Charles A. Poteet
Rensselaer Polytechnic Institute
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Featured researches published by Charles A. Poteet.
Astrophysical Journal Supplement Series | 2016
Elise Furlan; William J. Fischer; Babar Ali; Amelia M. Stutz; T. Stanke; John J. Tobin; S. T. Megeath; Mayra Osorio; Lee Hartmann; Nuria Calvet; Charles A. Poteet; J. Booker; P. Manoj; Dan M. Watson; Lori E. Allen
We present key results from the Herschel Orion Protostar Survey (HOPS): spectral energy distributions (SEDs) and model fits of 330 young stellar objects, predominantly protostars, in the Orion molecular clouds. This is the largest sample of protostars studied in a single, nearby star-formation complex. With near-infrared photometry from 2MASS, mid- and far-infrared data from Spitzer and Herschel, and sub-millimeter photometry from APEX, our SEDs cover 1.2-870
arXiv: Astrophysics of Galaxies | 2014
Michael M. Dunham; Amelia M. Stutz; Lori E. Allen; Neal J. Evans; William J. Fischer; S. Thomas Megeath; Philip C. Myers; Stella S. R. Offner; Charles A. Poteet; John J. Tobin; Eduard I. Vorobyov
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The Astrophysical Journal | 2015
Charles A. Poteet; Douglas C. B. Whittet; B. T. Draine
m and sample the peak of the protostellar envelope emission at ~100
Astronomy and Astrophysics | 2013
K. Isokoski; Charles A. Poteet; Harold Linnartz
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Astronomy and Astrophysics | 2016
C. Lefèvre; L. Pagani; M. Min; Charles A. Poteet; Douglas C. B. Whittet
m. Using mid-IR spectral indices and bolometric temperatures, we classify our sample into 92 Class 0 protostars, 125 Class I protostars, 102 flat-spectrum sources, and 11 Class II pre-main-sequence stars. We implement a simple protostellar model (including a disk in an infalling envelope with outflow cavities) to generate a grid of 30400 model SEDs and use it to determine the best-fit model parameters for each protostar. We argue that far-IR data are essential for accurate constraints on protostellar envelope properties. We find that most protostars, and in particular the flat-spectrum sources, are well-fit. The median envelope density and median inclination angle decrease from Class 0 to Class I to flat-spectrum protostars, despite the broad range in best-fit parameters in each of the three categories. We also discuss degeneracies in our model parameters. Our results confirm that the different protostellar classes generally correspond to an evolutionary sequence with a decreasing envelope infall rate, but the inclination angle also plays a role in the appearance, and thus interpretation, of the SEDs.
The Astrophysical Journal | 2014
William J. Fischer; S. Thomas Megeath; John J. Tobin; Lee Hartmann; Amelia M. Stutz; Marina Kounkel; Charles A. Poteet; Babar Ali; Mayra Osorio; P. Manoj; Ian S. Remming; Thomas Stanke; Dan M. Watson
Stars form from the gravitational collapse of dense molecular cloud cores. In the protostellar phase, mass accretes from the core onto a protostar, likely through an accretion disk, and it is during this phase that the initial masses of stars and the initial conditions for planet formation are set. Over the past decade, new observational capabilities provided by the Spitzer Space Telescope and Herschel Space Observatory have enabled wide-field surveys of entire star-forming clouds with unprecedented sensitivity, resolution, and infrared wavelength coverage. We review resulting advances in the field, focusing both on the observations themselves and the constraints they place on theoretical models of star formation and protostellar evolution. We also emphasize open questions and outline new directions needed to further advance the field.
The Astrophysical Journal | 2018
Charles A. Poteet; C. H. Chen; Dean C. Hines; Marshall D. Perrin; John H. Debes; Laurent Pueyo; Glenn Schneider; Johan Mazoyer; Ludmilla Kolokolova
We investigate the composition of interstellar grains along the line of sight toward ? Ophiuchi, a well-studied environment near the diffuse-dense cloud transition. A spectral decomposition analysis of the solid-state absorbers is performed using archival spectroscopic observations from the Spitzer Space Telescope and Infrared Space Observatory. We find strong evidence for the presence of sub-micron-sized amorphous silicate grains, principally comprised of olivine-like composition, with no convincing evidence of H2O ice mantles. However, tentative evidence for thick H2O ice mantles on large (a 2.8 ?m) grains is presented. Solid-state abundances of elemental Mg, Si, Fe, and O are inferred from our analysis and compared to standard reference abundances. We find that nearly all of the Mg and Si atoms along the line of sight reside in amorphous silicate grains, while a substantial fraction of the elemental Fe resides in compounds other than silicates. Moreover, we find that the total abundance of elemental O is largely inconsistent with the adopted reference abundances, indicating that as much as ~156 ppm of interstellar O is missing along the line of sight. After taking into account additional limits on the abundance of elemental O in other O-bearing solids, we conclude that any missing reservoir of elemental O must reside on large grains that are nearly opaque to infrared radiation.
The Astrophysical Journal | 2013
D. C. B. Whittet; Charles A. Poteet; J. E. Chiar; L. Pagani; V. M. Bajaj; David J. Horne; Sachindev S. Shenoy; A. J. Adamson
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The Astrophysical Journal | 2013
Charles A. Poteet; Klaus M. Pontoppidan; S. Thomas Megeath; Dan M. Watson; K. Isokoski; J. E. Bjorkman; Patrick D. Sheehan; Harold Linnartz
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The Astrophysical Journal | 2016
Marina Kounkel; S. T. Megeath; Charles A. Poteet; William J. Fischer; Lee Hartmann
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