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          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 308819.0, MPI für Astronomie / Publikationen_mpia
Probing the multiphase interstellar medium of the dwarf starburst galaxy NGC 625 with FUSE spectroscopy
Authors:Cannon, J. M.; Skillman, E. D.; Sembach, K. R.; Bomans, D. J.
Date of Publication (YYYY-MM-DD):2006
Title of Proceedings:Astrophysics in the Far Ultraviolet: Five Years of Discovery with FUSE
Start Page:489
End Page:494
Title of Series:ASP Conf. Ser.
Volume (in Series):348
Name of Conference/Meeting:Astrophysics in the Far Ultraviolet: Five Years of Discovery with FUSE
Audience:Not Specified
Abstract / Description:We present new FUSE spectroscopy of the dwarf starburst galaxy NGC 625. These observations probe multiple phases of the interstellar medium, including the coronal, ionized, neutral and molecular gas. This nearby (D = 3.9 ± 0.2 Mpc) system shows a clear detection of outflowing coronal gas as traced by O VI lambda 1032 Å absorption. The centroid of the O VI profile is blueshifted with respect to the galaxy systemic velocity by ~ 30 km s-1, suggesting a low-velocity outflow. The implied O VI velocity extent is found to be 100 ± 20 km s-1, which is fully consistent with the detected H I outflow velocity found in radio synthesis observations. We detect multiple lines of diffuse H2 absorption from the ISM of NGC 625; this is one of only a few extragalactic systems with FUSE detections of H2 lines in the Lyman and Werner bands. We find a potential abundance offset between the neutral and nebular gas that exceeds the errors on the derived column densities. Since such an offset has been found in multiple dwarf galaxies, we discuss the implications of a lower-metallicity halo surrounding the central star forming regions of dwarf galaxies. The apparent offset may be due to saturation of the observed O I line, and higher S/N observations are required to resolve this issue. Because of an error in entering proof corrections, the term Mtot(t) is incorrectly identified as the gas mass in the text immediately following equation (3). The sentence following this equation should correctly read: ``The mass of the gas in the model galaxy at a time t, Mgas(t), is equal to M(t)-M*(t), where M*(t) is the mass locked up into stars at the time t.'' Regarding equation (3), it should be noted that Mtot(t)=Mtot except for those time steps t at which Mtot(t) is set to an appropriate smaller value by the Pègase2 code in order to prevent the mass in stars produced at that time step t from exceeding the mass of gas of the model galaxy at that time. The Press sincerely regrets this error.
Comment of the Author/Creator:Date: 2006, May 1, 2006
External Publication Status:published
Document Type:Conference-Paper
Communicated by:N. N.
Affiliations:MPI für Astronomie
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