The HIPASS catalogue — III. Optical counterparts and isolated dark galaxies

Doyle, M. T.; Drinkwater, Michael J.; Rohde, David; Pimbblet, Kevin A.; Read, M.; Meyer, M.; Zwaan, M. A.; Ryan-Weber, E. V.; Stevens, J.; Koribalski, B. S.; Webster, R. L.; Staveley‐Smith, L.; Barnes, David G.; Howlett, M.; Kilborn, V. A.; Waugh, M.; Pierce, Michael; Bhathal, Ragbir; Blok, W. J. G. de; Disney, M. J.; Ekers, R. D.; Freeman, K. C.; Garcia, Diego A.; Gibson, Brad K.; Harnett, J.; Henning, P. A.; Jerjen, Helmut; Kesteven, Michael; Knezek, Patricia; Mader, Stacy; Marquarding, M.; Minchin, R. F.; O’Brien, J. C.; Oosterloo, Tom; Price, R. M.; Putman, Mary E.; Ryder, S. D.; Sadler, E. M.; Stewart, I. M.; Stootman, F.; Wright, A. E.

doi:10.1111/j.1365-2966.2005.09159.x

Cited by 180 publications

(94 citation statements)

References 29 publications

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“…Further evidence for this is that virtually no HIPASS H i object is known without an accompanying galaxy or galaxy-component Doyle et al 2005;Meurer et al 2006;Karachentsev et al 2008). This was also demonstrated using disk evolutionary modeling by Taylor & Webster (2005).…”

Section: Discussionmentioning

confidence: 99%

“…KK246 is one of over 4500 H i objects detected in the HIPASS survey (HIPASS J2003-31, Meyer et al 2004) and was identified with the optical counterpart galaxy ESO 461-G036 (Doyle et al 2005). It was subsequently observed using the Very Large Array at 21 cm at higher resolution by Kreckel et al (2011), who found that KK246 is surrounded by a very extended H i region, at least ten times the diameter of the stellar disk.…”

Section: Extended H I Regionmentioning

confidence: 99%

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Nebular Metallicities in Two Isolated Local Void Dwarf Galaxies

Nicholls

Jerjen

Dopita

et al. 2013

ApJ

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Isolated dwarf galaxies, especially those situated in voids, may provide insight into primordial conditions in the universe and the physical processes that govern star formation in undisturbed stellar systems. The metallicity of H ii regions in such galaxies is key to investigating this possibility. From the SIGRID sample of isolated dwarf galaxies, we have identified two exceptionally isolated objects, the Local Void galaxy [KK98]246 (ESO 461-G036) and another somewhat larger dwarf irregular on the edge of the Local Void, MCG-01-41-006 (HIPASS J1609-04). We report our measurements of the nebular metallicities in these objects. The first object has a single low luminosity H ii region, while the second is in a more vigorous star forming phase with several bright H ii regions. We find that the metallicities in both galaxies are typical for galaxies of this size, and do not indicate the presence of any primordial gas, despite (for [KK98]246) the known surrounding large reservoir of neutral hydrogen.

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Section: Discussionmentioning

confidence: 99%

Section: Extended H I Regionmentioning

confidence: 99%

Nebular Metallicities in Two Isolated Local Void Dwarf Galaxies

Nicholls

Jerjen

Dopita

et al. 2013

ApJ

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“…Galaxy positions were found by Doyle et al (2005) by centring a 15-arcmin SuperCOSMOS image on the HIPASS locations. Overlaid on the image were galaxies found using SExtractor and galaxies in the NASA Extragalactic Database (NED) and 6dFGS.…”

Section: Hipass Analysismentioning

confidence: 99%

“…The resulting galaxy match catalogue is called HOPCAT (the HIPASS Optical Catalogue). Full HOPCAT details can be found in Doyle et al (2005). The galaxies in HOPCAT are taken to be the location of the galaxies, however, for optical magnitudes, the ESO-LV catalogue was used (Lauberts & Valentijn 1989).…”

Section: Hipass Analysismentioning

confidence: 99%

Extended Tully–Fisher relations using H i stacking

Meyer

Obreschkow

2015

Mon. Not. R. Astron. Soc.

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We present a new technique for the statistical evaluation of the Tully-Fisher relation (TFR) using spectral line stacking. This technique has the potential to extend TFR observations to lower masses and higher redshifts than possible through a galaxy-bygalaxy analysis. It further avoids the need for individual galaxy inclination measurements.To quantify the properties of stacked H i emission lines, we consider a simplistic model of galactic disks with analytically expressible line profiles. Using this model, we compare the widths of stacked profiles with those of individual galaxies. We then follow the same procedure using more realistic mock galaxies drawn from the S 3 -SAX model (a derivative of the Millennium simulation). Remarkably, when stacking the apparent H i lines of galaxies with similar absolute magnitude and random inclinations, the width of the stack is very similar to the width of the deprojected (= corrected for inclination) and dedispersed (= after removal of velocity dispersion) input lines. Therefore, the ratio between the widths of the stack and the deprojected/dedispersed input lines is approximately constant -about 0.93 -with very little dependence on the gas dispersion, galaxy mass, galaxy morphology, and shape of the rotation curve.Finally, we apply our technique to construct a stacked TFR using HIPASS data which already has a well defined TFR based on individual detections. We obtain a Bband TFR with a slope of −8.5 ± 0.4 and a K-band relation with a slope of −11.7 ± 0.6 for the HIPASS data set which is consistent with the existing results.

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“…We also calculate the stellar mass of this galaxy in order to place these results in context. The R-and I-band magnitudes of 13.33 and 13.34, respectively, were measured by the HIPASS optical counterparts survey (Doyle et al 2005). We use the Bell et al (2003) r − i mass-to-light ratio relation to estimate a stellar mass of 6.2 × 10 8 M , making it the lowest stellar mass object in our sample.…”

Section: Ngc 1427amentioning

confidence: 99%

Tracing Ram-Pressure Stripping With Warm Molecular Hydrogen Emission

Sivanandam

Rieke

2014

ApJ

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We use the Spitzer Infrared Spectrograph to study four infalling cluster galaxies with signatures of ongoing rampressure stripping. H 2 emission is detected in all four, and two show extraplanar H 2 emission. The emission usually has a warm (T ∼ 115-160 K) and a hot (T ∼ 400-600 K) component that is approximately two orders of magnitude less massive than the warm one. The warm component column densities are typically 10 19 to 10 20 cm −2 with masses of 10 6 to 10 8 M . The warm H 2 is anomalously bright compared with normal star-forming galaxies and therefore may be excited by ram-pressure. In the case of CGCG 97-073, the H 2 is offset from the majority of star formation along the direction of the galaxy's motion in the cluster, suggesting that it is forming in the ram-pressure wake of the galaxy. Another galaxy, NGC 4522, exhibits a warm H 2 tail approximately 4 kpc in length. These results support the hypothesis that H 2 within these galaxies is shock-heated from the interaction with the intracluster medium. Stripping of dust is also a common feature of the galaxies. For NGC 4522, where the distribution of dust at 8 μm is well resolved, knots and ripples demonstrate the turbulent nature of the stripping process. The Hα and 24 μm luminosities show that most of the galaxies have star-formation rates comparable to similar mass counterparts in the field. Finally, we suggest a possible evolutionary sequence primarily related to the strength of ram-pressure that a galaxy experiences to explain the varied results observed in our sample.

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The HIPASS catalogue — III. Optical counterparts and isolated dark galaxies

Cited by 180 publications

References 29 publications

Nebular Metallicities in Two Isolated Local Void Dwarf Galaxies

Nebular Metallicities in Two Isolated Local Void Dwarf Galaxies

Extended Tully–Fisher relations using H i stacking

Tracing Ram-Pressure Stripping With Warm Molecular Hydrogen Emission

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