Author: "Ponman, T." / Topic: fos: physical sciences - Searchworks@Jio Institute Digital Library Search Results

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34 results on '"Ponman, T."'

1. The XXL Survey XX: The 365 cluster catalogue

Author: Adami, C., Giles, P., Koulouridis, E., Pacaud, F., Caretta, C. A., Pierre, M., Eckert, D., Ramos-Ceja, M. E., Gastaldello, F., Fotopoulou, S., Guglielmo, V., Lidman, C., Sadibekova, T., Iovino, A., Maughan, B., Chiappetti, L., Alis, S., Altieri, B., Baldry, I., Bottini, D., Birkinshaw, M., Bremer, M., Brown, M., Cucciati, O., Driver, S., Elmer, E., Ettori, S., Evrard, A. E., Faccioli, L., Granett, B., Grootes, M., Guzzo, L., Hopkins, A., Horellou, C., Lef, J. P., Liske, J., Malek, K., Marulli, F., Maurogordato, S., Owers, M., Paltani, S., Poggianti, B., Polletta, M., Plionis, M., Pollo, A., Pompei, E., Ponman, T., Rapetti, D., Ricci, M., Robotham, A., Tuffs, R., Tasca, L., Valtchanov, I., Vergani, D., Wagner, G., Willis, J., consortium, the XXL, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Département d'Astrophysique (ex SAP) (DAP), Université de Genève = University of Geneva (UNIGE), INAF-IASF Milano, Istituto Nazionale di Astrofisica (INAF), Aristotle University of Thessaloniki, INAF- Milano, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fisica, Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB)-Università degli Studi di Milano = University of Milan (UNIMI), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Earth and Space Sciences [Göteborg], Chalmers University of Technology [Göteborg], Simon Fraser University (SFU.ca), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Thessaloniki], INAF - Osservatorio Astrofisico di Arcetri (OAA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Département de Physique des Particules (ex SPP) (DPP), University of Geneva [Switzerland], Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Milano [Milano]-Università di Milano-Bicocca, Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Milano-Bicocca [Milano] (UNIMIB)-Università degli Studi di Milano [Milano] (UNIMI), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of St Andrews. School of Physics and Astronomy, Adami, C., Giles, P., Koulouridis, E., Pacaud, F., Caretta, C.A., Pierre, M., Eckert, D., Ramos-Ceja, M.E., Gastaldello, F., Fotopoulou, S., Guglielmo, V., Sadibekova, T., Iovino, A., Maughan, B., Chiappetti, L., Alis, S., Altieri, B., Baldry, I., Bottini, D., Birkinshaw, M., Bremer, M., Brown, M., Cucciati, O., Driver, S., Elmer, E., Ettori, S., Evrard, A.E., Faccioli, L., Granett, B., Grootes, M., Guzzo, L., Hopkins, A., Horellou, C., Lefèvre, J.P., Liske, J., Malek, K., Marulli, F., Maurogordato, S., Owers, M., Paltani, S., Poggianti, B., Polletta, M., Plionis, M., Pollo, A., Pompei, E., Ponman, T., Rapetti, D., Ricci, M., Robotham, A., Tuffs, R., Tasca, L., Valtchanov, I., Vergani, D., Wagner, G., and Willis, J.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, astrophysics - astrophysics of galaxies, Large-scale structure of Universe, FOS: Physical sciences, galaxies: clusters: distance and redshifts, Context (language use), Sample (statistics), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: intracluster medium [Galaxies], clusters: general [Galaxies], 01 natural sciences, astrophysics - cosmology and nongalactic astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: groups: general, Large-scale structure of the universe, 0103 physical sciences, Cluster (physics), QB Astronomy, 010303 astronomy & astrophysics, QC, Luminosity function (astronomy), QB, Physics, 010308 nuclear & particles physics, Astronomy and Astrophysics, DAS, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, cosmology: large-scale structure of Universe, Redshift, Galaxy, groups: general [Galaxies], QC Physics, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), X-rays: galaxies: clusters, Cluster sampling, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: In the currently debated context of using clusters of galaxies as cosmological probes, the need for well-defined cluster samples is critical. The XXL Survey has been specifically designed to provide a well characterised sample of some 500 X-ray detected clusters suitable for cosmological studies. The main goal of present article is to make public and describe the properties of the cluster catalogue in its present state, as well as of associated catalogues as super-clusters and fossil groups. We release a sample containing 365 clusters in total. We give the details of the follow-up observations and explain the procedure adopted to validate the cluster spectroscopic redshifts. Considering the whole XXL cluster sample, we have provided two types of selection, both complete in a particular sense: one based on flux-morphology criteria, and an alternative based on the [0.5-2] keV flux within one arcmin of the cluster centre. We have also provided X-ray temperature measurements for 80$\%$ of the clusters having a flux larger than 9$\times$10$^{-15}$$\rm \thinspace erg \, s^{-1} \, cm^{-2}$. Our cluster sample extends from z$\sim$0 to z$\sim$1.2, with one cluster at z$\sim$2. Clusters were identified through a mean number of six spectroscopically confirmed cluster members. Our updated luminosity function and luminosity-temperature relation are compatible with our previous determinations based on the 100 brightest clusters, but show smaller uncertainties. We also present an enlarged list of super-clusters and a sample of 18 possible fossil groups. This intermediate publication is the last before the final release of the complete XXL cluster catalogue when the ongoing C2 cluster spectroscopic follow-up is complete. It provides a unique inventory of medium-mass clusters over a 50~\dd\ area out to z$\sim$1., Comment: A&A, in press Shortened abstract Full catalogues available online, see paper
Published: 2018

2. ORIGIN: metal creation and evolution from the cosmic dawn

Author: den, Herder Jan-Willem, Piro, Luigi, Kouveliotou, Chryssa, Hartmann, Dieter H., Kaastra, Jelle S., Amati, L., Andersen, M. I., Arnaud, M., Atteia, J.-L., Bandler, S., Barbera, M., Barcons, X., Barthelmy, S., Basa, S., Basso, S., Boer, M., Branchini, E., Branduardi-Raymont, G., Borgani, S., Boyarsky, A., Brunetti, G., Budtz-Jorgensen, C., Burrows, D., Butler, N., Campana, S., Caroli, E., Ceballos, M., Christensen, F., Churazov, E., Comastri, A., Colasanti, L., Cole, R., Content, R., Corsi, A., Costantini, E., Conconi, P., Cusumano, G., de, Plaa J., De, Rosa A., Del, Santo M., Di, Cosimo S., De, Pasquale M., Doriese, R., Ettori, S., Evans, P., Ferrari, L., Finger, H., Figueroa-Feliciano, T., Friedrich, P., Furuzawa, A., Fynbo, J., Gatti, F., Galeazzi, M., Gehrels, N., Gendre, B., Ghirlanda, G., Ghisellini, G., Gilfanov, M., Giommi, P., Girardi, M., Grindlay, J., Cocchi, M., Godet, O., Guedel, M., Haardt, F., den, Hartog R., Hepburn, I., Hermsen, W., Hjorth, J., Hoekstra, H., Holland, A., Hornstrup, A., van, der Horst A., int, Zand J., Irwin, K., Jonker, P., Kitayama, T., Kawahara, H., Kawai, N., Kelley, R., Kilbourne, C., de, Korte P., Kusenko, A., Kuvvetli, I., Labanti, M., Macculi, C., Maiolino, R., Mas, Hesse M., Matsushita, K., Mazzotta, P., McCammon, D., Mendez, M., Mignani, R., Mineo, T., Mushotzky, R., Molendi, S., Moscardini, L., Natalucci, L., Nicastro, F., O'Brien, P., Osborne, J., Paerels, F., Page, M., Paltani, S., Pedersen, K., Perinati, E., Ponman, T., Pointecouteau, E., Predehl, P., Porter, S., Rasmussen, A., Rauw, G., Rottgering, H., Roncarelli, M., Rosati, P., Quadrini, E., Ruchayskiy, O., Salvaterra, R., Sasaki, S., Sato, K., Savaglio, S., Schaye, J., Sciortino, S., Shaposhnikov, M., Sharples, R., Shinozaki, K., Spiga, D., Sunyaev, R., Suto, Y., Tanvir, N., Troja, E., Ubertini, P., Ullom, J., Ursino, E., Verbunt, F., van, de Voort F., Viel, M., Wachter, S., Watson, D., Weisskopf, M., Werner, N., White, N., Willingale, R., Wijers, R., Yoshikawa, K., Zane, S., Ohashi, Takaya, Ezoe, Y., Fujimoto, R., Hoshino, A., Ishisaki, Y., Mitsuda, Kazuhisa, Takei, Yoh, Tashiro, Makoto, Tamura, Takayuki, Tawara, Yuzuru, Tsujimoto, Masahiro, Tsuru, Takeshi, Yamasaki, Noriko, den Herder, JW, Piro, L, Ohashi, T, Kouveliotou, C, Hartmann, DH, Kaastra, JS, Amati, L, Andersen, MI, Arnaud, M, Attèia, JL, Bandler, S, Barbera, M, Barcons, X, Barthelmy, S, Basa, S, Basso, S, Boer, M, Branchini, E, Branduardi-Raymont, G, Borgani, S, Boyarsky, A, Brunetti, G, Budtz-Jorgensen, C, Burrows, D, Butler, N, Campana, S, Caroli, E, Ceballos, M, Christensen, F, Churazov, E, Comastri, A, Colasanti, L, Cole, R, Content, R, Corsi, A, Costantini, E, Conconi, P, Cusumano, G, de Plaa, J, De Rosa, A, Del Santo, M, Di Cosimo, S, De Pasquale, M, Doriese, R, Ettori, S, Evans, P, Ezoe, Y, Ferrari, L, Finger, H, Figueroa-Feliciano, T, Friedrich, P, Fujimoto, R, Furuzawa, A, Fynbo, J, Gatti, F, Galeazzi, M, Gehrels, N, Gendre, B, Ghirlanda, G, Ghisellini, G, Gilfanov, M, Giommi, P, Girardi, M, Grindlay, J, Cocchi, M, Godet, O, Guedel, M, Haardt, F, den Hartog, R, Hepburn, I, Hermsen, W, Hjorth, J, Hoekstra, H, Holland, A, Hornstrup, A, van der Horst, A, Hoshino, A, in't Zand, J, Irwin, K, Ishisaki, Y, Jonker, P, Kitayama, T, Kawahara, H, Kawai, N, Kelley, R, Kilbourne, C, de Korte, P, Kusenko, A, Kuvvetli, I, Labanti, M, Macculi, C, Maiolino, R, Hesse, MM, Matsushita, K, Mazzotta, P, McCammon, D, Mèndez, M, Mignani, R, Mineo, T, Mitsuda, K, Mushotzky, R, Molendi, S, Moscardini, L, Natalucci, L, Nicastro, F, O'Brien, P, Osborne, J, Paerels, F, Page, M, Paltani, S, Pedersen, K, Perinati, E, Ponman, T, Pointecouteau, E, Predehl, P, Porter, S, Rasmussen, A, Rauw, G, Rottgering, H, Roncarelli, M, Rosati, P, Quadrini, E, Ruchayskiy, O, Salvaterra, R, Sasaki, S, Sato, K, Savaglio, S, Schaye, J, Sciortino, S, Shaposhnikov, M, Sharples, R, Shinozaki, K, Spiga, D, Sunyaev, R, Suto, Y, Takei, Y, Tanvir, N, Tashiro, M, Tamura, T, Tawara, Y, Troja, E, Tsujimoto, M, Tsuru, T, Ubertini, P, Ullom, J, Ursino, E, Verbunt, F, van de Voort, F, Viel, M, Wachter, S, Watson, D, Weisskopf, M, Werner, N, White, N, Willingale, R, Wijers, R, Yamasaki, N, Yoshikawa, K, Zane, S, Airbus, High Energy Astrophys. & Astropart. Phys (API, FNWI), Massachusetts Institute of Technology. Department of Physics, Figueroa-Feliciano, Enectali, Astronomy, J. W., den Herder, L., Piro, T., Ohashi, C., Kouveliotou, D. H., Hartmann, J. S., Kaastra, L., Amati, M. I., Andersen, M., Arnaud, J. L., Attéia, S., Bandler, M., Barbera, X., Barcon, S., Barthelmy, S., Basa, S., Basso, M., Boer, E., Branchini, G., Branduardi Raymont, Borgani, Stefano, A., Boyarsky, G., Brunetti, C., Budtz Jorgensen, D., Burrow, N., Butler, S., Campana, E., Caroli, M., Ceballo, F., Christensen, E., Churazov, A., Comastri, L., Colasanti, R., Cole, R., Content, A., Corsi, E., Costantini, P., Conconi, G., Cusumano, J., de Plaa, A., De Rosa, M., Del Santo, S., Di Cosimo, M., De Pasquale, R., Doriese, S., Ettori, P., Evan, Y., Ezoe, L., Ferrari, H., Finger, T., Figueroa Feliciano, P., Friedrich, R., Fujimoto, A., Furuzawa, J., Fynbo, F., Gatti, M., Galeazzi, N., Gehrel, B., Gendre, G., Ghirlanda, G., Ghisellini, M., Gilfanov, P., Giommi, Girardi, Marisa, J., Grindlay, M., Cocchi, O., Godet, M., Guedel, F., Haardt, R., den Hartog, I., Hepburn, W., Hermsen, J., Hjorth, H., Hoekstra, A., Holland, A., Hornstrup, A., van der Horst, A., Hoshino, J. in t., Zand, K., Irwin, Y., Ishisaki, P., Jonker, T., Kitayama, H., Kawahara, N., Kawai, R., Kelley, C., Kilbourne, P., de Korte, A., Kusenko, I., Kuvvetli, M., Labanti, C., Macculi, R., Maiolino, M., Mas Hesse, K., Matsushita, P., Mazzotta, D., Mccammon, M., Méndez, R., Mignani, T., Mineo, K., Mitsuda, R., Mushotzky, S., Molendi, L., Moscardini, L., Natalucci, F., Nicastro, P. O., Brien, J., Osborne, F., Paerel, M., Page, S., Paltani, K., Pedersen, E., Perinati, T., Ponman, E., Pointecouteau, P., Predehl, S., Porter, A., Rasmussen, G., Rauw, H., Röttgering, M., Roncarelli, P., Rosati, E., Quadrini, O., Ruchayskiy, R., Salvaterra, S., Sasaki, K., Sato, S., Savaglio, J., Schaye, S., Sciortino, M., Shaposhnikov, R., Sharple, K., Shinozaki, D., Spiga, R., Sunyaev, Y., Suto, Y., Takei, N., Tanvir, M., Tashiro, T., Tamura, Y., Tawara, E., Troja, M., Tsujimoto, T., Tsuru, P., Ubertini, J., Ullom, E., Ursino, F., Verbunt, F., van de Voort, M., Viel, S., Wachter, D., Watson, M., Weisskopf, N., Werner, N., White, R., Willingale, R., Wijer, N., Yamasaki, K., Yoshikawa, S., Zane, Jan-Willem Herder, Luigi Piro, Takaya Ohashi, Chryssa Kouveliotou, Dieter H. Hartmann, Jelle S. Kaastra, L. Amati, M. I. Andersen, M. Arnaud, J. -L. Attéia, S. Bandler, M. Barbera, X. Barcon, S. Barthelmy, S. Basa, S. Basso, M. Boer, E. Branchini, G. Branduardi-Raymont, S. Borgani, A. Boyarsky, G. Brunetti, C. Budtz-Jorgensen, D. Burrow, N. Butler, S. Campana, E. Caroli, M. Ceballo, F. Christensen, E. Churazov, A. Comastri, L. Colasanti, R. Cole, R. Content, A. Corsi, E. Costantini, P. Conconi, G. Cusumano, J. Plaa, A. Rosa, M. Santo, S. Cosimo, M. Pasquale, R. Doriese, S. Ettori, P. Evan, Y. Ezoe, L. Ferrari, H. Finger, T. Figueroa-Feliciano, P. Friedrich, R. Fujimoto, A. Furuzawa, J. Fynbo, F. Gatti, M. Galeazzi, N. Gehrel, B. Gendre, G. Ghirlanda, G. Ghisellini, M. Gilfanov, P. Giommi, M. Girardi, J. Grindlay, M. Cocchi, O. Godet, M. Guedel, F. Haardt, R. Hartog, I. Hepburn, W. Hermsen, J. Hjorth, H. Hoekstra, A. Holland, A. Hornstrup, A. Horst, A. Hoshino, J. Zand, K. Irwin, Y. Ishisaki, P. Jonker, T. Kitayama, H. Kawahara, N. Kawai, R. Kelley, C. Kilbourne, P. Korte, A. Kusenko, I. Kuvvetli, M. Labanti, C. Macculi, R. Maiolino, M. Mas Hesse, K. Matsushita, P. Mazzotta, D. McCammon, M. Méndez, R. Mignani, T. Mineo, K. Mitsuda, R. Mushotzky, S. Molendi, L. Moscardini, L. Natalucci, F. Nicastro, P. O’Brien, J. Osborne, F. Paerel, M. Page, S. Paltani, K. Pedersen, E. Perinati, T. Ponman, E. Pointecouteau, P. Predehl, S. Porter, A. Rasmussen, G. Rauw, H. Röttgering, M. Roncarelli, P. Rosati, E. Quadrini, O. Ruchayskiy, R. Salvaterra, S. Sasaki, K. Sato, S. Savaglio, J. Schaye, S. Sciortino, M. Shaposhnikov, R. Sharple, K. Shinozaki, D. Spiga, R. Sunyaev, Y. Suto, Y. Takei, N. Tanvir, M. Tashiro, T. Tamura, Y. Tawara, E. Troja, M. Tsujimoto, T. Tsuru, P. Ubertini, J. Ullom, E. Ursino, F. Verbunt, F. Voort, M. Viel, S. Wachter, D. Watson, M. Weisskopf, N. Werner, N. White, R. Willingale, R. Wijer, N. Yamasaki, K. Yoshikawa, S. Zane, den Herder Jan, Willem, Piro, Luigi, Ohashi, Takaya, Kouveliotou, Chryssa, Hartmann Dieter, H., Kaastra Jelle, S., Amati, L., Andersen, M. I., Arnaud, M., Atteia, J. L., Bandler, S., Barbera, M., Barcons, X., Barthelmy, S., Basa, S., Basso, S., Boer, M., Branchini, ENZO FRANCO, Branduardi Raymont, G., Borgani, S., Boyarsky, A., Brunetti, G., Budtz Jorgensen, C., Burrows, D., Butler, N., Campana, S., Caroli, E., Ceballos, M., Christensen, F., Churazov, E., Comastri, A., Colasanti, L., Cole, R., Content, R., Corsi, A., Costantini, E., Conconi, P., Cusumano, G., de Plaa, J., De Rosa, A., Del Santo, M., Di Cosimo, S., De Pasquale, M., Doriese, R., Ettori, S., Evans, P., Ezoe, Y., Ferrari, L., Finger, H., Figueroa Feliciano, T., Friedrich, P., Fujimoto, R., Furuzawa, A., Fynbo, J., Gatti, F., Galeazzi, M., Gehrels, N., Gendre, B., Ghirlanda, G., Ghisellini, G., Gilfanov, M., Giommi, P., Girardi, M., Grindlay, J., Cocchi, M., Godet, O., Guedel, M., Haardt, F., den Hartog, R., Hepburn, I., Hermsen, W., Hjorth, J., Hoekstra, H., Holland, A., Hornstrup, A., van der Horst, A., Hoshino, A., in't Zand, J., Irwin, K., Ishisaki, Y., Jonker, P., Kitayama, T., Kawahara, H., Kawai, N., Kelley, R., Kilbourne, C., de Korte, P., Kusenko, A., Kuvvetli, I., Labanti, M., Macculi, C., Maiolino, R., Mas Hesse, M., Matsushita, K., Mazzotta, P., Mccammon, D., Mendez, M., Mignani, R., Mineo, T., Mitsuda, K., Mushotzky, R., Molendi, S., Moscardini, L., Natalucci, L., Nicastro, F., O'Brien, P., Osborne, J., Paerels, F., Page, M., Paltani, S., Pedersen, K., Perinati, E., Ponman, T., Pointecouteau, E., Predehl, P., Porter, S., Rasmussen, A., Rauw, G., Rottgering, H., Roncarelli, M., Rosati, P., Quadrini, E., Ruchayskiy, O., Salvaterra, R., Sasaki, S., Sato, K., Savaglio, S., Schaye, J., Sciortino, S., Shaposhnikov, M., Sharples, R., Shinozaki, K., Spiga, D., Sunyaev, R., Suto, Y., Takei, Y., Tanvir, N., Tashiro, M., Tamura, T., Tawara, Y., Troja, E., Tsujimoto, M., Tsuru, T., Ubertini, P., Ullom, J., Ursino, E., Verbunt, F., van de Voort, F., Viel, M., Wachter, S., Watson, D., Weisskopf, M., Werner, N., White, N., Willingale, R., Wijers, R., Yamasaki, N., Yoshikawa, K., and Zane, S.
Subjects: HOT INTERGALACTIC MEDIUM, UNIVERSE, Chemical evolution, Mission, 7. Clean energy, 01 natural sciences, Spectral line, Settore FIS/05 - Astronomia E Astrofisica, 010303 astronomy & astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), NUCLEOSYNTHESIS, COSMIC cancer database, Clusters of galaxies, Satellite Mission, Epoch (reference date), Astrophysics::Instrumentation and Methods for Astrophysics, FOREST, GALAXIES, Gamma-ray bursts, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, X-ray, Mission, Gamma-ray bursts, Clusters of galaxies, Warm-hot intergalactic medium, Chemical evolution, Warm-hot intergalactic medium, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and Astronomy, Structure formation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Clusters of galaxie, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, REDSHIFT, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, X-ray Mission, Gamma-ray bursts, Clusters of galaxies, Warm-hot intergalactic medium, Chemical evolution, ABSORPTION-SPECTRA, 010309 optics, X-ray, YIELDS, 0103 physical sciences, Gamma-ray burst, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astronomy, Astronomy and Astrophysics, Redshift, Galaxy, Universe, 13. Climate action, Space and Planetary Science, CLUSTERS
Abstract: Herder, Jan-Willem den et al., ORIGIN is a proposal for the M3 mission call of ESA aimed at the study of metal creation from the epoch of cosmic dawn. Using high-spectral resolution in the soft X-ray band, ORIGIN will be able to identify the physical conditions of all abundant elements between C and Ni to red-shifts of z = 10, and beyond. The mission will answer questions such as: When were the first metals created? How does the cosmic metal content evolve? Where do most of the metals reside in the Universe? What is the role of metals in structure formation and evolution? To reach out to the early Universe ORIGIN will use Gamma-Ray Bursts (GRBs) to study their local environments in their host galaxies. This requires the capability to slew the satellite in less than a minute to the GRB location. By studying the chemical composition and properties of clusters of galaxies we can extend the range of exploration to lower redshifts (z-0.2). For this task we need a high-resolution spectral imaging instrument with a large field of view. Using the same instrument, we can also study the so far only partially detected baryons in the Warm-Hot Intergalactic Medium (WHIM). The less dense part of the WHIM will be studied using absorption lines at low redshift in the spectra for GRBs. The ORIGIN mission includes a Transient Event Detector (coded mask with a sensitivity of 0.4 photon/cm2/s in 10 s in the 5–150 keV band) to identify and localize 2000 GRBs over a five year mission, of which -65 GRBs have a redshift > 7. The Cryogenic Imaging Spectrometer, with a spectral resolution of 2.5 eV, a field of view of 30 arcmin and large effective area below 1 keV has the sensitivity to study clusters up to a significant fraction of the virial radius and to map the denser parts of the WHIM (factor 30 higher than achievable with current instruments). The payload is complemented by a Burst InfraRed Telescope to enable onboard red-shift determination of GRBs (hence securing proper follow up of high-z bursts) and also probes the mildly ionized state of the gas. Fast repointing is achieved by a dedicated ControlledMomentum Gyro and a low background is achieved by the selected low Earth orbit., The team likes to express its appreciation for the support of Astrium UK for the present study.
Published: 2011

3. LoCuSS: Connecting the Dominance and Shape of Brightest Cluster Galaxies with the Assembly History of Massive Clusters

Author: Smith, Graham P., Khosroshahi, Habib G., Dariush, A., Sanderson, A. J. R., Ponman, T. J., Stott, J. P., Haines, C. P., Egami, E., and Stark, D. P.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the luminosity gap, dm12, between the first and second ranked galaxies in a sample of 59 massive galaxy clusters, using data from the Hale Telescope, HST, Chandra, and Spitzer. We find that the dm12 distribution, p(dm12), is a declining function of dm12, to which we fitted a straight line: p(dm12) propto -(0.13+/-0.02)dm12. The fraction of clusters with "large" luminosity gaps is p(dm12>=1)=0.37+/-0.08, which represents a 3sigma excess over that obtained from Monte Carlo simulations of a Schechter function that matches the mean cluster galaxy luminosity function. We also identify four clusters with "extreme" luminosity gaps, dm12>=2, giving a fraction of p(dm12>=2)=0.07+0.05-0.03. More generally, large luminosity gap clusters are relatively homogeneous, with elliptical/disky brightest cluster galaxies (BCGs), cuspy gas density profiles (i.e. strong cool cores), high concentrations, and low substructure fractions. In contrast, small luminosity gap clusters are heterogeneous, spanning the full range of boxy/elliptical/disky BCG morphologies, the full range of cool core strengths and dark matter concentrations, and have large substructure fractions. Taken together, these results imply that the amplitude of the luminosity gap is a function of both the formation epoch, and the recent infall history of the cluster. "BCG dominance" is therefore a phase that a cluster may evolve through, and is not an evolutionary "cul-de-sac". We also compare our results with semi-analytic model predictions based on the Millennium Simulation. None of the models are able to reproduce all of the observational results, underlining the inability of current models to match the empirical properties of BCGs. We identify the strength of AGN feedback and the efficiency with which cluster galaxies are replenished after they merge with the BCG in each model as possible causes of these discrepancies. [Abridged], 15 pages, 12 figures, accepted for publication in MNRAS
Published: 2010
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4. The Evolution of Galaxy Disks in Dense Environments - Lessons from Compact Galaxy Groups

Author: Rasmussen, J., Ponman, T. J., Verdes-Montenegro, L., Yun, M. S., and Borthakur, S.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: Disk galaxies in compact galaxy groups exhibit a remarkable shortfall of neutral hydrogen compared to both isolated spirals and spirals in more loose groups, but the origin of this HI deficiency remains unclear. Based on a sample of highly HI deficient compact galaxy groups, here updated to also include HCG 58 and HCG 93, we summarise the first results of a multi-wavelength campaign aimed at understanding the processes responsible for modifying the HI content of galaxy disks in these environments. While tidal stripping, ram pressure stripping by hot intragroup gas, and star-formation induced strangulation could individually be affecting the ISM in some of the group members, these processes each face specific difficulties in explaining the inferred deficiency of HI for the sample as a whole. A complete picture of the mechanisms driving the ISM evolution in the disk galaxies of these groups has thus yet to emerge, but promising avenues for further progress in this field are briefly discussed on the basis of the present sample., 6 pages, 3 figures, to appear in online Proc. IAU Symp. 254, "The Galaxy Disk in Cosmological Context", Eds. J. Andersen, J. Bland-Hawthorn, B. Nordstroem
Published: 2008

5. The XMM-LSS survey: the Class 1 cluster sample over the initial 5 square degrees and its cosmological modelling

Author: Pacaud, F., Pierre, M., Adami, C., Altieri, B., Andreon, S., Chiappetti, L., Detal, A., Duc, P. -A., Galaz, G., Gueguen, A., Fèvre, J. -P. Le, Hertling, G., Libbrecht, C., Melin, J. -B., Ponman, T. J., Quintana, H., Refregier, A., Sprimont, P. -G., Surdej, J., Valtchanov, I., Willis, J. P., Alloin, D., Birkinshaw, M., Bremer, M. N., Garcet, O., Jean, C., Jones, L. R., Fèvre, O. Le, Maccagni, D., Mazure, A., Proust, D., Röttgering, H. J. A., Trinchieri, G., Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Departamento de Astronomía y Astrofísica [Santiago], Pontificia Universidad Católica de Chile (UC), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We present a sample of 29 galaxy clusters from the XMM-LSS survey over an area of some 5deg2 out to a redshift of z=1.05. The sample clusters, which represent about half of the X-ray clusters identified in the region, follow well defined X-ray selection criteria and are all spectroscopically confirmed. For all clusters, we provide X-ray luminosities and temperatures as well as masses. The cluster distribution peaks around z=0.3 and T =1.5 keV, half of the objects being groups with a temperature below 2 keV. Our L-T(z) relation points toward self-similar evolution, but does not exclude other physically plausible models. Assuming that cluster scaling laws follow self-similar evolution, our number density estimates up to z=1 are compatible with the predictions of the concordance cosmology and with the findings of previous ROSAT surveys. Our well monitored selection function allowed us to demonstrate that the inclusion of selection effects is essential for the correct determination of the evolution of the L-T relation, which may explain the contradictory results from previous studies. Extensive simulations show that extending the survey area to 10deg2 has the potential to exclude the non-evolution hypothesis, but that constraints on more refined ICM models will probably be limited by the large intrinsic dispersion of the L-T relation. We further demonstrate that increasing the dispersion in the scaling laws increases the number of detectable clusters, hence generating further degeneracy [in addition to sigma8, Omega_m, L(M,z) and T(M,z)] in the cosmological interpretation of the cluster number counts. We provide useful empirical formulae for the cluster mass-flux and mass-count-rate relations as well as a comparison between the XMM-LSS mass sensitivity and that of forthcoming SZ surveys., Comment: Accepted for publication by MNRAS. Full resolution images as well as additional cluster data are available through a dedicated database at http://l3sdb.in2p3.fr:8080/l3sdb/
Published: 2007
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6. The XMM-LSS catalogue: X-ray sources and associated optical data. Version I

Author: Pierre, M., Chiappetti, L., Pacaud, F., Gueguen, A., Libbrecht, C., Altieri, B., Aussel, H., Gandhi, P., Garcet, O., Gosset, E., Paioro, L., Ponman, T. J., Read, A. M., Refregier, A., Starck, Jean-Luc, Surdej, J., Valtchanov, I., Adami, C., Alloin, D., Alshino, A., Andreon, S., Birkinshaw, M., Bremer, M., Detal, A., Duc, P. -A., Galaz, G., Jones, L., Fèvre, J. -P. Le, Fèvre, O. Le, Maccagni, D., Mazure, A., Quintana, H., Röttgering, H. J. A., Sprimont, P. -G., Tasse, C., Trinchieri, G., Willis, J. P., Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), XMM-Newton Science Operations Centre, European Space Agency (ESA), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Agence Spatiale Européenne = European Space Agency (ESA), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: Following the presentation of the XMM-LSS X-ray source detection package by Pacaud et al., we provide the source lists for the first 5.5 surveyed square degrees. The catalogues pertain to the [0.5-2] and [2-10] keV bands and contain in total 3385 point-like or extended sources above a detection likelihood of 15 in either band. The agreement with deep logN-logS is excellent. The main parameters considered are position, countrate, source extent with associated likelihood values. A set of additional quantities such as astrometric corrections and fluxes are further calculated while errors on the position and countrate are deduced from simulations. We describe the construction of the band-merged catalogue allowing rapid sub-sample selection and easy cross-correlation with external multi-wavelength catalogues. A small optical CFHTLS multi-band subset of objects is associated wich each source along with an X-ray/optical overlay. We make the full X-ray images available in FITS format. The data are available at CDS and, in a more extended form, at the Milan XMM-LSS database., 13 pages, 7 figures and 11 tables (fig. 1 and 6 are enclosed in reduced resolution), MNRAS Latex, accepted by MNRAS
Published: 2007

7. AGN heating in galaxy groups: A statistical study

Author: Jetha, N. N., Ponman, T. J., Hardcastle, M. J., and Croston, J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We present gas temperature, density, entropy and cooling time profiles for the cores of a sample of 15 galaxy groups observed with {\it Chandra}. We find that the entropy profiles follow a power-law profile down to very small fractions of $R_{500}$. Differences between the gas profiles of groups with radio loud and radio quiet BGGs are only marginally significant, and there is only a small difference in the $L_X:T_X$ relations, for the central regions we study with {\it Chandra}, between the radio-loud and radio-quiet objects in our sample, in contrast to the much larger difference found on scales of the whole group in earlier work. However, there is evidence, from splitting the sample based on the mass of the central black holes, that repeated outbursts of AGN activity may have a long term cumulative effect on the entropy profiles. We argue that, to first-order, energy injection from radio sources does not change the global structure of the gas in the cores of groups, although it can displace gas on a local level. In most systems, it appears that AGN energy injection serves primarily to counter the effects of radiative cooling, rather than being responsible for the similarity breaking between groups and clusters., 14 pages, 13 figures, accepted MNRAS
Published: 2006

8. The XMM-LSS Survey: A well controlled X-ray cluster sample over the D1 CFHTLS area

Author: Pierre, M., Pacaud, F., Duc, P. -A., Willis, J. P., Andreon, S., Valtchanov, I., Altieri, B., Galaz, G., Gueguen, A., Fèvre, J. -P. Le, Fèvre, O. Le, Ponman, T., Sprimont, P. -G., Surdej, J., Adami, C., Alshino, A., Bremer, M., Chiappetti, L., Detal, A., Garcet, O., Gosset, E., Jean, C., Maccagni, D., Marinoni, Christian, Mazure, A., Quintana, H., Read, A., Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We present the XMM-LSS cluster catalogue corresponding to the CFHTLS D1 area. The list contains 13 spectroscopically confirmed, X-ray selected galaxy clusters over 0.8 deg2 to a redshift of unity and so constitutes the highest density sample of clusters to date. Cluster X-ray bolometric luminosities range from 0.03 to 5x10^{44} erg/s. In this study, we describe our catalogue construction procedure: from the detection of X-ray cluster candidates to the compilation of a spectroscopically confirmed cluster sample with an explicit selection function. The procedure further provides basic X-ray products such as cluster temperature, flux and luminosity. We detected slightly more clusters with a (0.5-2.0 keV) X-ray fluxes of >2x10^{-14} erg/s/cm^{-2} than we expected based on expectations from deep ROSAT surveys. We also present the Luminosity-Temperature relation for our 9 brightest objects possessing a reliable temperature determination. The slope is in good agreement with the local relation, yet compatible with a luminosity enhancement for the 0.15 < z< 0.35 objects having 1 < T < 2 keV, a population that the XMM-LSS is identifying systematically for the first time. The present study permits the compilation of cluster samples from XMM images whose selection biases are understood. This allows, in addition to studies of large-scale structure, the systematic investigation of cluster scaling law evolution, especially for low mass X-ray groups which constitute the bulk of our observed cluster population. All cluster ancillary data (images, profiles, spectra) are made available in electronic form via the XMM-LSS cluster database., 12 pages 5 figures, MNRAS accepted. The paper with full resolution cluster images is available at http://vela.astro.ulg.ac.be/themes/spatial/xmm/LSS/rel_pub_e.html
Published: 2006

9. XMM-Newton study of 0.012

Author: Finoguenov, A., Ponman, T. J., Osmond, J. P. F., and Zimer, M.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We study the thermodynamic properties of the hot gas in a sample of groups in the 0.012-0.024 redshift range, using XMM-Newton observations. We present measurements of temperature, entropy, pressure and iron abundance. Non-parametric fits are used to derive the mean properties of the sample and to study dispersion in the values of entropy and pressure. The scaling of the entropy at 0.2r500 matches well the results of Ponman et al. (2003). However, compared to cool clusters, the groups in our sample reveal larger entropy at inner radii and a substantially flatter slope in the entropy in the outskirts, compared to both the prediction of pure gravitational heating and to observations of clusters. This difference corresponds to the systematically flatter group surface brightness profiles, reported previously. The scaled pressure profiles can be well approximated with a Sersic model with n=4. We find that groups exhibit a systematically larger dispersion in pressure, compared to clusters of galaxies, while the dispersion in entropy is similar., 11 pages, MNRAS in press, the 25 page version with all 176 figures included is at ftp://ftp.xray.mpe.mpg.de/people/alexis/2dxgs_astroph.ps.gz
Published: 2006
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10. The XMM Large-Scale Structure Survey: An initial sample of galaxy groups and clusters to a redshift z<0.6

Author: Willis, J. P., Pacaud, F., Valtchanov, I., Pierre, M., Ponman, T., Read, A., Andreon, S., Altieri, B., Quintana, H., Santos, S. Dos, Birkinshaw, M., Bremer, M., Duc, P. A., Galaz, G., Gosset, E., Jones, L., and Surdej, J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present X-ray and optical spectroscopic observations of twelve galaxy groups and clusters identified within the XMM Large-Scale Structure (LSS) survey. Groups and clusters are selected as extended X-ray sources from a 3.5 deg2 XMM image mosaic above a flux limit 8e-15 ergs/s/cm2 in the [0.5-2] keV energy band. Deep BVRI images and multi-object spectroscopy confirm each source as a galaxy concentration located within the redshift interval 0.29, 18 pages, MNRAS accepted
Published: 2005
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11. XMM-Newton observations of the late-stage merger-remnant galaxies NGC 3921 and NGC 7252

Author: Nolan, L. A., Ponman, T. J., Read, A. M., and Schweizer, Francois
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Using the high sensitivity of XMM, we have studied the X-ray emission of the two proto-typical late-stage merger remnants, NGC 3921 and NGC 7252. In the case of NGC 7252, this is complemented by archival Chandra data. We investigate the nature of the discrete X-ray point source populations and the hot diffuse gas components in these two galaxies, and compare them in the light of their different merger ages and histories. We detect 3 candidate ultra-luminous X-ray point sources in NGC 3921 and at least 6 in NGC 7252, for which we have high spatial resolution Chandra data. These have luminosities ranging from \~1.4x10^39-10^40 erg s^-1 (for H_0= 75 km s-1 Mpc^-1). We expect these ULXs to be high mass X-ray binaries, associated with the recent star formation in these two galaxies. Extended hot gas is observed in both galaxies. We have sufficient counts in the XMM data to fit two-component hot plasma models to their X-ray spectra and estimate the X-ray luminosities of the hot diffuse gas components to be 2.75x10^40 erg s^-1 and 2.09x10^40 erg s^-1 in NGC 3921 and NGC 7252, respectively. These luminosities are low compared with the luminosities observed in typical mature elliptical galaxies LX ~10^(41-42) erg s^-1), into which these merger remnants are expected to evolve. We do not see evidence that the X-ray halos of these galaxies are currently being regenerated to the masses and luminosities seen in typical elliptical galaxies. The mass of atomic gas available to fall back into the main bodies of these galaxies and shock-heat to X-ray temperatures is insufficient for this to be the sole halo regeneration mechanism. We conclude that halo regeneration is most likely a long-term (>10 Gyr) process, occurring predominantly via mass loss from evolving stars, in a sub-sonic outflow stage commencing ~2 Gyr after the merging event., 24 pages, 18 figures, MNRAS accepted. A high resolution graphics version can be downloaded from http://www.sr.bham.ac.uk/~lan/pubs.html
Published: 2004
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12. An XMM-Newton observation of the galaxy group MKW 4

Author: O'Sullivan, E., Vrtilek, J. M., Read, A. M., David, L. P., and Ponman, T. J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present an X-ray study of the galaxy group or poor cluster MKW 4. Working with XMM data we examine the distribution and properties of the hot gas which makes up the group halo. The inner halo shows some signs of structure, with circular or elliptical beta models providing a poor fit to the surface brightness profile. This may be evidence of large scale motion in the inner halo, but we do not find evidence of sharp fronts or edges in the emission. The temperature of the halo declines in the core, with deprojected spectral fits showing a central temperature of ~1.3 keV compared to ~3 keV at 100 kpc. In the central ~30 kpc of the group multi-temperature spectral models are required to fit the data, but they indicate a lack of gas at low temperatures. Steady state cooling flow models provide poor fits to the inner regions of the group and the estimated cooling time of the gas is long except within the central dominant galaxy, NGC 4073. Abundance profiles show a sharp increase in the core of the group, with mean abundance rising by a factor of two in the centre of NGC 4073. Fitting individual elements shows the same trend, with high values of Fe, Si and S in the core. We estimate that ~50% of the Fe in the central 40 kpc was injected by SNIa, in agreement with previous ASCA studies. Using our best fitting surface brightness and temperature models, we calculate the mass, gas fraction, entropy and mass-to-light ratio of the group. At 100 kpc (~0.1 virial radii) the total mass and gas entropy of the system (~2x10^13 Msol and ~300 keV cm^2) are quite comparable to those of other systems of similar temperature, but the gas fraction is rather low (~1%). We conclude that MKW 4 is a fairly relaxed group, which has developed a strong central temperature gradient but not a large-scale cooling flow., Comment: 17 pages, 9 postscript figures, accepted for publication in MNRAS
Published: 2003
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13. Are X-ray properties of loose groups different from those of compact groups?

Author: Helsdon, S. F. and Ponman, T. J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We compare the X-ray properties of loose and compact galaxy groups, using a combined sample of 42 groups. We find that we are unable to separate loose and compact groups on the luminosity-temperature relation, the luminosity-velocity dispersion relation or the velocity dispersion-temperature relation using equally weighted errors. This suggests that the distinction between compact and loose groups is not a fundamental one, and we argue that a more useful distinction is that between X-ray bright and X-ray faint systems. Given their similarity in X-ray properties, we combine the loose and compact subsamples to derive relations based on the full sample. This provides the highest statistical quality results to date on the way in which the correlations in X-ray properties of low mass systems depart from those seen in rich clusters., 6 pages, 6 figures. Accepted for publication in MNRAS
Published: 2000

14. Constraining the Role of SN Ia and SN II in Galaxy Groups by Spatially Resolved Analysis of ROSAT and ASCA Observations

Author: Finoguenov, A. and Ponman, T. J.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We present the results of modelling the distribution of gas properties in the galaxy groups HCG51, HCG62 and NGC5044, and in the poor cluster AWM7, using both ASCA SIS and ROSAT data. The spectral quality of the ASCA data allows the radial distribution in the abundances of several elements to be resolved. In all systems apart from HCG51, we see both central cooling flows, and a general decline in metal abundances with radius. The ratio of iron to alpha-element abundances varies significantly, and in comparison with theoretical supernova yields, indicates a significant contribution to the metal abundance of the intergalactic medium (IGM) from type Ia supernovae. This is seen both within the groups, and also throughout much of the cluster AWM7. The total energy input into the IGM from supernovae can be calculated from our results, and is typically 20-40 per cent of the thermal energy of the gas, mostly from SNe II. Our results support the idea that the SN II ejecta have been more widely distributed in the IGM, probably due to the action of galaxy winds, and the lower iron mass to light ratio in groups suggests that some of this enriched gas has been lost altogether from the shallower potential wells of the smaller systems., Comment: 14 pages, accepted for MNRAS
Published: 1999
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15. Chandra X-Ray Detection of the Radio Hotspots of 3C295

Author: Harris, D. E., Nulsen, P. E. J., Ponman, T. P., Bautz, M., Cameron, R. A., David, L. P., Donnelly, R. H., Forman, W. R., Grego, L., Hardcastle, M. J., Henry, J. P., Jones, C., Leahy, J. P., Markevitch, M., Martel, A. R., McNamara, B. R., Mazzotta, P., Tucker, W., Virani, S. N., and Vrtilek, J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: An observation of the radio galaxy 3C295 during the calibration phase of the Chandra X-ray Observatory reveals X-ray emission from the core of the galaxy, from each of the two prominent radio hotspots, and from the previously known cluster gas. We discuss the possible emission processes for the hotspots and argue that a synchrotron self-Compton model is preferred for most or all of the observed X-ray emission. SSC models with near equipartition fields thus explain the X-ray emission from the hotspots in the two highest surface brightness FRII radio galaxies, Cygnus A and 3C295. This lends weight to the assumption of equipartition and suggests that relativistic protons do not dominate the particle energy density., Comment: 4 pages, 3 figures
Published: 1999
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16. Multi-wavelength observations of an evolved galaxy group: An endpoint of galaxy merging?

Author: Jones, L. R., Ponman, T. J., and Forbes, Duncan A.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The group of galaxies RXJ1340.6+4018 has approximately the same bolometric X-ray luminosity as other bright galaxy groups and poor clusters such as the Virgo cluster. However, 70% of the optical luminosity of the group comes from a dominant giant elliptical galaxy, compared to 5% from M87 in Virgo. The second brightest galaxy in RXJ1340.6+4018 is a factor of 10 fainter (2.5 mag) than the dominant elliptical, and the galaxy luminosity function has a gap at about L*. We interpret the properties of the system as a result of galaxy merging within a galaxy group. We find that the central galaxy lies on the fundamental plane of ellipticals, has an undisturbed, non-cD morphology, and has no spectral features indicative of recent star formation, suggesting that the last major merger occurred >4 Gyr ago. The deviation of the system from the cluster Lx-T relation in the opposite sense to most groups may be due to an early epoch of formation of the group or due to a strong cooling flow. The unusual elongation of the X-ray isophotes and the similarity between the X-ray and optical ellipticities at large radii (~230 kpc) suggest that both the X-ray gas and the outermost stars of the dominant galaxy are responding to an elongated dark matter distribution. RXJ1340.6+4018 may be part of a filamentary structure related to infall in the outskirts of the cluster A1774., 13 pages, 12 figures, to appear in MNRAS
Published: 1999
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17. The Imprint of Galaxy Formation on X-ray Clusters

Author: Ponman, T. J., Cannon, D. B., and Navarro, J. F.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: It is widely believed that structure in the Universe evolves hierarchically, as primordial density fluctuations, amplified by gravity, collapse and merge to form progressively larger systems. The structure and evolution of X-ray clusters, however, seems at odds with this hierarchical scenario for structure formation. Poor clusters and groups, as well as most distant clusters detected to date, are substantially fainter than expected from the tight relations between luminosity, temperature and redshift predicted by these models. Here we show that these discrepancies arise because, near the centre, the entropy of the hot, diffuse intracluster medium (ICM) is higher tha$ achievable through gravitational collapse, indicating substantial non-gravitational heating of the ICM. We estimate this excess entropy for the first time, and argue that it represents a relic of the energetic winds through which forming galaxies polluted the ICM with metals. Energetically, this is onl$ possible if the ICM is heated at modest redshift ($z \ltsim 2$) but prior to cluster collapse, indicating that the formation of galaxies precedes that of clusters and that most clusters have been assembled very recently., 5 pages, plus 2 postscript figures (one in colour), accepted for publication in Nature
Published: 1998

18. The Properties of the Hot Gas in Galaxy Groups and Clusters from 1-D Hydrodynamical Simulations -- I. Cosmological Infall Models

Author: Knight, P. A. and Ponman, T. J.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We report the results of 1-D hydrodynamical modelling of the evolution of gas in galaxy clusters. We have incorporated many of the effects missing from earlier 1-D treatments: improved modelling of the dark matter and galaxy distributions, cosmologically realistic evolution of the cluster potential, and the effects of a multiphase cooling flow. The model utilises a fairly standard 1-D Lagrangian hydrodynamical code to calculate the evolution of the intracluster gas. This is coupled to a theoretical model for the growth of dark matter density perturbations. The main advantages of this treatment over 3-D codes are (1) improved spatial resolution within the cooling flow region, (2) much faster execution time, allowing a fuller exploration of parameter space, and (3) the inclusion of additional physics. In the present paper, we explore the development of infall models -- in which gas relaxes into a deepening potential well -- covering a wide range of cluster mass scales. We find that such simple models reproduce many of the global properties of observed clusters. Very strong cooling flows develop in these 1-D cluster models. In practice, disruption by major mergers probably reduces the cooling rate in most clusters. The models overpredict the gas fraction in low mass systems, indicating the need for additional physical processes, such as preheating or galaxy winds, which become important on small mass scales., Comment: 38 pages, 21 encapsulated postscript figures, accepted for publication in MNRAS
Published: 1997
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19. EUV Emission from Normal Galaxies

Author: Read, A. M. and Ponman, T. J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Using data from the ROSAT Wide Field Camera all-sky survey, we have established upper limits to the extreme ultraviolet (EUV) flux from a sample of 30 bright, nearby, non-active spiral galaxies. These galaxies were chosen to be those most likely to be detected in the EUV on the basis of (i) low interstellar absorption within our own galaxy, (ii) brightness in other wavebands, (iii) high star formation activity, and (iv) proximity. The derived EUV upper limits are restrictive, and establish that the EUV flux escaping from galaxies does not contribute a major component of their bolometric luminosity, and in particular that it is very unlikely to be the sink for the energy injected into the interstellar medium by supernova explosions, as had been suggested following the failure to detect this power in the X-ray band., 10 pages plus 5 figures, uuencoded encapsulated postscript file. Accepted for publication in MNRAS
Published: 1995

20. The XXL survey: first results and future

Author: Pierre, M., Adami, C., Birkinshaw, M., Chiappetti, L., Ettori, S., Evrard, A., Faccioli, L., Gastaldello, F., Giles, P., Horellou, C., Iovino, A., Koulouridis, E., Lidman, C., Brun, A. Le, Maughan, B., Maurogordato, S., McCarthy, I., Miyazaki, S., Pacaud, F., Paltani, S., Plionis, M., Reiprich, T., Sadibekova, T., Smolcic, V., Snowden, S., Surdej, J., Tsirou, M., Vignali, C., Willis, J., Alis, S., Altieri, B., Baran, N., Benoist, C., Bongiorno, A., Bremer, M., Butler, A., Cappi, A., Caretta, C., Ciliegi, P., Clerc, N., Corasaniti, P. S., Coupon, J., Delhaize, J., Delvecchio, I., Democles, J., Desai, Sh., Devriendt, J., Dubois, Y., Eckert, D., Elyiv, A., Farahi, A., Ferrari, C., Fotopoulou, S., Forman, W., Georgantopoulos, I., Guglielmo, V., Huynh, M., Jerlin, N., Jones, Ch., Lavoie, S., Fevre, J. -P. Le, Lieu, M., Kilbinger, M., Marulli, F., Mantz, A., McGee, S., Melin, J. -B., Melnyk, O., Moscardini, L., Novak, M., Piconcelli, E., Poggianti, B., Pomarede, D., Pompei, E., Ponman, T., Ceja, M. E. Ramos, Ranalli, P., Rapetti, D., Raychaudhury, S., Ricci, M., Rottgering, H., Sahlén, M., Sauvageot, J. -L., Schimd, C., Sereno, M., Smith, G. P., Umetsu, K., Valageas, P., Valotti, A., Valtchanov, I., Veropalumbo, A., Ascaso, B., Barnes, D., De Petris, M., Durret, F., Donahue, M., Ithana, M., Jarvis, M., Johnston-Hollitt, M., Kalfountzou, E., Kay, S., La Franca, F., Okabe, N., Muzzin, A., Rettura, A., Ricci, F., Ridl, J., Risaliti, G., Takizawa, M., Thomas, P., Truong, N., Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), University of Bristol [Bristol], Istituto Nazionale di Astrofisica (INAF), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), INAF - Osservatorio Astronomico di Bologna (OABO), University of Michigan [Ann Arbor], University of Michigan System, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Earth and Space Sciences [Göteborg], Chalmers University of Technology [Göteborg], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Anglo-Australian Observatory (AAO), Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), University of Liverpool, National Astronomical Observatory of Japan (NAOJ), Rheinische Friedrich-Wilhelms-Universität Bonn, Department of Physics [Thessaloniki], Aristotle University of Thessaloniki, Argelander-Institut für Astronomie (AlfA), University of Zagreb, NASA Goddard Space Flight Center (GSFC), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, University of Victoria [Canada] (UVIC), Istanbul University, European Space Astronomy Centre (ESAC), European Space Agency (ESA), INAF - Osservatorio Astronomico di Roma (OAR), Department of Physics [Oxford], University of Oxford [Oxford], Max Planck Institute for Extraterrestrial Physics (MPE), Max-Planck-Gesellschaft, Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Indian Institute of Technology [Hyderabad] (IIT Hyderabad), University of Geneva [Switzerland], Uppsala University, INTEGRAL Science Data Center (ISDC), Geneva Observatory, University of Geneva [Switzerland]-University of Geneva [Switzerland], Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Institute for Space Applications and Remote Sensing (ISARS/NOA), National Observatory of Athens (NOA), The University of Western Australia (UWA), University of Bologna, University of Chicago, University of Birmingham [Birmingham], CEA, DSM, SPP, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), INAF - Osservatorio Astronomico di Padova (OAPD), European Southern Observatory (ESO), Lund University [Lund], University of Colorado [Boulder], Inter-University Centre for Astronomy and Astrophysics [Pune] (IUCAA), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, Service de Physique Théorique (SPhT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Yamagata University, Victoria University of Wellington, Roma Tre University, Hiroshima University, York University [Toronto], Department of Physics and Astronomy [Riverside], University of California [Riverside] (UCR), University of California-University of California, Caltech Department of Astronomy [Pasadena], California Institute of Technology (CALTECH), INAF - Osservatorio Astrofisico di Arcetri (OAA), University of Sussex, Università degli Studi di Roma Tor Vergata [Roma], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Smithsonian Institution-Harvard University [Cambridge], Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), National Observatory of Athens, Institute for Space Applications and Remote Sensing, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Jodrell Bank Centre for Astrophysics, Università degli Studi di Roma 'La Sapienza' [Rome], Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Pierre, M, Adami, C., Birkinshaw, M., Chiappetti, L., Ettori, S., Evrard, A., Faccioli, L., Gastaldello, F., Giles, P., Horellou, C., Iovino, A., Koulouridis, E., Lidman, C., Le Brun, A., Maughan, B., Maurogordato, S., Mccarthy, I., Miyazaki, S., Pacaud, F., Paltani, S., Plionis, M., Reiprich, T., Sadibekova, T., Smolcic, V., Snowden, S., Surdej, J., Tsirou, M., Vignali, C., Willis, J., Alis, S., Altieri, B., Baran, N., Benoist, C., Bongiorno, A., Bremer, M., Butler, A., Cappi, A., Caretta, C., Ciliegi, P., Clerc, N., Corasaniti, P.S., Coupon, J., Delhaize, J., Delvecchio, I., Democles, J., Desai, Sh., Devriendt, J., Dubois, Y., Eckert, D., Elyiv, A., Farahi, A., Ferraril, C., Fotopoulou, S., Forman, W., Georgantopoulos, I., Guglielmo, V., Huynh, M., Jerlin, N., Jones, Ch., Lavoie, S., Le Fevre, J.-P., Lieu, M., Kilbinger, M., Marulli, F., Mantz, A., Mcgee, S., Melin, J.-B., Melnyk, O., Moscardini, L., Novak, M., Piconcelli, E., Poggianti, B., Pomarede, D., Pompei, E., Ponman, T., Ramos Ceja, M.E., Rana, P., Rapetti, D., Raychaudhury, S., Ricci, M., Rottgering, H., Sahlen, M., Sauvageot, J.-L., Schimd, C., Sereno, M., Smith, G.P., Umetsu, K., Valageas, P., Valotti, A., Valtchanov, I., Veropalumbo, A., Ascaso, B., Barnes, D., De Petris, M., Durret, F., Donahue, M., Ithana, M., Jarvis, M., Johnston-Hollitt, M., Kalfountzou, E., Kay, S., La Franca, F., Okabe, N., Muzzin, A., Rettura, A., Ricci, F., Ridl, J., Risaliti, G., Takizawa, M., Thomas, P., Truong, N., Corasaniti, P. S., Desai, S. h., Jones, C. h., Le Fevre, J. P., Maruili, F., Melin, J. B., Ramos Ceja, M. E., Sauvageot, J. L., Smith, G. P., Johnston Hollitt, M., LA FRANCA, Fabio, Ricci, Federica, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA), Agence Spatiale Européenne = European Space Agency (ESA), University of Oxford, Université de Genève = University of Geneva (UNIGE), Université de Genève = University of Geneva (UNIGE)-Université de Genève = University of Geneva (UNIGE), Harvard University-Smithsonian Institution, University of Bologna/Università di Bologna, Universiteit Leiden, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Università degli Studi Roma Tre = Roma Tre University (ROMA TRE), University of California [Riverside] (UC Riverside), and University of California (UC)-University of California (UC)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: active, X-ray: general, FOS: Physical sciences, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, XXL survey, Space and Planetary Science, galaxies: clusters: general, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], clusters: general [galaxies], cosmological parameter, X-ray:general, cosmological parameters, general [X-ray], QC, Astrophysics - Cosmology and Nongalactic Astrophysics, QB
Abstract: The XXL survey currently covers two 25 sq. deg. patches with XMM observations of ~10ks. We summarise the scientific results associated with the first release of the XXL data set, that occurred mid 2016. We review several arguments for increasing the survey depth to 40 ks during the next decade of XMM operations. X-ray (z1 cluster density. It will eventually constitute a reference study and an ideal calibration field for the upcoming eROSITA and Euclid missions., Proceeding of the XMM Next Decade Workshop held at ESAC, 9-11 May 2016

21. The effects of similarity breaking on the intracluster medium

Author: Lloyd-Davies, E. J., Richard Bower, and Ponman, T. J.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We construct a family of simple analytical models of galaxy clusters at the present epoch and compare its predictions with observational data. We explore two processes that break the self-similarity of galaxy clusters: systematic variation in the dark matter halo concentration and energy injection into the intracluster gas, through their effects on the observed cluster properties. Three observed relations between cluster properties and temperature are employed to constrain the model; mass, slope of gas density profile (beta) and luminosity. The slope of the mass-temperature relation is found to be reproduced by our model when the observed variation in concentration is included, raising the slope from the self-similar prediction of 1.5, to that of the observed relation, ~ 2. Heating of the gas is observed to have little effect on the mass-temperature relation. The mean trend in the beta-temperature relation is reproduced by energy injection of 0.5-0.75 keV per particle, while concentration variation has only a small effect. Excess energies calculated for individual systems from the beta-temperature relation suggest that the lowest mass systems may have excess energies that are biased to lower values by selection effects. The observed properties of the luminosity-temperature relation are reproduced by the combined effects of excess energy and a trend in the dark matter concentration. At high masses the observed variation in dark matter concentration results a slope of ~ 2.7 compared to recent observations in the range 2.6-2.9, whilst the observed steepening in galaxy groups is predicted when heating of 0.5-0.75 keV per particle is included. Hence a combination of energy injection and dark matter concentration variation appears able to account for the mean trends in the observed relations., 16 pages, 10 figures, submitted for publication in MNRAS

22. The Hot and Energetic Universe: AGN feedback in galaxy clusters and groups

Author: Croston, J. H., Sanders, J. S., Heinz, S., Hardcastle, M. J., Zhuravleva, I., Bîrzan, L., Richard Bower, Brüggen, M., Churazov, E., Edge, A. C., Ettori, S., Fabian, A. C., Finoguenov, A., Kaastra, J., Gaspari, M., Gitti, M., Nulsen, P. E. J., Mcnamara, B. R., Pointecouteau, E., Ponman, T. J., Pratt, G. W., Rafferty, D. A., Reiprich, T. H., Sijacki, D., Worrall, D. M., Kraft, R. P., Mccarthy, I., Wise, M., Fabian, Andrew [0000-0002-9378-4072], Sijacki, Debora [0000-0002-3459-0438], and Apollo - University of Cambridge Repository
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, astro-ph.CO, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, QB, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Mechanical feedback via Active Galactic Nuclei (AGN) jets in the centres of galaxy groups and clusters is a crucial ingredient in current models of galaxy formation and cluster evolution. Jet feedback is believed to regulate gas cooling and thus star formation in the most massive galaxies, but a robust physical understanding of this feedback mode is currently lacking. The large collecting area, excellent spectral resolution and high spatial resolution of Athena+ will provide the breakthrough diagnostic ability necessary to develop this understanding, via: (1) the first kinematic measurements on relevant spatial scales of the hot gas in galaxy, group and cluster haloes as it absorbs the impact of AGN jets, and (2) vastly improved ability to map thermodynamic conditions on scales well-matched to the jets, lobes and gas disturbances produced by them. Athena+ will therefore determine for the first time how jet energy is dissipated and distributed in group and cluster gas, and how a feedback loop operates in group/cluster cores to regulate gas cooling and AGN fuelling. Athena+ will also establish firmly the cumulative impact of powerful radio galaxies on the evolution of baryons from the epoch of group/cluster formation to the present day., Supporting paper for the science theme The Hot and Energetic Universe to be implemented by the Athena+ X-ray observatory (http://www.the-athena-x-ray-observatory.eu). 9 pages, 7 figures

23. The Evolution of Galaxy Clusters Across Cosmic Time

Author: Arnaud, M., Bohringer, H., Jones, C., Mcnamara, B., Ohashi, T., Patnaude, D., Arnaud, K., Bautz, M., Blanchard, A., Bregman, J., Chartas, G., Croston, J., David, L., Donahue, M., Fabian, A., Finoguenov, A., Furuzawa, A., Gallagher, S., Haba, Y., Hornschemeier, A., Heinz, S., Kaastra, J., Kapferer, W., Lamer, G., Mahdavi, A., Makishima, K., Matsushita, K., Nakazawa, K., Paul Nulsen, Ogle, P., Perlman, E., Ponman, T., Proga, D., Pratt, G., Randall, S., Richards, G., Romer, K., Ruszkowski, M., Schmidt, R., Smith, R., Tananbaum, H., Vrtilek, J., and Worrall, D.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The large scale structure of the present Universe is determined by the growth of dark matter density fluctuations and by the dynamical action of dark energy and dark matter. While much progress has been made in recent years in constraining the cosmological parameters, and in reconstructing the evolution in the large--scale structure of the dark matter distribution, we still lack an understanding of the evolution of the baryonic component of the Universe. Located at nodes of the cosmic web, clusters of galaxies are the largest collapsed structures in the Universe with total masses up to 10$^{15}$ M$_{\sun}$. Over 80% of their mass resides in the form of dark matter. The remaining mass is composed of baryons, most of which (about 85%) is a diffuse, hot plasma that radiates primarily in X-rays. X-ray observations of the evolving cluster population provide a unique opportunity to address such open and fundamental questions as: How do hot diffuse baryons dynamically evolve in dark matter potentials? How and when was the excess energy which we observe in the intergalactic medium generated? What is the cosmic history of heavy-element production and circulation? Our current knowledge comes primarily from detailed studies of clusters in the relatively nearby Universe (z$, Comment: Science white paper submitted to the Astro2010 Decadal Survey

24. The Hot and Energetic Universe: The astrophysics of galaxy groups and clusters

Author: Stefano Ettori, Pratt, G. W., Plaa, J., Eckert, D., Nevalainen, J., Battistelli, E. S., Borgani, S., Croston, J. H., Finoguenov, A., Kaastra, J., Gaspari, M., Gastaldello, F., Gitti, M., Molendi, S., Pointecouteau, E., Ponman, T. J., Reiprich, T. H., Roncarelli, M., Rossetti, M., Sanders, J. S., Sun, M., Trinchieri, G., Vazza, F., Arnaud, M., Böringher, H., Brighenti, F., Dahle, H., Grandi, S., Mohr, J. J., Moretti, A., and Schindler, S.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: As the nodes of the cosmic web, clusters of galaxies trace the large-scale distribution of matter in the Universe. They are thus privileged sites in which to investigate the complex physics of structure formation. However, the complete story of how these structures grow, and how they dissipate the gravitational and non-thermal components of their energy budget over cosmic time, is still beyond our grasp. Fundamental questions such as How do hot diffuse baryons accrete and dynamically evolve in dark matter potentials? How and when was the energy that we observe in the ICM generated and distributed? Where and when are heavy elements produced and how are they circulated? are still unanswered. Most of the cluster baryons exists in the form of a diffuse, hot, metal-enriched plasma that radiates primarily in the X-ray band (the intracluster medium, ICM), allowing the X-ray observations of the evolving cluster population to provide a unique opportunity to address these topics. Athena+ with its large collecting area and unprecedented combination of high spectral and angular resolution offers the only way to make major advances in answering these questions. Athena+ will show how the baryonic gas evolves in the dark matter potential wells by studying the motions and turbulence in the ICM. Athena+ will be able to resolve the accreting region both spatially and spectroscopically, probing the true nature and physical state of the X-ray emitting plasma. Athena+ has the capabilities to permit a definitive understanding of the formation and evolution of large-scale cosmic structure through the study of the cluster population., Supporting paper for the science theme The Hot and Energetic Universe to be implemented by the Athena+ X-ray observatory (http://www.the-athena-x-ray-observatory.eu). 10 pages, 5 figures

25. EDGE: explorer of diffuse emission and gamma-ray burst explosions

Author: Piro, L., den Herder, J. W. , Ohashi, T. , Amati, L. , Atteia, J. L. , Barthelmy, S. , Barbera, M. , Barret, D. , Basso, S. , Boer, M. , Borgani, S. , Boyarskiy, Branduardi Raymont, G. , Briggs, M. , Brunetti, Budtz Jorgensen, C. , Burrows, D. , Campana, S. , Caroli, E. , Chincarini, G. , Christensen, F. , Cocchi, M. , Comastri, A. , Corsi, A. , Cotroneo, V. , Conconi, P. , Colasanti, L. , Cusumano, de Rosa, Del Santo, M. , Ettori, S. , Ezoe, Y. , Ferrari, L. , Feroci, M. , Finger, M. , Fishman, G. , Fujimoto, R. , Galeazzi, M. , Galli, A. , Gatti, F. , Gehrels, N. , Gendre, B. , Ghirlanda, G. , Ghisellini, G. , Giommi, P. , Girardi, M. , Guzzo, L. , Haardt, F. , Hepburn, I. , Hermsen, W. , Hoevers, H. , Holland, in't Zand, J. , Ishisaki, Y. , Kawahara, H. , Kawai, N. , Kaastra, J. , Kippen, de Korte, P. A. J. , Kouveliotou, C. , Kusenko, A. , Labanti, C. , Lieu, R. , Macculi, C. , Makishima, K. , Matt, G. , Mazzotta, P. , McCammon, D. , Méndez, M. , Mineo, T. , Mitchell, S. , Mitsuda, K. , Molendi, S. , Moscardini, L. , Mushotzky, R. , Natalucci, L. , Nicastro, F. , O'Brien, P. , Osborne, J. , Paerels, F. , Page, M. , Paltani, S. , Pareschi, G. , Perinati, E. , Perola, C. , Ponman, T. , Rasmussen, A. , Roncarelli, M. , Rosati, P. , Ruchayskiy, O. , Quadrini, E. , Sakurai, I. , Salvaterra, R. , Sasaki, S. , Sato, G. , Schaye, J. , Schmitt, J. , Sciortino, S. , Shaposhnikov, M. , Shinozaki, K. , Spiga, D. , Suto, Y. , Tagliaferri, G. , Takahashi, T. , Takei, Y. , Tawara, Y. , Tozzi, P. , Tsunemi, H. , Tsuru, T. , Ubertini, P. , Ursino, E. , Viel, M. , Vink, J. , White, N. , Willingale, R. , Wijers, R. , Yoshikawa, K. , Yamasaki, BRANCHINI, ENZO FRANCO, Piro, L, den Herder, J W, Ohashi, T, Amati, L, Atteia, J L, Barthelmy, S, Barbera, M, Barret, D, Basso, S, Boer, M, Borgani, S, Boyarskiy, O, Branchini, E, Branduardi-Raymont, G, Briggs, M, Brunetti, G, Budtz-Jorgensen, C, Burrows, D, Campana, S, Caroli, E, Chincarini, G, Christensen, F, Cocchi, M, Comastri, A, Corsi, A, Cotroneo, V, Conconi, P, Colasanti, L, Cusumano, G, de Rosa, A, Del Santo, M, Ettori, S, Ezoe, Y, Ferrari, L, Feroci, M, Finger, M, Fishman, G, Fujimoto, R, Galeazzi, M, Galli, A, Gatti, F, Gehrels, N, Gendre, B, Ghirlanda, G, Ghisellini, G, Giommi, P, Girardi, M, Guzzo, L, Haardt, F, Hepburn, I, Hermsen, W, Hoevers, H, Holland, A, in't Zand, J, Ishisaki, Y, Kawahara, H, Kawai, N, Kaastra, J, Kippen, M, de Korte, P A J, Kouveliotou, C, Kusenko, A, Labanti, C, Lieu, R, Macculi, C, Makishima, K, Matt, G, Mazzotta, P, McCammon, D, Méndez, M, Mineo, T, Mitchell, S, Mitsuda, K, Molendi, S, Moscardini, L, Mushotzky, R, Natalucci, L, Nicastro, F, O'Brien, P, Osborne, J, Paerels, F, Page, M, Paltani, S, Pareschi, G, Perinati, E, Perola, C, Ponman, T, Rasmussen, A, Roncarelli, M, Rosati, P, Ruchayskiy, O, Quadrini, E, Sakurai, I, Salvaterra, R, Sasaki, S, Sato, G, Schaye, J, Schmitt, J, Sciortino, S, Shaposhnikov, M, Shinozaki, K, Spiga, D, Suto, Y, Tagliaferri, G, Takahashi, T, Takei, Y, Tawara, Y, Tozzi, P, Tsunemi, H, Tsuru, T, Ubertini, P, Ursino, E, Viel, M, Vink, J, White, N, Willingale, R, Wijers, R, Yoshikawa, K, Yamasaki, N, JW DEN HERDER, L PIRO, T OHASHI, L AMATI, J ATTEIA, S BARTHELMY, BARBERA M, D BARRET, S BASSO, M BOER, S BORGANI, O BOYARSKIY BRANCHINI, BRANDUARDI-RAYMONT, M BRIGGS, G BRUNETTI, C BUDTZ-JORGENSEN, D BURROWS, S CAMPANA, E CAROLI, F CHRISTENSEN, M COCCHI, A COMASTRI, A CORSI, V COTRONEO, P CONCONI, L COLASANTI, G CUSUMANO, A DE ROSA, M DEL SANTO, S ETTORI, Y EZOE, L FERRARI, M FEROCI, M FINGER, G FISHMAN, R FUJIMOTO, M GALEAZZI, A GALLI, F GATTI, N GEHRELS, B GENDRE, G GHIRLANDA, G GHISELLINI, P GIOMMI, M GIRARDI, L GUZZO, F HAARDT, I HEPBURN, W HERMSEN, H HOEVERS, A HOLLAND, J INT ZAND, Y ISHISAKI, H KAWAHARA, N KAWAI, J KAASTRA, M KIPPEN, PAJ DE KORTE, C KOUVELIOTOU, A KUSENKO, C LABANTI, R LIEU, C MACCULI, K MAKISHIMA, G MATT, P MAZOTTA, D MCCAMMON, M MNDEZ, T MINEO, S MITCHELL, K MITSUDA, S MOLENDI, L MOSCARDINI, R MUSHOTZKY, L NATALUCCI, F NICASTRO, P OBRIEN, J OSBORNE, F PAERELS, M PAGE, S PALTANI, G PARESCHI, E PERINATI, C PEROLA, T PONMAN, A RASMUSSEN, M RONCARELLI, P ROSATI, O RUCHAYSKIY, E QUADRINI, I SAKURAI, R SALVATERRA, S SASAKI, G SATO, J SCHAYE, J SCHMIDTT, S SCIORITINO, M SHAPOOSHNIKOV, K SHINOZAKI, D SPIGA, Y SUTO, G TAGLIAFERRI, T TAKAHASHI, Y TAKEI, Y TAWARA, P TOZZI, H TSUNEMI, T TSURU, P UBERTINI, E URSINO, M VIEL, J VINK, N WHITE, R WILLINGALE, R WIJERS, K YOSHIKAWA, N YAMASAKI, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), European Organization for Nuclear Research (CERN), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), L. Piro, J. W. den Herder, T. Ohashi, L. Amati, J. L. Atteia, S. Barthelmy, M. Barbera, D. Barret, S. Basso, M. Boer, S. Borgani, O. Boyarskiy, E. Branchini, G. Branduardi-Raymont, M. Brigg, G. Brunetti, C. Budtz-Jorgensen, D. Burrow, S. Campana, E. Caroli, G. Chincarini, F. Christensen, M. Cocchi, A. Comastri, A. Corsi, V. Cotroneo, P. Conconi, L. Colasanti, G. Cusumano, A. Rosa, M. Del Santo, S. Ettori, Y. Ezoe, L. Ferrari, M. Feroci, M. Finger, G. Fishman, R. Fujimoto, M. Galeazzi, A. Galli, F. Gatti, N. Gehrel, B. Gendre, G. Ghirlanda, G. Ghisellini, P. Giommi, M. Girardi, L. Guzzo, F. Haardt, I. Hepburn, W. Hermsen, H. Hoever, A. Holland, J. in’t Zand, Y. Ishisaki, H. Kawahara, N. Kawai, J. Kaastra, M. Kippen, P. A. J. Korte, C. Kouveliotou, A. Kusenko, C. Labanti, R. Lieu, C. Macculi, K. Makishima, G. Matt, P. Mazzotta, D. McCammon, M. Méndez, T. Mineo, S. Mitchell, K. Mitsuda, S. Molendi, L. Moscardini, R. Mushotzky, L. Natalucci, F. Nicastro, P. O’Brien, J. Osborne, F. Paerel, M. Page, S. Paltani, G. Pareschi, E. Perinati, C. Perola, T. Ponman, A. Rasmussen, M. Roncarelli, P. Rosati, O. Ruchayskiy, E. Quadrini, I. Sakurai, R. Salvaterra, S. Sasaki, G. Sato, J. Schaye, J. Schmitt, S. Sciortino, M. Shaposhnikov, K. Shinozaki, D. Spiga, Y. Suto, G. Tagliaferri, T. Takahashi, Y. Takei, Y. Tawara, P. Tozzi, H. Tsunemi, T. Tsuru, P. Ubertini, E. Ursino, M. Viel, J. Vink, N. White, R. Willingale, R. Wijer, K. Yoshikawa, N. Yamasaki, High Energy Astrophys. & Astropart. Phys (API, FNWI), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Osservatorio Astronomico di Brera, Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Astronomy, Stephen L. O'Dell, Giovanni Pareschi, den Herder, J. W., Piro, L., Ohashi, T., Amati, L., Atteia, J., Barthelmy, S., Barbera, M., Barret, D., Basso, S., Boer, M., Borgani, S., Boyarskiy, O., Branchini, E., Branduardi-Raymont, G., Briggs, M., Brunetti, G., Budtz-Jorgensenf, C., Burrows, D., Campana, S., Caroli, E., Chincarini, G., Christensen, F., Cocchi, M., Comastri, A., Corsi, A., Cotroneo, V., Conconi, P., Colasanti, L., Cusamano, G., de Rosa, A., Del Santo, M., Ettori, S., Ezoe, Y., Ferrari, L., Feroci, M., Finger, M., Fishman, G., Fujimoto, R., Galeazzi, M., Galli, A., Gatti, F., Gehrels, N., Gendre, B., Ghirlanda, G., Ghisellini, G., Giommi, P., Girardi, M., Guzzo, L., Haardt, F., Hepburn, I., Hermsen, W., Hoevers, H., Holland, A., In't Zand, J., Ishisaki, Y., Kawahara, H., Kawai, N., Kaastra, J., Kippen, M., de Korte, P. A. J., Kouveliotou, C., Kusenko, A., Labanti, C., Lieu, R., Macculi, C., Makishima, K., Matt, G., Mazotta, P., Mccammon, D., Méndez, M., Mineo, T., Mitchell, S., Mitsuda, K., Molendi, S., Moscardini, L., Mushotzky, R., Natalucci, L., Nicastro, F., O'Brien, P., Osborne, J., Paerels, F., Page, M., Paltani, S., Pareschi, G., Perinati, E., Perola, C., Ponman, T., Rasmussen, A., Roncarelli, M., Rosati, P., Ruchayskiy, O., Quadrini, E., Sakurai, I., Salvaterra, R., Sasaki, S., Sato, G., Schaye, J., Schmidtt, J., Scioritino, S., Shaposhnikov, M., Shinozaki, K., Spiga, D., Suto, Y., Tagliaferri, G., Takahashi, T., Takei, Y., Tawara, Y., Tozzi, P., Tsunemi, H., Tsuru, T., Ubertini, P., Ursino, E., Viel, M., Vink, J., White, N., Willingale, R., Wijers, R., Yoshikawa, K., Yamasaki, N., DEN HERDER, J. W. . OHASHI T., Atteia, J. L., Borgani, Stefano, Coauthors, Girardi, Marisa, Den, Herder, J. W., Ohashi, T., Amati, L., Atteia, J. L., Barthelmy, S., Barbera, M., Barret, D., Basso, S., Boer, M., Borgani, S., Boyarskiy, Branchini, ENZO FRANCO, Branduardi, Raymont, G., Brigg, M., Brunetti, Budtz, Jorgensen, C., Burrow, D., Campana, S., Caroli, E., Chincarini, G., Christensen, F., Cocchi, M., Comastri, A., Corsi, A., Cotroneo, V., Conconi, P., Colasanti, L., Cusumano, De, Rosa, Del, Santo, M., Ettori, S., Ezoe, Y., Ferrari, L., Feroci, M., Finger, M., Fishman, G., Fujimoto, R., Galeazzi, M., Galli, A., Gatti, F., Gehrel, N., Gendre, B., Ghirlanda, G., Ghisellini, G., Giommi, P., Girardi, M., Guzzo, L., Haardt, F., Hepburn, I., Hermsen, W., Hoever, H., Holland, In'T, Zand, J., Ishisaki, Y., Kawahara, H., Kawai, N., Kaastra, J., Kippen, De, Korte, P. A. J., Kouveliotou, C., Kusenko, A., Labanti, C., Lieu, R., Macculi, C., Makishima, K., Matt, G., Mazzotta, P., Mccammon, D., Méndez, M., Mineo, T., Mitchell, S., Mitsuda, K., Molendi, S., Moscardini, L., Mushotzky, R., Natalucci, L., Nicastro, F., O'Brien, P., Osborne, J., Paerel, F., Page, M., Paltani, S., Pareschi, G., Perinati, E., Perola, C., Ponman, T., Rasmussen, A., Roncarelli, M., Rosati, P., Ruchayskiy, O., Quadrini, E., Sakurai, I., Salvaterra, R., Sasaki, S., Sato, G., Schaye, J., Schmitt, J., Sciortino, S., Shaposhnikov, M., Shinozaki, K., Spiga, D., Suto, Y., Tagliaferri, G., Takahashi, T., Takei, Y., Tawara, Y., Tozzi, P., Tsunemi, H., Tsuru, T., Ubertini, P., Ursino, E., Viel, M., Vink, J., White, N., Willingale, R., Wijer, R., Yoshikawa, K., Yamasaki, Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3)
Subjects: Vision, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Warm–hot intergalactic medium, Astrophysics, 7. Clean energy, 01 natural sciences, Cosmology, Settore FIS/05 - Astronomia E Astrofisica, Intergalactic Medium, Warm-Hot Intergalactic Medium, X-rays, Cosmology, Clusters, Gamma-ray bursts, Warm-hot intergalactic medium, Missions, 010303 astronomy & astrophysics, X-ray telescopes, X-rays, Clusters, Gamma-ray bursts, Warm– hot intergalactic medium, Missions, Physics, Equipment and services, Satellite Mission, Spectrometers, Astrophysics (astro-ph), X-rays, Cosmology, Clusters, Gamma-ray bursts, Warm–, hot intergalactic medium, Missions, Temperature, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic Vision, Spectral resolution, Galaxy Clusters, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Warm&ndash, Astrophysics::Cosmology and Extragalactic Astrophysics, hot intergalactic medium, Absorption, NO, 010309 optics, X-ray, Galaxy groups and clusters, 0103 physical sciences, Imaging systems, 010306 general physics, Gamma-ray burst, Galaxy cluster, Spatial resolution, Sensors, Astronomy, X-rays, clusters, Gamma-Ray Bursts, Warm-Hot Intergalactic Medium, missions, Astronomy and Astrophysics, Galaxy, Redshift, Cluster, 13. Climate action, Space and Planetary Science
Abstract: How structures on various scales formed and evolved from the early Universe up to present time is a fundamental question of astrophysical cosmology. EDGE will trace the cosmic history of the baryons from the early generations of massive star by Gamma-Ray Burst (GRB) explosions, through the period of cluster formation, down to very low redshifts, when between a third and one half of the baryons are expected to reside in cosmic filaments undergoing gravitational collapse by dark matter (Warm Hot Intragalactic Medium: WHIM). In addition EDGE, with its unprecedented observational capabilities, will provide key results on several other topics. The science is feasible with a medium class mission using existing technology combined with innovative instrumental and observational capabilities on a single satellite by: a) observing with fast reaction Gamma-Ray Bursts with a high spectral resolution (R ~ 500). This enables the study of their (star-forming) environment from the Dark to the local Universe and the use of GRB as back light of large scale cosmological structures b) Observing and surveying extended sources (clusters, WHIM) with high sensitivity using two wide field of view X-ray telescopes (one with a high angular resolution and the other with a high spectral resolution)., This is a low resolution version of the proposal submitted to ESA in response to the Cosmic Vision Call. A high quality version is available at the web address reported in the cover page
Published: 2007

26. The XXL Survey : XXVII. The 3XLSS point source catalogue

Author: Ivan Valtchanov, Michael J. I. Brown, P. Franzetti, E. Elmer, Bruno Altieri, Sinan Aliş, Matt S. Owers, Maria del Carmen Polletta, Bianca M. Poggianti, Ivan K. Baldry, Trevor J. Ponman, Meiert W. Grootes, C. Adami, T. Sadibekova, Angela Bongiorno, Elias Koulouridis, Stéphane Paltani, Florian Pacaud, Christopher Lidman, Manolis Plionis, Jochen Liske, Cristian Vignali, Sotiria Fotopoulou, Glenn Wagner, V. Guglielmo, Simon P. Driver, O. Melnyk, Richard J. Tuffs, Marguerite Pierre, L. Chiappetti, Sophie Maurogordato, A. Iovino, M. Bolzonella, Andrii Elyiv, J. P. Lefevre, L. Faccioli, Aaron S. G. Robotham, E. Pompei, University of St Andrews. School of Physics and Astronomy, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Chiappetti, L., Fotopoulou, S., Lidman, C., Faccioli, L., Pacaud, F., Elyiv, A., Paltani, S., Pierre, M., Plionis, M., Adami, C., Alis, S., Altieri, B., Baldry, I., Bolzonella, M., Bongiorno, A., Brown, M., Driver, S., Elmer, E., Franzetti, P., Grootes, M., Guglielmo, V., Iovino, A., Koulouridis, E., Lefèvre, J.P., Liske, J., Maurogordato, S., Melnyk, O., Owers, M., Poggianti, B., Polletta, M., Pompei, E., Ponman, T., Robotham, A., Sadibekova, T., Tuffs, R., Valtchanov, I., Vignali, C., and Wagner, G.
Subjects: Point source, FOS: Physical sciences, Astrophysics, Surveys, X-rays: general, 01 natural sciences, surveys, general [X-rays], 0103 physical sciences, QB Astronomy, Survey, 010303 astronomy & astrophysics, QC, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astronomy and Astrophysics, DAS, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Redshift, NATURAL SCIENCES. Physics, PRIRODNE ZNANOSTI. Fizika, catalogs, QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Catalog, Catalogs, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present the version of the point source catalogue of the XXL Survey that was used, in part, in the first series of XXL papers. In this paper we release, in our database in Milan and at CDS: (i) the X-ray source catalogue with 26056 objects in two areas of 25 deg2; (ii) the associated multiwavelength catalogues with candidate counterparts of the X-ray sources in the infrared, near-infrared, optical, and ultraviolet (plus spectroscopic redshift when available); and (iii) a catalogue of spectroscopic redshifts recently obtained in the southern XXL area. We also present the basic properties of the X-ray point sources and their counterparts. Other catalogues described in the second series of XXL papers will be released contextually, and will constitute the second XXL data release., Comment: 19 pages, 11 figures, part of A&A Special Issue "The XXL Survey: second series" https://www.aanda.org/component/toc/?task=topic&id=927
Published: 2018

27. The XXL Survey. XXX. Characterisation of the XLSSsC N01 supercluster and analysis of the galaxy stellar populations

Author: August E. Evrard, Angela Bongiorno, Cathy Horellou, Mark Birkinshaw, Elias Koulouridis, Andrii Elyiv, R. J. Tuffs, Sophie Maurogordato, A. Iovino, Fabio Gastaldello, L. Guennou, Aaron S. G. Robotham, Florian Pacaud, Paul Giles, M. E. Ramos Ceja, Jacopo Fritz, Stéphane Paltani, Vernesa Smolčić, T. Sadibekova, Matt S. Owers, Cristian Vignali, Marguerite Pierre, J. Willis, V. Guglielmo, Bianca M. Poggianti, César A. Caretta, Ivan K. Baldry, Andrew M. Hopkins, Trevor J. Ponman, Meiert W. Grootes, Michael J. I. Brown, Manolis Plionis, C. Adami, L. Chiappetti, Alberto Moretti, Benedetta Vulcani, Simon P. Driver, University of St Andrews. School of Physics and Astronomy, Guglielmo, V., Poggianti, B.M., Vulcani, B., Moretti, A., Fritz, J., Gastaldello, F., Adami, C., Caretta, C.A., Willis, J., Koulouridis, E., Ramos Ceja, M.E., Giles, P., Baldry, I., Birkinshaw, M., Bongiorno, A., Brown, M., Chiappetti, L., Driver, S., Elyiv, A., Evrard, A., Grootes, M., Guennou, L., Hopkins, A., Horellou, C., Iovino, A., Maurogordato, S., Owers, M., Pacaud, F., Paltani, S., Pierre, M., Plionis, M., Ponman, T., Robotham, A., Sadibekova, T., Smolčić, V., Tuffs, R., and Vignali, C.
Subjects: PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika, Stellar population, FOS: Physical sciences, Perturbation (astronomy), large-scale structure of Universe, X-rays: galaxies: clusters, galaxies: groups: general, galaxies: evolution, galaxies: star formation, galaxies: stellar content, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, star formation [Galaxies], Virial theorem, Supercluster, Large-scale structure of the universe, 0103 physical sciences, Cluster (physics), NATURAL SCIENCES. Physics. Astronomy and Astrophysics, QB Astronomy, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, 85A04, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, 3rd-DAS, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, groups: general [Galaxies], QC Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, stellar content [Galaxies], galaxies: clusters [X-rays]
Abstract: Superclusters form from the largest enhancements in the primordial density perturbation field and extend for tens of Mpc, tracing the large-scale structure of the Universe. We characterise XLSSsCN01, a rich supercluster at z~0.3 detected in the XXL Survey, composed of X-ray clusters of different virial masses and luminosities. As one of the first studies on this topic, we investigate the stellar populations of galaxies in different environments in the supercluster region. We study a magnitude-limited (r10.8) of galaxies in the virialised region and in the outskirts of 11 XLSSsCN01 clusters, in high- and low-density field. We compute the stellar population properties of galaxies using spectral energy distribution and spectral fitting techniques, and study the dependence of star formation rates (SFR), colours, and stellar ages on environment. For r-12 and with (g-r)_rf10.8, no trends with environment emerge, as massive galaxies are mostly already passive in all environments. No differences among low- and high-density field members and cluster members emerge in the sSFR-mass relation. The luminosity-weighted age-mass relation of the passive populations within cluster virial radii show signatures of recent environmental quenching. The study of luminous and massive galaxies in this supercluster shows that while environment has a prominent role in determining the fractions of SFing/blue galaxies, its effects on the star formation activity in SFing galaxies are negligible., 16 pages, 10 figures, 2 tables, accepted for publication in A&A
Published: 2018

28. The XXL Survey

Author: Paul Giles, Cathy Horellou, Stefano Ettori, Elias Koulouridis, C. Lidman, V. Smolvcic, Mark Birkinshaw, C. Adami, M. Bolzonella, S. Paltani, T. Sadibekova, Matt S. Owers, R. J. Tuffs, Florian Pacaud, L. Chiappetti, B. Garilli, L. Guennou, S. Maurogordato, Jochen Liske, Andrii Elyiv, Trevor J. Ponman, Meiert W. Grootes, A. Iovino, M. E. Ramos Ceja, Mauro Sereno, Michael J. I. Brown, Sean L. McGee, J. L. Willis, Bruno Altieri, I. Valtchanov, Andrew M. Hopkins, Ivan K. Baldry, Angela Bongiorno, S. Fotoupoulou, Aaron S. G. Robotham, Bianca M. Poggianti, V. Guglielmo, Cristian Vignali, Simon P. Driver, August E. Evrard, Fabio Gastaldello, Benedetta Vulcani, M. Plionis, Marco Scodeggio, Marguerite Pierre, University of St Andrews. School of Physics and Astronomy, Guglielmo, V., Poggianti, B.M., Vulcani, B., Adami, C., Gastaldello, F., Ettori, S., Fotoupoulou, S., Koulouridis, E., Ramos Ceja, M.E., Giles, P., McGee, S., Altieri, B., Baldry, I., Birkinshaw, M., Bolzonella, M., Bongiorno, A., Brown, M., Chiappetti, L., Driver, S., Elyiv, A., Evrard, A., Garilli, B., Grootes, M., Guennou, L., Hopkins, A., Horellou, C., Iovino, A., Lidman, C., Liske, J., Maurogordato, S., Owers, M., Pacaud, F., Paltani, S., Pierre, M., Plionis, M., Ponman, T., Robotham, A., Sadibekova, T., Scodeggio, M., Sereno, M., Smolčić, V., Tuffs, R., Valtchanov, I., Vignali, C., Willis, J., Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: luminosity function, mass function [Galaxies], Stellar mass, astro-ph.GA, FOS: Physical sciences, Astrophysics, clusters: general [Galaxies], 01 natural sciences, Virial theorem, galaxies: groups: general, 0103 physical sciences, QB Astronomy, Infrarot-Astrophysik - Abteilung Hinton, 010303 astronomy & astrophysics, QC, luminosity function [galaxies], QB, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 85A04, 010308 nuclear & particles physics, X-ray, DAS, Astronomy and Astrophysics, Virial mass, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, NATURAL SCIENCES. Physics, Redshift, Galaxy, PRIRODNE ZNANOSTI. Fizika, galaxies: luminosity function, groups: general [Galaxies], QC Physics, [SDU]Sciences of the Universe [physics], galaxies: clusters: general, mass function, Space and Planetary Science, Homogeneous, Astrophysics of Galaxies (astro-ph.GA), X-rays: galaxies: clusters, galaxies: luminosity function, mass function, galaxies: clusters [X-rays], Halo, galaxies: evolution
Abstract: The fraction of galaxies bound in groups in the nearby Universe is high (50% at z~0). Systematic studies of galaxy properties in groups are important in order to improve our understanding of the evolution of galaxies and of the physical phenomena occurring within this environment. We have built a complete spectrophotometric sample of galaxies within X-ray detected, optically spectroscopically confirmed groups and clusters (G&C), covering a wide range of halo masses at z, 20 pages, 18 figures, 6 tables, accepted for publication in A&A
Published: 2018

29. Galaxy Cluster Mass Reconstruction Project: II. Quantifying scatter and bias using contrasting mock catalogues

Author: Frazer R. Pearce, Trevor J. Ponman, Ramin A. Skibba, J. C. Muñoz-Cuartas, Michael R. Merrifield, Stuart I. Muldrew, Elmo Tempel, R. R. de Carvalho, Eduardo Rozo, Lyndsay Old, Meghan E. Gray, Daniel Gifford, R. Wojtak, Eli S. Rykoff, Steven P. Bamford, Alexandro Saro, R. J. Pearson, A. von der Linden, Gary A. Mamon, T. Sepp, Peter Behroozi, Darren J. Croton, Cristóbal Sifón, Volker Müller, Old, L., Wojtak, R., Mamon, G. A., Skibba, R. A., Pearce, F. R., Croton, D., Bamford, S., Behroozi, P., de Carvalho, R., Muñoz-Cuartas, J. C., Gifford, D., Gray, M. E., von der Linden, A., Merrifield, M. R., Muldrew, S. I., Müller, V., Pearson, R. J., Ponman, T. J., Rozo, E., Rykoff, E., Saro, A., Sepp, T., Sifón, C., and Tempel, E.
Subjects: statistical [Methods], Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, observation [Cosmology], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, haloe [Galaxies], Set (abstract data type), Range (statistics), Cluster (physics), Galaxies: haloes, Galaxy cluster, Methods: statistical, Astrophysics::Galaxy Astrophysics, Physics, numerical [Methods], Series (mathematics), Methods: numerical, kinematics and dynamic [Galaxies], Cosmology: observations, Galaxies: kinematics and dynamics, Astronomy, Astronomy and Astrophysics, Function (mathematics), Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Halo, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This article is the second in a series in which we perform an extensive comparison of various galaxy-based cluster mass estimation techniques that utilise the positions, velocities and colours of galaxies. Our aim is to quantify the scatter, systematic bias and completeness of cluster masses derived from a diverse set of 25 galaxy-based methods using two contrasting mock galaxy catalogues based on a sophisticated halo occupation model and a semi-analytic model. Analysing 968 clusters, we find a wide range in the RMS errors in log M200c delivered by the different methods (0.18 to 1.08 dex, i.e., a factor of ~1.5 to 12), with abundance matching and richness methods providing the best results, irrespective of the input model assumptions. In addition, certain methods produce a significant number of catastrophic cases where the mass is under- or over-estimated by a factor greater than 10. Given the steeply falling high-mass end of the cluster mass function, we recommend that richness or abundance matching-based methods are used in conjunction with these methods as a sanity check for studies selecting high mass clusters. We see a stronger correlation of the recovered to input number of galaxies for both catalogues in comparison with the group/cluster mass, however, this does not guarantee that the correct member galaxies are being selected. We do not observe significantly higher scatter for either mock galaxy catalogues. Our results have implications for cosmological analyses that utilise the masses, richnesses, or abundances of clusters, which have different uncertainties when different methods are used., 25 pages, 19 figures, 7 tables. Accepted for publication in MNRAS
Published: 2015

30. Galaxy Cluster Mass Reconstruction Project: I. Methods and first results on galaxy-based techniques

Author: Meghan E. Gray, Alexandro Saro, R. J. Pearson, Ramin A. Skibba, Trevor J. Ponman, T. Sepp, Michael R. Merrifield, Darren J. Croton, Elmo Tempel, E. Tundo, Frazer R. Pearce, Stuart I. Muldrew, A. von der Linden, Daniel Gifford, Cristóbal Sifón, Volker Müller, J. C. Muñoz-Cuartas, Yang Wang, Lyndsay Old, Radosław Wojtak, Gary A. Mamon, Old, L., Skibba, R. A., Pearce, F. R., Croton, D., Muldrew, S. I., Muñoz-Cuartas, J. C., Gifford, D., Gray, M. E., von der Linden, A., Mamon, G. A., Merrifield, M. R., Müller, V., Pearson, R. J., Ponman, T. J., Saro, A., Sepp, T., Sifón, C., Tempel, E., Tundo, E., Wang, Y. O., and Wojtak, R.
Subjects: Statistical-galaxie, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Kinematics and dynamics-cosmology, Haloes-galaxies, FOS: Physical sciences, Method, Observation, Clusters, General-galaxies, Methods, Numerical-methods, Observations, Statistical-galaxies, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Halo occupation distribution, Numerical-method, 0103 physical sciences, Cluster (physics), Brightest cluster galaxy, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, General-galaxie, 010308 nuclear & particles physics, Velocity dispersion, Type-cD galaxy, Astronomy and Astrophysic, Haloes-galaxie, Galaxy, Cluster, Substructure, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This paper is the first in a series in which we perform an extensive comparison of various galaxy-based cluster mass estimation techniques that utilise the positions, velocities and colours of galaxies. Our primary aim is to test the performance of these cluster mass estimation techniques on a diverse set of models that will increase in complexity. We begin by providing participating methods with data from a simple model that delivers idealised clusters, enabling us to quantify the underlying scatter intrinsic to these mass estimation techniques. The mock catalogue is based on a Halo Occupation Distribution (HOD) model that assumes spherical Navarro, Frenk and White (NFW) haloes truncated at R_200, with no substructure nor colour segregation, and with isotropic, isothermal Maxwellian velocities. We find that, above 10^14 M_solar, recovered cluster masses are correlated with the true underlying cluster mass with an intrinsic scatter of typically a factor of two. Below 10^14 M_solar, the scatter rises as the number of member galaxies drops and rapidly approaches an order of magnitude. We find that richness-based methods deliver the lowest scatter, but it is not clear whether such accuracy may simply be the result of using an over-simplistic model to populate the galaxies in their haloes. Even when given the true cluster membership, large scatter is observed for the majority non-richness-based approaches, suggesting that mass reconstruction with a low number of dynamical tracers is inherently problematic., 25 pages, 15 figures, 5 tables. Accepted for publication in MNRAS
Published: 2014

31. Substructure of the galaxy clusters in the REXCESS sample: observed statistics and comparison to numerical simulations

Author: G. W. Pratt, Silvia Ameglio, Hans Boehringer, Stefano Borgani, Trevor J. Ponman, Judith H. Croston, Klaus Dolag, M. Arnaud, R. F. Temple, Böhringer, H., Pratt, G. W., Arnaud, M., Borgani, Stefano, Croston, J. H., Ponman, T. J., Ameglio, S., Temple, R. F., and Dolag, K.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Centroid, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Redshift, astrofisica, cosmologia, Space and Planetary Science, Statistics, ROSAT, Cluster (physics), Substructure, Cluster sampling, Astrophysics - High Energy Astrophysical Phenomena, ammassi di galassie, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the substructure statistics of a representative sample of galaxy clusters by means of two currently popular substructure characterisation methods, power ratios and centroid shifts. We use the 31 clusters from the REXCESS sample, compiled from the southern ROSAT All-Sky cluster survey REFLEX with a morphologically unbiased selection in X-ray luminosity and redshift, all of which have been reobserved with XMM-Newton. We investigate the uncertainties of the substructure parameters and examine the dependence of the results on projection effects, finding that the uncertainties of the parameters can be quite substantial. Thus while the quantification of the dynamical state of individual clusters with these parameters should be treated with extreme caution, these substructure measures provide powerful statistical tools to characterise trends of properties in large cluster samples. The centre shift parameter, w, is found to be more sensitive in general. For the REXCESS sample neither the occurence of substructure nor the presence of cool cores depends on cluster mass. There is a significant anti-correlation between the existence of substantial substructure and cool cores. The simulated clusters show on average larger substructure parameters than the observed clusters, a trend that is traced to the fact that cool regions are more pronounced in the simulated clusters, leading to stronger substructure measures in merging clusters and clusters with offset cores. Moreover, the frequency of cool regions is higher in the simulations than in the observations, implying that the description of the physical processes shaping cluster formation in the simulations requires further improvement., Mauscript submitted to Astronomy and Astrophysics, 20 figures
Published: 2010

32. Gas entropy in a representative sample of nearby X-ray galaxy clusters (REXCESS): relationship to gas mass fraction

Author: Hans Boehringer, Judith H. Croston, G. M. Voit, Stefano Borgani, M. Arnaud, R. Piffaretti, Trevor J. Ponman, Richard G. Bower, G. W. Pratt, Pratt, G. W., Arnaud, M., Piffaretti, R., Böhringer, H., Ponman, T. J., Croston, J. H., Voit, G. M., Borgani, Stefano, and Bower, R. G.
Subjects: Physics, education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, FOS: Physical sciences, Astronomy and Astrophysics, Radius, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, ammassi di galassie, cosmologia, Power law, Space and Planetary Science, Entropy (information theory), education, Scaling, Mass fraction, Galaxy cluster, Dimensionless quantity, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: (Abridged) We examine the radial entropy distribution and its scaling using 31 nearby galaxy clusters from the Representative XMM-Newton Cluster Structure Survey (REXCESS). The entropy profiles are robustly measured at least out to R_1000 in all systems and out to R_500 in 13 systems. Compared to theoretical expectations, the observed distributions show a radial and mass-dependent excess entropy that is greater and extends to larger radii in lower mass systems. At R_500, the mass dependence and entropy excess are both negligible within the uncertainties. Mirroring this behaviour, the scaling of gas entropy is shallower than self-similar in the inner regions, but steepens with radius, becoming consistent with self-similar at R_500. The dispersion in scaled entropy in the inner regions is linked to the presence of cool cores and dynamical activity; at larger radii the dispersion decreases by a factor of two and the dichotomy between subsamples disappears. Parameterising the profiles with a power law plus constant model, there are two peaks in central entropy K_0; however, we cannot distinguish between a bimodal or a left-skewed distribution. The outer slopes are correlated with system temperature; their distribution is unimodal with a median value of 0.98. Renormalising the dimensionless entropy profiles by the gas mass fraction profile f_gas(< R), leads to a remarkable reduction in the scatter, implying that gas mass fraction variations with radius and mass are the cause of the observed entropy properties. We discuss a tentative scenario to explain the behaviour of the entropy and gas mass fraction in the REXCESS sample, in which extra heating and merger mixing maintains an elevated central entropy level in the majority of the population, and a smaller fraction of systems develops a cool core., 14 pages, 9 figures, A&A, in press. Final version corrects Eqn. 3 and columns 5-8 in Table 1 and has additional minor text clarifications
Published: 2010

33. Entropy amplification from energy feedback in simulated galaxy groups and clusters

Author: Trevor J. Ponman, Stefano Borgani, Scott T. Kay, Volker Springel, Paolo Tozzi, G. M. Voit, Alexis Finoguenov, Borgani, Stefano, Finoguenov, A., Kay, S. T., Ponman, T. J., Springel, V., Tozzi, P., and Voit, G. M.
Subjects: Physics, Radiative cooling, Star formation, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift, Cosmology, Supernova, Galaxy groups and clusters, Space and Planetary Science, numerical simulation, galaxy cluster [X-rays], Entropy (energy dispersal), Adiabatic process, Galaxy cluster, Astrophysics::Galaxy Astrophysics
Abstract: We use hydrodynamical simulations of galaxy clusters and groups to study the effect of pre-heating on the entropy structure of the ICM. Our simulations account for non-gravitational heating of the gas either by imposing a minimum entropy floor at redshift z=3, or by considering feedback by galactic winds powered by supernova (SN) energy. In the adiabatic simulations we find that the entropy is increased out to the external regions as a consequence of the transition from clumpy to smooth accretion induced by extra heating. This result is in line with the predictions of the semi-analytical model by Voit et al. However, the introduction of radiative cooling substantially reduces this entropy amplification effect. While galactic winds of increasing strength are effective in regulating star formation, they have a negligible effect on the entropy profile of cluster-sized halos. Only in models where the action of the winds is complemented with diffuse heating corresponding to a pre-collapse entropy do we find a sizable entropy amplification out to the virial radius of the groups. Observational evidence for entropy amplification in the outskirts of galaxy clusters and groups therefore favours a scenario for feedback that distributes heating energy in a more diffuse way than predicted by the model for galactic winds from SN explosions explored here., Comment: 12 pages, 7 figures to appear in MNRAS. Full resolution preprint available at http://adlibitum.oat.ts.astro.it/clustersim/EntrAmpl/borgani_2.ps.gz
Published: 2005
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34. XMM-Newton First-Light Observations of the Hickson Galaxy Group 16

Author: James Reeves, R. G. Griffiths, S. Dos Santos, C. V. Goodall, R. Lainé, William C. Priedhorsky, J. Clavel, S. Vercellone, Jean-François Hochedez, F. A. Cordova, L. Vigroux, Lothar Strüder, Joachim Trümper, P. Salvetat, F. A. Jansen, Simona Ghizzardi, Trevor J. Ponman, N. La Palombara, E. Kendziorra, Ulrich G. Briel, P. Dhez, Gabriele E. Villa, I. Butler, Keith O. Mason, Marco Barbera, J. L. Sauvageot, Martin J. L. Turner, D. Schmitt, Andrew D. Holland, R. Rothenflug, M. Boer, C. Pigot, A. Lagostina, M. Trifoglio, S. Molendi, Steven Sembay, P. Ferrando, Monique Arnaud, A. Short, P. J. Bennie, Claus Reppin, M. Lortholary, Martin Ward, Turner, M., Reeves, J., Ponman, T., Arnaud, M., Barbera, M., Bennie, P., Boer, M., Briel, U., Butler, I., Clavel, J., Dhez, P., Cordova, F., Dos Santos, S., Ferrando, P., Ghizzardi, S., Goodall, C., Griffiths, R., Hochedez, J., Holland, A., Jansen, F., Kendziorra, E., Lagostina, A., Laine, R., La Palombara, N., Lortholary, M., Mason, K., Molendi, S., Pigot, C., Priedhorsky, W., Reppin, C., Rothenflug, R., Salvetat, P., Sauvageot, J., Schmitt, D., Sembay, S., Short, A., Strüder, L., Trifoglio, M., Trümper, J., Vercellone, S., Vigroux, L., Villa, G., and Ward, M.
Subjects: Physics, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Continuum (design consultancy), FOS: Physical sciences, Astronomy and Astrophysics, Galaxies: active, Astrophysics, First light, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, Galaxy, Universe, Redshift, Compact group, Space and Planetary Science, Galaxy group, Galaxies: starburst, X-rays: galaxie, Astrophysics::Galaxy Astrophysics, media_common
Abstract: This paper presents the XMM-Newton first-light observations of the Hickson-16 compact group of galaxies. Groups are possibly the oldest large-scale structures in the Universe, pre-dating clusters of galaxies, and are highly evolved. This group of small galaxies, at a redshift of 0.0132 (or 80 Mpc) is exceptional in the having the highest concentration of starburst or AGN activity in the nearby Universe. So it is a veritable laboratory for the study of the relationship between galaxy interactions and nuclear activity. Previous optical emission line studies indicated a strong ionising continuum in the galaxies, but its origin, whether from starbursts, or AGN, was unclear. Combined imaging and spectroscopy with the EPIC X-ray CCDs unequivocally reveals a heavily obscured AGN and a separately identified thermal (starburst) plasma, in NGC 835, NGC 833 and NGC 839. NGC 838 shows only starburst thermal emission. Starbursts and AGN can evidently coexist in members of this highly evolved system of merged and merging galaxies, implying a high probability for the formation of AGN as well as starbursts in post-merger galaxies., 6 pages, accepted for publication in A&A Special Letters Edition (First results from XMM-Newton)
Published: 2000

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34 results on '"Ponman, T."'

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34. XMM-Newton First-Light Observations of the Hickson Galaxy Group 16

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