Origin of the hot gas in low-mass protostars: Herschel-PACS spectroscopy of HH 46

T. A. van Kempen; L. E. Kristensen; G. J. Herczeg; R. Visser; E. F. van Dishoeck; S. F. Wampfler; S. Bruderer; A. O. Benz; S. D. Doty; C. Brinch; M. R. Hogerheijde; J. K. Jorgensen; M. Tafalla; D. Neufeld; R. Bachiller; A. Baudry; M. Benedettini; E. A. Bergin; P. Bjerkeli; G.A. Blake; S. Bontemps; J. Braine; P. Caselli; J. Cernicharo; C. Codella; F. Daniel; A. M. di Giorgio; C. Dominik; P. Encrenaz; M. Fich; A. Fuente; T. Giannini; J. R. Goicoechea; Th. de Graauw; F. Helmich; F. Herpin; T. Jacq; D. Johnstone; M. J. Kaufman; B. Larsson; D. Lis; R. Liseau; M. Marseille; C. McCoey; G. Melnick; B. Nisini; M. Olberg; B. Parise; J. C. Pearson; R. Plume; C. Risacher; J. Santiago-Garcia; P. Saraceno; R. Shipman; F. van der Tak; F. Wyrowski; U. A. Yildiz; M. Ciechanowicz; L. Dubbeldam; S. Glenz; R. Huisman; R. H. Lin; P. Morris; J. A. Murphy; N. Trappe

doi:10.1051/0004-6361/201014615

Origin of the hot gas in low-mass protostars: Herschel-PACS spectroscopy of HH 46

T. A. van Kempen^*, L. E. Kristensen, G. J. Herczeg, R. Visser, E. F. van Dishoeck, S. F. Wampfler, S. Bruderer, A. O. Benz, S. D. Doty, C. Brinch, M. R. Hogerheijde, J. K. Jorgensen, M. Tafalla, D. Neufeld, R. Bachiller, A. Baudry, M. Benedettini, E. A. Bergin, P. Bjerkeli, G.A. BlakeS. Bontemps, J. Braine, P. Caselli, J. Cernicharo, C. Codella, F. Daniel, A. M. di Giorgio, C. Dominik, P. Encrenaz, M. Fich, A. Fuente, T. Giannini, J. R. Goicoechea, Th. de Graauw, F. Helmich, F. Herpin, T. Jacq, D. Johnstone, M. J. Kaufman, B. Larsson, D. Lis, R. Liseau, M. Marseille, C. McCoey, G. Melnick, B. Nisini, M. Olberg, B. Parise, J. C. Pearson, R. Plume, C. Risacher, J. Santiago-Garcia, P. Saraceno, R. Shipman, F. van der Tak, F. Wyrowski, U. A. Yildiz, M. Ciechanowicz, L. Dubbeldam, S. Glenz, R. Huisman, R. H. Lin, P. Morris, J. A. Murphy, N. Trappe

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Aims: “Water In Star-forming regions with Herschel” (WISH) is a Herschel key programme aimed at understanding the physical and chemical structure of young stellar objects (YSOs) with a focus on water and related species. Methods: The low-mass protostar HH 46 was observed with the Photodetector Array Camera and Spectrometer (PACS) on the Herschel Space Observatory to measure emission in H2O, CO, OH, [O i], and [C ii] lines located between 63 and 186 μm. The excitation and spatial distribution of emission can disentangle the different heating mechanisms of YSOs, with better spatial resolution and sensitivity than previously possible. Results: Far-IR line emission is detected at the position of the protostar and along the outflow axis. The OH emission is concentrated at the central position, CO emission is bright at the central position and along the outflow, and H2O emission is concentrated in the outflow. In addition, [O i] emission is seen in low-velocity gas, assumed to be related to the envelope, and is also seen shifted up to 170 km s-1 in both the red- and blue-shifted jets. Envelope models are constructed based on previous observational constraints. They indicate that passive heating of a spherical envelope by the protostellar luminosity cannot explain the high-excitation molecular gas detected with PACS, including CO lines with upper levels at >2500 K above the ground state. Instead, warm CO and H2O emission is probably produced in the walls of an outflow-carved cavity in the envelope, which are heated by UV photons and non-dissociative C-type shocks. The bright OH and [O i] emission is attributed to J-type shocks in dense gas close to the protostar. In the scenario described here, the combined cooling by far-IR lines within the central spatial pixel is estimated to be 2 × 10-2 L_⊙, with 60-80% attributed to J- and C-type shocks produced by interactions between the jet and the envelope. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Table 2 is only available in electronic form at http//www.aanda.org

Originele taal-2	English
Artikelnummer	L121
Aantal pagina's	6
Tijdschrift	Astronomy & Astrophysics
Volume	518
DOI's	https://doi.org/10.1051/0004-6361/201014615
Status	Published - jul.-2010

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van Kempen, T. A., Kristensen, L. E., Herczeg, G. J., Visser, R., van Dishoeck, E. F., Wampfler, S. F., Bruderer, S., Benz, A. O., Doty, S. D., Brinch, C., Hogerheijde, M. R., Jorgensen, J. K., Tafalla, M., Neufeld, D., Bachiller, R., Baudry, A., Benedettini, M., Bergin, E. A., Bjerkeli, P., ... Trappe, N. (2010). Origin of the hot gas in low-mass protostars: Herschel-PACS spectroscopy of HH 46. Astronomy & Astrophysics, 518, Artikel L121. https://doi.org/10.1051/0004-6361/201014615

@article{b7718638d5194437b3a1f1d604caa5a8,

title = "Origin of the hot gas in low-mass protostars: Herschel-PACS spectroscopy of HH 46",

abstract = "Aims: “Water In Star-forming regions with Herschel” (WISH) is a Herschel key programme aimed at understanding the physical and chemical structure of young stellar objects (YSOs) with a focus on water and related species. Methods: The low-mass protostar HH 46 was observed with the Photodetector Array Camera and Spectrometer (PACS) on the Herschel Space Observatory to measure emission in H2O, CO, OH, [O i], and [C ii] lines located between 63 and 186 μm. The excitation and spatial distribution of emission can disentangle the different heating mechanisms of YSOs, with better spatial resolution and sensitivity than previously possible. Results: Far-IR line emission is detected at the position of the protostar and along the outflow axis. The OH emission is concentrated at the central position, CO emission is bright at the central position and along the outflow, and H2O emission is concentrated in the outflow. In addition, [O i] emission is seen in low-velocity gas, assumed to be related to the envelope, and is also seen shifted up to 170 km s-1 in both the red- and blue-shifted jets. Envelope models are constructed based on previous observational constraints. They indicate that passive heating of a spherical envelope by the protostellar luminosity cannot explain the high-excitation molecular gas detected with PACS, including CO lines with upper levels at >2500 K above the ground state. Instead, warm CO and H2O emission is probably produced in the walls of an outflow-carved cavity in the envelope, which are heated by UV photons and non-dissociative C-type shocks. The bright OH and [O i] emission is attributed to J-type shocks in dense gas close to the protostar. In the scenario described here, the combined cooling by far-IR lines within the central spatial pixel is estimated to be 2 × 10-2 L_⊙, with 60-80% attributed to J- and C-type shocks produced by interactions between the jet and the envelope. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Table 2 is only available in electronic form at http//www.aanda.org",

keywords = "astrochemistry, stars: formation, ISM: molecules, ISM: jets and outflows, ISM: individual objects: HH 46, EMISSION, WATER, SHOCK, HH-46/47, OUTFLOW, JETS, I.",

author = "{van Kempen}, {T. A.} and Kristensen, {L. E.} and Herczeg, {G. J.} and R. Visser and {van Dishoeck}, {E. F.} and Wampfler, {S. F.} and S. Bruderer and Benz, {A. O.} and Doty, {S. D.} and C. Brinch and Hogerheijde, {M. R.} and Jorgensen, {J. K.} and M. Tafalla and D. Neufeld and R. Bachiller and A. Baudry and M. Benedettini and Bergin, {E. A.} and P. Bjerkeli and G.A. Blake and S. Bontemps and J. Braine and P. Caselli and J. Cernicharo and C. Codella and F. Daniel and {di Giorgio}, {A. M.} and C. Dominik and P. Encrenaz and M. Fich and A. Fuente and T. Giannini and Goicoechea, {J. R.} and {de Graauw}, Th. and F. Helmich and F. Herpin and T. Jacq and D. Johnstone and Kaufman, {M. J.} and B. Larsson and D. Lis and R. Liseau and M. Marseille and C. McCoey and G. Melnick and B. Nisini and M. Olberg and B. Parise and Pearson, {J. C.} and R. Plume and C. Risacher and J. Santiago-Garcia and P. Saraceno and R. Shipman and {van der Tak}, F. and F. Wyrowski and Yildiz, {U. A.} and M. Ciechanowicz and L. Dubbeldam and S. Glenz and R. Huisman and Lin, {R. H.} and P. Morris and Murphy, {J. A.} and N. Trappe",

year = "2010",

month = jul,

doi = "10.1051/0004-6361/201014615",

language = "English",

volume = "518",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = " EDP Sciences",

}

van Kempen, TA, Kristensen, LE, Herczeg, GJ, Visser, R, van Dishoeck, EF, Wampfler, SF, Bruderer, S, Benz, AO, Doty, SD, Brinch, C, Hogerheijde, MR, Jorgensen, JK, Tafalla, M, Neufeld, D, Bachiller, R, Baudry, A, Benedettini, M, Bergin, EA, Bjerkeli, P, Blake, GA, Bontemps, S, Braine, J, Caselli, P, Cernicharo, J, Codella, C, Daniel, F, di Giorgio, AM, Dominik, C, Encrenaz, P, Fich, M, Fuente, A, Giannini, T, Goicoechea, JR, de Graauw, T, Helmich, F, Herpin, F, Jacq, T, Johnstone, D, Kaufman, MJ, Larsson, B, Lis, D, Liseau, R, Marseille, M, McCoey, C, Melnick, G, Nisini, B, Olberg, M, Parise, B, Pearson, JC, Plume, R, Risacher, C, Santiago-Garcia, J, Saraceno, P, Shipman, R , van der Tak, F, Wyrowski, F, Yildiz, UA, Ciechanowicz, M, Dubbeldam, L, Glenz, S, Huisman, R, Lin, RH, Morris, P, Murphy, JA & Trappe, N 2010, 'Origin of the hot gas in low-mass protostars: Herschel-PACS spectroscopy of HH 46', Astronomy & Astrophysics, vol. 518, L121. https://doi.org/10.1051/0004-6361/201014615

TY - JOUR

T1 - Origin of the hot gas in low-mass protostars

T2 - Herschel-PACS spectroscopy of HH 46

AU - van Kempen, T. A.

AU - Kristensen, L. E.

AU - Herczeg, G. J.

AU - Visser, R.

AU - van Dishoeck, E. F.

AU - Wampfler, S. F.

AU - Bruderer, S.

AU - Benz, A. O.

AU - Doty, S. D.

AU - Brinch, C.

AU - Hogerheijde, M. R.

AU - Jorgensen, J. K.

AU - Tafalla, M.

AU - Neufeld, D.

AU - Bachiller, R.

AU - Baudry, A.

AU - Benedettini, M.

AU - Bergin, E. A.

AU - Bjerkeli, P.

AU - Blake, G.A.

AU - Bontemps, S.

AU - Braine, J.

AU - Caselli, P.

AU - Cernicharo, J.

AU - Codella, C.

AU - Daniel, F.

AU - di Giorgio, A. M.

AU - Dominik, C.

AU - Encrenaz, P.

AU - Fich, M.

AU - Fuente, A.

AU - Giannini, T.

AU - Goicoechea, J. R.

AU - de Graauw, Th.

AU - Helmich, F.

AU - Herpin, F.

AU - Jacq, T.

AU - Johnstone, D.

AU - Kaufman, M. J.

AU - Larsson, B.

AU - Lis, D.

AU - Liseau, R.

AU - Marseille, M.

AU - McCoey, C.

AU - Melnick, G.

AU - Nisini, B.

AU - Olberg, M.

AU - Parise, B.

AU - Pearson, J. C.

AU - Plume, R.

AU - Risacher, C.

AU - Santiago-Garcia, J.

AU - Saraceno, P.

AU - Shipman, R.

AU - van der Tak, F.

AU - Wyrowski, F.

AU - Yildiz, U. A.

AU - Ciechanowicz, M.

AU - Dubbeldam, L.

AU - Glenz, S.

AU - Huisman, R.

AU - Lin, R. H.

AU - Morris, P.

AU - Murphy, J. A.

AU - Trappe, N.

PY - 2010/7

Y1 - 2010/7

N2 - Aims: “Water In Star-forming regions with Herschel” (WISH) is a Herschel key programme aimed at understanding the physical and chemical structure of young stellar objects (YSOs) with a focus on water and related species. Methods: The low-mass protostar HH 46 was observed with the Photodetector Array Camera and Spectrometer (PACS) on the Herschel Space Observatory to measure emission in H2O, CO, OH, [O i], and [C ii] lines located between 63 and 186 μm. The excitation and spatial distribution of emission can disentangle the different heating mechanisms of YSOs, with better spatial resolution and sensitivity than previously possible. Results: Far-IR line emission is detected at the position of the protostar and along the outflow axis. The OH emission is concentrated at the central position, CO emission is bright at the central position and along the outflow, and H2O emission is concentrated in the outflow. In addition, [O i] emission is seen in low-velocity gas, assumed to be related to the envelope, and is also seen shifted up to 170 km s-1 in both the red- and blue-shifted jets. Envelope models are constructed based on previous observational constraints. They indicate that passive heating of a spherical envelope by the protostellar luminosity cannot explain the high-excitation molecular gas detected with PACS, including CO lines with upper levels at >2500 K above the ground state. Instead, warm CO and H2O emission is probably produced in the walls of an outflow-carved cavity in the envelope, which are heated by UV photons and non-dissociative C-type shocks. The bright OH and [O i] emission is attributed to J-type shocks in dense gas close to the protostar. In the scenario described here, the combined cooling by far-IR lines within the central spatial pixel is estimated to be 2 × 10-2 L_⊙, with 60-80% attributed to J- and C-type shocks produced by interactions between the jet and the envelope. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Table 2 is only available in electronic form at http//www.aanda.org

AB - Aims: “Water In Star-forming regions with Herschel” (WISH) is a Herschel key programme aimed at understanding the physical and chemical structure of young stellar objects (YSOs) with a focus on water and related species. Methods: The low-mass protostar HH 46 was observed with the Photodetector Array Camera and Spectrometer (PACS) on the Herschel Space Observatory to measure emission in H2O, CO, OH, [O i], and [C ii] lines located between 63 and 186 μm. The excitation and spatial distribution of emission can disentangle the different heating mechanisms of YSOs, with better spatial resolution and sensitivity than previously possible. Results: Far-IR line emission is detected at the position of the protostar and along the outflow axis. The OH emission is concentrated at the central position, CO emission is bright at the central position and along the outflow, and H2O emission is concentrated in the outflow. In addition, [O i] emission is seen in low-velocity gas, assumed to be related to the envelope, and is also seen shifted up to 170 km s-1 in both the red- and blue-shifted jets. Envelope models are constructed based on previous observational constraints. They indicate that passive heating of a spherical envelope by the protostellar luminosity cannot explain the high-excitation molecular gas detected with PACS, including CO lines with upper levels at >2500 K above the ground state. Instead, warm CO and H2O emission is probably produced in the walls of an outflow-carved cavity in the envelope, which are heated by UV photons and non-dissociative C-type shocks. The bright OH and [O i] emission is attributed to J-type shocks in dense gas close to the protostar. In the scenario described here, the combined cooling by far-IR lines within the central spatial pixel is estimated to be 2 × 10-2 L_⊙, with 60-80% attributed to J- and C-type shocks produced by interactions between the jet and the envelope. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Table 2 is only available in electronic form at http//www.aanda.org

KW - astrochemistry

KW - stars: formation

KW - ISM: molecules

KW - ISM: jets and outflows

KW - ISM: individual objects: HH 46

KW - EMISSION

KW - WATER

KW - SHOCK

KW - HH-46/47

KW - OUTFLOW

KW - JETS

KW - I.

UR - http://adsabs.harvard.edu/abs/2010A%26A...518L.121V

U2 - 10.1051/0004-6361/201014615

DO - 10.1051/0004-6361/201014615

M3 - Article

SN - 0004-6361

VL - 518

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

M1 - L121

ER -

Origin of the hot gas in low-mass protostars: Herschel-PACS spectroscopy of HH 46

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