The galactic nature of high-velocity cloud complex WB

C. Thom; M. E. Putman; B. K. Gibson; N. Christlieb; C. Flynn; T. C. Beers; R. Wilhelm; Y. S. Lee

doi:10.1086/501005

The galactic nature of high-velocity cloud complex WB

C. Thom
, M. E. Putman
, B. K. Gibson
, N. Christlieb
, C. Flynn
, T. C. Beers
, R. Wilhelm
, Y. S. Lee

Physics And Astronomy

Producción científica: Article › revisión exhaustiva

63 Citas (Scopus)

Resumen

We have detected absorption lines from the high-velocity cloud (HVC) complex WB in the spectrum of the star HE 1048+0231. This detection sets an upper limit on the distance to the cloud of 8.8_-1.3^+2.3 kpc. Nondetection (at greater than 3 σ confidence) in the star HE 1138-1303 at 7.7 ± 0.2 kpc sets a probable lower limit. The equivalent width of the Ca II K line due to the HVC [W_λ(Ca II K) = 114.6 ± 4.4 mÅ] corresponds to a column density of N(Ca II) = (1.32 ± 0.05) × 10¹² cm^-2. Using an H I spectrum from the Leiden/Argentine/Bonn survey, we calculate N(Ca II)/N(H I) = (81 ± 16) × 10^-9. These distance limits imply an H I mass limit of 3.8 × 10⁵ M_⊙ < M_HI < 4.9 × 10⁵ M_⊙. The upper distance limit imposed by these observations shows that this HVC complex has a probable Galactic or circumgalactic origin. Future metallicity measurements will be able to confirm or refute this interpretation.

Idioma original	English
Páginas (desde-hasta)	L97-L100
Publicación	Astrophysical Journal
Volumen	638
N.º	2 II
DOI	https://doi.org/10.1086/501005
Estado	Published - feb 20 2006

Nota bibliográfica

Funding Information:
We are grateful to Rebecca Bernstein, Ian Thompson, and Steve Shectman for help with the MIKE spectrograph. We thank Scott Burles and Jason Prochaska for help with the MIKE Redux package. Thanks to Peter Kalberla for providing the LAB survey data before publication. Nathan DeLee participated in the WIYN observations, for which we are grateful. C. T. would like to thank Tuorla Observatory for its support and acknowledges travel support from the Australian Nuclear Science and Technology Organisation Access to Major Research Facilities Program. The financial support of the Australian Research Council is greatly appreciated. T. C. B. acknowledges partial support from NSF grants AST 04-06784 and PHY 02-16783.

Financiación

We are grateful to Rebecca Bernstein, Ian Thompson, and Steve Shectman for help with the MIKE spectrograph. We thank Scott Burles and Jason Prochaska for help with the MIKE Redux package. Thanks to Peter Kalberla for providing the LAB survey data before publication. Nathan DeLee participated in the WIYN observations, for which we are grateful. C. T. would like to thank Tuorla Observatory for its support and acknowledges travel support from the Australian Nuclear Science and Technology Organisation Access to Major Research Facilities Program. The financial support of the Australian Research Council is greatly appreciated. T. C. B. acknowledges partial support from NSF grants AST 04-06784 and PHY 02-16783.

Financiadores	Número del financiador
National Science Foundation (NSF)	PHY 02-16783, AST 04-06784
Australian Nuclear Science and Technology Organisation
Australian Research Council

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1086/501005

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@article{6d7aa961320847b797fba15b02b862a6,

title = "The galactic nature of high-velocity cloud complex WB",

abstract = "We have detected absorption lines from the high-velocity cloud (HVC) complex WB in the spectrum of the star HE 1048+0231. This detection sets an upper limit on the distance to the cloud of 8.8-1.3+2.3 kpc. Nondetection (at greater than 3 σ confidence) in the star HE 1138-1303 at 7.7 ± 0.2 kpc sets a probable lower limit. The equivalent width of the Ca II K line due to the HVC [Wλ(Ca II K) = 114.6 ± 4.4 m{\AA}] corresponds to a column density of N(Ca II) = (1.32 ± 0.05) × 1012 cm-2. Using an H I spectrum from the Leiden/Argentine/Bonn survey, we calculate N(Ca II)/N(H I) = (81 ± 16) × 10-9. These distance limits imply an H I mass limit of 3.8 × 105 M⊙ < MHI < 4.9 × 105 M⊙. The upper distance limit imposed by these observations shows that this HVC complex has a probable Galactic or circumgalactic origin. Future metallicity measurements will be able to confirm or refute this interpretation.",

keywords = "Galaxy: Evolution, Galaxy: Halo, ISM: Clouds, ISM: Individual (HVC complex WB)",

author = "C. Thom and Putman, \{M. E.\} and Gibson, \{B. K.\} and N. Christlieb and C. Flynn and Beers, \{T. C.\} and R. Wilhelm and Lee, \{Y. S.\}",

note = "Funding Information: We are grateful to Rebecca Bernstein, Ian Thompson, and Steve Shectman for help with the MIKE spectrograph. We thank Scott Burles and Jason Prochaska for help with the MIKE Redux package. Thanks to Peter Kalberla for providing the LAB survey data before publication. Nathan DeLee participated in the WIYN observations, for which we are grateful. C. T. would like to thank Tuorla Observatory for its support and acknowledges travel support from the Australian Nuclear Science and Technology Organisation Access to Major Research Facilities Program. The financial support of the Australian Research Council is greatly appreciated. T. C. B. acknowledges partial support from NSF grants AST 04-06784 and PHY 02-16783.",

year = "2006",

month = feb,

day = "20",

doi = "10.1086/501005",

language = "English",

volume = "638",

pages = "L97--L100",

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T1 - The galactic nature of high-velocity cloud complex WB

AU - Thom, C.

AU - Putman, M. E.

AU - Gibson, B. K.

AU - Christlieb, N.

AU - Flynn, C.

AU - Beers, T. C.

AU - Wilhelm, R.

AU - Lee, Y. S.

N1 - Funding Information: We are grateful to Rebecca Bernstein, Ian Thompson, and Steve Shectman for help with the MIKE spectrograph. We thank Scott Burles and Jason Prochaska for help with the MIKE Redux package. Thanks to Peter Kalberla for providing the LAB survey data before publication. Nathan DeLee participated in the WIYN observations, for which we are grateful. C. T. would like to thank Tuorla Observatory for its support and acknowledges travel support from the Australian Nuclear Science and Technology Organisation Access to Major Research Facilities Program. The financial support of the Australian Research Council is greatly appreciated. T. C. B. acknowledges partial support from NSF grants AST 04-06784 and PHY 02-16783.

PY - 2006/2/20

Y1 - 2006/2/20

N2 - We have detected absorption lines from the high-velocity cloud (HVC) complex WB in the spectrum of the star HE 1048+0231. This detection sets an upper limit on the distance to the cloud of 8.8-1.3+2.3 kpc. Nondetection (at greater than 3 σ confidence) in the star HE 1138-1303 at 7.7 ± 0.2 kpc sets a probable lower limit. The equivalent width of the Ca II K line due to the HVC [Wλ(Ca II K) = 114.6 ± 4.4 mÅ] corresponds to a column density of N(Ca II) = (1.32 ± 0.05) × 1012 cm-2. Using an H I spectrum from the Leiden/Argentine/Bonn survey, we calculate N(Ca II)/N(H I) = (81 ± 16) × 10-9. These distance limits imply an H I mass limit of 3.8 × 105 M⊙ < MHI < 4.9 × 105 M⊙. The upper distance limit imposed by these observations shows that this HVC complex has a probable Galactic or circumgalactic origin. Future metallicity measurements will be able to confirm or refute this interpretation.

AB - We have detected absorption lines from the high-velocity cloud (HVC) complex WB in the spectrum of the star HE 1048+0231. This detection sets an upper limit on the distance to the cloud of 8.8-1.3+2.3 kpc. Nondetection (at greater than 3 σ confidence) in the star HE 1138-1303 at 7.7 ± 0.2 kpc sets a probable lower limit. The equivalent width of the Ca II K line due to the HVC [Wλ(Ca II K) = 114.6 ± 4.4 mÅ] corresponds to a column density of N(Ca II) = (1.32 ± 0.05) × 1012 cm-2. Using an H I spectrum from the Leiden/Argentine/Bonn survey, we calculate N(Ca II)/N(H I) = (81 ± 16) × 10-9. These distance limits imply an H I mass limit of 3.8 × 105 M⊙ < MHI < 4.9 × 105 M⊙. The upper distance limit imposed by these observations shows that this HVC complex has a probable Galactic or circumgalactic origin. Future metallicity measurements will be able to confirm or refute this interpretation.

KW - Galaxy: Evolution

KW - Galaxy: Halo

KW - ISM: Clouds

KW - ISM: Individual (HVC complex WB)

UR - https://www.scopus.com/pages/publications/33644798408

UR - https://www.scopus.com/pages/publications/33644798408#tab=citedBy

U2 - 10.1086/501005

DO - 10.1086/501005

M3 - Article

AN - SCOPUS:33644798408

SN - 0004-637X

VL - 638

SP - L97-L100

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2 II

ER -

The galactic nature of high-velocity cloud complex WB

Resumen

Nota bibliográfica

Financiación

ASJC Scopus subject areas

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