The neutral hydrogen environments of the nearby galaxies WLM, NGC 1313 and Sextans A

Barnes, David G.; Blok, W. J. G. de

doi:10.1111/j.1365-2966.2004.07790.x

Cited by 20 publications

(25 citation statements)

References 26 publications

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“…We calculate a total H i mass of 1.1 × 10 8 M . This is 1.6× more than the mass of 7.0 × 10 7 M reported by Kepley et al (2007), 1.9× the mass of 5.9 × 10 7 M detected by Huchtmeier et al (1981), three times higher than the mass of Jackson et al (2004), and 60% higher than Barnes & De Blok's (2004) mass-all corrected to our choice of distance for WLM. However, because of the structure of our map, our total mass is uncertain.…”

Section: Wlmmentioning

confidence: 70%

“…Two other dwarf galaxies-WLM and NGC 2366-have also been reported by Huchtmeier et al (1981) to have extended H i with diameters that are 3-3.6 times their optical Holmberg diameters, and this gas has gone undetected by others (Hunter et al 2001;Barnes & De Blok 2004;Jackson et al 2004). Both are fairly typical nearby, gas-rich dIm galaxies with modest absolute magnitudes.…”

Section: Introductionmentioning

confidence: 91%

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Mapping the Extended H I Distribution of Three Dwarf Galaxies

Hunter

Zahedy

Bowsher

et al. 2011

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We present large field H i-line emission maps obtained with the single-dish Green Bank Telescope centered on the dwarf irregular galaxies Sextans A, NGC 2366, and WLM. We do not detect the extended skirts of emission associated with the galaxies that were reported from Effelsberg observations. The ratio of H i at 10 19 atoms cmto optical extents of these galaxies is instead 2-3, which is normal for this type of galaxy. There is no evidence for a truncation in the H i distribution 10 19 atoms cm −2 .

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Section: Wlmmentioning

confidence: 70%

Section: Introductionmentioning

confidence: 91%

Mapping the Extended H I Distribution of Three Dwarf Galaxies

Hunter

Zahedy

Bowsher

et al. 2011

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“…We, fortunately, resolve out the Magellanic Stream. Given the line profiles shown in Figure 7 and in Barnes & de Blok (2004), it is clear that WLM's line profile is not symmetric and that the Huchtmeier et al (1981) integrated H i mass and maps for this galaxy are not accurate.…”

Section: H I Mass and Extentmentioning

confidence: 92%

“…The emission at the edge of the plot is result of the mosaicking process (we have better sensitivity at the center of the image due to the overlap of pointings than at the edges) and is not real emission. Barnes & de Blok (2004) find no companion H i clouds near WLM with a detection limit of 1:9 ; 10 5 M for an object with a velocity dispersion of 10 km s À1 . The beam is given in the lower left-hand corner of the image.…”

Section: H I Mass and Extentmentioning

confidence: 94%

A High-Resolution Study of the HiContent of Local Group Dwarf Irregular Galaxy WLM

Kepley

Wilcots

Hunter

et al. 2007

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Dwarf irregular galaxies are unique laboratories for studying the interaction between stars and the interstellar medium in low-mass environments. We present the highest spatial resolution observations to date of the neutral hydrogen content of the Local Group dwarf irregular galaxy WLM. We find that WLM's neutral hydrogen distribution is typical for a galaxy of its type and size and derive an H i mass of (6:3 AE 0:3) ; 10 7 M . In addition, we derive an H i extent for WLM of $30 0 , which is much less than the 45 0 extent found by Huchtmeier and coworkers. We show that the broken ring of high column density neutral hydrogen surrounding the center of WLM is likely the result of star formation propagating out from the center of the galaxy. The young stars and H emission in this galaxy are mostly correlated with the high column density neutral hydrogen. The gap in the central ring is the result of star formation in that region using up, blowing out, or ionizing all of the neutral hydrogen. Like many late-type galaxies, WLM's velocity field is asymmetric with the approaching (northern) side appearing to be warped and a steeper velocity gradient for the approaching side than for the receding side in the inner region of the galaxy. We derive a dynamical mass for WLM of 2:16 ; 10 9 M .

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“…WLM has a stellar mass of M * = 4.3 × 10 7 M (Jack son et al 2007;McConnachie 2012), and an H i mass of M HI = (6.3 ± 0.3) × 10 7 M (Kepley et al 2007; see also Huchtmeier et al 1981;Barnes & de Blok 2004;Jackson et al 2004). Leaman et al (2012) estimate WLM's darkmatter halo mass M h based on its stellar rotation curve and line-of-sight dispersion velocity.…”

Section: Introductionmentioning

confidence: 99%

Tentative detection of the circumgalactic medium of the isolated low-mass dwarf galaxy WLM

Zheng

Putman

Emerick

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We report a tentative detection of the circumgalactic medium (CGM) of WLM, an isolated, low-mass (logM * /M ≈ 7.6), dwarf irregular galaxy in the Local Group (LG). We analyze an HST/COS archival spectrum of a quasar sightline (PHL2525), which is 45 kpc (0.5 virial radius) from WLM and close to the Magellanic Stream (MS). Along this sightline, two ion absorbers are detected in Si II, Si III, Si IV, C II, and C IV at velocities of ∼-220 km s −1 (Component v-220) and ∼-150 km s −1 (Component v-150). To identify their origins, we study the position-velocity alignment of the components with WLM and the nearby MS. Near the Magellanic longitude of PHL2525, the MSrelated neutral and ionized gas moves at −190 km s −1 , suggesting an MS origin for Component v-220, but not for Component v-150. Because PHL2525 passes near WLM and Component v-150 is close to WLM's systemic velocity (∼-132 km s −1 ), it is likely that Component v-150 arises from the galaxy's CGM. This results in a total Si mass in WLM's CGM of M CGM Si ∼ (0.2 − 1.0) × 10 5 M using assumption from other COS dwarf studies. Comparing M CGM Si to the total Si mass synthesized in WLM over its lifetime (∼1.3×10 5 M ), we find ∼3% is locked in stars, ∼6% in the ISM, ∼15%-77% in the CGM, and the rest (∼14%-76%) is likely lost beyond the virial radius. Our finding resonates with other COS dwarf galaxy studies and theoretical predictions that low-mass galaxies can easily lose metals into their CGM due to stellar feedback and shallow gravitational potential.

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The neutral hydrogen environments of the nearby galaxies WLM, NGC 1313 and Sextans A

Cited by 20 publications

References 26 publications

Mapping the Extended H I Distribution of Three Dwarf Galaxies

Mapping the Extended H I Distribution of Three Dwarf Galaxies

A High-Resolution Study of the HiContent of Local Group Dwarf Irregular Galaxy WLM

Tentative detection of the circumgalactic medium of the isolated low-mass dwarf galaxy WLM

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