Sofia/forcast observations of warm dust in S106: A fragmented environment

J. D. Adams; T. L. Herter; J. L. Hora; N. Schneider; R. M. Lau; J. G. Staguhn; R. Simon; N. Smith; R. D. Gehrz; L. E. Allen; S. Bontemps; S. J. Carey; G. G. Fazio; R. A. Gutermuth; A. Guzman Fernandez; M. Hankins; T. Hill; E. Keto; X. P. Koenig; K. E. Kraemer; S. T. Megeath; D. R. Mizuno; F. Motte; P. C. Myers; H. A. Smith

doi:10.1088/0004-637X/814/1/54

Sofia/forcast observations of warm dust in S106: A fragmented environment

J. D. Adams
, T. L. Herter
, J. L. Hora
, N. Schneider
, R. M. Lau
, J. G. Staguhn
, R. Simon
, N. Smith
, R. D. Gehrz
, L. E. Allen
, S. Bontemps
, S. J. Carey
, G. G. Fazio
, R. A. Gutermuth
, A. Guzman Fernandez
, M. Hankins
, T. Hill
, E. Keto
, X. P. Koenig
, K. E. Kraemer

S. T. Megeath, D. R. Mizuno, F. Motte, P. C. Myers, H. A. Smith

Astronomy

Research output: Contribution to journal › Article › peer-review

6 Scopus citations

Abstract

We present mid-IR (19-37 μm) imaging observations of S106 from SOFIA/FORCAST, complemented with IR observations from Spitzer/IRAC (3.6-8.0 μm), IRTF/MIRLIN (11.3 and 12.5 μm), and Herschel/PACS (70 and 160 μm). We use these observations, observations in the literature, and radiation transfer modeling to study the heating and composition of the warm (∼100 K) dust in the region. The dust is heated radiatively by the source S106 IR, with little contributions from grain-electron collisions and Lyα radiation. The dust luminosity is (9.02 ± 1.01) × 10⁴ L_o, consistent with heating by a mid- to late-type O star. We find a temperature gradient (∼75-107 K) in the lobes, which is consistent with a dusty equatorial geometry around S106 IR. Furthermore, the SOFIA observations resolve several cool (∼65-70 K) lanes and pockets of warmer (∼75-90 K) dust in the ionization shadow, indicating that the environment is fragmented. We model the dust mass as a composition of amorphous silicates, amorphous carbon, big grains, very small grains, and polycyclic aromatic hydrocarbons. We present the relative abundances of each grain component for several locations in S106.

Original language	English (US)
Article number	54
Journal	Astrophysical Journal
Volume	814
Issue number	1
DOIs	https://doi.org/10.1088/0004-637X/814/1/54
State	Published - Nov 20 2015

Keywords

H II regions
circumstellar matter
infrared: stars
radiative transfer
stars: formation

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1088/0004-637X/814/1/54

Cite this

Adams, J. D., Herter, T. L., Hora, J. L., Schneider, N., Lau, R. M., Staguhn, J. G., Simon, R., Smith, N., Gehrz, R. D., Allen, L. E., Bontemps, S., Carey, S. J., Fazio, G. G., Gutermuth, R. A., Fernandez, A. G., Hankins, M., Hill, T., Keto, E., Koenig, X. P., ... Smith, H. A. (2015). Sofia/forcast observations of warm dust in S106: A fragmented environment. Astrophysical Journal, 814(1), Article 54. https://doi.org/10.1088/0004-637X/814/1/54

Adams, JD, Herter, TL, Hora, JL, Schneider, N, Lau, RM, Staguhn, JG, Simon, R, Smith, N, Gehrz, RD, Allen, LE, Bontemps, S, Carey, SJ, Fazio, GG, Gutermuth, RA, Fernandez, AG, Hankins, M, Hill, T, Keto, E, Koenig, XP, Kraemer, KE, Megeath, ST, Mizuno, DR, Motte, F, Myers, PC & Smith, HA 2015, 'Sofia/forcast observations of warm dust in S106: A fragmented environment', Astrophysical Journal, vol. 814, no. 1, 54. https://doi.org/10.1088/0004-637X/814/1/54

@article{f2f6fe822fa34a27975e1804a7b0d3b7,

title = "Sofia/forcast observations of warm dust in S106: A fragmented environment",

abstract = "We present mid-IR (19-37 μm) imaging observations of S106 from SOFIA/FORCAST, complemented with IR observations from Spitzer/IRAC (3.6-8.0 μm), IRTF/MIRLIN (11.3 and 12.5 μm), and Herschel/PACS (70 and 160 μm). We use these observations, observations in the literature, and radiation transfer modeling to study the heating and composition of the warm (∼100 K) dust in the region. The dust is heated radiatively by the source S106 IR, with little contributions from grain-electron collisions and Lyα radiation. The dust luminosity is (9.02 ± 1.01) × 104 Lo, consistent with heating by a mid- to late-type O star. We find a temperature gradient (∼75-107 K) in the lobes, which is consistent with a dusty equatorial geometry around S106 IR. Furthermore, the SOFIA observations resolve several cool (∼65-70 K) lanes and pockets of warmer (∼75-90 K) dust in the ionization shadow, indicating that the environment is fragmented. We model the dust mass as a composition of amorphous silicates, amorphous carbon, big grains, very small grains, and polycyclic aromatic hydrocarbons. We present the relative abundances of each grain component for several locations in S106.",

keywords = "H II regions, circumstellar matter, infrared: stars, radiative transfer, stars: formation",

author = "Adams, \{J. D.\} and Herter, \{T. L.\} and Hora, \{J. L.\} and N. Schneider and Lau, \{R. M.\} and Staguhn, \{J. G.\} and R. Simon and N. Smith and Gehrz, \{R. D.\} and Allen, \{L. E.\} and S. Bontemps and Carey, \{S. J.\} and Fazio, \{G. G.\} and Gutermuth, \{R. A.\} and Fernandez, \{A. Guzman\} and M. Hankins and T. Hill and E. Keto and Koenig, \{X. P.\} and Kraemer, \{K. E.\} and Megeath, \{S. T.\} and Mizuno, \{D. R.\} and F. Motte and Myers, \{P. C.\} and Smith, \{H. A.\}",

year = "2015",

month = nov,

day = "20",

doi = "10.1088/0004-637X/814/1/54",

language = "English (US)",

volume = "814",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "American Astronomical Society",

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TY - JOUR

T1 - Sofia/forcast observations of warm dust in S106

T2 - A fragmented environment

AU - Adams, J. D.

AU - Herter, T. L.

AU - Hora, J. L.

AU - Schneider, N.

AU - Lau, R. M.

AU - Staguhn, J. G.

AU - Simon, R.

AU - Smith, N.

AU - Gehrz, R. D.

AU - Allen, L. E.

AU - Bontemps, S.

AU - Carey, S. J.

AU - Fazio, G. G.

AU - Gutermuth, R. A.

AU - Fernandez, A. Guzman

AU - Hankins, M.

AU - Hill, T.

AU - Keto, E.

AU - Koenig, X. P.

AU - Kraemer, K. E.

AU - Megeath, S. T.

AU - Mizuno, D. R.

AU - Motte, F.

AU - Myers, P. C.

AU - Smith, H. A.

PY - 2015/11/20

Y1 - 2015/11/20

N2 - We present mid-IR (19-37 μm) imaging observations of S106 from SOFIA/FORCAST, complemented with IR observations from Spitzer/IRAC (3.6-8.0 μm), IRTF/MIRLIN (11.3 and 12.5 μm), and Herschel/PACS (70 and 160 μm). We use these observations, observations in the literature, and radiation transfer modeling to study the heating and composition of the warm (∼100 K) dust in the region. The dust is heated radiatively by the source S106 IR, with little contributions from grain-electron collisions and Lyα radiation. The dust luminosity is (9.02 ± 1.01) × 104 Lo, consistent with heating by a mid- to late-type O star. We find a temperature gradient (∼75-107 K) in the lobes, which is consistent with a dusty equatorial geometry around S106 IR. Furthermore, the SOFIA observations resolve several cool (∼65-70 K) lanes and pockets of warmer (∼75-90 K) dust in the ionization shadow, indicating that the environment is fragmented. We model the dust mass as a composition of amorphous silicates, amorphous carbon, big grains, very small grains, and polycyclic aromatic hydrocarbons. We present the relative abundances of each grain component for several locations in S106.

AB - We present mid-IR (19-37 μm) imaging observations of S106 from SOFIA/FORCAST, complemented with IR observations from Spitzer/IRAC (3.6-8.0 μm), IRTF/MIRLIN (11.3 and 12.5 μm), and Herschel/PACS (70 and 160 μm). We use these observations, observations in the literature, and radiation transfer modeling to study the heating and composition of the warm (∼100 K) dust in the region. The dust is heated radiatively by the source S106 IR, with little contributions from grain-electron collisions and Lyα radiation. The dust luminosity is (9.02 ± 1.01) × 104 Lo, consistent with heating by a mid- to late-type O star. We find a temperature gradient (∼75-107 K) in the lobes, which is consistent with a dusty equatorial geometry around S106 IR. Furthermore, the SOFIA observations resolve several cool (∼65-70 K) lanes and pockets of warmer (∼75-90 K) dust in the ionization shadow, indicating that the environment is fragmented. We model the dust mass as a composition of amorphous silicates, amorphous carbon, big grains, very small grains, and polycyclic aromatic hydrocarbons. We present the relative abundances of each grain component for several locations in S106.

KW - H II regions

KW - circumstellar matter

KW - infrared: stars

KW - radiative transfer

KW - stars: formation

UR - https://www.scopus.com/pages/publications/84948696708

UR - https://www.scopus.com/pages/publications/84948696708#tab=citedBy

U2 - 10.1088/0004-637X/814/1/54

DO - 10.1088/0004-637X/814/1/54

M3 - Article

AN - SCOPUS:84948696708

SN - 0004-637X

VL - 814

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 1

M1 - 54

ER -

Sofia/forcast observations of warm dust in S106: A fragmented environment

Abstract

Keywords

ASJC Scopus subject areas

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