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52. Association between common cardiovascular risk factors and clinical phenotype in patients with hypertrophic cardiomyopathy from the European Society of Cardiology (ESC) EurObservational Research Programme (EORP) Cardiomyopathy/Myocarditis registry

Author

Lopes, Luis R, Losi, Maria-Angela, Sheikh, Nabeel, Laroche, Cécile, Charron, Philippe, Gimeno, Juan, Kaski, Juan P, Maggioni, Aldo P, Tavazzi, Luigi, Arbustini, Eloisa, Brito, Dulce, Celutkiene, Jelena, Hagege, Albert, Linhart, Ales, Mogensen, Jens, Garcia-Pinilla, José Manuel, Ripoll-Vera, Tomas, Seggewiss, Hubert, Villacorta, Eduardo, Caforio, Alida, Elliott, Perry M, Komissarova, S, Chakova, N, Niyazova, S, Linhart, A, Kuchynka, P, Palecek, T, Podzimkova, J, Fikrle, M, Nemecek, E, Bundgaard, H, Tfelt-Hansen, J, Theilade, J, Thune, J J, Axelsson, A, Mogensen, J, Henriksen, F, Hey, T, Nielsen, S K, Videbaek, L, Andreasen, S, Arnsted, H, Saad, A, Ali, M, Lommi, J, Helio, T, Nieminen, M S, Dubourg, O, Mansencal, N, Arslan, M, Tsieu, V Siam, Damy, T, Guellich, A, Guendouz, S, Tissot, C M, Lamine, A, Rappeneau, S, Hagege, A, Desnos, M, Bachet, A, Hamzaoui, M, Charron, P, Isnard, R, Legrand, L, Maupain, C, Gandjbakhch, E, Kerneis, M, Pruny, J-F, Bauer, A, Pfeiffer, B, Felix, S B, Dorr, M, Kaczmarek, S, Lehnert, K, Pedersen, A-L, Beug, D, Bruder, M, Böhm, M, Kindermann, I, Linicus, Y, Werner, C, Neurath, B, Schild-Ungerbuehler, M, Seggewiss, H, Neugebauer, A, Mckeown, P, Muir, A, Mcosker, J, Jardine, T, Divine, G, Elliott, P, Lorenzini, M, Watkinson, O, Wicks, E, Iqbal, H, Mohiddin, S, O'Mahony, C, Sekri, N, Carr-White, G, Bueser, T, Rajani, R, Clack, L, Damm, J, Jones, S, Sanchez-Vidal, R, Smith, M, Walters, T, Wilson, K, Rosmini, S, Anastasakis, A, Ritsatos, K, Vlagkouli, V, Forster, T, Sepp, R, Borbas, J, Nagy, V, Tringer, A, Kakonyi, K, Szabo, L A, Maleki, M, Bezanjani, F Noohi, Amin, A, Naderi, N, Parsaee, M, Taghavi, S, Ghadrdoost, B, Jafari, S, Khoshavi, M, Rapezzi, C, Biagini, E, Corsini, A, Gagliardi, C, Graziosi, M, Longhi, S, Milandri, A, Ragni, L, Palmieri, S, Olivotto, I, Arretini, A, Castelli, G, Cecchi, F, Fornaro, A, Tomberli, B, Spirito, P, Devoto, E, Bella, P Della, Maccabelli, G, Sala, S, Guarracini, F, Peretto, G, Russo, M G, Calabro, R, Pacileo, G, Limongelli, G, Masarone, D, Pazzanese, V, Rea, A, Rubino, M, Tramonte, S, Valente, F, Caiazza, M, Cirillo, A, Del Giorno, G, Esposito, A, Gravino, R, Marrazzo, T, Trimarco, B, Losi, M-A, Nardo, C Di, Giamundo, A, Musella, F, Pacelli, F, Scatteia, A, Canciello, G, Caforio, A, Iliceto, S, Calore, C, Leoni, L, Marra, M Perazzolo, Rigato, I, Tarantini, G, Schiavo, A, Testolina, M, Arbustini, E, Toro, A Di, Giuliani, L P, Serio, A, Fedele, F, Frustaci, A, Alfarano, M, Chimenti, C, Drago, F, Baban, A, Calò, L, Lanzillo, C, Martino, A, Uguccioni, M, Zachara, E, Halasz, G, Re, F, Sinagra, G, Carriere, C, Merlo, M, Ramani, F, Kavoliuniene, A, Krivickiene, A, Tamuleviciute-Prasciene, E, Viezelis, M, Celutkiene, J, Balkeviciene, L, Laukyte, M, Paleviciute, E, Pinto, Y, Wilde, A, Asselbergs, F W, Sammani, A, Van Der Heijden, J, Van Laake, L, De Jonge, N, Hassink, R, Kirkels, J H, Ajuluchukwu, J, Olusegun-Joseph, A, Ekure, E, Mizia-Stec, K, Tendera, M, Czekaj, A, Sikora-Puz, A, Skoczynska, A, Wybraniec, M, Rubis, P, Dziewiecka, E, Wisniowska-Smialek, S, Bilinska, Z, Chmielewski, P, Nieradko, B Foss, Michalak, E, Stepien-Wojno, M, Mazek, B, Lopes, L Rocha, Almeida, A R, Cruz, I, Gomes, A C, Pereira, A R, Brito, D, Madeira, H, Francisco, A R, Menezes, M, Moldovan, O, Guimaraes, T Oliveira, Silva, D, Ginghina, C, Jurcut, R, Mursa, A, Popescu, B A, Apetrei, E, Militaru, S, Coman, I Mircea, Frigy, A, Fogarasi, Z, Kocsis, I, Szabo, I A, Fehervari, L, Nikitin, I, Resnik, E, Komissarova, M, Lazarev, V, Shebzukhova, M, Ustyuzhanin, D, Blagova, O, Alieva, I, Kulikova, V, Lutokhina, Y, Pavlenko, E, Varionchik, N, Ristic, A D, Seferovic, P M, Veljic, I, Zivkovic, I, Milinkovic, I, Pavlovic, A, Radovanovic, G, Simeunovic, D, Zdravkovic, M, Aleksic, M, Djokic, J, Hinic, S, Klasnja, S, Mircetic, K, Monserrat, L, Fernandez, X, Garcia-Giustiniani, D, Larrañaga, J M, Ortiz-Genga, M, Barriales-Villa, R, Martinez-Veira, C, Veira, E, Cequier, A, Salazar-Mendiguchia, J, Manito, N, Gonzalez, J, Fernández-Avilés, F, Medrano, C, Yotti, R, Cuenca, S, Espinosa, M A, Mendez, I, Zatarain, E, Alvarez, R, Pavia, P Garcia, Briceno, A, Cobo-Marcos, M, Dominguez, F, Galvan, E De Teresa, Pinilla, J M García, Abdeselam-Mohamed, N, Lopez-Garrido, M A, Hidalgo, L Morcillo, Ortega-Jimenez, M V, Mezcua, A Robles, Guijarro-Contreras, A, Gomez-Garcia, D, Robles-Mezcua, M, Blanes, J R Gimeno, Castro, F J, Esparza, C Munoz, Molina, M Sabater, García, M Sorli, Cuenca, D Lopez, Ripoll-Vera, T, Alvarez, J, Nunez, J, Gomez, Y, Fernandez, P L Sanchez, Villacorta, E, Avila, C, Bravo, L, Diaz-Pelaez, E, Gallego-Delgado, M, Garcia-Cuenllas, L, Plata, B, Lopez-Haldon, J E, Pena Pena, M L, Perez, E M Cantero, Zorio, E, Arnau, M A, Sanz, J, Marques-Sule, E, Gale, Christopher Peter, Beleslin, Branko, Budaj, Andrzej, Chioncel, Ovidiu, Dagres, Nikolaos, Danchin, Nicolas, Erlinge, David, Emberson, Jonathan, Glikson, Michael, Gray, Alastair, Kayikcioglu, Meral, Maggioni, Aldo, Nagy, Klaudia Vivien, Nedoshivin, Aleksandr, Petronio, Anna-Sonia, Hesselink, Jolien Roo, Wallentin, Lars, Zeymer, Uwe, Caforio, Alida, Blanes, Juan Ramon Gimeno, Charron, Philippe, Elliott, Perry, Kaski, Juan Pablo, Maggioni, Aldo P, Tavazzi, Luigi, Tendera, Michal, Komissarova, S., Chakova, N., Niyazova, S., Linhart, A., Kuchynka, P., Palecek, T., Podzimkova, J., Fikrle, M., Nemecek, E., Bundgaard, H., Tfelt-Hansen, J., Theilade, J., Thune, J J, Axelsson, A., Mogensen, J., Henriksen, F., Hey, T., Nielsen, S K, Videbaek, L., Andreasen, S., Arnsted, H., Saad, A., Ali, M., Lommi, J., Helio, T., Nieminen, M S, Dubourg, O., Mansencal, N., Arslan, M., Tsieu, V Siam, Damy, T., Guellich, A., Guendouz, S., Tissot, C M, Lamine, A., Rappeneau, S., Hagege, A., Desnos, M., Bachet, A., Hamzaoui, M., Charron, P., Isnard, R., Legrand, L., Maupain, C., Gandjbakhch, E., Kerneis, M., Pruny, J-F, Bauer, A., Pfeiffer, B., Felix, S B, Dorr, M., Kaczmarek, S., Lehnert, K., Pedersen, A-L, Beug, D., Bruder, M., Böhm, M., Kindermann, I., Linicus, Y., Werner, C., Neurath, B., Schild-Ungerbuehler, M., Seggewiss, H., Neugebauer, A., McKeown, P., Muir, A., McOsker, J., Jardine, T., Divine, G., Elliott, P., Lorenzini, M., Watkinson, O., Wicks, E., Iqbal, H., Mohiddin, S., O'Mahony, C., Sekri, N., Carr-White, G., Bueser, T., Rajani, R., Clack, L., Damm, J., Jones, S., Sanchez-Vidal, R., Smith, M., Walters, T., Wilson, K., Rosmini, S., Anastasakis, A., Ritsatos, K., Vlagkouli, V., Forster, T., Sepp, R., Borbas, J., Nagy, V., Tringer, A., Kakonyi, K., Szabo, L A, Maleki, M., Bezanjani, F Noohi, Amin, A., Naderi, N., Parsaee, M., Taghavi, S., Ghadrdoost, B., Jafari, S., Khoshavi, M., Rapezzi, C., Biagini, E., Corsini, A., Gagliardi, C., Graziosi, M., Longhi, S., Milandri, A., Ragni, L., Palmieri, S., Olivotto, I., Arretini, A., Castelli, G., Cecchi, F., Fornaro, A., Tomberli, B., Spirito, P., Devoto, E., Bella, P Della, Maccabelli, G., Sala, S., Guarracini, F., Peretto, G., Russo, M G, Calabro, R., Pacileo, G., Limongelli, G., Masarone, D., Pazzanese, V., Rea, A., Rubino, M., Tramonte, S., Valente, F., Caiazza, M., Cirillo, A., Del Giorno, G., Esposito, A., Gravino, R., Marrazzo, T., Trimarco, B., Losi, M-A, Di Nardo, C., Giamundo, A., Musella, F., Pacelli, F., Scatteia, A., Canciello, G., Caforio, A., Iliceto, S., Calore, C., Leoni, L., Marra, M Perazzolo, Rigato, I., Tarantini, G., Schiavo, A., Testolina, M., Arbustini, E., Di Toro, A., Giuliani, L P, Serio, A., Fedele, F., Frustaci, A., Alfarano, M., Chimenti, C., Drago, F., Baban, A., Calò, L., Lanzillo, C., Martino, A., Uguccioni, M., Zachara, E., Halasz, G., Re, F., Sinagra, G., Carriere, C., Merlo, M., Ramani, F., Kavoliūnienė, Aušra, Krivickienė, Aušra, Tamulevičiūtė-Prascienė, Eglė, Vieželis, Mindaugas, Balkevičienė, Laura, Laukytė, M., Palevičiūtė, Eglė, Pinto, Y., Wilde, A., Asselbergs, F W, Sammani, A., Van Der Heijden, J., Van Laake, L., De Jonge, N., Hassink, R., Kirkels, J H, Ajuluchukwu, J., Olusegun-Joseph, A., Ekure, E., Mizia-Stec, K., Tendera, M., Czekaj, A., Sikora-Puz, A., Skoczynska, A., Wybraniec, M., Rubis, P., Dziewiecka, E., Wisniowska-Smialek, S., Bilinska, Z., Chmielewski, P., Foss-Nieradko, B., Michalak, E., Stepien-Wojno, M., Mazek, B., Lopes, L Rocha, Almeida, A R, Cruz, I., Gomes, A C, Pereira, A R, Brito, D., Madeira, H., Francisco, A R, Menezes, M., Moldovan, O., Guimaraes, T Oliveira, Silva, D., Ginghina, C., Jurcut, R., Mursa, A., Popescu, B A, Apetrei, E., Militaru, S., Coman, I Mircea, Frigy, A., Fogarasi, Z., Kocsis, I., Szabo, I A, Fehervari, L., Nikitin, I., Resnik, E., Komissarova, M., Lazarev, V., Shebzukhova, M., Ustyuzhanin, D., Blagova, O., Alieva, I., Kulikova, V., Lutokhina, Y., Pavlenko, E., Varionchik, N., Ristic, A D, Seferovic, P M, Veljic, I., Zivkovic, I., Milinkovic, I., Pavlovic, A., Radovanovic, G., Simeunovic, D., Zdravkovic, M., Aleksic, M., Djokic, J., Hinic, S., Klasnja, S., Mircetic, K., Monserrat, L., Fernandez, X., Garcia-Giustiniani, D., Larrañaga, J M, Ortiz-Genga, M., Barriales-Villa, R., Martinez-Veira, C., Veira, E., Cequier, A., Salazar-Mendiguchia, J., Manito, N., Gonzalez, J., Fernández-Avilés, F., Medrano, C., Yotti, R., Cuenca, S., Espinosa, M A, Mendez, I., Zatarain, E., Alvarez, R., Pavia, P Garcia, Briceno, A., Cobo-Marcos, M., Dominguez, F., Galvan, E De Teresa, Pinilla, J M García, Abdeselam-Mohamed, N., Lopez-Garrido, M A, Hidalgo, L Morcillo, Ortega-Jimenez, M V, Mezcua, A Robles, Guijarro-Contreras, A., Gomez-Garcia, D., Robles-Mezcua, M., Blanes, J R Gimeno, Castro, F J, Esparza, C Munoz, Molina, M Sabater, García, M Sorli, Cuenca, D Lopez, de Mallorca, Palma, Ripoll-Vera, T., Alvarez, J., Nunez, J., Gomez, Y., Fernandez, P L Sanchez, Villacorta, E., Avila, C., Bravo, L., Diaz-Pelaez, E., Gallego-Delgado, M., Garcia-Cuenllas, L., Plata, B., Lopez-Haldon, J E, Pena Pena, M L, Perez, E M Cantero, Zorio, E., Arnau, M A, Sanz, J., Marques-Sule, E., Repositório da Universidade de Lisboa, Lopes, Lr, Losi, Ma, Sheikh, N, Laroche, C, Charron, P, Gimeno, J, Kaski, Jp, Maggioni, Ap, Tavazzi, L, Arbustini, E, Brito, D, Celutkiene, J, Hagege, A, Linhart, A, Mogensen, J, Garcia-Pinilla, Jm, Ripoll-Vera, T, Seggewiss, H, Villacorta, E, Caforio, A, and Elliott, Pm

Subjects
Genotype, Health Policy, Diabetes, Cardiovascular risk factors, Hypertension, Hypertrophic cardiomyopathy, Obesity, Cardiomyopathy, Hypertrophic, Ventricular Dysfunction, Left, diabete, Cardiovascular Diseases, Risk Factors, Heart Disease Risk Factors, cardiovascular risk factor, Humans, Female, 03.02. Klinikai orvostan, Cardiology and Cardiovascular Medicine, Cardiomyopathies, obesity
Abstract

© The Author(s) 2022. Published by Oxford University Press on behalf of the European Society of Cardiology. This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., Aims: The interaction between common cardiovascular risk factors (CVRF) and hypertrophic cardiomyopathy (HCM) is poorly studied. We sought to explore the relation between CVRF and the clinical characteristics of patients with HCM enrolled in the EURObservational Research Programme (EORP) Cardiomyopathy registry. Methods and results: 1739 patients with HCM were studied. The relation between hypertension (HT), diabetes (DM), body mass index (BMI) and clinical traits was analyzed. Analyses were stratified according to the presence or absence of a pathogenic variant in a sarcomere gene.The prevalence of HT, DM and obesity (Ob) was 37%, 10%, and 21%, respectively. HT, DM and Ob were associated with older age (p

Published
2022

55. Evidence of Runaway Gas Cooling in the Absence of Supermassive Black Hole Feedback at the Epoch of Cluster Formation

Author

MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Hlavacek-Larrondo, J, Rhea, CL, Webb, T, McDonald, Michael A., Muzzin, A, Wilson, G, Finner, K, Valin, F, Bonaventura, N, Cooper, M, Fabian, AC, Gendron-Marsolais, ML, Jee, MJ, Lidman, C, Mezcua, M, Noble, A, Russell, HR, Surace, J, Trudeau, A, Yee, HKC, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Hlavacek-Larrondo, J, Rhea, CL, Webb, T, McDonald, Michael A., Muzzin, A, Wilson, G, Finner, K, Valin, F, Bonaventura, N, Cooper, M, Fabian, AC, Gendron-Marsolais, ML, Jee, MJ, Lidman, C, Mezcua, M, Noble, A, Russell, HR, Surace, J, Trudeau, A, and Yee, HKC

Abstract

© 2020. The American Astronomical Society. All rights reserved.. Cosmological simulations, as well as mounting evidence from observations, have shown that supermassive black holes play a fundamental role in regulating the formation of stars throughout cosmic time. This has been clearly demonstrated in the case of galaxy clusters in which powerful feedback from the central black hole is preventing the hot intracluster gas from cooling catastrophically, thus reducing the expected star formation rates by orders of magnitude. These conclusions, however, have been almost entirely based on nearby clusters. Based on new Chandra X-ray observations, we present the first observational evidence for massive, runaway cooling occurring in the absence of supermassive black hole feedback in the high-redshift galaxy cluster SpARCS104922.6 + 564032.5 (z = 1.709). The hot intracluster gas appears to be fueling a massive burst of star formation (≈900 M o˙ yr-1) that is offset by dozens of kpc from the central galaxy. The burst is co-spatial with the coolest intracluster gas but not associated with any galaxy in the cluster. In less than 100 million years, such runaway cooling can form the same amount of stars as in the Milky Way. Therefore, intracluster stars are not only produced by tidal stripping and the disruption of cluster galaxies, but can also be produced by runaway cooling of hot intracluster gas at early times. Overall, these observations show the dramatic impact when supermassive black hole feedback fails to operate in clusters. They indicate that in the highest overdensities, such as clusters and protoclusters, runaway cooling may be a new and important mechanism for fueling massive bursts of star formation in the early universe.

Published
2022

62. Evidence of Runaway Gas Cooling in the Absence of Supermassive Black Hole Feedback at the Epoch of Cluster Formation

Author

Hlavacek-Larrondo, J, Rhea, CL, Webb, T, McDonald, M, Muzzin, A, Wilson, G, Finner, K, Valin, F, Bonaventura, N, Cooper, M, Fabian, AC, Gendron-Marsolais, ML, Jee, MJ, Lidman, C, Mezcua, M, Noble, A, Russell, HR, Surace, J, Trudeau, A, Yee, HKC, Hlavacek-Larrondo, J, Rhea, CL, Webb, T, McDonald, M, Muzzin, A, Wilson, G, Finner, K, Valin, F, Bonaventura, N, Cooper, M, Fabian, AC, Gendron-Marsolais, ML, Jee, MJ, Lidman, C, Mezcua, M, Noble, A, Russell, HR, Surace, J, Trudeau, A, and Yee, HKC

Abstract

© 2020. The American Astronomical Society. All rights reserved.. Cosmological simulations, as well as mounting evidence from observations, have shown that supermassive black holes play a fundamental role in regulating the formation of stars throughout cosmic time. This has been clearly demonstrated in the case of galaxy clusters in which powerful feedback from the central black hole is preventing the hot intracluster gas from cooling catastrophically, thus reducing the expected star formation rates by orders of magnitude. These conclusions, however, have been almost entirely based on nearby clusters. Based on new Chandra X-ray observations, we present the first observational evidence for massive, runaway cooling occurring in the absence of supermassive black hole feedback in the high-redshift galaxy cluster SpARCS104922.6 + 564032.5 (z = 1.709). The hot intracluster gas appears to be fueling a massive burst of star formation (≈900 M o˙ yr-1) that is offset by dozens of kpc from the central galaxy. The burst is co-spatial with the coolest intracluster gas but not associated with any galaxy in the cluster. In less than 100 million years, such runaway cooling can form the same amount of stars as in the Milky Way. Therefore, intracluster stars are not only produced by tidal stripping and the disruption of cluster galaxies, but can also be produced by runaway cooling of hot intracluster gas at early times. Overall, these observations show the dramatic impact when supermassive black hole feedback fails to operate in clusters. They indicate that in the highest overdensities, such as clusters and protoclusters, runaway cooling may be a new and important mechanism for fueling massive bursts of star formation in the early universe.

Published
2021

69. Contributors

Author

Can Başer, K. Hüsnü, primary, Blumberg, Leonid M., additional, Caruso, Joseph A., additional, Chan, Qilin, additional, Yong Chan, Eric Chun, additional, Cruz-Hernandez, Cristina, additional, Dawes, Peter, additional, Dejaegher, Bieke, additional, Destaillats, Frédéric, additional, Dorman, Frank L., additional, Ebeler, Susan E., additional, Fernandez-alba, Amadeo R., additional, Héberger, Károly, additional, Heyden, Yvan Vander, additional, Jennings, Walter G., additional, Kim, Leesun, additional, Klee, Matthew S., additional, Mal, Mainak, additional, Marriott, Philip J, additional, Martinez-Uroz, Angeles, additional, Mezcua, M Milagros, additional, Millar, Jocelyn G., additional, Nadeau, Jeremy S., additional, Özek, Temel, additional, Pasikanti, Kishore Kumar, additional, Pierce, Karisa M., additional, Pietrogrande, Maria Chiara, additional, Poole, Colin F., additional, Reiner, Eric J., additional, Schurig, Volker, additional, Seeley, John V., additional, Sithersingh, Michael J., additional, Smeyers-Verbeke, Johanna, additional, Smith, Philip A., additional, Snow, Nicholas H., additional, Stearns, Stanley D., additional, Synovec, Robert E., additional, Tipler, Andrew, additional, Voelkel, Adam, additional, Wampler, Thomas P., additional, Wawrzyniak, Rafał, additional, Wilkins, Charles L., additional, and Woolfenden, Elizabeth, additional

Published
2012
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74. Glimmering in the Dark: Modeling the Low-mass End of the M ∙-σ Relation and of the Quasar Luminosity Function

Author

Pacucci, F., Loeb, A., Mezcua, M., and Martín-Navarro, I.

Abstract

The {M}\bullet {--}σ relation establishes a connection between central black holes (BHs) and their host spheroids. Supported by observations at {M}\bullet ≳ {10}5 {M}☉ , there is limited data on its validity at lower masses. Employing a semi-analytical model to simulate the combined evolution of BHs and their host galaxies, we predict the observational consequences of assuming a bimodality in the accretion efficiency of BHs, with low-mass BHs ({M}\bullet ≲ {10}5 {M}☉ ) accreting inefficiently. We predict a departure from the {M}\bullet {--}σ relation at a transitional BH mass ̃ {10}5 {M}☉ , with lower-mass BHs unable to reach the mass dictated by the relation and becoming disconnected from the evolution of the host galaxy. This prediction is an alternative to previous works suggesting a flattening of the relation at ̃ {10}5{--}{10}6 {M}☉ . Furthermore, we predict a deficit of BHs shining at bolometric luminosities ̃ {10}42 {erg} {{{s}}}-1. Joined with a detection bias, this could partly explain the scarce number of intermediate-mass BHs detected. Conversely, we predict an increase in source density at lower bolometric luminosities, < {10}42 {erg} {{{s}}}-1. Because our predictions assume a bimodal population of high-redshift BH seeds, future observations of fainter BHs will be fundamental for constraining the nature of these seeds.

Published
2018

76. $\textit{Chandra}$ X-ray observations of the hyper-luminous infrared galaxy IRAS F15307+3252

Author

Hlavacek-Larrondo, J, Gandhi, P, Hogan, MT, Gendron-Marsolais, M-L, Edge, AC, Fabian, AC, Russell, HR, Iwasawa, K, Mezcua, M, Fabian, Andrew [0000-0002-9378-4072], and Apollo - University of Cambridge Repository

Subjects
X-rays: individual: IRAS F15307+3252, galaxies: high-redshift, Astrophysics::High Energy Astrophysical Phenomena, X-rays: galaxies: clusters, black hole physics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, infrared: galaxies
Abstract

Hyper-luminous infrared galaxies (HyLIRGs) lie at the extreme luminosity end of the IR galaxy population with $L_{IR}$ > 10$^{13}$ L$_\odot$. They are thought to be closer counterparts of the more distant sub-millimeter galaxies, and should therefore be optimal targets to study the most massive systems in formation. We present deep $\textit{Chandra}$ observations of IRAS F15307+3252 (100 ks), a classical HyLIRG located at $z$=0.93 and hosting a radio-loud AGN ($L_{1.4 GHz}$ ~3.5 × 10$^{25}$ W Hz$^{−1}$). The $\textit{Chandra}$ images reveal the presence of extended ($r$ = 160 kpc), asymmetric X-ray emission in the soft 0.3–2.0 keV band that has no radio counterpart. We therefore argue that the emission is of thermal origin originating from a hot intragroup or intracluster medium virializing in the potential. We find that the temperature (~2 keV) and bolometric X-ray luminosity (~3 × 10$^{43}$ erg s$^{−1}$) of the gas follow the expected $L_{X-ray}$–$T$ correlation for groups and clusters, and that the gas has a remarkably short cooling time of 1.2 Gyr. In addition, VLA radio observations reveal that the galaxy hosts an unresolved compact steep-spectrum (CSS) source, most likely indicating the presence of a young radio source similar to 3C186. We also confirm that the nucleus is dominated by a redshifted 6.4 keV Fe K$\alpha$ line, strongly suggesting that the AGN is Compton-thick. Finally, $\textit{Hubble}$ images reveal an overdensity of galaxies and sub-structure in the galaxy that correlates with soft X-ray emission. This could be a snapshot view of on-going groupings expected in a growing cluster environment. IRAS F15307+3252 might therefore be a rare example of a group in the process of transforming into a cluster.

Published
2017
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80. Mystery solved: discovery of extended radio emission in the merging galaxy cluster Abell 2146

Author

Hlavacek-Larrondo, J, primary, Gendron-Marsolais, M-L, additional, Fecteau-Beaucage, D, additional, van Weeren, R J, additional, Russell, H R, additional, Edge, A, additional, Olamaie, M, additional, Rumsey, C, additional, King, L, additional, Fabian, A C, additional, McNamara, B, additional, Hogan, M, additional, Mezcua, M, additional, and Taylor, G, additional

Published
2017
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82. ULX behaviour: the ultraluminous state, winds and interesting anomalies

Author

Roberts, T. P., Middleton, M. J., Sutton, A. D., Mezcua, M., Walton, D. J., Heil, L. M., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Recent evidence - in particular the hard X-ray spectra obtained by {NuSTAR}, and the large amplitude hard X-ray variability observed when ULXs show soft spectra - reveals that common ultraluminous X-ray source (ULX) behaviour is inconsistent with known sub-Eddington accretion modes, as would be expected for an intermediate-mass black hole (IMBH). Instead, it appears that the majority of ULXs are powered by super-Eddington accretion onto stellar-mass black holes. Here, we will review work that delves deeper into ULX spectral-timing behaviour, demonstrating it remains consistent with the expectations of super-Eddington accretion. One critical missing piece from this picture is the direct detection of the massive, radiatively-driven winds expected from ULXs as atomic emission/absorption line features in ULX spectra; we will show it is very likely these have already been detected as residuals in the soft X-ray spectra of ULXs. Finally, we will discuss ULXs that do not appear to conform to the emerging ULX behaviour patterns. In particular we discuss the implications of the identification of a good IMBH candidate as a background QSO; and the confirmation of an IMBH/ULX candidate in the galaxy NGC 2276 via the radio/X-ray fundamental plane.

Published
2015

83. Very Long Baseline Interferometry with the SKA

Author

Paragi, Z., Godfrey, L., Reynolds, C., Rioja, M. J., Deller, A., Zhang, B., Gurvits, L., Bietenholz, M., Szomoru, A., Bignall, H. E., Boven, P., Charlot, P., Dodson, R., Frey, S., Garrett, M. A., Imai, H., Lobanov, A., Reid, M. J., Ros, E., van Langevelde, H. J., Zensus, A. J., Zheng, X. W., Alberdi, A., Agudo, I., An, T., Argo, M., Beswick, R., Biggs, A., Brunthaler, A., Campbell, B., Cimo, G., Colomer, F., Corbel, S., Conway, J. E., Cseh, D., Deane, R., Falcke, H. D. E., Gawronski, M., Gaylard, M., Giovannini, G., Giroletti, M., Goddi, C., Goedhart, S., Gómez, J. L., Gunn, A., Kharb, P., Kloeckner, H. R., Koerding, E., Kovalev, Y., Kunert-Bajraszewska, M., Lindqvist, M., Lister, M., Mantovani, F., Marti-Vidal, I., Mezcua, M., McKean, J., Middelberg, E., Miller-Jones, J. C. A., Moldon, J., Muxlow, T., O'Brien, T., Perez-Torres, M., Pogrebenko, S. V., Quick, J., Rushton, A., Schilizzi, R., Smirnov, O., Sohn, B. W., Surcis, G., Taylor, G. B., Tingay, S., Tudose, V. M., van der Horst, A., van Leeuwen, J., Venturi, T., Vermeulen, R., Vlemmings, W. H. T., de Witt, A., Wucknitz, O., Yang, J., Gabänyi, K., and Jung, T.

Abstract

Adding VLBI capability to the SKA arrays will greatly broaden the science of the SKA, and is feasible within the current specifications. SKA-VLBI can be initially implemented by providing phased-array outputs for SKA1-MID and SKA1-SUR and using these extremely sensitive stations with other radio telescopes, and in SKA2 by realising a distributed configuration providing baselines up to thousands of km, merging it with existing VLBI networks. The motivation for and the possible realization of SKA-VLBI is described in this paper.

Published
2015

88. Radio investigation of Ultra-Luminous X-ray Sources in the SKA Era

Author

Bourke, T.L., Wolter, A., Rushton, A.P., Mezcua, M., Cseh, D., Pintore, F., Prandoni, I., Paragi, Z., Zampieri, L., Bourke, T.L., Wolter, A., Rushton, A.P., Mezcua, M., Cseh, D., Pintore, F., Prandoni, I., Paragi, Z., and Zampieri, L.

Abstract

AASKA14 : Advancing Astrophysics with the Square Kilometre Array June 8-13, 2014 Giardini Naxos, Italy, Contains fulltext : 143822.pdf (publisher's version ) (Open Access)

Published
2015

89. Mystery solved: discovery of extended radio emission in the merging galaxy cluster Abell 2146.

Author

Hlavacek-Larrondo, J., Gendron-Marsolais, M.-L., Fecteau-Beaucage, D., van Weeren, R. J., Russell, H. R., Edge, A., Olamaie, M., Rumsey, C., King, L., Fabian, A. C., McNamara, B., Hogan, M., Mezcua, M., and Taylor, G.

Subjects
SOLAR radio emission, GALAXY clusters, GALAXY mergers, SHOCK waves, WAVELENGTH measurement, VERY large array telescopes
Abstract

Abell 2146 (z = 0.232) is a massive galaxy cluster currently undergoing a spectacular merger in the plane of the sky with a bullet-like morphology. It was the first system in which both the bow and upstream shock fronts were detected at X-ray wavelengths (Mach ~2), yet deep Giant MetreWave Telescope 325 MHz observations failed to detect extended radio emission associated with the cluster as is typically seen in such systems. We present new, multiconfiguration 1-2 GHz Karl G. Jansky Very Large Array (VLA) observations of Abell 2146 totalling 16 h of observations. These data reveal for the first time the presence of an extended (≈850 kpc), faint radio structure associated with Abell 2146. The structure appears to harbour multiple components, one associated with the upstream shock that we classify as a radio relic and one associated with the subcluster core that is consisted as being a radio halo bounded by the bow shock. The newly detected structures have some of the lowest radio powers detected thus far in any cluster (P1.4 GHz, halo = 2.4± 0.2 × 1023 W Hz-1 and P1.4 GHz, relic = 2.2 ± 0.2 × 1023 W Hz-1). The flux measurement of the halo, as well as its morphology, also suggests that the halo was recently created (≈0.3 Gyr after core passage), consistent with the dynamical state of the cluster. These observations demonstrate the capacity of the upgraded VLA to detect extremely faint and extended radio structures. Based on these observations, we predict that many more radio relics and radio haloes in merging clusters should be detected by future radio facilities such as the Square Kilometre Array. [ABSTRACT FROM AUTHOR]

Published
2018
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90. The most massive black holes on the Fundamental Plane of black hole accretion.

Author

Mezcua, M., Hlavacek-Larrondo, J., Lucey, J. R., Hogan, M. T., Edge, A. C., and McNamara, B. R.

Subjects
*BLACK holes, *OPEN clusters of stars, *GALAXIES, *ACCRETION (Astrophysics), *X-ray astronomy
Abstract

We perform a detailed study of the location of brightest cluster galaxies (BCGs) on the Fundamental Plane of black hole (BH) accretion, which is an empirical correlation between a BH X-ray and radio luminosity and mass supported by theoretical models of accretion. The sample comprises 72 BCGs out to z ~ 0.3 and with reliable nuclear X-ray and radio luminosities. These are found to correlate as LX ∝ L0.75±0.08 R, favouring an advection-dominated accretion flow as the origin of the X-ray emission. BCGs are found to be on average offset from the Fundamental Plane such that their BH masses seem to be underestimated by the MBH-MK relation a factor ~10. The offset is not explained by jet synchrotron cooling and is independent of emission process or amount of cluster gas cooling. Those core-dominated BCGs are found to be more significantly offset than those with weak core radio emission. For BCGs to on average follow the Fundamental Plane, a large fraction (~40 per cent) should have BH masses >1010M⊙ and thus host ultramassive BHs. The local BH-galaxy scaling relations would not hold for these extreme objects. The possible explanations for their formation, either via a two-phase process (the BH formed first, the galaxy grows later) or as descendants of high-z seed BHs, challenge the current paradigm of a synchronized galaxy-BH growth. [ABSTRACT FROM AUTHOR]

Published
2018
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94. A Candidate Massive Black Hole in the Low-Metallicity Dwarf Galaxy Pair Mrk 709

Author

Reines, A., Plotkin, R., Russell, Thomas, Mezcua, M., Condon, J., Sivakoff, G., Johnson, K., Reines, A., Plotkin, R., Russell, Thomas, Mezcua, M., Condon, J., Sivakoff, G., and Johnson, K.

Abstract

The incidence and properties of present-day dwarf galaxies hosting massive black holes (BHs) can provide important constraints on the origin of high-redshift BH seeds. Here we present high-resolution X-ray and radio observations of the low-metallicity, star-forming, dwarf-galaxy system Mrk 709 with the Chandra X-ray Observatory and the Karl G. Jansky Very Large Array. These data reveal spatially coincident hard X-ray and radio point sources with luminosities suggesting the presence of an accreting massive BH (M BH ~ 105-7 M ). Based on imaging from the Sloan Digital Sky Survey (SDSS), we find that Mrk 709 consists of a pair of compact dwarf galaxies that appear to be interacting with one another. The position of the candidate massive BH is consistent with the optical center of the southern galaxy (Mrk 709 S), while no evidence for an active BH is seen in the northern galaxy (Mrk 709 N). We derive stellar masses of M ~2.5 × 109 M ☉ and M ~ 1.1 × 109 M ☉ for Mrk 709 S and Mrk 709 N, respectively, and present an analysis of the SDSS spectrum of the BH host Mrk 709 S. At a metallicity of just ~10% solar, Mrk 709 is among the most metal-poor galaxies with evidence for an active galactic nucleus. Moreover, this discovery adds to the growing body of evidence that massive BHs can form in dwarf galaxies and that deep, high-resolution X-ray and radio observations are ideally suited to reveal accreting massive BHs hidden at optical wavelengths.

Published
2014

95. Very long baseline interferometry with the SKA

Author

Paragi, Z., Godfrey, L., Reynolds, C., Rioja, M., Deller, A., Zhang, B., Gurvits, L., Bietenholz, M., Szomoru, A., Bignall, H., Boven, P., Charlot, P., Dodson, R., Frey, S., Garrett, M., Imai, H., Lobanov, A., Reid, M., Ros, E., Van Langevelde, H., Zensus, J., Zheng, X., Alberdi, A., Agudo, I., An, T., Argo, M., Beswick, R., Biggs, A., Brunthaler, A., Campbell, R., Cimó, G., Colomer, F., Corbel, S., Conway, J., Cseh, D., Deane, R., Falcke, H., Gabányi, K., Gawronski, M., Gaylard, M., Giovannini, G., Giroletti, M., Goddi, C., Goedhart, S., Gómez, J., Gunn, A., Jung, T., Kharb, P., Klöckner, H., Körding, E., Kovalev, Y., Kunert-Bajraszewska, M., Lindqvist, M., Lister, M., Mantovani, F., Martí-Vidal, I., Mezcua, M., Mckean, J., Middelberg, E., Miller-Jones, James, Moldon, J., Muxlow, T., O'brien, T., Pérez-Torres, M., Pogrebenko, S., Quick, J., Rushton, A., Schilizzi, R., Smirno, O., Sohn, B., Surcis, G., Taylor, G., Tingay, S., Tudose, V., Van Der Horst, A., Van Leeuwen, J., Venturi, T., Vermeulen, R., Vlemmings, W., De Witt, A., Wucknitz, O., Yang, J., Paragi, Z., Godfrey, L., Reynolds, C., Rioja, M., Deller, A., Zhang, B., Gurvits, L., Bietenholz, M., Szomoru, A., Bignall, H., Boven, P., Charlot, P., Dodson, R., Frey, S., Garrett, M., Imai, H., Lobanov, A., Reid, M., Ros, E., Van Langevelde, H., Zensus, J., Zheng, X., Alberdi, A., Agudo, I., An, T., Argo, M., Beswick, R., Biggs, A., Brunthaler, A., Campbell, R., Cimó, G., Colomer, F., Corbel, S., Conway, J., Cseh, D., Deane, R., Falcke, H., Gabányi, K., Gawronski, M., Gaylard, M., Giovannini, G., Giroletti, M., Goddi, C., Goedhart, S., Gómez, J., Gunn, A., Jung, T., Kharb, P., Klöckner, H., Körding, E., Kovalev, Y., Kunert-Bajraszewska, M., Lindqvist, M., Lister, M., Mantovani, F., Martí-Vidal, I., Mezcua, M., Mckean, J., Middelberg, E., Miller-Jones, James, Moldon, J., Muxlow, T., O'brien, T., Pérez-Torres, M., Pogrebenko, S., Quick, J., Rushton, A., Schilizzi, R., Smirno, O., Sohn, B., Surcis, G., Taylor, G., Tingay, S., Tudose, V., Van Der Horst, A., Van Leeuwen, J., Venturi, T., Vermeulen, R., Vlemmings, W., De Witt, A., Wucknitz, O., and Yang, J.

Abstract

Adding VLBI capability to the SKA arrays will greatly broaden the science of the SKA, and is feasible within the current specifications. SKA-VLBI can be initially implemented by providing phased-array outputs for SKA1-MID and SKA1-SUR and using these extremely sensitive stations with other radio telescopes, and in SKA2 by realising a distributed configuration providing baselines up to thousands of km, merging it with existing VLBI networks. The motivation for and the possible realization of SKA-VLBI is described in this paper.

Published
2014

96. Radio investigation of Ultra-Luminous X-ray Sources in the SKA Era

Author

Wolter, A., Rushton, A.P., Mezcua, M., Cseh, D., Pintore, F., Prandoni, I., Paragi, Z., Zampieri, L., Bourke, T.L., and Bourke, T.L.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics of Galaxies (astro-ph.GA), Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Proceedings of Science [POS], Astrophysics - High Energy Astrophysical Phenomena, POS : Proceedings of Science, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

A puzzling class of exotic objects, which have been known about for more than 30 years, is reaching a new era of understanding. We have discovered hundreds of Ultra Luminous X-ray sources (ULXs) - non-nuclear sources with X-ray luminosity in excess of the Eddington luminosity for "normal" size stellar Black Holes (BH) - and we are making progresses towards understanding their emission mechanisms. The current explanations imply either a peculiar state of accretion onto a stellar size BH or the presence of an intermediate mass BH, the long-sought link between stellar and supermassive BHs. Both models might co-exist and therefore studying this class of object will give insight into the realm of accretion in a variety of environments and at the same time find look-alikes of the primordial seed BHs that are thought to be at the origin of todays supermassive BHs at the centre of galaxies. The radio band has been exploited only scantily due to the relative faint fluxes of the sources, but we know a number of interesting sources exhibiting both extended emission (like bubbles and possibly jets) and cores, as well as observed transient behaviour. The new eras of the SKA will lead us to a major improvement of our insight of the extreme accretion within ULXs. We will both investigate in detail known sources and research new and fainter ones. When we have reached a thorough understanding of radio emission in ULX we could also use the SKA as a discovery instrument for new ULX candidates. The new array will give an enormous space to discovery: sources like the ones currently known will be detected in a snapshot up to 50 Mpc instead of at 5 Mpc with long, pointed observations., 13 pages, 2 figures; to appear as part of 'Continuum Science' in Proceedings 'Advancing Astrophysics with the SKA (AASKA14)'

Published
2015

97. Chandra X-ray observations of the hyper-luminous infrared galaxy IRAS F15307+3252.

Author

Hlavacek-Larrondo, J., Gandhi, P., Hogan, M. T., Gendron-Marsolais, M.-L., Edge, A. C., Fabian, A. C., Russell, H. R., Iwasawa, K., and Mezcua, M.

Subjects
LUMINOSITY, SUBMILLIMETER astronomy, GALAXY clusters
Abstract

Hyper-luminous infrared galaxies (HyLIRGs) lie at the extreme luminosity end of the IR galaxy population with LIR > 1013 L⊙. They are thought to be closer counterparts of the more distant sub-millimeter galaxies, and should therefore be optimal targets to study the most massive systems in formation. We present deep Chandra observations of IRAS F15307+3252 (100 ks), a classical HyLIRG located at z=0.93 and hosting a radio-loudAGN(L1.4 GHz ~3.5× 1025WHz-1). The Chandra images reveal the presence of extended (r=160 kpc), asymmetric X-ray emission in the soft 0.3-2.0 keV band that has no radio counterpart. We therefore argue that the emission is of thermal origin originating from a hot intragroup or intracluster medium virializing in the potential. We find that the temperature (~2 keV) and bolometric X-ray luminosity (~3 × 1043 erg s-1) of the gas follow the expected LX-ray-T correlation for groups and clusters, and that the gas has a remarkably short cooling time of 1.2 Gyr. In addition, VLA radio observations reveal that the galaxy hosts an unresolved compact steep-spectrum (CSS) source, most likely indicating the presence of a young radio source similar to 3C186. We also confirm that the nucleus is dominated by a redshifted 6.4 keV Fe Ka line, strongly suggesting that the AGN is Compton-thick. Finally, Hubble images reveal an overdensity of galaxies and sub-structure in the galaxy that correlates with soft X-ray emission. This could be a snapshot view of on-going groupings expected in a growing cluster environment. IRAS F15307+3252 might therefore be a rare example of a group in the process of transforming into a cluster. [ABSTRACT FROM AUTHOR]

Published
2017
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