Predicting dust extinction properties of star-forming galaxies from Hα/UV ratio

Koyama, Yusei; Kodama, Tadayuki; Hayashi, Masao; Shimakawa, Rhythm; Yamamura, I.; Egusa, Fumi; Oi, Nagisa; Tanaka, Ichi; Tadaki, Ken-ichi; Takita, Satoshi; Makiuti, S.

doi:10.1093/mnras/stv1599

Cited by 41 publications

(67 citation statements)

References 76 publications

(78 reference statements)

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“…with Luminous Infrared Galaxies (LIRGs) class luminosity), in order to complement the COLDGASS sample which mostly covers the galaxies on and below the SF main sequence (see Section 2.4 for details). The L IR s are computed by Koyama et al (2015) following Takeuchi et al (2010) using AKARI far-IR photometric bands (Kawada et al 2007); WIDE-S (90 µm) and WIDE-L (140 µm).…”

Section: Sample Selectionmentioning

confidence: 99%

A Universal Correlation between Star Formation Activity and Molecular Gas Properties Across Environments

Koyama¹,

Koyama²,

Yamashita³

et al. 2017

ApJ

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We present the molecular gas mass fraction (f H2 ) and star-formation efficiency (SFE) of local galaxies on the basis of our new CO(J = 1 − 0) observations with the Nobeyama 45m radio telescope, combined with the COLDGASS galaxy catalog, as a function of galaxy environment defined as the local number density of galaxies measured with SDSS DR7 spectroscopic data. Our sample covers a wide range in the stellar mass and SFR, and covers wide environmental range over two orders of magnitude. This allows us to conduct the first, systematic study of environmental dependence of molecular gas properties in galaxies from the lowest-to the highest-density environments in the local universe. We confirm that both f H2 and SFE have strong positive correlations with the SFR offset from the star-forming main sequence (∆MS), and most importantly, we find that these correlations are universal across all environments. Our result demonstrates that star-formation activity within individual galaxies is primarily controlled by their molecular gas content, regardless of their global environment. Therefore, we claim that one always needs to be careful about the ∆MS distribution of the sample when investigating the environmental effects on the H 2 gas content in galaxies.

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Section: Sample Selectionmentioning

confidence: 99%

A Universal Correlation between Star Formation Activity and Molecular Gas Properties Across Environments

Koyama¹,

Koyama²,

Yamashita³

et al. 2017

ApJ

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“…Unfortunately, F Hα /F FUV is sensitive to a large number of variables, which makes interpretation of these trends difficult. In addition to dust extinction (in fact, F Hα /F FUV correlates extremely well with extinction, to the point that it can itself be used as an extinction estimator; Cortese et al 2006;Koyama et al 2015), F Hα /F FUV decreases rapidly with age (e.g. Leroy et al 2012) as the high-mass stars traced by Hα emission die off.…”

Section: Introductionmentioning

confidence: 99%

Star-forming Environments throughout the M101 Group

Watkins¹,

Mihos²,

Harding³

2017

ApJ

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We present a multiwavelength study of star formation within the nearby M101 Group, including new deep Hα imaging of M101 and its two companions. We perform a statistical analysis of the Hα to FUV flux ratios in H II regions located in three different environments: M101's inner disk, M101's outer disk, and M101's lower mass companion galaxy NGC 5474. We find that, once bulk radial trends in extinction are taken into account, both the median and scatter in F Hα /F FUV in H II regions are invariant across all of these environments. Also, using Starburst99 models, we are able to qualitatively reproduce the distributions of F Hα /F FUV throughout these different environments using a standard Kroupa IMF, hence we find no need to invoke truncations in the upper mass end of the IMF to explain the young star-forming regions in the M101 Group even at extremely low surface density. This implies that star formation in low density environments differs from star formation in high density environments only by intensity and not by cloud-to-cloud physics.

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“…However, this ratio may be a function of galaxy properties (e.g., Wuyts et al 2013;Koyama et al 2015). We examine the ratio of continuum-to-nebular attenuation as a function of galaxy properties.…”

Section: Introductionmentioning

confidence: 99%

Stellar Absorption Line Analysis of Local Star-forming Galaxies: The Relation between Stellar Mass, Metallicity, Dust Attenuation, and Star Formation Rate

Zahid

Kudritzki

Conroy

et al. 2017

ApJ

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We analyze the optical continuum of star-forming galaxies in SDSS by fitting stacked spectra with stellar population synthesis models to investigate the relation between stellar mass, stellar metallicity, dust attenuation and star formation rate. We fit models calculated with star formation and chemical evolution histories that are derived empirically from multi-epoch observations of the stellar mass-star formation rate and the stellar mass-gas-phase metallicity relations, respectively. We also fit linear combinations of single burst models with a range of metallicities and ages. Star formation and chemical evolution histories are unconstrained for these models. The stellar mass-stellar metallicity relations obtained from the two methods agree with the relation measured from individual supergiant stars in nearby galaxies. These relations are also consistent with the relation obtained from emission line analysis of gas-phase metallicity after accounting for systematic offsets in the gas-phase-metallicity. We measure dust attenuation of the stellar continuum and show that its dependence on stellar mass and star formation rate is consistent with previously reported results derived from nebular emission lines. However, stellar continuum attenuation is smaller than nebular emission line attenuation. The continuum-to-nebular attenuation ratio depends on stellar mass and is smaller in more massive galaxies. Our consistent analysis of stellar continuum and nebular emission lines paves the way for a comprehensive investigation of stellar metallicities of star-forming and quiescent galaxies.

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Predicting dust extinction properties of star-forming galaxies from Hα/UV ratio

Abstract: Using star-forming galaxies sample in the nearby Universe (0.02 Show more

Cited by 41 publications

References 76 publications

A Universal Correlation between Star Formation Activity and Molecular Gas Properties Across Environments

A Universal Correlation between Star Formation Activity and Molecular Gas Properties Across Environments

Star-forming Environments throughout the M101 Group

Stellar Absorption Line Analysis of Local Star-forming Galaxies: The Relation between Stellar Mass, Metallicity, Dust Attenuation, and Star Formation Rate

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