The Distance to the Center of the Galaxy

Reid, M. J.; Schneps, M. H.; Moran, J. M.; Gwinn, C. R.; Genzel, R.; Downes, D.; Ronnang, B. O.

doi:10.1007/978-94-009-4782-5_169

Cited by 18 publications

(28 citation statements)

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“…The masers were assumed to have a uniform expansion velocity V exp away from IRc2, centred on an unknown radial velocity V z0 , plus solid body rotation corresponding to V rot at 1‐arcsec separation from IRc2. The rotation axis is tilted by an angle α about the y ‐axis and an angle β about the x ‐axis from the x – z plane (following Reid et al 1988). The parameters V exp , V z0 , V rot , α and β were the five unknowns.…”

Section: Discussionmentioning

confidence: 99%

Hydroxyl maser disc and outflow in the Orion-BN/KL region

Cohen¹,

Gasiprong²,

Meaburn³

et al. 2006

Monthly Notices of the Royal Astronomical Society

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Multi Element Radio Linked Interferometer Network (MERLIN) measurements of 1.6‐GHz hydroxyl (OH) masers associated with Orion‐Becklin–Neugebauer/Kleinmann–Low (Orion‐BN/KL) are presented, and the data are compared with data on other masers, molecular lines, compact radio continuum sources and infrared sources in the region. OH masers are detected over an area of 30 arcsec in diameter, with the majority lying along an approximately E–W structure that extends for ∼18 arcsec, encompassing the infrared sources IRc2, IRc6 and IRc7. Radial velocities range from −13 to +42 km s−1. The system of OH masers shows a velocity gradient together with non‐circular motions. The kinematics are modelled in terms of an expanding and rotating disc or torus. The rotation axis is found to be in the same direction as the molecular outflow. There is an inner cavity of radius ∼1300 au with no OH masers. The inner cavity, like the H2O ‘shell’ masers and SiO masers, is centred on radio source I. Some of the OH masers occur in velocity‐coherent strings or arcs that are longer than 5 arcsec (2250 au). One such feature, Stream A, is a linear structure at position angle ∼45°, lying between IRc2 and BN. We suggest that these masers trace shock fronts, and have appeared, like a vapour trail, 200 yr after the passage of the runaway star BN. The radio proper motions of BN, source I and source n project back to a region near the base of Stream A that is largely devoid of OH masers. The 1612‐MHz masers are kinematically distinct from the other OH masers. They are also more widely distributed and appear to be associated with the outflow as traced by H2O masers and by the 2.12‐μm emission from shocked H2. The magnetic field traced by the OH masers ranges from 1.8 to 16.3 mG, with a possible reversal. No OH masers were found associated with even the most prominent proplyds within 10 arcsec of θ1 Ori C.

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Section: Discussionmentioning

confidence: 99%

Hydroxyl maser disc and outflow in the Orion-BN/KL region

Cohen¹,

Gasiprong²,

Meaburn³

et al. 2006

Monthly Notices of the Royal Astronomical Society

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“…An approximate association of mass with spectral type is indicated in the upper horizontal axis (Cox 2000). The apparent K-band magnitudes are given for a plausible range of distance and extinction coefficient values: the top curve for the fiducial distance to the GC of R 0 =8 kpc (Reid 1993;Eisenhauer et al 2003) and K-band extinction of A K =3 mag (Rieke et al 1989), and the bottom curve for the more recent determination of R 0 = 7.62 kpc and A K = 2.8 mag. A rough estimate of the two-body relaxation time in the GC, t r ∼ 3 ×10 9 yr (Alexander 1999), the current detection limit in the K-band with the VLT (K =18 mag with completeness of 63%, Genzel et al 2003b) and the anticipated limit for the VLTI interferometer with adaptive optics (Paresce et al 2003) are also shown.…”

Section: The Central 100 Parsecsmentioning

confidence: 99%

“…The distance to the GC is also an important (though not the only) lower rung in the extragalactic distance scale, useful for calibrating standard candles such as RR Lyrae stars, Cepheids and red clump giants. Until recently, the adopted distance to the GC, R 0 = 8.0±0.5 kpc (Reid 1993) was based on the average of various primary (geometric), secondary (standard candles) and tertiary (theoretical models) distance indicators (see brief summary in Eisenhauer et al 2003). Geometric distance indicators are in principle the most reliable, if the assumptions about physical properties of the system used are well founded.…”

Section: Distance To the Galactic Centermentioning

confidence: 99%

Stellar processes near the massive black hole in the Galactic center

2005

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“…The differential event rate is directly proportional to the local WIMP density, ρ 0 ≡ ρ(r = R 0 ) where R 0 = (8.0 ± 0.5) kpc [11] is the solar radius. Any observational uncertainty in ρ 0 therefore translates directly into in an uncertainty in the event rate and the inferred constraints on, or measurements of, the scattering cross-sections.…”

Section: Astrophysics Input 31 Local Dm Densitymentioning

confidence: 99%

Direct detection of WIMPs

Cerdeño¹,

Green²

2010

Particle Dark Matter

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Citation for published item:gerde£ noD hFqF nd qreenD eFwF @PHIHA 9hiret detetion of swsF9D in rtile drk mtterX oservtionsD models nd serhesF gmridgeX gmridge niversity ressD ppF QRUEQTWF Further information on publisher's website: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. Abstract A generic weakly interacting massive particle (WIMP) is one of the most attractive candidates to account for the cold dark matter in our Universe, since it would be thermally produced with the correct abundance to account for the observed dark matter density. WIMPs can be searched for directly through their elastic scattering with a target material, and a variety of experiments are currently operating or planned with this aim. In these notes we overview the theoretical calculation of the direct detection rate of WIMPs as well as the different detection signals. We discuss the various ingredients (from particle physics and astrophysics) that enter the calculation and review the theoretical predictions for the direct detection of WIMPs in particle physics models.

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The Distance to the Center of the Galaxy

Cited by 18 publications

References 0 publications

Hydroxyl maser disc and outflow in the Orion-BN/KL region

Hydroxyl maser disc and outflow in the Orion-BN/KL region

Stellar processes near the massive black hole in the Galactic center

Direct detection of WIMPs

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