Dust attenuation inz~ 1 galaxies fromHerscheland 3D-HST Hαmeasurements

Puglisi, A.; Rodighiero, G.; Franceschini, A.; Talia, M.; Cimatti, A.; Baronchelli, Ivano; Daddi, E.; Renzini, A.; Schawinski, Kevin; Mancini, C.; Silverman, John D.; Gruppioni, C.; Lutz, D.; Berta, S.; Oliver, S.

doi:10.1051/0004-6361/201526782

Cited by 68 publications

(87 citation statements)

References 72 publications

(96 reference statements)

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“…Comparison between the two sets of contours in Figure 9 reveals that the scatter of ∆(A V,star /A V,gas ) is further reduced after normalization by the global A V,star /A V,gas of each galaxy. This result implies that the global values of A V,star /A V,gas indeed vary between galaxies, which was already suggested by many previous works on either local (e.g., Wild et al 2011; Koyama et al 2015;Zahid et al 2017;Koyama et al 2019) or high-redshift (e.g., Price et al 2014;Puglisi et al 2016) galaxies.…”

Section: The Smooth a Vstar Mapssupporting

confidence: 79%

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A Variant Stellar-to-nebular Dust Attenuation Ratio on Subgalactic and Galactic Scales

Lin

Kong

2020

ApJ

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The state-of-the-art geometry models of stars/dust suggest that dust attenuation toward nebular regions (A V,gas ) is always larger than that of stellar regions (A V,star ). Utilizing the newly released integral field spectroscopic data from the Mapping Nearby Galaxies at Apache Point Observatory survey, we investigate whether and how the A V,star /A V,gas ratio varies from subgalactic to galactic scales. On a subgalactic scale, we report a stronger correlation between A V,star and A V,gas for more active H ii regions. The local A V,star /A V,gas is found to have moderate nonlinear correlations with three tracers of diffuse ionized gas (DIG), as well as indicators of gas-phase metallicity and ionization. The DIG regions tend to have larger A V,star /A V,gas compared to classic H ii regions excited by young OB stars. Metal-poor regions with a higher ionized level suffer much less nebular attenuation and thus have larger A V,star /A V,gas ratios. A low-A V,gas and high-A V,star /A V,gas sequence, which can be resolved into DIG-dominated and metal-poor regions, on the three BPT diagrams is found. Based on these observations, we suggest that besides the geometry of stars/dust, local physical conditions such as metallicity and ionized level also play an important role in determining the A V,star /A V,gas . On a galactic scale, the global A V,star /A V,gas ratio has strong correlations with stellar mass (M * ), moderate correlations with star formation rate (SFR) and metallicity, and weak correlations with inclination and specific SFR. Galaxies with larger M * and higher SFR that are more metal-rich tend to have smaller A V,star /A V,gas ratios. Such correlations form a decreasing trend of A V,star /A V,gas along the star-forming main sequence and mass-metallicity relation. The dust growth process accompanied by galaxy growth might be one plausible explanation for our observations.

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Section: The Smooth a Vstar Mapssupporting

confidence: 79%

“…High-redshift studies also revealed a wide diversity of the stellar-to-nebular reddening ratio, varying from 0.44 (Wuyts et al 2011) to ∼ 1 (Pannella et al 2015;Puglisi et al 2016), as well as the dependences of A V,star /A V,gas on the physical properties of galaxies (Price et al 2014;Reddy et al 2015;Puglisi et al 2016).…”

Section: Introductionmentioning

confidence: 99%

A Variant Stellar-to-nebular Dust Attenuation Ratio on Subgalactic and Galactic Scales

Lin

Kong

2020

ApJ

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“…is the attenuation at 1215Å (Reddy et al 2016a). The nebular color excess is assumed to be the same as the one measured for the stellar continuum (e.g., Erb et al 2006;Puglisi et al 2016).…”

Section: Lyα Linementioning

confidence: 99%

Rest-frame UV properties of luminous strong gravitationally lensed Lyα emitters from the BELLS GALLERY Survey

Marques-Chaves

Pérez-Fournón

Shu

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present deep rest-frame UV spectroscopic observations using the Gran Telescopio Canarias of six gravitationally lensed Lyα emitters (LAEs) at 2.36 < z < 2.82 selected from the BELLS GALLERY survey. By taking the magnifications into account, we show that LAEs can be as luminous as L Lyα 30 × 10 42 erg s −1 and M UV −23 (AB) without invoking an AGN component, in contrast with previous findings. We measure Lyα rest-frame equivalent widths, EW 0 (Lyα), ranging from 16Å to 50Å and Lyα escape fractions, f esc (Lyα), from 10% to 40%. Large EW 0 (Lyα) and f esc (Lyα) are found predominantly in LAEs showing weak low-ionization ISM absorption (EW 0 1Å) and narrow Lyα profiles ( 300 km s −1 FWHM) with their peak close ( 80 km s −1 ) to their systemic redshifts, suggestive of less scatter from low H i column densities that favours the escape of Lyα photons. We infer stellar metallicities of Z/Z 0.2 in almost all LAEs by comparing the P-Cygni profiles of the wind lines N v1240Å and C iv1549Å with those from stellar synthesis models. We also find a trend between M UV and the velocity offset of ISM absorption lines, such as the most luminous LAEs experience stronger outflows. The most luminous LAEs show star formation rates up to 180 M yr −1 , yet they appear relatively blue (β UV −1.8 to −2.0) showing evidence of little dust attenuation (E(B − V) = 0.10 − 0.14). These luminous LAEs may be particular cases of young starburst galaxies that have had no time to form large amounts of dust. If so, they are ideal laboratories to study the early phase of massive star formation, stellar and dust mass growth, and chemical enrichment histories of starburst galaxies at high-z.

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“…In particular, it was argued by e.g. Calzetti et al (2000) that the ratio of the stellar extinction to the nebular extinction for local SFGs is only 0.44 and may vary in the range 0.44 -1.0 for both the local and highz SFGs (Calzetti 1997;Erb et al 2006;Reddy et al 2010;Kashino et al 2013;Price et al 2014;Pannella et al 2015;Valentino et al 2015;Puglisi et al 2016). Low values of the ratio imply that stars and ionised gas are not co-spatial.…”

Section: Comparison Of Modelled and Observed Apparent Fuv And Nuv Magmentioning

confidence: 99%

The efficiency of ionizing photon production and the radiation energy balance in compact star-forming galaxies

Izotov

Гусева

Fricke

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We derive apparent and absolute ultraviolet (UV) magnitudes, and luminosities in the infrared (IR) range of a large sample of low-redshift (0 < z < 1) compact starforming galaxies (CSFGs) selected from the Data Release 12 of the Sloan Digital Sky Survey (SDSS). These data are used to constrain the extinction law in the UV for our galaxies and to compare the absorbed radiation in the UV range with the emission in the IR range. We find that the modelled far-and near-UV apparent magnitudes are in good agreement with the observed Galaxy Evolution Explorer (GALEX) magnitudes. It is found that galaxies with low and high equivalent widths EW(Hβ) of the Hβ emission line require different reddening laws with steeper slopes for galaxies with higher EW(Hβ). This implies an important role of the hard ionising radiation in shaping the dust grain size distribution. The IR emission in the range of 8 -1000 µm is determined using existing data obtained by various infrared space telescopes. We find that the radiation energy absorbed in the UV range is nearly equal to the energy emitted in the IR range leaving very little room for hidden star formation in our galaxies. Using extinction-corrected Hβ luminosities and modelled SEDs in the UV range we derive efficiencies of ionising photon production ξ for the entire sample of CSFGs. It is found that ξ in CSFGs with high EW(Hβ) are among the highest known for low-and high-redshift galaxies. If galaxies with similar properties existed at redshifts z = 5 -10, they could be considered as promising candidates for the reionisation of the Universe.

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Dust attenuation inz~ 1 galaxies fromHerscheland 3D-HST Hαmeasurements

Cited by 68 publications

References 72 publications

A Variant Stellar-to-nebular Dust Attenuation Ratio on Subgalactic and Galactic Scales

A Variant Stellar-to-nebular Dust Attenuation Ratio on Subgalactic and Galactic Scales

Rest-frame UV properties of luminous strong gravitationally lensed Lyα emitters from the BELLS GALLERY Survey

The efficiency of ionizing photon production and the radiation energy balance in compact star-forming galaxies

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