Spectroscopic Observation and Analysis of H ii Regions in M33 with MMT: Temperatures and Oxygen Abundances

Lin, Zhoubin; Hu, Ning; Kong, Xu; Gao, Yongheng; Zou, Hu; Wang, Enci; Cheng, F. H.; Fang, Guanwen; Lin, Lin; Wang, Jing

doi:10.3847/1538-4357/aa6f14

Cited by 37 publications

(45 citation statements)

References 66 publications

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“…Properties The electron temperature (T e ) method is generally deemed as the most reliable approach for deriving metallicity, which is based on the ratios of faint auroralto-nebular emission lines (Lin et al 2017 Pettini & Pagel 2004), are calibrated by empirical fitting to the electronic temperature (T e ) method with strong-line ratios for H ii regions and galaxies. However, there is a large discrepancy between the metallicities derived by different calibrators (Kehrig et al 2013;Morisset et al 2016).…”

Section: Determinations Of Metallicity and Other Physicalmentioning

confidence: 99%

What Determines the Local Metallicity of Galaxies: Global Stellar Mass, Local Stellar Mass Surface Density, or Star Formation Rate?

Gao

Wang

Kong

et al. 2018

ApJ

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The metallicity and its relationship with other galactic properties is a fundamental probe of the evolution of galaxies. In this work, we select about 750,000 star-forming spatial pixels from 1122 blue galaxies in the MaNGA survey to investigate the global stellar mass -local stellar mass surface density -gas-phase metallicity (M * -Σ * -Z ) relation. At a fixed M * , the metallicity increases steeply with increasing Σ * . Similarly, at a fixed Σ * , the metallicity increases strongly with increasing M * at low mass end, while this trend becomes less obvious at high mass end. We find the metallicity to be more strongly correlated to Σ * than to M * . Furthermore, we construct a tight (0.07 dex scatter) M * -Σ * -Z relation, which reduces the scatter in the Σ * -Z relation by about 30% for galaxies with 7.8 < log(M * /M ) < 11.0, while the reduction of scatter is much weaker for high-mass galaxies. This result suggests that, especially for low-mass galaxies, the M * -Σ * -Z relation is largely more fundamental than the M * -Z and Σ * -Z relations, meaning that both M * and Σ * play important roles in shaping the local metallicity. We also find that the local metallicity is probably independent on the local star formation rate surface density at a fixed M * and Σ * . Our results are consistent with the scenario that the local metallicities in galaxies are shaped by the combination of the local stars formed in the history and the metal loss caused by galactic winds.

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Section: Determinations Of Metallicity and Other Physicalmentioning

confidence: 99%

What Determines the Local Metallicity of Galaxies: Global Stellar Mass, Local Stellar Mass Surface Density, or Star Formation Rate?

Gao

Wang

Kong

et al. 2018

ApJ

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“…Despite that limitation, it represents a good subset of M33 ionized regions for our analysis. Figure 11 compares the Hα surface brightnesses for the Lin et al (2017) fiber positions with the background distribution computed from a set of shifted regions. Five different shifts of 1 arcmin were used to determine the background distribution.…”

Section: Identification Of H II Regionsmentioning

confidence: 99%

“…Lin et al (2017) H II catalog Catalog positions Shifted background positions Hα surface brightness [erg cm -2 s -1 arcsec -2 ]Figure 11. A comparison of the Hα surface brightnesses for theLin et al (2017) H II region sample (red) with the background Hα surface brightness distribution (blue). The surface brightnesses are averaged from our Hα image over the region in the catalog.…”

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confidence: 99%

A New, Deep JVLA Radio Survey of M33

White

Long

Becker

et al. 2019

ApJS

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We have performed new 1.4 GHz and 5 GHz observations of the Local Group galaxy M33 with the Jansky Very Large Array. Our survey has a limiting sensitivity of 20 µJy (4σ) and a resolution of 5.9 (FWHM), corresponding to a spatial resolution of 24 pc at 817 kpc. Using a new multi-resolution algorithm, we have created a catalog of 2875 sources, including 675 with well-determined spectral indices. We detect sources at the position of 319 of the X-ray sources in the Tüllmann et al. (2011) Chandra survey of M33, the majority of which are likely to be background galaxies. The radio source coincident with M33 X-8, the nuclear source, appears to be extended. Along with numerous H II regions or portions of H II region complexes, we detect 155 of the 217 optical supernova remnants included in the lists of Long et al. (2010) and Lee & Lee (2014), making this by far the largest sample of remnants at known distances with multiwavelength coverage. The remnants show a large dispersion in the ratio of radio to X-ray luminosity at a given diameter, a result that challenges the current generation of models for synchrotron radiation evolution in supernova remnants.

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“…and can be used as an indicator of gas-phase metallicity (e.g., Kewley & Ellison 2008;Marino et al 2013;Lin et al 2017). To characterize the location of spaxels, we use the deprojected distances to the galactic centers normalized by the effective radius r e (r/r e ).…”

Section: Dependence On Local Physical Propertiesmentioning

confidence: 99%

Dust Attenuation Curve for Local Subgalactic Star-forming Regions

Teklu

Lin

Kong

et al. 2020

ApJ

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We compile a sample of about 157,000 spaxels from the Mapping Nearby Galaxies at the Apache Point Observatory (MaNGA) survey to derive the average dust attenuation curve for subgalactic star-forming regions of local star-forming galaxies (SFGs) in the optical wavelength, following the method of Calzetti et al. We obtain a D n (4000)-independent average attenuation curve for spaxels with 1.1 ≤ D n (4000) < 1.3, which is similar to the one derived from either local starbursts or normal SFGs. We examine whether and how the shape of the average attenuation curve changes with several local and global physical properties. For spaxels with 1.2 ≤ D n (4000) < 1.3, we find no dependence on either local or global physical properties for the shape of the average attenuation curve. However, for spaxels with younger stellar population (1.1 ≤ D n (4000) < 1.2), shallower average attenuation curves are found for star-forming regions with smaller stellar mass surface density, smaller star formation rate surface density, or those residing in the outer region of galaxies. These results emphasize the risk of using one single attenuation curve to correct the dust reddening for all type of star-forming regions, especially for those with fairly young stellar population.

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Spectroscopic Observation and Analysis of H ii Regions in M33 with MMT: Temperatures and Oxygen Abundances

Cited by 37 publications

References 66 publications

What Determines the Local Metallicity of Galaxies: Global Stellar Mass, Local Stellar Mass Surface Density, or Star Formation Rate?

What Determines the Local Metallicity of Galaxies: Global Stellar Mass, Local Stellar Mass Surface Density, or Star Formation Rate?

A New, Deep JVLA Radio Survey of M33

Dust Attenuation Curve for Local Subgalactic Star-forming Regions

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