Matches in SemOpenAlex for { <https://semopenalex.org/work/W4294942218> ?p ?o ?g. }
- W4294942218 endingPage "A53" @default.
- W4294942218 startingPage "A53" @default.
- W4294942218 abstract "The far-infrared (FIR) lines are key tracers of the physical conditions of the interstellar medium (ISM) and are becoming workhorse diagnostics for galaxies throughout the universe. Our goal is to explain the differences and trends observed in the FIR line emission of dwarf galaxies compared to more metal-rich galaxies. We present Herschel PACS spectroscopic observations of the CII157um, OI63 and 145um, OIII88um, NII122 and 205um, and NIII57um fine-structure cooling lines in a sample of 48 low-metallicity star-forming galaxies of the guaranteed time key program Dwarf Galaxy Survey. We correlate PACS line ratios and line-to-LTIR ratios with LTIR, LTIR/LB, metallicity, and FIR color, and interpret the observed trends in terms of ISM conditions and phase filling factors with Cloudy radiative transfer models. We find that the FIR lines together account for up to 3 percent of LTIR and that star-forming regions dominate the overall emission in dwarf galaxies. Compared to metal-rich galaxies, the ratios of OIII/NII122 and NIII/NII122 are high, indicative of hard radiation fields. In the photodissociation region (PDR), the CII/OI63 ratio is slightly higher than in metal-rich galaxies, with a small increase with metallicity, and the OI145/OI63 ratio is generally lower than 0.1, demonstrating that optical depth effects should be small on the scales probed. The OIII/OI63 ratio can be used as an indicator of the ionized gas/PDR filling factor, and is found ~4 times higher in the dwarfs than in metal-rich galaxies. The high CII/LTIR, OI/LTIR, and OIII/LTIR ratios, which decrease with increasing LTIR and LTIR/LB, are interpreted as a combination of moderate FUV fields and low PDR covering factor. Harboring compact phases of low filling factor and a large volume filling factor of diffuse gas, the ISM of low-metallicity dwarf galaxies has a more porous structure than that in metal-rich galaxies." @default.
- W4294942218 created "2022-09-08" @default.
- W4294942218 creator A5002739725 @default.
- W4294942218 creator A5011335986 @default.
- W4294942218 creator A5012560990 @default.
- W4294942218 creator A5017619493 @default.
- W4294942218 creator A5019278701 @default.
- W4294942218 creator A5025202674 @default.
- W4294942218 creator A5025592914 @default.
- W4294942218 creator A5028588360 @default.
- W4294942218 creator A5032719578 @default.
- W4294942218 creator A5035438409 @default.
- W4294942218 creator A5036350828 @default.
- W4294942218 creator A5038703475 @default.
- W4294942218 creator A5041000604 @default.
- W4294942218 creator A5062773650 @default.
- W4294942218 creator A5066444951 @default.
- W4294942218 creator A5069914511 @default.
- W4294942218 creator A5072280155 @default.
- W4294942218 creator A5080091223 @default.
- W4294942218 creator A5086494315 @default.
- W4294942218 creator A5087041838 @default.
- W4294942218 date "2015-06-01" @default.
- W4294942218 modified "2023-10-03" @default.
- W4294942218 title "The<i>Herschel</i>Dwarf Galaxy Survey" @default.
- W4294942218 cites W1518747726 @default.
- W4294942218 cites W1527117010 @default.
- W4294942218 cites W1623182580 @default.
- W4294942218 cites W1836334235 @default.
- W4294942218 cites W1912314976 @default.
- W4294942218 cites W1964844412 @default.
- W4294942218 cites W1964925572 @default.
- W4294942218 cites W1973833544 @default.
- W4294942218 cites W1977521416 @default.
- W4294942218 cites W1981918493 @default.
- W4294942218 cites W1992393936 @default.
- W4294942218 cites W1992570077 @default.
- W4294942218 cites W1993384070 @default.
- W4294942218 cites W1996689021 @default.
- W4294942218 cites W2006433467 @default.
- W4294942218 cites W2010112668 @default.
- W4294942218 cites W2014783219 @default.
- W4294942218 cites W2017609025 @default.
- W4294942218 cites W2031562483 @default.
- W4294942218 cites W2031622689 @default.
- W4294942218 cites W2034608771 @default.
- W4294942218 cites W2038688917 @default.
- W4294942218 cites W2042523227 @default.
- W4294942218 cites W2045276265 @default.
- W4294942218 cites W2047969239 @default.
- W4294942218 cites W2053716388 @default.
- W4294942218 cites W2056076677 @default.
- W4294942218 cites W2058484847 @default.
- W4294942218 cites W2060850421 @default.
- W4294942218 cites W2068061676 @default.
- W4294942218 cites W2069524830 @default.
- W4294942218 cites W2078001023 @default.
- W4294942218 cites W2085713960 @default.
- W4294942218 cites W2088116600 @default.
- W4294942218 cites W2088892484 @default.
- W4294942218 cites W2093906672 @default.
- W4294942218 cites W2095502601 @default.
- W4294942218 cites W2095757078 @default.
- W4294942218 cites W2096147217 @default.
- W4294942218 cites W2096761182 @default.
- W4294942218 cites W2101378182 @default.
- W4294942218 cites W2103901347 @default.
- W4294942218 cites W2105671661 @default.
- W4294942218 cites W2111817932 @default.
- W4294942218 cites W2121855414 @default.
- W4294942218 cites W2123091654 @default.
- W4294942218 cites W2123924478 @default.
- W4294942218 cites W2127979873 @default.
- W4294942218 cites W2131276156 @default.
- W4294942218 cites W2133831267 @default.
- W4294942218 cites W2135536375 @default.
- W4294942218 cites W2149406070 @default.
- W4294942218 cites W2150550921 @default.
- W4294942218 cites W2167262338 @default.
- W4294942218 cites W2197630840 @default.
- W4294942218 cites W2963811913 @default.
- W4294942218 cites W3035852092 @default.
- W4294942218 cites W3042750865 @default.
- W4294942218 cites W3100064752 @default.
- W4294942218 cites W3100106758 @default.
- W4294942218 cites W3100115799 @default.
- W4294942218 cites W3100349731 @default.
- W4294942218 cites W3101150100 @default.
- W4294942218 cites W3101922027 @default.
- W4294942218 cites W3102054457 @default.
- W4294942218 cites W3102554229 @default.
- W4294942218 cites W3102560695 @default.
- W4294942218 cites W3104282610 @default.
- W4294942218 cites W3104494392 @default.
- W4294942218 cites W3104535821 @default.
- W4294942218 cites W3104543873 @default.
- W4294942218 cites W3104752065 @default.
- W4294942218 cites W3104773051 @default.