On the distance to the Ophiuchus star‐forming region

Mamajek, Eric E.

doi:10.1002/asna.200710827

Cited by 128 publications

(140 citation statements)

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“…For this paper we chose RNO 90, a young solar-mass star (G5) with strong water vapor emission in the mid-infrared. RNO 90 is located near (but not inside) the LDN 43 dark cloud roughly 10 degrees from the well-known ρ Ophiuchus young stellar cluster at a distance generally assumed to be that of the cluster of 125 pc 23,24 . The disk is optically thick in the infrared at all radii, and there have been no detections of structural "complications" as seen in more evolved disks, such as TW Hya 25 , although RNO 90 is also not as thoroughly observed.…”

Section: Example Disk: Rno 90mentioning

confidence: 99%

The chemistry of planet-forming regions is not interstellar

Pontoppidan

Blevins

2014

Faraday Discuss.

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Advances in infrared and submillimeter technology have allowed for detailed observations of the molecular content of the planet-forming regions of protoplanetary disks. In particular, disks around solar-type stars now have growing molecular inventories that can be directly compared with both prestellar chemistry and that inferred for the early solar nebula. The data directly address the old question whether the chemistry of planet-forming matter is similar or different and unique relative to the chemistry of dense clouds and protostellar envelopes. The answer to this question may have profound consequences for the structure and composition of planetary systems. The practical challenge is that observations of emission lines from disks do not easily translate into chemical concentrations. Here, we present a two-dimensional radiative transfer model of RNO 90, a classical protoplanetary disk around a solar-mass star, and retrieve the concentrations of dominant molecular carriers of carbon, oxygen and nitrogen in the terrestrial region around 1 AU. We compare our results to the chemical inventory of dense clouds and protostellar envelopes, and argue that inner disk chemistry is, as expected, fundamentally different from prestellar chemistry. We find that the clearest discriminant may be the concentration of CO 2 , which is extremely low in disks, but one of the most abundant constituents of dense clouds and protostellar envelopes.

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Section: Example Disk: Rno 90mentioning

confidence: 99%

The chemistry of planet-forming regions is not interstellar

Pontoppidan

Blevins

2014

Faraday Discuss.

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“…Ophiuchus is considered to be the nearest site of clustered star formation (Wilking & Lada 1983;Motte, André & Neri 1998). Star formation in Ophiuchus is heavily influenced by the nearby Sco OB2 association (Vrba 1977), the centre of which is at a distance of 11 ± 3 pc from Ophiuchus (Mamajek 2008). The southwest/northeast-aligned filamentary streamers from each of the central regions are thought to be due to the effects of this association (Vrba 1977;Loren 1989).…”

Section: Introductionmentioning

confidence: 99%

The JCMT Gould Belt Survey: first results from the SCUBA-2 observations of the Ophiuchus molecular cloud and a virial analysis of its prestellar core population

Pattle¹,

Ward-Thompson²,

Kirk³

et al. 2015

Monthly Notices of the Royal Astronomical Society

140

146

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In this paper we present the first observations of the Ophiuchus molecular cloud performed as part of the James Clerk Maxwell Telescope (JCMT) Gould Belt Survey (GBS) with the SCUBA-2 instrument. We demonstrate methods for combining these data with previous HARP CO, Herschel, and IRAM N 2 H + observations in order to accurately quantify the properties of the SCUBA-2 sources in Ophiuchus. We produce a catalogue of all of the sources found by SCUBA-2. We separate these into protostars and starless cores. We list all of the starless cores and perform a full virial analysis, including external pressure. This is the first time that external pressure has been included in this level of detail. We find that the majority of our cores are either bound or virialised. Gravitational energy and external pressure are on average of a similar order of magnitude, but with some variation from region to region. We find that cores in the Oph A region are gravitationally bound prestellar cores, while cores in the Oph C and E regions are pressure-confined. We determine that N 2 H + is a good tracer of the bound material of prestellar cores, although we find some evidence for N 2 H + freezeout at the very highest core densities. We find that non-thermal linewidths decrease substantially between the gas traced by C 18 O and that traced by N 2 H + , indicating the dissipation of turbulence at higher densities. We find that the critical Bonnor-Ebert stability criterion is not a good indicator of the boundedness of our cores. We detect the pre-brown dwarf candidate Oph B-11 and find a flux density and mass consistent with previous work. We discuss regional variations in the nature of the cores and find further support for our previous hypothesis of a global evolutionary gradient across the cloud from southwest to northeast, indicating sequential star formation across the region.

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“…Ophiuchus is considered to be the nearest site of clustered star formation (Wilking & Lada 1983;Motte et al 1998). Star formation in Ophiuchus is heavily influenced by the nearby Sco OB2 association (Vrba 1977), the centre of which is at a distance of 11 ± 3 pc from Ophiuchus (Mamajek 2008). The southwest/northeast-aligned filamentary streamers from each of the central regions are thought to be due to the effects of this association (Vrba 1977;).…”

Section: Discussionmentioning

confidence: 99%

“…De Geus (1992) proposed that star formation proceeded through the three sub-groups of the Scorpius-Centaurus OB association, beginning in the Lower-Centaurus Crux group, followed by the Upper-Centarus Lupus group, and continuing into the Upper Scorpius group. It has long been suggested that the material in the Ophiuchus molecular cloud is being compressed by interaction with a subset of the Upper Scorpius group, the Sco OB2 association (Vrba 1977); furthermore, ascribes the extended filamentary streamers in the Ophiuchus molecular cloud to the effects of the Sco OB2 association, ∼ 11 pc distant (Mamajek 2008 find that the regions of Ophiuchus in closest proximity to the Sco OB2 association have the most active star formation history, and suggest that this is a result of sequential star formation in the region. The Scorpius-Centaurus OB association is shown in Figure 1.5.…”

Section: Sequential Star Formationmentioning

confidence: 99%