Annual Parallax Measurements of an Infrared Dark Cloud, MSXDC G034.43+00.24 with VERA

Kurayama, Tomoharu; Nakagawa, Akiharu; Sawada-Satoh, Satoko; Sato, Katsuhisa; Honma, Mareki; Sunada, Kazuyoshi; Hirota, Tomoya; Imai, Hiroshi

doi:10.1093/pasj/63.3.513

Cited by 83 publications

(61 citation statements)

References 42 publications

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“…Column 8 gives the kinematic distance of the cloud from Simon et al (2006). While Kurayama et al (2011) find a 1.56 kpc distance for IRDC F, containing F1 and F2, Foster et al (2012) find a distance consistent with the kinematic distance for IRDC F, based upon extinction measurements. We thus elect to use the kinematic distances from Simon et al (2006) for all four clumps in this paper.…”

Section: Introductionmentioning

confidence: 64%

Mid-JCO shock tracing observations of infrared dark clouds. I.

Pon¹,

Caselli²,

Johnstone³

et al. 2015

A&A

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Infrared dark clouds (IRDCs) are dense, molecular structures in the interstellar medium that can harbour sites of high-mass star formation. IRDCs contain supersonic turbulence, which is expected to generate shocks that locally heat pockets of gas within the clouds. We present observations of the CO J = 8-7, 9-8, and 10-9 transitions, taken with the Herschel Space Observatory, towards four dense, starless clumps within IRDCs (C1 in G028.37+00.07, F1 and F2 in G034.43+0007, and G2 in G034.77-0.55). We detect the CO J = 8-7 and 9-8 transitions towards three of the clumps (C1, F1, and F2) at intensity levels greater than expected from photodissociation region (PDR) models. The average ratio of the 8-7 to 9-8 lines is also found to be between 1.6 and 2.6 in the three clumps with detections, significantly smaller than expected from PDR models. These low line ratios and large line intensities strongly suggest that the C1, F1, and F2 clumps contain a hot gas component not accounted for by standard PDR models. Such a hot gas component could be generated by turbulence dissipating in low velocity shocks.

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Section: Introductionmentioning

confidence: 64%

Mid-JCO shock tracing observations of infrared dark clouds. I.

Pon¹,

Caselli²,

Johnstone³

et al. 2015

A&A

View full text Add to dashboard Cite

show abstract

“…Column 10 gives the kinematic distance of the cloud from Simon et al (2006). While Kurayama et al (2011) find a 1.56 kpc distance for IRDC F, containing F1 and F2, Foster et al (2012) find a distance consistent with the kinematic distance for IRDC F, based upon extinction measurements. We thus elect to use the kinematic distances from Simon et al (2006) for both IRDCs in this paper.…”

Section: Introductionmentioning

confidence: 66%

Mid-JCO shock tracing observations of infrared dark clouds

Pon

Johnstone

Caselli

et al. 2016

A&A

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Infrared dark clouds are kinematically complex molecular structures in the interstellar medium that can host sites of massive star formation. We present maps measuring 4 square arcminutes of the 12 CO, 13 CO, and C 18 O J = 3 to 2 lines from selected locations within the C and F (G028.37+00.07 and G034.43+00.24) infrared dark clouds (IRDCs), as well as single pointing observations of the 13 CO and C 18 O J = 2 to 1 lines towards three cores within these clouds. We derive CO gas temperatures throughout the maps and find that CO is significantly frozen out within these IRDCs. We find that the CO depletion tends to be the highest near column density peaks with maximum depletion factors between 5 and 9 in IRDC F and between 16 and 31 in IRDC C. We also detect multiple velocity components and complex kinematic structure in both IRDCs. Therefore, the kinematics of IRDCs seem to point to dynamically evolving structures yielding dense cores with considerable depletion factors.

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“…We acknowledge, however, that the error in the kinematic distance can be larger due to randomly oriented peculiar motions of up to 20 or 30 km s −1 with respect to Galactic rotation, as shown, e.g., by the hydrodynamical simulations by Baba et al (2009). Similarly, such large systematic velocities have been found from maser parallax observations, leading to up to a factor 2 wrong kinematic distances (e.g., Xu et al 2006;Kurayama et al 2011). However, in some such cases it has been found also that the star-forming region does follow circular rotation (e.g., Sato et al 2010).…”

Section: B43 Derivation Of the Kinematic Distancesmentioning

confidence: 72%

Stellar clusters in the inner Galaxy and their correlation with cold dust emission

Morales

Wyrowski

Schüller

et al. 2013

A&A

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Context. Stars are born within dense clumps of giant molecular clouds, and constitute young stellar agglomerates known as embedded clusters, which only evolve into bound open clusters under special conditions. Aims. We statistically study all embedded clusters (ECs) and open clusters (OCs) known so far in the inner Galaxy, in particular investigating their interaction with the surrounding molecular environment and the differences in their evolution. Methods. We first compiled a merged list of 3904 clusters from optical and infrared cluster catalogs in the literature, including 75 new (mostly embedded) clusters discovered by us in the GLIMPSE survey. From this list, 695 clusters are within the Galactic range | | ≤ 60 • and |b| ≤ 1.5 • covered by the ATLASGAL survey, which was used to search for correlations with submm dust continuum emission tracing dense molecular gas. We defined an evolutionary sequence of five morphological types: deeply embedded cluster (EC1), partially embedded cluster (EC2), emerging open cluster (OC0), OC still associated with a submm clump in the vicinity (OC1), and OC without correlation with ATLASGAL emission (OC2). Together with this process, we performed a thorough literature survey of these 695 clusters, compiling a considerable number of physical and observational properties in a catalog that is publicly available. Results. We found that an OC defined observationally as OC0, OC1, or OC2 and confirmed as a real cluster is equivalent to the physical concept of OC (a bound exposed cluster) for ages in excess of ∼16 Myr. Some observed OCs younger than this limit can actually be unbound associations. We found that our OC and EC samples are roughly complete up to ∼1 kpc and ∼1.8 kpc from the Sun, respectively, beyond which the completeness decays exponentially. Using available age estimates for a few ECs, we derived an upper limit of 3 Myr for the duration of the embedded phase. Combined with the OC age distribution within 3 kpc of the Sun, which shows an excess of young exposed clusters compared to a theoretical fit that considers classical disruption mechanisms, we computed an embedded and young cluster dissolution fraction of 88 ± 8%. This high fraction is thought to be produced by several factors and not only by the classical paradigm of fast gas expulsion.

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Annual Parallax Measurements of an Infrared Dark Cloud, MSXDC G034.43+00.24 with VERA

Cited by 83 publications

References 42 publications

Mid-JCO shock tracing observations of infrared dark clouds. I.

Mid-JCO shock tracing observations of infrared dark clouds. I.

Mid-JCO shock tracing observations of infrared dark clouds

Stellar clusters in the inner Galaxy and their correlation with cold dust emission

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