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73 results on '"Robitaille, T. P."'

54. SPITZERSAGE-SMC INFRARED PHOTOMETRY OF MASSIVE STARS IN THE SMALL MAGELLANIC CLOUD

Author

Bonanos, A. Z., primary, Lennon, D. J., additional, Köhlinger, F., additional, van Loon, J. Th., additional, Massa, D. L., additional, Sewilo, M., additional, Evans, C. J., additional, Panagia, N., additional, Babler, B. L., additional, Block, M., additional, Bracker, S., additional, Engelbracht, C. W., additional, Gordon, K. D., additional, Hora, J. L., additional, Indebetouw, R., additional, Meade, M. R., additional, Meixner, M., additional, Misselt, K. A., additional, Robitaille, T. P., additional, Shiao, B., additional, and Whitney, B. A., additional

Published
2010
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56. A CATALOG OF EXTENDED GREEN OBJECTS IN THE GLIMPSE SURVEY: A NEW SAMPLE OF MASSIVE YOUNG STELLAR OBJECT OUTFLOW CANDIDATES

Author

Cyganowski, C. J., primary, Whitney, B. A., additional, Holden, E., additional, Braden, E., additional, Brogan, C. L., additional, Churchwell, E., additional, Indebetouw, R., additional, Watson, D. F., additional, Babler, B. L., additional, Benjamin, R., additional, Gomez, M., additional, Meade, M. R., additional, Povich, M. S., additional, Robitaille, T. P., additional, and Watson, C., additional

Published
2008
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58. SPITZERSAGE SURVEY OF THE LARGE MAGELLANIC CLOUD. III. STAR FORMATION AND ∼1000 NEW CANDIDATE YOUNG STELLAR OBJECTS

Author

Whitney, B. A., primary, Sewilo, M., additional, Indebetouw, R., additional, Robitaille, T. P., additional, Meixner, M., additional, Gordon, K., additional, Meade, M. R., additional, Babler, B. L., additional, Harris, J., additional, Hora, J. L., additional, Bracker, S., additional, Povich, M. S., additional, Churchwell, E. B., additional, Engelbracht, C. W., additional, For, B-Q, additional, Block, M., additional, Misselt, K., additional, Vijh, U., additional, Leitherer, C., additional, Kawamura, A., additional, Blum, R. D., additional, Cohen, M., additional, Fukui, Y., additional, Mizuno, A., additional, Mizuno, N., additional, Srinivasan, S., additional, Tielens, A. G. G. M., additional, Volk, K., additional, Bernard, J-P., additional, Boulanger, F., additional, Frogel, J. A., additional, Gallagher, J., additional, Gorjian, V., additional, Kelly, D., additional, Latter, W. B., additional, Madden, S., additional, Kemper, F., additional, Mould, J. R., additional, Nota, A., additional, Oey, M. S., additional, Olsen, K. A., additional, Onishi, T., additional, Paladini, R., additional, Panagia, N., additional, Perez-Gonzalez, P., additional, Reach, W., additional, Shibai, H., additional, Sato, S., additional, Smith, L. J., additional, Staveley-Smith, L., additional, Ueta, T., additional, Dyk, S. Van, additional, Werner, M., additional, Wolff, M., additional, and Zaritsky, D., additional

Published
2008
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62. The Frequency of Mid‐Infrared Excess Sources in Galactic Surveys

Author

Uzpen, B., primary, Kobulnicky, H. A., additional, Monson, A. J., additional, Pierce, M. J., additional, Clemens, D. P., additional, Backman, D. E., additional, Meade, M. R., additional, Babler, B. L., additional, Indebetouw, R., additional, Whitney, B. A., additional, Watson, C., additional, Wolfire, M. G., additional, Benjamin, R. A., additional, Bracker, S., additional, Bania, T. M., additional, Cohen, M., additional, Cyganowski, C. J., additional, Devine, K. E., additional, Heitsch, F., additional, Jackson, J. M., additional, Mathis, J. S., additional, Mercer, E. P., additional, Povich, M. S., additional, Rho, J., additional, Robitaille, T. P., additional, Sewilo, M., additional, Stolovy, S. R., additional, Watson, D. F., additional, Wolff, M. J., additional, and Churchwell, E., additional

Published
2007
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65. Early-stage young stellar objects in the Small Magellanic Cloud.

Author

Oliveira, J. M., van Loon, J. Th., Sloan, G. C., Sewiło, M., Kraemer, K. E., Wood, P. R., Indebetouw, R., Filipović, M. D., Crawford, E. J., Wong, G. F., Hora, J. L., Meixner, M., Robitaille, T. P., Shiao, B., and Simon, J. D.

Subjects
EARLY stars, SMALL magellanic cloud, ASTRONOMICAL observations, PHOTOMETRY, GALACTIC evolution, OPTICAL spectroscopy
Abstract

We present new observations of 34 young stellar object (YSO) candidates in the Small Magellanic Cloud (SMC). The photometric selection required sources to be bright at 24 and 70 μm (to exclude evolved stars and galaxies). The anchor of the analysis is a set of Spitzer Infrared Spectrograph (IRS) spectra, supplemented by ground-based 3–5 μm spectra, Spitzer Infrared Array Camera and Multiband Imaging Photometer for Spitzer photometry, near-infrared (IR) imaging and photometry, optical spectroscopy and radio data. The sources’ spectral energy distributions and spectral indices are consistent with embedded YSOs; prominent silicate absorption is observed in the spectra of at least 10 sources, silicate emission is observed towards four sources. Polycyclic aromatic hydrocarbon (PAH) emission is detected towards all but two sources. Based on band ratios (in particular the strength of the 11.3-μm and the weakness of the 8.6-μm bands) PAH emission towards SMC YSOs is dominated by predominantly small neutral grains. Ice absorption is observed towards 14 sources in the SMC. The comparison of H2O and CO2 ice column densities for SMC, Large Magellanic Cloud and Galactic samples suggests that there is a significant H2O column density threshold for the detection of CO2 ice. This supports the scenario proposed by Oliveira et al., where the reduced shielding in metal-poor environments depletes the H2O column density in the outer regions of the YSO envelopes. No CO ice is detected towards the SMC sources. Emission due to pure rotational 0–0 transitions of molecular hydrogen is detected towards the majority of SMC sources, allowing us to estimate rotational temperatures and H2 column densities. All but one source are spectroscopically confirmed as SMC YSOs. Based on the presence of ice absorption, silicate emission or absorption and PAH emission, the sources are classified and placed in an evolutionary sequence. Of the 33 YSOs identified in the SMC, 30 sources populate different stages of massive stellar evolution. The presence of ice- and/or silicate-absorption features indicates sources in the early embedded stages; as a source evolves, a compact H ii region starts to emerge, and at the later stages the source’s IR spectrum is completely dominated by PAH and fine-structure emission. The remaining three sources are classified as intermediate-mass YSOs with a thick dusty disc and a tenuous envelope still present. We propose one of the SMC sources is a D-type symbiotic system, based on the presence of Raman, H and He emission lines in the optical spectrum, and silicate emission in the IRS spectrum. This would be the first dust-rich symbiotic system identified in the SMC. [ABSTRACT FROM AUTHOR]

Published
2013
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66. The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

Author

The Astropy Collaboration, Price-Whelan, A. M., Sipőcz, B. M., Günther, H. M., Lim, P. L., Crawford, S. M., Conseil, S., Shupe, D. L., Craig, M. W., Dencheva, N., Ginsburg, A., Vanderplas, J. T., Bradley, L. D., Pérez-Suárez, D., Val-Borro, M., Aldcroft, T. L., Cruz, K. L., Robitaille, T. P., Tollerud, E. J., Ardelean, C., Babej, T., Bachetti, M., Bakanov, A. V., Bamford, S. P., Barentsen, G., Barmby, P., Baumbach, A., Berry, K. L., Biscani, F., Boquien, M., Bostroem, K. A., Bouma, L. G., Brammer, G. B., Bray, E. M., Breytenbach, H., Buddelmeijer, H., Burke, D. J., Calderone, G., Cano Rodríguez, J. L., Cara, M., Cardoso, J. V. M., Cheedella, S., Yannick Copin, Crichton, D., Dávella, D., Deil, C., Depagne, É, Dietrich, J. P., Donath, A., Droettboom, M., Earl, N., Erben, T., Fabbro, S., Ferreira, L. A., Finethy, T., Fox, R. T., Garrison, L. H., Gibbons, S. L. J., Goldstein, D. A., Gommers, R., Greco, J. P., Greenfield, P., Groener, A. M., Grollier, F., Hagen, A., Hirst, P., Homeier, D., Horton, A. J., Hosseinzadeh, G., Hu, L., Hunkeler, J. S., Ivezić, Ž, Jain, A., Jenness, T., Kanarek, G., Kendrew, S., Kern, N. S., Kerzendorf, W. E., Khvalko, A., King, J., Kirkby, D., Kulkarni, A. M., Kumar, A., Lee, A., Lenz, D., Littlefair, S. P., Ma, Z., Macleod, D. M., Mastropietro, M., Mccully, C., Montagnac, S., Morris, B. M., Mueller, M., Mumford, S. J., Muna, D., Murphy, N. A., Nelson, S., Nguyen, G. H., Ninan, J. P., Nöthe, M., Ogaz, S., Oh, S., Parejko, J. K., Parley, N., Pascual, S., Patil, R., Patil, A. A., Plunkett, A. L., Prochaska, J. X., Rastogi, T., Reddy Janga, V., Sabater, J., Sakurikar, P., Seifert, M., Sherbert, L. E., Sherwood-Taylor, H., Shih, A. Y., Sick, J., Silbiger, M. T., Singanamalla, S., Singer, L. P., Sladen, P. H., Sooley, K. A., Sornarajah, S., Streicher, O., Teuben, P., Thomas, S. W., Tremblay, G. R., Turner, J. E. H., Terrón, V., Kerkwijk, M. H., La Vega, A., Watkins, L. L., Weaver, B. A., Whitmore, J. B., Woillez, J., and Zabalza, V.

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The Astropy project supports and fosters the development of open-source and openly-developed Python packages that provide commonly-needed functionality to the astronomical community. A key element of the Astropy project is the core package Astropy, which serves as the foundation for more specialized projects and packages. In this article, we provide an overview of the organization of the Astropy project and summarize key features in the core package as of the recent major release, version 2.0. We then describe the project infrastructure designed to facilitate and support development for a broader ecosystem of inter-operable packages. We conclude with a future outlook of planned new features and directions for the broader Astropy project., Minor changes to author list and title. Comments and feedback welcome through the paper source repository: https://github.com/astropy/astropy-v2.0-paper For more information about Astropy, see http://www.astropy.org/

70. The Red MSX Source survey: the bolometric fluxes and luminosity distributions of young massive stars⋆

Author

Mottram, J. C., Hoare, M. G., Urquhart, J. S., Lumsden, S. L., Oudmaijer, R. D., Robitaille, T. P., Moore, T. J. T., Davies, B., and Stead, J.

Abstract

Context.The Red MSX Source (RMS) survey is returning a large sample of massive young stellar objects (MYSOs) and ultra-compact (UC) H ii regions using follow-up observations of colour-selected candidates from the MSX point source catalogue.

Published
2011
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71. HERschelInventory of The Agents of Galaxy Evolution (HERITAGE): The Large Magellanic Cloud dust*

Author

Meixner, M., Galliano, F., Hony, S., Roman-Duval, J., Robitaille, T., Panuzzo, P., Sauvage, M., Gordon, K., Engelbracht, C., Misselt, K., Okumura, K., Beck, T., Bernard, J.-P., Bolatto, A., Bot, C., Boyer, M., Bracker, S., Carlson, L. R., Clayton, G. C., R. Chen, C.-H., Churchwell, E., Fukui, Y., Galametz, M., Hora, J. L., Hughes, A., Indebetouw, R., Israel, F. P., Kawamura, A., Kemper, F., Kim, S., Kwon, E., Lawton, B., Li, A., Long, K. S., Marengo, M., Madden, S. C., Matsuura, M., Oliveira, J. M., Onishi, T., Otsuka, M., Paradis, D., Poglitsch, A., Riebel, D., Reach, W. T., Rubio, M., Sargent, B., Sewiło, M., Simon, J. D., Skibba, R., Smith, L. J., Srinivasan, S., Tielens, A. G. G. M., van Loon, J. Th., Whitney, B., and Woods, P. M.

Abstract

The HERschelInventory of The Agents of Galaxy Evolution (HERITAGE) of the Magellanic Clouds will use dust emission to investigate the life cycle of matter in both the Large and Small Magellanic Clouds (LMC and SMC). Using the HerschelSpace Observatory's PACS and SPIRE photometry cameras, we imaged a 2° × 8° strip through the LMC, at a position angle of ~22.5° as part of the science demonstration phase of the Herschelmission. We present the data in all 5 Herschelbands: PACS 100 and 160 μm and SPIRE 250, 350 and 500 μm. We present two dust models that both adequately fit the spectral energy distribution for the entire strip and both reveal that the SPIRE 500 μm emission is in excess of the models by ~6 to 17%. The SPIRE emission follows the distribution of the dust mass, which is derived from the model. The PAH-to-dust mass (fPAH) image of the strip reveals a possible enhancement in the LMC bar in agreement with previous work. We compare the gas mass distribution derived from the HI21 cm and CO J= 1–0 line emission maps to the dust mass map from the models and derive gas-to-dust mass ratios (GDRs). The dust model, which uses the standard graphite and silicate optical properties for Galactic dust, has a very low GDR = 65-18+15making it an unrealistic dust model for the LMC. Our second dust model, which uses amorphous carbon instead of graphite, has a flatter emissivity index in the submillimeter and results in a GDR = 287-42+25that is more consistent with a GDR inferred from extinction.

Published
2010

72. Clouds, filaments, and protostars: The HerschelHi-GAL Milky Way *

Author

Molinari, S., Swinyard, B., Bally, J., Barlow, M., Bernard, J.-P., Martin, P., Moore, T., Noriega-Crespo, A., Plume, R., Testi, L., Zavagno, A., Abergel, A., Ali, B., Anderson, L., André, P., Baluteau, J.-P., Battersby, C., Beltrán, M. T., Benedettini, M., Billot, N., Blommaert, J., Bontemps, S., Boulanger, F., Brand, J., Brunt, C., Burton, M., Calzoletti, L., Carey, S., Caselli, P., Cesaroni, R., Cernicharo, J., Chakrabarti, S., Chrysostomou, A., Cohen, M., Compiegne, M., de Bernardis, P., de Gasperis, G., di Giorgio, A. M., Elia, D., Faustini, F., Flagey, N., Fukui, Y., Fuller, G. A., Ganga, K., Garcia-Lario, P., Glenn, J., Goldsmith, P. F., Griffin, M., Hoare, M., Huang, M., Ikhenaode, D., Joblin, C., Joncas, G., Juvela, M., Kirk, J. M., Lagache, G., Li, J. Z., Lim, T. L., Lord, S. D., Marengo, M., Marshall, D. J., Masi, S., Massi, F., Matsuura, M., Minier, V., Miville-Deschênes, M.-A., Montier, L. A., Morgan, L., Motte, F., Mottram, J. C., Müller, T. G., Natoli, P., Neves, J., Olmi, L., Paladini, R., Paradis, D., Parsons, H., Peretto, N., Pestalozzi, M., Pezzuto, S., Piacentini, F., Piazzo, L., Polychroni, D., Pomarès, M., Popescu, C. C., Reach, W. T., Ristorcelli, I., Robitaille, J.-F., Robitaille, T., Rodón, J. A., Roy, A., Royer, P., Russeil, D., Saraceno, P., Sauvage, M., Schilke, P., Schisano, E., Schneider, N., Schuller, F., Schulz, B., Sibthorpe, B., Smith, H. A., Smith, M. D., Spinoglio, L., Stamatellos, D., Strafella, F., Stringfellow, G. S., Sturm, E., Taylor, R., Thompson, M. A., Traficante, A., Tuffs, R. J., Umana, G., Valenziano, L., Vavrek, R., Veneziani, M., Viti, S., Waelkens, C., Ward-Thompson, D., White, G., Wilcock, L. A., Wyrowski, F., Yorke, H. W., and Zhang, Q.

Abstract

We present the first results from the science demonstration phase for the Hi-GAL survey, the Herschelkey program that will map the inner Galactic plane of the Milky Way in 5 bands. We outline our data reduction strategy and present some science highlights on the two observed 2° × 2° tiles approximately centered at l= 30° and l= 59°. The two regions are extremely rich in intense and highly structured extended emission which shows a widespread organization in filaments. Source SEDs can be built for hundreds of objects in the two fields, and physical parameters can be extracted, for a good fraction of them where the distance could be estimated. The compact sources (which we will call cores' in the following) are found for the most part to be associated with the filaments, and the relationship to the local beam-averaged column density of the filament itself shows that a core seems to appear when a threshold around AV~ 1 is exceeded for the regions in the l= 59° field; a AVvalue between 5 and 10 is found for the l= 30° field, likely due to the relatively higher distances of the sources. This outlines an exciting scenario where diffuse clouds first collapse into filaments, which later fragment to cores where the column density has reached a critical level. In spite of core L/M ratios being well in excess of a few for many sources, we find coresurface densities between 0.03 and 0.5 g cm-2. Our results are in good agreement with recent MHD numerical simulations of filaments forming from large-scale converging flows.

Published
2010

73. A Herschelstudy of YSO evolutionary stages and formation timelines in two fields of the Hi-GAL survey*

Author

Elia, D., Schisano, E., Molinari, S., Robitaille, T., Anglés-Alcázar, D., Bally, J., Battersby, C., Benedettini, M., Billot, N., Calzoletti, L., Di Giorgio, A. M., Faustini, F., Li, J. Z., Martin, P., Morgan, L., Motte, F., Mottram, J. C., Natoli, P., Olmi, L., Paladini, R., Piacentini, F., Pestalozzi, M., Pezzuto, S., Polychroni, D., Smith, M. D., Strafella, F., Stringfellow, G. S., Testi, L., Thompson, M. A., Traficante, A., and Veneziani, M.

Abstract

We present a first study of the star-forming compact dust condensations revealed by Herschelin the two 2° × 2° Galactic Plane fields centered at [$\ell$, b] = [30°, 0°] and [$\ell$, b] =[59°, 0°] , respectively, and observed during the science demonstration phase for the HerschelInfrared GALactic plane survey (Hi-GAL) key-project. Compact source catalogs extracted for the two fields in the five Hi-GAL bands (70, 160, 250, 350 and 500 μm) were merged based on simple criteria of positional association and spectral energy distribution (SED) consistency into a final catalog which contains only coherent SEDs with counterparts in at least three adjacent Herschelbands. These final source lists contain 528 entries for the $\ell$= 30° field, and 444 entries for the $\ell$= 59° field. The SED coverage has been augmented with ancillary data at 24 μm and 1.1 mm. SED modeling for the subset of 318 and 101 sources (in the two fields, respectively) for which the distance is known was carried out using both a structured star/disk/envelope radiative transfer model and a simple isothermal grey-body. Global parameters like mass, luminosity, temperature and dust properties have been estimated. The Lbol/Menvratio spans four orders of magnitudes from values compatible with the pre-protostellar phase to embedded massive zero-age main sequence stars. Sources in the $\ell$= 59° field have on average lower L/M, possibly outlining an overall earlier evolutionary stage with respect to the sources in the $\ell$= 30° field. Many of these cores are actively forming high-mass stars, although the estimated core surface densities appear to be an order of magnitude below the 1 g cm-2critical threshold for high-mass star formation.

Published
2010

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