Erratum: “Little Things” (2012, Aj, 144, 134)

Hunter, Deidre A.; Ficut-Vicas, Dana; Ashley, Trisha; Brinks, E.; Cigan, Phil; Elmegreen, Bruce G.; Heesen, V.; Herrmann, Kimberly A.; Johnson, Megan; Oh, Se–Heon; Rupen, M. P.; Schruba, Andreas; Simpson, Caroline E.; Walter, Fabian; Westpfahl, David J.; Young, Lisa M.

doi:10.3847/1538-3881/153/1/47

Cited by 131 publications

(282 citation statements)

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“…For galaxies drawn from Little THINGS and SHIELD, we infer the stellar mass of the system using the published V -band absolute magnitudes (Hunter et al 2012;Haurberg et al 2015) and assuming a mass-to-light ratio of unity, which is roughly consistent with the expectations for a ∼ 1 Gyr-old simple stellar population following a Salpeter initial mass function (e.g. Maraston 1998).…”

Section: Estimating σGas(r) and M (R)mentioning

confidence: 75%

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Fillingham

Cooper

Pace

et al. 2016

Mon. Not. R. Astron. Soc.

121

123

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Recent studies of galaxies in the local Universe, including those in the Local Group, find that the efficiency of environmental (or satellite) quenching increases dramatically at satellite stellar masses below ∼ 10 8 M . This suggest a physical scale where quenching transitions from a slow "starvation" mode to a rapid "stripping" mode at low masses. We investigate the plausibility of this scenario using observed HI surface density profiles for a sample of 66 nearby galaxies as inputs to analytic calculations of ram-pressure and turbulent viscous stripping. Across a broad range of host properties, we find that stripping becomes increasingly effective at M * 10 8−9 M , reproducing the critical mass scale observed. However, for canonical values of the circumgalactic medium density (n halo < 10 −3.5 cm −3 ), we find that stripping is not fully effective; infalling satellites are, on average, stripped of only 40 − 60% of their cold gas reservoir, which is insufficient to match observations. By including a host halo gas distribution that is clumpy and therefore contains regions of higher density, we are able to reproduce the observed HI gas fractions (and thus the high quenched fraction and short quenching timescale) of Local Group satellites, suggesting that a host halo with clumpy gas may be crucial for quenching low-mass systems in Local Group-like (and more massive) host halos.

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Section: Estimating σGas(r) and M (R)mentioning

confidence: 75%

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Fillingham

Cooper

Pace

et al. 2016

Mon. Not. R. Astron. Soc.

121

123

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“…Young & Lo (1997) also compute timescales for the collapse of the HI gas, considering that it is not rotationally supported, and suggest that magnetized turbulence is a plausible explanation to help support the gas and prevent more rapid collapse. Much of the structure of the gas discussed by these authors is visible in the LITTLE THINGS HI map (Hunter et al 2012) shown in Figure 2. Karachentsev et al (1999) obtained resolved stellar photometry in the V and I bands for Sag DIG.…”

Section: The Sagittarius Dwarf Irregular Galaxymentioning

confidence: 97%

“…Figure 2 shows the processed i band MegaCam image and an enlarged g, i composite image of the central 6' by 6' region. Also overlaid in Figure 2 are HI gas contours from the LITTLE THINGS survey (Hunter et al 2012) and the HST ACS field of view studied by Momany et al (2005) which is discussed later.…”

Section: The Sagittarius Dwarf Irregular Galaxymentioning

confidence: 99%

“…If the very low level distortion on the outermost contours of the Figure 2. The underlying grey scale shows the velocity divided by dispersion from the analysis by Hunter et al (2012). Right: The RGB star distribution is shown in the contours (1.5, 3, 10 σ above the mean background) overlaying the HI distribution in greyscale.…”

Section: On the Content And Structure Of Sag Digmentioning

confidence: 99%

“…arcsec −2 and an absolute magnitude of MV = −11.74. The star formation history was estimated by generating a synthetic CMD, showing Overlaid blue contours show the HI distribution from LITTLE THINGS (Hunter et al 2012), with contours at 10, 50, 100, 250, 500 (Jy/beam)(m/s). The inner 6' by 6' region is shown in the composite g and i band image, with the green dashed box indicating the HST ACS observations analyzed by Momany et al (2005).…”

Section: The Sagittarius Dwarf Irregular Galaxymentioning

confidence: 99%

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Solo dwarfs I: survey introduction and first results for the Sagittarius dwarf irregular galaxy

Higgs¹,

McConnachie²,

Irwin³

et al. 2016

Mon. Not. R. Astron. Soc.

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We introduce the Solitary Local Dwarfs Survey (Solo), a wide field photometric study targeting every isolated dwarf galaxy within 3 Mpc of the Milky Way. Solo is based on (u)gi multi-band imaging from CFHT/MegaCam for northern targets, and Magellan/Megacam for southern targets. All galaxies fainter than M V −18 situated beyond the nominal virial radius of the Milky Way and M31 ( 300 kpc) are included in this volume-limited sample, for a total of 42 targets. In addition to reviewing the survey goals and strategy, we present results for the Sagittarius Dwarf Irregular Galaxy (Sag DIG), one of the most isolated, low mass galaxies, located at the edge of the Local Group. We analyze its resolved stellar populations and their spatial distributions. We provide updated estimates of its central surface brightness and integrated luminosity, and trace its surface brightness profile to a level fainter than 30 mag./sq.arcsec. Sag DIG is well described by a highly elliptical (disk-like) system following a single component Sersic model. However, a low-level distortion is present at the outer edges of the galaxy that, were Sag DIG not so isolated, would likely be attributed to some kind of previous tidal interaction. Further, we find evidence of an extremely low level, extended distribution of stars beyond ∼ 5 arcmins (> 1.5 kpc) that suggests Sag DIG may be embedded in a very low density stellar halo. We compare the stellar and HI structures of Sag DIG, and discuss results for this galaxy in relation to other isolated, dwarf irregular galaxies in the Local Group.

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Chemical abundances in the dwarf galaxy NGC 4163 based on the nebular and auroral emission lines

Zinchenko

Pilyugin

2022

Astron Nachr

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We constructed an oxygen abundance map and N/O ratio map of the unusually low excitation dwarf irregular galaxy NGC 4163 based on publicly available spectroscopy obtained by the MaNGA survey. We detected auroral emission line [O II]𝜆𝜆7320,7330 which allows us to measure chemical abundance by direct T e method. We found that the scatter of the oxygen abundance derived by the strong line method is large. The oxygen abundances 12 + log(O/H) derived by strong line method vary from ∼ 7.3 to ∼ 7.8 with a mean value of ∼ 7.55. The oxygen abundances derived in two apertures of 2 arcseconds by the direct T e method using our measurements of the O + auroral line is about 7.8 dex. The nitrogen-to-oxygen ratio log(N∕O) of about −1.5 is typical value for a low metallicity galaxy, maybe slightly shifted towards higher N/O ratios with respect to the N/O values in the H II regions in nearby galaxies. An unusual negative trend between log(N/O) and oxygen abundance is detected. NGC 4163 is a gas-poor galaxy with a neutral atomic gas mass fraction of around 0.25. The oxygen abundance in the galaxy is only around 0.1 of the oxygen abundance potentially attainable in a galaxy with such a gas mass fraction. The low metallicity coupled with the low gas mass fraction implies that either the metallicity of the interstellar medium of the galaxy was reduced by pristine gas infall in the recent epoch or the evolution of this galaxy was accompanied by strong galactic winds.

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Erratum: “Little Things” (2012, Aj, 144, 134)

Cited by 131 publications

References 1 publication

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Under pressure: quenching star formation in low-mass satellite galaxies via stripping

Solo dwarfs I: survey introduction and first results for the Sagittarius dwarf irregular galaxy

Chemical abundances in the dwarf galaxy NGC 4163 based on the nebular and auroral emission lines

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