A [C ii] 158 Micron Line Map of the rho Ophiuchi Cloud

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

doi:10.1086/187131

Cited by 17 publications

(21 citation statements)

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“…The [C ii ]λ158 μm image of ρ Oph A by Yui et al (1993), with a 15 arcmin beam, shows that C + is present and that [C ii ]λ158 μm shares a similar extent as the cm‐wave continuum. It is remarkable that S1 is not coincident with a [C ii ]λ158 μm peak.…”

Section: Discussionmentioning

confidence: 98%

Centimetre-wave continuum radiation from the ρ Ophiuchi molecular cloud

Casassus

Dickinson

Cleary

et al. 2008

Monthly Notices of the Royal Astronomical Society

128

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The ρ Oph molecular cloud is undergoing intermediate‐mass star formation. Ultraviolet radiation from its hottest young stars heats and dissociates exposed layers, but does not ionize hydrogen. Only faint radiation from the Rayleigh‐Jeans tail of ∼10–100 K dust is expected at wavelengths longwards of ∼3 mm. Yet cosmic background imager (CBI) observations reveal that the ρ Oph W photodissociation region is surprisingly bright at centimetre wavelengths. We searched for interpretations consistent with the Wilkinson Microwave Anisotropy Probe radio spectrum, new Infrared Space Observatory‐Long Wavelength Spectrograph (LWS) parallel mode images and archival Spitzer data. Dust‐related emission mechanisms at 1 cm, as proposed by Draine & Lazarian, are a possibility. But a magnetic enhancement of the grain opacity at 1 cm is inconsistent with the morphology of the dust column maps Nd and the lack of detected polarization. Spinning dust, or electric‐dipole radiation from spinning very small grains (VSGs), comfortably explains the radio spectrum, although not the conspicuous absence from the CBI data of the infrared circumstellar nebulae around the B‐type stars S1 and SR3. Allowing for VSG depletion can marginally reconcile spinning dust with the data. As an alternative interpretation, we consider the continuum from residual charges in ρ Oph W, where most of carbon should be photoionized by the close binary HD 147889 (B2IV, B3IV). Electron densities of ∼102 cm−3, or H‐nucleus densities nH > 106 cm−3, are required to interpret ρ Oph W as the C ii Strömgren sphere of HD 147889. However, the observed steep and positive low‐frequency spectral index would then imply optically thick emission from an hitherto unobserved ensemble of dense clumps or sheets with a filling factor of ∼10−4 and nH∼ 107 cm−3.

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Section: Discussionmentioning

confidence: 98%

Centimetre-wave continuum radiation from the ρ Ophiuchi molecular cloud

Casassus

Dickinson

Cleary

et al. 2008

Monthly Notices of the Royal Astronomical Society

128

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“…The [C ] 158 µm line is one of the major cooling lines in PDRs and has been detected in a wide range of objects as well as in the diffuse Galactic emission (e.g., Crawford et al 1985;Matsuhara et al 1989;Shibai et al 1991Shibai et al , 1996Wright et al 1991;Bock et al 1993;Yui et al 1993;Stacey et al 1991Stacey et al , 1993Nakagawa et al 1998;Makiuti et al 1996Makiuti et al , 2002Li et al 2002). C + ions exist in regions where hydrogen is neutral or ionized because the ionization potential (11.26 eV) is less than that of hydrogen.…”

Section: Introductionmentioning

confidence: 99%

Origin of diffuse C II 158 micron and Si II 35 micron emission in the Carina nebula

Mizutani

Onaka

Shibai

2004

A&A

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“…Therefore, the detection of the [C II] line without any correlation of its spatial distribution with any other molecular emission indicates an external PDR activity around GSS30-IRS1. Yui et al (1993) and Liseau et al (1999) reported three possible candidates of external UV sources: HD 147889 (B2 V), S 1 (B3 V), and SR 3 (B7 V) in the Oph cloud. Their visual extinctions are A v = 4.6, 12.5, and 6.2 mag, respectively (Elias 1978).…”

Section: Atomic Linesmentioning

confidence: 99%

“…The Oph molecular cloud is a good region to study the [C II] emission, which is known as a tracer of the PDRs excited by stellar or interstellar radiation field: (1) the cloud contains three B-type stars, (2) is close to us, and (3) is at a high enough galactic latitude to avoid the emission from the galactic plane (Yui et al 1993). Our PACS observations also show extended [C II] emission around GSS30-IRS1 ( Figure 14).…”

Section: Atomic Linesmentioning

confidence: 99%

“…The [O I] and [C II] lines at FIR wavelengths have been used to measure the strength of the interstellar radiation field (ISRF) in order to predict the presence of photo-dissociation regions (PDRs) as well as understand the heating mechanism associated with YSOs (Yui et al 1993;Nisini et al 2002). Although the enhanced interstellar radiation fields result in the high excitation conditions, the effects of the external radiation fields on the low mass YSOs are poorly understood.…”

Section: Introductionmentioning

confidence: 99%

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“DUST, ICE, AND GAS IN TIME” (DIGIT) HERSCHEL OBSERVATIONS OF GSS30-IRS1 IN OPHIUCHUS

Je¹,

Lee²,

Lee³

et al. 2015

ApJS

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As a part of the "Dust, Ice, and Gas In Time" (DIGIT) key program on Herschel, we observed GSS30-IRS1, a Class I protostar located in Ophiuchus (d = 120 pc), with Herschel /Photodetector Array Camera and Spectrometer (PACS). More than 70 lines were detected within a wavelength range from 50 µm to 200 µm, including CO, H 2 O, OH, and two atomic [O I] lines at 63 and 145 µm. The [C II] line, known as a tracer of externally heated gas by the interstellar radiation field, is also detected at 158 µm. All lines, except [O I] and [C II], are detected only at the central spaxel of 9 ′′ .4 × 9 ′′ .4. The [O I] emissions are extended along a NE-SW orientation, and the [C II] line is detected over all spaxels, indicative of external PDR. The total [C II] intensity aroundGSS30 reveals that the far-ultraviolet radiation field is in the range of 3 to 20 G 0 , where G 0 is in units of the Habing Field, 1.6 × 10 −3 erg cm −2 s −1 . This enhanced external radiation field heats the envelope of GSS30-IRS1, causing the continuum emission to be extended, unlike the molecular emission. The bestfit continuum model of GSS30-IRS1 with the physical structure including flared disk, envelope, and outflow shows that the internal luminosity is 10 L ⊙ , and the region is externally heated by a radiation field enhanced by a factor of 130 compared to the standard local interstellar radiation field.Subject headings: .....

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A [C ii] 158 Micron Line Map of the rho Ophiuchi Cloud

Cited by 17 publications

References 0 publications

Centimetre-wave continuum radiation from the ρ Ophiuchi molecular cloud

Centimetre-wave continuum radiation from the ρ Ophiuchi molecular cloud

Origin of diffuse C II 158 micron and Si II 35 micron emission in the Carina nebula

“DUST, ICE, AND GAS IN TIME” (DIGIT) HERSCHEL OBSERVATIONS OF GSS30-IRS1 IN OPHIUCHUS

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