The c2d Spitzer spectroscopic survey of ices around low-mass young stellar objects. I. H2O and the 5-8 μm bands

A. C.A. Boogert; K. M. Pontoppidan; C. Knez; F. Lahuis; J. Kessler-Silacci; E. F. Van Dishoeck; G. A. Blake; J. C. Augereau; S. E. Bisschop; S. Bottinelli; T. Y. Brooke; J. Brown; A. Crapsi; N. J. Evans; H. J. Fraser; V. Geers; T. L. Huard; J. K. Jørgensen; K. I. Öberg; L. E. Allen; P. M. Harvey; D. W. Koerner; L. G. Mundy; D. L. Padgett; A. I. Sargent; K. R. Stapelfeldt

doi:10.1086/533425

The c2d Spitzer spectroscopic survey of ices around low-mass young stellar objects. I. H₂O and the 5-8 μm bands

A. C.A. Boogert, K. M. Pontoppidan, C. Knez, F. Lahuis, J. Kessler-Silacci, E. F. Van Dishoeck, G. A. Blake, J. C. Augereau, S. E. Bisschop, S. Bottinelli, T. Y. Brooke, J. Brown, A. Crapsi, N. J. Evans, H. J. Fraser, V. Geers, T. L. Huard, J. K. Jørgensen, K. I. Öberg, L. E. AllenP. M. Harvey, D. W. Koerner, L. G. Mundy, D. L. Padgett, A. I. Sargent, K. R. Stapelfeldt

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Abstract

To study the physical and chemical evolution of ices in solar-mass systems, a spectral survey is conducted of a sample of 41 low-luminosity YSOs(L, ∼ 0.1-10 L_⊙) using 3-38 μm. Spitzer and ground-based spectra. The sample is complemented with previously published Spitzer spectra of background stars and with ISO spectra of well-studied massive YSOs (L ∼ 10⁵ L_⊙). The long-known 6.0 and 6.85 μm bands are detected toward all sources, with the Class 0-type YSOs showing the deepest bands ever observed. The 6.0 μm band is often deeper than expected from the bending mode of pure solid H₂O. The additional 5-7 μm absorption consists of five independent components, which, by comparison to laboratory studies, must be from at least eight different carriers. Much of this absorption is due to simple species likely formed by grain surface chemistry, at abundances of 1%-30% for CH₃OH, 3%-8% for NH₃, 1%-5% for HCOOH, ∼6% for H₂CO, and ∼0.3% for HCOO^- relative to solid H₂O. The 6.85 μm band has one or two carriers, of which one may be less volatile than H₂O. Its carrier(s) formed early in the molecular cloud evolution and do not survive in the diffuse ISM. If an NH ₄⁺-containing salt is the carrier, its abundance relative to solid H₂O is ∼7%, demonstrating the efficiency of low-temperature acid-base chemistry or cosmic-ray-induced reactions. Possible origins are discussed for enigmatic, very broad absorption between 5 and 8 μm. Finally, the same ices are observed toward massive and low-mass YSOs, indicating that processing by internal UV radiation fields is a minor factor in their early chemical evolution.

Original language	English
Journal	Astrophysical Journal
Volume	678
Issue number	2
Pages (from-to)	985-1004
Number of pages	20
ISSN	0004-637X
DOIs	https://doi.org/10.1086/533425
Publication status	Published - 10 May 2008

Keywords

Astrochemistry
Infrared: ISM
Infrared: Stars
ISM: Abundances
ISM: Molecules
Stars: Formation

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10.1086/533425

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Boogert, A. C. A., Pontoppidan, K. M., Knez, C., Lahuis, F., Kessler-Silacci, J., Van Dishoeck, E. F., Blake, G. A., Augereau, J. C., Bisschop, S. E., Bottinelli, S., Brooke, T. Y., Brown, J., Crapsi, A., Evans, N. J., Fraser, H. J., Geers, V., Huard, T. L., Jørgensen, J. K., Öberg, K. I., ... Stapelfeldt, K. R. (2008). The c2d Spitzer spectroscopic survey of ices around low-mass young stellar objects. I. H₂O and the 5-8 μm bands. Astrophysical Journal, 678(2), 985-1004. https://doi.org/10.1086/533425

Boogert, ACA, Pontoppidan, KM, Knez, C, Lahuis, F, Kessler-Silacci, J, Van Dishoeck, EF, Blake, GA, Augereau, JC, Bisschop, SE, Bottinelli, S, Brooke, TY, Brown, J, Crapsi, A, Evans, NJ, Fraser, HJ, Geers, V, Huard, TL, Jørgensen, JK, Öberg, KI, Allen, LE, Harvey, PM, Koerner, DW, Mundy, LG, Padgett, DL, Sargent, AI & Stapelfeldt, KR 2008, 'The c2d Spitzer spectroscopic survey of ices around low-mass young stellar objects. I. H₂O and the 5-8 μm bands', Astrophysical Journal, vol. 678, no. 2, pp. 985-1004. https://doi.org/10.1086/533425

@article{6d1de27f3f88400697b5e80b48074056,

title = "The c2d Spitzer spectroscopic survey of ices around low-mass young stellar objects. I. H2O and the 5-8 μm bands",

abstract = "To study the physical and chemical evolution of ices in solar-mass systems, a spectral survey is conducted of a sample of 41 low-luminosity YSOs(L, ∼ 0.1-10 L⊙) using 3-38 μm. Spitzer and ground-based spectra. The sample is complemented with previously published Spitzer spectra of background stars and with ISO spectra of well-studied massive YSOs (L ∼ 105 L⊙). The long-known 6.0 and 6.85 μm bands are detected toward all sources, with the Class 0-type YSOs showing the deepest bands ever observed. The 6.0 μm band is often deeper than expected from the bending mode of pure solid H2O. The additional 5-7 μm absorption consists of five independent components, which, by comparison to laboratory studies, must be from at least eight different carriers. Much of this absorption is due to simple species likely formed by grain surface chemistry, at abundances of 1%-30% for CH3OH, 3%-8% for NH3, 1%-5% for HCOOH, ∼6% for H2CO, and ∼0.3% for HCOO- relative to solid H2O. The 6.85 μm band has one or two carriers, of which one may be less volatile than H2O. Its carrier(s) formed early in the molecular cloud evolution and do not survive in the diffuse ISM. If an NH 4+-containing salt is the carrier, its abundance relative to solid H2O is ∼7%, demonstrating the efficiency of low-temperature acid-base chemistry or cosmic-ray-induced reactions. Possible origins are discussed for enigmatic, very broad absorption between 5 and 8 μm. Finally, the same ices are observed toward massive and low-mass YSOs, indicating that processing by internal UV radiation fields is a minor factor in their early chemical evolution.",

keywords = "Astrochemistry, Infrared: ISM, Infrared: Stars, ISM: Abundances, ISM: Molecules, Stars: Formation",

author = "Boogert, {A. C.A.} and Pontoppidan, {K. M.} and C. Knez and F. Lahuis and J. Kessler-Silacci and {Van Dishoeck}, {E. F.} and Blake, {G. A.} and Augereau, {J. C.} and Bisschop, {S. E.} and S. Bottinelli and Brooke, {T. Y.} and J. Brown and A. Crapsi and Evans, {N. J.} and Fraser, {H. J.} and V. Geers and Huard, {T. L.} and J{\o}rgensen, {J. K.} and {\"O}berg, {K. I.} and Allen, {L. E.} and Harvey, {P. M.} and Koerner, {D. W.} and Mundy, {L. G.} and Padgett, {D. L.} and Sargent, {A. I.} and Stapelfeldt, {K. R.}",

year = "2008",

month = may,

day = "10",

doi = "10.1086/533425",

language = "English",

volume = "678",

pages = "985--1004",

journal = "Astrophysical Journal",

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publisher = "Institute of Physics Publishing, Inc",

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T1 - The c2d Spitzer spectroscopic survey of ices around low-mass young stellar objects. I. H2O and the 5-8 μm bands

AU - Boogert, A. C.A.

AU - Pontoppidan, K. M.

AU - Knez, C.

AU - Lahuis, F.

AU - Kessler-Silacci, J.

AU - Van Dishoeck, E. F.

AU - Blake, G. A.

AU - Augereau, J. C.

AU - Bisschop, S. E.

AU - Bottinelli, S.

AU - Brooke, T. Y.

AU - Brown, J.

AU - Crapsi, A.

AU - Evans, N. J.

AU - Fraser, H. J.

AU - Geers, V.

AU - Huard, T. L.

AU - Jørgensen, J. K.

AU - Öberg, K. I.

AU - Allen, L. E.

AU - Harvey, P. M.

AU - Koerner, D. W.

AU - Mundy, L. G.

AU - Padgett, D. L.

AU - Sargent, A. I.

AU - Stapelfeldt, K. R.

PY - 2008/5/10

Y1 - 2008/5/10

N2 - To study the physical and chemical evolution of ices in solar-mass systems, a spectral survey is conducted of a sample of 41 low-luminosity YSOs(L, ∼ 0.1-10 L⊙) using 3-38 μm. Spitzer and ground-based spectra. The sample is complemented with previously published Spitzer spectra of background stars and with ISO spectra of well-studied massive YSOs (L ∼ 105 L⊙). The long-known 6.0 and 6.85 μm bands are detected toward all sources, with the Class 0-type YSOs showing the deepest bands ever observed. The 6.0 μm band is often deeper than expected from the bending mode of pure solid H2O. The additional 5-7 μm absorption consists of five independent components, which, by comparison to laboratory studies, must be from at least eight different carriers. Much of this absorption is due to simple species likely formed by grain surface chemistry, at abundances of 1%-30% for CH3OH, 3%-8% for NH3, 1%-5% for HCOOH, ∼6% for H2CO, and ∼0.3% for HCOO- relative to solid H2O. The 6.85 μm band has one or two carriers, of which one may be less volatile than H2O. Its carrier(s) formed early in the molecular cloud evolution and do not survive in the diffuse ISM. If an NH 4+-containing salt is the carrier, its abundance relative to solid H2O is ∼7%, demonstrating the efficiency of low-temperature acid-base chemistry or cosmic-ray-induced reactions. Possible origins are discussed for enigmatic, very broad absorption between 5 and 8 μm. Finally, the same ices are observed toward massive and low-mass YSOs, indicating that processing by internal UV radiation fields is a minor factor in their early chemical evolution.

AB - To study the physical and chemical evolution of ices in solar-mass systems, a spectral survey is conducted of a sample of 41 low-luminosity YSOs(L, ∼ 0.1-10 L⊙) using 3-38 μm. Spitzer and ground-based spectra. The sample is complemented with previously published Spitzer spectra of background stars and with ISO spectra of well-studied massive YSOs (L ∼ 105 L⊙). The long-known 6.0 and 6.85 μm bands are detected toward all sources, with the Class 0-type YSOs showing the deepest bands ever observed. The 6.0 μm band is often deeper than expected from the bending mode of pure solid H2O. The additional 5-7 μm absorption consists of five independent components, which, by comparison to laboratory studies, must be from at least eight different carriers. Much of this absorption is due to simple species likely formed by grain surface chemistry, at abundances of 1%-30% for CH3OH, 3%-8% for NH3, 1%-5% for HCOOH, ∼6% for H2CO, and ∼0.3% for HCOO- relative to solid H2O. The 6.85 μm band has one or two carriers, of which one may be less volatile than H2O. Its carrier(s) formed early in the molecular cloud evolution and do not survive in the diffuse ISM. If an NH 4+-containing salt is the carrier, its abundance relative to solid H2O is ∼7%, demonstrating the efficiency of low-temperature acid-base chemistry or cosmic-ray-induced reactions. Possible origins are discussed for enigmatic, very broad absorption between 5 and 8 μm. Finally, the same ices are observed toward massive and low-mass YSOs, indicating that processing by internal UV radiation fields is a minor factor in their early chemical evolution.

KW - Astrochemistry

KW - Infrared: ISM

KW - Infrared: Stars

KW - ISM: Abundances

KW - ISM: Molecules

KW - Stars: Formation

UR - http://www.scopus.com/inward/record.url?scp=43949130406&partnerID=8YFLogxK

U2 - 10.1086/533425

DO - 10.1086/533425

M3 - Journal article

AN - SCOPUS:43949130406

SN - 0004-637X

VL - 678

SP - 985

EP - 1004

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

ER -

The c2d Spitzer spectroscopic survey of ices around low-mass young stellar objects. I. H₂O and the 5-8 μm bands

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Keywords

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