Spectroscopy of Outlying H [CSC]ii[/CSC] Regions in Spiral Galaxies: Abundances and Radial Gradients

Zee, Liese van; Salzer, John J.; Haynes, Martha P.; O’Donoghue, Aileen A.; Balonek, T. J.

doi:10.1086/300647

Cited by 433 publications

(502 citation statements)

References 55 publications

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“…This suggests that Si dust depletion is not large for the majority of the DLAs/sub-DLAs. We also compared our results with the measurements in the H ii regions of spiral (van Zee et al 1998) and BCD galaxies (Izotov & Thuan 2004). Clearly, measurements in BCD galaxies indicating a constant ratio with metallicity, seem to favour a primary N production in these systems albeit with a large scatter.…”

Section: The [N/α] Bimodalitymentioning

confidence: 76%

“…The N-production duality is revealed when the measurements of N in H ii regions of spiral (van Zee et al 1998), BCD (Izotov & Thuan 1999, 2004, and emissionline galaxies (Nava et al 2006;Izotov et al 2006;Pérez-Montero & Contini 2009) are compared. In low metallicity environments N goes in lockstep with O, so that (N/O) remains approximately constant.…”

Section: The Origin Of Nitrogenmentioning

confidence: 99%

“…Measurements of nitrogen have been performed in different astrophysical sites. In H ii regions of spiral and dwarf-irregular galaxies c 2013 RAS (van Zee et al 1998;van Zee & Haynes 2006), metal-poor emission-line galaxies (Nava et al 2006;Izotov et al 2006;Pérez-Montero & Contini 2009), and H ii regions in blue compact dwarf (BCD) galaxies (Izotov & Thuan 1999, 2004, (N/O) ratios show a primary plateau at low oxygen abundances and a secondary behaviour for [O/H] > −1. Nitrogen abundances were also measured in low-metallicity galactic halo stars (Spite et al 2005) and H ii regions in Large Magellanic Cloud (Bekki & Tsujimoto 2010).…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The ESO UVES advanced data products quasar sample – III. Evidence of bimodality in the [N/α] distribution

Zafar¹,

Centurión²,

Péroux³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Section: The [N/α] Bimodalitymentioning

confidence: 76%

Section: The Origin Of Nitrogenmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The ESO UVES advanced data products quasar sample – III. Evidence of bimodality in the [N/α] distribution

Zafar¹,

Centurión²,

Péroux³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…The secular evolution of disk galaxies produces a regular pattern with the metallicity decreasing inside out, i.e., having a negative gradient with galactocentric distance (Vilchez et al 1988;Edmunds and Greenhow 1995;van Zee et al 1998;Magrini et al 2007;). The timescale for gas mixing in a disk inside an annulus is fairly short, on the order of a rotational period or a few hundred Myr (Sect.…”

Section: Metallicity Inhomogeneities and Inverted Gradientsmentioning

confidence: 99%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

183

130

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Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the formation of disk galaxies. This paper discusses how cosmic gas accretion controls star formation, and summarizes the physical properties expected for the cosmic gas accreted by galaxies. The paper also collects observational evidence for gas accretion sustaining star formation. It reviews evidence inferred from neutral and ionized hydrogen, as well as from stars. A number of properties characterizing large samples of star-forming galaxies can be explained by metal-poor gas accretion, in particular, the relationship among stellar mass, metallicity, and star-formation rate (the so-called fundamental metallicity relationship). They are put forward and analyzed. Theory predicts gas accretion to be particularly important at high redshift, so indications based on distant objects are reviewed, including the global star-formation history of the universe, and the gas around galaxies as inferred from absorption features in the spectra of background sources.

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“…Spectroscopy data (line intensities and EW (Hβ)) for IC 2574 are taken from Croxall et al (2009), data for NGC 628 are partly from Gusev et al (2012) and partly from van Zee et al (1998), data for NGC 6946 are taken from Gusev, Sakhibov & Dodonov (2013), and NGC 925 and NGC 3184 data are taken from van Zee et al (1998). Finally, NGC 3621 data are from Ryder (1995).…”

Section: Spectroscopic Datamentioning

confidence: 99%

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

Khramtsova¹,

Wiebe²,

Lozinskaya³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present an analysis of optical spectroscopy and infrared aperture photometry of more than 100 H ii complexes in nine galaxies. Spectra obtained with the 6-m telescope of SAO RAS are used along with archival data from Spitzer and several ground-based telescopes to infer a strength of polycyclic aromatic hydrocarbon (PAH) emission, age, properties of the UV radiation field, and metallicity of studied H ii complexes. Physical properties (age, radiation field parameters, metallicity) are related to the F 8 /F 24 ratio used as a proxy for the PAH abundance in order to reveal factors that may influence the PAH evolution in H ii complexes. The well-known correlation between the F 8 /F 24 ratio and metallicity is confirmed in the studied complexes. The infrared flux ratio also correlates with the [O iii]λ5007/Hβ ratio which is often considered as an indicator of the radiation field hardness, but this correlation seems to be a mere reflection of a correlation between [O iii]λ5007/Hβ and metallicity. In separate metallicity bins, the F 8 /F 24 ratio is found to correlate with an age of an H ii complex, which is estimated from the equivalent width of Hβ line. The correlation is positive for low metallicity complexes and negative for high metallicity complexes. Analysing various mechanisms of PAH formation and destruction in the context of found correlations, we suggest that PAH abundance is likely altered by the UV radiation within H ii complexes, but this is not necessarily due to their destruction. If PAHs can also form in H ii complexes due to some processes like aromatisation, photodestruction, shattering and sputtering of very small grains, the net F 8 /F 24 ratio is determined by a balance between all these processes that can be different at different metallicities.

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Spectroscopy of Outlying H [CSC]ii[/CSC] Regions in Spiral Galaxies: Abundances and Radial Gradients

Cited by 433 publications

References 55 publications

The ESO UVES advanced data products quasar sample – III. Evidence of bimodality in the [N/α] distribution

The ESO UVES advanced data products quasar sample – III. Evidence of bimodality in the [N/α] distribution

Star formation sustained by gas accretion

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

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