Trigonometric parallaxes of star-forming regions in the Sagittarius spiral arm

Wu, Y. W.; Sato, M.; Reid, M. J.; Moscadelli, L.; Zhang, B.; Xu, Ye; Brunthaler, A.; Menten, K. M.; Dame, T. M.; Zheng, Xingwu

doi:10.1051/0004-6361/201322765

Cited by 144 publications

(108 citation statements)

References 71 publications

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“…As Wu et al (2014) note, the parallax distances to G014.63-00.57 and M17 are in agreement, while the significantly nearer distance to G014.33-00.64 indicates that this maser belongs to a foreground cloud. All three masers have similar v LSR and are assigned to the Sagittarius-Carina spiral arm by Reid et al (2014) and Wu et al (2014), with M17 and G014.63-00.57 on the far side and G014.33-00.64 on the near side of the arm.…”

Section: Introductionsupporting

confidence: 57%

“…This parallax distance does not strongly depart from the kinematic distance and has become the generally accepted distance to the H II region and M17 SW. Wu et al (2014) report a parallax distance of 1.8 ± 0.1 kpc to a water maser associated with G014.63-00.57, located at the end of M17 SWex closest to the M17 H II region. As Wu et al (2014) note, the parallax distances to G014.63-00.57 and M17 are in agreement, while the significantly nearer distance to G014.33-00.64 indicates that this maser belongs to a foreground cloud. All three masers have similar v LSR and are assigned to the Sagittarius-Carina spiral arm by Reid et al (2014) and Wu et al (2014), with M17 and G014.63-00.57 on the far side and G014.33-00.64 on the near side of the arm.…”

Section: Introductionmentioning

confidence: 88%

“…M17 SWex is kinematically associated with the M17 H II region and its adjacent GMC, M17 SW, with the bulk of the molecular emission found in the range v LSR = 19-22 km s −1 , and the entire complex has historically been assumed to lie at the near kinematic distance of 2.3 kpc (Elmegreen & Lada 1976;Jaffe & Fazio 1982;B13). Recent maser parallax measurements using very long baseline interferometry have both clarified and complicated the threedimensional picture of the M17 complex Wu et al 2014). Sato et al (2010) reported a distance of 1.1 ± 0.1 kpc from parallax measurements to the water maser associated with the dense molecular core and ultracompact H II region G014.33-00.64, located in the midst of the M17 SWex IRDC lanes.…”

Section: Introductionmentioning

confidence: 99%

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RAPID CIRCUMSTELLAR DISK EVOLUTION AND AN ACCELERATING STAR FORMATION RATE IN THE INFRARED DARK CLOUD M17 SWex

Povich

Townsley

Robitaille

et al. 2016

ApJ

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We present a catalog of 840 X-ray sources and first results from a 100 ks Chandra X-ray Observatory imaging study of the filamentary infrared (IR) dark cloud G014.225-00.506, which forms the central regions of a larger cloud complex known as the M17 southwest extension (M17 SWex). In addition to the rich population of protostars and young stellar objects with dusty circumstellar disks revealed by archival data from the Spitzer Space Telescope, we discover a population of X-ray-emitting, intermediate-mass pre-main-sequence stars that lack IR excess emission from circumstellar disks. We model the IR spectral energy distributions of this source population to measure its mass function and place new constraints on the destruction timescales for the inner dust disk for 2-8 M ☉ stars. We also place a lower limit on the star formation rate (SFR) and find that it is quite high (  M 0.007 M ☉ yr −1 ), equivalent to several Orion Nebula Clusters in G14.225-0.506 alone, and likely accelerating. The cloud complex has not produced a population of massive, O-type stars commensurate with its SFR. This absence of very massive (20 M ☉ ) stars suggests that either (1) M17 SWex is an example of a distributed mode of star formation that will produce a large OB association dominated by intermediate-mass stars but relatively few massive clusters, or (2) the massive cores are still in the process of accreting sufficient mass to form massive clusters hosting O stars.

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Section: Introductionsupporting

confidence: 57%

Section: Introductionmentioning

confidence: 88%

Section: Introductionmentioning

confidence: 99%

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RAPID CIRCUMSTELLAR DISK EVOLUTION AND AN ACCELERATING STAR FORMATION RATE IN THE INFRARED DARK CLOUD M17 SWex

Povich

Townsley

Robitaille

et al. 2016

ApJ

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“…Hence, a temperature correction is neces- Sanna et al (2014) (g) Moisés et al (2011) ( †) We revised the spectrophotometric distance of 1.81 kpc by Moisés et al (2011). (h) Wu et al (2014) (i) Wu et al (2012) (j) Reid et al (2014) (k) Dutra et al (2003) (l) Straw et al (1987) (m) Xu et al (2011) (n) Sanna et al (2009) (o) Leurini et al (2011) (p) Kurayama et al (2011) (q) Russeil (2003) (r) Motogi et al (2011) (s) López et al (2011) ( ‡) Peretto et al (2013) adopts 3.25 kpc.…”

Section: Temperature Estimatesmentioning

confidence: 99%

The ATLASGAL survey: The sample of young massive cluster progenitors

Csengeri

Bontemps

Wyrowski

et al. 2017

A&A

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Context. The progenitors of high-mass stars and clusters are still challenging to recognise. Only unbiased surveys, sensitive to compact regions of high dust column density, can unambiguously reveal such a small population of particularly massive and cold clumps. Aims. Here we use the ATLASGAL survey to identify a sample of candidate progenitors of massive clusters in the inner Galaxy. Methods. We characterise a flux limited sample of compact sources selected from the ATLASGAL survey. Sensitive mid-infrared data at 21−24 µm from the WISE and MIPSGAL surveys were explored to search for embedded objects, and complementary spectroscopic data were used to investigate their stability and their star formation activity. Results. We identify an unbiased sample of infrared-quiet massive clumps in the Galaxy that potentially represent the earliest stages of massive cluster formation. An important fraction of this sample consists of sources that have not been studied in detail before. We first find that clumps hosting more evolved embedded objects and infrared-quiet clumps exhibit similar physical properties in terms of mass and size, suggesting that the sources are not only capable of forming high-mass stars, but likely also follow a single evolutionary track leading to the formation of massive clusters. The majority of the clumps are likely not in virial-equilibrium, suggesting collapse on the clump scale. Conclusions. We identify the precursors of the most massive clusters in the Galaxy within our completeness limit, and argue that these objects are undergoing large-scale collapse. This is in line with the low number of infrared-quiet massive clumps and earlier findings that star formation, in particular for high-mass objects is a fast, dynamic process. We propose a scenario in which massive clumps start to fragment and collapse before their final mass is accumulated indicating that strong self-gravity and global collapse is needed to build up rich clusters and the most massive stars.

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“…Recent cases include the Local arm by Xu et al (2013), the Perseus arm by (Zhang et al 2013;Choi et al 2014), and the Saggitarius arm by Wu et al (2014). The general structure is discussed in Reid et al (2014).…”

Section: Structure Of the Local Armmentioning

confidence: 99%

Trigonometric Distance and Proper Motion of Iras 20056+3350: A Massive Star-Forming Region on the Solar Circle

Burns

Nagayama

Handa

et al. 2014

ApJ

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We report our measurement of the trigonometric distance and proper motion of IRAS 20056+3350, obtained from the annual parallax of H 2 O masers. Our distance of D = 4.69 +0.65 −0.51 kpc, which is 2.8 times larger than the near kinematic distance adopted in the literature, places IRAS 20056+3350 at the leading tip of the Local arm and proximal to the solar circle. Using our distance, we reevaluate past observations to reveal IRAS 20056+3350 as a site of massive star formation at a young stage of evolution. This result is consistent with the spectral energy distribution of the source evaluated with published photometric data from UKIDSS, WISE, AKARI, IRAS, and the submillimeter continuum. Both analytical approaches reveal the luminosity of the region to be 2.4 × 10 4 L , and suggest that IRAS 20056+3350 is forming an embedded star of 16 M . We estimated the proper motion of IRAS 20056+3350 to be (μ α cos δ, μ δ ) = (−2.62 ± 0.33, −5.65 ± 0.52) mas yr −1 from the group motion of H 2 O masers, and use our results to estimate the angular velocity of Galactic rotation at the Galactocentric distance of the Sun, Ω 0 = 29.75 ± 2.29 km s −1 kpc −1 , which is consistent with the values obtained for other tangent point and solar circle objects.

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Trigonometric parallaxes of star-forming regions in the Sagittarius spiral arm

Cited by 144 publications

References 71 publications

RAPID CIRCUMSTELLAR DISK EVOLUTION AND AN ACCELERATING STAR FORMATION RATE IN THE INFRARED DARK CLOUD M17 SWex

RAPID CIRCUMSTELLAR DISK EVOLUTION AND AN ACCELERATING STAR FORMATION RATE IN THE INFRARED DARK CLOUD M17 SWex

The ATLASGAL survey: The sample of young massive cluster progenitors

Trigonometric Distance and Proper Motion of Iras 20056+3350: A Massive Star-Forming Region on the Solar Circle

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