Trigonometric Parallaxes of High Mass Star Forming Regions: The Structure and Kinematics of the Milky Way

Reid, M. J.; Menten, K. M.; Brunthaler, A.; Zheng, Xingwu; Dame, T. M.; Xu, Ye; Wu, Y. W.; Zhang, B.; Sanna, A.; Sato, M.; Hachisuka, Kazuya; Choi, Yoon Kyung; Immer, K.; Moscadelli, L.; Rygl, K. L. J.; Bartkiewicz, A.

doi:10.1088/0004-637x/783/2/130

Cited by 1,305 publications

(1,960 citation statements)

References 87 publications

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“…This estimate of circular velocity at the solar position is substantially smaller than our value of Vc(R0) = 239.89 ± 5.92 km s −1 , which is in excellent agreement with most of the recent independent determinations (e.g. McMillan 2011; Schönrich 2012; Reid et al 2014;Sharma et al 2014). Their analysis also yields an estimate of V⊙ of 26 ± 3 km s −1 .…”

Section: Comparisons With Other Worksupporting

confidence: 92%

“…Finally, at present, the best constraint on the V φ,⊙ comes from the proper motion measurements of Sgr A * , yielding a value that is also in accordance with other most recent independent determinations (e.g. Reid et al 2014;Sharma et al 2014). Therefore, we have assumed that there are no systematic errors arising from our adopted value of V φ,⊙ in deriving the RC.…”

Section: Systematicssupporting

confidence: 72%

“…Combining this estimate of Vc(R0) and the known V φ,⊙ , we find an azimuthal peculiar velocity of the Sun, V⊙, of 12.09 ± 7.61 km s −1 . As defined in Section 2.1, the current analysis assumes R0 = 8.34 kpc as determined by Reid et al (2014). Actually, as evident from Eq.…”

Section: Fitting and Resultsmentioning

confidence: 99%

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The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution

Huang

Liu

Yuan

et al. 2016

Mon. Not. R. Astron. Soc.

159

179

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The rotation curve (RC) of the Milky Way out to ∼ 100 kpc has been constructed using ∼ 16, 000 primary red clump giants (PRCGs) in the outer disk selected from the LSS-GAC and the SDSS-III/APOGEE survey, combined with ∼ 5700 halo K giants (HKGs) selected from the SDSS/SEGUE survey. To derive the RC, the PRCG sample of the warm disc population and the HKG sample of halo stellar population are respectively analyzed using a kinematical model allowing for the asymmetric drift corrections and re-analyzed using the spherical Jeans equation along with measurements of the anisotropic parameter β currently available. The typical uncertainties of RC derived from the PRCG and HKG samples are respectively 5-7 km s −1 and several tens km s −1 . We determine a circular velocity at the solar position, V c (R 0 ) = 240 ± 6 km s −1 and an azimuthal peculiar speed of the Sun, V ⊙ = 12.1 ± 7.6 km s −1 , both in good agreement with the previous determinations. The newly constructed RC has a generally flat value of 240 km s −1 within a Galactocentric distance r of 25 kpc and then decreases steadily to 150 km s −1 at r ∼ 100 kpc. On top of this overall trend, the RC exhibits two prominent localized dips, one at r ∼ 11 kpc and another at r ∼ 19 kpc. From the newly constructed RC, combined with other constraints, we have built a parametrized mass model for the Galaxy, yielding a virial mass of the Milky Way's dark matter halo of 0.90 +0.07 −0.08 × 10 12 M ⊙ and a local dark matter density, ρ ⊙,dm = 0.32 +0.02 −0.02 GeV cm −3 .

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Section: Comparisons With Other Worksupporting

confidence: 92%

Section: Systematicssupporting

confidence: 72%

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The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution

Huang

Liu

Yuan

et al. 2016

Mon. Not. R. Astron. Soc.

159

179

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show abstract

“…For this model, at least 50% of the total absorption comes from beyond 7 kpc from the Sun, and 90% from within 50 kpc. In the simplest case of a stationary halo, the Galactic rotation of the Local Standard of Rest (Reid et al 2014 Figure 3 shows the measured velocities with the stationary and corotating models.…”

Section: Halo Modelmentioning

confidence: 99%

The Rotation of the Hot Gas Around the Milky Way

Hodges-Kluck

Miller

Bregman

2016

ApJ

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The hot gaseous halos of galaxies likely contain a large amount of mass and are an integral part of galaxy formation and evolution. The Milky Way has a2 10 6 K halo that is detected in emission and by absorption in the O VII resonance line against bright background active galactic nuclei (AGNs), and for which the best current model is an extended spherical distribution. Using XMM-Newton Reflection Grating Spectrometer data, we measure the Doppler shifts of the O VII absorption-line centroids toward an ensemble of AGNs. These Doppler shifts constrain the dynamics of the hot halo, ruling out a stationary halo at about s 3 and a co-rotating halo at s 2 , and leading to a best-fit rotational velocity of =  f v 183 41 km s −1 for an extended halo model. These results suggest that the hot gas rotates and that it contains an amount of angular momentum comparable to that in the stellar disk. We examined the possibility of a model with a kinematically distinct disk and spherical halo. To be consistent with the emission-line X-ray data, the disk must contribute less than 10% of the column density, implying that the Doppler shifts probe motion in the extended hot halo.

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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: Introductionmentioning

confidence: 96%

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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Trigonometric Parallaxes of High Mass Star Forming Regions: The Structure and Kinematics of the Milky Way

Cited by 1,305 publications

References 87 publications

The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution

The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution

The Rotation of the Hot Gas Around the Milky Way

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

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