Erratum: "Deficit of Far-Infrared [C II] Line Emission toward the Galactic Center" (ApJ, 455, L35 [1995])

Doi, Yasuo; Yui, Yukari Y.; Okuda, H.; Mochizuki, Kenji; Shibai, Hiroshi; Nishimura, Tetsuo; Low, F. J.

doi:10.1086/309907

Cited by 14 publications

(28 citation statements)

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“…A stellar population deficient in massive mainsequence stars, as a result of either an aging starburst or an initial mass function with a low upper mass cutoff, could give rise to a soft UV field, and consequently a small F ½C ii / F FIR ratio (Spaans et al 1994;Nakagawa et al 1995;Malhotra et al 2001). S. Satyapal et al (in preparation) model the decrease in L ½C ii /L FIR as a function of starburst age.…”

Section: Soft Uv Radiation Field: Aging Starburstsmentioning

confidence: 99%

The [Cii] 158 Micron Line Deficit in Ultraluminous Infrared Galaxies Revisited

Luhman

Satyapal

Fischer

et al. 2003

ApJ

215

350

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We present a study of the [C ii] 157.74 lm fine-structure line in a sample of 15 ultraluminous infrared (IR) galaxies (IR luminosity L IR k10 12 L ; ULIRGs) using the Long Wavelength Spectrometer (LWS) on the Infrared Space Observatory (ISO). We confirm the observed order of magnitude deficit (compared to normal and starburst galaxies) in the strength of the [C ii] line relative to the far-infrared (FIR) dust continuum emission found in our initial report, but here with a sample that is twice as large. This result suggests that the deficit is a general phenomenon affecting 4 out of 5 ULIRGs. We present an analysis using observations of generally acknowledged photodissociation region (PDR) tracers ([C ii], [O i] 63 and 145 lm, and FIR continuum emission), which suggests that a high ultraviolet flux G 0 incident on a moderate density n PDR could explain the deficit. However, comparisons with other ULIRG observations, including CO (1-0), [C i] (1-0), and 6.2 lm polycyclic aromatic hydrocarbon (PAH) emission, suggest that high G 0 =n PDRs alone cannot produce a self-consistent solution that is compatible with all of the observations. We propose that non-PDR contributions to the FIR continuum can explain the apparent [C ii] deficiency. Here, unusually high G 0 and/ or n physical conditions in ULIRGs as compared to those in normal and starburst galaxies are not required to explain the [C ii] deficit. Dust-bounded photoionization regions, which generate much of the FIR emission but do not contribute significant [C ii] emission, offer one possible physical origin for this additional non-PDR component. Such environments may also contribute to the observed suppression of FIR fine-structure emission from ionized gas and PAHs, as well as the warmer FIR colors found in ULIRGs. The implications for observations at higher redshifts are also revisited.

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Section: Soft Uv Radiation Field: Aging Starburstsmentioning

confidence: 99%

The [Cii] 158 Micron Line Deficit in Ultraluminous Infrared Galaxies Revisited

Luhman

Satyapal

Fischer

et al. 2003

ApJ

215

350

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“…[Cii] -3.82 -4.23 8.0 ± 0.7 -2.92 -4.67 18.1 ± 0.5 -2.04 -5.13 17.3 ± 1.4 -1.14 -5.58 13.0 ± 1.4 -3.37 -3.35 6.6 ± 0.4 -2.47 -3.78 16.8 ± 1.1 -1.59 -4.25 28.1 ± 0.5 -0.69 -4.68 16.2 ± 0.8 -2.92 -2.45 5.4 ± 0.2 -2.02 -2.89 11.8 ± 1.4 -1.13 -3.35 18.4 ± 0.6 -0.23 -3.79 12.2 ± 0.5 -2.47 -1.56 4.5 ± 0.4 -1.57 -2.00 7.2 ± 0.6 -0.68 -2.46 11.6 ± 0.8 0.22 -2.90 8.8 ± 0.7 -2.02 -0.66 4.6 ± 0.4 -1.12 -1.10 5.9 ± 0.7 -0.23 -1.57 13.7 ± 1.2 0.67 -2.01 8.5 ± 0.9 -1.57 0.22 6.2 ± 0.6 -0.66 -0.21 7.6 ± 0.7 0.22 -0.68 14.5 ± 0.7 1.12 -1.11 9.2 ± 0.8 -1.11 1.12 6.0 ± 0.7 -0.22 0.68 11.9 ± 0.6 0.67 0.22 14.9 ± 0.7 1.57 -0.22 9.9 ± 0. (Nakagawa et al 1995). Regarding other external galaxies, few data of sufficient sensitivity are available.…”

Section: The [C Ii]/fir Ratiomentioning

confidence: 99%

[CII] emission and star formation in the spiral arms of M 31

Rodríguez-Fernández

Braine²,

Brouillet³

et al. 2006

A&A

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Context. The [Cii] 158 µm line is the most important coolant of the interstellar medium in galaxies but substantial variations are seen from object to object. The main source of the emission at a galactic scale is still poorly understood and candidates range from photodissociation regions (PDRs) to the cold neutral or diffuse warm ionized medium. Previous studies of the [Cii] emission in galaxies have a resolution of several kpc or more so the observed emission is an average of different ISM components. Aims. The aim of this work is to study, for the first time, the [Cii] emission at the scale of a spiral arm. We want to investigate the origin of this line and its use as a tracer of star formation. Methods. We present [Cii] and [Oi] observations of a segment of a spiral arm of M 31 using the Infrared Space Observatory. The [Cii] emission is compared with tracers of neutral gas (CO, Hi) and star formation (Hα, Spitzer 24 µm). Results. The similarity of the [Cii] emission with the Hα and 24 µm images is striking when smoothed to the same resolution, whereas the correlation with the neutral gas is much weaker. The [Cii] cooling rate per H atom increases dramatically from ∼2.7 × 10 −26 erg s −1 atom −1 in the border of the map to ∼1.4 × 10 −25 erg s −1 atom −1 in the regions of star formation. The [Cii]/FIR 42−122 ratio is almost constant at 2%, a factor 3 higher than typically quoted. However, we do not believe that M 31 is unusual. Rather, the wholegalaxy fluxes used for the comparisons include the central regions where the [Cii]/FIR ratio is known to be lower and the resolved observations neither isolate a spiral arm nor include data as far out in the galactic disk as the observations presented here. A fit to published PDR models yields a plausible average solution of G 0 ∼ 100 and n ∼ 3000 for the PDR emission in the regions of star formation in the arm of M 31.

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“…These results can be combined with CO data to provide insight into conditions A&A 523, A45 (2010) References. 1) Burton & Liszt (1983); 2) Jaffe et al (1996); 3) Nakagawa et al (1995); 4) Bania (1986); 5) Bitran et al (1997); 6) Fukui et al (2006); 7) Oka et al (1996); 8) Sawada et al (2001); 9) Oka et al (2007); 10) Bally et al (1987); 11) Dahmen et al (1997); 12) Morris et al (1983); 13) Martín-Pintado et al 199714) Boyce & Cohen (1994); 15) Zylka et al (1992); 16) Fukui et al (1977); 17) Jackson et al (1996); 18) Lee (1996). Notes.…”

Section: Introductionunclassified

A survey of the Galactic center region in HCO⁺, H¹³CO⁺, and SiO

Riquelme

Bronfman

Mauersberger

et al. 2010

A&A

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Aims. A large-scale survey of the Galactic center region in the 3 mm rotational transitions of SiO, HCO + and H 13 CO + (beamsize ∼3. 6) was conducted to provide an estimate of cloud conditions, heating mechanisms, chemistry, and other properties. Methods. Using the NANTEN 4 m telescope from Nagoya University, a region between −5. • 75 < l < 5.• 6 and −0.• 68 < b < 1.• 3 was mapped in the J = 1 → 0 lines of HCO + and H 13 CO + and in the J = 2 → 1 line of SiO with a spacing of 3. 75 (HCO + ) and 1. 875 (SiO and H 13 CO + ). Results. Velocity channel maps, longitude-velocity maps, and latitude-velocity maps are presented. We identify 51 molecular clouds; 33 of them belong to the Galactic center and 18 to disk gas. We derive an average of the luminosity ratio of SiO(J = 2 → 1)/CO(J = 1 → 0) in clouds belonging to the Galactic center of 4.9 × 10 −3 and for disk clouds of 3.4 × 10 −3 . The luminosity ratio of HCO + (J = 1 → 0)/CO(J = 1 → 0) in the Galactic center is 3.5 × 10 −2 , and for disk clouds it is 1.5 × 10 −2 . We can distinguish clearly between regions where the SiO or HCO + dominate.

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Erratum: "Deficit of Far-Infrared [C II] Line Emission toward the Galactic Center" (ApJ, 455, L35 [1995])

Cited by 14 publications

References 0 publications

The [Cii] 158 Micron Line Deficit in Ultraluminous Infrared Galaxies Revisited

The [Cii] 158 Micron Line Deficit in Ultraluminous Infrared Galaxies Revisited

[CII] emission and star formation in the spiral arms of M 31

A survey of the Galactic center region in HCO⁺, H¹³CO⁺, and SiO

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Erratum: "Deficit of Far-Infrared [C II] Line Emission toward the Galactic Center" (ApJ, 455, L35 [1995])

Cited by 14 publications

References 0 publications

The [Cii] 158 Micron Line Deficit in Ultraluminous Infrared Galaxies Revisited

The [Cii] 158 Micron Line Deficit in Ultraluminous Infrared Galaxies Revisited

[CII] emission and star formation in the spiral arms of M 31

A survey of the Galactic center region in HCO+, H13CO+, and SiO

Contact Info

Product

Resources

About

A survey of the Galactic center region in HCO⁺, H¹³CO⁺, and SiO