Search

Your search keyword '"Lortholary, M."' showing total 36 results
Start Over Author "Lortholary, M."
36 results on '"Lortholary, M."'

2. Characterizing filaments in regions of high-mass star formation: High-resolution submilimeter imaging of the massive star-forming complex NGC 6334 with ArT\'eMiS

Author

André, Ph., Revéret, V., Könyves, V., Arzoumanian, D., Tigé, J., Gallais, P., Roussel, H., Pennec, J. Le, Rodriguez, L., Doumayrou, E., Dubreuil, D., Lortholary, M., Martignac, J., Talvard, M., Delisle, C., Visticot, F., Dumaye, L., De Breuck, C., Shimajiri, Y., Motte, F., Bontemps, S., Hennemann, M., Zavagno, A., Russeil, D., Schneider, N., Palmeirim, P., Peretto, N., Hill, T., Minier, V., Roy, A., and Rygl, K. L. J.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Herschel observations of nearby molecular clouds suggest that interstellar filaments and prestellar cores represent two fundamental steps in the star formation process. The observations support a picture of low-mass star formation according to which ~ 0.1 pc-wide filaments form first in the cold interstellar medium, probably as a result of large-scale compression of interstellar matter by supersonic turbulent flows, and then prestellar cores arise from gravitational fragmentation of the densest filaments. Whether this scenario also applies to regions of high-mass star formation is an open question, in part because Herschel data cannot resolve the inner width of filaments in the nearest regions of massive star formation. We used the bolometer camera ArTeMiS on the APEX telescope to map the central part of the NGC6334 complex at a factor of > 3 higher resolution than Herschel at 350 microns. Combining ArTeMiS data with Herschel data allowed us to study the structure of the main filament of the complex with a resolution of 8" or < 0.07 pc at d ~ 1.7 kpc. Our study confirms that this filament is a very dense, massive linear structure with a line mass ranging from ~ 500 Msun/pc to ~ 2000 Msun/pc over nearly 10 pc. It also demonstrates that its inner width remains as narrow as W ~ 0.15 +- 0.05 pc all along the filament length, within a factor of < 2 of the characteristic 0.1 pc value found with Herschel for lower-mass filaments in the Gould Belt. While it is not completely clear whether the NGC 6334 filament will form massive stars or not in the future, it is two to three orders of magnitude denser than the majority of filaments observed in Gould Belt clouds, and yet has a very similar inner width. This points to a common physical mechanism for setting the filament width and suggests that some important structural properties of nearby clouds also hold in high-mass star forming regions., Comment: 10 pages, 6 figures. A&A, in press

Published
2016
Full Text
View/download PDF

3. Resolving the Vela C ridge with P-ArTeMiS and Herschel

Author

Hill, T., Andre, Ph., Arzoumanian, D., Motte, F., Minier, V., Menshchikov, A., Didelon, P., Hennemann, M., Konyves, V., Nguyen-Luong, Q., Palmeirim, P., Peretto, N., Schneider, N., Bontemps, S., Louvet, F., Elia, D., Giannini, T., Reveret, V., Pennec, J. Le, Rodriguez, L., Boulade, O., Doumayrou, E., Dubreuil, D., Gallais, P., Lortholary, M., Martignac, J., Talvard, M., and De Breuck, C.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

We present APEX/P-ArT\'eMiS 450\mu m continuum observations of RCW 36 and the adjacent ridge, a high-mass high-column density filamentary structure at the centre of the Vela C molecular cloud. These observations, at higher resolution than Herschel's SPIRE camera, reveal clear fragmentation of the central star-forming ridge. Combined with PACS far-infrared and SPIRE sub-millimetre observations from the Herschel HOBYS project we build a high resolution column density map of the region mapped with P-ArT\'eMiS. We extract the radial density profile of the Vela C ridge which with a ~ 0.1pc central width is consistent with that measured for low-mass star-forming filaments in the Herschel Gould Belt survey. Direct comparison with Serpens South, of the Gould Belt Aquila complex, reveals many similarities between the two regions. Despite likely different formation mechanisms and histories, the Vela C ridge and Serpens South filament share common characteristics, including their filament central widths., Comment: Accepted by A&A Letters; 4 pages with an appendix; 6 figures - 2 online, 1 in an appendix

Published
2012
Full Text
View/download PDF

6. Evidence of triggered star formation in G327.3-0.6. Dust-continuum mapping of an infrared dark cloud with P-ArT\'eMiS

Author

Minier, V., André, Ph., Bergman, P., Motte, F., Wyrowski, F., Pennec, J. Le, Rodriguez, L., Boulade, O., Doumayrou, E., Dubreuil, D., Gallais, P., Hamon, G., Lagage, P. -O., Lortholary, M., Martignac, J., Revéret, V., Roussel, H., Talvard, M., Willmann, G., and Olofsson, H.

Subjects
Astrophysics - Galaxy Astrophysics
Abstract

Aims. Expanding HII regions and propagating shocks are common in the environment of young high-mass star-forming complexes. They can compress a pre-existing molecular cloud and trigger the formation of dense cores. We investigate whether these phenomena can explain the formation of high-mass protostars within an infrared dark cloud located at the position of G327.3-0.6 in the Galactic plane, in between two large infrared bubbles and two HII regions. Methods: The region of G327.3-0.6 was imaged at 450 ? m with the CEA P-ArT\'eMiS bolometer array on the Atacama Pathfinder EXperiment telescope in Chile. APEX/LABOCA and APEX-2A, and Spitzer/IRAC and MIPS archives data were used in this study. Results: Ten massive cores were detected in the P-ArT\'eMiS image, embedded within the infrared dark cloud seen in absorption at both 8 and 24 ?m. Their luminosities and masses indicate that they form high-mass stars. The kinematical study of the region suggests that the infrared bubbles expand toward the infrared dark cloud. Conclusions: Under the influence of expanding bubbles, star formation occurs in the infrared dark areas at the border of HII regions and infrared bubbles., Comment: 4 pages

Published
2009
Full Text
View/download PDF

7. First 450-micron dust continuum mapping of the massive star-forming region NGC 3576 with the P-ArTeMiS bolometer camera

Author

André, P., Minier, V., Gallais, P., Reveret, V., Pennec, J. Le, Rodriguez, L., Boulade, O., Doumayrou, E., Dubreuil, D., Lortholary, M., Martignac, J., Talvard, M., De Breuck, C., Hamon, G., Schneider, N., Bontemps, S., Lagage, P. O., Pantin, E., Roussel, H., Miller, M., Purcell, C. R., Hill, T., and Stutzki, J.

Subjects
Astrophysics
Abstract

Context: The earliest phases of massive star formation are currently much debated. Aims. In an effort to make progress, we took a census of Class0-like protostellar dense cores in the NGC 3576 region, one of the nearest and most luminous embedded sites of high-mass star formation in the Galaxy. Methods: We used the P-ArTeMiS bolometer camera on the APEX telescope to produce the first 450-micron dust continuum map of the filamentary dense clump associated with NGC 3576. Results: Combining our 450-micron observations with existing data at other wavelengths, we have identified seven massive protostellar sources along the NGC 3576 filament and placed them in the M_env - L_bol evolutionary diagram for protostars. Conclusions: Comparison with theoretical evolutionary tracks suggests that these seven protostellar sources will evolve into massive stars with masses M* ~ 15-50 Msun. Four sources are classified as candidate high-mass Class 0 objects, two sources as massive Class I objects, and one source appears to be at an intermediate stage., Comment: 9 pages, 2 figures + 2 online figures, 2 online tables. Accepted for publication in A&A (Letters)

Published
2008
Full Text
View/download PDF

12. Latest results and prospects of the ArTeMiS camera on APEX.

Author

Talvard, M., Revéret, V., Le-Pennec, Y., André, Ph., Arnaud, A., Clerc, L., de Breuck, C., Delisle, C., Doumayrou, E., Duband, L., Dubreuil, D., Dumaye, L., Ercolani, E., Gallais, P., Lortholary, M., Martignac, J., Relland, J., Rodriguez, L., Roussel, H., and Schuller, F.

Published
2018
Full Text
View/download PDF

14. Characterizing filaments in regions of high-mass star formation: High-resolution submilimeter imaging of the massive star-forming complex NGC 6334 with ArTéMiS

Author

André, Ph., primary, Revéret, V., additional, Könyves, V., additional, Arzoumanian, D., additional, Tigé, J., additional, Gallais, P., additional, Roussel, H., additional, Le Pennec, J., additional, Rodriguez, L., additional, Doumayrou, E., additional, Dubreuil, D., additional, Lortholary, M., additional, Martignac, J., additional, Talvard, M., additional, Delisle, C., additional, Visticot, F., additional, Dumaye, L., additional, De Breuck, C., additional, Shimajiri, Y., additional, Motte, F., additional, Bontemps, S., additional, Hennemann, M., additional, Zavagno, A., additional, Russeil, D., additional, Schneider, N., additional, Palmeirim, P., additional, Peretto, N., additional, Hill, T., additional, Minier, V., additional, Roy, A., additional, and Rygl, K. L. J., additional

Published
2016
Full Text
View/download PDF

15. Resolving the Vela C ridge with P-ArTéMiS and Herschel [Letter]

Author

Hill, T., Andre, Ph., Arzoumanian, D., Motte, F., Minier, V., Men'shchikov, A., Didelon, P., Hennemann, M., Koenyves, V., Nguyen-Luong, Q., Palmeirim, P., Peretto, Nicolas, Schneider, N., Bontemps, S., Louvet, F., Elia, D., Giannini, T., Reveret, V., Le Pennec, J., Rodriguez, L., Boulade, O., Doumayrou, E., Dubreuil, D., Gallais, P., Lortholary, M., Martignac, J., Talvard, M., and De Breuck, C.

Subjects
QB
Abstract

We present APEX/P-ArTéMiS 450 μm continuum observations of RCW 36 and the adjacent ridge, a high-mass high-column density filamentary structure at the centre of the Vela C molecular cloud. These observations, at higher resolution than Herschel/SPIRE camera, reveal clear fragmentation of the central star-forming ridge. Combined with PACS far-infrared and SPIRE sub-millimetre observations from the Herschel HOBYS project we build a high resolution column density map of the region mapped with P-ArTéMiS. We extract the radial density profile of the Vela C ridge which with a ~0.1 pc central width is consistent with that measured for low-mass star-forming filaments in the Herschel Gould Belt survey. Direct comparison with Serpens South, of the Gould Belt Aquila complex, reveals many similarities between the two regions. Despite likely different formation mechanisms and histories, the Vela C ridge and Serpens South filament share common characteristics, including their filament central widths.

Published
2012

16. The European Photon Imaging Camera on XMM-Newton: The MOS Cameras

Author

Turner, M., Abbey, A., Arnaud, M., Balasini, M., Belsole, E., Bennie, P., Bernard, J., Bignami, G., Boer, M., Briel, U., Butler, I., Cara, C., Chabaud, C., Cole, R., Collura, A., Conte, M., Cros, A., Denby, M., Dhez, P., Di Coco, G., Dowson, J., Ferrando, P., Ghizzardi, S., Gianotti, F., Goodall, C., Gretton, L., Griffiths, R., Hainaut, O., Hochedez, J., Holland, A., Jourdain, E., Kendziorra, E., Lagostina, A., Laine, R., La Palombara, N., Lortholary, M., Lumb, D., Marty, P., Molendi, S., Pigot, C., Poindron, E., Pounds, K., Reeves, J., Reppin, C., Rothenflug, R., Salvetat, P., Sauvageot, J., Schmitt, D., Sembay, S., Short, A., Spragg, J., Stephen, J., Strüder, L., Tiengo, A., Trifoglio, M., Trümper, J., Vercellone, S., Vigroux, L., Villa, G., Ward, M., Whitehead, S., Zonca, E., BARBERA, Marco, Turner, M., Abbey, A., Arnaud, M., Balasini, M., Barbera, M., Belsole, E., Bennie, P., Bernard, J., Bignami, G., Boer, M., Briel, U., Butler, I., Cara, C., Chabaud, C., Cole, R., Collura, A., Conte, M., Cros, A., Denby, M., Dhez, P., Di Coco, G., Dowson, J., Ferrando, P., Ghizzardi, S., Gianotti, F., Goodall, C., Gretton, L., Griffiths, R., Hainaut, O., Hochedez, J., Holland, A., Jourdain, E., Kendziorra, E., Lagostina, A., Laine, R., La Palombara, N., Lortholary, M., Lumb, D., Marty, P., Molendi, S., Pigot, C., Poindron, E., Pounds, K., Reeves, J., Reppin, C., Rothenflug, R., Salvetat, P., Sauvageot, J., Schmitt, D., Sembay, S., Short, A., Spragg, J., Stephen, J., Strüder, L., Tiengo, A., Trifoglio, M., Trümper, J., Vercellone, S., Vigroux, L., Villa, G., Ward, M., Whitehead, S., and Zonca, E.

Subjects
Physics, Instrumentation: detector, Photon, Spectrometer, business.industry, Dynamic range, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Field of view, Astrophysics, X-rays: general, Optics, Cardinal point, Space and Planetary Science, Calibration, Spectral resolution, business, Focus (optics)
Abstract

The EPIC focal plane imaging spectrometers on XMM-Newton use CCDs to record the images and spectra of celestial X-ray sources focused by the three X-ray mirrors. There is one camera at the focus of each mirror; two of the cameras contain seven MOS CCDs, while the third uses twelve PN CCDs, defining a circular field of view of 30 arcmin diameter in each case. The CCDs were specially developed for EPIC, and combine high quality imaging with spectral resolution close to the Fano limit. A filter wheel carrying three kinds of X-ray transparent light blocking filter, a fully closed, and a fully open position, is fitted to each EPIC instrument. The CCDs are cooled passively and are under full closed loop thermal control. A radio-active source is fitted for internal calibration. Data are processed on-board to save telemetry by removing cosmic ray tracks, and generating X-ray event files; a variety of different instrument modes are available to increase the dynamic range of the instrument and to enable fast timing. The instruments were calibrated using laboratory X-ray beams, and synchrotron generated monochromatic X-ray beams before launch; in-orbit calibration makes use of a variety of celestial X-ray targets. The current calibration is better than 10% over the entire energy range of 0.2 to 10 keV. All three instruments survived launch and are performing nominally in orbit. In particular full field-of-view coverage is available, all electronic modes work, and the energy resolution is close to pre-launch values. Radiation damage is well within pre-launch predictions and does not yet impact on the energy resolution. The scientific results from EPIC amply fulfil pre-launch expectations., Comment: 9 pages, 11 figures, accepted for publication in the A&A Special Issue on XMM-Newton

Published
2000
Full Text
View/download PDF

20. Status of the ArTeMiS camera to be installed on APEX

Author

Talvard, M., primary, André, P., additional, Le-Pennec, Y., additional, Doumayrou, E., additional, Dubreuil, D., additional, Lortholary, M., additional, Martignac, J., additional, De Breuck, C., additional, Rabanus, D., additional, Agnèse, P., additional, Boulade, O., additional, Ercolani, E., additional, Gallais, P., additional, Horeau, B., additional, Lagage, P. O., additional, Leriche, B., additional, Relland, J., additional, Revéret, V., additional, and Rodriguez, L., additional

Published
2010
Full Text
View/download PDF

21. Evidence of triggered star formation in G327.3-0.6

Author

Minier, V., primary, André, Ph., additional, Bergman, P., additional, Motte, F., additional, Wyrowski, F., additional, Le Pennec, J., additional, Rodriguez, L., additional, Boulade, O., additional, Doumayrou, E., additional, Dubreuil, D., additional, Gallais, P., additional, Hamon, G., additional, Lagage, P.-O., additional, Lortholary, M., additional, Martignac, J., additional, Revéret, V., additional, Roussel, H., additional, Talvard, M., additional, Willmann, G., additional, and Olofsson, H., additional

Published
2009
Full Text
View/download PDF

22. Bolometers at CEA: ARTEMIS and beyond

Author

Revéret, V., primary, Talvard, M., additional, André, P., additional, Rodriguez, L., additional, Le-Pennec, Y., additional, De Breuck, C., additional, Agnèse, P., additional, Boulade, O., additional, Delisle, C., additional, Doumayrou, E., additional, Dubreuil, D., additional, Ercolani, E., additional, Gallais, P., additional, Horeau, B., additional, Lagage, P.-O., additional, Leriche, B., additional, Lortholary, M., additional, Martignac, J., additional, Minier, V., additional, Pantin, E., additional, Rabanus, D., additional, Relland, J., additional, Visticot, F., additional, and Willmann, G., additional

Published
2009
Full Text
View/download PDF

27. First 450 $\sf \mu$m dust continuum mapping of the massive star-forming region NGC 3576 with the P-ArTéMiS bolometer camera

Author

André, Ph., primary, Minier, V., additional, Gallais, P., additional, Revéret, V., additional, Le Pennec, J., additional, Rodriguez, L., additional, Boulade, O., additional, Doumayrou, E., additional, Dubreuil, D., additional, Lortholary, M., additional, Martignac, J., additional, Talvard, M., additional, De Breuck, C., additional, Hamon, G., additional, Schneider, N., additional, Bontemps, S., additional, Lagage, P. O., additional, Pantin, E., additional, Roussel, H., additional, Miller, M., additional, Purcell, C. R., additional, Hill, T., additional, and Stutzki, J., additional

Published
2008
Full Text
View/download PDF

28. Recent results obtained on the APEX 12 m antenna with the ArTeMiS prototype camera

Author

Talvard, M., primary, André, P., additional, Rodriguez, L., additional, Le-Pennec, Y., additional, De Breuck, C., additional, Revéret, V., additional, Agnèse, P., additional, Boulade, O., additional, Doumayrou, E., additional, Dubreuil, D., additional, Ercolani, E., additional, Gallais, P., additional, Horeau, B., additional, Lagage, PO, additional, Leriche, B., additional, Lortholary, M., additional, Martignac, J., additional, Minier, V., additional, Pantin, E., additional, Rabanus, D., additional, Relland, J., additional, and Willmann, G., additional

Published
2008
Full Text
View/download PDF

30. XMM-Newton first-light observations of the Hickson galaxy group 16

Author

Turner, M. J. L., primary, Reeves, J. N., additional, Ponman, T. J., additional, Arnaud, M., additional, Barbera, M., additional, Bennie, P. J., additional, Boer, M., additional, Briel, U., additional, Butler, I., additional, Clavel, J., additional, Dhez, P., additional, Cordova, F., additional, Dos Santos, S., additional, Ferrando, P., additional, Ghizzardi, S., additional, Goodall, C. V., additional, Griffiths, R. G., additional, Hochedez, J. F., additional, Holland, A. D., additional, Jansen, F., additional, Kendziorra, E., additional, Lagostina, A., additional, Laine, R., additional, La Palombara, N., additional, Lortholary, M., additional, Mason, K. O., additional, Molendi, S., additional, Pigot, C., additional, Priedhorsky, W., additional, Reppin, C., additional, Rothenflug, R., additional, Salvetat, P., additional, Sauvageot, J., additional, Schmitt, D., additional, Sembay, S., additional, Short, A., additional, Strüder, L., additional, Trifoglio, M., additional, Trümper, J., additional, Vercellone, S., additional, Vigroux, L., additional, Villa, G., additional, and Ward, M., additional

Published
2001
Full Text
View/download PDF

31. The European Photon Imaging Camera on XMM-Newton: The MOS cameras

Author

Turner, M. J. L., primary, Abbey, A., additional, Arnaud, M., additional, Balasini, M., additional, Barbera, M., additional, Belsole, E., additional, Bennie, P. J., additional, Bernard, J. P., additional, Bignami, G. F., additional, Boer, M., additional, Briel, U., additional, Butler, I., additional, Cara, C., additional, Chabaud, C., additional, Cole, R., additional, Collura, A., additional, Conte, M., additional, Cros, A., additional, Denby, M., additional, Dhez, P., additional, Di Coco, G., additional, Dowson, J., additional, Ferrando, P., additional, Ghizzardi, S., additional, Gianotti, F., additional, Goodall, C. V., additional, Gretton, L., additional, Griffiths, R. G., additional, Hainaut, O., additional, Hochedez, J. F., additional, Holland, A. D., additional, Jourdain, E., additional, Kendziorra, E., additional, Lagostina, A., additional, Laine, R., additional, La Palombara, N., additional, Lortholary, M., additional, Lumb, D., additional, Marty, P., additional, Molendi, S., additional, Pigot, C., additional, Poindron, E., additional, Pounds, K. A., additional, Reeves, J. N., additional, Reppin, C., additional, Rothenflug, R., additional, Salvetat, P., additional, Sauvageot, J. L., additional, Schmitt, D., additional, Sembay, S., additional, Short, A. D. T., additional, Spragg, J., additional, Stephen, J., additional, Strüder, L., additional, Tiengo, A., additional, Trifoglio, M., additional, Trümper, J., additional, Vercellone, S., additional, Vigroux, L., additional, Villa, G., additional, Ward, M. J., additional, Whitehead, S., additional, and Zonca, E., additional

Published
2001
Full Text
View/download PDF

33. First 450??m dust continuum mapping of the massive star-forming region NGC?3576 with the P-ArT?MiS bolometer camera

Author

Andr?, Ph., Minier, V., Gallais, P., Rev?ret, V., Le Pennec, J., Rodriguez, L., Boulade, O., Doumayrou, E., Dubreuil, D., Lortholary, M., Martignac, J., Talvard, M., De Breuck, C., Hamon, G., Schneider, N., Bontemps, S., Lagage, P., Pantin, E., Roussel, H., Miller, M., Purcell, C., Hill, T., and Stutzki, J.

Abstract

Aims. In an effort to make progress in the current debate on the earliest phases of massive star formation, we took a census of Class?0-like protostellar dense cores in the NGC?3576 region, one of the nearest and most luminous embedded sites of high-mass star formation in the Galaxy.Methods. We used the P-ArT?MiS bolometer camera on the APEX telescope to produce the first 450??m dust continuum map of the filamentary dense clump associated with NGC?3576.Results. Combining our 450??m observations with existing data at other wavelengths, we identified seven massive protostellar sources along the NGC?3576 filament and placed them in the Menv?Lbolevolutionary diagram for protostars. Conclusions. Comparison with theoretical evolutionary tracks suggests that these seven protostellar sources will evolve into massive stars with masses M*?15?50?M?. Four sources are classified as candidate high-mass Class?0 objects, two sources as massive Class?I objects, and one source appears to be at an intermediate stage.

Published
2008

34. Latest results and prospects of the ArTeMiS camera on APEX

Author

Zmuidzinas, Jonas, Gao, Jian-Rong, Talvard, M., Revéret, V., Le-Pennec, Y., André, Ph., Arnaud, A., Clerc, L., de Breuck, C., Delisle, C., Doumayrou, E., Duband, L., Dubreuil, D., Dumaye, L., Ercolani, E., Gallais, P., Lortholary, M., Martignac, J., Relland, J., Rodriguez, L., Roussel, F., Schuller, F., and Visticot, F.

Published
2018
Full Text
View/download PDF

36. 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

Catalog

Books, media, physical & digital resources
See catalog results