The CARMA-NRO Orion Survey

Kong, Shuo; Arce, Héctor G.; Feddersen, Jesse R.; Carpenter, John M.; Nakamura, Fúmitaka; Shimajiri, Yoshito; Isella, Andrea; Ossenkopf-Okada, Volker; Sargent, Anneila I.; Sánchez-Monge, Á.; Suri, S.; Kauffmann, Jens; Pillai, T.; Pineda, Jaime E.; Koda, Jin; Bally, John; Lis, D. C.; Padoan, Paolo; Klessen, Ralf S.; Mairs, Steve; Goodman, Alyssa A.; Goldsmith, Paul F.; McGehee, P.; Schilke, P.; Teuben, Peter; Maureira, María José; Hara, Chihomi; Ginsburg, Adam; Burkhart, Blakesley; Smith, Rowan J.; Schmiedeke, A.; Pineda, J. L.; Ishii, Shun; Sasaki, Kazushige; Kawabe, Ryohei; Urasawa, Yumiko; Oyamada, Shuri; Tanabe, Yoshihiro

doi:10.3847/1538-4365/aabafc

Cited by 77 publications

(103 citation statements)

References 86 publications

(96 reference statements)

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“…The main filament has somewhat higher temperatures at ∼ 50 K in the northern region. The southern part including L1641N and NGC 1999 has somewhat lower temperature at 10−20 K. This temperature distribution is consistent with that of Kong et al (2018) with a finer angular resolution.…”

Section: Orion Asupporting

confidence: 82%

“…In the present paper, we present the data obtained with the Nobeyama 45-m telescope. The detail of the CARMA+Nobeyama combined data is presented in Kong et al (2018). OMC-1 is a part of the north area of Orion A.…”

Section: Aquila Rift (Serpens South)mentioning

confidence: 99%

“…The result of accurate outflow identification is presented in Tanabe et al (2018), who found 44 CO outflows in Orion A, 17 out of which are new detections. Based on the identified outflow physical parameters, they estimated the momentum injection rates due to the molecular outflows and found that the total momentum injection rate due to the outflows and the expanding shells identified in the 13 CO data by Feddersen et al (2018) is larger than the turbulence dissipation rate in Orion A. Thus, the stellar feedback such as the molecular outflows and expanding shells driven by stellar winds is an important mechanism to replenish the internal cloud turbulence.…”

mentioning

confidence: 99%

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Nobeyama 45 m mapping observations toward the nearby molecular clouds Orion A, Aquila Rift, and M17: Project overview

Nakamura

Ishii

Dobashi

et al. 2019

Publications of the Astronomical Society of Japan

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We carried out mapping observations toward three nearby molecular clouds, Orion A, Aquila Rift, and M17, using a new 100 GHz receiver, FOREST, on the Nobeyama 45-m telescope. In the present paper, we describe the details of the data obtained such as intensity calibration, data sensitivity, angular resolution, and velocity resolution. Each target contains at least one high-mass star-forming region. The target molecular lines were 12 CO (J = 1 − 0), 13 CO (J =, and CCS (J N = 8 7 − 7 6 ), with which we covered the density range of 10 2 cm −3 to 10 6 cm −3 with an angular resolution of ∼ 20 and a velocity resolution of ∼ 0.1 km s −1 . Assuming the representative distances of 414 pc, 436 pc, and 2.1 kpc, the maps of Orion A, Aquila Rift, and M17 cover most of the densest parts with areas of about 7 pc × 15 pc, 7 pc × 7 pc, and 36 pc × 18 pc, respectively. On the basis of the 13 CO column density distribution, the total molecular masses are derived to be 3.86 × 10 4 M , 2.67 × 10 4 M , and 8.1 × 10 5 M for Orion A, Aquila Rift, and M17, respectively. For all the clouds, the H 2 column density exceeds the theoretical threshold for high-mass star formation of > ∼ 1 g cm −2 , only toward the regions which contain current high-mass star-forming sites. For other areas, further mass accretion or dynamical compression would be necessary for future high-mass star formation. This is consistent with the current star formation activity. Using the 12 CO data, we demonstrate that our data have enough capability to identify molecular outflows, and for Aquila Rift, we identify 4 new outflow candidates. The scientific results will be discussed in details in separate papers.

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Section: Orion Asupporting

confidence: 82%

Section: Aquila Rift (Serpens South)mentioning

confidence: 99%

mentioning

confidence: 99%

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Nobeyama 45 m mapping observations toward the nearby molecular clouds Orion A, Aquila Rift, and M17: Project overview

Nakamura

Ishii

Dobashi

et al. 2019

Publications of the Astronomical Society of Japan

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“…For M43, we use CO data observed with the Combined Array for Millimeter-Wave Astronomy (CARMA), within the CARMA-NRO Orion Survey project (Kong et al 2018;Suri et al 2019). The molecular lines observed are 13 CO J = 1-0 and C 18 O J = 1-0 for the seven [C ii] positions.…”

Section: Co Molecular Emissionmentioning

confidence: 99%

[C II] 158 μm self-absorption and optical depth effects

Guevara

Stützki

Ossenkopf-Okada

et al. 2020

A&A

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Context. The [C ii] 158 µm far-infrared (FIR) fine-structure line is one of the most important cooling lines of the star-forming interstellar medium (ISM). It is used as a tracer of star formation efficiency in external galaxies and to study feedback effects in parental clouds. High spectral resolution observations have shown complex structures in the line profiles of the [C ii] emission. Aims. Our aim is to determine whether the complex profiles observed in [ 12 C ii] are due to individual velocity components along the line-of-sight or to self-absorption based on a comparison of the [ 12 C ii] and isotopic [ 13 C ii] line profiles. Methods. Deep integrations with the SOFIA/upGREAT 7-pixel array receiver in the sources of M43, Horsehead PDR, Monoceros R2, and M17 SW allow for the detection of optically thin [ 13 C ii] emission lines, along with the [ 12 C ii] emission lines, with a high signalto-noise ratio (S/N). We first derived the [ 12 C ii] optical depth and the [C ii] column density from a single component model. However, the complex line profiles observed require a double layer model with an emitting background and an absorbing foreground. A multicomponent velocity fit allows us to derive the physical conditions of the [C ii] gas: column density and excitation temperature. Results. We find moderate to high [ 12 C ii] optical depths in all four sources and self-absorption of [ 12 C ii] in Mon R2 and M17 SW. The high column density of the warm background emission corresponds to an equivalent A v of up to 41 mag. The foreground absorption requires substantial column densities of cold and dense [C ii] gas, with an equivalent A v ranging up to about 13 mag. Conclusions. The column density of the warm background material requires multiple photon-dominated region (PDR) surfaces stacked along the line of sight and in velocity. The substantial column density of dense and cold foreground [C ii] gas detected in absorption cannot be explained with any known scenario and we can only speculate on its origins. Key words. ISM:clouds -ISM:individual objects: M43 -ISM:individual objects: M17 -photon-dominated region (PDR) -ISM:individual objects: Horsehead -ISM:individual objects: MonR2 1 At that time, the spectroscopic data were less accurate and the wavelength of the transition was assumed to fall at 157 µm instead of 158 µm.Article number, page 1 of 40 A&A proofs: manuscript no. 34380corr_2 mentum change F=2→1, F=1→0, and F=1→1. The frequencies of the fine structure transitions of both isotopes were determined by Cooksy et al. (1986). The astronomical observations are fully consistent with these frequencies, as was discussed by Ossenkopf et al. (2013), who also noted that the relative strengths of the [ 13 C ii] hyperfine satellites (s F→F , see Table 1) given by Cooksy et al. (1986) are incorrect. We summarize all the relevant [ 12 C ii] and [ 13 C ii] spectroscopic parameters in Table 1, including the velocity offsets of the [ 13 C ii] hyperfine components relative to [ 12 C ii]. The frequency separation of the hyperfi...

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“…The GMC is mainly composed of a large and dense integral-shaped-filament (ISF, Bally et al 1987) in the northern part that contains star-forming regions OMC 1-4, and a relatively extended and less dense tail in the southern part that covers the LDN 1641 region. Kong et al (2018) have made a brief review of the surveys that covers the ISF in their table 1. The broad dynamic range of column densities revealed by the previous studies makes the GMC an ideal case for N-PDF analysis.…”

Section: Introductionmentioning

confidence: 99%

The column density structure of Orion A depicted by N-PDF

Wang

et al. 2020

Res. Astron. Astrophys.

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We have conducted a large-field simultaneous survey of 12 CO, 13 CO, and C 18 O J = 1 − 0 emission toward the Orion A giant molecular cloud (GMC) with a sky coverage of ∼ 4.4 deg 2 using the PMO-13.7 m millimeter-wavelength telescope. We use the probability distribution function of the column density (N-PDF) to investigate the distribution of molecular hydrogen in the Orion A GMC. The H 2 column density, derived from the 13 CO emission, of the GMC is dominated by log-normal distribution in the range from ∼4×10 21 to ∼1.5×10 23 cm −2 with excesses both at the low-density and high-density ends. The excess of the low-density end is possibly caused by an extended and low-temperature (∼10 K) component with velocities in the range of 5−8 km s −1 . Compared with the northern sub-regions, the southern sub-regions of the Orion A GMC contain less gas with column density in N H2 > 1.25 × 10 22 cm −2 . The dispersions of the N-PDFs of the sub-regions are found to correlate with the evolutionary stages of the clouds across the Orion A GMC. The structure hierarchy of Orion A GMC is explored with the DENDROGRAM algorithm, and it is found that the GMC is composed of two branches. All structures except one in the tree have virial parameters less than 2, indicating self-gravity is important on the spatial scales from ∼0.3 to ∼4 pc. Although power-laws and departures from log-normal distributions are found at the high-density end of N-PDFs of active star-forming regions, the N-PDFs of structures in the Orion A GMC are predominantly log-normal on scales from R∼0.4 to 4 pc.

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The CARMA-NRO Orion Survey

Cited by 77 publications

References 86 publications

Nobeyama 45 m mapping observations toward the nearby molecular clouds Orion A, Aquila Rift, and M17: Project overview

Nobeyama 45 m mapping observations toward the nearby molecular clouds Orion A, Aquila Rift, and M17: Project overview

[C II] 158 μm self-absorption and optical depth effects

The column density structure of Orion A depicted by N-PDF

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The CARMA-NRO Orion Survey

Cited by 77 publications

References 86 publications

Nobeyama 45 m mapping observations toward the nearby molecular clouds Orion A, Aquila Rift, and M17: Project overview

Nobeyama 45 m mapping observations toward the nearby molecular clouds Orion A, Aquila Rift, and M17: Project overview

[C II] 158 μm self-absorption and optical depth effects

The column density structure of Orion A depicted by N-PDF

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Product

Resources

About

[C II] 158 μm self-absorption and optical depth effects