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1. Using graph neural networks to reconstruct charged pion showers in the CMS High Granularity Calorimeter

Author

Aamir, M., Acar, B., Adamov, G., Adams, T., Adloff, C., Afanasiev, S., Agrawal, C., Ahmad, A., Ahmed, H. A., Akbar, S., Akchurin, N., Akgul, B., Akgun, B., Akpinar, R. O., Aktas, E., AlKadhim, A., Alexakhin, V., Alimena, J., Alison, J., Alpana, A., Alshehri, W., Dominguez, P. Alvarez, Alyari, M., Amendola, C., Amir, R. B., Andersen, S. B., Andreev, Y., Antoszczuk, P. D., Aras, U., Ardila, L., Aspell, P., Avila, M., Awad, I., Aydilek, O., Azimi, Z., Pretel, A. Aznar, Bach, O. A., Bainbridge, R., Bakshi, A., Bam, B., Banerjee, S., Barney, D., Bayraktar, O., Beaudette, F., Beaujean, F., Becheva, E., Behera, P. K., Belloni, A., Bergauer, T., Besancon, M., Bylund, O. Bessidskaia, Bhatt, L., Bhowmil, D., Blekman, F., Blinov, P., Bloch, P., Bodek, A., Boger, a., Bonnemaison, A., Bouyjou, F., Brennan, L., Brondolin, E., Brusamolino, A., Bubanja, I., Perraguin, A. Buchot, Bunin, P., Misura, A. Burazin, Butler-nalin, A., Cakir, A., Callier, S., Campbell, S., Canderan, K., Cankocak, K., Cappati, A., Caregari, S., Carron, S., Carty, C., Cauchois, A., Ceard, L., Cerci, S., Chang, P. J., Chatterjee, R. M., Chatterjee, S., Chattopadhyay, P., Chatzistavrou, T., Chaudhary, M. S., Chauhan, A., Chen, J. A., Chen, J., Chen, Y., Cheng, K., Cheung, H., Chhikara, J., Chiron, A., Chiusi, M., Chokheli, D., Chudasama, R., Clement, E., Mendez, S. Coco, Coko, D., Coskun, K., Couderc, F., Crossman, B., Cui, Z., Cuisset, T., Cummings, G., Curtis, E. M., D'Alfonso, M., D-hler-ball, J., Dadazhanova, O., Damgov, J., Das, I., DasGupta, S., Dauncey, P., Mendes, A. David Tinoco, Davies, G., Davignon, O., DeLa, P. deBarbaroC., DeSilva, M., DeWit, A., Debbins, P., Defranchis, M. M., Delagnes, E., Devouge, P., Dewangan, C., DiGuglielmo, G., Diehl, L., Dilsiz, K., Dincer, G. G., Dittmann, J., Dragicevic, M., Du, D., Dubinchik, B., Dugad, S., Dulucq, F., Dumanoglu, I., Duran, B., Dutta, S., Dutta, V., Dychkant, A., Dünser, M., Edberg, T., Ehle, I. T., Berni, A. El, Elias, F., Eno, S. C., Erdogan, E. N., Erkmen, B., Ershov, Y., Ertorer, E. Y., Extier, S., Eychenne, L., Fedar, Y. E., Fedi, G., De Almeida, J. P. Figueiredo De De Sá Sousa, Alves, B. A. Fontana Santos Santos, Frahm, E., Francis, K., Freeman, J., French, T., Gaede, F., Gandhi, P. K., Ganjour, S., Garcia-Bellido, A., Gastaldi, F., Gazi, L., Gecse, Z., Gerwig, H., Gevin, O., Ghosh, S., Gill, K., Gleyzer, S., Godinovic, N., Goek, M., Goettlicher, P., Goff, R., Golunov, A., Gonultas, B., Martínez, J. D. González, Gorbounov, N., Gouskos, L., Gray, A., Gray, L., Grieco, C., Groenroos, S., Groner, D., Gruber, A., Grummer, A., Grönroos, S., Guilloux, F., Guler, Y., Gungordu, A. D., Guo, J., Guo, K., Guler, E. Gurpinar, Gutti, H. K., Guvenli, A. A., Gülmez, E., Hacisahinoglu, B., Halkin, Y., Machado, G. Hamilton Ilha, Hare, H. S., Hatakeyama, K., Heering, A. H., Hegde, V., Heintz, U., Hinton, N., Hinzmann, A., Hirschauer, J., Hitlin, D., Hos, İ., Hou, B., Hou, X., Howard, A., Howe, C., Hsieh, H., Hsu, T., Hua, H., Hummer, F., Imran, M., Incandela, J., Iren, E., Isildak, B., Jackson, P. S., Jackson, W. J., Jain, S., Jana, P., Jaroslavceva, J., Jena, S., Jige, A., Jordano, P. P., Joshi, U., Kaadze, K., Kafizov, A., Kalipoliti, L., Tharayil, A. Kallil, Kaluzinska, O., Kamble, S., Kaminskiy, A., Kanemura, M., Kanso, H., Kao, Y., Kapic, A., Kapsiak, C., Karjavine, V., Karmakar, S., Karneyeu, A., Kaya, M., Topaksu, A. Kayis, Kaynak, B., Kazhykarim, Y., Khan, F. A., Khudiakov, A., Kieseler, J., Kim, R. S., Klijnsma, T., Kloiber, E. G., Klute, M., Kocak, Z., Kodali, K. R., Koetz, K., Kolberg, T., Kolcu, O. B., Komaragiri, J. R., Komm, M., Kopsalis, I., Krause, H. A., Krawczyk, M. A., Vinayakam, T. R. Krishnaswamy, Kristiansen, K., Kristic, A., Krohn, M., Kronheim, B., Krüger, K., Kudtarkar, C., Kulis, S., Kumar, M., Kumar, N., Kumar, S., Verma, R. Kumar, Kunori, S., Kunts, A., Kuo, C., Kurenkov, A., Kuryatkov, V., Kyre, S., Ladenson, J., Lamichhane, K., Landsberg, G., Langford, J., Laudrain, A., Laughlin, R., Lawhorn, J., Dortz, O. Le, Lee, S. W., Lektauers, A., Lelas, D., Leon, M., Levchuk, L., Li, A. J., Li, J., Li, Y., Liang, Z., Liao, H., Lin, K., Lin, W., Lin, Z., Lincoln, D., Linssen, L., Litomin, A., Liu, G., Liu, Y., Lobanov, A., Lohezic, V., Loiseau, T., Lu, C., Lu, R., Lu, S. Y., Lukens, P., Mackenzie, M., Magnan, A., Magniette, F., Mahjoub, A., Mahon, D., Majumder, G., Makarenko, V., Malakhov, A., Malgeri, L., Mallios, S., Mandloi, C., Mankel, A., Mannelli, M., Mans, J., Mantilla, C., Martinez, G., Massa, C., Masterson, P., Matthewman, M., Matveev, V., Mayekar, S., Mazlov, I., Mehta, A., Mestvirishvili, A., Miao, Y., Milella, G., Mirza, I. R., Mitra, P., Moccia, S., Mohanty, G. B., Monti, F., Moortgat, F., Murthy, S., Music, J., Musienko, Y., Nabili, S., Nayak, S., Nelson, J. W., Nema, A., Neutelings, I., Niedziela, J., Nikitenko, A., Noonan, D., Noy, M., Nurdan, K., Obraztsov, S., Ochando, C., Ogul, H., Olsson, J., Onel, Y., Ozkorucuklu, S., Paganis, E., Palit, P., Pan, R., Pandey, S., Pantaleo, F., Papageorgakis, C., Paramesvaran, S., Paranjpe, M. M., Parolia, S., Parsons, A. G., Parygin, P., Paulini, M., Paus, C., Peñaló, K., Pedro, K., Pekic, V., Peltola, T., Peng, B., Perego, A., Perini, D., Petrilli, A., Pham, H., Pierre-Emile, T., Podem, S. K., Popov, V., Portales, L., Potok, O., Pradeep, P. B., Pramanik, R., Prosper, H., Prvan, M., Qasim, S. R., Qu, H., Quast, T., Trivino, A. Quiroga, Rabour, L., Raicevic, N., Rajpoot, H., Rao, M. A., Rapacz, K., Redjeb, W., Reinecke, M., Revering, M., Roberts, A., Rohlf, J., Rosado, P., Rose, A., Rothman, S., Rout, P. K., Rovere, M., Rumerio, P., Rusack, R., Rygaard, L., Ryjov, V., Sadivnycha, S., Sahin, M. Ö., Sakarya, U., Salerno, R., Saradhy, R., Saraf, M., Sarbandi, K., Sarkisla, M. A., Satyshev, I., Saud, N., Sauvan, J., Schindler, G., Schmidt, A., Schmidt, I., Schmitt, M. H., Sculac, A., Sculac, T., Sedelnikov, A., Seez, C., Sefkow, F., Selivanova, D., Selvaggi, M., Sergeychik, V., Sert, H., Shahid, M., Sharma, P., Sharma, R., Sharma, S., Shelake, M., Shenai, A., Shih, C. W., Shinde, R., Shmygol, D., Shukla, R., Sicking, E., Silva, P., Simsek, C., Simsek, E., Sirasva, B. K., Sirois, Y., Song, S., Song, Y., Soudais, G., Sriram, S., StJacques, R. R., StahlLeiton, A. G., Steen, A., Stein, J., Strait, J., Strobbe, N., Su, X., Sukhov, E., Suleiman, A., Cerci, D. Sunar, Suryadevara, P., Swain, K., Syal, C., Tali, B., Tanay, K., Tang, W., Tanvir, A., Tao, J., Tarabini, A., Tatli, T., Taylor, R., Taysi, Z. C., Teafoe, G., Tee, C. Z., Terrill, W., Thienpont, D., Thomas, R., Titov, M., Todd, C., Todd, E., Toms, M., Tosun, A., Troska, J., Tsai, L., Tsamalaidze, Z., Tsionou, D., Tsipolitis, G., Tsirigoti, M., Tu, R., Polat, S. N. Tural, Undleeb, S., Usai, E., Uslan, E., Ustinov, V., Vernazza, E., Viahin, O., Viazlo, O., Vichoudis, P., Vijay, A., Virdee, T., Voirin, E., Vojinovic, M., Voytishin, N., Vámi, T. Á., Wade, A., Walter, D., Wang, C., Wang, F., Wang, J., Wang, K., Wang, X., Wang, Y., Wang, Z., Wanlin, E., Wayne, M., Wetzel, J., Whitbeck, A., Wickwire, R., Wilmot, D., Wilson, J., Wu, H., Xiao, M., Yang, J., Yazici, B., Ye, Y., Yetkin, T., Yi, R., Yohay, R., Yu, T., Yuan, C., Yuan, X., Yuksel, O., YushmanoV, I., Yusuff, I., Zabi, A., Zareckis, D., Zarubin, A., Zehetner, P., Zghiche, A., Zhang, C., Zhang, D., Zhang, H., Zhang, J., Zhang, Z., Zhao, X., Zhong, J., Zhou, Y., and Zorbilmez, Ç.

Subjects
Physics - Instrumentation and Detectors, High Energy Physics - Experiment, Physics - Data Analysis, Statistics and Probability
Abstract

A novel method to reconstruct the energy of hadronic showers in the CMS High Granularity Calorimeter (HGCAL) is presented. The HGCAL is a sampling calorimeter with very fine transverse and longitudinal granularity. The active media are silicon sensors and scintillator tiles readout by SiPMs and the absorbers are a combination of lead and Cu/CuW in the electromagnetic section, and steel in the hadronic section. The shower reconstruction method is based on graph neural networks and it makes use of a dynamic reduction network architecture. It is shown that the algorithm is able to capture and mitigate the main effects that normally hinder the reconstruction of hadronic showers using classical reconstruction methods, by compensating for fluctuations in the multiplicity, energy, and spatial distributions of the shower's constituents. The performance of the algorithm is evaluated using test beam data collected in 2018 prototype of the CMS HGCAL accompanied by a section of the CALICE AHCAL prototype. The capability of the method to mitigate the impact of energy leakage from the calorimeter is also demonstrated., Comment: Prepared for submission to JINST

Published
2024

2. The WHaD diagram: Classifying the ionizing source with one single emission line

Author

Sánchez, S. F., Lugo-Aranda, A. Z., Almeida, J. Sánchez, Barrera-Ballesteros, J. K., Gonzalez-Martín, O., Salim, S., and Agostino6, C. J.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The usual approach to classify the ionizing source using optical spectroscopy is based on the use of diagnostic diagrams that compares the relative strength of pairs of collisitional metallic lines (e.g., [O iii] and [N ii]) with respect to recombination hydrogen lines (e.g., H{\beta} and H{\alpha}). Despite of being accepted as the standard procedure, it present known problems, including confusion regimes and/or limitations related to the required signal-to-noise of the involved emission lines. These problems affect not only our intrinsic understanding of inter-stellar medium and its poroperties, but also fundamental galaxy properties, such as the star-formation rate and the oxygen abundance, and key questions just as the fraction of active galactic nuclei, among several others. We explore the existing alternatives in the literature to minimize the confusion among different ionizing sources and proposed a new simple diagram that uses the equivalent width and the velocity dispersion from one single emission line, H{\alpha}, to classify the ionizing sources. We use aperture limited and spatial resolved spectroscopic data in the nearby Universe (z{\sim}0.01) to demonstrate that the new diagram, that we called WHaD, segregates the different ionizing sources in a more efficient way that previously adopted procedures. A new set of regions are defined in this diagram to select betweeen different ionizing sources. The new proposed diagram is well placed to determine the ionizing source when only H{\alpha} is available, or when the signal-to-noise of the emission lines involved in the classical diagnostic diagrams (e.g., H{\beta})., Comment: 10 pages, 5 figures, accepted for publishing in A&A

Published
2023

3. Supermassive black hole wake or bulgeless edge-on galaxy? II: Order-of-magnitude analysis of the two physical scenarios

Author

Almeida, J. Sanchez

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

-- Context. A recently discovered thin long object aligned with a nearby galaxy could be the stellar wake induced by the passage of a supermassive black hole (SMBH) kicked out from the nearby galaxy by the slingshot effect of a three-body encounter of SMBHs. Alternatively, the object could be a bulgeless edge-on galaxy coincidentally aligned with a second nearby companion. In contrast with the latter, the SMBH interpretation requires a number of unlikely events to happen simultaneously. -- Aims. We aim to assign a probability of occurrence to the two competing scenarios. -- Methods. The probability that the SMBH passage leaves a trace of stars is factorized as the product of the probabilities of all the independent events required for this to happen (PSMBH). Then, each factor is estimated individually. The same exercise is repeated with the edge-on galaxy interpretation (Pgalax). -- Results. Our estimate yields log(Pgalax/PSMBH) simeq 11.4 pm 1.6, where the error is evaluated considering that both Pgalax and PSMBH are products of a large number of random independent variables. Based on the estimated probabilities, PSMBH < 6 x 10**-17 and Pgalax > 1.4 x 10**-5, we determined the number of objects to be expected in various existing, ongoing, and forthcoming surveys, as well as among all observable galaxies (i.e., when observing between 10**6 and 2 x 10**12 galaxies). In the edge-on galaxy scenario, there are always objects to be detected, whereas in the SMBH scenario, the expectation is always compatible with zero. -- Conclusions. Despite the appeal of the runaway SMBH explanation, arguments based on the Occam's razor clearly favor the bulgeless edge-on galaxy interpretation. Our work does not rule out the existence of runaway SMBHs leaving stellar trails. It tells that the vD23 object is more likely to be a bulgeless edge-on galaxy., Comment: Accepted for publication in A&A. Follow up of SA+23, A&A, 673, L9

Published
2023

4. The PAU Survey: Classifying low-z SEDs using Machine Learning clustering

Author

González-Morán, A. L., Haro, P. Arrabal, Muñóz-Tuñón, C., Rodríguez-Espinosa, J. M., Sánchez-Almeida, J., Calhau, J., Gaztañaga, E., Castander, F. J., Renard, P., Cabayol, L., Fernandez, E., Padilla, C., Garcia-Bellido, J., Miquel, R., De Vicente, J., Sanchez, E., Sevilla-Noarbe, I., and Navarro-Gironés, D.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present an application of unsupervised Machine Learning Clustering to the PAU Survey of galaxy spectral energy distribution (SED) within the COSMOS field. The clustering algorithm is implemented and optimized to get the relevant groups in the data SEDs. We find 12 groups from a total number of 5,234 targets in the survey at $0.01 <$ z $< 0.28$. Among the groups, 3,545 galaxies (68\%) show emission lines in the SEDs. These groups also include 1,689 old galaxies with no active star formation. We have fitted the SED to every single galaxy in each group with CIGALE. The mass, age and specific star formation rates (sSFR) of the galaxies range from $0.15 <$ age/Gyr $< 11$; $6 <$ log (M$_{\star}$/M$_{\odot}$) $< 11.26$, and $-14.67 <$ log (sSFR/yr $^{-1}$) $< -8$. The groups are well defined in their properties with galaxies having clear emission lines also having lower mass, are younger and have higher sSFR than those with elliptical like patterns. The characteristic values of galaxies showing clear emission lines are in agreement with the literature for starburst galaxies in COSMOS and GOODS-N fields at low redshift. The star-forming main sequence, sSFR vs. stellar mass and UVJ diagram show clearly that different groups fall into different regions with some overlap among groups. Our main result is that the joint of low-resolution (R $\sim$ 50) photometric spectra provided by the PAU survey together with the unsupervised classification provides an excellent way to classify galaxies. Moreover, it helps to find and extend the analysis of extreme ELGs to lower masses and lower SFRs in the local Universe., Comment: Published in the main journal of the Monthly Notices of the Royal Astronomical Society, July 2023

Published
2023
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5. Spatially-resolved chemodynamics of the starburst dwarf galaxy CGCG 007-025: Evidence for recent accretion of metal-poor gas

Author

del Valle-Espinosa, M. G., Sanchez-Janssen, R., Amorin, R., Fernandez, V., Almeida, J. Sanchez, Lorenzo, B. Garcia, and Papaderos, P.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Nearby metal-poor starburst dwarf galaxies present a unique opportunity to probe the physics of high-density star formation with a detail and sensitivity unmatched by any observation of the high-z Universe. Here we present the first results from a chemodynamical study of the nearby, gas-rich starburst dwarf CGCG 007-025. We use VLT/MUSE integral field spectroscopy to characterise the properties of the star-forming (SF) gas, from its metal content to its kinematics. The star formation rate (SFR) surface density presents a clumpy distribution, with the brightest knot hosting a 5 Myr young, Wolf-Rayet (WR) population (revealed by the presence of the characteristic 5808\AA~WR bump). The ionised gas kinematics are dominated by disordered motions. A superposition of a narrow ($\sigma \approx$ 50 km s$^{-1}$), intermediate (150 km s$^{-1}$) and broad (1000 km s$^{-1}$) kinematic components are needed to model the emission line profiles in the brightest SF region, suggesting the presence of energetic outflows from massive stars. The gas-phase metallicity of the galaxy spans 0.6 dex and displays a strong anti-correlation with SFR surface density, dropping to 12+log(O/H) = 7.7 in the central SF knot. The spatially-resolved BPTs indicates the gas is being ionised purely by SF processes. Finally, the anti-correlation between the SFR and the gas metallicity points out to accretion of metal-poor gas as the origin of the recent off-centre starburst, in which the infalling material ignites the SF episode., Comment: 15 pages, 11 figures, 1 table; published in MNRAS

Published
2022
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6. Electromyography Associated with Biofeedback in Rehabilitation Therapy in Stroke-Stricken Individuals: An Integrative Review

Author

Almeida, L. S., Almeida, J. D., Kozan, R. F., Magjarević, Ratko, Series Editor, Ładyżyński, Piotr, Associate Editor, Ibrahim, Fatimah, Associate Editor, Lackovic, Igor, Associate Editor, Rock, Emilio Sacristan, Associate Editor, Marques, Jefferson Luiz Brum, editor, Rodrigues, Cesar Ramos, editor, Suzuki, Daniela Ota Hisayasu, editor, Marino Neto, José, editor, and García Ojeda, Renato, editor

Published
2024
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7. Biofeedback Analysis in Upper Limb Prostheses: A Literature Review

Author

Almeida, J. D., Almeida, L. S., Kozan, R. F., Magjarević, Ratko, Series Editor, Ładyżyński, Piotr, Associate Editor, Ibrahim, Fatimah, Associate Editor, Lackovic, Igor, Associate Editor, Rock, Emilio Sacristan, Associate Editor, Marques, Jefferson Luiz Brum, editor, Rodrigues, Cesar Ramos, editor, Suzuki, Daniela Ota Hisayasu, editor, Marino Neto, José, editor, and García Ojeda, Renato, editor

Published
2024
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8. Performance of the CMS High Granularity Calorimeter prototype to charged pion beams of 20$-$300 GeV/c

Author

Acar, B., Adamov, G., Adloff, C., Afanasiev, S., Akchurin, N., Akgün, B., Alhusseini, M., Alison, J., de Almeida, J. P. Figueiredo de sa Sousa, de Almeida, P. G. Dias, Alpana, A., Alyari, M., Andreev, I., Aras, U., Aspell, P., Atakisi, I. O., Bach, O., Baden, A., Bakas, G., Bakshi, A., Banerjee, S., DeBarbaro, P., Bargassa, P., Barney, D., Beaudette, F., Beaujean, F., Becheva, E., Becker, A., Behera, P., Belloni, A., Bergauer, T., Berni, M. El, Besancon, M., Bhattacharya, S., Bhowmik, D., Bilki, B., Bilokin, S., Blazey, G. C., Blekman, F., Bloch, P., Bodek, A., Bonanomi, M., Bonis, J., Bonnemaison, A., Bonomally, S., Borg, J., Bouyjou, F., Bower, N., Braga, D., Brennan, L., Brianne, E., Brondolin, E., Bryant, P., Buhmann, E., Buhmann, P., Butler-Nalin, A., Bychkova, O., Callier, S., Calvet, D., Canderan, K., Cankocak, K., Cao, X., Cappati, A., Caraway, B., Caregari, S., Carty, C., Cauchois, A., Ceard, L., Cerci, D. S., Cerci, S., Cerminara, G., Chadeeva, M., Charitonidis, N., Chatterjee, R., Chen, J. A., Chen, Y. M., Cheng, H. J., Cheng, K. Y., Cheung, H., Chokheli, D., Cipriani, M., Čoko, D., Couderc, F., Cuba, E., Danilov, M., Dannheim, D., Daoud, W., Das, I., Dauncey, P., Davies, G., Davignon, O., Day, E., Debbins, P., Defranchis, M. M., Delagnes, E., Demiragli, Z., Demirbas, U., Derylo, G., Diaz, D., Diehl, L., Dinaucourt, P., Dincer, G. G., Dittmann, J., Dragicevic, M., Dugad, S., Dulucq, F., Dumanoglu, I., Dünser, M., Dutta, S., Dutta, V., Edberg, T. K., Elias, F., Emberger, L., Eno, S. C., Ershov, Yu., Extier, S., Fahim, F., Fallon, C., Fard, K. Sarbandi, Fedi, G., Ferragina, L., Forthomme, L., Frahm, E., Franzoni, G., Freeman, J., French, T., Gadow, K., Gandhi, P., Ganjour, S., Gao, X., Garcia, M. T. Ramos, Garcia-Bellido, A., Garutti, E., Gastaldi, F., Gastler, D., Gecse, Z., Germer, A., Gerwig, H., Gevin, O., Ghosh, S., Gilbert, A., Gilbert, W., Gill, K., Gingu, C., Gninenko, S., Golunov, A., Golutvin, I., Gonultas, B., Gorbounov, N., Göttlicher, P., Gouskos, L., Graf, C., Gray, A. B., Grieco, C., Gr\"önroos, S., Gu, Y., Guilloux, F., Guler, E. Gurpinar, Guler, Y., Gülmez, E., Guo, J., Gutti, H., Hakimi, A., Hammer, M., Hartbrich, O., Hassanshahi, H. M., Hatakeyama, K., Hazen, E., Heering, A., Hegde, V., Heintz, U., Heuchel, D., Hinton, N., Hirschauer, J., Hoff, J., Hou, W. S., Hou, X., Hua, H., Huck, S., Hussain, A., Incandela, J., Irles, A., Irshad, A., Isik, C., Jain, S., Jaroslavceva, J., Jheng, H. R., Joshi, U., Kaadze, K., Kachanov, V., Kalipoliti, L., Kaminskiy, A., Kanuganti, A. R., Kao, Y. W., Kapoor, A., Kara, O., Karneyeu, A., Kałuzińska, O., Kaya, M., Kaya, O., Kazhykharim, Y., Khan, F. A., Khukhunaishvili, A., Kieseler, J., Kilpatrick, M., Kim, S., Koetz, K., Kolberg, T., Komm, M., Köseyan, O. K., Kraus, V., Krawczyk, M., Kristiansen, K., Kristić, A., Krohn, M., Kronheim, B., Krüger, K., Kulis, S., Kumar, M., Kunori, S., Kuo, C. M., Kuryatkov, V., Kvasnicka, J., Kyre, S., Lai, Y., Lamichhane, K., Landsberg, G., Lange, C., Langford, J., Laurien, S., Lee, M. Y., Lee, S. W., Leiton, A. G. Stahl, Levin, A., Li, A., Li, J. H., Li, Y. Y., Liang, Z., Liao, H., Lin, Z., Lincoln, D., Linssen, L., Lipton, R., Liu, G., Liu, Y., Lobanov, A., Lohezic, V., Lomidze, D., Lu, R. S., Lu, S., Lupi, M., Lysova, I., Magnan, A. -M., Magniette, F., Mahjoub, A., Martens, S., Matysek, M., Meier, B., Malakhov, A., Mallios, S., Mandjavize, I., Mannelli, M., Mans, J., Marchioro, A., Martelli, A., Martinez, G., Masterson, P., Matthewman, M., Mayekar, S. N., David, A., Coco, S., Meng, B., Menkel, A ., Mestvirishvili, A., Milella, G., Mirza, I., Moccia, S., Mohanty, G. B., Monti, F., Moortgat, F. W., Morrissey, I., Motta, J., Murthy, S., Musić, J., Musienko, Y., Nabili, S., Nguyen, M., Nikitenko, A., Noonan, D., Noy, M., Nurdan, K., Nursanto, M. Wulansatiti, Ochando, C., Odell, N., Okawa, H., Onel, Y., Ortez, W., Ozegović, J., Ozkorucuklu, S., Paganis, E., Palmer, C. A., Pandey, S., Pantaleo, F., Papageorgakis, C., Papakrivopoulos, I., Paranjpe, M., Parshook, J., Pastika, N., Paulini, M., Peitzmann, T., Peltola, T., Peng, N., Perraguin, A. Buchot, Petiot, P., Pierre-Emile, T., Pinto, M. Vicente Barreto, Popova, E., Pöschl, R., Prosper, H., Prvan, M., Puljak, I., Qasim, S. R., Qu, H., Quast, T., Quinn, R., Quinnan, M., Rane, A., Rao, K. K., Rapacz, K., Raux, L., Redjeb, W., Reinecke, M., Revering, M., Richard, F., Roberts, A., Sanchez, A. M., Rohlf, J., Rolph, J., Romanteau, T., Rosado, M., Rose, A., Rovere, M., Roy, A., Rubinov, P., Rusack, R., Rusinov, V., Ryjov, V., Sahin, O. M., Salerno, R., Saradhy, R., Sarkar, T., Sarkisla, M. A., Sauvan, J. B., Schmidt, I., Schmitt, M., Schuwalow, S., Scott, E., Seez, C., Sefkow, F., Selivanova, D., Sharma, S., Shelake, M., Shenai, A., Shukla, R., Sicking, E., De, M., Silva, P., Simkina, P., Simon, F., Simsek, A. E., Sirois, Y., Smirnov, V., Sobering, T. J., Spencer, E., Srimanobhas, N., Steen, A., Strait, J., Strobbe, N., Su, X. F., Sudo, Y., Suarez, C. Mantilla, Sukhov, E., Sulak, L., Sun, L., Suryadevara, P., Syal, C., de La Taille, C., Tali, B., Tan, C. L., Tao, J., Tarabini, A., Tatli, T., Thaus, R., Taylor, R. D., Tekten, S., Thiebault, A., Thienpont, D., Tiley, C., Tiras, E., Titov, M., Tlisov, D., Tok, U. G., Kayis, A., Troska, J., Tsai, L. S., Tsamalaidze, Z., Tsipolitis, G., Tsirou, A., Undleeb, S., Urbanski, D., Uslan, E., Ustinov, V., Uzunian, A., Varela, J., Velasco, M., Vernazza, E., Viazlo, O., Vichoudis, P., Virdee, T., Voirin, E., Vojinovi\c, M., Vojinovic, M., Wade, A., Wang, C., Wang, C. C., Wang, D., Wang, F., Wang, X., Wang, Z., Wayne, M., Webb, S. N., Whitbeck, A., Wickwire, R., Wilson, J. S., Wu, H. Y., Wu, L., Xiao, M., Yang, J., Yeh, C. H, Yohay, R., Yu, D., Yu, S. S., Yuan, C., Miao, Y., Yumiceva, F., Yusuff, I., Zabi, A., Zacharopoulou, A., Zamiatin, N., Zarubin, A., Zehetner, P., Zerwas, D., Zhang, H., Zhang, J., Zhang, Y., Zhang, Z., and Zhao, X.

Subjects
Physics - Instrumentation and Detectors
Abstract

The upgrade of the CMS experiment for the high luminosity operation of the LHC comprises the replacement of the current endcap calorimeter by a high granularity sampling calorimeter (HGCAL). The electromagnetic section of the HGCAL is based on silicon sensors interspersed between lead and copper (or copper tungsten) absorbers. The hadronic section uses layers of stainless steel as an absorbing medium and silicon sensors as an active medium in the regions of high radiation exposure, and scintillator tiles directly readout by silicon photomultipliers in the remaining regions. As part of the development of the detector and its readout electronic components, a section of a silicon-based HGCAL prototype detector along with a section of the CALICE AHCAL prototype was exposed to muons, electrons and charged pions in beam test experiments at the H2 beamline at the CERN SPS in October 2018. The AHCAL uses the same technology as foreseen for the HGCAL but with much finer longitudinal segmentation. The performance of the calorimeters in terms of energy response and resolution, longitudinal and transverse shower profiles is studied using negatively charged pions, and is compared to GEANT4 predictions. This is the first report summarizing results of hadronic showers measured by the HGCAL prototype using beam test data., Comment: Accepted for publication by JINST

Published
2022

9. Dwarf galaxies with central cores in modified Newtonian dynamics (MOND) gravity

Author

Almeida, J. Sanchez

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Some dwarf galaxies are within the Mondian regime at all radii, i.e., the gravitational acceleration provided by the observed baryons is always below the threshold of $g_\dag\simeq 1.2\times 10^{-10}\,{\rm m\,s^{-2}}$. These dwarf galaxies often show cores, in the sense that assuming Newton's gravity to explain their rotation curves, the total density profile $\rho(r)$ presents a central plateau or {\em core} ($d\log \rho/d\log r\rightarrow 0$ when $r\rightarrow 0$). Here we show that under MOND gravity, the existence of this core implies a baryon content whose density $g_{\rm bar}$ must decrease toward the center of the gravitational potential ($g_{\rm bar}\rightarrow 0$ when $r\rightarrow 0$). Such drop of baryons toward the central region is neither observed nor appears in numerical simulations of galaxy formation following MOND gravity. We analyze the problem posed for MOND as well as possible workarounds., Comment: Accepted for publication in ApJ

Published
2022
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10. Cor de solo, formas do fósforo e adsorção de fosfatos em Latossolos desenvolvidos de basalto do extremo-sul do Brasil

Author

Almeida J. A., Torrent J., and Barrón V.

Subjects
Latossolos, refletância difusa, adsorção de P, óxidos de ferro, fracionamento do fósforo, hematita, goethita, Agriculture (General), S1-972
Abstract

Latossolos Brunos e Vermelhos férricos desenvolvidos de basalto representam parcela expressiva dos solos intensivamente cultivados do Sul do Brasil. Além dos perfis monomatizados típicos, brunos ou vermelhos, incluem-se, atualmente, nestas duas classes perfis polimatizados, que apresentam os horizontes superficiais brunados e os subsuperficiais mais avermelhados, anteriormente individualizados como Latossolo "Bruno/Roxo". Não há, ainda, no Sistema Brasileiro de Classificação de Solos, um consenso quanto aos componentes de cor mais apropriados para separação dos Latossolos Brunos e Vermelhos. Graças à sua textura muito argilosa e ao alto conteúdo de óxidos de ferro, tais solos apresentam elevada capacidade de adsorção de fosfatos, à qual se pressupõe seja diferenciada de acordo com as formas dos óxidos de ferro presentes em cada modalidade. Por outro lado, a matéria orgânica, ao interagir com os óxidos de ferro, pode igualmente mascarar o efeito individual desses óxidos na fixação. Desse modo, o presente trabalho objetivou: (a) testar a utilidade e a eficácia do uso de dados espectrais obtidos por refletância difusa como ferramenta para identificação dos óxidos de ferro goethita (FeOOH) e hematita (Fe2O3); (b) quantificar, por fracionamento químico, as diferentes formas ou compartimentos onde se encontra o fósforo nesses solos, e (c) avaliar o efeito dos diferentes tipos e proporções de hematita e goethita na adsorção de fósforo, bem como o efeito da matéria orgânica na redução dessa capacidade sortiva. Foram selecionados seis perfis de solo em Santa Catarina e Rio Grande do Sul, sendo dois Latossolos Brunos típicos, dois Latossolos Vermelhos férricos e dois Latossolos Brunos, provisoriamente denominados Latossolo Bruno/Vermelho férrico. Os perfis foram caracterizados do ponto de vista físico, químico e mineralógico, sendo as amostras de quatro horizontes de cada perfil selecionadas para análises mais detalhadas. As técnicas de refletância difusa utilizadas mostraram-se altamente promissoras para a identificação e quantificação dos óxidos de ferro presentes. O matiz 4 YR, em amostras naturais úmidas, correspondeu a valores aproximadamente iguais de hematita e de goethita nos solos, sendo esse valor proposto como limite de separação entre Latossolos Brunos e Vermelhos e entre Nitossolos Vermelhos e Háplicos. Para a maioria dos solos, as quantidades totais de fósforo foram superiores a 1.000 mg kg-1, indicando alta reserva potencial desse nutriente. No fracionamento químico seqüencial, evidenciou-se o predomínio das formas "oclusas" de fósforo (Pdcb), seguida das formas orgânicas, P adsorvido a formas cristalinas dos óxidos de ferro e P ligado a compostos de ferro de baixa cristalinidade. O coeficiente A da equação de Freundlich modificada, que estima a quantidade de P necessária para manter 1 mg L-1 P na solução após um dia de equilíbrio, foi menor nos Latossolos Vermelhos em relação aos Brunos. Em todos os solos, entretanto, o valor de A mostrou-se inversamente correlacionado com o conteúdo de matéria orgânica, indicando que, além do efeito individual dos óxidos de ferro na fixação, o aumento no conteúdo de matéria orgânica exerce papel extremamente importante na redução da sorção de fosfatos desses solos.

Published
2003

11. Avaliação de três áreas de solo construído após mineração de carvão a céu aberto em Lauro Müller, Santa Catarina

Author

Campos M. L., Almeida J. A., and Souza L. S.

Subjects
oxidação da pirita, variabilidade espacial, solos construídos, Agriculture (General), S1-972
Abstract

Em solos construídos após mineração de carvão, a contaminação das camadas superficiais com pirita provoca intensa acidificação do solo, acelera a intemperização de minerais, eleva os teores de Al e Mn e aumenta a lixiviação de bases. O presente trabalho avaliou características químicas, teor de argila e mineralogia, bem como a variabilidade espacial para algumas dessas características em três áreas de solos construídos após mineração de carvão a céu aberto no município de Lauro Müller, Santa Catarina. As três áreas selecionadas apresentavam diferenças no modo de construção topográfico. A primeira, denominada Mina Juliana (MJ), foi construída em 1996, utilizando material (sólum, regolito argiloso e rocha) que foi separado e estocado antes da mineração, conforme previsto no plano de reabilitação. A segunda, denominada Mina do Apertado (MA), foi construída, em 1996, usando, como material de cobertura, o sólum proveniente do decapeamento de um morro adjacente à área. A terceira área, denominada Mina Rio do Meio (MRM), sofreu apenas construção topográfica em 1983, com mistura de resíduos de pirita de carvão e rochas de várias camadas. Amostras de solo foram coletadas em sistema de grade de pontos, em três profundidades, sendo analisados o pH em água, teores de Ca, Mg, K e Al trocáveis, H + Al e condutividade elétrica. Em amostras selecionadas, analisaram-se alguns metais pesados e a mineralogia da fração argila. Análises efetuadas em dois perfis de solo representativos das condições anteriores à mineração foram utilizados, para comparação. Todas as áreas apresentaram grande dispersão de valores para características químicas e teor de argila dos solos entre os pontos amostrados. O processo de construção do solo que resultou em maior uniformidade destas características e melhores condições para o estabelecimento de espécies vegetais foi o da área MJ. O solo da área MA, graças à mistura de resíduos de carvão piritoso com o solo superficial, está em franco processo de acidificação e contém alta concentração de sais. O solo da área MRM, em virtude do abandono e do longo período de exposição de resíduos piritosos na camada superficial, mostra elevada acidez, tendo já sofrido intensa lixiviação dos sais. As únicas variáveis testadas que apresentaram modelo definido para semivariância foram Al trocável, H + Al e argila, cujo alcance variou de 50 a 70 m.

Published
2003

13. Discovery of faint double-peak Halpha emission in the halo of low redshift galaxies

Author

Almeida, J. Sanchez, Calhau, J., Munoz-Tunon, C., Gonzalez-Moran, A. L., and Rodriguez-Espinosa, J. M.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Aiming at the detection of cosmological gas being accreted onto galaxies of the local Universe, we examined the Halpha emission in the halo of 164 galaxies in the field of view of the Multi-Unit Spectroscopic Explorer Wide survey (\musew ) with observable Halpha (redshift < 0.42). An exhaustive screening of the corresponding Halpha images led us to select 118 reliable Halpha emitting gas clouds. The signals are faint, with a surface brightness of 10**(-17.3 pm 0.3) erg/s/cm2/arcsec2. Through statistical tests and other arguments, we ruled out that they are created by instrumental artifacts, telluric line residuals, or high redshift interlopers. Around 38% of the time, the Halpha line profile shows a double peak with the drop in intensity at the rest-frame of the central galaxy, and with a typical peak-to-peak separation of the order of pm 200 km/s. Most line emission clumps are spatially unresolved. The mass of emitting gas is estimated to be between one and 10**(-3) times the stellar mass of the central galaxy. The signals are not isotropically distributed; their azimuth tends to be aligned with the major axis of the corresponding galaxy. The distances to the central galaxies are not random either. The counts drop at a distance > 50 galaxy radii, which roughly corresponds to the virial radius of the central galaxy. We explore several physical scenarios to explain this Halpha emission, among which accretion disks around rogue intermediate mass black holes fit the observations best., Comment: pay attention to the last sentence of the abstract! Accepted for publication in ApJ

Published
2022
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14. The principle of maximum entropy and the distribution of mass in galaxies

Author

Almeida, J. Sanchez

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We do not have a final answer to the question of why galaxies choose a particular internal mass distribution. Here we examine whether the distribution is set by thermodynamic equilibrium (TE). Traditionally, TE is discarded for a number of reasons including the inefficiency of two-body collisions to thermalize the mass distribution in a Hubble time, and the fact that the mass distribution maximizing the classical Boltzmann-Gibbs entropy is unphysical. These arguments are questionable. In particular, when the Tsallis entropy that describes self-gravitating systems is used to define TE, the mass distributions that result (i.e., the polytropes) are physically sensible. This work spells out this and other arguments for TE, and presents the polytropes and their properties. It puts forward empirical evidence for the mass distribution observed in galaxies to be consistent with polytropes. It compares polytropes with Sersic functions and it shows how the DM halos resulting from cosmological numerical simulations become polytropes when efficient collisions are allowed. It also discusses pathways to thermalization bypassing two-body collisions. It finally outlines future developments including deciphering whether or not DM particles collide efficiently., Comment: Review to appear in a special issue of Universe on "Kinetic Processes in Relativistic Domain" edited by G. Vereshchagin

Published
2022

15. Quality Inspection Aspects of Hybrid Prototypes for the CMS Outer Tracker Upgrade at HL-LHC

Author

La Rosa, A., Ahmed, I., Almeida, J., Blanchot, G., Cooperstein, S., Dominguez, I., Honma, A., Kovacs, M., and Zografos, A.

Subjects
Physics - Instrumentation and Detectors
Abstract

At the High Luminosity LHC (HL-LHC), the CMS experiment will need to operate at up to 200 interactions per 25 ns beam crossing time and with up to 4000 fb-1 of integrated luminosity. To achieve the physics goals the experiment needs to improve the tracking resolution and the ability to selectively trigger on specific physics events. The CMS tracker upgrade requires designing a new detector to cope with the HL-LHC conditions. The new Outer Tracker is based on two types of silicon modules (strip-strip and pixel-strip). Each module type has a few types of high-density interconnect hybrid circuits which house the front-end and auxiliary electronics. This paper introduces the technological choices for modules and hybrids and presents the quality inspection aspects of the first hybrid prototypes., Comment: 4 pages, 4 figures, accepted for publication in the proceedings of TIPP 2021 to be published in Journal of Physics: Conference Series

Published
2021
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17. Super-resolving collective quantum measurements

Author

de Almeida, J. O., Lewenstein, M., and Skotiniotis, M.

Subjects
Quantum Physics
Abstract

We show how to super-resolve signals encoded in bosonic modes using collective quantum measurements exploiting permutation symmetry. Our collective measurement strategy does not rely on estimating or knowing additional nuisance parameters of the signals, such as the mean or median value of the signals distribution, a necessary condition in almost all spatial, temporal or spectral super-resolution schemes employed to date. More importantly, we show that careful fine-graining of our collective measurement strategy allows for estimation of additional signal parameters, such as the relative intensity of the bosonic sources, at the quantum limit., Comment: 12 pages, 4 figures

Published
2021

18. Physically motivated fit to mass surface density profiles observed in galaxies

Author

Almeida, J. Sanchez, Trujillo, I., and Plastino, A. R.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Polytropes have gained renewed interest because they account for several seemingly-disconnected observational properties of galaxies. Here we study if polytropes are also able to explain the stellar mass distribution within galaxies. We develop a code to fit surface density profiles using polytropes projected in the plane of the sky (propols). Sersic profiles are known to be good proxies for the global shapes of galaxies and we find that, ignoring central cores, propols and Sersic profiles are indistinguishable within observational errors (within 5 % over 5 orders of magnitude in surface density). The range of physically meaningful polytropes yields Sersic indexes between 0.4 and 6. The code has been systematically applied to ~750 galaxies with carefully measured mass density profiles and including all morphological types and stellar masses (7 < log (Mstar/Msun) < 12). The propol fits are systematically better than Sersic profiles when log(Mstar/Msun) < 9 and systematically worst when log(Mstar/Msun) > 10. Although with large scatter, the observed polytropic indexes increase with increasing mass and tend to cluster around m=5. For the most massive galaxies, propols are very good at reproducing their central parts, but they do not handle well cores and outskirts altogether. Polytropes are self-gravitating systems in thermal meta-equilibrium as defined by the Tsallis entropy. Thus, the above results are compatible with the principle of maximum Tsallis entropy dictating the internal structure in dwarf galaxies and in the central region of massive galaxies., Comment: Accepted for publication in ApJ. The fitting code is publicly available at https://github.com/jorgesanchezalmeida/polytropic-fits

Published
2021
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22. History of the gas fuelling star formation in eagle galaxies

Author

Scholz-Diaz, L., Almeida, J. Sanchez, and Vecchia, C. Dalla

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Theory predicts that cosmological gas accretion plays a fundamental role fuelling star formation in galaxies. However, a detailed description of the accretion process to be used when interpreting observations is still lacking. Using the state-of-the-art cosmological hydrodynamical simulation eagle, we work out the chemical inhomogeneities arising in the disk of galaxies due to the randomness of the accretion process. In low-mass systems and outskirts of massive galaxies, low metallicity regions are associated with enhanced star-formation, a trend that reverses in the centers of massive galaxies. These predictions agree with the relation between surface density of star formation rate and metallicity observed in the local spiral galaxies from the MaNGA survey. Then, we analyse the origin of the gas that produces stars at two key epochs, z simeq 0 and z simeq 2. The main contribution comes from gas already in the galaxy about 1 Gyr before stars are formed, with a share from external gas that is larger at high redshift. The accreted gas may come from major and minor mergers, but also as gravitationally unbound gas and from mergers with dark galaxies (i.e., haloes where more than 95 % of the baryon mass is in gas). We give the relative contribution of these sources of gas as a function of stellar mass (8 < log Mstar < 11). Even at z = 0, some low-mass galaxies form a significant fraction of their total stellar mass during the last Gyr from mergers with dark galaxies., Comment: Accepted for publication in MNRAS. 12 figures, 14 pages. Fig. 8 compares simulations with observations

Published
2021
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23. Extreme Emission-Line Galaxies in SDSS. I. Empirical and model-based calibrations of chemical abundances

Author

Pérez-Montero, E., Amorín, R., Almeida, J. Sánchez, Vílchez, J. M., García-Benito, R., and Kehrig, C.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Local star-forming galaxies show properties that are thought to differ from galaxies in the early Universe. Among them, the ionizing stellar populations and the gas geometry make the recipes designed to derive chemical abundances from nebular emission lines to differ from those calibrated in the Local Universe. A sample of 1969 Extreme Emission Line Galaxies (EELGs) at a redshift 0 < z < 0.49, selected from the Sloan Digital Sky Survey (SDSS) to be local analogues of high-redshift galaxies, was used to analyze their most prominent emission lines and to derive total oxygen abundances and nitrogen-to-oxygen ratios following the direct method in the ranges 7.7 < 12+log(O/H) < 8.6 and -1.8 < log(N/O) < -0.8. They allow us to obtain new empirically calibrated strong-line methods and to evaluate other recipes based on photoionization models that can be later used for a chemical analysis of actively star-forming galaxies in very early stages of galaxy evolution. Our new relations are in agreement with others found for smaller samples of objects at higher redshifts. When compared with other relations calibrated in the local Universe, they differ when the employed strong-line ratio depends on the hardness of the ionizing radiation, such as O32 or Ne3O2, but they do not when the main dependence is on the ionization parameter, such as S23. In the case of strong-line ratios depending on [NII] lines, the derivation of O/H becomes very uncertain due to the very high N/O values derived in this sample, above all in the low-metallicity regime. Finally, we adapt the bayesian-like code HII-Chi-mistry for the conditions found in this kind of galaxies and we prove that it can be used to derive within errors both O/H and N/O, in consistency with the direct method ., Comment: 16 pages, 13 figures. Accepted for publication by MNRAS

Published
2021
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25. The Mass-Metallicity Relation at z ~ 1-2 and Its Dependence on the Star Formation Rate

Author

Henry, A, Rafelski, M, Sunnquist, B, Pirzkal, N, Pacifici, C, Atek, H, Bagley, M, Baronchelli, I, Barro, G, Bunker, AJ, Colbert, J, Dai, YS, Elmegreen, BG, Elmegreen, DM, Finkelstein, S, Kocevski, D, Koekemoer, A, Malkan, M, Martin, CL, Mehta, V, Pahl, A, Papovich, C, Rutkowski, M, Sánchez Almeida, J, Scarlata, C, Snyder, G, and Teplitz, H

Subjects
Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We present a new measurement of the gas-phase mass-metallicity relation (MZR) and its dependence on star formation rates (SFRs) at 1.3 < z < 2.3. Our sample comprises 1056 galaxies with a mean redshift of z = 1.9, identified from the Hubble Space Telescope Wide Field Camera 3 (WFC3) grism spectroscopy in the Cosmic Assembly Near-infrared Deep Extragalactic Survey and the WFC3 Infrared Spectroscopic Parallel Survey. This sample is four times larger than previous metallicity surveys at z ~ 2 and reaches an order of magnitude lower in stellar mass (108 M o?). Using stacked spectra, we find that the MZR evolves by 0.3 dex relative to z ~ 0.1. Additionally, we identify a subset of 49 galaxies with high signal-to-noise (S/N) spectra and redshifts between 1.3 < z < 1.5, where Ha emission is observed along with [O iii] and [O ii]. With accurate measurements of SFR in these objects, we confirm the existence of a mass-metallicity-SFR (M-Z-SFR) relation at high redshifts. These galaxies show systematic differences from the local M-Z-SFR relation, which vary depending on the adopted measurement of the local relation. However, it remains difficult to ascertain whether these differences could be due to redshift evolution, as the local M-Z-SFR relation is poorly constrained at the masses and SFRs of our sample. Lastly, we reproduced our sample selection in the IllustrisTNG hydrodynamical simulation, demonstrating that our line flux limit lowers the normalization of the simulated MZR by 0.2 dex. We show that the M-Z-SFR relation in IllustrisTNG has an SFR dependence that is too steep by a factor of around 3.

Published
2021

26. Impact of primary kidney disease on the effects of empagliflozin in patients with chronic kidney disease: secondary analyses of the EMPA-KIDNEY trial

Author

Judge, PK, Staplin, N, Mayne, KJ, Wanner, C, Green, JB, Hauske, SJ, Emberson, JR, Preiss, D, Ng, SYA, Roddick, AJ, Sammons, E, Zhu, D, Hill, M, Stevens, W, Wallendszus, K, Brenner, S, Cheung, AK, Liu, ZH, Li, J, Hooi, LS, Liu, WJ, Kadowaki, T, Nangaku, M, Levin, A, Cherney, D, Maggioni, AP, Pontremoli, R, Deo, R, Goto, S, Rossello, X, Tuttle, KR, Steubl, D, Massey, D, Landray, MJ, Baigent, C, Haynes, R, Herrington, WG, Abat, S, Abd Rahman, R, Abdul Cader, R, Abdul Hafidz, MI, Abdul Wahab, MZ, Abdullah, NK, Abdul-Samad, T, Abe, M, Abraham, N, Acheampong, S, Achiri, P, Acosta, JA, Adeleke, A, Adell, V, Adewuyi-Dalton, R, Adnan, N, Africano, A, Agharazii, M, Aguilar, F, Aguilera, A, Ahmad, M, Ahmad, MK, Ahmad, NA, Ahmad, NH, Ahmad, NI, Ahmad Miswan, N, Ahmad Rosdi, H, Ahmed, I, Ahmed, S, Aiello, J, Aitken, A, AitSadi, R, Aker, S, Akimoto, S, Akinfolarin, A, Akram, S, Alberici, F, Albert, C, Aldrich, L, Alegata, M, Alexander, L, Alfaress, S, Alhadj Ali, M, Ali, A, Alicic, R, Aliu, A, Almaraz, R, Almasarwah, R, Almeida, J, Aloisi, A, Al-Rabadi, L, Alscher, D, Alvarez, P, Al-Zeer, B, Amat, M, Ambrose, C, Ammar, H, An, Y, Andriaccio, L, Ansu, K, Apostolidi, A, Arai, N, Araki, H, Araki, S, Arbi, A, Arechiga, O, Armstrong, S, Arnold, T, Aronoff, S, Arriaga, W, Arroyo, J, Arteaga, D, Asahara, S, Asai, A, Asai, N, Asano, S, Asawa, M, Asmee, MF, Aucella, F, Augustin, M, Avery, A, Awad, A, Awang, IY, Awazawa, M, Axler, A, Ayub, W, Azhari, Z, Baccaro, R, Badin, C, Bagwell, B, Bahlmann-Kroll, E, Bahtar, AZ, Bains, D, Bajaj, H, Baker, R, Baldini, E, Banas, B, Banerjee, D, Banno, S, Bansal, S, Barberi, S, Barnes, S, Barnini, C, Barot, C, Barrett, K, Barrios, R, Bartolomei Mecatti, B, Barton, I, Barton, J, Basily, W, Bavanandan, S, Baxter, A, Becker, L, Beddhu, S, Beige, J, Beigh, S, Bell, S, Benck, U, Beneat, A, Bennett, A, Bennett, D, Benyon, S, Berdeprado, J, Bergler, T, Bergner, A, Berry, M, Bevilacqua, M, Bhairoo, J, Bhandari, S, Bhandary, N, Bhatt, A, Bhattarai, M, Bhavsar, M, Bian, W, Bianchini, F, Bianco, S, Bilous, R, Bilton, J, Bilucaglia, D, Bird, C, Birudaraju, D, Biscoveanu, M, Blake, C, Bleakley, N, Bocchicchia, K, Bodine, S, Bodington, R, Boedecker, S, Bolduc, M, Bolton, S, Bond, C, Boreky, F, Boren, K, Bouchi, R, Bough, L, Bovan, D, Bowler, C, Bowman, L, Brar, N, Braun, C, Breach, A, Breitenfeldt, M, Brettschneider, B, Brewer, A, Brewer, G, Brindle, V, Brioni, E, Brown, C, Brown, H, Brown, L, Brown, R, Brown, S, Browne, D, Bruce, K, Brueckmann, M, Brunskill, N, Bryant, M, Brzoska, M, Bu, Y, Buckman, C, Budoff, M, Bullen, M, Burke, A, Burnette, S, Burston, C, Busch, M, Bushnell, J, Butler, S, Büttner, C, Byrne, C, Caamano, A, Cadorna, J, Cafiero, C, Cagle, M, Cai, J, Calabrese, K, Calvi, C, Camilleri, B, Camp, S, Campbell, D, Campbell, R, Cao, H, Capelli, I, Caple, M, Caplin, B, Cardone, A, Carle, J, Carnall, V, Caroppo, M, Carr, S, Carraro, G, Carson, M, Casares, P, Castillo, C, Castro, C, Caudill, B, Cejka, V, Ceseri, M, Cham, L, Chamberlain, A, Chambers, J, Chan, CBT, Chan, JYM, Chan, YC, Chang, E, Chant, T, Chavagnon, T, Chellamuthu, P, Chen, F, Chen, J, Chen, P, Chen, TM, Chen, Y, Cheng, C, Cheng, H, Cheng, MC, Ching, CH, Chitalia, N, Choksi, R, Chukwu, C, Chung, K, Cianciolo, G, Cipressa, L, Clark, S, Clarke, H, Clarke, R, Clarke, S, Cleveland, B, Cole, E, Coles, H, Condurache, L, Connor, A, Convery, K, Cooper, A, Cooper, N, Cooper, Z, Cooperman, L, Cosgrove, L, Coutts, P, Cowley, A, Craik, R, Cui, G, Cummins, T, Dahl, N, Dai, H, Dajani, L, D'Amelio, A, Damian, E, Damianik, K, Danel, L, Daniels, C, Daniels, T, Darbeau, S, Darius, H, Dasgupta, T, Davies, J, Davies, L, Davis, A, Davis, J, Davis, L, Dayanandan, R, Dayi, S, Dayrell, R, De Nicola, L, Debnath, S, Deeb, W, Degenhardt, S, DeGoursey, K, Delaney, M, DeRaad, R, Derebail, V, Dev, D, Devaux, M, Dhall, P, Dhillon, G, Dienes, J, Dobre, M, Doctolero, E, Dodds, V, Domingo, D, Donaldson, D, Donaldson, P, Donhauser, C, Donley, V, Dorestin, S, Dorey, S, Doulton, T, Draganova, D, Draxlbauer, K, Driver, F, Du, H, Dube, F, Duck, T, Dugal, T, Dugas, J, Dukka, H, Dumann, H, Durham, W, Dursch, M, Dykas, R, Easow, R, Eckrich, E, Eden, G, Edmerson, E, Edwards, H, Ee, LW, Eguchi, J, Ehrl, Y, Eichstadt, K, Eid, W, Eilerman, B, Ejima, Y, Eldon, H, Ellam, T, Elliott, L, Ellison, R, Emberson, J, Epp, R, Er, A, Espino-Obrero, M, Estcourt, S, Estienne, L, Evans, G, Evans, J, Evans, S, Fabbri, G, Fajardo-Moser, M, Falcone, C, Fani, F, Faria-Shayler, P, Farnia, F, Farrugia, D, Fechter, M, Fellowes, D, Feng, F, Fernandez, J, Ferraro, P, Field, A, Fikry, S, Finch, J, Finn, H, Fioretto, P, Fish, R, Fleischer, A, Fleming-Brown, D, Fletcher, L, Flora, R, Foellinger, C, Foligno, N, Forest, S, Forghani, Z, Forsyth, K, Fottrell-Gould, D, Fox, P, Frankel, A, Fraser, D, Frazier, R, Frederick, K, Freking, N, French, H, Froment, A, Fuchs, B, Fuessl, L, Fujii, H, Fujimoto, A, Fujita, A, Fujita, K, Fujita, Y, Fukagawa, M, Fukao, Y, Fukasawa, A, Fuller, T, Funayama, T, Fung, E, Furukawa, M, Furukawa, Y, Furusho, M, Gabel, S, Gaidu, J, Gaiser, S, Gallo, K, Galloway, C, Gambaro, G, Gan, CC, Gangemi, C, Gao, M, Garcia, K, Garcia, M, Garofalo, C, Garrity, M, Garza, A, Gasko, S, Gavrila, M, Gebeyehu, B, Geddes, A, Gentile, G, George, A, George, J, Gesualdo, L, Ghalli, F, Ghanem, A, Ghate, T, Ghavampour, S, Ghazi, A, Gherman, A, Giebeln-Hudnell, U, Gill, B, Gillham, S, Girakossyan, I, Girndt, M, Giuffrida, A, Glenwright, M, Glider, T, Gloria, R, Glowski, D, Goh, BL, Goh, CB, Gohda, T, Goldenberg, R, Goldfaden, R, Goldsmith, C, Golson, B, Gonce, V, Gong, Q, Goodenough, B, Goodwin, N, Goonasekera, M, Gordon, A, Gordon, J, Gore, A, Goto, H, Gowen, D, Grace, A, Graham, J, Grandaliano, G, Gray, M, Greene, T, Greenwood, G, Grewal, B, Grifa, R, Griffin, D, Griffin, S, Grimmer, P, Grobovaite, E, Grotjahn, S, Guerini, A, Guest, C, Gunda, S, Guo, B, Guo, Q, Haack, S, Haase, M, Haaser, K, Habuki, K, Hadley, A, Hagan, S, Hagge, S, Haller, H, Ham, S, Hamal, S, Hamamoto, Y, Hamano, N, Hamm, M, Hanburry, A, Haneda, M, Hanf, C, Hanif, W, Hansen, J, Hanson, L, Hantel, S, Haraguchi, T, Harding, E, Harding, T, Hardy, C, Hartner, C, Harun, Z, Harvill, L, Hasan, A, Hase, H, Hasegawa, F, Hasegawa, T, Hashimoto, A, Hashimoto, C, Hashimoto, M, Hashimoto, S, Haskett, S, Hawfield, A, Hayami, T, Hayashi, M, Hayashi, S, Hazara, A, Healy, C, Hecktman, J, Heine, G, Henderson, H, Henschel, R, Hepditch, A, Herfurth, K, Hernandez, G, Hernandez Pena, A, Hernandez-Cassis, C, Herzog, C, Hewins, S, Hewitt, D, Hichkad, L, Higashi, S, Higuchi, C, Hill, C, Hill, L, Himeno, T, Hing, A, Hirakawa, Y, Hirata, K, Hirota, Y, Hisatake, T, Hitchcock, S, Hodakowski, A, Hodge, W, Hogan, R, Hohenstatt, U, Hohenstein, B, Hooi, L, Hope, S, Hopley, M, Horikawa, S, Hosein, D, Hosooka, T, Hou, L, Hou, W, Howie, L, Howson, A, Hozak, M, Htet, Z, Hu, X, Hu, Y, Huang, J, Huda, N, Hudig, L, Hudson, A, Hugo, C, Hull, R, Hume, L, Hundei, W, Hunt, N, Hunter, A, Hurley, S, Hurst, A, Hutchinson, C, Hyo, T, Ibrahim, FH, Ibrahim, S, Ihana, N, Ikeda, T, Imai, A, Imamine, R, Inamori, A, Inazawa, H, Ingell, J, Inomata, K, Inukai, Y, Ioka, M, Irtiza-Ali, A, Isakova, T, Isari, W, Iselt, M, Ishiguro, A, Ishihara, K, Ishikawa, T, Ishimoto, T, Ishizuka, K, Ismail, R, Itano, S, Ito, H, Ito, K, Ito, M, Ito, Y, Iwagaitsu, S, Iwaita, Y, Iwakura, T, Iwamoto, M, Iwasa, M, Iwasaki, H, Iwasaki, S, Izumi, K, Izumi, T, Jaafar, SM, Jackson, C, Jackson, Y, Jafari, G, Jahangiriesmaili, M, Jain, N, Jansson, K, Jasim, H, Jeffers, L, Jenkins, A, Jesky, M, Jesus-Silva, J, Jeyarajah, D, Jiang, Y, Jiao, X, Jimenez, G, Jin, B, Jin, Q, Jochims, J, Johns, B, Johnson, C, Johnson, T, Jolly, S, Jones, L, Jones, S, Jones, T, Jones, V, Joseph, M, Joshi, S, Judge, P, Junejo, N, Junus, S, Kachele, M, Kadoya, H, Kaga, H, Kai, H, Kajio, H, Kaluza-Schilling, W, Kamaruzaman, L, Kamarzarian, A, Kamimura, Y, Kamiya, H, Kamundi, C, Kan, T, Kanaguchi, Y, Kanazawa, A, Kanda, E, Kanegae, S, Kaneko, K, Kang, HY, Kano, T, Karim, M, Karounos, D, Karsan, W, Kasagi, R, Kashihara, N, Katagiri, H, Katanosaka, A, Katayama, A, Katayama, M, Katiman, E, Kato, K, Kato, M, Kato, N, Kato, S, Kato, T, Kato, Y, Katsuda, Y, Katsuno, T, Kaufeld, J, Kavak, Y, Kawai, I, Kawai, M, Kawase, A, Kawashima, S, Kazory, A, Kearney, J, Keith, B, Kellett, J, Kelley, S, Kershaw, M, Ketteler, M, Khai, Q, Khairullah, Q, Khandwala, H, Khoo, KKL, Khwaja, A, Kidokoro, K, Kielstein, J, Kihara, M, Kimber, C, Kimura, S, Kinashi, H, Kingston, H, Kinomura, M, Kinsella-Perks, E, Kitagawa, M, Kitajima, M, Kitamura, S, Kiyosue, A, Kiyota, M, Klauser, F, Klausmann, G, Kmietschak, W, Knapp, K, Knight, C, Knoppe, A, Knott, C, Kobayashi, M, Kobayashi, R, Kobayashi, T, Koch, M, Kodama, S, Kodani, N, Kogure, E, Koizumi, M, Kojima, H, Kojo, T, Kolhe, N, Komaba, H, Komiya, T, Komori, H, Kon, SP, Kondo, M, Kong, W, Konishi, M, Kono, K, Koshino, M, Kosugi, T, Kothapalli, B, Kozlowski, T, Kraemer, B, Kraemer-Guth, A, Krappe, J, Kraus, D, Kriatselis, C, Krieger, C, Krish, P, Kruger, B, Ku Md Razi, KR, Kuan, Y, Kubota, S, Kuhn, S, Kumar, P, Kume, S, Kummer, I, Kumuji, R, Küpper, A, Kuramae, T, Kurian, L, Kuribayashi, C, Kurien, R, Kuroda, E, Kurose, T, Kutschat, A, Kuwabara, N, Kuwata, H, La Manna, G, Lacey, M, Lafferty, K, LaFleur, P, Lai, V, Laity, E, Lambert, A, Langlois, M, Latif, F, Latore, E, Laundy, E, Laurienti, D, Lawson, A, Lay, M, Leal, I, Lee, AK, Lee, J, Lee, KQ, Lee, R, Lee, SA, Lee, YY, Lee-Barkey, Y, Leonard, N, Leoncini, G, Leong, CM, Lerario, S, Leslie, A, Lewington, A, Li, N, Li, X, Li, Y, Liberti, L, Liberti, ME, Liew, A, Liew, YF, Lilavivat, U, Lim, SK, Lim, YS, Limon, E, Lin, H, Lioudaki, E, Liu, H, Liu, J, Liu, L, Liu, Q, Liu, X, Liu, Z, Loader, D, Lochhead, H, Loh, CL, Lorimer, A, Loudermilk, L, Loutan, J, Low, CK, Low, CL, Low, YM, Lozon, Z, Lu, Y, Lucci, D, Ludwig, U, Luker, N, Lund, D, Lustig, R, Lyle, S, Macdonald, C, MacDougall, I, Machicado, R, MacLean, D, Macleod, P, Madera, A, Madore, F, Maeda, K, Maegawa, H, Maeno, S, Mafham, M, Magee, J, Mah, DY, Mahabadi, V, Maiguma, M, Makita, Y, Makos, G, Manco, L, Mangiacapra, R, Manley, J, Mann, P, Mano, S, Marcotte, G, Maris, J, Mark, P, Markau, S, Markovic, M, Marshall, C, Martin, M, Martinez, C, Martinez, S, Martins, G, Maruyama, K, Maruyama, S, Marx, K, Maselli, A, Masengu, A, Maskill, A, Masumoto, S, Masutani, K, Matsumoto, M, Matsunaga, T, Matsuoka, N, Matsushita, M, Matthews, M, Matthias, S, Matvienko, E, Maurer, M, Maxwell, P, Mazlan, N, Mazlan, SA, Mbuyisa, A, McCafferty, K, McCarroll, F, McCarthy, T, McClary-Wright, C, McCray, K, McDermott, P, McDonald, C, McDougall, R, McHaffie, E, McIntosh, K, McKinley, T, McLaughlin, S, McLean, N, McNeil, L, Measor, A, Meek, J, Mehta, A, Mehta, R, Melandri, M, Mené, P, Meng, T, Menne, J, Merritt, K, Merscher, S, Meshykhi, C, Messa, P, Messinger, L, Miftari, N, Miller, R, Miller, Y, Miller-Hodges, E, Minatoguchi, M, Miners, M, Minutolo, R, Mita, T, Miura, Y, Miyaji, M, Miyamoto, S, Miyatsuka, T, Miyazaki, M, Miyazawa, I, Mizumachi, R, Mizuno, M, Moffat, S, Mohamad Nor, FS, Mohamad Zaini, SN, Mohamed Affandi, FA, Mohandas, C, Mohd, R, Mohd Fauzi, NA, Mohd Sharif, NH, Mohd Yusoff, Y, Moist, L, Moncada, A, Montasser, M, Moon, A, Moran, C, Morgan, N, Moriarty, J, Morig, G, Morinaga, H, Morino, K, Morisaki, T, Morishita, Y, Morlok, S, Morris, A, Morris, F, Mostafa, S, Mostefai, Y, Motegi, M, Motherwell, N, Motta, D, Mottl, A, Moys, R, Mozaffari, S, Muir, J, Mulhern, J, Mulligan, S, Munakata, Y, Murakami, C, Murakoshi, M, Murawska, A, Murphy, K, Murphy, L, Murray, S, Murtagh, H, Musa, MA, Mushahar, L, Mustafa, R, Mustafar, R, Muto, M, Nadar, E, Nagano, R, Nagasawa, T, Nagashima, E, Nagasu, H, Nagelberg, S, Nair, H, Nakagawa, Y, Nakahara, M, Nakamura, J, Nakamura, R, Nakamura, T, Nakaoka, M, Nakashima, E, Nakata, J, Nakata, M, Nakatani, S, Nakatsuka, A, Nakayama, Y, Nakhoul, G, Naverrete, G, Navivala, A, Nazeer, I, Negrea, L, Nethaji, C, Newman, E, Ng, TJ, Ngu, LLS, Nimbkar, T, Nishi, H, Nishi, M, Nishi, S, Nishida, Y, Nishiyama, A, Niu, J, Niu, P, Nobili, G, Nohara, N, Nojima, I, Nolan, J, Nosseir, H, Nozawa, M, Nunn, M, Nunokawa, S, Oda, M, Oe, M, Oe, Y, Ogane, K, Ogawa, W, Ogihara, T, Oguchi, G, Ohsugi, M, Oishi, K, Okada, Y, Okajyo, J, Okamoto, S, Okamura, K, Olufuwa, O, Oluyombo, R, Omata, A, Omori, Y, Ong, LM, Ong, YC, Onyema, J, Oomatia, A, Oommen, A, Oremus, R, Orimo, Y, Ortalda, V, Osaki, Y, Osawa, Y, Osmond Foster, J, O'Sullivan, A, Otani, T, Othman, N, Otomo, S, O'Toole, J, Owen, L, Ozawa, T, Padiyar, A, Page, N, Pajak, S, Paliege, A, Pandey, A, Pandey, R, Pariani, H, Park, J, Parrigon, M, Passauer, J, Patecki, M, Patel, M, Patel, R, Patel, T, Patel, Z, Paul, R, Paulsen, L, Pavone, L, Peixoto, A, Peji, J, Peng, BC, Peng, K, Pennino, L, Pereira, E, Perez, E, Pergola, P, Pesce, F, Pessolano, G, Petchey, W, Petr, EJ, Pfab, T, Phelan, P, Phillips, R, Phillips, T, Phipps, M, Piccinni, G, Pickett, T, Pickworth, S, Piemontese, M, Pinto, D, Piper, J, Plummer-Morgan, J, Poehler, D, Polese, L, Poma, V, Postal, A, Pötz, C, Power, A, Pradhan, N, Pradhan, R, Preiss, E, Preston, K, Prib, N, Price, L, Provenzano, C, Pugay, C, Pulido, R, Putz, F, Qiao, Y, Quartagno, R, Quashie-Akponeware, M, Rabara, R, Rabasa-Lhoret, R, Radhakrishnan, D, Radley, M, Raff, R, Raguwaran, S, Rahbari-Oskoui, F, Rahman, M, Rahmat, K, Ramadoss, S, Ramanaidu, S, Ramasamy, S, Ramli, R, Ramli, S, Ramsey, T, Rankin, A, Rashidi, A, Raymond, L, Razali, WAFA, Read, K, Reiner, H, Reisler, A, Reith, C, Renner, J, Rettenmaier, B, Richmond, L, Rijos, D, Rivera, R, Rivers, V, Robinson, H, Rocco, M, Rodriguez-Bachiller, I, Rodriquez, R, Roesch, C, Roesch, J, Rogers, J, Rohnstock, M, Rolfsmeier, S, Roman, M, Romo, A, Rosati, A, Rosenberg, S, Ross, T, Roura, M, Roussel, M, Rovner, S, Roy, S, Rucker, S, Rump, L, Ruocco, M, Ruse, S, Russo, F, Russo, M, Ryder, M, Sabarai, A, Saccà, C, Sachson, R, Sadler, E, Safiee, NS, Sahani, M, Saillant, A, Saini, J, Saito, C, Saito, S, Sakaguchi, K, Sakai, M, Salim, H, Salviani, C, Sampson, A, Samson, F, Sandercock, P, Sanguila, S, Santorelli, G, Santoro, D, Sarabu, N, Saram, T, Sardell, R, Sasajima, H, Sasaki, T, Satko, S, Sato, A, Sato, D, Sato, H, Sato, J, Sato, T, Sato, Y, Satoh, M, Sawada, K, Schanz, M, Scheidemantel, F, Schemmelmann, M, Schettler, E, Schettler, V, Schlieper, GR, Schmidt, C, Schmidt, G, Schmidt, U, Schmidt-Gurtler, H, Schmude, M, Schneider, A, Schneider, I, Schneider-Danwitz, C, Schomig, M, Schramm, T, Schreiber, A, Schricker, S, Schroppel, B, Schulte-Kemna, L, Schulz, E, Schumacher, B, Schuster, A, Schwab, A, Scolari, F, Scott, A, Seeger, W, Segal, M, Seifert, L, Seifert, M, Sekiya, M, Sellars, R, Seman, MR, Shah, S, Shainberg, L, Shanmuganathan, M, Shao, F, Sharma, K, Sharpe, C, Sheikh-Ali, M, Sheldon, J, Shenton, C, Shepherd, A, Shepperd, M, Sheridan, R, Sheriff, Z, Shibata, Y, Shigehara, T, Shikata, K, Shimamura, K, Shimano, H, Shimizu, Y, Shimoda, H, Shin, K, Shivashankar, G, Shojima, N, Silva, R, Sim, CSB, Simmons, K, Sinha, S, Sitter, T, Sivanandam, S, Skipper, M, Sloan, K, Sloan, L, Smith, R, Smyth, J, Sobande, T, Sobata, M, Somalanka, S, Song, X, Sonntag, F, Sood, B, Sor, SY, Soufer, J, Sparks, H, Spatoliatore, G, Spinola, T, Squyres, S, Srivastava, A, Stanfield, J, Staylor, K, Steele, A, Steen, O, Steffl, D, Stegbauer, J, Stellbrink, C, Stellbrink, E, Stevenson, A, Stewart-Ray, V, Stickley, J, Stoffler, D, Stratmann, B, Streitenberger, S, Strutz, F, Stubbs, J, Stumpf, J, Suazo, N, Suchinda, P, Suckling, R, Sudin, A, Sugamori, K, Sugawara, H, Sugawara, K, Sugimoto, D, Sugiyama, H, Sugiyama, T, Sullivan, M, Sumi, M, Suresh, N, Sutton, D, Suzuki, H, Suzuki, R, Suzuki, Y, Swanson, E, Swift, P, Syed, S, Szerlip, H, Taal, M, Taddeo, M, Tailor, C, Tajima, K, Takagi, M, Takahashi, K, Takahashi, M, Takahashi, T, Takahira, E, Takai, T, Takaoka, M, Takeoka, J, Takesada, A, Takezawa, M, Talbot, M, Taliercio, J, Talsania, T, Tamori, Y, Tamura, R, Tamura, Y, Tan, CHH, Tan, EZZ, Tanabe, A, Tanabe, K, Tanaka, A, Tanaka, N, Tang, S, Tang, Z, Tanigaki, K, Tarlac, M, Tatsuzawa, A, Tay, JF, Tay, LL, Taylor, J, Taylor, K, Te, A, Tenbusch, L, Teng, KS, Terakawa, A, Terry, J, Tham, ZD, Tholl, S, Thomas, G, Thong, KM, Tietjen, D, Timadjer, A, Tindall, H, Tipper, S, Tobin, K, Toda, N, Tokuyama, A, Tolibas, M, Tomita, A, Tomita, T, Tomlinson, J, Tonks, L, Topf, J, Topping, S, Torp, A, Torres, A, Totaro, F, Toth, P, Toyonaga, Y, Tripodi, F, Trivedi, K, Tropman, E, Tschope, D, Tse, J, Tsuji, K, Tsunekawa, S, Tsunoda, R, Tucky, B, Tufail, S, Tuffaha, A, Turan, E, Turner, H, Turner, J, Turner, M, Tye, YL, Tyler, A, Tyler, J, Uchi, H, Uchida, H, Uchida, T, Udagawa, T, Ueda, S, Ueda, Y, Ueki, K, Ugni, S, Ugwu, E, Umeno, R, Unekawa, C, Uozumi, K, Urquia, K, Valleteau, A, Valletta, C, van Erp, R, Vanhoy, C, Varad, V, Varma, R, Varughese, A, Vasquez, P, Vasseur, A, Veelken, R, Velagapudi, C, Verdel, K, Vettoretti, S, Vezzoli, G, Vielhauer, V, Viera, R, Vilar, E, Villaruel, S, 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2024
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27. Effects of empagliflozin on progression of chronic kidney disease: a prespecified secondary analysis from the empa-kidney trial

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Staplin, N, Haynes, R, Judge, PK, Wanner, C, Green, JB, Emberson, J, Preiss, D, Mayne, KJ, Ng, SYA, Sammons, E, Zhu, D, Hill, M, Stevens, W, Wallendszus, K, Brenner, S, Cheung, AK, Liu, ZH, Li, J, Hooi, LS, Liu, WJ, Kadowaki, T, Nangaku, M, Levin, A, Cherney, D, Maggioni, AP, Pontremoli, R, Deo, R, Goto, S, Rossello, X, Tuttle, KR, Steubl, D, Petrini, M, Seidi, S, Landray, MJ, Baigent, C, Herrington, WG, Abat, S, Abd Rahman, R, Abdul Cader, R, Abdul Hafidz, MI, Abdul Wahab, MZ, Abdullah, NK, Abdul-Samad, T, Abe, M, Abraham, N, Acheampong, S, Achiri, P, Acosta, JA, Adeleke, A, Adell, V, Adewuyi-Dalton, R, Adnan, N, Africano, A, Agharazii, M, Aguilar, F, Aguilera, A, Ahmad, M, Ahmad, MK, Ahmad, NA, Ahmad, NH, Ahmad, NI, Ahmad Miswan, N, Ahmad Rosdi, H, Ahmed, I, Ahmed, S, Aiello, J, Aitken, A, AitSadi, R, Aker, S, Akimoto, S, Akinfolarin, A, Akram, S, Alberici, F, Albert, C, Aldrich, L, Alegata, M, Alexander, L, Alfaress, S, Alhadj Ali, M, Ali, A, Alicic, R, Aliu, A, Almaraz, R, 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Miyazawa, I, Mizumachi, R, Mizuno, M, Moffat, S, Mohamad Nor, FS, Mohamad Zaini, SN, Mohamed Affandi, FA, Mohandas, C, Mohd, R, Mohd Fauzi, NA, Mohd Sharif, NH, Mohd Yusoff, Y, Moist, L, Moncada, A, Montasser, M, Moon, A, Moran, C, Morgan, N, Moriarty, J, Morig, G, Morinaga, H, Morino, K, Morisaki, T, Morishita, Y, Morlok, S, Morris, A, Morris, F, Mostafa, S, Mostefai, Y, Motegi, M, Motherwell, N, Motta, D, Mottl, A, Moys, R, Mozaffari, S, Muir, J, Mulhern, J, Mulligan, S, Munakata, Y, Murakami, C, Murakoshi, M, Murawska, A, Murphy, K, Murphy, L, Murray, S, Murtagh, H, Musa, MA, Mushahar, L, Mustafa, R, Mustafar, R, Muto, M, Nadar, E, Nagano, R, Nagasawa, T, Nagashima, E, Nagasu, H, Nagelberg, S, Nair, H, Nakagawa, Y, Nakahara, M, Nakamura, J, Nakamura, R, Nakamura, T, Nakaoka, M, Nakashima, E, Nakata, J, Nakata, M, Nakatani, S, Nakatsuka, A, Nakayama, Y, Nakhoul, G, Naverrete, G, Navivala, A, Nazeer, I, Negrea, L, Nethaji, C, Newman, E, Ng, TJ, Ngu, LLS, Nimbkar, T, Nishi, H, Nishi, M, Nishi, S, Nishida, Y, Nishiyama, A, Niu, J, Niu, P, Nobili, G, Nohara, N, Nojima, I, Nolan, J, Nosseir, H, Nozawa, M, Nunn, M, Nunokawa, S, Oda, M, Oe, M, Oe, Y, Ogane, K, Ogawa, W, Ogihara, T, Oguchi, G, Ohsugi, M, Oishi, K, Okada, Y, Okajyo, J, Okamoto, S, Okamura, K, Olufuwa, O, Oluyombo, R, Omata, A, Omori, Y, Ong, LM, Ong, YC, Onyema, J, Oomatia, A, Oommen, A, Oremus, R, Orimo, Y, Ortalda, V, Osaki, Y, Osawa, Y, Osmond Foster, J, O'Sullivan, A, Otani, T, Othman, N, Otomo, S, O'Toole, J, Owen, L, Ozawa, T, Padiyar, A, Page, N, Pajak, S, Paliege, A, Pandey, A, Pandey, R, Pariani, H, Park, J, Parrigon, M, Passauer, J, Patecki, M, Patel, M, Patel, R, Patel, T, Patel, Z, Paul, R, Paulsen, L, Pavone, L, Peixoto, A, Peji, J, Peng, BC, Peng, K, Pennino, L, Pereira, E, Perez, E, Pergola, P, Pesce, F, Pessolano, G, Petchey, W, Petr, EJ, Pfab, T, Phelan, P, Phillips, R, Phillips, T, Phipps, M, Piccinni, G, Pickett, T, Pickworth, S, Piemontese, M, Pinto, D, Piper, J, Plummer-Morgan, J, Poehler, D, Polese, L, Poma, V, Postal, A, Pötz, C, Power, A, Pradhan, N, Pradhan, R, Preiss, E, Preston, K, Prib, N, Price, L, Provenzano, C, Pugay, C, Pulido, R, Putz, F, Qiao, Y, Quartagno, R, Quashie-Akponeware, M, Rabara, R, Rabasa-Lhoret, R, Radhakrishnan, D, Radley, M, Raff, R, Raguwaran, S, Rahbari-Oskoui, F, Rahman, M, Rahmat, K, Ramadoss, S, Ramanaidu, S, Ramasamy, S, Ramli, R, Ramli, S, Ramsey, T, Rankin, A, Rashidi, A, Raymond, L, Razali, WAFA, Read, K, Reiner, H, Reisler, A, Reith, C, Renner, J, Rettenmaier, B, Richmond, L, Rijos, D, Rivera, R, Rivers, V, Robinson, H, Rocco, M, Rodriguez-Bachiller, I, Rodriquez, R, Roesch, C, Roesch, J, Rogers, J, Rohnstock, M, Rolfsmeier, S, Roman, M, Romo, A, Rosati, A, Rosenberg, S, Ross, T, Roura, M, Roussel, M, Rovner, S, Roy, S, Rucker, S, Rump, L, Ruocco, M, Ruse, S, Russo, F, Russo, M, Ryder, M, Sabarai, A, Saccà, C, Sachson, R, Sadler, E, Safiee, NS, Sahani, M, Saillant, A, Saini, J, Saito, C, Saito, S, Sakaguchi, K, Sakai, M, Salim, H, Salviani, C, Sampson, A, Samson, F, Sandercock, P, Sanguila, S, Santorelli, G, Santoro, D, Sarabu, N, Saram, T, Sardell, R, Sasajima, H, Sasaki, T, Satko, S, Sato, A, Sato, D, Sato, H, Sato, J, Sato, T, Sato, Y, Satoh, M, Sawada, K, Schanz, M, Scheidemantel, F, Schemmelmann, M, Schettler, E, Schettler, V, Schlieper, GR, Schmidt, C, Schmidt, G, Schmidt, U, Schmidt-Gurtler, H, Schmude, M, Schneider, A, Schneider, I, Schneider-Danwitz, C, Schomig, M, Schramm, T, Schreiber, A, Schricker, S, Schroppel, B, Schulte-Kemna, L, Schulz, E, Schumacher, B, Schuster, A, Schwab, A, Scolari, F, Scott, A, Seeger, W, Segal, M, Seifert, L, Seifert, M, Sekiya, M, Sellars, R, Seman, MR, Shah, S, Shainberg, L, Shanmuganathan, M, Shao, F, Sharma, K, Sharpe, C, Sheikh-Ali, M, Sheldon, J, Shenton, C, Shepherd, A, Shepperd, M, Sheridan, R, Sheriff, Z, Shibata, Y, Shigehara, T, Shikata, K, Shimamura, K, Shimano, H, Shimizu, Y, Shimoda, H, Shin, K, Shivashankar, G, Shojima, N, Silva, R, Sim, CSB, Simmons, K, Sinha, S, Sitter, T, Sivanandam, S, Skipper, M, Sloan, K, Sloan, L, Smith, R, Smyth, J, Sobande, T, Sobata, M, Somalanka, S, Song, X, Sonntag, F, Sood, B, Sor, SY, Soufer, J, Sparks, H, Spatoliatore, G, Spinola, T, Squyres, S, Srivastava, A, Stanfield, J, Staylor, K, Steele, A, Steen, O, Steffl, D, Stegbauer, J, Stellbrink, C, Stellbrink, E, Stevenson, A, Stewart-Ray, V, Stickley, J, Stoffler, D, Stratmann, B, Streitenberger, S, Strutz, F, Stubbs, J, Stumpf, J, Suazo, N, Suchinda, P, Suckling, R, Sudin, A, Sugamori, K, Sugawara, H, Sugawara, K, Sugimoto, D, Sugiyama, H, Sugiyama, T, Sullivan, M, Sumi, M, Suresh, N, Sutton, D, Suzuki, H, Suzuki, R, Suzuki, Y, Swanson, E, Swift, P, Syed, S, Szerlip, H, Taal, M, Taddeo, M, Tailor, C, Tajima, K, Takagi, M, Takahashi, K, Takahashi, M, Takahashi, T, Takahira, E, Takai, T, Takaoka, M, Takeoka, J, Takesada, A, Takezawa, M, Talbot, M, Taliercio, J, Talsania, T, Tamori, Y, Tamura, R, Tamura, Y, Tan, CHH, Tan, EZZ, Tanabe, A, Tanabe, K, Tanaka, A, Tanaka, N, Tang, S, Tang, Z, Tanigaki, K, Tarlac, M, Tatsuzawa, A, Tay, JF, Tay, LL, Taylor, J, Taylor, K, Te, A, Tenbusch, L, Teng, KS, Terakawa, A, Terry, J, Tham, ZD, Tholl, S, Thomas, G, Thong, KM, Tietjen, D, Timadjer, A, Tindall, H, Tipper, S, Tobin, K, Toda, N, Tokuyama, A, Tolibas, M, Tomita, A, Tomita, T, Tomlinson, J, Tonks, L, Topf, J, Topping, S, Torp, A, Torres, A, Totaro, F, Toth, P, Toyonaga, Y, Tripodi, F, Trivedi, K, Tropman, E, Tschope, D, Tse, J, Tsuji, K, Tsunekawa, S, Tsunoda, R, Tucky, B, Tufail, S, Tuffaha, A, Turan, E, Turner, H, Turner, J, Turner, M, Tye, YL, Tyler, A, Tyler, J, Uchi, H, Uchida, H, Uchida, T, Udagawa, T, Ueda, S, Ueda, Y, Ueki, K, Ugni, S, Ugwu, E, Umeno, R, Unekawa, C, Uozumi, K, Urquia, K, Valleteau, A, Valletta, C, van Erp, R, Vanhoy, C, Varad, V, Varma, R, Varughese, A, Vasquez, P, Vasseur, A, Veelken, R, Velagapudi, C, Verdel, K, Vettoretti, S, Vezzoli, G, Vielhauer, V, Viera, R, Vilar, E, Villaruel, S, Vinall, L, Vinathan, J, Visnjic, M, Voigt, E, von-Eynatten, M, Vourvou, M, Wada, J, Wada, T, Wada, Y, Wakayama, K, Wakita, Y, Walters, T, Wan Mohamad, WH, Wang, L, Wang, W, Wang, X, Wang, Y, Wanninayake, S, Watada, H, Watanabe, K, Watanabe, M, Waterfall, H, Watkins, D, Watson, S, Weaving, L, Weber, B, Webley, Y, Webster, A, Webster, M, Weetman, M, Wei, W, Weihprecht, H, Weiland, L, Weinmann-Menke, J, Weinreich, T, Wendt, R, Weng, Y, Whalen, M, Whalley, G, Wheatley, R, Wheeler, A, Wheeler, J, Whelton, P, White, K, Whitmore, B, Whittaker, S, Wiebel, J, Wiley, J, Wilkinson, L, Willett, M, Williams, A, Williams, E, Williams, K, Williams, T, Wilson, A, Wilson, P, Wincott, L, Wines, E, Winkelmann, B, Winkler, M, Winter-Goodwin, B, Witczak, J, Wittes, J, Wittmann, M, Wolf, G, Wolf, L, Wolfling, R, Wong, C, Wong, E, Wong, HS, Wong, LW, Wong, YH, Wonnacott, A, Wood, A, Wood, L, Woodhouse, H, Wooding, N, Woodman, A, Wren, K, Wu, J, Wu, P, Xia, S, Xiao, H, Xiao, X, Xie, Y, Xu, C, Xu, Y, Xue, H, Yahaya, H, Yalamanchili, H, Yamada, A, Yamada, N, Yamagata, K, Yamaguchi, M, Yamaji, Y, Yamamoto, A, Yamamoto, S, Yamamoto, T, Yamanaka, A, Yamano, T, Yamanouchi, Y, Yamasaki, N, Yamasaki, Y, Yamashita, C, Yamauchi, T, Yan, Q, Yanagisawa, E, Yang, F, Yang, L, Yano, S, Yao, S, Yao, Y, Yarlagadda, S, Yasuda, Y, Yiu, V, Yokoyama, T, Yoshida, S, Yoshidome, E, Yoshikawa, H, Young, A, Young, T, Yousif, V, Yu, H, Yu, Y, Yuasa, K, Yusof, N, Zalunardo, N, Zander, B, Zani, R, Zappulo, F, Zayed, M, Zemann, B, Zettergren, P, Zhang, H, Zhang, L, Zhang, N, Zhang, X, Zhao, J, Zhao, L, Zhao, S, Zhao, Z, Zhong, H, Zhou, N, Zhou, S, Zhu, L, Zhu, S, Zietz, M, Zippo, M, Zirino, F, and Zulkipli, FH

Published
2024
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28. Significant nonclassical paths with atoms and cavities in the double-slit experiment

Author

de Almeida, J. O., Lewenstein, M., and Quach, J. Q.

Subjects
Quantum Physics
Abstract

In the the double-slit experiment, nonclassical paths are Feynman paths that go through both slits. Prior work with atom cavities as which-way detectors in the double-slit experiment has shown these paths to be experimentally inaccessible. In this paper, we show how such a setup can indeed detect nonclassical paths with 1% probability if one considers a different type of nonclassical path than previously investigated. We also show how this setup can be used to erase and restore the coherence of the nonclassical paths. Finally, we also show how atom cavities may be used to implement a exact measure of Born-rule violation [Quach, Which-way double-slit experiments and Born-rule violation, Phys. Rev. A 95, 042129 (2017)], which up until now has only been a formal construct.

Published
2020
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29. Analysis of the galaxy size versus stellar mass relation

Author

Almeida, J. Sanchez

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The scatter in the galaxy size versus stellar mass (Mstar) relation gets largely reduced when, rather than the half-mass radius Re, the size at a fixed surface density is used. Here we address why this happens. We show how a reduction is to be expected because any two galaxies with the same Mstar have at least one radius with identical surface density, where the galaxies have identical size. However, the reason why the scatter is reduced to the observed level is not trivial, and we pin it down to the galaxy surface density profiles approximately following Sersic profiles with their Re and Sersic index (n) anti-correlated (i.e., given Mstar, n increases when Re decreases). Our analytical results describe very well the behavior of the observed galaxies as portrayed in the NASA Sloan Atlas (NSA), which contains more than half a million local objects with 7 < log(Mstar/Msun) < 11.5. The comparison with NSA galaxies also allows us to find the optimal values for the mass surface density (2.4m0.9p1.3 Msun/pc2) and surface brightness (r-band 24.7pm0.5 mag/arcsec2) that minimize the scatter, although the actual values depend somehow on the subset of NSA galaxies used for optimization. The physical reason for the existence of optimal values is unknown but, as Trujillo+20 point out, they are close to the gas surface density threshold to form stars and thus may trace the physical end of a galaxy. Our NSA-based size--mass relation agrees with theirs on the slope as well as on the magnitude of the scatter. As a by-product of the narrowness of the size--mass relation (only 0.06 dex), we propose to use the size of a galaxy to measure its stellar mass. In terms of observing time, it is not more demanding than the usual photometric techniques and may present practical advantages in particular cases., Comment: Accepted for publication in MNRAS. 11 figures. 12 pages

Published
2020
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30. Discrimination and estimation of incoherent sources under misalignment

Author

de Almeida, J. O., Kołodyński, J., Hirche, C., Lewenstein, M., and Skotiniotis, M.

Subjects
Quantum Physics
Abstract

Spatially resolving two incoherent point sources whose separation is well below the diffraction limit dictated by classical optics has recently been shown possible using techniques that decompose the incoming radiation into orthogonal transverse modes. Such a demultiplexing procedure, however, must be perfectly calibrated to the transverse profile of the incoming light as any misalignment of the modes effectively restores the diffraction limit for small source separations. We study by how much can one mitigate such an effect at the level of measurement which, after being imperfectly demultiplexed due to inevitable misalignment, may still be partially corrected by linearly transforming the relevant dominating transverse modes. We consider two complementary tasks: the estimation of the separation between the two sources and the discrimination between one and two incoherent point sources. We show that, although one cannot fully restore super-resolving powers even when the value of the misalignment is perfectly known its negative impact on the ultimate sensitivity can be significantly reduced. In the case of estimation we analytically determine the exact relation between the minimal resolvable separation as a function of misalignment whereas for discrimination we analytically determine the relation between misalignment and the probability of error, as well as numerically determine how the latter scales in the limit of long interrogation times., Comment: 15 pages, 13 figures

Published
2020
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31. Profinite congruences and unary algebras

Author

Almeida, J. and Klíma, O.

Subjects
Mathematics - Group Theory, Computer Science - Logic in Computer Science, 08A60, 08A62, 20M07, 20M05
Abstract

Profinite congruences on profinite algebras determining profinite quotients are difficult to describe. In particular, no constructive description is known of the least profinite congruence containing a given binary relation on the algebra. On the other hand, closed congruences and fully invariant congruences can be described constructively. In a previous paper, we conjectured that fully invariant closed congruences on a relatively free profinite algebra are always profinite. Here, we show that our conjecture fails for unary algebras and that closed congruences on relatively free profinite semigroups are not necessarily profinite. As part of our study of unary algebras, we establish an adjunction between profinite unary algebras and profinite monoids. We also show that the Polish representation of the free profinite unary algebra is faithful.

Published
2020

32. Triaxiality can explain the alleged dark matter deficiency in some dwarf galaxies

Author

Almeida, J. Sanchez and Filho, M.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Dark Matter (DM) is an ingredient essential to the current cosmological concordance model. It provides the gravitational pull needed for the baryons to form galaxies. Therefore, the existence of galaxies without DM is both disquieting and extremely interesting. Guo et al. recently presented "further evidence for a population of DM-deficient dwarf galaxies", however, their analysis bypasses the triaxiality of the dwarf galaxies. We carry out a Monte Carlo simulation showing how triaxiality must be considered to measure dynamical masses from projected axial ratios, calling into question the evidence for a population of DM-deficient dwarf galaxies. Such a population may consist of normal almost face-on HI disks with their inclination overestimated., Comment: To appear as a RNAAS

Published
2019

35. A contribution of star-forming clumps and accreting satellites to the mass assembly of z ~ 2 galaxies

Author

Zanella, A., Floc'h, E. Le, Harrison, C. M., Daddi, E., Bernhard, E., Gobat, R., Strazzullo, V., Valentino, F., Cibinel, A., Almeida, J. Sánchez, Kohandel, M., Fensch, J., Behrendt, M., Burkert, A., Onodera, M., Bournaud, F., and Scholtz, J.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We investigate the contribution of clumps and satellites to the galaxy mass assembly. We analyzed spatially-resolved Hubble Space Telescope observations (imaging and slitless spectroscopy) of 53 star-forming galaxies at z ~ 1 - 3. We created continuum and emission line maps and pinpointed residual "blobs" detected after subtracting the galaxy disk. Those were separated into compact (unresolved) and extended (resolved) components. Extended components have sizes ~ 2 kpc and comparable stellar mass and age as the galaxy disks, whereas the compact components are 1.5 dex less massive and 0.4 dex younger than the disks. Furthermore the extended blobs are typically found at larger distances from the galaxy barycenter than the compact ones. Prompted by these observations and by the comparison with simulations, we suggest that compact blobs are in-situ formed clumps, whereas the extended ones are accreting satellites. Clumps and satellites enclose respectively ~ 20% and ~< 80% of the galaxy stellar mass, ~ 30% and ~ 20% of its star formation rate. Considering the compact blobs, we statistically estimated that massive clumps (Mstar >~ 10^9 Msun) have lifetimes of ~ 650 Myr, and the less massive ones (10^8 < Mstar < 10^9 Msun) of ~ 145 Myr. This supports simulations predicting long-lived clumps (lifetime > 100 Myr). Finally, ~< 30% (13%) of our sample galaxies are undergoing single (multiple) merger(s), they have a projected separation ~< 10 kpc, and the typical mass ratio of our satellites is 1:5 (but ranges between 1:10 and 1:1), in agreement with literature results for close pair galaxies., Comment: 20 pages (plus appendix), 8 figures, 2 tables. Accepted for publication in MNRAS

Published
2019
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36. Inferring the 3-D shapes of extremely metal-poor galaxies from sets of projected shapes

Author

Putko, J., Almeida, J. Sanchez, Munoz-Tunon, C., Ramos, A. Asensio, Elmegreen, B. G., and Elmegreen, D. M.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The three-dimensional (3-D) shape of a galaxy inevitably is tied to how it has formed and evolved and to its dark matter halo. Local extremely metal-poor galaxies (XMPs; defined as having an average gas-phase metallicity < 0.1 solar) are important objects for understanding galaxy evolution largely because they appear to be caught in the act of accreting gas from the cosmic web, and their 3-D shape may reflect this. Here we report on the 3-D shape of XMPs as inferred from their observed projected minor-to-major axial ratios using a hierarchical Bayesian inference model, which determines the likely shape and orientation of each galaxy while simultaneously inferring the average shape and dispersion. We selected a sample of 149 XMPs and divided it into three sub-samples according to physical size and found that (1) the stellar component of XMPs of all sizes tends to be triaxial, with an intermediate axis approx 0.7 times the longest axis and that (2) smaller XMPs tend to be relatively thicker, with the shortest axis going from approx 0.15 times the longest axis for the large galaxies to approx 0.4 for the small galaxies. We provide the inferred 3-D shape and inclination of the individual XMPs in electronic format. We show that our results for the intermediate axis are not clouded by a selection effect against face-on XMPs. We discuss how an intermediate axis significantly smaller than the longest axis may be produced by several mechanisms, including lopsided gas accretion, non-axisymmetric star formation, or coupling with an elongated dark matter halo. Large relative thickness may reflect slow rotation, stellar feedback, or recent gas accretion., Comment: Accepted for publicaction in ApJ. 15 pages, 9 figures. Table with the shapes of the individual XMP galaxies available

Published
2019
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37. The fundamental metallicity relation emerges from the local anti-correlation between star formation rate and gas-phase metallicity existing in disk galaxies

Author

Almeida, J. Sanchez and Sanchez-Menguiano, L.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The fundamental metallicity relation (FMR) states that galaxies of the same stellar mass but larger star formation rate (SFR) tend to have smaller gas-phase metallicity (). It is thought to be fundamental because it naturally arises from the stochastic feeding of star-formation from external metal-poor gas accretion, a process extremely elusive to observe but essential according the cosmological simulations of galaxy formation. In this letter, we show how the FMR emerges from the local anti-correlation between SFR surface density and Zg recently observed to exist in disk galaxies. We analytically derive the global FMR from the local law, and then show that both relations agree quantitatively when considering the star-forming galaxies of the MaNGA survey. Thus, understanding the FMR becomes equivalent to understanding the origin of the anti-correlation between SFR and metallicity followed by the set of star-forming regions of any typical galaxy. The correspondence between local and global laws is not specific of the FMR, so that a number of local relations should exist associated with known global relations., Comment: Accepted for publication in ApJL. 6 pages and 3 figures

Published
2019
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38. Stellar content, planetary nebulae, and globular clusters of [KKS2000]04 (NGC1052-DF2)

Author

Ruiz-Lara, T., Trujillo, I., Beasley, M. A., Falcón-Barroso, J., Vazdekis, A., Filho, M., Monelli, M., Román, J., and Almeida, J. Sánchez

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

[KKS2000]04 (NGC1052-DF2) has become a controversial and well-studied galaxy after the claims suggesting a lack of dark matter and the presence of an anomalously bright globular cluster (GC) system around it. A precise determination of its overall star formation history (SFH) as well as a better characterisation of its GC or planetary nebulae (PN) systems are crucial aspects to: i) understand its real nature, in particular placing it within the family of ultra diffuse galaxies; ii) shed light on its possible formation, evolution, and survival in the absence of dark matter. With this purpose we expand on the knowledge of [KKS2000]04 from the analysis of OSIRIS@GTC spectroscopic data. On the one hand, we claim the possible detection of two new PNe and confirm membership of 5 GCs. On the other hand, we find that the stars shaping [KKS2000]04 are intermediate-age to old (90\% of its stellar mass older than 5 Gyr, average age of 8.7 $\pm$ 0.7 Gyr) and metal-poor ([M/H] $\sim$ -1.18 $\pm$ 0.05), in general agreement with previous results. We do not find any clear hints of significant changes in its stellar content with radius. In addition, the possibility of [KKS2000]04 being a tidal dwarf galaxy with no dark matter is highly disfavoured., Comment: 10 pages, 4 figures, accepted for publication in MNRAS

Published
2019
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43. Design and Performance of Combined Basic Devices to Control Undesirable Bridge Deck Displacements and Damage, During Major Earthquakes

Author

Romo, M., Morales, E., Hidalgo, G., Almeida, J., Puebla, R., O’Connor, J., Angrisani, Leopoldo, Series Editor, Arteaga, Marco, Series Editor, Panigrahi, Bijaya Ketan, Series Editor, Chakraborty, Samarjit, Series Editor, Chen, Jiming, Series Editor, Chen, Shanben, Series Editor, Chen, Tan Kay, Series Editor, Dillmann, Rüdiger, Series Editor, Duan, Haibin, Series Editor, Ferrari, Gianluigi, Series Editor, Ferre, Manuel, Series Editor, Hirche, Sandra, Series Editor, Jabbari, Faryar, Series Editor, Jia, Limin, Series Editor, Kacprzyk, Janusz, Series Editor, Khamis, Alaa, Series Editor, Kroeger, Torsten, Series Editor, Li, Yong, Series Editor, Liang, Qilian, Series Editor, Martín, Ferran, Series Editor, Ming, Tan Cher, Series Editor, Minker, Wolfgang, Series Editor, Misra, Pradeep, Series Editor, Möller, Sebastian, Series Editor, Mukhopadhyay, Subhas, Series Editor, Ning, Cun-Zheng, Series Editor, Nishida, Toyoaki, Series Editor, Oneto, Luca, Series Editor, Pascucci, Federica, Series Editor, Qin, Yong, Series Editor, Seng, Gan Woon, Series Editor, Speidel, Joachim, Series Editor, Veiga, Germano, Series Editor, Wu, Haitao, Series Editor, Zamboni, Walter, Series Editor, Zhang, Junjie James, Series Editor, Botto-Tobar, Miguel, editor, Cruz, Henry, editor, and Diaz Cadena, Angela, editor

Published
2022
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44. The ADMORPH Approach for Adaptively Morphing Embedded Systems

Author

Pimentel, A., primary, Grelck, C., additional, Miedema, L., additional, Sapra, D., additional, Völp, M., additional, Lucchetti, F., additional, Matovic, A., additional, Maggio, M., additional, Vreman, N., additional, Altmeyer, S., additional, Haas, F., additional, Casimiro, A., additional, Cecílio, J., additional, Jäger, G., additional, Espindola, A., additional, Skalistis, S., additional, Kouwer, J., additional, Lange, G. de, additional, Almeida, J., additional, Blasum, H., additional, Brotz, M., additional, Wagner, S., additional, and Novobílský, P., additional

Published
2024
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47. A headless tadpole galaxy: the high gas-phase metallicity of the ultra-diffuse galaxy UGC 2162

Author

Almeida, J. Sanchez, Olmo-Garcia, A., Elmegreen, B. G., Elmegreen, D. M., Filho, M., Munoz-Tunon, C., Perez-Montero, E., and Roman, J.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The cosmological numerical simulations tell us that accretion of external metal-poor gas drives star-formation (SF) in galaxy disks. One the best pieces of observational evidence supporting this prediction is the existence of low metallicity star-forming regions in relatively high metallicity host galaxies. The SF is thought to be fed by metal-poor gas recently accreted. Since the gas accretion is stochastic, there should be galaxies with all the properties of a host but without the low metallicity starburst. These galaxies have not been identified yet. The exception may be UGC 2162, a nearby ultra-diffuse galaxy (UDG) which combines low surface brightness and relatively high metallicity. We confirm the high metallicity of UGC 2162 (12 + log(O/H) = 8.52+0.27-0.24 ) using spectra taken with the 10-m GTC telescope. GC2162 has the stellar mass, metallicity, and star-formation rate (SFR) surface density expected for a host galaxy in between outbursts. This fact suggests a physical connection between some UDGs and metal-poor galaxies, which may be the same type of object in a different phase of the SF cycle. UGC 2162 is a high-metallicity outlier of the mass-metallicity relation, a property shared by the few UDGs with known gas-phase metallicity., Comment: Accepted for publication in ApJ. 10 pages. 5 figures

Published
2018
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48. Smooth and compactly supported viscous sub-cell shock capturing for Discontinuous Galerkin methods

Author

Glaubitz, J., Nogueira Jr., A. C., Almeida, J. L. S., Cantão, R. F., and Silva, C. A. C.

Subjects
Mathematics - Numerical Analysis, 35L65, 65N30, 65N35, 35L67, 35D40
Abstract

In this work, a novel artificial viscosity method is proposed using smooth and compactly supported viscosities. These are derived by revisiting the widely used piecewise constant artificial viscosity method of Persson and Peraire as well as the piecewise linear refinement of Kl\"ockner et al. with respect to the fundamental design criteria of conservation and entropy stability. Further investigating the method of modal filtering in the process, it is demonstrated that this strategy has inherent shortcomings, which are related to problems of Legendre viscosities to handle shocks near element boundaries. This problem is overcome by introducing certain functions from the fields of robust reprojection and mollififers as viscosity distributions. To the best of our knowledge, this is proposed for the first time in this work. The resulting $C_0^\infty$ artificial viscosity method is demonstrated to provide sharper profiles, steeper gradients and a higher resolution of small-scale features while still maintaining stability of the method., Comment: 21 pages, accepted for publication in Journal of Scientific Computing

Published
2018
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49. Optoelectronic properties of zinc oxide: A first-principles investigation using the Tran-Blaha modified Becke-Johnson potentia

Author

Almeida, R. M. V. S., da Rosa, A. L., and de Almeida, J. S.

Subjects
Condensed Matter - Materials Science
Abstract

In this work we use density functional theory (DFT) to investigate the influence of semi-local exchange and correlation effects on the electronic and optical properties of zinc oxide. We find that the inclusion of such effects using the Tran-Blaha modified Becke-Johnson potential yields an excellent description of the electronic structure of this material giving energy band gap which is systematically larger than the one obtained with standard local functionals such as the generalized gradient approximation. The discrepancy between the experimental and theoretical band gaps is then significantly reduced at a computational low cost. We also calculated the dielectric functions of ZnO and find a violet shift to the absorption edge which is in good agreement with experimental results., Comment: 12 pages, 2 figures

Published
2018
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50. An Unusual Transient in the Extremely Metal-Poor Galaxy SDSS J094332.35+332657.6 (Leoncino Dwarf)

Author

Filho, Mercedes E. and Almeida, J. Sánchez

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We have serendipitously discovered that Leoncino Dwarf, an ultra-faint, low-metallicity record-holder dwarf galaxy, may have hosted a transient source, and possibly exhibited a change in morphology, a shift in the center of brightness, and peak variability of the main (host) source in images taken approximately 40 yr apart; it is highly likely that these phenomena are related. Scenarios involving a Solar System object, a stellar cluster, dust enshrouding, and accretion variability have been considered, and discarded, as the origin of the transient. Although a combination of time-varying strong and weak lensing effects, induced by an intermediate mass black hole (10$^4$ - 5 $\times$ 10$^{5}$ M$_{\odot}$) moving within the Milky Way halo (0.1 -- 4 kpc), can conceivably explain all of the observed variable galaxy properties, it is statistically highly unlikely according to current theoretical predictions, and, therefore, also discarded. A cataclysmic event such as a supernova/hypernova could have occurred, as long as the event was observed towards the later/late-stage descent of the light curve, but this scenario fails to explain the absence of a post-explosion source and/or host HII region in recent optical images. An episode related to the giant eruption of a luminous blue variable star, a stellar merger or a nova, observed at, or near, peak magnitude may explain the transient source and possibly the change in morphology/center of brightness, but can not justify the main source peak variability, unless stellar variability is evoked.

Published
2018
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