THE<i>SPITZER</i>LOCAL VOLUME LEGACY: SURVEY DESCRIPTION AND INFRARED PHOTOMETRY

Dale, Daniel A.; Cohen, S.; Johnson, L. Clifton; Schuster, Micah D.; Calzetti, Daniela; Engelbracht, C. W.; Paz, A. Gil de; Kennicutt, Robert C.; Lee, Janice; Begum, Ayesha; Block, M.; Dalcanton, Julianne J.; Funes, J. G.; Gordon, K. D.; Johnson, Benjamin D.; Marble, Andrew R.; Sakai, Shoko; Skillman, Evan D.; Zee, Liese van; Walter, Fabian; Weisz, Daniel R.; Williams, Benjamin F.; Wu, Szu-Ying; Wu, Yanling

doi:10.1088/0004-637x/703/1/517

Cited by 480 publications

(632 citation statements)

References 73 publications

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“…These two galaxies are indeed very similar in many aspects: comparable near-IR magnitudes (K=6.25 and 6.38, respectively, see Jarrett et al 2003) and midinfrared fluxes (see Dale et al 2009) that point towards comparable stellar masses. However, they have different morphologies.…”

Section: Discussionmentioning

confidence: 82%

NGC 55: a disc galaxy with flat abundance gradients

Magrini

Gonçalves

Vajgel

2016

Mon. Not. R. Astron. Soc.

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We present new spectroscopic observations obtained with GMOS@Gemini-S of a sample of 25 H ii regions located in NGC 55, a late-type galaxy in the nearby Sculptor group. We derive physical conditions and chemical composition through the T e -method for 18 H ii regions, and strong-line abundances for 22 H ii regions. We provide abundances of He, O, N, Ne, S, Ar, finding a substantially homogenous composition in the ionised gas of the disc of NGC 55, with no trace of radial gradients. The oxygen abundances, both derived with T e -and strong-line methods, have similar mean values and similarly small dispersions: 12+log(O/H)=8.13±0.18 dex with the former and 12+log(O/H)=8.17±0.13 dex with the latter. The average metallicities and the flat gradients agree with previous studies of smaller samples of H ii regions and there is a qualitative agreement with the blue supergiant radial gradient as well. We investigate the origin of such flat gradients comparing NGC 55 with NGC 300, its companion galaxy, which is also twin of NGC 55 in terms of mass and luminosity. We suggest that the differences in the metal distributions in the two galaxies might be related to the differences in their K-band surface density profile. The flatter profile of NGC 55 probably causes in this galaxy higher infall/outflow rates than in similar galaxies. This likely provokes a strong mixing of gas and a re-distribution of metals.

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Section: Discussionmentioning

confidence: 82%

NGC 55: a disc galaxy with flat abundance gradients

Magrini

Gonçalves

Vajgel

2016

Mon. Not. R. Astron. Soc.

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“…The plotted isophotes (upper right panel of Fig. 17) are based on a Spitzer IRAC1 image from the Local Volume Legacy (Dale et al 2009); the ellipse fits are based on this image, the K-band image of Knapen et al (2003), and an HST NICMOS F160W image (Martini et al 2003).…”

Section: Comparison To Ngc 3368mentioning

confidence: 99%

The formation of stellar nuclear discs in bar-induced gas inflows

Cole

Debattista

Erwin

et al. 2014

Monthly Notices of the Royal Astronomical Society

123

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The role of gas in the mass assembly at the nuclei of galaxies is still subject to some uncertainty. Stellar nuclear discs bridge the gap between the large-scale galaxy and the central massive objects that reside there. Using a high resolution simulation of a galaxy forming out of gas cooling and settling into a disc, we study the formation and properties of nuclear discs. Gas, driven to the centre by a bar, settles into a rotating star-forming nuclear disc (ND). This ND is thinner, younger, kinematically cooler, and more metal-rich than the surrounding bar. The ND is elliptical and orthogonal to the bar. The complex kinematics in the region of the ND are a result of the superposition of older stars streaming along the bar and younger stars circulating within the ND. The signature of the ND is therefore subtle in the kinematics. Instead the ND stands out clearly in metallicity and age maps. We compare the model to the density and kinematics of real galaxies with NDs finding qualitative similarities. Our results suggest that gas dissipation is very important for forming nuclear structures.

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“…The map from the final iteration of FRUITloops was subtracted from the time-stream data and an input test map was then added into that time-stream. The test map for M 51 was the 24 µm map of M 51 from Dale et al (2009) and for M 83 it was the 5 GHz map of M 83 from Neininger et al (1993). These test maps were placed on the same pixel grid as the corresponding AzTEC maps and were convolved to the 18 resolution of those maps.…”

Section: Data Reductionmentioning

confidence: 99%

Continuum observations of M 51 and M 83 at 1.1 mm with AzTEC

Wall

Puerari

Tilanus

et al. 2016

Mon. Not. R. Astron. Soc.

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We observed the spiral galaxies M 51 and M 83 at 20" spatial resolution with the bolometer array AzTEC on the JCMT in the 1.1 mm continuum, recovering the extended emission out to galactocentric radii of more than 12 kpc in both galaxies. The 1.1 mm-continuum fluxes are 5.6±0.7 and 9.9±1.4 Jy, with associated gas masses estimated at 9.4 × 10 9 M and 7.2 × 10 9 M for M 51 and M 83, respectively. In the interarm regions of both galaxies the N(H 2 )/I(CO) (or X-factor) ratios exceed those in the arms by factors of ∼ 1.5-2. In the inner disks of both galaxies, the X-factor is about 1 × 10 20 cm −2 · (K · km · s −1 ) −1 . In the outer parts, the CO-dark molecular gas becomes more important.While the spiral density wave in M 51 appears to influence the interstellar medium and stars in a similar way, the bar potential in M 83 influences the interstellar medium and the stars differently. We confirm the result of Foyle et al. (2010) that the arms merely heighten the star formation rate and the gas surface density in the same proportion. Our maps reveal a threshold gas surface density for an SFR increase by two or more orders of magnitude. In both galaxy centers, the molecular gas depletion time is about 1 Gyr climbing to 10-20 Gyr at radii of 6-8 kpc. This is consistent with an inside-out depletion of the molecular gas in the disks of spiral galaxies.

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THESPITZERLOCAL VOLUME LEGACY: SURVEY DESCRIPTION AND INFRARED PHOTOMETRY

Cited by 480 publications

References 73 publications

NGC 55: a disc galaxy with flat abundance gradients

NGC 55: a disc galaxy with flat abundance gradients

The formation of stellar nuclear discs in bar-induced gas inflows

Continuum observations of M 51 and M 83 at 1.1 mm with AzTEC

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