Observation of the Far-Ultraviolet Continuum Background With Spear/Fims

Seon, Kwang‐Il; Edelstein, Jerry; Korpela, E. J.; Witt, A. N.; Kang, Min; Han, Wonyong; Shinn, Jong-Ho; Kim, I.-J.; Park, J.-W.

doi:10.1088/0067-0049/196/2/15

Cited by 61 publications

(92 citation statements)

References 98 publications

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“…6 http://www.stsci.edu/science/starburst99/ where G 0,MW = 9.6 × 10 −4 erg cm −2 s −1 (= 0.6 Habing) is the Galactic FUV field flux (Seon et al 2011), and Σ SFR and Σ SFR,MW are the average SFR surface densities of the model galaxy in question and the MW, respectively. Σ SFR is defined as the total SFR divided by the area of the galaxy disk seen face-on, using the radii listed in Table 1.…”

Section: Cosmological Galaxy Formation Simulationsmentioning

confidence: 99%

SÍGAME Simulations of the , , and Line Emission from Star-forming Galaxies at

Olsen

Greve

Narayanan

et al. 2017

ApJ

103

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Of the almost 40 star forming galaxies at z > ∼ 5 (not counting QSOs) observed in [C II] to date, nearly half are either very faint in [C II], or not detected at all, and fall well below expectations based on locally derived relations between star formation rate and [C II] luminosity. This has raised questions as to how reliable [C II] is as a tracer of star formation activity at these epochs and how factors such as metallicity might affect the [C II] emission. Combining cosmological zoom simulations of galaxies with SÍGAME (SImulator of GAlaxy Millimeter/submillimeter Emission) we have modeled the multi-phased interstellar medium ( We find that the [C II] emission is dominated by the diffuse ionized gas phase and molecular clouds, which on average contribute ∼ 66% and ∼ 27%, respectively. The molecular gas, which constitutes only ∼ 10% of the total gas mass is thus a more efficient emitter of [C II] than the ionized gas, which makes up ∼ 85% of the total gas mass. A principal component analysis shows that the [C II] luminosity correlates with the star formation activity of a galaxy as well as its average metallicity. The low metallicities of our simulations together with their low molecular gas mass fractions can account for their [C II]-faintness, and we suggest these factors may also be responsible for the [C II]-faint normal galaxies observed at these early epochs.

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Section: Cosmological Galaxy Formation Simulationsmentioning

confidence: 99%

SÍGAME Simulations of the , , and Line Emission from Star-forming Galaxies at

Olsen

Greve

Narayanan

et al. 2017

ApJ

103

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“…The background values are consistent with those of Gil de Paz et al (2007), which were estimated by using the data set with less exposure time. The UV background in our Galaxy is mostly caused by the dust scattering of starlight (Witt et al 1997;Seon et al 2011;Hamden et al 2013). Using Eq.…”

Section: Discussionmentioning

confidence: 99%

“…Using Eq. (10) of Seon et al (2011), which were derived from the FUV background observation of our Galaxy, we obtain the FUV background of ∼ 1400 CU at the Galactic latitude of NGC 891. Therefore, the estimated background is consistent with the FUV background observation.…”

Section: Discussionmentioning

confidence: 99%

Diffuse Extraplanar Dust in NGC 891

Seon

Witt

Shinn

et al. 2014

ApJ

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We report the detection of vertically extended far-ultraviolet (FUV) and near-UV emissions in an edge-on spiral galaxy NGC 891, which we interpret as being due to dust-scattered starlight. Three-dimensional radiative transfer models are used to investigate the content of the extraplanar dust that is required to explain the UV emission. The UV halos are well reproduced by a radiative transfer model with two exponential dust disks, one with a scaleheight of ≈ 0.2 − 0.25 kpc and the other with a scaleheight of ≈ 1.2 − 2.0 kpc. The central face-on optical depth of the geometrically thick disk is found to be τ thick B ≈ 0.3 − 0.5 at B-band. The results indicate that the dust mass at |z| > 2 kpc is ≈ 3 − 5% of the total dust mass, which accord well with the recent Herschel sub-millimeter observation. Our results, together with the recent discovery of the UV halos in other edge-on galaxies, suggest the widespread existence of the geometrically thick dust layer above the galactic plane in spirals.

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“…In fact, it is generally known that the FUV and IR intensities correlate with each other in optically thin regions, where the visual extinction A v < 1, corresponding to E(B − V ) < 0.3 for the assumed ratio of R v ∼ 3.1 (Hurwitz 1994;Seon et al 2011a). We would like to test this relationship for the present region of the Aquila Rift and its neighborhood.…”

Section: Discussionmentioning

confidence: 99%

FAR-ULTRAVIOLET OBSERVATION OF THE AQUILA RIFT WITHFIMS/SPEAR

Park

Kang

Seon

et al. 2012

ApJ

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We present the results of far ultraviolet (FUV) observations of the broad region around the Aquila Rift including the Galactic plane. As compared with various wavelength data sets, dust scattering is found to be the major origin of the diffuse FUV continuum in this region. The FUV intensity clearly correlates with the dust extinction level for E(B − V ) < 0.2, while this correlation disappears for E(B − V ) > 0.2 due to heavy dust extinction combined with the effect of nonuniform interstellar radiation fields. The FUV intensity also correlates well with Hα intensity, implying that at least some fraction of the observed Hα emission could be the dust-scattered light of Hα photons originating elsewhere in the Galaxy. Most of the Aquila Rift region is seen devoid of diffuse FUV continuum due to heavy extinction while strong emission is observed in the surrounding regions. Molecular hydrogen fluorescent emission lines are clearly seen in the spectrum of "Aquila-Serpens," while "Aquila-East" does not show any apparent line features. CO emission intensity is also found to be higher in the "Aquila-Serpens" region than in the "Aquila-East" region. In this regard, we note that regions of star formation have been found in "Aquila-Serpens" but not in "Aquila-East."

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Observation of the Far-Ultraviolet Continuum Background With Spear/Fims

Cited by 61 publications

References 98 publications

SÍGAME Simulations of the , , and Line Emission from Star-forming Galaxies at

SÍGAME Simulations of the , , and Line Emission from Star-forming Galaxies at

Diffuse Extraplanar Dust in NGC 891

FAR-ULTRAVIOLET OBSERVATION OF THE AQUILA RIFT WITHFIMS/SPEAR

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