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7 results on '"P. Predehl"'

1. XMM-Newton and Chandra High Resolution X-Ray Spectroscopy of Magnetic Cataclysmic Variables and Low Mass X-Ray Binaries

Author

V. Burwitz, K. Dennerl, F. Haberl, P. Predehl, K. Reinseh, and B. Stelzer

Subjects
Astronomy, QB1-991
Abstract

Here we discuss the helium-like triplet plasma diagnostic method that can be applied to high resolution X-ray spectra of magnetic CVs and low mass X-ray binaries obtained with the high-resolution spectrographs on the ESA satellite XMM-Newton and the NASA satellite Chandra . The two observations of Her X-1 obtained with the Chandra Low Energy Transmission Grating (LETGS), one lasting 30 ks during the anomalous low state (ALS) and the other 20 ks during main on just before eclipse ingress. During the ALS and the pre-eclipse dips only the intercombination line of the He-like O VII and N VI triplets are detected. Thus the resonance line must be scattered out of the line of sight indicating an optical depth of ῖ- > 1. The missing forbidden lines give for collisional plasma a lower limit for density of ne > 10 11….12 cm -3 and for the temperature of T ~ 10 6,0….6,5 K. These constraints require the corona to be at a distance r ~ 10 10-11 cm from the central source. XMM-Newton RGS spectra during similar states show exactly the same He-like triplet structure as the Chandra observations. For the magnetic CVs AM Her and PQ Gem the most remarcable result is that the lines emitted in the post-shock flow from the cooling hot plasma are strongly broadned. The most likely reason for this is the Doppler-shifting of the lines due to the changing angle between the observer and the accretion column as the white dwarf rotates. The maximum detectable shift in the case of AM her is of the order of 750 km/s.

Published
2017
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2. On Flamsteed's supernova Cas A

Author

D.H. Hartmann, P. Predehl, J. Greiner, R. Egger, J. Trümper, B. Aschenbach, A.F. Iyudin, R.D. Diehl, U. Oberlack, V. Schönfelder, M.D. Leising, L.-S. The, F.X. Timmes, S.E. Woosley, R. Hoffman, N. Langer, and G. Garcia-Segura

Subjects
Physics, Nuclear and High Energy Physics, Line-of-sight, Opacity, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Near-Earth supernova, Supernova, ROSAT, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Halo, Supernova remnant, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

The Galactic supernova remnant Cas A is believed to be the result of a recent (∼ 300 yrs) and nearby (D ∼ 3 kpc) explosion of a massive star. The discovery of gamma-ray line emission due to radioactive 44 Ti with COMPTEL supports the massive star origin of Cas A. However, the ejection of 44 Ti should be accompanied by large amounts of 56 Ni and 57 Ni, which would have made this a very bright supernova. No 17th century sightings of this event exist, with the notable exception of the ∼ 6th mag star 3 Cas reported by Sir John Flamsteed. This mystery may be solved by assuming that the supernova was enshrouded by a dusty envelope, perhaps provided by a pre-supernova wind. X-ray observations with ROSAT provide evidence for this scenario through the simultaneous analysis of absorption along the line of sight and the extended X-ray scattering halo around Cas A. The supernova shock destroyed the dust, reducing the line-of-sight opacity to a value consistent with a 3 kpc path through an average ISM. ROSAT detects the evaporated dust as excess absorption.

Published
1997
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3. [Untitled]

Author

P. Predehl

Subjects
Physics, Scattering, Astrophysics::High Energy Astrophysical Phenomena, Extinction (astronomy), Interstellar cloud, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Dust lane, Supernova, Interplanetary dust cloud, Space and Planetary Science, Circumstellar dust, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Cosmic dust
Abstract

The interaction of X-rays with interstellar dust leads to small angle scattering. X-ray sources behind sufficiently dense dust columns are therefore surrounded by haloes of faint and diffuse X-ray emission. Since these X-ray sources are also highly absorbed, X-ray observations offer the unique opportunity to measure both components of interstellar extinction simultaneously. This method provides an excellent means of determining interstellar gas to dust ratios, a differentiation between interstellar and circumstellar matter, and, last but not least, a clue to the physical nature of dust itself. In particular we have a plausible explanation why the supernova- explosion in Cassiopaea 300 years ago, of which we know today the remnant Cas A, has not been seen. Furthermore, we find that dust grains must be ‘fluffy’ or porous with voids up to 70%.

Published
1997
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4. ART-XC: a medium-energy x-ray telescope system for the Spectrum-R-Gamma mission

Author

V. Arefiev, M. Pavlinsky, I. Lapshov, A. Tkachenko, S. Sazonov, M. Revnivtsev, N. Semena, M. Buntov, A. Vikhlinin, M. Gubarev, S. O'Dell, B. Ramsey, S. Romaine, D. Swartz, M. Weisskopf, G. Hasinger, P. Predehl, S. Grigorovich, D. Litvin, N. Meidinger, and L. W. Strüder

Subjects
Physics, X-ray astronomy, Photon, Active galactic nucleus, business.industry, Detector, Astronomy, Field of view, X-ray telescope, Gamma-ray astronomy, law.invention, Telescope, Optics, law, business
Abstract

The ART-XC instrument is an X-ray grazing-incidence telescope system in an ABRIXAS-type optical configuration optimized for the survey observational mode of the Spectrum-RG astrophysical mission which is scheduled to be launched in 2011. ART-XC has two units, each equipped with four identical X-ray multi-shell mirror modules. The optical axes of the individual mirror modules are not parallel but are separated by several degrees to permit the four modules to share a single CCD focal plane detector, 1/4 of the area each. The 450-micron-thick pnCCD (similar to the adjacent eROSITA telescope detector) will allow the detection of X-ray photons up to 15 keV. The field of view of the individual mirror module is about 18×18 arcminutes2 and the sensitivity of the ART-XC system for 4 years of survey will be better than 10-12 erg s-1 cm-2 over the 4-12 keV energy band. This will allow the ART-XC instrument to discover several thousands new AGNs.

Published
2008
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5. The Galactic Center

Author

P. Predehl

Subjects
Physics, Molecular cloud, Galactic Center, Astronomy, Galactic plane, Supernova remnant
Published
2008
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6. The ROSAT Mission

Author

B. Aschenbach, H. Bräuninger, U. Briel, W. Brinkmann, H. Fink, N. Heinecke, H. Hippmann, G. Kettenring, G. Metzner, A. Ondrusch, E. Pfeffermann, P. Predehl, G. Reger, K.-H. Stephan, J. Trümper, and H. U. Zimmermann

Subjects
Physics, X-ray astronomy, Einstein Telescope, media_common.quotation_subject, Astronomy, X-ray telescope, Astrophysics, law.invention, Telescope, Sky, law, Orders of magnitude (luminous flux), ROSAT, Large Magellanic Cloud, media_common
Abstract

The primary scientific objective of the ROSAT mission is to perform the first all sky survey with an imaging X-ray telescope leading to an improvement in sensitivity by several orders of magnitude compared with previous surveys. Consequently a large number of new sources (> 105) will be discovered and located with an accuracy of 1 arcmin. After completion of the survey which will take about half a year the instrument will be used for detailed observations of selected targets.

Published
1981
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7. 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
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