Search

Your search keyword '"Triou, H."' showing total 12 results
Start Over Author "Triou, H."
12 results on '"Triou, H."'

1. Designing large pixelated CdTe detection planes for hard X-ray transients detection

Author

Lacombe, K., Amoros, C., Atteia, J. -L., Bajat, A., Bouchet, L., Dezalay, J. -P., Guillemot, P., Houret, B., Lebrun, F., Mate, S., Pons, R., Triou, H., and Waegebaert, V.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We discuss the need for very large detection planes for the detection of hard X-ray transients in the multi-messenger era that started with the quasi-simultaneous detection of GRB~170817A by \textit{Fermi}/GBM and \textit{INTEGRAL}/SPI on one hand and the gravitational waves event GW 170817, detected by the LVC collaboration, on the other hand. Then, we present a brief survey of current and future instruments and their expected sensitivity, pointing the fact that the gain in the number of GRBs is achieved by future projects thanks to their larger field of view rather than to their larger effective area. Based on our experience with \textit{SVOM}/ECLAIRs, we then address various problems associated with the realization of very large detection planes (\mbox{$\ge 1 \mathrm m^{2}$}), and we demonstrate that CdTe detectors are well suited for this task. We conclude with a discussion of some key parameters that must be taken into account in the realization of instruments based on these detectors. We hope that this paper will motivate the elaboration of detailed proposals of large area wide-field hard X-ray monitors that will be crucially needed in the next decade., Comment: 27 pages, 8 figures

Published
2019
Full Text
View/download PDF

2. The X-/Gamma-ray camera ECLAIRs for the Gammay-ray burst mission SVOM

Author

Godet, O., Nasser, G., Atteia, J. -L., Cordier, B., Mandrou, P., Barret, D., Triou, H., Pons, R., Amoros, C., Bordon, S., Gevin, O., Gonzalez, F., Götz, D., Gros, A., Houret, B., Lachaud, C., Lacombe, K., Marty, W., Mercier, K., Rambaud, D., Ramon, P., Rouaix, G., Schanne, S., and Waegebaert, V

Subjects
Physics - Instrumentation and Detectors, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present ECLAIRs, the Gamma-ray burst (GRB) trigger camera to fly on-board the Chinese-French mission SVOM. ECLAIRs is a wide-field ($\sim 2$\,sr) coded mask camera with a mask transparency of 40\% and a 1024 $\mathrm{cm}^2$ detection plane coupled to a data processing unit, so-called UGTS, which is in charge of locating GRBs in near real time thanks to image and rate triggers. We present the instrument science requirements and how the design of ECLAIRs has been optimized to increase its sensitivity to high-redshift GRBs and low-luminosity GRBs in the local Universe, by having a low-energy threshold of 4 keV. The total spectral coverage ranges from 4 to 150 keV. ECLAIRs is expected to detect $\sim 200$ GRBs of all types during the nominal 3 year mission lifetime. To reach a 4 keV low-energy threshold, the ECLAIRs detection plane is paved with 6400 $4\times 4~\mathrm{mm}^2$ and 1 mm-thick Schottky CdTe detectors. The detectors are grouped by 32, in 8x4 matrices read by a low-noise ASIC, forming elementary modules called XRDPIX. In this paper, we also present our current efforts to investigate the performance of these modules with their front-end electronics when illuminated by charged particles and/or photons using radioactive sources. All measurements are made in different instrument configurations in vacuum and with a nominal in-flight detector temperature of $-20^\circ$C. This work will enable us to choose the in-flight configuration that will make the best compromise between the science performance and the in-flight operability of ECLAIRs. We will show some highlights of this work., Comment: 15 pages, 12 figures, Proceeding SPIE - Montreal 2014

Published
2014
Full Text
View/download PDF

3. In-flight calibration of the Herschel-SPIRE instrument

Author

Swinyard, B. M., Ade, P., Baluteau, J-P., Aussel, H., Barlow, M. J., Bendo, G. J., Benielli, D., Bock, J., Brisbin, D., Conley, A., Conversi, L., Dowell, A., Dowell, D., Ferlet, M., Fulton, T., Glenn, J., Glauser, A., Griffin, D., Griffin, M., Guest, S., Imhof, P., Isaak, K., Jones, S., King, K., Leeks, S., Levenson, L., Lim, T. L., Lu, N., Makiwa, G., Naylor, D., Nguyen, H., Oliver, S., Panuzzo, P., Papageorgiou, A., Pearson, C., Pohlen, M., Polehampton, E., Pouliquen, D., Rigopoulou, D., Ronayette, S., Roussel, H., Rykala, A., Savini, G., Schulz, B., Schwartz, A., Shupe, D., Sibthorpe, B., Sidher, S., Smith, A. J., Spencer, L., Trichas, M., Triou, H., Valtchanov, I., Wesson, R., Woodcraft, A., Xu, C. K., Zemcov, M., and Zhang, L.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

SPIRE, the Spectral and Photometric Imaging Receiver, is the Herschel Space Observatory's submillimetre camera and spectrometer. It contains a three-band imaging photometer operating at 250, 350 and 500 {\mu}m, and an imaging Fourier transform spectrometer (FTS) covering 194-671 {\mu}m (447-1550 GHz). In this paper we describe the initial approach taken to the absolute calibration of the SPIRE instrument using a combination of the emission from the Herschel telescope itself and the modelled continuum emission from solar system objects and other astronomical targets. We present the photometric, spectroscopic and spatial accuracy that is obtainable in data processed through the "standard" pipelines. The overall photometric accuracy at this stage of the mission is estimated as 15% for the photometer and between 15 and 50% for the spectrometer. However, there remain issues with the photometric accuracy of the spectra of low flux sources in the longest wavelength part of the SPIRE spectrometer band. The spectrometer wavelength accuracy is determined to be better than 1/10th of the line FWHM. The astrometric accuracy in SPIRE maps is found to be 2 arcsec when the latest calibration data are used. The photometric calibration of the SPIRE instrument is currently determined by a combination of uncertainties in the model spectra of the astronomical standards and the data processing methods employed for map and spectrum calibration. Improvements in processing techniques and a better understanding of the instrument performance will lead to the final calibration accuracy of SPIRE being determined only by uncertainties in the models of astronomical standards., Comment: Accepted for publication in Astronomy&Astrophysics, Herschel First Results special issue

Published
2010
Full Text
View/download PDF

4. The Herschel-SPIRE instrument and its in-flight performance

Author

Griffin, M. J., Abergel, A., Abreu, A., Ade, P. A. R., André, P., Augueres, J. -L., Babbedge, T., Bae, Y., Baillie, T., Baluteau, J. -P., Barlow, M. J., Bendo, G., Benielli, D., Bock, J. J., Bonhomme, P., Brisbin, D., Brockley-Blatt, C., Caldwell, M., Cara, C., Castro-Rodriguez, N., Cerulli, R., Chanial, P., Chen, S., Clark, E., Clements, D. L., Clerc, L., Coker, J., Communal, D., Conversi, L., Cox, P., Crumb, D., Cunningham, C., Daly, F., Davis, G. R., De Antoni, P., Delderfield, J., Devin, N., Di Giorgio, A., Didschuns, I., Dohlen, K., Donati, M., Dowell, A., Dowell, C. D., Duband, L., Dumaye, L., Emery, R. J., Ferlet, M., Ferrand, D., Fontignie, J., Fox, M., Franceschini, A., Frerking, M., Fulton, T., Garcia, J., Gastaud, R., Gear, W. K., Glenn, J., Goizel, A., Griffin, D. K., Grundy, T., Guest, S., Guillemet, L., Hargrave, P. C., Harwit, M., Hastings, P., Hatziminaoglou, E., Herman, M., Hinde, B., Hristov, V., Huang, M., Imhof, P., Isaak, K. J., Israelsson, U., Ivison, R. J., Jennings, D., Kiernan, B., King, K. J., Lange, A. E., Latter, W., Laurent, G., Laurent, P., Leeks, S. J., Lellouch, E., Levenson, L., Li, B., Li, J., Lilienthal, J., Lim, T., Liu, J., Lu, N., Madden, S., Mainetti, G., Marliani, P., McKay, D., Mercier, K., Molinari, S., Morris, H., Moseley, H., Mulder, J., Mur, M., Naylor, D. A., Nguyen, H., O'Halloran, B., Oliver, S., Olofsson, G., Olofsson, H. -G., Orfei, R., Page, M. J., Pain, I., Panuzzo, P., Papageorgiou, A., Parks, G., Parr-Burman, P., Pearce, A., Pearson, C., Pérez-Fournon, I., Pinsard, F., Pisano, G., Podosek, J., Pohlen, M., Polehampton, E. T., Pouliquen, D., Rigopoulou, D., Rizzo, D., Roseboom, I. G., Roussel, H., Rowan-Robinson, M., Rownd, B., Saraceno, P., Sauvage, M., Savage, R., Savini, G., Sawyer, E., Scharmberg, C., Schmitt, D., Schneider, N., Schulz, B., Schwartz, A., Shafer, R., Shupe, D. L., Sibthorpe, B., Sidher, S., Smith, A., Smith, A. J., Smith, D., Spencer, L., Stobie, B., Sudiwala, R., Sukhatme, K., Surace, C., Stevens, J. A., Swinyard, B. M., Trichas, M., Tourette, T., Triou, H., Tseng, S., Tucker, C., Turner, A., Vaccari, M., Valtchanov, I., Vigroux, L., Virique, E., Voellmer, G., Walker, H., Ward, R., Waskett, T., Weilert, M., Wesson, R., White, G. J., Whitehouse, N., Wilson, C. D., Winter, B., Woodcraft, A. L., Wright, G. S., Xu, C. K., Zavagno, A., Zemcov, M., Zhang, L., and Zonca, E.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Spectral and Photometric Imaging Receiver (SPIRE), is the Herschel Space Observatory`s submillimetre camera and spectrometer. It contains a three-band imaging photometer operating at 250, 350 and 500 microns, and an imaging Fourier Transform Spectrometer (FTS) which covers simultaneously its whole operating range of 194-671 microns (447-1550 GHz). The SPIRE detectors are arrays of feedhorn-coupled bolometers cooled to 0.3 K. The photometer has a field of view of 4' x 8', observed simultaneously in the three spectral bands. Its main operating mode is scan-mapping, whereby the field of view is scanned across the sky to achieve full spatial sampling and to cover large areas if desired. The spectrometer has an approximately circular field of view with a diameter of 2.6'. The spectral resolution can be adjusted between 1.2 and 25 GHz by changing the stroke length of the FTS scan mirror. Its main operating mode involves a fixed telescope pointing with multiple scans of the FTS mirror to acquire spectral data. For extended source measurements, multiple position offsets are implemented by means of an internal beam steering mirror to achieve the desired spatial sampling and by rastering of the telescope pointing to map areas larger than the field of view. The SPIRE instrument consists of a cold focal plane unit located inside the Herschel cryostat and warm electronics units, located on the spacecraft Service Module, for instrument control and data handling. Science data are transmitted to Earth with no on-board data compression, and processed by automatic pipelines to produce calibrated science products. The in-flight performance of the instrument matches or exceeds predictions based on pre-launch testing and modelling: the photometer sensitivity is comparable to or slightly better than estimated pre-launch, and the spectrometer sensitivity is also better by a factor of 1.5-2., Comment: Accepted for publication in Astronomy & Astrophyics (Herschel first results special issue)

Published
2010
Full Text
View/download PDF

5. On-ground calibration highlights for the SVOM/ECLAIRs camera

Author

den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Godet, O., Atteia, J.-L, Amoros, C., Roger, P., Bouchet, L., Dezalay, J.-P, Yassine, M., Arcier, B., Bordon, S., Lacombe, K., Lecomte, E., Llamas, M., Maestre, S., Marty, W., Papais, S., Ramon, P., Verdeil, C., Waegebaert, V., Schanne, S., Dagoneau, N., Chateau, F., Kestener, P., Le Provost, H., Tahoulan, C., Cordier, B., Tourrette, Th., Daly, F., Triou, H., Coleiro, A., Goldwurm, A., Lachaud, C., Guillemot, Ph., Mouret, J-M., Charmeau, M.-C., Perraud, L., Bousquet, F., Cervantes, Y., Gasc, Ph., Pasquier, H., Perrin, L., Ruellan, M., Simonella, O., and Yadallee, M.

Published
2022
Full Text
View/download PDF

6. In-flight calibration of the Herschel-SPIRE instrument [Letter]

Author

Swinyard, B. M., Ade, Peter A. R., Baluteau, J.-P., Aussel, H., Barlow, M. J., Bendo, G. J., Benielli, D., Bock, J., Brisbin, D., Conley, A., Conversi, L., Dowell, A., Dowell, D., Ferlet, M., Fulton, T., Glenn, J., Glauser, A., Griffin, D., Griffin, Matthew Joseph, Guest, S., Imhof, P., Isaak, Kate Gudrun, Jones, S., King, K., Leeks, S., Levenson, L., Lim, T. L., Lu, N., Makiwa, G., Naylor, D., Nguyen, H., Oliver, S., Panuzzo, P., Papageorgiou, Andreas, Pearson, C., Pohlen, Michael, Polehampton, E., Pouliquen, D., Rigopoulou, D., Ronayette, S., Roussel, H., Rykala, Adam John, Savini, G., Schulz, B., Schwartz, A., Shupe, D., Sibthorpe, B., Sidher, S., Smith, A. J., Spencer, Locke, Trichas, M., Triou, H., Valtchanov, I., Wesson, R., Woodcraft, A., Xu, C. K., Zemcov, M., and Zhang, L.

Subjects
Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, QB
Abstract

SPIRE, the Spectral and Photometric Imaging REceiver, is the Herschel Space Observatory's submillimetre camera and spectrometer. It contains a three-band imaging photometer operating at 250, 350 and 500 μm, and an imaging Fourier-transform spectrometer (FTS) covering 194–671 μm (447-1550 GHz). In this paper we describe the initial approach taken to the absolute calibration of the SPIRE instrument using a combination of the emission from the Herschel telescope itself and the modelled continuum emission from solar system objects and other astronomical targets. We present the photometric, spectroscopic and spatial accuracy that is obtainable in data processed through the “standard” pipelines. The overall photometric accuracy at this stage of the mission is estimated as 15% for the photometer and between 15 and 50% for the spectrometer. However, there remain issues with the photometric accuracy of the spectra of low flux sources in the longest wavelength part of the SPIRE spectrometer band. The spectrometer wavelength accuracy is determined to be better than 1/10th of the line FWHM. The astrometric accuracy in SPIRE maps is found to be 2 arcsec when the latest calibration data are used. The photometric calibration of the SPIRE instrument is currently determined by a combination of uncertainties in the model spectra of the astronomical standards and the data processing methods employed for map and spectrum calibration. Improvements in processing techniques and a better understanding of the instrument performance will lead to the final calibration accuracy of SPIRE being determined only by uncertainties in the models of astronomical standards.

Published
2010

7. The x-/gamma-ray camera ECLAIRs for the gamma-ray burst mission SVOM

Author

Godet, O., additional, Nasser, G., additional, Atteia, J.-., additional, Cordier, B., additional, Mandrou, P., additional, Barret, D., additional, Triou, H., additional, Pons, R., additional, Amoros, C., additional, Bordon, S., additional, Gevin, O., additional, Gonzalez, F., additional, Götz, D., additional, Gros, A., additional, Houret, B., additional, Lachaud, C., additional, Lacombe, K., additional, Marty, W., additional, Mercier, K., additional, Rambaud, D., additional, Ramon, P., additional, Rouaix, G., additional, Schanne, S., additional, and Waegebaert, V., additional

Published
2014
Full Text
View/download PDF

8. TheHerschelrevolution: Unveiling the morphology of the high-mass star-formation sites N44 and N63 in the LMC

Author

Hony, S., primary, Galliano, F., additional, Madden, S. C., additional, Panuzzo, P., additional, Meixner, M., additional, Engelbracht, C., additional, Misselt, K., additional, Galametz, M., additional, Sauvage, M., additional, Roman-Duval, J., additional, Gordon, K., additional, Lawton, B., additional, Bernard, J.-P., additional, Bolatto, A., additional, Okumura, K., additional, Chen, C.-H. R., additional, Indebetouw, R., additional, Israel, F. P., additional, Kwon, E., additional, Li, A., additional, Kemper, F., additional, Oey, M. S., additional, Rubio, M., additional, and Triou, H. E., additional

Published
2010
Full Text
View/download PDF

9. TheHerschel-SPIRE instrument and its in-flight performance

Author

Griffin, M. J., primary, Abergel, A., additional, Abreu, A., additional, Ade, P. A. R., additional, André, P., additional, Augueres, J.-L., additional, Babbedge, T., additional, Bae, Y., additional, Baillie, T., additional, Baluteau, J.-P., additional, Barlow, M. J., additional, Bendo, G., additional, Benielli, D., additional, Bock, J. J., additional, Bonhomme, P., additional, Brisbin, D., additional, Brockley-Blatt, C., additional, Caldwell, M., additional, Cara, C., additional, Castro-Rodriguez, N., additional, Cerulli, R., additional, Chanial, P., additional, Chen, S., additional, Clark, E., additional, Clements, D. L., additional, Clerc, L., additional, Coker, J., additional, Communal, D., additional, Conversi, L., additional, Cox, P., additional, Crumb, D., additional, Cunningham, C., additional, Daly, F., additional, Davis, G. R., additional, De Antoni, P., additional, Delderfield, J., additional, Devin, N., additional, Di Giorgio, A., additional, Didschuns, I., additional, Dohlen, K., additional, Donati, M., additional, Dowell, A., additional, Dowell, C. D., additional, Duband, L., additional, Dumaye, L., additional, Emery, R. J., additional, Ferlet, M., additional, Ferrand, D., additional, Fontignie, J., additional, Fox, M., additional, Franceschini, A., additional, Frerking, M., additional, Fulton, T., additional, Garcia, J., additional, Gastaud, R., additional, Gear, W. K., additional, Glenn, J., additional, Goizel, A., additional, Griffin, D. K., additional, Grundy, T., additional, Guest, S., additional, Guillemet, L., additional, Hargrave, P. C., additional, Harwit, M., additional, Hastings, P., additional, Hatziminaoglou, E., additional, Herman, M., additional, Hinde, B., additional, Hristov, V., additional, Huang, M., additional, Imhof, P., additional, Isaak, K. J., additional, Israelsson, U., additional, Ivison, R. J., additional, Jennings, D., additional, Kiernan, B., additional, King, K. J., additional, Lange, A. E., additional, Latter, W., additional, Laurent, G., additional, Laurent, P., additional, Leeks, S. J., additional, Lellouch, E., additional, Levenson, L., additional, Li, B., additional, Li, J., additional, Lilienthal, J., additional, Lim, T., additional, Liu, S. J., additional, Lu, N., additional, Madden, S., additional, Mainetti, G., additional, Marliani, P., additional, McKay, D., additional, Mercier, K., additional, Molinari, S., additional, Morris, H., additional, Moseley, H., additional, Mulder, J., additional, Mur, M., additional, Naylor, D. A., additional, Nguyen, H., additional, O'Halloran, B., additional, Oliver, S., additional, Olofsson, G., additional, Olofsson, H.-G., additional, Orfei, R., additional, Page, M. J., additional, Pain, I., additional, Panuzzo, P., additional, Papageorgiou, A., additional, Parks, G., additional, Parr-Burman, P., additional, Pearce, A., additional, Pearson, C., additional, Pérez-Fournon, I., additional, Pinsard, F., additional, Pisano, G., additional, Podosek, J., additional, Pohlen, M., additional, Polehampton, E. T., additional, Pouliquen, D., additional, Rigopoulou, D., additional, Rizzo, D., additional, Roseboom, I. G., additional, Roussel, H., additional, Rowan-Robinson, M., additional, Rownd, B., additional, Saraceno, P., additional, Sauvage, M., additional, Savage, R., additional, Savini, G., additional, Sawyer, E., additional, Scharmberg, C., additional, Schmitt, D., additional, Schneider, N., additional, Schulz, B., additional, Schwartz, A., additional, Shafer, R., additional, Shupe, D. L., additional, Sibthorpe, B., additional, Sidher, S., additional, Smith, A., additional, Smith, A. J., additional, Smith, D., additional, Spencer, L., additional, Stobie, B., additional, Sudiwala, R., additional, Sukhatme, K., additional, Surace, C., additional, Stevens, J. A., additional, Swinyard, B. M., additional, Trichas, M., additional, Tourette, T., additional, Triou, H., additional, Tseng, S., additional, Tucker, C., additional, Turner, A., additional, Vaccari, M., additional, Valtchanov, I., additional, Vigroux, L., additional, Virique, E., additional, Voellmer, G., additional, Walker, H., additional, Ward, R., additional, Waskett, T., additional, Weilert, M., additional, Wesson, R., additional, White, G. J., additional, Whitehouse, N., additional, Wilson, C. D., additional, Winter, B., additional, Woodcraft, A. L., additional, Wright, G. S., additional, Xu, C. K., additional, Zavagno, A., additional, Zemcov, M., additional, Zhang, L., additional, and Zonca, E., additional

Published
2010
Full Text
View/download PDF

10. In-flight calibration of theHerschel-SPIRE instrument

Author

Swinyard, B. M., primary, Ade, P., additional, Baluteau, J.-P., additional, Aussel, H., additional, Barlow, M. J., additional, Bendo, G. J., additional, Benielli, D., additional, Bock, J., additional, Brisbin, D., additional, Conley, A., additional, Conversi, L., additional, Dowell, A., additional, Dowell, D., additional, Ferlet, M., additional, Fulton, T., additional, Glenn, J., additional, Glauser, A., additional, Griffin, D., additional, Griffin, M., additional, Guest, S., additional, Imhof, P., additional, Isaak, K., additional, Jones, S., additional, King, K., additional, Leeks, S., additional, Levenson, L., additional, Lim, T. L., additional, Lu, N., additional, Makiwa, G., additional, Naylor, D., additional, Nguyen, H., additional, Oliver, S., additional, Panuzzo, P., additional, Papageorgiou, A., additional, Pearson, C., additional, Pohlen, M., additional, Polehampton, E., additional, Pouliquen, D., additional, Rigopoulou, D., additional, Ronayette, S., additional, Roussel, H., additional, Rykala, A., additional, Savini, G., additional, Schulz, B., additional, Schwartz, A., additional, Shupe, D., additional, Sibthorpe, B., additional, Sidher, S., additional, Smith, A. J., additional, Spencer, L., additional, Trichas, M., additional, Triou, H., additional, Valtchanov, I., additional, Wesson, R., additional, Woodcraft, A., additional, Xu, C. K., additional, Zemcov, M., additional, and Zhang, L., additional

Published
2010
Full Text
View/download PDF

11. The x-/gamma-ray camera ECLAIRs for the gamma-ray burst mission SVOM

Author

Takahashi, Tadayuki, den Herder, Jan-Willem A., Bautz, Mark, Godet, O., Nasser, G., Atteia, J.-., Cordier, B., Mandrou, P., Barret, D., Triou, H., Pons, R., Amoros, C., Bordon, S., Gevin, O., Gonzalez, F., Götz, D., Gros, A., Houret, B., Lachaud, C., Lacombe, K., Marty, W., Mercier, K., Rambaud, D., Ramon, P., Rouaix, G., Schanne, S., and Waegebaert, V.

Published
2014
Full Text
View/download PDF

12. The Herschelrevolution: Unveiling the morphology of the high-mass star-formation sites N44 and N63 in the LMC*

Author

Hony, S., Galliano, F., Madden, S. C., Panuzzo, P., Meixner, M., Engelbracht, C., Misselt, K., Galametz, M., Sauvage, M., Roman-Duval, J., Gordon, K., Lawton, B., Bernard, J.-P., Bolatto, A., Okumura, K., Chen, C.-H. R., Indebetouw, R., Israel, F. P., Kwon, E., Li, A., Kemper, F., Oey, M. S., Rubio, M., and Triou, H. E.

Abstract

Aims. We study the structure of the medium surrounding sites of high-mass star formation to determine the interrelation between the H iiregions and the environment from which they were formed. The density distribution of the surroundings is key in determining how the radiation of the newly formed stars interacts with the surroundings in a way that allows it to be used as a star-formation tracer.Methods. We present new Herschel/SPIRE 250 μm, 350 μm and 500 μm data of LHA 120-N44 and LHA 120-N63 in the LMC. We construct average spectral energy distributions (SEDs) for annuli centered on the IR bright part of the star-formation sites. The annuli cover ~10–~100 pc. We use a phenomenological dust model to fit these SEDs to derive the dust column-densities, characterize the incident radiation field and the abundance of polycyclic aromatic hydrocarbon molecules. We see a decrease of a factor 5 in the radiation field energy-density as a function of radial distance around N63. The source N44 does not show a systematic trend. We construct a simple geometrical model to derive the 3D density profile of the surroundings of these two regions.Results. Herschel/SPIRE data have proven very efficient in deriving the dust-mass distribution. We find that the radiation field in the two sources behaves very differently. N63 is more or less spherically symmetric and the average radiation field drops with distance. N44 shows no systematic decrease of the radiation intensity, which is probably due to the inhomogeneity of the surrounding molecular material and to the complex distribution of several star-forming clusters in the region.

Published
2010

Catalog

Books, media, physical & digital resources
See catalog results