The Bones of the Milky Way

Goodman, Alyssa A.; Alves, J.; Beaumont, Christopher N.; Benjamin, Robert A.; Borkin, Michelle A.; Burkert, Andreas; Dame, T. M.; Jackson, James M.; Kauffmann, Jens; Robitaille, Thomas; Smith, Rowan J.

doi:10.1088/0004-637x/797/1/53

Cited by 151 publications

(196 citation statements)

References 50 publications

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“…Spatial, velocity and luminosity distributions used in the current model. We assumed the sun's vertical position to be z=0 pc and any change in this value, which Goodman et al (2014) suggested to be 25 pc, was found negligible at these scales. References: (1) , (2) Green & McClureGriffiths (2011), and (3) Pestalozzi et al (2007).…”

Section: Model For the 67 Ghz Methanol Maser Distribution In The Spimentioning

confidence: 99%

Simulated Galactic methanol maser distribution to constrain Milky Way parameters

Quiroga-Nuñez

Langevelde

Reid

et al. 2017

A&A

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Context. Using trigonometric parallaxes and proper motions of masers associated with massive young stars, the Bar and Spiral Structure Legacy (BeSSeL) survey has reported the most accurate values of the Galactic parameters so far. The determination of these parameters with high accuracy has a widespread impact on Galactic and extragalactic measurements. Aims. This research is aimed at establishing the confidence with which such parameters can be determined. This is relevant for the data published in the context of the BeSSeL survey collaboration, but also for future observations, in particular from the southern hemisphere. In addition, some astrophysical properties of the masers can be constrained, notably the luminosity function. Methods. We have simulated the population of maser-bearing young stars associated with Galactic spiral structure, generating several samples and comparing them with the observed samples used in the BeSSeL survey. Consequently, we checked the determination of Galactic parameters for observational biases introduced by the sample selection. Results. Galactic parameters obtained by the BeSSeL survey do not seem to be biased by the sample selection used. In fact, the published error estimates appear to be conservative for most of the parameters. We show that future BeSSeL data and future observations with southern arrays will improve the Galactic parameters estimates and smoothly reduce their mutual correlation. Moreover, by modeling future parallax data with larger distance values and, thus, greater relative uncertainties for a larger numbers of sources, we found that parallax-distance biasing is an important issue. Hence, using fractional parallax uncertainty in the weighting of the motion data is imperative. Finally, the luminosity function for 6.7 GHz methanol masers was determined, allowing us to estimate the number of Galactic methanol masers.

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Section: Model For the 67 Ghz Methanol Maser Distribution In The Spimentioning

confidence: 99%

Simulated Galactic methanol maser distribution to constrain Milky Way parameters

Quiroga-Nuñez

Langevelde

Reid

et al. 2017

A&A

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“…The observed variation of Galactic latitude with repect to Galactic longitude can be understood in terms of the Sun's vertical displacement from the physical mid-plane (e.g., Hammersley et al 1995;Su et al 2016). Various observations have revealed that the Sun is about 10-30 pc above the physical mid-plane (e.g., Chen et al 2001;Reed 2006;Majaess et al 2009;Goodman et al 2014;Su et al 2016;Karim & Mamajek 2016).…”

Section: The Spiral Arm and Warp Of The Galactic Plane Traced By Co Ementioning

confidence: 99%

Molecular Clouds in the Extreme Outer Galaxy between l = 34.°75 to 45.°25

Sun

Zhang

et al. 2017

ApJS

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We present the result of an unbiased CO survey in Galactic range of 34.75• ≤l≤ 45.25• and -5.25• ≤b≤ 5.25• , and velocity range beyond the Outer arm. A total of 168 molecular clouds (MCs) are identified within the Extreme Outer Galaxy (EOG) region, and 31 of these MCs are associated with 13 CO emission. However, none of them show significant C 18 O emission under current detection limit. The typical size and mass of these MCs are 5 pc and 3×10 3 M ⊙ , implying the lack of large and massive MCs in the EOG region. Similar to MCs in the outer Galaxy, the velocity dispersions of EOG clouds are also correlated with their sizes, however, are well displaced below the scaling relationship defined by the inner Galaxy MCs. These MCs with a median Galactocentric radius of 12.6 kpc, show very different distributions from those of the MCs in the Outer arm published in our previous paper, while roughly follow the Outer Scutum-Centaurus arm defined by Dame & Thaddeus (2011). This result may provide a robust evidence for the existence of the Outer Scutum-Centaurus arm. The lower limit of the total mass of this segment is about 2.7×10 5 M ⊙ , which is about one magnitude lower than that of the Outer arm. The mean thickness of gaseous disk is about 1.45• or 450 pc, and the scale height is about 1.27• or 400 pc above the b = 0 • plane. The warp traced by CO emission is very obvious in the EOG region and its amplitude is consistent with the predictions by other warp models using different tracers, such as dust, HI and stellar components of our Galaxy.

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“…Nessie IRDC is rare object so far. Jackson et al (2010) obtained that the length of Nessie IRDC is 80 pc, but Goodman et al (2014) suggested that Nessie is probably longer than 80 pc. A similar filament of more than 50 pc length has been presented by Kainulainen et al (2011).…”

Section: Distribution Of Young Stellar Objectsmentioning

confidence: 99%

Gas Kinematics and Star Formation in the Filamentary Irdc G34.43+0.24

Zhang

et al. 2016

ApJ

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We performed a multiwavelength study toward the infrared dark cloud (IRDC) G34.43+0.24. New maps of 13 CO J = 1-0 and C 18 O J = 1-0 were obtained from the Purple Mountain Observatory (PMO) 13.7 m radio telescope. At 8 μm (Spitzer-IRAC), IRDC G34.43+0.24 appears to be a dark filament extended by 18′ along the north-south direction. Based on the association with the 870 μm and C 18 O J = 1-0 emission, we suggest that IRDC G34.43+0.24 should not be 18′ in length, but extend to 34′. IRDC G34.43+0.24 contains some massive protostars, UC H II regions, and infrared bubbles. The spatial extend of IRDC G34.43+0.24 is about 37 pc, assuming a distance of 3.7 kpc. IRDC G34.43+0.24 has a linear mass density of ∼1.6×103 M e pc −1 , which is roughly consistent with its critical mass to length ratio. The turbulent motion may help stabilize the filament against the radial collapse. Both infrared bubbles N61 and N62 show a ringlike structure at 8 μm. In particular, N61 has a double-shell structure that has expanded into IRDC G34.43+0.24. The outer shell is traced by 8 μm and 13 CO J = 1-0 emission, while the inner shell is traced by 24 μm and 20 cm emission. We suggest that the outer shell (9.9×10 5 years) is created by the expansion of H II region G34.172+0.175, while the inner shell (4.1∼6.3×10 5 years) may be produced by the energetic stellar wind of its central massive star. From the GLIMPSE I catalog, we selected some Class I sources with an age of ∼10 5 years. These Class I sources are clustered along the filamentary molecular cloud.

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The Bones of the Milky Way

Cited by 151 publications

References 50 publications

Simulated Galactic methanol maser distribution to constrain Milky Way parameters

Simulated Galactic methanol maser distribution to constrain Milky Way parameters

Molecular Clouds in the Extreme Outer Galaxy between l = 34.°75 to 45.°25

Gas Kinematics and Star Formation in the Filamentary Irdc G34.43+0.24

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