H I mapping of galaxies in the Hercules cluster

Salpeter, E. E.; Dickey, John M.

doi:10.1086/163171

Cited by 6 publications

(3 citation statements)

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“…γ + ≈= −0.013 mag kpc −1 in B−V (mean colour 0.22 mag); V−I colour gradient of 0.016 mag kpc −1 , mean colour 0.56 mag. H  detections of IC 1882 were also reported by Bieging & Biermann (1983), Bird et al (1993), Bothun et al (1981Bothun et al ( , 1985, Mirabel & Wilson (1984), Salpeter & Dickey (1985) and Schommer et al (1981). The average profile parameters from these references are V HI = 10 239 ± 62 km s −1 , W 20 = 592 ± 48 km s −1 and I HI = 3.6 ± 0.8 Jy km s −1 .…”

Section: Discussionsupporting

confidence: 59%

A study of H I-selected galaxies in the Hercules cluster

Iglésias-Páramo¹,

Driel²,

Duc³

et al. 2003

A&A

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Abstract. The present study focuses on a sample of 22 galaxies detected in the blind VLA H  survey of the Hercules cluster by Dickey (1997), 18 of which were selected on an H  line width smaller than 270 km s −1 and 4 others with only tentative optical counterparts in the Palomar Sky Survey. Sensitive single-dish H  line spectra were obtained for 20 of them, and for one the VLA detection was not confirmed. Optical surface photometry has been carried out for 10 objects, for 8 of which optical spectroscopy was obtained as well. Based on various criteria, we classify two sample galaxies (ce-143 and ne-204) as genuine dwarfs whereas the remaining sample objects are found to be intrinsically luminous galaxies. For those objects investigated in optical wavelengths we determine properties similar to those of actively star-forming galaxies, and find that approximately one half of them has properties intermediate between those of dwarf galaxies and low-luminosity disc galaxies. No optical redshifts could be determined for two of the galaxies (sw-103 and sw-194) and their physical association with the H  clouds detected at their positions therefore remains uncertain. A particularly interesting object in our sample is the Tidal Dwarf Galaxy candidate ce-061 in the galaxy merger IC 1182.

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Section: Discussionsupporting

confidence: 59%

A study of H I-selected galaxies in the Hercules cluster

Iglésias-Páramo¹,

Driel²,

Duc³

et al. 2003

A&A

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“…Bothun et al (1981) found that it has total colors that correspond to an early type object, except U − B, that is too blue for an E or S0 galaxy. They also reported (see also Salpeter & Dickey 1985) that IC 1182 has an unusually large HI mass fraction for an early type galaxy. Their data reveal the contribution to the observed HI profile of a close companion, most likely interacting with IC 1182, but even after taking into account that contamination, IC 1182 is still very HI-rich, with log (M HI /L B ) ≈ −0.5.…”

Section: Introductionmentioning

confidence: 79%

The peculiar galaxy IC 1182: An ongoing merger?

Moles¹,

Bettoni

Fasano

et al. 2004

A&A

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Abstract. High resolution broad and narrow band images and long slit spectroscopy of the peculiar galaxy IC 1182 are presented. The analysis of the broad band images reveals a distorted morphology with a large, heavily obscured disk-like structure and several knots in the central region. Galactic material, some of it in the form of two slender tails, is detected well beyond the main body of the galaxy. The second, fainter tail and several knots are reported here for the first time. The galaxy has color indices of an early type object except U − B, which is significantly bluer than what is typical for this kind of galaxy. The narrow band images centered on different emission lines show that the galaxy is a very powerful emitter. Most of the knots detected in the central region and in the prominent tail emerging eastward from the galaxy are very luminous in Hα, and have typical sizes about 1 kpc (FWHM). The emission in the main lines extends all over the galaxy, with plumes and arc-like structures seen in Hα at large distances from the center. The observed, uncorrected Hα flux corresponds to a total luminosity of 3.51 × 10 41 erg s −1 , about 3 times that of the starburst galaxy Arp 220. We have found that the internal extinction deduced from the observed Balmer decrement is high all along the slit, with E B−V ≈ 1, so the corrected SFR could amount to 90 M per year. On this basis IC 1182 is found to be a very powerful starburst galaxy. Surprisingly, the source is not in the IRAS Point Source Catalogue. The emission knots detected in the central region of the galaxy have line ratios that place them close to the border of the region occupied by active nuclei in the diagnostic diagrams. Using the best determined diagnostic ratio, [O III]/Hβ vs. [N II]/Hα, they can still be classified as extreme HII-like regions. We notice that the same kind of line ratios are also measured at different places in the galaxy, adding to the idea that the nuclear line ratios can be explained in terms of stellar photoionization. The metallicity we have measured for the ionized gas in the two brightest central knots is low, 0.1 Z and 0.06 Z respectively, and their measured helium abundance is also lower than solar. In the main body of the galaxy, besides the reported knots, the distribution of the ionized gas resembles that of an inclined disk about 12 kpc in size. The spectroscopic data show however a complex rotation pattern. We interpret them as corresponding to two identifiable disk galaxies with observed rotation amplitudes of 200 km s −1 and 100 km s −1 respectively. The stellar absorption lines detected in the bigger system do not show any clear rotation pattern. The data presented here indicate that IC 1182 is a high luminosity starburst system. Its global properties and peculiarities can be understood as corresponding to two systems that can still be recognized, in the process of merging, with two tidal tails emerging from the central region of the galaxy. In the main tail there are several candidates forming tidal dwarf galaxies....

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“…The solid data points are taken from Briggs (1990). They all come from pointed observations towards different clusters, but including different proportions of foreground and background objects: solid squares, Leo group (Schneider et al 1989); circles, Virgo (Hoffman et al 1989); triangle, Hercules (Salpeter & Dickey 1985). Unfortunately these surveys are all highly biased.…”

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confidence: 99%

Cosmology using the Parkes HI Multibeam Southern Sky Survey

Thomas

1997

Publ. – Astron. Soc. Aust

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I discuss the implications of the Parkes Multibeam Southern Sky HI Survey for cosmology. It will determine the local mass function of HI clouds, detecting several hundred per decade of mass. Each of these will come with a redshift and, for the more massive clouds, an estimate of the velocity width. This will provide an ideal database for peculiar motion studies and for measurements of biasing of galaxies relative to the underlying matter distribution.

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H I mapping of galaxies in the Hercules cluster

Cited by 6 publications

References 0 publications

A study of H I-selected galaxies in the Hercules cluster

A study of H I-selected galaxies in the Hercules cluster

The peculiar galaxy IC 1182: An ongoing merger?

Cosmology using the Parkes HI Multibeam Southern Sky Survey

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