Search

Your search keyword '"van de Voort F"' showing total 178 results
Start Over Author "van de Voort F"
178 results on '"van de Voort F"'

2. Strongly Time-Variable Ultra-Violet Metal Line Emission from the Circum-Galactic Medium of High-Redshift Galaxies

Author

Sravan, N., Faucher-Giguere, C. -A., van de Voort, F., Keres, D., Muratov, A. L., Hopkins, P. F., Feldmann, R., Quataert, E., and Murray, N.

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

We use cosmological simulations from the Feedback In Realistic Environments (FIRE) project, which implement a comprehensive set of stellar feedback processes, to study ultra-violet (UV) metal line emission from the circum-galactic medium of high-redshift (z=2-4) galaxies. Our simulations cover the halo mass range Mh ~ 2x10^11 - 8.5x10^12 Msun at z=2, representative of Lyman break galaxies. Of the transitions we analyze, the low-ionization C III (977 A) and Si III (1207 A) emission lines are the most luminous, with C IV (1548 A) and Si IV (1394 A) also showing interesting spatially-extended structures. The more massive halos are on average more UV-luminous. The UV metal line emission from galactic halos in our simulations arises primarily from collisionally ionized gas and is strongly time variable, with peak-to-trough variations of up to ~2 dex. The peaks of UV metal line luminosity correspond closely to massive and energetic mass outflow events, which follow bursts of star formation and inject sufficient energy into galactic halos to power the metal line emission. The strong time variability implies that even some relatively low-mass halos may be detectable. Conversely, flux-limited samples will be biased toward halos whose central galaxy has recently experienced a strong burst of star formation. Spatially-extended UV metal line emission around high-redshift galaxies should be detectable by current and upcoming integral field spectrographs such as the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope and Keck Cosmic Web Imager (KCWI)., Comment: 16 pages, 8 figures, accepted for publication in MNRAS

Published
2015
Full Text
View/download PDF

3. ORIGIN: Metal Creation and Evolution from the Cosmic Dawn

Author

Herder, J. W. den, Piro, L., Ohashi, T., Kouveliotou, C., Hartmann, D. H., Kaastra, J. S., Amati, L., Andersen, M. I., Arnaud, M., Attéia, 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., 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., Hartog, R. den, Hepburn, I., Hermsen, W., Hjorth, J., Hoekstra, H., Holland, A., Hornstrup, A., van der Horst, A., Hoshino, A., Zand, J. in 't, 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, M. Mas, Matsushita, K., Mazzotta, P., McCammon, D., Méndez, 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., Röttgering, 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
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

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., Comment: 34 pages, 13 figures. ESA Cosmic Vision medium-class mission (M3) proposal. Accepted for publication in Experimental Astronomy. Including minor corrections in the author list

Published
2011
Full Text
View/download PDF

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

Author

den Herder, Jan-Willem, Piro, Luigi, Ohashi, Takaya, Kouveliotou, Chryssa, Hartmann, Dieter H., Kaastra, Jelle S., Amati, L., Andersen, M. I., Arnaud, M., Attéia, 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., 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, M. Mas, Matsushita, K., Mazzotta, P., McCammon, D., Méndez, 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., Röttgering, 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.

Published
2012
Full Text
View/download PDF

8. AlFoCS + Fornax3D:resolved star formation in the Fornax cluster with ALMA and MUSE

Author

Zabel, N. (N.), Davis, T. A. (T. A.), Sarzi, M. (M.), Nedelchev, B. (Boris), Chevance, M. (M.), Kruijssen, M. D. (M. Diederik), Iodice, E. (E.), Baes, M. (M.), Bendo, G. J. (G. J.), Corsini, E. M. (E. Maria), De Looze, I. (I.), de Zeeuw, P. T. (P. Tim), Gadotti, D. A. (D. A.), Grossi, M. (M.), Peletier, R. (R.), Pinna, F. (F.), Serra, P. (Paolo), van de Voort, F. (F.), Venhola, A. (A.), Viaene, S. (S.), Vlahakis, C. (C.), Zabel, N. (N.), Davis, T. A. (T. A.), Sarzi, M. (M.), Nedelchev, B. (Boris), Chevance, M. (M.), Kruijssen, M. D. (M. Diederik), Iodice, E. (E.), Baes, M. (M.), Bendo, G. J. (G. J.), Corsini, E. M. (E. Maria), De Looze, I. (I.), de Zeeuw, P. T. (P. Tim), Gadotti, D. A. (D. A.), Grossi, M. (M.), Peletier, R. (R.), Pinna, F. (F.), Serra, P. (Paolo), van de Voort, F. (F.), Venhola, A. (A.), Viaene, S. (S.), and Vlahakis, C. (C.)

Abstract

We combine data from ALMA and MUSE to study the resolved (∼300 pc scale) star formation relation (star formation rate, SFR, versus molecular gas surface density) in cluster galaxies. Our sample consists of nine Fornax cluster galaxies, including spirals, ellipticals, and dwarfs, covering a stellar mass range of ∼10⁸.⁸–10¹¹ M⊙. CO(1–0) and extinction corrected Hα were used as tracers for the molecular gas mass and SFR, respectively. We compare our results with Kennicutt and Bigiel et al. Furthermore, we create depletion time maps to reveal small-scale variations in individual galaxies. We explore these further in FCC290, using the ‘uncertainty principle for star formation’ (Kruijssen & Longmore) to estimate molecular cloud lifetimes, which we find to be short (<10 Myr) in this galaxy. Galaxy-averaged depletion times are compared with other parameters such as stellar mass and cluster-centric distance. We find that the star formation relation in the Fornax cluster is close to those from Kennicutt and Bigiel et al., but overlaps mostly with the shortest depletion times predicted by Bigiel et al. This slight decrease in depletion time is mostly driven by dwarf galaxies with disturbed molecular gas reservoirs close to the virial radius. In FCC90, a dwarf galaxy with a molecular gas tail, we find that depletion times are a factor ≳10 higher in its tail than in its stellar body.

Published
2020

20. AlFoCS + Fornax3D: resolved star formation in the Fornax cluster with ALMA and MUSE

Author

Zabel, N, primary, Davis, T A, primary, Sarzi, M, primary, Nedelchev, Boris, primary, Chevance, M, primary, Kruijssen, J M Diederik, primary, Iodice, E, primary, Baes, M, primary, Bendo, G J, primary, Corsini, E Maria, primary, De Looze, I, primary, de Zeeuw, P Tim, primary, Gadotti, D A, primary, Grossi, M, primary, Peletier, R, primary, Pinna, F, primary, Serra, Paolo, primary, van de Voort, F, primary, Venhola, A, primary, Viaene, S, primary, and Vlahakis, C, primary

Published
2020
Full Text
View/download PDF

31. The ALMA Fornax Cluster Survey I:stirring and stripping of the molecular gas in cluster galaxies

Author

Zabel, N. (Nikki), Davis, T. A. (Timothy A.), Smith, M. W. (Matthew W. L.), Maddox, N. (Natasha), Bendo, G. J. (George J.), Peletier, R. (Reynier), Iodice, E. (Enrichetta), Venhola, A. (Aku), Baes, M. (Maarten), Davies, J. I. (Jonathan I.), de Looze, I. (Ilse), Gomez, H. (Haley), Grossi, M. (Marco), Kenney, J. D. (Jeffrey D. P.), Serra, P. (Paolo), van de Voort, F. (Freeke), Vlahakis, C. (Catherine), Young, L. M. (Lisa M.), Zabel, N. (Nikki), Davis, T. A. (Timothy A.), Smith, M. W. (Matthew W. L.), Maddox, N. (Natasha), Bendo, G. J. (George J.), Peletier, R. (Reynier), Iodice, E. (Enrichetta), Venhola, A. (Aku), Baes, M. (Maarten), Davies, J. I. (Jonathan I.), de Looze, I. (Ilse), Gomez, H. (Haley), Grossi, M. (Marco), Kenney, J. D. (Jeffrey D. P.), Serra, P. (Paolo), van de Voort, F. (Freeke), Vlahakis, C. (Catherine), and Young, L. M. (Lisa M.)

Abstract

We present the first results of the ALMA Fornax Cluster Survey: a complete ALMA survey of all members of the Fornax galaxy cluster that were detected in H i or in the far-infrared with Herschel. The sample consists of a wide variety of galaxy types, ranging from giant ellipticals to spiral galaxies and dwarfs, located in all (projected) areas of the cluster. It spans a mass range of 10∼8.5–11 M⊙. The CO(1–0) line was targeted as a tracer for the cold molecular gas, along with the associated 3 mm continuum. CO was detected in 15 of the 30 galaxies observed. All 8 detected galaxies with stellar masses below 3 × 109 M⊙ have disturbed molecular gas reservoirs; only 7 galaxies are regular/undisturbed. This implies that Fornax is still a very active environment, having a significant impact on its members. Both detections and non-detections occur at all projected locations in the cluster. Based on visual inspection, and the detection of molecular gas tails in alignment with the direction of the cluster centre, in some cases ram pressure stripping is a possible candidate for disturbing the molecular gas morphologies and kinematics. Derived gas fractions in almost all galaxies are lower than expected for field objects with the same mass, especially for the galaxies with disturbed molecular gas, with differences of sometimes more than an order of magnitude. The detection of these disturbed molecular gas reservoirs reveals the importance of the cluster environment for even the tightly bound molecular gas phase.

Published
2019

34. The origin of the diverse morphologies and kinematics of MilkyWay-mass galaxies in the FIRE-2 simulations

Author

Garrison-Kimmel, S, Hopkins, PF, Wetzel, A, El-Badry, K, Sanderson, RE, Bullock, JS, Ma, X, van de Voort, F, Hafen, Z, Faucher-Giguère, CA, Hayward, CC, Quataert, E, Kereš, D, and Boylan-Kolchin, M

Subjects
Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. We use hydrodynamic cosmological zoom-in simulations from the Feedback in Realistic Environments project to explore the morphologies and kinematics of 15 Milky Way (MW)- mass galaxies. Our sample ranges from compact, bulge-dominated systems with 90 per cent of their stellar mass within 2.5 kpc to well-ordered discs that reach ≳15 kpc. The gas in our galaxies always forms a thin, rotation-supported disc at z = 0, with sizes primarily determined by the gas mass. For stars, we quantify kinematics and morphology both via the fraction of stars on disc-like orbits and with the radial extent of the stellar disc. In this mass range, stellar morphology and kinematics are poorly correlated with the properties of the halo available from dark matter-only simulations (halo merger history, spin, or formation time). They more strongly correlate with the gaseous histories of the galaxies: those that maintain a high gas mass in the disc after z ~ 1 develop well-ordered stellar discs. The best predictor of morphology we identify is the spin of the gas in the halo at the time the galaxy formed 1/2 of its stars (i.e. the gas that builds the galaxy). High-z mergers, before a hot halo emerges, produce some of the most massive bulges in the sample (from compact discs in gas-rich mergers), while later-forming bulges typically originate from internal processes, as satellites are stripped of gas before the galaxies merge. Moreover, most stars in z = 0 MW-mass galaxies (even z = 0 bulge stars) form in a disc: ≳60-90 per cent of stars begin their lives rotationally supported.

Published
2018
Full Text
View/download PDF

36. 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
Full Text
View/download PDF

37. Microwave heating characteristics of rutile.

Author

Kudra, T., Raghavan, G. S. V., and van de Voort, F. R.

Subjects
THERMOPHYSICAL properties, RUTILE, ORES
Abstract

Presents a study that determined thermophysical properties of rutile ore and used to quantify the heating effect due to microwave absorption. Materials and methods; Results of the study; Conclusions.

Published
1993
Full Text
View/download PDF

38. Potential of determining moisture content in mineral insulating oil by fourier transform infrared spectroscopy

Author

Hadjadj, Yazid, Fofana, Issouf, van de Voort, F. R., Bussières, Denis, Hadjadj, Yazid, Fofana, Issouf, van de Voort, F. R., and Bussières, Denis

Abstract

Transformer oils are vulnerable to moisture, which can have adverse effects including a dramatic reduction in dielectric strength, accelerating the aging of the solid insulation (cellulose depolymerization) and the formation of decompositional gasses at high temperatures. Moisture may be generated inside the transformer due to degradation of the oil-paper insulation or there may be ingress of moisture due to free-breathing arrangements. A moisture content exceeding 50% of oil saturation greatly reduces the breakdown voltage, resulting in catastrophic failures as well as the potential for transformer fires [1]. The detrimental effect of water within a transformer is not only limited to the breakdown voltage of the oil. The rate of degradation of paper insulation increases in direct proportion to the water content [2], [3]. Moisture also has a decisive effect on the maximum temperature that the transformer can run at before moisture-induced failure occurs. Consequently, transformer life expectancy can be calculated from water content and temperature [3]. A failure of transformer accessories such as condenser bushings sometimes leads to a transformer failure and long-term outage. Often, moisture is a cause of explosion for service-aged bushings.

Published
2016

40. ORIGIN: Metal Creation and Evolution from the Cosmic Dawn

Author

den Herder, Jan-Willem, Piro, Luigi, 大橋, 隆哉, 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., 江副, 祐一郎, Ferrari, L., Finger, H., Figueroa-Feliciano, T., Friedrich, P., 藤本, 龍一, 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., 星野, 晶夫, int Zand, J., Irwin, K., 石崎, 欣尚, 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., 満田, 和久, 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., 竹井, 洋, Tanvir, N., 田代, 信, 田村, 隆幸, 田原, 譲, Troja, E., 辻本, 匡弘, 鶴, 剛, 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., 山崎, 典子, 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, Jan-Willem, Piro, Luigi, 大橋, 隆哉, 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., 江副, 祐一郎, Ferrari, L., Finger, H., Figueroa-Feliciano, T., Friedrich, P., 藤本, 龍一, 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., 星野, 晶夫, int Zand, J., Irwin, K., 石崎, 欣尚, 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., 満田, 和久, 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., 竹井, 洋, Tanvir, N., 田代, 信, 田村, 隆幸, 田原, 譲, Troja, E., 辻本, 匡弘, 鶴, 剛, 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., 山崎, 典子, 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, and Yamasaki, Noriko

Abstract

著者人数: 159名, Accepted: 2011-04-11

Published
2015

43. Cold accretion flows and the nature of high column density H I absorption at redshift 3

Author

van de Voort, F., Schaye, J., Altay, G., and Theuns, Tom

Subjects
absorption lines [Quasars], high‐redshift [Galaxies], theory. [Cosmology], Astrophysics::Cosmology and Extragalactic Astrophysics, evolution [Galaxies], formation [Galaxies], Astrophysics::Galaxy Astrophysics, Intergalactic medium
Abstract

Simulations predict that galaxies grow primarily through the accretion of gas that has not gone through an accretion shock near the virial radius and that this cold gas flows towards the central galaxy along dense filaments and streams. There is, however, little observational evidence for the existence of these cold flows. We use a large, cosmological, hydrodynamical simulation that has been post‐processed with radiative transfer to study the contribution of cold flows to the observed z= 3 column density distribution of neutral hydrogen, which our simulation reproduces. We find that nearly all of the H I absorption arises in gas that has remained colder than 105.5 K, at least while it was extragalactic. In addition, the majority of the H I is falling rapidly towards a nearby galaxy, with non‐negligible contributions from outflowing and static gas. Above a column density of Graphic cm−2, most of the absorbers reside inside haloes, but the interstellar medium only dominates for Graphic cm−2. Haloes with total mass below 1010 M⊙ dominate the absorption for Graphic cm−2, but the average halo mass increases sharply for higher column densities. Although very little of the H I in absorbers with Graphic cm−2 resides inside galaxies, systems with Graphic cm−2 are closely related to star formation: most of their H I either will become part of the interstellar medium before z= 2 or has been ejected from a galaxy at z > 3. Cold accretion flows are critical for the success of our simulation in reproducing the observed rate of incidence of damped Lyman‐α and particularly that of Lyman limit systems. We therefore conclude that cold accretion flows exist and have already been detected in the form of high column density H I absorbers.

Published
2012

49. Regulatory Infrared Spectroscopic Method for the Rapid Determination of Total Isolated Trans Fat: A Collaborative Study

Author

Mossoba, M. M., primary, Seiler, A., additional, Steinhart, H., additional, Kramer, J. K. G., additional, Rodrigues-Saona, L., additional, Griffith, A. P., additional, Pierceall, R., additional, van de Voort, F. R., additional, Sedman, J., additional, Ismail, A. A., additional, Barr, D., additional, Da Costa Filho, P. A., additional, Li, H., additional, Zhang, Y., additional, Liu, X., additional, and Bradley, M., additional

Published
2010
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results