Milky Way Gas Dynamics

Englmaier, P.; Gerhard, Ortwin

doi:10.1007/s10569-006-9003-3

Cited by 16 publications

(40 citation statements)

References 28 publications

(48 reference statements)

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“…Jaffe et al (1982) associated IRDC G10.74-0.13 with 12 CO 1 ! 2 ð Þ emission centered at 32 km s À1 , implying d < 3:8 þ0:5 À0:5 kpc for a flat rotation curve and d < 4:4 þ0:6 À0:3 kpc for the Weiner & Sellwood (1999) and Englmaier & Gerhard (2006) models. Our OH spectra (see x 8 below) show a large spectral feature at the same velocities that we also associate with the IRDC.…”

Section: An Upper Limit On the Distance Toward Xte J1810à197mentioning

confidence: 98%

“…The Englmaier & Gerhard (2006) Weiner & Sellwood (1999) result provides an indication of how spiral arms may be affecting the velocity-distance relationship toward XTE J1810À197. We can again rule out distances that lie on the far side of the tangent point and distances that include 30Y 40 km s À1 gas along the line of sight.…”

Section: The Kinematic Distance To Xte J1810à197mentioning

confidence: 99%

“…1). The weak absorption line at V LSR ¼ 14:1 km s À1 can be kinematically associated with gas in the Carina-Sagittarius spiral arm (the first spiral arm inward of the Sun's Galactic position), assuming that the line arises on the near side of the tangent point and using the Galactic rotation model of Englmaier & Gerhard (2006). Likewise, the V LSR ¼ 22:8 and 25.7 km s À1 lines can be kinematically associated with the Crux-Scutum spiral arm (the second spiral arm inward of the Sun).…”

Section: The Absorption Spectra Toward Xte J1810à197mentioning

confidence: 99%

“…The rotation model of Englmaier & Gerhard (2006) used in Figure 9 takes into account the effects of a potential associated with the Galactic bar as well as those associated with spiral arms. The Englmaier & Gerhard (2006) Weiner & Sellwood (1999) result provides an indication of how spiral arms may be affecting the velocity-distance relationship toward XTE J1810À197.…”

Section: The Kinematic Distance To Xte J1810à197mentioning

confidence: 99%

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Neutral Hydrogen Absorption toward XTE J1810−197: The Distance to a Radio‐emitting Magnetar

Minter

Camilo

Ransom

et al. 2008

ApJ

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We have used the Green Bank Telescope (GBT) to measure H i absorption against the anomalous X-ray pulsar XTE J1810À197. Using a flat rotation curve, we find that XTE J1810À197 is located at a distance of 3:4 AE 0:6 kpc. The Galactic bar, however, does have an influence on Galactic rotation velocities that impacts the distance estimate of XTE J1810À197. When rotation curve models that include the Galactic bar are used, we find that XTE J1810À197 is located in the distance range of 3.1Y 4.3 kpc. From information gleaned from the literature, we find an upper limit on the distance to XTE J1810À197 of 4 kpc based on its infrared detection, its location just in front of an Infrared Dark Cloud (G10.74-0.13), and a measurement of the infrared absorption versus distance for this line of sight. Our best determination for the distance to XTE J1810À197 is thus 3.1Y4 kpc. This distance, 3.1Y 4 kpc, is consistent with the distance to XTE J1810À197 of about 3.3 kpc derived from its dispersion measure, and estimates of 2Y5 kpc obtained from fits to its X-ray spectra. We also used the GBT in an attempt to measure absorption in the four OH 18 cm lines against XTE J1810À 197. We were unsuccessful in this, mainly because of its declining radio flux density. Analysis of H i 21 cm, OH 18 cm, and 12 CO(2 ! 1) emission toward XTE J1810À197 allows us to place a lower limit of N H k 4:6 ; 10 21 cm À2 on the nonionized hydrogen column density to XTE J1810À197, consistent with estimates obtained from fits to its X-ray spectra.

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Section: An Upper Limit On the Distance Toward Xte J1810à197mentioning

confidence: 98%

Section: The Kinematic Distance To Xte J1810à197mentioning

confidence: 99%

Section: The Absorption Spectra Toward Xte J1810à197mentioning

confidence: 99%

Section: The Kinematic Distance To Xte J1810à197mentioning

confidence: 99%

See 2 more Smart Citations

Neutral Hydrogen Absorption toward XTE J1810−197: The Distance to a Radio‐emitting Magnetar

Minter

Camilo

Ransom

et al. 2008

ApJ

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“…Nakanishi & Sofue (2006) employed similar CO data and created a three-dimensional gas map based on an assumed circularrotation kinematical model and radial-velocity gradients. Englmaier & Gerhard (2006) used mass models to fit to the terminal velocity curves and spiral arm tangents from CO and H 2 gas. They did not restrict their models to logarithmic shapes.…”

Section: Valléementioning

confidence: 99%

New Velocimetry and Revised Cartography of the Spiral Arms in the Milky Way—a Consistent Symbiosis

Vallée

2008

The Astronomical Journal

244

283

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Recent advances in the determinations of the positions (pitch angle, shape, numbers, interarm separation) and velocities (rotation curve) of the spiral arms are evaluated and compared to previous determinations. Based on these results, an average cartographic model is developed that fits the means of basic input data and provides predictions for the locations of the arms in the Milky Way, for each galactic quadrant. For each spiral arm segment in each galactic quadrant, the LSR radial velocities are calculated for the radial distance as well as for its galactic longitude. From our velocimetric model, arm intercepts (between line of sights and spiral arms) are indicated in velocity space and may be used to find the distance and velocity to any arm, in a given longitude range. Velocity comparisons between model predictions and published CO velocity distribution are done for each galactic quadrant, with good results. Our velocimetric model is not hydromagnetic in character, nor is it a particle-simulation scheme, yet it is simple to use for comparisons with the observations and it is in symbiosis and consistent with our cartographic model (itself simple to use for comparisons with observations). A blending in velocity of the Perseus and Cygnus arms is further demonstrated, as well as an apparent longitude-velocity blending of the starting points of the four spiral arms near 4 kpc (not a physical ring). An integrated (distance, velocity) model for the mass in the disk is employed, to yield the total mass of 3.0 × 10 11 M Sun within a galactic radius of 28 kpc.

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