Neutral hydrogen profiles of cluster galaxies

Mould, Jeremy; Martín, S.; Bothun, G. D.; Huchra, J. P.; Schommer, B.

doi:10.1086/192111

Cited by 9 publications

(3 citation statements)

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“…Other a (1950) Mould et al 1995 ;(8) Mathewson & Ford 1996 ;(9) et al 1990 ; (10) Magri 1994 ; (11) Gavazzi et al 1996 ;(12) Gavazzi 1989 ; (13) Fouque Giovanelli & Haynes 1985. presented in Haynes, Giovanelli, & Chamaraux (1999a). The H I widths presented here are used for our analysis of the local peculiar velocity Ðeld via the TF relation (Giovanelli et al 1997d(Giovanelli et al , 1998b(Giovanelli et al , 1998cBorgani et al 1997 ;da Costa et al 1996da Costa et al , 1998Freudling et al 1999).…”

Section: Numbermentioning

confidence: 99%

The [ITAL]I[/ITAL]-Band Tully-Fisher Relation for S[CLC]c[/CLC] Galaxies: 21 Centimeter H [CSC]i[/CSC] Line Data

Haynes

Giovanelli

Chamaraux

et al. 1999

The Astronomical Journal

119

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A compilation of 21 cm line spectral parameters speciÐcally designed for application of the TullyFisher (TF) distance method is presented for 1201 spiral galaxies, primarily Ðeld Sc galaxies, for which optical I-band photometric imaging is also available. New H I line spectra have been obtained for 881 galaxies. For an additional 320 galaxies, spectra available in a digital archive have been reexamined to allow application of a single algorithm for the derivation of the TF velocity width parameter. A velocity width algorithm is used that provides a robust measurement of rotational velocity and permits an estimate of the error on that width taking into account the e †ects of instrumental broadening and signal-tonoise. The digital data are used to establish regression relations between measurements of velocity widths using other common prescriptions so that comparable widths can be derived through conversion of values published in the literature. The uniform H I line widths presented here provide the rotational velocity measurement to be used in deriving peculiar velocities via the TF method.

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Section: Numbermentioning

confidence: 99%

The [ITAL]I[/ITAL]-Band Tully-Fisher Relation for S[CLC]c[/CLC] Galaxies: 21 Centimeter H [CSC]i[/CSC] Line Data

Haynes

Giovanelli

Chamaraux

et al. 1999

The Astronomical Journal

119

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“…Therefore, NGC 5514 and 5519-with ∆V = 120 km s −1 -are probably associated. We note that Mould et al (1993Mould et al ( , 1995 included NGC 5519 in their study of nearby groups and clusters of galaxies, within the 100 Mpc.…”

Section: The Ngc 5514 Small Group Of Galaxiesmentioning

confidence: 99%

Infrared mergers and infrared quasi-stellar objects with galactic winds - II. NGC 5514: two extranuclear starbursts with LINER properties and a supergiant bubble in the rupture phase

Lípari

Mediavilla

García-Lorenzo

et al. 2004

Monthly Notices of the Royal Astronomical Society

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A study of the morphology, kinematics and ionization structure of the infrared (IR) merger NGC 5514 is presented. This study is based mainly on INTEGRAL two-dimensional (2D) spectroscopy (obtained at the 4.2-m William Herschel Telescope, WHT), plus optical and near-IR images. Clear evidence of two extranuclear starbursts with young outflows (OFs) and low-ionization nuclear emission region (LINER) activity are reported. One of these OFs has generated a supergiant bubble and the other is associated with an extended complex of H II regions.In the galactic bubble it was found that: (i) the [S II], Hα, [N II], [O I] and [O III] emissionline maps show a bubble with a distorted ellipsoidal shape, with major and minor axes of ∼6.5 kpc [13.6 arcsec; at position angle (PA) = 120• ± 10 • ] and ∼4.5 kpc (9.6 arcsec); (ii) these maps depict four main knots, a very strong one and three others more compact and located at the border; (iii) the centre of the bubble is located at ∼4.1 kpc (8.5 arcsec) to the west of the main nucleus; (iv) the WHT spectra show, in this area, two strong components: blue and red emission-line systems, probably associated with emission from the near and far side of the external shell, for which the mean OF velocities were measured as V OF blue = (−320 ± 20) km s −1 and V OF red = (+265 ± 25) km s −1 ; (v) these two components depict LINER properties, probably associated with large-scale OF + shocks; (vi) at the east border, the kinematics of the ionized gas and the [S II] emission-line maps show an extended ejection of 4 kpc aligned with the PA of the major axis; (vii) three other ejections were found, two of them perpendicular to the extended one. Each ejection starts in one of the knots. These results suggest that the bubble is in the rupture phase.For the complex of giant H II regions it was found that: (i) the Hα, [N II] and [S II] emissionline maps show a compact strong emission area (peaking at ∼810 pc ∼1.7 arcsec, to the east of the second nucleus) and faint extended emission with an elongated shape, and major and minor axes of ∼5.1 kpc (10.8 arcsec; at PA ∼20• ) and ∼2.9 kpc (6.0 arcsec); (ii) inside this complex, the spectra show H II region and transition LINER/H II characteristics; (iii) at the border of this extended H II area the spectra have outflow components and LINER properties.

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“…NGC 4522 (Kenney & Koopmann 1999), UGC 6697 (Nulsen 1982) or several Virgo cluster galaxies (Cayatte et al 1994). However, a larger survey of 67 cluster galaxies showed no evidence of these effects (Mould et al 1995).…”

Section: Introductionmentioning

confidence: 99%

Ram pressure stripping of spiral galaxies in clusters

Abadi

Moore

Bower

1999

Monthly Notices of the Royal Astronomical Society

704

721

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We use three‐dimensional SPH/N‐body simulations to study ram pressure stripping of gas from spiral galaxies orbiting in clusters. We find that the analytic expectation of Gunn & Gott, relating the gravitational restoring force provided by the disc to the ram pressure force, provides a good approximation to the radius at which gas will be stripped from a galaxy. However, at small radii it is also important to consider the potential provided by the bulge component. A spiral galaxy passing through the core of a rich cluster, such as Coma, will have its gaseous disc truncated to ∼4 kpc, thus losing ∼80 per cent of its diffuse gas mass. The time‐scale for this to occur is a fraction of a crossing time ∼107 yr. Galaxies orbiting within poorer clusters, or inclined to the direction of motion through the intracluster medium, will lose significantly less gas. We conclude that ram pressure alone is insufficient to account for the rapid and widespread truncation of star formation observed in cluster galaxies, or the morphological transformation of Sabs to S0s that is necessary to explain the Butcher–Oemler effect.

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Neutral hydrogen profiles of cluster galaxies

Cited by 9 publications

References 0 publications

The [ITAL]I[/ITAL]-Band Tully-Fisher Relation for S[CLC]c[/CLC] Galaxies: 21 Centimeter H [CSC]i[/CSC] Line Data

The [ITAL]I[/ITAL]-Band Tully-Fisher Relation for S[CLC]c[/CLC] Galaxies: 21 Centimeter H [CSC]i[/CSC] Line Data

Infrared mergers and infrared quasi-stellar objects with galactic winds - II. NGC 5514: two extranuclear starbursts with LINER properties and a supergiant bubble in the rupture phase

Ram pressure stripping of spiral galaxies in clusters

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