant events ($\sim 330$ Mpc), we reach a $\sim 60\%$ probability of detection, a factor of $\sim 2$ increase. For a brighter kilonova model dominated by the blue component that reproduces the observations of GW170817/AT2017gfo, we find that we can reach $\sim 90\%$ probability of detection out to 330 Mpc, representing an increase of $\sim 20 \%$, while also reducing the total telescope time required to follow-up events by $\sim 20\%$., Comment: 26 pages, 11 figures, accepted by ApJ
Published: 2023

13. Environmental Quenching of Low Surface Brightness Galaxies near Milky Way mass Hosts

Author: Bhattacharyya, J., Peter, A. H. G., Martini, P., Mutlu-Pakdil, B., Drlica-Wagner, A., Pace, A. B., Strigari, L. E., Cheng, Y. -T., Roberts, D., Tanoglidis, D., Aguena, M., Alves, O., Andrade-Oliveira, F., Bacon, D., Brooks, D., Rosell, A. Carnero, Carretero, J., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Doel, P., Ferrero, I., Frieman, J., García-Bellido, J., Giannini, G., Gruen, D., Gruendl, R. A., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Marshall, J. L., Mena-Fernández, J., Miquel, R., Palmese, A., Pieres, A., Malagón, A. A. Plazas, Sanchez, E., Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Vincenzi, M., Walker, A. R., Weaverdyck, N., Wiseman, P., Bhattacharyya, J., Peter, A. H. G., Martini, P., Mutlu-Pakdil, B., Drlica-Wagner, A., Pace, A. B., Strigari, L. E., Cheng, Y. -T., Roberts, D., Tanoglidis, D., Aguena, M., Alves, O., Andrade-Oliveira, F., Bacon, D., Brooks, D., Rosell, A. Carnero, Carretero, J., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Doel, P., Ferrero, I., Frieman, J., García-Bellido, J., Giannini, G., Gruen, D., Gruendl, R. A., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Marshall, J. L., Mena-Fernández, J., Miquel, R., Palmese, A., Pieres, A., Malagón, A. A. Plazas, Sanchez, E., Santiago, B., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Vincenzi, M., Walker, A. R., Weaverdyck, N., and Wiseman, P.
Abstract: Low Surface Brightness Galaxies (LSBGs) are excellent probes of quenching and other environmental processes near massive galaxies. We study an extensive sample of LSBGs near massive hosts in the local universe that are distributed across a diverse range of environments. The LSBGs with surface-brightness $\mu_{\rm eff,g}> $24.2 mag arcsec$^{-2}$ are drawn from the Dark Energy Survey Year 3 catalog while the hosts with masses $9.0< log(M_{\star}/M_{\odot})< 11.0$ comparable to the Milky Way and the Large Magellanic Cloud are selected from the z0MGS sample. We study the projected radial density profiles of LSBGs as a function of their color and surface brightness around hosts in both the rich Fornax-Eridanus cluster environment and the low-density field. We detect an overdensity with respect to the background density, out to 2.5 times the virial radius for both hosts in the cluster environment and the isolated field galaxies. When the LSBG sample is split by $g-i$ color or surface brightness $\mu_{\rm eff,g}$, we find the LSBGs closer to their hosts are significantly redder and brighter, like their high surface-brightness counterparts. The LSBGs form a clear 'red sequence' in both the cluster and isolated environments that is visible beyond the virial radius of the hosts. This suggests a pre-processing of infalling LSBGs and a quenched backsplash population around both host samples. However, the relative prominence of the 'blue cloud' feature implies that pre-processing is ongoing near the isolated hosts compared to the cluster hosts., Comment: 22 pages, 7 figures
Published: 2023

14. The mass and galaxy distribution around SZ-selected clusters

Author: Shin, T, Jain, B, Adhikari, S, Baxter, E, Chang, C, Pandey, S, Salcedo, A, Weinberg, D, Amsellem, A, Battaglia, N, Belyakov, M, Dacunha, T, Goldstein, S, Kravtsov, A, Varga, T, Abbott, T, Aguena, M, Alarcon, A, Allam, S, Amon, A, Andrade-Oliveira, F, Annis, J, Bacon, D, Bechtol, K, Becker, M, Bernstein, G, Bertin, E, Bocquet, S, Bond, J, Brooks, D, Buckley-Geer, E, Burke, D, Campos, A, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Chen, R, Choi, A, Costanzi, M, da Costa, L, Derose, J, Desai, S, de Vicente, J, Devlin, M, Diehl, H, Dietrich, J, Dodelson, S, Doel, P, Doux, C, Drlica-Wagner, A, Eckert, K, Elvin-Poole, J, Everett, S, Ferraro, S, Ferrero, I, Ferte, A, Flaugher, B, Frieman, J, Gallardo, P, Gatti, M, Gaztanaga, E, Gerdes, D, Gruen, D, Gruendl, R, Gutierrez, G, Harrison, I, Hartley, W, Hill, J, Hilton, M, Hinton, S, Hollowood, D, Hughes, J, James, D, Jarvis, M, Jeltema, T, Koopman, B, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Lokken, M, Maccrann, N, Madhavacheril, M, Maia, M, Mccullough, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Mohr, J, Moodley, K, Morgan, R, Myles, J, Nati, F, Navarro-Alsina, A, Niemack, M, Ogando, R, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Pereira, M, Pieres, A, Plazas Malagon, A, Prat, J, Raveri, M, Rodriguez-Monroy, M, Rollins, R, Romer, A, Rykoff, E, Salatino, M, Sanchez, C, Sanchez, E, Santiago, B, Scarpine, V, Schillaci, A, Secco, L, Serrano, S, Sevilla-Noarbe, I, Sheldon, E, Sherwin, B, Sifon, C, Smith, M, Soares-Santos, M, Staggs, S, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Troxel, M, Tutusaus, I, Vavagiakis, E, Weller, J, Wollack, E, Yanny, B, Yin, B, Zhang, Y, Shin T., Jain B., Adhikari S., Baxter E. J., Chang C., Pandey S., Salcedo A., Weinberg D. H., Amsellem A., Battaglia N., Belyakov M., Dacunha T., Goldstein S., Kravtsov A. V., Varga T. N., Abbott T. M. C., Aguena M., Alarcon A., Allam S., Amon A., Andrade-Oliveira F., Annis J., Bacon D., Bechtol K., Becker M. R., Bernstein G. M., Bertin E., Bocquet S., Bond J. R., Brooks D., Buckley-Geer E., Burke D. L., Campos A., Carnero Rosell A., Carrasco Kind M., Carretero J., Chen R., Choi A., Costanzi M., da Costa L. N., DeRose J., Desai S., de Vicente J., Devlin M. J., Diehl H. T., Dietrich J. P., Dodelson S., Doel P., Doux C., Drlica-Wagner A., Eckert K., Elvin-Poole J., Everett S., Ferraro S., Ferrero I., Ferte A., Flaugher B., Frieman J., Gallardo P. A., Gatti M., Gaztanaga E., Gerdes D. W., Gruen D., Gruendl R. A., Gutierrez G., Harrison I., Hartley W. G., Hill J. C., Hilton M., Hinton S. R., Hollowood D. L., Hughes J. P., James D. J., Jarvis M., Jeltema T., Koopman B. J., Krause E., Kuehn K., Kuropatkin N., Lahav O., Lima M., Lokken M., MacCrann N., Madhavacheril M. S., Maia M. A. G., McCullough J., McMahon J., Melchior P., Menanteau F., Miquel R., Mohr J. J., Moodley K., Morgan R., Myles J., Nati F., Navarro-Alsina A., Niemack M. D., Ogando R. L. C., Page L. A., Palmese A., Partridge B., Paz-Chinchon F., Pereira M. E. S., Pieres A., Plazas Malagon A. A., Prat J., Raveri M., Rodriguez-Monroy M., Rollins R. P., Romer A. K., Rykoff E. S., Salatino M., Sanchez C., Sanchez E., Santiago B., Scarpine V., Schillaci A., Secco L. F., Serrano S., Sevilla-Noarbe I., Sheldon E., Sherwin B. D., Sifon C., Smith M., Soares-Santos M., Staggs S. T., Suchyta E., Swanson M. E. C., Tarle G., Thomas D., To C., Troxel M. A., Tutusaus I., Vavagiakis E. M., Weller J., Wollack E. J., Yanny B., Yin B., Zhang Y., Shin, T, Jain, B, Adhikari, S, Baxter, E, Chang, C, Pandey, S, Salcedo, A, Weinberg, D, Amsellem, A, Battaglia, N, Belyakov, M, Dacunha, T, Goldstein, S, Kravtsov, A, Varga, T, Abbott, T, Aguena, M, Alarcon, A, Allam, S, Amon, A, Andrade-Oliveira, F, Annis, J, Bacon, D, Bechtol, K, Becker, M, Bernstein, G, Bertin, E, Bocquet, S, Bond, J, Brooks, D, Buckley-Geer, E, Burke, D, Campos, A, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, Chen, R, Choi, A, Costanzi, M, da Costa, L, Derose, J, Desai, S, de Vicente, J, Devlin, M, Diehl, H, Dietrich, J, Dodelson, S, Doel, P, Doux, C, Drlica-Wagner, A, Eckert, K, Elvin-Poole, J, Everett, S, Ferraro, S, Ferrero, I, Ferte, A, Flaugher, B, Frieman, J, Gallardo, P, Gatti, M, Gaztanaga, E, Gerdes, D, Gruen, D, Gruendl, R, Gutierrez, G, Harrison, I, Hartley, W, Hill, J, Hilton, M, Hinton, S, Hollowood, D, Hughes, J, James, D, Jarvis, M, Jeltema, T, Koopman, B, Krause, E, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Lokken, M, Maccrann, N, Madhavacheril, M, Maia, M, Mccullough, J, Mcmahon, J, Melchior, P, Menanteau, F, Miquel, R, Mohr, J, Moodley, K, Morgan, R, Myles, J, Nati, F, Navarro-Alsina, A, Niemack, M, Ogando, R, Page, L, Palmese, A, Partridge, B, Paz-Chinchon, F, Pereira, M, Pieres, A, Plazas Malagon, A, Prat, J, Raveri, M, Rodriguez-Monroy, M, Rollins, R, Romer, A, Rykoff, E, Salatino, M, Sanchez, C, Sanchez, E, Santiago, B, Scarpine, V, Schillaci, A, Secco, L, Serrano, S, Sevilla-Noarbe, I, Sheldon, E, Sherwin, B, Sifon, C, Smith, M, Soares-Santos, M, Staggs, S, Suchyta, E, Swanson, M, Tarle, G, Thomas, D, To, C, Troxel, M, Tutusaus, I, Vavagiakis, E, Weller, J, Wollack, E, Yanny, B, Yin, B, Zhang, Y, Shin T., Jain B., Adhikari S., Baxter E. J., Chang C., Pandey S., Salcedo A., Weinberg D. H., Amsellem A., Battaglia N., Belyakov M., Dacunha T., Goldstein S., Kravtsov A. V., Varga T. N., Abbott T. M. C., Aguena M., Alarcon A., Allam S., Amon A., Andrade-Oliveira F., Annis J., Bacon D., Bechtol K., Becker M. R., Bernstein G. M., Bertin E., Bocquet S., Bond J. R., Brooks D., Buckley-Geer E., Burke D. L., Campos A., Carnero Rosell A., Carrasco Kind M., Carretero J., Chen R., Choi A., Costanzi M., da Costa L. N., DeRose J., Desai S., de Vicente J., Devlin M. J., Diehl H. T., Dietrich J. P., Dodelson S., Doel P., Doux C., Drlica-Wagner A., Eckert K., Elvin-Poole J., Everett S., Ferraro S., Ferrero I., Ferte A., Flaugher B., Frieman J., Gallardo P. A., Gatti M., Gaztanaga E., Gerdes D. W., Gruen D., Gruendl R. A., Gutierrez G., Harrison I., Hartley W. G., Hill J. C., Hilton M., Hinton S. R., Hollowood D. L., Hughes J. P., James D. J., Jarvis M., Jeltema T., Koopman B. J., Krause E., Kuehn K., Kuropatkin N., Lahav O., Lima M., Lokken M., MacCrann N., Madhavacheril M. S., Maia M. A. G., McCullough J., McMahon J., Melchior P., Menanteau F., Miquel R., Mohr J. J., Moodley K., Morgan R., Myles J., Nati F., Navarro-Alsina A., Niemack M. D., Ogando R. L. C., Page L. A., Palmese A., Partridge B., Paz-Chinchon F., Pereira M. E. S., Pieres A., Plazas Malagon A. A., Prat J., Raveri M., Rodriguez-Monroy M., Rollins R. P., Romer A. K., Rykoff E. S., Salatino M., Sanchez C., Sanchez E., Santiago B., Scarpine V., Schillaci A., Secco L. F., Serrano S., Sevilla-Noarbe I., Sheldon E., Sherwin B. D., Sifon C., Smith M., Soares-Santos M., Staggs S. T., Suchyta E., Swanson M. E. C., Tarle G., Thomas D., To C., Troxel M. A., Tutusaus I., Vavagiakis E. M., Weller J., Wollack E. J., Yanny B., Yin B., and Zhang Y.
Abstract: We present measurements of the radial profiles of the mass and galaxy number density around Sunyaev–Zel’dovich (SZ)-selected clusters using both weak lensing and galaxy counts. The clusters are selected from the Atacama Cosmology Telescope Data Release 5 and the galaxies from the Dark Energy Survey Year 3 data set. With signal-to-noise ratio of 62 (45) for galaxy (weak lensing) profiles over scales of about 0.2–20 h-1 Mpc, these are the highest precision measurements for SZ-selected clusters to date. Because SZ selection closely approximates mass selection, these measurements enable several tests of theoretical models of the mass and light distribution around clusters. Our main findings are: (1) The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations. (2) The full mass profile is also consistent with the simulations. (3) The shapes of the galaxy and lensing profiles are remarkably similar for our sample over the entire range of scales, from well inside the cluster halo to the quasilinear regime. We measure the dependence of the profile shapes on the galaxy sample, redshift, and cluster mass. We extend the Diemer & Kravtsov model for the cluster profiles to the linear regime using perturbation theory and show that it provides a good match to the measured profiles. We also compare the measured profiles to predictions of the standard halo model and simulations that include hydrodynamics. Applications of these results to cluster mass estimation, cosmology, and astrophysics are discussed.
Published: 2021

15. Probing Galaxy Evolution in Massive Clusters Using ACT and DES: Splashback as a Cosmic Clock

Author: Adhikari, S, Shin, T, Jain, B, Hilton, M, Baxter, E, Chang, C, Wechsler, R, Battaglia, N, Bond, J, Bocquet, S, Choi, S, Derose, J, Devlin, M, Dunkley, J, Evrard, A, Ferraro, S, Hill, J, Hughes, J, Gallardo, P, Lokken, M, Macinnis, A, Madhavacheril, M, Mcmahon, J, Nati, F, Newburgh, L, Niemack, M, Page, L, Palmese, A, Partridge, B, Rozo, E, Rykoff, E, Salatino, M, Schillaci, A, Sehgal, N, Sifon, C, To, C, Wollack, E, Wu, H, Xu, Z, Aguena, M, Allam, S, Amon, A, Annis, J, Avila, S, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Burke, D, Rosell, A, Kind, M, Carretero, J, Castander, F, Choi, A, Costanzi, M, Da Costa, L, Vicente, J, Desai, S, Diehl, T, Doel, P, Everett, S, Ferrero, I, Ferte, A, Flaugher, B, Fosalba, P, Frieman, J, Garcia-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, R, Gschwend, J, Gutierrez, G, Hartley, W, Hinton, S, Hollowood, D, Honscheid, K, James, D, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, M, Marshall, J, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, L. C. Ogando, R, Paz-Chinchon, F, Malagon, A, Sanchez, E, Santiago, B, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, E. C. Swanson, M, Varga, T, Wilkinson, R, Zhang, Y, Austermann, J, Beall, J, Becker, D, Denison, E, Duff, S, Hilton, G, Hubmayr, J, Ullom, J, Lanen, J, Vale, L, Adhikari S., Shin T. -H., Jain B., Hilton M., Baxter E., Chang C., Wechsler R. H., Battaglia N., Bond J. R., Bocquet S., Choi S. K., Derose J., Devlin M., Dunkley J., Evrard A. E., Ferraro S., Hill J. C., Hughes J. P., Gallardo P. A., Lokken M., Macinnis A., Madhavacheril M. S., McMahon J., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Palmese A., Partridge B., Rozo E., Rykoff E., Salatino M., Schillaci A., Sehgal N., Sifon C., To C. -H., Wollack E., Wu H. -Y., Xu Z., Aguena M., Allam S., Amon A., Annis J., Avila S., Bacon D., Bertin E., Bhargava S., Brooks D., Burke D. L., Rosell A. C., Kind M. C., Carretero J., Castander F. J., Choi A., Costanzi M., Da Costa L. N., Vicente J. D., Desai S., Diehl T. H., Doel P., Everett S., Ferrero I., Ferte A., Flaugher B., Fosalba P., Frieman J., Garcia-Bellido J., Gaztanaga E., Gruen D., Gruendl R. A., Gschwend J., Gutierrez G., Hartley W. G., Hinton S. R., Hollowood D. L., Honscheid K., James D. J., Jeltema T., Kuehn K., Kuropatkin N., Lahav O., Lima M., Maia M. A. G., Marshall J. L., Martini P., Melchior P., Menanteau F., Miquel R., Morgan R., L. C. Ogando R., Paz-Chinchon F., Malagon A. P., Sanchez E., Santiago B., Scarpine V., Serrano S., Sevilla-Noarbe I., Smith M., Soares-Santos M., Suchyta E., E. C. Swanson M., Varga T. N., Wilkinson R. D., Zhang Y., Austermann J. E., Beall J. A., Becker D. T., Denison E. V., Duff S. M., Hilton G. C., Hubmayr J., Ullom J. N., Lanen J. V., Vale L. R., Adhikari, S, Shin, T, Jain, B, Hilton, M, Baxter, E, Chang, C, Wechsler, R, Battaglia, N, Bond, J, Bocquet, S, Choi, S, Derose, J, Devlin, M, Dunkley, J, Evrard, A, Ferraro, S, Hill, J, Hughes, J, Gallardo, P, Lokken, M, Macinnis, A, Madhavacheril, M, Mcmahon, J, Nati, F, Newburgh, L, Niemack, M, Page, L, Palmese, A, Partridge, B, Rozo, E, Rykoff, E, Salatino, M, Schillaci, A, Sehgal, N, Sifon, C, To, C, Wollack, E, Wu, H, Xu, Z, Aguena, M, Allam, S, Amon, A, Annis, J, Avila, S, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Burke, D, Rosell, A, Kind, M, Carretero, J, Castander, F, Choi, A, Costanzi, M, Da Costa, L, Vicente, J, Desai, S, Diehl, T, Doel, P, Everett, S, Ferrero, I, Ferte, A, Flaugher, B, Fosalba, P, Frieman, J, Garcia-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, R, Gschwend, J, Gutierrez, G, Hartley, W, Hinton, S, Hollowood, D, Honscheid, K, James, D, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, M, Marshall, J, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, L. C. Ogando, R, Paz-Chinchon, F, Malagon, A, Sanchez, E, Santiago, B, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, E. C. Swanson, M, Varga, T, Wilkinson, R, Zhang, Y, Austermann, J, Beall, J, Becker, D, Denison, E, Duff, S, Hilton, G, Hubmayr, J, Ullom, J, Lanen, J, Vale, L, Adhikari S., Shin T. -H., Jain B., Hilton M., Baxter E., Chang C., Wechsler R. H., Battaglia N., Bond J. R., Bocquet S., Choi S. K., Derose J., Devlin M., Dunkley J., Evrard A. E., Ferraro S., Hill J. C., Hughes J. P., Gallardo P. A., Lokken M., Macinnis A., Madhavacheril M. S., McMahon J., Nati F., Newburgh L. B., Niemack M. D., Page L. A., Palmese A., Partridge B., Rozo E., Rykoff E., Salatino M., Schillaci A., Sehgal N., Sifon C., To C. -H., Wollack E., Wu H. -Y., Xu Z., Aguena M., Allam S., Amon A., Annis J., Avila S., Bacon D., Bertin E., Bhargava S., Brooks D., Burke D. L., Rosell A. C., Kind M. C., Carretero J., Castander F. J., Choi A., Costanzi M., Da Costa L. N., Vicente J. D., Desai S., Diehl T. H., Doel P., Everett S., Ferrero I., Ferte A., Flaugher B., Fosalba P., Frieman J., Garcia-Bellido J., Gaztanaga E., Gruen D., Gruendl R. A., Gschwend J., Gutierrez G., Hartley W. G., Hinton S. R., Hollowood D. L., Honscheid K., James D. J., Jeltema T., Kuehn K., Kuropatkin N., Lahav O., Lima M., Maia M. A. G., Marshall J. L., Martini P., Melchior P., Menanteau F., Miquel R., Morgan R., L. C. Ogando R., Paz-Chinchon F., Malagon A. P., Sanchez E., Santiago B., Scarpine V., Serrano S., Sevilla-Noarbe I., Smith M., Soares-Santos M., Suchyta E., E. C. Swanson M., Varga T. N., Wilkinson R. D., Zhang Y., Austermann J. E., Beall J. A., Becker D. T., Denison E. V., Duff S. M., Hilton G. C., Hubmayr J., Ullom J. N., Lanen J. V., and Vale L. R.
Abstract: We measure the projected number density profiles of galaxies and the splashback feature in clusters selected by the Sunyaev-Zel'dovich effect from the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxies observed by the Dark Energy Survey (DES). The splashback radius is consistent with CDM-only simulations and is located at 2.4-0.4+0.3 Mpc h-1. We split the galaxies on color and find significant differences in their profile shapes. Red and green-valley galaxies show a splashback-like minimum in their slope profile consistent with theory, while the bluest galaxies show a weak feature at a smaller radius. We develop a mapping of galaxies to subhalos in simulations and assign colors based on infall time onto their hosts. We find that the shift in location of the steepest slope and different profile shapes can be mapped to the average time of infall of galaxies of different colors. The steepest slope traces a discontinuity in the phase space of dark matter halos. By relating spatial profiles to infall time, we can use splashback as a clock to understand galaxy quenching. We find that red galaxies have on average been in clusters over 3.2 Gyr, green galaxies about 2.2 Gyr, while blue galaxies have been accreted most recently and have not reached apocenter. Using the full radial profiles, we fit a simple quenching model and find that the onset of galaxy quenching occurs after a delay of about a gigayear and that galaxies quench rapidly thereafter with an exponential timescale of 0.6 Gyr.
Published: 2021

16. Análisis formal y estructural de la iglesia de Santa María del Camino en Santiago de Compostela

Author: Franco Taboada, José Antonio, Tarrío Carrodeguas, Santiago B., Franco Taboada, José Antonio, and Tarrío Carrodeguas, Santiago B.
Abstract: [Resumen] Esta investigación tiene como principal objetivo determinar la situación estructural de la iglesia de Santa María del Camino, en Santiago de Compostela, con especial énfasis en las deformaciones de sus arcos. Para lograrlo, se llevó a cabo un exhaustivo trabajo de levantamiento gráfico, que mediante la combinación de distintas técnicas de captación y restitución, nos permitió definir de un modo preciso la forma, las dimensiones y la posición en el espacio del objeto de estudio. El artículo describe la metodología y los resultados obtenidos en cada etapa, que se ilustran a través de una completa selección de imágenes que van desde los primeros bocetos a mano alzada hasta las ortoimágenes generadas desde los modelos 3D (nube de puntos y malla con textura). Constituye además un ejemplo práctico de cómo la fotogrametría puede registrar la complejidad tridimensional de las geometrías deformadas que caracterizan a los edificios históricos.
Published: 2022

17. The DECam Local Volume Exploration Survey Data Release 2

Author: Drlica-Wagner, A., Ferguson, P. S., Adamów, M., Aguena, M., Andrade-Oliveira, F., Bacon, D., Bechtol, K., Bell, E. F., Bertin, E., Bilaji, P., Bocquet, S., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Carlin, J. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cerny, W., Chang, C., Choi, Y., Conselice, C., Costanzi, M., Crnojević, D., da Costa, L. N., De Vicente, J., Desai, S., Esteves, J., Everett, S., Ferrero, I., Fitzpatrick, M., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hernandez-Lang, D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, A. K., Jacques, A., James, D. J., Johnson, M. D., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lidman, C., Lin, H., March, M., Marshall, J. L., Martínez-Delgado, D., Martínez-Vázquez, C. E., Massana, P., Mau, S., McNanna, M., Melchior, P., Menanteau, F., Miller, A. E., Miquel, R., Mohr, J. J., Morgan, R., Mutlu-Pakdil, B., Muñoz, R. R., Neilsen, E. H., Nidever, D. L., Nikutta, R., Castellon, J. L. Nilo, Noël, N. E. D., Ogando, R. L. C., Olsen, K. A. G., Pace, A. B., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Prat, J., Riley, A. H., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sako, M., Sakowska, J. D., Sanchez, E., Sánchez, F. J., Sand, D. J., Santana-Silva, L., Santiago, B., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Simon, J. D., Smith, M., Soares-Santos, M., Stringfellow, G. S., Suchyta, E., Suson, D. J., Tan, C. Y., Tarle, G., Tavangar, K., Thomas, D., To, C., Tollerud, E. J., Troxel, M. A., Tucker, D. L., Varga, T. N., Vivas, A. K., Walker, A. R., Weller, J., Wilkinson, R. D., Wu, J. F., Yanny, B., Zaborowski, E., Zenteno, A., Drlica-Wagner, A., Ferguson, P. S., Adamów, M., Aguena, M., Andrade-Oliveira, F., Bacon, D., Bechtol, K., Bell, E. F., Bertin, E., Bilaji, P., Bocquet, S., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Carlin, J. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cerny, W., Chang, C., Choi, Y., Conselice, C., Costanzi, M., Crnojević, D., da Costa, L. N., De Vicente, J., Desai, S., Esteves, J., Everett, S., Ferrero, I., Fitzpatrick, M., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hernandez-Lang, D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, A. K., Jacques, A., James, D. J., Johnson, M. D., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lidman, C., Lin, H., March, M., Marshall, J. L., Martínez-Delgado, D., Martínez-Vázquez, C. E., Massana, P., Mau, S., McNanna, M., Melchior, P., Menanteau, F., Miller, A. E., Miquel, R., Mohr, J. J., Morgan, R., Mutlu-Pakdil, B., Muñoz, R. R., Neilsen, E. H., Nidever, D. L., Nikutta, R., Castellon, J. L. Nilo, Noël, N. E. D., Ogando, R. L. C., Olsen, K. A. G., Pace, A. B., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Prat, J., Riley, A. H., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sako, M., Sakowska, J. D., Sanchez, E., Sánchez, F. J., Sand, D. J., Santana-Silva, L., Santiago, B., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Simon, J. D., Smith, M., Soares-Santos, M., Stringfellow, G. S., Suchyta, E., Suson, D. J., Tan, C. Y., Tarle, G., Tavangar, K., Thomas, D., To, C., Tollerud, E. J., Troxel, M. A., Tucker, D. L., Varga, T. N., Vivas, A. K., Walker, A. R., Weller, J., Wilkinson, R. D., Wu, J. F., Yanny, B., Zaborowski, E., and Zenteno, A.
Abstract: We present the second public data release (DR2) from the DECam Local Volume Exploration survey (DELVE). DELVE DR2 combines new DECam observations with archival DECam data from the Dark Energy Survey, the DECam Legacy Survey, and other DECam community programs. DELVE DR2 consists of ~160,000 exposures that cover >21,000 deg^2 of the high Galactic latitude (|b| > 10 deg) sky in four broadband optical/near-infrared filters (g, r, i, z). DELVE DR2 provides point-source and automatic aperture photometry for ~2.5 billion astronomical sources with a median 5{\sigma} point-source depth of g=24.3, r=23.9, i=23.5, and z=22.8 mag. A region of ~17,000 deg^2 has been imaged in all four filters, providing four-band photometric measurements for ~618 million astronomical sources. DELVE DR2 covers more than four times the area of the previous DELVE data release and contains roughly five times as many astronomical objects. DELVE DR2 is publicly available via the NOIRLab Astro Data Lab science platform., Comment: 23 pages, 10 figures, 5 tables; to be submitted to AAS Journals; public data release at https://datalab.noirlab.edu/delve/. arXiv admin note: substantial text overlap with arXiv:2103.07476
Published: 2022

18. La construcción del revestimiento en la obra de Álvaro Siza: la línea como materia, la geometría como construcción: análisis pormenorizado de dos de sus proyectos

Author: Franco Taboada, José Antonio, Tarrío Carrodeguas, Santiago B. (Titor), Seoane González, José Carlos, Franco Taboada, José Antonio, Tarrío Carrodeguas, Santiago B. (Titor), and Seoane González, José Carlos
Abstract: [Resumo] Mediante a análise de dous proxectos moi diferentes — case contrapostos — canto ao seu programa (unha facultade universitaria fronte a un restaurante), canto ao instrumento utilizado para a súa definición (debuxos a man fronte a debuxos realizados con programas de computadora) e canto ao seu resultado final (un construído e outro non), como son a Facultade de Xornalismo de Santiago de Compostela e o restaurante Pai Ramiro, no Porto, estúdase a existencia dunha estrutura xeométrica tridimensional como soporte da definición dos espazos e dos seus detalles construtivos e de que maneira esa case imperceptible malla xeométrica serve para definir a escala maior e a máis pequena, o macro e o microcosmos nestes dous proxectos e, en transposición, na obra do recoñecido arquitecto portugués Álvaro Siza., [Resumen] Mediante el análisis de dos proyectos muy diferentes — casi contrapuestos — en cuanto a su programa (una facultad universitaria frente a un restaurante), en cuanto al instrumento utilizado para su definición (dibujos a mano frente a dibujos realizados con programas de ordenador) y en cuanto a su resultado final (uno construido y otro no), como son la Facultad de Periodismo de Santiago de Compostela y el restaurante Pai Ramiro, en Oporto, se estudia la existencia de una estructura geométrica tridimensional como soporte de la definición de los espacios y de sus detalles constructivos y cómo esa casi imperceptible malla geométrica sirve para definir la escala mayor y la más pequeña, el macro y el microcosmos en estos dos proyectos y, en transposición, en la obra del reconocido arquitecto portugués Álvaro Siza., [Abstract] Through the analysis of two very different, almost opposing projects, in terms of their functional — a university faculty versus a restaurant —, in terms of the instrument used for their definition — hand drawings versus drawings made with computer software —, and in terms of their final result — one built and the other not built — such as the Faculty of Journalism in Santiago de Compostela (Spain) and the Pai Ramiro restaurant in Porto (Portugal), the existence of a three-dimensional geometric structure is analyzed as a support for the definition of the spaces and their construction details and how this almost imperceptible geometric grid serves to define the larger and smaller scale, the macro and microcosm in these two projects and in transposition in the work of the prestigious Portuguese architect Álvaro Siza.
Published: 2022

19. Grupo de Bioinformática (GdT-BIOINFO21): Actualización en el análisis de datos de NGS para el Diagnóstico. La importancia de ¿compartir conocimiento?

Author: Mínguez P., Pérez-Florido J., Álvarez-Mora M.I., Peña-Chillet M., Rodríguez-Santiago B., Castejón-Fernández N., Fernández S., Martín Y., López D., Rojano E., Seoane P., Fernández-Rueda J. L., Fernández G., del Pozo A., Arroyo A., Maynou, J., Bravo N., Dopazo J., Ortuño F., Tejedor J.R., Morte, B., Mínguez P., Pérez-Florido J., Álvarez-Mora M.I., Peña-Chillet M., Rodríguez-Santiago B., Castejón-Fernández N., Fernández S., Martín Y., López D., Rojano E., Seoane P., Fernández-Rueda J. L., Fernández G., del Pozo A., Arroyo A., Maynou, J., Bravo N., Dopazo J., Ortuño F., Tejedor J.R., and Morte, B.
Published: 2022

20. Timing the r-Process Enrichment of the Ultra-Faint Dwarf Galaxy Reticulum II

Author: Simon, Joshua D., Brown, Thomas M., Mutlu-Pakdil, Burçin, Ji, Alexander P., Drlica-Wagner, Alex, Avila, Roberto J., Martínez-Vázquez, Clara E., Li, Ting S., Balbinot, Eduardo, Bechtol, Keith, Frebel, Anna, Geha, Marla, Hansen, Terese T., James, David J., Pace, Andrew B., Aguena, M., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gatti, M., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuehn, K., Kuropatkin, N., Marshall, J. L., Mena-Fernández, J., Miquel, R., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Raveri, M., Rodriguez-Monroy, M., Sanchez, E., Santiago, B., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Vincenzi, M., Weaverdyck, N., Wilkinson, R. D., Simon, Joshua D., Brown, Thomas M., Mutlu-Pakdil, Burçin, Ji, Alexander P., Drlica-Wagner, Alex, Avila, Roberto J., Martínez-Vázquez, Clara E., Li, Ting S., Balbinot, Eduardo, Bechtol, Keith, Frebel, Anna, Geha, Marla, Hansen, Terese T., James, David J., Pace, Andrew B., Aguena, M., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Doel, P., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gatti, M., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuehn, K., Kuropatkin, N., Marshall, J. L., Mena-Fernández, J., Miquel, R., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Raveri, M., Rodriguez-Monroy, M., Sanchez, E., Santiago, B., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Vincenzi, M., Weaverdyck, N., and Wilkinson, R. D.
Abstract: The ultra-faint dwarf galaxy Reticulum II (Ret II) exhibits a unique chemical evolution history, with 72 +10/-12% of its stars strongly enhanced in r-process elements. We present deep Hubble Space Telescope photometry of Ret II and analyze its star formation history. As in other ultra-faint dwarfs, the color-magnitude diagram is best fit by a model consisting of two bursts of star formation. If we assume that the bursts were instantaneous, then the older burst occurred around the epoch of reionization and formed ~80% of the stars in the galaxy, while the remainder of the stars formed ~3 Gyr later. When the bursts are allowed to have nonzero durations we obtain slightly better fits. The best-fitting model in this case consists of two bursts beginning before reionization, with approximately half the stars formed in a short (100 Myr) burst and the other half in a more extended period lasting 2.6 Gyr. Considering the full set of viable star formation history models, we find that 28% of the stars formed within 500 +/- 200 Myr of the onset of star formation. The combination of the star formation history and the prevalence of r-process-enhanced stars demonstrates that the r-process elements in Ret II must have been synthesized early in its initial star-forming phase. We therefore constrain the delay time between the formation of the first stars in Ret II and the r-process nucleosynthesis to be less than 500 Myr. This measurement rules out an r-process source with a delay time of several Gyr or more such as GW170817., Comment: 14 pages, 5 figures, 1 table. Accepted for publication in ApJ
Published: 2022
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21. Identification of Galaxy-Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning

Author: Zaborowski, E. A., Drlica-Wagner, A., Ashmead, F., Wu, J. F., Morgan, R., Bom, C. R., Shajib, A. J., Birrer, S., Cerny, W., Buckley-Geer, L., Mutlu-Pakdil, B., Ferguson, P. S., Glazebrook, K., Lozano, S. J. Gonzalez, Gordon, Y., Martinez, M., Manwadkar, V., O'Donnell, J., Poh, J., Riley, A., Sakowska, J. D., Santana-Silva, L., Santiago, B. X., Sluse, D., Tan, C. Y., Tollerud, E. J., Verma, A., Carballo-Bello, J. A., Choi, Y., James, D. J., Kuropatkin, N., Martínez-Vázquez, C. E., Nidever, D. L., Castellon, J. L. Nilo, Noël, N. E. D., Olsen, K. A. G., Pace, A. B., Mau, S., Yanny, B., Zenteno, A., Abbott, T. M. C., Aguena, M., Alves, O., Andrade-Oliveira, F., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Conselice, C. J., Costanzi, M., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuehn, K., Lin, H., Marshall, J. L., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Prat, J., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., To, C., Weaverdyck, N., Zaborowski, E. A., Drlica-Wagner, A., Ashmead, F., Wu, J. F., Morgan, R., Bom, C. R., Shajib, A. J., Birrer, S., Cerny, W., Buckley-Geer, L., Mutlu-Pakdil, B., Ferguson, P. S., Glazebrook, K., Lozano, S. J. Gonzalez, Gordon, Y., Martinez, M., Manwadkar, V., O'Donnell, J., Poh, J., Riley, A., Sakowska, J. D., Santana-Silva, L., Santiago, B. X., Sluse, D., Tan, C. Y., Tollerud, E. J., Verma, A., Carballo-Bello, J. A., Choi, Y., James, D. J., Kuropatkin, N., Martínez-Vázquez, C. E., Nidever, D. L., Castellon, J. L. Nilo, Noël, N. E. D., Olsen, K. A. G., Pace, A. B., Mau, S., Yanny, B., Zenteno, A., Abbott, T. M. C., Aguena, M., Alves, O., Andrade-Oliveira, F., Bocquet, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Conselice, C. J., Costanzi, M., Pereira, M. E. S., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gruen, D., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuehn, K., Lin, H., Marshall, J. L., Melchior, P., Mena-Fernández, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Pieres, A., Malagón, A. A. Plazas, Prat, J., Rodriguez-Monroy, M., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., To, C., and Weaverdyck, N.
Abstract: We perform a search for galaxy-galaxy strong lens systems using a convolutional neural network (CNN) applied to imaging data from the first public data release of the DECam Local Volume Exploration Survey (DELVE), which contains $\sim 520$ million astronomical sources covering $\sim 4,000$ $\mathrm{deg}^2$ of the southern sky to a $5\sigma$ point-source depth of $g=24.3$, $r=23.9$, $i=23.3$, and $z=22.8$ mag. Following the methodology of similar searches using DECam data, we apply color and magnitude cuts to select a catalog of $\sim 11$ million extended astronomical sources. After scoring with our CNN, the highest scoring 50,000 images were visually inspected and assigned a score on a scale from 0 (definitely not a lens) to 3 (very probable lens). We present a list of 581 strong lens candidates, 562 of which are previously unreported. We categorize our candidates using their human-assigned scores, resulting in 55 Grade A candidates, 149 Grade B candidates, and 377 Grade C candidates. We additionally highlight eight potential quadruply lensed quasars from this sample. Due to the location of our search footprint in the northern Galactic cap ($b > 10$ deg) and southern celestial hemisphere (${\rm Dec.}<0$ deg), our candidate list has little overlap with other existing ground-based searches. Where our search footprint does overlap with other searches, we find a significant number of high-quality candidates which were previously unidentified, indicating a degree of orthogonality in our methodology. We report properties of our candidates including apparent magnitude and Einstein radius estimated from the image separation., Comment: 24 pages; published version (ApJ)
Published: 2022
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22. Abundance analysis of APOGEE spectra for 58 metal-poor stars from the bulge spheroid

Author: Razera, R., Barbuy, B., Moura, T. C., Ernandes, H., Pérez-Villegas, A., Souza, S. O., Chiappini, C., Queiroz, A. B. A., Anders, F., Fernández-Trincado, J. G., Friaça, A. C. S., Cunha, K., Smith, V. V., Santiago, B. X., Schiavon, R. P., Valentini, M., Minniti, D., Schultheis, M., Geisler, D., Sobeck, J., Placco, V. M, Zoccali, M., Razera, R., Barbuy, B., Moura, T. C., Ernandes, H., Pérez-Villegas, A., Souza, S. O., Chiappini, C., Queiroz, A. B. A., Anders, F., Fernández-Trincado, J. G., Friaça, A. C. S., Cunha, K., Smith, V. V., Santiago, B. X., Schiavon, R. P., Valentini, M., Minniti, D., Schultheis, M., Geisler, D., Sobeck, J., Placco, V. M, and Zoccali, M.
Abstract: The central part of the Galaxy host a multitude of stellar populations, including the spheroidal bulge stars, stars moved to the bulge through secular evolution of the bar, inner halo, inner thick disk, inner thin disk, as well as debris from past accretion events. We identified a sample of 58 candidate stars belonging to the stellar population of the spheroidal bulge, and analyse their abundances. The present calculations of Mg, Ca, and Si lines are in agreement with the APOGEE-ASPCAP abundances, whereas abundances of C, N, O, and Ce are re-examined. We find normal $\alpha$-element enhancements in oxygen, similar to magnesium, Si, and Ca abundances, which are typical of other bulge stars surveyed in the optical in Baade's Window. The enhancement of [O/Fe] in these stars suggests that they do not belong to accreted debris. No spread in N abundances is found, and none of the sample stars is N-rich, indicating that these stars are not second generation stars originated in globular clusters. Ce instead is enhanced in the sample stars, which points to an s-process origin such as due to enrichment from early generations of massive fast rotating stars, the so-called spinstars, Comment: to be published in Monthly Notices of the Royal Astronomical Society
Published: 2022
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23. The DECam Local Volume Exploration Survey Data Release 2

Author: Drlica-Wagner, A., Ferguson, P. S., Adamów, M., Aguena, M., Andrade-Oliveira, F., Bacon, D., Bechtol, K., Bell, E. F., Bertin, E., Bilaji, P., Bocquet, S., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Carlin, J. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cerny, W., Chang, C., Choi, Y., Conselice, C., Costanzi, M., Crnojević, D., da Costa, L. N., De Vicente, J., Desai, S., Esteves, J., Everett, S., Ferrero, I., Fitzpatrick, M., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hernandez-Lang, D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, A. K., Jacques, A., James, D. J., Johnson, M. D., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lidman, C., Lin, H., March, M., Marshall, J. L., Martínez-Delgado, D., Martínez-Vázquez, C. E., Massana, P., Mau, S., McNanna, M., Melchior, P., Menanteau, F., Miller, A. E., Miquel, R., Mohr, J. J., Morgan, R., Mutlu-Pakdil, B., Muñoz, R. R., Neilsen, E. H., Nidever, D. L., Nikutta, R., Castellon, J. L. Nilo, Noël, N. E. D., Ogando, R. L. C., Olsen, K. A. G., Pace, A. B., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Prat, J., Riley, A. H., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sako, M., Sakowska, J. D., Sanchez, E., Sánchez, F. J., Sand, D. J., Santana-Silva, L., Santiago, B., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Simon, J. D., Smith, M., Soares-Santos, M., Stringfellow, G. S., Suchyta, E., Suson, D. J., Tan, C. Y., Tarle, G., Tavangar, K., Thomas, D., To, C., Tollerud, E. J., Troxel, M. A., Tucker, D. L., Varga, T. N., Vivas, A. K., Walker, A. R., Weller, J., Wilkinson, R. D., Wu, J. F., Yanny, B., Zaborowski, E., Zenteno, A., Drlica-Wagner, A., Ferguson, P. S., Adamów, M., Aguena, M., Andrade-Oliveira, F., Bacon, D., Bechtol, K., Bell, E. F., Bertin, E., Bilaji, P., Bocquet, S., Bom, C. R., Brooks, D., Burke, D. L., Carballo-Bello, J. A., Carlin, J. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cerny, W., Chang, C., Choi, Y., Conselice, C., Costanzi, M., Crnojević, D., da Costa, L. N., De Vicente, J., Desai, S., Esteves, J., Everett, S., Ferrero, I., Fitzpatrick, M., Flaugher, B., Friedel, D., Frieman, J., García-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Hartley, W. G., Hernandez-Lang, D., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hughes, A. K., Jacques, A., James, D. J., Johnson, M. D., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lidman, C., Lin, H., March, M., Marshall, J. L., Martínez-Delgado, D., Martínez-Vázquez, C. E., Massana, P., Mau, S., McNanna, M., Melchior, P., Menanteau, F., Miller, A. E., Miquel, R., Mohr, J. J., Morgan, R., Mutlu-Pakdil, B., Muñoz, R. R., Neilsen, E. H., Nidever, D. L., Nikutta, R., Castellon, J. L. Nilo, Noël, N. E. D., Ogando, R. L. C., Olsen, K. A. G., Pace, A. B., Palmese, A., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Prat, J., Riley, A. H., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sako, M., Sakowska, J. D., Sanchez, E., Sánchez, F. J., Sand, D. J., Santana-Silva, L., Santiago, B., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Simon, J. D., Smith, M., Soares-Santos, M., Stringfellow, G. S., Suchyta, E., Suson, D. J., Tan, C. Y., Tarle, G., Tavangar, K., Thomas, D., To, C., Tollerud, E. J., Troxel, M. A., Tucker, D. L., Varga, T. N., Vivas, A. K., Walker, A. R., Weller, J., Wilkinson, R. D., Wu, J. F., Yanny, B., Zaborowski, E., and Zenteno, A.
Abstract: We present the second public data release (DR2) from the DECam Local Volume Exploration survey (DELVE). DELVE DR2 combines new DECam observations with archival DECam data from the Dark Energy Survey, the DECam Legacy Survey, and other DECam community programs. DELVE DR2 consists of ~160,000 exposures that cover >21,000 deg^2 of the high Galactic latitude (|b| > 10 deg) sky in four broadband optical/near-infrared filters (g, r, i, z). DELVE DR2 provides point-source and automatic aperture photometry for ~2.5 billion astronomical sources with a median 5{\sigma} point-source depth of g=24.3, r=23.9, i=23.5, and z=22.8 mag. A region of ~17,000 deg^2 has been imaged in all four filters, providing four-band photometric measurements for ~618 million astronomical sources. DELVE DR2 covers more than four times the area of the previous DELVE data release and contains roughly five times as many astronomical objects. DELVE DR2 is publicly available via the NOIRLab Astro Data Lab science platform., Comment: 23 pages, 10 figures, 5 tables; to be submitted to AAS Journals; public data release at https://datalab.noirlab.edu/delve/. arXiv admin note: substantial text overlap with arXiv:2103.07476
Published: 2022
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24. Arqueología de la arquitectura oculta: el caso del conjunto arquitectónico de San Martín Pinario de Santiago de Compostela

Author: Franco Taboada, José Antonio, Tarrío Carrodeguas, Santiago B., Franco Taboada, José Antonio, and Tarrío Carrodeguas, Santiago B.
Abstract: [Resumen] Este artículo es el resultado de un trabajo de investigación que comenzó en 2003 como un proyecto de levantamiento planimétrico del conjunto arquitectónico de San Martín Pinario y finalizó en 2021 como un estudio arqueológico de su arquitectura presente y pasada. Si bien la investigación nació con el objetivo fundamental de documentar de forma gráfica, por primera vez y de manera exhaustiva, la totalidad del Monasterio, el trabajo de campo evidenció la existencia de una arquitectura oculta que solo podría revelarse mediante el estudio en profundad de sus elementos más singulares, como la cripta que se encuentra bajo el altar mayor, cuyo acceso había sido sellado, o los espacios bajo-cubiertas del Claustro de las Oficinas. Un estudio que solo podría llevarse a cabo de forma eficiente si se realiza en el marco de una disciplina integradora como la arqueología de la arquitectura, entendida esta en su sentido más amplio., [Abstract] This article is the result of research work that began in 2003 as a planimetric survey project of the architectural complex of San Martín Pinario and ended in 2021 as an archaeological study of its present and past architecture. Although the research was undertaken with the fundamental objective of documenting in a graphic way, for the first time and in an exhaustive way, the entirety of the Monastery, the field work uncovered the existence of a hidden architecture that could only be revealed through the indepth study of its more unique elements, such as the crypt under the main altar, whose access had been sealed, or the under-roof spaces of the Cloister of the Offices. A study that could only be carried out efficiently if done so within the framework of an integrative discipline such as the archaeology of architecture, understood in its broadest sense.
Published: 2021

25. Interferon-Gamma Release Assays Differentiate between Mycobacterium avium Complex and Tuberculous Lymphadenitis in Children

Author: Martinez-Planas, Aina, Baquero-Artigao, Fernando, Santiago, B., Fortuny, Claudia, Mendez-Echevarria, Ana, Rosal, Teresa Del, Ingen, J. van, Tebruegge, Marc, Noguera-Julian, Antoni, Martinez-Planas, Aina, Baquero-Artigao, Fernando, Santiago, B., Fortuny, Claudia, Mendez-Echevarria, Ana, Rosal, Teresa Del, Ingen, J. van, Tebruegge, Marc, and Noguera-Julian, Antoni
Abstract: Item does not contain fulltext
Published: 2021

26. Disease-related cortical thinning in presymptomatic granulin mutation carriers

Author: Borrego-Écija, S. (Sergi), Sala-Llonch, R. (Roser), Swieten, J.C. (John) van, Borroni, B. (Barbara), Moreno, F. (Fermin), Masellis, M. (Mario), Tartaglia, C. (Carmela), Graff, C. (Caroline), Galimberti, D. (Daniela), Laforce, R. (Robert), Rowe, J.B. (James), Finger, E. (Elizabeth), Vandenberghe, R. (Rik), Tagliavini, F. (Fabrizio), De Mendonça, A. (Alexandre), Santana, I. (Isabel), Synofzik, M. (Matthis), Ducharme, S. (Simon), Levin, J. (Johannes), Danek, A. (Adrian), Gerhard, A. (Alex), Otto, M. (Markus), Butler, C. (Chris), Frisoni, G.B. (Giovanni B.), Sorbi, S. (Sandro), Heller, C. (Carolin), Bocchetta, M. (Martina), Cash, D.M. (David M), Convery, R.S. (Rhian S), Moore, K.M. (Katrina M), Rohrer, J.D. (Jonathan), Sánchez-Valle, R. (Raquel), Rossor, M.N. (Martin N.), Fox, N.C. (Nick), Woollacott, I.O.C. (Ione O.C.), Shafei, R. (Rachelle), Greaves, C. (Caroline), Neason, M. (Mollie), Guerreiro, R. (Rita), Bras, J. (Jose), Thomas, D.L. (David L), Nicholas, J. (Jennifer), Mead, S. (Simon), Meeter, L.H.H. (Lieke), Panman, J.L. (Jessica), Papma, J.M. (Janne), Thornton, A.S. (Andrew), Pijnenburg, Y.A.L. (Yolande), Indakoetxea, B. (Begoña), Gabilondo, A. (Alazne), TaintaMD, M. (Mikel), de Arriba, M. (Maria), Gorostidi, A. (Ana), Zulaica, M. (Miren), Villanua, J. (Jorge), Diaz, Z. (Zigor), Olives, J. (Jaume), Lladó, A. (Albert), Balasa, M. (Mircea), Antonell, A. (Anna), Bargallo, N. (Nuria), Premi, E. (Enrico), Cosseddu, M. (Maura), Gazzina, S. (Stefano), Padovani, A. (Alessandro), Gasparotti, R. (Roberto), Archetti, S. (Silvana), Black, S. (Sandra), Mitchell, S. (Sara), Rogaeva, E. (Ekaterina), Freedman, M. (Morris), Keren, R. (Ron), Tang-Wai, D. (David), Öijerstedt, L. (Linn), Andersson, C. (Christin), Jelic, S. (Svetislav Svetislav), Thonberg, H. (Håkan), Arighi, A. (Andrea), Fenoglio, C. (Chiara), Scarpini MD, E. (Elio), Fumagalli, G. (Giorgio), Cope, T. (Thomas), Timberlake, C. (Carolyn), Rittman, T. (Timothy), Shoesmith, C. (Christen), Bartha, R. (Robart), Rademakers, S. (Suzanne), Wilke, C. (Carlo), Bender, B. (Benjamin), Bruffaerts, R. (Rose), Vandamme, P. (Philip), Vandenbulcke, M. (Mathieu), Maruta, C. (Carolina), Ferreira, C.B. (Catarina B.), Miltenberger, G. (Gabriel), Verdelho, A. (Ana), Afonso, S. (Sónia), Taipa, R. (Ricardo), Caroppo, P. (Paola), Di Fede, G. (Giuseppe), Giaccone, G. (Giorgio), Prioni, S. (Sara), Redaelli, V. (Veronica), Rossi, G. (Giacomina), Tiraboschi, P. (Pietro), Duro, D. (Diana), Rosario Almeida, M. (Maria), Castelo-Branco, M. (Miguel), João Leitão, M. (Maria), Tabuas-Pereira, M. (Miguel), Santiago, B. (Beatriz), Gauthier, S. (Serge), Rosa-Neto, P. (Pedro), Veldsman, M. (Michele), Flanagan, T. (Toby), Prix, C. (Catharina), Hoegen, T. (Tobias), Wlasich, E. (Elisabeth), Loosli, S. (Sandra), Schonecker, S. (Sonja), Semler, E. (Elisa), Anderl-Straub, S. (Sarah), Borrego-Écija, S. (Sergi), Sala-Llonch, R. (Roser), Swieten, J.C. (John) van, Borroni, B. (Barbara), Moreno, F. (Fermin), Masellis, M. (Mario), Tartaglia, C. (Carmela), Graff, C. (Caroline), Galimberti, D. (Daniela), Laforce, R. (Robert), Rowe, J.B. (James), Finger, E. (Elizabeth), Vandenberghe, R. (Rik), Tagliavini, F. (Fabrizio), De Mendonça, A. (Alexandre), Santana, I. (Isabel), Synofzik, M. (Matthis), Ducharme, S. (Simon), Levin, J. (Johannes), Danek, A. (Adrian), Gerhard, A. (Alex), Otto, M. (Markus), Butler, C. (Chris), Frisoni, G.B. (Giovanni B.), Sorbi, S. (Sandro), Heller, C. (Carolin), Bocchetta, M. (Martina), Cash, D.M. (David M), Convery, R.S. (Rhian S), Moore, K.M. (Katrina M), Rohrer, J.D. (Jonathan), Sánchez-Valle, R. (Raquel), Rossor, M.N. (Martin N.), Fox, N.C. (Nick), Woollacott, I.O.C. (Ione O.C.), Shafei, R. (Rachelle), Greaves, C. (Caroline), Neason, M. (Mollie), Guerreiro, R. (Rita), Bras, J. (Jose), Thomas, D.L. (David L), Nicholas, J. (Jennifer), Mead, S. (Simon), Meeter, L.H.H. (Lieke), Panman, J.L. (Jessica), Papma, J.M. (Janne), Thornton, A.S. (Andrew), Pijnenburg, Y.A.L. (Yolande), Indakoetxea, B. (Begoña), Gabilondo, A. (Alazne), TaintaMD, M. (Mikel), de Arriba, M. (Maria), Gorostidi, A. (Ana), Zulaica, M. (Miren), Villanua, J. (Jorge), Diaz, Z. (Zigor), Olives, J. (Jaume), Lladó, A. (Albert), Balasa, M. (Mircea), Antonell, A. (Anna), Bargallo, N. (Nuria), Premi, E. (Enrico), Cosseddu, M. (Maura), Gazzina, S. (Stefano), Padovani, A. (Alessandro), Gasparotti, R. (Roberto), Archetti, S. (Silvana), Black, S. (Sandra), Mitchell, S. (Sara), Rogaeva, E. (Ekaterina), Freedman, M. (Morris), Keren, R. (Ron), Tang-Wai, D. (David), Öijerstedt, L. (Linn), Andersson, C. (Christin), Jelic, S. (Svetislav Svetislav), Thonberg, H. (Håkan), Arighi, A. (Andrea), Fenoglio, C. (Chiara), Scarpini MD, E. (Elio), Fumagalli, G. (Giorgio), Cope, T. (Thomas), Timberlake, C. (Carolyn), Rittman, T. (Timothy), Shoesmith, C. (Christen), Bartha, R. (Robart), Rademakers, S. (Suzanne), Wilke, C. (Carlo), Bender, B. (Benjamin), Bruffaerts, R. (Rose), Vandamme, P. (Philip), Vandenbulcke, M. (Mathieu), Maruta, C. (Carolina), Ferreira, C.B. (Catarina B.), Miltenberger, G. (Gabriel), Verdelho, A. (Ana), Afonso, S. (Sónia), Taipa, R. (Ricardo), Caroppo, P. (Paola), Di Fede, G. (Giuseppe), Giaccone, G. (Giorgio), Prioni, S. (Sara), Redaelli, V. (Veronica), Rossi, G. (Giacomina), Tiraboschi, P. (Pietro), Duro, D. (Diana), Rosario Almeida, M. (Maria), Castelo-Branco, M. (Miguel), João Leitão, M. (Maria), Tabuas-Pereira, M. (Miguel), Santiago, B. (Beatriz), Gauthier, S. (Serge), Rosa-Neto, P. (Pedro), Veldsman, M. (Michele), Flanagan, T. (Toby), Prix, C. (Catharina), Hoegen, T. (Tobias), Wlasich, E. (Elisabeth), Loosli, S. (Sandra), Schonecker, S. (Sonja), Semler, E. (Elisa), and Anderl-Straub, S. (Sarah)
Abstract: Mutations in the granulin gene (GRN) cause familial frontotemporal dementia. Understanding the structural brain changes in presymptomatic GRN carriers would enforce the use of neuroimaging biomarkers for early diagnosis and monitoring. We studied 100 presymptomatic GRN mutation carriers and 94 noncarriers from the Genetic Frontotemporal dementia initiative (GENFI), with MRI structural images. We analyzed 3T MRI structural images using the FreeSurfer pipeline to calculate the whole brain cortical thickness (CTh) for each subject. We also perform a vertex-wise general linear model to assess differences between groups in the relationship between CTh and diverse covariables as gender, age, the estimated years to onset and education. We also explored differences according to TMEM106B genotype, a possible disease modifier. Whole brain CTh did not differ between carriers and noncarriers. Both groups showed age-related cortical thinning. The group-by-age interaction analysis showed that this age-related cortical thinning was significantly greater in GRN carriers in the left superior frontal cortex. TMEM106B did not significantly influence the age-related cortical thinning. Our results validate and expand previous findings suggesting an
Published: 2021
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27. Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia EDR3 stars brighter than G=18.5

Author: Anders, F., Khalatyan, A., Queiroz, A. B. A., Chiappini, C., Ardèvol, J., Casamiquela, L., Figueras, F., Jiménez-Arranz, Ó., Jordi, C., Monguió, M., Romero-Gómez, M., Altamirano, D., Antoja, T., Assaad, R., Cantat-Gaudin, T., Castro-Ginard, A., Enke, H., Girardi, L., Guiglion, G., Khan, S., Luri, X., Miglio, A., Minchev, I., Ramos, P., Santiago, B. X., Steinmetz, M., Anders, F., Khalatyan, A., Queiroz, A. B. A., Chiappini, C., Ardèvol, J., Casamiquela, L., Figueras, F., Jiménez-Arranz, Ó., Jordi, C., Monguió, M., Romero-Gómez, M., Altamirano, D., Antoja, T., Assaad, R., Cantat-Gaudin, T., Castro-Ginard, A., Enke, H., Girardi, L., Guiglion, G., Khan, S., Luri, X., Miglio, A., Minchev, I., Ramos, P., Santiago, B. X., and Steinmetz, M.
Abstract: We present a catalogue of 362 million stellar parameters, distances, and extinctions derived from Gaia's early third data release (EDR3) cross-matched with the photometric catalogues of Pan-STARRS1, SkyMapper, 2MASS, and AllWISE. The higher precision of the Gaia EDR3 data, combined with the broad wavelength coverage of the additional photometric surveys and the new stellar-density priors of the {\tt StarHorse} code allow us to substantially improve the accuracy and precision over previous photo-astrometric stellar-parameter estimates. At magnitude $G=14\, (17)$, our typical precisions amount to 3% (15%) in distance, 0.13 mag (0.15 mag) in $V$-band extinction, and 140 K (180 K) in effective temperature. Our results are validated by comparisons with open clusters, as well as with asteroseismic and spectroscopic measurements, indicating systematic errors smaller than the nominal uncertainties for the vast majority of objects. We also provide distance- and extinction-corrected colour-magnitude diagrams, extinction maps, and extensive stellar density maps that reveal detailed substructures in the Milky Way and beyond. The new density maps now probe a much greater volume, extending to regions beyond the Galactic bar and to Local Group galaxies, with a larger total number density. We publish our results through an ADQL query interface ({\tt gaia.aip.de}) as well as via tables containing approximations of the full posterior distributions. Our multi-wavelength approach and the deep magnitude limit make our results useful also beyond the next Gaia release, DR3., Comment: A&A, accepted, 27 pages, 25 figures. Fig. 5 has changed with respect to v1 (post-processing bug corrected). For various options to access the data see https://data.aip.de/projects/starhorse2021.html
Published: 2021
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28. The Observed Evolution of the Stellar Mass - Halo Mass Relation for Brightest Central Galaxies

Author: Golden-Marx, Jesse B., Miller, C. J., Zhang, Y., Ogando, R. L. C., Palmese, A., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Constanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., de Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchon, F., Petravick, D., Pieres, A., Malagon, A. A. Plazas, Prat, J., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Varga, T. N., Golden-Marx, Jesse B., Miller, C. J., Zhang, Y., Ogando, R. L. C., Palmese, A., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Constanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., de Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchon, F., Petravick, D., Pieres, A., Malagon, A. A. Plazas, Prat, J., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., and Varga, T. N.
Abstract: We quantify evolution in the cluster scale stellar mass - halo mass (SMHM) relation's parameters using 2323 clusters and brightest central galaxies (BCGs) over the redshift range $0.03 \le z \le 0.60$. The precision on inferred SMHM parameters is improved by including the magnitude gap ($\rm m_{gap}$) between the BCG and fourth brightest cluster member (M14) as a third parameter in the SMHM relation. At fixed halo mass, accounting for $\rm m_{gap}$, through a stretch parameter, reduces the SMHM relation's intrinsic scatter. To explore this redshift range, we use clusters, BCGs, and cluster members identified using the Sloan Digital Sky Survey C4 and redMaPPer cluster catalogs and the Dark Energy Survey redMaPPer catalog. Through this joint analysis, we detect no systematic differences in BCG stellar mass, $\rm m_{gap}$, and cluster mass (inferred from richness) between the datsets. We utilize the Pareto function to quantify each parameter's evolution. We confirm prior findings of negative evolution in the SMHM relation's slope (3.5$\sigma$) and detect negative evolution in the stretch parameter (4.0$\sigma$) and positive evolution in the offset parameter (5.8$\sigma$). This observed evolution, combined with the absence of BCG growth, when stellar mass is measured within 50kpc, suggests that this evolution results from changes in the cluster's $\rm m_{gap}$. For this to occur, late-term growth must be in the intra-cluster light surrounding the BCG. We also compare the observed results to Illustris TNG 300-1 cosmological hydrodynamic simulations and find modest qualitative agreement. However, the simulations lack the evolutionary features detected in the real data., Comment: 21 pages, 12 Figures, 3 Tables. Submitted to ApJ on July 1
Published: 2021
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29. Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and galaxy-galaxy lensing using the MagLim lens sample

Author: Porredon, A., Crocce, M., Elvin-Poole, J., Cawthon, R., Giannini, G., De Vicente, J., Rosell, A. Carnero, Ferrero, I., Krause, E., Fang, X., Prat, J., Rodriguez-Monroy, M., Pandey, S., Pocino, A., Castander, F. J., Choi, A., Amon, A., Tutusaus, I., Dodelson, S., Sevilla-Noarbe, I., Fosalba, P., Gaztanaga, E., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Camacho, H., Campos, A., Kind, M. Carrasco, Chintalapati, P., Cordero, J., DeRose, J., Di Valentino, E., Doux, C., Eifler, T. F., Everett, S., Ferté, A., Friedrich, O., Gatti, M., Gruen, D., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jain, B., Jarvis, M., Lee, S., Lemos, P., MacCrann, N., Mena-Fernández, J., Muir, J., Myles, J., Park, Y., Raveri, M., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Cid, D. Sanchez, Scolnic, D., Secco, L. F., Sheldon, E., Troja, A., Troxel, M. A., Weaverdyck, N., Yanny, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Malagón, A. A. Plazas, Romer, A. K., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Porredon, A., Crocce, M., Elvin-Poole, J., Cawthon, R., Giannini, G., De Vicente, J., Rosell, A. Carnero, Ferrero, I., Krause, E., Fang, X., Prat, J., Rodriguez-Monroy, M., Pandey, S., Pocino, A., Castander, F. J., Choi, A., Amon, A., Tutusaus, I., Dodelson, S., Sevilla-Noarbe, I., Fosalba, P., Gaztanaga, E., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Camacho, H., Campos, A., Kind, M. Carrasco, Chintalapati, P., Cordero, J., DeRose, J., Di Valentino, E., Doux, C., Eifler, T. F., Everett, S., Ferté, A., Friedrich, O., Gatti, M., Gruen, D., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jain, B., Jarvis, M., Lee, S., Lemos, P., MacCrann, N., Mena-Fernández, J., Muir, J., Myles, J., Park, Y., Raveri, M., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Cid, D. Sanchez, Scolnic, D., Secco, L. F., Sheldon, E., Troja, A., Troxel, M. A., Weaverdyck, N., Yanny, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Malagón, A. A. Plazas, Romer, A. K., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., and Weller, J.
Abstract: Two of the most sensitive probes of the large scale structure of the universe are the clustering of galaxies and the tangential shear of background galaxy shapes produced by those foreground galaxies, so-called galaxy-galaxy lensing. Combining the measurements of these two two-point functions leads to cosmological constraints that are independent of the galaxy bias factor. The optimal choice of foreground, or lens, galaxies is governed by the joint, but conflicting requirements to obtain accurate redshift information and large statistics. We present cosmological results from the full 5000 sq. deg. of the Dark Energy Survey first three years of observations (Y3) combining those two-point functions, using for the first time a magnitude-limited lens sample (MagLim) of 11 million galaxies especially selected to optimize such combination, and 100 million background shapes. We consider two cosmological models, flat $\Lambda$CDM and $w$CDM. In $\Lambda$CDM we obtain for the matter density $\Omega_m = 0.320^{+0.041}_{-0.034}$ and for the clustering amplitude $S_8 = 0.778^{+0.037}_{-0.031}$, at 68\% C.L. The latter is only 1$\sigma$ smaller than the prediction in this model informed by measurements of the cosmic microwave background by the Planck satellite. In $w$CDM we find $\Omega_m = 0.32^{+0.044}_{-0.046}$, $S_8=0.777^{+0.049}_{-0.051}$, and dark energy equation of state $w=-1.031^{+0.218}_{-0.379}$. We find that including smaller scales while marginalizing over non-linear galaxy bias improves the constraining power in the $\Omega_m-S_8$ plane by $31\%$ and in the $\Omega_m-w$ plane by $41\%$ while yielding consistent cosmological parameters from those in the linear bias case. These results are combined with those from cosmic shear in a companion paper to present full DES-Y3 constraints from the three two-point functions (3x2pt)., Comment: 25 pages, 16 figures, to be submitted to PRD. See https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 cosmology release
Published: 2021

30. The mass and galaxy distribution around SZ-selected clusters

Author: Shin, T., Jain, B., Adhikari, S., Baxter, E. J., Chang, C., Pandey, S., Salcedo, A., Weinberg, D. H., Amsellem, A., Battaglia, N., Belyakov, M., Dacunha, T., Goldstein, S., Kravtsov, A. V., Varga, T. N., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Amon, A., Andrade-Oliveira, F., Annis, J., Bacon, D., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bocquet, S., Bond, J. R., Brooks, D., Buckley-Geer, E., Burke, D. L., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chen, R., Choi, A., Costanzi, M., da Costa, L. N., DeRose, J., Desai, S., De Vicente, J., Devlin, M. J., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gallardo, P. A., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hartley, W. G., Hill, J. C., Hilton, M., Hinton, S. R., Hollowood, D. L., Hughes, J. P., James, D. J., Jarvis, M., Jeltema, T., Koopman, B. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lokken, M., MacCrann, N., Madhavacheril, M. S., Maia, M. A. G., McCullough, J., McMahon, J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moodley, K., Morgan, R., Myles, J., Nati, F., Navarro-Alsina, A., Niemack, M. D., Ogando, R. L. C., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Rykoff, E. S., Salatino, M., Sánchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schillaci, A., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifón, C., Smith, M., Soares-Santos, M., Staggs, S. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tutusaus, I., Vavagiakis, E. M., Weller, J., Wollack, E. J., Yanny, B., Yin, B., Zhang, Y., Shin, T., Jain, B., Adhikari, S., Baxter, E. J., Chang, C., Pandey, S., Salcedo, A., Weinberg, D. H., Amsellem, A., Battaglia, N., Belyakov, M., Dacunha, T., Goldstein, S., Kravtsov, A. V., Varga, T. N., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Amon, A., Andrade-Oliveira, F., Annis, J., Bacon, D., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bocquet, S., Bond, J. R., Brooks, D., Buckley-Geer, E., Burke, D. L., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chen, R., Choi, A., Costanzi, M., da Costa, L. N., DeRose, J., Desai, S., De Vicente, J., Devlin, M. J., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gallardo, P. A., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hartley, W. G., Hill, J. C., Hilton, M., Hinton, S. R., Hollowood, D. L., Hughes, J. P., James, D. J., Jarvis, M., Jeltema, T., Koopman, B. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lokken, M., MacCrann, N., Madhavacheril, M. S., Maia, M. A. G., McCullough, J., McMahon, J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moodley, K., Morgan, R., Myles, J., Nati, F., Navarro-Alsina, A., Niemack, M. D., Ogando, R. L. C., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Rykoff, E. S., Salatino, M., Sánchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schillaci, A., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifón, C., Smith, M., Soares-Santos, M., Staggs, S. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tutusaus, I., Vavagiakis, E. M., Weller, J., Wollack, E. J., Yanny, B., Yin, B., and Zhang, Y.
Abstract: We present measurements of the radial profiles of the mass and galaxy number density around Sunyaev-Zel'dovich-selected clusters using both weak lensing and galaxy counts. The clusters are selected from the Atacama Cosmology Telescope Data Release 5 and the galaxies from the Dark Energy Survey Year 3 dataset. With signal-to-noise of 62 (43) for galaxy (weak lensing) profiles over scales of about $0.2-20h^{-1}$ Mpc, these are the highest precision measurements for SZ-selected clusters to date. Because SZ selection closely approximates mass selection, these measurements enable several tests of theoretical models of the mass and light distribution around clusters. Our main findings are: 1. The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations. 2. The full mass profile is also consistent with the simulations; hence it can constrain alternative dark matter models that modify the mass distribution of clusters. 3. The shapes of the galaxy and lensing profiles are remarkably similar for our sample over the entire range of scales, from well inside the cluster halo to the quasilinear regime. This can be used to constrain processes such as quenching and tidal disruption that alter the galaxy distribution inside the halo, and scale-dependent features in the transition regime outside the halo. We measure the dependence of the profile shapes on the galaxy sample, redshift and cluster mass. We extend the Diemer \& Kravtsov model for the cluster profiles to the linear regime using perturbation theory and show that it provides a good match to the measured profiles. We also compare the measured profiles to predictions of the standard halo model and simulations that include hydrodynamics. Applications of these results to cluster mass estimation and cosmology are discussed., Comment: 15 pages, 6 figures (main) + 3 pages, 6 figures (appendix), submitted to MNRAS
Published: 2021
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31. Probing Galaxy Evolution in Massive Clusters Using ACT and DES: Splashback as a Cosmic Clock

Author: Adhikari, S, Adhikari, S, Shin, TH, Jain, B, Hilton, M, Baxter, E, Chang, C, Wechsler, RH, Battaglia, N, Bond, JR, Bocquet, S, Choi, SK, Derose, J, Devlin, M, Dunkley, J, Evrard, AE, Ferraro, S, Hill, JC, Hughes, JP, Gallardo, PA, Lokken, M, Macinnis, A, Madhavacheril, MS, McMahon, J, Nati, F, Newburgh, LB, Niemack, MD, Page, LA, Palmese, A, Partridge, B, Rozo, E, Rykoff, E, Salatino, M, Schillaci, A, Sehgal, N, Sifón, C, To, CH, Wollack, E, Wu, HY, Xu, Z, Aguena, M, Allam, S, Amon, A, Annis, J, Avila, S, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Burke, DL, Rosell, AC, Kind, MC, Carretero, J, Castander, FJ, Choi, A, Costanzi, M, Da Costa, LN, Vicente, JD, Desai, S, Diehl, TH, Doel, P, Everett, S, Ferrero, I, Ferté, A, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hinton, SR, Hollowood, DL, Honscheid, K, James, DJ, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, Marshall, JL, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, L. C. Ogando, R, Paz-Chinchón, F, Malagón, AP, Sanchez, E, Santiago, B, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, Adhikari, S, Adhikari, S, Shin, TH, Jain, B, Hilton, M, Baxter, E, Chang, C, Wechsler, RH, Battaglia, N, Bond, JR, Bocquet, S, Choi, SK, Derose, J, Devlin, M, Dunkley, J, Evrard, AE, Ferraro, S, Hill, JC, Hughes, JP, Gallardo, PA, Lokken, M, Macinnis, A, Madhavacheril, MS, McMahon, J, Nati, F, Newburgh, LB, Niemack, MD, Page, LA, Palmese, A, Partridge, B, Rozo, E, Rykoff, E, Salatino, M, Schillaci, A, Sehgal, N, Sifón, C, To, CH, Wollack, E, Wu, HY, Xu, Z, Aguena, M, Allam, S, Amon, A, Annis, J, Avila, S, Bacon, D, Bertin, E, Bhargava, S, Brooks, D, Burke, DL, Rosell, AC, Kind, MC, Carretero, J, Castander, FJ, Choi, A, Costanzi, M, Da Costa, LN, Vicente, JD, Desai, S, Diehl, TH, Doel, P, Everett, S, Ferrero, I, Ferté, A, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hinton, SR, Hollowood, DL, Honscheid, K, James, DJ, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, Marshall, JL, Martini, P, Melchior, P, Menanteau, F, Miquel, R, Morgan, R, L. C. Ogando, R, Paz-Chinchón, F, Malagón, AP, Sanchez, E, Santiago, B, Scarpine, V, Serrano, S, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, and Suchyta, E
Abstract: We measure the projected number density profiles of galaxies and the splashback feature in clusters selected by the Sunyaev-Zel'dovich effect from the Advanced Atacama Cosmology Telescope (AdvACT) survey using galaxies observed by the Dark Energy Survey (DES). The splashback radius is consistent with CDM-only simulations and is located at 2.4-0.4+0.3 Mpc h-1. We split the galaxies on color and find significant differences in their profile shapes. Red and green-valley galaxies show a splashback-like minimum in their slope profile consistent with theory, while the bluest galaxies show a weak feature at a smaller radius. We develop a mapping of galaxies to subhalos in simulations and assign colors based on infall time onto their hosts. We find that the shift in location of the steepest slope and different profile shapes can be mapped to the average time of infall of galaxies of different colors. The steepest slope traces a discontinuity in the phase space of dark matter halos. By relating spatial profiles to infall time, we can use splashback as a clock to understand galaxy quenching. We find that red galaxies have on average been in clusters over 3.2 Gyr, green galaxies about 2.2 Gyr, while blue galaxies have been accreted most recently and have not reached apocenter. Using the full radial profiles, we fit a simple quenching model and find that the onset of galaxy quenching occurs after a delay of about a gigayear and that galaxies quench rapidly thereafter with an exponential timescale of 0.6 Gyr.
Published: 2021

32. Interferon-Gamma Release Assays Differentiate between Mycobacterium avium Complex and Tuberculous Lymphadenitis in Children

Author: Martinez-Planas, Aina, Baquero-Artigao, Fernando, Santiago, B., Fortuny, Claudia, Mendez-Echevarria, Ana, Rosal, Teresa Del, Ingen, J. van, Tebruegge, Marc, Noguera-Julian, Antoni, Martinez-Planas, Aina, Baquero-Artigao, Fernando, Santiago, B., Fortuny, Claudia, Mendez-Echevarria, Ana, Rosal, Teresa Del, Ingen, J. van, Tebruegge, Marc, and Noguera-Julian, Antoni
Abstract: Item does not contain fulltext
Published: 2021

33. Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia EDR3 stars brighter than G=18.5

Author: Anders, F., Khalatyan, A., Queiroz, A. B. A., Chiappini, C., Ardèvol, J., Casamiquela, L., Figueras, F., Jiménez-Arranz, Ó., Jordi, C., Monguió, M., Romero-Gómez, M., Altamirano, D., Antoja, T., Assaad, R., Cantat-Gaudin, T., Castro-Ginard, A., Enke, H., Girardi, L., Guiglion, G., Khan, S., Luri, X., Miglio, A., Minchev, I., Ramos, P., Santiago, B. X., Steinmetz, M., Anders, F., Khalatyan, A., Queiroz, A. B. A., Chiappini, C., Ardèvol, J., Casamiquela, L., Figueras, F., Jiménez-Arranz, Ó., Jordi, C., Monguió, M., Romero-Gómez, M., Altamirano, D., Antoja, T., Assaad, R., Cantat-Gaudin, T., Castro-Ginard, A., Enke, H., Girardi, L., Guiglion, G., Khan, S., Luri, X., Miglio, A., Minchev, I., Ramos, P., Santiago, B. X., and Steinmetz, M.
Abstract: We present a catalogue of 362 million stellar parameters, distances, and extinctions derived from Gaia's early third data release (EDR3) cross-matched with the photometric catalogues of Pan-STARRS1, SkyMapper, 2MASS, and AllWISE. The higher precision of the Gaia EDR3 data, combined with the broad wavelength coverage of the additional photometric surveys and the new stellar-density priors of the {\tt StarHorse} code allow us to substantially improve the accuracy and precision over previous photo-astrometric stellar-parameter estimates. At magnitude $G=14\, (17)$, our typical precisions amount to 3% (15%) in distance, 0.13 mag (0.15 mag) in $V$-band extinction, and 140 K (180 K) in effective temperature. Our results are validated by comparisons with open clusters, as well as with asteroseismic and spectroscopic measurements, indicating systematic errors smaller than the nominal uncertainties for the vast majority of objects. We also provide distance- and extinction-corrected colour-magnitude diagrams, extinction maps, and extensive stellar density maps that reveal detailed substructures in the Milky Way and beyond. The new density maps now probe a much greater volume, extending to regions beyond the Galactic bar and to Local Group galaxies, with a larger total number density. We publish our results through an ADQL query interface ({\tt gaia.aip.de}) as well as via tables containing approximations of the full posterior distributions. Our multi-wavelength approach and the deep magnitude limit make our results useful also beyond the next Gaia release, DR3., Comment: A&A, accepted, 27 pages, 25 figures. Fig. 5 has changed with respect to v1 (post-processing bug corrected). For various options to access the data see https://data.aip.de/projects/starhorse2021.html
Published: 2021
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34. The Observed Evolution of the Stellar Mass - Halo Mass Relation for Brightest Central Galaxies

Author: Golden-Marx, Jesse B., Miller, C. J., Zhang, Y., Ogando, R. L. C., Palmese, A., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Constanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., de Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchon, F., Petravick, D., Pieres, A., Malagon, A. A. Plazas, Prat, J., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Varga, T. N., Golden-Marx, Jesse B., Miller, C. J., Zhang, Y., Ogando, R. L. C., Palmese, A., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Buckley-Geer, E., Rosell, A. Carnero, Kind, M. Carrasco, Castander, F. J., Constanzi, M., Crocce, M., da Costa, L. N., Pereira, M. E. S., de Vicente, J., Desai, S., Diehl, H. T., Doel, P., Drlica-Wagner, A., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Jeltema, T., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Paz-Chinchon, F., Petravick, D., Pieres, A., Malagon, A. A. Plazas, Prat, J., Romer, A. K., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., and Varga, T. N.
Abstract: We quantify evolution in the cluster scale stellar mass - halo mass (SMHM) relation's parameters using 2323 clusters and brightest central galaxies (BCGs) over the redshift range $0.03 \le z \le 0.60$. The precision on inferred SMHM parameters is improved by including the magnitude gap ($\rm m_{gap}$) between the BCG and fourth brightest cluster member (M14) as a third parameter in the SMHM relation. At fixed halo mass, accounting for $\rm m_{gap}$, through a stretch parameter, reduces the SMHM relation's intrinsic scatter. To explore this redshift range, we use clusters, BCGs, and cluster members identified using the Sloan Digital Sky Survey C4 and redMaPPer cluster catalogs and the Dark Energy Survey redMaPPer catalog. Through this joint analysis, we detect no systematic differences in BCG stellar mass, $\rm m_{gap}$, and cluster mass (inferred from richness) between the datsets. We utilize the Pareto function to quantify each parameter's evolution. We confirm prior findings of negative evolution in the SMHM relation's slope (3.5$\sigma$) and detect negative evolution in the stretch parameter (4.0$\sigma$) and positive evolution in the offset parameter (5.8$\sigma$). This observed evolution, combined with the absence of BCG growth, when stellar mass is measured within 50kpc, suggests that this evolution results from changes in the cluster's $\rm m_{gap}$. For this to occur, late-term growth must be in the intra-cluster light surrounding the BCG. We also compare the observed results to Illustris TNG 300-1 cosmological hydrodynamic simulations and find modest qualitative agreement. However, the simulations lack the evolutionary features detected in the real data., Comment: 21 pages, 12 Figures, 3 Tables. Submitted to ApJ on July 1
Published: 2021
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35. Dark Energy Survey Year 3 results: Cosmological constraints from galaxy clustering and galaxy-galaxy lensing using the MagLim lens sample

Author: Porredon, A., Crocce, M., Elvin-Poole, J., Cawthon, R., Giannini, G., De Vicente, J., Rosell, A. Carnero, Ferrero, I., Krause, E., Fang, X., Prat, J., Rodriguez-Monroy, M., Pandey, S., Pocino, A., Castander, F. J., Choi, A., Amon, A., Tutusaus, I., Dodelson, S., Sevilla-Noarbe, I., Fosalba, P., Gaztanaga, E., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Camacho, H., Campos, A., Kind, M. Carrasco, Chintalapati, P., Cordero, J., DeRose, J., Di Valentino, E., Doux, C., Eifler, T. F., Everett, S., Ferté, A., Friedrich, O., Gatti, M., Gruen, D., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jain, B., Jarvis, M., Lee, S., Lemos, P., MacCrann, N., Mena-Fernández, J., Muir, J., Myles, J., Park, Y., Raveri, M., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Cid, D. Sanchez, Scolnic, D., Secco, L. F., Sheldon, E., Troja, A., Troxel, M. A., Weaverdyck, N., Yanny, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Malagón, A. A. Plazas, Romer, A. K., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., Weller, J., Porredon, A., Crocce, M., Elvin-Poole, J., Cawthon, R., Giannini, G., De Vicente, J., Rosell, A. Carnero, Ferrero, I., Krause, E., Fang, X., Prat, J., Rodriguez-Monroy, M., Pandey, S., Pocino, A., Castander, F. J., Choi, A., Amon, A., Tutusaus, I., Dodelson, S., Sevilla-Noarbe, I., Fosalba, P., Gaztanaga, E., Alarcon, A., Alves, O., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M. R., Bernstein, G. M., Blazek, J., Camacho, H., Campos, A., Kind, M. Carrasco, Chintalapati, P., Cordero, J., DeRose, J., Di Valentino, E., Doux, C., Eifler, T. F., Everett, S., Ferté, A., Friedrich, O., Gatti, M., Gruen, D., Harrison, I., Hartley, W. G., Herner, K., Huff, E. M., Huterer, D., Jain, B., Jarvis, M., Lee, S., Lemos, P., MacCrann, N., Mena-Fernández, J., Muir, J., Myles, J., Park, Y., Raveri, M., Rosenfeld, R., Ross, A. J., Rykoff, E. S., Samuroff, S., Sánchez, C., Sanchez, E., Sanchez, J., Cid, D. Sanchez, Scolnic, D., Secco, L. F., Sheldon, E., Troja, A., Troxel, M. A., Weaverdyck, N., Yanny, B., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bacon, D., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Burke, D. L., Carretero, J., Costanzi, M., da Costa, L. N., Pereira, M. E. S., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Drlica-Wagner, A., Eckert, K., Evrard, A. E., Flaugher, B., Frieman, J., García-Bellido, J., Gerdes, D. W., Giannantonio, T., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Morgan, R., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Malagón, A. A. Plazas, Romer, A. K., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., Thomas, D., To, C., Varga, T. N., and Weller, J.
Abstract: Two of the most sensitive probes of the large scale structure of the universe are the clustering of galaxies and the tangential shear of background galaxy shapes produced by those foreground galaxies, so-called galaxy-galaxy lensing. Combining the measurements of these two two-point functions leads to cosmological constraints that are independent of the galaxy bias factor. The optimal choice of foreground, or lens, galaxies is governed by the joint, but conflicting requirements to obtain accurate redshift information and large statistics. We present cosmological results from the full 5000 sq. deg. of the Dark Energy Survey first three years of observations (Y3) combining those two-point functions, using for the first time a magnitude-limited lens sample (MagLim) of 11 million galaxies especially selected to optimize such combination, and 100 million background shapes. We consider two cosmological models, flat $\Lambda$CDM and $w$CDM. In $\Lambda$CDM we obtain for the matter density $\Omega_m = 0.320^{+0.041}_{-0.034}$ and for the clustering amplitude $S_8 = 0.778^{+0.037}_{-0.031}$, at 68% C.L. The latter is only 1$\sigma$ smaller than the prediction in this model informed by measurements of the cosmic microwave background by the Planck satellite. In $w$CDM we find $\Omega_m = 0.32^{+0.044}_{-0.046}$, $S_8=0.777^{+0.049}_{-0.051}$, and dark energy equation of state $w=-1.031^{+0.218}_{-0.379}$. We find that including smaller scales while marginalizing over non-linear galaxy bias improves the constraining power in the $\Omega_m-S_8$ plane by $31$% and in the $\Omega_m-w$ plane by $41$% while yielding consistent cosmological parameters from those in the linear bias case. These results are combined with those from cosmic shear in a companion paper to present full DES-Y3 constraints from the three two-point functions (3x2pt)., Comment: 27 pages, 17 figures, matches the version accepted in PRD. See https://www.darkenergysurvey.org/des-year-3-cosmology-results-papers/ for the full DES Y3 cosmology release
Published: 2021
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36. The mass and galaxy distribution around SZ-selected clusters

Author: Shin, T., Jain, B., Adhikari, S., Baxter, E. J., Chang, C., Pandey, S., Salcedo, A., Weinberg, D. H., Amsellem, A., Battaglia, N., Belyakov, M., Dacunha, T., Goldstein, S., Kravtsov, A. V., Varga, T. N., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Amon, A., Andrade-Oliveira, F., Annis, J., Bacon, D., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bocquet, S., Bond, J. R., Brooks, D., Buckley-Geer, E., Burke, D. L., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chen, R., Choi, A., Costanzi, M., da Costa, L. N., DeRose, J., Desai, S., De Vicente, J., Devlin, M. J., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gallardo, P. A., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hartley, W. G., Hill, J. C., Hilton, M., Hinton, S. R., Hollowood, D. L., Hughes, J. P., James, D. J., Jarvis, M., Jeltema, T., Koopman, B. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lokken, M., MacCrann, N., Madhavacheril, M. S., Maia, M. A. G., McCullough, J., McMahon, J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moodley, K., Morgan, R., Myles, J., Nati, F., Navarro-Alsina, A., Niemack, M. D., Ogando, R. L. C., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Rykoff, E. S., Salatino, M., Sánchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schillaci, A., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifón, C., Smith, M., Soares-Santos, M., Staggs, S. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tutusaus, I., Vavagiakis, E. M., Weller, J., Wollack, E. J., Yanny, B., Yin, B., Zhang, Y., Shin, T., Jain, B., Adhikari, S., Baxter, E. J., Chang, C., Pandey, S., Salcedo, A., Weinberg, D. H., Amsellem, A., Battaglia, N., Belyakov, M., Dacunha, T., Goldstein, S., Kravtsov, A. V., Varga, T. N., Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Amon, A., Andrade-Oliveira, F., Annis, J., Bacon, D., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bocquet, S., Bond, J. R., Brooks, D., Buckley-Geer, E., Burke, D. L., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chen, R., Choi, A., Costanzi, M., da Costa, L. N., DeRose, J., Desai, S., De Vicente, J., Devlin, M. J., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferraro, S., Ferrero, I., Ferté, A., Flaugher, B., Frieman, J., Gallardo, P. A., Gatti, M., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Harrison, I., Hartley, W. G., Hill, J. C., Hilton, M., Hinton, S. R., Hollowood, D. L., Hughes, J. P., James, D. J., Jarvis, M., Jeltema, T., Koopman, B. J., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Lokken, M., MacCrann, N., Madhavacheril, M. S., Maia, M. A. G., McCullough, J., McMahon, J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J. J., Moodley, K., Morgan, R., Myles, J., Nati, F., Navarro-Alsina, A., Niemack, M. D., Ogando, R. L. C., Page, L. A., Palmese, A., Partridge, B., Paz-Chinchón, F., Pereira, M. E. S., Pieres, A., Malagón, A. A. Plazas, Prat, J., Raveri, M., Rodriguez-Monroy, M., Rollins, R. P., Romer, A. K., Rykoff, E. S., Salatino, M., Sánchez, C., Sanchez, E., Santiago, B., Scarpine, V., Schillaci, A., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Sherwin, B. D., Sifón, C., Smith, M., Soares-Santos, M., Staggs, S. T., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tutusaus, I., Vavagiakis, E. M., Weller, J., Wollack, E. J., Yanny, B., Yin, B., and Zhang, Y.
Abstract: We present measurements of the radial profiles of the mass and galaxy number density around Sunyaev-Zel'dovich-selected clusters using both weak lensing and galaxy counts. The clusters are selected from the Atacama Cosmology Telescope Data Release 5 and the galaxies from the Dark Energy Survey Year 3 dataset. With signal-to-noise of 62 (43) for galaxy (weak lensing) profiles over scales of about $0.2-20h^{-1}$ Mpc, these are the highest precision measurements for SZ-selected clusters to date. Because SZ selection closely approximates mass selection, these measurements enable several tests of theoretical models of the mass and light distribution around clusters. Our main findings are: 1. The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations. 2. The full mass profile is also consistent with the simulations; hence it can constrain alternative dark matter models that modify the mass distribution of clusters. 3. The shapes of the galaxy and lensing profiles are remarkably similar for our sample over the entire range of scales, from well inside the cluster halo to the quasilinear regime. This can be used to constrain processes such as quenching and tidal disruption that alter the galaxy distribution inside the halo, and scale-dependent features in the transition regime outside the halo. We measure the dependence of the profile shapes on the galaxy sample, redshift and cluster mass. We extend the Diemer \& Kravtsov model for the cluster profiles to the linear regime using perturbation theory and show that it provides a good match to the measured profiles. We also compare the measured profiles to predictions of the standard halo model and simulations that include hydrodynamics. Applications of these results to cluster mass estimation and cosmology are discussed., Comment: 15 pages, 6 figures (main) + 3 pages, 6 figures (appendix), submitted to MNRAS
Published: 2021
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37. The Dark Energy Survey Data Release 2

Author: DES Collaboration, Abbott, T. M. C., Adamow, M., Aguena, M., Allam, S., Amon, A., Annis, J., Avila, S., Bacon, D., Banerji, M., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Choi, A., Conselice, C., Costanzi, M., Crocce, M., da Costa, L. N., Davis, T. M., De Vicente, J., DeRose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Evrard, A. E., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Friedel, D., Frieman, J., García-Bellido, J., Gelman, L., Gerdes, D. W., Giannantonio, T., Gill, M., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Jeltema, T., Johnson, M. D., Kent, S., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lidman, C., Lin, H., MacCrann, N., Maia, M. A. G., Manning, T., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Myles, J., Neilsen, E., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas, A. A., Pond, C., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Rykoff, E. S., Sako, M., Sanchez, E., Santiago, B., Serrano, S., Sevilla-Noarbe, I., Smith, J. Allyn., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tremblay, P. E., Troxel, M. A., Tucker, D. L., Turner, D. J, Varga, T. N., Walker, A. R., Wechsler, R. H., Weller, J., Wester, W., Wilkinson, R. D., Yanny, B., Zhang, Y., Nikutta, R., Fitzpatrick, M., Jacques, A., Scott, A., Olsen, K., Huang, L., Herrera, D., Juneau, S., Nidever, D., Weaver, B. A., Adean, C., Correia, V., de Freitas, M., Freitas, F. N., Singulani, C., Vila-Verde, G., DES Collaboration, Abbott, T. M. C., Adamow, M., Aguena, M., Allam, S., Amon, A., Annis, J., Avila, S., Bacon, D., Banerji, M., Bechtol, K., Becker, M. R., Bernstein, G. M., Bertin, E., Bhargava, S., Bridle, S. L., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Choi, A., Conselice, C., Costanzi, M., Crocce, M., da Costa, L. N., Davis, T. M., De Vicente, J., DeRose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Evrard, A. E., Ferrero, I., Ferté, A., Flaugher, B., Fosalba, P., Friedel, D., Frieman, J., García-Bellido, J., Gelman, L., Gerdes, D. W., Giannantonio, T., Gill, M., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Huterer, D., James, D. J., Jeltema, T., Johnson, M. D., Kent, S., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lidman, C., Lin, H., MacCrann, N., Maia, M. A. G., Manning, T., March, M., Marshall, J. L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Myles, J., Neilsen, E., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Petravick, D., Pieres, A., Plazas, A. A., Pond, C., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Rykoff, E. S., Sako, M., Sanchez, E., Santiago, B., Serrano, S., Sevilla-Noarbe, I., Smith, J. Allyn., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Tremblay, P. E., Troxel, M. A., Tucker, D. L., Turner, D. J, Varga, T. N., Walker, A. R., Wechsler, R. H., Weller, J., Wester, W., Wilkinson, R. D., Yanny, B., Zhang, Y., Nikutta, R., Fitzpatrick, M., Jacques, A., Scott, A., Olsen, K., Huang, L., Herrera, D., Juneau, S., Nidever, D., Weaver, B. A., Adean, C., Correia, V., de Freitas, M., Freitas, F. N., Singulani, C., and Vila-Verde, G.
Abstract: We present the second public data release of the Dark Energy Survey, DES DR2, based on optical/near-infrared imaging by the Dark Energy Camera mounted on the 4-m Blanco telescope at Cerro Tololo Inter-American Observatory in Chile. DES DR2 consists of reduced single-epoch and coadded images, a source catalog derived from coadded images, and associated data products assembled from 6 years of DES science operations. This release includes data from the DES wide-area survey covering ~5000 deg2 of the southern Galactic cap in five broad photometric bands, grizY. DES DR2 has a median delivered point-spread function full-width at half maximum of g= 1.11, r= 0.95, i= 0.88, z= 0.83, and Y= 0.90 arcsec photometric uniformity with a standard deviation of < 3 mmag with respect to Gaia DR2 G-band, a photometric accuracy of ~10 mmag, and a median internal astrometric precision of ~27 mas. The median coadded catalog depth for a 1.95 arcsec diameter aperture at S/N= 10 is g= 24.7, r= 24.4, i= 23.8, z= 23.1 and Y= 21.7 mag. DES DR2 includes ~691 million distinct astronomical objects detected in 10,169 coadded image tiles of size 0.534 deg2 produced from 76,217 single-epoch images. After a basic quality selection, benchmark galaxy and stellar samples contain 543 million and 145 million objects, respectively. These data are accessible through several interfaces, including interactive image visualization tools, web-based query clients, image cutout servers and Jupyter notebooks. DES DR2 constitutes the largest photometric data set to date at the achieved depth and photometric precision., Comment: Accepted version. Copyright AAS. Reproduced with permission. 29 pages, 13 figures. Visit https://des.ncsa.illinois.edu/releases/dr2
Published: 2021
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38. Geometría Descriptiva y Arquitectura. Trabajos Docentes. Curso 2016-2017

Author: Pérez Naya, Antonia María, Tarrío Carrodeguas, Santiago B., Pérez Naya, Antonia María, and Tarrío Carrodeguas, Santiago B.
Published: 2021

39. Geometría Descriptiva y Arquitectura. Trabajos Docentes. Curso 2017-2018

Author: Pérez Naya, Antonia María, Tarrío Carrodeguas, Santiago B., Pérez Naya, Antonia María, and Tarrío Carrodeguas, Santiago B.
Published: 2021

40. Geometría Descriptiva y Arquitectura. Trabajos Docentes. Curso 2018-2019

Author: Pérez Naya, Antonia María, Tarrío Carrodeguas, Santiago B., Pérez Naya, Antonia María, and Tarrío Carrodeguas, Santiago B.
Published: 2021

41. Social cognition impairment in genetic frontotemporal dementia within the GENFI cohort

Author: Russell, L.L. (Lucy L.), Greaves, C.V. (Caroline V.), Bocchetta, M. (Martina), Nicholas, J.M. (Jennifer), Convery, R.S. (Rhian S.), Moore, K. (Katrina), Cash, D.M. (David M.), Swieten, J.C. (John) van, Jiskoot, L.C. (Lize), Moreno, F. (Fermin), Sánchez-Valle, R. (Raquel), Borroni, B. (Barbara), Laforce, R. (Robert), Masellis, M. (Mario), Tartaglia, M.C. (Maria Carmela), Graff, C. (Caroline), Rotondo, E. (Emanuela), Galimberti, D. (Daniela), Rowe, J.B. (James), Finger, E. (Elizabeth), Synofzik, M. (Matthis), Vandenberghe, R. (Rik), De Mendonça, A. (Alexandre), Tagliavini, F. (Fabrizio), Santana, I. (Isabel), Ducharme, S. (Simon), Butler, C. (Chris), Gerhard, A. (Alex), Levin, J. (Johannes), Danek, A. (Adrian), Otto, M. (Markus), Warren, J.D. (Jason), Rohrer, J.D. (Jonathan), Rossor, M. (Martin), Fox, N.C. (Nick), Woollacott, I.O.C. (Ione O.C.), Shafei, R. (Rachelle), Heller, C. (Carolin), Guerreiro, R. (Rita), Bras, J. (Jose), Thomas, D.L. (David L), Mead, S. (Simon), Meeter, L.H.H. (Lieke), Panman, J.L. (Jessica), Papma, J.M. (Janne), Poos, J.M. (Jackie), Thornton, A.S. (Andrew), Pijnenburg, Y. (Yolanda), Barandiaran, M. (Myriam), Indakoetxea, B. (Begoña), Gabilondo, A. (Alazne), Tainta, M. (Mikel), de Arriba, M. (Maria), Gorostidi, A. (Ana), Zulaica, M. (Miren), Villanua, J. (Jorge), Diaz, Z. (Zigor), Borrego-Ecija, S. (Sergi), Olives, J. (Jaume), Lladó, A. (Albert), Balasa, M. (Mircea), Antonell, A. (Anna), Bargallo, N. (Nuria), Premi, E. (Enrico), Cosseddu MPsych, M. (Maura), Gazzina, S. (Stefano), Padovani, A. (Alessandro), Gasparotti, R. (Roberto), Archetti, S. (Silvana), Black, S.E. (Sandra), Mitchell, S. (Sara), Rogaeva, E. (Ekaterina), Freedman, M. (Morris), Keren, R. (Ron), Tang-Wai, D. (Daid), Öijerstedt, L. (Linn), Andersson, C. (Christin), Jelic, S. (Svetislav Svetislav), Thonberg, H. (Håkan), Arighi, A. (Andrea), Fenoglio, C. (Chiara), Scarpini, E. (Elio), Fumagalli, G. (Giorgio), Cope, T. (Thomas), Timberlake, C. (Carolyn), Rittman, T. (Timothy), Shoesmith, C. (Christen), Bartha, R. (Robart), Rademakers, S. (Suzanne), Wilke, C. (Carlo), Karnarth, H.-O. (Hans-Otto), Bender, B. (Benjamin), Bruffaerts, R. (Rose), Vandamme, P. (Philip), Vandenbulcke, M. (Mathieu), Ferreira, C.B. (Catarina B.), Miltenberger, G. (Gabriel), Maruta MPsych, C. (Carolina), Verdelho, A. (Ana), Afonso, S. (Sónia), Taipa, R. (Ricardo), Caroppo, P. (Paola), Di Fede, G. (Giuseppe), Giaccone, G. (Giuseppe), Muscio, C. (Cristina), Prioni, S. (Sara), Redaelli, V. (Veronica), Rossi, G. (Giacomina), Tiraboschi, P. (Pietro), Duro NPsych, D. (Diana), Almeida, M.R. (Maria R.), Castelo-Branco, M. (Miguel), Leitão, M.J. (Maria J.), Tabuas-Pereira, M. (Miguel), Santiago, B. (Beatriz), Gauthier, S. (Serge), Rosa-Neto, P. (Pedro), Veldsman, M. (Michele), Thompson, P.M. (Paul), Langheinrich, T. (Tobias), Prix, C. (Catharina), Hoegen, T. (Tobias), Wlasich, E. (Elisabeth), Loosli, S. (Sandra), Schonecker, S. (Sonja), Semler, E. (Elisa), Anderl-Straub, S. (Sarah), Russell, L.L. (Lucy L.), Greaves, C.V. (Caroline V.), Bocchetta, M. (Martina), Nicholas, J.M. (Jennifer), Convery, R.S. (Rhian S.), Moore, K. (Katrina), Cash, D.M. (David M.), Swieten, J.C. (John) van, Jiskoot, L.C. (Lize), Moreno, F. (Fermin), Sánchez-Valle, R. (Raquel), Borroni, B. (Barbara), Laforce, R. (Robert), Masellis, M. (Mario), Tartaglia, M.C. (Maria Carmela), Graff, C. (Caroline), Rotondo, E. (Emanuela), Galimberti, D. (Daniela), Rowe, J.B. (James), Finger, E. (Elizabeth), Synofzik, M. (Matthis), Vandenberghe, R. (Rik), De Mendonça, A. (Alexandre), Tagliavini, F. (Fabrizio), Santana, I. (Isabel), Ducharme, S. (Simon), Butler, C. (Chris), Gerhard, A. (Alex), Levin, J. (Johannes), Danek, A. (Adrian), Otto, M. (Markus), Warren, J.D. (Jason), Rohrer, J.D. (Jonathan), Rossor, M. (Martin), Fox, N.C. (Nick), Woollacott, I.O.C. (Ione O.C.), Shafei, R. (Rachelle), Heller, C. (Carolin), Guerreiro, R. (Rita), Bras, J. (Jose), Thomas, D.L. (David L), Mead, S. (Simon), Meeter, L.H.H. (Lieke), Panman, J.L. (Jessica), Papma, J.M. (Janne), Poos, J.M. (Jackie), Thornton, A.S. (Andrew), Pijnenburg, Y. (Yolanda), Barandiaran, M. (Myriam), Indakoetxea, B. (Begoña), Gabilondo, A. (Alazne), Tainta, M. (Mikel), de Arriba, M. (Maria), Gorostidi, A. (Ana), Zulaica, M. (Miren), Villanua, J. (Jorge), Diaz, Z. (Zigor), Borrego-Ecija, S. (Sergi), Olives, J. (Jaume), Lladó, A. (Albert), Balasa, M. (Mircea), Antonell, A. (Anna), Bargallo, N. (Nuria), Premi, E. (Enrico), Cosseddu MPsych, M. (Maura), Gazzina, S. (Stefano), Padovani, A. (Alessandro), Gasparotti, R. (Roberto), Archetti, S. (Silvana), Black, S.E. (Sandra), Mitchell, S. (Sara), Rogaeva, E. (Ekaterina), Freedman, M. (Morris), Keren, R. (Ron), Tang-Wai, D. (Daid), Öijerstedt, L. (Linn), Andersson, C. (Christin), Jelic, S. (Svetislav Svetislav), Thonberg, H. (Håkan), Arighi, A. (Andrea), Fenoglio, C. (Chiara), Scarpini, E. (Elio), Fumagalli, G. (Giorgio), Cope, T. (Thomas), Timberlake, C. (Carolyn), Rittman, T. (Timothy), Shoesmith, C. (Christen), Bartha, R. (Robart), Rademakers, S. (Suzanne), Wilke, C. (Carlo), Karnarth, H.-O. (Hans-Otto), Bender, B. (Benjamin), Bruffaerts, R. (Rose), Vandamme, P. (Philip), Vandenbulcke, M. (Mathieu), Ferreira, C.B. (Catarina B.), Miltenberger, G. (Gabriel), Maruta MPsych, C. (Carolina), Verdelho, A. (Ana), Afonso, S. (Sónia), Taipa, R. (Ricardo), Caroppo, P. (Paola), Di Fede, G. (Giuseppe), Giaccone, G. (Giuseppe), Muscio, C. (Cristina), Prioni, S. (Sara), Redaelli, V. (Veronica), Rossi, G. (Giacomina), Tiraboschi, P. (Pietro), Duro NPsych, D. (Diana), Almeida, M.R. (Maria R.), Castelo-Branco, M. (Miguel), Leitão, M.J. (Maria J.), Tabuas-Pereira, M. (Miguel), Santiago, B. (Beatriz), Gauthier, S. (Serge), Rosa-Neto, P. (Pedro), Veldsman, M. (Michele), Thompson, P.M. (Paul), Langheinrich, T. (Tobias), Prix, C. (Catharina), Hoegen, T. (Tobias), Wlasich, E. (Elisabeth), Loosli, S. (Sandra), Schonecker, S. (Sonja), Semler, E. (Elisa), and Anderl-Straub, S. (Sarah)
Abstract: A key symptom of frontotemporal dementia (FTD) is difficulty interacting socially with others. Social cognition problems in FTD include impaired emotion processing and theory of mind difficulties, and whilst these have been studied extensively in sporadic FTD, few studies have investigated them in familial FTD. Facial Emotion Recognition (FER) and Faux Pas (FP) recognition tests were used to study social cognition within the Genetic Frontotemporal Dementia Initiative (GENFI), a large familial FTD cohort of C9orf72, GRN, and MAPT mutation carriers. 627 participants undertook at least one of the tasks, and were separated into mutation-negative healthy controls, presymptomatic mutation carriers (split into early and late groups) and symptomatic mutation carriers. Groups were compared using a linear regression model with bootstrapping, adjusting for age, sex, education, and for the FP recognition test, language. Neural correlates of social cognition deficits were explored using a voxel-based morphometry (VBM) study. All three of the symptomatic genetic groups were impaired on both tasks with no significant difference between them. However, prior to onset, only the late presymptomatic C9orf72 mutation carriers on the FER test were impaired compared to the control group, with a subanalysis showing differences particularly in fear and sadness. The VBM analysis revealed that impaired social cognition was mainly associated with a left hemisphere predominant network of regions involving particularly the striatum, orbitofrontal cortex and insula, and to a lesser extent the inferomedial temporal lobe and other areas of the frontal lobe. In conclusion, theory of mind and emotion processing abilities are impaired in familial FTD, with early changes occurring prior to symptom onset in C9orf72 presymptomatic mutation carriers. Future work should investigate how performance changes over time, in order to gain a clearer insight into social cognitive impairment over the course of the
Published: 2020
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42. Constraining radio mode feedback in galaxy clusters with the cluster radio AGNs properties to z similar to 1

Author: Gupta, N., Pannella, M., Mohr, J. J., Klein, M., Rykoff, E. S., Annis, J., Avila, S., Bianchini, F., Brooks, D., Buckley-Geer, E., Bulbul, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chiu, L, Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Evrard, A. E., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., McDonald, M., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Reichardt, C. L., Sanchez, E., Santiago, B., Saro, A., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Shao, X., Smith, M., Stott, J. P., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Vikram, V., Zenteno, A., Gupta, N., Pannella, M., Mohr, J. J., Klein, M., Rykoff, E. S., Annis, J., Avila, S., Bianchini, F., Brooks, D., Buckley-Geer, E., Bulbul, E., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chiu, L, Costanzi, M., da Costa, L. N., De Vicente, J., Desai, S., Dietrich, J. P., Doel, P., Everett, S., Evrard, A. E., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lidman, C., Lima, M., Maia, M. A. G., Marshall, J. L., McDonald, M., Menanteau, F., Miquel, R., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Reichardt, C. L., Sanchez, E., Santiago, B., Saro, A., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Shao, X., Smith, M., Stott, J. P., Strazzullo, V., Suchyta, E., Swanson, M. E. C., Vikram, V., and Zenteno, A.
Abstract: We study the properties of the Sydney University Molonglo Sky Survey (SUMSS) 843 MHz radio active galactic nuclei (AGNs) population in galaxy clusters from two large catalogues created using the Dark Energy Survey (DES): similar to 11 800 optically selected RM-Y3 and similar to 1000 X-ray selected MARD-Y3 clusters. We show that cluster radio loud AGNs are highly concentrated around cluster centres to z similar to 1. We measure the halo occupation number for cluster radio AGNs above a threshold luminosity, finding that the number of radio AGNs per cluster increases with cluster halo mass as N proportional to M-1(.2 +/- 0.1) (N proportional to M-0.(68 +/- 0.34)) for the RM-Y3 (MARD-Y3) sample. Together, these results indicate that radio mode feedback is favoured in more massive galaxy clusters. Using optical counterparts for these sources, we demonstrate weak redshift evolution in the host broad-band colours and the radio luminosity at fixed host galaxy stellar mass. We use the redshift evolution in radio luminosity to break the degeneracy between density and luminosity evolution scenarios in the redshift trend of the radio AGNs luminosity function (LF). The LF exhibits a redshift trend of the form (1 + z)(gamma) in density and luminosity, respectively, of gamma(D) = 3.0 +/- 0.4 and gamma(P) = 0.21 +/- 0.15 in the RM-Y3 sample, and gamma(D) = 2.6 +/- 0.7 and gamma(P) = 0.31 +/- 0.15 in MARD-Y3. We discuss the physical drivers of radio mode feedback in cluster AGNs, and we use the cluster radio galaxy LF to estimate the average radio-mode feedback energy as a function of cluster mass and redshift and compare it to the core (
Published: 2020

43. OzDES multi-object fibre spectroscopy for the Dark Energy Survey: Results and second data release

Author: Lidman, C., Tucker, B. E., Davis, T. M., Uddin, S. A., Asorey, J., Bolejko, K., Brout, D., Calcino, J., Carollo, D., Carr, A., Childress, M., Hoormann, J. K., Foley, R. J., Galbany, L., Glazebrook, K., Hinton, S. R., Kessler, R., Kim, A. G., King, A., Kremin, A., Kuehn, K., Lagattuta, D., Lewis, G. F., Macaulay, E., Malik, U., March, M., Martini, P., Möller, A., Mudd, D., Nichol, R. C., Panther, F., Parkinson, D., Pursiainen, M., Sako, M., Swann, E., Scalzo, R., Scolnic, D., Sharp, R., Smith, M., Sommer, N. E., Sullivan, M., Webb, S., Wiseman, P., Yu, Z., Yuan, F., Zhang, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., De Vicente, J., Doel, P., Eifler, T. F., Everett, S., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kuropatkin, N., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Rykoff, E. S., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Varga, T. N., Walker, A. R., Wester, W., Wilkinson, R. D., Lidman, C., Tucker, B. E., Davis, T. M., Uddin, S. A., Asorey, J., Bolejko, K., Brout, D., Calcino, J., Carollo, D., Carr, A., Childress, M., Hoormann, J. K., Foley, R. J., Galbany, L., Glazebrook, K., Hinton, S. R., Kessler, R., Kim, A. G., King, A., Kremin, A., Kuehn, K., Lagattuta, D., Lewis, G. F., Macaulay, E., Malik, U., March, M., Martini, P., Möller, A., Mudd, D., Nichol, R. C., Panther, F., Parkinson, D., Pursiainen, M., Sako, M., Swann, E., Scalzo, R., Scolnic, D., Sharp, R., Smith, M., Sommer, N. E., Sullivan, M., Webb, S., Wiseman, P., Yu, Z., Yuan, F., Zhang, B., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Costanzi, M., da Costa, L. N., De Vicente, J., Doel, P., Eifler, T. F., Everett, S., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., James, D. J., Kuropatkin, N., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Rykoff, E. S., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Swanson, M. E. C., Tarle, G., Tucker, D. L., Varga, T. N., Walker, A. R., Wester, W., and Wilkinson, R. D.
Abstract: We present a description of the Australian Dark Energy Survey (OzDES) and summarise the results from its six years of operations. Using the 2dF fibre positioner and AAOmega spectrograph on the 3.9-metre Anglo-Australian Telescope, OzDES has monitored 771 AGN, classified hundreds of supernovae, and obtained redshifts for thousands of galaxies that hosted a transient within the 10 deep fields of the Dark Energy Survey. We also present the second OzDES data release, containing the redshifts of almost 30,000 sources, some as faint as $r_{\mathrm AB}=24$ mag, and 375,000 individual spectra. These data, in combination with the time-series photometry from the Dark Energy Survey, will be used to measure the expansion history of the Universe out to $z\sim1.2$ and the masses of hundreds of black holes out to $z\sim4$. OzDES is a template for future surveys that combine simultaneous monitoring of targets with wide-field imaging cameras and wide-field multi-object spectrographs., Comment: 20 pages, 16 figures. Accepted for publication by MNRAS. Data release available at https://datacentral.org.au
Published: 2020
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44. A Deeper Look at DES Dwarf Galaxy Candidates: Grus I and Indus II

Author: Cantu, Sarah A., Pace, Andrew B., Marshall, Jennifer, Strigari, Louis E., Crnojevic, Denija, Simon, Joshua D., Drlica-Wagner, A., Bechtol, K., Martínez-Vázquez, Clara E., Santiago, B., Amara, A., Stringer, K. M., Diehl, H. T., Collaboration, The DES, Cantu, Sarah A., Pace, Andrew B., Marshall, Jennifer, Strigari, Louis E., Crnojevic, Denija, Simon, Joshua D., Drlica-Wagner, A., Bechtol, K., Martínez-Vázquez, Clara E., Santiago, B., Amara, A., Stringer, K. M., Diehl, H. T., and Collaboration, The DES
Abstract: We present deep $g$- and $r$-band Magellan/Megacam photometry of two dwarf galaxy candidates discovered in the Dark Energy Survey (DES), Grus I and Indus II (DES J2038-4609). For the case of Grus I, we resolved the main sequence turn-off (MSTO) and $\sim 2$ mags below it. The MSTO can be seen at $g_0\sim 24$ with a photometric uncertainty of $0.03$ mag. We show Grus I to be consistent with an old, metal-poor ($\sim 13.3$ Gyr, [Fe/H]$\sim-1.9$) dwarf galaxy. We derive updated distance and structural parameters for Grus I using this deep, uniform, wide-field data set. We find an azimuthally averaged half-light radius more than two times larger ($\sim 151^{+21}_{-31}$ pc; $\sim 4.^{\prime} 16^{+0.54}_{-0.74}$) and an absolute $V$-band magnitude $\sim-4.1$ that is $\sim 1$ magnitude brighter than previous studies. We obtain updated distance, ellipticity, and centroid parameters which are in agreement with other studies within uncertainties. Although our photometry of Indus II is $\sim 2-3$ magnitudes deeper than the DES Y1 Public release, we find no coherent stellar population at its reported location. The original detection was located in an incomplete region of sky in the DES Y2Q1 data set and was flagged due to potential blue horizontal branch member stars. The best fit isochrone parameters are physically inconsistent with both dwarf galaxies and globular clusters. We conclude that Indus II is likely a false-positive, flagged due to a chance alignment of stars along the line of sight., Comment: 16 pages, 8 figures; submitted to ApJ
Published: 2020
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45. Chemical Analysis of the Ultra-Faint Dwarf Galaxy Grus~II. Signature of high-mass stellar nucleosynthesis

Author: Hansen, T. T., Marshall, J. L., Simon, J. D., Li, T. S., Bernstein, R. A., Pace, A. B., Ferguson, P., Nagasawa, D. Q., Kuehn, K., Carollo, D., Geha, M., James, D., Walker, A., Diehl, H. T., Aguena, M., Allam, S., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., Desai, S., De Vicente, J., Doel, P., Eckert, K., Eifler, T. F., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuropatkin, N., Maia, M. A. G., March, M., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Varga, T. N., Wilkinson, R., Hansen, T. T., Marshall, J. L., Simon, J. D., Li, T. S., Bernstein, R. A., Pace, A. B., Ferguson, P., Nagasawa, D. Q., Kuehn, K., Carollo, D., Geha, M., James, D., Walker, A., Diehl, H. T., Aguena, M., Allam, S., Avila, S., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Costanzi, M., da Costa, L. N., Desai, S., De Vicente, J., Doel, P., Eckert, K., Eifler, T. F., Everett, S., Ferrero, I., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Kuropatkin, N., Maia, M. A. G., March, M., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Varga, T. N., and Wilkinson, R.
Abstract: We present a detailed abundance analysis of the three brightest member stars at the top of the giant branch of the ultra-faint dwarf galaxy Grus~II. All stars exhibit a higher than expected $\mathrm{[Mg/Ca]}$ ratio compared to metal-poor stars in other ultra-faint dwarf galaxies and in the Milky Way halo. Nucleosynthesis in high mass ($\geqslant 20$M$_\odot$) core-collapse supernovae has been shown to create this signature. The abundances of this small sample (3) stars suggest the chemical enrichment of Grus~II could have occurred through substantial high-mass stellar evolution and is consistent with the framework of a top-heavy initial mass function. However, with only three stars it can not be ruled out that the abundance pattern is the result of a stochastic chemical enrichment at early times in the galaxy. The most metal-rich of the three stars also possesses a small enhancement in rapid neutron-capture ($r$-process) elements. The abundance pattern of the $r$-process elements in this star matches the scaled $r$-process pattern of the solar system and $r$-process enhanced stars in other dwarf galaxies and in the Milky Way halo, hinting at a common origin for these elements across a range of environments. All current proposed astrophysical sites of $r$-process element production are associated with high-mass stars, thus the possible top-heavy initial mass function of Grus~II would increase the likelihood of any of these events occurring. The time delay between the $\alpha$ and $r$-process element enrichment of the galaxy favors a neutron star merger as the origin of the $r$-process elements in Grus~II., Comment: 17 pages, 6 figures, accepted for publication in ApJ
Published: 2020
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46. Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution?

Author: Sampaio-Santos, H., Zhang, Y., Ogando, R. L. C., Shin, T., Golden-Marx, Jesse B., Yanny, B., Herner, K., Hilton, M., Choi, A., Gatti, M., Gruen, D., Hoyle, B., Rau, M. M., De Vicente, J., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Kind, M. Carrasco, Carretero, J., Chang, C., Costanzi, M., da Costa, L. N., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., March, M., Marshall, J. L., Miquel, R., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Smith, M., Suchyta, E., Tarle, G., Tucker, D. L., Varga, T. N., Wechsler, R. H., Sampaio-Santos, H., Zhang, Y., Ogando, R. L. C., Shin, T., Golden-Marx, Jesse B., Yanny, B., Herner, K., Hilton, M., Choi, A., Gatti, M., Gruen, D., Hoyle, B., Rau, M. M., De Vicente, J., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Kind, M. Carrasco, Carretero, J., Chang, C., Costanzi, M., da Costa, L. N., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., March, M., Marshall, J. L., Miquel, R., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Smith, M., Suchyta, E., Tarle, G., Tucker, D. L., Varga, T. N., and Wechsler, R. H.
Abstract: We explore the relation between diffuse intracluster light (central galaxy included) and the galaxy cluster (baryonic and dark) matter distribution using a sample of 528 clusters at $0.2\leq z \leq 0.35$ found in the Dark Energy Survey (DES) Year 1 data. The surface brightness of the diffuse light shows an increasing dependence on cluster total mass at larger radius, and appears to be self-similar with a universal radial dependence after scaling by cluster radius. We also compare the diffuse light radial profiles to the cluster (baryonic and dark) matter distribution measured through weak lensing and find them to be comparable. The IllustrisTNG galaxy formation simulation, TNG300, offers further insight into the connection between diffuse stellar mass and cluster matter distributions -- the simulation radial profile of the diffuse stellar component does not have a similar slope with the total cluster matter content, although that of the cluster satellite galaxies does. Regardless of the radial trends, the amount of diffuse stellar mass has a low-scatter scaling relation with cluster's total mass in the simulation, out-performing the total stellar mass of cluster satellite galaxies. We conclude that there is no consistent evidence yet on whether or not diffuse light is a faithful radial tracer of the cluster matter distribution. Nevertheless, both observational and simulation results reveal that diffuse light is an excellent indicator of the cluster's total mass., Comment: Accepted on MNRAS
Published: 2020
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47. Increasing the census of L and T dwarfs in wide binary and multiple systems using Dark Energy Survey DR1 and Gaia DR2 data

Author: Ponte, M. dal, Santiago, B., Rosell, A. Carnero, Burningham, B., Yanny, B., Marshall, J. L., Bechtol, K., Martini, P., Li, T. S., De Paris, L., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Kind, M. Carrasco, Carretero, J., da Costa, L. N., De Vicente, J., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Maia, M. A. G., March, M., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., Walker, A. R., Ponte, M. dal, Santiago, B., Rosell, A. Carnero, Burningham, B., Yanny, B., Marshall, J. L., Bechtol, K., Martini, P., Li, T. S., De Paris, L., Abbott, T. M. C., Aguena, M., Allam, S., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Buckley-Geer, E., Kind, M. Carrasco, Carretero, J., da Costa, L. N., De Vicente, J., Diehl, H. T., Doel, P., Eifler, T. F., Everett, S., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Maia, M. A. G., March, M., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Varga, T. N., and Walker, A. R.
Abstract: We present the discovery of 255 binary and six multiple system candidates with wide > 5" separation composed by ultracool dwarfs companions to stars, plus nine double ultracool dwarf systems. These systems were selected based on common distance criteria. About 90% of the total sample has proper motions available and 73% of the systems also satisfy a common proper motion criterion. The sample of ultracool candidates was taken from the Dark Energy Survey (DES) and the candidate stellar primaries are from Gaia DR2 and DES data. We compute chance alignment probabilities in order to assess the physical nature of each pair. We find that 174 candidate pairs with Gaia DR2 primaries and 81 pairs with a DES star as a primary have chance alignment probabilities < 5%. Only nine candidate systems composed of two ultracool dwarfs were identified. The sample of candidate multiple systems is made up of five triple systems and one quadruple system. The majority of the ultracool dwarfs found in binaries and multiples are of early L type and the typical wide binary fraction over the L spectral types is 2-4%. Our sample of candidate wide binaries with ultracool dwarfs as secondaries constitutes a substantial increase over the known number of such systems, which are very useful to constrain the formation and evolution of ultracool dwarfs., Comment: 18 pages, 10 figures. Accepted by MNRAS
Published: 2020
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48. Age at symptom onset and death and disease duration in genetic frontotemporal dementia: an international retrospective cohort study

Author: Moore, KM, Nicholas, J, Grossman, M, McMillan, CT, Irwin, DJ, Massimo, L, Van Deerlin, VM, Warren, JD, Fox, NC, Rossor, MN, Mead, S, Bocchetta, M, Boeve, BF, Knopman, DS, Graff-Radford, NR, Forsberg, LK, Rademakers, R, Wszolek, ZK, van Swieten, JC, Jiskoot, LC, Meeter, LH, Dopper, EGP, Papma, JM, Snowden, JS, Saxon, J, Jones, M, Pickering-Brown, S, Le Ber, I, Camuzat, A, Brice, A, Caroppo, P, Ghidoni, R, Pievani, M, Benussi, L, Binetti, G, Dickerson, BC, Lucente, D, Krivensky, S, Graff, C, Oijerstedt, L, Fallstrom, M, Thonberg, H, Ghoshal, N, Morris, JC, Borroni, B, Benussi, A, Padovani, A, Galimberti, D, Scarpini, E, Fumagalli, GG, Mackenzie, IR, Hsiung, G-YR, Sengdy, P, Boxer, AL, Rosen, H, Taylor, JB, Synofzik, M, Wilke, C, Sulzer, P, Hodges, JR, Halliday, G, Kwok, J, Sanchez-Valle, R, Llado, A, Borrego-Ecija, S, Santana, I, Almeida, MR, Tabuas-Pereira, M, Moreno, F, Barandiaran, M, Indakoetxea, B, Levin, J, Danek, A, Rowe, JB, Cope, TE, Otto, M, Anderl-Straub, S, de Mendonca, A, Maruta, C, Masellis, M, Black, SE, Couratier, P, Lautrette, G, Huey, ED, Sorbi, S, Nacmias, B, Laforce, R, Tremblay, M-PL, Vandenberghe, R, Van Damme, P, Rogalski, EJ, Weintraub, S, Gerhard, A, Onyike, CU, Ducharme, S, Papageorgiou, SG, Ng, ASL, Brodtmann, A, Finger, E, Guerreiro, R, Bras, J, Rohrer, JD, Heller, C, Convery, R, Woollacott, IOC, Shafei, R, Graff-Radford, J, Jones, DT, Dheel, CM, Savica, R, Lapid, MI, Baker, M, Fields, JA, Gavrilova, R, Domoto-Reilly, K, Poos, JM, van der Ende, EL, Panman, JL, Kaat, LD, Seelaar, H, Richardson, A, Frisoni, G, Mega, A, Fostinelli, S, Chiang, H-H, Alberici, A, Arighi, A, Fenoglio, C, Heuer, H, Miller, B, Karydas, A, Fong, J, Leitao, MJ, Santiago, B, Duro, D, Ferreira, C, Gabilondo, A, de Arriba, M, Tainta, M, Zulaica, M, Ferreira, CB, Semler, E, Ludolph, A, Landwehrmeyer, B, Volk, AE, Miltenberger, G, Verdelho, A, Afonso, S, Tartaglia, MC, Freedman, M, Rogaeva, E, Ferrari, C, Piaceri, I, Bessi, V, Lombardi, G, St-Onge, F, Dore, M-C, Bruffaerts, R, Vandenbulcke, M, Van den Stock, J, Mesulam, MM, Bigio, E, Koros, C, Papatriantafyllou, J, Kroupis, C, Stefanis, L, Shoesmith, C, Roberson, E, Coppola, G, Ramos, EMDS, Geschwind, D, Moore, KM, Nicholas, J, Grossman, M, McMillan, CT, Irwin, DJ, Massimo, L, Van Deerlin, VM, Warren, JD, Fox, NC, Rossor, MN, Mead, S, Bocchetta, M, Boeve, BF, Knopman, DS, Graff-Radford, NR, Forsberg, LK, Rademakers, R, Wszolek, ZK, van Swieten, JC, Jiskoot, LC, Meeter, LH, Dopper, EGP, Papma, JM, Snowden, JS, Saxon, J, Jones, M, Pickering-Brown, S, Le Ber, I, Camuzat, A, Brice, A, Caroppo, P, Ghidoni, R, Pievani, M, Benussi, L, Binetti, G, Dickerson, BC, Lucente, D, Krivensky, S, Graff, C, Oijerstedt, L, Fallstrom, M, Thonberg, H, Ghoshal, N, Morris, JC, Borroni, B, Benussi, A, Padovani, A, Galimberti, D, Scarpini, E, Fumagalli, GG, Mackenzie, IR, Hsiung, G-YR, Sengdy, P, Boxer, AL, Rosen, H, Taylor, JB, Synofzik, M, Wilke, C, Sulzer, P, Hodges, JR, Halliday, G, Kwok, J, Sanchez-Valle, R, Llado, A, Borrego-Ecija, S, Santana, I, Almeida, MR, Tabuas-Pereira, M, Moreno, F, Barandiaran, M, Indakoetxea, B, Levin, J, Danek, A, Rowe, JB, Cope, TE, Otto, M, Anderl-Straub, S, de Mendonca, A, Maruta, C, Masellis, M, Black, SE, Couratier, P, Lautrette, G, Huey, ED, Sorbi, S, Nacmias, B, Laforce, R, Tremblay, M-PL, Vandenberghe, R, Van Damme, P, Rogalski, EJ, Weintraub, S, Gerhard, A, Onyike, CU, Ducharme, S, Papageorgiou, SG, Ng, ASL, Brodtmann, A, Finger, E, Guerreiro, R, Bras, J, Rohrer, JD, Heller, C, Convery, R, Woollacott, IOC, Shafei, R, Graff-Radford, J, Jones, DT, Dheel, CM, Savica, R, Lapid, MI, Baker, M, Fields, JA, Gavrilova, R, Domoto-Reilly, K, Poos, JM, van der Ende, EL, Panman, JL, Kaat, LD, Seelaar, H, Richardson, A, Frisoni, G, Mega, A, Fostinelli, S, Chiang, H-H, Alberici, A, Arighi, A, Fenoglio, C, Heuer, H, Miller, B, Karydas, A, Fong, J, Leitao, MJ, Santiago, B, Duro, D, Ferreira, C, Gabilondo, A, de Arriba, M, Tainta, M, Zulaica, M, Ferreira, CB, Semler, E, Ludolph, A, Landwehrmeyer, B, Volk, AE, Miltenberger, G, Verdelho, A, Afonso, S, Tartaglia, MC, Freedman, M, Rogaeva, E, Ferrari, C, Piaceri, I, Bessi, V, Lombardi, G, St-Onge, F, Dore, M-C, Bruffaerts, R, Vandenbulcke, M, Van den Stock, J, Mesulam, MM, Bigio, E, Koros, C, Papatriantafyllou, J, Kroupis, C, Stefanis, L, Shoesmith, C, Roberson, E, Coppola, G, Ramos, EMDS, and Geschwind, D
Abstract: BACKGROUND: Frontotemporal dementia is a heterogenous neurodegenerative disorder, with about a third of cases being genetic. Most of this genetic component is accounted for by mutations in GRN, MAPT, and C9orf72. In this study, we aimed to complement previous phenotypic studies by doing an international study of age at symptom onset, age at death, and disease duration in individuals with mutations in GRN, MAPT, and C9orf72. METHODS: In this international, retrospective cohort study, we collected data on age at symptom onset, age at death, and disease duration for patients with pathogenic mutations in the GRN and MAPT genes and pathological expansions in the C9orf72 gene through the Frontotemporal Dementia Prevention Initiative and from published papers. We used mixed effects models to explore differences in age at onset, age at death, and disease duration between genetic groups and individual mutations. We also assessed correlations between the age at onset and at death of each individual and the age at onset and at death of their parents and the mean age at onset and at death of their family members. Lastly, we used mixed effects models to investigate the extent to which variability in age at onset and at death could be accounted for by family membership and the specific mutation carried. FINDINGS: Data were available from 3403 individuals from 1492 families: 1433 with C9orf72 expansions (755 families), 1179 with GRN mutations (483 families, 130 different mutations), and 791 with MAPT mutations (254 families, 67 different mutations). Mean age at symptom onset and at death was 49·5 years (SD 10·0; onset) and 58·5 years (11·3; death) in the MAPT group, 58·2 years (9·8; onset) and 65·3 years (10·9; death) in the C9orf72 group, and 61·3 years (8·8; onset) and 68·8 years (9·7; death) in the GRN group. Mean disease duration was 6·4 years (SD 4·9) in the C9orf72 group, 7·1 years (3·9) in the GRN group, and 9·3 years (6·4) in the MAPT group. Individual age at onset and at
Published: 2020

49. Reducing ground-based astrometric errors with Gaia and Gaussian processes

Author: Fortino, W. F., Bernstein, G. M., Bernardinelli, P. H., Aguena, M., Allam, S., Annis, J., Bacon, D., Bechtol, K., Bhargava, S., Brooks, D., Burke, D. L., Carretero, J., Choi, A., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Doel, P., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Evrard, A. E., Ferrero, I., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Kent, S., Kuehn, K., Kuropatkin, N., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Myles, J., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Rykoff, E. S., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., To, C., Tucker, D. L., Varga, T. N., Walker, A. R., Weller, J., Wester, W., Fortino, W. F., Bernstein, G. M., Bernardinelli, P. H., Aguena, M., Allam, S., Annis, J., Bacon, D., Bechtol, K., Bhargava, S., Brooks, D., Burke, D. L., Carretero, J., Choi, A., Costanzi, M., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., Doel, P., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Evrard, A. E., Ferrero, I., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Kent, S., Kuehn, K., Kuropatkin, N., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Myles, J., Ogando, R. L. C., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Roodman, A., Rykoff, E. S., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., To, C., Tucker, D. L., Varga, T. N., Walker, A. R., Weller, J., and Wester, W.
Abstract: Stochastic field distortions caused by atmospheric turbulence are a fundamental limitation to the astrometric accuracy of ground-based imaging. This distortion field is measurable at the locations of stars with accurate positions provided by the Gaia DR2 catalog; we develop the use of Gaussian process regression (GPR) to interpolate the distortion field to arbitrary locations in each exposure. We introduce an extension to standard GPR techniques that exploits the knowledge that the 2-dimensional distortion field is curl-free. Applied to several hundred 90-second exposures from the Dark Energy Survey as a testbed, we find that the GPR correction reduces the variance of the turbulent distortions $\approx12\times$, on average, with better performance in denser regions of the Gaia catalog. The RMS per-coordinate distortion in the $riz$ bands is typically $\approx7$ mas before any correction, and $\approx2$ mas after application of the GPR model. The GPR astrometric corrections are validated by the observation that their use reduces, from 10 to 5 mas RMS, the residuals to an orbit fit to $riz$-band observations over 5 years of the $r=18.5$ trans-Neptunian object Eris. We also propose a GPR method, not yet implemented, for simultaneously estimating the turbulence fields and the 5-dimensional stellar solutions in a stack of overlapping exposures, which should yield further turbulence reductions in future deep surveys., Comment: 18 pages, 6 figures
Published: 2020
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50. Dark Energy Survey Year 1 Results: Cosmological Constraints from Cluster Abundances, Weak Lensing, and Galaxy Correlations

Author: To, C., Krause, E., Rozo, E., Wu, H., Gruen, D., Wechsler, R. H., Eifler, T. F., Rykoff, E. S., Costanzi, M., Becker, M. R., Bernstein, G. M., Blazek, J., Bocquet, S., Bridle, S. L., Cawthon, R., Choi, A., Crocce, M., Davis, C., DeRose, J., Drlica-Wagner, A., Elvin-Poole, J., Fang, X., Farahi, A., Friedrich, O., Gatti, M., Gaztanaga, E., Giannantonio, T., Hartley, W. G., Hoyle, B., Jarvis, M., MacCrann, N., McClintock, T., Miranda, V., Pereira, M. E. S., Park, Y., Porredon, A., Prat, J., Rau, M. M., Ross, A. J., Samuroff, S., Sánchez, C., Sevilla-Noarbe, I., Sheldon, E., Troxel, M. A., Varga, T. N., Vielzeuf, P., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Annis, J., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chang, C., Conselice, C., da Costa, L. N., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Huterer, D., James, D. J., Jeltema, T., Kron, R., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Myles, J., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Weller, J., Wester, W., To, C., Krause, E., Rozo, E., Wu, H., Gruen, D., Wechsler, R. H., Eifler, T. F., Rykoff, E. S., Costanzi, M., Becker, M. R., Bernstein, G. M., Blazek, J., Bocquet, S., Bridle, S. L., Cawthon, R., Choi, A., Crocce, M., Davis, C., DeRose, J., Drlica-Wagner, A., Elvin-Poole, J., Fang, X., Farahi, A., Friedrich, O., Gatti, M., Gaztanaga, E., Giannantonio, T., Hartley, W. G., Hoyle, B., Jarvis, M., MacCrann, N., McClintock, T., Miranda, V., Pereira, M. E. S., Park, Y., Porredon, A., Prat, J., Rau, M. M., Ross, A. J., Samuroff, S., Sánchez, C., Sevilla-Noarbe, I., Sheldon, E., Troxel, M. A., Varga, T. N., Vielzeuf, P., Zhang, Y., Zuntz, J., Abbott, T. M. C., Aguena, M., Annis, J., Avila, S., Bertin, E., Bhargava, S., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Chang, C., Conselice, C., da Costa, L. N., Davis, T. M., Desai, S., Diehl, H. T., Dietrich, J. P., Everett, S., Evrard, A. E., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gruendl, R. A., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Huterer, D., James, D. J., Jeltema, T., Kron, R., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Muir, J., Myles, J., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Santiago, B., Scarpine, V., Serrano, S., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Tucker, D. L., Weller, J., and Wester, W.
Abstract: Combining multiple observational probes is a powerful technique to provide robust and precise constraints on cosmological parameters. In this letter, we present the first joint analysis of cluster abundances and auto/cross correlations of three cosmic tracer fields measured from the first year data of the Dark Energy Survey: galaxy density, weak gravitational lensing shear, and cluster density split by optical richness. From a joint analysis of cluster abundances, three cluster cross-correlations, and auto correlations of galaxy density, we obtain $\Omega_{\rm{m}}=0.305^{+0.055}_{-0.038}$ and $\sigma_8=0.783^{+0.064}_{-0.054}$. This result is consistent with constraints from the DES-Y1 galaxy clustering and weak lensing two-point correlation functions for the flat $\nu\Lambda$CDM model. We thus combine cluster abundances and all two-point correlations from three cosmic tracer fields and find improved constraints on cosmological parameters as well as on the cluster observable--mass scaling relation. This analysis is an important advance in both optical cluster cosmology and multi-probe analyses of upcoming wide imaging surveys., Comment: 14 pages, 7 figures, 2 tables; submitted to PRL; comments are welcome
Published: 2020
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